FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Fischer, DA Anglada-Escude, G Arriagada, P Baluev, RV Bean, JL Bouchy, F Buchhave, LA Carroll, T Chakraborty, A Crepp, JR Dawson, RI Diddams, SA Dumusque, X Eastman, JD Endl, M Figueira, P Ford, EB Foreman-Mackey, D Fournier, P Furesz, G Gaudi, BS Gregory, PC Grundahl, F Hatzes, AP Hebrard, G Herrero, E Hogg, DW Howard, AW Johnson, JA Jorden, P Jurgenson, CA Latham, DW Laughlin, G Loredo, TJ Lovis, C Mahadevan, S McCracken, TM Pepe, F Perez, M Phillips, DF Plavchan, PP Prato, L Quirrenbach, A Reiners, A Robertson, P Santos, NC Sawyer, D Segransan, D Sozzetti, A Steinmetz, T Szentgyorgyi, A Udry, S Valenti, JA Wang, SX Wittenmyer, RA Wright, JT AF Fischer, Debra A. Anglada-Escude, Guillem Arriagada, Pamela Baluev, Roman V. Bean, Jacob L. Bouchy, Francois Buchhave, Lars A. Carroll, Thorsten Chakraborty, Abhijit Crepp, Justin R. Dawson, Rebekah I. Diddams, Scott A. Dumusque, Xavier Eastman, Jason D. Endl, Michael Figueira, Pedro Ford, Eric B. Foreman-Mackey, Daniel Fournier, Paul Furesz, Gabor Gaudi, B. Scott Gregory, Philip C. Grundahl, Frank Hatzes, Artie P. Hebrard, Guillaume Herrero, Enrique Hogg, David W. Howard, Andrew W. Johnson, John A. Jorden, Paul Jurgenson, Colby A. Latham, David W. Laughlin, Greg Loredo, Thomas J. Lovis, Christophe Mahadevan, Suvrath McCracken, Tyler M. Pepe, Francesco Perez, Mario Phillips, David F. Plavchan, Peter P. Prato, Lisa Quirrenbach, Andreas Reiners, Ansgar Robertson, Paul Santos, Nuno C. Sawyer, David Segransan, Damien Sozzetti, Alessandro Steinmetz, Tilo Szentgyorgyi, Andrew Udry, Stephane Valenti, Jeff A. Wang, Sharon X. Wittenmyer, Robert A. Wright, Jason T. TI State of the Field: Extreme Precision Radial Velocities SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE instrumentation: spectrographs; methods: observational; methods: statistical; techniques: radial velocities; techniques: spectroscopic ID EARTH-LIKE PLANETS; OPTICAL FREQUENCY COMB; FIBER-FED SPECTROGRAPH; PULSAR-TIMING PACKAGE; ORBITING HD 7924; SOLAR-TYPE STARS; LOW-MASS PLANETS; SUN-LIKE STAR; 1 CM S(-1); HIGH-RESOLUTION AB The Second Workshop on Extreme Precision Radial Velocities defined circa 2015 the state of the art Doppler precision and identified the critical path challenges for reaching 10 cm s(-1) measurement precision. The presentations and discussion of key issues for instrumentation and data analysis and the workshop recommendations for achieving this bold precision are summarized here. Beginning with the High Accuracy Radial Velocity Planet Searcher spectrograph, technological advances for precision radial velocity (RV) measurements have focused on building extremely stable instruments. To reach still higher precision, future spectrometers will need to improve upon the state of the art, producing even higher fidelity spectra. This should be possible with improved environmental control, greater stability in the illumination of the spectrometer optics, better detectors, more precise wavelength calibration, and broader bandwidth spectra. Key data analysis challenges for the precision RV community include distinguishing center of mass (COM) Keplerian motion from photospheric velocities (time correlated noise) and the proper treatment of telluric contamination. Success here is coupled to the instrument design, but also requires the implementation of robust statistical and modeling techniques. COM velocities produce Doppler shifts that affect every line identically, while photospheric velocities produce line profile asymmetries with wavelength and temporal dependencies that are different from Keplerian signals. Exoplanets are an important subfield of astronomy and there has been an impressive rate of discovery over the past two decades. However, higher precision RV measurements are required to serve as a discovery technique for potentially habitable worlds, to confirm and characterize detections from transit missions, and to provide mass measurements for other space-based missions. The future of exoplanet science has very different trajectories depending on the precision that can ultimately be achieved with Doppler measurements. C1 [Fischer, Debra A.; Jurgenson, Colby A.; McCracken, Tyler M.; Sawyer, David] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Anglada-Escude, Guillem] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Coll Lane, Hatfield AL10 9AB, Herts, England. [Anglada-Escude, Guillem] Queen Mary Univ London, Sch Phys & Astron, 327 Mile End Rd, London E1 4NS, England. [Arriagada, Pamela] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Baluev, Roman V.] Russian Acad Sci, Cent Astron Observ Pulkovo, Pulkovskoje Shosse 65, St Petersburg 196140, Russia. [Baluev, Roman V.] St Petersburg State Univ, Sobolev Astron Inst, Univ Skij Prospekt 28, St Petersburg 198504, Russia. [Bean, Jacob L.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Bouchy, Francois] Aix Marseille Univ, CNRS, UMR 7326, LAM, F-13388 Marseille, France. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. [Carroll, Thorsten] Leibniz Inst Astrophys Potsdam, Sternwarte 16, D-14482 Potsdam, Germany. [Chakraborty, Abhijit] PRL, Astron & Astrophys Div, Ahmadabad 380009, Gujarat, India. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, South Bend, IN USA. [Dawson, Rebekah I.; Ford, Eric B.; Mahadevan, Suvrath; Robertson, Paul; Wang, Sharon X.; Wright, Jason T.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Dawson, Rebekah I.; Ford, Eric B.; Mahadevan, Suvrath; Robertson, Paul; Wang, Sharon X.; Wright, Jason T.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Diddams, Scott A.] NIST, 325 Broadway, Boulder, CO 80305 USA. [Diddams, Scott A.] Univ Colorado, Dept Phys, 2000 Colorado Ave, Boulder, CO 80309 USA. [Dumusque, Xavier; Lovis, Christophe; Pepe, Francesco; Segransan, Damien; Udry, Stephane] Univ Geneva, Astron Observ, 51 Chemin Maillettes, CH-1290 Versoix, Switzerland. [Eastman, Jason D.; Johnson, John A.; Latham, David W.; Phillips, David F.; Szentgyorgyi, Andrew] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Endl, Michael] Univ Texas Austin, 2515 Speedway,C1400, Austin, TX 78712 USA. [Endl, Michael] Dept Astron, 2515 Speedway,C1400, Austin, TX 78712 USA. [Endl, Michael] McDonald Observ, 2515 Speedway,C1400, Austin, TX 78712 USA. [Figueira, Pedro; Santos, Nuno C.] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, Rua Estrelas, P-4150762 Oporto, Portugal. [Foreman-Mackey, Daniel; Hogg, David W.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Foreman-Mackey, Daniel] Univ Washington, Dept Astron, Box 951580, Seattle, WA 98195 USA. [Fournier, Paul] Fibertech Opt Inc, Kitchener, ON N2M 5C6, Canada. [Furesz, Gabor] MIT, Kavli Inst Astrophys & Space Res, 77 Mass Ave,37-515, Cambridge, MA 02139 USA. [Gaudi, B. Scott] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. [Gregory, Philip C.] Univ British Columbia, Phys & Astron, 6244 Agr Rd, Vancouver, BC V6T 1Z1, Canada. [Grundahl, Frank] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Hatzes, Artie P.] Thuringer Landessternwarte, Sternwarte 5,Tautenburg 5, D-07778 Tautenburg, Germany. [Hebrard, Guillaume] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, 98Bis Blvd Arago, F-75014 Paris, France. [Hebrard, Guillaume] Univ Aix Marseille, Observ Haute Provence, F-04870 St Michel Lobservatoire, France. [Hebrard, Guillaume] CNRS, F-04870 St Michel Lobservatoire, France. [Herrero, Enrique] Fac Ciencies, Inst Ciencies Espai CSICIEEC, Campus UAB,Torre C5 Parell,2a Pl, E-08193 Bellaterra, Spain. [Hogg, David W.] NYU, Ctr Data Sci, New York, NY 10003 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Jorden, Paul] E2v Technol, 106 Waterhouse Lane, Chelmsford, Essex, England. [Laughlin, Greg] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Loredo, Thomas J.] Cornell Univ, Ctr Radiophys & Space Res, Space Sci Bldg, Ithaca, NY 14853 USA. [Mahadevan, Suvrath; Wright, Jason T.] Penn State Univ, Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA. [Perez, Mario] NASA Headquarters, Washington, DC USA. [Plavchan, Peter P.] Missouri State Univ, Dept Phys Astron & Mat Sci, 901 S Natl Ave, Springfield, MO 65897 USA. [Prato, Lisa] Lowell Observ, 1400 West Mars Hill, Flagstaff, AZ 86001 USA. [Quirrenbach, Andreas] Heidelberg Univ, Zentrum Astron, Landessternwarte, Konigstuhl 12, D-69117 Heidelberg, Germany. [Reiners, Ansgar] Georg August Univ, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany. [Santos, Nuno C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, Rua Campo Alegre, P-4169007 Oporto, Portugal. [Sozzetti, Alessandro] Osservatorio Astrofis Torino, INAF, Via Osservatorio 20, I-10025 Pino Torinese, Italy. [Steinmetz, Tilo] Menlo Syst GmbH, Klopferspitz 19a, D-82152 Martinsried, Germany. [Valenti, Jeff A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Wittenmyer, Robert A.] Univ New South Wales, Sch Phys, Sydney, NSW 2052, Australia. [Wittenmyer, Robert A.] Univ New South Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Wittenmyer, Robert A.] Univ Southern Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. RP Fischer, DA (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA. EM debra.fischer@yale.edu RI Baluev, Roman/H-3312-2013; Figueira, Pedro/J-4916-2013; OI Baluev, Roman/0000-0001-9535-3965; Figueira, Pedro/0000-0001-8504-283X; Wright, Jason/0000-0001-6160-5888; Anglada Escude, Guillem/0000-0002-3645-5977 FU Yale University; National Science Foundation [AST-1458915, AST-1313075]; NASA Exoplanet Science Institute (NExScI); NIST; NSF [AST-1310875, AST-1211441, AST1109727]; Society in Science; NASA [NNX15AE21G, NNX14AN81H, NNX12AC01G]; NSF CAREER [AST-1056524]; NASA Astrobiology Institute; NASA TESS Mission; European Research Council [279347]; DFG [RE 1664/9-1]; Fundacao para a Ciencia e a Tecnologia (FCT) [UID/FIS/04434/2013, PTDC/FIS-AST/1526/2014]; FCT [IF/01037/2013, IF/00169/2012, IF/01037/2013CP1191/CT0001]; POPH/FSE (EC) by FEDER through the program "Programa Operacional de Factores de Competitividade-COMPETE"; Giant Magellan Telescope Organization [GMT-INS-CON-00584]; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; Department of Space, Govt. of India; Physical Research Laboratory (PRL), Ahmedabed, India; Centre of Exoplanets and Habitable Worlds at Penn State University; NASA FX We thank the anonymous referee for providing an exceptionally careful review of this paper and for many suggested changes which improved the quality of the paper. We are grateful to Yale University, to the National Science Foundation grant AST-1458915 and to the NASA Exoplanet Science Institute (NExScI) for providing financial support that enabled this workshop and provided support for participants. D.A.F. thanks NASA NNX12ACG01 C for inspiring the study of extreme precision RV measurements. R.I.D. acknowledges the Miller Institute at the Univ of California, Berkeley for Basic Research in Science. S.A.D. acknowledges support from NIST and the NSF grant AST-1310875. X.D. would like to thank the Society in Science for its support through a Branco Weiss Fellowship. E.B.F. was supported in part by NASA Exoplanet Research Program award NNX15AE21G. Work by B.S.G. was partially supported by NSF CAREER Grant AST-1056524. G.L. acknowledges support from the NASA Astrobiology Institute through a cooperative agreement between NASA Ames Research Center and the University of California at Santa Cruz, and from the NASA TESS Mission through a cooperative agreement between M.I.T. and UCSC. A.R. acknowledges support from the European Research Council under the FP7 Starting Grant agreement number 279347 and from DFG grant RE 1664/9-1. N.C.S. and P.F. acknowledge support by Fundacao para a Ciencia e a Tecnologia (FCT) through the research grants UID/FIS/04434/2013 and PTDC/FIS-AST/1526/2014 as well as through Investigador FCT contracts of reference IF/01037/2013 and IF/00169/2012, and POPH/FSE (EC) by FEDER funding through the program "Programa Operacional de Factores de Competitividade-COMPETE." P.F. further acknowledges support from FCT in the form of an exploratory project reference IF/01037/2013CP1191/CT0001. A.S. thanks the Giant Magellan Telescope Organization for their support for much the work described in his contribution to this paper under Contract No. GMT-INS-CON-00584. S.X.W. is supported by a NASA Earth and Space Science Fellowship (NNX14AN81H). S.X.W. and J.T.W. acknowledge support from NSF grant AST-1211441 for the work on telluric contamination. J.T.W. acknowledges NSF grant AST1109727 and NASA grant NNX12AC01G for work on barycentric corrections. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. The PARAS program is fully supported and funded by the Department of Space, Govt. of India and Physical Research Laboratory (PRL), Ahmedabed, India. The PARAS team would like to acknowledge the support of the Director, PRL, and the Mt. Abu Observatory staff for running the program and Francesco Pepe (Geneva Observatory) and Larry Ramsey (Pen State University) for many scientific and technical inputs. Two of the PARAS team members, Suvrath Mahadevan and Arpita Roy would like to thank the Centre of Exoplanets and Habitable Worlds at Penn State University for their partial support. The McDonald Observatory planet search is currently supported by the National Science Foundation under Astrophysics grant AST-1313075, and has been supported in the past by various NASA grants. NR 231 TC 13 Z9 13 U1 9 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUN PY 2016 VL 128 IS 964 AR 066001 DI 10.1088/1538-3873/128/964/066001 PG 43 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB1KP UT WOS:000387110500005 ER PT J AU Annis, J Soares-Santos, M Berger, E Brout, D Chen, H Chornock, R Cowperthwaite, PS Diehl, HT Doctor, Z Drlica-Wagner, A Drout, MR Farr, B Finley, DA Flaugher, B Foley, RJ Frieman, J Gruendl, RA Herner, K Holz, D Kessler, R Lin, H Marriner, J Neilsen, E Rest, A Sako, M Smith, M Smith, N Sobreira, F Walker, AR Yanny, B Abbott, TMC Abdalla, FB Allam, S Benoit-Levy, A Bernstein, RA Bertin, E Buckley-Geer, E Burke, DL Capozzi, D Rosell, AC Kind, MC Carretero, J Castander, FJ Cenko, SB Crocce, M Cunha, CE D'Andrea, CB da Costa, LN Desai, S Dietrich, JP Eifler, TF Evrard, AE Fernandez, E Fischer, J Fong, W Fosalba, P Fox, DB Fryer, CL Garcia-Bellido, J Gaztanaga, E Gerdes, DW Goldstein, DA Gruen, D Gutierrez, G Honscheid, K James, DJ Karliner, I Kasen, D Kent, S Kuehn, K Kuropatkin, N Lahav, O Li, TS Lima, M Maia, MAG Martini, P Metzger, BD Miller, CJ Miquel, R Mohr, JJ Nichol, RC Nord, B Ogando, R Peoples, J Petravic, D Plazas, AA Quataert, E Romer, AK Roodman, A Rykoff, ES Sanchez, E Santiago, B Scarpine, V Schindler, R Schubnell, M Sevilla-Noarbe, I Sheldon, E Smith, RC Stebbins, A Swanson, MEC Tarle, G Thaler, J Thomas, RC Tucker, DL Vikram, V Wechsler, RH Weller, J Wester, W AF Annis, J. Soares-Santos, M. Berger, E. Brout, D. Chen, H. Chornock, R. Cowperthwaite, P. S. Diehl, H. T. Doctor, Z. Drlica-Wagner, A. Drout, M. R. Farr, B. Finley, D. A. Flaugher, B. Foley, R. J. Frieman, J. Gruendl, R. A. Herner, K. Holz, D. Kessler, R. Lin, H. Marriner, J. Neilsen, E. Rest, A. Sako, M. Smith, M. Smith, N. Sobreira, F. Walker, A. R. Yanny, B. Abbott, T. M. C. Abdalla, F. B. Allam, S. Benoit-Levy, A. Bernstein, R. A. Bertin, E. Buckley-Geer, E. Burke, D. L. Capozzi, D. Carnero Rosell, A. Kind, M. Carrasco Carretero, J. Castander, F. J. Cenko, S. B. Crocce, M. Cunha, C. E. D'Andrea, C. B. da Costa, L. N. Desai, S. Dietrich, J. P. Eifler, T. F. Evrard, A. E. Fernandez, E. Fischer, J. Fong, W. Fosalba, P. Fox, D. B. Fryer, C. L. Garcia-Bellido, J. Gaztanaga, E. Gerdes, D. W. Goldstein, D. A. Gruen, D. Gutierrez, G. Honscheid, K. James, D. J. Karliner, I. Kasen, D. Kent, S. Kuehn, K. Kuropatkin, N. Lahav, O. Li, T. S. Lima, M. Maia, M. A. G. Martini, P. Metzger, B. D. Miller, C. J. Miquel, R. Mohr, J. J. Nichol, R. C. Nord, B. Ogando, R. Peoples, J. Petravic, D. Plazas, A. A. Quataert, E. Romer, A. K. Roodman, A. Rykoff, E. S. Sanchez, E. Santiago, B. Scarpine, V. Schindler, R. Schubnell, M. Sevilla-Noarbe, I. Sheldon, E. Smith, R. C. Stebbins, A. Swanson, M. E. C. Tarle, G. Thaler, J. Thomas, R. C. Tucker, D. L. Vikram, V. Wechsler, R. H. Weller, J. Wester, W. CA DES Collaboration TI A DARK ENERGY CAMERA SEARCH FOR MISSING SUPERGIANTS IN THE LMC AFTER THE ADVANCED LIGO GRAVITATIONAL-WAVE EVENT GW150914 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: individual (LMC); gravitational waves; Magellanic Clouds; supergiants; supernovae: general ID LARGE-MAGELLANIC-CLOUD; CORE-COLLAPSE SUPERNOVAE; MASSIVE STARS; FAILED SUPERNOVAE; NEUTRINO BURST; CONSTRAINTS; I. AB The collapse of a stellar core is expected to produce gravitational waves (GWs), neutrinos, and in most cases a luminous supernova. Sometimes, however, the optical event could be significantly less luminous than a supernova and a direct collapse to a black hole, where the star just disappears, is possible. The GW event GW150914 was detected by the LIGO Virgo Collaboration via a burst analysis that gave localization contours enclosing the Large Magellanic Cloud (LMC). Shortly thereafter, we used DECam to observe 102 deg(2) of the localization area, including 38 deg(2) on the LMC for a missing supergiant search. We construct a complete catalog of LMC luminous red supergiants, the best candidates to undergo invisible core collapse, and collected catalogs of other candidates: less luminous red supergiants, yellow supergiants, blue supergiants, luminous blue variable stars, and Wolf-Rayet stars. Of the objects in the imaging region, all are recovered in the images. The timescale for stellar disappearance is set by the free-fall time, which is a function of the stellar radius. Our observations at 4 and 13 days after the event result in a search sensitive to objects of up to about 200 solar radii. We conclude that it is unlikely that GW150914 was caused by the core collapse of a relatively compact supergiant in the LMC, consistent with the LIGO Collaboration analyses of the gravitational waveform as best interpreted as a high mass binary black hole merger. We discuss how to generalize this search for future very nearby core-collapse candidates. C1 [Annis, J.; Soares-Santos, M.; Diehl, H. T.; Drlica-Wagner, A.; Finley, D. A.; Flaugher, B.; Frieman, J.; Herner, K.; Lin, H.; Marriner, J.; Neilsen, E.; Yanny, B.; Allam, S.; Buckley-Geer, E.; Gutierrez, G.; Kent, S.; Kuropatkin, N.; Nord, B.; Peoples, J.; Scarpine, V.; Stebbins, A.; Tucker, D. L.; Wester, W.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Berger, E.; Cowperthwaite, P. S.; Drout, M. R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Brout, D.; Sako, M.; Eifler, T. F.; Fischer, J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Chen, H.; Doctor, Z.; Farr, B.; Frieman, J.; Holz, D.; Kessler, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Chornock, R.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, 251B Clippinger Lab, Athens, OH 45701 USA. [Foley, R. J.; Gruendl, R. A.; Kind, M. Carrasco; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Foley, R. J.; Karliner, I.; Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. [Gruendl, R. A.; Kind, M. Carrasco; Petravic, D.; Swanson, M. E. C.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Rest, A.] STScI, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Smith, M.; D'Andrea, C. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Smith, N.; Fong, W.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Sobreira, F.] Univ Estadual Paulista, Inst Fis Teor, Rua Dr Bento T Ferraz 271, BR-01140070 Sao Paulo, SP, Brazil. [Walker, A. R.; Abbott, T. M. C.; James, D. J.; Smith, R. C.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile. [Abdalla, F. B.; Benoit-Levy, A.; Lahav, O.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Benoit-Levy, A.; Bertin, E.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Benoit-Levy, A.; Bertin, E.] Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Bernstein, R. A.] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Burke, D. L.; Cunha, C. E.; Gruen, D.; Roodman, A.; Rykoff, E. S.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Burke, D. L.; Gruen, D.; Roodman, A.; Rykoff, E. S.; Schindler, R.; Wechsler, R. H.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Capozzi, D.; D'Andrea, C. B.; Nichol, R. C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Carnero Rosell, A.; da Costa, L. N.; Lima, M.; Maia, M. A. G.; Ogando, R.; Santiago, B.] Lab Interinst & Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carretero, J.; Castander, F. J.; Crocce, M.; Fosalba, P.; Gaztanaga, E.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain. [Carretero, J.; Fernandez, E.; Miquel, R.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA. [Cenko, S. B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Desai, S.; Dietrich, J. P.; Mohr, J. J.; Weller, J.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Evrard, A. E.; Gerdes, D. W.; Miller, C. J.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Fox, D. B.] Penn State Univ, Ctr Particle & Gravitat Astrophys, University Pk, PA 16802 USA. [Fox, D. B.] Penn State Univ, Ctr Theoret & Observat Cosmol, University Pk, PA 16802 USA. [Fryer, C. L.] Los Alamos Natl Lab, CCS Div, POB 1663, Los Alamos, NM 87545 USA. [Garcia-Bellido, J.; Sanchez, E.; Sevilla-Noarbe, I.] CIEMAT, E-28040 Madrid, Spain. [Goldstein, D. A.] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA. [Goldstein, D. A.; Kasen, D.; Thomas, R. C.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Honscheid, K.; Martini, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA. [Kasen, D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Kasen, D.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Li, T. S.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Li, T. S.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil. [Martini, P.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. [Metzger, B. D.] Columbia Univ, Columbia Astrophys Lab, Pupin Hall, New York, NY 10027 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Mohr, J. J.; Weller, J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Quataert, E.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Quataert, E.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Santiago, B.] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil. [Sheldon, E.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA. [Wechsler, R. H.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Weller, J.] Univ Munich, Fak Phys, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany. RP Annis, J (reprint author), Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. RI Ogando, Ricardo/A-1747-2010; Lima, Marcos/E-8378-2010; Sobreira, Flavia/F-4168-2015; Fernandez, Enrique/L-5387-2014; OI Ogando, Ricardo/0000-0003-2120-1154; Sobreira, Flavia/0000-0002-7822-0658; Fernandez, Enrique/0000-0002-6405-9488; Weller, Jochen/0000-0002-8282-2010; Gaztanaga, Enrique/0000-0001-9632-0815; Soares-Santos, Marcelle/0000-0001-6082-8529; Abdalla, Filipe/0000-0003-2063-4345; Garcia-Bellido, Juan/0000-0002-9370-8360 FU U.S. Department of Energy; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat Munchen; associated Excellence Cluster Universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford University; University of Sussex; Texas AM University; National Science Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Research Council under the European Union, ERC [240672, 291329, 306478]; NSF [AST-1518052]; Alfred P. Sloan Foundation; So Paulo Research Foundation (FAPESP) [2015/12338-1] FX Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey.r The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University.r The DES data management system is supported by the National Science Foundation under grant number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the European Research Council under the European Unions Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478.r R.J.F. gratefully acknowledges support from NSF grant AST-1518052 and the Alfred P. Sloan Foundation. F.S. acknowledges financial support provided by So Paulo Research Foundation (FAPESP) under grants 2015/12338-1. NR 44 TC 6 Z9 6 U1 3 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 JUN 1 PY 2016 VL 823 IS 2 AR L34 DI 10.3847/2041-8205/823/2/L34 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN4JL UT WOS:000377031700013 ER PT J AU Annis, J Soares-Santos, M Berger, E Brout, D Chen, H Chornock, R Cowperthwaite, PS Diehl, HT Doctor, Z Drlica-Wagner, A Drout, MR Farr, B Finley, DA Flaugher, B Foley, RJ Frieman, J Gruendl, RA Herner, K Holz, D Kessler, R Lin, H Marriner, J Neilsen, E Rest, A Sako, M Smith, M Smith, N Sobreira, F Walker, AR Yanny, B Abbott, TMC Abdalla, FB Allam, S Benoit-Levy, A Bernstein, RA Bertin, E Buckley-Geer, E Burke, DL Capozzi, D Rosell, AC Kind, MC Carretero, J Castander, FJ Cenko, SB Crocce, M Cunha, CE D'Andrea, CB da Costa, LN Desai, S Dietrich, JP Eifler, TF Evrard, AE Fernandez, E Fischer, J Fong, W Fosalba, P Fox, DB Fryer, CL Garcia-Bellido, J Gaztanaga, E Gerdes, DW Goldstein, DA Gruen, D Gutierrez, G Honscheid, K James, DJ Karliner, I Kasen, D Kent, S Kuehn, K Kuropatkin, N Lahav, O Li, TS Lima, M Maia, MAG Martini, P Metzger, BD Miller, CJ Miquel, R Mohr, JJ Nichol, RC Nord, B Ogando, R Peoples, J Petravic, D Plazas, AA Quataert, E Romer, AK Roodman, A Rykoff, ES Sanchez, E Santiago, B Scarpine, V Schindler, R Schubnell, M Sevilla-Noarbe, I Sheldon, E Smith, RC Stebbins, A Swanson, MEC Tarle, G Thaler, J Thomas, RC Tucker, DL Vikram, V Wechsler, RH Weller, J Wester, W AF Annis, J. Soares-Santos, M. Berger, E. Brout, D. Chen, H. Chornock, R. Cowperthwaite, P. S. Diehl, H. T. Doctor, Z. Drlica-Wagner, A. Drout, M. R. Farr, B. Finley, D. A. Flaugher, B. Foley, R. J. Frieman, J. Gruendl, R. A. Herner, K. Holz, D. Kessler, R. Lin, H. Marriner, J. Neilsen, E. Rest, A. Sako, M. Smith, M. Smith, N. Sobreira, F. Walker, A. R. Yanny, B. Abbott, T. M. C. Abdalla, F. B. Allam, S. Benoit-Levy, A. Bernstein, R. A. Bertin, E. Buckley-Geer, E. Burke, D. L. Capozzi, D. Carnero Rosell, A. Carrasco Kind, M. Carretero, J. Castander, F. J. Cenko, S. B. Crocce, M. Cunha, C. E. D'Andrea, C. B. da Costa, L. N. Desai, S. Dietrich, J. P. Eifler, T. F. Evrard, A. E. Fernandez, E. Fischer, J. Fong, W. Fosalba, P. Fox, D. B. Fryer, C. L. Garcia-Bellido, J. Gaztanaga, E. Gerdes, D. W. Goldstein, D. A. Gruen, D. Gutierrez, G. Honscheid, K. James, D. J. Karliner, I. Kasen, D. Kent, S. Kuehn, K. Kuropatkin, N. Lahav, O. Li, T. S. Lima, M. Maia, M. A. G. Martini, P. Metzger, B. D. Miller, C. J. Miquel, R. Mohr, J. J. Nichol, R. C. Nord, B. Ogando, R. Peoples, J. Petravic, D. Plazas, A. A. Quataert, E. Romer, A. K. Roodman, A. Rykoff, E. S. Sanchez, E. Santiago, B. Scarpine, V. Schindler, R. Schubnell, M. Sevilla-Noarbe, I. Sheldon, E. Smith, R. C. Stebbins, A. Swanson, M. E. C. Tarle, G. Thaler, J. Thomas, R. C. Tucker, D. L. Vikram, V. Wechsler, R. H. Weller, J. Wester, W. CA DES Collaboration TI A DARK ENERGY CAMERA SEARCH FOR MISSING SUPERGIANTS IN THE LMC AFTER THE ADVANCED LIGO GRAVITATIONAL-WAVE EVENT GW150914 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: individual (LMC); gravitational waves; Magellanic Clouds; supergiants; supernovae: general ID LARGE-MAGELLANIC-CLOUD; CORE-COLLAPSE SUPERNOVAE; WOLF-RAYET STARS; MASSIVE STARS; FAILED SUPERNOVAE; NEUTRINO BURST; CONSTRAINTS; I. AB The collapse of a stellar core is expected to produce gravitational waves (GWs), neutrinos, and in most cases a luminous supernova. Sometimes, however, the optical event could be significantly less luminous than a supernova and a direct collapse to a black hole, where the star just disappears, is possible. The GW event GW150914 was detected by the LIGO Virgo Collaboration via a burst analysis that gave localization contours enclosing the Large Magellanic Cloud (LMC). Shortly thereafter, we used DECam to observe 102 deg(2) of the localization area, including 38 deg(2) on the LMC for a missing supergiant search. We construct a complete catalog of LMC luminous red supergiants, the best candidates to undergo invisible core collapse, and collected catalogs of other candidates: less luminous red supergiants, yellow supergiants, blue supergiants, luminous blue variable stars, and Wolf-Rayet stars. Of the objects in the imaging region, all are recovered in the images. The timescale for stellar disappearance is set by the free-fall time, which is a function of the stellar radius. Our observations at 4 and 13 days after the event result in a search sensitive to objects of up to about 200 solar radii. We conclude that it is unlikely that GW150914 was caused by the core collapse of a relatively compact supergiant in the LMC, consistent with the LIGO Collaboration analyses of the gravitational waveform as best interpreted as a high mass binary black hole merger. We discuss how to generalize this search for future very nearby core-collapse candidates. C1 [Annis, J.; Soares-Santos, M.; Diehl, H. T.; Drlica-Wagner, A.; Finley, D. A.; Flaugher, B.; Frieman, J.; Herner, K.; Lin, H.; Marriner, J.; Neilsen, E.; Yanny, B.; Allam, S.; Buckley-Geer, E.; Gutierrez, G.; Kent, S.; Kuropatkin, N.; Nord, B.; Peoples, J.; Scarpine, V.; Stebbins, A.; Tucker, D. L.; Wester, W.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Berger, E.; Cowperthwaite, P. S.; Drout, M. R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Brout, D.; Sako, M.; Eifler, T. F.; Fischer, J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Chen, H.; Doctor, Z.; Farr, B.; Frieman, J.; Holz, D.; Kessler, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Chen, H.; Doctor, Z.; Farr, B.; Frieman, J.; Holz, D.; Kessler, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Chornock, R.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Clippinger Lab 251B, Athens, OH 45701 USA. [Foley, R. J.; Gruendl, R. A.; Carrasco Kind, M.; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Foley, R. J.; Karliner, I.; Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. [Gruendl, R. A.; Carrasco Kind, M.; Petravic, D.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Rest, A.] STScI, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Smith, M.; D'Andrea, C. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Smith, N.; Fong, W.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Sobreira, F.] Univ Estadual Paulista, Inst Fis Teor, Rua Dr Bento T Ferraz 271, BR-01140070 Sao Paulo, SP, Brazil. [Walker, A. R.; Abbott, T. M. C.; James, D. J.; Smith, R. C.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. [Abdalla, F. B.; Benoit-Levy, A.; Lahav, O.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Benoit-Levy, A.; Bertin, E.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Benoit-Levy, A.; Bertin, E.] UPMC Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Bernstein, R. A.] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Burke, D. L.; Cunha, C. E.; Gruen, D.; Roodman, A.; Rykoff, E. S.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Burke, D. L.; Gruen, D.; Roodman, A.; Rykoff, E. S.; Schindler, R.; Wechsler, R. H.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Capozzi, D.; D'Andrea, C. B.; Nichol, R. C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Carnero Rosell, A.; da Costa, L. N.; Lima, M.; Maia, M. A. G.; Ogando, R.; Santiago, B.] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carretero, J.; Castander, F. J.; Crocce, M.; Fosalba, P.; Gaztanaga, E.] CSIC, IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain. [Carretero, J.; Fernandez, E.; Miquel, R.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA. [Cenko, S. B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Desai, S.; Dietrich, J. P.; Mohr, J. J.; Weller, J.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Evrard, A. E.; Gerdes, D. W.; Miller, C. J.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fox, D. B.] Penn State Univ, Ctr Particle & Gravitat Astrophys, University Pk, PA 16802 USA. [Fox, D. B.] Penn State Univ, Ctr Theoret & Observat Cosmol, University Pk, PA 16802 USA. [Fryer, C. L.] Los Alamos Natl Lab, CCS Div, Los Alamos, NM 87545 USA. [Garcia-Bellido, J.; Sanchez, E.; Sevilla-Noarbe, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain. [Goldstein, D. A.] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA. [Goldstein, D. A.; Kasen, D.; Thomas, R. C.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Honscheid, K.; Martini, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Kasen, D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Kasen, D.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Li, T. S.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Li, T. S.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil. [Martini, P.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. [Metzger, B. D.] Columbia Astrophys Lab, Pupin Hall, New York, NY 10027 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Mohr, J. J.; Weller, J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Quataert, E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Quataert, E.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Santiago, B.] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil. [Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA. [Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA. [Wechsler, R. H.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Weller, J.] Ludwig Maximilians Univ Munchen, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany. RP Annis, J (reprint author), Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. RI Ogando, Ricardo/A-1747-2010; Lima, Marcos/E-8378-2010; Sobreira, Flavia/F-4168-2015; Fernandez, Enrique/L-5387-2014; OI Ogando, Ricardo/0000-0003-2120-1154; Sobreira, Flavia/0000-0002-7822-0658; Fernandez, Enrique/0000-0002-6405-9488; Weller, Jochen/0000-0002-8282-2010; Gaztanaga, Enrique/0000-0001-9632-0815; Soares-Santos, Marcelle/0000-0001-6082-8529; Abdalla, Filipe/0000-0003-2063-4345; Garcia-Bellido, Juan/0000-0002-9370-8360 FU U.S. Department of Energy; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas; Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat Munchen; associated Excellence Cluster Universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford University; University of Sussex; Texas AM University; National Science Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Research Council under the European Union [240672, 291329, 306478]; NSF [AST-1518052]; Alfred P. Sloan Foundation; So Paulo Research Foundation (FAPESP) [2015/12338-1] FX Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey.; The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University.; The DES data management system is supported by the National Science Foundation under grant number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the European Research Council under the European Unions Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478.; R.J.F. gratefully acknowledges support from NSF grant AST-1518052 and the Alfred P. Sloan Foundation. F.S. acknowledges financial support provided by So Paulo Research Foundation (FAPESP) under grants 2015/12338-1. NR 43 TC 6 Z9 6 U1 3 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 JUN 1 PY 2016 VL 823 IS 2 AR L34 DI 10.3847/2041-8205/823/2/L34 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ3WH UT WOS:000385779800002 ER PT J AU Soares-Santos, M Kessler, R Berger, E Annis, J Brout, D Buckley-Geer, E Chen, H Cowperthwaite, PS Diehl, HT Doctor, Z Drlica-Wagner, A Farr, B Finley, DA Flaugher, B Foley, RJ Frieman, J Gruendl, RA Herner, K Holz, D Lin, H Marriner, J Neilsen, E Rest, A Sako, M Scolnic, D Sobreira, F Walker, AR Wester, W Yanny, B Abbott, TMC Abdalla, FB Allam, S Armstrong, R Banerji, M Benoit-Levy, A Bernstein, RA Bertin, E Brown, DA Burke, DL Capozzi, D Rosell, AC Kind, MC Carretero, J Castander, FJ Cenko, SB Chornock, R Crocce, M D'Andrea, CB da Costa, LN Desai, S Dietrich, JP Drout, MR Eifler, TF Estrada, J Evrard, AE Fairhurst, S Fernandez, E Fischer, J Fong, W Fosalba, P Fox, DB Fryer, CL Garcia-Bellido, J Gaztanaga, E Gerdes, DW Goldstein, DA Gruen, D Gutierrez, G Honscheid, K James, DJ Karliner, I Kasen, D Kent, S Kuropatkin, N Kuehn, K Lahav, O Li, TS Lima, M Maia, MAG Margutti, R Martini, P Matheson, T McMahon, RG Metzger, BD Miller, CJ Miquel, R Mohr, JJ Nichol, RC Nord, B Ogando, R Peoples, J Plazas, AA Quataert, E Romer, AK Roodman, A Rykoff, ES Sanchez, E Scarpine, V Schindler, R Schubnell, M Sevilla-Noarbe, I Sheldon, E Smith, M Smith, N Smith, RC Stebbins, A Sutton, PJ Swanson, MEC Tarle, G Thaler, J Thomas, RC Tucker, DL Vikram, V Wechsler, RH Weller, J AF Soares-Santos, M. Kessler, R. Berger, E. Annis, J. Brout, D. Buckley-Geer, E. Chen, H. Cowperthwaite, P. S. Diehl, H. T. Doctor, Z. Drlica-Wagner, A. Farr, B. Finley, D. A. Flaugher, B. Foley, R. J. Frieman, J. Gruendl, R. A. Herner, K. Holz, D. Lin, H. Marriner, J. Neilsen, E. Rest, A. Sako, M. Scolnic, D. Sobreira, F. Walker, A. R. Wester, W. Yanny, B. Abbott, T. M. C. Abdalla, F. B. Allam, S. Armstrong, R. Banerji, M. Benoit-Levy, A. Bernstein, R. A. Bertin, E. Brown, D. A. Burke, D. L. Capozzi, D. Carnero Rosell, A. Carrasco Kind, M. Carretero, J. Castander, F. J. Cenko, S. B. Chornock, R. Crocce, M. D'Andrea, C. B. da Costa, L. N. Desai, S. Dietrich, J. P. Drout, M. R. Eifler, T. F. Estrada, J. Evrard, A. E. Fairhurst, S. Fernandez, E. Fischer, J. Fong, W. Fosalba, P. Fox, D. B. Fryer, C. L. Garcia-Bellido, J. Gaztanaga, E. Gerdes, D. W. Goldstein, D. A. Gruen, D. Gutierrez, G. Honscheid, K. James, D. J. Karliner, I. Kasen, D. Kent, S. Kuropatkin, N. Kuehn, K. Lahav, O. Li, T. S. Lima, M. Maia, M. A. G. Margutti, R. Martini, P. Matheson, T. McMahon, R. G. Metzger, B. D. Miller, C. J. Miquel, R. Mohr, J. J. Nichol, R. C. Nord, B. Ogando, R. Peoples, J. Plazas, A. A. Quataert, E. Romer, A. K. Roodman, A. Rykoff, E. S. Sanchez, E. Scarpine, V. Schindler, R. Schubnell, M. Sevilla-Noarbe, I. Sheldon, E. Smith, M. Smith, N. Smith, R. C. Stebbins, A. Sutton, P. J. Swanson, M. E. C. Tarle, G. Thaler, J. Thomas, R. C. Tucker, D. L. Vikram, V. Wechsler, R. H. Weller, J. CA DES Collaboration TI A DARK ENERGY CAMERA SEARCH FOR AN OPTICAL COUNTERPART TO THE FIRST ADVANCED LIGO GRAVITATIONAL WAVE EVENT GW150914 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: close; catalogs; gravitational waves; stars: neutron; surveys ID RADIOACTIVELY POWERED TRANSIENTS; NEUTRON-STAR MERGERS; EMISSION; VIRGO AB We report the results of a deep search for an optical counterpart to the gravitational wave (GW) event GW150914, the first trigger from the Advanced LIGO GW detectors. We used the Dark Energy Camera (DECam) to image a 102 deg(2) area, corresponding to 38% of the initial trigger high-probability sky region and to 11% of the revised high-probability region. We observed in the i and z bands at 4-5, 7, and 24 days after the trigger. The median 5 sigma point-source limiting magnitudes of our search images are i = 22.5 and z = 21.8 mag. We processed the images through a difference-imaging pipeline using templates from pre-existing Dark Energy Survey data and publicly available DECam data. Due to missing template observations and other losses, our effective search area subtends 40 deg(2), corresponding to a 12% total probability in the initial map and 3% in the final map. In this area, we search for objects that decline significantly between days 4-5 and day 7, and are undetectable by day 24, finding none to typical magnitude limits of i = 21.5, 21.1, 20.1 for object colors (i -z) = 1, 0, -1, respectively. Our search demonstrates the feasibility of a dedicated search program with DECam and bodes well for future research in this emerging field. C1 [Soares-Santos, M.; Annis, J.; Buckley-Geer, E.; Diehl, H. T.; Drlica-Wagner, A.; Finley, D. A.; Flaugher, B.; Frieman, J.; Herner, K.; Lin, H.; Marriner, J.; Neilsen, E.; Wester, W.; Yanny, B.; Allam, S.; Estrada, J.; Gutierrez, G.; Kent, S.; Kuropatkin, N.; Nord, B.; Peoples, J.; Scarpine, V.; Stebbins, A.; Tucker, D. L.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Kessler, R.; Chen, H.; Doctor, Z.; Farr, B.; Frieman, J.; Holz, D.; Scolnic, D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Berger, E.; Cowperthwaite, P. S.; Drout, M. R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Brout, D.; Sako, M.; Eifler, T. F.; Fischer, J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Foley, R. J.; Gruendl, R. A.; Carrasco Kind, M.; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Foley, R. J.; Karliner, I.; Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. [Gruendl, R. A.; Carrasco Kind, M.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Rest, A.] STScI, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Sobreira, F.] Univ Estadual Paulista, Inst Fis Teor, Rua Dr Bento T Ferraz 271, BR-01140070 Sao Paulo, SP, Brazil. [Walker, A. R.; Abbott, T. M. C.; James, D. J.; Smith, R. C.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. [Abdalla, F. B.; Benoit-Levy, A.; Lahav, O.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Armstrong, R.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Banerji, M.; McMahon, R. G.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Banerji, M.; McMahon, R. G.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Benoit-Levy, A.; Bertin, E.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Benoit-Levy, A.; Bertin, E.] UPMC Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Bernstein, R. A.] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Brown, D. A.] Syracuse Univ, Dept Phys, Syracuse, NY 13244 USA. [Burke, D. L.; Gruen, D.; Roodman, A.; Rykoff, E. S.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Burke, D. L.; Gruen, D.; Roodman, A.; Rykoff, E. S.; Schindler, R.; Wechsler, R. H.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Capozzi, D.; D'Andrea, C. B.; Nichol, R. C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Carnero Rosell, A.; da Costa, L. N.; Lima, M.; Maia, M. A. G.; Ogando, R.] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carretero, J.; Castander, F. J.; Crocce, M.; Fosalba, P.; Gaztanaga, E.] CSIC, IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain. [Carretero, J.; Fernandez, E.; Miquel, R.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, Bellaterra 08193, Barcelona, Spain. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA. [Cenko, S. B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Chornock, R.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Clippinger Lab 251B, Athens, OH 45701 USA. [D'Andrea, C. B.; Smith, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Desai, S.; Dietrich, J. P.; Mohr, J. J.; Weller, J.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Evrard, A. E.; Gerdes, D. W.; Miller, C. J.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Fairhurst, S.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Fong, W.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Fox, D. B.] Penn State Univ, Ctr Particle & Gravitat Astrophys, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fox, D. B.] Penn State Univ, Ctr Theoret & Observat Cosmol, University Pk, PA 16802 USA. [Fryer, C. L.] Los Alamos Natl Lab, CCS Div, Los Alamos, NM 87545 USA. [Garcia-Bellido, J.; Sanchez, E.; Sevilla-Noarbe, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain. [Goldstein, D. A.; Kasen, D.] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA. [Goldstein, D. A.; Kasen, D.; Thomas, R. C.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Honscheid, K.; Martini, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Li, T. S.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Li, T. S.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil. [Margutti, R.] NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. [Martini, P.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. [Matheson, T.] Natl Opt Astron Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA. [Metzger, B. D.] Columbia Astrophys Lab, Pupin Hall, New York, NY 10027 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Mohr, J. J.; Weller, J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Quataert, E.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Quataert, E.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA. [Smith, N.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Sutton, P. J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA. [Wechsler, R. H.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Weller, J.] Ludwig Maximilians Univ Munchen, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany. RP Soares-Santos, M (reprint author), Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. RI Ogando, Ricardo/A-1747-2010; Lima, Marcos/E-8378-2010; Sobreira, Flavia/F-4168-2015; Fernandez, Enrique/L-5387-2014; OI Ogando, Ricardo/0000-0003-2120-1154; Sobreira, Flavia/0000-0002-7822-0658; Fernandez, Enrique/0000-0002-6405-9488; Weller, Jochen/0000-0002-8282-2010; Gaztanaga, Enrique/0000-0001-9632-0815; Soares-Santos, Marcelle/0000-0001-6082-8529; Abdalla, Filipe/0000-0003-2063-4345; Garcia-Bellido, Juan/0000-0002-9370-8360 FU U.S. Department of Energy; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas; Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat Munchen; associated Excellence Cluster universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford University; University of Sussex; Texas AM University; National Science Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Research Council [240672, 291329, 306478] FX Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey.; The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University.; The DES data management system is supported by the National Science Foundation under grant No. AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and the Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the European Research Council under the European Unions Seventh Framework Programme (FP7/2007-2013), including ERC grant agreements 240672, 291329, and 306478. NR 27 TC 11 Z9 11 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2016 VL 823 IS 2 AR L33 DI 10.3847/2041-8205/823/2/L33 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ3WH UT WOS:000385779800001 ER PT J AU Soares-Santos, M Kessler, R Berger, E Annis, J Brout, D Buckley-Geer, E Chen, H Cowperthwaite, PS Diehl, HT Doctor, Z Drlica-Wagner, A Farr, B Finley, DA Flaugher, B Foley, RJ Frieman, J Gruendl, RA Herner, K Holz, D Lin, H Marriner, J Neilsen, E Rest, A Sako, M Scolnic, D Sobreira, F Walker, AR Wester, W Yanny, B Abbott, TMC Abdalla, FB Allam, S Armstrong, R Banerji, M Benoit-Levy, A Bernstein, RA Bertin, E Brown, DA Burke, DL Capozzi, D Rosell, AC Kind, MC Carretero, J Castander, FJ Cenko, SB Chornock, R Crocce, M D'Andrea, CB da Costa, LN Desai, S Dietrich, JP Drout, MR Eifler, TF Estrada, J Evrard, AE Fairhurst, S Fernandez, E Fischer, J Fong, W Fosalba, P Fox, DB Fryer, CL Garcia-Bellido, J Gaztanaga, E Gerdes, DW Goldstein, DA Gruen, D Gutierrez, G Honscheid, K James, DJ Karliner, I Kasen, D Kent, S Kuropatkin, N Kuehn, K Lahav, O Li, TS Lima, M Maia, MAG Margutti, R Martini, P Matheson, T McMahon, RG Metzger, BD Miller, CJ Miquel, R Mohr, JJ Nichol, RC Nord, B Ogando, R Peoples, J Plazas, AA Quataert, E Romer, AK Roodman, A Rykoff, ES Sanchez, E Scarpine, V Schindler, R Schubnell, M Sevilla-Noarbe, I Sheldon, E Smith, M Smith, N Smith, RC Stebbins, A Sutton, PJ Swanson, MEC Tarle, G Thaler, J Thomas, RC Tucker, DL Vikram, V Wechsler, RH Weller, J AF Soares-Santos, M. Kessler, R. Berger, E. Annis, J. Brout, D. Buckley-Geer, E. Chen, H. Cowperthwaite, P. S. Diehl, H. T. Doctor, Z. Drlica-Wagner, A. Farr, B. Finley, D. A. Flaugher, B. Foley, R. J. Frieman, J. Gruendl, R. A. Herner, K. Holz, D. Lin, H. Marriner, J. Neilsen, E. Rest, A. Sako, M. Scolnic, D. Sobreira, F. Walker, A. R. Wester, W. Yanny, B. Abbott, T. M. C. Abdalla, F. B. Allam, S. Armstrong, R. Banerji, M. Benoit-Levy, A. Bernstein, R. A. Bertin, E. Brown, D. A. Burke, D. L. Capozzi, D. Carnero Rosell, A. Kind, M. Carrasco Carretero, J. Castander, F. J. Cenko, S. B. Chornock, R. Crocce, M. D'Andrea, C. B. da Costa, L. N. Desai, S. Dietrich, J. P. Drout, M. R. Eifler, T. F. Estrada, J. Evrard, A. E. Fairhurst, S. Fernandez, E. Fischer, J. Fong, W. Fosalba, P. Fox, D. B. Fryer, C. L. Garcia-Bellido, J. Gaztanaga, E. Gerdes, D. W. Goldstein, D. A. Gruen, D. Gutierrez, G. Honscheid, K. James, D. J. Karliner, I. Kasen, D. Kent, S. Kuropatkin, N. Kuehn, K. Lahav, O. Li, T. S. Lima, M. Maia, M. A. G. Margutti, R. Martini, P. Matheson, T. McMahon, R. G. Metzger, B. D. Miller, C. J. Miquel, R. Mohr, J. J. Nichol, R. C. Nord, B. Ogando, R. Peoples, J. Plazas, A. A. Quataert, E. Romer, A. K. Roodman, A. Rykoff, E. S. Sanchez, E. Scarpine, V. Schindler, R. Schubnell, M. Sevilla-Noarbe, I. Sheldon, E. Smith, M. Smith, N. Smith, R. C. Stebbins, A. Sutton, P. J. Swanson, M. E. C. Tarle, G. Thaler, J. Thomas, R. C. Tucker, D. L. Vikram, V. Wechsler, R. H. Weller, J. CA DES Collaboration TI A DARK ENERGY CAMERA SEARCH FOR AN OPTICAL COUNTERPART TO THE FIRST ADVANCED LIGO GRAVITATIONAL WAVE EVENT GW150914 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: close; catalogs; gravitational waves; stars: neutron; surveys ID RADIOACTIVELY POWERED TRANSIENTS; NEUTRON-STAR MERGERS; VIRGO AB We report the results of a deep search for an optical counterpart to the gravitational wave (GW) event GW150914, the first trigger from the Advanced LIGO GW detectors. We used the Dark Energy Camera (DECam) to image a 102 deg(2) area, corresponding to 38% of the initial trigger high-probability sky region and to 11% of the revised high-probability region. We observed in the i and z bands at 4-5, 7, and 24 days after the trigger. The median 5 sigma point-source limiting magnitudes of our search images are i = 22.5 and z = 21.8 mag. We processed the images through a difference-imaging pipeline using templates from pre-existing Dark Energy Survey data and publicly available DECam data. Due to missing template observations and other losses, our effective search area subtends 40 deg(2), corresponding to a 12% total probability in the initial map and 3% in the final map. In this area, we search for objects that decline significantly between days 4-5 and day 7, and are undetectable by day 24, finding none to typical magnitude limits of i = 21.5, 21.1, 20.1 for object colors (i - z) = 1, 0, - 1, respectively. Our search demonstrates the feasibility of a dedicated search program with DECam and bodes well for future research in this emerging field. C1 [Soares-Santos, M.; Annis, J.; Buckley-Geer, E.; Diehl, H. T.; Drlica-Wagner, A.; Finley, D. A.; Flaugher, B.; Frieman, J.; Herner, K.; Lin, H.; Marriner, J.; Neilsen, E.; Wester, W.; Yanny, B.; Allam, S.; Estrada, J.; Gutierrez, G.; Kent, S.; Kuropatkin, N.; Nord, B.; Peoples, J.; Scarpine, V.; Stebbins, A.; Tucker, D. L.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Kessler, R.; Chen, H.; Doctor, Z.; Farr, B.; Frieman, J.; Holz, D.; Scolnic, D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Berger, E.; Cowperthwaite, P. S.; Drout, M. R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Brout, D.; Sako, M.; Eifler, T. F.; Fischer, J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Foley, R. J.; Gruendl, R. A.; Kind, M. Carrasco; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Foley, R. J.; Karliner, I.; Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. [Gruendl, R. A.; Kind, M. Carrasco; Swanson, M. E. C.] Univ Illinois, Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Rest, A.] STScI, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Sobreira, F.] Univ Estadual Paulista, Inst Fis Teor, Rua Dr Bento T Ferraz 271, BR-01140070 Sao Paulo, SP, Brazil. [Walker, A. R.; Abbott, T. M. C.; James, D. J.; Smith, R. C.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile. [Abdalla, F. B.; Benoit-Levy, A.; Lahav, O.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Armstrong, R.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Banerji, M.; McMahon, R. G.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Banerji, M.; McMahon, R. G.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Benoit-Levy, A.; Bertin, E.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Benoit-Levy, A.; Bertin, E.] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Bernstein, R. A.] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Brown, D. A.] Syracuse Univ, Dept Phys, Syracuse, NY 13244 USA. [Burke, D. L.; Gruen, D.; Roodman, A.; Rykoff, E. S.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Burke, D. L.; Gruen, D.; Roodman, A.; Rykoff, E. S.; Schindler, R.; Wechsler, R. H.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Capozzi, D.; D'Andrea, C. B.; Nichol, R. C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Carnero Rosell, A.; da Costa, L. N.; Lima, M.; Maia, M. A. G.; Ogando, R.] Lab Interinst & Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carretero, J.; Castander, F. J.; Crocce, M.; Fosalba, P.; Gaztanaga, E.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain. [Carretero, J.; Fernandez, E.; Miquel, R.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, Bellaterra 08193, Barcelona, Spain. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA. [Cenko, S. B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Chornock, R.] Ohio Univ, Clippinger Lab 251B, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [D'Andrea, C. B.; Smith, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Desai, S.; Dietrich, J. P.; Mohr, J. J.; Weller, J.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Evrard, A. E.; Gerdes, D. W.; Miller, C. J.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Fairhurst, S.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Fong, W.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, Ctr Particle & Gravitat Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Fox, D. B.] Penn State Univ, Ctr Theoret & Observat Cosmol, University Pk, PA 16802 USA. [Fryer, C. L.] Los Alamos Natl Lab, CCS Div, POB 1663, Los Alamos, NM 87545 USA. [Garcia-Bellido, J.; Sanchez, E.; Sevilla-Noarbe, I.] CIEMAT, E-28040 Madrid, Spain. [Goldstein, D. A.; Kasen, D.] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA. [Goldstein, D. A.; Kasen, D.; Thomas, R. C.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Honscheid, K.; Martini, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Li, T. S.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Li, T. S.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil. [Margutti, R.] NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. [Martini, P.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. [Matheson, T.] Natl Opt Astron Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA. [Metzger, B. D.] Columbia Astrophys Lab, Pupin Hall, New York, NY 10027 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Mohr, J. J.; Weller, J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Quataert, E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Quataert, E.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA. [Smith, N.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Sutton, P. J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA. [Wechsler, R. H.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Weller, J.] Univ Munich, Fak Phys, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany. RP Soares-Santos, M (reprint author), Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. RI Ogando, Ricardo/A-1747-2010; Lima, Marcos/E-8378-2010; Sobreira, Flavia/F-4168-2015; Fernandez, Enrique/L-5387-2014; OI Ogando, Ricardo/0000-0003-2120-1154; Sobreira, Flavia/0000-0002-7822-0658; Fernandez, Enrique/0000-0002-6405-9488; Weller, Jochen/0000-0002-8282-2010; Gaztanaga, Enrique/0000-0001-9632-0815; Soares-Santos, Marcelle/0000-0001-6082-8529; Abdalla, Filipe/0000-0003-2063-4345; Garcia-Bellido, Juan/0000-0002-9370-8360 FU U.S. Department of Energy; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat Munchen; associated Excellence Cluster universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford University; University of Sussex; Texas AM University; National Science Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Research Council under the European Union, ERC [240672, 291329, 306478] FX Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey.r The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University.r The DES data management system is supported by the National Science Foundation under grant No. AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and the Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the European Research Council under the European Unions Seventh Framework Programme (FP7/2007-2013), including ERC grant agreements 240672, 291329, and 306478. NR 31 TC 11 Z9 11 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2016 VL 823 IS 2 AR L33 DI 10.3847/2041-8205/823/2/L33 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN4JL UT WOS:000377031700012 ER PT J AU Braje, TJ Rick, TC Erlandson, JM Rogers-Bennett, L Catton, CA AF Braje, Todd J. Rick, Torben C. Erlandson, Jon M. Rogers-Bennett, Laura Catton, Cynthia A. TI Historical ecology can inform restoration site selection: the case of black abalone (Haliotis cracherodii) along California's Channel Islands SO AQUATIC CONSERVATION-MARINE AND FRESHWATER ECOSYSTEMS LA English DT Article DE ecological history; fishery data; endangered species; enhancement; stocking; shellfish ID SAN-MIGUEL ISLAND; COMPLEX HUNTER-GATHERERS; WITHERING SYNDROME; FISHERIES; CONSERVATION; POPULATIONS; ARCHAEOLOGY; LEACH; ENHANCEMENT; SUBSISTENCE AB 1. Identifying appropriate ecological conditions for population restoration is important for endangered species such as black abalone (Haliotis cracherodii) in California, but limited information exists regarding restoration locations. 2. Using a combination of ancient and historical archaeological data and modern commercial fishing records, four optimal locations for restoration based on past relative abundances of black abalone were identified: north-western, north-eastern, and south-central San Miguel Island and western San Nicolas Island. 3. These locations around California's Channel Islands have supported dense black abalone populations for at least 10 000 years and may offer optimal environmental conditions to enhance the success of black abalone restoration. 4. The strategy outlined here illustrates the promise of integrating prehistoric, historical, and modern fishery data to inform restoration of threatened and endangered abalone, oysters, and other shellfish around the world. Copyright (C) 2015 John Wiley & Sons, Ltd. C1 [Braje, Todd J.] San Diego State Univ, Dept Anthropol, San Diego, CA 92182 USA. [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Erlandson, Jon M.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. [Rogers-Bennett, Laura; Catton, Cynthia A.] Calif Dept Fish & Wildlife, Bodega Marine Lab, Bodega Bay, CA USA. RP Braje, TJ (reprint author), San Diego State Univ, Dept Anthropol, San Diego, CA 92182 USA. EM tbraje@mail.sdsu.edu OI Erlandson, Jon/0000-0002-4705-4319 FU California Department of Fish and Wildlife FX We thank Russell Galipeau, Ann Huston, Kelly Minas, Dan Richards, Mark Senning, and Ian Williams for their support. Thanks to Leslie Reeder-Myers for graphical assistance. We are grateful to Paul Dayton, two anonymous reviewers, and the editorial staff at Aquatic Conservation. This is a joint contribution of San Diego State University, the Smithsonian Institute, the University of Oregon, and the UC Davis, Bodega Marine Lab. We thank the California Department of Fish and Wildlife for fishery data and support to LRB and CAC. NR 52 TC 2 Z9 2 U1 13 U2 13 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1052-7613 EI 1099-0755 J9 AQUAT CONSERV JI Aquat. Conserv.-Mar. Freshw. Ecosyst. PD JUN PY 2016 VL 26 IS 3 BP 470 EP 481 DI 10.1002/aqc.2561 PG 12 WC Environmental Sciences; Marine & Freshwater Biology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA DW5FR UT WOS:000383669200006 ER PT J AU Sohn, JC Baraniak, E AF Sohn, J. -C. Baraniak, E. TI Eidophasia infuscata Staudinger, [1871] 1870, status nova with the first description of male and female genitalia (Lepidoptera: Plutellidae) SO SHILAP-REVISTA DE LEPIDOPTEROLOGIA LA English DT Article DE Lepidoptera; Plutellidae; Eidophasia infuscata; redescription; taxonomy; Greece AB Eidophasia infuscata Staudinger from Greece, previously regarded as an infrasubspecies or a subspecies of Eidophasia messingiella, is proposed as a full species based on the differences in the coloration of the head, the forewing patterns, and the male and female genitalia. Eidophasia infuscata is reported from Turkey for the first time. The first descriptions of the genitalia of both sexes are provided for E. infuscata. A diagnostic summary is provided with illustrations for three similar congeners, Eidophasia messingiella, E. infuscata, and E. albifasciata. C1 [Sohn, J. -C.] Smithsonian Inst, US Natl Museum Nat istory, Dept Entomol, 10th & Constitut NW, Washington, DC 20560 USA. [Baraniak, E.] Adam Mickiewicz Univ, Zaklad Zool Systematycznej, Ul Umultowska 89 61-614, PL-61614 Poznan, Poland. RP Sohn, JC (reprint author), Smithsonian Inst, US Natl Museum Nat istory, Dept Entomol, 10th & Constitut NW, Washington, DC 20560 USA. EM jay.c.sohn@gmail.com; baraniak@amu.edu.pl FU Ministry of Sciences and Higher Education [NN303 568538] FX We would like to thank Donald Davis (United States National Museum of Natural History, Washington, DC), Ulf Buchsbaum, Axel Hausmann (both, Zoologische Staatssammlung Munchen, Munich). Ole Karsholt (Zoologisk Museum, Copenhagen, Denmark), and Wolfram Mey (Museum fur Naturkunde, Humboldt-Universitat, Berlin) for allowing me to examine the institutional collections under their responsibility. This study was supported by the Ministry of Sciences and Higher Education (grant no. NN303 568538). NR 11 TC 1 Z9 1 U1 0 U2 0 PU SOC HISPANO-LUSO-AMER LEPIDOPTEROLOGIA-SHILAP PI MADRID PA APARTADO DE CORREOS, 331, MADRID, 28080, SPAIN SN 0300-5267 J9 SHILAP-REV LEPIDOPT JI Shilap-Revista Lepidopterol. PD JUN PY 2016 VL 44 IS 174 BP 259 EP 264 PG 6 WC Entomology SC Entomology GA DZ4WV UT WOS:000385862800006 ER PT J AU Wong, RKW Kashyap, VL Lee, TCM van Dyk, DA AF Wong, Raymond K. W. Kashyap, Vinay L. Lee, Thomas C. M. van Dyk, David A. TI DETECTING ABRUPT CHANGES IN THE SPECTRA OF HIGH-ENERGY ASTROPHYSICAL SOURCES SO ANNALS OF APPLIED STATISTICS LA English DT Article DE Astronomy; change point estimation; FK Comae Berenices; marked poisson process; minimum description length principle; semi-parametric modeling; stars; stellar coronae; stellar flare; X-ray astronomy ID CHANGE-POINT MODEL; FK-COMAE; BAYESIAN-ANALYSIS; POISSON-PROCESS; STELLAR CORONAE; SELECTION; CALIBRATION; CRITERION; NUMBER; IMAGES AB Variable-intensity astronomical sources are the result of complex and often extreme physical processes. Abrupt changes in source intensity are typically accompanied by equally sudden spectral shifts, that is, sudden changes in the wavelength distribution of the emission. This article develops a method for modeling photon counts collected from observation of such sources. We embed change points into a marked Poisson process, where photon wavelengths are regarded as marks and both the Poisson intensity parameter and the distribution of the marks are allowed to change. To the best of our knowledge, this is the first effort to embed change points into a marked Poisson process. Between the change points, the spectrum is modeled nonparametrically using a mixture of a smooth radial basis expansion and a number of local deviations from the smooth term representing spectral emission lines. Because the model is over-parameterized, we employ an l(1) penalty. The tuning parameter in the penalty and the number of change points are determined via the minimum description length principle. Our method is validated via a series of simulation studies and its practical utility is illustrated in the analysis of the ultra-fast rotating yellow giant star known as FK Com. C1 [Wong, Raymond K. W.] Iowa State Univ, Dept Stat, 1121 Snedecor Hall, Ames, IA 50011 USA. [Kashyap, Vinay L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Lee, Thomas C. M.] Univ Calif Davis, Dept Stat, 399 Crocker Dr, Davis, CA 95616 USA. [van Dyk, David A.] Imperial Coll London, Dept Math, London SW7 2AZ, England. RP Wong, RKW (reprint author), Iowa State Univ, Dept Stat, 1121 Snedecor Hall, Ames, IA 50011 USA. EM raywong@iastate.edu; vkashyap@cfa.harvard.edu; tcmlee@ucdavis.edu; dvandyk@imperial.ac.uk FU CHASC International Astrostatistics Center; NSF [DMS-12-08791, DMS-12-09232, DMS-1513484, DMS-12-09226, DMS-15-12945]; Chandra Grant [GO1-12021X]; NASA [NAS8-03060]; British Royal Society [WM110023]; European Commission [FP7-PEOPLE-2012-CIG-321865, H2020-MSCA-RISE-2015-691164] FX This work was conducted under the auspices of the CHASC International Astrostatistics Center. CHASC is supported by NSF grants DMS-12-08791, DMS-12-09232 and DMS-1513484.; Supported in part from Chandra Grant GO1-12021X, and from NASA's contract to the Chandra X-ray Center, NAS8-03060.; Supported by NSF Grants DMS-12-09226 and DMS-15-12945.; Supported by a Wolfson Research Merit Award (WM110023) provided by the British Royal Society and from Marie-Curie Career Integration (FP7-PEOPLE-2012-CIG-321865) and Marie-Skodowska-Curie RISE (H2020-MSCA-RISE-2015-691164) Grants both provided by the European Commission. NR 49 TC 0 Z9 0 U1 1 U2 1 PU INST MATHEMATICAL STATISTICS PI CLEVELAND PA 3163 SOMERSET DR, CLEVELAND, OH 44122 USA SN 1932-6157 J9 ANN APPL STAT JI Ann. Appl. Stat. PD JUN PY 2016 VL 10 IS 2 BP 1107 EP 1134 DI 10.1214/16-AOAS933 PG 28 WC Statistics & Probability SC Mathematics GA DY3XA UT WOS:000385029700024 ER PT J AU ZuHone, JA Roediger, E AF ZuHone, John A. Roediger, E. TI Cold fronts: probes of plasma astrophysics in galaxy clusters SO JOURNAL OF PLASMA PHYSICS LA English DT Article ID KELVIN-HELMHOLTZ INSTABILITIES; ANISOTROPIC THERMAL CONDUCTION; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; FIELD POWER SPECTRUM; X-RAY-CLUSTERS; MAGNETIC-FIELD; INTRACLUSTER MEDIUM; COOLING FLOWS; MERGING CLUSTERS; HEAT-CONDUCTION AB The most massive baryonic component of galaxy clusters is the 'intracluster medium' (ICM), a diffuse, hot, weakly magnetized plasma that is most easily observed in the X-ray band. Despite being observed for decades, the macroscopic transport properties of the ICM are still not well constrained. A path to determine macroscopic ICM properties opened up with the discovery of 'cold fronts'. These were observed as sharp discontinuities in surface brightness and temperature in the ICM, with the property that the denser side of the discontinuity is the colder one. The high spatial resolution of the Chandra X-ray Observatory revealed two puzzles about cold fronts. First, they should be subject to Kelvin-Helmholtz instabilities, yet in many cases they appear relatively smooth and undisturbed. Second, the width of the interface between the two gas phases is typically narrower than the mean free path of the particles in the plasma, indicating negligible thermal conduction. It was thus realized that these special characteristics of cold fronts may be used to probe the properties of the cluster plasma. In this review, we will discuss the recent simulations of cold fronts in galaxy clusters, focusing on those which have attempted to use these features to constrain ICM physics. In particular, we will examine the effects of magnetic fields, viscosity, and thermal conductivity on the stability properties and long-term evolution of cold fronts. We conclude with a discussion on what important questions remain unanswered, and the future role of simulations and the next generation of X-ray observatories. C1 [ZuHone, John A.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [ZuHone, John A.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Roediger, E.] Univ Hull, Dept Math & Phys, EA Milne Ctr Astrophys, Kingston Upon Hull HU6 7RX, N Humberside, England. RP ZuHone, JA (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.; ZuHone, JA (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM john.zuhone@cfa.harvard.edu FU NASA [SV2-8203, NAS8-03060]; Chandra X-ray Center [G04-15088X] FX The authors would like to thank the reviewers, E. Churazov and C. Reynolds, for their reading of this manuscript and their helpful comments. J.A.Z. acknowledges support from NASA through subcontract SV2-8203 to MIT from the Smithsonian Astrophysical Observatory, and through Chandra Award Number G04-15088X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. NR 149 TC 1 Z9 1 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-3778 EI 1469-7807 J9 J PLASMA PHYS JI J. Plasma Phys. PD JUN PY 2016 VL 82 AR 535820301 DI 10.1017/S0022377816000544 PN 3 PG 48 WC Physics, Fluids & Plasmas SC Physics GA DS9LA UT WOS:000381103200003 ER PT J AU Seijo, MM Huerta, RPI Torne, JM Torne, CM Vidal, EA AF Martin Seijo, Maria Pique I Huerta, Raquel Mayo Torne, Julia Mayo Torne, Carlos Abad Vidal, Emilio TI CARBONISED WOOD IN FUNERARY CONTEXTS OF THE RIO GRANDE CHIEFDOM, PANAMA: CHARCOAL ANALYSIS AT THE SITE OF EL CANO SO CHUNGARA-REVISTA DE ANTROPOLOGIA CHILENA LA Spanish DT Article DE Charcoal analysis; Archaeobotany; chiefdoms; funerary contexts; wood resources ID MAYA SALT; BELIZE; ECOLOGY; FOREST AB The charcoal analysis undertaken at the El Cano site (Cocle Province, Panama) provided an opportunity to explore the possibilities this kind of archaeobotanical analysis supplies for the study of chiefdoms, particularly in their funerary context. The identification of the utilization of wood resources, and the establishment of a hypothesis about their possible funerary ritual function is fundamental in order to deepen our understanding of the ritual and the management of resources by chiefdoms in the Isthmus of Panama. C1 [Martin Seijo, Maria; Mayo Torne, Carlos] Univ Santiago de Compostela, Dept Hist 1, GEPN Grp Estudos Prehist NW Iberico GI 1534, Santiago De Compostela, Spain. [Pique I Huerta, Raquel] Univ Autonoma Barcelona, Dept Prehist, Bellaterra 08193, Spain. [Mayo Torne, Julia; Mayo Torne, Carlos] Fdn El Cano, Ctr Invest Arqueol Istmo, APO 819-4446, Panama City, Panama. [Mayo Torne, Julia] Smithsonian Trop Res Inst, Ctr Trop Archaeol & Paleoecol, Panama City, Panama. [Mayo Torne, Carlos] Direcc Nacl Patrimonio Hist, Panama City, Panama. [Abad Vidal, Emilio] CESGA Fdn Ctr Tecnol Supercomp Galicia, Santiago De Compostela 15705, Spain. RP Seijo, MM (reprint author), Fac Xeog & Hist, Praza Univ S-N, Santiago De Compostela 15782, Spain. EM maria.martin.seijo@gmail.com; raquel.pique@uab.cat; juliamayo@fundacionelcano.org; carlosmayo@fundacionelcano.org; eav@cesga.es NR 72 TC 1 Z9 1 U1 0 U2 0 PU UNIV TARAPACA PI ARICA PA CASILLA 6-D, ARICA, 1775, CHILE SN 0717-7356 J9 CHUNGARA JI Chungara PD JUN PY 2016 VL 48 IS 2 BP 277 EP 294 DI 10.4067/S0717-73562016005000013 PG 18 WC Anthropology SC Anthropology GA DX9TR UT WOS:000384738800007 ER PT J AU Einzmann, HJR Docke, L Zotz, G AF Einzmann, Helena Julia Regina Doecke, Lisa Zotz, Gerhard TI Epiphytes in human settlements in rural Panama SO PLANT ECOLOGY & DIVERSITY LA English DT Article DE epiphyte diversity; human influence; isolated trees; mistletoes; rainfall gradient; tropical lowlands ID CRASSULACEAN ACID METABOLISM; VASCULAR EPIPHYTES; SEEDLING ESTABLISHMENT; CACAO PLANTATIONS; ANDEAN LANDSCAPE; TROPICAL FOREST; RAIN-FOREST; LAND-USE; DIVERSITY; CONSERVATION AB Background: An ever-increasing proportion of tropical ecosystems are affected by on-going land-use changes, stressing the importance of understanding how organisms cope with biotic and abiotic challenges outside their natural habitat. An important group in the tropics are vascular epiphytes, whose response to human disturbance is poorly understood.Aims: Creating a baseline data set of epiphyte diversity in human settlements and assessing differences with assemblages of less disturbed habitats.Methods: We surveyed the vascular epiphyte assemblages in 25 settlements of south-west Panama along a rainfall gradient. We tested how epiphyte assemblages were affected by human disturbance and climate by comparing our data to that of pastures and forest.Results: Almost half (238 of 499) of all studied trees hosted at least one epiphyte. Altogether, 10,700 epiphytes of 56 species were found. Rainfall strongly affected both composition and diversity of epiphyte assemblages, whereas geographic proximity did not. In settlements, the species pool was considerably smaller than in pastures and undisturbed forest; however, settlements' diversity was only significantly lower compared to pastures.Conclusions: Epiphyte assemblages in settlements had a diminished species pool but diversity per tree was comparable to less disturbed habitats. Unsurprisingly, rainfall seems to be the main determinant of epiphyte diversity in rural settlements. C1 [Einzmann, Helena Julia Regina; Doecke, Lisa; Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, Dept Biol & Environm Sci, Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Panama City, Panama. RP Einzmann, HJR (reprint author), Carl von Ossietzky Univ Oldenburg, Dept Biol & Environm Sci, Oldenburg, Germany. EM helena.einzmann@uni-oldenburg.de FU DAAD; Smithsonian Tropical Research Institute FX Funding was received from DAAD (HE) and Smithsonian Tropical Research Institute (GZ). NR 74 TC 0 Z9 0 U1 5 U2 5 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 1755-0874 EI 1755-1668 J9 PLANT ECOL DIVERS JI Plant Ecol. Divers. PD JUN PY 2016 VL 9 IS 3 BP 277 EP 287 DI 10.1080/17550874.2016.1177127 PG 11 WC Plant Sciences SC Plant Sciences GA DX3WT UT WOS:000384308300004 ER PT J AU Cater, C AF Cater, Casey TI The Power Brokers: The Struggle to Shape and Control the Electric Power Industry SO BUSINESS HISTORY REVIEW LA English DT Book Review C1 [Cater, Casey] Georgia State Univ, Hist, Atlanta, GA 30303 USA. [Cater, Casey] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Cater, C (reprint author), Georgia State Univ, Hist, Atlanta, GA 30303 USA.; Cater, C (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0007-6805 EI 2044-768X J9 BUS HIST REV JI Bus. Hist. Rev. PD SUM PY 2016 VL 90 IS 2 BP 382 EP 385 DI 10.1017/S0007680516000611 PG 5 WC Business; History Of Social Sciences SC Business & Economics; Social Sciences - Other Topics GA DW6RH UT WOS:000383778100026 ER PT J AU Ashton, GV Davidson, IC Geller, J Ruiz, GM AF Ashton, G. V. Davidson, I. C. Geller, J. Ruiz, G. M. TI Disentangling the biogeography of ship biofouling: barnacles in the Northeast Pacific SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE Cirripedia; dispersal; introduction; mitochondrial DNA; non-native; phylogenetics; range expansion; ship biofouling ID MEGABALANUS-COCCOPOMA DARWIN; OXIDASE SUBUNIT-I; CLIMATE-CHANGE; BALLAST WATER; CIRRIPEDIA BALANOMORPHA; SPECIES INTRODUCTIONS; TETRACLITA-RUBESCENS; ATLANTIC BARNACLE; VOLCANO BARNACLE; MARINE INVASIONS AB Aim The movement of biofouling organisms by ships results in the transfer of marine species across biogeographical boundaries on a global scale. We used barnacles, a relatively well-studied taxon, to investigate the extent to which modern commercial vessels disperse biofouling species beyond their current known ranges. Location Vessels predominantly operated in the North Pacific; sampling was conducted in Los Angeles (CA), Portland (OR), Ketchikan (AK) and Apra Harbor (GU). Methods Barnacles were collected from submerged surfaces of commercial vessel hulls and identified to the lowest taxonomic unit using a combination of taxonomic and molecular phylogenetic techniques. Their known native and non-native geographical ranges were assessed and compared with the voyage history of the vessels. Results Forty distinct taxonomic groups of barnacles (22 assigned to species) were detected from 15 vessels. Six of these recognized species have a worldwide distribution, due to natural and anthropogenic dispersal. Sixteen species were on vessels with voyage routes that extend beyond the barnacles' known distributions, including 12 species sampled outside of their known range. Main conclusions A diverse suite of barnacle species is in continuous motion globally on commercial vessel hulls, and the potential scale of this transfer is underscored by the documented species richness for ship biofouling and what is known about the global fleet of vessels. We estimate roughly 680,000 separate arrival events per year for barnacle species to US ports distributed on both Atlantic and Pacific coasts. Genetic methods revealed high richness compared with previous studies, and the real rate is likely to be much higher than this because (1) it is likely that not all species on a vessel were sampled and (2) only a subset of sampled barnacles were successfully sequenced. Our limited knowledge about the total species pool in flux on ship hulls around the globe constrains our ability to analyse and interpret processes affecting species distribution patterns in the Anthropocene. C1 [Ashton, G. V.; Ruiz, G. M.] Smithsonian Environm Res Ctr, Marine Invas Res Lab, Tiburon, CA 94920 USA. [Davidson, I. C.; Ruiz, G. M.] Smithsonian Environm Res Ctr, Marine Invas Res Lab, POB 28, Edgewater, MD 21037 USA. [Geller, J.] Moss Landing Marine Labs, Invertebrate Zool, Moss Landing, CA 95309 USA. [Ashton, G. V.] British Antarct Survey, Madingley Rd, Cambridge CB3 0ET, England. RP Ashton, GV (reprint author), Smithsonian Environm Res Ctr, Marine Invas Res Lab, Tiburon, CA 94920 USA. EM ashtong@si.edu OI Ruiz, Gregory/0000-0003-2499-441X; Davidson, Ian/0000-0002-8729-6048 FU California State Lands Commission; Department of Defense; Smithsonian Institution FX Assistance in the field and laboratory was provided by C. Scianni, C. Brown, L. Ceballos-Osuna, M. Torchin and C. Schloeder. H. Hawk and M. Marraffini completed the DNA extraction and PCR reactions. We are grateful to the four ports for access and logistical assistance; also to the commercial vessel operators, staff and agents for their cooperation, coordination and support. This research was funded by the California State Lands Commission, Department of Defense and Smithsonian Institution. The authors would also like to thank the editor and four referees for their valuable comments on the manuscript. NR 71 TC 1 Z9 1 U1 6 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1466-822X EI 1466-8238 J9 GLOBAL ECOL BIOGEOGR JI Glob. Ecol. Biogeogr. PD JUN PY 2016 VL 25 IS 6 BP 739 EP 750 DI 10.1111/geb.12450 PG 12 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA DW3BC UT WOS:000383516100010 ER PT J AU Smith, H AF Smith, Howard TI ALONE IN THE UNIVERSE SO ZYGON LA English DT Article DE astrobiology; astroethics; astrotheology; exoplanets; extraterrestrial life; Judaism; Kabbalah; Misanthropic Principle; Talmud ID EXTRATERRESTRIAL LIFE; PLANET OCCURRENCE; M-DWARFS; EXOPLANETS; SEARCH; LIMITS; EARTH AB We are probably alone in the universe-a conclusion based on observations of over 4,000 exoplanets and fundamental physical constraints. This article updates earlier arguments with the latest astrophysical results. Since the discovery of exoplanets, theologians have asked with renewed urgency what the presence of extraterrestrial intelligence (ETI) says about salvation and human purpose, but this is the wrong question. The more urgent question is what their absence says. The "Misanthropic Principle" is the observation that, in a universe fine-tuned for life ("Anthropic Principle"), the circumstances necessary for intelligence are rare. Rabbis for 2,000 years discussed the existence of ETI using scriptural passages. We examine the traditional Jewish approaches to ETI, including insights on how ETI affects our perception of God, self, free-will, and responsibility. We explore the implications of our probable solitude, and offer a Jewish response to the ethical lessons to be drawn from the absence of ETI. C1 [Smith, Howard] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Smith, H (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM hsmith@cfa.harvard.edu NR 53 TC 2 Z9 2 U1 9 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0591-2385 EI 1467-9744 J9 ZYGON JI Zygon PD JUN PY 2016 VL 51 IS 2 BP 497 EP 519 DI 10.1111/zygo.12256 PG 23 WC Social Issues; Religion SC Social Issues; Religion GA DV1HQ UT WOS:000382672200015 ER PT J AU Bell, JA AF Bell, Joshua A. TI The Echo of Things: the lives of photographs in the Solomon Islands SO JOURNAL OF PACIFIC HISTORY LA English DT Book Review C1 [Bell, Joshua A.] Smithsonian Inst, Washington, DC 20560 USA. RP Bell, JA (reprint author), Smithsonian Inst, Washington, DC 20560 USA. EM bellja@si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-3344 EI 1469-9605 J9 J PAC HIST JI J. Pac. Hist. PD JUN PY 2016 VL 51 IS 2 BP 222 EP 223 DI 10.1080/00223344.2016.1178898 PG 2 WC History SC History GA DT3VJ UT WOS:000381409000010 ER PT J AU Tsai, CH Fordyce, RE AF Tsai, C. H. Fordyce, R. E. TI Archaic baleen whale from the Kokoamu Greensand: earbones distinguish a new late Oligocene mysticete (Cetacea: Mysticeti) from New Zealand SO JOURNAL OF THE ROYAL SOCIETY OF NEW ZEALAND LA English DT Article DE Ecology; fossil; hearing; morphology; skull; tympanoperiotic ID BALAENOPTERA-ACUTOROSTRATA; PHYLOGENETIC-RELATIONSHIPS; MORPHOLOGY; MAMMALIA; TRANSITION; SKULL; EAR AB dagger Whakakai waipata is a new genus and species of Mysticeti from the Kokoamu Greensand (Chattian, Late Oligocene, 25-27Ma) of The Earthquakes', North Otago. The holotype of dagger Whakakai waipata is a partial skull, periotics, tympanic bulla, vertebrae and scapula. The earbone morphology of dagger Whakakai waipata shows a unique combination of diagnostic features including: massive periotic; flange of posterior process and caudal tympanic process flooring stapedial muscle fossa; and an elongated stylomastoid fossa that invades the robust posterior process of the periotic. The tympanoperiotic features in dagger Whakakai waipata suggest a different acoustic niche from other Oligocene mysticetes, and by inference different feeding habits and habitat.http://zoobank.org/NomenclaturalActs/9D04EC04-1425-4631-9B96-3C279C51E928http://zoobank.org/urn:lsid:zoobank.org:act:9D04EC04-1425-4631-9B96-3C279C51E928 C1 [Tsai, C. H.; Fordyce, R. E.] Univ Otago, Dept Geol, Dunedin, New Zealand. [Fordyce, R. E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Fordyce, R. E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Tsai, CH (reprint author), Natl Museum Nat & Sci, Dept Geol & Paleontol, Tsukuba, Ibaraki, Japan. EM cheng-hsiu.tsai@otago.ac.nz OI Tsai, Cheng-Hsiu/0000-0003-3617-366X FU University of Otago Doctoral Scholarship; National Geographic Society [3542-87, 3657-87] FX This study is part of CHT's PhD thesis and supported by a University of Otago Doctoral Scholarship. Grants 3542-87 and 3657-87 from the National Geographic Society to REF supported field and laboratory work on OU 21927. NR 33 TC 3 Z9 3 U1 5 U2 5 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 0303-6758 EI 1175-8899 J9 J ROY SOC NEW ZEAL JI J. R. Soc. N.Z. PD JUN PY 2016 VL 46 IS 2 BP 117 EP 138 DI 10.1080/03036758.2016.1156552 PG 22 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DU6HM UT WOS:000382315100003 ER PT J AU Balestra, I Mercurio, A Sartoris, B Girardi, M Grillo, C Nonino, M Rosati, P Biviano, A Ettori, S Forman, W Jones, C Koekemoer, A Medezinski, E Merten, J Ogrean, GA Tozzi, P Umetsu, K Vanzella, E van Weeren, RJ Zitrin, A Annunziatella, M Caminha, GB Broadhurst, T Coe, D Donahue, M Fritz, A Frye, B Kelson, D Lombardi, M Maier, C Meneghetti, M Monna, A Postman, M Scodeggio, M Seitz, S Ziegler, B AF Balestra, I. Mercurio, A. Sartoris, B. Girardi, M. Grillo, C. Nonino, M. Rosati, P. Biviano, A. Ettori, S. Forman, W. Jones, C. Koekemoer, A. Medezinski, E. Merten, J. Ogrean, G. A. Tozzi, P. Umetsu, K. Vanzella, E. van Weeren, R. J. Zitrin, A. Annunziatella, M. Caminha, G. B. Broadhurst, T. Coe, D. Donahue, M. Fritz, A. Frye, B. Kelson, D. Lombardi, M. Maier, C. Meneghetti, M. Monna, A. Postman, M. Scodeggio, M. Seitz, S. Ziegler, B. TI CLASH-VLT: DISSECTING THE FRONTIER FIELDS GALAXY CLUSTER MACS J0416.1-2403 WITH similar to 800 SPECTRA OF MEMBER GALAXIES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (MACS J0416.1-2403); galaxies: distances and redshifts; galaxies: kinematics and dynamics ID CONCENTRATION-MASS RELATION; SCALE-INDEPENDENT METHOD; DARK-MATTER HALOS; LENSING ANALYSIS; VELOCITY DISPERSIONS; MERGING CLUSTER; RICH CLUSTERS; ACS/NIC3 OBSERVATIONS; DENSITY PROFILE; INFALL REGIONS AB We present VIMOS-Very Large Telescope (VLT) spectroscopy of the Frontier Fields cluster MACS. J0416.1-2403 (z = 0.397). Taken as part of the CLASH-VLT survey, the large spectroscopic campaign provided more than 4000 reliable redshifts over similar to 600 arcmin(2), including similar to 800 cluster member galaxies. The unprecedented sample of cluster members at this redshift allows us to perform a highly detailed dynamical and structural analysis of the cluster out to similar to 2.2 r(200) (similar to 4Mpc). Our analysis of substructures reveals a complex system composed of a main massive cluster (M-200 similar to 0.9 x 10(15) M-circle dot and sigma(V r200) similar to 1000 km s(-1)) presenting two major features: (i) a bimodal velocity distribution, showing two central peaks separated by Delta V-rf similar to 1100 km s(-1) with comparable galaxy content and velocity dispersion, and (ii) a projected elongation of the main substructures along the NE-SW direction, with a prominent sub-clump similar to 600 kpc SW of the center and an isolated BCG approximately halfway between the center and the SW clump. We also detect a low-mass structure at z similar to 0.390, similar to 10' south of the cluster center, projected at similar to 3Mpc, with a relative line-of-sight velocity of Delta V-rf similar to 1700 km s(-1). The cluster mass profile that we obtain through our dynamical analysis deviates significantly from the "universal" NFW, being best fit by a Softened Isothermal Sphere model instead. The mass profile measured from the galaxy dynamics is found to be in relatively good agreement with those obtained from strong and weak lensing, as well as with that from the X-rays, despite the clearly unrelaxed nature of the cluster. Our results reveal an overall complex dynamical state of this massive cluster and support the hypothesis that the two main subclusters are being observed in a pre-collisional phase, in agreement with recent findings from radio and deep X-ray data. In this article, we also release the entire redshift catalog of 4386 sources in the field of this cluster, which includes 60 identified Chandra X-ray sources and 105 JVLA radio sources. C1 [Balestra, I.; Sartoris, B.; Girardi, M.; Nonino, M.; Biviano, A.] Osserv Astron Trieste, INAF, Via G B Tiepolo 11, I-34131 Trieste, Italy. [Balestra, I.; Monna, A.; Seitz, S.] Univ Observ Munich, Scheinerstr 1, D-81679 Munich, Germany. [Mercurio, A.] Osserv Astron Capodimonte, INAF, Via Moiariello 16, I-80131 Naples, Italy. [Sartoris, B.; Girardi, M.; Annunziatella, M.] Univ Trieste, Dipartimento Fis, Via Tiepolo 11, I-34143 Trieste, Italy. [Grillo, C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. [Rosati, P.; Caminha, G. B.] Univ Ferrara, Dipartimento Fis & Sci Terra, Via Saragat 1, I-44122 Ferrara, Italy. [Ettori, S.; Vanzella, E.; Meneghetti, M.] Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy. [Ettori, S.; Meneghetti, M.] INFN Bologna, Via Ranzani 1, I-40127 Bologna, Italy. [Forman, W.; Jones, C.; Ogrean, G. A.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Koekemoer, A.; Coe, D.; Postman, M.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21208 USA. [Medezinski, E.; Zitrin, A.] CALTECH, Cahill Ctr Astron & Astrophys, MS 249-17, Pasadena, CA 91125 USA. [Medezinski, E.] Hebrew Univ Jerusalem, Racah Inst Phys, Ctr Astrophys & Planetary Sci, IL-91904 Jerusalem, Israel. [Merten, J.] Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England. [Ogrean, G. A.] Stanford Univ, KIPAC, 452 Lomita Mall, Stanford, CA 94305 USA. [Tozzi, P.] Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. [Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. [Broadhurst, T.] Ikerbasque, Basque Fdn Sci, Alameda Urquijo, 36-5 Plaza Bizkaia, E-48011 Bilbao, Spain. [Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Fritz, A.; Scodeggio, M.] INAF, Ist Astrofis Spaziale Fis Cosm IASF Milano, Via Bassini 15, I-20133 Milan, Italy. [Frye, B.] Univ Arizona, Dept Astron, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [Kelson, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Lombardi, M.] Univ Milan, Dipartimento Fis, Via Celoria 16, I-20133 Milan, Italy. [Maier, C.; Ziegler, B.] Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria. [Seitz, S.] Max Planck Inst Extraterr Phys, Postfach 1312,Giessenbachstr, D-85741 Garching, Germany. RP Balestra, I (reprint author), Osserv Astron Trieste, INAF, Via G B Tiepolo 11, I-34131 Trieste, Italy.; Balestra, I (reprint author), Univ Observ Munich, Scheinerstr 1, D-81679 Munich, Germany. EM balestra@oats.inaf.it RI Bartosch Caminha, Gabriel/C-8952-2013; OI Bartosch Caminha, Gabriel/0000-0001-6052-3274; Balestra, Italo/0000-0001-9660-894X; LOMBARDI, MARCO/0000-0002-3336-4965; Koekemoer, Anton/0000-0002-6610-2048 FU PRIN-INAF [2014 1.05.01.94.02]; MIUR [J91J12000450001]; European Union [267251, 627288]; Consorzio per la Fisica-Trieste; DFG cluster of excellence "Origin and Structure of the Universe"; NASA [HST-HF2-51345.001-A, HST-HF2-51334.001-A, NAS5-26555]; Space Telescope Science Institute; ESO VLT [186.A-0798] FX We thank the anonymous referee for a careful reading of the manuscript and the valuable comments and suggestions provided. We acknowledge the continuous help of the ESO user support group, especially our project support astronomer, Vincenzo Mainieri, for his excellent support and advices. We acknowledge financial support from PRIN-INAF 2014 1.05.01.94.02 and from MIUR PRIN2010-2011 (J91J12000450001). I.B. acknowledges funding support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 267251 "Astronomy Fellowships in Italy" (AstroFIt). B.S. acknowledges a grant from "Consorzio per la Fisica-Trieste." P.R. acknowledges the hospitality and support of the visitor program of the DFG cluster of excellence "Origin and Structure of the Universe." G.A.O. and A.Z. are supported by NASA through Hubble Fellowship grants HST-HF2-51345.001-A and #HST-HF2-51334.001-A, respectively, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated under NASA contract NAS5-26555. J.M. is supported by the People Programme (Marie Curie Actions) of the European Union Seventh Framework Programme (FP7/2007-2013) under REA grant agreement No. 627288. This work is based on data collected at the ESO VLT (prog.ID 186.A-0798), at the NASA HST, and at the NASJ Subaru telescope. Based in part on data collected at Subaru Telescope and obtained from the SMOKA, which is operated by the Astronomy Data Center, NAOJ (Baba et al. 2002). NR 97 TC 4 Z9 4 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 JUN PY 2016 VL 224 IS 2 AR 33 DI 10.3847/0067-0049/224/2/33 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DS8DK UT WOS:000381013200020 ER PT J AU Laigle, C McCracken, HJ Ilbert, O Hsieh, BC Davidzon, I Capak, P Hasinger, G Silverman, JD Pichon, C Coupon, J Aussel, H Le Borgne, D Caputi, K Cassata, P Chang, YY Civano, F Dunlop, J Fynbo, J Kartaltepe, JS Koekemoer, A Le Fevre, O Le Floc'h, E Leauthaud, A Lilly, S Lin, L Marchesi, S Milvang-Jensen, B Salvato, M Sanders, DB Scoville, N Smolcic, V Stockmann, M Taniguchi, Y Tasca, L Toft, S Vaccari, M Zabl, J AF Laigle, C. McCracken, H. J. Ilbert, O. Hsieh, B. C. Davidzon, I. Capak, P. Hasinger, G. Silverman, J. D. Pichon, C. Coupon, J. Aussel, H. Le Borgne, D. Caputi, K. Cassata, P. Chang, Y. -Y. Civano, F. Dunlop, J. Fynbo, J. Kartaltepe, J. S. Koekemoer, A. Le Fevre, O. Le Floc'h, E. Leauthaud, A. Lilly, S. Lin, L. Marchesi, S. Milvang-Jensen, B. Salvato, M. Sanders, D. B. Scoville, N. Smolcic, V. Stockmann, M. Taniguchi, Y. Tasca, L. Toft, S. Vaccari, Mattia Zabl, J. TI THE COSMOS2015 CATALOG: EXPLORING THE 1 < z < 6 UNIVERSE WITH HALF A MILLION GALAXIES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies: evolution; galaxies: high-redshift; galaxies: photometry; methods: observational; techniques: photometric ID STAR-FORMING GALAXIES; SIMILAR-TO 2; STELLAR MASS FUNCTION; WIDE-FIELD SURVEY; VLT DEEP SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; EVOLUTION SURVEY COSMOS; ACTIVE GALACTIC NUCLEI; UV-SELECTED GALAXIES; NEAR-INFRARED SURVEY AB We present the COSMOS2015(24) catalog, which contains precise photometric redshifts and stellar masses for more than half a million objects over the 2deg(2) COSMOS field. Including new YJHK(s) images from the UltraVISTA-DR2 survey, Y-band images from Subaru/Hyper-Suprime-Cam, and infrared data from the Spitzer Large Area Survey with the Hyper-Suprime-Cam Spitzer legacy program, this near-infrared-selected catalog is highly optimized for the study of galaxy evolution and environments in the early universe. To maximize catalog completeness for bluer objects and at higher redshifts, objects have been detected on a chi(2) sum of the YJHK(s) and z(++) images. The catalog contains similar to 6 x 10(5) objects in the 1.5 deg(2) UltraVISTA-DR2 region and similar to 1.5 x 10(5) objects are detected in the "ultra-deep stripes" (0.62 deg(2)) at K-s <= 24.7 (3 sigma, 3 '', AB magnitude). Through a comparison with the zCOSMOS-bright spectroscopic redshifts, we measure a photometric redshift precision of sigma(Delta z(1) (+ zs)) = 0.007 and a catastrophic failure fraction of eta = 0.5%. At 3 < z < 6, using the unique database of spectroscopic redshifts in COSMOS, we find sigma(Delta z(1) (+ zs)) = 0.021 and eta = 13.2%. The deepest regions reach a 90% completeness limit of 10(10)M(circle dot) to z = 4. Detailed comparisons of the color distributions, number counts, and clustering show excellent agreement with the literature in the same mass ranges. COSMOS2015 represents a unique, publicly available, valuable resource with which to investigate the evolution of galaxies within their environment back to the earliest stages of the history of the universe. The COSMOS2015 catalog is distributed via anonymous ftp and through the usual astronomical archive systems (CDS, ESO Phase 3, IRSA). C1 [Laigle, C.; McCracken, H. J.; Pichon, C.; Le Borgne, D.] Univ Paris 06, Sorbonne Univ, 98b Bd Arago, F-75014 Paris, France. [Laigle, C.; McCracken, H. J.; Pichon, C.; Le Borgne, D.] CNRS, UMR 7095, IAP, 98b Bd Arago, F-75014 Paris, France. [Ilbert, O.; Davidzon, I.; Le Fevre, O.; Tasca, L.] Univ Aix Marseille, LAM, 38 Rue F Joliot Curie, F-13388 Marseille 13, France. [Ilbert, O.; Davidzon, I.; Le Fevre, O.; Tasca, L.] CNRS, UMR7326, 38 Rue F Joliot Curie, F-13388 Marseille 13, France. [Hsieh, B. C.; Lin, L.] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. [Capak, P.] CALTECH, Pasadena, CA 91125 USA. [Hasinger, G.; Sanders, D. B.] Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Silverman, J. D.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Pichon, C.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Coupon, J.] Univ Geneva, Astron Observ, Ch Ecogia 16, CH-1290 Versoix, Switzerland. [Aussel, H.; Chang, Y. -Y.; Le Floc'h, E.] Univ Paris 07, CNRS, CEA, Lab AIM Paris Saclay,UMR 7158,CE SACLAY, Bat 709, F-91191 Gif Sur Yvette, France. [Caputi, K.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. [Cassata, P.] Univ Valparaiso, Inst Fis & Astron, Av Gran Bretana, Valparaiso 1111, Chile. [Civano, F.; Marchesi, S.] Yale Ctr Astron & Astrophys, 260 Withney Ave, New Haven, CT 06520 USA. [Civano, F.