FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Tomsick, JA Gotthelf, EV Rahoui, F Assef, RJ Bauer, FE Bodaghee, A Boggs, SE Christensen, FE Craig, WW Fornasini, FM Grindlay, J Hailey, CJ Harrison, FA Krivonos, R Natalucci, L Stern, D Zhang, WW AF Tomsick, John A. Gotthelf, Eric V. Rahoui, Farid Assef, Roberto J. Bauer, Franz E. Bodaghee, Arash Boggs, Steven E. Christensen, Finn E. Craig, William W. Fornasini, Francesca M. Grindlay, Jonathan Hailey, Charles J. Harrison, Fiona A. Krivonos, Roman Natalucci, Lorenzo Stern, Daniel Zhang, William W. TI NuSTAR J163433-4738.7: A FAST X-RAY TRANSIENT IN THE GALACTIC PLANE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: stellar content; stars: variables: general; surveys; X-rays: individual NuSTAR J1634334738.7); X-rays: stars ID MILKY-WAY; BINARIES; SUPERFLARE; EVOLUTION; CATALOG; MISSION; GALAXY; SWIFT; FLARE; WIND AB During hard X-ray observations of the Norma spiral arm region by the Nuclear Spectroscopic Telescope Array (NuSTAR) in 2013 February, a new transient source, NuSTAR J163433-4738.7, was detected at a significance level of 8s in the 3-10 keV bandpass. The source is consistent with having a constant NuSTAR count rate over a period of 40 ks and is also detected simultaneously by Swift at lower significance. The source is not significantly detected by NuSTAR, Swift, or Chandra in the days before or weeks after the discovery of the transient, indicating that the strong X-ray activity lasted between similar to 0.5 and 1.5 days. Near-infrared imaging observations were carried out before and after the X-ray activity, but we are not able to identify the counterpart. The combined NuSTAR and Swift energy spectrum is consistent with a power law with a photon index of Gamma = 4.1(-1.0)(+1.5) (90% confidence errors), a blackbody with kT = 1.2 +/- 0.3 keV, or a Bremsstrahlung model with kT = 3.0(-1.2)(+2.1) keV. The reduced-chi(2) values for the three models are not significantly different, ranging from 1.23 to 1.44 for 8 degrees of freedom. The spectrum is strongly absorbed with N-Pi = (2.8(-1.4)(+2.3)) x 10(23) cm(-2), (9(-7)(+15)) x 10(22) cm(-2), and (1.7(-0.9)(+1.7)) x 10(23) cm(-2), for the power-law, blackbody, and Bremsstrahlung models, respectively. Although the high column density could be due to material local to the source, it is consistent with absorption from interstellar material along the line of sight at a distance of 11 kpc, which would indicate an X-ray luminosity >10(34) erg s(-1). Although we do not reach a definitive determination of the nature of NuSTAR J163433-4738.7, we suggest that it may be an unusually bright active binary or a magnetar. C1 [Tomsick, John A.; Bodaghee, Arash; Boggs, Steven E.; Craig, William W.; Fornasini, Francesca M.; Krivonos, Roman] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Gotthelf, Eric V.; Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Rahoui, Farid] European So Observ, D-85748 Garching, Germany. [Rahoui, Farid] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Assef, Roberto J.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. [Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Fornasini, Francesca M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Grindlay, Jonathan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Natalucci, Lorenzo] INAF IAPS, Ist Nazl Astrofis, I-00133 Rome, Italy. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tomsick, JA (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM jtomsick@ssl.berkeley.edu RI Boggs, Steven/E-4170-2015 OI Boggs, Steven/0000-0001-9567-4224 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; Gemini-CONICYT [32120009]; Basal-CATA [PFB-06/2007]; CONICYT-Chile through FONDECYT [1101024]; CONICYT-Chile through Gemini-CONICYT [32120003]; CONICYT-Chile through Anillo [ACT1101]; Italian Space Agency (ASI) by ASI/INAF grant [I/037/12/0-011/13] 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 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 (NuSTARDAS) jointly developed by the ASI Science Data Center (Italy) and the California Institute of Technology (USA). R.J.A. was supported by Gemini-CONICYT grant 32120009. F.E.B. was supported by Basal-CATA PFB-06/2007 and CONICYT-Chile (through FONDECYT 1101024, Gemini-CONICYT 32120003, and Anillo ACT1101). L.N. wishes to acknowledge the Italian Space Agency (ASI) for financial support by ASI/INAF grant I/037/12/0-011/13. The authors thank Harvey Tananbaum for providing Chandra Director's Discretionary Time for this project. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 36 TC 2 Z9 2 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 4 DI 10.1088/0004-637X/785/1/4 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300004 ER PT J AU Williams, PKG Cook, BA Berger, E AF Williams, P. K. G. Cook, B. A. Berger, E. TI TRENDS IN ULTRACOOL DWARF MAGNETISM. I. X-RAY SUPPRESSION AND RADIO ENHANCEMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; radio continuum: stars; stars: activity; stars: coronae; X-rays: stars ID LOW-MASS STARS; SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; ACTIVITY-ROTATION RELATIONSHIP; NEAR-INFRARED SPECTROSCOPY; ELECTRON-CYCLOTRON MASER; FULLY CONVECTIVE STARS; H-ALPHA OBSERVATIONS; MAIN-SEQUENCE STARS; PROPER-MOTION STARS; BINARY BROWN DWARF AB Although ultracool dwarfs (UCDs) are now known to generate and dissipate strong magnetic fields, a clear understanding of the underlying dynamo is still lacking. We have performed X-ray and radio observations of seven UCDs in a narrow range of spectral type (M6.5-M9.5) but spanning a wide range of projected rotational velocities (v sin i approximate to 3-40 km s(-1)). We have also analyzed unpublished archival Chandra observations of four additional objects. All of the newly observed targets are detected in the X-ray, while only one is detected in the radio, with the remainder having sensitive upper limits. We present a database of UCDs with both radio and X-ray measurements and consider the data in light of the so-called Gudel-Benz relation (GBR) between magnetic activity in these bands. Some UCDs have very bright radio emission and faint X-ray emission compared to what would be expected for rapid rotators, while others show the opposite behavior. We show that UCDs would still be radio-overluminous relative to the GBR even if their X-ray emission were at standard rapid-rotator "saturation" levels. Recent results from Zeeman-Doppler imaging and geodynamo simulations suggest that rapidly rotating UCDs may harbor a bistable dynamo that supports either a stronger, axisymmetric magnetic field or a weaker, non-axisymmetric field. We suggest that the data can be explained in a scenario in which strong-field objects obey the GBR while weak-field objects are radio-overluminous and X-ray-underluminous, possibly because of a population of gyrosynchrotron-emitting coronal electrons that is continuously replenished by low-energy reconnection events. C1 [Williams, P. K. G.; Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cook, B. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Williams, PKG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pwilliams@cfa.harvard.edu FU National Science Foundation REU and Department of Defense ASSURE programs under NSF [1262851]; Smithsonian Institution; National Science Foundation [AST-1008361]; National Aeronautics and Space Administration through Chandra Award [GO2-13007A]; National Aeronautics Space Administration [NAS8-03060] FX We thank Scott Wolk and Katja Poppenhaeger for enlightening discussions. We also thank the anonymous referee for helpful, constructive comments. This work is supported in part by the National Science Foundation REU and Department of Defense ASSURE programs under NSF Grant no. 1262851 and by the Smithsonian Institution. E.B. and P.K.G.W. acknowledge support for this work from the National Science Foundation through Grant AST-1008361, and from the National Aeronautics and Space Administration through Chandra Award Number GO2-13007A 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. 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. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and NASA's Astrophysics Data System. NR 157 TC 24 Z9 24 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 9 DI 10.1088/0004-637X/785/1/9 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300009 ER PT J AU Archambault, S Aune, T Behera, B Beilicke, M Benbow, W Berger, K Bird, R Biteau, J Bugaev, V Byrum, K Cardenzana, JV Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fleischhack, H Fortson, L Furniss, A Galante, N Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Johnson, CA Kaaret, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Kumar, S Lang, MJ Madhavan, AS Maier, G McCann, A Meagher, K Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Park, N Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Rajotte, J Reyes, LC Reynolds, PT Richards, GT Roache, E Sembroski, GH Shahinyan, K Staszak, D Telezhinsky, I Tucci, JV Tyler, J Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Weinstein, A Welsing, R Wilhelm, A Williams, DA Ackermann, M Ajello, M Albert, A Baldini, L Bastieri, D Bellazzini, R Bissaldi, E Bregeon, J Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cavazzuti, E Charles, E Chiang, J Ciprini, S Claus, R Cutini, S D'Ammando, F de Angelis, A de Palma, F Dermer, CD Digel, SW Di Venere, L Drell, PS Favuzzi, C Franckowiak, A Fusco, P Gargano, F Gasparrini, D Giglietto, N Giordano, F Giroletti, M Grenier, IA Guiriec, S Jogler, T Kuss, M Larsson, S Latronico, L Longo, F Loparco, F Lubrano, P Madejski, GM Mayer, M Mazziotta, MN Michelson, PF Mizuno, T Monzani, ME Morselli, A Murgia, S Nuss, E Ohsugi, T Ormes, JF Paneque, D Perkins, JS Piron, F Pivato, G Raino, S Razzano, M Reimer, A Reimer, O Ritz, S Schaal, M Sgro, C Siskind, EJ Spinelli, P Takahashi, H Tibaldo, L Tinivella, M Troja, E Vianello, G Werner, M Wood, M AF Archambault, S. Aune, T. Behera, B. Beilicke, M. Benbow, W. Berger, K. Bird, R. Biteau, J. Bugaev, V. Byrum, K. Cardenzana, J. V. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fleischhack, H. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Johnson, C. A. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Kumar, S. Lang, M. J. Madhavan, A. S. Maier, G. McCann, A. Meagher, K. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Rajotte, J. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Sembroski, G. H. Shahinyan, K. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Weinstein, A. Welsing, R. Wilhelm, A. Williams, D. A. Ackermann, M. Ajello, M. Albert, A. Baldini, L. Bastieri, D. Bellazzini, R. Bissaldi, E. Bregeon, J. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cavazzuti, E. Charles, E. Chiang, J. Ciprini, S. Claus, R. Cutini, S. D'Ammando, F. de Angelis, A. de Palma, F. Dermer, C. D. Digel, S. W. Di Venere, L. Drell, P. S. Favuzzi, C. Franckowiak, A. Fusco, P. Gargano, F. Gasparrini, D. Giglietto, N. Giordano, F. Giroletti, M. Grenier, I. A. Guiriec, S. Jogler, T. Kuss, M. Larsson, S. Latronico, L. Longo, F. Loparco, F. Lubrano, P. Madejski, G. M. Mayer, M. Mazziotta, M. N. Michelson, P. F. Mizuno, T. Monzani, M. E. Morselli, A. Murgia, S. Nuss, E. Ohsugi, T. Ormes, J. F. Paneque, D. Perkins, J. S. Piron, F. Pivato, G. Raino, S. Razzano, M. Reimer, A. Reimer, O. Ritz, S. Schaal, M. Sgro, C. Siskind, E. J. Spinelli, P. Takahashi, H. Tibaldo, L. Tinivella, M. Troja, E. Vianello, G. Werner, M. Wood, M. CA VERITAS Collaboration Fermi LAT Collaboration TI DEEP BROADBAND OBSERVATIONS OF THE DISTANT GAMMA-RAY BLAZAR PKS 1424+240 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE BL Lacertae objects: individual (PKS 1424+240)-cosmic background radiation; gamma rays: galaxies ID EXTRAGALACTIC BACKGROUND LIGHT; SPACE-TELESCOPE MISSION; LARGE-AREA TELESCOPE; ENERGY COSMIC-RAY; TEV BLAZARS; SPECTRA; REDSHIFT; ABSORPTION; RADIATION; UNIVERSE AB We present deep VERITAS observations of the blazar PKS 1424+240, along with contemporaneous Fermi Large Area Telescope, Swift X-ray Telescope, and Swift UV Optical Telescope data between 2009 February 19 and 2013 June 8. This blazar resides at a redshift of z >= 0.6035, displaying a significantly attenuated gamma-ray flux above 100 GeV due to photon absorption via pair-production with the extragalactic background light. We present more than 100 hr of VERITAS observations over three years, a multiwavelength light curve, and the contemporaneous spectral energy distributions. The source shows a higher flux of (2.1 +/- 0.3) x 10(-7) photons m(-2) s(-1) above 120 GeV in 2009 and 2011 as compared to the flux measured in 2013, corresponding to (1.02 +/- 0.08) x 10-7 photons m(-2) s(-1) above 120 GeV. The measured differential very high energy (VHE; E >= 100 GeV) spectral indices are Gamma = 3.8 +/- 0.3, 4.3 +/- 0.6 and 4.5 +/- 0.2 in 2009, 2011, and 2013, respectively. No significant spectral change across the observation epochs is detected. We find no evidence for variability at gamma-ray opacities of greater than tau = 2, where it is postulated that any variability would be small and occur on timescales longer than a year if hadronic cosmic-ray interactions with extragalactic photon fields provide a secondary VHE photon flux. The data cannot rule out such variability due to low statistics. C1 [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Aune, T.; Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Behera, B.; Chen, X.; Federici, S.; Fleischhack, H.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.; Wilhelm, A.] DESY, D-15738 Zeuthen, Germany. [Beilicke, M.; Bugaev, V.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Galante, N.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Biteau, J.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Biteau, J.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Byrum, K.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cardenzana, J. V.; Krennrich, F.; Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Federici, S.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Griffiths, S. T.; Kaaret, P.] Stanford Univ, SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Humensky, T. B.; Nieto, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kieda, D.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [McCann, A.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Moriarty, P.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Moriarty, P.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Park, N.; Wakely, S. P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Reyes, L. C.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Reynolds, P. T.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Furniss, A.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Ackermann, M.; Buehler, R.; Mayer, M.] DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Albert, A.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Franckowiak, A.; Jogler, T.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Reimer, A.; Reimer, O.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Albert, A.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Franckowiak, A.; Jogler, T.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Reimer, A.; Reimer, O.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.; Bellazzini, R.; Kuss, M.; Razzano, M.; Sgro, C.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bastieri, D.; Buson, S.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Pivato, G.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bissaldi, E.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Bissaldi, E.] Univ Trieste, I-34127 Trieste, Italy. [Bregeon, J.; Nuss, E.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France. [Caliandro, G. A.] CIFS, I-10133 Turin, Italy. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Rome, Italy. [D'Ammando, F.; Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Dermer, C. D.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Grenier, I. A.] Univ Paris Diderot, CNRS, CEA IRFU, CEA Saclay,Lab AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Guiriec, S.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Guiriec, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Larsson, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Larsson, S.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Latronico, L.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Longo, F.; Lubrano, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Lubrano, P.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Morselli, A.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA. [Murgia, S.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Ormes, J. F.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Razzano, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Razzano, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.; Werner, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Reimer, A.; Reimer, O.; Werner, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ritz, S.] Natl Acad Sci, Natl Res Council, Res Associate, Washington, DC 20001 USA. [Schaal, M.; Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. Univ Maryland, Dept Phys, College Pk, MD 20742 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Archambault, S (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM amy.furniss@gmail.com RI Reimer, Olaf/A-3117-2013; Bissaldi, Elisabetta/K-7911-2016; Di Venere, Leonardo/C-7619-2017; Morselli, Aldo/G-6769-2011; Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Sgro, Carmelo/K-3395-2016; OI Reimer, Olaf/0000-0001-6953-1385; Bissaldi, Elisabetta/0000-0001-9935-8106; Di Venere, Leonardo/0000-0003-0703-824X; Cui, Wei/0000-0002-6324-5772; Morselli, Aldo/0000-0002-7704-9553; Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Bastieri, Denis/0000-0002-6954-8862; Giroletti, Marcello/0000-0002-8657-8852; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the UK; NASA through the Space Telescope Science Institute [HST-GO-12863]; NASA [NAS 5-26555]; INAF in Italy; CNES in France FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution; by NSERC in Canada; by Science Foundation Ireland (SFI 10/RFP/AST2748); and by STFC in the 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.; Support for program HST-GO-12863 was provided by NASA, awarded through the Space Telescope Science Institute, operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555.; The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States; CEA/Irfu and IN2P3/CNRS in France; ASI and INFN in Italy; MEXT, KEK, and JAXA in Japan; and the K. A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. NR 50 TC 19 Z9 19 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 10 PY 2014 VL 785 IS 1 AR L16 DI 10.1088/2041-8205/785/1/L16 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE9RA UT WOS:000334345000016 ER PT J AU Banerjee, DPK Joshi, V Venkataraman, V Ashok, NM Marion, GH Hsiao, EY Raj, A AF Banerjee, D. P. K. Joshi, Vishal Venkataraman, V. Ashok, N. M. Marion, G. H. Hsiao, E. Y. Raj, A. TI NEAR-IR STUDIES OF RECURRENT NOVA V745 SCORPII DURING ITS 2014 OUTBURST SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE infrared: stars; novae, cataclysmic variables; stars: individual (V745 Scorpii); techniques: spectroscopic ID RS-OPHIUCHI; SYMBIOTIC STARS; RAY-EMISSION; LIGHT-CURVE; V407 CYG; SYSTEMS; SPECTRA; EJECTA AB The recurrent nova V745 Scorpii underwent its third known outburst on 2014 February 6. Infrared monitoring of the eruption on an almost daily basis, starting from 1.3 days after discovery, shows the emergence of a powerful blast wave generated by the high velocity nova ejecta exceeding 4000 km s(-1) plowing into its surrounding environment. The temperature of the shocked gas is raised to a high value exceeding 10(8) K immediately after outburst commencement. The energetics of the outburst clearly surpass those of similar symbiotic systems like RS Oph and V407 Cyg which have giant secondaries. The shock does not show a free-expansion stage but rather shows a decelerative Sedov-Taylor phase from the beginning. Such strong shock fronts are known to be sites for. gamma-ray generation. V745 Sco is the latest nova, apart from five other known novae, to show. gamma-ray emission. It may be an important testbed to resolve the crucial question of whether or not all novae are generically. gamma-ray emitters by virtue of having a circumbinary reservoir of material that is shocked by the ejecta rather than. gamma-ray generation being restricted to only symbiotic systems with a shocked red giant (RG) wind. The lack of a free-expansion stage favors V745 Sco to have a density enhancement around the white dwarf (WD), above that contributed by a RG wind. Our analysis also suggests that the WD in V745 Sco is very massive and a potential progenitor for a future SN Ia explosion. C1 [Banerjee, D. P. K.; Joshi, Vishal; Venkataraman, V.; Ashok, N. M.; Raj, A.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. [Marion, G. H.] Univ Texas Austin, Austin, TX 78712 USA. [Marion, G. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hsiao, E. Y.] Carnegie Observ, Las Campanas Observ, Colina El Pino 601, Casilla, Chile. RP Banerjee, DPK (reprint author), Phys Res Lab, Ahmadabad 380009, Gujarat, India. EM orion@prl.res.in FU Department of Space, Government of India; NSF [AST-1211196] FX Research at PRL is supported by the Department of Space, Government of India. G. H. M. thanks D. Osip, P. Palunas, Y. Beletsky, and the engineering group at the Las Campanas Observatory for their support of observations. The CfA Supernova Program is supported by NSF grant AST-1211196 to the Harvard College Observatory. We thank the reviewer Professor Ulisse Munari for helpful comments. NR 40 TC 15 Z9 15 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 10 PY 2014 VL 785 IS 1 AR L11 DI 10.1088/2041-8205/785/1/L11 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE9RA UT WOS:000334345000011 ER PT J AU Morfeld, KA Lehnhardt, J Alligood, C Bolling, J Brown, JL AF Morfeld, Kari A. Lehnhardt, John Alligood, Christina Bolling, Jeff Brown, Janine L. TI Development of a Body Condition Scoring Index for Female African Elephants Validated by Ultrasound Measurements of Subcutaneous Fat SO PLOS ONE LA English DT Article ID HOLSTEIN DAIRY-COWS; ZOO ELEPHANTS; REPRODUCTIVE DISORDERS; HORMONE CONCENTRATIONS; BLUBBER THICKNESS; CONDITION SCORES; NORTH-AMERICA; OBESITY; WOMEN; HORSES AB Obesity-related health and reproductive problems may be contributing to non-sustainability of zoo African elephant (Loxodonta africana) populations. However, a major constraint in screening for obesity in elephants is lack of a practical method to accurately assess body fat. Body condition scoring (BCS) is the assessment of subcutaneous fat stores based on visual evaluation and provides an immediate appraisal of the degree of obesity of an individual. The objective of this study was to develop a visual BCS index for female African elephants and validate it using ultrasound measures of subcutaneous fat. To develop the index, standardized photographs were collected from zoo (n = 50) and free-ranging (n = 57) female African elephants for identifying key body regions and skeletal features, which were then used to visually determine body fat deposition patterns. This information was used to develop a visual BCS method consisting of a list of body regions and the physical criteria for assigning an overall score on a 5-point scale, with 1 representing the lowest and 5 representing the highest levels of body fat. Results showed that as BCS increased, ultrasound measures of subcutaneous fat thickness also increased (P<0.01), indicating the scores closely coincide with physical measures of fat reserves. The BCS index proved to be reliable and repeatable based on high intra- and inter-assessor agreement across three assessors. In comparing photographs of wild vs. captive African elephants, the median BCS in the free-ranging individuals (BCS = 3, range 1-5) was lower (P<0.001) than that of the zoo population (BCS = 4, range 2-5). In sum, we have developed the first validated BCS index for African elephants. This tool can be used to examine which factors impact body condition in zoo and free-ranging elephants, providing valuable information on how it affects health and reproductive potential of individual elephants. C1 [Morfeld, Kari A.; Brown, Janine L.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Roya, VA USA. [Lehnhardt, John; Bolling, Jeff] Natl Elephant Ctr, Fellsmere, FL USA. [Alligood, Christina] Disneys Anim Kingdom, Bay Lake, FL USA. RP Morfeld, KA (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Roya, VA USA. EM morfeldk@si.edu FU Morris Animal Foundation; Shared Earth Foundation; FBB Capital Partners; Wolcott Fund; Siemens Medical Solutions Diagnostics FX Morris Animal Foundation, Shared Earth Foundation, FBB Capital Partners, Wolcott Fund, Siemens Medical Solutions Diagnostics. The funders had no role in the study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 68 TC 7 Z9 7 U1 5 U2 23 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 9 PY 2014 VL 9 IS 4 AR e93802 DI 10.1371/journal.pone.0093802 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AE9PC UT WOS:000334339000047 PM 24718304 ER PT J AU Toth, AB Lyons, SK Behrensmeyer, AK AF Toth, Aniko B. Lyons, S. Kathleen Behrensmeyer, Anna K. TI A Century of Change in Kenya's Mammal Communities: Increased Richness and Decreased Uniqueness in Six Protected Areas SO PLOS ONE LA English DT Article ID SPATIALLY EXPLICIT; HABITAT LOSS; HYDE 3.1; CONSERVATION; DYNAMICS; DISTRIBUTIONS; ASSEMBLAGES; POPULATION; EXTINCTION; SERENGETI AB The potential for large-scale biodiversity losses as a result of climate change and human impact presents major challenges for ecology and conservation science. Governments around the world have established national parks and wildlife reserves to help protect biodiversity, but there are few studies on the long-term consequences of this strategy. We use Kenya as a case study to investigate species richness and other attributes of mammal communities in 6 protected areas over the past century. Museum records from African expeditions that comprehensively sampled mammals from these same areas in the early 1900's provide a baseline for evaluating changes in species richness and community structure over time. We compare species lists assembled from archived specimens (1896-1950) to those of corresponding modern protected areas (19502013). Species richness in Kenya was stable or increased at 5 out of 6 sites from historical to modern times. Beta-diversity, in contrast, decreased across all sites. Potential biases such as variable historical vs. modern collection effort and detection of small-bodied, rare, and low-visibility species do not account for the observed results. We attribute the pattern of decreased beta diversity primarily to increased site occupancy by common species across all body size classes. Despite a decrease in land area available to wildlife, our data do not show the extinctions predicted by species-area relationships. Moreover, the results indicate that species-area curves based solely on protected areas could underestimate diversity because they do not account for mammal species whose ranges extend beyond protected area boundaries. We conclude that the 6 protected areas have been effective in preserving species richness in spite of continuing conversion of wild grasslands to cropland, but the overall decrease in beta diversity indicates a decline in the uniqueness of mammal communities that historically characterized Kenya's varied landscape. C1 [Toth, Aniko B.; Lyons, S. Kathleen; Behrensmeyer, Anna K.] Smithsonian Inst Washington, Natl Museum Nat Hist, Dept Paleobiol, Evolut Terr Ecosyst Program, Washington, DC 20560 USA. RP Toth, AB (reprint author), Smithsonian Inst Washington, Natl Museum Nat Hist, Dept Paleobiol, Evolut Terr Ecosyst Program, Washington, DC 20560 USA. EM totha@si.edu FU National Museum of Natural History internal grant FX This project was supported by a National Museum of Natural History internal grant to the Evolution of Terrestrial Ecosystems Program. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 52 TC 3 Z9 3 U1 1 U2 23 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 9 PY 2014 VL 9 IS 4 AR e93092 DI 10.1371/journal.pone.0093092 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AE9PC UT WOS:000334339000027 PM 24718262 ER PT J AU Glowska, E Schmidt, BK AF Glowska, Eliza Schmidt, Brian K. TI New quill mites (Cheyletoidea: Syringophilidae) parasitizing the black-headed paradise-flycatcher Terpsiphone rufiventer (Passeriformes: Monarchidae) in Gabon SO ZOOTAXA LA English DT Article DE Quill mites; Syringophilidae; Pipicobia; Syringophiloidus; monarchid birds; systematics ID GENUS PICOBIA HALLER; ACARI SYRINGOPHILIDAE; BIRDS; PROSTIGMATA; ACARIFORMES; PASSERINES; RECORDS AB A new genus of quill mites (Cheyletoidea: Syringophilidae) and two new species Pipicobia terpsiphoni gen. nov. and sp. nov. and Syringophiloidus furthi sp. nov. parasitizing the black-headed paradise-flycatcher Terpsiphone rufiventer (Swainson) (Passeriformes: Monarchidae) in Gabon are described. Three species of the Neopicobia Skoracki, 2011 are moved to the newly established genus: Pipicobia locustella (Skoracki, Bochkov and Wauthy, 2004) comb. nov., Pipicobia pyrrholaemus (Skoracki and Glowska, 2008) comb. nov., and Pipicobia glossopsitta (Skoracki, Glowska and Sikora, 2008) comb. nov. Syringophilids are recorded on hosts of the family Monarchidae and in Gabon for the first time. A key to the genera of the subfamily Picobiinae is proposed. C1 [Glowska, Eliza] Adam Mickiewicz Univ, Fac Biol, Dept Anim Morphol, PL-61614 Poznan, Poland. [Schmidt, Brian K.] Smithsonian Inst, Div Birds, Washington, DC 20013 USA. RP Glowska, E (reprint author), Adam Mickiewicz Univ, Fac Biol, Dept Anim Morphol, Umultowska 89, PL-61614 Poznan, Poland. EM glowska@amu.edu.pl FU Smithsonian Institution Monitoring and Assessment of Biodiversity (SI-MAB) programme; Shell Foundation; Shell Gabon; Government of Gabon FX We are very grateful to the staff of the Department of Vertebrate Zoology, Division of Birds, USNM for making the collection of feathers available for this study. The collection of the bird specimens was supported by the Smithsonian Institution Monitoring and Assessment of Biodiversity (SI-MAB) programme, the Shell Foundation, Shell Gabon, and the Government of Gabon. NR 17 TC 13 Z9 13 U1 0 U2 6 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD APR 8 PY 2014 VL 3786 IS 1 BP 57 EP 64 PG 8 WC Zoology SC Zoology GA AE3RC UT WOS:000333892900003 PM 24869522 ER PT J AU Wolfe, E Yelin, SF AF Wolfe, Elie Yelin, S. F. TI Certifying Separability in Symmetric Mixed States of N Qubits, and Superradiance SO PHYSICAL REVIEW LETTERS LA English DT Article ID ENTANGLEMENT; SYSTEMS AB Separability criteria are typically of the necessary, but not sufficient, variety, in that satisfying some separability criterion, such as positivity of eigenvalues under partial transpose, does not strictly imply separability. Certifying separability amounts to proving the existence of a decomposition of a target mixed state into some convex combination of separable states; determining the existence of such a decomposition is "hard." We show that it is effective to ask, instead, if the target mixed state "fits" some preconstructed separable form, in that one can generate a sufficient separability criterion relevant to all target states in some family by ensuring enough degrees of freedom in the preconstructed separable form. We demonstrate this technique by inducing a sufficient criterion for "diagonally symmetric" states of N qubits. A sufficient separability criterion opens the door to study precisely how entanglement is (not) formed; we use ours to prove that, counterintuitively, entanglement is not generated in idealized Dicke model superradiance despite its exemplification of many-body effects. We introduce a quantification of the extent to which a given preconstructed parametrization comprises the set of all separable states; for "diagonally symmetric" states our preconstruction is shown to be fully complete. This implies that our criterion is necessary in addition to sufficient, among other ramifications which we explore. C1 [Wolfe, Elie; Yelin, S. F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Yelin, S. F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Wolfe, E (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. EM wolfe@phys.uconn.edu RI Wolfe, Elie/F-7888-2014 OI Wolfe, Elie/0000-0002-6960-3796 FU NSF; AFOSR FX We thank Szilard Szalay of Budapest University for feedback on phrasing and notation. We wish to thank the NSF and the AFOSR for funding. NR 23 TC 7 Z9 7 U1 0 U2 5 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 APR 7 PY 2014 VL 112 IS 14 AR 140402 DI 10.1103/PhysRevLett.112.140402 PG 5 WC Physics, Multidisciplinary SC Physics GA AL9VL UT WOS:000339490700002 PM 24765924 ER PT J AU Herranz, M Boyle, MJ Pardos, F Neves, RC AF Herranz, Maria Boyle, Michael J. Pardos, Fernando Neves, Ricardo C. TI Comparative myoanatomy of Echinoderes (Kinorhyncha): a comprehensive investigation by CLSM AND 3D reconstruction SO FRONTIERS IN ZOOLOGY LA English DT Article DE Ecdysozoa; Scalidophora; Segmentation; Phalloidin; Organ system; Circular muscle; Introvert; Pharynx ID POSTEMBRYONIC DEVELOPMENT; PHYLOGENETIC-RELATIONSHIPS; COMPARATIVE MORPHOLOGY; IDENTIFICATION KEYS; NERVOUS-SYSTEM; SISTER-GROUP; CYCLORHAGIDA; ARTHROPODS; ECDYSOZOA; ULTRASTRUCTURE AB Introduction: Kinorhyncha is a clade of marine invertebrate meiofauna. Their body plan includes a retractable introvert bearing rings of cuticular spines, and a limbless trunk with distinct segmentation of nervous, muscular and epidermal organ systems. As derived members within the basal branch of Ecdysozoa, kinorhynchs may provide an important example of convergence on the evolution of segmentation within one of three bilaterian superclades. We describe the myoanatomy of Echinoderes, the most specious kinorhynch genus, and build upon historical studies of kinorhynch ultrastructure and gross morphology. This is the first multi-species comparison of a complete organ system by confocal microscopy and three-dimensional reconstruction within Kinorhyncha. Results: Myoanatomy of adult Echinoderes is composed of the following: Head with two mouth cone circular muscles, nine pairs of oral style muscles, ten introvert retractors, one introvert circular muscle, and fourteen introvert circular muscle retractors; Neck with one circular muscle; Trunk showing distinct pairs of ventral and dorsal muscles within segments 1-10, dorsoventral muscles within segments 3-10, diagonal muscles within segments 1-8, longitudinal fibers spanning segments 1-9, three pairs of terminal spine muscles, and one pair of male penile spine muscles; Gut showing a pharynx with ten alternating rings of radial and circular muscle fibers enclosed in a complex sheath of protractors and retractors, an orthogonal grid of longitudinal and circular fibers surrounding the intestine, and paired hindgut dilators. Conclusions: Myoanatomy is highly conserved between species of Echinoderes. Interspecific variation is observed in the arrangement and number of introvert fibers and the composition of pharyngeal muscles. Segmented trunk musculature facilitates the movements of articulated cuticular plates along the anterior-posterior axis. Intersegmental muscle fibers assist with dorsoventral and lateral trunk movements. Protractors, retractors and circular muscles coordinate eversion and retraction of the introvert and mouth cone, and relocation of the pharynx during locomotion and feeding behaviors. Pairs of posterior fibers suggest independent movements of terminal spines, and male penile spines. Within Scalidophora, myoanatomy is more similar between Kinorhyncha and Loricifera, than either group is to Priapulida. Kinorhynch myoanatomy may reflect a convergent transition from vermiform to segmented body plans during the early radiation of Ecdysozoa. C1 [Herranz, Maria; Pardos, Fernando] Univ Complutense Madrid, Fac Biol, Dpto Zool & Antropol Fis Zool Invertebrados, E-28040 Madrid, Spain. [Boyle, Michael J.] Smithsonian Trop Res Inst, Naos Marine Labs, Panama City 084303092, Panama. [Neves, Ricardo C.] Univ Basel, Biozentrum, CH-4056 Basel, Switzerland. RP Herranz, M (reprint author), Univ Complutense Madrid, Fac Biol, Dpto Zool & Antropol Fis Zool Invertebrados, C Jose Antonio Novais 2, E-28040 Madrid, Spain. EM mariaherranz@bio.ucm.es RI HERRANZ, MARIA/J-8042-2014; Neves, Ricardo/J-9822-2014; OI PARDOS MARTINEZ, FERNANDO/0000-0002-6292-9793 FU Ministerio de Ciencia y Tecnolog a, Government of Spain [2009-08928]; Smithsonian Institution/Link Foundation Graduate Fellowship; ASSEMBLE [227799] FX MH is grateful to Dr. Mary Rice and Dr. Jon Norenburg for sponsorship and scientific advisement, and to Dr. Valerie Paul and technical staff at the Smithsonian Marine Station at Fort Pierce (SMSFP). We acknowledge technical and field staff at CCMAR (Portugal). MH is very grateful to Dr. Heinrich Reichert, and staff at the Imaging Core Facility at Biozentrum, University of Basel (Switzerland). Dr. Reinhardt Mobjerg Kristensen generously loaned us unpublished TEM images. Part of this research was funded by Project CGL 2009-08928 (Ministerio de Ciencia y Tecnologia, Government of Spain) to FP. Field collection, imaging and research in Florida (USA) was funded by a Smithsonian Institution/Link Foundation Graduate Fellowship to MH. Field collection and imaging in Faro (Portugal) was funded by ASSEMBLE Grant No. 227799 to RCN and MH. This publication is Smithsonian Marine Station contribution no. 948. NR 60 TC 6 Z9 6 U1 2 U2 12 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1742-9994 J9 FRONT ZOOL JI Front. Zool. PD APR 5 PY 2014 VL 11 AR 31 DI 10.1186/1742-9994-11-31 PG 26 WC Zoology SC Zoology GA AF2HN UT WOS:000334533300001 PM 24708877 ER PT J AU Faynel, C Robbins, RK AF Faynel, Christophe Robbins, Robert K. TI New Lycaenidae from the inselberg of the Nouragues and from Kaw Mountain in French Guiana (Lepidoptera: Theclinae: Eumaeini) SO ANNALES DE LA SOCIETE ENTOMOLOGIQUE DE FRANCE LA French DT Article DE Siderus philinna; Siderus giapor; Butterflies; Reserve Naturelle des Nouragues; rock-savanna; Nicolaea castinotus; Ostrinotes empusa; Ostrinotes purpuriticus; Nicolaea cupa AB R < span class="greekletter"> e sum < span class="greekletter"> e Dans le cadre de l'inventaire des Eumaeini de Guyane (Lycaenidae, Theclinae), trois nouvelles especes sont decrites: Siderus nouraguensis n. sp., Nicolaea salki n. sp. et Ostrinotes silva n. sp. Elles appartiennent a des genres differents regroupes dans la section Tmolus de la tribu des Eumaeini. La premiere espece provient de la Reserve Naturelle des Nouragues (ONF/CNRS). Elle a ete capturee au sommet de l'inselberg dans un biotope tres particulier (savane-roche) et pourrait etre infeodee a cette vegetation typique basse et xerophile poussant sur la roche. En plus d'etre ecologiquement inhabituelle, cette espece est morphologiquement insolite puisque c'est la seule dans ce groupe dont les genitalia male possedent des soies sur la partie dorsale du vinculum. Les deux autres especes ont ete capturees dans la foret primaire de la montagne de Kaw mais egalement dans d'autres pays d'Amerique du Sud. C1 [Faynel, Christophe] Soc Entomol Antilles Guyane, F-34160 Montaud, France. [Robbins, Robert K.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Faynel, C (reprint author), Soc Entomol Antilles Guyane, 16 Rue Aspres, F-34160 Montaud, France. EM christophe.faynel@wanadoo.fr NR 26 TC 1 Z9 1 U1 1 U2 7 PU SOC ENTOMOLOGIQUE FRANCE PI PARIS PA 45 RUE BUFFON, 75005 PARIS, FRANCE SN 0037-9271 EI 2168-6351 J9 ANN SOC ENTOMOL FR JI Ann. Soc. Entomol. Fr. PD APR 3 PY 2014 VL 50 IS 2 BP 191 EP 201 DI 10.1080/00379271.2014.934040 PG 11 WC Entomology SC Entomology GA AT3UU UT WOS:000344861700008 ER PT J AU Jerep, FC Malabarba, LR AF Jerep, Fernando C. Malabarba, Luiz R. TI A new species of Serrapinnus Malabarba, 1998 (Characidae: Cheirodontinae) from Rio Grande do Norte State, northeastern Brazil SO NEOTROPICAL ICHTHYOLOGY LA English DT Article DE Cheirodontini; Neotropics; Sexual Dimorphism; Taxonomy ID CHARACIFORMES CHARACIDAE; AMAZON BASIN; TELEOSTEI; GENUS; REDESCRIPTION; OSTARIOPHYSI; COMPSURINI; FISH AB Serrapinnus potiguar, new species, is described from the rio Ceara-Mirim, a coastal drainage in the Rio Grande do Norte State, northeastern Brazil. The new species is distinguished from the other species of the genus by the shape and arrangement of the ventral procurrent caudal-fin rays of the sexually dimorphic males; where the hypertrophied elements present the shape of a series of scimitars arranged radially, forming a semi-circle on the ventral margin of the caudal peduncle. Furthermore, the new species is diagnosed from S. heterodon and S. piaba, sympatric congeners from the northeastern Brazilian drainages, respectively by the presence of incomplete lateral line and teeth bearing at most five cusps. C1 [Jerep, Fernando C.] Univ Estadual Londrina, Dept Biol Anim & Vegetal, Ctr Ciencias Biol, Londrina, PR, Brazil. [Jerep, Fernando C.] Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Malabarba, Luiz R.] Univ Fed Rio Grande do Sul, Dept Zool, BR-91501970 Porto Alegre, RS, Brazil. RP Jerep, FC (reprint author), Univ Estadual Londrina, Dept Biol Anim & Vegetal, Ctr Ciencias Biol, Rodovia Celso Garcia Cid,PR 445,Km 380, Londrina, PR, Brazil. EM fjerep@gmail.com; malabarb@ufrgs.br RI Jerep, Fernando/F-5274-2015 FU CNPq [300705/2010-7, 477318/2012-6] FX We are thankful to H. Gurgel (UFRN) for help in fieldwork and donation of material. We thank Carlos A. Lucena (MCP), Osvaldo Oyakawa (MZUSP), Mary Anne Rogers, Kevin Swagel (FMNH), Richard Vari, Jerry Finan, Jeffrey Clayton (NMNH), David Catania and Jon D. Fong (CAS) for loan of specimens, and for museum and technical support. To Centro de Microscopia Eletronica (CME - UFRGS) and Centro de Microscopia e Microanalises (CEMM - PUCRS) for the SEM preparations and images. LRM research is supported by CNPq (300705/2010-7; 477318/2012-6). NR 18 TC 3 Z9 3 U1 0 U2 3 PU SOC BRASILEIRA ICTIOLOGIA PI SAO PAULO PA UNIV SAO PAULO, DEPT FISIOLOGIA-IB, RUA DO MATAO, TRAVESSA 14 N 321, SAO PAULO, SP 05508-900, BRAZIL SN 1679-6225 J9 NEOTROP ICHTHYOL JI Neotrop. Ichthyol. PD APR-JUN PY 2014 VL 12 IS 2 BP 301 EP 308 DI 10.1590/1982-0224-20130218 PG 8 WC Zoology SC Zoology GA AZ0AO UT WOS:000347909200008 ER PT J AU Melo, BF Vari, RP AF Melo, Bruno F. Vari, Richard P. TI New species of Cyphocharax (Characiformes: Curimatidae) from the upper rio Negro, Amazon basin SO NEOTROPICAL ICHTHYOLOGY LA English DT Article DE Biodiversity; Blackwater; Neotropical fish; Pigmentation; Taxonomy ID OSTARIOPHYSI AB A new species of Cyphocharax, Curimatidae, apparently endemic to the blackwater upper rio Negro of the Amazon basin in northern Brazil, is described. The new species is readily distinguished from its congeners by the presence of a distinctly longitudinally elongate, posteriorly vertically expanding patch of dark pigmentation along the midlateral surface of the caudal peduncle, with the patch extending from the base of the middle caudal-fin rays anteriorly past the vertical through the posterior terminus of the adipose fin. The new species additionally differs from all congeners in details of body and fin pigmentation and meristic and morphometric ratios. Evidence for the assignment of the species to Cyphocharax and the occurrence of other species of the Curimatidae apparently endemic to the upper rio Negro catchment is discussed. C1 [Melo, Bruno F.] Univ Estadual Paulista, Inst Biociencias, Dept Morfol, Lab Biol & Genet Peixes, BR-18618970 Botucatu, SP, Brazil. [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fisheries, Washington, DC 20013 USA. RP Melo, BF (reprint author), Univ Estadual Paulista, Inst Biociencias, Dept Morfol, Lab Biol & Genet Peixes, Dist Rubiao Jr S-N, BR-18618970 Botucatu, SP, Brazil. EM melo@ibb.unesp.br; varir@si.edu RI Melo, Bruno F./G-1644-2012 OI Melo, Bruno F./0000-0002-0499-567X FU Fundacao de Amparo a Pesquisa do Estado de Sao Paulo [Proc. 2011/08374-1, Proc. 2013/16436-2]; National Science Foundation [DEB-1257898] FX We thank Hertz F. Santos and Thiago N. Pereira (LIRP) for assistance with the radiographs. We are also grateful to Flavio A. Bockmann and Ricardo M. C. Castro (LIRP) for assistance with the radiography of the type series and to Claudio Oliveira (LBP) and Michel D. Gianeti (MZUSP) for curatorial assistance. Martin I. Taylor provided the photograph in Fig. 3 and habitat information. The authors were financially supported by the Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (Proc. 2011/08374-1 and Proc. 2013/16436-2) to BFM and the National Science Foundation (DEB-1257898) to RPV. NR 22 TC 4 Z9 4 U1 0 U2 2 PU SOC BRASILEIRA ICTIOLOGIA PI SAO PAULO PA UNIV SAO PAULO, DEPT FISIOLOGIA-IB, RUA DO MATAO, TRAVESSA 14 N 321, SAO PAULO, SP 05508-900, BRAZIL SN 1679-6225 J9 NEOTROP ICHTHYOL JI Neotrop. Ichthyol. PD APR-JUN PY 2014 VL 12 IS 2 BP 327 EP 332 DI 10.1590/1982-0224-20130153 PG 6 WC Zoology SC Zoology GA AZ0AO UT WOS:000347909200011 ER PT J AU Philip, S Martin, RV Pierce, JR Jimenez, JL Zhang, Q Canagaratna, MR Spracklen, DV Nowlan, CR Lamsal, LN Cooper, MJ Krotkov, NA AF Philip, S. Martin, R. V. Pierce, J. R. Jimenez, J. L. Zhang, Q. Canagaratna, M. R. Spracklen, D. V. Nowlan, C. R. Lamsal, L. N. Cooper, M. J. Krotkov, N. A. TI Spatially and seasonally resolved estimate of the ratio of organic mass to organic carbon SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Organic aerosol; Organic carbon; NO2; AMS; OMI; GEOS-Chem ID UNITED-STATES; HYDROCARBON-LIKE; INTEX-B; AEROSOL; SPECTROMETER; PARTICLES; EMISSIONS; VISIBILITY; CHEMISTRY; PITTSBURGH AB Particulate organic matter is of interest for air quality and climate research, but the relationship between ambient organic mass (OM) and organic carbon (CC) remains ambiguous both in measurements and in modeling. We present a simple method to derive an estimate of the spatially and seasonally resolved global, lower tropospheric, ratio between OM and CC. We assume ambient NO2 concentrations as a surrogate for fresh emission which mostly determines the continental scale OM/OC ratio. For this, we first develop a parameterization for the OM/OC ratio using the primary organic aerosol (POA) fraction of total OM estimated globally from Aerosol Mass Spectrometer (AMS) measurements, and evaluate it with high mass resolution AMS data. Second, we explore the ability of ground-level NO2 concentrations derived from the OMI satellite sensor to serve as a proxy for fresh emissions that have a high POA fraction, and apply NO2 data to derive ambient POA fraction. The combination of these two methods yields an estimate of OM/OC from NO2 measurements. Although this method has inherent deficiencies over biomass burning, free-tropospheric, and marine environments, elsewhere it offers more information than the currently used global-mean OM/OC ratios. The OMI-derived global OM/OC ratio ranges from 1.3 to 2.1 (mu g/mu gC), with distinct spatial variation between urban and rural regions. The seasonal OM/OC ratio has a summer maximum and a winter minimum over regions dominated by combustion emissions. This dataset serves as a tool for interpreting organic carbon measurements, and for evaluating modeling of atmospheric organics. We also develop an additional parameterization for models to estimate the ratio of primary OM to OC from simulated NOx concentrations. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Philip, S.; Martin, R. V.; Pierce, J. R.; Nowlan, C. R.; Cooper, M. J.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pierce, J. R.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Jimenez, J. L.] Univ Colorado, Dept Chem & Biochem, CIRES, Boulder, CO 80309 USA. [Zhang, Q.] Univ Calif Davis, Dept Environm Toxicol, Davis, CA 95616 USA. [Canagaratna, M. R.] Aerodyne Res Inc, Billerica, MA USA. [Spracklen, D. V.] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England. [Lamsal, L. N.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA. [Lamsal, L. N.; Krotkov, N. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Philip, S (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. EM philip.sajeev@dal.ca RI Pierce, Jeffrey/E-4681-2013; Jimenez, Jose/A-5294-2008; Zhang, Qi/F-9653-2010; Martin, Randall/C-1205-2014; Krotkov, Nickolay/E-1541-2012; Spracklen, Dominick/B-4890-2014; OI Pierce, Jeffrey/0000-0002-4241-838X; Jimenez, Jose/0000-0001-6203-1847; Martin, Randall/0000-0003-2632-8402; Krotkov, Nickolay/0000-0001-6170-6750; Nowlan, Caroline/0000-0002-8718-9752 FU NSERC; DOE (BER/ASR) [DE SC0006035/DE-SC0006711/DE-FG02-11ER65293]; [DE-FG02-11ER65293] FX This work was supported by NSERC. JLJ was supported by DOE (BER/ASR) DE SC0006035/DE-SC0006711/DE-FG02-11ER65293. QZ was supported by DE-FG02-11ER65293. We thank Aaron van Donkelaar and Ian Folkins for useful comments. NR 61 TC 11 Z9 12 U1 5 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD APR PY 2014 VL 87 BP 34 EP 40 DI 10.1016/j.atmosenv.2013.11.065 PG 7 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AY2QR UT WOS:000347434900005 ER PT J AU Hartstone-Rose, A Selvey, H Boyde, B Villari, J AF Hartstone-Rose, Adam Selvey, Hannah Boyde, Bryttin Villari, Joseph TI The cranial morphology of large captive versus wild felids SO FASEB JOURNAL LA English DT Meeting Abstract C1 [Villari, Joseph] George Mason Univ, Fairfax, VA 22030 USA. [Villari, Joseph] Smithsonian Inst, Washington, DC 20560 USA. [Selvey, Hannah; Boyde, Bryttin] Univ S Carolina, Columbia, SC 29208 USA. [Hartstone-Rose, Adam] Univ S Carolina, Sch Med, Columbia, SC USA. RI Hartstone-Rose, Adam/I-3503-2016 OI Hartstone-Rose, Adam/0000-0001-5307-5573 NR 0 TC 0 Z9 0 U1 2 U2 5 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 EI 1530-6860 J9 FASEB J JI Faseb J. PD APR PY 2014 VL 28 IS 1 SU S MA 918.11 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA AX0OG UT WOS:000346651003383 ER PT J AU Caragol, TB AF Caragol, Taina B. TI Rafael Ferrer SO AMERICAS LA English DT Book Review C1 [Caragol, Taina B.] Natl Portrait Gallery, Smithsonian Inst, Washington, DC 20001 USA. RP Caragol, TB (reprint author), Natl Portrait Gallery, Smithsonian Inst, Washington, DC 20001 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ACAD AMER FRANCISCAN HIST PI WEST BETHESDA PA BOX 34440, WEST BETHESDA, MD 20817 USA SN 0003-1615 EI 1533-6247 J9 AMERICAS JI Americas PD APR PY 2014 VL 70 IS 4 BP 768 EP 770 PG 3 WC History SC History GA AU9CT UT WOS:000345890000026 ER PT J AU Takei, D Tsujimoto, M Drake, JJ Kitamoto, S AF Takei, Dai Tsujimoto, Masahiro Drake, Jeremy J. Kitamoto, Shunji TI X-ray development of the classical nova V2672 Ophiuchi with Suzaku SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE stars: individual (Nova Ophiuchi 2009, V2672 Ophiuchi); stars: novae; cataclysmic variables; X-rays: stars ID RS-OPHIUCHI; BOARD SUZAKU; 2006 OUTBURST; LIGHT-CURVE; U SCO; SPECTROSCOPY; PHASE; MODEL; ABSORPTION; EVOLUTION AB We report on the Suzaku detection of a rapid flare-like X-ray flux amplification early in the development of the classical nova V2672 Ophiuchi. Two target-of-opportunity similar to 25 ks X-ray observations were made 12 and 22 d after the outburst. The flux amplification was found in the latter half of day 12. Time-sliced spectra are characterized by a growing supersoft excess with edge-like structures and a relatively stable optically-thin thermal component with K alpha emission lines from highly ionized Si. The observed spectral evolution is consistent with a model that has a time development of circumstellar absorption, for which we obtained a decline rate of similar to 10%-40% on a time scale of 0.2 d on day 12. Such a rapid drop of absorption and short-term flux variability on day 12 suggests inhomogeneous ejecta with dense blobs/holes in the line-of-sight. Then on day 22 the fluxes of both supersoft and thin-thermal plasma components became significantly fainter. Based on the serendipitous results we discuss the nature of this source in the context of both short- and long-term X-ray behavior. C1 [Takei, Dai] RIKEN SPring 8 Ctr, Inst Phys & Chem Res RIKEN, Sayo, Hyogo 6795148, Japan. [Takei, Dai; Drake, Jeremy J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Tsujimoto, Masahiro] Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Kitamoto, Shunji] Rikkyo Univ, Dept Phys, Toshima Ku, Tokyo 1718501, Japan. RP Takei, D (reprint author), RIKEN SPring 8 Ctr, Inst Phys & Chem Res RIKEN, 1-1-1 Kouto, Sayo, Hyogo 6795148, Japan. EM takei@spring8.or.jp RI XRAY, SUZAKU/A-1808-2009 FU JSPS; Special Postdoctoral Researchers Program in RIKEN; NASA [NAS8-03060] FX The authors appreciate the reviewer for useful suggestions. We thank the Suzaku telescope managers for allocating a part of the director's discretionary time, and also thank Greg Schwarz, the principal investigator of the Swift observations, and the Nova-CV group for providing the Swift data. Optical data are from AAVSO and VSOLJ databases. This research has made use of data obtained from: (1) DARTS by C-SODA in JAXA/ISAS, (2) HEASARC by NASA/GSFC, and (3) SIMBAD by CDS, France. We acknowledge Jan-Uwe Ness for his comments on this paper. D. T. acknowledges financial support from JSPS and by the Special Postdoctoral Researchers Program in RIKEN. J. J. D. was supported by the NASA contract NAS8-03060 to the CXC and thanks the Director, H. Tananbaum, for continuing advice and support. NR 54 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD APR PY 2014 VL 66 IS 2 AR 37 DI 10.1093/pasj/psu019 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL8YZ UT WOS:000339427200020 ER PT J AU Lopez-Baucells, A Rocha, R Fernandez-Arellano, G Bobrowiec, PED Palmeirim, JM Meyer, CFJ AF Lopez-Baucells, Adria Rocha, Ricardo Fernandez-Arellano, Gilberto Bobrowiec, Paulo Estefano D. Palmeirim, Jorge M. Meyer, Christoph F. J. TI Echolocation of the big red bat Lasiurus egregius (Chiroptera: Vespertilionidae) and first record from the Central Brazilian Amazon SO STUDIES ON NEOTROPICAL FAUNA AND ENVIRONMENT LA English DT Article DE Brazil; echolocation; Lasiurini; species distribution; acoustic identification ID INSECTIVOROUS BATS; CINEREUS; CALLS; DIVERSITY; FOREST; IDENTIFICATION; CONSERVATION; MAMMALIA; YUCATAN; MEXICO AB Lasiurus egregius (Peters, 1870) is a rare Neotropical vespertilionid bat and virtually no data on its ecology and echolocation calls are currently available. We report the capture of four individuals in the Central Amazon, representing the first record for the region and a significant (> 800 km) expansion of the species' known range. Echolocation calls, recorded for the first time under natural conditions, were 1.5-8 ms in duration, and characterized by high mean bandwidth (18 kHz) and a mean frequency of maximum energy of 30 kHz. C1 [Lopez-Baucells, Adria; Rocha, Ricardo; Palmeirim, Jorge M.; Meyer, Christoph F. J.] Univ Lisbon, Fac Ciencias, Dept Biol Anim, Ctr Biol Ambiental, Lisbon, Portugal. [Lopez-Baucells, Adria] Museu Ciencies Nat Granollers, Area Invest Quiropters, Granollers, Spain. [Lopez-Baucells, Adria; Rocha, Ricardo; Fernandez-Arellano, Gilberto; Bobrowiec, Paulo Estefano D.; Meyer, Christoph F. J.] Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil. [Lopez-Baucells, Adria; Rocha, Ricardo; Fernandez-Arellano, Gilberto; Bobrowiec, Paulo Estefano D.; Meyer, Christoph F. J.] Smithsonian Trop Res Inst, Manaus, Amazonas, Brazil. [Rocha, Ricardo] Univ Helsinki, Fac Biosci, Metapopulat Res Grp, Helsinki, Finland. [Bobrowiec, Paulo Estefano D.] INPA, Conselho Nacl Desenvolvimento Cient & Tecnol, Inst Nacl Ciencia & Tecnol Estudos Integrados Bio, Minist Ciencia & Tecnol, Manaus, Amazonas, Brazil. RP Lopez-Baucells, A (reprint author), Univ Lisbon, Fac Ciencias, Dept Biol Anim, Ctr Biol Ambiental, Lisbon, Portugal. EM adria.baucells@gmail.com RI Palmeirim, Jorge/A-1323-2014; Meyer, Christoph/A-4363-2012; OI Palmeirim, Jorge/0000-0003-4734-8162; Meyer, Christoph/0000-0001-9958-8913; Lopez-Baucells, Adria/0000-0001-8446-0108 FU Portuguese Foundation for Science and Technology [PTDC/BIA-BIC/111184/2009, SFRH/BD/80488/2011] FX We would like to thank Fabio Zanella Farneda and Madalena Boto for fieldwork assistance and Jose Luis Camargo, Rosely Hipolito, and Ary Jorge Ferreira for logistic support. We are grateful to two anonymous reviewers for comments on an earlier version of the manuscript. This work was supported by the Portuguese Foundation for Science and Technology under Grant PTDC/BIA-BIC/111184/2009 & SFRH/BD/80488/2011. This is publication 636 in the Technical Series of the BDFPP. NR 39 TC 1 Z9 1 U1 2 U2 15 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0165-0521 EI 1744-5140 J9 STUD NEOTROP FAUNA E JI Stud. Neotrop. Fauna Environ. PD APR PY 2014 VL 49 IS 1 BP 18 EP 25 DI 10.1080/01650521.2014.907600 PG 8 WC Zoology SC Zoology GA AJ3VD UT WOS:000337595100003 ER PT J AU Konstantinov, AS Linzmeier, AM Savini, VP AF Konstantinov, Alexander S. Linzmeier, Adelita M. Savini, Vilma P. TI STEVENALTICA, A NEW GENUS OF MOSS AND LEAF-LITTER INHABITING FLEA BEETLES FROM BOLIVIA (COLEOPTERA: CHRYSOMELIDAE: GALERUCINAE: ALTICINI). SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Bryobionts; key to genera; Neotropics AB A new genus, Stevenaltica, with two new species, S. normi and S. erronis, from Bolivia is described and illustrated. It is similar to Exoceras Jacoby. An identification key for all flea beetle genera known to occur in mosses in the Western Hemisphere is provided. C1 [Konstantinov, Alexander S.] USDA ARS, Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, Washington, DC 20013 USA. [Linzmeier, Adelita M.] Fundacao Univ Fed Grande Dourados, Fac Ciencias Biol & Ambientais, BR-79804980 Dourados, Mato Grosso Sul, Brazil. [Savini, Vilma P.] Cent Univ Venezuela, Fac Agron, Museo Inst Zool Agr, Maracay 2101 A, Estado Aragua, Venezuela. RP Konstantinov, AS (reprint author), USDA ARS, Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, POB 37012, Washington, DC 20013 USA. EM alex.konstantinov@ars.usda.gov; alinzmeier@yahoo.com.br; vsgioia@gmail.com RI caputo, carlo/N-3747-2014 NR 14 TC 0 Z9 0 U1 1 U2 4 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2014 VL 116 IS 2 BP 159 EP 171 DI 10.4289/0013-8797.116.2.159 PG 13 WC Entomology SC Entomology GA AI2BG UT WOS:000336661200003 ER PT J AU Murphy, WL AF Murphy, William L. TI REDISCOVERY OF DICTYA DISJUNCTA ORTH (DIPTERA: SCIOMYZIDAE) WITH DESCRIPTIONS OF ALL LIFE STAGES AND LIFE CYCLE SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Tetanocerini; taxonomy; Nearctic; snail-killing; distribution; new records ID SNAIL-KILLING FLY; BIOLOGY; LARVAE; MEIGEN; FLIES AB Eighty-nine years after the only known specimen of Dictya disjuncta Orth was collected, in Mississippi in 1921, the species was rediscovered in Indiana, U.S.A. in 2010. A gravid female laid eggs that gave rise to two generations of flies. The egg, three larval stages, puparium, and adult female are described and illustrated for the first time, the life cycle is elucidated, the holotype male is redescribed, and the geographical distribution of the species is depicted. C1 Smithsonian Inst, Fishers, IN 46038 USA. RP Murphy, WL (reprint author), Smithsonian Inst, 7835 Tufton St, Fishers, IN 46038 USA. EM billmurphy8@sbcglobal.net FU Indiana Academy of Science FX I thank Karl R. Valley, Harrisburg, PA, for meticulously describing the three larval instars; Karolyn Darrow, Department of Entomology, Smithsonian Institution, Washington, DC, for producing and enhancing the images of D. disjuncta; Kevin Cummings, Illinois Natural History Survey, Champaign-Urbana, for identifying molluscs; Lynn Carta and Andrea Skantar, Nematode Laboratory, Agricultural Research Service, U.S. Department of Agriculture, Beltsville, MD, for helping to identify the oligochaete worm; John. B. Churchill, Frostburg State University, Frostburg, MD, for producing the distribution map; the Blatchley Nature Study Club, Noblesville, IN, and the Indiana Academy of Science for partially funding this project; and especially Lloyd V. Knutson, Gaeta, Italy, for valuable suggestions on all aspects of this paper. NR 27 TC 1 Z9 1 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2014 VL 116 IS 2 BP 172 EP 187 DI 10.4289/0013-8797.116.2.172 PG 16 WC Entomology SC Entomology GA AI2BG UT WOS:000336661200004 ER PT J AU Malagon-Aldana, LA Serna, F Smith, AR AF Malagon-Aldana, Leonardo Andres Serna, Francisco Smith, Anddavid R. TI Siricidae (Hymenoptera) in Colombia, the first report of Urocerus gigas (Linnaeus) from northern South America SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material C1 [Malagon-Aldana, Leonardo Andres; Serna, Francisco] Univ Nacl Colombia, UNAB, Fac Ciencias Agr, Museo Entomol, Bogota, DC, Colombia. [Smith, Anddavid R.] USDA ARS, Smithsonian Inst, Systemat Entomol Lab, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Malagon-Aldana, LA (reprint author), Univ Nacl Colombia, UNAB, Fac Ciencias Agr, Museo Entomol, Cra 30 45-03, Bogota, DC, Colombia. EM lamalagona@unal.edu.co; fjsernac@unal.edu.co; sawfly2@aol.com NR 3 TC 1 Z9 1 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2014 VL 116 IS 2 BP 191 EP 192 DI 10.4289/0013-8797.116.2.191 PG 2 WC Entomology SC Entomology GA AI2BG UT WOS:000336661200006 ER PT J AU McKamey, SH Xue, QQ Viraktamath, CA Zhang, YL AF McKamey, Stuart H. Xue, Qingquan Viraktamath, Chandra A. Zhang, Yalin TI New Name for One and Fixation of Correct Spelling of Two Leafhopper Taxa (Hemiptera: Cicadellidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material C1 [McKamey, Stuart H.] USDA ARS, Smithsonian Inst, Systemat Entomol Lab, Natl Museum Nat Hist, Washington, DC 20560 USA. [Xue, Qingquan; Zhang, Yalin] Northwest A&F Univ, Entomol Museum, Yangling 712100, Shaanxi, Peoples R China. [Viraktamath, Chandra A.] Univ Agr Sci, GKVK, Dept Entomol, Bangalore 560065, Karnataka, India. RP McKamey, SH (reprint author), USDA ARS, Smithsonian Inst, Systemat Entomol Lab, Natl Museum Nat Hist, MRC 168,10th & Constitut Ave, Washington, DC 20560 USA. EM smckamey@ars.usda.gov NR 5 TC 0 Z9 0 U1 0 U2 3 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2014 VL 116 IS 2 BP 193 EP 194 DI 10.4289/0013-8797.116.2.193 PG 2 WC Entomology SC Entomology GA AI2BG UT WOS:000336661200007 ER PT J AU Smith, DR Williams, G AF Smith, David R. Williams, Gaye TI Waldheimia carbonaria (Cresson) (Hymenoptera: Tenthredinidae), a sawfly on Missouri primrose, Oenothera missouriensis Sims (Onagraceae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material C1 [Smith, David R.] USDA ARS, Smithsonian Inst, Natl Museum Nat Hist, Dept Agr,Systemat Entomol Lab, Washington, DC 20013 USA. [Williams, Gaye] Maryland Dept Agr, Plant Protect & Weed Management Sect, Annapolis, MD 21401 USA. RP Smith, DR (reprint author), USDA ARS, Smithsonian Inst, Natl Museum Nat Hist, Dept Agr,Systemat Entomol Lab, POB 37012,MRC 168, Washington, DC 20013 USA. EM sawfly2@aol.com; gaye.williams@maryland.gov NR 4 TC 3 Z9 3 U1 0 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2014 VL 116 IS 2 BP 197 EP 198 DI 10.4289/0013-8797.116.2.197 PG 2 WC Entomology SC Entomology GA AI2BG UT WOS:000336661200009 ER PT J AU Zhang, JQ Meng, SY Wen, J Rao, GY AF Zhang, Jian-Qiang Meng, Shi-Yong Wen, Jun Rao, Guang-Yuan TI Phylogenetic Relationships and Character Evolution of Rhodiola (Crassulaceae) based on Nuclear Ribosomal ITS and Plastid trnL-F and psbA-trnH Sequences SO SYSTEMATIC BOTANY LA English DT Article DE Classification; dioecy; marcescent flowering stems; molecular phylogenetics; Qinghai-Tibetan Plateau ID QINGHAI-TIBETAN PLATEAU; CHLOROPLAST DNA; FLOWERING PLANTS; MOLECULAR EVOLUTION; GENETIC-STRUCTURE; SEXUAL SYSTEMS; DIOECY; RADIATION; MODEL; SEDUM AB Rhodiola (Crassulaceae) comprises about 70 species and shows a high level of morphological diversity. The genus is mainly distributed in alpine areas and cold regions of the Northern Hemisphere with the Qinghai-Tibetan Plateau as its center of diversity. The phylogenetic relationships within Rhodiola remain poorly understood largely because of difficulties in collecting samples and specimens. In the present study, 51 species/varieties from Rhodiola representing all morphological sections were analyzed using sequences of the nuclear ribosomal internal transcribed spacers region and the plastid psbA-trnH and troL-F markers. Our results suggest that Rhodiola and Pseudosedum form a well-supported clade, but the relationship between these two genera is not resolved. None of the four currently recognized subgenera is monophyletic; yet three of seven sections, R. sects. Trifida, Prainia, and Pseudorhodiola are each supported to be monophyletic. Rhodiola rosea is a popular medicinal plant that has an adaptogenic effect. The three accessions of R. rosea from eastern Asia, eastern North America, and Europe form a well-supported clade. Rhodiola species independently reached North America from Asia twice, once in the R. rosea lineage, and the other in the R. integrifolia-R. rhodantha lineage. Two taxonomically important characters, dioecy and marcescent flowering stems, are inferred to have evolved multiple times within Rhodiola. C1 [Zhang, Jian-Qiang; Meng, Shi-Yong; Rao, Guang-Yuan] Peking Univ, Coll Life Sci, Beijing 100871, Peoples R China. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. RP Wen, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. EM wenj@si.edu; rao@pku.edu.cn FU Open Project Program of the State Key Laboratory of Systematic and Evolutionary Botany (LSEB) of China [LSEB2009-06]; Laboratory of Analytical Biology of the National Museum of Natural History; Smithsonian Institution; China Scholarship Council [201206010113] FX The authors thank Associate Editor Austin Mast and two anonymous reviewers for their most helpful suggestions, which greatly improved the paper. We also thank Yiming An and Dongqing Zhang for field assistance, Gerry Allen for providing samples, and Gabriel Johnson, Matt Kweskin and Marc Appelhans for assistance in the lab and in data analyses. This research was supported by the Open Project Program of the State Key Laboratory of Systematic and Evolutionary Botany (LSEB) of China (Grant Number: LSEB2009-06) and the Laboratory of Analytical Biology of the National Museum of Natural History, the Smithsonian Institution. Jianqiang Zhang has been supported by a scholarship for exchanging Ph. D. candidates from the China Scholarship Council (No. 201206010113) for his studies at the Smithsonian Institution. The study represents part of Jianqiang Zhang's dissertation research. NR 96 TC 7 Z9 8 U1 3 U2 36 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 EI 1548-2324 J9 SYST BOT JI Syst. Bot. PD APR-JUN PY 2014 VL 39 IS 2 BP 441 EP 451 DI 10.1600/036364414X680753 PG 11 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA AH9LD UT WOS:000336463000010 ER PT J AU Fryer, CL Even, W Grefenstette, BW Wong, TW AF Fryer, Chris L. Even, Wesley Grefenstette, Brian W. Wong, Tsing-Wai TI Observational constraints of stellar collapse: Diagnostic probes of nature's extreme matter experiment SO AIP ADVANCES LA English DT Article ID METAL-POOR STARS; R-PROCESS NUCLEOSYNTHESIS; GAMMA-RAY BURST; COMPACT OBJECT FORMATION; NEUTRINO-DRIVEN WINDS; II-P SUPERNOVAE; MASS-DISTRIBUTION; BLACK-HOLES; CASSIOPEIA-A; BINARY CHARACTERISTICS AB Supernovae are Nature's high-energy, high density laboratory experiments, reaching densities in excess of nuclear densities and temperatures above 10 MeV. Astronomers have built up a suite of diagnostics to study these supernovae. If we can utilize these diagnostics, and tie them together with a theoretical understanding of supernova physics, we can use these cosmic explosions to study the nature of matter at these extreme densities and temperatures. Capitalizing on these diagnostics will require understanding a wide range of additional physics. Here we review the diagnostics and the physics neeeded to use them to learn about the supernova engine, and ultimate nuclear physics. (C) 2014 Author(s). All article content, except where otherwise noted, is licensed under a Creative Commons Attribution 3.0 Unported License. C1 [Fryer, Chris L.; Even, Wesley] Los Alamos Natl Lab, CCS Div, Los Alamos, NM 87545 USA. [Grefenstette, Brian W.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Wong, Tsing-Wai] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Wong, Tsing-Wai] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Wong, Tsing-Wai] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fryer, Chris L.] Los Alamos Natl Lab, Dept Phys & Astron, Los Alamos, NM 87545 USA. [Fryer, Chris L.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. RP Fryer, CL (reprint author), Los Alamos Natl Lab, CCS Div, POB 1663, Los Alamos, NM 87545 USA. EM fryer@lanl.gov OI Even, Wesley/0000-0002-5412-3618 FU National Nuclear Security Administration of the U.S. Department of Energy at Los Alamos National Laboratory [DE-AC52-06NA25396] FX The work of C.L.F. and W.E. was done under the auspices of the National Nuclear Security Administration of the U.S. Department of Energy at Los Alamos National Laboratory under Contract DE-AC52-06NA25396. NR 166 TC 3 Z9 3 U1 1 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 2158-3226 J9 AIP ADV JI AIP Adv. PD APR PY 2014 VL 4 IS 4 AR 041014 DI 10.1063/1.4870404 PG 26 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA AH4FG UT WOS:000336082000015 ER PT J AU Koenig, WD Marra, PP AF Koenig, Walter D. Marra, Peter P. TI Russell S. Greenberg, 1953-2013 MEMORIAM SO AUK LA English DT Biographical-Item C1 [Koenig, Walter D.] Cornell Univ, Ornithol Lab, Ithaca, NY 14850 USA. [Marra, Peter P.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Migratory Bird Ctr, Washington, DC USA. RP Koenig, WD (reprint author), Cornell Univ, Ornithol Lab, Ithaca, NY 14850 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 EI 1938-4254 J9 AUK JI AUK PD APR PY 2014 VL 131 IS 2 BP 255 EP 256 DI 10.1642/AUK-13-241.1 PG 2 WC Ornithology SC Zoology GA AH9QQ UT WOS:000336477300014 ER PT J AU Rushing, CS Ryder, TB Saracco, JF Marra, PP AF Rushing, Clark S. Ryder, Thomas B. Saracco, James F. Marra, Peter P. TI Assessing migratory connectivity for a long-distance migratory bird using multiple intrinsic markers SO ECOLOGICAL APPLICATIONS LA English DT Article DE deuterium; geographical variation; hydrogen isoscapes; Hylocichla mustilena; intrinsic markers; migratory connectivity; morphology; probabilistic assignment; stable isotopes; Wood Thrush ID LIGHT-LEVEL GEOLOCATORS; GEOGRAPHIC-VARIATION; STABLE-ISOTOPES; NEOTROPICAL MIGRANT; HYDROGEN ISOTOPES; BREEDING ORIGINS; WILSONIA-PUSILLA; GENETIC-MARKERS; RECAPTURE DATA; POPULATION AB Patterns of migratory connectivity are a vital yet poorly understood component of the ecology and evolution of migratory birds. Our ability to accurately characterize patterns of migratory connectivity is often limited by the spatial resolution of the data, but recent advances in probabilistic assignment approaches have begun pairing stable isotopes with other sources of data (e.g., genetic and mark-recapture) to improve the accuracy and precision of inferences based on a single marker. Here, we combine stable isotopes and geographic variation in morphology (wing length) to probabilistically assign Wood Thrush (Hylocichla mustilena) captured on the wintering grounds to breeding locations. In addition, we use known-origin samples to validate our model and assess potentially important impacts of isotopic and morphological covariates (age, sex, and breeding location). Our results show that despite relatively high levels of mixing across their breeding and nonbreeding ranges, moderate levels of migratory connectivity exist along an east-west gradient. In addition, combining stable isotopes with geographic variation in wing length improved the precision of breeding assignments by 10% and 37% compared to assignments based on isotopes alone or wing length alone, respectively. These results demonstrate that geographical variation in morphological traits can greatly improve estimates of migratory connectivity when combined with other intrinsic markers (e.g., stable isotopes or genetic data). The wealth of morphological data available from museum specimens across the world represents a tremendously valuable, but largely untapped, resource that is widely applicable for quantifying patterns of migratory connectivity. C1 [Rushing, Clark S.] Univ Maryland, Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA. [Rushing, Clark S.; Ryder, Thomas B.; Marra, Peter P.] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA. [Saracco, James F.] Inst Bird Populat, Point Reyes Stn, CA 94956 USA. RP Rushing, CS (reprint author), Univ Maryland, Dept Biol, Biol Psychol Bldg, College Pk, MD 20742 USA. EM crushing@umd.edu FU Strategic Environmental Resource and Development Program (SERDP) [RC-2121] FX Thanks to T. B. Smith for providing feather samples archived as part of the Neotropical Migrant Conservation Genetics Project (NMCGP) of the University of California at Los Angeles. We thank the many MAPS station operators who have contributed wing chord data. Individual MoSI contributors who provided feather samples and wing chord data include O. Arroliga (GUAT; Amigos del Rio San Juan), R. Coates and D. Curiel (RBTT; Universidad Nacional Autonoma de Mexico), A. Cerezo (CSGI; FUNDAECO), J. M. Zolotoff (MOMB; Fundacion Cocibolca), L. and G. Duriaux Chavarria (JAGU; Reserva Privada El Jaguar), and F. De Clerck and A. Martinez (CATI; Centro Agronomico Tropical de Investigacion y Ensenanza). This is contribution no. 464 of The Institute for Bird Populations. Funding provided by the Strategic Environmental Resource and Development Program (SERDP Award RC-2121). NR 79 TC 14 Z9 15 U1 2 U2 46 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1051-0761 EI 1939-5582 J9 ECOL APPL JI Ecol. Appl. PD APR PY 2014 VL 24 IS 3 BP 445 EP 456 DI 10.1890/13-1091.1 PG 12 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA AD4TA UT WOS:000333242300003 PM 24834732 ER PT J AU Hirsch, BT Prange, S Hauver, SA Gehrt, SD AF Hirsch, Ben T. Prange, Suzanne Hauver, Stephanie A. Gehrt, Stanley D. TI PATTERNS OF LATRINE USE BY RACCOONS (PROCYON LOTOR) AND IMPLICATION FOR BAYLISASCARIS PROCYONIS TRANSMISSION SO JOURNAL OF WILDLIFE DISEASES LA English DT Article DE Baylisascaris procyonis; latrine; Peromyscus; Procyon; raccoon; roundworm; zoonosis ID SCENT MARKING STRATEGIES; PEROMYSCUS-LEUCOPUS; ROUNDWORM; SYSTEM; AVAILABILITY; INTERFERENCE; PREVALENCE; FECES; SIZE; FOOD AB Mammals often use latrine sites for defecation, yet little is known about patterns of latrine use in many common species such as raccoons (Procyon lotor). Because raccoon latrines are important foci for the transmission of raccoon roundworm (Baylisascaris procyonis), documenting metrics of raccoon latrine use may have public health implications. Although some studies have provided evidence that multiple raccoons visit single latrine sites, exact latrine visitation patterns of raccoons have never been documented. We monitored raccoon latrine usage using proximity-logging collars placed at 15 latrine sites. We found that latrine sites were visited by multiple raccoons (range 1-7), and raccoons visited as many as six latrines during a 2-wk period. No sex differences were found in the number of latrines visited or time spent during visits. We posit that the use of multiple latrine sites by raccoons may lead to the pattern that rates of B. procyonis infection at latrines are greater than infection rates found in individual raccoon fecal samples. This in turn could lead to greater transmission of B. procyonis to paratenic hosts. Our results support the conclusion that raccoon latrines can be major foci for the infection and spread of B. procyonis. C1 [Hirsch, Ben T.; Gehrt, Stanley D.] Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA. [Hirsch, Ben T.] Smithsonian Trop Res Inst, Panama City, Panama. [Prange, Suzanne] Ohio Div Wildlife, Athens, OH 45701 USA. [Hauver, Stephanie A.] Cornell Univ, Anim Hlth Diagnost Ctr, Ithaca, NY 14850 USA. RP Hirsch, BT (reprint author), Ohio State Univ, Sch Environm & Nat Resources, 2021 Coffey Rd, Columbus, OH 43210 USA. EM hirschb@si.edu RI Gehrt, Stanley/J-8700-2012 FU National Science Foundation [ID-0425203]; Cook County Animal and Rabies Control; Max McGraw Wildlife Foundation; Ohio State University's Terrestrial Wildlife Ecology Lab FX This project was funded in part by the National Science Foundation (ID-0425203), Cook County Animal and Rabies Control, and the Max McGraw Wildlife Foundation. We thank the Cook County Forest Preserve District and C. Anchor for access to our study site, and are especially grateful for the support of D. Farmer (deceased). We also thank The Ohio State University's Terrestrial Wildlife Ecology Lab for support. We are deeply indebted to all of the technicians who assisted on this project. We thank Kristin Page, James Mills, and one anonymous reviewer for helpful comments on earlier versions of this manuscript. NR 43 TC 4 Z9 4 U1 3 U2 36 PU WILDLIFE DISEASE ASSOC, INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 0090-3558 EI 1943-3700 J9 J WILDLIFE DIS JI J. Wildl. Dis. PD APR PY 2014 VL 50 IS 2 BP 243 EP 249 DI 10.7589/2013-09-251 PG 7 WC Veterinary Sciences SC Veterinary Sciences GA AH6JT UT WOS:000336237900010 PM 24484480 ER PT J AU McCormick, MK Jacquemyn, H AF McCormick, Melissa K. Jacquemyn, Hans TI What constrains the distribution of orchid populations? SO NEW PHYTOLOGIST LA English DT Review DE mycorrhiza; orchid; rarity; recruitment limitation; specificity ID MYCO-HETEROTROPHIC PLANTS; LADYS SLIPPER ORCHIDS; TERRESTRIAL ORCHID; MYCORRHIZAL FUNGI; IN-SITU; DUST SEEDS; RECRUITMENT LIMITATION; SYMBIOTIC GERMINATION; GOODYERA-REPENS; SPECIFICITY AB The distribution and abundance of orchid populations depend on a suite of biological and ecological factors, including seed production and dispersal, availability of mycorrhizal fungi and appropriate environmental conditions, with the weighting of these factors depending on the spatial scale considered. Disentangling the factors determining successful orchid establishment represents a major challenge, involving seed germination experiments, molecular techniques and assessment of environmental conditions. Identification of fungi from large-scale surveys of mycorrhizal associations in a range of orchid species has shown that mycorrhizal fungi may be widespread and occur in varied habitats. Further, a meta-analysis of seed introduction experiments revealed similar seed germination in occupied and unoccupied habitat patches. Orchid rarity was also unrelated to mycorrhizal specificity. Nonetheless, seed germination within sites appears to depend on both biotic and abiotic conditions. In the few cases that have been examined, coexisting orchids have distinct mycorrhizal communities and show strong spatial segregation, suggesting that mycorrhizal fungi are important drivers of niche partitioning and contribute to orchid coexistence. A broader investigation of orchid mycorrhizal fungus distribution in the soil, coupled with fungus and recruitment mapping, is needed to translate fungal abundance to orchid population dynamics and may lead to better orchid conservation. C1 [McCormick, Melissa K.] Smithsonian Environm Res Ctr, Edgewater, MD 20137 USA. [Jacquemyn, Hans] Katholieke Univ Leuven, Lab Plant Populat & Conservat Biol, Dept Biol, B-3001 Louvain, Belgium. RP McCormick, MK (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 20137 USA. EM mccormickm@si.edu FU European Research Council (ERC) [260601 - MYCASOR]; US National Park Service (PMIS) [144281] FX The authors would like to thank the New Phytologist Trust for inviting them to the 31st New Phytologist Symposium, Orchid symbioses: models for evolutionary ecology, where the idea for this paper was generated and some of the new directions for future research were presented. Three anonymous reviewers and Marc-Andre Selosse provided helpful comments on an earlier draft. We would like to thank Ryan Phillips and Tamara Tesitelova for providing data on seed germination. This project was supported by the European Research Council (ERC starting grant 260601 - MYCASOR) and the US National Park Service (PMIS #144281). NR 80 TC 35 Z9 37 U1 14 U2 104 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0028-646X EI 1469-8137 J9 NEW PHYTOL JI New Phytol. PD APR PY 2014 VL 202 IS 2 BP 392 EP 400 DI 10.1111/nph.12639 PG 9 WC Plant Sciences SC Plant Sciences GA AD2JH UT WOS:000333060500012 ER PT J AU Wendler, JE Meyers, SR Wendler, I Kuss, J AF Wendler, Jens E. Meyers, Stephen R. Wendler, Ines Kuss, Jochen TI A million-year-scale astronomical control on Late Cretaceous sea-level SO NEWSLETTERS ON STRATIGRAPHY LA English DT Article DE Cyclostratigraphy; Astronomical forcing; Sequence stratigraphy; Time series analysis; Late Cretaceous; Cenomanian/Turonian ID CENOMANIAN-TURONIAN BOUNDARY; CARBON-ISOTOPE STRATIGRAPHY; ORBITAL TIME-SCALE; WEST-CENTRAL JORDAN; LEVANT PLATFORM; SEQUENCE STRATIGRAPHY; GLOBAL CORRELATION; HARMONIC-ANALYSIS; NORTHERN GERMANY; PALEOCLIMATE AB An evaluation of the global synchronicity and duration of "3rd-order" sea-level fluctuations during the Cretaceous greenhouse has been hampered by poor constraints on potential climatic and tectonic drivers, and limitations of geochronology and chronostratigraphic correlation. To provide insight into the nature of such sea-level fluctuations, here we present a new Late Cretaceous record from the Jordanian Levant Platform, comprising a detailed physical-, bio-, chemo-and sequence stratigraphy. Carbonate content of these strata reflects overall sequence stratigraphic development, and demonstrates a dramatic 3rd-order-scale cycle that is also apparent in the delta C-13 record. Updated radioisotopic constraints and astrochronologic testing provide support for the inference of an similar to 1 million year long sea-level oscillation associated with this 3rd-order cycle, which likely reflects a long-period obliquity (1.2 Myr) control on eustasy and stratigraphic sequence development, linked to the global carbon cycle. The observation of cyclic sea-level fluctuations on this time scale suggests sustained global modulation of continental fresh-water-storage. The hypothesized link between astronomical forcing and sea-level forms a baseline approach in the global correlation of sequence boundaries. C1 [Wendler, Jens E.; Wendler, Ines] NMNH, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Meyers, Stephen R.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Wendler, Jens E.; Wendler, Ines; Kuss, Jochen] Univ Bremen, Dept Geosci, D-28334 Bremen, Germany. RP Wendler, JE (reprint author), Univ Bremen, Dept Geosci, POB 330440, D-28334 Bremen, Germany. EM wendler@uni-bremen.de FU DFG [KU 642/B20-1, WE 4587/1-1]; US NSF [EAR-0959108] FX This research was funded by the DFG grants KU 642/B20-1 and WE 4587/1-1 (Wendler), and US NSF grant EAR-0959108 (Meyers). We thank A. Masri (NRA, Jordan), R. Stein (AWI Bremerhaven), and M. Segl (Bremen University) for technical assistance. We are grateful to L. Hinnov (Johns Hopkins University), G. Weedon (Met Office Wallingford) and B. Huber (Smithsonian Institution) for comments on an earlier version of the manuscript. B. Sageman (Northwestern University) and M. Arthur (Pennsylvania State University) provided delta13C data from the U.S.G.S. #1 Portland core. NR 70 TC 21 Z9 21 U1 1 U2 16 PU GEBRUDER BORNTRAEGER PI STUTTGART PA JOHANNESSTR 3A, D-70176 STUTTGART, GERMANY SN 0078-0421 J9 NEWSL STRATIGR JI Newsl. Stratigr. PD APR PY 2014 VL 47 IS 1 BP 1 EP 19 DI 10.1127/0078-0421/2014/0038 PG 19 WC Geology SC Geology GA AH9EB UT WOS:000336443000001 ER PT J AU Buden, DW de Queiroz, K Van Rooijen, J Stinson, DW Wiles, GJ Robert, S AF Buden, Donald W. de Queiroz, Kevin Van Rooijen, Johan Stinson, Derek W. Wiles, Gary J. Robert, Sabrino TI New Information and Reappraisals Concerning Some Alien and Indigenous Snake Records from the Federated States of Micronesia and the Mariana Islands SO PACIFIC SCIENCE LA English DT Article ID BROWN TREE SNAKE; COLUBRIDAE; REPTILIA AB New information is presented on old records of four species of snakes from four different islands in Micronesia. A record of Dendrelaphis caudolineatus from Saipan is reexamined and the specimen reidentified as D. philippinensis, and a snake from Pohnpei previously recorded only as an unidentified species of Dendrelaphis is identified as D. punctulatus striolatus. We also provide supplementary data on circumstances surrounding records of a brown tree snake, Boiga irregularis, from Chuuk, and a yellow-bellied sea snake, Hydrophis platurus (Pelamis platura), from Kosrae. C1 [Buden, Donald W.] Coll Micronesia FSM, Div Nat Sci & Math, Kolonia 96941, Pohnpei, Micronesia. [de Queiroz, Kevin] Natl Museum Nat Hist, Smithsonian Inst, Div Amphibians & Reptiles, Washington, DC 20013 USA. [Van Rooijen, Johan] Netherlands Ctr Biodivers Naturalis, NL-2300 RA Leiden, Netherlands. [Stinson, Derek W.; Wiles, Gary J.] Washington Dept Fish & Wildlife, Olympia, WA 98501 USA. [Robert, Sabrino] FSM Quarantine, Weno 96942, Chunk, Micronesia. RP Buden, DW (reprint author), Coll Micronesia FSM, Div Nat Sci & Math, POB 159, Kolonia 96941, Pohnpei, Micronesia. EM don_buden@comfsm.fm NR 26 TC 0 Z9 0 U1 1 U2 6 PU UNIV HAWAII PRESS PI HONOLULU PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA SN 0030-8870 EI 1534-6188 J9 PAC SCI JI Pac. Sci. PD APR PY 2014 VL 68 IS 2 BP 287 EP 293 DI 10.2984/68.2.8 PG 7 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA AH6JY UT WOS:000336238400008 ER PT J AU Sun, Y Gu, LH Dickinson, RE Pallardy, SG Baker, J Cao, YH DaMatta, FM Dong, XJ Ellsworth, D Van Goethem, D Jensen, AM Law, BE Loos, R Martins, SCV Norby, RJ Warren, J Weston, D Winter, K AF Sun, Ying Gu, Lianhong Dickinson, Robert E. Pallardy, Stephen G. Baker, John Cao, Yonghui DaMatta, Fabio Murilo Dong, Xuejun Ellsworth, David Van Goethem, Davina Jensen, Anna M. Law, Beverly E. Loos, Rodolfo Vitor Martins, Samuel C. Norby, Richard J. Warren, Jeffrey Weston, David Winter, Klaus TI Asymmetrical effects of mesophyll conductance on fundamental photosynthetic parameters and their relationships estimated from leaf gas exchange measurements SO PLANT CELL AND ENVIRONMENT LA English DT Article DE parameter estimation; carbon cycle model; leaf photosynthesis; A/Ci curves; LeafWeb ID CARBON-ISOTOPE DISCRIMINATION; CO2 TRANSFER CONDUCTANCE; DIOXIDE RESPONSE CURVES; INTERNAL CONDUCTANCE; DIFFUSION CONDUCTANCE; RUBP CARBOXYLATION; PINUS-SYLVESTRIS; FAGUS-SYLVATICA; SEASONAL-CHANGE; SHADE LEAVES AB Worldwide measurements of nearly 130 C-3 species covering all major plant functional types are analysed in conjunction with model simulations to determine the effects of mesophyll conductance (g(m)) on photosynthetic parameters and their relationships estimated from A/C-i curves. We find that an assumption of infinite g(m) results in up to 75% underestimation for maximum carboxylation rate V-cmax, 60% for maximum electron transport rate J(max), and 40% for triose phosphate utilization rate T-u. V-cmax is most sensitive, J(max) is less sensitive, and T-u has the least sensitivity to the variation of g(m). Because of this asymmetrical effect of g(m), the ratios of J(max) to V-cmax, T-u to V-cmax and T-u to J(max) are all overestimated. An infinite g(m) assumption also limits the freedom of variation of estimated parameters and artificially constrains parameter relationships to stronger shapes. These findings suggest the importance of quantifying g(m) for understanding in situ photosynthetic machinery functioning. We show that a nonzero resistance to CO2 movement in chloroplasts has small effects on estimated parameters. A non-linear function with g(m) as input is developed to convert the parameters estimated under an assumption of infinite g(m) to proper values. This function will facilitate g(m) representation in global carbon cycle models. C1 [Sun, Ying; Dickinson, Robert E.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA. [Gu, Lianhong; Jensen, Anna M.; Norby, Richard J.; Warren, Jeffrey] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [Pallardy, Stephen G.] Univ Missouri, Dept Forestry, Columbia, MO 65211 USA. [Baker, John] Univ Minnesota, USDA Soil & Water Management Unit, St Paul, MN 55108 USA. [Baker, John] Univ Minnesota, Dept Soil Water & Climate, St Paul, MN 55108 USA. [Cao, Yonghui] Chinese Acad Forestry, Res Inst Subtrop Forestry, Fuyang, Zhejiang, Peoples R China. [DaMatta, Fabio Murilo; Vitor Martins, Samuel C.] Univ Fed Vicosa, Dept Biol Vegetal, BR-36570000 Vicosa, MG, Brazil. [Dong, Xuejun] N Dakota State Univ, Cent Grasslands Res Extens Ctr, Streeter, ND 58483 USA. [Ellsworth, David] Univ Western Sydney, Hawkesbury Inst Environm, Penrith, NSW 2751, Australia. [Van Goethem, Davina] Univ Antwerp, Dept Biosci Engn, B-2020 Antwerp, Belgium. [Law, Beverly E.] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA. [Loos, Rodolfo] Fibria Celulose SA, Technol Ctr, BR-29197900 Aracruz, Brazil. [Weston, David] Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA. [Winter, Klaus] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Gu, LH (reprint author), Oak Ridge Natl Lab, Div Environm Sci, POB 2008, Oak Ridge, TN 37831 USA. EM lianhong-gu@ornl.gov RI Warren, Jeffrey/B-9375-2012; Norby, Richard/C-1773-2012; Sun, Ying/G-6611-2016; Gu, Lianhong/H-8241-2014; Law, Beverly/G-3882-2010; OI Warren, Jeffrey/0000-0002-0680-4697; Norby, Richard/0000-0002-0238-9828; Gu, Lianhong/0000-0001-5756-8738; Law, Beverly/0000-0002-1605-1203; Ellsworth, David/0000-0002-9699-2272; DaMatta, Fabio/0000-0002-9637-8475 FU Department of Energy [DE-FG02-01ER63198]; U.S. Department of Energy, Office of Science, Biological and Environmental Research Program, Climate and Environmental Sciences Division; ORNL's LDRD programme; UT-Battelle, LLC, for the U.S. Department of Energy [DE-AC05-00OR22725]; U.S. Department of Energy [DE-FG02-03ER63683] FX We thank Dr. Tom Sharkey and two anonymous reviewers for providing insightful suggestions that led to substantial improvements of the paper. This study was carried out at multiple institutions. The support for research at UT - Austin came from the Department of Energy (DE-FG02-01ER63198). The support for research at ORNL came from the U.S. Department of Energy, Office of Science, Biological and Environmental Research Program, Climate and Environmental Sciences Division. The ORNL's LDRD programme also partially supported the research. ORNL is managed by UT-Battelle, LLC, for the U.S. Department of Energy under contract DE-AC05-00OR22725. U.S. Department of Energy support for the University of Missouri (Grant DE-FG02-03ER63683) is gratefully acknowledged. NR 59 TC 23 Z9 23 U1 5 U2 63 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0140-7791 EI 1365-3040 J9 PLANT CELL ENVIRON JI Plant Cell Environ. PD APR PY 2014 VL 37 IS 4 BP 978 EP 994 DI 10.1111/pce.12213 PG 17 WC Plant Sciences SC Plant Sciences GA AB9BV UT WOS:000332085000014 PM 24117476 ER PT J AU Boldt, LN Stritzinger, MD Burns, C Hsiao, E Phillips, MM Goobar, A Marion, GH Stanishev, V AF Boldt, Luis N. Stritzinger, Maximilian D. Burns, Chris Hsiao, Eric Phillips, M. M. Goobar, Ariel Marion, G. H. Stanishev, Vallery TI Near-Infrared K Corrections of Type Ia Supernovae and their Errors SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID LIGHT CURVES; ABSOLUTE MAGNITUDES; HUBBLE DIAGRAM; LEGACY SURVEY; REDSHIFT; PROJECT; PHOTOMETRY; SPECTRA; 1999EE; SPECTROSCOPY AB In this paper we use near-infrared (NIR) spectral observations of Type Ia supernovae (SNe Ia) to study the uncertainties inherent in NIR K corrections. To do so, 75 previously published NIR spectra of 33 SNe Ia are employed to determine K-correction uncertainties in the YJHK(s) passbands as a function of temporal phase and redshift. The resultant K corrections are then fed into an interpolation algorithm that provides mean K corrections as a function of temporal phase and robust estimates of the associated errors. These uncertainties are both statistical and intrinsic-i.e., due to the diversity of spectral features from object to object and must be included in the overall error budget of cosmological parameters constrained through the use of NIR observations of SNe Ia. Intrinsic variations are likely the dominant source of error for all four passbands at maximum light. Given the present data, the total Y-band K-correction uncertainties at maximum are smallest, amounting to +/- 0.04 mag at a redshift of z = 0.08. The J-band K-term errors are also reasonably small (+/- 0.06 mag), but intrinsic variations of spectral features and noise introduced by telluric corrections in the H-band currently limit its total K-correction errors at maximum to +/- 0.10 mag at z = 0.08. Finally, uncertainties in the K-s-band K terms at maximum amount to +/- 0.07 mag at this same redshift. These results are largely constrained by the small number of published NIR spectra of SNe Ia, which do not yet allow spectral templates to be constructed as a function of the light curve decline rate. C1 [Boldt, Luis N.] Univ Bonn, Argelander Inst Astron, D-53111 Bonn, Germany. [Stritzinger, Maximilian D.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Burns, Chris] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Hsiao, Eric; Phillips, M. M.] Carnegie Observ, Campanas Observ, La Serena, Chile. [Goobar, Ariel] Stockholm Univ, AlbaNova, Oskar Klein Ctr, Dept Phys, SE-10691 Stockholm, Sweden. [Marion, G. H.] Univ Texas Austin, Austin, TX 78712 USA. [Marion, G. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stanishev, Vallery] Inst Super Tecn, CENTRA Ctr Multidisciplinar Astrofs, P-1049001 Lisbon, Portugal. RP Boldt, LN (reprint author), Univ Bonn, Argelander Inst Astron, Hugel 71, D-53111 Bonn, Germany. RI Stanishev, Vallery/M-8930-2013 OI Stanishev, Vallery/0000-0002-7626-1181 FU Danish Agency for Science and Technology and Innovation through a Sapere Aude Level 2 grant; USA's NSF [AST-0306969, AST-0607438, AST-1008343]; National Aeronautics and Space Administration FX M. D. S. gratefully acknowledges generous support provided by the Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant. We also acknowledge support from the USA's NSF through grants AST-0306969, AST-0607438, and AST-1008343. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 46 TC 3 Z9 3 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD APR PY 2014 VL 126 IS 938 BP 324 EP 337 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH5TK UT WOS:000336193800002 ER PT J AU Fujihara, M Comizzoli, P Keefer, CL Wildt, DE Songsasen, N AF Fujihara, Mayako Comizzoli, Pierre Keefer, Carol L. Wildt, David E. Songsasen, Nucharin TI Epidermal Growth Factor (EGF) Sustains In Vitro Primordial Follicle Viability by Enhancing Stromal Cell Proliferation via MAPK and PI3K Pathways in the Prepubertal, but Not Adult, Cat Ovary SO BIOLOGY OF REPRODUCTION LA English DT Article DE cat; folliculogenesis; in vitro culture; ovary; primordial follicle ID DIFFERENTIATION FACTOR-9; STIMULATING-HORMONE; FACTOR RECEPTOR; DOMESTIC CAT; PREANTRAL FOLLICLES; GRANULOSA-CELLS; SURVIVAL; OOCYTE; CULTURE; ACTIVATION AB This study examined the influences of epidermal growth factor (EGF) and growth differentiation factor 9 (GDF9) on in vitro viability and activation of primordial follicles in the ovarian tissue of prepubertal (age,,6 mo) versus adult (age,.8 mo) cats. Ovarian cortical slices were cultured in medium containing EGF and/or GDF9 for 14 days. EGF, but not GDF9, improved (P, 0.05) follicle viability in prepubertal donors in a dosedependent fashion. Neither EGF nor GDF9 enhanced follicle viability in ovarian tissue from adults, and neither factor activated primordial follicles regardless of age group. We then explored how EGF influenced primordial follicles in the prepubertal donors by coincubation with an inhibitor of EGF receptor (AG1478), mitogen-activated protein kinase (MAPK; U0126), or phosphoinositide 3-kinase (PI3K; LY294002). EGF enhanced (P, 0.05) MAPK and AKT phosphorylation, follicle viability, and stromal cell proliferation. These effects were suppressed (P, 0.05) when the tissue was cultured with this growth factor combined with each inhibitor. To identify the underlying influence of age in response to EGF, we assessed cell proliferation and discovered a greater thriving stromal cell population in prepubertal compared to adult tissue. We conclude that EGF plays a significant role in maintaining intraovarian primordial follicle viability (but without promoting activation) in the prepubertal cat. The mechanism of action is via stimulation of MAPK and PI3K signaling pathways that, in turn, promote ovarian cell proliferation. Particularly intriguing is that the ability of cat ovarian cells to multiply in reaction to EGF is age-dependent and highly responsive in prepubertal females. C1 [Fujihara, Mayako; Comizzoli, Pierre; Wildt, David E.; Songsasen, Nucharin] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. [Keefer, Carol L.] Univ Maryland, Dept Anim & Avian Sci, College Pk, MD 20742 USA. RP Fujihara, M (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA. EM fujiharam@si.edu FU Smithsonian Institution Fellowship Program FX Supported by a grant from the Smithsonian Institution Fellowship Program and a generous gift from Dr. Clinton and Missy Kelly. NR 59 TC 11 Z9 12 U1 1 U2 4 PU SOC STUDY REPRODUCTION PI MADISON PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA SN 0006-3363 EI 1529-7268 J9 BIOL REPROD JI Biol. Reprod. PD APR PY 2014 VL 90 IS 4 AR 86 DI 10.1095/biolreprod.113.115089 PG 10 WC Reproductive Biology SC Reproductive Biology GA AH3NR UT WOS:000336031300008 PM 24554736 ER PT J AU An, FX Zheng, XZ Wang, WH Huang, JS Kong, X Wang, JX Fang, GW Zhu, FF Gu, QS Wu, H Hao, L Xia, XY AF An, Fang Xia Zheng, Xian Zhong Wang, Wei-Hao Huang, Jia-Sheng Kong, Xu Wang, Jun-Xian Fang, Guan Wen Zhu, Feifan Gu, Qiu-Sheng Wu, Hong Hao, Lei Xia, Xiao-Yang TI THE PROPERTIES OF H alpha EMISSION-LINE GALAXIES AT z=2.24 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: luminosity function, mass function; galaxies: star formation ID STAR-FORMING GALAXIES; HIGH-REDSHIFT GALAXIES; DEEP FIELD-SOUTH; SPECTRAL ENERGY-DISTRIBUTIONS; EXTRAGALACTIC LEGACY SURVEY; YALE-CHILE MUSYC; COLD DARK-MATTER; EQUAL-TO 2.5; LUMINOSITY FUNCTION; DUST EXTINCTION AB Using deep narrowband H(2)S1 and K-s-band imaging data obtained with CFHT/WIRCam, we identify a sample of 56 H alpha emission-line galaxies (ELGs) at z = 2.24 with the 5 sigma depths of H(2)S1 = 22.8 and K-s = 24.8 (AB) over a 383 arcmin(2) area in the Extended Chandra Deep Field South. A detailed analysis is carried out with existing multi-wavelength data in this field. Three of the 56 H alpha ELGs are detected in Chandra 4 Ms X-ray observations and two of them are classified as active galactic nuclei. The rest-frame UV and optical morphologies revealed by HST/ACS and WFC3 deep images show that nearly half of the H alpha ELGs are either merging systems or have a close companion, indicating that the merging/interacting processes play a key role in regulating star formation at cosmic epoch z = 2-3. About 14% are too faint to be resolved in the rest-frame UV morphology due to high dust extinction. We estimate dust extinction from spectral energy distributions. We find that dust extinction is generally correlated with Ha luminosity and stellar mass. Our results suggest that H alpha ELGs are representative of star-forming galaxies. Applying extinction corrections to individual objects, we examine the intrinsic Ha luminosity function (LF) at z = 2.24, obtaining a best-fit Schechter function characterized by a faint-end slope of alpha similar or equal to -1.3. This is shallower than the typical slope of a z-1.6 in previous works based on constant extinction correction. We demonstrate that this difference is mainly due to the different extinction corrections. The proper extinction correction is thus the key to recovering the intrinsic LF as the extinction globally increases with H alpha luminosity. Moreover, we find that our H alpha LF mirrors the stellar mass function of star-forming galaxies at the same cosmic epoch. This finding indeed reflects the tight correlation between star formation rate and stellar mass for star-forming galaxies, i.e., the so-called main sequence. C1 [An, Fang Xia; Zheng, Xian Zhong] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. [Wang, Wei-Hao] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Huang, Jia-Sheng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huang, Jia-Sheng; Wu, Hong] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Kong, Xu; Wang, Jun-Xian; Zhu, Feifan] Univ Sci & Technol China, Dept Astron, CAS Key Lab Res Galaxies & Cosmol, Hefei 230026, Peoples R China. [Fang, Guan Wen] Dali Univ, Inst Astron & Hist Sci & Technol, Dali 671003, Yunnan, Peoples R China. [Fang, Guan Wen] Nanjing Univ, Key Lab Modern Astron & Astrophys, Minist Educ, Nanjing 210093, Jiangsu, Peoples R China. [Gu, Qiu-Sheng] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. [Hao, Lei] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Xia, Xiao-Yang] Tianjin Normal Univ, Tianjin Astrophys Ctr, Tianjin 300387, Peoples R China. RP An, FX (reprint author), Chinese Acad Sci, Purple Mt Observ, West Beijing Rd 2, Nanjing 210008, Jiangsu, Peoples R China. EM fangxiaan@pmo.ac.cn FU National Astronomical Observatories; Special Fund for Astronomy from the Ministry of Finance; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [XDB09000000]; National Basic Research Program of China (973 Program) [2013CB834900]; National Science Council of Taiwan [102-2119-M-001-007-MY3]; National Natural Science Foundation of China (NSFC) [11225315, 11320101002]; Specialized Research Fund for the Doctoral Program of Higher Education (SRFDP) [20123402110037] FX We are grateful to the referee for valuable comments and suggestions, which have improved our manuscript. F.X.A. acknowledges Cong Ma for his kind assistance. This research uses data obtained through the Telescope Access Program (TAP), which is funded by the National Astronomical Observatories and the Special Fund for Astronomy from the Ministry of Finance. This work is supported by the Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences (Grant No. XDB09000000) and the National Basic Research Program of China (973 Program 2013CB834900). W.-H.W. acknowledges the grant of the National Science Council of Taiwan (102-2119-M-001-007-MY3). X.K. is supported by the National Natural Science Foundation of China (NSFC; Nos. 11225315 and 11320101002) and the Specialized Research Fund for the Doctoral Program of Higher Education (SRFDP, No. 20123402110037). NR 85 TC 10 Z9 10 U1 2 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 APR 1 PY 2014 VL 784 IS 2 AR 152 DI 10.1088/0004-637X/784/2/152 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400067 ER PT J AU Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Blandford, RD Borgland, AW Bregeon, J Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cavazzuti, E Cecchi, C Chaves, RCG Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J D'Ammando, F de Angelis, A Dermer, CD Digel, SW Silva, EDE Drell, PS Drlica-Wagner, A Favuzzi, C Focke, WB Franckowiak, A Fukazawa, Y Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Hadasch, D Hayashida, M Hays, E Hughes, RE Jackson, MS Jogler, T Knodlseder, J Kuss, M Lande, J Larsson, S Longo, F Loparco, F Lovellette, MN Lubrano, P Mazziotta, MN Mehault, J Michelson, PF Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nemmen, R Nuss, E Ohsugi, T Omodei, N Orienti, M Orlando, E Paneque, D Perkins, JS Piron, F Pivato, G Prokhorov, D Raino, S Razzano, M Razzaque, S Reimer, A Reimer, O Ritz, S Romoli, C Sanchez-Conde, M Sanchez, DA Sgro, C Siskind, EJ Spandre, G Spinelli, P Takahashi, H Tanaka, T Tibaldo, L Tinivella, M Tosti, G Troja, E Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Winer, BL Wood, KS Yang, Z AF Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Blandford, R. D. Borgland, A. W. Bregeon, J. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cavazzuti, E. Cecchi, C. Chaves, R. C. G. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. D'Ammando, F. de Angelis, A. Dermer, C. D. Digel, S. W. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Focke, W. B. Franckowiak, A. Fukazawa, Y. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Hadasch, D. Hayashida, M. Hays, E. Hughes, R. E. Jackson, M. S. Jogler, T. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Mazziotta, M. N. Mehault, J. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nemmen, R. Nuss, E. Ohsugi, T. Omodei, N. Orienti, M. Orlando, E. Paneque, D. Perkins, J. S. Piron, F. Pivato, G. Prokhorov, D. Raino, S. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Ritz, S. Romoli, C. Sanchez-Conde, M. Sanchez, D. A. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Takahashi, H. Tanaka, T. Tibaldo, L. Tinivella, M. Tosti, G. Troja, E. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Winer, B. L. Wood, K. S. Yang, Z. TI Fermi LARGE AREA TELESCOPE OBSERVATIONS OF BLAZAR 3C 279 OCCULTATIONS BY THE SUN SO ASTROPHYSICAL JOURNAL LA English DT Article DE astroparticle physics; gamma rays: general; occultations; quasars: individual (3C 279); Sun: X-rays, gamma rays ID ACTIVE GALACTIC NUCLEI; GAMMA-RAY EMISSION; MAGNETIC-FIELDS; PAIR HALOS; EGRET DATA; CONSEQUENCES; PHOTON; AXION AB Observations of occultations of bright. gamma-ray sources by the Sun may reveal predicted pair halos around blazars and/or new physics, such as, e.g., hypothetical light dark matter particles-axions. We use Fermi Gamma-Ray Space Telescope (Fermi) data to analyze four occultations of blazar 3C 279 by the Sun on October 8 each year from 2008 to 2011. A combined analysis of the observations of these occultations allows a point-like source at the position of 3C 279 to be detected with significance of approximate to 3 sigma, but does not reveal any significant excess over the flux expected from the quiescent Sun. The likelihood ratio test rules out complete transparency of the Sun to the blazar. gamma-ray emission at a 3s confidence level. C1 [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.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Pivato, G.; Romoli, C.; Tibaldo, L.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bechtol, K.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Prokhorov, D.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Tanaka, T.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Bechtol, K.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Prokhorov, D.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Tanaka, T.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Bellazzini, R.; Bregeon, J.; Kuss, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bruel, P.] Ecole Polytech, CNRS IN2P3, Lab Leprince Ringuet, Palaiseau, France. [Caliandro, G. A.; Hadasch, D.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cavazzuti, E.; Ciprini, S.; Gasparrini, D.; Giommi, P.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Cecchi, C.; D'Ammando, F.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA IRFU CNRS, F-91191 Gif Sur Yvette, France. [Cheung, C. C.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS IN2P3, Lab Univers & Particules Montpellier, Montpellier, France. [D'Ammando, F.; Mehault, J.] IASF Palermo, I-90146 Palermo, Italy. [Chekhtman, A.; D'Ammando, F.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Grp Coll Udine, Ist Nazl Fis Nucl, Sez Trieste, I-33100 Udine, Italy. [Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [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. [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. [Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.; Hays, E.; Nemmen, R.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Jackson, M. S.] Royal Inst Technol KTH, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden. [Jackson, M. S.; Larsson, S.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Knoedlseder, J.; Yang, Z.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France. [Larsson, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Moiseev, A. A.; Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA. [Moiseev, A. A.; Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [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.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Astron & Astrophys, Santa Cruz, CA 95064 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. [Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. RP Barbiellini, G (reprint author), Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. EM imos@stanford.edu; phdmitry@stanford.edu RI Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Orlando, E/R-5594-2016; OI Reimer, Olaf/0000-0001-6953-1385; Caraveo, Patrizia/0000-0003-2478-8018; Morselli, Aldo/0000-0002-7704-9553; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Giordano, Francesco/0000-0002-8651-2394; giommi, paolo/0000-0002-2265-5003; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Bastieri, Denis/0000-0002-6954-8862; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Gasparrini, Dario/0000-0002-5064-9495 NR 24 TC 4 Z9 4 U1 1 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 118 DI 10.1088/0004-637X/784/2/118 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400033 ER PT J AU Crawford, TM Schaffer, KK Bhattacharya, S Aird, KA Benson, BA Bleem, LE Carlstrom, JE Chang, CL Cho, HM Crites, AT de Haan, T Dobbs, MA Dudley, J George, EM Halverson, NW Holder, GP Holzapfel, WL Hoover, S Hou, Z Hrubes, JD Keisler, R Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D McMahon, JJ Mehl, J Meyer, SS Millea, M Mocanu, LM Mohr, JJ Montroy, TE Padin, S Plagge, T Pryke, C Reichardt, CL Ruhl, JE Sayre, JT Shaw, L Shirokoff, E Spieler, HG Staniszewski, Z Stark, AA Story, KT van Engelen, A Vanderlinde, K Vieira, JD Williamson, R Zahn, O AF Crawford, T. M. Schaffer, K. K. Bhattacharya, S. Aird, K. A. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Cho, H-M. Crites, A. T. de Haan, T. Dobbs, M. A. Dudley, J. George, E. M. Halverson, N. W. Holder, G. P. 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. McMahon, J. J. Mehl, J. Meyer, S. S. Millea, M. Mocanu, L. M. Mohr, J. J. Montroy, T. E. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Ruhl, J. E. Sayre, J. T. 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. Zahn, O. TI A MEASUREMENT OF THE SECONDARY-CMB AND MILLIMETER-WAVE-FOREGROUND BISPECTRUM USING 800 deg(2) OF SOUTH POLE TELESCOPE DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; methods: data analysis ID MICROWAVE BACKGROUND ANISOTROPIES; PROBE WMAP OBSERVATIONS; ATACAMA COSMOLOGY TELESCOPE; ZELDOVICH POWER SPECTRUM; SPT-SZ SURVEY; STAR-FORMING GALAXIES; X-RAY OBSERVATIONS; NUMBER COUNTS; IMPROVED CONSTRAINTS; PRESSURE PROFILES AB We present a measurement of the angular bispectrum of the millimeter-wave sky in observing bands centered at roughly 95, 150, and 220 GHz, on angular scales of 1' less than or similar to theta less than or similar to 10' (multipole number 1000 less than or similar to l less than or similar to 10,000). At these frequencies and angular scales, the main contributions to the bispectrum are expected to be the thermal Sunyaev-Zel'dovich (tSZ) effect and emission from extragalactic sources, predominantly dusty, star-forming galaxies (DSFGs) and active galactic nuclei. We measure the bispectrum in 800 deg(2) of three-band South Pole Telescope data, and we use a multi-frequency fitting procedure to separate the bispectrum of the tSZ effect from the extragalactic source contribution. We simultaneously detect the bispectrum of the tSZ effect at > 10 sigma, the unclustered component of the extragalactic source bispectrum at > 5 sigma in each frequency band, and the bispectrum due to the clustering of DSFGs-i.e., the clustered cosmic infrared background (CIB) bispectrum-at > 5 sigma. This is the first reported detection of the clustered CIB bispectrum. We use the measured tSZ bispectrum amplitude, compared to model predictions, to constrain the normalization of the matter power spectrum to be s sigma = 0.787 +/- 0.031 and to predict the amplitude of the tSZ power spectrum at l = 3000. This prediction improves our ability to separate the thermal and kinematic contributions to the total SZ power spectrum. The addition of bispectrum data improves our constraint on the tSZ power spectrum amplitude by a factor of two compared to power spectrum measurements alone and demonstrates a preference for a nonzero kinematic SZ ( kSZ) power spectrum, with a derived constraint on the kSZ amplitude at l = 3000 of A(kSZ) = 2.9 +/- 1.6 mu K-2, or A(kSZ) = 2.6 +/- 1.8 mu K-2 if the default AkSZ > 0 prior is removed. C1 [Crawford, T. M.; Schaffer, K. K.; Bhattacharya, S.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crites, A. T.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L. M.; Padin, S.; Plagge, T.; Story, K. T.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Crawford, T. M.; Carlstrom, J. E.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Mocanu, L. M.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Schaffer, K. K.; Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Bhattacharya, S.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 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. [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. [de Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P.; Shaw, L.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [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. [Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; 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. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP Crawford, TM (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. EM tcrawfor@kicp.uchicago.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937]; NSF [PHY-1125897, AST-1009811, 0709498]; 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; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; University of Chicago Computing-Cooperative (UC3); Open Science Grid, NSF [PHY-1148698]; NASA Office of Space Science; [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, O. Zahn from a BCCP fellowship, and L. Knox and M. Millea from NSF grant 0709498.; Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) package. This research used resources of the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, and resources of the University of Chicago Computing-Cooperative (UC3), supported in part by the Open Science Grid, NSF grant PHY-1148698. 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 88 TC 20 Z9 20 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 143 DI 10.1088/0004-637X/784/2/143 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400058 ER PT J AU Dittmann, JA Irwin, JM Charbonneau, D Berta-Thompson, ZK AF Dittmann, Jason A. Irwin, Jonathan M. Charbonneau, David Berta-Thompson, Zachory K. TI TRIGONOMETRIC PARALLAXES FOR 1507 NEARBY MID-TO-LATE M DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; stars: fundamental parameters ID HUBBLE-SPACE-TELESCOPE; EARTH GJ 1214B; LOW-MASS STARS; METAL-RICH ATMOSPHERE; LSPM-NORTH CATALOG; PRE-MAIN-SEQUENCE; GUIDANCE SENSOR 3; INTERFEROMETRIC ASTROMETRY; TRANSMISSION SPECTROSCOPY; OBSERVATORY PARALLAXES AB The MEarth survey is a search for small rocky planets around the smallest, nearest stars to the Sun as identified by high proper motion with red colors. We augmented our planetary search time series with lower cadence astrometric imaging and obtained two million images of approximately 1800 stars suspected to be mid-to-late M dwarfs. We fit an astrometric model to MEarth's images for 1507 stars and obtained trigonometric distance measurements to each star with an average precision of 5 mas. Our measurements, combined with the Two Micron All Sky Survey photometry, allowed us to obtain an absolute K-s magnitude for each star. In turn, this allows us to better estimate the stellar parameters than those obtained with photometric estimates alone and to better prioritize the targets chosen to monitor at high cadence for planetary transits. The MEarth sample is mostly complete out to a distance of 25 pc for stars of type M5.5V and earlier, and mostly complete for later type stars out to 20 pc. We find eight stars that are within 10 pc of the Sun for which there did not exist a published trigonometric parallax distance estimate. We release with this work a catalog of the trigonometric parallax measurements for 1507 mid-to-late M dwarfs, as well as new estimates of their masses and radii. C1 [Dittmann, Jason A.; Irwin, Jonathan M.; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Berta-Thompson, Zachory K.] MIT, Cambridge, MA 02139 USA. RP Dittmann, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Berta-Thompson, Zachory/0000-0002-3321-4924 FU David and Lucile Packard Fellowship for Science and Engineering; National Science Foundation (NSF) [AST-0807690, AST-1109468]; MEarth Project; John Templeton Foundation FX We would like to thank the input of our referee, Dr. John Subasavage, whose comments have improved the quality of this manuscript. The authors would like to acknowledge W. Olson for his extensive assistance in code optimization, without which our results would have taken far longer to compile. We acknowledge the work of M. Irwin, which we used in this research. We gratefully acknowledge funding for the MEarth Project from the David and Lucile Packard Fellowship for Science and Engineering and from the National Science Foundation (NSF) under grant numbers AST-0807690 and AST-1109468. The MEarth team is grateful to the staff at the Fred Lawrence Whipple Observatory for their efforts in construction and maintenance of the facility and would like to thank W. Peters, T. Groner, K. Erdman-Myres, G. Alegria, R. Harris, B. Hutchins, D. Martina, D. Jankovsky, T. Welsh, R. Hyne, M. Calkins, P. Berlind, and G. Esquerdo for their support. This research has made use of NASA's Astrophysics Data System. This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. NR 92 TC 32 Z9 32 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 156 DI 10.1088/0004-637X/784/2/156 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400071 ER PT J AU Duchene, G Arriaga, P Wyatt, M Kennedy, G Sibthorpe, B Lisse, C Holland, W Wisniewski, J Clampin, M Kalas, P Pinte, C Wilner, D Booth, M Horner, J Matthews, B Greaves, J AF Duchene, G. Arriaga, P. Wyatt, M. Kennedy, G. Sibthorpe, B. Lisse, C. Holland, W. Wisniewski, J. Clampin, M. Kalas, P. Pinte, C. Wilner, D. Booth, M. Horner, J. Matthews, B. Greaves, J. TI SPATIALLY RESOLVED IMAGING OF THE TWO-COMPONENT eta Crv DEBRIS DISK WITH HERSCHEL SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; stars: individual (eta Crv) ID SUN-LIKE STARS; TERRESTRIAL PLANET FORMATION; MAIN-SEQUENCE STARS; CIRCUMSTELLAR DISK; KUIPER-BELT; SPACE-TELESCOPE; HD 207129; HOT DUST; COLLISIONAL EVOLUTION; SOLAR NEIGHBORHOOD AB We present far-infrared and submillimeter images of the eta Crv debris disk system obtained with Herschel and SCUBA-2, as well as Hubble Space Telescope visible and near-infrared coronagraphic images. In the 70 mu m Herschel image, we clearly separate the thermal emission from the warm and cold belts in the system, find no evidence for a putative dust population located between them, and precisely determine the geometry of the outer belt. We also find marginal evidence for azimuthal asymmetries and a global offset of the outer debris ring relative to the central star. Finally, we place stringent upper limits on the scattered light surface brightness of the outer ring. Using radiative transfer modeling, we find that it is impossible to account for all observed properties of the system under the assumption that both rings contain dust populations with the same properties. While the outer belt is in reasonable agreement with the expectations of steady-state collisional cascade models, albeit with a minimum grain size that is four times larger than the blow-out size, the inner belt appears to contain copious amounts of small dust grains, possibly below the blow-out size. This suggests that the inner belt cannot result from a simple transport of grains from the outer belt and rather supports a more violent phenomenon as its origin. We also find that the emission from the inner belt has not declined over three decades, a much longer timescale than its dynamical timescale, which indicates that the belt is efficiently replenished. C1 [Duchene, G.; Arriaga, P.; Kalas, P.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Wyatt, M.; Kennedy, G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sibthorpe, B.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Lisse, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Holland, W.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Wisniewski, J.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Clampin, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pinte, C.] France UMI 3386, CNRS INSU, UMI FCA, Paris, France. [Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Booth, M.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile. [Horner, J.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Horner, J.] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. [Matthews, B.] Natl Res Council Canada Herzberg Astron & Astroph, Victoria, BC V9E 2E7, Canada. [Greaves, J.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. RP Duchene, G (reprint author), UJF Grenoble 1, CNRS, INSU, Inst Planetol & Astrophys IPAG,UMR 5274, F-38041 Grenoble, France. RI Lisse, Carey/B-7772-2016 OI Lisse, Carey/0000-0002-9548-1526 FU NASA [1353184, NNX11AD21G]; ANR [ANR-07-BLAN-0221, ANR-2010-JCJC-0504-01, ANR-2010-JCJC-0501-01]; European Commission's 7th Framework Program [PERG06-GA-2009-256513]; European Union through ERC [279973]; NSF [AST-0909188]; JPL/NASA [NMO711043]; NSERC Discovery Accelerator Supplement FX We are grateful to Tushar Mittal, Christine Chen, and Karl Stapelfeldt for discussions regarding various aspects of the data analyzed here, and to Angelo Ricarte and Noel Moldvai for their contribution to the modified blackbody model used in this work. We thank the DEBRIS team for many and varied fruitful discussions throughout the duration of this project. In particular, we are grateful to Paul Harvey for his review of a draft of this manuscript. Comments from an anonymous referee also helped improved this manuscript. This work was supported in part by NASA through a contract (No. 1353184, PI: H. M. Butner) issued by the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. We acknowledge the Service Commun de Calcul Intensif de l'Observatoire de Grenoble (SCCI) for computations on the super-computer funded by ANR (contracts ANR-07-BLAN-0221, ANR-2010-JCJC-0504-01 and ANR-2010-JCJC-0501-01) and the European Commission's 7th Framework Program (contract PERG06-GA-2009-256513). M.W. and G.K. are grateful for support from the European Union through ERC grant number 279973. C.L. acknowledges support from grants NASA NNX11AB21G and NSF AAG-NNX09AU31G in working on this project. P.K. acknowledges support from NASA NNX11AD21G, NSF AST-0909188, and JPL/NASA award NMO711043. M.B. acknowledges support from an NSERC Discovery Accelerator Supplement. Data presented in this paper were obtained with Herschel, an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. Additional data presented in this work were obtained at the JCMT, which is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK, the Netherlands Organisation for Scientific Research and the National Research Council of Canada. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. 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 SIMBAD database, operated at CDS, Strasbourg, France, and of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 95 TC 18 Z9 18 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 148 DI 10.1088/0004-637X/784/2/148 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400063 ER PT J AU Jiang, YF Stone, JM Davis, SW AF Jiang, Yan-Fei Stone, James M. Davis, Shane W. TI RADIATION MAGNETOHYDRODYNAMIC SIMULATIONS OF THE FORMATION OF HOT ACCRETION DISK CORONAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; magnetohydrodynamics (MHD); methods: numerical; radiative transfer ID X-RAY BINARIES; DOMINATED ACCRETION; BLACK-HOLE; GAS-PRESSURE; COMPARABLE RADIATION; MAGNETIZED CORONA; LOCAL SIMULATIONS; SEYFERT-GALAXIES; GALACTIC NUCLEI; SPECTRA AB A new mechanism to form a magnetic pressure supported, high temperature corona above the photosphere of an accretion disk is explored using three dimensional radiation magnetohydrodynamic (MHD) simulations. The thermal properties of the disk are calculated self-consistently by balancing radiative cooling through the surfaces of the disk with heating due to dissipation of turbulence driven by magneto-rotational instability (MRI). As has been noted in previous work, we find the dissipation rate per unit mass increases dramatically with height above the mid-plane, in stark contrast to the a-disk model which assumes this quantity is a constant. Thus, we find that in simulations with a low surface density (and therefore a shallow photosphere), the fraction of energy dissipated above the photosphere is significant (about 3.4% in our lowest surface density model), and this fraction increases as surface density decreases. When a significant fraction of the accretion energy is dissipated in the optically thin photosphere, the gas temperature increases substantially and a high temperature, magnetic pressure supported corona is formed. The volume-averaged temperature in the disk corona is more than 10 times larger than at the disk mid-plane. Moreover, gas temperature in the corona is strongly anti-correlated with gas density, which implies the corona formed by MRI turbulence is patchy. This mechanism to form an accretion disk corona may help explain the observed relation between the spectral index and luminosity from active galactic nucleus (AGNs), and the soft X-ray excess from some AGNs. It may also be relevant to spectral state changes in X-ray binaries. C1 [Jiang, Yan-Fei] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jiang, Yan-Fei; Stone, James M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Davis, Shane W.] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H4, Canada. RP Jiang, YF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA ATP program [NNX11AF49G]; U.S. National Science Foundation [NSF-OCI-108849, NSF-AST-1333091] FX Y.F.J. thanks Jenny Greene, Yue Shen, and Jianfeng Wu for helpful discussions on the X-ray and optical observations of AGNs, and J. Goodman for discussions which motivated this project. We also thank the anonymous referee for helpful comments that improved the paper. This work was supported by the NASA ATP program through grant NNX11AF49G, and by computational resources provided by the Princeton Institute for Computational Science and Engineering. Some of the simulations were performed on the Pleiades Supercomputer provided by NASA. Y. F. J. is supported by NASA through Einstein Postdoctoral Fellowship grant number PF-140109 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. This work was also supported in part by the U.S. National Science Foundation, grant NSF-OCI-108849 and NSF-AST-1333091. NR 48 TC 12 Z9 12 U1 4 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 APR 1 PY 2014 VL 784 IS 2 AR 169 DI 10.1088/0004-637X/784/2/169 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400084 ER PT J AU Morganson, E Burgett, WS Chambers, KC Green, PJ Kaiser, N Magnier, EA Marshall, PJ Morgan, JS Price, PA Rix, HW Schlafly, EF Tonry, JL Walter, F AF Morganson, E. Burgett, W. S. Chambers, K. C. Green, P. J. Kaiser, N. Magnier, E. A. Marshall, P. J. Morgan, J. S. Price, P. A. Rix, H. -W. Schlafly, E. F. Tonry, J. L. Walter, F. TI MEASURING QUASAR VARIABILITY WITH Pan-STARRS1 AND SDSS SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars: general ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; EFFICIENT PHOTOMETRIC SELECTION; LARGE-MAGELLANIC-CLOUD; HIGH-REDSHIFT QUASARS; 7TH DATA RELEASE; OPTICAL VARIABILITY; STRIPE 82; CANDIDATE SELECTION; TIME VARIABILITY AB We measure quasar variability using the Panoramic Survey Telescope and Rapid Response System 1 Survey (Pan-STARRS1 or PS1) and the Sloan Digital Sky Survey (SDSS) and establish a method of selecting quasars via their variability in 10(4) deg(2) surveys. We use 10(5) spectroscopically confirmed quasars that have been well measured in both PS1 and SDSS and take advantage of the decadal timescales that separate SDSS measurements and PS1 measurements. A power law model fits the data well over the entire time range tested, 0.01-10 yr. Variability in the current PS1-SDSS data set can efficiently distinguish between quasars and nonvarying objects. It improves the purity of a griz quasar color cut from 4.1% to 48% while maintaining 67% completeness. Variability will be very effective at finding quasars in data sets with no u band and in redshift ranges where exclusively photometric selection is not efficient. We show that quasars' rest-frame ensemble variability, measured as a root mean squared in. magnitudes, is consistent with V (z, L, t) = A(0)(1 + z)(0.37)(L/L-0)(-0.16)(t/1yr)(0.246), where L-0 = 1046 erg s(-1) and A(0) = 0.190, 0.162, 0.147, or 0.141 in the g(P1), r(P1), i(P1), or (zP1) filter, respectively. We also fit across all four filters and obtain median variability as a function of z, L, and. as lambda (z, L, lambda, t) = 0.079(1 + z)(0.15) (L/L-0)(-0.2) (lambda/1000 nm)(-0.44) (t/1yr)(0.246). C1 [Morganson, E.; Rix, H. -W.; Schlafly, E. F.; Walter, F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Burgett, W. S.; Chambers, K. C.; Kaiser, N.; Magnier, E. A.; Morgan, J. S.; Tonry, J. L.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Green, P. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marshall, P. J.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Morganson, E (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM morganson@mpia.de OI Chambers, Kenneth /0000-0001-6965-7789; Schlafly, Edward Ford/0000-0002-3569-7421 FU National Aeronautics and Space Administration [NNX08AR22G] FX The PS1 surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, and the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, and the Las Cumbres Observatory Global Telescope Network, Incorporated, the National Central University of Taiwan, and the National Aeronautics and Space Administration under grant NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate. NR 55 TC 18 Z9 18 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 92 DI 10.1088/0004-637X/784/2/92 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400007 ER PT J AU Pillepich, A Kuhlen, M Guedes, J Madau, P AF Pillepich, Annalisa Kuhlen, Michael Guedes, Javiera Madau, Piero TI THE DISTRIBUTION OF DARK MATTER IN THE MILKY WAY'S DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE astroparticle physics; dark matter; methods: numerical ID COSMOLOGICAL SIMULATIONS; GALAXY FORMATION; DWARF GALAXY; LAMBDA-CDM; DENSITY; HALO; KINEMATICS; SEARCH; SHAPES; CORES AB We present an analysis of the effects of dissipational baryonic physics on the local dark matter (DM) distribution at the location of the Sun, with an emphasis on the consequences for direct detection experiments. Our work is based on a comparative analysis of two cosmological simulations with identical initial conditions of a Milky Way halo, one of which (Eris) is a full hydrodynamic simulation and the other (ErisDark) is a DM-only one. We find that in Eris two distinct processes lead to a 30% enhancement of DM in the disk plane at the location of the Sun: the accretion and disruption of satellites resulting in a DM component with net angular momentum, and the contraction of baryons pulling the DM into the disk plane without forcing it to co-rotate. Owing to its particularly quiescent merger history for dark halos of Milky Way mass, the co-rotating dark disk in Eris is less massive than what has been suggested by previous work, contributing only 9% of the local DM density. Yet, since the simulation results in a realistic Milky Way analog galaxy, its DM halo provides a plausible alternative to the Maxwellian standard halo model (SHM) commonly used in direct detection analyses. The speed distribution in Eris is broadened and shifted to higher speeds, compared to its DM-only twin simulation ErisDark. At high speeds f(v) falls more steeply in Eris than in ErisDark or the SHM, easing the tension between recent results from the CDMS-II and XENON100 experiments. The non-Maxwellian aspects of f(v) are still present, but much less pronounced in Eris than in the DM-only runs. The weak dark disk increases the time-averaged scattering rate by only a few percent at low recoil energies. On the high velocity tail, however, the increase in typical speeds due to baryonic contraction results in strongly enhanced mean scattering rates compared to ErisDark, although they are still suppressed compared to the SHM. Similar trends are seen regarding the amplitude of the annual modulation, while the modulated fraction is increased compared to the SHM and decreased compared to ErisDark. C1 [Pillepich, Annalisa; Kuhlen, Michael; Madau, Piero] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Pillepich, Annalisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kuhlen, Michael] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Guedes, Javiera] ETH, Inst Astron, CH-8049 Zurich, Switzerland. RP Pillepich, A (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA. EM apillepich@cfa.harvard.edu FU NSF [OIA-1124453]; NASA [NNX12AF87G]; ETH Zurich Postdoctoral Fellowship; Marie Curie Actions for People COFUND Program FX Support for this work was provided by the NSF through grant OIA-1124453, and by NASA through grant NNX12AF87G (P.M.). J.G. was funded by the ETH Zurich Postdoctoral Fellowship and the Marie Curie Actions for People COFUND Program. The Eris Simulation was carried out at NASA's Pleiades supercomputer, the UCSC Pleiades cluster, and ErisDark was performed at the UCSC Pleiades cluster. NR 77 TC 29 Z9 29 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 161 DI 10.1088/0004-637X/784/2/161 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400076 ER PT J AU Regnier, S Alexander, CE Walsh, RW Winebarger, AR Cirtain, J Golub, L Korreck, KE Mitchell, N Platt, S Weber, M De Pontieu, B Title, A Kobayashi, K Kuzin, S DeForest, CE AF Regnier, S. Alexander, C. E. Walsh, R. W. Winebarger, A. R. Cirtain, J. Golub, L. Korreck, K. E. Mitchell, N. Platt, S. Weber, M. De Pontieu, B. Title, A. Kobayashi, K. Kuzin, S. DeForest, C. E. TI SPARKLING EXTREME-ULTRAVIOLET BRIGHT DOTS OBSERVED WITH Hi-C SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: magnetic fields; Sun: UV radiation ID DYNAMICS-OBSERVATORY SDO; SOLAR MAGNETIC ELEMENTS; CORONA; REGIONS; DIAGNOSTICS; NANOFLARES; RESOLUTION; TELESCOPE; EVENTS; PLASMA AB Observing the Sun at high time and spatial scales is a step toward understanding the finest and fundamental scales of heating events in the solar corona. The high-resolution coronal (Hi-C) instrument has provided the highest spatial and temporal resolution images of the solar corona in the EUV wavelength range to date. Hi-C observed an active region on 2012 July 11 that exhibits several interesting features in the EUV line at 193 angstrom. One of them is the existence of short, small brightenings "sparkling" at the edge of the active region; we call these EUV bright dots (EBDs). Individual EBDs have a characteristic duration of 25 s with a characteristic length of 680 km. These brightenings are not fully resolved by the SDO/AIA instrument at the same wavelength; however, they can be identified with respect to the Hi-C location of the EBDs. In addition, EBDs are seen in other chromospheric/coronal channels of SDO/AIA, which suggests a temperature between 0.5 and 1.5 MK. Based on their frequency in the Hi-C time series, we define four different categories of EBDs: single peak, double peak, long duration, and bursty. Based on a potential field extrapolation from an SDO/HMI magnetogram, the EBDs appear at the footpoints of large-scale, trans-equatorial coronal loops. The Hi-C observations provide the first evidence of small-scale EUV heating events at the base of these coronal loops, which have a free magnetic energy of the order of 10(26) erg. C1 [Regnier, S.; Alexander, C. E.; Walsh, R. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Winebarger, A. R.; Cirtain, J.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Golub, L.; Korreck, K. E.; Weber, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mitchell, N.; Platt, S.] Univ Cent Lancashire, Sch Comp Engn & Phys Sci, Preston PR1 2HE, Lancs, England. [De Pontieu, B.; Title, A.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Kobayashi, K.] Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA. [Kuzin, S.] Russian Acad Sci, PN Lebedev Phys Inst, Moscow 119991, Russia. [DeForest, C. E.] Southwest Res Inst, Boulder, CO 80302 USA. RP Regnier, S (reprint author), Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. RI Regnier, Stephane/H-9107-2012; Kuzin, Sergey/M-3435-2015; Regnier, Stephane/K-2423-2015; Platt, Simon/C-6048-2008 OI Regnier, Stephane/0000-0001-8954-4183; Regnier, Stephane/0000-0001-8954-4183; Platt, Simon/0000-0003-4431-8814 NR 32 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 134 DI 10.1088/0004-637X/784/2/134 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400049 ER PT J AU Skibba, RA Smith, MSM Coil, AL Moustakas, J Aird, J Blanton, MR Bray, AD Cool, RJ Eisenstein, DJ Mendez, AJ Wong, KC Zhu, GT AF Skibba, Ramin A. Smith, M. Stephen M. Coil, Alison L. Moustakas, John Aird, James Blanton, Michael R. Bray, Aaron D. Cool, Richard J. Eisenstein, Daniel J. Mendez, Alexander J. Wong, Kenneth C. Zhu, Guangtun TI PRIMUS: GALAXY CLUSTERING AS A FUNCTION OF LUMINOSITY AND COLOR AT 0.2 < z < 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: distances and redshifts; galaxies: evolution; galaxies: halos; galaxies: high-redshift; galaxies: statistics; large-scale structure of universe ID DIGITAL SKY SURVEY; HALO OCCUPATION DISTRIBUTION; VLT DEEP SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; STAR-FORMATION RATE; DARK-MATTER HALOES; 3-POINT CORRELATION-FUNCTIONS; 2-POINT CORRELATION-FUNCTION; LARGE-SCALE STRUCTURE; 7TH DATA RELEASE AB We present measurements of the luminosity and color-dependence of galaxy clustering at 0.2 < z < 1.0 in the Prism Multi-object Survey. We quantify the clustering with the redshift-space and projected two-point correlation functions, xi(r(p), pi) and w(p) (r(p)), using volume-limited samples constructed from a parent sample of over similar to 130,000 galaxies with robust redshifts in seven independent fields covering 9 deg(2) of sky. We quantify how the scale-dependent clustering amplitude increases with increasing luminosity and redder color, with relatively small errors over large volumes. We find that red galaxies have stronger small-scale (0.1 Mpc h(-1) < r(p) < 1 Mpc h(-1)) clustering and steeper correlation functions compared to blue galaxies, as well as a strong color dependent clustering within the red sequence alone. We interpret our measured clustering trends in terms of galaxy bias and obtain values of b(gal) approximate to 0.9-2.5, quantifying how galaxies are biased tracers of dark matter depending on their luminosity and color. We also interpret the color dependence with mock catalogs, and find that the clustering of blue galaxies is nearly constant with color, while redder galaxies have stronger clustering in the one-halo term due to a higher satellite galaxy fraction. In addition, we measure the evolution of the clustering strength and bias, and we do not detect statistically significant departures from passive evolution. We argue that the luminosity-and color-environment (or halo mass) relations of galaxies have not significantly evolved since z similar to 1. Finally, using jackknife subsampling methods, we find that sampling fluctuations are important and that the COSMOS field is generally an outlier, due to having more overdense structures than other fields; we find that "cosmic variance" can be a significant source of uncertainty for high-redshift clustering measurements. C1 [Skibba, Ramin A.; Smith, M. Stephen M.; Coil, Alison L.; Mendez, Alexander J.] Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Aird, James] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Blanton, Michael R.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Bray, Aaron D.; Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cool, Richard J.] Univ Arizona, MMT Observ, Tucson, AZ 85721 USA. [Wong, Kenneth C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Zhu, Guangtun] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Skibba, RA (reprint author), Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM rskibba@ucsd.edu RI Zhu, Guangtun/C-8552-2012; OI Zhu, Guangtun/0000-0002-7574-8078 FU NSF [AST-1055081, AST-0607701, 0908246, 0908442, 0908354]; NASA [08-ADP08-0019, NNX09AC95G] FX A.L.C. and R.A.S. acknowledge support from the NSF CAREER award AST-1055081. We thank Hong Guo, Peder Norberg, and Idit Zehavi for valuable discussions about our clustering results. This paper also benefited from discussions with Peter Behroozi, Surhud More, Doug Watson, and others at the "Galaxies in the Cosmic Web" conference in Chicago. We thank the anonymous referee for detailed comments and suggestions for improving the paper. We also thank Andrew Hearin and Ashley Ross for helpful comments on a previous draft.; We acknowledge Scott Burles for his contribution to the PRIMUS project. Funding for PRIMUS has been provided by NSF grants AST-0607701, 0908246, 0908442, 0908354, and NASA grants 08-ADP08-0019, NNX09AC95G. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. NR 183 TC 26 Z9 26 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 128 DI 10.1088/0004-637X/784/2/128 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400043 ER PT J AU Sur, S Pan, LB Scannapieco, E AF Sur, Sharanya Pan, Liubin Scannapieco, Evan TI MIXING IN MAGNETIZED TURBULENT MEDIA SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; magnetic fields; magnetohydrodynamics (MHD); turbulence ID STAGGERED MESH SCHEME; PASSIVE SCALAR; INTERGALACTIC METALS; INTRACLUSTER MEDIUM; INTERSTELLAR-MEDIUM; GALACTIC DISK; DYNAMO THEORY; 1ST STARS; SIMULATIONS; CLUSTER AB Turbulent motions are essential to the mixing of entrained fluids and are also capable of amplifying weak initial magnetic fields by small-scale dynamo action. Here we perform a systematic study of turbulent mixing in magnetized media, using three-dimensional magnetohydrodynamic simulations that include a scalar concentration field. We focus on how mixing depends on the magnetic Prandtl number, Pm, from 1 to 4 and the Mach number, M, from 0.3 to 2.4. For all subsonic flows, we find that the velocity power spectrum has a k(-5/3) slope in the early kinematic phase, but steepens due to magnetic back reactions as the field saturates. The scalar power spectrum, on the other hand, flattens compared to k(-5/3) at late times, consistent with the Obukohov-Corrsin picture of mixing as a cascade process. At higher Mach numbers, the velocity power spectrum also steepens due to the presence of shocks, and the scalar power spectrum again flattens accordingly. Scalar structures are more intermittent than velocity structures in subsonic turbulence, whereas for supersonic turbulence, velocity structures appear more intermittent than the scalars only in the kinematic phase. Independent of the Mach number of the flow, scalar structures are arranged in sheets in both the kinematic and saturated phases of the magnetic field evolution. For subsonic turbulence, scalar dissipation is hindered in the strong magnetic field regions, probably due to Lorentz forces suppressing the buildup of scalar gradients, whereas for supersonic turbulence, scalar dissipation increases monotonically with increasing magnetic field strength. At all Mach numbers, mixing is significantly slowed by the presence of dynamically important small-scale magnetic fields, implying that mixing in the interstellar medium and in galaxy clusters is less efficient than modeled in hydrodynamic simulations. C1 [Sur, Sharanya; Scannapieco, Evan] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Pan, Liubin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sur, S (reprint author), Arizona State Univ, Sch Earth & Space Explorat, POB 876004, Tempe, AZ 85287 USA. EM sharanya.sur@asu.edu; lpan@cfa.harvard.edu; evan.scannapieco@asu.edu FU National Science Foundation [AST11-03608]; NASA theory [NNX09AD106]; Clay postdoctoral fellowship at Harvard-Smithsonian Center for Astrophysics; Advanced Computing Center at Arizona State University; Texas Advanced Computing Center (TACC) at The University of Texas at Austin; Extreme Science and Engineering Discovery Environment (XSEDE) for providing HPC [TG-AST130021] FX S. S. and E. S. were supported by the National Science Foundation under grant AST11-03608 and NASA theory grant NNX09AD106. L. P. acknowledges support from the Clay postdoctoral fellowship at Harvard-Smithsonian Center for Astrophysics. The authors also acknowledge the Advanced Computing Center at Arizona State University (http://a2c2.asu.edu/), the Texas Advanced Computing Center (TACC) at The University of Texas at Austin (http://www.tacc.utexas.edu), and the Extreme Science and Engineering Discovery Environment (XSEDE) for providing HPC resources via grant TG-AST130021, which have contributed to the results reported within this paper. We thank Robert Fisher, Dongwook Lee, and Dean Townsley for helpful discussions. The FLASH code is developed in part by the DOE-supported Alliances Center for Astrophysical Thermonuclear Flashes (ASC) at the University of Chicago. NR 65 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2014 VL 784 IS 2 AR 94 DI 10.1088/0004-637X/784/2/94 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG6HJ UT WOS:000335519400009 ER PT J AU Yeshurun, R Yaroshevich, A AF Yeshurun, Reuven Yaroshevich, Alla TI Bone projectile injuries and Epipaleolithic hunting: new experimental and archaeological results SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Bone modification; Experimental archaeology; Projectiles; Taphonomy; Hunting methods; Natufian; Microliths ID EL-WAD TERRACE; SOUTHERN LEVANT; MOUNT-CARMEL; RAQEFET CAVE; MT.-CARMEL; STONE-AGE; CUT MARKS; GAZELLE; ISRAEL; SITE AB Hunting was an important aspect of life in the Epipaleolithic period of the Levant (ca. 24,000 -11,500 cal. BP), but direct evidence on hunting methods and techniques is scarce, mainly due to the illusive archaeological signature of animal capture methods. Here we approach this problem directly with the intention of reading Epipaleolithic animal remains for signs of weapon injuries. We present new experimental results from an archery experiment with microlith-tipped arrows. The shooting resulted in diagnostic holes, notches, striations and embedded flint chips on the bones of the target animal carcass. This experimental reference was integrated into a comprehensive taphonomic study of Late Epipaleolithic (Natufian) faunas. We found that, even with the help of a modern reference, Epipaleolithic bone fragmentation and preservation issues may greatly reduce the chance of recognizing projectile injuries on archaeofaunal remains. This mode of preservation illustrates the need for a systematic inspection of rib and vertebrae fragments for all types of projectile injuries, including less conspicuous types. Considering this, we managed to identify two mountain gazelle (Gazella gazella) specimens with lithic projectile injuries, the first such evidence for animal bones in Natufian context. The injuries constitute direct evidence of gazelle hunting with lithic-tipped weapons, supplementing previous inferences from diagnostic impact fracture analysis and use-wear analysis of microliths. Natufian hunters frequently targeted specific gazelle individuals (e.g., males), which may suggest that shooting at the desired animals using projectile weapons was indeed preferred over other, less focused methods for gazelle hunting. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Yeshurun, Reuven] Univ Haifa, Zinman Inst Archaeol, IL-31905 Haifa, Israel. [Yeshurun, Reuven] Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. [Yaroshevich, Alla] Israel Antiqu Author, IL-91004 Jerusalem, Israel. RP Yeshurun, R (reprint author), Univ Haifa, Zinman Inst Archaeol, IL-31905 Haifa, Israel. EM ryeshuru@research.haifa.ac.il FU Irene Levi Sala CARE Archaeological Foundation FX We thank G. Bar-Oz, M. Weinstein-Evron and an anonymous reviewer for commenting on previous drafts, and E. Gerstein and A. Regev-Gisis for their help with photography and graphics. The archery experiments were supported by the Irene Levi Sala CARE Archaeological Foundation. NR 51 TC 2 Z9 2 U1 1 U2 15 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 EI 1095-9238 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD APR PY 2014 VL 44 BP 61 EP 68 DI 10.1016/j.jas.2014.01.019 PG 8 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA AG7PS UT WOS:000335610800007 ER PT J AU Martin-Garcia, L Herrera, R Moro-Abad, L Sangil, C Barquin-Diez, J AF Martin-Garcia, Laura Herrera, Rogelio Moro-Abad, Leopoldo Sangil, Carlos Barquin-Diez, Jacinto TI Predicting the potential habitat of the harmful cyanobacteria Lyngbya majuscula in the Canary Islands (Spain) SO HARMFUL ALGAE LA English DT Article DE Harmful algae; Ecological niche modeling; Canary Islands; Potential habitat; Maxent ID EASTERN ATLANTIC-OCEAN; SPECIES DISTRIBUTIONS; DISTRIBUTION MODELS; MICROCOLEUS-LYNGBYACEUS; BENTHIC CYANOBACTERIAL; MARINE CYANOBACTERIUM; MULTIBEAM BATHYMETRY; MORETON BAY; BLOOMS; AUSTRALIA AB This study presents the ecological niche and the potential distribution of Lyngbya majuscula in the Canary Islands (Spain) based on a bloom of this species on the eastern side of the Canarian Archipelago, in the Marine Reserve of La Graciosa (MRG). This finding represents the first L majuscula bloom recorded in waters around the Canary Islands and this side of the Atlantic Ocean. The modeled suitability map revealed a potential distribution of L majuscula in rocky and sandy habitats within shallow and sheltered areas exposed to sedimentation; where L. majuscula blooms had not previously been reported. The L. majuscula bloom detected in MRG is affecting rocky and sandy communities in this area. The possible expansion of these blooms may have harmful effects on important communities in the Canary Islands, including some of high ecological importance such as the Cymodocea nodosa meadows. Results of the L. majuscula distribution model presented here can be used to develop management strategies that avoid or minimize the risk of future bloom occurrences or expansions and their negative effects on the environment. The causes of L. majuscula blooms in MRG are being investigated.(c) 2014 Elsevier B.V. All rights reserved. C1 [Martin-Garcia, Laura; Barquin-Diez, Jacinto] Univ La Laguna, Dept Anim Biol, San Cristobal la Laguna 38205, S C De Tenerife, Spain. [Herrera, Rogelio] Viceconsejeria Medio Ambiente, Serv Biodiversidad, Las Palmas Gran Canaria 35071, Spain. [Moro-Abad, Leopoldo] Viceconsejeria Medio Ambiente, Serv Biodiversidad, Santa Cruz De Tenerife 38071, S C De Tenerife, Spain. [Sangil, Carlos] Smithsonian Inst, Smithsonian Trop Res Inst, Panama City 084303092, Panama. RP Martin-Garcia, L (reprint author), Univ La Laguna, Dept Anim Biol, Avda Astrofis Francisco Sanchez S-N, San Cristobal la Laguna 38205, S C De Tenerife, Spain. EM lagalathea@gmail.com; rherperg@gobiernodecanarias.org; lmoraba2@gmail.com; casangil@ull.es; jacintobarquin@gmail.com FU SIGMACAN - European Regional Development Fund (ERDF) - Canarian Agency for Research, Innovation and Information Society (Agencia Canaria de Investigacion, Innovacion y Sociedad de la Informacion, ACISII) of the Canary Government [PI 2007/004] FX The authors would like to acknowledge with thanks the scientist Maria Candelaria Gil Rodriguez and The Spanish Bank of Algae (BEA-Banco Espanol de Algas) for the identification and confirmation of L. majuscula. We are grateful to the Technological Institute of the Canary Islands (Canary Government) for wind data and the CREPAD Center (INTA) for remote sensing information, Blas M. Benito for providing the tool for the ROC analysis, and the Department of the Environment of the Canary Government (Viceconsejeria de Medio Ambiente del Gobierno de Canarias) for providing the data from the monitoring campaigns of NATURA 2000 in the Canary Islands. We are also grateful to Miguel Abella (Dive Center Corralejo), Silvia Gonzalez, Ezequiel Rodriguez, sailors and skippers of La Graciosa Marine Reserve for field logistical support, Marta Sanson for her helpful comments and Marta Rodriguez Plata for her kind linguistic revision. This research was funded under the SIGMACAN project (PI 2007/004) co-financed by the European Regional Development Fund (ERDF) and Canarian Agency for Research, Innovation and Information Society (Agencia Canaria de Investigacion, Innovacion y Sociedad de la Informacion, ACISII) of the Canary Government.[ SS] NR 68 TC 4 Z9 4 U1 4 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1568-9883 EI 1878-1470 J9 HARMFUL ALGAE JI Harmful Algae PD APR PY 2014 VL 34 BP 76 EP 86 DI 10.1016/j.hal.2014.02.008 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AG2VX UT WOS:000335276300009 ER PT J AU Henry, AG Brooks, AS Piperno, DR AF Henry, Amanda G. Brooks, Alison S. Piperno, Dolores R. TI Plant foods and the dietary ecology of Neanderthals and early modern humans SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Phytolith; Starch grain; Microfossil; Microremain; Neanderthal diet; Dental calculus ID MIDDLE STONE-AGE; MODERN HUMAN-BEHAVIOR; STARCH GRAIN ANALYSIS; UPPER SEMLIKI VALLEY; DIVISION-OF-LABOR; KEBARA CAVE; SMALL-GAME; MT CARMEL; SUBSISTENCE; TECHNOLOGY AB One of the most important challenges in anthropology is understanding the disappearance of Neanderthals. Previous research suggests that Neanderthals had a narrower diet than early modern humans, in part because they lacked various social and technological advances that lead to greater dietary variety, such as a sexual division of labor and the use of complex projectile weapons. The wider diet of early modern humans would have provided more calories and nutrients, increasing fertility, decreasing mortality and supporting large population sizes, allowing them to out-compete Neanderthals. However, this model for Neanderthal dietary behavior is based on analysis of animal remains, stable isotopes, and other methods that provide evidence only of animal food in the diet. This model does not take into account the potential role of plant food. Here we present results from the first broad comparison of plant foods in the diets of Neanderthals and early modern humans from several populations in Europe, the Near East, and Africa. Our data comes from the analysis of plant microremains (starch grains and phytoliths) in dental calculus and on stone tools. Our results suggest that both species consumed a similarly wide array of plant foods, including foods that are often considered low-ranked, like underground storage organs and grass seeds. Plants were consumed across the entire range of individuals and sites we examined, and none of the expected predictors of variation (species, geographic region, or associated stone tool technology) had a strong influence on the number of plant species consumed. Our data suggest that Neanderthal dietary ecology was more complex than previously thought. This implies that the relationship between Neanderthal technology, social behavior, and food acquisition strategies must be better explored. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Henry, Amanda G.] Max Planck Inst Evolutionary Anthropol, Plant Foods Hominin Dietary Ecol Res Grp, D-04103 Leipzig, Germany. [Brooks, Alison S.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Piperno, Dolores R.] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. [Piperno, Dolores R.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Henry, AG (reprint author), Max Planck Inst Evolutionary Anthropol, Plant Foods Hominin Dietary Ecol Res Grp, Deutsch Pl 6, D-04103 Leipzig, Germany. EM amanda_henry@eva.mpg.de; abrooks@gwu.edu; pipernod@si.edu OI Henry, Amanda/0000-0002-2923-4199 FU US NSF IGERT grant; Smithsonian Predoctoral Fellowship; Wenner Gren Dissertation Fieldwork Grant; Archaeobiology Program of the National Museum of Natural History; Max Planck Society; George Washington University; US NSF HOMINID grant; Smithsonian National Museum of Natural History; Smithsonian Tropical Research Institute FX We are grateful to R. Mundry for help with the GLMMs and R, though any mistakes are the fault of A.G.H. alone. We thank the following for providing access to the fossil and lithic material: R. Potts, M. Zeder, and J. Clark at the Smithsonian National Museum of Natural History; D. Lieberman, O. Bar-Yosef, O. Hirschensohn, and M. Morgan at Harvard University's Peabody Museum; A. Froment, P. Mennecier, and L Huet at the Musee de l'Homme; P. Semal, R. Orban, and I. Crevecoeur at the Institut royal des Sciences naturelles de Belgique; J. Svoboda, I. Jarosova, and M. Dockalova at the Moravian Museum of Brno; C. and G. Finlayson, D. Fa, and F.G. Pacheco at the Gibraltar Museum; and S. Wurz at the IZIKO Museum of South Africa. Some of the modern plant reference material was provided by the US Department of Agriculture National Plant Germplasm System and the Smithsonian National Herbarium. The South African Iridaceae reference material was collected in part by S. Stickler from the Kirstenbosch Botanical Garden, and by A.G.H. and N. Dominy at the University of California Santa Cruz Botanical Garden. A.G.H. was supported by a US NSF IGERT grant to the George Washington University's Hominid Paleobiology Doctoral Program, a Smithsonian Predoctoral Fellowship, a Wenner Gren Dissertation Fieldwork Grant, the Archaeobiology Program of the National Museum of Natural History, and the Max Planck Society. A.S.B. was supported in part by a selective excellence grant from the George Washington University and a US NSF HOMINID grant to the Smithsonian Institution. D.R.P. is supported by the Smithsonian National Museum of Natural History and the Smithsonian Tropical Research Institute. NR 84 TC 37 Z9 38 U1 15 U2 97 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 APR PY 2014 VL 69 BP 44 EP 54 DI 10.1016/j.jhevol.2013.12.014 PG 11 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AG2WX UT WOS:000335278900004 PM 24612646 ER PT J AU Russell, TD Soria, R Motch, C Pakull, MW Torres, MAP Curran, PA Jonker, PG Miller-Jones, JCA AF Russell, T. D. Soria, R. Motch, C. Pakull, M. W. Torres, M. A. P. Curran, P. A. Jonker, P. G. Miller-Jones, J. C. A. TI The face-on disc of MAXI J1836-194(star) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; X-rays: binaries; X-rays: individual: MAXI J1836-194 ID X-RAY BINARIES; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; BLACK-HOLE BINARIES; ACCRETION DISKS; SPECTRAL STATE; COMPACT JET; OUTBURST; TRANSIENTS; MODEL; INCLINATION AB We present Very Large Telescope optical spectra of the black hole candidate X-ray binary MAXI J1836-194 at the onset of its 2011 outburst. Although the spectrum was taken at the beginning of the outburst and contains a significant contribution from the optically thin synchrotron emission that originates in the radio jet, we find that the accretion disc was already large and bright. Single-peaked, narrow H alpha and He ii lambda 4686 lines imply the most face-on accretion disc observed in a black hole low-mass X-ray binary to date, with an inclination angle between 4 degrees and 15 degrees, assuming a black hole mass of between 5 and 12 M-circle dot, for distances of between 4 and 10 kpc. We use New Technology Telescope observations of the system in quiescence to place strong upper limits on the mass and radius of the donor star and the orbital period. The donor is a main-sequence star with a mass < 0.65 M-circle dot and a radius < 0.59 R-circle dot with an orbital period of < 4.9 h. From those values and Roche lobe geometry constraints we find that the compact object must be > 1.9 M-circle dot if the system is located 4 kpc away and > 7.0 M-circle dot at 10 kpc. C1 [Russell, T. D.; Soria, R.; Curran, P. A.; Miller-Jones, J. C. A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Motch, C.; Pakull, M. W.] Univ Strasbourg, Observ Astron Strasbourg, UMR 7550, CNRS, F-67000 Strasbourg, France. [Torres, M. A. P.; Jonker, P. G.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Torres, M. A. P.; Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. RP Russell, TD (reprint author), Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia. EM thomas.russell@postgrad.curtin.edu.au RI Curran, Peter/B-5293-2013; Miller-Jones, James/B-2411-2013 OI Russell, Thomas/0000-0001-6958-8891; Curran, Peter/0000-0003-3003-4626; Miller-Jones, James/0000-0003-3124-2814 FU Australian Research Council [DP 120102393]; Robert Martin Ayers Sciences Fund FX We would like to thank the anonymous referee for comments that have improved this paper. We also thank Gary Da Costa and Daniel Bayliss for their contribution and help with optical monitoring. This research was supported under the Australian Research Council's Discovery Projects funding scheme (project number DP 120102393). This research has made use of the APASS data base, located at the AAVSO web site. Funding for APASS has been provided by the Robert Martin Ayers Sciences Fund. NR 67 TC 5 Z9 5 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 APR PY 2014 VL 439 IS 2 BP 1381 EP 1389 DI 10.1093/mnras/stt2480 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6OS UT WOS:000334114000012 ER PT J AU Matsuura, M Bernard-Salas, J Evans, TL Volk, KM Hrivnak, BJ Sloan, GC Chu, YH Gruendl, R Kraemer, KE Peeters, E Szczerba, R Wood, PR Zijlstra, AA Hony, S Ita, Y Kamath, D Lagadec, E Parker, QA Reid, WA Shimonishi, T Van Winckel, H Woods, PM Kemper, F Meixner, M Otsuka, M Sahai, R Sargent, BA Hora, JL McDonald, I AF Matsuura, Mikako Bernard-Salas, Jeronimo Evans, T. Lloyd Volk, Kevin M. Hrivnak, Bruce J. Sloan, G. C. Chu, You-Hua Gruendl, Robert Kraemer, Kathleen E. Peeters, Els Szczerba, R. Wood, P. R. Zijlstra, Albert A. Hony, S. Ita, Yoshifusa Kamath, Devika Lagadec, Eric Parker, Quentin A. Reid, Warren A. Shimonishi, Takashi Van Winckel, H. Woods, Paul M. Kemper, F. Meixner, Margaret Otsuka, M. Sahai, R. Sargent, B. A. Hora, J. L. McDonald, Iain TI Spitzer Space Telescope spectra of post-AGB stars in the Large Magellanic Cloud - polycyclic aromatic hydrocarbons at low metallicities SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: AGB and post-AGB; circumstellar matter; galaxies: individual: Large Magellanic Cloud; infrared: stars ID R-CORONAE-BOREALIS; YOUNG STELLAR OBJECTS; 21 MU-M; RICH PROTOPLANETARY NEBULAE; ASYMPTOTIC GIANT BRANCH; LONG-PERIOD VARIABLES; EXTREME CARBON STARS; WOLF-RAYET STARS; INFRARED-EMISSION BANDS; LUMINOUS BLUE VARIABLES AB This paper reports variations of polycyclic aromatic hydrocarbons (PAHs) features that were found in Spitzer Space Telescope spectra of carbon-rich post-asymptotic giant branch (post-AGB) stars in the Large Magellanic Cloud (LMC). The paper consists of two parts. The first part describes our Spitzer spectral observing programme of 24 stars including post-AGB candidates. The latter half of this paper presents the analysis of PAH features in 20 carbon-rich post-AGB stars in the LMC, assembled from the Spitzer archive as well as from our own programme. We found that five post-AGB stars showed a broad feature with a peak at 7.7 mu m, that had not been classified before. Further, the 10-13 mu m PAH spectra were classified into four classes, one of which has three broad peaks at 11.3, 12.3 and 13.3 mu m rather than two distinct sharp peaks at 11.3 and 12.7 mu m, as commonly found in H ii regions. Our studies suggest that PAHs are gradually processed while the central stars evolve from post-AGB phase to planetary nebulae, changing their composition before PAHs are incorporated into the interstellar medium. Although some metallicity dependence of PAH spectra exists, the evolutionary state of an object is more significant than its metallicity in determining the spectral characteristics of PAHs for LMC and Galactic post-AGB stars. C1 [Matsuura, Mikako; Woods, Paul M.] Univ London Univ Coll, Dept Phys & Astron, London WC1E 6BT, England. [Bernard-Salas, Jeronimo] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Bernard-Salas, Jeronimo] Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France. [Evans, T. Lloyd] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Volk, Kevin M.; Meixner, Margaret] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Hrivnak, Bruce J.] Valparaiso Univ, Dept Phys & Astron, Valparaiso, IN 46383 USA. [Sloan, G. C.; Lagadec, Eric] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Chu, You-Hua; Gruendl, Robert] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Kraemer, Kathleen E.] Boston Coll, Inst Sci Res, Newton, MA 02459 USA. [Peeters, Els] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Peeters, Els] SETI Inst, Mountain View, CA 94043 USA. [Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Wood, P. R.; Kamath, Devika] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Zijlstra, Albert A.; McDonald, Iain] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Hony, S.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Ita, Yoshifusa] Tohoku Univ, Grad Sch Sci, Astron Inst, Sendai, Miyagi 9808578, Japan. [Parker, Quentin A.; Reid, Warren A.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia. [Parker, Quentin A.] Macquarie Univ, Res Ctr Astron Astrophys & Astrophoton MQAAAstro, N Ryde, NSW 2109, Australia. [Parker, Quentin A.] Australian Astron Observ, Epping, NSW 2121, Australia. [Shimonishi, Takashi] Kobe Univ, Grad Sch Sci, Dept Earth & Planetary Sci, Nada Kobe 6578501, Japan. [Van Winckel, H.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Woods, Paul M.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Kemper, F.; Otsuka, M.] AS NTU, Acad Sin, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sargent, B. A.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. [Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Matsuura, M (reprint author), Univ London Univ Coll, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM mikako@star.ucl.ac.uk RI Kemper, Francisca/D-8688-2011; Woods, Paul/E-6926-2011; OI Kemper, Francisca/0000-0003-2743-8240; Woods, Paul/0000-0003-4340-3590; Hora, Joseph/0000-0002-5599-4650; Kraemer, Kathleen/0000-0002-2626-7155; Van Winckel, Hans/0000-0001-5158-9327 FU NASA [1378453]; National Aeronautics and Space Administration; National Science Foundation; Marie Curie Actions IRSES of EU [269193]; Polish NCN [2011/01/B/ST9/02031]; National Science Council [NSC100-2112-M-001-023-MY3]; NASA; Spitzer Guest Observer programme FX MM thanks Professor I. D. Howarth for his inputs about the classifications of high-mass stars. We thank Dr J. P. Searle for providing the Herschel measurements of IRAS 05189-7008 fluxes. Support for this research was provided by NASA through contract 1378453 issued by JPL/Caltech. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France. RSz acknowledges support from Marie Curie Actions IRSES (project No. 269193) of EU and from Polish NCN grant 2011/01/B/ST9/02031. FK acknowledges financial support from the National Science Council under grant number NSC100-2112-M-001-023-MY3. RS's contribution to the research described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA, and supported via an award issued by JPL/Caltech in support of his Spitzer Guest Observer programme. NR 135 TC 13 Z9 13 U1 2 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 APR PY 2014 VL 439 IS 2 BP 1472 EP 1493 DI 10.1093/mnras/stt2495 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6OS UT WOS:000334114000016 ER PT J AU Milone, AP Marino, AF Bedin, LR Piotto, G Cassisi, S Dieball, A Anderson, J Jerjen, H Asplund, M Bellini, A Brogaard, K Dotter, A Giersz, M Heggie, DC Knigge, C Rich, RM van den Berg, M Buonanno, R AF Milone, A. P. Marino, A. F. Bedin, L. R. Piotto, G. Cassisi, S. Dieball, A. Anderson, J. Jerjen, H. Asplund, M. Bellini, A. Brogaard, K. Dotter, A. Giersz, M. Heggie, D. C. Knigge, C. Rich, R. M. van den Berg, M. Buonanno, R. TI The M 4 Core Project with HST - II. Multiple stellar populations at the bottom of the main sequence SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: Population II; globular clusters: individual: NGC 6121 ID GLOBULAR-CLUSTER M4; DWARF COOLING SEQUENCE; LOW-MASS STARS; NGC 2808; ABUNDANCE VARIATIONS; EVOLUTION DATABASE; HORIZONTAL-BRANCH; NGC-2808; GIANTS; MODELS AB The M 4 Core Project with HST is designed to exploit the Hubble Space Telescope (HST) to investigate the central regions of M 4, the Globular Cluster closest to the Sun. In this paper we combine optical and near-infrared photometry to study multiple stellar populations in M 4. We detected two sequences of M-dwarfs containing similar to 38 per cent (MSI) and similar to 62 per cent (MSII) of MS stars below the main-sequence (MS) knee. We compare our observations with those of NGC 2808, which is the only other GCs where multiple MSs of very low-mass stars have been studied to date. We calculate synthetic spectra for M-dwarfs, assuming the chemical composition mixture inferred from spectroscopic studies of stellar populations along the red giant branch, and different helium abundances, and we compare predicted and observed colours. Observations are consistent with two populations, one with primordial abundance and another with enhanced nitrogen and depleted oxygen. C1 [Milone, A. P.; Marino, A. F.; Jerjen, H.; Asplund, M.; Dotter, A.] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Bedin, L. R.; Piotto, G.] Osserv Astron Padova, Ist Nazl Astrofis, I-35122 Padua, Italy. [Piotto, G.] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35122 Padua, Italy. [Cassisi, S.; Buonanno, R.] INAF Osservatorio Astron Collurania, I-64100 Teramo, Italy. [Dieball, A.; Knigge, C.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Anderson, J.; Bellini, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Brogaard, K.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Brogaard, K.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Giersz, M.] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Heggie, D. C.] Univ Edinburgh, Sch Math, Edinburgh EH9 3JZ, Midlothian, Scotland. [Heggie, D. C.] Univ Edinburgh, Maxwell Inst Math Sci, Edinburgh EH9 3JZ, Midlothian, Scotland. [Rich, R. M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [van den Berg, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [van den Berg, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Milone, AP (reprint author), Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Via Cotter Rd, Weston, ACT 2611, Australia. EM milone@mso.anu.edu.au OI BUONANNO, Roberto/0000-0002-8255-815X; bedin, luigi/0000-0003-4080-6466; Brogaard, Karsten/0000-0003-2001-0276; Cassisi, Santi/0000-0001-5870-3735; Piotto, Giampaolo/0000-0002-9937-6387 FU Australian Research Council [DP120100475]; PRIN-INAF; PRIN MIUR; project 'The Chemical and Dynamical Evolution of the Milky Way and Local Group Galaxies' [prot. 2010LY5N2T] FX APM and HJ acknowledge the financial support from the Australian Research Council through Discovery Project grant DP120100475. SC is grateful for financial support from PRIN-INAF 2011 'Multiple Populations in Globular Clusters: their role in the Galaxy assembly' (PI: E. Carretta), and from PRIN MIUR 2010-2011, project 'The Chemical and Dynamical Evolution of the Milky Way and Local Group Galaxies', prot. 2010LY5N2T (PI: F. Matteucci). LRB and GP acknowledge PRIN-INAF 2012 funding under the project entitled: 'The M4 Core Project with Hubble Space Telescope'. NR 46 TC 18 Z9 18 U1 2 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 APR PY 2014 VL 439 IS 2 BP 1588 EP 1595 DI 10.1093/mnras/stu030 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6OS UT WOS:000334114000023 ER PT J AU Kirk, H Offner, SSR Redmond, KJ AF Kirk, Helen Offner, Stella S. R. Redmond, Kayla J. TI The formation and evolution of small star clusters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; stars: formation; open clusters and associations: general ID INITIAL MASS FUNCTION; RADIATION-HYDRODYNAMIC SIMULATIONS; SELF-GRAVITATIONAL HYDRODYNAMICS; ADAPTIVE MESH REFINEMENT; YOUNG STELLAR CLUSTERS; MOLECULAR CLOUDS; BROWN DWARFS; DENSE CORES; DYNAMICAL EVOLUTION; SOLAR NEIGHBORHOOD AB Recent observations show that small, young, stellar groupings of similar to 10 to 40 members tend to have a centrally located most massive member, reminiscent of mass segregation seen in large clustered systems. Here, we analyse hydrodynamic simulations which form small clusters and analyse their properties in a manner identical to the observations. We find that the simulated clusters possess similar properties to the observed clusters, including a tendency to exhibit mass segregation. In the simulations, the central location of the most massive member is not due to dynamical evolution, since there is little interaction between the cluster members. Instead, the most massive cluster member appears to form at the centre. We also find that the more massive stars in the cluster form at slightly earlier times. C1 [Kirk, Helen; Offner, Stella S. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kirk, Helen] McMaster Univ, Origins Inst, Hamilton, ON L8S 4M1, Canada. [Offner, Stella S. R.] Yale Univ, New Haven, CT 06511 USA. [Redmond, Kayla J.] Univ N Carolina, Asheville, NC 28804 USA. RP Kirk, H (reprint author), Natl Res Council Canada, Radio Astron Program, Ottawa, ON K1A 0R6, Canada. EM helen.kirk@nrc-cnrc.gc.ca FU Smithsonian Scholarly Studies Program; Smithsonian Astrophysical Observatory; NSF [AST-0901055]; NSF REU program under NSF; DOD ASSURE program under NSF [0754568]; Banting Postdoctoral Fellowship; NASA [51311.01, NAS 5-26555]; Space Telescope Science Institute FX The authors thank the referee, Ian Bonnell, as well as Thomas Maschberger and Cathie Clarke for helpful suggestions. The authors thank Phil Myers for interesting discussions which inspired several of the figures presented here. The authors also thank Jonathan Tan, Sourav Chatterjee and Cara Battersby for helpful discussions. This research has been supported by the Smithsonian Scholarly Studies Program (HK), the Smithsonian Astrophysical Observatory (HK, KR), the NSF through grant AST-0901055 (SSRO), and the NSF REU and DOD ASSURE programs under NSF grant no. 0754568 (KR). HK acknowledges support from the Banting Postdoctoral Fellowship, administered by the Government of Canada. Support for this work was provided by NASA through Hubble Fellowship grant #51311.01 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 (SSRO). The simulations were performed on the XSEDE Trestles resource (SSRO). NR 63 TC 9 Z9 9 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 APR PY 2014 VL 439 IS 2 BP 1765 EP 1780 DI 10.1093/mnras/stu052 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6OS UT WOS:000334114000031 ER PT J AU Bufano, F Pignata, G Bersten, M Mazzali, PA Ryder, SD Margutti, R Milisavljevic, D Morelli, L Benetti, S Cappellaro, E Gonzalez-Gaitan, S Romero-Canizales, C Stritzinger, M Walker, ES Anderson, JP Contreras, C de Jaeger, T Forster, F Gutierrez, C Hamuy, M Hsiao, E Morrell, N Olivares, F Paillas, E Parker, S Pian, E Pickering, TE Sanders, N Stockdale, C Turatto, M Valenti, S Fesen, RA Maza, J Nomoto, K Phillips, MM Soderberg, A AF Bufano, F. Pignata, G. Bersten, M. Mazzali, P. A. Ryder, S. D. Margutti, R. Milisavljevic, D. Morelli, L. Benetti, S. Cappellaro, E. Gonzalez-Gaitan, S. Romero-Canizales, C. Stritzinger, M. Walker, E. S. Anderson, J. P. Contreras, C. de Jaeger, T. Foerster, F. Gutierrez, C. Hamuy, M. Hsiao, E. Morrell, N. Olivares E, F. Paillas, E. Parker, S. Pian, E. Pickering, T. E. Sanders, N. Stockdale, C. Turatto, M. Valenti, S. Fesen, R. A. Maza, J. Nomoto, K. Phillips, M. M. Soderberg, A. TI SN 2011hs: a fast and faint Type IIb supernova from a supergiant progenitor SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; supernovae: individual: SN 2011hs ID SOUTHERN SPECTROPHOTOMETRIC STANDARDS; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; STRIPPED-ENVELOPE SUPERNOVAE; RAY TRANSIENT 080109; X-RAY; LIGHT CURVES; BINARY PROGENITOR; RADIO SUPERNOVAE; IB SUPERNOVAE; STELLAR POPULATIONS AB Observations spanning a large wavelength range, from X-ray to radio, of the Type IIb supernova (SN) 2011hs are presented, covering its evolution during the first year after explosion. The optical light curve presents a narrower shape and a fainter luminosity at peak than previously observed for Type IIb SNe. High expansion velocities are measured from the broad absorption H i and He i lines. From the comparison of the bolometric light curve and the time evolution of the photospheric velocities with hydrodynamical models, we found that SN 2011hs is consistent with the explosion of a 3-4 M-circle dot He-core progenitor star, corresponding to a main-sequence mass of 12-15 M-circle dot, that ejected a mass of Ni-56 of about 0.04 M-circle dot, with an energy of E = 8.5 x 10(50) ERG. Such a low-mass progenitor scenario is in full agreement with the modelling of the nebular spectrum taken at similar to 215 d from maximum. From the modelling of the adiabatic cooling phase, we infer a progenitor radius of approximate to 500-600 R-circle dot, clearly pointing to an extended progenitor star. The radio light curve of SN 2011hs yields a peak luminosity similar to that of SN 1993J, but with a higher mass-loss rate and a wind density possibly more similar to that of SN 2001ig. Although no significant deviations from a smooth decline have been found in the radio light curves, we cannot rule out the presence of a binary companion star. C1 [Bufano, F.; Pignata, G.; Olivares E, F.; Paillas, E.] Univ Andres Bello, Dept Ciencias Fis, Santiago 8320000, Chile. [Bersten, M.; Nomoto, K.] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Mazzali, P. A.] Liverpool John Moores Univ, IC2, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Mazzali, P. A.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Mazzali, P. A.; Benetti, S.; Cappellaro, E.; Turatto, M.; Valenti, S.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Ryder, S. D.; Stockdale, C.] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Margutti, R.; Milisavljevic, D.; Sanders, N.; Soderberg, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morelli, L.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35122 Padua, Italy. [Gonzalez-Gaitan, S.; Anderson, J. P.; de Jaeger, T.; Foerster, F.; Gutierrez, C.; Hamuy, M.; Maza, J.] Univ Chile, Dept Astron, Santiago, Chile. [Romero-Canizales, C.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Stritzinger, M.; Contreras, C.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Walker, E. S.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Hsiao, E.; Morrell, N.; Phillips, M. M.] Las Campanas Observ, Carnegie Observ, Colina El Pino, Chile. [Parker, S.] Backyard Observ Supernova Search, Canterbury, New Zealand. [Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Pian, E.] INAF Ist Astrofis Spaziale & Fis Cosm, I-40129 Bologna, Italy. [Pickering, T. E.] Southern African Astron Observ, ZA-7925 Observatory, South Africa. [Stockdale, C.] Marquette Univ, Dept Phys, Milwaukee, WI 53201 USA. [Fesen, R. A.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. RP Bufano, F (reprint author), Univ Andres Bello, Dept Ciencias Fis, Avda Republ 252, Santiago 8320000, Chile. EM milena.bufano@gmail.com RI Hamuy, Mario/G-7541-2016; Maza, Jose/I-5722-2016; OI Turatto, Massimo/0000-0002-9719-3157; Benetti, Stefano/0000-0002-3256-0016; Pian, Elena/0000-0001-8646-4858; Maza, Jose/0000-0003-2068-1328; Cappellaro, Enrico/0000-0001-5008-8619 FU FONDECYT [3120227, 3130680, 3110142, 3110042]; Millennium Center for Supernova Science [P10-064-F]; 'Fondo de Innovacion para la Competitividad, del Ministerio de Economa, Fomento y Turismo de Chile'; WPI Initiative, MEXT, Japan; PRIN-INAF; project 'Transient Universe: from ESO Large to PESSTO'; CONICYT; 'Proyecto interno UNAB' [DI-303-13/R]; Padua University [CPS0204]; INAF PRIN; Danish Agency for Science and Technology and Innovation; ALMA-CONICYT FUND [31100004]; John Simon Guggenheim Memorial Foundation; European Organization for Astronomical Research in the Southern hemisphere, Chile (ESO) [ID 184, D-115, VLT 089.D-0032, 090.D-0081]; National Science Foundation [AST-1008343]; [ASI-INAF I/088/06/0] FX FB acknowledges support from FONDECYT through post-doctoral grant 3120227. FB, GP, SGG, JPA and MH thank the support by the Millennium Center for Supernova Science (P10-064-F), with input from 'Fondo de Innovacion para la Competitividad, del Ministerio de Economa, Fomento y Turismo de Chile'. We acknowledge the Backyard Observatory Supernova Search (BOSS) team for their passionate effort and work in SN search, in particular Peter Marples (Loganholme Observatory, Queensland Australia), Greg Bock and Colin Drescher (Windaroo Observatory, Queensland, Australia). FB thanks the Kavli Institute or the Physics and Mathematics of the Universe (Tokyo) for the hospitality and support during her visit while this paper was in progress. This research has been supported in part by WPI Initiative, MEXT, Japan. EC, MT, SB and PM are partially supported by the PRIN-INAF 2011 with the project 'Transient Universe: from ESO Large to PESSTO'. SGG, JPA and FF acknowledge support by CONICYT through FONDECYT post-doctoral grant 3130680, grant 3110142 and grant 3110042, respectively. GP acknowledges partial support by 'Proyecto interno UNAB' DI-303-13/R. LM acknowledges financial support from Padua University grant CPS0204. LM also acknowledges the Universidad Andres Bello in Santiago del Chile for hospitality while this paper was in progress. EP is partially supported by grants INAF PRIN 2009 and 2011 and ASI-INAF I/088/06/0. MS and CC gratefully acknowledge generous support provided by the Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant. CRC is supported by the ALMA-CONICYT FUND Project 31100004. MH acknowledges support from the John Simon Guggenheim Memorial Foundation. We are grateful to Elizabeth Mahoney, the ATCA staff and numerous volunteer Duty Astronomers for assistance with carrying out the radio observations remotely, often at short notice. We thank Kurt Weiler for providing the radio light-curve fitting code. This work is partially based on observations collected at the European Organization for Astronomical Research in the Southern hemisphere, Chile (ESO), under the programmes: at NTT, ID 184. D-115 (P. I. S. Benetti); at VLT 089. D-0032 (P. I. P. Mazzali) and 090. D-0081 (P. I. E. Cappellaro). Observations were taken with REM, La Silla, Chile under the programme AOT 24003 (P. I. F. Bufano). This paper is based on observations obtained through the CNTAC proposals CN2011B-092, CN2011B-068 and CN2012A-059. Part of the optical/NIR photometry and spectroscopy presented in this paper were obtained by the Carnegie Supernova Project, which is supported by the National Science Foundation under Grant No. AST-1008343. NR 112 TC 14 Z9 14 U1 0 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2014 VL 439 IS 2 BP 1807 EP 1828 DI 10.1093/mnras/stu065 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6OS UT WOS:000334114000035 ER PT J AU Jimenez-Serra, I Caselli, P Fontani, F Tan, JC Henshaw, JD Kainulainen, J Hernandez, AK AF Jimenez-Serra, I. Caselli, P. Fontani, F. Tan, J. C. Henshaw, J. D. Kainulainen, J. Hernandez, A. K. TI Gas kinematics and excitation in the filamentary IRDC G035.39-00.33 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: formation; ISM: individual objects: G035.39-00.33; ISM: molecules ID INFRARED DARK CLOUDS; LARGE ARRAY OBSERVATIONS; STAR-FORMATION; MOLECULAR CLOUDS; DENSE CORES; SIO EMISSION; CO DEPLETION; MILKY-WAY; COLLISIONS; EVOLUTION AB Some theories of dense molecular cloud formation involve dynamical environments driven by converging atomic flows or collisions between preexisting molecular clouds. The determination of the dynamics and physical conditions of the gas in clouds at the early stages of their evolution is essential to establish the dynamical imprints of such collisions, and to infer the processes involved in their formation. We present multitransition (CO)-C-13 and (CO)-O-18 maps towards the IRDC G035.39-00.33, believed to be at the earliest stages of evolution. The (CO)-C-13 and (CO)-O-18 gas is distributed in three filaments (Filaments 1, 2 and 3), where the most massive cores are preferentially found at the intersecting regions between them. The filaments have a similar kinematic structure with smooth velocity gradients of similar to 0.4-0.8 km s(-1) pc(-1). Several scenarios are proposed to explain these gradients, including cloud rotation, gas accretion along the filaments, global gravitational collapse and unresolved sub-filament structures. These results are complemented by HCO+, HNC, (HCO+)-C-13 and (HNC)-C-13 single-pointing data to search for gas infall signatures. The (CO)-C-13 and (CO)-O-18 gas motions are supersonic across G035.39-00.33, with the emission showing broader linewidths towards the edges of the infrared dark cloud (IRDC). This could be due to energy dissipation at the densest regions in the cloud. The average H-2 densities are similar to 5000-7000 cm(-3), with Filaments 2 and 3 being denser and more massive than Filament 1. The (CO)-O-18 data unveil three regions with high CO depletion factors (f(D) similar to 5-12), similar to those found in massive starless cores. C1 [Jimenez-Serra, I.] European So Observ, D-85748 Garching, Germany. [Jimenez-Serra, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Caselli, P.; Henshaw, J. D.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Fontani, F.] Osserv Astrofis Arcetri, I-50125 Florence, Italy. [Tan, J. C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Kainulainen, J.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Hernandez, A. K.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Jimenez-Serra, I (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM ijimenez@eso.org OI Fontani, Francesco/0000-0003-0348-3418 FU European Union [PIIF-GA-2011-301538]; UK Science and Technology Funding Council; European Research Council (ERC) [PALs 320620]; Deutsche Forschungsgemeinschaft [1573]; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX We acknowledge the IRAM and JCMT staff, in particular H. Wiesemayer and I. Coulson, for their great help during the observations and reduction of the data. We also thank an anonymous referee for valuable comments that helped to improve the paper. We would like to thank Phil Myers, Qizhou Zhang and Eric Keto for stimulating discussions. The research leading to these results has received funding 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. PC acknowledges the financial support of successive rolling grants awarded by the UK Science and Technology Funding Council and of the European Research Council (ERC; project PALs 320620). The work of JK was supported by the Deutsche Forschungsgemeinschaft priority programme 1573 ('Physics of the Interstellar Medium'). IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). This paper has made use of JCMT data from Program M08BU35. 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 National Research Council of Canada and (until 31 March 2013) the Netherlands Organization for Scientific Research. NR 61 TC 15 Z9 15 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 APR PY 2014 VL 439 IS 2 BP 1996 EP 2013 DI 10.1093/mnras/stu078 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6OS UT WOS:000334114000047 ER PT J AU Costa, T Sijacki, D Trenti, M Haehnelt, MG AF Costa, Tiago Sijacki, Debora Trenti, Michele Haehnelt, Martin G. TI The environment of bright QSOs at z similar to 6: star-forming galaxies and X-ray emission SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics-methods; numerical-cosmology; theory-large-scale structure of Universe ID SUPERMASSIVE BLACK-HOLES; DIGITAL SKY SURVEY; MOVING-MESH COSMOLOGY; ACTIVE GALACTIC NUCLEI; DARK-MATTER HALOES; PARTICLE HYDRODYNAMICS SIMULATIONS; HIGH-REDSHIFT GALAXIES; EARLY RELEASE SCIENCE; QUASAR HOST GALAXIES; Z-GREATER-THAN-5.7 QUASARS AB We employ cosmological hydrodynamical simulations to investigate models in which the supermassive black holes powering luminous z similar to 6 quasars (QSOs) grow from massive seeds. We simulate 18 regions with densities ranging from the mean cosmic density to the highest Sigma peaks in the Millennium simulation volume. Only in the most massive haloes situated in the most overdense regions, can black holes grow to masses up to approximate to 10(9) M-circle dot by z similar to 6 without invoking super-Eddington accretion. Accretion on to the most massive black holes becomes limited by thermal active galactic nucleus (AGN) feedback by z similar to 9-8 with further growth proceeding in short Eddington-limited bursts. Our modelling suggests that current flux-limited surveys of QSOs at high redshift preferentially detect objects at their peak luminosity and therefore miss a substantial population of QSOs powered by similarly massive black holes but with low accretion rates. To test whether the required host halo masses are consistent with the observed galaxy environments of z similar to 6 QSOs, we produce realistic rest-frame UV images of our simulated galaxies. Without strong stellar feedback, our simulations predict numbers of bright galaxies larger than observed by a factor of 10 or more. Supernova-driven galactic winds reduce the predicted numbers to a level consistent with observations indicating that stellar feedback was already very efficient at high redshifts. We further investigate the effect of thermal AGN feedback on the surrounding gas. AGN outflows are highly anisotropic and mostly energy driven, pushing gas at greater than or similar to 1000 km s(-1) out to tens of kpc consistently with observations. The spatially extended thermal X-ray emission around bright QSOs is powered by these outflows and is an important diagnostic of the mechanism whereby AGN feedback energy couples to surrounding gas. C1 [Costa, Tiago; Sijacki, Debora; Trenti, Michele; Haehnelt, Martin G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Costa, Tiago; Sijacki, Debora; Trenti, Michele; Haehnelt, Martin G.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Trenti, Michele] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Costa, T (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM taf34@ast.cam.ac.uk OI Trenti, Michele/0000-0001-9391-305X; Haehnelt, Martin/0000-0001-8443-2393 FU STFC; ERC [320596] FX We thank George Becker for useful discussions and suggestions and Roberto Maiolino, Roderik Overzier and the anonymous referee for comments on the manuscript. We are also grateful to Simon White for granting access to Millennium Simulation data and Stefan Hilbert for assistance. All simulations presented in this paper were run using the DIRAC Complexity cluster based at the University of Leicester and the COSMOS Supercomputer based at the University of Cambridge funded by STFC. TC acknowledges an STFC studentship. MH acknowledges support by the FP7 ERC Grant Emergence-320596. NR 137 TC 14 Z9 14 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2014 VL 439 IS 2 BP 2146 EP 2174 DI 10.1093/mnras/stu101 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6OS UT WOS:000334114000060 ER PT J AU Werner, N Oonk, JBR Sun, M Nulsen, PEJ Allen, SW Canning, REA Simionescu, A Hoffer, A Connor, T Donahue, M Edge, AC Fabian, AC von der Linden, A Reynolds, CS Ruszkowski, M AF Werner, N. Oonk, J. B. R. Sun, M. Nulsen, P. E. J. Allen, S. W. Canning, R. E. A. Simionescu, A. Hoffer, A. Connor, T. Donahue, M. Edge, A. C. Fabian, A. C. von der Linden, A. Reynolds, C. S. Ruszkowski, M. TI The origin of cold gas in giant elliptical galaxies and its role in fuelling radio-mode AGN feedback SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: elliptical and lenticular, cD; galaxies: ISM; infrared: galaxies; X-rays: galaxies ID ACTIVE-GALACTIC-NUCLEUS; BRIGHTEST CLUSTER GALAXIES; COOLING FLOW CLUSTERS; FAR-INFRARED SPECTROSCOPY; H-ALPHA FILAMENTS; X-RAY; STAR-FORMATION; MOLECULAR-HYDROGEN; IONIZED-GAS; THERMAL-INSTABILITY AB The nature and origin of the cold interstellar medium (ISM) in early-type galaxies are still a matter of debate, and understanding the role of this component in galaxy evolution and in fuelling the central supermassive black holes requires more observational constraints. Here, we present a multiwavelength study of the ISM in eight nearby, X-ray and optically bright, giant elliptical galaxies, all central dominant members of relatively low-mass groups. Using far-infrared spectral imaging with the Herschel Photodetector Array Camera & Spectrometer, we map the emission of cold gas in the cooling lines of [C ii]lambda 157 mu m, [O i] lambda 63 mu m and [O ib] lambda 145 mu m. Additionally, we present H alpha+[N ii] imaging of warm ionized gas with the Southern Astrophysical Research (SOAR) telescope, and a study of the thermodynamic structure of the hot X-ray emitting plasma with Chandra. All systems with extended H alpha emission in our sample (6/8 galaxies) display significant [C ii] line emission indicating the presence of reservoirs of cold gas. This emission is cospatial with the optical H alpha+[N ii] emitting nebulae and the lowest entropy soft X-ray emitting plasma. The entropy profiles of the hot galactic atmospheres show a clear dichotomy, with the systems displaying extended emission-line nebulae having lower entropies beyond r greater than or similar to 1 kpc than the cold-gas-poor systems. We show that while the hot atmospheres of the cold-gas-poor galaxies are thermally stable outside of their innermost cores, the atmospheres of the cold-gas-rich systems are prone to cooling instabilities. This provides considerable weight to the argument that cold gas in giant ellipticals is produced chiefly by cooling from the hot phase. We show that cooling instabilities may develop more easily in rotating systems and discuss an alternative condition for thermal instability for this case. The hot atmospheres of cold-gas-rich galaxies display disturbed morphologies indicating that the accretion of clumpy multiphase gas in these systems may result in variable power output of the AGN jets, potentially triggering sporadic, larger outbursts. In the two cold-gas-poor, X-ray morphologically relaxed galaxies of our sample, NGC 1399 and NGC 4472, powerful AGN outbursts may have destroyed or removed most of the cold gas from the cores, allowing the jets to propagate and deposit most of their energy further out, increasing the entropy of the hot galactic atmospheres and leaving their cores relatively undisturbed. C1 [Werner, N.; Allen, S. W.; Canning, R. E. A.; von der Linden, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Werner, N.; Allen, S. W.; Canning, R. E. A.; von der Linden, A.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Oonk, J. B. R.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Sun, M.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Simionescu, A.] JAXA, Inst Space & Astronaut Sci ISAS, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Hoffer, A.; Connor, T.; Donahue, M.] Michigan State Univ, Phys & Astron Dept, E Lansing, MI 48824 USA. [Edge, A. C.] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [von der Linden, A.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Reynolds, C. S.] Univ Maryland, Maryland Astron Ctr Theory & Computat, College Pk, MD 20742 USA. [Ruszkowski, M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Ruszkowski, M.] Michigan Ctr Theoret Phys, Randall Lab 3444, Ann Arbor, MI 48109 USA. RP Werner, N (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA. EM norbertw@stanford.edu OI Edge, Alastair/0000-0002-3398-6916; Nulsen, Paul/0000-0003-0297-4493 FU NASA issued by JPL/Caltech [1428053]; US Department of Energy [DE-AC02-76SF00515]; NSF [AST 1008454]; NASA ATP [12-ATP12-0017] FX This work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through award number 1428053 issued by JPL/Caltech. This work is based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministerio da Ciencia, Tecnologia, e Inovacao (MCTI) da Republica Federativa do Brasil, the US National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC) and Michigan State University (MSU). SWA acknowledges support from the US Department of Energy under contract number DE-AC02-76SF00515. MR acknowledges the NSF grant AST 1008454 and NASA ATP grant (12-ATP12-0017). NR 136 TC 35 Z9 35 U1 1 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 APR PY 2014 VL 439 IS 3 BP 2291 EP 2306 DI 10.1093/mnras/stu006 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PB UT WOS:000334114900005 ER PT J AU Oguri, M Rusu, CE Falco, EE AF Oguri, Masamune Rusu, Cristian E. Falco, Emilio E. TI The stellar and dark matter distributions in elliptical galaxies from the ensemble of strong gravitational lenses SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: strong; galaxies: elliptical and lenticular, cD; galaxies: formation; galaxies: haloes; dark matter ID INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; SPECTROSCOPICALLY SELECTED SAMPLE; TO-LIGHT RATIO; QUASAR PG 1115+080; 3RD DATA RELEASE; X-RAY; DENSITY PROFILE; SAURON PROJECT; ACS SURVEY AB We derive the average mass profile of elliptical galaxies from the ensemble of 161 strong gravitational lens systems selected from several surveys, assuming that the mass profile scales with the stellar mass and effective radius of each lensing galaxy. The total mass profile is well fitted by a power law (r) proportional to r(gamma) with best-fitting slope gamma = -2.11 +/- 0.05. The decomposition of the total mass profile into stellar and dark matter distributions is difficult due to a fundamental degeneracy between the stellar initial mass function (IMF) and the dark matter fraction f(DM). We demonstrate that this IMF-f(DM) degeneracy can be broken by adding direct stellar mass fraction measurements by quasar microlensing observations. Our best-fitting model prefers the Salpeter IMF over the Chabrier IMF and a smaller central dark matter fraction than that predicted by adiabatic contraction models. C1 [Oguri, Masamune] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Oguri, Masamune] Univ Tokyo, Kavli IPMU, WPI, Chiba 2778583, Japan. [Rusu, Cristian E.] Natl Astron Observ Japan, Opt & Infrared Astron Div, Mitaka, Tokyo 1818588, Japan. [Rusu, Cristian E.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Falco, Emilio E.] Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. RP Oguri, M (reprint author), Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. EM masamune.oguri@ipmu.jp RI Oguri, Masamune/C-6230-2011 FU FIRST programme 'Subaru Measurements of Images and Redshifts (SuMIRe)', World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan; JSPS [23740161] FX We thank Masataka Fukugita and Surhud More for useful discussions and Dominique Sluse for comments. We also thank an anonymous referee for useful suggestions. This work was supported in part by the FIRST programme 'Subaru Measurements of Images and Redshifts (SuMIRe)', World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and grant-in-aid for Scientific Research from the JSPS (23740161). NR 110 TC 33 Z9 33 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 APR PY 2014 VL 439 IS 3 BP 2494 EP 2504 DI 10.1093/mnras/stu106 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PB UT WOS:000334114900022 ER PT J AU Percival, WJ Ross, AJ Sanchez, AG Samushia, L Burden, A Crittenden, R Cuesta, AJ Magana, MV Manera, M Beutler, F Chuang, CH Eisenstein, DJ Ho, S McBride, CK Montesano, F Padmanabhan, N Reid, B Saito, S Schneider, DP Seo, HJ Tojeiro, R Weaver, BA AF Percival, Will J. Ross, Ashley J. Sanchez, Ariel G. Samushia, Lado Burden, Angela Crittenden, Robert Cuesta, Antonio J. Magana, Mariana Vargas Manera, Marc Beutler, Florian Chuang, Chia-Hsun Eisenstein, Daniel J. Ho, Shirley McBride, Cameron K. Montesano, Francesco Padmanabhan, Nikhil Reid, Beth Saito, Shun Schneider, Donald P. Seo, Hee-Jong Tojeiro, Rita Weaver, Benjamin A. TI The clustering of Galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: including covariance matrix errors SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmology: observations; distance scale; large-scale structure of Universe ID DIGITAL SKY SURVEY; LARGE-SCALE STRUCTURE; DATA RELEASE; UNIVERSE; GROWTH; SAMPLE; Z=0.57 AB We present improved methodology for including covariance matrices in the error budget of Baryon Oscillation Spectroscopic Survey (BOSS) galaxy clustering measurements, revisiting Data Release 9 (DR9) analyses, and describing a method that is used in DR10/11 analyses presented in companion papers. The precise analysis method adopted is becoming increasingly important, due to the precision that BOSS can now reach: even using as many as 600 mock catalogues to estimate covariance of two-point clustering measurements can still lead to an increase in the errors of similar to 20 per cent, depending on how the cosmological parameters of interest are measured. In this paper, we extend previous work on this contribution to the error budget, deriving formulae for errors measured by integrating over the likelihood, and to the distribution of recovered best-fitting parameters fitting the simulations also used to estimate the covariance matrix. Both are situations that previous analyses of BOSS have considered. We apply the formulae derived to baryon acoustic oscillation (BAO) and redshift-space distortion (RSD) measurements from BOSS in our companion papers. To further aid these analyses, we consider the optimum number of bins to use for two-point measurements using the monopole power spectrum or correlation function for BAO, and the monopole and quadrupole moments of the correlation function for anisotropic-BAO and RSD measurements. C1 [Percival, Will J.; Ross, Ashley J.; Samushia, Lado; Burden, Angela; Crittenden, Robert; Manera, Marc; Tojeiro, Rita] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth P01 3FX, Hants, England. [Sanchez, Ariel G.; Montesano, Francesco; Padmanabhan, Nikhil] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Samushia, Lado] Ilia State Univ, Natl Abastumani Astrophys Observ, GE-1060 Tbilisi, Rep of Georgia. [Cuesta, Antonio J.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Magana, Mariana Vargas; Ho, Shirley] Carnegie Mellon Univ, Dept Phys, Bruce & Astrid McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Beutler, Florian; Reid, Beth; Saito, Shun; Seo, Hee-Jong] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Chuang, Chia-Hsun] Univ Autonoma Madrid, Inst Fs Teor, UAM CSIC, E-28049 Madrid, Spain. [Eisenstein, Daniel J.; McBride, Cameron K.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Saito, Shun] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Todai Inst Adv Study, Chiba 2778582, Japan. [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. [Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. RP Percival, WJ (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth P01 3FX, Hants, England. EM will.percival@port.ac.uk RI Ho, Shirley/P-3682-2014; OI Ho, Shirley/0000-0002-1068-160X; Beutler, Florian/0000-0003-0467-5438; Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470 FU UK Science & Technology Facilities Council (STFC) [ST/K0090X/1]; European Research Council [202686]; Trans-regional Collaborative Research Centre 'The Dark Universe' of the German Research Foundation (DFG) [TR33]; HEFCE; STFC; CGI/Intel; Alfred P. Sloan Foundation; National Science Foundation; US 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 WJP acknowledges support from the UK Science & Technology Facilities Council (STFC) through the consolidated grant ST/K0090X/1 and from the European Research Council through the 'Starting Independent Research' grant 202686, MDEPUGS. AGS acknowledges support from the Trans-regional Collaborative Research Centre TR33 'The Dark Universe' of the German Research Foundation (DFG). Power spectrum calculations and fits made use of the COSMOS/Universe super-computer, a UK-Dirac facility supported by HEFCE and STFC in cooperation with CGI/Intel.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 31 TC 49 Z9 49 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2014 VL 439 IS 3 BP 2531 EP 2541 DI 10.1093/mnras/stu112 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PB UT WOS:000334114900025 ER PT J AU Abramowski, A Aharonian, F Benkhali, FA Akhperjanian, AG Anguner, E Anton, G Balenderan, S Balzer, A Barnacka, A Becherini, Y Tjus, JB Bernlohr, K Birsin, E Bissaldi, E Biteau, J Bottcher, M 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 Cui, Y 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 Giavitto, G Giebels, B Glicenstein, JF Grondin, MH Grudzinska, M Haffner, S 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 Krueger, PP Laffon, H Lamanna, G Lefaucheur, J Lemiere, A Lemoine-Goumard, M Lenain, JP Lennarz, D Lohse, T Lopatin, A Lu, CC Marandon, V Marcowith, A Marx, R Maurin, G Maxted, N Mayer, M McComb, TJL Mehault, J Meintjes, PJ Menzler, U Meyer, M Moderski, R Mohamed, M Moulin, E Murach, T Naumann, CL de Naurois, M 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 Romoli, C 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 Spies, F Stawarz, L Steenkamp, R Stegmann, C Stinzing, F Stycz, K Sushch, I Szostek, A Tavernet, JP Tavernier, T Taylor, AM Terrier, R Tluczykont, M Trichard, C Valerius, K van Eldik, C van Soelen, B Vasileiadis, G Venter, C Viana, A Vincent, P Vink, J Volk, HJ Volpe, F Vorster, M Vuillaume, T Wagner, SJ Wagner, P Ward, M Weidinger, M Weitzel, Q White, R Wierzcholska, A Willmann, P Wornlein, A Wouters, D Zabalza, V Zacharias, M Zajczyk, A Zdziarski, AA Zech, A Zechlin, HS AF Abramowski, A. Aharonian, F. Benkhali, F. Ait 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. Boettcher, M. 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. Cui, Y. Dalton, M. Daniel, M. K. Davids, I. D. Degrange, B. Deil, C. deWilt, P. Dickinson, H. J. Djannati-Ataie, 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. Giavitto, G. Giebels, B. Glicenstein, J. F. Grondin, M. -H. Grudzinska, M. Haeffner, S. 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. Lemiere, A. Lemoine-Goumard, M. Lenain, J. -P. Lennarz, D. Lohse, T. Lopatin, A. Lu, C. -C. Marandon, V. Marcowith, A. Marx, R. Maurin, G. Maxted, N. Mayer, M. McComb, T. J. L. Mehault, J. Meintjes, P. J. Menzler, U. Meyer, M. Moderski, R. Mohamed, M. Moulin, E. Murach, T. Naumann, C. L. de Naurois, M. 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. Romoli, C. 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. Spies, F. Stawarz, L. Steenkamp, R. Stegmann, C. Stinzing, F. Stycz, K. Sushch, I. Szostek, A. Tavernet, J. -P. Tavernier, T. Taylor, A. M. Terrier, R. Tluczykont, M. Trichard, C. Valerius, K. van Eldik, C. van Soelen, B. Vasileiadis, G. Venter, C. Viana, A. Vincent, P. Vink, J. Voelk, H. J. Volpe, F. Vorster, M. Vuillaume, T. Wagner, S. J. Wagner, P. Ward, M. Weidinger, M. Weitzel, Q. White, R. Wierzcholska, A. Willmann, P. Woernlein, A. Wouters, D. Zabalza, V. Zacharias, M. Zajczyk, A. Zdziarski, A. A. Zech, A. Zechlin, H. -S. CA Hess Collaboration TI HESS J1640-465-an exceptionally luminous TeV gamma-ray supernova remnant SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: non-thermal; ISM: individual objects: G338.3-0.0; ISM: supernova remnants ID PULSAR WIND NEBULA; LARGE-AREA TELESCOPE; RX J1713.7-3946; X-RAY; MOLECULAR CLOUDS; FERMI-LAT; EMISSION; EVOLUTION; CATALOG; ACCELERATION AB The results of follow-up observations of the TeV gamma-ray source HESS J1640-465 from 2004 to 2011 with the High Energy Stereoscopic System (HESS) are reported in this work. The spectrum is well described by an exponential cut-off power law with photon index Gamma = 2.11 +/- 0.09(stat) +/- 0.10(sys), and a cut-off energy of E-2 = 6.0(-1.2)(+2.0) TeV. The TeV emission is significantly extended and overlaps with the northwestern part of the shell of the SNR G338.3-0.0. The new HESS results, a re-analysis of archival XMM-Newton data and multiwavelength observations suggest that a significant part of the gamma-ray emission from HESS J1640-465 originates in the supernova remnant shell. In a hadronic scenario, as suggested by the smooth connection of the GeV and TeV spectra, the product of total proton energy and mean target density could be as high as W(p)n(H) similar to 4 x 10(52)(d/10kpc)(2) erg cm(-3). C1 [Cerruti, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Abramowski, A.; Fernandes, M. V.; Heinzelmann, G.; Horns, D.; Kastendieck, M. A.; Kneiske, T.; Opitz, B.; Raue, M.; Spies, F.; Zechlin, H. -S.] Univ Hamburg, Inst Experimentalphys, D-22761 Hamburg, Germany. [Aharonian, F.; Benkhali, F. Ait; Bernloehr, K.; Brun, F.; Carrigan, S.; Casanova, S.; Deil, C.; Domainko, W.; Edwards, T.; Eger, P.; Foerster, A.; Grondin, M. -H.; Hahn, J.; Hermann, G.; Hillert, A.; Hofmann, W.; Hofverberg, P.; Krueger, P. P.; Lennarz, D.; Lu, C. -C.; Marandon, V.; Marx, R.; 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.; Weitzel, Q.; Zabalza, V.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Aharonian, F.; Drury, L. O'C.; Romoli, C.; Taylor, A. M.] Dublin Inst Adv Studies, Dublin 2, Ireland. [Aharonian, F.; Akhperjanian, A. G.; Sahakian, V.] Natl Acad Sci,Republ Armenia, Yerevan 0019, 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.; 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.; Giavitto, G.; Klepser, S.; Schulz, A.; Stegmann, C.; Stycz, K.] DESY, D-15738 Zeuthen, Germany. [Balzer, A.; Fuessling, M.; Holler, M.; Mayer, M.; Stegmann, C.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, 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.] Linnaeus Univ, Dept Phys & Elect Engn, SE-35195 Vaxjo, Sweden. [Tjus, J. Becker; Krakau, S.; Menzler, U.; Schlickeiser, R.; Weidinger, M.; Zacharias, M.] Ruhr Univ Bochum, Inst Theoret Phys Lehrstuhl IV Weltraum & Astroph, D-44780 Bochum, Germany. [Egberts, K.; Kolitzus, D.; Perez, J.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Biteau, J.; Degrange, B.; Fegan, S.; Fontaine, G.; Giebels, B.; de Naurois, M.] Ecole Polytech, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Boettcher, M.; Casanova, S.; Davids, I. D.; Krueger, P. P.; Pekeur, N. W.; Sushch, I.; Venter, C.; Vorster, M.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Boisson, C.; Cerruti, M.; Hervet, O.; Rulten, C. B.; Sol, H.; Zech, A.] Univ Paris Diderot, CNRS, Observatoire Paris, LUTH, F-92190 Meudon, France. [Bolmont, J.; Chalme-Calvet, R.; Chretien, M.; Couturier, C.; Garrigoux, T.; Kieffer, M.; Naumann, C. L.; Tavernet, J. -P.; Vincent, P.] Univ Paris 06, CNRS IN2P3, Univ Denis Diderot Paris 7, LPNHE, F-75252 Paris, France. [Bordas, P.; Cui, Y.; 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.; Moulin, E.; Peyaud, B.; Schuessler, F.; Wouters, D.] CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France. [Bulik, T.; Grudzinska, M.] Univ Warsaw, PL-00478 Warsaw, Poland. [Colafrancesco, S.] Univ Witwatersrand, Sch Phys, ZA-2050 Johannesburg, South Africa. [Cologna, G.; Grondin, M. -H.; Jankowsky, F.; Kaufmann, S.; Mohamed, M.; Quirrenbach, A.; Schwemmer, S.; Wagner, S. J.] Heidelberg Univ, D-69117 Heidelberg, Germany. [Conrad, J.; Dickinson, H. J.; Farnier, C.; Meyer, M.] Stockholm Univ, Dept Phys, Oskar Klein Ctr, Albanova Univ Ctr, SE-10691 Stockholm, Sweden. [Dalton, M.; Laffon, H.; Lemoine-Goumard, M.; Mehault, J.] Univ Bordeaux 1, CEN Bordeaux Gradignan, 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. [Djannati-Ataie, A.; Espigat, P.; Khelifi, B.; Lefaucheur, J.; Lemiere, A.; Pita, S.; Punch, M.; Tavernier, T.; Terrier, R.] Univ Paris Diderot, APC Astroparticule & Cosmol, CNRS IN2P3, CEA Irfu, F-75205 Paris 13, France. [Dubus, G.; Henri, G.; Pelletier, G.; Petrucci, P. -O.; Vuillaume, T.] UJF Grenoble 1, CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG, UMR 5274, 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. [Feinstein, F.; Fernandez, D.; Gallant, Y. A.; Marcowith, A.; Renaud, M.; Vasileiadis, G.; Zajczyk, A.] Univ Montpellier 2, Lab Univ & Particules Montpellier, CNRS IN2P3, CC 72, F-34095 Montpellier, France. [Fiasson, A.; Komin, Nu.; Krayzel, F.; Lamanna, G.; Maurin, G.; Rosier-Lees, S.; Sanchez, D. A.; Trichard, C.] Univ Savoie, CNRS IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France. [Jamrozy, M.; Ostrowski, M.; Stawarz, L.; Szostek, A.; Wierzcholska, A.] Uniwersytet Jagiellonski, PL-30244 Krakow, Poland. [Katarzynski, K.