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Dunlop, J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Fynbo, J.; Milvang-Jensen, B.; Stockmann, M.; Toft, S.; Zabl, J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. [Kartaltepe, J. S.] Inst Technol, Sch Phys & Astron, 84 Lomb Mem Dr, Rochester, NY 14623 USA. [Koekemoer, A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Taniguchi, Y.] Kindai Univ, Fac Sci & Engn, Higashiosaka, Osaka, Japan. [Marchesi, S.] Univ Bologna, Dipartimento Fis & Astron, Via Ranzini 1, I-40127 Bologna, Italy. [Salvato, M.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Smolcic, V.] Univ Zagreb, Dept Phys, Bijenicka Cesta 32, HR-10000 Zagreb, Croatia. [Lilly, S.] Swiss Fed Inst Technol, Dept Phys, Inst Astron, Zurich, Switzerland. [Vaccari, Mattia] Univ Western Cape, Dept Phys, Astrophys Grp, Private Bag X17, ZA-7535 Cape Town, South Africa. RP Laigle, C (reprint author), Univ Paris 06, Sorbonne Univ, 98b Bd Arago, F-75014 Paris, France.; Laigle, C (reprint author), CNRS, UMR 7095, IAP, 98b Bd Arago, F-75014 Paris, France. RI Vaccari, Mattia/R-3431-2016; OI Vaccari, Mattia/0000-0002-6748-0577; Koekemoer, Anton/0000-0002-6610-2048 FU ILP LABEX [ANR-10-LABX-63, ANR-11-IDEX-0004-02]; French Agence Nationale de la Recherche [ANR-13-BS05-0005]; "Programme national cosmologie et galaxies" (PNCG); French Agence Nationale de la Recherche; JSPS [26400221]; World Premier International Research Center Initiative (WPI); MEXT, Japan; CREST, JST; ERC-StG grant [EGGS-278202]; DNRF; ERC [648179]; Centre National dEtudes Spatiales (CNES); ESO [179.A-2005]; European Union [337595] FX C.L. is supported by the ILP LABEX (under reference ANR-10-LABX-63 and ANR-11-IDEX-0004-02). This work is partially supported by the Spin(e) grants ANR-13-BS05-0005 of the French Agence Nationale de la Recherche. H.J.M.C.C. acknowledges financial support form the "Programme national cosmologie et galaxies" (PNCG). O.I. acknowledges the funding of the French Agence Nationale de la Recherche for the project "SAGACE". J.D.S. is supported by JSPS KAKENHI grant No. 26400221, the World Premier International Research Center Initiative (WPI), MEXT, Japan and by CREST, JST. B.M.J. and J.P.U.F. acknowledge support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the DNRF. S.T. and M.S. acknowledge support from the ERC Consolidator Grant funding scheme (project ConTExt, grant No. 648179). This research is also partly supported by the Centre National dEtudes Spatiales (CNES). This work is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. V.S. acknowledges the European Union's Seventh Framework program under grant agreement 337595. NR 119 TC 16 Z9 16 U1 5 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2016 VL 224 IS 2 AR 24 DI 10.3847/0067-0049/224/2/24 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DS8DK UT WOS:000381013200011 ER PT J AU Mao, PY Urry, CM Massaro, F Paggi, A Cauteruccio, J Kunzel, SR AF Mao, Peiyuan Urry, C. Megan Massaro, Francesco Paggi, Alessandro Cauteruccio, Joe Kunzel, Soren R. TI A COMPREHENSIVE STATISTICAL DESCRIPTION OF RADIO-THROUGH-gamma-RAY SPECTRAL ENERGY DISTRIBUTIONS OF ALL KNOWN BLAZARS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE accretion, accretion disks; BL Lacertae objects: general; miscellaneous; quasars: general ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS; FERMI BRIGHT BLAZARS; DIGITAL SKY SURVEY; SOURCE CATALOG; DATA RELEASE; SIMPLIFIED VIEW; LAC OBJECTS; 1ST SURVEY AB We combined multi-wavelength data for blazars from the Roma-BZCAT catalog and analyzed hundreds of X-ray spectra. We present the fluxes and spectral energy distributions (SEDs), in 12 frequency bands from radio to gamma-rays, for a final sample of 2214 blazars. Using a model-independent statistical approach, we looked for systematic trends in the SEDs; the most significant trends involved the radio luminosities and X-ray spectral indices of the blazars. We used a principal component analysis (PCA) to determine the basis vectors of the blazar SEDs and, in order to maximize the size of the sample, imputed missing fluxes using the K-nearest neighbors method. Using more than an order of magnitude more data than was available when Fossati et al. first reported trends of SED shape with blazar luminosity, we confirmed the anti-correlation between radio luminosity and synchrotron peak frequency, although with greater scatter than was seen in the smaller sample. The same trend can be seen between bolometric luminosity and synchrotron peak frequency. Finally, we used all of the available blazar data to determine an empirical SED description that depends only on the radio luminosity at 1.4 GHz and the redshift. We verified that this statistically significant relation was not a result of the luminosity-luminosity correlations that are natural in flux-limited samples (i.e., where the correlation is actually caused by the redshift rather than the luminosity). C1 [Mao, Peiyuan; Urry, C. Megan; Massaro, Francesco] Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA. [Massaro, Francesco] Univ Turin, Dept Phys, Via Pietro Giuria 1, I-10125 Turin, Italy. [Massaro, Francesco] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Paggi, Alessandro] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Cauteruccio, Joe; Kunzel, Soren R.] Yale Univ, Dept Stat, New Haven, CT 06520 USA. RP Mao, PY (reprint author), Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA. RI Massaro, Francesco/L-9102-2016; Paggi, Alessandro/C-1219-2017; OI Massaro, Francesco/0000-0002-1704-9850; Paggi, Alessandro/0000-0002-5646-2410; Mao, Peiyuan/0000-0001-6188-8187; Urry, Meg/0000-0002-0745-9792 FU National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science 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; Programma Giovani Ricercatori-Rita Levi Montalcini-Rientro dei Cervelli; NASA [NNX12AO97G, NNX13AP20G] FX 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.r 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.r The work by is supported by the Programma Giovani Ricercatori-Rita Levi Montalcini-Rientro dei Cervelli (2012). This review is also supported by the NASA grants NNX12AO97G and NNX13AP20G. NR 64 TC 4 Z9 4 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2016 VL 224 IS 2 AR 26 DI 10.3847/0067-0049/224/2/26 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DS8DK UT WOS:000381013200013 ER PT J AU Prakash, A Licquia, TC Newman, JA Ross, AJ Myers, AD Dawson, KS Kneib, JP Percival, WJ Bautista, JE Comparat, J Tinker, JL Schlegel, DJ Tojeiro, R Ho, S Lang, D Rao, SM McBride, CK Ben Zhu, GT Brownstein, JR Bailey, S Bolton, AS Delubac, T Mariappan, V Blanton, MR Reid, B Schneider, DP Seo, HJ Rosell, AC Prada, F AF Prakash, Abhishek Licquia, Timothy C. Newman, Jeffrey A. Ross, Ashley J. Myers, Adam D. Dawson, Kyle S. Kneib, Jean-Paul Percival, Will J. Bautista, Julian E. Comparat, Johan Tinker, Jeremy L. Schlegel, David J. Tojeiro, Rita Ho, Shirley Lang, Dustin Rao, Sandhya M. McBride, Cameron K. Ben Zhu, Guangtun Brownstein, Joel R. Bailey, Stephen Bolton, Adam S. Delubac, Timothee Mariappan, Vivek Blanton, Michael R. Reid, Beth Schneider, Donald P. Seo, Hee-Jong Rosell, Aurelio Carnero Prada, Francisco TI THE SDSS-IV EXTENDED BARYON OSCILLATION SPECTROSCOPIC SURVEY: LUMINOUS RED GALAXY TARGET SELECTION SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; cosmology: observations; galaxies: distances and redshifts; galaxies: general; galaxies: photometry; methods: data analysis ID DIGITAL SKY SURVEY; COSMOLOGICAL IMPLICATIONS; PHOTOMETRIC CALIBRATION; POWER SPECTRUM; STELLAR MASS; DATA RELEASE; GROWTH-RATE; SYSTEMATICS; SCALE; CLASSIFICATION AB We describe the algorithm used to select the luminous red galaxy (LRG) sample for the extended Baryon Oscillation Spectroscopic Survey (eBOSS) of the Sloan Digital Sky Survey IV (SDSS-IV) using photometric data from both the SDSS and the Wide-field Infrared Survey Explorer. LRG targets are required to meet a set of color selection criteria and have z-band and i-band MODEL magnitudes z < 19.95 and 19.9 < i < 21.8, respectively. Our algorithm selects roughly 50 LRG targets per square degree, the great majority of which lie in the redshift range 0.6 < z < 1.0 (median redshift 0.71). We demonstrate that our methods are highly effective at eliminating stellar contamination and lower-redshift galaxies. We perform a number of tests using spectroscopic data from SDSS-III/BOSS ancillary programs to determine the redshift reliability of our target selection and its ability to meet the science requirements of eBOSS. The SDSS spectra are of high enough signal-to-noise ratio that at least similar to 89% of the target sample yields secure redshift measurements. We also present tests of the uniformity and homogeneity of the sample, demonstrating that it should be clean enough for studies of the large-scale structure of the universe at higher redshifts than SDSS-III/BOSS LRGs reached. C1 [Prakash, Abhishek; Licquia, Timothy C.; Newman, Jeffrey A.; Rao, Sandhya M.] Univ Pittsburgh, Dept Phys & Astron, PITT PACC, Pittsburgh, PA 15260 USA. [Ross, Ashley J.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Ross, Ashley J.; Percival, Will J.] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Dawson, Kyle S.; Bautista, Julian E.; Brownstein, Joel R.; Bolton, Adam S.; Mariappan, Vivek] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kneib, Jean-Paul; Delubac, Timothee] Ecole Polytech Fed Lausanne, Astrophys Lab, Observ Sauverny, CH-1290 Versoix, Switzerland. [Kneib, Jean-Paul] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Comparat, Johan; Prada, Francisco] Univ Autonoma Madrid, Inst Fis Teor UAM CSIC, E-28049 Madrid, Spain. [Tinker, Jeremy L.; Blanton, Michael R.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. [Schlegel, David J.; Bailey, Stephen] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Tojeiro, Rita] Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Ho, Shirley; Lang, Dustin] Carnegie Mellon Univ, Dept Phys, Bruce & Astrid McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA. [McBride, Cameron K.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Ben Zhu, Guangtun] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Reid, Beth] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA. [Reid, Beth] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Seo, Hee-Jong] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Rosell, Aurelio Carnero] Observatorio Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, Brazil. [Rosell, Aurelio Carnero] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, Brazil. [Prada, Francisco] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain. [Prada, Francisco] CSIC, Glorieta Astron, Inst Astrofis Andalucia, E-18080 Granada, Spain. RP Prakash, A (reprint author), Univ Pittsburgh, Dept Phys & Astron, PITT PACC, Pittsburgh, PA 15260 USA. EM abp15@pitt.edu FU U.S. Department of Energy Office of Science; Alfred P. Sloan Foundation; National Science Foundation; National Aeronautics and Space Administration; Brazilian Participation Group; Carnegie Institution for Science; Carnegie Mellon University; Chilean Participation Group; French Participation Group; Harvard-Smithsonian Center for Astrophysics; Instituto de Astrofisica de Canarias; Johns Hopkins University; Kavli Institute for the Physics and Mathematics of the universe (IPMU)/University of Tokyo; Lawrence Berkeley National Laboratory; Leibniz Institut fur Astrophysik Potsdam (AIP); Max-Planck-Institut fur Astronomie (MPIA Heidelberg); Max-Planck-Institut fur Astrophysik (MPA Garching); Max-Planck-Institut fur Extraterrestrische Physik (MPE); National Astronomical Observatory of China; New Mexico State University; New York University; University of Notre Dame; Observatario Nacional/MCTI; Ohio State University; Pennsylvania State University; Shanghai Astronomical Observatory; United Kingdom Participation Group; Universidad Nacional Autonoma de Mexico; University of Arizona; University of Colorado Boulder; University of Portsmouth; University of Utah; University of Virginia; University of Washington; University of Wisconsin; Vanderbilt University; Yale University FX This work was supported by an Early Career Grant from the U.S. Department of Energy Office of Science. This paper represents an effort by both the SDSS-III and SDSS-IV collaborations. Funding for SDSS-III was provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science.; This paper includes targets derived from the images of the Wide-Field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.; Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss.org. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofisica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut fur Astrophysik Potsdam (AIP), Max-Planck-Institut fur Astronomie (MPIA Heidelberg), Max-Planck-Institut fur Astrophysik (MPA Garching), Max-Planck-Institut fur Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observatario Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autonoma de Mexico, University of Arizona, University of Colorado Boulder, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University. NR 52 TC 6 Z9 6 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2016 VL 224 IS 2 AR 34 DI 10.3847/0067-0049/224/2/34 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DS8DK UT WOS:000381013200021 ER PT J AU Wang, S Liu, JF Qiu, YL Bai, Y Yang, HQ Guo, JC Zhang, P AF Wang, Song Liu, Jifeng Qiu, Yanli Bai, Yu Yang, Huiqin Guo, Jincheng Zhang, Peng TI CHANDRA ACIS SURVEY OF X-RAY POINT SOURCES: THE SOURCE CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; X-rays: general ID MASS BLACK-HOLE; MULTIWAVELENGTH PROJECT; EXTERNAL GALAXIES; LOCKMAN-HOLE; FIELD; CONSTRAINTS; DISCOVERY; OUTBURST; BINARY; M101 AB The Chandra archival data is a valuable resource for various studies on different X-ray astronomy topics. In this paper, we utilize this wealth of information and present a uniformly processed data set, which can be used to address a wide range of scientific questions. The data analysis procedures are applied to 10,029 Advanced CCD Imaging Spectrometer observations, which produces 363,530 source detections belonging to 217,828 distinct X-ray sources. This number is twice the size of the Chandra Source Catalog (Version 1.1). The catalogs in this paper provide abundant estimates of the detected X-ray source properties, including source positions, counts, colors, fluxes, luminosities, variability statistics, etc. Cross-correlation of these objects with galaxies shows that 17,828 sources are located within the D-25 isophotes of 1110 galaxies, and 7504 sources are located between the D-25 and 2D(25) isophotes of 910 galaxies. Contamination analysis with the log N-log S relation indicates that 51.3% of objects within 2D(25) isophotes are truly relevant to galaxies, and the "net" source fraction increases to 58.9%, 67.3%, and 69.1% for sources with luminosities above 10(37), 10(38), and 10(39) erg s(-1), respectively. Among the possible scientific uses of this catalog, we discuss the possibility of studying intra-observation variability, inter-observation variability, and supersoft sources (SSSs). About 17,092 detected sources above 10 counts are classified as variable in individual observation with the Kolmogorov-Smirnov (K-S) criterion (PK-S < 0.01). There are 99,647 sources observed more than once and 11,843 sources observed 10 times or more, offering us a wealth of data with which to explore the long-term variability. There are 1638 individual objects (similar to 2350 detections) classified as SSSs. As a quite interesting subclass, detailed studies on X-ray spectra and optical spectroscopic follow-up are needed to categorize these SSSs and pinpoint their properties. In addition, this survey can enable a wide range of statistical studies, such as X-ray activity in different types of stars, X-ray luminosity functions in different types of galaxies, and multi-wavelength identification and classification of different X-ray populations. C1 [Wang, Song; Liu, Jifeng; Qiu, Yanli; Bai, Yu; Yang, Huiqin; Guo, Jincheng; Zhang, Peng] Chinese Acad Sci, Key Lab Opt Astron, Natl Astron Observ, Beijing 100012, Peoples R China. [Liu, Jifeng] Univ Chinese Acad Sci, Coll Astron & Space Sci, Beijing 100049, Peoples R China. [Qiu, Yanli; Yang, Huiqin; Guo, Jincheng; Zhang, Peng] Univ Chinese Acad Sci, Beijing 100049, Peoples R China. [Guo, Jincheng] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 10, Cambridge, MA 02138 USA. [Zhang, Peng] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. RP Liu, JF (reprint author), Chinese Acad Sci, Key Lab Opt Astron, Natl Astron Observ, Beijing 100012, Peoples R China.; Liu, JF (reprint author), Univ Chinese Acad Sci, Coll Astron & Space Sci, Beijing 100049, Peoples R China. EM songw@bao.ac.cn; jfliu@bao.ac.cn OI Wang, Song/0000-0003-3116-5038 FU National Science Foundation of China [NSFC-11273028, NSFC-11333004]; National Astronomical Observatories, Chinese Academy of Sciences FX This research has made use of data obtained from the Chandra Data Archive, and software provided by the Chandra X-ray Center (CXC) in the application packages CIAO. This research has made use of software obtained from the High Energy Astrophysics Science Archive Research Center (HEA-SARC), a service of the Astrophysics Science Division at NASA/GSFC and of the Smithsonian Astrophysical Observatory's High Energy Astrophysics Division. This research has made use of the SIMBAD database and the VizieR catalog access tool, operated at CDS, Strasbourg, France. Some of the data used in this research are obtained from the Digitized Sky Surveys, produced at the Space Telescope Science Institute. The authors acknowledge support from the National Science Foundation of China under grants NSFC-11273028 and NSFC-11333004, and support from the National Astronomical Observatories, Chinese Academy of Sciences under the Young Researcher Grant. NR 40 TC 4 Z9 5 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 JUN PY 2016 VL 224 IS 2 AR 40 DI 10.3847/0067-0049/224/2/40 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DS8DK UT WOS:000381013200027 ER PT J AU Ewango, CEN Kenfack, D Sainge, MN Thomas, DW van der Burgt, XM AF Ewango, Corneille E. N. Kenfack, David Sainge, Moses Nsanyi Thomas, Duncan W. van der Burgt, Xander M. TI Gambeya korupensis (Sapotaceae: Chrysophylloideae), a new rain forest tree species from the Southwest Region in Cameroon SO KEW BULLETIN LA English DT Article DE Chrysophyllum; conservation; IUCN Vulnerable; Korup National Park ID NATIONAL-PARK AB Gambeya korupensis Ewango & Kenfack (Sapotaceae: Chrysophylloideae), a new rain forest tree species from the Southwest Region in Cameroon, is described and illustrated. A distribution map is provided. G. korupensis has the leaf blade below pubescent on the midribs and secondary nerves, flowers with a pedicel 0.5 - 1 mm long, and a fruit which is ovoid, attenuate at the apex, 5-ridged, verrucose between the ridges, and bright red at maturity. The conservation status of G. korupensis is assessed as Vulnerable according to IUCN criteria. C1 [Ewango, Corneille E. N.] Wildlife Conservat Soc, Kinshasa, DEM REP CONGO. [Ewango, Corneille E. N.] Univ Kisangani, Kisangani, Orientale Provi, DEM REP CONGO. [Kenfack, David] Smithsonian Trop Res Inst, Ctr Trop Forest Sci ForestGEO, POB 37012, Washington, DC 20013 USA. [Sainge, Moses Nsanyi] Trop Plant Explorat Grp TroPEG Cameroon, POB 18, Mundemba, Southwest Regio, Cameroon. [Thomas, Duncan W.] Washington State Univ, Sch Biol Sci, Vancouver, WA USA. [van der Burgt, Xander M.] Royal Bot Gardens, Herbarium, Richmond TW9 3AE, Surrey, England. RP Ewango, CEN (reprint author), Wildlife Conservat Soc, Kinshasa, DEM REP CONGO.; Ewango, CEN (reprint author), Univ Kisangani, Kisangani, Orientale Provi, DEM REP CONGO. EM cewango@wcs.org NR 24 TC 0 Z9 0 U1 1 U2 1 PU SPRINGER LONDON LTD PI LONDON PA 236 GRAYS INN RD, 6TH FLOOR, LONDON WC1X 8HL, ENGLAND SN 0075-5974 EI 1874-933X J9 KEW BULL JI Kew Bull. PD JUN PY 2016 VL 71 IS 2 AR 28 DI 10.1007/S12225-016-9633-X PG 6 WC Plant Sciences SC Plant Sciences GA DS9DN UT WOS:000381083000013 ER PT J AU Candido, ES De Vargas, W Vatanparast, M Mansano, VD Machado, SR Fortuna-Perez, AP AF Candido, Elisa Silva De Vargas, Wanderleia Vatanparast, Mohammad Mansano, Vidal De Freitas Machado, Silvia Rodrigues Fortuna-Perez, Ana Paula TI A New Species of Eriosema (Leguminosae, Papilionoideae, Phaseoleae) from Mato Grosso do Sul, Brazil, with a Secretory Structure Novel to the Genus SO PHYTOTAXA LA English DT Article DE Cajaninae; Fabaceae; Neotropics; secretory structures; taxonomy ID MINAS-GERAIS; MILLETTIEAE; EVOLUTION; CAVITIES; CERRADO; GLANDS AB Eriosema grearii, a new species for the genus (Leguminosae, Papilionoideae, Phaseoleae, Cajaninae), is described and illustrated. Similar to E. heterophyllum, it differs from it morphologically by the free (vs. joined) stipules, lax flowers distributed along the inflorescence axis (vs. congested and concentrated at its apex), inflorescences not opposite to the leaves (vs. opposite), and leaflets with secretory cells at the base of trichomes (vs. absence of secretory cells at the base of trichomes). A survey of the leaflet secretory structures revealed that E. grearii has distinct secretory structures, referred here as secretory- base trichomes, and reported for the first time for the Phaseoleae tribe. An identification key for the Eriosema species in Mato Grosso do Sul, where the new species occurs, is provided. C1 [Candido, Elisa Silva; Fortuna-Perez, Ana Paula] Univ Estadual Campinas, Inst Biol, Dept Biol Vegetal, Programa Pos Grad Biol Vegetal, BR-13083862 Campinas, SP, Brazil. [De Vargas, Wanderleia; Machado, Silvia Rodrigues; Fortuna-Perez, Ana Paula] Univ Estadual Paulista, Inst Biociencias, Dept Bot, Programa Pos Grad Ciencias Biol Bot, BR-18618000 Botucatu, SP, Brazil. [Vatanparast, Mohammad] Smithsonian Inst NMNH, US Natl Herbarium US, Dept Bot, MRC 166,10th & Constitut Ave, Washington, DC 20560 USA. [Mansano, Vidal De Freitas] Inst Pesquisas Jardim Bot Rio de Janeiro, Rua Pacheco Leao 915, BR-22460030 Rio De Janeiro, RJ, Brazil. RP Fortuna-Perez, AP (reprint author), Univ Estadual Campinas, Inst Biol, Dept Biol Vegetal, Programa Pos Grad Biol Vegetal, BR-13083862 Campinas, SP, Brazil.; Fortuna-Perez, AP (reprint author), Univ Estadual Paulista, Inst Biociencias, Dept Bot, Programa Pos Grad Ciencias Biol Bot, BR-18618000 Botucatu, SP, Brazil. EM bio.fortuna@gmail.com FU CNPq [457911/2013-1, 140598/2015-4, 302657/2011-8]; CAPES; FAPESP [2015/13386-0] FX The authors gratefully acknowledge financial support from CNPq (process 457911/2013-1) for field work, for a PhD scholarship to Wanderleia de Vargas (process 140598/2015-4), and a grant to Silvia R. Machado (process 302657/2011-8); from CAPES for a PhD scholarship to the first author; from FAPESP (process 2015/13386-0) for a grant to Ana Paula Fortuna-Perez. We are also grateful to Klei Sousa for preparing the illustration; to the curators of the visited herbaria (especially those of HRB) for providing access to their collections; and to personnel from Electron Microscopy Center of the Institute of Bioscience of the UNESP (Botucatu) for the assistance with sample preparation. NR 36 TC 1 Z9 1 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1179-3155 EI 1179-3163 J9 PHYTOTAXA JI Phytotaxa PD JUN 1 PY 2016 VL 263 IS 2 BP 122 EP 130 DI 10.11646/phytotaxa.263.2.4 PG 9 WC Plant Sciences SC Plant Sciences GA DT9NB UT WOS:000381827400004 ER PT J AU Sander, SJ Joyner, PH Cray, C Rotstein, DS Aitken-Palmer, C AF Sander, Samantha J. Joyner, Priscilla H. Cray, Carolyn Rotstein, David S. Aitken-Palmer, Copper TI ACUTE PHASE PROTEINS AS A MARKER OF RESPIRATORY INFLAMMATION IN PRZEWALSKI'S HORSE (EQUUS FERUS PRZEWALSKII) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Acute phase protein; Equus ferus przewalskii; haptoglobin; Przewalski's horse; serum amyloid A; surfactant protein D ID SERUM; IDENTIFICATION; SAA AB Acute phase proteins are sensitive markers of inflammation, which are highly conserved across taxa. Although the utility of these proteins are becoming well defined in human and domestic animal medical fields, their role in nondomestic species remains unclear. In this communication, a 20-yr-old Przewalski's horse was presented for unresolving aspiration pneumonia, which cultured a unique Actinomyces-like bacteria. Despite waxing and waning clinical signs and minimal changes on baseline hematologic analysis, protein electrophoresis, serum amyloid A, and surfactant protein D serum concentrations showed changes that more accurately reflected the clinical severity of this case. C1 [Sander, Samantha J.] Smithsonians Natl Zool Pk, Wildlife Hlth Sci, POB 37012,MRC 5501, Washington, DC 20008 USA. [Joyner, Priscilla H.; Aitken-Palmer, Copper] Smithsonian Conservat Biol Inst, Dept Conservat Med, 1500 Remount Rd, Front Royal, VA 22630 USA. [Cray, Carolyn] Univ Miami, Miller Sch Med, Dept Pathol & Lab Med, 1600 NW 10th Ave, Miami, FL 33136 USA. [Rotstein, David S.] 19117 Bloomfield Rd, Olney, MD 20832 USA. [Sander, Samantha J.] Maryland Zoo Baltimore, 1876 Mansion House Dr, Baltimore, MD 21217 USA. RP Sander, SJ (reprint author), Smithsonians Natl Zool Pk, Wildlife Hlth Sci, POB 37012,MRC 5501, Washington, DC 20008 USA.; Sander, SJ (reprint author), Maryland Zoo Baltimore, 1876 Mansion House Dr, Baltimore, MD 21217 USA. EM Samantha.sander@marylandzoo.org NR 16 TC 0 Z9 0 U1 3 U2 3 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 JUN PY 2016 VL 47 IS 2 BP 654 EP 658 PG 5 WC Veterinary Sciences SC Veterinary Sciences GA DS5PI UT WOS:000380834100038 PM 27468045 ER PT J AU Reynolds, J Wesson, K Desbiez, ALJ Ochoa-Quintero, JM Leimgruber, P AF Reynolds, Jason Wesson, Kathryn Desbiez, Arnaud L. J. Ochoa-Quintero, Jose M. Leimgruber, Peter TI Using Remote Sensing and Random Forest to Assess the Conservation Status of Critical Cerrado Habitats in Mato Grosso do Sul, Brazil SO LAND LA English DT Article DE Brazil; Cerrado; random forest; giant armadillo; Mato Grosso do Sul; remote sensing ID LAND-COVER CLASSIFICATION; PROTECTED-AREA; BIODIVERSITY; REGRESSION; VEGETATION; DECLINES; SAVANNA; IMAGERY AB Brazil's Cerrado is a highly diverse ecosystem and it provides critical habitat for many species. Cerrado habitats have suffered significant degradation and decline over the past decades due to expansion of cash crops and livestock farming across South America. Approximately 1,800,000 km(2) of the Cerrado remain in Brazil, but detailed maps and conservation assessments of the Cerrado are lacking. We developed a land cover classification for the Cerrado, focusing on the state of Mato Grosso do Sul, which may also be used to map critical habitat for endangered species. We used a Random Forest algorithm to perform a supervised classification on a set of Landsat 8 images. To determine habitat fragmentation for the Cerrado, we used Fragstats. A habitat connectivity analysis was performed using Linkage Mapper. Our final classification had an overall accuracy of 88%. Our classification produced higher accuracies (72%) in predicting Cerrado than existing government maps. We found that remaining Cerrado habitats were severely fragmented. Four potential corridors were identified in the southwest of Mato Grosso do Sul, where large Cerrado patches are located. Only two large patches remain in Mato Grosso do Sul: one within the Kadiweu Indian Reserve, and one near the southeastern edge of the Pantanal-dominated landscape. These results are alarming for rare species requiring larger tracts of habitat such as the giant armadillo (Priodontes maximus). C1 [Reynolds, Jason; Wesson, Kathryn; Leimgruber, Peter] Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. [Desbiez, Arnaud L. J.] Edinburgh Zoo, Royal Zool Soc Scotland, Giant Armadillo Conservat Program, Edinburgh EH126TS, Midlothian, Scotland. [Ochoa-Quintero, Jose M.] Univ Fed Mato Grosso do Sul, Programa Posgrad Ecol & Conservacao, BR-79070900 Campo Grande, Brazil. [Ochoa-Quintero, Jose M.] Corp Invest Biol, 78 B 141,Carrera 72 A, Medellin, Colombia. RP Wesson, K (reprint author), Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM jdreyno3@gmail.com; kwesson@chesapeakeconservancy.org; adesbiez@hotmail.com; jmochoaquintero@gmail.com; leimgruberp@si.edu OI Ochoa Quintero, Jose Manuel/0000-0002-5619-0777 NR 49 TC 1 Z9 1 U1 12 U2 12 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2073-445X J9 LAND JI Land PD JUN PY 2016 VL 5 IS 2 AR 12 DI 10.3390/land5020012 PG 12 WC Geography, Physical SC Physical Geography GA DR9YW UT WOS:000380253200006 ER PT J AU Hasse, JE AF Hasse, John Edward TI Jazz Journeys SO TRANSYLVANIAN REVIEW LA English DT Article DE jazz; history of music; jazz styles; National Museum of American History AB The paper offers a synthetic presentation of the "journeys" of jazz across the world, from the beginnings of the genre in New Orleans until today, when jazz belongs to the whole world. Attention is also given to the stylistic changes experienced by jazz in the course of time, under the influence of various historic events and trends, such as the civil-rights and counterculture movements, and to the manner in which this music could itself operate as an agent of social change. The second part of the paper presents biographic information, outlining the personal jazz journey of the author. C1 [Hasse, John Edward] Smithsonian Natl Museum Amer Hist, Amer Mus, MRC 616, Washington, DC 20001 USA. [Hasse, John Edward] Smithsonian Jazz Masterworks Orchestra, Washington, DC USA. RP Hasse, JE (reprint author), Smithsonian Natl Museum Amer Hist, Amer Mus, MRC 616, Washington, DC 20001 USA.; Hasse, JE (reprint author), Smithsonian Jazz Masterworks Orchestra, Washington, DC USA. EM hasse@si.edu NR 36 TC 0 Z9 0 U1 2 U2 2 PU CENTER TRANSYLVANIAN STUDIES PI CLUJ-NAPOCA PA 2 NASAUD ST, CLUJ-NAPOCA, 400610, ROMANIA SN 1221-1249 J9 TRANSYLV REV JI Transylv. Rev. PD SUM PY 2016 VL 25 IS 2 BP 112 EP 128 PG 17 WC Area Studies; History SC Area Studies; History GA DT7GO UT WOS:000381655300011 ER PT J AU Hirsch, BT Reynolds, JJH Gehrt, SD Craft, ME AF Hirsch, Ben T. Reynolds, Jennifer J. H. Gehrt, Stanley D. Craft, Meggan E. TI Which mechanisms drive seasonal rabies outbreaks in raccoons? A test using dynamic social network models SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE contact network; epidemiological modelling; host-pathogen interactions; infectious disease management; network modelling; proximity collar; rabies; raccoon; transmission dynamics; wildlife disease; seasonality ID UNITED-STATES; PROCYON-LOTOR; DISEASE TRANSMISSION; CONTACT NETWORKS; NORTH-AMERICA; MATING SYSTEM; EPIDEMIOLOGY; VACCINATION; WILDLIFE; POPULATION AB 1. The timing of raccoon rabies outbreaks in the eastern USA is non-random and often exhibits a seasonal peak. While fluctuations in disease transmission can be driven by seasonal changes in animal population dynamics, behaviour and physiology, it is still unclear which causal factors lead to seasonal outbreaks of raccoon rabies. 2. We used dynamic network modelling to test which of three seasonally changing factors are most likely responsible for raccoon rabies outbreaks: (i) birth pulses, (ii) changes in social network structure and (iii) changes in social contact duration. 3. In contrast to previous predictions, we found that a change in social contact duration was the single most important driver of rabies seasonality. More specifically, co-denning for thermoregulation during the winter increases the amount of time individuals spend in close contact, which in turn should lead to peaks in rabies transmission during the winter. 4. Increased time spent in close proximity during cold winter months has implications for seasonal disease patterns in raccoon populations across a latitudinal gradient, as well as potentially being important for pathogens transmitted by close contact in other wildlife hosts. 5. Synthesis and applications. By incorporating detailed empirical data describing variation in raccoon contacts into a network modelling framework, it is possible to determine the likely causal mechanisms driving seasonal disease patterns. This can be crucial information for wildlife and public health officials implementing wildlife disease control programmes. C1 [Hirsch, Ben T.] James Cook Univ, Coll Marine & Environm Sci, Townsville, Qld 4810, Australia. [Hirsch, Ben T.] Smithsonian Trop Res Inst STRI, Balboa, Panama. [Reynolds, Jennifer J. H.; Craft, Meggan E.] Univ Minnesota, Dept Vet Populat Med, St Paul, MN 55018 USA. [Gehrt, Stanley D.] Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA. RP Hirsch, BT (reprint author), James Cook Univ, Coll Marine & Environm Sci, Townsville, Qld 4810, Australia.; Hirsch, BT (reprint author), Smithsonian Trop Res Inst STRI, Balboa, Panama. EM ben.hirsch@jcu.edu.au FU Cook County Animal and Rabies Control office; Max McGraw Wildlife Foundation; National Science Foundation [EF-0425203, DEB-1413925]; University of Minnesota's Institute on the Environment; Office of the Vice President for Research; Cooperative State Research Service, U.S. Department of Agriculture [MINV 62-044, 62-051] FX Access to the field site and logistical support were provided by the Forest Preserve District of Cook County. Numerous technicians assisted with fieldwork and we are particularly grateful for the contributions of Stephanie Hauver and Suzanne Prange. We also extend thanks to Chris Anchor, Eva Enns, Dan Parmer (deceased), Tiffany Wolf, Kimberly VanderWaal and Donna Alexander for their support in various aspects of the project. This project was funded by grants from the Cook County Animal and Rabies Control office as administered through the Environmental Research Program; Max McGraw Wildlife Foundation; National Science Foundation (EF-0425203, DEB-1413925); University of Minnesota's Institute on the Environment and Office of the Vice President for Research; and the Cooperative State Research Service, U.S. Department of Agriculture, under Project Numbers MINV 62-044 and 62-051. NR 67 TC 0 Z9 0 U1 16 U2 20 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 JUN PY 2016 VL 53 IS 3 BP 804 EP 813 DI 10.1111/1365-2664.12628 PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA DR7FM UT WOS:000380065400020 ER PT J AU Leonard-Pingel, JS Jackson, JBC AF Leonard-Pingel, Jill S. Jackson, Jeremy B. C. TI Drilling predation increased in response to changing environments in the Caribbean Neogene SO PALEOBIOLOGY LA English DT Article ID REEF PRIMARY PRODUCTIVITY; PANAMA LAND-BRIDGE; FOSSIL RECORD; CORAL-REEF; BIOTIC INTERACTIONS; UNITED-STATES; RED-SEA; FUNCTIONAL-MORPHOLOGY; THALASSIA COMMUNITIES; TEMPORAL PATTERNS AB Changes in the physical environment are major drivers of evolutionary change, either through direct effects on the distribution and abundance of species or more subtle shifts in the outcome of biological interactions. To investigate this phenomenon, we built a fossil data set of drilling gastropod predation on bivalve prey for the last 11 Myr to determine how the regional collapse in Caribbean upwelling and planktonic productivity affected predator-prey interactions. Contrary to theoretical expectations, predation increased nearly twofold after productivity declined, while the ratio of drilling predators to prey remained unchanged. This increase reflects a gradual, several-fold increase in the extent of shallow-water coral reefs and seagrass meadows in response to the drop in productivity that extended over several million years. Drilling predation is uniformly higher in biogenic habitats than in soft sediments. Thus, changes in predation intensity were driven by a shift in dominant habitats rather than a direct effect of decreased productivity. Most previous analyses of predation through time have not accounted for variations in environmental conditions, raising questions about the patterns observed. More fundamentally, however, the consequences of large-scale environmental perturbations may not be instantaneous, especially when changes in habitat and other aspects of local environmental conditions cause cascading series of effects. C1 [Leonard-Pingel, Jill S.; Jackson, Jeremy B. C.] Scripps Inst Oceanog, Geosci Res Div, La Jolla, CA 92093 USA. [Leonard-Pingel, Jill S.] Washington & Lee Univ, Dept Geol, 204 W Washington St, Lexington, VA 24450 USA. [Jackson, Jeremy B. C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Jackson, Jeremy B. C.] Smithsonian Trop Res Inst, POB 0843-03093, Balboa, Panama. RP Leonard-Pingel, JS (reprint author), Scripps Inst Oceanog, Geosci Res Div, La Jolla, CA 92093 USA.; Leonard-Pingel, JS (reprint author), Washington & Lee Univ, Dept Geol, 204 W Washington St, Lexington, VA 24450 USA. EM leonard-pingelj@wlu.edu NR 142 TC 0 Z9 0 U1 1 U2 1 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0094-8373 EI 1938-5331 J9 PALEOBIOLOGY JI Paleobiology PD SUM PY 2016 VL 42 IS 3 BP 394 EP 409 DI 10.1017/pab.2016.2 PG 16 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA DS5QZ UT WOS:000380838700003 ER PT J AU Fortuna-Perez, AP Vatanparast, M Candido, ES de Vargas, W AF Fortuna-Perez, Ana Paula Vatanparast, Mohammad Candido, Elisa S. de Vargas, Wanderleia TI Zornia melanocarpa (Leguminosae, Papilionoideae, Dalbergieae), a New Species from Serra do Espinhaco, Brazil, and its Phylogenetic Position in the Genus SO SYSTEMATIC BOTANY LA English DT Article DE Campos rupestres; Cerrado; Neotropics; taxonomy AB Zornia melanocarpa, a new species of Leguminosae (Papilionoideae, Dalbergieae) from Serra do Espinhaco, Minas Gerais, Brazil, is described and illustrated. The species is characterized by black fruits with white hairs and an absence of bristles, characters unique within the genus. The species is morphologically similar to Z. crinita and Z. hebecarpa, but differs from both by having a shorter inflorescence of 1.2-4 cm (vs. 10-20 and 8-20 cm in Z. crinita and Z. hebecarpa, respectively) and in the size of the plant (7-16 cm vs. 20-60 cm in Z. crinita and Z. hebecarpa), in addition to the black fruits with white hairs. A phylogenetic analysis using molecular data from the nuclear rDNA ITS gene region was performed to verify its position within the genus. Additionally, a survey of leaflet secretory structures and a micro-morphological analysis of fruit structures using scanning electron microscopy (SEM) was performed for the newly described species. C1 [Fortuna-Perez, Ana Paula; de Vargas, Wanderleia] Univ Estadual Paulista, Dept Bot, Inst Biociencias, Programa Pos Grad Bot, BR-18618000 Botucatu, SP, Brazil. [Fortuna-Perez, Ana Paula; Candido, Elisa S.] Univ Estadual Campinas, Inst Biol, Dept Biol Vegetal, Programa Pos Grad Biol Vegetal, BR-13083862 Campinas, SP, Brazil. [Vatanparast, Mohammad] Smithsonian Inst NMNH, US Natl Herbarium US, Dept Bot, MRC 166,10th & Constitut Ave, Washington, DC 20560 USA. RP Fortuna-Perez, AP (reprint author), Univ Estadual Paulista, Dept Bot, Inst Biociencias, Programa Pos Grad Bot, BR-18618000 Botucatu, SP, Brazil.; Fortuna-Perez, AP (reprint author), Univ Estadual Campinas, Inst Biol, Dept Biol Vegetal, Programa Pos Grad Biol Vegetal, BR-13083862 Campinas, SP, Brazil. EM bio.fortuna@gmail.com FU CNPq [457911/2013-1, 140598/2015-4]; CAPES; Systematics Association/Linnean Society (U. K.); Smithsonian Institution (U. S. A.) FX The authors gratefully acknowledge the financial support of the CNPq (process 457911/2013-1) for field work; of the CAPES for a PhD scholarship to Elisa Silva Candido; of the CNPq (process 140598/2015-4) for a PhD scholarship to Wanderleia de Vargas. We are grateful to Jesiani Rigon for preparing the illustrations and to curators of the herbaria visited for providing access to their collections. We also thank the Antonio Augusto Tonhao de Almeida (chief of the PERP) and staff of the Park for their help with the fieldwork. MV is grateful to the Systematics Association/Linnean Society (U. K.) for funding his research and to the Smithsonian Institution (U. S. A.) for a GGI grant to finance his field trip. NR 25 TC 0 Z9 0 U1 0 U2 0 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 JUN PY 2016 VL 41 IS 2 BP 298 EP 306 DI 10.1600/036364416X691867 PG 9 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA DR9UE UT WOS:000380240800005 ER PT J AU Kitzberger, T Perry, GLW Paritsis, J Gowda, JH Tepley, AJ Holz, A Veblen, TT AF Kitzberger, T. Perry, G. L. W. Paritsis, J. Gowda, J. H. Tepley, A. J. Holz, A. Veblen, T. T. TI Fire-vegetation feedbacks and alternative states: common mechanisms of temperate forest vulnerability to fire in southern South America and New Zealand SO NEW ZEALAND JOURNAL OF BOTANY LA English DT Article DE Alternative stable states; Argentina; bamboo; Chile; flammability; Kunzea; Leptospermum; New Zealand; Nothofagus; rainforest; shrubland ID NORTHERN NEW-ZEALAND; SOIL SEED BANK; RAIN-FOREST; WESTERN PATAGONIA; LANDSCAPE TRANSFORMATION; NORTHWESTERN PATAGONIA; NOTHOFAGUS FORESTS; POSTFIRE RECOVERY; OFFSHORE ISLANDS; CLIMATE CHANGES AB In the context of global warming and increasing impacts of invasive plants and animals, we examine how positive fire-vegetation feedbacks are increasing the vulnerability of pyrophobic temperate forests to conversion to pyrophytic non-forest vegetation in southern South America and New Zealand. We extensively review the relevant literature to reveal how these temperate southern hemisphere floras have generated similar positive fire-vegetation feedback mechanisms resulting in increased vulnerability to anthropogenically altered fire regimens. For the two regions, we address the following questions. 1. What are the major plant species, physiognomic types and functional types characteristic of pyrophytic versus pyrophobic vegetation types and how do their traits affect flammability, resistance to fire and recovery after fire? 2. What are the roles of herbivory and microclimate in enhancing fire-vegetation feedbacks? 3. Are there similarities in trends of cover type transitions in relation to altered fire regimens? 4. How are climate change, land-use trends and the effects of introduced plants and animals affecting the vulnerability of these ecosystems to fire-induced transitions to alternative stable states? Most temperate forests of New Zealand and southern South America evolved under conditions of low fire frequencies so few taxa became adapted to recurrent fire. Current dichotomous landscapes consisting of juxtaposed pyrophobic and pyrophytic vegetation types are the outcome of the expansion of fire-resilient and fire-promoting species associated with the arrival of humans. Despite considerable differences in human history and biogeographic history, the case studies presented here show remarkable parallels in life-history traits of the key pyrophobic taxa, fire-vegetation feedback mechanisms, overall ecosystem responses to anthropogenic alteration of fire regimens, and likely vulnerability to expected global change influences on future fire regimens. C1 [Kitzberger, T.] Univ Nacl Comahue, Dept Ecol, San Carlos De Bariloche, Rio Negro, Argentina. [Kitzberger, T.; Paritsis, J.; Gowda, J. H.] Univ Nacl Comahue, CONICET, INIBIOMA, Lab Ecotono, San Carlos De Bariloche, Rio Negro, Argentina. [Perry, G. L. W.] Univ Auckland, Sch Environm, Auckland, New Zealand. [Tepley, A. J.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Holz, A.] Portland State Univ, Dept Geog, Portland, OR 97207 USA. [Veblen, T. T.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA. RP Veblen, TT (reprint author), Univ Colorado, Dept Geog, Boulder, CO 80309 USA. EM kitzberger@comahue-conicet.gob.ar OI Tepley, Alan/0000-0002-5701-9613 NR 99 TC 1 Z9 1 U1 15 U2 20 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 0028-825X EI 1175-8643 J9 NEW ZEAL J BOT JI N. Z. J. Bot. PD JUN PY 2016 VL 54 IS 2 SI SI BP 247 EP 272 DI 10.1080/0028825X.2016.1151903 PG 26 WC Plant Sciences SC Plant Sciences GA DR3TQ UT WOS:000379825900009 ER PT J AU Danner, RM Olsen, BJ Luther, D AF Danner, Raymond M. Olsen, Brian J. Luther, David TI Migratory Status, Winter Subspecies Interactions, and Habitat Segregation of Atlantic Song Sparrows (Melospiza melodia atlantica) SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article DE Atlantic Song Sparrow; habitat segregation; Melospiza melodia atlantica; migration; partial migration; winter ecology ID TEMPERATE-ZONE AB We performed the first winter surveys of the Atlantic Song Sparrow (Melospiza melodia atlantica), a poorly known subspecies that is endemic to sand dunes of the mid-Atlantic coast. Novel findings include that the Atlantic Song Sparrow is a year-round resident or partial migrant, primarily flocks with the same subspecies despite occurring in sympatry with the eastern Song Sparrow (M. m. melodia) in winter, and exhibits age-specific habitat use in winter, with immatures greatly outnumbering adults in adjacent saltmarshes. These results are important for conservation planning and understanding the ecology and evolution of this unique subspecies across the annual cycle. C1 [Danner, Raymond M.] Smithsonian Conservat Biol Inst, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Danner, Raymond M.; Luther, David] George Mason Univ, Dept Biol, Fairfax, VA 22030 USA. [Danner, Raymond M.] Univ North Carolina Wilmington, Dept Biol & Marine Biol, Wilmington, NC 28403 USA. [Olsen, Brian J.] Univ Maine, Sch Biol & Ecol, Orono, ME 04469 USA. RP Danner, RM (reprint author), Smithsonian Conservat Biol Inst, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA.; Danner, RM (reprint author), George Mason Univ, Dept Biol, Fairfax, VA 22030 USA.; Danner, RM (reprint author), Univ North Carolina Wilmington, Dept Biol & Marine Biol, Wilmington, NC 28403 USA. EM dannerR@uncw.edu OI Olsen, Brian/0000-0001-5608-2779 NR 15 TC 1 Z9 1 U1 3 U2 6 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 JUN PY 2016 VL 128 IS 2 BP 434 EP 437 PG 5 WC Ornithology SC Zoology GA DQ8GN UT WOS:000379447200021 ER PT J AU Cowie, RH Heros, V Yeung, NW Hayes, KA AF Cowie, Robert H. Heros, Virginie Yeung, Norine W. Hayes, Kenneth A. TI Annotated catalogue of types of Hawaiian land and freshwater snails (Mollusca: Gastropoda) in the Museum national d'Histoire naturelle, Paris, with lectotype designations SO ZOOSYSTEMA LA English DT Article DE Achatinellidae; Amastridae; types; Hawaii; lectotypification ID EXTINCTION; PACIFIC; SOCIETY; DECLINE AB Pacific island land snail faunas are among the most threatened faunas in the world, having suffered a higher rate of extinction than any other major animal group. The Hawaiian land snails are among the most species rich and most severely impacted of these faunas, yet the current status of most of the Hawaiian species is unknown. Most of the major taxonomic studies on the fauna were under-taken 50-100 years ago and only certain groups were comprehensively revised. New research is uncovering undescribed species, both extant and extinct. The need for rigorous taxonomic treatment of the group is acute if the validity and conservation status of the many species is to be ascertained, and the basis for such research is comprehensive study of type material. The Museum national d'Histoire naturelle, Paris, holds type material of 38 nominal species-group taxa of Hawaiian land and freshwater snails belonging to six families, overwhelmingly the Achatinellidae Gulick, 1873 and Amastridae Pilsbry, 1910; this annotated catalogue provides details of this material. We designate lectotypes for 17 species-group taxa. Name-bearing types (holotypes, lectotypes and representative syntypes) are illustrated. C1 [Cowie, Robert H.; Yeung, Norine W.] Univ Hawaii, Pacific Biosci Res Ctr, 3050 Maile Way,Gilmore 408, Honolulu, HI 96822 USA. [Heros, Virginie] Univ Paris 04, Museum Natl Hist Nat, Inst Systemat, UMR 7205,CNRS,UPMC,EPHE,Biodiversite,Evolut, Case Postale 50,57 Rue Cuvier, F-75231 Paris 05, France. [Yeung, Norine W.] Bernice P Bishop Museum, 1525 Bernice St, Honolulu, HI 96817 USA. [Yeung, Norine W.; Hayes, Kenneth A.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Hayes, Kenneth A.] Howard Univ, Dept Biol, 415 Coll St NW,EE 332, Washington, DC 20059 USA. RP Cowie, RH (reprint author), Univ Hawaii, Pacific Biosci Res Ctr, 3050 Maile Way,Gilmore 408, Honolulu, HI 96822 USA. EM cowie@hawaii.edu; malaco@mnhn.fr; nyeung@hawaii.edu; kenneth.hayes@howard.edu FU MNHN project E-RECOLNAT [ANR-11-INBS-0004]; National Science Foundation [DEB-1120906]; MNHN Visiting Curatorship FX We thank Philippe Bouchet and Neal Evenhuis for nomenclatural advice and discussion, and the latter for detailed review of the manuscript. Manuel Caballer of the MNHN project E-RECOLNAT ANR-11-INBS-0004 and Yuri Kantor helped with photography. This work is part of a US National Science Foundation funded project (DEB-1120906) and was partially supported by an MNHN Visiting Curatorship to Robert Cowie, initiated by Philippe Bouchet, whom we thank for his support. NR 69 TC 1 Z9 1 U1 2 U2 2 PU PUBLICATIONS SCIENTIFIQUES DU MUSEUM, PARIS PI PARIS CEDEX 05 PA CP 39-57, RUE CUVIER, F-75231 PARIS CEDEX 05, FRANCE SN 1280-9551 EI 1638-9387 J9 ZOOSYSTEMA JI Zoosystema PD JUN PY 2016 VL 38 IS 2 BP 245 EP 266 DI 10.5252/z2016n2a4 PG 22 WC Zoology SC Zoology GA DR6QL UT WOS:000380026300004 ER PT J AU Sousa, JPB Aguilar-Perez, MM Arnold, AE Rios, N Coley, PD Kursar, TA Cubilla-Rios, L AF Sousa, J. P. B. Aguilar-Perez, M. M. Arnold, A. E. Rios, N. Coley, P. D. Kursar, T. A. Cubilla-Rios, L. TI Chemical constituents and their antibacterial activity from the tropical endophytic fungus Diaporthe sp F2934 SO JOURNAL OF APPLIED MICROBIOLOGY LA English DT Article DE antimicrobials; chromanones; culture identification; Diaporthe sp.; endophytic fungi; Phomopsis sp.; phomosines ID PHOMOPSIS SP; BIARYL ETHERS; METABOLITES; ALKALOIDS; SIPARUNA; GENUS AB Aims: To isolate, characterize and determine the antibacterial activities of compounds produced by the endophytic fungus Diaporthe sp. F2934, cultivated on malt extract agar. Methods and Results: The fungus was cultivated aseptically in Petri dishes containing malt extract agar at 25 degrees C for 15 days. Crude extract was obtained from mycelium using ethyl acetate and sonication, and was fractioned using classic chromatography and HPLC. The structures of phomosines and chromanones were established by NMR experiments including HMQC, HMBC and COSY. Their molecular formulas were determined by ESI-TOFMS. We obtained six compounds: (1) 4H-1-benzopyra-4-one-2,3-dihydro-5-hydroxy-2,8-dimetyl, (2) 4H-1-benzopyran-4-one-2,3-dihydro-5-hydroxy-8-(hydroxy-lmethyl)-2-methyl, (3) 4H-1-benzopyra-4-one-2,3-dihydro-5-methoxyl-2,8-dimetyl, (4) phomosine A, (5) phomosine D and (6) phomosine C. Isolated compounds 1, 2 and 5 were inactive against 15 micro-organisms, but phomosines A and C were active against diverse Gram-negative and Gram-positive bacteria. Conclusions: A group of new chromanones and known phomosines have been isolated from the genus Diaporthe (Diaporthe sp. F2934). The results obtained confirm the wide chemical diversity produced by endophytic fungi, specifically the genus Diaporthe. In addition, phomosines A and C may be considered as antimicrobial agents that can be used to guide the development of new antibiotics. Significance and Impact of the Study: Our phylogenetic analysis places Diaporthe sp. F2934 as sister to the Diaporthe cynaroidis clade. Three chromanones were isolated and identified, for the first time, using crude extract obtained from Diaporthe F2934. From this extract phomosines A, C and D were also purified. Regarding Staphylococcus aureus, the inhibition zone diameter (IZD) for phomosine A was 20% higher than the standard drug, vancomycin. When cultivated as described here, Diaporthe sp. F2934 produced new and antimicrobial compounds. C1 [Sousa, J. P. B.; Aguilar-Perez, M. M.; Cubilla-Rios, L.] Smithsonian Trop Res Inst, Panama City, Panama. [Aguilar-Perez, M. M.; Cubilla-Rios, L.] Univ Panama, Fac Nat & Exact Sci & Technol, Lab Trop Bioorgan Chem, Panama City, Panama. [Arnold, A. E.] Univ Arizona, Sch Plant Sci, Tucson, AZ USA. [Arnold, A. E.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ USA. [Rios, N.] Univ Panama, Dept Microbiol, Panama City, Panama. [Coley, P. D.; Kursar, T. A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. RP Cubilla-Rios, L (reprint author), Univ Panama, Fac Nat & Exact Sci & Technol, Lab Trop Bioorgan Chem, Panama City, Panama. EM luis.cubilla@up.ac.pa FU Global Environment Facility (GEF) through the Project of Nagoya Protocols Application in Panama; U.S. NIH FX The Global Environment Facility (GEF) through the Project of Nagoya Protocols Application in Panama supported this work. We also give our thanks to the personnel of Panama's Ministry of Environment, for their assistance in conducting this research project; and we thank the long-standing support given by a U.S. NIH grant for the International Cooperative Biodiversity Groups Program establish in Panama (ICBG-Panama). NR 34 TC 0 Z9 0 U1 14 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1364-5072 EI 1365-2672 J9 J APPL MICROBIOL JI J. Appl. Microbiol. PD JUN PY 2016 VL 120 IS 6 BP 1501 EP 1508 DI 10.1111/jam.13132 PG 8 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA DQ9MU UT WOS:000379534800005 PM 26991693 ER PT J AU Norrgard, EB Sitaraman, N Barry, JF McCarron, DJ Steinecker, MH DeMille, D AF Norrgard, E. B. Sitaraman, N. Barry, J. F. McCarron, D. J. Steinecker, M. H. DeMille, D. TI In-vacuum scattered light reduction with black cupric oxide surfaces for sensitive fluorescence detection SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID DIATOMIC MOLECULE; GROWTH AB We demonstrate a simple and easy method for producing low-reflectivity surfaces that are ultra-high vacuum compatible, may be baked to high temperatures, and are easily applied even on complex surface geometries. Black cupric oxide (CuO) surfaces are chemically grown in minutes on any copper surface, allowing for low-cost, rapid prototyping, and production. The reflective properties are measured to be comparable to commercially available products for creating optically black surfaces. We describe a vacuum apparatus which uses multiple blackened copper surfaces for sensitive, low-background detection of molecules using laser-induced fluorescence. Published by AIP Publishing. C1 [Norrgard, E. B.; Sitaraman, N.; Barry, J. F.; McCarron, D. J.; Steinecker, M. H.; DeMille, D.] Yale Univ, Dept Phys, POB 208120, New Haven, CT 06520 USA. [Sitaraman, N.] Cornell Univ, Dept Phys, 142 Sci Dr, Ithaca, NY 14853 USA. [Barry, J. F.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Norrgard, EB (reprint author), Yale Univ, Dept Phys, POB 208120, New Haven, CT 06520 USA. EM eric.norrgard@yale.edu RI McCarron, Daniel/M-7341-2016 OI McCarron, Daniel/0000-0002-8562-3439 FU ARO; ARO (MURI); NSF GRFP; Yale College Dean's Research Fellowship FX The authors thank E. R. Edwards for contributions toward the construction of the vacuum chamber. The authors acknowledge financial support from ARO and ARO (MURI). E.B.N. acknowledges funding from the NSF GRFP. N.S. acknowledges funding from Yale College Dean's Research Fellowship. NR 25 TC 0 Z9 0 U1 4 U2 5 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0034-6748 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD JUN PY 2016 VL 87 IS 5 AR 053119 DI 10.1063/1.4949503 PG 6 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA DQ4QE UT WOS:000379187600039 PM 27250404 ER PT J AU Graves, GR Tedford, BL AF Graves, Gary R. Tedford, Bruce L. TI Common Denominators of Swainson's Warbler Breeding Habitat in Bottomland Hardwood Forest in the White River Watershed in Southeastern Arkansas SO SOUTHEASTERN NATURALIST LA English DT Article ID SELECTION; RANGE; PARASITISM; TERRITORY; ECOLOGY; BIRDS; RATES; USA AB The most intensively studied breeding population of Limnothlypis swainsonii (Swainson's Warbler) is in the White River watershed of southeastern Arkansas. However, because vegetation sampling protocols employed at this site have been significantly different from those used elsewhere, it has been difficult for land managers to reconcile datasets across the species' range in order to construct consensus quantitative benchmarks for optimal breeding habitat in bottomland hardwoods. We used a standardized sampling protocol to compare the physiognomic and floristic characteristics of breeding territories at 2 sites in the White River watershed with comparable data from other populations in Arkansas, Mississippi, Louisiana, Florida, and Virginia. Breeding territories in the combined dataset for this rare migratory species varied substantially in successional stage, floristic diversity, hydrology, and management history. Visual screening provided by understory thickets of saplings, vine tangles, and shrubs emerged as the most important common denominator of breeding territories in bottomland hardwood forests across the warbler's breeding range. Basal area, abundance of trees in larger-diameter classes, and floristic diversity appear to have little direct influence on habitat selection across the species' range. Although warblers are often associated with Arundinaria spp. (canebrakes), some of the most robust breeding populations occur in cane-free areas. Land managers tasked with generating and sustaining prime breeding habitat should strive for high counts of small woody stems (> 45,000/ha or 4.5/m(2)) in areas that are infrequently subjected to flooding. This benchmark can be achieved through periodic canopy thinning and agroforestry clearcutting. C1 [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC 116,POB 37012, Washington, DC 20013 USA. [Graves, Gary R.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark. [Tedford, Bruce L.] Arkansas Tech Univ, Dept Biol Sci, 1701 North Boulder Ave, Russellville, AR 72801 USA. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC 116,POB 37012, Washington, DC 20013 USA.; Graves, GR (reprint author), Univ Copenhagen, Nat Hist Museum Denmark, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark. EM gravesg@si.edu RI publicationpage, cmec/B-4405-2017 FU Research Opportunities Fund; Alexander Wetmore Fund of the Smithsonian Institution; USFWS [14-48-0005-92-9013, 14-48-0009-946]; Smoketree Trust FX We thank John Gerwin, T.J. Benson, Karl E. Miller, and 2 anonymous reviewers for providing critiques of the manuscript, and the USFWS and Anderson-Tully Lumber Company (ATLC) for access to lands. Richard Hines (USFWS), Pam Hines, and Mike Staten (ATLC) provided logistical support in St. Charles and on Big Island. Funding (1988-2014) was provided by the Research Opportunities Fund and the Alexander Wetmore Fund of the Smithsonian Institution, the USFWS (14-48-0005-92-9013 and 14-48-0009-946) for surveys in the Great Dismal Swamp, and by the Smoketree Trust. NR 52 TC 0 Z9 0 U1 4 U2 6 PU HUMBOLDT FIELD RESEARCH INST PI STEUBEN PA PO BOX 9, STEUBEN, ME 04680-0009 USA SN 1528-7092 EI 1938-5412 J9 SOUTHEAST NAT JI Southeast. Nat. PD JUN PY 2016 VL 15 IS 2 BP 315 EP 330 PG 16 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA DQ7AN UT WOS:000379359000014 ER PT J AU Holtum, JAM Hancock, LP Edwards, EJ Crisp, MD Crayn, DM Sage, R Winter, K AF Holtum, Joseph A. M. Hancock, Lillian P. Edwards, Erika J. Crisp, Michael D. Crayn, Darren M. Sage, Rowan Winter, Klaus TI Australia lacks stem succulents but is it depauperate in plants with crassulacean acid metabolism (CAM)? SO CURRENT OPINION IN PLANT BIOLOGY LA English DT Review ID PORTULACINEAE CARYOPHYLLALES; PHOTOSYNTHESIS; EVOLUTION; C-4; PORTULACACEAE; PERSPECTIVE; RADIATIONS; WORLD AB In the flora of Australia, the driest vegetated continent, crassulacean acid metabolism (CAM), the most water-use efficient form of photosynthesis, is documented in only 0.6% of native species. Most are epiphytes and only seven terrestrial. However, much of Australia is unsurveyed, and carbon isotope signature, commonly used to assess photosynthetic pathway diversity, does not distinguish between plants with low-levels of CAM and C3 plants. We provide the first census of CAM for the Australian flora and suggest that the real frequency of CAM in the flora is double that currently known, with the number of terrestrial CAM species probably 10-fold greater. Still unresolved is the question why the large stem-succulent life form is absent from the native Australian flora even though exotic large cacti have successfully invaded and established in Australia. C1 [Holtum, Joseph A. M.] James Cook Univ, Coll Marine & Environm Sci, Terr Ecosyst & Climate Change, Townsville, Qld 4811, Australia. [Holtum, Joseph A. M.; Winter, Klaus] Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Ancon, Panama. [Hancock, Lillian P.; Edwards, Erika J.] Brown Univ, Dept Ecol & Evolutionary Biol, Box G-W, Providence, RI 02912 USA. [Crisp, Michael D.] Australian Natl Univ, Res Sch Biol, Canberra, ACT 2601, Australia. [Crayn, Darren M.] James Cook Univ, Australian Trop Herbarium, POB 6811, Cairns, Qld 4870, Australia. [Sage, Rowan] Univ Toronto, Dept Ecol & Evolutionary Biol, Toronto, ON M5S 1A1, Canada. RP Holtum, JAM (reprint author), James Cook Univ, Coll Marine & Environm Sci, Terr Ecosyst & Climate Change, Townsville, Qld 4811, Australia.; Holtum, JAM (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Ancon, Panama. EM joseph.holtum@jcu.edu.au RI Crisp, Michael/A-4888-2008; OI Crisp, Michael/0000-0002-8255-6349; Crayn, Darren/0000-0001-6614-4216 FU Australian Research Council [DP160100098]; U.S. National Science Foundation [DEB-1252901]; Smithsonian Tropical Research Institute FX This research was supported by the Australian Research Council Discovery Project DP160100098 by the U.S. National Science Foundation grant DEB-1252901, and by the Smithsonian Tropical Research Institute. NR 47 TC 1 Z9 1 U1 9 U2 13 PU CURRENT BIOLOGY LTD PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 1369-5266 EI 1879-0356 J9 CURR OPIN PLANT BIOL JI Curr. Opin. Plant Biol. PD JUN PY 2016 VL 31 BP 109 EP 117 DI 10.1016/j.pbi.2016.03.018 PG 9 WC Plant Sciences SC Plant Sciences GA DQ3LF UT WOS:000379103100016 PM 27088716 ER PT J AU Wirshing, HH Baker, AC AF Wirshing, Herman H. Baker, Andrew C. TI On the difficulty of recognizing distinct Symbiodinium species in mixed communities of algal symbionts SO MOLECULAR ECOLOGY LA English DT Editorial Material DE coral reef; host flexibility; octocoral; species; Symbiodinium ID GENUS SYMBIODINIUM; CORAL ENDOSYMBIONTS; RARE ALLELES; SP NOV.; DINOPHYCEAE; HOST; BIODIVERSITY; DELIMITATION; FREUDENTHAL; POPULATION C1 [Wirshing, Herman H.] Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012,NHB MRC 163, Washington, DC 20013 USA. [Baker, Andrew C.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Dept Marine Biol & Ecol, 4600 Rickenbacker Cswy, Miami, FL 33149 USA. RP Wirshing, HH (reprint author), Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012,NHB MRC 163, Washington, DC 20013 USA. EM wirshingh@si.edu NR 27 TC 0 Z9 0 U1 2 U2 5 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 JUN PY 2016 VL 25 IS 12 BP 2724 EP 2726 DI 10.1111/mec.13676 PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA DQ1DQ UT WOS:000378941800006 PM 27265255 ER PT J AU Tu, QC Deng, Y Yan, QY Shen, LN Lin, L He, ZL Wu, LY Van Nostrand, JD Buzzard, V Michaletz, ST Enquist, BJ Weiser, MD Kaspari, M Waide, RB Brown, JH Zhou, JZ AF Tu, Qichao Deng, Ye Yan, Qingyun Shen, Lina Lin, Lu He, Zhili Wu, Liyou Van Nostrand, Joy D. Buzzard, Vanessa Michaletz, Sean T. Enquist, Brian J. Weiser, Michael D. Kaspari, Michael Waide, Robert B. Brown, James H. Zhou, Jizhong TI Biogeographic patterns of soil diazotrophic communities across six forests in the North America SO MOLECULAR ECOLOGY LA English DT Article DE biogeography; diversity gradients; nifH; soil diazotrophs; taxa-area relationship ID LATITUDINAL DIVERSITY GRADIENT; SPECIES-AREA RELATIONSHIP; BACTERIAL COMMUNITIES; GENE DIVERSITY; HABITAT HETEROGENEITY; MICROBIAL COMMUNITIES; GLOBAL PATTERNS; BIODIVERSITY; FIXATION; MICROENVIRONMENTS AB Soil diazotrophs play important roles in ecosystem functioning by converting atmospheric N-2 into biologically available ammonium. However, the diversity and distribution of soil diazotrophic communities in different forests and whether they follow biogeographic patterns similar to macroorganisms still remain unclear. By sequencing nifH gene amplicons, we surveyed the diversity, structure and biogeographic patterns of soil diazotrophic communities across six North American forests (126 nested samples). Our results showed that each forest harboured markedly different soil diazotrophic communities and that these communities followed traditional biogeographic patterns similar to plant and animal communities, including the taxa-area relationship (TAR) and latitudinal diversity gradient. Significantly higher community diversity and lower microbial spatial turnover rates (i.e. z-values) were found for rainforests (similar to 0.06) than temperate forests (similar to 0.1). The gradient pattern of TARs and community diversity was strongly correlated (r(2) > 0.5) with latitude, annual mean temperature, plant species richness and precipitation, and weakly correlated (r(2) < 0.25) with pH and soil moisture. This study suggests that even microbial subcommunities (e.g. soil diazotrophs) follow general biogeographic patterns (e.g. TAR, latitudinal diversity gradient), and indicates that the metabolic theory of ecology and habitat heterogeneity may be the major underlying ecological mechanisms shaping the biogeographic patterns of soil diazotrophic communities. C1 [Tu, Qichao; Lin, Lu] Zhejiang Univ, Ocean Coll, Dept Marine Sci, Hangzhou 310058, Zhejiang, Peoples R China. [Tu, Qichao; Yan, Qingyun; Shen, Lina; He, Zhili; Wu, Liyou; Van Nostrand, Joy D.; Zhou, Jizhong] Univ Oklahoma, Inst Environm Genom, Dept Microbiol & Plant Biol, Norman, OK 73019 USA. [Deng, Ye] Chinese Acad Sci, Res Ctr Ecoenvironm Sci, Beijing 100085, Peoples R China. [Buzzard, Vanessa; Michaletz, Sean T.; Enquist, Brian J.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. [Michaletz, Sean T.] Los Alamos Natl Lab, Earth & Environm Sci Div, MS J495, Los Alamos, NM 87545 USA. [Enquist, Brian J.] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. [Weiser, Michael D.; Kaspari, Michael] Univ Oklahoma, Dept Biol, EEB Grad Program, Norman, OK 73019 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa 084303092, Panama. [Waide, Robert B.; Brown, James H.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Zhou, Jizhong] Tsinghua Univ, Sch Environm, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100084, Peoples R China. [Zhou, Jizhong] Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA 94270 USA. RP Zhou, JZ (reprint author), Univ Oklahoma, Inst Environm Genom, Dept Microbiol & Plant Biol, Norman, OK 73019 USA.; Zhou, JZ (reprint author), Tsinghua Univ, Sch Environm, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100084, Peoples R China.; Zhou, JZ (reprint author), Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA 94270 USA. EM jzhou@ou.edu OI Michaletz, Sean/0000-0003-2158-6525; ?, ?/0000-0002-7584-0632 FU U.S. National Science Foundation [NSF EF-1065844]; Office of the Vice President for Research at the University of Oklahoma; Collaborative Innovation Center for Regional Environmental Quality; State Key Joint Laboratory of Environment Simulation and Pollution Control FX This study was supported by the U.S. National Science Foundation MacroSystems Biology programme under the contract (NSF EF-1065844), by the Office of the Vice President for Research at the University of Oklahoma, by the Collaborative Innovation Center for Regional Environmental Quality and by the State Key Joint Laboratory of Environment Simulation and Pollution Control. NR 73 TC 1 Z9 1 U1 15 U2 29 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 JUN PY 2016 VL 25 IS 12 BP 2937 EP 2948 DI 10.1111/mec.13651 PG 12 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA DQ1DQ UT WOS:000378941800020 PM 27085668 ER PT J AU Brown, WR AF Brown, Warren R. TI Hypervelocity stars in the Milky Way SO PHYSICS TODAY LA English DT Article ID GALACTIC-CENTER; BLACK-HOLE; HALO AB Because gravity keeps stars on their orbits, astronomers can use the motions of stars to infer the mass distribution of the visible and invisible constituents of the Milky Way. The Milky Way is the only galaxy whose visible mass distribution we can see in three dimensions and in which we can accurately measure the velocities of millions of individual stars. Gravitational accelerations in the galaxy are usually small, however. Our sun, for instance, experiences a gravitational acceleration of just 2 angstrom/s(2) as it orbits the Milky Way. That's 10(-11) of what we experience on Earth's surface. It's also the gravitational-acceleration regime of dark matter-the unseen material inferred to exist in and around galaxies. C1 [Brown, Warren R.] Smithsonian Astrophys Observ, Cambridge, MA USA. RP Brown, WR (reprint author), Smithsonian Astrophys Observ, Cambridge, MA USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0031-9228 EI 1945-0699 J9 PHYS TODAY JI Phys. Today PD JUN PY 2016 VL 69 IS 6 BP 53 EP 58 PG 6 WC Physics, Multidisciplinary SC Physics GA DQ4MU UT WOS:000379178800020 ER PT J AU Graddy, LK AF Graddy, Lisa Kathleen TI Ida McKinley: The Turn-of-the-Century First Lady through War, Assassination, and Secret Disability SO HISTORIAN LA English DT Book Review C1 [Graddy, Lisa Kathleen] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Graddy, LK (reprint author), Smithsonian Inst, Natl Museum Amer Hist, 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 0018-2370 EI 1540-6563 J9 HISTORIAN JI Historian PD SUM PY 2016 VL 78 IS 2 BP 313 EP 315 DI 10.1111/hisn.12167 PG 3 WC History SC History GA DP5MM UT WOS:000378541600007 ER PT J AU Rota, J Pena, C Miller, SE AF Rota, Jadranka Pena, Carlos Miller, Scott E. TI The importance of long-distance dispersal and establishment events in small insects: historical biogeography of metalmark moths (Lepidoptera, Choreutidae) SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE founder-event dispersal; insect flight; insect migration; microlepidoptera; oceanic islands; vicariance ID CONVECTIVE BOUNDARY-LAYER; BUTTERFLY GENUS; PHYLOGENETIC INFERENCE; GEOGRAPHIC RANGE; FLIGHT BEHAVIOR; NEW-GUINEA; EVOLUTION; DIVERSIFICATION; HYPOTHESIS; NYMPHALIDAE AB Aim To determine the importance of different biogeographical processes (vicariance, dispersal, long-distance dispersal and establishment or LDDE) for the current distribution of metalmark moths, a group of small insects, using a time-calibrated molecular tree. Location Global. Methods We sampled 104 species of metalmark moths with representatives from all six major biogeographical regions of the world (Afrotropical, Australasian, Neotropical, Nearctic, Oriental and Palaearctic). The taxon sampling includes c. 20% of known species in the family and covers both subfamilies. Using an eight-locus molecular data set and secondary calibration points, we inferred a time-calibrated tree, which was then used for ancestral range estimation with variants of the dispersal-extinction-cladogenesis model (DEC), some of which incorporated the founder-event j-parameter for modelling of LDDEs (DECj). Results The inferred phylogeny is well resolved and in accordance with earlier works. The metalmark moth distribution is best explained with DECj models. It remains unclear what the ancestral area was. Different models differ in the number and type of events estimated - DEC models infer vicariance for several nodes where DECj models usually infer LDDEs. However, the pattern that emerges from all the analyses is that dispersal and/or LDDE over transoceanic distances such as between the Afrotropics and Australasia and the Afrotropics and Neotropics occurred several times in the evolutionary history of this group. Main conclusions Vicariance may have played an important role in the early evolution of metalmark moths, while dispersal and LDDEs mostly shaped the group's distribution later on. Based on insect flight research using aerial radars, the best mechanism for explaining how small insects cross oceans is by being adapted for exploiting atmospheric conditions as opposed to employing active flight. C1 [Rota, Jadranka; Pena, Carlos] Univ Turku, Dept Biol, FI-20014 Turku, Finland. [Rota, Jadranka] Lund Univ, Dept Biol, Lund, Sweden. [Miller, Scott E.] Smithsonian Inst, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. RP Rota, J (reprint author), Lund Univ, Dept Biol, Lund, Sweden. EM jadranka.rota@biol.lu.se RI Rota, Jadranka/C-6702-2011; OI Rota, Jadranka/0000-0003-0220-3920; Miller, Scott/0000-0002-4138-1378 FU US National Science Foundation [DEB-0211591, 0515678]; Czech Science Foundation [206/09/0115]; Czech Ministry of Education [CZ.1.-07/2.3.00/20.0064]; European Union [CZ.1.-07/2.3.00/20.0064]; Genome Canada; Ontario Genomics Institute; Academy of Finland [265511] FX The Papua New Guinea (PNG) specimens come from a rearing campaign led by Vojtech Novotny, George Weiblen, Yves Basset and Scott Miller, and supported by the US National Science Foundation (grants DEB-0211591, 0515678 and others), Czech Science Foundation grant 206/09/0115 and others, and Czech Ministry of Education & European Union grant CZ.1.-07/2.3.00/20.0064. We thank the staff at the PNG Binatang Research Center for field assistance, PNG land owners for access to field sites and assistance, and PNG agencies for permits. For many other specimens we thank the following people: David Agassiz, Roland Breithaupt, Jurate De Prins, Jason Dombroskie, Ole Karsholt, Dave Wagner, Shen-Horn Yen and the late Janusz Wojtusiak. DNA barcodes were largely provided by Paul Hebert through a grant from Genome Canada and the Ontario Genomics Institute in support of the iBOL project. Karolyn Darrow, Lauren Helgen and Margaret Rosati provided assistance at the Smithsonian. We thank Pavel Matos-Maravi and Niklas Wahlberg for helpful discussion of many aspcts of this project. Thanks are due to two anonymous referees, Lukasz Banasiak, and Fabien L. Condamine, whose comments greatly improved the manuscript. We also thank Nick Matzke for answering our questions about BioGeoBEARS. J.R. was funded by the Finnish Kone Foundation experienced researcher grant during this project; and C.P. was funded by the Academy of Finland Grant No. 265511 awarded to Niklas Wahlberg. NR 75 TC 4 Z9 4 U1 11 U2 20 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 JUN PY 2016 VL 43 IS 6 BP 1254 EP 1265 DI 10.1111/jbi.12721 PG 12 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA DP7WX UT WOS:000378711000016 ER PT J AU Friscia, A Sanin, GD Lindsay, WR Day, LB Schlinger, BA Tan, J Fuxjager, MJ AF Friscia, Anthony Sanin, Gloria D. Lindsay, Willow R. Day, Lainy B. Schlinger, Barney A. Tan, Josh Fuxjager, Matthew J. TI Adaptive Evolution of a Derived Radius Morphology in Manakins (Aves, Pipridae) to Support Acrobatic Display Behavior SO JOURNAL OF MORPHOLOGY LA English DT Article DE avian skeleton; sexual selection; courtship display; manakin; passerine bird ID GOLDEN-COLLARED-MANAKINS; ELABORATE MALE COURTSHIP; FINITE-ELEMENT-ANALYSIS; SPEED VIDEO ANALYSIS; AVIAN HYBRID ZONE; MANACUS-VITELLINUS; SEXUAL SELECTION; FEMALE CHOICE; BIRDS; BONE AB The morphology of the avian skeleton is often studied in the context of adaptations for powered flight. The effects of other evolutionary forces, such as sexual selection, on avian skeletal design are unclear, even though birds produce diverse behaviors that undoubtedly require a variety of osteological modifications. Here, we investigate this issue in a family of passerine birds called manakins (Pipridae), which have evolved physically unusual and elaborate courtship displays. We report that, in species within the genus Manacus, the shaft of the radius is heavily flattened and shows substantial solidification. Past work anecdotally notes this morphology and attributes it to the species' ability to hit their wings together above their heads to produce loud mechanical sonations. Our results show that this feature is unique to Manacus compared to the other species in our study, including a variety of taxa that produce other sonations through alternate wing mechanisms. At the same time, our data reveal striking similarities across species in total radius volume and solidification. Together, this suggests that supposedly adaptive alterations in radial morphology occur within a conserved framework of a set radius volume and solidness, which in turn is likely determined by natural selection. Further allometric analyses imply that the radius is less constrained by body size and the structural demands that underlie powered flight, compared to other forelimb bones that are mostly unmodified across taxa. These results are consistent with the idea that the radius is more susceptible to selective modification by sexual selection. Overall, this study provides some of the first insight into the osteological evolution of passerine birds, as well as the way in which opposing selective forces can shape skeletal design in these species. (C) 2016 Wiley Periodicals, Inc. C1 [Friscia, Anthony; Schlinger, Barney A.] Univ Calif Los Angeles, Dept Integrat Biol & Physiol, Los Angeles, CA 90095 USA. [Sanin, Gloria D.; Fuxjager, Matthew J.] Wake Forest Univ, Dept Biol, Winston Salem, NC 27109 USA. [Lindsay, Willow R.] Gothenburg Univ, Dept Biol & Environm Sci, Gothenburg, Sweden. [Lindsay, Willow R.; Day, Lainy B.] Univ Mississippi, Dept Biol, University, MS 38677 USA. [Schlinger, Barney A.] Univ Calif Los Angeles, Neuroendocrinol Lab, Los Angeles, CA 90095 USA. [Schlinger, Barney A.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Schlinger, Barney A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Tan, Josh] Wake Forest Univ, Bowman Gray Sch Med, Dept Radiol, 300 S Hawthorne Rd, Winston Salem, NC 27157 USA. RP Fuxjager, MJ (reprint author), Wake Forest Univ, Dept Biol, Winston Salem, NC 27109 USA. EM mfoxhunter@gmail.com FU Wake Forest University FX We thank A. Tripati, R. Eagle, E. Schuppe, and D. Birds for help using the micro-CT and technical assistance with data collection and interpretation. We thank Joel Stitzel for allowing us to use Mimics software. We thank K. Garret at the Los Angeles Museum of Natural History for providing the cotinga and phoebe specimens, as well as B. Van Valkenburgh for providing valuable insight into this manuscript. We also thank STRI and its administrative staff for their assistance with this project as well as Autoridad Nacional del Ambiente and the Autoridad del Canal de Panama for permission to conduct these studies. This work was funded by intramural start-up funds from Wake Forest University (to M.J.F.). NR 48 TC 1 Z9 1 U1 18 U2 21 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0362-2525 EI 1097-4687 J9 J MORPHOL JI J. Morphol. PD JUN PY 2016 VL 277 IS 6 BP 766 EP 775 DI 10.1002/jmor.20534 PG 10 WC Anatomy & Morphology SC Anatomy & Morphology GA DP8IK UT WOS:000378741400006 PM 27027525 ER PT J AU Torres-Mendoza, D Gonzalez, Y Gomez-Reyes, JF Guzman, HM Lopez-Perez, JL Gerwick, WH Fernandez, PL Gutierrez, M AF Torres-Mendoza, Daniel Gonzalez, Yisett Felix Gomez-Reyes, Jose Guzman, Hector M. Luis Lopez-Perez, Jose Gerwick, William H. Fernandez, Patricia L. Gutierrez, Marcelino TI Uprolides N, O and P from the Panamanian Octocoral Eunicea succinea SO MOLECULES LA English DT Article DE Eunicea succinea; cembranolide diterpenes; uprolides; anti-inflammatory ID CARIBBEAN GORGONIAN OCTOCORAL; CEMBRANOLIDES; DITERPENOIDS; MAMMOSA AB Three new diterpenes, uprolide N (1), uprolide O (2), uprolide P (3) and a known one, dolabellane (4), were isolated from the CH2Cl2-MeOH extract of the gorgonian octocoral Eunicea succinea, collected from Bocas del Toro, on the Caribbean coast of Panama. Their structures were determined using spectroscopic analyses, including 1D and 2D NMR and high-resolution mass spectrometry (HRMS) together with molecular modeling studies. Compounds 1-3 displayed anti-inflammatory properties by inhibiting production of Tumor Necrosis Factor (TNF) and Interleukin (IL)-6 induced by lipopolysaccharide (LPS) in murine macrophages. C1 [Torres-Mendoza, Daniel; Felix Gomez-Reyes, Jose; Gutierrez, Marcelino] Inst Sci Res & Technol Serv INDICASAT, Ctr Biodivers & Drug Discovery, City Of Knowledge 084301103, Panama. [Torres-Mendoza, Daniel; Gonzalez, Yisett] Acharya Nagarjuna Univ, Dept Biotechnol, Nagarjuna Nagar 522510, Guntur, India. [Gonzalez, Yisett; Fernandez, Patricia L.] Inst Sci Res & Technol Serv INDICASAT, Ctr Mol & Cellular Biol Dis, City Of Knowledge 084301103, Panama. [Guzman, Hector M.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. [Luis Lopez-Perez, Jose] Univ Salamanca, Dept Pharmaceut Sci, Fac Pharm, Ave Campo Charro S-N, Salamanca 37007, Spain. [Gerwick, William H.] Univ Calif San Diego, Ctr Marine Biotechnol & Biomed, Scripps Inst Oceanog, La Jolla, CA 92037 USA. [Gerwick, William H.] Univ Calif San Diego, Skaggs Sch Pharm & Pharmaceut Sci, La Jolla, CA 92037 USA. RP Gutierrez, M (reprint author), Inst Sci Res & Technol Serv INDICASAT, Ctr Biodivers & Drug Discovery, City Of Knowledge 084301103, Panama. EM dtorres@indicasat.org.pa; yisettgonzalez@gmail.com; gomezjosefelix@gmail.com; guzmanh@si.edu; lopez@usal.es; wgerwick@ucsd.edu; pllanes@indicasat.org.pa; mgutierrez@indicasat.org.pa OI Torres-Mendoza, Daniel/0000-0002-3540-4238 FU National Secretariat for Science and Technology of Panama (SENACYT) [COL08-061, COL09-047]; Fogarty International Center's International Cooperative Biodiversity Groups program [TW006634]; Global Environmental Fund [GEF ID 4780-UNDP 81860]; SENACYT-IFARHU FX We gratefully acknowledge the Government of Panama (Ministerio de Ambiente) for granting permission to collect the coral used in this study. This work was partially supported by the National Secretariat for Science and Technology of Panama (SENACYT, grant numbers COL08-061 and COL09-047), the Fogarty International Center's International Cooperative Biodiversity Groups program (grant number TW006634), and the Global Environmental Fund (GEF ID 4780-UNDP 81860). We thank Carlos Guevara for his assistance during the collections trips. Daniel Torres-Mendoza and Yisett Gonzalez thank SENACYT-IFARHU for financial support. NR 17 TC 0 Z9 0 U1 1 U2 1 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 1420-3049 J9 MOLECULES JI Molecules PD JUN PY 2016 VL 21 IS 6 AR 819 DI 10.3390/molecules21060819 PG 11 WC Chemistry, Organic SC Chemistry GA DP8ON UT WOS:000378757600141 ER PT J AU Rocha, R Gordo, M Lopez-Baucells, A AF Rocha, Ricardo Gordo, Marcelo Lopez-Baucells, Adria TI Completing the menu: addition of Scinax cruentommus and Scinax cf. garbei (Anura: Hylidae) to the diet of Trachops cirrhosus (Chiroptera: Phyllostomidae) in Central Amazon SO NORTH-WESTERN JOURNAL OF ZOOLOGY LA English DT Letter ID BAT PREDATION; FROG; VOCALIZATIONS; PANAMA; CALLS C1 [Rocha, Ricardo; Lopez-Baucells, Adria] Univ Lisbon, Ctr Ecol Evolut & Environm Changes, Fac Ciencias, Bloco C2, P-1749016 Lisbon, Portugal. [Rocha, Ricardo; Lopez-Baucells, Adria] Univ Helsinki, Metapopulat Res Grp, Fac Biosci, POB 65,Viikinkaari 1, FI-00014 Helsinki, Finland. [Rocha, Ricardo] Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, CP 478, BR-69011970 Manaus, Amazonas, Brazil. [Rocha, Ricardo] Smithsonian Trop Res Inst, CP 478, BR-69011970 Manaus, Amazonas, Brazil. [Gordo, Marcelo] Univ Fed Amazonas, Dept Biol, Inst Ciencias Biol, Ave Gen Rodrigo Octavio Jordao Ramos 3000, BR-69077000 Manaus, Amazonas, Brazil. [Lopez-Baucells, Adria] Museu Ciencies Nat Granollers, Area Invest Quiropters, Ave Francesc Macia 51, Granollers 08402, Catalonia, Spain. RP Rocha, R (reprint author), Univ Lisbon, Ctr Ecol Evolut & Environm Changes, Fac Ciencias, Bloco C2, P-1749016 Lisbon, Portugal.; Rocha, R (reprint author), Univ Helsinki, Metapopulat Res Grp, Fac Biosci, POB 65,Viikinkaari 1, FI-00014 Helsinki, Finland.; Rocha, R (reprint author), Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, CP 478, BR-69011970 Manaus, Amazonas, Brazil.; Rocha, R (reprint author), Smithsonian Trop Res Inst, CP 478, BR-69011970 Manaus, Amazonas, Brazil. EM ricardo.nature@gmail.com NR 32 TC 0 Z9 0 U1 1 U2 2 PU UNIV ORADEA PUBL HOUSE PI ORADEA PA UNIVERSITATII NR 1, ORADEA, 410087, ROMANIA SN 1584-9074 EI 1842-6441 J9 NORTH-WEST J ZOOL JI North-West. J. Zool. PD JUN PY 2016 VL 12 IS 1 BP 199 EP U201 AR e157501 PG 3 WC Zoology SC Zoology GA DP3SO UT WOS:000378415600025 ER PT J AU Cai, WJ Matthews, JH Paul, VJ Luesch, H AF Cai, Weijing Matthews, James H. Paul, Valerie J. Luesch, Hendrik TI Pitiamides A and B, Multifunctional Fatty Acid Amides from Marine Cyanobacteria SO PLANTA MEDICA LA English DT Article DE Marine cyanobacteria; fatty acid amides; pitiamides; antiproliferative activity; membrane hyperpolarization ID LYNGBYA-MAJUSCULA; METABOLITES; ASSEMBLAGE; CELL AB Two geometric isomers related to pitiamide A, termed 1E-pitiamide B (1) and 1Z-pitiamide B (2), were isolated from a marine cyanobacterium collected from the shallow reef flat at Piti Bomb Holes, Guam, Mariana Islands. The structures of these analogues were elucidated using 1D and 2D NMR analysis. Pitiamide A, which has been previously described, but has not been investigated in bioassays, was co-isolated. Pitiamides A and B were subjected to a biological evaluation and they both showed antiproliferative effects on HCT116 cells with IC50 values of 1-5 mu M. Pitiamide Awas investigated individually and caused plasma membrane hyperpolarization and an increase of intracellular calcium in HCT116 cells. C1 [Cai, Weijing; Matthews, James H.; Luesch, Hendrik] Univ Florida, Dept Med Chem, 1345 Ctr Dr, Gainesville, FL 32610 USA. [Cai, Weijing; Matthews, James H.; Luesch, Hendrik] Univ Florida, CNPD3, Gainesville, FL USA. [Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL USA. RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, 1345 Ctr Dr, Gainesville, FL 32610 USA. EM luesch@cop.ufl.edu FU National Institutes of Health, NCI [R01CA172310] FX This research was supported by the National Institutes of Health, NCI grant R01CA172310. We are grateful to L. Spiers for assistance with the collection of the cyanobacterium and J. Biggs for general support on Guam. NR 20 TC 1 Z9 1 U1 1 U2 4 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 0032-0943 EI 1439-0221 J9 PLANTA MED JI Planta Med. PD JUN PY 2016 VL 82 IS 9-10 SI SI BP 897 EP 902 DI 10.1055/s-0042-105157 PG 6 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA DQ0TN UT WOS:000378913600016 PM 27135625 ER PT J AU Einzmann, HJR Zotz, G AF Einzmann, Helena Julia Regina Zotz, Gerhard TI How diverse are epiphyte assemblages in plantations and secondary forests in tropical lowlands? SO TROPICAL CONSERVATION SCIENCE LA English DT Article DE accidental epiphyte; land-use change; plantations; secondary forest; vascular epiphytes ID OIL PALM PLANTATIONS; VASCULAR EPIPHYTES; MANAGEMENT INTENSITY; COFFEE PLANTATIONS; CACAO PLANTATIONS; CENTRAL VERACRUZ; CLOUD FOREST; RAIN-FOREST; COSTA-RICA; BIODIVERSITY AB The on-going destruction of old-growth forests puts tropical forest species under great pressure because of the resulting loss of habitat. An important biotic component of these forests are vascular epiphytes, which structurally depend on trees. In human-modified landscapes potential hosts may still be present, e.g. in the form of isolated remnant trees, small groups of planted trees, in patches of secondary forests, or in plantations. For this study, we assessed the potential of timber monocultures and secondary forest patches to function as refuges for vascular epiphytes. We studied epiphyte assemblages in teak and pine plantations and secondary forest patches of unknown age along a rainfall gradient (1100 - 4200 mm) at the Pacific coast of western Panama and also in a few oil palm plantations. Invariably, rainfall had the expected positive influence on epiphyte diversity and abundance. Individual-based rarefaction curves showed that species richness was significantly lower in timber and oil palm plantations compared to secondary forest patches, which in turn hosted less species-rich epiphyte assemblages than (cultivated and wild grown) pasture trees from the same study region. Our results suggest that the value of timber and oil palm plantations as refuges for vascular epiphytes in human-modified landscapes is limited. Secondary forest patches were more promising in that regard. C1 [Einzmann, Helena Julia Regina; Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, Dept Biol & Environm Sci, Ammerlander Heerstr 114-118, D-26129 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama. RP Einzmann, HJR (reprint author), Carl von Ossietzky Univ Oldenburg, Dept Biol & Environm Sci, Ammerlander Heerstr 114-118, D-26129 Oldenburg, Germany. EM helena.einzmann@uni-oldenburg.de FU DAAD; Smithsonian Tropical Research Institute FX We would like to thank all the plantation owners for giving us permission to work on their property and Calixto Elias Rodriguez Quiel for valuable field assistance. Birgit Vollrath (Oldenburg) prepared Fig. 1. We also thank two reviewers for their constructive comments. Funding was received from DAAD (HE) and the Smithsonian Tropical Research Institute (GZ). NR 71 TC 0 Z9 0 U1 14 U2 17 PU TROPICAL CONSERVATION SCIENCE PI MENLO PARK PA PO BOX 0291, MENLO PARK, CA 94026-0291 USA SN 1940-0829 J9 TROP CONSERV SCI JI Trop. Conserv. Sci. PD JUN PY 2016 VL 9 IS 2 BP 629 EP 647 PG 19 WC Biodiversity Conservation SC Biodiversity & Conservation GA DQ0KQ UT WOS:000378888400005 ER PT J AU Schoch, RR Sues, HD AF Schoch, Rainer R. Sues, Hans-Dieter TI The diapsid origin of turtles SO ZOOLOGY LA English DT Article DE Carapace; Plastron; Reptiles; Turtle origins ID EVOLUTIONARY ORIGIN AB The origin of turtles has been a persistent unresolved problem involving unsettled questions in embryology, morphology, and paleontology. New fossil taxa from the early Late Triassic of China (Odontochelys) and the Late Middle Triassic of Germany (Pappochelys) now add to the understanding of (i) the evolutionary origin of the turtle shell, (ii) the ancestral structural pattern of the turtle skull, and (iii) the phylogenetic position of Testudines. As has long been postulated on the basis of molecular data, turtles evolved from diapsid reptiles and are more closely related to extant diapsids than to parareptiles, which had been suggested as stem group by some paleontologists. The turtle cranium with its secondarily closed temporal region represents a derived rather than a primitive condition and the plastron partially evolved through the fusion of gastralia. (C) 2016 Elsevier GmbH. All rights reserved. C1 [Schoch, Rainer R.] Staatliches Museum Nat, Rosenstein 1, D-70191 Stuttgart, Germany. [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. RP Schoch, RR (reprint author), Staatliches Museum Nat, Rosenstein 1, D-70191 Stuttgart, Germany. EM rainer.schoch@smns-bw.de NR 8 TC 1 Z9 1 U1 31 U2 39 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 0944-2006 J9 ZOOLOGY JI Zoology PD JUN PY 2016 VL 119 IS 3 BP 159 EP 161 DI 10.1016/j.zool.2016.01.004 PG 3 WC Zoology SC Zoology GA DQ1KP UT WOS:000378960200001 PM 26934902 ER PT J AU Archambault, S Archer, A Benbow, W Bird, R Biteau, J Buchovecky, M Buckley, JH Bugaev, V Byrum, K Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Eisch, JD Errando, M Falcone, A Feng, Q Finley, JP Fleischhack, H Fortin, P Fortson, L Furniss, A Gillanders, GH Griffin, S Grube, J Gyuk, G Hutten, M Hakansson, N Hanna, D Holder, J Humensky, TB Johnson, CA Kaaret, P Kar, P Kelley-Hoskins, N Kertzman, M Kieda, D Krause, M Krennrich, F Kumar, S Lang, MJ Maier, G McArthur, S McCann, A Meagher, K Moriarty, P Mukherjee, R Nguyen, T Nieto, D de Bhroithe, AO Ong, RA Otte, AN Park, N Perkins, JS Pichel, A Pohl, M Popkow, A Pueschel, E Quinn, J Ragan, K Reynolds, PT Richards, GT Roache, E Rovero, AC Santander, M Sembroski, GH Shahinyan, K Smith, AW Staszak, D Telezhinsky, I Tucci, JV Tyler, J Vincent, S Wakely, SP Weiner, OM Weinstein, A Williams, DA Zitzer, B Fumagalli, M Prochaska, JX AF Archambault, S. Archer, A. Benbow, W. Bird, R. Biteau, J. Buchovecky, M. Buckley, J. H. Bugaev, V. Byrum, K. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Eisch, J. D. Errando, M. Falcone, A. Feng, Q. Finley, J. P. Fleischhack, H. Fortin, P. Fortson, L. Furniss, A. Gillanders, G. H. Griffin, S. Grube, J. Gyuk, G. Huetten, M. Hakansson, N. Hanna, D. Holder, J. Humensky, T. B. Johnson, C. A. Kaaret, P. Kar, P. Kelley-Hoskins, N. Kertzman, M. Kieda, D. Krause, M. Krennrich, F. Kumar, S. Lang, M. J. Maier, G. McArthur, S. McCann, A. Meagher, K. Moriarty, P. Mukherjee, R. Nguyen, T. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Perkins, J. S. Pichel, A. Pohl, M. Popkow, A. Pueschel, E. Quinn, J. Ragan, K. Reynolds, P. T. Richards, G. T. Roache, E. Rovero, A. C. Santander, M. Sembroski, G. H. Shahinyan, K. Smith, A. W. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Vincent, S. Wakely, S. P. Weiner, O. M. Weinstein, A. Williams, D. A. Zitzer, B. Fumagalli, M. Prochaska, J. X. CA VERITAS Collaboration TI UPPER LIMITS FROM FIVE YEARS OF BLAZAR OBSERVATIONS WITH THE VERITAS CHERENKOV TELESCOPES SO ASTRONOMICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; galaxies: active; gamma rays: galaxies; radiation mechanisms: non-thermal ID BL-LACERTAE OBJECTS; ACTIVE GALACTIC NUCLEI; ENERGY GAMMA-RAYS; ALL-SKY SURVEY; SPECTRUM RADIO QUASARS; LARGE-AREA TELESCOPE; FERMI-LAT BLAZARS; X-RAY; OPTICAL SPECTROSCOPY; COMPLETE SAMPLE AB Between the beginning of its full-scale scientific operations in 2007 and 2012, the VERITAS Cherenkov telescope array observed more than 130 blazars; of these, 26 were detected as very-high-energy (VHE; E > 100 GeV) gamma-ray sources. In this work, we present the analysis results of a sample of 114 undetected objects. The observations constitute a total live-time of similar to 570 hr. The sample includes several unidentified Fermi-Large Area Telescope (LAT) sources (located at high Galactic latitude) as well as all the sources from the second Fermi-LAT catalog that are contained within the field of view of the VERITAS observations. We have also performed optical spectroscopy measurements in order to estimate the redshift of some of these blazars that do not have spectroscopic distance estimates. We present new optical spectra from the Kast instrument on the Shane telescope at the Lick observatory for 18 blazars included in this work, which allowed for the successful measurement or constraint on the redshift of four of them. For each of the blazars included in our sample, we provide the flux upper limit in the VERITAS energy band. We also study the properties of the significance distributions and we present the result of a stacked analysis of the data set, which shows a 4s excess. C1 [Archambault, S.; Griffin, S.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. [Archer, A.; Buckley, J. H.; Bugaev, V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bird, R.; Pueschel, E.; 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. [Buchovecky, M.; Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA. [Chen, X.; Hakansson, N.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Chen, X.; Fleischhack, H.; Huetten, M.; Kelley-Hoskins, N.; Krause, M.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Telezhinsky, I.; Vincent, S.] DESY, Platanenallee 6, 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.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; McArthur, S.; Sembroski, G. H.; Tucci, J. V.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. [Eisch, J. D.; Krennrich, F.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Errando, M.; Mukherjee, R.; Santander, M.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Furniss, A.] Calif State Univ East Bay, Dept Phys, Hayward, CA 94542 USA. [Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Humensky, T. B.; Nieto, D.; Weiner, O. M.] Columbia Univ, Dept Phys, 538 W 120th St, New York, NY 10027 USA. [Kaaret, P.] Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA. [Kar, P.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Meagher, K.; Nguyen, T.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, 837 State St NW, Atlanta, GA 30332 USA. [Meagher, K.; Nguyen, T.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, 837 State St NW, Atlanta, GA 30332 USA. [Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. [Pichel, A.; Rovero, A. C.] Inst Astron & Fis Espacio, Casilla Correo 67 Sucursal 28,C1428ZAA, RA-1428 Buenos Aires, DF, Argentina. [Reynolds, P. T.] Cork Inst Technol, Dept Phys Sci, Cork, Ireland. [Smith, A. W.] Univ Maryland, College Pk, MD 20742 USA. [Smith, A. W.] NASA GSFC, College Pk, MD 20742 USA. [Fumagalli, M.] Univ Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England. [Fumagalli, M.] Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England. [Prochaska, J. X.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Cerruti, M.] Univ Paris Diderot, Univ Paris 06, Sorbonne Univ, LPNHE,CNRS, 4 Pl Jussieu, F-75252 Paris 5, France. RP Benbow, W (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. EM wystan.benbow@cfa.harvard.edu; matteo.cerruti@lpnhe.in2p3.fr; caajohns@ucsc.edu RI Fumagalli, Michele/K-9510-2015; OI Fumagalli, Michele/0000-0001-6676-3842; Pueschel, Elisa/0000-0002-0529-1973; Krause, Maria/0000-0001-7595-0914; Santander, Juan Marcos/0000-0001-7297-8217 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science and Technology Facilities Council [ST/L00075X/1] 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, and by NSERC in Canada. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. The VERITAS Collaboration is grateful to Trevor Weekes for his seminal contributions and leadership in the field of VHE gamma-ray astrophysics, which made this study possible. M.F. acknowledges support by the Science and Technology Facilities Council (grant number ST/L00075X/1). NR 149 TC 4 Z9 4 U1 3 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUN PY 2016 VL 151 IS 6 AR 142 DI 10.3847/0004-6256/151/6/142 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO7VE UT WOS:000377990300009 ER PT J AU Burkhart, LD Ragozzine, D Brown, ME AF Burkhart, Luke D. Ragozzine, Darin Brown, Michael E. TI A DEEP SEARCH FOR ADDITIONAL SATELLITES AROUND THE DWARF PLANET HAUMEA SO ASTRONOMICAL JOURNAL LA English DT Article DE Kuiper belt objects: individual (Haumea); methods: data analysis; techniques: image processing ID EL61 COLLISIONAL FAMILY; TRANS-NEPTUNIAN OBJECTS; KUIPER-BELT; CANDIDATE MEMBERS; SOLAR-SYSTEM; PLUTO-CHARON; EVOLUTION; DISCOVERY; ORIGIN; SIZE AB Haumea is a dwarf planet with two known satellites, an unusually high spin rate, and a large collisional family, making it one of the most interesting objects in the outer solar system. A fully self-consistent formation scenario responsible for the satellite and family formation is still elusive, but some processes predict the initial formation of many small moons, similar to the small moons recently discovered around Pluto. Deep searches for regular satellites around Kuiper belt objects are difficult due to observational limitations, but Haumea is one of the few for which sufficient data exist. We analyze Hubble Space Telescope (HST) observations, focusing on a 10 consecutive -orbit sequence obtained in 2010 July, to search for new very small satellites. To maximize the search depth, we implement and validate a nonlinear shift -and -stack method. No additional satellites of Haumea are found, but by implanting and recovering artificial sources, we characterize our sensitivity. At distances between 10,000 and 350,000 km from Haumea, satellites with radii as small as 10 km are ruled out, assuming an albedo (p similar or equal to 0.7) similar to Haumea. We also rule out satellites larger than greater than or similar to 40 km in most of the Hill sphere using other HST data. This search method rules out objects similar in size to the small moons of Pluto. By developing clear criteria for determining the number of nonlinear rates to use, we find that far fewer shift rates are required (similar to 35) than might be expected. The nonlinear shift -and -stack method to discover satellites (and other moving transients) is tractable, particularly in the regime where nonlinear motion begins to manifest itself. C1 [Burkhart, Luke D.; Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Burkhart, Luke D.] Yale Univ, Dept Phys, 217 Prospect St, New Haven, CT 06511 USA. [Ragozzine, Darin] Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Ragozzine, Darin] Florida Inst Technol, Dept Phys & Space Sci, 150 West Univ Blvd, Melbourne, FL 32901 USA. [Brown, Michael E.] CALTECH, Div Geol & Planetary Sci, MC 150-21, Pasadena, CA 91125 USA. RP Ragozzine, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Ragozzine, D (reprint author), Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.; Ragozzine, D (reprint author), Florida Inst Technol, Dept Phys & Space Sci, 150 West Univ Blvd, Melbourne, FL 32901 USA. EM darin.ragozzine@gmail.com OI Ragozzine, Darin/0000-0003-1080-9770 FU Harvard Institute for Theory and Computation Fellowship; NASA/ESA Hubble Space Telescope Program [12243]; NASA from Space Telescope Science Institute (STScI) [HST-GO-12243]; NASA [NAS 5-26555] FX We thank Alex Parker, Danielle Hastings, and the anonymous referee for discussions and suggestions that improved the manuscript. D.R. acknowledges the support of a Harvard Institute for Theory and Computation Fellowship. This work is based on NASA/ESA Hubble Space Telescope Program 12243. Support was provided by NASA through grants HST-GO-12243 from the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. NR 54 TC 0 Z9 0 U1 1 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 JUN PY 2016 VL 151 IS 6 AR 162 DI 10.3847/0004-6256/151/6/162 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO7VE UT WOS:000377990300029 ER PT J AU Perez, AEG Prieto, CA Holtzman, JA Shetrone, M Meszaros, S Bizyaev, D Carrera, R Cunha, K Garcia-Hernandez, DA Johnson, JA Majewski, SR Nidever, DL Schiavon, RP Shane, N Smith, VV Sobeck, J Troup, N Zamora, O Weinberg, DH Bovy, J Eisenstein, DJ Feuillet, D Frinchaboy, PM Hayden, MR Hearty, FR Nguyen, DC O'Connell, RW Pinsonneault, MH Wilson, JC Zasowski, G AF Garcia Perez, Ana E. Allende Prieto, Carlos Holtzman, Jon A. Shetrone, Matthew Meszaros, Szabolcs Bizyaev, Dmitry Carrera, Ricardo Cunha, Katia Garcia-Hernandez, D. A. Johnson, Jennifer A. Majewski, Steven R. Nidever, David L. Schiavon, Ricardo P. Shane, Neville Smith, Verne V. Sobeck, Jennifer Troup, Nicholas Zamora, Olga Weinberg, David H. Bovy, Jo Eisenstein, Daniel J. Feuillet, Diane Frinchaboy, Peter M. Hayden, Michael R. Hearty, Fred R. Nguyen, Duy C. O'Connell, Robert W. Pinsonneault, Marc H. Wilson, John C. Zasowski, Gail TI ASPCAP: THE APOGEE STELLAR PARAMETER AND CHEMICAL ABUNDANCES PIPELINE SO ASTRONOMICAL JOURNAL LA English DT Article DE Galaxy: center; Galaxy: structure; methods: data analysis; stars: abundances; stars: atmospheres ID GALACTIC EVOLUTION EXPERIMENT; DIGITAL SKY SURVEY; SDSS-III/APOGEE SURVEY; DATA RELEASE; ATMOSPHERIC PARAMETERS; MILKY-WAY; SPECTROSCOPY; SPECTRA; STARS; SYSTEMS AB The Apache Point Observatory Galactic Evolution Experiment (APOGEE) has built the largest moderately high-resolution (R approximate to 22,500) spectroscopic map of the stars across the Milky Way, and including dust-obscured areas. The APOGEE Stellar Parameter and Chemical Abundances Pipeline (ASPCAP) is the software developed for the automated analysis of these spectra. ASPCAP determines atmospheric parameters and chemical abundances from observed spectra by comparing observed spectra to libraries of theoretical spectra, using. 2 minimization in a multidimensional parameter space. The package consists of a FORTRAN90 code that does the actual minimization and a wrapper IDL code for book-keeping and data handling. This paper explains in detail the ASPCAP components and functionality, and presents results from a number of tests designed to check its performance. ASPCAP provides stellar effective temperatures, surface gravities, and metallicities precise to 2%, 0.1 dex, and 0.05 dex, respectively, for most APOGEE stars, which are predominantly giants. It also provides abundances for up to 15 chemical elements with various levels of precision, typically under 0.1 dex. The final data release (DR12) of the Sloan Digital Sky Survey III contains an APOGEE database of more than 150,000 stars. ASPCAP development continues in the SDSS-IV APOGEE-2 survey. C1 [Garcia Perez, Ana E.; Majewski, Steven R.; Shane, Neville; Sobeck, Jennifer; O'Connell, Robert W.; Wilson, John C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Garcia Perez, Ana E.; Allende Prieto, Carlos; Carrera, Ricardo; Garcia-Hernandez, D. A.; Zamora, Olga] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Tenerife, Spain. [Garcia Perez, Ana E.; Allende Prieto, Carlos; Carrera, Ricardo; Garcia-Hernandez, D. A.; Zamora, Olga] Univ La Laguna, Dept Astrofis, E-38206 San Cristobal la Laguna, Tenerife, Spain. [Holtzman, Jon A.; Feuillet, Diane; Hayden, Michael R.] New Mexico State Univ, Las Cruces, NM 88003 USA. [Shetrone, Matthew] Univ Texas Austin, McDonald Observ, Ft Davis, TX 79734 USA. [Meszaros, Szabolcs] ELTE Gothard Astrophys Observ, Szent Imre Herceg St 112, H-9704 Szombathely, Hungary. [Bizyaev, Dmitry] Apache Point Observ, POB 59, Sunspot, NM 88349 USA. [Bizyaev, Dmitry] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow, Russia. [Cunha, Katia] Observ Nacl, Rio De Janeiro, Brazil. [Cunha, Katia] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA. [Johnson, Jennifer A.; Weinberg, David H.; Pinsonneault, Marc H.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. [Nidever, David L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Schiavon, Ricardo P.] Liverpool John Moores Univ, Astrophys Res Inst, Wirral CH41 1LD, Merseyside, England. [Smith, Verne V.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Bovy, Jo] Inst Adv Study, Einstein Dr, Princeton, NJ 08540 USA. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Frinchaboy, Peter M.] Texas Christian Univ, Dept Phys & Astron, Ft Worth, TX 76129 USA. [Hearty, Fred R.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Nguyen, Duy C.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Zasowski, Gail] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Perez, AEG (reprint author), Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.; Perez, AEG (reprint author), Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Tenerife, Spain.; Perez, AEG (reprint author), Univ La Laguna, Dept Astrofis, E-38206 San Cristobal la Laguna, Tenerife, Spain. EM agp@iac.es RI Carrera, Ricardo/K-8760-2014; Meszaros, Szabolcs/N-2287-2014; OI Carrera, Ricardo/0000-0001-6143-8151; Meszaros, Szabolcs/0000-0001-8237-5209; Shane, Neville/0000-0003-1024-7739 FU NSF [AST11-09718, AST-907873]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University; Spanish Ministry of Economy and Competitiveness (MINECO) [AYA2014-56359-P]; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences; Spanish Ministry of Economy and Competitiveness [AYA-2011-27754, AYA2014-58082-P] FX We acknowledge funding from NSF grants AST11-09718 and AST-907873. 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 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.; Support for AEGP was provided by SDSS-III/APOGEE. CAP is thankful for support from the Spanish Ministry of Economy and Competitiveness (MINECO) through grant AYA2014-56359-P. SzM has been supported by the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. DAGH, and OZ acknowledge support provided by the Spanish Ministry of Economy and Competitiveness under grant AYA-2011-27754 and AYA2014-58082-P. NR 37 TC 22 Z9 22 U1 2 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUN PY 2016 VL 151 IS 6 AR 144 DI 10.3847/0004-6256/151/6/144 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO7VE UT WOS:000377990300011 ER PT J AU Rodriguez, JE Colon, KD Stassun, KG Wright, D Cargile, PA Bayliss, D Pepper, J Collins, KA Kuhn, RB Lund, MB Siverd, RJ Zhou, G Gaudi, BS Tinney, CG Penev, K Tan, TG Stockdale, C Curtis, IA James, D Udry, S Segransan, D Bieryla, A Latham, DW Beatty, TG Eastman, JD Myers, G Bartz, J Bento, J Jensen, ELN Oberst, TE Stevens, DJ AF Rodriguez, Joseph E. Colon, Knicole D. Stassun, Keivan G. Wright, Duncan Cargile, Phillip A. Bayliss, Daniel Pepper, Joshua Collins, Karen A. Kuhn, Rudolf B. Lund, Michael B. Siverd, Robert J. Zhou, George Gaudi, B. Scott Tinney, C. G. Penev, Kaloyan Tan, T. G. Stockdale, Chris Curtis, Ivan A. James, David Udry, Stephane Segransan, Damien Bieryla, Allyson Latham, David W. Beatty, Thomas G. Eastman, Jason D. Myers, Gordon Bartz, Jonathan Bento, Joao Jensen, Eric L. N. Oberst, Thomas E. Stevens, Daniel J. TI KELT-14b AND KELT-15b: AN INDEPENDENT DISCOVERY OF WASP-122b AND A NEW HOT JUPITER SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (KELT-14, KELT-15); techniques: photometric; techniques: radial velocities; techniques: spectroscopic ID TRANSITING PLANET; SHORT-PERIOD; SKY SURVEY; F-DWARF; STARS; EVOLUTION; MIGRATION; MISSION; ORBIT; SPECTROGRAPH AB We report the discovery of KELT-14b and KELT-15b, two hot Jupiters from the KELT-South survey. KELT-14b, an independent discovery of the recently announced WASP-122b, is an inflated Jupiter mass planet that orbits a similar to 5.0(-0.7)(+0.3) (0)7 Gyr, V= 11.0, G2 star that is near the main sequence turnoff. The host star, KELT-14 (TYC 7638-981-1), has an inferred mass M* = 1.18(-0.7)(+0.3) M-circle dot and radius R* = 1.37 +/- -0.08 R-circle dot), and has T-eff = 58021 K, log g* = 4.23(-0.7)(+0.3) SI and [Fe/H] = 0.33 +/- -0.09. The planet orbits with a period of 1.7100588 +/- 0.0000025 days (T-0 = 2457091.02863 +/- 0.00047) and has a radius R-p = 1.521 Ri and mass Mp = 1.196 +/- 0.072 MI, and the eccentricity is consistent with zero. KELT-15b is another inflated Jupiter mass planet that orbits a similar to 4.6(-0.4)(+0.5) Gyr, V = 11.2, GO star (TYC 8146-86-1) that is near the "blue hook" stage of evolution prior to the Hertzsprung gap, and has an inferred mass M* = 1.181(0.050)(+0.05) M-circle dot and radius R* = 1.481 R-circle dot, and T-eff = 6003-% K, log g* = 4.17(-0.04)(+0.02) and [Fe/H] = 0.05 +/- 0.03. The planet orbits on a period of 3.329441 +/- 0.000016 days (T0 = 2457029.1663 0.0073) and has a radius Rp = 1.443 (o)Ols7 Ri and mass M-p = 0.91 531 MI and an eccentricity consistent with zero. KELT-14b has the second largest expected emission signal in the K-band for known transiting planets brighter than K < 10.5. Both KELT-14b and KELT-15b are predicted to have large enough emission signals that their secondary eclipses should be detectable using ground-based observatories. C1 [Rodriguez, Joseph E.; Stassun, Keivan G.; Collins, Karen A.; Lund, Michael B.] Vanderbilt Univ, Dept Phys & Astron, Stevenson Ctr 6301, Nashville, TN 37235 USA. [Colon, Knicole D.] NASA, Ames Res Ctr, M-S 244-30, Moffett Field, CA 94035 USA. [Colon, Knicole D.] Bay Area Environm Res Inst, 625 2nd St Ste 209, Petaluma, CA 94952 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, 1000 17th Ave North, Nashville, TN 37208 USA. [Wright, Duncan; Tinney, C. G.] UNSW Australia, Sch Phys, Sydney, NSW 2052, Australia. [Wright, Duncan; Tinney, C. G.] UNSW Australia, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Cargile, Phillip A.; Zhou, George; Bieryla, Allyson; Latham, David W.; Eastman, Jason D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Bayliss, Daniel; Udry, Stephane; Segransan, Damien] Univ Geneva, Astron Observ, Chemin Maillettes 51, CH-1290 Sauverny, Switzerland. [Pepper, Joshua; Bartz, Jonathan] Lehigh Univ, Dept Phys, 16 Mem Dr East, Bethlehem, PA 18015 USA. [Kuhn, Rudolf B.] S African Astron Observ, POB 9, ZA-7935 Observatory, South Africa. [Siverd, Robert J.] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Santa Barbara, CA 93117 USA. [Zhou, George; Bento, Joao] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Gaudi, B. Scott; Stevens, Daniel J.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. [Penev, Kaloyan] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Tan, T. G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Stockdale, Chris; Myers, Gordon] Amer Assoc Variable Star Observers, 49 Bay State Rd, Cambridge, MA 02138 USA. [Stockdale, Chris] Hazelwood Observ, Hazelwood South, Vic, Australia. [Curtis, Ivan A.] IAU Minor Planet Ctr Observ Code D79, Vale Pk, Adelaide, SA, Australia. [James, David] Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. [Beatty, Thomas G.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Beatty, Thomas G.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, Davey Lab 525, University Pk, PA 16802 USA. [Myers, Gordon] 5 Inverness Way, Hillsborough, CA 94010 USA. [Jensen, Eric L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Oberst, Thomas E.] Westminster Coll, Dept Phys, New Wilmington, PA 16172 USA. RP Rodriguez, JE (reprint author), Vanderbilt Univ, Dept Phys & Astron, Stevenson Ctr 6301, Nashville, TN 37235 USA. OI Jensen, Eric/0000-0002-4625-7333; Rodriguez, Joseph/0000-0001-8812-0565; Tan, Thiam-Guan/0000-0001-5603-6895; Pepper, Joshua/0000-0002-3827-8417; Lund, Michael/0000-0003-2527-1598; Stassun, Keivan/0000-0002-3481-9052 FU NASA [NNX13AQ62G]; NSF [AST-1056524]; NSF PAARE grant [AST-1358862]; ARC LIEF grant [LE0989347]; ARC Super Science Fellowship [FS100100046]; ARC [DP130102695]; National Aeronautics and Space Administration; National Science Foundation; Robert Martin Ayers Sciences Fund FX KELT-South is hosted by the South African Astronomical Observatory and we are grateful for their ongoing support and assistance. K.P. acknowledges support from NASA grant NNX13AQ62G. Work by B.S.G. and D.J.S. was partially supported by NSF CAREER Grant AST-1056524. Work by K.G.S. was supported by NSF PAARE grant AST-1358862. D.W. and C.G.T.'s role in this research has been supported by ARC LIEF grant LE0989347, ARC Super Science Fellowship FS100100046, and ARC Discovery grant DP130102695.; 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 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 was made possible through the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund. This paper uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope. NR 67 TC 4 Z9 4 U1 2 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUN PY 2016 VL 151 IS 6 DI 10.3847/0004-6256/151/6/138 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO7VE UT WOS:000377990300005 ER PT J AU Aalto, S Costagliola, F Muller, S Sakamoto, K Gallagher, JS Dasyra, K Wada, K Combes, F Garcia-Burillo, S Kristensen, LE Martin, S van der Werf, P Evans, AS Kotilainen, J AF Aalto, S. Costagliola, F. Muller, S. Sakamoto, K. Gallagher, J. S. Dasyra, K. Wada, K. Combes, F. Garcia-Burillo, S. Kristensen, L. E. Martin, S. van der Werf, P. Evans, A. S. Kotilainen, J. TI A precessing molecular jet signaling an obscured, growing supermassive black hole in NGC 1377? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; galaxies: active; galaxies: individual: NGC 1377; galaxies: jets; galaxies: ISM; ISM: molecules ID ACTIVE GALACTIC NUCLEI; VIBRATIONALLY EXCITED HCN; NARROW-LINE REGION; RADIO GALAXIES; STAR-FORMATION; PROTOSTELLAR SYSTEM; ACCRETION DISKS; GAS OUTFLOW; FEEDBACK; DRIVEN AB With high resolution (0 ''.25 x 0 ''.18) ALMA CO 3-2 (345 GHz) observations of the nearby (D = 21 Mpc, 1 '' = 102 pc), extremely radio-quiet galaxy NGC 1377, we have discovered a high-velocity, very collimated nuclear outflow which we interpret as a molecular jet with a projected length of +/- 150 pc. The launch region is unresolved and lies inside a radius r < 10 pc. Along the jet axis we find strong velocity reversals where the projected velocity swings from -150 km s(-1) to +150 km s(-1). A simple model of a molecular jet precessing around an axis close to the plane of the sky can reproduce the observations. The velocity of the outflowing gas is difficult to constrain due to the velocity reversals but we estimate it to be between 240 and 850 km s(-1) and the jet to precess with a period P = 0.3-1.1 Myr. The CO emission is clumpy along the jet and the total molecular mass in the high-velocity (+/-(60 to 150 km s(-1))) gas lies between 2 x 10(6) M-circle dot (light jet) and 2 x 10(7) M-circle dot (massive jet). There is also CO emission extending along the minor axis of NGC 1377. It holds >40% of the flux in NGC 1377 and may be a slower, wide-angle molecular outflow which is partially entrained by the molecular jet. We discuss the driving mechanism of the molecular jet and suggest that it is either powered by a (faint) radio jet or by an accretion disk-wind similar to those found towards protostars. It seems unlikely that a massive jet could have been driven out by the current level of nuclear activity which should then have undergone rapid quenching. The light jet would only have expelled 10% of the inner gas and may facilitate nuclear activity instead of suppressing it. The nucleus of NGC 1377 harbours intense embedded activity and we detect emission from vibrationally excited HCN J = 4-3 nu(2) = 1 integral which is consistent with hot gas and dust. We find large columns of H-2 in the centre of NGC 1377 which may be a sign of a high rate of recent gas infall. The dynamical age of the molecular jet is short (<1 Myr), which could imply that it is young and consistent with the notion that NGC 1377 is caught in a transient phase of its evolution. However, further studies are required to determine the age of the molecular jet, its mass and the role it is playing in the growth of the nucleus of NGC 1377. C1 [Aalto, S.; Costagliola, F.; Muller, S.; Gallagher, J. S.] Chalmers, Dept Earth & Space Sci, Onsala Observ, S-43992 Onsala, Sweden. [Sakamoto, K.] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. [Gallagher, J. S.] Univ Wisconsin, Dept Astron, 5534 Sterling,475 North Charter St, Madison, WI 53706 USA. [Dasyra, K.] Univ Athens, Fac Phys, Dept Astrophys Astron & Mech, Panepistimiopolis 15784, Greece. [Wada, K.] Kagoshima Univ, Kagoshima 8900065, Japan. [Combes, F.] Observ Paris, LERMA CNRS UMR 8112, 61 Av Observ, F-75014 Paris, France. [Garcia-Burillo, S.] Observ Madrid, Observ Astron Nacl, Alfonso 7 3, Madrid 28014, Spain. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Martin, S.] European So Observ, Alonso de Cordova 3107, Santiago, Chile. [Martin, S.] Joint ALMA Observ, Alonso de Cordova 3107, Santiago, Chile. [Martin, S.] Inst Radio Astron Millimetr, 300 Rue Piscine,Domaine Univ Grenoble, F-38406 St Martin Dheres, France. [van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Evans, A. S.] Univ Virginia, Charlottesville, VA 22904 USA. [Evans, A. S.] NRAO, 520 Edgemont Rd, Charlottesville, VA 22903 USA. [Kotilainen, J.] Univ Turku, Finnish Ctr Astron ESO FINCA, Vaisalantie 20, Kaarina 21500, Finland. RP Aalto, S (reprint author), Chalmers, Dept Earth & Space Sci, Onsala Observ, S-43992 Onsala, Sweden. EM saalto@chalmers.se OI Martin Ruiz, Sergio/0000-0001-9281-2919; Garcia-Burillo, Santiago/0000-0003-0444-6897; Combes, Francoise/0000-0003-2658-7893; /0000-0002-9931-1313 FU Swedish National Science Council [621-2011-4143, 637-2013-7261]; MOST [102-2119-M-001-011-MY3]; [AYA2012-32295] FX This paper makes use of the following ALMA data: ADS/JAO.ALMA#2012.1.00900.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. We thank the Nordic ALMA ARC node for excellent support. S.A. acknowledges support from the Swedish National Science Council grant 621-2011-4143. F.C. acknowledges support from Swedish National Science Council grant 637-2013-7261 KS was supported by grant MOST 102-2119-M-001-011-MY3 SGB thanks support from Spanish grant AYA2012-32295. JSG thanks the Chalmers University for the appointment of Jubileumsprofessor for 2015. S.A. thanks S. Konig, angstrom. Hjalmarson, R. Haas and S. Bourke for discussions of the manuscript. NR 84 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2016 VL 590 AR A73 DI 10.1051/0004-6361/201527664 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO9LB UT WOS:000378106800045 ER PT J AU Benz, AO Bruderer, S van Dishoeck, EF Melchior, M Wampfler, SF van der Tak, F Goicoechea, JR Indriolo, N Kristensen, LE Lis, DC Mottram, JC Bergin, EA Caselli, P Herpin, F Hogerheijde, MR Johnstone, D Liseau, R Nisini, B Tafalla, M Visser, R Wyrowski, F AF Benz, A. O. Bruderer, S. van Dishoeck, E. F. Melchior, M. Wampfler, S. F. van der Tak, F. Goicoechea, J. R. Indriolo, N. Kristensen, L. E. Lis, D. C. Mottram, J. C. Bergin, E. A. Caselli, P. Herpin, F. Hogerheijde, M. R. Johnstone, D. Liseau, R. Nisini, B. Tafalla, M. Visser, R. Wyrowski, F. TI Water in star-forming regions with Herschel (WISH) VI. Constraints on UV and X-ray Irradiation from a survey of hydrides in low- to high-mass young stellar objects SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; stars: low-mass; stars: massive; ISM: molecules; ultraviolet: ISM; astrochemistry ID NGC 6334 I; J CO OBSERVATIONS; INTERSTELLAR-MEDIUM; PROTOSTELLAR ENVELOPES; CONTINUUM OBSERVATIONS; PHYSICAL STRUCTURE; ABSORPTION-LINES; SULFUR CHEMISTRY; IONIZATION RATE; DIFFUSE CLOUDS AB Context. Hydrides are simple compounds containing one or a few hydrogen atoms bonded to a heavier atom. They are fundamental precursor molecules in cosmic chemistry and many hydride ions have become observable in high quality for the first time thanks to the Herschel Space Observatory. Ionized hydrides such as CH+ and OH+ (and also HCO+), which affect the chemistry of molecules such as water, provide complementary information on irradiation by far-UV (FUV) or X-rays and gas temperature. Aims. We explore hydrides of the most abundant heavier elements in an observational survey covering young stellar objects (YSOs) with different mass and evolutionary state. The focus is on hydrides associated with the dense protostellar envelope and outflows, contrary to previous work that focused on hydrides in diffuse foreground clouds. Methods. Twelve YSOs were observed with HIFI on Herschel in six spectral settings providing fully velocity-resolved line profiles as part of the Water in star-forming regions with Herschel (WISH) program. The YSOs include objects of low (Class 0 and I), intermediate, and high mass, with luminosities ranging from 4 L-circle dot to 2 x 10(5) L-circle dot. Results. The targeted lines of CH+, OH+, H2O+, C+, and CH are detected mostly in blue-shifted absorption. H3O+ and SH+ are detected in emission and only toward some high-mass objects. The observed line parameters and correlations suggest two different origins related to gas entrained by the outflows and to the circumstellar envelope. The derived column densities correlate with bolometric luminosity and envelope mass for all molecules, best for CH, CH+, and HCO+. The column density ratios of CH+/OH+ are estimated from chemical slab models, assuming that the H-2 density is given by the specific density model of each object at the beam radius. For the low-mass YSOs the observed ratio can be reproduced for an FUV flux of 2-400 times the interstellar radiation field (ISRF) at the location of the molecules. In two high-mass objects, the UV flux is 20-200 times the ISRF derived from absorption lines, and 300-600 ISRF using emission lines. Upper limits for the X-ray luminosity can be derived from H3O+ observations for some low-mass objects. Conclusions. If the FUV flux required for low-mass objects originates at the central protostar, a substantial FUV luminosity, up to 1.5 L-circle dot, is required. There is no molecular evidence for X-ray induced chemistry in the low-mass objects on the observed scales of a few 1000 AU. For high-mass regions, the FUV flux required to produce the observed molecular ratios is smaller than the unattenuated flux expected from the central object(s) at the Herschel beam radius. This is consistent with an FUV flux reduced by circumstellar extinction or by bloating of the protostar. C1 [Benz, A. O.; Bruderer, S.; Melchior, M.; Wampfler, S. F.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Bruderer, S.; van Dishoeck, E. F.; Caselli, P.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [van Dishoeck, E. F.; Hogerheijde, M. R.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Melchior, M.] Univ Appl Sci FHNW, Inst Technol 4D, CH-5210 Windisch, Switzerland. [Wampfler, S. F.] Nat Hist Museum Denmark, Ctr Star & Planet Format, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. [Wampfler, S. F.] Niels Bohr Inst, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. [van der Tak, F.] SRON Netherlands Inst Space Res, POB 800, NL-9700 AV Groningen, Netherlands. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. [Goicoechea, J. R.] CSIC, Grp Astrofis Mol, ICMM, Calle Sor Juana Ines de la Cruz 3, Madrid, Spain. [Indriolo, N.; Bergin, E. A.] Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Lis, D. C.] Univ Paris 06, Sorbonne Univ, LERMA, Observ Paris,PSL Res Univ,CNRS, F-75014 Paris, France. [Lis, D. C.] CALTECH, Cahill Ctr Astron & Astrophys, MS 301-17, Pasadena, CA 91125 USA. [Herpin, F.] Univ Bordeaux, LAB, UMR 5804, F-33270 Florac, France. [Herpin, F.] CNRS, LAB, UMR 5804, F-33270 Florac, France. [Johnstone, D.] Natl Res Council Canada, Herzberg Astron & Astrophys, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Liseau, R.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Tafalla, M.] Observ Astron Nacl IGN, Calle Alfonso 12,3, Madrid 28014, Spain. [Visser, R.] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Wyrowski, F.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Mottram, J. C.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. RP Benz, AO (reprint author), ETH, Inst Astron, CH-8093 Zurich, Switzerland. EM Benz@astro.phys.ethz.ch RI Wampfler, Susanne/D-2270-2015 OI Wampfler, Susanne/0000-0002-3151-7657 FU Swiss National Science Foundation [200020-113556]; Netherlands Research School for Astronomy (NOVA); Royal Netherlands Academy of Arts and Sciences (KNAW); European Union A-ERC [291141 CHEMPLAN]; NASA FX We thank the WISH team for inspiring discussions and support. We acknowledge the referee for helpful criticism and Goran Sandell for the confirmation of the NGC6334 I(N) object parameters. This program is made possible thanks to the Swiss Herschel guaranteed time program. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research Groningen, The Netherlands and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INT); Sweden: Chalmers University of Technology, Onsala Space Observatory, Stockholm University; Switzerland: ETH Zurich, FHNW Windisch; USA: Caltech, JPL, NHSC. The work on star formation at ETH Zurich was partially funded by the Swiss National Science Foundation (grant No. 200020-113556). Astrochemistry in Leiden is supported by the Netherlands Research School for Astronomy (NOVA), by a Royal Netherlands Academy of Arts and Sciences (KNAW) professor prize, and by the European Union A-ERC grant 291141 CHEMPLAN. Support for this work was also provided by NASA (Herschel OT funding) through an award issued by JPL/Caltech. NR 103 TC 1 Z9 1 U1 2 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2016 VL 590 AR A105 DI 10.1051/0004-6361/201525835 PG 38 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO9LB UT WOS:000378106800009 ER PT J AU Castro, M Duarte, T Pace, G do Nascimento, JD AF Castro, M. Duarte, T. Pace, G. do Nascimento, J. -D., Jr. TI Mass effect on the lithium abundance evolution of open clusters: Hyades, NGC 752, and M 67 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: fundamental parameters; stars: abundances; stars: evolution; stars: interiors; stars: solar-type ID SOLAR-TYPE STARS; STELLAR RADIATIVE ZONES; MAIN-SEQUENCE STARS; INCLUDING ROTATION; ELEMENT DIFFUSION; INTERMEDIATE-AGE; GRAVITY-WAVES; F-STARS; NGC-752; DEPLETION AB Lithium abundances in open clusters provide an effective way of probing mixing processes in the interior of solar-type stars and convection is not the only mixing mechanism at work. To understand which mixing mechanisms are occurring in low-mass stars, we test non-standard models, which were calibrated using the Sun, with observations of three open clusters of different ages, the Hyades, NGC 752, and M 67. We collected all available data, and for the open cluster NGC 752, we redetermine the equivalent widths and the lithium abundances. Two sets of evolutionary models were computed, one grid of only standard models with microscopic diffusion and one grid with rotation-induced mixing, at metallicity [Fe/H] = 0.13, 0.0, and 0.01 dex, respectively, using the Toulouse-Geneva evolution code. We compare observations with models in a color-magnitude diagram for each cluster to infer a cluster age and a stellar mass for each cluster member. Then, for each cluster we analyze the lithium abundance of each star as a function of mass. The data for the open clusters Hyades, NGC 752, and M 67, are compatible with lithium abundance being a function of both age and mass for stars in these clusters. Our models with meridional circulation qualitatively reproduce the general trend of lithium abundance evolution as a function of stellar mass in all three clusters. This study points out the importance of mass dependence in the evolution of lithium abundance as a function of age. Comparison between models with and without rotation-induced mixing shows that the inclusion of meridional circulation is essential to account for lithium depletion in low-mass stars. However, our results suggest that other mechanisms should be included to explain the Li-dip and the lithium dispersion in low-mass stars. C1 [Castro, M.; Duarte, T.; do Nascimento, J. -D., Jr.] Univ Fed Rio Grande do Norte, Dept Fis Teor & Expt, BR-59072970 Natal, RN, Brazil. [Pace, G.] Univ Porto, Inst Astrofis & Ciencia Espaco, Rua Estrelas, P-4150762 Oporto, Portugal. [do Nascimento, J. -D., Jr.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Castro, M (reprint author), Univ Fed Rio Grande do Norte, Dept Fis Teor & Expt, BR-59072970 Natal, RN, Brazil. EM mcastro@dfte.ufrn.br FU Fundacao para a Ciencia e a Tecnologia (FCT), Portugal [SFRH/BPD/39254/2007, PTDC/CTE-AST/098528/2008]; CNPq Brazilian Agency; FAPERN Brazilian Agency; CNPq (Bolsa de Produtividade) FX This research made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of WEBDA, an open cluster database developed and maintained by Jean-Claude Mermilliod. G.P. is supported by grant SFRH/BPD/39254/2007 and by the project PTDC/CTE-AST/098528/2008, funded by Fundacao para a Ciencia e a Tecnologia (FCT), Portugal. Research activities of the Stellar Board at the Federal University of Rio Grande do Norte are supported by continuous grants from CNPq and FAPERN Brazilian Agencies. J.D.N. and M.C. would like to acknowledge support from CNPq (Bolsa de Produtividade). NR 91 TC 0 Z9 0 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 JUN PY 2016 VL 590 AR A94 DI 10.1051/0004-6361/201527583 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO9LB UT WOS:000378106800042 ER PT J AU Chidiac, C Rani, B Krichbaum, TP Angelakis, E Fuhrmann, L Nestoras, I Zensus, JA Sievers, A Ungerechts, H Itoh, R Fukazawa, Y Uemura, M Sasada, M Gurwell, M Fedorova, E AF Chidiac, C. Rani, B. Krichbaum, T. P. Angelakis, E. Fuhrmann, L. Nestoras, I. Zensus, J. A. Sievers, A. Ungerechts, H. Itoh, R. Fukazawa, Y. Uemura, M. Sasada, M. Gurwell, M. Fedorova, E. TI Exploring the nature of the broadband variability in the flat spectrum radio quasar 3C 273 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; quasars: individual: 3C 273; galaxies: jets; gamma rays: galaxies; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; RAY LIGHT CURVES; FERMI BRIGHT BLAZARS; SIMULTANEOUS X-RAY; FLARING BEHAVIOR; BLACK-HOLES; RED NOISE; 3C-273; EMISSION; JET AB The detailed investigation of the broadband flux variability in the blazar 3C 273 allowed us to probe the location and size of emission regions and their physical conditions. We conducted correlation studies of the flaring activity in 3C 273, which was observed for the period between 2008 and 2012. The observed broadband variations were investigated using the structure function and the discrete correlation function methods. Starting from the commonly used power spectral density (PSD) analysis at X-ray frequencies, we extended our investigation to characterise the nature of variability at radio, optical, and gamma-ray frequencies. The PSD analysis showed that the optical and infrared light-curve slopes are consistent with the slope of white-noise processes, while the PSD slopes at radio, X-ray, and gamma-ray energies are consistent with red-noise processes. We found that the estimated fractional variability amplitudes strongly depend on the observed frequency. The flux variations at gamma-ray and mm-radio bands are found to be significantly correlated. Using the estimated time lag of (110 +/- 27) days between gamma-ray and radio light-curves, where gamma-ray variations lead the radio bands, we constrained the location of the gamma-ray emission region at a de-projected distance of 1.2 +/- 0.9 pc from the jet apex. Flux variations at X-ray bands were found to have a significant correlation with variations at both radio and gamma-ray energies. The correlation between X-ray and gamma-ray light curves indicates two possible time lags, which suggests that two components are responsible for the X-ray emission. A negative time lag of (50 +/- 20) days, where the X-rays are leading the emission, suggests that X-rays are emitted closer to the jet apex from a compact region (0.02-0.05 pc in size), most likely from the corona at a distance of (0.5 +/- 0.4) pc from the jet apex. A positive time lag of (110 +/- 20) days (gamma-rays are leading the emission) suggests a jet-base origin of the other X-ray component at similar to 4 to 5 pc from the jet apex. The flux variations at radio frequencies were found to be well correlated with each other such that the variations at higher frequencies are leading the lower frequencies, which is expected from the standard shock-in-jet model. C1 [Chidiac, C.; Rani, B.; Krichbaum, T. P.; Angelakis, E.; Fuhrmann, L.; Nestoras, I.; Zensus, J. A.] Max Planck Inst Radioastron MPIfR, Hugel 69, D-53121 Bonn, Germany. [Sievers, A.; Ungerechts, H.] Inst Radioastron Milimetr IRAM, Ave Div Pastora 7,Local 20, Granada 18012, Spain. [Itoh, R.; Fukazawa, Y.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Uemura, M.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Sasada, M.] Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA. [Gurwell, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Fedorova, E.] Natl Taras Shevchenko Univ Kiev, Astron Observ, UA-01601 Kiev, Ukraine. [Chidiac, C.] Univ Bonn, Argelander Inst Astron, Bonn, Germany. RP Rani, B (reprint author), Max Planck Inst Radioastron MPIfR, Hugel 69, D-53121 Bonn, Germany. EM brani@mpifr-bonn.mpg.de RI Fedorova, Elena/F-4925-2017; OI Fedorova, Elena/0000-0002-8882-7496; Sasada, Mahito/0000-0001-5946-9960; Angelakis, Emmanouil/0000-0001-7327-5441 FU International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Bonn; International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Cologne; Fermi Guest Investigator grants [NNX08AW56G, NNX09AU10G, NNX12AO93G, NNX15AU81G]; Smithsonian Institution; Academia Sinica; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX C.C. was supported for this research through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. The authors would like to thank Dimitris Emmanoulopoulos, Sam Connolly, and Walter Max-Moerbeck for useful discussions on statistical analysis and for their suggestions and comments on the paper draft. This research is partly based on observations with the 100 m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg. The optical/IR observations are provided by the Yale Fermi/SMARTS project. Data from the Steward Observatory spectropolarimetric monitoring project were used. This program is supported by Fermi Guest Investigator grants NNX08AW56G, NNX09AU10G, NNX12AO93G, and NNX15AU81G. 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 research is partly based on observations carried out with the IRAM 30 m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). NR 60 TC 1 Z9 1 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2016 VL 590 AR A61 DI 10.1051/0004-6361/201628347 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO9LB UT WOS:000378106800128 ER PT J AU Coutens, A Jorgensen, JK van der Wiel, MHD Muller, HSP Lykke, JM Bjerkeli, P Bourke, TL Calcutt, H Drozdovskaya, MN Favre, C Fayolle, EC Garrod, RT Jacobsen, SK Ligterink, NFW Oberg, KI Persson, MV van Dishoeck, EF Wampfler, SF AF Coutens, A. Jorgensen, J. K. van der Wiel, M. H. D. Mueller, H. S. P. Lykke, J. M. Bjerkeli, P. Bourke, T. L. Calcutt, H. Drozdovskaya, M. N. Favre, C. Fayolle, E. C. Garrod, R. T. Jacobsen, S. K. Ligterink, N. F. W. Oberg, K. I. Persson, M. V. van Dishoeck, E. F. Wampfler, S. F. TI The ALMA-PILS survey: First detections of deuterated formamide and deuterated isocyanic acid in the interstellar medium SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; stars: protostars; ISM: molecules; ISM: individual objects: IRAS 16293-2422; astrobiology ID GRAIN-SURFACE-CHEMISTRY; SOLAR-TYPE PROTOSTAR; GAS-PHASE REACTIONS; LOW-MASS PROTOSTAR; IRAS 16293-2422; 1 THZ; MOLECULAR-SPECTROSCOPY; ROTATIONAL SPECTRUM; MICROWAVE-SPECTRUM; COLOGNE DATABASE AB Formamide (NH2CHO) has previously been detected in several star-forming regions and is thought to be a precursor for different prebiotic molecules. Its formation mechanism is still debated, however. Observations of formamide, related species, and their isopotologues may provide useful clues to the chemical pathways leading to their formation. The Protostellar Interferometric Line Survey (PILS) represents an unbiased, high angular resolution and sensitivity spectral survey of the low-mass protostellar binary IRAS 16293-2422 with the Atacama Large Millimeter/submillimeter Array (ALMA). For the first time, we detect the three singly deuterated forms of NH2CHO (NH2CDO, cis-and trans-NHDCHO), as well as DNCO towards the component B of this binary source. The images reveal that the different isotopologues are all present in the same region. Based on observations of the C-13 isotopologues of formamide and a standard C-12/C-13 ratio, the deuterium fractionation is found to be similar for the three different forms with a value of about 2%. The DNCO/HNCO ratio is also comparable to the D/H ratio of formamide (similar to 1%). These results are in agreement with the hypothesis that NH2CHO and HNCO are chemically related through grain-surface formation. C1 [Coutens, A.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Jorgensen, J. K.; van der Wiel, M. H. D.; Lykke, J. M.; Bjerkeli, P.; Calcutt, H.; Jacobsen, S. K.; Wampfler, S. F.] Univ Copenhagen, Niels Bohr Inst, Ctr Star & Planet Format, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. [Jorgensen, J. K.; van der Wiel, M. H. D.; Lykke, J. M.; Bjerkeli, P.; Calcutt, H.; Jacobsen, S. K.; Wampfler, S. F.] Univ Copenhagen, Nat Hist Museum Denmark, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. [Mueller, H. S. P.] Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. [Bjerkeli, P.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. [Bourke, T. L.] Jodrell Bank Observ, SKA Org, Macclesfield SK11 9DL, Cheshire, England. [Drozdovskaya, M. N.; Ligterink, N. F. W.; Persson, M. V.; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Favre, C.] UJF Grenoble 1 CNRS, UMR 5274, Inst Planetol & Astrophys Grenoble, F-38041 Grenoble, France. [Fayolle, E. C.; Oberg, K. I.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Garrod, R. T.] Univ Virginia, Dept Chem & Astron, Charlottesville, VA 22904 USA. [van Dishoeck, E. F.] Max Planck Inst Extraterrestr Phys MPE, Giessenbachstr 1, D-85748 Garching, Germany. RP Coutens, A (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM a.coutens@ucl.ac.uk RI Wampfler, Susanne/D-2270-2015; Jacobsen, Steffen/Q-4606-2016; OI Wampfler, Susanne/0000-0002-3151-7657; Jacobsen, Steffen/0000-0002-7449-5638; Persson, Magnus Vilhelm/0000-0002-1100-5734; Coutens, Audrey/0000-0003-1805-3920; Calcutt, Hannah/0000-0003-3393-294X FU STFC grant; COST action [CM1401]; Lundbeck Foundation Group Leader Fellowship; European Research Council (ERC) under the European Union's Horizon research and innovation programme through ERC Consolidator Grant S4F [646908]; Danish National Research Foundation; A-ERC grant [291141]; ADS/JAO.ALMA [2013.1.00278.S] FX The authors thank Gleb Fedoseev and Harold Linnartz for fruitful discussions. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00278.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 work of A.C. was funded by an STFC grant. A.C. thanks the COST action CM1401 Our Astrochemical History for additional financial support. The group of J.K.J. acknowledges support from a Lundbeck Foundation Group Leader Fellowship, as well as the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No 646908) through ERC Consolidator Grant S4F. Research at the Centre for Star and Planet Formation is funded by the Danish National Research Foundation. The group of E.v.D. acknowledges A-ERC grant 291141 CHEMPLAN. NR 53 TC 3 Z9 3 U1 11 U2 16 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2016 VL 590 AR L6 DI 10.1051/0004-6361/201628612 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO9LB UT WOS:000378106800142 ER PT J AU Dahle, H Aghanim, N Guennou, L Hudelot, P Kneissl, R Pointecouteau, E Beelen, A Bayliss, M Douspis, M Nesvadba, N Hempel, A Gronke, M Burenin, R Dole, H Harrison, D Mazzotta, P Sunyaev, R AF Dahle, H. Aghanim, N. Guennou, L. Hudelot, P. Kneissl, R. Pointecouteau, E. Beelen, A. Bayliss, M. Douspis, M. Nesvadba, N. Hempel, A. Gronke, M. Burenin, R. Dole, H. Harrison, D. Mazzotta, P. Sunyaev, R. TI Discovery of an exceptionally bright giant arc at z=2.369, gravitationally lensed by the Planck cluster PSZ1 G311.65-18.48 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: individual: PSZ1 G311.65-18.48; gravitational lensing: strong; cosmology: observations ID LYMAN BREAK GALAXIES; REST-FRAME ULTRAVIOLET; LY-ALPHA; TO 3; SPECTRA; RING AB As part of an all-sky follow-up of the Planck catalogue of Sunyaev-Zeldovich (SZ) cluster candidates detected in the first 14 months of data, we are observing cluster candidates in the southern sky in the optical imaging and spectroscopy through an ESO Large Programme. Inspection of ESO New Technology Telescope (NTT) R-and z-band imaging data from our programme has revealed an unusually large and bright arc in the field of PSZ1 G311.65-18.48. We establish the basic photometric and morphological properties of the arc and provide conclusive evidence for the gravitational lensing nature of this object. Guided by the NTT images, we have obtained a long-slit spectrum with IMACS on the Magellan-I Baade Telescope, covering a part of the arc and the brightest cluster galaxy of PSZ1 G311.65-18.48. Our imaging data confirm the presence of a galaxy cluster coinciding (within 0'.6) with the position of the Planck SZ source. The arc is separated by similar to 30 '' from the brightest cluster galaxy, which closely coincides with the center of curvature of the arc. A photometric analysis yields integrated (Vega) magnitudes of (R,z, J, K-s) = (17.82, 17.38, 16.75, 15.43) for the arc, more than one magnitude brighter than any previously known lensed arc at z similar to 2-3. The arc is a vigorously star-forming galaxy at z = 2.369, while the Planck SZ cluster lens is at z = 0.443. Even when allowing for lensing magnifications as high as mu = 100 still leads to the conclusion that the source galaxy is among the intrinsically most luminous normal (i.e., non-AGN) galaxies known at z similar to 2-3. C1 [Dahle, H.; Gronke, M.] Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway. [Aghanim, N.; Guennou, L.; Beelen, A.; Douspis, M.; Nesvadba, N.; Dole, H.] Univ Paris Saclay, Univ Paris 11, CNRS, Inst Astrophys Spatiale,UMR 8617, Bat 121, F-91405 Orsay, France. [Hudelot, P.] Univ Paris 06, Sorbonne Univ, UMR Astrophys Paris, F-75014 Paris, France. [Kneissl, R.] European So Observ, ESO Vitacura, Alonso Cordova 3107, Santiago 19001, Chile. [Kneissl, R.] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Alonso Cordova 3107, Santiago 7630355, Chile. [Pointecouteau, E.] Univ Toulouse, UPS Observ Midi Pyrenees, IRAP, F-31000 Toulouse, France. [Pointecouteau, E.] CNRS, IRAP, 9 Ave Colonel Roche, F-31028 Toulouse 4, France. [Bayliss, M.] Colby Coll, 5800 Mayflower Hill, Waterville, ME 04901 USA. [Bayliss, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA USA. [Bayliss, M.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. [Hempel, A.] Univ Andres Bello, Dept Ciencias Fis, Campus Casona Las ,Fernandez Cconcha 700, Santiago, Chile. [Burenin, R.; Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Profsoyuznaya Str 84-32, Moscow 117997, Russia. Moscow Inst Phys & Technol, Inst Per 9, Dolgoprudry 141700, Russia. Kavli Inst Cosmol Cambridge, Madingley Rd, Cambridge CB3 0HA, England. [Harrison, D.] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Mazzotta, P.] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy. [Sunyaev, R.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. RP Dahle, H (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway. EM hdahle@astro.uio.no RI Mazzotta, Pasquale/B-1225-2016 OI Mazzotta, Pasquale/0000-0002-5411-1748 FU ESA; CNES; CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy); NASA; DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA; RES (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); PRACE (EU); Research Council of Norway; CNRS-INSU "Programme National de Cosmologie et Galaxies"; French Agence Nationale de la Recherche [ANR-11-BS56-015]; Russian Science Foundation [RNF-14-22-00271] FX Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 192.A-0762. This paper includes data gathered with the 6.5 m Magellan telescopes located at Las Campanas Observatory, Chile. The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). H.D. acknowledges support from the Research Council of Norway. The authors acknowledge support from the CNRS-INSU "Programme National de Cosmologie et Galaxies" and the use of the TERAPIX facility for the data reduction. E.P. acknowledges the support of the French Agence Nationale de la Recherche under grant ANR-11-BS56-015. R.B. and R.S. acknowledge support from Russian Science Foundation grant RNF-14-22-00271. This publication makes use of data products from the Two Micron All Sky Survey. This research made use of the SZ-cluster (http://szcluster-db.ias.u-psud.fr/) database operated by IDOC at IAS Orsay, France; NASA/IPAC Extragalactic Database (NED) and the SIMBAD database, operated at CDS, Strasbourg, France. NR 31 TC 0 Z9 0 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2016 VL 590 AR L4 DI 10.1051/0004-6361/201628297 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO9LB UT WOS:000378106800119 ER PT J AU Dauser, T Garcia, J Walton, DJ Eikmann, W Kallman, T McClintock, J Wilms, J AF Dauser, T. Garcia, J. Walton, D. J. Eikmann, W. Kallman, T. McClintock, J. Wilms, J. TI Normalizing a relativistic model of X-ray reflection Definition of the reflection fraction and its implementation in relxill SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion; accretion disks; line: profiles; galaxies: active; X-rays: galaxies ID BLACK-HOLE SPIN; K-ALPHA LINE; ACTIVE GALACTIC NUCLEI; INNER ACCRETION DISK; CYGNUS X-1; GX 339-4; SUZAKU OBSERVATIONS; SEYFERT-GALAXIES; COLD MATTER; HARD STATE AB Aims. The only relativistic reflection model that implements a parameter relating the intensity incident on an accretion disk to the observed intensity is relxill. The parameter used in earlier versions of this model, referred to as the reflection strength, is unsatisfactory; it has been superseded by a parameter that provides insight into the accretion geometry, namely the reflection fraction. The reflection fraction is defined as the ratio of the coronal intensity illuminating the disk to the coronal intensity that reaches the observer. Methods. The relxill model combines a general relativistic ray-tracing code and a photoionization code to compute the component of radiation reflected from an accretion that is illuminated by an external source. The reflection fraction is a particularly important parameter for relativistic models with well-defined geometry, such as the lamp post model, which is a focus of this paper. Results. Relativistic spectra are compared for three inclinations and for four values of the key parameter of the lamp post model, namely the height above the black hole of the illuminating, on-axis point source. In all cases, the strongest reflection is produced for low source heights and high spin. A low-spin black hole is shown to be incapable of producing enhanced relativistic reflection. Results for the relxill model are compared to those obtained with other models and a Monte Carlo simulation. Conclusions. Fitting data by using the relxill model and the recently implemented reflection fraction, the geometry of a system can be constrained. The reflection fraction is independent of system parameters such as inclination and black hole spin. The reflection-fraction parameter was implemented with the name refl_frac in all flavours of the relxill model, and the non-relativistic reflection model xillver, in v0.4a (18 January 2016). C1 [Dauser, T.; Eikmann, W.; Wilms, J.] Univ Erlangen Nurnberg, Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany. [Dauser, T.; Eikmann, W.; Wilms, J.] Univ Erlangen Nurnberg, ECAP, Sternwartstr 7, D-96049 Bamberg, Germany. [Garcia, J.; McClintock, J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Walton, D. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Kallman, T.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. RP Dauser, T (reprint author), Univ Erlangen Nurnberg, Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany.; Dauser, T (reprint author), Univ Erlangen Nurnberg, ECAP, Sternwartstr 7, D-96049 Bamberg, Germany. EM thomas.dauser@sternwarte.uni-erlangen.de RI Wilms, Joern/C-8116-2013 OI Wilms, Joern/0000-0003-2065-5410 NR 38 TC 5 Z9 5 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2016 VL 590 AR A76 DI 10.1051/0004-6361/201628135 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO9LB UT WOS:000378106800100 ER PT J AU Karamanavis, V Fuhrmann, L Angelakis, E Nestoras, I Myserlis, I Krichbaum, TP Zensus, JA Ungerechts, H Sievers, A Gurwell, MA AF Karamanavis, V. Fuhrmann, L. Angelakis, E. Nestoras, I. Myserlis, I. Krichbaum, T. P. Zensus, J. A. Ungerechts, H. Sievers, A. Gurwell, M. A. TI What can the 2008/10 broadband flare of PKS 1502+106 tell us? Nuclear opacity, magnetic fields, and the location of gamma rays SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: jets; radiation mechanisms: non-thermal; radio continuum: galaxies; gamma rays: galaxies ID ACTIVE GALACTIC NUCLEI; EXTRAGALACTIC RADIO-SOURCES; RELATIVISTIC JETS; BLAZARS; EMISSION; VARIABILITY; TELESCOPE; SAMPLE; SITE; VLBI AB Context. The origin of blazar variability, as seen from radio up to gamma rays, is still a heavily debated matter, and broadband flares off er a unique testbed for developing a better understanding of these extreme objects. One of these energetic outbursts was detected by Fermi/LAT in 2008 from the blazar PKS 1502 + 106. The outburst was observed from gamma rays down to radio frequencies. Aims. Through the delay between flare maxima at different radio frequencies, we study the frequency-dependent position of the unitopacity surface and infer its absolute position with respect to the jet base. This nuclear opacity profile enables the jet's magnetic field tomography. We also localize the gamma-ray emission region and explore the flare production mechanism. Methods. The PKS 1502 + 106 radio flare is studied through single-dish flux density measurements at 12 frequencies in the range 2.64 to 226.5 GHz. To quantify the flare, we employ both a Gaussian process regression and a discrete cross-correlation function analysis. Results. We find that the light curve parameters (flare amplitude and cross-band delays) show a power-law dependence on frequency. Delays decrease with frequency, and the flare amplitudes increase up to about 43 GHz, and then decay. This behavior is consistent with the propagation of a shock downstream in the jet. The self-absorbed radio cores are located between approximately ten and four pc from the jet base, and their magnetic field strengths range between 14 and 176 mG, at the frequencies 2.64 to 86.24 GHz. Finally, the gamma-ray active region is located at (1.9 +/- 1.1) pc away from the jet base. C1 [Karamanavis, V.; Fuhrmann, L.; Angelakis, E.; Nestoras, I.; Myserlis, I.; Krichbaum, T. P.; Zensus, J. A.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Ungerechts, H.; Sievers, A.] Inst Radio Astron Millimetr, Ave Divina Pastora 7,Local 20, Granada 18012, Spain. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Karamanavis, V (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM vkaramanavis@mpifr.de FU International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne; INSU/CNRS (France); MPG (Germany); IGN (Spain); NASA [NNX08AW31G, NNX11A043G]; NSF [AST-0808050, AST-1109911] FX V.K. is thankful to B. Boccardi, A. P. Lobanov, W. Max-Moerbeck, B. Rani, S. Larsson, and A. Karastergiou for informative and fruitful discussions. We thank the anonymous referee for useful suggestions. V.K., I.N., and I.M. were supported for this research through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. Based on observations with the 100-m telescope of the MPIfR at Effelsberg and with the IRAM 30-m telescope. The single-dish mm observations were coordinated with the flux density monitoring conducted by IRAM, and data from both programs are included here. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). The OVRO 40-m Telescope Fermi Blazar Monitoring Program is supported by NASA under awards NNX08AW31G and NNX11A043G, and by the NSF under awards AST-0808050 and AST-1109911. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics who also fund it. This research has made use of NASA's Astrophysics Data System and the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 40 TC 1 Z9 1 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2016 VL 590 AR A48 DI 10.1051/0004-6361/201527796 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO9LB UT WOS:000378106800058 ER PT J AU Micelotta, ER Dwek, E Slavin, JD AF Micelotta, Elisabetta R. Dwek, Eli Slavin, Jonathan D. TI Dust destruction by the reverse shock in the Cassiopeia A supernova remnant SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE dust, extinction; ISM: supernova remnants; shock waves; supernovae: general; supernovae: individual: Cassiopeia A ID EARLY UNIVERSE; SPACE-TELESCOPE; HIGH-REDSHIFT; A SUPERNOVA; ASTROPHYSICAL PLASMAS; NUMERICAL SIMULATIONS; INTERSTELLAR GRAINS; MAGELLANIC CLOUDS; CARBON-MONOXIDE; II SUPERNOVAE AB Context. Core collapse supernovae (CCSNe) are important sources of interstellar dust, which are potentially capable of producing 1 M-circle dot of dust in their explosively expelled ejecta. However, unlike other dust sources, the dust has to survive the passage of the reverse shock, generated by the interaction of the supernova blast wave with its surrounding medium. Knowledge of the net amount of dust produced by CCSNe is crucial for understanding the origin and evolution of dust in the local and high-redshift Universe. Aims. We identify the dust destruction mechanisms in the ejecta and derive the net amount of dust that survives the passage of the reverse shock. Methods. We use analytical models for the evolution of a supernova blast wave and of the reverse shock with special application to the clumpy ejecta of the remnant of Cassiopeia A (Cas A). We assume that the dust resides in cool oxygen-rich clumps, which are uniformly distributed within the remnant and surrounded by a hot X-ray emitting plasma (smooth ejecta), and that the dust consists of silicates (MgSiO3) and amorphous carbon grains. The passage of the reverse shock through the clumps gives rise to a relative gas-grain motion and also destroys the clumps. While residing in the ejecta clouds, dust is processed via kinetic sputtering, which is terminated either when the grains escape the clumps or when the clumps are destroyed by the reverse shock. In either case, grain destruction proceeds thereafter by thermal sputtering in the hot shocked smooth ejecta. Results. We find that 11.8 and 15.9 percent of silicate and carbon dust, respectively, survive the passage of the reverse shock by the time the shock has reached the centre of the remnant. These fractions depend on the morphology of the ejecta and the medium into which the remnant is expanding, as well as the composition and size distribution of the grains that formed in the ejecta. Results will therefore differ for different types of supernovae. C1 [Micelotta, Elisabetta R.] Univ Paris 11, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. [Micelotta, Elisabetta R.; Dwek, Eli] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. [Slavin, Jonathan D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Micelotta, Elisabetta R.] Univ Helsinki, Dept Phys, Helsinki 00014, Finland. RP Micelotta, ER (reprint author), Univ Paris 11, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France.; Micelotta, ER (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.; Micelotta, ER (reprint author), Univ Helsinki, Dept Phys, Helsinki 00014, Finland. EM elisabetta.micelotta@helsinki.fi OI Micelotta, Elisabetta/0000-0002-6555-5109; Slavin, Jonathan/0000-0002-7597-6935 FU Marie Curie Intra-European Fellowship within 7th European Community Framework Programme NANOCOSMOS [PIEF-GA-2012-328902]; NASA's [13-ADAP13-0094] FX We are grateful to our anonymous referee for the careful reading and valuable suggestions and we would like to thank Martin Laming, Richard Arendt, Mordecai-Mark Mac Low, and Alex Hill for useful and stimulating discussions. E.R.M. wishes to acknowledge the support from a Marie Curie Intra-European Fellowship within the 7th European Community Framework Programme under project number PIEF-GA-2012-328902 NANOCOSMOS. E.D. acknowledges the support of NASA's 13-ADAP13-0094. NR 96 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2016 VL 590 AR A65 DI 10.1051/0004-6361/201527350 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO9LB UT WOS:000378106800034 ER PT J AU Miskovicova, I Hell, N Hanke, M Nowak, MA Pottschmidt, K Schulz, NS Grinberg, V Duro, R Madej, OK Lohfink, AM Rodriguez, J Bel, MC Bodaghee, A Tomsick, JA Lee, JC Brown, GV Wilms, J AF Miskovicova, Ivica Hell, Natalie Hanke, Manfred Nowak, Michael A. Pottschmidt, Katja Schulz, Norbert S. Grinberg, Victoria Duro, Refiz Madej, Oliwia K. Lohfink, Anne M. Rodriguez, Jerome Bel, Marion Cadolle Bodaghee, Arash Tomsick, John A. Lee, Julia C. Brown, Gregory V. Wilms, Joern TI Chandra X-ray spectroscopy of focused wind in the Cygnus X-1 system II. The non-dip spectrum in the low/hard state - modulations with orbital phase SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; stars: individual: Cyg X-1; stars: individual: HDE 226868; X-rays: binaries; stars: winds, outflows ID LONG-TERM VARIABILITY; PROPORTIONAL COUNTER ARRAY; RADIATION-DRIVEN WINDS; ION LINE-INTENSITIES; ALL-SKY MONITOR; BLACK-HOLE; STELLAR WIND; TIMING-EXPLORER; TRANSIENT DIPS; WARM ABSORBER AB Accretion onto the black hole in the system HDE 226868/Cygnus X-1 is powered by the strong line-driven stellar wind of the O-type donor star. We study the X-ray properties of the stellar wind in the hard state of Cyg X-1, as determined using data from the Chandra High Energy Transmission Gratings. Large density and temperature inhomogeneities are present in the wind, with a fraction of the wind consisting of clumps of matter with higher density and lower temperature embedded in a photoionized gas. Absorption dips observed in the light curve are believed to be caused by these clumps. This work concentrates on the non-dip spectra as a function of orbital phase. The spectra show lines of H-like and He-like ions of S, Si, Na, Mg, Al, and highly ionized Fe (Fe XVII-Fe XXIV). We measure velocity shifts, column densities, and thermal broadening of the line series. The excellent quality of these five observations allows us to investigate the orbital phase-dependence of these parameters. We show that the absorber is located close to the black hole. Doppler shifted lines point at a complex wind structure in this region, while emission lines seen in some observations are from a denser medium than the absorber. The observed line profiles are phase-dependent. Their shapes vary from pure, symmetric absorption at the superior conjunction to P Cygni profiles at the inferior conjunction of the black hole. C1 [Miskovicova, Ivica; Hell, Natalie; Hanke, Manfred; Grinberg, Victoria; Duro, Refiz; Wilms, Joern] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte, Sternwartstr 7, D-96049 Bamberg, Germany. [Miskovicova, Ivica; Hell, Natalie; Hanke, Manfred; Grinberg, Victoria; Duro, Refiz; Wilms, Joern] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Sternwartstr 7, D-96049 Bamberg, Germany. [Hell, Natalie; Brown, Gregory V.] Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA. [Nowak, Michael A.; Schulz, Norbert S.; Grinberg, Victoria] MIT Kavli Inst Astrophys & Space Res, NE80,77 Mass Ave, Cambridge, MA 02139 USA. [Pottschmidt, Katja] Univ Maryland Baltimore Cty, CRESST, 1000 Hilltop Circle, Baltimore, MD 21250 USA. [Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA. [Duro, Refiz] AIT Austrian Inst Technol GmbH, Donau City Str 1, A-1220 Vienna, Austria. [Madej, Oliwia K.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. [Madej, Oliwia K.] SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. [Lohfink, Anne M.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Rodriguez, Jerome] Univ Paris Diderot, CEA DSM, CNRS, Lab AIM,UMR 7158,IRFU SAp, F-91191 Gif Sur Yvette, France. [Bel, Marion Cadolle] Max Planck Comp & Data Facil, Giessenbachstr 2, D-85748 Garching, Germany. [Bodaghee, Arash] Georgia Coll & State Univ, Dept Chem Phys & Astron, Milledgeville, GA 31061 USA. [Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. [Lee, Julia C.] Harvard Univ, John A Paulson Sch Engn & Appl Sci, 60 Garden St MS-6, Cambridge, MA 02138 USA. [Lee, Julia C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St MS-6, Cambridge, MA 02138 USA. RP Wilms, J (reprint author), Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte, Sternwartstr 7, D-96049 Bamberg, Germany.; Wilms, J (reprint author), Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Sternwartstr 7, D-96049 Bamberg, Germany. EM joern.wilms@sternwarte.uni-erlangen.de RI Wilms, Joern/C-8116-2013 OI Wilms, Joern/0000-0003-2065-5410 FU European Community [ITN 215212]; Bundesministerium fur Wirtschaft und Technologie [DLR 50OR0701, 50OR1113]; Lawrence Livermore National Laboratory (LLNL) [DE-AC52-07NA27344]; NASA; NASA through the Smithsonian Astrophysical Observatory (SAO) [SV3-73016]; NASA [NAS8-03060]; DFG Cluster of Excellence "Origin and Structure of the Universe"; Computational Center for Particles and Astrophysics (C2PAP) FX The research leading to these results was funded by the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement number ITN 215212 "Black Hole Universe" and by the Bundesministerium fur Wirtschaft und Technologie under grant numbers DLR 50OR0701 and 50OR1113. This work was partially completed by Lawrence Livermore National Laboratory (LLNL) under Contract DE-AC52-07NA27344, and is supported by NASA grants to LLNL. Support for this work was also provided by NASA through the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to MIT for Support of the Chandra X-Ray Center (CXC) and Science Instruments; CXC is operated by SAO for and on behalf of NASA under contract NAS8-03060. We acknowledge the support by the DFG Cluster of Excellence "Origin and Structure of the Universe" and are grateful for the support by MCB through the Computational Center for Particles and Astrophysics (C2PAP). We are thankful to John E. Davis for the SLXfig package that was used to create the figures throughout this paper, to David Huenemoerder for the AGLC routines that handled the grating lightcurves and routines related to plasma diagnostics, and to Thomas Dauser for parallel computing routines. This research has made use of the MAXI data provided by RIKEN, JAXA, and the MAXI team. NR 88 TC 1 Z9 1 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2016 VL 590 AR A114 DI 10.1051/0004-6361/201322490 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO9LB UT WOS:000378106800001 ER PT J AU Olah, K Kovari, Z Petrovay, K Soon, W Baliunas, S Kollath, Z Vida, K AF Olah, K. Kovari, Zs. Petrovay, K. Soon, W. Baliunas, S. Kollath, Z. Vida, K. TI Magnetic cycles at different ages of stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: activity; starspots; stars: late-type; stars: solar-type; Sun: activity ID MAIN-SEQUENCE STARS; FIELD STARS; CHROMOSPHERIC VARIATIONS; ROTATION PERIOD; CHANGING CYCLES; NSTARS PROJECT; COOL STARS; DYNAMO; GYROCHRONOLOGY; MULTIPLE AB Aims. We study the different patterns of interannual magnetic variability in stars on or near the lower main sequence, approximately solar-type (G-K dwarf) stars in time series of 36 yr from the Mount Wilson Observatory Ca II H&K survey. Our main aim is to search for correlations between cycles, activity measures, and ages. Methods. Time-frequency analysis has been used to discern and reveal patterns and morphology of stellar activity cycles, including multiple and changing cycles, in the datasets. Both the results from short-term Fourier transform and its refinement using the Choi-Williams distribution, with better frequency resolution, are presented in this study. Rotational periods of the stars were derived using multifrequency Fourier analysis. Results. We found at least one activity cycle on 28 of the 29 stars we studied. Twelve stars, with longer rotational periods (39.7 +/- 6.0 days), have simple smooth cycles, and the remaining stars, with much faster rotation (18.1 +/- 12.2 days) on average, show complex and sometimes vigorously changing multiple cycles. The cycles are longer and quite uniform in the first group (9.7 +/- 1.9 yr), while they are generally shorter and vary more strongly in the second group (7.6 +/- 4.9). The clear age division between stars with smooth and complex cycles follows the known separation between the older and younger stars at around 2 to 3 Gyr of age. C1 [Olah, K.; Kovari, Zs.; Vida, K.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Mu 15-17, H-1121 Budapest, Hungary. [Petrovay, K.] Eotvos Lorand Univ, Dept Astron, Pf 32, H-1518 Budapest, Hungary. [Soon, W.; Baliunas, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kollath, Z.] Univ West Hungary, Inst Math & Phys, Savaria Campus, H-9400 Sopron, Hungary. RP Olah, K (reprint author), Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Mu 15-17, H-1121 Budapest, Hungary. EM olah@konkoly.hu FU Hungarian Science Research Program [OTKA-109276]; Lendulet Young Researchers' Programs of the Hungarian Academy of Sciences; SAO grant [SAO-504514-4210-40504514SS5000, SAO proposal 000000000003010-V101] FX Thanks are due to the anonymous referee for the useful advice and suggestions. This work has been supported by the Hungarian Science Research Program OTKA-109276 and the Lendulet-2012 Young Researchers' Programs of the Hungarian Academy of Sciences. K.O. is grateful to G. Kovacs for enlightening discussions about stellar ages, and to A. Moor for useful advice. W.S. works were partially supported by SAO grant SAO-504514-4210-40504514SS5000 and SAO proposal 000000000003010-V101. NR 46 TC 2 Z9 2 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2016 VL 590 AR A133 DI 10.1051/0004-6361/201628479 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO9LB UT WOS:000378106800137 ER PT J AU Reig, P Nersesian, A Zezas, A Gkouvelis, L Coe, MJ AF Reig, P. Nersesian, A. Zezas, A. Gkouvelis, L. Coe, M. J. TI Long-term optical variability of high-mass X-ray binaries II. Spectroscopy SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: emission-line, Be; stars: massive; X-rays: binaries ID 4U 0115+63/V635 CASSIOPEIAE; EMISSION-LINE SPECTROSCOPY; ONE-ARMED OSCILLATIONS; BE-SHELL STARS; H-ALPHA; GIANT OUTBURSTS; PHASE-CHANGES; NEUTRON-STAR; DISC-LOSS; MULTIWAVELENGTH OBSERVATIONS AB Context. High-mass X-ray binaries are bright X-ray sources. The high-energy emission is caused by the accretion of matter from the massive companion onto a neutron star. The accreting material comes from either the strong stellar wind in binaries with supergiant companions or the cirscumstellar disk in Be/X-ray binaries. In either case, the H-alpha line stands out as the main source of information about the state of the accreting material. Aims. We present the results of our monitoring program to study the long-term variability of the H-alpha line in high-mass X-ray binaries. Our aim is to characterise the optical variability timescales and study the interaction between the neutron star and the accreting material. Methods. We fitted the H-alpha line with Gaussian profiles and obtained the line parameters and equivalent width. The peak separation in split profiles was used to determine the disk velocity law and estimate the disk radius. The relative intensity of the two peaks (V/R ratio) allowed us to investigate the distribution of gas particles in the disk. The equivalent width was used to characterise the degree of variability of the systems. We also studied the variability of the H-alpha line in correlation with the X-ray activity. Results. Our results can be summarised as follows: i) we find that Be/X-ray binaries with narrow orbits are more variable than systems with long orbital periods; ii) we show that a Keplerian distribution of gas particles provides a good description of the disks in Be/X-ray binaries, as it does in classical Be stars; iii) a decrease in the H-alpha equivalent width is generally observed after major X-ray outbursts; iv) we confirm that the H-alpha equivalent width correlates with disk radius; v) while systems with supergiant companions display multi-structured profiles, most of the Be/X-ray binaries show, at some epoch, double-peak asymmetric profiles, which indicates that density inhomogeneities is a common property in the disk of Be/X-ray binaries; vi) the profile variability (V/R ratio) timescales are shorter and the H-alpha equivalent widths are smaller in Be/X-ray binaries than in isolated Be stars; and vii) we provide new evidence that the disk in Be/X-ray binaries is, on average, denser than in classical Be stars. Conclusions. We carried out the most complete optical spectroscopic study of the global properties of high-mass X-ray binaries with the analysis of more than 1100 spectra from 20 sources. Our results provide further evidence for the truncation of the disk in Be/X-ray binaries. We conclude that the interaction between the compact object and the Be-type star works in two directions: the massive companion provides the source of matter for accretion, affecting the surroundings of the compact object, and the continuous revolution of the neutron star around the optical counterpart also produces the truncation of the Be star's equatorial disk. C1 [Reig, P.; Zezas, A.] Fdn Res & Technol Hellas, IESL, Iraklion 71110, Greece. [Reig, P.; Nersesian, A.; Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Zezas, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Gkouvelis, L.] Univ Valencia, Astron Observ, E-46100 Burjassot, Spain. [Coe, M. J.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Reig, P (reprint author), Fdn Res & Technol Hellas, IESL, Iraklion 71110, Greece.; Reig, P (reprint author), Univ Crete, Dept Phys, Iraklion 71003, Greece. EM pau@physics.uoc.gr RI Reig, Pablo/A-1198-2014; Nersesian, Angelos/C-9225-2017; Zezas, Andreas/C-7543-2011 OI Reig, Pablo/0000-0002-6446-3050; Zezas, Andreas/0000-0001-8952-676X FU Smithsonian Astrophysical Observatory; European Union Marie Curie grant [MTKD-CT-2006-039965]; EU FP7 Capacities [GA 206469]; European Research Council under the European Union's Seventh Framework Programme/ERC Grant [617001]; NASA ADAP grant [NNX12AN05G]; NASA LTSA grant [NAG5-13056]; EU IRG grant [224878]; [GO3-14051X] FX Skinakas Observatory is a collaborative project of the University of Crete and the Foundation for Research and Technology-Hellas. This paper uses observations made at the South African Astronomical Observatory (SAAO) and data products produced by the OIR Telescope Data Center, supported by the Smithsonian Astrophysical Observatory. We thank observers P. Berlind and M. Calkins for performing the FLWO observations. This work was supported in part by the European Union Marie Curie grant MTKD-CT-2006-039965 and EU FP7 Capacities GA No206469. A.Z. acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement No. 617001. During the period of this work AZ has also been supported by the Chandra grant GO3-14051X, NASA ADAP grant NNX12AN05G, NASA LTSA grant NAG5-13056, and the EU IRG grant 224878. This work used NASA's Astrophysics Data System Bibliographic Services and of the SIMBAD database, operated at the CDS, Strasbourg, France. The WHT and its service programme (service proposal references SW2012b14 and SW2013a19) are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Swift/BAT transient monitor results provided by the Swift/BAT team. Quick-look results provided by the ASM/RXTE team. NR 87 TC 2 Z9 2 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2016 VL 590 AR A122 DI 10.1051/0004-6361/201628271 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO9LB UT WOS:000378106800114 ER PT J AU Beaudrot, L Kroetz, K Alvarez-Loayza, P Amaral, I Breuer, T Fletcher, C Jansen, PA Kenfack, D Lima, MGM Marshall, AR Martin, EH Ndoundou-Hockemba, M O'Brien, T Razafimahaimodison, JC Romero-Saltos, H Rovero, F Roy, CH Sheil, D Silva, CEF Spironello, WR Valencia, R Zvoleff, A Ahumada, J Andelman, S AF Beaudrot, Lydia Kroetz, Kailin Alvarez-Loayza, Patricia Amaral, Ieda Breuer, Thomas Fletcher, Christine Jansen, Patrick A. Kenfack, David Moreira Lima, Marcela Guimaraes Marshall, Andrew R. Martin, Emanuel H. Ndoundou-Hockemba, Mireile O'Brien, Timothy Razafimahaimodison, Jean Claude Romero-Saltos, Hugo Rovero, Francesco Roy, Cisquet Hector Sheil, Douglas Silva, Carlos E. F. Spironello, Wilson Roberto Valencia, Renato Zvoleff, Alex Ahumada, Jorge Andelman, Sandy TI Limited carbon and biodiversity co-benefits for tropical forest mammals and birds SO ECOLOGICAL APPLICATIONS LA English DT Article DE biodiversity co-benefit; camera trapping; carbon stocks; conservation planning; REDD; tropical ecology assessment and monitoring network; wildlife conservation ID SPECIES RICHNESS; ELEVATIONAL GRADIENT; DIVERSITY; CONSERVATION; VERTEBRATES; PRIORITIES; PRIMATES; COSTS; SCALE; MAPS AB The conservation of tropical forest carbon stocks offers the opportunity to curb climate change by reducing greenhouse gas emissions from deforestation and simultaneously conserve biodiversity. However, there has been considerable debate about the extent to which carbon stock conservation will provide benefits to biodiversity in part because whether forests that contain high carbon density in their aboveground biomass also contain high animal diversity is unknown. Here, we empirically examined medium to large bodied ground-dwelling mammal and bird (hereafter "wildlife") diversity and carbon stock levels within the tropics using camera trap and vegetation data from a pantropical network of sites. Specifically, we tested whether tropical forests that stored more carbon contained higher wildlife species richness, taxonomic diversity, and trait diversity. We found that carbon stocks were not a significant predictor for any of these three measures of diversity, which suggests that benefits for wildlife diversity will not be maximized unless wildlife diversity is explicitly taken into account; prioritizing carbon stocks alone will not necessarily meet biodiversity conservation goals. We recommend conservation planning that considers both objectives because there is the potential for more wildlife diversity and carbon stock conservation to be achieved for the same total budget if both objectives are pursued in tandem rather than independently. Tropical forests with low elevation variability and low tree density supported significantly higher wildlife diversity. These tropical forest characteristics may provide more affordable proxies of wildlife diversity for future multi-objective conservation planning when fine scale data on wildlife are lacking. C1 [Beaudrot, Lydia; Zvoleff, Alex; Ahumada, Jorge; Andelman, Sandy] Conservat Int, Moore Ctr Sci, TEAM Network, Arlington, VA USA. [Kroetz, Kailin] Resources Future Inc, 1616 P ST NW,Suite 600, Washington, DC 20036 USA. [Alvarez-Loayza, Patricia] Duke Univ, Ctr Trop Conservat, 3705 Erwin Rd B, Durham, NC 27705 USA. [Amaral, Ieda; Silva, Carlos E. F.; Spironello, Wilson Roberto] Natl Inst Amazonian Res INPA, Av Andre Arauijo 2936, BR-69067 Manaus, Amazonas, Brazil. [Breuer, Thomas; Ndoundou-Hockemba, Mireile; Roy, Cisquet Hector] Wildlife Conservat Soc, Congo Program, BP 14537, Brazzaville, Rep Congo. [Fletcher, Christine] Forest Res Inst Malaysia, Jalan Frim, Kuala Lumpur, Selangor 52109, Malaysia. [Jansen, Patrick A.] Wageningen Univ, Dept Environm Sci, NL-6700 AP Wageningen, Netherlands. [Jansen, Patrick A.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Panama City 084303092, Panama. [Kenfack, David] Trop Res Inst, Ctr Trop Forest Sci, Smithsonian 10th & Constitut Ave NW, Washington, DC 20560 USA. [Moreira Lima, Marcela Guimaraes] Museu Paraense Emilio Goeldi, Av Governador Magalhaes Barata 376, BR-66040 Belem, Para, Brazil. [Marshall, Andrew R.] Univ York, Dept Environm, CIRCLE, Wentworth Way, York YO10 K, N Yorkshire, England. [Martin, Emanuel H.] Coll African Wildlife Management, Dept Wildlife Management, POB 3031, Moshi, Tanzania. [Martin, Emanuel H.] Ecol Monitoring Ctr, POB 99, Mangula Morogoro, Tanzania. [O'Brien, Timothy] Wildlife Conservat Soc, 2300 So Blvd, Bronx, NY 10460 USA. [Razafimahaimodison, Jean Claude] Ctr ValBio Ranomafana, Ranomafana 312, Madagascar. [Romero-Saltos, Hugo] Yachay Tech, Ciudad Conocimiento Yachay, Urcuqui 100115, Imbabura, Ecuador. [Rovero, Francesco] Museo Sci MUSE, Trop Biodivers, Corso Lavoro Sci 3, I-38123 Trento, Italy. [Sheil, Douglas] Norwegian Univ Life Sci NMBU, Dept Ecol & Nat Resource Management INA, Box 5003, N-1432 As, Norway. [Valencia, Renato] Pontifical Catholic Univ Ecuador, Ave 12 Octubre & Vicente Ramon Roca, Quito, Ecuador. [Beaudrot, Lydia] Univ Michigan, Dept Ecol & Evolutionary Biol, 830 Univ Ave, Ann Arbor, MI 48109 USA. [Beaudrot, Lydia] Univ Michigan, Michigan Soc Fellows, 830 Univ Ave, Ann Arbor, MI 48109 USA. RP Sheil, D (reprint author), Norwegian Univ Life Sci NMBU, Dept Ecol & Nat Resource Management INA, Box 5003, N-1432 As, Norway. EM beaudrot@umich.edu FU Gordon and Betty Moore Foundation; Leverhulme Trust FX All TEAM data in this publication were provided by the Tropical Ecology Assessment and Monitoring (TEAM) Network, a collaboration between Conservation International, the Smithsonian Institution, and the Wildlife Conservation Society, and partially funded by these institutions, the Gordon and Betty Moore Foundation, and other donors. All TEAM data are publically available at teamnetwork.org/data.; We thank A. Campos-Arceiz, P. Boundja, R. Condit, M. Nusalaqo, L. Valle Ferreira, J. Hurtado, R. Vasquez, J. Salvador, D. Auz, and all of the field assistants for their contributions to the TEAM site data; M. Rosa, J. MacCarthy, and E. Fegraus for technical support; S. Davies, N. Beaudrot, and K. Feilen for discussion; J. Ho for research assistance. We acknowledge the Valuing the Arc project, through which ARM established plots under funding from the Leverhulme Trust and we gratefully thank J. Lovett, S. Lewis, and P. Munishi for their contributions. We thank D. Schimel and the anonymous reviewers whose comments helped improve earlier versions of this manuscript. NR 69 TC 2 Z9 2 U1 26 U2 36 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1051-0761 EI 1939-5582 J9 ECOL APPL JI Ecol. Appl. PD JUN PY 2016 VL 26 IS 4 BP 1098 EP 1111 DI 10.1890/15-0935 PG 14 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA DO9GK UT WOS:000378092900011 PM 27509751 ER PT J AU Bret, A Novo, AS Narayan, R Ruyer, C Dieckmann, ME Silva, LO AF Bret, A. Novo, A. Stockem Narayan, R. Ruyer, C. Dieckmann, M. E. Silva, L. O. TI Theory of the formation of a collisionless Weibel shock: pair vs. electron/proton plasmas SO LASER AND PARTICLE BEAMS LA English DT Article DE Collisionless shocks; Weibel instability ID RAY BURST SHOCKS; PARTICLE-ACCELERATION; ELECTROMAGNETIC INSTABILITIES; COSMIC-RAYS; GENERATION; MECHANISM; ENERGY; STREAM; WAVES; BEAM AB Collisionless shocks are shocks in which the mean-free path is much larger than the shock front. They are ubiquitous in astrophysics and the object of much current attention as they are known to be excellent particle accelerators that could be the key to the cosmic rays enigma. While the scenario leading to the formation of a fluid shock is well known, less is known about the formation of a collisionless shock. We present theoretical and numerical results on the formation of such shocks when two relativistic and symmetric plasma shells (pair or electron/proton) collide. As the two shells start to interpenetrate, the overlapping region turns Weibel unstable. A key concept is the one of trapping time tau(p), which is the time when the turbulence in the central region has grown enough to trap the incoming flow. For the pair case, this time is simply the saturation time of the Weibel instability. For the electron/proton case, the filaments resulting from the growth of the electronic and protonic Weibel instabilities, need to grow further for the trapping time to be reached. In either case, the shock formation time is 2 tau(p) in two-dimensional (2D), and 3 tau(p) in 3D. Our results are successfully checked by particle-in-cell simulations and may help designing experiments aiming at producing such shocks in the laboratory. C1 [Bret, A.] Univ Castilla La Mancha, ETSI Ind, E-13071 Ciudad Real, Spain. [Bret, A.] Inst Invest Energet & Aplicac Ind, Campus Univ Ciudad Real, Ciudad Real 13071, Spain. [Novo, A. Stockem] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44801 Bochum, Germany. [Narayan, R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. [Ruyer, C.] SLAC Natl Accelerator Lab, High Energy Dens Sci Div, Menlo Pk, CA 94025 USA. [Dieckmann, M. E.] Linkoping Univ, Dept Sci & Technol, SE-60174 Norrkoping, Sweden. [Silva, L. O.] Inst Super Tecn, GoLP, Inst Plasmas & Fusao Nucl, Lab Associado, Lisbon, Portugal. RP Bret, A (reprint author), Univ Castilla La Mancha, ETSI Ind, E-13071 Ciudad Real, Spain. EM antoineclaude.bret@uclm.es RI Dieckmann, Mark Eric/C-8591-2009 OI Dieckmann, Mark Eric/0000-0003-4055-0552 FU European Research Council [267841]; Ministerio de Educacion y Ciencia, Spain [ENE2013-45661-C2-1-P]; Junta de Comunidades de Castilla-La Mancha [PEII-2014-008-P] FX This work was supported by the European Research Council (ERC-2010-AdG grant 267841), by grant ENE2013-45661-C2-1-P from the Ministerio de Educacion y Ciencia, Spain, and grant PEII-2014-008-P from the Junta de Comunidades de Castilla-La Mancha. The authors acknowledge the Gauss Centre for Supercomputing (GCS) for providing computing time through the John von Neumann Institute for Computing (NIC) on the GCS share of the supercomputer JUQUEEN at Julich Supercomputing Centre (JSC). NR 40 TC 0 Z9 0 U1 2 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0263-0346 EI 1469-803X J9 LASER PART BEAMS JI Laser Part. Beams PD JUN PY 2016 VL 34 IS 2 BP 362 EP 367 DI 10.1017/S0263034616000197 PG 6 WC Physics, Applied SC Physics GA DP2XZ UT WOS:000378358100019 ER PT J AU Nkrumah, EE Vallo, P Klose, SM Ripperger, S Badu, EK Drosten, C Kalko, EKV Tschapka, M Oppong, SK AF Nkrumah, Evans E. Vallo, Peter Klose, Stefan M. Ripperger, Simon Badu, Ebenezer K. Drosten, Christian Kalko, Elisabeth K. V. Tschapka, Marco Oppong, Samuel K. TI Home range of Noack's round-leaf bat (Hipposideros aff. ruber) in an agricultural landscape of central Ghana SO ACTA CHIROPTEROLOGICA LA English DT Article DE core area; foraging area; local convex hull; maximum foraging distance; radio-tracking ID CHIROPTERA HIPPOSIDERIDAE; UTILIZATION DISTRIBUTIONS; CAFFER CHIROPTERA; HABITAT SELECTION; FORAGING BEHAVIOR; SIZE; AREA; TERRITORIALITY; ECHOLOCATION; CONSERVATION AB Thirteen individuals of Noack's round-leaf bat, Hipposideros aff. ruber, were radio-tracked for 38 nights in an agricultural landscape in Kwamang, Ashanti Region, Ghana. Local convex hulls were used to estimate home range sizes of the bats. Based on 1,192 fixes, the mean (+/-SD) home range size was 36 ha +/- 35 ha. Individual home range size ranged from six to 95 ha and frequently overlapped among individuals. The foraging area covered 50% of the home range while the core area formed 2%. The mean maximum foraging distance was 1.1 km, with individual distances up to 2.6 km, suggesting Hipposideros aff. ruber is capable of covering relatively long distances. Male bats returned to the cave more often than females during the night. Although the cave was the main roost, each bat also had individual night roosts on trees. C1 [Nkrumah, Evans E.; Badu, Ebenezer K.; Oppong, Samuel K.] Kwame Nkrumah Univ Sci & Technol, Dept Wildlife & Range Management, Kumasi, Ghana. [Vallo, Peter; Klose, Stefan M.; Ripperger, Simon; Kalko, Elisabeth K. V.; Tschapka, Marco] Univ Ulm, Evolutionary Ecol & Conservat Genom, Albert Einstein Allee 11, D-89069 Ulm, Germany. [Vallo, Peter] Acad Sci Czech Republic, Inst Vertebrate Biol, Vvi, Kvetna 8, CS-60365 Brno, Czech Republic. [Drosten, Christian] Univ Bonn, Med Ctr, Inst Virol, D-53127 Bonn, Germany. [Kalko, Elisabeth K. V.; Tschapka, Marco] Smithsonian Trop Res Inst, Balboa, Panama. RP Oppong, SK (reprint author), Kwame Nkrumah Univ Sci & Technol, Dept Wildlife & Range Management, Kumasi, Ghana. EM kobbyoppong@yahoo.com RI Vallo, Peter/F-9650-2014 FU DFG [KA 1241/18-1]; Kumasi Centre for Collaborative Research in Tropical Medicine (KCCR) in Ghana FX All field work was done with the help of the German Research Foundation (DFG) Bat Project field workers in Ghana. We would like to thank all field workers, especially David Ofori Agyei, Kathrin Kubiczek (University of Ulm) and Ebenezer Gyimah for their outstanding contributions to data collection. We also thank Heather J. Baldwin for bringing field supplies from Germany to Ghana. Funds for this study were provided by DFG to Elisabeth K. V. Kalko (KA 1241/18-1). We would also like to thank Julia Morrison and Lucinda Kirkpatrick who volunteered during part of the study. Finally, we thank the Kumasi Centre for Collaborative Research in Tropical Medicine (KCCR) in Ghana for providing the research platform and the necessary support to the project. NR 56 TC 1 Z9 1 U1 3 U2 7 PU MUSEUM & INST ZOOLOGY PAS-POLISH ACAD SCIENCES PI WARSAW PA WILCZA STREET 64, 00-679 WARSAW, POLAND SN 1508-1109 EI 1733-5329 J9 ACTA CHIROPTEROL JI Acta Chiropt. PD JUN PY 2016 VL 18 IS 1 BP 239 EP 247 DI 10.3161/15081109ACC2016.18.1.014 PG 9 WC Zoology SC Zoology GA DO4ZT UT WOS:000377794100014 ER PT J AU Edwards, MH Shjegstad, SM Wilkens, R King, JC Carton, G Bala, D Bingham, B Bissonnette, MC Briggs, C Bruso, NS Camilli, R Cremer, M Davis, RB DeCarlo, EH DuVal, C Fornari, DJ Kaneakua-Pia, I Kelley, CD Koide, S Mah, CL Kerby, T Kurras, GJ Rognstad, MR Sheild, L Silva, J Wellington, B Van Woerkom, M AF Edwards, Margo H. Shjegstad, Sonia M. Wilkens, Roy King, James C. Carton, Geoff Bala, Deserie Bingham, Brian Bissonnette, Martine C. Briggs, Christian Bruso, Natalie S. Camilli, Rich Cremer, Max Davis, Roger B. DeCarlo, Eric H. DuVal, Carter Fornari, Daniel J. Kaneakua-Pia, Iolana Kelley, Christopher D. Koide, Shelby Mah, Christopher L. Kerby, Terry Kurras, Gregory J. Rognstad, Mark R. Sheild, Lukas Silva, Jeff Wellington, Basil Van Woerkom, Michael TI The Hawaii Undersea Military Munitions Assessment SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article DE Disposed munitions; Mustard agent; Marine geophysics; Marine biology ID DISPOSAL AB The Hawaii Undersea Military Munitions Assessment (HUMMA) is the most comprehensive deep-water investigation undertaken by the United States to look at sea-disposed chemical and conventional munitions. HUMMA's primary scientific objective is to bound, characterize and assess a historic deep-water munitions sea-disposal site to determine the potential impact of the ocean environment on sea-disposed munitions and of sea-disposed munitions on the ocean environment and those that use it Between 2007 and 2012 the HUMMA team conducted four field programs, collecting hundreds of square kilometers of acoustic data for high-resolution seafloor maps, tens of thousands of digital images, hundreds of hours of video of individual munitions, hundreds of physical samples acquired within two meters of munitions casings, and a suite of environmental data to characterize the ocean surrounding munitions in the study area. Using these data we examined six factors in the study area: (1) the spatial extent and distribution of munitions; (2) the integrity of munitions casings; (3) whether munitions constituents could be detected in sediment, seawater or animals near munitions; (4) whether constituent levels at munitions sites differed significantly from levels at reference control sites; (5) whether statistically significant differences in ecological population metrics could be detected between the two types of sites; and (6) whether munitions constituents or their derivatives potentially pose an unacceptable risk to human health. Herein we provide a general overview of HUMMA including overarching goals, methodologies, physical characteristics of the study area, data collected and general results. Detailed results, conclusions and recommendations for future research are discussed in the accompanying papers included in this volume. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Edwards, Margo H.; Wilkens, Roy; Bruso, Natalie S.; Davis, Roger B.; Rognstad, Mark R.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, 1680 East West Rd, Honolulu, HI 96822 USA. [Shjegstad, Sonia M.; Bala, Deserie; Bissonnette, Martine C.; Briggs, Christian; Kaneakua-Pia, Iolana; Koide, Shelby; Sheild, Lukas; Silva, Jeff; Wellington, Basil; Van Woerkom, Michael] Environet Inc, 1286 Queen Emma St, Honolulu, HI 96813 USA. [King, James C.] Headquarters Dept Army, Off Deputy Assistant Secretary Environm Safety &, Washington, DC USA. [Carton, Geoff] CALIBRE Syst Inc, Alexandria, VA USA. [Bingham, Brian] Univ Hawaii Manoa, Coll Engn, 2540 Dole St, Honolulu, HI 96822 USA. [Camilli, Rich] Woods Hole Oceanog Inst, Dept Appl Ocean Phys & Engn, Deep Submergence Lab, Woods Hole, MA 02543 USA. [Cremer, Max; Kerby, Terry] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Undersea Res Lab, 1000 Pope Rd, Honolulu, HI 96822 USA. [DeCarlo, Eric H.; Kelley, Christopher D.