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. [Meintjes, P. J.; van Soelen, B.] Univ Free State, Dept Phys, ZA-9300 Bloemfontein, South Africa. [Rob, L.] Charles Univ Prague, Fac Math & Phys, Inst Particle & Nucl Phys, Prague 18000 8, Czech Republic. [Vink, J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. RP Abramowski, A (reprint author), Univ Hamburg, Inst Experimentalphys, Luruper Chaussee 149, D-22761 Hamburg, Germany. RI Drury, Luke/B-1916-2017; Moulin, Emmanuel/B-5959-2017; Daniel, Michael/A-2903-2010; Meyer, Manuel/E-2697-2016; Bissaldi, Elisabetta/K-7911-2016; Venter, Christo/E-6884-2011; Reimer, Olaf/A-3117-2013; Tjus, Julia/G-8145-2012; Schussler, Fabian/G-5313-2013; van Eldik, Christopher/C-3901-2013; Katarzynski, Krzysztof/G-4528-2014; Jamrozy, Marek/F-4507-2015; Katz, Uli/E-1925-2013; Casanova, Sabrina/J-8935-2013; Anton, Gisela/C-4840-2013 OI Drury, Luke/0000-0002-9257-2270; Moulin, Emmanuel/0000-0003-4007-0145; Chadwick, Paula/0000-0002-1468-2685; Kneiske, Tanja M./0000-0002-3210-6200; mohamed, mahmoud/0000-0002-4625-6242; Daniel, Michael/0000-0002-8053-7910; de los Reyes Lopez, Raquel/0000-0003-0485-9552; Kruger, Paulus/0000-0003-0664-8521; Meyer, Manuel/0000-0002-0738-7581; Bissaldi, Elisabetta/0000-0001-9935-8106; Venter, Christo/0000-0002-2666-4812; Reimer, Olaf/0000-0001-6953-1385; Schussler, Fabian/0000-0003-1500-6571; van Eldik, Christopher/0000-0001-9669-645X; Katz, Uli/0000-0002-7063-4418; Casanova, Sabrina/0000-0002-6144-9122; Anton, Gisela/0000-0003-2039-4724 FU German Ministry for Education and Research (BMBF); Max Planck Society; French Ministry for Research; CNRS-IN2P3; Astroparticle Interdisciplinary Programme of the CNRS; UK Science and Technology Facilities Council (STFC); IPNP of the Charles University; Czech Science Foundation; Polish Ministry of Science and Higher Education; South African Department of Science and Technology; National Research Foundation; University of Namibia; Humboldt foundation; NASA 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 Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Czech Science Foundation, the Polish Ministry of Science and Higher Education, 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. SO acknowledges the support of the Humboldt foundation by a Feodor-Lynen research fellowship. We are also grateful to Gabriela Castelletti, who kindly provided the 610 MHz map and Patrick Slane for the PWN model curve. The authors would also like to thank the anonymous referee for her/his detailed and constructive comments, which significantly improved the quality of this paper. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 53 TC 9 Z9 9 U1 2 U2 15 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2014 VL 439 IS 3 BP 2828 EP 2836 DI 10.1093/mnras/stu139 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PB UT WOS:000334114900046 ER PT J AU Matt, G Marinucci, A Guainazzi, M Brenneman, LW Elvis, M Lohfink, A Arevalo, P Boggs, SE Cappi, M Christensen, FE Craig, WW Fabian, AC Fuerst, F Hailey, CJ Harrison, FA Parker, M Reynolds, CS Stern, D Walton, DJ Zhang, WW AF Matt, G. Marinucci, A. Guainazzi, M. Brenneman, L. W. Elvis, M. Lohfink, A. Arevalo, P. Boggs, S. E. Cappi, M. Christensen, F. E. Craig, W. W. Fabian, A. C. Fuerst, F. Hailey, C. J. Harrison, F. A. Parker, M. Reynolds, C. S. Stern, D. Walton, D. J. Zhang, W. W. TI The soft-X-ray emission of Ark 120. XMM-Newton, NuSTAR, and the importance of taking the broad view SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; galaxies: active; galaxies: individual: Ark 120 ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; LINE REGION SIZES; SUZAKU OBSERVATIONS; CENTRAL MASSES; SKY SURVEY; SPECTRA; EXCESS; PHOTOIONIZATION; SEYFERT-1 AB We present simultaneous XMM-Newton and NuSTAR observations of the 'bare' Seyfert 1 galaxy, Ark 120, a system in which ionized absorption is absent. The NuSTAR hard-X-ray spectral coverage allows us to constrain different models for the excess soft-X-ray emission. Among phenomenological models, a cutoff power law best explains the soft-X-ray emission. This model likely corresponds to Comptonization of the accretion disc seed UV photons by a population of warm electrons: using Comptonization models, a temperature of similar to 0.3 keV and an optical depth of similar to 13 are found. If the UV-to-X-ray optxagnf model is applied, the UV fluxes from the XMM-Newton Optical Monitor suggest an intermediate black hole spin. Contrary to several other sources observed by NuSTAR, no high-energy cutoff is detected with a lower limit of 190 keV. C1 [Matt, G.; Marinucci, A.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Guainazzi, M.] European Space Astron Ctr ESA, E-28080 Madrid, Spain. [Brenneman, L. W.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lohfink, A.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Arevalo, P.] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Santiago 22, Chile. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Cappi, M.] IASF Bologna, INAF, I-40129 Bologna, Italy. [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Fabian, A. C.; Parker, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Fuerst, F.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Matt, G (reprint author), Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy. EM matt@fis.uniroma3.it RI Boggs, Steven/E-4170-2015; Cappi, Massimo/F-4813-2015; OI Boggs, Steven/0000-0001-9567-4224; Cappi, Massimo/0000-0001-6966-8920 FU National Aeronautics and Space Administration; ESA Member States; USA (NASA); Italian Space Agency under grant ASI/INAF [I/037/12/0-011/13]; European Union [312789] FX We thank the anonymous referee for useful comments which helped us to improve the clarity of the paper, and Chris Done for comments and advices on the OPTXAGNF model. This work has 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 NUSTARDAS jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The work is also based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). GM and AM acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13 and from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement n. 312789. NR 32 TC 26 Z9 26 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 APR PY 2014 VL 439 IS 3 BP 3016 EP 3021 DI 10.1093/mnras/stu159 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PB UT WOS:000334114900063 ER PT J AU Maccarone, TJ Lehmer, BD Leyder, JC Antoniou, V Hornschemeier, A Ptak, A Wik, D Zezas, A AF Maccarone, Thomas J. Lehmer, Bret D. Leyder, J. C. Antoniou, Vallia Hornschemeier, Ann Ptak, Andrew Wik, Daniel Zezas, Andreas TI A new candidate Wolf-Rayet X-ray binary in NGC 253 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: Wolf-Rayet; galaxies: individual: NGC 253; galaxies: starburst; X-rays: binaries ID STAR-FORMATION HISTORY; DOUBLE BLACK-HOLE; GRAVITATIONAL-RADIATION; GLOBULAR-CLUSTER; IC-10 X-1; MASS; ACCRETION; EVOLUTION; GALAXIES; VARIABILITY AB We have discovered a persistent, but highly variable X-ray source in the nearby starburst galaxy NGC 253. The source varies at the level of a factor of about 5 in count rate on time-scales of a few hours. Two long observations of the source with Chandra and XMM-Newton show suggestive evidence for the source having a period of about 14-15 hours, but the time sampling in existing data is insufficient to allow a firm determination that the source is periodic. Given the amplitude of variation and the location in a nuclear starburst, the source is likely to be a Wolf-Rayet X-ray binary, with the tentative period being the orbital period of the system. In light of the fact that we have demonstrated that careful examination of the variability of moderately bright X-ray sources in nearby galaxies can turn up candidate Wolf-Rayet X-ray binaries, we discuss the implications of Wolf-Rayet X-ray binaries for predictions of the gravitational wave source event rate, and, potentially, interpretations of the events. C1 [Maccarone, Thomas J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Lehmer, Bret D.; Ptak, Andrew] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Lehmer, Bret D.; Leyder, J. C.; Hornschemeier, Ann; Ptak, Andrew; Wik, Daniel] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Leyder, J. C.] European Space Agcy, European Space Astron Ctr, E-28691 Madrid, Spain. [Antoniou, Vallia] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Antoniou, Vallia] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zezas, Andreas] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. RP Maccarone, TJ (reprint author), Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. EM thomas.maccarone@ttu.edu RI Zezas, Andreas/C-7543-2011; Antoniou, Vallia/E-3837-2013 OI Zezas, Andreas/0000-0001-8952-676X; Antoniou, Vallia/0000-0001-7539-1593 NR 60 TC 6 Z9 6 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2014 VL 439 IS 3 BP 3064 EP 3072 DI 10.1093/mnras/stu167 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PB UT WOS:000334114900068 ER PT J AU Foster, G Hickish, J Magro, A Price, D Adami, KZ AF Foster, G. Hickish, J. Magro, A. Price, D. Adami, K. Zarb TI Implementation of a direct-imaging and FX correlator for the BEST-2 array SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: interferometers; instrumentation: miscellaneous; techniques: interferometric; radio continuum: general ID RADIO; REIONIZATION; SPECTRUM AB A new digital backend has been developed for the Basic Element for SKA Training II (BEST-2) array at Radiotelescopi di Medicina, INAF-IRA, Italy, which allows concurrent operation of an FX correlator, and a direct-imaging correlator and beamformer. This backend serves as a platform for testing some of the spatial Fourier transform concepts which have been proposed for use in computing correlations on regularly gridded arrays. While spatial Fourier transform-based beamformers have been implemented previously, this is, to our knowledge, the first time a direct-imaging correlator has been deployed on a radio astronomy array. Concurrent observations with the FX and direct-imaging correlator allow for direct comparison between the two architectures. Additionally, we show the potential of the direct-imaging correlator for time-domain astronomy, by passing a subset of beams though a pulsar and transient detection pipeline. These results provide a timely verification for spatial Fourier transform-based instruments that are currently in commissioning. These instruments aim to detect highly redshifted hydrogen from the epoch of reionization and/or to perform wide-field surveys for time-domain studies of the radio sky. We experimentally show the direct-imaging correlator architecture to be a viable solution for correlation and beamforming. C1 [Foster, G.; Hickish, J.; Price, D.; Adami, K. Zarb] Univ Oxford, Dept Phys, Subdept Astrophys, Oxford OX1 3RH, England. [Foster, G.; Adami, K. Zarb] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Magro, A.] Univ Malta, Dept Phys, MSD-2080 Msida, Malta. [Price, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Foster, G (reprint author), Univ Oxford, Dept Phys, Subdept Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. EM griffin.foster@gmail.com FU South African Research Chairs Initiative of the Department of Science and Technology; National Research Foundation FX This work is based upon research supported by the South African Research Chairs Initiative of the Department of Science and Technology and National Research Foundation. NR 22 TC 1 Z9 1 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 APR PY 2014 VL 439 IS 3 BP 3180 EP 3188 DI 10.1093/mnras/stu188 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PB UT WOS:000334114900078 ER PT J AU Wang, K Zhang, QZ Testi, L van der Tak, F Wu, YF Zhang, HW Pillai, T Wyrowski, F Carey, S Ragan, SE Henning, T AF Wang, Ke Zhang, Qizhou Testi, Leonardo van der Tak, Floris Wu, Yuefang Zhang, Huawei Pillai, Thushara Wyrowski, Friedrich Carey, Sean Ragan, Sarah E. Henning, Thomas TI Hierarchical fragmentation and differential star formation in the Galactic 'Snake': infrared dark cloud G11.11-0.12 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; masers; stars: early-type; stars: formation; ISM: individual objects: G11.11-012; ISM: jets and outflows ID YOUNG STELLAR OBJECTS; MOLECULAR LINE SURVEY; MASS PROTOSTELLAR CANDIDATES; LARGE ARRAY OBSERVATIONS; EXTENDED GREEN OBJECTS; INTERSTELLAR AMMONIA; SUBMILLIMETER ARRAY; FORMING REGION; TEMPERATURE STRUCTURE; PHYSICAL-PROPERTIES AB We present Submillimeter Array (SMA) lambda = 0.88 and 1.3 mm broad-band observations, and Very Large Array (VLA) observations in NH3 (J, K) = (1,1) up to (5,5), H2O and CH3OH maser lines towards the two most massive molecular clumps in infrared dark cloud (IRDC) G11.11-0.12. Sensitive high-resolution images reveal hierarchical fragmentation in dense molecular gas from the similar to 1 pc clump scale down to similar to 0.01 pc condensation scale. At each scale, the mass of the fragments is orders of magnitude larger than the Jeans mass. This is common to all four IRDC clumps we studied, suggesting that turbulence plays an important role in the early stages of clustered star formation. Masers, shock heated NH3 gas, and outflows indicate intense ongoing star formation in some cores while no such signatures are found in others. Furthermore, chemical differentiation may reflect the difference in evolutionary stages among these star formation seeds. We find NH3 ortho/para ratios of 1.1 +/- 0.4, 2.0 +/- 0.4, and 3.0 +/- 0.7 associated with three outflows, and the ratio tends to increase along the outflows downstream. Our combined SMA and VLA observations of several IRDC clumps present the most in-depth view so far of the early stages prior to the hot core phase, revealing snapshots of physical and chemical properties at various stages along an apparent evolutionary sequence. C1 [Wang, Ke; Testi, Leonardo] European So Observ, D-85748 Garching, Germany. [Wang, Ke; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wang, Ke; van der Tak, Floris] Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands. [Wang, Ke; Wu, Yuefang; Zhang, Huawei] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China. [Testi, Leonardo] Excellence Cluster Universe, D-85748 Garching, Germany. [Testi, Leonardo] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [van der Tak, Floris] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Pillai, Thushara] CALTECH, Pasadena, CA 91125 USA. [Wyrowski, Friedrich] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Carey, Sean] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Ragan, Sarah E.; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Wang, K (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM kwang@eso.org OI Ragan, Sarah/0000-0003-4164-5588; Wang, Ke/0000-0002-7237-3856; Zhang, Qizhou/0000-0003-2384-6589 FU ESO fellowship; European Union Lotus post-doctoral fellowship under the frame of Erasmus Mundus Action; SMA pre-doctoral fellowship; China Scholarship Council; China Ministry of Science and Technology under State Key Development Program for Basic Research [2012CB821800]; NSFC [11328301]; Deutsche Forschungsgemeinschaft priority program 1573 ('Physics of the Interstellar Medium') [RA 2158/1-1] FX We thank the referee Michael Burton for valuable comments that helped clarify the manuscript. KW acknowledges support from the ESO fellowship, the European Union Lotus post-doctoral fellowship under the frame of Erasmus Mundus Action during his stay at Kapteyn, and the SMA pre-doctoral fellowship and China Scholarship Council during his stay at Harvard CfA. YW and KW thank the support by China Ministry of Science and Technology under State Key Development Program for Basic Research (2012CB821800). QZ acknowledge the partially support by the NSFC grant 11328301. SER is supported by grant RA 2158/1-1, which is part of the Deutsche Forschungsgemeinschaft priority program 1573 ('Physics of the Interstellar Medium'). This research made use of open-source PYTHON packages APLPY and PYSPECKIT (Ginsburg & Mirocha 2011; Robitaille & Bressert 2012). NR 101 TC 36 Z9 36 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 APR PY 2014 VL 439 IS 4 BP 3275 EP 3293 DI 10.1093/mnras/stu127 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PG UT WOS:000334115400007 ER PT J AU Samushia, L Reid, BA White, M Percival, WJ Cuesta, AJ Zhao, GB Ross, AJ Manera, M Aubourg, E Beutler, F Brinkmann, J Brownstein, JR Dawson, KS Eisenstein, DJ Ho, S Honscheid, K Maraston, C Montesano, F Nichol, RC Roe, NA Ross, NP Sanchez, AG Schlegel, DJ Schneider, DP Streblyanska, A Thomas, D Tinker, JL Wake, DA Weaver, BA Zehavi, I AF Samushia, Lado Reid, Beth A. White, Martin Percival, Will J. Cuesta, Antonio J. Zhao, Gong-Bo Ross, Ashley J. Manera, Marc Aubourg, Eric Beutler, Florian Brinkmann, Jon Brownstein, Joel R. Dawson, Kyle S. Eisenstein, Daniel J. Ho, Shirley Honscheid, Klaus Maraston, Claudia Montesano, Francesco Nichol, Robert C. Roe, Natalie A. Ross, Nicholas P. Sanchez, Ariel G. Schlegel, David J. Schneider, Donald P. Streblyanska, Alina Thomas, Daniel Tinker, Jeremy L. Wake, David A. Weaver, Benjamin A. Zehavi, Idit TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measuring growth rate and geometry with anisotropic clustering SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitation; cosmological parameters; dark energy; dark matter; distance scale; large-scale structure of Universe ID DIGITAL SKY SURVEY; DARK ENERGY SURVEY; SPACE DISTORTION MEASUREMENTS; REDSHIFT-SPACE; ACOUSTIC-OSCILLATIONS; COSMOLOGICAL CONSTANT; COSMIC ACCELERATION; SYSTEMATIC-ERRORS; CENT DISTANCE; SCALE AB We use the observed anisotropic clustering of galaxies in the Baryon Oscillation Spectroscopic Survey Data Release 11 CMASS sample to measure the linear growth rate of structure, the Hubble expansion rate and the comoving distance scale. Our sample covers 8498 deg(2) and encloses an effective volume of 6 Gpc(3) at an effective redshift of (z) over bar = 0.57. We find f Sigma(8) = 0.441 +/- 0.044, H = 93.1 +/- 3.0 km s(-1) Mpc(-1) and D-A = 1380 +/- 23 Mpc when fitting the growth and expansion rate simultaneously. When we fix the background expansion to the one predicted by spatially flat Lambda cold dark matter (Lambda CDM) model in agreement with recent Planck results, we find f Sigma(8) = 0.447 +/- 0.028 (6 per cent accuracy). While our measurements are generally consistent with the predictions of Lambda CDM and general relativity, they mildly favour models in which the strength of gravitational interactions is weaker than what is predicted by general relativity. Combining our measurements with recent cosmic microwave background data results in tight constraints on basic cosmological parameters and deviations from the standard cosmological model. Separately varying these parameters, we find w = -0.983 +/- 0.075 (8 per cent accuracy) and gamma = 0.69 +/- 0.11 (16 per cent accuracy) for the effective equation of state of dark energy and the growth rate index, respectively. Both constraints are in good agreement with the standard model values of w = -1 and gamma = 0.554. C1 [Samushia, Lado; Percival, Will J.; Zhao, Gong-Bo; Ross, Ashley J.; Manera, Marc; Maraston, Claudia; Nichol, Robert C.; Thomas, Daniel] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth P01 3FX, Hants, England. [Samushia, Lado] Ilia State Univ, Natl Abastumani Astrophys Observ, GE-1060 Tbilisi, Rep of Georgia. [Reid, Beth A.; White, Martin; Beutler, Florian; Roe, Natalie A.; Ross, Nicholas P.; Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Reid, Beth A.; White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Reid, Beth A.; White, Martin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cuesta, Antonio J.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Cuesta, Antonio J.] CSIC, IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain. [Zhao, Gong-Bo] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Manera, Marc] UCL, London WC1E 6BT, England. [Aubourg, Eric] Univ Paris Diderot, CNRS, IN2P3, APC,CEA Irfu,Obs Paris,Sorbonne Paris Cit, F-75205 Paris, France. [Brinkmann, Jon] Apache Point Observ, Sunspot, NM 88349 USA. [Brownstein, Joel R.; Dawson, Kyle S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Shirley] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Honscheid, Klaus] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Honscheid, Klaus] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Montesano, Francesco; Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ross, Nicholas P.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 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. [Streblyanska, Alina] IAC, E-38200 Tenerife, Spain. [Streblyanska, Alina] ULL, Dept Astrofis, E-38206 Tenerife, Spain. [Tinker, Jeremy L.; Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Wake, David A.] Univ Wisconsin Madison, Dept Astron, Madison, WI 53706 USA. [Wake, David A.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. RP Samushia, L (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth P01 3FX, Hants, England. EM lado.samushia@port.ac.uk RI Ho, Shirley/P-3682-2014; White, Martin/I-3880-2015; OI Ho, Shirley/0000-0002-1068-160X; White, Martin/0000-0001-9912-5070; Beutler, Florian/0000-0003-0467-5438; Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470 FU European Research Council; NASA through Hubble Fellowship [51280]; Space Telescope Science Institute; NASA [NAS 5-26555]; Alfred P. Sloan Foundation; National Science Foundation; US 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 LS gratefully acknowledges support by the European Research Council. BAR gratefully acknowledges support provided by NASA through Hubble Fellowship grant 51280 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. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University. NR 81 TC 116 Z9 116 U1 2 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 APR PY 2014 VL 439 IS 4 BP 3504 EP 3519 DI 10.1093/mnras/stu197 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PG UT WOS:000334115400024 ER PT J AU Cybulski, R Yun, MS Fazio, GG Gutermuth, RA AF Cybulski, Ryan Yun, Min S. Fazio, Giovanni G. Gutermuth, Robert A. TI From voids to Coma: the prevalence of pre-processing in the local Universe SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; galaxies: evolution; infrared: galaxies; ultraviolet: galaxies ID STAR-FORMATION RATES; DIGITAL SKY SURVEY; MORPHOLOGY-DENSITY RELATION; RICH GALAXY CLUSTERS; MASS ASSEMBLY GAMA; SIMILAR-TO 1; STELLAR MASS; FORMATION HISTORIES; FORMING GALAXIES; DISTANT CLUSTERS AB We examine the effects of pre-processing across the Coma Supercluster, including 3505 galaxies over similar to 500 deg(2), by quantifying the degree to which star-forming (SF) activity is quenched as a function of environment. We characterize environment using the complementary techniques of Voronoi Tessellation, to measure the density field, and the Minimal Spanning Tree, to define continuous structures, and so we measure SF activity as a function of local density and the type of environment (cluster, group, filament, and void), and quantify the degree to which environment contributes to quenching of SF activity. Our sample covers over two orders of magnitude in stellar mass (10(8.5)-10(11) M-circle dot), and consequently, we trace the effects of environment on SF activity for dwarf and massive galaxies, distinguishing so-called mass quenching from environment quenching. Environmentally driven quenching of SF activity, measured relative to the void galaxies, occurs to progressively greater degrees in filaments, groups, and clusters, and this trend holds for dwarf and massive galaxies alike. A similar trend is found using g - r colours, but with a more significant disparity between galaxy mass bins driven by increased internal dust extinction in massive galaxies. The SFR distributions of massive SF galaxies have no significant environmental dependence, but the distributions for dwarf SF galaxies are found to be statistically distinct in most environments. Pre-processing plays a significant role at low redshift, as environmentally driven galaxy evolution affects nearly half of the galaxies in the group environment, and a significant fraction of the galaxies in the more diffuse filaments. Our study underscores the need for sensitivity to dwarf galaxies to separate mass-driven from environmentally driven effects, and the use of unbiased tracers of SF activity. C1 [Cybulski, Ryan; Yun, Min S.; Gutermuth, Robert A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Cybulski, Ryan; Fazio, Giovanni G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cybulski, R (reprint author), Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. EM jcybulsk@astro.umass.edu OI Cybulski, Ryan/0000-0002-4997-2308 FU National Aeronautics and Space Administration; NASA [NAS5-26555, 1391817]; NASA Office of Space Science [NNX09AF08G]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; National Aeronautics and Space Administration's Earth Science Technology Office, Computational Technologies Project [NCC5-626]; California Institute of Technology [NCC5-626]; Smithsonian Astrophysical Observatory (SAO) Predoctoral Fellowship; NASA ADAP grant [13-ADAP13-0155, NNX10AD64G, NNX11AD14G, NNX13AF08G]; Caltech/JPL awards [1373081, 1424329, 1440160] FX This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has also made use of NASA's Astrophysics Data System (ADS), 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. This publication makes use of data products from the WISE, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/. This research made use of Montage, funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computational Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology. The code is maintained by the NASA/IPAC Infrared Science Archive.; RC was supported by the Smithsonian Astrophysical Observatory (SAO) Predoctoral Fellowship, and funded under NASA Contract 1391817 and NASA ADAP grant 13-ADAP13-0155. MS Yun acknowledges support from the NASA ADAP grant NNX10AD64G. RA Gutermuth gratefully acknowledges funding support from NASA ADAP grants NNX11AD14G and NNX13AF08G and Caltech/JPL awards 1373081, 1424329, and 1440160 in support of Spitzer Space Telescope observing programmes. NR 121 TC 14 Z9 14 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 APR PY 2014 VL 439 IS 4 BP 3564 EP 3586 DI 10.1093/mnras/stu200 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PG UT WOS:000334115400028 ER PT J AU Chavarria, L Allen, L Brunt, C Hora, JL Muench, A Fazio, G AF Chavarria, L. Allen, L. Brunt, C. Hora, J. L. Muench, A. Fazio, G. TI A multiwavelength study of embedded clusters in W5-east, NGC 7538, S235, S252 and S254-S258 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: early-type; stars: formation; stars: pre-main sequence; H ii regions; infrared: stars ID INFRARED ARRAY CAMERA; H-II REGIONS; MASSIVE-STAR-FORMATION; APERTURE SYNTHESIS OBSERVATIONS; YOUNG STELLAR OBJECTS; MOLECULAR CLOUD COMPLEX; SPITZER-SPACE-TELESCOPE; GALACTIC HII-REGIONS; BRIGHT-RIMMED CLOUDS; FORMING REGIONS AB We present Spitzer, near-IR (NIR) and millimetre observations of the massive star-forming regions W5-east, S235, S252, S254-S258 and NGC 7538. Spitzer data is combined with NIR observations to identify and classify the young population while (CO)-C-12 and (CO)-C-13 observations are used to examine the parental molecular cloud. We detect in total 3021 young stellar objects (YSOs). Of those, 539 are classified as Class I, and 1186 as Class II sources. YSOs are distributed in groups surrounded by a more scattered population. Class I sources are more hierarchically organized than Class II and associated with the most dense molecular material. We identify in total 41 embedded clusters containing between 52 and 73 per cent of the YSOs. Clusters are in general non-virialized, turbulent and have star formation efficiencies between 5 and 50 per cent. We compare the physical properties of embedded clusters harbouring massive stars (MEC) and low-mass embedded clusters (LEC) and find that both groups follow similar correlations where the MEC are an extrapolation of the LEC. The mean separation between MEC members is smaller compared to the cluster Jeans length than for LEC members. These results are in agreement with a scenario where stars are formed in hierarchically distributed dusty filaments where fragmentation is mainly driven by turbulence for the more massive clusters. We find several young OB-type stars having IR-excess emission which may be due to the presence of an accretion disc. C1 [Chavarria, L.] Univ Chile, Santiago, Chile. [Chavarria, L.; Hora, J. L.; Muench, A.; Fazio, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chavarria, L.] Lab Astrophys Bordeaux, F-33271 Floirac, France. [Chavarria, L.] Ctr Astrobiol CSIC INTA, E-28850 Madrid, Spain. [Allen, L.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Brunt, C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. RP Chavarria, L (reprint author), Univ Chile, Camino Observ 1515, Santiago, Chile. EM luisagustinchavarria@gmail.com OI Hora, Joseph/0000-0002-5599-4650; Muench, August/0000-0003-0666-6367 FU NASA; NSF [AST 0540852]; RCUK Fellowship at the University of Exeter, UK; Canadian Space Agency; National Aeronautics and Space Administration; Spanish MINECO [CSD2009-00038, AYA2009-07304, AYA2012-32032] FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, Caltech, under a contract with NASA. Support for this work was provided by NASA through a contract issued by JPL/Caltech. We also thank NOAO for their student thesis support. The Five College Radio Astronomy Observatory was supported by NSF grant AST 0540852. CB is supported by an RCUK Fellowship at the University of Exeter, UK. This work is based in part on the IRAC post-BCD processing software 'IRACPROC' developed by Mike Schuster, Massimo Marengo and Brian Patten at the Smithsonian Astrophysical Observatory. 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. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We thank the Spanish MINECO for funding support from grants CSD2009-00038, AYA2009-07304 and AYA2012-32032. NR 127 TC 10 Z9 11 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 APR PY 2014 VL 439 IS 4 BP 3719 EP 3754 DI 10.1093/mnras/stu224 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE6PG UT WOS:000334115400041 ER PT J AU Tapia, M Rodriguez, LF Tovmassian, G Rodriguez-Gomez, V Gonzalez-Buitrago, D Zharikov, S Ortiz-Leon, GN AF Tapia, Mauricio Rodriguez, Luis F. Tovmassian, Gagik Rodriguez-Gomez, Vicente Gonzalez-Buitrago, Diego Zharikov, Sergei Ortiz-Leon, Gisela N. TI PERIODIC RADIO CONTINUUM EMISSION ASSOCIATED WITH THE beta CEPHEI STAR V2187 CYG SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA LA English DT Article DE radio continuum; stars-stars; individual (V1287 Cyg, beta Cephei) ID OB STARS; NONTHERMAL EMISSION; SPACED DATA; PARAMETERS; PHOTOMETRY; CLUSTERS; SYSTEM; REGION AB We present new optical time-resolved photometry and medium-resolution spectroscopy of V2187 Cyg. We confirm its classification as a beta Cephei star based on sinusoidal light variations with a period of 0.2539 days and mean amplitudes of 0.037 and 0.042 magnitudes in i and V, respectively. We classified the spectrum of this star as B2-3 V with no evidence of variations in the profiles of its absorption lines in timescales of hours or days. The stellar spectrum is totally absent of emission lines. We detected unexpected faint radio continuum emission (between 0.4 and 0.8 mJy at 6-cm) showing a sinusoidal variation with a period of 12.8 days. The radio spectrum is thermal. We searched in the Very Large Array archive for radio continuum emission toward 15 beta other Cephei stars. None of these additional stars, some of them, much closer to the Sun than V2187 Cyg, was detected, indicating that radio emission from beta Cephei stars is extremely uncommon. C1 [Tapia, Mauricio; Tovmassian, Gagik; Gonzalez-Buitrago, Diego; Zharikov, Sergei] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22830, Baja California, Mexico. [Rodriguez, Luis F.; Ortiz-Leon, Gisela N.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Rodriguez-Gomez, Vicente] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rodriguez, Luis F.] King Abdulaziz Univ, Fac Sci, Dept Astron, Jeddah 21589, Saudi Arabia. RP Tapia, M (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 877, Ensenada 22830, Baja California, Mexico. EM mt@astrosen.unam.mx; l.rodriguez@crya.unam.mx; gag@astrosen.unam.mx; zhar@astrosen.unam.mx; g.ortiz@crya.unam.mx RI Faculty of, Sciences, KAU/E-7305-2017 NR 33 TC 0 Z9 0 U1 0 U2 1 PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA PI MEXICO CITY PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 0185-1101 J9 REV MEX ASTRON ASTR JI Rev. Mex. Astron. Astrofis. PD APR PY 2014 VL 50 IS 1 BP 127 EP 136 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG4XV UT WOS:000335424600015 ER PT J AU Schuettpelz, E Davila, A Prado, J Hirai, RY Yatskievych, G AF Schuettpelz, Eric Davila, Alex Prado, Jefferson Hirai, Regina Y. Yatskievych, George TI Molecular phylogenetic and morphological affinities of Adiantum senae (Pteridaceae) SO TAXON LA English DT Article DE Adiantopsis; atpA; cheilanthoid ferns; rbcL; molecular systematics ID CHEILANTHOID FERNS; RBCL SEQUENCES; INFERENCE; REVISION; MRBAYES; GENERA; BRAZIL AB Adiantum senae, a diminutive fern nearly restricted to southern Brazil, was described by Baker in 1885. In subsequent Floras, it was either completely overlooked or simply retained in the maidenhair genus Adiantum. However, a molecular phylogenetic analysis and a thorough morphological evaluation clearly demonstrate that this species does not belong in this genus. We find strong molecular support for the inclusion of A. senae within the cheilanthoid genus Adiantopsis, as a rather isolated lineage resolved as sister to the large, generally echinate-spored Glade. The position of sporangia in A. senae-along the vein tips of the main laminar tissue rather than on the abaxial tissue of the pseudoindusia-confirms the separation of this species from Adiantum, and the presence of arachnoid-echinulate spores reinforces its resolved position within Adiantopsis. Based on the sum of this evidence, we here provide a new combination, Adiantopsis senae (Baker) Schuettp. & A.Davila. Additionally, we designate a lectotype for A. senae, as well as for a later synonym. C1 [Schuettpelz, Eric] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Schuettpelz, Eric; Davila, Alex] Univ N Carolina, Dept Biol & Marine Biol, Wilmington, NC 28403 USA. [Prado, Jefferson; Hirai, Regina Y.] Inst Bot, BR-04045972 Sao Paulo, Brazil. [Yatskievych, George] Missouri Bot Garden, St Louis, MO 63166 USA. RP Schuettpelz, E (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM schuettpelze@si.edu RI Hirai, Regina/K-3913-2013; Prado, Jefferson/C-4766-2012; OI Prado, Jefferson/0000-0003-4783-3125; Schuettpelz, Eric/0000-0003-3891-9904 FU National Science Foundation [DEB-0717398, DEB-0717430, DEB-1145614, DEB-1145925]; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico [301157/2010-3]; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo [2011/07164-3] FX This research was funded in part by the National Science Foundation (awards DEB-0717398, DEB-0717430, DEB-1145614, and DEB-1145925), as well as by Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (301157/2010-3) and Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (2011/07164-3). The illustration of Adiantopsis senae was drawn by Klei Sousa. Robbin Moran and Judith Garrison Hanks kindly imaged the spores of A. senae. Two anonymous reviewers provided helpful comments on the manuscript. NR 31 TC 3 Z9 4 U1 1 U2 6 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 APR PY 2014 VL 63 IS 2 BP 258 EP 264 PG 7 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA AG0SO UT WOS:000335126100003 ER PT J AU Peterson, PM Romaschenko, K Arrieta, YH AF Peterson, Paul M. Romaschenko, Konstantin Herrera Arrieta, Yolanda TI A molecular phylogeny and classification of the Cteniinae, Farragininae, Gouiniinae, Gymnopogoninae, Perotidinae, and Trichoneurinae (Poaceae: Chloridoideae: Cynodonteae) SO TAXON LA English DT Article DE classification; ITS; phylogeny; plastid DNA sequences; Tridentopsis ID SEQUENCES; TREES; GENUS; CHLORIDEAE; INFERENCE; GRASSES; MRBAYES AB The classification of twenty Cynodonteae genera (Bewsia, Craspedorhachis, Ctenium, Dignathia, Farrago, Goiania, Gymnopogon, Latipes, Leptocarydion, Leptothrium, Lophacme, Lopholepis, Mosdenia, Perotis, Schenckochloa, Toliara, Trichoneura, Trigonochloa, Triplasis, Vaseyochloa) has been poorly understood. The goals of this study were to reconstruct the evolutionary history of the tribe Cynodonteae, emphasizing these twenty genera using molecular data with increased species sampling. A phylogenetic analysis was conducted on 159 samples, of which 94 species (140 individuals) were in the Cynodonteae, using four plastid (rpl32-trnL spacer, ndhA intron, rps16-trnK spacer, rps16 intron) and nuclear ITS 1&2 (ribosomal internal transcribed spacer regions) sequences to infer evolutionary relationships and revise the classification. Strong support was found for six lineages. Craspedorhachis, Ctenium, Dignathia, Gymnopogon, Trichoneura, and Triplasis appear monophyletic; Leptothrium is paraphyletic with Latipes inermis embedded within; Perotis is paraphyletic with Lopholepis and Toliara embedded within; and Goiania is monophyletic with the resurrection of Schenckochloa. The molecular results support the recognition of six subtribes; five (Cteniinae, Farragininae, Gymnopogoninae, Perotidinae, Trichoneurinae) are newly described. A new genus, Tridentopsis, is described; five new combinations, Leptothrium inerme, Perotis arenacea, Perotis ornithocephala, Tridentopsis eragrostoides, and Tridentopsis mutica are made; and Holboellia ornithocephala is lectotypified. C1 [Peterson, Paul M.; Romaschenko, Konstantin] Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Romaschenko, Konstantin] Natl Acad Sci, MG Kholodny Inst Bot, UA-01601 Kiev, Ukraine. [Herrera Arrieta, Yolanda] Inst Politecn Nacl, CHDIR Unidad Durango COFAA, Durango, Mexico. RP Peterson, PM (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. EM peterson@si.edu RI Romaschenko, Konstantin/K-3096-2014 OI Romaschenko, Konstantin/0000-0002-7248-4193 FU National Geographic Society Committee for Research and Exploration [8848-10, 8087-06]; Smithsonian Institution; Scholarly Studies Program; Research Opportunities; Atherton Seidell Foundation; Biodiversity Surveys; Inventories Program; Small Grants Program; Laboratory of Analytical Biology FX We thank the National Geographic Society Committee for Research and Exploration (Grant No. 8848-10, 8087-06) for field and laboratory support, the Smithsonian Institution's Restricted Endowments Fund, the Scholarly Studies Program, Research Opportunities, Atherton Seidell Foundation, Biodiversity Surveys and Inventories Program, Small Grants Program, and the Laboratory of Analytical Biology, all for financial support. We would also like to acknowledge Lee Weigt, Jeffery Hunt, Gabriel Johnson, and David Erickson for help in the laboratory; Robert J. Soreng and Jeffery M. Saarela for accompanying the first author on numerous field expeditions; Riccardo Baldini for sending us digital photos of the type of Latipes inermis; Robert J. Soreng for many extended discussions pertinent to the manuscript; and two anonymous reviewers for providing helpful comments on the manuscript. NR 43 TC 11 Z9 13 U1 3 U2 9 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 APR PY 2014 VL 63 IS 2 BP 275 EP 286 PG 12 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA AG0SO UT WOS:000335126100005 ER PT J AU Agra-Amboage, V Cabrit, S Dougados, C Kristensen, LE Ibgui, L Reunanen, J AF Agra-Amboage, V. Cabrit, S. Dougados, C. Kristensen, L. E. Ibgui, L. Reunanen, J. TI Origin of the wide-angle hot H-2 in DG Tauri New insight from SINFONI spectro-imaging SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; stars: winds, outflows; stars: variables: T Tauri, Herbig Ae/Be; techniques: imaging spectroscopy; molecular data; infrared: stars ID HUBBLE-SPACE-TELESCOPE; MOLECULAR-HYDROGEN EMISSION; PLUME SIGNATURE CALCULATIONS; YOUNG STELLAR OBJECTS; WIND-DRIVEN ACCRETION; BY-LINE CODE; PHOTODISSOCIATION REGIONS; SUB-ARCSECOND; CIRCUMSTELLAR ENVIRONMENTS; PROTOPLANETARY DISKS AB Context. The origin of protostellar jets remains a major open question in star formation. Magnetohydrodynamical (MHD) disc winds are an important mechanism to consider, because they would have a significant impact on planet formation and migration. Aims. We wish to test the origins proposed for the extended hot H-2 at 2000 K around the atomic jet from the T Tauri star DG Tau, in order to constrain the wide-angle wind structure and the possible presence of an MHD disc wind in this prototypical source. Methods. We present spectro-imaging observations of the DG Tau jet in H-2 1-0 S(1) with 0.'' 12 angular resolution, obtained with SINFONI/VLT. Thanks to spatial deconvolution by the point spread function and to careful correction for wavelength calibration and for uneven slit illumination (to within a few km s(-1)), we performed a thorough analysis and modeled the morphology and kinematics. We also compared our results with studies in [Fe II], [O I], and FUV-pumped H-2, Absolute flux calibration yields the H2 column/volume density and emission surface, and narrows down possible shock conditions. Results. The limb-brightened H-2 1-0 S(1) emission in the blue lobe is strikingly similar to FUV-pumped H-2 imaged 6 yr later, confirming that they trace the same hot gas and setting an upper limit <12 km s(-1) on any expansion proper motion. The wide-angle rims are at lower blueshifts (between -5 and 0 km s(-1)) than probed by narrow long-slit spectra. We confirm that they extend to larger angle and to lower speed the onion-like velocity structure observed in optical atomic lines. The latter is shown to be steady over >= 4 yr but undetected in [Fe II] by SINFONI, probably due to strong iron depletion. The rim thickness <= 14 AU rules out excitation by C-type shocks, and J-type shock speeds are constrained to similar or equal to 10 km s(-1). Conclusions. We find that explaining the H-2 1-0 S(1) wide-angle emission with a shocked layer requires either a recent outburst (15 yr) into a pre-existing ambient outflow or an excessive wind mass flux. A slow photoevaporative wind from the dense irradiated disc surface and an MHD disc wind heated by ambipolar diffusion seem to be more promising and need to be modeled in more detail. Better observational constraints on proper motion and rim thickness would also be crucial for clarifying the origin of this structure. C1 [Agra-Amboage, V.] Univ Porto, Fac Engn, Dept Engn Fis, SIM Unidade FCT 4006, P-4200465 Oporto, Portugal. [Cabrit, S.; Ibgui, L.] CNRS, UMR 8112, LERMA, F-75014 Paris, France. [Cabrit, S.; Ibgui, L.] UPMC, UCP, ENS, Observ Paris, F-75014 Paris, France. [Dougados, C.] CNRS, Lab Franco Chilien Astron, UMI 3386, Santiago, Chile. [Cabrit, S.; Dougados, C.] CNRS, UMR 5274, IPAG, F-38041 Grenoble, France. [Cabrit, S.; Dougados, C.] Univ Grenoble 1, F-38041 Grenoble, France. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reunanen, J.] Univ Turku, Dept Phys & Astron, Tuorla Observ, Piikkio 21500, Finland. RP Agra-Amboage, V (reprint author), Univ Porto, Fac Engn, Dept Engn Fis, SIM Unidade FCT 4006, Rua Dr Roberto Frias S-N, P-4200465 Oporto, Portugal. EM vaa@fe.up.pt RI Kristensen, Lars/F-4774-2011 OI Kristensen, Lars/0000-0003-1159-3721 FU Fundacao para a Ciencia e Tecnologia (FCT) [SERH/BPD/69670/2010]; FCT-Portugal [PTDC/CTE-AST/116561/2010]; Marie Curie Research Training Network JETSET (Jet simulations, Experiments and Theory) [MRTN-CT-2004-005592]; french Programme National de Physique Stellaire (PNPS) FX The authors are grateful to D. Coffey for kindly providing the [O I] transverse slit data shown in Fig. 5, to G. Herczeg for precious advice on velocity calibration, and to the referee, M. Takami, for insightful comments that led to significant improvement of the paper. V. Agra-Amboage acknowledges financial support through the Fundacao para a Ciencia e Tecnologia (FCT) under contract SERH/BPD/69670/2010. This research was partially supported by FCT-Portugal through Project PTDC/CTE-AST/116561/2010. The authors also acknowledge financial and travel support through the Marie Curie Research Training Network JETSET (Jet simulations, Experiments and Theory) under contract MRTN-CT-2004-005592, and through the french Programme National de Physique Stellaire (PNPS). NR 72 TC 8 Z9 8 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 APR PY 2014 VL 564 AR A11 DI 10.1051/0004-6361/201220488 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000011 ER PT J AU Arnold, L Ehrenreich, D Vidal-Madjar, A Dumusque, X Nitschelm, C Querel, RR Hedelt, P Berthier, J Lovis, C Moutou, C Ferlet, R Crooker, D AF Arnold, L. Ehrenreich, D. Vidal-Madjar, A. Dumusque, X. Nitschelm, C. Querel, R. R. Hedelt, P. Berthier, J. Lovis, C. Moutou, C. Ferlet, R. Crooker, D. TI The Earth as an extrasolar transiting planet II. HARPS and UVES detection of water vapour, biogenic O-2, and O-3 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Earth; Moon; atmospheric effects; planets and satellites: atmospheres; planets and satellites: terrestrial planets; astrobiology ID ROTATIONAL RAMAN-SCATTERING; LUNAR ECLIPSE OBSERVATIONS; TRANSMISSION SPECTRUM; ATMOSPHERE; EXOPLANET; SEARCH; PARAMETERS; LATITUDE; IMPACT; GASES AB Context. The atmospheric composition of transiting exoplanets can be characterized during transit by spectroscopy. Detections of several chemical species have previously been reported in the atmosphere of gaseous giant exoplanets. For the transit of an Earth twin, models predict that biogenic oxygen (O-2) and ozone (O-3) atmospheric gases should be detectable, as well as water vapour (H2O), a molecule linked to habitability as we know it on Earth. Aims. The aim is to measure the Earth radius versus wavelength lambda - or the atmosphere thickness h(lambda) - at the highest spectral resolution available to fully characterize the signature of Earth seen as a transiting exoplanet. Methods. We present observations of the Moon eclipse of December 21, 2010. Seen from the Moon, the Earth eclipses the Sun and opens access to the Earth atmosphere transmission spectrum. We used two different ESO spectrographs (HARPS and UVES) to take penumbra and umbra high-resolution spectra from approximate to 3100 to 10 400 angstrom. A change of the quantity of water vapour above the telescope compromised the quality of the UVES data. We corrected for this effect in the data processing. We analyzed the data by three different methods. The first method is based on the analysis of pairs of penumbra spectra. The second makes use of a single penumbra spectrum, and the third of all penumbra and umbra spectra. Results. Profiles h(lambda) are obtained with the three methods for both instruments. The first method gives the best result, in agreement with a model. The second method seems to be more sensitive to the Doppler shift of solar spectral lines with respect to the telluric lines. The third method makes use of umbra spectra, which bias the result by increasing the overall negative slope of h(lambda). It can be corrected for this a posteriori from results with the first method. The three methods clearly show the spectral signature of the Rayleigh scattering in the Earth atmosphere and the bands of H2O, O-2, and O-3. Sodium is detected. Assuming no atmospheric perturbations, we show that the E-ELT is theoretically able to detect the O-2 A-band in 8 h of integration for an Earth twin at 10 pc. Conclusions. Biogenic O-2, O-3, and water vapour are detected in Earth observed as a transiting planet, and, in principle, would be within reach of the E-ELT for an Earth twin at 10 pc. C1 [Arnold, L.] Aix Marseille Univ, CNRS, Observ Haute Provence, Inst Pytheas UMS 3470, F-04870 St Michel Lobservatoire, France. [Ehrenreich, D.; Lovis, C.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [Vidal-Madjar, A.; Ferlet, R.] Univ Paris 06, CNRS UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Dumusque, X.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nitschelm, C.] Univ Antofagasta, Fac Ciencias Basicas, Unidad Astron, Antofagasta, Chile. [Querel, R. R.] Univ Chile, Dept Elect Engn, Santiago, Chile. [Querel, R. R.] Natl Inst Water & Atmospher Res NIWA, Auchland 1010, Lauder, New Zealand. [Hedelt, P.] Deutsch Zentrum Luft & Raumfahrt eV DER, D-82234 Oberpfaffenhofen, Wessling, Germany. [Berthier, J.] Observ Paris, Inst Mecan Celeste & Calcul Ephemerides, F-75014 Paris, France. [Moutou, C.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. [Moutou, C.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Crooker, D.] Univ Chile, Dept Astron, Santiago, Chile. RP Arnold, L (reprint author), Aix Marseille Univ, CNRS, Observ Haute Provence, Inst Pytheas UMS 3470, F-04870 St Michel Lobservatoire, France. EM Luc.Arnold@osupytheas.fr RI Querel, Richard/D-3770-2015 OI Querel, Richard/0000-0001-8792-2486 FU Conicyt through Fondecyt grant [3120150] FX We thank Gaspare Lo Curt (HARPS), and Claudio Melo and Lorenzo Monaco (UVES) for their help in the preparation of these relatively unusual observations, as well as the teams who operated the telescopes that night. We also thank I. Snellen, and the referee, W. A. Traub, for their constructive comments on the manuscript. R. R. Querel acknowledges funding from Conicyt through Fondecyt grant 3120150. NR 63 TC 4 Z9 4 U1 2 U2 8 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2014 VL 564 AR A58 DI 10.1051/0004-6361/201323041 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000058 ER PT J AU Israel, H Reiprich, TH Erben, T Massey, RJ Sarazin, CL Schneider, P Vikhlinin, A AF Israel, Holger Reiprich, Thomas H. Erben, Thomas Massey, Richard J. Sarazin, Craig L. Schneider, Peter Vikhlinin, Alexey TI The 400d Galaxy Cluster Survey weak lensing programme III. Evidence for consistent WL and X-ray masses at z approximate to 0.5 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: general; cosmology: observations; gravitational lensing: weak; X-rays: galaxies: clusters ID SOUTH-POLE TELESCOPE; BONN DEEP SURVEY; SCALING RELATIONS; TEMPERATURE RELATION; NONTHERMAL PRESSURE; LINEAR-REGRESSION; ASTRONOMICAL DATA; DENSITY PROFILE; NON-GAUSSIANITY; RICH CLUSTERS AB Context. Scaling properties of galaxy cluster observables with cluster mass provide central insights into the processes shaping clusters. Calibrating proxies for cluster mass that are relatively cheap to observe will moreover be crucial to harvest the cosmological information available from the number and growth of clusters with upcoming surveys like eROSITA and Euclid. The recent Planck results led to suggestions that X-ray masses might be biased low by similar to 40%, more than previously considered. Aims. We aim to extend knowledge of the weak lensing - X-ray mass scaling towards lower masses (as low as 1 x 10(14) M-circle dot) in a sample representative of the z similar to 0.4-0.5 population. Thus, we extend the direct calibration of cluster mass estimates to higher redshifts. Methods. We investigate the scaling behaviour of MMT/Megacam weak lensing (WL) masses for 8 clusters at 0.39 <= z <= 0.80 as part of the 400d WL programme with hydrostatic Chandra X-ray masses as well as those based on the proxies, e.g. Y-x = TxMgas. Results. Overall, we find good agreement between WL and X-ray masses, with different mass bias estimators all consistent with zero. When subdividing the sample into a low-mass and a high-mass subsample, we find the high-mass subsample to show no significant mass bias while for the low-mass subsample, there is a bias towards overestimated X-ray masses at the similar to 2 sigma level for some mass proxies. The overall scatter in the mass-mass scaling relations is surprisingly low. Investigating possible causes, we find that neither the greater range in WL than in X-ray masses nor the small scatter can be traced back to the parameter settings in the WL analysis. Conclusions. We do not find evidence for a strong (similar to 40%) underestimate in the X-ray masses, as suggested to reconcile recent Planck cluster counts and cosmological constraints. For high-mass clusters, our measurements are consistent with other studies in the literature. The mass dependent bias, significant at similar to 2 sigma, may hint at a physically different cluster population (less relaxed clusters with more substructure and mergers); or it may be due to small number statistics. Further studies of low-mass high-z lensing clusters will elucidate their mass scaling behaviour. C1 [Israel, Holger; Massey, Richard J.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Israel, Holger; Reiprich, Thomas H.; Erben, Thomas; Schneider, Peter] Argelander Inst Astron, D-53121 Bonn, Germany. [Sarazin, Craig L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Vikhlinin, Alexey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Israel, H (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. EM holger.israel@durham.ac.uk FU Deutsche Forschungsgemeinschaft (DFG) through Transregional Collaborative Research Centre [TR 33]; Deutsche Forschungsgemeinschaft (DFG) through the Schwerpunkt Program [1177]; Deutsche Forschungsgemeinschaft (DFG) through European Research Council [MIRG-CT-208994]; DFG [ER 327/3-1]; Transregional Collaborative Research Centre [TR 33]; Royal Society; MMT through NOAO [2007B-0046]; Silicon Valley Community Foundation FX The authors express their thanks to M. Arnaud and EXCPRES collaboration (private communication) for providing the hydrostatic masses of the Foex et al. (2012) clusters. We further thank A. Mahdavi for providing the masses of the Mahdavi et al. (2013) clusters via their helpful online interface. H.I. likes to thank M. Klein, J. Stott, and Y.-Y. Zhang, and the audiences of his presentations for useful comments. The authors thank the anonymous referee for their constructive suggestions. H.I. acknowledges support for this work has come from the Deutsche Forschungsgemeinschaft (DFG) through Transregional Collaborative Research Centre TR 33 as well as through the Schwerpunkt Program 1177 and through European Research Council grant MIRG-CT-208994. T.H.R. acknowledges support by the DFG through Heisenberg grant RE 1462/5 and grant RE 1462/6. T.E. is supported by the DFG through project ER 327/3-1 and by the Transregional Collaborative Research Centre TR 33 "The Dark Universe". R.M. is supported by a Royal Society University Research Fellowship. We acknowledge the grant of MMT observation time (program 2007B-0046) through NOAO public access. MMT time was also provided through support from the F. H. Levinson Fund of the Silicon Valley Community Foundation. NR 111 TC 23 Z9 23 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 APR PY 2014 VL 564 AR A129 DI 10.1051/0004-6361/201322870 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000129 ER PT J AU Menu, J van Boekel, R Henning, T Chandler, CJ Linz, H Benisty, M Lacour, S Min, M Waelkens, C Andrews, SM Calvet, N Carpenter, JM Corder, SA Deller, AT Greaves, JS Harris, RJ Isella, A Kwon, W Lazio, J Le Bouquin, JB Menard, F Mundy, LG Perez, LM Ricci, L Sargent, AI Storm, S Testi, L Wilner, DJ AF Menu, J. van Boekel, R. Henning, Th. Chandler, C. J. Linz, H. Benisty, M. Lacour, S. Min, M. Waelkens, C. Andrews, S. M. Calvet, N. Carpenter, J. M. Corder, S. A. Deller, A. T. Greaves, J. S. Harris, R. J. Isella, A. Kwon, W. Lazio, J. Le Bouquin, J. -B. Menard, F. Mundy, L. G. Perez, L. M. Ricci, L. Sargent, A. I. Storm, S. Testi, L. Wilner, D. J. TI On the structure of the transition disk around TW Hydrae SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE protoplanetary disks; techniques: interferometric; stars: individual: TW Hya ID INTERSTELLAR SILICATE MINERALOGY; HERBIG AE/BE STARS; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; HD 100546; SCATTERED-LIGHT; GRAIN-GROWTH; RADIATIVE-TRANSFER; ACCRETION DISKS; INNER HOLE AB Context. For over a decade, the structure of the inner cavity in the transition disk of TW Hydrae has been a subject of debate. Modeling the disk with data obtained at different wavelengths has led to a variety of proposed disk structures. Rather than being inconsistent, the individual models might point to the different faces of physical processes going on in disks, such as dust growth and planet formation. Aims. Our aim is to investigate the structure of the transition disk again and to find to what extent we can reconcile apparent model differences. Methods. A large set of high-angular-resolution data was collected from near-infrared to centimeter wavelengths. We investigated the existing disk models and established a new self-consistent radiative-transfer model. A genetic fitting algorithm was used to automatize the parameter fitting, and uncertainties were investigated in a Bayesian framework. Results. Simple disk models with a vertical inner rim and a radially homogeneous dust composition from small to large grains cannot reproduce the combined data set. Two modifications are applied to this simple disk model: (1) the inner rim is smoothed by exponentially decreasing the surface density in the inner similar to 3 AU, and (2) the largest grains (>100 mu m) are concentrated towards the inner disk region. Both properties can be linked to fundamental processes that determine the evolution of protoplanetary disks: the shaping by a possible companion and the different regimes of dust-grain growth, respectively. Conclusions. The full interferometric data set from near-infrared to centimeter wavelengths requires a revision of existing models for the TW Hya disk. We present a new model that incorporates the characteristic structures of previous models but deviates in two key aspects: it does not have a sharp edge at 4 AU, and the surface density of large grains differs from that of smaller grains. This is the first successful radiative-transfer-based model for a full set of interferometric data. C1 [Menu, J.; Waelkens, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Menu, J.; van Boekel, R.; Henning, Th.; Linz, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Chandler, C. J.; Perez, L. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Benisty, M.; Le Bouquin, J. -B.; Menard, F.] CNRS UJF Grenoble 1, UMR 5274, Inst Planetol & Astrophys Grenoble, F-38041 Grenoble, France. [Lacour, S.] Univ Paris Diderot, CNRS, UPMC, LESIA,Observ Paris, F-92195 Meudon, France. [Min, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Andrews, S. M.; Harris, R. J.; Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Calvet, N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Carpenter, J. M.; Isella, A.; Ricci, L.; Sargent, A. I.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Corder, S. A.] Joint ALMA Observ, Santiago 7630000, Chile. [Deller, A. T.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Greaves, J. S.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Kwon, W.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Lazio, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA. [Menard, F.] Univ Chile, CNRS INSU France UMI 3386, UMI FCA, Santiago, Chile. [Menard, F.] Univ Chile, Dept Astron, Santiago, Chile. [Mundy, L. G.; Storm, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Testi, L.] European So Observ, D-85748 Garching, Germany. [Testi, L.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Menu, J (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Louvain, Belgium. EM jonathan.menu@ster.kuleuven.be OI Deller, Adam/0000-0001-9434-3837 FU FWO travel grant [V448412N]; Millennium Science Initiative (Chilean Ministry of Economy) [Nucleus P10-022F]; EU FP7 [284405]; Smithsonian Institution; Academia Sinica FX J. Menu wishes to thank B. Acke for useful discussions, K. Johnston for support with the CASA software, and P. Degroote for providing SED analysis/fitting software. We are grateful to I. Pascucci and to the anonymous referee for comments that helped improving the manuscript. J. Menu acknowledges an FWO travel grant for a long research stay abroad (V448412N). F. Menard acknowledges support from the Millennium Science Initiative (Chilean Ministry of Economy), through grant "Nucleus P10-022F". F. Menard also acknowledges funding from the EU FP7-2011 under Grant Agreement No 284405. 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 NR 126 TC 31 Z9 31 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2014 VL 564 AR A93 DI 10.1051/0004-6361/201322961 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000093 ER PT J AU Petralia, A Reale, F Testa, P Del Zanna, G AF Petralia, A. Reale, F. Testa, P. Del Zanna, G. TI Thermal structure of a hot non-flaring corona from Hinode/EIS SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: corona; Sun: UV radiation; Sun: X-rays, gamma rays; techniques: spectroscopic; techniques: imaging spectroscopy ID SOLAR ACTIVE REGIONS; X-RAY-LINES; ATOMIC DATA; SPECTROSCOPIC OBSERVATIONS; IMAGING SPECTROMETER; EIS OBSERVATIONS; FE IX; EMISSION; PLASMA; DIAGNOSTICS AB Aims. In previous studies, a very hot plasma component has been diagnosed in solar active regions through the images in three different narrow-band channels of Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). This diagnostic from extreme ultraviolet (EUV) imaging data has also been supported by the matching morphology of emission in the hot Ca XVII line, as observed with Extreme-Ultraviolet Imaging Spectrometer (EIS) on board Hinode. This evidence is debated because of the unknown distribution of the emission measure along the line of sight. Here we investigate in detail the thermal distribution of one such region using EUV spectroscopic data. Methods. In an active region observed with SDO/AIA, Hinode/EIS, and X-ray telescope (XRT), we select a sub-region with a very hot plasma component and another cooler sub-region for comparison. The average spectrum is extracted for both, and 14 intense lines are selected for analysis that probe the 5.5 < log T < 7 temperature range uniformly. From these lines, the emission measure distributions are reconstructed with the Markov-chain Monte Carlo method. Results are cross-checked in comparison with the two sub-regions, with a different inversion method, with the morphology of the images, and with the addition of fluxes measured with narrow, and broadband imagers. Results. We find that, whereas the cool region has a flat and featureless distribution that drops at temperature log T >= 6.3, the distribution of the hot region shows a well-defined peak at log T = 6.6 and gradually decreasing trends on both sides, thus supporting the very hot nature of the hot component diagnosed with imagers. The other cross-checks are consistent with this result. Conclusions. This study provides a completion of the analysis of active region components, and the resulting scenario supports the presence of a minor very hot plasma component in the core, with temperatures log T > 6.6. C1 [Petralia, A.; Reale, F.] Univ Palermo, Dipartimento Fis & Chim, I-90134 Palermo, Italy. [Reale, F.] INAF, Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Testa, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Del Zanna, G.] DAMTP, Ctr Math Sci, Cambridge, England. RP Petralia, A (reprint author), Univ Palermo, Dipartimento Fis & Chim, Piazza Parlamento 1, I-90134 Palermo, Italy. EM apetralia@astropa.unipa.it OI Petralia, Antonino/0000-0002-9882-1020; Reale, Fabio/0000-0002-1820-4824 FU Italian Ministero dell'Universita e Ricerca (MIUR); STFC (UK); Lockheed-Martin [SP02H1701R]; NASA [NNM07AB07C, NNX11AC20G] FX A.P. and ER. acknowledge support from Italian Ministero dell'Universita e Ricerca (MIUR). G.D.Z. acknowledges support from STFC (UK). P.T. was supported by contract SP02H1701R from Lockheed-Martin, NASA contract NNM07AB07C to SAO, and NASA grant NNX11AC20G. CHIANTI is a collaborative project involving the NRL (USA), the Universities of Florence (Italy) and Cambridge (UK), and George Mason University (USA). 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). SDO data were supplied courtesy of the SDO/AIA consortium. SDO is the first mission to be launched for NASA's Living With a Star Program. We thank the International Space Science Institute (ISSI) for hosting the International Team of S. Bradshaw and H. Mason: Coronal Heating - Using Observables to Settle the Question of Steady vs. Impulsive Heating. NR 43 TC 7 Z9 7 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2014 VL 564 AR A3 DI 10.1051/0004-6361/201322998 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000003 ER PT J AU Phan-Bao, N Lee, CF Ho, PTP Martin, EL AF Phan-Bao, N. Lee, C. -F. Ho, P. T. P. Martin, E. L. TI Submillimeter Array observations of the proto brown dwarf candidate SSTB213 J041757 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: jets and outflows; brown dwarfs; techniques: interferometric; stars: formation ID BIPOLAR MOLECULAR OUTFLOW; CLOUD CORE; SKY SURVEY; DISCOVERY; COLORS; TAURUS; PHOTOMETRY; TELESCOPE; PASSBANDS; L1014-IRS AB Context. The previously identified source SSTB213 J041757 is a proto brown dwarf candidate in Taurus, which has two possible components A and B. It was found that component B is probably a class 0/I proto brown dwarf associated with an extended envelope. Aims. Studying molecular outflows from young brown dwarfs provides important insight into brown dwarf formation mechanisms, particularly brown dwarfs at the earliest stages such as class 0, I. We therefore conducted a search for molecular outflows from SSTB213 J041757. Methods. We observed SSTB213 J041757 with the Submillimeter Array to search for CO molecular outflow emission from the source. Results. Our CO maps do not show any outflow emission from the proto brown dwarf candidate. Conclusions. The non-detection implies that the molecular outflows from the source are weak; deeper observations are therefore needed to probe the outflows from the source. C1 [Phan-Bao, N.] HCM Int Univ VNU, Dept Phys, Linh Trung Ward, Ho Chi Minh City, Vietnam. [Phan-Bao, N.; Lee, C. -F.; Ho, P. T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Martin, E. L.] Ctr Astrobiol CAB CSIC, Madrid 28850, Spain. [Ho, P. T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Phan-Bao, N (reprint author), HCM Int Univ VNU, Dept Phys, Linh Trung Ward, Block 6, Ho Chi Minh City, Vietnam. EM pbngoc@hcmiu.edu.vn FU Viet Nam NAFOSTED grant [103.08-2010.17]; Spanish Ministry of Economy and Competitiveness (MINECO) [AyA2011-30147-C03-03] FX N.P.-B. has been supported by Viet Nam NAFOSTED grant 103.08-2010.17. E.M. has been supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under grant AyA2011-30147-C03-03 and wishes to thank the Geosciences Department at the University of Florida for a visiting appointment. We also thank the referee for valuable comments. This work is based in part on data obtained as part of the UKIRT Infrared Deep Sky Survey and has made use of the Centre de Donnees astronomiques de Strasbourg (CDS) database. NR 26 TC 3 Z9 3 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 APR PY 2014 VL 564 AR A32 DI 10.1051/0004-6361/201323055 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000032 ER PT J AU Pinilla, P Benisty, M Birnstie, T Ricci, L Isella, A Natta, A Dullemond, CP Quiroga-Nunez, LH Henning, T Testi, L AF Pinilla, P. Benisty, M. Birnstie, T. Ricci, L. Isella, A. Natta, A. Dullemond, C. P. Quiroga-Nunez, L. H. Henning, T. Testi, L. TI Millimetre spectral indices of transition disks and their relation to the cavity radius SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; protoplanetary disks; circumstellar matter; planets and satellites: formation ID T-TAURI STARS; PROTOPLANETARY ACCRETION DISKS; GRAIN-GROWTH; PLANET FORMATION; CIRCUMSTELLAR DISKS; YOUNG STARS; DUST FILTRATION; BROWN DWARF; SAO 206462; GAP EDGES AB Context. Transition disks are protoplanetary disks with inner depleted dust cavities that are excellent candidates for investigating the dust evolution when there is a pressure bump. A pressure bump at the outer edge of the cavity allows dust grains from the outer regions to stop their rapid inward migration towards the star and to efficiently grow to millimetre sizes. Dynamical interactions with planet(s) have been one of the most exciting theories to explain the clearing of the inner disk. Aims. We look for evidence of millimetre dust particles in transition disks by measuring their spectral index alpha(mm), with new and available photometric data. We investigate the influence of the size of the dust depleted cavity on the disk integrated millimetre spectral index. Methods. We present the 3-mm (100 GHz) photometric observations carried out with the Plateau de Bure Interferometer of four transition disks: LkH alpha 330, UX Tau A, LRLL 31, and LRLL 67. We used the available values of their fluxes at 345 GHz to calculate their spectral index, as well as the spectral index for a sample of twenty transition disks. We compared the observations with two kinds of models. In the first set of models, we considered coagulation and fragmentation of dust in a disk in which a cavity is formed by a massive planet located at different positions. The second set of models assumes disks with truncated inner parts at different radii and with power-law dust-size distributions, where the maximum size of grains is calculated considering turbulence as the source of destructive collisions. Results. We show that the integrated spectral index is higher for transition disks (TD) than for regular protoplanetary disks (PD) with mean values of (alpha) over bar (TD)(mm) = 2.70 +/- 0.13 and (alpha) over bar (PD)(mm) = 2.20 +/- 0.07 respectively. For transition disks, the probability that the measured spectral index is positively correlated with the cavity radius is 95%. High angular resolution imaging of transition disks is needed to distinguish between the dust trapping scenario and the truncated disk case. C1 [Pinilla, P.; Quiroga-Nunez, L. H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Pinilla, P.; Dullemond, C. P.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Benisty, M.] CNRS UJF UMR 5571, Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Birnstie, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ricci, L.; Isella, A.] CALTECH, Pasadena, CA 91125 USA. [Natta, A.; Testi, L.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Natta, A.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Testi, L.] European So Observ, D-85748 Garching, Germany. RP Pinilla, P (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM pinilla@strw.leidenuniv.nl OI Dullemond, Cornelis/0000-0002-7078-5910 FU NASA Origins of Solar Systems grant [NNX12AJ04G]; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX The authors are very thankful to J. M. Winters for his help understanding GILDAS for the PdBI data reduction. We acknowledge S. Andrews, N. van der Marel, and E. van Dishoeck for the helpful comments and feedback on the manuscript. TB acknowledges support from NASA Origins of Solar Systems grant NNX12AJ04G. This publication is based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). NR 81 TC 9 Z9 9 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 APR PY 2014 VL 564 AR A51 DI 10.1051/0004-6361/201323322 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4GW UT WOS:000334671000051 ER PT J AU Gomez, CG Guzman, HM Gonzalez, A Breedy, O AF Gomez, Catalina G. Guzman, Hector M. Gonzalez, Andrew Breedy, Odalisca TI Survival, growth, and recruitment of octocoral species (Coelenterata: Octocorallia) in Coiba National Park, Pacific Panama SO BULLETIN OF MARINE SCIENCE LA English DT Article ID MASS MORTALITY EVENT; 2 GORGONIAN CORALS; CARIJOA-RIISEI; POPULATION-DYNAMICS; PARAMURICEA-CLAVATA; PACIFIGORGIA COELENTERATA; ANTHOZOA OCTOCORALLIA; DISTRIBUTION PATTERNS; EUNICELLA-SINGULARIS; ECOLOGICAL STRUCTURE AB Octocorals (order Alcyonacea) from the tropical eastern Pacific have been largely ignored in coral reef studies, with the exception of recent taxonomic reviews. This study is the first to examine the population dynamics of 10 shallow water species in six genera (Leptogorgia, Pacifigorgia, Muricea, Psammogorgia, Heterogorgia, and Carijoa) found in rocky coral communities in Coiba National Park, Pacific Panama. For a 17-mo period, we monitored, every 4 mo, 1445 colonies of 15 species in fixed plots at 20 m depth in four coral communities. Size distribution, survivorship, and recruitment rates were calculated. Growth rate was calculated for Leptogorgia alba Duchassaing and Michelotti, 1864, Pacifigorgia Irene Bayer, 1951, Psammogorgia arbuscula Verrill, 1868, and Muricea austera Lamouroux, 1821. Average octocoral density was 38.7 (SD 27.55) colonies m(-2) (n = 1394) with a range of 1-103 colonies m-2 and 1-11 species within a study plot. An overall population decline of 25.2% was observed in 1 yr. Leptogorgia alba was the most common species; it was abundant at all sites and exhibited characteristics of an r-selected species. In contrast, M. austera showed traits of a K-selected species, with low mortality and recruitment rates. Studied species were grouped into two distinct clusters based on their distribution, average density, mortality, and recruitment rates. Five species were grouped with L. alba and six species were grouped with M. austera. C1 [Gomez, Catalina G.; Guzman, Hector M.; Breedy, Odalisca] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Gonzalez, Andrew] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, Ctr Invest Estruct Microscop, San Jose 115012060, Costa Rica. RP Gomez, CG (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM gomezc@si.edu; guzmanh@si.edu; andrew.gonzalez@mcgill.ca; odaliscab@gmail.com FU Secretaria Nacional de Ciencia y Tecnologia de Panama (SENACYT- Grant) [PNCOIBA-08-024]; Smithsonian Tropical Research Institute; McGill-STRI NEO Program FX The authors thank C Guevara for laborious assistance in the field; the Government of Panama (ANAM), which provided permits to work in Coiba National Park; and the reviewers for their comments. This research was partially sponsored by Secretaria Nacional de Ciencia y Tecnologia de Panama (SENACYT- Grant No, PNCOIBA-08-024), the Smithsonian Tropical Research Institute, and the McGill-STRI NEO Program. NR 99 TC 0 Z9 0 U1 4 U2 21 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 APR PY 2014 VL 90 IS 2 BP 623 EP 650 DI 10.5343/bms.2013.1092 PG 28 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA AF8OQ UT WOS:000334975900007 ER PT J AU Roberts, TR AF Roberts, Tyson R. TI Wallago Bleeker, 1851 and Wallagonia Myers, 1938 (Ostariophysi, Siluridae), Distinct Genera of Tropical Asian Catfishes, with Description of dagger Wallago maemohensis from the Miocene of Thailand SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article DE Catfishes; Siluridae; Wallago attu; Wallagonia leerii; Wallago maemohensis; Miocene; Thailand ID SILURIFORMES AB The Southeast Asian silurid catfish genus Wallagonia Myers, 1938, although regarded as a junior synonym of Wallago Bleeker, 1851 by recent authors following Myers (1948), differs fundamentally from it in many external and osteological characters. The genera evidently have been distinct since at least the middle Miocene and apparently are not closely related to each other. Wallagonia seems most similar to the silurid genus Ompok. Wallago differs most strikingly from all other silurids in having a much longer gape, extending ventroposteriorly well beyond the eyes. The extremely elongate upper jaw has a unique bony composition and suspension. It consists of three bones: the toothed premaxillary bone anteriorly, and the toothless suborbital and first postorbital bones posteriorly. The premaxillary bone is partially suspended from the cranium by the infraorbital bone. The closest relatives of Wallago have not been identified. Wallagonia and Wallago have no previously reported fossil records. Fossils of the family Siluridae have been identified as representatives of the Eurasian temperate genus Silurus (Kobayakawa, 1989). Here an extinct species of Wallago is described, W. maemohensis, on the basis of a complete cranium with attached, fully toothed left premaxillary in an unusually fine state of preservation from a Miocene deposit near Lampang in northern Thailand. Fossil catfishes previously reported from Thailand belong to the families Bagridae and Pangasiidae and are from Pliocene deposits (Roberts and Junmongthai 1999). C1 [Roberts, Tyson R.] Mahidol Univ, Inst Mol Biosci, Nakon Phatom, Thailand. [Roberts, Tyson R.] Smithsonian Trop Res Inst, Panama City, Panama. RP Roberts, TR (reprint author), Mahidol Univ, Inst Mol Biosci, Salaya Campus, Nakon Phatom, Thailand. EM tysonregalecus@gmail.com NR 17 TC 0 Z9 0 U1 1 U2 9 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118 USA SN 0079-032X EI 2162-4135 J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD APR PY 2014 VL 55 IS 1 BP 35 EP 47 PG 13 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AF7MF UT WOS:000334898500002 ER PT J AU Moser, WE Richardson, DJ Hammond, CI Lazo-Wasem, EA AF Moser, William E. Richardson, Dennis J. Hammond, Charlotte I. Lazo-Wasem, Eric A. TI Redescription and Molecular Characterization of Placobdella hollensis (Whitman, 1892) (Hirudinida: Glossiphoniidae) SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article DE Rhychobdellida; Hirudinea; Clitellata; Glossiphoniidae; Placobdella; Clepsine; Massachusetts; leech AB Placobdella hollensis was originally named Clepsine hollensis by Whitman (1892) from specimens collected near Woods Hole, Massachusetts; however, type specimens were neither declared nor deposited. Specimens of P. hollensis were collected from Coonamessett Pond in Barnstable County (47 degrees 37'10.25"N, 70 degrees 34'20.42"W), Massachusetts, on 4 and 30 May, 2013. Their acquisition from the general locality where Whitman (1892) collected specimens facilitated redescription of P. hollensis. A neotype is designated to stabilize the concept of P. hollensis. Placobdella hollensis is unique among its congeners in its possession of accessory "eyes." Placobdella hollensis is modestly papillated and has a dorsomedial row and a pair of paralateral rows of unpigmented papillae, two rows of three paramedial pre-anal papillae, and two rows of two paralateral pre-anal papillae. Unlike P. all, P. multilineata, P. papillifera, and P. parasitica, the ventrum of P. hollensis does not have stripes. Placobdella hollensis does have two thin paramedial dark lines on its ventrum, which are also present in P. papillifera. Molecular comparison of CO-I sequence data from P. hollensis revealed differences of 14% from P. multilineata, 15% from P. picta, 15% to 16% from P. papillifera, 16% from P. translucens, 16% to 17% from P. rugosa, 16% to 17% from P. ornata, 17% from P. montifera, 17% to 18% from P. ali, and 18% from P. biannulata. C1 [Moser, William E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Museum Support Ctr MRC 534, Suitland, MD 20746 USA. [Richardson, Dennis J.; Hammond, Charlotte I.] Quinnipiac Univ, Sch Biol Sci, Hamden, CT 06518 USA. [Lazo-Wasem, Eric A.] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA. RP Moser, WE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Museum Support Ctr MRC 534, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM moserw@si.edu; Dennis.Richardson@quinnipiac.edu; Charlotte.Hammond@quinnipiac.edu; eric.lazo-wasem@yale.edu NR 15 TC 1 Z9 1 U1 3 U2 4 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118 USA SN 0079-032X EI 2162-4135 J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD APR PY 2014 VL 55 IS 1 BP 49 EP 54 PG 6 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AF7MF UT WOS:000334898500003 ER PT J AU Esquivias, MP Zunzunegui, M Barradas, MCD Alvarez-Cansino, L AF Paz Esquivias, M. Zunzunegui, Maria Diaz Barradas, Mari Cruz Alvarez-Cansino, Leonor TI The role of water use and uptake on two Mediterranean shrubs' interaction in a brackish coastal dune ecosystem SO ECOHYDROLOGY LA English DT Article DE Thymus carnosus; Retama monosperma; water potential; proline; stable isotopes; drought; competition; facilitation ID STABLE-ISOTOPE COMPOSITION; PROLINE ACCUMULATION; EVERGREEN SCLEROPHYLLS; POSITIVE INTERACTIONS; SEMIARID ENVIRONMENT; RETAMA-SPHAEROCARPA; GAS-EXCHANGE; STRESS; PLANTS; PRECIPITATION AB Water relations are essential in plant-plant interactions, particularly in Mediterranean coastal sand dunes, owing to marked drought periods and the possibility of groundwater (GW) salinization. In this study, seasonal water use dynamics were explored in the interaction between a native-invasive species, Retama monosperma, and the endangered Thymus carnosus, in south-western Spain. The following variables were measured: xylem water isotopic composition to determine water sources, predawn and midday stem water potential and free leaf proline content as stress indicator. GW electrical conductivity and stable isotopes were also analysed to assess water table salinity. In late summer and spring, the warmest seasons, Thymus beneath Retama displayed significantly lower water potential and higher leaf proline content than isolated Thymus, whereas Retama showed the highest proline content in autumn and winter. Water sources showed different patterns depending on the Thymus situation: Isolated ones always matched the brackish GW, as well as Retama plants, whereas Thymus beneath Retama switched among rainfall, soil and water table, showing a seasonal change in the water-harvesting strategy. Overall, competition for water sources between both species was discovered, which led to a shift in water use and water uptake strategies of understorey Thymus. The results also demonstrate the importance and potential use of species interaction studies in the development of threatened species management strategies. Copyright (c) 2013 John Wiley & Sons, Ltd. C1 [Paz Esquivias, M.; Zunzunegui, Maria; Diaz Barradas, Mari Cruz] Univ Seville, Dept Plant Biol & Ecol, Seville 41080, Spain. [Alvarez-Cansino, Leonor] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. [Alvarez-Cansino, Leonor] Smithsonian Trop Res Inst, Panama City, Panama. RP Esquivias, MP (reprint author), Univ Seville, Dept Plant Biol & Ecol, POB 1095, Seville 41080, Spain. EM esquiviasmp@us.es RI Zunzunegui, Maria/L-8357-2014; OI Zunzunegui, Maria/0000-0002-3815-9290; Esquivias, M. Paz/0000-0001-5647-9936 FU Spanish Ministry of Education and Science [CGL2005-02142]; FPDI-Junta de Andalucia fellowship FX We thank Alba Cuecas, Sofia Segura, Carlos Perez, Miguel Clavero, Elena Garcia-Gomez, Amara Lastres, Ana Fernandez and Jon Jauregui for field assistance. Pablo Fernandez and Esperanza Moguer were of great help with stem distillation and proline extraction. We also thank Juan B. Gallego Fernandez and two anonymous reviewers for their helpful comments on earlier versions of this paper. The Junta de Andalucia Environmental Agency provided permission to work in the Natural Reserve and with the protected species. This work was partly funded by the Spanish Ministry of Education and Science (CGL2005-02142). M. P. E. was supported by a FPDI-Junta de Andalucia fellowship. NR 57 TC 2 Z9 2 U1 4 U2 32 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1936-0584 EI 1936-0592 J9 ECOHYDROLOGY JI Ecohydrology PD APR PY 2014 VL 7 IS 2 BP 783 EP 793 DI 10.1002/eco.1401 PG 11 WC Ecology; Environmental Sciences; Water Resources SC Environmental Sciences & Ecology; Water Resources GA AF4HC UT WOS:000334671600047 ER PT J AU Kaspari, M Clay, NA Donoso, DA Yanoviak, SP AF Kaspari, Michael Clay, Natalie A. Donoso, David A. Yanoviak, Steven P. TI Sodium fertilization increases termites and enhances decomposition in an Amazonian forest SO ECOLOGY LA English DT Article DE sodium ecosystem respiration (SER) hypothesis; tropical rainforest; nutrient limitation; ecosystem respiration; Yasuni Ecological Research Station, Ecuador; oceanic aerosols; decomposition; biogeochemistry; precipitation; brown food web; sodium ID TROPICAL RAIN-FOREST; SOIL ORGANIC-MATTER; COARSE WOODY DEBRIS; LITTER DECOMPOSITION; PLANT LITTER; CARBON-CYCLE; DYNAMICS; CLIMATE; PHOSPHORUS; LIMITATION AB Added Na was used to determine whether litter decomposition and associated fungal biomass and termites are limited by Na availability in a lowland tropical rainforest at Yasuni, Ecuador. This is a partial test of the "sodium ecosystem respiration" (SER) hypothesis that posits Na is critical for consumers but not plants, that Na shortfall is more likely on highly weathered soils inland from oceanic aerosols, and that this shortfall results in decreased decomposer activity. We fertilized 4 x 4 m plots twice a month for a year with quantities of Na comparable to those falling on a coastal tropical rainforest. Decomposition rates of four substrates were consistently higher on +NaCl plots by up to 70% for cellulose, and 78%, 68%, and 29% for three woods of increasing percentage lignin. The density of termite workers averaged 17-fold higher on +NaCl plots; fungal biomass failed to differ. After controlling for temperature and precipitation, which co-limit gross primay productivity (GPP) and ecosystem respiration (ER), these results suggest that Na shortfall is an agent enhancing the storage of coarse woody debris in inland tropical forests. C1 [Kaspari, Michael; Clay, Natalie A.; Donoso, David A.] Univ Oklahoma, Grad Program Ecol & Evolut, Dept Biol, Norman, OK 73019 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama. [Donoso, David A.] Univ Tecn Particular Loja, Dept Ciencias Nat, Loja, Ecuador. [Yanoviak, Steven P.] Univ Louisville, Dept Biol, Louisville, KY 40292 USA. RP Kaspari, M (reprint author), Univ Oklahoma, Grad Program Ecol & Evolut, Dept Biol, Norman, OK 73019 USA. EM mkaspari@ou.edu RI Donoso, David/A-2059-2016; OI Donoso, David/0000-0002-3408-1457; Kaspari, Michael/0000-0002-9717-5768 FU NSF [DEB-0948762] FX Funding was provided by NSF DEB-0948762 to M. Kaspari. Thanks to Nina Velasco and Sophie King for help in the field. NR 63 TC 19 Z9 19 U1 4 U2 64 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD APR PY 2014 VL 95 IS 4 BP 795 EP 800 DI 10.1890/13-1274.1 PG 6 WC Ecology SC Environmental Sciences & Ecology GA AF2WQ UT WOS:000334573600001 PM 24933800 ER PT J AU Wood, CL Lafferty, KD DeLeo, G Young, HS Hudson, PJ Kuris, AM AF Wood, Chelsea L. Lafferty, Kevin D. DeLeo, Giulio Young, Hillary S. Hudson, Peter J. Kuris, Armand M. TI Does biodiversity protect humans against infectious disease? SO ECOLOGY LA English DT Article DE biodiversity loss; zoonosis; disease; conservation; parasite; dilution effect; pathogen ID SIN NOMBRE VIRUS; LYME-DISEASE; SPECIES-DIVERSITY; PATHOGEN TRANSMISSION; FOREST FRAGMENTATION; HOST DIVERSITY; RISK-FACTORS; ECOLOGY; IMPACT; EMERGENCE AB Control of human infectious disease has been promoted as a valuable ecosystem service arising from the conservation of biodiversity. There are two commonly discussed mechanisms by which biodiversity loss could increase rates of infectious disease in a landscape. First, loss of competitors or predators could facilitate an increase in the abundance of competent reservoir hosts. Second, biodiversity loss could disproportionately affect non-competent, or less competent reservoir hosts, which would otherwise interfere with pathogen transmission to human populations by, for example, wasting the bites of infected vectors. A negative association between biodiversity and disease risk, sometimes called the "dilution effect hypothesis," has been supported for a few disease agents, suggests an exciting win-win outcome for the environment and society, and has become a pervasive topic in the disease ecology literature. Case studies have been assembled to argue that the dilution effect is general across disease agents. Less touted are examples in which elevated biodiversity does not affect or increases infectious disease risk for pathogens of public health concern. In order to assess the likely generality of the dilution effect, we review the association between biodiversity and public health across a broad variety of human disease agents. Overall, we hypothesize that conditions for the dilution effect are unlikely to be met for most important diseases of humans. Biodiversity probably has little net effect on most human infectious diseases but, when it does have an effect, observation and basic logic suggest that biodiversity will be more likely to increase than to decrease infectious disease risk. C1 [Wood, Chelsea L.; DeLeo, Giulio] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Wood, Chelsea L.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. [Lafferty, Kevin D.] Univ Calif Santa Barbara, US Geol Survey, Western Ecol Res Ctr, Inst Marine Sci, Santa Barbara, CA 93106 USA. [DeLeo, Giulio] Univ Parma, Dipartimento Sci Ambientali, I-43100 Parma, Italy. [Young, Hillary S.; Kuris, Armand M.] Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. [Young, Hillary S.; Kuris, Armand M.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Young, Hillary S.] Smithsonian Inst, Div Mammals, Washington, DC 20013 USA. [Hudson, Peter J.] Penn State Univ, Ctr Infect Dis Dynam, University Pk, PA 16802 USA. RP Wood, CL (reprint author), Stanford Univ, Dept Biol, Stanford, CA 94305 USA. EM chelsea.wood@colorado.edu RI Lafferty, Kevin/B-3888-2009 OI Lafferty, Kevin/0000-0001-7583-4593 FU National Science Foundation; Alyce B. and Henry J. Ramey, Jr. Stanford Graduate Fellowship; Italian Ministry of Research; NSF-NIH Ecology and Evolution of Infectious Diseases Program grant [OCE-1115965]; NIH RAPIDD program FX C. L. Wood was supported by a National Science Foundation Graduate Research Fellowship and an Alyce B. and Henry J. Ramey, Jr. Stanford Graduate Fellowship. G. DeLeo was partially supported by the Italian Ministry of Research under the program PRIN2008, A. M. Kuris and K. D. Lafferty were supported by an NSF-NIH Ecology and Evolution of Infectious Diseases Program grant (OCE-1115965), and P. J. Hudson was supported by the NIH RAPIDD program. Mike Begon, Andy Dobson, Andres Gomez, Fiorenza Micheli, and Natalie Cooper made helpful comments on earlier versions of the manuscript, and Heather Ferguson and Joanne Webster contributed useful suggestions on the analysis of Table 1. NR 87 TC 41 Z9 42 U1 29 U2 210 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD APR PY 2014 VL 95 IS 4 BP 817 EP 832 DI 10.1890/13-1041.1 PG 16 WC Ecology SC Environmental Sciences & Ecology GA AF2WQ UT WOS:000334573600004 PM 24933803 ER PT J AU Lebrija-Trejos, E Wright, SJ Hernandez, A Reich, PB AF Lebrija-Trejos, Edwin Wright, S. Joseph Hernandez, Andres Reich, Peter B. TI Does relatedness matter? Phylogenetic density-dependent survival of seedlings in a tropical forest SO ECOLOGY LA English DT Article DE density dependence; conspecific; Panama; tropical forest; relative nearest taxon phylodiversity (NTPd'); phylogenetic distance; average relative phylodiversity (APd'); phylogenetic signal; seedling survival; heterospecific; functional traits; neighborhood ID SPECIES SHADE TOLERANCE; DISPERSAL DISTANCE; FUNCTIONAL TRAITS; RAIN-FOREST; HOST-RANGE; TREE; COMMUNITY; MORTALITY; DIVERSITY; PATHOGENS AB A complex set of interactions among neighbors influences plant performance and community structure. Understanding their joint operation requires extensive information on species characteristics and individual performance. We evaluated first-year survival of 35 719 tropical forest seedlings of 222 species and 15 annual cohorts relative to the density of conspecific and heterospecific neighbors and the phylogenetic similarity of heterospecific neighbors. Neighbors were from two size classes, and size asymmetric interactions provided insight into likely mechanisms. Large heterospecific and conspecific neighbors reduced seedling survival equally, suggesting resource competition rather than host-specific enemies as a mechanism. In contrast, much stronger negative conspecific effects were associated with seedling neighbors capable of limited resource uptake, suggesting shared pests rather than competition as the mechanism. Survival improved, however, near phylogenetically similar heterospecific neighbors, suggesting habitat associations shared among closely related species affect spatial patterns of performance. Improved performance near phylogenetically similar neighbors is an emerging pattern in the handful of similar studies. C1 [Lebrija-Trejos, Edwin; Wright, S. Joseph; Hernandez, Andres] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Lebrija-Trejos, Edwin; Reich, Peter B.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. [Reich, Peter B.] Univ Western Sydney, Hawkesbury Inst Environm, Richmond 2753, Australia. RP Lebrija-Trejos, E (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa Ancon, Panama. EM elebrija@gmail.com RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU Smithsonian Institution Global Earth Observatory; Institute of the Environment, University of Minnesota; NSF [DEB-1046113] FX E. Lebrija-Trejos was supported by a post-doctoral fellowship from the Smithsonian Institution Global Earth Observatory and the Institute of the Environment, University of Minnesota. Analyses were facilitated by workshops sponsored by NSF grant DEB-1046113 to S. Davies. NR 65 TC 21 Z9 23 U1 6 U2 72 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD APR PY 2014 VL 95 IS 4 BP 940 EP 951 DI 10.1890/13-0623.1 PG 12 WC Ecology SC Environmental Sciences & Ecology GA AF2WQ UT WOS:000334573600014 PM 24933813 ER PT J AU Tonra, CM Marini, KLD Marra, PP Germain, RR Holberton, RL Reudink, MW AF Tonra, Christopher M. Marini, Kristen L. D. Marra, Peter P. Germain, Ryan R. Holberton, Rebecca L. Reudink, Matthew W. TI Color expression in experimentally regrown feathers of an overwintering migratory bird: implications for signaling and seasonal interactions SO ECOLOGY AND EVOLUTION LA English DT Article DE American redstart; carotenoid; delayed plumage maturation; molt; plumage color; Setophaga ruticilla ID NON-BREEDING SEASON; REDSTART SETOPHAGA-RUTICILLA; AMERICAN REDSTART; SEXUAL SELECTION; HABITAT QUALITY; NUTRITIONAL CONDITION; PLUMAGE COLORATION; NONBREEDING SEASON; TERRITORY QUALITY; BODY CONDITION AB Plumage coloration in birds plays a critical role in communication and can be under selection throughout the annual cycle as a sexual and social signal. However, for migratory birds, little is known about the acquisition and maintenance of colorful plumage during the nonbreeding period. Winter habitat could influence the quality of colorful plumage, ultimately carrying over to influence sexual selection and social interactions during the breeding period. In addition to the annual growth of colorful feathers, feather loss from agonistic interactions or predator avoidance could require birds to replace colorful feathers in winter or experience plumage degradation. We hypothesized that conditions on the wintering grounds of migratory birds influence the quality of colorful plumage. We predicted that the quality of American redstart (Setophaga ruticilla) tail feathers regrown after experimental removal in Jamaica, West Indies, would be positively associated with habitat quality, body condition, and testosterone. Both yearling (SY) and adult (ASY) males regrew feathers with lower red chroma, suggesting reduced carotenoid content. While we did not observe a change in hue in ASY males, SY males shifted from yellow to orange plumage resembling experimentally regrown ASY feathers. We did not observe any effects of habitat, testosterone, or mass change. Our results demonstrate that redstarts are limited in their ability to adequately replace colorful plumage, regardless of habitat, in winter. Thus, feather loss on the nonbreeding grounds can affect social signals, potentially negatively carrying over to the breeding period. C1 [Tonra, Christopher M.; Marra, Peter P.] Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Tonra, Christopher M.; Holberton, Rebecca L.] Univ Maine, Sch Biol & Ecol, Orono, ME USA. [Marini, Kristen L. D.; Reudink, Matthew W.] Thompson Rivers Univ, Dept Biol Sci, Kamloops, BC V2C 0C8, Canada. [Germain, Ryan R.] Univ British Columbia, Ctr Appl Conservat Res, Vancouver, BC V6T 1Z4, Canada. RP Tonra, CM (reprint author), Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, POB 37012-MRC 5503, Washington, DC 20013 USA. EM tonrac@si.edu RI Tonra, Christopher/B-1620-2013; OI Reudink, Matthew/0000-0001-8956-5849 FU National Science Foundation [0649679, 0717338]; Holberton [0615701]; Doctoral Dissertation Improvement Grant [1011123]; National Sciences and Engineering Research Council of Canada; Thompson Rivers University CUEF U-REAP; American Ornithologist Union Student Research Award; American Museum of Natural History Frank M. Chapman Award; Cooper Ornithological Society Joseph Grinnell Student Research Award; Wilson Ornithological Society; Smithsonian Institution; Maine Agricultural and Forest Experimental Station FX Funding for this project was provided by grants awarded by the National Science Foundation to Marra (0649679, 0717338), Holberton (0615701), a Doctoral Dissertation Improvement Grant to Tonra (1011123), a National Sciences and Engineering Research Council of Canada Discovery Grant to Reudink, and a Thompson Rivers University CUEF U-REAP to Marini. Additional funds were provided to Tonra by the American Ornithologist Union Student Research Award, the American Museum of Natural History Frank M. Chapman Award, the Cooper Ornithological Society Joseph Grinnell Student Research Award, the Wilson Ornithological Society Louis Agassiz Fuertes Award, and a Pre-doctoral Fellowship from the Smithsonian Institution. The Maine Agricultural and Forest Experimental Station, with funds awarded to Holberton, also helped to support this project. We are grateful to the National Environmental Protection Agency of Jamaica and the Petroleum Corporation of Jamaica for permission to conduct this research at the Font Hill Nature Preserve. We wish to thank Laurene Ratcliffe for her input and support on this project. We are indebted to all of the dedicated biologists, too numerous to name here, who contributed to data collection for this study. We especially want to thank Frederic Angelier, Nathan Cooper, Rob Dobbs, Jeannine Randall, and Mark Thomas. NR 53 TC 5 Z9 5 U1 2 U2 21 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD APR PY 2014 VL 4 IS 8 BP 1222 EP 1232 DI 10.1002/ece3.994 PG 11 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA AF3GZ UT WOS:000334601100002 PM 24834321 ER PT J AU Jerep, FC Vari, RP Vreven, E AF Jerep, Fernando C. Vari, Richard P. Vreven, Emmanuel TI Nannocharax dageti, a new distichodontid from the Democratic Republic of the Congo and Zambia (Teleostei: Characiformes) SO ICHTHYOLOGICAL EXPLORATION OF FRESHWATERS LA English DT Article ID CAMEROON; RIVER AB Nannocharax dageti, new species, is described from southern tributaries of the Congo River basin in the Democratic Republic of the Congo and Zambia and the Kafue River basin of the Zambezi River catchment in Zambia. The new species is distinguished from its congeners by the pigmentation pattern consisting of vertically elongated, dark, rounded blotches overlapping a dark midlateral longitudinal stripe; the separation of the blotches in many cases from the dorsal saddles that extend to the middorsal line; the symmetrical coloration pattern on each caudal-fin lobe consisting of a dark spot on the base of each lobe and a series of dark spots forming a transverse narrow stripe across each lobe approximately one-third of the distance from the fin margin; a dorsal-fin origin situated anterior of the pelvic-fin origin; and the possession of 40 to 43 scales along the incompletely pored lateral-line series. Nannocharax dageti is apparently allopatric to other species of Nannocharax in southern tributaries of the Congo River. C1 [Jerep, Fernando C.; Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. [Jerep, Fernando C.] Univ Estadual Londrina, Ctr Ciencias Biol, Dept Biol Anim & Vegetal, BR-86051990 Londrina, PR, Brazil. [Vreven, Emmanuel] Royal Museum Cent Africa, Vertebrate Sect, B-3080 Tervuren, Belgium. [Vreven, Emmanuel] Katholieke Univ Leuven, Lab Biodivers & Evolutionary Genom, B-3000 Louvain, Belgium. RP Jerep, FC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. EM fierep@gmail.com; varir@si.edu; emmanuel.vreven@africamuseum.be RI Jerep, Fernando/F-5274-2015 FU National Museum of Natural History; Smithsonian Institution; Herbert R. and Evelyn Axelrod Chair in the Division of Fishes, National Museum of Natural History FX We thank M. Stiassny and B. Brown (AMNH), J. Maclaine and O. Crimmen (BMNH), J. Friel (CUMV), M. Parrent (MRAC) and D. Neumann (ZSM) for assistance during visits to their institutions and/or loan of specimens. For assistance at USNM we thank S. Raredon who prepared Figure 1, J. Clayton and L. Palmer. This project was funded and supported by the National Museum of Natural History, Smithsonian Institution and the Herbert R. and Evelyn Axelrod Chair in the Division of Fishes, National Museum of Natural History. NR 20 TC 0 Z9 0 U1 0 U2 3 PU VERLAG DR FRIEDRICH PFEIL PI MUNICH PA WOLFRATSHAUSER STRASSE 27, MUNICH, D-81379, GERMANY SN 0936-9902 J9 ICHTHYOL EXPLOR FRES JI Ichthyol. Explor. Freshw. PD APR PY 2014 VL 24 IS 4 BP 361 EP 369 PG 9 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA AF7ND UT WOS:000334900900006 ER PT J AU Agarwal, N Ho, S Myers, AD Seo, HJ Ross, AJ Bahcall, N Brinkmann, J Eisenstein, DJ Muna, D Palanque-Delabrouille, N Paris, I Petitjean, P Schneider, DP Streblyanska, A Weaver, BA Yeche, C AF Agarwal, Nishant Ho, Shirley Myers, Adam D. Seo, Hee-Jong Ross, Ashley J. Bahcall, Neta Brinkmann, Jonathan Eisenstein, Daniel J. Muna, Demitri Palanque-Delabrouille, Nathalie Paris, Isabelle Petitjean, Patrick Schneider, Donald P. Streblyanska, Alina Weaver, Benjamin A. Yeche, Christophe TI Characterizing unknown systematics in large scale structure surveys SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE power spectrum; redshift surveys; cosmological parameters from LSS; galaxy surveys ID DIGITAL SKY SURVEY; PRIMORDIAL NON-GAUSSIANITY; WEAK-LENSING SURVEYS; MICROWAVE BACKGROUND ANISOTROPIES; OSCILLATION SPECTROSCOPIC SURVEY; GALAXY POWER SPECTRUM; SDSS-III; DATA RELEASE; BARYON OSCILLATIONS; REDSHIFT SURVEYS AB Photometric large scale structure (LSS) surveys probe the largest volumes in the Universe, but are inevitably limited by systematic uncertainties. Imperfect photometric calibration leads to biases in our measurements of the density fields of LSS tracers such as galaxies and quasars, and as a result in cosmological parameter estimation. Earlier studies have proposed using cross-correlations between different redshift slices or cross-correlations between different surveys to reduce the effects of such systematics. In this paper we develop a method to characterize unknown systematics. We demonstrate that while we do not have sufficient information to correct for unknown systematics in the data, we can obtain an estimate of their magnitude. We define a parameter to estimate contamination from unknown systematics using cross-correlations between different redshift slices and propose discarding bins in the angular power spectrum that lie outside a certain contamination tolerance level. We show that this method improves estimates of the bias using simulated data and further apply it to photometric luminous red galaxies in the Sloan Digital Sky Survey as a case study. C1 [Agarwal, Nishant; Ho, Shirley] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Seo, Hee-Jong] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA. [Seo, Hee-Jong] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Ross, Ashley J.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Bahcall, Neta] Princeton Univ Observ, Princeton, NJ 08544 USA. [Brinkmann, Jonathan] Apache Point Observ, Sunspot, NM 88349 USA. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Muna, Demitri] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Palanque-Delabrouille, Nathalie; Yeche, Christophe] CEA, Ctr Saclay, Irfu SPP, F-91191 Gif Sur Yvette, France. [Paris, Isabelle] Univ Chile, Dept Astron, Santiago, Chile. [Petitjean, Patrick] Univ Paris 06, F-75014 Paris, France. [Petitjean, Patrick] CNRS, Inst Astrophys Paris, F-75014 Paris, France. [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. [Streblyanska, Alina] IAC, E-38200 Tenerife, Spain. [Streblyanska, Alina] ULL, Dept Astrofis, E-38200 Tenerife, Spain. [Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. RP Agarwal, N (reprint author), Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. EM nishanta@andrew.cmu.edu RI Ho, Shirley/P-3682-2014 OI Ho, Shirley/0000-0002-1068-160X FU McWilliams fellowship of the Bruce; Astrid McWilliams Center for Cosmology; New Frontiers in Astronomy and Cosmology program at the John Templeton Foundation; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX It is a pleasure to thank Dragan Huterer and AnZe Slosar for many useful comments on this paper. We also thank Rachel Mandelbaum, Hiranya Peiris, Anthony Pullen, and Uros Seljak for helpful discussions. N. A. is supported by the McWilliams fellowship of the Bruce and Astrid McWilliams Center for Cosmology. N. A. also acknowledges support by the New Frontiers in Astronomy and Cosmology program at the John Templeton Foundation.; 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 74 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD APR PY 2014 IS 4 AR 007 DI 10.1088/1475-7516/2014/04/007 PG 24 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AF1TK UT WOS:000334496500007 ER PT J AU de Oliveira, AA Vicentini, A Chave, J Castanho, CD Davies, SJ Martini, AMZ Lima, RAF Ribeiro, RR Iribar, A Souza, VC AF de Oliveira, Alexandre A. Vicentini, Alberto Chave, Jerome Castanho, Camila de T. Davies, Stuart J. Martini, Adriana M. Z. Lima, Renato A. F. Ribeiro, Ricardo R. Iribar, Amaia Souza, Vinicius C. TI Habitat specialization and phylogenetic structure of tree species in a coastal Brazilian white-sand forest SO JOURNAL OF PLANT ECOLOGY LA English DT Article DE habitat association; torus-translation test; phylogenetic community structure; niche partitioning; edaphic condition ID RAIN-FOREST; PLANT-COMMUNITIES; ECOLOGICAL COMMUNITIES; LIMITING SIMILARITY; DIPTEROCARP FOREST; FUNCTIONAL TRAITS; AMAZONIAN FOREST; TROPICAL TREES; DNA BARCODES; NICHE AB Aims The coastal Brazilian rainforest on white-sand (restinga) ranks among the most fragmented forest types in the tropics, owing to both the patchy distribution of sandy soils and widespread coastal development activities. Here we study the environmental and evolutionary determinants of a forest tree assemblage at a single restinga forest in Southeastern Brazil. We also explore the ability of competing hypotheses to explain the maintenance of species diversity in this forest type, which includes contrasting extremes of edaphic conditions associated with flooding stress. Methods The study was conducted in a white-sand forest permanent plot of 10.24 ha on the coastal plain of Southeastern Brazil. This plot was divided into 256 quadrats of 20 x 20 m, which were classified into two main edaphic habitats (flooded and drained). Trees with a diameter >= 1 cm at breast height were identified. We assembled DNA sequence data for each of the 116 morphospecies recognized using two chloroplast markers (rbcL and matK). A phylogenetic tree was obtained using the maximum likelihood method, and a phylogenetic distance matrix was produced from an ultra-metric tree. We analyzed similarity in floristic composition and structure between habitats and related them to cross-plot distances using permutation procedures. Null model torus shift simulations were performed to obtain a statistical significance level for habitat association for each species. The phylogenetic structure for the two habitats and for each 20 x 20 m quadrat was calculated using the mean phylogenetic distance weighted by species abundance and checked for significance using the standardized effect size generated by 5000 randomizations of phylogenetic tip labels. Important Findings Our results indicate that partitioning among edaphic habitats is important for explaining species distributions and coexistence in restinga forests. Species distributions within the plot were found to be non-random: there was greater floristic similarity within than between habitats, and >40% of the more abundant species were positively or negatively associated with at least one habitat. Patterns of habitat association were not independent of phylogenetic relatedness: the community was overdispersed with respect to space and habitat type. Closely related species tended to occur in different habitats, while neighboring trees tended to belong to more distantly related species. We conclude that habitat specialization is important for the coexistence of species in restinga forests and that habitat heterogeneity is therefore an essential factor in explaining the maintenance of diversity of this unique but fragile and threatened type of forest. C1 [de Oliveira, Alexandre A.; Castanho, Camila de T.; Martini, Adriana M. Z.; Lima, Renato A. F.] Univ Sao Paulo, Inst Biociencias, BR-0550890 Sao Paulo, Brazil. [Vicentini, Alberto] Inst Nacl de Pesquisas da Amazonia, BR-69060001 Manaus, Amazonas, Brazil. [Chave, Jerome; Iribar, Amaia] Univ Toulouse 3, F-31062 Toulouse, France. [Davies, Stuart J.] Smithsonian Trop Res Inst, Washington, DC 20013 USA. [Ribeiro, Ricardo R.; Souza, Vinicius C.] Univ Sao Paulo, ESALQ, BR-13418900 Piracicaba, SP, Brazil. RP de Oliveira, AA (reprint author), Univ Sao Paulo, Inst Biociencias, Rua Matao,321,Travessa 14, BR-0550890 Sao Paulo, Brazil. EM adalardo@usp.br RI Lima, Renato/C-6744-2013; Rodrigues, Ricardo/D-5557-2012; Castanho, Camila/D-4583-2012; OI Oliveira, Alexandre/0000-0001-5526-8109 FU Petrobras; Center for Tropical Forest Science; State of Sao Paulo Research Foundation; Fondation pour la Recherche sur la Biodiversite; Centre National de la Recherche Scientifique; French Investissements d'Avenir funds [ANR-10-LABX-0025, ANR-10-LABX-0041] FX Petrobras, Center for Tropical Forest Science, The State of Sao Paulo Research Foundation, Fondation pour la Recherche sur la Biodiversite, Centre National de la Recherche Scientifique, French Investissements d'Avenir funds managed by Agence Nationale pour la Recherche (CEBA; ANR-10-LABX-0025, and TULIP; ANR-10-LABX-0041). NR 72 TC 4 Z9 4 U1 4 U2 45 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1752-9921 EI 1752-993X J9 J PLANT ECOL JI J. Plant Ecol. PD APR PY 2014 VL 7 IS 2 SI SI BP 134 EP 144 DI 10.1093/jpe/rtt073 PG 11 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA AF7XL UT WOS:000334928700005 ER PT J AU Carrillo-Briceno, JD Aguilera, OA Rodriguez, F AF Carrillo-Briceno, Jorge D. Aguilera, Orange A. Rodriguez, Felix TI Fossil Chondrichthyes from the central eastern Pacific Ocean and their paleoceanographic significance SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Neogene; Tropical America; Ecuador; Sharks; Rays; Paleoenviroments ID UPPER ONZOLE FORMATION; SEQUENCE STRATIGRAPHY; NORTHWESTERN ECUADOR; FRILLED SHARK; MIOCENE; PLIOCENE; ELASMOBRANCHII; NEOGENE; BASIN; FISHES AB The study of the chondrichthyan fauna from the Angostura, Onzole, Canoa and Jama formations, in the Neogene of Bordon and Manabi basins, Ecuador, reveals the presence of 30 taxa, including the deep water shark dagger Chlamydoselachus landinii sp. nov. The assemblages are dominated by tropical shallow and deep water chondrichthyans, suggesting paleoenvironments associated with a short platform shelf bordering a deep margin. These assemblages are the most diverse shark and ray association known from the Tropical Central Eastern Pacific Ocean in the South American coastal basin, and provide new information on the paleoecology and paleodiversity of Neogene chondrichthyans. (c) 2014 Elsevier Ltd. All rights reserved. C1 [Carrillo-Briceno, Jorge D.] Univ Zurich, Paleontol Inst & Museum, CH-8006 Zurich, Switzerland. [Aguilera, Orange A.] Univ Fed Fluminense, Inst Biol, Dept Biol Marinha, Programa Posgrad Biol Marinha, BR-2402014 Niteroi, RJ, Brazil. [Rodriguez, Felix] Smithsonian Trop Res Inst, Balboa, Panama. RP Carrillo-Briceno, JD (reprint author), Univ Zurich, Paleontol Inst & Museum, Karl Schmid Str 4, CH-8006 Zurich, Switzerland. EM Jorge.carrillo@pim.uxh.ch; orangel.aguilera@gmail.com; RodriguezF@si.edu OI Carrillo Briceno, Jorge Domingo/0000-0002-8652-7692 NR 153 TC 7 Z9 9 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD APR PY 2014 VL 51 BP 76 EP 90 DI 10.1016/j.jsames.2014.01.001 PG 15 WC Geosciences, Multidisciplinary SC Geology GA AF1PL UT WOS:000334485700006 ER PT J AU Kuznetsova, E Liu, GY Malinovskaya, SA AF Kuznetsova, Elena Liu, Gengyuan Malinovskaya, Svetlana A. TI Adiabatic rapid passage two-photon excitation of a Rydberg atom SO PHYSICA SCRIPTA LA English DT Article; Proceedings Paper CT 20th Central European Workshop on Quantum Optics CY JUN 16-20, 2013 CL Stockholm, SWEDEN DE Rydberg atoms; dipole blockade; chirped pulses AB We considered the two-photon adiabatic rapid passage excitation of a single atom from the ground to a Rydberg state. Three schemes were analyzed: both pump and Stokes fields chirped and pulsed, only the pump field chirped, and only the pump field pulsed and chirped while the Stokes field is continuous wave (CW). In all three cases high transfer efficiencies >99% were achieved for the experimentally realizable Rabi frequencies and the pulse durations of the fields. C1 [Kuznetsova, Elena] Russian Quantum Ctr, Skolkovo 143025, Russia. [Kuznetsova, Elena] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Liu, Gengyuan; Malinovskaya, Svetlana A.] Stevens Inst Technol, Dept Phys & Engn Phys, Hoboken, NJ 07030 USA. RP Kuznetsova, E (reprint author), Russian Quantum Ctr, Skolkovo 143025, Russia. EM smalinov@stevens.edu OI Malinovskaya, Svetlana/0000-0003-4125-3947 FU NSF [PHY-1205454]; Russian Quantum Center FX This work was supported by an NSF grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics, NSF Grant No. PHY-1205454 and the Russian Quantum Center. NR 14 TC 3 Z9 3 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0031-8949 EI 1402-4896 J9 PHYS SCRIPTA JI Phys. Scr. PD APR PY 2014 VL T160 AR 014024 DI 10.1088/0031-8949/2014/T160/014024 PG 4 WC Physics, Multidisciplinary SC Physics GA AG2CY UT WOS:000335224700025 ER PT J AU Olson, SL AF Olson, Storrs L. TI The early scientific history of Galapagos iguanas SO ARCHIVES OF NATURAL HISTORY LA English DT Article DE Andrew Bloxam; John Scouler; David Douglas; HMS Beagle; James McRae; Conolophus; HMS Blonde; Charles Darwin; Amblyrhynchus ID ARCHIPELAGO AB The oldest known specimen of Galapagos marine iguana (Amblyrhynchus cristatus), now in the University Museum, Oxford, was originally thought to have come from Mexico. A plausible history of its origin with sealers in the Galapagos Islands about 1824 and transportation to and across Mexico is advanced. The naturalists David Douglas and John Scouler, on James (Santiago) Island in January 1825, encountered and attempted unsuccessfully to preserve specimens of the land iguana (Conolophus subcristatus) but only a Scouler specimen of marine iguana made it back to England, and it has since disappeared. Published and previously unpublished journal entries from the voyage of HMS Blonde, which had shore parties at Albemarle (Isabela) and Narborough (Fernandina) islands in March 1825, establish that the specimens on which the original description of Amblyrhynchus (later Conolophus) subcristatus J. E. Gray, 1831, was based originated in the voyage of the Blonde. Banks Bay, Albemarle Island, is here designated as the type locality for Conolophus subcristatus. Specimens of the marine iguana were also brought back by the Blonde. The published accounts of Scouler and the voyage of the Blonde established the Galapagos as the true home of the marine iguana well before the return of Charles Darwin and HMS Beagle in 1836. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Div Birds,NHB MRC 116, Washington, DC 20013 USA. RP Olson, SL (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Div Birds,NHB MRC 116, POB 37012, Washington, DC 20013 USA. NR 36 TC 0 Z9 0 U1 2 U2 21 PU EDINBURGH UNIV PRESS PI EDINBURGH PA THE TUN-HOLYROOD RD, 12 2F JACKSONS ENTRY, EDINBURGH EH8 8PJ, ENGLAND SN 0260-9541 EI 1755-6260 J9 ARCH NAT HIST JI Arch. Nat. Hist. PD APR PY 2014 VL 41 IS 1 BP 141 EP 153 DI 10.3366/anh.2014.0217 PG 13 WC History & Philosophy Of Science; Multidisciplinary Sciences SC History & Philosophy of Science; Science & Technology - Other Topics GA AE0EK UT WOS:000333636200012 ER PT J AU Ahn, CP Alexandroff, R Prieto, CA Anders, F Anderson, SF Anderton, T Andrews, BH Aubourg, E Bailey, S Bastien, FA Bautista, JE Beers, TC Beifiori, A Bender, CF Berlind, AA Beutler, F Bhardwaj, V Bird, JC Bizyaev, D Blake, CH Blanton, MR Blomqvist, M Bochanski, JJ Bolton, AS Borde, A Bovy, J Bradley, AS Brandt, WN Brauer, D Brinkmann, J Brownstein, JR Busca, NG Carithers, W Carlberg, JK Carnero, AR Carr, MA Chiappini, C Chojnowski, SD Chuang, CH Comparat, J Crepp, JR Cristiani, S Croft, RAC Cuesta, AJ Cunha, K da Costa, LN Dawson, KS De Lee, N Dean, JDR Delubac, T Deshpande, R Dhital, S Ealet, A Ebelke, GL Edmondson, EM Eisenstein, DJ Epstein, CR Escoffier, S Esposito, M Evans, ML Fabbian, D Fan, XH Favole, G Castella, BF Alvar, EF Feuillet, D Ak, NF Finley, H Fleming, SW Font-Ribera, A Frinchaboy, PM Galbraith-Frew, JG Garcia-Hernandez, DA Perez, AEG Ge, J Genova-Santos, R Gillespie, BA Girardi, L Hernandez, JIG Gott, JR Gunn, JE Guo, H Halverson, S Harding, P Harris, D Hasselquist, S Hawley, SL Hayden, M Hearty, FR Davo, AH Ho, S Hogg, DW Holtzman, JA Honscheid, K Huehnerhoff, J Ivans, II Jackson, KM Jiang, P Johnson, JA Kinemuchi, K Kirkby, D Klaene, MA Kneib, JP Koesterke, L Lan, TW Lang, D Le Goff, JM Leauthaud, A Lee, KG Lee, YS Long, DC Loomis, CP Lucatello, S Lupton, RH Ma, B Mack, CE Mahadevan, S Maia, MAG Majewski, SR Malanushenko, E Malanushenko, V Manchado, A Manera, M Maraston, C Margala, D Martell, SL Masters, KL McBride, CK McGreer, ID McMahon, RG Menard, B Meszaros, S Miralda-Escude, J Miyatake, H Montero-Dorta, AD Montesano, F More, S Morrison, HL Muna, D Munn, JA Myers, AD Nguyen, DC Nichol, RC Nidever, DL Noterdaeme, P Nuza, SE O'Connell, JE O'Connell, RW O'Connell, R Olmstead, MD Oravetz, DJ Owen, R Padmanabhan, N Palanque-Delabrouille, N Pan, K Parejko, JK Parihar, P Paris, I Pepper, J Percival, WJ Perez-Rafols, I Perottoni, HD Petitjean, P Pieri, MM Pinsonneault, MH Prada, F Price-Whelan, AM Raddick, MJ Rahman, M Rebolo, R Reid, BA Richards, JC Riffel, R Robin, AC Rocha-Pinto, HJ Rockosi, CM Roe, NA Ross, AJ Ross, NP Rossi, G Roy, A Rubino-Martin, JA Sabiu, CG Sanchez, AG Santiago, B Sayres, C Schiavon, RP Schlegel, DJ Schlesinger, KJ Schmidt, SJ Schneider, DP Schultheis, M Sellgren, K Seo, HJ Shen, Y Shetrone, M Shu, YP Simmons, AE Skrutskie, MF Slosar, A Smith, VV Snedden, SA Sobeck, JS Sobreira, F Stassun, KG Steinmetz, M Strauss, MA Streblyanska, A Suzuki, N Swanson, MEC Terrien, RC Thakar, AR Thomas, D Thompson, BA Tinker, JL Tojeiro, R Troup, NW Vandenberg, J Magana, MV Viel, M Vogt, NP Wake, DA Weaver, BA Weinberg, DH Weiner, BJ White, M White, SDM Wilson, JC Wisniewski, JP Wood-Vasey, WM Yeche, C York, DG Zamora, O Zasowski, G Zehavi, I Zhao, GB Zheng, Z Zhu, GT AF Ahn, Christopher P. Alexandroff, Rachael Allende Prieto, Carlos Anders, Friedrich Anderson, Scott F. Anderton, Timothy Andrews, Brett H. Aubourg, Eric Bailey, Stephen Bastien, Fabienne A. Bautista, Julian E. Beers, Timothy C. Beifiori, Alessandra Bender, Chad F. Berlind, Andreas A. Beutler, Florian Bhardwaj, Vaishali Bird, Jonathan C. Bizyaev, Dmitry Blake, Cullen H. Blanton, Michael R. Blomqvist, Michael Bochanski, John J. Bolton, Adam S. Borde, Arnaud Bovy, Jo Bradley, Alaina Shelden Brandt, W. N. Brauer, Dorothee Brinkmann, J. Brownstein, Joel R. Busca, Nicolas G. Carithers, William Carlberg, Joleen K. Carnero, Aurelio R. Carr, Michael A. Chiappini, Cristina Chojnowski, S. Drew Chuang, Chia-Hsun Comparat, Johan Crepp, Justin R. Cristiani, Stefano Croft, Rupert A. C. Cuesta, Antonio J. Cunha, Katia da Costa, Luiz N. Dawson, Kyle S. De Lee, Nathan Dean, Janice D. R. Delubac, Timothee Deshpande, Rohit Dhital, Saurav Ealet, Anne Ebelke, Garrett L. Edmondson, Edward M. Eisenstein, Daniel J. Epstein, Courtney R. Escoffier, Stephanie Esposito, Massimiliano Evans, Michael L. Fabbian, D. Fan, Xiaohui Favole, Ginevra Femenia Castella, Bruno Fernandez Alvar, Emma Feuillet, Diane Ak, Nurten Filiz Finley, Hayley Fleming, Scott W. Font-Ribera, Andreu Frinchaboy, Peter M. Galbraith-Frew, J. G. Garcia-Hernandez, D. A. Perez, Ana E. Garcia Ge, Jian Genova-Santos, R. Gillespie, Bruce A. Girardi, Leo Gonzalez Hernandez, Jonay I. Gott, J. Richard, III Gunn, James E. Guo, Hong Halverson, Samuel Harding, Paul Harris, DavidW. Hasselquist, Sten Hawley, Suzanne L. Hayden, Michael Hearty, Frederick R. Herrero Davo, Artemio Ho, Shirley Hogg, David W. Holtzman, Jon A. Honscheid, Klaus Huehnerhoff, Joseph Ivans, Inese I. Jackson, Kelly M. Jiang, Peng Johnson, Jennifer A. Kinemuchi, K. Kirkby, David Klaene, Mark A. Kneib, Jean-Paul Koesterke, Lars Lan, Ting-Wen Lang, Dustin Le Goff, Jean-Marc Leauthaud, Alexie Lee, Khee-Gan Lee, Young Sun Long, Daniel C. Loomis, Craig P. Lucatello, Sara Lupton, Robert H. Ma, Bo Mack, Claude E., III Mahadevan, Suvrath Maia, Marcio A. G. Majewski, Steven R. Malanushenko, Elena Malanushenko, Viktor Manchado, A. Manera, Marc Maraston, Claudia Margala, Daniel Martell, Sarah L. Masters, Karen L. McBride, Cameron K. McGreer, Ian D. McMahon, Richard G. Menard, Brice Meszaros, Sz. Miralda-Escude, Jordi Miyatake, Hironao Montero-Dorta, Antonio D. Montesano, Francesco More, Surhud Morrison, Heather L. Muna, Demitri Munn, Jeffrey A. Myers, Adam D. Duy Cuong Nguyen Nichol, Robert C. Nidever, David L. Noterdaeme, Pasquier Nuza, Sebastian E. O'Connell, Julia E. O'Connell, Robert W. O'Connell, Ross Olmstead, Matthew D. Oravetz, Daniel J. Owen, Russell Padmanabhan, Nikhil Palanque-Delabrouille, Nathalie Pan, Kaike Parejko, John K. Parihar, Prachi Paris, Isabelle Pepper, Joshua Percival, Will J. Perez-Rafols, Ignasi Perottoni, Helio Dotto Petitjean, Patrick Pieri, Matthew M. Pinsonneault, M. H. Prada, Francisco Price-Whelan, Adrian M. Raddick, M. Jordan Rahman, Mubdi Rebolo, Rafael Reid, Beth A. Richards, Jonathan C. Riffel, Rogerio Robin, Annie C. Rocha-Pinto, H. J. Rockosi, Constance M. Roe, Natalie A. Ross, Ashley J. Ross, Nicholas P. Rossi, Graziano Roy, Arpita Rubino-Martin, J. A. Sabiu, Cristiano G. Sanchez, Ariel G. Santiago, Basilio Sayres, Conor Schiavon, Ricardo P. Schlegel, David J. Schlesinger, Katharine J. Schmidt, Sarah J. Schneider, Donald P. Schultheis, Mathias Sellgren, Kris Seo, Hee-Jong Shen, Yue Shetrone, Matthew Shu, Yiping Simmons, Audrey E. Skrutskie, M. F. Slosar, Anze Smith, Verne V. Snedden, Stephanie A. Sobeck, Jennifer S. Sobreira, Flavia Stassun, Keivan G. Steinmetz, Matthias Strauss, Michael A. Streblyanska, Alina Suzuki, Nao Swanson, Molly E. C. Terrien, Ryan C. Thakar, Aniruddha R. Thomas, Daniel Thompson, Benjamin A. Tinker, Jeremy L. Tojeiro, Rita Troup, Nicholas W. Vandenberg, Jan Magana, Mariana Vargas Viel, Matteo Vogt, Nicole P. Wake, David A. Weaver, Benjamin A. Weinberg, David H. Weiner, Benjamin J. White, Martin White, Simon D. M. Wilson, John C. Wisniewski, John P. Wood-Vasey, W. M. Yeche, Christophe York, Donald G. Zamora, O. Zasowski, Gail Zehavi, Idit Zhao, Gong-Bo Zheng, Zheng Zhu, Guangtun TI THE TENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST SPECTROSCOPIC DATA FROM THE SDSS-III APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atlases; catalogs; surveys ID BARYON ACOUSTIC-OSCILLATIONS; STELLAR POPULATION SYNTHESIS; INITIAL MASS FUNCTION; 7TH DATA RELEASE; 9TH DATA RELEASE; TARGET SELECTION; GALAXY SAMPLE; MILKY-WAY; MORPHOLOGICAL CLASSIFICATIONS; PHOTOMETRIC SYSTEM AB The Sloan Digital Sky Survey (SDSS) has been in operation since 2000 April. This paper presents the Tenth Public Data Release (DR10) from its current incarnation, SDSS-III. This data release includes the first spectroscopic data from the Apache Point Observatory Galaxy Evolution Experiment (APOGEE), along with spectroscopic data from the Baryon Oscillation Spectroscopic Survey (BOSS) taken through 2012 July. The APOGEE instrument is a near-infrared R similar to 22,500 300 fiber spectrograph covering 1.514-1.696 mu m. The APOGEE survey is studying the chemical abundances and radial velocities of roughly 100,000 red giant star candidates in the bulge, bar, disk, and halo of the Milky Way. DR10 includes 178,397 spectra of 57,454 stars, each typically observed three or more times, from APOGEE. Derived quantities from these spectra (radial velocities, effective temperatures, surface gravities, and metallicities) are also included. DR10 also roughly doubles the number of BOSS spectra over those included in the Ninth Data Release. 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[Sobeck, Jennifer S.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Sobeck, Jennifer S.] Univ Chicago, JINA, Chicago, IL 60637 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Wake, David A.] Univ Wisconsin, Dept Astron, Madison, WI 53703 USA. [White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [White, Simon D. M.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, PITT PACC, Pittsburgh, PA 15260 USA. [York, Donald G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [York, Donald G.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Zhao, Gong-Bo] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RP Strauss, MA (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RI EPFL, Physics/O-6514-2016; Riffel, Rogerio/I-5787-2013; Rocha-Pinto, Helio/C-2719-2008; Meszaros, Szabolcs/N-2287-2014; Sobreira, Flavia/F-4168-2015; Croft, Rupert/N-8707-2014; More, Surhud/A-5049-2013; Zamora, Olga/M-1776-2014; Filiz Ak, Nurten/C-9686-2015; Kneib, Jean-Paul/A-7919-2015; Guo, Hong/J-5797-2015; White, Martin/I-3880-2015; Brandt, William/N-2844-2015 OI Schmidt, Sarah/0000-0002-7224-7702; Finley, Hayley/0000-0002-1216-8914; Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470; Fabbian, Damian/0000-0002-0347-9243; Bovy, Jo/0000-0001-6855-442X; Roy, Arpita/0000-0001-8127-5775; McMahon, Richard/0000-0001-8447-8869; Hogg, David/0000-0003-2866-9403; Pepper, Joshua/0000-0002-3827-8417; Cristiani, Stefano/0000-0002-2115-5234; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Rahman, Mubdi/0000-0003-1842-6096; Escoffier, Stephanie/0000-0002-2847-7498; Kirkby, David/0000-0002-8828-5463; Fleming, Scott/0000-0003-0556-027X; Viel, Matteo/0000-0002-2642-5707; Zhu, Guangtun/0000-0002-7574-8078; Beutler, Florian/0000-0003-0467-5438; Riffel, Rogerio/0000-0002-1321-1320; Meszaros, Szabolcs/0000-0001-8237-5209; Sobreira, Flavia/0000-0002-7822-0658; Croft, Rupert/0000-0003-0697-2583; More, Surhud/0000-0002-2986-2371; Zamora, Olga/0000-0003-2100-1638; Filiz Ak, Nurten/0000-0003-3016-5490; Kneib, Jean-Paul/0000-0002-4616-4989; Guo, Hong/0000-0003-4936-8247; White, Martin/0000-0001-9912-5070; Brandt, William/0000-0002-0167-2453 FU National Aeronautics and Space Administration; National Science Foundation; Alfred P. Sloan Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; 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 SDSS-III DR10 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.; SDSS-III DR10 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 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, 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 74 TC 443 Z9 448 U1 9 U2 75 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2014 VL 211 IS 2 AR 17 DI 10.1088/0067-0049/211/2/17 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE5KT UT WOS:000334028600001 ER PT J AU Ebeling, H Ma, CJ Barrett, E AF Ebeling, Harald Ma, Cheng-Jiun Barrett, Elizabeth TI SPECTROSCOPIC REDSHIFTS OF GALAXIES WITHIN THE FRONTIER FIELDS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: clusters: individual (MACSJ0416.1-2403, MACSJ0717.5+3745 MACSJ1149.5+2223); galaxies: distances and redshifts ID CLUSTER MACS J0717.5+3745; ABELL 2744; DISTANT; MERGERS; Z=0.31 AB We present a catalog of 1921 spectroscopic redshifts measured in the fields of the massive galaxy clusters MACSJ0416.1-2403 (z = 0.397), MACSJ0717.5+3745 (z = 0.546), and MACSJ1149.5+2223 (z = 0.544), i.e., three of the four clusters selected by Space Telescope Science Institute as the targets of the Frontier Fields (FFs) initiative for studies of the distant Universe via gravitational lensing. Compiled in the course of the Massive Cluster Survey project (MACS) that detected the FF clusters, this catalog is provided to the community for three purposes: (1) to allow the identification of cluster members for studies of the galaxy population of these extreme systems, (2) to facilitate the removal of unlensed galaxies and thus reduce shear dilution in weak-lensing analyses, and (3) to improve the calibration of photometric redshifts based on both ground-and spacebased observations of the FF clusters. C1 [Ebeling, Harald; Ma, Cheng-Jiun; Barrett, Elizabeth] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Ma, Cheng-Jiun] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Ma, Cheng-Jiun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Ma, Cheng-Jiun] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. RP Ebeling, H (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. FU STScI [GO-9722, GO-10420] FX H.E. gratefully acknowledges financial support from STScI grants GO-9722 and GO-10420. The HST images of the FF shown in Figures 1 and 2 were reduced and kindly made available by Anton Koekemoer. NR 20 TC 20 Z9 20 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2014 VL 211 IS 2 AR 21 DI 10.1088/0067-0049/211/2/21 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE5KT UT WOS:000334028600005 ER PT J AU Pukazhenthi, BS Johnson, A Guthrie, HD Songsasen, N Padilla, LR Wolfe, BA da Silva, MC Alvarenga, MA Wildt, DE AF Pukazhenthi, Budhan S. Johnson, Aime Guthrie, H. David Songsasen, Nucharin Padilla, Luis R. Wolfe, Barbara A. da Silva, Marco Coutinho Alvarenga, Marco A. Wildt, David E. TI Improved sperm cryosurvival in diluents containing amides versus glycerol in the Przewalski's. horse (Equus ferus przewalskii) SO CRYOBIOLOGY LA English DT Article DE Equid; Spermatozoa; Semen; Cryoprotectant; Freezing; Mitochondria ID PHASCOLARCTOS-CINEREUS SPERMATOZOA; STALLION SPERMATOZOA; FROZEN-SEMEN; MITOCHONDRIAL-FUNCTION; COLLECTION TECHNIQUES; MEMBRANE INTEGRITY; RABBIT SPERMATOZOA; FLOW-CYTOMETRY; CRYOPRESERVATION; CRYOPROTECTANTS AB Two studies were conducted to understand sperm cryosensitivity in an endangered equid, the Przewalski's horse (Equus ferns przewalski), while testing the cryoprotectant ability of formamides. The first assessed the toxicity of permeating cryoprotectants (glycerol, methylformamide IMF] and dimethylformamide [DMF]) to Przewalski's horse spermatozoa during liquid storage at 4 C. The second examined the comparative influence of three diluents (with or without formamides) on cryosurvival of sperm from the Przewalski's versus domestic horse. When Przewalski's horse spermatozoa were incubated at 4 C in INRA 96 with differing concentrations of glycerol, MF or DMF or a combination of these amides, cells tolerated all but the highest concentration (10% v/v) of MF alone or in combination with DMF, both of which decreased (P < 0.05) motility traits. There was no effect of cryoprotectants on sperm acrosomal integrity. In the cryosurvival study, average sperm motility and proportion of cells with intact acrosomes in fresh ejaculates were similar (P> 0.05) between the Przewalski's (67%, 84%, respectively) and domestic (66%, 76%) horse donors. Sperm from both species were diluted in lactose-EDTA-glycerol (EQ), Botu-Crio (BOTU; a proprietary product containing glycerol and MF) or SM (INRA 96 plus 2% [v/v] egg yolk and 2.5% [v/v] MF and DMF) and then frozen over liquid nitrogen vapor. After thawing, the highest values recovered for total and progressive sperm motility, acrosomal integrity and mitochondria] membrane potential were 42.4%, 21.8%, 88.7% and 25.4 CN (CN = mean JC-1 fluorescence intensity/cell on a channel number scale), respectively, in the Przewalski's and 49.3%, 24.6%, 88.9% and 25.8 CN, respectively, in the domestic horse. Although sperm progressive motility and acrosome integrity did not differ (P> 0.05) among treatments across species, mitochondrial membrane potential was higher (P< 0.05) in both species using EQ compared to BOTU or SM media. Additionally, Przewalski's stallion sperm expressed higher (P < 0.05) post-thaw total motility in BOTU and SM compared to EQ whereas there were no differences among freezing diluents in the domestic horse. In summary, Przewalski's stallion sperm benefit from exposure to either MF or DMF as an alternative cryoprotectant to glycerol. Overt sperm quality appears similar between the Przewalski's and domestic horse, although the total motility of cells from the former appears more sensitive to certain freezing diluents. Nonetheless, post-thaw motility and acrosomal integrity values for Przewalski's horse spermatozoa mimic findings in the domestic horse in the presence of INRA 96 supplemented with 2% (v/v) egg yolk and a combined 2.5% concentration of MF and DMF. Published by Elsevier Inc. C1 [Pukazhenthi, Budhan S.; Songsasen, Nucharin; Padilla, Luis R.; Wildt, David E.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Johnson, Aime] Auburn Univ, Coll Vet Med, Dept Clin Sci, Auburn, AL 36849 USA. [Guthrie, H. David] ARS, Anim Biosci & Biotechnol Lab, USDA, Beltsville, MD 20705 USA. [Wolfe, Barbara A.] The Wilds, Cumberland, OH 43732 USA. [da Silva, Marco Coutinho] Ohio State Univ, Coll Vet Med, Dept Vet Clin Sci, Columbus, OH 43210 USA. [Alvarenga, Marco A.] Sao Paulo State Univ, UNESP, Sch Vet Med, Dept Anim Reprod & Vet Radiol, Sao Paulo, Brazil. RP Pukazhenthi, BS (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. EM pukazhenthib@si.edu; akj0001@auburn.edu; dave.guthrie@ars.usda.gov; songsasenn@si.edu; padilla@stlzoo.org; Barbara.wolfe@cvm.osu.edu; Marco.CoutinhoDaSilva@cvm.osu.edu; malvarenga@fmvz.unesp.br; wildtd@si.edu FU Sichel Endowment FX This work was supported by the Sichel Endowment. NR 63 TC 5 Z9 5 U1 2 U2 14 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0011-2240 EI 1090-2392 J9 CRYOBIOLOGY JI Cryobiology PD APR PY 2014 VL 68 IS 2 BP 205 EP 214 DI 10.1016/j.cryobio1.2014.01.013 PG 10 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA AE6ZG UT WOS:000334145900007 PM 24508651 ER PT J AU Fleischer, NL Merialdi, M van Donkelaar, A Vadillo-Ortega, F Martin, RV Betran, AP Souza, JP O'Neill, MS AF Fleischer, Nancy L. Merialdi, Mario van Donkelaar, Aaron Vadillo-Ortega, Felipe Martin, Randall V. Betran, Ana Pilar Souza, Joao Paulo O'Neill, Marie S. TI Outdoor Air Pollution, Preterm Birth, and Low Birth Weight: Analysis of the World Health Organization Global Survey on Maternal and Perinatal Health SO ENVIRONMENTAL HEALTH PERSPECTIVES LA English DT Article ID TIME-SERIES-ANALYSIS; LONG-TERM EXPOSURE; OF-THE-LITERATURE; PREGNANCY OUTCOMES; GROWTH-RETARDATION; CALIFORNIA; ENVIRONMENT; DISEASE; ANGELES; BRAZIL AB Background: Inhaling fine particles (particulate matter with diameter <= 2.5 mu m; PM2.5) can induce oxidative stress and inflammation, and may contribute to onset of preterm labor and other adverse perinatal outcomes. Objectives: We examined whether outdoor PM2.5 was associated with adverse birth outcomes among 22 countries in the World Health Organization Global Survey on Maternal and Perinatal Health from 2004 through 2008. Methods: Long-term average (2001-2006) estimates of outdoor PM2.5 were assigned to 50-km-radius circular buffers around each health clinic where births occurred. We used generalized estimating equations to determine associations between clinic-level PM2.5 levels and preterm birth and low birth weight at the individual level, adjusting for seasonality and potential confounders at individual, clinic, and country levels. Country-specific associations were also investigated. Results: Across all countries, adjusting for seasonality, PM2.5 was not associated with preterm birth, but was associated with low birth weight [ odds ratio (OR) = 1.22; 95% CI: 1.07, 1.39 for fourth quartile of PM2.5 (> 20.2 mu/m(3)) compared with the first quartile (< 6.3 mu g/m(3))]. In China, the country with the largest PM2.5 range, preterm birth and low birth weight both were associated with the highest quartile of PM2.5 only, which suggests a possible threshold effect (OR = 2.54; CI: 1.42, 4.55 and OR = 1.99; CI: 1.06, 3.72 for preterm birth and low birth weight, respectively, for PM2.5 = 36.5 mu g/m(3) compared with PM2.5 < 12.5 mu g/m(3)). Conclusions: Outdoor PM2.5 concentrations were associated with low birth weight but not preterm birth. In rapidly developing countries, such as China, the highest levels of air pollution may be of concern for both outcomes. C1 [Fleischer, Nancy L.] Univ S Carolina, Arnold Sch Publ Hlth, Columbia, SC 29208 USA. [Merialdi, Mario; Betran, Ana Pilar; Souza, Joao Paulo] WHO, Dept Reprod Hlth & Res, CH-1211 Geneva, Switzerland. [van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Vadillo-Ortega, Felipe] Univ Nacl Autonoma Mexico, Sch Med, Mexico City 04510, DF, Mexico. [Vadillo-Ortega, Felipe] Inst Nacl Med Genom, Mexico City, DF, Mexico. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [O'Neill, Marie S.] Univ Michigan, Sch Publ Hlth, Ann Arbor, MI 48109 USA. RP Fleischer, NL (reprint author), Univ S Carolina, Arnold Sch Publ Hlth, Dept Epidemiol & Biostat, 915 Greene St,4th Floor, Columbia, SC 29208 USA. EM nfleischer@sc.edu RI Souza, Joao Paulo/G-1982-2010; Martin, Randall/C-1205-2014 OI Souza, Joao Paulo/0000-0002-2288-4244; Martin, Randall/0000-0003-2632-8402 FU World Health Organization [200174365]; National Institute of Environmental Health Sciences, National Institutes of Health [ES016932, ES017022] FX Support for this work provided by the World Health Organization (contract 200174365) and R01 grants ES016932 and ES017022 from the National Institute of Environmental Health Sciences, National Institutes of Health. NR 49 TC 34 Z9 38 U1 4 U2 57 PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE PI RES TRIANGLE PK PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233, RES TRIANGLE PK, NC 27709-2233 USA SN 0091-6765 EI 1552-9924 J9 ENVIRON HEALTH PERSP JI Environ. Health Perspect. PD APR PY 2014 VL 122 IS 4 BP 425 EP 430 DI 10.1289/ehp.1306837 PG 6 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA AE5ZY UT WOS:000334069100028 PM 24508912 ER PT J AU Launius, RD AF Launius, Roger D. TI Inventing the American Astronaut SO HISTORICAL STUDIES IN THE NATURAL SCIENCES LA English DT Book Review C1 [Launius, Roger D.] Smithsonian Inst, Natl Air & Space Museum, Collect & Curatorial Affairs, Washington, DC 20013 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Collect & Curatorial Affairs, POB 37012,MRC 311, Washington, DC 20013 USA. EM launiusr@si.edu NR 1 TC 0 Z9 0 U1 1 U2 1 PU UNIV CALIFORNIA PRESS PI OAKLAND PA 155 GRAND AVE, SUITE 400, OAKLAND, CA 94612-3758 USA SN 1939-1811 EI 1939-182X J9 HIST STUD NAT SCI JI Hist. Stud. Nat. Sci. PD APR PY 2014 VL 44 IS 2 BP 187 EP 195 PG 9 WC History & Philosophy Of Science SC History & Philosophy of Science GA AE6HK UT WOS:000334091000006 ER PT J AU Launius, RD AF Launius, Roger D. TI Plane Queer: Labor, Sexuality, and AIDS in the History of Male Flight Attendants SO HISTORICAL STUDIES IN THE NATURAL SCIENCES LA English DT Book Review C1 [Launius, Roger D.] Smithsonian Inst, Natl Air & Space Museum, Collect & Curatorial Affairs, Washington, DC 20013 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Collect & Curatorial Affairs, POB 37012,MRC 311, Washington, DC 20013 USA. EM launiusr@si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIFORNIA PRESS PI OAKLAND PA 155 GRAND AVE, SUITE 400, OAKLAND, CA 94612-3758 USA SN 1939-1811 EI 1939-182X J9 HIST STUD NAT SCI JI Hist. Stud. Nat. Sci. PD APR PY 2014 VL 44 IS 2 BP 187 EP 195 PG 9 WC History & Philosophy Of Science SC History & Philosophy of Science GA AE6HK UT WOS:000334091000009 ER PT J AU Launius, RD AF Launius, Roger D. TI Imagining Outer Space: European Astroculture in the Twentieth Century SO HISTORICAL STUDIES IN THE NATURAL SCIENCES LA English DT Book Review C1 [Launius, Roger D.] Smithsonian Inst, Natl Air & Space Museum, Collect & Curatorial Affairs, Washington, DC 20013 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Collect & Curatorial Affairs, POB 37012,MRC 311, Washington, DC 20013 USA. EM launiusr@si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIFORNIA PRESS PI OAKLAND PA 155 GRAND AVE, SUITE 400, OAKLAND, CA 94612-3758 USA SN 1939-1811 EI 1939-182X J9 HIST STUD NAT SCI JI Hist. Stud. Nat. Sci. PD APR PY 2014 VL 44 IS 2 BP 187 EP 195 PG 9 WC History & Philosophy Of Science SC History & Philosophy of Science GA AE6HK UT WOS:000334091000005 ER PT J AU Launius, RD AF Launius, Roger D. TI Blue Sky Metropolis: The Aerospace Century in Southern California SO HISTORICAL STUDIES IN THE NATURAL SCIENCES LA English DT Book Review C1 [Launius, Roger D.] Smithsonian Inst, Natl Air & Space Museum, Collect & Curatorial Affairs, Washington, DC 20013 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Collect & Curatorial Affairs, POB 37012,MRC 311, Washington, DC 20013 USA. EM launiusr@si.edu NR 1 TC 0 Z9 0 U1 0 U2 3 PU UNIV CALIFORNIA PRESS PI OAKLAND PA 155 GRAND AVE, SUITE 400, OAKLAND, CA 94612-3758 USA SN 1939-1811 EI 1939-182X J9 HIST STUD NAT SCI JI Hist. Stud. Nat. Sci. PD APR PY 2014 VL 44 IS 2 BP 187 EP 195 PG 9 WC History & Philosophy Of Science SC History & Philosophy of Science GA AE6HK UT WOS:000334091000010 ER PT J AU Launius, RD AF Launius, Roger D. TI To Touch the Face of God: The Sacred, the Profane, and the American Space Program SO HISTORICAL STUDIES IN THE NATURAL SCIENCES LA English DT Book Review C1 [Launius, Roger D.] Smithsonian Inst, Natl Air & Space Museum, Collect & Curatorial Affairs, Washington, DC 20013 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Collect & Curatorial Affairs, POB 37012,MRC 311, Washington, DC 20013 USA. EM launiusr@si.edu NR 1 TC 0 Z9 0 U1 0 U2 1 PU UNIV CALIFORNIA PRESS PI OAKLAND PA 155 GRAND AVE, SUITE 400, OAKLAND, CA 94612-3758 USA SN 1939-1811 EI 1939-182X J9 HIST STUD NAT SCI JI Hist. Stud. Nat. Sci. PD APR PY 2014 VL 44 IS 2 BP 187 EP 195 PG 9 WC History & Philosophy Of Science SC History & Philosophy of Science GA AE6HK UT WOS:000334091000008 ER PT J AU Launius, RD AF Launius, Roger D. TI A Single Sky: How an International Community Forged the Science of Radio Astronomy SO HISTORICAL STUDIES IN THE NATURAL SCIENCES LA English DT Book Review C1 [Launius, Roger D.] Smithsonian Inst, Natl Air & Space Museum, Collect & Curatorial Affairs, Washington, DC 20013 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Collect & Curatorial Affairs, POB 37012,MRC 311, Washington, DC 20013 USA. EM launiusr@si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIFORNIA PRESS PI OAKLAND PA 155 GRAND AVE, SUITE 400, OAKLAND, CA 94612-3758 USA SN 1939-1811 EI 1939-182X J9 HIST STUD NAT SCI JI Hist. Stud. Nat. Sci. PD APR PY 2014 VL 44 IS 2 BP 187 EP 195 PG 9 WC History & Philosophy Of Science SC History & Philosophy of Science GA AE6HK UT WOS:000334091000007 ER PT J AU Byrne, PK Klimczak, C Sengor, AMC Solomon, SC Watters, TR Hauck, SA AF Byrne, Paul K. Klimczak, Christian Sengor, A. M. Celal Solomon, Sean C. Watters, Thomas R. Hauck, Steven A., II TI Mercury's global contraction much greater than earlier estimates SO NATURE GEOSCIENCE LA English DT Article ID LOBATE SCARPS; MESSENGER; EVOLUTION; VOLCANISM; THRUST; LITHOSPHERE; TOPOGRAPHY; TECTONICS; SURFACE; MARS AB Mercury, a planet with a lithosphere that forms a single tectonic plate, is replete with tectonic structures interpreted to be the result of planetary cooling and contraction. However, the amount of global contraction inferred from spacecraft images has been far lower than that predicted by models of the thermal evolution of the planets interior. Here we present a synthesis of the global contraction of Mercury from orbital observations acquired by the MESSENGER spacecraft. We show that Mercurys global contraction has been accommodated by a substantially greater number and variety of structures than previously recognized, including long belts of ridges and scarps where the crust has been folded and faulted. The tectonic features on Mercury are consistent with models for large-scale deformation proposed for a globally contracting Earthnow obsoletethat pre-date plate tectonics theory. We find that Mercury has contracted radially by as much as 7 km, well in excess of the 0.83 km previously reported from photogeology and resolving the discrepancy with thermal models. Our findings provide a key constraint for studies of Mercurys thermal history, bulk silicate abundances of heat-producing elements, mantle convection and the structure of its large metallic core. C1 [Byrne, Paul K.; Klimczak, Christian; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Byrne, Paul K.] Univ Space Res Assoc, Lunar & Planetary Inst, Houston, TX 77058 USA. [Sengor, A. M. Celal] Istanbul Tech Univ, Fac Mines, Dept Geol, TR-34469 Istanbul, Turkey. [Sengor, A. M. Celal] Istanbul Tech Univ, Eurasia Inst Earth Sci, TR-34469 Istanbul, Turkey. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Hauck, Steven A., II] Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA. RP Byrne, PK (reprint author), Univ Space Res Assoc, Lunar & Planetary Inst, Houston, TX 77058 USA. EM pbyrne@carnegiescience.edu RI Hauck, Steven/A-7865-2008 OI Hauck, Steven/0000-0001-8245-146X FU NASA [NASW-00002]; Carnegie Institution of Washington [NAS5 97271] FX We thank C. M. Ernst and N. L.Chabot (The Johns Hopkins University Applied Physics Laboratory, JHU/APL) for the incidence angle maps shown in Supplementary Fig. 2b,c and H. J. Melosh (Purdue University) for his constructive advice during the preparation of this paper. We also thank W. B. McKinnon for comments that substantially improved this manuscript. The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5 97271 to HU/APL. This research has made use of NASA's Astrophysics Data System and Planetary Data System. NR 50 TC 40 Z9 40 U1 4 U2 33 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD APR PY 2014 VL 7 IS 4 BP 301 EP 307 DI 10.1038/ngeo2097 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AE2PP UT WOS:000333815700019 ER PT J AU Wilson, RM Peden, BM Clark, CW Rittenhouse, ST AF Wilson, Ryan M. Peden, Brandon M. Clark, Charles W. Rittenhouse, Seth T. TI Spin Waves and Dielectric Softening of Polar Molecule Condensates SO PHYSICAL REVIEW LETTERS LA English DT Article ID BOSE-EINSTEIN CONDENSATION; TRAPPED DIPOLAR GASES; EXCITATIONS; ATOMS; STATE AB We consider an oblate Bose-Einstein condensate of heteronuclear polar molecules in a weak applied electric field. This system supports a rich quasiparticle spectrum that plays a critical role in determining its bulk dielectric properties. In particular, in sufficiently weak fields the system undergoes a polarization wave rotonization, leading to the development of textured electronic structure and a dielectric instability that is characteristic of the onset of a negative static dielectric function. C1 [Wilson, Ryan M.; Clark, Charles W.] NIST, Joint Quantum Inst, Gaithersburg, MD 20899 USA. [Wilson, Ryan M.; Clark, Charles W.] Univ Maryland, Gaithersburg, MD 20899 USA. [Peden, Brandon M.; Rittenhouse, Seth T.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Rittenhouse, Seth T.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Wilson, RM (reprint author), NIST, Joint Quantum Inst, Gaithersburg, MD 20899 USA. RI Clark, Charles/A-8594-2009 OI Clark, Charles/0000-0001-8724-9885 FU NRC postdoctoral fellowship FX We acknowledge useful conversations with B.L. Johnson, H.R. Sadeghpour, C. Ticknor, E. Timmermans, and J.L. Bohn. R.M.W. acknowledges support from an NRC postdoctoral fellowship. NR 47 TC 2 Z9 2 U1 0 U2 5 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 APR 1 PY 2014 VL 112 IS 13 AR 135301 DI 10.1103/PhysRevLett.112.135301 PG 5 WC Physics, Multidisciplinary SC Physics GA AE9OH UT WOS:000334336600008 PM 24745433 ER PT J AU Khonmee, J Brown, JL Rojanasthien, S Thumasanukul, D Kongphoemphun, A Siriaroonrat, B Tipkantha, W Punyapornwithaya, V Thitaram, C AF Khonmee, Jaruwan Brown, Janine L. Rojanasthien, Suvichai Thumasanukul, Dissakul Kongphoemphun, Adisorn Siriaroonrat, Boripat Tipkantha, Wanlaya Punyapornwithaya, Veerasak Thitaram, Chatchote TI Seasonality of fecal androgen and glucocorticoid metabolite excretion in male goral (Naemorhedus griseus) in Thailand SO ANIMAL REPRODUCTION SCIENCE LA English DT Article DE Goral; Glucocorticoid metabolites; Androgen metabolites; Non-invasive hormone monitoring; Seasonality ID REINDEER RANGIFER-TARANDUS; STRESS-INDUCED SUPPRESSION; STAGS CERVUS-ELAPHUS; WHITE-TAILED DEER; IBERIAN RED DEER; REPRODUCTIVE-BEHAVIOR; RUTTING BEHAVIOR; TESTICULAR STEROIDOGENESIS; MELENGESTROL ACETATE; PLASMA TESTOSTERONE AB There is no information on the endocrinology of Chinese goral (Naemorhedus griseus), a high priority species for captive breeding and reintroduction in Thailand. This study characterized fecal androgen and glucocorticoid metabolites in male goral at Omkoi Wildlife Sanctuary to investigate seasonal relationships. Fecal samples were collected 3 days/week for 1 year from eight adult males. Mean androgen metabolite concentrations were greater (P < 0.05) during the rainy season (289.82 +/- 9.18 ng/g) and winter (224.09+/-11.97 ng/g) compared to the summer (195.48 +/- 8.23 ng/g), and were related to breeding activity. A similar pattern was observed for glucocorticoid concentrations (22.10 +/- 0.72 ng/g compared to 21.98 +/- 0.98 ng/g compared to 15.30 +/- 0.48 ng/g), respectively, and this resulted in a positive correlation between the two hormones (P < 0.05). There also were positive correlations between fecal androgen metabolite concentrations and temperature (P < 0.05) and day length (P < 0.05). In summary, this is the first study to assess endocrine function in male goral, and results showed seasonal variation in testicular and adrenal steroidogenic function, with greater activity in the rainy season and winter. Given that resources for captive male goral are consistent throughout the year, reproduction may be regulated primarily by photoperiod in this species. (C) 2014 Elsevier B.V. All rights reserved. C1 [Khonmee, Jaruwan; Rojanasthien, Suvichai; Punyapornwithaya, Veerasak; Thitaram, Chatchote] Chiang Mai Univ, Fac Vet Med, Chiang Mai 50100, Thailand. [Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. [Thumasanukul, Dissakul; Kongphoemphun, Adisorn] Omkoi Wildlife Sanctuary, Dept Natl Pk Wildlife & Plant Conservat, Chiang Mai 50310, Thailand. [Siriaroonrat, Boripat; Tipkantha, Wanlaya] Zool Pk Org, Conservat Res & Educ Div, Bangkok 10300, Thailand. RP Khonmee, J (reprint author), Chiang Mai Univ, Fac Vet Med, Chiang Mai 50100, Thailand. EM jaruwan.khonmee@cmu.ac.th FU National Research Council of Thailand (NRCT); Graduate School of Chiang Mai University FX This study was supported by National Research Council of Thailand (NRCT) and the Graduate School of Chiang Mai University. The authors extend their gratitude to the staff of the Zoological Park Organization of Thailand, and Omkoi Wildlife Sanctuary for their assistance in sample collection. We are also grateful to Ms. Nicole Presley at the Smithsonian Conservation Biology Institute, and staff of the endocrinology lab at the Faculty of Veterinary Medicine, Chiang Mai University (Ms. Manisorn Tuantammarak, Ms. Patharanun Wongchai, and Mr. P allop Tankaew) for technical support. NR 57 TC 3 Z9 3 U1 2 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-4320 EI 1873-2232 J9 ANIM REPROD SCI JI Anim. Reprod. Sci. PD APR PY 2014 VL 146 IS 1-2 BP 70 EP 78 DI 10.1016/j.anireprosci.2014.02.008 PG 9 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA AE6UW UT WOS:000334134500010 PM 24630044 ER PT J AU Higgins, KL Arnold, AE Coley, PD Kursar, TA AF Higgins, K. Lindsay Arnold, A. Elizabeth Coley, Phyllis D. Kursar, Thomas A. TI Communities of fungal endophytes in tropical forest grasses: highly diverse host- and habitat generalists characterized by strong spatial structure SO FUNGAL ECOLOGY LA English DT Article DE Barro Colorado Island; Biodiversity; Community assembly; Fungal endophytes; Poaceae; Similarity; Tropical forest ID ENVIRONMENTAL-SAMPLES; BRACHIARIA-BRIZANTHA; GEOGRAPHIC STRUCTURE; ENDOLICHENIC FUNGI; PUERTO-RICO; TREE; BIODIVERSITY; BIOGEOGRAPHY; LEAVES; PALM AB Plant-symbiotic fungi influence the structure and function of all terrestrial ecosystems, but factors shaping their distributions in time and space are rarely well understood. Grasses (Poaceae), which first arose and diversified in tropical forests, harbor diverse but little-studied endophytes in the lowland forests of Panama. We used sequence data for 402 isolates from two sampling years, 11 host species, and 55 microsites at Barro Colorado Island, Panama to investigate the influence of host and habitat (soil type, forest age) in shaping endophyte diversity and composition. In contrast to previous studies, we found no evidence for host- or habitat specificity. Instead, endophytes demonstrated strong spatial structure consistent with dispersal limitation, with community similarity decaying markedly over a scale of hundreds of meters. Spatial structure that is independent of host species and habitat reveals remarkable heterogeneity of endophyte host associations at small geographic scales and adds an important spatial component to extrapolative estimates of fungal diversity. (C) 2013 Elsevier Ltd and The British Mycological Society. All rights reserved. C1 [Higgins, K. Lindsay; Coley, Phyllis D.; Kursar, Thomas A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Arnold, A. Elizabeth] Univ Arizona, Sch Plant Sci, Tucson, AZ 85721 USA. [Coley, Phyllis D.; Kursar, Thomas A.] Smithsonian Trop Res Inst, Balboa, Panama. RP Arnold, AE (reprint author), Univ Arizona, Sch Plant Sci, Tucson, AZ 85721 USA. EM klindsay.higgins@gmail.com; arnold@ag.arizona.edu; coley@biology.utah.edu; kursar@biology.utah.edu FU Smithsonian Tropical Research Institute; Sigma Xi; Garden Club of America Anne S. Chatham Fellowship in Medicinal Botany; College of Agriculture and Life Sciences (University of Arizona); organizing committee of IMC9; NSF [DEB-0234936, DEB-0640996] FX We thank the Smithsonian Tropical Research Institute for logistical support; Panama's Autoridad Nacional del Ambiente (ANAM) for permission to conduct this research and export samples for molecular analysis; M. Gunatilaka, M. Hoffman, J. U'Ren, D. Kandalepas, D. Mahana, and the Arnold lab group at the University of Arizona for technical assistance and/or comments on the manuscript; J. U'Ren for scriptwriting; F. Adler and D. Feener for guidance and statistical advice; F. Adler for critical evaluation of the manuscript; R. J. Steidl for insightful discussion; and the organizers of the 'Secret World of Endophytes' symposium at the 9th International Mycological Congress (IMC9), James White and Barbara Schulz, for the opportunity to submit this paper. We gratefully acknowledge funding from the Smithsonian Tropical Research Institute (Ernst Mayr Short-Term Fellowship, KLH), a Sigma Xi Grant-in-Aid of Research (KLH), the Garden Club of America Anne S. Chatham Fellowship in Medicinal Botany (KLH), the College of Agriculture and Life Sciences (University of Arizona; AEA), the organizing committee of IMC9, NSF DEB-0234936 (TAK and PDC), and NSF DEB-0640996 (AEA). This paper fulfills a portion of the MS requirements for KLH at the University of Utah. All work complied with the laws of Panama and ANAM. NR 79 TC 22 Z9 23 U1 4 U2 78 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1754-5048 EI 1878-0083 J9 FUNGAL ECOL JI Fungal Ecol. PD APR PY 2014 VL 8 BP 1 EP 11 DI 10.1016/j.funeco.2013.12.005 PG 11 WC Ecology; Mycology SC Environmental Sciences & Ecology; Mycology GA AE5CS UT WOS:000334006000001 ER PT J AU Eastrada, C Rojas, EI Wcislo, WT Van Bael, SA AF Eastrada, Catalina Rojas, Enith I. Wcislo, William T. Van Bael, Sunshine A. TI Fungal endophyte effects on leaf chemistry alter the in vitro growth rates of leaf-cutting ants' fungal mutualist, Leucocoprinus gongylophorus SO FUNGAL ECOLOGY LA English DT Article DE Atta colombica; Cochliobolus; Colletotrichurn tropicale; Endophytic fungi; Leaf-cutting ants; Leucocoprinus gongylophorus; Merremia umbellata; Symbiosis ID THEOBROMA-CACAO; GROWING ANTS; COLLETOTRICHUM-GLOEOSPORIOIDES; SUBSTRATE PREPARATION; SYMBIOTIC FUNGUS; PLANT-EXTRACTS; ATTA-CEPHALOTES; ATTINE ANTS; CUTTER ANTS; GARDENS AB Fungal symbionts that colonize leaf tissue asymptomatically (endophytes) can alter the foraging behaviour of leaf-cutting ants, and decrease the productivity of this herbivore's mutualistic fungal cultivar, Leucocoprinus gongylophorus. This negative effect of endophytes on the ant's cultivar could be the result of direct fungal fungal interaction or indirect reductions in the quality of leaves, the cultivar's growth substratum. To test for the indirect effects, we measured in vitro growth rates of cultivars in media that contained sterilized leaf extracts from plants with high (E-high) and low (E-low) endophyte colonization. We found that, opposite to our expectations, cultivars grew significantly faster in E-high leaf extracts compared to Elow extracts. Our results suggest that endophyte-driven changes in leaf chemistry are a less likely explanation for the observed in vivo reduction in the ant's symbiotic fungal growth and imply that the effect of direct endophyte cultivar interactions inside nests are potentially more important. (C) 2014 Elsevier Ltd and The British Mycological Society. All rights reserved. C1 [Eastrada, Catalina; Rojas, Enith I.; Wcislo, William T.; Van Bael, Sunshine A.] Smithsonian Trop Res Inst, Balboa, Panama. [Van Bael, Sunshine A.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. RP Eastrada, C (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM estradac@si.edu FU Smithsonian Institute Scholarly Studies Program; Restricted Endowment Funds; Smithsonian Institute Postdoctoral Fellowship; NSF [DEB-0949602]; SENACYT [FID10-091] FX We thank M. Caballero, F. Santos, M. Franco, K. Shaffer for laboratory support; R. Urriola, A. Ruiz, P. Galgani for logistic support; L. C. Mejia, E. R. Rodriguez, C. Bracho for molecular identification of leaf symbiont, H. Fernandez-Mann for insightful discussion on leaf-cutting ants. This work was funded by the Smithsonian Institute Scholarly Studies Program to WTW and SAV, Restricted Endowment Funds to CE, SAV, WTW, a Smithsonian Institute Postdoctoral Fellowship to CE, NSF DEB-0949602 to SAV and WTW, and SENACYT FID10-091 to SAV and WTW. Permission was granted to do this research by Panama's Authority on the Environment (ANAM). NR 90 TC 1 Z9 1 U1 4 U2 39 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1754-5048 EI 1878-0083 J9 FUNGAL ECOL JI Fungal Ecol. PD APR PY 2014 VL 8 BP 37 EP 45 DI 10.1016/j.funeco.2013.12.009 PG 9 WC Ecology; Mycology SC Environmental Sciences & Ecology; Mycology GA AE5CS UT WOS:000334006000005 ER PT J AU O'Mara, MT Wikelski, M Dechmann, DKN AF O'Mara, M. Teague Wikelski, Martin Dechmann, Dina K. N. TI 50years of bat tracking: device attachment and future directions SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Review DE 5% rule; movement; GPS tracking; radiotracking; telemetry ID FLIGHT PERFORMANCE; EPTESICUS-FUSCUS; CHIROPTERA; BEHAVIOR; RADIOTRANSMITTERS; MANEUVERABILITY; CONSERVATION; GUIDELINES; TELEMETRY; MIGRATION AB Radiotelemetry and satellite-based telemetry approaches are essential to describe the behaviour and biology of animals. This is especially true for bats, whose small size and cryptic lifestyles make them challenging to study. However, only a handful of studies have evaluated how transmitter mass and the attachment method affect bat behaviour or health, and none have assessed the development of technical methods in the field. We review the past 50years of bat tracking studies to determine how devices have been attached, how guidelines have been followed or changed, and whether any health or fitness impacts from these transmitters can be determined. Half of the nearly 300 studies available used devices heavier than the recommended 5% of body mass with minimal justification. Devices were typically glued directly to the backs of small bats and remained attached for 9days. This is far shorter than battery life span of most devices. Little information is available regarding the overall impact of attaching transmitters on the health, survival and reproductive success of bats, and there has been little development in attachment methods since the first tracking studies. We consequently developed a collar for small bats with a degradable weak link and tested it on several species. The collar worked successfully on three of four species. This allows longer habituation and tracking times while ensuring that the device drops off after the battery expires. Future studies will need to invest more effort in assessing potential long-term effects of tracking. They also need to build upon previous knowledge to find the best attachment method, size and shape for their study species to effectively improve wildlife tracking. C1 [O'Mara, M. Teague; Wikelski, Martin; Dechmann, Dina K. N.] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Baden Wurttembe, Germany. [O'Mara, M. Teague; Wikelski, Martin; Dechmann, Dina K. N.] Univ Konstanz, Dept Biol, Constance, Germany. [O'Mara, M. Teague; Wikelski, Martin; Dechmann, Dina K. N.] Smithsonian Trop Res Inst, Balboa, Panama. RP O'Mara, MT (reprint author), Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Baden Wurttembe, Germany. EM tomara@orn.mpg.de RI O'Mara, M. Teague/J-6090-2012 OI O'Mara, M. Teague/0000-0002-6951-1648 NR 54 TC 10 Z9 10 U1 6 U2 77 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 APR PY 2014 VL 5 IS 4 BP 311 EP 319 DI 10.1111/2041-210X.12172 PG 9 WC Ecology SC Environmental Sciences & Ecology GA AE5NY UT WOS:000334037100002 ER PT J AU Martin, MD Zimmer, EA Olsen, MT Foote, AD Gilbert, MTP Brush, GS AF Martin, Michael D. Zimmer, Elizabeth A. Olsen, Morten T. Foote, Andrew D. Gilbert, M. Thomas P. Brush, Grace S. TI Herbarium specimens reveal a historical shift in phylogeographic structure of common ragweed during native range disturbance SO MOLECULAR ECOLOGY LA English DT Article DE hybridization; population genetics-empirical; phylogeography; invasive species; contemporary evolution; landscape genetics ID AMBROSIA-ARTEMISIIFOLIA L.; ENEMY RELEASE HYPOTHESIS; POPULATION-STRUCTURE; GENETIC DIFFERENTIATION; SPECIES INVASIONS; PLANT INVASIONS; NORTH-AMERICA; LAND-USE; PHENOTYPIC PLASTICITY; PHYLOGENETIC ANALYSIS AB Invasive plants provide ample opportunity to study evolutionary shifts that occur after introduction to novel environments. However, although genetic characters pre-dating introduction can be important determinants of later success, large-scale investigations of historical genetic structure have not been feasible. Common ragweed (Ambrosia artemisiifolia L.) is an invasive weed native to North America that is known for its allergenic pollen. Palynological records from sediment cores indicate that this species was uncommon before European colonization of North America, and ragweed populations expanded rapidly as settlers deforested the landscape on a massive scale, later becoming an aggressive invasive with populations established globally. Towards a direct comparison of genetic structure now and during intense anthropogenic disturbance of the late 19th century, we sampled 45 natural populations of common ragweed across its native range as well as historical herbarium specimens collected up to 140years ago. Bayesian clustering analyses of 453 modern and 473 historical samples genotyped at three chloroplast spacer regions and six nuclear microsatellite loci reveal that historical ragweed's spatial genetic structure mirrors both the palaeo-record of Ambrosia pollen deposition and the historical pattern of agricultural density across the landscape. Furthermore, for unknown reasons, this spatial genetic pattern has changed substantially in the intervening years. Following on previous work relating morphology and genetic expression between plants collected from eastern North America and Western Europe, we speculate that the cluster associated with humans' rapid transformation of the landscape is a likely source of these aggressive invasive populations. C1 [Martin, Michael D.; Olsen, Morten T.; Foote, Andrew D.; Gilbert, M. Thomas P.] Univ Copenhagen, Ctr GeoGenet, DK-1350 Copenhagen K, Denmark. [Martin, Michael D.; Zimmer, Elizabeth A.] Smithsonian Inst, Natl Museum Nat Hist, MRC 166, Dept Bot, Washington, DC 20013 USA. [Martin, Michael D.; Brush, Grace S.] Johns Hopkins Univ, Dept Geog & Environm Engn, Baltimore, MD 21218 USA. RP Martin, MD (reprint author), Univ Copenhagen, Ctr GeoGenet, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. EM sameoldmike@gmail.com RI Olsen, Morten/J-4783-2013; Brush, Grace S./A-3288-2010; Gilbert, Marcus/A-8936-2013 OI Olsen, Morten/0000-0001-6716-6345; Brush, Grace S./0000-0003-1280-5933; Gilbert, Marcus/0000-0002-5805-7195 FU Laboratories of Analytical Biology; United States-Israel Binational Science Foundation [2006214]; Lundbeck Foundation [R52-5062]; Sigma Xi; Villum Foundation FX We are indebted to J. Shykoff and M. B. Hamilton for early advice and to Y.-J. Chun and F. Bretagnolle for providing access to primer sequences before publication. Many thanks to G. Johnson, J. Hunt, J. Horn, K. Wurdack, D. Erickson, V. Gowda, M. Cortes, S. Kingston, B. Davidson, L. Weigt and the rest of the staff and researchers at the Smithsonian Institution Laboratories of Analytical Biology (LAB) for technical advice and additional funds provided by the Laboratories of Analytical Biology. Thanks to E. Quiroz-Claros, R. Bello and other LAB student interns for their assistance with laboratory work. For providing generous access to herbarium materials, we acknowledge the curators and staff of the National Museum of Natural History (US), the Academy of Natural Sciences (PH), the New York Botanical Garden (NY), the Harvard University Herbaria (A), the Missouri Botanical Garden (MO) and the University of Massachusetts, Amherst (MASS). We are grateful to M. Allentoft and two anonymous reviewers for critical readings of the manuscript, to G. Guillot for technical advice and to N. Wales for assistance with the GIS analysis. Funding for this study was provided by United States-Israel Binational Science Foundation grant 2006214 to GSB, Lundbeck Foundation grant R52-5062 to MTPG and a Sigma Xi Grant-in-Aid of Research to MDM. MTO was supported by a postdoctoral scholarship from the Villum Foundation. NR 98 TC 11 Z9 11 U1 4 U2 69 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 EI 1365-294X J9 MOL ECOL JI Mol. Ecol. PD APR PY 2014 VL 23 IS 7 BP 1701 EP 1716 DI 10.1111/mec.12675 PG 16 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA AD5ZY UT WOS:000333333500008 PM 24450363 ER PT J AU Grinolds, MS Warner, M De Greve, K Dovzhenko, Y Thiel, L Walsworth, RL Hong, S Maletinsky, P Yacoby, A AF Grinolds, M. S. Warner, M. De Greve, K. Dovzhenko, Y. Thiel, L. Walsworth, R. L. Hong, S. Maletinsky, P. Yacoby, A. TI Subnanometre resolution in three-dimensional magnetic resonance imaging of individual dark spins SO NATURE NANOTECHNOLOGY LA English DT Article ID AMBIENT CONDITIONS; ROOM-TEMPERATURE; FORCE MICROSCOPY; ELECTRON-SPIN; DIAMOND; CENTERS; SENSOR AB Magnetic resonance imaging (MRI) has revolutionized biomedical science by providing non-invasive, three-dimensional biological imaging(1). However, spatial resolution in conventional MRI systems is limited to tens of micrometres(2), which is insufficient for imaging on molecular scales. Here, we demonstrate an MRI technique that provides subnanometre spatial resolution in three dimensions, with single electron-spin sensitivity. Our imaging method works under ambient conditions and can measure ubiquitous `dark' spins, which constitute nearly all spin targets of interest. In this technique, the magnetic quantum-projection noise of dark spins is measured using a single nitrogen-vacancy (NV) magnetometer located near the surface of a diamond chip. The distribution of spins surrounding the NV magnetometer is imaged with a scanning magnetic-field gradient. To evaluate the performance of the NV-MRI technique, we image the three-dimensional landscape of electronic spins at the diamond surface and achieve an unprecedented combination of resolution (0.8 nm laterally and 1.5 nm vertically) and single-spin sensitivity. Our measurements uncover electronic spins on the diamond surface that can potentially be used as resources for improved magnetic imaging. This NV-MRI technique is immediately applicable to diverse systems including imaging spin chains, readout of spin-based quantum bits, and determining the location of spin labels in biological systems. C1 [Grinolds, M. S.; Warner, M.; De Greve, K.; Dovzhenko, Y.; Thiel, L.; Walsworth, R. L.; Yacoby, A.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Thiel, L.; Maletinsky, P.] Univ Basel, Dept Phys, CH-4056 Basel, Switzerland. [Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hong, S.] Univ Vienna, Fac Phys, Vienna Ctr Quantum Sci & Technol VCQ, A-1090 Vienna, Austria. RP Grinolds, MS (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM yacoby@physics.harvard.edu RI Maletinsky, Patrick/L-1851-2015 OI Maletinsky, Patrick/0000-0003-1699-388X FU Department of Defense (NDSEG programme); National Science Foundation; Marie Curie Fellowship; Harvard Quantum Optics Center; DARPA QuEST programme; DARPA QuASAR programme; MURI QuISM FX The authors thank S. Kolkowitz, N. de Leon and C. Belthangady for technical discussions regarding optimizing NV-based sensors and M. Markham and Element Six for providing diamond samples. The authors acknowledge discussions on the detection of dark spins using DEER with M. D. Lukin, A. Sushkov, I. Lovchinsky, N. Chisholm, S. Bennett, and N. Yao. M. S. G. is supported through fellowships from the Department of Defense (NDSEG programme) and the National Science Foundation. M. W. is supported through a Marie Curie Fellowship and K. D. G. acknowledges support from the Harvard Quantum Optics Center as an HQOC postdoctoral fellow. This work was supported by the DARPA QuEST and QuASAR programmes and the MURI QuISM. NR 35 TC 52 Z9 52 U1 4 U2 82 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1748-3387 EI 1748-3395 J9 NAT NANOTECHNOL JI Nat. Nanotechnol. PD APR PY 2014 VL 9 IS 4 BP 279 EP 284 DI 10.1038/NNANO.2014.30 PG 6 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA AE5ZV UT WOS:000334068800013 PM 24658168 ER PT J AU Fletcher, F AF Fletcher, Francis TI Mantegna's Fictive Bronze Judith and Dido: Beyond Exemplarity SO ART HISTORY LA English DT Article C1 [Fletcher, Francis] Smithsonian Inst, Washington, DC 20560 USA. [Fletcher, Francis] Lib Congress, Washington, DC USA. [Fletcher, Francis] Dumbarton Oaks, Washington, DC USA. [Fletcher, Francis] Rutgers State Univ, Piscataway, NJ 08855 USA. [Fletcher, Francis] Dickinson Coll, Carlisle, PA 17013 USA. [Fletcher, Francis] Virginia Commonwealth Univ, Richmond, VA 23284 USA. RP Fletcher, F (reprint author), Rutgers State Univ, Piscataway, NJ 08855 USA. NR 57 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0141-6790 EI 1467-8365 J9 ART HIST JI Art Hist. PD APR PY 2014 VL 37 IS 2 SI SI BP 376 EP 399 DI 10.1111/1467-8365.12080 PG 24 WC Art SC Art GA AC9DO UT WOS:000332834700009 ER PT J AU Bieryla, A Hartman, JD Bakos, GA Bhatti, W Kovacs, G Boisse, I Latham, DW Buchhave, LA Csubry, Z Penev, K de Val-Borro, M Beky, B Falco, E Torres, G Noyes, RW Berlind, P Calkins, MC Esquerdo, GA Lazar, J Papp, I Sari, P AF Bieryla, A. Hartman, J. D. Bakos, G. A. Bhatti, W. Kovacs, G. Boisse, I. Latham, D. W. Buchhave, L. A. Csubry, Z. Penev, K. de Val-Borro, M. Beky, B. Falco, E. Torres, G. Noyes, R. W. Berlind, P. Calkins, M. C. Esquerdo, G. A. Lazar, J. Papp, I. Sari, P. TI HAT-P-49b: A 1.7 M-J PLANET TRANSITING A BRIGHT 1.5 M-circle dot F-STAR SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HAT-P-49, HD 340099); techniques: photometric; techniques: pectroscopic ID HOT JUPITERS; KEPLER FIELD; EXOPLANETS; COMPANIONS; ISOCHRONES; SUBGIANTS; ALGORITHM; HOSTS AB We report the discovery of the transiting extrasolar planet HAT-P-49b. The planet transits the bright (V = 10.3) slightly evolved F-star HD 340099 with a mass of 1.54 M-circle dot and a radius of 1.83 R-circle dot. HAT-P-49b is orbiting one of the 25 brightest stars to host a transiting planet which makes this a favorable candidate for detailed follow-up. This system is an especially strong target for Rossiter-McLaughlin follow-up due to the host star's fast rotation, 16 km s(-1). The planetary companion has a period of 2.6915 days, mass of 1.73 M-J, and radius of 1.41 R-J. The planetary characteristics are consistent with that of a classical hot Jupiter but we note that this is the fourth most massive star to host a transiting planet with both M-p and R-p well determined. C1 [Bieryla, A.; Latham, D. W.; Buchhave, L. A.; Beky, B.; Falco, E.; Torres, G.; Noyes, R. W.; Berlind, P.; Calkins, M. C.; Esquerdo, G. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hartman, J. D.; Bakos, G. A.; Bhatti, W.; Csubry, Z.; Penev, K.; de Val-Borro, M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Kovacs, G.] Konkoly Observ Budapest, H-1121 Budapest, Hungary. [Kovacs, G.] Univ N Dakota, Dept Phys & Astrophys, Grand Forks, ND 58201 USA. [Boisse, I.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, L. A.] Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, H-1461 Budapest, Hungary. RP Bieryla, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM abieryla@cfa.harvard.edu; gbakos@astro.princeton.edu FU NASA grants [NNGO4GN74G, NNX13AJ15G, NNX09AB29G, NNX09AF59G]; NSF grant [AST-1108686]; Kepler Mission under NASA Cooperative [NCC2-1390]; Hungarian Scientific Research Foundation (OTKA) [K-81373]; European Research Council/European Community under the FP7 through Starting Grant; Fundaccao para a Ciencia e a Tecnologia (FCT), Portugal [SFRH/BPD/81084/2011, PTDC/CTE-AST/098528/2008] FX HATNet operations have been funded by NASA grants NNGO4GN74G and NNX13AJ15G. Follow-up of HATNet targets has been partially supported through NSF grant AST-1108686. G.A.B., Z.C., and K.P. acknowledge partial support from NASA grant NNX09AB29G. K.P. acknowledges support from NASA grant NNX13AQ62G. G.T. acknowledges partial support from NASA grant NNX09AF59G. We also acknowledge partial support from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 (PI: D.W.L.). G.K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-81373. Data presented in this paper are based on observations obtained at the HAT station at the Submillimeter Array of SAO, and the HAT station at the Fred Lawrence Whipple Observatory of SAO. The authors thank all the staff of Haute-Provence Observatory for their contribution to the success of the SOPHLE project and their support at the 1.93 m telescope. I.B. acknowledges the support of the European Research Council/European Community under the FP7 through a Starting Grant, as well as from Fundaccao para a Ciencia e a Tecnologia (FCT), Portugal, through SFRH/BPD/81084/2011 and the project PTDC/CTE-AST/098528/2008. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 30 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD APR PY 2014 VL 147 IS 4 AR 84 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE1KP UT WOS:000333728500016 ER PT J AU Cody, AM Stauffer, J Baglin, A Micela, G Rebull, LM Flaccomio, E Morales-Calderon, M Aigrain, S Bouvier, J Hillenbrand, LA Gutermuth, R Song, I Turner, N Alencar, SHP Zwintz, K Plavchan, P Carpenter, J Findeisen, K Carey, S Terebey, S Hartmann, L Calvet, N Teixeira, P Vrba, FJ Wolk, S Covey, K Poppenhaeger, K Gunther, HM Forbrich, J Whitney, B Affer, L Herbst, W Hora, J Barrado, D Holtzman, J Marchis, F Wood, K Guimaraes, MM Box, JL Gillen, E McQuillan, A Espaillat, C Allen, L D'Alessio, P Favata, F AF Cody, Ann Marie Stauffer, John Baglin, Annie Micela, Giuseppina Rebull, Luisa M. Flaccomio, Ettore Morales-Calderon, Maria Aigrain, Suzanne Bouvier, Jerome Hillenbrand, Lynne A. Gutermuth, Robert Song, Inseok Turner, Neal Alencar, Silvia H. P. Zwintz, Konstanze Plavchan, Peter Carpenter, John Findeisen, Krzysztof Carey, Sean Terebey, Susan Hartmann, Lee Calvet, Nuria Teixeira, Paula Vrba, Frederick J. Wolk, Scott Covey, Kevin Poppenhaeger, Katja Guenther, Hans Moritz Forbrich, Jan Whitney, Barbara Affer, Laura Herbst, William Hora, Joseph Barrado, David Holtzman, Jon Marchis, Franck Wood, Kenneth Guimaraes, Marcelo Medeiros Lillo Box, Jorge Gillen, Ed McQuillan, Amy Espaillat, Catherine Allen, Lori D'Alessio, Paola Favata, Fabio TI CSI 2264: SIMULTANEOUS OPTICAL AND INFRARED LIGHT CURVES OF YOUNG DISK-BEARING STARS IN NGC 2264 WITH CoRoT and SPITZER-EVIDENCE FOR MULTIPLE ORIGINS OF VARIABILITY SO ASTRONOMICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; protoplanetary disks; stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be; techniques: photometric ID T-TAURI STARS; MAIN-SEQUENCE STARS; ORION NEBULA CLUSTER; TERM PHOTOMETRIC VARIABILITY; ROTATION PERIOD DISTRIBUTION; INITIAL MASS FUNCTION; X-RAY OBSERVATIONS; MIDINFRARED VARIABILITY; MOLECULAR CLOUD; BROWN DWARFS AB We present the Coordinated Synoptic Investigation of NGC 2264, a continuous 30 day multi-wavelength photometric monitoring campaign on more than 1000 young cluster members using 16 telescopes. The unprecedented combination of multi-wavelength, high-precision, high-cadence, and long-duration data opens a new window into the time domain behavior of young stellar objects. Here we provide an overview of the observations, focusing on results from Spitzer and CoRoT. The highlight of this work is detailed analysis of 162 classical T Tauri stars for which we can probe optical and mid-infrared flux variations to 1% amplitudes and sub-hour timescales. We present a morphological variability census and then use metrics of periodicity, stochasticity, and symmetry to statistically separate the light curves into seven distinct classes, which we suggest represent different physical processes and geometric effects. We provide distributions of the characteristic timescales and amplitudes and assess the fractional representation within each class. The largest category (>20%) are optical "dippers" with discrete fading events lasting similar to 1-5 days. The degree of correlation between the optical and infrared light curves is positive but weak; notably, the independently assigned optical and infrared morphology classes tend to be different for the same object. Assessment of flux variation behavior with respect to (circum)stellar properties reveals correlations of variability parameters with Ha emission and with effective temperature. Overall, our results point to multiple origins of young star variability, including circumstellar obscuration events, hot spots on the star and/or disk, accretion bursts, and rapid structural changes in the inner disk. C1 [Cody, Ann Marie; Stauffer, John; Rebull, Luisa M.; Carey, Sean] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Baglin, Annie] Observ Paris, LESIA, F-92195 Meudon, France. [Micela, Giuseppina; Flaccomio, Ettore; Affer, Laura] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Morales-Calderon, Maria; Barrado, David; Lillo Box, Jorge] INTA CSIC, Ctr Astrobiol, Dpto Astrofis, E-28691 Madrid, Spain. [Aigrain, Suzanne; Gillen, Ed] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Bouvier, Jerome] UJF Grenoble 1 CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG UMR 5274, F-38041 Grenoble, France. [Hillenbrand, Lynne A.; Carpenter, John; Findeisen, Krzysztof] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Gutermuth, Robert] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Turner, Neal] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Alencar, Silvia H. P.] Dept Fis ICEx UFMG, BR-30270901 Belo Horizonte, MG, Brazil. [Zwintz, Konstanze] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Plavchan, Peter] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Terebey, Susan] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90032 USA. [Hartmann, Lee; Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48105 USA. [Teixeira, Paula; Forbrich, Jan] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Vrba, Frederick J.] US Naval Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Wolk, Scott; Poppenhaeger, Katja; Guenther, Hans Moritz; Forbrich, Jan; Hora, Joseph] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Covey, Kevin] Lowell Observ, Flagstaff, AZ 86001 USA. [Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Herbst, William] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. [Holtzman, Jon] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Marchis, Franck] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Wood, Kenneth] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9AD, Fife, Scotland. [Guimaraes, Marcelo Medeiros] Dept Fis & Matemat UFSJ, BR-36420000 Ouro Branco, MG, Brazil. [McQuillan, Amy] Tel Aviv Univ, Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Espaillat, Catherine] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Allen, Lori] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [D'Alessio, Paola] UNAM, Ctr Radioastron & Astrofs, Morelia 58089, Michoacan, Mexico. [Favata, Fabio] European Space Agcy, F-75738 Paris 15, France. RP Cody, AM (reprint author), CALTECH, Spitzer Sci Ctr, 1200 East Calif Blvd, Pasadena, CA 91125 USA. EM amc@ipac.caltech.edu RI Lillo-Box, Jorge/I-2841-2015; Alencar, Silvia/C-2803-2013; Teixeira, Paula Stella/O-2289-2013; Guimaraes, Marcelo/H-5897-2012; Barrado Navascues, David/C-1439-2017; Morales-Calderon, Maria/C-8384-2017; OI Lillo-Box, Jorge/0000-0003-3742-1987; Teixeira, Paula Stella/0000-0002-3665-5784; Guimaraes, Marcelo/0000-0002-0517-4507; Barrado Navascues, David/0000-0002-5971-9242; Morales-Calderon, Maria/0000-0001-9526-9499; Micela, Giuseppina/0000-0002-9900-4751; Findeisen, Krzysztof/0000-0003-1898-5760; Poppenhaeger, Katja/0000-0003-1231-2194; Gunther, Hans Moritz/0000-0003-4243-2840; Flaccomio, Ettore/0000-0002-3638-5788; Hora, Joseph/0000-0002-5599-4650; Zwintz, Konstanze/0000-0001-9229-8315; Rebull, Luisa/0000-0001-6381-515X; Covey, Kevin/0000-0001-6914-7797 FU NASA through JPL/Caltech.; JPL/Caltech [1373081, 1424329, 1440160]; CNpq; CAPES; Fapemig; NASA ADAP [NNX11AD14G, NNX13AF08G]; INCT-A/CNPq; Pegasus Marie Curie Fellowship of the Research Foundation Flanders (FWO); European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant [227224] FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. S.H.P.A. acknowledges support from CNpq, CAPES, and Fapemig. R.G. gratefully acknowledges funding support from NASA ADAP grants NNX11AD14G and NNX13AF08G and Caltech/JPL awards 1373081, 1424329, and 1440160 in support of Spitzer Space Telescope observing programs. M.M.G. acknowledges support from INCT-A/CNPq. K.Z. received a Pegasus Marie Curie Fellowship of the Research Foundation Flanders (FWO) during part of this work and received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 227224 (PROSPERITY). NR 109 TC 73 Z9 73 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD APR PY 2014 VL 147 IS 4 DI 10.1088/0004-6256/147/4/82 PG 47 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE1KP UT WOS:000333728500014 ER PT J AU Ishioka, R Wang, SY Zhang, ZW Lehner, MJ Alcock, C Axelrod, T Bianco, FB Byun, YI Chen, WP Cook, KH Kim, DW King, SK Lee, T Marshall, SL Protopapas, P Rice, JA Schwamb, ME Wang, JH Wen, CY Ngeow, CC AF Ishioka, R. Wang, S. -Y. Zhang, Z. -W. Lehner, M. J. Alcock, C. Axelrod, T. Bianco, F. B. Byun, Y. -I. Chen, W. P. Cook, K. H. Kim, D. -W. King, S. -K. Lee, T. Marshall, S. L. Protopapas, P. Rice, J. A. Schwamb, M. E. Wang, J. -H. Wen, C. -Y. Ngeow, C. -C. TI THE TAIWANESE-AMERICAN OCCULTATION SURVEY PROJECT STELLAR VARIABILITY. III. DETECTION OF 58 NEW VARIABLE STARS SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: variables: Cepheids; stars: variables: delta Scuti; stars: variables: general ID SKY; INVENTORY; CEPHEIDS; CATALOG; BULGE; TAOS AB The Taiwanese-American Occultation Survey project is designed for the detection of stellar occultations by smallsize Kuiper Belt Objects, and it has monitored selected fields along the ecliptic plane by using four telescopes with a 3 deg(2) field of view on the sky since 2005. We have analyzed data accumulated during 2005-2012 to detect variable stars. Sixteen fields with observations of more than 100 epochs were examined. We recovered 85 variables among a total of 158 known variable stars in these 16 fields. Most of the nnrecovered variables are located in the fields observed less frequently. We also detected 58 variable stars which are not listed in the International Variable Star Index of the American Association of Variable Star Observers. These variable stars are classified as 3 RR Lyrae, 4 Cepheid, 1 delta Scuti, 5 Mira, 15 semi-regular, and 27 eclipsing binaries based on the periodicity and the profile of the light curves. C1 [Ishioka, R.; Wang, S. -Y.; Zhang, Z. -W.; Lehner, M. J.; Cook, K. H.; King, S. -K.; Lee, T.; Marshall, S. L.; Schwamb, M. E.; Wang, J. -H.; Wen, C. -Y.] 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. [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 & Univ Observ, Seoul 120749, South Korea. [Chen, W. P.; Ngeow, C. -C.] Natl Cent Univ, Inst Astron, Jhongli 320, Taoyuan County, Taiwan. [Kim, D. -W.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Protopapas, P.] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA. [Rice, J. A.] Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA. RP Ishioka, R (reprint author), Natl Taiwan Univ, Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan. EM ishioka@asiaa.sinica.edu.tw RI Lee, Typhoon/N-8347-2013; OI Lehner, Matthew/0000-0003-4077-0985; Schwamb, Megan/0000-0003-4365-1455 FU National Central University [NSC 96-2112-M-008-024-MY3]; NSC [101-2112-M-008-017-MY3]; National Research Foundation of Korea [2009-0075376]; thematic research program [AS-88-TP-A02]; National Science Foundation [AST-0501681]; NASA; Lawrence Livermore National Laboratory [W-7405-Eng-48]; Stanford Linear Accelerator Center [DEC-AO2-76SF00515]; Research Fellowship of the Japan Society FX The work at National Central University was supported by the grant NSC 96-2112-M-008-024-MY3 C.C. N a separate NSC grant 101-2112-M-008-017-MY3. Y.I.B. acknowledges the support of the National Research Foundation of Korea through grant 2009-0075376. Work at Academia Sinica was supported in part by the thematic research program AS-88-TP-A02. Work at the Harvard College Observatory was supported in part by the National Science Foundation under grant AST-0501681 and by NASA under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory in part under Contract W-7405-Eng-48 and by Stanford Linear Accelerator Center under Contract DEC-AO2-76SF00515. Part of this work is supported by a Research Fellowship of the Japan Society for the Promotion of Science for Young Scientists. This research has made use of the International Variable Star Index (VSX) database, operated at AAVSO, Cambridge, Massachusetts, USA, and the SIMBAD database and the VizieR catalog access tool, operated at CDS, Strasbourg, France. We thank the anonymous referee for many comments that improved this paper. NR 31 TC 0 Z9 0 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD APR PY 2014 VL 147 IS 4 AR 70 DI 10.1088/0004-6256/147/4/70 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE1KP UT WOS:000333728500002 ER PT J AU Stauffer, J Cody, AM Baglin, A Alencar, S Rebull, L Hillenbrand, LA Venuti, L Turner, NJ Carpenter, J Plavchan, P Findeisen, K Carey, S Terebey, S Morales-Calderon, M Bouvier, J Micela, G Flaccomio, E Song, I Gutermuth, R Hartmann, L Calvet, N Whitney, B Barrado, D Vrba, FJ Covey, K Herbst, W Furesz, G Aigrain, S Favata, F AF Stauffer, John Cody, Ann Marie Baglin, Annie Alencar, Silvia Rebull, Luisa Hillenbrand, Lynne A. Venuti, Laura Turner, Neal J. Carpenter, John Plavchan, Peter Findeisen, Krzysztof Carey, Sean Terebey, Susan Morales-Calderon, Maria Bouvier, Jerome Micela, Giusi Flaccomio, Ettore Song, Inseok Gutermuth, Rob Hartmann, Lee Calvet, Nuria Whitney, Barbara Barrado, David Vrba, Frederick J. Covey, Kevin Herbst, William Furesz, Gabor Aigrain, Suzanne Favata, Fabio TI CSI 2264: CHARACTERIZING ACCRETION-BURST DOMINATED LIGHT CURVES FOR YOUNG STARS IN NGC 2264 SO ASTRONOMICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; stars: formation; stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be ID T-TAURI STARS; MAIN-SEQUENCE STARS; COROT PHOTOMETRIC-OBSERVATIONS; SPITZER-SPACE-TELESCOPE; INITIAL MASS FUNCTION; ARRAY CAMERA IRAC; MAGNETOSPHERIC ACCRETION; AA TAURI; MAGNETOHYDRODYNAMIC SIMULATIONS; MAGNETIZED STARS AB Based on more than four weeks of continuous high-cadence photometric monitoring of several hundred members of the young cluster NGC 2264 with two space telescopes, NASA's Spitzer and the CNES CoRoT (Convection, Rotation, and planetary Transits), we provide high-quality, multi-wavelength light curves for young stellar objects whose optical variability is dominated by short-duration flux bursts, which we infer are due to enhanced mass accretion rates. These light curves show many brief-several hours to one day-brightenings at optical and near-infrared wavelengths with amplitudes generally in the range of 5%-50% of the quiescent value. Typically, a dozen or more of these bursts occur in a 30 day period. We demonstrate that stars exhibiting this type of variability have large ultraviolet (UV) excesses and dominate the portion of the u - g versus g - r color-color diagram with the largest UV excesses. These stars also have large H alpha equivalent widths, and either centrally peaked, lumpy H alpha emission profiles or profiles with blueshifted absorption dips associated with disk or stellar winds. Light curves of this type have been predicted for stars whose accretion is dominated by Rayleigh-Taylor instabilities at the boundary between their magnetosphere and inner circumstellar disk, or where magneto-rotational instabilities modulate the accretion rate from the inner disk. Among the stars with the largest UV excesses or largest H alpha equivalent widths, light curves with this type of variability greatly outnumber light curves with relatively smooth sinusoidal variations associated with long-lived hot spots. We provide quantitative statistics for the average duration and strength of the accretion bursts and for the fraction of the accretion luminosity associated with these bursts. C1 [Stauffer, John; Cody, Ann Marie; Rebull, Luisa; Carey, Sean] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Baglin, Annie] LESIA, Observ Paris Meudon, F-92195 Meudon, France. [Alencar, Silvia] Univ Fed Minas Gerais, ICEx, Dept Fis, BR-30270901 Belo Horizonte, MG, Brazil. [Hillenbrand, Lynne A.; Carpenter, John; Findeisen, Krzysztof] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Venuti, Laura; Bouvier, Jerome] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. [Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plavchan, Peter] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Terebey, Susan] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90032 USA. [Morales-Calderon, Maria; Barrado, David] CSIC, INTA, Dpto Astrofis, Ctr Astrobiol, E-28691 Madrid, Spain. [Micela, Giusi; Flaccomio, Ettore] INAF, Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Gutermuth, Rob] Smith Coll, Coll Astron Dept 5, Northampton, MA 01063 USA. [Hartmann, Lee; Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48105 USA. [Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Vrba, Frederick J.] US Naval Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Covey, Kevin] Lowell Observ, Flagstaff, AZ 86001 USA. [Herbst, William] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. [Furesz, Gabor] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Aigrain, Suzanne] Univ Oxford, Dept Phys, Subdept Astrophys, Oxford OX1 3RH, England. [Favata, Fabio] European Space Agcy, F-75738 Paris 15, France. RP Stauffer, J (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. EM stauffer@ipac.caltech.edu RI Alencar, Silvia/C-2803-2013; Barrado Navascues, David/C-1439-2017; Morales-Calderon, Maria/C-8384-2017; OI Barrado Navascues, David/0000-0002-5971-9242; Morales-Calderon, Maria/0000-0001-9526-9499; Findeisen, Krzysztof/0000-0003-1898-5760; Micela, Giuseppina/0000-0002-9900-4751; Flaccomio, Ettore/0000-0002-3638-5788; Rebull, Luisa/0000-0001-6381-515X; Covey, Kevin/0000-0001-6914-7797 FU NASA; JPL/Caltech FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 60 TC 42 Z9 42 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD APR PY 2014 VL 147 IS 4 AR 83 DI 10.1088/0004-6256/147/4/83 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE1KP UT WOS:000333728500015 ER PT J AU Aslan, CE Pinsky, ML Ryan, ME Souther, S Terrell, KA AF Aslan, Clare E. Pinsky, Malin L. Ryan, Maureen E. Souther, Sara Terrell, Kimberly A. TI Cultivating Creativity in Conservation Science SO CONSERVATION BIOLOGY LA English DT Article DE creative; creativity training; effective conservation; innovative; strategic; conservacion efectiva; Creativo; entrenamiento en la creatividad; estrategico; innovador ID OBSTACLES; COUNTRIES; QUANTITY; CONFLICT; INSIGHT; BIOLOGY; MODEL; EEG AB Conservation practitioners and scientists are often faced with seemingly intractable problems in which traditional approaches fail. While other sectors (e.g., business) frequently emphasize creative thinking to overcome complex challenges, creativity is rarely identified as an essential skill for conservationists. Yet more creative approaches are urgently needed in the effort to sustain Earth's biodiversity. We identified 4 strategies to develop skills in creative thinking and discuss underlying research and examples supporting each strategy. First, by breaking down barriers between disciplines and surrounding oneself with unfamiliar people, concepts, and perspectives, one can expand base knowledge and experiences and increase the potential for new combinations of ideas. Second, by meeting people where they are (both literally and figuratively), one exposes oneself to new environments and perspectives, which again broadens experiences and increases ability to communicate effectively with stakeholders. Third, by embracing risk responsibly, one is more likely to develop new, nontraditional solutions and be open to high-impact outcomes. Finally, by following a cycle of learning, struggle, and reflection, one can trigger neurophysiological changes that allow the brain to become more creative. Creativity is a learned trait, rather than an innate skill. It can be actively developed at both the individual and institutional levels, and learning to navigate the relevant social and practical barriers is key to the process. To maximize the success of conservation in the face of escalating challenges, one must take advantage of what has been learned from other disciplines and foster creativity as both a professional skill and an essential component of career training and individual development. Cultivando la Creatividad en la Ciencia de la Conservacion Resumen Los practicantes de la conservacion y los cientificos frecuentemente se enfrentan a problemas aparentemente intratables en los cuales los acercamientos tradicionales fallan. Mientras otros sectores (p. ej.: empresarial) enfatizan frecuentemente el pensamiento creativo para sobreponerse a retos complejos, la creatividad rara vez se identifica como una habilidad esencial para los conservacionistas. A pesar de esto se necesitan urgentemente mas acercamientos creativos en el esfuerzo de mantener la biodiversidad de la Tierra. Identificamos 4 estrategias para desarrollar habilidades en el pensamiento creativo y discutir investigaciones subyacentes y ejemplos que apoyan cada estrategia. Primero, al romper barreras entre disciplinas y rodeandose de gente, conceptos y perspectivas desconocidas, uno puede expandir el conocimiento basico y las experiencias; e incrementar el potencial de combinaciones nuevas de estas ideas. Segundo, al conocer en donde estan (tanto literal como figurativamente), uno se expone a nuevos ambientes y perspectivas, lo que tambien amplia las experiencias e incrementa la habilidad de comunicarse efectivamente con las partes interesadas. Tercero, al aceptar responsablemente el riesgo, es mas probable desarrollar soluciones nuevas y no-tradicionales y estar mas abierto a resultados de alto impacto. Finalmente, al seguir un ciclo de aprendizaje, lucha y reflexion, uno puede disparar cambios neurofisiologicos que permiten al cerebro volverse mas creativo. La creatividad es una habilidad aprendida y no una innata. Puede desarrollarse activamente tanto en el nivel individual como en el institucional y aprender a navegar las barreras sociales y practicas relevantes es clave en este proceso. Para maximizar el exito de la conservacion frente a retos crecientes, uno debe tomar ventaja de lo que se ha aprendido de otras disciplinas y cultivar la creatividad como una habilidad profesional y un componente esencial del entrenamiento en la carrera y el desarrollo individual. C1 [Aslan, Clare E.] Arizona Sonora Desert Museum, Conservat Educ & Sci Dept, Tucson, AZ 85743 USA. [Pinsky, Malin L.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Ryan, Maureen E.] Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA. [Ryan, Maureen E.] Simon Fraser Univ, Earth Ocean Res Grp 2, Burnaby, BC V5A 1S6, Canada. [Ryan, Maureen E.] Western Washington Univ, Fairhaven Coll Interdisciplinary Studies, Bellingham, WA 98225 USA. [Souther, Sara] Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. [Terrell, Kimberly A.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20013 USA. RP Aslan, CE (reprint author), Arizona Sonora Desert Museum, Conservat Educ & Sci Dept, Tucson, AZ 85743 USA. EM caslan@desertmuseum.org RI Pinsky, Malin/K-2884-2015 OI Pinsky, Malin/0000-0002-8523-8952 FU David H. Smith Postdoctoral Fellowships; Cedar Tree Foundation FX We thank the following individuals for sharing their wisdom and experience: M. Dombeck, Jordan Fischer, M. Hammer, L. Hattendorf, M. Rist, and C. Rose. We also thank Joern Fischer, B. Gratwicke, M. McCarthy, W. Palen, D. E. Wildt, and an anonymous reviewer for insightful comments that improved this manuscript. We are grateful to P. Trenham for his creative artwork (Fig. 2) and to S. Foster for logistical support during the panel discussion and throughout many conversations. We also thank the following teachers from Carencro Middle School for their enthusiasm and participation in the climate-change discussion: L. Angelle, P. Guidry, B. Welch, S. Thomas, L. Kidder, T. Williams, S. Goodrich, N. Lalonde, A. Duhon, T. Elliott, and A. Roger. Additionally, we thank W. Mertes, M. Haddon, and A. Chavenson for organizing the teacher workshop and for introducing us to Wordle. All authors were supported by David H. Smith Postdoctoral Fellowships, funded by the Cedar Tree Foundation and administered by the Society for Conservation Biology. NR 61 TC 5 Z9 5 U1 5 U2 55 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD APR PY 2014 VL 28 IS 2 BP 345 EP 353 DI 10.1111/cobi.12173 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AD0KS UT WOS:000332923500006 PM 24283793 ER PT J AU Sattler, T Pezzatti, GB Nobis, MP Obrist, MK Roth, T Moretti, M AF Sattler, T. Pezzatti, G. B. Nobis, M. P. Obrist, M. K. Roth, T. Moretti, M. TI Selection of Multiple Umbrella Species for Functional and Taxonomic Diversity to Represent Urban Biodiversity SO CONSERVATION BIOLOGY LA English DT Article DE city; Complementarity of biodiversity; indicator value analysis; surrogate species; Switzerland; Analisis del valor indicador; ciudad; complementacion de la biodiversidad; especies sustitutas; Suiza ID CONSERVATION SURROGATES; RICHNESS; COMMUNITIES; TRAITS; SCALE; BIRD; INDICATORS; GRASSLAND; RESPONSES; ECOSYSTEM AB Surrogates, such as umbrella species, are commonly used to reduce the complexity of quantifying biodiversity for conservation purposes. The presence of umbrella species is often indicative of high taxonomic diversity; however, functional diversity is now recognized as an important metric for biodiversity and thus should be considered when choosing umbrella species. We identified umbrella species associated with high taxonomic and functional biodiversity in urban areas in Switzerland. We analyzed 39,752 individuals of 574 animal species from 96 study plots and 1397 presences of 262 plant species from 58 plots. Thirty-one biodiversity measures of 7 taxonomic groups (plants, spiders, bees, ground beetles, lady bugs, weevils and birds) were included in within- and across-taxa analyses. Sixteen measures were taxonomical (species richness and species diversity), whereas 15 were functional (species traits including mobility, resource use, and reproduction). We used indicator value analysis to identify umbrella species associated with single or multiple biodiversity measures. Many umbrella species were indicators of high biodiversity within their own taxonomic group (from 33.3% in weevils to 93.8% in birds), to a lesser extent they were indicators across taxa. Principal component analysis revealed that umbrella species for multiple measures of biodiversity represented different aspects of biodiversity, especially with respect to measures of taxonomic and functional diversity. Thus, even umbrella species for multiple measures of biodiversity were complementary in the biodiversity aspects they represented. Thus, the choice of umbrella species based solely on taxonomic diversity is questionable and may not represent biodiversity comprehensively. Our results suggest that, depending on conservation priorities, managers should choose multiple and complementary umbrella species to assess the state of biodiversity. Seleccion de Multiples Especies Paraguas para la Diversidad Funcional y Taxonomica para Representar la Biodiversidad Urbana Resumen Los sustitutos como las especies paraguas comunmente se usan para reducir la complejidad de la cuantificacion de la biodiversidad por motivos de conservacion. La presencia de una especie paraguas casi siempre es indicativa de una diversidad taxonomica alta; sin embargo, la diversidad funcional ahora se reconoce como una medida importante de la biodiversidad y por lo tanto debe considerarse al elegir especies paraguas. Identificamos especies paraguas asociadas con la biodiversidad taxonomica alta y funcional en areas urbanas en Suiza. Analizamos 39, 752 individuos de 574 especies de animales de 96 parcelas de estudio y 1, 397 registros de 262 especies de plantas de 58 parcelas. Treinta y un medidas de biodiversidad de siete grupos taxonomicos (plantas, aranas, abejas, carabidos, catarinas, gorgojos y aves) se incluyeron en los analisis dentro de- y a lo largo de- taxones. Dieciseis medidas fueron taxonomicas (riqueza de especies y diversidad de especies), mientras que 15 fueron funcionales (caracteristicas de especies incluyendo la movilidad, uso de recursos y reproduccion). Usamos el analisis del valor indicador para identificar especies paraguas asociadas con una o multiples medidas de biodiversidad. Muchas especies paraguas fueron indicadoras de alta biodiversidad dentro de su grupo taxonomico (desde 33.3% en gorgojos hasta 93.8% en aves) y en menor medida fueron indicadoras a lo largo de taxones. El analisis de componentes principales revelo que las especies paraguas para medidas multiples de la biodiversidad representaron diferentes aspectos de la biodiversidad, especialmente con respecto a las medidas de la diversidad taxonomica y funcional. Asi, incluso las especies paraguas para medidas multiples de la biodiversidad fueron complementarias en los aspectos de biodiversidad que representaron. Entonces, la eleccion de una especie paraguas basada unicamente en la diversidad taxonomica es cuestionable y puede no representar a la biodiversidad integralmente. Nuestros resultados sugieren que, dependiendo de las prioridades de conservacion, los administradores deben elegir especies paraguas multiples y complementarias para estudiar el estado de la biodiversidad. C1 [Sattler, T.; Pezzatti, G. B.; Moretti, M.] Swiss Fed Res Inst WSL, CH-6500 Bellinzona, Switzerland. [Nobis, M. P.; Obrist, M. K.] Swiss Fed Res Inst WSL, CH-8903 Birmensdorf, Switzerland. [Roth, T.] Biodivers Monitoring Switzerland, CH-4153 Reinach, BL, Switzerland. [Roth, T.] Univ Basel, Inst Zool, CH-4051 Basel, Switzerland. RP Sattler, T (reprint author), Smithsonian Trop Res Inst, Balboa, Ancon, Panama. EM thomassattler@gmx.net RI Nobis, Michael/F-6176-2010; Pezzatti, Gianni Boris/D-5102-2017 OI Pezzatti, Gianni Boris/0000-0003-2564-3435 FU Federal Office for the Environment; Swiss National Science Foundation FX We thank V. Albin, F. Bontadina, P. Duelli, B. Fecker, F. Fibbioli, S. Fontana, A. Hanggi, R. Home, W. Kastenholz, M. Cooke Kindermann, L. Milani, A. Niederer, M. Plattner, M. Ryf, A. Schulz, R. Siegwart, R. Tester, and P. Wirz who helped in the field, in the lab, or with the organization of the fauna study. The following arthropod specialists identified the species: F. Amiet, M. Herrmann and D. Kouakou (Apiformes), H. Luka and Y. Chittaro (Carabidae), X. Heer (Araneae), C. Canepari (Coccinelidae), C. Germann (Curculionidae). We thank D. Al-Jabaji, B. Berner, M. Bichsel, S. Birrer, U. Bollens, T. Breunig, J.-F. Burri, M. Camenisch, G. Carraro, E. Danner, Ph. Druart, M. Frei, D. Galeuchet, Ch. Hadorn, S. Joss, A. Jotterand, Ch. Kasermann, D. Knecht, U. Kradolfer, R. Langenauer, K. Marti, J. Paulsen, A. Persico, M. Ryf, N. Tonascia, M. Valencak, M. Vust, and U. Weber (plants). Our sincerest thanks go to B. Noon, T. Caro, R. Home, and J. Stapley who considerably improved earlier versions of the manuscript. The Swiss Federal Office for the Environment FOEN and the Swiss Ornithological Institute provided the plant and the bird distribution data, whereas the arthropod distribution data was obtained from the Swiss Biological Records Center CSCF (S. Capt). Financial support was provided by the Federal Office for the Environment (S. Pearson, N. Indermuhle). The project BiodiverCity was funded by the Swiss National Science Foundation as a project of NRP54 Sustainable development of the Built Environment (www.nrp54.ch). NR 53 TC 8 Z9 8 U1 34 U2 156 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD APR PY 2014 VL 28 IS 2 BP 414 EP 426 DI 10.1111/cobi.12213 PG 13 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AD0KS UT WOS:000332923500013 PM 24372620 ER PT J AU Luo, SJ Zhang, Y Johnson, WE Miao, L Martelli, P Antunes, A Smith, JLD O'Brien, SJ AF Luo, Shu-Jin Zhang, Yue Johnson, Warren E. Miao, Lin Martelli, Paolo Antunes, Agostinho Smith, James L. D. O'Brien, Stephen J. TI Sympatric Asian felid phylogeography reveals a major Indochinese-Sundaic divergence SO MOLECULAR ECOLOGY LA English DT Article DE Y chromosome; X chromosome; phylogeography; Indochinese-Sundaic divergence; Asian felids; central Thai-Malay Peninsula; mtDNA ID SOUTHEAST-ASIA; SPECIES DISTRIBUTIONS; BIOGEOGRAPHIC BARRIER; CLOUDED LEOPARD; PANTHERA-PARDUS; Y-CHROMOSOME; PLEISTOCENE; MITOCHONDRIAL; BENGALENSIS; DIVERSITY AB The dynamic geological and climatological history of Southeast Asia has spawned a complex array of ecosystems and 12 of the 37 known cat species, making it the most felid-rich region in the world. To examine the evolutionary histories of these poorly studied fauna, we compared phylogeography of six species (leopard cat Prionailurus bengalensis, fishing cat P.viverrinus, Asiatic golden cat Pardofelis temminckii, marbled cat P.marmorata, tiger Panthera tigris and leopard P.pardus) by sequencing over 5kb of DNA each from 445 specimens at multiple loci of mtDNA, Y and X chromosomes. All species except the leopard displayed significant phylogenetic partitions between Indochina and Sundaland, with the central Thai-Malay Peninsula serving as the biogeographic boundary. Concordant mtDNA and nuclear DNA genealogies revealed deep Indochinese-Sundaic divergences around 2 MYA in both P.bengalensis and P.marmorata comparable to previously described interspecific distances within Felidae. The divergence coincided with serial sea level rises during the late Pliocene and early Pleistocene, and was probably reinforced by repeated isolation events associated with environmental changes throughout the Pleistocene. Indochinese-Sundaic differentiations within P.tigris and P.temminckii were more recent at 72-108 and 250-1570kya, respectively. Overall, these results illuminate unexpected, deep vicariance events in Southeast Asian felids and provide compelling evidence of species-level distinction between the Indochinese and Sundaic populations in the leopard cat and marbled cat. Broader sampling and further molecular and morphometric analyses of these species will be instrumental in defining conservation units and effectively preserving Southeast Asian biodiversity. C1 [Luo, Shu-Jin; Zhang, Yue; Miao, Lin] Peking Univ, Coll Life Sci, Peking Tsinghua Ctr Life Sci, Beijing 100871, Peoples R China. [Johnson, Warren E.