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Dept Oceanog, 1000 Pope Rd, Honolulu, HI 96822 USA. [DuVal, Carter] Univ Delaware, 255 Acad St,Penny Hall 103, Newark, DE 19716 USA. [Fornari, Daniel J.] Woods Hole Oceanog Inst, Dept Geol & Geophys, Woods Hole, MA 02543 USA. [Mah, Christopher L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012,MRC 163, Washington, DC 20013 USA. [Kurras, Gregory J.] Seafloor Invest LLC, 93 South Jackson St 28990, Seattle, WA 98104 USA. RP Edwards, MH (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, 1680 East West Rd, Honolulu, HI 96822 USA. NR 37 TC 3 Z9 3 U1 6 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 EI 1879-0100 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PD JUN PY 2016 VL 128 BP 4 EP 13 DI 10.1016/j.dsr2.2016.04.011 PG 10 WC Oceanography SC Oceanography GA DO4FN UT WOS:000377737300002 ER PT J AU Edwards, MH Fornari, DJ Rognstad, MR Kelley, CD Mah, CL Davis, LK Flores, KRM Main, EL Bruso, NL AF Edwards, Margo H. Fornari, Daniel J. Rognstad, Mark R. Kelley, Christopher D. Mah, Christopher L. Davis, Logan K. Flores, Kyle R. M. Main, Erin L. Bruso, Natalie L. TI Time-lapse camera studies of sea-disposed chemical munitions in Hawaii SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article ID PHOTOGRAPHY; FLOOR AB The interactions between fauna and sea-disposed munitions provide important evidence regarding whether munitions constituents affect the health of the ocean environment and its inhabitants. To date few studies of these interactions have been conducted at deep-water disposal sites; typically observations of fauna in the vicinity of sea-disposed munitions are limited to the few minutes or hours required to collect physical samples at a specific location. During the 2012 Hawaii Undersea Military Munitions Assessment (HUMMA) field program we deployed two deep-sea time-lapse camera systems with the objectives of cataloging the diversity of fauna visiting sea-disposed chemical munitions and observing faunal behavior and physiology. Over the 1- and 3-day deployments we recorded 28 different species of fishes, crustaceans, mollusks, cnidarians, and echinoderms at the two sites. Both cameras captured the previously undocumented behavior of brisingid sea stars repositioning themselves along chemical munitions casings. Despite the fact that brisingid sea stars are able to move, for the duration of both time-lapse experiments they remained on chemical munitions casings. We interpret this result to indicate that the advantages of residing on a hard substrate slightly elevated above the seafloor outweigh the effects of chemical munitions constituents for brisingid sea stars. One type of physiological anomaly observed on several arms of the brisingid sea stars at the time-lapse sites led to the collection and examination of six specimens. As reported by Mah (2015. Deep Sea Res. II, 2015, XX-XX), these physiological features are the result of parasitic crustaceans and are not caused by chemical munitions constituents. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Edwards, Margo H.; Rognstad, Mark R.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, 1680 East West Rd, Honolulu, HI 96822 USA. [Fornari, Daniel J.] Woods Hole Oceanog Inst, Geol & Geophys Dept, Woods Hole, MA 02543 USA. [Kelley, Christopher D.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Dept Oceanog, 1000 Pope Rd, Honolulu, HI 96822 USA. [Mah, Christopher L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012,MRC 163, Washington, DC 20013 USA. [Davis, Logan K.; Flores, Kyle R. M.] Franklin W Olin Coll Engn, 1000 Olin Way, Needham, MA 02492 USA. [Main, Erin L.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Bruso, Natalie L.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, 1680 East West Rd, Honolulu, HI 96822 USA. RP Edwards, MH (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, 1680 East West Rd, Honolulu, HI 96822 USA. EM margo@soest.hawaii.edu FU U.S. Army's Night Vision Laboratory [W909MY-12-C-0029] FX We thank the Captain, crew and scientists of the Research Vessel Ka'imikai-o-Kanaloa for their assistance in deploying and recovering the time-lapse camera systems. This work would not have been successful without Colin Wollerman, Terry Kerby, Max Cremer and the rest of the Hawaii Undersea Research Laboratory group as well as the help of Greg Kurras. The unwavering encouragement of J.C. King and H. Wolfe greatly enhanced a student project. The U.S. Army's Night Vision Laboratory supported this research via contract W909MY-12-C-0029. SOEST contribution ####; HIGP contribution ####. NR 18 TC 3 Z9 3 U1 4 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 EI 1879-0100 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PD JUN PY 2016 VL 128 BP 25 EP 33 DI 10.1016/j.dsr2.2015.03.003 PG 9 WC Oceanography SC Oceanography GA DO4FN UT WOS:000377737300004 ER PT J AU Mah, CL AF Mah, Christopher L. TI A new species of Brisingenes from the Hawaii undersea military munitions assessment area with an overview of Hawaiian brisingid in situ video observations and functional morphology of subambulacral spines (Forcipulatacea; Asteroidea) SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article DE Deep-sea; Brisingida; Asteroidea; Echinodermata; Functional morphology ID ECHINODERMATA; CLASSIFICATION; PREDATION; URCHINS AB A new species of Brisingenes, Brisingenes margoae nov. sp. is described from the HUMMA Study Area (see overview (Edwards et al., 2016-a), Oahu in the Hawaiian Islands. This represents a range extension for Brisingenes to the North Pacific and is the fifth-known brisingid species in the Hawaiian region. An overview of other Hawaiian brisingid species based on HURL in situ video observations is presented. Submersible-collected B. margoae and Brisingenes panopla provides new insight into functional morphology of brisingid subambulacral spines. The high abundance of brisingids in the HUMMA Study Area is briefly reviewed. Identification keys for relevant taxa are provided. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Mah, Christopher L.] Smithsonian Inst, Dept Invertebrate Zool NMNH, Washington, DC 20560 USA. RP Mah, CL (reprint author), Smithsonian Inst, Dept Invertebrate Zool NMNH, Washington, DC 20560 USA. NR 60 TC 2 Z9 2 U1 3 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 EI 1879-0100 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PD JUN PY 2016 VL 128 BP 43 EP 52 DI 10.1016/j.dsr2.2014.06.003 PG 10 WC Oceanography SC Oceanography GA DO4FN UT WOS:000377737300006 ER PT J AU Thornton, R AF Thornton, Russell TI Colonial Genocide in Indigenous North America SO REVIEWS IN AMERICAN HISTORY LA English DT Book Review C1 [Thornton, Russell] Univ Calif Los Angeles, Los Angeles, CA 90024 USA. [Thornton, Russell] Smithsonian Inst, Native Amer Repatriat Review Comm, Washington, DC 20560 USA. RP Thornton, R (reprint author), Univ Calif Los Angeles, Los Angeles, CA 90024 USA. NR 1 TC 0 Z9 0 U1 2 U2 2 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0048-7511 EI 1080-6628 J9 REV AM HIST JI Rev. Am. Hist. PD JUN PY 2016 VL 44 IS 2 BP 210 EP 216 PG 7 WC History SC History GA DO8DT UT WOS:000378013500009 ER PT J AU Thornton, R AF Thornton, Russell TI Native America and the Question of Genocide SO REVIEWS IN AMERICAN HISTORY LA English DT Book Review C1 [Thornton, Russell] Univ Calif Los Angeles, Anthropol, Los Angeles, CA 90024 USA. [Thornton, Russell] Smithsonian Inst, Native Amer Repatriat Review Comm, Washington, DC 20560 USA. RP Thornton, R (reprint author), Univ Calif Los Angeles, Anthropol, Los Angeles, CA 90024 USA. NR 1 TC 0 Z9 0 U1 2 U2 2 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0048-7511 EI 1080-6628 J9 REV AM HIST JI Rev. Am. Hist. PD JUN PY 2016 VL 44 IS 2 BP 210 EP 216 PG 7 WC History SC History GA DO8DT UT WOS:000378013500007 ER PT J AU Thornton, R AF Thornton, Russell TI Ethnic Cleansing and the Indian: The Crime That Should Haunt America SO REVIEWS IN AMERICAN HISTORY LA English DT Book Review C1 [Thornton, Russell] Univ Calif Los Angeles, Anthropol, Los Angeles, CA 90024 USA. [Thornton, Russell] Smithsonian Inst, Native Amer Repatriat Review Comm, Washington, DC 20560 USA. RP Thornton, R (reprint author), Univ Calif Los Angeles, Anthropol, Los Angeles, CA 90024 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0048-7511 EI 1080-6628 J9 REV AM HIST JI Rev. Am. Hist. PD JUN PY 2016 VL 44 IS 2 BP 210 EP 216 PG 7 WC History SC History GA DO8DT UT WOS:000378013500008 ER PT J AU Carter, GG Wilkinson, GS AF Carter, Gerald G. Wilkinson, Gerald S. TI Common vampire bat contact calls attract past food-sharing partners SO ANIMAL BEHAVIOUR LA English DT Article DE bat; communication; cooperation; food sharing; individual recognition; kin recognition; social call; vampire bat; vocal recognition; vocalization ID TADARIDA-BRASILIENSIS-MEXICANA; FISSION-FUSION DYNAMICS; SPEAR-NOSED BATS; FREE-TAILED BATS; KIN RECOGNITION; PAIRWISE RELATEDNESS; SOCIAL-ORGANIZATION; RECIPROCAL ALTRUISM; MOLECULAR MARKERS; DESMODUS-ROTUNDUS AB Animals living with kin and nonkin should make social decisions based on the consequences for both direct and indirect fitness. Common vampire bats, Desmodus rotundus, invest in stable cooperative relationships that benefit both components of inclusive fitness. To disentangle these two factors, we conducted two types of playback trials using a captive group of familiar common vampire bats with mixed kinship and varying rates of dyadic food sharing. We presented each subject with two speakers, playing contact calls from two different familiar conspecifics. In 'past donor trials', 15 vampire bats chose between calls recorded from either a frequent or rare food donor, but both callers were related to a similar degree with the subject. In 'kinship trials', 31 vampire bats chose between calls recorded from either a close or distant relative, but both callers were matched for food-sharing history with the subject. We found that vampire bats were attracted to contact calls of frequent food donors when controlling for kinship, but not to calls of kin when controlling for food-sharing history. Responses and acoustic analyses suggested that bats recognized individuals from vocalizations. These results corroborate past findings that prior food sharing can overshadow relatedness in determining the social decisions of vampire bats. Common vampire bat contact calls allow food-sharing partners to recognize and find each other at a distance, which likely enables them to switch roosts together in the wild. (C) 2016 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Carter, Gerald G.] Smithsonian Trop Res Inst, Gamboa, Panama. [Wilkinson, Gerald S.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. Smithsonian Trop Res Inst, Attn Gerry Carter Rachel Page Lab, Gamboa, Panama. RP Carter, GG (reprint author), Smithsonian Trop Res Inst, Attn Gerry Carter Rachel Page Lab, POB 0843-00153, Gamboa, Panama. EM gerry@socialbat.org OI Carter, Gerald/0000-0001-6933-5501; Wilkinson, Gerald/0000-0001-7799-8444 FU Animal Behavior Society; American Society of Mammalogists; Doctoral Dissertation Improvement Grant from the National Science Foundation [1311336] FX This study was made possible by collaboration with the Organization for Bat Conservation, with help from R. Mies, A. Felk, N. Siekert, J. Fabian, L. Dehn and K. Vowles. The experimental maze was built by K. Sullenger. The work was supported by student research grants from the Animal Behavior Society and the American Society of Mammalogists, and a Doctoral Dissertation Improvement Grant from the National Science Foundation (1311336). We thank Brock Fenton, Ken Yasukawa and an anonymous referee for suggestions that improved the manuscript. NR 61 TC 1 Z9 1 U1 43 U2 71 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 JUN PY 2016 VL 116 BP 45 EP 51 DI 10.1016/j.anbehav.2016.03.005 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA DN7UY UT WOS:000377286700007 ER PT J AU Ramakers, JJC Dechmann, DKN Page, RA O'Mara, MT AF Ramakers, Jip J. C. Dechmann, Dina K. N. Page, Rachel A. O'Mara, M. Teague TI Frugivorous bats prefer information from novel social partners SO ANIMAL BEHAVIOUR LA English DT Article DE information centre; information scrounging; roostmate recognition; social information; social learning; Uroderma bilobatum ID PRODUCER-SCROUNGER GAME; FRUIT-EATING BATS; PUBLIC INFORMATION; LEARNING STRATEGIES; URODERMA-BILOBATUM; CENTER HYPOTHESIS; FOOD PREFERENCES; DECISION-MAKING; FAMILIARITY; BEHAVIOR AB Animals use social information from conspecifics as an extended sensor network to monitor their environment and may bias their preference to information from particular individuals, e.g. individuals they are most familiar with. This may be especially important for energy-constrained foragers, such as the frugivorous Peter's tent-making bat, Uroderma bilobatum. We used the outcome of a two-demonstrator social-learning test in which individual U. bilobatum had to make cue-elicited decisions based on food odours from bats from different social groups to test three alternative hypotheses. Bats could show either (1) a preference for information from roostmates ('familiar social partner'), (2) no bias in information used ('any social partner') or (3) a preference for novel cues from nonroostmates ('novel social partner' hypothesis). We found that U. bilobatum preferred food demonstrated by nonroostmates to that demonstrated by roostmates, providing support for the novel social partner hypothesis. Uroderma bilobatum bias their attention towards novel conspecifics, perhaps as a strategy for acquiring knowledge of unknown ephemeral food sources, which in turn might help them survive resource bottlenecks. (c) 2016 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Ramakers, Jip J. C.] Univ Utrecht, Dept Biol, Utrecht, Netherlands. [Ramakers, Jip J. C.] Netherlands Inst Ecol NIOO KNAW, Dept Anim Ecol, Wageningen, Netherlands. [Ramakers, Jip J. C.; Dechmann, Dina K. N.; Page, Rachel A.; O'Mara, M. Teague] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Dechmann, Dina K. N.; O'Mara, M. Teague] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, D-178315 Radolfzell am Bodensee, Germany. [Dechmann, Dina K. N.; O'Mara, M. Teague] Univ Konstanz, Dept Biol, Constance, Germany. [O'Mara, M. Teague] Univ Konstanz, Zukunftskolleg, Constance, Germany. RP O'Mara, MT (reprint author), Max Planck Inst Ornithol, D-178315 Radolfzell am Bodensee, Germany. EM tomara@om.mpg.de OI KNAW, NIOO-KNAW/0000-0002-3835-159X; O'Mara, M. Teague/0000-0002-6951-1648 FU Erasmus student fellowship; University of Konstanz; Max Planck Institute for Ornithology; Smithsonian Tropical Research Institute FX This study was supported in part by an Erasmus student fellowship to J. J. C. R.; additional funding was provided by the University of Konstanz, the Max Planck Institute for Ornithology and the Smithsonian Tropical Research Institute. We are grateful to researchers in the STRI bat lab for their logistic support, in particular Jenna Kohles, Sebastian Stockmaier and Tom Faughnan. Allert Bijleveld and two anonymous referees kindly provided constructive comments on the manuscript. NR 52 TC 0 Z9 0 U1 13 U2 27 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 JUN PY 2016 VL 116 BP 83 EP 87 DI 10.1016/j.anbehav.2016.03.021 PG 5 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA DN7UY UT WOS:000377286700011 ER PT J AU Chen, HRV Keto, E Zhang, QZ Sridharan, TK Liu, SY Su, YN AF Chen, Huei-Ru Vivien Keto, Eric Zhang, Qizhou Sridharan, T. K. Liu, Sheng-Yuan Su, Yu-Nung TI A HOT AND MASSIVE ACCRETION DISK AROUND THE HIGH-MASS PROTOSTAR IRAS 20126+4104 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: kinematics and dynamics; stars: early-type; stars: formation; stars: individual (IRAS 20126+4104) ID SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMING REGIONS; T-TAURI STARS; YOUNG STARS; STANDARD MODEL; ROTATING-DISK; IRAS-20126+4104; INSTABILITIES; EMISSION; SYSTEM AB We present new spectral line observations of the CH3CN molecule in the accretion disk around the massive protostar IRAS 20126+4104 with the Submillimeter Array, which, for the first time, measure the disk density, temperature, and rotational velocity with sufficient resolution (0 37, equivalent to similar to 600 au) to assess the gravitational stability of the disk through the Toomre-Q parameter. Our observations resolve the central 2000 au region that shows steeper velocity gradients with increasing upper state energy, indicating an increase in the rotational velocity of the hotter gas nearer the star. Such spin-up motions are characteristics of an accretion flow in a rotationally supported disk. We compare the observed data with synthetic image cubes produced by three-dimensional radiative transfer models describing a thin flared disk in Keplerian motion enveloped within the centrifugal radius of an angular-momentum-conserving accretion flow. Given a luminosity of 1.3 x 10(4) L-circle dot, the optimized model gives a disk mass of 1.5 M-circle dot and a radius of 858 au rotating about a 12.0 M-circle dot protostar with a disk mass accretion rate of 3.9 x 10(-5) M-circle dot yr(-1). Our study finds that, in contrast to some theoretical expectations, the disk is hot and stable to fragmentation with Q > 2.8 at all radii which permits a smooth accretion flow. These results put forward the first constraints on gravitational instabilities in massive protostellar disks, which are closely connected to the formation of companion stars and planetary systems by fragmentation. C1 [Chen, Huei-Ru Vivien] Natl Tsing Hua Univ, Inst Astron, 101,Sec 2,Kuang Fu Rd, Hsinchu 30013, Taiwan. [Chen, Huei-Ru Vivien] Natl Tsing Hua Univ, Dept Phys, 101,Sec 2,Kuang Fu Rd, Hsinchu 30013, Taiwan. [Chen, Huei-Ru Vivien; Liu, Sheng-Yuan; Su, Yu-Nung] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. [Keto, Eric; Zhang, Qizhou; Sridharan, T. K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02318 USA. RP Chen, HRV (reprint author), Natl Tsing Hua Univ, Inst Astron, 101,Sec 2,Kuang Fu Rd, Hsinchu 30013, Taiwan.; Chen, HRV (reprint author), Natl Tsing Hua Univ, Dept Phys, 101,Sec 2,Kuang Fu Rd, Hsinchu 30013, Taiwan.; Chen, HRV (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM hchen@phys.nthu.edu.tw OI Chen, Huei-Ru/0000-0002-9774-1846; Zhang, Qizhou/0000-0003-2384-6589; Liu, Sheng-Yuan/0000-0003-4603-7119 FU Taiwan Ministry of Science and Technology [MOST 103-2119-M-007-006-MY3] FX This work is supported by the Taiwan Ministry of Science and Technology, project MOST 103-2119-M-007-006-MY3. NR 50 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2016 VL 823 IS 2 AR 125 DI 10.3847/0004-637X/823/2/125 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN9OV UT WOS:000377410000056 ER PT J AU Choi, J Dotter, A Conroy, C Cantiello, M Paxton, B Johnson, BD AF Choi, Jieun Dotter, Aaron Conroy, Charlie Cantiello, Matteo Paxton, Bill Johnson, Benjamin D. TI MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: evolution; stars: general; stars: interiors ID ASYMPTOTIC GIANT BRANCH; LOW-MASS STARS; PRE-MAIN-SEQUENCE; LARGE-MAGELLANIC-CLOUD; ANGULAR-MOMENTUM TRANSPORT; M-CIRCLE-DOT; B-TYPE STARS; GAMMA-RAY BURSTS; METAL-POOR STARS; HERTZSPRUNG-RUSSELL DIAGRAM AB This is the first of a series of papers presenting the Modules for Experiments in Stellar Astrophysics (MESA) Isochrones and Stellar Tracks (MIST) project, a new comprehensive set of stellar evolutionary tracks and isochrones computed using MESA, a state-of-the-art open-source 1D stellar evolution package. In this work, we present models with solar-scaled abundance ratios covering a wide range of ages (5 <= log(Age)[year] <= 10.3), masses (0.1 <= M/M-circle dot <= 300), and metallicities (-2.0 <= [Z/H] <= 0.5). The models are self-consistently and continuously evolved from the pre-main sequence (PMS) to the end of hydrogen burning, the white dwarf cooling sequence, or the end of carbon burning, depending on the initial mass. We also provide a grid of models evolved from the PMS to the end of core helium burning for -4.0 <= [Z/H] < -2.0. We showcase extensive comparisons with observational constraints as well as with some of the most widely used existing models in the literature. The evolutionary tracks and isochrones can be downloaded from the project website at http://waps.cfa.harvard.edu/MIST/. C1 [Choi, Jieun; Conroy, Charlie; Johnson, Benjamin D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Dotter, Aaron] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Cantiello, Matteo; Paxton, Bill] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. RP Choi, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Science Foundation [NSF PHY11-25915]; National Science Foundation; Australian Research Council [FL110100012]; NASA [NNX13AI46G, NNX15AK14G]; NSF [AST-1313280]; Packard Foundation FX We thank the referee for his/her constructive comments. We thank Martha Boyer, Jason Kalirai, and Guillermo Torres for generously sharing their data with us and Francis Timmes for his assistance with nuclear reaction networks in MESA. We thank Leo Girardi and Dan Weisz for fruitful conversations and comments on the manuscript. We thank Conny Aerts, Lars Bildsten, Jonathan Bird, Phillip Cargile, Selma de Mink, Falk Herwig, Jessica Lu, Marc Pinsonneault, Philip Rosenfield, and Victor Silva-Aguirre for sharing their expertise. We also thank the entire MESA community for making this work possible, with special thanks to the MESA Council. Finally, we thank the participants of the KITP workshop "Galactic Archaeology and Precision Stellar Astrophysics" for stimulating discussions. This research was supported in part by the National Science Foundation under Grant No. NSF PHY11-25915. J.C. acknowledges support from the National Science Foundation Graduate Research Fellowship Program. A.D. received support from the Australian Research Council under grant FL110100012. C.C. acknowledges support from NASA grant NNX13AI46G, NSF grant AST-1313280, and the Packard Foundation. This work was supported in part by NASA grant NNX15AK14G. The computations in this paper were run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University. NR 460 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 JUN 1 PY 2016 VL 823 IS 2 AR 102 DI 10.3847/0004-637X/823/2/102 PG 48 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN9OV UT WOS:000377410000033 ER PT J AU Dai, F Winn, JN Albrecht, S Arriagada, P Bieryla, A Butler, RP Crane, JD Hirano, T Johnson, JA Kiilerich, A Latham, DW Narita, N Nowak, G Palle, E Ribas, I Rogers, LA Sanchis-Ojeda, R Shectman, SA Teske, JK Thompson, IB Van Eylen, V Vanderburg, A Wittenmyer, RA Yu, L AF Dai, Fei Winn, Joshua N. Albrecht, Simon Arriagada, Pamela Bieryla, Allyson Butler, R. Paul Crane, Jeffrey D. Hirano, Teriyaki Johnson, John Asher Kiilerich, Amanda Latham, David W. Narita, Norio Nowak, Grzegorz Palle, Enric Ribas, Ignasi Rogers, Leslie A. Sanchis-Ojeda, Roberto Shectman, Stephen A. Teske, Johanna K. Thompson, Ian B. Van Eylen, Vincent Vanderburg, Andrew Wittenmyer, Robert A. Yu, Liang TI DOPPLER MONITORING OF FIVE K2 TRANSITING PLANETARY SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: composition; techniques: radial velocities ID LOW-DENSITY PLANETS; SOLAR-TYPE STARS; TIMING VARIATIONS; ROCKY PLANET; SUPER-EARTHS; KEPLER; MASS; CANDIDATES; SEARCH; EXOPLANETS AB In an effort to measure the masses of planets discovered by the NASA K2 mission, we have conducted precise Doppler observations of five stars with transiting planets. We present the results of a joint analysis of these new data and previously published Doppler data. The first star, an M dwarf known as K2-3 or EPIC 201367065, has three transiting planets ("b," with radius 2.1 R-circle plus; "c," 1.7 R-circle plus; and "d," 1.5 R-circle plus). Our analysis leads to the mass constraints: M-b = 8.1(-1.9)(+2.0) M-circle plus and M-c < 4.2 M-circle plus (95% confidence). The mass of planet d is poorly constrained because its orbital period is close to the stellar rotation period, making it difficult to disentangle the planetary signal from spurious Doppler shifts due to stellar activity. The second star, a G dwarf known as K2-19 or EPIC 201505350, has two planets ("b," 7.7 R-circle plus; and "c," 4.9 R-circle plus) in a 3:2 mean-motion resonance, as well as a shorter-period planet ("d," 1.1 R-circle plus). We find M-b = 28.5(-5.0)(+5.4) M-circle plus, M-c = 25.6(-7.1)(+7.1) M-circle plus and M-d < 14.0 M-circle plus (95% conf.). The third star, a G dwarf known as K2-24 or EPIC 203771098, hosts two transiting planets ("b," 5.7 R-circle plus; and "c," 7.8 R-circle plus) with orbital periods in a nearly 2: 1 ratio. We find M-b = 19.8(-4.4)(+4.5) M-circle plus and M-c = 26.0(-6.1)(+5.8) M-circle plus. The fourth star, a G dwarf known as EPIC 204129699, hosts a hot Jupiter for which we measured the mass to be 1.857(-0.081)(+0.081) M-Jup . The fifth star, a G dwarf known as EPIC 205071984, contains three transiting planets ("b," 5.4 R-circle plus; "c," 3.5 R-circle plus; and "d," 3.8 R-circle plus), the outer two of which have a nearly 2: 1 period ratio. We find M-b = 21.1(-5.9)(+5.9) M-circle plus, M-c < 8.1 M-circle plus (95% conf.) and M-d < 35 M-circle plus (95% conf.). C1 [Dai, Fei; Winn, Joshua N.; Van Eylen, Vincent; Yu, Liang] MIT, Dept Phys, Cambridge, MA 02139 USA. [Dai, Fei; Winn, Joshua N.; Van Eylen, Vincent; Yu, Liang] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Albrecht, Simon; Kiilerich, Amanda; Van Eylen, Vincent] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Arriagada, Pamela; Bieryla, Allyson] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Butler, R. Paul; Johnson, John Asher; Latham, David W.; Teske, Johanna K.; Vanderburg, Andrew] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. [Crane, Jeffrey D.; Shectman, Stephen A.; Teske, Johanna K.; Thompson, Ian B.] Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Hirano, Teriyaki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan. [Narita, Norio] Natl Inst Nat Sci, Astrobiol Ctr, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Narita, Norio] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Narita, Norio] SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Nowak, Grzegorz; Palle, Enric] IAC, E-38205 Tenerife, Spain. [Nowak, Grzegorz; Palle, Enric] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Ribas, Ignasi] CSIC, IEEC, Inst Ciencies Espai, Campus UAB, E-08193 Bellaterra, Spain. [Rogers, Leslie A.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Sanchis-Ojeda, Roberto] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Wittenmyer, Robert A.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Wittenmyer, Robert A.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Wittenmyer, Robert A.] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. RP Dai, F (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.; Dai, F (reprint author), MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. EM fd284@mit.edu RI Nowak, Grzegorz/H-8234-2014; Butler, Robert/B-1125-2009; OI Nowak, Grzegorz/0000-0002-7031-7754; /0000-0002-8958-0683 FU Transiting Exoplanet Survey Satellite mission; NAOJ Fellowship; Inoue Science Research Award; JSPS KAKENHI [25247026]; California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) - NASA; National Science Foundation [DGE 1144152] FX We thank Kento Masuda for helpful discussions. We thank Saul Rappaport and Tushar Shrotriya for their contributions to the HARPS observing proposal. We are grateful to Xavier Bonfils, Nicola Astudillo, and collaborators, with whom we exchanged observing time at ESO's 3.6 m telescope, facilitating our observations. We thank Jason Eastman, Emmanuel Jehin, and Michal Gillon for scheduling ground-based transit observations with LCOGT and TRAPPIST. Work by F.D. and J.N.W. was supported by the Transiting Exoplanet Survey Satellite mission. N.N. acknowledges supports by the NAOJ Fellowship, Inoue Science Research Award, and Grant-in-Aid for Scientific Research (A) (JSPS KAKENHI Grant Number 25247026). This work was performed (in part) under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. A.V. is supported by the National Science Foundation Graduate Research Fellowship, Grant No. DGE 1144152. Australian access to the Magellan Telescopes was supported by the Australian Federal Government through the Department of Industry and Science. NR 70 TC 5 Z9 5 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 JUN 1 PY 2016 VL 823 IS 2 AR 115 DI 10.3847/0004-637X/823/2/115 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN9OV UT WOS:000377410000046 ER PT J AU Dunham, MM Offner, SSR Pineda, JE Bourke, TL Tobin, JJ Arce, HG Chen, XP Di Francesco, J Johnstone, D Lee, KI Myers, PC Price, D Sadavoy, SI Schnee, S AF Dunham, Michael M. Offner, Stella S. R. Pineda, Jaime E. Bourke, Tyler L. Tobin, John J. Arce, Hector G. Chen, Xuepeng Di Francesco, James Johnstone, Doug Lee, Katherine I. Myers, Philip C. Price, Daniel Sadavoy, Sarah I. Schnee, Scott TI AN ALMA SEARCH FOR SUBSTRUCTURE, FRAGMENTATION, AND HIDDEN PROTOSTARS IN STARLESS CORES IN CHAMAELEON I SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; stars: formation; stars: low-mass; submillimeter: ISM ID 1ST HYDROSTATIC CORE; ADAPTIVE MESH REFINEMENT; C2D LEGACY CLOUDS; GOULD BELT SURVEY; SELF-GRAVITATIONAL HYDRODYNAMICS; 2-DIMENSIONAL RADIATIVE-TRANSFER; PERSEUS MOLECULAR CLOUD; DUST CONTINUUM EMISSION; SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS AB We present an Atacama Large Millimeter/submillimeter Array (ALMA) 106 GHz (Band 3) continuum survey of the complete population of dense cores in the Chamaeleon I molecular cloud. We detect a total of 24 continuum sources in 19 different target fields. All previously known Class 0 and Class I protostars in Chamaeleon I are detected, whereas all of the 56 starless cores in our sample are undetected. We show that the Spitzer+Herschel census of protostars in Chamaeleon I is complete, with the rate at which protostellar cores have been misclassified as starless cores calculated as <1/56, or <2%. We use synthetic observations to show that starless cores collapsing following the turbulent fragmentation scenario are detectable by our ALMA observations when their central densities exceed similar to 10(8) cm(-3), with the exact density dependent on the viewing geometry. Bonnor-Ebert spheres, on the other hand, remain undetected to central densities at least as high as 10(10) cm(-3). Our starless core non-detections are used to infer that either the star-formation rate is declining in Chamaeleon I and most of the starless cores are not collapsing, matching the findings of previous studies, or that the evolution of starless cores are more accurately described by models that develop less substructure than predicted by the turbulent fragmentation scenario, such as Bonnor-Ebert spheres. We outline future work necessary to distinguish between these two possibilities. C1 [Dunham, Michael M.; Lee, Katherine I.; Myers, Philip C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. [Offner, Stella S. R.] Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA. [Pineda, Jaime E.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Bourke, Tyler L.] SKA Org Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. [Tobin, John J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Arce, Hector G.] Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. [Chen, Xuepeng] Chinese Acad Sci, Purple Mt Observ, 2 West Beijing Rd, Nanjing 210008, Jiangsu, Peoples R China. [Di Francesco, James; Johnstone, Doug] Natl Res Council Canada, Herzberg Astron Program, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. [Di Francesco, James; Johnstone, Doug] Natl Res Council Canada, Herzberg Astrophys Program, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. [Johnstone, Doug] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Price, Daniel] Monash Univ, Monash Ctr Astrophys MoCA, Clayton, Vic 3800, Australia. [Price, Daniel] Monash Univ, Sch Math Sci, Clayton, Vic 3800, Australia. [Sadavoy, Sarah I.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Schnee, Scott] 1Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. RP Dunham, MM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM mdunham@cfa.harvard.edu OI Pineda, Jaime/0000-0002-3972-1978; Price, Daniel/0000-0002-4716-4235 FU National Aeronautics and Space Administration; National Science Foundation; Submillimeter Array (SMA) through an SMA postdoctoral fellowship; NASA [NNX13AE54G]; NSFC [11473069] FX We thank the referee for a set of helpful comments that have improved the quality of this publication. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO.ALMA# 2012.1.00031.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. This research made use of data from the Herschel Gould Belt survey (HGBS) project (http://gouldbelt-herschel.cea.fr). The HGBS is a Herschel Key Program jointly carried out by SPIRE Specialist Astronomy Group 3 (SAG 3), scientists of several institutes in the PACS Consortium (CEA Saclay, INAF-IFSI Rome and INAF-Arcetri, KU Leuven, MPIA Heidelberg), and scientists of the Herschel Science Center (HSC). 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 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 also made use of NASA's Astrophysics Data System (ADS) Abstract Service, the IDL Astronomy Library hosted by the NASA Goddard Space Flight Center, and the SIMBAD database operated at CDS, Strasbourg, France. MMD acknowledges support from the Submillimeter Array (SMA) through an SMA postdoctoral fellowship, and from NASA through grant NNX13AE54G. XC acknowledges support by the NSFC through grant 11473069. NR 113 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 JUN 1 PY 2016 VL 823 IS 2 AR 160 DI 10.3847/0004-637X/823/2/160 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN9OV UT WOS:000377410000091 ER PT J AU Kohn, SA Aguirre, JE Nunhokee, CD Bernardi, G Pober, JC Ali, ZS Bradley, RF Carilli, CL DeBoer, DR Gugliucci, NE Jacobs, DC Klima, P MacMahon, DHE Manley, JR Moore, DF Parsons, AR Stefan, II Walbrugh, WP AF Kohn, S. A. Aguirre, J. E. Nunhokee, C. D. Bernardi, G. Pober, J. C. Ali, Z. S. Bradley, R. F. Carilli, C. L. DeBoer, D. R. Gugliucci, N. E. Jacobs, D. C. Klima, P. MacMahon, D. H. E. Manley, J. R. Moore, D. F. Parsons, A. R. Stefan, I. I. Walbrugh, W. P. TI CONSTRAINING POLARIZED FOREGROUNDS FOR EoR EXPERIMENTS. I. 2D POWER SPECTRA FROM THE PAPER-32 IMAGING ARRAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dark ages, reionization, first stars; polarization; techniques: interferometric ID 21 CM EPOCH; UNDERSTANDING RADIO POLARIMETRY; LOW-FREQUENCY ARRAY; REIONIZATION WINDOWS; LOFAR OBSERVATIONS; NEXT-GENERATION; BASE-LINE; 150 MHZ; 3C 196; FIELD AB Current generation low-frequency interferometers constructed with the objective of detecting the high-redshift 21 cm background aim to generate power spectra of the brightness temperature contrast of neutral hydrogen in primordial intergalactic medium. Two-dimensional (2D) power spectra (power in Fourier modes parallel and perpendicular to the line of sight) that formed from interferometric visibilities have been shown to delineate a boundary between spectrally smooth foregrounds (known as the wedge) and spectrally structured 21 cm background emission (the EoR window). However, polarized foregrounds are known to possess spectral structure due to Faraday rotation, which can leak into the EoR window. In this work we create and analyze 2D power spectra from the PAPER-32 imaging array in Stokes I, Q, U, and V. These allow us to observe and diagnose systematic effects in our calibration at high signal-to-noise within the Fourier space most relevant to EoR experiments. We observe well-defined windows in the Stokes visibilities, with Stokes Q, U, and V power spectra sharing a similar wedge shape to that seen in Stokes I. With modest polarization calibration, we see no evidence that polarization calibration errors move power outside the wedge in any Stokes visibility to the noise levels attained. Deeper integrations will be required to confirm that this behavior persists to the depth required for EoR detection. C1 [Kohn, S. A.; Aguirre, J. E.; Moore, D. F.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Nunhokee, C. D.; Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Manley, J. R.; Walbrugh, W. P.] SKA South Africa, Pinelands, South Africa. [Bernardi, G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Pober, J. C.] Brown Univ, Dept Phys, Providence, RI 02912 USA. [Ali, Z. S.; DeBoer, D. R.; Parsons, A. R.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Bradley, R. F.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA USA. [Bradley, R. F.; Klima, P.] Natl Radio Astron Observ, Charlottesville, VA USA. [Bradley, R. F.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Carilli, C. L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Carilli, C. L.; Stefan, I. I.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Gugliucci, N. E.] St Anselm Coll, Manchester, NH USA. [Jacobs, D. C.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [MacMahon, D. H. E.; Parsons, A. R.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. RP Kohn, SA (reprint author), Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. EM saulkohn@sas.upenn.edu OI Pober, Jonathan/0000-0002-3492-0433; Kohn, Saul/0000-0001-6744-5328 FU NSF AST program [0804508, 1129258, 1125558]; Mount Cuba Astronomical Association; National Research Foundation [92725]; South African SKA Project (SKA SA); SKA SA scholarship program; University of California Office of the President Multicampus Research Programs and Initiatives [MR-15-328388]; NSF CAREER award [1352519]; NSF AST grant [1129258, 1440343] FX We thank SKA SA for their efforts in ensuring the smooth running of PAPER. PAPER is supported through the NSF AST program (awards 0804508, 1129258, and 1125558), the Mount Cuba Astronomical Association, and by significant efforts by the staff at NRAO. This work is based on research supported by the National Research Foundation under grant 92725. Any opinion, finding, and conclusion or recommendation expressed in this material is that of the author(s) and the NRF does not accept any liability in this regard. The financial assistance of the South African SKA Project (SKA SA) toward this research is hereby acknowledged. Opinions expressed and conclusions arrived at are those of the authors and are not necessarily to be attributed to the SKA SA. C.D.N. is supported by the SKA SA scholarship program. A.R.P. acknowledges support from the University of California Office of the President Multicampus Research Programs and Initiatives through award MR-15-328388, as well as from NSF CAREER award No. 1352519, NSF AST grant No. 1129258, and NSF AST grant No. 1440343. NR 50 TC 4 Z9 4 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 JUN 1 PY 2016 VL 823 IS 2 AR 88 DI 10.3847/0004-637X/823/2/88 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN9OV UT WOS:000377410000019 ER PT J AU MacGregor, MA Wilner, DJ Chandler, C Ricci, L Maddison, ST Cranmer, SR Andrews, SM Hughes, AM Steele, A AF MacGregor, Meredith A. Wilner, David J. Chandler, Claire Ricci, Luca Maddison, Sarah T. Cranmer, Steven R. Andrews, Sean M. Hughes, A. Meredith Steele, Amy TI CONSTRAINTS ON PLANETESIMAL COLLISION MODELS IN DEBRIS DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planets and satellites: formation; stars: individual (AU Mic); submillimeter: planetary systems ID MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; AU-MICROSCOPII; CIRCUMSTELLAR DISK; BETA-PICTORIS; HERSCHEL OBSERVATIONS; PROTOPLANETARY DISKS; SIZE DISTRIBUTIONS; ALMA OBSERVATIONS; GRAIN-GROWTH AB Observations of debris disks offer a window into the physical and dynamical properties of planetesimals in extrasolar systems through the size distribution of dust grains. In particular, the millimeter spectral index of thermal dust emission encodes information on the grain size distribution. We have made new VLA observations of a sample of seven nearby debris disks at 9 mm, with 3 '' resolution and similar to 5 mu Jy beam(-1)rms. We combine these with archival ATCA observations of eight additional debris disks observed at 7 mm, together with up-to-date observations of all disks at (sub) millimeter wavelengths from the literature, to place tight constraints on the millimeter spectral indices and thus grain size distributions. The analysis gives a weighted mean for the slope of the power-law grain size distribution, n(alpha) proportional to alpha(-q), of < q > = 3.36 +/- 0.02, with a possible trend of decreasing q for later spectral type stars. We compare our results to a range of theoretical models of collisional cascades, from the standard self-similar, steady-state size distribution (q = 3.5) to solutions that incorporate more realistic physics such as alternative velocity distributions and material strengths, the possibility of a cutoff at small dust sizes from radiation pressure, and results from detailed dynamical calculations of specific disks. Such effects can lead to size distributions consistent with the data, and plausibly the observed scatter in spectral indices. For the AU Mic system, the VLA observations show clear evidence of a highly variable stellar emission component; this stellar activity obviates the need to invoke the presence of an asteroid belt to explain the previously reported compact millimeter source in this system. C1 [MacGregor, Meredith A.; Wilner, David J.; Ricci, Luca; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Chandler, Claire] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Maddison, Sarah T.] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Cranmer, Steven R.] Univ Colorado, Dept Astrophys & Planetary Sci, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Hughes, A. Meredith] Wesleyan Univ, Van Vleck Observ, Dept Astron, Middletown, CT 06459 USA. [Steele, Amy] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP MacGregor, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI MacGregor, Meredith/0000-0001-7891-8143 FU National Science Foundation Graduate Research Fellowship [DGE1144152]; Australian Government FX M.A.M. acknowledges support from a National Science Foundation Graduate Research Fellowship (DGE1144152). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Australia Telescope Compact Array is part of the Australia Telescope National Facility, which is funded by the Australian Government for operation as a National Facility managed by CSIRO. We thank Margaret Pan, Hilke Schlichting, and Scott Kenyon for helpful conversations. We thank Meredith Hughes, Kate Su, David Rodriguez, Sebastian Marino, Aaron Boley, and Jacob White for providing data prior to publication. We also thank the anonymous referee for a careful and thoughtful review. NR 114 TC 3 Z9 3 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 JUN 1 PY 2016 VL 823 IS 2 AR 79 DI 10.3847/0004-637X/823/2/79 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN9OV UT WOS:000377410000010 ER PT J AU Paggi, A Fabbiano, G Civano, F Pellegrini, S Elvis, M Kim, DW AF Paggi, Alessandro Fabbiano, Giuseppina Civano, Francesca Pellegrini, Silvia Elvis, Martin Kim, Dong-Woo TI HIDDEN ACTIVE GALACTIC NUCLEI IN EARLY-TYPE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; surveys; X-rays: galaxies ID X-RAY BINARIES; STAR-FORMING GALAXIES; MASSIVE BLACK-HOLES; ELLIPTIC GALAXIES; HOT GAS; SCALING RELATIONS; STELLAR MASS; LUMINOSITY FUNCTION; HOST GALAXIES; COSMOS SURVEY AB We present a stacking analysis of the complete sample of early-type galaxies (ETGs) in the Chandra COSMOS (C-COSMOS) survey, to explore the nature of the X-ray luminosity in the redshift and stellar luminosity ranges 0 < z < 1.5 and 10(9) < L-K/L-circle dot < 10(13). Using established scaling relations, we subtract the contribution of X-ray binary populations to estimate the combined emission of hot ISM and active galactic nuclei (AGNs). To discriminate between the relative importance of these two components, we (1) compare our results with the relation observed in the local universe L-X,L-gas proportional to L-K(4.5) for hot gaseous halos emission in ETGs, and (2) evaluate the spectral signature of each stacked bin. We find two regimes where the non-stellar X-ray emission is hard, consistent with AGN emission. First, there is evidence of hard, absorbed X-ray emission in stacked bins including relatively high z (similar to 1.2) ETGs with average high X-ray luminosity (LX-LMXB greater than or similar to 6 x 10(42) ergs s(-1)). These luminosities are consistent with the presence of highly absorbed "hidden" AGNs in these ETGs, which are not visible in their optical-IR spectra and spectral energy distributions. Second, confirming the early indication from our C-COSMOS study of X-ray detected ETGs, we find significantly enhanced X-ray luminosity in lower stellar mass ETGs (L-K less than or similar to 10(11) L-circle dot), relative to the local L-X,L-gas proportional to L-K(4.5) relation. The stacked spectra of these ETGs also suggest X-ray emission harder than expected from gaseous hot halos. This emission is consistent with inefficient accretion 10(-5) - 10(-4) (M) over dot(Edd) onto M-BH similar to 10(6) - 10(8) M-circle dot. C1 [Paggi, Alessandro; Fabbiano, Giuseppina; Civano, Francesca; Elvis, Martin; Kim, Dong-Woo] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Civano, Francesca] Yale Univ, Dept Phys, POB 208121, New Haven, CT 06520 USA. [Civano, Francesca] Yale Univ, Yale Ctr Astron & Astrophys, POB 208121, New Haven, CT 06520 USA. [Pellegrini, Silvia] Univ Bologna, Dept Astron, Via Ranzani 1, I-40127 Bologna, Italy. RP Paggi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM apaggi@cfa.harvard.edu RI Paggi, Alessandro/C-1219-2017; OI Paggi, Alessandro/0000-0002-5646-2410; Fabbiano, Giuseppina/0000-0002-3554-3318; Elvis, Martin/0000-0001-5060-1398 FU NASA [NAS8-03060, 11-ADAP11-0218]; NASA Chandra grant [G01-12110X]; MIUR [2010LY5N2T]; NSF [1066293]; European Organisation for Astronomical Research in the Southern Hemisphere, Chile [179.A-2005] FX This work was partially supported by NASA contract NAS8-03060 (CXC), and NASA Chandra grant G01-12110X. S.P. acknowledges financial support from MIUR grant PRIN 2010-2011, project "The Chemical and Dynamical Evolution of the Milky Way and Local Group Galaxies," prot. 2010LY5N2T. F.C. acknowledges financial support by the NASA contract 11-ADAP11-0218. A.P. thanks Andy Goulding for useful discussion and suggestions. M.E. and G.F. thank the Aspen Center for Physics and the NSF Grant #1066293 for hospitality during the completion of this paper. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa. This research is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, program 179.A-2005 (Ultra-VISTA survey). NR 67 TC 2 Z9 2 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 JUN 1 PY 2016 VL 823 IS 2 AR 112 DI 10.3847/0004-637X/823/2/112 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN9OV UT WOS:000377410000043 ER PT J AU Randall, SW Clarke, TE van Weeren, RJ Intema, HT Dawson, WA Mroczkowski, T Blanton, EL Bulbul, E Giacintucci, S AF Randall, S. W. Clarke, T. E. van Weeren, R. J. Intema, H. T. Dawson, W. A. Mroczkowski, T. Blanton, E. L. Bulbul, E. Giacintucci, S. TI MULTI-WAVELENGTH OBSERVATIONS OF THE DISSOCIATIVE MERGER IN THE GALAXY CLUSTER CIZA J0107.7+5408 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: clusters: general; galaxies: clusters: individual (CIZA J0107.7+5408); galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID X-RAY SPECTROSCOPY; INTERACTION CROSS-SECTION; DIFFUSE RADIO-EMISSION; DARK-MATTER; SHOCK-WAVES; CHANDRA OBSERVATIONS; COMA CLUSTER; DATA RELEASE; MILKY-WAY; ACCELERATION AB We present results based on X-ray, optical, and radio observations of the massive galaxy cluster CIZA J0107.7+5408. We find that this system is a post-core-passage, dissociative, binary merger, with the optical galaxy density peaks of each subcluster leading their associated X-ray emission peaks. This separation occurs because the diffuse gas experiences ram pressure forces, while the effectively collisionless galaxies (and presumably their associated dark matter (DM) halos) do not. This system contains double-peaked diffuse radio emission,. possibly a double radio relic with the relics lying along the merger axis and also leading the X-ray cores. We find evidence for a temperature peak associated with the SW relic, likely created by the same merger shock that is powering the relic radio emission in this region. Thus, this system is a relatively rare, clean example of a dissociative binary merger, which can in principle be used to place constraints on the self-interaction cross-section of DM. Low-frequency radio observations reveal ultra-steep spectrum diffuse radio emission that is not correlated with the X-ray, optical, or high-frequency radio emission. We suggest that these sources are radio phoenixes, which are preexisting nonthermal particle populations that have been re-energized through adiabatic compression by the same merger shocks that power the radio relics. Finally, we place upper limits on inverse Compton emission from the SW radio relic. C1 [Randall, S. W.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Clarke, T. E.] Naval Res Lab, 4555 Overlook Ave SW,Code 7213, Washington, DC 20375 USA. [Intema, H. T.] Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA. [Dawson, W. A.] Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA. [Mroczkowski, T.] US Naval Res Lab, 4555 Overlook Ave SW, Washington, DC 20375 USA. [Blanton, E. L.] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. [Blanton, E. L.] Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA. [Bulbul, E.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Giacintucci, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Randall, SW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM srandall@cfa.harvard.edu RI Intema, Huib/D-1438-2012; OI Intema, Huib/0000-0002-5880-2730; Mroczkowski, Tony/0000-0003-3816-5372; van Weeren, Reinout/0000-0002-0587-1660 FU Chandra X-ray Center through NASA [NAS8-03060]; Smithsonian Institution; Chandra X-ray Observatory grant [GO3-14134X] FX Support for this work was partially provided by the Chandra X-ray Center through NASA contract NAS8-03060, the Smithsonian Institution, and by the Chandra X-ray Observatory grant GO3-14134X. Basic research in radio astronomy at the Naval Research Laboratory is supported by 6.1 Base funding. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We thank the staff of the GMRT who have made these GMRT observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank Dale Kocevski for providing spectroscopic redshifts for the BCGs and Paul Nulsen for useful discussions. NR 67 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 JUN 1 PY 2016 VL 823 IS 2 AR 94 DI 10.3847/0004-637X/823/2/94 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN9OV UT WOS:000377410000025 ER PT J AU Reid, MJ Dame, TM Menten, KM Brunthaler, A AF Reid, M. J. Dame, T. M. Menten, K. M. Brunthaler, A. TI A PARALLAX-BASED DISTANCE ESTIMATOR FOR SPIRAL ARM SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: structure; parallaxes; stars: formation ID STAR-FORMING REGIONS; TRIGONOMETRIC PARALLAXES; MILKY-WAY; FUNDAMENTAL PARAMETERS; GALAXIES; CATALOG AB The spiral arms of the Milky Way are being accurately located for the first time via trigonometric parallaxes of massive star-forming regions with the Bar and Spiral Structure Legacy Survey, using the Very Long Baseline Array and the European VLBI Network, and with the Japanese VLBI Exploration of Radio Astrometry project. Here we describe a computer program that leverages these results to significantly improve the accuracy and reliability of distance estimates to other sources that are known to follow spiral structure. Using a Bayesian approach, sources are assigned to arms based on their (l, b, v) coordinates with respect to arm signatures seen in CO and H I surveys. A source's kinematic distance, displacement from the plane, and proximity to individual parallax sources are also considered in generating a full distance probability density function. Using this program to estimate distances to large numbers of star-forming regions, we generate a realistic visualization of the Milky Way's spiral structure as seen from the northern hemisphere. C1 [Reid, M. J.; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Menten, K. M.; Brunthaler, A.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU ERC Advanced Investigator Grant GLOSTAR [247078] FX This work was partially funded by the ERC Advanced Investigator Grant GLOSTAR (247078). NR 26 TC 8 Z9 8 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 JUN 1 PY 2016 VL 823 IS 2 AR 77 DI 10.3847/0004-637X/823/2/77 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN9OV UT WOS:000377410000008 ER PT J AU Schlegel, EM Jones, C Machacek, M Vega, LD AF Schlegel, E. M. Jones, C. Machacek, M. Vega, L. D. TI NGC 5195 IN M51: FEEDBACK "BURPS" AFTER A MASSIVE MEAL? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: individual: (NGC 5195, M51); X-rays: galaxies ID SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; DIFFUSE IONIZED-GAS; CHANDRA OBSERVATIONS; ELLIPTIC GALAXY; SCALING RELATIONS; SPIRAL GALAXIES; HOST GALAXY; OUTFLOWS; NGC-5195 AB We describe a double-arc-like X-ray structure lying similar to 15 ''-30 '' (similar to 0.8-1.7 kpc) south of the NGC 5195 nucleus, visible in the merged exposures of long Chandra pointings of M51. The curvature and orientation of the arcs argues for a nuclear origin. The arcs are radially separated by similar to 15 '' (similar to 1 kpc), but are rotated relative to each other by similar to 30 degrees. From an archival image, we find a slender H alpha-emitting region just outside the outer edge of the outer X-ray arc, suggesting that the X-ray-emitting gas plowed up and displaced the H alpha-emitting material from the galaxy core. Star formation may have commenced in that arc. H alpha emission is present at the inner arc, but appears more complex in structure. In contrast to an explosion expected to be azimuthally symmetric, the X-ray arcs suggest a focused outflow. We interpret the arcs as episodic outbursts from the central super-massive black hole (SMBH). We conclude that NGC 5195 represents the nearest galaxy exhibiting on-going, large-scale outflows of gas, in particular, two episodes of a focused outburst of the SMBH. The arcs represent a clear demonstration of feedback. C1 [Schlegel, E. M.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX 78249 USA. [Jones, C.; Machacek, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Vega, L. D.] Vanderbilt Univ, Bridge Program, Fisk Univ, 221 Kirkland Hall, Nashville, TN 37235 USA. RP Schlegel, EM (reprint author), Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX 78249 USA. EM eric.schlegel@utsa.edu FU Vaughan Family Endowment FX We thank the referee for comments that improved our paper. The research of E.M.S. was partially supported by the Vaughan Family Endowment. NR 44 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2016 VL 823 IS 2 AR 75 DI 10.3847/0004-637X/823/2/75 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN9OV UT WOS:000377410000006 ER PT J AU Schwarz, KR Bergin, EA Cleeves, LI Blake, GA Zhang, K Oberg, KI van Dishoeck, EF Qi, CH AF Schwarz, Kamber R. Bergin, Edwin A. Cleeves, L. Ilsedore Blake, Geoffrey A. Zhang, Ke Oberg, Karin I. van Dishoeck, Ewine F. Qi, Chunhua TI THE RADIAL DISTRIBUTION OF H-2 AND CO IN TW HYA AS REVEALED BY RESOLVED ALMA OBSERVATIONS OF CO ISOTOPOLOGUES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; circumstellar matter; ISM: abundances; molecular data; protoplanetary disks; radio lines: ISM ID MAIN-SEQUENCE STARS; PROTOPLANETARY DISKS; MOLECULAR CLOUDS; OUTER DISK; GAS; ICE; CHEMISTRY; ABUNDANCE; HYDRAE; LINES AB CO is widely used as a tracer of molecular gas. However, there is now mounting evidence that gas phase carbon is depleted in the disk around TW Hya. Previous efforts to quantify this depletion have been hampered by uncertainties regarding the radial thermal structure in the disk. Here we present resolved ALMA observations of (CO)-C-13 3-2, (CO)-O-18 3-2, (CO)-C-13 6-5, and (CO)-O-18 6-5 emission in TW Hya, which allow us to derive radial gas temperature and gas surface density profiles, as well as map the CO abundance as a function of radius. These observations provide a measurement of the surface CO snowline at similar to 30 AU and show evidence for an outer ring of CO emission centered at 53 AU, a feature previously seen only in less abundant species. Further, the derived CO gas temperature profile constrains the freeze out temperature of CO in the warm molecular layer to <21 K. Combined with the previous detection of HD 1-0, these data constrain the surface density of the warm H-2 gas in the inner similar to 30 AU such that Sigma(warm gas) = 4.7(-2.9)(+3.0) cm(-2)(R/10 au)(-1/2) . We find that CO is depleted by two orders of magnitude from R = 10-60 AU, with the small amount of CO returning to the gas phase inside the surface CO snowline insufficient to explain the overall depletion. Finally, this new data is used in conjunction with previous modeling of the TW Hya disk to constrain the midplane CO snowline to 17-23 AU. C1 [Schwarz, Kamber R.; Bergin, Edwin A.; Zhang, Ke] Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI USA. [Cleeves, L. Ilsedore; Oberg, Karin I.; Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, MC 150-21,1200 E Calif Blvd, Pasadena, CA 91125 USA. [van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. RP Schwarz, KR (reprint author), Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI USA. RI zhang, ke/A-3898-2009; OI zhang, ke/0000-0002-0661-7517; Cleeves, L. Ilsedore/0000-0003-2076-8001 FU national science foundation grant [AST-1514670, AST-1344133] FX This paper makes use of the following ALMA data: ADS/JAO.ALMA#2012.1.00422.s. ALMA is a partnership of ESO (representing its member states), NSF (U.S.) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The joint ALMA observatory is operated by ESO, AUI/NRAO, and NAOJ. This work was supported by funding from the national science foundation grant AST-1514670 and AST-1344133 (INSPIRE). NR 48 TC 13 Z9 13 U1 3 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2016 VL 823 IS 2 AR 91 DI 10.3847/0004-637X/823/2/91 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN9OV UT WOS:000377410000022 ER PT J AU Baker, JL Dunn, KA Mingrone, J Wood, BA Karpinski, BA Sherwood, CC Wildman, DE Maynard, TM Bielawski, JP AF Baker, Jennifer L. Dunn, Katherine A. Mingrone, Joseph Wood, Bernard A. Karpinski, Beverly A. Sherwood, Chet C. Wildman, Derek E. Maynard, Thomas M. Bielawski, Joseph P. TI Functional Divergence of the Nuclear Receptor NR2C1 as a Modulator of Pluripotentiality During Hominid Evolution SO GENETICS LA English DT Article DE ancestral gene reconstruction (AGR); codon models; hominid evolutionary survey; nuclear receptors; NR2C1; testicular receptor 2 (TR2); pluripotentiality ID EMBRYONIC STEM-CELLS; DETECTING POSITIVE SELECTION; CODON-SUBSTITUTION MODELS; WIDE ASSOCIATION SCAN; LIKELIHOOD RATIO TEST; PROTEIN-CODING GENES; TR2 ORPHAN RECEPTOR; AMINO-ACID SITES; MAXIMUM-LIKELIHOOD; PHOSPHOENOLPYRUVATE CARBOXYKINASE AB Genes encoding nuclear receptors (NRs) are attractive as candidates for investigating the evolution of gene regulation because they (1) have a direct effect on gene expression and (2) modulate many cellular processes that underlie development. We employed a three-phase investigation linking NR molecular evolution among primates with direct experimental assessment of NR function. Phase 1 was an analysis of NR domain evolution and the results were used to guide the design of phase 2, a codon-model-based survey for alterations of natural selection within the hominids. By using a series of reliability and robustness analyses we selected a single gene, NR2C1, as the best candidate for experimental assessment. We carried out assays to determine whether changes between the ancestral and extant NR2C1s could have impacted stem cell pluripotency (phase 3). We evaluated human, chimpanzee, and ancestral NR2C1 for transcriptional modulation of Oct4 and Nanog (key regulators of pluripotency and cell lineage commitment), promoter activity for Pepck (a proxy for differentiation in numerous cell types), and average size of embryological stem cell colonies (a proxy for the self-renewal capacity of pluripotent cells). Results supported the signal for alteration of natural selection identified in phase 2. We suggest that adaptive evolution of gene regulation has impacted several aspects of pluripotentiality within primates. Our study illustrates that the combination of targeted evolutionary surveys and experimental analysis is an effective strategy for investigating the evolution of gene regulation with respect to developmental phenotypes. C1 [Baker, Jennifer L.; Wood, Bernard A.; Sherwood, Chet C.] George Washington Univ, Ctr Adv Study Human Paleobiol, Washington, DC 20052 USA. [Baker, Jennifer L.; Sherwood, Chet C.; Maynard, Thomas M.] George Washington Univ, George Washington Inst Neurosci, Washington, DC 20052 USA. [Wood, Bernard A.] George Washington Univ, Dept Anat & Regenerat Biol, Washington, DC 20052 USA. [Maynard, Thomas M.] George Washington Univ, Dept Physiol & Pharmacol, Washington, DC 20052 USA. [Baker, Jennifer L.] NHGRI, Ctr Res Genom & Global Hlth, NIH, 12 South Dr, Bethesda, MD 20892 USA. [Dunn, Katherine A.; Bielawski, Joseph P.] Dalhousie Univ, Dept Biol, 1355 Oxford St, Halifax, NS B3H 4R2, Canada. [Mingrone, Joseph; Bielawski, Joseph P.] Dalhousie Univ, Dept Math & Stat, Halifax, NS B3H 4R2, Canada. [Wood, Bernard A.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Wildman, Derek E.] Univ Illinois, Dept Mol & Integrat Physiol, Champaign, IL 61801 USA. [Wildman, Derek E.] Univ Illinois, Inst Genom Biol, Champaign, IL 61801 USA. RP Baker, JL (reprint author), NHGRI, Ctr Res Genom & Global Hlth, NIH, 12 South Dr, Bethesda, MD 20892 USA.; Bielawski, JP (reprint author), Dalhousie Univ, Dept Biol, 1355 Oxford St, Halifax, NS B3H 4R2, Canada. EM JenniferLBaker7@gmail.com; J.Bielawski@dal.ca RI Maynard, Thomas/I-9039-2012; OI Maynard, Thomas/0000-0001-6976-3936; Baker, Jennifer/0000-0002-5192-2377 FU National Science Foundation (NSF) doctoral dissertation research improvement grant [BSC-1455625]; Wenner-Gren Foundation dissertation fieldwork grant [8735]; NSF Integrative Graduate Education and Research traineeship grant [DGE-0801634]; NSF-Human Origins Moving in New Directions (HOMINID) grant [BCS-0827546]; James S. McDonnell Foundation [220020293]; George Washington (GW) Office of the Vice President for Research; GW Institute of Neuroscience Biomarker Core Facility, National Institutes of Health grant [DC-001534]; Natural Sciences and Engineering Research Council of Canada [DG298394]; Centre for Comparative Genomics and Evolutionary Bioinformatics - Tula Foundation; Canadian Institutes of Health Research [CMF-108026] FX The work described here was supported by a National Science Foundation (NSF) doctoral dissertation research improvement grant (BSC-1455625), a Wenner-Gren Foundation dissertation fieldwork grant (8735), an NSF Integrative Graduate Education and Research traineeship grant (DGE-0801634), an NSF-Human Origins Moving in New Directions (HOMINID) grant (BCS-0827546), a grant from the James S. McDonnell Foundation (220020293), George Washington (GW) Office of the Vice President for Research and the GW School of Medicine for the GW Institute of Neuroscience Biomarker Core Facility, National Institutes of Health grant (DC-001534), Natural Sciences and Engineering Research Council of Canada (DG298394), Centre for Comparative Genomics and Evolutionary Bioinformatics (funded by the Tula Foundation), and Canadian Institutes of Health Research (CMF-108026). NR 121 TC 1 Z9 1 U1 1 U2 1 PU GENETICS SOCIETY AMERICA PI BETHESDA PA 9650 ROCKVILLE AVE, BETHESDA, MD 20814 USA SN 0016-6731 EI 1943-2631 J9 GENETICS JI Genetics PD JUN PY 2016 VL 203 IS 2 BP 905 EP + DI 10.1534/genetics.115.183889 PG 53 WC Genetics & Heredity SC Genetics & Heredity GA DO0IO UT WOS:000377462800025 PM 27075724 ER PT J AU Collin, R Roof, KE Spangler, A AF Collin, Rachel Erin Roof, Karah Spangler, Abby TI Hatching plasticity in the tropical gastropod Nerita scabricosta SO INVERTEBRATE BIOLOGY LA English DT Article DE Neritimorpha; phenotypic plasticity; bet-hedging; rocky intertidal; life history evolution ID TRADE-OFFS; EXTENDED INCUBATION; CALIFORNIA GRUNION; EMBRYONIC DIAPAUSE; SALAMANDER EGGS; ROCKY SHORE; TEMPERATURE; SNAILS; RISK; PREDATION AB Hatching plasticity has been documented in diverse terrestrial and freshwater taxa, but in few marine invertebrates. Anecdotal observations over the last 80years have suggested that intertidal neritid snails may produce encapsulated embryos able to significantly delay hatching. The cause for delays and the cues that trigger hatching are unknown, but temperature, salinity, and wave action have been suggested to play a role. We followed individual egg capsules of Nerita scabricosta in 16 tide pools to document the variation in natural time to hatching and to determine if large delays in hatching occur in the field. Hatching occurred after about 30d and varied significantly among tide pools in the field. Average time to hatching in each pool was not correlated with presence of potential predators, temperature, salinity, or pool size. We also compared hatching time between egg capsules in the field to those kept in the laboratory at a constant temperature in motionless water, and to those kept in the laboratory with sudden daily water motion and temperature changes. There was no significant difference in the hatching rate between the two laboratory treatments, but capsules took, on average, twice as long to hatch in the laboratory as in the field. Observations of developing embryos showed that embryos in the field develop slowly and continuously until hatching, but embryos in the laboratory reach the hatching stage during the first month of development and remain in stasis after that. Instances of hatching plasticity in benthic marine invertebrates, like the one in N. scabricosta, could greatly enhance our ability to investigate the costs and benefits of benthic versus planktonic development, a long-standing area of interest for invertebrate larval biologists. C1 [Collin, Rachel; Erin Roof, Karah; Spangler, Abby] Smithsonian Trop Res Inst, Balboa 084303092, Panama. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Balboa 084303092, Panama. EM collinr@si.edu OI Collin, Rachel/0000-0001-5103-4460 FU National Science Foundation [REU 1359299]; STRI FX We thank Autoridad de Recursos Acuaticos de Panama for issuing permits (No. 06, 2014; No. 75, 2015). We thank Isis Ochoa and Nerea Nieto for help maintaining animals in the laboratory and photographing and measuring embryos, and Louise Page for sharing her translation of Risbec (1932). KER was supported by a fellowship from the National Science Foundation grant "REU 1359299: Integrative Tropical Biology at the Smithsonian Tropical Research Institute in Panama," and AS was supported by an internship from STRI. NR 51 TC 0 Z9 0 U1 5 U2 13 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1077-8306 EI 1744-7410 J9 INVERTEBR BIOL JI Invertebr. Biol. PD JUN PY 2016 VL 135 IS 2 BP 87 EP 96 DI 10.1111/ivb.12119 PG 10 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA DN7QH UT WOS:000377271600002 ER PT J AU Scherer, AE Lunt, J Draper, AM Smee, DL AF Scherer, Avery E. Lunt, Jessica Draper, Alex M. Smee, Delbert L. TI Phenotypic plasticity in oysters (Crassostrea virginica) mediated by chemical signals from predators and injured prey SO INVERTEBRATE BIOLOGY LA English DT Article DE inducible defenses; predator-prey interactions; chemical ecology; blue crab; clam ID FRESH-WATER SNAIL; INDUCIBLE DEFENSES; NUCELLA-LAPILLUS; DIET CUES; CALLINECTES-SAPIDUS; PIMEPHALES-PROMELAS; POPULATION-DYNAMICS; RESOURCE-ALLOCATION; FATHEAD MINNOWS; LIFE-HISTORY AB Prey organisms reduce predation risk by altering their behavior, morphology, or life history. Avoiding or deterring predators often incurs costs, such as reductions in growth or fecundity. Prey minimize costs by limiting predator avoidance or deterrence to situations that pose significant risk of injury or death, requiring them to gather information regarding the relative threat potential predators pose. Chemical cues are often used for risk evaluation, and we investigated morphological responses of oysters (Crassostrea virginica) to chemical cues from injured conspecifics, from heterospecifics, and from predatory blue crabs (Callinectes sapidus) reared on different diets. Previous studies found newly settled oysters reacted to crab predators by growing heavier, stronger shells, but that adult oysters did not. We exposed oysters at two size classes (newly settled oyster spat and juveniles similar to 2.0cm) to predation risk cue treatments including predator or injured prey exudates and to seawater controls. Since both of the size classes tested can be eaten by blue crabs, we hypothesized that both would react to crab exudates by producing heavier, stronger shells. Oyster spat grew heavier shells that required significantly more force to break, an effective measure against predatory crabs, when exposed to chemical exudates from blue crabs as compared to controls. When exposed to chemical cues from injured conspecifics or from injured clams (Mercenaria mercenaria), a sympatric bivalve, shell mass and force were intermediate between predator treatments and controls, indicating that oysters react to injured prey cues but not as strongly as to cues released by predators. Juvenile oysters of similar to 2.0cm did not significantly alter their shell morphology in any of the treatments. Thus, newly settled oysters can differentiate between predatory threats and adjust their responses accordingly, with the strongest responses being to exudates released by predators, but oysters of 2.0cm and larger do not react morphologically to predatory threats. C1 [Scherer, Avery E.; Smee, Delbert L.] Texas A&M Univ Corpus Christi, Dept Life Sci, Corpus Christi, TX 78412 USA. [Lunt, Jessica] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Draper, Alex M.] Georgia Inst Technol, Sch Biol, Atlanta, GA 30332 USA. RP Scherer, AE (reprint author), Texas A&M Univ Corpus Christi, Dept Life Sci, Corpus Christi, TX 78412 USA. EM avery.scherer@tamucc.edu OI Scherer, Avery/0000-0001-8378-5517 FU NSF-MSP ETEAMS [1321319]; Ruth A. Campbell Professorship FX We thank the members of the Marine Ecology Lab at TAMU-CC for assisting with the experiments, and the Center for Coastal Studies for providing lab facilities. Funding for this work was provided by NSF-MSP ETEAMS grant #1321319 and the Ruth A. Campbell Professorship to D.L.S. NR 67 TC 2 Z9 2 U1 5 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1077-8306 EI 1744-7410 J9 INVERTEBR BIOL JI Invertebr. Biol. PD JUN PY 2016 VL 135 IS 2 BP 97 EP 107 DI 10.1111/ivb.12120 PG 11 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA DN7QH UT WOS:000377271600003 ER PT J AU Lim, SSL Yong, AYP Christy, JH AF Lim, Shirley S. L. Yong, Adeline Y. P. Christy, John H. TI Ontogenetic changes in diet and related morphological adaptations in Ocypode gaudichaudii SO INVERTEBRATE BIOLOGY LA English DT Article DE claw morphology; ontogeny; diet shift; niche breadth; ghost crab ID LIEMS PARADOX; INTRASPECIFIC VARIATION; CARCINUS-MAENAS; CLAW MORPHOLOGY; CICHLID FISHES; NATURAL DIET; CRABS; SIZE; GENERALIST; DELTA-C-13 AB There are conflicting reports as to whether Ocypode gaudichaudii individuals switch from carnivory as juveniles to deposit-feeding primarily on diatoms as adults, or whether they expand diet range and become omnivorous with maturity. At the onset of deposit-feeding, crabs develop specialized claws with truncated ends that they use to shovel sediment during foraging. Eighty-eight crabs were collected from Culebra Island (Republic of Panama) to study how the diet of this crab shifts with changes in claw shape, mouthpart proportions, and setation, as well as gastric mill width. Forty-four crabs had identifiable material in their foreguts: 30 had animal material, 12 had diatoms, and two had a mix of both. There were no differences between the gastric mill, mandibles, and the proximal endites of the first maxillipeds of predators and deposit-feeders, but extra rows of plumose setae were present on the second maxilliped of deposit-feeding crabs with carapace length (CL) >10.6mm. All individuals with CL <12.3mm and non-truncated claws ate animals, but those with larger CL and truncated claws had animal, diatom, or mixed diets; hence, claw truncation does not restrict the crab's diet to diatoms but, instead, broadens the diet to include both animals and diatoms. Perhaps this is a strategy to balance the economics of foraging on animals and diatoms on medium to low-energy beaches that lack the larger invertebrates that adults of other species of ghost crabs eat. More generally, our study shows that specialized feeding structures need not imply a narrow or specialist diet. C1 [Lim, Shirley S. L.; Yong, Adeline Y. P.] Nanyang Technol Univ, Nat Sci & Sci Educ, NIE, Ecol Lab, Singapore 637616, Singapore. [Christy, John H.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. RP Lim, SSL (reprint author), Nanyang Technol Univ, Nat Sci & Sci Educ, NIE, Ecol Lab, Singapore 637616, Singapore. EM shirley.lim@nie.edu.sg FU National Institute of Education, Nanyang Technological University [RI 8/10 SL] FX Thanks to the Smithsonian Tropical Research Institute (STRI) for logistical support, and to Authoridad de Recursos Acuaticos de Panama for access to the study site and research permits. This study was funded by a grant (RI 8/10 SL) from the National Institute of Education, Nanyang Technological University, to Shirley Lim. NR 35 TC 1 Z9 1 U1 6 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1077-8306 EI 1744-7410 J9 INVERTEBR BIOL JI Invertebr. Biol. PD JUN PY 2016 VL 135 IS 2 BP 117 EP 126 DI 10.1111/ivb.12122 PG 10 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA DN7QH UT WOS:000377271600005 ER PT J AU Phillips, TC Wildt, DE Comizzoli, P AF Phillips, Tameka C. Wildt, David E. Comizzoli, Pierre TI Incidence of methylated histones H3K4 and H3K79 in cat germinal vesicles is regulated by specific nuclear factors at the acquisition of developmental competence during the folliculogenesis SO JOURNAL OF ASSISTED REPRODUCTION AND GENETICS LA English DT Article DE Germinal vesicle; Histone methylation; Folliculogenesis; Oocyte competence; Domestic cat model ID DOMESTIC CAT; IN-VITRO; PREIMPLANTATION DEVELOPMENT; CHROMATIN CONFIGURATION; OOCYTE MATURATION; DNA METHYLATION; STAGE OOCYTES; MOUSE OOCYTES; MICE; FERTILIZATION AB This study aims to characterize the regulations of histone methylations, key epigenetic markers of oocyte competence, in germinal vesicle (GV) from different follicles (preantral, early, small, or large antral stage) using the domestic cat model. In Experiment 1, the incidence of H3K4me3 or H3K79me2 was determined in GVs from the diverse follicle stages directly or after exposure to (1) a methyltransferase inhibitor, (2) sonication to fracture the cytoplasmic membranes and wash away the cytoplasmic content, or (3) methyltransferase inhibitor followed by sonication. In Experiment 2, the presence and maintenance of nuclear methyltransferases SMYD3 and DOT1L (regulating H3K4me3 and H3K79me2, respectively) was characterized in separate GV stages before and after sonication. Functionality of GVs from the various follicle stages (with or without transient isolation from the cytoplasm) then was assessed in Experiment 3 by transfer into recipient competent oocytes. The incidence of histones H3K4me3 and H3K79me2 within the GV were influenced by the cytoplasmic environment at all stages except at the transition to the early antral stage where nuclear regulating factors appeared to be mainly involved. The methyltransferase SMYD3 and DOT1L also appeared tightly bound to the nucleus at that transition. Interestingly, oocytes reconstructed with a GV isolated from the cytoplasm for a prolonged period had the capacity to form an embryo after fertilization which proved that communication between the donor GV and the host cytoplasm (likely including the regulation of epigenetic factors) could be restored. Histone methylation apparently becomes regulated by specific nuclear factors at the acquisition of competence during the folliculogenesis and does not seem to be disrupted by prolonged isolation from the surrounding cytoplasm. C1 [Phillips, Tameka C.; Wildt, David E.; Comizzoli, Pierre] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA. [Phillips, Tameka C.; Wildt, David E.; Comizzoli, Pierre] Smithsonian Conservat Biol Inst, Natl Zool Pk, Front Royal, VA 22630 USA. RP Comizzoli, P (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA.; Comizzoli, P (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Front Royal, VA 22630 USA. EM comizzolip@si.edu FU National Center for Research Resources, component of the National Institutes of Health (NIH) [R01 R026064]; Office of Research Infrastructure Programs/Office of the Director [R01 OD 010948] FX This project was funded by the National Center for Research Resources (R01 R026064), a component of the National Institutes of Health (NIH) and is currently supported by the Office of Research Infrastructure Programs/Office of the Director (R01 OD 010948). No conflict of interests to be declared. We thank Dr. Brent Whitaker (Maryland Line Animal Rescue) for providing domestic cat ovaries. NR 37 TC 0 Z9 0 U1 2 U2 3 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1058-0468 EI 1573-7330 J9 J ASSIST REPROD GEN JI J. Assist. Reprod. Genet. PD JUN PY 2016 VL 33 IS 6 BP 783 EP 794 DI 10.1007/s10815-016-0706-4 PG 12 WC Genetics & Heredity; Obstetrics & Gynecology; Reproductive Biology SC Genetics & Heredity; Obstetrics & Gynecology; Reproductive Biology GA DN7FZ UT WOS:000377242000013 PM 27059775 ER PT J AU Betancourt, A Loaiza, JR AF Betancourt, Angie Loaiza, Jose R. TI An effective sampling tool for adult crabhole inhabiting Deinocerites mosquitoes SO JOURNAL OF VECTOR ECOLOGY LA English DT Article ID CANCER C1 [Betancourt, Angie] Univ Texas El Paso, Coll Hlth Sci, El Paso, TX 79968 USA. [Loaiza, Jose R.] Inst Invest Cient & Serv Alta Tecnol, Saber, Panama. [Loaiza, Jose R.] Smithsonian Trop Res Inst, Panama City, Panama. RP Loaiza, JR (reprint author), Inst Invest Cient & Serv Alta Tecnol, Saber, Panama.; Loaiza, JR (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM jloaiza@indicasat.org.pa FU Instituto de Investigaciones Cientificas y Servicios de Alta Tecnologia (INDICASAT-AIP); Smithsonian Tropical Research Institute (STRI); Minority Health and Health Disparities International Research Training Program (MHIRT - College of Health Sciences, the University of Texas at El Paso); Minority Health and Health Disparities National Institutes of Health [5T37MD001376-06]; Secretariat for Science, Technology and Innovation of Panama (SENACYT) [ITE11-015, COL11-044]; JRL FX We thank three anonymous reviewers who provided valuable comments to improve the quality and clarity of this manuscript. We want to thank Jose R. Rovira, Larissa C. Dutari, Susana Koo, Gaudenia Mendoza, Jahzeel Samaniego, Alta Gracia Cepeda, Eric Alvarez, Indra G. Rodriguez, and Anel Justino Duncan, from the University of Panama, for supporting mosquito collections during this study. Financial support was provided by the Instituto de Investigaciones Cientificas y Servicios de Alta Tecnologia (INDICASAT-AIP), the Smithsonian Tropical Research Institute (STRI), and the Minority Health and Health Disparities International Research Training Program (MHIRT - College of Health Sciences, the University of Texas at El Paso). The MHIRT program is funded by the Minority Health and Health Disparities National Institutes of Health grant 5T37MD001376-06. The Secretariat for Science, Technology and Innovation of Panama (SENACYT), through research grants ITE11-015 and COL11-044 and the National System of Investigators (SNI), supports research activities by JRL. NR 11 TC 0 Z9 0 U1 1 U2 1 PU SOC VECTOR ECOLOGY PI CORONA PA 1966 COMPTON AVE, CORONA, CA 92881 USA SN 1081-1710 EI 1948-7134 J9 J VECTOR ECOL JI J. Vector Ecol. PD JUN PY 2016 VL 41 IS 1 BP 200 EP 203 DI 10.1111/jvec.12214 PG 4 WC Entomology SC Entomology GA DN6XK UT WOS:000377219600028 PM 27232145 ER PT J AU Mawatari, K Yamada, T Fazio, GG Huang, JS Ashby, MLN AF Mawatari, Ken Yamada, Toru Fazio, Giovanni G. Huang, Jia-Sheng Ashby, Matthew L. N. TI Possible identification of massive and evolved galaxies at z greater than or similar to 5 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift ID EXTREMELY RED OBJECTS; EXTRAGALACTIC LEGACY SURVEY; CAMPANAS INFRARED SURVEY; EMISSION-LINE GALAXIES; STAR-FORMING GALAXIES; WIDE-FIELD CAMERA; COLD DARK-MATTER; QUIESCENT GALAXIES; STELLAR MASS; HIGH-REDSHIFT AB We report on the identification of the old stellar population galaxy candidates at z greater than or similar to 5. We developed a new infrared color selection scheme to isolate galaxies with the strong Balmer breaks at z greater than or similar to 5, and applied it to the ultra-deep and wide infrared survey data from the Spitzer Extended Deep Survey (SEDS) and the UKIRT Infrared Deep Sky Survey. The eight objects satisfying K - [3.6] > 1.3 and K - [3.6] > 2.4([3.6] - [4.5]) + 0.6 are selected in the 0.34 deg(2) SEDS Ultra Deep Survey field. Rich multi-wavelength imaging data from optical to far-infrared are also used to reject blending sources and strong nebular line emitters, and we finally obtained the three most likely evolved galaxies at z greater than or similar to 5. Their stacked spectral energy distribution is fitted well with the old stellar population template with M-* = (7.5 +/- 1.5) x 10(10) M-circle dot, star formation rate = 0.9 +/- 0.2M(circle dot) yr(-1), dust A(V) < 1, and age = 0.7 +/- 0.4 Gyr at z = 5.7 +/- 0.6, where the dusty star-forming galaxies at z similar to 2.8 are disfavored because of the faintness in the 24 mu m. The stellar mass density of these evolved galaxy candidates, (6 +/- 4) x 10(4) M-circle dot Mpc(-3), is much lower than that of star-forming galaxies, but the non-zero fraction suggests that initial star-formation and quenching have been completed by z similar to 6. C1 [Mawatari, Ken] Osaka Sangyo Univ, Coll Gen Educ, 3-1-1 Nakagaito, Osaka 5748530, Japan. [Yamada, Toru] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. [Fazio, Giovanni G.; Huang, Jia-Sheng; Ashby, Matthew L. N.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Mawatari, K (reprint author), Osaka Sangyo Univ, Coll Gen Educ, 3-1-1 Nakagaito, Osaka 5748530, Japan. EM mawatari@las.osaka-sandai.ac.jp FU Japan Society for the Promotion of Science through Brain Circulation Program [R2301]; [13J02968]; [26400217] FX We thank Brett Salmon and Steven Finkelstein for the code they offered which calculates nebular emission line flux. We also appreciate Hisanori Furusawa for kindly offering the new Subaru z'-band imaging. This research was conducted as a part of K. M.'s phD thesis in Tohoku University. K. M. is grateful to Takashi Ichikawa, Masafumi Noguchi, and Masayuki Akiyama for valuable comments and suggestions. As this research started during K. M. stayed at the Harvard-Smithsonian Astrophysical Observatory, K. M. appreciates the SAO predoctoral program. This research is financially supported by Japan Society for the Promotion of Science through Brain Circulation Program (R2301) and Grant-in-aid for Scientific Research (13J02968 and 26400217). NR 98 TC 1 Z9 1 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD JUN PY 2016 VL 68 IS 3 AR 46 DI 10.1093/pasj/psw041 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN9UL UT WOS:000377426100021 ER PT J AU Malo, C Morrell, JM Crichton, EG Pukazhenthi, BS Skidmore, JA AF Malo, C. Morrell, J. M. Crichton, E. G. Pukazhenthi, B. S. Skidmore, J. A. TI Use of colloid single layer centrifugation for dromedary camel semen: Effect of initial dilution and comparison of two colloids on sperm quality parameters SO ANIMAL REPRODUCTION SCIENCE LA English DT Meeting Abstract CT 10th Biennial Conference of the Association-for-Applied-Animal-Androl CY JUN 24-26, 2016 CL Tours, FRANCE SP Assoc Appl Anim Androl C1 [Malo, C.; Crichton, E. G.; Skidmore, J. A.] Camel Reprod Ctr, Dubai, U Arab Emirates. [Morrell, J. M.] Swedish Univ Agr Sci SLU, Clin Sci, Box 7054, SE-75007 Uppsala, Sweden. [Pukazhenthi, B. S.] Smithsonian Conservat Biol Inst, Dept Reprod Sci, Front Royal, VA 22630 USA. NR 0 TC 1 Z9 1 U1 0 U2 2 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 JUN PY 2016 VL 169 SI SI MA P49 BP 123 EP 123 DI 10.1016/j.anireprosci.2016.03.068 PG 1 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA DN7CJ UT WOS:000377232600068 ER PT J AU Hughey, MC Walke, JB Becker, MH Umile, TP Burzynski, EA Minbiole, KPC Iannetta, AA Santiago, CN Hopkins, WA Belden, LK AF Hughey, Myra C. Walke, Jenifer B. Becker, Matthew H. Umile, Thomas P. Burzynski, Elizabeth A. Minbiole, Kevin P. C. Iannetta, Anthony A. Santiago, Celina N. Hopkins, William A. Belden, Lisa K. TI Short-Term Exposure to Coal Combustion Waste Has Little Impact on the Skin Microbiome of Adult Spring Peepers (Pseudacris crucifer) SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID BUFO-TERRESTRIS; GUT MICROBIOTA; SOUTHERN TOADS; INTESTINAL MICROBIOTA; AQUATIC DISPOSAL; ARSENIC EXPOSURE; EARLY-LIFE; ANTIBIOTICS; RESILIENCE; DIVERSITY AB Disruptions to the microbiome can impact host health as can exposure to environmental contaminants. However, few studies have addressed how environmental contaminants impact the microbiome. We explored this question for frogs that breed in wetlands contaminated with fly ash, a by-product of coal combustion that is enriched in trace elements. We found differences in the bacterial communities among a fly ash-contaminated site and several reference wetlands. We then experimentally assessed the impacts of fly ash on the skin microbiome of adult spring peepers (Pseudacris crucifer). Frogs were exposed to fly ash in the laboratory for 12 h, the duration of a typical breeding event, and the skin microbiome was assessed after 5 days (experiment 1) or after 5 and 15 days (experiment 2). We examined bacterial community structure using 16S rRNA gene amplicon sequencing and metabolite profiles using high-pressure liquid chromatography-mass spectrometry (HPLC-MS). We found little impact as the result of acute exposure to fly ash on the bacterial communities or metabolite profiles in either experiment, suggesting that the bacterial symbiont communities of adults may be relatively resistant to brief contaminant exposure. However, housing frogs in the laboratory altered bacterial community structure in the two experiments, which supports prior research suggesting that environmental source pools are important for maintaining the amphibian skin microbiome. Therefore, for contaminants like fly ash that may alter the potential source pool of symbionts, we think it may be important to explore how contaminants affect the initial assembly of the amphibian skin microbiome in larval amphibians that develop within contaminated sites. IMPORTANCE Animals are hosts to many symbiotic microorganisms, collectively called the microbiome, that play critical roles in host health. Therefore, environmental contaminants that alter the microbiome may impact hosts. Some of the most widespread contaminants, produced worldwide, are derived from the mining, storage, and combustion of coal for energy. Fly ash, for example, is a by-product of coal combustion. It contains compounds such as arsenic, selenium, cadmium, and strontium and is a recognized source of ground and surface water contamination. Here, we experimentally investigated the impacts of short-term fly ash exposure on the skin microbiome of spring peepers, one of many species of amphibian that sometimes breed in open fly ash disposal ponds. This research provides a look into the potential impacts of fly ash on an animal's microbiome and suggests important future directions for research on the effects of environmental contaminants on the microbiome. C1 [Hughey, Myra C.; Walke, Jenifer B.; Becker, Matthew H.; Belden, Lisa K.] Virginia Tech, Dept Biol Sci, Blacksburg, VA USA. [Umile, Thomas P.; Burzynski, Elizabeth A.; Minbiole, Kevin P. C.; Iannetta, Anthony A.; Santiago, Celina N.] Villanova Univ, Dept Chem, Villanova, PA 19085 USA. [Hopkins, William A.] Virginia Tech, Dept Fish & Wildlife Conservat, Blacksburg, VA USA. [Becker, Matthew H.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC USA. [Umile, Thomas P.] Gwynedd Mercy Univ, Div Nat & Computat Sci, Gwynedd Valley, PA USA. [Burzynski, Elizabeth A.] Cornell Univ, Dept Food Sci, Ithaca, NY 14853 USA. RP Hughey, MC (reprint author), Virginia Tech, Dept Biol Sci, Blacksburg, VA USA. EM myrahughey@gmail.com OI Umile, Thomas/0000-0003-3077-6689 FU Virginia Tech Fralin Life Sciences Institute Organismal Biology and Ecology group; National Science Foundation [DEB-1136640, DEB-1136662] FX This project was funded by the Virginia Tech Fralin Life Sciences Institute Organismal Biology and Ecology group and the National Science Foundation (DEB-1136640 to L.K.B. and DEB-1136662 to K.P.C.M.). NR 64 TC 0 Z9 0 U1 8 U2 12 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 EI 1098-5336 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD JUN PY 2016 VL 82 IS 12 BP 3493 EP 3502 DI 10.1128/AEM.00045-16 PG 10 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA DN4FI UT WOS:000377018400006 PM 27037118 ER PT J AU Shields, AL Barnes, R Agol, E Charnay, B Bitz, C Meadows, VS AF Shields, Aomawa L. Barnes, Rory Agol, Eric Charnay, Benjamin Bitz, Cecilia Meadows, Victoria S. TI The Effect of Orbital Configuration on the Possible Climates and Habitability of Kepler-62f SO ASTROBIOLOGY LA English DT Article DE Extrasolar planets; Habitability; Planetary environments ID MAIN-SEQUENCE STARS; SOLAR-SYSTEM; PLANETARY SYSTEMS; OBLIQUITY VARIATIONS; TERRESTRIAL PLANETS; TIDAL DISSIPATION; EARTHS OBLIQUITY; ALBEDO FEEDBACK; SUPER-EARTHS; EARLY MARS AB As lower-mass stars often host multiple rocky planets, gravitational interactions among planets can have significant effects on climate and habitability over long timescales. Here we explore a specific case, Kepler-62f (Borucki et al., 2013), a potentially habitable planet in a five-planet system with a K2V host star. N-body integrations reveal the stable range of initial eccentricities for Kepler-62f is 0.00 <= e <= 0.32, absent the effect of additional, undetected planets. We simulate the tidal evolution of Kepler-62f in this range and find that, for certain assumptions, the planet can be locked in a synchronous rotation state. Simulations using the 3-D Laboratoire de Meteorologie Dynamique (LMD) Generic global climate model (GCM) indicate that the surface habitability of this planet is sensitive to orbital configuration. With 3 bar of CO2 in its atmosphere, we find that Kepler-62f would only be warm enough for surface liquid water at the upper limit of this eccentricity range, providing it has a high planetary obliquity (between 60 degrees and 90 degrees). A climate similar to that of modern-day Earth is possible for the entire range of stable eccentricities if atmospheric CO2 is increased to 5 bar levels. In a low-CO2 case (Earth-like levels), simulations with version 4 of the Community Climate System Model (CCSM4) GCM and LMD Generic GCM indicate that increases in planetary obliquity and orbital eccentricity coupled with an orbital configuration that places the summer solstice at or near pericenter permit regions of the planet with above-freezing surface temperatures. This may melt ice sheets formed during colder seasons. If Kepler-62f is synchronously rotating and has an ocean, CO2 levels above 3 bar would be required to distribute enough heat to the nightside of the planet to avoid atmospheric freeze-out and permit a large enough region of open water at the planet's substellar point to remain stable. Overall, we find multiple plausible combinations of orbital and atmospheric properties that permit surface liquid water on Kepler-62f. C1 [Shields, Aomawa L.] Univ Calif Los Angeles, Dept Phys & Astron, Box 951547, Los Angeles, CA 90095 USA. [Shields, Aomawa L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Barnes, Rory; Agol, Eric; Charnay, Benjamin; Meadows, Victoria S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Barnes, Rory; Agol, Eric; Charnay, Benjamin; Meadows, Victoria S.] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA. [Bitz, Cecilia] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Shields, Aomawa L.; Barnes, Rory; Agol, Eric; Charnay, Benjamin; Bitz, Cecilia; Meadows, Victoria S.] NASA, Astrobiol Inst, Virtual Planetary Lab, Los Angeles, CA USA. RP Shields, AL (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Box 951547, Los Angeles, CA 90095 USA. EM ashields@astro.ucla.edu RI Bitz, Cecilia/S-8423-2016 OI Bitz, Cecilia/0000-0002-9477-7499 FU National Science Foundation [1401554, DGE-0718124, DGE-1256082]; University of California; National Science Foundation; National Aeronautics and Space Administration through the NASA Astrobiology Institute [NNH12ZDA002C, NNA13AA93A]; NSF [AST-1108882] FX This material is based upon work supported by the National Science Foundation under Award No. 1401554, and Grant Nos. DGE-0718124 and DGE-1256082, and by a University of California President's Postdoctoral Fellowship. This work was facilitated through the use of advanced computational, storage, and networking infrastructure provided by the Hyak supercomputer system at the University of Washington. We would also like to acknowledge high-performance computing support from Yellowstone (ark:/85065/d7wd3xhc) provided by NCAR's Computational and Information Systems Laboratory, sponsored by the National Science Foundation. This work was performed as part of the NASA Astrobiology Institute's Virtual Planetary Laboratory Lead Team, supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under solicitation NNH12ZDA002C and Cooperative Agreement Number NNA13AA93A. The authors wish to thank Dorian Abbot and an anonymous referee for their comments and suggestions, which improved the paper. B.C. acknowledges support from an appointment to the NASA Postdoctoral Program at NAI Virtual Planetary Laboratory, administered by Oak Ridge Affiliated Universities. R.B. acknowledges support from NSF grant AST-1108882. A.S. thanks Brad Hansen, Jonathan Mitchell, John Johnson, Russell Deitrick, and Tom Quinn for helpful discussions regarding this work. NR 115 TC 2 Z9 2 U1 18 U2 22 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2016 VL 16 IS 6 BP 443 EP + DI 10.1089/ast.2015.1353 PG 23 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA DN6TW UT WOS:000377210200006 PM 27176715 ER PT J AU Hull, CLH Girart, JM Kristensen, LE Dunham, MM Rodriguez-Kamenetzky, A Carrasco-Gonzalez, C Cortes, PC Li, ZY Plambeck, RL AF Hull, Charles L. H. Girart, Josep M. Kristensen, Lars E. Dunham, Michael M. Rodriguez-Kamenetzky, Adriana Carrasco-Gonzalez, Carlos Cortes, Paulo C. Li, Zhi-Yun Plambeck, Richard L. TI AN EXTREMELY HIGH VELOCITY MOLECULAR JET SURROUNDED BY AN IONIZED CAVITY IN THE PROTOSTELLAR SOURCE SERPENS SMM1 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: jets and outflows; radio continuum: stars; stars: formation; stars: protostars ID RADIO-CONTINUUM SOURCE; ENVELOPE STRUCTURE; REGIONS; OUTFLOWS; STAR; EMISSION; DENSITY; OBJECTS; SYSTEM; MOTION AB We report Atacama Large Millimeter/submillimeter Array (ALMA) observations of a one-sided, high-velocity (similar to 80 km s(-1)) CO(J = 2 -> 1) jet powered by the intermediate-mass protostellar source Serpens SMM1-a. The highly collimated molecular jet is flanked at the base by a wide-angle cavity; the walls of the cavity can be seen in both 4 cm free-free emission detected by the Very Large Array and 1.3 mm thermal dust emission detected by ALMA. This is the first time that ionization of an outflow cavity has been directly detected via free-free emission in a very young, embedded Class 0 protostellar source that is still powering a molecular jet. The cavity walls are ionized either by UV photons escaping from the accreting protostellar source or by the precessing molecular jet impacting the walls. These observations suggest that ionized outflow cavities may be common in Class 0 protostellar sources, shedding further light on the radiation, outflow, and jet environments in the youngest, most embedded forming stars. C1 [Hull, Charles L. H.; Girart, Josep M.; Kristensen, Lars E.; Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Girart, Josep M.] Inst Ciencies Espai, CSIC IEEC, Campus UAB,Carrer Can Magrans S-N, E-08193 Cerdanyola Del Valles, Catalonia, Spain. [Rodriguez-Kamenetzky, Adriana] UNC, IATE, X5000BGR, Cordoba, Argentina. [Rodriguez-Kamenetzky, Adriana; Carrasco-Gonzalez, Carlos] Inst Radioastron & Astrofis IRyA UNAM, Morelia 58089, Michoacan, Mexico. [Cortes, Paulo C.] Joint ALMA Observ, Av Alonso Cordova, Santiago 3104, Chile. [Cortes, Paulo C.] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. [Li, Zhi-Yun] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Plambeck, Richard L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Plambeck, Richard L.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Hull, Charles L. H.] Natl Radio Astron Observ, Charlottesville, VA 22904 USA. RP Hull, CLH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Hull, CLH (reprint author), Natl Radio Astron Observ, Charlottesville, VA 22904 USA. EM chat.hull@cfa.harvard.edu RI Kristensen, Lars E/F-4774-2011; OI Kristensen, Lars E/0000-0003-1159-3721; Plambeck, Richard/0000-0001-6765-9609; Hull, Charles/0000-0002-8975-7573; Girart, Josep Miquel/0000-0002-3829-5591 FU MICINN [AYA2014-57369-C3-P]; MECD grants (Spain) [PRX15/00435]; Submillimeter Array (SMA) through the SMA postdoctoral fellowship; NASA ADAP [NNX13AE54G]; UNAM-DGAPA-PAPIIT [IA101214, IA102816]; MINCyT-CONACyT [ME/13/47]; NASA [NNX14AB38G]; NSF [AST-1313083] FX The authors acknowledge the anonymous referee, whose constructive comments improved this work substantially. The authors also thank Ruud Visser for his careful reading of our paper and for his timely communication of a necessary correction. C.L.H.H. acknowledges the invaluable data reduction assistance from Crystal Brogan and Bill Cotton. The authors acknowledge Minho Choi for kindly supplying them with a FITS file of the 7 mm VLA data for the purpose of calculating the spectral index of the emission from the outflow cavity. J.M.G. acknowledges support from MICINN AYA2014-57369-C3-P and the MECD PRX15/00435 grants (Spain). L.E.K. and M.M.D. acknowledge support from the Submillimeter Array (SMA) through the SMA postdoctoral fellowship. M.M.D. acknowledges support from NASA ADAP grant NNX13AE54G. A.R.-K. and C.C.-G. acknowledge support by UNAM-DGAPA-PAPIIT grant numbers IA101214 and IA102816 and financial support from MINCyT-CONACyT ME/13/47 grant, corresponding to the Bilateral Cooperation Program. Z.-Y.L. is supported in part by NASA NNX14AB38G and NSF AST-1313083. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO. ALMA#2013.1.00726.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. NR 43 TC 1 Z9 1 U1 1 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 JUN 1 PY 2016 VL 823 IS 2 AR L27 DI 10.3847/2041-8205/823/2/L27 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN4JL UT WOS:000377031700006 ER PT J AU Willows-Munro, S Dowler, RC Jarcho, MR Phillips, RB Snell, HL Wilbert, TR Edwards, CW AF Willows-Munro, Sandi Dowler, Robert C. Jarcho, Michael R. Phillips, Reese B. Snell, Howard L. Wilbert, Tammy R. Edwards, Cody W. TI Cryptic diversity in Black rats Rattus rattus of the Galapagos Islands, Ecuador SO ECOLOGY AND EVOLUTION LA English DT Article DE Biological invasions; conservation biology; Galapagos; genetic diversity; invasive species; island biology; phylogeography; rodent ID MULTILOCUS GENOTYPE DATA; GENETIC-STRUCTURE; POPULATION-STRUCTURE; INTRODUCED PLANTS; MIGRATION RATES; HOUSE MOUSE; COLONIZATION; ARCHIPELAGO; CONSERVATION; INVASION AB Human activity has facilitated the introduction of a number of alien mammal species to the Galapagos Archipelago. Understanding the phylogeographic history and population genetics of invasive species on the Archipelago is an important step in predicting future spread and designing effective management strategies. In this study, we describe the invasion pathway of Rattus rattus across the Galapagos using microsatellite data, coupled with historical knowledge. Microsatellite genotypes were generated for 581 R. rattus sampled from 15 islands in the archipelago. The genetic data suggest that there are at least three genetic lineages of R. rattus present on the Galapagos Islands. The spatial distributions of these lineages correspond to the main centers of human settlement in the archipelago. There was limited admixture among these three lineages, and these finding coupled with low rates of gene flow among island populations suggests that interisland movement of R. rattus is rare. The low migration among islands recorded for the species will have a positive impact on future eradication efforts. C1 [Willows-Munro, Sandi] Univ KwaZulu Natal, Sch Life Sci, POB X01, ZA-3209 Scottsville, South Africa. [Dowler, Robert C.] Angelo State Univ, Dept Biol, San Angelo, TX 76909 USA. [Jarcho, Michael R.] Loras Coll, Neurosci Program, Dubuque, IA USA. [Phillips, Reese B.] US Fish & Wildlife Serv, Pacific Islands Fish & Wildlife Off, 300 Ala Moana Blvd,Rm 3-122, Honolulu, HI USA. [Snell, Howard L.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Snell, Howard L.] Univ New Mexico, Museum Southwestern Biol, Albuquerque, NM 87131 USA. [Wilbert, Tammy R.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC USA. [Edwards, Cody W.] George Mason Univ, Dept Biol, Fairfax, VA 22030 USA. RP Willows-Munro, S (reprint author), Univ KwaZulu Natal, Sch Life Sci, POB X01, ZA-3209 Scottsville, South Africa. EM willows-munro@ukzn.ac.za FU US AID; United Nations Development Fund; World Bank Global Environmental Fund; National Geographic Society; Charles Darwin Foundation (CDF); University of New Mexico (Latin American-Iberian Institute); Angelo State University; Galapagos National Park Service (GNPS); George Mason Presidential Fellowship FX Much of the fieldwork associated with this research was supported by grants from US AID, the United Nations Development Fund, the World Bank Global Environmental Fund, and the National Geographic Society, with additional support from the Charles Darwin Foundation (CDF), the University of New Mexico (including the Latin American-Iberian Institute), Angelo State University, and the Galapagos National Park Service (GNPS). The molecular work was also supported by the George Mason Presidential Fellowship of T. R. Wilbert. NR 59 TC 0 Z9 0 U1 10 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD JUN PY 2016 VL 6 IS 11 BP 3721 EP 3733 DI 10.1002/ece3.2033 PG 13 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA DN4ND UT WOS:000377043200022 ER PT J AU Martin, MD Olsen, MT Samaniego, JA Zimmer, EA Gilbert, MTP AF Martin, Michael D. Olsen, Morten Tange Samaniego, Jose A. Zimmer, Elizabeth A. Gilbert, M. Thomas P. TI The population genomic basis of geographic differentiation in North American common ragweed (Ambrosia artemisiifolia L.) SO ECOLOGY AND EVOLUTION LA English DT Article DE Ambrosia artemisiifolia; common ragweed; GBS; population genetics; population genomics; ragweed ID GENETIC-VARIATION; SESQUITERPENE LACTONES; PRINCIPAL-COMPONENTS; R-PACKAGE; EVOLUTION; INVASIVENESS; ASSOCIATION; ADAPTATION; INVASION; PLANTS AB Common ragweed (Ambrosia artemisiifolia L.) is an invasive, wind-pollinated plant nearly ubiquitous in disturbed sites in its eastern North American native range and present across growing portions of Europe, Africa, Asia, and Australia. Phenotypic divergence between European and native-range populations has been described as rapid evolution. However, a recent study demonstrated major human-mediated shifts in ragweed genetic structure before introduction to Europe and suggested that native-range genetic structure and local adaptation might fully explain accelerated growth and other invasive characteristics of introduced populations. Genomic differentiation that potentially influenced this structure has not yet been investigated, and it remains unclear whether substantial admixture during historical disturbance of the native range contributed to the development of invasiveness in introduced European ragweed populations. To investigate fine-scale population genetic structure across the species' native range, we characterized diallelic SNP loci via a reduced-representation genotyping-by-sequencing (GBS) approach. We corroborate phylogeographic domains previously discovered using traditional sequencing methods, while demonstrating increased power to resolve weak genetic structure in this highly admixed plant species. By identifying exome polymorphisms underlying genetic differentiation, we suggest that geographic differentiation of this important invasive species has occurred more often within pathways that regulate growth and response to defense and stress, which may be associated with survival in North America's diverse climatic regions. C1 [Martin, Michael D.; Olsen, Morten Tange; Samaniego, Jose A.; Gilbert, M. Thomas P.] Univ Copenhagen, Fac Sci, Nat Hist Museum Denmark, Ctr GeoGenet, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. [Martin, Michael D.] Univ Calif Berkeley, Ctr Theoret Evolutionary Genom, Valley Life Sci Bldg, Berkeley, CA 94720 USA. [Martin, Michael D.; Gilbert, M. Thomas P.] Norwegian Univ Sci & Technol NTNU, Univ Museum, Dept Nat Hist, NO-7491 Trondheim, Norway. [Zimmer, Elizabeth A.] Museum Support Ctr, Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. [Zimmer, Elizabeth A.] Museum Support Ctr, Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. [Gilbert, M. Thomas P.] Curtin Univ, Dept Environm & Agr, Trace & Environm DNA Lab, Perth, WA 6102, Australia. RP Martin, MD (reprint author), Norwegian Univ Sci & Technol NTNU, Univ Museum, NO-7491 Trondheim, Norway. EM mike.martin@ntnu.no RI Olsen, Morten/J-4783-2013 OI Olsen, Morten/0000-0001-6716-6345 FU Lundbeck Foundation [R52-5062] FX Lundbeck Foundation (Grant/Award Number: R52-5062). NR 57 TC 1 Z9 1 U1 23 U2 40 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD JUN PY 2016 VL 6 IS 11 BP 3760 EP 3771 DI 10.1002/ece3.2143 PG 12 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA DN4ND UT WOS:000377043200025 ER PT J AU Transue, WJ Velian, A Nava, M Martin-Drumel, MA Womack, CC Jiang, J Hou, GL Wang, XB McCarthy, MC Field, RW Cummins, CC AF Transue, Wesley J. Velian, Alexandra Nava, Matthew Martin-Drumel, Marie-Aline Womack, Caroline C. Jiang, Jun Hou, Gao-Lei Wang, Xue-Bin McCarthy, Michael C. Field, Robert W. Cummins, Christopher C. TI A Molecular Precursor to Phosphaethyne and Its Application in Synthesis of the Aromatic 1,2,3,4-Phosphatriazolate Anion SO JOURNAL OF THE AMERICAN CHEMICAL SOCIETY LA English DT Article ID COORDINATED PHOSPHORUS-COMPOUNDS; MICROWAVE SPECTROSCOPY; THERMAL-DECOMPOSITION; WAVE SPECTROSCOPY; PHOSPHAALKYNES; CHEMISTRY; BOND; HCP; FRAGMENTATION; DERIVATIVES AB Dibenzo-7-phosphanorbornadiene Ph3PC-(H)PA (1, A = 14 C- H-10, anthracene) is reported here as a molecular precursor to phosphaethyne (HC P), produced together with anthracene and triphenylphosphine. HCP generated by thermolysis of 1 has been observed by molecular beam mass spectrometry, laser induced fluorescence, microwave spectroscopy, and nuclear magnetic resonance (NMR) spectroscopy. In toluene, fragmentation of 1 has been found to proceed with activation parameters of Delta H-double dagger = 25.5 kcal/mol and Delta S-double dagger =-2.43 eu and is accompanied by formation of an orange insoluble precipitate. Results from computational studies of the mechanism of HCP generation are in good agreement with experimental data. This high-temperature method of HCP generation has pointed to new reaction chemistry with azide anion to produce the 1,2,3,4-phosphatriazolate anion, HCPN3-, for which structural data have been obtained in a single-crystal X-ray diffraction study. Negative-ion photoelectron spectroscopy has shown the adiabatic detachment energy for this anion to be 3.555(10) eV. The aromaticity of HCPN3- has been assessed using nucleus-independent chemical shift, quantum theory of atoms in molecules, and natural bond orbital methods. C1 [Transue, Wesley J.; Velian, Alexandra; Nava, Matthew; Womack, Caroline C.; Jiang, Jun; Field, Robert W.; Cummins, Christopher C.] MIT, Dept Chem, Cambridge, MA 02139 USA. [Martin-Drumel, Marie-Aline; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Hou, Gao-Lei; Wang, Xue-Bin] Pacific NW Natl Lab, Div Phys Sci, Richland, WA 99352 USA. RP Cummins, CC (reprint author), MIT, Dept Chem, Cambridge, MA 02139 USA. EM ccummins@mit.edu OI Cummins, Christopher/0000-0003-2568-3269; Martin-Drumel, Marie-Aline/0000-0002-5460-4294; /0000-0001-7445-5663 FU National Science Foundation [CHE-1362118]; Department of Energy [DE-FG0287ER13671]; NASA [NNX13AE59G]; CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory; DOE, Office of Science, Office of Basic Energy Sciences, Division of Chemical Sciences, Geosciences and Biosciences FX This material is based on research supported by the National Science Foundation grant CHE-1362118, the Department of Energy grant DE-FG0287ER13671, and the NASA grant NNX13AE59G. M.A.M.-D. was supported by a CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory. The NIPES research at PNNL was supported by the DOE, Office of Science, Office of Basic Energy Sciences, Division of Chemical Sciences, Geosciences and Biosciences, and performed using the EMSL. We gratefully acknowledge Ioana Knopf and Peter Muller for useful discussions on crystallography and Maciej D. Korzynski for assistance in acquiring TGA data. NR 50 TC 2 Z9 2 U1 22 U2 41 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0002-7863 J9 J AM CHEM SOC JI J. Am. Chem. Soc. PD JUN 1 PY 2016 VL 138 IS 21 BP 6731 EP 6734 DI 10.1021/jacs.6b03910 PG 4 WC Chemistry, Multidisciplinary SC Chemistry GA DN5ZW UT WOS:000377151400010 PM 27171847 ER PT J AU Riley, SM AF Riley, Sheila M. TI Loner SO LIBRARY JOURNAL LA English DT Book Review C1 [Riley, Sheila M.] Smithsonian Inst Libs, Washington, DC USA. RP Riley, SM (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2016 VL 141 IS 10 BP 86 EP 86 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA DN7EG UT WOS:000377237500093 ER PT J AU Whitcomb, D Jennings, M Creekmore, A Arce, I AF Whitcomb, Donald Jennings, Michael Creekmore, Andrew Arce, Ignacio TI KHIRBET AL-MAFJAR New Excavations and Hypotheses for an Umayyad Monument SO NEAR EASTERN ARCHAEOLOGY LA English DT Article ID SOUTHEASTERN TURKEY AB The Umayyad palace at Khirbet al-Mafiar, also known as Qasr Hisham, has been known and appreciated as the most beautifully decorated of the Umayyad qusur (socalled desert castles). Its fabulous mosaic carpets, human and animal figures, extensive stucco wall decorations, and frescoes have made this monumental complex, located just north of the city of Jericho, an extraordinary archaeological site. Excavated by Dimitri Baramki fir some 13 seasons, in the 1930s and 1940s, the site has been assumed to be completely revealed (Hamilton and Grabar 1959; Whitcomb I988).' C1 [Whitcomb, Donald] Univ Chicago, Oriental Inst, Chicago, IL 60637 USA. [Whitcomb, Donald] Univ Chicago, Middle East Ctr, Chicago, IL 60637 USA. [Whitcomb, Donald] Dept Near Eastern Languages & Civilizat, Program Islamic Archaeol, Cambridge, MA 02138 USA. [Whitcomb, Donald] Field Museum Nat Hist, Chicago, IL 60605 USA. [Whitcomb, Donald] Smithsonian Inst, New York, NY USA. [Whitcomb, Donald] Metropolitan Museum Art, New York, NY 10028 USA. [Jennings, Michael] Univ Calif Berkeley, Ctr Digital Archaeol CoDA, Field Data, Berkeley, CA 94720 USA. [Creekmore, Andrew] Univ No Colorado, Anthropol, Greeley, CO 80639 USA. RP Whitcomb, D (reprint author), Univ Chicago, Oriental Inst, Chicago, IL 60637 USA.; Whitcomb, D (reprint author), Univ Chicago, Middle East Ctr, Chicago, IL 60637 USA.; Whitcomb, D (reprint author), Dept Near Eastern Languages & Civilizat, Program Islamic Archaeol, Cambridge, MA 02138 USA.; Whitcomb, D (reprint author), Field Museum Nat Hist, Chicago, IL 60605 USA.; Whitcomb, D (reprint author), Smithsonian Inst, New York, NY USA.; Whitcomb, D (reprint author), Metropolitan Museum Art, New York, NY 10028 USA. NR 17 TC 0 Z9 0 U1 0 U2 0 PU AMER SCHS ORIENTAL RESEARCH PI BOSTON PA BOSTON UNIV, 656 BEACON ST, 5TH FLOOR, BOSTON, MA 02215 USA SN 1094-2076 J9 NEAR EAST ARCHAEOL JI Near East. Archaeol. PD JUN PY 2016 VL 79 IS 2 BP 78 EP 87 PG 10 WC Archaeology SC Archaeology GA DN2QK UT WOS:000376907900003 ER PT J AU Heredia, MD Robbins, RK AF Dolores Heredia, Maria Robbins, Robert K. TI Natural history of the mistletoe-feeding Thereus lomalarga (Lepidoptera, Lycaenidae, Eumaeini) in Colombia SO ZOOTAXA LA English DT Article DE Chaetotaxy; crypsis; honeydew; immatures; life cycle; Loranthaceae; myrmecophily; protogyny; Thereus ortalus ID ENEMY-FREE SPACE; IMMATURE STAGES; LIFE-HISTORY; KEYSTONE RESOURCE; BUTTERFLY LARVAE; THECLINAE; ANTS; MORPHOLOGY; CLASSIFICATION; ASSOCIATION AB The natural history and morphology of the immature stages of the butterfly Thereus lomalarga Robbins, Heredia & Busby are described and illustrated. The food plant is Oryctanthus alveolatus (H.B.K.) Kuijt (Loranthaceae). Chaetotaxy of the first instar is described and compared with that of three locally studied Thereus species. Larvae have four instars, and the dorsal nectary organ becomes functional in the third instar. They are facultatively tended by ants belonging to seven genera that are attracted to O. alveolatus by floral disc nectaries, honeydew producing Hemiptera, and secretory wounds produced by Hemiptera on the fleshy inflorescence rachis. The average period from egg to eclosion under lab conditions was 35.68 days. Females emerged before males. Adults of both sexes feed on nectar from the flowers of the food plant and on hemipteran secretions; adults were not observed feeding on other flowers. Campopleginae and Chalcidinae were the most important parasitoids. C1 [Dolores Heredia, Maria] Cra 76A,9A-34,Apto 404, Cali, Colombia. [Robbins, Robert K.] Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, POB 37012,NHB Stop 127,E-514, Washington, DC 20013 USA. RP Heredia, MD (reprint author), Cra 76A,9A-34,Apto 404, Cali, Colombia.; Robbins, RK (reprint author), Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, POB 37012,NHB Stop 127,E-514, Washington, DC 20013 USA. EM mdheredia@hotmail.com; robbinsr@si.edu NR 67 TC 0 Z9 0 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUN 1 PY 2016 VL 4117 IS 3 BP 301 EP 320 DI 10.11646/zootaxa.4117.3.1 PG 20 WC Zoology SC Zoology GA DN2FQ UT WOS:000376879900001 PM 27395176 ER PT J AU Freeman, AS Frischeisen, A Blakeslee, AMH AF Freeman, Aaren S. Frischeisen, Alejandro Blakeslee, April M. H. TI Estuarine fouling communities are dominated by nonindigenous species in the presence of an invasive crab SO BIOLOGICAL INVASIONS LA English DT Article DE Fouling community; Mud crabs; Invasion meltdown; Tunicates; Anthropogenic habitats; Panopeus herbstii; Hemigrapsus sanguineus; Botrylloides violaceous; Molgula manhattensis; Diplosoma listerianum ID MARINE INVASIONS; HEMIGRAPSUS-SANGUINEUS; BIOTIC RESISTANCE; NORTH-AMERICA; PREDATION; ASCIDIANS; REPLACEMENT; CALIFORNIA; PATTERNS; IMPACTS AB Interactions between anthropogenic disturbances and introduced and native species can shift ecological communities, potentially leading to the successful establishment of additional invaders. Since its discovery in New Jersey in 1988, the Asian shore crab (Hemigrapsus sanguineus) has continued to expand its range, invading estuarine and coastal habitats in eastern North America. In estuarine environments, H. sanguineus occupies similar habitats to native, panopeid mud crabs. These crabs, and a variety of fouling organisms (both NIS and native), often inhabit man-made substrates (like piers and riprap) and anthropogenic debris. In a series of in situ experiments at a closed dock in southwestern Long Island (New York, USA), we documented the impacts of these native and introduced crabs on hard-substrate fouling communities. We found that while the presence of native mud crabs did not significantly influence the succession of fouling communities compared to caged and uncaged controls, the presence of introduced H. sanguineus reduced the biomass of native tunicates (particularly Molgula manhattensis), relative to caged controls. Moreover, the presence of H. sanguineus favored fouling communities dominated by introduced tunicates (especially Botrylloides violaceous and Diplosoma listerianum). Altogether, our results suggest that H. sanguineus could help facilitate introduced fouling tunicates in the region, particularly in locations where additional solid substrates have created novel habitats. C1 [Freeman, Aaren S.; Frischeisen, Alejandro] Adelphi Univ, Garden City, NY USA. [Frischeisen, Alejandro] Triumvirate Environm, Astoria, NY USA. [Blakeslee, April M. H.] E Carolina Univ, Greenville, NY USA. [Blakeslee, April M. H.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RP Freeman, AS (reprint author), Adelphi Univ, Garden City, NY USA. EM afreeman@adelphi.edu NR 39 TC 0 Z9 0 U1 10 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 EI 1573-1464 J9 BIOL INVASIONS JI Biol. Invasions PD JUN PY 2016 VL 18 IS 6 BP 1653 EP 1665 DI 10.1007/s10530-016-1108-3 PG 13 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA DM9CZ UT WOS:000376663400011 ER PT J AU Liu, D Dong, HL Agrawal, A Singh, R Zhang, J Wang, HM AF Liu, Deng Dong, Hailiang Agrawal, Abinash Singh, Rajesh Zhang, Jing Wang, Hongmei TI Inhibitory effect of clay mineral on methanogenesis by Methanosarcina mazei and Methanothermobacter thermautotrophicus SO APPLIED CLAY SCIENCE LA English DT Article DE Clay minerals; Kaolinite; Microbial iron reduction; Methanogenesis; Aluminum toxicity ID SULFATE-REDUCING ACTIVITY; MICROBIAL REDUCTION; FERRIC IRON; BACILLUS-MEGATERIUM; SMECTITE MINERALS; ALUMINUM TOXICITY; METHANE; FE(III); OXIDATION; SIDEROPHORE AB With increased concentration of methane in the atmosphere and its impact on climate, effective mitigation of methane emission is of global importance. Recent studies have shown the inhibition of microbial methanogenesis upon addition of ferruginous clay minerals. To better elucidate the mechanism of the inhibitory effect of clay minerals on methanogenesis, laboratory experiments with Methanosarcina mazei and Methanothermobacter thermautotrophicus were performed in batch systems in which pristine kaolinite or iron-coated kaolinite were added as representative clay minerals. Soluble Al in solution and production of Fe(II) and methane gas were monitored over the course of the experiments. The mineralogical changes in the kaolinites were characterized with scanning electron microscopy. The results confirmed that both Ms. mazei and Mt. thermautotrophicus were capable of reducing ferric iron with H-2/CO2 as methanogenic reactants. Both pristine and iron-coated kaolinites could act as effective inhibitors of methanogenesis. The overall methane production was similar with pristine kaolinite and iron-coated kaolinite, although at the beginning of the experiment less CH4 was observed in iron-coated kaolinite system. The inhibition of methanogenic activity observed in pristine kaolinite was primarily ascribed to the toxicity effect of aluminum. A more effective inhibition of methanogenesis in iron-coated kaolinite during the first several days could be explained by the combined effects of aluminum toxicity and diversion of electron flow from CO2 to Fe(III). Our results have important implications for mitigating methane emission in natural or anthropogenic settings. (C) 2016 Elsevier B.V. All rights reserved. C1 [Liu, Deng; Dong, Hailiang; Wang, Hongmei] China Univ Geosci, State Key Lab Biogeol & Environm Geol, Wuhan 430074, Peoples R China. [Dong, Hailiang; Singh, Rajesh] Miami Univ, Dept Geol & Environm Earth Sci, Oxford, OH 45056 USA. [Agrawal, Abinash] Wright State Univ, Dept Earth & Environm Sci, Dayton, OH 45435 USA. [Zhang, Jing] Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20013 USA. RP Liu, D (reprint author), China Univ Geosci, State Key Lab Biogeol & Environm Geol, Wuhan 430074, Peoples R China. EM liud_cug@126.com FU National Natural Science Foundation of China [41302270, 41572323]; 111 Project [B08030]; Fundamental Research Funds for the Central Universities [CUGL140815, CUGL150409] FX This research is financially supported by grants from the National Natural Science Foundation of China (nos. 41302270 and 41572323), the 111 Project (no. B08030), and the Fundamental Research Funds for the Central Universities (CUGL140815 and CUGL150409). We are grateful to the Associate Editor and three anonymous reviewers whose comments improved the quality of the manuscript NR 50 TC 3 Z9 3 U1 6 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-1317 EI 1872-9053 J9 APPL CLAY SCI JI Appl. Clay Sci. PD JUN PY 2016 VL 126 BP 25 EP 32 DI 10.1016/j.day.2016.02.030 PG 8 WC Chemistry, Physical; Materials Science, Multidisciplinary; Mineralogy SC Chemistry; Materials Science; Mineralogy GA DM2YL UT WOS:000376213900004 ER PT J AU Dillman, CB Sidlauskas, BL Vari, RP AF Dillman, Casey B. Sidlauskas, Brian L. Vari, Richard P. TI A morphological supermatrix-based phylogeny for the Neotropical fish superfamily Anostomoidea (Ostariophysi: Characiformes): phylogeny, missing data and homoplasy SO CLADISTICS LA English DT Review ID LOCALLY SAMPLED CHARACTERS; FRESH-WATER FISHES; DATA SETS; MOLECULAR PHYLOGENY; TELEOSTEI CHARACIFORMES; SPARSE SUPERMATRICES; MAXIMUM-LIKELIHOOD; SPECIES OSTARIOPHYSI; PARSIMONY ANALYSIS; SKELETAL ANATOMY AB Although 11 studies have addressed the systematics of the four families and 281 fish species of the ecomorphologically diverse Anostomoidea, none has proposed a global hypothesis of relationships. We synthesized these studies to yield a supermatrix with 463 morphological characters among 174 ingroup species, and inferred phylogeny with parsimony and Bayesian optimization. We evaluated the applicability of the supermatrix approach to morphological datasets, tested its sensitivity to missing data, determined the impact of homoplastic characters on phylogenetic resolution, and determined the distribution of homologies and homoplasies on the topology. Despite more than 60% missing data, analyses supported the monophyly of all families, and phylogenetic structure degraded only with inclusion of species with high percentages of missing data and in analyses limited to homoplasies. The latter differs modestly from the full matrix indicating phylogenetic signal in homoplastic characters. Character distributions differ across the phylogeny, with a greater prevalence of homologies at deeper nodes and homoplasies nearer the tips than expected by chance. This may suggest early diversification into distinct bauplans with subsequent diversification of faster evolving character systems. The morphological supermatrix approach is powerful and allows integration of classical data with modern methods to examine the evolution of multiple character systems. C1 [Dillman, Casey B.; Sidlauskas, Brian L.; Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012,MRC 159, Washington, DC 20013 USA. [Sidlauskas, Brian L.] Oregon State Univ, Dept Fisheries & Wildlife, 104 Nash Hall, Corvallis, OR 97331 USA. [Sidlauskas, Brian L.] Natl Evolutionary Synth Ctr, 2024 W Main St A200, Durham, NC 27705 USA. RP Dillman, CB (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012,MRC 159, Washington, DC 20013 USA. EM dillmanc@si.edu FU NSF [DEB-1257898, DEB-1257813]; National Evolutionary Synthesis Center (NESCent), NSF [EF-0423641] FX Funding for this research was provided by NSF #DEB-1257898 and by the National Evolutionary Synthesis Center (NESCent), NSF #EF-0423641. S. Otto, M. Whitlock, D. Eernisse, D. Swofford and J. Wiens provided thoughtful advice on analysis and synthesis. M. Sabaj Perez kindly supplied the excellent life photographs and figure legend information for Fig. 1, and was supported by the iXingu project, NSF #DEB-1257813. TNT was made available through the Willi Hennig Society. NR 143 TC 2 Z9 2 U1 3 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0748-3007 EI 1096-0031 J9 CLADISTICS JI Cladistics PD JUN PY 2016 VL 32 IS 3 BP 276 EP 296 DI 10.1111/cla.12127 PG 21 WC Evolutionary Biology SC Evolutionary Biology GA DM3TH UT WOS:000376269000004 ER PT J AU Greenberg, R Cammen, KM Wilson, AG Olsen, BJ Ballentine, B McInerney, NC Fleischer, RC AF Greenberg, Russell Cammen, Kristina M. Wilson, Amy G. Olsen, Brian J. Ballentine, Barbara McInerney, Nancy C. Fleischer, Robert C. TI Geographic population structure and subspecific boundaries in a tidal marsh sparrow SO CONSERVATION GENETICS LA English DT Article DE Swamp sparrow; Melospiza georgiana; Microsatellite DNA; Local adaptation; Subspecies; Tidal marsh; Endemism ID BLUETHROAT LUSCINIA-SVECICA; ENDANGERED SPECIES ACT; SHARP-TAILED SPARROWS; PLAIN SWAMP SPARROW; SAN-FRANCISCO BAY; MELOSPIZA-MELODIA; SONG SPARROW; MICROSATELLITE LOCI; GENETIC-STRUCTURE; MORPHOLOGICAL ADAPTATION AB Subspecific genetic diversity is a source for ongoing evolutionary processes, can be predictive of a population's ability to respond to conservation challenges, and may represent the raw material for incipient speciation. As such, diagnosable subspecies are increasingly recognized as an important unit for conservation. Differentiating among subspecies can be particularly difficult in ecosystems characterized by recent phenotypic divergence, such as the tidal marshes of North America. These systems require approaches that can capture selective changes which occurred over only a few millennia as species adapted to new habitats following the Holocene glacial retreat. Here we test for genetic differentiation in morphologically distinct tidal-marsh-endemic subspecies of the swamp sparrow (Melospiza georgiana) using nuclear microsatellites. This case study serves as a test approach for the quantification of conservation units for tidal marsh ecosystems. Though prior surveys of mtDNA variation showed no detectable phylogeographic structure, we found evidence of genetic differentiation in seven microsatellite loci between two M. georgiana subspecies. The most likely model of population structure suggested two clusters in western Maryland/Pennsylvania and Delaware/Chesapeake Bays, with a zone of uncertain population assignment in New Jersey. The microsatellite intergrade zone is broader than the known area of morphological intergrades. We show that microsatellites can be used to support a subspecific status for tidal-marsh taxa such as the swamp sparrow, where changing post-glacial environments likely selected for locally adapted traits while neutral genetic structure is weak. This approach thus allows for the identification and conservation of hot spots that foster ongoing evolutionary change. C1 [Greenberg, Russell; Wilson, Amy G.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. [Cammen, Kristina M.; Olsen, Brian J.] Univ Maine, Sch Biol & Ecol, Climate Change Inst, Orono, ME 04469 USA. [Ballentine, Barbara] Western Carolina Univ, Dept Biol, Cullowhee, NC 28723 USA. [McInerney, Nancy C.; Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC 20008 USA. RP Olsen, BJ (reprint author), Univ Maine, Sch Biol & Ecol, Climate Change Inst, Orono, ME 04469 USA. EM brian.olsen@maine.edu OI Olsen, Brian/0000-0001-5608-2779 FU Smithsonian Institution; Center for Conservation and Evolutionary Genetics; USDA National Institute of Food and Agriculture [ME0-H-6-00492-12] FX N. Perlut provided many of the samples used in this analysis. M. Chu, P. Cordero, J. Maldonado, J. Reed, and L. Terwilliger assisted with genetic analyses. Funding was provided by the endowment funds of the Smithsonian Institution, the Center for Conservation and Evolutionary Genetics, and the USDA National Institute of Food and Agriculture project number ME0-H-6-00492-12. This is Maine Agricultural and Forest Experiment Station publication number 3458. Three anonymous reviewers provided useful comments that improved the manuscript. R. Greenberg conceived of this manuscript, wrote the initial draft, supervised field sampling, helped oversee the initial analysis before revision, and generally acted as a tireless advocate of "the few and highly selected" tidal marsh birds. He passed away before the final version was completed. We mourn our loss but celebrate his contributions to modern ornithology. He is continuously missed. NR 99 TC 1 Z9 1 U1 9 U2 20 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 EI 1572-9737 J9 CONSERV GENET JI Conserv. Genet. PD JUN PY 2016 VL 17 IS 3 BP 603 EP 613 DI 10.1007/s10592-016-0809-6 PG 11 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA DM1ED UT WOS:000376087200009 ER PT J AU O'Farrell, S Luckhurst, BE Box, SJ Mumby, PJ AF O'Farrell, Shay Luckhurst, Brian E. Box, Stephen J. Mumby, Peter J. TI Parrotfish sex ratios recover rapidly in Bermuda following a fishing ban SO CORAL REEFS LA English DT Article DE Coral reefs; Fishing; Fish traps; Ecosystem-based management; Herbivory; Scarinae ID CORAL-REEF FISHES; BIOMASS; SALMON; SIZE AB Parrotfishes are an ecologically and commercially important teleost group whose grazing contributes to maintaining coral-dominated states on hermatypic reefs. However, overfishing has skewed sex ratios of Atlantic parrotfishes because fishing has disproportionate impacts on larger individuals, and males are generally larger than females. Whether protection from fishing may allow sex ratios to return to equilibrium is unknown, as fishing can induce irreversible ecological and/or evolutionary shifts. Bermuda banned trap fishing in 1990, creating a unique opportunity to analyse long-term responses of Atlantic parrotfishes to release from fishing. We found that sex ratios of four common parrotfishes were initially skewed, with male proportions ranging from 0.04 to 0.18. However, male proportions rebounded within 3-4 yr, equilibrating at values ranging from 0.36 to 0.54, similar to those reported at unfished sites in the region. Our results are encouraging for regional efforts to recover lost grazing function by restoring overfished herbivore populations. C1 [O'Farrell, Shay; Mumby, Peter J.] Univ Queensland, Sch Biol Sci, Brisbane, Qld 4072, Australia. [O'Farrell, Shay; Box, Stephen J.] Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. [O'Farrell, Shay] Univ Calif Davis, Dept Environm Sci & Policy, One Shields Ave, Davis, CA 95616 USA. [Luckhurst, Brian E.] Div Fisheries, POB CR52, Crawl, Bermuda. [Luckhurst, Brian E.] 2-4 Via Chiesa, I-05023 Acqualoreto, Umbria, Italy. [Mumby, Peter J.] Univ Queensland, Australian Res Council, Ctr Excellence Coral Reef Studies, Brisbane, Qld 4072, Australia. RP O'Farrell, S (reprint author), Univ Queensland, Sch Biol Sci, Brisbane, Qld 4072, Australia.; O'Farrell, S (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA.; O'Farrell, S (reprint author), Univ Calif Davis, Dept Environm Sci & Policy, One Shields Ave, Davis, CA 95616 USA. EM shay.ofarrell.ac@gmail.com FU Natural Environment Research Council; Cefas; Smithsonian Institution; Australian Research Council Laureate Fellowship FX The authors wish to thank Iliana Chollett for valuable comments and Jules M. van Rooij for providing Bonaire data. S. O'F. was supported by the Natural Environment Research Council, Cefas, and the Smithsonian Institution. P. J. M. was funded by an Australian Research Council Laureate Fellowship. The authors declare no conflicts of interest. NR 30 TC 0 Z9 0 U1 12 U2 21 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 EI 1432-0975 J9 CORAL REEFS JI Coral Reefs PD JUN PY 2016 VL 35 IS 2 BP 421 EP 425 DI 10.1007/s00338-015-1389-5 PG 5 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA DM3KF UT WOS:000376244600005 ER PT J AU Olsen, K Sneed, JM Paul, VJ AF Olsen, K. Sneed, J. M. Paul, V. J. TI Differential larval settlement responses of Porites astreoides and Acropora palmata in the presence of the green alga Halimeda opuntia SO CORAL REEFS LA English DT Article DE Settlement; Coral recruitment; Macroalgae; Porites astreoides; Acropora palmata ID CORAL RECRUITMENT; ELEVATED-TEMPERATURE; CARIBBEAN CORAL; REEF CORALS; MACROALGAE; RESILIENCE; DISPERSAL; SURVIVAL AB Settlement is critical to maintaining coral cover on reefs, yet interspecific responses of coral planulae to common benthic macroalgae are not well characterized. Larval survival and settlement of two Caribbean reef-building corals, the broadcast-spawner Acropora palmata and the planulae-brooder Porites astreoides, were quantified following exposure to plastic algae controls and the green macroalga Halimeda opuntia. Survival and settlement rates were not significantly affected by the presence of H. opuntia in either species. However, similar to 10 % of P. astreoides larvae settled on the surface of the macroalga, whereas larvae of A. palmata did not. It is unlikely that corals that settle on macroalgae will survive post-settlement; therefore, H. opuntia may reduce the number of P. astreoides and other non-discriminatory larvae that survive to adulthood. Our results suggest that the presence of macroalgae on impacted reefs can have unexpected repercussions for coral recruitment and highlight discrepancies in settlement specificity between corals with distinct life history strategies. C1 [Olsen, K.; Sneed, J. M.; Paul, V. J.] Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. [Olsen, K.] Florida State Univ, Dept Biol Sci, 319 Stadium Dr, Tallahassee, FL 32306 USA. RP Paul, VJ (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM Paul@si.edu FU Mote Protect Our Reef Grant program [POR 2013-27]; Smithsonian Competitive Grants Program for Science; CCRE program [983] FX Funding was provided by Mote Protect Our Reef Grant program (POR 2013-27) and Smithsonian Competitive Grants Program for Science. We thank L. Johnston, M. Jones, Z. Foltz, A. Wood, M. Henley, D. Dixson, K. Ritchie, M. Schwartz, J. Skutas, A. Augustines and L. Spiers for assistance with larval collection and experiments. We thank the Belize Fisheries Department for providing permits to conduct research at Carrie Bow Cay, Belize. In the Florida Keys, coral larvae were collected under Permit No. FKNMS-2013-021. This is Contribution No. 1019 from the Smithsonian Marine Station and No. 983 from the CCRE program. NR 26 TC 0 Z9 0 U1 8 U2 19 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 EI 1432-0975 J9 CORAL REEFS JI Coral Reefs PD JUN PY 2016 VL 35 IS 2 BP 521 EP 525 DI 10.1007/s00338-015-1394-8 PG 5 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA DM3KF UT WOS:000376244600015 ER PT J AU Toscano, MA AF Toscano, Marguerite A. TI Revised paleoenvironmental analysis of the Holocene portion of the Barbados sea-level record: Cobbler's Reef revisited SO CORAL REEFS LA English DT Article DE Acropora palmata; Holocene sea levels; Reef decline; Paleotempestology; Paleoclimatology ID NORTHEASTERN ST-CROIX; CARIBBEAN CORAL-REEFS; LONG-TERM DECLINE; US VIRGIN-ISLANDS; WEST-INDIES; ACROPORA-PALMATA; ICE-AGE; PLEISTOCENE CORAL; FLORIDA-KEYS; NETHERLANDS-ANTILLES AB Sample elevations corrected for tectonic uplift and assessed relative to local modeled sea levels provide a new perspective on paleoenvironmental history at Cobbler's Reef, Barbados. Previously, C-14-dated surface samples of fragmented Acropora palmata plotted above paleo sea level based on their present (uplifted) elevations, suggesting supratidal rubble deposited during a period of extreme storms (4500-3000 cal BP), precipitating reef demise. At several sites, however, A. palmata persisted, existing until similar to 370 cal BP. Uplift-corrected A. palmata sample elevations lie below the western Atlantic sea-level curve, and similar to 2 m below ICE-6G-modeled paleo sea level, under slow rates of sea-level rise, negating the possibility that Cobbler's Reef is a supratidal storm ridge. Most sites show limited age ranges from corals likely damaged/killed on the reef crest, not the mixed ages of rubble ridges, strongly suggesting the reef framework died off in stages over 6500 yr. Reef crest death assemblages invoke multiple paleohistoric causes, from ubiquitous hurricanes to anthropogenic impacts. Comparison of death assemblage ages to dated regional paleotempestological sequences, proxy-based paleotemperatures, recorded hurricanes, tsunamis, European settlement, deforestation, and resulting turbidity, reveals many possible factors inimical to the survival of A. palmata along Cobbler's Reef. C1 [Toscano, Marguerite A.] Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. RP Toscano, MA (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM toscanom@si.edu FU National Science Foundation [0921879] FX The author thanks Ian Macintyre and Peter Glynn for their original field investigation of Cobbler's Reef, site descriptions, photographs, field notes, and their review of this paper; Klaus Rutzler, Ian Macintyre, Pamela Reid, and David Weintstein for taphonomic assessments; Venka Macintyre for expert editorial review; Mary Parrish for drafting Fig. 1; Dick Peltier and Rosemarie Drummond for geophysical models; and several anonymous reviewers of earlier drafts. This work was supported by National Science Foundation Project 0921879. NR 110 TC 1 Z9 1 U1 0 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 EI 1432-0975 J9 CORAL REEFS JI Coral Reefs PD JUN PY 2016 VL 35 IS 2 BP 641 EP 653 DI 10.1007/s00338-016-1397-0 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA DM3KF UT WOS:000376244600027 ER PT J AU Wielgus, M Sadowski, A Kluzniak, W Abramowicz, M Narayan, R AF Wielgus, Maciek Sadowski, Aleksander Kluzniak, Wlodek Abramowicz, Marek Narayan, Ramesh TI Levitating atmospheres of Eddington-luminosity neutron stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitation; stars: atmospheres; stars: neutron; X-rays: bursts ID X-RAY BURST; COMPTON-SCATTERING; RADIUS EXPANSION; CAPTURE SPHERE; MODELS; OUTBURSTS; BINARY; MATTER; WINDS AB We construct models of static, spherically symmetric shells supported by the radiation flux of a luminous neutron star in the Schwarzschild metric. The atmospheres are disconnected from the star and levitate above its surface. Gas pressure and density inversion appear in the inner region of these atmospheres, which is a purely relativistic phenomenon. We account for the scattering opacity dependence on temperature green by using the Klein-Nishina formula. The relativistic M-1 closure scheme for the radiation tensor provides a general relativity-consistent treatment of the photon flux and radiation tensor anisotropy. In this way, we are able to address atmospheres of both large and moderate/low optical depths with the same set of equations. We discuss properties of the levitating atmospheres and find that they may indeed be optically thick, with the distance between star surface and the photosphere expanding as luminosity increases. These results may be relevant for the photosphereric radius expansion X-ray bursts. C1 [Wielgus, Maciek; Kluzniak, Wlodek; Abramowicz, Marek] Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland. [Sadowski, Aleksander] MIT Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Sadowski, Aleksander; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Abramowicz, Marek] Gothenburg Univ, Dept Phys, SE-41296 Gothenburg, Sweden. [Abramowicz, Marek] Silesian Univ Opava, Fac Philosophy & Sci, Inst Phys, Bezrucovo 13, CZ-74601 Opava, Czech Republic. RP Wielgus, M; Kluzniak, W (reprint author), Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland.; Sadowski, A (reprint author), MIT Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.; Sadowski, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM maciek.wielgus@gmail.com; asadowsk@mit.edu; wlodek@camk.edu.pl OI Narayan, Ramesh/0000-0002-1919-2730 FU Polish NCN grants [UMO-2011/01/B/ST9/05439, UMO-2013/08/A/ST9/00795]; Czech 'Synergy' (Opava) project [ASCRM100031242 CZ.1.07/2.3.00/20.0071]; Foundation for Polish Science within the START programme FX We thank Omer Blaes, Feryal Ozel, and David Abarca for interesting comments on the subject of this paper. This research was partly supported by Polish NCN grants UMO-2011/01/B/ST9/05439 and UMO-2013/08/A/ST9/00795 as well as the Czech ASCRM100031242 CZ.1.07/2.3.00/20.0071 'Synergy' (Opava) project. MW also acknowledges the support of the Foundation for Polish Science within the START programme. NR 32 TC 2 Z9 2 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2016 VL 458 IS 4 BP 3420 EP 3428 DI 10.1093/mnras/stw548 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL7DG UT WOS:000375799500002 ER PT J AU Mortlock, A Conselice, CJ Hartley, WG Duncan, K Lani, C Ownsworth, JR Almaini, O van der Wel, A Huang, KH Ashby, MLN Willner, SP Fontana, A Dekel, A Koekemoer, AM Ferguson, HC Faber, SM Grogin, NA Kocevski, DD AF Mortlock, Alice Conselice, Christopher. J. Hartley, William G. Duncan, Ken Lani, Caterina Ownsworth, Jamie R. Almaini, Omar van der Wel, Arjen Huang, Kuang-Han Ashby, Matthew L. N. Willner, S. P. Fontana, Adriano Dekel, Avishai Koekemoer, Anton M. Ferguson, Harry C. Faber, Sandra M. Grogin, Norman A. Kocevski, Dale D. TI Deconstructing the Galaxy stellar mass function with UKIDSS and CANDELS: the impact of colour, structure and environment (vol 447, pg 2, 2015) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Correction DE erratam, addenda; galaxies: formation; galaxies: luminosity function, mass function; galaxies: structure C1 [Mortlock, Alice; Conselice, Christopher. J.; Hartley, William G.; Duncan, Ken; Lani, Caterina; Ownsworth, Jamie R.; Almaini, Omar] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Mortlock, Alice] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Hartley, William G.] ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [van der Wel, Arjen] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Huang, Kuang-Han] Univ Calif Davis, Dept Phys, One Shields Ave, Davis, CA 95616 USA. [Ashby, Matthew L. N.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Fontana, Adriano] INAF, Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. [Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Koekemoer, Anton M.; Ferguson, Harry C.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Faber, Sandra M.; Grogin, Norman A.] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Kocevski, Dale D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. RP Mortlock, A (reprint author), Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.; Mortlock, A (reprint author), Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. EM alicem@roe.ac.uk NR 1 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2016 VL 458 IS 4 BP 3478 EP 3478 DI 10.1093/mnros/stw390 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL7DG UT WOS:000375799500007 ER PT J AU Rowlinson, A Bell, ME Murphy, T Trott, CM Hurley-Walker, N Johnston, S Tingay, SJ Kaplan, DL Carbone, D Hancock, PJ Feng, L Offringa, AR Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Deshpande, AA Gaensler, BM Greenhill, LJ Hazelton, BJ Johnston-Hollitt, M Lonsdale, CJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Prabu, T Shankar, NU Srivani, KS Subrahmanyan, R Wayth, RB Webster, RL Williams, A Williams, CL AF Rowlinson, A. Bell, M. E. Murphy, T. Trott, C. M. Hurley-Walker, N. Johnston, S. Tingay, S. J. Kaplan, D. L. Carbone, D. Hancock, P. J. Feng, L. Offringa, A. R. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Deshpande, A. A. Gaensler, B. M. Greenhill, L. J. Hazelton, B. J. Johnston-Hollitt, M. Lonsdale, C. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Prabu, T. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Wayth, R. B. Webster, R. L. Williams, A. Williams, C. L. TI Limits on Fast Radio Bursts and other transient sources at 182 MHz using the Murchison Widefield Array SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: interferometers; techniques: image processing; catalogues radio continuum: general ID FREQUENCY SKY SURVEY; GAMMA-RAY BURSTS; REIONIZATION HISTORY; SEARCH; LOFAR; ENVIRONMENT; DISPERSION; DISCOVERY; TELESCOPE; EMISSION AB We present a survey for transient and variable sources, on time-scales from 28 s to similar to 1 yr, using the Murchison Widefield Array (MWA) at 182 MHz. Down to a detection threshold of 0.285 Jy, no transient candidates were identified, making this the most constraining low-frequency survey to date and placing a limit on the surface density of transients of < 4.1 x 10(-7) deg(-2) for the shortest time-scale considered. At these frequencies, emission from Fast Radio Bursts (FRBs) is expected to be detectable in the shortest time-scale images without any corrections for interstellar or intergalactic dispersion. At an FRB limiting flux density of 7980 Jy, we find a rate of < 82 FRBs per sky per day for dispersion measures < 700 pc cm(-3). Assuming a cosmological population of standard candles, our rate limits are consistent with the FRB rates obtained by Thornton et al. if they have a flat spectral slope. Finally, we conduct an initial variability survey of sources in the field with flux densities greater than or similar to 0.5 Jy and identify no sources with significant variability in their light curves. However, we note that substantial further work is required to fully characterize both the short-term and low-level variability within this field. C1 [Rowlinson, A.] Univ Amsterdam, Anton Pannekoek Inst, Postbus 94249, NL-1090 GE Amsterdam, Netherlands. [Rowlinson, A.] Netherlands Inst Radio Astron ASTRON, POB 2, NL-7990 AA Dwingeloo, Netherlands. [Rowlinson, A.; Bell, M. E.; Johnston, S.; Mitchell, D. A.] CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia. [Rowlinson, A.; Bell, M. E.; Murphy, T.; Trott, C. M.; Tingay, S. J.; Hancock, P. J.; Gaensler, B. M.; Mitchell, D. A.; Ord, S. M.; Subrahmanyan, R.; Wayth, R. B.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Melbourne, Vic, Australia. [Murphy, T.; Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Trott, C. M.; Hurley-Walker, N.; Tingay, S. J.; Hancock, P. J.; Gaensler, B. M.; Ord, S. M.; Wayth, R. B.; Williams, A.] Curtin Univ, ICRAR, Bentley, WA 6102, Australia. [Kaplan, D. L.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Feng, L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Bernardi, G.] SKA SA, 3rd Floor,The Pk,Pk Rd, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Cappallo, R. J.; Lonsdale, C. J.; McWhirter, S. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Gaensler, B. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [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. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. RP Rowlinson, A (reprint author), Univ Amsterdam, Anton Pannekoek Inst, Postbus 94249, NL-1090 GE Amsterdam, Netherlands.; Rowlinson, A (reprint author), Netherlands Inst Radio Astron ASTRON, POB 2, NL-7990 AA Dwingeloo, Netherlands.; Rowlinson, A (reprint author), CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia.; Rowlinson, A (reprint author), ARC Ctr Excellence All Sky Astrophys CAASTRO, Melbourne, Vic, Australia. EM b.a.rowlinson@uva.nl RI Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Subrahmanyan, Ravi/D-4889-2012; OI Wayth, Randall/0000-0002-6995-4131; Trott, Cathryn/0000-0001-6324-1766; Hancock, Paul/0000-0002-4203-2946 FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific 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); Commonwealth Scientific and Industrial Research Organization (CSIRO), 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), a Joint Venture of Curtin University; University of Western Australia; Western Australian State government; Australian Government; NCI National Facility at the ANU 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 U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant 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 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 Commonwealth Scientific and Industrial Research Organization (CSIRO), 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.; This research was undertaken with the assistance of resources from the National Computational Infrastructure (NCI), which is supported by the Australian Government. This work was supported by the Flagship Allocation Scheme of the NCI National Facility at the ANU. NR 65 TC 11 Z9 11 U1 1 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 JUN 1 PY 2016 VL 458 IS 4 BP 3506 EP 3522 DI 10.1093/mnras/stw451 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL7DG UT WOS:000375799500010 ER PT J AU Chen, X Chary, R Pearson, TJ McGehee, P Fowler, JW Helou, G AF Chen, X. Chary, R. Pearson, T. J. McGehee, P. Fowler, J. W. Helou, G. TI The bandmerged Planck Early Release Compact Source Catalogue: probing sub-structure in the molecular gas at high Galactic latitude SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: general; catalogues; surveys; radio continuum: galaxies ID RADIATION; GALAXIES; EMISSION; HEMISPHERE AB The Planck Early Release Compact Source Catalogue (ERCSC) includes nine lists of highly reliable sources, individually extracted at each of the nine Planck frequency channels. To facilitate the study of the Planck sources, especially their spectral behaviour across the radio/infrared frequencies, we provide a `bandmerged' catalogue of the ERCSC sources. This catalogue consists of 15 191 entries, with 79 sources detected in all nine frequency channels of Planck and 6818 sources detected in only one channel. We describe the bandmerging algorithm, including the various steps used to disentangle sources in confused regions. The multifrequency matching allows us to develop spectral energy distributions of sources between 30 and 857 GHz, in particular across the 100 GHz band, where the energetically important CO J = 1 -> 0 line enters the Planck bandpass. We find similar to 3 sigma-5 sigma evidence for contribution to the 100 GHz intensity from foreground CO along the line of sight to 147 sources with vertical bar b vertical bar > 3 degrees. The median excess contribution is 4.5 +/- 0.9 per cent of their measured 100 GHz flux density which cannot be explained by calibration or beam uncertainties. This translates to 0.5 +/- 0.1 K km s(-1) of CO which must be clumped on the scale of the Planck 100 GHz beam, i.e. similar to 10 arcmin. If this is due to a population of low-mass (similar to 15 Me) molecular gas clumps, the total mass in these clumps may be more than 2000 Me. Further, high-spatial-resolution, ground-based observations of the high-latitude sky will help shed light on the origin of this diffuse, clumpy CO emission. C1 [Chen, X.; Chary, R.; Pearson, T. J.; McGehee, P.; Fowler, J. W.; Helou, G.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Chary, R.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Pearson, T. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RP Chen, X; Chary, R (reprint author), CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.; Chary, R (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM xchen@ipac.caltech.edu; rchary@caltech.edu RI Pearson, Timothy/N-2376-2015 OI Pearson, Timothy/0000-0001-5213-6231 FU European Space Agency (ESA); ESA member states FX Planck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states (in particular the lead countries France and Italy), with contributions from NASA (USA) and telescope reflectors provided by a collaboration between ESA and a scientific consortium led and funded by Denmark. NR 25 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2016 VL 458 IS 4 BP 3619 EP 3632 DI 10.1093/mnras/stw479 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL7DG UT WOS:000375799500020 ER PT J AU Maccarone, TJ Yukita, M Hornschemeier, A Lehmer, BD Antoniou, V Ptak, A Wik, DR Zezas, A Boyd, P Kennea, J Page, KL Eracleous, M Williams, BF Boggs, SE Christensen, FE Craig, WW Hailey, CJ Harrison, FA Stern, D Zhang, WW AF Maccarone, Thomas J. Yukita, Mihoko Hornschemeier, Ann Lehmer, Bret D. Antoniou, Vallia Ptak, Andrew Wik, Daniel R. Zezas, Andreas Boyd, Padi Kennea, Jamie Page, Kim L. Eracleous, Mike Williams, Benjamin F. Boggs, Steven E. Christensen, Finn E. Craig, William W. Hailey, Charles J. Harrison, Fiona A. Stern, Daniel Zhang, William W. TI Demonstrating the likely neutron star nature of five M31 globular cluster sources with Swift-NuSTAR spectroscopy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE globular clusters: general; galaxies: individual: M 31; X-rays: binaries ID X-RAY BINARY; MASS BLACK-HOLES; HUBBLE-SPACE-TELESCOPE; ACCRETION DISC WINDS; MICROQUASAR GRS 1915+105; STELLAR-MASS; CATACLYSMIC VARIABLES; OMEGA-CENTAURI; CYGNUS X-1; DYNAMICAL MODELS AB We present the results of a joint Swift-NuSTAR spectroscopy campaign on M31. We focus on the five brightest globular cluster X-ray sources in our fields. Two of these had previously been argued to be black hole candidates on the basis of apparent hard-state spectra at luminosities above those for which neutron stars are in hard states. We show that these two sources are likely to be Z-sources (i.e. low magnetic field neutron stars accreting near their Eddington limits), or perhaps bright atoll sources (low magnetic field neutron stars which are just a bit fainter than this level) on the basis of simultaneous Swift and NuSTAR spectra which cover a broader range of energies. These new observations reveal spectral curvature above 6-8 keV that would be hard to detect without the broader energy coverage the NuSTAR data provide relative to Chandra and XMM-Newton. We show that the other three sources are also likely to be bright neutron star X-ray binaries, rather than black hole X-ray binaries. We discuss why it should already have been realized that it was unlikely that these objects were black holes on the basis of their being persistent sources, and we re-examine past work which suggested that tidal capture products would be persistently bright X-ray emitters. We discuss how this problem is likely due to neglecting disc winds in older work that predict which systems will be persistent and which will be transient. C1 [Maccarone, Thomas J.] Texas Tech Univ, Dept Phys, Box 41051,Sci Bldg, Lubbock, TX 79409 USA. [Yukita, Mihoko; Lehmer, Bret D.] Johns Hopkins Univ, Homewood Campus, Baltimore, MD 21218 USA. [Yukita, Mihoko; Hornschemeier, Ann; Lehmer, Bret D.; Ptak, Andrew; Wik, Daniel R.; Boyd, Padi; Zhang, William W.] NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. [Antoniou, Vallia] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Zezas, Andreas] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Zezas, Andreas] Univ Crete, Inst Theoret & Computat Phys, Iraklion 71003, Greece. [Zezas, Andreas] Fdn Res & Technol Hellas, EL-71110 Iraklion, Crete, Greece. [Kennea, Jamie; Eracleous, Mike] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Page, Kim L.] Univ Leicester, Dept Phys & Astron, Leicester LE2 2LL, Leics, England. [Williams, Benjamin F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DK-2100 Copenhagen, Denmark. [Hailey, Charles J.] Columbia Univ, Dept Phys, 538 W 120th St, New York, NY 10027 USA. [Harrison, Fiona A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Maccarone, TJ (reprint author), Texas Tech Univ, Dept Phys, Box 41051,Sci Bldg, Lubbock, TX 79409 USA. EM thomas.maccarone@ttu.edu RI Boggs, Steven/E-4170-2015; Yukita, Mihoko/E-4135-2017; Zezas, Andreas/C-7543-2011 OI Boggs, Steven/0000-0001-9567-4224; Zezas, Andreas/0000-0001-8952-676X FU European Research Council under European Union/ERC [617001] FX TJM thanks Christian Knigge for an illuminating talk at 'The Physics of Cataclysmic and Compact Binaries', and Helena Uthas, Joe Patterson, Christian Knigge and Jeno Sokoloski for having organized the meeting. He also thanks Joey Neilsen, Chris Done, and Maria Diaz Trigo for useful discussions about disc winds. AZ acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2103)/ERC Grant Agreement no. 617001. NR 126 TC 1 Z9 1 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2016 VL 458 IS 4 BP 3633 EP 3643 DI 10.1093/mnras/stw530 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL7DG UT WOS:000375799500021 ER PT J AU LaMassa, SM Urry, CM Cappelluti, N Civano, F Ranalli, P Glikman, E Treister, E Richards, G Ballantyne, D Stern, D Comastri, A Cardamone, C Schawinski, K Bohringer, H Chon, GY Murray, SS Green, P Nandra, K AF LaMassa, Stephanie M. Urry, C. Megan Cappelluti, Nico Civano, Francesca Ranalli, Piero Glikman, Eilat Treister, Ezequiel Richards, Gordon Ballantyne, David Stern, Daniel Comastri, Andrea Cardamone, Carie Schawinski, Kevin Boehringer, Hans Chon, Gayoung Murray, Stephen S. Green, Paul Nandra, Kirpal TI Finding rare AGN: XMM-Newton and Chandra observations of SDSS Stripe 82 (vol 436, pg 3581, 2013) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Correction DE errata, addenda; catalogues; surveys; galaxies: active; quasars: general; X-rays: galaxies C1 [LaMassa, Stephanie M.; Urry, C. Megan; Glikman, Eilat] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, POB 208120, New Haven, CT 06520 USA. [Cappelluti, Nico; Comastri, Andrea] Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy. [Cappelluti, Nico] Univ Maryland, Baltimore Coll, Ctr Space Sci & Technol, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. [Civano, Francesca; Murray, Stephen S.; Green, Paul] Dartmouth Coll, Wilder Lab, Dept Phys & Astron, Hanover, NH 03755 USA. [Civano, Francesca] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Ranalli, Piero] Natl Observ Athens, Inst Astron, Astrophys, GR-15236 Athens, Greece. [Treister, Ezequiel] Univ Concepcion, Casilla 160-c, Concepcion 4030000, Chile. [Richards, Gordon] Drexel Univ, Dept Phys, 3141 Chestnut St, Philadelphia, PA 19104 USA. [Ballantyne, David] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-221, Pasadena, CA 91109 USA. [Cardamone, Carie] Brown Univ, Harriet W Sheridan Ctr Teaching & Learning, Box 1912,96 Waterman St, Providence, RI 02912 USA. [Schawinski, Kevin] ETH, Inst Astron, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland. [Boehringer, Hans; Chon, Gayoung; Nandra, Kirpal] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. RP LaMassa, SM (reprint author), Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, POB 208120, New Haven, CT 06520 USA. EM stephanie.m.lamassa@nasa.gov RI Ranalli, Piero/K-6363-2013 OI Ranalli, Piero/0000-0003-3956-755X NR 2 TC 0 Z9 0 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2016 VL 458 IS 4 BP 3820 EP 3820 DI 10.1093/mnras/stw617 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL7DG UT WOS:000375799500037 ER PT J AU Rappaport, S Gary, BL Kaye, T Vanderburg, A Croll, B Benni, P Foote, J AF Rappaport, S. Gary, B. L. Kaye, T. Vanderburg, A. Croll, B. Benni, P. Foote, J. TI Drifting asteroid fragments around WD 1145+017 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE comets: general; minor planets, asteroids: general; planets and satellites: general; planetary systems; white dwarfs ID EXTRASOLAR MINOR PLANET; WHITE-DWARFS; DEBRIS DISKS; SYSTEMS; FREQUENCY; COMETS; DISCS; STARS AB We have obtained extensive photometric observations of the polluted white dwarf WD 1145+017 which has been reported to be transited by at least one, and perhaps several, large asteroids with dust emission. Observation sessions on 37 nights spanning 2015 November to 2016 January with small to modest size telescopes have detected 237 significant dips in flux. Periodograms reveal a significant periodicity of 4.5004 h consistent with the dominant ('A') period detected with K2. The folded light curve shows an hour-long depression in flux with a mean depth of nearly 10 per cent. This depression is, in turn, comprised of a series of shorter and sometimes deeper dips which would be unresolvable with K2. We also find numerous dips in flux at other orbital phases. Nearly all of the dips associated with this activity appear to drift systematically in phase with respect to the 'A' period by about 2.5 min d(-1) with a dispersion of similar to 0.5 min d(-1), corresponding to a mean drift period of 4.4928 h. We are able to track 15 discrete drifting features. The periods found with K2 are not detected, but we would not necessarily have expected to see them. We explain the drifting motion as due to smaller fragmented bodies that break off from the asteroid and go into a slightly smaller orbit. In this interpretation, we can use the drift rate to determine the mass of the asteroid, which we find to be approximate to 10(23) g, or about 1/10th the mass of Ceres. C1 [Rappaport, S.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Rappaport, S.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Gary, B. L.] Hereford Arizona Observ, Hereford, AZ 85615 USA. [Kaye, T.] Raemor Vista Observ, 7023 E Alhambra Dr, Sierra Vista, AZ 85650 USA. [Vanderburg, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Croll, B.] Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave Room 506, Boston, MA 02215 USA. [Benni, P.] Acton Sky Portal, 3 Concetta Circle, Acton, MA 01720 USA. [Foote, J.] Vermill Cliffs Observ, 4175 E Red Cliffs Dr, Kanab, UT 84741 USA. RP Rappaport, S (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.; Rappaport, S (reprint author), MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.; Gary, BL (reprint author), Hereford Arizona Observ, Hereford, AZ 85615 USA. EM sar@mit.edu; bgary1@cis-broadband.com OI Kaye, Thomas /0000-0001-7996-618X FU National Science Foundation [DGE 1144152] FX We thank an anonymous referee for some very helpful and insightful comments. AV is supported by the National Science Foundation Graduate Research Fellowship, Grant No. DGE 1144152. TK thanks Cheryl Healy and Beth Christie for material support in telescope operations and equipment. NR 32 TC 17 Z9 17 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2016 VL 458 IS 4 BP 3904 EP 3917 DI 10.1093/mnras/stw612 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL7DG UT WOS:000375799500045 ER PT J AU Wevers, T Hodgkin, ST Jonker, PG Bassa, C Nelemans, G van Grunsven, T Gonzalez-Solares, EA Torres, MAP Heinke, C Steeghs, D Maccarone, TJ Britt, C Hynes, RI Johnson, C Wu, JF AF Wevers, T. Hodgkin, S. T. Jonker, P. G. Bassa, C. Nelemans, G. van Grunsven, T. Gonzalez-Solares, E. A. Torres, M. A. P. Heinke, C. Steeghs, D. Maccarone, T. J. Britt, C. Hynes, R. I. Johnson, C. Wu, Jianfeng TI The Chandra Galactic Bulge Survey: optical catalogue and point-source counterparts to X-ray sources SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE catalogues; surveys; stars: imaging; Galaxy: bulge; X-rays: binaries ID MILKY-WAY BULGE; H-ALPHA SURVEY; PLANE IPHAS; ACCRETING BINARIES; HIGH-RESOLUTION; DATA RELEASE; IDENTIFICATION; POPULATION; EXTINCTION; STARS AB As part of the Chandra Galactic Bulge Survey (GBS), we present a catalogue of optical sources in the GBS footprint. This consists of two regions centred at Galactic latitude b = 1 degrees. 5 above and below the Galactic Centre, spanning (l x b) = (6 degrees x 1 degrees). The catalogue consists of two or more epochs of observations for each line of sight in r', i' and H alpha filters. The catalogue is complete down to r' = 20.2 and i' = 19.2 mag; the mean 5 sigma depth is r' = 22.5 and i' = 21.1mag. The mean root-mean-square residuals of the astrometric solutions is 0.04 arcsec. We cross-correlate this optical catalogue with the 1640 unique X-ray sources detected in Chandra observations of the GBS area, and find candidate optical counterparts to 1480 X-ray sources. We use a false alarm probability analysis to estimate the contamination by interlopers, and expect similar to 10 per cent of optical counterparts to be chance alignments. To determine the most likely counterpart for each X-ray source, we compute the likelihood ratio for all optical sources within the 4 sigma X-ray error circle. This analysis yields 1480 potential counterparts (similar to 90 per cent of the sample). 584 counterparts have saturated photometry (r' <= 17, i' <= 16), indicating these objects are likely foreground sources and the real counterparts. 171 candidate counterparts are detected only in the i' band. These sources are good qLMXB and CV candidates as they are X-ray bright and likely located in the Bulge. C1 [Wevers, T.; Jonker, P. G.; Nelemans, G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands. [Hodgkin, S. T.; Gonzalez-Solares, E. A.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Jonker, P. G.; van Grunsven, T.; Torres, M. A. P.] SRON Netherlands Inst Space Res, SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. [Bassa, C.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Nelemans, G.] Katholieke Univ Leuven, Inst Astron, Celestijnenlaan 200D, B-3001 Leuven, Belgium. [Heinke, C.] Univ Alberta, Dept Phys, CCLS 4-183, Edmonton, AB T6G 2E1, Canada. [Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Maccarone, T. J.; Britt, C.] Texas Tech Univ, Dept Phys, Box 41051, Lubbock, TX 79409 USA. [Britt, C.; Hynes, R. I.; Johnson, C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Wu, Jianfeng] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Wu, Jianfeng] Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA. RP Wevers, T (reprint author), Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands. EM t.wevers@astro.ru.nl OI Nelemans, Gijs/0000-0002-0752-2974 FU European Research Council [647208] FX We would like to thank the referee for his/her comments which helped to improve the manuscript. We thank professors P. Groot and F. Verbunt for a useful discussion on the Chandra astrometric uncertainties and false alarm probabilities. PGJ acknowledges support from European Research Council Consolidator Grant 647208. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory (2006A-0086, PI: Jonker), which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. NR 35 TC 2 Z9 2 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2016 VL 458 IS 4 BP 4530 EP 4546 DI 10.1093/mnras/stw643 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL7DG UT WOS:000375799500088 ER PT J AU Bryant, A AF Bryant, Aaron TI Devin Allen SO APERTURE LA English DT Article C1 [Bryant, Aaron] Smithsonian Inst, Photog, Natl Museum African Amer Hist & Culture, Washington, DC 20560 USA. RP Bryant, A (reprint author), Smithsonian Inst, Photog, Natl Museum African Amer Hist & Culture, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU APERTURE PI NEW YORK PA 20 EAST 23RD ST, NEW YORK, NY 10010 USA SN 0003-6420 J9 APERTURE JI Aperture PD SUM PY 2016 IS 223 BP 106 EP 109 PG 4 WC Art SC Art GA DL8LT UT WOS:000375894200018 ER PT J AU Nganvongpanit, K Buddhachat, K Brown, JL AF Nganvongpanit, Korakot Buddhachat, Kittisak Brown, Janine L. TI Comparison of Bone Tissue Elements Between Normal and Osteoarthritic Pelvic Bones in Dogs SO BIOLOGICAL TRACE ELEMENT RESEARCH LA English DT Article DE Bone; Dog; Element; Osteoarthritis; Subchondral ID X-RAY-FLUORESCENCE; SUBCHONDRAL BONE; ARTICULAR-CARTILAGE; SPECTROMETRY; MANGANESE; CADMIUM; URBAN; HIP AB Physiochemical analysis of bones affected with osteoarthritis (OA) can be used to better understand the etiology of this disease. We investigated the percentage of chemical elements in canine pelvic bone affected with varying degrees of OA using a handheld X-ray fluorescence (XRF) analyzer that discriminates magnesium (Mg-12) through bismuth (Bi-83). A total of 45 pelvic bones, including both ilium and subchondral acetabular bone plates, were categorized as normal (n = 20), mild grade OA (n = 5), moderate grade OA (n = 15), and severe grade OA (n = 5). In normal pelvic, seven elements (P, Ca, Mn, Ag, Cd, Sn, and Sb) differed (p < 0.005) in percentage between ilium and acetabulum. Comparisons among the four OA groups found Mn and Fe to be highest in severe grades (p < 0.05) in both ilium and acetabulum. Three heavy metals (Ag, Sn, and Sb) were detected in high percentages (p < 0.05) in the severe OA group in the acetabulum, but in ilium only Sn was high (p < 0.05) in severe OA. In conclusion, the percentages of several elements differed between pelvic types in dogs, and also with increasing severity of OA. The finding of high Mn and Fe in severe grade OA bone suggests these two elements may be useful in future studies of the etiology and pathophysiology of OA. C1 [Nganvongpanit, Korakot; Buddhachat, Kittisak] Chiang Mai Univ, Fac Vet Med, Dept Vet Biosci & Publ Hlth, Anim Bone & Joint Res Lab, Chiang Mai 50100, Thailand. [Nganvongpanit, Korakot] Chiang Mai Univ, Excellence Ctr Osteol Res, Chiang Mai 50200, Thailand. [Nganvongpanit, Korakot] Chiang Mai Univ, Training Ctr, Chiang Mai 50200, Thailand. [Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Natl Zool Pk 1500 Remount Rd, Front Royal, VA 22630 USA. RP Nganvongpanit, K (reprint author), Chiang Mai Univ, Fac Vet Med, Dept Vet Biosci & Publ Hlth, Anim Bone & Joint Res Lab, Chiang Mai 50100, Thailand.; Nganvongpanit, K (reprint author), Chiang Mai Univ, Excellence Ctr Osteol Res, Chiang Mai 50200, Thailand.; Nganvongpanit, K (reprint author), Chiang Mai Univ, Training Ctr, Chiang Mai 50200, Thailand. EM korakot.n@cmu.ac.th; k_buddhachat@yahoo.com; BrownJan@si.edu FU Chiang Mai University (CMU) FX The authors are grateful for the research funding from the Chiang Mai University (CMU) through the research administration office that provided a budget to our Excellence Center in Osteology Research and Training Center (ORTC). NR 34 TC 3 Z9 3 U1 1 U2 1 PU HUMANA PRESS INC PI TOTOWA PA 999 RIVERVIEW DRIVE SUITE 208, TOTOWA, NJ 07512 USA SN 0163-4984 EI 1559-0720 J9 BIOL TRACE ELEM RES JI Biol. Trace Elem. Res. PD JUN PY 2016 VL 171 IS 2 BP 344 EP 353 DI 10.1007/s12011-015-0556-4 PG 10 WC Biochemistry & Molecular Biology; Endocrinology & Metabolism SC Biochemistry & Molecular Biology; Endocrinology & Metabolism GA DL6ZC UT WOS:000375787600015 PM 26537116 ER PT J AU Torres-Herrera, EJ Tavora, M Santos, LF AF Torres-Herrera, E. J. Tavora, Marco Santos, Lea F. TI Survival Probability of the N,el State in Clean and Disordered Systems: An Overview SO BRAZILIAN JOURNAL OF PHYSICS LA English DT Article DE Non-equilibrium quantum physics; Quench dynamics; Spin systems; Disordered systems ID QUANTUM-SYSTEMS; ENERGY UNCERTAINTY; WAVE-FUNCTIONS; MOBILITY EDGE; DECAY THEORY; TIME; PARTICLE; EVOLUTION; CHAOS; LOCALIZATION AB In this work we provide an overview of our recent results about the quench dynamics of one-dimensional many-body quantum systems described by spin-1/2 models. To illustrate those general results, here we employ a particular and experimentally accessible initial state, namely the N,el state. Both cases are considered: clean chains without any disorder and disordered systems with static random on-site magnetic fields. The quantity used for the analysis is the probability for finding the initial state later in time, the so-called survival probability. At short times, the survival probability may decay faster than exponentially, Gaussian behaviors and even the limit established by the energy-time uncertainty relation are displayed. The dynamics at long times slows down significantly and shows a powerlaw behavior. For both scenarios, we provide analytical expressions that agree very well with our numerical results. C1 [Torres-Herrera, E. J.] Univ Autonoma Puebla, Inst Fis, Apt Postal J48, Puebla 72570, Mexico. [Santos, Lea F.] Yeshiva Univ, Dept Phys, New York, NY 10016 USA. [Santos, Lea F.] Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. RP Santos, LF (reprint author), Yeshiva Univ, Dept Phys, New York, NY 10016 USA.; Santos, LF (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM lsantos2@yu.edu RI Santos, Lea/D-5332-2012 OI Santos, Lea/0000-0001-9400-2709 FU NSF [DMR-1147430]; CONACyT, Mexico FX This work was motivated by a presentation given by one of the authors at the Workshop: Quantum Information and Thermodynamics held in Sao Carlos in February, 2015. This work was supported by the NSF grant No. DMR-1147430. E.J.T.H. acknowledges support from CONACyT, Mexico. LFS thanks the ITAMP hospitality, where part of this work was done. NR 63 TC 3 Z9 3 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0103-9733 EI 1678-4448 J9 BRAZ J PHYS JI Braz. J. Phys. PD JUN PY 2016 VL 46 IS 3 BP 239 EP 247 DI 10.1007/s13538-015-0366-3 PG 9 WC Physics, Multidisciplinary SC Physics GA DJ9YY UT WOS:000374570700001 ER PT J AU Looy, CV Ranks, SL Chaney, DS Sanchez, S Steyer, JS Smith, RMH Sidor, CA Myers, TS Ide, O Tabor, NJ AF Looy, Cindy V. Ranks, Stephanie L. Chaney, Dan S. Sanchez, Sophie Steyer, Jean-Sebastien Smith, Roger M. H. Sidor, Christian A. Myers, Timothy S. Ide, Oumarou Tabor, Neil J. TI Biological and physical evidence for extreme seasonality in central Permian Pangea SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Niger; Permian; Central Pangea; Climate; Desert; Paleobiology ID NIGERPETON-RICQLESI TEMNOSPONDYLI; NORTH-CENTRAL TEXAS; VERTEBRATE FAUNA; SOUTH-AFRICA; SOUTHWESTERN AUSTRALIA; MASS EXTINCTION; BONE-HISTOLOGY; CARBON-DIOXIDE; AGE ESTIMATION; 1ST EVIDENCE AB Climate models indicate increased desertification in the continental interior of Pangea during the Permian, which would have affected the composition of the flora and fauna. We present a multi-proxy paleoenvironmental reconstruction of a terrestrial ecosystem in central Pangea of Lopingian age. The reconstruction is based on biological and physical data from the Moradi Formation, located in the Tim Mersoi sub-Basin, northern Niger. Paleosols and sedimentological evidence indicate that the prevailing climate was semi-arid to very arid with marked intervals of high water availability. Carbon stable isotope data from organic matter and paleosols suggest that both the soil productivity and actual evapotranspiration were very low, corresponding to arid conditions. Histological analysis of pareiasaur bones shows evidence of active metabolism and reveals distinct growth marks. These interruptions of bone formation are indicative of growth rhythms, and are considered as markers for contrasting seasonality orepisodic climate events. The macrofossil floras have low diversity and represent gymnosperm dominated woodlands. Most notable are ovuliferous dwarf shoots of voltzian conifers, and a 25-m long tree trunk with irregularly positioned branch scars. The combined biological and physical evidence suggests that the Moradi Formation was deposited under a generally arid climate with recurring periods of water abundance, allowing for a well-established ground water-dependent ecosystem. With respect to its environment, this system is comparable with modern ecosystems such as the southern African Namib Desert and the Lake Eyre Basin in Australia, which are discussed as modern analogues. (C) 2016 Elsevier B.V. All rights reserved. C1 [Looy, Cindy V.; Ranks, Stephanie L.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Looy, Cindy V.; Ranks, Stephanie L.] Univ Calif Berkeley, Museum Paleontol, Berkeley, CA 94720 USA. [Chaney, Dan S.] Smithsonian Inst, NMNH, Dept Paleobiol, Washington, DC 20560 USA. [Sanchez, Sophie] Uppsala Univ, Evolutionary Biol Ctr, Dept Physiol & Dev Biol, Norbyvagen 18A, S-75236 Uppsala, Sweden. [Steyer, Jean-Sebastien] UPMC, Ctr Rech Paleobiodivers & Paleoenvironnements, MNHN, UMR 7207,CNRS, CP 38,8 Rue Buffon, F-75005 Paris, France. [Smith, Roger M. H.] Iziko South African Museum, Karoo Palaeontol, ZA-8000 Cape Town, South Africa. [Smith, Roger M. H.] Univ Witwatersrand, Evolutionary Studies Inst, 1 Jan Smuts Ave, ZA-2000 Johannesburg, South Africa. [Sidor, Christian A.] Univ Washington, Burke Museum, Seattle, WA 98195 USA. [Sidor, Christian A.] Univ Washington, Dept Biol, Seattle, WA 98195 USA. [Myers, Timothy S.; Tabor, Neil J.] So Methodist Univ, Huffington Dept Earth Sci, Dallas, TX 75275 USA. [Ide, Oumarou] Inst Rech Sci Humaines, Niamey, Niger. RP Looy, CV (reprint author), 1005 Valley Life Sci Bldg 3140, Berkeley, CA 94720 USA. EM looy@berkeley.edu FU Nigerien Ministry of Higher Education, Research, and Technology; National Museum of Niger; University of Niamey; National Science Foundation [EAR 0617250, EAR-0617718]; ERC [233111]; Hellman Foundation FX We are indebted to the Nigerien Ministry of Higher Education, Research, and Technology, the National Museum of Niger, and the University of Niamey for supporting our research. We thank T. Smiley, S. Thomas, A. Dindine, A. Maga and B. Tahirou for assistance in the field. N.J. Tabor thanks F. Massari (Padova University) for introducing and leading him through the late Permian strata of Italy. J.-S. Steyer and S. Sanchez acknowledge M. Lemoine (MNHN, Paris) for making the bone thin sections. C.V. Looy thanks I. Poole for making the wood thin sections. W. DiMichele and S. Finnegan are thanked for proof reading the draft manuscript. Two anonymous reviewers provided thoughtful and critical reviews, which greatly improved the paper. This project was supported by the National Science Foundation grants EAR 0617250 to N.J. Tabor and EAR-0617718 to C.A. Sidor. S. Sanchez was funded by ERC Advanced Investigator Grant 233111 (to P. E. Ahlberg), and S.L. Ranks work was funded by the Hellman Foundation (to C.V. Looy). This is University of California Museum of Paleontology Contribution No. 2075. NR 96 TC 0 Z9 0 U1 4 U2 10 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 JUN 1 PY 2016 VL 451 BP 210 EP 226 DI 10.1016/j.palaeo.2016.02.016 PG 17 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA DL3EU UT WOS:000375517800017 ER PT J AU Daylan, T Finkbeiner, DP Hooper, D Linden, T Portillo, SKN Rodd, NL Slatyer, TR AF Daylan, Tansu Finkbeiner, Douglas P. Hooper, Dan Linden, Tim Portillo, Stephen K. N. Rodd, Nicholas L. Slatyer, Tracy R. TI The characterization of the gamma-ray signal from the central Milky Way: A case for annihilating dark matter SO PHYSICS OF THE DARK UNIVERSE LA English DT Article DE Dark matter; Indirect detection; Gamma-rays ID LARGE-AREA TELESCOPE; INSTRUMENT RESPONSE FUNCTIONS; GALACTIC-CENTER; COSMIC-RAYS; FERMI; EMISSION; GALAXY; HALOS; PROPAGATION; CONTRACTION AB Past studies have identified a spatially extended excess of similar to 1-3 GeV gamma rays from the region surrounding the Galactic Center, consistent with the emission expected from annihilating dark matter. We revisit and scrutinize this signal with the intention of further constraining its characteristics and origin. By applying cuts to the Fermi event parameter CTBCORE, we suppress the tails of the point spread function and generate high resolution gamma-ray maps, enabling us to more easily separate the various gamma-ray components. Within these maps, we find the GeV excess to be robust and highly statistically significant, with a spectrum, angular distribution, and overall normalization that is in good agreement with that predicted by simple annihilating dark matter models. For example, the signal is very well fit by a 36-51 GeV dark matter particle annihilating to b (b) over bar with an annihilation cross section of sigma v = (1-3) x10(-26) cm(3)/s (normalized to a local dark matter density of 0.4 GeV/cm(3)). Furthermore, we confirm that the angular distribution of the excess is approximately spherically symmetric and centered around the dynamical center of the Milky Way (within similar to 0.05 degrees of Sgr A*), showing no sign of elongation along the Galactic Plane. The signal is observed to extend to at least similar or equal to 10 degrees from the Galactic Center, which together with its other morphological traits disfavors the possibility that this emission originates from previously known or modeled pulsar populations. (C) 2016 Elsevier B.V. All rights reserved. C1 [Daylan, Tansu; Finkbeiner, Douglas P.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Finkbeiner, Douglas P.; Portillo, Stephen K. N.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Hooper, Dan] Fermilab Natl Accelerator Lab, Theoret Astrophys Grp, POB 500, Batavia, IL 60510 USA. [Hooper, Dan] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Linden, Tim] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Rodd, Nicholas L.; Slatyer, Tracy R.] MIT, Ctr Theoret Phys, Boston, MA USA. [Slatyer, Tracy R.] Inst Adv Study, Sch Nat Sci, Olden Lane, Princeton, NJ 08540 USA. RP Linden, T (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. EM linden.70@osu.edu OI Portillo, Stephen/0000-0001-8132-8056 FU University of Chicago Research Computing Center; NASA Fermi Guest Investigator Program; Department of Energy; NASA through Einstein Postdoctoral Award [PF3-140110]; U.S. Department of Energy [DE-FG02-05ER41360] FX We would like to thank Keith Bechtol, Eric Charles and Alex Drlica-Wagner for their help with the Fermi-LAT likelihood analysis, Oscar Macias-Ramirez and Farhad Yusef-Zadeh for providing the 20 cm templates, and Simona Murgia, Jesse Thaler and Neal Weiner for helpful discussions. We particularly thank Francesca Calore, Ilias Cholis and Christoph Weniger for providing an independent cross-check of some of our sphericity results. We acknowledge the University of Chicago Research Computing Center for providing support for this work. DPF is supported in part by the NASA Fermi Guest Investigator Program, DH is supported by the Department of Energy, and TL is supported by NASA through Einstein Postdoctoral Award Number PF3-140110. TRS is supported by the U.S. Department of Energy under cooperative research agreement Contract Number DE-FG02-05ER41360. NR 103 TC 82 Z9 83 U1 3 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2212-6864 J9 PHYS DARK UNIVERSE JI Phys. Dark Universe PD JUN PY 2016 VL 12 BP 1 EP 23 DI 10.1016/j.dark.2015.12.005 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DK0VZ UT WOS:000374631600001 ER PT J AU LaManna, JA Walton, ML Turner, BL Myers, JA AF LaManna, Joseph A. Walton, Maranda L. Turner, Benjamin L. Myers, Jonathan A. TI Negative density dependence is stronger in resource-rich environments and diversifies communities when stronger for common but not rare species SO ECOLOGY LETTERS LA English DT Article DE Density dependence; diversity maintenance; diversity-environment relationship; Janzen-Connell hypothesis; natural enemies; resource availability; seedling and sapling recruitment; species coexistence; species relative abundance; temperate forest ID WET TROPICAL FOREST; SEEDLING MORTALITY; RAIN-FOREST; SPATIAL-PATTERNS; TREE; PRODUCTIVITY; RECRUITMENT; PATHOGENS; SURVIVAL; BIODIVERSITY AB Conspecific negative density dependence is thought to maintain diversity by limiting abundances of common species. Yet the extent to which this mechanism can explain patterns of species diversity across environmental gradients is largely unknown. We examined density-dependent recruitment of seedlings and saplings and changes in local species diversity across a soil-resource gradient for 38 woody-plant species in a temperate forest. At both life stages, the strength of negative density dependence increased with resource availability, becoming relatively stronger for rare species during seedling recruitment, but stronger for common species during sapling recruitment. Moreover, negative density dependence appeared to reduce diversity when stronger for rare than common species, but increase diversity when stronger for common species. Our results suggest that negative density dependence is stronger in resource-rich environments and can either decrease or maintain diversity depending on its relative strength among common and rare species. C1 [LaManna, Joseph A.; Walton, Maranda L.; Myers, Jonathan A.] Washington Univ, Dept Biol, St Louis, MO 63130 USA. [LaManna, Joseph A.; Walton, Maranda L.; Myers, Jonathan A.] Washington Univ, Tyson Res Ctr, St Louis, MO 63130 USA. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. RP LaManna, JA (reprint author), Washington Univ, Dept Biol, St Louis, MO 63130 USA.; LaManna, JA (reprint author), Washington Univ, Tyson Res Ctr, St Louis, MO 63130 USA. EM jlamanna@wustl.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU Washington University in St. Louis' Tyson Research Center; International Center for Advanced Renewable Energy and Sustainability (I-CARES) at Washington University in St. Louis; Tyson Research Center; National Science Foundation [DEB 1557094] FX We thank Kyle Harms, Scott Mangan, Michael Huston, two anonymous reviewers, Claudia Stein, Ivan Jimenez, Sebastian Tello, Holly Bernardo, Christopher Catano, Vincent Fasanello, Emma Moran and Dilys Vela Diaz for helpful comments on this manuscript. We also thank Kyle Harms for suggesting the methods used to link CNDD to species diversity (see Predicted effects of CNDD on species diversity). The Tyson Research Center Forest Dynamics Plot is supported by the Washington University in St. Louis' Tyson Research Center. Funding was provided by the International Center for Advanced Renewable Energy and Sustainability (I-CARES) at Washington University in St. Louis, the Tyson Research Center and the National Science Foundation (DEB 1557094). We thank the Tyson Research Center staff for providing logistical support, and the more than 60 high school students, undergraduate students and researchers that have contributed to the project. We thank James Dalling for assistance with soil-sampling protocols, Tania Romero for assistance with soil sampling, Claire Baldeck for Kriging soil data and Francis Baum for assistance with topographic analyses. The Tyson Research Center Forest Dynamics Plot is part of the Center for Tropical Forest Science-Forest Global Earth Observatory (CTFS-ForestGEO), a global network of large-scale forest dynamics plots. We declare no conflicts of interest. NR 50 TC 2 Z9 2 U1 14 U2 42 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 JUN PY 2016 VL 19 IS 6 BP 657 EP 667 DI 10.1111/ele.12603 PG 11 WC Ecology SC Environmental Sciences & Ecology GA DL6MD UT WOS:000375752400007 PM 27111545 ER PT J AU Dominy, NJ Yeakel, JD Bhat, U Ramsden, L Wrangham, RW Lucas, PW AF Dominy, Nathaniel J. Yeakel, Justin D. Bhat, Uttam Ramsden, Lawrence Wrangham, Richard W. Lucas, Peter W. TI How chimpanzees integrate sensory information to select figs SO INTERFACE FOCUS LA English DT Article DE Pan troglodytes schweinfurthii; Ficus; colour vision; manual prehension; Bayesian updating ID KIBALE NATIONAL-PARK; TRICHROMATIC VISION; FALLBACK FOODS; FRUIT; EVOLUTION; ECOLOGY; PRIMATES; CLASSIFICATION; THRESHOLDS; ANIMALS AB Figs are keystone resources that sustain chimpanzees when preferred fruits are scarce. Many figs retain a green(ish) colour throughout development, a pattern that causes chimpanzees to evaluate edibility on the basis of achromatic accessory cues. Such behaviour is conspicuous because it entails a succession of discrete sensory assessments, including the deliberate palpation of individual figs, a task that requires advanced visuomotor control. These actions are strongly suggestive of domain-specific information processing and decision-making, and they call attention to a potential selective force on the origin of advanced manual prehension and digital dexterity during primate evolution. To explore this concept, we report on the foraging behaviours of chimpanzees and the spectral, chemical and mechanical properties of figs, with cutting tests revealing ease of fracture in the mouth. By integrating the ability of different sensory cues to predict fructose content in a Bayesian updating framework, we quantified the amount of information gained when a chimpanzee successively observes, palpates and bites the green figs of Ficus sansibarica. We found that the cue eliciting ingestion was not colour or size, but fig mechanics (including toughness estimates from wedge tests), which relays higher-quality information on fructose concentrations than colour vision. This result explains why chimpanzees evaluate green figs by palpation and dental incision, actions that could explain the adaptive origins of advanced manual prehension. C1 [Dominy, Nathaniel J.] Dartmouth Coll, Dept Anthropol, 6047 Silsby Hall, Hanover, NH 03755 USA. [Dominy, Nathaniel J.] Dartmouth Coll, Dept Biol Sci, 78 Coll St, Hanover, NH 03755 USA. [Yeakel, Justin D.] Univ Calif, Sch Nat Sci, 5200 North Lake Rd, Merced, CA 95343 USA. [Yeakel, Justin D.; Bhat, Uttam] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. [Bhat, Uttam] Boston Univ, Dept Phys, 590 Commonwealth Ave, Boston, MA 02215 USA. [Ramsden, Lawrence] Univ Hong Kong, Sch Biol Sci, Pok Fu Lam Rd, Hong Kong, Hong Kong, Peoples R China. [Wrangham, Richard W.] Harvard Univ, Dept Human Evolutionary Biol, 11 Divin Ave, Cambridge, MA 02138 USA. [Lucas, Peter W.] Smithsonian Trop Res Inst, Apartado Postal, Balboa 08303092, Ancon, Panama. RP Dominy, NJ (reprint author), Dartmouth Coll, Dept Anthropol, 6047 Silsby Hall, Hanover, NH 03755 USA.; Dominy, NJ (reprint author), Dartmouth Coll, Dept Biol Sci, 78 Coll St, Hanover, NH 03755 USA. EM nathaniel.j.dominy@dartmouth.edu OI Yeakel, Justin/0000-0002-6597-3511 FU Explorer's Club; National Geographic Society [6584-99]; Research Grants Council of Hong Kong [7241/97M]; Sigma Xi; University of Hong Kong FX Funding was received from the Explorer's Club (to N.J.D.), the National Geographic Society (grant no. 6584-99 to P.W.L. and N.J.D.), the Research Grants Council of Hong Kong (grant no. 7241/97M to P.W.L.), Sigma Xi (grant in aid of research to N.J.D.) and the University of Hong Kong (postgraduate studentship to N.J.D.). NR 58 TC 0 Z9 0 U1 10 U2 23 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 2042-8898 EI 2042-8901 J9 INTERFACE FOCUS JI Interface Focus PD JUN PY 2016 VL 6 IS 3 AR 20160001 DI 10.1098/rsfs.2016.0001 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA DL1SC UT WOS:000375411300008 PM 27274803 ER PT J AU Kitajima, K Wright, SJ Westbrook, JW AF Kitajima, Kaoru Wright, S. Joseph Westbrook, Jared W. TI Leaf cellulose density as the key determinant of inter- and intra-specific variation in leaf fracture toughness in a species-rich tropical forest SO INTERFACE FOCUS LA English DT Article DE biomechanics; plant functional traits; fracture toughness; cell wall fibre; cellulose; lignin ID MECHANICAL-PROPERTIES; CELL-WALLS; BIOMECHANICAL PROPERTIES; LIFE-SPAN; TRAITS; LEAVES; LIGHT; CONSEQUENCES; HERBIVORY; PATTERNS AB Leaves as the main photosynthetic organ of plants must be well protected against various hazards to achieve their optimal lifespans. Yet, within-species variation and the material basis of leaf strength have been explored for very few species. Here, we present a large dataset of leaf fracture toughness from a species-rich humid tropical forest on Barro Colorado Island, Panama, reporting both among-and within-species variation in relation to light environment (sun-lit canopy versus shaded understorey) and ontogeny (seedlings versus adults). In this dataset encompassing 281 free-standing woody species and 428 species-light combinations, lamina fracture toughness varied ca 10 times. A central objective of our study was to identify generalizable patterns in the structural and material basis for interspecific variation in leaf lamina fracture toughness. The leaf lamina is a heterogeneous structure in which strong materials in cell walls, such as cellulose and lignin, contribute disproportionately to fracture toughness. We found significant increases in leaf fracture toughness from shade to sun and from seedling leaves to adult leaves. Both within and across species, leaf fracture toughness increased with total bulk density (dry biomass per unit volume) and cellulose mass concentration, but decreased with mass concentrations of lignin and hemicelluose. These bivariate relationships shift between light environments, but leaf cellulose density (cellulose mass per unit leaf volume) exhibits a common relationship with lamina fracture toughness between light environments and through ontogeny. Hence, leaf cellulose density is probably a universal predictor of leaf fracture toughness. C1 [Kitajima, Kaoru] Kyoto Univ, Grad Sch Agr, Kyoto, Japan. [Kitajima, Kaoru; Westbrook, Jared W.] Univ Florida, Dept Biol, Gainesville, FL USA. [Kitajima, Kaoru; Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Panama. RP Kitajima, K (reprint author), Kyoto Univ, Grad Sch Agr, Kyoto, Japan.; Kitajima, K (reprint author), Univ Florida, Dept Biol, Gainesville, FL USA.; Kitajima, K (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM kaoruk@kais.kyoto-u.ac.jp RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU F. H. Levinson Fund FX The F. H. Levinson Fund supported leaf trait measurements. NR 38 TC 1 Z9 1 U1 6 U2 8 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 2042-8898 EI 2042-8901 J9 INTERFACE FOCUS JI Interface Focus PD JUN PY 2016 VL 6 IS 3 AR 20150100 DI 10.1098/rsfs.2015.0100 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA DL1SC UT WOS:000375411300001 PM 27274796 ER PT J AU Canington, SL Hunt, DR AF Canington, Stephanie L. Hunt, David R. TI Rapid development of secondary hyperparathyroidism and fibrous osteodystrophy in a juvenile orangutan SO INTERNATIONAL JOURNAL OF PALEOPATHOLOGY LA English DT Article DE Metabolic disease; Orangutan; Osteodystrophia fibrosa; Zoo animal ID DISEASE; DEFICIENCY AB This study presents a probable case of rapidly-developed fibrous osteodystrophy and secondary hyperparathyroidism in a juvenile wild-caught zoo orangutan, Pongo pygmaeus. Cases of this metabolic disease, associated with captivity in primates, are underreported in non-human Hominidae, and none to the extent of postcranial afflictions. We present the first described case of these metabolic pathologies of a great ape at both the cranial and skeletal levels. (C) 2016 Published by Elsevier Inc. C1 [Canington, Stephanie L.] Johns Hopkins Univ, Sch Med, Ctr Funct Anat & Evolut, 1830 E Monument St, Baltimore, MD 21218 USA. [Canington, Stephanie L.