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Front Royal, VA 22630 USA. [Martelli, Paolo] Ocean Pk, Aberdeen, Hong Kong, Peoples R China. [Antunes, Agostinho] Univ Porto, Ctr Interdisciplinar Invest Marinha & Ambiental, CIMAR CIIMAR, P-4050123 Oporto, Portugal. [Antunes, Agostinho] Univ Porto, Dept Biol, Fac Ciencias, P-4169007 Oporto, Portugal. [Smith, James L. D.] Univ Minnesota, Dept Fisheries Wildlife & Conservat Biol, St Paul, MN 55108 USA. [O'Brien, Stephen J.] St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, St Petersburg 199004, Russia. [O'Brien, Stephen J.] Nova SE Univ, Oceanog Ctr, Ft Lauderdale, FL 33004 USA. RP Luo, SJ (reprint author), Peking Univ, Coll Life Sci, Peking Tsinghua Ctr Life Sci, Beijing 100871, Peoples R China. EM Luo.shujin@pku.edu.cn RI Johnson, Warren/D-4149-2016; OI Johnson, Warren/0000-0002-5954-186X; O'Brien, Stephen J./0000-0001-7353-8301 FU NIH; UMN Doctoral Dissertation Fellowship; National Natural Science Foundation of China (NSFC) [31271320]; Center for Life Sciences at PKU; ERDF through COMPETE [PEst-C/MAR/LA0015/2013, PTDC/AAC-AMB/121301/2010, FCOMP-01-0124-FEDER-019490]; Russian Ministry of Science [11.G34.31.0068] FX We thank all zoos, institutions and people listed in Table S1 for providing biological samples, particularly S.H. Oh, K. Lazarus, S. Vellayan, C.W. Yang, S.C. Chin, Z. Zhang, Z. Xie, S. Sun, R. Kumar, K.S. Tan, N. Marx, G.X. He, W. Tunwattana, S. Kamolnorranath, K. Pillai, P.V. Lam, N. Lim and P. Patumrattanathan. We appreciate technical assistance from X.S. Hu, R. Hanson, J. Marterson, B. Kessing, V. David, M. Raymond, W. Murphy, C. McIntosh, G.K. Pei, L. Maslan, P. Perelman, Y. Ishida, C. O'hUigin, G. Bar-Gal, E. Eizirik and A. Roca. We also thank D. Woodruff and A. Wilting for helpful discussions and L. Liu for graphical assistance. Financial support to the project and SJL was from the NIH Intramural Program (2000-2009), NIH Pre-Doctoral (2000-2003) and Post-Doctoral (2007-2009) Fellowships, UMN Doctoral Dissertation Fellowship (2005-2006), National Natural Science Foundation of China (NSFC No. 31271320), and Center for Life Sciences at PKU. AA was partially supported by ERDF through COMPETE (PEst-C/MAR/LA0015/2013, PTDC/AAC-AMB/121301/2010, and FCOMP-01-0124-FEDER-019490). SJO was supported in part by a Russian Ministry of Science Mega-Grant No.11.G34.31.0068. NR 58 TC 11 Z9 11 U1 2 U2 66 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 EI 1365-294X J9 MOL ECOL JI Mol. Ecol. PD APR PY 2014 VL 23 IS 8 BP 2072 EP 2092 DI 10.1111/mec.12716 PG 21 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA AE3DW UT WOS:000333858200015 PM 24629132 ER PT J AU Betancur, R Orti, G AF Betancur-R, Ricardo Orti, Guillermo TI Molecular evidence for the monophyly of flatfishes (Carangimorpharia: Pleuronectiformes) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Hypothesis testing; Taxonomic sampling; Genetic sampling; Systematic error; Gene tree discordance; Hard phylogenetic question ID SPECIES TREE ANALYSIS; EVOLUTIONARY ORIGIN; MAXIMUM-LIKELIHOOD; PHYLOGENY; TELEOSTEI; SEQUENCES; FISHES; PERSPECTIVE; INTERRELATIONSHIPS; ACANTHOMORPHA AB Proliferation of phylogenetic studies based on poor taxonomic sampling or insufficient molecular evidence usually leads to conflicting results. As a consequence, advancement of systematic knowledge yields to confusion. The problem is exacerbated for taxonomic groups with historically difficult resolution of evolutionary relationships such as the flatfishes. Molecular evidence to support monophyly for this emblematic group of fishes and their interrelationships has been elusive, and a recent paper published in this journal went as far as to claim that flatfish monophyly can be rejected with molecular data, implying that the asymmetric body plan unique to these fishes had two independent origins. A reanalysis of this evidence suggests the contrary and combination of the new data with existing datasets unequivocally supports the monophyly of this group based on analyses of concatenated data as well as species tree approaches. Resolution of difficult phylogenetic problems requires analysis of larger datasets with adequate taxonomic coverage and sound hypothesis-testing procedures. Proliferation of partial studies claiming extraordinary results should be avoided in order to advance the field of molecular phylogenetics. (C) 2014 Elsevier Inc. All rights reserved. C1 [Betancur-R, Ricardo; Orti, Guillermo] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Betancur-R, Ricardo] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, 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 National Science Foundation [DEB-1004765]; GWU Selective Excellence in Diversity of Life program; Peter Buck fellowship of the Smithsonian FX We thank D. Arcila for providing help running TNT and members in the Orti laboratory for comments on the manuscript. We also thank Associate Editor G. Bernardi and three anonymous reviewers for insightful comments. This research was partially funded by the National Science Foundation Grant DEB-1004765 (to GO), and the GWU Selective Excellence in Diversity of Life program and the Peter Buck fellowship of the Smithsonian to RBR. NR 48 TC 7 Z9 7 U1 3 U2 24 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD APR PY 2014 VL 73 BP 18 EP 22 DI 10.1016/j.ympev.2014.01.006 PG 5 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA AD6OD UT WOS:000333379500003 PM 24447882 ER PT J AU Voirin, B Scriba, MF Martinez-Gonzalez, D Vyssotski, AL Wikelski, M Rattenborg, NC AF Voirin, Bryson Scriba, Madeleine F. Martinez-Gonzalez, Dolores Vyssotski, Alexei L. Wikelski, Martin Rattenborg, Niels C. TI Ecology and Neurophysiology of Sleep in Two Wild Sloth Species SO SLEEP LA English DT Article DE Benzodiazepine; EEG; predation; NREM sleep; REM sleep; sloth; spindle; phasing; wild ID NATURALLY-OCCURRING BENZODIAZEPINES; GABA(A) RECEPTOR SUBTYPE; PHYLOGENETIC ANALYSIS; 3-TOED SLOTH; LEOPARDUS-PARDALIS; MAMMALIAN SLEEP; WAVE ACTIVITY; EEG; BRADYPUS; BEHAVIOR AB Study Objectives: Interspecific variation in sleep measured in captivity correlates with various physiological and environmental factors, including estimates of predation risk in the wild. However, it remains unclear whether prior comparative studies have been confounded by the captive recording environment. Herein we examine the effect of predation pressure on sleep in sloths living in the wild. Design: Comparison of two closely related sloth species, one exposed to predation and one free from predation. Setting: Panamanian mainland rainforest (predators present) and island mangrove (predators absent). Participants: Mainland (Bradypus variegatus, five males and four females) and island (Bradypus pygmaeus, six males) sloths. Interventions: None. Measurements and Results: Electroencephalographic (EEG) and electromyographic (EMG) activity was recorded using a miniature data logger. Although both species spent between 9 and 10 h per day sleeping, the mainland sloths showed a preference for sleeping at night, whereas island sloths showed no preference for sleeping during the day or night. Standardized EEG activity during nonrapid eye movement (NREM) sleep showed lower low-frequency power, and increased spindle and higher frequency power in island sloths when compared to mainland sloths. Conclusions: In sloths sleeping in the wild, predation pressure influenced the timing of sleep, but not the amount of time spent asleep. The preference for sleeping at night in mainland sloths may be a strategy to avoid detection by nocturnal cats. The pronounced differences in the NREM sleep EEG spectrum remain unexplained, but might be related to genetic or environmental factors. C1 [Voirin, Bryson; Scriba, Madeleine F.; Martinez-Gonzalez, Dolores; Rattenborg, Niels C.] Max Planck Inst Ornithol Seewiesen, Avian Sleep Grp, D-82319 Seewiesen, Germany. [Voirin, Bryson; Wikelski, Martin] Max Planck Inst Ornithol Radolfzell, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Germany. [Voirin, Bryson] Smithsonian Trop Res Inst Panama, Balboa, Ancona, Panama. [Scriba, Madeleine F.] Univ Lausanne, Dept Ecol & Evolut, Lausanne, Switzerland. [Vyssotski, Alexei L.] Univ Zurich, Inst Neuroinformat, Zurich, Switzerland. [Vyssotski, Alexei L.] Swiss Fed Inst Technol, Zurich, Switzerland. [Wikelski, Martin] Univ Konstanz, Dept Biol, Constance, Germany. RP Voirin, B (reprint author), Max Planck Inst Ornithol Seewiesen, Avian Sleep Grp, Eberhard Gwinner Str, D-82319 Seewiesen, Germany. EM voirin@orn.mpg.de OI Scriba, Madeleine F./0000-0003-3046-5004 FU Max Planck Society; Smithsonian Fellowship program FX The authors thank La Autoridad Nacional del Ambiente for granting us research permits to conduct fieldwork in Panama, and Sebastian Codas and Christian Lundeberg for their help catching sloths. We thank the Smithsonian Tropical Research Institute for logistical and administrative support, the Smithsonian Fellowship program, Gabriel Jacome and the entire staff of STRI Bocas station, and the International Max Planck Research School for Organismal Research. This research was funded by the Max Planck Society. NR 84 TC 5 Z9 5 U1 9 U2 50 PU AMER ACAD SLEEP MEDICINE PI WESTCHESTER PA ONE WESTBROOK CORPORATE CTR, STE 920, WESTCHESTER, IL 60154 USA SN 0161-8105 EI 1550-9109 J9 SLEEP JI Sleep PD APR 1 PY 2014 VL 37 IS 4 BP 753 EP 761 DI 10.5665/sleep.3584 PG 9 WC Clinical Neurology; Neurosciences SC Neurosciences & Neurology GA AE0RF UT WOS:000333673100015 PM 24899764 ER PT J AU Sohn, JC AF Sohn, Jae-Cheon TI Morphology-Based Phylogeny and Biogeography of Wockia (Lepidoptera: Urodidae) with Description of a New Species from Japan and South Korea SO ZOOLOGICAL SCIENCE LA English DT Article DE biogeography; cladistic analysis; taxonomy; Urodoidea; Wockia ID HEINEMANN; BUTTERFLIES; SALICACEAE; EOCENE; MOTHS; GENE AB Wockia, one of the six genera within the lepidopteran family Urodidae, currently includes nine species distributed in Holarctic, Oriental, and Neotropical regions. A new species of the genus, W. magna sp. nov., is described from Japan and South Korea. This is the first record of Urodidae from Japan. A cladistic analysis was constructed based on 27 morphological characters from five ingroup species and two outgroup taxa. A single most parsimonious tree was found (length = 38, CI = 71, RI = 70). The resulting tree failed to recover the monophyly of Wockia chewbacca and a clade Wockia sensu stricto, including four congeners from North America, temperate East Asia and Southeast Asia. Wockia sensu stricto was resolved as monophyletic and was divided into two subgroups, one including W. asperipunctella and W. magna, and the other including W. koreana and W. variata. The sister-group relationship of W. asperipunctella and W. magna was moderately supported. Synapomorphies of Wockia sensu stricto are provided from the resulting phylogeny. Systematic definitions of Wockia and other allied genera are revised. Optimal ancestral area reconstruction implemented in DIVA resulted in different hypotheses for Wockia, depending on how to constrain the maximum number of areas. The maximum area number set as two yielded a more likely scenario suggesting that Wockia sensu stricto originated in temperate East Asia and then dispersed into the Oriental region, North America, and Europe. A working hypothesis and other equally possible alternative explanations for the biogeography of Wockia are provided. C1 [Sohn, Jae-Cheon] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Sohn, Jae-Cheon] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Sohn, JC (reprint author), Univ Maryland, Dept Entomol, 4112 Plant Sci Bldg, College Pk, MD 20742 USA. EM jsohn@umd.edu NR 46 TC 1 Z9 1 U1 0 U2 10 PU ZOOLOGICAL SOC JAPAN PI TOKYO PA HONGO MT BUILDING 4F, HONGO 7-2-2, BUNKYO-KU, TOKYO, 113-0033, JAPAN SN 0289-0003 J9 ZOOL SCI JI Zool. Sci. PD APR PY 2014 VL 31 IS 4 BP 258 EP 265 DI 10.2108/zs130199 PG 8 WC Zoology SC Zoology GA AE0AG UT WOS:000333625300010 PM 24694229 ER PT J AU Dunn, RH Tocheri, MW Orr, CM Jungers, WL AF Dunn, Rachel H. Tocheri, Matthew W. Orr, Caley M. Jungers, William L. TI Ecological Divergence and Talar Morphology in Gorillas SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE foot; arboreality; terrestriality; talus; tarsals ID IMPENETRABLE NATIONAL-PARK; GEOMETRIC MORPHOMETRIC-ANALYSIS; SYMPATRIC LOWLAND GORILLAS; HUMAN SKIN PIGMENTATION; AUSTRALOPITHECUS-AFARENSIS; MOUNTAIN GORILLAS; MITOCHONDRIAL-DNA; EVOLUTIONARY HISTORY; NUCLEAR INTEGRATIONS; BEHAVIORAL ECOLOGY AB Gorillas occupy a variety of habitats from the west coast to eastern central Africa. These habitats differ considerably in altitude, which has a pronounced effect on forest ecology. Although all gorillas are obligate terrestrial knuckle-walking quadrupeds, those that live in lowland habitats eat fruits and climb more often than do those living in highland habitats. Here we test the hypothesis that gorilla talus morphology falls along a morphocline that tracks locomotor function related to a more inverted or everted foot set. This proposed morphocline predicts that gorillas living in lowland habitats may have a talocrural joint configured to facilitate a more medially oriented foot during climbing, suggesting that they may be more adaptively committed to arboreality than gorillas living in highland habitats. To quantify the relative set of the foot in gorillas, we chose two three-dimensional measurements of the talocrural joint: mediolateral curvature of the trochlea and relative surface area of the lateral malleolus. Our results show that, in comparison to their eastern counterparts, western gorillas have talar features that reflect a more medially directed sole of the foot. This morphology likely facilitates foot placement in a wider range of positions and minimization of shearing stresses across the joint when the foot is loaded on more curved or vertically oriented substrates as occurs during climbing and other arboreal behaviors. In contrast, eastern gorilla talar morphology is consistent with habitual placement of the foot with the sole directed more inferiorly, suggesting more effective loading during plantigrade push-off on terrestrial substrates. Am J Phys Anthropol 153:526-541, 2014. (c) 2013 Wiley Periodicals, Inc. C1 [Dunn, Rachel H.] Des Moines Univ, Dept Anat, Des Moines, IA 50312 USA. [Tocheri, Matthew W.] Smithsonian Inst, Dept Anthropol, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20560 USA. [Tocheri, Matthew W.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Orr, Caley M.] Midwestern Univ, Dept Anat, Downers Grove, IL 60515 USA. [Jungers, William L.] SUNY Stony Brook, Dept Anat Sci, Stony Brook, NY 11794 USA. RP Tocheri, MW (reprint author), Smithsonian Inst, Dept Anthropol, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20560 USA. EM tocherim@si.edu OI Tocheri, Matthew/0000-0001-7600-8998 FU Wenner-Gren Foundation [7822] FX Grant sponsor: Wenner-Gren Foundation post-PhD award to MWT; Grant number: 7822. NR 117 TC 16 Z9 16 U1 5 U2 20 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD APR PY 2014 VL 153 IS 4 BP 526 EP 541 DI 10.1002/ajpa.22451 PG 16 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AC2KK UT WOS:000332329500002 PM 24374860 ER PT J AU Nweeia, MT Eichmiller, FC Hauschka, PV Donahue, GA Orr, JR Ferguson, SH Watt, CA Mead, JG Potter, CW Dietz, R Giuseppetti, AA Black, SR Trachtenberg, AJ Kuo, WP AF Nweeia, Martin T. Eichmiller, Frederick C. Hauschka, Peter V. Donahue, Gretchen A. Orr, Jack R. Ferguson, Steven H. Watt, Cortney A. Mead, James G. Potter, Charles W. Dietz, Rune Giuseppetti, Anthony A. Black, Sandie R. Trachtenberg, Alexander J. Kuo, Winston P. TI Sensory Ability in the Narwhal Tooth Organ System SO ANATOMICAL RECORD-ADVANCES IN INTEGRATIVE ANATOMY AND EVOLUTIONARY BIOLOGY LA English DT Article DE narwhal; tusk; Monodon monoceros; tusk functional significance; Brannstrom hydrodynamic theory; tooth gene expression; pulp tissue; tusk histology ID GENE-RELATED PEPTIDE; HUMAN DENTAL-PULP; MONODON-MONOCEROS-L; ACID SIGNATURE ANALYSIS; AGGRESSIVE TUSK USE; NERVE-FIBERS; SUBSTANCE-P; MECHANICAL-PROPERTIES; THERMAL-STIMULATION; HOUSEKEEPING GENES AB The erupted tusk of the narwhal exhibits sensory ability. The hypothesized sensory pathway begins with ocean water entering through cementum channels to a network of patent dentinal tubules extending from the dentinocementum junction to the inner pulpal wall. Circumpulpal sensory structures then signal pulpal nerves terminating near the base of the tusk. The maxillary division of the fifth cranial nerve then transmits this sensory information to the brain. This sensory pathway was first described in published results of patent dentinal tubules, and evidence from dissection of tusk nerve connection via the maxillary division of the fifth cranial nerve to the brain. New evidence presented here indicates that the patent dentinal tubules communicate with open channels through a porous cementum from the ocean environment. The ability of pulpal tissue to react to external stimuli is supported by immunohistochemical detection of neuronal markers in the pulp and gene expression of pulpal sensory nerve tissue. Final confirmation of sensory ability is demonstrated by significant changes in heart rate when alternating solutions of high-salt and fresh water are exposed to the external tusk surface. Additional supporting information for function includes new observations of dentinal tubule networks evident in unerupted tusks, female erupted tusks, and vestigial teeth. New findings of sexual foraging divergence documented by stable isotope and fatty acid results add to the discussion of the functional significance of the narwhal tusk. The combined evidence suggests multiple tusk functions may have driven the tooth organ system's evolutionary development and persistence. Anat Rec, 297:599-617, 2014. (c) 2014 Wiley Periodicals, Inc. C1 [Nweeia, Martin T.] Harvard Univ, Sch Dent Med, Dept Restorat Dent & Biomat Sci, Boston, MA 02115 USA. [Nweeia, Martin T.; Mead, James G.; Potter, Charles W.] Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20004 USA. [Nweeia, Martin T.] Harvard Univ, Museum Comparat Zool, Dept Organism & Evolutionary, Cambridge, MA 02138 USA. [Eichmiller, Frederick C.] Delta Dent Wisconsin, Stevens Point, WI 54481 USA. [Hauschka, Peter V.] Boston Childrens Hosp, Orthopaed Res Ctr, Boston, MA 02115 USA. [Hauschka, Peter V.] Harvard Univ, Sch Med, Dept Orthopaed Surg, Boston, MA 02115 USA. [Hauschka, Peter V.; Kuo, Winston P.] Harvard Univ, Sch Dent Med, Dept Dev Biol, Boston, MA 02115 USA. [Donahue, Gretchen A.] Univ Minnesota, Carlson Sch Management, Minneapolis, MN 55455 USA. [Orr, Jack R.] Fisheries & Oceans Canada, Arctic Res Div, Winnipeg, MB R3T 2N6, Canada. [Ferguson, Steven H.; Watt, Cortney A.] Fisheries & Oceans Canada, Inst Freshwater, Winnipeg, MB R3T 2N6, Canada. [Dietz, Rune] Aarhus Univ, Inst Biosci, Arctic Res Ctr, Roskilde, Denmark. [Giuseppetti, Anthony A.] Natl Inst Stand & Technol, ADAF Paffenbarger Res Ctr, Gaithersburg, MD 20899 USA. [Black, Sandie R.] Calgary Zoo, Calgary, AB T2E 7V6, Canada. [Trachtenberg, Alexander J.; Kuo, Winston P.] Harvard Univ, Sch Dent Med, Catalyst Lab Innovat Translat Technol, Boston, MA 02115 USA. RP Nweeia, MT (reprint author), Harvard Univ, Sch Dent Med, Dept Restorat Dent & Biomat Sci, 188 Longwood Ave, Boston, MA 02115 USA. EM Martin_nweeia@hsdm.harvard.edu RI Dietz, Rune/F-9154-2015 NR 153 TC 2 Z9 2 U1 15 U2 95 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1932-8486 EI 1932-8494 J9 ANAT REC JI Anat. Rec. PD APR PY 2014 VL 297 IS 4 BP 599 EP 617 DI 10.1002/ar.22886 PG 19 WC Anatomy & Morphology SC Anatomy & Morphology GA AC9XF UT WOS:000332887400001 PM 24639076 ER PT J AU Roberts, JM Cairns, SD AF Roberts, J. Murray Cairns, Stephen D. TI Cold-water corals in a changing ocean SO CURRENT OPINION IN ENVIRONMENTAL SUSTAINABILITY LA English DT Article ID LOPHELIA-PERTUSA SCLERACTINIA; EUROPEAN CONTINENTAL-MARGIN; GLOBAL HABITAT SUITABILITY; DEEP-WATER; PARAGORGIA-ARBOREA; ANTHROPOGENIC CO2; CARBONATE MOUNDS; DRILL CUTTINGS; ATLANTIC; REEFS AB Although known since Antiquity, corals in deep, cold waters remained largely unappreciated and overlooked by the scientific community until the 1990s. The last two decades have seen a dramatic increase in our understanding of these diverse ecosystems alongside growing realisation that many cold-water coral habitats had been degraded by bottom trawling and are threatened by ocean warming and acidification. This paper discusses recent improvements in our understanding of cold-water coral ecology, taxonomy and biodiversity following a variety of advances from the application of predictive mapping to the use of molecular phylogenetic approaches. Since many cold-water coral ecosystems occur in deep-waters beyond national jurisdiction, conservation management measures are being developed through the United Nations and related conventions. All such management measures require not only international agreement but also monitoring and enforcement to ensure their success. C1 [Roberts, J. Murray] Heriot Watt Univ, Sch Life Sci, Ctr Marine Biodivers & Biotechnol, Edinburgh EH14 4AS, Midlothian, Scotland. [Roberts, J. Murray] Scottish Assoc Marine Sci, Oban PA37 1QA, Argyll, Scotland. [Roberts, J. Murray] Univ N Carolina, Ctr Marine Sci, Wilmington, NC 28403 USA. [Cairns, Stephen D.] Smithsonian Inst, Natl Museum Amer Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Roberts, JM (reprint author), Heriot Watt Univ, Sch Life Sci, Ctr Marine Biodivers & Biotechnol, Edinburgh EH14 4AS, Midlothian, Scotland. EM j.m.roberts@hw.ac.uk RI Roberts, Murray/D-8299-2013 OI Roberts, Murray/0000-0003-1688-5133 FU Heriot-Watt University; UK Natural Environment Research Council [NE/J021121/1, NE/H017305/1] FX JMR acknowledges support from Heriot-Watt University's Environment and Climate Change theme and the UK Natural Environment Research Council (grants NE/J021121/1 and NE/H017305/1). Many thanks to Les Watling (University of Hawaii) for supplying the images of Metallogorgia melanotrichos and Ophiocreas oedipus and to the Holland-1 remotely operated vehicle team and the captain and crew of RRS James Cook cruise 073 for assistance at sea. NR 62 TC 14 Z9 14 U1 9 U2 79 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1877-3435 EI 1877-3443 J9 CURR OPIN ENV SUST JI Curr. Opin. Environ. Sustain. PD APR PY 2014 VL 7 BP 118 EP 126 DI 10.1016/j.cosust.2014.01.004 PG 9 WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Environmental Sciences SC Science & Technology - Other Topics; Environmental Sciences & Ecology GA AE5HV UT WOS:000334019300017 ER PT J AU DeBoer, GE Quellmalz, ES Davenport, JL Timms, MJ Herrmann-Abell, CF Buckley, BC Jordan, KA Huang, CW Flanagan, JC AF DeBoer, George E. Quellmalz, Edys S. Davenport, Jodi L. Timms, Michael J. Herrmann-Abell, Cari F. Buckley, Barbara C. Jordan, Kevin A. Huang, Chun-Wei Flanagan, Jean C. TI Comparing Three OnlineTesting Modalities: Using Static, Active, and Interactive OnlineTesting Modalities to Assess Middle School Students' Understanding of Fundamental Ideas and Use of Inquiry Skills Related to Ecosystems SO JOURNAL OF RESEARCH IN SCIENCE TEACHING LA English DT Article DE assessment; online testing; ecosystems; inquiry; integrated knowledge structures; science education ID SCIENCE SIMULATIONS; ASSESSMENT SYSTEMS; EXPERIMENTATION; VISUALIZATIONS; MODEL AB Online testing holds much promise for assessing students' complex science knowledge and inquiry skills. In the current study, we examined the comparative effectiveness of assessment tasks and test items presented in online modules that used either a static, active, or interactive modality. A total of 1,836 students from the classrooms of 22 middle school science teachers in 12 states participated in the study as part of normal classroom activities. Students took assessments in the three different modalities on three consecutive days. The assessments tested key concepts about ecosystems and students' ability to use inquiry skills in an ecosystems context. Our in-depth analyses focused on how the different modalities elicited specific content knowledge of ecosystems (e.g., producers, consumers, predator-prey relationships) and specific inquiry skills (e.g., designing and interpreting experiments). We also investigated student use of technology supports, such as replaying animations or inspecting graphs. The results showed that the interactive modality enabled the testing of more complex reasoning and that additional experience working in the online environment improved student performance for all the modalities, especially for the interactive modality. Each of the three modalities provided useful information about students' understanding of ecosystems and related inquiry skills as well as their misconceptions. The study begins to build a knowledge base of what types of science knowledge and skills may be effectively measured in three different modalities of online assessment. (c) 2014 Wiley Periodicals, Inc. J Res Sci Teach 51: 523-554, 2014 C1 [DeBoer, George E.; Herrmann-Abell, Cari F.] AAAS Project 2061, Washington, DC 20005 USA. [Quellmalz, Edys S.; Davenport, Jodi L.; Buckley, Barbara C.; Jordan, Kevin A.; Huang, Chun-Wei] WestEd, Redwood City, CA USA. [Timms, Michael J.] Australian Council Educ Res, Camberwell, Vic, Australia. [Flanagan, Jean C.] Smithsonian Inst, Washington, DC 20560 USA. RP DeBoer, GE (reprint author), AAAS Project 2061, 1200 New York Ave NW, Washington, DC 20005 USA. NR 74 TC 2 Z9 2 U1 4 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-4308 EI 1098-2736 J9 J RES SCI TEACH JI J. Res. Sci. Teach. PD APR PY 2014 VL 51 IS 4 BP 523 EP 554 DI 10.1002/tea.21145 PG 32 WC Education & Educational Research SC Education & Educational Research GA AC5YM UT WOS:000332596900005 ER PT J AU Pogue, MG AF Pogue, M. G. TI A Review of the Copitarsia decolora (Guen,e) (Lepidoptera: Noctuidae) Species Complex with the Description of a New Species from Chile and Argentina SO NEOTROPICAL ENTOMOLOGY LA English DT Review DE Cryptic species; morphology; agriculture; pests; distribution ID CUCULLIINAE AB Copitarsia gibberosa n. sp. is described from Chile and Argentina. Morphological characters are discussed to differentiate it from Copitarsia decolora (Guen,e), Copitarsia incommoda (Walker), and Copitarsia corruda (Pogue & Simmons). Copitarsia corruda has its status revised based on CO1 and morphology. Copitarsia paraturbata Castillo & Angulo is a new synonym of C. incommoda based on morphology. Copitarsia uncilata Burgos & Leiva is a new synonym of C. decolora based on morphology. A review of recent literature revealed a misunderstanding of the complex of species related to C. decolora, and these papers are evaluated and species are identified. Host plant utilization is discussed between C. decolora and C. corruda. Adults and male and female genitalia are illustrated to differentiate between the species in the C. decolora species complex. Keys to male and females based on genitalic morphology are given. Distribution maps of collected specimens are provided. C1 ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst, Washington, DC 20013 USA. RP Pogue, MG (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst, POB 37012, Washington, DC 20013 USA. EM michael.pogue@ars.usda.gov NR 13 TC 0 Z9 1 U1 1 U2 10 PU ENTOMOLOGICAL SOC BRASIL PI LONDRINA, PA CAIXA POSTAL 481, 86001-970 LONDRINA,, PR, BRAZIL SN 1519-566X EI 1678-8052 J9 NEOTROP ENTOMOL JI Neotrop. Entomol. PD APR PY 2014 VL 43 IS 2 BP 143 EP 153 DI 10.1007/s13744-013-0190-9 PG 11 WC Entomology SC Entomology GA AD3GI UT WOS:000333125900007 PM 27193521 ER PT J AU Labandeira, CC Tremblay, SL Bartowski, KE Hernick, LV AF Labandeira, Conrad C. Tremblay, Susan L. Bartowski, Kenneth E. Hernick, Linda VanAller TI Middle Devonian liverwort herbivory and antiherbivore defence SO NEW PHYTOLOGIST LA English DT Article DE arthropod; external foliage feeding; galling; herbivore; Metzgeriothallus; New York state; oil body cells; piercing-and-sucking ID ANT ATTA-CEPHALOTES; EASTERN NEW-YORK; LAND PLANTS; TERRESTRIAL ARTHROPODS; EPIPHYLLOUS LIVERWORTS; FOSSIL EVIDENCE; RHYNIE CHERT; INSECT; MARCHANTIOPHYTA; COLONIZATION AB To test the extent of herbivory in early terrestrial ecosystems, we examined compression-impression specimens of the late Middle Devonian liverwort Metzgeriothallus sharonae, from the Catskill Delta deposit of eastern New York state. Shale fragments of field-collected specimens were processed by applying liquid nitrocellulose on exposed surfaces. After drying, the film coatings were lifted off and mounted on microscope slides for photography. Unprocessed fragments were photographed under cedarwood oil for enhanced contrast. An extensive repertoire of arthropodan-mediated herbivory was documented, representing three functional feeding groups and nine subordinate plant-arthropod damage types (DTs). The herbivory is the earliest occurrence of external foliage-feeding and galling in the terrestrial fossil record. Our evidence indicates that thallus oil body cells, similar to the terpenoid-containing oil bodies of modern liverworts, were probably involved in the chemical defence of M. sharonae against arthropod herbivores. Based on damage patterns of terrestrial plants and an accompanying but sparse body-fossil record, Devonian arthropodan herbivores were significantly smaller compared to those of the later Palaeozoic. These data collectively suggest that a broad spectrum herbivory may have had a more important role in early terrestrial ecosystems than previously thought. C1 [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20010 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Univ Maryland, BEES Program, College Pk, MD 20742 USA. [Tremblay, Susan L.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Bartowski, Kenneth E.; Hernick, Linda VanAller] New York State Museum & Sci Serv, Albany, NY 12230 USA. RP Labandeira, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20010 USA. EM labandec@si.edu FU New York State Museum; University of California Museum of Paleontology FX We acknowledge the organizers of the Colonization of the Terrestrial Environment, held at the University of Bristol during September of 2010, where these data were initially presented. We thank P. Lee and M. Holden for scanning of images and F. Mannolini for help with photography. J. Hernick provided assistance for GPS data. Taehee Han and Victoria Chu provided UCMP laboratory assistance for assessing damage types. We are grateful to three anonymous reviewers, and to Bill Stein, who provided reviews of the manuscript. Financial support was provided by the New York State Museum to L.V.H. and K.E.B., and the University of California Museum of Paleontology to S.T. Finnegan Marsh adeptly drafted the figures. This is contribution 253 of the Evolution of Terrestrial Ecosystems consortium of the National Museum of Natural History, in Washington, DC, USA. NR 95 TC 13 Z9 13 U1 4 U2 33 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1469-8137 J9 NEW PHYTOL JI New Phytol. PD APR PY 2014 VL 202 IS 1 BP 247 EP 258 DI 10.1111/nph.12643 PG 12 WC Plant Sciences SC Plant Sciences GA AB4CX UT WOS:000331737900032 PM 24372344 ER PT J AU Emsens, WJ Hirsch, BT Kays, R Jansen, PA AF Emsens, Willem-Jan Hirsch, Ben T. Kays, Roland Jansen, Patrick A. TI Prey refuges as predator hotspots: ocelot (Leopardus pardalis) attraction to agouti (Dasyprocta punctata) dens SO ACTA THERIOLOGICA LA English DT Article DE Agouti; Behavior; Movement; Ocelot; Predation; Refuge ID FELIS-PARDALIS; RISK; VISIBILITY; PROXIMITY AB We tested the hypothesis that prey refuges attract predators, leading to elevated predator activity in the vicinity of refuges. We used camera traps to determine whether the spatial activity of a predator, the ocelot (Leopardus pardalis), was biased toward refuge locations of its principal prey, the agouti (Dasyprocta punctata). We radio-tracked agoutis at night to locate active refuges and compared the activity of ocelots between these refuges and surrounding control grid locations. We found that ocelots visited the area near agouti refuges significantly more often and for longer periods of time than control locations, and that they actively investigated the refuge entrances. Both occupied and unoccupied refuges were visited, but the duration of inspection was longer at occupied refuges. As the ocelots could probably not see the agoutis within the refuges, olfaction likely cued foraging ocelots. Two refuges were repeatedly visited by the same ocelots on different days, suggesting spatial memory. Overall, our results suggest that predators can be attracted to prey refuges or refuging prey. The benefits to prey of staying nearby a refuge would thus be counterbalanced by higher likelihoods of predator encounter. This should stimulate prey to use multiple refuges alternatingly and to not enter or exit refuges at times of high predator activity. C1 [Emsens, Willem-Jan; Hirsch, Ben T.; Kays, Roland; Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa, Panama. [Emsens, Willem-Jan; Jansen, Patrick A.] Wageningen Univ, Dept Environm Sci, NL-6700 AA Wageningen, Netherlands. [Emsens, Willem-Jan] Univ Antwerp, Dept Biol, Ecosyst Management Res Grp, B-2610 Antwerp, Belgium. [Hirsch, Ben T.] Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA. [Kays, Roland] North Carolina Museum Nat Sci, Raleigh, NC 27601 USA. [Kays, Roland] N Carolina State Univ, Program Fisheries Wildlife & Conservat Biol, Raleigh, NC 27695 USA. [Emsens, Willem-Jan] Univ Antwerp, B-2610 Antwerp, Belgium. RP Emsens, WJ (reprint author), Univ Antwerp, Univ Pl 1, B-2610 Antwerp, Belgium. EM w.emsens@gmail.com RI Jansen, Patrick/G-2545-2015 OI Jansen, Patrick/0000-0002-4660-0314 FU National Science Foundation [NSF-DEB-0717071]; Netherlands Foundation for Scientific Research [NWO-WOTRO W85-239, NWO-ALW 863-07-008] FX We thank Sumana Serchan and Matt McElroy for field assistance, and two anonymous reviewers for their comments on the manuscript. We thank the National Science Foundation (NSF-DEB-0717071 to RK) and the Netherlands Foundation for Scientific Research (NWO-WOTRO W85-239 and NWO-ALW 863-07-008 to PAJ) for financial support. NR 32 TC 7 Z9 7 U1 1 U2 37 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0001-7051 EI 2190-3743 J9 ACTA THERIOL JI Acta Theriol. PD APR PY 2014 VL 59 IS 2 BP 257 EP 262 DI 10.1007/s13364-013-0159-4 PG 6 WC Zoology SC Zoology GA AD3HF UT WOS:000333128200006 ER PT J AU Jones, PL Ryan, MJ Page, RA AF Jones, Patricia L. Ryan, Michael J. Page, Rachel A. TI Population and seasonal variation in response to prey calls by an eavesdropping bat SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Behavioral plasticity; Bat; Eavesdrop; Population differences; Seasonal variation; Trachops cirrhosus ID FROG-EATING BAT; FORAGING BEHAVIOR; TRACHOPS-CIRRHOSUS; LEARNING SPEED; EVOLUTION; PREDATION; CUES; ADVERTISEMENT; MORPHOLOGY; ABUNDANCE AB The fringe-lipped bat, Trachops cirrhosus, is an eavesdropping predator that hunts frogs and katydids by approaching these preys' sexual advertisement calls. In captivity, bats can rapidly learn to associate novel acoustic stimuli with food rewards. It is unknown how this learning ability is related to foraging behavior in the wild where prey and the calls that identify them vary over space and time. In two bat populations that differ in available prey species (Soberania, Panama, and La Selva, Costa Rica), we presented wild-caught bats with frog calls, katydid calls, and control stimuli. Bats in Soberania were significantly more responsive to complex calls and choruses of the tA(0)ngara frog, Physalaemus pustulosus, than were bats in La Selva. La Selva bats were significantly more responsive to katydid calls (Steirodon sp.) than Soberania bats. We also examined seasonal variation in bat response to prey cues. Bats were captured in Soberania in dry and wet seasons and presented with the calls of a dry season breeding frog (Smilisca sila), a wet season breeding frog (P. pustulosus), and four katydid species. Bats captured in the dry season were significantly more responsive to the calls of S. sila than bats captured in the wet season, but there were no seasonal differences in response to the calls of P. pustulosus or the katydid calls. We demonstrate plasticity in the foraging behavior of this eavesdropping predator but also show that response to prey cues is not predicted solely by prey availability. C1 [Jones, Patricia L.; Ryan, Michael J.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. [Jones, Patricia L.; Ryan, Michael J.; Page, Rachel A.] Smithsonian Trop Res Inst, Balboa, Panama. RP Jones, PL (reprint author), Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. EM patricia.jones@utexas.edu FU National Science Foundation; University of Texas at Austin; Smithsonian Tropical Research Institute FX We thank the staff of the Smithsonian Tropical Research Institute and the Organization for Tropical Studies for aid and support with research and permits in Soberania and in La Selva. Thank you to Hannah ter Hofstede for providing the katydid calls, and Ximena E. Bernal, Roberto Ibanez, A. Stanley Rand, and Michael Reichert for recording the frog calls. Thanks also to Sara Troxell, Sean Griffin, Martha Moscoso, Christina Buelow, Sarah Richman, Jay Falk, Teia Schweizer, and Victoria Flores for help capturing and caring for bats. We thank the Gamboa Bat Lab, Christian Voigt, Brock Fenton, and one anonymous reviewer for insightful comments on the manuscript. This study was funded by a National Science Foundation Graduate Research Fellowship (PLJ) as well as grants from the University of Texas at Austin (PLJ) and the Smithsonian Tropical Research Institute (PLJ). NR 44 TC 5 Z9 5 U1 0 U2 35 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 EI 1432-0762 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD APR PY 2014 VL 68 IS 4 BP 605 EP 615 DI 10.1007/s00265-013-1675-6 PG 11 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA AD1FL UT WOS:000332979400008 ER PT J AU Kettenring, KM Mercer, KL Adams, CR Hines, J AF Kettenring, Karin M. Mercer, Kristin L. Adams, Carrie Reinhardt Hines, Jes TI Application of genetic diversity- ecosystem function research to ecological restoration SO JOURNAL OF APPLIED ECOLOGY LA English DT Review DE community genetics; ecological restoration; ecosystem functions; ecosystem multifunctionality; ecosystem services; genetic diversity; genotype richness; genotypic diversity; plant materials; restoration genetics ID PLANT GENOTYPIC DIVERSITY; ADAPTIVE POPULATION DIVERGENCE; LOCAL ADAPTATION; COMMUNITY STRUCTURE; NATIVE POPULATIONS; TALLGRASS PRAIRIE; BIODIVERSITY; SERVICES; COMPLEMENTARITY; CONSERVATION AB Three common goals for restoration are (i) rapid plant establishment, (ii) long-term plant persistence and (iii) restoration of functioning ecosystems. Restoration practitioners often use cultivars optimized for rapid plant establishment under highly disturbed conditions to achieve the first goal; locally adapted genotypes are championed for the second because they can be well suited for local environmental conditions. Restoring functioning ecosystems is considered a loftier goal that practitioners struggle to achieve because we lack proven techniques. Similar to the demonstrated benefits of species, functional and phylogenetic diversity for ecosystem functions (EFs), recent genetic diversity (GD)-ecosystem function (EF) experiments have shown that increases in plant GD can positively influence many different EFs. Would the introduction of diverse plant genotypes of a given species into a restoration enhance ecosystem functioning and the evolutionary potential of restored populations? In this review, we first examine three propagule-sourcing approaches: cultivar, local adaptation and GD. Next, we raise questions that if addressed, could help practitioners implement a GD approach in restoration: (i) How might the selection, relatedness and arrangement of genotypes be optimized to restore functioning ecosystems, (ii) How do traits that affect an EF relate to neutral or adaptive diversity, more common measures of GD and (iii) at which spatial and temporal scales does GD influence EFs in restorations?Synthesis and applications. Although each propagule-sourcing approach may be best suited for a particular restoration goal, each approach may simultaneously benefit other goals. Yet cultivars and locally adapted populations that have experienced artificial and/or natural selection may not possess the levels of diversity that will confer expected benefits to different ecosystem functions. Future research should determine the relative value of each approach (or a combination of approaches) for simultaneously achieving multiple restoration goals. Restoration experiments, where plant genetic diversity (GD) is manipulated and monitored over scales relevant to restoration, could reveal the true promise of a GD approach to restoration. Although each propagule-sourcing approach may be best suited for a particular restoration goal, each approach may simultaneously benefit other goals. Yet cultivars and locally adapted populations that have experienced artificial and/or natural selection may not possess the levels of diversity that will confer expected benefits to different ecosystem functions. Future research should determine the relative value of each approach (or a combination of approaches) for simultaneously achieving multiple restoration goals. Restoration experiments, where plant genetic diversity (GD) is manipulated and monitored over scales relevant to restoration, could reveal the true promise of a GD approach to restoration. C1 [Kettenring, Karin M.] Utah State Univ, Ctr Ecol, Logan, UT 84322 USA. [Kettenring, Karin M.] Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA. [Kettenring, Karin M.; Hines, Jes] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Mercer, Kristin L.] Ohio State Univ, Dept Hort & Crop Sci, Columbus, OH 43210 USA. [Adams, Carrie Reinhardt] Univ Florida, Dept Environm Hort, Gainesville, FL 32611 USA. [Hines, Jes] Leibniz Inst Freshwater Ecol & Inland Fisheries, Dept Expt Limnol, Neuglobsow, Germany. RP Kettenring, KM (reprint author), Utah State Univ, Ctr Ecol, Logan, UT 84322 USA. EM karin.kettenring@usu.edu RI Mercer, Kristin/K-2000-2012; Hines, Jes/L-7668-2016 OI Hines, Jes/0000-0002-9129-5179 NR 90 TC 26 Z9 26 U1 21 U2 191 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8901 EI 1365-2664 J9 J APPL ECOL JI J. Appl. Ecol. PD APR PY 2014 VL 51 IS 2 BP 339 EP 348 DI 10.1111/1365-2664.12202 PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AC9DX UT WOS:000332835600007 ER PT J AU Canoville, A Thomas, DB Chinsamy, A AF Canoville, Aurore Thomas, Daniel B. Chinsamy, Anusuya TI Insights into the habitat of Middle Permian pareiasaurs ( Parareptilia) from preliminary isotopic analyses SO LETHAIA LA English DT Article DE Dinocephalians; Karoo Basin; palaeoecology; South Africa; therocephalians ID TOOTH ENAMEL; DIAGENETIC ALTERATION; TRIASSIC BOUNDARY; SOUTH-AFRICA; OXYGEN; EVOLUTION; CARBONATE; APATITE; WATER; PHOSPHATE AB Pareiasaurs were an abundant group of large herbivores during Middle and Late Permian times. The habitat of pareiasaurs has proven enigmatic, and ecological interpretations from anatomical and taphonomic data have included aquatic, semi-aquatic to fully terrestrial lifestyles. Insight into the ecology of extinct taxa can also be gained from stable isotope analyses, and interpretations benefit from studies of multiple, coeval groups. Here, we report the first stable carbon and oxygen isotope analyses from the enamel, dentine and bone of pareiasaurs and contemporaneous therapsids (dinocephalians and therocephalians), in specimens recovered from the Permian Tapinocephalus to lower Pristerognathus Assemblage Zones of South Africa. Previous ecological inferences for dinocephalians (riparian to terrestrial) and therocephalians (terrestrial) are less ambiguous than reconstructions for pareiasaurs and provide an independent reference for interpreting stable isotope measurements. Oxygen isotopes of enamel carbonate were indistinguishable between pareiasaurs and therocephalians, which had higher values than dinocephalians. The data suggest that dinocephalians and pareiasaurs (megaherbivores) inhabited different ecological niches and that pareiasaurs may have shared a terrestrial habitat with therocephalians (carnivores). Our results agree with earlier suggestions of a terrestrial lifestyle among pareiasaurs and provide evidence of niche partitioning among large coeval Capitanian herbivores of South Africa. C1 [Canoville, Aurore; Chinsamy, Anusuya] Univ Cape Town, Dept Biol Sci, ZA-7707 Cape Town, South Africa. [Thomas, Daniel B.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Canoville, A (reprint author), Univ Cape Town, Dept Biol Sci, Private Bag X3 Rhodes Gift, ZA-7707 Cape Town, South Africa. EM canoville.aurore08@gmail.com; thomasd@si.edu; anus-uya.chinsamy-turan@uct.ac.za FU Claude Leon Foundation; URC; Research and Innovation Department of the University of Cape Town; National Research Foundation of South Africa FX We thank Roger Smith and Sheena Kaal (Iziko South African Museum, Cape Town) for access to specimens, and Ian Newton (Department of Archaeology, University of Cape Town) for processing isotope samples. We received helpful comments from two anonymous referees and from Romain Amiot and Juan Carlos Cisneros. The Claude Leon Foundation, the URC and the Research and Innovation Department of the University of Cape Town as well as, the National Research Foundation of South Africa are acknowledged for research support for A. Canoville, D. Thomas and A. Chinsamy-Turan, respectively. Last but not least, we thank Lethaia editorial staff for its efficient handling of this manuscript. NR 66 TC 2 Z9 2 U1 3 U2 14 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-1164 EI 1502-3931 J9 LETHAIA JI Lethaia PD APR PY 2014 VL 47 IS 2 BP 266 EP 274 DI 10.1111/let.12056 PG 9 WC Paleontology SC Paleontology GA AC8IJ UT WOS:000332776400010 ER PT J AU Richardson, ML Rynear, J Peterson, CL AF Richardson, Matthew L. Rynear, Juliet Peterson, Cheryl L. TI Microhabitat of critically endangered Lupinus aridorum (Fabaceae) at wild and introduced locations in Florida scrub SO PLANT ECOLOGY LA English DT Article DE Cytotype; Gap specialist; Niche; Scrub lupine; Soil; Spatial distribution ID BIODIVERSITY HOTSPOTS; POPULATION VIABILITY; SPATIAL-DISTRIBUTION; PLANT; FIRE; SEED; ESTABLISHMENT; ENVIRONMENTS; COMMUNITIES; LIMITATION AB Elucidating microhabitat preferences of a rare species are critical for its conservation. Lupinus aridorum McFarlin ex Beckner (Fabaceae) is a critically endangered plant known only from a few locations in imperiled Florida scrub habitat and nothing is known about its preferred microhabitat. Our goals were threefold. First, determine whether L. aridorum has multiple cytotypes because this can influence its spatial distribution. Second, measure how microhabitat characteristics at locations supporting wild L. aridorum vary from random locations, which will provide information about microhabitat characteristics that influence the spatial distribution of individuals. Third, measure whether microhabitat characteristics differ between locations supporting wild or introduced plants, which will provide information about the realized and fundamental niche. Our research determined that L. aridorum is diploid and grew, on average, in areas closer to trees and shrubs, with lower soil moisture, and with a greater mixture of detritus than random locations. Some microhabitat characteristics at locations where L. aridorum were introduced were similar to microhabitat supporting wild L. aridorum, but multiple soil characteristics differed as did the plant community, which contained more nonnative plant species near introduced plants. Therefore, the realized niche is narrower than the fundamental niche. Overall, information about the microhabitat of L. aridorum can be used to design appropriate management programs to conserve and restore populations of this plant species and species that occupy a similar niche in imperiled Florida scrub. C1 [Richardson, Matthew L.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat Educ & Sustainabil, Washington, DC 20013 USA. [Rynear, Juliet; Peterson, Cheryl L.] Bok Tower Gardens, Rare Plant Conservat Program, Lake Wales, FL 33853 USA. RP Peterson, CL (reprint author), Bok Tower Gardens, Rare Plant Conservat Program, 1151 Tower Blvd, Lake Wales, FL 33853 USA. EM richardsonml@si.edu; cpeterson@boktower.org FU State of Florida, Department of Agriculture and Consumer Services, Division of Plant Industry [018698]; U.S. Fish and Wildlife Service [F09AP00047] FX We thank R. Schwendler for data entry, G. Bupp, J. Burns, D. Diener, K. Noland, M. Sheets, and L. Smith for assistance with field work, and anonymous reviewers for their productive comments. We also thank the City of Lake Alfred, the City of Orlando, Orange County Parks, the State of Florida, and the U. S. Fish and Wildlife Service, Lake Wales Ridge National Wildlife Refuge, for access to sites. Funding was provided by the State of Florida, Department of Agriculture and Consumer Services, Division of Plant Industry (Contract number 018698) and the U.S. Fish and Wildlife Service (Agreement number F09AP00047) to Bok Tower Gardens. NR 37 TC 0 Z9 0 U1 2 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 EI 1573-5052 J9 PLANT ECOL JI Plant Ecol. PD APR PY 2014 VL 215 IS 4 BP 399 EP 410 DI 10.1007/s11258-014-0310-6 PG 12 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA AD2GN UT WOS:000333052400003 ER PT J AU Greenwalt, DE Rust, J AF Greenwalt, Dale E. Rust, Jes TI A new species of Pseudotettigonia Zeuner (Orthoptera: Tettigoniidae) with an intact stridulatory field and reexamination of the subfamily Pseudotettigoniinae SO SYSTEMATIC ENTOMOLOGY LA English DT Article ID INSECTA; EVOLUTION; FRANCE AB Pseudotettigonia leona sp.n. is described from a single left forewing collected from the Middle Eocene Kishenehn Formation in northwestern Montana, U.S.A. P. leona is the second of only two fossil macropterous Tettigoniidae that preserve an intact stridulatory apparatus. The subfamily Pseudotettigoniinae is reexamined. The specific epithet bricei is assigned to the late Miocene fossil tettigoniid Tettigonia bricei sp.n., originally described as the extant Tettigonia viridissima. This published work has been registered in ZooBank, . C1 [Greenwalt, Dale E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Rust, Jes] Univ Bonn, Steinmann Inst, Dept Palaeontol, Bonn, Germany. RP Greenwalt, DE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, 10th & Constitut Ave NW,MRC 121, Washington, DC 20013 USA. EM GreenwaltD@si.edu NR 49 TC 4 Z9 4 U1 1 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0307-6970 EI 1365-3113 J9 SYST ENTOMOL JI Syst. Entomol. PD APR PY 2014 VL 39 IS 2 BP 256 EP 263 DI 10.1111/syen.12050 PG 8 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA AC5ZO UT WOS:000332599700005 ER PT J AU Messmer, T Elsenbeer, H Wilcke, W AF Messmer, Tobias Elsenbeer, Helmut Wilcke, Wolfgang TI High exchangeable calcium concentrations in soils on Barro Colorado Island, Panama SO GEODERMA LA English DT Article DE Panama; Cation-exchange capacity; Exchangeable Ca; Clay mineralogy; Weathering indices ID INTERSTRATIFIED KAOLINITE-SMECTITE; CHEMICAL-WEATHERING INDEXES; TROPICAL RAIN-FOREST; COSTA-RICA; PARENT-MATERIAL; PEDOGENIC FORMATION; NUTRIENT FLUXES; VOLCANIC SOILS; ROCKS; RED AB The soils on four lithologies (basaltic conglomerates, Bohio; Andesite; volcanoclastic sediments with basaltic agglomerates, Caimito volcanic; foraminiferal limestone, Caimito marine) on Barro Colorado Island (BCI have high exchangeable Ca concentrations and cation-exchange capacities (CEC) compared to other tropical soils on similar parent material. In the 0-10 cm layer of 24 mineral soils, pH values ranged from 5.7 (Caimito volcanic and Andesite) to 6.5 (Caimito marine), concentrations of exchangeable Ca from 134 mmol(c) kg(-1) (Caimito volcanic) to 585 mmolc kg-1 (Caimito marine), and cation exchange capacities from 317 mmol(c) kg(-1) (Caimito volcanic) to 933 mmol(c) kg(-1) (Caimito marine). X-ray diffractometry of the fraction <2 mu m revealed that smectites dominated the clay mineral assemblage in soil except on Caimito volcanic, where kaolinite was the dominant clay mineral. Exchangeable Ca concentrations decreased with increasing soil depth except on Caimito marine. The weathering indices Chemical Index of Alteration (CIA), Plagioclase Index of Alteration (PIA) and Weathering Index of Parker (WIP) determined for five soils on all geological formations, suggested that in contrast to expectation the topsoil (0-10 cm) appeared to be the least and the subsoil (50-70 cm) and saprolite (isomorphically weathered rock in the soil matrix) the most weathered. Additionally, the weathering indices indicated depletion of base cations and enrichment of Al-(hydr)oxides throughout the soil profile. Tree species did not have an effect on soil properties. Impeded leaching and the related occurrence of overland flow seem to be important in determining clay mineralogy. Our results suggest that (i) edaphic conditions favor the formation of smectites on most lithologies resulting in high CEC and thus high retention capacity for Ca and (ii) that there is an external source such as dust or sea spray deposition supplying Ca to the soils. (C) 2013 Elsevier B.V. All rights reserved. C1 [Messmer, Tobias; Wilcke, Wolfgang] Univ Bern, Inst Geog, CH-3012 Bern, Switzerland. [Elsenbeer, Helmut] Univ Potsdam, Inst Earth & Environm Sci, D-14476 Potsdam, Germany. [Elsenbeer, Helmut] Smithsonian Trop Res Inst, Balboa, Panama. RP Wilcke, W (reprint author), Univ Bern, Inst Geog, Hallerstr 12, CH-3012 Bern, Switzerland. EM wolfgang.wilcke@giub.unibe.ch RI Wilcke, Wolfgang/P-4620-2016 OI Wilcke, Wolfgang/0000-0002-6031-4613 FU German Research Foundation (DFG) [Wi1601/14-1]; Smithsonian Tropical Research Institute FX We thank Oris Acevedo and Belkys Jimenez for their organizational and logistical support on BCI, the late Elisabeth K.V. Kalko, Larissa Albrecht and Inga Geipel for their helpful advices about and introduction to BCI, the Smithsonian Tropical Research Institute (STRI) for granting access to its research station, the Panamanian authorities (ANAM) for the export permit, the German Research Foundation (DFG, Wi1601/14-1) for financial support, and one reviewer for insightful comments on an earlier version of this manuscript. H. E. acknowledges support by the Smithsonian Tropical Research Institute during his sabbatical in 2012. We also thank the head of the XRD lab, Urs Eggenberger and the technical assistance Christine Lemp at the Institute of Geology in Bern for their instruction in XRD-measurements and Daniela Fischer for XRF-measurements. NR 85 TC 3 Z9 3 U1 3 U2 38 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0016-7061 EI 1872-6259 J9 GEODERMA JI Geoderma PD APR PY 2014 VL 217 BP 212 EP 224 DI 10.1016/j.geoderma.2013.10.021 PG 13 WC Soil Science SC Agriculture GA AB0PY UT WOS:000331495800023 ER PT J AU Dent, WRF Wyatt, MC Roberge, A Augereau, JC Casassus, S Corder, S Greaves, JS de Gregorio-Monsalvo, I Hales, A Jackson, AP Hughes, AM Lagrange, AM Matthews, B Wilner, D AF Dent, W. R. F. Wyatt, M. C. Roberge, A. Augereau, J-C Casassus, S. Corder, S. Greaves, J. S. de Gregorio-Monsalvo, I. Hales, A. Jackson, A. P. Hughes, A. Meredith Lagrange, A-M Matthews, B. Wilner, D. TI Molecular Gas Clumps from the Destruction of Icy Bodies in the beta Pictoris Debris Disk SO SCIENCE LA English DT Article ID CIRCUMSTELLAR DISK; PLANET FORMATION; GIANT PLANET; COLLISIONS; DUST; CO; STARS; VEGA; MYR AB Many stars are surrounded by disks of dusty debris formed in the collisions of asteroids, comets, and dwarf planets, but is gas also released in such events? Observations at submillimeter wavelengths of the archetypal debris disk around beta Pictoris show that 0.3% of a Moon mass of carbon monoxide orbits in its debris belt. The gas distribution is highly asymmetric, with 30% found in a single clump 85 astronomical units from the star, in a plane closely aligned with the orbit of the inner planet, beta Pictoris b. This gas clump delineates a region of enhanced collisions, either from a mean motion resonance with an unseen giant planet or from the remnants of a collision of Mars-mass planets. C1 [Dent, W. R. F.; Corder, S.; de Gregorio-Monsalvo, I.; Hales, A.] Atacama Large Millimeter Submillimeter Array ALMA, Santiago Cent Off, Santiago, Chile. [Wyatt, M. C.; Jackson, A. P.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Roberge, A.] NASA, Exoplanets & Stellar Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Augereau, J-C; Lagrange, A-M] Univ Grenoble 1, CNRS, Inst Planetol & Astrophys Grenoble, Inst Natl Sci Univers,UMR 5274, F-38041 Grenoble, France. [Casassus, S.] Univ Chile, Dept Astron, Santiago, Chile. [Greaves, J. S.] Univ St Andrews, Dept Astron, St Andrews, Fife, Scotland. [de Gregorio-Monsalvo, I.] European So Observ, D-85748 Garching, Germany. [Jackson, A. P.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Hughes, A. Meredith] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA. [Matthews, B.] Natl Res Council Canada, Herzberg Astron Program, Victoria, BC V9E 2E7, Canada. [Matthews, B.] Natl Res Council Canada, Astrophys Program, Victoria, BC V9E 2E7, Canada. [Matthews, B.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Wilner, D.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Dent, WRF (reprint author), Atacama Large Millimeter Submillimeter Array ALMA, Santiago Cent Off, Alonso de Cordova 3107,Casilla 763 0355, Santiago, Chile. EM wdent@alma.cl RI Roberge, Aki/D-2782-2012; Casassus, Simon/I-8609-2016 OI Roberge, Aki/0000-0002-2989-3725; FU Millenium Nucleus (Chilean Ministry of Economy) [P10-022-F]; Goddard Center for Astrobiology, part of the NASA Astrobiology Institute; European Union through European Research Council [279973]; Ministerio de Ciencia e Innovacion (Spain) [AYA2011-30228-C03]; Science and Technology Facilities Council; French National Research Agency (ANR) [ANR-2010 BLAN-0505-01] FX This paper makes use of the following ALMA data: ADS/JAO. ALMA#2011.0.00087. S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and National Institute of Natural Sciences (Japan), together with National Research Council (Canada) and National Science Council and Academia Sinica Institute of Astronomy and Astrophysics (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, Associated Universities, Inc./National Radio Astronomy Observatory and National Astronomical Observatory of Japan. Partial financial support for S. Casassus, M. C. W. and A. H. was provided by Millenium Nucleus P10-022-F (Chilean Ministry of Economy). A. R. acknowledges support by the Goddard Center for Astrobiology, part of the NASA Astrobiology Institute. M. C. W. was supported by the European Union through European Research Council grant number 279973, I.d. G.-M. acknowledges support from Ministerio de Ciencia e Innovacion (Spain) grant number AYA2011-30228-C03 (including European Funds for Economic and Regional Development), A.P.J. was supported by a Science and Technology Facilities Council postgraduate studentship, and J.-C.A. acknowledges the French National Research Agency (ANR) for support through contract number ANR-2010 BLAN-0505-01 (EXOZODI). NR 28 TC 57 Z9 57 U1 2 U2 8 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAR 28 PY 2014 VL 343 IS 6178 BP 1490 EP 1492 DI 10.1126/science.1248726 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AD7TZ UT WOS:000333471000041 PM 24603151 ER PT J AU Gharaibeh, MF El Hassan, N Al Shorman, MM Bizau, JM Cubaynes, D Guilbaud, S Sakho, I Blancard, C McLaughlin, BM AF Gharaibeh, M. F. El Hassan, N. Al Shorman, M. M. Bizau, J. M. Cubaynes, D. Guilbaud, S. Sakho, I. Blancard, C. McLaughlin, B. M. TI K-shell photoionization of B-like atomic nitrogen ions: experiment and theory SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article DE photoionization; K-shell; nitrogen ions; cross sections ID BORON ISOELECTRONIC SEQUENCE; PHOTOABSORPTION CROSS-SECTIONS; DOUBLY-EXCITED RESONANCES; R-MATRIX THEORY; CONFIGURATION-INTERACTION; OSCILLATOR-STRENGTHS; AUGER; OXYGEN; SPECTROSCOPY; TRANSITIONS AB Measurements of absolute cross sections for the K-shell photoionization of B-like atomic nitrogen ions were carried out utilizing the ion-photon merged-beam technique at the SOLEIL synchrotron radiation facility in Saint-Aubin, France. High-resolution spectroscopy with E/Delta E approximate to 13,500 was the maximum resolution achieved. We have investigated two photon energy regions: 404-409 eV and 439-442 eV. Resonance peaks found in the experimental measured cross sections are compared with theoretical estimates from the multi-configuration Dirac-Fock, R-matrix and empirical methods, allowing identification of the strong 1s -> 2p and the weaker 1s -> 3p resonances in the observed K-shell spectra of this B-like nitrogen ion. C1 [Gharaibeh, M. F.] Jordan Univ Sci & Technol, Dept Phys, Irbid 22110, Jordan. [El Hassan, N.; Al Shorman, M. M.; Bizau, J. M.; Cubaynes, D.; Guilbaud, S.] Univ Paris 11, ISMO, CNRS UMR 8214, F-91405 Orsay, France. [Bizau, J. M.; Cubaynes, D.] Synchrotron SOLEIL LOrme des Merisiers, F-91192 Gif Sur Yvette, France. [Sakho, I.] Univ Assane Seck Ziguinchor, UFR Sci & Technol, Dept Phys, Ziguinchor, Senegal. [Blancard, C.] CEA DAM DIF, F-91297 Bruyeres Le Chatel, Arpajon, France. [McLaughlin, B. M.] Queens Univ Belfast, Ctr Theoret Atom Mol & Opt Phys CTAMOP, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys ITAMP, Cambridge, MA 02138 USA. RP Bizau, JM (reprint author), Univ Paris 11, ISMO, CNRS UMR 8214, Bat 350, F-91405 Orsay, France. EM jean-marc.bizau@u-psud.fr; b.mclaughlin@qub.ac.uk FU US National Science Foundation; Queen's University Belfast; National Science Foundation [OCI-1053575] FX The experimental measurements were performed on the PLEIADES beamline [48, 49], at the SOLEIL Synchrotron radiation facility in Saint-Aubin, France. The authors would like to thank the SOLEIL staff and, in particular those of the PLEIADES beam line for their helpful assistance, C Miron, Xiao-Jing Liu, E Robert and C Nicolas. B M McLaughlin acknowledges support from the US National Science Foundation through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics, the RTRA network Triangle de le Physique and a visiting research fellowship from Queen's University Belfast. I Sakho acknowledges the hospitality of the Universite Paris-Sud and support from the University Assane Seck of Ziguinchor during a recent visit. We thank John C Raymond and Randall K Smith at the Harvard-Smithsonian Center for Astrophysics for discussions on the astrophysical applications and Javier Garcia for numerical values of the cross sections [38]. The computational work was carried out 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. We thank Stefan Andersson from Cray Research for his advice and assistance with the implementation and optimization of the parallel R-matrix codes on the Cray-XE6 at HLRS. The Kraken XT5 facility is a resource of the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number OCI-1053575. NR 79 TC 12 Z9 12 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD MAR 28 PY 2014 VL 47 IS 6 AR 065201 DI 10.1088/0953-4075/47/6/065201 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AC9EC UT WOS:000332836200003 ER PT J AU Zatsarinny, O Bartschat, K AF Zatsarinny, Oleg Bartschat, Klaus TI Benchmark calculation of total cross sections for ionization-excitation of helium SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article DE electron-helium collisions; simultaneous ionization-excitation; B-spline R-matrix; total cross sections ID ELECTRON-HYDROGEN COLLISIONS; IMPACT; SCATTERING; HE; MODEL AB The total cross section for simultaneous ionization-excitation of helium by electron impact has been revisited within the framework of the fully nonperturbative B-spline R-matrix with pseudostates approach. A long-standing discrepancy regarding the absolute normalization of the cross section for ionization with simultaneous excitation of the residual ion into the He+(2p) is resolved in favour of the values suggested by Bloemen et al (1981 J. Phys. B: At. Mol. Phys. 14 717) and Forand et al (1985 J. Phys. B: At. Mol. Phys. 18 1409) rather than the renormalization proposed by Merabet et al (2003 J. Phys. B: At. Mol. Opt. Phys. 36 3383). C1 [Zatsarinny, Oleg; Bartschat, Klaus] Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. [Bartschat, Klaus] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Zatsarinny, O (reprint author), Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. EM oleg.zatsarinny@drake.edu; klaus.bartschat@drake.edu FU United States National Science Foundation [PHY-1068140, PHY-1212450]; NSF; [PHY-090031] FX This work was supported by the United States National Science Foundation through grants no PHY-1068140 and PHY-1212450 as well as XSEDE resources provided under grant no PHY-090031. The calculations were carried out on Gordon at the San Diego Supercomputer Center and Stampede at the Texas Advanced Computing Center in Austin. KB also acknowledges partial support from the NSF through a grant to the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University and the Harvard-Smithsonian Center for Astrophysics. NR 31 TC 12 Z9 12 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD MAR 28 PY 2014 VL 47 IS 6 AR 061001 DI 10.1088/0953-4075/47/6/061001 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AC9EC UT WOS:000332836200001 ER PT J AU Martinez-Garcia, R Calabrese, JM Lopez, C AF Martinez-Garcia, Ricardo Calabrese, Justin M. Lopez, Cristobal TI Optimal search in interacting populations: Gaussian jumps versus Levy flights SO PHYSICAL REVIEW E LA English DT Article ID CONTEXT; STRATEGIES; PREDATORS; MOVEMENT; PATTERNS; WALKS AB We investigated the relationships between search efficiency, movement strategy, and nonlocal communication in the biological context of animal foraging. We considered situations where the members of a population of foragers perform either Gaussian jumps or Levy flights, and show that the search time is minimized when communication among individuals occurs at intermediate ranges, independently of the type of movement. Additionally, while Brownian strategies are more strongly influenced by the communication mechanism, Levy flights still result in shorter overall search durations. C1 [Martinez-Garcia, Ricardo; Lopez, Cristobal] Inst Fis Interdisciplinar & Sistemas Complejos CS, IFISC, E-07122 Palma De Mallorca, Spain. [Calabrese, Justin M.] Natl Zool Pk, Conservat Ecol Ctr, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 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; MINECO (Spain); FEDER (EU) [FIS2012-30634 (Intense-COSYP), CTM2012-39025-C02-01 (ESCOLA)]; US National Science Foundation [ABI-1062411] FX R.M.-G. is supported by the JAEPredoc program of CSIC. R.M.-G. and C.L. acknowledge support from MINECO (Spain) and FEDER (EU) through Grants No. FIS2012-30634 (Intense-COSYP) and No. CTM2012-39025-C02-01 (ESCOLA). J.M.C. is supported by US National Science Foundation Grant No. ABI-1062411. We thank Federico Vazquez for fruitful discussions. NR 39 TC 5 Z9 5 U1 0 U2 13 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1539-3755 EI 1550-2376 J9 PHYS REV E JI Phys. Rev. E PD MAR 26 PY 2014 VL 89 IS 3 AR 032718 DI 10.1103/PhysRevE.89.032718 PG 8 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA AE1BG UT WOS:000333699900007 PM 24730885 ER PT J AU Kaufman, JP Miller, NJ Shimon, M Barkats, D Bischoff, C Buder, I Keating, BG Kovac, JM Ade, PAR Aikin, R Battle, JO Bierman, EM Bock, JJ Chiang, HC Dowell, CD Duband, L Filippini, J Hivon, EF Holzapfel, WL Hristov, VV Jones, WC Kernasovskiy, SS Kuo, CL Leitch, EM Mason, PV Matsumura, T Nguyen, HT Ponthieu, N Pryke, C Richter, S Rocha, G Sheehy, C Su, M Takahashi, YD Tolan, JE Yoon, KW AF Kaufman, J. P. Miller, N. J. Shimon, M. Barkats, D. Bischoff, C. Buder, I. Keating, B. G. Kovac, J. M. Ade, P. A. R. Aikin, R. Battle, J. O. Bierman, E. M. Bock, J. J. Chiang, H. C. Dowell, C. D. Duband, L. Filippini, J. Hivon, E. F. Holzapfel, W. L. Hristov, V. V. Jones, W. C. Kernasovskiy, S. S. Kuo, C. L. Leitch, E. M. Mason, P. V. Matsumura, T. Nguyen, H. T. Ponthieu, N. Pryke, C. Richter, S. Rocha, G. Sheehy, C. Su, M. Takahashi, Y. D. Tolan, J. E. Yoon, K. W. TI Self-calibration of BICEP1 three-year data and constraints on astrophysical polarization rotation SO PHYSICAL REVIEW D LA English DT Article ID MICROWAVE BACKGROUND POLARIZATION; ANISOTROPY AB Cosmic microwave background (CMB) polarimeters aspire to measure the faint B-mode signature predicted to arise from inflationary gravitational waves. They also have the potential to constrain cosmic birefringence, rotation of the polarization of the CMB arising from parity-violating physics, which would produce nonzero expectation values for the CMB's temperature to B-mode correlation (TB) and E-mode to B-mode correlation (EB) spectra. However, instrumental systematic effects can also cause these TB and EB correlations to be nonzero. In particular, an overall miscalibration of the polarization orientation of the detectors produces TB and EB spectra which are degenerate with isotropic cosmological birefringence, while also introducing a small but predictable bias on the BB spectrum. We find that BICEP1 three-year spectra, which use our standard calibration of detector polarization angles from a dielectric sheet, are consistent with a polarization rotation of alpha = -2.77 degrees +/- 0.86 degrees (statistical) +/- 1.3 degrees (systematic). We have revised the estimate of systematic error on the polarization rotation angle from the two-year analysis by comparing multiple calibration methods. We also account for the (negligible) impact of measured beam systematic effects. We investigate the polarization rotation for the BICEP1 100 GHz and 150 GHz bands separately to investigate theoretical models that produce frequency-dependent cosmic birefringence. We find no evidence in the data supporting either of these models or Faraday rotation of the CMB polarization by the Milky Way galaxy's magnetic field. If we assume that there is no cosmic birefringence, we can use the TB and EB spectra to calibrate detector polarization orientations, thus reducing bias of the cosmological B-mode spectrum from leaked E-modes due to possible polarization orientation miscalibration. After applying this "self-calibration" process, we find that the upper limit on the tensor-to-scalar ratio decreases slightly, from r < 0.70 to r < 0.65 at 95% confidence. C1 [Kaufman, J. P.; Shimon, M.; Keating, B. G.; Bierman, E. M.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Miller, N. J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Shimon, M.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Barkats, D.] ESO, Joint ALMA Observ, Santiago 19001, Chile. [Bischoff, C.; Buder, I.; Kovac, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ade, P. A. R.] Univ Wales Coll Cardiff, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Aikin, R.; Bock, J. J.; Filippini, J.; Hristov, V. V.; Mason, P. V.; Richter, S.; Rocha, G.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Battle, J. O.; Bock, J. J.; Dowell, C. D.; Nguyen, H. T.; Rocha, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chiang, H. C.] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Duband, L.] Commissariat Energie Atom, SBT, F-38054 Grenoble, France. [Hivon, E. F.] Inst Astrophys, F-75014 Paris, France. [Holzapfel, W. L.; Takahashi, Y. D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Kernasovskiy, S. S.; Kuo, C. L.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Palo Alto, CA 94305 USA. [Kernasovskiy, S. S.; Kuo, C. L.; Tolan, J. E.; Yoon, K. W.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Leitch, E. M.; Sheehy, C.] Univ Chicago, Chicago, IL 60637 USA. [Matsumura, T.] KEK, High Energy Accelerator Res Org, Tsukuba, Ibaraki 3050801, Japan. [Ponthieu, N.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Su, M.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Su, M.] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. RP Kaufman, JP (reprint author), Univ Calif San Diego, Dept Phys, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM jkaufman@physics.ucsd.edu RI Holzapfel, William/I-4836-2015; OI Barkats, Denis/0000-0002-8971-1954; Hivon, Eric/0000-0003-1880-2733 FU NSF [OPP-0230438, AST-1255358]; Caltech Presidents Discovery Fund; Caltech Presidents Fund [PF-471]; JPL Research and Technology Development Fund; Harvard College Observatory; Alfred P. Sloan Research Fellowship; NSF PECASE Award [AST-0548262]; NASA Postdoctoral Program at Goddard Space Flight Center; Joan and Irwin Jacobs FX BICEP1 was supported by NSF Grant No. OPP-0230438, Caltech Presidents Discovery Fund, Caltech Presidents Fund PF-471, JPL Research and Technology Development Fund, and the late J. Robinson. This analysis was supported in part by NSF CAREER Award No. AST-1255358 and the Harvard College Observatory, and J. M. K. acknowledges support from an Alfred P. Sloan Research Fellowship. B. G. K acknowledges support from NSF PECASE Award No. AST-0548262. N. J. M.' s research was supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. M. S. acknowledges support from a grant from Joan and Irwin Jacobs. We thank the South Pole Station staff for helping make our observing seasons a success. We also thank our colleagues in the ACBAR, BOOMERANG, QUAD, BOLOCAM, SPT, WMAP and Planck experiments, as well as Kim Griest, Amit Yadav, and Casey Conger for advice and helpful discussions, and Kathy Deniston and Irene Coyle for logistical and administrative support. We thank Patrick Shopbell for computational support at Caltech and the FAS Science Division Research Computing Group at Harvard University for providing support to run all the computations for this paper on the Odyssey cluster. NR 38 TC 28 Z9 28 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD MAR 24 PY 2014 VL 89 IS 6 AR 062006 DI 10.1103/PhysRevD.89.062006 PG 11 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AE9EU UT WOS:000334308800004 ER PT J AU Gonzalez, BA Orozco-terWengel, P von Borries, R Johnson, WE Franklin, WL Marin, JC AF Gonzalez, Benito A. Orozco-terWengel, Pablo von Borries, Rainer Johnson, Warren E. Franklin, William L. Marin, Juan C. TI Maintenance of Genetic Diversity in an Introduced Island Population of Guanacos after Seven Decades and Two Severe Demographic Bottlenecks: Implications for Camelid Conservation SO PLOS ONE LA English DT Article ID SOUTH-AMERICAN CAMELIDS; ALLELE FREQUENCY DATA; LAMA-GUANICOE; MICROSATELLITE MARKERS; NUMBER; ARTIODACTYLA; ARGENTINA; SOFTWARE; CHILE; UNITS AB Fifteen guanacos were introduced to Staats Island in the Falklands/Malvinas archipelago from Patagonia in the 1930s. Twenty five years later, the population was culled from 300 to 10-20 individuals, but quickly rebounded to a population of almost 400 animals that today retain the genetic signature of the founding event and later bottleneck. The goals of this study were to (i) make a genetic assessment of this island population through comparisons with mainland populations and simulations, and (ii) assess the likely source-population of the introduced guanacos. Genetic variation was estimated from 513 bp of mitochondrial DNA sequence and 15 microsatellite loci among 154 guanacos collected from eight localities, including the adjacent mainland and the islands of Tierra del Fuego and Staats Island. Of the 23 haplotypes observed among our samples, the Staats Island population only contained three haplotypes, all of which were shared with the coastal Monte Leon population in southern Patagonia. Mitochondrial DNA and microsatellite variations on Staats Island were comparable to most mainland populations and greater than those observed on Tierra del Fuego. Patterns of genetic structure suggest that the Staats Island guanaco population was founded with animals from southern Patagonia (as opposed to northern Patagonia or Tierra del Fuego), but that effective reductions in population size lasted only a few generations and that surviving animals were a random sample of the pre-bottleneck genetic variation. C1 [Gonzalez, Benito A.] Univ Chile, Fac Ciencias Forestales & Conservac Nat, Lab Ecol Vida Silvestre, Santiago, Chile. [Orozco-terWengel, Pablo] Cardiff Univ, Sch Biosci, Cardiff CF10 3AX, S Glam, Wales. [von Borries, Rainer] Univ Chile, Fac Med, Santiago 7, Chile. [Johnson, Warren E.] Smithsonian Inst, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Franklin, William L.] Iowa State Univ, Dept Nat Resource Ecol & Management, Ames, IA USA. [Marin, Juan C.] Univ Bio Bio, Fac Ciencias, Lab Genom & Biodiversidad, Chillan, Chile. RP Marin, JC (reprint author), Univ Bio Bio, Fac Ciencias, Lab Genom & Biodiversidad, Chillan, Chile. EM jcmarin@ubiobio.cl RI Gonzalez, Benito/I-9570-2014; Johnson, Warren/D-4149-2016 OI Gonzalez, Benito/0000-0001-8201-8789; Johnson, Warren/0000-0002-5954-186X FU Falkland Research Expeditions; Hidden Corners Inc.; Turner Foundation; University of South Florida; Comision Nacional de Investigacion, Ciencia y Tecnologia (CONICYT) [3050046] FX This work was partially funded by Falkland Research Expeditions, Hidden Corners Inc., Turner Foundation, University of South Florida, and the Comision Nacional de Investigacion, Ciencia y Tecnologia (CONICYT, Post-Doctoral grants No 3050046). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 79 TC 2 Z9 2 U1 2 U2 22 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAR 24 PY 2014 VL 9 IS 3 AR e91714 DI 10.1371/journal.pone.0091714 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AD7QO UT WOS:000333459900027 PM 24663026 ER PT J AU Norrbom, AL Castillo-Meza, AL Garcia-Chavez, JH Aluja, M Rull, J AF Norrbom, Allen L. Lucia Castillo-Meza, Ana Hector Garcia-Chavez, Juan Aluja, Martin Rull, Juan TI A new species of Anastrepha (Diptera: Tephritidae) from Euphorbia tehuacana (Euphorbiaceae) in Mexico SO ZOOTAXA LA English DT Article DE fruit flies; taxonomy; host plant ID CLADE AB Anastrepha tehuacana, a new species of Tephritidae (Diptera) from Tehuacan, Puebla, Mexico reared from seeds of Euphorbia tehuacana (Brandegee) V.W. Steinm. (Euphorbiaceae), is described and illustrated. Its probable relationship to A. relicta Hernandez-Ortiz is discussed. C1 [Norrbom, Allen L.] ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, Washington, DC 20013 USA. [Lucia Castillo-Meza, Ana; Hector Garcia-Chavez, Juan] Benemerita Univ Autonoma Puebla, Escuela Biol, Puebla, Mexico. [Aluja, Martin; Rull, Juan] Inst Ecol AC, Xalapa, Veracruz, Mexico. RP Norrbom, AL (reprint author), ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM allen.norrbom@ars.usda.gov FU Terrence Walters (USDA, APHIS, CPHST) FX Jerrett McCormick, Lucrecia Rodriguez, George Venable, and Taina Litwak helped to produce or enhance some of the illustrations, and Terrence Walters (USDA, APHIS, CPHST) secured funding for some of the illustration work. We especially thank Vicente Hernandez-Ortiz (IEXA) for reexamining the types of A. relicta, and he and Roberto Zucchi (Universidade do Sao Paulo) and Cheslavo Korytkowski (Universidad de Panama) for comments on previous drafts of the manuscript. USDA is an equal opportunity provider and employer. NR 15 TC 0 Z9 0 U1 1 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 24 PY 2014 VL 3780 IS 3 BP 567 EP 576 PG 10 WC Zoology SC Zoology GA AD3VJ UT WOS:000333174000008 PM 24871852 ER PT J AU Gould, A Yee, JC AF Gould, Andrew Yee, Jennifer C. TI MICROLENS MASSES FROM ASTROMETRY AND PARALLAX IN SPACE-BASED SURVEYS: FROM PLANETS TO BLACK HOLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; gravitational lensing: micro; planetary systems ID EVENTS AB We show that space-based microlensing experiments can recover lens masses and distances for a large fraction of all events (those with individual photometric errors less than or similar to 0.01 mag) using a combination of one-dimensional microlens parallaxes and astrometric microlensing. This will provide a powerful probe of the mass distributions of planets, black holes, and neutron stars, the distribution of planets as a function of Galactic environment, and the velocity distributions of black holes and neutron stars. While systematics are in principle a significant concern, we show that it is possible to vet against all systematics (known and unknown) using single-epoch precursor observations with the Hubble Space Telescope roughly 10 years before the space mission. C1 [Gould, Andrew] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Yee, Jennifer C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gould, A (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. FU NSF [AST 1103471]; NASA [NNX12AB99G]; NASA through the Sagan Fellowship Program FX Work by A.G. was supported by NSF grant AST 1103471 and NASA grant NNX12AB99G. Work by J.C.Y. was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. NR 16 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 64 DI 10.1088/0004-637X/784/1/64 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000064 ER PT J AU Huang, JS Rigopoulou, D Magdis, G Rowan-Robinson, M Dai, Y Bock, JJ Burgarella, D Chapman, S Clements, DL Cooray, A Farrah, D Glenn, J Oliver, S Smith, AJ Wang, L Page, M Riechers, D Roseboom, I Symeonidis, M Fazio, GG Yun, M Webb, TMA Efstathiou, A AF Huang, J. -S. Rigopoulou, D. Magdis, G. Rowan-Robinson, M. Dai, Y. Bock, J. J. Burgarella, D. Chapman, S. Clements, D. L. Cooray, A. Farrah, D. Glenn, J. Oliver, S. Smith, A. J. Wang, L. Page, M. Riechers, D. Roseboom, I. Symeonidis, M. Fazio, G. G. Yun, M. Webb, T. M. A. Efstathiou, A. TI HerMES: SPECTRAL ENERGY DISTRIBUTIONS OF SUBMILLIMETER GALAXIES AT z > 4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: formation; infrared: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; SIMILAR-TO 2; HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; MOLECULAR GAS; MIDINFRARED SPECTROSCOPY; STARBURST GALAXY; PHOTOMETRIC REDSHIFTS; LUMINOUS STARBURSTS; SPACE-TELESCOPE AB We present a study of the infrared properties for a sample of seven spectroscopically confirmed submillimeter galaxies (SMGs) at z > 4.0. By combining ground-based near-infrared, Spitzer IRAC and MIPS, Herschel SPIRE, and ground-based submillimeter/millimeter photometry, we construct their spectral energy distributions (SEDs) and a composite model to fit the SEDs. The model includes a stellar emission component at lambda(rest) < 3.5 mu m ot dust component peaking at lambda(rest) similar to 5 mu m and cold dust component which becomes significant for lambda(rest) > 50 mu m. Six objects in the sample are detected at 250 and 350 mu m. The dust temperatures for the sources in this sample are in the range of 40-80 K, and their LFIR similar to 10(13) L circle dot qualifies them as hyper-luminous infrared galaxies. The mean FIR-radio index for this sample is around q = 2.2 indicating no radio excess in their radio emission. Most sources in the sample have 24 mu m detections corresponding to a rest-frame 4.5 mu m luminosity of Log(10)(L-4.5/L circle dot) = 11 similar to 11.5. Their L4.5/L-FIR ratios are very similar to those of starburst-dominated SMGs at z similar to 2. The LCO -LFIR relation for this sample is consistent with that determined for local ULIRGs and SMGs at z similar to 2. We conclude that SMGs at z > 4 are hotter and more luminous in the FIR but otherwise very similar to those at z similar to 2. None of these sources show any sign of the strong QSO phase being triggered. C1 [Huang, J. -S.] Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China. [Huang, J. -S.] Chinese Acad Sci, China Chile Joint Ctr Astron, Santiago 1515, Chile. [Huang, J. -S.; Dai, Y.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rigopoulou, D.; Magdis, G.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Rigopoulou, D.] Rutherford Appleton Lab, RAL Space Sci & Technol Facil Council, Didcot OX11 0QX, Oxon, England. [Rowan-Robinson, M.; Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Dai, Y.] Boston Coll, Newton, MA USA. [Bock, J. J.] CALTECH, Pasadena, CA 91125 USA. [Burgarella, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Burgarella, D.] Univ Aix marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Chapman, S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Oliver, S.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Page, M.; Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Riechers, D.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Riechers, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Roseboom, I.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Yun, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Webb, T. M. A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Efstathiou, A.] European Univ Cyprus, Sch Sci, CY-1516 Nicosia, Cyprus. RP Huang, JS (reprint author), Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China. RI Magdis, Georgios/C-7295-2014 OI Magdis, Georgios/0000-0002-4872-2294 FU NASA FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). Facilities: Herschel (SPIRE), Spitzer (IRAC, MIPS) NR 80 TC 13 Z9 13 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 52 DI 10.1088/0004-637X/784/1/52 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000052 ER PT J AU Kipping, DM Nesvorny, D Buchhave, LA Hartman, J Bakos, GA Schmitt, AR AF Kipping, D. M. Nesvorny, D. Buchhave, L. A. Hartman, J. Bakos, G. A. Schmitt, A. R. TI THE HUNT FOR EXOMOONS WITH KEPLER (HEK). IV. A SEARCH FOR MOONS AROUND EIGHT M DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: detection; stars: individual (KIC-8845205, KIC-7603200, KIC-12066335, KIC-6497146, KIC-6425957, KIC-10027323, KIC-3966801, KIC-11187837, KOI-463, KOI-314, KOI-784, KOI-3284, KOI-663, KOI-1596, KOI-494, KOI-252); techniques: photometric ID EXTRASOLAR GIANT PLANETS; EARTH-SIZED PLANET; HABITABLE-ZONE; TRANSIT; EFFICIENT; MASS; CONFIRMATION; CANDIDATES; SATELLITES; EXOPLANETS AB With their smaller radii and high cosmic abundance, transiting planets around cool stars hold a unique appeal. As part of our ongoing project to measure the occurrence rate of extrasolar moons, in this work we present results from a survey focusing on eight Kepler planetary candidates associated with M dwarfs. Using photodynamical modeling and Bayesian multimodal nested sampling, we find no compelling evidence for an exomoon in these eight systems. Upper limits on the presence of such bodies probe down to masses of similar to 0.4 M-circle plus. in the best case. For KOI-314, we are able to confirm the planetary nature of two out of the three known transiting candidates using transit timing variations. Of particular interest is KOI-314c, which is found to have a mass of 1.0(- 0.3)(+ 0.4) M-circle plus, making it the lowest mass transiting planet discovered to date. With a radius of 1.61(- 0.15)(+ 0.16) R-circle plus this Earth-mass world is likely enveloped by a significant gaseous envelope comprising >= 17(- 13)(+ 12)% of the planet by radius. We also find evidence to support the planetary nature of KOI-784 via transit timing, but we advocate further observations to verify the signals. In both systems, we infer that the inner planet has a higher density than the outer world, which may be indicative of photo-evaporation. These results highlight both the ability of Kepler to search for sub-Earth-mass moons and the exciting ancillary science that often results from such efforts. C1 [Kipping, D. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nesvorny, D.] Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, L. A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Hartman, J.; Bakos, G. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu OI Buchhave, Lars A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166 FU NASA Carl Sagan Fellowships; NSF [AST-1108686, AST-1008890]; NASA [NNX12AH91H] FX We would like to thank Rene Heller for his thoughtful review which improved the quality of our manuscript. This work made use of the Michael Dodds Computing Facility. 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. 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 55 TC 33 Z9 33 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 MAR 20 PY 2014 VL 784 IS 1 AR 28 DI 10.1088/0004-637X/784/1/28 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000028 ER PT J AU Kostov, VB McCullough, PR Carter, JA Deleuil, M Diaz, RF Fabrycky, DC Hebrard, G Hinse, TC Mazeh, T Orosz, JA Tsvetanov, ZI Welsh, WF AF Kostov, V. B. McCullough, P. R. Carter, J. A. Deleuil, M. Diaz, R. F. Fabrycky, D. C. Hebrard, G. Hinse, T. C. Mazeh, T. Orosz, J. A. Tsvetanov, Z. I. Welsh, W. F. TI KEPLER-413B: A SLIGHTLY MISALIGNED, NEPTUNE-SIZE TRANSITING CIRCUMBINARY PLANET SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; planetary systems; stars: individual (KIC 12351927, Kepler-413); techniques: photometric ID LONG-TERM STABILITY; EXTRASOLAR PLANETS; ECLIPSING BINARIES; SOPHIE VELOCIMETRY; HABITABLE ZONES; STELLAR-SYSTEMS; GLOBAL DYNAMICS; TILTING SATURN; GIANT PLANETS; TRIPLE STARS AB We report the discovery of a transiting, R-p=4.347 +/- 0.099R circle plus, circumbinary planet (CBP) orbiting the Kepler K+M eclipsing binary (EB) system KIC 12351927 (Kepler-413) every similar to 66 days on an eccentric orbit with a(p)=0.355 +/- 0.002 AU, e(p)=0.118 +/- 0.002. The two stars, with M-A=0.820 +/- 0.015M circle dot, R-A=0.776 +/- 0.009R circle dot and M-B=0.542 +/- 0.008M circle dot, R-B=0.484 +/- 0.024R circle dot, respectively, revolve around each other every 10.11615 +/- 0.00001 days on a nearly circular (e(EB)=0.037 +/- 0.002) orbit. The orbital plane of the EB is slightly inclined to the line of sight (i(EB)= 87 degrees.33 +/- 0 degrees.06), while that of the planet is inclined by similar to 2 degrees.5 to the binary plane at the reference epoch. Orbital precession with a period of similar to 11 yr causes the inclination of the latter to the sky plane to continuously change. As a result, the planet often fails to transit the primary star at inferior conjunction, causing stretches of hundreds of days with no transits corresponding to multiple planetary orbital periods). We predict that the next transit will not occur until 2020. The orbital configuration of the system places the planet slightly closer to its host stars than the inner edge of the extended habitable zone. Additionally, the orbital configuration of the system is such that the CBP may experience Cassini State dynamics under the influence of the EB, in which the planet's obliquity precesses with a rate comparable to its orbital precession. Depending on the angular precession frequency of the CBP, it could potentially undergo obliquity fluctuations of dozens of degrees (and complex seasonal cycles) on precession timescales. C1 [Kostov, V. B.; McCullough, P. R.; Tsvetanov, Z. I.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Kostov, V. B.; McCullough, P. R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Carter, J. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Deleuil, M.; Diaz, R. F.] Lab Astrophys Marseille, F-13388 Marseille 13, France. [Fabrycky, D. C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Hebrard, G.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Hebrard, G.] Univ Aix Marseille, Observ Haute Provence, F-04870 St Michel lObservatoire, France. [Hebrard, G.] CNRS, F-04870 St Michel lObservatoire, France. [Hinse, T. C.] Korea Astron & Space Sci Inst KASI, Adv Astron & Space Sci Div, Taejon 305348, South Korea. [Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Mazeh, T.] Tel Aviv Univ, Dept Astron & Astrophys, IL-69978 Tel Aviv, Israel. [Orosz, J. A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Kostov, VB (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. EM vkostov@pha.jhu.edu OI Diaz, Rodrigo/0000-0001-9289-5160; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA Origins of Solar Systems [NNX10AG30G]; NESSF [NNX13AM33H]; National Science Foundation [AST-1109928] FX This research used observations made with the SOPHIE instrument on the 1.93m telescope at Observatoire de Haute-Provence (CNRS), France, as part of programs 12B.PNP.MOUT and 13A.PNP.MOUT. This research made use of the SIMBAD database, operated at CDS, Strasbourg, France; data products from the Two Micron All Sky Survey (2MASS), the Digitized Sky Survey (DSS), the NASA exoplanet archive NexSci20, source code for transit light curves (Mandel & Agol 2002), and the SFI/HEA Irish Centre for High-End Computing (ICHEC). Numerical computations presented in this work were partly carried out using the SFI/HEA Irish Centre for High-End Computing (ICHEC, STOKES) and the PLUTO computing cluster at KASI; astronomical research at Armagh Observatory is funded by the Department of Culture, Arts and Leisure (DCAL). V.B.K. and P.R.M. received funding from a NASA Origins of Solar Systems grant NNX10AG30G and NESSF grant NNX13AM33H. W.F.W. and J.A.O. gratefully acknowledge support from the National Science Foundation via grant AST-1109928 and from NASA's Kepler Participating Scientist Program (NNX12AD23G) and Origins of Solar Systems Program (NNX13AI76G). T.C.H acknowledges support by the Korea Research Council for Science and Technology (KRCF) through the Young Scientist Research Fellowship Program grant number 2013-9-400-00. T. M. acknowledges support from the European Research Council under the EU's Seventh Framework Programme (FP7/(2007-2013)/ERC Grant Agreement No. 291352) and from the Israel Science Foundation ( grant No. 1423/11). NR 99 TC 54 Z9 54 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 MAR 20 PY 2014 VL 784 IS 1 AR 14 DI 10.1088/0004-637X/784/1/14 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000014 ER PT J AU Lissauer, JJ Marcy, GW Bryson, ST Rowe, JF Jontof-Hutter, D Agol, E Borucki, WJ Carter, JA Ford, EB Gilliland, RL Kolbl, R Star, KM Steffen, JH Torres, G AF Lissauer, Jack J. Marcy, Geoffrey W. Bryson, Stephen T. Rowe, Jason F. Jontof-Hutter, Daniel Agol, Eric Borucki, William J. Carter, Joshua A. Ford, Eric B. Gilliland, Ronald L. Kolbl, Rea Star, Kimberly M. Steffen, Jason H. Torres, Guillermo TI VALIDATION OF KEPLER'S MULTIPLE PLANET CANDIDATES. II. REFINED STATISTICAL FRAMEWORK AND DESCRIPTIONS OF SYSTEMS OF SPECIAL INTEREST SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: statistical; planetary systems; stars: individual (Kepler-90=KOI-351, Kepler-102=KOI-82, Kepler-122=KOI-232, Kepler-132=KOI-284, Kepler-223=KOI-730, Kepler-238=KOI-834, Kepler-292=KOI-1364, Kepler-296=KOI-1422) ID LOW-MASS; TRANSITING PLANET; FALSE POSITIVES; STARS; RADII; CONFIRMATION; EVOLUTION; DWARFS; MODELS; PAIRS AB We extend the statistical analysis performed by Lissauer et al. in 2012, which demonstrates that the overwhelming majority of Kepler candidate multiple transiting systems (multis) represents true transiting planets, and we develop therefrom a procedure to validate large numbers of planet candidates in multis as bona fide exoplanets. We show that this statistical framework correctly estimates the abundance of false positives already identified around Kepler targets with multiple sets of transit-like signatures based on their abundance around targets with single sets of transit-like signatures. We estimate the number of multis that represent split systems of one or more planets orbiting each component of a binary star system. We use the high reliability rate for multis to validate more than one dozen particularly interesting multi-planet systems herein. Hundreds of additional multi-planet systems are validated in a companion paper by Rowe et al. We note that few very short period (P < 1.6 days) planets orbit within multiple transiting planet systems and discuss possible reasons for their absence. There also appears to be a shortage of planets with periods exceeding a few months in multis. C1 [Lissauer, Jack J.; Bryson, Stephen T.; Rowe, Jason F.; Jontof-Hutter, Daniel; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Marcy, Geoffrey W.; Kolbl, Rea] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Carter, Joshua A.; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ford, Eric B.; Gilliland, Ronald L.; Star, Kimberly M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Ford, Eric B.; Gilliland, Ronald L.; Star, Kimberly M.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Steffen, Jason H.] Northwestern Univ, Dept Phys & Astron, CIERA, Evanston, IL 60208 USA. RP Lissauer, JJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Jack.Lissauer@nasa.gov OI /0000-0002-0802-9145; /0000-0001-6545-639X FU NASA's Science Mission Directorate FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. We dedicate this paper to the memory of Kepler Deputy Principal Investigator David G. Koch (1945 August 6-2012 September 12), whose work over more than two decades was key to making the Kepler mission a success. We acknowledge Ruth Murray-Clay for stimulating and valuable conversations about FP modes. Tony Dobrovolskis, Mike Haas, Billy Quarles, Leslie Rogers, and Alexandre Santerne provided constructive comments on the manuscript. Elisabeth Adams assisted with the preparation of Figure 12. NR 51 TC 77 Z9 77 U1 1 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 44 DI 10.1088/0004-637X/784/1/44 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000044 ER PT J AU Lupu, RE Zahnle, K Marley, MS Schaefer, L Fegley, B Morley, C Cahoy, K Freedman, R Fortney, JJ AF Lupu, R. E. Zahnle, Kevin Marley, Mark S. Schaefer, Laura Fegley, Bruce Morley, Caroline Cahoy, Kerri Freedman, Richard Fortney, Jonathan J. TI THE ATMOSPHERES OF EARTHLIKE PLANETS AFTER GIANT IMPACT EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; planetary systems; planets and satellites: general; radiative transfer; stars: low-mass ID MOLECULAR SPECTROSCOPIC DATABASE; DIRECT NUMERICAL DIAGONALIZATION; COOL STELLAR ATMOSPHERES; TERRESTRIAL MAGMA OCEAN; CONTINENTAL-CRUST; SYNTHETIC SPECTRA; BROWN DWARFS; MU-M; MULTIPLE-SCATTERING; MODEL ATMOSPHERES AB It is now understood that the accretion of terrestrial planets naturally involves giant collisions, the moon-forming impact being a well-known example. In the aftermath of such collisions, the surface of the surviving planet is very hot and potentially detectable. Here we explore the atmospheric chemistry, photochemistry, and spectral signatures of post-giant-impact terrestrial planets enveloped by thick atmospheres consisting predominantly of CO2 and H2O. The atmospheric chemistry and structure are computed self-consistently for atmospheres in equilibrium with hot surfaces with composition reflecting either the bulk silicate Earth (which includes the crust, mantle, atmosphere, and oceans) or Earth's continental crust. We account for all major molecular and atomic opacity sources including collision-induced absorption. We find that these atmospheres are dominated by H2O and CO2, while the formation of CH4 and NH3 is quenched because of short dynamical timescales. Other important constituents are HF, HCl, NaCl, and SO2. These are apparent in the emerging spectra and can be indicative that an impact has occurred. The use of comprehensive opacities results in spectra that are a factor of two lower brightness temperature in the spectral windows than predicted by previous models. The estimated luminosities show that the hottest post-giant-impact planets will be detectable with near-infrared coronagraphs on the planned 30m class telescopes. The 1-4 mu m will be most favorable for such detections, offering bright features and better contrast between the planet and a potential debris disk. We derive cooling timescales on the order of 10(5-6) yr on the basis of the modeled effective temperatures. This leads to the possibility of discovering tens of such planets in future surveys. C1 [Lupu, R. E.; Freedman, Richard] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Zahnle, Kevin; Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Schaefer, Laura] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fegley, Bruce] Washington Univ, Dept Earth & Planetary Sci, Planetary Chem Lab, St Louis, MO 63130 USA. [Fegley, Bruce] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Morley, Caroline; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Cahoy, Kerri] MIT, Cambridge, MA 02139 USA. RP Lupu, RE (reprint author), NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. EM Roxana.E.Lupu@nasa.gov RI Marley, Mark/I-4704-2013; Lupu, Roxana/P-9060-2014; OI Lupu, Roxana/0000-0003-3444-5908; Fortney, Jonathan/0000-0002-9843-4354; Marley, Mark/0000-0002-5251-2943; Schaefer, Laura/0000-0003-2915-5025 FU NASA; NSF Astronomy Program; NASA EPSCOR Program; NASA Cooperative Agreement [NNX09AG69A]; NASA Ames Research Center FX This work was supported by the NASA Origins program. B. F. was supported by the NSF Astronomy Program, the NASA EPSCOR Program, and by NASA Cooperative Agreement NNX09AG69A with the NASA Ames Research Center. NR 124 TC 18 Z9 18 U1 1 U2 24 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 27 DI 10.1088/0004-637X/784/1/27 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000027 ER PT J AU Mann, RK Di Francesco, J Johnstone, D Andrews, SM Williams, JP Bally, J Ricci, L Hughes, AM Matthews, BC AF Mann, Rita K. Di Francesco, James Johnstone, Doug Andrews, Sean M. Williams, Jonathan P. Bally, John Ricci, Luca Hughes, A. Meredith Matthews, Brenda C. TI ALMA OBSERVATIONS OF THE ORION PROPLYDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE protoplanetary disks; submillimeter: planetary systems ID MASS PROTOSTELLAR CANDIDATES; FAR-ULTRAVIOLET RADIATION; CIRCUMSTELLAR DUST DISKS; YOUNG STELLAR OBJECTS; NEBULA CLUSTER; PROTOPLANETARY DISKS; TRAPEZIUM-CLUSTER; RADIO-SOURCES; PHOTOEVAPORATION; SYSTEM AB We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of protoplanetary disks ("proplyds") in the Orion Nebula Cluster. We imaged five individual fields at 856 mu m containing 22 Hubble Space Telescope (HST)-identified proplyds and detected 21 of them. Eight of those disks were detected for the first time at submillimeter wavelengths, including the most prominent, well-known proplyd in the entire Orion Nebula, 114-426. Thermal dust emission in excess of any free-free component was measured in all but one of the detected disks, and ranged between 1 and 163 mJy, with resulting disk masses of 0.3-79 M-jup. An additional 26 stars with no prior evidence of associated disks in HST observations were also imaged within the 5 fields, but only 2 were detected. The disk mass upper limits for the undetected targets, which include OB stars,theta(1) Ori C, and theta(1) Ori F, range from 0.1 to 0.6 M-jup. Combining these ALMA data with previous Submillimeter Array observations, we find a lack of massive (greater than or similar to 3 M-jup) disks in the extreme-UV-dominated region of Orion, within 0.03 pc of theta(1) Ori C. At larger separations from theta(1) Ori C, in the far-UV-dominated region, there is a wide range of disk masses, similar to what is found in low-mass star forming regions. Taken together, these results suggest that a rapid dissipation of disk masses likely inhibits potential planet formation in the extreme-UV-dominated regions of OB associations, but leaves disks in the far-UV-dominated regions relatively unaffected. C1 [Mann, Rita K.; Di Francesco, James; Johnstone, Doug; Matthews, Brenda C.] Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. [Di Francesco, James; Johnstone, Doug; Matthews, Brenda C.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Johnstone, Doug] Joint Astron Ctr, Hilo, HI 96720 USA. [Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Bally, John] Univ Colorado, CASA, Boulder, CO 80309 USA. [Ricci, Luca] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Hughes, A. Meredith] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA. RP Mann, RK (reprint author), Natl Res Council Canada, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada. EM rita.mann@nrc-cnrc.gc.ca OI Johnstone, Doug/0000-0002-6773-459X; Williams, Jonathan/0000-0001-5058-695X NR 52 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 82 DI 10.1088/0004-637X/784/1/82 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000082 ER PT J AU McDonald, M Swinbank, M Edge, AC Wilner, DJ Veilleux, S Benson, BA Hogan, MT Marrone, DP McNamara, BR Wei, LH Bayliss, MB Bautz, MW AF McDonald, Michael Swinbank, Mark Edge, Alastair C. Wilner, David J. Veilleux, Sylvain Benson, Bradford A. Hogan, Michael T. Marrone, Daniel P. McNamara, Brian R. Wei, Lisa H. Bayliss, Matthew B. Bautz, Marshall W. TI THE STATE OF THE WARM AND COLD GAS IN THE EXTREME STARBURST AT THE CORE OF THE PHOENIX GALAXY CLUSTER ( SPT-CLJ2344-4243) SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: individual (Phoenix SPT-CLJ23444243); galaxies: elliptical and lenticular, cD; galaxies: high-redshift; galaxies: starburst ID COOLING FLOW CLUSTERS; LUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEI; OPTICAL-LINE EMISSION; SOUTH-POLE TELESCOPE; H-ALPHA FILAMENTS; MOLECULAR GAS; SUBMILLIMETER GALAXIES; PERSEUS CLUSTER; SERSIC 159-03 AB We present new optical integral field spectroscopy (Gemini South) and submillimeter spectroscopy (Submillimeter Array) of the central galaxy in the Phoenix cluster (SPT-CLJ2344-4243). This cluster was previously reported to have a massive starburst (similar to 800M(circle dot) yr(-1)) in the central, brightest cluster galaxy, most likely fueled by the rapidly cooling intracluster medium. These new data reveal a complex emission-line nebula, extending for > 30 kpc from the central galaxy, detected at [O ii]lambda lambda 3726, 3729, [O iii]lambda lambda 4959, 5007, H beta, H gamma, H delta, [Neiii].3869, and He ii.4686. The total Ha luminosity, assuming H alpha/H beta = 2.85, is L-H alpha = 7.6 +/- 0.4 x10(43) erg s(-1), making this the most luminous emission-line nebula detected in the center of a cool core cluster. Overall, the relative fluxes of the low-ionization lines (e.g., [Oii], H beta) to the UV continuum are consistent with photoionization by young stars. In both the center of the galaxy and in a newly discovered highly ionized plume to the north of the galaxy, the ionization ratios are consistent with both shocks and active galactic nucleus (AGN) photoionization. We speculate that this extended plume may be a galactic wind, driven and partially photoionized by both the starburst and central AGN. Throughout the cluster we measure elevated high-ionization line ratios (e. g., He ii/H beta, [Oiii]/H beta), coupled with an overall high-velocity width (FWHM greater than or similar to 500 km s-1), suggesting that shocks are likely important throughout the interstellar medium of the central galaxy. These shocks are most likely driven by a combination of stellar winds from massive young stars, core-collapse supernovae, and the central AGN. In addition to the warm, ionized gas, we detect a substantial amount of cold, molecular gas via the CO(3-2) transition, coincident in position with the galaxy center. We infer a molecular gas mass of M-H2 = 2.2 +/- 0.6 x 10(10)M(circle dot), which implies that the starburst will consume its fuel in similar to 30 Myr if it is not replenished. The L-IR/M-H2 that we measure for this cluster is consistent with the starburst limit of 500 L-circle dot/M-circle dot, above which radiation pressure is able to disperse the cold reservoir. The combination of the high level of turbulence in the warm phase and the high LIR/MH2 ratio suggests that this violent starburst may be in the process of quenching itself. We propose that phases of rapid star formation may be common in the cores of galaxy clusters, but so short-lived that their signatures are quickly erased and appear only in a subsample of the most strongly cooling clusters. C1 [McDonald, Michael; Bautz, Marshall W.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Swinbank, Mark; Edge, Alastair C.; Hogan, Michael T.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Wilner, David J.; Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Veilleux, Sylvain] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Benson, Bradford A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Marrone, Daniel P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McNamara, Brian R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Wei, Lisa H.] Atmospher & Environm Res, Lexington, MA 02421 USA. [Bayliss, Matthew B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP McDonald, M (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM mcdonald@space.mit.edu OI Marrone, Daniel/0000-0002-2367-1080; Edge, Alastair/0000-0002-3398-6916 FU STFC [ST/I001573/1]; Senior NPP Award held at NASA-GSFC; Humboldt Foundation; National Science Foundation through [ANT-0638937]; NSF [PHY-1125897, AST-1009012]; Kavli Foundation, and Chandra Award [13800883]; STFC FX The authors are grateful to the Directors of the Gemini Telescope and the Submillimeter Array, who graciously provided the observing time for this program, and to Ruta Kale, who provided access to the ATCA data. M. M. acknowledges support provided by NASA through a Hubble Fellowship grant from STScI. M. S. and A. C. E acknowledge support from STFC grant ST/I001573/1. S. V. acknowledges support from a Senior NPP Award held atNASA-GSFC and from the Humboldt Foundation to fund a long-term visit atMPE in 2012. B. A. B. is supported by the National Science Foundation through grant ANT-0638937, with partial support provided by NSF grant PHY-1125897, the Kavli Foundation, and Chandra Award Number 13800883 issued by the CXC. M. H. acknowledges support from an STFC studentship. M. B. B. acknowledges support from NSF through grant AST-1009012. NR 86 TC 13 Z9 13 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 DI 10.1088/0004-637X/784/1/18 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000018 ER PT J AU Rowe, JF Bryson, ST Marcy, GW Lissauer, JJ Jontof-Hutter, D Mullally, F Gilliland, RL Issacson, H Ford, E Howell, SB Borucki, WJ Haas, M Huber, D Steffen, JH Thompson, SE Quintana, E Barclay, T Still, M Fortney, J Gautier, TN Hunter, R Caldwell, DA Ciardi, DR Devore, E Cochran, W Jenkins, J Agol, E Carter, JA Geary, J AF Rowe, Jason F. Bryson, Stephen T. Marcy, Geoffrey W. Lissauer, Jack J. Jontof-Hutter, Daniel Mullally, Fergal Gilliland, Ronald L. Issacson, Howard Ford, Eric Howell, Steve B. Borucki, William J. Haas, Michael Huber, Daniel Steffen, Jason H. Thompson, Susan E. Quintana, Elisa Barclay, Thomas Still, Martin Fortney, Jonathan Gautier, T. N., III Hunter, Roger Caldwell, Douglas A. Ciardi, David R. Devore, Edna Cochran, William Jenkins, Jon Agol, Eric Carter, Joshua A. Geary, John TI VALIDATION OF KEPLER'S MULTIPLE PLANET CANDIDATES. III. LIGHT CURVE ANALYSIS AND ANNOUNCEMENT OF HUNDREDS OF NEW MULTI-PLANET SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: fundamental parameters ID TRANSIT TIMING OBSERVATIONS; MAIN-SEQUENCE STARS; 1ST 4 MONTHS; HABITABLE ZONES; INPUT CATALOG; EARTH; PARAMETERS; OBJECTS; RADII; SIZE AB The Kepler mission has discovered more than 2500 exoplanet candidates in the first two years of spacecraft data, with approximately 40% of those in candidate multi-planet systems. The high rate of multiplicity combined with the low rate of identified false positives indicates that the multiplanet systems contain very few false positive signals due to other systems not gravitationally bound to the target star. False positives in the multi-planet systems are identified and removed, leaving behind a residual population of candidate multi-planet transiting systems expected to have a false positive rate less than 1%. We present a sample of 340 planetary systems that contain 851 planets that are validated to substantially better than the 99% confidence level; the vast majority of these have not been previously verified as planets. We expect similar to two unidentified false positives making our sample of planet very reliable. We present fundamental planetary properties of our sample based on a comprehensive analysis of Kepler light curves, ground-based spectroscopy, and high-resolution imaging. Since we do not require spectroscopy or high-resolution imaging for validation, some of our derived parameters for a planetary system may be systematically incorrect due to dilution from light due to additional stars in the photometric aperture. Nonetheless, our result nearly doubles the number verified exoplanets. C1 [Rowe, Jason F.; Bryson, Stephen T.; Lissauer, Jack J.; Jontof-Hutter, Daniel; Mullally, Fergal; Howell, Steve B.; Borucki, William J.; Haas, Michael; Huber, Daniel; Thompson, Susan E.; Quintana, Elisa; Barclay, Thomas; Still, Martin; Hunter, Roger; Caldwell, Douglas A.; Jenkins, Jon] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rowe, Jason F.; Mullally, Fergal; Thompson, Susan E.; Quintana, Elisa; Caldwell, Douglas A.; Devore, Edna; Jenkins, Jon] SETI Inst, Mountain View, CA 94043 USA. [Marcy, Geoffrey W.; Issacson, Howard] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Gilliland, Ronald L.; Huber, Daniel] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Ford, Eric] Penn State Univ, State Coll, PA 16801 USA. [Steffen, Jason H.] Northwestern Univ, Dept Phys & Astron, CIERA, Evanston, IL 60208 USA. [Barclay, Thomas; Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Fortney, Jonathan] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Gautier, T. N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Cochran, William] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Cochran, William] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Carter, Joshua A.; Geary, John] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rowe, JF (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Jason.Rowe@nasa.gov RI Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Fortney, Jonathan/0000-0002-9843-4354; /0000-0002-0802-9145; Ciardi, David/0000-0002-5741-3047; /0000-0001-6545-639X FU NASA's Science Mission Directorate; Kepler Participating Scientist grant [NNX12AD21G] FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. We are indebted to the entire Kepler team for all the hard work and dedication that has made such discoveries possible. J.F.R. is partially supported by a Kepler Participating Scientist grant (NNX12AD21G). NR 57 TC 147 Z9 147 U1 12 U2 43 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 45 DI 10.1088/0004-637X/784/1/45 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000045 ER PT J AU Russell, HR McNamara, BR Edge, AC Nulsen, PEJ Main, RA Vantyghem, AN Combes, F Fabian, AC Murray, N Salome, P Wilman, RJ Baum, SA Donahue, M O'Dea, CP Oonk, JBR Tremblay, GR Voit, GM AF Russell, H. R. McNamara, B. R. Edge, A. C. Nulsen, P. E. J. Main, R. A. Vantyghem, A. N. Combes, F. Fabian, A. C. Murray, N. Salome, P. Wilman, R. J. Baum, S. A. Donahue, M. O'Dea, C. P. Oonk, J. B. R. Tremblay, G. R. Voit, G. M. TI MASSIVE MOLECULAR GAS FLOWS IN THE A1664 BRIGHTEST CLUSTER GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: individual (A1664); galaxies: ISM; galaxies: kinematics and dynamics ID RAY-LUMINOUS CLUSTERS; INTEGRAL FIELD SPECTROSCOPY; GALACTIC NUCLEUS FEEDBACK; POWERFUL RADIO GALAXIES; COOLING FLOW; STAR-FORMATION; COLD CLOUDS; PERSEUS CLUSTER; OPTICAL-SPECTRA; INFRARED SURVEY AB We report ALMA Early Science CO(1-0) and CO(3-2) observations of the brightest cluster galaxy (BCG) in A1664. The BCG contains 1.1 x 10(10)M circle dot of molecular gas divided roughly equally between two distinct velocity systems: one from -250 to +250 km s(-1) centered on the BCG's systemic velocity and a high-velocity system blueshifted by 570 km s(-1) with respect to the systemic velocity. The BCG's systemic component shows a smooth velocity gradient across the BCG center, suggestive of rotation about the nucleus. However, the mass and velocity structure are highly asymmetric and there is little star formation coincident with a putative disk. It may be an inflow of gas that will settle into a disk over several 108 yr. The high-velocity system consists of two gas clumps, each similar to 2 kpc across, located to the north and southeast of the nucleus. Each has a line of sight velocity spread of 250-300 km s(-1). The velocity of the gas in the high-velocity system increases toward the BCG center and may be a massive flow into the nucleus. However, the velocity gradient is not smooth. These structures are also coincident with low optical-ultraviolet surface brightness regions, which could indicate dust extinction associated with each clump. The structure is complex, making a clear interpretation difficult, but if the dusty, molecular gas lies predominantly in front of the BCG, the blueshifted velocities would indicate an outflow. Based on the energy requirements, such a massive outflow would most likely be driven by the active galactic nucleus. A merger origin is unlikely but cannot be ruled out. C1 [Russell, H. R.; McNamara, B. R.; Main, R. A.; Vantyghem, A. N.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada. [McNamara, B. R.; Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Edge, A. C.; Wilman, R. J.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Combes, F.; Salome, P.] Observ Paris, F-75014 Paris, France. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Murray, N.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Baum, S. A.; O'Dea, C. P.] Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA. [Donahue, M.; Voit, G. M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Oonk, J. B. R.] Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands. [Tremblay, G. R.] European So Observ, D-85748 Garching, Germany. RP Russell, HR (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. OI Edge, Alastair/0000-0002-3398-6916; Tremblay, Grant/0000-0002-5445-5401; Nulsen, Paul/0000-0003-0297-4493; Combes, Francoise/0000-0003-2658-7893; Voit, Gerard/0000-0002-3514-0383 FU Canadian Space Agency Space Science Enhancement Program; Natural Sciences and Engineering Research Council of Canada; STFC grant [ST/I001573/1] FX We thank the referee for helpful and constructive comments on the paper. H.R.R. and B.R.M. acknowledge generous financial support from the Canadian Space Agency Space Science Enhancement Program. R.A.M. and A.N.V. acknowledge support from the Natural Sciences and Engineering Research Council of Canada. A.C.E. acknowledges support from STFC grant ST/I001573/1. We thank the ALMA scientific support staff members Adam Leroy and Stephane Leon. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00374.S. 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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 74 TC 16 Z9 16 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 78 DI 10.1088/0004-637X/784/1/78 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000078 ER PT J AU Worrall, DM Birkinshaw, M AF Worrall, D. M. Birkinshaw, M. TI SLIDING NOT SLOSHING IN A3744: THE INFLUENCE OF RADIO GALAXIES NGC 7018 AND 7016 ON CLUSTER GAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: individual (A3744); galaxies: individual (NGC 7016, NGC 7017, NGC 7018); galaxies: jets; radio continuum; galaxies-X-rays; galaxies: clusters ID X-RAY-EMISSION; XMM-NEWTON; TEMPERATURE RELATION; ELLIPTIC GALAXY; COLD FRONTS; HOT-SPOTS; CHANDRA; SAMPLE; LOBES; JETS AB We present new X-ray (Chandra) and radio (JVLA) observations of the nearby cluster A3744. It hosts two prominent radio galaxies with powers in the range critical for radio-mode feedback. The radio emission from these galaxies terminates in buoyant tendrils reaching the cluster's outer edge, and the radio-emitting plasma clearly influences the cluster's X-ray-emitting atmosphere. The cluster's average gas temperature, of kT = 3.5 keV, is high for its bolometric luminosity of 3.2 x 10(43) erg s(-1), but the 100 kpc-scale cavity carved out by radio-emitting plasma shows evidence of less than 2% of the excess enthalpy. We suggest instead that a high-velocity encounter with a galaxy group is responsible for dispersing and increasing the entropy of the gas in this non-cool-core cluster. We see no evidence for shocks, or established isobaric gas motions (sloshing), but there is much sub-structure associated with a dynamically active central region that encompasses the brightest radio emission. Gas heating is evident in directions perpendicular to the inferred line of encounter between the infalling group and cluster. The radio-emitting tendrils run along boundaries between gas of different temperature, apparently lubricating the gas flows and inhibiting heat transfer. The first stages of the encounter may have helped trigger the radio galaxies into their current phase of activity, where we see X-rays from the nuclei, jets, and hotspots. C1 [Worrall, D. M.; Birkinshaw, M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Worrall, D. M.; Birkinshaw, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Worrall, DM (reprint author), Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England. EM d.worrall@bristol.ac.uk FU NASA [GO1-12010X]; National Aeronautics and Space Administration; National Science Foundation FX We acknowledge support from NASA grant GO1-12010X. We thank the anonymous referee for constructive comments, and Paul Giles for discussion of the temperature luminosity relation. Results are largely based on observations with Chandra, supported by the CXC. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 42 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2014 VL 784 IS 1 AR 36 DI 10.1088/0004-637X/784/1/36 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5KD UT WOS:000335457000036 ER PT J AU Goobar, A Johansson, J Amanullah, R Cao, Y Perley, DA Kasliwal, MM Ferretti, R Nugent, PE Harris, C Gal-Yam, A Ofek, EO Tendulkar, SP Dennefeld, M Valenti, S Arcavi, I Banerjee, DPK Venkataraman, V Joshi, V Ashok, NM Cenko, SB Diaz, RF Fremling, C Horesh, A Howell, DA Kulkarni, SR Papadogiannakis, S Petrushevska, T Sand, D Sollerman, J Stanishev, V Bloom, JS Surace, J Dupuy, TJ Liu, MC AF Goobar, A. Johansson, J. Amanullah, R. Cao, Y. Perley, D. A. Kasliwal, M. M. Ferretti, R. Nugent, P. E. Harris, C. Gal-Yam, A. Ofek, E. O. Tendulkar, S. P. Dennefeld, M. Valenti, S. Arcavi, I. Banerjee, D. P. K. Venkataraman, V. Joshi, V. Ashok, N. M. Cenko, S. B. Diaz, R. F. Fremling, C. Horesh, A. Howell, D. A. Kulkarni, S. R. Papadogiannakis, S. Petrushevska, T. Sand, D. Sollerman, J. Stanishev, V. Bloom, J. S. Surace, J. Dupuy, T. J. Liu, M. C. TI THE RISE OF SN 2014J IN THE NEARBY GALAXY M82 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dust, extinction; galaxies: individual (Messier 82); supernovae: individual (SN 2014J) ID HIGH-VELOCITY FEATURES; IA SUPERNOVA SPECTRA; OPTICAL PHOTOMETRY; CIRCUMSTELLAR GAS; TIME-SERIES; 2011FE; RADIO; SPECTROSCOPY; ENVIRONMENT; ULTRAVIOLET AB We report on the discovery of SN 2014J in the nearby galaxy M82. Given its proximity, it offers the best opportunity to date to study a thermonuclear supernova (SN) over a wide range of the electromagnetic spectrum. Optical, near-IR, and mid-IR observations on the rising light curve, orchestrated by the intermediate Palomar Transient Factory, show that SN 2014J is a spectroscopically normal Type Ia supernova (SN Ia), albeit exhibiting high-velocity features in its spectrum and heavily reddened by dust in the host galaxy. Our earliest detections start just hours after the fitted time of explosion. We use high-resolution optical spectroscopy to analyze the dense intervening material and do not detect any evolution in the resolved absorption features during the light curve rise. Similar to other highly reddened SNe Ia, a low value of total-to-selective extinction, R-V less than or similar to 2, provides the best match to our observations. We also study pre-explosion optical and near-IR images from Hubble Space Telescope with special emphasis on the sources nearest to the SN location. C1 [Goobar, A.; Johansson, J.; Amanullah, R.; Ferretti, R.; Papadogiannakis, S.; Petrushevska, T.] Stockholm Univ, Oskar Klein Ctr, Dept Phys, Albanova Univ Ctr, SE-10691 Stockholm, Sweden. [Cao, Y.; Perley, D. A.; Tendulkar, S. P.; Kulkarni, S. R.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Kasliwal, M. M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Nugent, P. E.; Harris, C.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Computat Res Div, Berkeley, CA 94720 USA. [Nugent, P. E.; Harris, C.; Bloom, J. S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Gal-Yam, A.; Ofek, E. O.; Horesh, A.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Dennefeld, M.] IAP, CNRS, F-75014 Paris, France. [Dennefeld, M.] Univ Paris 06, F-75014 Paris, France. [Valenti, S.; Arcavi, I.; Howell, D. A.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Valenti, S.; Howell, D. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Arcavi, I.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Banerjee, D. P. K.; Venkataraman, V.; Joshi, V.; Ashok, N. M.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Diaz, R. F.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [Fremling, C.; Sollerman, J.] Stockholm Univ, Oskar Klein Ctr, Dept Astron, Albanova Univ Ctr, SE-10691 Stockholm, Sweden. [Sand, D.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Stanishev, V.] IST, CENTRA Ctr Multidisciplinar Astrofis, P-1049001 Lisbon, Portugal. [Surace, J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Dupuy, T. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, M. C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Goobar, A (reprint author), Stockholm Univ, Oskar Klein Ctr, Dept Phys, Albanova Univ Ctr, SE-10691 Stockholm, Sweden. EM ariel@fysik.su.se RI Horesh, Assaf/O-9873-2016; Stanishev, Vallery/M-8930-2013; OI Horesh, Assaf/0000-0002-5936-1156; Ferretti, Raphael/0000-0001-7814-5814; Stanishev, Vallery/0000-0002-7626-1181; Sollerman, Jesper/0000-0003-1546-6615; Diaz, Rodrigo/0000-0001-9289-5160 FU Swedish Research Council; Swedish Space Board; Hubble Fellowship; Carnegie-Princeton Fellowship; National Energy Research Scientific Computing Center; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; ERC grant FX We thank S. Fossey for making the discovery R-band image of SN 2014J available to us. We are grateful to S. Fossey and M. Phillips for helpful comments on the manuscript. We acknowledge A. McKay, A. Bradley, N. Scoville, P.L. Capak, C. M. Carollo, S. Lilly, H. Sheth, V. Bhalerao, P. Donati, S. Geier, F. Saturni, G. Nowak, and A. Finoguenov for cooperating with ToO observations. A.G. and R.A. acknowledge support from the Swedish Research Council and the Swedish Space Board and A. G.-Y. an ERC grant. M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. 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, Faulkes Telescope North image observed by Gain Lee, the Mount Abu 1.2 m Infrared telescope, India, and the 1.93 m telescope of Haute-Provence Observatory, CNRS, France. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. NR 42 TC 60 Z9 60 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 20 PY 2014 VL 784 IS 1 AR L12 DI 10.1088/2041-8205/784/1/L12 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC8ME UT WOS:000332786300012 ER PT J AU Neilsen, J Coriat, M Fender, R Lee, JC Ponti, G Tzioumis, AK Edwards, PG Broderick, JW AF Neilsen, Joseph Coriat, Mickael Fender, Rob Lee, Julia C. Ponti, Gabriele Tzioumis, Anastasios K. Edwards, Philip G. Broderick, Jess W. TI A LINK BETWEEN X-RAY EMISSION LINES AND RADIO JETS IN 4U 1630-47? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; stars: winds, outflows; X-rays: binaries; X-rays: individual (4U 1630-47) ID BLACK-HOLE SPIN; GRS 1915+105; RELATIVISTIC JETS; A-ASTERISK; ACCRETION; WINDS; BINARIES; ENERGY; POWER; MECHANISM AB Recently, Diaz Trigo et al. reported an XMM-Newton detection of relativistically Doppler-shifted emission lines associated with steep-spectrum radio emission in the stellar-mass black hole candidate 4U 1630-47 during its 2012 outburst. They interpreted these lines as indicative of a baryonic jet launched by the accretion disk. Here we present a search for the same lines earlier in the same outburst using high-resolution X-ray spectra from the Chandra HETGS. While our observations (eight months prior to the XMM-Newton campaign) also coincide with detections of steep spectrum radio emission by the Australia Telescope Compact Array, we find no evidence for any relativistic X-ray emission lines. Indeed, despite similar to 5x brighter radio emission, our Chandra spectra allow us to place an upper limit on the flux in the blueshifted Fe xxvi line that is greater than or similar to 20x weaker than the line observed by Diaz Trigo et al. We explore several scenarios that could explain our differing results, including variations in the geometry of the jet or a mass-loading process or jet baryon content that evolves with the accretion state of the black hole. We also consider the possibility that the radio emission arises in an interaction between a jet and the nearby interstellar medium, in which case the X-ray emission lines might be unrelated to the radio emission. C1 [Neilsen, Joseph] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Neilsen, Joseph] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02138 USA. [Coriat, Mickael] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Fender, Rob; Broderick, Jess W.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Lee, Julia C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ponti, Gabriele] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Tzioumis, Anastasios K.; Edwards, Philip G.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Broderick, Jess W.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Neilsen, J (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. EM neilsenj@bu.edu RI Lee, Julia/G-2381-2015; OI Lee, Julia/0000-0002-7336-3588; Neilsen, Joseph/0000-0002-8247-786X FU NASA; CXC; SAO for NASA [NAS8-03060]; EU Marie Curie Intra-European Fellowship [FP7-PEOPLE-2012-IEF-331095]; Commonwealth of Australia; [PF2-130097] FX We thank the referee for constructive comments. J.N. acknowledges funding from NASA through the Einstein Postdoctoral Fellowship, grant PF2-130097, awarded by the CXC, which is operated by the SAO for NASA under contract NAS8-03060. G. P. acknowledges support via an EU Marie Curie Intra-European Fellowship under contract No. FP7-PEOPLE-2012-IEF-331095. We thank N. Schulz and D. Huenmoerder for advice regarding plasma models. The Australia Telescope Compact Array 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. NR 38 TC 12 Z9 12 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 20 PY 2014 VL 784 IS 1 AR L5 DI 10.1088/2041-8205/784/1/L5 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC8ME UT WOS:000332786300005 ER PT J AU Lamanna, MC Sues, HD Schachner, ER Lyson, TR AF Lamanna, Matthew C. Sues, Hans-Dieter Schachner, Emma R. Lyson, Tyler R. TI A New Large-Bodied Oviraptorosaurian Theropod Dinosaur from the Latest Cretaceous of Western North America SO PLOS ONE LA English DT Article ID HELL CREEK FORMATION; REPUBLIC-OF-CHINA; INNER-MONGOLIA; BAYAN-MANDAHU; DEPOSITIONAL-ENVIRONMENTS; OVIRAPTORID DINOSAURS; SOUTHERN CHINA; CHIROSTENOTES; FEATHERS; BRAIN AB The oviraptorosaurian theropod dinosaur clade Caenagnathidae has long been enigmatic due to the incomplete nature of nearly all described fossils. Here we describe Anzu wyliei gen. et sp. nov., a new taxon of large-bodied caenagnathid based primarily on three well-preserved partial skeletons. The specimens were recovered from the uppermost Cretaceous (upper Maastrichtian) Hell Creek Formation of North and South Dakota, and are therefore among the stratigraphically youngest known oviraptorosaurian remains. Collectively, the fossils include elements from most regions of the skeleton, providing a wealth of information on the osteology and evolutionary relationships of Caenagnathidae. Phylogenetic analysis reaffirms caenagnathid monophyly, and indicates that Anzu is most closely related to Caenagnathus collinsi, a taxon that is definitively known only from a mandible from the Campanian Dinosaur Park Formation of Alberta. The problematic oviraptorosaurs Microvenator and Gigantoraptor are recovered as basal caenagnathids, as has previously been suggested. Anzu and other caenagnathids may have favored well-watered floodplain settings over channel margins, and were probably ecological generalists that fed upon vegetation, small animals, and perhaps eggs. C1 [Lamanna, Matthew C.] Carnegie Museum Nat Hist, Sect Vertebrate Paleontol, Pittsburgh, PA 15213 USA. [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Schachner, Emma R.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Lyson, Tyler R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Lamanna, MC (reprint author), Carnegie Museum Nat Hist, Sect Vertebrate Paleontol, Pittsburgh, PA 15213 USA. EM lamannam@carnegiemnh.org FU Carnegie Museum of Natural History; American Philosophical Society Franklin Research Grant; National Museum of Natural History Peter Buck Postdoctoral Fellowship; American Association of Anatomists Postdoctoral Fellowship FX Funding was provided by the Carnegie Museum of Natural History (http://www.carnegiemnh.org), an American Association of Anatomists Postdoctoral Fellowship (http://www.anatomy.org/content/postdoctoral-fellowship-criteria), and an American Philosophical Society Franklin Research Grant (http://www.amphilsoc.org/grants/franklin) to E. R. S., and a National Museum of Natural History Peter Buck Postdoctoral Fellowship (http://vertebrates.si.edu/vz_buck_fell_info.html) to T. R. L. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 98 TC 18 Z9 21 U1 3 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 MAR 19 PY 2014 VL 9 IS 3 AR e92022 DI 10.1371/journal.pone.0092022 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AD6ER UT WOS:000333348500073 PM 24647078 ER PT J AU Khonmee, J Brown, JL Rojanasthien, S Aunsusin, A Thumasanukul, D Kongphoemphun, A Siriaroonrat, B Tipkantha, W Punyapornwithaya, V Thitaram, C AF Khonmee, Jaruwan Brown, Janine L. Rojanasthien, Suvichai Aunsusin, Anurut Thumasanukul, Dissakul Kongphoemphun, Adisorn Siriaroonrat, Boripat Tipkantha, Wanlaya Punyapornwithaya, Veerasak Thitaram, Chatchote TI Gender, Season and Management Affect Fecal Glucocorticoid Metabolite Concentrations in Captive Goral (Naemorhedus griseus) in Thailand SO PLOS ONE LA English DT Article ID BLACK-FOOTED FERRET; ADRENAL ACTIVITY; ENVIRONMENTAL ENRICHMENT; CORTISOL METABOLITES; SEX-DIFFERENCES; ADRENOCORTICAL ACTIVITY; DOMESTIC LIVESTOCK; ZOO VISITORS; STRESS; BEHAVIOR AB Chinese goral (Naemorhedus griseus) are a threatened species in Thailand and the focus of captive breeding for possible reintroduction. However, little is known of their biology or what factors in the captive environment affect welfare. Our objective was to determine the impact of gender, season, and management on goral adrenal activity. We hypothesized that differences in fecal glucocorticoid concentrations would be related to animal density. Fecal samples were collected 3 days/week for 1 year from 63 individuals (n = 32 males, 31 females) at two facilities that house the majority of goral in Thailand: Omkoi Wildlife Sanctuary (Omkoi), an off-exhibit breeding center that houses goral in individual pens (16 pens; n = 8 males, 8 females) and in small family groups (8 pens; n = 8 males, 8 females); and the Chiang Mai Night Safari (NS), a zoo that maintains 31 goral (n = 17 males, 14 females) in one large pen. Glucocorticoid metabolite concentrations were higher in male than female goral at Omkoi throughout the year, and there was a seasonal effect on adrenal activity (p<0.05). Goral at Omkoi and NS were used to test the effect of animal density on fecal glucocorticoid excretion of goral housed in similar-sized enclosures. Overall, the highest levels were found at NS (n = 31 adults/pen; 27 m(2) per animal) compared to Omkoi (n = 2 adults/pen; 400 m(2) per animal) (p<0.05). Overall findings support our hypothesis that animal density and aspects of the captive environment impact adrenal steroid activity in captive goral. In addition, gender and season also had significant effects on glucocorticoid metabolite production. Potential stressors pertaining to the welfare of this species were identified, which will guide future efforts to improve management and create self-sustaining and healthy populations of this threatened species. C1 [Khonmee, Jaruwan; Rojanasthien, Suvichai; Punyapornwithaya, Veerasak; Thitaram, Chatchote] Chiang Mai Univ, Fac Vet Med, Chiang Mai 50000, Thailand. [Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. [Aunsusin, Anurut] Chiang Mai Night Safari, Chiang Mai, Thailand. [Thumasanukul, Dissakul; Kongphoemphun, Adisorn] Omkoi Wildlife Sanctuary, Dept Natl Pk Wildlife & Plant Conservat, Chiang Mai, Thailand. [Siriaroonrat, Boripat; Tipkantha, Wanlaya] Zool Pk Org, Conservat Res & Educ Div, Bangkok, Thailand. RP Khonmee, J (reprint author), Chiang Mai Univ, Fac Vet Med, Chiang Mai 50000, Thailand. EM jaruwan.khonmee@cmu.ac.th; chatchote.thitaram@cmu.ac.th FU National Research Council of Thailand (NRCT) FX This study was funded by National Research Council of Thailand (NRCT). All laboratory analyses and additional lab support was provided by Faculty of Veterinary Medicine, Chiang Mai University. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 66 TC 3 Z9 3 U1 5 U2 20 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAR 17 PY 2014 VL 9 IS 3 AR e91633 DI 10.1371/journal.pone.0091633 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AD4XD UT WOS:000333254100049 PM 24637886 ER PT J AU Thomson, V Aplin, KP Cooper, A Hisheh, S Suzuki, H Maryanto, I Yap, G Donnellan, SC AF Thomson, Vicki Aplin, Ken P. Cooper, Alan Hisheh, Susan Suzuki, Hitoshi Maryanto, Ibnu Yap, Grace Donnellan, Stephen C. TI Molecular Genetic Evidence for the Place of Origin of the Pacific Rat, Rattus exulans SO PLOS ONE LA English DT Article ID PHYLOGENIES; NETWORKS; MTDNA; DNA AB Commensal plants and animals have long been used to track human migrations, with Rattus exulans (the Pacific rat) a common organism for reconstructing Polynesian dispersal in the Pacific. However, with no knowledge of the homeland of R. exulans, the place of origin of this human-commensal relationship is unknown. We conducted a mitochondrial DNA phylogeographic survey of R. exulans diversity across the potential natural range in mainland and Island Southeast Asia in order to establish the origin of this human-commensal dyad. We also conducted allozyme electrophoresis on samples from ISEA to obtain a perspective on patterns of genetic diversity in this critical region. Finally, we compared molecular genetic evidence with knowledge of prehistoric rodent faunas in mainland and ISEA. We find that ISEA populations of R. exulans contain the highest mtDNA lineage diversity including significant haplotype diversity not represented elsewhere in the species range. Within ISEA, the island of Flores in the Lesser Sunda group contains the highest diversity in ISEA (across all loci) and also has a deep fossil record of small mammals that appears to include R. exulans. Therefore, in addition to Flores harboring unusual diversity in the form of Homo floresiensis, dwarfed stegodons and giant rats, this island appears to be the homeland of R. exulans. C1 [Thomson, Vicki; Cooper, Alan] Univ Adelaide, Australian Ctr Ancient DNA, Sch Earth & Environm Sci, Adelaide, SA, Australia. [Aplin, Ken P.] Smithsonian Inst, Div Mammals, US Natl Museum, Washington, DC 20560 USA. [Aplin, Ken P.] Australian Natl Univ, Dept Archaeol & Nat Hist, Coll Asia & Pacific, Canberra, ACT, Australia. [Hisheh, Susan] Univ Melbourne, Austin Acad Ctr, Melbourne, Vic, Australia. [Suzuki, Hitoshi] Hokkaido Univ, Grad Sch Environm Earth Sci, Sapporo, Hokkaido 060, Japan. [Maryanto, Ibnu] Indonesian Inst Sci, Biol Res Ctr, Div Zool, Bogor, Indonesia. [Yap, Grace] Natl Environm Agcy, Environm Hlth Inst, Singapore, Singapore. [Donnellan, Stephen C.] S Australian Museum, Adelaide, SA 5000, Australia. [Donnellan, Stephen C.] Univ Adelaide, Australian Ctr Evolutionary Biol & Biodivers, Adelaide, SA, Australia. RP Thomson, V (reprint author), Univ Adelaide, Australian Ctr Ancient DNA, Sch Earth & Environm Sci, Adelaide, SA, Australia. EM vicki.thomson@adelaide.edu.au RI Thomson, Vicki/B-9971-2014; Suzuki, Hitoshi/F-8539-2012 OI Thomson, Vicki/0000-0001-8368-9664; Suzuki, Hitoshi/0000-0003-4426-385X FU National Geographic Society Exploration Grant; Australian Centre for International Agricultural Research; AUSAid; Australian Research Council [DP0988863]; Australian post-graduate award FX A National Geographic Society Exploration Grant provided funding for the vertebrate fauna survey in eastern Indonesia, and the Australian Centre for International Agricultural Research and AUSAid provided funding for fieldwork in the agricultural landscapes of Southeast Asia. The study was partially funded from Australian Research Council grant DP0988863 to SCD and KPA. VT was supported by an Australian post-graduate award. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 30 TC 5 Z9 5 U1 1 U2 23 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAR 17 PY 2014 VL 9 IS 3 AR e91356 DI 10.1371/journal.pone.0091356 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AD4XD UT WOS:000333254100030 PM 24637896 ER PT J AU Isler, ML Bravo, GA Brumfield, RT AF Isler, Morton L. Bravo, Gustavo A. Brumfield, Robb T. TI Inundicola Bravo, Isler, and Brumfield 2013 is a junior synonym of Akletos Dunajewski 1948 (Aves: Passeriformes: Thamnophilidae) SO ZOOTAXA LA English DT Letter C1 [Isler, Morton L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool Birds, Washington, DC 20560 USA. [Bravo, Gustavo A.; Brumfield, Robb T.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Bravo, Gustavo A.; Brumfield, Robb T.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. RP Isler, ML (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool Birds, Washington, DC 20560 USA. EM antbird@cox.net RI Brumfield, Robb/K-6108-2015 OI Brumfield, Robb/0000-0003-2307-0688 NR 4 TC 1 Z9 1 U1 0 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 17 PY 2014 VL 3779 IS 3 BP 399 EP 400 PG 2 WC Zoology SC Zoology GA AD0BX UT WOS:000332899900010 PM 24871736 ER PT J AU Jaffer, EK Gilmour, CC Graham, AM AF Jaffer, Elena K. Gilmour, Cynthia C. Graham, Andrew M. TI Effects of Fe(II) and dissolved organic matter on microbial mercury methylation in sulfidic solutions SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Jaffer, Elena K.; Graham, Andrew M.] Grinnell Coll, Dept Chem, Grinnell, IA 50112 USA. [Gilmour, Cynthia C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. EM jafferel@grinnell.edu NR 0 TC 0 Z9 0 U1 0 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 80-GEOC PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457600732 ER PT J AU McCarthy, M AF McCarthy, Michael TI Centimeter-wave rotational spectroscopy: A stepping stone to the FIR and beyond SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [McCarthy, Michael] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM mmccarthy@cfa.harvard.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 453-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457603832 ER PT J AU Post, JE Heaney, PJ AF Post, Jeffrey E. Heaney, Peter J. TI Crystal structures of natural manganese oxide minerals SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 247th National Spring Meeting of the American-Chemical-Society (ACS) CY MAR 16-20, 2014 CL Dallas, TX SP Amer Chem Soc C1 [Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Heaney, Peter J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM postj@si.edu NR 0 TC 0 Z9 0 U1 1 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 16 PY 2014 VL 247 MA 149-GEOC PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA AZ8HZ UT WOS:000348457600792 ER PT J AU Condit, R Lao, S Singh, A Esufali, S Dolins, S AF Condit, Richard Lao, Suzanne Singh, Anudeep Esufali, Shameema Dolins, Steven TI Data and database standards for permanent forest plots in a global network SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Forest plot database; Integrity errors; Normalized data; Tree census ID TREE; VEGETATION; DIVERSITY; DYNAMICS; RAINFOR; NICHES AB The Center for Tropical Forest Science established a network of 50-ha forest inventory plots in the 1980s, and now assists local scientists with field and database methods at 44 large-scale plots across boreal, temperate, and tropical forest biomes. We published detailed field methods over a decade ago, but at that time, data were maintained in spreadsheet-like formats, most harboring design flaws that resulted in frequent errors. We since established detailed database methods and a normalized data model for housing multiple censuses of large plots. Our largest databases include >2 million measurements, and each has a master version on a server where all collaborators can access and edit data. This paper focuses on the data requirements for handling tree census data and how to design databases to meet these requirements and to ensure data integrity. There are six key elements of a tree census which the database must reflect: (1) measurements, including individual trees (genetic units), stems within trees, and multiple measurements of stems; both field and data methods must assure that every tree, stem, and measurement is precisely identified and can be relocated easily; (2) coordinates, including quadrats within a plot, because field mapping is usually done by assigning x-y coordinates relative to local quadrat markers; (3) taxonomy, carrying a species identity for every tree with a history of individual re-identifications; (4) personnel, with records of the people who performed field and data work per quadrat; (5) assessment of field error via random re-measurements; and (6) a log of changes and a system of archiving so that errors can be tracked and past versions can be reconstructed and cited in publications. A well-designed database model reduces a variety of integrity errors and improves access to data tables in identical formats across many plots, allowing data analyses to be easily replicated and results to be compared. The principal disadvantage is that complexity of the database requires experienced data managers. Published by Elsevier B.V. C1 [Condit, Richard; Lao, Suzanne; Singh, Anudeep; Esufali, Shameema] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, Miami, FL 34002 USA. [Dolins, Steven] Bradley Univ, Dept Comp Sci & Informat Syst, Peoria, IL 61625 USA. RP Condit, R (reprint author), Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, Miami, FL 34002 USA. EM conditr@gmail.com FU National Science Foundation [DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9405933, DEB-9221033, DEB9100058, DEB-8906869, DEB-8605042, DEB-8206992, DEB7922197]; John D. and Catherine T. MacArthur Foundation; Mellon Foundation; Small World Institute Fund; Bradley University Department of Computer Science 82 Information Systems; Smithsonian Tropical Research Institute SIGeo program FX We thank the many principal investigators, field technicians, and database managers of all CTFS plots for their input on field and data methods, especially R. Foster and S. Hubbell for pioneering the idea of a large plots with small diameter limit at Barro Colorado Island. Funding for the plot has been provided by the National Science Foundation (DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9615226, DEB-9405933, DEB-9221033, DEB9100058, DEB-8906869, DEB-8605042, DEB-8206992, DEB7922197), the John D. and Catherine T. MacArthur Foundation, the Mellon Foundation, the Small World Institute Fund, and numerous small grants from other donors. M. Overholt, M. Campos, and H-C. Su assisted with database design. The Bradley University Department of Computer Science 82 Information Systems and Smithsonian Tropical Research Institute SIGeo program provided funding, and we thank S. Davies and E. Bermingham for their support. NR 33 TC 8 Z9 8 U1 1 U2 33 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 MAR 15 PY 2014 VL 316 SI SI BP 21 EP 31 DI 10.1016/j.foreco.2013.09.011 PG 11 WC Forestry SC Forestry GA AD0EE UT WOS:000332906500004 ER PT J AU Feist, J Zatsarinny, O Nagele, S Pazourek, R Burgdorfer, J Guan, XX Bartschat, K Schneider, BI AF Feist, Johannes Zatsarinny, Oleg Nagele, Stefan Pazourek, Renate Burgdoerfer, Joachim Guan, Xiaoxu Bartschat, Klaus Schneider, Barry I. TI Time delays for attosecond streaking in photoionization of neon SO PHYSICAL REVIEW A LA English DT Article ID SPECTROSCOPY; MOLECULES; MATRIX; ATOMS AB We revisit the time-resolved photoemission in neon atoms as probed by attosecond streaking. We calculate streaking time shifts for the emission of 2(p) and 2(s) electrons and compare the relative delay as measured in a recent experiment by Schultze et al. [Science 328, 1658 (2010)]. The B-spline R-matrix method is employed to calculate accurate Eisenbud- Wigner- Smith time delays from multielectron dipole transition matrix elements for photoionization. The additional laser field-induced time shifts in the exit channel are obtained from separate, time-dependent simulations of a full streaking process by solving the time-dependent Schr " odinger equation on the single-active-electron level. The resulting accurate total relative streaking time shifts between 2(s) and 2(p) emission lie well below the experimental data. We identify the presence of unresolved shake- up satellites in the experiment as a potential source of error in the determination of streaking time shifts. C1 [Feist, Johannes; Bartschat, Klaus] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Feist, Johannes] Univ Autonoma Madrid, Dept Fis Teor Materia Condensada, E-28049 Madrid, Spain. [Zatsarinny, Oleg; Guan, Xiaoxu; Bartschat, Klaus] Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. [Nagele, Stefan; Pazourek, Renate; Burgdoerfer, Joachim] Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria. [Schneider, Barry I.] Natl Sci Fdn, Off Cyberinfrastruct, Arlington, VA 22230 USA. RP Feist, J (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. EM johannes.feist@uam.es; stefan.nagele@tuwien.ac.at RI Feist, Johannes/J-7394-2012; Guan, Xiaoxu/A-1299-2013; Nagele, Stefan/E-6938-2011 OI Feist, Johannes/0000-0002-7972-0646; Nagele, Stefan/0000-0003-1213-0294 FU FWF-Austria [P23359- N16]; US National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University; Harvard-Smithsonian Center [PHY-1068140, PHY-1212450, PHY-090031]; European Research Council [290981] FX This work was supported in part by the FWF-Austria ( SFB NEXTLITE, SFB VICOM and P23359- N16), and by the US National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University and the Harvard-Smithsonian Center for Astrophysics, and through Grants No. PHY-1068140 and No. PHY-1212450 as well as XSEDE resources provided by NICS and TACC under Grant No. PHY-090031. Some of the computational results presented here were generated on the Vienna Scientific Cluster ( VSC). J. F. acknowledges support by the European Research Council under Grant No. 290981 (PLASMONANOQUANTA). R. P. acknowledges support by the TU Vienna Doctoral Program Functional Matter. NR 36 TC 24 Z9 24 U1 1 U2 21 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD MAR 14 PY 2014 VL 89 IS 3 AR 033417 DI 10.1103/PhysRevA.89.033417 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AD3ZG UT WOS:000333184400004 ER PT J AU Blake, DB Mah, CL AF Blake, Daniel B. Mah, Christopher L. TI Comments on "The phylogeny of post-Palaeozoic Asteroidea (Neoasteroidea, Echinodermata)" by AS Gale and perspectives on the systematics of the Asteroidea SO ZOOTAXA LA English DT Article DE Neoasteroidea; Echinodermata ID SEA STARS ASTEROIDEA; LARV-AE; CROWN-GROUP; MOLECULAR PHYLOGENY; SUPRASPECIFIC TAXA; MORPHOLOGY; CLASSIFICATION; LIFE; BEARING; GENUS AB A new, morphologically based classification of extant asteroids with comments on select fossils was published by A. S. Gale. Research approaches used limited sampling, and much literature treatment is not accurate and therefore misleading. We review these concerns, seeking to clarify argumentation on differing interpretations. C1 [Blake, Daniel B.] Univ Illinois, Dept Geol, Urbana, IL 61801 USA. [Mah, Christopher L.] Smithsonian Inst, Washington, DC 20013 USA. RP Blake, DB (reprint author), Univ Illinois, Dept Geol, Urbana, IL 61801 USA. NR 114 TC 1 Z9 1 U1 0 U2 9 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 14 PY 2014 VL 3779 IS 2 BP 177 EP 194 PG 18 WC Zoology SC Zoology GA AC8ER UT WOS:000332766700004 PM 24871720 ER PT J AU Risaliti, G AF Risaliti, Guido TI ASTROPHYSICS Cosmic lens reveals spinning black hole SO NATURE LA English DT Editorial Material ID RAY; DISK AB The power of a cosmic lens to magnify and split the light from a distant, mass-accreting giant black hole into four components has allowed researchers to measure the black hole's spin. C1 [Risaliti, Guido] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, Guido] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Risaliti, G (reprint author), INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. EM risaliti@arcetri.astro.it OI Risaliti, Guido/0000-0002-3556-977X NR 10 TC 0 Z9 0 U1 0 U2 6 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAR 13 PY 2014 VL 507 IS 7491 BP 173 EP 174 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC6RJ UT WOS:000332651800024 PM 24598542 ER PT J AU Meijer, HJM AF Meijer, Hanneke J. M. TI The avian fossil record in Insular Southeast Asia and its implications for avian biogeography and palaeoecology SO PEERJ LA English DT Article DE Insular Southeast Asia; Dispersal; Wallacea; Extinction; Paleontology; Fossil birds; Avian biogeography ID NORTH-WESTERN BORNEO; 2 INDONESIAN ISLANDS; LAST GLACIAL PERIOD; LATE PLEISTOCENE; MIDDLE PLEISTOCENE; MARABOU STORK; OMBILIN BASIN; LIANG BUA; BIRDS; FLORES AB Excavations and studies of existing collections during the last decades have significantly increased the abundance as well as the diversity of the avian fossil record for Insular Southeast Asia. The avian fossil record covers the Eocene through the Holocene, with the majority of bird fossils Pleistocene in age. Fossil bird skeletal remains represent at least 63 species in 54 genera and 27 families, and two ichnospecies are represented by fossil footprints. Birds of prey, owls and swiftlets are common elements. Extinctions seem to have been few, suggesting continuity of avian lineages since at least the Late Pleistocene, although some shifts in species ranges have occurred in response to climatic change. Similarities between the Late Pleistocene avifaunas of Flores and Java suggest a dispersal route across southern Sundaland. Late Pleistocene assemblages of Niah Cave (Borneo) and Liang Bua (Flores) support the rainforest refugium hypothesis in Southeast Asia as they indicate the persistence of forest cover, at least locally, throughout the Late Pleistocene and Holocene. C1 [Meijer, Hanneke J. M.] Inst Catala Paleontol Miquel Crusafont, Cerdanyola Del Valles, Spain. [Meijer, Hanneke J. M.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Meijer, Hanneke J. M.] Nat Biodivers Ctr, Leiden, Netherlands. RP Meijer, HJM (reprint author), Inst Catala Paleontol Miquel Crusafont, Cerdanyola Del Valles, Spain. EM Hanneke.Meijer@icp.cat RI Meijer, Hanneke/A-1912-2013 OI Meijer, Hanneke/0000-0001-7066-6869 FU Spanish Ministerio de Economia y Competitividad [CGL2011-28681]; Generalitat de Catalunya [BP-B-00174] FX This work has been supported by the Spanish Ministerio de Economia y Competitividad (CGL2011-28681), and the Generalitat de Catalunya (BP-B-00174 to HJMM). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 81 TC 5 Z9 5 U1 0 U2 12 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD MAR 11 PY 2014 VL 2 AR e295 DI 10.7717/peerj.295 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AY4QK UT WOS:000347563200005 PM 24688871 ER PT J AU Barkats, D Aikin, R Bischoff, C Buder, I Kaufman, JP Keating, BG Kovac, JM Su, M Ade, PAR Battle, JO Bierman, EM Bock, JJ Chiang, HC Dowell, CD Duband, L Filippini, J Hivon, EF Holzapfel, WL Hristov, VV Jones, WC Kuo, CL Leitch, EM Mason, PV Matsumura, T Nguyen, HT Ponthieu, N Pryke, C Richter, S Rocha, G Sheehy, C Kernasovskiy, SS Takahashi, YD Tolan, JE Yoon, KW AF Barkats, D. Aikin, R. Bischoff, C. Buder, I. Kaufman, J. P. Keating, B. G. Kovac, J. M. Su, M. Ade, P. A. R. Battle, J. O. Bierman, E. M. Bock, J. J. Chiang, H. C. Dowell, C. D. Duband, L. Filippini, J. Hivon, E. F. Holzapfel, W. L. Hristov, V. V. Jones, W. C. Kuo, C. L. Leitch, E. M. Mason, P. V. Matsumura, T. Nguyen, H. T. Ponthieu, N. Pryke, C. Richter, S. Rocha, G. Sheehy, C. Kernasovskiy, S. S. Takahashi, Y. D. Tolan, J. E. Yoon, K. W. CA BICEP1 Collaboration TI DEGREE-SCALE COSMIC MICROWAVE BACKGROUND POLARIZATION MEASUREMENTS FROM THREE YEARS OF BICEP1 DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; gravitational waves; inflation; polarization ID PROBE WMAP OBSERVATIONS; POWER SPECTRA; GRAVITY-WAVES; EMISSION; TEMPERATURE; MODEL; DUST; QUAD; MAPS; GHZ AB BICEP1 is a millimeter-wavelength telescope designed specifically to measure the inflationary B-mode polarization of the cosmic microwave background at degree angular scales. We present results from an analysis of the data acquired during three seasons of observations at the South Pole (2006-2008). This work extends the two-year result published in Chiang et al., with additional data from the third season and relaxed detector-selection criteria. This analysis also introduces a more comprehensive estimation of band power window functions, improved likelihood estimation methods, and a new technique for deprojecting monopole temperature-to-polarization leakage that reduces this class of systematic uncertainty to a negligible level. We present maps of temperature, E-and B-mode polarization, and their associated angular power spectra. The improvement in the map noise level and polarization spectra error bars are consistent with the 52% increase in integration time relative to Chiang et al. We confirm both self-consistency of the polarization data and consistency with the two-year results. We measure the angular power spectra at 21 <= l <= 335 and find that the EE spectrum is consistent with Lambda cold dark matter cosmology, with the first acoustic peak of the EE spectrum now detected at 15 sigma. The BB spectrum remains consistent with zero. From B-modes only, we constrain the tensor-to-scalar ratio to r = 0.03(+) (0.27)(-0.23), or r < 0.70 at 95% confidence level. C1 [Barkats, D.] ESO, Joint ALMA Observ, Santiago, Chile. [Aikin, R.; Bock, J. J.; Filippini, J.; Hristov, V. V.; Mason, P. V.; Richter, S.; Rocha, G.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Bischoff, C.; Buder, I.; Kovac, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kaufman, J. P.; Keating, B. G.; Bierman, E. M.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Su, M.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Su, M.] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. [Ade, P. A. R.] Univ Wales Coll Cardiff, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Battle, J. O.; Bock, J. J.; Dowell, C. D.; Nguyen, H. T.; Rocha, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chiang, H. C.] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Durban, South Africa. [Duband, L.] CEA Grenoble, SBT, F-38041 Grenoble, France. [Hivon, E. F.] Inst Astrophys, F-75014 Paris, France. [Holzapfel, W. L.; Takahashi, Y. D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Kuo, C. L.; Kernasovskiy, S. S.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Stanford, CA 94305 USA. [Kuo, C. L.; Kernasovskiy, S. S.; Tolan, J. E.; Yoon, K. W.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Leitch, E. M.; Sheehy, C.] Univ Chicago, Chicago, IL 60637 USA. [Matsumura, T.] KEK, High Energy Accelerator Org, Tsukuba, Ibaraki 3050801, Japan. [Ponthieu, N.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. RP Barkats, D (reprint author), ESO, Joint ALMA Observ, Santiago, Chile. EM dbarkats@alma.cl RI Holzapfel, William/I-4836-2015; OI Barkats, Denis/0000-0002-8971-1954; Hivon, Eric/0000-0003-1880-2733 FU NSF [OPP-0230438]; Caltech President's Fund [PF-471]; NSF CAREER [AST-1255358]; Harvard College Observatory; Alfred P.Sloan Research Fellowship; NSF PECASE [AST-0548262]; Caltech President's Fund; JPL Research and Technology Development Fund FX Bicep1 was supported by NSF grant No. OPP-0230438, Caltech President's Discovery Fund, Caltech President's Fund PF-471, JPL Research and Technology Development Fund, and the late J. Robinson. This analysis was supported in part by NSF CAREER award No. AST-1255358 and the Harvard College Observatory, and J.M.K. acknowledges support from an Alfred P. Sloan Research Fellowship. B.G.K acknowledges support from NSF PECASE Award No. AST-0548262. We thank the South Pole Station staff for helping make our observing seasons a success. We also thank our colleagues in ACBAR, Boomerang, QUAD, BOLOCAM, SPT, WMAP, and Planck for advice and helpful discussions, and Kathy Deniston and Irene Coyle for logistical and administrative support. We thank Patrick Shopbell for computational support at Caltech and the FAS Science Division Research Computing Group at Harvard University for providing support to run all the computations for this paper on the Odyssey cluster. NR 55 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2014 VL 783 IS 2 AR 67 DI 10.1088/0004-637X/783/2/67 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900003 ER PT J AU Green, GM Schlafly, EF Finkbeiner, DP Juric, M Rix, HW Burgett, W Chambers, KC Draper, PW Flewelling, H Kudritzki, RP Magnier, E Martin, N Metcalfe, N Tonry, J Wainscoat, R Waters, C AF Green, Gregory Maurice Schlafly, Edward F. Finkbeiner, Douglas P. Juric, Mario Rix, Hans-Walter Burgett, Will Chambers, Kenneth C. Draper, Peter W. Flewelling, Heather Kudritzki, Rolf Peter Magnier, Eugene Martin, Nicolas Metcalfe, Nigel Tonry, John Wainscoat, Richard Waters, Christopher TI MEASURING DISTANCES AND REDDENINGS FOR A BILLION STARS: TOWARD A 3D DUST MAP FROM PAN-STARRS 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; Galaxy: structure; ISM: structure; methods: statistical; stars: distances ID MILKY-WAY TOMOGRAPHY; MONO-ABUNDANCE SUBPOPULATIONS; DIGITAL SKY SURVEY; INTERSTELLAR EXTINCTION; DENSITY DISTRIBUTION; STELLAR; SEGUE; DISK; EVOLUTION; SAGITTARIUS AB We present a method to infer reddenings and distances to stars based only on their broad-band photometry, and show how this method can be used to produce a three-dimensional (3D) dust map of the Galaxy. Our method samples from the full probability density function of distance, reddening, and stellar type for individual stars, as well as the full uncertainty in reddening as a function of distance in the 3D dust map. We incorporate prior knowledge of the distribution of stars in the Galaxy and the detection limits of the survey. For stars in the Pan-STARRS 1 (PS1) 3 pi survey, we demonstrate that our reddening estimates are unbiased and accurate to similar to 0.13 mag in E(B -V) for the typical star. Based on comparisons with mock catalogs, we expect distances for main-sequence stars to be constrained to within similar to 20%-60%, although this range can vary, depending on the reddening of the star, the precise stellar type, and its position on the sky. A later paper will present a 3D map of dust over the three quarters of the sky surveyed by PS1. Both the individual stellar inferences and the 3D dust map will enable a wealth of Galactic science in the plane. The method we present is not limited to the passbands of the PS1 survey but may be extended to incorporate photometry from other surveys, such as the Two Micron All Sky Survey, the Sloan Digital Sky Survey (where available), and in the future, LSST and Gaia. C1 [Green, Gregory Maurice; Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schlafly, Edward F.; Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Juric, Mario] LSST Corp, Tucson, AZ 85721 USA. [Burgett, Will; Chambers, Kenneth C.; Flewelling, Heather; Kudritzki, Rolf Peter; Magnier, Eugene; Tonry, John; Wainscoat, Richard; Waters, Christopher] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Draper, Peter W.; Metcalfe, Nigel] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Martin, Nicolas] Observ Astron, F-67000 Strasbourg, France. RP Green, GM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ggreen@cfa.harvard.edu OI Schlafly, Edward Ford/0000-0002-3569-7421; Green, Gregory/0000-0001-5417-2260; Chambers, Kenneth /0000-0001-6965-7789; Metcalfe, Nigel/0000-0001-9034-4402; Flewelling, Heather/0000-0002-1050-4056 FU Institute for Astronomy; University of Hawaii; PS1 Project Office; Max- Planck Society; Max Planck Institute for Astronomy; Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching; Johns Hopkins University; Durham University; University of Edinburgh; Queens University Belfast; Harvard- Smithsonian Center for Astrophysics; Las Cumbres Observatory Global Telescope Network Incorporated; National Central University of Taiwan; Space Telescope Science Institute; National Aeronautics and Space Administration through Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877]; University of Maryland; Eotvos Lorand University (ELTE); NSF [AST-1312891] FX The Pan-STARRS1 (PS1) surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the PS1 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, Queens 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, the University of Maryland, and Eotvos Lorand University (ELTE). Gregory M. Green and Douglas P. Finkbeiner are partially supported by NSF grant AST-1312891. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. NR 53 TC 28 Z9 28 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2014 VL 783 IS 2 AR 144 DI 10.1088/0004-637X/783/2/114 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900050 ER PT J AU Reid, MJ Menten, KM Brunthaler, A Zheng, XW Dame, TM Xu, Y Wu, Y Zhang, B Sanna, A Sato, M Hachisuka, K Choi, YK Immer, K Moscadelli, L Rygl, KLJ Bartkiewicz, A AF Reid, M. J. Menten, K. M. Brunthaler, A. Zheng, X. W. Dame, T. M. Xu, Y. Wu, Y. Zhang, B. Sanna, A. Sato, M. Hachisuka, K. Choi, Y. K. Immer, K. Moscadelli, L. Rygl, K. L. J. Bartkiewicz, A. TI TRIGONOMETRIC PARALLAXES OF HIGH MASS STAR FORMING REGIONS: THE STRUCTURE AND KINEMATICS OF THE MILKY WAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: fundamental parameters; Galaxy: kinematics and dynamics; Galaxy: structure; gravitational waves; parallaxes; stars: formation ID LOCAL STELLAR KINEMATICS; PERSEUS SPIRAL ARM; BASE-LINE ARRAY; GALACTIC-CENTER; ROTATION CURVE; BLACK-HOLE; FUNDAMENTAL PARAMETERS; CIRCULAR-VELOCITY; DENSITY PROFILE; VERA ESTIMATION AB Over 100 trigonometric parallaxes and proper motions for masers associated with young, high- mass stars have been measured with the Bar and Spiral Structure Legacy Survey, a Very Long Baseline Array key science project, the European VLBI Network, and the Japanese VLBI Exploration of Radio Astrometry project. These measurements provide strong evidence for the existence of spiral arms in the MilkyWay, accurately locating many arm segments and yielding spiral pitch angles ranging from about 7 degrees to 20 degrees. The widths of spiral arms increase with distance from the Galactic center. Fitting axially symmetric models of the MilkyWay with the three- dimensional position and velocity information and conservative priors for the solar and average source peculiar motions, we estimate the distance to the Galactic center, R-0, to be 8.34 +/- 0.16 kpc, a circular rotation speed at the Sun, Theta(0), to be 240 +/- 8 km s(-1), and a rotation curve that is nearly flat ( i. e., a slope of -0.2 +/- 0.4 km s(-1) kpc(-1)) between Galactocentric radii of approximate to 5 and 16 kpc. Assuming a " universal" spiral galaxy form for the rotation curve, we estimate the thin disk scale length to be 2.44 +/- 0.16 kpc. With this large data set, the parameters R-0 and Theta(0) are no longer highly correlated and are relatively insensitive to different forms of the rotation curve. If one adopts a theoretically motivated prior that high- mass star forming regions are in nearly circular Galactic orbits, we estimate a global solar motion component in the direction of Galactic rotation, V-circle dot = 14.6 +/- 5.0 km s(-1). While Theta(0) and V-circle dot are significantly correlated, the sum of these parameters is well constrained, Theta(0) + V circle dot = 255.2 +/- 5.1 km s(-1), as is the angular speed of the Sun in its orbit about the Galactic center, ( Theta(0) + V-circle dot)/R-0 = 30.57 +/- 0.43 km s(-1) kpc(-1). These parameters improve the accuracy of estimates of the accelerations of the Sun and the Hulse-Taylor binary pulsar in their Galactic orbits, significantly reducing the uncertainty in tests of gravitational radiation predicted by general relativity. C1 [Reid, M. J.; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K. M.; Brunthaler, A.; Wu, Y.; Zhang, B.; Sanna, A.; Sato, M.; Choi, Y. K.; Immer, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Zheng, X. W.] Nanjing Univ, Dept Astron, Nanjing 210093, Jiangsu, Peoples R China. [Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. [Hachisuka, K.] Shanghai Astron Observ, Shanghai, Peoples R China. [Moscadelli, L.] Arcetri Observ, Florence, Italy. [Rygl, K. L. J.] European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands. [Bartkiewicz, A.] Nicholas Copernicus Univ, Ctr Astron, Fac Phys Astron & Informat, PL-87100 Torun, Poland. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Bartkiewicz, Anna/D-6212-2014; OI Moscadelli, Luca/0000-0002-8517-8881 FU ERC [GLOSTAR (247078)]; National Science Foundation of China [10921063, 11073046, 11073054, 11133008]; Key Laboratory for Radio Astronomy; Chinese Academy of Sciences; National Science Centre Poland [2011/03/B/ST9/00627] FX This work was partially funded by the ERC Advanced Investigator Grant GLOSTAR (247078).The work was supported in part by the National Science Foundation of China (under grants 10921063, 11073046, 11073054 and 11133008) and the Key Laboratory for Radio Astronomy, Chinese Academy of Sciences.A.B.acknowledges support by the National Science Centre Poland through grant 2011/03/B/ST9/00627. NR 93 TC 250 Z9 252 U1 2 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2014 VL 783 IS 2 AR 130 DI 10.1088/0004-637X/783/2/130 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900066 ER PT J AU Steiner, JF McClintock, JE Orosz, JA Buxton, MM Bailyn, CD Remillard, RA Kara, E AF Steiner, James F. McClintock, Jeffrey E. Orosz, Jerome A. Buxton, Michelle M. Bailyn, Charles D. Remillard, Ronald A. Kara, Erin TI MODELING THE OPTICAL-X-RAY ACCRETION LAG IN LMC X-3: INSIGHTS INTO BLACK-HOLE ACCRETION PHYSICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; X-rays:binaries ID LONG-TERM VARIABILITY; GRO J1655-40; DISK; DISCOVERY; TOMOGRAPHY; VISCOSITY; EMISSION; BINARIES; DOPPLER; SYSTEMS AB The X- ray persistence and characteristically soft spectrum of the black hole X-ray binary LMCX-3make this source a touchstone for penetrating studies of accretion physics. We analyze a rich, ten-year collection of optical/infrared (OIR) time-series data in conjunction with all available contemporaneous X-ray data collected by the All-Sky Monitor and Proportional Counter Array detectors aboard the Rossi X-ray Timing Explorer. A cross-correlation analysis reveals an X-ray lag of approximate to 2 weeks. Motivated by this result, we develop a model that reproduces the complex OIR light curves of LMC X-3. The model is comprised of three components of emission: stellar light, accretion luminosity from the outer disk inferred from the time-lagged X-ray emission, and light from the X-ray-heated star and outer disk. Using the model, we filter a strong noise component out of the ellipsoidal light curves and derive an improved orbital period for the system. Concerning accretion physics, we find that the local viscous timescale in the disk increases with the local mass accretion rate; this in turn implies that the viscosity parameter a decreases with increasing luminosity. Finally, we find that X-ray heating is a strong function of X-ray luminosity below approximate to 50% of the Eddington limit, while above this limit X-ray heating is heavily suppressed. We ascribe this behavior to the strong dependence of the flaring in the disk upon X-ray luminosity, concluding that for luminosities above approximate to 50% of Eddington, the star lies fully in the shadow of the disk. C1 [Steiner, James F.; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Buxton, Michelle M.; Bailyn, Charles D.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Remillard, Ronald A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kara, Erin] Univ Cambridge, Dept Astron, Cambridge CB3 0HA, England. RP Steiner, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jsteiner@cfa.harvard.edu NR 51 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2014 VL 783 IS 2 DI 10.1088/0004-637X/783/2/101 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900037 ER PT J AU Tsukagoshi, T Momose, M Hashimoto, J Kudo, T Andrews, S Saito, M Kitamura, Y Ohashi, N Wilner, D Kawabe, R Abe, L Akiyama, E Brandner, W Brandt, TD Carson, J Currie, T Egner, SE Goto, M Grady, C Guyon, O Hayano, Y Hayashi, M Hayashi, S Henning, T Hodapp, KW Ishii, M Iye, M Janson, M Kandori, R Knapp, GR Kusakabe, N Kuzuhara, M Kwon, J McElwain, M Matsuo, T Mayama, S Miyama, S Morino, JI Moro-Martin, A Nishimura, T Pyo, TS Serabyn, E Suenaga, T Suto, H Suzuki, R Takahashi, Y Takami, H Takami, M Takato, N Terada, H Thalmann, C Tomono, D Turner, EL Usuda, T Watanabe, M Wisniewski, JP Yamada, T Tamura, M AF Tsukagoshi, Takashi Momose, Munetake Hashimoto, Jun Kudo, Tomoyuki Andrews, Sean Saito, Masao Kitamura, Yoshimi Ohashi, Nagayoshi Wilner, David Kawabe, Ryohei Abe, Lyu Akiyama, Eiji Brandner, Wolfgang Brandt, Timothy D. Carson, Joseph Currie, Thayne Egner, Sebastian E. Goto, Miwa Grady, Carol Guyon, Olivier Hayano, Yutaka Hayashi, Masahiko Hayashi, Saeko Henning, Thomas Hodapp, Klaus W. Ishii, Miki Iye, Masanori Janson, Markus Kandori, Ryo Knapp, Gillian R. Kusakabe, Nobuhiko Kuzuhara, Masayuki Kwon, Jungmi McElwain, Mike Matsuo, Taro Mayama, Satoshi Miyama, Shoken Morino, Jun-Ichi Moro-Martin, Amaya Nishimura, Tetsuro Pyo, Tae-Soo Serabyn, Eugene Suenaga, Takuya Suto, Hiroshi Suzuki, Ryuji Takahashi, Yasuhiro Takami, Hideki Takami, Michihiro Takato, Naruhisa Terada, Hiroshi Thalmann, Christian Tomono, Daigo Turner, Edwin L. Usuda, Tomonori Watanabe, Makoto Wisniewski, John P. Yamada, Toru Tamura, Motohide TI HIGH- RESOLUTION SUBMILLIMETER AND NEAR-INFRARED STUDIES OF THE TRANSITION DISK AROUND Sz 91 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars:individual (Sz 91); stars:pre-main sequence ID T-TAURI STARS; CIRCUMSTELLAR DUST DISKS; MAIN-SEQUENCE STARS; PROTOPLANETARY-DISK; PLANET FORMATION; MILLIMETER EMISSION; UPPER SCORPIUS; MOLECULAR GAS; RHO-OPHIUCHI; LKCA 15 AB To reveal the structures of a transition disk around a young stellar object in Lupus, Sz 91, we have performed aperture synthesis 345 GHz continuum and CO(3-2) observations with the Submillimeter Array (similar to 1"-3" resolution) and high-resolution imaging of polarized intensity at the K-s-band using the HiCIAO instrument on the Subaru Telescope (0".25 resolution). Our observations successfully resolved the inner and outer radii of the dust disk to be 65 and 170 AU, respectively, which indicates that Sz 91 is a transition disk source with one of the largest known inner holes. The model fitting analysis of the spectral energy distribution reveals an H-2 mass of 2.4 Chi 10(-3) M-circle dot in the cold (T < 30 K) outer part at 65 AU < r < 170 AU by assuming a canonical gas-to-dust mass ratio of 100, although a small amount (> 3 Chi 10(-9)M(circle dot)) of hot (T similar to 180 K) dust possibly remains inside the inner hole of the disk. The structure of the hot component could be interpreted as either an unresolved self-luminous companion body (not directly detected in our observations) or a narrow ring inside the inner hole. Significant CO(3-2) emission with a velocity gradient along the major axis of the dust disk is concentrated on the Sz 91 position, suggesting a rotating gas disk with a radius of 420 AU. The Sz 91 disk is possibly a rare disk in an evolutionary stage immediately after the formation of protoplanets because of the large inner hole and the lower disk mass than other transition disks studied thus far. C1 [Tsukagoshi, Takashi; Momose, Munetake] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan. [Kudo, Tomoyuki; Saito, Masao; Ohashi, Nagayoshi; Kawabe, Ryohei; Akiyama, Eiji; Hayashi, Masahiko; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Kusakabe, Nobuhiko; Kuzuhara, Masayuki; Morino, Jun-Ichi; Suto, Hiroshi; Suzuki, Ryuji; Takami, Hideki; Takami, Michihiro] Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. [Kitamura, Yoshimi] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Andrews, Sean; Wilner, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hashimoto, Jun] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Takahashi, Yasuhiro; Tamura, Motohide] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lboratoire Lagrange UMR 7293, F-06108 Nice 2, France. [Abe, Lyu] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Brandner, Wolfgang; Henning, Thomas; Janson, Markus; Knapp, Gillian R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Brandt, Timothy D.; Turner, Edwin L.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Carson, Joseph] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Egner, Sebastian E.; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko; Nishimura, Tetsuro; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo; Usuda, Tomonori] Subaru Telescope, Hilo, HI 96720 USA. [Goto, Miwa] Univ Munich, Univ Sternwarte, D-81679 Munich, Germany. [Grady, Carol] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Hodapp, Klaus W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Kuzuhara, Masayuki] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. [McElwain, Mike] Grad Univ Adv Studies SOKENDAI, Hayama, Kanagawa 2400193, Japan. [Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Miyama, Shoken] Hiroshima Univ, Higashihiroshima, Hiroshima 7398511, Japan. [Moro-Martin, Amaya] CSIC, CAB, INTA, Dept Astrophys, E-28850 Madrid, Spain. [Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Takami, Michihiro] Univ Tokyo, Sch Sci, Tokyo 1130033, Japan. [Thalmann, Christian] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Watanabe, Makoto] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Wisniewski, John P.] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan. [Yamada, Toru] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Kwon, Jungmi; Mayama, Satoshi; Suenaga, Takuya] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. RP Tsukagoshi, T (reprint author), Ibaraki Univ, Coll Sci, Bunkyo 2-1-1, Mito, Ibaraki 3108512, Japan. EM ttsuka@mx.ibaraki.ac.jp RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016 OI Watanabe, Makoto/0000-0002-3656-4081 FU MEXT; JSPS KAKENHI [24103504, 23103004]; NSF [T-1009203]; Academia Sinica Institute of Astronomy and Astrophysics; Smithsonian Institution; Academia Sinica FX We are grateful for the ASTE and AzTEC staff for the operation and maintenance of the observation instruments. A part of this work was conducted as the Observatory Project of "SEEDS: Strategic Explorations of Exoplanets and Disks with Subaru" supported by the MEXT Grant-in-Aid for Scientific Research on Priority Areas. This work is partially supported by JSPS KAKENHI grant numbers 24103504 (T.T.) and 23103004 (M.M.). J.C. gratefully acknowledges support from NSF grant AST-1009203. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NR 65 TC 14 Z9 14 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2014 VL 783 IS 2 AR 90 DI 10.1088/0004-637X/783/2/90 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900026 ER PT J AU Wilkins, AN Deming, D Madhusudhan, N Burrows, A Knutson, H McCullough, P Ranjan, S AF Wilkins, Ashlee N. Deming, Drake Madhusudhan, Nikku Burrows, Adam Knutson, Heather McCullough, Peter Ranjan, Sukrit TI THE EMERGENT 1.1-1.7 mu m SPECTRUM OF THE EXOPLANET COROT-2B AS MEASURED USING THE HUBBLE SPACE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: atmospheres; planets and satellites: individual (CoRoT-2b); stars: individual (CoRoT-2); techniques: photometric; techniques: spectroscopic ID EXTRASOLAR GIANT PLANETS; HD 209458B; TRANSMISSION SPECTROSCOPY; SECONDARY ECLIPSE; TRANSITING EXOPLANETS; LIGHT CURVES; HOT; ATMOSPHERES; EMISSION; 189733B AB We have used Hubble/WFC3 and the G141 grism to measure the secondary eclipse of the transiting, very hot Jupiter CoRoT-2b in the 1.1-1.7 mu m spectral region. We find an eclipse depth averaged over this band equal to 395(-45)(+69) parts per million, equivalent to a blackbody temperature of 1788 +/- 18 K. We study and characterize several WFC3 instrumental effects, especially the "hook" phenomenon described by Deming et al. We use data from several transiting exoplanet systems to find a quantitative relation between the amplitude of the hook and the exposure level of a given pixel. Although the uncertainties in this relation are too large to allow us to develop an empirical correction for our data, our study provides a useful guide for optimizing exposure levels in future WFC3 observations. We derive the planet's spectrum using a differential method. The planet-to-star contrast increases to longer wavelength within the WFC3 bandpass, but without water absorption or emission to a 3 sigma limit of 85 ppm. The slope of the WFC3 spectrum is significantly less than the slope of the best-fit blackbody. We compare all existing eclipse data for this planet to a blackbody spectrum, and to spectra from both solar abundance and carbon-rich (C/O = 1) models. A blackbody spectrum is an acceptable fit to the full data set. Extra continuous opacity due to clouds or haze, and flattened temperature profiles, are strong candidates to produce quasi-blackbody spectra, and to account for the amplitude of the optical eclipses. Our results show ambiguous evidence for a temperature inversion in this planet. C1 [Wilkins, Ashlee N.; Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Madhusudhan, Nikku] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Knutson, Heather] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [McCullough, Peter] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ranjan, Sukrit] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wilkins, AN (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM awilkins@astro.umd.edu NR 43 TC 20 Z9 20 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2014 VL 783 IS 2 AR 113 DI 10.1088/0004-637X/783/2/113 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG5DQ UT WOS:000335439900049 ER PT J AU Lockwood, AC Johnson, JA Bender, CF Carr, JS Barman, T Richert, AJW Blake, GA AF Lockwood, Alexandra C. Johnson, John A. Bender, Chad F. Carr, John S. Barman, Travis Richert, Alexander J. W. Blake, Geoffrey A. TI NEAR-IR DIRECT DETECTION OF WATER VAPOR IN TAU BOOTIS b SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: atmospheres; techniques: spectroscopic ID ORBITAL MOTION; MU-M; SPECTRUM; PLANETS; MASS; ATMOSPHERES; SPECTROGRAPH; EXOPLANETS; TELESCOPE; ALGORITHM AB We use high dynamic range, high-resolution L-band spectroscopy to measure the radial velocity (RV) variations of the hot Jupiter in the tau Bootis planetary system. The detection of an exoplanet by the shift in the stellar spectrum alone provides a measure of the planet's minimum mass, with the true mass degenerate with the unknown orbital inclination. Treating the tau Boo system as a high flux ratio double-lined spectroscopic binary permits the direct measurement of the planet's true mass as well as its atmospheric properties. After removing telluric absorption and cross-correlating with a model planetary spectrum dominated by water opacity, we measure a 6 sigma detection of the planet at K-p = 111 +/- 5 km s(-1), with a 1 sigma upper limit on the spectroscopic flux ratio of 10(-4). This RV leads to a planetary orbital inclination of i = 45(-4)(+3)degrees. and a mass of M-P = 5.90(-0.20)(+0.35) M-Jup. We report the first detection of water vapor in the atmosphere of a non-transiting hot Jupiter, tau Boo b. C1 [Lockwood, Alexandra C.; Johnson, John A.; Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Johnson, John A.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Bender, Chad F.; Richert, Alexander J. W.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Bender, Chad F.; Richert, Alexander J. W.] Penn State Univ, Ctr Exoplanet & Habitable Worlds, University Pk, PA 16802 USA. [Carr, John S.] Naval Res Lab, Washington, DC 20375 USA. [Barman, Travis] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Lockwood, AC (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM alock@caltech.edu OI Richert, Alexander/0000-0002-9613-6863 FU W. M. Keck Foundation; NSF GRFP program; NSF AAG program; David and Lucile Packard Foundation; Alfred P. Sloan Foundation; Center for Exoplanets and Habitable Worlds; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; 6.1 base funding FX The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA, and was made possible by the financial support of the W. M. Keck Foundation. A.C.L. and G.A.B. gratefully acknowledge support from the NSF GRFP and AAG programs, JAJ the generous grants from the David and Lucile Packard and Alfred P. Sloan Foundations, and C.F.B. support from the Center for Exoplanets and Habitable Worlds, which is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. Basic research in infrared astronomy at the Naval Research Laboratory is supported by 6.1 base funding. We thank Jacques Sauval for kindly providing a copy of his solar linelist. Finally, the authors wish to acknowledge the significant cultural role of the summit of Mauna Kea. NR 40 TC 24 Z9 24 U1 2 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2014 VL 783 IS 2 AR L29 DI 10.1088/2041-8205/783/2/L29 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC4UJ UT WOS:000332516300005 ER PT J AU Sridharan, TK Rao, R Qiu, K Cortes, P Li, H Pillai, T Patel, NA Zhang, Q AF Sridharan, T. K. Rao, R. Qiu, K. Cortes, P. Li, H. Pillai, T. Patel, N. A. Zhang, Q. TI HOT CORE, OUTFLOWS, AND MAGNETIC FIELDS IN W43-MM1 (G30.79 FIR 10) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: jets and outflows; ISM: magnetic fields; stars: formation; stars: massive ID STAR-FORMING REGIONS; MASS PROTOSTELLAR CANDIDATES; SUBMILLIMETER ARRAY; THERMAL EMISSION; POLARIZATION; EVOLUTION; DUST; AMMONIA; W43; PROTOSTARS AB We present submillimeter spectral line and dust continuum polarization observations of a remarkable hot core and multiple outflows in the high-mass, star-forming region W43-MM1 (G30.79 FIR 10), obtained using the Submillimeter Array. A temperature of similar to 400 K is estimated for the hot core using CH3CN (J = 19-18) lines, with detections of 11 K-ladder components. The high temperature and the mass estimates for the outflows indicate high-mass star formation. The continuum polarization pattern shows an ordered distribution, and its orientation over the main outflow appears to be aligned with the outflow. The derived magnetic field indicates slightly super-critical conditions. While the magnetic and outflow energies are comparable, the B-field orientation appears to have changed from parsec scales to similar to 0.1 pc scales during the core/star formation process. C1 [Sridharan, T. K.; Qiu, K.; Li, H.; Pillai, T.; Patel, N. A.; Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rao, R.] Acad Sinica, Inst Astron & Astrophys, Hilo, HI 96720 USA. [Qiu, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Qiu, K.] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. [Cortes, P.] Natl Radio Astron Observ, Joint ALMA Off, Santiago, Chile. [Li, H.] Max Planck Inst Astron, Hiedelberg, Germany. [Li, H.] Chinese Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Pillai, T.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. RP Sridharan, TK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tksridha@cfa.harvard.edu OI Zhang, Qizhou/0000-0003-2384-6589 FU Smithsonian Institution; Academia Sinica FX The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, and is funded by the Smithsonian Institution and the Academia Sinica. NR 41 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2014 VL 783 IS 2 AR L31 DI 10.1088/2041-8205/783/2/L31 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC4UJ UT WOS:000332516300007 ER PT J AU Keitel, D Prix, R Papa, MA Leaci, P Siddiqi, M AF Keitel, David Prix, Reinhard Papa, Maria Alessandra Leaci, Paola Siddiqi, Maham TI Search for continuous gravitational waves: Improving robustness versus instrumental artifacts SO PHYSICAL REVIEW D LA English DT Article ID NEUTRON-STARS AB The standard multidetector F-statistic for continuous gravitational waves is susceptible to false alarms from instrumental artifacts, for example monochromatic sinusoidal disturbances ("lines"). This vulnerability to line artifacts arises because the F-statistic compares the signal hypothesis to a Gaussian-noise hypothesis, and hence is triggered by anything that resembles the signal hypothesis more than Gaussian noise. Various ad-hoc veto methods to deal with such line artifacts have been proposed and used in the past. Here we develop a Bayesian framework that includes an explicit alternative hypothesis to model disturbed data. We introduce a simple line model that defines lines as signal candidates appearing only in one detector. This allows us to explicitly compute the odds between the signal hypothesis and an extended noise hypothesis, resulting in a new detection statistic that is more robust to instrumental artifacts. We present and discuss results from Monte-Carlo tests on both simulated data and on detector data from the fifth LIGO science run. We find that the line-robust statistic retains the detection power of the standard F-statistic in Gaussian noise. In the presence of line artifacts it is more sensitive, even compared to the popular F-statistic consistency veto, over which it improves by as much as a factor of two in detectable signal strength. C1 [Keitel, David; Prix, Reinhard; Papa, Maria Alessandra; Leaci, Paola; Siddiqi, Maham] Albert Einstein Inst, D-30167 Hannover, Germany. [Papa, Maria Alessandra; Leaci, Paola] Albert Einstein Inst, D-14476 Golm, Germany. [Papa, Maria Alessandra] Univ Wisconsin, Milwaukee, WI 53201 USA. [Siddiqi, Maham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Keitel, D (reprint author), Albert Einstein Inst, Callinstr 38, D-30167 Hannover, Germany. EM David.Keitel@aei.mpg.de; Reinhard.Prix@aei.mpg.de OI Keitel, David/0000-0002-2824-626X; Prix, Reinhard/0000-0002-3789-6424; Papa, M.Alessandra/0000-0002-1007-5298 FU "Sonderforschungsbereich" Collaborative Research Centre [SFB/TR7]; IMPRS on Gravitational Wave Astronomy; LIGO [LIGO-P1300167]; AEI-preprint [AEI-2013-260] FX This work has benefited from numerous discussions and comments from colleagues, in particular John T. Whelan, Karl Wette, Evan Goetz, Berit Behnke, Heinz-Bernd Eggenstein, and Thomas Dent. We acknowledge the LIGO Scientific Collaboration for providing the data from the LIGO S5 run. The injection studies were carried out on the ATLAS cluster at AEI Hannover. P. L. and M. A. P. acknowledge support of the "Sonderforschungsbereich" Collaborative Research Centre (SFB/TR7). D. K. was supported by the IMPRS on Gravitational Wave Astronomy. This paper has been assigned LIGO document number LIGO-P1300167 and AEI-preprint number AEI-2013-260. NR 50 TC 13 Z9 13 U1 2 U2 4 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 MAR 10 PY 2014 VL 89 IS 6 AR 064023 DI 10.1103/PhysRevD.89.064023 PG 19 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AD3AD UT WOS:000333107900004 ER PT J AU DiTommaso, A Morris, SH Parker, JD Cone, CL Agrawal, AA AF DiTommaso, Antonio Morris, Scott H. Parker, John D. Cone, Caitlin L. Agrawal, Anurag A. TI Deer Browsing Delays Succession by Altering Aboveground Vegetation and Belowground Seed Banks SO PLOS ONE LA English DT Article ID WHITE-TAILED DEER; COMMUNITY STRUCTURE; FOREST ECOSYSTEMS; PLANT-COMMUNITIES; COASTAL-PLAIN; DISTURBANCE; DISPERSAL; DIVERSITY; DYNAMICS; REDUCTIONS AB Soil seed bank composition is important to the recovery of natural and semi-natural areas from disturbance and serves as a safeguard against environmental catastrophe. White-tailed deer (Odocoileus virginianus) populations have increased dramatically in eastern North America over the past century and can have strong impacts on aboveground vegetation, but their impacts on seed bank dynamics are less known. To document the long-term effects of deer browsing on plant successional dynamics, we studied the impacts of deer on both aboveground vegetation and seed bank composition in plant communities following agricultural abandonment. In 2005, we established six 15615 m fenced enclosures and paired open plots in recently fallowed agricultural fields near Ithaca, NY, USA. In late October of each of six years (2005-2010), we collected soil from each plot and conducted seed germination cycles in a greenhouse to document seed bank composition. These data were compared to measurements of aboveground plant cover (2005-2008) and tree density (2005-2012). The impacts of deer browsing on aboveground vegetation were severe and immediate, resulting in significantly more bare soil, reduced plant biomass, reduced recruitment of woody species, and relatively fewer native species. These impacts persisted throughout the experiment. The impacts of browsing were even stronger on seed bank dynamics. Browsing resulted in significantly decreased overall species richness (but higher diversity), reduced seed bank abundance, relatively more short-lived species (annuals and biennials), and fewer native species. Both seed bank richness and the relative abundance of annuals/biennials were mirrored in the aboveground vegetation. Thus, deer browsing has long-term and potentially reinforcing impacts on secondary succession, slowing succession by selectively consuming native perennials and woody species and favoring the persistence of short-lived, introduced species that continually recruit from an altered seed bank. C1 [DiTommaso, Antonio; Morris, Scott H.; Cone, Caitlin L.] Cornell Univ, Dept Crop & Soil Sci, Ithaca, NY 14850 USA. [Parker, John D.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Agrawal, Anurag A.] Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY USA. RP DiTommaso, A (reprint author), Cornell Univ, Dept Crop & Soil Sci, Ithaca, NY 14850 USA. EM ad97@cornell.edu RI Parker, John/F-9761-2010 OI Parker, John/0000-0002-3632-7625 FU NSF [DEB-1118783]; United States Department of Agriculture [NYC-183430] FX This work was funded by NSF DEB-1118783 and federal formula funds from the United States Department of Agriculture (Hatch project NYC-183430) to AAA. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 50 TC 7 Z9 7 U1 6 U2 65 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAR 7 PY 2014 VL 9 IS 3 AR e91155 DI 10.1371/journal.pone.0091155 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC4IY UT WOS:000332485800108 PM 24608258 ER PT J AU Kay, AD Bruning, AJ van Alst, A Abrahamson, TT Hughes, WOH Kaspari, M AF Kay, Adam D. Bruning, Abbie J. van Alst, Andy Abrahamson, Tyler T. Hughes, W. O. H. Kaspari, Michael TI A carbohydrate-rich diet increases social immunity in ants SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE ants; disease resistance; ecoimmunology; geometric framework; nutrition; social behaviour ID LEAF-CUTTING ANTS; DISEASE RESISTANCE; TRADE-OFFS; EVOLUTIONARY ECOLOGY; METAPLEURAL GLAND; ARGENTINE ANTS; PROTEIN COSTS; COMPETITION; EXPRESSION; NUTRITION AB Increased potential for disease transmission among nest-mates means living in groups has inherent costs. This increased potential is predicted to select for disease resistance mechanisms that are enhanced by cooperative exchanges among group members, a phenomenon known as social immunity. One potential mediator of social immunity is diet nutritional balance because traits underlying immunity can require different nutritional mixtures. Here, we show how dietary protein-carbohydrate balance affects social immunity in ants. When challenged with a parasitic fungus Metarhizium anisopliae, workers reared on a high-carbohydrate diet survived approximately 2.8x longer in worker groups than in solitary conditions, whereas workers reared on an isocaloric, high-protein diet survived only approximately 1.3x longer in worker groups versus solitary conditions. Nutrition had little effect on social grooming, a potential mechanism for social immunity. However, experimentally blocking metapleural glands, which secrete antibiotics, completely eliminated effects of social grouping and nutrition on immunity, suggesting a causal role for secretion exchange. A carbohydrate-rich diet also reduced worker mortality rates when whole colonies were challenged with Metarhizium. These results provide a novel mechanism by which carbohydrate exploitation could contribute to the ecological dominance of ants and other social groups. C1 [Kay, Adam D.; Bruning, Abbie J.; van Alst, Andy; Abrahamson, Tyler T.] Univ St Thomas, Dept Biol, St Paul, MN 55105 USA. [Hughes, W. O. H.] Univ Sussex, Sch Life Sci, Brighton, E Sussex, England. [Kaspari, Michael] Univ Oklahoma, Dept Zool, Grad Program EEB, Norman, OK 73019 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama. RP Kay, AD (reprint author), Univ St Thomas, Dept Biol, St Paul, MN 55105 USA. EM adkay@stthomas.edu FU National Science Foundation of the United States [DEB 0842038, REU 1214433] FX Financial support was provided by a grant from the National Science Foundation of the United States (DEB 0842038 to A. D. K. and M. K., and REU 1214433 to A.D.K.). NR 46 TC 8 Z9 8 U1 13 U2 82 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 MAR 7 PY 2014 VL 281 IS 1778 AR 20132374 DI 10.1098/rspb.2013.2374 PG 6 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AC2YN UT WOS:000332382300004 PM 24430844 ER PT J AU Lobo, E Dalling, JW AF Lobo, Elena Dalling, James W. TI Spatial scale and sampling resolution affect measures of gap disturbance in a lowland tropical forest: implications for understanding forest regeneration and carbon storage SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Barro Colorado Island; light detecting and ranging; gap dynamics; forest succession ID PHASE REGENERATION; RAIN-FORESTS; TREE DIVERSITY; LANDSCAPE; DYNAMICS; REGIMES; AMAZON; PANAMA; STATE; BIAS AB Treefall gaps play an important role in tropical forest dynamics and in determining above-ground biomass (AGB). However, our understanding of gap disturbance regimes is largely based either on surveys of forest plots that are small relative to spatial variation in gap disturbance, or on satellite imagery, which cannot accurately detect small gaps. We used high-resolution light detection and ranging data from a 1500 ha forest in Panama to: (i) determine how gap disturbance parameters are influenced by study area size, and the criteria used to define gaps; and (ii) to evaluate how accurately previous ground-based canopy height sampling can determine the size and location of gaps. We found that plot-scale disturbance parameters frequently differed significantly from those measured at the landscape-level, and that canopy height thresholds used to define gaps strongly influenced the gap-size distribution, an important metric influencing AGB. Furthermore, simulated ground surveys of canopy height frequently misrepresented the true location of gaps, which may affect conclusions about how relatively small canopy gaps affect successional processes and contribute to the maintenance of diversity. Across site comparisons need to consider how gap definition, scale and spatial resolution affect characterizations of gap disturbance, and its inferred importance for carbon storage and community composition. C1 [Lobo, Elena] DMCii, Guildford GU2 7AG, Surrey, England. [Lobo, Elena; Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Dalling, James W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Lobo, E (reprint author), DMCii, Guildford GU2 7AG, Surrey, England. EM elobo2@illinois.edu FU NSF [0939907]; Smithsonian Tropical Research Institute; University of Illinois; University of California Los Angeles; Clemson University FX This study was financially supported by NSF grant no. 0939907, and with additional support from the Smithsonian Tropical Research Institute, University of Illinois, University of California Los Angeles and Clemson University. NR 31 TC 6 Z9 6 U1 0 U2 31 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 MAR 7 PY 2014 VL 281 IS 1778 AR 20133218 DI 10.1098/rspb.2013.3218 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AC2YN UT WOS:000332382300025 PM 24452032 ER PT J AU Davies, N Field, D Amaral-Zettler, L Clark, MS Deck, J Drummond, A Faith, DP Geller, J Gilbert, J Glockner, FO Hirsch, PR Leong, JA Meyer, C Obst, M Planes, S Scholin, C Vogler, AP Gates, RD Toonen, R Berteaux-Lecellier, V Barbier, M Barker, K Bertilsson, S Bicak, M Bietz, MJ Bobe, J Bodrossy, L Borja, A Coddington, J Fuhrman, J Gerdts, G Gillespie, R Goodwin, K Hanson, PC Hero, JM Hoekman, D Jansson, J Jeanthon, C Kao, R Klindworth, A Knight, R Kottmann, R Koo, MS Kotoulas, G Lowe, AJ Marteinsson, VT Meyer, F Morrison, N Myrold, DD Pafilis, E Parker, S Parnell, JJ Polymenakou, PN Ratnasingham, S Roderick, GK Rodriguez-Ezpeleta, N Schonrogge, K Simon, N Valette-Silver, NJ Springer, YP Stone, GN Stones-Havas, S Sansone, SA Thibault, KM Wecker, P Wichels, A Wooley, JC Yahara, T Zingone, A AF Davies, Neil Field, Dawn Amaral-Zettler, Linda Clark, Melody S. Deck, John Drummond, Alexei Faith, Daniel P. Geller, Jonathan Gilbert, Jack Gloeckner, Frank Oliver Hirsch, Penny R. Leong, Jo-Ann Meyer, Chris Obst, Matthias Planes, Serge Scholin, Chris Vogler, Alfried P. Gates, Ruth D. Toonen, Rob Berteaux-Lecellier, Veronique Barbier, Michele Barker, Katherine Bertilsson, Stefan Bicak, Mesude Bietz, Matthew J. Bobe, Jason Bodrossy, Levente Borja, Angel Coddington, Jonathan Fuhrman, Jed Gerdts, Gunnar Gillespie, Rosemary Goodwin, Kelly Hanson, Paul C. Hero, Jean-Marc Hoekman, David Jansson, Janet Jeanthon, Christian Kao, Rebecca Klindworth, Anna Knight, Rob Kottmann, Renzo Koo, Michelle S. Kotoulas, Georgios Lowe, Andrew J. Marteinsson, Viggo Thor Meyer, Folker Morrison, Norman Myrold, David D. Pafilis, Evangelos Parker, Stephanie Parnell, John Jacob Polymenakou, Paraskevi N. Ratnasingham, Sujeevan Roderick, George K. Rodriguez-Ezpeleta, Naiara Schonrogge, Karsten Simon, Nathalie Valette-Silver, Nathalie J. Springer, Yuri P. Stone, Graham N. Stones-Havas, Steve Sansone, Susanna-Assunta Thibault, Kate M. Wecker, Patricia Wichels, Antje Wooley, John C. Yahara, Tetsukazu Zingone, Adriana CA GOs-COS TI The founding charter of the Genomic Observatories Network SO GIGASCIENCE LA English DT Editorial Material DE Biodiversity; Genomics; Biocode; Earth observations ID BIODIVERSITY AB The co-authors of this paper hereby state their intention to work together to launch the Genomic Observatories Network (GOs Network) for which this document will serve as its Founding Charter. We define a Genomic Observatory as an ecosystem and/or site subject to long-term scientific research, including (but not limited to) the sustained study of genomic biodiversity from single-celled microbes to multicellular organisms. An international group of 64 scientists first published the call for a global network of Genomic Observatories in January 2012. The vision for such a network was expanded in a subsequent paper and developed over a series of meetings in Bremen (Germany), Shenzhen (China), Moorea (French Polynesia), Oxford (UK), Pacific Grove (California, USA), Washington (DC, USA), and London (UK). While this community-building process continues, here we express our mutual intent to establish the GOs Network formally, and to describe our shared vision for its future. The views expressed here are ours alone as individual scientists, and do not necessarily represent those of the institutions with which we are affiliated. C1 [Davies, Neil] Univ Calif Berkeley, Gump South Pacific Res Stn, Moorea 98728, Fr Polynesia. [Davies, Neil; Field, Dawn] Univ Oxford, Dept Zool, Biodivers Inst, Oxford OX1 3PS, England. [Field, Dawn; Bicak, Mesude; Sansone, Susanna-Assunta] Univ Oxford, Oxford E Res Ctr, Oxford OX1 3QG, England. [Field, Dawn; Schonrogge, Karsten] Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England. [Amaral-Zettler, Linda] Josephine Bay Paul Ctr Comparat Mol Biol & Evolut, Marine Biol Lab, Woods Hole, MA 02543 USA. [Clark, Melody S.] British Antarctic Survey, Nat Environm Res Council, Cambridge CB3 0ET, England. [Deck, John] Univ Calif Berkeley, Berkeley Nat Hist Museums, Valley Life Sci 1007, Berkeley, CA 94720 USA. [Drummond, Alexei] Univ Auckland, Dept Comp Sci, Auckland 1142, New Zealand. [Drummond, Alexei] Univ Auckland, Allan Wilson Ctr Mol Ecol & Evolut, Auckland 1, New Zealand. [Faith, Daniel P.] Australian Museum, Sydney, NSW 2010, Australia. [Geller, Jonathan] Calif State Univ, Moss Landing Marine Labs, Moss Landing, CA 95039 USA. [Gilbert, Jack; Meyer, Folker] Argonne Natl Lab, Inst Genom & Syst Biol, Argonne, IL 60439 USA. [Gilbert, Jack] Univ Chicago, Dept Ecol & Evolut, Chicago, IL 60637 USA. [Gloeckner, Frank Oliver; Klindworth, Anna; Kottmann, Renzo] Max Planck Inst Marine Microbiol, Microbial Genom & Bioinformat Res Grp, D-28359 Bremen, Germany. [Gloeckner, Frank Oliver; Klindworth, Anna; Kottmann, Renzo] Jacobs Univ Bremen, D-28759 Bremen, Germany. [Hirsch, Penny R.] Rothamsted Res, Harpenden AL5 2JQ, Herts, England. [Leong, Jo-Ann; Gates, Ruth D.; Toonen, Rob] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA. [Meyer, Chris] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Obst, Matthias] Univ Gothenburg, Dept Biol & Environm Sci, SE-40530 Gothenburg, Sweden. [Planes, Serge; Berteaux-Lecellier, Veronique; Wecker, Patricia] EPHE Ctr Rech Insulaire & Observ Environm CRIOBE, CNRS, USR 3278, Papetoai 98729, Moorea, Fr Polynesia. [Scholin, Chris] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. [Vogler, Alfried P.] Univ London Imperial Coll Sci Technol & Med, Dept Life Sci, London SW7 2AZ, England. [Vogler, Alfried P.] Nat Hist Museum, Dept Life Sci, London SW7 5BD, England. [Barker, Katherine; Coddington, Jonathan] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Bertilsson, Stefan] Uppsala Univ, Dept Ecol & Genet, SE-75236 Uppsala, Sweden. [Bertilsson, Stefan] Uppsala Univ, Sci Life Lab, SE-75236 Uppsala, Sweden. [Bietz, Matthew J.] Univ Calif Irvine, Dept Informat, Irvine, CA 92697 USA. [Bobe, Jason] PersonalGenomes Org, Boston, MA 02215 USA. [Bodrossy, Levente] CSIRO Marine & Atmospher Res & Wealth Oceans Natl, Hobart, Tas, Australia. [Borja, Angel] AZTI Tecnalia, Div Marine Res, Pasaia 20110, Spain. [Fuhrman, Jed; Wichels, Antje] Univ So Calif, Dept Biol Sci, Los Angeles, CA 90089 USA. [Gerdts, Gunnar] Alfred Wegener Inst Polar & Marine Res, Biol Anstalt Helgoland, D-27498 Helgoland, Germany. [Gillespie, Rosemary] Univ Calif Berkeley, Essig Museum Entomol, Berkeley, CA 94720 USA. [Goodwin, Kelly] NOAA, AOML Stationed La Jolla, La Jolla, CA 92037 USA. [Hanson, Paul C.] Univ Wisconsin, Ctr Limnol, Madison, WI 53706 USA. [Hero, Jean-Marc] Griffith Univ, Environm Futures Res Inst, Gold Coast, Qld 4222, Australia. [Hoekman, David; Parker, Stephanie; Parnell, John Jacob; Springer, Yuri P.; Thibault, Kate M.] Natl Ecol Observ Network, Boulder, CO 80301 USA. [Jansson, Janet] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA 94720 USA. [Jeanthon, Christian; Simon, Nathalie] UPMC, CNRS, Stn Biol Roscoff, F-29688 Roscoff, France. [Kao, Rebecca] Denver Bot Gardens, Denver, CO 80206 USA. [Knight, Rob] Howard Hughes Med Inst, Chevy Chase, MD USA. [Knight, Rob] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA. [Knight, Rob] Univ Colorado, Dept Comp Sci, Boulder, CO 80309 USA. [Knight, Rob] Univ Colorado, BioFrontiers Inst, Boulder, CO 80309 USA. [Koo, Michelle S.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. [Kotoulas, Georgios; Pafilis, Evangelos; Polymenakou, Paraskevi N.] HCMR, Inst Marine Biol Biotechnol & Aquaculture IMBBC, Iraklion, Greece. [Lowe, Andrew J.] Univ Adelaide, Terr Ecosyst Res Network, Adelaide, SA 5005, Australia. [Lowe, Andrew J.] Univ Adelaide, Inst Environm, Adelaide, SA 5005, Australia. [Marteinsson, Viggo Thor] Food Safety Environm & Genet, IS-113 Reykjavik, Iceland. [Morrison, Norman] Univ Manchester, Sch Comp Sci, Manchester M13 9PL, Lancs, England. [Myrold, David D.] Oregon State Univ, Dept Crop & Soil Sci, Corvallis, OR 97331 USA. [Ratnasingham, Sujeevan] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. [Roderick, George K.] Univ Calif Berkeley, Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Rodriguez-Ezpeleta, Naiara] AZTI Tecnalia, Div Marine Res, Sukarrieta 48395, Bizkaia, Spain. [Valette-Silver, Nathalie J.] NOAA, Off Explorat & Res, Silver Spring, MD 20910 USA. [Stone, Graham N.] Univ Edinburgh, Inst Evolutionary Biol, Edinburgh EH9 3JT, Midlothian, Scotland. [Stones-Havas, Steve] Biomatters Ltd, Auckland 1010, New Zealand. [Wooley, John C.] Univ Calif San Diego, Ctr Res BioSyst, La Jolla, CA 92093 USA. [Yahara, Tetsukazu] Kyushu Univ, Ctr Asian Conservat Ecol, Fukuoka 8128581, Japan. [Zingone, Adriana] Stn Zool, Ecol & Evolut Plankton Lab, I-80121 Naples, Italy. RP Davies, N (reprint author), Univ Calif Berkeley, Gump South Pacific Res Stn, BP 244, Moorea 98728, Fr Polynesia. EM ndavies@moorea.berkeley.edu; dfield@ceh.ac.uk RI Ratnasingham, Sujeevan/G-9103-2014; Drummond, Alexei/A-3209-2010; Davies, Neil/E-5863-2012; U-ID, Kyushu/C-5291-2016; Myrold, David/E-1813-2011; Hirsch, Penny/B-5135-2008; Goodwin, Kelly/B-4985-2014; Schonrogge, Karsten /E-8818-2010; Bodrossy, Levente/Q-3745-2016; Zingone, Adriana/E-4518-2010; Rodriguez-Ezpeleta, Naiara/B-7138-2014 OI Toonen, Rob/0000-0001-6339-4340; Drummond, Alexei/0000-0003-4454-2576; Davies, Neil/0000-0001-8085-5014; Myrold, David/0000-0001-6418-226X; Hirsch, Penny/0000-0002-5909-1934; Goodwin, Kelly/0000-0001-9583-8073; Schonrogge, Karsten /0000-0003-0122-6493; Bodrossy, Levente/0000-0001-6940-452X; Zingone, Adriana/0000-0001-5946-6532; Rodriguez-Ezpeleta, Naiara/0000-0001-6735-6755 FU Biotechnology and Biological Sciences Research Council [BB/E025080/1, BB/I000771/1] NR 5 TC 5 Z9 5 U1 2 U2 14 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND EI 2047-217X J9 GIGASCIENCE JI GigaScience PD MAR 7 PY 2014 VL 3 AR 2 DI 10.1186/2047-217X-3-2 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CX4EL UT WOS:000365651500001 PM 24606731 ER PT J AU Schultheiss, R Van Bocxlaer, B Riedel, F von Rintelen, T Albrecht, C AF Schultheiss, Roland Van Bocxlaer, Bert Riedel, Frank von Rintelen, Thomas Albrecht, Christian TI Disjunct distributions of freshwater snails testify to a central role of the Congo system in shaping biogeographical patterns in Africa SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Freshwater biogeography; East African Rift System; Congo; Lake Malawi; Lake Tanganyika; Zambezi ID SOUTH-CENTRAL AFRICA; DRAINAGE EVOLUTION; LAKE TANGANYIKA; LANDSCAPE EVOLUTION; SYNODONTIS CATFISH; SPECIES FLOCK; ANCIENT LAKES; EAST-AFRICA; RIFT; MOLLUSKS AB Background: The formation of the East African Rift System has decisively influenced the distribution and evolution of tropical Africa's biota by altering climate conditions, by creating basins for large long-lived lakes, and by affecting the catchment and drainage directions of river systems. However, it remains unclear how rifting affected the biogeographical patterns of freshwater biota through time on a continental scale, which is further complicated by the scarcity of molecular data from the largest African river system, the Congo. Results: We study these biogeographical patterns using a fossil-calibrated multi-locus phylogeny of the gastropod family Viviparidae. This group allows reconstructing drainage patterns exceptionally well because it disperses very poorly in the absence of existing freshwater connections. Our phylogeny covers localities from major drainage basins of tropical Africa and reveals highly disjunct sister-group relationships between (a) the endemic viviparids of Lake Malawi and populations from the Middle Congo as well as between (b) the Victoria region and the Okavango/ Upper Zambezi area. Conclusions: The current study testifies to repeated disruptions of the distribution of the Viviparidae during the formation of the East African Rift System, and to a central role of the Congo River system for the distribution of the continent's freshwater fauna during the late Cenozoic. By integrating our results with previous findings on palaeohydrographical connections, we provide a spatially and temporarily explicit model of historical freshwater biogeography in tropical Africa. Finally, we review similarities and differences in patterns of vertebrate and invertebrate dispersal. Amongst others we argue that the closest relatives of present day viviparids in Lake Malawi are living in the Middle Congo River, thus shedding new light on the origin of the endemic fauna of this rift lake. C1 [Schultheiss, Roland] Univ Turku, Dept Biol, Div Genet & Physiol, Turku 20014, Finland. [Schultheiss, Roland; Albrecht, Christian] Univ Giessen, Dept Anim Ecol & Systemat, D-35392 Giessen, Germany. [Van Bocxlaer, Bert] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol & Invertebrate Zool, Washington, DC 20013 USA. [Van Bocxlaer, Bert] Univ Ghent, Dept Geol & Soil Sci, Res Unit Palaeontol, B-9000 Ghent, Belgium. [Riedel, Frank] Free Univ Berlin, Inst Geol Sci, D-12249 Berlin, Germany. [Riedel, Frank] Yunnan Normal Univ, Key Lab Plateau Lake Ecol & Global Change, Chenggong, Kunming, Peoples R China. [von Rintelen, Thomas] Humboldt Univ, Leibniz Inst Evolut & Biodivers Forsch, Museum Naturkunde, D-10115 Berlin, Germany. RP Schultheiss, R (reprint author), Univ Turku, Dept Biol, Div Genet & Physiol, Itainen Pitkakatu 4, Turku 20014, Finland. EM rolsch@utu.fi FU DFG [AL 1076/5-2, AL 1076/6-2, RI 1738/3-1, RI 809/20-1, RI 809/20-2]; Flanders Research Foundation; Boyekoli Ebale Congo through the Belgian Federal Directorate General for Development Cooperation (DGDC); Belgian Science Policy (BELSPO) FX We are grateful to Andrew Goudie, Jacek Stankiewicz, and Woody Cotterill for an evaluation of the model. Daniel Engelhard, Thies Geertz, Andreas Schumann, Jean-Papy Mongindo, Ernest Tambwe, Martin Pickford, Ezra Mussime and Kitam Ali are thanked for support in the field and access to museum specimens. Romy Richter, Catharina Clewing, and Silvia Nachtigall provided assistance in the laboratory. The manuscript benefited from careful readings by Woody Cotterill, Thomas Wilke, Gene Hunt, and two anonymous reviewers. The study was funded by the DFG projects AL 1076/5-2, AL 1076/6-2, RI 1738/3-1, and RI 809/20-1,2. BVB is a Peter-Buck Fellow of the Smithsonian Institution; his fieldwork related to the present study was funded by the Flanders Research Foundation and the Boyekoli Ebale Congo 2010 expedition through the Belgian Federal Directorate General for Development Cooperation (DGDC) and the Belgian Science Policy (BELSPO). NR 70 TC 10 Z9 10 U1 5 U2 28 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 MAR 6 PY 2014 VL 14 AR 42 DI 10.1186/1471-2148-14-42 PG 12 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA AF1FI UT WOS:000334459400001 PM 24597925 ER PT J AU Stephenson, NL Das, AJ Condit, R Russo, SE Baker, PJ Beckman, NG Coomes, DA Lines, ER Morris, WK Ruger, N Alvarez, E Blundo, C Bunyavejchewin, S Chuyong, G Davies, SJ Duque, A Ewango, CN Flores, O Franklin, JF Grau, HR Hao, Z Harmon, ME Hubbell, SP Kenfack, D Lin, Y Makana, JR Malizia, A Malizia, LR Pabst, RJ Pongpattananurak, N Su, SH Sun, IF Tan, S Thomas, D van Mantgem, PJ Wang, X Wiser, SK Zavala, MA AF Stephenson, N. L. Das, A. J. Condit, R. Russo, S. E. Baker, P. J. Beckman, N. G. Coomes, D. A. Lines, E. R. Morris, W. K. Rueger, N. Alvarez, E. Blundo, C. Bunyavejchewin, S. Chuyong, G. Davies, S. J. Duque, A. Ewango, C. N. Flores, O. Franklin, J. F. Grau, H. R. Hao, Z. Harmon, M. E. Hubbell, S. P. Kenfack, D. Lin, Y. Makana, J. -R. Malizia, A. Malizia, L. R. Pabst, R. J. Pongpattananurak, N. Su, S. -H. Sun, I-F. Tan, S. Thomas, D. van Mantgem, P. J. Wang, X. Wiser, S. K. Zavala, M. A. TI Rate of tree carbon accumulation increases continuously with tree size SO NATURE LA English DT Article ID AGE-RELATED DECLINE; FOREST PRODUCTIVITY; GROWTH EFFICIENCY; OLD TREES; STAND; COMPETITION; PLANT; LIMITATION; ALLOCATION; ALLOMETRY AB Forests are major components of the global carbon cycle, providing substantial feedback to atmospheric greenhouse gas concentrations(1). Our ability to understand and predict changes in the forest carbon cycle-particularly net primary productivity and carbon storage-increasingly relies on models that represent biological processes across several scales of biological organization, from tree leaves to forest stands(2,3). Yet, despite advances in our understanding of productivity at the scales of leaves and stands, no consensus exists about the nature of productivity at the scale of the individual tree(4-7), in part because we lack a broad empirical assessment of whether rates of absolute tree mass growth (and thus carbon accumulation) decrease, remain constant, or increase as trees increase in size and age. Here we present a global analysis of 403 tropical and temperate tree species, showing that for most species mass growth rate increases continuously with tree size. Thus, large, old trees do not act simply as senescent carbon reservoirs but actively fix large amounts of carbon compared to smaller trees; at the extreme, a single big tree can add the same amount of carbon to the forest within a year as is contained in an entire mid-sized tree. The apparent paradoxes of individual tree growth increasing with tree size despite declining leaf-level(8-10) and stand-level(10) productivity can be explained, respectively, by increases in a tree's total leaf area that outpace declines in productivity per unit of leaf area and, among other factors, age-related reductions in population density. Our results resolve conflicting assumptions about the nature of tree growth, inform efforts to under-tand and model forest carbon dynamics, and have additional implications for theories of resource allocation(11) and plant senescence(12). C1 [Stephenson, N. L.; Das, A. J.] US Geol Survey, Western Ecol Res Ctr, Three Rivers, CA 93271 USA. [Condit, R.; Rueger, N.; Hubbell, S. P.] Smithsonian Trop Res Inst, Balboa, Panama. [Russo, S. E.; Beckman, N. G.] Univ Nebraska, Sch Biol Sci, Lincoln, NE 68588 USA. [Baker, P. J.] Univ Melbourne, Dept Forest & Ecosyst Sci, Melbourne, Vic 3121, Australia. [Coomes, D. A.] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England. [Lines, E. R.] UCL, Dept Geog, London WC1E 6BT, England. [Morris, W. K.] Univ Melbourne, Sch Bot, Melbourne, Vic 3010, Australia. [Rueger, N.] Univ Leipzig, spebot, D-04103 Leipzig, Germany. [Alvarez, E.] Jardin Bot Medellin, Medellin, Colombia. [Blundo, C.; Grau, H. R.; Malizia, A.] Univ Nacl Tucuman, Inst Ecol Reg, RA-4107 Yerba Buena, Tucuman, Argentina. [Bunyavejchewin, S.] Dept Natl Pk Wildlife & Plant Conservat, Res Off, Bangkok 10900, Thailand. [Chuyong, G.] Dept Bot & Plant Physiol, Buea, Southwest Provi, Cameroon. [Davies, S. J.; Kenfack, D.] Smithsonian Inst, Ctr Trop Forest Sci, Global Earth Observ, Washington, DC 20013 USA. [Duque, A.] Univ Nacl Colombia, Dept Ciencias Forestales, Medellin, Colombia. [Ewango, C. N.; Makana, J. -R.] Wildlife Conservat Soc, Kinshasa, Zaire. [Flores, O.] Univ Reunion, CIRAD, Unite Mixte Rech Peuplements Vegetaux & Bioagrees, F-97410 St Pierre, France. [Franklin, J. F.] Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA. [Hao, Z.; Wang, X.] Chinese Acad Sci, Inst Appl Ecol, State Key Lab Forest & Soil Ecol, Shenyang 110164, Peoples R China. [Harmon, M. E.; Pabst, R. J.] Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA. [Hubbell, S. P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Lin, Y.] Tunghai Univ, Dept Life Sci, Taichung 40704, Taiwan. [Malizia, A.] Univ Nacl Jujuy, Fac Ciencias Agr, RA-4600 San Salvador De Jujuy, Argentina. [Pongpattananurak, N.] Kasetsart Univ, Fac Forestry, Chatuchak Bangkok 10900, Thailand. [Su, S. -H.] Taiwan Forestry Res Inst, Taipei 10066, Taiwan. [Sun, I-F.] Natl Dong Hwa Univ, Dept Nat Resources & Environm Studies, Hualien 97401, Taiwan. [Tan, S.] Sarawak Forestry Dept, Kuching 93660, Sarawak, Malaysia. [Thomas, D.] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [van Mantgem, P. J.] US Geol Survey, Western Ecol Res Ctr, Arcata, CA 95521 USA. [Wiser, S. K.] Landcare Res, Lincoln 7640, New Zealand. [Zavala, M. A.] Univ Alcala de Henares, Dept Life Sci, Forest Ecol & Restorat Grp, Madrid 28805, Spain. RP Stephenson, NL (reprint author), US Geol Survey, Western Ecol Res Ctr, Three Rivers, CA 93271 USA. EM nstephenson@usgs.gov RI wang, xugao/B-1111-2015; Zavala, Miguel/H-3603-2015; Ruger, Nadja/J-6393-2015; Beckman, Noelle/E-5554-2011; iDiv, Deutsches Zentrum/B-5164-2016; wiser, susan/G-1975-2011; OI wang, xugao/0000-0003-1207-8852; Zavala, Miguel/0000-0003-1456-0132; Ruger, Nadja/0000-0003-2371-4172; Beckman, Noelle/0000-0001-5822-0610; wiser, susan/0000-0002-8938-8181; Baker, Patrick/0000-0002-6560-7124; Flores, Olivier/0000-0002-1416-0449 FU United States Geological Survey (USGS) John Wesley Powell Center for Analysis and Synthesis; USGS Ecosystems and Climate and Land Use Change mission areas; Smithsonian Institution Global Earth Observatory-Center for Tropical Forest Science (CTFS); University of Nebraska-Lincoln Program of Excellence in Population Biology Postdoctoral Fellowship; National Natural Science Foundation of China [31370444]; State Key Laboratory of Forest and Soil Ecology [LFSE2013-11]; USGS; CTFS; US National Science Foundation; Andrews LTER [NSF-LTER DEB-0823380]; US National Park Service; US Forest Service (USFS); USFS Forest Inventory and Analysis Program; John D. and Catherine T. MacArthur Foundation; Andrew W. Mellon Foundation; MAGRAMA; Council of Agriculture of Taiwan; National Science Council of Taiwan; National Natural Science Foundation of China; Knowledge Innovation Program of the Chinese Academy of Sciences; Landcare Research; National Vegetation Survey Database (NVS) of New Zealand; French Fund for the Global Environment; Fundacion ProYungas FX We thank the hundreds of people who have established and maintained the forest plots and their associated databases; M. G. Ryan for comments on the manuscript; C. D. Canham and T. Hart for supplying data; C. D. Canham for discussions and feedback; J. S. Baron for hosting our workshops; and Spain's Ministerio de Agricultura, Alimentacion y Medio Ambiente (MAGRAMA) for granting access to the Spanish Forest Inventory Data. Our analyses were supported by the United States Geological Survey (USGS) John Wesley Powell Center for Analysis and Synthesis, the USGS Ecosystems and Climate and Land Use Change mission areas, the Smithsonian Institution Global Earth Observatory-Center for Tropical Forest Science (CTFS), and a University of Nebraska-Lincoln Program of Excellence in Population Biology Postdoctoral Fellowship (to N.G.B.). In addition, X. W. was supported by National Natural Science Foundation of China (31370444) and State Key Laboratory of Forest and Soil Ecology (LFSE2013-11). Data collection was funded by a broad range of organizations including the USGS, the CTFS, the US National Science Foundation, the Andrews LTER (NSF-LTER DEB-0823380), the US National Park Service, the US Forest Service (USFS), the USFS Forest Inventory and Analysis Program, the John D. and Catherine T. MacArthur Foundation, the Andrew W. Mellon Foundation, MAGRAMA, the Council of Agriculture of Taiwan, the National Science Council of Taiwan, the National Natural Science Foundation of China, the Knowledge Innovation Program of the Chinese Academy of Sciences, Landcare Research and the National Vegetation Survey Database (NVS) of New Zealand, the French Fund for the Global Environment and Fundacion ProYungas. This paper is a contribution from the Western Mountain Initiative, a USGS global change research project. Any use of trade names is for descriptive purposes only and does not imply endorsement by the USA government. NR 50 TC 155 Z9 158 U1 41 U2 341 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAR 6 PY 2014 VL 507 IS 7490 BP 90 EP + DI 10.1038/nature12914 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC0ZQ UT WOS:000332224400048 PM 24429523 ER PT J AU Muster, C Meyer, M Sattler, T AF Muster, Christoph Meyer, Marc Sattler, Thomas TI Spatial Arrangement Overrules Environmental Factors to Structure Native and Non-Native Assemblages of Synanthropic Harvestmen SO PLOS ONE LA English DT Article ID ECOLOGICAL COMMUNITIES; BIOLOGICAL INVASIONS; NEIGHBOR MATRICES; HABITAT; URBANIZATION; FRAMEWORK; ALIEN; SCALE; BIODIVERSITY; DIVERSITY AB Understanding how space affects the occurrence of native and non-native species is essential for inferring processes that shape communities. However, studies considering spatial and environmental variables for the entire community - as well as for the native and non-native assemblages in a single study - are scarce for animals. Harvestmen communities in central Europe have undergone drastic turnovers during the past decades, with several newly immigrated species, and thus provide a unique system to study such questions. We studied the wall-dwelling harvestmen communities from 52 human settlements in Luxembourg and found the assemblages to be largely dominated by non-native species (64% of specimens). Community structure was analysed using Moran's eigenvector maps as spatial variables, and landcover variables at different radii (500 m, 1000 m, 2000 m) in combination with climatic parameters as environmental variables. A surprisingly high portion of pure spatial variation (15.7% of total variance) exceeded the environmental (10.6%) and shared (4%) components of variation, but we found only minor differences between native and non-native assemblages. This could result from the ecological flexibility of both, native and non-native harvestmen that are not restricted to urban habitats but also inhabit surrounding semi-natural landscapes. Nevertheless, urban landcover variables explained more variation in the non-native community, whereas coverage of semi-natural habitats (forests, rivers) at broader radii better explained the native assemblage. This indicates that some urban characteristics apparently facilitate the establishment of non-native species. We found no evidence for competitive replacement of native by invasive species, but a community with novel combination of native and non-native species. C1 [Muster, Christoph] Ernst Moritz Arndt Univ Greifswald, Museum & Inst Zool, Greifswald, Germany. [Meyer, Marc] Musee Natl Hist Nat Luxembourg, Luxembourg, Luxembourg. [Sattler, Thomas] Swiss Fed Inst Forest Snow & Landscape Res WSL, Bellinzona, Switzerland. [Sattler, Thomas] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Sattler, Thomas] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Muster, C (reprint author), Ernst Moritz Arndt Univ Greifswald, Museum & Inst Zool, Greifswald, Germany. EM christoph.muster@uni-greifswald.de FU Fonds National de la Recherche Luxembourg through an AMC2 - Mobility Mobility of researchers grant [FNR/09/AM2c/03]; Federal Office for the Environment Switzerland; Swiss National Science Foundation FX Field work of CM in Luxembourg was funded by the Fonds National de la Recherche Luxembourg through an AMC2 - Mobility Mobility of researchers grant (FNR/09/AM2c/03)(http://www.fnr.lu/). The salary of TS was funded by the Federal Office for the Environment Switzerland (http://www.bafu.admin.ch/index.html?lang = en) and the Swiss National Science Foundation (http://www.snf.ch/E/Pages/default.aspx). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 70 TC 3 Z9 5 U1 3 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 MAR 4 PY 2014 VL 9 IS 3 AR e90474 DI 10.1371/journal.pone.0090474 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC4FD UT WOS:000332475500055 PM 24595309 ER PT J AU Finkbeiner, SD AF Finkbeiner, Susan D. TI COMMUNAL ROOSTING IN HELICONIUS BUTTERFLIES (NYMPHALIDAE): ROOST RECRUITMENT, ESTABLISHMENT, FIDELITY, AND RESOURCE USE TRENDS BASED ON AGE AND SEX SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY LA English DT Article DE Aggregation; trapline; following behavior; butterfly memory; Heliconius erato ID LEPIDOPTERA NYMPHALIDAE; BEHAVIORAL THERMOREGULATION; NOCTURNAL AGGREGATIONS; COSTA-RICA; HOME-RANGE; BODY-SIZE; CONSEQUENCES; INFORMATION; EVOLUTION; PREDATION AB Heliconius passion-vine butterflies form communal roosts on a nightly basis as an anti-predatory defense. Although past studies have evaluated various components of this behavior, much remains unknown about many basic aspects of roost dynamics. To learn more about communal roosting I examined roost establishment, recruitment, roost-mate resource use, roosting participation in a population, and roost arrival, departure, and perch preferences in natural populations of Heliconius erato petiverana in Panama. My observations suggest that 1) younger butterflies are recruited more readily than older butterflies, 2) roosts are first established by a single butterfly roosting consecutively in the same location that later recruits butterflies, 3) males depart roosts earlier than females in the morning, 4) older butterflies tend to roost on the same perch in the same roost every night, 5) roost-mates share the same resource traplines, and 6) most butterflies in a population participate in roosts. These observations present an improved portrait of Heliconius roosting and raise several new questions about this behavior. C1 [Finkbeiner, Susan D.] Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. [Finkbeiner, Susan D.] Smithsonian Trop Res Inst, Panama City 084303092, Panama. RP Finkbeiner, SD (reprint author), Univ Calif Irvine, Dept Ecol & Evolutionary Biol, 321 Steinhaus Hall, Irvine, CA 92697 USA. EM sfinkbei@uci.edu FU Smithsonian Tropical Research Institute; U.S. Department of Education GAANN; National Science Foundation (NSF) [DGE-0808392] FX Many thanks to Robert Reed for project guidance and manuscript suggestions; Kailen Mooney, Nancy Burley, Owen McMillan, James Mallet, Larry Gilbert, and Santiago Meneses for advice and comments on project design; Jasmine Velez and Talia Gustafson for field assistance; Adriana Briscoe, Kyle McCulloch, Aide Macias Munoz, Arnaud Martin, Christian Salcedo, and an anonymous reviewer for manuscript feedback; The Smithsonian Tropical Research Institute (STRI) for use of field sites; La Autoridad Nacional del Ambiente (ANAM) for research permit approval; and my funding sources: Smithsonian Tropical Research Institute, the U.S. Department of Education GAANN; this material is based upon work supported by the National Science Foundation (NSF) Graduate Research Fellowship under Award No. DGE-0808392. NR 42 TC 1 Z9 1 U1 1 U2 16 PU LEPIDOPTERISTS SOC PI LOS ANGELES PA 900 EXPOSITION BLVD, LOS ANGELES, CA 90007-4057 USA SN 0024-0966 J9 J LEPID SOC JI J. Lepid. Soc. PD MAR 3 PY 2014 VL 68 IS 1 BP 10 EP 16 PG 7 WC Entomology SC Entomology GA AC8WR UT WOS:000332816300002 ER PT J AU Thessen, AE Parr, CS AF Thessen, Anne E. Parr, Cynthia Sims TI Knowledge Extraction and Semantic Annotation of Text from the Encyclopedia of Life SO PLOS ONE LA English DT Article ID BIOLOGY; ECOINFORMATICS; ONTOLOGY AB Numerous digitization and ontological initiatives have focused on translating biological knowledge from narrative text to machine-readable formats. In this paper, we describe two workflows for knowledge extraction and semantic annotation of text data objects featured in an online biodiversity aggregator, the Encyclopedia of Life. One workflow tags text with DBpedia URIs based on keywords. Another workflow finds taxon names in text using GNRD for the purpose of building a species association network. Both workflows work well: the annotation workflow has an F1 Score of 0.941 and the association algorithm has an F1 Score of 0.885. Existing text annotators such as Terminizer and DBpedia Spotlight performed well, but require some optimization to be useful in the ecology and evolution domain. Important future work includes scaling up and improving accuracy through the use of distributional semantics. C1 [Thessen, Anne E.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85283 USA. [Parr, Cynthia Sims] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Thessen, AE (reprint author), Arizona State Univ, Sch Life Sci, Tempe, AZ 85283 USA. EM annethessen@gmail.com OI Thessen, Anne/0000-0002-2908-3327 FU Encyclopedia of Life; John D. and Catherine T. MacArthur Foundation; Alfred P. Sloan Foundation FX Funding for CSP and AET came from the Encyclopedia of Life. Funding for the Encyclopedia of Life comes from the John D. and Catherine T. MacArthur Foundation, the Alfred P. Sloan Foundation, the participating institutions in the Encyclopedia of Life consortium, and individual donations from users around the world. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 43 TC 6 Z9 7 U1 0 U2 17 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAR 3 PY 2014 VL 9 IS 3 AR e89550 DI 10.1371/journal.pone.0089550 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC4CT UT WOS:000332468900023 PM 24594988 ER PT J AU van Tussenbroek, BI Cortes, J Collin, R Fonseca, AC Gayle, PMH Guzman, HM Jacome, GE Juman, R Koltes, KH Oxenford, HA Rodriguez-Ramirez, A Samper-Villarreal, J Smith, SR Tschirky, JJ Weil, E AF van Tussenbroek, Brigitta I. Cortes, Jorge Collin, Rachel Fonseca, Ana C. Gayle, Peter M. H. Guzman, Hector M. Jacome, Gabriel E. Juman, Rahanna Koltes, Karen H. Oxenford, Hazel A. Rodriguez-Ramirez, Alberto Samper-Villarreal, Jimena Smith, Struan R. Tschirky, John J. Weil, Ernesto TI Caribbean-Wide, Long-Term Study of Seagrass Beds Reveals Local Variations, Shifts in Community Structure and Occasional Collapse SO PLOS ONE LA English DT Article ID COSTA-RICA CARICOMP; CORAL-REEF; WATER-QUALITY; THALASSIA-TESTUDINUM; CARBONATE PRODUCTION; SEDIMENT NUTRIENTS; FLORIDA-KEYS; GULF-COAST; HABITATS; PATTERNS AB The CARICOMP monitoring network gathered standardized data from 52 seagrass sampling stations at 22 sites (mostly Thalassia testudinum-dominated beds in reef systems) across the Wider Caribbean twice a year over the period 1993 to 2007 (and in some cases up to 2012). Wide variations in community total biomass (285 to >2000 g dry m(-2)) and annual foliar productivity of the dominant seagrass T. testudinum (<200 and >2000 g dry m(-2)) were found among sites. Solar-cycle related intra-annual variations in T. testudinum leaf productivity were detected at latitudes > 16 degrees N. Hurricanes had little to no long-term effects on these well-developed seagrass communities, except for 1 station, where the vegetation was lost by burial below similar to 1 m sand. At two sites (5 stations), the seagrass beds collapsed due to excessive grazing by turtles or sea-urchins (the latter in combination with human impact and storms). The low-cost methods of this regional-scale monitoring program were sufficient to detect long-term shifts in the communities, and fifteen (43%) out of 35 long-term monitoring stations (at 17 sites) showed trends in seagrass communities consistent with expected changes under environmental deterioration. C1 [van Tussenbroek, Brigitta I.] Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Cancun, Mexico. [Cortes, Jorge; Fonseca, Ana C.; Samper-Villarreal, Jimena] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, San Pedro, Costa Rica. [Collin, Rachel; Guzman, Hector M.; Jacome, Gabriel E.] Smithsonian Trop Res Inst, Panama City, Panama. [Gayle, Peter M. H.] Discovery Bay Marine Lab, Discovery Bay, Hong Kong, Jamaica. [Juman, Rahanna] Inst Marine Affairs, Trinidad, Trinid & Tobago. [Koltes, Karen H.] Off Insular Affairs, Dept Interior, Washington, DC USA. [Oxenford, Hazel A.] Univ W Indies, CERMES, Wanstead, Barbados. [Rodriguez-Ramirez, Alberto] Inst Invest Marinas & Costeras INVEMAR, Santa Marta, Colombia. [Smith, Struan R.] Bermuda Biol Stn Res, St George, Bermuda. [Weil, Ernesto] Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00709 USA. RP van Tussenbroek, BI (reprint author), Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Cancun, Mexico. EM vantuss@cmarl.unam.mx FU John D. and Catherine T. MacArthur Foundation; UNESCO Environment and Development in Coastal Regions and in Small Islands (CSI); US National Science Foundation-Division of International Programs and Division of Ocean Sciences; CARICOMP data Management Centre; Centre for Marine Sciences; University of West Indies, Jamaica FX CARICOMP received support from the John D. and Catherine T. MacArthur Foundation, UNESCO Environment and Development in Coastal Regions and in Small Islands (CSI), US National Science Foundation-Division of International Programs and Division of Ocean Sciences, CARICOMP data Management Centre, Centre for Marine Sciences, University of West Indies, Jamaica, and the directors and administrators of the participating institutions. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 58 TC 5 Z9 5 U1 8 U2 65 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAR 3 PY 2014 VL 9 IS 3 AR e90600 DI 10.1371/journal.pone.0090600 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC4CT UT WOS:000332468900123 PM 24594732 ER PT J AU Walls, RL Deck, J Guralnick, R Baskauf, S Beaman, R Blum, S Bowers, S Buttigieg, PL Davies, N Endresen, D Gandolfo, MA Hanner, R Janning, A Krishtalka, L Matsunaga, A Midford, P Morrison, N Tuama, EO Schildhauer, M Smith, B Stucky, BJ Thomer, A Wieczorek, J Whitacre, J Wooley, J AF Walls, Ramona L. Deck, John Guralnick, Robert Baskauf, Steve Beaman, Reed Blum, Stanley Bowers, Shawn Buttigieg, Pier Luigi Davies, Neil Endresen, Dag Gandolfo, Maria Alejandra Hanner, Robert Janning, Alyssa Krishtalka, Leonard Matsunaga, Andrea Midford, Peter Morrison, Norman Tuama, Eamonn O. Schildhauer, Mark Smith, Barry Stucky, Brian J. Thomer, Andrea Wieczorek, John Whitacre, Jamie Wooley, John TI Semantics in Support of Biodiversity Knowledge Discovery: An Introduction to the Biological Collections Ontology and Related Ontologies SO PLOS ONE LA English DT Article ID INTEGRATION; INFORMATICS; ANNOTATION; LANGUAGE; RCN4GSC; ACCESS; LIFE AB The study of biodiversity spans many disciplines and includes data pertaining to species distributions and abundances, genetic sequences, traitmeasurements, and ecological niches, complemented by information on collection and measurement protocols. A review of the current landscape of metadata standards and ontologies in biodiversity science suggests that existing standards such as the Darwin Core terminology are inadequate for describing biodiversity data in a semantically meaningful and computationally useful way. Existing ontologies, such as the Gene Ontology and others in the Open Biological and Biomedical Ontologies (OBO) Foundry library, provide a semantic structure but lack many of the necessary terms to describe biodiversity data in all its dimensions. In this paper, we describe the motivation for and ongoing development of a new Biological Collections Ontology, the Environment Ontology, and the Population and Community Ontology. These ontologies share the aim of improving data aggregation and integration across the biodiversity domain and can be used to describe physical samples and sampling processes (for example, collection, extraction, and preservation techniques), as well as biodiversity observations that involve no physical sampling. Together they encompass studies of: 1) individual organisms, including voucher specimens from ecological studies and museum specimens, 2) bulk or environmental samples (e.g., gut contents, soil, water) that include DNA, other molecules, and potentially many organisms, especially microbes, and 3) survey-based ecological observations. We discuss how these ontologies can be applied to biodiversity use cases that span genetic, organismal, and ecosystem levels of organization. We argue that if adopted as a standard and rigorously applied and enriched by the biodiversity community, these ontologies would significantly reduce barriers to data discovery, integration, and exchange among biodiversity resources and researchers. C1 [Walls, Ramona L.] Univ Arizona, iPlant Collaborat, Tucson, AZ 85721 USA. [Deck, John] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Guralnick, Robert; Stucky, Brian J.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. [Guralnick, Robert] Univ Colorado, CU Museum Nat Hist, Boulder, CO 80309 USA. [Baskauf, Steve] Vanderbilt Univ, Dept Biol Sci, Nashville, TN 37235 USA. [Beaman, Reed] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Blum, Stanley] Calif Acad Sci, San Francisco, CA 94118 USA. [Bowers, Shawn] Gonzaga Univ, Spokane, WA 99258 USA. [Buttigieg, Pier Luigi] Helmholtz Ctr Polar & Marine Res, Alfred Wegener Inst, Bremerhaven, Germany. [Davies, Neil] Univ Calif Berkeley, Gump South Pacific Res Stn, Moorea, Fr Polynesia. [Endresen, Dag] Univ Oslo, Nat Hist Museum, GBIF Norway, Oslo, Norway. [Gandolfo, Maria Alejandra] Cornell Univ, Dept Plant Biol, LH Bailey Hortorium, Ithaca, NY USA. [Hanner, Robert] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. [Janning, Alyssa] Univ Arizona, Sch Informat Resources & Lib Sci, Tucson, AZ USA. [Krishtalka, Leonard] Univ Kansas, Biodivers Inst & Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. [Matsunaga, Andrea] Univ Florida, Gainesville, FL USA. [Midford, Peter] Univ Kansas, Lawrence, KS 66045 USA. [Morrison, Norman] Univ Manchester, Sch Comp Sci, BioVeL Project, Manchester, Lancs, England. [Tuama, Eamonn O.] GBIF Secretariat, Copenhagen, Denmark. [Schildhauer, Mark] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA USA. [Smith, Barry] SUNY Buffalo, Dept Philosophy, Buffalo, NY 14260 USA. [Thomer, Andrea] Univ Illinois, Grad Sch Lib & Informat Sci, Urbana, IL USA. [Wieczorek, John] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. [Whitacre, Jamie] Smithsonian Inst, Informat Branch, Informat Technol Off, Natl Museum Nat Hist, Washington, DC 20560 USA. [Wooley, John] Univ Calif San Diego, La Jolla, CA 92093 USA. RP Walls, RL (reprint author), Univ Arizona, iPlant Collaborat, Tucson, AZ 85721 USA. EM rwalls@iplantcollaborative.org RI Davies, Neil/E-5863-2012; Endresen, Dag/G-1284-2010; OI Davies, Neil/0000-0001-8085-5014; Baskauf, Steve/0000-0003-4365-3135; Endresen, Dag/0000-0002-2352-5497; Thomer, Andrea/0000-0001-6238-3498; Matsunaga, Andrea/0000-0001-9036-5895; Smith, Barry/0000-0003-1384-116X; Midford, Peter/0000-0001-6512-3296; Schildhauer, Mark/0000-0003-0632-7576; Buttigieg, Pier Luigi/0000-0002-4366-3088 FU US National Science Foundation (NSF) [DBI-0840989, IIS-1255035, DBI: 0956371, 0956350, 0956426, DBI-0851313]; National Institutes of Health (NIH) [U54 HG004028]; European Commission [287589, 283359]; [DBI-0735191] FX We gratefully acknowledge the support from the US National Science Foundation (NSF - http://www.nsf.gov/) through the following grants: Research Coordination Network for Genomic Standards Consortium (DBI-0840989), EAGER: An Interoperable Information Infrastructure for Biodiversity Research (IIS-1255035), Collaborative Research: BiSciCol Tracker: Towards a tagging and tracking infrastructure for biodiversity science collections (DBI: 0956371, 0956350, 0956426), Collaborative Research: Data Integration for Repository Services in Biodiversity Informatics (DBI-0851313), and the National Institutes of Health (NIH - http://www.nih.gov/) through a grant to the National Center for Biomedical Ontology (U54 HG004028). RW is supported by DBI-0735191 (The iPlant Collaborative). PLB is supported by the European Commission under Grant Agreement no 287589 (MicroB3). NM is supported by the European Commission 7th Framework Programme (FP7) as part of its e-Infrastructures activity (Grant no. 283359, BioVeL). Any opinions, findings, conclusions, or recommendations expressed in this report are those of the participants and do not necessarily represent the official views, opinions, or policy of the National Science Foundation. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 66 TC 24 Z9 25 U1 6 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 MAR 3 PY 2014 VL 9 IS 3 AR e89606 DI 10.1371/journal.pone.0089606 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC4CT UT WOS:000332468900024 PM 24595056 ER PT J AU Cialdella, JS AF Cialdella, Joseph Stanhope TI A Landscape of Ruin and Repair: Parks, Potatoes, and Detroit's Environmental Past, 1879-1900 SO MICHIGAN HISTORICAL REVIEW LA English DT Article C1 [Cialdella, Joseph Stanhope] Univ Michigan, Dept Amer Culture, Ann Arbor, MI 48109 USA. [Cialdella, Joseph Stanhope] Smithsonian Inst Arch Amer Gardens, Washington, DC USA. RP Cialdella, JS (reprint author), Univ Michigan, Dept Amer Culture, Ann Arbor, MI 48109 USA. NR 45 TC 0 Z9 0 U1 1 U2 1 PU CENTRAL MICHIGAN UNIV CLARKE HISTORICAL LIBRARY PI MT PLEASANT PA MT PLEASANT, MI 48859 USA SN 0360-1846 J9 MICH HIST REV JI Mich. Hist. Rev. PD SPR PY 2014 VL 40 IS 1 BP 49 EP 72 PG 24 WC History SC History GA CA0RR UT WOS:000348624800004 ER PT J AU Labandeira, CC Prevec, R AF Labandeira, Conrad C. Prevec, Rose TI Plant paleopathology and the roles of pathogens and insects SO INTERNATIONAL JOURNAL OF PALEOPATHOLOGY LA English DT Article DE Bacteria; Fossil record; Fungi; Insects; Nematodes; Paleopathology; Pathogens; Plant-insect interactions; Plants; Vectors; Viruses ID DUTCH ELM DISEASE; DEVONIAN RHYNIE CHERT; YELLOW DWARF VIRUS; RED-RING DISEASE; LAND PLANTS; HYPERSENSITIVE RESPONSE; ARBUSCULAR MYCORRHIZAE; ARMILLARIA-OSTOYAE; FUNGAL PATHOGENS; PALEOZOIC FUNGI AB Plant pathologies are the consequence of physical and chemical responses by plants to invasive microorganisms or to imbalances in nutritional or environmental conditions. Many factors determine the potential for plant disease infection and disease, but the primary components are the terrestrial host plant, the pathogen, the environment, and occasionally a biological vector. Pathogens typically are one of four major causative groups: viruses, bacteria, fungi, and nematodes. The vector often is a passive abiotic agent such as wind, water or soil, but it also may be an insect that actively facilitates transmission of the pathogen to a plant. Pathogenic invasion of plants may require sophisticated structures for penetration of host tissues and can elicit a range of host responses such as production of defensive compounds, callus tissue, galls and necroses to seal wounded or infected areas. Fossil diseases primarily are diagnosed from surface leaf structures internal tissues, categorized into damage types (DTs), important for tracking the evolution of herbivore and pathogen attack and host-plant response in time, space and habitat. The fossil record is a useful, underappreciated, but accessible archive of plant damage. We present an overview of pathogens and life cycles that involve insects in the production of these disease symptoms in fossil plants. Published by Elsevier Inc. C1 [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Labandeira, Conrad C.; Prevec, Rose] 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 NSF [DEB-0919071] FX We thank Jane Buikstra for inviting us to submit this contribution, and providing us the opportunity to allow our research on fossil plant-insect interactions become better known among the broader community of paleopathologists. Finnegan Marsh adroitly formatted the figures. We thank two anonymous reviewers for providing thoughtful reviews of the manuscript, and Torsten Wappler for bringing to our attention an error in a figure caption. We acknowledge NSF grant DEB-0919071 to Peter Wilf. This is contribution 255 of the Evolution of Terrestrial Ecosystems at the National Museum of Natural History, in Washington, DC. NR 177 TC 9 Z9 9 U1 9 U2 38 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1879-9817 EI 1879-9825 J9 INT J PALEOPATHOL JI Int. J. Paleopathol. PD MAR PY 2014 VL 4 BP 1 EP 16 DI 10.1016/j.ijpp.2013.10.002 PG 16 WC Paleontology; Pathology SC Paleontology; Pathology GA AT2PN UT WOS:000344776800001 ER PT J AU Klaus, HD Ortner, DJ AF Klaus, Haagen D. Ortner, Donald J. TI Treponemal infection in Peru's Early Colonial period: A case of complex lesion patterning and unusual funerary treatment SO INTERNATIONAL JOURNAL OF PALEOPATHOLOGY LA English DT Article DE Treponematosis; Differential diagnosis; Mortuary archaeology; Andes ID CONGENITAL-SYPHILIS; SOCIAL IMPLICATIONS; NORTH COAST; SKELETAL; DISEASE; PALEOPATHOLOGY; ANTIQUITY; AMERICA; MORROPE; ORIGIN AB This study describes a series of skeletal lesions observed in a mid 16th century individual of an old adult female from the Early Colonial Period of northern coastal Peru. This fragmented skeleton revealed evidence of complex, active, and systemic chronic infection that included multiple pathological foci on the cranial vault, extensive pathological new bone formation in both arms, the sternum, ribs, left scapula, clavicles, femora, and fibulae, which was paralleled by extensive endosteal obliteration of affected long bone medullary cavities. Differential diagnosis included hematogenous osteomyelitis, Paget's disease, fluorosis, melorheostosis, endosteal hyperostosis, and hypertrophic osteoarthropathy. Simultaneous periosteal and endosteal bone deposition of the clavicles, in addition to patterns of florid bone deposition on long bones and superficial cavitation, point most directly to treponemal disease. Co-morbidity with a non-specified respiratory disease and well-healed fractures of the tibiae are also considered. We also relate this person's illness to the highly informal disposal of their body to underscore how social perceptions of disease may have shaped this unusual and informal funerary ritual. Ultimately, this research cautions against overly "tibia-centric" thinking regarding treponemal syndromes, raises questions regarding the history and nature of treponemal disease in Peru, and highlights cross-disciplinary connections between paleopathology and mortuary archaeology. (C) 2013 Elsevier Inc. All rights reserved. C1 [Klaus, Haagen D.] George Mason Univ, Dept Sociol & Anthropol, Fairfax, VA 22030 USA. [Ortner, Donald J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. RP Klaus, HD (reprint author), George Mason Univ, Robinson Hall B,Room 305,MSN 3G5, Fairfax, VA 22030 USA. EM hklaus@gmu.edu FU Wenner-Gren Foundation [7302] FX This research was possible thanks to the generous funding of the Wenner-Gren Foundation (Gr. 7302). An earlier version of this work was presented at the 39th Annual Meeting of the Paleopathology Association in Portland, Oregon (April, 2012). Manuel Tam co-directed the 2005 excavations in Marrope. We owe debts of gratitude to Rosabella Alvarez-Calderon and family, Victor Curay, Carlos Elera, Marco Fernandez, Gabriella Jakubowska, Juan Martinez, Emily Middleton, Raul Saavedra, and Carlos Wester for their many and varied contributions in supporting the field and lab work. We also thank John Verano for a series of conversations on Andean treponematosis and sharing his El Brujo case with us. The editor-in-chief, associate editor, Clark Larsen, Molly Zuckerman, and the anonymous reviewers provided knowledgeable commentaries and thoughtful corrections. NR 84 TC 2 Z9 2 U1 17 U2 26 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1879-9817 EI 1879-9825 J9 INT J PALEOPATHOL JI Int. J. Paleopathol. PD MAR PY 2014 VL 4 BP 25 EP 36 DI 10.1016/j.ijpp.2013.12.001 PG 12 WC Paleontology; Pathology SC Paleontology; Pathology GA AT2PN UT WOS:000344776800003 ER PT J AU Harvey, EJ AF Harvey, Eleanor Jones TI WHISTLER A Life for Art's Sake SO AMERICAN SCHOLAR LA English DT Book Review C1 [Harvey, Eleanor Jones] Smithsonian Amer Art Museum, Washington, DC 20004 USA. RP Harvey, EJ (reprint author), Smithsonian Amer Art Museum, Washington, DC 20004 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU PHI BETA KAPPA SOC PI WASHINGTON PA 1785 MASSACHUSETTS AVENUE, N W FOURTH FL,, WASHINGTON, DC 20036 USA SN 0003-0937 EI 2162-2892 J9 AM SCHOLAR JI Am. Sch. PD SPR PY 2014 VL 83 IS 2 BP 116 EP 117 PG 2 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA AS3ZR UT WOS:000344214000042 ER PT J AU Belanus, BJ AF Belanus, Betty J. TI Tradition in the 21st Century: Locating the Role of the Past in the Present SO WESTERN FOLKLORE LA English DT Book Review C1 [Belanus, Betty J.] Smithsonian Inst, Washington, DC 20560 USA. RP Belanus, BJ (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CALIFORNIA FOLKLORE SOC PI POMONA PA WESTERN FOLKLORE DEPT OF ENGL/FOREIGN LANGUAGES 3801 W.TEMPLE AVENUE, POMONA, CA 91768-4010 USA SN 0043-373X J9 WESTERN FOLKLORE JI West. Folk. PD SPR PY 2014 VL 73 IS 2-3 BP 378 EP 380 PG 3 WC Folklore SC Arts & Humanities - Other Topics GA AS5JW UT WOS:000344308300020 ER PT J AU Collins, M AF Collins, Martin TI Untitled SO HISTORY AND TECHNOLOGY LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Collins, M (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 2 TC 1 Z9 1 U1 0 U2 0 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0734-1512 EI 1477-2620 J9 HIST TECHNOL JI Hist. Technol. PD MAR-JUN PY 2014 VL 30 IS 1-2 BP 1 EP 2 DI 10.1080/07341512.2014.941138 PG 2 WC History SC History GA AO9AY UT WOS:000341649100001 ER PT J AU Bishop, RL AF Bishop, Ronald L. TI INSTRUMENTAL APPROACHES TO UNDERSTANDING MESOAMERICAN ECONOMY: ELUSIVE PROMISES SO ANCIENT MESOAMERICA LA English DT Article ID NEUTRON-ACTIVATION ANALYSIS; PLASMA-MASS SPECTROMETRY; EARLY FORMATIVE POTTERY; OBSIDIAN ARTIFACTS; CERAMIC PRODUCTION; CLASSIC MAYA; CHEMICAL CHARACTERIZATION; PETROGRAPHIC ANALYSIS; POLITICAL ECONOMIES; TEOTIHUACAN VALLEY AB More than four decades ago, instrumental developments, such as those involving neutron activation and X-ray florescence, began to generate relatively large quantities of data from the analysis of archaeological materials. These data served as the basis for many models of long-distance exchange as a means of explaining the development of cultural complexity. I review aspects of this early history and the how use of compositional data is now more directed toward localized investigations of economic activity. Even with this refocus of research interest, studies involving material characterization appear to be declining. Using traditional citation, personal experience, and highly selective examples, I discuss the use of analytical techniques for studies of long-distance trade, as it developed and now confronts interpretive difficulties that are inherent in the data and rendered more so by use of abstract constructs and resource limitations. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. RP Bishop, RL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, MRC 112 POB 37012, Washington, DC 20013 USA. EM BishopR@si.edu NR 201 TC 1 Z9 1 U1 1 U2 7 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0956-5361 EI 1469-1787 J9 ANCIENT MESOAM JI Anc. Mesoam. PD SPR PY 2014 VL 25 IS 1 BP 251 EP 269 DI 10.1017/S0956536114000157 PG 19 WC Archaeology SC Archaeology GA AN6MO UT WOS:000340708800015 ER PT J AU Clyde, WC Wilf, P Iglesias, A Slingerland, RL Barnum, T Bijl, PK Bralower, TJ Brinkhuis, H Comer, EE Huber, BT Ibanez-Mejia, M Jicha, BR Krause, JM Schueth, JD Singer, BS Raigemborn, MS Schmitz, MD Sluijs, A Zamaloa, MD AF Clyde, William C. Wilf, Peter Iglesias, Ari Slingerland, Rudy L. Barnum, Timothy Bijl, Peter K. Bralower, Timothy J. Brinkhuis, Henk Comer, Emily E. Huber, Brian T. Ibanez-Mejia, Mauricio Jicha, Brian R. Krause, J. Marcelo Schueth, Jonathan D. Singer, Bradley S. Raigemborn, Maria Sol Schmitz, Mark D. Sluijs, Appy Zamaloa, Maria del Carmen TI New age constraints for the Salamanca Formation and lower Rio Chico Group in the western San Jorge Basin, Patagonia, Argentina: Implications for Cretaceous-Paleogene extinction recovery and land mammal age correlations SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Article ID BAJO BARREAL FORMATION; EOCENE THERMAL MAXIMUM; EARLY PALEOCENE; SOUTH-AMERICA; AR-40/AR-39 GEOCHRONOLOGY; MASS-EXTINCTION; NEW-JERSEY; BOUNDARY; CLIMATE; CHUBUT AB The Salamanca Formation of the San Jorge Basin (Patagonia, Argentina) preserves critical records of Southern Hemisphere Paleocene biotas, but its age remains poorly resolved, with estimates ranging from Late Cretaceous to middle Paleocene. We report a multi-disciplinary geochronologic study of the Salamanca Formation and overlying Rio Chico Group in the western part of the basin. New constraints include (1) an Ar-40/Ar-39 age determination of 67.31 +/- 0.55 Ma from a basalt flow underlying the Salamanca Formation, (2) micropaleontological results indicating an early Danian age for the base of the Salamanca Formation, (3) laser ablation HR-MC-ICP-MS (high resolution-multi collector-inductively coupled plasmamass spectrometry) U-Pb ages and a high-resolution TIMS (thermal ionization mass spectrometry) age of 61.984 +/- 0.041(0.074) [0.100] Ma for zircons from volcanic ash beds in the Penas Coloradas Formation (Rio Chico Group), and (4) paleomagnetic results indicating that the Salamanca Formation in this area is entirely of normal polarity, with reversals occurring in the Rio Chico Group. Placing these new age constraints in the context of a sequence stratigraphic model for the basin, we correlate the Salamanca Formation in the study area to Chrons C29n and C28n, with the Banco Negro Inferior (BNI), a mature widespread fossiliferous paleosol unit at the top of the Salamanca Formation, corresponding to the top of Chron C28n. The diverse paleobotanical assemblages from this area are here assigned to C28n (64.67-63.49 Ma), similar to 2-3 million years older than previously thought, adding to growing evidence for rapid Southern Hemisphere floral recovery after the Cretaceous-Paleogene extinction. Important Peligran and "Carodnia" zone vertebrate fossil assemblages from coastal BNI and Penas Coloradas exposures are likely older than previously thought and correlate to the early Torrejonian and early Tiffanian North American Land Mammal Ages, respectively. C1 [Clyde, William C.; Barnum, Timothy] Univ New Hampshire, Dept Earth Sci, Durham, NH 03824 USA. [Wilf, Peter; Slingerland, Rudy L.; Bralower, Timothy J.; Comer, Emily E.; Schueth, Jonathan D.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Iglesias, Ari] Univ Nacl Comahue, Div Paleontol, Inst Invest Biodiversidad & Ambiente INIBIOMA CON, RA-8400 San Carlos De Bariloche, Rio Negro, Argentina. [Bijl, Peter K.; Brinkhuis, Henk] Univ Utrecht, Palaeobot & Palynol Lab, Fac Geosci, Dept Earth Sci, NL-3584 CD Utrecht, Netherlands. [Huber, Brian T.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Ibanez-Mejia, Mauricio] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Jicha, Brian R.; Singer, Bradley S.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Krause, J. Marcelo] Museo Paleontol Egidio Feruglio CONICET UNPSJB, RA-9100 Trelew, Argentina. [Raigemborn, Maria Sol] Univ Nacl La Plata, Fac Ciencias Nat & Museo, Ctr Invest Geol CONICET UNLP, RA-1900 La Plata, Argentina. [Schmitz, Mark D.] Boise State Univ, Dept Geosci, Boise, ID 83725 USA. [Zamaloa, Maria del Carmen] Univ Buenos Aires, Dept Ecol Genet & Evoluc, RA-1053 Buenos Aires, DF, Argentina. RP Clyde, WC (reprint author), Univ New Hampshire, Dept Earth Sci, 56 Coll Rd, Durham, NH 03824 USA. EM will.clyde@unh.edu RI Singer, Bradley/F-4991-2012; Schmitz, Mark/A-2540-2012; Sluijs, Appy/B-3726-2009; Clyde, William/C-9595-2017; OI Singer, Bradley/0000-0003-3595-5168; Sluijs, Appy/0000-0003-2382-0215; Clyde, William/0000-0001-8814-3409; Ibanez-Mejia, Mauricio/0000-0002-7839-2425 FU National Science Foundation (NSF) [DEB-0919071]; European Research Council under the European Community [259627]; Netherlands Organization for Scientific Research (NWO) [86610110]; NSF [EAR-0443387, EAR-0732436] FX Thanks to N.R. Cuneo, K. Johnson, and P. Puerta for discussion and help with field logistics; N.L.D Welters, J.v. Tongeren, C. Jaramillo, and Paleoflora Ltd. for palynological slide preparation; P. Balcells for the preparation of the pollen and spores figure; J.P. Perez Panera for discussion of nannofosils; Secretaria de Cultura and Secretaria de Turismo y Areas Protegidas from Chubut Province and Sarmiento City for land permits; and H. Visser, C. Salazar-Bochatey, Martinez families, and A. Balercia for land access. This research was funded by National Science Foundation (NSF) grant DEB-0919071 to P.W., A.I., and R.L.S., and by the European Research Council under the European Community's Seventh Framework Program through Starting Grant 259627 to A.S. P.K.B. thanks the LPP foundation and H.B. the Netherlands Organization for Scientific Research (NWO grant 86610110). The Arizona Laserchron center is supported by NSF grants EAR-0443387 and EAR-0732436. NR 124 TC 20 Z9 23 U1 1 U2 9 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0016-7606 EI 1943-2674 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD MAR-APR PY 2014 VL 126 IS 3-4 BP 289 EP 306 DI 10.1130/B30915.1 PG 18 WC Geosciences, Multidisciplinary SC Geology GA AO2YC UT WOS:000341192900003 ER PT J AU Hong, T AF Hong, Terry TI I'll Be Right There. SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20004 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20004 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 MAR 1 PY 2014 VL 139 IS 4 BP 85 EP 85 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA AC4LT UT WOS:000332493500123 ER PT J AU Prado, A Sierra, A Windsor, D Bede, JC AF Prado, Alberto Sierra, Adriel Windsor, Donald Bede, Jacqueline C. TI LEAF TRAITS AND HERBIVORY LEVELS IN A TROPICAL GYMNOSPERM, ZAMIA STEVENSONII (ZAMIACEAE) SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Aulacoscelis; azoxyglycosides; delayed greening; Eumaeus; leaf toughness; specialist insects; trichomes; Zamia; Zamiaceae ID PERFORMANCE LIQUID-CHROMATOGRAPHY; NATURALLY OCCURRING CARCINOGEN; EUMAEUS-ATALA-FLORIDA; RAIN-FOREST CYCAD; ANTIHERBIVORE DEFENSE; SPECIALIST HERBIVORE; CHEMICAL DEFENSE; METHYLAZOXYMETHANOL; LEAVES; CHRYSOMELIDAE AB Premise of the study: Slow-growing understory cycads invest heavily in defenses to protect the few leaves they produce annually. The Neotropical cycad Zamia stevensonii has chemical and mechanical barriers against insect herbivores. Mechanical barriers, such as leaf toughness, can be established only after the leaf has expanded. Therefore, chemical defenses may be important during leaf expansion. How changes in leaf traits affect the feeding activity of cycad specialist insects is unknown. We investigated leaf defenses and incidence of specialist herbivores on Z. stevensonii during the first year after leaf flush. Methods: Herbivore incidence, leaf production, and leaf traits that might affect herbivory-including leaf age, lamina thickness, resistance-to-fracture, work-to-fracture, trichome density, and chlorophyll, water, and toxic azoxyglycoside (AZG) content-were measured throughout leaf development. Principal component analysis and generalized linear models identified characteristics that may explain herbivore incidence. Key results: Synchronized leaf development in Z. stevensonii is characterized by quick leaf expansion and delayed greening. Specialist herbivores feed on leaves between 10 and 100 d after flush and damage similar to 37% of all leaflets produced. Young leaves are protected by AZGs, but these defenses rapidly decrease as leaves expand. Leaves older than 100 d are protected by toughness. Conclusions: Because AZG concentrations drop before leaves become sufficiently tough, there is a vulnerable period during which leaves are susceptible to herbivory by specialist insects. This slow-growing gymnosperm invests heavily in constitutive defenses against highly specialized herbivores, underlining the convergence in defensive syndromes by major plant lineages. C1 [Prado, Alberto; Bede, Jacqueline C.] McGill Univ, Dept Plant Sci, Ste Anne De Bellevue, PQ, Canada. [Prado, Alberto; Sierra, Adriel; Windsor, Donald] Smithsonian Trop Res Inst, Panama City, Panama. RP Prado, A (reprint author), McGill Univ, Dept Plant Sci, 21,111 Lakeshore Rd, Ste Anne De Bellevue, PQ, Canada. EM alberto.prado@mail.mcgill.ca FU CONACYT; STRI; FQRNT; NSERC FX The authors thank A. S. Taylor, the C. Buddle Laboratory, M. Lechowicz, E. Leigh, and three anonymous reviewers for their advice and comments on the manuscript; and C. Correa, R. Royaute, and E. Pederson for assistance with data modeling and analysis. The project was funded by scholarships and grants through CONACYT (A.P.), STRI (D.W.), FQRNT (A.P.), and NSERC (J.C.B.). NR 58 TC 2 Z9 3 U1 8 U2 32 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 MAR PY 2014 VL 101 IS 3 BP 437 EP 447 DI 10.3732/ajb.1300337 PG 11 WC Plant Sciences SC Plant Sciences GA AN2YO UT WOS:000340452200005 PM 24638164 ER PT J AU Strang, CB AF Strang, Cameron B. TI Violence, Ethnicity, and Human Remains during the Second Seminole War SO JOURNAL OF AMERICAN HISTORY LA English DT Article ID ETHNOGENESIS; BONES C1 Smithsonian Inst, Margaret Henry Dabney Penick Resident Scholar Pro, Washington, DC 20560 USA. RP Strang, CB (reprint author), Smithsonian Inst, Margaret Henry Dabney Penick Resident Scholar Pro, Washington, DC 20560 USA. NR 124 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0021-8723 EI 1945-2314 J9 J AM HIST JI J. Am. Hist. PD MAR PY 2014 VL 100 IS 4 BP 973 EP 994 DI 10.1093/jahist/jau002 PG 22 WC History SC History GA AM5GR UT WOS:000339885600001 ER PT J AU Marrow, JC Basu, P Walsh, TF Siegal-Willott, JL AF Marrow, Judilee C. Basu, Puja Walsh, Timothy F. Siegal-Willott, Jessica L. TI HEPATOCELLULAR CARCINOMA IN CAPTIVE SLENDER TAILED MEERKATS (SURICATA SURICATTA): 5 CASES SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Hepatocellular carcinoma; Herpestidae; meerkat; Suricata suricatta ID FERRETS MUSTELA-NIGRIPES; HEPATIC NEOPLASMS; TUMORS; BEARS; DOGS AB Hepatocellular carcinoma was diagnosed in five slender tailed meerkats (Suricata suricatta) housed at the Smithsonian Institution's National Zoological Park between 1980 and 2013. Animals included four females and one male, ranging from 7 to 15 yr of age. Common clinical signs included weight loss and lethargy. Three of the neoplasms originated from the right medial liver lobe and were located adjacent to or partially incorporated in the gall bladder. Three animals had solitary masses, and two animals had multiple hepatic masses; all were characterized by polygonal to round neoplastic hepatocytes arranged in a trabecular pattern with smaller regions of varied solid, adenoid, and rarely peliod cell patterns. Hemorrhage and necrosis often with cystic degeneration was noted in all five cases. There was no evidence of metastatic disease in any of the cases examined. C1 [Marrow, Judilee C.; Basu, Puja; Walsh, Timothy F.; Siegal-Willott, Jessica L.] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. RP Marrow, JC (reprint author), Binder Pk Zoo, 7400 Div Dr, Battle Creek, MI 49014 USA. EM judileemarrowdvm@gmail.com NR 34 TC 0 Z9 0 U1 2 U2 4 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 EI 1937-2825 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD MAR PY 2014 VL 45 IS 1 BP 134 EP 142 PG 9 WC Veterinary Sciences SC Veterinary Sciences GA AM2AA UT WOS:000339649200017 PM 24712172 ER PT J AU Doster, E Chislock, MF Roberts, JF Kottwitz, JJ Wilson, AE AF Doster, Enrique Chislock, Michael F. Roberts, John F. Kottwitz, Jack J. Wilson, Alan E. TI RECOGNITION OF AN IMPORTANT WATER QUALITY ISSUE AT ZOOS: PREVALENCE AND POTENTIAL THREAT OF TOXIC CYANOBACTERIA SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Animal health; eutrophication; hepatotoxin; microcystin; phosphorus ID MICROCYSTIN AB Zoo animals may be particularly vulnerable to water sources contaminated with cyanobacterial toxins given their nonvoluntary close association with this resource. However, the prevalence and potential threat of toxic cyanobacteria in this setting are unknown. Several otherwise unexplained yellow-bellied slider (Trachemys scripta scripta) deaths were documented in a zoo moat with recurring blooms of toxic Microcystis aeruginosa. Furthermore, an extremely high and potentially lethal concentration of the hepatotoxin microcystin (166 ng/g) was found in the liver of a necropsied turtle that died in this moat. A subsequent monthly survey of water quality revealed detectable concentrations of microcystin in all moats (0.0001 to 7.5 mu g/L), with moats higher than 1 mu g/L being significantly higher than the threshold for safe drinking water recommended by the World Health Organization. These results demonstrate that cyanobacterial blooms are an important water quality issue in zoos, and future research is necessary to identify potential associations among water quality, zoo animal health, and moat management strategies. C1 [Doster, Enrique; Chislock, Michael F.; Wilson, Alan E.] Auburn Univ, Dept Fisheries & Allied Aquacultures, Auburn, AL 36849 USA. [Roberts, John F.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Anim Care Sci, Washington, DC 20013 USA. [Kottwitz, Jack J.] Auburn Univ, Coll Vet Med, Auburn, AL 36849 USA. RP Kottwitz, JJ (reprint author), Auburn Univ, Coll Vet Med, Auburn, AL 36849 USA. EM jack_kottwitz@hotmail.com FU Environmental Protection Agency Science to Achieve Results (STAR) Graduate Fellowship; Auburn University Dissertation Research Award; Auburn University Undergraduate Research Fellowship; National Science Foundation [DBI-0965272, DEB-0891944]; United States Geological Survey [2011AL121G] FX Zoo staff and management provided assistance and logistical support. Del Anderson, Jo-Marie Kasinak, Brie Olsen, Kayannush Pillai, Catherine Priester, Sydney Stewart, and Rachel Zitomer assisted during sampling and laboratory analyses. Beth Chislock and Lauren Jernigan provided helpful comments on the manuscript. This study was supported by an Environmental Protection Agency Science to Achieve Results (STAR) Graduate Fellowship, Auburn University Dissertation Research Award, Auburn University Undergraduate Research Fellowship, National Science Foundation grant (DBI-0965272 and DEB-0891944). and United States Geological Survey grant (2011AL121G). NR 12 TC 1 Z9 1 U1 4 U2 15 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 EI 1937-2825 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD MAR PY 2014 VL 45 IS 1 BP 165 EP 168 DI 10.1638/2013-0040R1.1 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA AM2AA UT WOS:000339649200023 PM 24712178 ER PT J AU Jerep, FC Van, RP AF Jerep, Fernando C. Van, Richard P. TI New Species of Nannocharax (Characiformes: Distichodontidae) from the Northwestern Congo River Basin, with an Appraisal of Hemigrammocharax SO COPEIA LA English DT Article ID TELEOSTEI; CAMEROON AB Nannocharax hastatus, new species, is described from the Lekoli River in the Likouala River system, Pool Malebo, and the Luilaka and Tshuapa rivers of the Momboyo river basin in the northwestern and central portions of the Congo River basin. The new species shares with N. ocellicauda and N. maculicauda a distinctive coloration pattern of a nearly completely unpigmented body other than for dark lines along the bases of the anal and dorsal fins and a longitudinally elongate, ovoid, dark spot on the posterior portion of the caudal peduncle and basal region of the central caudal-fin rays. That pigmentation pattern is unique to these three species in what was defined as the Hemigrammocharax-Nannocharax clade. In addition to coloration the three species share a distinctive overall elongate form of the head and body. Nannocharax hastatus differs from N. ocellicauda and N. maculicauda in the extent of poring along the lateral line and number of lateral line and circumpeduncular scales. Variation in the degree of poring of the lateral line in the species complex formed by these three species provides further evidence that the feature used-to-date to delimit Hemigrammocharax from Nannocharax the extent of poring along the lateral line fails to define monophyletic assemblages, and Hemigrammocharax is placed into the synonymy of Nannocharax which now forms a monophyletic assemblage. C1 [Jerep, Fernando C.; Van, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. [Jerep, Fernando C.] Univ Estadual Londrina, Ctr Ciencias Biol, Dept Biol Anim & Vegetal, BR-86057970 Londrina, PR, Brazil. RP Jerep, FC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. EM fjerep@gmail.com; varir@si.edu RI Jerep, Fernando/F-5274-2015 FU National Museum of Natural History; Smithsonian Institution; Herbert R. and Evelyn Axelrod Chair in the Division of Fishes, National Museum of Natural History FX We thank M. Stiassny and B. Brown (AMNH), J. Maclaine and O. Crimmen (BMNH), J. Friel (CUMV), E. Vreven and M. Parrent (MRAC), and D. Neumann (ZSM) for the loan of specimens and/or assistance during visits to their institutions. For assistance at NMNH we thank S. Raredon, J. Clayton, and L. Palmer. T. Griswold prepared Figure 1 and C. de Santana provided valuable input. U. Schliewen (ZSM) contributed valuable recommendations for the improvement of the paper. This project was made possible by support from the National Museum of Natural History, Smithsonian Institution and the Herbert R. and Evelyn Axelrod Chair in the Division of Fishes, National Museum of Natural History. NR 16 TC 3 Z9 3 U1 0 U2 0 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 MAR PY 2014 IS 1 BP 44 EP 49 DI 10.1643/CI-13-048 PG 6 WC Zoology SC Zoology GA AI9PS UT WOS:000337265700005 ER PT J AU Guerra, MA Ryan, MJ Cannatella, DC AF Guerra, Monica A. Ryan, Michael J. Cannatella, David C. TI Ontogeny of Sexual Dimorphism in the Larynx of the Tungara Frog, Physalaemus pustulosus SO COPEIA LA English DT Article ID XENOPUS-LAEVIS; NEOTROPICAL FROG; SOUND PRODUCTION; COMPLEX CALL; MATE CHOICE; MORPHOLOGY; MECHANISM; ANURA; ADVERTISEMENT; COMMUNICATION AB In the majority of frogs, males but not females produce vocalizations to attract mates. Sexual selection can influence the evolution of these vocalizations by modifying the frog's morphology. The larynx is the main organ responsible for sound production; thus, it constitutes a target of selection. The goal of this study was to determine qualitatively and quantitatively the sexual differences in the developmental sequence of larynges of Physakmmus pustulosus (=Engystomops pustulosus). We examined larynges of individuals ranging from recent metamorphs to adults. We provide quantitative measurements of laryngeal area and volume, vocal cords, and fibrous mass 1 (FM1), as well as qualitative descriptions of the developmental origin of vocal cords and FM1. Larynges of small male and female juveniles (less than 16 mm SVL) are similar, both externally and internally. The area of these larynges is no more than 1 mm(2); no vocal cords or FM1 are present in either sex at this developmental stage. In individuals larger than 16 mm SVL, there is a marked divergence in relative size of the larynx between the sexes. The male larynx begins to exhibit a strong positive allometry until it reaches a plateau at 24 mm SVL. Also, at 16 mm SVL, the vocal cords and FM1 appear as distinctive outgrowths on the wall of the arytenoid cartilage in male larynges. Female growth rate of the larynx, however, is constant and exhibits negative allometry throughout ontogeny. Female vocal cords and FM1 are barely distinguishable as adults, and never attain the size and most likely neither the mobility as in the adult male larynx. C1 [Guerra, Monica A.; Ryan, Michael J.; Cannatella, David C.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Panama. [Cannatella, David C.] Univ Texas Austin, Texas Nat Sci Ctr, Austin, TX 78712 USA. RP Guerra, MA (reprint author), Univ Texas Austin, Dept Integrat Biol, 1 Univ Stn C0990, Austin, TX 78712 USA. EM m.guerra@utexas.edu; mryan@utexas.edu; catfish@austin.utexas.edu FU Hubbs Regents Professorship (MJR); IACUC protocol [AUP-2010-00041] FX We thank J. Bond for the help provided breeding the frogs in the colony. We thank M. Chao and J. Dombroski for their help in taking and editing many of the photographs and K. Jiang for our long talks regarding R code. We also thank T. LaDuc for his assistance at the Herpetology Collection of the Texas Natural Science Center and M. Jansen for gently helping with the German to English translation of a paper. B. McClelland and members of the Cannatella and Ryan lab provided helpful comments on the manuscript. Partial support was provided by the Hubbs Regents Professorship (MJR). Procedures on live frogs were performed under IACUC protocol AUP-2010-00041. NR 50 TC 3 Z9 3 U1 2 U2 13 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 MAR PY 2014 IS 1 BP 123 EP 129 DI 10.1643/CG-13-051 PG 7 WC Zoology SC Zoology GA AI9PS UT WOS:000337265700015 ER PT J AU Smith, DG Platania, SP AF Smith, David G. Platania, Steven P. TI The Changing Face of Copeia SO COPEIA LA English DT Editorial Material C1 [Smith, David G.] Smithsonian Inst, MRC, Museum Support Ctr, Suitland, MD 20746 USA. [Platania, Steven P.] ASIR LLC, Albuquerque, NM 87102 USA. RP Smith, DG (reprint author), Smithsonian Inst, MRC, Museum Support Ctr, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM smithd@si.edu; platania@unm.edu NR 0 TC 0 Z9 0 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 MAR PY 2014 IS 1 BP 176 EP 180 DI 10.1643/OT-14-036 PG 5 WC Zoology SC Zoology GA AI9PS UT WOS:000337265700022 ER PT J AU Ben-Shlomo, D AF Ben-Shlomo, David TI Tell Jemmeh, Philistia and the Neo-Assyrian Empire during the Late Iron Age SO LEVANT LA English DT Article DE Tell Jemmeh; Neo-Assyrian Empire; Assyrian-style pottery; vaults; Philistia ID HOUSEHOLD ARCHAEOLOGY AB The site of Tell Jemmeh near Gaza has long been suggested as the location of an Assyrian administrative centre or even the seat of an Assyrian governor. This paper revisits this issue in the light of the more comprehensive evidence we now have on the site from Van Beek's excavations. Tell Jemmeh yielded both architectural features (in plans and building techniques) and Assyrian-style pottery that link it strongly to the Neo-Assyrian world. Whether these links indicate a massive Neo-Assyrian presence at the site, or that the site was an Assyrian administrative centre is still an open question. The archaeological and textual evidence from this period will be combined in order to examine the nature and extent of Neo-Assyrian influence on Tell Jemmeh in particular, and on Philistia in general. The characteristics of each of the Assyrian features will be studied in detail in order to assess its significance with regard to the Assyrian connection and the regional historical background. It seems that the Neo-Assyrian Empire had special interests in the region of Philistia and its city-states, together with other regions in the southern Levant. However, the nature of these interests, of imperial policies, and the consequences for the local cultures may have changed during the reign of the different Assyrian rulers during the late 8th and early 7th centuries BC. The management of the Assyrian Empire in its distant provinces and vassaldoms will also be discussed in the light of the archaeological evidence. C1 Smithsonian Inst, Dept Anthropol, NMNH, Washington, DC 20560 USA. RP Ben-Shlomo, D (reprint author), Smithsonian Inst, Dept Anthropol, NMNH, Washington, DC 20560 USA. EM davben187@yahoo.com NR 143 TC 3 Z9 3 U1 0 U2 2 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0075-8914 EI 1756-3801 J9 LEVANT JI Levant PD SPR PY 2014 VL 46 IS 1 BP 58 EP 88 DI 10.1179/0075891413Z.00000000031 PG 31 WC Archaeology SC Archaeology GA AI7TO UT WOS:000337102100005 ER PT J AU Paine, SN Turner, DD Kuchler, N AF Paine, Scott N. Turner, David D. Kuechler, Nils TI Understanding Thermal Drift in Liquid Nitrogen Loads Used for Radiometric Calibration in the Field SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Instrumentation; sensors; Microwave observations; Profilers; atmospheric; Remote sensing ID PHASES; WATER AB An absorbing load in a liquid nitrogen bath is commonly used as a radiance standard for calibrating radiometers operating at microwave to infrared wavelengths. It is generally assumed that the physical temperature of the load is stable and equal to the boiling point temperature of pure N-2 at the ambient atmospheric pressure. However, this assumption will fail to hold when air movement, as encountered in outdoor environments, allows O-2 gas to condense into the bath. Under typical conditions, initial boiling point drift rates of order 25 mK min(-1) can occur, and the boiling point of a bath maintained by repeated refilling with pure N-2 can eventually shift by approximately 2 K. Laboratory bench tests of a liquid nitrogen bath under simulated wind conditions are presented together with an example of an outdoor radiometer calibration that demonstrates the effect, and the physical processes involved are explained in detail. A key finding is that in windy conditions, changes in O-2 volume fraction are related accurately to fractional changes in bath volume due to boiloff, independent of wind speed. This relation can be exploited to ensure that calibration errors due to O-2 contamination remain within predictable bounds. C1 [Paine, Scott N.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Turner, David D.] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA. [Kuechler, Nils] Univ Cologne, Inst Geophys & Meteorol, Cologne, Germany. RP Paine, SN (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM spaine@cfa.harvard.edu OI Paine, Scott/0000-0003-4622-5857 FU TransRegio32 project FX We thank Drs. Susanne Crewell, Ulrich Lohnert, Gerrit Maschwitz, and Thomas Rose for helpful discussions regarding this work, and R. Haseneder-Lind for assistance with the field experiments. This study was partly funded by the TransRegio32 project, which also provided travel support for DDT to visit the University of Cologne. NR 14 TC 4 Z9 4 U1 0 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD MAR PY 2014 VL 31 IS 3 BP 647 EP 655 DI 10.1175/JTECH-D-13-00171.1 PG 9 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AH6EF UT WOS:000336222800007 ER PT J AU Schwadron, NA Goelzer, ML Smith, CW Kasper, JC Korreck, K Leamon, RJ Lepri, ST Maruca, BA McComas, D Steven, ML AF Schwadron, N. A. Goelzer, M. L. Smith, C. W. Kasper, J. C. Korreck, K. Leamon, R. J. Lepri, S. T. Maruca, B. A. McComas, D. Steven, M. L. TI Coronal electron temperature in the protracted solar minimum, the cycle 24 mini maximum, and over centuries SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID OPEN MAGNETIC-FLUX; WIND; FIELD; PREDICTION; EVOLUTION AB Recent in situ observations of the solar wind show that charge states (e.g., the O7+/O6+ and C6+/C5+ abundance ratios) evolved through the extended, deep solar minimum between solar cycles 23 and 24 (i.e., from 2006 to 2009) reflecting cooler electron temperatures in the corona. We extend previous analyses to study the evolution of the coronal electron temperature through the protracted solar minimum and observe not only the reduction in coronal temperature in the cycles 23-24 solar minimum but also a small increase in coronal temperature associated with increasing activity during the "mini maximum" in cycle 24. We use a new model of the interplanetary magnetic flux since 1749 to estimate coronal electron temperatures over more than two centuries. The reduction in coronal electron temperature in the cycles 23-24 protracted solar minimum is similar to reductions observed at the beginning of the Dalton Minimum (similar to 1805-1840). If these trends continue to reflect the evolution of the Dalton Minimum, we will observe further reductions in coronal temperature in the cycles 24-25 solar minimum. Preliminary indications in 2013 do suggest a further post cycle 23 decline in solar activity. Thus, we extend our understanding of coronal electron temperature using the solar wind scaling law and compare recent reductions in coronal electron temperature in the protracted solar minimum to conditions that prevailed in the Dalton Minimum. C1 [Schwadron, N. A.; Goelzer, M. L.; Smith, C. W.] Univ New Hampshire, Durham, NH 03824 USA. [Schwadron, N. A.; McComas, D.] SW Res Inst, San Antonio, TX USA. [Kasper, J. C.; Korreck, K.; Steven, M. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Leamon, R. J.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Lepri, S. T.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Maruca, B. A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [McComas, D.] Univ Texas San Antonio, San Antonio, TX USA. RP Schwadron, NA (reprint author), Univ New Hampshire, Durham, NH 03824 USA. EM n.schwadron@unh.edu RI Lepri, Susan/I-8611-2012; Kasper, Justin/D-1152-2010 OI Kasper, Justin/0000-0002-7077-930X FU LRO/CRaTER (NASA) [NNG11PA03C]; NASA Coronal-Solar Wind Energetic Particle Acceleration Modules (C-SWEPA [NNX07AC14G]; NSF [AGS1135432]; Solar Probe Plus Integrated Investigation of the Sun (SPP-ISIS) project; DREAM 2 investigation (NASA) [NNX10AB17A]; ACE/MAG Caltech [44A-1062037]; ACE/SWEPAM; WIND/SWE project; NSF-Solar REU program FX N.A.S. was supported by LRO/CRaTER (NASA contract NNG11PA03C), the NASA Coronal-Solar Wind Energetic Particle Acceleration Modules (C-SWEPA; NASA grant NNX07AC14G) project, the NSF Sun-2-Ice project (NSF grant AGS1135432), the Solar Probe Plus Integrated Investigation of the Sun (SPP-ISIS) project, and the DREAM 2 investigation (NASA Grant NNX10AB17A). Both C. W. S. and M. L. G. were supported by the ACE/MAG Caltech subcontract 44A-1062037 to UNH. D. M. C. was supported by ACE/SWEPAM. J.C.K., M. L. S., K. E. K., and B. A. M. were supported by the WIND/SWE project. K. K. was supported by the NSF-Solar REU program. We thank the ACE SWICS and SWIMS instrument team and the Ion Mass Spectrometer (SWIMS) ACE Science Center for providing the ACE data. NR 27 TC 7 Z9 7 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAR PY 2014 VL 119 IS 3 BP 1486 EP 1492 DI 10.1002/2013JA019397 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6CM UT WOS:000336218300007 ER PT J AU Rocha, R Lopez-Baucells, A AF Rocha, Ricardo Lopez-Baucells, Adria TI Opportunistic predation by Crested Owl Lophostrix cristata upon Seba's Short-tailed Bat Carollia perspicillata SO REVISTA BRASILEIRA DE ORNITOLOGIA LA English DT Article DE central Amazon; diet; Phyllostomidae; Strigidae; trophic interaction. ID NOCTURNAL BIRDS; BRAZIL; FOREST AB This note reports two opportunistic events of predation on Seba's Short-tailed Bats Carollia perspicillata (Chiroptera: Phyllostomidae) by an immature Crested Owl Lophostrix cristata (Strigiformes: Strigidae), in Central Amazonia, Brazil. Both predation events took place while bats were mist-netted. Given the abundance of C. perspicillata in the study area we argue that this bat species likely constitutes a natural prey for L. cristata. C1 [Rocha, Ricardo; Lopez-Baucells, Adria] Univ Lisbon, Fac Ciencias, Ctr Biol Ambiental, Dept Biol Anim, P-1749016 Lisbon, Portugal. [Rocha, Ricardo] Univ Helsinki, Fac Biosci, Metapopulat Res Grp, FI-00014 Helsinki, Finland. [Rocha, Ricardo; Lopez-Baucells, Adria] Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. [Rocha, Ricardo; Lopez-Baucells, Adria] Smithsonian Trop Res Inst, BR-69011970 Manaus, Amazonas, Brazil. [Lopez-Baucells, Adria] Museu Ciencies Nat Granollers, Granollers, Catalonia, Spain. RP Rocha, R (reprint author), Univ Lisbon, Fac Ciencias, Ctr Biol Ambiental, Dept Biol Anim, Bloco C2, P-1749016 Lisbon, Portugal. EM ricardo.nature@gmail.com OI Lopez-Baucells, Adria/0000-0001-8446-0108 FU Portuguese Foundation for Science and Technology [PTDC/BIA-BIC/111184/2009, SFRH/BD/80488/2011] FX We would like to thank Christoph F. J. Meyer, Paulo Bobrowiec, and Jorge Palmeirim for assistance during all phases of the project and Jose L. C. Camargo, Rosely Hipolito, and Ary Jorge Ferreira for logistic support. We also thank Jared Wolfe and Goncalo Ferraz for assisting on the owl identification and Sasha Vasconcelos for commenting on early drafts. Financial support was provided by the Portuguese Foundation for Science and Technology through the grants PTDC/BIA-BIC/111184/2009 and SFRH/BD/80488/2011. This is publication 632 of the Technical Series of the BDFPP. NR 14 TC 2 Z9 2 U1 0 U2 6 PU SOC BRASILEIRA ORNITOLOGIA PI VICOSA PA C/O ROMULO RIBON, MUSEU ZOOLOGIA JOAO MOOJEN, LADEIRA DOS OPERARIOS 54-204, VICOSA, MG 36570-000, BRAZIL SN 0103-5657 J9 REV BRAS ORNITOL JI Rev. Bras. Ornitol. PD MAR PY 2014 VL 22 IS 1 BP 35 EP 37 PG 3 WC Ornithology SC Zoology GA AH6LA UT WOS:000336241200005 ER PT J AU Davias, LA Kornis, MS Breitburg, DL AF Davias, Lori A. Kornis, Matthew S. Breitburg, Denise L. TI Environmental factors influencing C-13 and N-15 in three Chesapeake Bay fishes SO ICES JOURNAL OF MARINE SCIENCE LA English DT Article DE Chesapeake Bay; estuarine foodwebs; fish; habitat; land use; shoreline development; stable isotopes ID STABLE-ISOTOPE RATIOS; CORDGRASS SPARTINA-ALTERNIFLORA; REED PHRAGMITES-AUSTRALIS; SCULPIN COTTUS-COGNATUS; FOOD-WEB SUPPORT; SALT-MARSH FISH; FUNDULUS-HETEROCLITUS; TROPHIC POSITION; SITE FIDELITY; WHITE PERCH AB Stable isotope analysis has become a common tool for mapping trophic relationships, describing foodweb changes, and assessing ecosystem health. Clear interpretation of stable isotopes is facilitated by understanding how environmental factors can affect isotopic values; in estuarine systems, these factors may include salinity, land use, and shoreline habitat. To evaluate these factors, fish were collected from shallow-water habitats next to hardened (bulkhead and riprap) and unhardened (beach and marsh) shorelines within five subestuaries of the Chesapeake Bay that differed in predominant land use and salinity. This study focused on three common mid-Atlantic fish species: mummichog, Fundulus heteroclitus, Atlantic silverside, Menidia menidia, and white perch, Morone americana. Multiple regression analyses pointed to standard length, salinity, of watershed as developed or crop land, and shoreline habitat type as important predictors for N-15 in all three species and for C-13 in mummichog and white perch. Further analysis controlling for the effects of salinity, land use, and fish size demonstrated that C-13 and N-15 were lower in tissues of fish collected next to marsh compared with hardened or beach habitat. Habitat effects were strongest for mummichog. This study focused on overarching patterns driving stable isotope signatures in fish; however, it also indicated potentially important interactions between nearshore habitat type and land use or salinity that deserve further analysis. Results have implications for the scale of isotope inquiry and give justification for more detailed follow-up studies of foodweb structure along modified and natural shorelines. C1 [Davias, Lori A.; Kornis, Matthew S.; Breitburg, Denise L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Davias, Lori A.] Mansfield Univ Penn, Mansfield, PA 16933 USA. RP Davias, LA (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM ldavias@mansfield.edu FU NOAA, National Centers for Coastal Ocean Science, Center for Sponsored Coastal Ocean Research [NA09NOS4780214] FX This research was supported by grant NA09NOS4780214 from NOAA, National Centers for Coastal Ocean Science, Center for Sponsored Coastal Ocean Research. S. Giordano was critical to field collection of fish. C. France ran isotope samples at the Smithsonian Center for Museum Conservation. T. Jordan and J. Miklas provided nitrogen concentration data. Many thanks to J. Malek, D. Shikashio, E. Gamelin, M. Finch, K. Sellers, J. Nora, K. Heggie, A. Keppel, and C. Little for field and lab assistance. Thanks to K. Gedan for comments on analyses and to K. Maloney, J.C. Hoffman and an anonymous reviewer for comments on drafts of this manuscript. This paper is dedicated to the memory of Rob Klumb, who influenced the early career of L. Davias. NR 84 TC 0 Z9 0 U1 2 U2 26 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1054-3139 EI 1095-9289 J9 ICES J MAR SCI JI ICES J. Mar. Sci. PD MAR-APR PY 2014 VL 71 IS 3 BP 689 EP 702 DI 10.1093/icesjms/fst143 PG 14 WC Fisheries; Marine & Freshwater Biology; Oceanography SC Fisheries; Marine & Freshwater Biology; Oceanography GA AF4OY UT WOS:000334694300026 ER PT J AU Ripperger, SP Tschapka, M Kalko, EKV Rodriguez-Herrera, B Mayer, F AF Ripperger, Simon P. Tschapka, Marco Kalko, Elisabeth K. V. Rodriguez-Herrera, Bernal Mayer, Frieder TI Resisting habitat fragmentation: High genetic connectivity among populations of the frugivorous bat Carollia castanea in an agricultural landscape SO AGRICULTURE ECOSYSTEMS & ENVIRONMENT LA English DT Article DE Carollia castanea; Habitat fragmentation; Genetic population structure; Isolation by distance; Mitochondrial D-loop ID TAILED FRUIT BATS; PHYLLOSTOMID BATS; COSTA-RICA; DIVERSITY; FLOW; DISPERSAL; BIRD; DIFFERENTIATION; CONSERVATION; BIODIVERSITY AB Anthropogenically dominated landscapes are frequently a patchwork composed of manmade structures and natural habitat remnants. Especially tropical landscapes are progressively turning into such heterogeneous mosaics leading to simplification of animal communities and (partial) isolation of the scattered survivors. Modern molecular approaches provide powerful tools to detect discontinuities in gene flow among local populations. The aim of this study was to evaluate genetic connectivity on a small geographic scale among local bat populations that inhabit forest fragments in an agricultural matrix in north-east Costa Rica. We focused on Carollia castanea (Phyllostomidae), a small frugivorous bat that mainly feeds on pepper plants. We analyzed DNA sequences of the mitochondrial D-loop of 173 adult individuals. There was no significant global population differentiation detectable (F-ST = 0.008, p = 0.17) and regular gene flow among populations was indicated by low pairwise F-ST-values, even in highly fragmented areas. Solely with increasing geographic distance gene flow was weakened, indicated by a significant isolation by distance pattern (R-2 = 0.55, p < 0.05). Our study shows that C. castanea can cope better with small-scale habitat fragmentation than other phyllostomid bat species, at least in an agriculturally dominated landscape. This is probably because of its tolerance toward disturbed habitats for foraging that enables it to maintain genetic exchange among populations that are separated by areas under human influence. (C) 2013 Elsevier B.V. All rights reserved. C1 [Ripperger, Simon P.; Mayer, Frieder] Leibniz Inst Evolut & Biodiversitatsforsch, Museum Nat Kunde, D-10115 Berlin, Germany. [Ripperger, Simon P.; Tschapka, Marco; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Tschapka, Marco; Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Rodriguez-Herrera, Bernal] Univ Costa Rica, Escuela Biol, San Pedro, Costa Rica. [Mayer, Frieder] Berlin Brandenburg Inst Adv Biodivers Res BBIB, D-14195 Berlin, Germany. RP Ripperger, SP (reprint author), Leibniz Inst Evolut & Biodiversitatsforsch, Museum Nat Kunde, Invalidenstr 43, D-10115 Berlin, Germany. EM simon.ripperger@mfn-berlin.de FU "Deutscher Akademischer Austauschdienst" (DAAD) FX We thank Marcelo Lopez of Sueno Azul Resort, Alberto Quintana of Hacienda Pozo Azul, Giovanna Holbrook of Selva Verde Lodge and all private land owners for the permission to conduct fieldwork. For assistance in the field we are grateful to Emanuel Rojas, Elder Miranda, and Katrin Heer, and to Martina Nagy for advising in the laboratory. We thank Steven Sesnie for providing the land cover map and Ann Cespedes & Emma Berdan for their help to improve this manuscript. Logistical support was provided by Chiquita Brands International. This work was approved by Javier Guevara (Resolutions: 047-2010-SINAC, 004-2011-SINAC, 128-2011-SINAC). Funding for field work was provided by a grant of the "Deutscher Akademischer Austauschdienst" (DAAD) to SPR. NR 59 TC 3 Z9 3 U1 2 U2 37 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-8809 EI 1873-2305 J9 AGR ECOSYST ENVIRON JI Agric. Ecosyst. Environ. PD MAR 1 PY 2014 VL 185 BP 9 EP 15 DI 10.1016/j.agee.2013.12.006 PG 7 WC Agriculture, Multidisciplinary; Ecology; Environmental Sciences SC Agriculture; Environmental Sciences & Ecology GA AF8PL UT WOS:000334978000002 ER PT J AU Aliu, E Aune, T Behera, B Beilicke, M Benbow, W Berger, K Bird, R Buckley, JH Bugaev, V Cardenzana, JV Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Duke, C Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fortin, P Fortson, L Furniss, A Galante, N Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Kaaret, P Kargaltsev, O Kertzman, M Khassen, Y Kieda, D Krawczynski, H Lang, MJ Madhavan, AS Maier, G Majumdar, P McCann, A Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Pandel, D Perkins, JS Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Rajotte, J Reyes, LC Reynolds, PT Richards, GT Roache, E Sembroski, GH Skole, C Staszak, D Telezhinsky, I Theiling, M Tucci, JV Tyler, J Varlotta, A Vincent, S Wakely, SP Weekes, TC Weinstein, A Welsing, R Williams, DA Zitzer, B AF Aliu, E. Aune, T. Behera, B. Beilicke, M. Benbow, W. Berger, K. Bird, R. Buckley, J. H. Bugaev, V. Cardenzana, J. V. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Duke, C. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Kaaret, P. Kargaltsev, Oleg Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Lang, M. J. Madhavan, A. S. Maier, G. Majumdar, P. McCann, A. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Rajotte, J. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Sembroski, G. H. Skole, C. Staszak, D. Telezhinsky, I. Theiling, M. Tucci, J. V. Tyler, J. Varlotta, A. Vincent, S. Wakely, S. P. Weekes, T. C. Weinstein, A. Welsing, R. Williams, D. A. Zitzer, B. TI OBSERVATIONS OF THE UNIDENTIFIED GAMMA-RAY SOURCE TeV J2032+4130 BY VERITAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: general; pulsars: individual (PSR J2032+4127) ID CYGNUS REGION; SOURCE TEV-J2032+4130; FOLLOW-UP; ASTRONOMY; TELESCOPE; POPULATION; SEPARATION; DISCOVERY; EMISSION; GALAXY AB TeV J2032+4130 was the first unidentified source discovered at very high energies (VHEs; E > 100 GeV), with no obvious counterpart in any other wavelength. It is also the first extended source to be observed in VHE gamma rays. Following its discovery, intensive observational campaigns have been carried out in all wavelengths in order to understand the nature of the object, which have met with limited success. We report here on a deep observation of TeV J2032+4130 based on 48.2 hr of data taken from 2009 to 2012 by the Very Energetic Radiation Imaging Telescope Array System experiment. The source is detected at 8.7 standard deviations (sigma) and is found to be extended and asymmetric with a width of 9'.5 +/- 1'.2 along the major axis and 4'.0 +/- 0'.5 along the minor axis. The spectrum is well described by a differential power law with an index of 2.10 +/- 0.14(stat) +/- 0.21(sys) and a normalization of (9.5 +/- 1.6(stat) +/- 2.2(sys)) x 10(-13) TeV-1 cm(-2) s(-1) at 1 TeV. We interpret these results in the context of multiwavelength scenarios which particularly favor the pulsar wind nebula interpretation. C1 [Aliu, E.; Errando, M.; Mukherjee, R.; Nieto, D.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Aune, T.; Majumdar, P.; Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Behera, B.; Chen, X.; Federici, S.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Skole, C.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Roache, E.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cardenzana, J. V.; Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Tucci, J. V.; 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.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Humensky, T. B.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kargaltsev, Oleg] George Washington Univ, Dept Phys, Washington, DC USA. [Kertzman, M.] DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Majumdar, P.] Saha Inst Nucl Phys, Kolkata 700064, India. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.; Richards, G. T.] 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, Goddard Space Flight Ctr, Greenbelt, MD 20771 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. [Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. EM gareth.hughes@desy.de; pratik.majumdar@saha.ac.in RI Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755; Cui, Wei/0000-0002-6324-5772; 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]; STFC in the U.K.; Young Investigators Program of the Helmholtz Association; NASA [NNX09AC84G, NNX09AC81G] FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. G. H. acknowledges support through the Young Investigators Program of the Helmholtz Association. The work by O.K. was supported by NASA grants NNX09AC84G and NNX09AC81G. NR 50 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 16 DI 10.1088/0004-637X/783/1/16 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600016 ER PT J AU Auchettl, K Slane, P Castro, D AF Auchettl, Katie Slane, Patrick Castro, Daniel TI FERMI-LAT OBSERVATIONS OF SUPERNOVA REMNANTS KESTEVEN 79 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: ISM; ISM: individual objects (Kesteven 79, G33.6+0.1, Kesteven 78, G32.8-0.1); ISM: supernova remnants ID LARGE-AREA TELESCOPE; COSMIC-RAY ACCELERATION; GALACTIC RADIO-SOURCES; CHANDRA X-RAY; MOLECULAR CLOUDS; INTERSTELLAR-MEDIUM; RX J1713.7-3946; SHOCK ACCELERATION; NEUTRAL HYDROGEN; MASER EMISSION AB In this paper, we report on the detection of gamma-ray emission coincident with the Galactic supernova remnant (SNR) Kesteven 79 (Kes 79). We analyzed approximately 52 months of data obtained with the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. Kes 79 is thought to be interacting with adjacent molecular clouds, based on the presence of strong (CO)-C-12 J = 1 -> 0 and HCO+ J = 1 -> 0 emission and the detection of 1720 MHz line emission toward the east of the remnant. Acceleration of cosmic rays is expected to occur at SNR shocks, and SNRs interacting with dense molecular clouds provide a good testing ground for detecting and analyzing the production of gamma-rays from the decay of pi(0) into two gamma-ray photons. This analysis investigates gamma-ray emission coincident with Kes 79, which has a detection significance of similar to 7 sigma. Additionally, we present an investigation of the spatial and spectral characteristics of Kes 79 using multiple archival XMM-Newton observations of this remnant. We determine the global X-ray properties of Kes 79 and estimate the ambient density across the remnant. We also performed a similar analysis for Galactic SNR Kesteven 78 (Kes 78), but due to large uncertainties in the gamma-ray background model, no conclusion can be made about an excess of GeV gamma-ray associated with the remnant. C1 [Auchettl, Katie; Slane, Patrick] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Auchettl, Katie] Monash Univ, Sch Phys, Melbourne, Vic 3800, Australia. [Auchettl, Katie] Monash Univ, Monash Ctr Astrophys, Melbourne, Vic 3800, Australia. [Auchettl, Katie] Monash Univ, ARC Ctr Excellence Particle Phys Tera Scale, Melbourne, Vic 3800, Australia. [Castro, Daniel] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. RP Auchettl, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [NNX 11AQ096, NAS8-03060]; NASA through SAO of the Chandra X-Ray Center [NAS8-03060, SV3-73016] FX The authors thank Dr. Thomas M. Dame for his in depth discussions in regards to the association and interaction of Kes 79 with its surrounding molecular cloud. K. A. thanks Dr. Jasmina Lazendic-Galloway for her helpful discussions in regards to the X-ray analysis. This work was partially funded by NASA grant NNX 11AQ096. P. S. acknowledges support from NASA contract NAS8-03060. D. C. acknowledges support for this work provided by NASA through SAO contract SV3-73016 to MIT for Support of the Chandra X-Ray Center, which is operated by the SAO under contract NAS8-03060. NR 93 TC 11 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 32 DI 10.1088/0004-637X/783/1/32 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600032 ER PT J AU Bayliss, MB Johnson, T Gladders, MD Sharon, K Oguri, M AF Bayliss, Matthew B. Johnson, Traci Gladders, Michael D. Sharon, Keren Oguri, Masamune TI LINE-OF-SIGHT STRUCTURE TOWARD STRONG LENSING GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: distances and redshifts; gravitational lensing: strong; large-scale structure of universe; techniques: spectroscopic ID GIANT-ARC STATISTICS; POLE TELESCOPE SURVEY; LARGE-SCALE STRUCTURE; RAY-SELECTED SAMPLE; DIGITAL SKY SURVEY; GRAVITATIONAL LENSES; MILLENNIUM SIMULATION; MATTER DISTRIBUTION; REDSHIFT SURVEY; CROSS-SECTIONS AB We present an analysis of the line-of-sight structure toward a sample of 10 strong lensing cluster cores. Structure is traced by groups that are identified spectroscopically in the redshift range, 0.1 <= z <= 0.9, and we measure the projected angular and comoving separations between each group and the primary strong lensing clusters in each corresponding line of sight. From these data we measure the distribution of projected angular separations between the primary strong lensing clusters and uncorrelated large-scale structure as traced by groups. We then compare the observed distribution of angular separations for our strong lensing selected lines of sight against the distribution of groups that is predicted for clusters lying along random lines of sight. There is clear evidence for an excess of structure along the line of sight at small angular separations (theta <= 6') along the strong lensing selected lines of sight, indicating that uncorrelated structure is a significant systematic that contributes to producing galaxy clusters with large cross sections for strong lensing. The prevalence of line-of-sight structure is one of several biases in strong lensing clusters that can potentially be folded into cosmological measurements using galaxy cluster samples. These results also have implications for current and future studies-such as the Hubble Space Telescope Frontier Fields-that make use of massive galaxy cluster lenses as precision cosmological telescopes; it is essential that the contribution of line-of-sight structure be carefully accounted for in the strong lens modeling of the cluster lenses. C1 [Bayliss, Matthew B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Johnson, Traci; Sharon, Keren] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [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. [Oguri, Masamune] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Oguri, Masamune] Univ Tokyo, WPI, Kavli IPMU, Chiba 2778583, Japan. RP Bayliss, MB (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM mbayliss@cfa.harvard.edu RI Oguri, Masamune/C-6230-2011 FU National Science Foundation [AST-1009012]; NASA from the Space Telescope Science Institute [HST-GO-13003.01]; NASA [NAS5-26555]; FIRST program Subaru Measurements of Images and Redshifts (SuMIRe), World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan; JSPS [23740161]; Harvard-Smithsonian Center for Astrophysics (CfA); Harvard Library; Institute for Quantitative Social Science FX We thank Eric Bell for helpful discussion that improved the quality of this paper significantly. This work was supported by the National Science Foundation through grant AST-1009012. Support was also provided by NASA through grant HST-GO-13003.01 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555, and by the FIRST program Subaru Measurements of Images and Redshifts (SuMIRe), World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and Grant-in-Aid for Scientific Research from the JSPS (23740161). The data used in this work is publicly hosted with support from the Harvard-Smithsonian Center for Astrophysics (CfA) in collaboration with Harvard Library and the Institute for Quantitative Social Science, with infrastructure provided by Harvard University Information Technology Services. NR 82 TC 14 Z9 14 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 41 DI 10.1088/0004-637X/783/1/41 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600041 ER PT J AU Cohen, O Drake, JJ AF Cohen, O. Drake, J. J. TI A GRID OF MHD MODELS FOR STELLAR MASS LOSS AND SPIN-DOWN RATES OF SOLAR ANALOGS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: evolution; stars: mass loss; stars: solar-type; stars: winds, outflows ID X-RAY-EMISSION; ACTIVITY-ROTATION RELATIONSHIP; ANGULAR-MOMENTUM LOSS; LATE-TYPE DWARFS; MAGNETIC-FIELDS; HOT JUPITERS; LOCAL BUBBLE; COOL STARS; WIND; EVOLUTION AB Stellar winds are believed to be the dominant factor in the spin-down of stars over time. However, stellar winds of solar analogs are poorly constrained due to observational challenges. In this paper, we present a grid of magnetohydrodynamic models to study and quantify the values of stellar mass loss and angular momentum loss rates as a function of the stellar rotation period, magnetic dipole component, and coronal base density. We derive simple scaling laws for the loss rates as a function of these parameters, and constrain the possible mass loss rate of stars with thermally driven winds. Despite the success of our scaling law in matching the results of the model, we find a deviation between the "solar dipole" case and a real case based on solar observations that overestimates the actual solar mass loss rate by a factor of three. This implies that the model for stellar fields might require a further investigation with additional complexity. Mass loss rates in general are largely controlled by the magnetic field strength, with the wind density varying in proportion to the confining magnetic pressure B-2. We also find that the mass loss rates obtained using our grid models drop much faster with the increase in rotation period than scaling laws derived using observed stellar activity. For main-sequence solar-like stars, our scaling law for angular momentum loss versus poloidal magnetic field strength retrieves the well-known Skumanich decline of angular velocity with time, Omega(star) alpha t(-1/2) , if the large-scale poloidal magnetic field scales with rotation rate as B-p alpha Omega(2)(star). C1 [Cohen, O.; Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Cohen, Ofer/0000-0003-3721-0215 FU Chandra CXC grant [TM2-13001X]; SI Grand Challenges [40510298OO5000]; NASA [NAS8-03060]; NASA ESS; NASA ESTO-CT; NSF KDI; DoD MURI FX We thank an anonymous referee for her/his useful comments and suggestions. We also thank Vinay Kahsyap and Cecilia Garraffo for useful discussions, and Steve Cranmer for providing the results from his model. This work was supported by Chandra CXC grant TM2-13001X and SI Grand Challenges grant number 40510298OO5000. We thank the Director of the Unlocking the Mysteries of the Universe Consortium, Christine Jones, for support and encouragement. J.J.D. was supported by NASA contract NAS8-03060 to the Chandra X-ray Center and thanks the Director, H. Tananbaum, for continuing advice and support. Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI. NR 59 TC 15 Z9 15 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 55 DI 10.1088/0004-637X/783/1/55 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600055 ER PT J AU Drake, JJ Ratzlaff, P Kashyap, V Huenemoerder, DP Wargelin, BJ Pease, DO AF Drake, Jeremy J. Ratzlaff, Peter Kashyap, Vinay Huenemoerder, David P. Wargelin, Bradford J. Pease, Deron O. TI A 33 yr CONSTANCY OF THE X-RAY CORONAE OF AR Lac AND ECLIPSE DIAGNOSIS OF SCALE HEIGHT SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; stars: activity; stars: coronae; stars: late-type; stars: individual (AR Lac); X-rays: stars ID RS CANUM-VENATICORUM; EXTREME-ULTRAVIOLET EMISSION; TRANSITION-REGION STRUCTURE; ACTIVE STELLAR CORONAE; BINARIES V711 TAURI; ROTATIONAL MODULATION; XMM-NEWTON; II PEGASI; PERIOD CHANGES; CVN SYSTEMS AB Extensive X-ray and EUV photometric observations of the eclipsing RS CVn system AR Lac were obtained over the years 1997-2013 with the Chandra X-Ray Observatory Extreme-Ultraviolet Explorer (EUVE). During primary eclipse, High Resolution Camera count rates decrease by similar to 40%. A similar minimum is seen during one primary eclipse observed by EUVE but not in others owing to intrinsic source variability. Little evidence for secondary eclipses is present in either the X-ray or EUV data, reminiscent of earlier X-ray and EUV observations. Primary eclipses allow us to estimate the extent of a spherically symmetric corona on the primary G star of about 1.3 R-circle dot, or 0.86 R-star, and indicate that the G star is likely brighter than the K component by a factor of 2-5. Brightness changes not attributable to eclipses appear to be dominated by stochastic variability and are generally non-repeating. X-ray and EUV light curves cannot therefore be reliably used to reconstruct the spatial distribution of emission assuming that only eclipses and rotational modulation are at work. Moderate flaring is observed, where count rates increase by up to a factor of three above quiescence. Combined with older ASCA, Einstein, EXOSAT, ROSAT, and BeppoSAX observations, the data show that the level of quiescent coronal emission at X-ray wavelengths has remained remarkably constant over 33 yr, with no sign of variation due to magnetic cycles. Variations in base level X-ray emission seen by Chandra over 13 yr are only similar to 10%, while variations back to pioneering Einstein observations in 1980 amount to a maximum of 45% and more typically about 15%. C1 [Drake, Jeremy J.; Ratzlaff, Peter; Kashyap, Vinay; Wargelin, Bradford J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huenemoerder, David P.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Pease, Deron O.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Drake, JJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [NAS8-03060]; Smithsonian Astrophysical Observatory [SV3-73016] FX J.J.D., V. K., P. R., and B.J.W. were funded by NASA contract NAS8-03060 to the Chandra X-ray Center (CXC) and thank the CXC director, H. Tananbaum, and the CXC science team for advice and support. D. P. H. was supported by Smithsonian Astrophysical Observatory contract SV3-73016 to MIT for Support of the Chandra X-Ray Center. NR 74 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 2 DI 10.1088/0004-637X/783/1/2 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600002 ER PT J AU Dunham, MM Arce, HG Mardones, D Lee, JE Matthews, BC Stutz, AM Williams, JP AF Dunham, Michael M. Arce, Hector G. Mardones, Diego Lee, Jeong-Eun Matthews, Brenda C. Stutz, Amelia M. Williams, Jonathan P. TI MOLECULAR OUTFLOWS DRIVEN BY LOW-MASS PROTOSTARS. I. CORRECTING FOR UNDERESTIMATES WHEN MEASURING OUTFLOW MASSES AND DYNAMICAL PROPERTIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: jets and outflows; stars: formation; stars: low-mass; submillimeter: ISM ID YOUNG STELLAR OBJECTS; SPITZER C2D SURVEY; HERBIG-HARO OBJECTS; OBSERVED LUMINOSITY SPREAD; DARK CLOUD DC-303.8-14.2; DUST CONTINUUM EMISSION; STAR-FORMING REGIONS; SPECTRAL-LINE SURVEY; R-CORONAE-AUSTRALIS; NEARBY DENSE CORES AB We present a survey of 28 molecular outflows driven by low-mass protostars, all of which are sufficiently isolated spatially and/or kinematically to fully separate into individual outflows. Using a combination of new and archival data from several single-dish telescopes, 17 outflows are mapped in (CO)-C-12 (2-1) and 17 are mapped in (CO)-C-12 (3-2), with 6 mapped in both transitions. For each outflow, we calculate and tabulate the mass (M-flow), momentum (P-flow), kinetic energy (E-flow), mechanical luminosity (L-flow), and force (F-flow) assuming optically thin emission in LTE at an excitation temperature, T-ex, of 50 K. We show that all of the calculated properties are underestimated when calculated under these assumptions. Taken together, the effects of opacity, outflow emission at low velocities confused with ambient cloud emission, and emission below the sensitivities of the observations increase outflow masses and dynamical properties by an order of magnitude, on average, and factors of 50-90 in the most extreme cases. Different (and non-uniform) excitation temperatures, inclination effects, and dissociation of molecular gas will all work to further increase outflow properties. Molecular outflows are thus almost certainly more massive and energetic than commonly reported. Additionally, outflow properties are lower, on average, by almost an order of magnitude when calculated from the (CO)-C-12 (3-2) maps compared to the (CO)-C-12 (2-1) maps, even after accounting for different opacities, map sensitivities, and possible excitation temperature variations. It has recently been argued in the literature that the (CO)-C-12 (3-2) line is subthermally excited in outflows, and our results support this finding. C1 [Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dunham, Michael M.; Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Mardones, Diego] Univ Chile, Dept Astron, Santiago, Chile. [Lee, Jeong-Eun] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Gyeonggi, South Korea. [Matthews, Brenda C.] Natl Res Council Canada, Herzberg Astron & Astrophys, Victoria, BC V9E 2E7, Canada. [Stutz, Amelia M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Dunham, MM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM mdunham@cfa.harvard.edu RI Lee , Jeong-Eun/E-2387-2013; Mardones, Diego/I-5719-2016; OI Williams, Jonathan/0000-0001-5058-695X; Stutz, Amelia/0000-0003-2300-8200 FU National Aeronautics and Space Administration; National Science Foundation; NASA; Canadian Space Agency; SMA; NSF [AST-0845619]; Deutsche Forschungsgemeinschaft [1573] FX The authors express their gratitude to Stella Offner, Adele Plunkett, Xuepeng Chen, and Neal Evans for helpful discussions and/or for commenting on drafts of this manuscript. We also thank Neal Evans for assistance with obtaining APEX data, and the anonymous referee for a set of comments that have improved the quality of this publication. We gratefully acknowledge the assistance provided by the staff of the CSO in obtaining some of the observations presented here. This work is based on data obtained with the following facilities: the Atacama Pathfinder Experiment (APEX), a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory; the Caltech Submillimeter Observatory (CSO), which is operated by the California Institute of Technology under cooperative agreement with the National Science Foundation (AST-0838261); The James Clark Maxwell Telescope (JCMT), which is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the National Research Council of Canada, and (until 2013 March 31) the Netherlands Organisation for Scientific Research. This publication makes use of data products from the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. These data were provided by the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This research has made use of NASA's Astrophysics Data System (ADS) Abstract Service, the IDL Astronomy Library hosted by the NASA Goddard Space Flight Center, the SIMBAD database operated at CDS, Strasbourg, France, and the facilities of the Canadian Astronomy Data Center (CADC) operated by the National Research Council of Canada with the support of the Canadian Space Agency. M. M. D. acknowledges support as an SMA postdoctoral fellow. M. M. D. and H. G. A. acknowledge support from the NSF through grant AST-0845619 to H. G. A. The work of A. M. S. was supported by the Deutsche Forschungsgemeinschaft priority program 1573 (Physics of the Inter-stellar Medium). NR 259 TC 27 Z9 27 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 29 DI 10.1088/0004-637X/783/1/29 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600029 ER PT J AU Geller, MJ Hwang, HS Diaferio, A Kurtz, MJ Coe, D Rines, KJ AF Geller, Margaret J. Hwang, Ho Seong Diaferio, Antonaldo Kurtz, Michael J. Coe, Dan Rines, Kenneth J. TI A REDSHIFT SURVEY OF THE STRONG-LENSING CLUSTER ABELL 383 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: clusters: individual (Abell 3833); galaxies: distances and redshifts; galaxies:kinematics and dynamics; gravitational lensing: weak ID LUMINOUS GALAXY CLUSTERS; DARK-MATTER HALOES; DIGITAL SKY SURVEY; MASS PROFILES; DENSITY PROFILES; INFALL PATTERNS; OUTER REGIONS; SDSS-III; VELOCITY; CONSTRAINTS AB Abell 383 is a famous rich cluster (z = 0.1887) imaged extensively as a basis for intensive strong-and weak-lensing studies. Nonetheless, there are few spectroscopic observations. We enable dynamical analyses by measuring 2360 new redshifts for galaxies with r(Petro) <= 20.5 and within 50' of the Brightest Cluster Galaxy (BCG; R. A.(2000) = 42 degrees.014125, decl.(2000) = -03 degrees.529228). We apply the caustic technique to identify 275 cluster members within 7h(-1) Mpc of the hierarchical cluster center. The BCG lies within -11 +/- 110 km s(-1) and 21 +/- 56 h(-1) kpc of the hierarchical cluster center; the velocity dispersion profile of the BCG appears to be an extension of the velocity dispersion profile based on cluster members. The distribution of cluster members on the sky corresponds impressively with the weak-lensing contours of Okabe et al. especially when the impact of foreground and background structure is included. The values of R-200 = 1.22 +/- 0.01 h(-1) Mpc and M-200 = (5.07 +/- 0.09) x 10(14) h(-1)M(circle dot) obtained by application of the caustic technique agree well with recent completely independent lensing measures. The caustic estimate extends direct measurement of the cluster mass profile to a radius of similar to 5 h(-1) Mpc. C1 [Geller, Margaret J.; Hwang, Ho Seong; Kurtz, Michael J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Diaferio, Antonaldo] Univ Torino, Dipartimento Fis, I-10125 Turin, Italy. [Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Coe, Dan] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Rines, Kenneth J.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. RP Geller, MJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mgeller@cfa.harvard.edu; hhwang@cfa.harvard.edu; diaferio@ph.unito.it; mkurtz@cfa.harvard.edu; DCoe@STScI.edu; kenneth.rines@wwu.edu FU The Smithsonian Institution; INFN grant Indark; University of Torino [TO_Call_2012_0011]; Cottrell College Science Award from the Research Corporation FX We thank Andrew Newman for providing his unpublished redshifts and we thank Graham Smith for providing a coordinate for the position of the secondary peak in the Subaru weak-lensing map. Discussions with Ian Dell'Antonio clarified many issues in the application of weak gravitational lensing. We also profited from valuable comments by Adi Zitrin and Scott Kenyon. Perry Berlind and Michael Calkins masterfully operated the Hectospec on the MMT and Susan Tokarz efficiently reduced the data. The Smithsonian Institution supports the research of M.J.G., H. S. H., and M.J.K. A. D. acknowledges partial support from the INFN grant Indark and from the grand Progetti di Ateneo TO_Call_2012_0011 "Marco Polo" of the University of Torino. K. R. is partially supported by a Cottrell College Science Award from the Research Corporation. NR 53 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 52 DI 10.1088/0004-637X/783/1/52 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600052 ER PT J AU Goulding, AD Forman, WR Hickox, RC Jones, C Murray, SS Paggi, A Ashby, MLN Coil, AL Cooper, MC Huang, JS Kraft, R Newman, JA Weiner, BJ Willner, SP AF Goulding, A. D. Forman, W. R. Hickox, R. C. Jones, C. Murray, S. S. Paggi, A. Ashby, M. L. N. Coil, A. L. Cooper, M. C. Huang, J. -S. Kraft, R. Newman, J. A. Weiner, B. J. Willner, S. P. TI TRACING THE EVOLUTION OF ACTIVE GALACTIC NUCLEI HOST GALAXIES OVER THE LAST 9 Gyr OF COSMIC TIME SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: statistics; infrared: galaxies; radio continuum: galaxies; surveys; X-rays: galaxies ID DIGITAL-SKY-SURVEY; STAR-FORMING GALAXIES; EXTENDED GROTH STRIP; SIMILAR-TO 1; QUASAR LUMINOSITY FUNCTION; SUPERMASSIVE BLACK-HOLES; RAY SELECTED AGN; SPECTROSCOPIC TARGET SELECTION; COLOR-MAGNITUDE RELATION; SPITZER-SPACE-TELESCOPE AB We present the results of a combined galaxy population analysis for the host galaxies of active galactic nuclei (AGN) identified at 0 < z < 1.4 within the Sloan Digital Sky Survey, Bootes, and DEEP2 surveys. We identified AGN in a uniform and unbiased manner at X-ray, infrared, and radio wavelengths. Supermassive black holes undergoing radiatively efficient accretion (detected as X-ray and/or infrared AGN) appear to be hosted in a separate and distinct galaxy population than AGN undergoing powerful mechanically dominated accretion (radio AGN). Consistent with some previous studies, radiatively efficient AGN appear to be preferentially hosted in modest star-forming galaxies, with little dependence on AGN or galaxy luminosity. AGN exhibiting radio-emitting jets due to mechanically dominated accretion are almost exclusively observed in massive, passive galaxies. Crucially, we now provide strong evidence that the observed host-galaxy trends are independent of redshift. In particular, these different accretion-mode AGN have remained as separate galaxy populations throughout the last 9 Gyr. Furthermore, it appears that galaxies hosting AGN have evolved along the same path as galaxies that are not hosting AGN with little evidence for distinctly separate evolution. C1 [Goulding, A. D.; Jones, C.; Murray, S. S.; Paggi, A.; Ashby, M. L. N.; Kraft, R.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Coil, A. L.] Univ Calif San Diego, Ctr Astrophys & Space Sci, Dept Phys, San Diego, CA 92093 USA. [Cooper, M. C.] Univ Calif Irvine, Ctr Galaxy Evolut, Dept Phys & Astron, Irvine, CA 92697 USA. [Newman, J. A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Weiner, B. J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Goulding, AD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM agoulding@cfa.harvard.edu RI Paggi, Alessandro/C-1219-2017; OI Paggi, Alessandro/0000-0002-5646-2410; Forman, William/0000-0002-9478-1682 FU NASA [AR1-12007X]; National Aeronautics and Space Administration; NASA; 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 insightful comments that allowed us to improve and clarify aspects of the manuscript. The authors acknowledge support from NASA grant AR1-12007X. We are grateful to J. Donley for kindly providing a set of star-forming infrared spectral energy distribution templates and associated photometry measurements. We also acknowledge enlightening conversations with W. Joye. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This work is also based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Furthermore, we make use of data from the Sloan Digital Sky Survey, which is managed by the Astrophysical Research Consortium for the Participating Institutions and funding 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. Finally, we acknowledge use of NASA's astrophysics data system. NR 153 TC 15 Z9 15 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 40 DI 10.1088/0004-637X/783/1/40 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600040 ER PT J AU Jimenez-Vicente, J Mediavilla, E Kochanek, CS Munoz, JA Motta, V Falco, E Mosquera, AM AF Jimenez-Vicente, J. Mediavilla, E. Kochanek, C. S. Munoz, J. A. Motta, V. Falco, E. Mosquera, A. M. TI THE AVERAGE SIZE AND TEMPERATURE PROFILE OF QUASAR ACCRETION DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; gravitational lensing: micro; quasars: general ID GRAVITATIONALLY LENSED QUASAR; BROAD EMISSION-LINES; X-RAY; OBSERVATIONAL APPEARANCE; MICROLENSING EVIDENCE; QSO 2237+0305; BLACK-HOLES; FE-II; EXTINCTION; GALAXIES AB We use multi-wavelength microlensing measurements of a sample of 10 image pairs from 8 lensed quasars to study the structure of their accretion disks. By using spectroscopy or narrowband photometry, we have been able to remove contamination from the weakly microlensed broad emission lines, extinction, and any uncertainties in the large-scale macro magnification of the lens model. We determine a maximum likelihood estimate for the exponent of the size versus wavelength scaling (r(s) proportional to lambda(p), corresponding to a disk temperature profile of T proportional to r(-1/p)) of p = 0.75(-0.2)(+0.2) and a Bayesian estimate of p = 0.8 +/- 0.2, which are significantly smaller than the prediction of the thin disk theory (p = 4/3). We have also obtained a maximum likelihood estimate for the average quasar accretion disk size of r(s) = 4.5(-1.2)(+1.5) lt-day at a rest frame wavelength of lambda = 1026 angstrom for microlenses with a mean mass of M = 1 M-circle dot, in agreement with previous results, and larger than expected from thin disk theory. C1 [Jimenez-Vicente, J.] Univ Granada, Dept Fis Teor & Cosmos, E-18071 Granada, Spain. [Jimenez-Vicente, J.] Univ Granada, Inst Carlos Fis Teor & Computac, E-18071 Granada, Spain. [Mediavilla, E.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Mediavilla, E.] Univ La Laguna, Dept Astrofis, E-38200 Tenerife, Spain. [Kochanek, C. S.; Mosquera, A. M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Kochanek, C. S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Munoz, J. A.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. [Motta, V.] Univ Valparaiso, Dept Fis & Astron, Valparaiso 2360102, Chile. [Falco, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jimenez-Vicente, J (reprint author), Univ Granada, Dept Fis Teor & Cosmos, Campus Fuentenueva, E-18071 Granada, Spain. RI Jimenez-Vicente, Jorge/K-1209-2014 OI Jimenez-Vicente, Jorge/0000-0001-7798-3453 FU Spanish Ministerio de Educacion y Ciencia [AYA2011-24728, AYA2007-67342-C03-01/03, AYA2010-21741-C03/02]; Junta de Andalucia through the FQM-108 project; Generalitat Valenciana [PROMETEO/2009/64]; NSF [AST-1009756]; FONDECYT [1120741] FX We gratefully acknowledge the anonymous referee for useful suggestions that improved the presentation of this work. This research was supported by the Spanish Ministerio de Educacion y Ciencia with the grants AYA2011-24728, AYA2007-67342-C03-01/03, and AYA2010-21741-C03/02. J.J.V. is also supported by the Junta de Andalucia through the FQM-108 project. J.A.M. is also supported by the Generalitat Valenciana with the grant PROMETEO/2009/64. C. S. K. is supported by NSF grant AST-1009756. V. M. gratefully acknowledges support from FONDECYT 1120741. NR 44 TC 17 Z9 17 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 47 DI 10.1088/0004-637X/783/1/47 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600047 ER PT J AU Rawle, TD Egami, E Bussmann, RS Gurwell, M Ivison, RJ Boone, F Combes, F Danielson, ALR Rex, M Richard, J Smail, I Swinbank, AM Altieri, B Blain, AW Clement, B Dessauges-Zavadsky, M Edge, AC Fazio, GG Jones, T Kneib, JP Omont, A Perez-Gonzalez, PG Schaerer, D Valtchanov, I van der Werf, PP Walth, G Zamojski, M Zemcov, M AF Rawle, T. D. Egami, E. Bussmann, R. S. Gurwell, M. Ivison, R. J. Boone, F. Combes, F. Danielson, A. L. R. Rex, M. Richard, J. Smail, I. Swinbank, A. M. Altieri, B. Blain, A. W. Clement, B. Dessauges-Zavadsky, M. Edge, A. C. Fazio, G. G. Jones, T. Kneib, J. -P. Omont, A. Perez-Gonzalez, P. G. Schaerer, D. Valtchanov, I. van der Werf, P. P. Walth, G. Zamojski, M. Zemcov, M. TI [C II] AND (CO)-C-12(1-0) EMISSION MAPS IN HLSJ091828.6+514223: A STRONGLY LENSED INTERACTING SYSTEM AT z=5.24 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: star formation; submillimeter: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; LYMAN BREAK GALAXY; DEEP-FIELD-SOUTH; SUBMILLIMETER GALAXIES; MOLECULAR GAS; HIGH-REDSHIFT; INTERSTELLAR-MEDIUM; HERSCHEL-SPIRE AB We present Submillimeter Array [ C II] 158 mu m and Karl G. Jansky Very Large Array (CO)-C-12(1-0) line emission maps for the bright, lensed, submillimeter source at z = 5.2430 behind A 773: HLSJ091828.6+514223 (HLS0918). We combine these measurements with previously reported line profiles, including multiple 12CO rotational transitions, [C II], water, and [N II], providing some of the best constraints on the properties of the interstellarmedium in a galaxy at z > 5. HLS0918 has a total far-infrared (FIR) luminosity L-FIR(8-1000 mu m) = (1.6 +/- 0.1) x 1014 L-circle dot mu(-1), where the total magnification mu(total) = 8.9 +/- 1.9, via a new lens model from the [C II] and continuum maps. Despite a HyLIRG luminosity, the FIR continuum shape resembles that of a local LIRG. We simultaneously fit all of the observed spectral line profiles, finding four components that correspond cleanly to discrete spatial structures identified in the maps. The two most redshifted spectral components occupy the nucleus of a massive galaxy, with a source-plane separation < 1 kpc. The reddest dominates the continuum map (demagnified L-FIR,L- (component) = (1.1 +/- 0.2) x10(13) L-circle dot) and excites strong water emission in both nuclear components via a powerful FIR radiation field from the intense star formation. A third star-forming component is most likely a region of a merging companion (Delta V similar to 500 kms(-1)) exhibiting generally similar gas properties. The bluest component originates from a spatially distinct region and photodissociation region analysis suggests that it is lower density, cooler, and forming stars less vigorously than the other components. Strikingly, it has very strong [N II] emission, which may suggest an ionized, molecular outflow. This comprehensive view of gas properties and morphology in HLS0918 previews the science possible for a large sample of high-redshift galaxies once ALMA attains full sensitivity. C1 [Rawle, T. D.; Altieri, B.; Valtchanov, I.] ESA, ESAC, E-28691 Madrid, Spain. [Rawle, T. D.; Egami, E.; Rex, M.; Clement, B.; Perez-Gonzalez, P. G.; Walth, G.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bussmann, R. S.; Gurwell, M.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ivison, R. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Boone, F.] Univ Toulouse, CNRS, UPS OMP, IRAP, F-310284 Toulouse, France. [Combes, F.] CNRS, LERMA, Observ Paris, F-75014 Paris, France. [Danielson, A. L. R.; Smail, I.; Swinbank, A. M.; Edge, A. C.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Richard, J.] Univ Lyon 1, CRAL, F-69561 St Genis Laval, France. [Blain, A. W.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Dessauges-Zavadsky, M.; Schaerer, D.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [Jones, T.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Kneib, J. -P.] Observ Sauverny, Lab Astrophys EPFL, CH-1290 Versoix, Switzerland. [Omont, A.] CNRS, Inst Astrophys Paris, F-75014 Paris, France. [Omont, A.] UPMC, UMR7095, F-75014 Paris, France. [Perez-Gonzalez, P. G.] Univ Complutense Madrid, Fac CC, Dept Astrofis, E-28040 Madrid, Spain. [Schaerer, D.] CNRS, IRAP, F-31400 Toulouse, France. [van der Werf, P. P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rawle, TD (reprint author), ESA, ESAC, POB 78, E-28691 Madrid, Spain. EM tim.rawle@sciops.esa.int RI Kneib, Jean-Paul/A-7919-2015; Smail, Ian/M-5161-2013; Perez-Gonzalez, Pablo/J-2871-2016; Ivison, R./G-4450-2011; OI Kneib, Jean-Paul/0000-0002-4616-4989; Smail, Ian/0000-0003-3037-257X; Perez-Gonzalez, Pablo/0000-0003-4528-5639; Ivison, R./0000-0001-5118-1313; Edge, Alastair/0000-0002-3398-6916 FU European Space Agency (ESA) Research Fellowship at the European Space Astronomy Centre (ESAC), in Madrid, Spain; STFC; Leverhulme Fellowship; ERC Advanced Investigator program [DUSTYGAL 321334]; Royal Society/Wolfson Merit Award; Smithsonian Institution; Academia Sinica; INSU/CNRS (France); MPG (Germany); IGN (Spain); NASA through JPL/Caltech FX T.D.R. is supported by a European Space Agency (ESA) Research Fellowship at the European Space Astronomy Centre (ESAC), in Madrid, Spain. I. R. S. acknowledges support from STFC, a Leverhulme Fellowship, the ERC Advanced Investigator program DUSTYGAL 321334, and a Royal Society/Wolfson Merit Award.; The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This work also includes observations carried out with the Karl G. Jansky Very Large Array (VLA): The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Additionally, based on observations carried out with the IRAM Plateau de Bure Interferometer and the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).; This work follows on from observations made with the Herschel Space Observatory, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. We would also like to thank the HSC and NHSC consortia for support with data reduction. NR 96 TC 38 Z9 38 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 59 DI 10.1088/0004-637X/783/1/59 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600059 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 (vol 774, 54, 2013) SO ASTROPHYSICAL JOURNAL LA English DT Correction 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, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM rsanchis86@gmail.com; sar@mit.edu; jwinn@mit.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600064 ER PT J AU Schlieder, JE Bonnefoy, M Herbst, TM Lepine, S Berger, E Henning, T Skemer, A Chauvin, G Rice, E Biller, B Girard, JHV Lagrange, AM Hinz, P Defrere, D Bergfors, C Brandner, W Lacour, S Skrutskie, M Leisenring, J AF Schlieder, Joshua E. Bonnefoy, Mickael Herbst, T. M. Lepine, Sebastien Berger, Edo Henning, Thomas Skemer, Andrew Chauvin, Gael Rice, Emily Biller, Beth Girard, Julien H. V. Lagrange, Anne-Marie Hinz, Philip Defrere, Denis Bergfors, Carolina Brandner, Wolfgang Lacour, Sylvestre Skrutskie, Michael Leisenring, Jarron TI CHARACTERIZATION OF THE BENCHMARK BINARY NLTT 33370 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; stars: individual (NLTT 33370); stars: late-type ID LOW-MASS STARS; YOUNG BROWN DWARFS; STELLAR KINEMATIC GROUPS; NEAR-INFRARED SPECTRA; URSA-MAJOR GROUP; INTEGRAL FIELD SPECTROSCOPY; EXTRASOLAR GIANT PLANETS; ORION NEBULA CLUSTER; DORADUS MOVING GROUP; LITHIUM DEPLETION AB We confirm the binary nature of the nearby, very low mass (VLM) system NLTT 33370 with adaptive optics imaging and present resolved near-infrared photometry and integrated light optical and near-infrared spectroscopy to characterize the system. VLT-NaCo and LBTI-LMIRCam images show significant orbital motion between 2013 February and 2013 April. Optical spectra reveal weak, gravity-sensitive alkali lines and strong lithium 6708 angstrom absorption that indicate the system is younger than field age. VLT-SINFONI near-IR spectra also show weak, gravity-sensitive features and spectral morphology that is consistent with other young VLM dwarfs. We combine the constraints from all age diagnostics to estimate a system age of similar to 30-200 Myr. The 1.2-4.7 mu m spectral energy distribution of the components point toward T-eff = 3200 +/- 500 K and T-eff = 3100 +/- 500 K for NLTT 33370 A and B, respectively. The observed spectra, derived temperatures, and estimated age combine to constrain the component spectral types to the range M6-M8. Evolutionary models predict masses of 97(-48)(+41) M-Jup and 91(-44)(+41) M-Jup from the estimated luminosities of the components. KPNO-Phoenix spectra allow us to estimate the systemic radial velocity of the binary. The Galactic kinematics of NLTT 33370AB are broadly consistent with other young stars in the solar neighborhood. However, definitive membership in a young, kinematic group cannot be assigned at this time and further follow-up observations are necessary to fully constrain the system's kinematics. The proximity, age, and late-spectral type of this binary make it very novel and an ideal target for rapid, complete orbit determination. The system is one of only a few model calibration benchmarks at young ages and VLMs. C1 [Schlieder, Joshua E.; Bonnefoy, Mickael; Herbst, T. M.; Henning, Thomas; Biller, Beth; Bergfors, Carolina; Brandner, Wolfgang] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Bonnefoy, Mickael; Chauvin, Gael; Lagrange, Anne-Marie] UJF Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France. [Lepine, Sebastien; Rice, Emily] Amer Museum Nat Hist, Dept Astrophys, Div Phys Sci, New York, NY 10024 USA. [Lepine, Sebastien] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Berger, Edo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Skemer, Andrew; Hinz, Philip; Defrere, Denis; Leisenring, Jarron] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA. [Chauvin, Gael; Rice, Emily] CUNY Coll Staten Isl, Dept Engn Sci & Phys, Staten Isl, NY 10314 USA. [Biller, Beth] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Girard, Julien H. V.] European So Observ, Santiago 19, Chile. [Bergfors, Carolina] Univ London Univ Coll, Dept Phys & Astron, London WC1E 6BT, England. [Lacour, Sylvestre] Univ Paris 06, CNRS, LESIA, Observ Paris, F-92195 Meudon, France. [Lacour, Sylvestre] Univ Denis Diderot Paris 7, F-92195 Meudon, France. [Skrutskie, Michael] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Leisenring, Jarron] ETH, Inst Astron, CH-8093 Zurich, Switzerland. RP Schlieder, JE (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM schlieder@mpia-hd.mpg.de OI Biller, Beth/0000-0003-4614-7035; Skemer, Andrew/0000-0001-6098-3924 FU German Science Foundation [SFB 881]; National Science Foundation [AST-1008361]; French "Agence Nationale de la Recherche" [ANR10-BLANC0504-01]; "Programme Nationale de Physique Stellaire" (PNPS) of CNRS (INSU); National Aeronautics and Space Administration FX We thank the anonymous referee for a thorough and constructive review that improved this manuscript. We thank the ESO Paranal staff for conducting the service mode observations presented here. We also thank the LBTI/LMIRCam instrument team for providing support during those observations. The authors are grateful for the support of the KPNO staff, particularly Dick Joyce, Dave Summers, and Kristin Reetz. We are grateful to Chad Bender for making available his software for the two-dimensional cross-correlation of stellar spectra. J.E.S. thanks Roland Gredel, Niall Deacon, Eddie Schlafly, and Taisiya Kopytova for helpful conversations regarding the observations and analyses presented here. The research of Thomas Henning on moving groups and the low-mass stellar population in the solar neighborhood is partly supported by the German Science Foundation SFB 881 "The Milky Way System." E. B. acknowledges support for this work from the National Science Foundation through Grant AST-1008361. The research leading to these results has received funding from the French "Agence Nationale de la Recherche" through project grant ANR10-BLANC0504-01, the "Programme Nationale de Physique Stellaire" (PNPS) of CNRS (INSU). This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. 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. Based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). This research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. NR 96 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 27 DI 10.1088/0004-637X/783/1/27 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600027 ER PT J AU Slane, P Lee, SH Ellison, DC Patnaude, DJ Hughes, JP Eriksen, KA Castro, D Nagataki, S AF Slane, P. Lee, S. -H. Ellison, D. C. Patnaude, D. J. Hughes, J. P. Eriksen, K. A. Castro, D. Nagataki, S. TI A CR-HYDRO-NEI MODEL OF THE STRUCTURE AND BROADBAND EMISSION FROM TYCHO'S SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; ISM: individual objects (Tycho's SNR); ISM: supernova remnants; shock waves ID GAMMA-RAY EMISSION; EFFICIENT PARTICLE-ACCELERATION; DIFFUSIVE SHOCK ACCELERATION; FERMI-LAT OBSERVATIONS; XMM-NEWTON OBSERVATION; RX J1713.7-3946; MOLECULAR CLOUDS; COSMIC-RAYS; X-RAYS; IA AB Tycho's supernova remnant (SNR) is well-established as a source of particle acceleration to very high energies. Constraints from numerous studies indicate that the observed gamma-ray emission results primarily from hadronic processes, providing direct evidence of highly relativistic ions that have been accelerated by the SNR. Here we present an investigation of the dynamical and spectral evolution of Tycho's SNR by carrying out hydrodynamical simulations that include diffusive shock acceleration of particles in the amplified magnetic field at the forward shock of the SNR. Our simulations provide a consistent view of the shock positions, the nonthermal emission, the thermal X-ray emission from the forward shock, and the brightness profiles of the radio and X-ray emission. We compare these with the observed properties of Tycho to determine the density of the ambient material, the particle acceleration efficiency and maximum energy, the accelerated electron-to-proton ratio, and the properties of the shocked gas downstream of the expanding SNR shell. We find that evolution of a typical Type Ia supernova in a low ambient density (n(0) similar to 0.3 cm(-3)), with an upstream magnetic field of similar to 5 mu G, and with similar to 16% of the SNR kinetic energy being converted into relativistic electrons and ions through diffusive shock acceleration, reproduces the observed properties of Tycho. Under such a scenario, the bulk of observed gamma-ray emission at high energies is produced by pi(0)-decay resulting from the collisions of energetic hadrons, while inverse-Compton emission is significant at lower energies, comprising roughly half of the flux between 1 and 10 GeV. C1 [Slane, P.; Patnaude, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lee, S. -H.; Nagataki, S.] RIKEN, Astrophys Big Bang Lab, Wako, Saitama 3510198, Japan. [Ellison, D. C.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Hughes, J. P.; Eriksen, K. A.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Eriksen, K. A.] Los Alamos Natl Lab, XTD IDA, Los Alamos, NM 87545 USA. [Castro, D.] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM slane@cfa.harvard.edu; shiu-hang.lee@riken.jp; don_ellison@ncsu.edu; dpatnaude@cfa.harvard.edu; jph@physics.rutgers.edu; keriksen@lanl.gov; castro@mit.edu; shigehiro.nagataki@riken.jp FU NASA [NAS8-03060, NNX11AE03G, NNX08AZ86G]; Chandra grant [GO9-0078X] FX The authors acknowledge important discussions with Brian Williams and Carles Badenes concerning this work. P. S. acknowledges support from NASA Contract NAS8-03060. D. C. E. acknowledges support from NASA grant NNX11AE03G. J.P.H. acknowledges support from Chandra grant GO9-0078X and NASA Suzaku grant NNX08AZ86G. NR 54 TC 16 Z9 16 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2014 VL 783 IS 1 AR 33 DI 10.1088/0004-637X/783/1/33 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600033 ER PT J AU Vargas, CJ Bish, H Acquaviva, V Gawiser, E Finkelstein, SL Ciardullo, R Ashby, MLN Feldmeier, J Ferguson, H Gronwall, C Guaita, L Hagen, A Koekemoer, A Kurczynski, P Newman, JA Padilla, N AF Vargas, Carlos J. Bish, Hannah Acquaviva, Viviana Gawiser, Eric Finkelstein, Steven L. Ciardullo, Robin Ashby, Matthew L. N. Feldmeier, John Ferguson, Henry Gronwall, Caryl Guaita, Lucia Hagen, Alex Koekemoer, Anton Kurczynski, Peter Newman, Jeffrey A. Padilla, Nelson TI TO STACK OR NOT TO STACK: SPECTRAL ENERGY DISTRIBUTION PROPERTIES OF Ly alpha-EMITTING GALAXIES AT z=2.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift ID EXTRAGALACTIC LEGACY SURVEY; FRAME ULTRAVIOLET-SPECTRA; POST-STARBURST GALAXIES; HUBBLE DEEP FIELD; GOODS-SOUTH FIELD; TP-AGB STARS; STELLAR POPULATIONS; FORMING GALAXIES; SPACE-TELESCOPE; SURVEY DESIGN AB We use the Cosmic Assembly Near-Infrared Deep Extragalactic Legacy Survey (CANDELS) GOODS-S multi-wavelength catalog to identify counterparts for 20 Ly alpha emitting (LAE) galaxies at z = 2.1. We build several types of stacked spectral energy distributions (SEDs) of these objects. We combine photometry to form average and median flux-stacked SEDs, and postage-stamp images to form average and median image-stacked SEDs. We also introduce scaled flux stacks that eliminate the influence of variation in overall brightness. We use the SED fitting code SpeedyMC to constrain the physical properties of individual objects and stacks. Our LAEs at z = 2.1 have stellar masses ranging from 2 x 10(7) M-circle dot to 8 x 10(9) M-circle dot (median = 3 x 10(8) M-circle dot), ages ranging from 4 Myr to 500 Myr (median = 100 Myr), and E(B - V) between 0.02 and 0.24 (median = 0.12). Although still low, this represents significantly more dust reddening than has been reported for LAEs at higher redshifts. We do not observe strong correlations between Ly alpha equivalent width (EW) and age or E(B - V). The Ly alpha radiative transfer (q) factors of our sample are predominantly close to one and do not correlate strongly with EW or E(B - V). The absence of strong correlations with EW or q implies that Ly alpha radiative transfer is highly anisotropic and/or prevents Ly alpha photons from scattering in dusty regions. The SED parameters of the flux stacks match the average and median values of the individual objects, with the flux-scaled median SED performing best with uncertainties reduced by a factor of two. Median image-stacked SEDs provide a poor representation of the median individual object, and none of the stacking methods capture the large dispersion of LAE properties. C1 [Vargas, Carlos J.; Bish, Hannah; Gawiser, Eric; Kurczynski, Peter] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Vargas, Carlos J.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88001 USA. [Acquaviva, Viviana] CUNY, New York City Coll Technol, Dept Phys, Brooklyn, NY 11201 USA. [Finkelstein, Steven L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Ciardullo, Robin; Gronwall, Caryl; Hagen, Alex] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Ciardullo, Robin; Gronwall, Caryl; Hagen, Alex] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Ashby, Matthew L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Feldmeier, John] Youngstown State Univ, Dept Phys & Astron, Youngstown, OH 44555 USA. [Ferguson, Henry] Space Telescope Sci Inst, Baltimore, MD USA. [Guaita, Lucia] Stockholm Univ, Oskar Klein Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Padilla, Nelson] Catholic Univ Chile, Dept Astron & Astrophys, Santiago, Chile. RP Vargas, CJ (reprint author), Rutgers State Univ, Dept Phys & Astron, POB 849, Piscataway, NJ 08854 USA. OI Koekemoer, Anton/0000-0002-6610-2048 FU NASA [NAS5-26555]; NASA; NASA through a grant from the Space Telescope Science Institute [12060.57, 12445.56]; Eberly College of Science; Office of the Senior Vice President for Research at the Pennsylvania State University; National Science Foundation [AST-1055919]; [GO-9352]; [GO-9425]; [GO-9583]; [GO-9728]; [GO-10189]; [GO-10339]; [GO-10340]; [GO-11359]; [GO-12060]; [GO-12061]; [LP168.A-0485] FX We would like to thank both the CANDELS and MUSYC collaborations for making this work possible. We would also like to thank the anonymous referee for helpful comments that greatly improved the quality of the paper. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. These observations are associated with programs GO-9352, GO-9425, GO-9583, GO-9728, GO-10189, GO-10339, GO-10340, GO-11359, GO-12060, and GO-12061. Observations have been carried out using the Very Large Telescope at the ESO Paranal Observatory under Program ID(s): LP168.A-0485. This work is also based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for Program numbers 12060.57 and 12445.56 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. The Institute for Gravitation and the Cosmos is supported by the Eberly College of Science and the Office of the Senior Vice President for Research at the Pennsylvania State University. This material is based on work supported by the National Science Foundation under CAREER grant AST-1055919 awarded to Eric Gawiser. This research has made use of NASA's Astrophysics Data System. NR 51 TC 17 Z9 17 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 MAR 1 PY 2014 VL 783 IS 1 AR 26 DI 10.1088/0004-637X/783/1/26 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF7UF UT WOS:000334919600026 ER PT J AU Melott, AL Bambach, RK AF Melott, Adrian L. Bambach, Richard K. TI Analysis of periodicity of extinction using the 2012 geological timescale SO PALEOBIOLOGY LA English DT Article ID LARGE IGNEOUS PROVINCES; MARINE FOSSIL RECORD; MASS EXTINCTIONS; LATE ORDOVICIAN; OCEAN ACIDIFICATION; GENERAL TRENDS; BIODIVERSITY; ORIGINATION; DIVERSITY; EVOLUTION AB Analysis of two independent data sets with increased taxonomic resolution (genera rather than families) using the revised 2012 timescale reveals that an extinction periodicity first detected by Raup and Sepkoski (1984) for only the post-Paleozoic actually runs through the entire Phanerozoic. Although there is not a local peak of extinction every 27 Myr, an excess of the fraction of genus extinction by interval follows a 27-Myr timing interval and differs from a random distribution at the p similar to 0.02 level. A 27-Myr periodicity in the spectrum of interval lengths no longer appears, removing the question of a possible artifact arising from it. Using a method originally developed in Bambach (2006) we identify 19 intervals of marked extinction intensity, including mass extinctions, spanning the last 470 Myr (and with another six present in the Cambrian) and find that ten of the 19 lie within +/- 3 Myr of the maxima in the spacing of the 27-Myr periodicity, which differs from a random distribution at the p = 0.004 level. These 19 intervals of marked extinction intensity also preferentially occur during decreasing diversity phases of a well-known 62-Myr periodicity in diversity (16 of 19, p = 0.002). Both periodicities appear to enhance the likelihood of increased severity of extinction, but the cause of neither periodicity is known. Variation in the strength of the many suggested causes of extinction coupled to the variation in combined effect of the two different periodidties as they shift in and out of phase is surely one of the reasons that definitive comparative study of the causes of major extinction events is so elusive. C1 [Melott, Adrian L.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Bambach, Richard K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Melott, AL (reprint author), Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. EM melott@ku.edu; richard.bambach@verizon.net NR 75 TC 9 Z9 9 U1 4 U2 27 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0094-8373 EI 1938-5331 J9 PALEOBIOLOGY JI Paleobiology PD SPR PY 2014 VL 40 IS 2 BP 177 EP 196 DI 10.1666/13047 PG 20 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA AF1MR UT WOS:000334478500003 ER PT J AU Sepulchre, P Arsouze, T Donnadieu, Y Dutay, JC Jaramillo, C Le Bras, J Martin, E Montes, C Waite, AJ AF Sepulchre, P. Arsouze, T. Donnadieu, Y. Dutay, J. -C. Jaramillo, C. Le Bras, J. Martin, E. Montes, C. Waite, A. J. TI Consequences of shoaling of the Central American Seaway determined from modeling Nd isotopes SO PALEOCEANOGRAPHY LA English DT Article DE Panama closure; Central American Seaway; climate modelling; Miocene; epsilon neodymium; Nd isotopes ID GENERAL-CIRCULATION MODEL; MERIDIONAL OVERTURNING CIRCULATION; NORTHERN-HEMISPHERE GLACIATION; OCEAN CIRCULATION; SOUTH-AMERICA; PANAMA SEAWAY; BIOTIC INTERCHANGE; ATLANTIC-OCEAN; WATER MASSES; CLOSURE AB The Central American Seaway played a pivotal role in shaping global climate throughout the late Cenozoic. Recent geological surveys have provided new constraints on timing of the seaway shoaling, while neodymium isotopic (epsilon(Nd)) data measured on fossil teeth, debris, and ferromanganese crusts have helped define the history of water masses in the region. Here we provide the first 3-D simulations of epsilon(Nd) responses to the shoaling seaway. Our model suggests that a narrow and shallow seaway is sufficient to affect interoceanic circulation, that inflow/outflow balance between the Caribbean and the Antilles responds nonlinearly to sill depth, and that a seaway narrower than 400km is consistent with an active Atlantic meridional overturning circulation during the late Miocene. Simulated epsilon(Nd) values in the Caribbean confirm that inputs from radiogenic Pacific waters in the Caribbean decrease as the seaway shoals. Despite model limitations, a comparison between our results and epsilon(Nd) values recorded in the Caribbean helps constrain the depth of the Central American Seaway through time, and we infer that a depth between 50 and 200m could have been reached 10Ma ago. Key Points Model/data comparison of epsilon Nd suggests a shallow CAS during the Miocene CAS throughflow depends on seaway geometry and atmospheric coupling Ocean circulation responds nonlinearly to CAS shoaling C1 [Sepulchre, P.; Arsouze, T.; Donnadieu, Y.; Dutay, J. -C.; Le Bras, J.] Univ Versailles St Quentin Yvelines, CEA, CNRS, Lab Sci Climat & Environm, Gif Sur Yvette, France. [Jaramillo, C.] Smithsonian Trop Res Inst, Ancon, Panama. [Martin, E.; Waite, A. J.] Univ Florida, Dept Geol Sci, Gainesville, FL USA. [Montes, C.] Univ Los Andes, Bogota, Colombia. RP Sepulchre, P (reprint author), Univ Versailles St Quentin Yvelines, CEA, CNRS, Lab Sci Climat & Environm, Gif Sur Yvette, France. EM pierre.sepulchre@lsce.ipsl.fr RI Donnadieu, Yannick/G-7546-2016; Waite, Amanda/A-1675-2011; OI Donnadieu, Yannick/0000-0002-7315-2684; Waite, Amanda/0000-0002-1863-666X; Montes, Camilo/0000-0002-3553-0787 FU Panama Canal Authority [SAA-199520-KRP]; Mark Tupper; Senacyt [SUM-07-001, EST010-080 A]; U.S. National Science Foundation (NSF) [0966884]; NSF [EAR 0824299]; National Geographic; Smithsonian Institution; Ricardo Perez S.A. FX We thank Martin Frank and an anonymous reviewer for their constructive reviews. The authors also thank Olivier Marti for helping design the boundary conditions of the simulations and Didier Swingedouw for fruitful discussion of our results. Figures have been designed with FAST package for Ferret, developed by Patrick Brockmann at LSCE. This project was supported by Panama Canal Authority contract SAA-199520-KRP; Mark Tupper; Senacyt grants SUM-07-001 and EST010-080 A; U.S. National Science Foundation (NSF) grant 0966884 (OISE, EAR, DRL); NSF EAR 0824299; National Geographic; Smithsonian Institution; and Ricardo Perez S.A. NR 70 TC 27 Z9 28 U1 2 U2 30 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0883-8305 EI 1944-9186 J9 PALEOCEANOGRAPHY JI Paleoceanography PD MAR PY 2014 VL 29 IS 3 BP 176 EP 189 DI 10.1002/2013PA002501 PG 14 WC Geosciences, Multidisciplinary; Oceanography; Paleontology SC Geology; Oceanography; Paleontology GA AE9SO UT WOS:000334349800004 ER PT J AU Aleksie, J Antonelli, LA Antoranz, P Babic, A de Almeida, UB Barrio, JA Gonzalez, JB Bednarek, W Berger, K Bernardini, E Biland, A Blanch, O Bock, RK Boller, A Bonnefoy, S Bonnoli, G Tridon, DB Borracci, F Bretz, T Carmona, E Carosi, A Fidalgo, DC Colin, P Colombo, E Contreras, JL Cortina, J Cossio, L Covino, S Da Vela, P Dazzi, F De Angelis, A De Caneva, G Mendez, CD De Lotto, B Doert, M Dominguez, A Prester, DD Dorner, D Doro, M Eisenacher, D Elsaesser, D Farina, E Ferenc, D Fonseca, MV Font, L Fruck, C Lopez, RJG Garczarczyk, M Terrats, DG Gaug, M Giavitto, G Godinovic, N Munoz, AG Gozzini, SR Hadamek, A Hadasch, D Hafner, D Herrero, A Hose, J Hrupec, D Idec, W Kadenius, V Knoetig, ML Krahenbuhl, T Krause, J Kushida, J La Barbera, A Lelas, D Lewandowska, N Lindfors, E Lombardi, S Lopez-Coto, R Lopez, M Lopez-Oramas, A Lorenz, E Lozano, I Makariev, M Mallot, K Maneva, G Mankuzhiyil, N Mannheim, K Maraschi, L Marcote, B Mariotti, M Martiinez, M Masbou, J Mazin, D Meucci, M Miranda, JM Mirzoyan, R Moldoon, J Moralejo, A Munar-Adrover, P Nakajima, D Niedzwiecki, A Nilsson, K Nowak, N Orito, R Overkemping, A Paiano, S Palatiello, M Paneque, D Paoletti, R Paredes, JM Partini, S Persic, M Prada, F PradaMoroni, PG Prandini, E Preziuso, S Puljak, I Reichardt, I Reinthal, R Rhode, W Ribo, M Rico, J Ruegamer, S Saggion, A Saito, K Saito, TY Salvati, M Satalecka, K Scalzotto, V Scapin, V Schultz, C Schweizer, T Shore, SN Sillanpaa, A Sitarek, J Snidaric, I Sobczynska, D Spanier, F Spiro, S Stamatescu, V Stamerra, A Steinke, B Storz, J Sun, S Suric, T Takalo, L Takami, H Tavecchio, F Temnikov, P Terzic, T Tescaro, D Teshima, M Thaele, J Tibolla, O Torres, DF Toyama, T Treves, A Uellenbeck, M Vogler, P Wagner, RM Weitzel, Q Zandanel, F Zanin, R Dauser, T Fortin, P Kadler, M Krauss, F Wilbert, S Wilms, J AF Aleksie, J. Antonelli, L. A. Antoranz, P. Babic, A. de Almeida, U. Barres Barrio, J. A. Becerra Gonzalez, J. Bednarek, W. Berger, K. Bernardini, E. Biland, A. Blanch, O. Bock, R. K. Boller, A. Bonnefoy, S. Bonnoli, G. Tridon, D. Borla Borracci, F. Bretz, T. Carmona, E. Carosi, A. Carreto Fidalgo, D. Colin, P. Colombo, E. Contreras, J. L. Cortina, J. Cossio, L. Covino, S. Da Vela, P. Dazzi, F. De Angelis, A. De Caneva, G. Delgado Mendez, C. De Lotto, B. Doert, M. Dominguez, A. Dominis Prester, D. Dorner, D. Doro, M. Eisenacher, D. Elsaesser, D. Farina, E. Ferenc, D. Fonseca, M. V. Font, L. Fruck, C. Garcia Lopez, R. J. Garczarczyk, M. Terrats, D. Garrido Gaug, M. Giavitto, G. Godinovic, N. Gonzalez Munoz, A. Gozzini, S. R. Hadamek, A. Hadasch, D. Haefner, D. Herrero, A. Hose, J. Hrupec, D. Idec, W. Kadenius, V. Knoetig, M. L. Kraehenbuehl, T. Krause, J. Kushida, J. La Barbera, A. Lelas, D. Lewandowska, N. Lindfors, E. Lombardi, S. Lopez-Coto, R. Lopez, M. Lopez-Oramas, A. Lorenz, E. Lozano, I. Makariev, M. Mallot, K. Maneva, G. Mankuzhiyil, N. Mannheim, K. Maraschi, L. Marcote, B. Mariotti, M. Martinez, M. Masbou, J. Mazin, D. Meucci, M. Miranda, J. M. Mirzoyan, R. Moldon, J. Moralejo, A. Munar-Adrover, P. Nakajima, D. Niedzwiecki, A. Nilsson, K. Nowak, N. Orito, R. Overkemping, A. Paiano, S. Palatiello, M. Paneque, D. Paoletti, R. Paredes, J. M. Partini, S. Persic, M. Prada, F. PradaMoroni, P. G. Prandini, E. Preziuso, S. Puljak, I. Reichardt, I. Reinthal, R. Rhode, W. Ribo, M. Rico, J. Ruegamer, S. Saggion, A. Saito, K. Saito, T. Y. Salvati, M. Satalecka, K. Scalzotto, V. Scapin, V. Schultz, C. Schweizer, T. Shore, S. N. Sillanpaeae, A. Sitarek, J. Snidaric, I. Sobczynska, D. Spanier, F. Spiro, S. Stamatescu, V. Stamerra, A. Steinke, B. Storz, J. Sun, S. Suric, T. Takalo, L. Takami, H. Tavecchio, F. Temnikov, P. Terzic, T. Tescaro, D. Teshima, M. Thaele, J. Tibolla, O. Torres, D. F. Toyama, T. Treves, A. Uellenbeck, M. Vogler, P. Wagner, R. M. Weitzel, Q. Zandanel, F. Zanin, R. Dauser, T. Fortin, P. Kadler, M. Krauss, F. Wilbert, S. Wilms, J. CA MAGIC Collaboration TI Rapid and multiband variability of the TeV bright active nucleus of the galaxy IC 310 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: individual: IC 310; gamma rays: galaxies; X-rays: galaxies ID GAMMA-RAY EMISSION; LARGE-AREA TELESCOPE; EXTRAGALACTIC BACKGROUND LIGHT; PERSEUS CLUSTER; MAGIC TELESCOPES; GALACTIC NUCLEI; RADIO GALAXIES; M87; CATALOG; BLAZARS AB Context. The radio galaxy IC 310 has recently been identified as a gamma-ray emitter based on observations at GeV energies with Fermi-LAT and at very high energies (VHE, E > 100 GeV) with the MAGIC telescopes. Originally classified as a head-tail radio galaxy, the nature of this object is subject of controversy since its nucleus shows blazar-like behavior. Aims. To understand the nature of IC310 and the origin of the VHE emission, we studied the spectral and flux variability of IC 310 from the X-ray band to the VHE gamma-ray regime. Methods. The light curve of IC310 above 300GeV has been measured with the MAGIC telescopes from 2009 October to 2010 February. Contemporaneous Fermi-LAT data (2008-2011) in the 10-500 GeV energy range were also analyzed. In the X-ray regime, archival observations from 2003 to 2007 with XMM-Newton, Chandra, and Swift-XRT in the 0.5-10 keV band were studied. Results. The VHE light curve reveals several high-amplitude and short-duration flares. Day-to-day flux variability is clearly present (>5 sigma). The photon index between 120 GeV and 8 TeV remains at the value Gamma similar to 2.0 during both low and high flux states. The VHE spectral shape does not show significant variability, whereas the flux at 1 TeV changes by a factor of similar to 7. Fermi-LAT detected only eight gamma-ray events in the energy range 10 GeV-500 GeV in three years of observation. The measured photon index of Gamma = 1.3 +/- 0.5 in the Fermi-LAT range is very hard. The X-ray measurements show strong variability in both flux and photon index. The latter varied from 1.76 +/- 0.07 to 2.55 +/- 0.07. Conclusions. The rapid variability measured in gamma-rays and X-rays confirms the blazar-like behavior of IC310. The multi-TeV gamma-ray emission seems to originate from scales of less than 80 Schwarzschild radii (for a black hole mass of 2 x 10(8) M-circle dot) within the compact core of its FR I radio jet with orientation angle 10 degrees-38 degrees. The spectral energy distribution resembles that of an extreme blazar, albeit the luminosity is more than two orders of magnitude lower. C1 [Aleksie, J.; Blanch, O.; Cortina, J.; Giavitto, G.; Gonzalez Munoz, A.; Lopez-Coto, R.; Lopez-Oramas, A.; Martinez, M.; Moralejo, A.; Reichardt, I.; Rico, J.; Sitarek, J.; Stamatescu, V.] IFAE, Bellaterra 08193, Spain. [Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; La Barbera, A.; Lombardi, S.; Maraschi, L.; Salvati, M.; Spiro, S.; Tavecchio, F.] INAF Natl Inst Astrophys, I-00136 Rome, Italy. [Antoranz, P.; Da Vela, P.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Preziuso, S.; Stamerra, A.] Univ Siena, I-53100 Siena, Italy. [Antoranz, P.; Da Vela, P.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Preziuso, S.; Stamerra, A.] INFN Pisa, I-53100 Siena, Italy. [Babic, A.; Dominis Prester, D.; Ferenc, D.; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Suric, T.; Terzic, T.] Univ Rijeka, Croatian MAGIC Consortium, Rudjer Boskov Inst, Zagreb 10000, Croatia. [Babic, A.; Dominis Prester, D.; Ferenc, D.; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Suric, T.; Terzic, T.] Univ Split, Zagreb 10000, Croatia. [de Almeida, U. Barres; Bock, R. K.; Tridon, D. Borla; Borracci, F.; Colin, P.; Fruck, C.; Haefner, D.; Hose, J.; Knoetig, M. L.; Krause, J.; Lorenz, E.; Mazin, D.; Mirzoyan, R.; Nakajima, D.; Nowak, N.; Overkemping, A.; Paneque, D.; Saito, T. Y.; Schweizer, T.; Steinke, B.; Sun, S.; Teshima, M.; Toyama, T.; Wagner, R. M.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Barrio, J. A.; Bonnefoy, S.; Carreto Fidalgo, D.; Contreras, J. L.; Fonseca, M. V.; Lopez, M.; Lozano, I.; Satalecka, K.; Scapin, V.] Univ Complutense, E-28040 Madrid, Spain. [Becerra Gonzalez, J.; Berger, K.; Colombo, E.; Garcia Lopez, R. J.; Garczarczyk, M.; Herrero, A.; Tescaro, D.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Bednarek, W.; Idec, W.; Niedzwiecki, A.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland. [Berger, K.; Garcia Lopez, R. J.; Herrero, A.; Tescaro, D.] Univ La Laguna, Depto Astrofis, San Cristobal la Laguna 38206, Spain. [Bernardini, E.; De Caneva, G.; Gozzini, S. R.; Mallot, K.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Biland, A.; Boller, A.; Kraehenbuehl, T.; Lorenz, E.; Vogler, P.; Weitzel, Q.] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland. [Bretz, T.; Carreto Fidalgo, D.; Dorner, D.; Eisenacher, D.; Elsaesser, D.; Lewandowska, N.; Mannheim, K.; Overkemping, A.; Ruegamer, S.; Spanier, F.; Storz, J.; Tibolla, O.; Kadler, M.; Krauss, F.; Wilbert, S.] Univ Wurzburg, D-97074 Wurzburg, Germany. [Carmona, E.; Delgado Mendez, C.] Ctr Invest Energet Medioambientales & Tecnol, Madrid 28040, Spain. [Cossio, L.; Dazzi, F.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Overkemping, A.; Palatiello, M.; Persic, M.] Univ Udine, I-33100 Udine, Italy. [Cossio, L.; Dazzi, F.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Palatiello, M.; Persic, M.] INFN Trieste, I-33100 Udine, Italy. [Doert, M.; Hadamek, A.; Overkemping, A.; Rhode, W.; Thaele, J.; Uellenbeck, M.] Tech Univ Dortmund, D-44221 Dortmund, Germany. [Dominguez, A.; Prada, F.; Zandanel, F.] Inst Astrofis Andalucia CSIC, Granada 18080, Spain. [Doro, M.; Mariotti, M.; Masbou, J.; Overkemping, A.; Paiano, S.; Prandini, E.; Saggion, A.; Scalzotto, V.; Schultz, C.] Univ Padua, I-35131 Padua, Italy. [Doro, M.; Mariotti, M.; Masbou, J.; Overkemping, A.; Paiano, S.; Prandini, E.; Saggion, A.; Scalzotto, V.; Schultz, C.] INFN, I-35131 Padua, Italy. [Doro, M.; Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, Unitat Fis Radiac, Dept Fis, Bellaterra 08193, Spain. [Doro, M.; Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain. [Farina, E.; Treves, A.] Univ Insubria, I-22100 Como, Italy. [Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Bellaterra 08193, Spain. [Kadenius, V.; Lindfors, E.; Nilsson, K.; Reinthal, R.; Sillanpaeae, A.; Takalo, L.] Univ Turku, Tuorla Observ, Piikkio 21500, Finland. [Kushida, J.; Orito, R.; Saito, K.; Takami, H.] Kyoto Univ, Japanese MAGIC Consortium, Div Phys & Astron, Kahiwa, Chiba 2778582, Japan. [Makariev, M.; Maneva, G.; Temnikov, P.] Inst Nucl Energy Res, Sofia 1784, Bulgaria. [Marcote, B.; Moldon, J.; Munar-Adrover, P.; Paredes, J. M.; Ribo, M.; Zanin, R.] Univ Barcelona ICC IEEC, Barcelona 08028, Spain. [Persic, M.] INAF Osservatorio Astron, I-34143 Trieste, Italy. [Persic, M.] INFN, I-34143 Trieste, Italy. [PradaMoroni, P. G.; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy. [PradaMoroni, P. G.; Shore, S. N.] INFN Pisa, I-56126 Pisa, Italy. [Torres, D. F.] ICREA, Barcelona 08010, Spain. [Prada, F.] UAM CSIC, Inst Fis Teor, Madrid 28049, Spain. [Dauser, T.; Krauss, F.; Wilms, J.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Dauser, T.; Krauss, F.; Wilms, J.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. [Fortin, P.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. RP Eisenacher, D (reprint author), Univ Wurzburg, D-97074 Wurzburg, Germany. EM deisenacher@astro.uni-wuerzburg.de RI Fonseca Gonzalez, Maria Victoria/I-2004-2015; Contreras Gonzalez, Jose Luis/K-7255-2014; Maneva, Galina/L-7120-2016; Temnikov, Petar/L-6999-2016; Makariev, Martin/M-2122-2016; Torres, Diego/O-9422-2016; Reichardt, Ignasi/P-7478-2016; Barrio, Juan/L-3227-2014; Martinez Rodriguez, Manel/C-2539-2017; Cortina, Juan/C-2783-2017; Wilms, Joern/C-8116-2013; Rico, Javier/K-8004-2014; Fernandez, Ester/K-9734-2014; Babic, Ana/B-9599-2014; Ribo, Marc/B-3579-2015; Antoranz, Pedro/H-5095-2015; Miranda, Jose Miguel/F-2913-2013; Delgado, Carlos/K-7587-2014; Stamatescu, Victor/C-9945-2016; Lopez Moya, Marcos/L-2304-2014; GAug, Markus/L-2340-2014; Font, Lluis/L-4197-2014; Moralejo Olaizola, Abelardo/M-2916-2014 OI Becerra Gonzalez, Josefa/0000-0002-6729-9022; Paredes, Josep M./0000-0002-1566-9044; Tavecchio, Fabrizio/0000-0003-0256-0995; Bonnoli, Giacomo/0000-0003-2464-9077; Doro, Michele/0000-0001-9104-3214; Stamerra, Antonio/0000-0002-9430-5264; Prandini, Elisa/0000-0003-4502-9053; LA BARBERA, ANTONINO/0000-0002-5880-8913; Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; De Lotto, Barbara/0000-0003-3624-4480; Persic, Massimo/0000-0003-1853-4900; Dominguez, Alberto/0000-0002-3433-4610; Farina, Emanuele Paolo/0000-0002-6822-2254; Ribo, Marc/0000-0002-9931-4557; Ahnen, Max Ludwig/0000-0003-1000-0082; Covino, Stefano/0000-0001-9078-5507; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Temnikov, Petar/0000-0002-9559-3384; Torres, Diego/0000-0002-1522-9065; Reichardt, Ignasi/0000-0003-3694-3820; Barrio, Juan/0000-0002-0965-0259; Cortina, Juan/0000-0003-4576-0452; Prada Moroni, Pier Giorgio/0000-0001-9712-9916; Wilms, Joern/0000-0003-2065-5410; Rico, Javier/0000-0003-4137-1134; Babic, Ana/0000-0001-9549-9710; Antoranz, Pedro/0000-0002-3015-3601; Miranda, Jose Miguel/0000-0002-1472-9690; Delgado, Carlos/0000-0002-7014-4101; Stamatescu, Victor/0000-0001-9030-7513; Lopez Moya, Marcos/0000-0002-8791-7908; GAug, Markus/0000-0001-8442-7877; Font, Lluis/0000-0003-2109-5961; Moralejo Olaizola, Abelardo/0000-0002-1344-9080 FU German BMBF; German MPG; Italian INFN; Swiss National Fund SNF; Spanish MICINN; CPAN project of the Spanish Consolider-Ingenio programme [CSD2007-00042]; MultiDark project of the Spanish Consolider-Ingenio programme [CSD2009-00064]; Academy of Finland [127740]; DFG Cluster of Excellence "Origin and Structure of the Universe"; DFG Collaborative Research Centers [SFB823/C4, SFB876/C3]; Polish MNiSzW grant [745/N-HESS-MAGIC/2010/0]; Croatian National Science Foundation [09/176]; National Aeronautics and Space Administration; ESA Member States; NASA; INAF in Italy; CNES in France; Bundesministerium fur Forschung und Technologie under Deutsches Zentrum fur Luft- und Raumfahrt [50OR1207] FX We would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence "Origin and Structure of the Universe", by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0, and the Croatian National Science Foundation grant 09/176. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of 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. Based 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 data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. The Fermi-LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. T. Dauser would like to thank the Bayerisches Elitenetzwerk and the Bundesministerium fur Forschung und Technologie under Deutsches Zentrum fur Luft- und Raumfahrt grant 50OR1207". We would like to thank the referee for helpful comments. NR 63 TC 14 Z9 14 U1 2 U2 20 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 MAR PY 2014 VL 563 AR A91 DI 10.1051/0004-6361/201321938 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2JB UT WOS:000333798000091 ER PT J AU Codella, C Maury, AJ Gueth, F Maret, S Belloche, A Cabrit, S Andre, P AF Codella, C. Maury, A. J. Gueth, F. Maret, S. Belloche, A. Cabrit, S. Andre, Ph TI First results from the CALYPSO IRAM-PdBI survey III. Monopolar jets driven by a proto-binary system in NGC1333-IRAS2A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: jets and outflows; ISM: molecules; planetary nebulae: individual: NGC 1333-IRAS2A ID STAR-FORMING REGIONS; LOW-MASS PROTOSTARS; SIO LINE EMISSION; PROTOSTELLAR JET; NGC 1333; SUBMILLIMETER ARRAY; SUBARCSECOND RESOLUTION; INTERSTELLAR JETS; SHOCK-WAVES; DISK WINDS AB Context. The earliest evolutionary stages of low-mass protostars are characterised by hot and fast jets which remove angular momentum from the circumstellar disk, thus allowing mass accretion onto the central object. However, the launch mechanism is still being debated. Aims. We would like to exploit high-angular (similar to 0 ''.8) resolution and high-sensitivity images to investigate the origin of protostellar jets using typical molecular tracers of shocked regions, such as SiO and SO. Methods. We mapped the inner 22 '' of the NGC 1333-IRAS2A protostar in SiO(5-4), SO(6(5)-5(4)), and the continuum emission at 1.4 mm using the IRAM Plateau de Bure Interferometer in the framework of the CALYPSO IRAM large program. Results. For the first time, we disentangle the NGC1333-IRAS2A Class 0 object into a proto-binary system revealing two protostars (MM1, MM2) separated by similar to 560 AU, each of them driving their own jet, while past work considered a single protostar with a quadrupolar outflow. We reveal (i) a clumpy, fast (up to vertical bar V -V-LSR vertical bar >= 50 km s(-1)), and blueshifted jet emerging from the brightest MM1 source; and (ii) a slower redshifted jet, driven by MM2. Silicon monoxide emission is a powerful tracer of high-excitation (T-kin >= 100 K; n(H2) = 10(5) cm(-3)) jets close to the launching region. At the highest velocities, SO appears to mimic SiO tracing the jets, whereas at velocities close to the systemic one, SO is dominated by extended emission, tracing the cavity opened by the jet. Conclusions. Both jets are intrinsically monopolar, and intermittent in time. The dynamical time of the SiO clumps is <= 30-90 yr, indicating that one-sided ejections from protostars can take place on these timescales. C1 [Codella, C.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Maury, A. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maury, A. J.] ESO, D-85748 Garching, Germany. [Gueth, F.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Maret, S.; Cabrit, S.] UJF Grenoble1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. [Belloche, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Cabrit, S.] UPMC, UCP, CNRS, LERMA,Observ Paris,ENS, F-75014 Paris, France. [Andre, Ph] Univ Paris Diderot, CE Saclay, CNRS, Lab AIM Paris Saclay,CEA,DSM,Irfu, F-91191 Gif Sur Yvette, France. RP Codella, C (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. EM codella@arcetri.astro.it OI Codella, Claudio/0000-0003-1514-3074; Maret, Sebastien/0000-0003-1104-4554 FU European Community [229517, 291294]; French Agence Nationale de la Recherche (ANR) [ANR-12-JS05-0005] FX We are very grateful to all the IRAM staff, whose dedication allowed us to carry out the CALYPSO project. The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013/) under grant agreements No. 229517 (ESO COFUND) and No. 291294 (ORISTARS), and from the French Agence Nationale de la Recherche (ANR), under reference ANR-12-JS05-0005. NR 44 TC 19 Z9 19 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 MAR PY 2014 VL 563 AR L3 DI 10.1051/0004-6361/201323024 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2JB UT WOS:000333798000148 ER PT J AU Ellerbroek, LE Podio, L Dougados, C Cabrit, S Sitko, ML Sana, H Kaper, L de Koter, A Klaassen, PD Mulders, GD Mendigutia, I Grady, CA Grankin, K van Winckel, H Bacciotti, F Russell, RW Lynch, DK Hammel, HB Beerman, LC Day, AN Huelsman, DM Werren, C Henden, A Grindlay, J AF Ellerbroek, L. E. Podio, L. Dougados, C. Cabrit, S. Sitko, M. L. Sana, H. Kaper, L. de Koter, A. Klaassen, P. D. Mulders, G. D. Mendigutia, I. Grady, C. A. Grankin, K. van Winckel, H. Bacciotti, F. Russell, R. W. Lynch, D. K. Hammel, H. B. Beerman, L. C. Day, A. N. Huelsman, D. M. Werren, C. Henden, A. Grindlay, J. TI Relating jet structure to photometric variability: the Herbig Ae star HD 163296 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; circumstellar matter; stars: variables: T Tauri, Herbig Ae/Be; ISM: jets and outflows; Herbig-Haro objects; stars: individual: HD 163296 ID PRE-MAIN-SEQUENCE; T-TAURI STARS; HUBBLE-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; INTERMEDIATE-MASS STARS; NEAR-INFRARED EMISSION; SYSTEM Z CMA; AE/BE STARS; PROTOPLANETARY DISKS; ACCRETION RATES AB Herbig Ae/Be stars are intermediate-mass pre-main sequence stars surrounded by circumstellar dust disks. Some are observed to produce jets, whose appearance as a sequence of shock fronts (knots) suggests a past episodic outflow variability. This "jet fossil record" can be used to reconstruct the outflow history. We present the first optical to near-infrared (NIR) spectra of the jet from the Herbig Ae star HD 163296, obtained with VLT/X-shooter. We determine the physical conditions in the knots and also their kinematic "launch epochs". Knots are formed simultaneously on either side of the disk, with a regular interval of similar to 16 yr. The velocity dispersion versus jet velocity and the energy input are comparable between both lobes. However, the mass-loss rate, velocity, and shock conditions are asymmetric. We find. (M) over dot(jet)/(M) over dot(acc) similar to 0.01-0.1, which is consistent with magneto-centrifugal jet launching models. No evidence of any dust is found in the high-velocity jet, suggesting a launch region within the sublimation radius (<0.5 au). The jet inclination measured from proper motions and radial velocities confirms that it is perpendicular to the disk. A tentative relation is found between the structure of the jet and the photometric variability of the central source. Episodes of NIR brightening were previously detected and attributed to a dusty disk wind. We report for the first time significant optical fadings lasting from a few days up to a year, coinciding with the NIR brightenings. These are very likely caused by dust lifted high above the disk plane, and this supports the disk wind scenario. The disk wind is launched at a larger radius than the high-velocity atomic jet, although their outflow variability may have a common origin. No significant relation between outflow and accretion variability could be established. Our findings confirm that this source undergoes periodic ejection events, which may be coupled with dust ejections above the disk plane. C1 [Ellerbroek, L. E.; Kaper, L.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Podio, L.; Dougados, C.; Cabrit, S.] Inst Planetol & Astrophys Grenoble, F-38400 St Martin Dheres, France. [Podio, L.; Bacciotti, F.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Dougados, C.] CNRS Univ Chile, Lab Franco Chilien Astron LFCA, Santiago, Chile. [Cabrit, S.] Observ Paris, UMR CNRS 8112, LERMA, F-75014 Paris, France. [Sitko, M. L.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Sitko, M. L.] Space Sci Inst, Boulder, CO 80303 USA. [Sana, H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [de Koter, A.; van Winckel, H.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium. [Klaassen, P. D.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Mulders, G. D.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Mendigutia, I.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Grady, C. A.] Eureka Sci Inc, Oakland, CA 94602 USA. [Grady, C. A.] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Grankin, K.] Sci Res Inst, Crimean Astrophys Observ, Nauchnyi, Ukraine. [Russell, R. W.; Lynch, D. K.] Aerosp Corp, Los Angeles, CA 90009 USA. [Russell, R. W.; Lynch, D. K.] Aerosp Corp, Los Angeles, CA 90009 USA. [Lynch, D. K.] Thule Sci, Topanga, CA 90290 USA. [Hammel, H. B.] Associated Univ Res Astron Inc, Washington, DC 20005 USA. [Beerman, L. C.] Univ Washington, Dept Astron, Seattle, WA 98105 USA. [Day, A. N.] Miami Univ, Dept Phys, Oxford, OH 45056 USA. [Huelsman, D. M.] Stanford Univ, Dept Management Sci & Engn, Stanford, CA 94305 USA. [Henden, A.] Amer Assoc Variable Star Observers, Cambridge, MA 02138 USA. [Grindlay, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ellerbroek, LE (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM lucas.ellerbroek@gmail.com RI Sana, Hugues/B-2664-2013; OI Sana, Hugues/0000-0001-6656-4130; Grankin, Konstantin/0000-0001-5707-8448; BACCIOTTI, FRANCESCA/0000-0001-5776-9476; Mendigutia, Ignacio/0000-0002-0233-5328 FU Netherlands Research School for Astronomy (NOVA); NASA ADP [NNH06CC28C, NNX09AC73G]; IR&D program at The Aerospace Corporation; FP7 Intra-European Marie Curie Fellowship [PIEF-GA-2009-253896] FX The referee, Dr. Tom Ray, is acknowledged for useful comments that helped improve the manuscript. The authors thank Myriam Benisty, Jerome Bouvier, Carsten Dominik, Patrick Hartigan, Henny Lamers, Koen Maaskant, Michiel Min, Brunella Nisini, Charlie Qi, Alex Raga, and Rens Waters for discussions about this work. Patrick Hartigan is also acknowledged for kindly providing the shock model results in tabular form. The ESO staff and Christophe Martayan in particular are acknowledged for their careful support of the VLT/X-shooter observations. Daryl Kim is acknowledged for his technical support of the BASS observing runs. The authors thank Bill Vacca, Mike Cushing, and John Rayner for useful discussions on the use of the SpeX instrument and the Spextool processing package. This work was supported by a grant from the Netherlands Research School for Astronomy (NOVA), NASA ADP grants NNH06CC28C and NNX09AC73G, and the IR&D program at The Aerospace Corporation. LP acknowledges the funding from the FP7 Intra-European Marie Curie Fellowship (PIEF-GA-2009-253896). NR 126 TC 18 Z9 18 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2014 VL 563 AR A87 DI 10.1051/0004-6361/201323092 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2JB UT WOS:000333798000087 ER PT J AU Immer, K Cyganowski, C Reid, MJ Menten, KM AF Immer, K. Cyganowski, C. Reid, M. J. Menten, K. M. TI The cometary H II regions of DR 21: Bow shocks or champagne flows or both? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE HII regions; stars: formation; ISM: individual objects: DR21; ISM: kinematics and dynamics; radio lines: ISM ID HII-REGIONS; DYNAMICS; COMPACT; MODELS; SCUBA AB We present deep Very Large Array H66 alpha radio recombination line (RRL) observations of the two cometary H II regions in DR 21. With these sensitive data, we test the "hybrid" bow shock/champagne flow model previously proposed for the DR 21 H II regions. The ionized gas down the tail of the southern H II region is redshifted by up to similar to 30 km s(-1) with respect to the ambient molecular gas, as expected in the hybrid scenario. The RRL velocity structure, however, reveals the presence of two velocity components in both the northern and southern H II regions. This suggests that the ionized gas is flowing along cone-like shells, swept-up by stellar winds. The observed velocity structure of the well-resolved southern H II region is most consistent with a picture that combines a stellar wind with stellar motion (as in bow shock models) along a density gradient (as in champagne flow models). The direction of the implied density gradient is consistent with that suggested by maps of dust continuum and molecular line emission in the DR 21 region. C1 [Immer, K.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Immer, K.; Cyganowski, C.; Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. RP Immer, K (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM kimmer@mpifr-bonn.mpg.de FU NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1003134] FX K.I. would like to thank M. Hoare for fruitful discussions. This research has made use of NASA's Astrophysics Data System Bibliographic Services. C.J.C. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1003134. NR 15 TC 4 Z9 4 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 MAR PY 2014 VL 563 AR A39 DI 10.1051/0004-6361/201321736 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2JB UT WOS:000333798000039 ER PT J AU Maret, S Belloche, A Maury, AJ Gueth, F Andre, P Cabrit, S Codella, C Bontemps, S AF Maret, S. Belloche, A. Maury, A. J. Gueth, F. Andre, Ph Cabrit, S. Codella, C. Bontemps, S. TI First results from the CALYPSO IRAM-PdBI survey I. Kinematics of the inner envelope of NGC 1333-IRAS2A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: individual objects: NGC 1333-IRAS2A; ISM: kinematics and dynamics; ISM: molecules; stars: formation ID LOW-MASS PROTOSTARS; STAR-FORMING REGIONS; PROTOSTELLAR ENVELOPES; KEPLERIAN DISK; WATER; ABUNDANCE; ROTATION; MASERS; CLOUDS; CORES AB The structure and kinematics of Class 0 protostars on scales of a few hundred AU is poorly known. Recent observations have revealed the presence of Keplerian disks with a diameter of 150-180 AU in L1527-IRS and VLA1623A, but it is not clear if such disks are common in Class 0 protostars. Here we present high-angular-resolution observations of two methanol lines in NGC1333-IRAS2A. We argue that these lines probe the inner envelope, and we use them to study the kinematics of this region. Our observations suggest the presence of a marginal velocity gradient normal to the direction of the outflow. However, the position velocity diagrams along the gradient direction appear inconsistent with a Keplerian disk. Instead, we suggest that the emission originates from the infalling and perhaps slowly rotating envelope, around a central protostar of 0.1-0.2 M-circle dot. If a disk is present, it is smaller than the disk of L1527-IRS, perhaps suggesting that NGC 1333-IRAS2A is younger. C1 [Maret, S.; Cabrit, S.] UJF Grenoble 1, CNRS, INSU, Inst Planetol & Astrophys Grenoble,UMR 5274, F-38041 Grenoble, France. [Belloche, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Maury, A. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gueth, F.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Andre, Ph] Univ Paris Diderot, CE Saclay, CNRS, Lab AIM Paris Saclay,CEA,DSM,Irfu, F-91191 Gif Sur Yvette, France. [Cabrit, S.] UPMC, UCP, CNRS, LERMA,Observa Paris,ENS, F-75014 Paris, France. [Codella, C.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Bontemps, S.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Bontemps, S.] CNRS, LAB, UMR 5804, F-33270 Floirac, France. RP Maret, S (reprint author), UJF Grenoble 1, CNRS, INSU, Inst Planetol & Astrophys Grenoble,UMR 5274, F-38041 Grenoble, France. EM sebastien.maret@obs.ujf-grenoble.fr OI Codella, Claudio/0000-0003-1514-3074 FU European Community [229517, 291294]; French Agence Nationale de la Recherche (ANR) [ANR-12-JS05-0005] FX The research leading to these results has received funding from the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreements No. 229517 (ESO COFUND) and No. 291294 (ORISTARS), and from the French Agence Nationale de la Recherche (ANR), under reference ANR-12-JS05-0005. NR 23 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 MAR PY 2014 VL 563 AR L1 DI 10.1051/0004-6361/201323028 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2JB UT WOS:000333798000146 ER PT J AU Maury, AJ Belloche, A Andre, P Maret, S Gueth, F Codella, C Cabrit, S Testi, L Bontemps, S AF Maury, A. J. Belloche, A. Andre, Ph Maret, S. Gueth, F. Codella, C. Cabrit, S. Testi, L. Bontemps, S. TI First results from the CALYPSO IRAM-PdBI survey II. Resolving the hot corino in the Class 0 protostar NGC 1333-IRAS2A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; circumstellar matter; ISM: individual objects: NGC 1333-IRAS2A; radio lines: ISM; methods: observational ID LOW-MASS PROTOSTARS; STAR-FORMING REGIONS; SUBMILLIMETER ARRAY; RESOLUTION OBSERVATIONS; SUBARCSECOND SURVEY; ORGANIC-MOLECULES; COMPLEX-MOLECULES; LINE SURVEY; CORE; IRAS-16293-2422 AB Aims. We investigate the origin of complex organic molecules (COMs) in the gas phase around the low-mass Class 0 protostar NGC 1333-IRAS2A, to determine if the COM emission lines trace an embedded disk, shocks from the protostellar jet, or the warm inner parts of the protostellar envelope. Methods. In the framework of the CALYPSO IRAM Plateau de Bure survey, we obtained large bandwidth spectra at sub-arcsecond resolution towards NGC 1333-IRAS2A. We identify the emission lines towards the central protostar and perform Gaussian fits to constrain the size of the emitting region for each of these lines, tracing various physical conditions and scales. Results. The emission of numerous COMs such as methanol, ethylene glycol, and methyl formate is spatially resolved by our observations. This allows us to measure, for the first time, the size of the COM emission inside the protostellar envelope, finding that it originates from a region of radius 40-100 AU, centered on the NGC 1333-IRAS2A protostellar object. Our analysis shows no preferential elongation of the COM emission along the jet axis, and therefore does not support the hypothesis that COM emission arises from shocked envelope material at the base of the jet. Down to similar sizes, the dust continuum emission is well reproduced with a single power-law envelope model, and therefore does not favor the hypothesis that COM emission arises from the thermal sublimation of grains embedded in a circumstellar disk. Finally, the typical scale similar to 60 AU observed for COM emission is consistent with the size of the inner envelope where T-dust > 100 K is expected. Our data therefore strongly suggest that the COM emission traces the hot corino in IRAS2A, i.e., the warm inner envelope material where the icy mantles of dust grains evaporate because they are passively heated by the central protostellar object. C1 [Maury, A. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maury, A. J.; Testi, L.] ESO, D-85748 Garching, Germany. [Belloche, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Maury, A. J.; Andre, Ph] Univ Paris Diderot, CE Saclay, CNRS, Lab AIM Paris Saclay,CEA,DSM,Irfu, F-91191 Gif Sur Yvette, France. [Maret, S.; Cabrit, S.] UJF Grenoble1, CNRS, INSU, Inst Planetol & Astrophys Grenoble,UMR 5274, F-38041 Grenoble, France. [Gueth, F.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Codella, C.; Testi, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Cabrit, S.] UPMC, UCP, PSL, LERMA,Observ Paris,ENS, F-75014 Paris, France. [Testi, L.] Excellence Cluster Univ, D-85748 Garching, Germany. [Bontemps, S.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Bontemps, S.] CNRS, LAB, UMR 5804, F-33270 Floirac, France. RP Maury, AJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM amaury@cfa.harvard.edu OI Codella, Claudio/0000-0003-1514-3074; Maret, Sebastien/0000-0003-1104-4554 FU European Community [229517, 291294]; French Agence Nationale de la Recherche (ANR) [ANR-12-JS05-0005] FX We thank Holger Muller for the spectroscopic predictions of HNCO, upsilon5 = 1. We are very thankful to the IRAM staff, whose dedication allowed us to carry out the CALYPSO project. This research has received funding from the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreements No. 229517 (ESO COFUND) and No. 291294 (ORISTARS). S. M. acknowledges the support of the French Agence Nationale de la Recherche (ANR), under reference ANR-12-JS05-0005. NR 33 TC 29 Z9 29 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2014 VL 563 AR L2 DI 10.1051/0004-6361/201323033 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE2JB UT WOS:000333798000147 ER PT J AU Williams, AA Eastman, SF Eash-Loucks, WE Kimball, ME Lehmann, ML Parker, JD AF Williams, Asher A. Eastman, Scott F. Eash-Loucks, Wendy E. Kimball, Matthew E. Lehmann, Michael L. Parker, John D. TI Record Northernmost Endemic Mangroves on the United States Atlantic Coast with a Note on Latitudinal Migration SO SOUTHEASTERN NATURALIST LA English DT Article ID SALT-MARSH; RESISTANCE; FORESTS; FLORIDA AB The northern limits of three mangrove species-Avicennia germinans (Black Mangrove), Rhizophora mangle (Red Mangrove). Laguncularia racemosa (White Mangrove)-on the United States Atlantic coast are vouchered and described in comparison to previous boundaries defined in literature and herbarium collections. The location and general status of individual trees were used to delineate northern maxima and show that present ranges extend beyond historic records. The gradient structure of the ecotone within an area of uniform climate is interpreted as ongoing latitudinal movement. C1 [Williams, Asher A.; Eastman, Scott F.; Eash-Loucks, Wendy E.; Kimball, Matthew E.] Guana Tolomato Matanzas Natl Estuarine Res Reserv, Ponte Vedra Beach, FL 32082 USA. [Williams, Asher A.; Eastman, Scott F.; Kimball, Matthew E.] Univ N Florida, Dept Biol Sci, Jacksonville, FL 32224 USA. [Williams, Asher A.] Louisiana State Univ, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70803 USA. [Eash-Loucks, Wendy E.] King Cty Dept Nat Resources & Pk, Seattle, WA 98104 USA. [Kimball, Matthew E.] Univ S Carolina, Baruch Marine Field Lab, Georgetown, SC 29442 USA. [Lehmann, Michael L.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Parker, John D.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Williams, AA (reprint author), Guana Tolomato Matanzas Natl Estuarine Res Reserv, 505 Guana River Rd, Ponte Vedra Beach, FL 32082 USA. EM awil336@tigers.lsu.edu RI Parker, John/F-9761-2010 OI Parker, John/0000-0002-3632-7625 FU National Aeronautics and Space Administration [NNX-11AO94G]; National Science Foundation [EF1065821] FX Bruce Hansen expediently vouchered plant samples into the USF Herbarium. Torn Harding observed potential northernmost mangroves. which was part of the impetus to formalize the locations. Critical insights were provided by two anonymous reviewers. This material is based upon work supported by the National Aeronautics and Space Administration (NNX-11AO94G) and the National Science Foundation (EF1065821). NR 25 TC 9 Z9 9 U1 1 U2 15 PU HUMBOLDT FIELD RESEARCH INST PI STEUBEN PA PO BOX 9, STEUBEN, ME 04680-0009 USA SN 1528-7092 EI 1938-5412 J9 SOUTHEAST NAT JI Southeast. Nat. PD MAR PY 2014 VL 13 IS 1 BP 56 EP 63 DI 10.1656/058.013.0104 PG 8 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AE3QN UT WOS:000333891100007 ER PT J AU Karasawa, H Schweitzer, CE Feldmann, RM Luque, J AF Karasawa, Hiroaki Schweitzer, Carrie E. Feldmann, Rodney M. Luque, Javier TI PHYLOGENY AND CLASSIFICATION OF RANINOIDA (DECAPODA: BRACHYURA) SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article DE Lyreididae; Necrocarcinoidea; Palaeocorystidae; phylogeny; Raninidae; Raninoidea ID CRABS CRUSTACEA; MIDDLE EOCENE; SOUTH-DAKOTA; RANINID CRAB; PIERRE SHALE; FOSSIL CRABS; NEW-ZEALAND; N-GEN; PODOTREMATA; MEXICO AB Phylogenetic analysis of most genera within fossil and extant Raninoida (Brachyura) based on 72 adult morphological characters yielded a new superfamily and family level classification for the section. The section was most diverse at the family level during the Late Cretaceous but remains diverse at the genus and species level in the Holocene. New subfamilies include Bicornisranininae, Macroacaeninae, and Rogueinae within Lyreididae. New genera include Colombicarcinus, Alessandranizza, Claudioranina, Giulianolyreidus and Italianira, and one new species, Colombicarcinus laevis, is described. New combinations include Alessandranina ornata (Wright and Collins, 1972), Claudioranina oblonga (Beschin, Busulini, de Angeli, and Tessier, 1988), Heus manningi (Bishop and Williams, 2000), Italianira punctulata (Beschin, Busulini, de Angeli, and Tessier, 1988), Giulianolyreidus bidentatus (Rathbun, 1935a), G. johnsoni (Rathbun, 1935a), Lyreidus teodorii (van Bakel et al., 2012), Macroacaena tridens (Roberts, 1962), M. teshimai (Fujiyama and Takeda, 1980), M. yanini (Ilyin and Alekseev, 1998) and Quasilaeviranina eocenica (Rathbun, 1935a). C1 [Karasawa, Hiroaki] Mizunami Fossil Museum, Gifu 5096132, Japan. [Schweitzer, Carrie E.] Kent State Univ Stark, Dept Geol, North Canton, OH 44720 USA. [Feldmann, Rodney M.] Kent State Univ, Dept Geol, Kent, OH 44242 USA. [Luque, Javier] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. [Luque, Javier] Smithsonian Trop Res Inst, Panama City 084303092, Panama. RP Feldmann, RM (reprint author), Kent State Univ, Dept Geol, Kent, OH 44242 USA. EM rfeldman@kent.edu OI Luque, Javier/0000-0002-4391-5951 FU NSF [EF-0531670, INT-0313606, EAR-1223206, OPP-9909184, INT-0003058]; National Geographic Society [6265-98]; Natural Science and Engineering Research Council of Canada (NSERC CGS-D) FX Examination of type and comparative material in museum collections in Europe, Japan, and USA was funded by NSF grants EF-0531670 and INT-0313606 and National Geographic Society Grant 6265-98 to Feldmann and Schweitzer. Diversity analysis was conducted under NSF grant EAR-1223206 to Schweitzer and Feldmann. Field work for collection of comparative material and the species herein described by Feldmann and Schweitzer was funded by NSF grant OPP-9909184 to Feldmann and Bice and NSF grant INT-0003058 to Feldmann and Schweitzer. Graduate Scholarship to Luque was provided by the Natural Science and Engineering Research Council of Canada (NSERC CGS-D). G. Schweigert, Staatliches Museum fur Naturkunde, Stuttgart, Germany; M. Nose, Bayerische Staatsammlung fur Palaontologie, Munchen, Germany; O. Schultz and A. Kroh, Geological and Palaeontological Department of the Naturhistorisches Museum Wien, Vienna, Austria; I. Zorn, Geological Survey of Austria, Vienna, Austria; M. Munt and C. Mellish, The Natural History Museum, London, UK; M. Riley, Sedgwick Museum, Cambridge University, Cambridge, UK; P. Muller, Termeszettudomanyi Muzeum, Fold-es oslenytar, Budapest, Hungary; S. Charbonnier, Museum national d'Histoire naturelle, Paris, France; P. Anal and S. Calzada, Museo Geologic del Seminario de Barcelona, Barcelona, Spain; S. Shelton and J. Martin, South Dakota School of Mines and Technology, Rapid City, SD, USA; H. Kato and K. Komai, Natural History Museum and Institute of Chiba, Chiba, Japan; R. Lemaitre and K. Reed (Crustacea) and K. Hollis and M. Florence (Paleobiology), Smithsonian Institution, United States National Museum of Natural History, Washington, DC, USA; M. Ohara, Wakayama Prefectural Museum of Natural History, Kainan, Japan; N. S. Rugh and T. Demere, San Diego Museum of Natural History, San Diego, CA, USA; A. Lord and C. Franz (Paleontology) and M. Turkay (Crustacea), Senckenberg Museum, Frankfurt, Germany; M. Coyne, Geological Survey of Canada, Ottawa, ON, Canada; the late A. Dhondt, Institut Royal des Sciences Naturelles de Belgique, Brussels, Belgium; J. Sklenar, National Museum, Prague, Czech Republic; J. Sprinkle and A. Molineux, University of Texas Austin, Austin, TX, USA; C. Beschin, A. de Angeli and V. Frisone, Museo Civico "G. Zannato" di Montecchio Maggiore (Vicenza), Vicenza, Italy; R. Fraaije, Oertijdmuseum De Groene Poort, Boxtel, The Netherlands; E. Nesbitt, Burke Museum of Natural History and Culture, Washington, DC, USA; S. L. Jakobsen, Geological Museum, University of Copenhagen, Copenhagen, Denmark; and A. E. Sanders, Charleston Museum, Charleston, SC, USA, all provided access to their collections or facilitated loans from their institutions. T. Nyborg provided photos of Bicornisranina bocki. J. Huang, Chengdu Institute of Geology and Mineral Resources, assisted in Chinese translation. T. Snyder and all of the staff at the Inter-Library Loan service at the KSU library assisted in finding old and obscure literature. Schweigert provided much needed assistance in determining the modern-day equivalents of 19th century formation names and in determining the age of 19th century occurrences. F. Vega, UNAM, Mexico City, Mexico, and an anonymous reviewer provided constructive comments on the manuscript. NR 262 TC 10 Z9 15 U1 2 U2 12 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 EI 1937-240X J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD MAR PY 2014 VL 34 IS 2 BP 216 EP 272 DI 10.1163/1937240X-00002216 PG 57 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AE2FB UT WOS:000333787600010 ER PT J AU Olson, SL AF Olson, Storrs L. TI A HARD NUT TO CRACK: RAPID EVOLUTION IN THE KONA GROSBEAK OF HAWAII FOR A LOCALLY ABUNDANT FOOD SOURCE (DREPANIDINI: CHLORIDOPS KONA) SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article DE Chloridops wahi; feeding adaptations; Myoporum sandwicense; naio; seed-cracking finches; Wahi Grosbeak; Zanthoxylum ID FINCHES; KAUAI AB The Kona Grosbeak (Chloridops kona), last seen in 1892, was restricted to a small mid-elevation area on the leeward (Kona) side of the island of Hawaii. It was reported to feed almost exclusively on the fruits of the naio tree (Myoporum sandwicense), which are extremely hard, requiring a force of perhaps 400 newtons or more to open. The morphology of the skull and mandible of the Kona Grosbeak was accordingly much more modified for the hypertrophied adductor musculature needed to crack naio fruits than its closest relative, the Wahi Grosbeak (Chloridops wahi), which has been found as fossils on most of the other main Hawaiian islands. The Wahi Grosbeak is here hypothesized to have fed on less resistant seeds, such as those of the Hawaiian prickly-ash (Zanthoxylum spp.). Naio is widely distributed in diverse habitats in the Hawaiian Islands but its fruits were apparently an energetically viable food source only on relatively young (ca. 1200 year old) aa lava flows on the dry side of Hawaii, where the plants produce abundant flowers and fruit on a year-round basis. The Kona Grosbeak therefore appears to have evolved in less than the ca. 400,000 years since Mauna Loa became high enough to create a rain shadow and develop younger an flows and associated vegetation. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012, Washington, DC 20013 USA. EM olsons@si.edu NR 18 TC 0 Z9 0 U1 1 U2 10 PU WILSON ORNITHOLOGICAL SOC PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 1559-4491 EI 1938-5447 J9 WILSON J ORNITHOL JI Wilson J. Ornithol. PD MAR PY 2014 VL 126 IS 1 BP 1 EP 8 PG 8 WC Ornithology SC Zoology GA AD9GN UT WOS:000333573100001 ER PT J AU Jedlicka, JA Greenberg, R Raimondi, PT AF Jedlicka, Julie A. Greenberg, Russell Raimondi, Peter T. TI VINEYARD AND RIPARIAN HABITAT, NOT NEST BOX PRESENCE, ALTER AVIAN COMMUNITY COMPOSITION SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article DE associated diversity; bird nest boxes; boundary effects; conservation; corridor; oak woodlands; riparian buffer; vineyard ID WESTERN BLUEBIRDS; BIRD ASSEMBLAGES; POINT COUNTS; MIST NETS; ABUNDANCE; FORESTS AB In California, oak woodlands are being converted into vineyards, resulting in a loss of songbird nesting sites. Although many vineyards contain wooded riparian habitat, no previous research has examined the avian species composition in oak-vineyard landscapes. We compared the avian communities associated with vineyard, edge, and riparian habitats and examined to what degree the riparian habitat in vineyard landscapes continues to support birds associated with native oak woodland habitat that spanned the region before agricultural intensification. We further tested whether the presence of nest boxes in vineyard and riparian areas altered avian species composition in the landscape. Mist nets were used to survey the avian community in vineyard, edge, and riparian habitat at four sites during the breeding season. Permutational ANOVAs, using presence-absence data from captures, identified habitat, study sites, and time over the breeding season as highly significant main effects that explained differences in species composition. Establishment of songbird nest boxes did not alter the species composition. Two-thirds of the birds identified as woodland species in prior studies were found in riparian areas adjacent to vineyards, including five watch-list species. Overall the species composition of birds using riparian habitat was greater and significantly different from those found in the vineyard. This highlights the importance of maintaining natural areas like riparian habitat in agricultural landscapes. C1 [Jedlicka, Julie A.] Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. [Greenberg, Russell] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Raimondi, Peter T.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. RP Jedlicka, JA (reprint author), Univ Calif Berkeley, Dept Environm Sci Policy & Management, 130 Mulford Hall, Berkeley, CA 94720 USA. EM julie.jedlicka@gmail.com FU Annie's Sustainable Agriculture Graduate Scholarship; Animal Behavior Society; Smithsonian Migratory Bird Center; Environmental Studies Department at University of California Santa Cruz. Vertebrate animals [22665]; University of California's Institutional Animal Care and Use Committee [Letod0705] FX M. Poonamallee and L. Barrow provided invaluable field assistance. We thank D. Kenworthy, R. Burney, J. Peterson, D. Koball, M. Fetzer, Fetzer Vineyards, and Bedrock Vineyards for their cooperation and access to study sites. D. Thayer and D. Smith at University of California Santa Cruz were instrumental in helping to construct 200 nest boxes. We thank E. Heaton for advice, the Hop land Research and Extension Center for housing and services, and A. Merenlender for sharing avian species lists from her published data. T. Cornelisse, D. Letourneau, and anonymous reviewers provided helpful comments on earlier drafts of the manuscript. Funding was provided to J. A. I by Annie's Sustainable Agriculture Graduate Scholarship, E. O. Wilson Conservation Award from the Animal Behavior Society, the Smithsonian Migratory Bird Center, and the Environmental Studies Department at University of California Santa Cruz. Vertebrate animals were approved for use in the study by the U.S. Geological Survey (Permit Number: 22665) and the University of California's Institutional Animal Care and Use Committee (Permit Number: Letod0705). NR 28 TC 4 Z9 5 U1 1 U2 26 PU WILSON ORNITHOLOGICAL SOC PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 1559-4491 EI 1938-5447 J9 WILSON J ORNITHOL JI Wilson J. Ornithol. PD MAR PY 2014 VL 126 IS 1 BP 60 EP 68 PG 9 WC Ornithology SC Zoology GA AD9GN UT WOS:000333573100008 ER PT J AU Sironi, L Spitkovsky, A AF Sironi, Lorenzo Spitkovsky, Anatoly TI RELATIVISTIC RECONNECTION: AN EFFICIENT SOURCE OF NON-THERMAL PARTICLES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE acceleration of particles; galaxies: jets; gamma-ray burst: general; magnetic reconnection; pulsars: general; radiation mechanisms: non-thermal ID STRIPED PULSAR WIND; GAMMA-RAY BURSTS; MAGNETIC RECONNECTION; TERMINATION SHOCK; ELECTRON ACCELERATION; COLLISIONLESS SHOCKS; CRAB-NEBULA; DISSIPATION; ENERGY; JETS AB In magnetized astrophysical outflows, the dissipation of field energy into particle energy via magnetic reconnection is often invoked to explain the observed non-thermal signatures. By means of two-and three-dimensional particle-in-cell simulations, we investigate anti-parallel reconnection in magnetically dominated electron-positron plasmas. Our simulations extend to unprecedentedly long temporal and spatial scales, so we can capture the asymptotic state of the system beyond the initial transients, and without any artificial limitation by the boundary conditions. At late times, the reconnection layer is organized into a chain of large magnetic islands connected by thin X-lines. The plasmoid instability further fragments each X-line into a series of smaller islands, separated by X-points. At the X-points, the particles become unmagnetized and they get accelerated along the reconnection electric field. We provide definitive evidence that the late-time particle spectrum integrated over the whole reconnection region is a power law whose slope is harder than -2 for magnetizations sigma greater than or similar to 10. Efficient particle acceleration to non-thermal energies is a generic by-product of the long-term evolution of relativistic reconnection in both two and three dimensions. In three dimensions, the drift-kink mode corrugates the reconnection layer at early times, but the long-term evolution is controlled by the plasmoid instability which facilitates efficient particle acceleration, analogous to the two-dimensional physics. Our findings have important implications for the generation of hard photon spectra in pulsar winds and relativistic astrophysical jets. C1 [Sironi, Lorenzo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Spitkovsky, Anatoly] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Sironi, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lsironi@cfa.harvard.edu; anatoly@astro.princeton.edu FU Einstein grant [PF1-120090]; NASA [NNX12AD01G, NNX13AO80G]; Simons Foundation [267233]; XSEDE [TG-AST120010] FX L.S. is supported by Einstein grant PF1-120090, and A.S. by NASA grants NNX12AD01G and NNX13AO80G and Simons Foundation grant 267233. The simulations used PICSciE-OIT HPCC at Princeton University, XSEDE under contract TG-AST120010, and NASA HEC. NR 45 TC 103 Z9 104 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 1 PY 2014 VL 783 IS 1 AR L21 DI 10.1088/2041-8205/783/1/L21 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC4UB UT WOS:000332515500021 ER PT J AU Petersen, JJ Parker, IM Potter, D AF Petersen, Jennifer J. Parker, Ingrid M. Potter, Daniel TI Domestication of the neotropical tree Chrysophyllum cainito from a geographically limited yet genetically diverse gene pool in Panama SO ECOLOGY AND EVOLUTION LA English DT Article DE caimito; fruit trees; genetic diversity; Mesoamerica; Sapotaceae; semidomesticates ID MULTILOCUS GENOTYPE DATA; POPULATION-STRUCTURE; CULTIVATED POPULATIONS; AGROFORESTRY SYSTEMS; NATURAL-SELECTION; TROPICAL TREES; STAR APPLE; IN-SITU; FRUIT; WILD AB Species in the early stages of domestication, in which wild and cultivated forms co-occur, provide important opportunities to develop and test hypotheses about the origins of crop species. Chrysophyllum cainito (Sapotaceae), the star apple or caimito, is a semidomesticated tree widely cultivated for its edible fruits; it is known to be native to the neotropics, but its precise geographic origins have not been firmly established. Here, we report results of microsatellite marker analyses supporting the hypothesis that the center of domestication for caimito was the Isthmus of Panama, a region in which few crop species are believed to have originated, despite its importance as a crossroads for the dispersal of domesticated plants between North and South America. Our data suggest that caimito was domesticated in a geographically restricted area while incorporating a diverse gene pool. These results refute the generally accepted Antillean origin of caimito, as well as alternative hypotheses that the species was domesticated independently in the two areas or over a broad geographic range including both. Human-mediated dispersal from Panama to the north and east was accompanied by strong reductions in both genotypic and phenotypic diversity. Within Panama, cultivated and wild trees show little neutral genetic divergence, in contrast to striking phenotypic differentiation in fruit and seed traits. In addition to providing a rare example of data that support the hypothesis of a narrow geographic origin on the Isthmus of Panama for a now widespread cultivated plant species, this study is one of the first investigations of the origins of an edible species of the large pantropical family Sapotaceae. C1 [Petersen, Jennifer J.; Potter, Daniel] Univ Calif Davis, Dept Plant Sci, Davis, CA 95616 USA. [Parker, Ingrid M.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Parker, Ingrid M.] Smithsonian Trop Res Inst, Balboa, Panama. RP Petersen, JJ (reprint author), Univ Calif Davis, Dept Plant Sci, Mail Stop 3,One Shields Ave, Davis, CA 95616 USA. EM jjpetersen@ucdavis.edu FU Davis Botanical Society; UC Davis Center for Biosystematics; Henry A. Jastro Research Scholarship; Peter J. Shields Research Scholarship; UC MEXUS Dissertation Research Grant; Fulbright-Garcia Robles Scholarship; U.C. Davis Academic Senate Committee on Research; University Outreach and International Programs; UC Santa Cruz FX This work was supported by the Davis Botanical Society, the UC Davis Center for Biosystematics, Henry A. Jastro and Peter J. Shields Research Scholarships, a UC MEXUS Dissertation Research Grant, and a Fulbright-Garcia Robles Scholarship awarded to JJP and a grant from the U.C. Davis Academic Senate Committee on Research and University Outreach and International Programs awarded to JJP and DP. Funding for Open Access provided by the UC Santa Cruz Open Access Fund. NR 66 TC 0 Z9 0 U1 1 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD MAR PY 2014 VL 4 IS 5 BP 539 EP 553 DI 10.1002/ece3.948 PG 15 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA AB9TY UT WOS:000332139800001 PM 25035796 ER PT J AU Luther, D Greenberg, R AF Luther, David Greenberg, Russell TI Habitat type and ambient temperature contribute to bill morphology SO ECOLOGY AND EVOLUTION LA English DT Article DE Ambient temperature regulation; bill morphology; island syndrome; mangrove; sexual dimorphism; yellow warbler ID SEXUAL-DIMORPHISM; SIZE DIMORPHISM; MARSH SPARROWS; BODY-SIZE; BIRDS; EVOLUTION; HUMMINGBIRDS; ECOLOGY; FINCH; RULE AB Avian bills are iconic structures for the study of ecology and evolution, with hypotheses about the morphological structure of bills dating back to Darwin. Several ecological and physiological hypotheses have been developed to explain the evolution of the morphology of bill shape. Here, we test some of these hypotheses such as the role of habitat, ambient temperature, body size, intraspecific competition, and ecological release on the evolution of bill morphology. Bill morphology and tarsus length were measured from museum specimens of yellow warblers, and grouped by habitat type, sex, and subspecies. We calculated the mean maximum daily temperature for the month of July, the hottest month for breeding specimens at each collecting location. Analysis of covariance models predicted total bill surface area as a function of sex, habitat type, body size, and temperature, and model selection techniques were used to select the best model. Habitat, mangrove forests compared with inland habitats, and climate had the largest effects on bill size. Coastal wetland habitats and island populations of yellow warblers had similar bill morphology, both of which are larger than mainland inland populations. Temperate but not tropical subspecies exhibited sexual dimorphism in bill morphology. Overall, this study provides evidence that multiple environmental factors, such as temperature and habitat, contribute to the evolution of bill morphology. C1 [Luther, David] George Mason Univ, Biol Program, Fairfax, VA 22030 USA. [Greenberg, Russell] Smithsonian Conservat Biol Inst, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Luther, D (reprint author), George Mason Univ, Biol Program, Fairfax, VA 22030 USA. EM dluther@gmu.edu NR 35 TC 3 Z9 3 U1 15 U2 47 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD MAR PY 2014 VL 4 IS 6 BP 699 EP 705 DI 10.1002/ece3.911 PG 7 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA AD0CW UT WOS:000332902900003 PM 24683453 ER PT J AU Stanley, JD Bernasconi, MP Nickerson, GAJ AF Stanley, Jean-Daniel Bernasconi, Maria Pia Nickerson, Graham A. J. TI Large Scarps and Massive Slide on the Briatico-Bivona Shelf, Calabria, Italy: Potential Link with the Destructive September 1905 Earthquake SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE Calabrian Arc; Capo Vaticano peninsula; epicenters; faults; gravity flows; land uplift; sand waves; sediment displacement; seismotectonics; shelf breaks; Tyrrhenian Sea ID SOUTHERN; QUATERNARY; SEA AB A multibeam sonar (MBS) survey of the northern Capo Vaticano shelf between the towns of Briatico and Bivona, Calabria, Italy, has revealed a markedly broken margin offset by three large scarps: the upper scarp (Si) at approximate depths of 16-22 m, the middle scarp (S2) at,similar to 36-58 m, and the deeper scarp (S3) at similar to 88-101 m. The configuration of Si shows high relief to 33 m and a slope to 59 degrees, which suggests a fault or tectonic gravitative origin. Substantial volumes of sediment, mostly sand, are being rapidly transferred from the inner shelf toward and across the upper shelf break, and one could expect a smoothing and burial of the upper scarp, but 10 MBS profiles show the sharp, angular shape of that feature. Some of the mass gravitative deposits just below some headwall scarps that extend to the shelf-slope that break NE of Briatico also reveal very recent origins. Additionally, a massive slide block north of Bivona, similar to 350-400 m in length, appears to have detached from the inner shelf and shifted onto the middle shelf. It is proposed that several of these seafloor features may, in some manner, be associated with the powerful and destructive September 1905 earthquake that affected a large sector of Calabria. Five potential epicenters on the SW margin of Calabria have previously been proposed for that event, and this MBS study area is in proximity to one of those. It is recommended that two localities in the survey area, one NE of Briatico and the other north of Bivona, be selected as test zones for further geological and geophysical analyses. C1 [Stanley, Jean-Daniel] Smithsonian Inst, Geoarchaeol Program, Washington, DC 20013 USA. [Stanley, Jean-Daniel] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Bernasconi, Maria Pia] Univ Calabria, Dipartimento Biol Ecol & Sci Terra DiBEST, I-87036 Cosenza, Italy. [Nickerson, Graham A. J.] Highland Geo Solut, Taymouth, NB E6C1Y2, Canada. RP Bernasconi, MP (reprint author), Univ Calabria, Dipartimento Biol Ecol & Sci Terra DiBEST, Cubo 15B, I-87036 Cosenza, Italy. EM bernasconi@unical.it FU Director's Office and Department of Paleobiology of the National Museum of Natural History; Highland Geo Solutions; RPM Nautical Foundation; University of Calabria (Ministry of Education); Office of Fellowships; Smithsonian Institution, Washington, DC FX Appreciation is expressed to Dr. J. Royal, RPM Nautical Foundation for generously providing ship time and equipment on the R/V Hercules; Captain E. Vella and crew for their valued assistance; and Mr. K. Llewellyn of Highland Geo Solutions for efficient collection of the MBS data during the cruise. The authors thank Mr. W. Boardman for assistance in compiling the final figures in this article, and Mr. P. L. Clemente for editorial assistance and text preparation. Dives were conducted, by personnel of the Nucleo Sommozzatori-Guardia di Finanza of Vibo Valentia Marina, Calabria, through the sponsorship of Commander A. D'Amico. Helpful, constructive, outside reviews were made by Drs. F. Muto, University of Calabria-Rende, and C. Tansi, IRPI-CNR of Cosenza, Calabria. Travel funds for this project (to J.D.S) were provided by the Director's Office and Department of Paleobiology of the National Museum of Natural History, Highland Geo Solutions, and the RPM Nautical Foundation; funds for field work and travel were provided (to M.P.B.) by the University of Calabria (Ministry of Education, Universities and Research grant ex-60%), and by the Office of Fellowships and Grants of the Smithsonian Institution, Washington, DC. NR 38 TC 0 Z9 0 U1 1 U2 3 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 EI 1551-5036 J9 J COASTAL RES JI J. Coast. Res. PD MAR PY 2014 VL 30 IS 2 BP 215 EP 227 DI 10.2112/JCOASTRES-D-13-00158.1 PG 13 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA AD4NY UT WOS:000333229000002 ER PT J AU Merow, C Silander, JA AF Merow, Cory Silander, John A., Jr. TI A comparison of Maxlike and Maxent for modelling species distributions SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE species distribution modelling; occurrence model; presence-only data; probability of presence; resource selection function ID PRESENCE-ONLY DATA; POINT PROCESS MODELS; LOGISTIC-REGRESSION; USE-AVAILABILITY; SELECTION; PROBABILITY; ABSENCE; PERFORMANCE; ECOLOGY; ERRORS AB Understanding species spatial occurrence patterns and their environmental dependence is one of the fundamental goals in ecology and evolution. Often, occurrence models are built with presence-only data because absence data are unavailable. We compare the strengths and limitations of the recently developed presence-only modelling method, Maxlike, with the more widely used Maxent. In spite of disparities highlighted by the developers of Maxlike and Maxent, we show approximate formal relationships between the parameters of Maxlike and Maxent for two scenarios to illustrate their similarity. Using case studies based on real and simulated data, we show how these similarities manifest in practice. We find more similarities than differences between Maxlike and Maxent, including coefficient values, predicted spatial distributions, similarity to presence-absence models, predictive performance and ranking the predicted suitability of cells. Maxlike reliably predicted absolute occurrence probabilities for very large data sets on landscapes where occurrence probability approximately spanned [0,1]. For smaller data sets, the uncertainty in predicted occurrence probability by Maxlike was very large, due to the inherent limitations of presence-only data. In contrast, Maxent is constrained to predicting relative occurrence probabilities or relative occurrence rates unless it is provided with additional information from presence-absence data. Both models can reliably predict relative differences in occurrence probability. The choice of which model to use depends partly on sampling assumptions, which we discuss in detail. Due to limitations of presence-only data, ecologists should typically focus on interpretations relying on relative differences in occurrence probability or relative occurrence rates. We discuss how to remedy a number of concerns about the use of Maxent and how to avoid some potential pitfalls with Maxlike - particularly related to high variance predictions. We conclude that both methods are similarly valuable for understanding and predicting species' distributions in terms of relative differences in occurrence probability when the models are specified carefully. C1 [Merow, Cory] Smithsonian Environm Res Ctr, Edgewater, MD 21307 USA. [Merow, Cory; Silander, John A., Jr.] Univ Connecticut, Storrs, CT 06269 USA. RP Merow, C (reprint author), Smithsonian Environm Res Ctr, 647 ConteesWharf Rd, Edgewater, MD 21307 USA. EM cory.merow@gmail.com FU NSF [1046328, 1137366] FX We thank Jane Elith, John Fieberg, Rune Halvorsen, Sean McMahon, Steven Phillips, Andrew Royle and Matthew Smith for helpful comments on the manuscript. CM acknowledges support from NSF Grant 1046328 to JAS and NSF Grant 1137366 to Sean M. McMahon. NR 44 TC 16 Z9 18 U1 5 U2 109 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 MAR PY 2014 VL 5 IS 3 BP 215 EP 225 DI 10.1111/2041-210X.12152 PG 11 WC Ecology SC Environmental Sciences & Ecology GA AC4UR UT WOS:000332517100003 ER PT J AU Anderson, L Aubourg, E Bailey, S Beutler, F Bolton, AS Brinkmann, J Brownstein, JR Chuang, CH Cuesta, AJ Dawson, KS Eisenstein, DJ Ho, S Honscheid, K Kazin, EA Kirkby, D Manera, M McBride, CK Mena, O Nichol, RC Olmstead, MD Padmanabhan, N Palanque-Delabrouille, N Percival, WJ Prada, F Ross, AJ Ross, NP Sanchez, AG Samushia, L Schlegel, DJ Schneider, DP Seo, HJ Strauss, MA Thomas, D Tinker, JL Tojeiro, R Verde, L Wake, D Weinberg, DH Xu, XY Yeche, C AF Anderson, Lauren Aubourg, Eric Bailey, Stephen Beutler, Florian Bolton, Adam S. Brinkmann, J. Brownstein, Joel R. Chuang, Chia-Hsun Cuesta, Antonio J. Dawson, Kyle S. Eisenstein, Daniel J. Ho, Shirley Honscheid, Klaus Kazin, Eyal A. Kirkby, David Manera, Marc McBride, Cameron K. Mena, O. Nichol, Robert C. Olmstead, Matthew D. Padmanabhan, Nikhil Palanque-Delabrouille, N. Percival, Will J. Prada, Francisco Ross, Ashley J. Ross, Nicholas P. Sanchez, Ariel G. Samushia, Lado Schlegel, David J. Schneider, Donald P. Seo, Hee-Jong Strauss, Michael A. Thomas, Daniel Tinker, Jeremy L. Tojeiro, Rita Verde, Licia Wake, David Weinberg, David H. Xu, Xiaoying Yeche, Christophe TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measuring D-A and H at z=0.57 from the baryon acoustic peak in the Data Release 9 spectroscopic Galaxy sample SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmological parameters; cosmology: observations; dark energy; distance scale; large scale structure of Universe ID DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; LARGE-SCALE STRUCTURE; POWER-SPECTRUM ANALYSIS; PROBING DARK ENERGY; SURVEY IMAGING DATA; CENT DISTANCE; COSMOLOGICAL CONSTANT; REDSHIFT SURVEYS; FLUCTUATIONS AB We present measurements of the angular diameter distance to and Hubble parameter at z = 0.57 from the measurement of the baryon acoustic peak in the correlation of galaxies from the Sloan Digital Sky Survey III Baryon Oscillation Spectroscopic Survey. Our analysis is based on a sample from Data Release 9 of 264 283 galaxies over 3275 square degrees in the redshift range 0.43 < z < 0.70. We use two different methods to provide robust measurement of the acoustic peak position across and along the line of sight in order to measure the cosmological distance scale. We find D-A(0.57) = 1408 +/- 45 Mpc and H(0.57) = 92.9 +/- 7.8 km s(-1) Mpc(-1) for our fiducial value of the sound horizon. These results from the anisotropic fitting are fully consistent with the analysis of the spherically averaged acoustic peak position presented in Anderson et al. Our distance measurements are a close match to the predictions of the standard cosmological model featuring a cosmological constant and zero spatial curvature. C1 [Anderson, Lauren] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Aubourg, Eric] Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu,Obs Paris, Sorbonne Paris, France. [Bailey, Stephen; Beutler, Florian; Ross, Nicholas P.; Schlegel, David J.; Seo, Hee-Jong] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Bolton, Adam S.; Brownstein, Joel R.; Dawson, Kyle S.; Olmstead, Matthew D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Brinkmann, J.] Apache Point Observ, Sunspot, NM 88349 USA. [Chuang, Chia-Hsun; Prada, Francisco] Univ Autonoma Madrid, Inst Fis Teor UAM CSIC, E-28049 Madrid, Spain. [Cuesta, Antonio J.; Padmanabhan, Nikhil] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Eisenstein, Daniel J.; McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Shirley; Xu, Xiaoying] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Honscheid, Klaus; Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Honscheid, Klaus; Weinberg, David H.] Ohio State Univ, CCAPP, Columbus, OH 43210 USA. [Dawson, Kyle S.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Kirkby, David] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Manera, Marc; Nichol, Robert C.; Percival, Will J.; Ross, Ashley J.; Thomas, Daniel; Tojeiro, Rita] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Mena, O.] IFIC CSIC UV, Valencia, Spain. [Palanque-Delabrouille, N.; Yeche, Christophe] CEA, Ctr Saclay, Irfu SPP, F-91191 Gif Sur Yvette, France. [Prada, Francisco] Inst Astrofis Andalucia CSIC, E-18080 Granada, Spain. [Prada, Francisco] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain. [Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Samushia, Lado] Ilia State Univ, Natl Abastumani Astrophys Observ, GE-1060 Tbilisi, Rep of Georgia. [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. [Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Tinker, Jeremy L.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Verde, Licia] ICREA, E-08028 Barcelona, Spain. [Verde, Licia] ICC Univ Barcelona IEEC UB, E-08028 Barcelona, Spain. [Wake, David] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Anderson, L (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM djschlegel@lbl.gov RI Ho, Shirley/P-3682-2014 OI Ho, Shirley/0000-0002-1068-160X FU Alfred P. Sloan Foundation; National Science Foundation; US 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 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. NR 93 TC 64 Z9 65 U1 1 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2014 VL 439 IS 1 BP 83 EP 101 DI 10.1093/mnras/stt2206 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD5MR UT WOS:000333297700026 ER PT J AU Sadowski, A Narayan, R McKinney, JC Tchekhovskoy, A AF Sadowski, Aleksander Narayan, Ramesh McKinney, Jonathan C. Tchekhovskoy, Alexander TI Numerical simulations of super-critical black hole accretion flows in general relativity SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; relativistic processes; methods: numerical; galaxies: jets ID ADVECTION-DOMINATED ACCRETION; RADIATION-MAGNETOHYDRODYNAMIC SIMULATIONS; SUPER-EDDINGTON ACCRETION; ACTIVE GALACTIC NUCLEI; TIDAL DISRUPTION EVENT; ULTRA-FAST OUTFLOWS; 2 DIMENSIONS; DISKS; DISCS; SCHEME AB A new general relativistic radiation magnetohydrodynamical code KORAL is described, which employs the M1 scheme to close the radiation moment equations. The code has been successfully verified against a number of tests. Axisymmetric simulations of super-critical magnetized accretion on non-rotating (a(*) = 0.0) and spinning (a(*) = 0.9) black holes are presented. The accretion rates in the two models are (M) over dot approximate to 100-200 (M) over dot(Edd). These first general relativistic simulations of super-critical black hole accretion are potentially relevant to tidal disruption events and hyper-accreting supermassive black holes in the early Universe. Both simulated models are optically and geometrically thick, and have funnels through which energy escapes in the form of relativistic gas, Poynting flux and radiative flux. The jet is significantly more powerful in the a(*) = 0.9 run. The net energy outflow rate in the two runs correspond to efficiencies of 5 per cent (a(*) = 0) and 33 per cent (a(*) = 0.9), as measured with respect to the mass accretion rate at the black hole. These efficiencies agree well with those measured in previous simulations of non-radiative geometrically thick discs. Furthermore, in the a(*) = 0.9 run, the outflow power appears to originate in the spinning black hole, suggesting that the associated physics is again similar in non-radiative and super-critical accretion flows. While the two simulations are efficient in terms of total energy outflow, both runs are radiatively inefficient. Their luminosities are only similar to 1-10L(Edd), which corresponds to a radiative efficiency similar to 0.1 per cent. Interestingly, most of the radiative luminosity emerges through the funnels where the local radiative flux is highly super-Eddington. C1 [Sadowski, Aleksander; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02134 USA. [McKinney, Jonathan C.] Univ Maryland, Dept Phys, Joint Space Sci Inst, College Pk, MD 20742 USA. [Tchekhovskoy, Alexander] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP Sadowski, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02134 USA. EM asadowski@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NSF [AST1312651]; NASA [NNX11AE16G]; NSF via XSEDE resources [TG-AST080026N, TG-AST100040]; NASA via the High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center FX We thank Juri Poutanen and Ken Ohsuga for useful comments. RN and AS were supported in part by NSF grant AST1312651 and NASA grant NNX11AE16G. We also acknowledge computational support from NSF via XSEDE resources (grant TG-AST080026N to RN and AS, and grant TG-AST100040 to AT), and from NASA (to RN and AS) via the High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 76 TC 51 Z9 51 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 MAR PY 2014 VL 439 IS 1 BP 503 EP 520 DI 10.1093/mnras/stt2479 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD5MR UT WOS:000333297700054 ER PT J AU Landt, H Ward, MJ Elvis, M Karovska, M AF Landt, Hermine Ward, Martin J. Elvis, Martin Karovska, Margarita TI Constraints on the outer radius of the broad emission line region of active galactic nuclei SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: nuclei; quasars: emission lines; infrared: galaxies ID SPECTRAL ENERGY-DISTRIBUTION; OPTIMALLY EMITTING CLOUDS; BLACK-HOLE MASSES; GALAXY 3C 390.3; ACCRETION DISKS; LUMINOSITY RELATIONSHIP; OPTICAL-SPECTRA; INNER RADIUS; DUSTY TORUS; REVERBERATION AB Here we present observational evidence that the broad emission line region (BELR) of active galactic nuclei (AGN) generally has an outer boundary. This was already clear for sources with an obvious transition between the broad and narrow components of their emission lines. We show that the narrow component of the higher-order Paschen lines is absent in all sources, revealing a broad emission line profile with a broad, flat top. This indicates that the BELR is kinematically separate from the narrow emission line region. We use the virial theorem to estimate the BELR outer radius from the flat top width of the unblended profiles of the strongest Paschen lines, Pa alpha and Pa beta, and find that it scales with the ionizing continuum luminosity roughly as expected from photoionization theory. The value of the incident continuum photon flux resulting from this relationship corresponds to that required for dust sublimation. A flat-topped broad emission line profile is produced by both a spherical gas distribution in orbital motion and an accretion disc wind if the ratio between the BELR outer and inner radius is assumed to be less than similar to 100-200. On the other hand, a pure Keplerian disc can be largely excluded, since for most orientations and radial extents of the disc the emission line profile is double-horned. C1 [Landt, Hermine; Ward, Martin J.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Elvis, Martin; Karovska, Margarita] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Landt, H (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. EM hermine.landt@durham.ac.uk FU European Union FX We thank Kirk Korista and Brad Peterson for their comments on an earlier version of this manuscript. HL acknowledges financial support by the European Union through the COFUND scheme. This work is partly 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, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). NR 53 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 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2014 VL 439 IS 1 BP 1051 EP 1062 DI 10.1093/mnras/stu031 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD5MR UT WOS:000333297700093 ER PT J AU Welch, AJ Olson, SL Fleischer, RC AF Welch, Andreanna J. Olson, Storrs L. Fleischer, Robert C. TI Phylogenetic relationships of the extinct St Helena petrel, Pterodroma rupinarum Olson, 1975 (Procellariiformes: Procellariidae), based on ancient DNA SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE cytochromeb; extinction; petrel; phylogeny; Pseudobulweria; Pterodroma; StHelena ID SHEARWATER PUFFINUS; CONSERVATION IMPLICATIONS; INTRODUCED PREDATORS; GENE FLOW; SEABIRD; POPULATION; PSEUDOBULWERIA; ISLAND; EVOLUTION; ATLANTIC AB Palaeontological studies show that three endemic procellariid seabird species became extinct on the remote island of StHelena in the South Atlantic Ocean. At least one of these, Pterodroma rupinarumOlson, 1975, is likely to have survived until human colonization of the island, although it is known only from subfossil bones. Several species of Pterodroma are distributed across the Atlantic, but the skull and bill of Pt.rupinarum were judged to be more similar to the Indo-Pacific Pterodroma rostrata group, which was recently split into the separate genus Pseudobulweria. We used ancient DNA techniques to sequence the mitochondrial cytochromeb gene of the extinct Pt.rupinarum, and conducted phylogenetic analyses to investigate the placement of this enigmatic taxon. In trees constructed using maximum likelihood and Bayesian inference, Pt.rupinarum did not group with Pseudobulweria, but instead fell within a strongly supported clade of Atlantic Pterodroma, including the endangered Black-capped [Pterodroma hasitata (Kuhl, 1820)] and Bermuda [Pterodroma cahow (Nichols & Mowbray, 1916)] petrels, as well as the Macaronesian petrels [Pterodroma madeiraMathews, 1934, Pterodroma feae (Salvadori, 1899) and Pterodroma deserta Mathews, 1934]. Pterodroma rupinarum shared a particularly close relationship with Pt.feae of the Cape Verde Islands, which is also the geographically closest species within the clade. Considering the osteological distinctiveness of Pt.rupinarum it was probably a separate species, or at least a highly diverged population that was isolated for a substantial period of time prior to its extinction.(c) 2013 The Linnean Society of London C1 [Welch, Andreanna J.] SUNY Buffalo, Dept Biol Sci, Buffalo, NY 14260 USA. [Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Fleischer, Robert C.] Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. RP Welch, AJ (reprint author), Univ Durham, Sch Biol & Biomed Sci, Durham DH1 3HP, England. EM andreanna05@gmail.com FU Center for Conservation and Evolutionary Genetics; [NSF-DEB0745604] FX We would like to thank Helen James, Nancy Rotzel, and members of the Center for Conservation and Evolutionary Genetics at the Smithsonian Institution's National Zoological Park for helpful discussion and logistical support. Two reviewers provided useful comments that improved this article. We would like to thank Chris Milensky, Division of Birds, National Museum of Natural History, Smithsonian Institution, for access to samples, and the Center for Computational Resources at the University at Buffalo for access to the high-performance computer cluster. The Center for Conservation and Evolutionary Genetics and NSF-DEB0745604 provided funding for the laboratory work. NR 60 TC 3 Z9 4 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 MAR PY 2014 VL 170 IS 3 SI SI BP 494 EP 505 DI 10.1111/zoj.12078 PG 12 WC Zoology SC Zoology GA AC6CJ UT WOS:000332608300002 ER PT J AU Tan, BK Yassin, G Grimes, P AF Tan, Boon-Kok Yassin, Ghassan Grimes, Paul TI Ultra-Wide Intermediate Bandwidth for High-Frequency SIS Mixers SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Mixers; submillimeter-wave devices; superconducting integrated circuits; system-on-a-chip AB We present a simple method for widening the Intermediate frequency (IF) bandwidth of high frequency superconductor-insulator-superconductor (SIS) mixers. The method only requires a mixer with a single similar to 1 mu m(2) tunnel junction and an IF transformer fabricated with standard printed circuit board technology, avoiding the complexity of requiring several very small tunnel junctions in series or the use of on-chip IF tuning circuits. The method is based on employing a multi-stage microstrip IF transformer to transform the dynamic impedance of the SIS mixer chip to 50 Omega output over a wide IF bandwidth. This method assumes moderately high capacitance junction (75 fF/mu m(2)), and is particularly useful for high frequency SIS mixers. In this paper, we shall first describe the design methodology of the IF transformer using an existing 650 GHz SIS mixer chip design as an illustration and then present the measured IF performance of the mixer. C1 [Tan, Boon-Kok; Yassin, Ghassan] Univ Oxford, Dept Phys Astrophys, Oxford OX1 3RH, England. [Tan, Boon-Kok] Wawasan Open Univ, Inst Res & Innovat, George Town 10050, Malaysia. [Grimes, Paul] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tan, BK (reprint author), Univ Oxford, Dept Phys Astrophys, Oxford OX1 3RH, England. EM tanbk@astro.ox.ac.uk NR 11 TC 2 Z9 2 U1 0 U2 2 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 MAR PY 2014 VL 4 IS 2 SI SI BP 165 EP 170 DI 10.1109/TTHZ.2013.2296567 PG 6 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA AD0VB UT WOS:000332951100006 ER PT J AU Velez-Juarbe, J Domning, DP AF Velez-Juarbe, Jorge Domning, Daryl P. TI FOSSIL SIRENIA OF THE WEST ATLANTIC AND CARIBBEAN REGION. IX. METAXYTHERIUM ALBIFONTANUM, SP NOV. SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID MAMMALIA; MIOCENE; DUGONGINAE; MOROCCO; INDIA AB We describe a new species of the halitheriine dugongid genus Metaxytherium from the late Oligocene of Florida and South Carolina. The new species is represented by cranial and postcranial material, including parts of the axial and appendicular skeleton. Metaxytherium albifontanum, sp. nov., differs from other species of Metaxytherium by the following unique combination of plesiomorphic and derived characters: posterior end of nasal process of premaxilla broad and flat relative to what is observed in most other members of the genus (somewhat resembling M. subapenninum); ventral extremity of jugal under posterior edge of orbit (character 85[1]) (shared with M. krahuletzi); exoccipitals separated in dorsal midline (character 66[1]) (shared with all other species in the genus, except some M. krahuletzi); and innominate with acetabulum (nearly lost or lost in M. crataegense, M. floridanum, M. serresii). This new species was sympatric with two dugongines, Crenatosiren olseni and Dioplotherium manigaulti. The small tusks and cranial morphology of M. albifontanum, sp. nov., indicate that it was likely a consumer of small seagrasses. Our phylogenetic analysis is consistent with previous ones in placing Hydrodamalinae within a paraphyletic Metaxytherium spp. and placing the Metaxytherium spp. + Hydrodamalinae clade as the sister group to Dugonginae. Metaxytherium albifontanum, sp. nov., is the oldest known member of its genus; this might indicate that the group originated in the West Atlantic and Caribbean region and later dispersed to the Old World Tethys region. SUPPLEMENTAL DATASupplemental materials are available for this article for free at www.tandfonline.com/UJVP. C1 [Velez-Juarbe, Jorge; Domning, Daryl P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Domning, Daryl P.] Howard Univ, Dept Anat, Lab Evolutionary Biol, Washington, DC 20059 USA. RP Velez-Juarbe, J (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM velezjuarbe@gmail.com; ddomning@howard.edu FU WBHR-LSAMP Bridge; National Museum of Natural History; Smithsonian Institution; Remington Kellogg Fund, Smithsonian Institution; NSF Earth Sciences [0929117] FX We thank R. Hulbert and K. Auffenberg (FLMNH), J. Knight and D. Cicimurri (SCSM), and A. Sanders (ChM) for access and loans of specimens under their care. J.V.J. was partially supported by the WBHR-LSAMP Bridge to the Doctorate Program at Howard University, a predoctoral fellowship from the National Museum of Natural History, Smithsonian Institution, and the Remington Kellogg Fund, Smithsonian Institution. Ongoing work by D.P.D. and J.V.J. is supported by NSF Earth Sciences grant no. 0929117. We wish to thank N. D. Pyenson (USNM) for comments on the morphology of the specimens and guidance to J.V.J. during his fellowship at NMNH. Alan and Jane Hopkins are gratefully acknowledged for the collecting of ChM PV4757. This work benefited from the comments and corrections of I. Zalmout (King Saud University, Riyadh, Saudi Arabia) and an anonymous reviewer. NR 53 TC 11 Z9 11 U1 0 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD MAR 1 PY 2014 VL 34 IS 2 BP 444 EP 464 DI 10.1080/02724634.2013.799072 PG 21 WC Paleontology SC Paleontology GA AC0FY UT WOS:000332171400014 ER PT J AU Lamborg, C Bowman, K Hammerschmidt, C Gilmour, C Munson, K Selin, N Tseng, CM AF Lamborg, Carl Bowman, Katlin Hammerschmidt, Chad Gilmour, Cindy Munson, Kathleen Selin, Noelle Tseng, Chun-Mao TI MERCURY in the Anthropocene Ocean SO OCEANOGRAPHY LA English DT Article ID SOUTH CHINA SEA; ELEMENTAL MERCURY; METHYLMERCURY; DEPOSITION; EMISSIONS; WATERS; FISH AB The toxic metal mercury is present only at trace levels in the ocean, but it accumulates in fish at concentrations high enough to pose a threat to human and environmental health. Human activity has dramatically altered the global mercury cycle, resulting in loadings to the ocean that have increased by at least a factor of three from pre-anthropogenic levels. Loadings are likely to continue to increase as a result of higher atmospheric emissions and other factors related to global environmental change. The impact that these loadings will have on the production of methylated mercury (the form that accumulates in fish) is unclear. In this article, we summarize the biogeochemistry of mercury in the ocean and use this information to examine past impacts that human activity has had on the cycling of this toxic metal. We also highlight ways in which the mercury cycle may continue to be affected and its potential impact on mercury in fish. C1 [Lamborg, Carl] Woods Hole Oceanog Inst WHOI, Dept Marine Chem & Geochem, Woods Hole, MA USA. [Bowman, Katlin; Hammerschmidt, Chad] Wright State Univ, Dept Earth & Environm Sci, Dayton, OH 45435 USA. [Gilmour, Cindy] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Munson, Kathleen] WHOI, Dept Marine Chem & Geochem, Woods Hole, MA USA. [Selin, Noelle] MIT, Engn Syst Div, Cambridge, MA 02139 USA. [Selin, Noelle] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [Tseng, Chun-Mao] Natl Taiwan Univ, Inst Oceanog, Taipei, Taiwan. RP Lamborg, C (reprint author), Woods Hole Oceanog Inst WHOI, Dept Marine Chem & Geochem, Woods Hole, MA USA. EM clamborg@whoi.edu RI Selin, Noelle/A-4158-2008; Hammerschmidt, Chad/M-3139-2014; Gilmour, Cynthia/G-1784-2010; OI Selin, Noelle/0000-0002-6396-5622; Gilmour, Cynthia/0000-0002-1720-9498; TSENG, CHUN-MAO/0000-0003-1922-3936 FU US National Science Foundation Chemical Oceanography program; National Taiwan University [NTU 102R3252] FX We thank Elsie Sunderland, Rob Mason, Ken Johnson, and Bill Landing for helpful discussions. The US GEOTRACES research reported herein was supported by the US National Science Foundation Chemical Oceanography program. National Taiwan University also supported this work through the Drunken Moon Lake Scientific Integrated Scientific Research Platform grant, NTU#102R3252. NR 34 TC 12 Z9 12 U1 1 U2 37 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD MAR PY 2014 VL 27 IS 1 BP 76 EP 87 PG 12 WC Oceanography SC Oceanography GA AC7YK UT WOS:000332750000012 ER PT J AU Gelfand, JD Slane, PO Temim, T AF Gelfand, J. D. Slane, P. O. Temim, T. TI The properties of the progenitor, neutron star, and pulsar wind in the supernova remnant Kes 75 SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT XMM Newton Conference CY MAY 22-24, 2013 CL Madrid, SPAIN DE ISM: (Kes 75); pulsars: individual (J1846-0258); supernova remnants ID HIGH MAGNETIC-FIELD; SPECTRAL EVOLUTION; PSR J1846-0258; BRAKING INDEX; NEBULAE; YOUNG; SPECTROSCOPY; KESTEVEN-75; OUTBURST; MODEL AB By studying composite supernova remnants (SNRs), remnants which contain a pulsar wind nebula (PWN), it is possible to estimate physical properties of the progenitor explosion, central neutron star, and its pulsar wind that are difficult to measure directly. This is best done by fitting the dynamical and broadband spectral properties of a PWN with an evolutionary model for a PWN inside an SNR. We apply such a model to the composite SNR Kes 75, whose associated pulsar PSR J1846-0258 is thought to have an extremely strong surface magnetic field. If approximate to 3 M of mass was ejected in the supernova, our model suggests a normal or slightly subenergetic supernova in a low density environment. Additionally, for the measured pre-outburst braking index of p = 2.65, our model prefers an age of approximate to 430 years and an initial spin period P-0 approximate to 0.2 s. Lastly, the magnetization of the pulsar wind and energy spectrum of particles injected at the termination shock are similar to those observed from other PWNe powered by less magnetized neutron stars. While further study is needed to verify these results, they are nominally inconsistent with strong neutron star magnetic fields resulting from very fast initial rotation. ((c) 2014 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) C1 [Gelfand, J. D.] NYU Abu Dhabi, Abu Dhabi, U Arab Emirates. [Gelfand, J. D.] New York Univ, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Slane, P. O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Temim, T.] Goddard Space Flight Ctr, Greenbelt, MD USA. RP Gelfand, JD (reprint author), NYU Abu Dhabi, POB 129188, Abu Dhabi, U Arab Emirates. EM jg168@nyu.edu RI Gelfand, Joseph/F-1110-2015; OI Gelfand, Joseph/0000-0003-4679-1058; Temim, Tea/0000-0001-7380-3144 FU NASA through JPL/Caltech (RSA) [1479542] FX Support for this work was provided by NASA through an award issued by JPL/Caltech (RSA No. 1479542). NR 22 TC 4 Z9 4 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD MAR PY 2014 VL 335 IS 3 BP 318 EP 323 DI 10.1002/asna.201312039 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC2MG UT WOS:000332334600018 ER PT J AU Hong, T AF Hong, Terry TI The Great White Way: Race and the Broadway Musical. SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20004 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20004 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 MAR 1 PY 2014 VL 139 IS 4 BP 94 EP 94 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA AC4LT UT WOS:000332493500158 ER PT J AU Baker, JL Bielawski, JP Maynard, TM Wood, B AF Baker, Jennifer L. Bielawski, Joseph P. Maynard, Thomas M. Wood, Bernard TI Dental evolution: Patterns of sequence evolution within the primate lineage suggestive of positive selection on genes involved in tooth growth and morphology SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [Baker, Jennifer L.] George Washington Univ, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Baker, Jennifer L.; Wood, Bernard] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Bielawski, Joseph P.] Dalhousie Univ, Dept Biol, Halifax, NS, Canada. [Bielawski, Joseph P.] Dalhousie Univ, Dept Math & Stat, Halifax, NS, Canada. [Maynard, Thomas M.] George Washington Univ, GW Inst Neurosci, Washington, DC 20052 USA. [Maynard, Thomas M.] George Washington Univ, Dept Pharmacol & Physiol, Washington, DC 20052 USA. [Wood, Bernard] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 71 EP 72 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100036 ER PT J AU Chirchir, H Kivell, TL Ruff, CB Hublin, JJ Richmond, BG AF Chirchir, Habiba Kivell, Tracy L. Ruff, Christopher B. Hublin, Jean-Jacques Richmond, Brian G. TI The evolution of trabecular bone density in humans SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [Chirchir, Habiba; Richmond, Brian G.] Smithsonian Inst, Human Origins Program, Washington, DC 20560 USA. [Kivell, Tracy L.] Univ Kent, Sch Anthropol & Conservat, Canterbury CT2 7NZ, Kent, England. [Ruff, Christopher B.] Johns Hopkins Univ, Sch Med, Ctr Funct Anat & Evolut, Baltimore, MD 21218 USA. [Kivell, Tracy L.; Hublin, Jean-Jacques] Max Planck Inst Human Evolut, Dept Human Evolut, Leipzig, Germany. [Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. NR 0 TC 0 Z9 0 U1 2 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 93 EP 93 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100132 ER PT J AU Crofoot, MC Kays, R Alavi, S Wikelski, M AF Crofoot, Margaret C. Kays, Roland Alavi, Shauhin Wikelski, Martin TI Democracy or despotism? How do baboons decide? SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [Crofoot, Margaret C.] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [Crofoot, Margaret C.; Alavi, Shauhin] Smithsonian Trop Res Inst, Balboa, Panama. [Kays, Roland] North Carolina Museum Nat Sci, Nat Res Ctr, Raleigh, NC 27601 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 99 EP 100 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100159 ER PT J AU Dingwall, HL Tocheri, MW Awe, RD Sutikna, T Saptomo, EW Jatmiko Wasisto, S Jungers, WL AF Dingwall, Heather L. Tocheri, Matthew W. Awe, Rokus Due Sutikna, Thomas Saptomo, E. Wahyu Jatmiko Wasisto, Sri Jungers, William L. TI Comparative morphology of the proximal hallucal phalanges of Homo floresiensis SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [Dingwall, Heather L.] Harvard Univ, Cambridge, MA 02138 USA. [Tocheri, Matthew W.] Natl Museum Nat Hist, Human Origins Program, Dept Anthropol, Smithsonian Inst, Washington, DC USA. [Jungers, William L.] SUNY Stony Brook, Med Ctr, Dept Anat Sci, Stony Brook, NY USA. NR 0 TC 1 Z9 1 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 106 EP 106 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100190 ER PT J AU Foerster, S Ali, N Cords, M Monfort, SL AF Foerster, Steffen Ali, Nadya Cords, Marina Monfort, Steven L. TI Social network structure in female forest guenons (Cercopithecus mitis): Ecological and physiological correlates SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [Foerster, Steffen; Ali, Nadya] Columbia Univ, Barnard Coll, New York, NY 10027 USA. [Foerster, Steffen; Cords, Marina] Columbia Univ, New York, NY 10027 USA. [Monfort, Steven L.] Smithsonian Inst, Conservat Biol Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 2 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 118 EP 118 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100243 ER PT J AU Early, EDG AF Early, Emily D. Goble TI The changing landscape of Pliocene Baringo SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [Early, Emily D. Goble] Smithsonian, Human Origins Program, Phoenix Coll, Dept Anthropol, Washington, DC USA. 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 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 126 EP 126 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100277 ER PT J AU Kralick, AE Tocheri, MW AF Kralick, Alexandra E. Tocheri, Matthew W. TI A 3D quantitative comparative analysis of wrist morphology among western and eastern gorillas SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [Kralick, Alexandra E.] George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. [Kralick, Alexandra E.; Tocheri, Matthew W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 161 EP 161 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100432 ER PT J AU Ledogar, JA Smith, AL Benazzi, S Weber, GW Spencer, MA Carlson, KB Mcnulty, KP Dechow, PC Grosse, IR Ross, CF Richmond, BG Wright, BW Wang, Q Byron, C Slice, DE Carlson, KJ De Ruiter, DJ Berger, LR Tamvada, K Smith, LCP Berthaume, MA Strait, DS AF Ledogar, Justin A. Smith, Amanda L. Benazzi, Stefano Weber, Gerhard W. Spencer, Mark A. Carlson, Keely B. Mcnulty, Kieran P. Dechow, Paul C. Grosse, Ian R. Ross, Callum F. Richmond, Brian G. Wright, Barth W. Wang, Qian Byron, Craig Slice, Dennis E. Carlson, Kristian J. De Ruiter, Darryl J. Berger, Lee R. Tamvada, Kelli Smith, Leslie C. Pryor Berthaume, Michael A. Strait, David S. TI Constraints on feeding biomechanics in Australopithecus sediba SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [Ledogar, Justin A.; Smith, Amanda L.; Tamvada, Kelli; Strait, David S.] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Benazzi, Stefano] Max Planck Inst Evolutionare Anthropol, Dept Human Evolut, D-04103 Leipzig, Germany. [Weber, Gerhard W.; Slice, Dennis E.] Univ Vienna, Dept Anthropol, A-1010 Vienna, Austria. [Spencer, Mark A.] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. [Carlson, Keely B.; De Ruiter, Darryl J.] Texas A&M Univ, Dept Anthropol, College Stn, TX 77843 USA. [Mcnulty, Kieran P.] Univ Minnesota, Dept Anthropol, Minneapolis, MN 55455 USA. [Dechow, Paul C.; Smith, Leslie C. Pryor] Texas A&M Univ, Baylor Coll Dent, Dept Biomed Sci, College Stn, TX 77843 USA. [Grosse, Ian R.] Univ Massachusetts, Dept Mech & Ind Engn, Amherst, MA 01003 USA. [Ross, Callum F.] Univ Chicago, Dept Organismal Biol & Anat, Chicago, IL 60637 USA. [Richmond, Brian G.] Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, St Louis, MO 63130 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Wright, Barth W.] Kansas City Univ Med & Biosci, Dept Anat, Kansas City, MO USA. [Wang, Qian] Mercer Univ, Sch Med, Div Basic Med Sci, Macon, GA USA. [Byron, Craig] Mercer Univ, Dept Biol, Macon, GA 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. [Carlson, Kristian J.; De Ruiter, Darryl J.; Berger, Lee R.] Univ Witwatersrand, Evolutionary Studies Inst, ZA-2050 Johannesburg, South Africa. [Carlson, Kristian J.] Indiana Univ, Dept Anthropol, Bloomington, IN 47405 USA. [Berthaume, Michael A.] Univ Hull, Dept Engn, Kingston Upon Hull HU6 7RX, N Humberside, England. [Berthaume, Michael A.] Univ Massachusetts, Dept Anthropol, Amherst, MA 01003 USA. RI Weber, Gerhard/F-2583-2010 NR 0 TC 0 Z9 0 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 166 EP 167 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100458 ER PT J AU O'Mara, T AF O'Mara, Teague TI Ring-tailed lemurs and the evolution of the primate juvenile period SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [O'Mara, Teague] Univ Konstanz, Dept Biol, Dept Migrat & Immunoecol, Max Planck Inst Ornithol, Constance, Germany. [O'Mara, Teague] Smithsonian Trop Res Inst, Balboa, Panama. NR 0 TC 0 Z9 0 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 199 EP 199 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100600 ER PT J AU Ostrofsky, KR Williams, SA Churchill, SE Berger, LR Richmond, BG AF Ostrofsky, Kelly R. Williams, Scott A. Churchill, Steven E. Berger, Lee R. Richmond, Brian G. TI Australopith lumbar vertebral morphology: Insights from Australopithecus sediba SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [Ostrofsky, Kelly R.; Richmond, Brian G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Williams, Scott A.] NYU, Dept Anthropol, Ctr Study Human Origins, New York, NY 10003 USA. [Williams, Scott A.] New York Consortium Evolutionary Primatol, New York, NY USA. [Churchill, Steven E.] Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27706 USA. [Churchill, Steven E.; Berger, Lee R.] Univ Witwatersrand, Evolutionary Studies Inst, ZA-2050 Johannesburg, South Africa. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 202 EP 202 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100613 ER PT J AU Ramirez, SM Campbell, CJ Wright, SJ Bartlett, TQ AF Ramirez, Stephanie M. Campbell, Christina J. Wright, S. J. Bartlett, Thad Q. TI The effects of resource availability on the diet and activity budget of female Spider Monkeys (Ateles geoffroyi) on Barro Colorado Island (BCI), Panama SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [Ramirez, Stephanie M.; Bartlett, Thad Q.] Univ Texas San Antonio, Dept Anthropol, San Antonio, TX USA. [Campbell, Christina J.] Calif State Univ Northridge, Dept Anthropol, Northridge, CA 91330 USA. Smithsonian Trop Res Inst, Balboa, Panama. RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 0 TC 0 Z9 0 U1 1 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 216 EP 216 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100676 ER PT J AU Richmond, BG Hatala, KG Behrensmeyer, AK Bobe, R Braun, DR Dingwall, HL Green, DJ Kiura, P Ostrofsky, K Roach, NT Villmoare, BA Wunderlich, RE Harris, JWK AF Richmond, Brian G. Hatala, Kevin G. Behrensmeyer, Anna K. Bobe, Rene Braun, David R. Dingwall, Heather L. Green, David J. Kiura, Purity Ostrofsky, Kelly Roach, Neil T. Villmoare, Brian A. Wunderlich, Roshna E. Harris, John W. K. TI Hominin size, behavior, and ecology based on 1.5-million-year-old footprint assemblages from Ileret, Kenya SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [Richmond, Brian G.; Hatala, Kevin G.; Bobe, Rene; Braun, David R.; Ostrofsky, Kelly; Roach, Neil T.; Villmoare, Brian A.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Behrensmeyer, Anna K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Dingwall, Heather L.] Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA. [Green, David J.] Midwestern Univ, Dept Anat, Downers Grove, IL USA. [Wunderlich, Roshna E.] James Madison Univ, Dept Biol, Harrisonburg, VA 22807 USA. [Harris, John W. K.] Rutgers State Univ, Dept Anthropol, Piscataway, NJ 08855 USA. NR 0 TC 0 Z9 0 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 221 EP 222 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100698 ER PT J AU Ross, AC Power, ML AF Ross, Abigail C. Power, Michael L. TI Nutritional quality and biological significance of foods consumed by Coquerel's sifaka (Propithecus coquereli) mothers during lactation SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [Ross, Abigail C.] Univ Toronto, Dept Anthropol, Toronto, ON M5S 1A1, Canada. [Power, Michael L.] Smithsonian Conservat Biol Inst, Nutr Lab, Conservat Ecol Ctr, Front Royal, VA USA. NR 0 TC 0 Z9 0 U1 5 U2 14 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 225 EP 225 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100714 ER PT J AU Villmoare, BA Ledogar, JA Smith, A Strait, D Senck, S Weber, G Benazzi, S Spencer, M Dechow, P Grosse, I Ross, C Wright, B Wang, Q Byron, C Slice, D Richmond, BG AF Villmoare, Brian A. Ledogar, Justin A. Smith, Amanda Strait, David Senck, Sasha Weber, Gerhard Benazzi, Stefano Spencer, Mark Dechow, Paul Grosse, Ian Ross, Callum Wright, Barth Wang, Qian Byron, Craig Slice, Dennis Richmond, Brian G. TI Facial biomechanics of Australopithecus afarensis based on AL 444-2 SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [Villmoare, Brian A.; Richmond, Brian G.] George Washinton Univ, Ctr Adv Study Hominid Paleobiol, Washington, DC USA. [Ledogar, Justin A.; Smith, Amanda; Strait, David] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Senck, Sasha] Univ Appl Sci, Upper Austria, Spain. [Weber, Gerhard; Slice, Dennis] Univ Vienna, Dept Anthropol, A-1010 Vienna, Austria. [Benazzi, Stefano] Max Planck Inst Evolutionary Anthropol, Dept Human Evolut, Leipzig, Germany. [Spencer, Mark] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. [Dechow, Paul] Texas A&M Univ, Baylor Coll Dent, Dept Biomed Sci, College Stn, TX 77843 USA. [Grosse, Ian] Univ Massachusetts, Dept Mech & Ind Engn, Amherst, MA 01003 USA. [Ross, Callum] Univ Chicago, Dept Organismal Biol & Anat, Chicago, IL 60637 USA. [Wright, Barth] Kansas City Univ Med & Biosci, Dept Anat, Kansas City, KS USA. [Wang, Qian] Mercer Univ, Sch Med, Div Basic Med Sci, Macon, GA USA. [Byron, Craig] Mercer Univ, Dept Biol, Macon, GA USA. [Slice, Dennis] Florida State Univ, Sch Computat Sci, Tallahassee, FL 32306 USA. [Slice, Dennis] Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Villmoare, Brian A.] UCL, Dept Anthropol, London WC1E 6BT, England. NR 0 TC 0 Z9 0 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 262 EP 262 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100879 ER PT J AU Williams, EM Chai, H Richmond, BG AF Williams, Erin Marie Chai, Herzl Richmond, Brian G. TI The effects of stone toughness on manual force distribution during stone tool production SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 83rd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 08-12, 2014 CL Calgary, CANADA SP Amer Assoc Phys Anthropologists C1 [Williams, Erin Marie] Chatham Univ, Dept Biol, Pittsburgh, PA USA. [Chai, Herzl] Tel Aviv Univ, Sch Mech Engn, IL-69978 Tel Aviv, Israel. [Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAR PY 2014 VL 153 SU 58 SI SI BP 273 EP 273 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AA6RH UT WOS:000331225100929 ER PT J AU Conrad, JL Head, JJ Carrano, MT AF Conrad, Jack L. Head, Jason J. Carrano, Matthew T. TI Unusual Soft-Tissue Preservation of a Crocodile Lizard (Squamata, Shinisauria) From the Green River Formation (Eocene) and Shinisaur Relationships SO ANATOMICAL RECORD-ADVANCES IN INTEGRATIVE ANATOMY AND EVOLUTIONARY BIOLOGY LA English DT Article DE shinisaur; fossil skin; Eocene; Anguimorpha; phylogeny ID MOLECULAR PHYLOGENETICS; ANGUID LIZARDS; BALTIC AMBER; EVOLUTION; SNAKES; ANGUIMORPHA; REPTILIA; CHINA; ADRIOSAURUS; SYSTEMATICS AB We describe an unusual squamate fossil from the Green River Formation (Uintan, Eocene) from the Piceance Creek Basin, Colorado, USA. The new specimen, USNM PAL 540708, is a small fossil squamate skin lacking skeletal elements. It is preserved as a part and counterpart in fine-grained limestone. Recovery of a fossil organism's skin (not a shed, but a true skin) is unusual and is most often accompanied by bone preservation. Phylogenetic analysis of a combined morphology (phenotype) and genetic data set reveals that USNM PAL 540708 is a shinisaur and reaffirms that shinisaurs are more closely related to varanids than to Xenosaurus. Shinisaur fossils are very rare, with only three species having been described (Dalinghosaurus longidigitus, Bahndwivici ammoskius, and Merkurosaurus ornatus). Despite differences in the relative size of scales, the new fossil demonstrates that shinisaurs have remained unchanged in the distribution of scales and patterns of scale size during the Cenozoic. This, paired with the osteological similarity between another Green River fossil (Bahndwivici ammoskius) demonstrates considerable overall conservatism within shinisaurs over the past 50 million years. Anat Rec, 297:545-559, 2014. (c) 2014 Wiley Periodicals, Inc. C1 [Conrad, Jack L.] NYIT Coll Osteopath Med, Dept Anat, Old Westbury, NY 10024 USA. [Conrad, Jack L.] Amer Museum Nat Hist, Dept Vertebrate Paleontol, New York, NY 10024 USA. [Head, Jason J.] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE USA. [Carrano, Matthew T.] Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20560 USA. RP Conrad, JL (reprint author), NYIT Coll Osteopath Med, Dept Anat, Northern Blvd,Cent Pk West & 79th St, Old Westbury, NY 10024 USA. EM jack.conrad@gmail.com RI Carrano, Matthew/C-7601-2011; OI Carrano, Matthew/0000-0003-2129-1612; Head, Jason/0000-0002-2237-6901 NR 81 TC 2 Z9 2 U1 0 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1932-8486 EI 1932-8494 J9 ANAT REC JI Anat. Rec. PD MAR PY 2014 VL 297 IS 3 SI SI BP 545 EP 559 DI 10.1002/ar.22868 PG 15 WC Anatomy & Morphology SC Anatomy & Morphology GA AA9CF UT WOS:000331390600015 PM 24482393 ER PT J AU Huber, D Aguirre, VS Matthews, JM Pinsonneault, MH Gaidos, E Garcia, RA Hekker, S Mathur, S Mosser, B Torres, G Bastien, FA Basu, S Bedding, TR Chaplin, WJ Demory, BO Fleming, SW Guo, Z Mann, AW Rowe, JF Serenelli, AM Smith, MA Stello, D AF Huber, Daniel Aguirre, Victor Silva Matthews, Jaymie M. Pinsonneault, Marc H. Gaidos, Eric Garcia, Rafael A. Hekker, Saskia Mathur, Savita Mosser, Benoit Torres, Guillermo Bastien, Fabienne A. Basu, Sarbani Bedding, Timothy R. Chaplin, William J. Demory, Brice-Olivier Fleming, Scott W. Guo, Zhao Mann, Andrew W. Rowe, Jason F. Serenelli, Aldo M. Smith, Myron A. Stello, Dennis TI REVISED STELLAR PROPERTIES OF KEPLER TARGETS FOR THE QUARTER 1-16 TRANSIT DETECTION RUN SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; planetary systems; stars: fundamental parameters; stars: oscillations; techniques: photometric ID LOW-MASS STARS; SOLAR-LIKE OSCILLATIONS; SUN-LIKE STAR; CANDIDATE HOST STARS; R-CIRCLE-PLUS; GENEVA-COPENHAGEN SURVEY; MULTIPLE-PLANET SYSTEMS; RED GIANT STARS; 1ST 4 MONTHS; TIMING VARIATIONS AB We present revised properties for 196,468 stars observed by the NASA Kepler mission and used in the analysis of Quarter 1-16 (Q1-Q16) data to detect and characterize transiting planets. The catalog is based on a compilation of literature values for atmospheric properties (temperature, surface gravity, and metallicity) derived from different observational techniques (photometry, spectroscopy, asteroseismology, and exoplanet transits), which were then homogeneously fitted to a grid of Dartmouth stellar isochrones. We use broadband photometry and asteroseismology to characterize 11,532 Kepler targets which were previously unclassified in the Kepler Input Catalog (KIC). We report the detection of oscillations in 2762 of these targets, classifying them as giant stars and increasing the number of known oscillating giant stars observed by Kepler by similar to 20% to a total of similar to 15,500 stars. Typical uncertainties in derived radii and masses are similar to 40% and similar to 20%, respectively, for stars with photometric constraints only, and 5%-15% and similar to 10% for stars based on spectroscopy and/or asteroseismology, although these uncertainties vary strongly with spectral type and luminosity class. A comparison with the Q1-Q12 catalog shows a systematic decrease in radii of M dwarfs, while radii for K dwarfs decrease or increase depending on the Q1-Q12 provenance (KIC or Yonsei-Yale isochrones). Radii of F-G dwarfs are on average unchanged, with the exception of newly identified giants. The Q1-Q16 star properties catalog is a first step toward an improved characterization of all Kepler targets to support planet-occurrence studies. C1 [Huber, Daniel; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huber, Daniel; Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA. [Aguirre, Victor Silva; Bedding, Timothy R.; Chaplin, William J.; Stello, Dennis] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Matthews, Jaymie M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Pinsonneault, Marc H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Gaidos, Eric] Univ Hawaii Manoa, Dept Geol & Geophys, Honolulu, HI 96822 USA. [Garcia, Rafael A.] Univ Paris 07, IRFU SAp, Ctr Saclay, Lab AIM,CEA DSM CNRS, F-91191 Gif Sur Yvette, France. [Hekker, Saskia] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Mathur, Savita] Space Sci Inst, Boulder, CO 80301 USA. [Mosser, Benoit] Univ Paris 06, Univ Denis, Observ Paris, LESIA,CNRS, F-92195 Meudon, France. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bastien, Fabienne A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Bedding, Timothy R.; Stello, Dennis] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Chaplin, William J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Demory, Brice-Olivier] MIT, Dept Phys, Cambridge, MA 02139 USA. [Fleming, Scott W.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Guo, Zhao] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA. [Mann, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Serenelli, Aldo M.] Inst Ciencias Espacio CSIC IEEC, Fac Ciencias, E-08193 Bellaterra, Spain. [Smith, Myron A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Huber, D (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM daniel.huber@nasa.gov OI Fleming, Scott/0000-0003-0556-027X; Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661; Demory, Brice-Olivier/0000-0002-9355-5165; Garcia, Rafael/0000-0002-8854-3776; Serenelli, Aldo/0000-0001-6359-2769 FU NASA [NNX13AE70G, NNX12AE17G]; Kepler Participating Scientist Program; NSF [AST-1105930]; Netherlands organisation for Scientific Research; ERC [338251]; NASA Harriet Jenkins Fellowship and a Vanderbilt Provost Graduate Fellowship; UK Science and Technology Facilities Council (STFC); MICINN [AYA2011-24704]; ESF EUROCORES Program EuroGENESIS (MICINN) [EUI2009-04170]; Danish National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler); European Research Council [267864]; National Aeronautics and Space Administration; National Science Foundation FX We thank Lars Buchhave, Bill Cochran, Jonas Debosscher, Joris De Ridder, Mathieu Havel, Ulrich Kolb, Dave Latham, Mikkel Lund, Phil Muirhead, and Angie Wolfgang for helpful discussions and comments. Funding for the Kepler mission is provided by NASA's Science Mission Directorate. D. H. acknowledges support by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA and support by the Kepler Participating Scientist Program. S. B. acknowledges support from NSF grant AST-1105930 and NASA grant NNX13AE70 G. S. H. acknowledges financial support from the Netherlands organisation for Scientific Research and ERC starting grant No. 338251 (Stellar Ages). S. M. acknowledges support from the NASA grant NNX12AE17G. F. A. B. acknowledges support from a NASA Harriet Jenkins Fellowship and a Vanderbilt Provost Graduate Fellowship. W. J. C. acknowledges support from the UK Science and Technology Facilities Council (STFC). A. M. S. is supported by the MICINN grant AYA2011-24704 and by the ESF EUROCORES Program EuroGENESIS (MICINN grant EUI2009-04170). Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement no.: 267864). This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the NASA 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. NR 172 TC 169 Z9 169 U1 7 U2 30 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 MAR PY 2014 VL 211 IS 1 AR 2 DI 10.1088/0067-0049/211/1/2 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB9DN UT WOS:000332090200002 ER PT J AU Trabert, E Beiersdorfer, P Brickhouse, NS Golub, L AF Traebert, Elmar Beiersdorfer, Peter Brickhouse, Nancy S. Golub, Leon TI HIGH-RESOLUTION LABORATORY SPECTRA ON THE lambda 131 CHANNEL OF THE AIA INSTRUMENT ON BOARD THE SOLAR DYNAMICS OBSERVATORY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atomic data; methods: laboratory: atomic; Sun: corona; Sun: UV radiation; techniques: spectroscopic ID EXTREME-ULTRAVIOLET REGION; ATOMIC DATABASE; EMISSION-LINES; FE-VII; GRATING SPECTROMETER; X-RAY; CHIANTI; ANGSTROM; ELEMENTS; SDO/AIA AB Extreme ultraviolet spectra of C, O, F, Ne, Si, S, Ar, Ca, Fe, and Ni have been excited in an electron beam ion trap and studied with much higher resolution than available on Solar Dynamics Observatory (SDO) in order to ascertain the spectral composition of the SDO observations. We presently show our findings in the wavelength range 124-134 angstrom, which encompasses the lambda 131 observation channel of the Atmospheric Imaging Assembly (AIA). While the general interpretation of the spectral composition of the lambda 131 Fe channel is being corroborated, a number of new lines have been observed that might help to improve the diagnostic value of the SDO/AIA data. C1 [Traebert, Elmar; Beiersdorfer, Peter] Lawrence Livermore Natl Lab, Div Phys, Livermore, CA 94550 USA. [Traebert, Elmar] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany. [Brickhouse, Nancy S.; Golub, Leon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Trabert, E (reprint author), Lawrence Livermore Natl Lab, Div Phys, Livermore, CA 94550 USA. FU U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; Solar and Heliospherical Physics Program of the National Aeronautics and Space Administration [NNH10AN31I]; German Research Association (DFG) [Tr171/18, Tr171/19] FX This work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344 and was supported by the Solar and Heliospherical Physics Program of the National Aeronautics and Space Administration under award NNH10AN31I. E. T. acknowledges support from the German Research Association (DFG) (grants Tr171/18 and Tr171/19). NR 26 TC 5 Z9 5 U1 1 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 MAR PY 2014 VL 211 IS 1 AR 14 DI 10.1088/0067-0049/211/1/14 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB9DN UT WOS:000332090200014 ER PT J AU Appelhans, MS Wen, J Wood, KR Allan, GJ Zimmer, EA Wagner, WL AF Appelhans, Marc S. Wen, Jun Wood, Kenneth R. Allan, Gerard J. Zimmer, Elizabeth A. Wagner, Warren L. TI Molecular phylogenetic analysis of Hawaiian Rutaceae (Melicope, Platydesma and Zanthoxylum) and their different colonization patterns SO BOTANICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Pelea; Hawaiian Islands; dispersal; Rutaceae.; Pacific biogeography; colonization events ID CYRTANDRA GESNERIACEAE; SANDALWOODS SANTALUM; RETICULATE EVOLUTION; CHLOROPLAST DNA; BIOGEOGRAPHY; ORIGIN; PACIFIC; ISLANDS; CONGRUENCE; ALIGNMENT AB Melicope (Rutaceae) is one of the largest plant genera on the Hawaiian Islands. We present here a detailed molecular phylogenetic analysis of the Hawaiian species of this genus and compare the results with the other genera of Hawaiian Rutaceae, Platydesma and Zanthoxylum. Four nuclear and two plastid markers were sequenced, with the goals of untangling phylogenetic relationships, inferring biogeographic events and comparing patterns of distribution among the three genera. Our results show that there were two colonization events (Melicope + Platydesma, and Zanthoxylum) to the Hawaiian Islands, that Hawaiian Rutaceae have an Asian, Australian or Pacific origin and that there were two independent colonization events of Hawaiian Melicope lineages to the Marquesas Islands. The two most widely distributed Hawaiian Melicope spp. are not monophyletic and the current subgeneric classification of Hawaiian Melicope is highly artificial. On the Hawaiian Islands, Melicope and Zanthoxylum show contrasting biogeographic patterns, suggesting different patterns of dispersal. Melicope has a high percentage of single-island endemics suggesting low dispersal ability, whereas Zanthoxylum taxa tend to occur across multiple islands. (c) 2013 The Linnean Society of London, Botanical Journal of the Linnean Society, 2014, 174, 425-448. C1 [Appelhans, Marc S.; Wen, Jun; Zimmer, Elizabeth A.; Wagner, Warren L.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Appelhans, Marc S.] Univ Gottingen, Dept Systemat Bot, Albrecht von Haller Inst Plant Sci, D-37073 Gottingen, Germany. [Wood, Kenneth R.] Natl Trop Bot Garden, Kalaheo, HI 96741 USA. [Allan, Gerard J.] No Arizona Univ, Environm Genet & Genom Lab, Flagstaff, AZ 86011 USA. RP Appelhans, MS (reprint author), Smithsonian Inst, Dept Bot, POB 37012, Washington, DC 20013 USA. EM marc.appelhans@biologie.uni-goettingen.de; wagnerw@si.edu NR 70 TC 12 Z9 12 U1 3 U2 30 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4074 EI 1095-8339 J9 BOT J LINN SOC JI Bot. J. Linnean Soc. PD MAR PY 2014 VL 174 IS 3 SI SI BP 425 EP 448 DI 10.1111/boj.12123 PG 24 WC Plant Sciences SC Plant Sciences GA AB4RW UT WOS:000331778600012 ER PT J AU Garzon-Lopez, CX Jansen, PA Bohlman, SA Ordonez, A Olff, H AF Garzon-Lopez, Carol X. Jansen, Patrick A. Bohlman, Stephanie A. Ordonez, Alejandro Olff, Han TI Effects of sampling scale on patterns of habitat association in tropical trees SO JOURNAL OF VEGETATION SCIENCE LA English DT Article DE Niche differentiation; Species co-existence; Tropical moist forest; Point pattern analysis; Panama; Habitat association; Dispersal limitation ID RAIN-FOREST TREES; SPATIAL-PATTERNS; ENVIRONMENTAL HETEROGENEITY; RECRUITMENT LIMITATION; MESOSCALE DISTRIBUTION; ECOLOGICAL COMMUNITY; NEOTROPICAL FOREST; NEUTRAL THEORY; LANDSCAPE; DISTRIBUTIONS AB Questions Niche differentiation is a central explanation for the co-existence and distribution patterns of numerous tree species in tropical forests, but functional equivalence leading to neutral dynamics has been proposed as an alternative explanation. This niche vs neutral debate is fuelled by the highly variable results yielded by studies of the association between tree species distributions and environmental factors, where some studies find strong associations but others do not. Here, we ask how differences in sampling scale between studies contribute to this variation. Location Barro Colorado Island, Panama. Methods Using distribution maps of canopy-statured individuals, we evaluated patterns of habitat association in five tropical tree species on Barro Colorado Island across a wide range of sampling scales (from 50 to 1600ha). We investigated the scale-dependency of species clumping patterns (Ripley's K) and the association of species distributions with important environmental variables (forest age, topography and geological formation) using point pattern analyses. Results Clump size and clump density had high variances within and among spatial scales. Significant habitat associations were found in all five species, with the number of habitat associations generally increasing with the sampling scale. Ignoring dispersal constraints inflated the number of significant habitat associations. Conclusions We found that patterns of habitat association (and hence conclusions on the importance of niche vs neutral processes) are strongly affected by the choice of sampling scale and location. Explicit inclusion of the effect of spatial scale is critical for studies of habitat association and the main processes that structure communities of tropical trees. C1 [Garzon-Lopez, Carol X.; Jansen, Patrick A.; Ordonez, Alejandro; Olff, Han] Univ Groningen, Ctr Life Sci, NL-9747 AG Groningen, Netherlands. [Jansen, Patrick A.] Wageningen Univ, Dept Environm Sci, NL-6700 AA Wageningen, Netherlands. [Jansen, Patrick A.; Bohlman, Stephanie A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Bohlman, Stephanie A.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA. [Ordonez, Alejandro] CCR, Nelson Inst Environm Studies, Madison, WI 53706 USA. RP Garzon-Lopez, CX (reprint author), Univ Groningen, Ctr Life Sci, Nijenborgh 7, NL-9747 AG Groningen, Netherlands. EM c.x.garzon@gmail.com; patrick.jansen@wur.nl; sbohlman@ufl.edu; ordonezglori@wisc.edu; h.olff@rug.nl RI Garzon-Lopez, Carol/G-6251-2014; Jansen, Patrick/G-2545-2015; Ordonez, Alejandro/I-7950-2013; Olff, Han/A-8516-2008 OI Garzon-Lopez, Carol/0000-0002-4099-2740; Jansen, Patrick/0000-0002-4660-0314; Ordonez, Alejandro/0000-0003-2873-4551; Olff, Han/0000-0003-2154-3576 FU Ubbo Emmius scholarship programme of the University of Groningen FX We thank Helene Muller-Landau for her valuable help with the aerial photos taken by Marcos Guerra, and the Smithsonian Tropical Research Institute for their logistical support. We are very grateful to Joe Wright for his vital support. We wish to thank Sara Pinzon-Navarro, Noelle Beckman and Eduardo Medina for all their support and help in the analysis. This work was funded by the Ubbo Emmius scholarship programme of the University of Groningen (CXG). NR 62 TC 22 Z9 23 U1 2 U2 39 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1100-9233 EI 1654-1103 J9 J VEG SCI JI J. Veg. Sci. PD MAR PY 2014 VL 25 IS 2 BP 349 EP 362 DI 10.1111/jvs.12090 PG 14 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA AB3LW UT WOS:000331693300005 ER PT J AU Greiss, S Steeghs, D Jonker, PG Torres, MAP Maccarone, TJ Hynes, RI Britt, CT Nelemans, G Gansicke, BT AF Greiss, S. Steeghs, D. Jonker, P. G. Torres, M. A. P. Maccarone, T. J. Hynes, R. I. Britt, C. T. Nelemans, G. Gaensicke, B. T. TI Near-infrared counterparts to the Galactic Bulge Survey X-ray source population SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; infrared: stars; X-rays: binaries; X-rays: stars ID ROSAT ALL-SKY; SERENDIPITOUS SOURCE CATALOG; CHANDRA SOURCE CATALOG; CATACLYSMIC VARIABLES; BLACK-HOLE; CHAMPLANE SURVEY; ORBITAL PERIOD; UNIFORM SAMPLE; DATA RELEASE; IDENTIFICATION AB We report on the near-infrared matches, drawn from three surveys, to the 1640 unique X-ray sources detected by Chandra in the Galactic Bulge Survey (GBS). This survey targets faint X-ray sources in the bulge, with a particular focus on accreting compact objects. We present all viable counterpart candidates and associate a false alarm probability (FAP) to each near-infrared match in order to identify the most likely counterparts. The FAP takes into account a statistical study involving a chance alignment test, as well as considering the positional accuracy of the individual X-ray sources. We find that although the star density in the bulge is very high, similar to 90 per cent of our sources have an FAP < 10 per cent, indicating that for most X-ray sources, viable near-infrared counterparts candidates can be identified. In addition to the FAP, we provide positional and photometric information for candidate counterparts to similar to 95 per cent of the GBS X-ray sources. This information in combination with optical photometry, spectroscopy and variability constraints will be crucial to characterize and classify secure counterparts. C1 [Greiss, S.; Steeghs, D.; Gaensicke, B. T.] Univ Warwick, Dept Phys, Astron & Astrophys Grp, Coventry CV4 7AL, W Midlands, England. [Steeghs, D.; Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.; Torres, M. A. P.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.; Nelemans, G.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6525 AJ Nijmegen, Netherlands. [Maccarone, T. J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Hynes, R. I.; Britt, C. T.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Nelemans, G.] Katholieke Univ Leuven, Inst Astron, B-3001 Louvain, Belgium. RP Greiss, S (reprint author), Univ Warwick, Dept Phys, Astron & Astrophys Grp, Coventry CV4 7AL, W Midlands, England. EM s.greiss@warwick.ac.uk RI Gaensicke, Boris/A-9421-2012; Nelemans, Gijs/D-3177-2012 OI Gaensicke, Boris/0000-0002-2761-3005; Nelemans, Gijs/0000-0002-0752-2974 FU Warwick Postgraduate Research Scholarship; STFC [PP/D005914/1]; National Science Foundation [AST-0908789]; ESO Public Survey programme [179.B-2002]; [ST/I001719/1] FX SG acknowledges support through a Warwick Postgraduate Research Scholarship. DS acknowledges support from STFC through an Advanced Fellowship (PP/D005914/1) as well as grant ST/I001719/1. RIH and CTB acknowledge support from the National Science Foundation under Grant no. AST-0908789. We gratefully acknowledge use of data from the ESO Public Survey programme ID 179.B-2002 taken with the VISTA telescope and data products from CASU. We warmly thank D. Minniti and P. Lucas for early access to the VVV data, as well as O. Gonzalez early access to his calculated reddening values. We are grateful for all the help provided by R. Saito and M. Irwin with the access and reduction of the CASU data. NR 45 TC 7 Z9 8 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 MAR PY 2014 VL 438 IS 4 BP 2839 EP 2852 DI 10.1093/mnras/stt2390 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB8KD UT WOS:000332038000009 ER PT J AU Greiss, S Gansicke, BT Hermes, JJ Steeghs, D Koester, D Ramsay, G Barclay, T Townsley, DM AF Greiss, S. Gaensicke, B. T. Hermes, J. J. Steeghs, D. Koester, D. Ramsay, G. Barclay, T. Townsley, D. M. TI KIC 11911480: the second ZZ Ceti in the Kepler field SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE asteroseismology; surveys; stars: individual: WD J192024; 90+501721; 3; white dwarfs ID PULSATING WHITE-DWARF; WHOLE EARTH TELESCOPE; SPECTROSCOPIC ANALYSIS; ROTATION VELOCITIES; EVOLUTIONARY MODELS; MASS-DISTRIBUTION; HYDROGEN-RICH; DATA RELEASE; STARS; ASTEROSEISMOLOGY AB We report the discovery of the second pulsating hydrogen-rich (DA) white dwarf in the Kepler field, KIC 11911480. It was selected from the Kepler-INT Survey (KIS) on the basis of its colours and its variable nature was confirmed using ground-based time series photometry. An atmosphere model fit to an intermediate-resolution spectrum of KIC 11911480 places this DA white dwarf close to the blue edge of the empirical boundaries of the ZZ Ceti instability strip: T-eff = 12 160 +/- 250 K and log g = 7.94 +/- 0.10. Assuming a mass-radius relation and cooling models for DA white dwarfs, the atmospheric parameters yield: M-WD = 0.57 +/- 0.06 M-circle dot. We also obtained two quarters (Q12 and Q16) of nearly uninterrupted short-cadence Kepler data on this star. We detect a total of six independent pulsation modes with a >= 3 Sigma confidence in its amplitude power spectrum. These pulsations have periods ranging between 172.9 and 324.5 s, typical of the hotter ZZ Ceti stars. Our preliminary asteroseismic study suggests that KIC 11911480 has a rotation rate of 3.5 +/- 0.5 days. C1 [Greiss, S.; Gaensicke, B. T.; Hermes, J. J.; Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Koester, D.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. [Ramsay, G.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Barclay, T.] NASA Ames Res Ctr Inst, Moffett Field, CA 94035 USA. [Barclay, T.] Bay Area Environm Res Ins, Sonoma, CA 95476 USA. [Townsley, D. M.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. RP Greiss, S (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM s.greiss@warwick.ac.uk RI Gaensicke, Boris/A-9421-2012 OI Gaensicke, Boris/0000-0002-2761-3005 FU Warwick Postgraduate Research Scholarship; European Research Council under the European Union [320964]; UK's Science and Technology Facilities Council [ST/I001719/1]; STFC [PP/D005914/1]; NASA Science Mission directorate; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX SG acknowledges support through a Warwick Postgraduate Research Scholarship. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement n. 320964 (WDTracer). BTG was supported in part by the UK's Science and Technology Facilities Council (ST/I001719/1). DS acknowledges support from STFC through an Advanced Fellowship (PP/D005914/1) as well as grant ST/I001719/1.; This paper also includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. The Kepler data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 62 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 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2014 VL 438 IS 4 BP 3086 EP 3092 DI 10.1093/mnras/stt2420 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB8KD UT WOS:000332038000028 ER PT J AU Vogelsberger, M Genel, S Sijacki, D Torrey, P Springel, V Hernquist, L AF Vogelsberger, Mark Genel, Shy Sijacki, Debora Torrey, Paul Springel, Volker Hernquist, Lars TI A model for cosmological simulations of galaxy formation physics (vol 436, pg 3031, 2013) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Correction DE errata, addenda; methods: numerical; cosmology: theory C1 [Vogelsberger, Mark; Genel, Shy; Sijacki, Debora; Torrey, Paul; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sijacki, Debora] Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Sijacki, Debora] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, Zentrum Astron, D-69120 Heidelberg, Germany. RP Vogelsberger, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mvogelsberger@cfa.harvard.edu NR 1 TC 6 Z9 6 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 MAR PY 2014 VL 438 IS 4 BP 3607 EP 3607 DI 10.1093/mnras/stt2414 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB8KD UT WOS:000332038000072 ER PT J AU McKellar, AE Marra, PP Boag, PT Ratcliffe, LM AF McKellar, Ann E. Marra, Peter P. Boag, Peter T. Ratcliffe, Laurene M. TI Form, function and consequences of density dependence in a long-distance migratory bird SO OIKOS LA English DT Article ID SEXUAL SELECTION; NEST PREDATION; POPULATION REGULATION; REPRODUCTIVE SUCCESS; NATURAL-POPULATIONS; EXTRAPAIR PATERNITY; BREEDING SYNCHRONY; AMERICAN REDSTARTS; HABITAT SELECTION; WATERFOWL NESTS AB The density dependence of demographic parameters and its implications for population regulation have long been recognized. Recent work has revealed potential effects of density on mating systems and sexual selection, but few studies concurrently assess the consequences of density on both demography and sexual selection. Such an approach is important because population processes and individual behaviors can interact to influence population growth and evolutionary trajectories. In this study, we tested the density dependence of breeding success, extra-pair paternity, and the opportunity for sexual selection in a population of American redstarts Setophaga ruticilla using two different measures of density. To evaluate temporal patterns, we analyzed annual territory density, based on the total number of territories at our study site each year. To evaluate spatial patterns, we analyzed local territory density within years, based on the number of territories surrounding a focal territory. Greater annual density was associated with fewer offspring fledged per female, a reduced mean population rate of fledging success, and a lower relative contribution of extra-pair paternity to male fitness. Greater local density was associated with fewer offspring fledged, reduced fledgling success, higher rates of nest loss, and higher rates of paternity loss on focal territories. Interestingly, greater local density was also associated with greater nestling mass on focal territories, which could imply that more densely-packed territories contain superior resources. Overall, our results suggest that the effects of crowding via greater territory density reduce fecundity through increased nest predation, rather than reduced food availability, and increase rates of extra-pair paternity. Thus, the selective pressures faced by individuals and their reproductive behaviors are likely to differ based on the annual and local density they experience, which may then feed back into population demography. C1 [McKellar, Ann E.; Boag, Peter T.; Ratcliffe, Laurene M.] Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. [Marra, Peter P.] Smithsonian Inst, Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. RP McKellar, AE (reprint author), Univ Missouri, Dept Fisheries & Wildlife Sci, Columbia, MO 65211 USA. EM mckellara@missouri.edu RI Boag, Peter/B-2907-2014 OI Boag, Peter/0000-0003-0050-2089 FU Queen's University; Natural Sciences and Engineering Research Council of Canada; Canadian Foundation for Innovation; National Science Foundation; Smithsonian Institution; Ontario Innovation Trust; Sigma Xi; American Ornithologists' Union; Society of Canadian Ornithologists; American Museum of Natural History FX We thank all of the field assistants who contributed to this study. Funding was provided by J. Fotheringham, Queen's University, the Natural Sciences and Engineering Research Council of Canada, the Canadian Foundation for Innovation, the National Science Foundation, the Smithsonian Institution, the Ontario Innovation Trust, Sigma Xi, the American Ornithologists' Union, the Society of Canadian Ornithologists, and the American Museum of Natural History. NR 52 TC 7 Z9 7 U1 0 U2 28 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 MAR PY 2014 VL 123 IS 3 BP 356 EP 364 DI 10.1111/j.1600-0706.2013.00756.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA AB2ZJ UT WOS:000331660800007 ER PT J AU Launius, RD AF Launius, Roger D. TI Reacting to nuclear power systems in space: American public protests over outer planetary probes since the 1980s SO ACTA ASTRONAUTICA LA English DT Article DE Nuclear; RTG; Spaceflight; NASA; Galileo; Cassini ID CASSINI MISSION; SATURN AB The United States has pioneered the use of nuclear power systems for outer planetary space probes since the 1970s. These systems have enabled the Viking landings to reach the surface of Mars and both Pioneers 10 and 11 and Voyagers 1 and 2 to travel to the limits of the solar system. Although the American public has long been concerned about safety of these systems, in the 1980s a reaction to nuclear accidents - especially the Soviet Cosmos 954 spacecraft destruction and the Three Mile Island nuclear power plant accidents heightened awareness about the hazards of nuclear power and every spacecraft launch since that time has been contested by opponents of nuclear energy. This has led to a debate over the appropriateness of the use of nuclear power systems for spacecraft. It has also refocused attention on the need for strict systems of control and rigorous checks and balances to assure safety. This essay describes the history of space radioisotope power systems, the struggles to ensure safe operations, and the political confrontation over whether or not to allow the launch the Galileo and Cassini space probes to the outer planets. Effectively, these efforts have led to the successful flights of 12 deep space planetary probes, two-thirds of them operated since the accidents of Cosmos 954, Three Mile Island, and Chernobyl. IAA. Published by Elsevier Ltd. All rights reserved. C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, POB 37012,NASM Room 3556,MRC 311, Washington, DC 20013 USA. EM launiusr@si.edu NR 91 TC 1 Z9 1 U1 1 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD MAR-APR PY 2014 VL 96 BP 188 EP 200 DI 10.1016/j.actaastro.2013.12.004 PG 13 WC Engineering, Aerospace SC Engineering GA AB3BN UT WOS:000331666400020 ER PT J AU Elvis, M Esty, T AF Elvis, Martin Esty, Thomas TI How many assay probes to find one ore-bearing asteroid? SO ACTA ASTRONAUTICA LA English DT Article DE Near-Earth asteroids; Mining; Prospecting ID NEAR-EARTH OBJECTS; POPULATION; METEORITES AB The number of ore-bearing asteroids could well be small and remote telescopic techniques are inadequate to identify such asteroids confidently. Finding an asteroid that can be profitably mined requires proximate observations from assay probes. Here we use a simple statistical approach to estimate the number of assay probes, N-assay, needed to find at least one ore-bearing asteroid at a high confidence (90%, 95%, and 99%). We present results for a wide range of values of the probability of an asteroid being rich in the resource of interest, P-rich. We find that N-assay depends strongly on P-rich, for likely values of P-rich ( < 0.5). For a plausible value of P-rich similar to 0.1 then to obtain 90% confidence that at least one ore-bearing asteroid is found, N-assay=22, and for 99% confidence N-assay=44. A factor two increase in P-rich roughly halves N-assay, while for P-rich similar to 0.5, N-assay (90%)=4. Hence any improvement in asteroid characterization prior to sending probes to its proximity would be an effective way to cost-effectively search for valuable resources among the asteroids. Some possibilities for doing so are briefly discussed. IAA. Published by Elsevier Ltd. All rights reserved. C1 [Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Esty, Thomas] Harvard Univ, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM melvis@cfa.harvard.edu; martinselvis2@gmail.com OI Elvis, Martin/0000-0001-5060-1398 NR 35 TC 1 Z9 1 U1 0 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD MAR-APR PY 2014 VL 96 BP 227 EP 231 DI 10.1016/j.actaastro.2013.11.027 PG 5 WC Engineering, Aerospace SC Engineering GA AB3BN UT WOS:000331666400023 ER PT J AU Bacelar, FS Calabrese, JM Hernandez-Garcia, E AF Bacelar, Flora S. Calabrese, Justin M. Hernandez-Garcia, Emilio TI Exploring the tug of war between positive and negative interactions among savanna trees: Competition, dispersal, and protection from fire SO ECOLOGICAL COMPLEXITY LA English DT Article DE Savanna; Tree-tree competition; Tree-grass equilibrium; Individual based model; Clustering; Fire-spread model ID SELF-ORGANIZED CRITICALITY; AFRICAN SAVANNAS; PATCH-DYNAMICS; ARID SAVANNA; KALAHARI; MODEL; VEGETATION; MORTALITY; PATTERNS; COEXISTENCE AB Savannas are characterized by a discontinuous tree layer superimposed on a continuous layer of grass. Identifying the mechanisms that facilitate this tree-grass coexistence has remained a persistent challenge in ecology and is known as the "savanna problem". In this work, we propose a model that combines a previous savanna model Calabrese et al., 2010, which includes competitive interactions among trees and dispersal, with the Drossel-Schwabl forest fire model, therefore representing fire in a spatially explicit manner. The model is used to explore how the pattern of fire-spread, coupled with an explicit, fire-vulnerable tree life stage, affects tree density and spatial pattern. Tree density depends strongly on both fire frequency and tree-tree competition although the fire frequency, which induces indirect interactions between trees and between trees and grass, appears to be the crucial factor controlling the tree-extinction transition in which the savanna becomes grassland. Depending on parameters, adult trees may arrange in different regular or clumped patterns, the later of two different types (compact or open). Cluster-size distributions have fat tails but clean power-law behavior is only attained in specific cases. (C) 2013 Elsevier B.V. All rights reserved. C1 [Bacelar, Flora S.; Hernandez-Garcia, Emilio] Inst Fis Interdisciplinary & Sistemas Complejos, IFISC CSIC UIB, E-07122 Palma De Mallorca, Spain. [Calabrese, Justin M.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA. [Calabrese, Justin M.] UFZ Helmholtz Ctr Environm Res, Dept Ecol Modelling, D-04318 Leipzig, Germany. [Bacelar, Flora S.] Univ Fed Bahia, Inst Fis, BR-40210340 Salvador, BA, Brazil. RP Bacelar, FS (reprint author), Univ Fed Bahia, Inst Fis, BR-40210340 Salvador, BA, Brazil. EM fbacelar@ufba.br RI Calabrese, Justin/B-9131-2012; Hernandez-Garcia, Emilio/B-1271-2008; Souza Bacelar, Flora /H-5665-2015 OI Hernandez-Garcia, Emilio/0000-0002-9568-8287; Souza Bacelar, Flora /0000-0002-1301-3092 FU Spanish MINECO; FEDER through project FISICOS [FIS2007-60327]; FEDER through project INTENSE@COSYP [FIS2012-30634]; European Union [NEST 43268]; Balearic Government FX F.S.B. and E.H.-G. acknowledge financial support from Spanish MINECO and FEDER through projects FISICOS (FIS2007-60327) and INTENSE@COSYP (FIS2012-30634). J.M.C. acknowledges the support of the European Union project PATRES (Pattern Resilience; project NEST 43268). F.S.B. acknowledges a grant from the Balearic Government. We thank Volker Grimm and Richard D. Zinck for helpful discussions. NR 37 TC 6 Z9 6 U1 3 U2 18 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1476-945X EI 1476-9840 J9 ECOL COMPLEX JI Ecol. Complex. PD MAR PY 2014 VL 17 BP 140 EP 148 DI 10.1016/j.ecocom.2013.11.007 PG 9 WC Ecology SC Environmental Sciences & Ecology GA AB3GJ UT WOS:000331679000014 ER PT J AU Kingston, SE Navarro-Siguenza, A Garcia-Trejo, EA Vazquez-Miranda, H Fagan, WF Braun, MJ AF Kingston, Sarah E. Navarro-Sigueenza, Adolfo G. Garcia-Trejo, Erick A. Vazquez-Miranda, Hernan Fagan, William F. Braun, Michael J. TI Genetic differentiation and habitat connectivity across towhee hybrid zones in Mexico SO EVOLUTIONARY ECOLOGY LA English DT Article DE Gene flow; Habitat connectivity; Hybrid zone; Introgression; Dispersal ID MULTILOCUS GENOTYPE DATA; MOLECULAR PHYLOGENETICS; POPULATION-GENETICS; LANDSCAPE GENETICS; CIRCUIT-THEORY; METHODS REVEAL; FLOW; DIVERGENCE; INFERENCE; MARKERS AB Hybridization can either reinforce or erode species boundaries; therefore, hybrid zones offer a natural experimental setting in which to assess the dynamics of reproductive isolation. Secondary contact zones, in particular, present a partial separation of the original divergence mechanisms and the subsequent genomic architecture of reproductive isolation (or lack thereof). The spatial context of secondary contact and its consequent effect on dispersal play vital roles on the contact's outcome. In a hybrid complex between two towhee species in Mexico, Pipilo maculatus and Pipilo ocai, two major hybrid gradients provide natural replicates for comparison. However, genetic analyses demonstrate significant divergence between geographically separate parental populations of each species and divergence of populations within each hybrid zone. The two hybrid transects (Teziutlan and Transvolcanic) are distinct and evidence suggests allelic introgression both across the species boundary and between the two transects. Habitat corridors for dispersal represent functional connectivity hotspots where the two transects meet. Both habitat connectivity and genetic differentiation between geographically disparate parental populations appear to influence the dynamics of gene flow across the hybrid gradients. In southern sympatric populations (Mt. Orizaba and Oaxaca) where morphological evidence for hybridization is scarce, opposing species' alleles appear to traverse through the hybrid zones rather than arising from cryptic local hybridization. These results illustrate the importance of environmentally mediated gene flow in the context of secondary contact as an important force influencing evolutionary trajectory. C1 [Kingston, Sarah E.; Braun, Michael J.] Univ Maryland, Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA. [Kingston, Sarah E.; Braun, Michael J.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Navarro-Sigueenza, Adolfo G.; Garcia-Trejo, Erick A.; Vazquez-Miranda, Hernan] Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Evolut Biol, Museo Zool Alfonso L Herrera, Mexico City 04510, DF, Mexico. [Vazquez-Miranda, Hernan] Univ Minnesota, Bell Museum, St Paul, MN 55108 USA. [Vazquez-Miranda, Hernan] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. [Fagan, William F.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Kingston, SE (reprint author), Univ Maryland, Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA. EM kingstons@si.edu RI Vazquez-Miranda, Hernan/M-1323-2013; OI Vazquez-Miranda, Hernan/0000-0002-4275-6979; Navarro-Siguenza, Adolfo G./0000-0003-2652-7719; Garcia-Trejo, Erick Alejandro/0000-0002-1443-8068 FU Smithsonian Research Endowment Fund; University of Maryland Program in Behavior, Ecology, Evolution, and Systematics; Smithsonian Ornithology; Department of Vertebrate Zoology, National Museum of Natural History (NMNH); NSF [DEB0228675, DEB0733029] FX We appreciate greatly Blanca Hernandez for extending us collecting permits in Mexico. We thank Laura Villasenor, Sarahy Contreras, Alejandro Gordillo, Gala Cortes, Daniela Tovilla-Sierra, Ruben Ortega, Marco Ortiz, Mauricio Perez-Vera, Laila Yunes-Jimenez, and Cesar A. Rios-Munoz for their invaluable guidance, leadership, and assistance in the field across the Transvolcanic Belt in Mexico. We thank David Braun, Stephen Braun, Nicholas Lanson, Nimrod Funk, and George Oliver for their able assistance in the field in the Teziutlan gradient. Thanks to Darrilyn Albright for labwork assistance. We thank our funding sources for this project: Smithsonian Research Endowment Fund, University of Maryland Program in Behavior, Ecology, Evolution, and Systematics, Smithsonian Ornithology, and the Department of Vertebrate Zoology, National Museum of Natural History (NMNH). S. Kingston received research assistantships from the NMNH Frontiers in Phylogenetics Program and NSF grants DEB0228675 and DEB0733029. NR 64 TC 2 Z9 2 U1 5 U2 39 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 MAR PY 2014 VL 28 IS 2 BP 277 EP 297 DI 10.1007/s10682-013-9673-8 PG 21 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA AB3SX UT WOS:000331711600005 ER PT J AU Pons, JM Sonsthagen, S Dove, C Crochet, PA AF Pons, J-M Sonsthagen, S. Dove, C. Crochet, P-A TI Extensive mitochondrial introgression in North American Great Black-backed Gulls (Larus marinus) from the American Herring Gull (Larus smithsonianus) with little nuclear DNA impact SO HEREDITY LA English DT Article DE hybridization; mitochondrial DNA; microsatellites; speciation; Larus; North America ID WHITE-HEADED GULLS; RECENT SECONDARY CONTACT; GENE FLOW; HYBRID ZONE; EVOLUTIONARY HISTORY; POPULATION-GENETICS; MICROSATELLITE DATA; HYBRIDIZATION; SELECTION; LOCI AB Recent genetic studies have shown that introgression rates among loci may greatly vary according to their location in the genome. In particular, several cases of mito-nuclear discordances have been reported for a wide range of organisms. In the present study, we examine the causes of discordance between mitochondrial (mtDNA) and nuclear DNA introgression detected in North American populations of the Great Black-backed Gull (Larus marinus), a Holarctic species, from the Nearctic North American Herring Gull (Larus smithsonianus). Our results show that extensive unidirectional mtDNA introgression from Larus smithsonianus into Larus marinus in North America cannot be explained by ancestral polymorphism but most likely results from ancient hybridization events occurring when Larus marinus invaded the North America. Conversely, our nuclear DNA results based on 12 microsatellites detected very little introgression from Larus smithsonianus into North American Larus marinus. We discuss these results in the framework of demographic and selective mechanisms that have been postulated to explain mito-nuclear discrepancies. We were unable to demonstrate selection as the main cause of mito-nuclear introgression discordance but cannot dismiss the possible role of selection in the observed pattern. Among demographic explanations, only drift in small populations and bias in mate choice in an invasive context may explain our results. As it is often difficult to demonstrate that selection may be the main factor driving the introgression of mitochondrial DNA in natural populations, we advocate that evaluating alternative demographic neutral hypotheses may help to indirectly support or reject hypotheses invoking selective processes. C1 [Pons, J-M] Museum Natl Hist Nat, Dept Systemat & Evolut, Origine Struct & Evolut Biodiversite UMR7205, F-75005 Paris, France. [Pons, J-M] Museum Natl Hist Nat, Serv Systemat Mol, UMS 2700, F-75005 Paris, France. [Sonsthagen, S.; Dove, C.] Smithsonian Inst, Dept Vertebrate Zool, Div Birds, Natl Museum Nat Hist, Washington, DC 20560 USA. [Crochet, P-A] CNRS, Ctr Ecol Fonct & Evolut, UMR5175, F-34033 Montpellier 5, France. RP Pons, JM (reprint author), Museum Natl Hist Nat, Dept Systemat & Evolut, UMR 7205, 55 Rue Buffon,CP 51, F-75005 Paris, France. EM pons@mnhn.fr FU Smithsonian; FAA FX We are very grateful to R Barret, R Bradbury, B Cadiou (Bretagne vivante, SEPNB), J Dean (National Museum of Natural History), D Dittmann (Louisiana State University Museum of Natural Science), G Chapdelaine and J-F Rail (Service Canadien de la Faune) R Evans, A Forsten, G Fox, D Mourier, M Robbins (Kansas Natural History Museum), V Rauste, P Sweet (American Museum of Natural History), N Rice (Academy of Natural Sciences of Philadelphia) and P Yesou for kindly providing us tissue samples. HYBRIDLAB is currently difficult to find in the internet as the links provided in the original publication are broken; S Consuegra, EE Nielsen, U Saarma and RA Sanchez-Guillen helped us in various ways to obtain this program. Laboratory assistance was provided by C Bonillo, J Lambourdiere and A Tillier at MNHN and J Hunt and L Weight (Laboratories of Analytical Biology, Smithsonian Institution). We thank Daniel Pons who helped to draw the Figure 1 as well as Bailey D McKay and three anonymous referees for helpful comments on an earlier version of the manuscript. Part of this research was funded through an interagency agreement between the Smithsonian and the FAA. NR 83 TC 6 Z9 6 U1 2 U2 38 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0018-067X EI 1365-2540 J9 HEREDITY JI Heredity PD MAR PY 2014 VL 112 IS 3 BP 226 EP 239 DI 10.1038/hdy.2013.98 PG 14 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA AB2MJ UT WOS:000331626500002 PM 24105440 ER PT J AU Morlok, A Lisse, CM Mason, AB Bullock, ES Grady, MM AF Morlok, A. Lisse, C. M. Mason, A. B. Bullock, E. S. Grady, M. M. TI Mid-infrared spectroscopy of components in chondrites: Search for processed materials in young Solar Systems and comets SO ICARUS LA English DT Article DE Infrared observations; Disks; Meteorites ID HERBIG-AE/BE STARS; INFRARED-ABSORPTION SPECTRA; T-TAURI STARS; INTERPLANETARY DUST PARTICLES; PROTOPLANETARY DISKS; CRYSTALLINE SILICATES; GRAIN-GROWTH; COMPOSITIONAL DEPENDENCE; CARBONACEOUS CHONDRITE; HALE-BOPP AB We obtained mid-infrared spectra of chondrules, matrix, CAIs and bulk material from primitive type 1-4 chondrites in order to compare them with the dust material in young, forming Solar Systems and around comets. Our aim is to investigate whether there are similarities between the first processed materials in our early Solar System and protoplanetary disks currently forming around other stars. Comparison between the laboratory infrared data and astronomical spectra indicate a general similarity between processed Solar System materials and circumstellar dust. This includes fine-grained matrix material, but also processed component like chondrules and or impact shock processed CM like material. Comets investigated in this study also have spectral features that could allow contents of chondrules or impact shock processed matrix material. Chondrule spectra can be divided into two groups: (1) chondrules dominated by olivine features at similar to 11.3 mu m and similar to 10.0 mu m and (2) mesostasis rich chondrules that show main features at similar to 10 mu m. Bulk ordinary chondrites show similar features to both groups. Fine-grained matrix is divided into three groups: (1) phyllosilicate-rich with a main band at similar to 10 mu m, (2) olivine-rich with bands at 11.3 mu m and similar to 10 mu m, and (3) pyroxene-rich with several peaks between 9.3 mu m and 11.2 mu m. Impact shock-processed matrix from Murchison (CM2) shows features from phyllosilicate-rich, amorphous and olivine-rich material. CAIs show melilite/spinel-rich features between 10.2 mu m and 12.5 mu m. Astronomical spectra are divided into four groups based on their spectral characteristics - amorphous (group 1), pyroxene-rich (group 2), olivine-rich (group 3) and 'complex' (group 4). Group 2 is similar to enstatite-rich fine grained material like e.g. Kakangari (K3) matrix. Groups 3 and 4 can be explained by a combination of varying concentrations of olivine and mesostasis-rich chondrules and fine-grained matrix, but also show very good agreement with shock processed material. Comparison of band ratios confirms the similarity with chondritic material e.g. for HD100546, while the inner disk of HD142527 show no sign of chondrule material. For some systems, though, we find that other amorphous materials such as IDP/GEMS have to be taken into account to fully fit their spectra. (C) 2014 Elsevier Inc. All rights reserved. C1 [Morlok, A.; Grady, M. M.] Nat Hist Museum, Dept Mineral, London SW7 5BD, England. [Lisse, C. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Mason, A. B.] Univ Turku, ESO FINCA, Finnish Ctr Astron, Tuorla Observ, FI-21500 Pukkio, Finland. [Bullock, E. S.] Smithsonian Inst, Washington, DC 20013 USA. [Grady, M. M.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. RP Morlok, A (reprint author), WWU Munster, Inst Planetol, Wilhelm Klemm Str 10, D-48149 Munster, Germany. EM morlokan@uni-muenster.de; carey.lisse@jhuapl.edu; andmas@utu.fi; bullocke@si.edu; m.m.grady@open.ac.uk RI Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Grady, Monica/0000-0002-4055-533X FU UK PPARC (STFC); NASA [1407]; ESA Member States FX A.M. and MMG were funded for part of the research by the UK PPARC (STFC). Many thanks to Roy van Boekel (Heidelberg) for the space resolved MIDI spectra, to Takahito Osawa (Ibaraki) for the additional matrix data. Also, many thanks to Caroline Smith (London) for providing the Allende samples. Also we would like to thank two anonymous reviewers and editor M.E.Combi for helping to improve the original manuscript significantly.; This work is partially based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA Contract 1407. Part of this work is based on observations with ISO, an ESA project with instruments funded by ESA Member States and with the participation of ISAS and NASA. Also, part of the data is based on observations obtained at the European Southern Observatory (ESO). NR 110 TC 3 Z9 3 U1 1 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR 1 PY 2014 VL 231 BP 338 EP 355 DI 10.1016/j.icarus.2013.12.018 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB3CE UT WOS:000331668100028 ER PT J AU Campbell, BA Putzig, NE Foss, FJ Phillips, RJ AF Campbell, Bruce A. Putzig, Nathaniel E. Foss, Frederick J., II Phillips, Roger J. TI SHARAD Signal Attenuation and Delay Offsets Due to the Martian Ionosphere SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE Ionosphere; Mars; radar remote sensing ID RADAR; MARS AB We estimate and correct variable time-delay offsets among Mars Shallow Radar (SHARAD) sounding observations of the north polar layered deposits of Mars under a broad range of ionospheric conditions. We find that these delay offsets are linearly related to the magnitude of the phase distortion, which is determined by optimization of the surface and subsurface echo response by autofocusing. We use this relationship to determine an empirical scaling between the phase parameter and the total electron content (TEC) of the Martian ionosphere. This method allows simultaneous correction of the image blurring and time-delay errors induced by the ionosphere, corrections that are crucial for 3-D imaging of subsurface features. We also characterize the attenuation of SHARAD echoes as a function of TEC to facilitate detection of seasonal changes in surface physical properties. During solar flare events, SHARAD signals experience phase distortion and delay consistent with a 50%-100% increase in TEC relative to typical dayside conditions, but up to tenfold greater attenuation than predicted. The increased signal absorption is likely due to enhanced electron content at lower altitudes where the neutral particle density is higher. C1 [Campbell, Bruce A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Putzig, Nathaniel E.] Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Foss, Frederick J., II] Freestyle Analyt & Quantitat Serv LLC, Longmont, CO 80504 USA. [Phillips, Roger J.] Southwest Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA. RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. EM campbellb@si.edu FU National Aeronautics and Space Administration through the Mars Reconnaissance Orbiter Program FX This work was supported in part by the National Aeronautics and Space Administration through the Mars Reconnaissance Orbiter Program. NR 15 TC 7 Z9 8 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X EI 1558-0571 J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD MAR PY 2014 VL 11 IS 3 BP 632 EP 635 DI 10.1109/LGRS.2013.2273396 PG 4 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AC0KG UT WOS:000332182600010 ER PT J AU Slepian, Z Gott, JR Zinn, J AF Slepian, Zachary Gott, J. Richard, III Zinn, Joel TI A one-parameter formula for testing slow-roll dark energy: observational prospects SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE equation of state; cosmology: theory; dark energy; inflation ID LARGE-SCALE STRUCTURE; IA SUPERNOVAE; COSMOLOGICAL CONSTANT; INFLATIONARY UNIVERSE; GALAXY CLUSTERS; MATTER; TELESCOPE; FORECASTS; FLATNESS; HORIZON AB Numerous upcoming observations, such as Wide-Field Infrared Survey Telescope, Baryon Oscillation Spectroscopic Survey (BOSS), BigBOSS, Large Synoptic Survey Telescope, Euclid and Planck, will constrain dark energy (DE)'s equation of state with great precision. They may well find that the ratio of pressure to energy density, w, is -1, meaning DE is equivalent to a cosmological constant. However, many time-varying DE models have also been proposed. A single parametrization to test a broad class of them and that is itself motivated by a physical picture is therefore desirable. We suggest that the simplest model of DE has the same mechanism as inflation, likely a scalar field slowly rolling down its potential. If this is so, DE will have a generic equation of state and the Universe will have a generic dependence of the Hubble constant on redshift, independent of the potential's starting value and shape. This equation of state and expression for the Hubble constant offer the desired model-independent but physically motivated parametrization, because they will hold for most of the standard scalar field models of DE such as quintessence and phantom DE. Up until now two-parameter descriptions of w have been available, but this work finds an additional approximation that leads to a single-parameter model. Using it, we conduct a chi(2) analysis and find that experiments in the next seven years should be able to distinguish any of these time-varying DE models on the one hand from a cosmological constant on the other to 73 per cent confidence if w today differs from -1 by 3.5 per cent. In the limit of perfectly accurate measurements of (m) and H-0, this confidence would rise to 96 per cent. We also include discussion of the current status of DE experiments, a table compiling the techniques each will use and tables of the precisions of the experiments for which this information was available at the time of publication. C1 [Slepian, Zachary] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gott, J. Richard, III; Zinn, Joel] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Slepian, Z (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM zslepian@cfa.harvard.edu; jrg@astro.princeton.edu; jzinn@princeton.edu OI Zinn, Joel/0000-0002-7550-7151 FU National Science Foundation [DGE-1144152] FX ZS thanks Paul Steinhardt, Daniel Eisenstein, Neta Bahcall, Harvey Tananbaum, Stephen Portillo, Philip Mocz, Aisha Down and Laura Kulowski for many helpful conversations during the course of this work. ZS particularly appreciates the willingness of the first on this list to be both critic and sounding board. All authors thank Michael Blanton for helpful comments during revision. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144152. NR 76 TC 9 Z9 9 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2014 VL 438 IS 3 BP 1948 EP 1970 DI 10.1093/mnras/stt2195 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB6DE UT WOS:000331877000003 ER PT J AU Torrey, P Vogelsberger, M Genel, S Sijacki, D Springel, V Hernquist, L AF Torrey, Paul Vogelsberger, Mark Genel, Shy Sijacki, Debora Springel, Volker Hernquist, Lars TI A model for cosmological simulations of galaxy formation physics: multi-epoch validation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: evolution; galaxies: formation; cosmology: theory ID TULLY-FISHER RELATION; STAR-FORMING GALAXIES; SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; STELLAR MASS FUNCTION; MOVING-MESH COSMOLOGY; COLD DARK-MATTER; LYMAN-BREAK GALAXIES; SUPERNOVA-DRIVEN WINDS; FORMATION RATE DENSITY AB We present a multi-epoch analysis of the galaxy populations formed within the cosmological hydrodynamical simulations presented in Vogelsberger et al. These simulations explore the performance of a recently implemented feedback model which includes primordial and metal line radiative cooling with self-shielding corrections; stellar evolution with associated mass-loss and chemical enrichment; feedback by stellar winds; black hole seeding, growth and merging; and active galactic nuclei (AGN) quasar- and radio-mode heating with a phenomenological prescription for AGN electro-magnetic feedback. We illustrate the impact of the model parameter choices on the resulting simulated galaxy population properties at high and intermediate redshifts. We demonstrate that our scheme is capable of producing galaxy populations that broadly reproduce the shape of the observed galaxy stellar mass function extending from redshift z = 0 to z = 3. We also characterize the evolving galactic B-band luminosity function, stellar mass to halo mass ratio, star formation main sequence, Tully-Fisher relation and gas-phase mass-metallicity relation and confront them against recent observational estimates. This detailed comparison allows us to validate elements of our feedback model, while also identifying areas of tension (e.g., the shape and normalization of the mass-metallicity relation and normalization of the star formation main sequence) that will be addressed in future work. C1 [Torrey, Paul; Vogelsberger, Mark; Genel, Shy; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sijacki, Debora] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sijacki, Debora] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, Zentrum Astron, ARI, D-69120 Heidelberg, Germany. RP Torrey, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ptorrey@cfa.harvard.edu OI Torrey, Paul/0000-0002-5653-0786; Genel, Shy/0000-0002-3185-1540 FU NASA [HST-HF-51317.01, NNX12AC67G]; European Research Council [EXAGAL-308037] FX We thank Greg Snyder, Dylan Nelson, Dave Patton, Sara Ellison, Lisa Kewley, Jabran Zahid and Giovani Cresci for helpful suggestions on this work. We thank the referee, Joop Schaye, for giving constructive comments that helped improve the quality of this paper. MV acknowledges support from NASA through Hubble Fellowship grant HST-HF-51317.01. VS acknowledges support from the European Research Council under ERC-StG grant EXAGAL-308037. LH acknowledges support from NASA through grant NNX12AC67G. NR 215 TC 65 Z9 65 U1 1 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2014 VL 438 IS 3 BP 1985 EP 2004 DI 10.1093/mnras/stt2295 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB6DE UT WOS:000331877000005 ER PT J AU Maravelias, G Zezas, A Antoniou, V Hatzidimitriou, D AF Maravelias, G. Zezas, A. Antoniou, V. Hatzidimitriou, D. TI Optical spectra of five new Be/X-ray binaries in the Small Magellanic Cloud and the link of the supergiant B[e] star LHA 115-S 18 with an X-ray source SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: emission-line, Be; stars: individual: LHA 115-S 18; Galaxy: stellar content; galaxies: individual; Magellanic Clouds; X-rays: binaries ID GRAVITATIONAL LENSING EXPERIMENT; MASSIVE STARS; XMM-NEWTON; SPACED DATA; BVI MAPS; CATALOG; DISCOVERY; EMISSION; SMC; VELOCITIES AB The Small Magellanic Cloud (SMC) is well known to harbour a large number of high-mass X-ray binaries (HMXBs). The identification of their optical counterparts provides information on the nature of the donor stars and can help to constrain the parameters of these systems and their evolution. We obtained optical spectra for a number of HMXBs identified in previous Chandra and XMM-Newton surveys of the SMC using the AAOmega/2dF fibre-fed spectrograph at the Anglo-Australian Telescope. We find five new Be/X-ray binaries (BeXRBs; including a tentative one), by identifying the spectral type of their optical counterparts, and we confirm the spectral classification of an additional 15 known BeXRBs. We compared the spectral types, orbital periods and eccentricities of the BeXRB populations in the SMC and the Milky Way and we find marginal evidence for difference between the spectral type distributions, but no statistically significant differences for the orbital periods and the eccentricities. Moreover, our search revealed that the well-known supergiant B[e] star LHA 115-S 18 (or AzV 154) is associated with the weak X-ray source CXOU J005409.57-724143.5. We provide evidence that the supergiant star LHA 115-S 18 is the optical counterpart of the X-ray source, and we discuss different possibilities of the origin of its low X-ray luminosity (L-x similar to 4 x 10(33) erg s(-1)). C1 [Maravelias, G.; Zezas, A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. [Maravelias, G.; Zezas, A.] Inst Theoret & Computat Phys, GR-71003 Iraklion, Crete, Greece. [Zezas, A.] Fdn Res & Technol Hellas, Inst Elect Struct & Laser, GR-71110 Iraklion, Crete, Greece. [Zezas, A.; Antoniou, V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Antoniou, V.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Hatzidimitriou, D.] Univ Athens, Dept Phys, Sect Astrophys Astron & Mech, GR-15784 Athens, Greece. RP Maravelias, G (reprint author), Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. EM gmaravel@physics.uoc.gr RI Hatzidimitriou, Despina/A-3732-2015; Zezas, Andreas/C-7543-2011; Antoniou, Vallia/E-3837-2013 OI Zezas, Andreas/0000-0001-8952-676X; Antoniou, Vallia/0000-0001-7539-1593 FU State Scholarships Foundation of Greece; Chandra grant [GO3-14051X]; NASA [NNX12AL39G, NNX10AH47G]; EU IRG [224878]; EU FP7-REGPOT grant [206469]; National Aeronautics and Space Administration; National Science Foundation FX We would like to thank the referee, Phil Charles, whose comments and suggestions helped to improve the paper. We would like to thank the staff of the Anglo-Australian Observatory for obtaining the data used in this work. We thank A. Manousakis and R. Walter for useful discussions regarding the class of heavily obscured sgXRBs, and A. Pollock for advice regarding the class of colliding-wind binaries. GM acknowledges support by State Scholarships Foundation of Greece in the form of a scholarship. AZ acknowledges support by the Chandra grant GO3-14051X, the NASA grant NNX12AL39G and the EU IRG grant 224878. Space Astrophysics at the University of Crete is supported by EU FP7-REGPOT grant 206469 (ASTRO-SPACE). VA acknowledges support by NASA grant NNX10AH47G issued through the Astrophysics Data Analysis Program, and Chandra grant GO3-14051X.; This research has made use of NASA's Astrophysics Data System, SIMBAD data base (operated at CDS, Strasbourg, France), and data products from the Optical Gravitational Lensing Experiment and 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. Figures were generated using the MATPLOTLIB7 library in the PYTHON8 programming language. NR 80 TC 3 Z9 3 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 MAR PY 2014 VL 438 IS 3 BP 2005 EP 2025 DI 10.1093/mnras/stt2302 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB6DE UT WOS:000331877000006 ER PT J AU Wilson, PA Colon, KD Sing, DK Ballester, GE Desert, JM Ehrenreich, D Ford, EB Fortney, JJ des Etangs, AL Lopez-Morales, M Morley, CV Pettitt, AR Pont, F Vidal-Madjar, A AF Wilson, P. A. Colon, K. D. Sing, D. K. Ballester, G. E. Desert, J-M. Ehrenreich, D. Ford, E. B. Fortney, J. J. des Etangs, A. Lecavelier Lopez-Morales, M. Morley, C. V. Pettitt, A. R. Pont, F. Vidal-Madjar, A. TI A search for methane in the atmosphere of GJ 1214b via GTC narrow-band transmission spectrophotometry SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; stars: individual: GJ 1214; planetary systems ID SUPER-EARTH GJ1214B; METAL-RICH ATMOSPHERE; OSIRIS TUNABLE IMAGER; STELLAR VARIABILITY; TRANSIT PHOTOMETRY; HIGH-RESOLUTION; LIGHT CURVES; SPECTRUM; PLANETS; SYSTEM AB We present narrow-band photometric measurements of the exoplanet GJ 1214b using the 10.4 m Gran Telescopio Canarias and the Optical System for Imaging and low Resolution Integrated Spectroscopy instrument. Using tuneable filters, we observed a total of five transits, three of which were observed at two wavelengths nearly simultaneously, producing a total of eight individual light curves, six of these probed the possible existence of a methane absorption feature in the 8770-8850 A region at high resolution. We detect no increase in the planet-to-star radius ratio across the methane feature with a change in radius ratio of Delta(R) over bar = -0.0007 +/- 0.0017 corresponding to a scaleheight (H) change of -0.5 +/- 1.2H across the methane feature, assuming a hydrogen-dominated atmosphere. We find that a variety of water and cloudy atmospheric models fit the data well, but find that cloud-free models provide poor fits. These observations support a flat transmission spectrum resulting from the presence of a high-altitude haze or a water-rich atmosphere, in agreement with previous studies. In this study, the observations are pre-dominantly limited by the photometric quality and the limited number of data points (resulting from a long observing cadence), which make the determination of the systematic noise challenging. With tuneable filters capable of high-resolution measurements (R approximate to 600-750) of narrow absorption features, the interpretation of our results are also limited by the absence of high-resolution methane models below 1 mu m. C1 [Wilson, P. A.; Sing, D. K.; Pettitt, A. R.; Pont, F.] Univ Exeter, Sch Phys, Astrophys Grp, Exeter EX4 4QL, Devon, England. [Colon, K. D.] Univ Hawaii Manoa, Dept Geol & Geophys, Honolulu, HI 96822 USA. [Colon, K. D.; Ford, E. B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Ballester, G. E.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Desert, J-M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Ehrenreich, D.; des Etangs, A. Lecavelier] Univ Geneva, Astron Observ, CH-1290 Sauverny, Switzerland. [Fortney, J. J.; Morley, C. V.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Lopez-Morales, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vidal-Madjar, A.] Univ Paris 06, CNRS, Inst Astrophys Paris, F-75014 Paris, France. RP Wilson, PA (reprint author), Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England. EM paw@astro.ex.ac.uk OI Sing, David /0000-0001-6050-7645; Fortney, Jonathan/0000-0002-9843-4354; Ehrenreich, David/0000-0001-9704-5405 FU UK Science and Technology Facilities Council (STFC); STFC; Halliday fellowship [ST/F011083/1]; National Science Foundation (NSF); STScI [HST-GO-12473.01-A]; National Geographic Society's Young Explorers Grant FX We thank the entire GTC staff and in particular Antonio Cabrera Lavers and Robert C. Morehead for their help in conducting these observations. This work is based on observations made with the GTC, installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias on the island of La Palma. The GTC is a joint initiative of Spain (led by the Instituto de Astrofisica de Canarias), the University of Florida and Mexico, including the Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico (IA-UNAM) and Instituto Nacional de Astrofisica, Optica y Electronica (INAOE). PAW, DKS and ARP acknowledge support from the UK Science and Technology Facilities Council (STFC). FP is grateful for the STFC grant and Halliday fellowship (ST/F011083/1). KDC and RCM were supported by the National Science Foundation (NSF) Graduate Research Fellowships. GEB acknowledges support from STScI through grants HST-GO-12473.01-A. This work was also aided by the National Geographic Society's Young Explorers Grant, awarded to KDC. The authors would like to acknowledge the anonymous referee for their useful comments. NR 37 TC 8 Z9 9 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 MAR PY 2014 VL 438 IS 3 BP 2395 EP 2405 DI 10.1093/mnras/stt2356 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB6DE UT WOS:000331877000031 ER PT J AU Helbig-Bonitz, M Rutten, G Kalko, EKV AF Helbig-Bonitz, Maria Rutten, Gemma Kalko, Elisabeth K. V. TI Fruit bats can disperse figs over different land-use types on Mount Kilimanjaro, Tanzania SO AFRICAN JOURNAL OF ECOLOGY LA English DT Article ID TROPICAL FORESTS; SPECIES-RICH; INTENSIFICATION; BIODIVERSITY; CONSERVATION; DIVERSITY C1 [Helbig-Bonitz, Maria; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Rutten, Gemma] Univ Bern, Inst Plant Sci, CH-3013 Bern, Switzerland. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Helbig-Bonitz, M (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM maria.helbig@uni-ulm.de; ggpmrutten@gmail.com FU Research-Unit of the German Research Foundation (DFG) [1246]; COSTECH [2010-340-ER-NA-96-44, 2011-340-ER-96-44]; TANAPA [TNO/HQ/C.10/13/VOL.III] FX We thank K. Bohning-Gaese, M. Fischer, A. Hemp for implementing the study design and the facilities as well as S.W. Ferger and R.S. Mary for help during fieldwork. M. Parepa, M.A.R. Mello and M. Tschapka for useful comments on the manuscript. G. Rutten and M. Helbig-Bonitz were sponsored by the Research-Unit 1246 (https://www.kilimanjaro.biozentrum.uni-wuerzburg.de/) of the German Research Foundation (DFG). The research permit was granted by COSTECH (2010-340-ER-NA-96-44 and 2011-340-ER-96-44) and TANAPA (TNO/HQ/C.10/13/VOL.III). NR 23 TC 1 Z9 1 U1 1 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0141-6707 EI 1365-2028 J9 AFR J ECOL JI Afr. J. Ecol. PD MAR PY 2014 VL 52 IS 1 BP 122 EP 125 DI 10.1111/aje.12090 PG 4 WC Ecology SC Environmental Sciences & Ecology GA AA6ER UT WOS:000331192100014 ER PT J AU Mawdsley, JR Mawdsley, AS Sithole, H Harrison, JD AF Mawdsley, Jonathan R. Mawdsley, Alice S. Sithole, Hendrik Harrison, James du G. TI High-resolution digital photography reveals details of plant-pollinator interactions in a southern African savannah SO AFRICAN JOURNAL OF ECOLOGY LA English DT Article C1 [Mawdsley, Jonathan R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Mawdsley, Alice S.] Cleveland State Univ, Cleveland, OH 44114 USA. [Sithole, Hendrik] Dept Invertebrates, Kimberley, South Africa. [Harrison, James du G.] Univ Witwatersrand, Sch Anim Plant & Environm Sci, Johannesburg, South Africa. RP Mawdsley, JR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187,POB 37012, Washington, DC 20013 USA. EM mawdsley@heinzctr.org NR 9 TC 1 Z9 1 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0141-6707 EI 1365-2028 J9 AFR J ECOL JI Afr. J. Ecol. PD MAR PY 2014 VL 52 IS 1 BP 126 EP 128 DI 10.1111/aje.12099 PG 3 WC Ecology SC Environmental Sciences & Ecology GA AA6ER UT WOS:000331192100015 ER PT J AU Reiner, WB Petzinger, C Power, ML Hyeroba, D Rothman, JM AF Reiner, Whitney B. Petzinger, Christina Power, Michael L. Hyeroba, David Rothman, Jessica M. TI Fatty Acids in Mountain Gorilla Diets: Implications for Primate Nutrition and Health SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE nutritional ecology; essential fatty acid; linoleic; alpha-linolenic; polyunsaturated; ape diets ID IMPENETRABLE NATIONAL-PARK; MONKEYS ALOUATTA-PALLIATA; SEASONAL-VARIATION; FRUIT ABUNDANCE; ENERGY; BRAIN; CHIMPANZEES; EVOLUTION; UGANDA; CERCOPITHECINES AB Little is known about the fatty acid composition of foods eaten by wild primates. A total of 18 staple foods that comprise 97% of the annual dietary intake of the mountain gorilla (Gorilla beringei) were analyzed for fatty acid concentrations. Fruits and herbaceous leaves comprise the majority of the diet, with fruits generally having a higher mean percentage of fat (of dry matter; DM), as measured by ether extract (EE), than herbaceous leaves (13.0%+/- SD 13.0% vs. 2.3 +/- SD 0.8%). The mean daily EE intake by gorillas was 3.1% (DM). Fat provided approximate to 14% of the total dietary energy intake, and approximate to 22% of the dietary non-protein energy intake. Saturated fatty acids accounted for 32.4% of the total fatty acids in the diet, while monounsaturated fatty acids accounted for 12.5% and polyunsaturated fatty acids (PUFA) accounted for 54.6%. Both of the two essential PUFA, linoleic acid (LA, n-6) and -linolenic acid (ALA, n-3), were found in all of the 17 staple foods containing crude fat and were among the three most predominant fatty acids in the diet: LA (C18:2n-6) (30.3%), palmitic acid (C16:0) (23.9%), and ALA (C18:3n-3) (21.2%). Herbaceous leaves had higher concentrations of ALA, while fruit was higher in LA. Fruits provided high amounts of fatty acids, especially LA, in proportion to their intake due to the higher fat concentrations; despite being low in fat, herbaceous leaves provided sufficient ALA due to the high intake of these foods. As expected, we found that wild mountain gorillas consume a diet lower in EE, than modern humans. The ratio of LA:ALA was 1.44, closer to agricultural paleolithic diets than to modern human diets. Am. J. Primatol. (c) 2013 Wiley Periodicals, Inc. C1 [Reiner, Whitney B.; Rothman, Jessica M.] CUNY Hunter Coll, New York, NY 10065 USA. [Reiner, Whitney B.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Petzinger, Christina; Power, Michael L.] Smithsonian Natl Zool Pk, Nutr Lab, Washington, DC USA. [Power, Michael L.] Amer Coll Obstetricians & Gynecologists, Res Dept, Washington, DC 20024 USA. [Hyeroba, David] Jane Goodall Inst, Entebbe, Uganda. [Rothman, Jessica M.] NYCEP, New York, NY USA. RP Rothman, JM (reprint author), CUNY Hunter Coll, Dept Anthropol, 695 Pk Ave,Room 724, New York, NY 10065 USA. EM jessica.rothman@hunter.cuny.edu OI Power, Michael/0000-0002-6120-3528 FU Jane V. Engel Family Foundation; Cornell University; Hunter College's Presidential Fund for Faculty Advancement FX Contract grant sponsor: Jane V. Engel Family Foundation; contract grant sponsor: Cornell University; contract grant sponsor: Hunter College's Presidential Fund for Faculty Advancement. NR 51 TC 6 Z9 6 U1 3 U2 47 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 EI 1098-2345 J9 AM J PRIMATOL JI Am. J. Primatol. PD MAR PY 2014 VL 76 IS 3 BP 281 EP 288 DI 10.1002/ajp.22232 PG 8 WC Zoology SC Zoology GA AA8OF UT WOS:000331354100008 PM 24243235 ER PT J AU Ritson-Williams, R Arnold, SN Paul, VJ Steneck, RS AF Ritson-Williams, R. Arnold, S. N. Paul, V. J. Steneck, R. S. TI Larval settlement preferences of Acropora palmata and Montastraea faveolata in response to diverse red algae SO CORAL REEFS LA English DT Article DE Larval ecology; Supply-side ecology; Coralline algae; Coral reefs; Recruitment ID CORAL RECRUITMENT; SCLERACTINIAN CORALS; PLANULA LARVAE; METAMORPHOSIS; PATTERNS; REEFS; ASSEMBLAGES; BEHAVIOR; CORALLINALES; CONSEQUENCES AB Settlement specificity can regulate recruitment but remains poorly understood for coral larvae. We studied larvae of the corals, Acropora palmata and Montastraea faveolata, to determine their rates of settlement and metamorphosis in the presence of ten species of red algae, including eight species of crustose coralline algae, one geniculated coralline and one encrusting peyssonnelid. Twenty to forty percent of larvae of A. palmata settled on coralline surfaces of Hydrolithon boergesenii, Lithoporella atlantica, Neogoniolithon affine, and Titanoderma prototypum, whereas none settled and metamorphosed on Neogoniolithon mamillare. Larvae of M. faveolata had 13-25 % settlement onto the surface of Amphiroa tribulus, H. boergesenii, N. affine, N. munitum, and T. prototypum, but had no settlement on the surface of N. mamillare, Porolithon pachydermum, and a noncoralline crust Peyssonnelia sp. Some of these algal species were common on Belizean reefs, but the species that induced the highest rates of larval settlement and metamorphosis tended to be rare and primarily found in low-light environments. The shallow coral, A. palmata, and the deeper coral, M. faveolata, both had increased larval settlement rates in the presence of only a few species of red algae found at deeper depths suggesting that patterns of coral distribution can only sometimes be related to the distribution of red algae species. C1 [Ritson-Williams, R.; Paul, V. J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Ritson-Williams, R.] Univ Hawaii Manoa, Dept Biol, Honolulu, HI 96822 USA. [Arnold, S. N.; Steneck, R. S.] Univ Maine, Darling Marine Ctr, Sch Marine Sci, Walpole, ME 04573 USA. RP Ritson-Williams, R (reprint author), Univ Hawaii Manoa, Dept Biol, Honolulu, HI 96822 USA. EM rrw33@hawaii.edu FU Hunterdon Oceanographic Fund; Marine Science Network at the Smithsonian Institution FX Special thanks to Nikki Fogarty for advice, intellectual discussions, and help with our experiments. We appreciate the logistical support of Klaus Ruetzler, Michael Carpenter, Zach Foltz, and Scott Jones for facilitating our work at Carrie Bow Cay. Belize Fisheries Department provided us with permits to conduct this research. This work was supported by the Hunterdon Oceanographic Fund and the Marine Science Network at the Smithsonian Institution. This is contribution number 953 of the Caribbean Coral Reef Ecosystems program and 935 of the Smithsonian Marine Station at Fort Pierce. NR 60 TC 11 Z9 11 U1 1 U2 55 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 EI 1432-0975 J9 CORAL REEFS JI Coral Reefs PD MAR PY 2014 VL 33 IS 1 BP 59 EP 66 DI 10.1007/s00338-013-1113-2 PG 8 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AA3AJ UT WOS:000330965000008 ER PT J AU Chollett, I Stoyle, G Box, S AF Chollett, I. Stoyle, G. Box, S. TI Honduran Miskito Cays: among the last unexplored reef systems in the Caribbean SO CORAL REEFS LA English DT Editorial Material C1 [Chollett, I.] Univ Exeter, MSEL, Exeter EX4 4PS, Devon, England. [Stoyle, G.] Seacology Ltd, Muston YO14 0ER, N Yorkshire, England. [Box, S.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Chollett, I (reprint author), Univ Queensland, Brisbane, Qld 4072, Australia. EM i.c.chollett-ordaz@exeter.ac.uk NR 1 TC 3 Z9 3 U1 0 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 EI 1432-0975 J9 CORAL REEFS JI Coral Reefs PD MAR PY 2014 VL 33 IS 1 BP 155 EP 155 DI 10.1007/s00338-013-1084-3 PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AA3AJ UT WOS:000330965000018 ER PT J AU Neal, BP Condit, C Liu, G dos Santos, S Kahru, M Mitchell, BG Kline, DI AF Neal, B. P. Condit, C. Liu, G. dos Santos, S. Kahru, M. Mitchell, B. G. Kline, D. I. TI When depth is no refuge: cumulative thermal stress increases with depth in Bocas del Toro, Panama SO CORAL REEFS LA English DT Article DE Temperature stress; Bleaching; Depth stratification; Caribbean ID CORAL-REEFS; CLIMATE-CHANGE; TEMPERATURE-VARIATION; LONG-TERM; RESILIENCE; MORTALITY; IMPACTS; SURFACE AB Coral reefs are increasingly affected by high-temperature stress events and associated bleaching. Monitoring and predicting these events have largely utilized sea surface temperature data, due to the convenience of using large-scale remotely sensed satellite measurements. However, coral bleaching has been observed to vary in severity throughout the water column, and variations in coral thermal stress across depths have not yet been well investigated. In this study, in situ water temperature data from 1999 to 2011 from three depths were used to calculate thermal stress on a coral reef in Bahia Almirante, Bocas del Toro, Panama, which was compared to satellite surface temperature data and thermal stress calculations for the same area and time period from the National Oceanic and Atmospheric Administration Coral Reef Watch Satellite Bleaching Alert system. The results show similar total cumulative annual thermal stress for both the surface and depth-stratified data, but with a striking difference in the distribution of that stress among the depth strata during different high-temperature events, with the greatest thermal stress unusually recorded at the deepest measured depth during the most severe bleaching event in 2005. Temperature records indicate that a strong density-driven temperature inversion may have formed in this location in that year, contributing to the persistence and intensity of bleaching disturbance at depth. These results indicate that depth may not provide a stress refuge from high water temperature events in some situations, and in this case, the water properties at depth appear to have contributed to greater coral bleaching at depth compared to near-surface locations. This case study demonstrates the importance of incorporating depth-stratified temperature monitoring and small-scale oceanographic and hydrologic data for understanding and predicting local reef responses to elevated water temperature events. C1 [Neal, B. P.; Kahru, M.; Mitchell, B. G.; Kline, D. I.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Condit, C.] Univ Calif San Diego, San Diego Supercomp Ctr, La Jolla, CA 92093 USA. [Liu, G.] NOAA Coral Reef Watch GST, College Pk, MD USA. [dos Santos, S.] Smithsonian Trop Res Inst, Phys Monitoring Program, Bocas Del Toro, Panama. RP Neal, BP (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. EM bpneal@ucsd.edu RI Liu, Gang/E-7921-2011 OI Liu, Gang/0000-0001-8369-6805 FU National Science Foundation, Cyber Enabled Discovery and Innovation Award [0941760]; NOAA Climate Data Record (CDR) Program FX This study was funded by the National Science Foundation, Cyber Enabled Discovery and Innovation Award # 0941760. Collection of SST data from GHRSST and the US National Oceanographic Data Center supported by the NOAA Climate Data Record (CDR) Program. In situ data provided by the Smithsonian Tropical Research Institute Physical Monitoring Program. NR 30 TC 2 Z9 2 U1 1 U2 26 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 EI 1432-0975 J9 CORAL REEFS JI Coral Reefs PD MAR PY 2014 VL 33 IS 1 BP 193 EP 205 DI 10.1007/s00338-013-1081-6 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AA3AJ UT WOS:000330965000022 ER PT J AU Seemann, J Gonzalez, CT Carballo-Bolanos, R Berry, K Heiss, GA Struck, U Leinfelder, RR AF Seemann, Janina Gonzalez, Cindy T. Carballo-Bolanos, Rodrigo Berry, Kathryn Heiss, Georg A. Struck, Ulrich Leinfelder, Reinhold R. TI Assessing the ecological effects of human impacts on coral reefs in Bocas del Toro, Panama SO ENVIRONMENTAL MONITORING AND ASSESSMENT LA English DT Article DE Reef cover; Biodiversity; Environmental; Biological monitoring ID GREAT-BARRIER-REEF; FISH COMMUNITY STRUCTURE; MARINE PROTECTED AREAS; PHASE-SHIFTS; CARIBBEAN CORAL; CLIMATE-CHANGE; FRESH-WATER; CONSERVATION STATUS; ALTERNATIVE STATES; CONTINENTAL REEFS AB Environmental and biological reef monitoring was conducted in Almirante Bay (Bahia Almirante) in Bocas del Toro, Panama, to assess impacts from anthropogenic developments. An integrated monitoring investigated how seasonal temperature stress, turbidity, eutrophication and physical impacts threatened reef health and biodiversity throughout the region. Environmental parameters such as total suspended solids [TSS], carbon isotopes (delta C-13), C/N ratios, chlorophyll a, irradiance, secchi depth, size fractions of the sediments and isotope composition of dissolved inorganic carbon [DIC] of the water were measured throughout the years 2010 and 2011 and were analysed in order to identify different impact sources. Compared to data from Collin et al. (Smithsonian Contributions to the Marine Sciences 38:324-334, 2009) chlorophyll a has doubled at sites close to the city and the port Almirante (from 0.46-0.49 to 0.78-0.97 mu g l(-1)) and suspension load increased, visible by a decrease in secchi depth values. Visibility decreased from 9-13 m down to 4 m at the bay inlet Boca del Drago, which is strongly exposed to river run off and dredging for the shipping traffic. Eutrophication and turbidity levels seemed to be the determining factor for the loss of hard coral diversity, most significant at chlorophyll a levels higher than 0.5 mu g l(-1) and TSS levels higher than 4.7 mg l(-1). Hard coral cover within the bay has also declined, at some sites down to < 10 % with extremely low diversities (7 hard coral species). The hard coral species Porites furcata dominated the reefs in highly impacted areas and showed a strong recovery after bleaching and a higher tolerance to turbidity and eutrophication compared to other hard coral species in the bay. Serious overfishing was detected in the region by a lack of adult and carnivorous fish species, such as grunts, snappers and groupers. Study sites less impacted by anthropogenic activities and/or those with local protection showed a higher hard coral cover and fish abundance; however, an overall loss of hard coral diversity was observed. C1 [Seemann, Janina; Heiss, Georg A.; Leinfelder, Reinhold R.] Free Univ Berlin, D-12249 Berlin, Germany. [Seemann, Janina; Carballo-Bolanos, Rodrigo; Berry, Kathryn] Humboldt Univ, D-10099 Berlin, Germany. [Seemann, Janina; Struck, Ulrich] Museum Nat Kunde, D-10115 Berlin, Germany. [Gonzalez, Cindy T.] Smithsonian Trop Res Inst, Balboaanconpanama, Panama. RP Seemann, J (reprint author), Free Univ Berlin, Malteserstr 74-100, D-12249 Berlin, Germany. EM janina.seemann@fu-berlin.de OI Leinfelder, Reinhold/0000-0002-4107-2161 FU von Pawel-Rammingen foundation; German Academic Exchange Service (DAAD) FX This study was supported by the von Pawel-Rammingen foundation and the German Academic Exchange Service (DAAD). We want to thank people from the Smithsonian Tropical Research Institute Bocas del Toro in particular Rachel Collin, Gabriel Jacome, Plinio Gondola and Eric Brown for their invaluable help, great support in organization, field work and space acquisition at the station. Special thanks to Ewgenija Kuhl for her great help in the isotope analysis and to Regine Bluhdorn for the English correction. Thank you Claudio Richter for your supervision, helpful input, discussions and advices. NR 84 TC 5 Z9 5 U1 9 U2 120 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-6369 EI 1573-2959 J9 ENVIRON MONIT ASSESS JI Environ. Monit. Assess. PD MAR PY 2014 VL 186 IS 3 BP 1747 EP 1763 DI 10.1007/s10661-013-3490-y PG 17 WC Environmental Sciences SC Environmental Sciences & Ecology GA 303ZP UT WOS:000330715300033 PM 24254491 ER PT J AU Bryson, RW Chaves, J Smith, BT Miller, MJ Winker, K Perez-Eman, JL Klicka, J AF Bryson, Robert W., Jr. Chaves, Jaime Smith, Brian Tilston Miller, Matthew J. Winker, Kevin Perez-Eman, Jorge L. Klicka, John TI Diversification across the New World within the 'blue' cardinalids (Aves: Cardinalidae) SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Ancestral area; birds; Cyanocompsa; dispersal; diversification rates; migration; Neotropics; Passerina; phylogeography ID GREAT AMERICAN INTERCHANGE; AVIAN DIVERSIFICATION; GENETIC DIVERSITY; CLIMATE-CHANGE; SOUTH-AMERICA; MOLECULAR PERSPECTIVE; NICHE CONSERVATISM; MIDDLE AMERICA; ANDEAN UPLIFT; SPECIATION AB AimTo examine the history of diversification of blue' cardinalids (Cardinalidae) across North and South America. LocationNorth America (including Middle America) and South America. MethodsWe collected 163 individuals of the 14 species of blue cardinalids and generated multilocus sequence data (3193 base pairs from one mitochondrial and three nuclear genes) to infer phylogeographical structure and reconstruct time-calibrated species trees. We then estimated the ancestral range at each divergence event and tested for temporal shifts in diversification rate. ResultsTwenty-five lineages of blue cardinalids clustered into two major clades: one confined to North America, and a second concentrated in South America. Blue cardinalids probably originated in North America, but reconstructions were influenced by how migrant taxa were assigned to biogeographical regions. Most of the pre-Pleistocene divergences between extant taxa occurred in the North American clade, whereas most divergences in South America and adjacent Middle America occurred during the Pleistocene. Despite these differences, the rate of diversification for both clades has been similar and relatively constant over the past 10 million years, with little geographical exchange between North and South America outside the Panamanian isthmus region. Main conclusionsOur reconstruction of the diversification history of blue cardinalids indicates a role of both Neogene and Quaternary events in generating biotic diversity across North and South America. Although ancestral area reconstruction suggests a possible North American origin for blue cardinalids, the occurrence of seasonal migration in this group and their relatives limits inference. Our study highlights the importance of considering ecological and behavioural characteristics together with palaeogeological events in order to gain an understanding of the diversification history of widespread, mobile taxonomic groups. C1 [Bryson, Robert W., Jr.; Klicka, John] Univ Washington, Dept Biol, Seattle, WA 98195 USA. [Bryson, Robert W., Jr.; Klicka, John] Univ Washington, Burke Museum Nat Hist & Culture, Seattle, WA 98195 USA. [Chaves, Jaime] Univ Miami, Dept Biol, Coral Gables, FL 33146 USA. [Chaves, Jaime] Univ San Francisco Quito, Colegio Ciencias Biol & Ambientales, Quito, Ecuador. [Smith, Brian Tilston] Louisiana State Univ, Louisiana Museum Nat Sci, Baton Rouge, LA 70803 USA. [Miller, Matthew J.] Smithsonian Trop Res Inst, Panama City, Panama. [Miller, Matthew J.; Winker, Kevin] Univ Alaska Museum, Fairbanks, AK 99775 USA. [Perez-Eman, Jorge L.] Cent Univ Venezuela, Inst Zool & Ecol Trop, Caracas 1041 A, Venezuela. [Perez-Eman, Jorge L.] Colecc Ornitol Phelps, Caracas 1010 A, Venezuela. RP Bryson, RW (reprint author), Univ Washington, Dept Biol, Box 351800, Seattle, WA 98195 USA. EM brysonjr@uw.edu RI Winker, Kevin/M-2042-2014; caputo, carlo/N-3747-2014; OI Winker, Kevin/0000-0002-8985-8104; Miller, Matthew/0000-0002-2939-0239 NR 84 TC 6 Z9 6 U1 1 U2 32 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 EI 1365-2699 J9 J BIOGEOGR JI J. Biogeogr. PD MAR PY 2014 VL 41 IS 3 BP 587 EP 599 DI 10.1111/jbi.12218 PG 13 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA AA2EL UT WOS:000330907800015 ER PT J AU Winston, B Hausmann, S Escobar, J Kenney, WF AF Winston, Byron Hausmann, Sonja Escobar, Jaime Kenney, William F. TI A sediment record of trophic state change in an Arkansas (USA) reservoir SO JOURNAL OF PALEOLIMNOLOGY LA English DT Article DE Paleolimnology; Reservoir; Sediments; Water quality; Geochemistry ID ORGANIC-MATTER; NITRATE UTILIZATION; DELTA-N-15 VALUES; DIATOM ANALYSIS; LAKE; NITROGEN; EUTROPHICATION; PHOSPHORUS; CARBON; DELTA-C-13 AB Reservoir sediments are used cautiously in paleolimnological studies because of dating uncertainties, possible sediment disturbances and even concerns that indicators of trophic status may behave differently in reservoirs as opposed to natural lakes. We measured loss on ignition (LOI), carbon to nitrogen ratio (C:N), diatom abundance, total nitrogen (TN), total phosphorus (TP), TN:TP ratio, and carbon and nitrogen isotopes (delta C-13 and delta N-15) in an 83-cm sediment core to track recent trophic status changes in Beaver Reservoir, Northwest Arkansas, USA. Measurements showed that LOI, TN, TP and diatom abundance increased significantly from the bottom to the top of the core (p < 0.001). The C:N ratio and delta C-13 indicated a predominantly algal source for organic matter in the sediments. Increases in TN and TP were positively correlated with human population growth (p < 0.01) and the TN:TP ratio recorded a shift from phosphorus to nitrogen limitation around 1990. This shift may have encouraged cyanobacterial growth that caused episodes of taste and odor problems in the reservoir. This study suggests that despite concerns about sediment dating and disturbance, reservoir sediments can provide valuable information on past water quality changes. C1 [Winston, Byron] Univ Arkansas, Dept Crop Soil & Environm Sci, Fayetteville, AR 72701 USA. [Hausmann, Sonja] Drexel Univ, Acad Nat Sci, Philadelphia, PA 19103 USA. [Escobar, Jaime] Univ Norte, Dept Ingn Civil & Ambiental, Barranquilla, Colombia. [Escobar, Jaime] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Panama City, Panama. [Kenney, William F.] Univ Florida, Land Use & Environm Change Inst, Gainesville, FL 32611 USA. RP Winston, B (reprint author), Univ Arkansas, Dept Crop Soil & Environm Sci, 114 Plant Sci Bldg, Fayetteville, AR 72701 USA. EM bwinsto@uark.edu FU NSF; Arkansas Water Resource Center; Beaver Water District; USGS [104B] FX We thank the Beaver Water District for assistance with fieldwork, and Anna Nottemeir. We also thank Troy Munhofen and Lanayah Turley, NSF-funded REU students who assisted with stable isotope measurements during the summer of 2009. Funding for this project was provided by the Arkansas Water Resource Center, Beaver Water District and a USGS 104B Grant. NR 46 TC 2 Z9 3 U1 6 U2 39 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0921-2728 EI 1573-0417 J9 J PALEOLIMNOL JI J. Paleolimn. PD MAR PY 2014 VL 51 IS 3 BP 393 EP 403 DI 10.1007/s10933-013-9762-2 PG 11 WC Environmental Sciences; Geosciences, Multidisciplinary; Limnology SC Environmental Sciences & Ecology; Geology; Marine & Freshwater Biology GA AA4ZP UT WOS:000331105500005 ER PT J AU Vidal, EAG Vecchione, M von Boletzky, S AF Vidal, Erica A. G. Vecchione, Mike von Boletzky, Sigurd TI Dedication to Professor Malcolm R. Clarke (1930-2013) SO HYDROBIOLOGIA LA English DT Editorial Material C1 [Vidal, Erica A. G.] Univ Parana, Ctr Marine Studies, Pontal Do Parana, PR, Brazil. [Vecchione, Mike] Smithsonian Inst, NMFS Natl Systemat Lab, Natl Museum Nat Hist, Washington, DC 20560 USA. [von Boletzky, Sigurd] CNRS, Lab Arago, Banyuls Sur Mer, France. RP Vidal, EAG (reprint author), Univ Parana, Ctr Marine Studies, Pontal Do Parana, PR, Brazil. EM erica.vidal@ufpr.br NR 0 TC 1 Z9 1 U1 1 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 EI 1573-5117 J9 HYDROBIOLOGIA JI Hydrobiologia PD MAR PY 2014 VL 725 IS 1 BP 1 EP 1 DI 10.1007/s10750-013-1789-x PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 302ZQ UT WOS:000330644400001 ER PT J AU Strugnell, JM Norman, MD Vecchione, M Guzik, M Allcock, AL AF Strugnell, Jan M. Norman, Mark D. Vecchione, Michael Guzik, Michelle Allcock, A. Louise TI The ink sac clouds octopod evolutionary history SO HYDROBIOLOGIA LA English DT Article DE Octopoda; Evolution; Molecular; Phylogenetics ID LENGTH DIFFERENCE TEST; COLEOID CEPHALOPODS MOLLUSCA; MOLECULAR PHYLOGENY; SOUTHERN-OCEAN; VULCANOCTOPUS-HYDROTHERMALIS; INCONGRUENCE; CHARACTER; OCTOPUSES; ORIGIN; MODEL AB Difficulties in elucidating the evolutionary history of the octopods have arisen from problems in identifying informative morphological characters. Recent classifications have divided the largest group, the incirrate octopods, into five groups. These include the pelagic superfamily Argonautoidea and three gelatinous pelagic families (Vitreledonellidae, Bolitaenidae, Amphitretidae). All benthic incirrate octopods have been accommodated in the family Octopodidae, itself divided into four subfamilies, Octopodinae, Eledoninae, Bathypolypodinae and Graneledoninae, which are defined by the presence or absence of an ink sac, and uniserial or biserial sucker arrangements on the arms. We used relaxed clock models in a Bayesian framework and maximum likelihood methods to analyse three nuclear and four mitochondrial genes of representatives from each of the previous subfamilies. Strong evidence indicates that the family Octopodidae is paraphyletic and contains the gelatinous pelagic families. The subfamilies of Octopodidae recognised in earlier works do not reflect evolutionary history. The following clades were supported in all analyses: (1) Eledone/Aphrodoctopus, (2) Callistoctopus/Grimpella/Macroctopus/Scaeurgus, (3) Abdopus/Ameloctopus/Amphioctopus/Cistopus/Hapalochlaena/Octopus, (4) Enteroctopus/Muusoctopus/Vulcanoctopus, (5) Vitreledonella/Japetella, (6) Southern Ocean endemic and deep-sea taxa with uniserial suckers. These clades form the basis for a suite of taxa assigned family taxonomic rank: Amphitretidae, Bathypolypodidae, Eledonidae, Enteroctopodidae, Megaleledonidae and Octopodidae sensu nov. They are placed within the superfamily Octopodoidea. C1 [Strugnell, Jan M.] La Trobe Univ, Dept Genet, La Trobe Inst Mol Sci, Bundoora, Vic 3086, Australia. [Norman, Mark D.] Museum Victoria, Melbourne, Vic 3001, Australia. [Vecchione, Michael] Smithsonian Inst, NMFS Natl Systemat Lab, Natl Museum Nat Hist, Washington, DC 20013 USA. [Guzik, Michelle] Univ Adelaide, Australian Ctr Evolutionary Biol & Biodivers, Sch Earth & Environm Sci, Adelaide, SA, Australia. [Allcock, A. Louise] Natl Univ Ireland, Sch Nat Sci, Galway, Ireland. [Allcock, A. Louise] Natl Univ Ireland, Ryan Inst, Galway, Ireland. RP Strugnell, JM (reprint author), La Trobe Univ, Dept Genet, La Trobe Inst Mol Sci, Bundoora, Vic 3086, Australia. EM J.Strugnell@latrobe.edu.au RI Allcock, Louise/A-7359-2012; Strugnell, Jan/P-9921-2016 OI Allcock, Louise/0000-0002-4806-0040; FU Natural Environment Research Council (NERC) Antarctic Funding Initiative (AFI) [NE/C506321/1]; Lloyd's Tercentenary Fellowship; Systematic Association grant; Antarctic Science Bursary; Edith Mary Pratt Musgrave fund FX Jan Strugnell was supported by Natural Environment Research Council (NERC) Antarctic Funding Initiative (AFI) NE/C506321/1 (awarded to Louise Allcock), and a Lloyd's Tercentenary Fellowship, a Systematic Association grant, an Antarctic Science Bursary and the Edith Mary Pratt Musgrave fund. We are grateful to David Carlini, Joao Sendao, C.C. Lu, Malcom Smale, Sean Fennessey, Janet Voight and Roger Villanueva for providing tissue samples which made this study possible. The majority of the analyses in this paper were done on the CamGrid cluster at the University of Cambridge and we are grateful to the Cambridge eScience Centre for its support of the system. NR 88 TC 10 Z9 11 U1 4 U2 55 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 EI 1573-5117 J9 HYDROBIOLOGIA JI Hydrobiologia PD MAR PY 2014 VL 725 IS 1 BP 215 EP 235 DI 10.1007/s10750-013-1517-6 PG 21 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 302ZQ UT WOS:000330644400018 ER PT J AU Hayes, P Turner, BL Lambers, H Laliberte, E AF Hayes, Patrick Turner, Benjamin L. Lambers, Hans Laliberte, Etienne TI Foliar nutrient concentrations and resorption efficiency in plants of contrasting nutrient-acquisition strategies along a 2-million-year dune chronosequence SO JOURNAL OF ECOLOGY LA English DT Article ID PHOSPHORUS-IMPOVERISHED SOILS; TEMPERATE RAIN-FOREST; WESTERN-AUSTRALIA; MANGANESE ACCUMULATION; LITTER DECOMPOSITION; TERRESTRIAL PLANTS; LIMITATION; PROTEACEAE; NITROGEN; LEAVES C1 [Hayes, Patrick; Turner, Benjamin L.; Lambers, Hans; Laliberte, Etienne] Univ Western Australia, Sch Plant Biol, Perth, WA 6009, Australia. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. 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 Hayes, Patrick/D-4679-2014; Turner, Benjamin/E-5940-2011; Laliberte, Etienne/B-6855-2008; Lambers, Hans/A-1544-2008 OI Hayes, Patrick/0000-0001-7554-4588; Turner, Benjamin/0000-0002-6585-0722; Laliberte, Etienne/0000-0002-3167-2622; Lambers, Hans/0000-0002-4118-2272 FU Western Australia Department of Environment and Conservation; School of Plant Biology, UWA Research Development Award; ARC DECRA [DE120100352]; ARC [DP0985685] FX We thank Graham Zemunik for help with plant species identification and for providing the vegetation cover data. Staff from ChemCentre (Perth, Western Australia), particularly Katrina Walton, provided guidance for leaf nutrient analyses. Greg Cawthray, Elizabeth Halladin and Paul Damon provided technical assistance with sample preparation. We also thank Troy Allwright and Osmarina Marinho for help with field work, and the Western Australia Department of Environment and Conservation for their support and collaboration. Funding came from the School of Plant Biology, a UWA Research Development Award and ARC DECRA (DE120100352) grant to E. L., and an ARC Discovery (DP0985685) to H.L. NR 81 TC 51 Z9 51 U1 15 U2 116 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 EI 1365-2745 J9 J ECOL JI J. Ecol. PD MAR PY 2014 VL 102 IS 2 BP 396 EP 410 PG 15 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA AB0FN UT WOS:000331467300011 ER PT J AU Hopkins, MJ Simpson, C Kiessling, W AF Hopkins, Melanie J. Simpson, Carl Kiessling, Wolfgang TI Differential niche dynamics among major marine invertebrate clades SO ECOLOGY LETTERS LA English DT Article DE Carbonate environments; climate change; niche conservatism; species turnover; substrate affinity; terrigenous clastic environments ID LATITUDINAL DIVERSITY GRADIENT; CONSERVATION BIOLOGY; BIO-MINERALOGY; EVOLUTION; BIODIVERSITY; HISTORY; TIME; MORPHOLOGY; PATTERNS; BREADTH AB The degree to which organisms retain their environmental preferences is of utmost importance in predicting their fate in a world of rapid climate change. Notably, marine invertebrates frequently show strong affinities for either carbonate or terrigenous clastic environments. This affinity is due to characteristics of the sediments as well as correlated environmental factors. We assessed the conservatism of substrate affinities of marine invertebrates over geological timescales, and found that niche conservatism is prevalent in the oceans, and largely determined by the strength of initial habitat preference. There is substantial variation in niche conservatism among major clades with corals and sponges being among the most conservative. Time-series analysis suggests that niche conservatism is enhanced during times of elevated nutrient flux, whereas niche evolution tends to occur after mass extinctions. Niche evolution is not necessarily elevated in genera exhibiting higher turnover in species composition. C1 [Hopkins, Melanie J.; Kiessling, Wolfgang] Univ Erlangen Nurnberg, GeoZentrum Nordbayern, D-91054 Erlangen, Germany. [Hopkins, Melanie J.; Simpson, Carl; Kiessling, Wolfgang] Humboldt Univ, Leibniz Inst Evolut & Biodiversitatsforsch, Museum Nat Kunde, D-10115 Berlin, Germany. [Simpson, Carl] Smithsonian Inst, Natl Museum Amer Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Hopkins, MJ (reprint author), Univ Erlangen Nurnberg, GeoZentrum Nordbayern, Loewenichstr 28, D-91054 Erlangen, Germany. EM Melanie.Hopkins@fau.de RI Kiessling, Wolfgang/E-2259-2015 NR 50 TC 12 Z9 12 U1 0 U2 30 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1461-023X EI 1461-0248 J9 ECOL LETT JI Ecol. Lett. PD MAR PY 2014 VL 17 IS 3 BP 314 EP 323 DI 10.1111/ele.12232 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 291IV UT WOS:000329823300006 PM 24313951 ER PT J AU Narukage, N Sakao, T Kano, R Shimojo, M Winebarger, A Weber, M Reeves, KK AF Narukage, N. Sakao, T. Kano, R. Shimojo, M. Winebarger, A. Weber, M. Reeves, K. K. TI Coronal-Temperature-Diagnostic Capability of the Hinode/X-Ray Telescope Based on Self-consistent Calibration. II. Calibration with On-Orbit Data SO SOLAR PHYSICS LA English DT Article DE Corona; Instrumentation and data management ID XRT; MISSION AB The X-Ray Telescope (XRT) onboard the Hinode satellite is an X-ray imager that observes the solar corona with the capability of diagnosing coronal temperatures from less than 1 MK to more than 10 MK. To make full use of this capability, Narukage et al. (Solar Phys. 269, 169, 2011) determined the thickness of each of the X-ray focal-plane analysis filters based on calibration measurements from the ground-based end-to-end test. However, in their paper, the calibration of the thicker filters for observations of active regions and flares, namely the med-Be, med-Al, thick-Al and thick-Be filters, was insufficient due to the insufficient X-ray flux used in the measurements. In this work, we recalibrate those thicker filters using quiescent active region data taken with multiple filters of XRT. On the basis of our updated calibration results, we present the revised coronal-temperature-diagnostic capability of XRT. C1 [Narukage, N.; Sakao, T.] Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Kano, R.; Shimojo, M.] NAOJ, Mitaka, Tokyo 1818588, Japan. [Winebarger, A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Weber, M.; Reeves, K. K.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Narukage, N (reprint author), Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan. EM narukage@solar.isas.jaxa.jp RI Reeves, Katharine/P-9163-2014; Shimojo, Masumi/J-2605-2016 OI Shimojo, Masumi/0000-0002-2350-3749 FU NASA [NNM07AB07C] FX The authors thank members of the XRT team for useful discussions and comments. Hinode is a Japanese mission developed and launched by ISAS/JAXA, collaborating with NAOJ as a domestic partner, NASA and STFC (UK) as international partners. Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/JAXA. This team mainly consists of scientists from institutes in the partner countries. Support for the post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK), NASA, ESA, and NSC (Norway). MW and KKR acknowledge support from contract NNM07AB07C through NASA to SAO. NR 7 TC 12 Z9 12 U1 0 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD MAR PY 2014 VL 289 IS 3 BP 1029 EP 1042 DI 10.1007/s11207-013-0368-7 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268VV UT WOS:000328199700024 ER PT J AU Grant, JA Wilson, SA Mangold, N Calef, F Grotzinger, JP AF Grant, John A. Wilson, Sharon A. Mangold, Nicolas Calef, Fred, III Grotzinger, John P. TI The timing of alluvial activity in Gale crater, Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Mars; Gale crater; alluvial fan; craters; Hesperian ID CONSTRAINTS; CHRONOLOGY; EVOLUTION; MOUND AB The Curiosity rover's discovery of rocks preserving evidence of past habitable conditions in Gale crater highlights the importance of constraining the timing of responsible depositional settings to understand the astrobiological implications for Mars. Crater statistics and mapping reveal the bulk of the alluvial deposits in Gale, including those interrogated by Curiosity, were likely emplaced during the Hesperian, thereby implying that habitable conditions persisted after the Noachian. Crater counting data sets and upper Peace Vallis fan morphology also suggest a possible younger period of fluvial activation that deposited similar to 10-20m of sediments on the upper fan after emplacement of the main body of the fan. If validated, water associated with later alluvial activity may have contributed to secondary diagenetic features in Yellowknife Bay. Key Points The bulk of alluvial deposits in Gale were likely emplaced during the Hesperian Habitable conditions persisted in Gale crater after the Noachian Limited evidence for possible younger fluvial activation on Peace Vallis fan C1 [Grant, John A.; Wilson, Sharon A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Mangold, Nicolas] Univ Nantes, LPGN CNRS UMR6112, Lab Planetol & Geodynam Nantes, Nantes, France. [Calef, Fred, III] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA. [Grotzinger, John P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Grant, JA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM grantj@si.edu FU NASA FX We thank the Jet Propulsion Laboratory, University of Arizona, Ball Aerospace, Malin Space Science Systems, and Lockheed Martin that built and operate the Curiosity rover, HiRISE and CTX cameras, and the Mars Reconnaissance Orbiter. Reviews by Devon Burr and David Crown improved this paper. This work was supported by NASA. NR 23 TC 18 Z9 18 U1 0 U2 23 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 28 PY 2014 VL 41 IS 4 BP 1142 EP 1148 DI 10.1002/2013GL058909 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AD1VV UT WOS:000333022700010 ER PT J AU Simon, R Knoernschild, M Tschapka, M Schneider, A Passauer, N Kalko, EKV von Helversen, O AF Simon, Ralph Knoernschild, Mirjam Tschapka, Marco Schneider, Annkathrin Passauer, Nadine Kalko, Elisabeth K. V. von Helversen, Otto TI Biosonar resolving power: echo-acoustic perception of surface structures in the submillimeter range SO FRONTIERS IN PHYSIOLOGY LA English DT Article DE echolocation; bat; resolving power; structure recognition; resolution ID NECTAR-FEEDING BATS; BIG BROWN BAT; ECHOLOCATING BAT; EPTESICUS-FUSCUS; DISCRIMINATION; SONAR; TARGETS; IMAGES; RECEIVER; MODEL AB The minimum distance for which two points still can be separated from each other defines the resolving power of a visual system. In an echo-acoustic context, the resolving power is usually measured as the smallest perceivable distance of two reflecting surfaces on the range axis and is found to be around half a millimeter for bats employing frequency modulated (FM) echolocation calls. Only few studies measured such thresholds with physical objects, most often bats were trained on virtual echoes i.e., echoes generated and played back by a computer; moreover, bats were sitting while they received the stimuli. In these studies differences in structure depth between 200 and 340 mu m were found. However, these low thresholds were never verified for free-flying bats and real physical objects. Here, we show behavioral evidence that the echo-acoustic resolving power for surface structures in fact can be as low as measured for computer generated echoes and even lower, sometimes below 100 mu m. We found this exceptional fine discrimination ability only when one of the targets showed spectral interferences in the frequency range of the bats' echolocation call while the other target did not. This result indicates that surface structure is likely to be perceived as a spectral quality rather than being perceived strictly in the time domain. Further, it points out that sonar resolving power directly depends on the highest frequency/shortest wavelength of the signal employed. C1 [Simon, Ralph] Univ Erlangen Nurnberg, Dept Sensor Technol, D-91052 Erlangen, Germany. [Simon, Ralph; Knoernschild, Mirjam; Tschapka, Marco; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Knoernschild, Mirjam; Tschapka, Marco; Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Schneider, Annkathrin; Passauer, Nadine; von Helversen, Otto] Univ Erlangen Nurnberg, Inst Zool, D-91052 Erlangen, Germany. RP Simon, R (reprint author), Univ Erlangen Nurnberg, Dept Sensor Technol, Paul Gordan Str 3-5, D-91052 Erlangen, Germany. EM ralph.simon@fau.de RI Knornschild, Mirjam/C-9401-2011 FU Deutsche Forschungsgemeinschaft [HE 1180/15]; Deutsche Forschungsgemeinschaft and Friedrich-Alexander-University Erlangen-Nuremberg FX We are grateful to Reinhard Lerch and Stefan Rupitsch for valuable suggestions on the manuscript. We thank Benjamin Fink for helping us to set up the training apparatus and Klaus Hochradel for help with figures. This work was supported by Deutsche Forschungsgemeinschaft (HE 1180/15) and we acknowledge support by Deutsche Forschungsgemeinschaft and Friedrich-Alexander-University Erlangen-Nuremberg within the funding programme Open Access Publishing. NR 29 TC 3 Z9 4 U1 0 U2 8 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1664-042X J9 FRONT PHYSIOL JI Front. Physiol. PD FEB 26 PY 2014 VL 5 AR UNSP 64 DI 10.3389/fphys.2014.00064 PG 9 WC Physiology SC Physiology GA AX3HG UT WOS:000346830100001 PM 24616703 ER PT J AU Cikanek, SJ Nockold, S Brown, JL Carpenter, JW Estrada, A Guerrel, J Hope, K Ibanez, R Putman, SB Gratwicke, B AF Cikanek, Shawna J. Nockold, Simon Brown, Janine L. Carpenter, James W. Estrada, Angie Guerrel, Jorge Hope, Katharine Ibanez, Roberto Putman, Sarah B. Gratwicke, Brian TI Evaluating Group Housing Strategies for the Ex-Situ Conservation of Harlequin Frogs (Atelopus spp.) Using Behavioral and Physiological Indicators SO PLOS ONE LA English DT Article ID TOAD RHINELLA-MARINA; CORTICOSTERONE RESPONSES; BUFONIDAE; STRESS; EXTINCTIONS; METABOLISM; AMPHIBIANS; DECLINES; CAPTURE; FELIDS AB We have established ex situ assurance colonies of two endangered Panamanian harlequin frogs, Atelopus certus and Atelopus glyphus, but observed that males fought with each other when housed as a group. Housing frogs individually eliminated this problem, but created space constraints. To evaluate the potential stress effects from aggressive interactions when grouping frogs, we housed male frogs in replicated groups of one, two, and eight. We measured aggressive behavioral interactions and fecal glucocorticoid metabolite (GC) concentrations as indicators of stress in each tank. In both small and large groups, frogs initially interacted aggressively, but aggressive interactions and fecal GCs declined significantly after the first 2 weeks of being housed together, reaching the lowest levels by week 4. We conclude that aggressive interactions in same-sex groups of captive Atelopus may initially cause stress, but the frogs become habituated within a few weeks and they can safely be housed in same-sex groups for longer periods of time. C1 [Cikanek, Shawna J.; Carpenter, James W.] Kansas State Univ, Coll Vet Med, Dept Clin Sci, Manhattan, KS 66506 USA. [Nockold, Simon; Estrada, Angie; Guerrel, Jorge; Ibanez, Roberto] Smithsonian Trop Res Inst, Panama Amphibian Rescue & Conservat Project, Gamboa, Panama. [Brown, Janine L.; Hope, Katharine; Putman, Sarah B.; Gratwicke, Brian] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. RP Gratwicke, B (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. EM gratwickeb@si.edu FU Africam Safari; Cheyenne Mountain Zoo; Houston Zoo; Smithsonian Conservation Biology Institute; Smithsonian Tropical Research Institute; Zoo New England; US Fish and Wildlife Service program Wildlife Without Borders, USAID; Shared Earth Foundation; Anele Kolohe Foundation; Defenders of Wildlife FX The authors conducted this research under the auspices of the Panama Amphibian Rescue and Conservation Project, a partnership between Africam Safari, the Cheyenne Mountain Zoo, Defenders of Wildlife, the Houston Zoo, the Smithsonian Conservation Biology Institute, the Smithsonian Tropical Research Institute and Zoo New England. The authors would like to thank the US Fish and Wildlife Service program Wildlife Without Borders, USAID, the Shared Earth Foundation and the Anele Kolohe Foundation for financial support of aspects of this program that made this work possible. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 29 TC 3 Z9 3 U1 10 U2 28 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 25 PY 2014 VL 9 IS 2 AR e90218 DI 10.1371/journal.pone.0090218 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC2ZX UT WOS:000332385900129 PM 24587290 ER PT J AU Kistler, L Montenegro, A Smith, BD Gifford, JA Green, RE Newsom, LA Shapiro, B AF Kistler, Logan Montenegro, Alvaro Smith, Bruce D. Gifford, John A. Green, Richard E. Newsom, Lee A. Shapiro, Beth TI Transoceanic drift and the domestication of African bottle gourds in the Americas SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE long-distance dispersal; New World domestication; archaeogenomics ID LAST GLACIAL MAXIMUM; LAGENARIA-SICERARIA; SOUTH-ATLANTIC; ASIAN ORIGIN; DNA; CUCURBITACEAE; SIMULATION; CIRCULATION; DYNAMICS; PLANTS AB Bottle gourd (Lagenaria siceraria) was one of the first domesticated plants, and the only one with a global distribution during pre-Columbian times. Although native to Africa, bottle gourd was in use by humans in east Asia, possibly as early as 11,000 y ago (BP) and in the Americas by 10,000 BP. Despite its utilitarian importance to diverse human populations, it remains unresolved how the bottle gourd came to be so widely distributed, and in particular how and when it arrived in the New World. A previous study using ancient DNA concluded that Paleoindians transported already domesticated gourds to the Americas from Asia when colonizing the New World [Erickson et al. (2005) Proc Natl Acad Sci USA 102 (51):18315-18320]. However, this scenario requires the propagation of tropical-adapted bottle gourds across the Arctic. Here, we isolate 86,000 base pairs of plastid DNA from a geographically broad sample of archaeological and living bottle gourds. In contrast to the earlier results, we find that all pre-Columbian bottle gourds are most closely related to African gourds, not Asian gourds. Ocean-current drift modeling shows that wild African gourds could have simply floated across the Atlantic during the Late Pleistocene. Once they arrived in the New World, naturalized gourd populations likely became established in the Neotropics via dispersal by megafaunal mammals. These wild populations were domesticated in several distinct New World locales, most likely near established centers of food crop domestication. C1 [Kistler, Logan; Newsom, Lee A.] Penn State Univ, Dept Anthropol, University Pk, PA 16802 USA. [Newsom, Lee A.] Penn State Univ, Inst Energy, University Pk, PA 16802 USA. [Newsom, Lee A.] Penn State Univ, Inst Environm, University Pk, PA 16802 USA. [Montenegro, Alvaro] Ohio State Univ, Dept Geog, Columbus, OH 43210 USA. [Smith, Bruce D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. [Gifford, John A.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Affairs & Policy, Miami, FL 33149 USA. [Shapiro, Beth] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Green, Richard E.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. RP Kistler, L (reprint author), Penn State Univ, Dept Anthropol, University Pk, PA 16802 USA. EM ljk187@psu.edu RI Montenegro, Alvaro/B-4744-2013; OI Montenegro, Alvaro/0000-0001-6848-1996; Kistler, Logan/0000-0002-5730-5986; Shapiro, Beth/0000-0002-2733-7776 FU Pennsylvania State University College of Liberal Arts; Huck Institute of Life Sciences [NSF ARC-09090456]; University of California at Cruz; Universidade Estadual Paulista FX Modern samples were provided by B. D. S., Deena Decker-Walters, Mike Burtenshaw, the US Department of Agriculture-Agricultureal Research Service National Plant Germplasm System, and the Indiana University Herbarium. Access to ancient specimens was granted by the Phoebe A. Hearst Museum of Anthropology at University of California at Berkeley, the National Museum of Natural History at the Smithsonian Institution, the University Museum at the University of Arkansas, and the Kentucky Archaeological Survey. The El Gigante specimen was provided by Ken Hirth, and the Spring Branch Shelter specimen was provided by Jack Rossen. This work was supported in part by Pennsylvania State University College of Liberal Arts and Huck Institute of Life Sciences Grant NSF ARC-09090456, start-up funds from the University of California at Cruz (to B. S.), and the Universidade Estadual Paulista (A.M.). NR 44 TC 14 Z9 14 U1 3 U2 26 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 FEB 25 PY 2014 VL 111 IS 8 BP 2937 EP 2941 DI 10.1073/pnas.1318678111 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AC0JP UT WOS:000332180900023 PM 24516122 ER PT J AU Okawa, H Cardoso, V Pani, P AF Okawa, Hirotada Cardoso, Vitor Pani, Paolo TI Collapse of self-interacting fields in asymptotically flat spacetimes: Do self-interactions render Minkowski spacetime unstable? SO PHYSICAL REVIEW D LA English DT Article ID NUMERICAL RELATIVITY; SCALAR FIELD; STARS AB The nonlinear instability of anti-de Sitter spacetime has recently been established with the striking result that generic initial data collapse to form black holes. This outcome suggests that confined matter might generically collapse, and that collapse could only be halted-at most-by nonlinear bound states. Here, we provide evidence that such a mechanism can operate even in asymptotically flat spacetimes by studying the evolution of the Einstein-Klein-Gordon system for a self-interacting scalar field. We show that (i) configurations which do not collapse promptly can do so after successive reflections off the potential barrier, but (ii) that at intermediate amplitudes and Compton wavelengths, collapse to black holes is replaced by the appearance of oscillating soliton stars, or "oscillatons." Finally, (iii) for very small initial amplitudes, the field disperses away in a manner consistent with power-law tails of massive fields. Minkowski is stable against gravitational collapse. Our results provide one further piece to the rich phenomenology of gravitational collapse and show the important interplay between bound states, blueshift, dissipation and confinement effects. C1 [Okawa, Hirotada; Cardoso, Vitor; Pani, Paolo] Univ Lisbon, CENTRA, Inst Super Tecn, Dept Fis, P-1049 Lisbon, Portugal. [Cardoso, Vitor] Perimeter Inst Theoret Phys, Waterloo, ON N2J 2W9, Canada. [Pani, Paolo] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Okawa, H (reprint author), Univ Lisbon, CENTRA, Inst Super Tecn, Dept Fis, Ave Rovisco Pais 1, P-1049 Lisbon, Portugal. RI Pani, Paolo/G-7412-2012; Cardoso, Vitor/K-1877-2015 OI Pani, Paolo/0000-0003-4443-1761; Okawa, Hirotada/0000-0001-7372-5131; Cardoso, Vitor/0000-0003-0553-0433 FU European Union's FP7 ERC Starting Grant [DyBHo-256667]; Intra-European Marie Curie Contract [aStronGR-2011-298297]; Perimeter Institute for Theoretical Physics; Government of Canada through Industry Canada; province of Ontario through the Ministry of Economic Development Innovation; NRHEP [295189]; FCT-Portugal [CERN/FP/123593/2011, IF/00293/2013] FX We appreciate useful discussions with Juan Degollado, Oscar Dias, Roberto Emparan, Gyula Fodor, Akihiro Ishibashi, Luis Lehner, Maciej Maliborski, Jose Natario, Andrzej Rostworowski, Jorge Santos and all participants of the "NR/HEP2 Spring School" in Lisbon, of the YITP-T-11-08 workshop on "Recent advances in numerical and analytical methods for black hole dynamics," the Perimeter Institute workshop "Exploring AdS-CFT Dualities in Dynamical Settings," and the "MM13" meeting in Mons. We acknowledge financial support provided under the European Union's FP7 ERC Starting Grant "The dynamics of black holes: testing the limits of Einstein's theory" Grant No. DyBHo-256667 and through the Intra-European Marie Curie Contract No. aStronGR-2011-298297. This research was supported in part by the Perimeter Institute for Theoretical Physics. Research at the Perimeter Institute is supported by the Government of Canada through Industry Canada and by the province of Ontario through the Ministry of Economic Development & Innovation. This work was also supported by the NRHEP Grant No. 295189 FP7-PEOPLE-2011-IRSES, and by FCT-Portugal through Grants No. CERN/FP/123593/2011 and No. IF/00293/2013. Computations were performed on the "Baltasar Sete-Sois" cluster at IST and on the "venus" cluster at YITP. NR 29 TC 13 Z9 13 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD FEB 24 PY 2014 VL 89 IS 4 AR 041502 DI 10.1103/PhysRevD.89.041502 PG 6 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AC0GA UT WOS:000332171600001 ER PT J AU Bryan, ML Alsubai, KA Latham, DW Parley, NR Cameron, AC Quinn, SN Carter, JA Fulton, BJ Berlind, P Brown, WR Buchhave, LA Calkins, ML Esquerdo, GA Furesz, G Jorgensen, UG Horne, KD Stefanik, RP Street, RA Torres, G West, RG Dominik, M Harpsoe, KBW Liebig, C Novati, SC Ricci, D Skottfelt, JF AF Bryan, Marta L. Alsubai, Khalid A. Latham, David W. Parley, Neil R. Cameron, Andrew Collier Quinn, Samuel N. Carter, Joshua A. Fulton, Benjamin J. Berlind, Perry Brown, Warren R. Buchhave, Lars A. Calkins, Michael L. Esquerdo, Gilbert A. Furesz, Gabor Jorgensen, Uffe Grae Horne, Keith D. Stefanik, Robert P. Street, Rachel A. Torres, Guillermo West, Richard G. Dominik, Martin Harpsoe, Kennet B. W. Liebig, Christine Novati, Sebastiano Calchi Ricci, Davide Skottfelt, Jesper F. TI QATAR-2: A K DWARF ORBITED BY A TRANSITING HOT JUPITER AND A MORE MASSIVE COMPANION IN AN OUTER ORBIT (vol 750, pg 84, 2012) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Bryan, Marta L.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Alsubai, Khalid A.] Qatar Fdn, Doha, Qatar. [Latham, David W.; Quinn, Samuel N.; Carter, Joshua A.; Berlind, Perry; Brown, Warren R.; Esquerdo, Gilbert A.; Furesz, Gabor; Stefanik, Robert P.; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Parley, Neil R.; Cameron, Andrew Collier; Horne, Keith D.; Dominik, Martin; Liebig, Christine] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Fulton, Benjamin J.; Street, Rachel A.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Buchhave, Lars A.; Jorgensen, Uffe Grae; Harpsoe, Kennet B. W.; Skottfelt, Jesper F.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.; Jorgensen, Uffe Grae; Harpsoe, Kennet B. W.; Skottfelt, Jesper F.] Geol Museum, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Furesz, Gabor] Hungarian Acad Sci, Konkoly Observ, Budapest, Hungary. [West, Richard G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Novati, Sebastiano Calchi] Univ Salerno, Dipartimento Fis ER Caianiello, I-84081 Baronissi, SA, Italy. [Novati, Sebastiano Calchi] Ist Nazl Fis Nucl, Sez Napoli, Grp Collegato Salerno, Naples, Italy. [Ricci, Davide] Inst Astrophys & Geophys, B-4000 Liege, Belgium. RP Bryan, ML (reprint author), Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. NR 1 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2014 VL 782 IS 2 AR 121 DI 10.1088/0004-637X/782/2/121 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3AV UT WOS:000334584700064 ER PT J AU Dermer, CD Cerruti, M Lott, B Boisson, C Zech, A AF Dermer, Charles D. Cerruti, Matteo Lott, Benoit Boisson, Catherine Zech, Andreas TI EQUIPARTITION GAMMA-RAY BLAZARS AND THE LOCATION OF THE GAMMA-RAY EMISSION SITE IN 3C 279 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: jets; gamma rays: general; radiation mechanisms: non-thermal ID ACTIVE GALACTIC NUCLEI; SPACE-TELESCOPE OBSERVATIONS; SPECTRAL ENERGY-DISTRIBUTION; LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS; EXTRAGALACTIC RADIO-SOURCES; PHOTON-PHOTON COLLISIONS; FERMI-DETECTED BLAZARS; LOG-PARABOLIC SPECTRA; QUASAR PKS 1510-089 AB Blazar spectral models generally have numerous unconstrained parameters, leading to ambiguous values for physical properties like Doppler factor delta(D) or fluid magnetic field B'. To help remedy this problem, a few modifications of the standard leptonic blazar jet scenario are considered. First, a log-parabola function for the electron distribution is used. Second, analytic expressions relating energy loss and kinematics to blazar luminosity and variability, written in terms of equipartition parameters, imply delta(D), B', and the peak electron Lorentz factor gamma(pk)'. The external radiation field in a blazar is approximated by Ly alpha radiation from the broad-line region (BLR) and approximate to 0.1 eV infrared radiation from a dusty torus. When used to model 3C 279 spectral energy distributions from 2008 and 2009 reported by Hayashida et al., we derive delta(D) similar to 20-30, B' similar to few G, and total (IR + BLR) external radiation field energy densities u similar to 10(-2)-10(-3) erg cm(-3), implying an origin of the gamma-ray emission site in 3C 279 at the outer edges of the BLR. This is consistent with the gamma-ray emission site being located at a distance R less than or similar to Gamma(2)ct(var) similar to 0.1(Gamma/30)(2)(t(var)/10(4) s) pc from the black hole powering 3C 279's jets, where t(var) is the variability timescale of the radiation in the source frame, and at farther distances for narrow-jet and magnetic-reconnection models. Excess greater than or similar to 5GeV gamma-ray emission observed with Fermi LAT from 3C 279 challenges the model, opening the possibility of a second leptonic component or a hadronic origin of the emission. For low hadronic content, absolute jet powers of approximate to 10% of the Eddington luminosity are calculated. C1 [Dermer, Charles D.] US Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Cerruti, Matteo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cerruti, Matteo; Boisson, Catherine; Zech, Andreas] Observ Paris, LUTH, F-92195 Meudon, France. [Lott, Benoit] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3,UMR 5797, F-33175 Gradignan, France. RP Dermer, CD (reprint author), US Naval Res Lab, Div Space Sci, Code 7653, Washington, DC 20375 USA. EM charles.dermer@nrl.navy.mil; matteo.cerruti@cfa.harvard.edu FU Office of Naval Research; NASA Fermi Guest Investigator Program FX We thank Dr. M. Hayashida for providing the 3C 279 data, and J. D. Finke and S. Razzaque for discussions. We thank the referee for an excellent and challenging report. The work of C. D. D. is supported by the Office of Naval Research and the NASA Fermi Guest Investigator Program. NR 112 TC 30 Z9 30 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2014 VL 782 IS 2 AR 82 DI 10.1088/0004-637X/782/2/82 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3AV UT WOS:000334584700024 ER PT J AU Fraser, WC Brown, ME Morbidelli, A Parker, A Batygin, K AF Fraser, Wesley C. Brown, Michael E. Morbidelli, Alessandro Parker, Alex Batygin, Konstantin TI THE ABSOLUTE MAGNITUDE DISTRIBUTION OF KUIPER BELT OBJECTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Kuiper belt: general; minor planets, asteroids: general ID TRANS-NEPTUNIAN OBJECTS; JOVIAN TROJAN ASTEROIDS; DWARF PLANET MAKEMAKE; SIZE DISTRIBUTION; SOLAR-SYSTEM; COLLISIONAL EVOLUTION; LUMINOSITY FUNCTION; HERSCHEL-PACS; TNOS; COOL AB Here we measure the absolute magnitude distributions (H-distribution) of the dynamically excited and quiescent (hot and cold) Kuiper Belt objects (KBOs), and test if they share the same H-distribution as the Jupiter Trojans. From a compilation of all useable ecliptic surveys, we find that the KBO H-distributions are well described by broken power laws. The cold population has a bright-end slope, alpha(1) = 1.5(-0.2)(+0.4), and break magnitude, H-B = 6.9(-0.2)(+0.1) (r'-band). The hot population has a shallower bright-end slope of, alpha(1) = 0.87(-0.2)(+0.07), and break magnitude H-B = 7.7(-0.5)(+1.0). Both populations share similar faint-end slopes of alpha(2) similar to 0.2. We estimate the masses of the hot and cold populations are similar to 0.01 and similar to 3 x 10(-4) M-circle plus. The broken power-law fit to the Trojan H-distribution has alpha(1) = 1.0 +/- 0.2, alpha(2) = 0.36 +/- 0.01, and H-B = 8.3. The Kolmogorov-Smirnov test reveals that the probability that the Trojans and cold KBOs share the same parent H-distribution is less than 1 in 1000. When the bimodal albedo distribution of the hot objects is accounted for, there is no evidence that the H-distributions of the Trojans and hot KBOs differ. Our findings are in agreement with the predictions of the Nice model in terms of both mass and H-distribution of the hot and Trojan populations. Wide-field survey data suggest that the brightest few hot objects, with H-r' less than or similar to 3, do not fall on the steep power-law slope of fainter hot objects. Under the standard hierarchical model of planetesimal formation, it is difficult to account for the similar break diameters of the hot and cold populations given the low mass of the cold belt. C1 [Fraser, Wesley C.] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Fraser, Wesley C.; Brown, Michael E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Morbidelli, Alessandro] Univ Nice Sophia Antipolis, Lab Lagrange, CNRS, Observ Cote Azur,UMR7293, F-06304 Nice, France. [Parker, Alex] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Batygin, Konstantin] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Fraser, WC (reprint author), Herzberg Inst Astrophys, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. EM wesley.fraser@nrc.ca NR 61 TC 35 Z9 35 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 FEB 20 PY 2014 VL 782 IS 2 AR 100 DI 10.1088/0004-637X/782/2/100 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3AV UT WOS:000334584700042 ER PT J AU Garcia, J Dauser, T Lohfink, A Kallman, TR Steiner, JF McClintock, JE Brenneman, L Wilms, J Eikmann, W Reynolds, CS Tombesi, F AF Garcia, J. Dauser, T. Lohfink, A. Kallman, T. R. Steiner, J. F. McClintock, J. E. Brenneman, L. Wilms, J. Eikmann, W. Reynolds, C. S. Tombesi, F. TI IMPROVED REFLECTION MODELS OF BLACK HOLE ACCRETION DISKS: TREATING THE ANGULAR DISTRIBUTION OF X-RAYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: individual (Ark 120); line: formation; radiative transfer; X-rays: general ID ACTIVE GALACTIC NUCLEI; K-ALPHA LINE; FLUORESCENT IRON LINES; XMM-NEWTON; COLD MATTER; SPECTRAL VARIABILITY; COMPTON REFLECTION; SEYFERT-GALAXIES; LOW/HARD STATE; STRONG GRAVITY AB X-ray reflection models are used to constrain the properties of the accretion disk, such as the degree of ionization of the gas and the elemental abundances. In combination with general relativistic ray tracing codes, additional parameters like the spin of the black hole and the inclination to the system can be determined. However, current reflection models used for such studies only provide angle-averaged solutions for the flux reflected at the surface of the disk. Moreover, the emission angle of the photons changes over the disk due to relativistic light bending. To overcome this simplification, we have constructed an angle-dependent reflection model with the xillver code and self-consistently connected it with the relativistic blurring code RELLINE. The new model, relxill, calculates the proper emission angle of the radiation at each point on the accretion disk and then takes the corresponding reflection spectrum into account. We show that the reflected spectra from illuminated disks follow a limb-brightening law highly dependent on the ionization of disk and yet different from the commonly assumed form I alpha ln(1 + 1/mu). A detailed comparison with the angle-averaged model is carried out in order to determine the bias in the parameters obtained by fitting a typical relativistic reflection spectrum. These simulations reveal that although the spin and inclination are mildly affected, the Fe abundance can be overestimated by up to a factor of two when derived from angle-averaged models. The fit of the new model to the Suzaku observation of the Seyfert galaxy Ark 120 clearly shows a significant improvement in the constraint of the physical parameters, in particular by enhancing the accuracy in the inclination angle and the spin determinations. C1 [Garcia, J.; Steiner, J. F.; McClintock, J. E.; Brenneman, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dauser, T.; Wilms, J.; Eikmann, W.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Dauser, T.; Wilms, J.; Eikmann, W.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. [Lohfink, A.; Reynolds, C. S.; Tombesi, F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Lohfink, A.; Reynolds, C. S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Kallman, T. R.; Tombesi, F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. RP Garcia, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM javier@head.cfa.harvard.edu; thomas.dauser@sternwarte.uni-erlangen.de; alohfink@astro.umd.edu; timothy.r.kallman@nasa.gov; jsteiner@head.cfa.harvard.edu; jem@cfa.harvard.edu; lbrenneman@cfa.harvard.edu; joern.wilms@sternwarte.uni-erlangen.de; wiebke.eikmann@sternwarte.uni-erlangen.de; chris@astro.umd.edu; ftombesi@astro.umd.edu RI Wilms, Joern/C-8116-2013; XRAY, SUZAKU/A-1808-2009 OI Wilms, Joern/0000-0003-2065-5410; FU NASA [NNX11AD08G, HST-HF-51315.01, NNX10AE41G]; Elitenetzwerk Bayern FX The calculations presented here were performed in the Odyssey cluster of the Research Computing Facilities of Harvard University. J.G. and J.E.M. acknowledge the support of NASA grant NNX11AD08G. J.F.S. was supported by NASA Hubble Fellowship grant HST-HF-51315.01. C.S.R. thanks support from NASA under grant NNX10AE41G. T.D. acknowledges support by a fellowship from the Elitenetzwerk Bayern. We thank John E. Davis for the development of the SLxfig module used to prepare most figures in this paper. NR 74 TC 76 Z9 76 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2014 VL 782 IS 2 AR 76 DI 10.1088/0004-637X/782/2/76 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3AV UT WOS:000334584700018 ER PT J AU Hou, Z Reichardt, CL Story, KT Follin, B Keisler, R Aird, KA Benson, BA Bleem, LE Carlstrom, JE Chang, CL Cho, HM Crawford, TM Crites, AT De Haan, T De Putter, R Dobbs, MA Dodelson, S Dudley, J George, EM Halverson, NW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Joy, M Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D McMahon, JJ Mehl, J Meyer, SS Millea, M Mohr, JJ Montroy, TE Padin, S Plagge, T Pryke, C Ruhl, JE Sayre, JT Schaffer, KK Shaw, L Shirokoff, E Spieler, HG Staniszewski, Z Stark, AA Van Engelen, A Vanderlinde, K Vieira, JD Williamson, R Zahn, O AF Hou, Z. Reichardt, C. L. Story, K. T. Follin, B. Keisler, R. Aird, K. A. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Cho, H. -M. Crawford, T. M. Crites, A. T. De Haan, T. De Putter, R. Dobbs, M. A. Dodelson, S. Dudley, J. George, E. M. Halverson, N. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Joy, M. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. McMahon, J. J. Mehl, J. Meyer, S. S. Millea, M. Mohr, J. J. Montroy, T. E. Padin, S. Plagge, T. Pryke, C. Ruhl, J. E. Sayre, J. T. Schaffer, K. K. Shaw, L. Shirokoff, E. Spieler, H. G. Staniszewski, Z. Stark, A. A. Van Engelen, A. Vanderlinde, K. Vieira, J. D. Williamson, R. Zahn, O. TI CONSTRAINTS ON COSMOLOGY FROM THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM OF THE 2500 deg(2) SPT-SZ SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmological parameters; early universe; inflation ID SOUTH-POLE TELESCOPE; BARYON ACOUSTIC-OSCILLATIONS; BIG-BANG NUCLEOSYNTHESIS; 720 SQUARE DEGREES; PRIMORDIAL NUCLEOSYNTHESIS; PRECISION COSMOLOGY; HELIUM ABUNDANCE; GALAXY CLUSTERS; HUBBLE CONSTANT; CENT DISTANCE AB We explore extensions to the Lambda CDM cosmology using measurements of the cosmic microwave background (CMB) from the recent SPT-SZ survey, along with data from WMAP7 and measurements of H-0 and baryon acoustic oscillation (BAO). We check for consistency within Lambda CDM between these data sets, and find some tension. The CMB alone gives weak support to physics beyond Lambda CDM, due to a slight trend relative to Lambda CDM of decreasing power toward smaller angular scales. While it may be due to statistical fluctuation, this trend could also be explained by several extensions. We consider running of the primordial spectral index (dn(s)/d ln k), as well as two extensions that modify the damping tail power (the primordial helium abundance Y-p and the effective number of neutrino species N-eff) and one that modifies the large-scale power due to the integrated Sachs-Wolfe effect (the sum of neutrino masses Sigma m(nu)). These extensions have similar observational consequences and are partially degenerate when considered simultaneously. Of the six one-parameter extensions considered, we find CMB to have the largest preference for dn(s)/d ln k with -0.046 < dn(s)/d lnk < -0.003 at 95% confidence, which strengthens to a 2.7 sigma indication of dn(s)/d lnk < 0 from CMB+BAO+H-0. Detectable dn(s)/d ln k not equal 0 is difficult to explain in the context of single-field, slow-roll inflation models. We find N-eff = 3.62 +/- 0.48 for the CMB, which tightens to N-eff = 3.71 +/- 0.35 from CMB+BAO+H-0. Larger values of N-eff relieve the mild tension between CMB, BAO, and H-0. When the Sunyaev-Zel'dovich selected galaxy cluster abundances (SPTCL) data are also included, we obtain N-eff = 3.29 +/- 0.31. Allowing for Sigma m(nu) gives a 3.0s detection of Sigma m(nu) > 0 from CMB+BAO+H-0 +SPTCL. The median value is (0.32+/-0.11) eV, a factor of six above the lower bound set by neutrino oscillation observations. All data sets except H-0 show some preference for massive neutrinos; data combinations including H-0 favor nonzero masses only if BAO data are also included. We also constrain the two-parameter extensions N-eff + Sigma m(nu) and N-eff + Y-p to explore constraints on additional light species and big bang nucleosynthesis, respectively. C1 [Hou, Z.; Follin, B.; Knox, L.; Millea, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Reichardt, C. L.; George, E. M.; Holzapfel, W. L.; Lee, A. T.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Story, K. T.; Keisler, R.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Dodelson, S.; Hoover, S.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Story, K. T.; Keisler, R.; Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Meyer, S. S.; Padin, S.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, 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. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Dodelson, S.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.; Mehl, J.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H. -M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [De Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P.; Shaw, L.; Van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [De Putter, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [De Putter, R.] CALTECH, Pasadena, CA 91125 USA. [Dodelson, S.; Lueker, M.; Vieira, J. D.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 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. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Univ, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Schaffer, K. K.] Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP Hou, Z (reprint author), Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA. RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937]; NSF [PHY-1125897, NSF PHY 1148698]; 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; M. Dobbs an Alfred P. Sloan Research Fellowship; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; NASA Office of Space Science 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. R. Keisler acknowledges support from NASA Hubble Fellowship grant HF-51275.01, B. A. Benson a KICP Fellowship, M. Dobbs an Alfred P. Sloan Research Fellowship, O. Zahn a BCCP fellowship. This research used resources of the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, and the resources of the University of Chicago Computing Cooperative (UC3), supported in part by the Open Science Grid, NSF grant NSF PHY 1148698. 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 87 TC 117 Z9 117 U1 2 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2014 VL 782 IS 2 AR 74 DI 10.1088/0004-637X/782/2/74 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3AV UT WOS:000334584700016 ER PT J AU Rosenfeld, KA Chiang, E Andrews, SM AF Rosenfeld, Katherine A. Chiang, Eugene Andrews, Sean M. TI FAST RADIAL FLOWS IN TRANSITION DISK HOLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; protoplanetary disks; stars: pre-main sequence ID T TAURI STARS; ANGULAR-MOMENTUM TRANSPORT; MASS ACCRETION RATES; PROTOPLANETARY DISK; CIRCUMSTELLAR DISK; HD 142527; GM-AURIGAE; LKCA 15; SURROUNDING HD-142527; TEMPERATURE-GRADIENT AB Protoplanetary "transition" disks have large, mass-depleted central cavities, yet also deliver gas onto their host stars at rates comparable to disks without holes. The paradox of simultaneous transparency and accretion can be explained if gas flows inward at much higher radial speeds inside the cavity than outside the cavity, since surface density (and by extension optical depth) varies inversely with inflow velocity at fixed accretion rate. Radial speeds within the cavity might even have to approach free-fall values to explain the huge surface density contrasts inferred for transition disks. We identify observational diagnostics of fast radial inflow in channel maps made in optically thick spectral lines. Signatures include (1) twisted isophotes in maps made at low systemic velocities and (2) rotation of structures observed between maps made in high-velocity line wings. As a test case, we apply our new diagnostic tools to archival Atacama Large Millimeter Array data on the transition disk HD 142527 and uncover evidence for free-fall radial velocities inside its cavity. Although the observed kinematics are also consistent with a disk warp, the radial inflow scenario is preferred because it predicts low surface densities that appear consistent with recent observations of optically thin CO isotopologues in this disk. How material in the disk cavity sheds its angular momentum wholesale to fall freely onto the star is an unsolved problem; gravitational torques exerted by giant planets or brown dwarfs are briefly discussed as a candidate mechanism. C1 [Rosenfeld, Katherine A.; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chiang, Eugene] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Chiang, Eugene] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. RP Rosenfeld, KA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 79 TC 28 Z9 28 U1 0 U2 0 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 FEB 20 PY 2014 VL 782 IS 2 AR 62 DI 10.1088/0004-637X/782/2/62 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3AV UT WOS:000334584700004 ER PT J AU Bogdan, A van Weeren, RJ Kraft, RP Forman, WR Randall, S Giacintucci, S Churazov, E O'Dea, CP Baum, SA Noell-Storr, J Jones, C AF Bogdan, Akos van Weeren, Reinout J. Kraft, Ralph P. Forman, William R. Randall, Scott Giacintucci, Simona Churazov, Eugene O'Dea, Christopher P. Baum, Stefi A. Noell-Storr, Jacob Jones, Christine TI YOUNG AGN OUTBURST RUNNING OVER OLDER X-RAY CAVITIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual (NGC 193); radio continuum: galaxies; X-rays: galaxies; X-rays: ISM ID ACTIVE GALACTIC NUCLEI; COOLING FLOWS; BLACK-HOLES; TELESCOPE OBSERVATIONS; CHANDRA OBSERVATION; GALAXY; CLUSTER; SHOCKS; JETS; ATMOSPHERES AB Although the energetic feedback from active galactic nuclei (AGNs) is believed to have a profound effect on the evolution of galaxies and clusters of galaxies, details of AGN heating remain elusive. Here, we study NGC 193-a nearby lenticular galaxy-based on X-ray (Chandra) and radio (Very Large Array and Giant Meter-wave Radio Telescope) observations. These data reveal the complex AGN outburst history of the galaxy: we detect a pair of inner X-ray cavities, an outer X-ray cavity, a shock front, and radio lobes extending beyond the inner cavities. We suggest that the inner cavities were produced similar to 78 Myr ago by a weaker AGN outburst, while the outer cavity, the radio lobes, and the shock front are due to a younger (13-26 Myr) and 4-8 times more powerful outburst. Combining this with the observed morphology of NGC 193, we conclude that NGC 193 likely represents the first example of a second, more powerful, AGN outburst overrunning an older, weaker outburst. These results help us to understand how the outburst energy is dissipated uniformly in the core of galaxies, and therefore may play a crucial role in resolving how AGN outbursts suppress the formation of large cooling flows at cluster centers. C1 [Bogdan, Akos; van Weeren, Reinout J.; Kraft, Ralph P.; Forman, William R.; Randall, Scott; Jones, Christine] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Giacintucci, Simona] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Giacintucci, Simona] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Churazov, Eugene] Max Planck Inst Astrophys, D-85741 Garching, Germany. [O'Dea, Christopher P.; Baum, Stefi A.; Noell-Storr, Jacob] Rochester Inst Technol, Rochester, NY 14623 USA. RP Bogdan, A (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM abogdan@cfa.harvard.edu RI Churazov, Eugene/A-7783-2013; OI Randall, Scott/0000-0002-3984-4337; van Weeren, Reinout/0000-0002-0587-1660; Forman, William/0000-0002-9478-1682 FU NASA through Einstein Postdoctoral Fellowship by the CXC; NASA [NAS8-03060] FX We thank Paul Nulsen for helpful discussions. This research made use of Chandra data provided by the Chandra X-ray Center (CXC). The VLA is a facility of NRAO, which is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. A.B. and R. vW. acknowledge support provided by NASA through Einstein Postdoctoral Fellowship awarded by the CXC, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. NR 30 TC 3 Z9 3 U1 0 U2 0 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 FEB 20 PY 2014 VL 782 IS 2 AR L19 DI 10.1088/2041-8205/782/2/L19 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5PV UT WOS:000331153000006 ER PT J AU Cheung, CC Larsson, S Scargle, JD Amin, MA Blandford, RD Bulmash, D Chiang, J Ciprini, S Corbet, RHD Falco, EE Marshall, PJ Wood, DL Ajello, M Bastieri, D Chekhtman, A D'Ammando, F Giroletti, M Grove, JE Lott, B Ojha, R Orienti, M Perkins, JS Razzano, M Smith, AW Thompson, DJ Wood, KS AF Cheung, C. C. Larsson, S. Scargle, J. D. Amin, M. A. Blandford, R. D. Bulmash, D. Chiang, J. Ciprini, S. Corbet, R. H. D. Falco, E. E. Marshall, P. J. Wood, D. L. Ajello, M. Bastieri, D. Chekhtman, A. D'Ammando, F. Giroletti, M. Grove, J. E. Lott, B. Ojha, R. Orienti, M. Perkins, J. S. Razzano, M. Smith, A. W. Thompson, D. J. Wood, K. S. TI FERMI LARGE AREA TELESCOPE DETECTION OF GRAVITATIONAL LENS DELAYED gamma-RAY FLARES FROM BLAZAR B0218+357 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; gamma rays: galaxies; gravitational lensing: strong; quasars: individual (B0218+357) ID ACTIVE GALACTIC NUCLEI; ALL-SKY SURVEY; TIME-DELAY; HUBBLE CONSTANT; EINSTEIN RING; RADIO-SOURCES; VARIABILITY; SYSTEM; CALIBRATION; REDSHIFT AB Using data from the Fermi Large Area Telescope (LAT), we report the first clear gamma-ray measurement of a delay between flares from the gravitationally lensed images of a blazar. The delay was detected in B0218+357, a known double-image lensed system, during a period of enhanced gamma-ray activity with peak fluxes consistently observed to reach >20-50x its previous average flux. An auto-correlation function analysis identified a delay in the gamma-ray data of 11.46 +/- 0.16 days (1 sigma) that is similar to 1 day greater than previous radio measurements. Considering that it is beyond the capabilities of the LAT to spatially resolve the two images, we nevertheless decomposed individual sequences of superposing gamma-ray flares/delayed emissions. In three such similar to 8-10 day-long sequences within a similar to 4 month span, considering confusion due to overlapping flaring emission and flux measurement uncertainties, we found flux ratios consistent with similar to 1, thus systematically smaller than those from radio observations. During the first, best-defined flare, the delayed emission was detailed with a Fermi pointing, and we observed flux doubling timescales of similar to 3-6 hr implying as well extremely compact gamma-ray emitting regions. C1 [Cheung, C. C.; Grove, J. E.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Larsson, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Amin, M. A.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Amin, M. A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Blandford, R. D.; Chiang, J.; Marshall, P. J.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Blandford, R. D.; Chiang, J.; Marshall, P. J.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Bulmash, D.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Ciprini, S.] ASI, Sci Data Ctr, I-00133 Rome, Italy. [Ciprini, S.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Roma, Italy. [Corbet, R. H. D.] Ctr Res & Explorat Space Sci & Technol CRESST, Greenbelt, MD 20771 USA. [Corbet, R. H. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Corbet, R. H. D.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Falco, E. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marshall, P. J.] Univ Oxford, Dept Phys Astrophys, Oxford OX1 3RH, England. [Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bastieri, D.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Lott, B.] Univ Bordeaux 1, IN2P3 CNRS, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Ojha, R.; Perkins, J. S.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Orienti, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. RP Cheung, CC (reprint author), Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. EM Teddy.Cheung@nrl.navy.mil; Jeffrey.D.Scargle@nasa.gov FU Royal Swedish Academy Crafoord Foundation; Italian Ministry of Education, University and Research (MIUR) [FIRB-2012-RBFR12PM1F] FX Supported by the Royal Swedish Academy Crafoord Foundation.; Funded by contract FIRB-2012-RBFR12PM1F from the Italian Ministry of Education, University and Research (MIUR). NR 50 TC 21 Z9 21 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2014 VL 782 IS 2 AR L14 DI 10.1088/2041-8205/782/2/L14 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5PV UT WOS:000331153000001 ER PT J AU Zatsarinny, O Wang, Y Bartschat, K AF Zatsarinny, Oleg Wang, Yang Bartschat, Klaus TI Electron-impact excitation of argon at intermediate energies SO PHYSICAL REVIEW A LA English DT Article ID SCATTERING CROSS-SECTIONS; R-MATRIX; ELASTIC-SCATTERING; INCIDENT ENERGIES; ATOMS; AR; IONIZATION; HELIUM; STATES; HE AB Large-scale R-matrix-with-pseudostates calculations for electron collisions with argon atoms, using a recently developed parallel version of our B-spline R-matrix code, are reported. The calculations were carried out in the semirelativistic jK-coupling scheme. They are intended to provide converged (with respect to the number of coupled states) results for electron-impact excitation of individual target states with dominant configurations 3p(5)4s, 3p(5)4p, 3p(5)3d, and 3p(5)5s for incident electron energies from threshold to 300 eV. The close-coupling expansion includes 500 target states, with the lowest 78 states representing the bound spectrum and the remaining 422 the ionization continuum. The results reveal dramatic reductions of the predicted excitation cross sections at intermediate energies due to a strong influence of coupling to the target continuum and the higher-lying Rydberg states. Comparison with available experimental data for excitation raises questions about the absolute normalization in the measurements. C1 [Zatsarinny, Oleg; Wang, Yang; Bartschat, Klaus] Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. [Wang, Yang] Harbin Inst Technol, Acad Fundamental & Interdisciplinary Sci, Ctr Theoret Atom & Mol Phys, Harbin 150080, Peoples R China. [Bartschat, Klaus] ITAMP, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zatsarinny, O (reprint author), Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. EM oleg.zatsarinny@drake.edu; yangwang0624@foxmail.com; klaus.bartschat@drake.edu FU United States National Science Foundation [PHY-0903818, PHY-1212450]; XSEDE supercomputer allocation [PHY-090031]; China Scholarship Council FX We thank Leanne Pitchford for many discussions regarding our calculations. This work was supported by the United States National Science Foundation under Grants No. PHY-0903818 and No. PHY-1212450 and by the XSEDE supercomputer allocation No. PHY-090031. The calculations were carried out on Stampede at the Texas Advanced Computing Center and Gordon at the San Diego Supercomputer Center. Y. W. was sponsored by the China Scholarship Council and would like to thank Drake University for hospitality during his visit. NR 53 TC 21 Z9 21 U1 3 U2 23 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 FEB 18 PY 2014 VL 89 IS 2 AR 022706 DI 10.1103/PhysRevA.89.022706 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AC2KM UT WOS:000332329800016 ER PT J AU Ballen, GA Mojica, JI AF Ballen, Gustavo A. Mojica, Jose Ivan TI A new trans-Andean Stick Catfish of the genus Farlowella Eigenmann & Eigenmann, 1889 (Siluriformes: Loricariidae) with the first record of the genus for the rio Magdalena Basin in Colombia SO ZOOTAXA LA English DT Article DE Loricariinae; Farlowella gracilis; trans-Andean; Serrania de los Yariguies; taxonomy AB A new species of Farlowella is described from El Carmen de Chucuri in the Departamento de Santander, western flank of the Cordillera Oriental, rio Magdalena Basin, Colombia. Farlowella yarigui n. sp. differs from its congeners in lateral body plate morphology, abdominal cover, cephalic hypertrophied odontodes, and details of coloration. This is the first verifiable record of the genus in the Magdalena drainage. Aspects of natural history and implications of this finding are provided concerning the state of knowledge of the fishes of the rio Magdalena Basin. Previous records of Farlowella gracilis in the rio Cauca basin are examined and herein considered erroneous, rendering the new species the only representative of the genus in the Magdalena-Cauca system. A key to species of Farlowella from Colombia is provided. C1 [Ballen, Gustavo A.] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Ancon, Panama. [Ballen, Gustavo A.] Univ Nacl Colombia, Inst Ciencias Nat, Grp Cladist Profunda & Biogeog Hist, Bogota, Colombia. [Mojica, Jose Ivan] Univ Nacl Colombia, Inst Ciencias Nat, Bogota, Colombia. RP Ballen, GA (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Ancon, Panama. EM gaballench@gmail.com; jimojicac@unal.edu.co FU Center for Tropical Paleoecology and Archaeology, Smithsonian Tropical Research Institute FX We are grateful to the students of the 2011-I undergraduate course "Taxonom a Animal" (M. Castro, M. Henao, D. Hernandez, C. Briceno, F. Paternina, A. Pinto, L. Calderon, N. Perez, and P. Pabon; Biology Department, Universidad Nacional de Colombia) for their diligence during collection. Unidad Administrativa Especial de Parques Nacionales Naturales provided workspace and field facilities during an expedition to the PNN Serrania de los Yariguies and its area of influence. Gary Stiles provided useful data on Batty's collections in Colombia. Don Taphorn kindly revised the English and provided useful corrections. Two anonymous reviewers and the editor are acknowledged for their diligence in the review phase and for important comments and discussions. GAB acknowledges the Center for Tropical Paleoecology and Archaeology, Smithsonian Tropical Research Institute, for funding during the late phase of this project. NR 13 TC 3 Z9 3 U1 1 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 17 PY 2014 VL 3765 IS 2 BP 134 EP 142 PG 9 WC Zoology SC Zoology GA AA5VL UT WOS:000331167600002 PM 24870891 ER PT J AU Owen, RB Renaut, RW Behrensmeyer, AK Potts, R AF Owen, R. Bernhart Renaut, Robin W. Behrensmeyer, Anna K. Potts, Richard TI Quaternary geochemical stratigraphy of the Kedong-Olorgesailie section of the southern Kenya Rift valley SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Geochemistry; Weathering; Diatoms; Palaeoenvironments; Tectonism; Climate ID RARE-EARTH-ELEMENT; PLIOPLEISTOCENE AFRICAN CLIMATE; EAST-AFRICA; LACUSTRINE SEDIMENTATION; ENVIRONMENTAL-CHANGE; HUMAN-EVOLUTION; TURKANA BASIN; WA GICHERU; PLEISTOCENE; ROCKS AB This study uses a variety of geochemical parameters to reconstruct a Quaternary environmental history of the Kedong-Olorgesailie sector of the southern Kenya Rift Valley. Lacustrine, wetland and fluvial deposition took place between about 1.9 and 0.72 Ma at Munyu wa Gicheru in the northern part of the study area. Sedimentation continued about 40 km further south to produce the lake, wetland, fluvial and pedogenic deposits of the Olorgesailie Formation between about 1.2 and 0.5 Ma. Faulting subsequently led to basin breakup at Olorgesailie and the development of Middle to Late Pleistocene cut-and-fill fluvial deposits, as well as pond, wetland and terrestrial sediments that were locally altered by pedogenesis. Tufas and calcretes also accumulated during this latter time interval. Sedimentation in these different depositional sequences reflects several long-term trends, including: 1) an increase in carbonate deposition; 2) a decrease in biogenic silica; and 3) decreased chemical weathering indices (Chemical Index of Alteration, Vogt ratios), which imply increasing Quaternary aridity and/or erosion of catchment soils. The biophile elements Br and S also increase upwards, suggesting pulses of erosion of organic soils. Plants permineralized by silica became widespread after about 0.5 Ma, providing evidence that groundwater bodies were becoming silica-enriched, possibly as a result of deeper water circulation along active faults. Several fault-aligned fossil hot spring deposits with siliceous vent, pedogenic and swamp facies have been identified at Emerit in the central part of the Kedong-Olorgesailie rift. Tectonism also provided pathways for meteoric water that led to the formation of carbonate springs in the Olorgesailie area. REE patterns in clastic sediments are stable throughout the Quaternary, reflecting the dominant trachytic source rocks, but these patterns become variable in later Pleistocene calcretes and tufas documenting changing hydrochemical conditions. The geochemical evolution of the area partly reflects climate change through time. However, it also documents the influence of Quaternary rifting processes. Rift faulting affected the geochemistry of the basin sediments by 1) causing changes in the depth of fracture systems that controlled groundwater movements and sourcing of fluids, 2) changing accommodation space in which sediments could accumulate, and 3) altering relief and thus rainfall and evaporation patterns across the rift system, as well as erosion and weathering rates. (C) 2014 Elsevier B.V. All rights reserved. C1 [Owen, R. Bernhart] Hong Kong Baptist Univ, Dept Geog, Kowloon Tong, Hong Kong, Peoples R China. [Renaut, Robin W.] Univ Saskatchewan, Dept Geol Sci, Saskatoon, SK S7N 5E2, Canada. [Behrensmeyer, Anna K.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Potts, Richard] Smithsonian Inst, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20013 USA. [Potts, Richard] Natl Museums Kenya, Palaeontol Sect, Dept Earth Sci, Nairobi, Kenya. RP Owen, RB (reprint author), Hong Kong Baptist Univ, Dept Geog, Kowloon Tong, Hong Kong, Peoples R China. EM owen@hkbu.edu.hk OI Owen, Richard Bernhart/0000-0001-5267-5366 FU National Museums of Kenya; Research Grant Council of Hong Kong [HKBU201911]; NSERC (Canada) Discovery Grant [629-08]; National Science Foundation (HOMINID grant) [0218511]; Peter Buck Fund for Human Origins Research FX The authors would like to thank the National Museums of Kenya for their support of work at Olorgesailie and the Ministry of Science and Technology, Republic of Kenya for permission to carry out this investigation. Funding for Owen was provided by the Research Grant Council of Hong Kong (HKBU201911). Renaut was supported by NSERC (Canada) Discovery Grant 629-08. Behrensmeyer and Potts were supported by the National Science Foundation (HOMINID grant 0218511), the Peter Buck Fund for Human Origins Research, and the Smithsonian Human Origins Program. Prof. Stanley Ambrose first reported the fossil silica sinters at Emerit to the authors. We thank Peter Ditchfield for the use of his logged section D99/06a/b. NR 76 TC 1 Z9 1 U1 4 U2 36 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD FEB 15 PY 2014 VL 396 BP 194 EP 212 DI 10.1016/j.palaeo.2014.01.011 PG 19 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA AD8GY UT WOS:000333505700014 ER PT J AU Zimbelman, JR AF Zimbelman, James R. TI Introduction to the Planetary Dunes special issue, and the aeolian career of Ronald Greeley SO ICARUS LA English DT Editorial Material ID WIND-TUNNEL SIMULATIONS; PATHFINDER LANDING SITE; MARTIAN DUST DEVILS; LABORATORY SIMULATIONS; SURFACE-ROUGHNESS; FRICTION SPEEDS; SAND-SEA; MARS; VENUS; FEATURES C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Zimbelman, JR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. EM zimbelmanj@si.edu NR 75 TC 0 Z9 0 U1 1 U2 7 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 FEB 15 PY 2014 VL 230 SI SI BP 1 EP 4 DI 10.1016/j.icarus.2014.01.003 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 298OF UT WOS:000330333100001 ER PT J AU Zimbelman, JR Scheidt, SP AF Zimbelman, James R. Scheidt, Stephen P. TI Precision topography of a reversing sand dune at Bruneau Dunes, Idaho, as an analog for Transverse Aeolian Ridges on Mars SO ICARUS LA English DT Article; Proceedings Paper CT 3rd International Planetary Dunes Workshop CY JUN 12-15, 2012 CL Lowell Observ, Flagstaff, AZ HO Lowell Observ DE Mars, Surface; Mars; Earth; Geological processes; Data reduction techniques ID HIRISE IMAGES; PROFILES AB Ten high precision topographic profiles across a reversing dune were created from a differential global position system (DGPS). The shapes of the profiles reveal a progression from immature to transitional to mature characteristics moving up the dune. When scaled by the basal width along each profile, shape characteristics can be compared for profiles whose horizontal scales differ by orders of magnitude. The comparison of width-scaled Bruneau Dunes profiles to similarly scaled profiles of Transverse Aeolian Ridges (TARs) on Mars indicates that many TARs are likely similar to transitional or mature reversing sand dunes. Published by Elsevier Inc. C1 [Zimbelman, James R.; Scheidt, Stephen P.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Zimbelman, JR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC 315, Washington, DC 20013 USA. EM zimbelmanj@si.edu; sscheidt77@gmail.com NR 32 TC 4 Z9 4 U1 1 U2 9 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 FEB 15 PY 2014 VL 230 SI SI BP 29 EP 37 DI 10.1016/j.icarus.2013.08.004 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 298OF UT WOS:000330333100004 ER PT J AU Kunz, MW Stone, JM Bai, XN AF Kunz, Matthew W. Stone, James M. Bai, Xue-Ning TI Pegasus: A new hybrid-kinetic particle-in-cell code for astrophysical plasma dynamics SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Hybrid; Particle-in-cell; Numerical methods; Plasma ID FIELD-REVERSED CONFIGURATIONS; COULOMB COLLISION MODEL; UNSPLIT GODUNOV METHOD; CURRENT ADVANCE METHOD; DELTA-F; CONSTRAINED TRANSPORT; SIMULATION CODES; MAGNETOROTATIONAL INSTABILITY; LANGEVIN REPRESENTATION; NUMERICAL-SOLUTION AB We describe Pegasus, a new hybrid-kinetic particle-in-cell code tailored for the study of astrophysical plasma dynamics. The code incorporates an energy-conserving particle integrator into a stable, second-order-accurate, three-stage predictor-predictor-corrector integration algorithm. The constrained transport method is used to enforce the divergence-free constraint on the magnetic field. A delta f scheme is included to facilitate a reduced-noise study of systems in which only small departures from an initial distribution function are anticipated. The effects of rotation and shear are implemented through the shearing-sheet formalism with orbital advection. These algorithms are embedded within an architecture similar to that used in the popular astrophysical magnetohydrodynamics code Athena, one that is modular, well-documented, easy to use, and efficiently parallelized for use on thousands of processors. We present a series of tests in one, two, and three spatial dimensions that demonstrate the fidelity and versatility of the code. (C) 2013 Elsevier Inc. All rights reserved. C1 [Kunz, Matthew W.; Stone, James M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bai, Xue-Ning] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Kunz, MW (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. EM mkunz@princeton.edu FU NASA [PF1-120084, NAS8-03060, HST-HF-51301.01-A, NAS5-26555]; Chandra X-ray Observatory Center; Space Telescope Science Institute; NSF [OCI-1053575]; [TG-AST090105] FX Support for M.W.K. was provided by NASA through Einstein Postdoctoral Fellowship Award Number PF1-120084, issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. Support for X.-N.B. was provided by NASA through Hubble Postdoctoral Fellowship Award Number HST-HF-51301.01-A, issued by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy for and on behalf of NASA under contract NAS5-26555. The Texas Advanced Computer Center at The University of Texas at Austin provided HPC resources under grant number TG-AST090105, as did the PICSciE-OIT TIGRESS High Performance Computing Center and Visualization Laboratory at Princeton University. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by NSF grant OCI-1053575. Aspects of this work were facilitated by the Max-Planck/Princeton Center for Plasma Physics. The authors would like to thank Greg Hammett and Elena Belova for their encouragement, for their suggestions on how to improve our numerical algorithm, and for introducing us to the delta f method; Anatoly Spitkovsky for fruitful discussions regarding the optimization of PIC algorithms; Damiano Caprioli for his assistance setting up the shock test problem; Lehman Garrison for providing his optimized digital filter algorithm; Joshua Dolence and Ammar Hakim for their advice with coding issues; Tobias Heinemann for useful conversations regarding the shearing-sheet formalism in the context of the hybrid-kinetic equations; and Alexander Schekochihin and Steven Cowley for sharing their expertise on multiscale plasma kinetics and inspiring much of the work presented here. NR 79 TC 13 Z9 13 U1 2 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 EI 1090-2716 J9 J COMPUT PHYS JI J. Comput. Phys. PD FEB 15 PY 2014 VL 259 BP 154 EP 174 DI 10.1016/j.jcp.2013.11.035 PG 21 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 286YZ UT WOS:000329506500010 ER PT J AU Moini, M Martinez, B AF Moini, Mehdi Martinez, Ben TI Ultrafast capillary electrophoresis/mass spectrometry with adjustable porous tip for a rapid analysis of protein digest in about a minute SO RAPID COMMUNICATIONS IN MASS SPECTROMETRY LA English DT Article ID FLIGHT MASS-SPECTROMETRY; IONIZATION; OPERATION AB RATIONALEThis paper introduces a novel ultrafast capillary electrophoresis (UFCE) mass spectrometry (MS) method comprised of a short (< 20 cm) and narrow ( 5 mu m) capillary, with an integrated porous segment at the terminus of the capillary, for sheathless interfacing of CE to MS. The sheathless nature of the interface minimizes dead volume which is particularly important for ultrafast CE because of the small diameters of the capillaries. METHODSThe separation voltage across the capillary was set to produce an electric field of 1000 V/cm to provide an analysis time of approximately 1 min. For the analysis of peptides and protein digests, a background electrolyte containing 0.1% cationic polymer (polybrene or Poly-E) in 0.1% acetic acid in water was used to prevent analyte-wall interaction. RESULTSUniquely, the porous tip of the capillary is adjustable. This allows the porous tip to be pulled inside the sheath liquid for sample stacking during injection, or sample focusing in isoelectric focusing (IEF), or, alternatively, pushed outside of the sheath liquid for electrospray ionization (ESI). The adjustable interface preserves electrical conductivity during electrokinetic injection with reverse electro-osmotic flow. Therefore, pre-concentration of analytes at the capillary inlet is achieved without the need to disassemble the interface, improving the throughput. CONCLUSIONSAs a proof of concept, the application of UFCE-MS was demonstrated by the analysis of a peptide mixture and a protein digest in 1 min. Copyright (c) 2013 John Wiley & Sons, Ltd. C1 [Moini, Mehdi] Smithsonian Inst, Museum Conservat Inst, Suitland, MD USA. [Martinez, Ben] SW Texas State Univ, Dept Chem, San Marcos, TX 78666 USA. RP Moini, M (reprint author), Smithsonian Inst, Museum Conservat Inst, Suitland, MD USA. EM moinim@si.edu NR 16 TC 13 Z9 13 U1 1 U2 76 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0951-4198 EI 1097-0231 J9 RAPID COMMUN MASS SP JI Rapid Commun. Mass Spectrom. PD FEB 15 PY 2014 VL 28 IS 3 BP 305 EP 310 DI 10.1002/rcm.6786 PG 6 WC Biochemical Research Methods; Chemistry, Analytical; Spectroscopy SC Biochemistry & Molecular Biology; Chemistry; Spectroscopy GA 277MH UT WOS:000328823200009 PM 24375882 ER PT J AU Schile, LM Callaway, JC Morris, JT Stralberg, D Parker, VT Kelly, M AF Schile, Lisa M. Callaway, John C. Morris, James T. Stralberg, Diana Parker, V. Thomas Kelly, Maggi TI Modeling Tidal Marsh Distribution with Sea-Level Rise: Evaluating the Role of Vegetation, Sediment, and Upland Habitat in Marsh Resiliency SO PLOS ONE LA English DT Article ID CLIMATE-CHANGE; SALT MARSHES; SPARTINA-ALTERNIFLORA; ELEVATION MODEL; COASTAL MARSHES; SOIL FORMATION; ACCRETION; RIVER; BAY; USA AB Tidal marshes maintain elevation relative to sea level through accumulation of mineral and organic matter, yet this dynamic accumulation feedback mechanism has not been modeled widely in the context of accelerated sea-level rise. Uncertainties exist about tidal marsh resiliency to accelerated sea-level rise, reduced sediment supply, reduced plant productivity under increased inundation, and limited upland habitat for marsh migration. We examined marsh resiliency under these uncertainties using the Marsh Equilibrium Model, a mechanistic, elevation-based soil cohort model, using a rich data set of plant productivity and physical properties from sites across the estuarine salinity gradient. Four tidal marshes were chosen along this gradient: two islands and two with adjacent uplands. Varying century sea-level rise (52, 100, 165, 180 cm) and suspended sediment concentrations (100%, 50%, and 25% of current concentrations), we simulated marsh accretion across vegetated elevations for 100 years, applying the results to high spatial resolution digital elevation models to quantify potential changes in marsh distributions. At low rates of sea-level rise and mid-high sediment concentrations, all marshes maintained vegetated elevations indicative of mid/high marsh habitat. With century sea-level rise at 100 and 165 cm, marshes shifted to low marsh elevations; mid/high marsh elevations were found only in former uplands. At the highest century sea-level rise and lowest sediment concentrations, the island marshes became dominated by mudflat elevations. Under the same sediment concentrations, low salinity brackish marshes containing highly productive vegetation had slower elevation loss compared to more saline sites with lower productivity. A similar trend was documented when comparing against a marsh accretion model that did not model vegetation feedbacks. Elevation predictions using the Marsh Equilibrium Model highlight the importance of including vegetation responses to sea-level rise. These results also emphasize the importance of adjacent uplands for long-term marsh survival and incorporating such areas in conservation planning efforts. C1 [Schile, Lisa M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Schile, Lisa M.; Kelly, Maggi] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Callaway, John C.] Univ San Francisco, Dept Environm Sci, San Francisco, CA 94117 USA. [Morris, James T.] Univ S Carolina, Belle W Baruch Inst Marine Biol & Coastal Res, Columbia, SC 29208 USA. [Stralberg, Diana] Univ Alberta, Dept Biol Sci, Edmonton, AB, Canada. [Parker, V. Thomas] San Francisco State Univ, Dept Biol, San Francisco, CA 94132 USA. RP Schile, LM (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM lschile@berkeley.edu OI Stralberg, Diana/0000-0003-4900-024X FU California Bay-Delta Authority for research under California Bay-Delta Authority [U-04-SC-005]; CALFED Science Program [1037] FX This paper was prepared in cooperation with the California Bay-Delta Authority for research funded under California Bay-Delta Authority Agreement No. U-04-SC-005 and under CALFED Science Program Grant #1037. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 75 TC 25 Z9 25 U1 7 U2 118 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 FEB 13 PY 2014 VL 9 IS 2 AR e88760 DI 10.1371/journal.pone.0088760 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AA7GP UT WOS:000331266000064 PM 24551156 ER PT J AU Lee, TE Chan, CK Wang, SS AF Lee, Tony E. Chan, Ching-Kit Wang, Shenshen TI Entanglement tongue and quantum synchronization of disordered oscillators SO PHYSICAL REVIEW E LA English DT Article ID COUPLED NONLINEAR OSCILLATORS; LIMIT-CYCLE OSCILLATORS; STEADY-STATE; STANDARD MAP; DEATH; DISSIPATION; POPULATION; NETWORKS; DYNAMICS; BEHAVIOR AB We study the synchronization of dissipatively coupled van der Pol oscillators in the quantum limit, when each oscillator is near its quantum ground state. Two quantum oscillators with different frequencies exhibit an entanglement tongue, which is the quantum analog of an Arnold tongue. It means that the oscillators are entangled in steady state when the coupling strength is greater than a critical value, and the critical coupling increases with detuning. An ensemble of many oscillators with random frequencies still exhibits a synchronization phase transition in the quantum limit, and we analytically calculate how the critical coupling depends on the frequency disorder. Our results can be experimentally observed with trapped ions or neutral atoms. C1 [Lee, Tony E.; Chan, Ching-Kit] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Lee, Tony E.; Chan, Ching-Kit] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Wang, Shenshen] MIT, Dept Phys, Cambridge, MA 02139 USA. [Wang, Shenshen] MIT, Dept Chem Engn, Cambridge, MA 02139 USA. RP Lee, TE (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. FU NSF; Croucher Foundation FX This work was supported by the NSF through a grant to ITAMP. C.K.C. is supported by the Croucher Foundation. NR 61 TC 24 Z9 24 U1 0 U2 9 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1539-3755 EI 1550-2376 J9 PHYS REV E JI Phys. Rev. E PD FEB 12 PY 2014 VL 89 IS 2 AR 022913 DI 10.1103/PhysRevE.89.022913 PG 10 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA AC0ID UT WOS:000332177100007 PM 25353551 ER PT J AU Aliu, E Archambault, S Arlen, T Aune, T Behera, B Beilicke, M Benbow, W Berger, K Bird, R Bouvier, A Buckley, JH Bugaev, V Byrum, K Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Duke, C Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fleischhack, H Fortin, P Fortson, L Furniss, A Galante, N Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Johnson, CA Kaaret, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lang, MJ Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Meagher, K Millis, J Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Park, N Perkins, JS Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Richards, GT Roache, E Sembroski, GH Smith, AW Staszak, D Telezhinsky, I Theiling, M Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Weekes, TC Weinstein, A Welsing, R Williams, DA Zajczyk, A Zitzer, B AF Aliu, E. Archambault, S. Arlen, T. Aune, T. Behera, B. Beilicke, M. Benbow, W. Berger, K. Bird, R. Bouvier, A. Buckley, J. H. Bugaev, V. Byrum, K. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Duke, C. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fleischhack, H. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Johnson, C. A. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Meagher, K. Millis, J. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Sembroski, G. H. Smith, A. W. Staszak, D. Telezhinsky, I. Theiling, M. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Weekes, T. C. Weinstein, A. Welsing, R. Williams, D. A. Zajczyk, A. Zitzer, B. TI A THREE-YEAR MULTI-WAVELENGTH STUDY OF THE VERY-HIGH-ENERGY gamma-RAY BLAZAR 1ES 0229+200 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; BL Lacertae objects: individual (1ES 0229+200, VER J0232+202); diffuse radiation; galaxies: active; gamma rays: general; magnetic fields ID EXTRAGALACTIC BACKGROUND LIGHT; ACTIVE GALACTIC NUCLEI; BL LACERTAE OBJECTS; INTERGALACTIC MAGNETIC-FIELD; LARGE-AREA TELESCOPE; X-RAY; TEV BLAZARS; SPACE-TELESCOPE; DISTANT BLAZARS; LORENTZ FACTOR AB The high-frequency-peaked BL Lacertae object 1ES 0229+200 is a relatively distant (z = 0.1396), hard-spectrum (Gamma similar to 2.5), very-high-energy (VHE; E > 100 GeV) emitting gamma-ray blazar. VHE measurements of this active galactic nucleus have been used to place constraints on the intensity of the extragalactic background light and the intergalactic magnetic field (IGMF). A multi-wavelength study of this object centered around VHE observations by Very Energetic Radiation Imaging Telescope Array System (VERITAS) is presented. This study obtained, over a period of three years, an 11.7 standard deviation detection and an average integral flux F(E > 300 GeV) = (23.3 +/- 2.8(stat) +/- 5.8(sys)) x 10(-9) photons m(-2) s(-1), or 1.7% of the Crab Nebula's flux (assuming the Crab Nebula spectrum measured by H. E. S. S). Supporting observations from Swift and RXTE are analyzed. The Swift observations are combined with previously published Fermi observations and the VHE measurements to produce an overall spectral energy distributionwhich is then modeled assuming one-zone synchrotron-self-Compton emission. The chi(2) probability of the TeV flux being constant is 1.6%. This, when considered in combination with measured variability in the X-ray band, and the demonstrated variability of many TeV blazars, suggests that the use of blazars such as 1ES 0229+200 for IGMF studies may not be straightforward and challenges models that attribute hard TeV spectra to secondary gamma-ray production along the line of sight. 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.; Staszak, D.] McGill Univ, Dept Phys, Montreal, PQ, 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. [Behera, B.; Chen, X.; Federici, S.; Fleischhack, H.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.; Zajczyk, A.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Roache, E.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Bouvier, A.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Chen, X.; Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [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.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Humensky, T. B.