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. [Hunt, David R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. RP Canington, SL (reprint author), Johns Hopkins Univ, Sch Med, Ctr Funct Anat & Evolut, 1830 E Monument St, Baltimore, MD 21218 USA. EM scaning1@jhmi.edu; huntd@si.edu NR 14 TC 0 Z9 0 U1 4 U2 4 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 JUN PY 2016 VL 13 BP 96 EP 99 DI 10.1016/j.ijpp.2016.03.002 PG 4 WC Paleontology; Pathology SC Paleontology; Pathology GA DK5ZO UT WOS:000375000000012 ER PT J AU Renner, SC Suarez-Rubio, M Wiesner, KR Drogemuller, C Gockel, S Kalko, EKV Ayasse, M Frantz, AC AF Renner, Swen C. Suarez-Rubio, Marcela Wiesner, Kerstin R. Droegemueller, Cord Gockel, Sonja Kalko, Elisabeth K. V. Ayasse, Manfred Frantz, Alain C. TI Using multiple landscape genetic approaches to test the validity of genetic clusters in a species characterized by an isolation-by-distance pattern SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Bayesian clustering algorithms; habitat fragmentation; least-cost paths; population genetic structure; Sus scrofa; wild boar ID DEER CERVUS-ELAPHUS; BOAR SUS-SCROFA; WILD BOAR; POPULATION-STRUCTURE; PROGRAM STRUCTURE; COMPUTER-PROGRAM; HABITAT USE; DISPERSAL; FLOW; MULTICOLLINEARITY AB Bayesian clustering methods are typically used to identify barriers to gene flow, but they are prone to deduce artificial subdivisions in a study population characterized by an isolation-by-distance pattern (IbD). Here we analysed the landscape genetic structure of a population of wild boars (Sus scrofa) from south-western Germany. Two clustering methods inferred the presence of the same genetic discontinuity. However, the population in question was characterized by a strong IbD pattern. While landscape-resistance modelling failed to identify landscape features that influenced wild boar movement, partial Mantel tests and multiple regression of distance matrices (MRDMs) suggested that the empirically inferred clusters were separated by a genuine barrier. When simulating random lines bisecting the study area, 60% of the unique barriers represented, according to partial Mantel tests and MRDMs, significant obstacles to gene flow. By contrast, the random-lines simulation showed that the boundaries of the inferred empirical clusters corresponded to the most important genetic discontinuity in the study area. Given the degree of habitat fragmentation separating the two empirical partitions, it is likely that the clustering programs correctly identified a barrier to gene flow. The differing results between the work published here and other studies suggest that it will be very difficult to draw general conclusions about habitat permeability in wild boar from individual studies. C1 [Renner, Swen C.; Suarez-Rubio, Marcela] Univ Nat Resources & Life Sci, Inst Zool, Gregor Mendel Str 33, A-1180 Vienna, Austria. [Renner, Swen C.] Smithsonian Inst, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Woodbridge, VA 22630 USA. [Wiesner, Kerstin R.; Gockel, Sonja] Tech Univ Munich, Dept Ecol & Ecosyst Management, Hans Carl von Carlowitz Pl 2, D-85354 Freising Weihenstephan, Germany. [Droegemueller, Cord] Univ Bern, Inst Genet, Bremgartenstr 109a, CH-3001 Bern, Switzerland. [Kalko, Elisabeth K. V.; Ayasse, Manfred] Univ Ulm, Inst Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. [Frantz, Alain C.] Musee Natl Hist Nat, 25 Rue Munster, L-2160 Luxembourg, Luxembourg. [Frantz, Alain C.] Fdn Faune Flore, L-2160 Luxembourg, Luxembourg. RP Renner, SC (reprint author), Univ Nat Resources & Life Sci, Inst Zool, Gregor Mendel Str 33, A-1180 Vienna, Austria.; Renner, SC (reprint author), Smithsonian Inst, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Woodbridge, VA 22630 USA. EM swen.renner@boku.ac.at OI Suarez-Rubio, Marcela/0000-0002-0596-2626; Renner, Swen/0000-0002-6893-4219 FU Deutsche Forschungsgemeinschaft FX We thank all hunters and volunteers who provided tissue samples for the research project, the Forstamt Munsingen and Curt Witzemann (head of hunters' organization Jagdverband Munsingen) for contacting these hunters in the first place, Gerald Kerth for enabling the fruitful cooperation between A.C.F., C.D. and S.C.R., and Hugh Loxdale, the editor J.A. Allen and five anonymous reviewers for their helpful comments on previous versions of the manuscript. The Deutsche Forschungsgemeinschaft funded the study (www.dfg.de). The hunters and funding organization had no role in study design, analysis, decision to publish, or preparation or finalizing of the manuscript. The authors have no conflict of interest to declare. NR 43 TC 0 Z9 0 U1 7 U2 19 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 JUN PY 2016 VL 118 IS 2 BP 292 EP 303 DI 10.1111/bij.12737 PG 12 WC Evolutionary Biology SC Evolutionary Biology GA DJ7HU UT WOS:000374383300010 ER PT J AU Wang, HQ Toigo, AD AF Wang, Huiqun Toigo, Anthony D. TI The variability, structure and energy conversion of the northern hemisphere traveling waves simulated in a Mars general circulation model SO ICARUS LA English DT Article DE Atmospheres, dynamics; Mars, atmosphere; Mars ID TIME SPECTRAL-ANALYSIS; DUST STORMS; MARTIAN ATMOSPHERE; GLOBAL SURVEYOR; BAROCLINIC WAVES; ORBITER CAMERA; DYNAMICS; ORIGIN; DISTURBANCES; CLIMATOLOGY AB Investigations of the variability, structure and energetics of the m = 1-3 traveling waves in the northern hemisphere of Mars are conducted with the MarsWRF general circulation model. Using a simple, annually repeatable dust scenario, the model reproduces many general characteristics of the observed traveling waves. The simulated m = 1 and m = 3 traveling waves show large differences in terms of their structures and energetics. For each representative wave mode, the geopotential signature maximizes at a higher altitude than the temperature signature, and the wave energetics suggests a mixed baroclinic-barotropic nature. There is a large contrast in wave energetics between the near-surface and higher altitudes, as well as between the lower latitudes and higher latitudes at high altitudes. Both barotropic and baroclinic conversions can act as either sources or sinks of eddy kinetic energy. Band-pass filtered transient eddies exhibit strong zonal variations in eddy kinetic energy and various energy transfer terms. Transient eddies are mainly interacting with the time mean flow. However, there appear to be non-negligible wave-wave interactions associated with wave mode transitions. These interactions include those between traveling waves and thermal tides and those among traveling waves. (C) 2016 Elsevier Inc. All rights reserved. C1 [Wang, Huiqun] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Toigo, Anthony D.] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. RP Wang, HQ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM hwang@cfa.harvard.edu FU NASA [NNX10AB85G, NNX14AG55G] FX This paper is supported partially by NASA grant NNX10AB85G and partially by NASA grant NNX14AG55G. The computations were run on the Odyssey cluster supported by the Faculty of Arts & Sciences (FAS) Research Computing Group at Harvard University. The MACDA dataset used in Section 2 is downloaded from the British Atmospheric Data Centre (BADC) website. NR 36 TC 0 Z9 0 U1 2 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUN 1 PY 2016 VL 271 BP 207 EP 221 DI 10.1016/j.icarus.2016.02.005 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI7AP UT WOS:000373651800016 ER PT J AU Velasquez, G Ngo, PT Rumpel, C Calabi-Floody, M Redel, Y Turner, BL Condron, LM Mora, MD AF Velasquez, Gabriela Phuong-Thi Ngo Rumpel, Cornelia Calabi-Floody, Marcela Redel, Yonathan Turner, Benjamin L. Condron, Leo M. de la Luz Mora, Maria TI Chemical nature of residual phosphorus in Andisols SO GEODERMA LA English DT Article DE Phosphorus fractionation; Recalcitrant phosphorus; 31P nuclear magnetic resonance spectroscopy ID P-31 NMR-SPECTROSCOPY; SOIL-PHOSPHORUS; INOSITOL PHOSPHATES; ORGANIC PHOSPHORUS; TEMPERATE SOILS; VOLCANIC SOILS; LAND-USE; FRACTIONATION; BIOAVAILABILITY; ASSOCIATIONS AB Sequential fractionation has been widely used to study the nature and dynamics of soil P. Residual P - the recalcitrant P fraction remaining after sequential extraction with alkali and acid reagents - often constitutes the majority of the soil P, yet its nature and bioavailability is poorly understood. The objective of this study was to isolate, quantify, and characterize residual P following Hedley fractionation in a range of Andisols under grazed pasture by 31P nuclear magnetic resonance (NMR) spectroscopy. Residual P accounted for 45-63% of the total soil P, of which 53-77% was inorganic orthophosphate. Organic P accounted for 21-42% of the residual P, the majority of which occurred as phosphomonoesters including myo- (16% of the residual P) and scyllo-inositol hexaldsphosphate (10% of the residual P). No phosphodiesters were detected in the residual fraction. We conclude that residual P in Andisols consists of a mixture of inorganic P and organic P. Our findings provide the basis for the development of new approaches to improve P use efficiency in agriculture. (C) 2016 Elsevier B.V. All rights reserved. C1 [Velasquez, Gabriela; Phuong-Thi Ngo; Calabi-Floody, Marcela; Redel, Yonathan; de la Luz Mora, Maria] Univ La Frontera, Ctr Plant Soil Interact & Nat Resources Biotechno, Sci & Biotechnol Bioresource Nucleus BIOREN UFRO, Ave Francisco Salazar 01145, Temuco, Chile. [Phuong-Thi Ngo] Univ Loraine, LSE, Vandoeurve Les Nancy, France. [Rumpel, Cornelia] UMR Univ Paris VI & XII CNRS INRA IRD, Campus AgroParisTech, Thiverval Grignon, France. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. [Condron, Leo M.] Lincoln Univ, Fac Agr & Life Sci, POB 85084, Christchurch 7647, New Zealand. RP Mora, MD (reprint author), Univ La Frontera, Ctr Plant Soil Interact & Nat Resources Biotechno, Sci & Biotechnol Bioresource Nucleus BIOREN UFRO, Ave Francisco Salazar 01145, Temuco, Chile. EM mariluz.mora@ufrontera.cl RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU FONDECYT from Chilean Government [1141247]; ECOSSUD-CONICYT [C13U02] FX The authors thank the FONDECYT project No 1141247 from Chilean Government for financial support and the ECOSSUD-CONICYT C13U02 project for financial support of French and Chilean research groups. NR 40 TC 2 Z9 2 U1 15 U2 40 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 JUN 1 PY 2016 VL 271 BP 27 EP 31 DI 10.1016/j.geoderma.2016.01.027 PG 5 WC Soil Science SC Agriculture GA DI5LY UT WOS:000373541800004 ER PT J AU Guo, LC Shih, CK Li, LF Ren, D AF Guo, Lichao Shih, Chungkun Li, Longfeng Ren, Dong TI New pelecinid wasps (Hymenoptera: Pelecinidae) from the Yixian Formation of western Liaoning, China SO CRETACEOUS RESEARCH LA English DT Article DE New genus; New species; Lower Cretaceous; Huangbanjigou; Jehol Biota ID EARLIEST FOSSIL RECORD; PROCTOTRUPOIDEA PELECINIDAE; CRETACEOUS ECOSYSTEM; LAIYANG FORMATION; NORTHEAST CHINA; JEHOL BIOTA; INSECTA; MONGOLIA; GENUS; SHANDONG AB A new species, Shoushida infera sp. nov. and a new genus with a new species, Stelepelecinus longus gen. et sp. nov., both in Pelecinidae, are described and illustrated. All specimens were collected from the Lower Cretaceous of Yixian Formation, Jehol Biota at Huangbanjigou, Beipiao City, western Liaoning Province, China. The forewing of Shoushida infera sp. nov. has a rudimentary "X" pattern, formed by veins of Rs, Rs(1), Rs(2) and 2r-rs, which is similar to but slightly different from that of Shoushida regilla Liu, Shih et Ren, 2009. Consistent with the phylogeny of Pelecinidae reported by Shih et al., 2010, this new species and S. regilla represent a transition between basal and crown pelecinids and the rudimentary "X" pattern evolved later to a more developed and robust "X" pattern in more derived pelecinids. In addition, the long petiole of the basalmost segment of metasoma, present in the male Stelepelecinus longus gen. et sp. nov., is documented for the first time, suggesting a likely Early Cretaceous origination of metasomal evolution leading to the thin and long petiole structure in the extant male Pelecinus thoracicus. We proposed two probable pathways of the transformation of the pelecinid male metasoma from the most plesiomorphic state to the more apomorphic states. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Guo, Lichao; Shih, Chungkun; Li, Longfeng; Ren, Dong] Capital Normal Univ, Coll Life Sci, 105 Xisanhuanbeilu, Beijing 100048, Peoples R China. [Shih, Chungkun] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Ren, D (reprint author), Capital Normal Univ, Coll Life Sci, 105 Xisanhuanbeilu, Beijing 100048, Peoples R China. EM rendong@mail.cnu.edu.cn FU National Basic Research Program of China (973 Program) [2012CB821906]; National Natural Science Foundation of China [31230065, 41272006]; Great Wall Scholar; KEY project of Beijing Municipal Commission of Education Project [KZ201310028033]; Program for Changjiang Scholars and Innovative Research Team in University [IRT13081] FX We appreciate valuable comments and constructive suggestion on our manuscript from Drs. Koutsoukos and Rasnitsyn, and an anonymous reviewer. We are grateful to Dr. Taiping Gao and Hongyun Zhao (College of Life Sciences, Capital Normal University) for kind assistance and useful advice. This research was supported by grants from the National Basic Research Program of China (973 Program) (Grant 2012CB821906), the National Natural Science Foundation of China (No. 31230065, 41272006), Great Wall Scholar and KEY project of Beijing Municipal Commission of Education Project (grant KZ201310028033), Program for Changjiang Scholars and Innovative Research Team in University (IRT13081). NR 40 TC 1 Z9 1 U1 3 U2 7 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0195-6671 EI 1095-998X J9 CRETACEOUS RES JI Cretac. Res. PD JUN PY 2016 VL 61 BP 151 EP 160 DI 10.1016/j.cretres.2016.01.009 PG 10 WC Geology; Paleontology SC Geology; Paleontology GA DG2ZJ UT WOS:000371939000015 ER PT J AU Suchley, A McField, MD Alvarez-Filip, L AF Suchley, Adam McField, Melanie D. Alvarez-Filip, Lorenzo TI Rapidly increasing macroalgal cover not related to herbivorous fishes on Mesoamerican reefs SO PEERJ LA English DT Article DE Coral reefs; Top-down control; Marine Protected Areas; Macroalgae; Mesoamerican Reef; Phase shifts; Herbivory; Caribbean ID MARINE PROTECTED AREAS; CARIBBEAN CORAL-REEFS; PHASE-SHIFTS; BUILDING CORALS; MASS MORTALITY; COMMUNITIES; GROWTH; PARROTFISHES; COMPETITION; RESILIENCE AB Long-term phase shifts from coral to macroalgal dominated reef systems are well documented in the Caribbean. Although the impact of coral diseases, climate change and other factors is acknowledged, major herbivore loss through disease and overfishing is often assigned a primary role. However, direct evidence for the link between herbivore abundance, macroalgal and coral cover is sparse, particularly over broad spatial scales. In this study we use a database of coral reef surveys performed at 85 sites along the Mesoamerican Reef of Mexico, Belize, Guatemala and Honduras, to examine potential ecological links by tracking site trajectories over the period 20052014. Despite the long-term reduction of herbivory capacity reported across the Caribbean, the Mesoamerican Reef region displayed relatively low macroalgal cover at the onset of the study. Subsequently, increasing fleshy macroalgal cover was pervasive. Herbivorous fish populations were not responsible for this trend as fleshy macroalgal cover change was not correlated with initial herbivorous fish biomass or change, and the majority of sites experienced increases in macroalgae browser biomass. This contrasts the coral reef top-down herbivore control paradigm and suggests the role of external factors in making environmental conditions more favourable for algae. Increasing macroalgal cover typically suppresses ecosystem services and leads to degraded reef systems. Consequently, policy makers and local coral reef managers should reassess the focus on herbivorous fish protection and consider complementary measures such as watershed management in order to arrest this trend. C1 [Suchley, Adam] Univ Nacl Autonoma Mexico, Posgrad Ciencias Mar & Limnol, Inst Ciencias Mar & Limnol, Mexico City 04510, DF, Mexico. [Suchley, Adam; Alvarez-Filip, Lorenzo] Univ Nacl Autonoma Mexico, Unidad Acad Sistemas Arrecifales, Inst Ciencias Mar & Limnol, Puerto Morelos, Quintana Roo, Mexico. [McField, Melanie D.] Smithsonian Inst, Healthy Reefs Healthy People Initiat, Ft Lauderdale, FL USA. RP Alvarez-Filip, L (reprint author), Univ Nacl Autonoma Mexico, Unidad Acad Sistemas Arrecifales, Inst Ciencias Mar & Limnol, Puerto Morelos, Quintana Roo, Mexico. EM lorenzoaf@gmail.com FU Summit Foundation; Oak Foundation; JRS Biodiversity Foundation; CONACyT [667112/587102]; Rufford Foundation; Mexican Council of Science and Technology (CONACyT) [PDC-247104] FX Data collection was funded by the Summit Foundation, Oak Foundation, JRS Biodiversity Foundation and an anonymous donor organization. A.S. was supported by a PhD scholarship (No. 667112/587102) from CONACyT and an RSG grant from The Rufford Foundation. L.A.-F. was funded by the Mexican Council of Science and Technology (CONACyT, PDC-247104). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 76 TC 3 Z9 3 U1 13 U2 23 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD MAY 31 PY 2016 VL 4 AR e2084 DI 10.7717/peerj.2084 PG 20 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DO3KY UT WOS:000377681700002 PM 27280075 ER PT J AU Duffy, JE Lefcheck, JS Stuart-Smith, RD Navarrete, SA Edgar, GJ AF Duffy, J. Emmett Lefcheck, Jonathan S. Stuart-Smith, Rick D. Navarrete, Sergio A. Edgar, Graham J. TI Biodiversity enhances reef fish biomass and resistance to climate change SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE global change; fisheries; functional diversity; macroecology; structural equation model ID CORAL-REEFS; MARINE ECOSYSTEMS; DIVERSITY; PRODUCTIVITY; PATTERNS; IMPACTS; ECOLOGY; VULNERABILITY; PREDICTORS; PREDATORS AB Fishes are the most diverse group of vertebrates, play key functional roles in aquatic ecosystems, and provide protein for a billion people, especially in the developing world. Those functions are compromised by mounting pressures on marine biodiversity and ecosystems. Because of its economic and food value, fish biomass production provides an unusually direct link from biodiversity to critical ecosystem services. We used the Reef Life Survey's global database of 4,556 standardized fish surveys to test the importance of biodiversity to fish production relative to 25 environmental drivers. Temperature, biodiversity, and human influence together explained 47% of the global variation in reef fish biomass among sites. Fish species richness and functional diversity were among the strongest predictors of fish biomass, particularly for the largebodied species and carnivores preferred by fishers, and these biodiversity effects were robust to potentially confounding influences of sample abundance, scale, and environmental correlations. Warmer temperatures increased biomass directly, presumably by raising metabolism, and indirectly by increasing diversity, whereas temperature variability reduced biomass. Importantly, diversity and climate interact, with biomass of diverse communities less affected by rising and variable temperatures than species-poor communities. Biodiversity thus buffers global fish biomass from climate change, and conservation of marine biodiversity can stabilize fish production in a changing ocean. C1 [Duffy, J. Emmett] Smithsonian Inst, Tennenbaum Marine Observ Network, Washington, DC 20013 USA. [Lefcheck, Jonathan S.] Coll William & Mary, Dept Biol Sci, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. [Stuart-Smith, Rick D.; Edgar, Graham J.] Univ Tasmania, Inst Marine & Antarctic Studies, Hobart, Tas 7001, Australia. [Navarrete, Sergio A.] Pontificia Univ Catolica Chile, Estn Costera Invest Marinas, Casilla 114-D, Santiago, Chile. [Navarrete, Sergio A.] Pontificia Univ Catolica Chile, Ctr Marine Conservat, Casilla 114-D, Santiago, Chile. RP Duffy, JE (reprint author), Smithsonian Inst, Tennenbaum Marine Observ Network, Washington, DC 20013 USA. EM duffye@si.edu OI Stuart-Smith, Rick/0000-0002-8874-0083 NR 60 TC 7 Z9 7 U1 50 U2 97 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAY 31 PY 2016 VL 113 IS 22 BP 6230 EP 6235 DI 10.1073/pnas.1524465113 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DN0VL UT WOS:000376784600048 PM 27185921 ER PT J AU Davis, JM Vicenzi, EP AF Davis, Jeffrey M. Vicenzi, Edward P. TI Optimizing compositional images of daguerreotype photographs using post processing methods SO HERITAGE SCIENCE LA English DT Article DE Early photography; Image analysis; Image processing; Noise suppression; Spectrum imaging; XRF; X-ray imaging ID PROGRAM AB Microfocused X-ray fluorescence imaging was used to examine two 19th century daguerreotypes. The distribution of Hg-bearing nanoparticles beneath the Au gilding layer gives rise to contrast in the photographs. The sum image for Au + Hg M line X-rays is therefore a compositional image that mimics daguerreotype photograph contrast. Because the thickness of the Au and Hg on the surface represents a small fraction of the X-ray activation depth, the resulting sum images are not of high quality and are dominated by Poisson noise. This is true even for long collection times up to multiple days in length. Achieving superior contrast resolution by increasing the duration of data collection further is impractical. In this study, a new image processing technique based upon the Haar-Fisz algorithm and wavelet theory was used to improve the image quality of compositional maps. The digitally processed images show a reduction in noise without a loss of spatial resolution over the length-scale of photographic features. The Haar-Fisz denoising algorithm decreased the contribution of the Poisson noise in compositional images. Multiple resolution analysis improved image quality further. Features within the portraits are uniformly more recognizable in the final processed images relative to the raw X-ray images. Intensity line profiles that traverse midtone, highlight and shadow regions of the daguerreotype reveal that spatial resolution is not degraded by the image processing routines. Improvement in image quality is quantified by comparing the relative variance of the raw and Haar-Fisz processed imagery. The use of a Haar-Fisz denoising transformation, coupled with multiple resolution analysis was found to improve the quality of low count X-ray images without impacting the spatial resolution at the scale of photograph features. The process can be implemented in freely available open-source software with a minimum of programming effort. Such digital post processing routines offset the need for longer acquisition times to achieve improved X-ray fluorescence image quality. Finally, because the Au + Hg map is insensitive to surface imperfections and tarnishing via atmospheric adsorption of sulfur, digitally processed images may be used to reconstruct photograph features in heavily disfigured daguerreotypes. C1 [Davis, Jeffrey M.] PNDetector GmbH, Emil Nolde Str 10, D-81735 Munich, Germany. [Vicenzi, Edward P.] Museum Conservat Inst, Smithsonian Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA. RP Vicenzi, EP (reprint author), Museum Conservat Inst, Smithsonian Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM vicenzie@si.edu NR 20 TC 0 Z9 0 U1 1 U2 1 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 2050-7445 J9 HERIT SCI JI Herit. Sci. PD MAY 27 PY 2016 VL 4 AR 14 DI 10.1186/s40494-016-0080-7 PG 8 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA DO4YX UT WOS:000377791900001 ER PT J AU Mathis, WN Marinoni, L AF Mathis, Wayne N. Marinoni, Luciane TI Revision of Ephydrini Zetterstedt (Diptera: Ephydridae) from the Americas south of the United States SO ZOOTAXA LA English DT Article DE Diptera; Ephydridae; Ephydrini; neotropics; new species; taxonomy ID GENUS; NORTH; FLIES AB The Neotropical genera and species of the tribe Ephydrini are revised and include nine genera and 33 species. Of the nine genera, Setacera Cresson, Cirrula Cresson, Dimecoenia Cresson, Paracoenia Cresson and Ephydra Fallen are mostly temperate in distribution, primarily in the Northern Hemisphere. The other four genera, which are exclusively Neotropical, include two, Austrocoenia and Notiocoenia, that were treated previously in the tribe Scatellini, and two recently described genera: Paraephydra (type species: Paraephydra freitasi (Oliveira)) and Neoephydra (type species: Neoephydra araucaria Mathis). New species described herein are: Neoephydra neotropica (Chile), N. dasycephala (Argentina and Peru), N. mallonota (Argentina, Bolivia, and Chile), N. shewelli (Argentina, Bolivia, and Chile), N. inca (Argentina, Bolivia, Peru), N. penai (Chile) and N. trichina (Argentina and Chile). New synonyms are (cited in their original combinations): Ephydra densepilosa Hendel = E. ciligena Rondani, Dimecoenia grumanni Oliveira = E. ciligena Rondani, D. coltaensis Cresson = D. zurcheri Hendel, D. carrerai Oliveira = D. zurcheri Hendel, D. lopesi = E. ciligena Rondani, D. travassosi Mello and Oliveira = E. prionoptera Thomson. A neotype is designated for E. caesia Wulp, and the following lectotype designations have also been made to better stabilize nomenclature (here cited in their original combination): Ephydra chilensis Macquart, Ephydra densepilosa Hendel, Ephydra pravoneura Hendel, Ephydra prionoptera Thomson, and Dimecoenia zurcheri Hendel. Dimecoenia venteli Oliveira is listed as a species inquirenda, as the type series includes only female specimens that we cannot presently recognize. Although the genera and subgenera are fairly easily distinguished, the included species are frequently difficult to separate, and we have generally relied on characters of the male terminalia to determine a species identity. Illustrations of male terminalia and distribution maps are included for each species and keys to all taxa have been provided. C1 [Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, NHB 169,POB 37012, Washington, DC 20013 USA. [Marinoni, Luciane] Univ Fed Parana, Dept Zool, BR-81531980 Curitiba, Parana, Brazil. RP Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, NHB 169,POB 37012, Washington, DC 20013 USA.; Marinoni, L (reprint author), Univ Fed Parana, Dept Zool, BR-81531980 Curitiba, Parana, Brazil. EM mathisw@si.edu; lmarinoni@ufpr.br RI Marinoni, Luciane /C-5720-2013 FU Research Opportunity Fund; Biodiversity Program (Biological Surveys and Inventories, BSI); National Museum of Natural History; Smithsonian Institution; CNPq [401609/2009-0, 201945/2012-6] FX Field work on St. Vincent, St. Lucia, and Dominica was supported by a grant from the Research Opportunity Fund, administered by Stanwyn G. Shetler, former Deputy Director, USNM. In 1995 and 1996, field work on the West Indies was funded in large measure by grants from the Biodiversity Program (Biological Surveys and Inventories, BSI), National Museum of Natural History, Smithsonian Institution (Lynne R. Parenti, chair). Field work on the West Indies was greatly expedited through the able and pleasant assistance of N. Dianne Mathis, Amnon Freidberg, collector nonpareil of Diptera, Hollis B. Williams, Kelvin Guerrero, and Oliver S. Flint, Jr., whose enthusiasm for collecting was catching.; Recent field work in Brazil (December 2009-June 2010) that resulted in many specimens studied in this paper was supported by a grant from CNPq (Visiting Researcher/Process number 401609/2009-0), which we gratefully acknowledge and thank. We thank Dianne Mathis for helping with all aspects of the production of this paper, especially field work in Brazil. We also express thanks to CNPQ for a grant to Luciane Marinoni for a postdoctoral fellowship to the National Museum of Natural History (Smithsonian Institution; Process number 201945/2012-6). NR 93 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 27 PY 2016 VL 4116 IS 1 BP 1 EP 110 DI 10.11646/zootaxa.4116.1.1 PG 110 WC Zoology SC Zoology GA DM7DE UT WOS:000376513900001 PM 27395155 ER PT J AU Schachat, SR Brown, RL AF Schachat, Sandra R. Brown, Richard L. TI Forewing color pattern in Micropterigidae (Insecta: Lepidoptera): homologies between contrast boundaries, and a revised hypothesis for the origin of symmetry systems SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Developmental constraints; Microlepidoptera; Nymphalid groundplan; Symmetry systems ID EVOLUTION; MOTH; ENDOPTERYGOTA; TRICHOPTERA; BUTTERFLIES; TORTRICIDAE; MORPHOLOGY; VENATION; NORTHERN; WINGLESS AB Background: Despite the great importance of lepidopteran wing patterns in various biological disciplines, homologies between wing pattern elements in different moth and butterfly lineages are still not understood. Among other reasons, this may be due to an incomplete understanding of the relationship between color pattern and wing venation; many individual wing pattern elements have a known relationship with venation, but a framework to unite all wing pattern elements with venation is lacking. Though plesiomorphic wing veins are known to influence color patterning even when not expressed in the adult wing, most studies of wing pattern evolution have focused on derived taxa with a reduced suite of wing veins. Results: The present study aims to address this gap through an examination of Micropterigidae, a very early-diverged moth family in which all known plesiomorphic lepidopteran veins are expressed in the adult wing. The relationship between wing pattern and venation was examined in 66 species belonging to 9 genera. The relationship between venation and pattern element location, predicted based on moths in the family Tortricidae, holds for Sabatinca just as it does for Micropterix. However, the pattern elements that are lightly colored in Micropterix are dark in Sabatinca, and vice-versa. When plotted onto a hypothetical nymphalid wing in accordance with the relationship between pattern and venation discussed here, the wing pattern of Sabatinca doroxena very closely resembles the nymphalid groundplan. Conclusions: The color difference in pattern elements between Micropterix and Sabatinca indicates that homologies exist among the contrast boundaries that divide wing pattern elements, and that color itself is not a reliable indicator of homology. The similarity between the wing pattern of Sabatinca doroxena and the nymphalid groundplan suggests that the nymphalid groundplan may have originated from a Sabatinca-like wing pattern subjected to changes in wing shape and reduced expression of venation. C1 [Schachat, Sandra R.; Brown, Richard L.] Mississippi Entomol Museum, Mississippi State, MS 39762 USA. [Schachat, Sandra R.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP Schachat, SR (reprint author), Mississippi Entomol Museum, Mississippi State, MS 39762 USA.; Schachat, SR (reprint author), Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. EM schachatsr@si.edu OI Schachat, Sandra/0000-0003-3237-5619 FU USDA National Institute of Food and Agriculture [MIS-012040]; Mather Fund of the Mississippi State University Development Foundation; National Science Foundation Graduate Research Fellowship Program [DGE-1125191]; Australian National University/National Science Foundation Graduate Research Opportunities Worldwide; National Science Foundation Graduate Research Internship Program; Sigma Xi [G201503151194219] FX The research was supported in part by the USDA National Institute of Food and Agriculture project # MIS-012040 and by the Mather Fund of the Mississippi State University Development Foundation. SRS is supported by the National Science Foundation Graduate Research Fellowship Program under grant # DGE-1125191, Australian National University/National Science Foundation Graduate Research Opportunities Worldwide, National Science Foundation Graduate Research Internship Program, and Sigma Xi Grant-in-Aid of Research # G201503151194219. NR 63 TC 3 Z9 3 U1 3 U2 5 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD MAY 26 PY 2016 VL 16 AR 116 DI 10.1186/s12862-016-0687-z PG 25 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA DM6XQ UT WOS:000376496600002 PM 27230100 ER PT J AU Cheung, E Bundy, K Cappellari, M Peirani, S Rujopakarn, W Westfall, K Yan, RB Bershady, M Greene, JE Heckman, TM Drory, N Law, DR Masters, KL Thomas, D Wake, DA Weijmans, AM Rubin, K Belfiore, F Vulcani, B Chen, YM Zhang, K Gelfand, JD Bizyaev, D Roman-Lopes, A Schneider, DP AF Cheung, Edmond Bundy, Kevin Cappellari, Michele Peirani, Sebastien Rujopakarn, Wiphu Westfall, Kyle Yan, Renbin Bershady, Matthew Greene, Jenny E. Heckman, Timothy M. Drory, Niv Law, David R. Masters, Karen L. Thomas, Daniel Wake, David A. Weijmans, Anne-Marie Rubin, Kate Belfiore, Francesco Vulcani, Benedetta Chen, Yan-mei Zhang, Kai Gelfand, Joseph D. Bizyaev, Dmitry Roman-Lopes, A. Schneider, Donald P. TI Suppressing star formation in quiescent galaxies with supermassive black hole winds SO NATURE LA English DT Article ID MULTI-GAUSSIAN EXPANSION; ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; FORMATION HISTORIES; LUMINOSITY FUNCTION; ELLIPTIC GALAXIES; AGN POPULATION; STELLAR MASSES; COOLING FLOWS; HOST GALAXIES AB Quiescent galaxies with little or no ongoing star formation dominate the population of galaxies with masses above 2 x 10(10) times that of the Sun; the number of quiescent galaxies has increased by a factor of about 25 over the past ten billion years (refs 1-4). Once star formation has been shut down, perhaps during the quasar phase of rapid accretion onto a supermassive black hole(5-7), an unknown mechanism must remove or heat the gas that is subsequently accreted from either stellar mass loss(8) or mergers and that would otherwise cool to form stars(9,10). Energy output from a black hole accreting at a low rate has been proposed(11-13), but observational evidence for this in the form of expanding hot gas shells is indirect and limited to radio galaxies at the centres of clusters(14,15), which are too rare to explain the vast majority of the quiescent population(16). Here we report bisymmetric emission features co-aligned with strong ionized-gas velocity gradients from which we infer the presence of centrally driven winds in typical quiescent galaxies that host low-luminosity active nuclei. These galaxies are surprisingly common, accounting for as much as ten per cent of the quiescent population with masses around 2 x 10(10) times that of the Sun. In a prototypical example, we calculate that the energy input from the galaxy's low-level active supermassive black hole is capable of driving the observed wind, which contains sufficient mechanical energy to heat ambient, cooler gas (also detected) and thereby suppress star formation. C1 [Cheung, Edmond; Bundy, Kevin; Peirani, Sebastien; Rujopakarn, Wiphu; Vulcani, Benedetta] Univ Tokyo, World Premier Int Res Ctr Initiative, Kavli Inst Phys & Math Universe, Inst Adv Study, Kashiwa, Chiba 2778583, Japan. [Cappellari, Michele] Univ Oxford, Subdept Astrophys, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. [Peirani, Sebastien] CNRS, UMR 7095, Inst Astrophys Paris, 98 Bis Blvd Arago, F-75014 Paris, France. [Peirani, Sebastien] UPMC, 98 Bis Blvd Arago, F-75014 Paris, France. [Rujopakarn, Wiphu] Chulalongkorn Univ, Dept Phys, Fac Sci, 254 Phayathai Rd, Bangkok 10330, Thailand. [Westfall, Kyle; Masters, Karen L.; Thomas, Daniel] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg,Burnaby Rd, Portsmouth PO1 3FX, Hants, England. [Yan, Renbin; Zhang, Kai] Univ Kentucky, Dept Phys & Astron, 505 Rose St, Lexington, KY 40506 USA. [Bershady, Matthew; Wake, David A.] Univ Wisconsin, Dept Astron, 475 North Charter St, Madison, WI 53706 USA. [Greene, Jenny E.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Heckman, Timothy M.] Johns Hopkins Univ, Dept Phys & Astron, Ctr Astrophys Sci, Baltimore, MD 21218 USA. [Drory, Niv] Univ Texas Austin, Dept Astron, McDonald Observ, 1 Univ Stn, Austin, TX 78712 USA. [Law, David R.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Wake, David A.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Weijmans, Anne-Marie] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Rubin, Kate] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Belfiore, Francesco] Univ Cambridge, Cavendish Lab, 19 JJ Thomson Ave, Cambridge CB3 0HE, England. [Belfiore, Francesco] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HE, England. [Chen, Yan-mei] Nanjing Univ, Dept Astron, Nanjing 210093, Jiangsu, Peoples R China. [Gelfand, Joseph D.] New York Univ Abu Dhabi, POB 129188, Abu Dhabi, U Arab Emirates. [Gelfand, Joseph D.] NYU, Ctr Cosmol & Particle Phys, Meyer Hall Phys,4 Washington Pl, New York, NY 10003 USA. [Bizyaev, Dmitry] Apache Point Observ, POB 59, Sunspot, NM 88349 USA. [Bizyaev, Dmitry] New Mexico State Univ, POB 59, Sunspot, NM 88349 USA. [Bizyaev, Dmitry] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow, Russia. [Roman-Lopes, A.] Univ La Serena, Fac Ciencias, Dept Fis & Astron, Cisternas 1200, La Serena, Chile. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. RP Cheung, E (reprint author), Univ Tokyo, World Premier Int Res Ctr Initiative, Kavli Inst Phys & Math Universe, Inst Adv Study, Kashiwa, Chiba 2778583, Japan. EM ec2250@gmail.com OI Cheung, Edmond/0000-0001-8546-1428; Vulcani, Benedetta/0000-0003-0980-1499; Rujopakarn, Wiphu/0000-0002-0303-499X; Cappellari, Michele/0000-0002-1283-8420 FU World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan; JSPS KAKENHI [15K17603]; Leverhulme Trust; Japan Society for the Promotion of Science (JSPS); Royal Society; Chulalongkorn University; Alfred P. Sloan Foundation; US Department of Energy Office of Science; Center for High-Performance Computing at the University of Utah; Brazilian Participation Group; Carnegie Institution for Science; Carnegie Mellon University; Chilean Participation Group; French Participation Group; Harvard-Smithsonian Center for Astrophysics; Instituto de Astrofisica de Canarias; Johns Hopkins University; Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo; Lawrence Berkeley National Laboratory; Leibniz Institut fur Astrophysik Potsdam (AIP); Max-Planck-Institut fur Astronomie (MPIA Heidelberg); Max-Planck-Institut fur Astrophysik (MPA Garching); Max-Planck-Institut fur Extraterrestrische Physik (MPE); National Astronomical Observatory of China; New Mexico State University; New York University; University of Notre Dame; Observatorio Nacional/MCTI; Ohio State University; Pennsylvania State University; Shanghai Astronomical Observatory; UK Participation Group; Universidad Nacional Autonoma de Mexico; University of Arizona; University of Colorado Boulder; University of Oxford; University of Portsmouth; University of Utah; University of Virginia; University of Washington; University of Wisconsin; Vanderbilt University; Yale University FX We are grateful to Y.-Y. Chang for checks on the SED fitting and implied SFR. We thank S. Juneau, J. Newman, H. Fu, K. Nyland, and S. F. Sanchez for discussions and comments. This work was supported by the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and JSPS KAKENHI grant no. 15K17603. A.W. acknowledges support of a Leverhulme Trust Early Career Fellowship. S.P. acknowledges support from the Japan Society for the Promotion of Science (JSPS long-term invitation fellowship). M.C. acknowledges support from a Royal Society University Research Fellowship. W.R. is supported by a CUniverse Grant (CUAASC) from Chulalongkorn University. Funding for the Sloan Digital Sky Survey IV (SDSS-VI) has been provided by the Alfred P. Sloan Foundation, the US Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration, including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofisica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut fur Astrophysik Potsdam (AIP), Max-Planck-Institut fur Astronomie (MPIA Heidelberg), Max-Planck-Institut fur Astrophysik (MPA Garching), Max-Planck-Institut fur Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observatorio Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, UK Participation Group, Universidad Nacional Autonoma de Mexico, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University and Yale University. NR 69 TC 11 Z9 11 U1 2 U2 7 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAY 26 PY 2016 VL 533 IS 7604 BP 504 EP + DI 10.1038/nature18006 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DM6EJ UT WOS:000376443100034 PM 27225122 ER PT J AU Farji-Brener, AG Elizalde, L Fernandez-Marin, H Amador-Vargas, S AF Farji-Brener, Alejandro G. Elizalde, Luciana Fernandez-Marin, Hermogenes Amador-Vargas, Sabrina TI Social life and sanitary risks: evolutionary and current ecological conditions determine waste management in leaf-cutting ants SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Acromyrmex; ant waste; ant behaviour; Atta; group living; waste management ID DIVISION-OF-LABOR; ATTA-SEXDENS-RUBROPILOSA; ACROMYRMEX-LOBICORNIS; FOREL HYMENOPTERA; REFUSE DUMPS; NEST; FORMICIDAE; COLOMBICA; COLONY; CEPHALOTES AB Adequate waste management is vital for the success of social life, because waste accumulation increases sanitary risks in dense societies. We explored why different leaf-cutting ants (LCA) species locate their waste in internal nest chambers or external piles, including ecological context and accounting for phylogenetic relations. We propose that waste location depends on whether the environmental conditions enhance or reduce the risk of infection. We obtained the geographical range, habitat and refuse location of LCA from published literature, and experimentally determined whether pathogens on ant waste survived to the high soil temperatures typical of xeric habitats. The habitat of the LCA determined waste location after phylogenetic correction: species with external waste piles mainly occur in xeric environments, whereas those with internal waste chambers mainly inhabit more humid habitats. The ancestral reconstruction suggests that dumping waste externally is less derived than digging waste nest chambers. Empirical results showed that high soil surface temperatures reduce pathogen prevalence from LCA waste. We proposed that LCA living in environments unfavourable for pathogens (i.e. xeric habitats) avoid digging costs by dumping the refuse above ground. Conversely, in environments suitable for pathogens, LCA species prevent the spread of diseases by storing waste underground, presumably, a behaviour that contributed to the colonization of humid habitats. These results highlight the adaptation of organisms to the hygienic challenges of social living, and illustrate how sanitary behaviours can result from a combination of evolutionary history and current environmental conditions. C1 [Farji-Brener, Alejandro G.; Elizalde, Luciana] INIBIOMA CONICET, Lab Ecotono, Pasaje Gutierrez 1125, RA-8400 San Carlos De Bariloche, Rio Negro, Argentina. [Fernandez-Marin, Hermogenes] Inst Invest Cient & Serv Alta Tecnol, Ctr Biodiversidad & Descrubrimiento Drogas, Panama City, Panama. [Amador-Vargas, Sabrina] Smithsonian Trop Res Inst, Panama City, Panama. RP Farji-Brener, AG (reprint author), INIBIOMA CONICET, Lab Ecotono, Pasaje Gutierrez 1125, RA-8400 San Carlos De Bariloche, Rio Negro, Argentina. EM alefarji@yahoo.com OI Farji-Brener, Alejandro Gustavo/0000-0001-7251-3866 FU Smithsonian Tropical Research Institute; FONCYT, Argentina [PICT1406]; SNI FX A.G.F.-B. was partially funded by a fellowship of the Smithsonian Tropical Research Institute and a grant of FONCYT, Argentina (PICT1406). H.F.-M. was supported by SNI funds. NR 72 TC 2 Z9 2 U1 5 U2 7 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD MAY 25 PY 2016 VL 283 IS 1831 AR 20160625 DI 10.1098/rspb.2016.0625 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA DP2KW UT WOS:000378318300019 ER PT J AU Trillo, PA Bernal, XE Caldwell, MS Halfwerk, WH Wessel, MO Page, RA AF Trillo, Paula A. Bernal, Ximena E. Caldwell, Michael S. Halfwerk, Wouter H. Wessel, Mallory O. Page, Rachel A. TI Collateral damage or a shadow of safety? The effects of signalling heterospecific neighbours on the risks of parasitism and predation SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE mating signals; risk; tu'ngara frogs; hourglass treefrogs; Trachops cirrhosus; Corethrella midges ID FROG-BITING MIDGES; LOCALIZATION PERFORMANCE; NEOTROPICAL TREEFROG; SEXUAL SELECTION; HYLA-EBRACCATA; BAT PREDATION; TUNGARA FROG; MATE CHOICE; BEHAVIOR; ANURAN AB Although males often display from mixed-species aggregations, the influence of nearby heterospecifics on risks associated with sexual signalling has not been previously examined. We tested whether predation and parasitism risks depend on proximity to heterospecific signallers. Using field playback experiments with calls of two species that often display from the same ponds, tu'ngara frogs and hourglass treefrogs, we tested two hypotheses: (1) calling near heterospecific signallers attractive to eavesdroppers results in increased attention from predatory bats and parasitic midges (collateral damage hypothesis) or (2) calling near heterospecific signallers reduces an individual's predation and parasitism risks, as eavesdroppers are drawn to the heterospecifics (shadow of safety hypothesis). Bat visitation was not affected by calling neighbours. The number of frog-biting midges attracted to hourglass treefrog calls, however, rose threefold when played near tu'ngara calls, supporting the collateral damage hypothesis. We thus show that proximity to heterospecific signallers can drastically alter both the absolute risks of signalling and the relative strengths of pressures from predation and parasitism. Through these mechanisms, interactions between heterospecific guild members are likely to influence the evolution of signalling strategies and the distribution of species at both local and larger scales. C1 [Trillo, Paula A.; Caldwell, Michael S.] Gettysburg Coll, Dept Biol, Gettysburg, PA 17325 USA. [Trillo, Paula A.; Bernal, Ximena E.; Caldwell, Michael S.; Halfwerk, Wouter H.; Wessel, Mallory O.; Page, Rachel A.] Smithsonian Trop Res Inst, Panama City, Panama. [Bernal, Ximena E.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. [Halfwerk, Wouter H.] Vrije Univ Amsterdam, Dept Ecol Sci, Amsterdam, Netherlands. [Wessel, Mallory O.] Butler Univ, Dept Biol Sci, Indianapolis, IN 46208 USA. RP Trillo, PA (reprint author), Gettysburg Coll, Dept Biol, Gettysburg, PA 17325 USA.; Trillo, PA (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM ptrillo@gettysburg.edu FU Smithsonian Tropical Institute; Butler University; NSF IOS [1433990] FX This research was funded by a Smithsonian Tropical Institute and Butler University post-doctoral fellowship to P.A.T. X.E.B. was funded by NSF IOS no. 1433990. NR 44 TC 0 Z9 0 U1 4 U2 9 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD MAY 25 PY 2016 VL 283 IS 1831 AR 20160343 DI 10.1098/rspb.2016.0343 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA DP2KW UT WOS:000378318300010 ER PT J AU Ma, ZY Wen, J Ickert-Bond, SM Chen, LQ Liu, XQ AF Ma, Zhi-Yao Wen, Jun Ickert-Bond, Stefanie M. Chen, Long-Qing Liu, Xiu-Qun TI Morphology, Structure, and Ontogeny of Trichomes of the Grape Genus (Vitis, Vitaceae) SO FRONTIERS IN PLANT SCIENCE LA English DT Article DE Vitis; trichome; morphology; structure; ontogeny; SEM; TEM ID PELTATE GLANDULAR TRICHOMES; ULTRAVIOLET-B RADIATION; DOWNY MILDEW RESISTANCE; NICOTIANA-TABACUM-L; PHYLOGENETIC ANALYSIS; ELECTRON-MICROSCOPY; LEONOTIS LEONURUS; UNCINULA-NECATOR; POWDERY MILDEW; RESIN GLANDS AB Trichomes are widely distributed on surfaces of different organs in the grape genus Vitis and are of taxonomic utility. To explore the morphology, structure and ontogeny of Vitis trichomes, we investigated the diversity and distribution of trichomes in 34 species of Vitis. Two main types of trichomes in Vitis are documented: non-glandular and glandular. Within non -glandular trichomes, ribbon and simple trichomes are found on different vegetative plant organs. The morphology and ontogeny of these types of trichomes are further examined with light microscopy and scanning electron microscopy. The ultrastructure of the glandular trichomes is explored with transmission electron microscopy. The ribbon trichomes are twisted, greatly elongated and unicellular, and this trichome type may be a morphological synapomorphy of Vitis and its closest tropical relative Ampelocissus and Pterisanthes in Vitaceae. The simple trichomes are documented in most species sampled in the genus. The glandular trichomes are multicellular, non-vascularized and composed of both epidermis and subjacent layers. We show that prickles occurring along the stems and petioles of Vitis davidii are modified glandular trichomes. We observed that glandular trichomes of V romanetii secrete mucilage and volatile substances which trap insectes on the glands. Transmission electron microscopy indicates that metabolic products accumulate in vacuoles, the cytoplasm and intercellular spaces. We infer that glandular trichomes and young prickles are involved in the secretion of these metabolic products and the intercellular spaces may be the places of temporary storage of these secretions. C1 [Ma, Zhi-Yao; Chen, Long-Qing; Liu, Xiu-Qun] Huazhong Agr Univ, Coll Hort & Forestry Sci, Key Lab Hort Plant Biol, Minist Educ, Wuhan, Peoples R China. [Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC166, Washington, DC 20560 USA. [Ickert-Bond, Stefanie M.] Univ Alaska Fairbanks, UA Museum North Herbarium, Fairbanks, AK USA. [Ickert-Bond, Stefanie M.] Univ Alaska Fairbanks, Dept Biol & Wildlife, Fairbanks, AK USA. RP Liu, XQ (reprint author), Huazhong Agr Univ, Coll Hort & Forestry Sci, Key Lab Hort Plant Biol, Minist Educ, Wuhan, Peoples R China. EM liu_xiuqun@sina.com RI Ickert-Bond, Stefanie/B-3216-2012 OI Ickert-Bond, Stefanie/0000-0001-8198-8898 FU National Natural Science Foundation of China [31370249, 31570216] FX This work was supported by the National Natural Science Foundation of China (Grants No. 31370249, No. 31570216). NR 69 TC 1 Z9 1 U1 12 U2 23 PU FRONTIERS MEDIA SA PI LAUSANNE PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015, SWITZERLAND SN 1664-462X J9 FRONT PLANT SCI JI Front. Plant Sci. PD MAY 25 PY 2016 VL 7 AR 704 DI 10.3389/fpls.2016.00704 PG 14 WC Plant Sciences SC Plant Sciences GA DN0HH UT WOS:000376744500001 PM 27252720 ER PT J AU Pikovski, I Loeb, A AF Pikovski, Igor Loeb, Abraham TI Quantum coherent oscillations in the early universe SO PHYSICAL REVIEW D LA English DT Article ID INFLATIONARY UNIVERSE; BLOCH OSCILLATIONS; ELECTRIC-FIELD; LATTICES; SUPERLATTICE; DYNAMICS; FLATNESS; HORIZON; MODEL AB Cosmic inflation is commonly assumed to be driven by quantum fields. Quantum mechanics predicts phenomena such as quantum fluctuations and tunneling of the field. Here, we show an example of a quantum interference effect which goes beyond the semiclassical treatment and which may be of relevance in the early Universe. We study the quantum coherent dynamics for a tilted, periodic potential, which results in genuine quantum oscillations of the inflaton field, analogous to Bloch oscillations in condensed matter and atomic systems. The underlying quantum superpositions are typically very fragile but may persist in the early Universe giving rise to quantum interference phenomena in cosmology. C1 [Pikovski, Igor] Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. [Pikovski, Igor] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, ITC, 60 Garden St, Cambridge, MA 02138 USA. [Loeb, Abraham] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. RP Pikovski, I (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA.; Pikovski, I (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.; Loeb, A (reprint author), Harvard Smithsonian Ctr Astrophys, ITC, 60 Garden St, Cambridge, MA 02138 USA.; Loeb, A (reprint author), Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. EM igor.pikovski@cfa.harvard.edu; aloeb@cfa.harvard.edu OI Pikovski, Igor/0000-0002-9441-2553 FU NSF [AST-1312034] FX We thank Cliff Burgess, Xingang Chen, James Hartle, Juan Maldacena, Stefan Pabst, Richard Schmidt and Alexander Vilenkin for discussions. This work was supported in part by NSF through Grant No. AST-1312034 and through a grant to ITAMP. NR 32 TC 1 Z9 1 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD MAY 25 PY 2016 VL 93 IS 10 AR 101302 DI 10.1103/PhysRevD.93.101302 PG 6 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA DM8VZ UT WOS:000376643900001 ER PT J AU Bhattacharya, D Agrawal, S Aranda, M Baumgarten, S Belcaid, M Drake, JL Erwin, D Foret, S Gates, RD Gruber, DF Kamel, B Lesser, MP Levy, O Liew, YJ MacManes, M Mass, T Medina, M Mehr, S Meyer, E Price, DC Putnam, HM Qiu, H Shinzato, C Shoguchi, E Stokes, AJ Tambutte, S Tchernov, D Voolstra, CR Wagner, N Walker, CW Weber, APM Weis, V Zelzion, E Zoccola, D Falkowski, PG AF Bhattacharya, Debashish Agrawal, Shobhit Aranda, Manuel Baumgarten, Sebastian Belcaid, Mandi Drake, Jeana L. Erwin, Douglas Foret, Sylvian Gates, Ruth D. Gruber, David F. Kamel, Bishoy Lesser, Michael P. Levy, Oren Liew, Yi Jin MacManes, Matthew Mass, Tali Medina, Monica Mehr, Shaadi Meyer, Eli Price, Dana C. Putnam, Hollie M. Qiu, Huan Shinzato, Chuya Shoguchi, Eiichi Stokes, Alexander J. Tambutte, Sylvie Tchernov, Dan Voolstra, Christian R. Wagner, Nicole Walker, Charles W. Weber, Andreas P. M. Weis, Virginia Zelzion, Ehud Zoccola, Didier Falkowski, Paul G. TI Comparative genomics explains the evolutionary success of reef-forming corals SO ELIFE LA English DT Article ID ACID-RICH PROTEINS; STYLOPHORA-PISTILLATA; ACROPORA-MILLEPORA; ORGANIC MATRIX; DINOFLAGELLATE SYMBIOSIS; MOLECULAR-CLONING; ALGAL SYMBIONTS; BUILDING CORAL; SHELL MATRIX; CD-HIT AB Transcriptome and genome data from twenty stony coral species and a selection of reference bilaterians were studied to elucidate coral evolutionary history. We identified genes that encode the proteins responsible for the precipitation and aggregation of the aragonite skeleton on which the organisms live, and revealed a network of environmental sensors that coordinate responses of the host animals to temperature, light, and pH. Furthermore, we describe a variety of stress-related pathways, including apoptotic pathways that allow the host animals to detoxify reactive oxygen and nitrogen species that are generated by their intracellular photosynthetic symbionts, and determine the fate of corals under environmental stress. Some of these genes arose through horizontal gene transfer and comprise at least 0.2% of the animal gene inventory. Our analysis elucidates the evolutionary strategies that have allowed symbiotic corals to adapt and thrive for hundreds of millions of years. C1 [Bhattacharya, Debashish; Qiu, Huan; Wagner, Nicole; Zelzion, Ehud] Rutgers State Univ, Dept Ecol Evolut & Nat Resources, New Brunswick, NJ 08903 USA. [Bhattacharya, Debashish] Rutgers State Univ, Dept Marine & Coastal Sci, New Brunswick, NJ 08903 USA. [Agrawal, Shobhit; Aranda, Manuel; Baumgarten, Sebastian; Liew, Yi Jin; Voolstra, Christian R.] King Abdullah Univ Sci & Technol, Biol & Environm Sci & Engn Div, Red Sea Res Ctr, Thuwal, Saudi Arabia. [Belcaid, Mandi; Gates, Ruth D.; Putnam, Hollie M.] Hawaii Inst Marine Biol, Kaneohe, HI USA. [Drake, Jeana L.; Mass, Tali; Falkowski, Paul G.] Rutgers State Univ, Dept Marine & Coastal Sci, Environm Biophys & Mol Ecol Program, New Brunswick, NJ 08903 USA. [Erwin, Douglas] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Foret, Sylvian] James Cook Univ, ARC Ctr Excellence Coral Reef Studies, Townsville, Qld 4811, Australia. [Foret, Sylvian] Australian Natl Univ, Res Sch Biol, Canberra, ACT, Australia. [Gruber, David F.; Mehr, Shaadi] Amer Museum Nat Hist, Sackler Inst Comparat Genom, New York, NY 10024 USA. [Gruber, David F.] CUNY Bernard M Baruch Coll, Dept Nat Sci, 17 Lexington Ave, New York, NY 10010 USA. [Gruber, David F.] CUNY, Grad Ctr, New York, NY USA. [Kamel, Bishoy; Medina, Monica] Penn State Univ, Dept Biol, Mueller Lab, University Pk, PA 16802 USA. [Lesser, Michael P.] Univ New Hampshire, Sch Marine Sci & Ocean Engn, Durham, NH 03824 USA. [Levy, Oren] Bar Ilan Univ, Mina & Everard Goodman Fac Life Sci, Ramat Gam, Israel. [MacManes, Matthew; Walker, Charles W.] Univ New Hampshire, Dept Mol Cellular & Biomed Sci, Durham, NH 03824 USA. [Mass, Tali; Tchernov, Dan] Univ Haifa, Leon H Charney Sch Marine Sci, Dept Marine Biol, Har Hakarmel, Israel. [Mehr, Shaadi] SUNY Coll Old Westbury, Dept Biol Sci, Old Westbury, NY USA. [Meyer, Eli; Weis, Virginia] Oregon State Univ, Dept Integrat Biol, Corvallis, OR 97331 USA. [Price, Dana C.] Rutgers State Univ, Dept Plant Biol & Pathol, New Brunswick, NJ 08903 USA. [Shinzato, Chuya; Shoguchi, Eiichi] Okinawa Inst Sci & Technol Grad Univ, Marine Genom Unit, Okinawa, Japan. [Stokes, Alexander J.] Univ Hawaii, John A Burns Sch Med, Expt Med Lab, Honolulu, HI 96822 USA. [Stokes, Alexander J.] Univ Hawaii, John A Burns Sch Med, Dept Cell & Mol Biol, Honolulu, HI 96822 USA. [Tambutte, Sylvie; Zoccola, Didier] Ctr Sci Monaco, Monaco, Monaco. [Weber, Andreas P. M.] Univ Dusseldorf, Inst Plant Biochem, Dusseldorf, Germany. [Falkowski, Paul G.] Rutgers State Univ, Dept Earth & Planetary Sci, Piscataway, NJ 08855 USA. RP Bhattacharya, D (reprint author), Rutgers State Univ, Dept Ecol Evolut & Nat Resources, New Brunswick, NJ 08903 USA.; Bhattacharya, D (reprint author), Rutgers State Univ, Dept Marine & Coastal Sci, New Brunswick, NJ 08903 USA.; Falkowski, PG (reprint author), Rutgers State Univ, Dept Marine & Coastal Sci, Environm Biophys & Mol Ecol Program, New Brunswick, NJ 08903 USA.; Falkowski, PG (reprint author), Rutgers State Univ, Dept Earth & Planetary Sci, Piscataway, NJ 08855 USA. EM d.bhattacharya@rutgers.edu; falko@marine.rutgers.edu RI Weber, Andreas/A-6250-2011; Zoccola, Didier/A-5997-2009; Aranda Lastra, Manuel/D-9530-2011; OI Weber, Andreas/0000-0003-0970-4672; Zoccola, Didier/0000-0002-1524-8098; Aranda Lastra, Manuel/0000-0001-6673-016X; Liew, Yi Jin/0000-0003-2553-8870; Kamel, Bishoy/0000-0003-2934-3827 FU National Science Foundation [EF-1416785, EF-1041143/RU 432635]; National Institutes of Health, NIMHD [P20MD006084]; Hawaii Community Foundation; Leahi Fund [13ADVC-60228]; NSF OCE PRF [1323822]; National Science Foundation Experimental Program [EPS-0903833]; King Abdullah University of Science and Technology (KAUST) FX National Science Foundation EF-1416785 Paul G Falkowskir This work was made possible by grants from the National Science Foundation, EF-1041143/RU 432635 and EF-1416785 awarded to PGF, DB, and TM, respectively. RDG, HMP, and AJS were supported by grants from the National Institutes of Health, NIMHD P20MD006084, the Hawaii Community Foundation, Leahi Fund 13ADVC-60228 and NSF OCE PRF 1323822 and National Science Foundation Experimental Program to Stimulate Competitive Research Hawaii: EPS-0903833. CRV and MA acknowledge funding by the King Abdullah University of Science and Technology (KAUST). NR 114 TC 10 Z9 10 U1 10 U2 20 PU ELIFE SCIENCES PUBLICATIONS LTD PI CAMBRIDGE PA SHERATON HOUSE, CASTLE PARK, CAMBRIDGE, CB3 0AX, ENGLAND SN 2050-084X J9 ELIFE JI eLife PD MAY 24 PY 2016 VL 5 AR e13288 DI 10.7554/eLife.13288 PG 26 WC Biology SC Life Sciences & Biomedicine - Other Topics GA DN5QG UT WOS:000377124600001 PM 27218454 ER PT J AU Muller, MA Devignot, S Lattwein, E Corman, VM Maganga, GD Gloza-Rausch, F Binger, T Vallo, P Emmerich, P Cottontail, VM Tschapka, M Oppong, S Drexler, JF Weber, F Leroy, EM Drosten, C AF Mueller, Marcel A. Devignot, Stephanie Lattwein, Erik Corman, Victor Max Maganga, Gael D. Gloza-Rausch, Florian Binger, Tabea Vallo, Peter Emmerich, Petra Cottontail, Veronika M. Tschapka, Marco Oppong, Samuel Drexler, Jan Felix Weber, Friedemann Leroy, Eric M. Drosten, Christian TI Evidence for widespread infection of African bats with Crimean-Congo hemorrhagic fever-like viruses SO SCIENTIFIC REPORTS LA English DT Article ID SHEEP DISEASE VIRUS; FAMILY BUNYAVIRIDAE; SEROLOGICAL RELATIONSHIPS; ANTIBODY-RESPONSE; MIGRATORY BIRDS; RAPID DETECTION; VIRAL LOAD; TICKS; NAIROVIRUS; GENUS AB Crimean Congo hemorrhagic fever virus (CCHFV) is a highly virulent tick-borne pathogen that causes hemorrhagic fever in humans. The geographic range of human CCHF cases largely reflects the presence of ticks. However, highly similar CCHFV lineages occur in geographically distant regions. Tick-infested migratory birds have been suggested, but not confirmed, to contribute to the dispersal. Bats have recently been shown to carry nairoviruses distinct from CCHFV. In order to assess the presence of CCHFV in a wide range of bat species over a wide geographic range, we analyzed 1,135 sera from 16 different bat species collected in Congo, Gabon, Ghana, Germany, and Panama. Using a CCHFV glycoprotein-based indirect immunofluorescence test (IIFT), we identified reactive antibodies in 10.0% (114/1,135) of tested bats, pertaining to 12/16 tested species. Depending on the species, 3.6%-42.9% of cave-dwelling bats and 0.6%-7.1% of foliage-living bats were seropositive (two-tailed t-test, p = 0.0447 cave versus foliage). 11/30 IIFT-reactive sera from 10 different African bat species had neutralizing activity in a virus-like particle assay. Neutralization of full CCHFV was confirmed in 5 of 7 sera. Widespread infection of cave-dwelling bats may indicate a role for bats in the life cycle and geographic dispersal of CCHFV. C1 [Mueller, Marcel A.; Corman, Victor Max; Binger, Tabea; Drexler, Jan Felix; Drosten, Christian] Univ Bonn, Med Ctr, Bonn, Germany. [Devignot, Stephanie; Weber, Friedemann] Univ Marburg, Inst Virol, D-35032 Marburg, Germany. [Devignot, Stephanie; Weber, Friedemann] Univ Giessen, Inst Virol, Vet Med FB10, Frankfurter Str 107, Giessen, Germany. [Lattwein, Erik] EUROIMMUN AG, Lubeck, Germany. [Corman, Victor Max; Drexler, Jan Felix; Drosten, Christian] German Ctr Infect Res DZIF, Partner Site Bonn Cologne, Bonn, Germany. [Maganga, Gael D.; Leroy, Eric M.] Ctr Int Rech Med Franceville, BP 769, Franceville, Gabon. [Gloza-Rausch, Florian] Noctalis, Bad Segeberg, Germany. [Vallo, Peter] Acad Sci Czech Republic, Inst Vertebrate Biol, Brno, Czech Republic. [Emmerich, Petra; Tschapka, Marco; Oppong, Samuel] Univ Ulm, D-89069 Ulm, Germany. [Emmerich, Petra] Bernhard Nocht Inst Trop Med, Bernhard Nocht Str 74, D-20359 Hamburg, Germany. [Cottontail, Veronika M.; Tschapka, Marco] Smithsonian Trop Res Inst, Balboa, Panama. [Oppong, Samuel] Kwame Nkrumah Univ Sci & Technol, Kumasi, Ghana. [Leroy, Eric M.] Inst Rech Dev, Montpellier, France. RP Drosten, C (reprint author), Univ Bonn, Med Ctr, Bonn, Germany.; Drosten, C (reprint author), German Ctr Infect Res DZIF, Partner Site Bonn Cologne, Bonn, Germany. EM drosten@virology-bonn.de RI Vallo, Peter/F-9650-2014; LEROY, Eric/I-4347-2016; OI LEROY, Eric/0000-0003-0022-0890; Corman, Victor Max/0000-0002-3605-0136 FU European Commission [278976, 260427]; Deutsche Forschungsgemeinschaft [DR772/3-1, DR772/12-1, DR722/10-1, We 2616/7-1, MU 3564/1-1, KA 1241/18-1] FX We thank Stephan Kallies, Monika Eschbach-Bludau, Tobias Bleicker, Sebastian Brunink and Anette Klein for excellent technical assistance, Gudrun Wibbelt and Kristin Muhldorfer (IZW, Berlin) for providing bat serum samples, Antje Seebens (Noctalis) for field work in Ghana, and Eric Bergeron and Stuart Nichol for donating the original minireplicon plasmids. We thank Tasnim Suliman (Stellenbosch University) for critically reading the manuscript and Dennis Bente (UTMB, Galveston) for helpful comments. The CCHFV N antibody and CCHFV strain IbAr10200 were kindly provided by Ali Mirazimi, SMI, Sweden. The CCHFV positive serum was provided by Gulay Korukluoglu (Refik Saydam National Public Health Agency, Ankara, Turkey), and the negative human serum by Andreas Kaufmann (Philipps Universitat Marburg, Germany). This work was supported by European Commission projects Antigone (contract no. 278976 to CD) and CCHFever Network (contract no. 260427 to FW). Samples and essential reagents were contributed by earlier projects funded by the Deutsche Forschungsgemeinschaft, including grants DR772/3-1, DR772/12-1, DR722/10-1 to CD, We 2616/7-1 to FW, MU 3564/1-1 to MAM, KA 1241/18-1 to E. Kalko and MT). The funders had no role in study design, data collection and analysis, decision to publish or preparation of the manuscript. NR 54 TC 2 Z9 3 U1 6 U2 8 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 MAY 24 PY 2016 VL 6 AR 26637 DI 10.1038/srep26637 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DM5LA UT WOS:000376389300001 PM 27217069 ER PT J AU Jiang, DY Motani, R Huang, JD Tintori, A Hu, YC Rieppel, O Fraser, NC Ji, C Kelley, NP Fu, WL Zhang, R AF Jiang, Da-Yong Motani, Ryosuke Huang, Jian-Dong Tintori, Andrea Hu, Yuan-Chao Rieppel, Olivier Fraser, Nicholas C. Ji, Cheng Kelley, Neil P. Fu, Wan-Lu Zhang, Rong TI A large aberrant stem ichthyosauriform indicating early rise and demise of ichthyosauromorphs in the wake of the end-Permian extinction SO SCIENTIFIC REPORTS LA English DT Article ID MASS EXTINCTION; SOUTH CHINA; EVOLUTION; REPTILIA; SAUROPTERYGIA; DIVERSITY; RECOVERY; ORIGIN; GEN. AB Contrary to the fast radiation of most metazoans after the end-Permian mass extinction, it is believed that early marine reptiles evolved slowly during the same time interval. However, emerging discoveries of Early Triassic marine reptiles are questioning this traditional view. Here we present an aberrant basal ichthyosauriform with a hitherto unknown body design that suggests a fast radiation of early marine reptiles. The new species is larger than coeval marine reptiles and has an extremely small head and a long tail without a fluke. Its heavily-built body bears flattened and overlapping gastral elements reminiscent of hupehsuchians. A phylogenetic analysis places the new species at the base of ichthyosauriforms, as the sister taxon of Cartorhynchus with which it shares a short snout with rostrally extended nasals. It now appears that ichthyosauriforms evolved rapidly within the first one million years of their evolution, in the Spathian (Early Triassic), and their true diversity has yet to be fully uncovered. Early ichthyosauromorphs quickly became extinct near the Early-Middle Triassic boundary, during the last large environmental perturbation after the end-Permian extinction involving redox fluctuations, sea level changes and volcanism. Marine reptile faunas shifted from ichthyosauromorph-dominated to sauropterygian-dominated composition after the perturbation. C1 [Jiang, Da-Yong; Fu, Wan-Lu] Peking Univ, Minist Educ, Lab Orogen Belt & Crustal Evolut, Yiheyuan St 5, Beijing 100871, Peoples R China. [Jiang, Da-Yong; Fu, Wan-Lu] Peking Univ, Dept Geol, Yiheyuan St 5, Beijing 100871, Peoples R China. [Jiang, Da-Yong; Fu, Wan-Lu] Peking Univ, Geol Museum, Yiheyuan St 5, Beijing 100871, Peoples R China. [Motani, Ryosuke] Univ Calif Davis, Dept Earth & Planetary Sci, One Shields Ave, Davis, CA 95616 USA. [Huang, Jian-Dong; Hu, Yuan-Chao; Zhang, Rong] Anhui Geol Museum, Dept Res, Jiahe Rd 999, Hefei 230031, Anhui, Peoples R China. [Tintori, Andrea] Univ Milan, Dipartimento Sci Terra, Via Mangiagalli 34, I-20133 Milan, Italy. [Rieppel, Olivier] Field Museum, Ctr Integrat Res, Chicago, IL 60605 USA. [Fraser, Nicholas C.] Natl Museums Scotland, Chambers St, Edinburgh EH1 1JF, Midlothian, Scotland. [Ji, Cheng] Chinese Acad Sci, Nanjing Inst Geol & Palaeontol, Key Lab Econ Stratig & Palaeogeog, 39 East Beijing Rd, Nanjing 210008, Jiangsu, Peoples R China. [Kelley, Neil P.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. RP Jiang, DY (reprint author), Peking Univ, Minist Educ, Lab Orogen Belt & Crustal Evolut, Yiheyuan St 5, Beijing 100871, Peoples R China.; Jiang, DY (reprint author), Peking Univ, Dept Geol, Yiheyuan St 5, Beijing 100871, Peoples R China.; Jiang, DY (reprint author), Peking Univ, Geol Museum, Yiheyuan St 5, Beijing 100871, Peoples R China.; Motani, R (reprint author), Univ Calif Davis, Dept Earth & Planetary Sci, One Shields Ave, Davis, CA 95616 USA.; Huang, JD (reprint author), Anhui Geol Museum, Dept Res, Jiahe Rd 999, Hefei 230031, Anhui, Peoples R China. EM djiang@pku.edu.cn; rmotani@ucdavis.edu; jiandongh2008@163.com RI Motani, Ryosuke/K-2607-2015 OI Motani, Ryosuke/0000-0001-5022-1053 FU Ministry of Land and Resources of China [201511054]; National Geographic Society Committee for Research and Exploration [8669-09]; National Natural Science Foundation of China [40920124002, 41372016]; State Key Laboratory of Palaeobiology and Stratigraphy (Nanjing Institute of Geology and Palaeontology, CAS) [123102]; Research Fund for the Doctoral Program of Higher Education [20120001110072] FX We thank T.-F. Hu for the excellent preparation of the holotype. Marta Boccaletti for help with the Greek language. The study was enabled by Project 201511054 from the Ministry of Land and Resources of China to J.-D.H., Y.-C.H., R.M. and D.-Y.J. grants from the National Geographic Society Committee for Research and Exploration (#8669-09) to R.M. Project 40920124002 and 41372016 from the National Natural Science Foundation of China to D.-Y.J. Project 123102 from the State Key Laboratory of Palaeobiology and Stratigraphy (Nanjing Institute of Geology and Palaeontology, CAS) to D.-Y.J. and Project 20120001110072 from the Research Fund for the Doctoral Program of Higher Education to D.-Y.J. NR 42 TC 2 Z9 2 U1 4 U2 5 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 MAY 23 PY 2016 VL 6 AR 26232 DI 10.1038/srep26232 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DM3FZ UT WOS:000376233500001 PM 27211319 ER PT J AU Rodriguez-Gomez, V Pillepich, A Sales, LV Genel, S Vogelsberger, M Zhu, QR Wellons, S Nelson, D Torrey, P Springel, V Ma, CP Hernquist, L AF Rodriguez-Gomez, Vicente Pillepich, Annalisa Sales, Laura V. Genel, Shy Vogelsberger, Mark Zhu, Qirong Wellons, Sarah Nelson, Dylan Torrey, Paul Springel, Volker Ma, Chung-Pei Hernquist, Lars TI The stellar mass assembly of galaxies in the Illustris simulation: growth by mergers and the spatial distribution of accreted stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: formation; galaxies: haloes; galaxies: interactions; cosmology: theory ID DARK-MATTER HALOES; MILKY-WAY; COSMOLOGICAL SIMULATIONS; LAMBDA-CDM; HYDRODYNAMICAL SIMULATIONS; HUBBLE SEQUENCE; SIZE EVOLUTION; MOVING-MESH; IN-SITU; FORMATION PHYSICS AB We use the Illustris simulation to study the relative contributions of in situ star formation and stellar accretion to the build-up of galaxies over an unprecedentedly wide range of masses (M-* = 10(9) - 10(12) M-circle dot), galaxy types, environments, and assembly histories. We find that the 'two-phase' picture of galaxy formation predicted by some models is a good approximation only for the most massive galaxies in our simulation - namely, the stellar mass growth of galaxies below a few times 10(11) M-circle dot is dominated by in situ star formation at all redshifts. The fraction of the total stellar mass of galaxies at z = 0 contributed by accreted stars shows a strong dependence on galaxy stellar mass, ranging from about 10 per cent for Milky Way-sized galaxies to over 80 per cent for M-* approximate to 10(12) M-circle dot objects, yet with a large galaxy-to-galaxy variation. At a fixed stellar mass, elliptical galaxies and those formed at the centres of younger haloes exhibit larger fractions of ex situ stars than disc-like galaxies and those formed in older haloes. On average, similar to 50 per cent of the ex situ stellar mass comes from major mergers (stellar mass ratio mu > 1/4), similar to 20 per cent from minor mergers (1/10 < mu < 1/4), similar to 20 per cent from very minor mergers (mu < 1/10), and similar to 10 per cent from stars that were stripped from surviving galaxies (e.g. flybys or ongoing mergers). These components are spatially segregated, with in situ stars dominating the innermost regions of galaxies, and ex situ stars being deposited at larger galactocentric distances in order of decreasing merger mass ratio. C1 [Rodriguez-Gomez, Vicente; Pillepich, Annalisa; Sales, Laura V.; Wellons, Sarah; Nelson, Dylan; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Sales, Laura V.] Univ Calif Riverside, Dept Phys & Astron, 900 Univ Ave, Riverside, CA 92521 USA. [Genel, Shy] Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA. [Vogelsberger, Mark; Torrey, Paul] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Zhu, Qirong] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Zhu, Qirong] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Nelson, Dylan] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. [Torrey, Paul] CALTECH, TAPIR, Mailcode 350-17, Pasadena, CA 91125 USA. [Springel, Volker] Heidelberg Inst Theoret Studies, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, Zentrum Astron, ARI, Monchhofstr 12-14, D-69120 Heidelberg, Germany. [Ma, Chung-Pei] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. RP Rodriguez-Gomez, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vrodriguez-gomez@cfa.harvard.edu OI Rodriguez-Gomez, Vicente/0000-0002-9495-0079 FU NASA through STScI [HST-HF2-51341.001-A]; NASA [NAS5-26555, NNX12AC67G]; European Research Council through ERC-StG [EXAGAL-308037]; NSF [AST-1312095]; PRACE project [RA0844]; SuperMUC computer at the Leibniz Computing Centre, Germany [pr85je] FX We thank Jeremiah P. Ostriker, Gurtina Besla, and Benedikt Diemer for useful comments and discussions. SG acknowledges support provided by NASA through Hubble Fellowship grant HST-HF2-51341.001-A awarded by the STScI, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. VS acknowledges support through the European Research Council through ERC-StG grant EXAGAL-308037. LH acknowledges support from NSF grant AST-1312095 and NASA grant NNX12AC67G. Simulations were run on the Harvard Odyssey and CfA/ITC clusters, the Ranger and Stampede supercomputers at the Texas Advanced Computing Center as part of XSEDE, the Kraken supercomputer at Oak Ridge National Laboratory as part of XSEDE, the CURIE supercomputer at CEA/France as part of PRACE project RA0844, and the SuperMUC computer at the Leibniz Computing Centre, Germany, as part of project pr85je. NR 88 TC 19 Z9 19 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2016 VL 458 IS 3 BP 2371 EP 2390 DI 10.1093/mnras/stw456 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL7DC UT WOS:000375799000009 ER PT J AU Zhuravleva, I Churazov, E Arevalo, P Schekochihin, AA Forman, WR Allen, SW Simionescu, A Sunyaev, R Vikhlinin, A Werner, N AF Zhuravleva, I. Churazov, E. Arevalo, P. Schekochihin, A. A. Forman, W. R. Allen, S. W. Simionescu, A. Sunyaev, R. Vikhlinin, A. Werner, N. TI The nature and energetics of AGN-driven perturbations in the hot gas in the Perseus Cluster SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: observational; methods: statistical; techniques: image processing; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; DEEP CHANDRA OBSERVATION; RAY SURFACE BRIGHTNESS; VELOCITY POWER SPECTRA; X-RAY; GALAXY CLUSTERS; INTRACLUSTER MEDIUM; SOUND-WAVES; COSMIC-RAYS; DENSITY FLUCTUATIONS AB Cores of relaxed galaxy clusters are often disturbed by AGN. Their Chandra observations revealed a wealth of structures induced by shocks, subsonic gas motions, bubbles of relativistic plasma, etc. In this paper, we determine the nature and energy content of gas fluctuations in the Perseus core by probing statistical properties of emissivity fluctuations imprinted in the soft- and hard-band X-ray images. About 80 per cent of the total variance of perturbations on similar to 8-70 kpc scales in the core have an isobaric nature, i.e. are consistent with subsonic displacements of the gas in pressure equilibrium with the ambient medium. The observed variance translates to the ratio of energy in perturbations to thermal energy of similar to 13 per cent. In the region dominated by weak 'ripples', about half of the total variance is associated with isobaric perturbations on scales of a few tens of kpc. If these isobaric perturbations are induced by buoyantly rising bubbles, then these results suggest that most of the AGN-injected energy should first go into bubbles rather than into shocks. Using simulations of a shock propagating through the Perseus atmosphere, we found that models reproducing the observed features of a central shock have more than 50 per cent of the AGN- injected energy associated with the bubble enthalpy and only about 20 per cent is carried away with the shock. Such energy partition is consistent with the AGN- feedback model, mediated by bubbles of relativistic plasma, and supports the importance of turbulence in the cooling-heating balance. C1 [Zhuravleva, I.; Allen, S. W.; Werner, N.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA. [Zhuravleva, I.; Allen, S. W.; Werner, N.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Churazov, E.; Sunyaev, R.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. [Churazov, E.; Sunyaev, R.] Space Res Inst IKI, Profsoyuznaya 84-32, Moscow 117997, Russia. [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Gran Bretana N 1111, Valparaiso, Chile. [Schekochihin, A. A.] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, 1 Keble Rd, Oxford OX1 3NP, England. [Schekochihin, A. A.] Univ Oxford Merton Coll, Merton St, Oxford OX1 4JD, England. [Forman, W. R.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Allen, S. W.] SLAC Natl Accelerator Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA. [Simionescu, A.] Japan Aerosp Explorat Agcy, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. RP Zhuravleva, I (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA.; Zhuravleva, I (reprint author), Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. EM zhur@stanford.edu RI Churazov, Eugene/A-7783-2013 FU NASA [AR4-15013X, NAS8-03060]; FONDECYT [1140304]; Centro de Astrofisica de Valparaiso; Russian Scientific Foundation [14-22-00271] FX Support for this work was provided by the NASA through Chandra award number AR4-15013X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the NASA under contract NAS8-03060. IZ thanks A.C. Fabian and J. Sanders for important comments and discussions. EC and AAS are grateful to the Wolfgang Pauli Institute, Vienna, for its hospitality. PA acknowledges support from FONDECYT grant 1140304 and Centro de Astrofisica de Valparaiso. EC and RS are partly supported by grant No. 14-22-00271 from the Russian Scientific Foundation. We are grateful to Hans-Thomas Janka for the provision of a one-dimensional Lagrangian hydrodynamics code, initially used for supernovae explosion calculations. NR 57 TC 4 Z9 4 U1 3 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 MAY 21 PY 2016 VL 458 IS 3 BP 2902 EP 2915 DI 10.1093/mnras/stw520 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL7DC UT WOS:000375799000046 ER PT J AU Russell, HR McNamara, BR Fabian, AC Nulsen, PEJ Edge, AC Combes, F Murray, NW Parrish, IJ Salome, P Sanders, JS Baum, SA Donahue, M Main, RA O'Connell, RW O'Dea, CP Oonk, JBR Tremblay, G Vantyghem, AN Voit, GM AF Russell, H. R. McNamara, B. R. Fabian, A. C. Nulsen, P. E. J. Edge, A. C. Combes, F. Murray, N. W. Parrish, I. J. Salome, P. Sanders, J. S. Baum, S. A. Donahue, M. Main, R. A. O'Connell, R. W. O'Dea, C. P. Oonk, J. B. R. Tremblay, G. Vantyghem, A. N. Voit, G. M. TI ALMA observations of cold molecular gas filaments trailing rising radio bubbles in PKS 0745-191 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: clusters: individual: PKS 0745-191; galaxies: evolution ID BRIGHTEST CLUSTER GALAXIES; ACTIVE GALACTIC NUCLEI; COOLING FLOW CLUSTERS; CO-TO-H-2 CONVERSION FACTOR; RAY-LUMINOUS CLUSTERS; STAR-FORMATION RATES; X-RAY; BLACK-HOLES; DOMINANT GALAXIES; MAGNETIC-FIELDS AB We present ALMA observations of the CO(1-0) and CO(3-2) line emission tracing filaments of cold molecular gas in the central galaxy of the cluster PKS 0745-191. The total molecular gas mass of 4.6 +/- 0.3 x 10(9)M(circle dot), assuming a Galactic X-CO factor, is divided roughly equally between three filaments each extending radially 3-5 kpc from the galaxy centre. The emission peak is located in the SE filament similar to 1 arcsec (2 kpc) from the nucleus. The velocities of the molecular clouds in the filaments are low, lying within +/- 100 km s(-1) of the galaxy's systemic velocity. Their full width at half-maximum (FWHM) are less than 150 km s(-1), which is significantly below the stellar velocity dispersion. Although the molecular mass of each filament is comparable to a rich spiral galaxy, such low velocities show that the filaments are transient and the clouds would disperse on < 10(7) yr time-scales unless supported, likely by the indirect effect of magnetic fields. The velocity structure is inconsistent with a merger origin or gravitational free-fall of cooling gas in this massive central galaxy. If the molecular clouds originated in gas cooling even a few kpc from their current locations their velocities would exceed those observed. Instead, the projection of the N and SE filaments underneath X-ray cavities suggests they formed in the updraft behind bubbles buoyantly rising through the cluster atmosphere. Direct uplift of the dense gas by the radio bubbles appears to require an implausibly high coupling efficiency. The filaments are coincident with low temperature X-ray gas, bright optical line emission and dust lanes indicating that the molecular gas could have formed from lifted warmer gas that cooled in situ. C1 [Russell, H. R.; Fabian, A. C.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [McNamara, B. R.; Vantyghem, A. N.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Nulsen, P. E. J.] Univ Western Australia, ICRAR, 35 Stirling Hwy, Crawley, WA 6009, Australia. [Edge, A. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Combes, F.; Salome, P.] Observ Paris, LERMA, 61 Av Observ, F-75014 Paris, France. [Murray, N. W.; Parrish, I. J.; Main, R. A.] Univ Toronto, Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada. [Sanders, J. S.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Baum, S. A.; O'Dea, C. P.] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. [Donahue, M.; Voit, G. M.] Michigan State Univ, Dept Phys & Astron, 567 Wilson Rd, E Lansing, MI 48824 USA. [O'Connell, R. W.] Univ Virginia, Dept Astron, POB 400235, Charlottesville, VA 22904 USA. [Oonk, J. B. R.] Netherlands Inst Radio Astron ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Oonk, J. B. R.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Tremblay, G.] Yale Univ, Dept Phys, 217 Prospect St, New Haven, CT 06511 USA. [Tremblay, G.] Yale Univ, Yale Ctr Astron & Astrophys, 217 Prospect St, New Haven, CT 06511 USA. RP Russell, HR (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM hrr27@ast.cam.ac.uk OI Tremblay, Grant/0000-0002-5445-5401; Sanders, Jeremy/0000-0003-2189-4501; Nulsen, Paul/0000-0003-0297-4493; Combes, Francoise/0000-0003-2658-7893; Voit, Gerard/0000-0002-3514-0383 FU ERC [340442]; Natural Sciences and Engineering Council of Canada; Canadian Space Agency; NASA [NAS8-03060]; STFC [ST/L00075X/1]; Einstein Postdoctoral Fellowship Award - Chandra X-ray Observatory Center [PF-150128]; National Aeronautics and Space Administration; National Science Foundation FX HRR and ACF acknowledge support from ERC Advanced Grant Feedback 340442. BRM acknowledges support from the Natural Sciences and Engineering Council of Canada and the Canadian Space Agency Space Science Enhancement Program. PEJN was partly supported by NASA contract NAS8-03060. ACE acknowledges support from STFC grant ST/L00075X/1. GRT acknowledges support from Einstein Postdoctoral Fellowship Award Number PF-150128, 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 the reviewer for their thorough reading of the paper and encouraging comments. This paper makes use of the following ALMA data: ADS/JAO.ALMA 2012.1.00837.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The scientific results reported in this article are based on data obtained from the Chandra Data Archive. This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 115 TC 2 Z9 2 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2016 VL 458 IS 3 BP 3134 EP 3149 DI 10.1093/mnras/stw409 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL7DC UT WOS:000375799000062 ER PT J AU Chen, X Gomez-Vargas, GA Guillochon, J AF Chen, Xian Gomez-Vargas, German Arturo Guillochon, James TI The gamma-ray afterglows of tidal disruption events SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE acceleration of particles; cosmic rays; galaxies: active; Local Group; gamma rays: galaxies ID MASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; COSMIC-RAYS; FERMI-LAT; SUPERNOVA-REMNANTS; SEYFERT-GALAXIES; RADIUS RELATIONS; SAGITTARIUS-A; STARS; EMISSION AB A star wandering too close to a supermassive black hole (SMBH) will be tidally disrupted. Previous studies of such 'tidal disruption event' (TDE) mostly focus on the stellar debris that are bound to the system, because they give rise to luminous flares. On the other hand, half of the stellar debris in principle are unbound and can stream to a great distance, but so far there is no clear evidence that this 'unbound debris stream' (UDS) exists. Motivated by the fact that the circum-nuclear region around SMBHs is usually filled with dense molecular clouds (MCs), here we investigate the observational signatures resulting from the collision between an UDS and an MC, which is likely to happen hundreds of years after a TDE. We focus on gamma-ray emission (0.1-105 GeV), which comes from the encounter of shock-accelerated cosmic rays with background protons and, more importantly, is not subject to extinction. We show that because of the high proton density inside an MC, the peak gamma-ray luminosity, about 1039 erg s(-1), is at least 100 times greater than that in the case without an MC(only with a smooth interstellar medium). The luminosity decays on a time-scale of decades, depending on the distance of the MC, and about a dozen of these 'TDE afterglows' could be detected within a distance of about 16 Mpc by the future Cherenkov Telescope Array. Without careful discrimination, these sources potentially could contaminate the searches for starburst galaxies, galactic nuclei containing millisecond pulsars or dark matter annihilation signals. C1 [Chen, Xian; Gomez-Vargas, German Arturo] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Santiago 7820436, Chile. [Gomez-Vargas, German Arturo] Pontificia Univ Catolica Chile, Inst Fis, Ave Vicuna Mackenna 4860, Santiago, Chile. [Gomez-Vargas, German Arturo] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Guillochon, James] Inst Theory & Computat, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Chen, X (reprint author), Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Santiago 7820436, Chile. EM xchen@astro.puc.cl FU CONICYT-Chile through Anillo [ACT1101]; NASA [PF3-140108]; Conicyt Anillo [ACT1102]; Spanish MINECO [MultiDark CSD2009-00064]; MINECO [FPA2012-34694]; 'VRI concurso estadias en el extranjero' of PUC FX We thank Fukun Liu, Maria Petropoulou and our Referee for many constructive comments. XC is supported by CONICYT-Chile through Anillo (ACT1101). JG is supported by the NASA Einstein grant PF3-140108. GAGV is supported by Conicyt Anillo grant ACT1102, the Spanish MINECO's Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064 and also partly by MINECO under grant FPA2012-34694. Part of this work is carried out at the Astronomy Department of Peking University, supported by the 'VRI concurso estadias en el extranjero' of PUC. NR 93 TC 4 Z9 4 U1 3 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 MAY 21 PY 2016 VL 458 IS 3 BP 3314 EP 3323 DI 10.1093/mnras/stw437 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL7DC UT WOS:000375799000073 ER PT J AU Crnojevic, D Sand, DJ Spekkens, K Caldwell, N Guhathakurta, P McLeod, B Seth, A Simon, JD Strader, J Toloba, E AF Crnojevic, D. Sand, D. J. Spekkens, K. Caldwell, N. Guhathakurta, P. McLeod, B. Seth, A. Simon, J. D. Strader, J. Toloba, E. TI THE EXTENDED HALO OF CENTAURUS A: UNCOVERING SATELLITES, STREAMS, AND SUBSTRUCTURES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: dwarf; galaxies: groups: individual (CenA); galaxies: halos; galaxies: photometry ID FAINT DWARF GALAXIES; MILKY-WAY SATELLITE; DARK-MATTER HALOES; RED GIANT BRANCH; TELESCOPE ADVANCED CAMERA; NORTH TRANSITION REGION; PAN-STARRS1 3-PI SURVEY; ULTRA-DIFFUSE GALAXIES; DIGITAL SKY SURVEY; STELLAR HALO AB We present the widest-field resolved stellar map to date of the closest (D similar to 3.8 Mpc) massive elliptical galaxy NGC 5128 (Centaurus A; Cen A), extending out to a projected galactocentric radius of similar to 150 kpc. The data set is part of our ongoing Panoramic Imaging Survey of Centaurus and Sculptor (PISCeS) utilizing the Magellan/Megacam imager. We resolve a population of old red giant branch (RGB) stars down to similar to 1.5 mag below the tip of the RGB, reaching surface brightness limits as low as mu(V,0) similar to 32 mag arcsec(-2). The resulting spatial stellar density map highlights a plethora of previously unknown streams, shells, and satellites, including the first tidally disrupting dwarf around Cen A (CenA-MM-Dw3), which underline its active accretion history. We report 13 previously unknown dwarf satellite candidates, of which 9 are confirmed to be at the distance of Cen A (the remaining 4 are not resolved into stars), with magnitudes in the range M-V = -7.2 to -13.0, central surface brightness values of mu(V,0) = 25.4-26.9 mag arcsec(-2), and half-light radii of r(h) = 0.22-2.92 kpc. These values are in line with Local Group dwarfs but also lie at the faint/diffuse end of their distribution; interestingly, CenA-MM-Dw3 has similar properties to the recently discovered ultradiffuse galaxies in Virgo and Coma. Most of the new dwarfs are fainter than the previously known Cen A satellites. The newly discovered dwarfs and halo substructures are discussed in light of their stellar populations, and they are compared to those discovered by the PAndAS survey of M31. C1 [Crnojevic, D.; Sand, D. J.; Toloba, E.] Texas Tech Univ, Dept Phys, Box 41051, Lubbock, TX 79409 USA. [Spekkens, K.] Royal Mil Coll Canada, Dept Phys, Stn Forces, Box 17000, Kingston, ON K7L 7B4, Canada. [Caldwell, N.; McLeod, B.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Guhathakurta, P.; Toloba, E.] Univ Calif Santa Cruz, UCO Lick Observ, 1156 High St, Santa Cruz, CA 95064 USA. [Seth, A.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Simon, J. D.] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Strader, J.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Crnojevic, D (reprint author), Texas Tech Univ, Dept Phys, Box 41051, Lubbock, TX 79409 USA. EM denija.crnojevic@ttu.edu OI McLeod, Brian/0000-0002-2924-2893; Guhathakurta, Puragra/0000-0001-8867-4234; Sand, David/0000-0003-4102-380X FU NSF [AST-1412504, AST-1010039, AST-1412792]; Natural Sciences and Engineering Research Council of Canada (NSERC); National Science Foundation [PHYS-1066293]; Aspen Center for Physics; Smithsonian Astrophysical Observatory FX We are grateful to the referee for a careful reading of the manuscript and for his/her useful suggestions that helped improve this work. We warmly thank Maureen Conroy, John Roll, Sean Moran, and David Osip for their prolonged efforts and help related to Megacam. D.C. wishes to kindly thank the hospitality of the Mullard Space Science Laboratory, University College of London, where part of this work has been carried out. D.C., D.J.S., P.G., and E.T. acknowledge support from NSF grant AST-1412504; P.G. and E.T. acknowledge additional support from NSF grant AST-1010039; J.D.S. acknowledges support from NSF grant AST-1412792. K.S. acknowledges support from the Natural Sciences and Engineering Research Council of Canada (NSERC). This work was supported in part by National Science Foundation Grant No. PHYS-1066293 and the Aspen Center for Physics. This paper uses data products produced by the OIR Telescope Data Center, supported by the Smithsonian Astrophysical Observatory. 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 110 TC 15 Z9 15 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 MAY 20 PY 2016 VL 823 IS 1 AR 19 DI 10.3847/0004-637X/823/1/19 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6WD UT WOS:000377216300019 ER PT J AU D'Onghia, E Madau, P Vera-Ciro, C Quillen, A Hernquist, L AF D'Onghia, E. Madau, P. Vera-Ciro, C. Quillen, A. Hernquist, L. TI EXCITATION OF COUPLED STELLAR MOTIONS IN THE GALACTIC DISK BY ORBITING SATELLITES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: kinematics and dynamics; Galaxy: disk; Galaxy: evolution; stars: kinematics and dynamics ID MILKY-WAY DISC; RING GALAXIES; MINOR MERGERS; SUBSTRUCTURE; WAVES; NUMBER; STARS; BAR AB We use a set of high-resolution N-body simulations of the Galactic disk to study its interactions with the population of cosmologically predicted satellites. One simulation illustrates that multiple passages of massive satellites with different velocities through the disk generate a wobble, which has the appearance of rings in face-on projections of the stellar disk. They also produce flares in the outer disk parts and gradually heat the disk through bending waves. A different numerical experiment shows that an individual satellite as massive as the Sagittarius dwarf galaxy passing through the disk will drive coupled horizontal and vertical oscillations of stars in underdense regions with small associated heating. This experiment shows that vertical excursions of stars in these low-density regions can exceed 1 kpc in the Solar neighborhood, resembling the recently locally detected coherent vertical oscillations. They can also induce non-zero vertical streaming motions as large as 10-20 km s(-1), which is consistent with recent observations in the Galactic disk. This phenomenon appears as a local ring with modest associated disk heating. C1 [D'Onghia, E.] Univ Wisconsin, Dept Astron, 2535 Sterling Hall,475 N Charter St, Madison, WI 53076 USA. [Madau, P.] Univ Calif Santa Cruz, 1156 High St, Santa Cruz, CA 95064 USA. [Vera-Ciro, C.] Univ Medellin, Dept Ciencias Basicas, Cra 87 N30-65, Medellin, Colombia. [Quillen, A.