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Krennrich, F.; Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Majumdar, P.] Saha Inst Nucl Phys, Kolkata 700064, India. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 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 mcerruti@cfa.harvard.edu; jeremy.s.perkins@nasa.gov RI Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755; Cui, Wei/0000-0002-6324-5772 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K; National Aeronautics and Space Administration FX VERITAS is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 73 TC 14 Z9 14 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2014 VL 782 IS 1 AR 13 DI 10.1088/0004-637X/782/1/13 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB5SG UT WOS:000331848200013 ER PT J AU Hickox, RC Mullaney, JR Alexander, DM Chen, CTJ Civano, FM Goulding, AD Hainline, KN AF Hickox, Ryan C. Mullaney, James R. Alexander, David M. Chen, Chien-Ting J. Civano, Francesca M. Goulding, Andy D. Hainline, Kevin N. TI BLACK HOLE VARIABILITY AND THE STAR FORMATION-ACTIVE GALACTIC NUCLEUS CONNECTION: DO ALL STAR-FORMING GALAXIES HOST AN ACTIVE GALACTIC NUCLEUS? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; quasars: general ID SIMILAR-TO 2; QUASAR LUMINOSITY FUNCTION; DIGITAL SKY SURVEY; CHANDRA-DEEP-FIELDS; M-ASTERISK RELATION; BROAD-LINE QUASARS; SGR A-ASTERISK; X-RAY AGN; FORMATION RATES; GOODS-HERSCHEL AB We investigate the effect of active galactic nucleus (AGN) variability on the observed connection between star formation and black hole accretion in extragalactic surveys. Recent studies have reported relatively weak correlations between observed AGN luminosities and the properties of AGN hosts, which has been interpreted to imply that there is no direct connection between AGN activity and star formation. However, AGNs may be expected to vary significantly on a wide range of timescales (from hours to Myr) that are far shorter than the typical timescale for star formation (greater than or similar to 100 Myr). This variability can have important consequences for observed correlations. We present a simple model in which all star-forming galaxies host an AGN when averaged over similar to 100 Myr timescales, with long-term average AGN accretion rates that are perfectly correlated with the star formation rate (SFR). We show that reasonable prescriptions for AGN variability reproduce the observed weak correlations between SFR and L-AGN in typical AGN host galaxies, as well as the general trends in the observed AGN luminosity functions, merger fractions, and measurements of the average AGN luminosity as a function of SFR. These results imply that there may be a tight connection between AGN activity and SFR over galaxy evolution timescales, and that the apparent similarities in rest-frame colors, merger rates, and clustering of AGNs compared to "inactive" galaxies may be due primarily to AGN variability. The results provide motivation for future deep, wide extragalactic surveys that can measure the distribution of AGN accretion rates as a function of SFR. C1 [Hickox, Ryan C.; Chen, Chien-Ting J.; Civano, Francesca M.; Hainline, Kevin N.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Mullaney, James R.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Mullaney, James R.; Alexander, David M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Civano, Francesca M.; Goulding, Andy D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hickox, RC (reprint author), Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. EM ryan.c.hickox@dartmouth.edu OI Chen, Chien-Ting/0000-0002-4945-5079; Alexander, David/0000-0002-5896-6313 FU Leverhulme Trust; NASA [11-ADAP11-0218]; Dartmouth Fellowship; Chandra grant [SP8-9001X] FX We thank David Rosario, Sara Ellison, and Philip Hopkins for helpful discussions, and are grateful to the anonymous referee for constructive comments that improved the paper. J.R.M. and D. M. A. acknowledge generous support from the Leverhulme Trust. F. C. acknowledges support by the NASA contract 11-ADAP11-0218. C.-T.J.C. acknowledges support from a Dartmouth Fellowship. This work was supported in part by Chandra grant SP8-9001X. This research has made use of NASA's Astrophysics Data System. NR 138 TC 102 Z9 102 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2014 VL 782 IS 1 AR 9 DI 10.1088/0004-637X/782/1/9 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB5SG UT WOS:000331848200009 ER PT J AU Yadav, N Ray, A Chakraborti, S Stockdale, C Chandra, P Smith, R Roy, R Bose, S Dwarkadas, V Sutaria, F Pooley, D AF Yadav, Naveen Ray, Alak Chakraborti, Sayan Stockdale, Christopher Chandra, Poonam Smith, Randall Roy, Rupak Bose, Subhash Dwarkadas, Vikram Sutaria, Firoza Pooley, David TI ELECTRON COOLING IN A YOUNG RADIO SUPERNOVA: SN 2012aw SO ASTROPHYSICAL JOURNAL LA English DT Article DE radiation mechanisms: non-thermal; radio continuum: general; stars: mass-loss; supernovae: individual (SN 2012aw); techniques: interferometric; X-rays: general ID X-RAY-EMISSION; CORE-COLLAPSE SUPERNOVAE; CIRCUMSTELLAR INTERACTION; II SUPERNOVAE; MASS-LOSS; HYDRODYNAMICAL MODELS; PLATEAU STAGE; LIGHT CURVES; PROGENITOR; RED AB We present the radio observations and modeling of an optically bright Type II-P supernova (SN), SN 2012aw which exploded in the nearby galaxy Messier 95 (M95) at a distance of 10 Mpc. The spectral index values calculated using C, X, and K bands are smaller than the expected values for the optically thin regime. During this time, the optical bolometric light curve stays in the plateau phase. We interpret the low spectral-index values to be a result of electron cooling. On the basis of comparison between the Compton cooling timescale and the synchrotron cooling timescale, we find that the inverse Compton cooling process dominates over the synchrotron cooling process. We therefore model the radio emission as synchrotron emission from a relativistic electron population with a high energy cutoff. The cutoff is determined by comparing the electron cooling timescale, t(cool), and the acceleration timescale, (t) over tilde (acc). We constrain the mass-loss rate in the wind ((M) over dot similar to 1.9x10(-6) M-circle dot yr(-1)) and the equipartition factor between relativistic electrons and the magnetic field ((alpha) over tilde = epsilon(e)/epsilon(B) similar to 1.12 x 10(2)) through our modeling of radio emission. Although the time of explosion is fairly well constrained by optical observations within about two days, we explore the effect of varying the time of explosion to best fit the radio light curves. The best fit is obtained for the explosion date as 2012 March 15.3 UT. C1 [Yadav, Naveen; Ray, Alak] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Chakraborti, Sayan] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Stockdale, Christopher] Marquette Univ, Milwaukee, WI 53233 USA. [Chandra, Poonam] Natl Ctr Radio Astron TIFR, Pune 411007, Maharashtra, India. [Smith, Randall] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Roy, Rupak; Bose, Subhash] Aryabhhata Res Inst Observat Sci, Naini Tal 263129, India. [Dwarkadas, Vikram] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Sutaria, Firoza] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Pooley, David] Sam Houston State Univ, Dept Phys, Huntsville, TX 77341 USA. RP Yadav, N (reprint author), Tata Inst Fundamental Res, Homi Bhabha Rd, Bombay 400005, Maharashtra, India. EM nyadav@tifr.res.in; akr@tifr.res.in OI Yadav, Naveen/0000-0002-4107-9443 FU TIFR [12P-0261]; CSIR-SPM [SPM-07/858(0057)/2009-EMR-I] FX Initial observation of SN 2012aw was requested under Joint Chandra-NRAO Cycle-13 ToO proposal (Proposal ID No. 13500809) on Type II-P SNe. A.R. thanks the Department of Physics at the West Virginia University for their hospitality during proposal development. We thank the anonymous reviewer for comments, queries, and suggestions, which significantly helped us in improving the manuscript. We acknowledge the support of TIFR 12th Five Year Plan (Project No: 12P-0261). We thank the Director Karl G. Jansky VLA for granting us the observations under Director's Discretionary Time. N.Y. wishes to acknowledge the support of CSIR-SPM fellowship (SPM-07/858(0057)/2009-EMR-I). NR 38 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2014 VL 782 IS 1 AR 30 DI 10.1088/0004-637X/782/1/30 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB5SG UT WOS:000331848200030 ER PT J AU Indebetouw, R Matsuura, M Dwek, E Zanardo, G Barlow, MJ Baes, M Bouchet, P Burrows, DN Chevalier, R Clayton, GC Fransson, C Gaensler, B Kirshner, R Lakicevic, M Long, KS Lundqvist, P Marti-Vidal, I Marcaide, J McCray, R Meixner, M Ng, CY Park, S Sonneborn, G Staveley-Smith, L Vlahakis, C van Loon, J AF Indebetouw, R. Matsuura, M. Dwek, E. Zanardo, G. Barlow, M. J. Baes, M. Bouchet, P. Burrows, D. N. Chevalier, R. Clayton, G. C. Fransson, C. Gaensler, B. Kirshner, R. Lakicevic, M. Long, K. S. Lundqvist, P. Marti-Vidal, I. Marcaide, J. McCray, R. Meixner, M. Ng, C. -Y. Park, S. Sonneborn, G. Staveley-Smith, L. Vlahakis, C. van Loon, J. TI DUST PRODUCTION AND PARTICLE ACCELERATION IN SUPERNOVA 1987A REVEALED WITH ALMA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: ISM; ISM: supernova remnants; Magellanic Clouds; supernovae: individual (1987A) ID HUBBLE-SPACE-TELESCOPE; SN 1987A; EARLY UNIVERSE; OPTICAL-PROPERTIES; MASSIVE STARS; REVERSE SHOCK; EVOLUTION; REMNANT; EJECTA; EMISSION AB Supernova (SN) explosions are crucial engines driving the evolution of galaxies by shock heating gas, increasing the metallicity, creating dust, and accelerating energetic particles. In 2012 we used the Atacama Large Millimeter/Submillimeter Array to observe SN 1987A, one of the best-observed supernovae since the invention of the telescope. We present spatially resolved images at 450 mu m, 870 mu m, 1.4 mm, and 2.8 mm, an important transition wavelength range. Longer wavelength emission is dominated by synchrotron radiation from shock-accelerated particles, shorter wavelengths by emission from the largest mass of dust measured in a supernova remnant (>0.2 M-circle dot). For the first time we show unambiguously that this dust has formed in the inner ejecta (the cold remnants of the exploded star's core). The dust emission is concentrated at the center of the remnant, so the dust has not yet been affected by the shocks. If a significant fraction survives, and if SN 1987A is typical, supernovae are important cosmological dust producers. C1 [Indebetouw, R.; Chevalier, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Indebetouw, R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Matsuura, M.; Barlow, M. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Dwek, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zanardo, G.; Staveley-Smith, L.] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia. [Baes, M.] Univ Ghent, Sterrenkundig Observat, B-9000 Ghent, Belgium. [Bouchet, P.] CEA Saclay, F-91191 Gif Sur Yvette, France. [Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Clayton, G. C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Fransson, C.; Lundqvist, P.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Fransson, C.; Lundqvist, P.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Gaensler, B.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Kirshner, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lakicevic, M.; van Loon, J.] Keele Univ, Lennard Jones Labs, Keele ST5 5BG, Staffs, England. [Long, K. S.; Meixner, M.; Sonneborn, G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Marti-Vidal, I.] Chalmers Univ, Dept Earth & Space Sci, Onsala Space Observ, SE-43992 Onsala, Sweden. [Marcaide, J.] Univ Valencia, E-46100 Burjassot, Spain. [McCray, R.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Meixner, M.] Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr 366, Baltimore, MD 21218 USA. [Ng, C. -Y.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Park, S.] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. [Vlahakis, C.] European So Observ, Joint ALMA Observ, Santiago 19, Chile. RP Indebetouw, R (reprint author), Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA. EM remy@virginia.edu RI Barlow, Michael/A-5638-2009; Ng, Chi Yung/A-7639-2013; Marti-Vidal, Ivan/A-8799-2017; Staveley-Smith, Lister/A-1683-2011; OI Barlow, Michael/0000-0002-3875-1171; Ng, Chi Yung/0000-0002-5847-2612; Marti-Vidal, Ivan/0000-0003-3708-9611; Staveley-Smith, Lister/0000-0002-8057-0294; Zanardo, Giovanna/0000-0003-2742-771X; Gaensler, Bryan/0000-0002-3382-9558; Baes, Maarten/0000-0002-3930-2757 FU NASA [NAG5-12595, NASA/ADAP NNX13AE36G] FX This Letter makes use of the following ALMA data: ADS/JAO. ALMA#2011.0.00273. S (PI: Indebetouw). 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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. M. M. was supported by NASA NAG5-12595 and NASA/ADAP NNX13AE36G. NR 49 TC 59 Z9 60 U1 0 U2 9 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 FEB 10 PY 2014 VL 782 IS 1 AR L2 DI 10.1088/2041-8205/782/1/L2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5OR UT WOS:000331149900002 ER PT J AU Milisavljevic, D Margutti, R Crabtree, KN Foster, JB Soderberg, AM Fesen, RA Parrent, JT Sanders, NE Drout, MR Kamble, A Chakraborti, S Pickering, TE Cenko, SB Silverman, JM Filippenko, AV Kirshner, RP Mazzali, P Maeda, K Marion, GHH Vinko, J Wheeler, JC AF Milisavljevic, Dan Margutti, Raffaella Crabtree, Kyle N. Foster, Jonathan B. Soderberg, Alicia M. Fesen, Robert A. Parrent, Jerod T. Sanders, Nathan E. Drout, Maria R. Kamble, Atish Chakraborti, Sayan Pickering, Timothy E. Cenko, S. Bradley Silverman, Jeffrey M. Filippenko, Alexei V. Kirshner, Robert P. Mazzali, Paolo Maeda, Keiichi Marion, G. H. Howie Vinko, Jozsef Wheeler, J. Craig TI INTERACTION BETWEEN THE BROAD-LINED TYPE Ic SUPERNOVA 2012ap AND CARRIERS OF DIFFUSE INTERSTELLAR BANDS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: lines and bands; ISM: molecules; molecular processes; supernovae: general; supernovae: individual (SN 2012ap) ID LUMINOUS BLUE VARIABLES; RAY TRANSIENT 080109; IA SUPERNOVA; CROSS-SECTIONS; IBC SUPERNOVA; MASS-LOSS; STARS; PHOTOIONIZATION; PHOTOABSORPTION; SPECTROSCOPY AB Diffuse interstellar bands (DIBs) are absorption features observed in optical and near-infrared spectra that are thought to be associated with carbon-rich polyatomic molecules in interstellar gas. However, because the central wavelengths of these bands do not correspond to electronic transitions of any known atomic or molecular species, their nature has remained uncertain since their discovery almost a century ago. Here we report on unusually strong DIBs in optical spectra of the broad-lined Type Ic supernova SN 2012ap that exhibit changes in equivalent width over short (less than or similar to 30 days) timescales. The 4428 angstrom and 6283 angstrom DIB features get weaker with time, whereas the 5780 angstrom feature shows a marginal increase. These nonuniform changes suggest that the supernova is interacting with a nearby source of DIBs and that the DIB carriers possess high ionization potentials, such as small cations or charged fullerenes. We conclude that moderate-resolution spectra of supernovae with DIB absorptions obtained within weeks of outburst could reveal unique information about the mass-loss environment of their progenitor systems and provide new constraints on the properties of DIB carriers. C1 [Milisavljevic, Dan; Margutti, Raffaella; Crabtree, Kyle N.; Soderberg, Alicia M.; Sanders, Nathan E.; Drout, Maria R.; Kamble, Atish; Chakraborti, Sayan; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Foster, Jonathan B.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Parrent, Jerod T.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Parrent, Jerod T.] Las Cumbres Observ Global Telescope Network, Goleta, CA USA. [Pickering, Timothy E.] Southern African Large Telescope, ZA-7935 Cape Town, South Africa. [Pickering, Timothy E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. Bradley; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Silverman, Jeffrey M.; Marion, G. H. Howie; Vinko, Jozsef; Wheeler, J. Craig] Univ Texas Austin, Austin, TX 78712 USA. [Mazzali, Paolo] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Mazzali, Paolo] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Maeda, Keiichi] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Maeda, Keiichi] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Univ WPI, Kashiwa, Chiba 2778583, Japan. [Vinko, Jozsef] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. RP Milisavljevic, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dmilisav@cfa.harvard.edu OI Crabtree, Kyle/0000-0001-5629-5192 FU W. M. Keck Foundation; David and Lucile Packard Foundation; NSF [AST-1302771, AST-1211196, AST-1109801, AST-1211916]; Richard and Rhoda Goldman Fund; Christopher R. Redlich Fund; TABASGO Foundation; CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory FX We thank an anonymous referee for a helpful, detailed, and critical reading of the Letter. T. Snow kindly provided comments on an early draft of the Letter. P. Massey provided insightful comments. G. Pignata, S. Valenti, D. Malesani, and G. Leloudas shared archival spectra that were examined. Many of the observations reported in this Letter were obtained with the Southern African Large Telescope. Additional data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. A. Miller, P. Nugent, and A. Morgan helped obtain the Keck observations. Some observations also came from the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Support 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. T. E. P. thanks the National Research Foundation of South Africa. R. P. K. and J.C.W. are grateful for NSF grants AST-1211196 and AST-1109801, respectively. A. V. F. and S. B. C. acknowledge generous support from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. K.N.C. has been supported by a CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory. This Letter made extensive use of the SUSPECT database (http://www.nhn.ou.edu/similar to suspect/). NR 50 TC 9 Z9 9 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 10 PY 2014 VL 782 IS 1 AR L5 DI 10.1088/2041-8205/782/1/L5 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5OR UT WOS:000331149900005 ER PT J AU Mokross, K Ryder, TB Cortes, MC Wolfe, JD Stouffer, PC AF Mokross, Karl Ryder, Thomas B. Cortes, Marina Correa Wolfe, Jared D. Stouffer, Philip C. TI Decay of interspecific avian flock networks along a disturbance gradient in Amazonia SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE forest fragmentation; insectivorous birds; mixed-species flocks; network theory; Amazon; heterogeneous landscapes ID SPECIES BIRD FLOCKS; RAIN-FOREST FRAGMENTS; SOCIAL NETWORK; FOOD WEBS; INSECTIVOROUS BIRDS; NEOTROPICAL FOREST; HABITAT DEGRADATION; SIZE; BIODIVERSITY; EVOLUTION AB Our understanding of how anthropogenic habitat change shapes species interactions is in its infancy. This is in large part because analytical approaches such as network theory have only recently been applied to characterize complex community dynamics. Network models are a powerful tool for quantifying how ecological interactions are affected by habitat modification because they provide metrics that quantify community structure and function. Here, we examine how large-scale habitat alteration has affected ecological interactions among mixed-species flocking birds in Amazonian rainforest. These flocks provide a model system for investigating how habitat heterogeneity influences non-trophic interactions and the subsequent social structure of forest-dependent mixed-species bird flocks. We analyse 21 flock interaction networks throughout a mosaic of primary forest, fragments of varying sizes and secondary forest (SF) at the Biological Dynamics of Forest Fragments Project in central Amazonian Brazil. Habitat type had a strong effect on network structure at the levels of both species and flock. Frequency of associations among species, as summarized by weighted degree, declined with increasing levels of forest fragmentation and SF. At the flock level, clustering coefficients and overall attendance positively correlated with mean vegetation height, indicating a strong effect of habitat structure on flock cohesion and stability. Prior research has shown that trophic interactions are often resilient to large-scale changes in habitat structure because species are ecologically redundant. By contrast, our results suggest that behavioural interactions and the structure of non-trophic networks are highly sensitive to environmental change. Thus, a more nuanced, system-by-system approach may be needed when thinking about the resiliency of ecological networks. C1 [Mokross, Karl; Wolfe, Jared D.; Stouffer, Philip C.] Louisiana State Univ, Ctr Agr, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA. [Mokross, Karl; Cortes, Marina Correa; Wolfe, Jared D.; Stouffer, Philip C.] INPA, Projeto Dinam Biol Fragmentos Florestais, BR-69083000 Manaus, Amazonas, Brazil. [Ryder, Thomas B.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20013 USA. [Cortes, Marina Correa] Univ Estadual Paulista, Dept Ecol, BR-13506900 Rio Claro, SP, Brazil. RP Mokross, K (reprint author), Louisiana State Univ, Ctr Agr, Sch Renewable Nat Resources, 227 RNR Bldg, Baton Rouge, LA 70803 USA. EM kmokro1@tigers.lsu.edu RI cortes, marina/I-2155-2012 FU US National Science Foundation [LTREB-0545491]; AOU FX Funding for the research was provided by US National Science Foundation grant LTREB-0545491 and by an AOU 2010 research award. NR 76 TC 11 Z9 12 U1 6 U2 44 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 FEB 7 PY 2014 VL 281 IS 1776 AR 20132599 DI 10.1098/rspb.2013.2599 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AC2YF UT WOS:000332381500013 PM 24335983 ER PT J AU Villanueva-Gutierrez, R Echazarreta-Gonzalez, C Roubik, DW Moguel-Ordonez, YB AF Villanueva-Gutierrez, R. Echazarreta-Gonzalez, C. Roubik, D. W. Moguel-Ordonez, Y. B. TI Transgenic soybean pollen (Glycine max L.) in honey from the Yucatan peninsula, Mexico SO SCIENTIFIC REPORTS LA English DT Article ID APIS-MELLIFERA AB Using precise pollen species determination by conventional microscopic methods, accompanied by molecular genetic markers, we found bees collect GMO (genetically modified) soybean pollen and incorporate it in Yucatan honey. Honey comb samples from Las Flores, Campeche, Mexico, often contained soybean pollen. Pollen in honey was analyzed in nine samples; six contained substantial soy pollen and two tested positive for soybean GMO. Our analyses confirm field observations that honey bees, Apis mellifera, gather soybean pollen and nectar. The resultant risk for honey production in the Yucatan Peninsula and Mexico is evident in wholesale price reduction of 12% when GMO products are detected and honey consignments are rejected. Although this affects only 1% of current export honey (2011-2013) GMO soybean is an unacknowledged threat to apiculture and its economics in one of the world's foremost honey producing areas. C1 [Villanueva-Gutierrez, R.] El Colegio Frontera Sur, Chetmal 77014, Quintana Roo, Mexico. [Echazarreta-Gonzalez, C.] Univ Autonoma Yucatan, Fac Med Vet & Zootecnia, Merida, Yucatan, Mexico. [Roubik, D. W.] Smithsonian Trop Res Inst, Panama City, Panama. [Moguel-Ordonez, Y. B.] INIFAP, CIR Sureste, CE Mococha, Campeche, Mexico. RP Roubik, DW (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM roubikd@si.edu NR 20 TC 3 Z9 3 U1 3 U2 47 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 FEB 7 PY 2014 VL 4 AR 4022 DI 10.1038/srep04022 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AA6RW UT WOS:000331226700005 PM 24503936 ER PT J AU Lumbantobing, DN AF Lumbantobing, Daniel N. TI Four new species of Rasbora of the Sumatrana group (Teleostei: Cyprinidae) from northern Sumatra, Indonesia SO ZOOTAXA LA English DT Article DE Danioninae; Rasbora; new species; northern Sumatra; Sundaland ID FISH AB Four new species of the minnow genus Rasbora of the Sumatrana group, R. arundinata, R. haru, R. maninjau, and R. bindumatoga, are described from northern Sumatra. Rasbora arundinata is distinguished from all congeners in the Sumatrana group by the black midlateral stripe overall forming a reed-leaf-like profile. Rasbora haru differs from its congeners in the Sumatrana group in having the black midlateral stripe overall forming a stamen-like profile. The new species endemic to Lake Maninjau in central west Sumatra, Rasbora maninjau, is unique among all the congeners in the Sumatrana group in having a combination of the black midlateral stripe extending from the midhumeral region of uniform width, the prominent acutely triangular basicaudal blotch, and the oval supra-anal pigmentation. Rasbora bindumatoga is distinguished from all congeners in the Sumatrana group by a combination of the black rectangular subdorsal blotch, the absence of supra-anal pigmentation, and the somewhat oval basicaudal blotch. Rasbora arundinata, R. maninjau, and R. bindumatoga occur allopatrically in the northwestern coastal region of Sumatra, while R. haru is known from northeastern coastal area of Sumatra. A new diagnostic character for the Sumatrana group is described: partial exposure of the upper lip due to a submedial contact between the maxilla and the lower lip, which is marked posteriorly by a lachrymal groove. C1 [Lumbantobing, Daniel N.] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Lumbantobing, Daniel N.] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20013 USA. RP Lumbantobing, DN (reprint author), George Washington Univ, Dept Biol Sci, 2023 G St NW,Lisner Hall 340, Washington, DC 20052 USA. EM dntobing@gwmail.gwu.edu FU Leonard P. Schultz Fund, Division of Fishes, USNM FX I express my thanks to L. Parenti (USNM) for her support and guidance throughout the project. I gratefully acknowledge J. Burns (GWU) for his supervision and critical comments on the text. I thank R. Vari (USNM) and L. Page (UF) who critically reviewed the manuscript. I am indebted to R. Hadiaty (MZB) who guided me in the field and facilitated the permits. I am grateful to M. Kottelat and H. H. Tan (ZRC) for the insightful discussion and constructive criticisms on the taxonomy of Rasbora. I acknowledge the following at USNM for their invaluable assistance: J. Clayton, J. Williams, J. Finan, S. Raredon, and D. Cole (base map). I thank the following for access to material under their care: M. Sabaj Perez (ANSP), R. Britz, O. Crimmen and P. Campbell (BMNH), M. Kottelat (CMK), K. Grossenbacher and S. Hertwig (NMBE), R. de Ruiter and M. van Oijen (RMNH), R. Robins (UF), R. Vonk and H. Praagman (ZMA), and K. Lim and H. H. Tan (ZRC). I am grateful to D. Rudaya, N. M. Ray, D. Syahril, and V. Simanjuntak for their fieldwork assistance. The 2006 ichthyofaunal survey in northern Sumatra was financially supported by the Leonard P. Schultz Fund, Division of Fishes, USNM. This article constitutes part of my dissertation submitted in partial fulfillment of the degree of Doctor of Philosophy to the Department of Biological Sciences, the George Washington University. NR 25 TC 1 Z9 1 U1 1 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 7 PY 2014 VL 3764 IS 1 BP 1 EP 25 PG 25 WC Zoology SC Zoology GA AA0CT UT WOS:000330763400001 PM 24870277 ER PT J AU Muller-Landau, HC AF Muller-Landau, Helene C. TI ECOLOGY Plant diversity rooted in pathogens SO NATURE LA English DT Editorial Material ID TROPICAL FOREST; DENSITY-DEPENDENCE; TREE C1 Smithsonian Trop Res Inst, Panama City, Panama. RP Muller-Landau, HC (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama. EM mullerh@si.edu NR 11 TC 1 Z9 1 U1 2 U2 61 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD FEB 6 PY 2014 VL 506 IS 7486 BP 44 EP 45 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 303BA UT WOS:000330648100027 PM 24463509 ER PT J AU Brodu, E Balat-Pichelin, M Sans, JL Kasper, JC AF Brodu, E. Balat-Pichelin, M. Sans, J. -L. Kasper, J. C. TI Influence of roughness and composition on the total emissivity of tungsten, rhenium and tungsten-25% rhenium alloy at high temperature SO JOURNAL OF ALLOYS AND COMPOUNDS LA English DT Article DE High temperature metals and alloys; Optical properties; BRDF; XRD; SEM ID NORMAL-SPECTRAL-EMISSIVITY; THERMAL-RADIATION; SURFACES; VACUUM AB Measurements of the total directional and hemispherical emissivity of tungsten, rhenium and tungsten with 25% rhenium samples of various surface states was carried out in two wavelength ranges, 0.6-2.8 and 0.6-40 mu m, from 1300 up to 2500 K in high vacuum. A clear trend was identified for the ratio of the 0.6-2.8 mu m to the 0.6-40 mu m hemispherical emissivity (assumed to be close to the true alpha/epsilon ratio, which is the ratio of the solar absorptivity a to the total emissivity epsilon) as a function of the RMS roughness. This ratio is decreasing with increasing RMS roughness rapidly up to around 1 mu m and then tends to stabilize for higher roughness. It suggests that increasing the roughness, starting from a flat surface, will progressively give more weight to the long wavelength range emissivities in comparison to the short wavelength ones. Beside the RMS roughness, a sharp surface structure on a finer scale found on some samples also led to an additional decrease of the alpha/epsilon ratio, but these structures are not stable at high temperature and disappear due to a natural high temperature smoothing. Finally our results also show that the alpha/epsilon ratio of rhenium is lower than the one of tungsten. (C) 2013 Elsevier B. V. All rights reserved. C1 [Brodu, E.; Balat-Pichelin, M.; Sans, J. -L.] PROMES CNRS, Lab Proc Mat & Energie Solaire, F-66120 Font Romeu, France. [Brodu, E.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Balat-Pichelin, M (reprint author), PROMES CNRS, Lab Proc Mat & Energie Solaire, 7 Rue 4 Solaire, F-66120 Font Romeu, France. EM marianne.balat@promes.cnrs.fr FU CNES FX The authors gratefully acknowledge CNES and particularly J.Y. Prado for the support of the Ph.D. of Etienne Brodu, Guillaume Libaude for his participation to the experiments and Daniele Perarnau for XRD measurements. NR 17 TC 5 Z9 5 U1 1 U2 28 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-8388 EI 1873-4669 J9 J ALLOY COMPD JI J. Alloy. Compd. PD FEB 5 PY 2014 VL 585 BP 510 EP 517 DI 10.1016/j.jallcom.2013.09.184 PG 8 WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering GA 258XS UT WOS:000327492600076 ER PT J AU Chen, H Burnett, RT Kwong, JC Villeneuve, PJ Goldberg, MS Brook, RD van Donkelaar, A Jerrett, M Martin, RV Kopp, A 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. Kopp, Alexander Brook, Jeffrey R. Copes, Ray TI Spatial Association Between Ambient Fine Particulate Matter and Incident Hypertension SO CIRCULATION LA English DT Article DE air pollution; cohort studies; epidemiology; hypertension ID LONG-TERM EXPOSURE; AIR-POLLUTION EXPOSURE; BLOOD-PRESSURE; CARDIOVASCULAR-DISEASE; RISK-FACTORS; MORTALITY; COHORT; ATHEROSCLEROSIS; PREVALENCE; ONTARIO AB Background Laboratory studies suggest that exposure to fine particulate matter (2.5 m in diameter) (PM2.5) can trigger a combination of pathophysiological responses that may induce the development of hypertension. However, epidemiological evidence relating PM2.5 and hypertension is sparse. We thus conducted a population-based cohort study to determine whether exposure to ambient PM2.5 is associated with incident hypertension. Methods and Results We assembled a cohort of 35 303 nonhypertensive adults from Ontario, Canada, who responded to 1 of 4 population-based health surveys between 1996 and 2005 and were followed up until December 31, 2010. Incident diagnoses of hypertension were ascertained from the Ontario Hypertension Database, a validated registry of persons diagnosed with hypertension in Ontario (sensitivity=72%, specificity=95%). Estimates of long-term exposure to PM2.5 at participants' postal-code residences were derived from satellite observations. We used Cox proportional hazards models, adjusting for various individual and contextual risk factors including body mass index, smoking, physical activity, and neighbourhood-level unemployment rates. We conducted various sensitivity analyses to assess the robustness of the effect estimate, such as investigating several time windows of exposure and controlling for potential changes in the risk of hypertension over time. Between 1996 and 2010, we identified 8649 incident cases of hypertension and 2296 deaths. For every 10-mu g/m(3) increase of PM2.5, the adjusted hazard ratio of incident hypertension was 1.13 (95% confidence interval, 1.05-1.22). Estimated associations were comparable among all sensitivity analyses. Conclusions This study supports an association between PM2.5 and incident hypertension. C1 [Chen, Hong; Kwong, Jeffrey C.; Copes, Ray] Publ Hlth Ontario, Toronto, ON M5G 1V2, Canada. [Chen, Hong; Kwong, Jeffrey C.; Villeneuve, Paul J.; Copes, Ray] Univ Toronto, Dalla Lana Sch Publ Hlth, Toronto, ON, Canada. [Chen, Hong; Kwong, Jeffrey C.; Kopp, Alexander] Inst Clin Evaluat Sci, Toronto, ON, Canada. [Burnett, Richard T.] Hlth Canada, Populat Studies Div, Ottawa, ON K1A 0L2, Canada. [Kwong, Jeffrey C.] Univ Toronto, Dept Family & Community Med, Toronto, ON M5S 1A1, Canada. [Villeneuve, Paul J.] Carleton Univ, Dept Hlth Sci, Ottawa, ON K1S 5B6, 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 Public Health Ontario from Health Canada [4500275504]; Health Canada; Natural Sciences and Engineering Research Council of Canada FX This work was supported by operating funds from Public Health Ontario and a contract (4500275504) from Health Canada. Drs Martin and van Donkelaar were supported by Health Canada and the Natural Sciences and Engineering Research Council of Canada. NR 50 TC 30 Z9 35 U1 5 U2 39 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0009-7322 EI 1524-4539 J9 CIRCULATION JI Circulation PD FEB 4 PY 2014 VL 129 IS 5 BP 562 EP 569 DI 10.1161/CIRCULATIONAHA.113.003532 PG 8 WC Cardiac & Cardiovascular Systems; Peripheral Vascular Disease SC Cardiovascular System & Cardiology GA 302EA UT WOS:000330583300012 PM 24190962 ER PT J AU Hinde, K Carpenter, AJ Clay, JS Bradford, BJ AF Hinde, Katie Carpenter, Abigail J. Clay, John S. Bradford, Barry J. TI Holsteins Favor Heifers, Not Bulls: Biased Milk Production Programmed during Pregnancy as a Function of Fetal Sex SO PLOS ONE LA English DT Article ID TRIVERS-WILLARD HYPOTHESIS; LOCAL RESOURCE COMPETITION; PARENT-OFFSPRING CONFLICT; DAIRY-COWS; MAMMARY-GLAND; MATERNAL INVESTMENT; BOVINE SOMATOTROPIN; LIFE-HISTORY; CALF SEX; FACULTATIVE ADJUSTMENT AB Mammalian females pay high energetic costs for reproduction, the greatest of which is imposed by lactation. The synthesis of milk requires, in part, the mobilization of bodily reserves to nourish developing young. Numerous hypotheses have been advanced to predict how mothers will differentially invest in sons and daughters, however few studies have addressed sex-biased milk synthesis. Here we leverage the dairy cow model to investigate such phenomena. Using 2.39 million lactation records from 1.49 million dairy cows, we demonstrate that the sex of the fetus influences the capacity of the mammary gland to synthesize milk during lactation. Cows favor daughters, producing significantly more milk for daughters than for sons across lactation. Using a sub-sample of this dataset (N = 113,750 subjects) we further demonstrate that the effects of fetal sex interact dynamically across parities, whereby the sex of the fetus being gestated can enhance or diminish the production of milk during an established lactation. Moreover the sex of the fetus gestated on the first parity has persistent consequences for milk synthesis on the subsequent parity. Specifically, gestation of a daughter on the first parity increases milk production by similar to 445 kg over the first two lactations. Our results identify a dramatic and sustained programming of mammary function by offspring in utero. Nutritional and endocrine conditions in utero are known to have pronounced and long-term effects on progeny, but the ways in which the progeny has sustained physiological effects on the dam have received little attention to date. C1 [Hinde, Katie] Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA. [Carpenter, Abigail J.; Bradford, Barry J.] Kansas State Univ, Dept Anim Sci & Ind, Manhattan, KS 66506 USA. [Clay, John S.] Dairy Records Management Syst, Raleigh, NC USA. [Hinde, Katie] Smithsonian Conservat Biol Inst, Nutr Lab, Washington, DE USA. [Hinde, Katie] Univ Calif Davis, Calif Natl Primate Res Ctr, Brain Mind & Behav Unit, Davis, CA 95616 USA. RP Hinde, K (reprint author), Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA. EM khinde@fas.harvard.edu OI Bradford, Barry/0000-0002-6775-4961; Hinde, Katie/0000-0002-0528-866X FU Kansas Agricultural Experiment Station [13-391-J] FX Contribution no. 13-391-J from the Kansas Agricultural Experiment Station to BJB and AJC supported, in part, the study. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. No additional external funding was received for this study. NR 95 TC 23 Z9 25 U1 2 U2 28 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 3 PY 2014 VL 9 IS 2 AR e86169 DI 10.1371/journal.pone.0086169 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 302TD UT WOS:000330626900016 PM 24498270 ER PT J AU Mandel, JR Dikow, RB Funk, VA Masalia, RR Staton, SE Kozik, A Michelmore, RW Rieseberg, LH Burke, JM AF Mandel, Jennifer R. Dikow, Rebecca B. Funk, Vicki A. Masalia, Rishi R. Staton, S. Evan Kozik, Alex Michelmore, Richard W. Rieseberg, Loren H. Burke, John M. TI A TARGET ENRICHMENT METHOD FOR GATHERING PHYLOGENETIC INFORMATION FROM HUNDREDS OF LOCI: AN EXAMPLE FROM THE COMPOSITAE SO APPLICATIONS IN PLANT SCIENCES LA English DT Article DE base tree; conserved; exon capture; next-generation sequencing; orthologs; phylogenomics ID MULTIPLE SEQUENCE ALIGNMENT; PLANT GENOMES; CAPTURE; ELEMENTS; BIOLOGY; MARKERS AB Premise of the study: The Compositae (Asteraceae) are a large and diverse family of plants, and the most comprehensive phylogeny to date is a meta-tree based on 10 chloroplast loci that has several major unresolved nodes. We describe the development of an approach that enables the rapid sequencing of large numbers of orthologous nuclear loci to facilitate efficient phylogenomic analyses. Methods and Results: We designed a set of sequence capture probes that target conserved orthologous sequences in the Compositae. We also developed a bioinformatic and phylogenetic workflow for processing and analyzing the resulting data. Application of our approach to 15 species from across the Compositae resulted in the production of phylogenetically informative sequence data from 763 loci and the successful reconstruction of known phylogenetic relationships across the family. Conclusions: These methods should be of great use to members of the broader Compositae community, and the general approach should also be of use to researchers studying other families. C1 [Mandel, Jennifer R.] Univ Memphis, Dept Biol Sci, Memphis, TN 38152 USA. [Dikow, Rebecca B.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20560 USA. [Dikow, Rebecca B.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. [Funk, Vicki A.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. [Masalia, Rishi R.; Burke, John M.] Univ Georgia, Dept Plant Biol, Miller Plant Sci, Athens, GA 30602 USA. [Staton, S. Evan] Univ Georgia, Dept Genet, Athens, GA 30602 USA. [Kozik, Alex; Michelmore, Richard W.] Univ Calif Davis, Genome Ctr, Davis, CA 95616 USA. [Rieseberg, Loren H.] Univ British Columbia, Dept Bot, Vancouver, BC V6T 1Z4, Canada. RP Mandel, JR (reprint author), Univ Memphis, Dept Biol Sci, Memphis, TN 38152 USA. EM jmandel@memphis.edu RI Masalia, Rishi/H-4761-2016; Burke, John/A-3502-2013; OI Burke, John/0000-0002-1412-5539; Masalia, Rishi/0000-0003-3661-690X FU Undersecretary for Science, Smithsonian Institution; Genome BC; Genome Canada; National Science Foundation Plant Genome Research Program [DBI-0820451] FX The authors thank Cristin Walters at the University of Georgia Herbarium for assistance in preparing voucher specimens and John Bowers, Savithri Nambeesan, and Katrien Devos for helpful discussion of the project. We also thank Aaron Liston and another anonymous reviewer for comments on a previous version of this manuscript. The authors thank the Undersecretary for Science, Smithsonian Institution, for the Next Generation Sequencing Small Grant to V.A.F. Funding was also provided by Genome BC, Genome Canada, and the National Science Foundation Plant Genome Research Program (DBI-0820451) to J.M.B., R.W.M., and L.H.R. NR 31 TC 27 Z9 29 U1 8 U2 26 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 2168-0450 J9 APPL PLANT SCI JI Appl. Plant Sci. PD FEB PY 2014 VL 2 IS 2 AR 1300085 DI 10.3732/apps.1300085 PG 6 WC Plant Sciences SC Plant Sciences GA AQ1RN UT WOS:000342558800008 ER PT J AU Petersen, JJ Parker, IM Potter, D AF Petersen, Jennifer J. Parker, Ingrid M. Potter, Daniel TI TEN POLYMORPHIC MICROSATELLITE PRIMERS IN THE TROPICAL TREE CAIMITO, CHRYSOPHYLLUM CAINITO (SAPOTACEAE) SO APPLICATIONS IN PLANT SCIENCES LA English DT Article DE caimito; Chrysophyllum cainito; microsatellite; Sapotaceae; tropical tree domestication ID FRUIT AB Premise of the study: We developed microsatellite primers for the tropical tree Chrysophyllum cainito (Sapotaceae) to determine the native range of the species, investigate the origin of cultivated populations, and examine the partitioning of genetic diversity in wild and cultivated populations. Methods and Results: We developed 10 polymorphic primers from C. cainito genomic DNA libraries enriched for di-, tri-, and tetranucleotide repeat motifs. The loci amplified were polymorphic in samples collected from Jamaica and Panama. The number of alleles per locus ranged from two to 10 and three to 12, while observed heterozygosities ranged from 0.074 to 0.704 and 0.407 to 0.852 in Jamaica and Panama, respectively. Conclusions: The microsatellite primers will be useful in future population genetic studies as well as those aimed at understanding the geographic origin(s) of wild and cultivated populations. C1 [Petersen, Jennifer J.; Potter, Daniel] Univ Calif Davis, Dept Plant Sci, Davis, CA 95616 USA. [Parker, Ingrid M.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Parker, Ingrid M.] Smithsonian Trop Res Inst, Balboa, Panama. RP Petersen, JJ (reprint author), Univ Calif Davis, Dept Plant Sci, Mail Stop 3,One Shields Ave, Davis, CA 95616 USA. EM jjpetersen@ucdavis.edu FU University of California, Davis; Henry A. Jastro Research Scholarship; Peter J. Shields Research Scholarship FX The authors thank the Montgomery Botanical Center and Fairchild Tropical Garden for providing leaf material and T. Commack, I. Lopez, H. Membache, and G. Proctor for fieldwork assistance. The authors thank the Smithsonian Tropical Research Institute for logistical support and the Autoridad Nacional del Ambiente (ANAM) and the Autoridad del Canal de Panama (ACP) for granting us permission to conduct research in the Republic of Panama. The authors thank M. Jasieniuk and M. Okada for technical assistance. J.J.P. acknowledges financial support from the University of California, Davis, and Henry A. Jastro and Peter J. Shields Research Scholarships. NR 10 TC 0 Z9 0 U1 1 U2 2 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 2168-0450 J9 APPL PLANT SCI JI Appl. Plant Sci. PD FEB PY 2014 VL 2 IS 2 AR 1300079 DI 10.3732/apps.1300079 PG 3 WC Plant Sciences SC Plant Sciences GA AQ1RN UT WOS:000342558800006 ER PT J AU Peppe, DJ Lemons, CR Royer, DL Wing, SL Wright, IJ Lusk, CH Rhoden, CH AF Peppe, Daniel J. Lemons, Casee R. Royer, Dana L. Wing, Scott L. Wright, Ian J. Lusk, Christopher H. Rhoden, Chazelle H. TI BIOMECHANICAL AND LEAF-CLIMATE RELATIONSHIPS: A COMPARISON OF FERNS AND SEED PLANTS SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE climate; ferns; leaf economic spectrum; leaf mass per area; leaf physiognomy; paleobotany; paleoecology ID ECONOMICS SPECTRUM; TOOTHED LEAVES; TRAITS; SIZE; CONVERGENCE; FORM; ANGIOSPERMS; EVOLUTION; ECOSYSTEMS; ALLOMETRY AB Premise of the study: Relationships of leaf size and shape (physiognomy) with climate have been well characterized for woody non-monocotyledonous angiosperms (dicots), allowing the development of models for estimating paleoclimate from fossil leaves. More recently, petiole width of seed plants has been shown to scale closely with leaf mass. By measuring petiole width and leaf area in fossils, leaf mass per area (M-A) can be estimated and an approximate leaf life span inferred. However, little is known about these relationships in ferns, a clade with a deep fossil record and with the potential to greatly expand the applicability of these proxies. Methods: We measured the petiole width, M-A, and leaf physiognomic characters of 179 fern species from 188 locations across six continents. We applied biomechanical models and assessed the relationship between leaf physiognomy and climate using correlational approaches. Key results: The scaling relationship between area-normalized petiole width and M A differs between fern fronds and pinnae. The scaling relationship is best modeled as an end-loaded cantilevered beam, which is different from the best-fit biomechanical model for seed plants. Fern leaf physiognomy is not influenced by climatic conditions. Conclusions: The cantilever beam model can be applied to fossil ferns. The lack of sensitivity of leaf physiognomy to climate in ferns argues against their use to reconstruct paleoclimate. Differences in climate sensitivity and biomechanical relationships between ferns and seed plants may be driven by differences in their hydraulic conductivity and/or their differing evolutionary histories of vein architecture and leaf morphology. C1 [Peppe, Daniel J.; Lemons, Casee R.] Baylor Univ, Dept Geol, Waco, TX 76798 USA. [Royer, Dana L.; Rhoden, Chazelle H.] Wesleyan Univ, Dept Earth & Environm Sci, Middletown, CT 06459 USA. [Wing, Scott L.] Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Wright, Ian J.] Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. [Lusk, Christopher H.] Univ Waikato, Dept Biol Sci, Hamilton, New Zealand. RP Peppe, DJ (reprint author), Baylor Univ, Dept Geol, Waco, TX 76798 USA. EM daniel_peppe@baylor.edu RI Wright, Ian/G-4979-2012; Peppe, Daniel/E-8449-2011; OI Wright, Ian/0000-0001-8338-9143; Peppe, Daniel/0000-0003-4263-133X; Royer, Dana/0000-0003-0976-953X; Wing, Scott/0000-0002-2954-8905 FU Young Investigator Development Program; Vice Provost for Research at Baylor University; National Science Foundation Asia and Pacific Summer Institute; Australian Academy of Science; Australian Government Department of Innovation, Industry, Science and Research; Smithsonian Minority Awards Program; Baylor University; Macquarie University FX The authors thank the Baylor University Herbarium, the Queensland Herbarium (Department of Environment and Resource Management), the Royal Botanic Gardens and Domain Trust (Office of Environment and Heritage, New South Wales Government), Te Papa Herbarium (Museum of New Zealand, Te Papa Tongarewa), the United States National Herbarium, and the University of Waikato Herbarium for access to material used in this study. D.J.P. acknowledges funding from the Young Investigator Development Program and the Vice Provost for Research at Baylor University, and C.R.L. acknowledges funding from the National Science Foundation Asia and Pacific Summer Institute; Australian Academy of Science; Australian Government Department of Innovation, Industry, Science and Research; the Smithsonian Minority Awards Program; Baylor University; and Macquarie University. NR 42 TC 3 Z9 3 U1 2 U2 27 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 FEB PY 2014 VL 101 IS 2 BP 338 EP 347 DI 10.3732/ajb.1300220 PG 10 WC Plant Sciences SC Plant Sciences GA AN2YJ UT WOS:000340451700011 PM 24509795 ER PT J AU Neufeld, MJ AF Neufeld, Michael J. TI Transforming solar system exploration: The origins of the Discovery Program, 1989-1993 SO SPACE POLICY LA English DT Article DE Space history; NASA; Space programme organization AB The Discovery Program is a rarity in the history of NASA solar system exploration: a reform program that has survived and continued to be influential. This article examines its emergence between 1989 and 1993, largely as the result of the intervention of two people: Stamatios "Tom" Krimigis of the Johns Hopkins University Applied Physics Laboratory (APL), and Wesley Huntress of NASA, who was Division Director of Solar System Exploration 1990-92 and the Associate Administrator for Space Science 1992-98. Krimigis drew on his leadership experience in the space physics community and his knowledge of its Explorer program to propose that it was possible to create new missions to the inner solar system for a fraction of the existing costs. He continued to push that idea for the next two years, but it took the influence of Huntress at NASA Headquarters to push it on to the agenda. Huntress explicitly decided to use APL to force change on the Jet Propulsion Laboratory and the planetary science community. He succeeded in moving the JPL Mars Pathfinder and APL Near Earth Asteroid Rendezvous (NEAR) mission proposals forward as the opening missions for Discovery. But it took Krimigis's political skill and access to Sen. Barbara Mikulski in 1993 to get the NEAR into the NASA budget, thereby likely ensuring that Discovery would not become another one-mission program. (C) 2014 Smithsonian Institution. Published by Elsevier Ltd. All rights reserved. C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. EM neufeldm@si.edu NR 37 TC 1 Z9 1 U1 0 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-9646 EI 1879-338X J9 SPACE POLICY JI Space Policy PD FEB PY 2014 VL 30 IS 1 BP 5 EP 12 DI 10.1016/j.spacepol.2013.10.002 PG 8 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA AL5CH UT WOS:000339150600002 ER PT J AU Ness, JU Parmar, AN Valencic, LA Smith, R Loiseau, N Salama, A Ehle, M Schartel, N AF Ness, J. -U. Parmar, A. N. Valencic, L. A. Smith, R. Loiseau, N. Salama, A. Ehle, M. Schartel, N. TI XMM-Newton publication statistics SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE publications, bibliography; space vehicles; telescopes ID PHOTON IMAGING CAMERA; CATALOG AB We assessed the scientific productivity of XMM-Newton by examining XMM-Newton publications and data usage statistics. We analyse 3272 refereed papers, published until the end of 2012, that directly use XMM-Newton data. The SAO/NASA Astrophysics Data System (ADS) was used to provide additional information on each paper including the number of citations. For each paper, the XMM-Newton observation identifiers and instruments used to provide the scientific results were determined. The identifiers were used to access the XMM-Newton Science Archive (XSA) to provide detailed information on the observations themselves and on the original proposals. The information obtained from these sources was then combined to allow the scientific productivity of the mission to be assessed. Since around three years after the launch of XMM-Newton there have been around 300 refereed papers per year that directly use XMM-Newton data. After more than 13 years in operation, this rate shows no evidence that it is decreasing. Since 2002, around 100 scientists per year become lead authors for the first time on a refereed paper which directly uses XMM-Newton data. Each refereed XMM-Newton paper receives around four citations per year in the first few years with a long-term citation rate of three citations per year, more than five years after publication. About half of the articles citing XMM-Newton articles are not primarily X-ray observational papers. The distribution of elapsed time between observations taken under the Guest Observer programme and first article peaks at 2 years with a possible second peak at 3.25 years. Observations taken under the Target of Opportunity programme are published significantly faster, after one year on average. The fraction of science time taken until the end of 2009 that has been used in at least one article is similar to 90%. Most observations were used more than once, yielding on average a factor of two in usage on available observing time per year. About 20% of all slew observations have been used in publications. The scientific productivity of XMM-Newton measured by the publication rate, number of new authors and citation rate, remains extremely high with no evidence that it is decreasing after more than 13 years of operations. (C) 2014 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Ness, J. -U.; Loiseau, N.; Salama, A.; Ehle, M.] ESAC, Sci Operat Dept ESA, XMM Newton Sci Operat Ctr, Villanueva De La Canada 28691, Madrid, Spain. [Parmar, A. N.] Estec, Directorate Sci & Robot Explorat, Sci Support Off, NL-2200 AG Noordwijk, Netherlands. [Valencic, L. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Valencic, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smith, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schartel, N.] ESAC, Res & Sci Support Dept ESA, Astrophys & Fundamental Phys Missions Div, Villanueva De La Canada 28691, Madrid, Spain. RP Ness, JU (reprint author), ESAC, Sci Operat Dept ESA, XMM Newton Sci Operat Ctr, Villanueva De La Canada 28691, Madrid, Spain. EM juness@sciops.esa.int OI Parmar, Arvind/0000-0002-3307-6517 NR 12 TC 0 Z9 0 U1 1 U2 4 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2014 VL 335 IS 2 BP 210 EP 220 DI 10.1002/asna.201312001 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI1DM UT WOS:000336590200012 ER PT J AU Campbell, BA Ray Hawke, B Morgan, GA Carter, LM Campbell, DB Nolan, M AF Campbell, Bruce A. Ray Hawke, B. Morgan, Gareth A. Carter, Lynn M. Campbell, Donald B. Nolan, Michael TI Improved discrimination of volcanic complexes, tectonic features, and regolith properties in Mare Serenitatis from Earth-based radar mapping SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Moon; volcanism; regolith; radar ID OCEANUS PROCELLARUM; ARISTARCHUS PLATEAU; WAVELENGTH RADAR; 70-CM WAVELENGTH; LUNAR NEARSIDE; MOON; THICKNESS; STRATIGRAPHY; CONSTRAINTS; DEPOSITS AB Radar images at 70 cm wavelength show 4-5dB variations in backscatter strength within regions of relatively uniform spectral reflectance properties in central and northern Mare Serenitatis, delineating features suggesting lava flow margins, channels, and superposition relationships. These backscatter differences are much less pronounced at 12.6 cm wavelength, consistent with a large component of the 70 cm echo arising from the rough or blocky transition zone between the mare regolith and the intact bedrock. Such deep probing is possible because the ilmenite content, which modulates microwave losses, of central Mare Serenitatis is generally low (2-3% by weight). Modeling of the radar returns from a buried interface shows that an average regolith thickness of 10m could lead to the observed shifts in 70 cm echo power with a change in TiO2 content from 2% to 3%. This thickness is consistent with estimates of regolith depth (10-15m) based on the smallest diameter for which fresh craters have obvious blocky ejecta. The 70 cm backscatter differences provide a view of mare flow-unit boundaries, channels, and lobes unseen by other remote sensing methods. A localized pyroclastic deposit associated with Rima Calippus is identified based on its low radar echo strength. Radar mapping also improves delineation of units for crater age dating and highlights a 250 km long, east-west trending feature in northern Mare Serenitatis that we suggest is a large graben flooded by late-stage mare flows. C1 [Campbell, Bruce A.; Morgan, Gareth A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Ray Hawke, B.] Univ Hawaii Manoa, HIGP SOEST, Honolulu, HI 96822 USA. [Carter, Lynn M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Campbell, Donald B.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Nolan, Michael] Natl Astron & Ionosphere Ctr, Arecibo Observ, Arecibo, PR 00613 USA. RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM campbellb@si.edu RI Carter, Lynn/D-2937-2012; OI Nolan, Michael/0000-0001-8316-0680 FU NASA's Planetary Astronomy and Planetary Geology and Geophysics Programs; National Science Foundation [AST-1100968]; National Aeronautics and Space Administration [NNX12AF24G] FX The authors thank J. Cahill and an anonymous reviewer for their thoughtful comments on the manuscript. This work was supported in part by grants from NASA's Planetary Astronomy and Planetary Geology and Geophysics Programs. The authors thank the staff at Arecibo Observatory and the Green Bank Telescope for invaluable assistance in collecting the lunar radar data. John Chandler of the Smithsonian Astrophysical Observatory provided the lunar ephemerides for our mapping. Mark Cintala offered helpful comments during our consideration of models for regolith structure. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), and in alliance with Ana G. Mendez-Universidad Metropolitana, and the Universities Space Research Association. The Arecibo Planetary Radar Program is supported by the National Aeronautics and Space Administration under grant NNX12AF24G issued through the Near Earth Object Observations program. The Green Bank Telescope is part of the National Radio Astronomy Observatory, a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. NR 53 TC 8 Z9 8 U1 1 U2 8 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 FEB PY 2014 VL 119 IS 2 BP 313 EP 330 DI 10.1002/2013JE004486 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AH6EZ UT WOS:000336224800001 ER PT J AU Loss, SR Wil, T Loss, SS Marra, PP AF Loss, Scott R. Wil, Tom Loss, Sara S. Marra, Peter P. TI Bird-building collisions in the United States: Estimates of annual mortality and species vulnerability SO CONDOR LA English DT Article DE anthropogenic mortality; Birds of Conservation Concern; individual residence; low-rise; high-rise; systematic review; window collision ID WINDOW COLLISIONS; AVIAN MORTALITY; CANADA; PERSISTENCE; LANDSCAPE; IMPACT; GLASS; RISK AB Building collisions, and particularly collisions with windows, are a major anthropogenic threat to birds, with rough estimates of between 100 million and 1 billion birds killed annually in the United States. However, no current U.S. estimates are based on systematic analysis of multiple data sources. We reviewed the published literature and acquired unpublished datasets to systematically quantify bird building collision mortality and species-specific vulnerability. Based on 23 studies, we estimate that between 365 and 988 million birds (median = 599 million) are killed annually by building collisions in the U.S., with roughly 56% of mortality at low-rises, 44% at residences, and <1% at high-rises. Based on >92,000 fatality records, and after controlling for population abundance and range overlap with study sites, we identified several species that are disproportionately vulnerable to collisions at all building types. In addition, several species listed as national Birds of Conservation Concern due to their declining populations were identified to be highly vulnerable to building collisions, including Golden-winged Warbler (Vermivora chrysoptera), Painted Bunting (Passerina ciris), Canada Warbler (Cardellina canadensis), Wood Thrush (Hylocichla mustelina), Kentucky Warbler (Geothlypis formosa), and Worm-eating Warbler (Helmitheros vermivorum). The identification of these five migratory species with geographic ranges limited to eastern and central North America reflects seasonal and regional biases in the currently available building-collision data. Most sampling has occurred during migration and in the eastern U.S. Further research across seasons and in underrepresented regions is needed to reduce this bias. Nonetheless, we provide quantitative evidence to support the conclusion that building collisions are second only to feral and free-ranging pet cats, which are estimated to kill roughly four times as many birds each year, as the largest source of direct human-caused mortality for U.S. birds. C1 [Loss, Scott R.; Loss, Sara S.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC USA. [Wil, Tom] US Fish & Wildlife Serv, Div Migratory Birds, Midwest Reg Off, Bloomington, MN USA. RP Loss, SR (reprint author), Oklahoma State Univ, Dept Nat Resource Ecol & Management, Stillwater, OK 74078 USA. EM scott.loss@okstate.edu FU U.S. Fish and Wildlife Service through the Smithsonian Institution's Postdoctoral Fellowship program FX We thank the following people and organizations for providing access to unpublished datasets from building collision monitoring programs: K. Brand (Lights Out Winston-Salem, Forsyth County Audubon Society & Audubon North Carolina), A. Conover (Lights Out Columbus, Ohio Bird Conservation Initiative & Grange Insurance Audubon Center), M. Coolidge (Bird Safe Portland, Audubon Society of Portland), S. Diehl and C. Sharlow-Schaefer (Wisconsin Night Guardians, Wisconsin Humane Society), J. Eckles, K. Nichols, and R. Zink (Project Bird Safe Minnesota, Audubon Minnesota & University of Minnesota), S. Elbin and A. Palmer (Project Safe Flight, New York City Audubon), M. Flannery (California Academy of Sciences), D. Gorney (Lights Out Indy, Amos W. Butler Audubon Society), A. Lewis and L. Fuisz (Lights Out DC, City Wildlife), M. Mesure (Toronto Fatal Light Awareness Program), W. Olson (Lights Out Baltimore, Baltimore Bird Club), A. Prince (Chicago Bird Collision Monitors, Chicago Audubon Society), K. Russell (Audubon Pennsylvania), and D. Willard (The Field Museum). A. Bracey, J. Ducey, M. Etterson, S. Hager, A. Harrington, D. Horn, G. Niemi, and T. O'Connell provided access to unpublished or otherwise unavailable data. R. Schneider and J. Rutter provided assistance with data collection and management; E. Bayne, C. Machtans, and C. Wedeles provided access to unpublished manuscripts; and M. Lynes and C. Sheppard assisted in locating datasets. We give special thanks to D. Klem for providing access to nearly all of his window collision data, investing significant effort along with P. Saenger to digitize historical records, and for pioneering the study of bird-window collisions. S.R.L. was supported by a postdoctoral fellowship funded by the U.S. Fish and Wildlife Service through the Smithsonian Institution's Postdoctoral Fellowship program. The findings and opinions expressed in this paper are those of the authors and do not necessarily reflect the opinions of the U.S. Fish and Wildlife Service or the Smithsonian Institution. NR 60 TC 49 Z9 51 U1 16 U2 99 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 EI 1938-5129 J9 CONDOR JI Condor PD FEB PY 2014 VL 116 IS 1 BP 8 EP 23 DI 10.1650/CONDOR-13-090.1 PG 16 WC Ornithology SC Zoology GA AG7PW UT WOS:000335611300003 ER PT J AU Fernandez, L Sanabria, EA Quiroga, LB Vari, RP AF Fernandez, L. Sanabria, E. A. Quiroga, L. B. Vari, R. P. TI A new species of Silvinichthys (Siluriformes, Trichomycteridae) lacking pelvic fins from mid-elevation localities of the southern Andes, with comments on the genus SO JOURNAL OF FISH BIOLOGY LA English DT Article DE Andean Cordillera; Argentina; catfish; neotropic; southern South America; Trichomycterinae ID ARGENTINA; CATFISH; TELEOSTEI; GIRDLE AB Silvinichthys huachi new species, is described from a stream along the lower slope of the Andean Cordillera in the Provincia de San Juan, Argentina. It shares the distinctive modifications characteristic of Silvinichthys, but is distinguished from the four previously described congeners by the combination of a lack of the pelvic fin and the pelvic girdle, details of pigmentation and various meristic and morphometric features. Silvinichthys huachi is apparently endemic to the type locality situated within an arid region of western central Argentina in the Andino Cuyana Province. Major gaps in the range of species of Silvinichthys may indicate that the origin of the genus predates the uplift events that subdivided drainages along the eastern slopes of the Andean Cordillera in west central Argentina. Silvinichthys huachi is hypothesized to be the sister species of Silvinichthys bortayro. (C) 2014 The Fisheries Society of the British Isles C1 [Fernandez, L.] Consejo Nacl Invest Cient & Tecn, Inst Miguel Lillo, RA-4000 San Miguel De Tucuman, Argentina. [Fernandez, L.] Univ Nacl Catamarca, Fac Ciencias Exactas & Nat, Catamarca, Argentina. [Sanabria, E. A.] Univ Nacl Cuyo, Inst Histol & Embriol Mendoza, Lab Invest Androl Mendoza,CONICET, Ctr Invest Ciencia & Tecn Mendoza,Fac Ciencias Me, RA-5500 Mendoza, Argentina. [Quiroga, L. B.] Univ Nacl San Juan, Dept Biol, Rivadavia, San Juan, Argentina. [Vari, R. P.] Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, Washington, DC 20013 USA. RP Fernandez, L (reprint author), Consejo Nacl Invest Cient & Tecn, Inst Miguel Lillo, Miguel Lillo 251, RA-4000 San Miguel De Tucuman, Argentina. EM luis1813@yahoo.com FU CIUNSA (Consejo Investigaciones de la Universidad Nacional Salta) [1663]; PIP (Projecto Investigacion Plurianual, CONICET) [11420090100321]; Programa Raices [404/08 106/09] FX Research associated with this project was supported by CIUNSA (Consejo Investigaciones de la Universidad Nacional Salta) Project no. 1663, PIP (Projecto Investigacion Plurianual, CONICET) Project no. 11420090100321 and Programa Raices no. 404/08 106/09. For the loan of specimens and various forms of other assistance, we thank S. Schaefer, B. Brown and R. Arrindell (AMNH), M. Sabaj Perez (ANSP), D. Catania (CAS), J. Maclaine (BMNH), M. Retzer (INHS), R. Robins (UF), M. Rogers (FMNH), A. Bentley (KU), G. Chiaramonte (MACN), K. Hartel (MCZ), J. Lima de Figueiredo and O. Oyakawa (MZUSP), L. Malabarba and R. Reis (PUCRS), H. Lopez (MLP), F. Carvajal, M. Arraya and M. Maldonado (UMSS), P. Buckup (MNRJ), H. Ortega and M. Velasquez (MUSM), V. Jerez (MZUC) and D. Nelson (UMMZ). V. Marinero and R. Cortez provided assistance with the field work and J. Andreoli (UNCa), G. Gonzo, F. Lobo, V. Martinez and S. Valdecantos (MCN-IBIGEO) graciously provided hospitality. NR 24 TC 2 Z9 2 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1112 EI 1095-8649 J9 J FISH BIOL JI J. Fish Biol. PD FEB PY 2014 VL 84 IS 2 BP 372 EP 382 DI 10.1111/jfb.12291 PG 11 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA AH4FQ UT WOS:000336083200007 PM 24422902 ER PT J AU Baeza, JA Behringer, DC Hart, RJ Dickson, MD Anderson, JR AF Antonio Baeza, J. Behringer, Donald C. Hart, Rebecca J. Dickson, Michael D. Anderson, Joshua R. TI Reproductive biology of the marine ornamental shrimp Lysmata boggessi in the south- eastern Gulf of Mexico SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article DE sex-ratio; density; size at first maturity; aquarium trade; hermaphrodite ID PROTANDRIC SIMULTANEOUS HERMAPHRODITISM; WURDEMANNI CARIDEA; SEX ALLOCATION; HIPPOLYTIDAE; TRADE; CRUSTACEA; EVOLUTION; DECAPODA; RATIO; GENUS AB Reproductive aspects of the intensively traded ornamental shrimp Lysmata boggessi were examined. Abundance, reproductive biology (fecundity, reproductive output and egg size) and population structure (frequency distribution, size at sex phase change and sex phase ratio) were examined at three different fishing grounds off south and west-central Florida between May 2011 and February 2012. Fishery-dependent densities of L. boggessi varied between 2.51 +/- 1.39 and 13.05 +/- 9.30 shrimps per 1000m(2) at two different localities. The proportion of brooding shrimp varied considerably at one locality during two different dates, suggesting reproductive seasonality. Reproductive output increased linearly with shrimp body weight (SBW) at one locality (May 2011), but scaled negatively with SBW at a second locality (January-February 2012). Lastly, no correlation between embryo size and shrimp carapace length (CL) was recorded at one locality (May 2011), but a slight negative correlation between embryo size and CL was found at the second locality (January-February 2012). Lysmata boggessi might be experiencing trade-offs between different reproductive parameters driven by environmental, probably seasonal, conditions during the year. All of this information needs to be considered in assessing shrimp stocks and establishing a sustainable management plan. C1 [Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Antonio Baeza, J.] Univ Catolica Norte, Coquimbo, Chile. [Behringer, Donald C.; Hart, Rebecca J.; Dickson, Michael D.; Anderson, Joshua R.] Univ Florida, Sch Forest Resources & Conservat, Fisheries & Aquat Sci Program, Gainesville, FL 32653 USA. [Behringer, Donald C.] Univ Florida, Emerging Pathogens Inst, Gainesville, FL 32611 USA. RP Baeza, JA (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM baeza.antonio@gmail.com OI Baeza, Juan Antonio/0000-0002-2573-6773 FU Florida Fish and Wildlife Conservation Commission [103232]; Old Dominion University FX This project was funded by the Florida Fish and Wildlife Conservation Commission contract 103232 to D. C. B. and J.A.B. J.A.B. was supported by a postdoctoral fellowship from Old Dominion University during the present study. NR 30 TC 2 Z9 2 U1 1 U2 10 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0025-3154 EI 1469-7769 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD FEB PY 2014 VL 94 IS 1 BP 141 EP 149 DI 10.1017/S0025315413001185 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AC3WO UT WOS:000332452300014 ER PT J AU Zimmermann, B Zimmermann, A Turner, BL Francke, T Elsenbeer, H AF Zimmermann, Beate Zimmermann, Alexander Turner, Benjamin L. Francke, Till Elsenbeer, Helmut TI Connectivity of overland flow by drainage network expansion in a rain forest catchment SO WATER RESOURCES RESEARCH LA English DT Article DE connectivity; overland flow; stormflow; suspended sediment; phosphorus; drainage network expansion ID BARRO-COLORADO ISLAND; QUANTILE REGRESSION FORESTS; SUSPENDED-SEDIMENT DYNAMICS; RUNOFF GENERATION; HYDROLOGICAL CONNECTIVITY; GEOMORPHIC SYSTEMS; LEAF-LITTER; PANAMA; EROSION; AREAS AB Soils in various places of the Panama Canal Watershed feature a low saturated hydraulic conductivity (K-s) at shallow depth, which promotes overland-flow generation and associated flashy catchment responses. In undisturbed forests of these areas, overland flow is concentrated in flow lines that extend the channel network and provide hydrological connectivity between hillslopes and streams. To understand the dynamics of overland-flow connectivity, as well as the impact of connectivity on catchment response, we studied an undisturbed headwater catchment by monitoring overland-flow occurrence in all flow lines and discharge, suspended sediment, and total phosphorus at the catchment outlet. We find that connectivity is strongly influenced by seasonal variation in antecedent wetness and can develop even under light rainfall conditions. Connectivity increased rapidly as rainfall frequency increased, eventually leading to full connectivity and surficial drainage of entire hillslopes. Connectivity was nonlinearly related to catchment response. However, additional information on factors such as overland-flow volume would be required to constrain relationships between connectivity, stormflow, and the export of suspended sediment and phosphorus. The effort to monitor those factors would be substantial, so we advocate applying the established links between rain event characteristics, drainage network expansion by flow lines, and catchment response for predictive modeling and catchment classification in forests of the Panama Canal Watershed and in similar regions elsewhere. Key Points Overland-flow connectivity occurs along an ephemeral drainage network Connectivity is nonlinearly related to catchment response The connectivity concept could be used for catchment classification C1 [Zimmermann, Beate; Zimmermann, Alexander; Francke, Till; Elsenbeer, Helmut] Univ Potsdam, Inst Earth & Environm Sci, Potsdam, Germany. [Turner, Benjamin L.; Elsenbeer, Helmut] Smithsonian Trop Res Inst, Panama City, Panama. RP Zimmermann, B (reprint author), Res Inst Post Min Landscapes, Finsterwalde, Germany. EM b.zimmermann@fib-ev.de RI Turner, Benjamin/E-5940-2011; Zimmermann, Alexander/B-6831-2011 OI Turner, Benjamin/0000-0002-6585-0722; FU German Research Foundation [El 255/6-1] FX This research was partially funded by the German Research Foundation (El 255/6-1). H. E. acknowledges support by the Smithsonian Tropical Research Institute during his sabbatical in 2008. We thank Anna Schurkmann for participating in the field work, Tania Romero for analytical support, Oris Acevedo (Smithsonian Tropical Research Institute, STRI) for logistical support, and Sergio dos Santos (Environmental Sciences Program, STRI) for providing the rainfall data. We are also grateful to four anonymous reviewers whose comments inspired us to rethink our data and the way of presenting them, which helped to improve the draft considerably. NR 64 TC 11 Z9 11 U1 8 U2 54 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD FEB PY 2014 VL 50 IS 2 BP 1457 EP 1473 DI 10.1002/2012WR012660 PG 17 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA AD9DC UT WOS:000333563900040 ER PT J AU Bruner, G Wcislo, WT Fernandez-Marin, H AF Bruner, G. Wcislo, W. T. Fernandez-Marin, H. TI Prudent inquilines and proactive hosts: behavioral dynamics between an ant social parasite, Megalomyrmex symmetochus and its fungus-growing ant host, Sericomyrmex amabilis SO INSECTES SOCIAUX LA English DT Article DE Amelioration; Coevolution; Symbiosis; Xenobiosis; Social parasitism ID LEAF-CUTTING ANTS; HYMENOPTERA-FORMICIDAE; DISEASE RESISTANCE; EVOLUTION; INFECTIONS; VIRULENCE; FITNESS; MANAGEMENT; BIOLOGY; BENEFIT AB Ant social parasites evolve adaptive relationships with their hosts. Theoretically, coevolution predicts strong selection to maximize fitness of the parasite that minimizes costs to its host, which potentially leads to the evolution of benign interactions. We studied the demographic and behavioral traits of the ant social parasite Megalomyrmex symmetochus (Solenopsidini), an agro-predator that feeds on larvae and fungal garden products of their host, Sericomyrmex amabilis (Attini). Based on demographic data from 15 parasitized colonies, the proportion of parasitic workers to those of the host is 1:2. Moreover, defensive prophylactic behaviors observed during infections with Metarhizium brunneum, a generalist entomopathogen, and Escovopsis, a specialized fungal garden parasite, showed that S. amabilis works extensively to remove and control fungal infections, in contrast to M. symmetochus. M. symmetochus, however, performed intraspecific allogrooming during infections with Escovopsis and M. brunneum, suggesting that they may recognize fungal pathogens and indirectly limit dispersion of spores. Our results indicate that M. symmetochus did not have a strong role in maintaining a hygienic nest. C1 [Bruner, G.; Wcislo, W. T.; Fernandez-Marin, H.] Smithsonian Trop Res Inst, Panama City, Panama. [Fernandez-Marin, H.] Inst Invest Cient, Panama City, Panama. [Fernandez-Marin, H.] Serv Alta Tecnol, Panama City, Panama. RP Fernandez-Marin, H (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama. EM hermogenes_f@hotmail.com FU Re-insertion grant from SENACYT; Tupper Postdoctoral Fellowships from STRI; International Collaboration Program at SENACYT [09-038]; STRI FX We thank the Autoridad Nacional del Ambiente for research and export permits, and STRI staff for logistic support. This work was supported by Re-insertion grant from SENACYT and Tupper Postdoctoral Fellowships from STRI (to HF-M), grants from International Collaboration Program at SENACYT to WTW and HFM (09-038), and general research funds from STRI (to WTW). NR 39 TC 2 Z9 2 U1 2 U2 30 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 EI 1420-9098 J9 INSECT SOC JI Insect. Soc. PD FEB PY 2014 VL 61 IS 1 BP 83 EP 88 DI 10.1007/s00040-013-0331-5 PG 6 WC Entomology SC Entomology GA AF1ZR UT WOS:000334512900009 ER PT J AU Edwards-Ingram, Y AF Edwards-Ingram, Ywone TI Before 1979: African American Coachmen, Visibility, and Representation at Colonial Williamsburg SO PUBLIC HISTORIAN LA English DT Article DE Coachmen; African American history; slavery; visibility; and representation AB Before the living history museum of Colonial Williamsburg started its concerted interpretation of slavery in 1979, the African American coachmen were already representing the past and implicating black history and slavery in this restored eighteenth-century capital of Virginia. Various records of photographs, postcards, letters, newspaper clippings, oral history accounts, visitor observations, and corporate papers provide a window to understand the social climates of the museum's period in the 1930s to the 1970s. This body of evidence supports the contention that the coachmen were visible and influenced public history within and outside the museum. C1 [Edwards-Ingram, Ywone] Colonial Williamsburg Fdn, Williamsburg, VA 23187 USA. [Edwards-Ingram, Ywone] Charles H Wright Museum African Amer Hist, Detroit, MI USA. [Edwards-Ingram, Ywone] Smithsonian Inst, Washington, DC 20560 USA. RP Edwards-Ingram, Y (reprint author), Colonial Williamsburg Fdn, Williamsburg, VA 23187 USA. NR 94 TC 0 Z9 0 U1 0 U2 1 PU UNIV CALIFORNIA PRESS PI OAKLAND PA 155 GRAND AVE, SUITE 400, OAKLAND, CA 94612-3758 USA SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD FEB PY 2014 VL 36 IS 1 BP 9 EP 35 DI 10.1525/tph.2014.36.1.9 PG 27 WC History SC History GA AD5VB UT WOS:000333320200002 PM 24988785 ER PT J AU Gingerich, O AF Gingerich, Owen TI Kepler's Astrology 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 1 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 EI 1753-8556 J9 J HIST ASTRON JI J. Hist. Astron. PD FEB PY 2014 VL 45 BP 137 EP 138 PN 1 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA AE2HJ UT WOS:000333793600015 ER PT J AU Gingerich, O AF Gingerich, Owen TI Kepler's Cosmological Synthesis: Astrology, Mechanism and the Soul 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 2 U2 2 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 EI 1753-8556 J9 J HIST ASTRON JI J. Hist. Astron. PD FEB PY 2014 VL 45 BP 137 EP 138 PN 1 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA AE2HJ UT WOS:000333793600014 ER PT J AU Gingerich, O AF Gingerich, Owen TI Johannes Kepler Collected Works XII 2.2. Astrology Manuscript, Pneumatic Manuscript 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 1 U2 2 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 EI 1753-8556 J9 J HIST ASTRON JI J. Hist. Astron. PD FEB PY 2014 VL 45 BP 137 EP 138 PN 1 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA AE2HJ UT WOS:000333793600016 ER PT J AU Frankham, R Lacy, RC Ballou, JD Dudash, MR Eldridge, MDB Fenster, CB Mendelson, JR Porton, IJ Ralls, K Ryder, OA AF Frankham, Richard Lacy, Robert C. Ballou, Jonathan D. Dudash, Michele R. Eldridge, Mark D. B. Fenster, Charles B. Mendelson, Joseph R., III Porton, Ingrid J. Ralls, Katherine Ryder, Oliver A. TI Species concepts for conservation - Reply to Russello and Amato SO BIOLOGICAL CONSERVATION LA English DT Letter C1 [Frankham, Richard] Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. [Frankham, Richard; Eldridge, Mark D. B.] Australian Museum, Australian Museum Res Inst, Sydney, NSW 2010, Australia. [Lacy, Robert C.] Chicago Zool Soc, Brookfield, IL 60513 USA. [Ballou, Jonathan D.; Ralls, Katherine] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Dudash, Michele R.; Fenster, Charles B.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Mendelson, Joseph R., III] Zoo Atlanta, Se Atlanta, GA 30315 USA. [Mendelson, Joseph R., III] Georgia Inst Technol, Sch Biol, Atlanta, GA 30332 USA. [Porton, Ingrid J.] St Louis Zoo, St Louis, MO 63110 USA. [Ryder, Oliver A.] San Diego Zoo Inst Conservat Res, Escondido, CA 92027 USA. RP Frankham, R (reprint author), Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. EM richard.frankham@mq.ed.au NR 3 TC 1 Z9 1 U1 1 U2 22 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 FEB PY 2014 VL 170 BP 334 EP 335 DI 10.1016/j.biocon.2013.12.039 PG 2 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AE2AA UT WOS:000333774500040 ER PT J AU DeVorkin, D AF DeVorkin, David TI Encyclopedia of the History of Astronomy and Astrophysics SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 [DeVorkin, David] Smithsonian Natl Air & Space Museum, Washington, DC USA. RP DeVorkin, D (reprint author), Smithsonian Natl Air & Space Museum, Washington, DC USA. EM DeVorkinD@si.edu NR 1 TC 0 Z9 0 U1 2 U2 2 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 EI 1753-8556 J9 J HIST ASTRON JI J. Hist. Astron. PD FEB PY 2014 VL 45 BP 130 EP 131 PN 1 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA AE2HJ UT WOS:000333793600009 ER PT J AU Cerrigone, L Umana, G Buemi, CS Hora, JL Trigilio, C Leto, P Hart, A AF Cerrigone, L. Umana, G. Buemi, C. S. Hora, J. L. Trigilio, C. Leto, P. Hart, A. TI Spitzer observations of a circumstellar nebula around the candidate luminous blue variable MWC 930 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE circtunstellar matter; stars: mass-loss; stars: winds, outflows; stars: individual: MWC 930; infrared: stars ID LOW-RESOLUTION SPECTROSCOPY; POST-AGB CANDIDATES; SPACE-TELESCOPE; INFRARED SPECTROGRAPH; INTERSTELLAR; STARS; EMISSION; MISSION; DUST; REGIONS AB Context. The source :MWC 930 is a star just similar to 2 degrees above the Galactic plane whose nature is not clear and has not been studied in detail so far. While a post-asymptotic giant branch classification was proposed in the past, studies of its optical spectrum and photometry pointed toward strong variability, therefore, the object was reclassified as a luminous blue variable (LBV) candidate. Aims. The LBVs typically undergo phases of strong mass loss in the form of eruptions that can create shells of ejecta around the star. Our goal is to search for the presence of such a circumstellar nebula in MWC 930 and investigate its properties. Methods. To do so, we make use of space-based infrared data from our Spitzer campaign performed with the InfraRed Array Camera (RAC) and the Infra:Red Spectrograph (IRS), as well as data from optical and infrared (IR) surveys. Results. In our Spitzer images, we clearly detect an extended shell around MWC 930 at wavelengths longer than 5 mu m. The mid-infrared spectrum is dominated by the central star and mostly shows forbidden lines of [FeII] with an underlying continuum that decreases with wavelengths up to similar to 15 mu m and then inverts its slope, displaying a second peak around 60 mu m, which is evidence of cold dust grains formed in a past eruption. By modeling the spectral energy distribution, we identify two central components, beside the star and the outer shell. These extra sources of radiation are interpreted as material close to the central star, which may be due to a recent ejection. Features of C-bearing molecules or grains are not detected. C1 [Cerrigone, L.] CSIC, INTA, Ctr Astrobiol, Torrejon De Ardoz 28850, Spain. [Umana, G.; Buemi, C. S.; Trigilio, C.; Leto, P.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Hora, J. L.; Hart, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cerrigone, L (reprint author), CSIC, INTA, Ctr Astrobiol, Torrejon De Ardoz 28850, Spain. EM cerrigone@cab.inta-csic.es OI Buemi, Carla Simona/0000-0002-7288-4613; Hora, Joseph/0000-0002-5599-4650; Umana, Grazia/0000-0002-6972-8388; Leto, Paolo/0000-0003-4864-2806 FU Spanish Consejo Superior de Investigaciones Cientificas; European Social Fund; Spanish MICINN [AYA2009-07304, CSD2009-00038]; NASA; National Aeronautics and Space Administration FX L.C. acknowledges funding from the Spanish Consejo Superior de Investigaciones Cientificas through a JAE-Doc research contract co-funded by the European Social Fund. L.C. thanks the Spanish MICINN for funding support through grants AYA2009-07304 and CSD2009-00038. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This 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 is based on observations with AKARI, a JAXA project with the participation of ESA. NR 34 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 FEB PY 2014 VL 562 AR A93 DI 10.1051/0004-6361/201323099 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800144 ER PT J AU Collaboration, HESS Abramowski, A Aharonian, F Benkhali, FA Akhperjanian, AG Anguner, E Anton, G Balenderan, S Balzer, A Barnacka, A Becherini, Y Tjus, JB Bernlohr, K Birsin, E Bissaldi, E Biteau, J Bottcher, M 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 Cui, Y Dalton, M Daniel, MK Davids, ID Degrange, B Deil, C de Wilt, P Dickinson, HJ Djannati-Ataii, 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 Giavitto, G Giebels, B Glicenstein, JF Grondin, MH Grudzinska, M Haffner, S 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 Lemiere, A Lemoine-Goumard, M Lenain, JP Lennarz, D Lohse, T Lopatin, A Lu, CC Marandon, V Marcowith, A Marx, R Maurin, G Maxted, N Mayer, M McComb, TJL Mehault, J Meintjes, PJ Menzler, U Meyer, M Moderski, R Mohamed, M Moulin, E Murach, T Naumann, CL de Naurois, M 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 Romoli, C 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 Spies, F Stawarz, L Steenkamp, R Stegmann, C Stinzing, F Stycz, K Sushch, I Szostek, A Tavernet, JP Tavernier, T Taylor, AM Terrier, R Tluczykont, M Trichard, C Valerius, K van Eldik, C van Soelen, B Vasileiadis, G Venter, C Viana, A Vincent, P Volk, HJ Volpe, F Vorster, M Vuillaume, T Wagner, SJ Wagner, P Ward, M Weidinger, M Weitzel, Q White, R Wierzcholska, A Willmann, P Wornlein, A Wouters, D Zabalza, V Zacharias, M Zajczyk, A Zdziarski, AA Zech, A Zechlin, HS AF Collaboration, H. E. S. S. Abramowski, A. Aharonian, F. Benkhali, F. Ait 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. Boettcher, M. 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. Cui, Y. Dalton, M. Daniel, M. K. Davids, I. D. Degrange, B. Deil, C. de Wilt, 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. Giavitto, G. Giebels, B. Glicenstein, J. F. Grondin, M. -H. Grudzinska, M. Haeffner, S. 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. Lemiere, A. Lemoine-Goumard, M. Lenain, J. -P. Lennarz, D. Lohse, T. Lopatin, A. Lu, C. -C. Marandon, V. Marcowith, A. Marx, R. Maurin, G. Maxted, N. Mayer, M. McComb, T. J. L. Mehault, J. Meintjes, P. J. Menzler, U. Meyer, M. Moderski, R. Mohamed, M. Moulin, E. Murach, T. Naumann, C. L. de Naurois, M. 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. Romoli, C. 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. Spies, F. Stawarz, L. Steenkamp, R. Stegmann, C. Stinzing, F. Stycz, K. Sushch, I. Szostek, A. Tavernet, J. -P. Tavernier, T. Taylor, A. M. Terrier, R. Tluczykont, M. Trichard, C. Valerius, K. van Eldik, C. van Soelen, B. Vasileiadis, G. Venter, C. Viana, A. Vincent, P. Voelk, H. J. Volpe, F. Vorster, M. Vuillaume, T. Wagner, S. J. Wagner, P. Ward, M. Weidinger, M. Weitzel, Q. White, R. Wierzcholska, A. Willmann, P. Woernlein, A. Wouters, D. Zabalza, V. Zacharias, M. Zajczyk, A. Zdziarski, A. A. Zech, A. Zechlin, H. -S. TI HESS observations of the Crab during its March 2013 GeV gamma-ray flare SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays: ISM; ISM: individual objects: Crab nebula; radiation mechanisms: non-thermal; relativistic processes ID HIGH-ENERGY; PARTICLE-ACCELERATION; STANDARD CANDLE; NEBULA FLARE; EMISSION; PULSAR; VARIABILITY; COMPTON; TEV; ASTROPHYSICS AB Context. On March 4, 2013 the Fermi-EAT and AGILE reported a flare from the direction of the Crab nebula in which the high-energy (HE; E > 100 MeV) flux was six times above its quiescent level. Simultaneous observations in other energy bands give us hints about the emission processes during the flare episode and the physics of pulsar wind nebulae in general. Aims. We search for variability in the emission of the Crab nebula at very-high energies (VHF,; E > 100 GeV), using contemporaneous data taken with the H.E.S.S. array of Cherenkov telescopes. Methods. Observational data taken with the H.E.S.S. instrument on five consecutive days during the flare were analysed for the flux and spectral shape of the emission from the Crab nebula. Night-wise light curves are presented with energy thresholds of 1 TeV and 5 TeV. Results. The observations conducted with H.E.S.S. on March 6 to March 10, 2013 show no significant changes in the flux. They limit the variation in the integral flux above 1 TeV to less than 63% and the integral flux above 5 TeV to less than 78% at a 95% confidence level. C1 [Abramowski, A.; Fernandes, M. V.; Heinzelmann, G.; Horns, D.; Kastendieck, M. A.; Kneiske, T.; Opitz, B.; Raue, M.; Spies, F.; Tluczykont, M.; Zechlin, H. -S.] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany. [Aharonian, F.; Benkhali, F. Ait; Bernloehr, K.; Brun, F.; Carrigan, S.; Casanova, S.; Deil, C.; Domainko, W.; Edwards, T.; Eger, P.; Foerster, A.; Grondin, M. -H.; Hahn, J.; Hermann, G.; Hillert, A.; Hofmann, W.; Hofverberg, P.; Krueger, P. P.; Lennarz, D.; Lu, C. -C.; Marandon, V.; Marx, R.; 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.; Weitzel, Q.; Zabalza, V.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Aharonian, F.; Drury, L. O'C.; Romoli, C.; Sanchez, D. A.; Taylor, A. M.] Dublin Inst Adv Studies, Dublin 2, Ireland. [Aharonian, F.; Akhperjanian, A. G.; Sahakian, V.] Natl Acad Sci Republ Armenia, Yerevan, 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; Sanchez, D. A.; Schwanke, U.; Spengler, G.; Sushch, I.; Wagner, P.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Anton, G.; Brucker, J.; 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.; Giavitto, G.; Klepser, S.; Schulz, A.; Stegmann, C.; Stycz, K.] DESY, D-15738 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.] Linnaeus Univ, Dept Phys & Elect Engn, S-35195 Vaxjo, Sweden. [Tjus, J. Becker; Krakau, S.; Menzler, U.; Schlickeiser, R.; Weidinger, M.; Zacharias, M.] Ruhr Univ Bochum, Inst Theoret Phys, 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. [Biteau, J.; Degrange, B.; Fegan, S.; Fontaine, G.; Giebels, B.; de Naurois, M.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Boettcher, M.; Casanova, S.; Davids, I. D.; Krueger, P. P.; Pekeur, N. W.; Sushch, I.; Venter, C.; Vorster, M.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [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 06, Univ Paris 07, CNRS IN2P3, LPNHE, F-75252 Paris 5, France. [Bordas, P.; Cui, Y.; 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.; 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. [Cerruti, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Colafrancesco, S.] Univ Witwatersrand, Sch Phys, ZA-2050 Johannesburg, South Africa. [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. [Conrad, J.; Dickinson, H. J.; Farnier, C.; Meyer, M.] Univ Stockholm, Albanova Univ Ctr, Oskar Klein Ctr, Dept Phys, S-10691 Stockholm, Sweden. [Conrad, J.] Wallenberg Acad, Stockholm, Sweden. [Dalton, M.; Laffon, H.; Lemoine-Goumard, M.; Mehault, J.] Univ Bordeaux 1, CNRS IN2P3, Ctr Etudes Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Davids, I. D.; Steenkamp, R.] Univ Namibia, Dept Phys, Windhoek, Namibia. [de Wilt, P.; Maxted, N.; Rowell, G.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Djannati-Atai, A.; Espigat, P.; Khelifi, B.; Lefaucheur, J.; Lemiere, A.; Pita, S.; Punch, M.; Tavernier, T.; Terrier, R.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, APC,Sorbonne Paris Cite, F-75205 Paris, France. [Dubus, G.; Henri, G.; Pelletier, G.; Petrucci, P. -O.; Vuillaume, T.] UJF Grenoble, CNRS INSU 1, IPAG, UMR 5274, 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. [Feinstein, F.; Fernandez, D.; Gallant, Y. A.; Marcowith, A.; Renaud, M.; Vasileiadis, G.; Zajczyk, A.] Univ Montpellier 2, CNRS IN2P3, Lab Univ & Particules Montpellier, F-34095 Montpellier 5, France. [Fiasson, A.; Komin, Nu.; Krayzel, F.; Lamanna, G.; Maurin, G.; Rosier-Lees, S.; Trichard, C.] Univ Savoie, CNRS IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France. [Jamrozy, M.; Ostrowski, M.; Stawarz, L.; Szostek, A.; Wierzcholska, A.] Uniwersytet Jagiellonski, Obserwatorium Astronomiczne, PL-30244 Krakow, Poland. [Katarzynski, K.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. [Meintjes, P. J.; van Soelen, B.] Univ Free State, Dept Phys, ZA-9300 Bloemfontein, South Africa. [Rob, L.] Charles Univ Prague, Fac Math & Phys, Inst Particle & Nucl Phys, CR-18000 Prague, Czech Republic. RP Balzer, A (reprint author), DESY, D-15738 Zeuthen, Germany. EM arnim.balzer@desy.de; dieter.horns@desy.de; kornelia.stycz@desy.de RI Bissaldi, Elisabetta/K-7911-2016; Drury, Luke/B-1916-2017; Moulin, Emmanuel/B-5959-2017; Schussler, Fabian/G-5313-2013; Meyer, Manuel/E-2697-2016; van Eldik, Christopher/C-3901-2013; Tjus, Julia/G-8145-2012; Venter, Christo/E-6884-2011; Reimer, Olaf/A-3117-2013; Katarzynski, Krzysztof/G-4528-2014; Jamrozy, Marek/F-4507-2015; Katz, Uli/E-1925-2013; Casanova, Sabrina/J-8935-2013; Anton, Gisela/C-4840-2013; Daniel, Michael/A-2903-2010 OI Lenain, Jean-Philippe/0000-0001-7284-9220; Maxted, Nigel/0000-0003-2762-8378; Punch, Michael/0000-0002-4710-2165; Sushch, Iurii/0000-0002-2814-1257; Bordas, Pol/0000-0002-0266-8536; Oya, Igor/0000-0002-3881-9324; de Ona Wilhelmi, Emma/0000-0002-5401-0744; Rowell, Gavin/0000-0002-9516-1581; Bissaldi, Elisabetta/0000-0001-9935-8106; Drury, Luke/0000-0002-9257-2270; Moulin, Emmanuel/0000-0003-4007-0145; Schussler, Fabian/0000-0003-1500-6571; Chadwick, Paula/0000-0002-1468-2685; Kneiske, Tanja M./0000-0002-3210-6200; mohamed, mahmoud/0000-0002-4625-6242; de los Reyes Lopez, Raquel/0000-0003-0485-9552; Kruger, Paulus/0000-0003-0664-8521; Meyer, Manuel/0000-0002-0738-7581; van Eldik, Christopher/0000-0001-9669-645X; Venter, Christo/0000-0002-2666-4812; Reimer, Olaf/0000-0001-6953-1385; Katz, Uli/0000-0002-7063-4418; Casanova, Sabrina/0000-0002-6144-9122; Anton, Gisela/0000-0003-2039-4724; Daniel, Michael/0000-0002-8053-7910 FU Namibian authorities and of the University of Namibia; German Ministry for Education and Research (BMBF); Max Planck Society; German Research Foundation (DFG); French Ministry for Research; CNRS-IN2P3; Astroparticle Interdisciplinary Programmne of the CNRS; UK Science and Technology Facilities Council (STFC); IPNP of the Charles University; Czech Science Foundation; Polish Ministry of Science and Higher Education; South African Department of Science and Technology; National Research Foundation; University of Namibia FX The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programmne of the CNRS, the UK Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Czech Science Foundation, the Polish Ministry of Science and Higher Education, 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 NR 46 TC 5 Z9 5 U1 2 U2 9 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2014 VL 562 AR L4 DI 10.1051/0004-6361/201323013 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC0CG UT WOS:000332161800140 ER PT J AU Acciari, VA Arlen, T Aune, T Benbow, W Bird, R Bouvier, A Bradbury, SM Buckley, JH Bugaev, V Perez, ID Carter-Lewis, DA Cesarini, A Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Duke, C Dumm, J Falcone, A Federici, S Fegan, DJ Fegan, SJ Finley, JP Finnegan, G Fortson, L Gaidos, J Galante, N Gall, D Gibbs, K Gillanders, GH Griffin, S Grube, J Gyuk, G Hanna, D Horan, D Humensky, TB Kaaret, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lang, MJ McEnery, JE Madhavan, AS Moriarty, P Nelson, T de Bhroithe, AO Ong, RA Orr, M Otte, AN Perkins, JS Petry, D Pichel, A Pohl, M Quinn, J Ragan, K Reynolds, T Roache, E Rovero, A Schroedter, M Sembroski, GH Smith, A Telezhinsky, I Theiling, M Toner, J Tyler, J Varlotta, A Vivier, M Wakely, SP Ward, JE Weekes, TC Weinstein, A Welsing, R Williams, DA Wissel, S AF Acciari, V. A. Arlen, T. Aune, T. Benbow, W. Bird, R. Bouvier, A. Bradbury, S. M. Buckley, J. H. Bugaev, V. de la Calle Perez, I. Carter-Lewis, D. A. Cesarini, A. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Duke, C. Dumm, J. Falcone, A. Federici, S. Fegan, D. J. Fegan, S. J. Finley, J. P. Finnegan, G. Fortson, L. Gaidos, J. Galante, N. Gall, D. Gibbs, K. Gillanders, G. H. Griffin, S. Grube, J. Gyuk, G. Hanna, D. Horan, D. Humensky, T. B. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. McEnery, J. E. Madhavan, A. S. Moriarty, P. Nelson, T. de Bhroithe, A. O'Faolain Ong, R. A. Orr, M. Otte, A. N. Perkins, J. S. Petry, D. Pichel, A. Pohl, M. Quinn, J. Ragan, K. Reynolds, T. Roache, E. Rovero, A. Schroedter, M. Sembroski, G. H. Smith, A. Telezhinsky, I. Theiling, M. Toner, J. Tyler, J. Varlotta, A. Vivier, M. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Welsing, R. Williams, D. A. Wissel, S. TI Observation of Markarian 421 in TeV gamma rays over a 14-year time span SO ASTROPARTICLE PHYSICS LA English DT Article DE AGN; TeV gamma rays; Markarian 421 ID ACTIVE GALACTIC NUCLEI; MULTIWAVELENGTH OBSERVATIONS; CORRELATED VARIABILITY; BLAZAR MARKARIAN-421; TIMING EXPLORER; CRAB-NEBULA; ENERGY; TELESCOPE; EMISSION; FLARE AB The variability of the blazar Markarian 421 in TeV gamma rays over a 14-year time period has been explored with the Whipple 10 m telescope. It is shown that the dynamic range of its flux variations is large and similar to that in X-rays. A correlation between the X-ray and TeV energy bands is observed during some bright flares and when the complete data sets are binned on long timescales. The main database consists of 878.4 h of observation with the Whipple telescope, spread over 783 nights. The peak energy response of the telescope was 400 GeV with 20% uncertainty. This is the largest database of any TeV-emitting active galactic nucleus (AGN) and hence was used to explore the variability profile of Markarian 421. The tithe-averaged flux from Markarian 421 over this period was 0.446 +/- 0.008 Crab flux units. The flux exceeded 10 Crab flux units on three separate occasions. For the 2000-2001 season the average flux reached 1.86 Crab units, while in the 1996-1997 season the average flux was only 0.23 Crab units. (C) 2013 Elsevier B.V. All rights reserved. C1 [Acciari, V. A.; Moriarty, P.] Galway Mayo Inst Technol, Sch Sci, Galway, Ireland. [Acciari, V. A.; Benbow, W.; Galante, N.; Gibbs, K.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Arlen, T.; Ong, R. A.; Wissel, S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Bouvier, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Bouvier, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Bird, R.; Collins-Hughes, E.; Fegan, D. J.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Bradbury, S. M.] Univ Leeds, Dept Phys, Leeds LS2 9JT, Yorks, England. [Buckley, J. H.; Bugaev, V.; Krawczynski, H.; Ward, J. E.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [de la Calle Perez, I.] European Space Astron Ctr, Madrid 28080, Spain. [Carter-Lewis, D. A.; Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Cesarini, A.; Connolly, M. P.; Gillanders, G. H.; Lang, M. J.; Toner, 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.; Finley, J. P.; Gaidos, J.; 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.; Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Federici, S.; Pohl, M.; Telezhinsky, I.; Welsing, R.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Federici, S.; Pohl, M.; Telezhinsky, I.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Riguet, F-91128 Palaiseau, France. [Finnegan, G.; Kieda, D.; Smith, A.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Gall, D.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Griffin, S.; Hanna, D.; Ragan, K.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Humensky, T. B.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [McEnery, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Perkins, J. S.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, Astroparticle Phys Lab, GSFC, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Petry, D.] ESO, ALMA Reg Ctr, D-85748 Garching, Germany. [Pichel, A.; Rovero, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Reynolds, T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. RP Weekes, TC (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. EM pat.moriarty@gmit.ie; weekes@veritas.sao.arizona.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; 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]; STFC in the U.K. FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instruments. NR 43 TC 11 Z9 11 U1 1 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 EI 1873-2852 J9 ASTROPART PHYS JI Astropart Phys. PD FEB PY 2014 VL 54 BP 1 EP 10 DI 10.1016/j.astropartphys.2013.10.004 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AC3PW UT WOS:000332434700001 ER PT J AU Elvis, M AF Elvis, Martin TI How many ore-bearing asteroids? SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Near-Earth asteroids; Surveys; Population; Mining; Meteorites ID NEAR-EARTH OBJECTS; IRON-METEORITES; POPULATION; HAZARD; IMPACT; SPACE; STONY AB A simple formalism is presented to assess how many asteroids contain ore, i.e., commercially profitable material, and not merely a high concentration of a resource. I apply this formalism to two resource cases: platinum group metals (PGMs) and water. Assuming for now that only Ni-Fe asteroids are of interest for PGMs, then 1% of NEOs are rich in PGMs. The dearth of ultra-low delta-v ( <4.5 km s(-1)) NEOs larger than 100 m diameter reduces the ore-bearing fraction to only similar to 1 in 2000 NEOs. As 100 m diameter NEOs are needed to have a value >= US$1B and the population of near-Earth objects (NEOs) larger than 100 m diameter is similar to 20,000 (Mainzer et al., 2011) the total population of PGM ore-bearing NEOs is roughly 10.1 stress that this is a conservative and highly uncertain value. For example, an order of magnitude increase in PGM ore-bearing NEOs occurs if delta-v can be as large as 5.7 km s(-1). Water ore for utilization in space is likely to be found in similar to 1/1100 NEOs. NEOs as small as 18 m diameter can be water-ore-bodies because of the high richness of water (similar to 20%) expected in similar to 25% of carbonaceous asteroids, bringing the number of water-ore-bearing NEOs to similar to 9000 out of the 10 million NEOs of this size. These small NEOs are, however, hard to find with present surveys. There will be similar to 18 water-ore-bearing NEOs > 100 m diameter. These estimates are at present highly imprecise and sensitive to small changes, especially in the maximum delta-v allowed. Nonetheless the low values found here mean that much improved determinations of each of the terms of the formalism are urgently needed. If better estimates still find small numbers of ore-bearing NEOs then thorough surveys for NEA discovery and, especially, characterization are needed. Strategies for the two classes are likely to be different. (C) 2013 Published by Elsevier Ltd. C1 Harvard Smithsonian Ctr Astrophys, HEAD, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, HEAD, 60 Garden St, Cambridge, MA 02138 USA. OI Elvis, Martin/0000-0001-5060-1398 NR 50 TC 11 Z9 12 U1 3 U2 33 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD FEB PY 2014 VL 91 BP 20 EP 26 DI 10.1016/j.pss.2013.11.008 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AC8YV UT WOS:000332821900003 ER PT J AU Joyce, CJ Schwadron, NA Wilson, JK Spence, HE Kasper, JC Golightly, M Blake, JB 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. Townsend, L. W. Case, A. W. Semones, E. Smith, S. Zeitlin, C. J. TI Radiation modeling in the Earth and Mars atmospheres using LRO/CRaTER with the EMMREM Module SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE radiation; modulation potential; galactic cosmic rays AB We expand upon the efforts of Joyce et al. (2013), who computed the modulation potential at the Moon using measurements from the Cosmic Ray Telescope for the Effects of Radiation (CRaTER) instrument on the Lunar Reconnaissance Orbiter (LRO) spacecraft along with data products from the Earth-Moon-Mars Radiation Environment Module (EMMREM). Using the computed modulation potential, we calculate galactic cosmic ray (GCR) dose and dose equivalent rates in the Earth and Mars atmospheres for various altitudes over the course of the LRO mission. While we cannot validate these predictions by directly comparable measurement, we find that our results conform to expectations and are in good agreement with the nearest available measurements and therefore may be used as reasonable estimates for use in efforts in risk assessment in the planning of future space missions as well as in the study of GCRs. PREDICCS (Predictions of radiation from REleASE, EMMREM, and Data Incorporating the CRaTER, COSTEP, and other solar energetic particles measurements) is an online system designed to provide the scientific community with a comprehensive resource on the radiation environments of the inner heliosphere. The data products shown here will be incorporated into PREDICCS in order to further this effort and daily updates will be made available on the PREDICCS website (http://prediccs.sr.unh.edu). C1 [Joyce, C. J.; Schwadron, N. A.; Wilson, J. K.; Spence, H. E.; Golightly, M.; Smith, S.] Univ New Hampshire, Ctr Space Sci, Dept Phys, Durham, NH 03824 USA. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Blake, J. B.] Aerosp Corp, Los Angeles, CA 90009 USA. [Townsend, L. W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. [Case, A. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Semones, E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Zeitlin, C. J.] Southwest Res Inst, Boulder, CO USA. RP Joyce, CJ (reprint author), Univ New Hampshire, Ctr Space Sci, Dept Phys, 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 Thanks to everyone on the CRaTER team for their help and guidance. 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). NR 10 TC 3 Z9 3 U1 1 U2 6 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 FEB PY 2014 VL 12 IS 2 BP 112 EP 119 DI 10.1002/2013SW000997 PG 8 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AD1HU UT WOS:000332985800002 ER PT J AU Cavanaugh, KC Siegel, DA Raimondi, PT Alberto, F AF Cavanaugh, Kyle C. Siegel, David A. Raimondi, Peter T. Alberto, Filipe TI Patch definition in metapopulation analysis: a graph theory approach to solve the mega-patch problem SO ECOLOGY LA English DT Article DE giant kelp; Landsat; metapopulation; modularity; network; patch dynamics; remote sensing; spatial autocorrelation; synchrony ID MACROCYSTIS-PYRIFERA PHAEOPHYCEAE; GIANT-KELP MACROCYSTIS; SANTA-BARBARA CHANNEL; ENVIRONMENTAL CONTROLS; CONNECTIVITY MEASURES; POPULATION-DYNAMICS; EXTINCTION DYNAMICS; COMMUNITY STRUCTURE; GENETIC-STRUCTURE; NETWORKS AB The manner in which patches are delineated in spatially realistic metapopulation models will influence the size, connectivity, and extinction and recolonization dynamics of those patches. Most commonly used patch-definition methods focus on identifying discrete, contiguous patches of habitat from a single temporal observation of species occurrence or from a model of habitat suitability. However, these approaches are not suitable for many metapopulation systems where entire patches may not be fully colonized at a given time. For these metapopulation systems, a single large patch of habitat may actually support multiple, interacting subpopulations. The interactions among these subpopulations will be ignored if the patch is treated as a single unit, a situation we term the mega-patch problem. Mega-patches are characterized by variable intra-patch synchrony, artificially low inter-patch connectivity, and low extinction rates. One way to detect this problem is by using time series data to calculate demographic synchrony within mega-patches. We present a framework for identifying subpopulations in mega-patches using a combination of spatial autocorrelation and graph theory analyses. We apply our approach to southern California giant kelp (Macrocystis pyrifera) forests using a new, long-term (27 years), satellite-based data set of giant kelp canopy biomass. We define metapopulation patches using our method as well as several other commonly used patch delineation methodologies and examine the colonization and extinction dynamics of the metapopulation under each approach. We find that the relationships between patch characteristics such as area and connectivity and the demographic processes of colonizations and extinctions vary among the different patch-definition methods. Our spatial-analysis/graph-theoretic framework produces results that match theoretical expectations better than the other methods. This approach can be used to identify subpopulations in metapopulations where the distributions of organisms do not always reflect the distribution of suitable habitat. C1 [Cavanaugh, Kyle C.] Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA. [Siegel, David A.] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA. [Raimondi, Peter T.] Univ Calif Santa Cruz, Ctr Ocean Hlth, Dept Ecol & Evolutionary Biol, Long Marine Lab, Santa Cruz, CA 95060 USA. [Alberto, Filipe] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. RP Cavanaugh, KC (reprint author), Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA. EM cavanaughk@si.edu OI Alberto, Filipe/0000-0003-0593-3240 FU NASA's Biodiversity and Ecological Forecasting Science program; National Science Foundation's (NSF); NSF [OCE-1233839] FX We thank D. Reed and B. Kendall for helpful discussions regarding this work. Financial support for this research was provided by NASA's Biodiversity and Ecological Forecasting Science program, the National Science Foundation's (NSF) support of the Santa Barbara Coastal Long Term Ecological Research (SBC LTER) project, and the by the NSF under the Biological Oceanography grant (Award number: OCE-1233839). NR 61 TC 16 Z9 16 U1 5 U2 52 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 FEB PY 2014 VL 95 IS 2 BP 316 EP 328 DI 10.1890/13-0221.1 PG 13 WC Ecology SC Environmental Sciences & Ecology GA AA9RB UT WOS:000331429500007 PM 24669726 ER PT J AU Dillon, ME Dudley, R AF Dillon, Michael E. Dudley, Robert TI Surpassing Mt. Everest: extreme flight performance of alpine bumble-bees SO BIOLOGY LETTERS LA English DT Article DE air density; altitude; hovering; hypobaria; insect; kinematics ID VERTICAL FORCE; ENERGETICS; PHYSIOLOGY; KINEMATICS; ALLOMETRY; ALTITUDE; INSECTS; APIDAE; LIMITS AB Animal flight at altitude involves substantial aerodynamic and physiological challenges. Hovering at high elevations is particularly demanding from the dual perspectives of lift and power output; nevertheless, some volant insects reside and fly at elevations in excess of 4000 m. Here, we demonstrate that alpine bumble-bees possess substantial aerodynamic reserves, and can sustain hovering flight under hypobaria at effective elevations in excess of 9000 m, i.e. higher than Mt. Everest. Modulation of stroke amplitude and not wingbeat frequency is the primary means of compensation for overcoming the aerodynamic challenge. The presence of such excess capacity in a high-altitude bumble-bee is surprising and suggests intermittent behavioural demands for extreme flight performance supplemental to routine foraging. C1 [Dillon, Michael E.; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. RP Dillon, ME (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM michael.dillon@uwyo.edu FU NSF Minority Postdoctoral fellowship; National Geographic Society CRE grant FX This work was supported by an NSF Minority Postdoctoral fellowship to M.E.D., and a National Geographic Society CRE grant to M.E.D. and R.D. NR 15 TC 11 Z9 11 U1 0 U2 29 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 EI 1744-957X J9 BIOL LETTERS JI Biol. Lett. PD FEB 1 PY 2014 VL 10 IS 2 AR 20130922 DI 10.1098/rsbl.2013.0922 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AC2WZ UT WOS:000332378300003 PM 24501268 ER PT J AU Libourel, G Corrigan, CM AF Libourel, Guy Corrigan, Catherine M. TI Asteroids: New Challenges, New Targets SO ELEMENTS LA English DT Article DE meteorites; meteors; asteroids; minor planets; sample-return missions ID MAIN BELT; SOLAR-SYSTEM; POPULATION; YARKOVSKY; EVOLUTION; SEARCH; ORIGIN AB At present, we know of similar to 600,000 asteroids in the asteroid belt, and there are very likely millions more. Orbiting the Sun between Mars and Jupiter, they are thought to be the shattered remnants of small bodies formed within the young Sun's solar nebula that never accreted enough material to become planets. These "minor bodies" are therefore keys to understanding how the Solar System formed and evolved. As leftover planetary building blocks, they are of great importance in understanding planetary compositions. They may also provide clues to the origin of life, as similar bodies may have delivered organics and water to the early Earth. For these reasons, several international space agencies have funded sample-return missions to asteroids. C1 [Libourel, Guy] Observ Cote Azur, F-06304 Nice 4, France. [Libourel, Guy] Univ Lorraine, CRPG, CNRS, UMR 7358, F-54501 Vandoeuvre Les Nancy, France. [Corrigan, Catherine M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20056 USA. RP Libourel, G (reprint author), Observ Cote Azur, BP 4229, F-06304 Nice 4, France. EM libou@oca.eu; corriganc@si.edu FU CNES; ANR Shocks Blanc SIMI [5-6 008-01] FX M. Delbo, E. Bullock, and T. McCoy are thanked for exciting conversations and for critically reading the manuscript. GL is indebted to the INSU-CNRS since he conducted part of his work as a CNRS delegate. GL was supported in this work by the CNES and by the ANR Shocks 2011 Blanc SIMI 5-6 008-01 grants, specifically to the Henderson Endowment to the Division of Meteorites. This article benefited from insightful reviews by Hap McSween, Travis Tenner, and John Valley. This issue also benefited from the expertise imparted by individual article reviewers Jean-Alix Barrat, Bill Bottke, Tom Burbine, Monica Grady, Vicky Hamilton, Tim McCoy, Ed Scott, Caroline Smith, Jessica Sunshine, and Mike Zolensky. We thank them for their time and assistance. Finally, we would like to express our sincere gratitude to Pierrette Tremblay and John Valley (without whom this issue would not exist) for their time, expertise and patience. NR 27 TC 3 Z9 3 U1 3 U2 11 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 1811-5209 EI 1811-5217 J9 ELEMENTS JI Elements PD FEB PY 2014 VL 10 IS 1 BP 11 EP 17 PG 7 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AB8RS UT WOS:000332058300003 ER PT J AU France, CAM Thomas, DB Doney, CR Madden, O AF France, Christine A. M. Thomas, Daniel B. Doney, Charlotte R. Madden, Odile TI FT-Raman spectroscopy as a method for screening collagen diagenesis in bone SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Raman; Bone; Collagen; Bioapatite; Diagenesis ID STABLE-ISOTOPE ANALYSIS; OXYGEN-ISOTOPE; FOSSIL BONE; PALEODIETARY RECONSTRUCTION; PLEISTOCENE MAMMALS; PHOSPHATE; NITROGEN; CARBON; BIOGEOCHEMISTRY; PRESERVATION AB This study examines Fourier transform (FT) Raman spectroscopy as a non-destructive screening method to determine collagen quality in archaeological and paleontological bones. Bone samples were characterized for collagen quality using well-established elemental abundance analyses (i.e., percentage nitrogen and C:N) as the primary criteria for classification. FT-Raman spectra were collected from outer surfaces and freshly cut cross-sections of both well-preserved and poorly-preserved historic mammal bones. Peak heights and peak areas were studied visually and with bivariate and multivariate statistics. Raman spectra from cross-sections provided the most accurate determination of collagen quality. A ratio of the 960 cm(-1) and 1636 cm(-1) peak heights provided the most unambiguous distinction between bones with well-preserved and poorly-preserved collagen. The 960 cm(-1) and 1636 cm(-1) peaks represent phosphate anion stretching in the bone mineral and amide carbonyl stretching in the collagen, respectively. FT-Raman spectra from bones with well-preserved collagen produced a 960 cm(-1):1636 cm(-1) ratio of 19.4 or less (after peaks were baseline corrected). This mineral to collagen ratio was typically greater in poorly-preserved samples as organic material tends to be more susceptible to early stages of diagenesis. These criteria now can be used to accurately determine collagen quality in bones before sacrificing samples to the lengthy and destructive chemical extractions necessary for carbon-14 dating, stable isotope analyses, proteomic analyses, and other techniques of archaeological or paleontological interest. Published by Elsevier Ltd. C1 [France, Christine A. M.; Thomas, Daniel B.; Doney, Charlotte R.; Madden, Odile] Smithsonian Museum Conservat Inst, Suitland, MD 20746 USA. [Thomas, Daniel B.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP France, CAM (reprint author), Smithsonian Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM francec@si.edu RI Madden, Odile/N-9909-2015 OI Madden, Odile/0000-0003-2322-2522 FU Smithsonian Peter Buck Post-doctoral Fellowship; National Science Foundation Research Experience for Undergraduates Award [SMA-1156360] FX The authors acknowledge K. Bruwelheide, S. McGuire, S. Mills, W. Miller, D. Owsley, and A. Warmack for assistance with sample procurement and preparation. Financial support for D. Thomas provided by Smithsonian Peter Buck Post-doctoral Fellowship. Financial support for C. Doney provided by National Science Foundation Research Experience for Undergraduates Award #SMA-1156360. All analyses performed at the Smithsonian OUSS/MCI Stable Isotope Mass Spectrometry Laboratory and the Smithsonian MCI Modern Materials Laboratory at the Smithsonian Museum Conservation Institute, Suitland, MD. NR 62 TC 9 Z9 9 U1 1 U2 34 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 EI 1095-9238 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD FEB PY 2014 VL 42 BP 346 EP 355 DI 10.1016/j.jas.2013.11.020 PG 10 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA AB9RJ UT WOS:000332133100028 ER PT J AU France, CAM Owsley, DW Hayek, LAC AF France, Christine A. M. Owsley, Douglas W. Hayek, Lee-Ann C. TI Stable isotope indicators of provenance and demographics in 18th and 19th century North Americans SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Stable isotopes; Bone; Teeth; Demography; Provenance; North America; Human ID BONE PHOSPHATE; OXYGEN-ISOTOPE; DIAGENETIC EVOLUTION; SPATIAL-DISTRIBUTION; COLLAGEN EXTRACTION; C-13/C-12 RATIOS; CARBON ISOTOPES; UNITED-STATES; DIET; NITROGEN AB Using stable isotopes to gain insight into individual life histories is a valuable tool for unidentified or incomplete remains lacking historic records. This study analyzed stable carbon, nitrogen, and oxygen isotopes from bones and teeth of 18th-19th century North Americans of known ancestry, social class, and region of origin in an effort to discern qualitative patterns and create a quantitative predictive model of demographic information. The delta C-13(collagen), delta C-13(structural carbonate), and delta O-18(structural carbonate) values provide the most overall information for detecting demographic differences, with delta N-15(collagen) and delta O-18(phosphate) to a lesser degree. Region of origin was the most predictable demographic factor with 82% correct classifications based on a two-variable model using delta C-13(collagen) and delta O-18(meteoric) water calculated from ebstructural carbonate, which reflects the influence of dominant local vegetation types and local drinking water. Ancestry was correctly identified in 68% of cases using delta C-13(collagen). Social class was less predictable with correct identification in 60% of cases based on delta C-13, delta N-15, and delta O-18 values where the upper class was phate o t most distinguishable. Isotope patterns observed in ancestry and social class groups are linked to cultural food preferences and food availability. Certain sample sites, such as military burials and urban cemeteries, show a greater range of isotope values suggesting a variety of individual regional origins and cultural backgrounds. Burials of extreme upper or lower class individuals show greater isotopic homogeneity suggesting reliance on localized food sources or cultural preferences for particular dietary choices. Published by Elsevier Ltd. C1 [France, Christine A. M.] Smithsonian Museum Conservat Inst, Suitland, MD 20746 USA. [Owsley, Douglas W.; Hayek, Lee-Ann C.] Smithsonian Natl Museum Nat Hist, Washington, DC 20013 USA. RP France, CAM (reprint author), Smithsonian Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM francec@si.edu NR 81 TC 3 Z9 3 U1 0 U2 10 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 EI 1095-9238 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD FEB PY 2014 VL 42 BP 356 EP 366 DI 10.1016/j.jas.2013.10.037 PG 11 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA AB9RJ UT WOS:000332133100029 ER PT J AU Zhang, L Liu, JZ Mcshea, WJ Wu, YL Wang, DJ Lu, Z AF Zhang, Lu Liu, Jiazi Mcshea, William J. Wu, Yonglin Wang, Dajun Lu, Zhi TI The Impact of Fencing on the Distribution of Przewalski's Gazelle SO JOURNAL OF WILDLIFE MANAGEMENT LA English DT Article DE barbed wire; fencing; grassland; Procapra przewalskii; Przewalski's gazelle; Tibetan Plateau ID PROCAPRA-PRZEWALSKII; NATIONAL-PARK; CONSERVATION BIOLOGY; MONGOLIAN GAZELLES; QINGHAI LAKE; MULE DEER; ECOLOGY; REGRESSION; BIOMASS; FENCES AB The endangered Przewalski's gazelle (Procapra przewalskii) experienced severe habitat loss and population decline over the last century. Illegal hunting of gazelles has been largely prevented since 2002, leaving fencing of pastures as one of the main threats to the gazelle. We conducted surveys on 810km of parallel transects on 8 gazelle-occupied sites and 4 nearby control sites where no gazelles were found, and evaluated the impact of fencing on gazelle distribution. A comparison of gazelle-occupied and control sites showed the former had a lower fence density and height, lower aboveground biomass (EVI), and a longer distance to houses. Logistic regression indicated that the presence of gazelle feces on the 1-km segment of transect was negatively affected by the density of fences and the proportion of fences with barbed wire both in spring and summer. In addition, we found a negative effect from distance to houses in spring and from EVI in summer. Gazelles did not occur more on grasslands with greater vegetation biomass, possibly because of the association of greater vegetation biomass with greater fence density and proportion of barbed wires. Although removing fences can be costly, lowering the top barbed wire, as well as constructing special gates and seasonal use of existing gates, may be beneficial for this endangered species at minimal disruption to local people. (c) 2014 The Wildlife Society. C1 [Zhang, Lu; Liu, Jiazi; Wang, Dajun; Lu, Zhi] Peking Univ, Sch Life Sci, Ctr Nat & Soc, Beijing 100871, Peoples R China. [Zhang, Lu; Mcshea, William J.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA. [Wu, Yonglin] Qinghai Lake Nat Reserve, Xining 810008, Qinghai, Peoples R China. [Lu, Zhi] Peking Univ, Shan Shui Conservat Ctr, Beijing 100871, Peoples R China. RP Zhang, L (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM zhanglu726@gmail.com FU Shan Shui Conservation Center; Conservation International; Peking University; Conservation Leadership Programme FX This work was funded by Shan Shui Conservation Center, Conservation International, Peking University, and Conservation Leadership Programme. We thank the staff of Qinghai Forestry Bureau, Shan Shui Conservation Center, and Qinghai Lake National Nature Reserve for cooperating and help. We also thank staff of forestry bureaus of Haiyan, Gangcha, Gonghe, and Tianjun County, and staff of Hudong Farm for helping with field surveys. Our sincere thanks go to G. B. Schaller, K. A. Olson, and J. R. Thompson, for their advice and effort to edit this paper. We also thank the reviewers for their helpful suggestions. We are grateful for Hua Qingjia, Kebujinjia, and Li Bao as field guides, and for Wang Rui, Tuo Chunxia, Yang Yufa, Feng Lang, and Zhu Wen (Qinghai Normal University) for helping us in the field as volunteers. NR 57 TC 1 Z9 1 U1 4 U2 23 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 FEB PY 2014 VL 78 IS 2 BP 255 EP 263 DI 10.1002/jwmg.653 PG 9 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA AB5XS UT WOS:000331862600009 ER PT J AU Castro, MC Carlini, AA Sanchez, R Sanchez-Villagra, MR AF Castro, Mariela C. Carlini, Alfredo A. Sanchez, Rodolfo Sanchez-Villagra, Marcelo R. TI A new Dasypodini armadillo (Xenarthra: Cingulata) from San Gregorio Formation, Pliocene of Venezuela: affinities and biogeographic interpretations SO NATURWISSENSCHAFTEN LA English DT Article DE Xenarthra; Cingulata; Dasypodidae; Pliodasypus; Pliocene; Venezuela ID AMERICAN BIOTIC INTERCHANGE; SOUTH-AMERICA; ITABORAI BASIN; ESTADO FALCON; LATE MIOCENE; MAMMALIA; PLEISTOCENE; BRAZIL; PALEOBIOGEOGRAPHY; MEGATHERIIDAE AB We describe Pliodasypus vergelianus gen. et sp. nov., a Dasypodini armadillo from the middle Pliocene of Venezuela (Vergel Member, San Gregorio Formation). Although scarce, the remains are remarkable because of their geochronologic proximity to the main phase of Great American Biotic Interchange (GABI). The cladistic analysis conducted reveals that Pliodasypus groups with Dasypus and both are sister taxa of Propraopus, whereas Anadasypus is at a basal position. With respect to the records of tribe Dasypodini, after its oldest representative (Anadasypus, middle and late Miocene), the chronologically subsequent form is Pl. vergelianus (middle Pliocene), followed by Dasypus bellus in higher northern latitudes (late Pliocene), and then by widespread occurrences in the Pleistocene of North America (D. bellus) and South America (Propraopus, Dasypus punctatus, and Dasypus novemcinctus). Thus, we infer that Dasypus differentiated in the late Pliocene at low latitudes in the northern South America. It leads to two alternative hypotheses of dispersal: (a) some early Dasypus remained cryptically in South America until the Pleistocene, whereas others dispersed to North America between 2.2 and 2.7 Ma, or (b) they dispersed to North America subsequently to the emersion of the Panamanian isthmus and D. bellus differentiated there; later, during the Pleistocene, D. bellus entered South America and experienced speciation. The same process of re-ingression has been proposed to other xenarthrans, breaking with the traditional assumption that the GABI was unidirectional. C1 [Castro, Mariela C.; Carlini, Alfredo A.] Univ Nacl La Plata, Fac Ciencias Nat & Museo, Div Paleontol Vertebrados, La Plata, Buenos Aires, Argentina. [Carlini, Alfredo A.] Consejo Nacl Invest Cient & Tecn, RA-1033 Buenos Aires, DF, Argentina. [Sanchez, Rodolfo] Smithsonian Trop Res Inst, Panama City, Panama. [Sanchez-Villagra, Marcelo R.] Univ Zurich, Palaontol Inst & Museum, CH-8006 Zurich, Switzerland. RP Castro, MC (reprint author), Univ Nacl La Plata, Fac Ciencias Nat & Museo, Div Paleontol Vertebrados, Paseo Bosque S-N,B1900WFA, La Plata, Buenos Aires, Argentina. EM marielaccastro@yahoo.com.br; acarlini@fcnym.unlp.edu.ar; rodolfosanchez128@hotmail.com; m.sanchez@pim.uzh.ch FU UNLP [N-593]; Capes [BEX 0840/10-6] FX The authors thank Instituto del Patrimonio Cultural, Venezuela and the curators that permitted the study of material under their care. We also thank the editors and anonymous reviewers for their valuable suggestions that certainly improved our manuscript. This research was partially funded by UNLP N-593 and Capes (BEX 0840/10-6). NR 73 TC 5 Z9 6 U1 5 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 EI 1432-1904 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD FEB PY 2014 VL 101 IS 2 BP 77 EP 86 DI 10.1007/s00114-013-1131-5 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AB7WD UT WOS:000332000700001 PM 24414134 ER PT J AU Ma, YN Filley, TR Szlavecz, K McCormick, MK AF Ma, Yini Filley, Timothy R. Szlavecz, Katalin McCormick, Melissa K. TI Controls on wood and leaf litter incorporation into soil fractions in forests at different successional stages SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Soil organic matter; Aboveground litter; Lignin; Substituted fatty acids; Soil fractions; Invasive earthworms; Earthworm species composition ID ORGANIC-MATTER CHEMISTRY; SIMULATED ACID-RAIN; COASTAL DUNE SOILS; EARTHWORM INVASION; HUMUS FORMS; TEMPERATE FORESTS; DECIDUOUS FOREST; CARBON STORAGE; NORWAY SPRUCE; PH GRADIENT AB In this study, we examined the response of surface soils to increased leaf and wood litter input within adjacent successional forests recovering from agricultural disturbance at the Smithsonian Environmental Research Center (SERC), Maryland, USA. Previous studies at this site demonstrated an arrested development of O-horizon, even after 130 years of forest growth, and an annual loss of leaf litter in forests with the highest abundance of invasive earthworms. Biogeochemical indices of plant biopolymer dynamics, i.e. extractable lignin and substituted fatty acids (SFAs), were applied to soil physical fractions in order to assess the fate of 5 years of increased Tulip poplar (Liriodendron tulipifera L) wood and leaf litter into O-horizon and mineral soil particles of purportedly different protection levels in this recovering forest system. Our results showed that in this continuously-disturbed recovering system the pattern of litter incorporation into soil varied with both litter type and forest age. For example, young successional forests, that also contained higher abundances of soil feeding endogeic earthworms, incorporated wood amendments deeper into soils and in a predominantly particulate organic matter (POM) form than older successional systems with predominantly litter and surface dwelling earthworms. Soil lignin concentration increased sharply with wood amendments in both forest stages, but young successional forests exhibited incorporation of fresher lignin into both POM and silt and clay (SC) fractions over 0-5 cm and 5-10 cm depths while old forests only increased in POM in the 0-5 cm depth. We attribute these differences to the higher rates of physical mixing from soil feeding endogeic species and potentially lower fungal activity in young successional forests. However, despite nearly 2.5 times of background annual leaf litter input over 5 years, neither total C content nor SFA concentration in soil fractions increased, a phenomenon we attribute to full decomposition of leaf litter amendments. These results demonstrate how the chemical trajectory of soils and litter layers in recovering forests can be a function of both legacy and current disturbance. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Ma, Yini; Filley, Timothy R.] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. [Ma, Yini; Filley, Timothy R.] Purdue Climate Change Res Ctr, W Lafayette, IN 47907 USA. [Szlavecz, Katalin] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21216 USA. [McCormick, Melissa K.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Ma, YN (reprint author), Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. EM ma25@purdue.edu OI Szlavecz, Katalin/0000-0003-2504-0298 FU National Science Foundation [NSF EAR-0748746]; United States Department of Agriculture [USDA-CSREES NRI 2007-35320-18375] FX This research was supported by grant from the National Science Foundation (NSF EAR-0748746) and from the United States Department of Agriculture (USDA-CSREES NRI 2007-35320-18375). We would like to thank jay O'Neill for the help on field site maintenance, Chih-Han Chang, Scott Pitz, and Helen Huang for helping earthworm sampling; Seth L. King and Grace Conyers for helping physical separation of soil samples; David Gamblin and Ian Schaller for helping lignin and SFA extraction and analysis. We thank two anonymous reviewers for valuable comments, which led to a considerable improvement of the manuscript. NR 94 TC 7 Z9 8 U1 14 U2 78 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 FEB PY 2014 VL 69 BP 212 EP 222 DI 10.1016/j.soilbio.2013.10.043 PG 11 WC Soil Science SC Agriculture GA AC1MV UT WOS:000332261600026 ER PT J AU Cutler, NA Chaput, DL van der Gast, CJ AF Cutler, Nick A. Chaput, Dominique L. van der Gast, Christopher J. TI Long-term changes in soil microbial communities during primary succession SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Iceland; Soil ecology; Community assembly; Plant soil interactions; Aboveground-belowground linkages; Mycorrhizal fungi ID 16S RIBOSOMAL-RNA; ECOSYSTEM PROPERTIES; GLACIER FOREFRONT; NITROGEN-FIXATION; PLANT DIVERSITY; VOLCANIC SOILS; ICELAND; FUNGI; CHRONOSEQUENCES; IDENTIFICATION AB Soil microbial communities (SMCs) play a critical role in the cycling of carbon and nutrients in terrestrial ecosystems, as well as regulating plant productivity and diversity. However, very little is known about long-term (decades-centuries) structural changes in these communities. The development of aboveground-belowground linkages during century-scale succession is also poorly understood. Our study addressed this knowledge gap by investigating SMC and plant communities undergoing primary succession on an 850-year chronosequence of lava flows in Iceland. We hypothesised that communities of microfungi and bacteria would respond to progressive changes in vegetation and that SMC diversity would increase with terrain age. Soil samples were collected from three lava flows at different stages of primary succession (165, 621 and 852 years after lava flow emplacement). Plant community composition was surveyed as the samples were collected. The composition of the SMCs present in the soil was determined using amplicon pyrosequencing. The physical and chemical properties of the soil were also analysed. The results of the study indicated changes in plant and fungal communities with increasing terrain age. Distinct plant and fungal assemblages were identified on the three sites and both communities became richer and more diverse with increasing terrain age. There was also evidence to suggest the development of mycorrhizal associations on older sites. In contrast, the composition and structure of the bacterial communities did not change systematically with terrain age. Similarly, there were few changes in soil properties: SOM concentrations and pH, both of which have been demonstrated to be important to SMCs, were constant across the chronosequence. These results suggest that plant community composition is significant for fungal communities, but less relevant for bacterial communities. This finding has implications for studies of primary succession and the biogeochemical impact of vegetation change in high-latitude ecosystems. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Cutler, Nick A.] Univ Cambridge, Scott Polar Res Inst, Cambridge CB2 1EP, England. [Chaput, Dominique L.] Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [van der Gast, Christopher J.] Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England. RP Cutler, NA (reprint author), Univ Cambridge Churchill Coll, Cambridge CB3 0DS, England. EM nac37@cam.ac.uk OI Chaput, Dominique/0000-0002-9736-2619; Cutler, Nick/0000-0003-1746-7769 FU British Ecological Society [2812/3507]; University of Oxford [091/148]; Trinity College, University of Cambridge FX We thank two anonymous reviewers for their helpful comments. This work was funded by a Small Ecological Project Grant from the British Ecological Society (grant number 2812/3507) and grants from the John Fell Fund, University of Oxford (grant number 091/148) and Trinity College, University of Cambridge. We are grateful for the assistance provided by Steve Boreham (Geography Science Laboratories, University of Cambridge) and James Rolfe (Godwin Laboratory for Palaeoclimate Research, University of Cambridge) in the geochemical analysis of the soil samples and to Gregor Sutherland for field support. NR 67 TC 16 Z9 18 U1 9 U2 116 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 FEB PY 2014 VL 69 BP 359 EP 370 DI 10.1016/j.soilbio.2013.11.022 PG 12 WC Soil Science SC Agriculture GA AC1MV UT WOS:000332261600041 ER PT J AU Zahid, HJ Torrey, P Vogelsberger, M Hernquist, L Kewley, L Dave, R AF Zahid, H. Jabran Torrey, Paul Vogelsberger, Mark Hernquist, Lars Kewley, Lisa Dave, Romeel TI Empirical constraints for the magnitude and composition of galactic winds SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE Galaxies: abundances; Galaxies: ISM; Galaxies: star-formation ID MOVING-MESH COSMOLOGY; STAR-FORMING GALAXIES; MASS-METALLICITY RELATION; SUPERMASSIVE BLACK-HOLES; ABSORPTION-LINE PROBES; GAS ACCRETION; OUTFLOWS; SIMULATIONS; STELLAR; ORIGIN AB Galactic winds are a key physical mechanism for understanding galaxy formation and evolution, yet empirical and theoretical constraints for the character of winds are limited and discrepant. Recent empirical models find that local star-forming galaxies have a deficit of oxygen that scales with galaxy stellar mass. The oxygen deficit provides unique empirical constraints on the magnitude of mass loss, composition of outflowing material and metal reaccretion onto galaxies. We formulate the oxygen deficit constraints so they may be easily implemented into theoretical models of galaxy evolution. We parameterize an effective metal loading factor which combines the uncertainties of metal outflows and metal reaccretion into a single function of galaxy virial velocity. We determine the effective metal loading factor by forward-fitting the oxygen deficit. The effective metal loading factor we derive has important implications for the implementation of mass loss in models of galaxy evolution. C1 [Zahid, H. Jabran] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Torrey, Paul; Vogelsberger, Mark; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kewley, Lisa] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Dave, Romeel] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Dave, Romeel] Univ Western Cape, ZA-7535 Bellville, Capte Town, South Africa. [Dave, Romeel] South African Astron Observ, ZA-7925 Cape Town, South Africa. [Dave, Romeel] African Inst Math Sci, ZA-7950 Cape Town, South Africa. RP Zahid, HJ (reprint author), Univ Hawaii Manoa, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM jabran@ifa.hawaii.edu OI Torrey, Paul/0000-0002-5653-0786 NR 37 TC 10 Z9 10 U1 1 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X EI 1572-946X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD FEB PY 2014 VL 349 IS 2 BP 873 EP 879 DI 10.1007/s10509-013-1666-0 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB2UU UT WOS:000331648400027 ER PT J AU Tian, SK Koty, PP Sangueza, OP Trizna, MG Qasem, SA AF Tian, S. K. Koty, P. P. Sangueza, O. P. Trizna, M. G. Qasem, S. A. TI Quantitative miRNA Expression Profiling as an Objective Tool to Differentiate Malignant Peripheral Nerve Sheath Tumors and Desmoplastic Melanomas SO LABORATORY INVESTIGATION LA English DT Meeting Abstract CT 103rd Annual Meeting of the United-States-and-Canadian-Academy-of-Pathology (USCAP) CY MAR 01-07, 2014 CL San Diego, CA SP US & Canadian Acad Pathol, Dako, Biocare Med, Leica Biosystems, LabCorp Specialty Testing Grp, Integrated Oncol, GenomOncology, Nephropath, Ventana, Diagnost BioSystems C1 Wake Sch Med, Winston Salem, NC USA. Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 0023-6837 EI 1530-0307 J9 LAB INVEST JI Lab. Invest. PD FEB PY 2014 VL 94 SU 1 MA 110 BP 30A EP 30A PG 1 WC Medicine, Research & Experimental; Pathology SC Research & Experimental Medicine; Pathology GA AA5QX UT WOS:000331155800111 ER PT J AU Tian, SK Koty, PP Sangueza, OP Trizna, MG Qasem, SA AF Tian, S. K. Koty, P. P. Sangueza, O. P. Trizna, M. G. Qasem, S. A. TI Quantitative miRNA Expression Profiling as an Objective Tool to Differentiate Malignant Peripheral Nerve Sheath Tumors and Desmoplastic Melanomas SO MODERN PATHOLOGY LA English DT Meeting Abstract CT 103rd Annual Meeting of the United-States-and-Canadian-Academy-of-Pathology (USCAP) CY MAR 01-07, 2014 CL San Diego, CA SP US & Canadian Acad Pathol, Dako, Biocare Med, Leica Biosystems, LabCorp Specialty Testing Grp, Integrated Oncol, GenomOncology, Nephropath, Ventana, Diagnost BioSystems C1 Wake Sch Med, Winston Salem, NC USA. Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 0893-3952 EI 1530-0285 J9 MODERN PATHOL JI Mod. Pathol. PD FEB PY 2014 VL 27 SU 2 MA 110 BP 30A EP 30A PG 1 WC Pathology SC Pathology GA AB0SK UT WOS:000331502200110 ER PT J AU Suselbeek, L Emsens, WJ Hirsch, BT Kays, R Rowcliffe, JM Zamora-Gutierrez, V Jansen, PA AF Suselbeek, Lennart Emsens, Willem-Jan Hirsch, Ben T. Kays, Roland Rowcliffe, J. Marcus Zamora-Gutierrez, Veronica Jansen, Patrick A. TI Food acquisition and predator avoidance in a Neotropical rodent SO ANIMAL BEHAVIOUR LA English DT Article DE camera trapping; daily activity patterns; Dasyprocta punctata; foraging-predation trade-off; Leopardus pardalis; optimal foraging; predation pressure; predator-prey interactions; radiotelemetry; risk allocation hypothesis ID AGOUTI DASYPROCTA-PUNCTATA; OCELOT LEOPARDUS-PARDALIS; SCATTER-HOARDING RODENT; BARRO-COLORADO ISLAND; ANTIPREDATOR BEHAVIOR; ALLOCATION HYPOTHESIS; MOONLIGHT AVOIDANCE; FORAGING BEHAVIOR; TIME ALLOCATION; HABITAT USE AB Foraging activity in animals reflects a compromise between acquiring food and avoiding predation. The risk allocation hypothesis predicts that prey animals optimize this balance by concentrating their foraging activity at times of relatively low predation risk, as much as their energy status permits, but empirical evidence is scarce. We used a unique combination of automated telemetry, manual radiotelemetry and camera trapping to test whether activity at high risk times declined with food availability as predicted in a Neotropical forest rodent, the Central American agouti, Dasyprocta punctata. We found that the relative risk of predation by the main predator, the ocelot, Leopardus pardalis, estimated as the ratio of ocelot to agouti activity on camera trap photographs, was up to four orders of magnitude higher between sunset and sunrise than during the rest of the day. Kills of radiotracked agoutis by ocelots during this high-risk period far exceeded expectations given agouti activity. Both telemetric monitoring of radio-tagged agoutis and camera monitoring of burrow entrances indicated that agoutis exited their burrows later at dawn, entered their burrows earlier at dusk and had lower overall activity levels when they lived in areas with higher food abundance. Thus, agoutis avoided activity during the high-risk period more strongly when access to food was higher. Our study provides quantitative empirical evidence of prey animals concentrating their activity at times of relatively low predation risk. (C) 2013 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Suselbeek, Lennart; Emsens, Willem-Jan; Zamora-Gutierrez, Veronica; Jansen, Patrick A.] Wageningen Univ, Dept Environm Sci, NL-6700 AA Wageningen, Netherlands. [Suselbeek, Lennart; Emsens, Willem-Jan; Hirsch, Ben T.; Kays, Roland; Zamora-Gutierrez, Veronica; Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Emsens, Willem-Jan] Univ Antwerp, Dept Biol, Antwerp, Belgium. [Hirsch, Ben T.] Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA. [Kays, Roland] North Carolina Museum Nat Sci, Nat Res Ctr, Raleigh, NC USA. [Kays, Roland] N Carolina State Univ, Fisheries Wildlife & Conservat Program, Raleigh, NC 27695 USA. [Rowcliffe, J. Marcus] Zool Soc London, Inst Zool, London NW1 4RY, England. [Zamora-Gutierrez, Veronica] Univ Cambridge, Dept Zool, Cambridge, England. [Jansen, Patrick A.] Univ Groningen, Ctr Ecol & Evolutionary Studies, Groningen, Netherlands. RP Suselbeek, L (reprint author), Wageningen Univ, Dept Environm Sci, POB 47, NL-6700 AA Wageningen, Netherlands. EM lennart.suselbeek@wur.nl RI Jansen, Patrick/G-2545-2015 OI Jansen, Patrick/0000-0002-4660-0314 FU National Science Foundation [NSF-DEB-0717071]; Netherlands Foundation for Scientific Research [NWO-ALW863-07-008]; Frank Levinson Family Foundation FX We gratefully acknowledge field support from Meg Crofoot, Annemarie Winkelhagen, Torrey Rodgers, Matthew Mc Elroy, Sumana Serchan, Daniel Rasmussen and Jose Alejandro Silva, technical support with the ARTS system from Daniel Obando and Alejandro Ortega, and logistical support from Belkys Jimenez, Oris Acevedo and the Smithsonian Tropical Research Institute. We thank Ron Ydenberg, Peter Bednekoff, Andrew King and four anonymous referees for constructive comments. Financial support was provided by the National Science Foundation (NSF-DEB-0717071 to R. K.) and the Netherlands Foundation for Scientific Research (NWO-ALW863-07-008 to P.A.J.). ARTS was supported by the Frank Levinson Family Foundation. NR 54 TC 4 Z9 4 U1 6 U2 74 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 FEB PY 2014 VL 88 BP 41 EP 48 DI 10.1016/j.anbehav.2013.11.012 PG 8 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA AA5KA UT WOS:000331134500006 ER PT J AU Cranmer, SR Bastien, FA Stassun, KG Saar, SH AF Cranmer, Steven R. Bastien, Fabienne A. Stassun, Keivan G. Saar, Steven H. TI STELLAR GRANULATION AS THE SOURCE OF HIGH-FREQUENCY FLICKER IN KEPLER LIGHT CURVES SO ASTROPHYSICAL JOURNAL LA English DT Article DE convection; stars: activity; stars: solar-type; starspots; techniques: photometric ID SOLAR-LIKE OSCILLATIONS; MAGNETIC-FIELDS; MASS STARS; CONVECTION; ASTEROSEISMOLOGY; SIMULATIONS; ROTATION; DWARFS; VARIABILITY; AMPLITUDES AB A large fraction of cool, low-mass stars exhibit brightness fluctuations that arise from a combination of convective granulation, acoustic oscillations, magnetic activity, and stellar rotation. Much of the short-timescale variability takes the form of stochastic noise, whose presence may limit the progress of extrasolar planet detection and characterization. In order to lay the groundwork for extracting useful information from these quasi-random signals, we focus on the origin of the granulation-driven component of the variability. We apply existing theoretical scaling relations to predict the star-integrated variability amplitudes for 508 stars with photometric light curves measured by the Kepler mission. We also derive an empirical correction factor that aims to account for the suppression of convection in F-dwarf stars with magnetic activity and shallow convection zones. So that we can make predictions of specific observational quantities, we performed Monte Carlo simulations of granulation light curves using a Lorentzian power spectrum. These simulations allowed us to reproduce the so-called flicker floor (i.e., a lower bound in the relationship between the full light-curve range and power in short-timescale fluctuations) that was found in the Kepler data. The Monte Carlo model also enabled us to convert the modeled fluctuation variance into a flicker amplitude directly comparable with observations. When the magnetic suppression factor described above is applied, the model reproduces the observed correlation between stellar surface gravity and flicker amplitude. Observationally validated models like these provide new and complementary evidence for a possible impact of magnetic activity on the properties of near-surface convection. C1 [Cranmer, Steven R.; Saar, Steven H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bastien, Fabienne A.; Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA Science Mission; NASA FX This paper includes data collected by the Kepler mission. Funding for Kepler is provided by the NASA Science Mission directorate. The authors gratefully acknowledge William Chaplin and John Eldridge for making their data available for use in this study. F.A.B. acknowledges support from a NASA Harriet Jenkins graduate fellowship. K.G.S. and F.A.B. acknowledge NSF AST-1009810 and NSF PAARE AST-0849736. NR 50 TC 9 Z9 9 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2014 VL 781 IS 2 AR 124 DI 10.1088/0004-637X/781/2/124 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200068 ER PT J AU Fang, GW Huang, JS Willner, SP Kong, X Wang, T Chen, Y Lin, XB AF Fang, Guanwen Huang, Jia-Sheng Willner, S. P. Kong, Xu Wang, Tao Chen, Yang Lin, Xuanbin TI SELECTION AND MID-INFRARED SPECTROSCOPY OF ULTRALUMINOUS STAR-FORMING GALAXIES AT z similar to 2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: high-redshift; galaxies: photometry; galaxies: starburst; infrared: galaxies ID DUST-OBSCURED GALAXIES; INFRARED LUMINOUS GALAXIES; SPITZER-SPACE-TELESCOPE; EXTENDED GROTH STRIP; EXTRAGALACTIC LEGACY SURVEY; ACTIVE GALACTIC NUCLEUS; HUBBLE DEEP FIELD; HIGH-REDSHIFT; MASSIVE GALAXIES; STELLAR MASS AB Starting from a sample of 24 m sources in the Extended Groth Strip, we use 3.6-8 mu m color criteria to select ultraluminous infrared galaxies (ULIRGs) at z similar to 2. Spectroscopy from 20-38 mu m of 14 objects verifies their nature and gives their redshifts. Multi-wavelength data for these objects imply stellar masses > 1011 M and star formation rates > 410 M circle dot yr(-1). Four objects of this sample observed at 1.6 mu m (rest-frame visible) with Hubble Space Telescope/WFC3 show diverse morphologies, suggesting that multiple formation processes create ULIRGs. Of the 14 objects, 4 show signs of active galactic nuclei, but the luminosity appears to be dominated by star formation in all cases. C1 [Fang, Guanwen; Kong, Xu; Chen, Yang; Lin, Xuanbin] Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Anhui, Peoples R China. [Fang, Guanwen] Dali Univ, Inst Astron & Hist Sci & Technol, Yunnan 671003, Peoples R China. [Fang, Guanwen; Wang, Tao] Nanjing Univ, Minist Educ, Key Lab Modern Astron & Astrophys, Nanjing 210093, Jiangsu, Peoples R China. [Huang, Jia-Sheng] Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China. [Huang, Jia-Sheng] Chinese Acad Sci, Camino El Observ, China Chile Joint Ctr Astron, Santiago 1515, Chile. [Huang, Jia-Sheng; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kong, Xu; Lin, Xuanbin] Chinese Acad Sci, USTC, Key Lab Res Galaxies & Cosmol, Beijing 100864, Peoples R China. [Wang, Tao] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. [Chen, Yang] SISSA, Astrophys Sect, I-34136 Trieste, Italy. RP Fang, GW (reprint author), Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Anhui, Peoples R China. EM jhuang@cfa.harvard.edu; xkong@ustc.edu.cn RI Chen, Yang/O-7911-2014 OI Chen, Yang/0000-0002-3759-1487 FU NASA through an award issued by JPL/Caltech; National Natural Science Foundation of China (NSFC) [11225315, 11373034, 11320101002, 11303002]; Chinese Universities Scientific Fund (CUSF); Specialized Research Fund for the Doctoral Program of Higher Education (SRFDP) [20123402110037]; Open Research Program of Key Laboratory for the Structure and Evolution of Celestial Objects, CAS FX We are grateful to the referee for comments which have improved this paper greatly. We thank Robert G. Abraham, Christopher J. Conselice, and Yu Dai for their valuable suggestions. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc; under NASA contract NAS5-26555. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This work was also supported by the National Natural Science Foundation of China (NSFC, No. 11225315), the Chinese Universities Scientific Fund (CUSF), and the Specialized Research Fund for the Doctoral Program of Higher Education (SRFDP, No. 20123402110037). This work was also supported by the National Natural Science Foundation of China (NSFC, Nos. 11373034, 11225315, 11320101002, and 11303002), the Open Research Program of Key Laboratory for the Structure and Evolution of Celestial Objects, CAS, the Specialized Research Fund for the Doctoral Program of Higher Education (SRFDP, No. 20123402110037), and Chinese Universities Scientific Fund (CUSF). NR 105 TC 3 Z9 4 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2014 VL 781 IS 2 AR 63 DI 10.1088/0004-637X/781/2/63 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200007 ER PT J AU Furukawa, N Ohama, A Fukuda, T Torii, K Hayakawa, T Sano, H Okuda, T Yamamoto, H Moribe, N Mizuno, A Maezawa, H Onishi, T Kawamura, A Mizuno, N Dawson, JR Dame, TM Yonekura, Y Aharonian, F Wilhelmi, ED Rowell, GP Matsumoto, R Asahina, Y Fukui, Y AF Furukawa, N. Ohama, A. Fukuda, T. Torii, K. Hayakawa, T. Sano, H. Okuda, T. Yamamoto, H. Moribe, N. Mizuno, A. Maezawa, H. Onishi, T. Kawamura, A. Mizuno, N. Dawson, J. R. Dame, T. M. Yonekura, Y. Aharonian, F. Wilhelmi, E. de Ona Rowell, G. P. Matsumoto, R. Asahina, Y. Fukui, Y. TI THE JET AND ARC MOLECULAR CLOUDS TOWARD WESTERLUND 2, RCW 49, AND HESS J1023-575; (CO)-C-12 AND (CO)-C-13 (J=2-1 and J=1-0) OBSERVATIONS WITH NANTEN2 AND MOPRA TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (jet and arc molecular clouds, HESS J1023-575); stars: individual (Westerlund 2) ID GAMMA-RAY EMISSION; REMNANT RX J1713.7-3946; GALACTIC PLANE SURVEY; HIGH-RESOLUTION RADIO; INTER-STELLAR CLOUDS; PULSAR-WIND NEBULAE; YOUNG OPEN CLUSTERS; EARLY-TYPE STARS; SUPERNOVA REMNANT; COSMIC-RAYS AB We have made new CO observations of two molecular clouds, which we call "jet" and "arc" clouds, toward the stellar cluster Westerlund 2 and the TeV gamma-ray source HESS J1023-575. The jet cloud shows a linear structure from the position of Westerlund 2 on the east. In addition, we have found a new counter jet cloud on the west. The arc cloud shows a crescent shape in the west of HESS J1023-575. A sign of star formation is found at the edge of the jet cloud and gives a constraint on the age of the jet cloud to be similar to Myr. An analysis with the multi CO transitions gives temperature as high as 20 K in a few places of the jet cloud, suggesting that some additional heating may be operating locally. The new TeV gamma-ray images by H.E.S.S. correspond to the jet and arc clouds spatially better than the giant molecular clouds associated with Westerlund 2. We suggest that the jet and arc clouds are not physically linked with Westerlund 2 but are located at a greater distance around 7.5 kpc. A microquasar with long-term activity may be able to offer a possible engine to form the jet and arc clouds and to produce the TeV gamma-rays, although none of the known microquasars have a Myr age or steady TeV gamma-rays. Alternatively, an anisotropic supernova explosion which occurred similar to Myr ago may be able to form the jet and arc clouds, whereas the TeV gamma-ray emission requires a microquasar formed after the explosion. C1 [Furukawa, N.; Ohama, A.; Fukuda, T.; Torii, K.; Hayakawa, T.; Sano, H.; Okuda, T.; Yamamoto, H.; Moribe, N.; Fukui, Y.] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Mizuno, A.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan. [Maezawa, H.; Onishi, T.] Osaka Prefecture Univ, Grad Sch Sci, Dept Astrophys, Sakai, Osaka 5998531, Japan. [Kawamura, A.; Mizuno, N.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Dawson, J. R.] Univ Tasmania, Sch Math & Phys, Sandy Bay, Tas 7005, Australia. [Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yonekura, Y.] Ibaraki Univ, Ctr Astron, Mito, Ibaraki 3108512, Japan. [Aharonian, F.] Dublin Inst Adv Studies, Dublin 2, Ireland. [Aharonian, F.; Wilhelmi, E. de Ona] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Rowell, G. P.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Matsumoto, R.; Asahina, Y.] Chiba Univ, Dept Phys, Grad Sch Sci, Inage Ku, Chiba 2638522, Japan. RP Furukawa, N (reprint author), Ibaraki Univ, Ctr Astron, 2-1-1 Bunkyo, Mito, Ibaraki 3108512, Japan. EM naoko@a.phys.nagoya-u.ac.jp; fukui@a.phys.nagoya-u.ac.jp OI de Ona Wilhelmi, Emma/0000-0002-5401-0744 FU Commonwealth of Australia; Australian Research Council; Japan Society for the Promotion of Science (JSPS) [24224005, 23403001, 23006148-01, 22740119, 22540250, 22244014, 23740149-1, R2211]; Ministry of Education, Culture, Sports, Science and Technology of Japan (MEXT); JPL/Caltech FX NANTEN2 is an international collaboration of 10 universities: Nagoya University, Osaka Prefecture University, University of Cologne, University of Bonn, Seoul National University, University of Chile, University of New South Wales, Macquarie University, University of Sydney, and University of ETH Zurich. 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. The University of New South Wales Digital Filter Bank used for the observations with the Mopra Telescope was provided with support from the Australian Research Council. This work is financially supported by Grant-in-Aid for Scientific Research (KAKENHI) from Japan Society for the Promotion of Science (JSPS) (Nos. 24224005, 23403001, 23006148-01, 22740119, 22540250, 22244014, and 23740149-1), young researcher overseas visits program for vitalizing brain circulation (no. R2211) from JSPS, and the Grant-in-Aid for Nagoya University Global COE Program, "Quest for Fundamental Principles in the Universe: From Particles to the Solar System and the Cosmos," from the Ministry of Education, Culture, Sports, Science and Technology of Japan (MEXT). This work is based in part on archival data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology under a contract with NASA. Support for this work was provided by an award issued by JPL/Caltech. NR 90 TC 2 Z9 2 U1 0 U2 0 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 FEB 1 PY 2014 VL 781 IS 2 AR 70 DI 10.1088/0004-637X/781/2/70 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200014 ER PT J AU Gianninas, A Hermes, JJ Brown, WR Dufour, P Barber, SD Kilic, M Kenyon, SJ Harrold, ST AF Gianninas, A. Hermes, J. J. Brown, Warren R. Dufour, P. Barber, Sara D. Kilic, Mukremin Kenyon, Scott J. Harrold, Samuel T. TI SDSS J074511.56+194926.5: DISCOVERY OF A METAL-RICH AND TIDALLY DISTORTED EXTREMELY LOW MASS WHITE DWARF SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; stars: abundances; stars: individual (SDSS J074511.56+194926.5); techniques: photometric; techniques: spectroscopic; white dwarfs ID 3D MODEL ATMOSPHERES; SURFACE GRAVITY DISTRIBUTION; EXTRASOLAR MINOR PLANET; DEBRIS DISKS; RADIATIVE LEVITATION; SPECTROSCOPIC ANALYSIS; CHEMICAL-COMPOSITION; MERGER SYSTEMS; SURVEY. III.; DUST DISKS AB We present the discovery of an unusual, tidally distorted extremely low mass white dwarf (WD) with nearly solar metallicity. Radial velocity measurements confirm that this is a compact binary with an orbital period of 2.6975 hr and a velocity semi-amplitude of K = 108.7 km s(-1). Analysis of the hydrogen Balmer lines yields an effective temperature of T-eff = 8380 K and a surface gravity of log g = 6.21 that in turn indicate a mass of M = 0.16 M-circle dot and a cooling age of 4.2 Gyr. In addition, a detailed analysis of the observed metal lines yields abundances of log (Mg/H) = -3.90, log(Ca/H) = -5.80, log(Ti/ H) = -6.10, log(Cr/H) = -5.60, and log(Fe/H) = -4.50, similar to the sun. We see no evidence of a debris disk from which these metals would be accreted, though the possibility cannot entirely be ruled out. Other potential mechanisms to explain the presence of heavy elements are discussed. Finally, we expect this system to ultimately undergo unstable mass transfer and merge to form a similar to 0.3-0.6 M-circle dot WD in a few Gyr. C1 [Gianninas, A.; Barber, Sara D.; Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Hermes, J. J.; Harrold, Samuel T.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Hermes, J. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Brown, Warren R.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Dufour, P.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. RP Gianninas, A (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. EM alexg@nhn.ou.edu RI Alexandros, Gianninas/B-8352-2016; OI Alexandros, Gianninas/0000-0002-8655-4308; Kenyon, Scott/0000-0003-0214-609X NR 82 TC 11 Z9 11 U1 1 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 FEB 1 PY 2014 VL 781 IS 2 AR 104 DI 10.1088/0004-637X/781/2/104 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200048 ER PT J AU Krivonos, RA Tomsick, JA Bauer, FE Baganoff, FK Barriere, NM Bodaghee, A Boggs, SE Christensen, FE Craig, WW Grefenstette, BW Hailey, CJ Harrison, FA Hong, J Madsen, KK Mori, K Nynka, M Stern, D Zhang, WW AF Krivonos, Roman A. Tomsick, John A. Bauer, Franz E. Baganoff, Frederick K. Barriere, Nicolas M. Bodaghee, Arash Boggs, Steven E. Christensen, Finn E. Craig, William W. Grefenstette, Brian W. Hailey, Charles J. Harrison, Fiona A. Hong, JaeSub Madsen, Kristin K. Mori, Kaya Nynka, Melania Stern, Daniel Zhang, William W. TI FIRST HARD X-RAY DETECTION OF THE NON-THERMAL EMISSION AROUND THE ARCHES CLUSTER: MORPHOLOGY AND SPECTRAL STUDIES WITH NuSTAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays - Galaxy; center - ISM; general - X-rays; individual (Arches cluster) ID SGR-A-ASTERISK; XMM-NEWTON OBSERVATION; GALACTIC-CENTER REGION; MOLECULAR CLOUDS; LINE EMISSION; STELLAR CLUSTERS; BRIGHTEST FLARE; MASSIVE STARS; DISCOVERY; CHANDRA AB The Arches cluster is a young, densely packed massive star cluster in our Galaxy that shows a high level of star formation activity. The nature of the extended non-thermal X-ray emission around the cluster remains unclear. The observed bright Fe Ku line emission at 6.4 keV from material that is neutral or in a low ionization state can be produced either by X-ray photoionization or by cosmic-ray particle bombardment or both. In this paper, we report on the first detection of the extended emission around the Arches cluster above 10 keV with the NuSTAR mission, and present results on its morphology and spectrum. The spatial distribution of the hard X-ray emission is found to be consistent with the broad region around the cluster where the 6.4 keV line is observed. The interpretation of the hard X-ray emission within the context of the X-ray reflection model puts a strong constraint on the luminosity of the possible illuminating hard X-ray source. The properties of the observed emission are also in broad agreement with the low-energy cosmic-ray proton excitation scenario. C1 [Krivonos, Roman A.; Tomsick, John A.; Barriere, Nicolas M.; Bodaghee, Arash; Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA. [Baganoff, Frederick K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Hailey, Charles J.; Mori, Kaya; Nynka, Melania] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hong, JaeSub] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Krivonos, RA (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM krivonos@ssl.berkeley.edu RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Madsen, Kristin/0000-0003-1252-4891; Krivonos, Roman/0000-0003-2737-5673 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. 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 (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). F. E. B. acknowledges support from Basal-CATA (PFB- 06/2007) and CONICYT- Chile (FONDECYT 1101024 and Anillo ACT1101). R. K. thanks Eugene Churazov for fruitful discussions and valuable suggestions to the paper. Facility: NuSTAR NR 50 TC 10 Z9 10 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2014 VL 781 IS 2 DI 10.1088/0004-637X/781/2/107 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200051 ER PT J AU Marion, GH Vinko, J Kirshner, RP Foley, RJ Berlind, P Bieryla, A Bloom, JS Calkins, ML Challis, P Chevalier, RA Chornock, R Culliton, C Curtis, JL Esquerdo, GA Everett, ME Falco, EE France, K Fransson, C Friedman, AS Garnavich, P Leibundgut, B Meyer, S Smith, N Soderberg, AM Sollerman, J Starr, DL Szklenar, T Takats, K Wheeler, JC AF Marion, G. H. Vinko, Jozsef Kirshner, Robert P. Foley, Ryan J. Berlind, Perry Bieryla, Allyson Bloom, Joshua S. Calkins, Michael L. Challis, Peter Chevalier, Roger A. Chornock, Ryan Culliton, Chris Curtis, Jason L. Esquerdo, Gilbert A. Everett, Mark E. Falco, Emilio E. France, Kevin Fransson, Claes Friedman, Andrew S. Garnavich, Peter Leibundgut, Bruno Meyer, Samuel Smith, Nathan Soderberg, Alicia M. Sollerman, Jesper Starr, Dan L. Szklenar, Tamas Takats, Katalin Wheeler, J. Craig TI TYPE IIb SUPERNOVA SN 2011dh: SPECTRA AND PHOTOMETRY FROM THE ULTRAVIOLET TO THE NEAR-INFRARED SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: general; supernovae: general; supernovae: individual (2011dh); ultraviolet: general ID HOBBY-EBERLY TELESCOPE; UBVRI PHOTOMETRY; IB SUPERNOVAE; MASSIVE STARS; IA SUPERNOVAE; LIGHT CURVES; X-RAY; EVOLUTION; SPECTROGRAPH; PROGENITOR AB We report spectroscopic and photometric observations of the Type IIb SN 201 ldh obtained between 4 and 34 days after the estimated date of explosion (May 31.5 UT). The data cover a wide wavelength range from 2000 angstrom in the ultraviolet (UV) to 2.4 mu m in the near-infrared (NIR). Optical spectra provide line profiles and velocity measurements of H I, He I, Call, and Fe It that trace the composition and kinematics of the supernova (SN). NIR spectra show that helium is present in the atmosphere as early as 11 days after the explosion. A UV spectrum obtained with the Space Telescope Imaging Spectrograph reveals that the UV flux for SN 2011dh is low compared to other SN IIb. Modeling the spectrum with SYNOW suggests that the UV deficit is due to line blanketing from TinH and Co II. The HI and He I velocities in SN 2011dh are separated by about 4000 km s(-1) at all phases. A velocity gap is consistent with models for a preexplosion structure in which a hydrogen-rich shell surrounds the progenitor. We estimate that the H shell of SN 2011dh is approximate to 8 times less massive than the shell of SN 1993J and approximate to 3 times more massive than the shell of SN 2008ax. Light curves (LCs) for 12 passbands are presented: UVW2, UVM2, UVW1, U, u', B, V, r', i', J, H, and Ks. In the B band, SN 2011dh reached peak brightness of 13.17 mag at 20.0 +/- 0.5 after the explosion. The maximum bolometric luminosity of 1.8 +/- 0.2 x 10(42) erg s(-1) occurred approximate to 22 days after the explosion. NIR emission provides more than 30% of the total bolometric flux at the beginning of our observations, and the NIR contribution increases to nearly 50% of the total by day 34. The UV produces 16% of the total flux on day 4, 5% on day 9, and 1% on day 34. We compare the bolometric LCs of SN 2011dh, SN 2008ax, and SN 1993J. The LC are very different for the first 12 days after the explosions, but all three SN IIb display similar peak luminosities, times of peak, decline rates, and colors after maximum. This suggests that the progenitors of these SN IIb may have had similar compositions and masses, but they exploded inside hydrogen shells that have a wide range of masses. SN 2011dh was well observed, and a likely progenitor star has been identified in preexplosion images. The detailed observations presented here will help evaluate theoretical models for this SN and lead to a better understanding of SN IIb. C1 [Marion, G. H.; Kirshner, Robert P.; Foley, Ryan J.; Berlind, Perry; Bieryla, Allyson; Calkins, Michael L.; Challis, Peter; Chornock, Ryan; Esquerdo, Gilbert A.; Falco, Emilio E.; Friedman, Andrew S.; Meyer, Samuel; Soderberg, Alicia M.; Szklenar, Tamas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marion, G. H.; Vinko, Jozsef; Wheeler, J. Craig] Univ Texas Austin, Austin, TX 78712 USA. [Vinko, Jozsef; Takats, Katalin] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Bloom, Joshua S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Chevalier, Roger A.; Starr, Dan L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Culliton, Chris; Curtis, Jason L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [France, Kevin] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Fransson, Claes] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Garnavich, Peter; Sollerman, Jesper] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Leibundgut, Bruno] European So Observ, D-85748 Garching, Germany. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Takats, Katalin] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. RP Marion, GH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gmarion@cfa.harvard.edu RI Friedman, Andrew/I-4691-2013; OI Friedman, Andrew/0000-0003-1334-039X; Sollerman, Jesper/0000-0003-1546-6615 FU NSF [AST-1211196, AST-0707769, AST-1109801]; Harvard College Observatory; National Science Foundation [NSF PHY-1125915]; Hungarian OTKA grants [K-76816, NN-107637]; Texas Advanced Research Project [ARP-009]; NASA Graduate Research Program Fellowship; NASA through a grant from the Space Telescope Science Institute [GO-12540]; NASA [NAS5-26555] FX The CfA Supernova Program is supported by NSF grant AST-1211196 to the Harvard College Observatory. R.P.K. was supported in part by the National Science Foundation under grant NSF PHY-1125915 to the Kavli Institute for Theoretical Physics. J.V. is supported by Hungarian OTKA grants K-76816 and NN-107637, NSF grant AST-0707769, and Texas Advanced Research Project ARP-009. J.C.W. is supported by NSF grant AST-1109801. A.S.F acknowledges support from a NSF Graduate Research Fellowship and a NASA Graduate Research Program Fellowship. Support for program GO-12540 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. K.T. has also received support from Hungarian OTKA grant K-76816. NR 69 TC 21 Z9 21 U1 1 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 FEB 1 PY 2014 VL 781 IS 2 AR 69 DI 10.1088/0004-637X/781/2/69 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200013 ER PT J AU Neufeld, DA Gusdorf, A Gusten, R Herczeg, GJ Kristensen, L Melnick, GJ Nisini, B Ossenkopf, V Tafalla, M van Dishoeck, EF AF Neufeld, David A. Gusdorf, Antoine Guesten, Rolf Herczeg, Greg J. Kristensen, Lars Melnick, Gary J. Nisini, Brunella Ossenkopf, Volker Tafalla, Mario van Dishoeck, Ewine F. TI THE WATER ABUNDANCE BEHIND INTERSTELLAR SHOCKS: RESULTS FROM HERSCHEL/PACS AND SPITZER/IRS OBSERVATIONS OF H(2)0, CO, AND H-2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; ISM: abundances; ISM: molecules; molecular processes; shock waves ID SUPERNOVA-REMNANTS; MAGNETOHYDRODYNAMIC SHOCKS; MOLECULAR GAS; BASIC DATA; OH MASERS; EMISSION; EXCITATION; WAVES; ASTRONOMY; CHEMISTRY AB We have investigated the water abundance in shock-heated molecular gas, making use of Herschel measurements of far-infrared (IR) CO and H2O line emissions in combination with Spitzer measurements of mid-IR H-2 rotational emissions. We present far-IR line spectra obtained with Herschel's Photodetector Array Camera and Spectrometer instrument in range spectroscopy mode toward two positions in the protostellar outflow NGC 2071 and one position each in the supernova remnants W28 and 3C391. These spectra provide unequivocal detections, at one or more positions, of 12 rotational lines of water, 14 rotational lines of CO, 8 rotational lines of OH (4 lambda doublets), and 7 fine-structure transitions of atoms or atomic ions. We first used a simultaneous fit to the CO line fluxes, along with H2 rotational line fluxes measured previously by Spitzer, to constrain the temperature and density distribution within the emitting gas; we then investigated the water abundances implied by the observed H(2)0 line fluxes. The water line fluxes are in acceptable agreement with standard theoretical models for nondissociative shocks that predict the complete vaporization of grain mantles in shocks of velocity v similar to 25 km s(-1), behind which the characteristic gas temperature is similar to 1300 K and the H(2)0/CO ratio is 1.2 C1 [Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Gusdorf, Antoine] Ecole Normale Super, LERMA, UMR CNRS 8112, Observ Paris, F-75005 Paris, France. [Guesten, Rolf] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Herczeg, Greg J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Kristensen, Lars; Melnick, Gary J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nisini, Brunella] Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. [Ossenkopf, Volker] Univ Cologne, Inst Phys, D-50937 Cologne, Germany. [Tafalla, Mario] Observ Astron Nacl IGN, E-28014 Madrid, Spain. [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 Neufeld, DA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. RI Kristensen, Lars/F-4774-2011; OI Kristensen, Lars/0000-0003-1159-3721; Herczeg, Gregory/0000-0002-7154-6065; , Brunella Nisini/0000-0002-9190-0113 NR 50 TC 12 Z9 12 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2014 VL 781 IS 2 AR 102 DI 10.1088/0004-637X/781/2/102 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200046 ER PT J AU Sanna, A Reid, MJ Menten, KM Dame, TM Zhang, B Sato, M Brunthaler, A Moscadelli, L Immer, K AF Sanna, A. Reid, M. J. Menten, K. M. Dame, T. M. Zhang, B. Sato, M. Brunthaler, A. Moscadelli, L. Immer, K. TI TRIGONOMETRIC PARALLAXES TO STAR-FORMING REGIONS WITHIN 4 kpc OF THE GALACTIC CENTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry - Galaxy; kinematics and dynamics - masers - techniques; high angular resolution ID ON SPIRAL GALAXIES; MILKY-WAY GALAXY; GAS-DYNAMICS; DUST LANES; FUNDAMENTAL PARAMETERS; MOLECULAR CLOUDS; BAR DIAGNOSTICS; CO SURVEY; ARM; ABSORPTION AB We report four trigonometric parallaxes for high-mass star-forming regions within 4 kpc of the Galactic center. These measurements were made with the Very Long Baseline Array as part of the BeSSeL Survey. By associating these sources kinematically with large-scale features in CO and H I longitude-velocity diagrams, we begin to outline some major features of the inner Milky Way: the Connecting arm, the near and far 3 kpc arms, and the Norma arm. The Connecting arm in the first Galactic quadrant lies closer to the Galactic center than the far 3 kpc arm and is offset by the long-bar's major axis near its leading edge, supporting the presence of an inner Lindblad resonance. Assuming the 3 kpc arms are a continuous physical structure, the relative Galactocentric distance of its near and far sides suggests highly elliptical streamlines of gas around the bar(s) and a bar corotation radius, rCR greater than or similar to 3.6 kpc. At a Galactic longitude near 10 degrees and a heliocentric distance of about 5 kpc, the near 3 kpc arm and the Norma arm intersect on a face-on view of our Galaxy, while passing at different Galactic latitudes. We provide an accurate distance measurement to the W 31 star-forming complex of 4.95(-0.43)(+0.51) kpc from the Sun, which associates it with a bright CO feature belonging to the near 3 kpc arm. C1 [Sanna, A.; Menten, K. M.; Zhang, B.; Sato, M.; Brunthaler, A.; Immer, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, M. J.; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Moscadelli, L.] INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Sanna, A (reprint author), Max Planck Inst Radioastron, Huigel 69, D-53121 Bonn, Germany. EM asanna@mpifr-bonn.mpg.de OI Moscadelli, Luca/0000-0002-8517-8881 NR 60 TC 36 Z9 36 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2014 VL 781 IS 2 DI 10.1088/0004-637X/781/2/108 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200052 ER PT J AU Xu, YD Yue, B Su, M Fan, ZH Chen, XL AF Xu, Yidong Yue, Bin Su, Meng Fan, Zuhui Chen, Xuelei TI AN ANALYTICAL MODEL OF THE LARGE NEUTRAL REGIONS DURING THE LATE STAGE OF REIONIZATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; dark ages, reionization, first stars; intergalactic medium; large-scale structure of universe; methods: analytical ID SIMILAR-TO 8; EXCURSION SET FORMALISM; LYMAN-BREAK GALAXIES; LY-ALPHA FOREST; LUMINOSITY FUNCTION; COSMIC REIONIZATION; HIGH-REDSHIFT; BUBBLE-GROWTH; BRIGHT-END; CORRELATED STEPS AB In this paper, we investigate the nature and distribution of large neutral regions during the late epoch of reionization. In the "bubble model" of reionization, the mass distribution of large ionized regions ("bubbles") during the early stage of reionization is obtained by using the excursion set model, where the ionization of a region corresponds to the first up-crossing of a barrier by random trajectories. We generalize this idea and develop a method to predict the distribution of large-scale neutral regions during the late stage of reionization, taking into account the ionizing background after the percolation of H In regions. The large-scale neutral regions, which we call "neutral islands," are not individual galaxies or minihalos, but larger regions where fewer galaxies formed and hence ionized later and they are identified in the excursion set model with the first down-crossings of the island barrier. Assuming that the consumption rate of ionizing background photons is proportional to the surface area of the neutral islands, we obtained the size distribution of the neutral islands. We also take the "bubbles-in-island" effect into account by considering the conditional probability of up-crossing a bubble barrier after down-crossing the island barrier. We find that this effect is very important. An additional barrier is set to avoid islands being percolated through. We find that there is a characteristic scale for the neutral islands, while the small islands are rapidly swallowed up by the ionizing background; this characteristic scale does not change much as the reionization proceeds. C1 [Xu, Yidong; Yue, Bin; Chen, Xuelei] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Su, Meng] MIT, Dept Phys, Cambridge, MA 02139 USA. [Su, Meng] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Su, Meng] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Fan, Zuhui] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Chen, Xuelei] Peking Univ, Ctr High Energy Phys, Beijing 100871, Peoples R China. RP Xu, YD (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. FU Ministry of Science and Technology 863 project grant [2012AA121701]; NSFC [11073024, 11173001, 11033005]; John Templeton foundation; China Postdoctoral Science Foundation; Young Researcher Grant of the National Astronomical Observatories, Chinese Academy of Sciences; NASA through an Einstein Postdoctoral Fellowship [PF2-130102]; Chandra X-ray Center; NASA [NAS8-03060] FX We deeply appreciate the insight of the referee and their constructive comments. We thank Jun Zhang, Jie Zhou, Hy Trac, and Renyue Cen for many helpful discussions. This work is supported by the Ministry of Science and Technology 863 project grant 2012AA121701, the NSFC grant 11073024, and the John Templeton foundation. Y.X. is supported by the China Postdoctoral Science Foundation and by the Young Researcher Grant of the National Astronomical Observatories, Chinese Academy of Sciences. Support for the work of M.S. was provided by NASA through an Einstein Postdoctoral Fellowship grant number PF2-130102 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. Z.F is supported by NSFC under grant 11173001 and 11033005. NR 64 TC 4 Z9 4 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2014 VL 781 IS 2 AR 97 DI 10.1088/0004-637X/781/2/97 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200041 ER PT J AU Zhang, B Moscadelli, L Sato, M Reid, MJ Menten, KM Zheng, XW Brunthaler, A Dame, TM Xu, Y Immer, K AF Zhang, B. Moscadelli, L. Sato, M. Reid, M. J. Menten, K. M. Zheng, X. W. Brunthaler, A. Dame, T. M. Xu, Y. Immer, K. TI THE PARALLAX OF W43: A MASSIVE STAR-FORMING COMPLEX NEAR THE GALACTIC BAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: kinematics and dynamics; masers; stars: formation; stars: individual (W43); techniques: high angular resolution ID H-II REGIONS; GHZ METHANOL MASERS; BASE-LINE INTERFEROMETRY; MILKY-WAY; TRIGONOMETRIC PARALLAXES; VLBI OBSERVATIONS; MOLECULAR CLOUDS; SPIRAL STRUCTURE; BESSEL SURVEY; INNER GALAXY AB We report trigonometric parallax measurements of masers in the massive star-forming complex W43 from Very Long Baseline Array observations as part of the Bar and Spiral Structure Legacy Survey. Based on measurements of three 12 GHz methanol maser sources (G029.86-00.04, G029.95-00.01, and G031.28+00.06) and one 22 GHz water maser source (G031.58+ 00.07) toward W43, we derived a distance of 5.49(-0.34)(+0.39) kpc to W43. By associating the masers with CO molecular clouds, and associating the clouds kinematically with CO longitude-velocity spiral features, we assign W43 to the Scutum spiral arm, close to the near end of the Galactic bar. The peculiar motion of W43 is about 20 km s(-1) toward the Galactic Center and is very likely induced by the gravitational attraction of the bar. C1 [Zhang, B.; Sato, M.; Menten, K. M.; Brunthaler, A.; Immer, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Zhang, B.] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Moscadelli, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Reid, M. J.; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zheng, X. W.] Nanjing Univ, Dept Astron, Nanjing 210093, Jiangsu, Peoples R China. [Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. RP Zhang, B (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. OI Moscadelli, Luca/0000-0002-8517-8881 FU National Science Foundation of China [10921063, 11073046, 11073054, 11133008]; Key Laboratory for Radio Astronomy, Chinese Academy of Sciences; ERC [247078] FX The work was supported by the National Science Foundation of China (under grants 10921063, 11073046, 11073054, and 11133008) and the Key Laboratory for Radio Astronomy, Chinese Academy of Sciences. This work was partially funded by the ERC Advanced Investigator Grant GLOSTAR (247078). We are grateful to Dr. James Urquhart for providing the ATLASGAL FITS files. NR 45 TC 27 Z9 27 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2014 VL 781 IS 2 AR 89 DI 10.1088/0004-637X/781/2/89 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA5WV UT WOS:000331171200033 ER PT J AU Zipkin, EF Sillett, TS Grant, EHC Chandler, RB Royle, JA AF Zipkin, Elise F. Sillett, T. Scott Grant, Evan H. Campbell Chandler, Richard B. Royle, J. Andrew TI Inferences about population dynamics from count data using multistate models: a comparison to capture-recapture approaches SO ECOLOGY AND EVOLUTION LA English DT Article ID JOLLY-SEBER MODEL; MIGRATORY SONGBIRD; DEMOGRAPHIC PARAMETERS; STRUCTURED POPULATION; BREEDING PROPORTIONS; WILDLIFE POPULATIONS; DENSITY-DEPENDENCE; MARKED ANIMALS; LONG-TERM; RATES C1 [Zipkin, Elise F.; Royle, J. Andrew] USGS Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. [Sillett, T. Scott] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Grant, Evan H. Campbell] USGS Patuxent Wildlife Res Ctr, Conte Anadromous Fish Lab, Turners Falls, MA 01376 USA. [Chandler, Richard B.] Univ Georgia, Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA. RP Zipkin, EF (reprint author), USGS Patuxent Wildlife Res Ctr, 12100 Beech Forest Rd, Laurel, MD 20708 USA. EM ezipkin@msu.edu RI Chandler, Richard/D-8831-2014; Grant, Evan/N-5160-2014; Chandler, Richard/F-9702-2016; OI Grant, Evan/0000-0003-4401-6496; Royle, Jeffrey/0000-0003-3135-2167 FU John Wesley Powell Center for Analysis and Synthesis; US Geological Survey; U.S. National Science Foundation FX Working Group supported by the John Wesley Powell Center for Analysis and Synthesis, funded by the US Geological Survey. Fieldwork was funded by U.S. National Science Foundation grants to R. T. Holmes (Dartmouth College), N. L. Rodenhouse (Wellesley College), TSS, and M. S. Webster (Cornell University). NR 51 TC 7 Z9 7 U1 3 U2 53 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD FEB PY 2014 VL 4 IS 4 BP 417 EP 426 PG 10 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA AA8OJ UT WOS:000331354500009 PM 24634726 ER PT J AU DiMichele, WA AF DiMichele, William A. TI WETLAND-DRYLAND VEGETATIONAL DYNAMICS IN THE PENNSYLVANIAN ICE AGE TROPICS SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Review DE Pennsylvanian; tropics; upland; Coal Age; paleoecology; climate; biodiversity ID CENTRAL APPALACHIAN BASIN; SAAR-NAHE BASIN; LATE PALEOZOIC CONIFERS; COAL-SWAMP VEGETATION; EASTERN UNITED-STATES; PLANT-FOSSIL RECORD; VOLCANIC ASH-FALL; SEA-LEVEL CHANGES; NOVA-SCOTIA; CLIMATE-CHANGE AB Premise of research.The Late Paleozoic Ice Age was the last extensive pre-Pleistocene ice age. It includes many climate changes of different intensities, permitting examination of many and varied biotic responses. The tropical Pennsylvanian Subperiod, usually visualized as one vast wetland coal forest, in fact also was dominated, periodically, by seasonally dry vegetation that, in turn, covered most of the central and western Pangean supercontinent. Equatorial wetland and dryland biomes oscillated during single glacial-interglacial cycles. This recognition changes understanding of the Coal Age tropics; examination of their spatiotemporal patterns indicates that these vegetation types responded differently to global environmental disturbances and long-term trends and points to potentially different underlying controls on evolutionary histories of their component lineages.Methodology.This study is based on the published literature and on examination of geological exposures and fossil floras, mainly from North America but also from other parts of the world.Pivotal results.Wetlands and seasonally dry habitats were equally part of the Coal Age Pangean tropics. They dominated these landscapes at different times, under different climatic regimes. Wetland vegetation was likely forced into refugia during seasonally dry (subhumid to semiarid) parts of glacial-interglacial cycles; it reemerged/reassembled during wet (humid to perhumid) periods. Seasonally dry vegetation resided permanently in areas of western and central Pangea and in microhabitats within the Central Pangean Mountains. Both floras had lower biodiversity than modern floras in similar habitats. The wetland flora species pool was more phylogenetically disparate than any modern vegetation. In contrast, seasonally dry floras were dominated by seed plants. These biomes responded differently to acute environmental changes and chronic long-term aridification.Conclusions.From ecological or evolutionary perspectives, the present-day world is but one possibility. Lower-diversity worlds such as the late Paleozoic, with a rich spectrum of environmental variations, offer insights into relationships between organisms and environments that expand understanding of these phenomena and enlarge our sense of what is possible or probable as we look to the future. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP DiMichele, WA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. EM dimichel@si.edu FU Smithsonian Institution; National Museum of Natural History; National Science Foundation; Bureau of Land Management FX I would like to extend particular thanks to Tom Phillips, Blaine Cecil, Isabel Montanez, and John Nelson, who, over many years, have contributed extensively to my understanding of the late Paleozoic world-they bear no responsibility for my misunderstandings or misinterpretations. Sincere thanks to Mary Parrish, Paleobiology Department, NMNH, for preparation of the artwork. I also owe a great deal to Alan Archer, Arden Bashforth, Richard Bateman, Dan Chaney, Peter Crane, Scott Elrick, Howard Falcon-Lang, Robert Gastaldo, Martin Gibling, Robert Hook, Hans Kerp, Cindy Looy, Spencer Lucas, Hermann Pfefferkorn, Chris Poulsen, and Neil Tabor for discussion of many and various matters and for freely sharing their ideas. Arden Bashforth's reading of this article is gratefully acknowledged. The comments of Hermann Pfefferkorn and two anonymous reviewers improved the article significantly. Appreciation is extended to Pat Herendeen for the invitation to write this review and for his patience while it was being completed. Much of the fieldwork that undergirds this discussion was financed by various grants from the Smithsonian Institution, the National Museum of Natural History, the National Science Foundation, and the Bureau of Land Management. NR 433 TC 28 Z9 28 U1 8 U2 37 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 EI 1537-5315 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD FEB 1 PY 2014 VL 175 IS 2 SI SI BP 123 EP 164 DI 10.1086/675235 PG 42 WC Plant Sciences SC Plant Sciences GA AA6VL UT WOS:000331236200001 ER PT J AU Jernigan, CM Roubik, DW Wcislo, WT Riveros, AJ AF Jernigan, C. M. Roubik, D. W. Wcislo, W. T. Riveros, A. J. TI Color-dependent learning in restrained Africanized honey bees SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE Apis mellifera; Classical conditioning; Proboscis extension response ID APIS-MELLIFERA L; PROBOSCIS EXTENSION; CONDITIONED-RESPONSE; SHORT-TERM; MEMORY; DISCRIMINATION; BUMBLEBEES; PREFERENCES; CONSTANCY; VISION AB Associative color learning has been demonstrated to be very poor using restrained European honey bees unless the antennae are amputated. Consequently, our understanding of proximate mechanisms in visual information processing is handicapped. Here we test learning performance of Africanized honey bees under restrained conditions with visual and olfactory stimulation using the proboscis extension response (PER) protocol. Restrained individuals were trained to learn an association between a color stimulus and a sugar-water reward. We evaluated performance for 'absolute' learning (learned association between a stimulus and a reward) and 'discriminant' learning (discrimination between two stimuli). Restrained Africanized honey bees (AHBs) readily learned the association of color stimulus for both blue and green LED stimuli in absolute and discriminatory learning tasks within seven presentations, but not with violet as the rewarded color. Additionally, 24-h memory improved considerably during the discrimination task, compared with absolute association (15-55%). We found that antennal amputation was unnecessary and reduced performance in AHBs. Thus color learning can now be studied using the PER protocol with intact AHBs. This finding opens the way towards investigating visual and multimodal learning with application of neural techniques commonly used in restrained honey bees. C1 [Jernigan, C. M.; Roubik, D. W.; Wcislo, W. T.; Riveros, A. J.] Smithsonian Trop Res Inst, Balboa, Panama. [Jernigan, C. M.] Butler Univ, Dept Biol Sci, Indianapolis, IN 46208 USA. [Riveros, A. J.] Pontificia Univ Javeriana, Dept Ciencias Fisiol, Bogota, Colombia. RP Riveros, AJ (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM andre.riveros@javeriana.edu.co FU Smithsonian Tropical Research Institute (STRI); Butler University; Office of Education of STRI; Latin American Scholar fellowship of the STRI; Scholarly Studies Grant of the Smithsonian Institution; Smithsonian Institution FX C.M.J. was supported by a collaborative internship of the Smithsonian Tropical Research Institute (STRI) and Butler University, and by generous support of the Office of Education of STRI. A.J.R. was supported by a Latin American Scholar fellowship of the STRI and by a Scholarly Studies Grant of the Smithsonian Institution (PI: William Eberhard). This project was generally supported by funds of the Smithsonian Institution to W.T.W. and C.M.J. NR 56 TC 4 Z9 4 U1 0 U2 14 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 EI 1477-9145 J9 J EXP BIOL JI J. Exp. Biol. PD FEB PY 2014 VL 217 IS 3 BP 337 EP 343 DI 10.1242/jeb.091355 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AA6JH UT WOS:000331204100013 PM 24072797 ER PT J AU Merow, C Dahlgren, JP Metcalf, CJE Childs, DZ Evans, MEK Jongejans, E Record, S Rees, M Salguero-Gomez, R McMahon, SM AF Merow, Cory Dahlgren, Johan P. Metcalf, C. Jessica E. Childs, Dylan Z. Evans, Margaret E. K. Jongejans, Eelke Record, Sydne Rees, Mark Salguero-Gomez, Roberto McMahon, Sean M. TI Advancing population ecology with integral projection models: a practical guide SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Review ID EVOLUTIONARY DEMOGRAPHY; LIFE-HISTORY; MONOCARPIC PERENNIALS; FLOWERING STRATEGIES; ENVIRONMENTAL-CHANGE; SENSITIVITY-ANALYSIS; DYNAMICS; GROWTH; SIZE; PLANTS C1 [Merow, Cory; McMahon, Sean M.] Smithsonian Environm Res Ctr, Edgewater, MD 21307 USA. [Merow, Cory] Univ Connecticut, Storrs, CT 06269 USA. [Dahlgren, Johan P.] Stockholm Univ, Dept Ecol Environm & Plant Sci, S-10691 Stockholm, Sweden. [Dahlgren, Johan P.] Univ Southern Denmark, Dept Biol, Odense, Denmark. [Dahlgren, Johan P.] Univ Southern Denmark, Max Planck Odense Ctr Biodemog Aging, Odense, Denmark. [Metcalf, C. Jessica E.] Univ Oxford, Dept Zool, Oxford OX1 3PS, England. [Metcalf, C. Jessica E.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Childs, Dylan Z.; Rees, Mark] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. [Evans, Margaret E. K.] Univ Arizona, Tree Ring Res Lab, Tucson, AZ 85721 USA. [Evans, Margaret E. K.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ USA. [Jongejans, Eelke] Radboud Univ Nijmegen, Dept Anim Ecol & Ecophysiol, Inst Water & Wetland Res, NL-6525 ED Nijmegen, Netherlands. [Record, Sydne] Harvard Univ, Harvard Forest, Petersham, MA USA. [Salguero-Gomez, Roberto] Max Planck Inst Demog Res, Evolutionary Demog Lab, Rostock, Germany. [Salguero-Gomez, Roberto] Univ Queensland, Ctr Biodivers & Conservat Sci, St Lucia, Qld, Australia. RP Merow, C (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21307 USA. EM cory.merow@gmail.com RI Jongejans, Eelke/B-4832-2008 OI Jongejans, Eelke/0000-0003-1148-7419 FU NSF [1046328, 1137366]; Evolutionary Demography laboratory; Modeling the Evolution of Aging-independent group of the MPIDR; Netherlands Organization for Scientific Research (NWO-meerwaarde Grant) [840.11.001]; Natural Environment Research Council [NE/I022027/1] FX This paper originated during a working group on IPMs hosted at the Max Plank Institute for Demographic Research (MPIDR; Rostock, Germany). We thank Florence Nicole for providing data for Appendices A and G. C. M. acknowledges funding from NSF Grant 1046328 and NSF Grant 1137366. R. S.-G, C.J.E.M, S. M, C. M. and E.J. acknowledge financial support for the working group from the Evolutionary Demography laboratory and Modeling the Evolution of Aging-independent group of the MPIDR. E.J. further acknowledges financial support from the Netherlands Organization for Scientific Research (NWO-meerwaarde Grant 840.11.001). DZC acknowledges support from the Natural Environment Research Council (NE/I022027/1). NR 66 TC 40 Z9 40 U1 22 U2 193 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 FEB PY 2014 VL 5 IS 2 BP 99 EP 110 PG 12 WC Ecology SC Environmental Sciences & Ecology GA AA9GO UT WOS:000331402000001 ER PT J AU Elvis, M AF Elvis, Martin TI The case for applied astronomy SO ASTRONOMY & GEOPHYSICS LA English DT Article C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 2 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1366-8781 EI 1468-4004 J9 ASTRON GEOPHYS JI Astron. Geophys. PD FEB PY 2014 VL 55 IS 1 BP 11 EP 12 PG 2 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA AA1CN UT WOS:000330834000019 ER PT J AU Brooke, JSA Ram, RS Western, CM Li, G Schwenke, DW Bernath, PF AF Brooke, James S. A. Ram, Ram S. Western, Colin M. Li, Gang Schwenke, David W. Bernath, Peter F. TI EINSTEIN A COEFFICIENTS AND OSCILLATOR STRENGTHS FOR THE A(2)Pi-X-2 Sigma(+) (RED) AND B-2 Sigma(+)-X-2 Sigma(+) (VIOLET) SYSTEMS AND ROVIBRATIONAL TRANSITIONS IN THE X-2 Sigma(+) STATE OF CN SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astronomical databases: miscellaneous; methods: laboratory: molecular; molecular data; opacity stars: abundances; techniques: spectroscopic ID TRANSFORM EMISSION-SPECTROSCOPY; TAIL BAND SYSTEM; CONFIGURATION-INTERACTION CALCULATIONS; DIPOLE-MOMENT FUNCTION; RADIATIVE LIFETIMES; INTERSTELLAR CN; ROTATIONAL PERTURBATIONS; PROJECTION OPERATORS; MOLECULAR-PROPERTIES; INFRARED-SPECTRUM AB Line strengths have been calculated in the form of Einstein A coefficients and f-values for a large number of bands of the A(2)Pi-X-2 Sigma(+) and B-2 Sigma(+)-X-2 Sigma(+) systems and rovibrational transitions within the X-2 Sigma(+) state of CN using Western's pgopher program. The J dependence of the transition dipole moment matrix elements (the Herman-Wallis effect) has been taken into account. Rydberg-Klein-Rees potential energy functions for the A(2)Pi, B-2 Sigma(+), and X-2 Sigma(+) states were computed using spectroscopic constants from the A(2)Pi-X-2 Sigma(+) and B-2 Sigma(+)-X-2 Sigma(+) transitions. New electronic transition dipole moment functions for these systems and a dipole moment function for the X-2 Sigma(+) state were generated from high level ab initio calculations and have been used in Le Roy's level program to produce transition dipole moment matrix elements (including their J dependence) for a large number of vibrational bands. The program pgopher was used to calculate Einstein A coefficients, and a line list was generated containing the observed and calculated wavenumbers, Einstein A coefficients and f-values for 290 bands of the A(2)Pi-X-2 Sigma(+) transition with v' = 0-22, v '' = 0-15, 250 bands of the B-2 Sigma(+)-X-2 Sigma(+) transition with v' = 0-15, v '' = 0-15 and 120 bands of the rovibrational transitions within the X-2 Sigma(+) state with v = 0-15. The Einstein A coefficients have been used to compute radiative lifetimes of several vibrational levels of the A(2)Pi and B-2 Sigma(+) states and the values compared with those available from previous experimental and theoretical studies. C1 [Brooke, James S. A.; Ram, Ram S.; Bernath, Peter F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Western, Colin M.] Univ Bristol, Sch Chem, Bristol BS8 1TS, Avon, England. [Li, Gang] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schwenke, David W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bernath, Peter F.] Old Dominion Univ, Dept Chem & Biochem, Norfolk, VA 23529 USA. RP Brooke, JSA (reprint author), Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. EM jsabrooke@gmail.com RI Bernath, Peter/B-6567-2012; schwenke, david/I-3564-2013; Li, Gang/P-2272-2015 OI Bernath, Peter/0000-0002-1255-396X; Li, Gang/0000-0002-5605-7896 FU Leverhulme Trust of UK; NASA laboratory astrophysics program FX The research described here was supported by funding from the Leverhulme Trust of UK and the NASA laboratory astrophysics program. The spectra used in this work were recorded at the National Solar Observatory at Kitt Peak, USA. NR 90 TC 25 Z9 25 U1 3 U2 25 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 FEB PY 2014 VL 210 IS 2 AR 23 DI 10.1088/0067-0049/210/2/23 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA6WN UT WOS:000331239000009 ER PT J AU Burke, CJ Bryson, ST Mullally, F Rowe, JF Christiansen, JL Thompson, SE Coughlin, JL Haas, MR Batalha, NM Caldwell, DA Jenkins, JM Still, M Barclay, T Borucki, WJ Chaplin, WJ Ciardi, DR Clarke, BD Cochran, WD Demory, BO Esquerdo, GA Gautier, TN Gilliland, RL Girouard, FR Havel, M Henze, CE Howell, SB Huber, D Latham, DW Li, J Morehead, RC Morton, TD Pepper, J Quintana, E Ragozzine, D Seader, SE Shah, Y Shporer, A Tenenbaum, P Twicken, JD Wolfgang, A AF Burke, Christopher J. Bryson, Stephen T. Mullally, F. Rowe, Jason F. Christiansen, Jessie L. Thompson, Susan E. Coughlin, Jeffrey L. Haas, Michael R. Batalha, Natalie M. Caldwell, Douglas A. Jenkins, Jon M. Still, Martin Barclay, Thomas Borucki, William J. Chaplin, William J. Ciardi, David R. Clarke, Bruce D. Cochran, William D. Demory, Brice-Olivier Esquerdo, Gilbert A. Gautier, Thomas N., III Gilliland, Ronald L. Girouard, Forrest R. Havel, Mathieu Henze, Christopher E. Howell, Steve B. Huber, Daniel Latham, David W. Li, Jie Morehead, Robert C. Morton, Timothy D. Pepper, Joshua Quintana, Elisa Ragozzine, Darin Seader, Shawn E. Shah, Yash Shporer, Avi Tenenbaum, Peter Twicken, Joseph D. Wolfgang, Angie TI PLANETARY CANDIDATES OBSERVED BY KEPLER IV: PLANET SAMPLE FROM Q1-Q8 (22 MONTHS) SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; eclipses; planetary systems; space vehicles ID TRANSIT TIMING OBSERVATIONS; SUN-LIKE STAR; 1ST 4 MONTHS; HABITABLE ZONE; LIGHT CURVES; ECLIPSING BINARIES; ERROR-CORRECTION; FALSE POSITIVES; BLEND SCENARIOS; MULTIPLE SYSTEM AB We provide updates to the Kepler planet candidate sample based upon nearly two years of high-precision photometry (i.e., Q1-Q8). From an initial list of nearly 13,400 threshold crossing events, 480 new host stars are identified from their flux time series as consistent with hosting transiting planets. Potential transit signals are subjected to further analysis using the pixel-level data, which allows background eclipsing binaries to be identified through small image position shifts during transit. We also re-evaluate Kepler Objects of Interest (KOIs) 1-1609, which were identified early in the mission, using substantially more data to test for background false positives and to find additional multiple systems. Combining the new and previous KOI samples, we provide updated parameters for 2738 Kepler planet candidates distributed across 2017 host stars. From the combined Kepler planet candidates, 472 are new from the Q1-Q8 data examined in this study. The new Kepler planet candidates represent similar to 40% of the sample with R-P similar to 1R(circle plus) and represent similar to 40% of the low equilibrium temperature (T-eq < 300 K) sample. We review the known biases in the current sample of Kepler planet candidates relevant to evaluating planet population statistics with the current Kepler planet candidate sample. C1 [Burke, Christopher J.; Mullally, F.; Rowe, Jason F.; Thompson, Susan E.; Coughlin, Jeffrey L.; Caldwell, Douglas A.; Jenkins, Jon M.; Li, Jie; Quintana, Elisa; Seader, Shawn E.; Tenenbaum, Peter; Twicken, Joseph D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bryson, Stephen T.; Haas, Michael R.; Batalha, Natalie M.; Borucki, William J.; Havel, Mathieu; Henze, Christopher E.; Howell, Steve B.; Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Christiansen, Jessie L.; Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Still, Martin; Barclay, Thomas] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Chaplin, William J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Chaplin, William J.] Aarhus Univ, SAC, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Clarke, Bruce D.; Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cochran, William D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Demory, Brice-Olivier] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Esquerdo, Gilbert A.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Girouard, Forrest R.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Morehead, Robert C.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Morton, Timothy D.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Pepper, Joshua] Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA. [Pepper, Joshua] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Ragozzine, Darin] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Shah, Yash] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Wolfgang, Angie] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Burke, CJ (reprint author), NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. EM christopher.j.burke@nasa.gov RI Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Ciardi, David/0000-0002-5741-3047; Demory, Brice-Olivier/0000-0002-9355-5165; Pepper, Joshua/0000-0002-3827-8417 FU NASA Postdoctoral Program at Ames Research Center FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. M.H. and D.H. are supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 70 TC 124 Z9 124 U1 2 U2 9 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 FEB PY 2014 VL 210 IS 2 AR 19 DI 10.1088/0067-0049/210/2/19 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA6WN UT WOS:000331239000005 ER PT J AU Jonker, PG Torres, MAP Hynes, RI Maccarone, TJ Steeghs, D Greiss, S Britt, CT Wu, JF Johnson, CB Nelemans, G Heinke, C AF Jonker, Peter G. Torres, Manuel A. P. Hynes, Robert I. Maccarone, Thomas J. Steeghs, Danny Greiss, Sandra Britt, Christopher T. Wu, Jianfeng Johnson, Christopher B. Nelemans, Gijs Heinke, Craig TI THE GALACTIC BULGE SURVEY: COMPLETION OF THE X-RAY SURVEY OBSERVATIONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE accretion, accretion disks; binaries: symbiotic; novae, cataclysmic variables; stars: activity; X-rays: binaries ID MASS-DISTRIBUTION; SOURCE CATALOG; BLACK-HOLES; EXPLOSION MECHANISM; ROSAT OBSERVATIONS; HIGH-RESOLUTION; ORBITAL PERIOD; NEUTRON-STARS; CENTER REGION; MILKY-WAY AB We provide the Chandra source list for the last similar to quarter of the area covered by the Galactic Bulge Survey (GBS). The GBS targets two strips of 6 degrees x 1 degrees (12 square degrees in total), one above (1 degrees < b < 2 degrees) and one below (-2 degrees < b < -1 degrees) the Galactic plane in the direction of the Galactic center at X-ray, optical, and near-infrared wavelengths. For the X-ray part of the survey we use 2 ks per Chandra pointing. We find 424 X-ray sources in the 63 Chandra observations on which we report here. These sources are in addition to the 1216 X-ray sources discovered in the first part of the GBS survey described previously. We discuss the characteristics and the X-ray variability of the brightest of the sources as well as the radio properties from existing radio surveys. We point out an interesting asymmetry in the number of X-ray sources as a function of their Galactic l and b coordinates which is probably caused by differences in average extinction toward the different parts of the GBS survey area. C1 [Jonker, Peter G.; Torres, Manuel A. P.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, Peter G.; Nelemans, Gijs] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 AJ Nijmegen, Netherlands. [Jonker, Peter G.; Torres, Manuel A. P.; Wu, Jianfeng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hynes, Robert I.; Britt, Christopher T.; Johnson, Christopher B.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Maccarone, Thomas J.; Britt, Christopher T.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Steeghs, Danny; Greiss, Sandra] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Nelemans, Gijs] Katholieke Univ Leuven, Inst Astron, B-3001 Louvain, Belgium. [Heinke, Craig] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. RP Jonker, PG (reprint author), SRON Netherlands Inst Space Res, SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. RI Nelemans, Gijs/D-3177-2012; OI Nelemans, Gijs/0000-0002-0752-2974; Heinke, Craig/0000-0003-3944-6109 FU National Science Foundation [AST-0908789]; National Aeronautics and Space Administration (NASA) FX The authors thank the CXC for scheduling the Chandra observations. R.I.H., C.T.B., and C.B.J., acknowledge support from the National Science Foundation under grant No. AST-0908789. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of the VizieR Catalogue access tool, CDS, Strasbourg, France. The original description of the VizieR service was published in A&AS, 143, 23. 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). This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 48 TC 10 Z9 10 U1 0 U2 0 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 FEB PY 2014 VL 210 IS 2 AR 18 DI 10.1088/0067-0049/210/2/18 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA6WN UT WOS:000331239000004 ER PT J AU Marcy, GW Isaacson, H Howard, AW Rowe, JF Jenkins, JM Bryson, ST Latham, DW Howell, SB Gautier, TN Batalha, NM Rogers, L Ciardi, D Fischer, DA Gilliland, RL Kjeldsen, H Christensen-Dalsgaard, J Huber, D Chaplin, WJ Basu, S Buchhave, LA Quinn, SN Borucki, WJ Koch, DG Hunter, R Caldwell, DA Van Cleve, J Kolbl, R Weiss, LM Petigura, E Seager, S Morton, T Johnson, JA Ballard, S Burke, C Cochran, WD Endl, M MacQueen, P Everett, ME Lissauer, JJ Ford, EB Torres, G Fressin, F Brown, TM Steffen, JH Charbonneau, D Basri, GS Sasselov, DD Winn, J Sanchis-Ojeda, R Christiansen, J Adams, E Henze, C Dupree, A Fabrycky, DC Fortney, JJ Tarter, J Holman, MJ Tenenbaum, P Shporer, A Lucas, PW Welsh, WF Orosz, JA Bedding, TR Campante, TL Davies, GR Elsworth, Y Handberg, R Hekker, S Karoff, C Kawaler, SD Lund, MN Lundkvist, M Metcalfe, TS Miglio, A Aguirre, VS Stello, D White, TR Boss, A Devore, E Gould, A Prsa, A Agol, E Barclay, T Coughlin, J Brugamyer, E Mullally, F Quintana, EV Still, M Thompson, SE Morrison, D Twicken, JD Desert, JM Carter, J Crepp, JR Hebrard, G Santerne, A Moutou, C Sobeck, C Hudgins, D Haas, MR Robertson, P Lillo-Box, J Barrado, D AF Marcy, Geoffrey W. Isaacson, Howard Howard, Andrew W. Rowe, Jason F. Jenkins, Jon M. Bryson, Stephen T. Latham, David W. Howell, Steve B. Gautier, Thomas N., III Batalha, Natalie M. Rogers, Leslie Ciardi, David Fischer, Debra A. Gilliland, Ronald L. Kjeldsen, Hans Christensen-Dalsgaard, Jorgen Huber, Daniel Chaplin, William J. Basu, Sarbani Buchhave, Lars A. Quinn, Samuel N. Borucki, William J. Koch, David G. Hunter, Roger Caldwell, Douglas A. Van Cleve, Jeffrey Kolbl, Rea Weiss, Lauren M. Petigura, Erik Seager, Sara Morton, Timothy Johnson, John Asher Ballard, Sarah Burke, Chris Cochran, William D. Endl, Michael MacQueen, Phillip Everett, Mark E. Lissauer, Jack J. Ford, Eric B. Torres, Guillermo Fressin, Francois Brown, Timothy M. Steffen, Jason H. Charbonneau, David Basri, Gibor S. Sasselov, Dimitar D. Winn, Joshua Sanchis-Ojeda, Roberto Christiansen, Jessie Adams, Elisabeth Henze, Christopher Dupree, Andrea Fabrycky, Daniel C. Fortney, Jonathan J. Tarter, Jill Holman, Matthew J. Tenenbaum, Peter Shporer, Avi Lucas, Philip W. Welsh, William F. Orosz, Jerome A. Bedding, T. R. Campante, T. L. Davies, G. R. Elsworth, Y. Handberg, R. Hekker, S. Karoff, C. Kawaler, S. D. Lund, M. N. Lundkvist, M. Metcalfe, T. S. Miglio, A. Aguirre, V. Silva Stello, D. White, T. R. Boss, Alan Devore, Edna Gould, Alan Prsa, Andrej Agol, Eric Barclay, Thomas Coughlin, Jeff Brugamyer, Erik Mullally, Fergal Quintana, Elisa V. Still, Martin Thompson, Susan E. Morrison, David Twicken, Joseph D. Desert, Jean-Michel Carter, Josh Crepp, Justin R. Hebrard, Guillaume Santerne, Alexandre Moutou, Claire Sobeck, Charlie Hudgins, Douglas Haas, Michael R. Robertson, Paul Lillo-Box, Jorge Barrado, David TI MASSES, RADII, AND ORBITS OF SMALL KEPLER PLANETS: THE TRANSITION FROM GASEOUS TO ROCKY PLANETS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE planetary systems; planets and satellites: detection; stars: individual (Kepler-25, Kepler-37, Kepler-48, Kepler-68, Kepler-93, Kepler-94, Kepler-95, Kepler-96, Kepler-97, Kepler-98, Kepler-99, Kepler-100, Kepler-102, Kepler-103, Kepler-106, Kepler-109, Kepler-113, Kepler-131, Kepler-406, Kepler-407, Kepler-409); techniques: photometric; techniques: radial velocities ID CANDIDATE HOST STARS; EARTH-SIZED PLANET; SOLAR-TYPE STARS; IN SUPER-EARTHS; TIMING VARIATIONS; M-DWARF; VELOCITY MEASUREMENTS; SOLID EXOPLANETS; BULK COMPOSITION; FALSE POSITIVES AB We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm(-3), suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than similar to 2 R-circle plus. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O). C1 [Marcy, Geoffrey W.; Isaacson, Howard; Kolbl, Rea; Weiss, Lauren M.; Petigura, Erik; Basri, Gibor S.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Howard, Andrew W.] Univ Hawaii, Honolulu, HI 96822 USA. [Rowe, Jason F.; Bryson, Stephen T.; Howell, Steve B.; Batalha, Natalie M.; Huber, Daniel; Borucki, William J.; Koch, David G.; Hunter, Roger; Lissauer, Jack J.; Christiansen, Jessie; Henze, Christopher; Morrison, David; Sobeck, Charlie; Haas, Michael R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Jenkins, Jon M.; Caldwell, Douglas A.; Van Cleve, Jeffrey; Burke, Chris; Tarter, Jill; Tenenbaum, Peter; Devore, Edna; Mullally, Fergal; Quintana, Elisa V.; Thompson, Susan E.; Twicken, Joseph D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Latham, David W.; Buchhave, Lars A.; Quinn, Samuel N.; Torres, Guillermo; Fressin, Francois; Charbonneau, David; Sasselov, Dimitar D.; Dupree, Andrea; Holman, Matthew J.; Desert, Jean-Michel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rogers, Leslie; Morton, Timothy; Johnson, John Asher; Shporer, Avi] CALTECH, Pasadena, CA 91109 USA. [Ciardi, David] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Fischer, Debra A.; Basu, Sarbani] Yale Univ, New Haven, CT 06510 USA. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Kjeldsen, Hans; Christensen-Dalsgaard, Jorgen; Chaplin, William J.; Campante, T. L.; Davies, G. R.; Elsworth, Y.; Handberg, R.; Karoff, C.; Lund, M. N.; Lundkvist, M.; Miglio, A.; Aguirre, V. Silva] Aarhus Univ, SAC, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Christensen-Dalsgaard, Jorgen] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Chaplin, William J.; Campante, T. L.; Davies, G. R.; Elsworth, Y.; Handberg, R.; Miglio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Seager, Sara; Winn, Joshua; Sanchis-Ojeda, Roberto; Carter, Josh] MIT, Cambridge, MA 02139 USA. [Ballard, Sarah; Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Cochran, William D.; Endl, Michael; MacQueen, Phillip; Robertson, Paul] Univ Texas Austin, Austin, TX 78712 USA. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Ford, Eric B.; Robertson, Paul] Penn State Univ, Ctr Exoplanets & Habitable Worlds, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Steffen, Jason H.] Northwestern Univ, Evanston, IL 60208 USA. [Adams, Elisabeth] Planetary Sci Inst, Tucson, AZ 85719 USA. [Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Lucas, Philip W.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Welsh, William F.; Orosz, Jerome A.] San Diego State Univ, San Diego, CA 92182 USA. [Bedding, T. R.; Stello, D.; White, T. R.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Hekker, S.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1012 WX Amsterdam, Netherlands. [Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Metcalfe, T. S.] Space Sci Inst, Boulder, CO 80301 USA. [Boss, Alan] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Gould, Alan] Lawrence Hall Sci, Berkeley, CA 94720 USA. [Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Barclay, Thomas; Coughlin, Jeff; Still, Martin] Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Brugamyer, Erik] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Crepp, Justin R.] Univ Notre Dame, Notre Dame, IN 46556 USA. [Hebrard, Guillaume] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France. [Hebrard, Guillaume] Observ Haute Provence, CNRS, OAMP, F-04870 St Michel, France. [Santerne, Alexandre] Aix Marseille Univ, CNRS, LAM UMR 7326, F-13388 Marseille, France. [Santerne, Alexandre] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Moutou, Claire] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Hudgins, Douglas] NASA Headquarters, Washginton, DC USA. [Lillo-Box, Jorge; Barrado, David] CSIC, Depto Astrofis, Ctr Astrobiol, INTA, E-28691 Villanueva De La Canada, Spain. RP Marcy, GW (reprint author), Univ Calif Berkeley, Berkeley, CA 94720 USA. RI Santerne, Alexandre/M-9265-2013; Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015; Lillo-Box, Jorge/I-2841-2015; Barrado Navascues, David/C-1439-2017; OI Handberg, Rasmus/0000-0001-8725-4502; Kawaler, Steven/0000-0002-6536-6367; Fabrycky, Daniel/0000-0003-3750-0183; Buchhave, Lars A./0000-0003-1605-5666; Weiss, Lauren/0000-0002-3725-3058; Metcalfe, Travis/0000-0003-4034-0416; Ciardi, David/0000-0002-5741-3047; Karoff, Christoffer/0000-0003-2009-7965; Bedding, Tim/0000-0001-5222-4661; Basu, Sarbani/0000-0002-6163-3472; /0000-0001-6545-639X; Lund, Mikkel Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571; Fischer, Debra/0000-0003-2221-0861; Santerne, Alexandre/0000-0002-3586-1316; Caldwell, Douglas/0000-0003-1963-9616; Howard, Andrew/0000-0001-8638-0320; Lillo-Box, Jorge/0000-0003-3742-1987; Barrado Navascues, David/0000-0002-5971-9242; Bedding, Timothy/0000-0001-5943-1460; Fortney, Jonathan/0000-0002-9843-4354; Davies, Guy/0000-0002-4290-7351; /0000-0002-0802-9145 FU NASA Science Mission Directorate; W. M. Keck Foundation; Danish National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler); European Research Council [267864]; UK Science and Technology Facilities Council (STFC); NSF [AST-1105930, AST-1109928, AST-0645416]; Netherlands organisation for Scientific Research (NWO); European Research Council under the European Community's Seventh Framewrok Programme/ERC [338251]; NASA [ADAP12-0172, NNX08AR04G, NNX12AF73G, NNX09AG09A]; Kepler Participating Scientist Program (PSP) [NNX12AC76G]; European Research Council/European Community [239953]; National Aeronautics and Space Administration FX Kepler was competitively selected as the tenth NASA Discovery mission. Funding for this mission is provided by the NASA Science Mission Directorate. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Some of the asteroseismology analysis was performed by the Stellar Astrophysics Centre which is funded by the Danish National Research Foundation (Grant DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant 267864). D. H. is supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. W.J.C., Y.E., T.L.C., G.R.D, R.H and A.M. acknowledge financial support from the UK Science and Technology Facilities Council (STFC). S.B. acknowledges NSF grant AST-1105930. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement no. 267864). S H. acknowledges financial support from the Netherlands organisation for Scientific Research (NWO). The research leading to the presented results has received funding from the European Research Council under the European Community's Seventh Framewrok Programme (FP7/2007-2013)/ERC grant agreement no. 338251 (StellarAges). W.F. Welsh and J.A. Orosz acknowledge support from NASA through the Kepler Participating Scientist Program and from the NSF via grant AST-1109928. D. Fischer acknowledges support from NASA ADAP12-0172. O. R. Sanchis-Ojeda & J. N. Winn are supported by the Kepler Participating Scientist Program (PSP) through grant NNX12AC76G. E. Ford is partially supported by NASA PSP grants NNX08AR04G & NNX12AF73G. Eric Agol acknowledges NSF Career grant AST-0645416. R.L.G. has been partially supported by NASA co-operative agreement: NNX09AG09A. A. Santerne acknowledges the support by the European Research Council/European Community under the FP7 through Starting Grant agreement number 239953. The authors would like to thank the many people who gave so generously of their time to make this Mission a success. All Kepler data products are available to the public at the Mikulski Archive for Space Telescopes http://stdatu.stsci.edu/kepler and the spectra and their products are made available at the NExSci Exoplanet Archive and its CFOP Web site: http://exoplanetarchive.ipac.caltech.edu. We thank the many observers who contributed to the measurements reported here. We gratefully acknowledge the efforts and dedication of the Keck Observatory staff, especially Scott Dahm, Hien Tran, and Grant Hill for support with HIRES and Greg Wirth for support with remote observing. This work made use of the SIMBAD database (operated at CDS, Strasbourg, France) and NASA's Astrophysics Data System Bibliographic Services. 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.; Finally, the authors wish to extend special thanks to those of Hawai'ian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. NR 119 TC 166 Z9 166 U1 24 U2 96 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 FEB PY 2014 VL 210 IS 2 AR 20 DI 10.1088/0067-0049/210/2/20 PG 70 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA6WN UT WOS:000331239000006 ER PT J AU Zoogman, P Jacob, DJ Chance, K Worden, HM Edwards, DP Zhang, L AF Zoogman, Peter Jacob, Daniel J. Chance, Kelly Worden, Helen M. Edwards, David P. Zhang, Lin TI Improved monitoring of surface ozone by joint assimilation of geostationary satellite observations of ozone and CO SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Ozone; Kalman filter; CO; Joint assimilation; Error correlation; Remote sensing ID NORTH-ATLANTIC OCEAN; TROPOSPHERIC OZONE; ATMOSPHERIC COMPOSITION; CARBON-MONOXIDE; AIR-QUALITY; TES; SENSITIVITY; TRANSPORT; MISSION; OMI AB Future geostationary satellite observations of tropospheric ozone aim to improve monitoring of surface ozone air quality. However, ozone retrievals from space have limited sensitivity in the lower troposphere (boundary layer). Data assimilation in a chemical transport model can propagate the information from the satellite observations to provide useful constraints on surface ozone. This may be aided by correlated satellite observations of carbon monoxide (CO), for which boundary layer sensitivity is easier to achieve. We examine the potential of concurrent geostationary observations of ozone and CO to improve constraints on surface ozone air quality through exploitation of ozone CO model error correlations in a joint data assimilation framework. The hypothesis is that model transport errors diagnosed for CO provide information on corresponding errors in ozone. A paired-model analysis of ozone CO error correlations in the boundary layer over North America in summer indicates positive error correlations in continental outflow but negative regional-scale error correlations over land, the latter reflecting opposite sensitivities of ozone and CO to boundary layer depth. Aircraft observations from the ICARIT campaign are consistent with this pattern but also indicate strong positive error correlations in fine-scale pollution plumes. We develop a joint ozone CO data assimilation system and apply it to a regional-scale Observing System Simulation Experiment (OSSE) of the planned NASA GEO-CAPE geostationary mission over North America. We find substantial benefit from joint ozone CO data assimilation in informing US ozone air quality if the instrument sensitivity for CO in the boundary layer is greater than VAR:irsome. A high-quality geostationary measurement of CO could potentially relax the requirements for boundary layer sensitivity of the ozone measurement. This is contingent on accurate characterization of ozone CO error correlations. A finer-resolution data assimilation system resolving the urban scale would need to account for the change in sign of the ozone CO error correlations between urban pollution plumes and the regional atmosphere. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Zoogman, Peter; Jacob, Daniel J.; Zhang, Lin] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Jacob, Daniel J.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Worden, Helen M.; Edwards, David P.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Zoogman, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pzoogman@cfa.harvard.edu RI Chem, GEOS/C-5595-2014; Zhang, Lin/A-6729-2008; OI Zhang, Lin/0000-0003-2383-8431; Chance, Kelly/0000-0002-7339-7577; Zoogman, Peter/0000-0002-8848-4999 FU NASA Atmospheric Composition and Modeling Program; NASA Earth and Space Science Fellowship FX This work was supported by the NASA Atmospheric Composition and Modeling Program and by a NASA Earth and Space Science Fellowship to Peter Zoogman. NR 50 TC 9 Z9 9 U1 0 U2 37 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD FEB PY 2014 VL 84 BP 254 EP 261 DI 10.1016/j.atmosenv.2013.11.048 PG 8 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 302JZ UT WOS:000330602100028 ER PT J AU Clarin, TMA Borissov, I Page, RA Ratcliffe, JM Siemers, BM AF Clarin, Theresa M. A. Borissov, Ivailo Page, Rachel A. Ratcliffe, John M. Siemers, Bjoern M. TI Social learning within and across species: information transfer in mouse-eared bats SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Article DE social learning; information transfer; long-term memory; foraging; interspecific learning; Myotis myotis; greater mouse-eared bat; Myotis oxygnathus; lesser mouse-eared bat ID FEMALE BECHSTEINS BATS; SPEAR-NOSED BATS; MYOTIS-MYOTIS; PREDATOR RECOGNITION; CULTURAL TRANSMISSION; HABITAT SELECTION; FEEDING-BEHAVIOR; WILD POPULATION; FIELD CRICKET; BLYTHII AB Social learning describes information transfer between individuals through observation or direct interaction. Bats can live and forage in large groups, sometimes comprising several species, and are thus well suited for investigations of both intraspecific and interspecific information transfer. Although social learning has been documented within several bat species, it has not been shown to occur between species. Furthermore, it is not fully understood what level of interaction between individuals is necessary for social learning in bats. We address these questions by comparing the efficiency of observation versus interaction in intraspecific social learning and by considering interspecific social learning in sympatric bat species. Observers learned from demonstrators to identify food sources using a light cue. We show that intraspecific social learning exists in the greater mouse-eared bat (Myotis myotis (Borkhausen, 1797)) and that direct interaction with a demonstrator more efficiently leads to information transfer than observational learning alone. We also found evidence for interspecific information transfer from M. myotis to the lesser mouse-eared bat (Myotis oxygnathus Monticelli, 1885). Additionally, we opportunistically retested one individual that we recaptured from the wild 1 year after initial learning and found long-term memory of the trained association. Our study adds to the understanding of learning, information transfer, and long-term memory in wild-living animals. C1 [Clarin, Theresa M. A.; Borissov, Ivailo; Siemers, Bjoern M.] Max Planck Inst Ornithol, Sensory Ecol Grp, D-82319 Seewiesen, Germany. [Page, Rachel A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Ratcliffe, John M.] Univ Southern Denmark, Dept Biol, DK-5230 Odense M, Denmark. RP Clarin, TMA (reprint author), Max Planck Inst Ornithol, Sensory Ecol Grp, Eberhard Gwinner Str 11, D-82319 Seewiesen, Germany. EM tclarin@orn.mpg.de FU International Max Planck Research School (IMPRS) for Organismal Biology; Max Planck Institute for Ornithology FX We thank K. Koselj for considerable help with the statistical analysis of our data. M. Crawley also provided helpful advice, during his GLIM course at Imperial College London. We thank the participants of the scientific writing workshop held in Balmaha, Scotland, especially B. Helm, for constructive criticism of an earlier draft of the manuscript. We are grateful to two reviewers for their insightful comments on the manuscript. We thank K. Koselj and M. Clarin for the same, and the Tabachka Bat Research Station Team 2011 and 2012 for logistical support. We thank M. Clarin for help designing and constructing the feeding boxes. T. C. was supported by the International Max Planck Research School (IMPRS) for Organismal Biology and this research was funded by the Max Planck Institute for Ornithology. Our greatest thanks go to the late Bjorn Siemers, head of the Sensory Ecology Group in Seewiesen, Germany, for his support, friendship, and unending inspiration. NR 59 TC 8 Z9 8 U1 10 U2 47 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA SN 0008-4301 EI 1480-3283 J9 CAN J ZOOL JI Can. J. Zool.-Rev. Can. Zool. PD FEB PY 2014 VL 92 IS 2 BP 129 EP 139 DI 10.1139/cjz-2013-0211 PG 11 WC Zoology SC Zoology GA AA4PE UT WOS:000331077300006 ER PT J AU Lynch, HJ Rhainds, M Calabrese, JM Cantrell, S Cosner, C Fagan, WF AF Lynch, Heather J. Rhainds, Marc Calabrese, Justin M. Cantrell, Stephen Cosner, Chris Fagan, William F. TI How climate extremes-not means-define a species' geographic range boundary via a demographic tipping point SO ECOLOGICAL MONOGRAPHS LA English DT Article DE Allee effect; bagworm; Thyridopteryx ephemeraeformis; climate change; female mating failure; geographic range boundary; invasion pinning; latitudinal gradient; overwinter survivorship; population-dynamic parameters; Psychidae; reproductive asynchrony; U; S; Midwest ID THYRIDOPTERYX-EPHEMERAEFORMIS LEPIDOPTERA; CRITICAL PATCH SIZE; INSECT POPULATIONS; REPRODUCTIVE ASYNCHRONY; BAGWORMS LEPIDOPTERA; DISTRIBUTION MODELS; DENDROCTONUS-FRONTALIS; HAWORTH LEPIDOPTERA; WINTER TEMPERATURES; CHANGE PERSPECTIVE AB Species' geographic range limits interest biologists and resource managers alike; however, scientists lack strong mechanistic understanding of the factors that set geographic range limits in the field, especially for animals. There exists a clear need for detailed case studies that link mechanisms to spatial dynamics and boundaries because such mechanisms allow us to predict whether climate change is likely to change a species' geographic range and, if so, how abundance in marginal populations compares to the core. The bagworm Thyridopteryx ephemeraeformis (Lepidoptera: Psychidae) is a major native pest of cedars, arborvitae, junipers, and other landscape trees throughout much of North America. Across dozens of bagworm populations spread over six degrees of latitude in the American Midwest we find latitudinal declines in fecundity and egg and pupal survivorship as one proceeds toward the northern range boundary. A spatial gradient of bagworm reproductive success emerges, which is associated with a progressive decline in local abundance and an increase in the risk of local population extinction near the species' geographic range boundary. We developed a mathematical model, completely constrained by empirically estimated parameters, to explore the relative roles of reproductive asynchrony and stage-specific survivorship in generating the range limit for this species. We find that overwinter egg mortality is the biggest constraint on bagworm persistence beyond their northern range limit. Overwinter egg mortality is directly related to winter temperatures that fall below the bagworm eggs' physiological limit. This threshold, in conjunction with latitudinal declines in fecundity and pupal survivorship, creates a nonlinear response to climate extremes that sets the geographic boundary and provides a path for predicting northward range expansion under altered climate conditions. Our mechanistic modeling approach demonstrates how species' sensitivity to climate extremes can create population tipping points not reflected in demographic responses to climate means, a distinction that is critical to successful ecological forecasting. C1 [Lynch, Heather J.] SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. [Rhainds, Marc] Nat Resources Canada, Canadian Forest Serv, Atlantic Forestry Ctr, Fredericton, NB, Canada. [Calabrese, Justin M.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA. [Cantrell, Stephen; Cosner, Chris] Univ Miami, Dept Math, Coral Gables, FL 33124 USA. [Fagan, William F.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Lynch, HJ (reprint author), SUNY Stony Brook, Dept Ecol & Evolut, 113 Life Sci Bldg, Stony Brook, NY 11794 USA. EM heather.lynch@stonybrook.edu RI Calabrese, Justin/B-9131-2012 FU U.S. National Science Foundation Division of Mathematical Sciences [NSF/DMS-0816068, NSF/DMS-1118623, NSF/DMS-1225917] FX We thank Matthew Aiello-Lammens and Caroline Wick for reviewing the manuscript. H. J. Lynch, and W. F. Fagan gratefully acknowledge assistance from the University of Maryland. The authors gratefully acknowledge funding from the U.S. National Science Foundation Division of Mathematical Sciences (Award numbers NSF/DMS-0816068 and NSF/DMS-1118623 to S. Cantrell and C. Cosner and Award number NSF/DMS-1225917 to W. F. Fagan). NR 117 TC 11 Z9 11 U1 5 U2 79 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9615 EI 1557-7015 J9 ECOL MONOGR JI Ecol. Monogr. PD FEB PY 2014 VL 84 IS 1 BP 131 EP 149 DI 10.1890/12-2235.1 PG 19 WC Ecology SC Environmental Sciences & Ecology GA AA6NT UT WOS:000331215700008 ER PT J AU Ransome, E Munn, CB Halliday, N Camara, M Tait, K AF Ransome, Emma Munn, Colin B. Halliday, Nigel Camara, Miguel Tait, Karen TI Diverse profiles of N-acyl-homoserine lactone molecules found in cnidarians SO FEMS MICROBIOLOGY ECOLOGY LA English DT Article DE coral microbiology; sea anemone; microbial regulation; autoinducers; DGGE; LC-MS; MS ID QUORUM-SENSING SIGNAL; CORAL-ASSOCIATED BACTERIA; MUCUS-ASSOCIATED BACTERIA; GREAT-BARRIER-REEF; MICROBIAL COMMUNITIES; ACYLHOMOSERINE LACTONES; SERRATIA-MARCESCENS; BIOFILM FORMATION; SUBTIDAL BIOFILM; MARINE SPONGES AB Many marine habitats, such as the surface and tissues of marine invertebrates, including corals, harbour diverse populations of microorganisms, which are thought to play a role in the health of their hosts and influence mutualistic and competitive interactions. Investigating the presence and stability of quorum sensing (QS) in these ecosystems may shed light on the roles and control of these bacterial communities. Samples of 13 cnidarian species were screened for the presence and diversity of N-acyl-homoserine lactones (AHLs; a prevalent type of QS molecule) using thin-layer chromatography and an Agrobacterium tumefaciens NTL4 biosensor. Ten of 13 were found to harbour species-specific, conserved AHL profiles. AHLs were confirmed in Anemonia viridis using liquid chromatography tandem mass spectrometry. To assess temporal role and stability, AHLs were investigated in A.viridis from intertidal pools over 16h. Patterns of AHLs showed conserved profiles except for two mid-chain length AHLs, which increased significantly over the day, peaking at 20:00, but had no correlation with pool chemistry. Denaturing gel electrophoresis of RT-PCR-amplified bacterial 16S rRNA showed the presence of an active bacterial community that changed in composition alongside AHL profiles and contained a number of bands that affiliate with known AHL-producing bacteria. Investigations into the quorum sensing-controlled, species-specific roles of these bacterial communities and how these regulatory circuits are influenced by the coral host and members of the bacterial community are imperative to expand our knowledge of these interactions with respect to the maintenance of coral health. C1 [Ransome, Emma; Tait, Karen] Plymouth Marine Lab, Plymouth, Devon, England. [Ransome, Emma; Munn, Colin B.] Univ Plymouth, Sch Marine Sci & Engn, Plymouth PL4 8AA, Devon, England. [Halliday, Nigel; Camara, Miguel] Univ Nottingham, Sch Mol Med Sci, Ctr Biomol Sci, Nottingham NG7 2RD, England. RP Ransome, E (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM RansomeE@si.edu FU Natural Environment Research Council [PML/PhD2008/03KT] FX This work was funded by a studentship from The Natural Environment Research Council (PML/PhD2008/03KT; ER). The authors also thank the National Marine Aquarium (Plymouth, UK), the Interuniversity Institute of Eilat (Israel) and Keith Hiscock (Marine Biological Association, UK) for providing samples used in this study, Dr Andy Foggo for guidance on statistics and Daniel Gilbert and Richard Pearce for providing support during sample collection. NR 75 TC 5 Z9 5 U1 4 U2 30 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 FEB PY 2014 VL 87 IS 2 BP 315 EP 329 DI 10.1111/1574-6941.12226 PG 15 WC Microbiology SC Microbiology GA AA7FK UT WOS:000331262700002 PM 24117852 ER PT J AU Liu, HP Hershler, R AF Liu, Hsiu-Ping Hershler, Robert TI MICROSATELLITE PRIMERS FOR A WESTERN NORTH AMERICAN SPRINGSNAIL (PYRGULOPSIS ROBUSTA): EVIDENCE FOR POLYPLOIDY AND CROSS-AMPLIFICATION IN P. BRUNEAUENSIS SO JOURNAL OF MOLLUSCAN STUDIES LA English DT Article ID SNAIL TAYLORCONCHA-SERPENTICOLA; POPULATION-STRUCTURE; RIVER-BASIN C1 [Liu, Hsiu-Ping] Metropolitan State Univ Denver, Dept Biol, Denver, CO 80217 USA. [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, POB 37012,NHB W-305,MRC 163, Washington, DC 20013 USA. EM hershlerr@si.edu FU Idaho Power Company [1600]; School of Letter, Arts, and Sciences, Metropolitan State College of Denver FX This project was supported (in part) by a contract (to R.H.) from the Idaho Power Company (Award #1600) and a small grant from the School of Letter, Arts, and Sciences, Metropolitan State College of Denver (to H.-P.L.). NR 21 TC 2 Z9 2 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0260-1230 EI 1464-3766 J9 J MOLLUS STUD JI J. Molluscan Stud. PD FEB PY 2014 VL 80 BP 107 EP 110 DI 10.1093/mollus/eyt050 PN 1 PG 4 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA AA1EK UT WOS:000330839000015 ER PT J AU Lopez-Baucells, A Rocha, R Garcia-Mayes, I Vulinec, K Meyer, CFJ AF Lopez-Baucells, Adria Rocha, Ricardo Garcia-Mayes, Ileana Vulinec, Kevina Meyer, Christoph F. J. TI First record of Micronycteris sanborni (Chiroptera: Phyllostomidae) from Central Amazonia, Brazil: range expansion and description of its echolocation SO MAMMALIA LA English DT Article DE echolocation; Micronycteris sanborni; Phyllostomidae; range expansion; secondary forest ID BATS; FOREST; CALLS; FRUIT AB This note reports the first record of Micronycteris sanborni in Amazonas State, Brazil. It extends the species' known range >2000 km northwestward and represents the first record of M. sanborni in a humid tropical ecosystem, suggesting that the species might not be exclusive to dry areas, as previously thought. The individual was captured in Vismia-dominated secondary forest within the fragmented landscape of the Biological Dynamics of Forest Fragments Project. We present morphometric data and provide the first description of the echolocation calls of this poorly known species. C1 [Lopez-Baucells, Adria; Rocha, Ricardo; Meyer, Christoph F. J.] Ctr Environm Biol, Fac Sci, Dept Anim Biol, P-1749016 Lisbon, Portugal. [Lopez-Baucells, Adria; Rocha, Ricardo; Vulinec, Kevina; Meyer, Christoph F. J.] Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. [Lopez-Baucells, Adria; Rocha, Ricardo; Vulinec, Kevina; Meyer, Christoph F. J.] Smithsonian Trop Res Inst, BR-69011970 Manaus, Amazonas, Brazil. [Lopez-Baucells, Adria] Granollers Museum Nat Sci, Chiroptera Res Area, Granollers 08402, Catalonia, Spain. [Rocha, Ricardo] Univ Helsinki, Fac Biosci, Metapopulat Res Grp, FI-00014 Helsinki, Finland. [Garcia-Mayes, Ileana; Vulinec, Kevina] Delaware State Univ, Dept Agr & Nat Resources, Dover, DE 19901 USA. RP Lopez-Baucells, A (reprint author), Ctr Environm Biol, Fac Sci, Dept Anim Biol, C2 Campo Grande, P-1749016 Lisbon, Portugal. EM adria.baucells@gmail.com RI Meyer, Christoph/A-4363-2012; OI Meyer, Christoph/0000-0001-9958-8913; Lopez-Baucells, Adria/0000-0001-8446-0108 FU Portuguese Foundation for Science and Technology (FCT) [PTDC/BIA-BIC/111184/2009, SFRH/BD/80488/2011]; Delaware State University Academic Enhancement Grant FX We would like to thank Prof. Jorge Palmeirim and Dr. Paulo D.E. Bobrowiec for their assistance during all phases of the project, and Jose L.C. Camargo, Rosely Hipolito, and Ary Jorge Ferreira for logistic support. Financial support was provided by the Portuguese Foundation for Science and Technology (FCT) through the grants PTDC/BIA-BIC/111184/2009 and SFRH/BD/80488/2011, and to KV through a Delaware State University Academic Enhancement Grant. We are grateful to Stephane Aulagnier and two anonymous reviewers for insightful suggestions that greatly improved the manuscript. This manuscript is number 625 of the BDFFP technical series. NR 28 TC 0 Z9 1 U1 1 U2 9 PU WALTER DE GRUYTER GMBH PI BERLIN PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY SN 0025-1461 EI 1864-1547 J9 MAMMALIA JI Mammalia PD FEB PY 2014 VL 78 IS 1 BP 127 EP 132 DI 10.1515/mammalia-2013-0006 PG 6 WC Zoology SC Zoology GA AA1TP UT WOS:000330878900015 ER PT J AU Hunt, D AF Hunt, David TI A COMPANION TO FORENSIC ANTHROPOLOYGY SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Book Review C1 [Hunt, David] Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, Washington, DC 20560 USA. RP Hunt, D (reprint author), Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD FEB PY 2014 VL 153 IS 2 BP 323 EP 324 DI 10.1002/ajpa.22442 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 304DV UT WOS:000330728000016 ER PT J AU Riley, SM AF Riley, Sheila M. TI Gemini SO LIBRARY JOURNAL LA English DT Book Review C1 [Riley, Sheila M.] Smithsonian Inst Libs, Washington, DC 20560 USA. RP Riley, SM (reprint author), Smithsonian Inst Libs, 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 FEB 1 PY 2014 VL 139 IS 2 BP 61 EP 61 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 302MY UT WOS:000330609800050 ER PT J AU Hao, H Elvis, M Civano, F Zamorani, G Ho, LC Comastri, A Brusa, M Bongiorno, A Merloni, A Trump, JR Salvato, M Impey, CD Koekemoer, AM Lanzuisi, G Celotti, A Jahnke, K Vignali, C Silverman, JD Urry, CM Schawinski, K Capak, P AF Hao, Heng Elvis, Martin Civano, Francesca Zamorani, Gianni Ho, Luis C. Comastri, Andrea Brusa, Marcella Bongiorno, Angela Merloni, Andrea Trump, Jonathan R. Salvato, Mara Impey, Chris D. Koekemoer, Anton M. Lanzuisi, Giorgio Celotti, Annalisa Jahnke, Knud Vignali, Cristian Silverman, John D. Urry, C. Megan Schawinski, Kevin Capak, Peter TI Spectral energy distributions of type 1 AGN in XMM-COSMOS - II. Shape evolution SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; galaxies: evolution; quasars: general ID ACTIVE GALACTIC NUCLEI; WIDE-FIELD SURVEY; BLACK-HOLE MASSES; X-RAY-EMISSION; HIGH-REDSHIFT QUASARS; DIGITAL SKY SURVEY; RADIO-QUIET QUASARS; EARLY DATA RELEASE; HOST GALAXIES; LUMINOSITY FUNCTION AB The mid-infrared-to-ultraviolet (0.1-10 mu m) spectral energy distribution (SED) shapes of 407 X-ray-selected radio-quiet type 1 active galactic nuclei (AGN) in the wide-field 'Cosmic Evolution Survey' (COSMOS) have been studied for signs of evolution. For a sub-sample of 200 radio-quiet quasars with black hole mass estimates and host galaxy corrections, we studied their mean SEDs as a function of a broad range of redshift, bolometric luminosity, black hole mass and Eddington ratio, and compared them with the Elvis et al. (E94) type 1 AGN mean SED. We found that the mean SEDs in each bin are closely similar to each other, showing no statistical significant evidence of dependence on any of the analysed parameters. We also measured the SED dispersion as a function of these four parameters, and found no significant dependences. The dispersion of the XMM-COSMOS SEDs is generally larger than E94 SED dispersion in the ultraviolet, which might be due to the broader 'window function' for COSMOS quasars, and their X-ray-based selection. C1 [Hao, Heng; Celotti, Annalisa] SISSA, I-34136 Trieste, Italy. [Hao, Heng; Elvis, Martin; Civano, Francesca] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Civano, Francesca] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Zamorani, Gianni; Comastri, Andrea; Vignali, Cristian] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Ho, Luis C.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Brusa, Marcella; Bongiorno, Angela; Merloni, Andrea; Lanzuisi, Giorgio] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Brusa, Marcella; Vignali, Cristian] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Bongiorno, Angela] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Trump, Jonathan R.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Salvato, Mara] IPP Max Planck Inst Plasma Phys, D-85748 Garching, Germany. [Salvato, Mara] Excellence Cluster, D-85748 Garching, Germany. [Impey, Chris D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Celotti, Annalisa] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Celotti, Annalisa] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Jahnke, Knud] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Silverman, John D.] Univ Tokyo, Kavli Inst Phys & Math Universe, Todai Inst Adv Study, Kashiwa, Chiba 2778583, Japan. [Urry, C. Megan] Yale Univ, Dept Phys, New Haven, CT 06511 USA. [Urry, C. Megan] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA. [Schawinski, Kevin] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Capak, Peter] CALTECH, Pasadena, CA 91125 USA. RP Hao, H (reprint author), SISSA, Via Bonomea 265, I-34136 Trieste, Italy. EM henghao@post.harvard.edu RI Vignali, Cristian/J-4974-2012; Lanzuisi, Giorgio/K-4378-2013; Comastri, Andrea/O-9543-2015; OI Urry, Meg/0000-0002-0745-9792; Vignali, Cristian/0000-0002-8853-9611; Lanzuisi, Giorgio/0000-0001-9094-0984; Comastri, Andrea/0000-0003-3451-9970; Koekemoer, Anton/0000-0002-6610-2048; Bongiorno, Angela/0000-0002-0101-6624; Jahnke, Knud/0000-0003-3804-2137; Schawinski, Kevin/0000-0001-5464-0888; Zamorani, Giovanni/0000-0002-2318-301X FU NASA Chandra [G07-8136A]; Smithsonian Scholarly Studies; Italian Space Agency (ASI) [ASI-INAF I/088/06/0, I/009/10/0]; German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize [FKZHA 1850/28-1]; Swiss National Science Foundation [PP00P2_138979/1] FX HH thanks Belinda Wilkes and Martin J. Ward for discussion. This work was supported in part by NASA Chandra grant number G07-8136A (HH, ME, FC) and the Smithsonian Scholarly Studies (FC). Support from the Italian Space Agency (ASI) under the contracts ASI-INAF I/088/06/0 and I/009/10/0 is acknowledged (AC and CV). MS acknowledges support by the German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize (FKZHA 1850/28-1). KS gratefully acknowledges support from Swiss National Science Foundation Grant PP00P2_138979/1. NR 95 TC 18 Z9 18 U1 0 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 FEB PY 2014 VL 438 IS 2 BP 1288 EP 1304 DI 10.1093/mnras/stt2274 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA2WW UT WOS:000330955900030 ER PT J AU Roth, N Stahler, SW Keto, E AF Roth, Nathaniel Stahler, Steven W. Keto, Eric TI The dynamics of ultracompact H II regions SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: early-type; stars: formation; ISM: clouds; H II regions; ISM: jets and outflows ID MASSIVE STAR-FORMATION; COMPACT HII-REGIONS; RECOMBINATION LINE; MOLECULAR CLOUDS; ORION NEBULA; PHYSICAL-PROPERTIES; RADIO-CONTINUUM; GAS-DYNAMICS; YOUNG STARS; COMETARY AB Many ultracompact H II regions exhibit a cometary morphology in radio continuum emission. In such regions, a young massive star is probably ablating, through its ultraviolet radiation, the molecular cloud clump that spawned it. On one side of the star, the radiation drives an ionization front that stalls in dense molecular gas. On the other side, ionized gas streams outwards into the more rarefied environment. This wind is underpressured with respect to the neutral gas. The difference in pressure draws in more cloud material, feeding the wind until the densest molecular gas is dissipated. Recent, time-dependent simulations of massive stars turning on within molecular gas show the system evolving in a direction similar to that just described. Here, we explore a semi-analytic model in which the wind is axisymmetric and has already achieved a steady state. Adoption of this simplified picture allows us to study the dependence of both the wind and its bounding ionization front on the stellar luminosity, the peak molecular density and the displacement of the star from the centre of the clump. For typical parameter values, the wind accelerates transonically to a speed of about 15 km s(-1), and transports mass outwards at a rate of 10(-4) M-circle dot yr(-1). Stellar radiation pressure acts to steepen the density gradient of the wind. C1 [Roth, Nathaniel] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Stahler, Steven W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Keto, Eric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Roth, N (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. EM nathaniel.roth@berkeley.edu OI Roth, Nathaniel/0000-0002-6485-2259 FU Department of Energy Office of Science Graduate Fellowship Program (DOE SCGF) [DE-AC05-06OR23100]; NSF [0908573] FX Throughout the work, NR was supported by the Department of Energy Office of Science Graduate Fellowship Program (DOE SCGF), made possible in part by the American Recovery and Reinvestment Act of 2009, administered by ORISE-ORAU under contract no. DE-AC05-06OR23100. SS was partially supported by NSF Grant 0908573. NR 60 TC 2 Z9 2 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 FEB PY 2014 VL 438 IS 2 BP 1335 EP 1354 DI 10.1093/mnras/stt2278 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA2WW UT WOS:000330955900034 ER PT J AU Sabin, L Zhang, Q Zijlstra, A Patel, NA Vazquez, R Zauderer, BA Contreras, ME Guillen, PF AF Sabin, L. Zhang, Q. Zijlstra, A. Patel, N. A. Vazquez, R. Zauderer, B. A. Contreras, M. E. Guillen, P. F. TI Submillimetre polarization and magnetic field properties in the envelopes of protoplanetary nebulae CRL 618 and OH 231.8+4.2 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE magnetic fields; polarization; stars: AGB and post-AGB; stars individual: CRL 618; stars individual: OH 231.8+4.2 ID SHAPING PLANETARY-NEBULAE; FORMING MOLECULAR CLOUDS; GRAIN ALIGNMENT; EVOLVED STARS; HERSCHEL/HIFI OBSERVATIONS; CIRCUMSTELLAR ENVELOPES; MILLIMETER-WAVELENGTH; INTERSTELLAR GRAINS; PHYSICAL STRUCTURE; BIPOLAR OUTFLOW AB We have carried out continuum and line polarization observations of two protoplanetary nebulae (PPNe), CRL 618 and OH 231.8+4.2, using the Submillimeter Array in its compact configuration. The frequency range of observations, 330-345 GHz, includes the CO(J=3 -> 2) line emission. CRL 618 and OH 231.8+4.2 show quadrupolar and bipolar optical lobes, respectively, surrounded by a dusty envelope reminiscent of their asymptotic giant branch phase. We report a detection of dust continuum polarized emission in both PPNe above 4 sigma but no molecular line polarization detection above a 3 sigma limit. OH 231.8+4.2 is slightly more polarized on average than CRL 618 with a mean fractional polarization of 4.3 and 0.3 per cent, respectively. This agrees with the previous finding that silicate dust shows higher polarization than carbonaceous dust. In both objects, an anticorrelation between the fractional polarization and the intensity is observed. Neither PPNe shows a well-defined toroidal equatorial field, rather the field is generally well aligned and organized along the polar direction. This is clearly seen in CRL 618 while in the case of OH 231.8+4.2, the geometry indicates an X-shaped structure coinciding overall with a dipole/polar configuration. However in the later case, the presence of a fragmented and weak toroidal field should not be discarded. Finally, in both PPNe, we observed that the well-organized magnetic field is parallel with the major axis of the (CO)-C-12 outflow. This alignment could indicate the presence of a magnetic outflow launching mechanism. Based on our new high-resolution data we propose two scenarios to explain the evolution of the magnetic field in evolved stars. C1 [Sabin, L.] Univ Guadalajara, CUCEI, Dept Fis, Inst Aston & Meteorol, Guadalajara 44130, Jalisco, Mexico. [Zhang, Q.; Patel, N. A.; Zauderer, B. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zijlstra, A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Vazquez, R.; Contreras, M. E.; Guillen, P. F.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. RP Sabin, L (reprint author), Univ Guadalajara, CUCEI, Dept Fis, Inst Aston & Meteorol, Av Vallarta 2602, Guadalajara 44130, Jalisco, Mexico. EM laurence.sabin@gmail.com RI Vazquez, Roberto/L-3613-2016; OI Vazquez, Roberto/0000-0002-3279-9764; Zhang, Qizhou/0000-0003-2384-6589 FU CONACYT [CB-2011-01-0168078]; PAPIIT-DGAPA-UNAM [IN107914]; NASA [NAS 5-26555] FX The authors thank the SMA personal for supporting the observations as well as the referee for comments and suggestions, which significantly contributed to improving the quality of the publication. LS also thanks S. Kemp for going through the paper and raising some issues. LS is supported by the CONACYT grant CB-2011-01-0168078, and RV is supported by PAPIIT-DGAPA-UNAM grant IN107914. This research has also made use of the SIMBAD data base, operated at CDS, Strasbourg, France and the NASA's Astrophysics Data System. We acknowledge the use of observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. NR 71 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 FEB PY 2014 VL 438 IS 2 BP 1794 EP 1804 DI 10.1093/mnras/stt2318 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AA2WW UT WOS:000330955900066 ER PT J AU Eggert, LS Buij, R Lee, ME Campbell, P Dallmeier, F Fleischer, RC Alonso, A Maldonado, JE AF Eggert, L. S. Buij, R. Lee, M. E. Campbell, P. Dallmeier, F. Fleischer, R. C. Alonso, A. Maldonado, J. E. TI Using Genetic Profiles of African Forest Elephants to Infer Population Structure, Movements, and Habitat Use in a Conservation and Development Landscape in Gabon SO CONSERVATION BIOLOGY LA English DT Article DE connectivity; conservation outside parks; Loxodonta cyclotis; multiple-use areas; noninvasive sampling ID LOXODONTA-AFRICANA; SAVANNA ELEPHANTS; PROTECTED AREAS; NATIONAL-PARK; RELATEDNESS; DEMOGRAPHY; PATTERNS; CRISIS; LOCI AB Conservation of wide-ranging species, such as the African forest elephant (Loxodonta cyclotis), depends on fully protected areas and multiple-use areas (MUA) that provide habitat connectivity. In the Gamba Complex of Protected Areas in Gabon, which includes 2 national parks separated by a MUA containing energy and forestry concessions, we studied forest elephants to evaluate the importance of the MUA to wide-ranging species. We extracted DNA from elephant dung samples and used genetic information to identify over 500 individuals in the MUA and the parks. We then examined patterns of nuclear microsatellites and mitochondrial control-region sequences to infer population structure, movement patterns, and habitat use by age and sex. Population structure was weak but significant, and differentiation was more pronounced during the wet season. Within the MUA, males were more strongly associated with open habitats, such as wetlands and savannas, than females during the dry season. Many of the movements detected within and between seasons involved the wetlands and bordering lagoons. Our results suggest that the MUA provides year-round habitat for some elephants and additional habitat for others whose primary range is in the parks. With the continuing loss of roadless wilderness areas in Central Africa, well-managed MUAs will likely be important to the conservation of wide-ranging species. C1 [Eggert, L. S.; Fleischer, R. C.; Maldonado, J. E.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Eggert, L. S.] Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA. [Buij, R.] Univ Groningen, Ctr Life Sci, NL-9747 AG Groningen, Netherlands. [Buij, R.; Campbell, P.; Dallmeier, F.; Alonso, A.] Smithsonian Conservat Biol Inst, Ctr Conservat Educ & Sustainabil, Washington, DC 20013 USA. [Lee, M. E.] Univ Oxford, Dept Zool, WildCRU, Recanati Kaplan Ctr, Abingdon OX13 5QL, Oxon, England. [Lee, M. E.] Ctr Natl Rech Sci & Technol, Inst Rech Ecol Trop, Libreville, Gabon. [Campbell, P.] Natl Pk Serv, Inventory & Monitoring Program, Washington, DC 20013 USA. [Maldonado, J. E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Eggert, LS (reprint author), Div Biol Sci, Columbia, MO 65211 USA. EM eggertl@missouri.edu FU Shell Gabon; Smithsonian Conservation Biology Institute FX We thank Shell Gabon and the Smithsonian Conservation Biology Institute for funding and in-kind support. We thank the National Center for Research and Scientific Technology, National Parks Gabon, and the Directorate of Wildlife and Hunting (DFC) for permits and the DFC and Wildlife Conservation Society (WCS)/Operation Loango for dedicating agents to our study. Logistics were facilitated by Satram, Sodexho, and WCS/Operation Loango. C. McIntosh and A. Garrison provided assistance with genotyping. This is publication 120 of the Gabon Biodiversity Program. NR 47 TC 3 Z9 3 U1 11 U2 73 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 2014 VL 28 IS 1 BP 107 EP 118 DI 10.1111/cobi.12161 PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 297OX UT WOS:000330265900012 PM 24471781 ER PT J AU West, KL Ramer, J Brown, JL Sweeney, J Hanahoe, EM Reidarson, T Proudfoot, J Bergfelt, DR AF West, Kristi L. Ramer, Jan Brown, Janine L. Sweeney, Jay Hanahoe, Erin M. Reidarson, Torn Proudfoot, Jeffry Bergfelt, Don R. TI Thyroid hormone concentrations in relation to age, sex, pregnancy, and perinatal loss in bottlenose dolphins (Tursiops truncatus). SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Bottlenose dolphin; Thyroid hormones; Age; Sex; Pregnancy; Perinatal loss ID DELPHINAPTERUS-LEUCAS; HALICHOERUS-GRYPUS; FUNCTION TESTS; BELUGA WHALES; SERUM; THYROXINE; LACTATION; SEASON; SEALS; CHILDREN AB This study evaluated circulating concentrations of thyroid hormones in relation to age, sex, pregnancy status, and perinatal loss in bottlenose dolphins (Tursiops truncatus) under human care. A total of 373 blood samples were collected from 60 individual dolphins housed at nine aquariums/oceanariums. Serum concentrations of total and free thyroxine (T-4) and triiodothyronine (T-3) were analyzed with commercial RIA kits validated for use with dolphins. While the effect of age was indicated by higher (P < 0.0001) concentrations of total and free T-4 and T-3 in juveniles than adults, the effect of sex on thyroid hormones was inconclusive. The effect of pregnancy was indicated by higher (P < 0.035) total and free T-4 and T-3 during early pregnancy compared to non-pregnancy. For both successful and unsuccessful pregnancy outcomes, maternal concentrations of thyroid hormones were highest during early, intermediate during mid, and lowest during late pregnancy (P < 0.07 to P < 0.0001). Compared to live and thriving births, concentrations of total and free T-4 and total T-3 were lower (P < 0.08 to P < 0.001) in dolphins with perinatal loss. Lower concentrations ranged from 10% to 14% during early, 11% to 18% during mid, and 23% to 37% during late pregnancy. In conclusion, the effects of age, reproductive status and stage of pregnancy on thyroid hormone concentrations are necessary factors to take into account when assessing thyroid gland function. Since perinatal loss may be associated with hypothyroidism in dolphins, analysis of serum T-4 and T-3 should be considered for those dolphins that have a history of pregnancy loss. (C) 2013 Elsevier Inc. All rights reserved. C1 [West, Kristi L.] Hawaii Pacific Univ, Coll Nat & Computat Sci, Kaneohe, HI 96744 USA. [Ramer, Jan; Proudfoot, Jeffry] Indianapolis Zoo, Indianapolis, IN 46222 USA. [Brown, Janine L.] Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. [Sweeney, Jay] Quest Global Management Dolphin Quest, San Diego, CA 92107 USA. [Hanahoe, Erin M.] Dolphin Quest Hawaii, Waikoloa, HI 96738 USA. [Reidarson, Torn] Sea World Calif, San Diego, CA 92109 USA. [Bergfelt, Don R.] US EPA, Washington, DC 20460 USA. RP West, KL (reprint author), Hawaii Pacific Univ, Coll Nat & Computat Sci, Kaneohe, HI 96744 USA. EM kwest@hpu.edu; jramer@indyzoo.com; brownjan@si.edu; jsweeney@dolphinquest.com; ehana-hoe@hotmail.com; reidarsongroup@me.com; jproudfoot@indyzoo.com; Bergfelt.Don@epa.gov FU Indianapolis Zoo; Dolphin Quest; Prescott Grant Program FX We thank each contributing institution including Dolphin Quest Hawaii, Dolphin Quest Oahu, Dolphin Quest Bermuda, Dolphin Quest French Polynesia, Indianapolis Zoo, Minnesota Zoo, Sea Life Park Hawaii, Sea World San Diego and West Edmonton Mall Dolphin Lagoon. We are especially thankful to the veterinary staff and animal husbandry staff at collaborating facilities for the diligent and frequent collection of samples. We would also like to thank Andre Theriault at the University of Hawaii at Manoa for providing laboratory facilities and guidance during this project. We are grateful to Nicole Presley for help with the laboratory work, to Holley Muraco for information on testis size at puberty, and to Dr. Mohd Beg for assistance with statistical analysis. We also thank Jennifer Leach, Whitney White, Susan Fertall White and Emily Spolarich for help with data management and references. F. David Horgen and Dr. Beg reviewed the manuscript. This study was funded by the Indianapolis Zoo. The first author (Dr. West) also received support from Dolphin Quest and the Prescott Grant Program during the course of this study. The views expressed in this article are those of the authors and do not necessarily reflect the views or policies of the USEPA or other institutions. NR 65 TC 3 Z9 3 U1 2 U2 19 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0016-6480 EI 1095-6840 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD FEB 1 PY 2014 VL 197 BP 73 EP 81 DI 10.1016/j.ygcen.2013.11.021 PG 9 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 301TP UT WOS:000330555300009 PM 24321177 ER PT J AU Morgan, AM Howard, AD Hobley, DEJ Moore, JM Dietrich, WE Williams, RME Burr, DM Grant, JA Wilson, SA Matsubara, Y AF Morgan, A. M. Howard, A. D. Hobley, D. E. J. Moore, J. M. Dietrich, W. E. Williams, R. M. E. Burr, D. M. Grant, J. A. Wilson, S. A. Matsubara, Y. TI Sedimentology and climatic environment of alluvial fans in the martian Saheki crater and a comparison with terrestrial fans in the Atacama Desert SO ICARUS LA English DT Article DE Geological processes; Mars; Mars, surface ID TRANSVERSE AEOLIAN RIDGES; NORTHERN CHILE; MIDLATITUDE SNOWPACKS; EBERSWALDE CRATER; IMPACT CRATERS; GALE CRATER; MARS; EVOLUTION; TRANSPORT; DESICCATION AB The deflated surfaces of the alluvial fans in Saheki crater reveal the most detailed record of fan stratigraphy and evolution found, to date, on Mars. During deposition of at least the uppermost 100 m of fan deposits, discharges from the source basin consisted of channelized flows transporting sediment (which we infer to be primarily sand- and gravel-sized) as bedload coupled with extensive overbank mud-rich flows depositing planar beds of sand-sized or finer sediment. Flow events are inferred to have been of modest magnitude (probably less than similar to 60 m(3)/s), of short duration, and probably occupied only a few distributaries during any individual flow event. Occasional channel avulsions resulted in the distribution of sediment across the entire fan. A comparison with fine-grained alluvial fans in Chile's Atacama Desert provides insights into the processes responsible for constructing the Saheki crater fans: sediment is deposited by channelized flows (transporting sand through boulder-sized material) and overbank mudflows (sand size and finer) and wind erosion leaves channels expressed in inverted topographic relief. The most likely source of water was snowmelt released after annual or epochal accumulation of snow in the headwater source basin on the interior crater rim during the Hesperian to Amazonian periods. We infer the Saheki fans to have been constructed by many hundreds of separate flow events, and accumulation of the necessary snow and release of meltwater may have required favorable orbital configurations or transient global warming. (C) 2013 Elsevier Inc. All rights reserved. C1 [Morgan, A. M.; Howard, A. D.; Hobley, D. E. J.; Matsubara, Y.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. [Moore, J. M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Dietrich, W. E.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Williams, R. M. E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Burr, D. M.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Grant, J. A.; Wilson, S. A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Morgan, AM (reprint author), Univ Virginia, Dept Environm Sci, POB 400123, Charlottesville, VA 22904 USA. EM amm5sy@virginia.edu RI Hobley, Daniel/G-5627-2011; Howard, Andrew/D-4148-2015; OI Hobley, Daniel/0000-0003-2371-0534; Howard, Andrew/0000-0001-8638-0320; Morgan, Alexander/0000-0003-2443-1676; Howard, Alan/0000-0002-5423-1600 FU NASA Graduate Student Researchers Program (NASA) [NNX12AM73H]; NASA Ames [NNX08AE47A]; NASA Planetary Geology and Geophysics [NNX08AM91G]; NASA Mars Data Analysis Program [NNX09AM02G]; Department of Environmental Sciences, University of Virginia FX This study was partially supported by the NASA Graduate Student Researchers Program (NASA grant NNX12AM73H), Cooperative Grant from NASA Ames (NNX08AE47A), NASA Planetary Geology and Geophysics (NNX08AM91G), NASA Mars Data Analysis Program (NNX09AM02G), and by an award to Y. Matsubara by the Department of Environmental Sciences, University of Virginia. NR 128 TC 17 Z9 18 U1 2 U2 21 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 FEB PY 2014 VL 229 BP 131 EP 156 DI 10.1016/j.icarus.2013.11.007 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 297LS UT WOS:000330257500011 ER PT J AU DeMeo, FE Binzel, RP Carry, B Polishook, D Moskovitz, NA AF DeMeo, Francesca E. Binzel, Richard P. Carry, Benoit Polishook, David Moskovitz, Nicholas A. TI Unexpected D-type interlopers in the inner main belt SO ICARUS LA English DT Article DE Asteroids; Spectroscopy; Asteroids, surfaces; Asteroids, composition ID ASTEROID SPECTROSCOPIC SURVEY; TRANS-NEPTUNIAN OBJECTS; NEAR-EARTH OBJECTS; ESO LARGE PROGRAM; DYNAMICAL FAMILIES; TROJAN ASTEROIDS; JUPITER TROJANS; SOLAR-SYSTEM; PHOTOMETRIC SURVEY; PHASE-II AB Very red featureless asteroids (spectroscopic D-types) are expected to have formed in the outer Solar System far from the Sun. They comprise the majority of asteroids in the Jupiter Trojan population, and are also commonly found in the outer main belt and among Hildas. The first evidence for D-types in the inner and middle parts of the main belt was seen in the Sloan Digital Sky Survey (SDSS). Here we report followup observations of SDSS D-type candidates in the near-infrared. Based on follow up observations of 13 SDSS D-type candidates, we find a similar to 20% positive confirmation rate. Known inner belt D-types range in diameter from roughly 7 to 30 km. Based on these detections we estimate there are similar to 100 inner belt D-types with diameters between 2.5 and 20 km. The lower and upper limits for total mass of inner belt D-types is 2 x 10(16) kg to 2 x 10(17) kg which represents 0.01-0.1% of the mass of the inner belt. The inner belt D-types have albedos at or above the upper end typical for D-types which raises the question as to whether these inner belt bodies represent only a subset of D-types, they have been altered by external factors such as weathering processes, or if they are compositionally distinct from other D-types. All Dtypes and candidates have diameters less than 30 km, yet there is no obvious parent body in the inner belt. Dynamical models have yet to show how D-types originating from the outer Solar System could penetrate into the inner reaches of the main belt under current scenarios of planet formation and subsequent Yarkovsky drift. (C) 2013 Elsevier Inc. All rights reserved. C1 [DeMeo, Francesca E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [DeMeo, Francesca E.; Binzel, Richard P.; Polishook, David; Moskovitz, Nicholas A.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Carry, Benoit] Observ Paris, Inst Mecan Celeste & Calcul Ephemerides, CNRS UMR8028, F-75014 Paris, France. [Carry, Benoit] ESA, European Space Astron Ctr, Madrid 28691, Spain. RP DeMeo, FE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-16, Cambridge, MA 02138 USA. EM fdemeo@cfa.harvard.edu FU Faculty of the European Space Astronomy Centre (ESAC); National Aeronautics and Space Administration [NNX12AL26G]; National Science Foundation [0907766] FX We thank Bill Bottke for discussions and providing source region probabilities for the NEOs. Observations reported here were obtained at the NASA Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement NCC 5-538 with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile. We acknowledge support from the Faculty of the European Space Astronomy Centre (ESAC) for FD's visit. DP is grateful to the AXA research fund. This material is based upon work supported by the National Aeronautics and Space Administration under Grant No. NNX12AL26G issued through the Planetary Astronomy Program and by the National Science Foundation under Grant 0907766. Any opinions, findings, and conclusions or recommendations expressed in this article are those of the authors and do not necessarily reflect the views of the National Aeronautics and Space Administration or the National Science Foundation. NR 59 TC 10 Z9 10 U1 0 U2 8 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 FEB PY 2014 VL 229 BP 392 EP 399 DI 10.1016/j.icarus.2013.11.026 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 297LS UT WOS:000330257500032 ER PT J AU Madej, OK Jonker, PG Trigo, MD Miskovicova, I AF Madej, O. K. Jonker, P. G. Trigo, M. Diaz Miskovicova, I. TI Variable Doppler shifts of the thermal wind absorption lines in low-mass X-ray binaries SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; X-rays: binaries; X-rays: individual: GX 13+1 ID OPTICAL LIGHT-CURVE; ACCRETION DISK WIND; BLACK-HOLE; GRO J1655-40; XMM-NEWTON; 2005 OUTBURST; GX 13+1; SPECTROSCOPY; CHANDRA; GRO-J1655-40 AB In this paper, we address the general applicability of the method pioneered by Zhang, Liao & Yao in which the motion of the compact object can be tracked using wind X-ray absorption lines. We present the velocity measurements of the thermal wind lines observed in the X-ray spectrum of a few low-mass X-ray binaries: GX 13+1, H 1743-322, GRO J1655-40 and GRS 1915+105. We find that the variability in the velocity of the wind lines in about all of the sources is larger than conceivable radial velocity variations of the compact object. GX 13+1 provides a potential exception, although it would require the red giant star to be massive with a mass of approximate to 5-6 M-circle dot. We conclude that the variability of the source luminosity occurring on a time-scale of days/months can affect the outflow properties making it difficult to track the orbital motion of the compact object using current observations. Given the intrinsic variability of the outflows we suggest that low-mass X-ray binaries showing stable coronae instead of an outflow (e. g. 4U 1254-69, MXB 1659-29, 4U 1624-49) could be more suitable targets for tracking the orbital motion of the compact object. C1 [Madej, O. K.; Jonker, P. G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Madej, O. K.; Jonker, P. G.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Trigo, M. Diaz] ESO, D-85748 Garching, Germany. [Miskovicova, I.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany. [Miskovicova, I.] Czech Tech Univ, Fac Elect Engn, CZ-16000 Prague 6, Czech Republic. RP Madej, OK (reprint author), Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands. EM O.Madej@sron.nl FU European Commission [ITN 215212]; GACR grants [13-33324S, 3-39464J] FX OKM thanks Mafred Hanke, Thomas Dauser, Rob Detmers, Jelle Kaastra, Tullio Bagnoli and Ton Raassen for useful discussions and help with the software packages for spectral fitting. We thank the referee for useful comments that helped us improve the paper. This research has made use of a collection of ISIS scripts provided by the Dr. Karl Remeis observatory, Bamberg, Germany at http://www.sternwarte.uni-erlangen.de/git.public/?p = isisscripts. IM acknowledges funding from the European Commission under grant agreement ITN 215212 'Black Hole Universe' and partial support by GACR grants 13-33324S and 3-39464J. NR 41 TC 3 Z9 3 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2014 VL 438 IS 1 BP 145 EP 155 DI 10.1093/mnras/stt2119 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IH UT WOS:000330457100031 ER PT J AU Bell, ME Murphy, T Kaplan, DL Hancock, P Gaensler, BM Banyer, J Bannister, K Trott, C Hurley-Walker, N Wayth, RB Macquart, JP Arcus, W Barnes, D Bernardi, G Bowman, JD Briggs, F Bunton, JD Cappallo, RJ Corey, BE Deshpande, A deSouza, L Emrich, D Goeke, R Greenhill, LJ Hazelton, BJ Herne, D Hewitt, JN Johnston-Hollitt, M Kasper, JC Kincaid, BB Koenig, R Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Pathikulangara, J Prabu, T Remillard, RA Rogers, AEE Roshi, A Salah, JE Sault, RJ Shankar, NU Srivani, KS Stevens, J Subrahmanyan, R Tingay, SJ Waterson, M Webster, RL Whitney, AR Williams, A Williams, CL Wyithe, JSB AF Bell, M. E. Murphy, T. Kaplan, D. L. Hancock, P. Gaensler, B. M. Banyer, J. Bannister, K. Trott, C. Hurley-Walker, N. Wayth, R. B. Macquart, J-P Arcus, W. Barnes, D. Bernardi, G. Bowman, J. D. Briggs, F. Bunton, J. D. Cappallo, R. J. Corey, B. E. Deshpande, A. deSouza, L. Emrich, D. Goeke, R. Greenhill, L. J. Hazelton, B. J. Herne, D. Hewitt, J. N. Johnston-Hollitt, M. Kasper, J. C. Kincaid, B. B. Koenig, R. Kratzenberg, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Pathikulangara, J. Prabu, T. Remillard, R. A. Rogers, A. E. E. Roshi, A. Salah, J. E. Sault, R. J. Shankar, N. Udaya Srivani, K. S. Stevens, J. Subrahmanyan, R. Tingay, S. J. Waterson, M. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. Wyithe, J. S. B. TI A survey for transients and variables with the Murchison Widefield Array 32-tile prototype at 154 MHz SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: interferometers; techniques: image processing; catalogues; radio continuum: general ID EXTRAGALACTIC RADIO-SOURCES; LOW-FREQUENCY VARIABILITY; INTERSTELLAR SCINTILLATION; COMPLETE SAMPLES; GALACTIC-CENTER; INTERPLANETARY SCINTILLATIONS; 318-MHZ VARIABILITY; SKY SURVEY; 2 FIELDS; GHZ AB We present a search for transient and variable radio sources at 154 MHz with the Murchison Widefield Array 32-tile prototype. 51 images were obtained that cover a field of view of 1430 deg(2) centred on Hydra A. The observations were obtained over three days in 2010 March and three days in 2011 April and May. The mean cadence of the observations was 26 min and there was additional temporal information on day and year time-scales. We explore the variability of a sample of 105 low-frequency radio sources within the field. Four bright (S > 6 Jy) candidate variable radio sources were identified that displayed low levels of short time-scale variability (26 min). We conclude that this variability is likely caused by simplifications in the calibration strategy or ionospheric effects. On the time-scale of 1 yr we find two sources that show significant variability. We attribute this variability to either refractive scintillation or intrinsic variability. No radio transients were identified and we place an upper limit on the surface density of sources rho < 7.5 x 10(-5) deg(-2) with flux densities > 5.5 Jy, and characteristic time-scales of both 26 min and 1 yr. C1 [Bell, M. E.; Murphy, T.; Hancock, P.; Gaensler, B. M.; Banyer, J.; deSouza, L.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Murphy, T.] Univ Sydney, Sch Informat Technol, Sydney, NSW 2006, Australia. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Bannister, K.; Bunton, J. D.; deSouza, L.; Koenig, R.; Pathikulangara, J.; Stevens, J.] CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia. [Trott, C.; Hurley-Walker, N.; Wayth, R. B.; Macquart, J-P; Arcus, W.; Emrich, D.; Herne, D.; Lynch, M. J.; Ord, S. M.; Tingay, S. J.; Waterson, M.; Williams, A.] Curtin Univ Technol, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Barnes, D.] Monash Univ, Monash eRes Ctr, Clayton, Vic 3168, Australia. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa. [Bowman, J. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Briggs, F.; Waterson, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [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.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Deshpande, A.; Prabu, T.; Roshi, A.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Goeke, R.; Hewitt, J. N.; Morgan, E.; Remillard, R. A.; Williams, C. L.] MIT, Haystack Observ, Westford, MA 01886 USA. [Greenhill, L. J.; Kasper, J. C.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Mitchell, D. A.; Sault, R. J.; Webster, R. L.; Wyithe, J. S. B.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Stevens, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. RP Bell, ME (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. EM mebell@physics.usyd.edu.au RI Bunton, John/A-4944-2008; Deshpande, Avinash/D-4868-2012; Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Udayashankar , N/D-4901-2012; Williams, Andrew/K-2931-2013; M, Manjunath/N-4000-2014; Hurley-Walker, Natasha/B-9520-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; OI Bannister, Keith/0000-0003-2149-0363; Gaensler, Bryan/0000-0002-3382-9558; Hancock, Paul/0000-0002-4203-2946; Wayth, Randall/0000-0002-6995-4131; Trott, Cathryn/0000-0001-6324-1766; Williams, Andrew/0000-0001-9080-0105; M, Manjunath/0000-0001-8710-0730; Hurley-Walker, Natasha/0000-0002-5119-4808; Emrich, David/0000-0002-4058-1837; Wyithe, Stuart/0000-0001-7956-9758; Murphy, Tara/0000-0002-2686-438X FU US National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF grants) [LE0775621, LE0882938]; US Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (CAASTRO); Australian Research Council Centre of Excellence [CE110001020]; Science Leveraging Fund of the New South Wales Department of Trade and Investment; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington from the New Zealand Ministry of Economic Development [MED-E1799]; Victoria University of Wellington (via IBM Shared University Research Grant); Australian Federal government; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University; International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of University of Western Australia; Western Australian State government FX This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the US National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753 and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the US Air Force Office of Scientific Research (grant FA9550-0510247). This work was supported by the Centre for All-sky Astrophysics (CAASTRO), an Australian Research Council Centre of Excellence (grant CE110001020) and through the Science Leveraging Fund of the New South Wales Department of Trade and Investment. Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the National Collaborative Research Infrastructure Strategy, Education Investment Fund and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. NR 88 TC 22 Z9 22 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 FEB PY 2014 VL 438 IS 1 BP 352 EP 367 DI 10.1093/mnras/stt2200 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IH UT WOS:000330457100046 ER PT J AU Wright, NJ Parker, RJ Goodwin, SP Drake, JJ AF Wright, Nicholas J. Parker, Richard J. Goodwin, Simon P. Drake, Jeremy J. TI Constraints on massive star formation: Cygnus OB2 was always an association SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: formation; stars: kinematics and dynamics; open clusters and associations: individual: Cygnus OB2 ID ORION NEBULA CLUSTER; STELLAR CLUSTERS; MOLECULAR CLOUDS; DYNAMICAL EVOLUTION; YOUNG CLUSTERS; BROWN DWARFS; CYG-OB2 ASSOCIATION; SOLAR NEIGHBORHOOD; SEGREGATION; REGION AB We examine substructure and mass segregation in the massive OB association Cygnus OB2 to better understand its initial conditions. Using a well-understood Chandra X-ray selected sample of young stars, we find that Cyg OB2 exhibits considerable physical substructure and has no evidence for mass segregation, both indications that the association is not dynamically evolved. Combined with previous kinematical studies we conclude that Cyg OB2 is dynamically very young, and what we observe now is very close to its initial conditions: Cyg OB2 formed as a highly substructured, unbound association with a low volume density (<100 stars pc(-3)). This is inconsistent with the idea that all stars form in dense, compact clusters. The massive stars in Cyg OB2 show no evidence for having formed particularly close to one another, nor in regions of higher than average density. Since Cyg OB2 contains stars as massive as similar to 100 M-circle dot, this result suggests that very massive stars can be born in relatively low-density environments. This would imply that massive stars in Cyg OB2 did not form by competitive accretion, or by mergers. C1 [Wright, Nicholas J.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Parker, Richard J.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Goodwin, Simon P.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Drake, Jeremy J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wright, NJ (reprint author), Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. EM nick.nwright@gmail.com NR 73 TC 38 Z9 38 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2014 VL 438 IS 1 BP 639 EP 646 DI 10.1093/mnras/stt2232 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IH UT WOS:000330457100065 ER PT J AU Guidorzi, C Mundell, CG Harrison, R Margutti, R Sudilovsky, V Zauderer, BA Kobayashi, S Cucchiara, A Melandri, A Pandey, SB Berger, E Bersier, D D'Elia, V Gomboc, A Greiner, J Japelj, J Kopac, D Kumar, B Malesani, D Mottram, CJ O'Brien, PT Rau, A Smith, RJ Steele, IA Tanvir, NR Virgili, F AF Guidorzi, C. Mundell, C. G. Harrison, R. Margutti, R. Sudilovsky, V. Zauderer, B. A. Kobayashi, S. Cucchiara, A. Melandri, A. Pandey, S. B. Berger, E. Bersier, D. D'Elia, V. Gomboc, A. Greiner, J. Japelj, J. Kopac, D. Kumar, B. Malesani, D. Mottram, C. J. O'Brien, P. T. Rau, A. Smith, R. J. Steele, I. A. Tanvir, N. R. Virgili, F. TI New constraints on gamma-ray burst jet geometry and relativistic shock physics SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: non-thermal ID AFTERGLOW LIGHT CURVES; EARLY OPTICAL AFTERGLOWS; X-RAY; OFF-AXIS; ALERT TELESCOPE; EARLY-TIME; INTERNAL SHOCKS; 2-COMPONENT JET; PROMPT EMISSION; COMPLETE SAMPLE AB We use high-quality, multiband observations of Swift GRB 120404A, from gamma-ray to radio frequencies, together with the new hydrodynamics code of van Eerten et al. to test the standard synchrotron shock model. The evolution of the radio and optical afterglow, with its prominent optical rebrightening at t(rest) similar to 260-2600 s, is remarkably well modelled by a decelerating jet viewed close to the jet edge, combined with some early re-energization of the shock. We thus constrain the geometry of the jet with half-opening and viewing angles of 23 degrees and 21 degrees, respectively, and suggest that wide jets viewed off-axis are more common in GRBs than previously thought. We also derive the fireball microphysics parameters epsilon(B) = 2.4 x 10(-4) and epsilon(e) = 9.3 x 10(-2) and a circumburst density of n = 240 cm(-3). The ability to self-consistently model the microphysics parameters and jet geometry in this way offers an alternative to trying to identify elusive canonical jet breaks at late times. The mismatch between the observed and model-predicted X-ray fluxes is explained by the local rather than the global cooling approximation in the synchrotron radiation model, constraining the microphysics of particle acceleration taking place in a relativistic shock and, in turn, emphasizing the need for a more realistic treatment of cooling in future developments of theoretical models. Finally, our interpretation of the optical peak as due to the passage of the forward shock synchrotron frequency highlights the importance of high-quality multiband data to prevent some optical peaks from being erroneously attributed to the onset of fireball deceleration. C1 [Guidorzi, C.] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy. [Mundell, C. G.; Harrison, R.; Kobayashi, S.; Bersier, D.; Smith, R. J.; Steele, I. A.; Virgili, F.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Margutti, R.; Zauderer, B. A.; Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sudilovsky, V.; Greiner, J.; Rau, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Cucchiara, A.] Univ Calif Santa Cruz, UCO, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Melandri, A.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Pandey, S. B.; Kumar, B.] Aryabhatta Res Inst Observat Sci, Naini Tal 263129, Uttarakhand, India. [D'Elia, V.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Gomboc, A.; Japelj, J.; Kopac, D.] Univ Ljubljana, Fac Math & Phys, SI-1000 Ljubljana, Slovenia. [Gomboc, A.] Ctr Excellence SPACE SI, SI-1000 Ljubljana, Slovenia. [Malesani, D.; Mottram, C. J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Kobehavn O, Denmark. [O'Brien, P. T.; Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Guidorzi, C (reprint author), Univ Ferrara, Dept Phys & Earth Sci, Via Saragat 1, I-44122 Ferrara, Italy. EM guidorzi@fe.infn.it OI D'Elia, Valerio/0000-0002-7320-5862 FU ASI (ASI-INAF) [I/088/06/0]; 'Large-Scale Facilities 2010' project [7746/2011]; Royal Society; Wolfson Foundation; Science and Technology Facilities Council; National Science Foundation [AST-1107973]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302954]; European Union; European Regional Development Fund; Republic of Slovenia, Ministry of Education, Science and Sport; NASA through the Astrophysics Theory Programme [NNX10AF62G]; NSF [AST-1009863]; Smithsonian Institution; Academia Sinica; Leibniz-Prize (DFG) [HA 1850/28-1] FX CG acknowledges ASI for financial support (ASI-INAF contract I/088/06/0) and University of Ferrara for use of the local HPC facility co-funded by the 'Large-Scale Facilities 2010' project (grant 7746/2011). CG thanks Hendrik van Eerten for useful discussions. CGM thanks the Royal Society, Wolfson Foundation and Science and Technology Facilities Council for support. EB and BAZ were supported in part by the National Science Foundation under Grant AST-1107973. BAZ is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302954. AG acknowledges founding from the Slovenian Research Agency and from the Centre of Excellence for Space Sciences and Technologies SPACE-SI, an operation partly financed by the European Union, the European Regional Development Fund and the Republic of Slovenia, Ministry of Education, Science and Sport. Development of the Boxfit code was supported in part by NASA through grant NNX10AF62G issued through the Astrophysics Theory Programme and by the NSF through grant AST-1009863. The NRAO is a facility of the NSF operated under cooperative agreement by AUI. Proposal VLA 12A-394 is acknowledged. The SMA is a joint project between SAO and the ASIAA and is funded by the Smithsonian Institution and the Academia Sinica. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Professor G. Hasinger (DFG grant HA 1850/28-1). We thank the anonymous referee for helpful comments that improved the paper. NR 115 TC 11 Z9 11 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 FEB PY 2014 VL 438 IS 1 BP 752 EP 767 DI 10.1093/mnras/stt2243 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IH UT WOS:000330457100074 ER PT J AU Gallo, E Plotkin, RM Jonker, PG AF Gallo, Elena Plotkin, Richard M. Jonker, Peter G. TI V4641 Sgr: a candidate precessing microblazar SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: individual: V4641 Sgr; ISM: jets and outflows; X-rays: binaries ID X-RAY BINARIES; BLACK-HOLE; MICROQUASAR V4641-SGR; SAX J1819.3-2525; JETS; EMISSION; OUTBURST; QUIESCENCE; LUMINOSITY; BLAZARS AB The X-ray spectrum of the Galactic X-ray binary V4641 Sgr in outburst has been found to exhibit a remarkably broad emission feature above 4 keV, with inferred equivalent widths up to 2 keV. Such a feature was first detected during the X-ray flaring activity associated with the giant outburst that the source experienced in 1999 September. The extraordinarily large equivalent width line was then ascribed to reflection/reprocessing of fluorescent Fe emission within an extended optically thick outflow enshrouding the binary system as a result of a short-lived, super-Eddington accretion episode. Making use of new and archival X-ray observations, we show here that a similar feature persists over four orders of magnitude in luminosity, down to Eddington ratios as low as log (L-X/L-Edd) similar or equal to -4.5, where the existence of an optically thick envelope appears at odds with any viable accretion flow model. Possible interpretations for this highly unusual X-ray spectrum include a blend of Doppler-shifted/boosted Fe lines from unresolved X-ray jets (a la SS433), or, the first Galactic analogue of a blazar spectrum, where the >4 keV emission would correspond to the onset of the inverse Compton hump. This either requires a low-inclination angle of the jet with respect to the line of sight, in agreement with the estimates for the 1999 superluminal jet (i(jet) < 10 degrees). The fast variability of the feature, combined with the high orbital axis inclination (60 degrees < i(orb) < 71 degrees), argue for a rapidly precessing accretion flow around V4641 Sgr, possibly leading to a transient microblazar behaviour. C1 [Gallo, Elena; Plotkin, Richard M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Gallo, Elena] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Jonker, Peter G.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, Peter G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, Peter G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. RP Gallo, E (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM egallo@umich.edu RI Plotkin, Richard/I-3221-2016 OI Plotkin, Richard/0000-0002-7092-0326 FU National Science Foundation [NSF PHY11-25915] FX This research was supported in part by the National Science Foundation under grant no. NSF PHY11-25915. EG would like to thank Mike Eracleous, Gabriele Ghisellini and Francesco Haardt for helpful suggestions. NR 32 TC 1 Z9 1 U1 0 U2 6 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 FEB PY 2014 VL 438 IS 1 BP L41 EP L45 DI 10.1093/mnrasl/slt152 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IH UT WOS:000330457100009 ER PT J AU Greaves, JS Kennedy, GM Thureau, N Eiroa, C Marshall, JP Maldonado, J Matthews, BC Olofsson, G Barlow, MJ Moro-Martin, A Sibthorpe, B Absil, O Ardila, DR Booth, M Broekhoven-Fiene, H Brown, DJA Cameron, AC del Burgo, C Di Francesco, J Eisloffel, J Duchene, G Ertel, S Holland, WS Horner, J Kalas, P Kavelaars, JJ Lestrade, JF Vican, L Wilner, DJ Wolf, S Wyatt, MC AF Greaves, J. S. Kennedy, G. M. Thureau, N. Eiroa, C. Marshall, J. P. Maldonado, J. Matthews, B. C. Olofsson, G. Barlow, M. J. Moro-Martin, A. Sibthorpe, B. Absil, O. Ardila, D. R. Booth, M. Broekhoven-Fiene, H. Brown, D. J. A. Cameron, A. Collier del Burgo, C. Di Francesco, J. Eisloeffel, J. Duchene, G. Ertel, S. Holland, W. S. Horner, J. Kalas, P. Kavelaars, J. J. Lestrade, J-F Vican, L. Wilner, D. J. Wolf, S. Wyatt, M. C. TI Alignment in star-debris disc systems seen by Herschel SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE circumstellar matter; planetary systems; infrared: stars ID MAIN-SEQUENCE STARS; SPIN-ORBIT MISALIGNMENT; ACCRETING MAGNETIC PROTOSTARS; RAPIDLY ROTATING STAR; KUIPER-BELT; HR 8799; EXOPLANETARY SYSTEMS; STELLAR ROTATION; EPSILON-ERIDANI; HABITABLE ZONE AB Many nearby main-sequence stars have been searched for debris using the far-infrared Herschel satellite, within the DEBRIS, DUNES and Guaranteed-Time Key Projects. We discuss here 11 stars of spectral types A-M where the stellar inclination is known and can be compared to that of the spatially resolved dust belts. The discs are found to be well aligned with the stellar equators, as in the case of the Sun's Kuiper belt, and unlike many close-in planets seen in transit surveys. The ensemble of stars here can be fitted with a star-disc tilt of less than or similar to 10 degrees. These results suggest that proposed mechanisms for tilting the star or disc in fact operate rarely. A few systems also host imaged planets, whose orbits at tens of au are aligned with the debris discs, contrary to what might be expected in models where external perturbers induce tilts. C1 [Greaves, J. S.; Thureau, N.; Brown, D. J. A.; Cameron, A. Collier] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Kennedy, G. M.; Wyatt, M. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Eiroa, C.; Marshall, J. P.; Maldonado, J.] Univ Autonoma Madrid, Fac Ciencias, Dpt Fis Teor, E-28049 Madrid, Spain. [Matthews, B. C.; Di Francesco, J.; Kavelaars, J. J.] Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. [Matthews, B. C.; Booth, M.; Broekhoven-Fiene, H.; Di Francesco, J.; Kavelaars, J. J.] Univ Victoria, Victoria, BC V8W 3P6, Canada. [Olofsson, G.] SCFAB, Stockholm Observ, SE-10691 Stockholm, Sweden. [Barlow, M. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Moro-Martin, A.] INTA, CSIC, Ctr Astrobiol, E-28850 Madrid, Spain. [Sibthorpe, B.; Holland, W. S.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Sibthorpe, B.] Univ Groningen, SRON, NL-9700 AV Groningen, Netherlands. [Absil, O.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Sart Tilman Par Liege, Belgium. [Ardila, D. R.] CALTECH, NASA, Herschel Sci Ctr, IPAC, Pasadena, CA 91125 USA. [del Burgo, C.] Inst Nacl Astrofis Opt & Electr, Puebla, Mexico. [Eisloeffel, J.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Duchene, G.; Kalas, P.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Duchene, G.; Ertel, S.] Univ Joseph Fourier, CNRS, IPAG, F-38400 St Martin Dheres, France. [Horner, J.] Univ New S Wales, Sch Phys, Dept Astrophys & Opt, Sydney, NSW 2052, Australia. [Kalas, P.] SETI Inst, Mountain View, CA 94043 USA. [Lestrade, J-F] CNRS, Observ Paris, F-75014 Paris, France. [Vican, L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24118 Kiel, Germany. RP Greaves, JS (reprint author), Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. EM jsg5@st-andrews.ac.uk RI Barlow, Michael/A-5638-2009; OI Barlow, Michael/0000-0002-3875-1171; Booth, Mark/0000-0001-8568-6336; Marshall, Jonathan/0000-0001-6208-1801; Horner, Jonti/0000-0002-1160-7970; Kennedy, Grant/0000-0001-6831-7547 FU ERC [279973]; Spanish grant [AYA 2011-26202] FX Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work was supported by ERC grant 279973 (GMK, MCW) and Spanish grant AYA 2011-26202 (CE, JPM, JM). NR 81 TC 19 Z9 19 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 FEB PY 2014 VL 438 IS 1 BP L31 EP L35 DI 10.1093/mnrasl/slt153 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IH UT WOS:000330457100007 ER PT J AU Kilic, M Hermes, JJ Gianninas, A Brown, WR Heinke, CO Agueros, MA Chote, P Sullivan, DJ Bell, KJ Harrold, ST AF Kilic, Mukremin Hermes, J. J. Gianninas, A. Brown, Warren R. Heinke, Craig O. Agueeros, M. A. Chote, Paul Sullivan, Denis J. Bell, Keaton J. Harrold, Samuel T. TI Found: the progenitors of AM CVn and supernovae .Ia SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: close; stars: individual: SDSS J075141.18-014120.9; stars: individual: SDSS J174140.49+652638.7; white dwarfs; Galaxy: stellar content ID WHITE-DWARF BINARY; SUB-CHANDRASEKHAR SUPERNOVAE; TIME-SERIES PHOTOMETER; MINUTE ORBITAL PERIOD; DIGITAL SKY SURVEY; DOUBLE-DETONATION; MASS MODELS; MERGER SYSTEMS; MILKY-WAY; STARS AB We present optical and X-ray observations of two tidally distorted, extremely low-mass white dwarfs (WDs) with massive companions. There is no evidence of neutron stars in our Chandra and XMM observations of these objects. SDSS J075141.18-014120.9 (J0751) is an eclipsing double WD binary containing a 0.19 M-circle dot WD with a 0.97 M-circle dot companion in a 1.9 h orbit. J0751 becomes the fifth eclipsing double WD system currently known. SDSS J174140.49+652638.7 (J1741) is another binary containing a 0.17 M-circle dot WD with an unseen M >= 1.11 M-circle dot WD companion in a 1.5-h orbit. With a mass ratio of approximate to 0.1, J1741 will have stable mass transfer through an accretion disc and turn into an interacting AM Canum Venaticorum (AM CVn) system in the next approximate to 160 Myr. With a mass ratio of 0.2, J0751 is likely to follow a similar evolutionary path. These are the first known AM CVn progenitor binary systems and they provide important constraints on the initial conditions for AM CVn. Theoretical studies suggest that both J0751 and J1741 may create thermonuclear supernovae in similar to 10(8) yr, either .Ia or Ia. Such explosions can account for similar to 1 per cent of the Type Ia supernova rate. C1 [Kilic, Mukremin; Gianninas, A.] Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. [Hermes, J. J.; Bell, Keaton J.; Harrold, Samuel T.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Hermes, J. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Brown, Warren R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Heinke, Craig O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Agueeros, M. A.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Chote, Paul; Sullivan, Denis J.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. RP Kilic, M (reprint author), Univ Oklahoma, Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. EM kilic@ou.edu RI Agueros, Marcel/K-7998-2014; Alexandros, Gianninas/B-8352-2016; OI Agueros, Marcel/0000-0001-7077-3664; Alexandros, Gianninas/0000-0002-8655-4308; Heinke, Craig/0000-0003-3944-6109 FU NSF [AST-1312678, AST-0909107]; Norman Hackerman Advanced Research Program; NSERC Discovery Grant Ingenuity New Faculty Award; NZ Marsden Fund FX MK and JJH acknowledge the support of the NSF under grants AST-1312678 and AST-0909107, and the Norman Hackerman Advanced Research Program. COH acknowledges support from an NSERC Discovery Grant and an Ingenuity New Faculty Award. DJS and PC thank the NZ Marsden Fund for financial support. NR 52 TC 26 Z9 26 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 FEB PY 2014 VL 438 IS 1 BP L26 EP L30 DI 10.1093/mnrasl/slt151 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IH UT WOS:000330457100006 ER PT J AU Givnish, TJ Barfuss, MHJ Van Ee, B Riina, R Schulte, K Horres, R Gonsiska, PA Jabaily, RS Crayn, DM Smith, JAC Winter, K Brown, GK Evans, TM Holst, BK Luther, H Till, W Zizka, G Berry, PE Sytsma, KJ AF Givnish, Thomas J. Barfuss, Michael H. J. Van Ee, Benjamin Riina, Ricarda Schulte, Katharina Horres, Ralf Gonsiska, Philip A. Jabaily, Rachel S. Crayn, Darren M. Smith, J. Andrew C. Winter, Klaus Brown, Gregory K. Evans, Timothy M. Holst, Bruce K. Luther, Harry Till, Walter Zizka, Georg Berry, Paul E. Sytsma, Kenneth J. TI Adaptive radiation, correlated and contingent evolution, and net species diversification in Bromeliaceae SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Biogeography; Evolutionary predictions; Epiphytes; Key innovations; Pollination syndromes; Species richness ID CRASSULACEAN ACID METABOLISM; ANCESTRAL CHARACTER STATES; ATLANTIC RAIN-FOREST; NDHF SEQUENCE DATA; VASCULAR EPIPHYTES; SOUTH-AMERICA; SOUTHEASTERN BRAZIL; CLIMATE-CHANGE; ELEVATIONAL GRADIENT; BROCCHINIA-REDUCTA AB We present an integrative model predicting associations among epiphytism, the tank habit, entangling seeds, C-3 vs. CAM photosynthesis, avian pollinators, life in fertile, moist montane habitats, and net rates of species diversification in the monocot family Bromeliaceae. We test these predictions by relating evolutionary shifts in form, physiology, and ecology to time and ancestral distributions, quantifying patterns of correlated and contingent evolution among pairs of traits and analyzing the apparent impact of individual traits on rates of net species diversification and geographic expansion beyond the ancestral Guayana Shield. All predicted patterns of correlated evolution were significant, and the temporal and spatial associations of phenotypic shifts with orogenies generally accorded with predictions. Net rates of species diversification were most closely coupled to life in fertile, moist, geographically extensive cordilleras, with additional significant ties to epiphytism, avian pollination, and the tank habit. The highest rates of net diversification were seen in the bromelioid tank-epiphytic clade (D-crown = 1.05 My(-1)), associated primarily with the Serra do Mar and nearby ranges of coastal Brazil, and in the core tillandsioids (D-crown = 0.67 My(-1)), associated primarily with the Andes and Central America. Six large-scale adaptive radiations and accompanying pulses of speciation account for 86% of total species richness in the family. This study is among the first to test a priori hypotheses about the relationships among phylogeny, phenotypic evolution, geographic spread, and net species diversification, and to argue for causality to flow from functional diversity to spatial expansion to species diversity. (C) 2013 Elsevier Inc. All rights reserved. C1 [Givnish, Thomas J.; Gonsiska, Philip A.; Sytsma, Kenneth J.] Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. [Barfuss, Michael H. J.; Till, Walter] Univ Vienna, Fac Life Sci, Dept Systemat & Evolutionary Bot, A-1030 Vienna, Austria. [Van Ee, Benjamin] Black Hills State Univ, Sch Nat Sci, Spearfish, SD 57799 USA. [Riina, Ricarda] CSIC, Real Jardin Bot, E-28014 Madrid, Spain. [Schulte, Katharina; Zizka, Georg] Res Inst Senckenberg, Dept Bot & Mol Evolut, D-60325 Frankfurt, Germany. [Schulte, Katharina; Zizka, Georg] Goethe Univ Frankfurt, D-60325 Frankfurt, Germany. [Schulte, Katharina; Crayn, Darren M.] James Cook Univ, Australian Trop Herbarium, Cairns, Qld 4878, Australia. [Horres, Ralf] GeriXPro, D-60438 Frankfurt, Germany. [Jabaily, Rachel S.] Rhodes Coll, Dept Biol, Memphis, TN 38112 USA. [Smith, J. Andrew C.] Univ Oxford, Dept Plant Sci, Oxford OX1 3RB, England. [Winter, Klaus] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Brown, Gregory K.] Univ Wyoming, Dept Bot, Laramie, WY 82071 USA. [Evans, Timothy M.] Grand Valley State Univ, Dept Biol, Allendale, MI 49401 USA. [Holst, Bruce K.] Marie Selby Bot Gardens, Sarasota, FL 34236 USA. [Luther, Harry] Natl Pk Board Headquarters, Gardens Bay, Singapore 259569, Singapore. [Berry, Paul E.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. RP Givnish, TJ (reprint author), Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. EM givnish@wisc.edu RI James Cook University, TESS/B-8171-2012; Schulte, Katharina/K-1256-2012; Crayn, Darren/A-7386-2011; Research ID, CTBCC /O-3564-2014; Riina, Ricarda/J-1032-2014; borba, jared/D-6810-2015 OI Crayn, Darren/0000-0001-6614-4216; Riina, Ricarda/0000-0002-7423-899X; FU National Science Foundation [DEB-9981587, DEB-0830036, DEB-0431258, DEB-0129446, DEB-0129414]; Hertel Gift Fund; Commission for Interdisciplinary Ecological Studies (KIOS) at the Austrian Academy of Sciences (OAW) [2007-02]; Deutsche Forschungsgemeinshaft [ZI 557/7-1, SCHU 2426/1-1]; Hessian initiative for the development of scientific and economic excellence (LOEWE) at the Biodiversity and Climate Research Centre FX The authors gratefully acknowledge financial support for this investigation by Grants from the National Science Foundation to PEB, KJS, and TJG (DEB-9981587), TJG (DEB-0830036 and DEB-0830036), KJS (DEB-0431258), and GKB and TME (DEB-0129446 and DEB-0129414), and from the Hertel Gift Fund to TJG; from the Commission for Interdisciplinary Ecological Studies (KIOS) at the Austrian Academy of Sciences (OAW; 2007-02 to WT and MHJB; and from the Deutsche Forschungsgemeinshaft (ZI 557/7-1, SCHU 2426/1-1) and the Hessian initiative for the development of scientific and economic excellence (LOEWE) at the Biodiversity and Climate Research Centre, Frankfurt am Mein, to GZ and KS. Plant material was kindly supplied by the Selby Botanical Garden, the Palmengarten Frankfurt am Main, and the Botanical Garden of Heidelberg. Cecile Ane provided invaluable advice on implementing MEDUSA and BiSSE. NR 258 TC 61 Z9 63 U1 7 U2 124 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 FEB PY 2014 VL 71 BP 55 EP 78 DI 10.1016/j.ympev.2013.10.010 PG 24 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 294ZI UT WOS:000330086000005 PM 24513576 ER PT J AU Collins, KA Eastman, JD Beatty, TG Siverd, RJ Gaudi, BS Pepper, J Kielkopf, JF Johnson, JA Howard, AW Fischer, DA Manner, M Bieryla, A Latham, DW Fulton, BJ Gregorio, J Buchhave, LA Jensen, ELN Stassun, KG Penev, K Crepp, JR Hinkley, S Street, RA Cargile, P Mack, CE Oberst, TE Avril, RL Mellon, SN McLeod, KK Penny, MT Stefanik, RP Berlind, P Calkins, ML Mao, QQ Richert, AJW Depoy, DL Esquerdo, GA Gould, A Marshall, JL Oelkers, RJ Pogge, RW Trueblood, M Trueblood, P AF Collins, Karen A. Eastman, Jason D. Beatty, Thomas G. Siverd, Robert J. Gaudi, B. Scott Pepper, Joshua Kielkopf, John F. Johnson, John Asher Howard, Andrew W. Fischer, Debra A. Manner, Mark Bieryla, Allyson Latham, David W. Fulton, Benjamin J. Gregorio, Joao Buchhave, Lars A. Jensen, Eric L. N. Stassun, Keivan G. Penev, Kaloyan Crepp, Justin R. Hinkley, Sasha Street, Rachel A. Cargile, Phillip Mack, Claude E. Oberst, Thomas E. Avril, Ryan L. Mellon, Samuel N. McLeod, Kim K. Penny, Matthew T. Stefanik, Robert P. Berlind, Perry Calkins, Michael L. Mao, Qingqing Richert, Alexander J. W. Depoy, Darren L. Esquerdo, Gilbert A. Gould, Andrew Marshall, Jennifer L. Oelkers, Ryan J. Pogge, Richard W. Trueblood, Mark Trueblood, Patricia TI KELT-6b: A P similar to 7.9 DAY HOT SATURN TRANSITING A METAL-POOR STAR WITH A LONG-PERIOD COMPANION SO ASTRONOMICAL JOURNAL LA English DT Article DE instrumentation: adaptive optics; planetary systems; stars: individual (KELT-6, BD+31 2447, TYC 2532-556-1, HD 209458); techniques: photometric; techniques: spectroscopic ID EXOPLANET HD 209458B; SUN-LIKE STAR; K-DWARF STAR; PLANETARY TRANSITS; IMAGE SUBTRACTION; RADIAL-VELOCITY; GIANT PLANETS; MONTE-CARLO; MASS STARS; TELESCOPE AB We report the discovery of KELT-6b, a mildly inflated Saturn-mass planet transiting a metal-poor host. The initial transit signal was identified in KELT-North survey data, and the planetary nature of the occulter was established using a combination of follow-up photometry, high-resolution imaging, high-resolution spectroscopy, and precise radial velocity measurements. The fiducial model from a global analysis including constraints from isochrones indicates that the V = 10.38 host star ( BD+ 31 2447) is a mildly evolved, late-F star with T-eff = 6102 +/- 43 K, log g* = 4.07(-0.07)(+0.04), and [Fe/H] = -0.28 +/- 0.04, with an inferred mass M* = 1.09 +/- 0.04M(circle dot) and radius R-* = 1.58(-0.09)(+0.16) R-circle dot. The planetary companion has mass M-P = 0.43 +/- 0.05MJup, radius R-P = 1.19(-0.08)(+0.13) R-Jup, surface gravity log g(P) = 2.86(-0.08)(+0.06), and density rho(P) = 0.31(-0.08)(+0.07) g cm(-3.) The planet is on an orbit with semimajor axis a = 0.079 +/- 0.001 AU and eccentricity e = 0.22(-0.10)(+0.12), which is roughly consistent with circular, and has ephemeris of T-c( BJD(TDB)) = 2456347.79679 +/- 0.00036 and P = 7.845631 +/- 0.000046 days. Equally plausible fits that employ empirical constraints on the host-star parameters rather than isochrones yield a larger planet mass and radius by similar to 4%-7%. KELT-6b has surface gravity and incident flux similar to HD 209458b, but orbits a host that is more metal poor than HD 209458 by similar to 0.3 dex. Thus, the KELT-6 system offers an opportunity to perform a comparative measurement of two similar planets in similar environments around stars of very different metallicities. The precise radial velocity data also reveal an acceleration indicative of a longer-period third body in the system, although the companion is not detected in Keck adaptive optics images. C1 [Collins, Karen A.; Kielkopf, John F.] Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. [Eastman, Jason D.; Street, Rachel A.] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Eastman, Jason D.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Beatty, Thomas G.; Gaudi, B. Scott; Penny, Matthew T.; Gould, Andrew; Pogge, Richard W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Siverd, Robert J.; Pepper, Joshua; Stassun, Keivan G.; Cargile, Phillip; Mack, Claude E.; Mao, Qingqing] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Pepper, Joshua] Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA. [Johnson, John Asher] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Johnson, John Asher] NASA Exoplanet Sci Inst NExScI, Pasadena, CA 91125 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Manner, Mark] Spot Observ, Nunnelly, TN 37137 USA. [Manner, Mark] Montgomery Bell Acad, Nashville, TN 37205 USA. [Bieryla, Allyson; Latham, David W.; Stefanik, Robert P.; Berlind, Perry; Calkins, Michael L.; Esquerdo, Gilbert A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gregorio, Joao] Atalaia Grp & Crow Observ, Portalegre, Portugal. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, Copenhagen, Denmark. [Buchhave, Lars A.] Geol Museum, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Jensen, Eric L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Penev, Kaloyan] Princeton Univ, Princeton, NJ 08544 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Avril, Ryan L.; Mellon, Samuel N.] Westminster Coll, New Wilmington, PA 16172 USA. [McLeod, Kim K.] Wellesley Coll, Wellesley, MA 02481 USA. [Richert, Alexander J. W.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Depoy, Darren L.; Marshall, Jennifer L.; Oelkers, Ryan J.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Depoy, Darren L.; Marshall, Jennifer L.; Oelkers, Ryan J.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Trueblood, Mark; Trueblood, Patricia] Winer Observ, Sonoita, AZ 85637 USA. RP Collins, KA (reprint author), Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. RI Howard, Andrew/D-4148-2015; Mao, Qingqing/E-2043-2016; OI Howard, Andrew/0000-0001-8638-0320; Mao, Qingqing/0000-0001-6001-6723; Eastman, Jason/0000-0003-3773-5142; Richert, Alexander/0000-0002-9613-6863; Jensen, Eric/0000-0002-4625-7333; Pepper, Joshua/0000-0002-3827-8417; Fischer, Debra/0000-0003-2221-0861 FU NASA Kentucky Space Grant Consortium Graduate Fellowship; NASA [NNG04GO70G, NNX09AB29G]; 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 [AST-0849736, AST-1009810]; NSF CAREER [AST-1056524]; NSF [1108686]; Kepler Mission through NASA [NNX11AB99A]; National Science Foundation [AST-1203023] FX K.A.C. was supported by a NASA Kentucky Space Grant Consortium Graduate Fellowship. 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. Work by B.S.G. and T.G.B. was partially supported by NSF CAREER Grant AST-1056524. K.P. acknowledges support from NASA grant NNX09AB29G and NSF award number 1108686. We thank the anonymous referee for a thoughtful reading of the manuscript and for useful suggestions. We thank GeoffMarcy and Howard Isaacson for Keck HIRES observations, calibration, and reduction of spectra to 1D form. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit ofMauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. 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.). A portion of this work was supported by the National Science Foundation under grant Nos. AST-1203023. We thank Roberto Zambelli of Societa Astronomica Lunae for participation in the KELT followup network. This work has made use of NASA's AstrophysicsData System, the Exoplanet OrbitDatabase at exoplanets. org, the Extrasolar Planet Encyclopedia at exoplanet. eu (Schneider et al. 2011), the SIMBAD database operated at CDS, Strasbourg, France, and Systemic (Meschiari et al. 2009). NR 84 TC 16 Z9 16 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2014 VL 147 IS 2 AR 39 DI 10.1088/0004-6256/147/2/39 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 291OD UT WOS:000329837100015 ER PT J AU Torres, G Vaz, LPR Lacy, CHS Claret, A AF Torres, Guillermo Vaz, Luiz Paulo R. Lacy, Claud H. Sandberg Claret, Antonio TI ABSOLUTE PROPERTIES OF THE ECLIPSING BINARY SYSTEM AQ SERPENTIS: A STRINGENT TEST OF CONVECTIVE CORE OVERSHOOTING IN STELLAR EVOLUTION MODELS SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; stars: evolution; stars: fundamental parameters ID LINED SPECTROSCOPIC BINARIES; M-CIRCLE-DOT; BOLOMETRIC CORRECTIONS; Y-2 ISOCHRONES; MASS STARS; ATMOSPHERES; CONSTRAINTS; EXTINCTION; DIMENSIONS; CURVES AB We report differential photometric observations and radial-velocity measurements of the detached, 1.69 day period, double-lined eclipsing binary AQ Ser. Accurate masses and radii for the components are determined to better than 1.8% and 1.1%, respectively, and are M-1 = 1.417 +/- 0.021 M circle dot, M-2 = 1.346 +/- 0.024 M circle dot, R-1 = 2.451 +/- 0.027 R circle dot, and R-2 = 2.281 +/- 0.014 R circle dot. The temperatures are 6340 +/- 100 K (spectral type F6) and 6430 +/- 100 K (F5), respectively. Both stars are considerably evolved, such that predictions from stellar evolution theory are particularly sensitive to the degree of extra mixing above the convective core (overshoot). The component masses are different enough to exclude a location in the H-R diagram past the point of central hydrogen exhaustion, which implies the need for extra mixing. Moreover, we find that current main-sequence models are unable to match the observed properties at a single age even when allowing the unknown metallicity, mixing length parameter, and convective overshooting parameter to vary freely and independently for the two components. The age of the more massive star appears systematically younger. AQ Ser and other similarly evolved eclipsing binaries showing the same discrepancy highlight an outstanding and largely overlooked problem with the description of overshooting in current stellar theory. C1 [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vaz, Luiz Paulo R.] ICEx UFMG, Depto Fis, BR-30161970 Belo Horizonte, MG, Brazil. [Lacy, Claud H. Sandberg] Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. [Claret, Antonio] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu; lpv@fisica.ufmg.br; clacy@uark.edu; claret@iaa.es FU NSF [AST-1007992]; CNPq; FAPEMIG; CAPES FX We thank P. Berlind, M. Calkins, G. Esquerdo, D. W. Latham, and R. P. Stefanik for their assistance in obtaining the spectra of AQ Ser, and R.J. Davis for maintaining the echelle database at the Harvard-Smithsonian Center for Astrophysics. We also thank Dr A. William (Bill) Neely, who operates and maintains the NFO WebScope, and who handles preliminary processing of the images and their distribution. We are grateful to the anonymous referee for helpful comments. G.T. acknowledges partial support from this work from NSF grant AST-1007992. L.P.R.V. gratefully acknowledges partial support from the Brazilian agencies CNPq, FAPEMIG, and CAPES. NR 63 TC 13 Z9 13 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2014 VL 147 IS 2 AR 36 DI 10.1088/0004-6256/147/2/36 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 291OD UT WOS:000329837100012 ER PT J AU Van Dyk, SD Zheng, WK Fox, OD Cenko, SB Clubb, KI Filippenko, AV Foley, RJ Miller, AA Smith, N Kelly, PL Lee, WH Ben-Ami, S Gal-Yam, A AF Van Dyk, Schuyler D. Zheng, WeiKang Fox, Ori D. Cenko, S. Bradley Clubb, Kelsey I. Filippenko, Alexei V. Foley, Ryan J. Miller, Adam A. Smith, Nathan Kelly, Patrick L. Lee, William H. Ben-Ami, Sagi Gal-Yam, Avishay TI THE TYPE IIb SUPERNOVA 2013df AND ITS COOL SUPERGIANT PROGENITOR SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 4414); stars: evolution; supernovae: general; supernovae: individual (SN 2013df) ID DIGITAL SKY SURVEY; SN 1993J; BINARY PROGENITOR; OPTICAL SPECTROSCOPY; STELLAR PHOTOMETRY; UBVRI PHOTOMETRY; HUBBLE CONSTANT; SHOCK BREAKOUT; LIGHT CURVES; NGC 4414 AB We have obtained early-time photometry and spectroscopy of supernova (SN) 2013df in NGC 4414. The SN is clearly of Type IIb, with notable similarities to SN 1993J. From its luminosity at secondary maximum light, it appears that less 56Ni (less than or similar to 0.06 M circle dot) was synthesized in the SN 2013df explosion than was the case for the SNe IIb 1993J, 2008ax, and 2011dh. Based on a comparison of the light curves, the SN 2013df progenitor must have been more extended in radius prior to explosion than the progenitor of SN 1993J. The total extinction for SN 2013df is estimated to be A(V) = 0.30 mag. The metallicity at the SN location is likely to be solar. We have conducted Hubble Space Telescope (HST) Target of Opportunity observations of the SN with the Wide Field Camera 3, and from a precise comparison of these new observations to archival HST observations of the host galaxy obtained 14 yr prior to explosion, we have identified the progenitor of SN 2013df to be a yellow supergiant, somewhat hotter than a red supergiant progenitor for a normal Type II-Plateau SN. From its observed spectral energy distribution, assuming that the light is dominated by one star, the progenitor had effective temperature T-eff = 4250 +/- 100 K and a bolometric luminosity L-bol = 104.94 +/- 0.06 L circle dot. This leads to an effective radius R-eff = 545 +/- 65 R circle dot. The star likely had an initial mass in the range of 13-17M circle dot; however, if it was a member of an interacting binary system, detailed modeling of the system is required to estimate this mass more accurately. The progenitor star of SN 2013df appears to have been relatively similar to the progenitor of SN 1993J. C1 [Van Dyk, Schuyler D.] Spitzer Sci Center Caltech, Pasadena, CA 91125 USA. [Zheng, WeiKang; Fox, Ori D.; Clubb, Kelsey I.; Filippenko, Alexei V.; Kelly, Patrick L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Foley, Ryan J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Miller, Adam A.] Jet Prop Lab, Pasadena, CA 91109 USA. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85720 USA. [Lee, William H.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Ben-Ami, Sagi; Gal-Yam, Avishay] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. RP Van Dyk, SD (reprint author), Spitzer Sci Center Caltech, Mail Code 220-6, Pasadena, CA 91125 USA. EM vandyk@ipac.caltech.edu OI Van Dyk, Schuyler/0000-0001-9038-9950 FU W. M. Keck Foundation; NASA [NNX09AH71G, NNX09AT02G, NNX10AI27G, NNX12AE66G, GO-12888, GO-13030, HST-HF-51325.01]; CONACyT [INFR2009- 01-122785]; UNAM PAPIIT [IN113810]; UC MEXUS-CONACyT grant; Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund; Christopher R. Redlich Fund; TABASGO Foundation; NSF [AST1211916]; EU/FP7 via ERC [307260]; ISA FX This work is based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under NASA contract NAS5-26555. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. KAIT and its ongoing research 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 and Jim Katzman Foundation, and the TABASGO Foundation. We thank the RATIR instrument team and the staff of the Observatorio Astron omico Nacional on Sierra San Pedro Martir. RATIR is a collaboration between the University of California, the Universidad Nacional Autonoma de Mexico, NASA Goddard Space Flight Center, and Arizona State University, benefiting from the loan of an H2RG detector from Teledyne Scientific and Imaging. RATIR, the automation of the Harold L. Johnson Telescope of the Observatorio Astronomico Nacional on Sierra San Pedro Martir, and the operation of both are funded by the partner institutions and through NASA grants NNX09AH71G, NNX09AT02G, NNX10AI27G, and NNX12AE66G, CONACyT grants INFR2009- 01-122785, UNAM PAPIIT grant IN113810, and a UC MEXUS-CONACyT grant. Support for this research was provided by NASA through grants GO-12888 and GO-13030 from STScI. A.V.F. and his group at UC Berkeley also wish to acknowledge generous support from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST1211916. Research by A.G. is supported by the EU/FP7 via ERC grant n 307260, " The Quantum Universe" I-Core program by the Israeli Committee for planning and budgeting, the ISF, GIF, and Minerva grants, and the Kimmel award. S.B. is supported by the Ilan Ramon Fellowship from ISA. A.A.M. acknowledges support for this work by NASA from a Hubble Fellowship grant HST-HF-51325.01, awarded by STScI, operated by AURA, Inc., for NASA, under contract NAS 5-Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 81 TC 28 Z9 28 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2014 VL 147 IS 2 AR 37 DI 10.1088/0004-6256/147/2/37 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 291OD UT WOS:000329837100013 ER PT J AU van Weeren, RJ Intema, HT Lal, DV Bonafede, A Jones, C Forman, WR Rottgering, HJA Bruggen, M Stroe, A Hoeft, M Nuza, SE de Gasperin, F AF van Weeren, R. J. Intema, H. T. Lal, D. V. Bonafede, A. Jones, C. Forman, W. R. Rottgering, H. J. A. Brueggen, M. Stroe, A. Hoeft, M. Nuza, S. E. de Gasperin, F. TI THE DISCOVERY OF A RADIO HALO IN PLCK G147.3-16.6 AT Z=0.65 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: clusters: individual (PLCK G147.3-16.6); galaxies: clusters: intracluster medium; large-scale structure of universe; radiation mechanisms: non-thermal; X-rays: galaxies: clusters ID GALAXY CLUSTERS; COSMIC-RAYS; EMISSION; ELECTRONS; MODELS; COMA AB Recent X-ray and Sunyaev-Zel'dovich (SZ) observations have dramatically increased the number of known distant galaxy clusters. In somemerging, low-redshift (z < 0.4) clusters, centrally located, diffuse, extended radio emission (radio halos) has been found. Using the Giant Metrewave Radio Telescope (GMRT), we report the detection of diffuse radio emission in the binary-merging cluster PLCK G147.3-16.6 located at z = 0.65. We classify the emission as a giant radio halo due to its large physical extent of about 0.9 Mpc and its low-surface brightness. We measure an integrated flux density of 7.3 +/- 1.1 mJy at 610 MHz for the radio halo, resulting in a 1.4 GHz radio power of 5.1 x 10(24) W Hz(-1). The radio halo power is consistent with that expected from the known correlation between X-ray luminosity or the cluster integrated SZ signal and radio power. Our observations also suggest that more of these distant radio halos could be discovered with the GMRT. C1 [van Weeren, R. J.; Jones, C.; Forman, W. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Intema, H. T.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Lal, D. V.] TIFR, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Bonafede, A.; Brueggen, M.; de Gasperin, F.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Rottgering, H. J. A.; Stroe, A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Hoeft, M.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Nuza, S. E.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. RP van Weeren, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rvanweeren@cfa.harvard.edu RI Intema, Huib/D-1438-2012; OI Intema, Huib/0000-0002-5880-2730; de Gasperin, Francesco/0000-0003-4439-2627; van Weeren, Reinout/0000-0002-0587-1660; Forman, William/0000-0002-9478-1682 FU NASA through the Einstein Post-doctoral [PF2-130104]; Chandra X-ray Center; ESA Member States; USA (NASA); Smithsonian Astrophysical Observatory for NASA [NAS8-03060]; National Radio Astronomy Observatory; National Science Foundation under Associated Universities, Inc.; research group FOR [1254]; Deutsche Forschungsgemeinschaft: "Magnetisation of interstellar and intergalactic media: the prospects of low-frequency radio observations."; DFG [MU1020 16-1] FX We used observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacion Galileo Galilei of the Istituto Nazionale di Astrofisica (INAF) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). R.J.W. is supported by NASA through the Einstein Post-doctoral 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. H.T.I. acknowledges support from the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. A.B., M.B., and M.H. acknowledge support by the research group FOR 1254 funded by the Deutsche Forschungsgemeinschaft: "Magnetisation of interstellar and intergalactic media: the prospects of low-frequency radio observations." S.E.N. is supported by the DFG grant MU1020 16-1. NR 25 TC 8 Z9 8 U1 0 U2 0 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 FEB 1 PY 2014 VL 781 IS 2 AR L32 DI 10.1088/2041-8205/781/2/L32 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 292OK UT WOS:000329911400009 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 Island history affects faunal composition: the treeshrews (Mammalia: Scandentia: Tupaiidae) from the Mentawai and Batu Islands, Indonesia SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE biogeography; conservation; cranium; digits; hand; mandible; manus; rays; skull; South-East Asia ID MOLECULAR PHYLOGENY; SOUTHEAST-ASIA; CONSERVATION; TAXONOMY; MORPHOLOGY; CRYPTOTIS; SORICIDAE; MACAQUES AB The Mentawai and Batu Island groups off the west coast of Sumatra have a complicated geological and biogeographical history. The Batu Islands have shared a connection with the Sumatran mainland' during periods of lowered sea level, whereas the Mentawai Islands, despite being a similar distance from Sumatra, have remained isolated from Sumatra, and probably from the Batu Islands as well. These contrasting historical relationships to Sumatra have influenced the compositions of the respective mammalian faunas of these island groups. Treeshrews (Scandentia, Tupaiidae) from these islands have, at various times in their history, been recognized as geographically circumscribed populations of a broadly distributed Tupaia glis, subspecies, or distinct species. We used multivariate analyses of measurements from the skull and hands to compare the island populations from Siberut (Mentawai Islands) and Tanahbala (Batu Islands) with the geographically adjacent species from the southern Mentawai Islands (T.chrysogaster) and Sumatra (T.ferruginea). Results from both the skull and manus of the Siberut population show that it is most similar to T.chrysogaster, whereas the Tanahbala population is more similar to T.ferruginea, confirming predictions based on island history. These results are further corroborated by mammae counts. Based on these lines of evidence, we include the Siberut population in T.chrysogaster and the Tanahbala population in T.ferruginea. Our conclusions expand the known distributions of both the Mentawai and Sumatran species. The larger geographical range of the endangered T.chrysogaster has conservation implications for this Mentawai endemic, so populations and habitat should be re-evaluated on each of the islands it inhabits. However, until such a re-evaluation is conducted, we recommend that the IUCN Red List status of this species be changed from Endangered' to Data Deficient'.Published 2013. This article is a U.S. Government work and is in the public domain in the USA, Biological Journal of the Linnean Society, 2014, 111, 290-304. 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] US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Smithsonian Inst, 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; US 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 E.J.S. and L.E.O. Additional support was provided to N.W. from the US Geological Survey's Patuxent Wildlife Research Center and to N.C.M 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, American Museum of Natural History (AMNH), New York, NY, USA; R. Portela-Miguez, L. Tomsett, and P. Jenkins, The Natural History Museum (BMNH), London, UK; B. Stanley and L. Heaney, Field Museum of Natural History (FMNH), Chicago, IL, USA; J. Dines, Los Angeles County Museum of Natural History (LACM), Los Angeles, CA, USA; J. Chupasko and M. Omura, Museum of Comparative Zoology at Harvard University (MCZ), Cambridge, MA, USA; C. Conroy and J. Patton, Museum of Vertebrate Zoology at University of California (MVZ), Berkeley, CA, USA; R. Winkler, Naturhistorisches Museum Basel (NMB), Basel, Switzerland; B. Herzig, A. Bibl, and A. Gamauf, Naturhistorisches Museum Wien (NMW), Vienna, Austria; H. van Grouw, Nationaal Natuurhistorisch Museum (RMNH), Leiden, The Netherlands; L. Gordon, R. Thorington, K. Helgen, and D. Lunde, United States National Museum of Natural History (USNM), Washington, DC, USA; R. Angermann and F. Mayer, Museum fur Naturkunde (ZMB), Berlin, Germany; and M. Anderson, Zoologisk Museum University of Copenhagen (ZMUC), Copenhagen, Denmark. 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 an X-ray of the T. glis siberu holotype. We thank Tim Webster for information on macaques and four anonymous reviewers 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 US Government. NR 42 TC 2 Z9 2 U1 1 U2 20 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 FEB PY 2014 VL 111 IS 2 BP 290 EP 304 DI 10.1111/bij.12195 PG 15 WC Evolutionary Biology SC Evolutionary Biology GA 290FE UT WOS:000329738700006 ER PT J AU Eberhard, WG AF Eberhard, William G. TI A new view of orb webs: multiple trap designs in a single structure SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE orb webs; orbicularian spiders; radius-density hypothesis ID LEUCAUGE-MARIANA ARANEAE; WEAVING SPIDERS ARANEAE; PREY CAPTURE; ASYMMETRY; SILK; EVOLUTION; ARANEIDAE; TETRAGNATHIDAE; CONSTRUCTION; NEPHILIDAE AB Spider orb webs are impressive for their apparently uniform geometric patterns. There are, however, consistent, substantial and taxonomically widespread periphery-to-hub differences in the distances between both adjacent radii and between sticky spiral lines. Radii in typical orbs were on average about 4-5 times farther apart at the outer edge than the inner edge of the area covered by sticky lines. Distances between sticky spiral loops were on average about two times larger near the outer edge than in more inner portions. This pattern in sticky spiral spacing was absent in the modified orbs of Nephila clavipes, in which distances between radii varied less. Thus, patterns in sticky spiral spacing may be related to inter-radial spacing; there is, however, probably no single explanation for all of the different patterns of sticky spiral spacing. The patterned differences in radius and sticky spiral spacing have important consequences for understanding orb function, because the lines in a prey's immediate vicinity largely determine whether it will be stopped and then retained, and elementary physics dictates that contact with more lines will tend to increase prey being stopped and retained. Rather than being a unit trap with a single set of prey capture properties, an orb has locally different trapping properties in different sectors. Abandoning the previous typological style of discussion of the' ability of a given design to stop and retain prey promises to lead to improved understanding of orb web designs.Published 2014. This article is a U.S. Government work and is in the public domain in the USA, Biological Journal of the Linnean Society, 2014, 111, 437-449. 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, Ciudad Univ, San Jose, Costa Rica. EM william.eberhard@gmail.com FU Smithsonian Tropical Research Institute; Vicerrectoria de Investigacion of the Universidad de Costa Rica FX I thank H. W. Levi for identifying specimens, Y. D. Lubin, G. Barrantes, S. Zschokke, A. Sensenig, anonymous reviewers and especially K. Harms for helpful comments on preliminary versions of the manuscript, and the Smithsonian Tropical Research Institute and the Vicerrectoria de Investigacion of the Universidad de Costa Rica for financial support. NR 57 TC 4 Z9 4 U1 1 U2 32 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 FEB PY 2014 VL 111 IS 2 BP 437 EP 449 DI 10.1111/bij.12207 PG 13 WC Evolutionary Biology SC Evolutionary Biology GA 290FE UT WOS:000329738700016 ER PT J AU Ojaveer, H Galil, BS Minchin, D Olenin, S Amorim, A Canning-Clode, J Chainho, P Copp, GH Gollasch, S Jelmert, A Lehtiniemi, M McKenzie, C Mikus, J Miossec, L Occhipinti-Ambrogi, A Pecarevic, M Pederson, J Quilez-Badia, G Wijsman, JWM Zenetos, A AF Ojaveer, Henn Galil, Bella S. Minchin, Dan Olenin, Sergej Amorim, Ana Canning-Clode, Joao Chainho, Paula Copp, Gordon H. Gollasch, Stephan Jelmert, Anders Lehtiniemi, Maiju McKenzie, Cynthia Mikus, Josip Miossec, Laurence Occhipinti-Ambrogi, Anna Pecarevic, Marijana Pederson, Judith Quilez-Badia, Gemma Wijsman, Jeroen W. M. Zenetos, Argyro TI Ten recommendations for advancing the assessment and management of non-indigenous species in marine ecosystems SO MARINE POLICY LA English DT Article DE Marine stressors; Non-native species; International experience; Indicators; EU MSFD ID BIOLOGICAL INVASIONS; CAULERPA-TAXIFOLIA; CALIFORNIA; PATHWAYS; SCIENCE; TRENDS; TRADE AB The main objective of recent international legislative measures and policies concerning marine ecosystems is to ensure sustainable environmental management to maintain a good status for marine waters, habitats and resources, with the ultimate target of achieving an integrated ecosystem-based approach to management. Because bioinvasions pose significant threats to marine ecosystems and the goods and services these provide, non-indigenous species (NIS) are included in the more recent legislative documents. A major challenge for the scientific community is to translate the principles of the legislative directives into a realistic, integrated ecosystem-based approach and at the same time provide stakeholders with best practices for managing NIS. The aim of this paper, prepared by members of the Working Group on Introductions and Transfers of Marine Organisms (WGITMO) of the International Council for the Exploration of the Sea (ICES), is to provide guidance for the application of NIS related management in the European Union Marine Strategy Framework Directive (MSFD). Ten recommendations, including NIS identification, standardization of sampling and data, indicators, propagule pressure and management issues are considered in this paper. While most of these suggestions were developed to improve the implementation of the MSFD, several may be more widely applicable. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Ojaveer, Henn] Univ Tartu, Estonian Marine Inst, EE-80012 Parnu, Estonia. [Galil, Bella S.] Natl Inst Oceanog, Israel Oceanog & Limnol Res, IL-31080 Haifa, Israel. [Minchin, Dan] Marine Organism Invest, Killaloe, Co Clare, Ireland. [Minchin, Dan; Olenin, Sergej] Klaipeda Univ, Coastal Res & Planning Inst, LT-92294 Klaipeda, Lithuania. [Amorim, Ana; Canning-Clode, Joao; Chainho, Paula] Univ Nova Lisboa, Ctr Oceanog, P-1749016 Lisbon, Portugal. [Canning-Clode, Joao] Univ Azores, Ctr IMAR, Dept Oceanog & Fisheries UAz, P-9901862 Horta, Azores, Portugal. [Canning-Clode, Joao] LARSyS Associated Lab, P-9901862 Horta, Azores, Portugal. [Canning-Clode, Joao] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Copp, Gordon H.] Ctr Environm Fisheries & Aquaculture Sci, Lowestoft NR33 0HT, Suffolk, England. [Gollasch, Stephan] GoConsult, D-22763 Hamburg, Germany. [Jelmert, Anders] Inst Marine Res, Flodevigen Marine Res Stn, N-4817 His, Norway. [Lehtiniemi, Maiju] Finnish Environm Inst, Ctr Marine Res, Helsinki 00251, Finland. [McKenzie, Cynthia] Fisheries & Oceans Canada, Northwest Atlantic Fisheries Ctr, St John, NF A1C 5X1, Canada. [Mikus, Josip; Pecarevic, Marijana] Univ Dubrovnik, Dept Aquaculture, Dubrovnik 20000, Croatia. [Miossec, Laurence] IFREMER, Nantes Ctr, F-44311 Nantes 3, France. [Occhipinti-Ambrogi, Anna] Univ Pavia, Dept Earth & Environm Sci, I-27100 Pavia, Italy. [Pederson, Judith] MIT, Sea Grant Coll Program, Cambridge, MA 02139 USA. [Quilez-Badia, Gemma] WWF Mediterranean Programme Off, Barcelona 08002, Spain. [Wijsman, Jeroen W. M.] Wageningen IMARES, NL-4400 AB Yerseke, Netherlands. [Zenetos, Argyro] Hellen Ctr Marine Res, Attica, Greece. RP Ojaveer, H (reprint author), Univ Tartu, Estonian Marine Inst, 2A Lootsi, EE-80012 Parnu, Estonia. EM henn.ojaveer@ut.ee RI Amorim, Ana/B-2117-2012; Canning Clode, Joao/G-5142-2011; Ojaveer, Henn/K-2160-2016; Chainho, Paula/B-3935-2012; OI Amorim, Ana/0000-0002-9612-4280; Canning Clode, Joao/0000-0003-2143-6535; Ojaveer, Henn/0000-0003-2742-6063; Chainho, Paula/0000-0002-3539-9942; OCCHIPINTI, ANNA CARMEN/0000-0002-5737-8317 NR 54 TC 39 Z9 39 U1 6 U2 50 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0308-597X EI 1872-9460 J9 MAR POLICY JI Mar. Pol. PD FEB PY 2014 VL 44 BP 160 EP 165 DI 10.1016/j.marpol.2013.08.019 PG 6 WC Environmental Studies; International Relations SC Environmental Sciences & Ecology; International Relations GA 287IW UT WOS:000329536400022 ER PT J AU Mederos-Lopez, J Gelhaus, JK AF Mederos-Lopez, Jorge Gelhaus, Jon K. TI A new Neotropical species of Trentepohlia (Mongoma) (Diptera: Tipulidae) from Cuba SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY LA English DT Article DE Trentepohlia; Mongoma; Tipulidae; Limoniinae; Neotropic; Cuba; crane fly AB A new Neotropical species of Trentepohlia (Mongoma) is described from Cuba. This is the first species of the subgenus from the West Indies, whereas the other four Trentepohlia spp. are from the subgenus Paramongoma. Notes on the phenology of this new species are provided. Also, we discuss the transfer of Trentepohlia suberrans Alexander, 1979 to Mongoma and provide a key for the identification of the three species of this subgenus present in the Neotropics. C1 [Mederos-Lopez, Jorge] Museu Ciencies Nat Barcelona, Dept Artropodes, Barcelona 08003, Catalonia, Spain. [Gelhaus, Jon K.] Drexel Univ, Acad Nat Sci, Dept Entomol, Philadelphia, PA 19103 USA. [Gelhaus, Jon K.] Smithsonian Inst, Washington, DC 20560 USA. RP Mederos-Lopez, J (reprint author), Museu Ciencies Nat Barcelona, Dept Artropodes, Passeig Picasso S-N, Barcelona 08003, Catalonia, Spain. EM mederos@gmail.com; gelhaus@ansp.org FU Barcelona City Council; Barcelona Zoo FX The authors thank Pjotr Oosterbroek, who kindly provided useful considerations. To Juli Pujade-Villar, thanks to its support has been possible to review this material. Nayla Garcia for its friendly attention and excellent management of the private collection of J. Mederos at the Ecology and Systematic Institute, La Habana, Cuba. Part of the equipment used during the study is due to the financial support of Barcelona City Council and the Barcelona Zoo. NR 16 TC 0 Z9 0 U1 1 U2 3 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0002-8320 EI 2162-3139 J9 T AM ENTOMOL SOC JI Trans. Am. Entomol. Soc. PD FEB PY 2014 VL 140 IS 1 BP 137 EP 144 PG 8 WC Entomology SC Entomology GA CN5UY UT WOS:000358498000008 ER PT J AU Leigh, EG O'Dea, A Vermeij, GJ AF Leigh, Egbert G. O'Dea, Aaron Vermeij, Geerat J. TI Historical biogeography of the Isthmus of Panama SO BIOLOGICAL REVIEWS LA English DT Article DE land bridge; invasions; predation; herbivory; extinction; diversification; trade-offs; vegetation zones; sea barriers; environmental change; plankton productivity; coral reefs ID AMERICAN BIOTIC INTERCHANGE; TROPICAL EASTERN PACIFIC; EOCENE THERMAL MAXIMUM; SERRANIA-DE-MACUIRA; RAIN-FOREST TREES; SOUTH-AMERICA; CORAL-REEFS; CARIBBEAN NEOGENE; FOSSIL RECORD; ENVIRONMENTAL-CHANGE AB About 3million years ago (Ma), the Isthmus of Panama joined the Americas, forming a land bridge over which inhabitants of each America invaded the otherthe Great American Biotic Interchange. These invasions transformed land ecosystems in South and Middle America. Humans invading from Asia over 12000years ago killed most mammals over 44kg, again transforming tropical American ecosystems. As a sea barrier, the isthmus induced divergent environmental change off its two coastscreating contrasting ecosystems through differential extinction and diversification. Approximately 65Ma invading marsupials and ungulates of North American ancestry, and xenarthrans of uncertain provenance replaced nearly all South America's non-volant mammals. There is no geological evidence for a land bridge at that time. Together with rodents and primates crossing from Africa 42 to 30Ma, South America's mammals evolved in isolation until the interchange's first heralds less than 10Ma. Its carnivores were ineffective marsupials. Meanwhile, North America was invaded by more competitive Eurasian mammals. The Americas had comparable expanses of tropical forest 55Ma; later, climate change confined North American tropical forest to a far smaller area. When the isthmus formed, North American carnivores replaced their marsupial counterparts. Although invaders crossed in both directions, North American mammals spread widely, diversified greatly, and steadily replaced South American open-country counterparts, unused to effective predators. Invading South American mammals were less successful. South America's birds, bats, and smaller rainforest mammals, equally isolated, mostly survived invasion. Its vegetation, enriched by many overseas invaders, remained intact. This vegetation resists herbivory effectively. When climate permitted, South America's rainforest, with its bats, birds and mammals, spread to Mexico. Present-day tropical American vegetation is largely zoned by trade-offs between exploiting well-watered settings versus surviving droughts, exploiting fertile versus coping with poor soil, and exploiting lowland warmth versus coping with cooler altitudes. At the start of the Miocene, a common marine biota extended from Trinidad to Ecuador and western Mexico, which evolved in isolation from the Indo-Pacific until the Pleistocene. The seaway between the Americas began shoaling over 12Ma. About 10Ma the land bridge was briefly near-complete, allowing some interchange of land mammals between the continents. By 7Ma, the rising sill had split deeper-water populations. Sea temperature, salinity and sedimentary carbon content had begun to increase in the Southern Caribbean, but not the Pacific. By 4Ma, the seaway's narrowing began to extinguish Caribbean upwellings. By 2Ma, upwellings remained only along Venezuela; Caribbean plankton, suspension-feeding molluscs and their predators had declined sharply, largely replaced by bottom-dwelling corals and calcareous algae and magnificent coral reefs. Closing the seaway extinguished the Eastern Pacific's reef corals (successors recolonized from the Indo-Pacific 6000years ago), whereas many molluscs of productive waters that once thrived in the Caribbean now survive only in the Eastern Pacific. The present-day productive Eastern Pacific, with few, small coral reefs and a plankton-based ecosystem contrasts with the Caribbean, whose clear water favours expansive coral reefs and bottom-dwelling primary producers. These ecosystems reflect the trade-off between fast growth and effective defence with attendant longevity. Overfishing with new technologies during the last few centuries, however, has caused population crashes of ever-smaller marine animals, devastating Caribbean ecosystems. C1 [Leigh, Egbert G.; O'Dea, Aaron] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Vermeij, Geerat J.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. RP Vermeij, GJ (reprint author), Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. EM gjvermeij@ucdavis.edu FU National System of Investigators (SNI) of Panama's National Secretariat for Science, Technology and Innovation (SENACYT) FX We are all most grateful to Mireya Correa for providing data from the herbaria of the Smithsonian Tropical Research Institute and the University of Panama on the diversity in Panama of various montane tree genera, to Carlos Jaramillo for suggesting that we write on this subject and for sending a crucial article on grassland evolution, to Anthony Coates for timely encouragement and advice, and to Tova Michlin and Alyssa Henry for formatting the references and many other kinds of assistance. A. O'D would like to thank Jeremy B. C. Jackson for insight and support through the years and the National System of Investigators (SNI) of Panama's National Secretariat for Science, Technology and Innovation (SENACYT) for financial support. E. G. L. thanks Neal Smith for drawing essential papers to his attention, the librarians of his Institute, especially Vielka Chang-Yau and Angel Aguirre, for procuring innumerable pdfs, Bruce MacFadden for answering a host of questions about the terrestrial side of this story, and the plants and animals of BCI for reminding us what we need to explain. NR 322 TC 45 Z9 47 U1 9 U2 135 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1464-7931 EI 1469-185X J9 BIOL REV JI Biol. Rev. PD FEB PY 2014 VL 89 IS 1 BP 148 EP 172 DI 10.1111/brv.12048 PG 25 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 284YE UT WOS:000329357500009 PM 23869709 ER PT J AU Kunert-Bajraszewska, M Labiano, A Siemiginowska, A Guainazzi, M AF Kunert-Bajraszewska, M. Labiano, A. Siemiginowska, A. Guainazzi, M. TI First X-ray observations of low-power compact steep spectrum sources SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: evolution; X-rays: galaxies ID GHZ-PEAKED-SPECTRUM; ACTIVE GALACTIC NUCLEI; RADIO-LOUD AGN; HUBBLE-SPACE-TELESCOPE; HI ABSORBING GAS; CHANDRA OBSERVATIONS; LINE REGION; CSS SOURCES; FR-I; GALAXIES AB We report on the first X-ray Chandra observations of a sample of seven low-luminosity compact sources, which belong to a class of young compact steep spectrum (CSS) radio sources. Four of these have been detected, while the other three have upper limit estimations for X-ray flux; one CSS galaxy is associated with an X-ray cluster. We have used the new observations, together with the observational data for known strong CSS and gigahertz-peaked spectrum (GPS) objects and large-scale Fanaroff-Riley types I and II objects (FR I and II), to study the relation between morphology, X-ray properties and excitation modes in radio-loud active galactic nuclei (AGNs). We have found the following. (i) The low-power objects fit well with the already established X-ray-radio luminosity correlation for AGNs and occupy the space among FR I objects, which are weaker in X-rays. (ii) The high-excitation and low-excitation galaxies occupy a distinct locus in the radio/X-ray luminosity plane, notwithstanding their evolutionary stage. This is in agreement with the postulated different origins of the X-ray emission in these two groups of objects. (iii) We have tested the AGN evolution models by comparing the radio/X-ray luminosity ratio with the size of the sources and, indirectly, with their age. We conclude that the division for two different X-ray emission modes, which originate in the base of the relativistic jet (FR Is) or in the accretion disc (FR IIs) is already present among the younger compact AGNs. (iv) Finally, we have found that the CSS sources are less obscured than the more compact GPS objects in X-rays. However, the anticorrelation between X-ray column density and radio size does not hold for the whole sample of GPS and CSS objects. C1 [Kunert-Bajraszewska, M.] NCU, Fac Phys Astron & Informat, Torun Ctr Astron, PL-87100 Torun, Poland. [Labiano, A.; Guainazzi, M.] European Space Astron Ctr ESA, E-28691 Madrid, Spain. [Labiano, A.; Siemiginowska, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kunert-Bajraszewska, M (reprint author), NCU, 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 National Aeronautics and Space Administration (NASA) [NAS8-03060]; Chandra grants [GO1-12124X, GO1-12145X]; Alfred P. Sloan Foundation; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX AL wishes to thank the Harvard-Smithsonian Center for Astro-physics for their hospitality and support during the visit. This research has made use of data obtained by the Chandra X-ray Observatory, and the application packages CIAO, CHIPS and SHERPA from the Chandra X-ray Center (CXC). This research is funded in part by the National Aeronautics and Space Administration (NASA) contract NAS8-03060. Partial support for this work was provided by the Chandra grants GO1-12124X and GO1-12145X. This research has made use of NASA's Astrophysics Data System Bibliographic Services and of the NASA/IPAC Extragalactic Data base (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 93 TC 8 Z9 8 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2014 VL 437 IS 4 BP 3063 EP 3071 DI 10.1093/mnras/stt1978 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 282MX UT WOS:000329177100004 ER PT J AU Kasparova, AV Saburova, AS Katkov, IY Chilingarian, IV Bizyaev, DV AF Kasparova, Anastasia V. Saburova, Anna S. Katkov, Ivan Yu Chilingarian, Igor V. Bizyaev, Dmitry V. TI A portrait of Malin 2: a case study of a giant low surface brightness galaxy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: haloes; galaxies: individual: Malin 2; galaxies: ISM ID STAR-FORMATION EFFICIENCY; INITIAL MASS FUNCTION; PHOTOMETRIC STANDARD STARS; OPTICAL VELOCITY-FIELDS; LARGE-MAGELLANIC-CLOUD; TULLY-FISHER RELATION; DIGITAL SKY SURVEY; EDGE-ON GALAXIES; GALACTIC DISKS; MOLECULAR GAS AB The low surface brightness (LSB) disc galaxy Malin 2 challenges the standard theory of galaxy evolution because of its enormous total mass similar to 2 x 10(12) M-circle dot, which must have been formed without recent major merger events. The aim of our work is to create a coherent picture of this exotic object by using new optical multicolour photometric and spectroscopic observations at the Apache Point Observatory as well as archival data sets from Gemini and wide-field surveys. We have performed Malin 2 mass modelling, we have estimated the contribution of the host dark halo and we have found that it acquired its low central density (0) similar or equal to 0.003 M-circle dot pc(-3) and huge isothermal sphere core radius r(c) = 27.3 kpc before the disc subsystem was formed. Our spectroscopic data analysis reveals complex kinematics of stars and gas in the very inner region (r = 5-7 kpc). We have measured the oxygen abundance in several clumps and we have concluded that the gas metallicity decreases from the solar value in the centre to a half of that at 20-30 kpc. We have found a small satellite projected on to the galaxy disc at 14 kpc from the centre and we have measured its mass (1/500 of the host galaxy) and gas metallicity (similar to that of the Malin 2 disc at the same distance). One of the unique properties of Malin 2 turned out to be the apparent imbalance of the interstellar media: the molecular gas is in excess with respect to the atomic gas for given values of the gas equilibrium turbulent pressure. We explain this imbalance by the presence of a significant portion of the dark gas not observable in CO and the H i 21-cm lines. We also show that the depletion time of the observed molecular gas traced by CO is nearly the same as in normal galaxies. Our modelling of the ultraviolet-to-optical spectral energy distribution favours the exponentially declined star formation history over a single-burst scenario. We argue that the massive and rarefied dark halo which formed before the disc component describes all the observed properties of Malin 2 well and we find that there is no need to assume additional catastrophic scenarios (such as major merging) proposed previously in order to explain the origin of giant LSB galaxies. C1 [Kasparova, Anastasia V.; Saburova, Anna S.; Katkov, Ivan Yu; Chilingarian, Igor V.; Bizyaev, Dmitry V.] 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. [Bizyaev, Dmitry V.] New Mexico State Univ, Sunspot, NM 88349 USA. [Bizyaev, Dmitry V.] Apache Point Observ, Sunspot, NM 88349 USA. RP Kasparova, AV (reprint author), Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Skij Pr 13, Moscow 119992, Russia. EM anastasya.kasparova@gmail.com RI Saburova, Anna/I-5871-2014; Kasparova, Anastasia/N-3019-2016; Katkov, Ivan/A-1867-2014; Chilingarian, Igor/N-5117-2016 OI Katkov, Ivan/0000-0002-6425-6879; Chilingarian, Igor/0000-0002-7924-3253 FU Ministry of Education and Science of the Russian Federation; Russian Foundation for Basic Research [12-02-00685, 12-02-31452]; Russian President's grant [MD-3288.2012.2]; Dmitry Zimin non-profit Dynasty Foundation FX We are grateful to Anatoly Zasov, Olga Sil'chenko and Oxana Abramova for productive discussions. We wish to thank Timothy Pickering who kindly provided the processed HI data cube of Malin 2. We thank Stacy McGaugh for providing us with the Malin 2 image with overplotted positions of the metallicity measurements. This work was supported by the Ministry of Education and Science of the Russian Federation and Russian Foundation for Basic Research (projects 12-02-00685 and 12-02-31452) and the Russian President's grant No. MD-3288.2012.2. IK and AS acknowledge support by the Dmitry Zimin non-profit Dynasty Foundation. We also thank our anonymous referee for comments on this paper. NR 111 TC 7 Z9 7 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 FEB PY 2014 VL 437 IS 4 BP 3072 EP 3086 DI 10.1093/mnras/stt1982 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 282MX UT WOS:000329177100005 ER PT J AU Bonsor, A Kennedy, GM Wyatt, MC Johnson, JA Sibthorpe, B AF Bonsor, Amy Kennedy, Grant M. Wyatt, Mark C. Johnson, John A. Sibthorpe, Bruce TI Herschel observations of debris discs orbiting planet-hosting subgiants SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planets and satellites: general; infrared: planetary systems ID SUN-LIKE STARS; STEADY-STATE EVOLUTION; SOLAR-TYPE STARS; WHITE-DWARFS; COLLISIONAL EVOLUTION; MASS-DISTRIBUTION; KAPPA-CRB; DISKS; SYSTEMS; DUST AB Debris discs are commonly detected orbiting main-sequence stars, yet little is known regarding their fate as the star evolves to become a giant. Recent observations of radial velocity detected planets orbiting giant stars highlight this population and its importance for probing, for example, the population of planetary systems orbiting intermediate mass stars. Our Herschel(dagger) survey observed a subset of the Johnson et al. program subgiants, finding that 4/36 exhibit excess emission thought to indicate debris, of which 3/19 are planet-hosting stars and 1/17 are stars with no current planet detections. Given the small numbers involved, there is no evidence that the disc detection rate around stars with planets is different to that around stars without planets. Our detections provide a clear indication that large quantities of dusty material can survive the star's main-sequence lifetime and be detected on the subgiant branch, with important implications for the evolution of planetary systems and observations of polluted or dusty white dwarfs. Our detection rates also provide an important constraint that can be included in models of debris disc evolution. C1 [Bonsor, Amy] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. [Bonsor, Amy] Univ Bristol, Sch Phys, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Kennedy, Grant M.; Wyatt, Mark C.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Johnson, John A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sibthorpe, Bruce] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. RP Bonsor, A (reprint author), UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. EM amy.bonsor@gmail.com OI Kennedy, Grant/0000-0001-6831-7547 FU ANR [BLAN-0505-01]; European Union through ERC [279973] FX AB acknowledges the support of the ANR-2010 BLAN-0505-01 (EXOZODI). MCW and GK acknowledge the support of the European Union through ERC grant number 279973. We thank Marta Bryan for useful discussions that improved the quality of this manuscript. NR 84 TC 16 Z9 16 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 FEB PY 2014 VL 437 IS 4 BP 3288 EP 3297 DI 10.1093/mnras/stt2128 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 282MX UT WOS:000329177100024 ER PT J AU Oonk, JBR van Weeren, RJ Salgado, F Morabito, LK Tielens, AGGM Rottgering, HJA Asgekar, A White, GJ Alexov, A Anderson, J Avruch, IM Batejat, F Beck, R Bell, ME van Bemmel, I Bentum, MJ Bernardi, G Best, P Bonafede, A Breitling, F Brentjens, M Broderick, J Bruggen, M Butcher, HR Ciardi, B Conway, JE Corstanje, A de Gasperin, F de Geus, E de Vos, M Duscha, S Eisloffel, J Engels, D van Enst, J Falcke, H Fallows, RA Fender, R Ferrari, C Frieswijk, W Garrett, MA Griessmeier, J Hamaker, JP Hassall, TE Heald, G Hessels, JWT Hoeft, M Horneffer, A van der Horst, A Iacobelli, M Jackson, NJ Juette, E Karastergiou, A Klijn, W Kohler, J Kondratiev, VI Kramer, M Kuniyoshi, M Kuper, G van Leeuwen, J Maat, P Macario, G Mann, G Markoff, S McKean, JP Mevius, M Miller-Jones, JCA Mol, JD Mulcahy, DD Munk, H Norden, MJ Orru, E Paas, H Pandey-Pommier, M Pandey, VN Pizzo, R Polatidis, AG Reich, W Scaife, AMM Schoenmakers, A Schwarz, D Shulevski, A Sluman, J Smirnov, O Sobey, C Stappers, BW Steinmetz, M Swinbank, J Tagger, M Tang, Y Tasse, C ter Veen, S Thoudam, S Toribio, C van Nieuwpoort, R Vermeulen, R Vocks, C Vogt, C Wijers, RAMJ Wise, MW Wucknitz, O Yatawatta, S Zarka, P Zensus, A AF Oonk, J. B. R. van Weeren, R. J. Salgado, F. Morabito, L. K. Tielens, A. G. G. M. Rottgering, H. J. A. Asgekar, A. White, G. J. Alexov, A. Anderson, J. Avruch, I. M. Batejat, F. Beck, R. Bell, M. E. van Bemmel, I. Bentum, M. J. Bernardi, G. Best, P. Bonafede, A. Breitling, F. Brentjens, M. Broderick, J. Brueggen, M. Butcher, H. R. Ciardi, B. Conway, J. E. Corstanje, A. de Gasperin, F. de Geus, E. de Vos, M. Duscha, S. Eisloeffel, J. Engels, D. van Enst, J. Falcke, H. Fallows, R. A. Fender, R. Ferrari, C. Frieswijk, W. Garrett, M. A. Griessmeier, J. Hamaker, J. P. Hassall, T. E. Heald, G. Hessels, J. W. T. Hoeft, M. Horneffer, A. van der Horst, A. Iacobelli, M. Jackson, N. J. Juette, E. Karastergiou, A. Klijn, W. Kohler, J. Kondratiev, V. I. Kramer, M. Kuniyoshi, M. Kuper, G. van Leeuwen, J. Maat, P. Macario, G. Mann, G. Markoff, S. McKean, J. P. Mevius, M. Miller-Jones, J. C. A. Mol, J. D. Mulcahy, D. D. Munk, H. Norden, M. J. Orru, E. Paas, H. Pandey-Pommier, M. Pandey, V. N. Pizzo, R. Polatidis, A. G. Reich, W. Scaife, A. M. M. Schoenmakers, A. Schwarz, D. Shulevski, A. Sluman, J. Smirnov, O. Sobey, C. Stappers, B. W. Steinmetz, M. Swinbank, J. Tagger, M. Tang, Y. Tasse, C. ter Veen, S. Thoudam, S. Toribio, C. van Nieuwpoort, R. Vermeulen, R. Vocks, C. Vogt, C. Wijers, R. A. M. J. Wise, M. W. Wucknitz, O. Yatawatta, S. Zarka, P. Zensus, A. TI Discovery of carbon radio recombination lines in absorption towards Cygnus A SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: general; ISM: structure; local interstellar matter; radio lines: ISM ID RAY IONIZATION RATE; CASSIOPEIA-A; INTERSTELLAR CLOUDS; BN FACTORS; DIRECTION; GAS; MHZ; REGIONS; CLUSTER; HI AB We present the first detection of carbon radio recombination line absorption along the line of sight to Cygnus A. The observations were carried out with the Low Frequency Array in the 33-57 MHz range. These low-frequency radio observations provide us with a new line of sight to study the diffuse, neutral gas in our Galaxy. To our knowledge this is the first time that foreground Milky Way recombination line absorption has been observed against a bright extragalactic background source. By stacking 48 carbon alpha lines in the observed frequency range we detect carbon absorption with a signal-to-noise ratio of about 5. The average carbon absorption has a peak optical depth of 2 x 10(-4), a line width of 10 km s(-1) and a velocity of +4 km s(-1) with respect to the local standard of rest. The associated gas is found to have an electron temperature T-e similar to 110 K and density n(e) similar to 0.06 cm(-3). These properties imply that the observed carbon alpha absorption likely arises in the cold neutral medium of the Orion arm of the Milky Way. Hydrogen and helium lines were not detected to a 3 Sigma peak optical depth limit of 1.5 x 10(-4) for a 4 km s(-1) channel width. Radio recombination lines associated with Cygnus A itself were also searched for, but are not detected. We set a 3 Sigma upper limit of 1.5 x 10(-4) for the peak optical depth of these lines for a 4 km s(-1) channel width. C1 [Oonk, J. B. R.; van Weeren, R. J.; Asgekar, A.; van Bemmel, I.; Bentum, M. J.; Brentjens, M.; de Geus, E.; de Vos, M.; Duscha, S.; van Enst, J.; Falcke, H.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Hamaker, J. P.; Heald, G.; Hessels, J. W. T.; Klijn, W.; Kondratiev, V. I.; Kuper, G.; van Leeuwen, J.; Maat, P.; McKean, J. P.; Mevius, M.; Mol, J. D.; Munk, H.; Norden, M. J.; Orru, E.; Pandey, V. N.; Pizzo, R.; Polatidis, A. G.; Schoenmakers, A.; Sluman, J.; Tang, Y.; Toribio, C.; van Nieuwpoort, R.; Vermeulen, R.; Vogt, C.; Wise, M. W.; Yatawatta, S.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [van Weeren, R. J.; Salgado, F.; Morabito, L. K.; Tielens, A. G. G. M.; Rottgering, H. J. A.; Garrett, M. A.; Iacobelli, M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [White, G. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [White, G. J.] STFC Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Alexov, A.; Hessels, J. W. T.; van der Horst, A.; van Leeuwen, J.; Markoff, S.; Miller-Jones, J. C. A.; Swinbank, J.; Wijers, R. A. M. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Anderson, J.; Beck, R.; Horneffer, A.; Kohler, J.; Kramer, M.; Kuniyoshi, M.; Mulcahy, D. D.; Reich, W.; Sobey, C.; Wucknitz, O.; Zensus, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Avruch, I. M.] SRON Netherlands Insitute Space Res, NL-9700 AV Groningen, Netherlands. [Batejat, F.; Conway, J. E.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Bell, M. E.] Univ Sydney, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Bernardi, G.; Smirnov, O.] Rhodes Univ, Ctr Radio Astron Tech & Technol RATT, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [Best, P.] Univ Edinburgh, Inst Astron, Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, Scotland. [Bonafede, A.; Brueggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Breitling, F.; Mann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Broderick, J.; Fender, R.; Hassall, T. E.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Corstanje, A.; Falcke, H.; ter Veen, S.; Thoudam, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Engels, D.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Ferrari, C.; Macario, G.] Univ Nice Sophia Antipolis, Lab Lagrange, CNRS, Observ Cote Azur,UMR7293, F-06300 Nice, France. [Griessmeier, J.; Tagger, M.] CNRS, Lab Phys & Chim Environm & Espace, LPC2E, UMR 7328, F-45071 Orleans 02, France. [Hassall, T. E.; Jackson, N. J.; Kramer, M.; Stappers, B. W.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Karastergiou, A.] Univ Oxford, Oxford OX1 3RH, England. [Kondratiev, V. I.] PN Lebedev Phys Inst, Astro Space Ctr, Moscow 117997, Russia. [Mevius, M.; Shulevski, A.] Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Miller-Jones, J. C. A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Paas, H.] Univ Groningen, CIT, NL-9700 CA Groningen, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Schwarz, D.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. [Tasse, C.; Zarka, P.] Observ Paris, LESIA, CNRS, UMR 8109, F-92195 Meudon, France. [van Nieuwpoort, R.] Netherlands ESci Ctr, NL-1098 XG Amsterdam, Netherlands. [Wucknitz, O.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. RP Oonk, JBR (reprint author), Netherlands Inst Radio Astron ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. EM oonk@strw.leidenuniv.nl RI Tagger, Michel/O-6615-2014; Shulevski, Aleksandar/E-5591-2015; Miller-Jones, James/B-2411-2013; Ciardi, Benedetta/N-7625-2015; Kondratiev, Vladislav/N-1105-2015; Yatawatta, Sarod/E-6037-2013; OI van Weeren, Reinout/0000-0002-0587-1660; Tagger, Michel/0000-0003-2962-3220; Shulevski, Aleksandar/0000-0002-1827-0469; Miller-Jones, James/0000-0003-3124-2814; Kondratiev, Vladislav/0000-0001-8864-7471; Swinbank, John/0000-0001-9445-1846; Wijers, Ralph/0000-0002-3101-1808; Yatawatta, Sarod/0000-0001-5619-4017; de Gasperin, Francesco/0000-0003-4439-2627 FU NASA [PF2-130104]; Chandra X-ray Center FX Support for this work was provided by NASA through Einstein Post-doctoral 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.; Chiara Ferrari and Giulia Macario acknowledge financial support by the Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. NR 38 TC 6 Z9 6 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 FEB PY 2014 VL 437 IS 4 BP 3506 EP 3515 DI 10.1093/mnras/stt2158 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 282MX UT WOS:000329177100038 ER PT J AU Torrelles, JM Trinidad, MA Curiel, S Estalella, R Patel, NA Gomez, JF Anglada, G Carrasco-Gonzalez, C Canto, J Raga, A Rodriguez, LF AF Torrelles, J. M. Trinidad, M. A. Curiel, S. Estalella, R. Patel, N. A. Gomez, J. F. Anglada, G. Carrasco-Gonzalez, C. Canto, J. Raga, A. Rodriguez, L. F. TI Multi-epoch VLBA H2O maser observations towards the massive YSOs AFGL 2591 VLA 2 and VLA 3 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE masers; stars: formation; ISM: individual objects: AFGL 2591; ISM: jets and outflows ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; WATER MASERS; RADIO-CONTINUUM; OUTFLOW; POLARIZATION; AFGL-2591; EVOLUTION; EMISSION; CEPHEUS AB We present multi-epoch Very Long Baseline Array (VLBA) H2O maser observations towards the massive young stellar objects (YSOs) VLA 2 and VLA 3 in the star-forming region AFGL 2591. Through these observations, we have extended the study of the evolution of the masers towards these objects up to a time-span of similar to 10 yr, measuring their radial velocities and proper motions. The H2O masers in VLA 3, the most massive YSO in AFGL 2591 (similar to 30-40 M-circle dot), are grouped within projected distances of less than or similar to 40 mas (less than or similar to 130 au) from VLA 3. In contrast to other H2O masers in AFGL 2591, the masers associated with VLA 3 are significantly blueshifted (up to similar to 30 km s(-1)) with respect to the velocity of the ambient molecular cloud. We find that the H2O maser cluster as a whole has moved westwards of VLA 3 between the 2001 and 2009 observations, with a proper motion of similar to 1.2 mas yr(-1) (similar to 20 km s(-1)). We conclude that these masers are tracing blueshifted outflowing material, shock excited at the inner parts of a cavity seen previously in ammonia molecular lines and infrared images, and proposed to be evacuated by the outflow associated with the massive VLA 3 source. The masers in the region of VLA 2 are located at projected distances of similar to 0.7 arcsec (similar to 2300 au) north from this source, with their kinematics suggesting that they are excited by a YSO other than VLA 2. This driving source has not yet been identified. C1 [Torrelles, J. M.] Univ Barcelona, UB IEEC, CSIC, Inst Ciencias Espacio, E-08028 Barcelona, Spain. [Trinidad, M. A.] Univ Guanajuato, Dept Astron, Guanajuato 36000, Mexico. [Curiel, S.; Canto, J.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Estalella, R.] Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. [Estalella, R.] Univ Barcelona, IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain. [Patel, N. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gomez, J. F.; Anglada, G.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Carrasco-Gonzalez, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Carrasco-Gonzalez, C.; Rodriguez, L. F.] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Raga, A.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. RP Torrelles, JM (reprint author), Univ Barcelona, UB IEEC, CSIC, Inst Ciencias Espacio, Marti i Franques 1, E-08028 Barcelona, Spain. EM torrelles@ieec.cat RI Gomez, Jose Francisco/D-8392-2016; OI Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 FU MICINN (Spain) [AYA2008-06189-C03, AYA2011-30228-C03]; FEDER funds; CONACyT [61547, 82543]; DGAPA (Mexico); UNAM (Mexico); CONACyT (Mexico); CSIC (Spain); AGAUR (Catalonia) [2009SGR1172] FX We would like to thank our referee for the very useful report on our manuscript. We also acknowledge Wouter Vlemmings and Moshe Elitzur for very helpful comments. GA, CC-G, RE, JFG and JMT acknowledge support from the MICINN (Spain) AYA2008-06189-C03 and AYA2011-30228-C03 grants (co-funded with FEDER funds). JC and AR acknowledge support from CONACyT grant 61547. SC acknowledges the support of DGAPA, UNAM, CONACyT (Mexico) and CSIC (Spain). LFR acknowledges the support of DGAPA, UNAM and CONACyT (Mexico). MAT acknowledges support from CONACyT grant 82543. RE and JMT acknowledge support from the AGAUR (Catalonia) 2009SGR1172 grant. JMT acknowledges the hospitality offered by the Science Operations Center of the NRAO (Socorro, NM, USA) where part of the data reduction was carried out (2013 June-July). The ICC (UB) is a CSIC-Associated Unit through the ICE (CSIC). NR 33 TC 3 Z9 3 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 FEB PY 2014 VL 437 IS 4 BP 3803 EP 3811 DI 10.1093/mnras/stt2177 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 282MX UT WOS:000329177100062 ER PT J AU Drake, JJ Garraffo, C Takei, D Gaensicke, B AF Drake, Jeremy J. Garraffo, Cecilia Takei, Dai Gaensicke, Boris TI A magnetic accretion switch in pre-cataclysmic binaries SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries: eclipsing; stars: coronae; novae, cataclysmic variables; stars: winds, outflows; X-rays: stars ID COMMON-ENVELOPE BINARIES; CORONAL MASS EJECTIONS; ANGULAR-MOMENTUM LOSS; X-RAY BINARIES; WHITE-DWARFS; QS VIR; PERIOD VARIATIONS; ECLIPSING BINARY; ACTIVITY CYCLES; ACTIVE STARS AB We have investigated the mass accretion rate implied by published surface abundances of Si and C in the white dwarf component of the 3.62 h period pre-cataclysmic binary and planet host candidate QS Vir (DA+M2-4). Diffusion time-scales for gravitational settling imply (M) over dot similar to 10(-16) M-circle dot yr(-1) for the 1999 epoch of the observations, which is three orders of magnitude lower than measured from a 2006 XMM-Newton observation. This is the first time that large accretion rate variations have been seen in a detached pre-cataclysmic variable (pre-CV). A third body in a 14 yr eccentric orbit suggested in a recent eclipse timing study is too distant to perturb the central binary sufficiently to influence accretion. A hypothetical coronal mass ejection just prior to the XMM-Newton observation might explain the higher accretion rate, but the implied size and frequency of such events appear too great. We suggest accretion is most likely modulated by a magnetic cycle on the secondary acting as a wind 'accretion switch', a mechanism that can be tested by X-ray and ultraviolet monitoring. If so, QS Vir and similar pre-CVs could provide powerful insights into hitherto inscrutable CV and M dwarf magnetospheres, and mass- and angular-momentum-loss rates. C1 [Drake, Jeremy J.; Garraffo, Cecilia; Takei, Dai] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gaensicke, Boris] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Drake, JJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jdrake@cfa.harvard.edu RI Gaensicke, Boris/A-9421-2012 OI Gaensicke, Boris/0000-0002-2761-3005 FU NASA [NAS8-03060]; JSPS; European Research Council under the European Union [320964]; UK's Science and Technology Facilities Council [ST/I001719/1] FX JJD was supported by NASA contract NAS8-03060 to the Chandra X-ray Center (CXC) and thanks the CXC director, Harvey Tananbaum, and the CXC science team for advice and support. DT was supported by JSPS Fellowship. Finally, we thank G. Schmidt for comments on Matranga et al. (2012) that provided the initial impetus for this further study. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement n. 320964 (WDTracer). BTG was supported in part by the UK's Science and Technology Facilities Council (ST/I001719/1). NR 51 TC 3 Z9 3 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2014 VL 437 IS 4 BP 3842 EP 3847 DI 10.1093/mnras/stt2186 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 282MX UT WOS:000329177100066 ER PT J AU Urban, O Simionescu, A Werner, N Allen, SW Ehlert, S Zhuravleva, I Morris, RG Fabian, AC Mantz, A Nulsen, PEJ Sanders, JS Takei, Y AF Urban, O. Simionescu, A. Werner, N. Allen, S. W. Ehlert, S. Zhuravleva, I. Morris, R. G. Fabian, A. C. Mantz, A. Nulsen, P. E. J. Sanders, J. S. Takei, Y. TI Azimuthally resolved X-ray spectroscopy to the edge of the Perseus Cluster SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: individual: Perseus; X-rays: galaxies: clusters ID MASSIVE GALAXY CLUSTERS; ACTIVE GALACTIC NUCLEI; VIRIAL RADIUS; INTRACLUSTER MEDIUM; SUZAKU OBSERVATIONS; REPRESENTATIVE SAMPLE; SURFACE BRIGHTNESS; NUMBER COUNTS; OUTER REGIONS; COMA CLUSTER AB We present the results from extensive, new observations of the Perseus Cluster of galaxies, obtained as a Suzaku Key Project. The 85 pointings analysed span eight azimuthal directions out to 2 degrees = 2.6 Mpc, to and beyond the virial radius r(200) similar to 1.8 Mpc, offering the most detailed X-ray measurements of the intracluster medium (ICM) at large radii in any cluster to date. The azimuthally averaged density profile for r > 0.4r(200) is relatively flat, with a best-fitting power-law index delta = 1.69 +/- 0.13, significantly smaller than expected from numerical simulations. The entropy profile in the outskirts lies systematically below the power-law behaviour expected from large-scale structure formation models which include only the heating associated with gravitational collapse. Conversely, the pressure profile beyond similar to 0.6r(200) shows an excess with respect to the best-fitting model describing the SZ measurements for a sample of clusters observed with the Planck satellite. The differences between the expected and measured density, entropy and pressure profiles can be explained by a systematic overestimation of the ICM density at large radii caused by homogeneous modelling of inhomogeneous gas distributions (i.e. gas clumping), with the density overestimates ranging from factors of similar to 1.2 to 2 or more at r(200) along different directions. We find no evidence for a bias in the temperature measurements within the virial radius. Along the cluster minor axis, we find a flattening of the entropy profiles outside similar to 0.6r(200), while along the major axis, the entropy rises all the way to the outskirts. C1 [Urban, O.; Simionescu, A.; Werner, N.; Allen, S. W.; Ehlert, S.; Zhuravleva, I.; Morris, R. G.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Urban, O.; Simionescu, A.; Werner, N.; Allen, S. W.; Ehlert, S.; Zhuravleva, I.; Morris, R. G.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Urban, O.; Allen, S. W.; Ehlert, S.; Morris, R. G.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Simionescu, A.; Takei, Y.] JAXA, ISAS, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Ehlert, S.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Mantz, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Mantz, A.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sanders, J. S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Urban, O (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA. EM ondrej@stanford.edu RI XRAY, SUZAKU/A-1808-2009; OI Sanders, Jeremy/0000-0003-2189-4501; Nulsen, Paul/0000-0003-0297-4493 FU Suzaku grants [NNX09AV64G, NNX10AR48G]; Chandra grant [GO2-13144X]; NASA ADAP grant [NNX12AE05G]; XMM-Newton grant [NNX12AB64G]; US Department of Energy [DE-AC02-76SF00515]; NSF [AST-0838187] FX We acknowledge support from Suzaku grants NNX09AV64G and NNX10AR48G, Chandra grant GO2-13144X, NASA ADAP grant NNX12AE05G and XMM-Newton grant NNX12AB64G. This work was supported in part by the US Department of Energy under contract number DE-AC02-76SF00515. AM acknowledges the support by the NSF grant AST-0838187. NR 71 TC 33 Z9 33 U1 1 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 FEB PY 2014 VL 437 IS 4 BP 3939 EP 3961 DI 10.1093/mnras/stt2209 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 282MX UT WOS:000329177100072 ER PT J AU Lasota, JP Gourgoulhon, E Abramowicz, M Tchekhovskoy, A Narayan, R AF Lasota, J. -P. Gourgoulhon, E. Abramowicz, M. Tchekhovskoy, A. Narayan, R. TI Extracting black-hole rotational energy: The generalized Penrose process SO PHYSICAL REVIEW D LA English DT Article ID 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; BLANDFORD-ZNAJEK MECHANISM; ACTIVE GALACTIC NUCLEI; ELECTROMAGNETIC EXTRACTION; ACCRETION FLOWS; ENERGETICS; HORIZONS; PLASMA; FIELD; JETS AB In the case involving particles, the necessary and sufficient condition for the Penrose process to extract energy from a rotating black hole is absorption of particles with negative energies and angular momenta. No torque at the black-hole horizon occurs. In this article we consider the case of arbitrary fields or matter described by an unspecified, general energy-momentum tensor T-mu nu and show that the necessary and sufficient condition for extraction of a black hole's rotational energy is analogous to that in the mechanical Penrose process: absorption of negative energy and negative angular momentum. We also show that a necessary condition for the Penrose process to occur is for the Noether current (the conserved energy-momentum density vector) to be spacelike or past directed (timelike or null) on some part of the horizon. In the particle case, our general criterion for the occurrence of a Penrose process reproduces the standard result. In the case of relativistic jet-producing "magnetically arrested disks," we show that the negative energy and angular-momentum absorption condition is obeyed when the Blandford-Znajek mechanism is at work, and hence the high energy extraction efficiency up to similar to 300% found in recent numerical simulations of such accretion flows results from tapping the black hole's rotational energy through the Penrose process. We show how black-hole rotational energy extraction works in this case by describing the Penrose process in terms of the Noether current. C1 [Lasota, J. -P.] Univ Paris 06, Inst Astrophys Paris, UMR CNRS 7095, F-75014 Paris, France. [Lasota, J. -P.; Abramowicz, M.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Lasota, J. -P.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Gourgoulhon, E.] Univ Paris Diderot, LUTH, Observ Paris, CNRS, F-92190 Meudon, France. [Abramowicz, M.] Univ Gothenburg, Dept Phys, SE-41296 Gothenburg, Sweden. [Abramowicz, M.] Silesian Univ Opava, Inst Phys, CZ-74601 Opava, Czech Republic. [Tchekhovskoy, A.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Tchekhovskoy, A.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Tchekhovskoy, A.] Princeton Univ, Ctr Theoret Sci, Princeton, NJ 08544 USA. [Narayan, R.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Lasota, JP (reprint author), Univ Paris 06, Inst Astrophys Paris, UMR CNRS 7095, 98bis Bd Arago, F-75014 Paris, France. EM lasota@iap.fr OI Narayan, Ramesh/0000-0002-1919-2730 FU Polish NCN [UMO-2011/01/B/ST9/05439, UMO-2011/01/B/ST9/05437, DEC-2012/04/A/ST9/00083]; Czech "Synergy" grant for international collaboration [CZ.1.07/2.3.00/20.0071]; French Space Agency CNES; Agence Nationale de la Recherche [ANR-12-BS01-012-01]; Princeton Center for Theoretical Science Fellowship; NASA through Einstein Postdoctoral Fellowship [PF3-140115]; Chandra X-ray Center; NASA [NAS8-03060]; NSF; NCSA MSS [TG-AST100040, TG-AST080026N] FX M. A. and J. P. L. thank Serguei Komissarov for an enlightening and stimulating exchange of Emails. Research reported here was partially supported by Polish NCN Grants No. UMO-2011/01/B/ST9/05439, No. UMO-2011/01/B/ST9/05437, and No. DEC-2012/04/A/ST9/00083. Research at the Silesian University in Opava was supported by the Czech CZ.1.07/2.3.00/20.0071 "Synergy" grant for international collaboration. JPL acknowledges a grant from the French Space Agency CNES and EG, Grant No. ANR-12-BS01-012-01 "Analyse Asymptotique en Relativite Generale" from Agence Nationale de la Recherche. Support for this work was provided by a Princeton Center for Theoretical Science Fellowship and by NASA through Einstein Postdoctoral Fellowship Grant No. PF3-140115 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under Contract No. NAS8-03060. We acknowledge support by the NSF through TeraGrid/XSEDE resources provided by NICS Kraken and LONI QueenBee, where simulations were carried out; NICS Nautilus, where data were analyzed; and TACC Ranch and NCSA MSS, where data were backed up, under Grants No. TG-AST100040 (A. T.) and No. TG-AST080026N (R. N.). NR 51 TC 23 Z9 23 U1 0 U2 11 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 JAN 31 PY 2014 VL 89 IS 2 AR 024041 DI 10.1103/PhysRevD.89.024041 PG 24 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AB6BW UT WOS:000331873500001 ER PT J AU Heyer, WR AF Heyer, W. Ronald TI Morphological analyses of frogs of the Leptodactylus latrans complex (Amphibia, Leptodactylidae) from selected localities in South America SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE external morphology; Leptodactylus latrans complex; species limits AB Two species of the Leptodactylus latrans complex in Argentina, Paraguay, and Uruguay (currently considered as Leptodactylus chaquensis and Leptodactylus latrans) are readily identifiable based on external morphological features. In contrast, analyses of external morphological features have not been successful in determining species limits of the complex in Brasil, Bolivia, Colombia, Venezuela, Guyana, Suriname, and French Guiana. The purpose of this study is to assess whether variation in a set of external morphological features is of value in determining species limits for a set of localities distributed throughout the range of the L. latrans complex. The morphological data as analyzed in this study provide some suggestions for delineating species limits, but overall, the data as analyzed are not sufficient to determine robust species limits within the L. latrans species complex. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Amphibians & Reptiles, Washington, DC 20013 USA. RP Heyer, WR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Amphibians & Reptiles, POB 37012, Washington, DC 20013 USA. EM heyerr@si.edu FU Sao Paulo State Research Foundation; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo FX Funding for this contribution was supported by the Sao Paulo State Research Foundation, Fundacao de Amparo a Pesquisa do Estado de Sao Paulo, and the Robert H. Gibbs, Jr., fund administered by the Department of Vertebrate Zoology, National Museum of Natural History, Smithsonian Institution. NR 7 TC 2 Z9 2 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 JAN 30 PY 2014 VL 126 IS 4 BP 369 EP 378 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 302JA UT WOS:000330599600007 ER PT J AU Zug, GR Kaiser, H AF Zug, George R. Kaiser, Hinrich TI A new species of four-toed skink (Squamata: Scincidae: Carlia peronii species group) from Pulau Sukur, Indonesia, and biogeographic notes on the herpetofauna of Flores and Komodo SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE biogeography; Indonesia; Lesser Sunda Islands; reptiles; Squamata ID PLEISTOCENE; TIMOR AB Even though Flores is a major island of the Inner Banda Arc in the Lesser Sunda Archipelago (Indonesia), its herpetofauna was last tabulated by Robert Mertens, based on a 47-day visit to the island in 1927. Few, even briefer, surveys of the Flores herpetofauna occurred since then, and our knowledge remains incomplete. Pulau Sukur is a small island lying about 35 km off the north coast of Flores. Its herpetofauna has not been previously documented and likely is a subset of the Flores herpetofauna; however, at least one unique lizard species occurs there. Carlia sukur, new species, is a member of the C. peronii species group and is described herein. Its geographic outlier position represents a peculiar biogeographic question, which we examine relative to the lizard fauna of Flores and offer an updated list to the Flores and Komodo herpetofauna. C1 [Zug, George R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Kaiser, Hinrich] Victor Valley Coll, Dept Biol, Victorville, CA 92395 USA. RP Zug, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012, Washington, DC 20013 USA. EM zugg@si.edu; hinrich.kaiser@vvc.edu NR 35 TC 4 Z9 4 U1 1 U2 9 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 JAN 30 PY 2014 VL 126 IS 4 BP 379 EP 392 PG 14 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 302JA UT WOS:000330599600008 ER PT J AU Olson, SL David, N AF Olson, Storrs L. David, Normand TI The gender of the tortoise genus Chelonoidis Fitzinger, 1835 (Testudines: Testudinidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Galapagos; Geochelone; Testudo AB Although currently treated as feminine, the rules of nomenclature dictate that the proper gender of the generic name Chelonoidis Fitzinger, 1835, used for certain tortoises of South America and the giant species of the Galapagos, is masculine. This necessitates changes to the endings of the following specific names Chelonoidis niger, C. californianus, C. nigritus, C. carbonarius, and C. denticulatus. C1 [Olson, Storrs L.] 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 10 TC 3 Z9 3 U1 3 U2 6 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 JAN 30 PY 2014 VL 126 IS 4 BP 393 EP 394 PG 2 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 302JA UT WOS:000330599600009 ER PT J AU Carleton, MD Smeenk, C Angermann, R Goodman, SM AF Carleton, Michael D. Smeenk, Chris Angermann, Renate Goodman, Steven M. TI Taxonomy of nesomyine rodents (Muroidea: Nesomyidae: Nesomyinae): Designation of lectotypes and restriction of type localities for species-group taxa in the genus Nesomys Peters SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE J. Audebert; A. Crossley; Madagascar; Nesomys audeberti; Nesomys lambertoni; Nesomys rufus; nomenclature ID WESTERN MADAGASCAR; MURIDAE AB Key foundational elements of taxonomic description were omitted in the original naming of species-group taxa now recognized in the Malagasy genus Nesomys: N. rufus Peters, 1870, N. audeberti (Jentink, 1879), and N. lambertoni G. Grandidier, 1928. Based on our review of the material available to the authors, we identified the holotype by monotypy of N. rufus, designated lectotypes of N. audeberti and N. lambertoni, restricted the type localities of N. audeberti and NI lambertoni, and localized the probable geographic source of the holotype of N. rufus. Refinement of the geographic source of N. lambertoni and N. rufus illuminates the incorrect placement of their type localities as currently interpreted and brings them within the presently understood distributions of those species. Extensive discussion is devoted to the travels of J. Audebert and A. Crossley, collectors not only of the types of N. audeberti and N. rufus, respectively, but also of important series of lemurs that remain relevant to understanding the taxonomy and distribution of these endangered mammals. C1 [Carleton, Michael D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Angermann, Renate] Leibniz Inst Evolut & Biodiversitatsforsch, Museum Nat Kunde, D-10115 Berlin, Germany. [Goodman, Steven M.] Field Museum Nat Hist, Chicago, IL 60605 USA. RP Carleton, MD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM carletonm@si.edu; chris.smeenk@ziggo.nl; renate.angermann@mfn-berlin.de; sgoodman@fieldmuseum.org NR 96 TC 0 Z9 0 U1 1 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 JAN 30 PY 2014 VL 126 IS 4 BP 414 EP + PG 42 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 302JA UT WOS:000330599600011 ER PT J AU DeMeo, FE Carry, B AF DeMeo, F. E. Carry, B. TI Solar System evolution from compositional mapping of the asteroid belt SO NATURE LA English DT Review ID SKY-SURVEY COLORS; JOVIAN TROJAN ASTEROIDS; S-TYPE ASTEROIDS; SURFACE-COMPOSITION; MAIN-BELT; SPECTROSCOPIC SURVEY; WATER-ICE; WISE/NEOWISE OBSERVATIONS; ORBITAL ARCHITECTURE; PHYSICAL-PROPERTIES AB Advances in the discovery and characterization of asteroids over the past decade have revealed an unanticipated underlying structure that points to a dramatic early history of the inner Solar System. The asteroids in the main asteroid belt have been discovered to be more compositionally diverse with size and distance from the Sun than had previously been known. This implies substantial mixing through processes such as planetary migration and the subsequent dynamical processes. C1 [DeMeo, F. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [DeMeo, F. E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Carry, B.] CNRS, UMR8028, Observ Paris, Inst Mecan Celeste & Calcul Ephemerides, F-75014 Paris, France. [Carry, B.] European Space Astron ESA Ctr, Madrid 28691, Spain. RP DeMeo, FE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 16, Cambridge, MA 02138 USA. EM fdemeo@cfa.harvard.edu FU ESAC faculty; National Science Foundation [0907766]; National Aeronautics and Space Administration (NASA) [NNX12AL26G, HST-HF-51319.01-A, NAS 5-26555]; Space Telescope Science Institute FX We are grateful to R. Binzel for help in shaping this review, and to K. Walsh, W. Bottke, N. Moskovitz, D. Polishook, T. Burbine, J. Wisdom and A. Morales for discussions. We thank C. Chapman for a review. We acknowledge support from the ESAC faculty for F.E.D.'s visit. This material is based upon work supported by the National Science Foundation under grant number 0907766 and by the National Aeronautics and Space Administration (NASA) under grant number NNX12AL26G. Any opinions, findings and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation or NASA. Support for this work was provided by NASA through the Hubble Fellowship grant HST-HF-51319.01-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. F.E.D. is a Hubble Fellow. NR 88 TC 49 Z9 49 U1 3 U2 32 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JAN 30 PY 2014 VL 505 IS 7485 BP 629 EP 634 DI 10.1038/nature12908 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 298JV UT WOS:000330321000030 PM 24476886 ER PT J AU Kung, D Bigler, L Davis, LR Gratwicke, B Griffith, E Woodhams, DC AF Kueng, Denise Bigler, Laurent Davis, Leyla R. Gratwicke, Brian Griffith, Edgardo Woodhams, Douglas C. TI Stability of Microbiota Facilitated by Host Immune Regulation: Informing Probiotic Strategies to Manage Amphibian Disease SO PLOS ONE LA English DT Article ID INFLAMMATORY BOWEL DISEASES; SKIN PEPTIDE DEFENSES; BATRACHOCHYTRIUM-DENDROBATIDIS; ANTIMICROBIAL PEPTIDES; POPULATION DECLINES; CUTANEOUS BACTERIA; WILD POPULATIONS; GUT MICROBIOTA; RANA-MUSCOSA; T-RFLP AB Microbial communities can augment host immune responses and probiotic therapies are under development to prevent or treat diseases of humans, crops, livestock, and wildlife including an emerging fungal disease of amphibians, chytridiomycosis. However, little is known about the stability of host-associated microbiota, or how the microbiota is structured by innate immune factors including antimicrobial peptides (AMPs) abundant in the skin secretions of many amphibians. Thus, conservation medicine including therapies targeting the skin will benefit from investigations of amphibian microbial ecology that provide a model for vertebrate host-symbiont interactions on mucosal surfaces. Here, we tested whether the cutaneous microbiota of Panamanian rocket frogs, Colostethus panamansis, was resistant to colonization or altered by treatment. Under semi-natural outdoor mesocosm conditions in Panama, we exposed frogs to one of three treatments including: (1) probiotic - the potentially beneficial bacterium Lysinibacillus fusiformis, (2) transplant - skin washes from the chytridiomycosis-resistant glass frog Espadarana prosoblepon, and (3) control - sterile water. Microbial assemblages were analyzed by a culture-independent T-RFLP analysis. We found that skin microbiota of C. panamansis was resistant to colonization and did not differ among treatments, but shifted through time in the mesocosms. We describe regulation of host AMPs that may function to maintain microbial community stability. Colonization resistance was metabolically costly and microbe-treated frogs lost 7-12% of body mass. The discovery of strong colonization resistance of skin microbiota suggests a well-regulated, rather than dynamic, host-symbiont relationship, and suggests that probiotic therapies aiming to enhance host immunity may require an approach that circumvents host mechanisms maintaining equilibrium in microbial communities. C1 [Kueng, Denise; Davis, Leyla R.; Woodhams, Douglas C.] Univ Zurich, Inst Evolutionary Biol & Environm Studies, Zurich, Switzerland. [Bigler, Laurent] Univ Zurich, Inst Organ Chem, Zurich, Switzerland. [Gratwicke, Brian] Smithsonian Inst, Natl Zool Pk, Ctr Species Survival Conservat & Sci, Washington, DC 20008 USA. [Griffith, Edgardo] El Valle Amphibian Conservat Ctr, El Valle, Panama. [Woodhams, Douglas C.] Smithsonian Trop Res Inst, Panama City, Panama. RP Woodhams, DC (reprint author), Univ Zurich, Inst Evolutionary Biol & Environm Studies, Zurich, Switzerland. EM dwoodhams@gmail.com FU Swiss National Science Foundation [31-125099] FX Funding was provided through Swiss National Science Foundation grant 31-125099 to D. C. W. and fieldwork was supported by SCNAT (Akademie der Naturwissenschaften Schweiz). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 85 TC 16 Z9 16 U1 2 U2 54 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 29 PY 2014 VL 9 IS 1 AR e87101 DI 10.1371/journal.pone.0087101 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 301ZC UT WOS:000330570000103 PM 24489847 ER PT J AU Ijjas, A Steinhardt, PJ Loeb, A AF Ijjas, Anna Steinhardt, Paul J. Loeb, Abraham TI Scale-free primordial cosmology SO PHYSICAL REVIEW D LA English DT Article ID INFLATIONARY UNIVERSE; PERTURBATIONS; FLUCTUATIONS; INFLATON; FLATNESS; CREATION; HORIZON; MODEL AB The large-scale structure of the Universe suggests that the physics underlying its early evolution is scale-free. This was the historic motivation for the Harrison-Zel'dovich-Peebles spectrum and for inflation. Based on a hydrodynamical approach, we identify scale-free forms for the background equation of state for both inflationary and cyclic scenarios and use these forms to derive predictions for the spectral tilt and tensor-to-scalar ratio of primordial density perturbations. For the case of inflation, we find three classes of scale-free models with distinct predictions. Including all classes, we show that scale-free inflation predicts tensor-to-scalar ratio r > 10(-4). We show that the observationally favored class is theoretically disfavored because it suffers from an initial conditions problem and the hydrodynamical form of an unlikeliness problem similar to that identified recently for certain inflaton potentials. We contrast these results with those for scale-free cyclic models. C1 [Ijjas, Anna] Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-14476 Potsdam, Germany. [Ijjas, Anna] Rutgers State Univ, New Brunswick, NJ 08901 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. [Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ijjas, A (reprint author), Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-14476 Potsdam, Germany. EM aijjas@princeton.edu; steinh@princeton.edu; aloeb@cfa.harvard.edu FU U.S. Department of Energy [DE-FG02-91ER40671]; NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DBB30A]; Perimeter Institute for Theoretical Physics; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research and Innovation; European Research Council [256994]; John Templeton Foundation FX This work was inspired in part by a talk and recent paper by V. Mukhanov [13]. We thank J. Khoury, J.-L. Lehners, and N. Turok for very helpful comments on the manuscript. This research was partially supported by the U.S. Department of Energy under Grant No. DE-FG02-91ER40671 (P. J. S.), by NSF Grant No. AST-0907890 and NASA Grants No. NNX08AL43G and No. NNA09DBB30A (A. L.), and the Perimeter Institute for Theoretical Physics (A. I. and P. J. S.). 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. A. I. also acknowledges the support of the European Research Council via the Starting Grant No. 256994. The work of A. I. is supported in part by a grant from the John Templeton Foundation. A. I. thanks the Physics Department of Princeton University for hospitality while this research was completed. NR 39 TC 7 Z9 7 U1 0 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JAN 28 PY 2014 VL 89 IS 2 AR 023525 DI 10.1103/PhysRevD.89.023525 PG 15 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AB6BJ UT WOS:000331872100004 ER PT J AU Halfwerk, W Jones, PL Taylor, RC Ryan, MJ Page, RA AF Halfwerk, W. Jones, P. L. Taylor, R. C. Ryan, M. J. Page, R. A. TI Risky Ripples Allow Bats and Frogs to Eavesdrop on a Multisensory Sexual Display SO SCIENCE LA English DT Article ID WATER-SURFACE-WAVES; MATING SIGNALS; COMMUNICATION; BEHAVIOR; CUES; PREDATION; EVOLUTION AB Animal displays are often perceived by intended and unintended receivers in more than one sensory system. In addition, cues that are an incidental consequence of signal production can also be perceived by different receivers, even when the receivers use different sensory systems to perceive them. Here we show that the vocal responses of male tungara frogs (Physalaemus pustulosus) increase twofold when call-induced water ripples are added to the acoustic component of a rival's call. Hunting bats (Trachops cirrhosus) can echolocate this signal by-product and prefer to attack model frogs when ripples are added to the acoustic component of the call. This study illustrates how the perception of a signal by-product by intended and unintended receivers through different sensory systems generates both costs and benefits for the signaler. C1 [Halfwerk, W.; Jones, P. L.; Ryan, M. J.; Page, R. A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Halfwerk, W.] Leiden Univ, Inst Biol, NL-2300 RA Leiden, Netherlands. [Jones, P. L.; Ryan, M. J.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. [Taylor, R. C.] Salisbury Univ, Dept Biol, Salisbury, MD 21801 USA. RP Halfwerk, W (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM w.halfwerk@biology.leidenuniv.nl OI Halfwerk, Wouter/0000-0002-4111-0930 FU Netherlands Organization for Scientific Research [825.11.026]; NSF [IOS 1120031] FX We are grateful to M. Dixon, A. Lea, K. Ottens, J. Jacobitz, J. Finley, F. Rhebergen, and M. Shuman-Goodier for valuable help during the experiments. Comments from D. Blumstein, H. Slabbekoorn, J. Ratcliffe, and one anonymous reviewer substantially improved the manuscript, and J. Touchon and S. Dennis provided statistical advice. We thank the late Stan Rand for illuminating discussions about ripples in communication. We thank B. Klein, P. Clements, and Moey Inc. for fabricating the pneumatic robotic frog system. The research was funded through a Rubicon grant (825.11.026) to W. H. from the Netherlands Organization for Scientific Research; an NSF grant (IOS 1120031) to R. C. T., M. J. R., and R. A. P.; and resources made available to R. A. P. from the Smithsonian Tropical Research Institute (STRI). All research reported here complied with STRI Institutional Animal Care and Use Committee protocols. We obtained all required permits from the government of Panama. The authors report no conflict of interest. Raw data will be made available at the Dryad Data Repository (10.5061/dryad.82t1k). NR 27 TC 25 Z9 25 U1 11 U2 59 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 JAN 24 PY 2014 VL 343 IS 6169 BP 413 EP 416 DI 10.1126/science.1244812 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 294IR UT WOS:000330039300047 PM 24458640 ER PT J AU Farley, KA Malespin, C Mahaffy, P Grotzinger, JP Vasconcelos, PM Milliken, RE Malin, M Edgett, KS Pavlov, AA Hurowitz, JA Grant, JA Miller, HB Arvidson, R Beegle, L Calef, F Conrad, PG Dietrich, WE Eigenbrode, J Gellert, R Gupta, S Hamilton, V Hassler, DM Lewis, KW McLennan, SM Ming, D Navarro-Gonzalez, R Schwenzer, SP Steele, A Stolper, EM Sumner, DY Vaniman, D Vasavada, A Williford, K Wimmer-Schweingruber, RF AF Farley, K. A. Malespin, C. Mahaffy, P. Grotzinger, J. P. Vasconcelos, P. M. Milliken, R. E. Malin, M. Edgett, K. S. Pavlov, A. A. Hurowitz, J. A. Grant, J. A. Miller, H. B. Arvidson, R. Beegle, L. Calef, F. Conrad, P. G. Dietrich, W. E. Eigenbrode, J. Gellert, R. Gupta, S. Hamilton, V. Hassler, D. M. Lewis, K. W. McLennan, S. M. Ming, D. Navarro-Gonzalez, R. Schwenzer, S. P. Steele, A. Stolper, E. M. Sumner, D. Y. Vaniman, D. Vasavada, A. Williford, K. Wimmer-Schweingruber, R. F. CA MSL Sci Team TI In Situ Radiometric and Exposure Age Dating of the Martian Surface SO SCIENCE LA English DT Article ID GALE CRATER; MARS; EVOLUTION; HISTORY; ORIGIN; CHRONOLOGY; ISOTOPES; FIELD AB We determined radiogenic and cosmogenic noble gases in a mudstone on the floor of Gale Crater. A K-Ar age of 4.21 +/- 0.35 billion years represents a mixture of detrital and authigenic components and confirms the expected antiquity of rocks comprising the crater rim. Cosmic-ray-produced He-3, Ne-21, and Ar-36 yield concordant surface exposure ages of 78 +/- 30 million years. Surface exposure occurred mainly in the present geomorphic setting rather than during primary erosion and transport. Our observations are consistent with mudstone deposition shortly after the Gale impact or possibly in a later event of rapid erosion and deposition. The mudstone remained buried until recent exposure by wind-driven scarp retreat. Sedimentary rocks exposed by this mechanism may thus offer the best potential for organic biomarker preservation against destruction by cosmic radiation. C1 [Farley, K. A.; Grotzinger, J. P.; Miller, H. B.; Stolper, E. M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Malespin, C.; Mahaffy, P.; Pavlov, A. A.; Conrad, P. G.; Eigenbrode, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Vasconcelos, P. M.] Univ Queensland, Sch Earth Sci, Brisbane, Qld 4072, Australia. [Milliken, R. E.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Malin, M.; Edgett, K. S.] Malin Space Sci Syst, San Diego, CA 92121 USA. [Hurowitz, J. A.; McLennan, S. M.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Grant, J. A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Arvidson, R.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Beegle, L.; Calef, F.; Vasavada, A.; Williford, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dietrich, W. E.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Gupta, S.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England. [Hamilton, V.; Hassler, D. M.] SW Res Inst, Boulder, CO 80302 USA. [Lewis, K. W.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Ming, D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Navarro-Gonzalez, R.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Schwenzer, S. P.] CEPSAR, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Steele, A.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Sumner, D. Y.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. [Vaniman, D.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Wimmer-Schweingruber, R. F.] Univ Kiel, D-24098 Kiel, Germany. RP Farley, KA (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM farley@gps.caltech.edu RI szopa, cyril/C-6865-2015; Martin-Torres, Francisco Javier/G-6329-2015; Harri, Ari-Matti/C-7142-2012; Glavin, Daniel/D-6194-2012; Zorzano, Maria-Paz/F-2184-2015; Dworkin, Jason/C-9417-2012; Frydenvang, Jens/D-4781-2013; Gonzalez, Rafael/D-1748-2009; Balic-Zunic, Tonci/A-6362-2013; Lemmon, Mark/E-9983-2010; de Pablo, Miguel Angel/J-6442-2014; Gomez-Elvira, Javier/K-5829-2014; Ramos, Miguel/K-2230-2014; Gomez, Felipe/L-7315-2014; Rodriguez-Manfredi, Jose/L-8001-2014; Hayes, Alexander/P-2024-2014; Zorzano, Maria-Paz/C-5784-2015 OI Schwenzer, Susanne Petra/0000-0002-9608-0759; szopa, cyril/0000-0002-0090-4056; Martin-Torres, Francisco Javier/0000-0001-6479-2236; Harri, Ari-Matti/0000-0001-8541-2802; Glavin, Daniel/0000-0001-7779-7765; Zorzano, Maria-Paz/0000-0002-4492-9650; Dworkin, Jason/0000-0002-3961-8997; Edgett, Kenneth/0000-0001-7197-5751; Muller, Jan-Peter/0000-0002-5077-3736; Frydenvang, Jens/0000-0001-9294-1227; Balic-Zunic, Tonci/0000-0003-1687-1233; Lemmon, Mark/0000-0002-4504-5136; de Pablo, Miguel Angel/0000-0002-4496-2741; Gomez-Elvira, Javier/0000-0002-9068-9846; Ramos, Miguel/0000-0003-3648-6818; Gomez, Felipe/0000-0001-9977-7060; Rodriguez-Manfredi, Jose/0000-0003-0461-9815; Hayes, Alexander/0000-0001-6397-2630; Zorzano, Maria-Paz/0000-0002-4492-9650 FU National Aeronautics and Space Administration FX The authors are indebted to the Mars Science Laboratory (MSL) Project engineering and management teams for their exceptionally skilled and diligent efforts in making the mission as effective as possible and enhancing science operations. We are also grateful to all those MSL team members who participated in tactical and strategic operations. Without the support of both the engineering and science teams, the data presented here could not have been collected. Three anonymous reviewers provided many helpful suggestions. Some of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Data presented in this paper are archived in the Planetary Data System (pds.nasa.gov). NR 35 TC 65 Z9 65 U1 7 U2 91 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 JAN 24 PY 2014 VL 343 IS 6169 AR 1247166 DI 10.1126/science.1247166 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 294IR UT WOS:000330039300007 PM 24324273 ER PT J AU McLennan, SM Anderson, RB Bell, JF Bridges, JC Calef, F Campbell, JL Clark, BC Clegg, S Conrad, P Cousin, A Des Marais, DJ Dromart, G Dyar, MD Edgar, LA Ehlmann, BL Fabre, C Forni, O Gasnault, O Gellert, R Gordon, S Grant, JA Grotzinger, JP Gupta, S Herkenhoff, KE Hurowitz, JA King, PL Le Mouelic, S Leshin, LA Leveille, R Lewis, KW Mangold, N Maurice, S Ming, DW Morris, RV Nachon, M Newsom, HE Ollila, AM Perrett, GM Rice, MS Schmidt, ME Schwenzer, SP Stack, K Stolper, EM Sumner, DY Treiman, AH VanBommel, S Vaniman, DT Vasavada, A Wiens, RC Yingst, RA AF McLennan, S. M. Anderson, R. B. Bell, J. F., III Bridges, J. C. Calef, F., III Campbell, J. L. Clark, B. C. Clegg, S. Conrad, P. Cousin, A. Des Marais, D. J. Dromart, G. Dyar, M. D. Edgar, L. A. Ehlmann, B. L. Fabre, C. Forni, O. Gasnault, O. Gellert, R. Gordon, S. Grant, J. A. Grotzinger, J. P. Gupta, S. Herkenhoff, K. E. Hurowitz, J. A. King, P. L. Le Mouelic, S. Leshin, L. A. Leveille, R. Lewis, K. W. Mangold, N. Maurice, S. Ming, D. W. Morris, R. V. Nachon, M. Newsom, H. E. Ollila, A. M. Perrett, G. M. Rice, M. S. Schmidt, M. E. Schwenzer, S. P. Stack, K. Stolper, E. M. Sumner, D. Y. Treiman, A. H. VanBommel, S. Vaniman, D. T. Vasavada, A. Wiens, R. C. Yingst, R. A. CA MSL Sci Team TI Elemental Geochemistry of Sedimentary Rocks at Yellowknife Bay, Gale Crater, Mars SO SCIENCE LA English DT Article ID CHEMCAM INSTRUMENT SUITE; CLAY MINERAL FORMATION; MERIDIANI-PLANUM; SILICICLASTIC SEDIMENTS; MASS-BALANCE; CANADA; PROVENANCE; PETROGENESIS; CHEMISTRY; PROFILES AB Sedimentary rocks examined by the Curiosity rover at Yellowknife Bay, Mars, were derived from sources that evolved from an approximately average martian crustal composition to one influenced by alkaline basalts. No evidence of chemical weathering is preserved, indicating arid, possibly cold, paleoclimates and rapid erosion and deposition. The absence of predicted geochemical variations indicates that magnetite and phyllosilicates formed by diagenesis under low-temperature, circumneutral pH, rock-dominated aqueous conditions. Analyses of diagenetic features (including concretions, raised ridges, and fractures) at high spatial resolution indicate that they are composed of iron-and halogen-rich components, magnesium-iron-chlorine-rich components, and hydrated calcium sulfates, respectively. Composition of a cross-cutting dike-like feature is consistent with sedimentary intrusion. The geochemistry of these sedimentary rocks provides further evidence for diverse depositional and diagenetic sedimentary environments during the early history of Mars. C1 [McLennan, S. M.; Hurowitz, J. A.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Anderson, R. B.; Herkenhoff, K. E.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Bell, J. F., III; Edgar, L. A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Bridges, J. C.] Univ Leicester, Dept Phys & Astron, Space Res Ctr, Leicester LE1 7RH, Leics, England. [Calef, F., III; Ehlmann, B. L.; Vasavada, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Campbell, J. L.; Gellert, R.; Perrett, G. M.; VanBommel, S.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Clark, B. C.] Space Sci Inst, Boulder, CO 80301 USA. [Clegg, S.; Cousin, A.] Los Alamos Natl Lab, Div Chem, Los Alamos, NM 87545 USA. [Conrad, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Des Marais, D. J.] NASA, Ames Res Ctr, Dept Space Sci, Moffett Field, CA 94035 USA. [Dromart, G.] Univ Lyon, Lab Geol Lyon, F-69364 Lyon, France. [Dyar, M. D.] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. [Ehlmann, B. L.; Grotzinger, J. P.; Rice, M. S.; Stack, K.; Stolper, E. M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Fabre, C.] Fac Sci, CNRS Georesources, UMR 7359, F-54506 Vandoeuvre Les Nancy, France. [Forni, O.; Gasnault, O.] Univ Toulouse, IRAP, UPS OMP CNRS, F-31028 Toulouse 4, France. [Gordon, S.; Newsom, H. E.; Ollila, A. M.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Grant, J. A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Sci, Washington, DC 20560 USA. [Gupta, S.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England. [King, P. L.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. [Le Mouelic, S.; Mangold, N.; Nachon, M.] LPGN CNRS UMR 6112, Lab Planetol & Geodynam, F-4432 Nantes, France. [Le Mouelic, S.; Mangold, N.; Nachon, M.] Univ Nantes, F-4432 Nantes, France. [Leshin, L. A.] Rensselaer Polytech Inst, Sch Sci, Troy, NY 12180 USA. [Leveille, R.] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. [Lewis, K. W.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Maurice, S.] Observ Midi Pyrenees, F-31400 Toulouse, France. [Ming, D. W.; Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Schmidt, M. E.] Brock Univ, Dept Earth Sci, St Catharines, ON L2S 3A1, Canada. [Schwenzer, S. P.] Open Univ, CEPSAR, Milton Keynes MK7 6AA, Bucks, England. [Sumner, D. Y.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Treiman, A. H.] Lunar Planetary Sci Inst, Houston, TX 77058 USA. [Vaniman, D. T.; Yingst, R. A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Wiens, R. C.] Los Alamos Natl Lab, Int Space & Response Div, Los Alamos, NM 87545 USA. RP McLennan, SM (reprint author), SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. EM scott.mclennan@stonybrook.edu RI Hayes, Alexander/P-2024-2014; Zorzano, Maria-Paz/C-5784-2015; Frydenvang, Jens/D-4781-2013; Gonzalez, Rafael/D-1748-2009; Balic-Zunic, Tonci/A-6362-2013; Lemmon, Mark/E-9983-2010; de Pablo, Miguel Angel/J-6442-2014; Gomez-Elvira, Javier/K-5829-2014; Ramos, Miguel/K-2230-2014; Gomez, Felipe/L-7315-2014; Rodriguez-Manfredi, Jose/L-8001-2014; szopa, cyril/C-6865-2015; Martin-Torres, Francisco Javier/G-6329-2015; King, Penelope/A-1791-2011; Harri, Ari-Matti/C-7142-2012; Glavin, Daniel/D-6194-2012; Zorzano, Maria-Paz/F-2184-2015; Dworkin, Jason/C-9417-2012; OI Schwenzer, Susanne Petra/0000-0002-9608-0759; Clegg, Sam/0000-0002-0338-0948; Hayes, Alexander/0000-0001-6397-2630; Zorzano, Maria-Paz/0000-0002-4492-9650; Frydenvang, Jens/0000-0001-9294-1227; Balic-Zunic, Tonci/0000-0003-1687-1233; Lemmon, Mark/0000-0002-4504-5136; de Pablo, Miguel Angel/0000-0002-4496-2741; Gomez-Elvira, Javier/0000-0002-9068-9846; Ramos, Miguel/0000-0003-3648-6818; Gomez, Felipe/0000-0001-9977-7060; Rodriguez-Manfredi, Jose/0000-0003-0461-9815; szopa, cyril/0000-0002-0090-4056; Martin-Torres, Francisco Javier/0000-0001-6479-2236; King, Penelope/0000-0002-8364-9168; Harri, Ari-Matti/0000-0001-8541-2802; Glavin, Daniel/0000-0001-7779-7765; Zorzano, Maria-Paz/0000-0002-4492-9650; Dworkin, Jason/0000-0002-3961-8997; Muller, Jan-Peter/0000-0002-5077-3736 FU French Space Agency; NASA; CNES; Canadian Space Agency; NSERC (Canada); United Kingdom Space Agency (UK) FX Much of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Development and operation of the ChemCam and APXS instruments were also supported by funds from the French Space Agency, CNES, and the Canadian Space Agency. Organizations supporting research include NASA, the Canadian Space Agency, NSERC (Canada), and the United Kingdom Space Agency (UK). Chemical data presented here are derived from archived data sets in the NASA Planetary Data System (PDS), http://pds-geosciences.wustl.edu/missions/msl. We are grateful to the MSL engineering and management teams for making the mission and this scientific investigation possible and to science team members who contributed to mission operations. S. M. M. thanks Lamont-Doherty Earth Observatory of Columbia University, and especially S. Hemming, for hospitality during a sabbatical when the manuscript was being prepared. NR 62 TC 105 Z9 106 U1 15 U2 158 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 JAN 24 PY 2014 VL 343 IS 6169 AR 1244734 DI 10.1126/science.1244734 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 294IR UT WOS:000330039300004 PM 24324274 ER PT J AU Ming, DW Archer, PD Glavin, DP Eigenbrode, JL Franz, HB Sutter, B Brunner, AE Stern, JC Freissinet, C McAdam, AC Mahaffy, PR Cabane, M Coll, P Campbell, JL Atreya, SK Niles, PB Bell, JF Bish, DL Brinckerhoff, WB Buch, A Conrad, PG Des Marais, DJ Ehlmann, BL Fairen, AG Farley, K Flesch, GJ Francois, P Gellert, R Grant, JA Grotzinger, JP Gupta, S Herkenhoff, KE Hurowitz, JA Leshin, LA Lewis, KW McLennan, SM Miller, KE Moersch, J Morris, RV Navarro-Gonzalez, R Pavlov, AA Perrett, GM Pradler, I Squyres, SW Summons, RE Steele, A Stolper, EM Sumner, DY Szopa, C Teinturier, S Trainer, MG Treiman, AH Vaniman, DT Vasavada, AR Webster, CR Wray, JJ Yingst, RA AF Ming, D. W. Archer, P. D., Jr. Glavin, D. P. Eigenbrode, J. L. Franz, H. B. Sutter, B. Brunner, A. E. Stern, J. C. Freissinet, C. McAdam, A. C. Mahaffy, P. R. Cabane, M. Coll, P. Campbell, J. L. Atreya, S. K. Niles, P. B. Bell, J. F., III Bish, D. L. Brinckerhoff, W. B. Buch, A. Conrad, P. G. Des Marais, D. J. Ehlmann, B. L. Fairen, A. G. Farley, K. Flesch, G. J. Francois, P. Gellert, R. Grant, J. A. Grotzinger, J. P. Gupta, S. Herkenhoff, K. E. Hurowitz, J. A. Leshin, L. A. Lewis, K. W. McLennan, S. M. Miller, K. E. Moersch, J. Morris, R. V. Navarro-Gonzalez, R. Pavlov, A. A. Perrett, G. M. Pradler, I. Squyres, S. W. Summons, R. E. Steele, A. Stolper, E. M. Sumner, D. Y. Szopa, C. Teinturier, S. Trainer, M. G. Treiman, A. H. Vaniman, D. T. Vasavada, A. R. Webster, C. R. Wray, J. J. Yingst, R. A. CA MSL Sci Team TI Volatile and Organic Compositions of Sedimentary Rocks in Yellowknife Bay, Gale Crater, Mars SO SCIENCE LA English DT Article ID MARTIAN SOIL; SULFUR-DIOXIDE; PERCHLORATE; HYDROGEN; SURFACE; ANALOG; SITE AB H2O, CO2, SO2, O-2, H-2, H2S, HCl, chlorinated hydrocarbons, NO, and other trace gases were evolved during pyrolysis of two mudstone samples acquired by the Curiosity rover at Yellowknife Bay within Gale crater, Mars. H2O/OH-bearing phases included 2:1 phyllosilicate(s), bassanite, akaganeite, and amorphous materials. Thermal decomposition of carbonates and combustion of organic materials are candidate sources for the CO2. Concurrent evolution of O-2 and chlorinated hydrocarbons suggests the presence of oxychlorine phase(s). Sulfides are likely sources for sulfur-bearing species. Higher abundances of chlorinated hydrocarbons in the mudstone compared with Rocknest windblown materials previously analyzed by Curiosity suggest that indigenous martian or meteoritic organic carbon sources may be preserved in the mudstone; however, the carbon source for the chlorinated hydrocarbons is not definitively of martian origin. C1 [Ming, D. W.; Niles, P. B.; Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. [Archer, P. D., Jr.; Sutter, B.] Jacobs, Houston, TX 77058 USA. [Glavin, D. P.; Eigenbrode, J. L.; Franz, H. B.; Brunner, A. E.; Stern, J. C.; Freissinet, C.; McAdam, A. C.; Mahaffy, P. R.; Brinckerhoff, W. B.; Conrad, P. G.; Pavlov, A. A.; Trainer, M. G.] NASA, Goddard Space Flight Ctr, Planetary Environments Lab, Greenbelt, MD 20771 USA. [Franz, H. B.] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA. [Brunner, A. E.] Univ Maryland, Dept Astron, Ctr Res & Explorat Space Sci & Technol, College Pk, MD 20742 USA. [Freissinet, C.] NASA, Goddard Space Flight Ctr, NASA Postdoctoral Program, Greenbelt, MD 20771 USA. [Cabane, M.] Univ Versailles St Quentin, Univ Paris 06, Lab Atmospheres, UMR CNRS 8970, F-75005 Paris, France. [Coll, P.; Francois, P.; Szopa, C.; Teinturier, S.] Univ Paris Diderot, Univ Paris Est Creteil, Lab Interuniv Syst Atmospher, F-94000 Creteil, France. [Coll, P.; Francois, P.; Szopa, C.; Teinturier, S.] CNRS, F-94000 Creteil, France. [Campbell, J. L.; Gellert, R.; Perrett, G. M.; Pradler, I.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Atreya, S. K.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Bell, J. F., III] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Bish, D. L.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. [Buch, A.] Ecole Cent Paris, Lab Genie Procedes & Mat, F-92295 Chatenay Malabry, France. [Des Marais, D. J.] NASA, Ames Res Ctr, Dept Space Sci, Moffett Field, CA 94035 USA. [Ehlmann, B. L.; Farley, K.; Grotzinger, J. P.; Stolper, E. M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Ehlmann, B. L.; Flesch, G. J.; Vasavada, A. R.; Webster, C. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fairen, A. G.; Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Grant, J. A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Gupta, S.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England. [Herkenhoff, K. E.] US Geol Survey, Flagstaff, AZ 86001 USA. [Hurowitz, J. A.; McLennan, S. M.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Leshin, L. A.] Rensselaer Polytech Inst, Dept Earth & Environm Sci, Troy, NY 12180 USA. [Leshin, L. A.] Rensselaer Polytech Inst, Sch Sci, Troy, NY 12180 USA. [Lewis, K. W.] Princeton Univ, Princeton, NJ 08544 USA. [Miller, K. E.; Summons, R. E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Moersch, J.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Navarro-Gonzalez, R.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Steele, A.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Sumner, D. Y.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Treiman, A. H.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Vaniman, D. T.; Yingst, R. A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Wray, J. J.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. RP Ming, DW (reprint author), NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. EM douglas.w.ming@nasa.gov RI Hayes, Alexander/P-2024-2014; Trainer, Melissa/E-1477-2012; Zorzano, Maria-Paz/C-5784-2015; szopa, cyril/C-6865-2015; Martin-Torres, Francisco Javier/G-6329-2015; Glavin, Daniel/D-6194-2012; Harri, Ari-Matti/C-7142-2012; Zorzano, Maria-Paz/F-2184-2015; Dworkin, Jason/C-9417-2012; Gomez-Elvira, Javier/K-5829-2014; Ramos, Miguel/K-2230-2014; Gomez, Felipe/L-7315-2014; Rodriguez-Manfredi, Jose/L-8001-2014; Wray, James/B-8457-2008; Stern, Jennifer/E-3135-2012; Frydenvang, Jens/D-4781-2013; Gonzalez, Rafael/D-1748-2009; Balic-Zunic, Tonci/A-6362-2013; Lemmon, Mark/E-9983-2010; de Pablo, Miguel Angel/J-6442-2014 OI Hayes, Alexander/0000-0001-6397-2630; Zorzano, Maria-Paz/0000-0002-4492-9650; szopa, cyril/0000-0002-0090-4056; Martin-Torres, Francisco Javier/0000-0001-6479-2236; Glavin, Daniel/0000-0001-7779-7765; Harri, Ari-Matti/0000-0001-8541-2802; Zorzano, Maria-Paz/0000-0002-4492-9650; Dworkin, Jason/0000-0002-3961-8997; Muller, Jan-Peter/0000-0002-5077-3736; Gomez-Elvira, Javier/0000-0002-9068-9846; Ramos, Miguel/0000-0003-3648-6818; Gomez, Felipe/0000-0001-9977-7060; Rodriguez-Manfredi, Jose/0000-0003-0461-9815; Wray, James/0000-0001-5559-2179; Stern, Jennifer/0000-0002-0162-8807; Frydenvang, Jens/0000-0001-9294-1227; Balic-Zunic, Tonci/0000-0003-1687-1233; Lemmon, Mark/0000-0002-4504-5136; de Pablo, Miguel Angel/0000-0002-4496-2741 FU National Aeronautics and Space Administration (NASA); French Space Agency (CNES); Canadian Space Agency; UK Space Agency; NASA ROSES MSL Participating Scientist Program FX We are indebted to the Mars Science Laboratory Project engineering and management teams for making this mission possible and enhancing science operations. Much of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). NASA provided support for the development of SAM. Data from these SAM experiments are archived in the Planetary Data System (pds.nasa.gov). Essential contributions to the successful operation of SAM on Mars and the acquisition of this data were provided by the SAM development, operations, and testbed teams. Development and operation of the SAM and APXS instruments were also supported by funds from the French Space Agency (CNES) and the Canadian Space Agency. Work in the UK was funded by the UK Space Agency. B. L. E., J.L.E., K. F., D. P. G., J.E.G., K. E. M., S. M. M., J.M., P.B.N., and R. E. S. acknowledge funding support from the NASA ROSES MSL Participating Scientist Program. NR 47 TC 96 Z9 97 U1 18 U2 184 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 JAN 24 PY 2014 VL 343 IS 6169 AR 1245267 DI 10.1126/science.1245267 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 294IR UT WOS:000330039300006 PM 24324276 ER PT J AU Grotzinger, JP Sumner, DY Kah, LC Stack, K Gupta, S Edgar, L Rubin, D Lewis, K Schieber, J Mangold, N Milliken, R Conrad, PG DesMarais, D Farmer, J Siebach, K Calef, F Hurowitz, J McLennan, SM Ming, D Vaniman, D Crisp, J Vasavada, A Edgett, KS Malin, M Blake, D Gellert, R Mahaffy, P Wiens, RC Maurice, S Grant, JA Wilson, S Anderson, RC Beegle, L Arvidson, R Hallet, B Sletten, RS Rice, M Bell, J Griffes, J Ehlmann, B Anderson, RB Bristow, TF Dietrich, WE Dromart, G Eigenbrode, J Fraeman, A Hardgrove, C Herkenhoff, K Jandura, L Kocurek, G Lee, S Leshin, LA Leveille, R Limonadi, D Maki, J McCloskey, S Meyer, M Minitti, M Newsom, H Oehler, D Okon, A Palucis, M Parker, T Rowland, S Schmidt, M Squyres, S Steele, A Stolper, E Summons, R Treiman, A Williams, R Yingst, A AF Grotzinger, J. P. Sumner, D. Y. Kah, L. C. Stack, K. Gupta, S. Edgar, L. Rubin, D. Lewis, K. Schieber, J. Mangold, N. Milliken, R. Conrad, P. G. DesMarais, D. Farmer, J. Siebach, K. Calef, F., III Hurowitz, J. McLennan, S. M. Ming, D. Vaniman, D. Crisp, J. Vasavada, A. Edgett, K. S. Malin, M. Blake, D. Gellert, R. Mahaffy, P. Wiens, R. C. Maurice, S. Grant, J. A. Wilson, S. Anderson, R. C. Beegle, L. Arvidson, R. Hallet, B. Sletten, R. S. Rice, M. Bell, J., III Griffes, J. Ehlmann, B. Anderson, R. B. Bristow, T. F. Dietrich, W. E. Dromart, G. Eigenbrode, J. Fraeman, A. Hardgrove, C. Herkenhoff, K. Jandura, L. Kocurek, G. Lee, S. Leshin, L. A. Leveille, R. Limonadi, D. Maki, J. McCloskey, S. Meyer, M. Minitti, M. Newsom, H. Oehler, D. Okon, A. Palucis, M. Parker, T. Rowland, S. Schmidt, M. Squyres, S. Steele, A. Stolper, E. Summons, R. Treiman, A. Williams, R. Yingst, A. CA MSL Sci Team TI A Habitable Fluvio-Lacustrine Environment at Yellowknife Bay, Gale Crater, Mars SO SCIENCE LA English DT Article ID LOW WATER ACTIVITY; MERIDIANI-PLANUM; SEDIMENTARY-ROCKS; LIFE; BASIN; HYDROGEN; DEPOSITS; ORIGIN; LACUSTRINE; SHRINKAGE AB The Curiosity rover discovered fine-grained sedimentary rocks, which are inferred to represent an ancient lake and preserve evidence of an environment that would have been suited to support a martian biosphere founded on chemolithoautotrophy. This aqueous environment was characterized by neutral pH, low salinity, and variable redox states of both iron and sulfur species. Carbon, hydrogen, oxygen, sulfur, nitrogen, and phosphorus were measured directly as key biogenic elements; by inference, phosphorus is assumed to have been available. The environment probably had a minimum duration of hundreds to tens of thousands of years. These results highlight the biological viability of fluvial-lacustrine environments in the post-Noachian history of Mars. C1 [Grotzinger, J. P.; Stack, K.; Siebach, K.; Rice, M.; Griffes, J.; Ehlmann, B.; Stolper, E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Sumner, D. Y.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Kah, L. C.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Gupta, S.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England. [Edgar, L.; Farmer, J.; Bell, J., III; Minitti, M.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Rubin, D.] US Geol Survey, Santa Cruz, CA 95060 USA. [Lewis, K.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Schieber, J.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. [Mangold, N.] LPGN CNRS UMR6112, LPGN, F-44322 Nantes, France. [Mangold, N.] Univ Nantes, F-44322 Nantes, France. [Milliken, R.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Conrad, P. G.; Mahaffy, P.; Eigenbrode, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [DesMarais, D.; Blake, D.; Bristow, T. F.] NASA, Ames Res Ctr, Dept Space Sci, Moffett Field, CA 94035 USA. [Calef, F., III; Crisp, J.; Vasavada, A.; Anderson, R. C.; Beegle, L.; Ehlmann, B.; Jandura, L.; Lee, S.; Limonadi, D.; Maki, J.; McCloskey, S.; Okon, A.; Parker, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hurowitz, J.; McLennan, S. M.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Ming, D.; Oehler, D.] NASA, Lyndon B Johnson Space Ctr, Jacobs Technol, Houston, TX 77058 USA. [Vaniman, D.; Williams, R.; Yingst, A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Edgett, K. S.; Malin, M.; Hardgrove, C.] Malin Space Sci Syst, San Diego, CA 92121 USA. [Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Wiens, R. C.] Los Alamos Natl Lab, Los Alamos, NM 87544 USA. [Maurice, S.] Univ Toulouse, CNRS, IRAP, F-31400 Toulouse, France. [Grant, J. A.; Wilson, S.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Arvidson, R.; Fraeman, A.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Hallet, B.; Sletten, R. S.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Anderson, R. B.; Herkenhoff, K.] US Geol Survey, Flagstaff, AZ 86001 USA. [Dietrich, W. E.; Palucis, M.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Dromart, G.] Univ Lyon, Lab Geol Lyon, F-69364 Lyon, France. [Kocurek, G.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA. [Leshin, L. A.] Rensselaer Polytech Inst, Sch Sci, Troy, NY 12180 USA. [Leveille, R.] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. [Meyer, M.] NASA Headquarters, Washington, DC 20546 USA. [Newsom, H.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Rowland, S.] Univ Hawaii Manoa, Dept Geol & Geophys, Honolulu, HI 96822 USA. [Schmidt, M.] Brock Univ, Dept Earth Sci, St Catharines, ON L2S 3A1, Canada. [Squyres, S.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Steele, A.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Summons, R.] MIT, Dept Earth & Planetary Sci, Cambridge, MA 02139 USA. [Treiman, A.] Lunar & Planetary Inst, Houston, TX 77058 USA. RP Grotzinger, JP (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM grotz@gps.caltech.edu RI Zorzano, Maria-Paz/C-5784-2015; Ramos, Miguel/K-2230-2014; Lemmon, Mark/E-9983-2010; Glavin, Daniel/D-6194-2012; Balic-Zunic, Tonci/A-6362-2013; Zorzano, Maria-Paz/F-2184-2015; Dworkin, Jason/C-9417-2012; Gomez, Felipe/L-7315-2014; Rodriguez-Manfredi, Jose/L-8001-2014; Harri, Ari-Matti/C-7142-2012; Crisp, Joy/H-8287-2016; Gonzalez, Rafael/D-1748-2009; szopa, cyril/C-6865-2015; Hayes, Alexander/P-2024-2014; Frydenvang, Jens/D-4781-2013; Gomez-Elvira, Javier/K-5829-2014; de Pablo, Miguel Angel/J-6442-2014; Martin-Torres, Francisco Javier/G-6329-2015 OI Edgett, Kenneth/0000-0001-7197-5751; Zorzano, Maria-Paz/0000-0002-4492-9650; Ramos, Miguel/0000-0003-3648-6818; Lemmon, Mark/0000-0002-4504-5136; Glavin, Daniel/0000-0001-7779-7765; Balic-Zunic, Tonci/0000-0003-1687-1233; Zorzano, Maria-Paz/0000-0002-4492-9650; Dworkin, Jason/0000-0002-3961-8997; Siebach, Kirsten/0000-0002-6628-6297; Gomez, Felipe/0000-0001-9977-7060; Rodriguez-Manfredi, Jose/0000-0003-0461-9815; Harri, Ari-Matti/0000-0001-8541-2802; Crisp, Joy/0000-0002-3202-4416; szopa, cyril/0000-0002-0090-4056; Hayes, Alexander/0000-0001-6397-2630; Frydenvang, Jens/0000-0001-9294-1227; Gomez-Elvira, Javier/0000-0002-9068-9846; de Pablo, Miguel Angel/0000-0002-4496-2741; Martin-Torres, Francisco Javier/0000-0001-6479-2236 FU NASA FX We are indebted to the MSL Project engineering and management teams for their exceptionally skilled and diligent efforts in making the mission as effective as possible and enhancing science operations. We are also grateful to all those MSL Science Team members who participated in tactical and strategic operations. Without the support of both the engineering and science teams, the data presented here could not have been collected. Some of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Data presented in this paper are archived in the Planetary Data System (pds.nasa.gov). NR 90 TC 165 Z9 169 U1 10 U2 33 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 JAN 24 PY 2014 VL 343 IS 6169 AR 1242777 DI 10.1126/science.1242777 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 294IR UT WOS:000330039300002 PM 24458635 ER PT J AU Hammer, TJ McMillan, WO Fierer, N AF Hammer, Tobin J. McMillan, W. Owen Fierer, Noah TI Metamorphosis of a Butterfly-Associated Bacterial Community SO PLOS ONE LA English DT Article ID MOTH LYMANTRIA-DISPAR; HELICONIUS BUTTERFLIES; MANDUCA-SEXTA; GUT BACTERIA; MICROBIAL DIVERSITY; LIFE STAGES; HOST-PLANT; LEPIDOPTERA; MIDGUT; INSECTS AB Butterflies are charismatic insects that have long been a focus of biological research. They are also habitats for microorganisms, yet these microbial symbionts are little-studied, despite their likely importance to butterfly ecology and evolution. In particular, the diversity and composition of the microbial communities inhabiting adult butterflies remain uncharacterized, and it is unknown how the larval (caterpillar) and adult microbiota compare. To address these knowledge gaps, we used Illumina sequencing of 16S rRNA genes from internal bacterial communities associated with multiple life stages of the neotropical butterfly Heliconius erato. We found that the leaf-chewing larvae and nectar-and pollen-feeding adults of H. erato contain markedly distinct bacterial communities, a pattern presumably rooted in their distinct diets. Larvae and adult butterflies host relatively small and similar numbers of bacterial phylotypes, but few are common to both stages. The larval microbiota clearly simplifies and reorganizes during metamorphosis; thus, structural changes in a butterfly's bacterial community parallel those in its own morphology. We furthermore identify specific bacterial taxa that may mediate larval and adult feeding biology in Heliconius and other butterflies. Although male and female Heliconius adults differ in reproductive physiology and degree of pollen feeding, bacterial communities associated with H. erato are not sexually dimorphic. Lastly, we show that captive and wild individuals host different microbiota, a finding that may have important implications for the relevance of experimental studies using captive butterflies. C1 [Hammer, Tobin J.; Fierer, Noah] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. [Hammer, Tobin J.; Fierer, Noah] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Hammer, Tobin J.; McMillan, W. Owen] Smithsonian Trop Res Inst, Panama City, Panama. RP Hammer, TJ (reprint author), Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. EM tobin.hammer@colorado.edu FU Chancellor's Fellowship from the University of Colorado; National Science Foundation [DEB-640279, IOS-1052541, NSF-CAREER 0953331] FX T.J.H. was supported by a Chancellor's Fellowship from the University of Colorado. The National Science Foundation provided grants to W.O.M. (DEB-640279 and IOS-1052541) and N.F. (NSF-CAREER 0953331). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 80 TC 16 Z9 17 U1 23 U2 118 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 JAN 23 PY 2014 VL 9 IS 1 AR e86995 DI 10.1371/journal.pone.0086995 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 297XI UT WOS:000330288000181 PM 24466308 ER PT J AU Averill, C Turner, BL Finzi, AC AF Averill, Colin Turner, Benjamin L. Finzi, Adrien C. TI Mycorrhiza-mediated competition between plants and decomposers drives soil carbon storage SO NATURE LA English DT Article ID ORGANIC-CARBON; LITTER DECOMPOSITION; MICROBIAL EFFICIENCY; NITROGEN LIMITATION; CLIMATE; ECOSYSTEMS; FUNGI; MODEL; PRODUCTIVITY; SENSITIVITY AB Soil contains more carbon than the atmosphere and vegetation combined(1). Understanding the mechanisms controlling the accumulation and stability of soil carbon is critical to predicting the Earth's future climate(2,3). Recent studies suggest that decomposition of soil organic matter is often limited by nitrogen availability to microbes(4-6) and that plants, via their fungal symbionts, compete directly with free-living decomposers for nitrogen(6,7). Ectomycorrhizal and ericoid mycorrhizal (EEM) fungi produce nitrogen-degrading enzymes, allowing them greater access to organic nitrogen sources than arbuscular mycorrhizal (AM) fungi(8-10). This leads to the theoretical prediction that soil carbon storage is greater in ecosystems dominated by EEM fungi than in those dominated by AM fungi(11). Using global data sets, we show that soil in ecosystems dominated by EEM-associated plants contains 70% more carbon per unit nitrogen than soil in ecosystems dominated by AM-associated plants. The effect of mycorrhizal type on soil carbon is independent of, and of far larger consequence than, the effects of net primary production, temperature, precipitation and soil clay content. Hence the effect of mycorrhizal type on soil carbon content holds at the global scale. This finding links the functional traits of mycorrhizal fungi to carbon storage at ecosystem-to-global scales, suggesting that plant-decomposer competition for nutrients exerts a fundamental control over the terrestrial carbon cycle. C1 [Averill, Colin] Univ Texas Austin, Dept Integrat Biol, Grad Program Ecol Evolut & Behav, Austin, TX 78712 USA. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Finzi, Adrien C.] Boston Univ, Dept Biol, Boston, MA 02215 USA. RP Averill, C (reprint author), Univ Texas Austin, Dept Integrat Biol, Grad Program Ecol Evolut & Behav, Austin, TX 78712 USA. EM colin.averill@utexas.edu RI Turner, Benjamin/E-5940-2011; Finzi, Adrien/A-7017-2016 OI Turner, Benjamin/0000-0002-6585-0722; Finzi, Adrien/0000-0003-2220-4533 FU Center for Tropical Forest Science (CTFS); Smithsonian Institution Geo-observatories (SIGEO); University of Texas at Austin; National Science Foundation [DGE-1110007]; NSF [DEB 07-43564]; DOE [10-DOE-1053, DE-SC0006916] FX We thank L. Nave and the International Soil Carbon Network for access to their database. C. Hawkes provided feedback during data collection and initial analyses of C storage. C. Iversen, J. Powers and M. Vadeboncouer provided unpublished data that contributed to this analysis. D. Jacquier provided the Australian soil database and E. Carlston helped to extract data from the Australian soil database. C. Shaw provided the Siltanen soil carbon database and the Forest Ecosystem Carbon Database of Canadian soils. T. Baisden provided scans of the California Soil-Vegetation Survey. E. Brzostek, N. Fowler, P. Groffman, E. Hobbie, B. Schlesinger and B. Waring provided feedback on earlier versions of this manuscript. The Center for Tropical Forest Science (CTFS) and Smithsonian Institution Geo-observatories (SIGEO) provided funding for the collection and analysis of soil profile data at large forest dynamics plots, and we thank the many collaborators, field assistants and laboratory technicians who assisted in the collection and analysis of soil profile data. This work benefited from extensive data contributions to the International Soil Carbon Network from both the USDA Natural Resources Conservation Service, National Cooperative Soil Survey, and the US Geological Survey. C.A. was supported by a fellowship from the University of Texas at Austin and by the National Science Foundation Graduate Research Fellowship Program (grant DGE-1110007). A.C.F. was supported by NSF grant number DEB 07-43564 and DOE grants 10-DOE-1053 and DE-SC0006916. Any opinions, findings and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. NR 40 TC 137 Z9 139 U1 77 U2 617 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JAN 23 PY 2014 VL 505 IS 7484 BP 543 EP + DI 10.1038/nature12901 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 293SW UT WOS:000329995000038 PM 24402225 ER PT J AU Shockley, FW Alekseev, VI AF Shockley, Floyd W. Alekseev, Vitaly I. TI Glesirhanis bercioi, a new genus and species from Baltic amber (Coleoptera: Endomychidae: Leiestinae) with a checklist and nomenclatural notes regarding fossil Endomychidae SO ZOOTAXA LA English DT Article DE new genus; new species; new status; Coleoptera; Endomychidae; Leiestinae; Baltic amber; Tertiary; Eocene; key; checklist; fossil ID PHYLOGENETIC ANALYSIS; CUCUJOIDEA; INSECTA; GENERA; FAMILY AB A new genus and species of handsome fungus beetle, Glesirhanis bercioi gen. nov., sp. nov. (Coleoptera: Endomychidae: Leiestinae) is described from Baltic amber. The newly described genus is compared with all known extant and extinct genera of the subfamily. A key to the genera of Leiestinae including fossils and a checklist of fossil Endomychidae are provided. The status of two taxa previously placed in Endomychidae, Palaeoendomychus gymnus Zhang and Tetrameropsis mesozoica Kirejtshuk & Azar, is discussed, and a new status for the latter, elevating it to the family-level as Tetrameropseidae status nov., is proposed. C1 [Shockley, Floyd W.] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Alekseev, Vitaly I.] Kaliningrad State Tech Univ, Dept Zootechny, Kaliningrad 236000, Russia. RP Shockley, FW (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, POB 37012,MRC 165, Washington, DC 20013 USA. EM shockleyf@si.edu; alekseew0802@yahoo.com NR 40 TC 2 Z9 2 U1 0 U2 4 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 23 PY 2014 VL 3755 IS 4 BP 391 EP 400 PG 10 WC Zoology SC Zoology GA 294DX UT WOS:000330023700005 PM 24869828 ER PT J AU Agnarsson, I Cheng, RC Kuntner, M AF Agnarsson, Ingi Cheng, Ren-Chung Kuntner, Matjaz TI A Multi-Clade Test Supports the Intermediate Dispersal Model of Biogeography SO PLOS ONE LA English DT Article ID OCEANIC DISPERSAL; SPECIES-DIVERSITY; DIVERSIFICATION; COLONIZATION; SPECIATION; ISLANDS; DIFFERENTIATION; METAANALYSIS; ARCHIPELAGO; POPULATIONS AB Background: Biogeography models typically focus on explaining patterns through island properties, such as size, complexity, age, and isolation. Such models explain variation in the richness of island biotas. Properties of the organisms themselves, such as their size, age, and dispersal abilities, in turn may explain which organisms come to occupy, and diversify across island archipelagos. Here, we restate and test the intermediate dispersal model (IDM) predicting peak diversity in clades of relatively intermediate dispersers. Methodology: We test the model through a review of terrestrial and freshwater organisms in the western Indian Ocean examining the correlation among species richness and three potential explanatory variables: dispersal ability quantified as the number of estimated dispersal events, average body size for animals, and clade age. Conclusions: Our study supports the IDM with dispersal ability being the best predictor of regional diversity among the explored variables. We find a weaker relationship between diversity and clade age, but not body size. Principally, we find that richness strongly and positively correlates with dispersal ability in poor to good dispersers while a prior study found a strong decrease in richness with increased dispersal ability among excellent dispersers. Both studies therefore support the intermediate dispersal model, especially when considered together. We note that many additional variables not here considered are at play. For example, some taxa may lose dispersal ability subsequent to island colonization and some poor dispersers have reached high diversity through within island radiations. Nevertheless, our findings highlight the fundamental importance of dispersal ability in explaining patterns of biodiversity generation across islands. C1 [Agnarsson, Ingi] Univ Vermont, Dept Biol, Burlington, VT 05405 USA. [Agnarsson, Ingi; Kuntner, Matjaz] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Cheng, Ren-Chung; Kuntner, Matjaz] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Ljubljana, Slovenia. [Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Wuhan, Hubei, Peoples R China. RP Agnarsson, I (reprint author), Univ Vermont, Dept Biol, Burlington, VT 05405 USA. EM iagnarsson@gmail.com FU National Science Foundation [DEB-1314749, 1050253, DEB-0516038]; National Geographic Society [8655-09, GEFNE29-11]; Slovenian Research Agency [Z1-9799-0618-07]; European Community [MIRG-CT-2005 036536] FX Funding for this work came from the National Science Foundation (grant DEB-1314749 to IA and 1050253 to GB) and the National Geographic Society (grants 8655-09 and GEFNE29-11 to IA and MK). This is contribution number 10 resulting from the 2008 Indian Ocean expedition, funded by the Slovenian Research Agency (grant Z1-9799-0618-07 to IA), the National Science Foundation (grant DEB-0516038 to TB) and the European Community 6th Framework Programme (a Marie Curie International Reintegration Grant MIRG-CT-2005 036536 to MK). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 38 TC 10 Z9 10 U1 2 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 JAN 21 PY 2014 VL 9 IS 1 AR e86780 DI 10.1371/journal.pone.0086780 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 297GT UT WOS:000330244500285 PM 24466238 ER PT J AU Kintigh, KW Altschul, JH Beaudry, MC Drennan, RD Kinzig, AP Kohler, TA Limp, WF Maschner, HDG Michener, WK Pauketat, TR Peregrine, P Sabloff, JA Wilkinson, TJ Wright, HT Zeder, MA AF Kintigh, Keith W. Altschul, Jeffrey H. Beaudry, Mary C. Drennan, Robert D. Kinzig, Ann P. Kohler, Timothy A. Limp, W. Fredrick Maschner, Herbert D. G. Michener, William K. Pauketat, Timothy R. Peregrine, Peter Sabloff, Jeremy A. Wilkinson, Tony J. Wright, Henry T. Zeder, Melinda A. TI Grand challenges for archaeology SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Editorial Material C1 [Kintigh, Keith W.] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. [Altschul, Jeffrey H.] Stat Res Inc, Tucson, AZ 85751 USA. [Beaudry, Mary C.] Boston Univ, Dept Archaeol, Boston, MA 02215 USA. [Drennan, Robert D.] Univ Pittsburgh, Dept Anthropol, Ctr Comparat Archaeol, Pittsburgh, PA 15260 USA. [Kinzig, Ann P.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. [Kohler, Timothy A.] Washington State Univ, Dept Anthropol, Pullman, WA 99164 USA. [Kohler, Timothy A.; Peregrine, Peter; Sabloff, Jeremy A.; Wright, Henry T.] Santa Fe Inst, Santa Fe, NM 87501 USA. [Limp, W. Fredrick] Univ Arkansas, Dept Geosci, Fayetteville, AR 72701 USA. [Maschner, Herbert D. G.] Idaho State Univ, Idaho Museum Nat Hist, Pocatello, ID 83209 USA. [Michener, William K.] Univ New Mexico, Univ Lib, Albuquerque, NM 87131 USA. [Pauketat, Timothy R.] Univ Illinois, Dept Anthropol, Urbana, IL 61801 USA. [Peregrine, Peter] Lawrence Univ, Dept Anthropol, Appleton, WI 54911 USA. [Wilkinson, Tony J.] Univ Durham, Dept Archaeol, Durham DH1 3LE, England. [Wright, Henry T.] Univ Michigan, Museum Anthropol, Ann Arbor, MI 48109 USA. [Zeder, Melinda A.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Kintigh, KW (reprint author), Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. EM kintigh@asu.edu NR 2 TC 14 Z9 14 U1 0 U2 20 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 JAN 21 PY 2014 VL 111 IS 3 BP 879 EP 880 DI 10.1073/pnas.1324000111 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 292UQ UT WOS:000329928400016 PM 24449827 ER PT J AU Giacintucci, S Markevitch, M Venturi, T Clarke, TE Cassano, R Mazzotta, P AF Giacintucci, Simona Markevitch, Maxim Venturi, Tiziana Clarke, Tracy E. Cassano, Rossella Mazzotta, Pasquale TI NEW DETECTIONS OF RADIO MINIHALOS IN COOL CORES OF GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (MACSJ0159.8-0849, MACSJ0329.6-0211, A478, ZwCl3146, A1795); galaxies: clusters: intracluster medium; radio continuum: general; X-rays: galaxies: clusters ID GALACTIC NUCLEUS FEEDBACK; X-RAY; COLD FRONTS; FLOW CLUSTERS; MINI-HALOS; CHANDRA OBSERVATIONS; NONTHERMAL EMISSION; SCALING RELATIONS; MAGNETIC-FIELDS; PERSEUS CLUSTER AB Cool cores of some galaxy clusters exhibit faint radio "minihalos." Their origin is unclear, and their study has been limited by their small number. We undertook a systematic search for minihalos in a large sample of X-ray luminous clusters with high-quality radio data. In this article, we report four new minihalos (Lambda 478, ZwCl 3146, RXJ 1532.9+3021, and A 2204) and five candidates found in the reanalyzed archival Very Large Array observations. The radio luminosities of our minihalos and candidates are in the range of 10(23-25) W Hz(-1) at 1.4 GHz, which is consistent with these types of radio sources. Their sizes (40-160 kpc in radius) are somewhat smaller than those of previously known minihalos. We combine our new detections with previously known minihalos, obtaining a total sample of 21 objects, and briefly compare the cluster radio properties to the average X-ray temperature and the total masses estimated from Planck. We find that nearly all clusters hosting minihalos are hot and massive. Beyond that, there is no clear correlation between the minihalo radio power and cluster temperature or mass (in contrast with the giant radio halos found in cluster mergers, whose radio luminosity correlates with the cluster mass). Chandra X-ray images indicate gas sloshing in the cool cores of most of our clusters, with minihalos contained within the sloshing regions in many of them. This supports the hypothesis that radio-emitting electrons are reaccelerated by sloshing. Advection of relativistic electrons by the sloshing gas may also play a role in the formation of the less extended minihalos. C1 [Giacintucci, Simona] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Giacintucci, Simona; Markevitch, Maxim] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Markevitch, Maxim] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Venturi, Tiziana; Cassano, Rossella] INAF Ist Radioastron, I-40129 Bologna, Italy. [Clarke, Tracy E.] Naval Res Lab, Washington, DC 20375 USA. [Mazzotta, Pasquale] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Mazzotta, Pasquale] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Giacintucci, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM simona@astro.umd.edu RI Mazzotta, Pasquale/B-1225-2016; OI Mazzotta, Pasquale/0000-0002-5411-1748; Cassano, Rossella/0000-0003-4046-0637; Venturi, Tiziana/0000-0002-8476-6307 FU NASA through Einstein Postdoctoral Fellowship [PF0-110071]; Chandra X-ray Center (CXC); Naval Research Laboratory FX S.G. acknowledges the support of NASA through Einstein Postdoctoral Fellowship PF0-110071 awarded by the Chandra X-ray Center (CXC), which is operated by SAO. Basic research in radio astronomy at the Naval Research Laboratory is supported by 6.1 base funding. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research work has used TIFR GMRT Sky Survey (http://tgss.ncra.tifr.res.in) data products. The authors thank the anonymous referee, whose comments and suggestions improved the paper. NR 86 TC 19 Z9 19 U1 0 U2 0 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 JAN 20 PY 2014 VL 781 IS 1 AR 9 DI 10.1088/0004-637X/781/1/9 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286AE UT WOS:000329436100009 ER PT J AU Guzman, AE Garay, G Brooks, KJ Voronkov, MA AF Guzman, Andres E. Garay, Guido Brooks, Kate J. Voronkov, Maxim A. TI SEARCH FOR IONIZED JETS TOWARD HIGH-MASS YOUNG STELLAR OBJECTS (vol 753, pg 51, 2012) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Guzman, Andres E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Garay, Guido] Univ Chile, Dept Astron, Santiago, Chile. [Brooks, Kate J.; Voronkov, Maxim A.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. RP Guzman, AE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Garay, Guido/H-8840-2013; OI Garay, Guido/0000-0003-1649-7958; Guzman, Andres/0000-0003-0990-8990 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 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2014 VL 781 IS 1 AR 56 DI 10.1088/0004-637X/781/1/56 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286AE UT WOS:000329436100056 ER PT J AU Kraus, AL Ireland, MJ Cieza, LA Hinkley, S Dupuy, TJ Bowler, BP Liu, MC AF Kraus, Adam L. Ireland, Michael J. Cieza, Lucas A. Hinkley, Sasha Dupuy, Trent J. Bowler, Brendan P. Liu, Michael C. TI THREE WIDE PLANETARY-MASS COMPANIONS TO FW TAU, ROXs 12, AND ROXs 42B SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; planetary systems; planets and satellites: formation; planets and satellites: gaseous planets; stars: individual (FW Tau, ROXs 12, ROXs 42B); stars: pre-main sequence ID SUB-STELLAR COMPANION; STAR-FORMING REGION; CENTAURUS OB ASSOCIATION; CIRCUMSTELLAR DUST DISKS; DEUTERIUM-BURNING LIMIT; YOUNG BINARY-SYSTEM; VERY-LOW MASS; EDGE-ON DISK; BROWN DWARF; UPPER SCORPIUS AB We report the discovery of three planetary-mass companions (M = 6-20 M-Jup) in wide orbits (rho similar to 150-300 AU) around the young stars FW Tau (Taurus-Auriga), ROXs 12 (Ophiuchus), and ROXs 42B (Ophiuchus). All three wide planetary-mass companions (PMCs) were reported as candidate companions in previous binary survey programs, but then were neglected for > 10 yr. We therefore obtained followup observations that demonstrate that each candidate is comoving with its host star. Based on the absolute M-K' magnitudes, we infer masses (from hot-start evolutionary models) and projected separations of 10 +/- 4 M-Jup and 330 +/- 30 AU for FW Tau b, 16 +/- 4 M-Jup and 210 +/- 20 AU for ROXs 12, and 10 +/- 4 M-Jup and 140 +/- 10 AU for ROXs 42B b. We also present similar observations for 10 other candidates that show that they are unassociated field stars, as well as multicolor JHK'L' near-infrared photometry for our new PMCs and for five previously identified substellar or planetary-mass companions. The near-infrared photometry for our sample of eight known and new companions generally parallels the properties of free-floating, low-mass brown dwarfs in these star-forming regions. However, five of the seven objects with M < 30 M-Jup are redder in K' - L' than the distribution of young free-floating counterparts of similar J - K' color. We speculate that this distinction could indicate a structural difference in circumplanetary disks, perhaps tied to higher disk mass since at least two of the objects in our sample are known to be accreting more vigorously than typical free-floating counterparts. C1 [Kraus, Adam L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Kraus, Adam L.; Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ireland, Michael J.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia. [Ireland, Michael J.] Australian Astron Observ, Epping, NSW 1710, Australia. [Cieza, Lucas A.; Bowler, Brendan P.; Liu, Michael C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Cieza, Lucas A.] Univ Diego Portales, Fac Ingn, Santiago, Chile. [Hinkley, Sasha; Bowler, Brendan P.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. RP Kraus, AL (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. FU Clay Fellowship; NASA through Hubble Fellowship [51257.01]; STScI; NASA [NAS 5-26555]; Australian Research Council's Discovery program [DP1094977]; Macquarie University Research Development Grant; NASA through Hubble Fellowship; NASA through the Sagan Fellowship program; ALMA-CONICYT fund [31120009]; NSF [AST09-09222]; NASA Keck PI Data Award FX We thank the referee for providing a thorough and helpful critique of this paper. A. L. K. was supported in part by a Clay Fellowship and by NASA through Hubble Fellowship grant 51257.01 awarded by STScI, which is operated by AURA, Inc., for NASA, under contract NAS 5-26555. M.J.I. acknowledges support from the Australian Research Council's Discovery program (DP1094977) and a Macquarie University Research Development Grant. T. D. was supported by NASA through Hubble Fellowship grant 51271.01 awarded by STScI, which is operated by AURA, Inc., for NASA, under contract NAS 5-26555. S. H. and L. C. were supported by NASA through the Sagan Fellowship program, and L. C. was supported by the ALMA-CONICYT fund allocated to the project number 31120009. M. L. acknowledges support from NSF grant AST09-09222. Finally, this work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Some of the data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to NASA through the agency's scientific partnership with Caltech and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 103 TC 45 Z9 45 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2014 VL 781 IS 1 AR 20 DI 10.1088/0004-637X/781/1/20 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286AE UT WOS:000329436100020 ER PT J AU Kumar, HS Safi-Harb, S Slane, PO Gotthelf, EV AF Kumar, Harsha S. Safi-Harb, Samar Slane, Patrick O. Gotthelf, E. V. TI CHANDRA AND XMM-NEWTON STUDY OF THE SUPERNOVA REMNANT KES 73 HOSTING THE MAGNETAR 1E 1841-045 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (SNR Kes 73); ISM: supernova remnants; pulsars: individual (SNR Kes 73); X-rays: ISM ID X-RAY PULSAR; PHOTON IMAGING CAMERA; GALACTIC PLANE; EMISSION; DISTANCE; STARS; NUCLEOSYNTHESIS; PROGENITOR; EXPLOSION; EVOLUTION AB We present a Chandra and XMM-Newton study of the supernova remnant (SNR) Kes 73 hosting the anomalous X-ray pulsar 1E 1841-045. The Chandra image reveals clumpy structures across the remnant with enhanced emission along the western rim. The X-ray emission fills the radio shell and spatially correlates with the infrared image. The global X-ray spectrum is described by a two-component thermal model with a column density N-H = 2.6(-0.3)(+0.4) x 10(22)cm(-2) and a total luminosity of L-X = 3.3(-0.5)(+0.7) x 10(37) erg s(-1) (0.5-10 keV, at an assumed distance of 8.5 kpc). The soft component is characterized by a temperature kT(s) = 0.5(-0.2)(+0.1) keV, a high ionization timescale, and enhanced Si and S abundances, suggesting emission that is dominated by shocked ejecta. The hard component has a temperature kT(h) = 1.6(-0.7)(+0.8) keV, a relatively low ionization timescale, and mostly solar abundances suggesting emission that is dominated by interstellar/circumstellar shocked material. A spatially resolved spectroscopy study reveals no significant variations in the spectral properties. We infer an SNR age ranging between 750 yr and 2100 yr, an explosion energy of 3.0(-1.8)(+2.8) x 10(50) erg and a shock velocity of (1.2 +/- 0.3) x 10(3) km s(-1) (under the Sedov phase assumption). We also discuss the possible scenario for Kes 73 expanding into the late red-supergiant wind phase of its massive progenitor. Comparing the inferred metal abundances to core-collapse nucleosynthesis model yields, we estimate a progenitor mass greater than or similar to 20 M-circle dot, adding a candidate to the growing list of highly magnetized neutron stars proposed to be associated with very massive progenitors. C1 [Kumar, Harsha S.; Safi-Harb, Samar] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. [Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. RP Kumar, HS (reprint author), Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. EM harsha@physics.umanitoba.ca; samar@physics.umanitoba.ca; slane@cfa.harvard.edu; eric@astro.columbia.edu FU Natural Sciences and Engineering Research Council of Canada (NSERC); Canada Research Chairs (CRC) program; Canada Foundation for Innovation; Canadian Institute for Theoretical Astrophysics; Canadian Space Agency; NASA [NAS8-03060] FX We thank Ken'ichi Nomoto for helpful discussions on the nucleosynthesis yield models for core-collapse supernovae and the referee for useful comments that helped improved the paper. This research made use of NASA's Astrophysics Data System (ADS) and of NASA's HEASARC maintained at the Goddard Space Flight Center (GSFC). S.S.-H. acknowledges support by a Discovery Grant from the Natural Sciences and Engineering Research Council of Canada (NSERC), the Canada Research Chairs (CRC) program, the Canada Foundation for Innovation, the Canadian Institute for Theoretical Astrophysics, and the Canadian Space Agency. P.O.S. acknowledges support from NASA Contract NAS8-03060. NR 49 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2014 VL 781 IS 1 AR 41 DI 10.1088/0004-637X/781/1/41 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286AE UT WOS:000329436100041 ER PT J AU Laskar, T Berger, E Tanvir, N Zauderer, BA Margutti, R Levan, A Perley, D Fong, WF Wiersema, K Menten, K Hrudkova, M AF Laskar, Tanmoy Berger, Edo Tanvir, Nial Zauderer, B. Ashley Margutti, Raffaella Levan, Andrew Perley, Daniel Fong, Wen-fai Wiersema, Klaas Menten, Karl Hrudkova, Marie TI GRB 120521C AT z similar to 6 AND THE PROPERTIES OF HIGH-REDSHIFT gamma-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual (GRB 120521C, GRB 050904, GRB 090423) ID LIGHT CURVES; STAR-FORMATION; Z-SIMILAR-TO-6 QUASARS; AFTERGLOW OBSERVATIONS; PHOTOMETRIC REDSHIFT; INTERSTELLAR-MEDIUM; COSMIC EXPLOSION; DUST EXTINCTION; FIREBALL MODEL; EARLY UNIVERSE AB We present optical, near-infrared, and radio observations of the afterglow of GRB 120521C. By modeling the multi-wavelength data set, we derive a photometric redshift of z approximate to 6.0, which we confirm with a low signal-to-noise ratio spectrum of the afterglow. We find that a model with a constant-density environment provides a good fit to the afterglow data, with an inferred density of n less than or similar to 0.05 cm(-3). The radio observations reveal the presence of a jet break at t(jet) approximate to 7 d, corresponding to a jet opening angle of theta(jet) approximate to 3 degrees. The beaming-corrected gamma-ray and kinetic energies are E-gamma approximate to E-K approximate to 3 x 10(50) erg. We quantify the uncertainties in our results using a detailed Markov Chain Monte Carlo analysis, which allows us to uncover degeneracies between the physical parameters of the explosion. To compare GRB 120521C to other high-redshift bursts in a uniform manner we re-fit all available afterglow data for the two other bursts at z greater than or similar to 6 with radio detections (GRBs 050904 and 090423). We find a jet break at t(jet) approximate to 15 d for GRB 090423, in contrast to previous work. Based on these three events, we find that gamma-ray bursts (GRBs) at z greater than or similar to 6 appear to explode in constant-density environments, and exhibit a wide range of energies and densities that span the range inferred for lower redshift bursts. On the other hand, we find a hint for narrower jets in the z greater than or similar to 6 bursts, potentially indicating a larger true event rate at these redshifts. Overall, our results indicate that long GRBs share a common progenitor population at least to z similar to 8. C1 [Laskar, Tanmoy; Berger, Edo; Zauderer, B. Ashley; Margutti, Raffaella; Fong, Wen-fai] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tanvir, Nial; Wiersema, Klaas] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Levan, Andrew] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Perley, Daniel] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Menten, Karl] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Hrudkova, Marie] Isaac Newton Grp Telescopes, E-38700 Santa Cruz De La Palma, Canary Islands, Spain. RP Laskar, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Science Foundation [AST-1107973]; NRAO; STFC FX We thank the anonymous referee for detailed comments on the manuscript. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Radio data for GRB 120521C were obtained under VLA project codes 12A-394 and 12A-480. Some of the data presented here were obtained at the Gemini-North Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the NSF on behalf of the Gemini-North partnership. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica deCanarias. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We thank Ofer Yaron and S. R. Kulkarni for the Keck observations. The Berger GRB group at Harvard is supported by the National Science Foundation under grant AST-1107973. T. L. acknowledges support by NRAO. K. W. acknowledges support by STFC. NR 100 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2014 VL 781 IS 1 AR 1 DI 10.1088/0004-637X/781/1/1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286AE UT WOS:000329436100001 ER PT J AU Levan, AJ Tanvir, NR Starling, RLC Wiersema, K Page, KL Perley, DA Schulze, S Wynn, GA Chornock, R Hjorth, J Cenko, SB Fruchter, AS O'Brien, PT Brown, GC Tunnicliffe, RL Malesani, D Jakobsson, P Watson, D Berger, E Bersier, D Cobb, BE Covino, S Cucchiara, A Postigo, AD Fox, DB Gal-Yam, A Goldoni, P Gorosabel, J Kaper, L Kruhler, T Karjalainen, R Osborne, JP Pian, E Sanchez-Ramirez, R Schmidt, B Skillen, I Tagliaferri, G Thone, C Vaduvescu, O Wijers, RAMJ Zauderer, BA AF Levan, A. J. Tanvir, N. R. Starling, R. L. C. Wiersema, K. Page, K. L. Perley, D. A. Schulze, S. Wynn, G. A. Chornock, R. Hjorth, J. Cenko, S. B. Fruchter, A. S. O'Brien, P. T. Brown, G. C. Tunnicliffe, R. L. Malesani, D. Jakobsson, P. Watson, D. Berger, E. Bersier, D. Cobb, B. E. Covino, S. Cucchiara, A. de Ugarte Postigo, A. Fox, D. B. Gal-Yam, A. Goldoni, P. Gorosabel, J. Kaper, L. Kruehler, T. Karjalainen, R. Osborne, J. P. Pian, E. Sanchez-Ramirez, R. Schmidt, B. Skillen, I. Tagliaferri, G. Thoene, C. Vaduvescu, O. Wijers, R. A. M. J. Zauderer, B. A. TI A NEW POPULATION OF ULTRA-LONG DURATION GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: distances and redshifts; gamma-ray burst: general; gamma-ray burst: individual (GRB 101225A, GRB 111209A, GRB 121027A) ID HUBBLE-SPACE-TELESCOPE; MASSIVE BLACK-HOLE; CORE-COLLAPSE SUPERNOVAE; AFTERGLOW LIGHT CURVES; EARLY X-RAY; HOST GALAXY; TIDAL DISRUPTION; STAR-FORMATION; COMPREHENSIVE ANALYSIS; SPECTRAL EVOLUTION AB We present comprehensive multiwavelength observations of three gamma-ray bursts (GRBs) with durations of several thousand seconds. We demonstrate that these events are extragalactic transients; in particular, we resolve the long-standing conundrum of the distance of GRB 101225A (the "Christmas-day burst"), finding it to have a redshift z = 0.847 and showing that two apparently similar events (GRB 111209A and GRB 121027A) lie at z = 0.677 and z = 1.773, respectively. The systems show extremely unusual X-ray and optical light curves, very different from classical GRBs, with long-lasting, highly variable X-ray emission and optical light curves that exhibit little correlation with the behavior seen in the X-ray. Their host galaxies are faint, compact, and highly star-forming dwarf galaxies, typical of "blue compact galaxies." We propose that these bursts are the prototypes of a hitherto largely unrecognized population of ultra-long GRBs, which while observationally difficult to detect may be astrophysically relatively common. The long durations may naturally be explained by the engine-driven explosions of stars of much larger radii than normally considered for GRB progenitors, which are thought to have compact Wolf-Rayet progenitor stars. However, we cannot unambiguously identify supernova signatures within their light curves or spectra. We also consider the alternative possibility that they arise from the tidal disruption of stars by massive black holes and conclude that the associated timescales are only consistent with the disruption of compact stars (e. g., white dwarfs) by black holes of relatively low mass (<10(5) M-circle dot). C1 [Levan, A. J.; Brown, G. C.; Tunnicliffe, R. L.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Tanvir, N. R.; Starling, R. L. C.; Wiersema, K.; Page, K. L.; Wynn, G. A.; O'Brien, P. T.; Osborne, J. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Perley, D. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Schulze, S.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Chornock, R.; Malesani, D.; Watson, D.; Berger, E.; de Ugarte Postigo, A.; Kruehler, T.; Zauderer, B. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hjorth, J.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Cenko, S. B.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fruchter, A. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Jakobsson, P.] Univ Iceland, Ctr Astrophys & Cosmol, Inst Sci, IS-107 Reykjavik, Iceland. [Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Cobb, B. E.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Covino, S.; Tagliaferri, G.] Osserv Astron Brera, INAF, I-23807 Merate, Italy. [Cucchiara, A.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [de Ugarte Postigo, A.; Gorosabel, J.; Sanchez-Ramirez, R.; Thoene, C.] Inst Astrofis Andalucia IAA CSIC, E-18008 Granada, Spain. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Gal-Yam, A.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, Fac Phys, IL-76100 Rehovot, Israel. [Goldoni, P.] Univ Paris Diderot, APC, CNRS IN2P3, CEA IRFU,Observ Paris,Sorbonne Paris Cit, F-75205 Paris 13, France. [Gorosabel, J.] Univ Pais Vasco UPV EHU, Unidad Asociada Grp Ciencia Planetarias UPV EHU I, Dept Fis Aplicada 1, ETS Ingn, E-48013 Bilbao, Spain. [Gorosabel, J.] Basque Fdn Sci, Ikerbasque, E-48008 Bilbao, Spain. [Kaper, L.; Wijers, R. A. M. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Karjalainen, R.; Skillen, I.; Vaduvescu, O.] Isaac Newton Grp Telescopes, E-38700 Santa Cruz De Palma, Spain. [Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Pian, E.] INAF Trieste Astron Observ, I-34143 Trieste, Italy. [Schmidt, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. RP Levan, AJ (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM a.j.levan@warwick.ac.uk RI Hjorth, Jens/M-5787-2014; Watson, Darach/E-4521-2015; Jakobsson, Pall/L-9950-2015; OI Tagliaferri, Gianpiero/0000-0003-0121-0723; Pian, Elena/0000-0001-8646-4858; Sanchez-Ramirez, Ruben/0000-0002-7158-5099; Kruehler, Thomas/0000-0002-8682-2384; Hjorth, Jens/0000-0002-4571-2306; Watson, Darach/0000-0002-4465-8264; Jakobsson, Pall/0000-0002-9404-5650; Wijers, Ralph/0000-0002-3101-1808; Thone, Christina/0000-0002-7978-7648; Schmidt, Brian/0000-0001-6589-1287; Schulze, Steve/0000-0001-6797-1889; de Ugarte Postigo, Antonio/0000-0001-7717-5085; Covino, Stefano/0000-0001-9078-5507 FU Science and Technology Facilities Council (STFC) [ST/I001719/1]; Leverhulme Trust; STFC [ST/H001972/1]; Royal Society Dorothy Hodgkin Fellowship; DNRF; ESO Telescopes at the La Silla Paranal Observatory [288.D-5027]; NASA through a grant from the Space Telescope Science Institute [11734, 12438]; NASA [NAS 5-26555]; NASA through Hubble Fellowship [HST-HF-51296.01-A]; Space Telescope Science Institute (STScI); National Science Foundation (United States); 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) [GN-2010B-Q-7, GN-2011A-Q-4, GS2011B-Q-7, GN-2011B-Q-34, GS-2012A-Q-25]; Iniciativa Cientifica Milenio grant [P10-064-F]; Basal-CATA [PFB-06/2007]; ERC through advanced investigator grant [247295]; Gran Telescopio Canarias (GTC) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias, La Palma under programme [GTC43-11B]; European Commission under the Marie Curie Career Integration Grant programme [FP7-PEOPLE-2012-CIG 322307]; ASI [I/004/11/0]; Gary & Cynthia Bengier fund; Richard and Rhoda Goldman Fund; Christopher R. Redlich Fund; NASA/Swift [NNX10AI21G, NNX12AD73G]; TABASGO Foundation; NSF [AST-1211916]; UK Space Agency; National Science Foundation [AST-1107973]; NASA/Swift AO7 grant [NNX12AD69G]; [AYA2010-21887-C04-01]; [AYA2011-24780/ESP] FX We thank D. A. Kann and the GROND team for sharing their photometric calibration and Jamie Kennea for providing information on the Swift slew strategy. A.J.L. acknowledges support from the Science and Technology Facilities Council (STFC, under grant ID ST/I001719/1) and is grateful to the Leverhulme Trust for a Philip Leverhulme Prize award. N.R.T., K. W., and P.T.O. thank STFC for support (grant ID ST/H001972/1). R. L. C. S. is supported by a Royal Society Dorothy Hodgkin Fellowship. The Dark Cosmology Centre is supported by the DNRF. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 288.D-5027. Support for programs 11734, 12438, and 12786 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Support for D. P. is provided by NASA through Hubble Fellowship grant HST-HF-51296.01-A awarded by the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., for NASA, under contract NAS 5-26555. 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). These observations were obtained as part of programme IDs GN-2010B-Q-7, GN-2011A-Q-4, GS2011B-Q-7, GN-2011B-Q-34, and GS-2012A-Q-25. This work was made possible by contributions from Iniciativa Cientifica Milenio grant P10-064-F (Millennium Center for Supernova Science), with input from "Fondo de Innovacion para la Competitividad, del Ministerio de Economia, Fomento y Turismo de Chile," and Basal-CATA (PFB-06/2007). R.A.M.J.W. is supported by the ERC through advanced investigator grant no. 247295. Partly based on observations made with the Gran Telescopio Canarias (GTC) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias, La Palma under programme GTC43-11B, PI: C. C. Thone. A. dUP acknowledges support by the European Commission under the Marie Curie Career Integration Grant programme (FP7-PEOPLE-2012-CIG 322307). C. C. T., J.G., and R. S. R. acknowledge support from AYA2010-21887-C04-01 (Estallidos) and AYA2011-24780/ESP. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. S. C. and G. T. acknowledge support from ASI grant I/004/11/0. S. B. C. acknowledges generous financial assistance from Gary & Cynthia Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund, NASA/Swift grants NNX10AI21G and NNX12AD73G, the TABASGO Foundation, and NSF grant AST-1211916. J.P.O. acknowledges support from the UK Space Agency. E. B. acknowledges support from the National Science Foundation under Grant AST-1107973 and from NASA/Swift AO7 grant NNX12AD69G. NR 156 TC 72 Z9 73 U1 2 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 JAN 20 PY 2014 VL 781 IS 1 AR 13 DI 10.1088/0004-637X/781/1/13 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286AE UT WOS:000329436100013 ER PT J AU Meisner, AM Finkbeiner, DP AF Meisner, Aaron M. Finkbeiner, Douglas P. TI A FULL-SKY, HIGH-RESOLUTION ATLAS OF GALACTIC 12 mu m DUST EMISSION WITH WISE SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared: ISM; ISM: structure ID INFRARED-SURVEY-EXPLORER; MISSION; PERFORMANCE; GALAXIES; IRTS AB We describe our custom processing of the entire Wide-field Infrared Survey Explorer (WISE) 12 mu m imaging data set, and present a high-resolution, full-sky map of diffuse Galactic dust emission that is free of compact sources and other contaminating artifacts. The principal distinctions between our resulting co-added images and the WISE Atlas stacks are our removal of compact sources, including their associated electronic and optical artifacts, and our preservation of spatial modes larger than 1 degrees.5. We provide access to the resulting full-sky map via a set of 430 12 degrees.5 x 12 degrees.5 mosaics. These stacks have been smoothed to 15 '' resolution and are accompanied by corresponding coverage maps, artifact images, and bit-masks for point sources, resolved compact sources, and other defects. When combined appropriately with other mid-infrared and far-infrared data sets, we expect our WISE 12 mu m co-adds to form the basis for a full-sky dust extinction map with angular resolution several times better than Schlegel et al. C1 [Meisner, Aaron M.; Finkbeiner, Douglas P.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Meisner, Aaron M.; Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Meisner, AM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ameisner@fas.harvard.edu; dfinkbeiner@cfa.harvard.edu OI Meisner, Aaron/0000-0002-1125-7384 FU NASA [NNX12AE08G]; DoD, Air Force Office of Scientific Research, National Defense Science and Engineering Graduate (NDSEG) Fellowship [32 CFR 168a]; National Aeronautics and Space Administration; Planetary Science Division of the National Aeronautics and Space Administration; National Science Foundation FX We acknowledge support of NASA grant NNX12AE08G for this research. This research was conducted with Government support under and awarded by DoD, Air Force Office of Scientific Research, National Defense Science and Engineering Graduate (NDSEG) Fellowship, 32 CFR 168a. This research made use of the NASA Astrophysics Data System (ADS) and the IDL Astronomy User's Library at Goddard.5; This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 20 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2014 VL 781 IS 1 AR 5 DI 10.1088/0004-637X/781/1/5 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286AE UT WOS:000329436100005 ER PT J AU Mommert, M Hora, JL Harris, AW Reach, WT Emery, JP Thomas, CA Mueller, M Cruikshank, DP Trilling, DE Delbo, M Smith, HA AF Mommert, Michael Hora, Joseph L. Harris, Alan W. Reach, William T. Emery, Joshua P. Thomas, Cristina A. Mueller, Michael Cruikshank, Dale P. Trilling, David E. Delbo, Marco Smith, Howard A. TI THE DISCOVERY OF COMETARY ACTIVITY IN NEAR-EARTH ASTEROID (3552) DON QUIXOTE SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: general; infrared: planetary systems; minor planets, asteroids: individual (3552 Don Quixote) ID SPITZER-SPACE-TELESCOPE; JUPITER-FAMILY COMETS; TAGISH LAKE METEORITE; SPECTROSCOPIC SURVEY; OBJECT SURVEY; BELT; SPECTROGRAPH; CHONDRITE; DUST; NUCLEUS AB The near-Earth object (NEO) population, which mainly consists of fragments from collisions between asteroids in the main asteroid belt, is thought to include contributions from short-period comets as well. One of the most promising NEO candidates for a cometary origin is near-Earth asteroid (3552) Don Quixote, which has never been reported to show activity. Here we present the discovery of cometary activity in Don Quixote based on thermal-infrared observations made with the Spitzer Space Telescope in its 3.6 and 4.5 mu m bands. Our observations clearly show the presence of a coma and a tail in the 4.5 mu m but not in the 3.6 mu m band, which is consistent with molecular band emission from CO2. Thermal modeling of the combined photometric data on Don Quixote reveals a diameter of 18.4(-0.4)(+0.3) km and an albedo of 0.03(-0.01)(+0.02), which confirms Don Quixote to be the third-largest known NEO. We derive an upper limit on the dust production rate of 1.9 kg s(-1) and derive a CO2 gas production rate of (1.1 +/- 0.1) x 10(26) molecules s(-1). Spitzer Infrared Spectrograph spectroscopic observations indicate the presence of fine-grained silicates, perhaps pyroxene rich, on the surface of Don Quixote. Our discovery suggests that CO2 can be present in near-Earth space over a long time. The presence of CO2 might also explain that Don Quixote's cometary nature remained hidden for nearly three decades. C1 [Mommert, Michael; Harris, Alan W.] German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany. [Mommert, Michael; Trilling, David E.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Hora, Joseph L.; Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reach, William T.] NASA, Ames Res Ctr, Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Emery, Joshua P.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Thomas, Cristina A.] NASA, Goddard Space Flight Ctr, NASA Postdoctoral Program, Greenbelt, MD 20771 USA. [Mueller, Michael] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Cruikshank, Dale P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Delbo, Marco] UNS CNRS Observ Cote Azur, F-06304 Nice 4, France. RP Mommert, M (reprint author), German Aerosp Ctr DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany. OI Hora, Joseph/0000-0002-5599-4650; Mueller, Michael/0000-0003-3217-5385; Reach, William/0000-0001-8362-4094 FU DFG [SPP 1385]; NASA [1367413]; University of California, Los Angeles; Jet Propulsion Laboratory/California Institute of Technology; National Aeronautics and Space Administration FX M.M. acknowledges support by the DFG SPP 1385. We thank an anonymous referee for a number of useful suggestions. 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 award 1367413 issued by JPL/Caltech. 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 64 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2014 VL 781 IS 1 AR 25 DI 10.1088/0004-637X/781/1/25 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286AE UT WOS:000329436100025 ER PT J AU Montet, BT Crepp, JR Johnson, JA Howard, AW Marcy, GW AF Montet, Benjamin T. Crepp, Justin R. Johnson, John Asher Howard, Andrew W. Marcy, Geoffrey W. TI THE TRENDS HIGH-CONTRAST IMAGING SURVEY. IV. THE OCCURRENCE RATE OF GIANT PLANETS AROUND M DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: observational; planets and satellites: detection; planets and satellites: fundamental parameters; techniques: high angular resolution; techniques: radial velocities ID LOW-MASS STARS; SOLAR-TYPE STARS; PHOTOMETRIC STANDARD STARS; CARNEGIE EXOPLANET SURVEY; K-CHROMOSPHERIC EMISSION; ADAPTIVE OPTICS SURVEY; SUN-LIKE STARS; M-CIRCLE-PLUS; CA-II H; BROWN DWARF AB Doppler-based planet surveys have discovered numerous giant planets but are incomplete beyond several AU. At larger star-planet separations, direct planet detection through high-contrast imaging has proven successful, but this technique is sensitive only to young planets and characterization relies upon theoretical evolution models. Here we demonstrate that radial velocity measurements and high-contrast imaging can be combined to overcome these issues. The presence of widely separated companions can be deduced by identifying an acceleration (long-term trend) in the radial velocity of a star. By obtaining high spatial resolution follow-up imaging observations, we rule out scenarios in which such accelerations are caused by stellar binary companions with high statistical confidence. We report results from an analysis of Doppler measurements of a sample of 111 M-dwarf stars with a median of 29 radial velocity observations over a median time baseline of 11.8 yr. By targeting stars that exhibit a radial velocity acceleration ("trend") with adaptive optics imaging, we determine that 6.5% +/- 3.0% of M-dwarf stars host one or more massive companions with 1 < m/M-J < 13 and 0 < a < 20 AU. These results are lower than analyses of the planet occurrence rate around higher-mass stars. We find the giant planet occurrence rate is described by a double power law in stellar mass M and metallicity F = [Fe/H] such that f(M, F) = 0.039(-0.028)(+0.056)M(0.8+1.1-0.9)10((3.8 +/- 1.2)F). Our results are consistent with gravitational microlensing measurements of the planet occurrence rate; this study represents the first model-independent comparison with microlensing observations. C1 [Montet, Benjamin T.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46656 USA. [Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Montet, BT (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, 1200 East Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. EM btm@astro.caltech.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Montet, Benjamin/0000-0001-7516-8308 FU W.M. Keck Foundation; National Aeronautics and Space Administration; National Science Foundation; National Science Foundation [DGE1144469]; NASA [NNX13AB03G]; David and Lucile Packard Foundation; Alfred P. Sloan Foundation FX Most of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We thank the staff of the Palomar Observatory for their help in maximizing the efficiency and quality of the 200 '' Hale Telescope. 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. We made use of the SIMBAD database operated at CDS, Strasbourg, France, and NASA's Astrophysics Data System Bibliographic Services. We thank Jon Swift for collecting NIRC2 observations of HIP 57050. We also thank Brendan Bowler for helpful comments on an early version of this manuscript. B. T. M. is supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE1144469. The TRENDS high-contrast imaging program is supported by NASA Origins grant NNX13AB03G. J.A.J. is supported by generous grants from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation. B. T. M. would also like to thank the Statistical and Applied Mathematical Sciences Institute; conversations at the 2013 June Modern Statistical and Computational Methods for Analysis of Kepler Data workshop at SAMSI improved the final version of this manuscript. NR 145 TC 42 Z9 42 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 JAN 20 PY 2014 VL 781 IS 1 AR 28 DI 10.1088/0004-637X/781/1/28 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286AE UT WOS:000329436100028 ER PT J AU Myers, PC AF Myers, Philip C. TI PROTOSTAR MASS FUNCTIONS IN YOUNG CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: formation; stars: luminosity function, mass function; stars: protostars ID EMBEDDED STELLAR CLUSTERS; HIGH ANGULAR RESOLUTION; MOLECULAR CLOUD CORES; STAR-FORMATION RATES; DENSE CORES; INITIAL CONDITIONS; DARK CLOUDS; LUMINOSITY FUNCTIONS; INTERNAL STRUCTURE; NH3 OBSERVATIONS AB In an improved model of protostar mass functions (PMFs), protostars gain mass from isothermal cores in turbulent clumps. Their mass accretion rate is similar to Shu accretion at low mass and to reduced Bondi accretion at high mass. Accretion durations follow a simple expression in which higher-mass protostars accrete for longer times. These times are set by ejections, stellar feedback, and gravitational competition, which terminate accretion and reduce its efficiency. The mass scale is the mass of a critically stable isothermal core. In steady state, the PMF approaches a power law at high mass because of competition between clump accretion and accretion stopping. The power law exponent is the ratio of the timescales of accretion and accretion stopping. The protostar luminosity function (PLF) peaks near 1 L-circle dot because of inefficient accretion of core gas. Models fit observed PLFs in four large embedded clusters. These indicate that their underlying PMFs may be top-heavy compared with the initial mass function, depending on the protostar radius model. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Myers, PC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pmyers@cfa.harvard.edu FU National Science Foundation [PHY-1066293]; hospitality of the Aspen Center for Physics FX Helpful discussions with Fred Adams, John Bally, Paola Caselli, Rob Gutermuth, Stella Offner, Norm Murray, Ralph Pudritz, Jonathan Tan, and Hans Zinnecker are gratefully acknowledged. Jonathan Foster kindly provided unpublished data associated with Foster et al. (2009). An anonymous referee made numerous suggestions that improved and clarified the paper. Terry Marshall and Irwin Shapiro provided support and encouragement. This material is based upon work supported in part by the National Science Foundation under grant No. PHY-1066293 and the hospitality of the Aspen Center for Physics. NR 105 TC 6 Z9 6 U1 0 U2 0 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 JAN 20 PY 2014 VL 781 IS 1 AR 33 DI 10.1088/0004-637X/781/1/33 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286AE UT WOS:000329436100033 ER PT J AU Newman, SF Buschkamp, P Genzel, R Schreiber, NMF Kurk, J Sternberg, A Gnat, O Rosario, D Mancini, C Lilly, SJ Renzini, A Burkert, A Carollo, CM Cresci, G Davies, R Eisenhauer, F Genel, S Griffin, KS Hicks, EKS Lutz, D Naab, T Peng, YJ Tacconi, LJ Wuyts, S Zamorani, G Vergani, D Weiner, BJ AF Newman, Sarah F. Buschkamp, Peter Genzel, Reinhard Schreiber, Natascha M. Foerster Kurk, Jaron Sternberg, Amiel Gnat, Orly Rosario, David Mancini, Chiara Lilly, Simon J. Renzini, Alvio Burkert, Andreas Carollo, C. Marcella Cresci, Giovanni Davies, Ric Eisenhauer, Frank Genel, Shy Griffin, Kristen Shapiro Hicks, Erin K. S. Lutz, Dieter Naab, Thorsten Peng, Yingjie Tacconi, Linda J. Wuyts, Stijn Zamorani, Gianni Vergani, Daniela Weiner, Benjamin J. TI NEBULAR EXCITATION IN z similar to 2 STAR-FORMING GALAXIES FROM THE SINS AND LUCI SURVEYS: THE INFLUENCE OF SHOCKS AND ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; infrared: galaxies ID INTEGRAL FIELD SPECTROSCOPY; MASS-METALLICITY RELATION; ULTRA DEEP FIELD; H-II REGIONS; HIGH-REDSHIFT; STELLAR POPULATIONS; HOST GALAXIES; ADAPTIVE OPTICS; DISK GALAXY; PHYSICAL CONDITIONS AB Based on high-resolution, spatially resolved data of 10 z similar to 2 star-forming galaxies from the SINS/zC-SINF survey and LUCI data for 12 additional galaxies, we probe the excitation properties of high-z galaxies and the impact of active galactic nuclei (AGNs), shocks, and photoionization. We explore how these spatially resolved line ratios can inform our interpretation of integrated emission line ratios obtained at high redshift. Many of our galaxies fall in the "composite" region of the z similar to 0 [N II]/H alpha versus [O III]/H beta diagnostic (BPT) diagram, between star-forming galaxies and those with AGNs. Based on our resolved measurements, we find that some of these galaxies likely host an AGN, while others appear to be affected by the presence of shocks possibly caused by an outflow or from an enhanced ionization parameter as compared with H II regions in normal, local star-forming galaxies. We find that the Mass-Excitation (MEx) diagnostic, which separates purely star-forming and AGN hosting local galaxies in the [O III]/H beta versus stellar mass plane, does not properly separate z similar to 2 galaxies classified according to the BPT diagram. However, if we shift the galaxies based on the offset between the local and z similar to 2 mass-metallicity relation (i.e., to the mass they would have at z similar to 0 with the same metallicity), we find better agreement between the MEx and BPT diagnostics. Finally, we find that metallicity calibrations based on [N II]/H alpha are more biased by shocks and AGNs at high-z than the [OIII]/H beta/[N II]/H alpha calibration. C1 [Newman, Sarah F.; Genzel, Reinhard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Buschkamp, Peter; Genzel, Reinhard; Schreiber, Natascha M. Foerster; Kurk, Jaron; Rosario, David; Davies, Ric; Eisenhauer, Frank; Lutz, Dieter; Tacconi, Linda J.; Wuyts, Stijn] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. [Genzel, Reinhard] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Sternberg, Amiel] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Gnat, Orly] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Mancini, Chiara; Renzini, Alvio] Osserv Astron Padova, I-35122 Padua, Italy. [Lilly, Simon J.; Carollo, C. Marcella; Peng, Yingjie] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. [Burkert, Andreas] Ludwig Maximilians Univ USM, Univ Sternwarte, D-81679 Munich, Germany. [Cresci, Giovanni] Ist Nazl Astrofis Osservatorio Bologna, I-40127 Bologna, Italy. [Genel, Shy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Griffin, Kristen Shapiro] Northrop Grumman Aerosp Syst, Space Sci Res Grp, Redondo Beach, CA 90278 USA. [Hicks, Erin K. S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Naab, Thorsten] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Zamorani, Gianni] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Vergani, Daniela] INAF Ist Astrofis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy. [Weiner, Benjamin J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Newman, SF (reprint author), Univ Calif Berkeley, Dept Astron, Campbell Hall, Berkeley, CA 94720 USA. EM sfnewman@berkeley.edu OI Vergani, Daniela/0000-0003-0898-2216; Cresci, Giovanni/0000-0002-5281-1417 FU NSF grfp grant; ASI grant; INAF grant; NASA through a grant from STScI [AR12655, NAS5-2655] FX We thank the ESO staff, especially those at Paranal Observatory, for their ongoing support during the many past and continuing observing runs over which the SINS project is being carried out, as well as the LBTO staff. We also acknowledge the SIN-FONI, PARSEC, and LUCI teams, whose devoted work on the instruments and lasers paved the way for the success of the SINS and LUCI observations. In addition, we thank Jonathan Trump for supplying the errors for his BPT data. S.F.N. is supported by an NSF grfp grant. C. M., A. R., and G.Z. acknowledge partial support by the ASI grant "COFIS-AnalisiDati" and by the INAF grant "PRIN-2008" and "PRIN-2010." O.G. was supported by program number AR12655 provided by NASA through a grant from STScI, under NASA contract NAS5-2655. NR 114 TC 40 Z9 40 U1 2 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 JAN 20 PY 2014 VL 781 IS 1 AR 21 DI 10.1088/0004-637X/781/1/21 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286AE UT WOS:000329436100021 ER PT J AU Rodler, F Lopez-Morales, M AF Rodler, Florian Lopez-Morales, Mercedes TI FEASIBILITY STUDIES FOR THE DETECTION OF O-2 IN AN EARTH-LIKE EXOPLANET SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; atmospheric effects; planetary systems; stars: late-type; techniques: spectroscopic ID HOT JUPITER; SYNTHETIC SPECTRA; ATMOSPHERE; PLANET; TRANSIT; SEARCH; LIFE; UVES AB We present the results of simulations on the detectability of O-2 in the atmosphere of Earth twins around nearby low mass stars using high resolution transmission spectroscopy. We explore such detectability with each of the three upcoming Extremely Large Telescopes (ELTs), i.e., GMT, TMT, and E-ELT, and high resolution spectrographs, assuming such instruments will be available in all ELTs. With these simulations we extend previous studies by taking into account atmospheric refraction in the transmission spectrum of the exo-Earth and observational white and red noise contributions. Our studies reveal that the number of transits necessary to detect O-2 in the atmosphere of an Earth twin around an M dwarf is by far higher than the number of transits estimated by Snellen et al. In addition, our simulations show that, when accounting for typical noise levels associated with observations in the optical and near-infrared, the O-2 A band at 760 nm is more favorable for detecting the exoplanetary signal than the O-2 band at 1268 nm for all the spectral types, except M9V. We conclude that, unless unpredicted instrumental limitations arise, the implementation of pre-slit optics such as image slicers appears to be key to significantly improving the yield of this particular science case. However, even in the most optimistic cases, we conclude that the detection of O-2 in the atmosphere of an Earth twin will only be feasible with the ELTs if the planet is orbiting a bright close by (d <= 8 pc) M dwarf with a spectral type later than M3. C1 [Rodler, Florian; Lopez-Morales, Mercedes] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rodler, Florian] Inst Ciencies Espai CSIC IEEC, Fac Ciencies, E-08193 Barcelona, Spain. RP Rodler, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU Spanish Ministry of Economy and Competitiveness (MINECO); "Fondo Europeo de Desarrollo Regional" (FEDER) [AYA2012-39612-C03-01] FX We are grateful to the constructive comments of the anonymous referee, who helped us to improve the manuscript. F. R. acknowledges financial support from the Spanish Ministry of Economy and Competitiveness (MINECO) and the "Fondo Europeo de Desarrollo Regional" (FEDER) through grant AYA2012-39612-C03-01. This research has made use of NASA's Astrophysics Data System Bibliographic Services. NR 33 TC 23 Z9 23 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2014 VL 781 IS 1 AR 54 DI 10.1088/0004-637X/781/1/54 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286AE UT WOS:000329436100054 ER PT J AU Wang, JF Nardini, E Fabbiano, G Karovska, M Elvis, M Pellegrini, S Max, C Risaliti, G Vivian, U Zezas, A AF Wang, Junfeng Nardini, Emanuele Fabbiano, Giuseppina Karovska, Margarita Elvis, Martin Pellegrini, Silvia Max, Claire Risaliti, Guido Vivian, U. Zezas, Andreas TI FAST AND FURIOUS: SHOCK HEATED GAS AS THE ORIGIN OF SPATIALLY RESOLVED HARD X-RAY EMISSION IN THE CENTRAL 5 kpc OF THE GALAXY MERGER NGC 6240 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 6240); galaxies: interactions; galaxies: starburst; X-rays: galaxies ID LUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEUS; HUBBLE-SPACE-TELESCOPE; KECK ADAPTIVE OPTICS; INTERSTELLAR-MEDIUM; STARBURST GALAXIES; LINE EMISSION; MOLECULAR GAS; SUPERNOVA-REMNANTS; STAR-FORMATION AB We have obtained a deep, subarcsecond resolution X-ray image of the nuclear region of the luminous galaxy merger NGC 6240 with Chandra, which resolves the X-ray emission from the pair of active nuclei and the diffuse hot gas in great detail. We detect extended hard X-ray emission from kT similar to 6 keV (similar to 70 MK) hot gas over a spatial scale of 5 kpc, indicating the presence of fast shocks with a velocity of similar to 2200 km s(-1). For the first time, we obtain the spatial distribution of this highly ionized gas emitting Fe xxv, which shows a remarkable correspondence to the large-scale morphology of H-2(1-0) S(1) line emission and H alpha filaments. Propagation of fast shocks originating in the starburst-driven wind into the ambient dense gas can account for this morphological correspondence. With an observed L0.5-8keV = 5.3 x 10(41) erg s(-1), the diffuse hard X-ray emission is similar to 100 times more luminous than that observed in the classic starburst galaxy M82. Assuming a filling factor of 1% for the 70 MK temperature gas, we estimate its total mass (M-hot = 1.8x10(8) M-circle dot) and thermal energy (E-th = 6.5x10(57) erg). The total iron mass in the highly ionized plasma is M-Fe = 4.6 x 10(5) M-circle dot. Both the energetics and the iron mass in the hot gas are consistent with the expected injection from the supernovae explosion during the starburst that is commensurate with its high star formation rate. No evidence for fluorescent Fe I emission is found in the CO filament connecting the two nuclei. C1 [Wang, Junfeng; Nardini, Emanuele; Fabbiano, Giuseppina; Karovska, Margarita; Elvis, Martin; Risaliti, Guido; Zezas, Andreas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pellegrini, Silvia] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Max, Claire] Univ Calif Santa Cruz, Ctr Adapt Opt, Santa Cruz, CA 95064 USA. [Risaliti, Guido] INAF Arcetri Observ, I-50125 Florence, Italy. [Vivian, U.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Zezas, Andreas] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. RP Wang, JF (reprint author), Northwestern Univ, CIERA, 2131 Tech Dr, Evanston, IL 60208 USA. EM jfwang@northwestern.edu RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Risaliti, Guido/0000-0002-3556-977X FU NASA [GO1-12123X, NAS8-03060]; CXC; Northwestern University CIERA Fellowship; National Science Foundation [1066293]; The W. M. Keck Observatory; Keck II AO system FX We acknowledge the anonymous referee for the careful reading and constructive suggestions. This work is supported by NASA grant GO1-12123X (PI: Fabbiano). We acknowledge support from the CXC, which is operated by the Smithsonian Astrophysical Observatory (SAO) for and on behalf of NASA under Contract NAS8-03060. J.W. acknowledges support from the Northwestern University CIERA Fellowship. This material is based upon work supported in part by the National Science Foundation grant No. 1066293 and the hospitality of the Aspen Center for Physics. M. K. is a member of CXC. Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA. The W. M. Keck Observatory and the Keck II AO system were made possible by the generous financial support of the W. M. Keck Foundation. This research has made use of data obtained from the Chandra Data Archive and software provided by the CXC in the application packages CIAO. This work has made use of 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 Center (CADC/NRC/CSA). NR 73 TC 12 Z9 12 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2014 VL 781 IS 1 AR 55 DI 10.1088/0004-637X/781/1/55 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286AE UT WOS:000329436100055 ER PT J AU Aliu, E Archambault, S Aune, T Benbow, W Berger, K Bird, R Bouvier, A Buckley, JH Bugaev, V Byrum, K Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fortin, P Fortson, L Furniss, A Galante, N Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Kaaret, P Kertzman, M Khassen, Y Kieda, D Krennrich, F Kumar, S Lang, MJ Lyutikov, M Maier, G McArthur, S McCann, A Meagher, K Millis, J Moriarty, P Mukherjee, R de Bhroithe, AO Ong, RA Otte, AN Park, N Perkins, JS Pohl, M Popkow, A Quinn, J Ragan, K Rajotte, J Reyes, LC Reynolds, PT Richards, GT Roache, E Sembroski, GH Sheidaei, F Smith, AW Staszak, D Telezhinsky, I Theiling, M Tucci, JV Tyler, J Varlotta, A Wakely, SP Weekes, TC Weinstein, A Welsing, R Williams, DA Zajczyk, A Zitzer, B AF Aliu, E. Archambault, S. Aune, T. Benbow, W. Berger, K. Bird, R. Bouvier, A. Buckley, J. H. Bugaev, V. Byrum, K. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krennrich, F. Kumar, S. Lang, M. J. Lyutikov, M. Maier, G. McArthur, S. McCann, A. Meagher, K. Millis, J. Moriarty, P. Mukherjee, R. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Quinn, J. Ragan, K. Rajotte, J. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Sembroski, G. H. Sheidaei, F. Smith, A. W. Staszak, D. Telezhinsky, I. Theiling, M. Tucci, J. V. Tyler, J. Varlotta, A. Wakely, S. P. Weekes, T. C. Weinstein, A. Welsing, R. Williams, D. A. Zajczyk, A. Zitzer, B. TI A SEARCH FOR ENHANCED VERY HIGH ENERGY GAMMA-RAY EMISSION FROM THE 2013 MARCH CRAB NEBULA FLARE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: general; ISM: individual objects (Crab Nebula) ID LARGE-AREA TELESCOPE; VARIABILITY; APRIL AB In 2013 March, a flaring episode from the Crab Nebula lasting similar to 2 weeks was detected by Fermi-LAT (Large Area Telescope on board the Fermi Gamma-ray Space Telescope). The Very Energetic Radiation Imaging Telescope Array System (VERITAS) provides simultaneous observations throughout this period. During the flare, Fermi-LAT detected a 20 fold increase in flux above the average synchrotron flux >100 MeV seen from the Crab Nebula. Simultaneous measurements with VERITAS are consistent with the non-variable long-term average Crab Nebula flux at TeV energies. Assuming a linear correlation between the very high energy flux change >1 TeV and the flux change seen in the Fermi-LAT band >100 MeV during the period of simultaneous observations, the linear correlation factor can be constrained to be at most 8.6 x 10(-3) with 95% confidence. C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA. [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Aune, T.; Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Roache, E.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; 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. [Buckley, J. H.; Bugaev, V.; Zajczyk, A.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Chen, X.; Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Chen, X.; Federici, S.; Hughes, G.; Maier, G.; Pohl, M.; Telezhinsky, I.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Lyutikov, M.; Sembroski, G. H.; Theiling, M.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Humensky, T. B.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Kieda, D.; Sheidaei, F.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Krennrich, F.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 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, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA. RI Khassen, Yerbol/I-3806-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Cui, Wei/0000-0002-6324-5772; 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; STFC in the U.K. FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. NR 36 TC 6 Z9 6 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 20 PY 2014 VL 781 IS 1 AR L11 DI 10.1088/2041-8205/781/1/L11 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 287ZY UT WOS:000329582400011 ER PT J AU Rigopoulou, D Hopwood, R Magdis, GE Thatte, N Swinyard, BM Farrah, D Huang, JS Alonso-Herrero, A Bock, JJ Clements, D Cooray, A Griffin, MJ Oliver, S Pearson, C Riechers, D Scott, D Smith, A Vaccari, M Valtchanov, I Wang, L AF Rigopoulou, D. Hopwood, R. Magdis, G. E. Thatte, N. Swinyard, B. M. Farrah, D. Huang, J. -S. Alonso-Herrero, A. Bock, J. J. Clements, D. Cooray, A. Griffin, M. J. Oliver, S. Pearson, C. Riechers, D. Scott, D. Smith, A. Vaccari, M. Valtchanov, I. Wang, L. TI HERSCHEL OBSERVATIONS OF FAR-INFRARED COOLING LINES IN INTERMEDIATE REDSHIFT (ULTRA)-LUMINOUS INFRARED GALAXIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: starburst; infrared: galaxies; infrared: ISM ID SIMILAR-TO 2; C-II LINE; STAR-FORMATION; SUBMILLIMETER GALAXIES; PHYSICAL CONDITIONS; PHOTODISSOCIATION REGIONS; INTERSTELLAR-MEDIUM; SPECTROSCOPY; DEFICIT; EMISSION AB We report the first results from a spectroscopic survey of the [C II] 158 mu m line from a sample of intermediate redshift (0.2 < z < 0.8) (ultra)-luminous infrared galaxies, (U) LIRGs (L-IR > 10(11.5) L-circle dot), using the Spectral and Photometric Imaging REceiver-Fourier Transform Spectrometer on board the Herschel Space Observatory. This is the first survey of [C II] emission, an important tracer of star formation, at a redshift range where the star formation rate density of the universe increases rapidly. We detect strong [C II] 158 mu m line emission from over 80% of the sample. We find that the [C II] line is luminous, in the range (0.8-4) x 10(-3) of the far-infrared continuum luminosity of our sources, and appears to arise from photodissociation regions on the surface of molecular clouds. The L-[C II]/L-IR ratio in our intermediate redshift (U) LIRGs is on average similar to 10 times larger than that of local ULIRGs. Furthermore, we find that the L-[C II]/L-IR and L-[C II]/LCO(1-0) ratios in our sample are similar to those of local normal galaxies and high-z star-forming galaxies. ULIRGs at z similar to 0.5 show many similarities to the properties of local normal and high-z star-forming galaxies. Our findings strongly suggest that rapid evolution in the properties of the star-forming regions of (U) LIRGs is likely to have occurred in the last 5 billion years. C1 [Rigopoulou, D.; Magdis, G. E.; Thatte, N.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Rigopoulou, D.; Swinyard, B. M.; Pearson, C.] Rutherford Appleton Lab, RAL Space Sci & Technol Facil Council, Didcot OX11 0QX, Oxon, England. [Hopwood, R.; Clements, D.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. [Swinyard, B. M.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Huang, J. -S.] Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China. [Huang, J. -S.] Chinese Acad Sci, China Chile Joint Ctr Astron, Santiago, Chile. [Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Alonso-Herrero, A.] CSIC UC, Inst Fis Cantabria, E-39006 Santander, Spain. [Bock, J. J.] CALTECH, Pasadena, CA 91125 USA. [Bock, J. J.; Cooray, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Griffin, M. J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Oliver, S.; Smith, A.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Pearson, C.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Riechers, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Vaccari, M.] Univ Western Cape, Astrophys Grp, Dept Phys, ZA-7535 Cape Town, South Africa. [Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, E-28691 Madrid, Spain. RP Rigopoulou, D (reprint author), Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England. RI Magdis, Georgios/C-7295-2014; Vaccari, Mattia/R-3431-2016; Alonso-Herrero, Almudena/H-1426-2015; OI Magdis, Georgios/0000-0002-4872-2294; Vaccari, Mattia/0000-0002-6748-0577; Alonso-Herrero, Almudena/0000-0001-6794-2519; Scott, Douglas/0000-0002-6878-9840 FU John Fell Oxford University Press (OUP) Research Fund; CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); NASA (USA); [ST/K00106X/1] FX We thank the anonymous referee for his/her insightful comments. D. R. and G. E. M. acknowledge support from grant ST/K00106X/1 and the John Fell Oxford University Press (OUP) Research Fund (G. E. M.). This Letter is based on data from Herschel's SPIRE-FTS. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including: University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). NR 42 TC 12 Z9 12 U1 1 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 JAN 20 PY 2014 VL 781 IS 1 AR L15 DI 10.1088/2041-8205/781/1/L15 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 287ZY UT WOS:000329582400015 ER PT J AU Huang, YM Rueda, LM AF Huang, Yiau-Min Rueda, Leopoldo M. TI A pictorial key to the species of Aedes (Ochlerotatus and Coetzeemyia) in the Afrotropical Region (Diptera: Culicidae) SO ZOOTAXA LA English DT Article DE Culicidae; mosquitoes; identification key; Africa ID ALLIED TAXA DIPTERA; LIFE STAGES; MORPHOLOGICAL DATA; AEDINI DIPTERA; CLASSIFICATION; PHYLOGENY; SUBGENERA AB Six species of the subgenus Ochlerotatus and one species of the subgenus Coetzeemyia of the genus Aedes in the Afrotropical Region are treated in a pictorial key based on diagnostic morphological features. Brief remarks on the new reclassification of the genus Aedes are also included. C1 [Huang, Yiau-Min] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Rueda, Leopoldo M.] Walter Reed Army Inst Res, Walter Reed Biosyst Unit, Entomol Branch, Silver Spring, MD 20910 USA. RP Rueda, LM (reprint author), Smithsonian Inst, Walter Reed Biosystemat Unit, Museum Support Ctr MRC 534, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM huangy@si.edu; ruedapol@si.edu NR 30 TC 3 Z9 3 U1 1 U2 4 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 17 PY 2014 VL 3754 IS 5 BP 592 EP 600 PG 9 WC Zoology SC Zoology GA 289RD UT WOS:000329698800005 PM 24869710 ER PT J AU Dillon, JS Liu, A Williams, CL Hewitt, JN Tegmark, M Morgan, EH Levine, AM Morales, MF Tingay, SJ Bernardi, G Bowman, JD Briggs, FH Cappallo, RC Emrich, D Mitchell, DA Oberoi, D Prabu, T Wayth, R Webster, RL AF Dillon, Joshua S. Liu, Adrian Williams, Christopher L. Hewitt, Jacqueline N. Tegmark, Max Morgan, Edward H. Levine, Alan M. Morales, Miguel F. Tingay, Steven J. Bernardi, Gianni Bowman, Judd D. Briggs, Frank H. Cappallo, Roger C. Emrich, David Mitchell, Daniel A. Oberoi, Divya Prabu, Thiagaraj Wayth, Randall Webster, Rachel L. TI Overcoming real-world obstacles in 21 cm power spectrum estimation: A method demonstration and results from early Murchison Widefield Array data SO PHYSICAL REVIEW D LA English DT Article ID FOREGROUND REMOVAL; RADIO-SOURCES; REIONIZATION OBSERVATORIES; COSMIC REIONIZATION; LOSING INFORMATION; 21-CM FLUCTUATIONS; SKY SURVEY; EPOCH; SUBTRACTION; SENSITIVITY AB We present techniques for bridging the gap between idealized inverse covariance weighted quadratic estimation of 21 cm power spectra and the real-world challenges presented universally by interferometric observation. By carefully evaluating various estimators and adapting our techniques for large but incomplete data sets, we develop a robust power spectrum estimation framework that preserves the so-called "Epoch of Reionization (EoR) window" and keeps track of estimator errors and covariances. We apply our method to observations from the 32-tile prototype of the Murchinson Widefield Array to demonstrate the importance of a judicious analysis technique. Lastly, we apply our method to investigate the dependence of the clean EoR window on frequency-especially the frequency dependence of the so-called "wedge" feature-and establish upper limits on the power spectrum from z = 6.2 to z = 11.7. Our lowest limit Delta(k) <0.3 Kelvin at 95% confidence at a comoving scale k = 0.046 Mpc(-1) and z = 9.5. C1 [Dillon, Joshua S.; Liu, Adrian; Williams, Christopher L.; Hewitt, Jacqueline N.; Tegmark, Max; Morgan, Edward H.; Levine, Alan M.] MIT, MIT Kavli Inst, Cambridge, MA 02139 USA. [Dillon, Joshua S.; Liu, Adrian; Williams, Christopher L.; Hewitt, Jacqueline N.; Tegmark, Max] MIT, Dept Phys, Cambridge, MA 02139 USA. [Liu, Adrian] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Liu, Adrian] Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Morales, Miguel F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Tingay, Steven J.; Emrich, David; Wayth, Randall] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6009, Australia. [Tingay, Steven J.; Briggs, Frank H.; Mitchell, Daniel A.; Wayth, Randall; Webster, Rachel L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [Bernardi, Gianni] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowman, Judd D.] Arizona State Univ, Sch Space & Earth Explorat, Tempe, AZ 85287 USA. [Briggs, Frank H.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, Roger C.; Oberoi, Divya] MIT, Haystack Observ, Westford, MA 01886 USA. [Mitchell, Daniel A.; Webster, Rachel L.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. [Oberoi, Divya] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Prabu, Thiagaraj] Raman Res Inst, Bangalore 560080, Karnataka, India. RP Dillon, JS (reprint author), MIT, MIT Kavli Inst, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM jsdillon@mit.edu; acliu@berkeley.edu RI Wayth, Randall/B-2444-2013; M, Manjunath/N-4000-2014; Emrich, David/B-7002-2013 OI Wayth, Randall/0000-0002-6995-4131; M, Manjunath/0000-0001-8710-0730; Emrich, David/0000-0002-4058-1837 FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF Grants) [LE0775621, LE0882938]; U.S. Air Force Office of Scientic Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (New Zealand Ministry of Economic Development) [MED-E1799]; Victoria University of Wellington (IBM Shared University Research Grant); National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Venture of Curtin University; University of Western Australia; Western Australian State government; NSF [AST-0821321, AST-1105835]; Berkeley Center for Cosmological Physics FX This work makes use of the Murchison Radio-astronomy Observatory. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (Grants No. AST-0457585, No. PHY-0835713, No. CAREER-0847753, and No. AST-0908884), the Australian Research Council (LIEF Grants No. LE0775621 and No. LE0882938), the U.S. Air Force Office of Scientic Research (Grant No. FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by Grant No. CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via Grant No. MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. Additionally, the authors wish to thank Aaron Ewall-Wice, Lu Feng, Abraham Neben, Aaron Parsons, Jonathan Pober, Ronald Remillard, and Richard Shaw for valuable discussions, and Rennan Barkana for both useful discussions and providing the theory results shown in Figs. 7 and 8. This work is partially supported by NSF Grants No. AST-0821321 and No. AST-1105835. A. L. acknowledges support from the Berkeley Center for Cosmological Physics. Because the contributions of the first two authors were essentially equal, we determined their order by a Monte Carlo algorithm inspired by the one presented in Sec. II B. NR 64 TC 63 Z9 63 U1 0 U2 2 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 JAN 15 PY 2014 VL 89 IS 2 AR 023002 DI 10.1103/PhysRevD.89.023002 PG 25 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AB5YP UT WOS:000331864900001 ER PT J AU Higginbotham, S Wong, WR Linington, RG Spadafora, C Iturrado, L Arnold, AE AF Higginbotham, Sarah Wong, Weng Ruh Linington, Roger G. Spadafora, Carmenza Iturrado, Liliana Arnold, A. Elizabeth TI Sloth Hair as a Novel Source of Fungi with Potent Anti-Parasitic, Anti-Cancer and Anti-Bacterial Bioactivity SO PLOS ONE LA English DT Article ID HOSPITAL-ACQUIRED INFECTIONS; GRAM-NEGATIVE BACTERIA; NATURAL-PRODUCTS; ENDOPHYTES; DIVERSITY; HOST; MICROORGANISMS; BIODIVERSITY; COMMUNITIES; ALIGNMENT AB The extraordinary biological diversity of tropical forests harbors a rich chemical diversity with enormous potential as a source of novel bioactive compounds. Of particular interest are new environments for microbial discovery. Sloths - arboreal mammals commonly found in the lowland forests of Panama - carry a wide variety of micro-and macro-organisms on their coarse outer hair. Here we report for the first time the isolation of diverse and bioactive strains of fungi from sloth hair, and their taxonomic placement. Eighty-four isolates of fungi were obtained in culture from the surface of hair that was collected from living three-toed sloths (Bradypus variegatus, Bradypodidae) in Soberania National Park, Republic of Panama. Phylogenetic analyses revealed a diverse group of Ascomycota belonging to 28 distinct operational taxonomic units (OTUs), several of which are divergent from previously known taxa. Seventy-four isolates were cultivated in liquid broth and crude extracts were tested for bioactivity in vitro. We found a broad range of activities against strains of the parasites that cause malaria (Plasmodium falciparum) and Chagas disease (Trypanosoma cruzi), and against the human breast cancer cell line MCF-7. Fifty fungal extracts were tested for antibacterial activity in a new antibiotic profile screen called BioMAP; of these, 20 were active against at least one bacterial strain, and one had an unusual pattern of bioactivity against Gram-negative bacteria that suggests a potentially new mode of action. Together our results reveal the importance of exploring novel environments for bioactive fungi, and demonstrate for the first time the taxonomic composition and bioactivity of fungi from sloth hair. C1 [Higginbotham, Sarah; Iturrado, Liliana] Smithsonian Trop Res Inst, Panama City, Panama. [Wong, Weng Ruh; Linington, Roger G.] Univ Calif Santa Cruz, Dept Chem & Biochem, Santa Cruz, CA 95064 USA. [Spadafora, Carmenza] Inst Invest Cient & Serv Alta Tecnol, Panama City, Panama. [Arnold, A. Elizabeth] Univ Arizona, Sch Plant Sci, Tucson, AZ USA. RP Higginbotham, S (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM higginbothams@si.edu OI Spadafora, Carmenza/0000-0002-3002-9467; Linington, Roger/0000-0003-1818-4971 FU International Cooperative Biodiversity Groups program (ICBG-Panama) [2 U01 TW006634-06]; College of Agriculture and Life Sciences at the University of Arizona FX This work was supported by the International Cooperative Biodiversity Groups program (ICBG-Panama http://www.icbg.org/, grant number 2 U01 TW006634-06) and the College of Agriculture and Life Sciences at the University of Arizona. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 65 TC 4 Z9 4 U1 18 U2 79 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 JAN 15 PY 2014 VL 9 IS 1 AR e84549 DI 10.1371/journal.pone.0084549 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 297DH UT WOS:000330235100024 PM 24454729 ER PT J AU Peplowski, PN Evans, LG Stockstill-Cahill, KR Lawrence, DJ Goldsten, JO McCoy, TJ Nittler, LR Solomon, SC Sprague, AL Starr, RD Weider, SZ AF Peplowski, Patrick N. Evans, Larry G. Stockstill-Cahill, Karen R. Lawrence, David J. Goldsten, John O. McCoy, Timothy J. Nittler, Larry R. Solomon, Sean C. Sprague, Ann L. Starr, Richard D. Weider, Shoshana Z. TI Enhanced sodium abundance in Mercury's north polar region revealed by the MESSENGER Gamma-Ray Spectrometer SO ICARUS LA English DT Article DE Mercury; Gamma-ray spectroscopy; Mercury, surface ID NEUTRON SPECTROMETER; EXOSPHERE; SURFACE; ATMOSPHERE; TRANSIT; MODEL; MOON; TEMPERATURES; STABILITY; VOLCANISM AB MESSENGER Gamma-Ray Spectrometer measurements demonstrate that the abundance of Na varies across the surface of Mercury. The maximum Na/Si abundance ratio of 0.20 +/- 0.03 by weight (similar to 5 wt% Na) is observed at high northern latitudes and is significantly larger than the equatorial Na/Si ratio of 0.11 +/- 0.01 (similar to 2.6 wt% Na). Comparisons of forward-modeled surface distributions with the gamma-ray measurements suggest that the observed distribution of Na can be explained by differences in elemental composition between the volcanic smooth plains units and heavily cratered terrain. The comparison improves when thermally driven depletion of Na from areas near Mercury's hot poles is included. When combined with other MESSENGER data sets, these results indicate that the smooth plains units include substantial abundances of alkali feldspars. Thermal depletion of Na from the hot poles without an assumed underlying compositional variability can also reproduce the measured Na/Si distribution, but that mechanism fails to account for other MESSENGER observations that support the presence of higher abundances of feldspars in the smooth plains units. (C) 2013 Elsevier Inc. All rights reserved. C1 [Peplowski, Patrick N.; Stockstill-Cahill, Karen R.; Lawrence, David J.; Goldsten, John O.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Evans, Larry G.] Comp Sci Corp, Lanham, MD 20706 USA. [Stockstill-Cahill, Karen R.; McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Nittler, Larry R.; Solomon, Sean C.; Weider, Shoshana Z.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Sprague, Ann L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Peplowski, PN (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM Patrick.Peplowski@jhuapl.edu RI Peplowski, Patrick/I-7254-2012; Lawrence, David/E-7463-2015; OI Peplowski, Patrick/0000-0001-7154-8143; Lawrence, David/0000-0002-7696-6667; Weider, Shoshana/0000-0003-1034-909X FU NASA [NAS5-97271, NASW-00002]; MESSENGER Participating Scientist Program FX We thank the entire MESSENGER team for their invaluable contributions to the development and operation of the MESSENGER spacecraft. The MESSENGER mission is supported by the NASA Discovery Program under contracts NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. LGE acknowledges support from the MESSENGER Participating Scientist Program. We thank David Paige for providing the modeled Mercury surface temperatures. We also thank two anonymous reviewers for providing constructive comments that improved the manuscript. NR 49 TC 25 Z9 25 U1 0 U2 15 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JAN 15 PY 2014 VL 228 BP 86 EP 95 DI 10.1016/j.icarus.2013.09.007 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 275HC UT WOS:000328665900008 ER PT J AU Thomas, CA Emery, JP Trilling, DE Delbo, M Hora, JL Mueller, M AF Thomas, Cristina A. Emery, Joshua P. Trilling, David E. Delbo, Marco Hora, Joseph L. Mueller, Michael TI Physical characterization of Warm Spitzer-observed near-Earth objects SO ICARUS LA English DT Article DE Asteroids; Asteroids, composition; Spectroscopy; Near-Earth objects ID ASTEROID SPECTROSCOPIC SURVEY; INFRARED TELESCOPE FACILITY; S-TYPE ASTEROIDS; REFLECTANCE SPECTRA; ORDINARY CHONDRITE; 433 EROS; MINERALOGICAL CHARACTERIZATION; SPACE-TELESCOPE; SOURCE REGIONS; DAWN MISSION AB Near-infrared spectroscopy of Near-Earth Objects (NEOs) connects diagnostic spectral features to specific surface mineralogies. The combination of spectroscopy with albedos and diameters derived from thermal infrared observations can increase the scientific return beyond that of the individual datasets. For instance, some taxonomic classes can be separated into distinct compositional groupings with albedo and different mineralogies with similar albedos can be distinguished with spectroscopy. To that end, we have completed a spectroscopic observing campaign to complement the ExploreNEOs Warm Spitzer program that obtained albedos and diameters of nearly 600 NEOs (Trilling, D.E. et al. [2010]. Astron. J. 140, 770-784. http://dx.doi.org/10.1088/0004-6256/140/3/770). The spectroscopy campaign included visible and near-infrared observations of ExploreNEOs targets from various observatories. Here we present the results of observations using the low-resolution prism mode (similar to 0.7-2.5 mu m) of the SpeX instrument on the NASA Infrared Telescope Facility (IRTF). We also include near-infrared observations of ExploreNEOs targets from the MIT-UH-IRTF Joint Campaign for Spectral Reconnaissance. Our dataset includes near-infrared spectra of 187 ExploreNEOs targets (125 observations of 92 objects from our survey and 213 observations of 154 objects from the MIT survey). We identify a taxonomic class for each spectrum and use band parameter analysis to investigate the mineralogies for the S-, Q-, and V-complex objects. Our analysis suggests that for spectra that contain near-infrared data but lack the visible wavelength region, the Bus-DeMeo system misidentifies some S-types as Q-types. We find no correlation between spectral band parameters and ExploreNEOs albedos and diameters. We investigate the correlations of phase angle with Band Area Ratio and near-infrared spectral slope. We find slightly negative Band Area Ratio (BAR) correlations with phase angle for Eros and Ivar, but a positive BAR correlation with phase angle for Ganymed. The results of our phase angle study are consistent with those of (Sanchez, J.A., Reddy, V., Nathues, A., Cloutis, E.A., Mann, P., Hiesinger, H. [2012]. Icarus 220, 36-50. http://dx.doi.org/10.1016/j.icarus.2012.04.008, arXiv:1205.0248). We find evidence for spectral phase reddening for Eros, Ganymed, and Ivar. We identify the likely ordinary chondrite type analog for an appropriate subset of our sample. Our resulting proportions of H, L, and LL ordinary chondrites differ from those calculated for meteorite falls and in previous studies of ordinary chondrite-like NEOs. (C) 2013 Elsevier Inc. All rights reserved. C1 [Thomas, Cristina A.; Trilling, David E.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Thomas, Cristina A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Thomas, Cristina A.] Oak Ridge Associated Univ, NASA, Postdoctoral Program, Oak Ridge, TN 37831 USA. [Emery, Joshua P.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Delbo, Marco] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice 4, France. [Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mueller, Michael] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. RP Thomas, CA (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 691, Greenbelt, MD 20771 USA. EM cristina.a.thomas@nasa.gov OI Hora, Joseph/0000-0002-5599-4650; Mueller, Michael/0000-0003-3217-5385 FU NASA Postdoctoral Program at Goddard Space Flight Center; NASA; JPL/Caltech; National Science Foundation [0506716] FX This research was supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA.; This work is based in part on observations made with the Spitzer Space Telescope, which is operated by JPL/Caltech under a contract with NASA. Support for this work was, provided by NASA through an award issued by JPL/Caltech.; Part of the data utilized in this publication were obtained and made available by the MIT-UH-IRTF Joint Campaign for NEO Reconnaissance. The IRTF is operated by the University of Hawaii under Cooperative Agreement No. NCC 5-538 with the National Aeronautics and Space Administration, Office of Space Science, Planetary Astronomy Program. The MIT component of this work is supported by the National Science Foundation under Grant No. 0506716. NR 71 TC 8 Z9 8 U1 0 U2 3 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 JAN 15 PY 2014 VL 228 BP 217 EP 246 DI 10.1016/j.icarus.2013.10.004 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 275HC UT WOS:000328665900017 ER PT J AU Jung, K Molinari, J Kalko, EKV AF Jung, Kirsten Molinari, Jesus Kalko, Elisabeth K. V. TI Driving Factors for the Evolution of Species-Specific Echolocation Call Design in New World Free-Tailed Bats (Molossidae) SO PLOS ONE LA English DT Article ID INSECTIVOROUS BATS; AERIAL-HAWKING; MOLECULAR PHYLOGENY; EMBALLONURID BATS; SIGNAL-DESIGN; CHIROPTERA; MORPHOLOGY; BEHAVIOR; VARIABILITY; ALTERNATION AB Phylogeny, ecology, and sensorial constraints are thought to be the most important factors influencing echolocation call design in bats. The Molossidae is a diverse bat family with a majority of species restricted to tropical and subtropical regions. Most molossids are specialized to forage for insects in open space, and thus share similar navigational challenges. We use an unprecedented dataset on the echolocation calls of 8 genera and 18 species of New World molossids to explore how habitat, phylogenetic relatedness, body mass, and prey perception contribute to echolocation call design. Our results confirm that, with the exception of the genus Molossops, echolocation calls of these bats show a typical design for open space foraging. Two lines of evidence point to echolocation call structure of molossids reflecting phylogenetic relatedness. First, such structure is significantly more similar within than among genera. Second, except for allometric scaling, such structure is nearly the same in congeneric species. Despite contrasting body masses, 12 of 18 species call within a relatively narrow frequency range of 20 to 35 kHz, a finding that we explain by using a modeling approach whose results suggest this frequency range to be an adaptation optimizing prey perception in open space. To conclude, we argue that the high variability in echolocation call design of molossids is an advanced evolutionary trait allowing the flexible adjustment of echolocation systems to various sensorial challenges, while conserving sender identity for social communication. Unraveling evolutionary drivers for echolocation call design in bats has so far been hampered by the lack of adequate model organisms sharing a phylogenetic origin and facing similar sensorial challenges. We thus believe that knowledge of the echolocation call diversity of New World molossid bats may prove to be landmark to understand the evolution and functionality of species-specific signal design in bats. C1 [Jung, Kirsten; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Molinari, Jesus] Univ Los Andes, Fac Ciencias, Dept Biol, Merida 5101, Venezuela. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Jung, K (reprint author), Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. EM kirsten.jung@uni-ulm.de RI caputo, carlo/N-3747-2014; OI Molinari, Jesus/0000-0002-9393-5483 FU German Academic Exchange Program (DAAD); DFG Schwerpunktprogramm; International Foundation for Science (Sweden) [B/2637] FX This work has partly been funded by the German Academic Exchange Program (DAAD) with a PhD-scholarship to K. Jung. Field work of E. Kalko was financed by the DFG Schwerpunktprogramm "Mechanismen der Aufrechterhaltung tropischer Diversitat". Field work by J. Molinari in Venezuela was partly funded by project B/2637 of the International Foundation for Science (Sweden). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 54 TC 16 Z9 16 U1 1 U2 73 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 JAN 14 PY 2014 VL 9 IS 1 AR e85279 DI 10.1371/journal.pone.0085279 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 292TQ UT WOS:000329925800033 PM 24454833 ER PT J AU Cavanaugh, KC Kellner, JR Forde, AJ Gruner, DS Parker, JD Rodriguez, W Feller, IC AF Cavanaugh, Kyle C. Kellner, James R. Forde, Alexander J. Gruner, Daniel S. Parker, John D. Rodriguez, Wilfrid Feller, Ilka C. TI Poleward expansion of mangroves is a threshold response to decreased frequency of extreme cold events SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE ecological threshold; frost tolerance; Landsat; coastal wetlands ID LEAF-AREA INDEX; CLIMATE-CHANGE; ECOLOGICAL THRESHOLDS; REGIME SHIFTS; SALT-MARSHES; SEA-LEVEL; FORESTS; FLORIDA; RESILIENCE; MANAGEMENT AB Regional warming associated with climate change is linked with altered range and abundance of species and ecosystems worldwide. However, the ecological impacts of changes in the frequency of extreme events have not been as well documented, especially for coastal and marine environments. We used 28 y of satellite imagery to demonstrate that the area of mangrove forests has doubled at the northern end of their historic range on the east coast of Florida. This expansion is associated with a reduction in the frequency of "extreme" cold events (days colder than -4 degrees C), but uncorrelated with changes in mean annual temperature, mean annual precipitation, and land use. Our analyses provide evidence for a threshold response, with declining frequency of severe cold winter events allowing for poleward expansion of mangroves. Future warming may result in increases in mangrove cover beyond current latitudinal limits of mangrove forests, thereby altering the structure and function of these important coastal ecosystems. C1 [Cavanaugh, Kyle C.; Parker, John D.; Rodriguez, Wilfrid; Feller, Ilka C.] Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA. [Cavanaugh, Kyle C.; Kellner, James R.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Forde, Alexander J.] Univ Maryland, Grad Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA. [Gruner, Daniel S.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. RP Cavanaugh, KC (reprint author), Smithsonian Environm Res Ctr, Smithsonian Inst, POB 28, Edgewater, MD 21037 USA. EM cavanaughk@si.edu RI Gruner, Daniel/A-5166-2010; Parker, John/F-9761-2010; OI Gruner, Daniel/0000-0002-3153-4297; Parker, John/0000-0002-3632-7625; Feller, Ilka/0000-0002-6391-1608 FU National Aeronautics and Space Administration Climate and Biological Response Program [NNX11AO94G]; National Science Foundation Macrosystems Biology Program [EF 1065821, 1065098] FX The authors thank Mark Spalding for permission to use the digital version of his World Atlas of Mangroves. Funding for this work was provided by National Aeronautics and Space Administration Climate and Biological Response Program NNX11AO94G and National Science Foundation Macrosystems Biology Program EF 1065821 and 1065098. NR 53 TC 60 Z9 62 U1 16 U2 104 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 JAN 14 PY 2014 VL 111 IS 2 BP 723 EP 727 DI 10.1073/pnas.1315800111 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 288LW UT WOS:000329614500043 PM 24379379 ER PT J AU Eckerle, I Ehlen, L Kallies, R Wollny, R Corman, VM Cottontail, VM Tschapka, M Oppong, S Drosten, C Muller, MA AF Eckerle, Isabella Ehlen, Lukas Kallies, Rene Wollny, Robert Corman, Victor M. Cottontail, Veronika M. Tschapka, Marco Oppong, Samuel Drosten, Christian Mueller, Marcel A. TI Bat Airway Epithelial Cells: A Novel Tool for the Study of Zoonotic Viruses SO PLOS ONE LA English DT Article ID SOUTH-AMERICAN BATS; SEROLOGICAL EVIDENCE; EIDOLON-HELVUM; FRUIT BATS; INFECTION; CORONAVIRUSES; RABIES; PARAMYXOVIRUSES; HANTAVIRUS; DISEASES AB Bats have been increasingly recognized as reservoir of important zoonotic viruses. However, until now many attempts to isolate bat-borne viruses in cell culture have been unsuccessful. Further, experimental studies on reservoir host species have been limited by the difficulty of rearing these species. The epithelium of the respiratory tract plays a central role during airborne transmission, as it is the first tissue encountered by viral particles. Although several cell lines from bats were established recently, no well-characterized, selectively cultured airway epithelial cells were available so far. Here, primary cells and immortalized cell lines from bats of the two important suborders Yangochiroptera and Yinpterochiroptera, Carollia perspicillata (Seba's short-tailed bat) and Eidolon helvum (Straw-colored fruit bat), were successfully cultured under standardized conditions from both fresh and frozen organ specimens by cell outgrowth of organ explants and by the use of serum-free primary cell culture medium. Cells were immortalized to generate permanent cell lines. Cells were characterized for their epithelial properties such as expression of cytokeratin and tight junctions proteins and permissiveness for viral infection with Rift-Valley fever virus and vesicular stomatitis virus Indiana. These cells can serve as suitable models for the study of bat-borne viruses and complement cell culture models for virus infection in human airway epithelial cells. C1 [Eckerle, Isabella; Ehlen, Lukas; Kallies, Rene; Wollny, Robert; Corman, Victor M.; Drosten, Christian; Mueller, Marcel A.] Univ Bonn, Med Ctr, Inst Virol, Bonn, Germany. [Cottontail, Veronika M.; Tschapka, Marco] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Tschapka, Marco] Smithsonian Trop Res Inst, Balboa, Panama. [Oppong, Samuel] Kwame Nkrumah Univ Sci & Technol, Kumasi, Ghana. RP Eckerle, I (reprint author), Univ Bonn, Med Ctr, Inst Virol, Bonn, Germany. EM eckerle@virology-bonn.de OI Mueller, Marcel/0000-0003-2242-5117; Corman, Victor Max/0000-0002-3605-0136 FU German Research Foundation (DFG) [DR 772/3- 1] FX The study was supported by the German Research Foundation (DFG grant DR 772/3- 1). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 58 TC 7 Z9 7 U1 1 U2 10 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 13 PY 2014 VL 9 IS 1 AR e84679 DI 10.1371/journal.pone.0084679 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 292SL UT WOS:000329922500014 PM 24454736 ER PT J AU Onofrio, R AF Onofrio, Roberto TI HIGH-ENERGY DENSITY IMPLICATIONS OF A GRAVITOWEAK UNIFICATION SCENARIO SO MODERN PHYSICS LETTERS A LA English DT Article DE Grasvitoweak unification; Yukawa couplings; dark matter; cosmological constant ID QUANTUM-FIELD THEORY; BLACK-HOLES; COSMOLOGICAL CONSTANT; ELEMENTARY-PARTICLES; GENERAL RELATIVITY; FUNDAMENTAL LENGTH; ASYMPTOTIC FREEDOM; POSSIBLE EXISTENCE; SCALE; MAXIMONS AB 'We discuss how a scenario recently proposed for the morphing of macroscopic gravit, tion into weak interactions at the at tometer scale affects our current understanding of high-energy density phenomena. We find that the Yukawa couplings of the fundamental fermions are directly related to their event horizons, setting an upper bound y(f) <= root 2 for their observability through gauge interactions. Particles With larger Yukawa you plings are not precluded, but should interact only gravitationally, providing a natural candidate for dark matter. Furthermore, the quantum vacuum contribution to the cosmological constant is reduced by several orders of magnitude with respect to the current estimates. The expected running of the Newtonian gravitational constant could provide a viable alternative scenario to the in stage of the Universe. C1 [Onofrio, Roberto] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35131 Padua, Italy. [Onofrio, Roberto] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Onofrio, R (reprint author), Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Via Marzolo 8, I-35131 Padua, Italy. EM onofrior@gmail.com NR 40 TC 0 Z9 0 U1 1 U2 14 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0217-7323 EI 1793-6632 J9 MOD PHYS LETT A JI Mod. Phys. Lett. A PD JAN 10 PY 2014 VL 29 IS 1 AR 1350187 DI 10.1142/S0217732313501873 PG 7 WC Physics, Nuclear; Physics, Particles & Fields; Physics, Mathematical SC Physics GA 302ZA UT WOS:000330642600008 ER PT J AU Aliu, E Archambault, S Aune, T Behera, B Beilicke, M Benbow, W Berger, K Bird, R Bouvier, A Buckley, JH Bugaev, V Byrum, K Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Duke, C Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fortin, P Fortson, L Furniss, A Galante, N Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Kaaret, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lang, MJ Madhavan, AS Maier, G Majumdar, P McCann, A Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Park, N Perkins, JS Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Rajotte, J Reyes, LC Reynolds, PT Richards, GT Roache, E Rousselle, J Sembroski, GH Sheidaei, F Skole, C Smith, AW Staszak, D Stroh, M Telezhinsky, I Theiling, M Tucci, JV Tyler, J Varlotta, A Vincent, S Wakely, SP Weinstein, A Welsing, R Williams, DA Zajczyk, A Zitzer, B Abramowski, A Aharonian, F Benkhali, FA Akhperjanian, AG Anguner, E Anton, G Balenderan, S Balzer, A Barnacka, A Becherini, Y Tjus, JB Bernlohr, K Birsin, E Bissaldi, E Biteau, J Bottcher, M 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 Giavitto, G Giebels, B Glicenstein, JF Grondin, MH Grudzinska, M Haffner, S 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 Lemiere, A Lemoine-Goumard, M Lenain, JP Lennarz, D Lohse, T Lopatin, A Lu, CC Marandon, V Marcowith, A Marx, R Maurin, G Maxted, N Mayer, M McComb, TJL Mehault, J Menzler, U Meyer, M Moderski, R Mohamed, M Moulin, E Murach, T Naumann, CL de Naurois, M 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 Romoli, C 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 Spies, F Stawarz, L Steenkamp, R Stegmann, C Stinzing, F Stycz, K Sushch, I Szostek, A Tavernet, JP Tavernier, T Taylor, AM 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 Weitzel, Q White, R Wierzcholska, A Willmann, P Wornlein, A Wouters, D Zacharias, M Zajczyk, A Zdziarski, AA Zech, A Zechlin, HS AF Aliu, E. Archambault, S. Aune, T. Behera, B. Beilicke, M. Benbow, W. Berger, K. Bird, R. Bouvier, A. Buckley, J. H. Bugaev, V. Byrum, K. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Duke, C. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. Madhavan, A. S. Maier, G. Majumdar, P. McCann, A. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Rajotte, J. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Rousselle, J. Sembroski, G. H. Sheidaei, F. Skole, C. Smith, A. W. Staszak, D. Stroh, M. Telezhinsky, I. Theiling, M. Tucci, J. V. Tyler, J. Varlotta, A. Vincent, S. Wakely, S. P. Weinstein, A. Welsing, R. Williams, D. A. Zajczyk, A. Zitzer, B. Abramowski, A. Aharonian, F. Benkhali, F. Ait 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. Boettcher, M. 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. Giavitto, G. Giebels, B. Glicenstein, J. F. Grondin, M. -H. Grudzinska, M. Haeffner, S. 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. Lemiere, A. Lemoine-Goumard, M. Lenain, J. -P. Lennarz, D. Lohse, T. Lopatin, A. Lu, C. -C. Marandon, V. Marcowith, A. Marx, R. Maurin, G. Maxted, N. Mayer, M. McComb, T. J. L. Mehault, J. Menzler, U. Meyer, M. Moderski, R. Mohamed, M. Moulin, E. Murach, T. Naumann, C. L. de Naurois, M. 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. Romoli, C. 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. Spies, F. Stawarz, L. Steenkamp, R. Stegmann, C. Stinzing, F. Stycz, K. Sushch, I. Szostek, A. Tavernet, J. -P. Tavernier, T. Taylor, A. M. 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. Weitzel, Q. White, R. Wierzcholska, A. Willmann, P. Woernlein, A. Wouters, D. Zacharias, M. Zajczyk, A. Zdziarski, A. A. Zech, A. Zechlin, H. -S. CA VERITAS Collaboration HESS Collaboration TI LONG-TERM TeV AND X-RAY OBSERVATIONS OF THE GAMMA- RAY BINARY HESS J0632+057 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; binaries: general; gamma rays: general(HESS J0632+057, VER J0633+057) ID LS-I +61-DEGREES-303; VERITAS OBSERVATIONS; I+61 303; EMISSION; I+61-DEGREES-303; VARIABILITY; DISCOVERY; WINDS; TELESCOPE; CATALOG AB HESS J0632+057 is the only gamma-ray binary known so far whose position in the sky allows observations with ground-based observatories in both the northern and southern hemispheres. Here we report on long-term observations of HESS J0632+057 conducted with the Very Energetic Radiation Imaging Telescope Array System and High Energy Stereoscopic System Cherenkov telescopes and the X-ray satellite Swift, spanning a time range from 2004 to 2012 and covering most of the system's orbit. The very-high-energy (VHE) emission is found to be variable and is correlated with that at X-ray energies. An orbital period of 315(-4)(+6) days is derived from the X-ray data set, which is compatible with previous results, P = (321 +/- 5) days. The VHE light curve shows a distinct maximum at orbital phases close to 0.3, or about 100 days after periastron passage, which coincides with the periodic enhancement of the X-ray emission. Furthermore, the analysis of the TeV data shows for the first time a statistically significant (> 6.5 sigma) detection at orbital phases 0.6-0.9. The obtained gamma-ray and X-ray light curves and the correlation of the source emission at these two energy bands are discussed in the context of the recent ephemeris obtained for the system. Our results are compared to those reported for other gamma-ray binaries. 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.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Aune, T.; Majumdar, P.; Ong, R. A.; Popkow, A.; Rousselle, J.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Behera, B.; Chen, X.; Federici, S.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Skole, C.; Telezhinsky, I.; Vincent, S.; Welsing, R.; Balzer, A.; Giavitto, G.; Holler, M.; Klepser, S.; Schulz, A.; Stegmann, C.; Stycz, K.] DESY, D-15738 Zeuthen, Germany. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.; Zajczyk, A.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; 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. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Chen, X.; Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Tucci, J. V.; 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.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.; Stroh, M.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Humensky, T. B.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Kieda, D.; Sheidaei, F.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Krennrich, F.; Madhavan, A. S.; 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. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 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. [Abramowski, A.; Fernandes, M. V.; Heinzelmann, G.; Horns, D.; Kastendieck, M. A.; Kneiske, T.; Meyer, M.; Opitz, B.; Raue, M.; Spies, F.; Tluczykont, M.; Zechlin, H. -S.] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany. [Aharonian, F.; Benkhali, F. Ait; Bernloehr, K.; Brun, F.; Carrigan, S.; Casanova, S.; Chaves, R. C. G.; Deil, C.; Domainko, W.; Edwards, T.; Eger, P.; Foerster, A.; Gallant, Y. A.; Grondin, M. -H.; Hahn, J.; Hermann, G.; Hillert, A.; Hofmann, W.; Hofverberg, P.; Krueger, P. P.; Lennarz, D.; Lu, C. -C.; Marandon, V.; Marcowith, A.; Marx, R.; Wilhelmi, E. de Ona; Panter, M.; Parsons, R. D.; de los Reyes, R.; Rieger, F.; Sanchez, D. A.; Viana, A.; Voelk, H. J.; Volpe, F.; Weitzel, Q.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Aharonian, F.; Akhperjanian, A. G.; Drury, L. O'C.; Romoli, C.; Rosier-Lees, S.; Taylor, A. M.] Dublin Inst Adv Studies, Dublin 2, Ireland. [Aharonian, F.; Mehault, J.; Sahakian, V.] Natl Acad Sci Republ Armenia, Yerevan, Armenia. [Akhperjanian, A. G.; Birsin, E.; Mehault, J.; Sahakian, V.] Yerevan Phys Inst, Yerevan 375036, Armenia. [Anguener, E.; Bernloehr, K.; 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.; 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.; Fuessling, M.; Mayer, M.; Stegmann, C.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Zajczyk, A.; Barnacka, A.; Dyks, J.; Janiak, M.; Kluzniak, W.; Moderski, R.; Rudak, B.; 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 Konigstuhl, D-69117 Heidelberg, Germany. [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. [Biteau, J.; Degrange, B.; Fegan, S.; Fontaine, G.; Giebels, B.; Khelifi, B.; de Naurois, M.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Boettcher, M.; 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.; Boisson, C.; 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, CNRS, LPNHE,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.; 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. [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.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, 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. [Djannati-Atai, A.; Espigat, P.; Lefaucheur, J.; Lemiere, A.; Pita, S.; Punch, M.; Tavernier, T.] Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, APC,CNRS,IN2P3,CEA Irfu, F-75205 Paris 13, France. [Dubus, G.; Henri, G.; Pelletier, G.; Petrucci, P. -O.] UJF Grenoble 1 CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG UMR 5274, 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.] Inst Fizyki Jadrowej PAN, PL-31342 Krakow, Poland. [Zajczyk, A.; Feinstein, F.; Fernandez, D.; Niemiec, J.; Poon, H.; Renaud, M.; Vasileiadis, G.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3, F-34095 Montpellier 5, France. [Fiasson, A.; Komin, Nu.; Krayzel, F.; Lamanna, G.; Maurin, G.; Trichard, C.] Univ Savoie, CNRS, IN2P3, Lab Annecy le Vieux Phys Particules, F-74941 Annecy Le Vieux, France. [Jamrozy, M.; Stawarz, L.; Szostek, A.; Wierzcholska, A.] Uniwersytet Jagiellonian, Obserwatorium Astron, PL-30244 Krakow, Poland. [Katarzynski, K.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. [Ohm, S.; Ostrowski, M.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Rob, L.] Charles Univ Prague, Fac Math & Phys, Inst Particle & Nucl Phys, CR-18000 Prague 8, Czech Republic. RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. EM afalcone@astro.psu.edu; gernot.maier@desy.de; pol.bordas@uni-tuebingen.de RI Tjus, Julia/G-8145-2012; Katz, Uli/E-1925-2013; Casanova, Sabrina/J-8935-2013; Anton, Gisela/C-4840-2013; Khassen, Yerbol/I-3806-2015; 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; Komin, Nukri/J-6781-2015; Nieto, Daniel/J-7250-2015; 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 OI Katz, Uli/0000-0002-7063-4418; Casanova, Sabrina/0000-0002-6144-9122; Anton, Gisela/0000-0003-2039-4724; Khassen, Yerbol/0000-0002-7296-3100; 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; Oya, Igor/0000-0002-3881-9324; de Ona Wilhelmi, Emma/0000-0002-5401-0744; Rowell, Gavin/0000-0002-9516-1581; Lenain, Jean-Philippe/0000-0001-7284-9220; de los Reyes Lopez, Raquel/0000-0003-0485-9552; Kruger, Paulus/0000-0003-0664-8521; Komin, Nukri/0000-0003-3280-0582; Errando, Manel/0000-0002-1853-863X; Maxted, Nigel/0000-0003-2762-8378; Punch, Michael/0000-0002-4710-2165; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563; Sushch, Iurii/0000-0002-2814-1257; Bordas, Pol/0000-0002-0266-8536; Nieto, Daniel/0000-0003-3343-0755; Meyer, Manuel/0000-0002-0738-7581; Bissaldi, Elisabetta/0000-0001-9935-8106; Drury, Luke/0000-0002-9257-2270; Moulin, Emmanuel/0000-0003-4007-0145; Chadwick, Paula/0000-0002-1468-2685; Kneiske, Tanja M./0000-0002-3210-6200; mohamed, mahmoud/0000-0002-4625-6242; Cui, Wei/0000-0002-6324-5772; Daniel, Michael/0000-0002-8053-7910 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K; Helmholtz Association; European Community [ERC-StG-259391]; German Ministry for Education and Research (BMBF); Max Planck Society; French Ministry for Research; CNRS-IN2P3; Astroparticle Interdisciplinary Programme of the CNRS; U.K. Particle Physics and Astronomy Research Council (PPARC); IPNP of the Charles University; South African Department of Science and Technology and National Research Foundation; University of Namibia FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. G.M. acknowledges support through the Young Investigators Program of the Helmholtz Association. M.D. is funded by contract ERC-StG-259391 from the European Community.; The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. 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 U.K. 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 H.E.S.S. equipment. NR 82 TC 11 Z9 11 U1 3 U2 23 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 JAN 10 PY 2014 VL 780 IS 2 AR 168 DI 10.1088/0004-637X/780/2/168 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281JL UT WOS:000329097100055 ER PT J AU Barnard, R Garcia, MR Primini, F Murray, SS AF Barnard, R. Garcia, M. R. Primini, F. Murray, S. S. TI DISCOVERY OF A NEW BLACK HOLE TRANSIENT WITHIN 100 '' (400 PC) of M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: black holes; X-rays: binaries; X-rays: general ID HUBBLE-SPACE-TELESCOPE; X-RAY TRANSIENTS; LIGHT CURVES; CENTRAL REGION; BINARIES; CHANDRA; STATES; NOVAE AB We identified a new X-ray transient CXOM31 004252.457+411631.17 (T13) in M31 during a 2013 June Chandra observation. This system is particularly exciting because it is located within 100 '' of M31*; it is thought that this region of the bulge is sufficiently dense to form X-ray binaries dynamically, but only systems with black hole accretors and/or short periods are expected to survive. A follow-up XMM-Newton observation yielded a soft spectrum, well described by a 0.39 +/- 0.02 keV disk blackbody; applying this model to the Chandra observation yielded an observed 0.3-10 keV luminosity peak of 6.2 +/- 0.6x10(37) erg s(-1) (4.7x10(36) erg s(-1) in the 2.0-10 keV band). Observing with Hubble Space Telescope/Advanced Camera for Surveys did not reveal an optical counterpart, but allowed us to place an upper limit of B > 26.9, corresponding to an absolute V band magnitude >2.0. From the 2-10 keV luminosity and absolute V magnitude, we estimate an orbital period <5 h from an empirical relation. Fitting a disk blackbody + blackbody model allows us to reject a neutron star accretor at a 14 sigma level. C1 [Barnard, R.; Garcia, M. R.; Primini, F.; 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. OI Primini, Francis/0000-0002-6077-0643 FU ESA; US (NASA); Chandra grants [GO2-13106X, GO1-12109X]; HST grants [GO-11833, GO-12014]; NASA [NAS8-03060] FX We thank the anonymous referee for their constructive comments. We thank Z. Li for merging the Chandra data. This research has made use of data obtained from the Chandra satellite, 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); we are very grateful to Norbert Schartel and the XMM-Newton team for granting our TOO observation. 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 15 TC 3 Z9 3 U1 0 U2 0 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 JAN 10 PY 2014 VL 780 IS 2 AR 169 DI 10.1088/0004-637X/780/2/169 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281JL UT WOS:000329097100056 ER PT J AU Birnstiel, T Andrews, SM AF Birnstiel, Tilman Andrews, Sean M. TI ON THE OUTER EDGES OF PROTOPLANETARY DUST DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; planets and satellites: formation; protoplanetary disks ID CIRCUMSTELLAR DISKS; SIZE DISTRIBUTION; KEPLERIAN DISK; EVOLUTION; TAURI; PARTICLES; EMISSION; SYSTEMS; OBJECTS; BELT AB The expectation that aerodynamic drag will force the solids in a gas-rich protoplanetary disk to spiral in toward the host star on short timescales is one of the fundamental problems in planet formation theory. The nominal efficiency of this radial drift process is in conflict with observations, suggesting that an empirical calibration of solid transport mechanisms in a disk is highly desirable. However, the fact that both radial drift and grain growth produce a similar particle size segregation in a disk (such that larger particles are preferentially concentrated closer to the star) makes it difficult to disentangle a clear signature of drift alone. We highlight a new approach, by showing that radial drift leaves a distinctive "fingerprint" in the dust surface density profile that is directly accessible to current observational facilities. Using an analytical framework for dust evolution, we demonstrate that the combined effects of drift and (viscous) gas drag naturally produce a sharp outer edge in the dust distribution (or, equivalently, a sharp decrease in the dust-to-gas mass ratio). This edge feature forms during the earliest phase in the evolution of disk solids, before grain growth in the outer disk has made much progress, and is preserved over longer timescales when both growth and transport effects are more substantial. The key features of these analytical models are reproduced in detailed numerical simulations, and are qualitatively consistent with recent millimeter-wave observations that find gas/dust size discrepancies and steep declines in dust continuum emission in the outer regions of protoplanetary disks. C1 [Birnstiel, Tilman; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Birnstiel, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tbirnstiel@cfa.harvard.edu; sandrews@cfa.harvard.edu OI Birnstiel, Tilman/0000-0002-1899-8783 FU NASA [NNX12AJ04G] FX We are grateful for support from the NASA Origins of Solar Systems grant NNX12AJ04G, computing time on the Smithsonian Institution high performance cluster, hydra, and for a thoughtful review by the anonymous referee which helped improve the quality of the article. NR 40 TC 33 Z9 33 U1 1 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 JAN 10 PY 2014 VL 780 IS 2 AR 153 DI 10.1088/0004-637X/780/2/153 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281JL UT WOS:000329097100040 ER PT J AU Fong, W Berger, E Metzger, BD Margutti, R Chornock, R Migliori, G Foley, RJ Zauderer, BA Lunnan, R Laskar, T Desch, SJ Meech, KJ Sonnett, S Dickey, C Hedlund, A Harding, P AF Fong, W. Berger, E. Metzger, B. D. Margutti, R. Chornock, R. Migliori, G. Foley, R. J. Zauderer, B. A. Lunnan, R. Laskar, T. Desch, S. J. Meech, K. J. Sonnett, S. Dickey, C. Hedlund, A. Harding, P. TI SHORT GRB 130603B: DISCOVERY OF A JET BREAK IN THE OPTICAL AND RADIO AFTERGLOWS, AND A MYSTERIOUS LATE-TIME X-RAY EXCESS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: individual (130603B) ID NEUTRON-STAR MERGERS; CONTINUOUS ENERGY INJECTION; COMPACT-OBJECT MERGERS; SWIFT XRT DATA; GAMMA-RAY; LIGHT CURVES; HOST GALAXY; BURST AFTERGLOWS; EXTENDED EMISSION; 2-COMPONENT JET AB We present radio, optical/NIR, and X-ray observations of the afterglow of the short-duration Swift and Konus-Wind GRB 130603B, and uncover a break in the radio and optical bands at approximate to 0.5 day after the burst, best explained as a jet break with an inferred jet opening angle of approximate to 4 degrees-8 degrees. GRB 130603B is only the third short GRB with a radio afterglow detection to date, and represents the first time that a jet break has been evident in the radio band. We model the temporal evolution of the spectral energy distribution to determine the burst explosion properties and find an isotropic-equivalent kinetic energy of approximate to (0.6-1.7) x 10(51) erg and a circumburst density of approximate to 5x10(-3)-30 cm(-3). From the inferred opening angle of GRB 130603B, we calculate beaming-corrected energies of E gamma approximate to (0.5-2) x 10(49) erg and E-K approximate to (0.1-1.6) x 10(49) erg. Along with previous measurements and lower limits we find a median opening angle of approximate to 10 degrees. Using the all-sky observed rate of 10 Gpc(-3) yr(-1), this implies a true short GRB rate of approximate to 20 yr(-1) within 200 Mpc, the Advanced LIGO/VIRGO sensitivity range for neutron star binarymergers. Finally, we uncover evidence for significant excess emission in the X-ray afterglow of GRB 130603B at greater than or similar to 1 day and conclude that the additional energy component could be due to fall-back accretion or spin-down energy from a magnetar formed following the merger. C1 [Fong, W.; Berger, E.; Margutti, R.; Chornock, R.; Migliori, G.; Zauderer, B. A.; Lunnan, R.; Laskar, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Metzger, B. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Metzger, B. D.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Foley, R. J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, R. J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Desch, S. J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Meech, K. J.; Sonnett, S.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Dickey, C.; Hedlund, A.] Pomona Coll, Claremont, CA 91711 USA. [Harding, P.] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. RP Fong, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Lunnan, Ragnhild/0000-0001-9454-4639; Dickey, Claire/0000-0002-1081-3991 FU National Science Foundation [AST-1107973]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302954]; ESA Member States; USA (NASA); [13A-046] FX We thank Barry Madore for obtaining Magellan observations. We thank the VLA staff for rapid response capabilities, and especially Joan Wrobel for scheduling of VLA observations. The Berger GRB group is supported by the National Science Foundation under AST-1107973. B.A.Z. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302954. VLA observations were obtained under Program 13A-046. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper includes data gathered with the 6.5 m Magellan telescopes located at Las Campanas Observatory, Chile. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). NR 110 TC 48 Z9 50 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 JAN 10 PY 2014 VL 780 IS 2 AR 118 DI 10.1088/0004-637X/780/2/118 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281JL UT WOS:000329097100005 ER PT J AU Kallman, T Evans, DA Marshall, H Canizares, C Longinotti, A Nowak, M Schulz, N AF Kallman, T. Evans, Daniel A. Marshall, H. Canizares, C. Longinotti, A. Nowak, M. Schulz, N. TI A CENSUS OF X-RAY GAS IN NGC 1068: RESULTS FROM 450 ks of CHANDRA HIGH ENERGY TRANSMISSION GRATING OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: Seyfert; X-rays: galaxies ID NARROW-LINE REGION; ACTIVE GALACTIC NUCLEI; ELECTRON-IMPACT EXCITATION; ATOMIC DECAY DATA; RESOLVED SPECTROSCOPY; FE-XVII; SHELL PHOTOIONIZATION; PHYSICAL CONDITIONS; VACANCY STATES; AUGER DECAY AB We present models for the X-ray spectrum of the Seyfert 2 galaxy NGC 1068. These are fitted to data obtained using the High Energy Transmission Grating on Chandra. The data show line and radiative recombination continuum emission from a broad range of ions and elements. The models explore the importance of excitation processes for these lines including photoionization followed by recombination, radiative excitation by absorption of continuum radiation, and inner shell fluorescence. The models show that the relative importance of these processes depends on the conditions in the emitting gas and that no single emitting component can fit the entire spectrum. In particular, the relative importance of radiative excitation and photoionization/recombination differs according to the element and ion stage emitting the line. This in turn implies a diversity of values for the ionization parameter of the various components of gas responsible for the emission, ranging from log(xi) = 1 to 3. Using this, we obtain an estimate for the total amount of gas responsible for the observed emission. The mass flux through the region included in the HETG extraction region is approximately 0.3 M-circle dot yr(-1), assuming ordered flow at the speed characterizing the line widths. This can be compared with what is known about this object from other techniques. C1 [Kallman, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Evans, Daniel A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marshall, H.; Canizares, C.; Nowak, M.; Schulz, N.] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA. [Longinotti, A.] ESA, European Space Astron Ctr, E-28691 Madrid, Spain. RP Kallman, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 51 TC 14 Z9 14 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2014 VL 780 IS 2 AR 121 DI 10.1088/0004-637X/780/2/121 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281JL UT WOS:000329097100008 ER PT J AU Liu, HB Galvan-Madrid, R Forbrich, J Rodriguez, LF Takami, M Costigan, G Manara, CF Yan, CH Karr, J Chou, MY Ho, PTP Zhang, QZ AF Liu, Hauyu Baobab Galvan-Madrid, Roberto Forbrich, Jan Rodriguez, Luis F. Takami, Michihiro Costigan, Grainne Manara, Carlo Felice Yan, Chi-Hung Karr, Jennifer Chou, Mei-Yin Ho, Paul T. -P. Zhang, Qizhou TI TIME MONITORING OF RADIO JETS AND MAGNETOSPHERES IN THE NEARBY YOUNG STELLAR CLUSTER R CORONAE AUSTRALIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: activity; stars: evolution; stars: formation; stars: magnetic field ID MAGNETOCENTRIFUGALLY DRIVEN FLOWS; STAR-FORMING REGIONS; SIMULTANEOUS X-RAY; MOLECULAR CLOUDS; FU ORIONIS; IMAGING SPECTROSCOPY; EXCITING SOURCES; SCALE STRUCTURE; RHO-OPHIUCHI; SOLAR-FLARE AB We report Karl G. Jansky Very Large Array 8-10 GHz (lambda = 3.0-3.7 cm) monitoring observations toward the young stellar object (YSO) cluster R Coronae Australis (R CrA), taken from 2012 March 15 to 2012 September 12. These observations were planned to measure the radio flux variabilities in timescales from 0.5 hr to several days, to tens of days, and up to similar to 200 days. We found that among the YSOs detectable in individual epochs, in general, the most reddened objects in the Spitzer observations show the highest mean 3.5 cm Stokes I emission, and the lowest fractional variabilities on <200 day timescales. The brightest radio flux emitters in our observations are the two reddest sources IRS7W and IRS7E. In addition, by comparing our observations with observations taken from 1996 to 1998 and 2005, we found that the radio fluxes of these two sources have increased by a factor of similar to 1.5. The mean 3.5 cm fluxes of the three Class I/II sources, IRSI, IRS2, and IRS6, appear to be correlated with their accretion rates derived by a previous near-infrared line survey. The weakly accreting Class I/II YSOs, or those in later evolutionary stages, present radio flux variability on <0.5 hr timescales. Some YSOs were detected only during occasional flaring events. The source R CrA went below our detection limit during a few fading events. C1 [Liu, Hauyu Baobab; Takami, Michihiro; Yan, Chi-Hung; Karr, Jennifer; Chou, Mei-Yin; Ho, Paul T. -P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Galvan-Madrid, Roberto; Costigan, Grainne; Manara, Carlo Felice] European So Observ, D-85748 Garching, Germany. [Forbrich, Jan] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Rodriguez, Luis F.] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Costigan, Grainne] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Costigan, Grainne] Armagh Observ, Armagh BT61 9DG, North Ireland. [Yan, Chi-Hung] Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 117, Taiwan. [Ho, Paul T. -P.; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Liu, HB (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM hyliu@asiaa.sinica.edu.tw OI Zhang, Qizhou/0000-0003-2384-6589 FU European Community [229517R] FX H.B.L. thanks Dr. Joseph L. Hora for his help and useful comments while organizing this project. R. G.-M. acknowledges funding from the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No. 229517R. NR 87 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2014 VL 780 IS 2 AR 155 DI 10.1088/0004-637X/780/2/155 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281JL UT WOS:000329097100042 ER PT J AU Migliori, G Siemiginowska, A Kelly, BC Stawarz, L Celotti, A Begelman, MC AF Migliori, G. Siemiginowska, A. Kelly, B. C. Stawarz, L. Celotti, A. Begelman, M. C. TI JET EMISSION IN YOUNG RADIO SOURCES: A FERMI LARGE AREA TELESCOPE GAMMA-RAY VIEW SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; gamma rays: galaxies; radiation mechanisms: non-thermal ID COMPACT STEEP-SPECTRUM; ACTIVE GALACTIC NUCLEI; HIGH-FREQUENCY PEAKERS; LARGE-SCALE JETS; X-RAY; QUASAR PKS-1127-145; EVOLUTIONARY MODELS; ENERGY-DISTRIBUTION; SPACE-TELESCOPE; CENTRAL-ENGINE AB We investigate the contribution of the beamed jet component to the high-energy emission in young and compact extragalactic radio sources, focusing for the first time on the gamma-ray band. We derive predictions on the gamma-ray luminosities associated with the relativistic jet assuming a leptonic radiative model. The high-energy emission is produced via Compton scattering by the relativistic electrons in a spherical region at the considered scales (less than or similar to 10 kpc). Simulations show a wide range of gamma-ray luminosities, with intensities up to similar to 10(46)-10(48) erg s(-1) depending on the assumed jet parameters. We find a highly linear relation between the simulated X-ray and gamma-ray luminosities that can be used to select candidates for gamma-ray detection. We compare the simulated luminosity distributions in the radio, X-ray, and gamma-ray regimes with observations for the largest sample of X-ray-detected young radio quasars. Our analysis of similar to 4-yr Fermi Large Area Telescope (LAT) data does not yield any statistically significant detections. However, the majority of the model-predicted gamma-ray fluxes for the sample are near or below the current Fermi-LAT flux threshold and compatible with the derived upper limits. Our study gives constraints on the minimum jet power (L-jet,L-kin/L-disk > 0.01) of a potential jet contribution to the X-ray emission in the most compact sources (less than or similar to 1 kpc) and on the particle-to-magnetic field energy density ratio that are in broad agreement with equipartition assumptions. C1 [Migliori, G.; Siemiginowska, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kelly, B. C.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93107 USA. [Stawarz, L.] Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. [Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Celotti, A.] SISSA, I-26534136 Trieste, Italy. [Celotti, A.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Celotti, A.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Begelman, M. C.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Begelman, M. C.] Natl Inst Stand & Technol, Boulder, CO 80309 USA. RP Migliori, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM migliori@cfa.harvard.edu FU National Aeronautics and Space Administration [NAS8-03060, NNX10AO60G, GO1-12145X]; Polish NSC [DEC-2012/04/A/ST9/00083] FX The authors thank M. Sikora and D. E. Harris for useful suggestions and comments. We are grateful to the anonymous referee for critical comments that helped to improve the paper. This work was supported by the National Aeronautics and Space Administration contract NAS8-03060 and under the following grants: NNX10AO60G issued through the Fermi Guest Observer Program and GO1-12145X issued through the Chandra X-Ray Observatory Guest Observer program. L. S. was supported by Polish NSC grant DEC-2012/04/A/ST9/00083. The authors thank the Fermi Science Support Center Help Desk team for support in the data analysis. This research has made used of TOPCAT16 (Taylor 2005) for the preparation and manipulation of the tabular data. NR 91 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 JAN 10 PY 2014 VL 780 IS 2 AR 165 DI 10.1088/0004-637X/780/2/165 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281JL UT WOS:000329097100052 ER PT J AU Miguel, Y Kaltenegger, L AF Miguel, Y. Kaltenegger, L. TI EXPLORING ATMOSPHERES OF HOT MINI-NEPTUNES AND EXTRASOLAR GIANT PLANETS ORBITING DIFFERENT STARS WITH APPLICATION TO HD 97658b, WASP-12b, CoRoT-2b, XO-1b, AND HD 189733b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: atmospheres ID EARTH-LIKE PLANETS; CARBON-MONOXIDE; C/O RATIO; GJ 436B; NONEQUILIBRIUM CHEMISTRY; EXOPLANET ATMOSPHERES; CHEMICAL-EQUILIBRIUM; MODEL ATMOSPHERES; THERMAL INVERSION; SUPER-EARTHS AB We calculated an atmospheric grid for hot mini-Neptune and giant exoplanets that links astrophysical observable parameters-orbital distance and stellar type-with the chemical atmospheric species expected. The grid can be applied to current and future observations to characterize exoplanet atmospheres and serves as a reference to interpret atmospheric retrieval analysis results. To build the grid, we developed a one-dimensional code for calculating the atmospheric thermal structure and linked it to a photochemical model that includes disequilibrium chemistry (molecular diffusion, vertical mixing, and photochemistry). We compare the thermal profiles and atmospheric composition of planets at different semimajor axes (0.01 AU <= a <= 0.1 AU) orbiting F, G, K, and M stars. Temperature andUVflux affect chemical species in the atmosphere. We explore which effects are due to temperature and which are due to stellar characteristics, showing the species most affected in each case. CH4 and H2O are the most sensitive to UV flux, H displaces H-2 as the most abundant gas in the upper atmosphere for planets receiving a high UV flux. CH4 is more abundant for cooler planets. We explore vertical mixing, to inform degeneracies on our models and in the resulting spectral observables. For lower pressures, observable species like H2O or CO2 can indicate the efficiency of vertical mixing, with larger mixing ratios for a stronger mixing. By establishing the grid, testing the sensitivity of the results, and comparing our model to published results, our paper provides a tool to estimate what observations could yield. We apply our model to WASP-12b, CoRoT-2b, XO-1b, HD189733b, and HD97658b. C1 [Miguel, Y.; Kaltenegger, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kaltenegger, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Miguel, Y (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM miguel@mpia.de FU DFG [ENP Ka 3142/1-1]; International Space Science Institute ISSI FX We would like to thank Ravi Kumar Kopparapu for in depth discussions. We are grateful to Jonathan Fortney, Ian Crossteld, Andras Zsom, Brad Hansen, and Jim Kasting for stimulating discussions and comments that strengthened our paper, as well as Sarah Rugheimer for providing the stellar fuxes. We thank the referee for fruitful suggestions. L.K. and Y.M. acknowledge DFG funding ENP Ka 3142/1-1 and the International Space Science Institute ISSI. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. NR 63 TC 17 Z9 17 U1 3 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 JAN 10 PY 2014 VL 780 IS 2 AR 166 DI 10.1088/0004-637X/780/2/166 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281JL UT WOS:000329097100053 ER PT J AU Mineo, S Fabbiano, G D'Abrusco, R Fragos, T Kim, DW Strader, J Brodie, JP Gallagher, JS Zezas, A Luo, B AF Mineo, S. Fabbiano, G. D'Abrusco, R. Fragos, T. Kim, D. -W. Strader, J. Brodie, J. P. Gallagher, J. S. Zezas, A. Luo, B. TI THE RADIAL DISTRIBUTION OF X-RAY BINARIES AND GLOBULAR CLUSTERS IN NGC 4649 AND THEIR RELATION WITH THE LOCAL STELLAR MASS DENSITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; galaxies: individual (NGC 4946/NGC 4947); galaxies: interactions; X-rays: binaries ID EARLY-TYPE GALAXIES; HUBBLE-SPACE-TELESCOPE; CHANDRA MONITORING OBSERVATIONS; ELLIPTIC GALAXIES; STAR-FORMATION; DEEP CHANDRA; LUMINOSITY FUNCTIONS; SPITZER OBSERVATIONS; WIDE-FIELD; CONNECTION AB We investigate the radial distribution of the low-mass X-ray binary (LMXB) population in the elliptical galaxy NGC 4649, using Chandra and Hubble data to separate the field and globular cluster (GC) populations. GCs with LMXBs have the same radial distribution as the parent red and blue GCs. The radial profile of field LMXBs follows the V-band profile within the D25 of NGC 4649. Using the spatial information provided by our data, we find that the global galaxy-wide relations among cumulative number and luminosity of LMXBs and the integrated stellar mass hold on local scales within D25. An excess of field LMXBs with respect to the V-band light is observed in the galaxy's outskirts, which may be partially due to unidentified GC sources or to a rejuvenated field LMXB population caused by past merging interactions. C1 [Mineo, S.; Fabbiano, G.; D'Abrusco, R.; Fragos, T.; Kim, D. -W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mineo, S.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Strader, J.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Brodie, J. P.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. [Gallagher, J. S.; Luo, B.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Zezas, A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. [Luo, B.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Mineo, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM smineo@head.cfa.harvard.edu RI D'Abrusco, Raffaele/L-2767-2016; Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016 OI D'Abrusco, Raffaele/0000-0003-3073-0605; Zezas, Andreas/0000-0001-8952-676X; Fragos, Tassos/0000-0003-1474-1523 FU CfA prize fellowship program; ITC prize fellowship program; NASA [NAS8-03060]; NASA Chandra [AR1-12008X, G01-12110X]; NASA HST grant [G0-12369.01-A]; National Science Foundation; National Aeronautics and Space Administration FX S.M. is grateful to Stefano Zibetti for helpful discussions and data and to Marat Gilfanov for his valuable comments and suggestions that improved the quality of the paper. T. F. acknowledges support from the CfA and the ITC prize fellowship programs. We thank Maurizio Paolillo for providing the data used in Figure 6. The authors thank the anonymous referee for helpful comments that improved this paper. This work was partially supported by NASA contract NAS8-03060 (CXC), NASA Chandra grants AR1-12008X and G01-12110X, and NASA HST grant G0-12369.01-A. 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 far-ultraviolet and 24 mu m images were taken from the 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. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 71 TC 8 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2014 VL 780 IS 2 AR 132 DI 10.1088/0004-637X/780/2/132 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281JL UT WOS:000329097100019 ER PT J AU Owers, MS Nulsen, PEJ Couch, WJ Ma, CJ David, LP Forman, WR Hopkins, AM Jones, C Van Weeren, RJ AF Owers, Matt S. Nulsen, Paul E. J. Couch, Warrick J. Ma, Cheng-Jiun David, Laurence P. Forman, William R. Hopkins, Andrew M. Jones, Christine Van Weeren, Reinout J. TI A MERGER SHOCK IN A2034 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (A2034); X-rays: galaxies: clusters ID MERGING GALAXY CLUSTER; FOSSIL RADIO PLASMA; DIGITAL SKY SURVEY; COLD-FRONT; X-RAY; CHANDRA OBSERVATION; NUMERICAL SIMULATIONS; INTERGALACTIC MEDIUM; MAGNETIC-FIELD; OUTER REGIONS AB We present a 250 ks Chandra observation of the cluster merger A2034 with the aim of understanding the nature of a sharp edge previously characterized as a cold front. The new data reveal that the edge is coherent over a larger opening angle and is significantly more bow-shock-shaped than previously thought. Within similar to 27 degrees about the axis of symmetry of the edge, the density, temperature, and pressure drop abruptly by factors of 1.83(-0.08)(+0.09), 1.85(-0.41)(+0.41), and 3.4(-0.7)(+0.8), respectively. This is inconsistent with the pressure equilibrium expected of a cold front and we conclude that the edge is a shock front. We measure a Mach number M = 1.59(-0.07)(+0.06) and corresponding shock velocity v(shock) similar or equal to 2057 km s(-1). Using spectra collected at the MMT with the Hectospec multi-object spectrograph, we identify 328 spectroscopically confirmed cluster members. Significantly, we find a local peak in the projected galaxy density associated with a bright cluster galaxy that is located just ahead of the nose of the shock. The data are consistent with a merger viewed within similar to 23 degrees. of the plane of the sky. The merging subclusters are now moving apart along a north-south axis approximately 0.3 Gyr after a small impact parameter core passage. The gas core of the secondary subcluster, which was driving the shock, appears to have been disrupted by the merger. Without a driving "piston," we speculate that the shock is dying. Finally, we propose that the diffuse radio emission near the shock is due to the revival of pre-existing radio plasma that has been overrun by the shock. C1 [Owers, Matt S.; Couch, Warrick J.; Hopkins, Andrew M.] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Nulsen, Paul E. J.; Ma, Cheng-Jiun; David, Laurence P.; Forman, William R.; Jones, Christine; Van Weeren, Reinout J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Couch, Warrick J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Ma, Cheng-Jiun] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. RP Owers, MS (reprint author), Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia. EM matthew.owers@aao.gov.au OI Owers, Matt/0000-0002-2879-1663; Nulsen, Paul/0000-0003-0297-4493; van Weeren, Reinout/0000-0002-0587-1660; Forman, William/0000-0002-9478-1682 FU Australian Research Council [ARC FS110200023]; National Aeronautics and Space Administration [GO1-12161X]; Chandra X-Ray Observatory Center; National Aeronautics Space Administration [NAS8-03060]; NASA [NAS8-03060, PF2-130104]; Australian Research Council; Chandra X-Ray Center FX The authors thank Maxim Markevitch and Trevor Ponman for helpful discussions. We thank the referee, Herve Bourdin, for his constructive suggestions. M.S.O. acknowledges the funding support from the Australian Research Council through a Super Science Fellowship (ARC FS110200023). Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award No. GO1-12161X 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.E.J.N. was partly supported by NASA contract NAS8-03060. W.J.C. acknowledges the funding support of the Australian Research Council through an Australian Professorial Fellowship throughout most of this work. R.J.vW. is supported by NASA through the Einstein Postdoctoral grant No. 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 has made use of software provided by the Chandra X-Ray Center in the application packages CIAO, ChIPS, and Sherpa and also data obtained from the Chandra archive at the NASA Chandra X-Ray Center (cxc.harvard.edu/cda/). Some of the observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. We thank the MMT operators and queue-schedule mode scientists for their help during observations and the staff at the Harvard-Smithsonian Center for Astrophysics Telescope Data Center for reducing the Hectospec data. NR 65 TC 11 Z9 11 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2014 VL 780 IS 2 AR 163 DI 10.1088/0004-637X/780/2/163 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281JL UT WOS:000329097100050 ER PT J AU Romani, RW Forman, WR Jones, C Murray, SS Readhead, AC Taylor, GB Zavala, RT AF Romani, Roger W. Forman, W. R. Jones, Christine Murray, S. S. Readhead, A. C. Taylor, Greg B. Zavala, R. T. TI A MULTI-WAVELENGTH STUDY OF THE HOST ENVIRONMENT OF SMBHB 4C+37.11 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: halos; X-rays: galaxies ID BLACK-HOLE SYSTEM; SUPERMASSIVE BINARY; GALAXY CLUSTERS; CHANDRA; EVOLUTION; CATALOG; SEARCH; GAS; VLA AB 4C+37.11, at z = 0.055, shows two compact radio nuclei, imaged by very long baseline interferometry at 7 mas separation, making it the closest known resolved supermassive black hole binary (SMBHB). An important question is whether this unique object is young and was caught on the way to a gravitational in-spiral and merger, or has "stalled" at 7 pc. We describe new radio/optical/X-ray observations of the massive host and its surrounding X-ray halo. These data reveal X-ray/optical channels following the radio outflow and large scale edges in the X-ray halo. These structures are promising targets for further study which should elucidate their relationship to the unique SMBHB core. C1 [Romani, Roger W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Forman, W. R.; Jones, Christine] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Murray, S. S.] Johns Hopkins Univ, Baltimore, MD USA. [Readhead, A. C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Taylor, Greg B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Zavala, R. T.] US Naval Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. RP Romani, RW (reprint author), Stanford Univ, Dept Phys, Stanford, CA 94305 USA. EM rwr@astro.stanford.edu OI Forman, William/0000-0002-9478-1682 FU NASA [NNX10AD11G, NNX10AP65G, NAS8-03060]; Chandra Award [GO2-13149X]; Chandra X-ray Observatory Center; W. M. Keck Foundation FX This work was supported in part by NASA grants NNX10AD11G and NNX10AP65G (R. W. R.) and Chandra Award number GO2-13149X (G. B. T.) issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. We thank Adam van Etten for help with the CIAO reductions. R.T.Z. thanks M. Stickel for providing his imaging data of 4C +37.11, S. Howell for assistance during the WIYN runs and K. Herrmann for helpful discussions on narrow-band imaging.; Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. 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 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2014 VL 780 IS 2 AR 149 DI 10.1088/0004-637X/780/2/149 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281JL UT WOS:000329097100036 ER PT J AU Yamaguchi, H Eriksen, KA Badenes, C Hughes, JP Brickhouse, NS Foster, AR Patnaude, DJ Petre, R Slane, PO Smith, RK AF Yamaguchi, Hiroya Eriksen, Kristoffer A. Badenes, Carles Hughes, John P. Brickhouse, Nancy S. Foster, Adam R. Patnaude, Daniel J. Petre, Robert Slane, Patrick O. Smith, Randall K. TI NEW EVIDENCE FOR EFFICIENT COLLISIONLESS HEATING OF ELECTRONS AT THE REVERSE SHOCK OF A YOUNG SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; hydrodynamics; ISM: individual objects (SN 1572, Tycho's SNR); ISM: supernova remnants; shock waves; X-rays: ISM ID X-RAY-EMISSION; TEMPERATURE EQUILIBRATION; PARTICLE-ACCELERATION; NONRADIATIVE SHOCKS; ION EQUILIBRATION; IA SUPERNOVAE; CYGNUS LOOP; SN 1006; SPECTRUM; LIGHT AB Although collisionless shocks are ubiquitous in astrophysics, certain key aspects of them are not well understood. In particular, the process known as collisionless electron heating, whereby electrons are rapidly energized at the shock front, is one of the main open issues in shock physics. Here, we present the first clear evidence for efficient collisionless electron heating at the reverse shock of Tycho's supernova remnant (SNR), revealed by FeK diagnostics using high-quality X-ray data obtained by the Suzaku satellite. We detect K beta (3p -> 1s) fluorescence emission from low-ionization Fe ejecta excited by energetic thermal electrons at the reverse shock front, which peaks at a smaller radius than Fe K alpha (2p -> 1s) emission dominated by a relatively highly ionized component. Comparisons with our hydrodynamical simulations imply instantaneous electron heating to a temperature 1000 times higher than expected from Coulomb collisions alone. The unique environment of the reverse shock, which is propagating with a high Mach number into rarefied ejecta with a low magnetic field strength, puts strong constraints on the physical mechanism responsible for this heating and favors a cross-shock potential created by charge deflection at the shock front. Our sensitive observation also reveals that the reverse shock radius of this SNR is about 10% smaller than the previous measurement using the Fe K alpha morphology from the Chandra observations. Since strong Fe K beta fluorescence is expected only from low-ionization plasma where Fe ions still have many 3p electrons, this feature is key to diagnosing the plasma state and distribution of the immediate postshock ejecta in a young SNR. C1 [Yamaguchi, Hiroya; Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yamaguchi, Hiroya] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Yamaguchi, Hiroya; Brickhouse, Nancy S.; Foster, Adam R.; Patnaude, Daniel J.; Slane, Patrick O.; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Eriksen, Kristoffer A.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Badenes, Carles] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Badenes, Carles] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, Pittsburgh, PA 15260 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. RP Yamaguchi, H (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM hiroya.yamaguchi@nasa.gov RI XRAY, SUZAKU/A-1808-2009; OI Brickhouse, Nancy/0000-0002-8704-4473 FU NASA Suzaku GO grant [NNX08AZ86G]; NASA ADP grant [NNX12AF44G] FX We are thankful to Drs. John D. Raymond and Timothy R. Kallman for useful information and discussion. This work is supported by funding from NASA Suzaku GO grant NNX08AZ86G (J.P.H.) and NASA ADP grant NNX12AF44G (R.K.S.). NR 46 TC 13 Z9 13 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2014 VL 780 IS 2 AR 136 DI 10.1088/0004-637X/780/2/136 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281JL UT WOS:000329097100023 ER PT J AU Rodrigues, FD Mathis, WN Couri, MS AF Rodrigues Junior, Francisco De Assis Mathis, Wayne Nielsen Couri, Marcia Souto TI Hydrellia Robineau-Desvoidy (Diptera: Ephydridae) from Brazil with an emphasis on the faunas from the states of Parana and Rio de Janeiro SO ZOOTAXA LA English DT Article DE Diversity; Acalyptratae; Shore-flies; Agricultural pest; Rice miner ID RICE; MINER AB With more than 200 species worldwide, Hydrellia Robineau-Desvoidy is the largest genus of the family Ephydridae (Diptera). However, knowledge of this genus is much reduced in Brazil and throughout the Neotropical Region, where only 8 species are known, including one from Brazil (H. xanthocera Cresson). The objective of this study is to review the species of Hydrellia from Brazil, with an emphasis on the faunas of Parana and Rio de Janeiro states. Six new species are described: H. bocaiuvensis sp. nov. (Brazil, Parana, Bocai va do Sul, 25 degrees 14.9' S, 49 degrees 8.9' W, 890 m), H. longiseta sp. nov. (Brazil, Parana, Parque Iguau, 25 degrees 33.4' S, 49 degrees 13.6' W, 880 m), H. vilelai sp. nov. (Brazil, Parana, Bocai va do Sul, 25 degrees 16.6' S, 48 degrees 58.5' W, 770 m), H. simplex sp. nov. (Brazil, Parana, Parque Iguau, 25 degrees 33.4' S, 49 degrees 13.6' W, 880 m) e H. schneiderae sp. nov. (Brazil, Parana, Parque Iguau (25 degrees 33.4' S, 49 degrees 13.6' W, 880 m), H. similis sp. nov. (Brazil, Parana, Bocai va do Sul, 25 degrees 14.9' S, 49 degrees 8.9' W, 890 m). Seven new registers are recorded: H. agitator (Para), H. apalachee (Parana and Rio de Janeiro), H. calverti (Amazonas and Parana), H. cavator (Rio de Janeiro), H. tibialis (Amazonas, Parana and Rio de Janeiro), H. vulgaris (Parana, Sao Paulo, Santa Catarina and Rio de Janeiro), H. wirthi (Para, Parana and Santa Catarina). Together with H. xanthocera, Hydrellia now includes 14 species from Brazil. C1 [Rodrigues Junior, Francisco De Assis; Couri, Marcia Souto] Univ Fed Rio de Janeiro, Museu Nacl, Dept Entomol, BR-20940040 Rio De Janeiro, Brazil. [Mathis, Wayne Nielsen] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Couri, Marcia Souto] CNPq, Brasilia, DF, Brazil. RP Rodrigues, FD (reprint author), Univ Fed Rio de Janeiro, Museu Nacl, Dept Entomol, Quinta Boa Vista S-N, BR-20940040 Rio De Janeiro, Brazil. EM rodriguesjuniorfa@gmail.com RI Couri, Marcia/I-6614-2012 FU CNPq [401609/2009-0, 130608/2011-4] FX Recent field works by WNM (December 2009-June 2010) and FARJ (March 2011-February 2012) in Brazil that resulted in many of the specimens studied in this paper were supported by grants from CNPq (Visiting Researcher/Process number 401609/2009-0) (Master's scholarship/Process number 130608/2011-4), which we gratefully acknowledge and thank. NR 42 TC 1 Z9 1 U1 0 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 10 PY 2014 VL 3753 IS 6 BP 501 EP 541 PG 41 WC Zoology SC Zoology GA 287UJ UT WOS:000329567400001 ER PT J AU Tseng, ZJ Wang, XM Slater, GJ Takeuchi, GT Li, Q Liu, J Xie, GP AF Tseng, Z. Jack Wang, Xiaoming Slater, Graham J. Takeuchi, Gary T. Li, Qiang Liu, Juan Xie, Guangpu TI Himalayan fossils of the oldest known pantherine establish ancient origin of big cats SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE first appearance; Himalaya; Pantherinae; Felidae; Miocene; Asia ID FELIDAE; LEO; PHYLOGENY; RADIATION; DISPERSAL; DIVERSITY; EVOLUTION; LEOPARD; TIBET; FAUNA AB Pantherine felids ('big cats') include the largest living cats, apex predators in their respective ecosystems. They are also the earliest diverging living cat lineage, and thus are important for understanding the evolution of all subsequent felid groups. Although the oldest pantherine fossils occur in Africa, molecular phylogenies point to Asia as their region of origin. This paradox cannot be reconciled using current knowledge, mainly because early big cat fossils are exceedingly rare and fragmentary. Here, we report the discovery of a fossil pantherine from the Tibetan Himalaya, with an age of Late Miocene-Early Pliocene, replacing African records as the oldest pantherine. A 'total evidence' phylogenetic analysis of pantherines indicates that the new cat is closely related to the snow leopard and exhibits intermediate characteristics on the evolutionary line to the largest cats. Historical biogeographic models provide robust support for the Asian origin of pantherines. The combined analyses indicate that 75% of the divergence events in the pantherine lineage extended back to the Miocene, up to 7 Myr earlier than previously estimated. The deeper evolutionary origin of big cats revealed by the new fossils and analyses indicate a close association between Tibetan Plateau uplift and diversification of the earliest living cats. C1 [Tseng, Z. Jack; Wang, Xiaoming] Univ So Calif, Dept Biol Sci, Los Angeles, CA 90089 USA. [Tseng, Z. Jack; Wang, Xiaoming; Takeuchi, Gary T.] Nat Hist Museum Los Angeles Cty, Dept Vertebrate Paleontol, Los Angeles, CA 90007 USA. [Tseng, Z. Jack; Wang, Xiaoming] Museum Nat Hist, Div Paleontol, New York, NY 10024 USA. [Wang, Xiaoming; Li, Qiang; Liu, Juan] Chinese Acad Sci, Inst Vertebrate Paleontol & Paleoanthropol, Key Lab Vertebrate Evolut & Human Origins, Beijing 100044, Peoples R China. [Slater, Graham J.] Smithsonian Inst, Natl Museum Nat Hist, NHB, Dept Paleobiol, Washington, DC 20013 USA. [Slater, Graham J.] Smithsonian Inst, Natl Museum Nat Hist, NHB, Div Mammals, Washington, DC 20013 USA. [Takeuchi, Gary T.] George C Page Museum, Los Angeles, CA 90036 USA. [Liu, Juan] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. [Xie, Guangpu] Gansu Prov Museum, Lanzhou 730050, Peoples R China. RP Tseng, ZJ (reprint author), Univ So Calif, Dept Biol Sci, Los Angeles, CA 90089 USA. EM jtseng@amnh.org; xwang@nhm.org OI Wang, Xiaoming/0000-0003-1610-3840 FU National Basic Research Program of China (973 program) [2012CB821904]; Chinese Academy of Sciences [XDB03020104]; NSF GRF; DDIG; AMNH Frick Post-Doctoral Fellowship; NSF [EAR-0446699, 0444073, 0958704, 1227212]; NMNH Peter Buck Post-Doctoral Fellowship; NGS Waitt Grant [W22-08] FX Funding was provided by National Basic Research Program of China (973 program; 2012CB821904) and Chinese Academy of Sciences (XDB03020104); NSF GRF, DDIG and AMNH Frick Post-Doctoral Fellowship to Z.J.T., NSF EAR-0446699, 0444073, 0958704, 1227212 to X.W., NMNH Peter Buck Post-Doctoral Fellowship to G.J.S., and an NGS Waitt Grant (W22-08) to Q.L. NR 27 TC 10 Z9 11 U1 7 U2 61 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 JAN 7 PY 2014 VL 281 IS 1774 AR 20132686 DI 10.1098/rspb.2013.2686 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AC2XS UT WOS:000332380200022 PM 24225466 ER PT J AU Knap, M Mathy, CJM Ganahl, M Zvonarev, MB Demler, E AF Knap, Michael Mathy, Charles J. M. Ganahl, Martin Zvonarev, Mikhail B. Demler, Eugene TI Quantum Flutter: Signatures and Robustness SO PHYSICAL REVIEW LETTERS LA English DT Article ID ONE-DIMENSION; INTERACTING FERMIONS; DYNAMICS; IMPURITY; LIQUIDS; SYSTEMS; GAS; BOSONS; STATE AB We investigate the motion of an impurity particle injected with finite velocity into an interacting one-dimensional quantum gas. Using large-scale numerical simulations based on matrix product states, we observe and quantitatively analyze long-lived oscillations of the impurity momentum around a nonzero saturation value, called quantum flutter. We show that the quantum flutter frequency is equal to the energy difference between two branches of collective excitations of the model. We propose an explanation of the finite saturation momentum of the impurity based on the properties of the edge of the excitation spectrum. Our results indicate that quantum flutter exists away from integrability and provide parameter regions in which it could be observed in experiments with ultracold atoms using currently available technology. C1 [Knap, Michael; Mathy, Charles J. M.; Demler, Eugene] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Knap, Michael; Mathy, Charles J. M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Knap, Michael; Ganahl, Martin] Graz Univ Technol, Inst Theoret & Computat Phys, A-8010 Graz, Austria. [Zvonarev, Mikhail B.] Univ Paris 11, Lab LPTMS, UMR8626, F-91405 Orsay, France. [Zvonarev, Mikhail B.] CNRS, F-91405 Orsay, France. RP Knap, M (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Knap, Michael/H-3344-2011 OI Knap, Michael/0000-0002-7093-9502 FU Harvard-MIT CUA; DARPA OLE program; AFOSR MURI on Ultracold Molecules; ARO-MURI on Atomtronics; Austrian Marshall Plan Foundation; Austrian Science Fund (FWF) [J3361-N20]; SFB ViCoM [F41]; Swiss National Science Foundation [PA00P2_126228] FX We are grateful to E. Bogomolny, E. Burovski, V. Cheianov, E. Haller, A. Kamenev, A. Lamacraft, H. C. Nagerl, and M. Schecter for fruitful discussions. The authors acknowledge support from Harvard-MIT CUA, the DARPA OLE program, AFOSR MURI on Ultracold Molecules, ARO-MURI on Atomtronics, the Austrian Marshall Plan Foundation, the Austrian Science Fund (FWF) Project No. J3361-N20, and SFB ViCoM (F41), as well as the Swiss National Science Foundation Project No. PA00P2_126228. Numerical calculations have been performed on the Vienna Scientific Cluster. NR 56 TC 16 Z9 16 U1 1 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 JAN 7 PY 2014 VL 112 IS 1 AR 015302 DI 10.1103/PhysRevLett.112.015302 PG 5 WC Physics, Multidisciplinary SC Physics GA AB6ZC UT WOS:000331937900015 PM 24483907 ER PT J AU Ward, CV Tocheri, MW Plavcan, JM Brown, FH Manthi, FK AF Ward, Carol V. Tocheri, Matthew W. Plavcan, J. Michael Brown, Francis H. Manthi, Fredrick Kyalo TI Early Pleistocene third metacarpal from Kenya and the evolution of modern human-like hand morphology SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID AUSTRALOPITHECUS-AFARENSIS HAND; ARTICULAR MORPHOLOGY; MANUAL PROPORTIONS; HOMO-FLORESIENSIS; SITE SIERRA; ETHIOPIA; AFRICANUS; CAPITATE; REMAINS; HADAR AB Despite discoveries of relatively complete hands from two early hominin species (Ardipithecus ramidus and Australopithecus sediba) and partial hands from another (Australopithecus afarensis), fundamental questions remain about the evolution of human-like hand anatomy and function. These questions are driven by the paucity of hand fossils in the hominin fossil record between 800,000 and 1.8 My old, a time interval well documented for the emergence and subsequent proliferation of Acheulian technology (shaped bifacial stone tools). Modern and Middle to Late Pleistocene humans share a suite of derived features in the thumb, wrist, and radial carpometacarpal joints that is noticeably absent in early hominins. Here we show that one of the most distinctive features of this suite in the Middle Pleistocene to recent human hand, the third metacarpal styloid process, was present similar to 1.42 Mya in an East African hominin from Kaitio, West Turkana, Kenya. This fossil thus provides the earliest unambiguous evidence for the evolution of a key shared derived characteristic of modern human and Neandertal hand morphology and suggests that the distinctive complex of radial carpometacarpal joint features in the human hand arose early in the evolution of the genus Homo and probably in Homo erectus sensu lato. C1 [Ward, Carol V.] Univ Missouri, Dept Pathol & Anat Sci, Integrat Anat Program, Columbia, MO 65212 USA. [Tocheri, Matthew W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA. [Tocheri, Matthew W.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Plavcan, J. Michael] Univ Arkansas, Dept Anthropol, Fayetteville, AR 72701 USA. [Brown, Francis H.] Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA. [Manthi, Fredrick Kyalo] Natl Museums Kenya, Dept Earth Sci, Nairobi, Kenya. RP Ward, CV (reprint author), Univ Missouri, Dept Pathol & Anat Sci, Integrat Anat Program, Columbia, MO 65212 USA. EM WardCV@missouri.edu OI Tocheri, Matthew/0000-0001-7600-8998; Ward, Carol/0000-0001-6255-9668 FU Leakey Foundation; Palaeontological Scientific Trust of South Africa; Wenner-Gren Foundation; University of Missouri Research Council; Smithsonian Scholarly Studies Grant Program; National Science Foundation [BCS06-21542]; National Museums of Kenya; Government of Kenya FX We thank the crew of the West Turkana Paleontology Project for their hard work and dedication and the National Museums of Kenya and the Government of Kenya for permission to conduct research and support. We also thank Wesley A. Niewoehner and Erik Trinkaus for sharing data; the Smithsonian's National Museum of Natural History, the National Museums of Kenya, the University of the Witswatersrand, and the National Museum of Ethiopia for access to comparative collections; and Erik Trinkaus, Wes Niewoehner, Kristina Aldridge, and Casey Holliday for helpful discussions. We thank Lee Berger and Job Kibii for permission to include the scan of MH2 in Fig. 1. This work was supported by the Leakey Foundation, the Palaeontological Scientific Trust of South Africa, the Wenner-Gren Foundation, the University of Missouri Research Council, the Smithsonian Scholarly Studies Grant Program, and National Science Foundation Grant BCS06-21542 (to F. H. B., T. Cerling, and R. Bruhn). KNM-WT 51260 is housed at the National Museums of Kenya. NR 40 TC 22 Z9 22 U1 5 U2 55 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 JAN 7 PY 2014 VL 111 IS 1 BP 121 EP 124 DI 10.1073/pnas.1316014110 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 284VY UT WOS:000329350700049 PM 24344276 ER PT J AU Allan, E Bossdorf, O Dormann, CF Prati, D Gossner, MM Tscharntke, T Bluthgen, N Bellach, M Birkhofer, K Boch, S Bohm, S Borschig, C Chatzinotas, A Christ, S Daniel, R Diekotter, T Fischer, C Friedl, T Glaser, K Hallmann, C Hodac, L Holzel, N Jung, K Klein, AM Klaus, VH Kleinebecker, T Krauss, J Lange, M Morris, EK Muller, J Nacke, H Pasalic, E Rillig, MC Rothenwohrer, C Schally, P Scherber, C Schulze, W Socher, SA Steckel, J Steffan-Dewenter, I Turke, M Weiner, CN Werner, M Westphal, C Wolters, V Wubet, T Gockel, S Gorke, M Hemp, A Renner, SC Schoning, I Pfeiffer, S Konig-Ries, B Buscot, F Linsenmair, KE Schulze, ED Weisser, WW Fischer, M AF Allan, Eric Bossdorf, Oliver Dormann, Carsten F. Prati, Daniel Gossner, Martin M. Tscharntke, Teja Bluethgen, Nico Bellach, Michaela Birkhofer, Klaus Boch, Steffen Boehm, Stefan Boerschig, Carmen Chatzinotas, Antonis Christ, Sabina Daniel, Rolf Diekoetter, Tim Fischer, Christiane Friedl, Thomas Glaser, Karin Hallmann, Christine Hodac, Ladislav Hoelzel, Norbert Jung, Kirsten Klein, Alexandra Maria Klaus, Valentin H. Kleinebecker, Till Krauss, Jochen Lange, Markus Morris, E. Kathryn Mueller, Joerg Nacke, Heiko Pasalic, Esther Rillig, Matthias C. Rothenwoehrer, Christoph Schally, Peter Scherber, Christoph Schulze, Waltraud Socher, Stephanie A. Steckel, Juliane Steffan-Dewenter, Ingolf Tuerke, Manfred Weiner, Christiane N. Werner, Michael Westphal, Catrin Wolters, Volkmar Wubet, Tesfaye Gockel, Sonja Gorke, Martin Hemp, Andreas Renner, Swen C. Schoening, Ingo Pfeiffer, Simone Koenig-Ries, Birgitta Buscot, Francois Linsenmair, Karl Eduard Schulze, Ernst-Detlef Weisser, Wolfgang W. Fischer, Markus TI Interannual variation in land-use intensity enhances grassland multidiversity SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE biodiversity loss; agricultural grasslands; Biodiversity Exploratories ID FARMLAND BIODIVERSITY; BIOTIC HOMOGENIZATION; NUTRIENT ENRICHMENT; USE INTENSIFICATION; PLANT DIVERSITY; COMMUNITIES; HETEROGENEITY; EXTINCTION; RICHNESS; INDEX AB Although temporal heterogeneity is a well-accepted driver of biodiversity, effects of interannual variation in land-use intensity (LUI) have not been addressed yet. Additionally, responses to land use can differ greatly among different organisms; therefore, overall effects of land-use on total local biodiversity are hardly known. To test for effects of LUI (quantified as the combined intensity of fertilization, grazing, and mowing) and interannual variation in LUI (SD in LUI across time), we introduce a unique measure of whole-ecosystem biodiversity, multidiversity. This synthesizes individual diversity measures across up to 49 taxonomic groups of plants, animals, fungi, and bacteria from 150 grasslands. Multidiversity declined with increasing LUI among grasslands, particularly for rarer species and aboveground organisms, whereas common species and belowground groups were less sensitive. However, a high level of interannual variation in LUI increased overall multidiversity at low LUI and was even more beneficial for rarer species because it slowed the rate at which the multidiversity of rare species declined with increasing LUI. In more intensively managed grasslands, the diversity of rarer species was, on average, 18% of the maximum diversity across all grasslands when LUI was static over time but increased to 31% of the maximum when LUI changed maximally over time. In addition to decreasing overall LUI, we suggest varying LUI across years as a complementary strategy to promote biodiversity conservation. C1 [Allan, Eric; Bossdorf, Oliver; Prati, Daniel; Boch, Steffen; Socher, Stephanie A.; Fischer, Markus] Univ Bern, Inst Plant Sci, CH-3013 Bern, Switzerland. [Bossdorf, Oliver] Univ Tubingen, D-72076 Tubingen, Germany. [Dormann, Carsten F.] Univ Freiburg, D-79106 Freiburg, Germany. [Gossner, Martin M.; Lange, Markus; Pasalic, Esther; Tuerke, Manfred; Weisser, Wolfgang W.] Univ Jena, Inst Ecol, D-07743 Jena, Germany. [Gossner, Martin M.; Tuerke, Manfred; Gockel, Sonja; Weisser, Wolfgang W.] Tech Univ Munich, Ctr Food & Life Sci Weihenstephan, Dept Ecol & Ecosyst Management, Terr Ecol Res Grp, D-85354 Freising Weihenstephan, Germany. [Tscharntke, Teja; Boerschig, Carmen; Rothenwoehrer, Christoph; Scherber, Christoph; Westphal, Catrin] Univ Gottingen, Dept Crop Sci, D-37077 Gottingen, Germany. [Bluethgen, Nico] Tech Univ Darmstadt, D-64287 Darmstadt, Germany. [Bellach, Michaela; Krauss, Jochen; Steckel, Juliane; Steffan-Dewenter, Ingolf; Weiner, Christiane N.; Werner, Michael; Linsenmair, Karl Eduard] Univ Wurzburg, Bioctr, Dept Anim Ecol & Trop Biol, D-97074 Wurzburg, Germany. [Birkhofer, Klaus] Lund Univ, SE-22362 Lund, Sweden. [Boch, Steffen; Boehm, Stefan] Univ Bern, Bot Garden, CH-3013 Bern, Switzerland. [Boehm, Stefan; Jung, Kirsten; Renner, Swen C.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Chatzinotas, Antonis; Glaser, Karin] UFZ Helmholtz Ctr Environm Res, Dept Environm Microbiol, D-04318 Leipzig, Germany. [Christ, Sabina] Fraunhofer Inst Cell Therapy & Immunol, Dept Diagnost, D-04103 Leipzig, Germany. [Daniel, Rolf; Fischer, Christiane; Nacke, Heiko] Univ Gottingen, Dept Genom & Appl Microbiol, D-37077 Gottingen, Germany. [Daniel, Rolf; Fischer, Christiane; Nacke, Heiko] Univ Gottingen, Gottingen Genom Lab, Inst Microbiol & Genet, D-37077 Gottingen, Germany. [Diekoetter, Tim; Wolters, Volkmar] Univ Giessen, Dept Anim Ecol, D-35392 Giessen, Germany. [Fischer, Christiane; Gorke, Martin; Pfeiffer, Simone; Fischer, Markus] Senckenberg Gesell Nat Forsch, Biodivers & Climate Res Ctr, D-60325 Frankfurt, Germany. [Friedl, Thomas; Hallmann, Christine; Hodac, Ladislav] Univ Gottingen, Albrecht von Haller Inst Plant Sci, Dept Expt Phycol & Culture Collect Algae Gottinge, D-37073 Gottingen, Germany. [Hoelzel, Norbert; Klaus, Valentin H.; Kleinebecker, Till] Univ Munster, Inst Landscape Ecol, D-48149 Munster, Germany. [Klein, Alexandra Maria] Univ Luneburg, Inst Ecol, D-21335 Luneburg, Germany. [Lange, Markus; Schoening, Ingo; Schulze, Ernst-Detlef] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [Morris, E. Kathryn] Xavier Univ, Dept Biol, Cincinnati, OH 45207 USA. [Morris, E. Kathryn; Rillig, Matthias C.] Free Univ Berlin, Inst Biol, D-14195 Berlin, Germany. [Mueller, Joerg; Fischer, Markus] Univ Potsdam, D-14469 Potsdam, Germany. [Rillig, Matthias C.] Berlin Brandenburg Inst Adv Biodivers Res, D-14195 Berlin, Germany. [Schally, Peter] Univ Gottingen, Dept Silviculture & Forest Ecol Temperate Zones, D-37077 Gottingen, Germany. [Schulze, Waltraud] Max Planck Inst Mol Plant Physiol, D-14476 Potsdam, Germany. [Schulze, Waltraud] Univ Hohenheim, Dept Plant Syst Biol, D-70593 Stuttgart, Germany. [Wubet, Tesfaye; Buscot, Francois] UFZ Helmholtz Ctr Environm Res, Dept Soil Ecol, D-06120 Halle, Saale, Germany. [Wubet, Tesfaye; Buscot, Francois] German Ctr Integrat Biodivers Res iDiv, D-04103 Leipzig, Germany. [Hemp, Andreas] Univ Bayreuth, Dept Plant Systemat, D-95445 Bayreuth, Germany. [Renner, Swen C.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Koenig-Ries, Birgitta] Univ Jena, D-07743 Jena, Germany. [Buscot, Francois] Univ Leipzig, Inst Biol, Chair Soil Ecol, D-04103 Leipzig, Germany. RP Allan, E (reprint author), Univ Bern, Inst Plant Sci, CH-3013 Bern, Switzerland. EM eric.allan@ips.unibe.ch RI Tscharntke, Teja/N-5123-2014; Schoning, Ingo/D-3341-2009; Bossdorf, Oliver/A-8328-2008; Fischer, Markus/C-6411-2008; Rillig, Matthias/B-3675-2009; Westphal, Catrin/F-9560-2015; Krauss, Jochen/C-6216-2014; Wolters, Volkmar/B-4635-2010; Schulze, Waltraud/E-9800-2011; Bluthgen, Nico/F-5983-2010; Wubet, Tesfaye/C-6241-2012; Morris, Kathryn/I-4701-2014; Schulze, Ernst-Detlef/K-9627-2014; iDiv, Deutsches Zentrum/B-5164-2016; Chatzinotas, Antonis/D-6232-2013; Weisser, Wolfgang/B-9718-2014; Diekotter, Tim/L-2463-2016; Boch, Steffen/L-5436-2016; Gossner, Martin M./J-2730-2015; Holzel, Norbert/H-8753-2013; OI Schoning, Ingo/0000-0002-9830-5026; Bossdorf, Oliver/0000-0001-7504-6511; Fischer, Markus/0000-0002-5589-5900; Rillig, Matthias/0000-0003-3541-7853; Westphal, Catrin/0000-0002-2615-1339; Krauss, Jochen/0000-0003-2304-9117; Schulze, Waltraud/0000-0001-9957-7245; Wubet, Tesfaye/0000-0001-8572-4486; Weiner, Christiane/0000-0003-4013-4663; Daniel, Rolf/0000-0002-8646-7925; Schall, Peter/0000-0003-4808-818X; Konig-Ries, Birgitta/0000-0002-2382-9722; Renner, Swen/0000-0002-6893-4219; Chatzinotas, Antonis/0000-0002-0387-9802; Weisser, Wolfgang/0000-0002-2757-8959; Gossner, Martin M./0000-0003-1516-6364; Steffan-Dewenter, Ingolf/0000-0003-1359-3944; Glaser, Karin/0000-0002-5962-3603; Scherber, Christoph/0000-0001-7924-8911 FU Deutsche Forschungsgemeinschaft Priority Program [1374] FX We thank Fabrice Grassein and Madalin Parepa for comments on the manuscript and Jens Nieschulze and Michael Owonibi for maintenance of the database. This work was funded by the Deutsche Forschungsgemeinschaft Priority Program 1374 "Infrastructure-Biodiversity Exploratories." Fieldwork permits were given by the responsible state environmental offices of Baden-Wurttemberg, Thuringen, and Brandenburg (according to 72 Brandenburgisches Naturschutzgesetz). NR 37 TC 41 Z9 43 U1 26 U2 149 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 JAN 7 PY 2014 VL 111 IS 1 BP 308 EP 313 DI 10.1073/pnas.1312213111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 284VY UT WOS:000329350700081 PM 24368852 ER PT J AU Joshi, PS Malafarina, D Narayan, R AF Joshi, Pankaj S. Malafarina, Daniele Narayan, Ramesh TI Distinguishing black holes from naked singularities through their accretion disc properties SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article DE gravitational collapse; black holes; naked singularity ID EVENT-HORIZON; SPHERICAL GALAXIES; GRAVITATIONAL COLLAPSE; DUST CLOUD; SPACETIMES; RELATIVITY; CANDIDATE; EQUATIONS; STRENGTHS; BINARIES AB We show that, in principle, a slowly evolving gravitationally collapsing perfect fluid cloud can asymptotically settle to a static spherically symmetric equilibrium configuration with a naked singularity at the center. We consider one such asymptotic final configuration with a finite outer radius, and construct a toy model in which it is matched to a Schwarzschild exterior geometry. We examine the properties of circular orbits in this model. We then investigate the observational signatures of a thermal accretion disc in this spacetime, comparing them with the signatures expected for a disc around a black hole of the same mass. Several notable differences emerge. A disc around the naked singularity is much more luminous than one around an equivalent black hole. Also, the disc around the naked singularity has a spectrum with a high frequency power law segment that carries a major fraction of the total luminosity. Thus, at least some naked singularities can, in principle, be distinguished observationally from the black holes of the same mass. We discuss the possible implications of these results. C1 [Joshi, Pankaj S.; Malafarina, Daniele] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Malafarina, Daniele] Fudan Univ, Dept Phys, Shanghai 200433, Peoples R China. [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Joshi, PS (reprint author), Tata Inst Fundamental Res, Homi Bhabha Rd, Bombay 400005, Maharashtra, India. EM psj@tifr.res.in; daniele@fudan.edu.cn; rnarayan@cfa.harvard.edu RI Malafarina, Daniele/O-2076-2013; OI Malafarina, Daniele/0000-0002-8100-8797; Narayan, Ramesh/0000-0002-1919-2730 NR 57 TC 28 Z9 28 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD JAN 7 PY 2014 VL 31 IS 1 AR 015002 DI 10.1088/0264-9381/31/1/015002 PG 22 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 259SR UT WOS:000327547100003 ER PT J AU Coley, PD Kursar, TA AF Coley, Phyllis D. Kursar, Thomas A. TI On Tropical Forests and Their Pests SO SCIENCE LA English DT Editorial Material ID SPECIES COEXISTENCE; EVOLUTION; TRAITS; TREES; INGA C1 [Coley, Phyllis D.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Smithsonian Trop Res Inst, Panama City, Panama. RP Coley, PD (reprint author), Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. EM coley@biology.utah.edu NR 14 TC 25 Z9 26 U1 11 U2 72 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 JAN 3 PY 2014 VL 343 IS 6166 BP 35 EP 36 DI 10.1126/science.1248110 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 282HR UT WOS:000329162000040 PM 24385624 ER PT J AU Barragan, T Esteve, J Garcia-Bellido, DC Zamora, S Alvaro, JJ AF Barragan, Tania Esteve, Jorge Garcia-Bellido, Diego C. Zamora, Samuel Javier Alvaro, J. TI New Middle Cambrian palaeoscolecid sclerites of Hadimopanella oezgueli from the Cantabrian Mountains, northern Spain SO GFF LA English DT Article DE Genestosa Member; Gondwana; parataxonomy; taphonomy AB A new assemblage of palaeoscolecid sclerites preserving all the details of the (para)species Hadimopanella oezgueli Gedik, 1977, including characteristic ornamentation, has been found in the Middle Cambrian Genestosa Member (Oville Formation) of the Cantabrian Mountains, northern Spain. The assemblage of sclerites shows a great morphological variability enabling emendation of its diagnosis. Some of them exhibit erosive facets as a result of reworking preceding definitive burial. One key specimen has lateral slits along the marginal brim, which represent a crown of eroded tubercles, and may be classified out the (para) genus Hadimopanella. C1 [Barragan, Tania; Javier Alvaro, J.] Ctr Astrobiol CSIC INTA, Torrejon De Ardoz 28850, Spain. [Esteve, Jorge] Chinese Acad Sci, Nanjing Inst Geol & Palaeontol, Nanjing 210008, Peoples R China. [Esteve, Jorge] Univ W Bohemia, Ctr Biol Earth & Environm Sci, Plzen 30619, Czech Republic. [Garcia-Bellido, Diego C.] Univ Adelaide, Sch Earth & Environm Sci, Sprigg Geobiol Ctr, Adelaide, SA 5005, Australia. [Zamora, Samuel] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Barragan, T (reprint author), Ctr Astrobiol CSIC INTA, Ctra Torrejon Ajalvir Km 4, Torrejon De Ardoz 28850, Spain. EM barragangt@cab.inta-csic.es; jorgeves@unizar.es; Diego.Garcia-Bellido@adelaide.edu.au; samuel@unizar.es; alvarobjj@cab.inta-csic.es OI Garcia-Bellido, Diego/0000-0003-1922-9836 FU Spanish MICINN [CGL2010-19491, CGL2011-24516]; FEDER [CGL2010-19491, CGL2011-24516]; Chinese Academy of Sciences [2012Y1ZB0010] FX The authors thank the revision made by John Peel and an anonymous referee. This article is a contribution to the projects CGL2010-19491 and CGL2011-24516 from Spanish MICINN and FEDER. J.E. is supported by Chinese Academy of Sciences Fellowship for Young International Scientists Grant (Grant No 2012Y1ZB0010). NR 14 TC 1 Z9 1 U1 0 U2 2 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1103-5897 EI 2000-0863 J9 GFF JI GFF PD JAN 2 PY 2014 VL 136 IS 1 SI SI BP 22 EP 25 DI 10.1080/11035897.2013.874039 PG 4 WC Geology; Paleontology SC Geology; Paleontology GA AH2IU UT WOS:000335945500005 ER PT J AU Pobiner, B AF Pobiner, Briana TI Stone tools and fossil bones: debates in the archaeology of human origins SO AZANIA-ARCHAEOLOGICAL RESEARCH IN AFRICA LA English DT Book Review C1 [Pobiner, Briana] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA. RP Pobiner, B (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA. EM pobinerb@si.edu NR 3 TC 0 Z9 0 U1 1 U2 5 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0067-270X EI 1945-5534 J9 AZANIA JI Azania PD JAN 2 PY 2014 VL 49 IS 1 BP 117 EP 119 DI 10.1080/0067270X.2013.873197 PG 3 WC Archaeology SC Archaeology GA AD7ZE UT WOS:000333485200007 ER PT J AU Schoch, RR Sues, HD AF Schoch, Rainer R. Sues, Hans-Dieter TI A new archosauriform reptile from the Middle Triassic (Ladinian) of Germany SO JOURNAL OF SYSTEMATIC PALAEONTOLOGY LA English DT Article DE Reptilia; Archosauriformes; Doswelliidae; Triassic; Germany; phylogeny ID PHYLOGENETIC-RELATIONSHIPS; BATRACHOTOMUS-KUPFERZELLENSIS; EARLY EVOLUTION; ANATOMY; ORIGIN; DINOSAURS; DIAPSIDA; REDESCRIPTION; MORPHOLOGY; ARGENTINA AB Numerous well-preserved skeletal remains of a distinctive armoured archosauriform reptile from the Lower Keuper (Erfurt Formation; Middle Triassic: Ladinian: Longobardian) of Baden-Wurttemberg (Germany) represent a new taxon, Jaxtasuchus salomoni gen. et sp. nov. The dermal armour of Jaxtasuchus comprises transverse rows of four rectangular osteoderms each in the cervical, dorsal and caudal regions, with the individual plates closely resembling those of Doswellia kaltenbachi from Carnian strata in North America. The long and low maxilla of Jaxtasuchus held at least 15 teeth. The labial and lingual surfaces of the tall, only slightly recurved crowns of the maxillary teeth bear distinct vertical ridges and smooth mesial and distal carinae. The cervical region of the vertebral column is long. Phylogenetic analysis places Jaxtasuchus as the sister taxon to Doswellia in Doswelliidae sensu Desojo etal. (2011). Doswelliidae is diagnosed by the coarsely reticulate, incised ornamentation of osteoderms composed of central regular pits of subequal size and contour, and a mostly smooth anterior articular lamina on each osteoderm. The discovery of Jaxtasuchus confirms that Doswelliidae had a wide palaeogeographical distribution during the latter half of the Triassic.http://www.zoobank.org/urn:lsid:zoobank.org:pub:4A400628-07F3-4D1B-9CA8-336C379721FA C1 [Schoch, Rainer R.] Staatliches Museum Nat Kunde, D-70191 Stuttgart, Germany. [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Schoch, RR (reprint author), Staatliches Museum Nat Kunde, Rosenstein 1, D-70191 Stuttgart, Germany. EM rainer.schoch@smns-bw.de FU Alexander von Humboldt Research Award FX We are greatly indebted to Hans Hagdorn, Werner Kugler, Frank Ullmann, Brigitte Rozynek, Traugott Haubold, Ute Gunter, Hans Michael Salomon, Alfred Bartholoma and Johann Wegele for their continuing enthusiastic efforts to recover vertebrate fossils from the Lower Keuper, donation of numerous specimens, and collaboration with RRS and his field crews. Norbert Adorf and Isabell Rosin organized and undertook fieldwork on behalf of the museum and skilfully prepared the material. We thank Ulrike Jager, Marit Kamenz, Kim Kramer, Achim Lehmkuhl, Olav Maass, Andreas Matzke, Christiane Schott, Stefanie Siegel and Jaco Weinstock for their assistance in the field. RRS is indebted to Michael Parrish for helpful discussion and advice during the initial phase of this project. We thank Julia Desojo, Randall Irmis, Michael Maisch, Jeffrey Martz and Rupert Wild for discussions and unpublished information. William Parker and an anonymous reviewer provided helpful comments on the manuscript. H-DS gratefully acknowledges support from an Alexander von Humboldt Research Award. The present study would not have been possible without the enthusiastic assistance of numerous private collectors who have generously donated a large amount of vertebrate fossils from the Lower Keuper to the Staatliches Museum fur Naturkunde Stuttgart. Last but not least we express our sincere appreciation to the Schumann family, the owners of the property that includes the type locality, for their continued interest and assistance. NR 66 TC 9 Z9 9 U1 0 U2 1 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1477-2019 EI 1478-0941 J9 J SYST PALAEONTOL JI J. Syst. Palaeontol. PD JAN 2 PY 2014 VL 12 IS 1 BP 113 EP 131 DI 10.1080/14772019.2013.781066 PG 19 WC Evolutionary Biology; Paleontology SC Evolutionary Biology; Paleontology GA 287TD UT WOS:000329564200005 ER PT J AU Warner, DJ AF Warner, Deborah Jean TI Illustrating the Phaenomena: Celestial Cartography in Antiquity and the Middle Ages SO IMAGO MUNDI-THE INTERNATIONAL JOURNAL FOR THE HISTORY OF CARTOGRAPHY LA English DT Book Review C1 [Warner, Deborah Jean] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Warner, DJ (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0308-5694 EI 1479-7801 J9 IMAGO MUNDI JI Imago Mundi PD JAN 2 PY 2014 VL 66 IS 1 BP 131 EP 132 DI 10.1080/03085694.2014.846011 PG 2 WC Geography; History; History & Philosophy Of Science; History Of Social Sciences SC Geography; History; History & Philosophy of Science; Social Sciences - Other Topics GA 259GB UT WOS:000327514300030 ER PT J AU Ripley, SD AF Ripley, Sidney Dillon TI Museums and the Natural Heritage SO MUSEUM INTERNATIONAL LA English DT Article C1 [Ripley, Sidney Dillon] Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1350-0775 EI 1468-0033 J9 MUSEUM INT JI Mus. Int. PY 2014 VL 66 IS 1-4 SI SI BP 45 EP 48 DI 10.1111/muse.12055 PG 4 WC Art SC Art GA CX5PV UT WOS:000365755300009 ER PT J AU Bahr, C Weldon, M Wilson, RW AF Bahr, Charles Weldon, Marcus Wilson, Robert W. TI 50TH ANNIVERSARY SPECIAL FEATURE: THE DISCOVERY OF COSMIC MICROWAVE BACKGROUND SO BELL LABS TECHNICAL JOURNAL LA English DT Article ID MATHEMATICAL-THEORY; COMMUNICATION C1 [Bahr, Charles] Alcatel Lucent, Integrated Informat Solut, Boulogne Billancourt, France. [Weldon, Marcus] Bell Labs, Murray Hill, NJ USA. [Weldon, Marcus] Alcatel Lucent, Boulogne Billancourt, France. [Wilson, Robert W.] Harvard Smithsonian Ctr Astrophys, SAO, Cambridge, MA 02138 USA. RP Bahr, C (reprint author), Alcatel Lucent, Integrated Informat Solut, Boulogne Billancourt, France. NR 10 TC 0 Z9 0 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1089-7089 EI 1538-7305 J9 BELL LABS TECH J JI Bell Labs Tech. J. PY 2014 VL 19 BP 1 EP 7 PG 7 WC Computer Science, Information Systems; Engineering, Electrical & Electronic; Telecommunications SC Computer Science; Engineering; Telecommunications GA CW2VK UT WOS:000364851000001 ER PT J AU Montiel-Reyes, F Maldonado, JE Del Real-Monroy, M Martinez-Mendez, N Ortega, J AF Montiel-Reyes, Fernando Maldonado, Jesus E. Del Real-Monroy, Melina Martinez-Mendez, Norberto Ortega, Jorge TI Non-invasive sampling reveals fine-scale genetic structure in black bear Ursus americanus populations from northeastern Mexico SO ENDANGERED SPECIES RESEARCH LA English DT Article ID ALLELE FREQUENCY DATA; MICROSATELLITE LOCI; GENOTYPING ERRORS; COMPUTER-PROGRAM; NULL ALLELE; OTTER FECES; DESERT; CONSERVATION; SOFTWARE; DNA AB The black bear Ursus americanus is one of the largest terrestrial carnivores that has a wide distribution in northeastern Mexico, the only country in which black bears are listed as endangered. We used 10 nuclear microsatellite loci to evaluate black bear genetic variability in 6 disjointed populations from northeastern Mexico. Non-invasive genetic techniques were applied to fecal and hair samples. Using a panel of 10 polymorphic microsatellites we identified 64 individuals. Black bears showed low to moderate levels of genetic diversity in all sampled populations (mean +/- SD expected heterozygosity, H-e = 0.63 +/- 0.628). Pairwise comparisons between all 6 populations (phi(ST) = 0.315, p < 0.05) detected significant genetic differentiation between the western Coahuila and the northeastern Nuevo Leon regions, suggesting that black bears have low levels of gene flow between these 2 regions. Microsatellites revealed significant structure within the complex of disjoint areas in the region. The inbreeding coefficient was also significant (phi(IS) = 0.143). The largest proportion of genetic variation (82.7%) was found between individuals within populations. Distance and anthropogenic activities may serve to limit gene exchange among populations which form at least 3 distinct genetic clusters; these may respond differently to environmental changes and should be considered distinct management units. C1 [Montiel-Reyes, Fernando; Martinez-Mendez, Norberto; Ortega, Jorge] Inst Politecn Nacl, Escuela Nacl Ciencias Biol, Dept Zool, Lab Bioconservac & Manejo, Mexico City 11340, DF, Mexico. [Maldonado, Jesus E.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Maldonado, Jesus E.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Ortega, J (reprint author), Inst Politecn Nacl, Escuela Nacl Ciencias Biol, Dept Zool, Lab Bioconservac & Manejo, Prolongac Carpio & Plan Ayala S-N,Col Sto Tomas, Mexico City 11340, DF, Mexico. EM artibeus2@aol.com NR 57 TC 0 Z9 0 U1 6 U2 18 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 1863-5407 EI 1613-4796 J9 ENDANGER SPECIES RES JI Endanger. Species Res. PY 2014 VL 26 IS 2 BP 179 EP 188 DI 10.3354/esr00626 PG 10 WC Biodiversity Conservation SC Biodiversity & Conservation GA AW7DY UT WOS:000346425900009 ER PT B AU Lovelock, CE Ruess, RW Feller, IC AF Lovelock, Catherine E. Ruess, Roger W. Feller, Ilka C. BE Bandyopadhyay, A TI CO2 EFFLUX FROM CLEARED MANGROVE PEAT SO CARBON CAPTURE AND STORAGE: CO2 MANAGEMENT TECHNOLOGIES LA English DT Article; Book Chapter ID SHRIMP PONDS; LAND-USE; FORESTS; SEQUESTRATION; RESPIRATION; SEDIMENTS; COLLAPSE; FUTURE C1 [Lovelock, Catherine E.] Univ Queensland, Sch Biol Sci, St Lucia, Qld, Australia. [Ruess, Roger W.] Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK USA. [Feller, Ilka C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Lovelock, CE (reprint author), Univ Queensland, Sch Biol Sci, St Lucia, Qld, Australia. RI Lovelock, Catherine/G-7370-2012 OI Lovelock, Catherine/0000-0002-2219-6855 NR 34 TC 0 Z9 0 U1 0 U2 1 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4822-5061-9; 978-1-77188-021-3 PY 2014 BP 267 EP 276 DI 10.1371/journal.pone.0021279 D2 10.1201/b16845 PG 10 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA BD7HF UT WOS:000363064600010 ER PT J AU Pekarik, AJ Schreiber, JB Hanemann, N Richmond, K Mogel, B AF Pekarik, Andrew J. Schreiber, James B. Hanemann, Nadine Richmond, Kelly Mogel, Barbara TI IPOP: A Theory of Experience Preference SO CURATOR-THE MUSEUM JOURNAL LA English DT Article ID POWER AB The theory and practice of IPOP emerged from structured observations and interviews with visitors to the Smithsonian Institution museums in Washington, D.C. from the 1990s to the present-a dataset useful in constructing a long view. This research has had one overarching intention: to serve museum visitors better, that is, to provide visitors with experiences that are above average, special, significant, and memorable. In numerous studies and interviews during the last 16 years, visitors have repeatedly spoken about their reactions to Smithsonian museum exhibitions in four typologies distilling their primary interests: I = ideas, P = people, O = objects, and-as we were obliged to add at a later stage-a second P for "physical." The evidence suggests that exhibitions that strongly appeal to all four visitor typologies will be highly successful with visitors. C1 [Pekarik, Andrew J.; Richmond, Kelly] Smithsonian Inst, Off Policy & Anal, Washington, DC 20560 USA. [Schreiber, James B.] Duquesne Univ, Pittsburgh, PA USA. [Hanemann, Nadine] Ctr Cultural Res, Bonn, Germany. [Mogel, Barbara] Natl Museum Amer Indian, Washington, DC USA. RP Pekarik, AJ (reprint author), Smithsonian Inst, Off Policy & Anal, Washington, DC 20560 USA. EM pekarika@si.edu NR 26 TC 3 Z9 3 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0011-3069 EI 2151-6952 J9 CURATOR JI Curator PD JAN PY 2014 VL 57 IS 1 BP 5 EP 27 DI 10.1111/cura.12048 PG 23 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA CU6IX UT WOS:000363636700002 ER PT J AU Schreiber, JB Pekarik, AJ AF Schreiber, James B. Pekarik, Andrew J. TI Technical Note: Using Latent Class Analysis versus K-means or Hierarchical Clustering to Understand Museum Visitors SO CURATOR-THE MUSEUM JOURNAL LA English DT Article AB This paper discusses the benefits of using Latent Class Analysis (LCA) versus K-means Cluster Analysis or Hierarchical Clustering as a way to understand differences among visitors in museums, and is part of a larger research program directed toward improving the museum-visit experience. For our comparison of LCA and K-means Clustering, we use data collected from 190 visitors leaving the exhibition Against All Odds; Rescue at the Chilean Mine in the National Museum of Natural History in January 2012. For the comparison of LCA and Hierarchical Clustering, we use data from 312 visitors leaving the exhibition Elvis at 21 in the National Portrait Gallery in January 2011. C1 [Schreiber, James B.] Duquesne Univ, Pittsburgh, PA 15282 USA. [Schreiber, James B.] Smithsonian Inst, Washington, DC 20560 USA. [Pekarik, Andrew J.] Smithsonian Inst, Off Policy & Anal, Washington, DC 20560 USA. RP Schreiber, JB (reprint author), Duquesne Univ, Pittsburgh, PA 15282 USA. EM jbschreiber@gmail.com; pekarika@si.edu NR 15 TC 3 Z9 3 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0011-3069 EI 2151-6952 J9 CURATOR JI Curator PD JAN PY 2014 VL 57 IS 1 BP 45 EP 59 DI 10.1111/cura.12050 PG 15 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA CU6IX UT WOS:000363636700004 ER PT B AU Canning-Clode, J Sugden, H AF Canning-Clode, Joao Sugden, Heather BE Dobretsov, S Thomason, JC Williams, DN TI Assessing fouling assemblages SO BIOFOULING METHODS LA English DT Article; Book Chapter ID SPECIES RICHNESS ESTIMATORS; MARINE BENTHIC COMMUNITIES; ACCUMULATION FUNCTIONS; REGIONAL RICHNESS; GLOBAL PATTERNS; BIODIVERSITY; DIVERSITY; ORGANISMS; INVENTORIES; PERSPECTIVE C1 [Canning-Clode, Joao] Univ Azores, Dept Oceanog & Fisheries, UAz & LARSyS Associated Lab, Ctr IMAR, Horta, Azores, Portugal. [Canning-Clode, Joao] Univ Lisbon, Fac Sci, Ctr Oceanog, P-1699 Lisbon, Portugal. [Canning-Clode, Joao] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Sugden, Heather] Newcastle Univ, Sch Marine Sci & Technol, Dove Marine Lab, North Shields, Tyne & Wear, England. [Sugden, Heather] Ecotekn UK Ltd, Newcastle Upon Tyne, Tyne & Wear, England. RP Canning-Clode, J (reprint author), Univ Azores, Dept Oceanog & Fisheries, UAz & LARSyS Associated Lab, Ctr IMAR, Horta, Azores, Portugal. NR 61 TC 1 Z9 1 U1 0 U2 1 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND BN 978-1-118-33614-4; 978-0-470-65985-4 PY 2014 BP 252 EP 270 D2 10.1002/9781118336144 PG 19 WC Agricultural Engineering SC Agriculture GA BD7DW UT WOS:000362910500031 ER PT J AU Seeger, A AF Seeger, Anthony TI Music as Intangible Cultural Heritage: Policy, Ideology, and Practice in the Preservation of East Asian Traditions SO YEARBOOK FOR TRADITIONAL MUSIC LA English DT Book Review C1 [Seeger, Anthony] Univ Calif Los Angeles, Ethnomusicol, Los Angeles, CA 90024 USA. [Seeger, Anthony] Smithsonian Folkways Recordings, Washington, DC USA. RP Seeger, A (reprint author), Univ Calif Los Angeles, Ethnomusicol, Los Angeles, CA 90024 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU INT COUNCIL TRADITIONAL MUSIC PI LJUBLJANA PA UNIV LJUBLJANA, DEPT MUSICOLOGY, FACULTY ARTS, ASKERCEVA 2, LJUBLJANA, 1000, SLOVENIA SN 0740-1558 J9 YEARB TRADIT MUSIC JI Yearb. Tradit. Mus. PY 2014 VL 46 BP 210 EP 211 PG 2 WC Music SC Music GA CT4SV UT WOS:000362798500013 ER PT J AU Cornelis, D Melletti, M Korte, L Ryan, SJ Mirabile, M Prin, T Prins, HHT AF Cornelis, Daniel Melletti, Mario Korte, Lisa Ryan, Sadie J. Mirabile, Marzia Prin, Thomas Prins, Herbert H. T. BE Melletti, M Burton, J TI African buffalo Syncerus caffer (Sparrman, 1779) SO ECOLOGY, EVOLUTION AND BEHAVIOUR OF WILD CATTLE: IMPLICATIONS FOR CONSERVATION LA English DT Article; Book Chapter ID KRUGER-NATIONAL-PARK; FOREST BUFFALO; SOUTH-AFRICA; CAPE BUFFALO; HABITAT SELECTION; ACTIVITY PATTERNS; LARGE HERBIVORES; LARGE MAMMALS; EAST-AFRICA; BOVINE TUBERCULOSIS C1 [Cornelis, Daniel] CIRAD, UPR AGIRs, Dept Environm & Societies, F-34398 Montpellier, France. [Cornelis, Daniel] Univ Zimbabwe, Res Platform Prod & Conservat Partnership, Harare, Zimbabwe. [Korte, Lisa] Smithsonian Conservat Biol Inst, Ctr Conservat Educ & Sustainabil, Natl Zool Pk, Washington, DC 20013 USA. [Ryan, Sadie J.] SUNY Coll Environm Sci & Forestry SUNY ESF, Syracuse, NY 13210 USA. [Prin, Thomas] Univ Lyon 1, CIRAD UPR AGIRs Dept Environm & Soc, IGF Fdn, CIRAD,UMR 5558,LBBE,CNRS, F-34398 Montpellier, France. [Prins, Herbert H. T.] Wageningen Univ, Resource Ecol Grp, NL-6708 PB Wageningen, Netherlands. RP Cornelis, D (reprint author), CIRAD, UPR AGIRs, Dept Environm & Societies, F-34398 Montpellier, France. NR 270 TC 1 Z9 1 U1 1 U2 2 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-1-107-03664-2 PY 2014 BP 326 EP 372 PG 47 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA BD0EO UT WOS:000357109900022 ER PT J AU Ripperger, SP Heymann, EW Tschapka, M Kalko, EKV AF Ripperger, Simon P. Heymann, Eckhard W. Tschapka, Marco Kalko, Elisabeth K. V. TI FRUIT CHARACTERISTICS ASSOCIATED WITH FRUIT PREFERENCES IN FRUGIVOROUS BATS AND SADDLE-BACK TAMARINS IN PERU SO ECOTROPICA LA English DT Article DE Stenodermatinae; Carolliinae; Saguinus nigrifrons; fruit chemistry; fruit preferences; seed dispersal; Peruvian Amazon ID SEED DISPERSAL; SAGUINUS-FUSCICOLLIS; EATING BATS; RAIN-FOREST; CAROLLIA-PERSPICILLATA; SECONDARY COMPOUNDS; AMAZONIAN PERU; SYMPATRIC TAMARINS; COLOBUS MONKEYS; FOOD SELECTION AB Many zoochorous fruit species evolved so-called fruit syndromes in order to attract certain dispersers on the basis of a combination of fruit traits. We evaluated visual (color) and chemical (compound composition) fruit traits associated with fruit preferences of free-ranging Neotropical frugivorous bats and saddle-back tamarins (Saguinus nigrifrons) living in sympatry. We documented 29 seed morphospecies carried by bats and report for the first time chiropterochorous dispersal of the plant genus Schefflera. Saddle-back tamarins fed on 15 species of fruits and overlapped with five species of fruits within the bats' diet. Generally, bats tended to prefer greenish fruits and S. nigrifrons selected mainly yellow fruits. The yellow color might enhance the visibility of the fruits against the dark foliage for the mainly visually-orienting tamarins. Bats, in contrast, rely more on olfactory cues for detection of fruits. Overall composition of fruit compounds did not differ between fruits eaten by saddle-back tamarins, by bats, or by both. Only fruits exclusively consumed by saddle-back tamarins were classified correctly to 100% by a discriminant function analysis pointing to similar chemical composition. These fruits were characterized by significantly lower lipid concentration and marginally lower protein concentration than fruits that were (also) eaten by bats. As bats show an energy-intense feeding strategy and cover their protein requirements largely by fruits, they might rely on fruits with higher protein and lipid concentration than saddle-back tamarins that complement their fruit diet more regularly with animal prey. C1 [Ripperger, Simon P.; Tschapka, Marco; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Ripperger, Simon P.] Museum Naturkunde, Leibniz Inst Evolut & Biodiversitatsforsch, D-10115 Berlin, Germany. [Heymann, Eckhard W.] German Primate Ctr DPZ, Behav Ecol & Sociobiol Unit, D-37077 Gottingen, Germany. [Tschapka, Marco; Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Ripperger, SP (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM simon.ripperger@mfn-berlin.de FU German Academic Exchange Service (DAAD) FX We are grateful to Prof Dr. J. Ganzhorn for the opportunity to conduct the chemical analyses at his institute, and to I. Tomaschewski for help during the lab work. We thank Ricardo Zarate for the identification of plants and the following people for help during fieldwork: Laia Prieto Rodriguez, Yvan Lledo Ferrer, Camilo Flores Arnasifuen, Jeisen Shahuano Tello, and Ney Shahuano Tello. INRENA kindly provided the permits for our fieldwork. Financial support was provided by a grant from the German Academic Exchange Service (DAAD) to SPR. NR 72 TC 0 Z9 0 U1 2 U2 12 PU SOC TROPICAL ECOLOGY, GTOE, ZOOLOGICAL RESEARCH INST & MUSE PI BONN PA ADENAUERALLE 160, BONN, 00000, GERMANY SN 0949-3026 J9 ECOTROPICA JI Ecotropica PY 2014 VL 20 IS 1-2 BP 53 EP 63 PG 11 WC Ecology SC Environmental Sciences & Ecology GA CN9DV UT WOS:000358747800005 ER PT J AU Sauvage, T Wynne, MJ Paul, VJ Fredericq, S AF Sauvage, Thomas Wynne, Michael J. Paul, Valerie J. Fredericq, Suzanne TI Morphological and molecular clarification of the enigmatic Caulerpa floridana WR Taylor (Chlorophyta, Bryopsidales) from the Dry Tortugas, Florida SO EUROPEAN JOURNAL OF PHYCOLOGY LA English DT Article DE Caulerpa; C. ashmeadii; C. floridana; C. prolifera; degraded DNA; Dry Tortugas; endemic; Gulf of Mexico; herbarium; tufA ID PELTATA COMPLEX CAULERPACEAE; ANCIENT DNA; PHYLOGENETIC ANALYSES; NORTHEAST PACIFIC; CHEMICAL DEFENSE; MARINE-ALGAE; RHODOPHYTA; CALIFORNIA; HALYMENIACEAE; SEQUENCES AB Morphological and molecular evidence is provided to further document the status of the enigmatic taxon known as Caulerpa floridana W.R. Taylor from White Shoal, Dry Tortugas, Florida. DNA sequencing of three historical herbarium specimens (WRT329, WRT345 and WRT349) housed at the University of Michigan Herbarium (MICH) demonstrated the molecular separation of this species based on the reconstruction of 931 nucleotides of the chloroplast gene tufA. Caulerpa floridana is sister to the western Atlantic endemic C. ashmeadii Harvey and an unknown Caulerpa taxon from the Florida Middle Grounds. Caulerpa floridana most reliably differs from C. ashmeadii by the presence of a sharp, unequivocal apiculus at the tip of each pinnule. A morphological review of southwestern Atlantic records of C. floridana from Brazil excludes these reports as representative of the species. C1 [Sauvage, Thomas; Fredericq, Suzanne] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. [Wynne, Michael J.] Univ Michigan Herbarium, Ann Arbor, MI 48108 USA. [Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. RP Sauvage, T (reprint author), Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. EM tomsauv@gmail.com FU Link Foundation/Smithsonian Marine Station Fellowship Award; NSF [DEB-0936855]; Gulf of Mexico Research Initiative (GoMRI-I) FX TS is indebted to the Link Foundation/Smithsonian Marine Station 2013 Fellowship Award for funding residency in Florida and at SMS for the completion of this research. TS is thankful to Rahul Ukey and Drs A. Chistoserdov and W. Schmidt (UL Lafayette), and Drs M. Boyle, N. Engene and J. Sneed (SMS) for technical and/or field assistance. Dr Ken Karol at NY is thanked for uploading an image of the isotype of Caulerpa floridana to the C.V. Starr Virtual Herbarium. We thank Dr James Norris and Barrett Brooks at US for discussion on deep Caulerpa taxa and interest in the study, as well as Dr Willem Prud'homme van Reine and an anonymous reviewer for comments on the manuscript. SF greatly acknowledges support from NSF DEB-0936855 and The Gulf of Mexico Research Initiative (GoMRI-I). This is SMS contribution No. 960. NR 64 TC 1 Z9 1 U1 0 U2 1 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0967-0262 EI 1469-4433 J9 EUR J PHYCOL JI Eur. J. Phycol. PY 2014 VL 49 IS 3 BP 370 EP 383 DI 10.1080/09670262.2014.947330 PG 14 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA CO6LO UT WOS:000359268400002 ER PT S AU Bouchez, AH Acton, DS Biasi, R Conan, R Espeland, B Esposito, S Filgueira, J Gallieni, D McLeod, BA Pinna, E Santoro, F Trancho, G van Dam, MA AF Bouchez, Antonin H. Acton, D. Scott Biasi, Roberto Conan, Rodolphe Espeland, Brady Esposito, Simone Filgueira, Josema Gallieni, Daniele McLeod, Brian A. Pinna, Enrico Santoro, Fernando Trancho, Gelys van Dam, Marcos A. BE Marchetti, E Close, LM Veran, JP TI The Giant Magellan Telescope Adaptive Optics Program SO ADAPTIVE OPTICS SYSTEMS IV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Adaptive Optics Systems IV CY JUN 22-27, 2014 CL Montreal, CANADA SP SPIE, American Astron Soc, Australian Astron Observatory, Assoc Univ Res Astron, Canadian Astron Soc, Canadian Space Agcy, European Astron Soc, European So Observatory, Natl Radio Astron Observatory, Royal Astron Soc, Sci & Technol Facilities Council DE Extremely Large Telescopes; Adaptive Optics; Adaptive Secondary Mirrors; Ground Layer AO AB The Giant Magellan Telescope (GMT) adaptive optics (AO) system will be an integral part of the telescope, providing laser guidestar generation, wavefront sensing, and wavefront correction to every instrument currently planned on the 25.4 m diameter GMT. There will be three first generation AO observing modes: Natural Guidestar, Laser Tomography, and Ground Layer AO. All three will use a segmented adaptive secondary mirror to deliver a corrected beam directly to the instruments. The Natural Guidestar mode will provide extreme AO performance, with a total wavefront error less than 185 nm RMS using bright guidestars. The Laser Tomography mode uses 6 lasers and a single off-axis natural guidestar to deliver better than 290 nm RMS wavefront error at the science target, over 50% of the sky at the galactic pole. The Ground Layer mode uses 4 natural guidestars on the periphery of the science field to tomographically reconstruct and correct the ground layer AO turbulence, improving the image quality for wide-field instruments. A phasing system maintains the relative alignment of the primary and secondary segments using edge sensors and continuous feedback from an off-axis guidestar. We describe the AO system preliminary design, predicted performance, and the remaining technical challenges as we move towards the start of construction. C1 [Bouchez, Antonin H.; Espeland, Brady; Filgueira, Josema; Santoro, Fernando; Trancho, Gelys] GMTO Corp, Pasadena, CA 91101 USA. [Acton, D. Scott] Ball Aerosp & Technol Corp, Boulder, CO 80306 USA. [Biasi, Roberto] Microgate Srl, I-89100 Bolzano, Italy. [Conan, Rodolphe] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Esposito, Simone; Pinna, Enrico] Osserv Astrofis Arcetri, I-50125 Florence, Italy. [Gallieni, Daniele] ADS Int Srl, I-23868 Valmadrera Lecco, Italy. [McLeod, Brian A.] Smithsonian Astrophys Observ, Cambridge, MA 02139 USA. [van Dam, Marcos A.] Flat Wavefronts, Christchurch 8140, New Zealand. RP Bouchez, AH (reprint author), GMTO Corp, 251 S Lake Ave, Pasadena, CA 91101 USA. EM abouchez@gmto.org OI Esposito, Simone/0000-0002-3114-677X; Pinna, Enrico/0000-0002-6243-5697 NR 34 TC 10 Z9 10 U1 0 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-9616-4 J9 PROC SPIE PY 2014 VL 9148 AR 91480W DI 10.1117/12.2057613 PG 19 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA BC8OD UT WOS:000355930800025 ER PT S AU Males, JR Close, LM Guyon, O Morzinski, K Puglisi, A Hinz, P Follette, KB Monnier, JD Tolls, V Rodigas, TJ Weinberger, A Boss, A Kopon, D Wu, YL Esposito, S Riccardi, A Xompero, M Briguglio, R Pinna, E AF Males, Jared R. Close, Laird M. Guyon, Olivier Morzinski, Katie Puglisi, Alfio Hinz, Philip Follette, Katherine B. Monnier, John D. Tolls, Volker Rodigas, Timothy J. Weinberger, Alycia Boss, Alan Kopon, Derek Wu, Ya-lin Esposito, Simone Riccardi, Armando Xompero, Marco Briguglio, Runa Pinna, Enrico BE Marchetti, E Close, LM Veran, JP TI Direct imaging of exoplanets in the habitable zone with adaptive optics SO ADAPTIVE OPTICS SYSTEMS IV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Adaptive Optics Systems IV CY JUN 22-27, 2014 CL Montreal, CANADA SP SPIE, American Astron Soc, Australian Astron Observatory, Assoc Univ Res Astron, Canadian Astron Soc, Canadian Space Agcy, European Astron Soc, European So Observatory, Natl Radio Astron Observatory, Royal Astron Soc, Sci & Technol Facilities Council DE extrasolar planets; habitable zone; adaptive optics; Magellan ID EXTRASOLAR GIANT PLANETS; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; OBSCURATIONAL COMPLETENESS; EARTH; MASS; I.; KEPLER; SYSTEM; METALLICITY AB One of the primary goals of exoplanet science is to find and characterize habitable planets, and direct imaging will play a key role in this effort. Though imaging a true Earth analog is likely out of reach from the ground, the coming generation of giant telescopes will find and characterize many planets in and near the habitable zones (HZs) of nearby stars. Radial velocity and transit searches indicate that such planets are common, but imaging them will require achieving extreme contrasts at very small angular separations, posing many challenges for adaptive optics (AO) system design. Giant planets in the HZ may even be within reach with the latest generation of high-contrast imagers for a handful of very nearby stars. Here we will review the definition of the HZ, and the characteristics of detectable planets there. We then review some of the ways that direct imaging in the HZ will be different from the typical exoplanet imaging survey today. Finally, we present preliminary results from our observations of the HZ of alpha Centauri A with the Magellan AO system's VisAO and Clio2 cameras. C1 [Males, Jared R.; Close, Laird M.; Guyon, Olivier; Morzinski, Katie; Hinz, Philip; Follette, Katherine B.; Wu, Ya-lin] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Puglisi, Alfio; Esposito, Simone; Riccardi, Armando; Xompero, Marco; Briguglio, Runa; Pinna, Enrico] Osserv Astrofis Arcetri, Inst Nazl Astrofis, Florence, Italy. [Monnier, John D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Tolls, Volker] Harvard Smithsonian, CfA, Boston, MA USA. [Rodigas, Timothy J.; Weinberger, Alycia; Boss, Alan] Carnegie Inst DTM, Washington, DC USA. [Kopon, Derek] MPiA Heidelberg, Heidelberg, Germany. RP Males, JR (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. EM jrmales@as.arizona.edu OI Esposito, Simone/0000-0002-3114-677X; Xompero, Marco/0000-0002-5565-084X; Pinna, Enrico/0000-0002-6243-5697; Riccardi, Armando/0000-0001-5460-2929; Morzinski, Katie/0000-0002-1384-0063; Rodigas, Timothy/0000-0002-7535-2997 NR 68 TC 4 Z9 4 U1 0 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-9616-4 J9 PROC SPIE PY 2014 VL 9148 AR 914820 DI 10.1117/12.2057135 PG 13 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA BC8OD UT WOS:000355930800059 ER PT S AU van Dam, MA Bouchez, AH McLeod, BA AF van Dam, Marcos A. Bouchez, Antonin H. McLeod, Brian A. BE Marchetti, E Close, LM Veran, JP TI Wide field adaptive optics correction for the GMT using natural guide stars SO ADAPTIVE OPTICS SYSTEMS IV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Adaptive Optics Systems IV CY JUN 22-27, 2014 CL Montreal, CANADA SP SPIE, American Astron Soc, Australian Astron Observatory, Assoc Univ Res Astron, Canadian Astron Soc, Canadian Space Agcy, European Astron Soc, European So Observatory, Natl Radio Astron Observatory, Royal Astron Soc, Sci & Technol Facilities Council DE Adaptive optics; Giant Magellan Telescope; ground layer adaptive optics; tomography; simulations AB The conceptual design of the Giant Magellan Telescope has four wavefront sensors used to maintain the shape and alignment of the segmented primary and secondary mirrors. In this paper, we show that by reading the sensors at 200 Hz, we can also compensate for low altitude turbulence. As a result, there is a large improvement in image quality, even at visible wavelengths, over the entire science field of view of the telescope. A minimum-variance reconstructor is presented that takes slope measurements from four stars of arbitrary location and magnitude and produces the optimal adaptive secondary mirror commands. The performance of the adaptive optics system in this mode is simulated using YAO, an end-to-end simulation tool. We present the results of trade studies performed to optimize the science return of the telescope. C1 [van Dam, Marcos A.] Flat Wavefronts, Christchurch 8140, New Zealand. [Bouchez, Antonin H.] Giant Magellan Telescope Observ Corp, Pasadena, CA 91109 USA. [McLeod, Brian A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP van Dam, MA (reprint author), Flat Wavefronts, POB 1060, Christchurch 8140, New Zealand. EM marcos@flatwavefronts.com NR 10 TC 3 Z9 3 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-9616-4 J9 PROC SPIE PY 2014 VL 9148 AR 914813 DI 10.1117/12.2054154 PG 12 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA BC8OD UT WOS:000355930800032 ER EF