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Hernquist, L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA USA. RP D'Onghia, E (reprint author), Univ Wisconsin, Dept Astron, 2535 Sterling Hall,475 N Charter St, Madison, WI 53076 USA. EM edonghia@astro.wisc.edu OI Madau, Piero/0000-0002-6336-3293 FU NSF [AST-1211258, PHY-1066293, AST-1229745, AST-1312095]; ATP-NASA grant [NNX14AP53G]; Alfred P. Sloan Foundation; NASA [NNX12AF87G, NNX12AC67G] FX This work is funded by NSF grant no. AST-1211258 and ATP-NASA grant no. NNX14AP53G. E.D. gratefully acknowledges the support of the Alfred P. Sloan Foundation and the hospitality of the Aspen Center for Physics, funded by NSF grant no. PHY-1066293. P.M. acknowledges support by the NSF through grant AST-1229745 and NASA through grant NNX12AF87G. L.H. acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. NR 43 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 MAY 20 PY 2016 VL 823 IS 1 AR 4 DI 10.3847/0004-637X/823/1/4 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6WD UT WOS:000377216300004 ER PT J AU Eksi, KY Andac, IC Cikintoglu, S Gugercinoglu, E Motlagh, AV Kiziltan, B AF Eksi, K. Y. Andac, I. C. Cikintoglu, S. Gugercinoglu, E. Motlagh, A. Vahdat Kiziltan, B. TI THE INCLINATION ANGLE AND EVOLUTION OF THE BRAKING INDEX OF PULSARS WITH PLASMA-FILLED MAGNETOSPHERE: APPLICATION TO THE HIGH BRAKING INDEX OF PSR J1640-4631 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: general; pulsars: individual (PSR J1640-4631); stars: evolution ID MAGNETIC-FIELD GROWTH; IN-CELL SIMULATIONS; YOUNG PULSAR; CRAB PULSAR; SPIN-DOWN; OBLIQUE ROTATORS; EMPIRICAL-THEORY; RADIO PULSARS; NEUTRON-STARS; VELA PULSAR AB The recently discovered rotationally powered pulsar PSR J1640-4631 is the first to have a braking index measured, with high enough precision, that is greater than 3. An inclined magnetic rotator in vacuum or plasma would be subject not only to spin-down but also to an alignment torque. The vacuum model can address the braking index only for an almost orthogonal rotator, which is incompatible with the single-peaked pulse profile. The magnetic dipole model with the corotating plasma predicts braking indices between 3 and 3.25. We find that the braking index of 3.15 is consistent with two different inclination angles, 18 degrees.5 +/- 3 degrees and 56 degrees +/- 4 degrees. The smaller angle is preferred given that the pulse profile has a single peak and the radio output of the source is weak. We infer the change in the inclination angle to be at the rate -0 degrees.23 per century, three times smaller in absolute value than the rate recently observed for the Crab pulsar. C1 [Eksi, K. Y.; Andac, I. C.; Cikintoglu, S.; Motlagh, A. Vahdat] Istanbul Tech Univ, Fac Sci & Letters, Dept Engn Phys, TR-34469 Istanbul, Turkey. [Eksi, K. Y.] Bogazici Univ, Feza Gursey Ctr Phys & Math, TR-34684 Istanbul, Turkey. [Gugercinoglu, E.] Istanbul Univ, Dept Astron & Space Sci, Fac Sci, TR-34119 Istanbul, Turkey. [Kiziltan, B.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Eksi, KY (reprint author), Istanbul Tech Univ, Fac Sci & Letters, Dept Engn Phys, TR-34469 Istanbul, Turkey.; Eksi, KY (reprint author), Bogazici Univ, Feza Gursey Ctr Phys & Math, TR-34684 Istanbul, Turkey. FU Scientific and Technological Council of Turkey (TUBITAK) [BIDEB 2221]; [113F354] FX K.Y.E. and B.K. acknowledge the Scientific and Technological Council of Turkey (TUBITAK) for BIDEB 2221 visiting scholar award and E.G. for support under the grant 113F354. We thank the referee, Alexander Philippov, for insightful comments that improved the paper. NR 51 TC 6 Z9 6 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 MAY 20 PY 2016 VL 823 IS 1 AR 34 DI 10.3847/0004-637X/823/1/34 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6WD UT WOS:000377216300034 ER PT J AU Poleski, R Zhu, W Christie, GW Udalski, A Gould, A Bachelet, E Skottfelt, J Novati, SC Szymanski, MK Soszynski, I Pietrzynski, G Wyrzykowski, L Ulaczyk, K Pietrukowicz, P Kozlowski, S Skowron, J Mroz, P Pawlak, M Beichman, C Bryden, G Carey, S Fausnaugh, M Gaudi, BS Henderson, CB Pogge, RW Shvartzvald, Y Wibking, B Yee, JC Beatty, TG Eastman, JD Drummond, J Friedmann, M Henderson, M Johnson, JA Kaspi, S Maoz, D McCormick, J McCrady, N Natusch, T Ngan, H Porritt, I Relles, HM Sliski, DH Tan, TG Wittenmyer, RA Wright, JT Street, RA Tsapras, Y Bramich, DM Horne, K Snodgrass, C Steele, IA Menzies, J Jaimes, RF Wambsganss, J Schmidt, R Cassan, A Ranc, C Mao, S Bozza, V Dominik, M Hundertmark, MPG Jorgensen, UG Andersen, MI Burgdorf, MJ Ciceri, S D'Ago, G Evans, DF Gu, SH Hinse, TC Kains, N Kerins, E Korhonen, H Kuffmeier, M Mancini, L Popovas, A Rabus, M Rahvar, S Rasmussen, RT Scarpetta, G Southworth, J Surdej, J Unda-Sanzana, E Verma, P von Essen, C Wang, YB Wertz, O AF Poleski, Radoslaw Zhu, Wei Christie, Grant W. Udalski, Andrzej Gould, Andrew Bachelet, Etienne Skottfelt, Jesper Novati, Sebastiano Calchi Szymanski, M. K. Soszynski, I. Pietrzynski, G. Wyrzykowski, L. Ulaczyk, K. Pietrukowicz, P. Kozlowski, Szymon Skowron, J. Mroz, P. Pawlak, M. Beichman, C. Bryden, G. Carey, S. Fausnaugh, M. Gaudi, B. S. Henderson, C. B. Pogge, R. W. Shvartzvald, Y. Wibking, B. Yee, J. C. Beatty, T. G. Eastman, J. D. Drummond, J. Friedmann, M. Henderson, M. Johnson, J. A. Kaspi, S. Maoz, D. McCormick, J. McCrady, N. Natusch, T. Ngan, H. Porritt, I. Relles, H. M. Sliski, D. H. Tan, T. -G. Wittenmyer, R. A. Wright, J. T. Street, R. A. Tsapras, Y. Bramich, D. M. Horne, K. Snodgrass, C. Steele, I. A. Menzies, J. Jaimes, R. Figuera Wambsganss, J. Schmidt, R. Cassan, A. Ranc, C. Mao, S. Bozza, V. Dominik, M. Hundertmark, M. P. G. Jorgensen, U. G. Andersen, M. I. Burgdorf, M. J. Ciceri, S. D'Ago, G. Evans, D. F. Gu, S. -H. Hinse, T. C. Kains, N. Kerins, E. Korhonen, H. Kuffmeier, M. Mancini, L. Popovas, A. Rabus, M. Rahvar, S. Rasmussen, R. T. Scarpetta, G. Southworth, J. Surdej, J. Unda-Sanzana, E. Verma, P. von Essen, C. Wang, Y. -B. Wertz, O. CA OGLE Grp Spitzer Team FUN Grp RoboNet Project MiNDSTEp Grp TI THE SPITZER MICROLENSING PROGRAM AS A PROBE FOR GLOBULAR CLUSTER PLANETS: ANALYSIS OF OGLE-2015-BLG-0448 SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters: individual (NGC6558); gravitational lensing: micro; planets and satellites: detection; proper motions ID GRAVITATIONAL LENSING EXPERIMENT; DIFFERENCE IMAGE-ANALYSIS; MILKY-WAY BULGE; RR LYRAE STARS; GALACTIC BULGE; OGLE-III; RED CLUMP; PHOTOMETRY; SYSTEMS; CATALOG AB The microlensing event OGLE-2015-BLG-0448 was observed by Spitzer and lay within the tidal radius of the globular cluster NGC 6558. The event had moderate magnification and was intensively observed, hence it had the potential to probe the distribution of planets in globular clusters. We measure the proper motion of NGC 6558 (mu(cl) (N, E) = (+0.36 +/- 0.10, +1.42 +/- 0.10) mas yr(-1)) as well as the source and show that the lens is not a cluster member. Even though this particular event does not probe the distribution of planets in globular clusters, other potential cluster lens events can be verified using our methodology. Additionally, we find that microlens parallax measured using Optical Gravitational Lens Experiment (OGLE) photometry is consistent with the value found based on the light curve displacement between the Earth and Spitzer. C1 [Poleski, Radoslaw; Zhu, Wei; Fausnaugh, M.; Gaudi, B. S.; Pogge, R. W.; Wibking, B.] Ohio State Univ, Dept Astron, 174 West 18th Ave, Columbus, OH 43210 USA. [Poleski, Radoslaw; Udalski, Andrzej; Szymanski, M. K.; Soszynski, I.; Pietrzynski, G.; Wyrzykowski, L.; Ulaczyk, K.; Pietrukowicz, P.; Kozlowski, Szymon; Skowron, J.; Mroz, P.; Pawlak, M.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. [Christie, Grant W.; Natusch, T.; Ngan, H.] Auckland Observ, Auckland, New Zealand. [Gould, Andrew] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Gould, Andrew] Korea Astron & Space Sci Inst, Daejon 305348, South Korea. [Bachelet, Etienne; Street, R. A.] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA. [Skottfelt, Jesper] Open Univ, Dept Phys Sci, Ctr Elect Imaging, Milton Keynes MK7 6AA, Bucks, England. [Skottfelt, Jesper; Kaspi, S.; Hundertmark, M. P. G.; Jorgensen, U. G.; Kuffmeier, M.; Popovas, A.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark. [Skottfelt, Jesper; Kaspi, S.; Hundertmark, M. P. G.; Jorgensen, U. G.; Kuffmeier, M.; Popovas, A.] Univ Copenhagen, Ctr Star & Planet Format, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark. [Novati, Sebastiano Calchi; Beichman, C.] CALTECH, NASA Exoplanet Sci Inst, MS 100-22, Pasadena, CA 91125 USA. [Novati, Sebastiano Calchi; Bozza, V.; D'Ago, G.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo 2 132, I-84084 Fisciano, Italy. [Novati, Sebastiano Calchi; D'Ago, G.; Scarpetta, G.; Verma, P.] Ist Int Alti Studi Sci, Via G Pellegrino 19, I-84019 Vietri Sul Mare, SA, Italy. [Pietrukowicz, P.] Univ Concepcion, Dept Astron, Casilla 160C, Concepcion, Chile. [Ulaczyk, K.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Bryden, G.; Carey, S.; Henderson, C. B.; Shvartzvald, Y.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Yee, J. C.; Eastman, J. D.; Johnson, J. A.; Relles, H. M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Beatty, T. G.; Wright, J. T.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Beatty, T. G.; Wright, J. T.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Drummond, J.] Possum Observ, Patutahi, New Zealand. [Friedmann, M.; Maoz, D.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Henderson, M.; McCrady, N.] Univ Montana, Dept Phys & Astron, 32 Campus Dr,1080, Missoula, MT 59812 USA. [McCormick, J.] Farm Cove Observ, Ctr Backyard Astrophys, Auckland, New Zealand. [Natusch, T.] AUT Univ, Auckland, New Zealand. [Porritt, I.] Turitea Observ, Palmerston North, New Zealand. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Tan, T. -G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Wittenmyer, R. A.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Wittenmyer, R. A.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Wittenmyer, R. A.] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. [Tsapras, Y.; Wambsganss, J.; Schmidt, R.] Univ Heidelberg ZAH, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany. [Bramich, D. M.] Qatar Fdn, HBKU, Qatar Environm & Energy Res Inst, Doha, Qatar. [Horne, K.; Jaimes, R. Figuera; Dominik, M.] Univ St Andrews, Dept Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England. [Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England. [Menzies, J.] S African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa. [Jaimes, R. Figuera] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Cassan, A.; Ranc, C.] Univ Paris 06, Sorbonne Univ, 98 Bis Bd Arago, F-75014 Paris, France. [Cassan, A.; Ranc, C.] CNRS, UMR 7095, Inst Astrophys Paris, 98 Bis Bd Arago, F-75014 Paris, France. [Mao, S.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, I-80125 Naples, Italy. [Andersen, M. I.] Univ Copenhagen, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. [Burgdorf, M. J.] Univ Hamburg, Inst Meteorol, Bundesstr 55, D-20146 Hamburg, Germany. [Ciceri, S.; Mancini, L.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Evans, D. F.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Gu, S. -H.; Wang, Y. -B.] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China. [Hinse, T. C.] Korea Astron & Space Sci Inst, 776 Daedukdae Ro, Daejeon 305348, South Korea. [Kains, N.; Kerins, E.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. [Korhonen, H.] Finnish Ctr Astron ESO FINCA, Vaisalantie 20, FI-21500 Piikkio, Finland. [Rabus, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile. [Rahvar, S.] Sharif Univ Technol, Dept Phys, POB 11155-9161, Tehran, Iran. [Rasmussen, R. T.; von Essen, C.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Surdej, J.; Wertz, O.] Inst Astrophys & Geophys, Allee 6 Aout 17,Sart Tilman,Bat B5c, B-4000 Liege, Belgium. [Unda-Sanzana, E.] Univ Antofagasta, Unidad Astron, Fac Ciencias Basicas, Avda U Antofagasta 02800, Antofagasta, Chile. RP Poleski, R (reprint author), Ohio State Univ, Dept Astron, 174 West 18th Ave, Columbus, OH 43210 USA.; Poleski, R (reprint author), Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. EM poleski.1@osu.edu RI Hundertmark, Markus/C-6190-2015; Korhonen, Heidi/E-3065-2016; D'Ago, Giuseppe/N-8318-2016; Skowron, Jan/M-5186-2014; OI Hundertmark, Markus/0000-0003-0961-5231; Korhonen, Heidi/0000-0003-0529-1161; D'Ago, Giuseppe/0000-0001-9697-7331; Skowron, Jan/0000-0002-2335-1730; Wang, Yi-Bo/0000-0002-5172-8558; Wright, Jason/0000-0001-6160-5888; ZHU, WEI/0000-0003-4027-4711 FU National Science Centre, Poland [MAESTRO 2014/14/A/ST9/00121]; NSF [AST 1516842]; JPL [1500811]; NASA through the Sagan Fellowship Program by the NASA Exoplanet Science Institute; NPRP from the Qatar National Research Fund (a member of Qatar Foundation) [X-019-1-006]; Chinese Academy of Sciences [XDB09000000]; National Natural Science Foundation of China (NSFC) [11333003, 11390372]; Villum Foundation; Danish Council for Independent Research, Natural Sciences; Centre for Star and Planet Formation FX The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A. U. Work by W. Z. and A. G. was supported by NSF AST 1516842. Work by Y. S. and C. B. H. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. Work by J. C. Y., A. G., and S. C. was supported by JPL grant 1500811. Work by J. C. Y. was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. This publication was made possible by NPRP grant # X-019-1-006 from the Qatar National Research Fund (a member of Qatar Foundation). Work by S. M. has been supported by the Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences Grant No. XDB09000000, and by the National Natural Science Foundation of China (NSFC) under grant numbers 11333003 and 11390372. M. P. G. H. acknowledges support from the Villum Foundation. This work makes use of observations from the LCOGT network, which includes three SUPAscopes owned by the University of St Andrews. The RoboNet programme is an LCOGT Key Project using time allocations from the University of St Andrews, LCOGT and the University of Heidelberg together with time on the Liverpool Telescope through the Science and Technology Facilities Council (STFC), UK. This research has made use of the LCOGT Archive, which is operated by the California Institute of Technology, under contract with the Las Cumbres Observatory. Operation of the Danish 1.54 m telescope at ESOs La Silla observatory was supported by The Danish Council for Independent Research, Natural Sciences, and by Centre for Star and Planet Formation. NR 50 TC 0 Z9 0 U1 3 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2016 VL 823 IS 1 AR 63 DI 10.3847/0004-637X/823/1/63 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6WD UT WOS:000377216300063 ER PT J AU Siemiginowska, A Sobolewska, M Migliori, G Guainazzi, M Hardcastle, M Ostorero, L Stawarz, L AF Siemiginowska, Aneta Sobolewska, Malgosia Migliori, Giulia Guainazzi, Matteo Hardcastle, Martin Ostorero, Luisa Stawarz, Lukasz TI X-RAY PROPERTIES OF THE YOUNGEST RADIO SOURCES AND THEIR ENVIRONMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; COMPACT STEEP-SPECTRUM; GHZ-PEAKED-SPECTRUM; SOURCE PMN J1603-4904; LARGE-AREA TELESCOPE; XMM-NEWTON SURVEY; K-ALPHA LINES; SYMMETRIC OBJECTS; SEYFERT-GALAXIES; SOURCE EVOLUTION AB We present the first results from our X-ray study of young radio sources classified as compact symmetric objects (CSOs). Using the Chandra X-ray Observatory we observed six CSOs for the first time in X-rays, and re-observed four CSOs already observed with XMM-Newton or BeppoSAX. We also included six other CSOs with archival data to built a pilot study of a sample of the 16 CSO sources observed in X-rays to date. All the sources are nearby, z < 1, and the age of their radio structures (< 3000 yr) has been derived from the expansion velocity of their hot spots. Our results show the heterogeneous nature of the CSOs' X-ray emission, indicating a complex environment associated with young radio sources. The sample covers a range in X-ray luminosity, L2-10keV similar to 10(41)-10(45) erg s(-1), and intrinsic absorbing column density of N-H similar or equal to 10(21)-10(22) cm(-2). In particular, we detected extended X-ray emission in 1718-649; a hard photon index of Gamma similar or equal to 1 in 2021+614 and 1511+0518 consistent with either a Compton-thick absorber or non-thermal emission from compact radio lobes, and in 0710+439 an ionized iron emission line at E-rest = (6.62 +/- 0.04) keV and EW similar to 0.15-1.4 keV, and a decrease by an order of magnitude in the 2-10 keV flux since the 2008 XMM-Newton observation in 1607+26. We conclude that our pilot study of CSOs provides a variety of exceptional diagnostics and highlights the importance of deep X-ray observations of large samples of young sources. This is necessary in order to constrain theoretical models for the earliest stage of radio source evolution and to study the interactions of young radio sources with the interstellar environment of their host galaxies. C1 [Siemiginowska, Aneta; Sobolewska, Malgosia] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Sobolewska, Malgosia] Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. [Migliori, Giulia] Univ Paris 07, CEA Saclay, CNRS, Lab AIM, F-75221 Paris 05, France. [Guainazzi, Matteo] Inst Space & Astronaut Sci, JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. [Guainazzi, Matteo] ESA, European Space Astron Ctr, POB 78, E-28691 Madrid, Spain. [Hardcastle, Martin] Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. [Ostorero, Luisa] Univ Turin, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy. [Ostorero, Luisa] Ist Nazl Fis Nucl, Via P Giuria 1, I-10125 Turin, Italy. [Stawarz, Lukasz] Jagiellonian Univ, Astron Observ, Ul Orla 171, PL-30244 Krakow, Poland. RP Siemiginowska, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM asiemiginowska@cfa.harvard.edu OI Hardcastle, Martin/0000-0003-4223-1117 FU National Aeronautics and Space Administration [NAS8-03060]; NASA [GO1-12145X, GO4-15099X, NNX10AO60G]; UnivEarthS Labex program of Sorbonne Paris Cite [ANR10LABX0023, ANR11IDEX000502]; INFN grant INDARK; Italian Ministry of University and Research; University of Torino; Polish NSC [DEC-2012/04/A/ST9/00083]; Compagnia di San Paolo FX We thank the anonymous referee for detailed comments. This research is funded in part by National Aeronautics and Space Administration contract NAS8-03060. Partial support for this work was provided by the NASA grants GO1-12145X, GO4-15099X, NNX10AO60G. G.M. acknowledges the financial support from the UnivEarthS Labex program of Sorbonne Paris Cite (ANR10LABX0023 and ANR11IDEX000502). L.O. acknowledges support from the INFN grant INDARK, the grant PRIN 2012 "Fisica Astroparticellare Teorica" of the Italian Ministry of University and Research, and the "Strategic Research Grant: Origin and Detection of Galactic and Extragalactic Cosmic Rays" funded by the University of Torino and Compagnia di San Paolo. L.S. was supported by Polish NSC grant DEC-2012/04/A/ST9/00083. This research has made use of data obtained by the Chandra X-ray Observatory, and software provided by Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa. NR 122 TC 0 Z9 0 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2016 VL 823 IS 1 AR 57 DI 10.3847/0004-637X/823/1/57 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6WD UT WOS:000377216300057 ER PT J AU Huang, J Oberg, KI Andrews, SM AF Huang, Jane Oberg, Karin I. Andrews, Sean M. TI EVIDENCE FOR A CO DESORPTION FRONT IN THE OUTER AS 209 DISK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: molecules; protoplanetary disks ID PROTOPLANETARY DISKS; TEMPERATURE-GRADIENT; CHEMICAL-PROCESSES; LINE; OPHIUCHUS; CONSTRAINTS; MOLECULES; CHEMISTRY; CAVITIES; MASSES AB Millimeter observations of CO isotopologues are often used to make inferences about protoplanetary disk gas density and temperature structures. The accuracy of these estimates depends on our understanding of CO freezeout and desorption from dust grains. Most models of these processes indicate that CO column density decreases monotonically with distance from the central star due to a decrease in gas density and freezeout beyond the CO snowline. We present ALMA Cycle 2 observations of (CO)-C-12, (CO)-C-13, and (CO)-O-18 J = 2 - 1 emission that instead suggest CO enhancement in the outer disk of T Tauri star AS 209. Most notably, the (CO)-O-18 emission consists of a central peak and a ring at a radius of similar to 1" (120 au), well outside the expected CO snowline. We propose that the ring arises from the onset of CO desorption near the edge of the millimeter dust disk. CO desorption exterior to a CO snowline may occur via non-thermal processes involving cosmic rays or high-energy photons, or via a radial thermal inversion arising from dust migration. C1 [Huang, Jane; Oberg, Karin I.; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Huang, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jane.huang@cfa.harvard.edu FU Alfred P. Sloan Foundation; Packard Foundation; National Science Foundation Graduate Research Fellowship [DGE-1144152] FX We thank the referee for comments improving this paper; Ian Czekala, Ilse Cleeves, and Meredith MacGregor for helpful discussions; and Ryan Loomis for access to VIS_SAMPLE. This Letter makes use of ALMA data ADS/JAO. ALMA#2013.1.00226.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. K.I.O. acknowledges funding from the Alfred P. Sloan Foundation and the Packard Foundation. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1144152. NR 36 TC 2 Z9 2 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 20 PY 2016 VL 823 IS 1 AR L18 DI 10.3847/2041-8205/823/1/L18 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DM5LY UT WOS:000376391700018 ER PT J AU Li, GJ Adams, FC AF Li, Gongjie Adams, Fred C. TI INTERACTION CROSS SECTIONS AND SURVIVAL RATES FOR PROPOSED SOLAR SYSTEM MEMBER PLANET NINE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planet-star interactions ID EMBEDDED CLUSTERS; WIDE ORBITS; NEIGHBORHOOD; STARS; MULTIPLICITY; EVOLUTION; SEDNA; GAS AB Motivated by the report of a possible new planetary member of the solar system, this work calculates cross sections for interactions between passing stars and this proposed Planet Nine. Evidence for the new planet is provided by the orbital alignment of Kuiper belt objects, and other solar system properties, which suggest a Neptune-mass object on an eccentric orbit with a semimajor axis a(9) approximate to 400-1500 au. With such a wide orbit, Planet Nine has a large interaction cross section and is susceptible to disruption by passing stars. Using a large ensemble of numerical simulations (several million) and Monte Carlo sampling, we calculate the cross sections for different classes of orbit-altering events: (A) scattering the planet into its proposed orbit from a smaller orbit, (B) ejecting it from the solar system from its current orbit, (C) capturing the planet from another system, and (D) capturing a free-floating planet. Results are presented for a range of orbital elements with planetary mass m(9) = 10M(circle plus). Removing Planet Nine from the solar system is the most likely outcome. Specifically, we obtain ejection cross sections sigma(int) similar to 5 x 10(6) au(2) (5 x 10(4) au(2)) for environments corresponding to the birth cluster (field). With these cross sections, Planet Nine is likely to be ejected if the Sun resides within its birth cluster longer than Delta t greater than or similar to 100 Myr. The probability of ejecting Planet Nine due to passing field stars is less than or similar to 3% over the age of the Sun. Probabilities for producing the inferred Planet Nine orbit are low (less than or similar to 5%). C1 [Li, Gongjie] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. [Adams, Fred C.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Adams, Fred C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Li, GJ (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. OI Li, Gongjie/0000-0001-8308-0808; Adams, Fred/0000-0002-8167-1767 NR 31 TC 8 Z9 8 U1 3 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 MAY 20 PY 2016 VL 823 IS 1 AR L3 DI 10.3847/2041-8205/823/1/L3 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DM5LY UT WOS:000376391700003 ER PT J AU Tian, H Young, PR Reeves, KK Wang, TJ Antolin, P Chen, B He, JS AF Tian, Hui Young, Peter R. Reeves, Katharine K. Wang, Tongjiang Antolin, Patrick Chen, Bin He, Jiansen TI GLOBAL SAUSAGE OSCILLATION OF SOLAR FLARE LOOPS DETECTED BY THE INTERFACE REGION IMAGING SPECTROGRAPH SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE line: profiles; magnetic reconnection; Sun: corona; Sun: flares; Sun: oscillations ID QUASI-PERIODIC PULSATIONS; DOPPLER-SHIFT OSCILLATIONS; X-RAY PULSATIONS; CORONAL LOOP; MAGNETIC RECONNECTION; WAVES; MODES; ACCELERATION; HINODE/EIS; DYNAMICS AB An observation from the Interface Region Imaging Spectrograph reveals coherent oscillations in the loops of an M1.6 flare on 2015 March 12. Both the intensity and Doppler shift of Fe XXI 1354.08 angstrom show clear oscillations with a period of similar to 25 s. Remarkably similar oscillations were also detected in the soft X-ray flux recorded by the Geostationary Operational Environmental Satellites (GOES). With an estimated phase speed of similar to 2420 km s(-1) and a derived electron density of at least 5.4 x 10(10) cm(-3), the observed short-period oscillation is most likely the global fast sausage mode of a hot flare loop. We find a phase shift of similar to pi/2 (1/4 period) between the Doppler shift oscillation and the intensity/GOES oscillations, which is consistent with a recent forward modeling study of the sausage mode. The observed oscillation requires a density contrast between the flare loop and coronal background of a factor >= 42. The estimated phase speed of the global mode provides a lower limit of the Alfven speed outside the flare loop. We also find an increase of the oscillation period, which might be caused by the separation of the loop footpoints with time. C1 [Tian, Hui; He, Jiansen] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China. [Young, Peter R.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Young, Peter R.; Wang, Tongjiang] NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA. [Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Wang, Tongjiang] Catholic Univ Amer, Washington, DC 20064 USA. [Antolin, Patrick] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Chen, Bin] New Jersey Inst Technol, Dept Phys, Newark, NJ 07102 USA. RP Tian, H (reprint author), Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China. EM huitian@pku.edu.cn RI He, Jiansen/B-1808-2012; OI Reeves, Katharine/0000-0002-6903-6832 FU ESA; Norwegian Space Centre; Recruitment Program of Global Experts of China, NSFC [41574166]; LMSAL [8100002705]; NASA [NNG11PL10A, NNX11AB61G, NNX13AE06G, NNX15AF48G, NNX15AJ93G] FX IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research center and major contributions to downlink communications funded by ESA and the Norwegian Space Centre. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and NSC ( Norway). This work is supported by the Recruitment Program of Global Experts of China, NSFC under grant 41574166, contract 8100002705 from LMSAL to SAO, NASA Cooperative Agreement NNG11PL10A to CUA, NASA grants NNX11AB61G, NNX13AE06G, NNX15AF48G, and NNX15AJ93G. NR 46 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 20 PY 2016 VL 823 IS 1 AR L16 DI 10.3847/2041-8205/823/1/L16 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DM5LY UT WOS:000376391700016 ER PT J AU Walsh, C Loomis, RA Oberg, KI Kama, M van't Hoff, MLR Millar, TJ Aikawa, Y Herbst, E Weaver, SLW Nomura, H AF Walsh, Catherine Loomis, Ryan A. Oberg, Karin I. Kama, Mihkel van't Hoff, Merel L. R. Millar, Tom J. Aikawa, Yuri Herbst, Eric Weaver, Susanna L. Widicus Nomura, Hideko TI FIRST DETECTION OF GAS-PHASE METHANOL IN A PROTOPLANETARY DISK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; protoplanetary disks; stars: individual (TW Hya); stars: pre-main sequence; submillimeter: planetary systems ID TW HYA; ULTRAVIOLET PHOTODESORPTION; WATER ICE; CO; DESORPTION; DUST; CHEMISTRY; ANALOGS; CARBON; PURE AB The first detection of gas-phase methanol in a protoplanetary disk (TW Hya) is presented. In addition to being one of the largest molecules detected in disks to date, methanol is also the first disk organic molecule with an unambiguous ice chemistry origin. The stacked methanol emission, as observed with the Atacama Large Millimeter/submillimeter Array, is spectrally resolved and detected across six velocity channels (>3 sigma), reaching a peak signal-to-noise of 5.5s, with the kinematic pattern expected for TW Hya. Using an appropriate disk model, a fractional abundance of 3 x 10(-12)-4 x 10(-1)1 (with respect to H-2) reproduces the stacked line profile and channel maps, with the favored abundance dependent upon the assumed vertical location (midplane versus molecular layer). The peak emission is offset from the source position, suggesting that the methanol emission has a ring-like morphology: the analysis here suggests it peaks at approximate to 30 au, reaching a column density approximate to 3-6 x 10(12) cm(-2). In the case of TW Hya, the larger (up to millimeter-sized) grains, residing in the inner 50 au, may thus host the bulk of the disk ice reservoir. The successful detection of cold gas-phase methanol in a protoplanetary disk implies that the products of ice chemistry can be explored in disks, opening a window into studying complex organic chemistry during planetary system formation. C1 [Walsh, Catherine; Kama, Mihkel; van't Hoff, Merel L. R.] Leiden Univ, Leiden Observ, POB 9531, NL-2300 RA Leiden, Netherlands. [Loomis, Ryan A.; Oberg, Karin I.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Millar, Tom J.] Queens Univ Belfast, Sch Math & Phys, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland. [Aikawa, Yuri] Univ Tsukuba, Ctr Computat Sci, 1-1-1 Tennodai, Tsukuba, Ibaraki 3058577, Japan. [Herbst, Eric] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Herbst, Eric] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Weaver, Susanna L. Widicus] Emory Univ, Dept Chem, Atlanta, GA 30322 USA. [Nomura, Hideko] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan. RP Walsh, C (reprint author), Leiden Univ, Leiden Observ, POB 9531, NL-2300 RA Leiden, Netherlands. EM cwalsh@strw.leidenuniv.nl OI Millar, Tom/0000-0001-5178-3656; Kama, Mihkel/0000-0003-0065-7267 FU Netherlands Organization for Scientific Research (NWO) [639.041.335]; NASA Exobiology and Evolutionary Biology Program from Rensselaer Polytechnic Institute; STFC; JSPS KAKENHI [23540266]; Simons Foundation: Simons Collaboration on the Origins of Life (SCOL) Investigator award [321183]; National Science Foundation Graduate Research Fellowship; Huygens fellowship from Leiden University; European Union A-ERC grant [291141 CHEMPLAN] FX We thank the anonymous referee for insightful comments that helped to improve this paper. This work uses the following ALMA data: ADS/JAO. ALMA#2013.1.00902.S and ADS/JAO. ALMA#2013.1.00114.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. C.W. acknowledges support from the Netherlands Organization for Scientific Research (NWO, program 639.041.335). E.H. acknowledges the support of the National Science Foundation for his program in astrochemistry, and support from the NASA Exobiology and Evolutionary Biology Program through a subcontract from Rensselaer Polytechnic Institute. Astrophysics at QUB is supported by a grant from the STFC. Y.A. acknowledges support from JSPS KAKENHI, grant number 23540266. K.I.O. also acknowledges funding from the Simons Foundation: Simons Collaboration on the Origins of Life (SCOL) Investigator award 321183. R.A.L. gratefully acknowledges funding from a National Science Foundation Graduate Research Fellowship. This work is supported by a Huygens fellowship from Leiden University and by the European Union A-ERC grant 291141 CHEMPLAN. NR 45 TC 3 Z9 3 U1 8 U2 15 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 20 PY 2016 VL 823 IS 1 AR L10 DI 10.3847/2041-8205/823/1/L10 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DM5LY UT WOS:000376391700010 ER PT J AU Miller, MJ Esser, HJ Loaiza, JR Herre, EA Aguilar, C Quintero, D Alvarez, E Bermingham, E AF Miller, Matthew J. Esser, Helen J. Loaiza, Jose R. Herre, Edward Allen Aguilar, Celestino Quintero, Diomedes Alvarez, Eric Bermingham, Eldredge TI Molecular Ecological Insights into Neotropical Bird-Tick Interactions SO PLOS ONE LA English DT Article ID MOUNTAIN-SPOTTED-FEVER; 16S RDNA SEQUENCES; ACARI IXODIDAE; WILD BIRDS; RICKETTSIAL INFECTION; AMBLYOMMA-AUREOLATUM; BORRELIA-BURGDORFERI; MIGRATORY BIRDS; BORNE PATHOGENS; RAIN-FOREST AB In the tropics, ticks parasitize many classes of vertebrate hosts. However, because many tropical tick species are only identifiable in the adult stage, and these adults usually parasitize mammals, most attention on the ecology of tick-host interactions has focused on mammalian hosts. In contrast, immature Neotropical ticks are often found on wild birds, yet difficulties in identifying immatures hinder studies of birds' role in tropical tick ecology and tick-borne disease transmission. In Panama, we found immature ticks on 227 out of 3,498 individually-sampled birds representing 93 host species (24% of the bird species sampled, and 13% of the Panamanian land bird fauna). Tick parasitism rates did not vary with rainfall or temperature, but did vary significantly with several host ecological traits. Likewise, Neotropical-Nearctic migratory birds were significantly less likely to be infested than resident species. Using a molecular library developed from morphologically-identified adult ticks specifically for this study, we identified eleven tick species parasitizing birds, indicating that a substantial portion of the Panamanian avian species pool is parasitized by a diversity of tick species. Tick species that most commonly parasitized birds had the widest diversity of avian hosts, suggesting that immature tick species are opportunistic bird parasites. Although certain avian ecological traits are positively associated with parasitism, we found no evidence that individual tick species show specificity to particular avian host ecological traits. Finally, our data suggest that the four principal vectors of Rocky Mountain Spotted Fever in the Neotropics rarely, if ever, parasitize Panamanian birds. However, other tick species that harbor newly-discovered rickettsial parasites of unknown pathogenicity are frequently found on these birds. Given our discovery of broad interaction between Panamanian tick and avian biodiversity, future work on tick ecology and the dynamics of emerging tropical tick-borne pathogens should explicitly consider wild bird as hosts. C1 [Miller, Matthew J.; Esser, Helen J.; Loaiza, Jose R.; Herre, Edward Allen; Aguilar, Celestino; Alvarez, Eric; Bermingham, Eldredge] Smithsonian Trop Res Inst, Panama City, Panama. [Miller, Matthew J.] Villanova Univ, Dept Biol, Villanova, PA 19085 USA. [Esser, Helen J.] Wageningen Univ, Dept Environm Sci, NL-6700 AP Wageningen, Netherlands. [Loaiza, Jose R.; Aguilar, Celestino] Inst Invest Cient & Serv Alta Tecnol INDICASAT AI, Ctr Biodiversidad & Descubrimiento Drogas, Panama City, Panama. [Alvarez, Eric] Univ Panama, Centralamer Masters Program Entomol, Panama City, Panama. [Quintero, Diomedes] Univ Panama, GB Fairchild Invertebrate Museum, Panama City, Panama. [Bermingham, Eldredge] Patricia & Phillip Frost Museum Sci, Miami, FL USA. [Miller, Matthew J.] Univ Oklahoma, Sam Noble Oklahoma Museum Nat Hist, Norman, OK 73019 USA. [Miller, Matthew J.] Univ Oklahoma, Dept Biol, Norman, OK 73019 USA. RP Miller, MJ (reprint author), Smithsonian Trop Res Inst, Panama City, Panama.; Miller, MJ (reprint author), Villanova Univ, Dept Biol, Villanova, PA 19085 USA.; Miller, MJ (reprint author), Univ Oklahoma, Sam Noble Oklahoma Museum Nat Hist, Norman, OK 73019 USA.; Miller, MJ (reprint author), Univ Oklahoma, Dept Biol, Norman, OK 73019 USA. EM mjmiller@ou.edu OI Miller, Matthew/0000-0002-2939-0239 FU US Centers for Disease Control; Smithsonian Grand Challenges Award; graduate school of Production Ecology and Resource Conservation of Wageningen University; NIH/NSF Ecology and Evolution of Infectious Diseases Award from the Fogarty International Center [3R01-TW005869-05S1]; Smithsonian Institution's DNA Barcoding Network FX This study was partially funded by an interagency award from the US Centers for Disease Control ("Effect of Anthropogenic Climate Change on the Ecology of Zoonotic and Vector-borne Diseases"; http://www.cdc.gov/), and a Smithsonian Grand Challenges Award ("Tropical Vertebrate Diversity Loss and the Emergence of Tick-borne Diseases"; https://www.si.edu/consortia). HJE was supported by the graduate school of Production Ecology and Resource Conservation of Wageningen University (https://www.pe-rc.nl/). The STRI Bird Collection was supported by an NIH/NSF Ecology and Evolution of Infectious Diseases Award from the Fogarty International Center (3R01-TW005869-05S1; http://www.fic.nih.gov/). DNA barcode sequencing was supported from a grant from the Smithsonian Institution's DNA Barcoding Network (http://barcoding.si.edu/). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 66 TC 1 Z9 2 U1 6 U2 13 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 20 PY 2016 VL 11 IS 5 AR e0155989 DI 10.1371/journal.pone.0155989 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DM4BV UT WOS:000376291500037 PM 27203693 ER PT J AU Roach, NT Hatala, KG Ostrofsky, KR Villmoare, B Reeves, JS Du, A Braun, DR Harris, JWK Behrensmeyer, AK Richmond, BG AF Roach, Neil T. Hatala, Kevin G. Ostrofsky, Kelly R. Villmoare, Brian Reeves, Jonathan S. Du, Andrew Braun, David R. Harris, John W. K. Behrensmeyer, Anna K. Richmond, Brian G. TI Pleistocene footprints show intensive use of lake margin habitats by Homo erectus groups SO SCIENTIFIC REPORTS LA English DT Article ID KRUGER-NATIONAL-PARK; TURKANA-BASIN; KOOBI-FORA; CONTINGENCY-TABLES; HOMINID EVOLUTION; NORTHERN KENYA; EAST-AFRICA; PLIOPLEISTOCENE; TERRESTRIAL; DINOSAURS AB Reconstructing hominin paleoecology is critical for understanding our ancestors' diets, social organizations and interactions with other animals. Most paleoecological models lack fine-scale resolution due to fossil hominin scarcity and the time-averaged accumulation of faunal assemblages. Here we present data from 481 fossil tracks from northwestern Kenya, including 97 hominin footprints attributed to Homo erectus. These tracks are found in multiple sedimentary layers spanning approximately 20 thousand years. Taphonomic experiments show that each of these trackways represents minutes to no more than a few days in the lives of the individuals moving across these paleolandscapes. The geology and associated vertebrate fauna place these tracks in a deltaic setting, near a lakeshore bordered by open grasslands. Hominin footprints are disproportionately abundant in this lake margin environment, relative to hominin skeletal fossil frequency in the same deposits. Accounting for preservation bias, this abundance of hominin footprints indicates repeated use of lakeshore habitats by Homo erectus. Clusters of very large prints moving in the same direction further suggest these hominins traversed this lakeshore in multi-male groups. Such reliance on near water environments, and possibly aquatic-linked foods, may have influenced hominin foraging behavior and migratory routes across and out of Africa. C1 [Roach, Neil T.] Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA. [Roach, Neil T.; Richmond, Brian G.] Amer Museum Nat Hist, Div Anthropol, New York, NY 10024 USA. [Hatala, Kevin G.; Richmond, Brian G.] Max Planck Inst Evolutionare Anthropol, Dept Human Evolut, D-04103 Leipzig, Germany. [Hatala, Kevin G.; Ostrofsky, Kelly R.; Reeves, Jonathan S.; Du, Andrew; Braun, David R.] George Washington Univ, Ctr Adv Study Human Paleobiol, Washington, DC 20052 USA. [Villmoare, Brian] Univ Nevada, Dept Anthropol, Las Vegas, NV 89154 USA. [Harris, John W. K.] Rutgers State Univ, Dept Anthropol, New Brunswick, NJ 08901 USA. [Behrensmeyer, Anna K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC NHB 121, Washington, DC 20013 USA. RP Roach, NT (reprint author), Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA.; Roach, NT; Richmond, BG (reprint author), Amer Museum Nat Hist, Div Anthropol, New York, NY 10024 USA.; Richmond, BG (reprint author), Max Planck Inst Evolutionare Anthropol, Dept Human Evolut, D-04103 Leipzig, Germany. EM ntroach@fas.harvard.edu; brichmond@amnh.org FU National Science Foundation [BCS - 1128170, 0924476, 1232522, DGE - 0801634, EAR77-23149, SMA - 1409612]; Wenner-Gren Foundation; Leakey Foundation; George Washington University Selective Excellence Initiative and University Facilitating Fund FX The authors would like to thank David Raichlen, Andrew Barr and David Pilbeam for helpful comments on earlier drafts of this paper. We also thank the National Museums of Kenya and the students and staff of the Koobi Fora Field School, without whose help this project could not have been completed. AKB also thanks Leo Laporte and the 1978-79 East Turkana field crew. Funding was generously provided by the National Science Foundation (BCS - 1128170, 0924476, 1232522; DGE - 0801634; EAR77-23149; SMA - 1409612), Wenner-Gren Foundation, Leakey Foundation and the George Washington University Selective Excellence Initiative and University Facilitating Fund. This paper is dedicated to the memory of our friend Andrew Hill. NR 50 TC 3 Z9 3 U1 16 U2 23 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 MAY 20 PY 2016 VL 6 AR 26374 DI 10.1038/srep26374 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DM2RR UT WOS:000376195100001 PM 27199261 ER PT J AU McCarthy, MC Gauss, J AF McCarthy, Michael C. Gauss, Juergen TI Exotic SiO2H2 Isomers: Theory and Experiment Working in Harmony SO JOURNAL OF PHYSICAL CHEMISTRY LETTERS LA English DT Article ID INFRARED SPECTROSCOPIC EVIDENCE; MOLECULAR-ORBITAL METHODS; SILICIC-ACID MOLECULES; GAS-PHASE; SILANOIC ACID; AB-INITIO; ROTATIONAL SPECTROSCOPY; VIBRATIONAL FREQUENCIES; OXYGEN; SILYLENE AB Replacing carbon with silicon can result in dramatic and unanticipated changes in isomeric stability, as the well-studied CO2H2 and the essentially unknown SiO2H2 systems illustrate. Guided by coupled cluster calculations, three SiO2H2 isomers have been detected and spectroscopically characterized in a molecular beam discharge source using rotational spectroscopy. The cis,trans conformer of dihydroxysilylene HOSiOH, the ground-state isomer, and the high-energy, metastable dioxasilirane c-H2SiO2 are abundantly produced in a dilute SiH4/O-2 electrical discharge, enabling precise structural determinations of both by a combination of isotopic measurements and calculated vibrational corrections. The isotopic studies also provide insight into their formation route, suggesting that c-H2SiO2 is formed promptly in the expansion but that cis,trans-HOSiOH is likely formed by secondary reactions following formation of the most stable dissociation pair, SiO + H2O. Although less abundant, the rotational spectrum of trans-silanoic acid, the silicon analogue of formic acid, HSi(O)OH, has also been observed. C1 [McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [McCarthy, Michael C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Gauss, Juergen] Johannes Gutenberg Univ Mainz, Inst Phys Chem, D-55128 Mainz, Germany. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; McCarthy, MC (reprint author), Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. EM mmccarthy@cfa.harvard.edu FU NSF [CHE-1058063]; NASA [NNX13AE59G]; Deutsche Forschungsgemeinschaft (DFG) [GA 370/6-1, 6-2] FX The work in Cambridge is supported by NSF Grant CHE-1058063 and NASA Grant NNX13AE59G, and the work in Mainz is supported by the Deutsche Forschungsgemeinschaft (DFG Grant GA 370/6-1 and 6-2). We thank E. S. Palmer and P. Antonucci for technical assistance, M.-A. Martin-Drumel and C. A. Gottlieb for helpful discussions, and O. Martinez and K N. Crabtree for assistance with initial laboratory searches. NR 34 TC 3 Z9 3 U1 4 U2 9 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1948-7185 J9 J PHYS CHEM LETT JI J. Phys. Chem. Lett. PD MAY 19 PY 2016 VL 7 IS 10 BP 1895 EP 1900 DI 10.1021/acs.jpclett.6b00632 PG 6 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Atomic, Molecular & Chemical SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA DM5WL UT WOS:000376421200022 PM 27139016 ER PT J AU Buddhachat, K Klinhom, S Siengdee, P Brown, JL Nomsiri, R Kaewmong, P Thitaram, C Mahakkanukrauh, P Nganvongpanit, K AF Buddhachat, Kittisak Klinhom, Sarisa Siengdee, Puntita Brown, Janine L. Nomsiri, Raksiri Kaewmong, Patcharaporn Thitaram, Chatchote Mahakkanukrauh, Pasuk Nganvongpanit, Korakot TI Elemental Analysis of Bone, Teeth, Horn and Antler in Different Animal Species Using Non-Invasive Handheld X- Ray Fluorescence SO PLOS ONE LA English DT Article ID CALCIUM HYDROXYAPATITE; MECHANICAL-PROPERTIES; TRACE-ELEMENTS; IN-VIVO; ELEPHANT; BOVINE; LEAD; AGE; QUANTIFICATION; IMMOBILIZATION AB Mineralized tissues accumulate elements that play crucial roles in animal health. Although elemental content of bone, blood and teeth of human and some animal species have been characterized, data for many others are lacking, as well as species comparisons. Here we describe the distribution of elements in horn (Bovidae), antler (Cervidae), teeth and bone (humerus) across a number of species determined by handheld X-ray fluorescence (XRF) to better understand differences and potential biological relevance. A difference in elemental profiles between horns and antlers was observed, possibly due to the outer layer of horns being comprised of keratin, whereas antlers are true bone. Species differences in tissue elemental content may be intrinsic, but also related to feeding habits that contribute to mineral accumulation, particularly for toxic heavy metals. One significant finding was a higher level of iron (Fe) in the humerus bone of elephants compared to other species. This may be an adaptation of the hematopoietic system by distributing Fe throughout the bone rather than the marrow, as elephant humerus lacks a marrow cavity. We also conducted discriminant analysis and found XRF was capable of distinguishing samples from different species, with humerus bone being the best source for species discrimination. For example, we found a 79.2% correct prediction and success rate of 80% for classification between human and non-human humerus bone. These findings show that handheld XRF can serve as an effective tool for the biological study of elemental composition in mineralized tissue samples and may have a forensic application. C1 [Buddhachat, Kittisak; Siengdee, Puntita; Nganvongpanit, Korakot] Chiang Mai Univ, Fac Vet Med, Dept Vet Biosci & Publ Hlth, Anim Bone & Joint Res Lab, Chiang Mai 50100, Thailand. [Klinhom, Sarisa; Thitaram, Chatchote; Nganvongpanit, Korakot] Chiang Mai Univ, Fac Vet Med, Elephant Res & Educ Ctr, Chiang Mai 50100, Thailand. [Brown, Janine L.] Ctr Species Survival, Smithsonian Conservat Biol Inst, Natl Zool Pk 1500 Remount Rd, Front Royal, VA 22630 USA. [Nomsiri, Raksiri] Chiang Mai Night Safari, Vet Conservat & Res Sect, Chiang Mai 50100, Thailand. [Kaewmong, Patcharaporn] Phuket Marine Biol Ctr, Phuket 83000, Thailand. [Mahakkanukrauh, Pasuk; Nganvongpanit, Korakot] Chiang Mai Univ, Osteol Res & Training Ctr, Excellence Ctr, Chiang Mai 50200, Thailand. RP Nganvongpanit, K (reprint author), Chiang Mai Univ, Fac Vet Med, Dept Vet Biosci & Publ Hlth, Anim Bone & Joint Res Lab, Chiang Mai 50100, Thailand.; Nganvongpanit, K (reprint author), Chiang Mai Univ, Fac Vet Med, Elephant Res & Educ Ctr, Chiang Mai 50100, Thailand.; Nganvongpanit, K (reprint author), Chiang Mai Univ, Osteol Res & Training Ctr, Excellence Ctr, Chiang Mai 50200, Thailand. EM korakot.n@cmu.ac.th FU Chiang Mai University (CMU); Elephant Research and Education Center (EREC) FX The authors are grateful for the research funding provided by the Chiang Mai University (CMU) through the research administration office that provided a budget to the Excellence Center in Osteology Research and Training Center (ORTC) and Elephant Research and Education Center (EREC). NR 55 TC 1 Z9 1 U1 10 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 MAY 19 PY 2016 VL 11 IS 5 AR e0155458 DI 10.1371/journal.pone.0155458 PG 21 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DM4BR UT WOS:000376291100045 PM 27196603 ER PT J AU Soliveres, S Manning, P Prati, D Gossner, MM Alt, F Arndt, H Baumgartner, V Binkenstein, J Birkhofer, K Blaser, S Bluthgen, N Boch, S Bohm, S Borschig, C Buscot, F Diekotter, T Heinze, J Holzel, N Jung, K Klaus, VH Klein, AM Kleinebecker, T Klemmer, S Krauss, J Lange, M Morris, EK Muller, J Oelmann, Y Overmann, J Pasalic, E Renner, SC Rillig, MC Schaefer, HM Schloter, M Schmitt, B Schoning, I Schrumpf, M Sikorski, J Socher, SA Solly, EF Sonnemann, I Sorkau, E Steckel, J Steffan-Dewenter, I Stempfhuber, B Tschapka, M Turke, M Venter, P Weiner, CN Weisser, WW Werner, M Westphal, C Wilcke, W Wolters, V Wubet, T Wurst, S Fischer, M Allan, E AF Soliveres, Santiago Manning, Peter Prati, Daniel Gossner, Martin M. Alt, Fabian Arndt, Hartmut Baumgartner, Vanessa Binkenstein, Julia Birkhofer, Klaus Blaser, Stefan Bluethgen, Nico Boch, Steffen Boehm, Stefan Boerschig, Carmen Buscot, Francois Diekoetter, Tim Heinze, Johannes Hoelzel, Norbert Jung, Kirsten Klaus, Valentin H. Klein, Alexandra-Maria Kleinebecker, Till Klemmer, Sandra Krauss, Jochen Lange, Markus Morris, E. Kathryn Mueller, Joerg Oelmann, Yvonne Overmann, Joerg Pasalic, Esther Renner, Swen C. Rillig, Matthias C. Schaefer, H. Martin Schloter, Michael Schmitt, Barbara Schoening, Ingo Schrumpf, Marion Sikorski, Johannes Socher, Stephanie A. Solly, Emily F. Sonnemann, Ilja Sorkau, Elisabeth Steckel, Juliane Steffan-Dewenter, Ingolf Stempfhuber, Barbara Tschapka, Marco Tuerke, Manfred Venter, Paul Weiner, Christiane N. Weisser, Wolfgang W. Werner, Michael Westphal, Catrin Wilcke, Wolfgang Wolters, Volkmar Wubet, Tesfaye Wurst, Susanne Fischer, Markus Allan, Eric TI Locally rare species influence grassland ecosystem multifunctionality SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE biodiversity; common species; ecosystem function; identity hypothesis; land use; multitrophic ID BELOW-GROUND BIODIVERSITY; LAND-USE INTENSIFICATION; FUNCTIONAL DIVERSITY; PLANT DIVERSITY; USE INTENSITY; RESISTANCE; ABUNDANCE; SERVICES; IDENTITY; FERTILIZATION AB Species diversity promotes the delivery of multiple ecosystem functions (multifunctionality). However, the relative functional importance of rare and common species in driving the biodiversity multifunctionality relationship remains unknown. We studied the relationship between the diversity of rare and common species (according to their local abundances and across nine different trophic groups), and multifunctionality indices derived from 14 ecosystem functions on 150 grasslands across a land use intensity (LUI) gradient. The diversity of above- and below-ground rare species had opposite effects, with rare above-ground species being associated with high levels of multifunctionality, probably because their effects on different functions did not trade off against each other. Conversely, common species were only related to average, not high, levels of multifunctionality, and their functional effects declined with LUI. Apart from the community level effects of diversity, we found significant positive associations between the abundance of individual species and multifunctionality in 6% of the species tested. Species specific functional effects were best predicted by their response to LUI: species that declined in abundance with land use intensification were those associated with higher levels of multifunctionality. Our results highlight the importance of rare species for ecosystem multifunctionality and help guiding future conservation priorities. C1 [Soliveres, Santiago; Prati, Daniel; Blaser, Stefan; Boch, Steffen; Schmitt, Barbara; Allan, Eric] Univ Bern, Inst Plant Sci, Altenbergrain 21, CH-3013 Bern, Switzerland. [Manning, Peter; Fischer, Markus] Biodivers & Climate Res Ctr BIK F, Senckenberg Gesell Nat Forsch, Senckenberganlage 25, D-60325 Frankfurt, Germany. [Gossner, Martin M.; Lange, Markus; Pasalic, Esther; Weisser, Wolfgang W.] Univ Jena, Inst Ecol, Dornburger Str 159, D-07743 Jena, Germany. [Gossner, Martin M.; Weisser, Wolfgang W.] Tech Univ Munich, Sch Life Sci Weihenstephan, Dept Ecol & Ecosyst Management, Terr Ecol Res Grp, Hans Carl von Carlowitz Pl 2, D-85354 Freising Weihenstephan, Germany. [Alt, Fabian; Oelmann, Yvonne; Sorkau, Elisabeth] Univ Tubingen, Geocol, Ruemelinstr 19-23, D-72070 Tubingen, Germany. [Arndt, Hartmut; Venter, Paul] Univ Cologne, Inst Zool, Dept Gen Ecol, D-50674 Cologne, Germany. [Baumgartner, Vanessa; Overmann, Joerg; Sikorski, Johannes] Leibniz Inst DSMZ German Collect Microorganisms &, Inhoffenstr 7B, D-38124 Braunschweig, Germany. [Binkenstein, Julia] Univ Freiburg, Inst Biol 1, Hauptstr 1, D-79104 Freiburg, Germany. [Birkhofer, Klaus] Lund Univ, Dept Biol, Lund, Sweden. [Bluethgen, Nico] Tech Univ Darmstadt, Ecol Networks, Biol, Schnittspahnstr 3, D-64287 Darmstadt, Germany. [Boehm, Stefan; Jung, Kirsten; Tschapka, Marco] Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. [Boerschig, Carmen; Westphal, Catrin] Univ Gottingen, Dept Crop Sci, Agroecol, Grisebachstr 6, D-37077 Gottingen, Germany. [Buscot, Francois; Klemmer, Sandra] UFZ Helmholtz Ctr Environm Res, Dept Soil Ecol, Theodor Lieser Str 4, D-06120 Halle, Saale, Germany. [Buscot, Francois; Tuerke, Manfred; Wubet, Tesfaye] German Ctr Integrat Biodivers Res iDiv, Deutsch Pl 5e, D-04103 Leipzig, Germany. [Diekoetter, Tim] Univ Kiel, Dept Landscape Ecol, Kiel, Germany. [Heinze, Johannes; Mueller, Joerg] Univ Potsdam, Biodivers Res Systemat Bot, Maulbeerallee, D-14469 Potsdam, Germany. [Hoelzel, Norbert; Klaus, Valentin H.; Kleinebecker, Till] Univ Munster, Inst Landscape Ecol, Heisenbergstr 2, D-48149 Munster, Germany. [Klein, Alexandra-Maria] Univ Freiburg, Nat Conservat & Landscape Ecol, Hugstetter Str 55, D-79106 Freiburg, Germany. [Krauss, Jochen; Steckel, Juliane; Steffan-Dewenter, Ingolf; Weiner, Christiane N.; Werner, Michael] Univ Wurzburg, Dept Anim Ecol & Trop Biol, Bioctr, D-97074 Wurzburg, Germany. [Lange, Markus; Schoening, Ingo; Schrumpf, Marion; Solly, Emily F.] Max Planck Inst Biogeochem, Hans Knoell Str 10, D-07745 Jena, Germany. [Morris, E. Kathryn] Xavier Univ, Dept Biol, 3800 Victory Pkwy, Cincinnati, OH 45207 USA. [Morris, E. Kathryn; Rillig, Matthias C.; Sonnemann, Ilja] Free Univ Berlin, Inst Biol Funkt Biodiversitat, Konigin Luise Str 1-3, D-14195 Berlin, Germany. [Renner, Swen C.] Natl Zool Pk, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. [Renner, Swen C.] Univ Nat Resources & Life Sci, Inst Zool, Gregor Mendel Str 33, A-1180 Vienna, Austria. [Rillig, Matthias C.] Berlin Brandenburg Inst Adv Biodivers Res BBIB, D-14195 Berlin, Germany. [Schaefer, H. Martin] Univ Freiburg, Dept Ecol & Evolutionary Biol, Fac Biol, Hauptstr 1, D-79104 Freiburg, Germany. [Schloter, Michael; Stempfhuber, Barbara] Helmholtz Zentrum Munchen, Res Unit Environm Genom, Ingolstadter Landstr 1, D-85758 Oberschleissheim, Germany. [Socher, Stephanie A.] Salzburg Univ, Dept Ecol & Evolut, A-65020 Salzburg 4, Austria. [Tuerke, Manfred] Univ Leipzig, Inst Biol, Johannisallee 21, D-04103 Leipzig, Germany. [Wilcke, Wolfgang] Karlsruhe Inst Technol, Inst Geog & Geoecol, Reinhard Baumeister Pl 1, D-76131 Karlsruhe, Germany. [Wolters, Volkmar] Univ Giessen, Dept Anim Ecol, D-35390 Giessen, Germany. [Wurst, Susanne] Free Univ Berlin, Inst Biol, Funct Biodivers, Konigin Luise Str 1-3, D-14195 Berlin, Germany. RP Soliveres, S (reprint author), Univ Bern, Inst Plant Sci, Altenbergrain 21, CH-3013 Bern, Switzerland. EM santiago.soliveres@ips.unibe.ch RI Schoning, Ingo/D-3341-2009; Wolters, Volkmar/B-4635-2010; Krauss, Jochen/C-6216-2014; Fischer, Markus/C-6411-2008; Manning, Peter/I-6523-2012; Diekotter, Tim/L-2463-2016; Boch, Steffen/L-5436-2016; Wilcke, Wolfgang/P-4620-2016; Gossner, Martin M./J-2730-2015; Holzel, Norbert/H-8753-2013; Rillig, Matthias/B-3675-2009; Bluthgen, Nico/F-5983-2010; OI Schoning, Ingo/0000-0002-9830-5026; Weiner, Christiane/0000-0003-4013-4663; Krauss, Jochen/0000-0003-2304-9117; Fischer, Markus/0000-0002-5589-5900; Manning, Peter/0000-0002-7940-2023; Wilcke, Wolfgang/0000-0002-6031-4613; Gossner, Martin M./0000-0003-1516-6364; Rillig, Matthias/0000-0003-3541-7853; Soliveres Codina, Santiago/0000-0001-9661-7192; Solly, Emily/0000-0002-3157-1805; Renner, Swen/0000-0002-6893-4219 FU DFG (Deutsche Forschungsgemeinschaft; German Research Foundation) Priority Program 'Infrastructure-Biodiversity Exploratories' [1374, WE 3018/21-1, Li150/22-1] FX This work was funded by the DFG (Deutsche Forschungsgemeinschaft; German Research Foundation) Priority Program 1374 'Infrastructure-Biodiversity Exploratories' (WE 3018/21-1, Li150/22-1). NR 65 TC 5 Z9 6 U1 52 U2 82 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 EI 1471-2970 J9 PHILOS T R SOC B JI Philos. Trans. R. Soc. B-Biol. Sci. PD MAY 19 PY 2016 VL 371 IS 1694 AR 20150269 DI 10.1098/rstb.2015.0269 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA DL8MQ UT WOS:000375896500003 ER PT J AU Shi, W Wen, J Pan, BR AF Shi, Wei Wen, Jun Pan, Borong TI A comparison of ITS sequence data and morphology for Calligonum pumilum and C. mongolicum (Polygonaceae) and its taxonomic implications SO PHYTOTAXA LA English DT Article DE Calligonum; China; species delimitation; synonymy; taxonomy ID PHYLOGENETIC INFERENCE; EVOLUTIONARY; POLYPLOIDY; COMOSUM; CLIMATE; TUNISIA; PLANTS; CHINA; SIZE AB Several lines of evidence including morphology, chromosome numbers, karyotypes, and phenology were previously used to clarify the taxonomic relationship between Calligonum mongolicum and C. pumilum (Polygonaceae). We employed sequences of the commonly used bar-coding locus, the nuclear ribosomal ITS region, to differentiate Calligonum mongolicum and C. pumilum, based on a sampling scheme of seven populations in three desert regions in China. Phylogenetic analyses did not support the monophyly of each of the two species; instead, populations of the two taxa are intermixed in the analysis. This pattern of intermixing is consistent with the result of the neighbor-net analysis. The ITS region can distinguish other species beyond the C. mongolicum complex defined by morphology both within a section and among sections in Calligonum. The intermixed non-monophyletic pattern of the widespread C. mongolicum and the narrowly distributed C. pumilum supports the merge of C. pumilum with C. mongolicum, consistent with morphological, cytological and karyotype analyses. We herein formally treat C. pumilum as the synonym of C. mongolicum. C1 [Shi, Wei; Pan, Borong] Chinese Acad Sci, Inst Ecol & Geog Xinjiang, CN-830011 Urumqi, Peoples R China. [Shi, Wei; Pan, Borong] Chinese Acad Sci, Turpan Eremophytes Bot Garden, CN-838008 Turpan, Peoples R China. [Shi, Wei; Wen, Jun] Smithsonian Inst, Dept Bot, POB 37012, Washington, DC 20013 USA. RP Wen, J (reprint author), Smithsonian Inst, Dept Bot, POB 37012, Washington, DC 20013 USA. EM WENJ@si.edu; brpan@163.com FU National Natural Science Foundation of China [31100150, 31200237]; Laboratories of Analytical Biology of the National Museum of Natural History, the Smithsonian Institution FX This work was supported by two grants from the National Natural Science Foundation of China (Project No 31100150 and 31200237) and the Laboratories of Analytical Biology of the National Museum of Natural History, the Smithsonian Institution. We thank Dr. Alexander Sennikov and two anonymous reviewers for their constructive suggestions to improve the paper. NR 53 TC 0 Z9 0 U1 2 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1179-3155 EI 1179-3163 J9 PHYTOTAXA JI Phytotaxa PD MAY 18 PY 2016 VL 261 IS 2 BP 157 EP 167 DI 10.11646/phytotaxa.261.2.5 PG 11 WC Plant Sciences SC Plant Sciences GA DT9ME UT WOS:000381824400005 ER PT J AU Machado, JP Johnson, WE Gilbert, MTP Zhang, GJ Jarvis, ED O'Brien, SJ Antunes, A AF Machado, Joao Paulo Johnson, Warren E. Gilbert, M. Thomas P. Zhang, Guojie Jarvis, Erich D. O'Brien, Stephen J. Antunes, Agostinho TI Bone-associated gene evolution and the origin of flight in birds SO BMC GENOMICS LA English DT Article ID FREE-RADICAL PRODUCTION; MAXIMUM-LIKELIHOOD; PHYLOGENETIC ANALYSIS; BODY-SIZE; FLYING VERTEBRATES; GLUCOSE REGULATION; ENERGY-METABOLISM; MINERAL DENSITY; MASS; BATS AB Background: Bones have been subjected to considerable selective pressure throughout vertebrate evolution, such as occurred during the adaptations associated with the development of powered flight. Powered flight evolved independently in two extant clades of vertebrates, birds and bats. While this trait provided advantages such as in aerial foraging habits, escape from predators or long-distance travels, it also imposed great challenges, namely in the bone structure. Results: We performed comparative genomic analyses of 89 bone-associated genes from 47 avian genomes (including 45 new), 39 mammalian, and 20 reptilian genomes, and demonstrate that birds, after correcting for multiple testing, have an almost two-fold increase in the number of bone-associated genes with evidence of positive selection (similar to 52.8 %) compared with mammals (similar to 30.3 %). Most of the positive-selected genes in birds are linked with bone regulation and remodeling and thirteen have been linked with functional pathways relevant to powered flight, including bone metabolism, bone fusion, muscle development and hyperglycemia levels. Genes encoding proteins involved in bone resorption, such as TPP1, had a high number of sites under Darwinian selection in birds. Conclusions: Patterns of positive selection observed in bird ossification genes suggest that there was a period of intense selective pressure to improve flight efficiency that was closely linked with constraints on body size. C1 [Machado, Joao Paulo; Antunes, Agostinho] Univ Porto, Interdisciplinary Ctr Marine & Environm Res, CIIMAR CIMAR, Rua Bragas 177, P-4050123 Oporto, Portugal. [Machado, Joao Paulo] Univ Porto, Abel Salazar Biomed Sci Inst ICBAS, Rua Campo Alegre 823, P-4100 Oporto, Portugal. [Johnson, Warren E.] Natl Zool Pk, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. [Gilbert, M. Thomas P.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, Oster Volgade 5-7, DK-1350 Copenhagen, Denmark. [Zhang, Guojie] BGI Shenzhen, China Natl GeneBank, Shenzhen 518083, Peoples R China. [Zhang, Guojie] Univ Copenhagen, Dept Biol, Ctr Social Evolut, Univ Pk 15, DK-2100 Copenhagen, Denmark. [Jarvis, Erich D.] Duke Univ, Med Ctr, Dept Neurobiol, Box 3209, Durham, NC 27710 USA. [Jarvis, Erich D.] Howard Hughes Med Inst, Chevy Chase, MD 20815 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, 8000 N Ocean Dr, Ft Lauderdale, FL 33004 USA. [Antunes, Agostinho] Univ Porto, Fac Sci, Dept Biol, Rua Campo Alegre 823, P-4100 Oporto, Portugal. RP Antunes, A (reprint author), Univ Porto, Interdisciplinary Ctr Marine & Environm Res, CIIMAR CIMAR, Rua Bragas 177, P-4050123 Oporto, Portugal.; Antunes, A (reprint author), Univ Porto, Fac Sci, Dept Biol, Rua Campo Alegre 823, P-4100 Oporto, Portugal. EM aantunes@ciimar.up.pt FU Portuguese "Fundacao para a Ciencia e a Tecnologia" (FCT) [SFRH/BD/65245/2009]; Howard Hughes Medical Institute; Russian Ministry of Science Mega-grant [11.G34.31.0068]; FCT [UID/Multi/04423/2013, PTDC/AAG-GLO/6887/2014]; European Regional Development Fund (ERDF) FX JPM was funded by the PhD grant SFRH/BD/65245/2009 from the Portuguese "Fundacao para a Ciencia e a Tecnologia" (FCT). EDJ was supported by the Howard Hughes Medical Institute. SJO was supported in part by Russian Ministry of Science Mega-grant no.11.G34.31.0068. AA was partially supported by the Strategic Funding UID/Multi/04423/2013 through national funds provided by FCT and European Regional Development Fund (ERDF) in the framework of the programme PT2020, and the FCT project PTDC/AAG-GLO/6887/2014. NR 99 TC 0 Z9 0 U1 24 U2 31 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2164 J9 BMC GENOMICS JI BMC Genomics PD MAY 18 PY 2016 VL 17 AR 371 DI 10.1186/s12864-016-2681-7 PG 14 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA DM5AD UT WOS:000376357800001 PM 27193938 ER PT J AU Fister, AS Mejia, LC Zhang, YF Herre, EA Maximova, SN Guiltinan, MJ AF Fister, Andrew S. Mejia, Luis C. Zhang, Yufan Allen Herre, Edward Maximova, Siela N. Guiltinan, Mark J. TI Theobroma cacao L. pathogenesis-related gene tandem array members show diverse expression dynamics in response to pathogen colonization SO BMC GENOMICS LA English DT Article DE Pathogenesis-related; PR genes; PR proteins; Gene duplication; Tandem arrays; Disease resistance; Pathogen; Phytophthora; Colletotrichum ID SYSTEMIC ACQUIRED-RESISTANCE; THAUMATIN-LIKE PROTEINS; GENOME-WIDE ANALYSIS; DISEASE RESISTANCE; SALICYLIC-ACID; MONILIOPHTHORA-PERNICIOSA; DUPLICATED GENES; COLLETOTRICHUM-GLOEOSPORIOIDES; ARABIDOPSIS-THALIANA; DEFENSE RESPONSE AB Background: The pathogenesis-related (PR) group of proteins are operationally defined as polypeptides that increase in concentration in plant tissues upon contact with a pathogen. To date, 17 classes of highly divergent proteins have been described that act through multiple mechanisms of pathogen resistance. Characterizing these families in cacao, an economically important tree crop, and comparing the families to those in other species, is an important step in understanding cacao's immune response. Results: Using publically available resources, all members of the 17 recognized pathogenesis-related gene families in the genome of Theobroma cacao were identified and annotated resulting in a set of similar to 350 members in both published cacao genomes. Approximately 50 % of these genes are organized in tandem arrays scattered throughout the genome. This feature was observed in five additional plant taxa (three dicots and two monocots), suggesting that tandem duplication has played an important role in the evolution of the PR genes in higher plants. Expression profiling captured the dynamics and complexity of PR genes expression at basal levels and after induction by two cacao pathogens (the oomycete, Phytophthora palmivora, and the fungus, Colletotrichum theobromicola), identifying specific genes within families that are more responsive to pathogen challenge. Subsequent qRT-PCR validated the induction of several PR-1, PR-3, PR-4, and PR-10 family members, with greater than 1000 fold induction detected for specific genes. Conclusions: We describe candidate genes that are likely to be involved in cacao's defense against Phytophthora and Colletotrichum infection and could be potentially useful for marker-assisted selection for breeding of disease resistant cacao varieties. The data presented here, along with existing cacao-omics resources, will enable targeted functional genetic screening of defense genes likely to play critical functions in cacao's defense against its pathogens. C1 [Fister, Andrew S.; Maximova, Siela N.; Guiltinan, Mark J.] Penn State Univ, Huck Inst Life Sci, 422 Life Sci Bldg, University Pk, PA 16802 USA. [Mejia, Luis C.] Inst Sci Res & High Technol Serv INDICASAT AIP, Panama City, Panama. [Mejia, Luis C.; Allen Herre, Edward] Smithsonian Trop Res Inst, Unit 9100,Box 0948, Balboa 340029998, Ancon Dpo, Panama. [Zhang, Yufan] Princeton Univ, Dept Elect Engn, Princeton, NJ 08544 USA. [Maximova, Siela N.; Guiltinan, Mark J.] Penn State Univ, Dept Plant Sci, 422 Life Sci Bldg, University Pk, PA 16802 USA. RP Guiltinan, MJ (reprint author), Penn State Univ, Huck Inst Life Sci, 422 Life Sci Bldg, University Pk, PA 16802 USA.; Guiltinan, MJ (reprint author), Penn State Univ, Dept Plant Sci, 422 Life Sci Bldg, University Pk, PA 16802 USA. EM mjg9@psu.edu FU Pennsylvania State University's College of Agricultural Sciences; Huck Institutes of the Life Sciences; Penn State Endowed Program in Molecular Biology of Cacao; National Science Foundation BREAD program [IOS-0965353]; Smithsonian Tropical Research Institute's Earl S. Tupper Postdoctoral Fellowship FX This work was supported by The Pennsylvania State University's College of Agricultural Sciences, The Huck Institutes of the Life Sciences, the Penn State Endowed Program in Molecular Biology of Cacao and by a grant from the National Science Foundation BREAD program (IOS-0965353) and by the Smithsonian Tropical Research Institute's Earl S. Tupper Postdoctoral Fellowship. NR 94 TC 2 Z9 2 U1 5 U2 10 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2164 J9 BMC GENOMICS JI BMC Genomics PD MAY 17 PY 2016 VL 17 AR 363 DI 10.1186/s12864-016-2693-3 PG 16 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA DM4WB UT WOS:000376346800001 PM 27189060 ER PT J AU West, JJ Cohen, A Dentener, F Brunekreef, B Zhu, T Armstrong, B Bell, ML Brauer, M Carmichael, G Costa, DL Dockery, DW Kleeman, M Krzyzanowski, M Kunzli, N Liousse, C Lung, SCC Martin, RV Poschl, U Pope, CA Roberts, JM Russell, AG Wiedinmyer, C AF West, J. Jason Cohen, Aaron Dentener, Frank Brunekreef, Bert Zhu, Tong Armstrong, Ben Bell, Michelle L. Brauer, Michael Carmichael, Gregory Costa, Dan L. Dockery, Douglas W. Kleeman, Michael Krzyzanowski, Michal Kuenzli, Nino Liousse, Catherine Lung, Shih-Chun Candice Martin, Randall V. Poeschl, Ulrich Pope, C. Arden, III Roberts, James M. Russell, Armistead G. Wiedinmyer, Christine TI "What We Breathe Impacts Our Health: Improving Understanding of the Link between Air Pollution and Health" SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID FINE PARTICULATE MATTER; LAND-USE REGRESSION; AEROSOL OPTICAL DEPTH; UNITED-STATES; DAILY MORTALITY; CLIMATE-CHANGE; EXPOSURE ESTIMATION; AMBIENT PM2.5; GLOBAL BURDEN; BLACK CARBON C1 [West, J. Jason] Univ N Carolina, Environm Sci & Engn, Chapel Hill, NC 27599 USA. [Cohen, Aaron] Hlth Effects Inst, Boston, MA 02110 USA. [Dentener, Frank] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy. [Brunekreef, Bert] Univ Utrecht, Inst Risk Assessment Sci, NL-3584 CJ Utrecht, Netherlands. [Brunekreef, Bert] Univ Med Ctr Utrecht, Julius Ctr Hlth Sci & Primary Care, NL-3584 CJ Utrecht, Netherlands. [Zhu, Tong] Peking Univ, Coll Environm Sci & Engn, State Key Lab Environm Simulat & Pollut Control, Beijing 100871, Peoples R China. [Armstrong, Ben] London Sch Hyg & Trop Med, Social & Environm Hlth Res, London WC1E 7HT, England. [Bell, Michelle L.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Brauer, Michael] Univ British Columbia, Sch Populat & Publ Hlth, Vancouver, BC V6T 1Z3, Canada. [Carmichael, Gregory] Univ Iowa, Chem & Biochem Engn, Iowa City, IA 52242 USA. [Costa, Dan L.] Off Res & Dev Environm Protect Agcy, Air Climate & Energy Res Program, Durham, NC 27705 USA. [Dockery, Douglas W.] Harvard TH Chan Sch Publ Hlth, Boston, MA 02115 USA. [Kleeman, Michael] Univ Calif Davis, Civil & Environm Engn, Davis, CA 95616 USA. [Krzyzanowski, Michal] Kings Coll London, Environm Res Grp, London SE1 9NH, England. [Kuenzli, Nino] Swiss Trop & Publ Hlth Inst, Epidemiol & Publ Hlth, Basel, Switzerland. [Kuenzli, Nino] Univ Basel, Basel, Switzerland. [Liousse, Catherine] Univ Toulouse, CNRS, Lab Aerol, F-31400 Toulouse, France. [Lung, Shih-Chun Candice] Acad Sinica, Res Ctr Environm Changes, Taipei 115, Taiwan. [Martin, Randall V.] Dalhousie Univ, Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Poeschl, Ulrich] Max Planck Inst Chem, Multiphase Chem Dept, D-55128 Mainz, Germany. [Pope, C. Arden, III] Brigham Young Univ, Econ, Provo, UT 84602 USA. [Roberts, James M.] Natl Ocean & Atmospher Adm, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA. [Russell, Armistead G.] Georgia Inst Technol, Civil & Environm Engn, Atlanta, GA 30332 USA. [Wiedinmyer, Christine] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, Boulder, CO 80301 USA. RP West, JJ (reprint author), Univ N Carolina, Environm Sci & Engn, Chapel Hill, NC 27599 USA.; Cohen, A (reprint author), Hlth Effects Inst, Boston, MA 02110 USA.; Dentener, F (reprint author), Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy.; Zhu, T (reprint author), Peking Univ, Coll Environm Sci & Engn, State Key Lab Environm Simulat & Pollut Control, Beijing 100871, Peoples R China. EM jasonwest@unc.edu; acohen@healtheffects.org; frank.dentener@jrc.ec.europa.eu; tzhu@pku.edu.cn RI Martin, Randall/C-1205-2014; Poschl, Ulrich/A-6263-2010; West, Jason/J-2322-2015; Roberts, James/A-1082-2009; Manager, CSD Publications/B-2789-2015; Kunzli, Nino/F-7195-2014; ZHU, TONG/H-6501-2011 OI Martin, Randall/0000-0003-2632-8402; Poschl, Ulrich/0000-0003-1412-3557; West, Jason/0000-0001-5652-4987; Roberts, James/0000-0002-8485-8172; Kunzli, Nino/0000-0001-8360-080X; FU U.S. National Institute of Environmental Health Sciences [1R21ES022600-01]; National Science Foundation; NOAA Health of the Atmosphere Initiative FX The views presented in this paper were stimulated by a workshop held in Boston in October, 2011: "Atmospheric Chemistry and Health: current knowledge and future directions". The authors thank the International Commission on Atmospheric Chemistry and Global Pollution (iCACGP), the International Global Atmospheric Chemistry Project (IGAC), the Health Effects Institute (HEI), the World Meteorological Organization (WMO), and the European Commission for providing travel and logistical support to this meeting. J.J.W. was supported by the U.S. National Institute of Environmental Health Sciences, grant #1R21ES022600-01. The National Center for Atmospheric Research is operated by the University Corporation for Atmospheric Research under the sponsorship of the National Science Foundation. The contribution from the National Oceanic and Atmospheric Administration was supported by the NOAA Health of the Atmosphere Initiative. The views expressed here do not necessarily reflect the policy of the U.S. Environmental Protection Agency, European Commission, or sponsoring organizations. We thank five anonymous reviewers for their comments. NR 87 TC 7 Z9 7 U1 24 U2 67 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD MAY 17 PY 2016 VL 50 IS 10 BP 4895 EP 4904 DI 10.1021/acs.est.5b03827 PG 10 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA DM4QJ UT WOS:000376331500002 PM 27010639 ER PT J AU Memiaghe, HR Lutz, JA Korte, L Alonso, A Kenfack, D AF Memiaghe, Herve R. Lutz, James A. Korte, Lisa Alonso, Alfonso Kenfack, David TI Ecological Importance of Small-Diameter Trees to the Structure, Diversity and Biomass of a Tropical Evergreen Forest at Rabi, Gabon SO PLOS ONE LA English DT Article AB Tropical forests have long been recognized for their biodiversity and ecosystem services. Despite their importance, tropical forests, and particularly those of central Africa, remain understudied. Until recently, most forest inventories in Central Africa have focused on trees >= 10 cm in diameter, even though several studies have shown that small-diameter tree population may be important to demographic rates and nutrient cycling. To determine the ecological importance of small-diameter trees in central African forests, we used data from a 25-ha permanent plot that we established in the rainforest of Gabon to study the diversity and dynamics of these forests. Within the plot, we censused 175,830 trees >= 1 cm dbh from 54 families, 192 genera, and 345 species. Average tree density was 7,026 trees/ha, basal area 31.64 m(2)/ha, and above-ground biomass 369.40 Mg/ha. Fabaceae, Ebenaceae and Euphorbiaceae were the most important families by basal area, density and above-ground biomass. Small-diameter trees (1 cm >= dbh <10 cm) comprised 93.7% of the total tree population, 16.5% of basal area, and 4.8% of the above-ground biomass. They also had diversity 18% higher at family level, 34% higher at genus level, and 42% higher at species level than trees >= 10 cm dbh. Although the relative contribution of small-diameter trees to biomass was comparable to other forests globally, their contribution to forest density, and diversity was disproportionately higher. The high levels of diversity within small-diameter classes may give these forests high levels of structural resilience to anthropogenic/natural disturbance and a changing climate. C1 [Memiaghe, Herve R.] IRET, Libreville, Gabon. [Lutz, James A.] Utah State Univ, Wildland Resources Dept, Logan, UT 84322 USA. [Korte, Lisa] Smithsonian Conservat Biol Inst, Ctr Conservat & Sustainabil, Gamba, Gabon. [Alonso, Alfonso] Smithsonian Conservat Biol Inst, Ctr Conservat & Sustainabil, Washington, DC USA. [Kenfack, David] Smithsonian Inst, Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Forest Global Earth Observ, Washington, DC 20560 USA. RP Kenfack, D (reprint author), Smithsonian Inst, Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Forest Global Earth Observ, Washington, DC 20560 USA. EM kenfackd@si.edu FU Shell Gabon; Smithsonian Tropical Research institute through the Forest Global Earth Observatory (ForestGEO); ForestGEO in China, US and Panama FX Shell Gabon provided financial support for field work, especially to HRM and LK. Shell Gabon also provided logistical support including flights, lodging and food to LK, HRM, DK and 14 other field staff. Shell Gabon had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. The Smithsonian Tropical Research institute through the Forest Global Earth Observatory (ForestGEO) provided funding for the salaries of 12 field staff including HRM, and also provided funding to DK for training and technical advice. The Rabi plot was established with the protocols developed by ForestGEO, and DK is African Program Coordinator for ForestGEO. The data was analyzed by HRM, DK and JL during a series of analytical workshops funded by ForestGEO in China, US and Panama. NR 34 TC 0 Z9 0 U1 9 U2 15 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 17 PY 2016 VL 11 IS 5 AR e0154988 DI 10.1371/journal.pone.0154988 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DM3YJ UT WOS:000376282300016 PM 27186658 ER PT J AU Hindson, L Johnston-Hollitt, M Hurley-Walker, N Callingham, JR Su, H Morgan, J Bell, M Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Deshpande, AA Dwarakanath, KS For, BQ Gaensler, BM Greenhill, LJ Hancock, P Hazelton, BJ Kapinska, AD Kaplan, DL Lenc, E Lonsdale, CJ Mckinley, B McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Offringa, A Ord, SM Procopio, P Prabu, T Shankar, NU Srivani, KS Staveley-Smith, L Subrahmanyan, R Tingay, SJ Wayth, RB Webster, RL Williams, A Williams, CL Wu, C Zheng, Q AF Hindson, L. Johnston-Hollitt, M. Hurley-Walker, N. Callingham, J. R. Su, H. Morgan, J. Bell, M. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Deshpande, A. A. Dwarakanath, K. S. For, B. -Q Gaensler, B. M. Greenhill, L. J. Hancock, P. Hazelton, B. J. Kapinska, A. D. Kaplan, D. L. Lenc, E. Lonsdale, C. J. Mckinley, B. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Offringa, A. Ord, S. M. Procopio, P. Prabu, T. Shankar, N. Udaya Srivani, K. S. Staveley-Smith, L. Subrahmanyan, R. Tingay, S. J. Wayth, R. B. Webster, R. L. Williams, A. Williams, C. L. Wu, C. Zheng, Q. TI A Large-Scale, Low-Frequency Murchison Widefield Array Survey of Galactic H II Regions between 260 < l < 340 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE catalogs; (ISM:) HII regions; radio continuum: ISM ID STAR-FORMING COMPLEX; RADIO SPECTRAL INDEX; SUPERNOVA-REMNANTS; PLANE SURVEY; DISCOVERY SURVEY; INFRARED SURVEY; SKY SURVEY; CONTINUUM; CATALOG; ABSORPTION AB We have compiled a catalogue of H II regions detected with the Murchison Widefield Array between 72 and 231 MHz. The multiple frequency bands provided by the Murchison Widefield Array allow us identify the characteristic spectrum generated by the thermal Bremsstrahlung process in H II regions. We detect 306 H II regions between 260 degrees < l < 340 degrees and report on the positions, sizes, peak, integrated flux density, and spectral indices of these H II regions. By identifying the point at which H II regions transition from the optically thin to thick regime, we derive the physical properties including the electron density, ionised gas mass, and ionising photon flux, towards 61 H II regions. This catalogue of H II regions represents the most extensive and uniform low frequency survey of H II regions in the Galaxy to date. C1 [Hindson, L.; Johnston-Hollitt, M.; Lonsdale, C. J.; Zheng, Q.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Hindson, L.] Univ Hertfordshire, Sch Phys Astron & Math, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, Herts, England. [Hurley-Walker, N.; Su, H.; Morgan, J.; Hancock, P.; Ord, S. M.; Tingay, S. J.; Wayth, R. B.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Callingham, J. R.; Gaensler, B. M.; Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Callingham, J. R.; Bell, M.; Gaensler, B. M.; Hancock, P.; Kapinska, A. D.; Lenc, E.; Mckinley, B.; Mitchell, D. A.; Offringa, A.; Ord, S. M.; Procopio, P.; Staveley-Smith, L.; Subrahmanyan, R.; Tingay, S. J.; Wayth, R. B.; Webster, R. L.; Williams, A.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW, Australia. [Callingham, J. R.; Bell, M.; Mitchell, D. A.] CSIRO Astron & Space Sci CASS, POB 76, Epping, NSW 1710, Australia. [Bernardi, G.] Sq Kilometre Array South Africa SKA SA, ZA-7405 Cape Town, South Africa. [Bernardi, G.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.; Mckinley, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, R. J.; Lonsdale, C. J.; McWhirter, S. R.] MIT Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Dwarakanath, K. S.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [For, B. -Q; Kapinska, A. D.; Staveley-Smith, L.; Wu, C.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Gaensler, B. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Mitchell, D. A.; Procopio, P.; Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Offringa, A.] Netherlands Inst Radio Astron ASTRON, POB 2, NL-7990 AA Dwingeloo, Netherlands. RP Hindson, L (reprint author), Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand.; Hindson, L (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, Herts, England. EM lukehindson1@gmail.com RI Kapinska, Anna/B-3999-2014; Wayth, Randall/B-2444-2013; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Subrahmanyan, Ravi/D-4889-2012; Dwarakanath, K /D-4876-2012; Staveley-Smith, Lister/A-1683-2011; OI Kapinska, Anna/0000-0002-5289-5729; Wayth, Randall/0000-0002-6995-4131; Staveley-Smith, Lister/0000-0002-8057-0294; Lenc, Emil/0000-0002-9994-1593; Callingham, Joseph/0000-0002-7167-1819; Hancock, Paul/0000-0002-4203-2946 FU Ministry of Business, Employment & Innovation, New Zealand [MED E1799]; Marsden Fund; NVIDIA at Harvard University FX LH was partially supported in this work via grant MED E1799 (PI: Johnston-Hollitt) provided by the Ministry of Business, Employment & Innovation, New Zealand. MJ-H acknowledges support from the Marsden Fund. 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. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University. The authors thank the referee for their very useful comments that resulted in the improvement of this paper. NR 74 TC 1 Z9 1 U1 2 U2 6 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1323-3580 EI 1448-6083 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PD MAY 17 PY 2016 VL 33 DI 10.1017/pasa.2016.19 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DM9JK UT WOS:000376681900001 ER PT J AU Rodriguez, PA Rodriguez, EJ Norrbom, AL Arevalo, E AF Alexander Rodriguez, Pedro Rodriguez, Erick J. Norrbom, Allen L. Arevalo, Emilio TI A new species and new records of Cryptodacus (Diptera: Tephritidae) from Colombia, Bolivia and Peru SO ZOOTAXA LA English DT Article DE Neotropical; fruit flies; new host plant; new distribution records AB Cryptodacus bernardoi Rodriguez & Rodriguez, new species, is described from Colombia. It was reared from fruits of Phoradendron sp. near piperoides (Kunth) Trel. New distribution records are reported for Cryptodacus ornatus Norrbom from Colombia and Peru, for Cryptodacus trinotatus Norrbom & Korytkowski from Colombia, and for Cryptodacus obliquus Hendel from Bolivia and Peru. The female abdomen and terminalia of C. obliquus is described for the first time. The Norrbom & Korytkowski (2008)'s key to species was modified to include C. bernardoi n. sp. C1 [Alexander Rodriguez, Pedro] ICA, Lab Moscas Fruta, CI Tibaitata Km 14 Via, Bogota, Colombia. [Rodriguez, Erick J.] Florida Dept Agr & Consumer Serv, Div Plant Ind Entomol, Gainesville, FL USA. [Norrbom, Allen L.] ARS, USDA, Smithsonian Inst, Systemat Entomol Lab, POB 37012,MRC 168, Washington, DC 20013 USA. [Arevalo, Emilio] PNMF, ICA, Direcc Tecn Epidemiol & Vigilancia Fitosanitaria, Cra 41 17-81 Zona Ind Puente Aranda, Bogota, Colombia. RP Rodriguez, PA (reprint author), ICA, Lab Moscas Fruta, CI Tibaitata Km 14 Via, Bogota, Colombia.; Rodriguez, EJ (reprint author), Florida Dept Agr & Consumer Serv, Div Plant Ind Entomol, Gainesville, FL USA.; Norrbom, AL (reprint author), ARS, USDA, Smithsonian Inst, Systemat Entomol Lab, POB 37012,MRC 168, Washington, DC 20013 USA.; Arevalo, E (reprint author), PNMF, ICA, Direcc Tecn Epidemiol & Vigilancia Fitosanitaria, Cra 41 17-81 Zona Ind Puente Aranda, Bogota, Colombia. EM pedro.rodriguez@ica.gov.co; erick.rodriguez@freshfromflorida.com; allen.norrbom@ars.usda.gov; emilio.arevalo@ica.gov.co NR 6 TC 0 Z9 0 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 16 PY 2016 VL 4111 IS 3 BP 276 EP 290 PG 15 WC Zoology SC Zoology GA DL9AQ UT WOS:000375934000005 PM 27395090 ER PT J AU Mitko, L Weber, MG Ramirez, SR Hedenstrom, E Wcislo, WT Eltz, T AF Mitko, Lukasz Weber, Marjorie G. Ramirez, Santiago R. Hedenstrom, Erik Wcislo, William T. Eltz, Thomas TI Olfactory specialization for perfume collection in male orchid bees SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE Euglossini; EAG; Olfaction; Olfactory specialization; Fragrance; Pheromone ID MALE EUGLOSSINE BEES; SEX-PHEROMONES; ATTRACTION; FRAGRANCES; EVOLUTION; RESPONSES; CHOICES; DIFFERENTIATION; COMMUNICATION; ACCUMULATION AB Insects rely on the olfactory system to detect a vast diversity of airborne molecules in their environment. Highly sensitive olfactory tuning is expected to evolve when detection of a particular chemical with great precision is required in the context of foraging and/or finding mates. Male neotropical orchid bees (Euglossini) collect odoriferous substances from multiple sources, store them in specialized tibial pouches and later expose them at display sites, presumably as mating signals to females. Previous analysis of tibial compounds among sympatric species revealed substantial chemical disparity in chemical composition among lineages with outstanding divergence between closely related species. Here, we tested whether specific perfume phenotypes coevolve with matching olfactory adaptations in male orchid bees to facilitate the location and harvest of species-specific perfume compounds. We conducted electroantennographic (EAG) measurements on males of 15 sympatric species in the genus Euglossa that were stimulated with 18 compounds present in variable proportions in male hind tibiae. Antennal response profiles were species-specific across all 15 species, but there was no conspicuous differentiation between closely related species. Instead, we found that the observed variation in EAG activity follows a Brownian motion model of trait evolution, where the probability of differentiation increases proportionally with lineage divergence time. However, we identified strong antennal responses for some chemicals that are present as major compounds in the perfume of the same species, thus suggesting that sensory specialization has occurred within multiple lineages. This sensory specialization was particularly apparent for semi-volatile molecules ('base note' compounds), thus supporting the idea that such compounds play an important role in chemical signaling of euglossine bees. Overall, our study found no close correspondence between antennal responses and behavioral preferences/tibial contents, but confirms the utility of EAG profiling for discovering certain behaviorally active compounds. C1 [Mitko, Lukasz; Eltz, Thomas] Ruhr Univ Bochum, Dept Anim Ecol Evolut & Biodivers, D-44780 Bochum, Germany. [Weber, Marjorie G.] Univ Calif Davis, Ctr Populat Biol, Davis, CA 95616 USA. [Ramirez, Santiago R.] Univ Calif Davis, Dept Ecol & Evolut, Davis, CA 95616 USA. [Hedenstrom, Erik] Mid Sweden Univ, Chem, Dept Nat Sci Engn & Math, SE-85170 Sundsvall, Sweden. [Wcislo, William T.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. RP Eltz, T (reprint author), Ruhr Univ Bochum, Dept Anim Ecol Evolut & Biodivers, D-44780 Bochum, Germany. EM thomas.eltz@ruhr-uni-bochum.de FU Deutsche Forschungsgemeinschaft (German Science Foundation) [EL 249/6]; David and Lucile Packard Foundation; National Science Foundation [DEB- 1457753] FX T.E. received funding from the Deutsche Forschungsgemeinschaft (German Science Foundation) [EL 249/6]; and S.R.R. received support from the David and Lucile Packard Foundation and the National Science Foundation [DEB- 1457753]. NR 57 TC 1 Z9 1 U1 9 U2 12 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 MAY 15 PY 2016 VL 219 IS 10 BP 1467 EP 1475 DI 10.1242/jeb.136754 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA DM1PM UT WOS:000376118500012 PM 27207952 ER PT J AU Bodony, DJ Day, L Friscia, AR Fusani, L Karon, A Swenson, GW Wikelski, M Schlinger, BA AF Bodony, Daniel J. Day, Lainy Friscia, Anthony R. Fusani, Leonida Karon, Aharon Swenson, George W., Jr. Wikelski, Martin Schlinger, Barney A. TI Determination of the wingsnap sonation mechanism of the golden-collared manakin (Manacus vitellinus) SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE Sonation; Manakin; Aeroacoustics ID SPEED VIDEO ANALYSIS; COURTING BIRD; COURTSHIP; FLIGHT; DISPLAY; SOUND; CLAP; SELECTION; PIPRIDAE; FEATHERS AB Male golden-collared manakins (Manacus vitellinus), small suboscine passeriform birds of Panamanian forests, communicate acoustically using a variety of non-vocal sonations. The most prominent sonations are single or multiple intense 'wingsnaps' with a dominant acoustic frequency around 5 kHz. Several hypotheses have been proposed addressing the source of the sound, ranging from purely aerodynamic origins (due to a rapid jet of air formed by the wings or by a 'whiplike' motion) to purely structural origins (such as physical contact of the wings), but without definitive assessment. Using anatomical analysis as well as high-speed video and synchronized audio recordings, we show that compared with related species, M. vitellinus radii are morphologically unique and confirm that they collide over the back of the bird at the moment (+/- 1 ms) the wingsnap is produced. Using aeroacoustic theory, we quantitatively estimate the acoustic signatures from several sonation mechanisms. We conclude that only the physical contact hypothesis, wherein the wing collisions create the sound, is consistent with the measured sonation. C1 [Bodony, Daniel J.] Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA. [Day, Lainy] Univ Mississippi, Dept Biol, University, MS 38677 USA. [Friscia, Anthony R.; Schlinger, Barney A.] Univ Calif Los Angeles, Dept Integrat Biol & Physiol, Los Angeles, CA 90095 USA. [Fusani, Leonida] Univ Vienna, Dept Cognit Biol, UZA 1,Biol Zentrum Althanstr 14, A-1090 Vienna, Austria. [Karon, Aharon] Univ Vienna, Dept Cognit Biol, UZA 1,Biol Zentrum Althanstr 14, A-1090 Vienna, Austria. [Karon, Aharon] Univ Vet Med, Konrad Lorenz Inst Ethol, Savoyenstr 1a, A-1160 Vienna, Austria. [Swenson, George W., Jr.] Univ Illinois, Dept Elect & Comp Engn, Urbana, IL 61801 USA. [Wikelski, Martin] Max Planck Inst Ornithol, Vogelwarte Radolfzell, Obstberg 1, D-78315 Radoflzell, Germany. [Wikelski, Martin] Univ Konstanz, Dept Biol, Postfach M633, D-78457 Constance, Germany. [Schlinger, Barney A.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Schlinger, Barney A.] Smithsonian Trop Res Inst, Roosevelt Ave,Tupper Bldg 401, Panama City 084303092, Panama. RP Bodony, DJ (reprint author), Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA. EM bodony@illinois.edu FU National Science Foundation [EK41, IBN0213194]; Max-Planck Society; University of Mississippi Office of Sponsored Research; National Science Foundation Research Experience for Undergraduates program [EK44] FX This work was supported by the National Science Foundation [EK41] (IBN0213194, B.A.S.), the Max-Planck Society (M.W.) and by the University of Mississippi Office of Sponsored Research (L.D.). D.J.B. and A.K. also acknowledge the financial support of the National Science Foundation [EK44] Research Experience for Undergraduates program. NR 43 TC 2 Z9 2 U1 7 U2 10 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 MAY 15 PY 2016 VL 219 IS 10 BP 1524 EP 1534 DI 10.1242/jeb.128231 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA DM1PM UT WOS:000376118500018 PM 26994170 ER PT J AU Lopez-Angarita, J Roberts, CM Tilley, A Hawkins, JP Cooke, RG AF Lopez-Angarita, Juliana Roberts, Callum M. Tilley, Alexander Hawkins, Julie P. Cooke, Richard G. TI Mangroves and people: Lessons from a history of use and abuse in four Latin American countries SO FOREST ECOLOGY AND MANAGEMENT LA English DT Review DE Archaeozoology; Protected area; Conservation; Management; Eastern Tropical Pacific; Historical ecology ID MARINE PROTECTED AREAS; SHRIMP AQUACULTURE; COASTAL; PANAMA; FORESTS; ECOSYSTEMS; MANAGEMENT; PACIFIC; WORLD; DYNAMICS AB From native pre-Columbian subsistence economies to the modern global economy, mangroves have played an important role providing goods and services to human societies for millennia. More than 90% of the world's mangroves are located in developing countries, where rates of destruction are increasing rapidly and on large scales. In order to design effective conservation strategies, it is critical to understand the natural dynamics and anthropogenic drivers of these coastal wetland habitats. We use retrospective techniques to reconstruct mangrove forest history in the Eastern Tropical Pacific. We examine available, present day estimates of mangrove area and evaluate the representation of mangroves in the protected area systems of Costa Rica, Panama, Colombia and Ecuador, evaluating existing policies regarding mangroves. Archaeozoological evidence shows that mangroves were exploited for many thousands of years by pre-Columbian societies. Post-conquest deforestation prevailed during the next 400 years. Since 1990, despite increasingly positive attitudes towards mangroves and their inclusion in protected areas and conservation policies, mangrove cover has continued to decline due to expanding human activities (agriculture, aquaculture, coastal development), even in the presence of laws prohibiting their removal. Here we provide an historical ecology baseline of mangroves in the Eastern Tropical Pacific, from which to view current trends and map future trajectories. Given the myriad negative consequences of mangrove loss recorded worldwide, and the strong ecological connectivity of the region, developing effective strategies for mangrove management at an appropriate scale will be paramount to protect coastal livelihoods and biodiversity. (C) 2016 Elsevier B.V. All rights reserved. C1 [Lopez-Angarita, Juliana; Roberts, Callum M.; Hawkins, Julie P.] Univ York, Dept Environm, York YO10 5DD, N Yorkshire, England. [Lopez-Angarita, Juliana; Tilley, Alexander] Fdn Talking Oceans, Carrera 16 127-81, Bogota, Colombia. [Lopez-Angarita, Juliana; Cooke, Richard G.] Smithsonian Trop Res Inst, Panama City, Panama. RP Lopez-Angarita, J (reprint author), Carrera 16 127-81, Bogota, Colombia. EM julianalop14@gmail.com FU Colombian Department of Science and Technology (COLCIENCIAS); Schlumberger Foundation; World Wildlife Fund's Russell E. Train Education for Nature program; Smithsonian Tropical Research Institute; Save our Seas Foundation FX This research was funded by fellowships (J. Lopez Angarita) from the Colombian Department of Science and Technology (COLCIENCIAS), the Schlumberger Foundation Faculty for the Future Programme, the World Wildlife Fund's Russell E. Train Education for Nature program, the Smithsonian Tropical Research Institute, and Save our Seas Foundation. We thank Dr A. Altieri for insights on an early manuscript. This work is dedicated to the memory of the Colombian botanist and historian Santiago Diaz Piedrahita (1944-2014), who shared his extensive knowledge and passion about Spanish conquest chronicles and botany, and provided active insight to this research. Our thanks to Axios Review, and to two anonymous reviewers for their comments. NR 84 TC 1 Z9 1 U1 32 U2 54 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 EI 1872-7042 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD MAY 15 PY 2016 VL 368 BP 151 EP 162 DI 10.1016/j.foreco.2016.03.020 PG 12 WC Forestry SC Forestry GA DK8FE UT WOS:000375161800017 ER PT J AU Oceguera-Figueroa, A Manzano-Marin, A Kvist, S Moya, A Siddall, ME Latorre, A AF Oceguera-Figueroa, Alejandro Manzano-Marin, Alejandro Kvist, Sebastian Moya, Andres Siddall, Mark E. Latorre, Amparo TI Comparative Mitogenomics of Leeches (Annelida: Clitellata): Genome Conservation and Placobdella-Specific trnD Gene Duplication SO PLOS ONE LA English DT Article ID COMPLETE MITOCHONDRIAL GENOME; RNA PUNCTUATION MODEL; FAMILY GLOSSIPHONIIDAE; PHYLOGENETIC ANALYSES; MOLECULAR PHYLOGENY; SEQUENCE; EVOLUTION; ORDER; DNA; INFORMATION AB Mitochondrial DNA sequences, often in combination with nuclear markers and morphological data, are frequently used to unravel the phylogenetic relationships, population dynamics and biogeographic histories of a plethora of organisms. The information provided by examining complete mitochondrial genomes also enables investigation of other evolutionary events such as gene rearrangements, gene duplication and gene loss. Despite efforts to generate information to represent most of the currently recognized groups, some taxa are underrepresented in mitochondrial genomic databases. One such group is leeches (Annelida: Hirudinea: Clitellata). Herein, we expand our knowledge concerning leech mitochondrial makeup including gene arrangement, gene duplication and the evolution of mitochondrial genomes by adding newly sequenced mitochondrial genomes for three bloodfeeding species: Haementeria officinalis, Placobdella lamothei and Placobdella parasitica. With the inclusion of three new mitochondrial genomes of leeches, a better understanding of evolution for this organelle within the group is emerging. We found that gene order and genomic arrangement in the three new mitochondrial genomes is identical to previously sequenced members of Clitellata. Interestingly, within Placobdella, we recovered a genus-specific duplication of the trnD gene located between cox2 and atp8. We performed phylogenetic analyses using 12 protein-coding genes and expanded our taxon sampling by including GenBank sequences for 39 taxa; the analyses confirm the monophyletic status of Clitellata, yet disagree in several respects with other phylogenetic hypotheses based on morphology and analyses of non-mitochondrial data. C1 [Oceguera-Figueroa, Alejandro] Univ Nacl Autonoma Mexico, Inst Biol, Dept Zool, Lab Helmintol, Mexico City 04510, DF, Mexico. [Oceguera-Figueroa, Alejandro] Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. [Manzano-Marin, Alejandro; Moya, Andres; Latorre, Amparo] Univ Valencia, Inst Cavanilles Biodiversitat & Biol Evolut, Catedrat Jose Beltran 2, Valencia 46008, Spain. [Kvist, Sebastian] Royal Ontario Museum, Dept Nat Hist, 100 Queens Pk, Toronto, ON M5S 2C6, Canada. [Kvist, Sebastian] Univ Toronto, Dept Ecol & Evolutionary Biol, 25 Willcocks St, Toronto, ON M5S 3B2, Canada. [Moya, Andres; Latorre, Amparo] Fdn Fomento Invest Sanitaria & Biomed Comunidad V, Area Genom & Salud, Ave Catalunya 21, Valencia 46020, Spain. [Siddall, Mark E.] Amer Museum Nat Hist, Sackler Inst Comparat Genom, Cent Pk West & 79th St, New York, NY 10024 USA. RP Oceguera-Figueroa, A (reprint author), Univ Nacl Autonoma Mexico, Inst Biol, Dept Zool, Lab Helmintol, Mexico City 04510, DF, Mexico.; Oceguera-Figueroa, A (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. EM aoceguera@ib.unam.mx RI Manzano-Marin, Alejandro/J-9922-2015 OI Manzano-Marin, Alejandro/0000-0002-0707-9052 FU Programa de Apoyo a Proyectos de Investigacion e Innovacion Tecnologica - Universidad Nacional Autonoma de Mexico [IA204114]; European Commission [264774]; Consejo Nacional de Ciencia y Tecnologia - Mexico [CONACYT 327211/381508]; Royal Ontario Museum Schad Gallery of Biodiversity Research Fund; Olle Engkvist Byggmastare Foundation; NSERC [RGPIN-2016-06125]; FEDER funds [BFU2012-39816-C02-01]; Ministerio de Economia y Competitividad, Spain [BFU2012-39816-C02-01]; Conselleria d'Educacio, Generalitat Valenciana, Spain [PrometeoII/2014/065] FX This work was supported by Consejo Nacional de Ciencia y Tecnologia - Mexico, Posdoctoral grant (http://www.conacyt.gob.mx/) and Programa de Apoyo a Proyectos de Investigacion e Innovacion Tecnologica - Universidad Nacional Autonoma de Mexico Project IA204114 (http://dgapa.unam.mx/html/papiit/papit.html) to AOF; European Commission (Marie Curie FP7-PEOPLE-2010-ITN SYMBIOMICS 264774) Ph. D. grant (https://ec.europa.eu/research/participants/portal/desktop/en/opportunit ies/fp7/calls/fp7-people-2013-ief.html) and Consejo Nacional de Ciencia y Tecnologia - Mexico, Ph. D. grant CONACYT 327211/381508 (http://www.conacyt.gob.mx/) to AMM; Royal Ontario Museum Schad Gallery of Biodiversity Research Fund, Olle Engkvist Byggmastare Foundation and NSERC Discovery Grant (RGPIN-2016-06125) (http://www.nserc-crsng.gc.ca) to SK; Grants BFU2012-39816-C02-01 (co-financed by FEDER funds and Ministerio de Economia y Competitividad, Spain) (www.mineco.gob.es/) to AL; and Grant PrometeoII/2014/065 (Conselleria d'Educacio, Generalitat Valenciana, Spain) (http://www.cece.gva.es/es/) to AM. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 78 TC 1 Z9 1 U1 1 U2 3 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 13 PY 2016 VL 11 IS 5 AR e0155441 DI 10.1371/journal.pone.0155441 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DM8CX UT WOS:000376589400016 PM 27176910 ER PT J AU Rodriguez-Brenes, S Rodriguez, D Ibanez, R Ryan, MJ AF Rodriguez-Brenes, Sofia Rodriguez, David Ibanez, Roberto Ryan, Michael J. TI Spread of Amphibian Chytrid Fungus across Lowland Populations of Tungara Frogs in Panama SO PLOS ONE LA English DT Article ID BATRACHOCHYTRIUM-DENDROBATIDIS; PHYSALAEMUS-PUSTULOSUS; INFECTIOUS-DISEASE; PCR ASSAY; CHYTRIDIOMYCOSIS; DECLINES; EXTINCTION; DYNAMICS; TIME AB Chytridiomycosis, caused by the fungal pathogen Batrachochytrium dendrobatidis (Bd), is an emergent infectious disease partially responsible for worldwide amphibian population declines. The spread of Bd along highland habitats (>500 meters above sea level, m a.s.l.) of Costa Rica and Panama is well documented and has been linked to amphibian population collapses. In contrast, data are scarce on the prevalence and dispersal of Bd in lowland habitats where amphibians may be infected but asymptomatic. Here we describe the spread (2009 to 2014) of Bd across lowland habitats east of the Panama Canal (<500 m a.s.l.) with a focus on the Tungara frog (Physalaemus [Engystomops] pustulosus), one of the most common and abundant frog species in this region. Highland populations in western Panama were already infected with Bd at the start of the study, which was consistent with previous studies indicating that Bd is enzootic in this region. In central Panama, we collected the first positive samples in 2010, and by 2014, we detected Bd from remote sites in eastern Panama (Darien National Park). We discuss the importance of studying Bd in lowland species, which may serve as potential reservoirs and agents of dispersal of Bd to highland species that are more susceptible to chytridiomycosis. C1 [Rodriguez-Brenes, Sofia; Ryan, Michael J.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. [Rodriguez, David] Texas State Univ, Dept Biol, San Marcos, TX USA. [Ibanez, Roberto] Smithsonian Trop Res Inst, Balboa, Panama. [Ibanez, Roberto] Univ Panama, Dept Zool, Panama City, Panama. RP Rodriguez-Brenes, S (reprint author), Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. EM sofiarb@utexas.edu FU National Science Foundation [IBN 0517328] FX This work was funded by National Science Foundation (http://www.nsf.gov/), IBN 0517328 to MJR. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 29 TC 1 Z9 1 U1 14 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 MAY 13 PY 2016 VL 11 IS 5 AR e0155745 DI 10.1371/journal.pone.0155745 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DM8CX UT WOS:000376589400051 PM 27176629 ER PT J AU Coppard, SE AF Coppard, Simon E. TI A new genus of mellitid sand dollar (Echinoidea: Mellitidae) from the eastern Pacific coast of the Americas SO ZOOTAXA LA English DT Article DE Lanthonia gen. nov.; Mellita; L. longifissa; L. grantii; bidentate pedicellariae ID LUNULE FUNCTION; QUINQUIESPERFORATA; ECHINODERMATA; DIVERGENCE; TURNOVER; ISTHMUS; PANAMA AB Lanthonia gen. nov. Coppard 2016 is a genus of clypeasteroid sand dollar whose members inhabit shallow, sandy waters from Mexico (including the Gulf of California) to Colombia in the tropical and subtropical eastern Pacific. Lanthonia includes Lanthonia longifissa (Michelin, 1858) and Lanthonia grantii (Mortensen, 1948), with L. longifissa hereby designated as the type species. Both L. longifissa and L. grantii were previously placed in the genus Mellita (L. Agassiz, 1841). However, levels of genetic divergence between a lineage containing L. longifissa and L. grantii and a lineage containing all other species of Mellita, including the type species M. quinquiesperforata (Leske, 1778), indicate genus level differentiation. The systematic interpretation of this group also supports the designation of this new genus as it allows the tree topology to be recovered from the nomenclature and clarifies the historical biogeography of these clades. This has resulted in members of both lineages today being sympatric in the eastern Pacific. Members of Lanthonia are morphologically differentiated from the type species of Mellita and all Pacific Mellita in having very narrow ambulacral regions between the food grooves and the ambulacral lunules on the oral surface, these being very broad in both M. quinquiesperforata and M. notabilis. The dentation of the bidentate pedicellariae also differentiate these genera, with small peripheral teeth present along the edge of the blade in species of Lanthonia and one to three enlarged intersecting teeth present distally in all species of Mellita. C1 [Coppard, Simon E.] Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Panama. [Coppard, Simon E.] Hamilton Coll, Dept Biol, 198 Coll Hill Rd, Clinton, NY 13323 USA. RP Coppard, SE (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Panama.; Coppard, SE (reprint author), Hamilton Coll, Dept Biol, 198 Coll Hill Rd, Clinton, NY 13323 USA. EM coppardse@gmail.com FU SENACYT (La Secretaria Nacional de Ciencia Tecnologia e Innovacion) (Panama) [COL08-002] FX I am grateful to H.A. Lessios and J. Ceballos for their support at STRI. I thank R. Mooi and an anonymous reviewer for their comments, which improved the manuscript. This study was funded by a fellowship to SEC from SENACYT (La Secretaria Nacional de Ciencia Tecnologia e Innovacion) (Panama) as part of project COL08-002. NR 28 TC 0 Z9 0 U1 2 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 MAY 13 PY 2016 VL 4111 IS 2 BP 158 EP 166 PG 9 WC Zoology SC Zoology GA DL9AP UT WOS:000375933900004 PM 27394905 ER PT J AU Wikelski, M Tertitski, G AF Wikelski, Martin Tertitski, Grigori TI Living sentinels for climate change effects SO SCIENCE LA English DT Editorial Material ID TRACKING; ECOLOGY; HAWKS C1 [Wikelski, Martin] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Germany. [Wikelski, Martin] Univ Konstanz, Dept Biol, Constance, Germany. [Wikelski, Martin] Smithsonian Trop Res Inst, Balboa, Panama. [Tertitski, Grigori] Russian Acad Sci, Inst Geog, Moscow V71, Russia. RP Wikelski, M (reprint author), Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Germany.; Wikelski, M (reprint author), Univ Konstanz, Dept Biol, Constance, Germany.; Wikelski, M (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM wikelski@orn.mpg.de NR 14 TC 2 Z9 2 U1 13 U2 23 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAY 13 PY 2016 VL 352 IS 6287 BP 775 EP 776 DI 10.1126/science.aaf6544 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DL5FP UT WOS:000375663000022 PM 27174976 ER PT J AU Roettenbacher, RM Monnier, JD Korhonen, H Aarnio, AN Baron, F Che, X Harmon, RO Kovari, Z Kraus, S Schaefer, GH Torres, G Zhao, M ten Brummelaar, TA Sturmann, J Sturmann, L AF Roettenbacher, R. M. Monnier, J. D. Korhonen, H. Aarnio, A. N. Baron, F. Che, X. Harmon, R. O. Kovari, Zs. Kraus, S. Schaefer, G. H. Torres, G. Zhao, M. ten Brummelaar, T. A. Sturmann, J. Sturmann, L. TI No Sun-like dynamo on the active star zeta Andromedae from starspot asymmetry SO NATURE LA English DT Article ID LOW-MASS STARS; BROWN DWARFS; LIGHT-CURVE; CHARA ARRAY; INTERFEROMETRY; SURFACE; SPOTS; CONTROVERSY; EVOLUTION; RADII AB Sunspots are cool areas caused by strong surface magnetic fields that inhibit convection(1,2). Moreover, strong magnetic fields can alter the average atmospheric structure(3), degrading our ability to measure stellar masses and ages. Stars that are more active than the Sun have more and stronger dark spots than does the Sun, including on the rotational pole(4). Doppler imaging, which has so far produced the most detailed images of surface structures on other stars, cannot always distinguish the hemisphere in which the starspots are located, especially in the equatorial region and if the data quality is not optimal(5). This leads to problems in investigating the north-south distribution of starspot active latitudes (those latitudes with more starspot activity); this distribution is a crucial constraint of dynamo theory. Polar spots, whose existence is inferred from Doppler tomography, could plausibly be observational artefacts(6). Here we report imaging of the old, magnetically active star zeta Andromedae using long-baseline infrared interferometry. In our data, a dark polar spot is seen in each of two observation epochs, whereas lower-latitude spot structures in both hemispheres do not persist between observations, revealing global starspot asymmetries. The north-south symmetry of active latitudes observed on the Sun(7) is absent on zeta And, which hosts global spot patterns that cannot be produced by solar-type dynamos(8). C1 [Roettenbacher, R. M.; Monnier, J. D.; Aarnio, A. N.; Baron, F.; Che, X.; Kraus, S.; Zhao, M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Korhonen, H.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Korhonen, H.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Baron, F.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Harmon, R. O.] Ohio Wesleyan Univ, Dept Phys & Astron, Delaware, OH USA. [Kovari, Zs.] Hungarian Acad Sci, Konkoly Observ, Res Ctr Astron & Earth Sci, H-1121 Budapest, Hungary. [Kraus, S.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Schaefer, G. H.; ten Brummelaar, T. A.; Sturmann, J.; Sturmann, L.] Georgia State Univ, Ctr High Angular Resolut Astron, Mt Wilson, CA 91023 USA. [Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zhao, M.] Penn State Univ, Dept Astron & Astrophys, State Coll, PA 16802 USA. RP Roettenbacher, RM (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. EM rmroett@umich.edu RI Korhonen, Heidi/E-3065-2016; Kovari, Zsolt/A-9098-2012 OI Korhonen, Heidi/0000-0003-0529-1161; Kovari, Zsolt/0000-0001-5160-307X FU National Science Foundation [AST-1211929, AST-1411654]; University of Michigan; National Science Foundation (NSF) [AST-1108963]; Hungarian Scientific Research Fund [OTKA K-109276]; Hungarian Academy of Sciences; STFC [ST/J004030/1, ST/K003445/1]; ERC [639889] FX We thank E. Pedretti for his early efforts in imaging. And. This work is based upon observations obtained with the Georgia State University Center for the High Angular Resolution Astronomy Array at Mount Wilson Observatory. The CHARA Array is supported by the National Science Foundation under grant numbers AST-1211929 and AST-1411654. Institutional support has been provided from the GSU College of Arts and Sciences and the GSU Office of the Vice President for Research and Economic Development. The MIRC instrument at the CHARA Array was funded by the University of Michigan. The 2013 CHARA/MIRC observations were supported by a Rackham Graduate Student Research Grant from the University of Michigan. This imaging work was supported by the National Science Foundation (NSF) grant AST-1108963. The SURFING software was developed in part with funding from the Observatoire de Paris, Meudon. This research made use of the SIMBAD database, operated at CDS, Strasbourg, France and the Jean-Marie Mariotti Center SearchCal and Aspro2 services co-developed by FIZEAU and LAOG/IPAG. This work was supported by the Hungarian Scientific Research Fund (OTKA K-109276), the 'Lendulet-2009' Young Researchers' programme of the Hungarian Academy of Sciences, an STFC Rutherford Fellowship and Grant (ST/J004030/1, ST/K003445/1), and an ERC Starting Grant (grant agreement number 639889). NR 42 TC 5 Z9 5 U1 2 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAY 12 PY 2016 VL 533 IS 7602 BP 217 EP + DI 10.1038/nature17444 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DM0BJ UT WOS:000376007200043 PM 27144357 ER PT J AU Bloch, JI Woodruff, ED Wood, AR Rincon, AF Harrington, AR Morgan, GS Foster, DA Montes, C Jaramillo, CA Jud, NA Jones, DS MacFadden, BJ AF Bloch, Jonathan I. Woodruff, Emily D. Wood, Aaron R. Rincon, Aldo F. Harrington, Arianna R. Morgan, Gary S. Foster, David A. Montes, Camilo Jaramillo, Carlos A. Jud, Nathan A. Jones, Douglas S. MacFadden, Bruce J. TI First North American fossil monkey and early Miocene tropical biotic interchange SO NATURE LA English DT Article ID SOUTH-AMERICA; MIDDLE EOCENE; PANAMA; ISTHMUS; ORIGINS; PLATYRRHINES; BIOGEOGRAPHY; CALIBRATION; CHRONOLOGY; EMERGENCE AB New World monkeys (platyrrhines) are a diverse part of modern tropical ecosystems in North and South America, yet their early evolutionary history in the tropics is largely unknown. Molecular divergence estimates suggest that primates arrived in tropical Central America, the southern-most extent of the North American landmass, with several dispersals from South America starting with the emergence of the Isthmus of Panama 3-4 million years ago (Ma)(1). The complete absence of primate fossils from Central America has, however, limited our understanding of their history in the New World. Here we present the first description of a fossil monkey recovered from the North American landmass, the oldest known crown platyrrhine, from a precisely dated 20.9-Ma layer in the Las Cascadas Formation in the Panama Canal Basin, Panama. This discovery suggests that family-level diversification of extant New World monkeys occurred in the tropics, with new divergence estimates for Cebidae between 22 and 25 Ma, and provides the oldest fossil evidence for mammalian interchange between South and North America. The timing is consistent with recent tectonic reconstructions(2,3) of a relatively narrow Central American Seaway in the early Miocene epoch, coincident with over-water dispersals inferred for many other groups of animals and plants(4). Discovery of an early Miocene primate in Panama provides evidence for a circum-Caribbean tropical distribution of New World monkeys by this time, with ocean barriers not wholly restricting their northward movements, requiring a complex set of ecological factors to explain their absence in well-sampled similarly aged localities at higher latitudes of North America. C1 [Bloch, Jonathan I.; Woodruff, Emily D.; Wood, Aaron R.; Rincon, Aldo F.; Harrington, Arianna R.; Jud, Nathan A.; Jones, Douglas S.; MacFadden, Bruce J.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Woodruff, Emily D.; Harrington, Arianna R.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Wood, Aaron R.] Iowa State Univ, Dept Geol & Atmospher Sci, Ames, IA 50011 USA. [Rincon, Aldo F.; Foster, David A.] Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA. [Harrington, Arianna R.] Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27708 USA. [Morgan, Gary S.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. [Montes, Camilo] Univ Los Andes, Geociencias, Calle 1A 18A-10,Edificio IP, Bogota 111711, Colombia. [Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Ancon, Panama. RP Bloch, JI (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM jbloch@flmnh.ufl.edu OI Bloch, Jonathan/0000-0003-1484-6931; Montes, Camilo/0000-0002-3553-0787 FU National Science Foundation (NSF) [BCS 1304045, BCS 0851272]; Edward P. Bass Distinguished Visiting Environmental Scholar in the Yale Institute for Biospheric Studies (YIBS); NSF (PIRE project) [0966884]; Smithsonian Tropical Research Institute Paleobiology Fund; Florida Museum of Natural History FX We thank M. Silcox, D. Boyer, G. Gunnell, S. Chester, P. Morse, E. Sargis, D. Steadman, E. Kowalski, Z. Randall, A. Rosenberger, J. Krigbaum and D. Daegling for advice and discussion, R. Kay and L. Marivaux for reviews that significantly improved the quality of the manuscript, D. Byerley and G. Maccracken for finding primate fossils in Panama, M. Droulliard for assistance with geochronology laboratory and fieldwork, R. Kay, P. Holroyd and D. Reed for access to comparative specimens, J. Bourque for fossil preparation, D. Byerley for artwork associated with Fig. 3, D. Boyer for facilitating access to the Duke University SMIF microCT facility, and D. Boyer, G. Yapuncich and J. Thostenson for help acquiring and processing microCT scan data (funded in part by National Science Foundation (NSF) BCS 1304045 to D. Boyer and E. St Clair, and BCS 0851272 to R. Kay). We thank O. Moskalenko, M. Gitzendanner and D. Reed for assistance with the high-performance computing resources at the University of Florida. We thank the Autoridad del Canal de Panama (ACP) and the Ministerio de Comercio e Industria (MICI) for logistical support and access to the Panama Canal Zone. Part of this manuscript was written when J.I.B. was supported as an Edward P. Bass Distinguished Visiting Environmental Scholar in the Yale Institute for Biospheric Studies (YIBS). The NSF (PIRE project 0966884), Smithsonian Tropical Research Institute Paleobiology Fund, and the Florida Museum of Natural History funded this research. This is University of Florida Contribution to Paleobiology 782. NR 30 TC 9 Z9 9 U1 14 U2 19 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAY 12 PY 2016 VL 533 IS 7602 BP 243 EP + DI 10.1038/nature17415 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DM0BJ UT WOS:000376007200049 PM 27096364 ER PT J AU Liao, JB Ying, ZX Woolnough, DA Miller, AD Li, ZQ Nijs, I AF Liao, Jinbao Ying, Zhixia Woolnough, Daelyn A. Miller, Adam D. Li, Zhenqing Nijs, Ivan TI Coexistence of species with different dispersal across landscapes: a critical role of spatial correlation in disturbance SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE colonization-competition trade-off; pair approximation; spatially correlated disturbance; species dispersal ID DISTANCE SEED DISPERSAL; STRUCTURED HETEROGENEITIES; FRAGMENTED LANDSCAPES; HABITAT FRAGMENTATION; EXTINCTION THRESHOLDS; POPULATION-DYNAMICS; PAIR APPROXIMATION; DIVERSITY; MODEL; BIODIVERSITY AB Disturbance is key to maintaining species diversity in plant communities. Although the effects of disturbance frequency and extent on species diversity have been studied, we do not yet have a mechanistic understanding of how these aspects of disturbance interact with spatial structure of disturbance to influence species diversity. Here we derive a novel pair approximation model to explore competitive outcomes in a two-species system subject to spatially correlated disturbance. Generally, spatial correlation in disturbance favoured long-range dispersers, while distance-limited dispersers were greatly suppressed. Interestingly, high levels of spatial aggregation of disturbance promoted long-term species coexistence that is not possible in the absence of disturbance, but only when the local disperser was intrinsically competitively superior. However, spatial correlation in disturbance led to different competitive outcomes, depending on the disturbed area. Concerning ecological conservation and management, we theoretically demonstrate that introducing a spatially correlated disturbance to the system or altering an existing disturbance regime can be a useful strategy either to control species invasion or to promote species coexistence. Disturbance pattern analysis may therefore provide new insights into biodiversity conservation. C1 [Liao, Jinbao; Ying, Zhixia; Li, Zhenqing] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing 100093, Peoples R China. [Liao, Jinbao; Ying, Zhixia] Univ Chinese Acad Sci, Beijing 100049, Peoples R China. [Woolnough, Daelyn A.] Cent Michigan Univ, Dept Biol, Mt Pleasant, MI 48858 USA. [Woolnough, Daelyn A.] Cent Michigan Univ, Inst Great Lakes Res, Mt Pleasant, MI 48858 USA. [Miller, Adam D.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Nijs, Ivan] Univ Antwerp, Dept Biol, Res Grp Plant & Vegetat Ecol, Campus Dr Eiken,Univ Pl 1, B-2610 Antwerp, Belgium. RP Li, ZQ (reprint author), Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing 100093, Peoples R China. EM lizq@ibcas.ac.cn OI Liao, Jinbao/0000-0002-9520-3235; Li, Zhenqing/0000-0002-3551-0188 FU National Key Basic Research Program of China [2013CB429905]; National Natural Science Foundation of China [41571505]; NSF grant [DEB-1353301] FX Z.L. was supported by the National Key Basic Research Program of China (no. 2013CB429905) and the National Natural Science Foundation of China (no. 41571505). A.D.M. was supported in part by an NSF grant (no. DEB-1353301). NR 58 TC 1 Z9 1 U1 5 U2 14 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD MAY 11 PY 2016 VL 283 IS 1830 AR 20160537 DI 10.1098/rspb.2016.0537 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA DM2EG UT WOS:000376158800024 ER PT J AU Selz, OM Thommen, R Pierotti, MER Anaya-Rojas, JM Seehausen, O AF Selz, O. M. Thommen, R. Pierotti, M. E. R. Anaya-Rojas, J. M. Seehausen, O. TI Differences in male coloration are predicted by divergent sexual selection between populations of a cichlid fish SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE mate choice; assortative mating; sexual selection; reproductive isolation; sensory drive; cichlid ID LAKE VICTORIA CICHLIDS; SENSORY DRIVE; ADAPTIVE RADIATION; SPECIATION; PREFERENCE; NYEREREI; TRAITS; MODEL; PAIR AB Female mating preferences can influence both intraspecific sexual selection and interspecific reproductive isolation, and have therefore been proposed to play a central role in speciation. Here, we investigate experimentally in the African cichlid fish Pundamilia nyererei if differences in male coloration between three para-allopatric populations (i.e. island populations with gene flow) of P. nyererei are predicted by differences in sexual selection by female mate choice between populations. Second, we investigate if female mating preferences are based on the same components of male coloration and go in the same direction when females choose among males of their own population, their own and other conspecific populations and a closely related para-allopatric sister-species, P. igneopinnis. Mate-choice experiments revealed that females of the three populations mated species-assortatively, that populations varied in their extent of population-assortative mating and that females chose among males of their own population based on different male colours. Females of different populations exerted directional intrapopulation sexual selection on different male colours, and these differences corresponded in two of the populations to the observed differences in male coloration between the populations. Our results suggest that differences in male coloration between populations of P. nyererei can be explained by divergent sexual selection and that population-assortative mating may directly result from intrapopulation sexual selection. C1 [Selz, O. M.; Seehausen, O.] EAWAG Swiss Fed Inst Aquat Sci & Technol, Ctr Ecol Evolut & Biogeochem, Dept Fish Ecol & Evolut, Seestr 79, CH-6047 Kastanienbaum, Switzerland. [Anaya-Rojas, J. M.] EAWAG Swiss Fed Inst Aquat Sci & Technol, Ctr Ecol Evolut & Biogeochem, Dept Aquat Ecol, Seestr 79, CH-6047 Kastanienbaum, Switzerland. [Selz, O. M.; Thommen, R.; Anaya-Rojas, J. M.; Seehausen, O.] Univ Bern, Inst Ecol & Evolut, Aquat Ecol & Evolut, Baltzerstr 6, CH-3012 Bern, Switzerland. [Pierotti, M. E. R.] Smithsonian Trop Res Inst, Naos Labs, Bd 356, Calzada De Amador 084303092, Panama. RP Selz, OM (reprint author), EAWAG Swiss Fed Inst Aquat Sci & Technol, Ctr Ecol Evolut & Biogeochem, Dept Fish Ecol & Evolut, Seestr 79, CH-6047 Kastanienbaum, Switzerland.; Selz, OM (reprint author), Univ Bern, Inst Ecol & Evolut, Aquat Ecol & Evolut, Baltzerstr 6, CH-3012 Bern, Switzerland. EM oliver.selz@eawag.ch FU Swiss National Science Foundation [31003A-118293] FX This research was supported by a Swiss National Science Foundation grant no. (31003A-118293). NR 47 TC 4 Z9 4 U1 24 U2 41 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD MAY 11 PY 2016 VL 283 IS 1830 AR 20160172 DI 10.1098/rspb.2016.0172 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA DM2EG UT WOS:000376158800013 ER PT J AU Corrales, LR Garcia, J Wilms, J Baganoff, F AF Corrales, L. R. Garcia, J. Wilms, J. Baganoff, F. TI The dust-scattering component of X-ray extinction: effects on continuum fitting and high-resolution absorption edge structure SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE scattering; dust, extinction; quasars: absorption lines; X-rays: binaries; X-rays: ISM ID INTERSTELLAR GRAINS; SPECTROSCOPY; MODELS; HALOS; STATE AB Small angle scattering by dust grains causes a significant contribution to the total interstellar extinction for any X-ray instrument with sub-arcminute resolution (Chandra, Swift, XMM-Newton). However, the dust-scattering component is not included in the current absorption models: , and . We simulate a large number of Chandra spectra to explore the bias in the spectral fit and N-H measurements obtained without including extinction from dust scattering. We find that without incorporating dust scattering, the measured N-H will be too large by a baseline level of 25 per cent. This effect is modulated by the imaging resolution of the telescope, because some amount of unresolved scattered light will be captured within the aperture used to extract point source information. In high-resolution spectroscopy, dust scattering significantly enhances the total extinction optical depth and the shape of the photoelectric absorption edges. We focus in particular on the Fe-L edge at 0.7 keV, showing that the total extinction template fits well to the high-resolution spectrum of three X-ray binaries from the Chandra archive: GX 9+9, XTE J1817-330, and Cyg X-1. In cases where dust is intrinsic to the source, a covering factor based on the angular extent of the dusty material must be applied to the extinction curve, regardless of angular imaging resolution. This approach will be particularly relevant for dust in quasar absorption line systems and might constrain clump sizes in active galactic nuclei. C1 [Corrales, L. R.; Baganoff, F.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave,37-241, Cambridge, MA 02139 USA. [Garcia, J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Observ, Sternwart Str 7, D-96049 Bamberg, Germany. RP Corrales, LR (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave,37-241, Cambridge, MA 02139 USA.; Garcia, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Wilms, J (reprint author), Univ Erlangen Nurnberg, Dr Karl Remeis Observ, Sternwart Str 7, D-96049 Bamberg, Germany. EM lia@space.mit.edu; javier@head.cfa.harvard.edu; joern.wilms@sternwarte.uni-erlangen.de RI Wilms, Joern/C-8116-2013 OI Wilms, Joern/0000-0003-2065-5410 NR 29 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 MAY 11 PY 2016 VL 458 IS 2 BP 1345 EP 1351 DI 10.1093/mnras/stw376 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ9YO UT WOS:000374569600017 ER PT J AU Crichton, D Gralla, MB Hall, K Marriage, TA Zakamska, NL Battaglia, N Bond, JR Devlin, MJ Hill, JC Hilton, M Hincks, AD Huffenberger, KM Hughes, JP Kosowsky, A Moodley, K Niemack, MD Page, LA Partridge, B Sievers, JL Sifon, C Staggs, ST Viero, MP Wollack, EJ AF Crichton, Devin Gralla, Megan B. Hall, Kirsten Marriage, Tobias A. Zakamska, Nadia L. Battaglia, Nick Bond, J. Richard Devlin, Mark J. Hill, J. Colin Hilton, Matt Hincks, Adam D. Huffenberger, Kevin M. Hughes, John P. Kosowsky, Arthur Moodley, Kavilan Niemack, Michael D. Page, Lyman A. Partridge, Bruce Sievers, Jonathan L. Sifon, Cristobal Staggs, Suzanne T. Viero, Marco P. Wollack, Edward J. TI Evidence for the thermal Sunyaev-Zel'dovich effect associated with quasar feedback SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; intergalactic medium; quasars: general ID ACTIVE GALACTIC NUCLEI; ATACAMA COSMOLOGY TELESCOPE; DIGITAL-SKY-SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; SUPERMASSIVE BLACK-HOLES; LUMINOUS OBSCURED QUASARS; RADIO-QUIET QUASARS; SIMILAR-TO 1.5; ABSORPTION-LINE QUASARS; EXTREME GAS KINEMATICS AB Using a radio-quiet subsample of the Sloan Digital Sky Survey spectroscopic quasar catalogue, spanning redshifts 0.5-3.5, we derive the mean millimetre and far-infrared quasar spectral energy distributions (SEDs) via a stacking analysis of Atacama Cosmology Telescope and Herschel-Spectral and Photometric Imaging REceiver data. We constrain the form of the far-infrared emission and find 3 sigma-4 sigma evidence for the thermal Sunyaev-Zel'dovich (SZ) effect, characteristic of a hot ionized gas component with thermal energy (6.2 +/- 1.7) x 10(60) erg. This amount of thermal energy is greater than expected assuming only hot gas in virial equilibrium with the dark matter haloes of (1-5) x 10(12) h(-1) M-circle dot that these systems are expected to occupy, though the highest quasar mass estimates found in the literature could explain a large fraction of this energy. Our measurements are consistent with quasars depositing up to (14.5 +/- 3.3) per cent of their radiative energy into their circumgalactic environment if their typical period of quasar activity is tau(8) x 10(8) yr. For high quasar host masses, similar to 10(13) h(-1) M-circle dot this percentage will be reduced. Furthermore, the uncertainty on this percentage is only statistical and additional systematic uncertainties enter at the 40 per cent level. The SEDs are dust dominated in all bands and we consider various models for dust emission. While sufficiently complex dust models can obviate the SZ effect, the SZ interpretation remains favoured at the 3 sigma-4 sigma level for most models. C1 [Crichton, Devin; Gralla, Megan B.; Hall, Kirsten; Marriage, Tobias A.; Zakamska, Nadia L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Gralla, Megan B.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Battaglia, Nick] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bond, J. Richard] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Devlin, Mark J.] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19104 USA. [Hill, J. Colin] Columbia Univ, Dept Astron, Pupin Hall, New York, NY 10027 USA. [Hilton, Matt; Moodley, Kavilan] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Stat & Comp Sci, ZA-4041 Durban, South Africa. [Hincks, Adam D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Huffenberger, Kevin M.] Florida State Univ, Dept Phys, POB 3064350, Tallahassee, FL 32306 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. [Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Page, Lyman A.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Jadwin Hall, Princeton, NJ 08544 USA. [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Sievers, Jonathan L.] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Chem & Phys, ZA-4041 Durban, South Africa. [Sifon, Cristobal] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Viero, Marco P.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Crichton, D (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. EM dcrichton@jhu.edu RI Wollack, Edward/D-4467-2012; OI Sifon, Cristobal/0000-0002-8149-1352; Wollack, Edward/0000-0002-7567-4451; Huffenberger, Kevin/0000-0001-7109-0099 FU US National Science Foundation [AST-0408698, AST-0965625, PHY-0855887, PHY-1214379]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation (CFI); Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT); CFI under the auspices of Compute Canada; Government of Ontario; Ontario Research Fund - Research Excellence; University of Toronto FX We thank the anonymous referee for their useful comments and suggestions. This work was supported by the US National Science Foundation through awards AST-0408698 and AST-0965625 for the ACT project, as well as awards PHY-0855887 and PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astronomico Atacama in northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT). Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund - Research Excellence; and the University of Toronto. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA), part of the High Energy Astrophysics Science Archive Center (HEASARC). HEASARC/LAMBDA is a service of the Astrophysics Science Division at the NASA Goddard Space Flight Center. This research made use of Astropy, a community-developed core PYTHON package for Astronomy (Astropy Collaboration et al. 2013) and the affine invariant MCMC ensemble sampler implementation provided by the EMCEE PYTHON package (Foreman-Mackey et al. 2013). NR 153 TC 1 Z9 1 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 MAY 11 PY 2016 VL 458 IS 2 BP 1478 EP 1492 DI 10.1093/mnras/stw344 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ9YO UT WOS:000374569600027 ER PT J AU Zhu, QR Marinacci, F Maji, M Li, YX Springel, V Hernquist, L AF Zhu, Qirong Marinacci, Federico Maji, Moupiya Li, Yuexing Springel, Volker Hernquist, Lars TI Baryonic impact on the dark matter distribution in Milky Way-sized galaxies and their satellites SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: evolution; dark matter ID SMOOTHED PARTICLE HYDRODYNAMICS; PROBE WMAP OBSERVATIONS; DWARF SPHEROIDAL GALAXIES; MOVING-MESH COSMOLOGY; LARGE-SCALE STRUCTURE; STELLAR FEEDBACK; LOCAL GROUP; STAR-FORMATION; LAMBDA-CDM; TOO BIG AB We study the impact of baryons on the distribution of dark matter in a Milky Way-sized halo by comparing a high-resolution, moving mesh cosmological simulation with its dark matter-only counterpart. We identify three main processes related to baryons - adiabatic contraction, tidal disruption, and reionization - which jointly shape the dark matter distribution in both the main halo and its subhaloes. The relative effect of each baryonic process depends strongly on the subhalo mass. For massive subhaloes with maximum circular velocity v(max) > 35 km s(-1), adiabatic contraction increases the dark matter concentration, making these haloes less susceptible to tidal disruption. For low-mass subhaloes with v(max) < 20 km s(-1), reionization effectively reduces their mass on average by a parts per thousand 30 per cent and v(max) by a parts per thousand 20 per cent. For intermediate subhaloes with 20 km s(-1) < v(max) < 35 km s(-1), which share a similar mass range as the classical dwarf spheroidals, strong tidal truncation induced by the main galaxy reduces their v(max). As a combined result of reionization and increased tidal disruption, the total number of low-mass subhaloes in the hydrodynamic simulation is nearly halved compared to that of the N-body simulation. We do not find dark matter cores in dwarf galaxies, unlike previous studies that employed bursty feedback-driven outflows. The substantial impact of baryons on the abundance and internal structure of subhaloes suggests that galaxy formation and evolution models based on N-body simulations should include these physical processes as major components. C1 [Zhu, Qirong; Maji, Moupiya; Li, Yuexing] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Zhu, Qirong; Maji, Moupiya; Li, Yuexing] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Marinacci, Federico] MIT, Kavli Inst Astrophys & Space Res, Dept Phys, Cambridge, MA 02139 USA. [Springel, Volker] Heidelberg Inst Theoret Studies, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, ARI, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany. [Hernquist, Lars] Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Zhu, QR (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.; Zhu, QR (reprint author), Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.; Marinacci, F (reprint author), MIT, Kavli Inst Astrophys & Space Res, Dept Phys, Cambridge, MA 02139 USA. EM zhuqirong1874@gmail.com; fmarinac@mit.edu OI /0000-0003-3816-7028 FU NSF [AST-0965694, AST-1009867, AST-1412719, AST-1312095]; NASA [NNX12AC67G]; DFG Research Centre [SFB-881]; European Research Council under ERC-StG grant [EXAGAL-308037]; Klaus Tschira Foundation; Eberly College of Science; Office of the Senior Vice President for Research at the Pennsylvania State University FX We thank Steinn Sigurdsson, Priyamvada Natarajan, Annalisa Pillepich, Arthur Kosowsky, Eddie Chua, and Dylan Nelson for their suggestions and helpful discussions. We also thank an anonymous referee for valuable comments that have helped improve the manuscript. YL acknowledges support from NSF grants AST-0965694, AST-1009867, and AST-1412719. LH acknowledges support from NSF grant AST-1312095 and NASA grant NNX12AC67G. VS acknowledges support by the DFG Research Centre SFB-881 'The Milky Way System' through project A1, by the European Research Council under ERC-StG grant EXAGAL308037, and by the Klaus Tschira Foundation. We acknowledge the Institute For CyberScience at the Pennsylvania State University for providing computational resources and services that have contributed to the research results reported in this paper. 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. NR 153 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 MAY 11 PY 2016 VL 458 IS 2 BP 1559 EP 1580 DI 10.1093/mnras/stw374 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ9YO UT WOS:000374569600034 ER PT J AU Krumholz, MR Burkhart, B AF Krumholz, Mark R. Burkhart, Blakesley TI Is turbulence in the interstellar medium driven by feedback or gravity? An observational test SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE turbulence; stars: formation; ISM: kinematics and dynamics; galaxies: ISM; galaxies: starburst ID STAR-FORMING GALAXIES; 3-DIMENSIONAL HYDRODYNAMIC SIMULATIONS; MULTIPHASE GALACTIC DISKS; GIANT MOLECULAR CLOUDS; SMALL-MAGELLANIC-CLOUD; HIGH-REDSHIFT; VELOCITY DISPERSION; RADIATION PRESSURE; NEARBY GALAXIES; GRAVITATIONAL-INSTABILITY AB Galaxies' interstellar media (ISM) are observed to be supersonically turbulent, but the ultimate power source that drives turbulent motion remains uncertain. The two dominant models are that the turbulence is driven by star formation feedback and/or that it is produced by gravitational instability in the gas. Here we show that, while both models predict that the galaxies' ISM velocity dispersions will be positively correlated with their star formation rates, the forms of the correlation predicted by these two models are subtly but measurably different. A feedback-driven origin for the turbulence predicts a velocity dispersion that rises more sharply with star formation rate, and that does not depend on the gas fraction (i.e. (M) over dot(*) proportional to sigma(2)), while a gravity-driven model yields a shallower rise and a strong dependence on gas fraction (i.e. (M) over dot(*) proportional to f(g)(2)sigma). We compare the models to a collection of data on local and high-redshift galaxies culled from the literature, and show that the correlation expected for gravity-driven turbulence is a better match to the observations than a feedback-driven model. This suggests that gravity is the ultimate source of ISM turbulence, at least in the rapidly star-forming, high-velocity dispersion galaxies for which our test is most effective. We conclude by discussing the limitations of the present data set, and the prospects for future measurements to enable a more definitive test of the two models. C1 [Krumholz, Mark R.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Krumholz, Mark R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Krumholz, Mark R.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Burkhart, Blakesley] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA USA. RP Krumholz, MR (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.; Krumholz, MR (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.; Krumholz, MR (reprint author), Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. EM mark.krumholz@anu.edu.au FU Australian Research Council [DP160100695]; US NSF [AST-1405962]; NASA Einstein Postdoctoral Fellowship FX MRK thanks F. Fraternali for helpful discussions. MRK is supported by grant DP160100695 from the Australian Research Council and grant AST-1405962 from the US NSF. BB is supported by the NASA Einstein Postdoctoral Fellowship. NR 92 TC 6 Z9 6 U1 2 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2016 VL 458 IS 2 BP 1671 EP 1677 DI 10.1093/mnras/stw434 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ9YO UT WOS:000374569600042 ER PT J AU Cunningham, N Lumsden, SL Cyganowski, CJ Maud, LT Purcell, C AF Cunningham, Nichol Lumsden, Stuart L. Cyganowski, Claudia J. Maud, Luke T. Purcell, Cormac TI Submillimeter array observations of NGC 2264-C: molecular outflows and driving sources SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: formation; ISM: jets and outflows; ISM: molecules ID STAR-FORMING REGIONS; YOUNG STELLAR OBJECTS; SIO LINE EMISSION; MSX SOURCE SURVEY; HIGH-MASS STARS; CLASS-I; PROTOSTELLAR CANDIDATES; INTERMEDIATE-MASS; METHANOL MASERS; CO OUTFLOWS AB We present 1.3 mm Submillimeter Array (SMA) observations at similar to 3 arcsec resolution towards the brightest section of the intermediate/massive star-forming cluster NGC 2264-C. The millimetre continuum emission reveals ten 1.3 mm continuum peaks, of which four are new detections. The observed frequency range includes the known molecular jet/outflow tracer SiO (5-4), thus providing the first high-resolution observations of SiO towards NGC 2264-C. We also detect molecular lines of 12 additional species towards this region, including CH3CN, CH3OH, SO, H2CO, DCN, HC3N, and (CO)-C-12. The SiO (5-4) emission reveals the presence of two collimated, high-velocity (up to 30 km s(-1) with respect to the systemic velocity) bipolar outflows in NGC 2264-C. In addition, the outflows are traced by emission from (CO)-C-12, SO, H2CO, and CH3OH. We find an evolutionary spread between cores residing in the same parent cloud. The two unambiguous outflows are driven by the brightest mm continuum cores, which are IR-dark, molecular line weak, and likely the youngest cores in the region. Furthermore, towards the Red MSX Source AFGL 989-IRS1, the IR-bright and most evolved source in NGC 2264-C, we observe no molecular outflow emission. A molecular line rich ridge feature, with no obvious directly associated continuum source, lies on the edge of a low-density cavity and may be formed from a wind driven by AFGL 989-IRS1. In addition, 229 GHz class I maser emission is detected towards this feature. C1 [Cunningham, Nichol; Lumsden, Stuart L.; Maud, Luke T.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Cunningham, Nichol] Natl Radio Astron Observ, POB 2, Green Bank, WV 24944 USA. [Cyganowski, Claudia J.] Univ St Andrews, Scottish Univ Phys Alliance, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Cyganowski, Claudia J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maud, Luke T.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Purcell, Cormac] Univ Sydney, Sydney Inst Astron, Sydney, NSW 2006, Australia. RP Cunningham, N (reprint author), Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.; Cunningham, N (reprint author), Natl Radio Astron Observ, POB 2, Green Bank, WV 24944 USA. EM ncunning@nrao.edu FU STFC [ST/M001296/1]; National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship [AST-1003134] FX We thank the anonymous referee for helpful comments that have improved the content and overall clarity of this manuscript. CJC acknowledges support from the STFC (grant number ST/M001296/1). CJC was partially supported during this work by a National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1003134. The authors are very grateful to N. Peretto for providing the reduced PdBI N2H+ (1-0) integrated intensity maps that were published in Peretto et al. (2007). This research made use of APLPY, an open-source plotting package for PYTHON hosted at http://aplpy.github.com; astrodendro, a dendrogram plotting routine for PYTHON hosted at http://www.dendrograms.org/ and the Splatalogue molecular data base (http:/splatalogue.net/). NR 97 TC 1 Z9 1 U1 2 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2016 VL 458 IS 2 BP 1742 EP 1767 DI 10.1093/mnras/stw359 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ9YO UT WOS:000374569600048 ER PT J AU Bordoloi, R Rigby, JR Tumlinson, J Bayliss, MB Sharon, K Gladders, MG Wuyts, E AF Bordoloi, Rongmon Rigby, Jane R. Tumlinson, Jason Bayliss, Matthew B. Sharon, Keren Gladders, Michael G. Wuyts, Eva TI Spatially resolved galactic wind in lensed galaxy RCSGA 032727-132609 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: high-redshift; intergalactic medium; ultraviolet: ISM ID STAR-FORMING GALAXIES; SIMILAR-TO 1; ABSORPTION-LINE PROBES; LYMAN BREAK GALAXIES; SINS/ZC-SINF SURVEY; MG II ABSORBERS; LESS-THAN 2; PHYSICAL CONDITIONS; ULTRAVIOLET-SPECTRA; STARBURST GALAXIES AB We probe the spatial distribution of outflowing gas along four lines of sight separated by up to 6 kpc in a gravitationally lensed star-forming galaxy at z = 1.70. Using Mg ii and Fe ii emission and absorption as tracers, we find that the clumps of star formation are driving galactic outflows with velocities of -170 to -250 km s(-1). The velocities of Mg ii emission are redshifted with respect to the systemic velocities of the galaxy, consistent with being back-scattered. By contrast, the Fe ii fluorescent emission lines are either slightly blueshifted or at the systemic velocity of the galaxy. Taken together, the velocity structure of the Mg ii and Fe ii emission is consistent with arising through scattering in galactic winds. Assuming a thin shell geometry for the outflowing gas, the estimated masses carried out by these outflows are large (a parts per thousand(3)30-50 M-aS (TM) yr(- 1)), with mass loading factors several times the star formation rate. Almost 20 per cent to 50 per cent of the blueshifted absorption probably escapes the gravitational potential of the galaxy. In this galaxy, the outflow is 'locally sourced', that is, the properties of the outflow in each line of sight are dominated by the properties of the nearest clump of star formation; the wind is not global to the galaxy. The mass outflow rates and the momentum flux carried out by outflows in individual star-forming knots of this object are comparable to that of starburst galaxies in the local Universe. C1 [Bordoloi, Rongmon; Tumlinson, Jason] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Bordoloi, Rongmon] MIT, Kavli Ctr Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. [Bayliss, Matthew B.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. [Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Sharon, Keren] Univ Michigan, Dept Astron & Astrophys, 500 Church St, Ann Arbor, MI 48109 USA. [Gladders, Michael G.] Univ Chicago, Dept Astron & Astrophys, 5640 South Ellis Ave, Chicago, IL 60637 USA. [Gladders, Michael G.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Wuyts, Eva] Max Planck Inst Extraterr Phys, Postfach 1312,Giessenbachstr, D-85741 Garching, Germany. RP Bordoloi, R (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.; Bordoloi, R (reprint author), MIT, Kavli Ctr Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM rongmon.bordoloi@gmail.com FU NSF [1066293]; NASA through Hubble Fellowship - Space Telescope Science Institute [51354]; NASA [NAS 5-26555] FX RB would like to thank the Aspen Center for Physics (supported by NSF grant 1066293) for hospitality and productive atmosphere and organizers of the workshop 'Physics of Accretion and Feedback in the Circum-Galactic Medium' in 2015 June, for opportunities to discuss results presented here during completion of this paper. RB would like to thank Timothy Heckman for stimulating discussions on this work. RB would also like to thank Peter Behroozi for providing mock catalogues to estimate halo mass of the host galaxy. Partial support for this work was provided by NASA through Hubble Fellowship grant #51354 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Magellan observing time for this programme was granted by the telescope allocation committees of the Carnegie Observatories, the University of Chicago, the University of Michigan, and Harvard University. NR 74 TC 2 Z9 2 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2016 VL 458 IS 2 BP 1891 EP 1908 DI 10.1093/mnras/stw449 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ9YO UT WOS:000374569600058 ER PT J AU Tkachenko, A Matthews, JM Aerts, C Pavlovski, K Papics, PI Zwintz, K Cameron, C Walker, GAH Kuschnig, R Degroote, P Debosscher, J Moravveji, E Kolbas, V Guenther, DB Moffat, AFJ Rowe, JF Rucinski, SM Sasselov, D Weiss, WW AF Tkachenko, A. Matthews, J. M. Aerts, C. Pavlovski, K. Papics, P. I. Zwintz, K. Cameron, C. Walker, G. A. H. Kuschnig, R. Degroote, P. Debosscher, J. Moravveji, E. Kolbas, V. Guenther, D. B. Moffat, A. F. J. Rowe, J. F. Rucinski, S. M. Sasselov, D. Weiss, W. W. TI Stellar modelling of Spica, a high-mass spectroscopic binary with a beta Cep variable primary component SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: spectroscopic; stars: fundamental parameters; stars: individual: alpha Virginis; stars: oscillations; stars: variables: general ID B-TYPE STARS; ECLIPSING BINARY; ALPHA-VIRGINIS; NONRADIAL OSCILLATIONS; CHEMICAL-COMPOSITION; ASTROPHYSICS MESA; APSIDAL CONSTANT; ORBITAL ELEMENTS; CLOSE BINARIES; SIGMA-SCORPII AB Binary stars provide a valuable test of stellar structure and evolution, because the masses of the individual stellar components can be derived with high accuracy and in a model-independent way. In this work, we study Spica, an eccentric double-lined spectroscopic binary system with a beta Cep type variable primary component. We use state-of-the-art modelling tools to determine accurate orbital elements of the binary system and atmospheric parameters of both stellar components. We interpret the short-period variability intrinsic to the primary component, detected on top of the orbital motion both in the photometric and spectroscopic data. The non-local thermodynamic equilibrium based spectrum analysis reveals two stars of similar atmospheric chemical composition consistent with the present-day cosmic abundance standard. The masses and radii of the stars are found to be 11.43 +/- A 1.15 M-aS (TM) and 7.21 +/- A 0.75 M-aS (TM), and 7.47 +/- A 0.54 R-aS (TM) and 3.74 +/- A 0.53 R-aS (TM) for the primary and secondary, respectively. We find the primary component to pulsate in three independent modes, of which one is identified as a radial mode, while the two others are found to be non-radial, low degree l modes. The frequency of one of these modes is an exact multiple of the orbital frequency, and the l = m = 2 mode identification suggests a tidal nature for this particular mode. We find a very good agreement between the derived dynamical and evolutionary masses for the Spica system to within the observational errors of the measured masses. The age of the system is estimated to be 12.5 +/- A 1 Myr. C1 [Tkachenko, A.; Aerts, C.; Papics, P. I.; Degroote, P.; Debosscher, J.; Moravveji, E.] Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Leuven, Belgium. [Matthews, J. M.; Cameron, C.; Walker, G. A. H.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. [Aerts, C.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Pavlovski, K.; Kolbas, V.] Univ Zagreb, Dept Phys, Bijenicka Cesta 32, Zagreb 10000, Croatia. [Zwintz, K.] Univ Innsbruck, Inst Astro & Particle Phys, Technikerstrasse 25-8, A-6020 Innsbruck, Austria. [Cameron, C.] Cape Breton Univ, Dept Math Phys & Geol, 1250 Grand Lake Rd, Sydney, NS B1P 6L2, Canada. [Kuschnig, R.] Univ Vienna, Inst Astron, Turkenschanzstrasse 17, AT-1180 Vienna, Austria. [Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Moffat, A. F. J.] Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada. [Rowe, J. F.] NASA, Ames Res Pk, MS-244-30, Moffett Field, CA 94035 USA. [Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Tkachenko, A.; Papics, P. I.] Res Fdn Flanders, Brussels, Belgium. RP Tkachenko, A (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Leuven, Belgium.; Tkachenko, A (reprint author), Res Fdn Flanders, Brussels, Belgium. EM andrew@ster.kuleuven.be FU European Research Council (ERC) under the European Union's Horizon research and innovation programme [670519]; European Community [FP7-SPACE-2011-1, 312844]; Fund for Scientific Research of Flanders (FWO), Belgium [G.0B69.13]; European Union [623303]; Croatian Science Foundation [2014-09-8656]; Austrian Fonds zur Foerderung der wissenschaftlichen Forschung (FWF) [V431-NBL] FX The research leading to these results has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No 670519: MAMSIE), from the European Community's Seventh Framework Programme FP7-SPACE-2011-1, project number 312844 (SPACEINN), and from the Fund for Scientific Research of Flanders (FWO), Belgium, under grant agreement G.0B69.13.EM has received funding from the People Programme (Marie Curie Actions) of the European Unions Seventh Framework Programme FP7/2007-2013/ under REA grant agreement no. 623303 for the project ASAMBA. KP was (partially) supported by the Croatian Science Foundation under the grant 2014-09-8656. KZ acknowledges support by the Austrian Fonds zur Foerderung der wissenschaftlichen Forschung (FWF, project V431-NBL). Mode identification results with the software package FAMIAS developed in the framework of the FP6 European Coordination Action HELAS (http://www.helas-eu.org/). AT dedicates this work to his grandfather, A. Solomchenko, who passed away in 2016 January. Based on data from the MOST satellite, a Canadian Space Agency mission, jointly operated by Dynacon Inc., the University of Toronto Institute for Aerospace Studies and the University of British Columbia, with the assistance of the University of Vienna. NR 64 TC 2 Z9 2 U1 3 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 MAY 11 PY 2016 VL 458 IS 2 BP 1964 EP 1976 DI 10.1093/mnras/stw255 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ9YO UT WOS:000374569600064 ER PT J AU Cranmer, SR Woolsey, LN AF Cranmer, Steven R. Woolsey, Lauren N. TI DRIVING SOLAR SPICULES AND JETS WITH MAGNETOHYDRODYNAMIC TURBULENCE: TESTING A PERSISTENT IDEA (vol 812, 71, 2015) SO ASTROPHYSICAL JOURNAL LA English DT Correction DE Sun: atmosphere; Sun: chromosphere; Sun: corona; turbulence; waves ID WAVES C1 [Cranmer, Steven R.] Univ Colorado, Atmospher & Space Phys Lab, Dept Astrophys & Planetary Sci, Campus Box 392, Boulder, CO 80309 USA. [Woolsey, Lauren N.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Dept Astrophys & Planetary Sci, Campus Box 392, Boulder, CO 80309 USA. NR 10 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 MAY 10 PY 2016 VL 822 IS 2 AR 119 DI 10.3847/0004-637X/822/2/119 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6RZ UT WOS:000377204900062 ER PT J AU Finkbeiner, DP Schlafly, EF Schlegel, DJ Padmanabhan, N Juric, M Burgett, WS Chambers, KC Denneau, L Draper, PW Flewelling, H Hodapp, KW Kaiser, N Magnier, EA Metcalfe, N Morgan, JS Price, PA Stubbs, CW Tonry, JL AF Finkbeiner, Douglas P. Schlafly, Edward F. Schlegel, David J. Padmanabhan, Nikhil Juric, Mario Burgett, William S. Chambers, Kenneth C. Denneau, Larry Draper, Peter W. Flewelling, Heather Hodapp, Klaus W. Kaiser, Nick Magnier, E. A. Metcalfe, N. Morgan, Jeffrey S. Price, Paul A. Stubbs, Christopher W. Tonry, John L. TI HYPERCALIBRATION: A PAN-STARRS1-BASED RECALIBRATION OF THE SLOAN DIGITAL SKY SURVEY PHOTOMETRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; surveys; techniques: photometric ID DATA RELEASE; SDSS-III; CALIBRATION; EXTINCTION; TELESCOPE; MONITOR AB We present a recalibration of the Sloan Digital Sky Survey (SDSS) photometry with new flat fields and zero points derived from Pan-STARRS1. Using point-spread function (PSF) photometry of 60 million stars with 16 < r < 20, we derive a model of amplifier gain and flat-field corrections with per-run rms residuals of 3 millimagnitudes (mmag) in griz bands and 15 mmag in u band. The new photometric zero points are adjusted to leave the median in the Galactic north unchanged for compatibility with previous SDSS work. We also identify transient nonphotometric periods in SDSS ("contrails") based on photometric deviations co-temporal in SDSS bands. The recalibrated stellar PSF photometry of SDSS and PS1 has an rms difference of {9, 7, 7, 8} mmag in griz, respectively, when averaged over 15' regions. C1 [Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS-51, Cambridge, MA 02138 USA. [Finkbeiner, Douglas P.; Stubbs, Christopher W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Schlafly, Edward F.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Padmanabhan, Nikhil] Yale Univ, Dept Phys, 260 Whitney Ave, New Haven, CT 06520 USA. [Juric, Mario] LSST Corp, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Burgett, William S.; Chambers, Kenneth C.; Denneau, Larry; Flewelling, Heather; Hodapp, Klaus W.; Kaiser, Nick; Magnier, E. A.; Morgan, Jeffrey S.; Tonry, John L.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Draper, Peter W.; Metcalfe, N.] Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. [Price, Paul A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Finkbeiner, DP (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS-51, Cambridge, MA 02138 USA.; Finkbeiner, DP (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. OI Chambers, Kenneth /0000-0001-6965-7789 FU NASA [NNX10AD69G]; German Research Foundation (DFG) [Sonderforschungsbereich SFB 881]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; National Aeronautics and Space Administration [NNX08AR22G]; National Science Foundation [AST-1238877] FX We acknowledge helpful conversations with Michael Blanton. DPF and EFS have been partially supported by NASA grant NNX10AD69G. EFS acknowledges funding by Sonderforschungsbereich SFB 881 "The Milky Way System" (subproject A3) of the German Research Foundation (DFG). This research made use of the NASA Astrophysics Data System (ADS) and the IDL Astronomy User's Library at Goddard.16; 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/.; The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, 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, and the University of Maryland. NR 30 TC 7 Z9 7 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 MAY 10 PY 2016 VL 822 IS 2 AR 66 DI 10.3847/0004-637X/822/2/66 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6RZ UT WOS:000377204900009 ER PT J AU Forbrich, J Rivilla, VM Menten, KM Reid, MJ Chandler, CJ Rau, U Bhatnagar, S Wolk, SJ Meingast, S AF Forbrich, J. Rivilla, V. M. Menten, K. M. Reid, M. J. Chandler, C. J. Rau, U. Bhatnagar, S. Wolk, S. J. Meingast, S. TI THE POPULATION OF COMPACT RADIO SOURCES IN THE ORION NEBULA CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE radio continuum: stars; stars: coronae; stars: formation; X-rays: stars ID YOUNG STELLAR OBJECTS; X-RAY; ULTRADEEP PROJECT; BN/KL REGION; STARS; EMISSION; VARIABILITY; ASTRONOMY; SOLAR AB We present a deep centimeter-wavelength catalog of the Orion Nebula Cluster (ONC), based on a 30 hr single-pointing observation with the Karl G. Jansky Very Large Array in its high-resolution A-configuration using two 1 GHz bands centered at 4.7 and 7.3 GHz. A total of 556 compact sources were detected in a map with a nominal rms noise of 3 mu Jy bm(-1), limited by complex source structure and the primary beam response. Compared to previous catalogs, our detections increase the sample of known compact radio sources in the ONC by more than a factor of seven. The new data show complex emission on a wide range of spatial scales. Following a preliminary correction for the wideband primary-beam response, we determine radio spectral indices for 170 sources whose index uncertainties are less than +/- 0.5. We compare the radio to the X-ray and near-infrared point-source populations, noting similarities and differences. C1 [Forbrich, J.; Meingast, S.] Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria. [Forbrich, J.; Reid, M. J.; Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Rivilla, V. M.] Osserv Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy. [Menten, K. M.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Rau, U.; Bhatnagar, S.] Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA. RP Forbrich, J (reprint author), Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria.; Forbrich, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jan.forbrich@univie.ac.at OI Wolk, Scott/0000-0002-0826-9261 FU National Aeronautics and Space Administration [GO2-13019X]; National Aeronautics Space Administration [NAS8-03060]; Italian Ministero dell'Istruzione, Universita e Ricerca FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO2-13019X 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. JF acknowledges informative discussions with Eric Feigelson and Kosta Getman. JF and VMR acknowledge the hospitality of NRAO Socorro during an extended data reduction visit. VMR is funded by the Italian Ministero dell'Istruzione, Universita e Ricerca through the grant Progetti Premiali 2012-iALMA. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com; Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013); matplotlib, a Python library for publication quality graphics (Hunter 2007). NR 44 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2016 VL 822 IS 2 AR 93 DI 10.3847/0004-637X/822/2/93 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6RZ UT WOS:000377204900036 ER PT J AU Gwinn, CR Popov, MV Bartel, N Andrianov, AS Johnson, MD Joshi, BC Kardashev, NS Karuppusamy, R Kovalev, YY Kramer, M Rudnitskii, AG Safutdinov, ER Shishov, VI Smirnova, TV Soglasnov, VA Steinmassl, SF Zensus, JA Zhuravlev, VI AF Gwinn, C. R. Popov, M. V. Bartel, N. Andrianov, A. S. Johnson, M. D. Joshi, B. C. Kardashev, N. S. Karuppusamy, R. Kovalev, Y. Y. Kramer, M. Rudnitskii, A. G. Safutdinov, E. R. Shishov, V. I. Smirnova, T. V. Soglasnov, V. A. Steinmassl, S. F. Zensus, J. A. Zhuravlev, V. I. TI PSR B0329+54: STATISTICS OF SUBSTRUCTURE DISCOVERED WITHIN THE SCATTERING DISK ON RADIOASTRON BASELINES OF UP TO 235,000 km SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (B0329+54); radio continuum: ISM; scattering; techniques: high angular resolution ID BROADENED IMAGE; INTERSTELLAR SCINTILLATION; VLBI OBSERVATIONS; PULSAR B0834+06; 1650 MHZ; PLASMA; NOISE; RADIATION; EMISSION; SPECTRUM AB We discovered fine-scale structure within the scattering disk of PSR B0329+54 in observations with the RadioAstron ground-space radio interferometer. Here we describe this phenomenon, characterize it with averages and correlation functions, and interpret it as the result of decorrelation of the impulse-response function of interstellar scattering between the widely separated antennas. This instrument included the 10 m Space Radio Telescope, the 110 m Green Bank Telescope, the 14 x 25 m Westerbork Synthesis Radio Telescope, and the 64 m Kalyazin Radio Telescope. The observations were performed at 324 MHz on baselines of up to 235,000 km in 2012 November and 2014 January. In the delay domain, on long baselines the interferometric visibility consists of many discrete spikes within a limited range of delays. On short baselines it consists of a sharp spike surrounded by lower spikes. The average envelope of correlations of the visibility function shows two exponential scales, with characteristic delays of tau(1) = 4.1 +/- 0.3 mu s and tau(2) = 23 +/- 3 mu s, indicating the presence of two scales of scattering in the interstellar medium. These two scales are present in the pulse-broadening function. The longer scale contains 0.38 times the scattered power of the shorter one. We suggest that the longer tail arises from highly scattered paths, possibly from anisotropic scattering or from substructure at large angles. C1 [Gwinn, C. R.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. [Popov, M. V.; Andrianov, A. S.; Kardashev, N. S.; Kovalev, Y. Y.; Rudnitskii, A. G.; Safutdinov, E. R.; Soglasnov, V. A.; Zhuravlev, V. I.] Ctr Astro Space, PN Lebedev Phys Inst, Profsoyuznaya 84-32, Moscow 117997, Russia. [Bartel, N.] York Univ, 4700 Keele St, Toronto, ON M3J 1P3, Canada. [Johnson, M. D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Joshi, B. C.] Natl Ctr Radio Astrophys, Post Bag 3, Pune 411007, Maharashtra, India. [Karuppusamy, R.; Kramer, M.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Kovalev, Y. Y.] Moscow Inst Phys & Technol, Inst Sky Per 9, Dolgoprudnyi 141700, Russia. [Shishov, V. I.; Smirnova, T. V.] Pushchino Radio Astron Observ, PN Lebedev Phys Inst, Pushchino 142290, Moscow Region, Russia. [Steinmassl, S. F.] Tech Univ Munich, Dept Phys, James Franck Str 1, D-85748 Garching, Germany. RP Gwinn, CR (reprint author), Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. RI Zhuravlev, Vladimir/M-6848-2015; Rudnitskiy, Alexey/M-6073-2013; Kovalev, Yuri/J-5671-2013; Soglasnov, Vladimir/O-7615-2015; Popov, Mikhail/M-6118-2015; Smirnova, Tatiana/N-1696-2015; Andrianov, Andrey/N-2638-2015; Shishov, Vladimir/N-1753-2015; Kardashev, Nikolai/O-6441-2015 OI Rudnitskiy, Alexey/0000-0003-1798-9444; Kovalev, Yuri/0000-0001-9303-3263; FU Russian Foundation for Basic Research [13-02-00460]; Presidium of the Russian Academy of Sciences [P-7]; U.S. National Science Foundation [AST-1008865]; NSERC FX The RadioAstron project is led by the Astro Space Center of the Lebedev Physical Institute of the Russian Academy of Sciences and the Lavochkin Scientific and Production Association under a contract with the Russian Federal Space Agency, in collaboration with partner organizations in Russia and other countries. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This study was supported by Russian Foundation for Basic Research grant 13-02-00460 and Basic Research Program P-7 of the Presidium of the Russian Academy of Sciences. C.R.G. acknowledges support of the U.S. National Science Foundation (AST-1008865). N.B. was supported by NSERC. We thank the referee for constructive comments that helped to improve the manuscript. NR 37 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 MAY 10 PY 2016 VL 822 IS 2 AR 96 DI 10.3847/0004-637X/822/2/96 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6RZ UT WOS:000377204900039 ER PT J AU Kipping, DM Torres, G Henze, C Teachey, A Ciardi, D Isaacson, H Petigura, E Marcy, GW Buchhave, LA Chen, J Bryson, ST Sandford, E AF Kipping, D. M. Torres, G. Henze, C. Teachey, A. Ciardi, D. Isaacson, H. Petigura, E. Marcy, G. W. Buchhave, L. A. Chen, J. Bryson, S. T. Sandford, E. TI A TRANSITING JUPITER ANALOG (vol 820, 112, 2016) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Kipping, D. M.; Teachey, A.; Chen, J.; Sandford, E.] Columbia Univ, Dept Astron, 550 W 120th St, New York, NY 10027 USA. [Torres, G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Henze, C.; Bryson, S. T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ciardi, D.] CALTECH, NASA, Exoplanet Sci Inst, M-C 100-22,770 South Wilson Ave, Pasadena, CA 91125 USA. [Isaacson, H.; Petigura, E.; Marcy, G. W.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Buchhave, L. A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. RP Kipping, DM (reprint author), Columbia Univ, Dept Astron, 550 W 120th St, New York, NY 10027 USA. EM dkipping@astro.columbia.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 MAY 10 PY 2016 VL 822 IS 2 AR 118 DI 10.3847/0004-637X/822/2/118 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6RZ UT WOS:000377204900061 ER PT J AU Narayan, G Axelrod, T Holberg, JB Matheson, T Saha, A Olszewski, E Claver, J Stubbs, CW Bohlin, RC Deustua, S Rest, A AF Narayan, G. Axelrod, T. Holberg, J. B. Matheson, T. Saha, A. Olszewski, E. Claver, J. Stubbs, C. W. Bohlin, R. C. Deustua, S. Rest, A. TI TOWARD A NETWORK OF FAINT DA WHITE DWARFS AS HIGH-PRECISION SPECTROPHOTOMETRIC STANDARDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; methods: data analysis; surveys; white dwarfs ID SPECTRAL-ENERGY DISTRIBUTION; PHOTOMETRIC CALIBRATION; ABSOLUTE FLUX; IA SUPERNOVAE; VEGA; TELESCOPE; SPECTROGRAPH; CONSTRAINTS; EXTINCTION; SPECTROSCOPY AB We present the initial results from a program aimed at establishing a network of hot DA white dwarfs to serve as spectrophotometric standards for present and future wide-field surveys. These stars span the equatorial zone and are faint enough to be conveniently observed throughout the year with large-aperture telescopes. The spectra of these white dwarfs are analyzed in order to generate a non-local-thermodynamic-equilibrium model atmosphere normalized to Hubble Space Telescope colors, including adjustments for wavelength-dependent interstellar extinction. Once established, this standard star network will serve ground-based observatories in both hemispheres as well as space-based instrumentation from the UV to the near IR. We demonstrate the effectiveness of this concept and show how two different approaches to the problem using somewhat different assumptions produce equivalent results. We discuss the lessons learned and the resulting corrective actions applied to our program. C1 [Narayan, G.; Matheson, T.; Saha, A.; Claver, J.] Natl Opt Astron Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA. [Axelrod, T.; Olszewski, E.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [Holberg, J. B.] Univ Arizona, Lunar & Planetary Lab, 1629 East Univ Blvd, Tucson, AZ 85721 USA. [Stubbs, C. W.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. [Stubbs, C. W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Bohlin, R. C.; Deustua, S.; Rest, A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. RP Narayan, G (reprint author), Natl Opt Astron Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA. EM gnarayan@noao.edu OI bohlin, ralph/0000-0001-9806-0551; Narayan, Gautham/0000-0001-6022-0484 FU NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina) [GS-2013A-Q-8, GS-2013B-Q-22] FX 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 NNX13AC07G and by other grants and contracts.; 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) (Programs GS-2013A-Q-8 and GS-2013B-Q-22). NR 39 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 MAY 10 PY 2016 VL 822 IS 2 AR 67 DI 10.3847/0004-637X/822/2/67 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6RZ UT WOS:000377204900010 ER PT J AU Peris, CS Remillard, RA Steiner, JF Vrtilek, SD Varniere, P Rodriguez, J Pooley, G AF Peris, Charith S. Remillard, Ronald A. Steiner, James F. Vrtilek, Saeqa D. Varniere, Peggy Rodriguez, Jerome Pooley, Guy TI X-RAY SPECTRAL ANALYSIS OF THE STEADY STATES OF GRS1915+105 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries: close; black hole physics; magnetic fields; X-rays: binaries; X-rays: individual (GRS1915+105) ID ACCRETION-EJECTION INSTABILITY; BLACK-HOLE BINARIES; ABSORPTION-LINE FEATURES; MICROQUASAR GRS 1915+105; NOVA-MUSCAE 1991; LOW/HARD STATE; GX 339-4; MAGNETIZED DISKS; RADIO-EMISSION; XTE J1550-564 AB We report on the X-ray spectral behavior within the steady states of GRS1915+105. Our work is based on the full data set of the source obtained using the Proportional Counter Array (PCA) on the Rossi X-ray Timing Explorer (RXTE) and 15 GHz radio data obtained using the Ryle Telescope. The steady observations within the X-ray data set naturally separated into two regions in the color-color diagram and we refer to these regions as steady-soft and steady-hard. GRS1915+105 displays significant curvature in the coronal component in both the soft and hard data within the RXTE/PCA bandpass. A majority of the steady-soft observations displays a roughly constant inner disk radius (R-in), while the steady-hard observations display an evolving disk truncation which is correlated to the mass accretion rate through the disk. The disk flux and coronal flux are strongly correlated in steady-hard observations and very weakly correlated in the steady-soft observations. Within the steady-hard observations, we observe two particular circumstances when there are correlations between the coronal X-ray flux and the radio flux with log slopes eta +/- 0.68 +/- 0.35. and eta +/- 1.12 +/- 0.13. They are consistent with the upper and lower tracks of Gallo et al. (2012), respectively. A comparison of the model parameters to the state definitions shows that almost all of the steady-soft observations match the criteria of either a thermal or steep power-law state, while a large portion of the steady-hard observations match the hard-state criteria when the disk fraction constraint is neglected. C1 [Peris, Charith S.; Steiner, James F.; Vrtilek, Saeqa D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Peris, Charith S.] Northeastern Univ, Dept Phys, 360 Huntington Ave, Boston, MA 02115 USA. [Remillard, Ronald A.; Steiner, James F.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Varniere, Peggy] Univ Paris Diderot, APC, AstroParticule & Cosmol, N2P3,CEA Irfu,Observ Paris,Sorbonne Paris Cite,UM, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. [Rodriguez, Jerome] Univ Paris Diderot, Lab AIM, CEA, IRFU CNRS,INSU,CEA DSM,IRFU,SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France. [Pooley, Guy] Univ Cambridge, Cavendish Lab, Astrophys, Madingley Rd, Cambridge CB3 0HE, England. RP Peris, CS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cperis@cfa.harvard.edu OI Rodriguez, Jerome/0000-0002-4151-4468 FU NASA Einstein Fellowship [PF5-160144]; Smithsonian Institution CGPS grant; French Research National Agency: CHAOS project [ANR-12-BS05-0009]; UnivEarthS Labex program at Sorbonne Paris Cite [ANR-10-LABX-0023, ANR-11-IDEX-0005-02] FX We acknowledge the use of the Smithsonian Institution High Performance Cluster (SI/HPC) for spectral fitting. We also thank Jeff McClintock, Ramesh Narayan, Javier Garcia, and Malgosia Sobolewska for interesting and helpful discussions on the content of this paper. J.F.S. has been supported by NASA Einstein Fellowship grant PF5-160144. S.D.V. acknowledges partial support through a Smithsonian Institution CGPS grant. J.R. acknowledges financial support from the French Research National Agency: CHAOS project ANR-12-BS05-0009 (http://www.chaos-project.fr). P.V. and J.R. acknowledge financial support from the UnivEarthS Labex program at Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). NR 99 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 MAY 10 PY 2016 VL 822 IS 2 AR 60 DI 10.3847/0004-637X/822/2/60 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6RZ UT WOS:000377204900003 ER PT J AU Rosenfield, P Marigo, P Girardi, L Dalcanton, JJ Bressan, A Williams, BF Dolphin, A AF Rosenfield, Philip Marigo, Paola Girardi, Leo Dalcanton, Julianne J. Bressan, Alessandro Williams, Benjamin F. Dolphin, Andrew TI EVOLUTION OF THERMALLY PULSING ASYMPTOTIC GIANT BRANCH STARS. V. CONSTRAINING THE MASS LOSS AND LIFETIMES OF INTERMEDIATE-MASS, LOW-METALLICITY AGB STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: dwarf; galaxies: stellar content; stars: AGB and post-AGB; stars: evolution; stars: general; stars: mass-loss ID LARGE-MAGELLANIC-CLOUD; COLOR-MAGNITUDE DIAGRAMS; FORMATION HISTORIES; STELLAR EVOLUTION; TP-AGB; SYNTHETIC PHOTOMETRY; POPULATION SYNTHESIS; SURROUNDING FIELDS; DWARF GALAXIES; OUTER DISK AB Thermally pulsing asymptotic giant branch (TP-AGB) stars are relatively short lived (less than a few Myr), yet their cool effective temperatures, high luminosities, efficient mass loss, and dust production can dramatically affect the chemical enrichment histories and the spectral energy distributions of their host galaxies. The ability to accurately model TP-AGB stars is critical to the interpretation of the integrated light of distant galaxies, especially in redder wavelengths. We continue previous efforts to constrain the evolution and lifetimes of TP-AGB stars by modeling their underlying stellar populations. Using Hubble Space Telescope (HST) optical and near-infrared photometry taken of 12 fields of 10 nearby galaxies imaged via the Advanced Camera for Surveys Nearby Galaxy Survey Treasury and the near-infrared HST/SNAP follow-up campaign, we compare the model and observed TP-AGB luminosity functions as well as the ratio of TP-AGB to red giant branch stars. We confirm the best-fitting mass-loss prescription, introduced by Rosenfield et al., in which two different wind regimes are active during the TP-AGB, significantly improves models of many galaxies that show evidence of recent star formation. This study extends previous efforts to constrain TP-AGB lifetimes to metallicities ranging -1.59 less than or similar to [Fe/H] <= -0.56 and initial TP-AGB masses up to similar to 4 M-circle dot, which include TP-AGB stars that undergo hot-bottom burning. C1 [Rosenfield, Philip] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Rosenfield, Philip; Marigo, Paola] Univ Padua, Dept Phys & Astron G Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy. [Girardi, Leo] Osservatorio Astron Padova INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Dalcanton, Julianne J.; Williams, Benjamin F.] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. [Bressan, Alessandro] SISSA, Astrophys Sector, Via Bonomea 265, I-34136 Trieste, Italy. [Dolphin, Andrew] Raytheon Co, 1151 East Hermans Rd, Tucson, AZ 85756 USA. RP Rosenfield, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Rosenfield, P (reprint author), Univ Padua, Dept Phys & Astron G Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy. OI Rosenfield, Philip/0000-0001-9306-6049 FU ERC [615604]; Progetto di Ateneo, University of Padova [CPDA125588/12]; National Science Foundation [1501205] FX We acknowledge the support from the ERC Consolidator Grant funding scheme ( project STARKEY, G. A. n. 615604), and from Progetto di Ateneo 2012, University of Padova, ID: CPDA125588/12. All figures in this paper were produced using matplotlib ( Hunter 2007). This research made use of Astropy, a community-developed core Python package for Astronomy Astropy Collaboration et al. ( 2013). This material is based upon work supported by the National Science Foundation under Award No. 1501205. NR 76 TC 13 Z9 13 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2016 VL 822 IS 2 AR 73 DI 10.3847/0004-637X/822/2/73 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6RZ UT WOS:000377204900016 ER PT J AU Strandet, ML Weiss, A Vieira, JD de Breuck, C Aguirre, JE Aravena, M Ashby, MLN Bethermin, M Bradford, CM Carlstrom, JE Chapman, SC Crawford, TM Everett, W Fassnacht, CD Furstenau, RM Gonzalez, AH Greve, TR Gullberg, B Hezaveh, Y Kamenetzky, JR Litke, K Ma, J Malkan, M Marrone, DP Menten, KM Murphy, EJ Nadolski, A Rotermund, KM Spilker, JS Stark, AA Welikala, N AF Strandet, M. L. Weiss, A. Vieira, J. D. de Breuck, C. Aguirre, J. E. Aravena, M. Ashby, M. L. N. Bethermin, M. Bradford, C. M. Carlstrom, J. E. Chapman, S. C. Crawford, T. M. Everett, W. Fassnacht, C. D. Furstenau, R. M. Gonzalez, A. H. Greve, T. R. Gullberg, B. Hezaveh, Y. Kamenetzky, J. R. Litke, K. Ma, J. Malkan, M. Marrone, D. P. Menten, K. M. Murphy, E. J. Nadolski, A. Rotermund, K. M. Spilker, J. S. Stark, A. A. Welikala, N. TI THE REDSHIFT DISTRIBUTION OF DUSTY STAR-FORMING GALAXIES FROM THE SPT SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; early universe; galaxies: evolution; galaxies: high-redshift; ISM: molecules ID DEEP-FIELD-SOUTH; SUBMILLIMETER GALAXIES; MOLECULAR GAS; FORMATION HISTORY; NUMBER COUNTS; POLE TELESCOPE; LABOCA SURVEY; ALMA SURVEY; BAND; EMISSION AB We use the Atacama Large Millimeter/submillimeter Array (ALMA) in Cycle 1 to determine spectroscopic redshifts of high-redshift dusty star-forming galaxies (DSFGs) selected by their 1.4 mm continuum emission in the South Pole Telescope (SPT) survey. We present ALMA 3 mm spectral scans between 84 and 114 GHz for 15 galaxies and targeted ALMA 1 mm observations for an additional eight sources. Our observations yield 30 new line detections from CO, [CI], [NII], H2O and NH3. We further present Atacama Pathfinder Experiment [CII] and CO mid-J observations for seven sources for which only a single line was detected in spectral-scan data from ALMA Cycle 0 or Cycle 1. We combine the new observations with previously published and new millimeter/submillimeter line and photometric data of the SPT-selected DSFGs to study their redshift distribution. The combined data yield 39 spectroscopic redshifts from molecular lines, a success rate of >85%. Our sample represents the largest data set of its kind today and has the highest spectroscopic completeness among all redshift surveys of high-z DSFGs. The median of the redshift distribution is z = 3.9 +/- 0.4, and the highest-redshift source in our sample is at z = 5.8. We discuss how the selection of our sources affects the redshift distribution, focusing on source brightness, selection wavelength, and strong gravitational lensing. We correct for the effect of gravitational lensing and find the redshift distribution for 1.4 mm selected sources with a median redshift of z = 3.1 +/- 0.3. Comparing to redshift distributions selected at shorter wavelengths from the literature, we show that selection wavelength affects the shape of the redshift distribution. C1 [Strandet, M. L.; Weiss, A.; Menten, K. M.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Vieira, J. D.; Furstenau, R. M.; Nadolski, A.] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [de Breuck, C.; Bethermin, M.; Gullberg, B.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [de Breuck, C.; Bethermin, M.; Gullberg, B.] Univ Illinois, Dept Phys, 1002 W Green St, Urbana, IL 61801 USA. [Aguirre, J. E.] Univ Penn, 209 South 33rd St, Philadelphia, PA 19104 USA. [Aravena, M.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Av Ejercito 441, Santiago, Chile. [Ashby, M. L. N.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Bradford, C. M.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Carlstrom, J. E.; Crawford, T. M.] Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Carlstrom, J. E.] Univ Chicago, Dept Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Carlstrom, J. E.] Univ Chicago, Enrico Fermi Inst, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Chapman, S. C.; Rotermund, K. M.] Dalhousie Univ, Halifax, NS, Canada. [Everett, W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Everett, W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Fassnacht, C. D.] Univ Calif Davis, Dept Phys, One Shields Ave, Davis, CA 95616 USA. [Gonzalez, A. H.; Ma, J.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Greve, T. R.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Hezaveh, Y.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Kamenetzky, J. R.; Litke, K.; Marrone, D. P.; Spilker, J. S.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Murphy, E. J.] CALTECH, Infrared Proc & Anal Ctr, MC 220-6, Pasadena, CA 91125 USA. [Welikala, N.] Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. RP Strandet, ML (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. OI De Breuck, Carlos/0000-0002-6637-3315; Aguirre, James/0000-0002-4810-666X; Stark, Antony/0000-0002-2718-9996 FU International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne; FONDECYT [1140099]; U.S. National Science Foundation [AST-1312950]; Herschel [OT1_jvieira_4, DDT_mstrande_1]; Commonwealth of Australia; VLT/X-Shooter under the ESO project [E-092.A-0503(A)]; National Science Foundation [PLR-1248097]; Kavli Foundation; Gordon and Betty Moore Foundation [GBMF 947]; [E-086. A-0793A-2010]; [M-085.F-0008-2010]; [M-087.F-0015-2011]; [M-091.F-0031-2013]; [E-094.A-0712A-2014]; [M-095.F-0028-2015]; [E-096.A-0939A-2015]; [PHY-1125897] FX M.L.S. was supported for this research through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. M.A. acknowledges partial support from FONDECYT through grant 1140099. J.D.V., K.C.L., D.P.M., and J.S.S. acknowledge support from the U.S. National Science Foundation under grant No. AST-1312950. This paper makes use of the following ALMA data: ADS/JAO. ALMA# 2012.1.00844.S, 2012.1.00994.S, 2011.0.00957.S, and 2011.0.00958.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. This work is based in part on observations made with Herschel under program IDs OT1_jvieira_4 and DDT_mstrande_1. Herschel is a European Space Agency Cornerstone Mission with significant participation by NASA. We also use data from the Atacama Pathfinder Experiment under program IDs E-086. A-0793A-2010, M-085.F-0008-2010, M-087.F-0015-2011, M-091.F-0031-2013, E-094.A-0712A-2014, M-095.F-0028-2015, E-096.A-0939A-2015. APEX is a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. We have also used data from VLT/X-Shooter under the ESO project ID E-092.A-0503(A). The SPT is supported by the National Science Foundation through grant PLR-1248097, with partial support through PHY-1125897, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. NR 65 TC 7 Z9 7 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 MAY 10 PY 2016 VL 822 IS 2 AR 80 DI 10.3847/0004-637X/822/2/80 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6RZ UT WOS:000377204900023 ER PT J AU Svoboda, BE Shirley, YL Battersby, C Rosolowsky, EW Ginsburg, AG Ellsworth-Bowers, TP Pestalozzi, MR Dunham, MK Evans, NJ Bally, J Glenn, J AF Svoboda, Brian E. Shirley, Yancy L. Battersby, Cara Rosolowsky, Erik W. Ginsburg, Adam G. Ellsworth-Bowers, Timothy P. Pestalozzi, Michele R. Dunham, Miranda K. Evans, Neal J., II Bally, John Glenn, Jason TI THE BOLOCAM GALACTIC PLANE SURVEY. XIV. PHYSICAL PROPERTIES OF MASSIVE STARLESS AND STAR-FORMING CLUMPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: molecules; masers; stars: formation; submillimeter: ISM; surveys ID INFRARED-DARK CLOUDS; YOUNG STELLAR OBJECTS; 6.7-GHZ METHANOL MASERS; FOLLOW-UP CATALOG; MSX SOURCE SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; PRE-PROTOSTELLAR CORES; EXTENDED GREEN OBJECTS; DUST CONTINUUM SOURCES; HI-GAL SURVEY AB We sort 4683 molecular clouds between 10 degrees < l < 65 degrees from the Bolocam Galactic Plane Survey based on observational diagnostics of star formation activity: compact 70 mu m sources, mid-IR color-selected YSOs, H2O and CH3OH masers, and UCH II. regions. We also present a combined NH3-derived gas kinetic temperature and H2O maser catalog for 1788 clumps from our own GBT 100 m observations and from the literature. We identify a subsample of 2223 (47.5%) starless clump candidates (SCCs), the largest and most robust sample identified from a blind survey to date. Distributions of flux density, flux concentration, solid angle, kinetic temperature, column density, radius, and mass show strong (>1 dex) progressions when sorted by star formation indicator. The median SCC is marginally subvirial (alpha similar to 0.7) with >75% of clumps with known distance being gravitationally bound (alpha < 2). These samples show a statistically significant increase in the median clump mass of Delta M similar to 170-370 M-circle dot from the starless candidates to clumps associated with protostars. This trend could be due to (i) mass growth of the clumps at (M) over dot similar to 200-440 M-circle dot Myr(-1) for an average freefall 0.8 Myr timescale, (ii) a systematic factor of two increase in dust opacity from starless to protostellar phases, and/or (iii). a variation in the ratio of starless to protostellar clump lifetime that scales as similar to M-0.4. By comparing to the observed number of CH3OH maser containing clumps, we estimate the phase. lifetime of massive (M > 10(3) M-circle dot) starless clumps to be 0.37 +/- 0.08 Myr (M/10(3) M-circle dot)(-1); the majority (M < 450 M-circle dot) have phase. lifetimes longer than their average freefall time. C1 [Svoboda, Brian E.; Shirley, Yancy L.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [Shirley, Yancy L.] Natl Radio Astron Observ, Charlottesville, VA USA. [Battersby, Cara] Univ Alberta, Dept Phys, 4-181 CCIS, Edmonton, AB T6G 2E1, Canada. [Rosolowsky, Erik W.] Univ Colorado, CASA, 389 UCB, Boulder, CO 80309 USA. [Ginsburg, Adam G.] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Ginsburg, Adam G.; Ellsworth-Bowers, Timothy P.; Bally, John; Glenn, Jason] Univ Gothenburg, SE-41296 Gothenburg, Sweden. [Pestalozzi, Michele R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Dunham, Miranda K.] Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. [Evans, Neal J., II] Univ Texas Austin, Dept Astron, 2515 Speedway,Stop C1400, Austin, TX 78712 USA. RP Svoboda, BE (reprint author), Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. EM svobodb@email.arizona.edu OI Evans , Neal/0000-0001-5175-1777; Rosolowsky, Erik/0000-0002-5204-2259 FU National Science Foundation [DGE-1143953]; NSF [AST-1008577, AST-1410190, AST-1109116]; NSERC of Canada FX We sincerely thank the observatory staff at the Green Bank Telescope for their help during observing. We also sincerely thank Shari Breen for sharing coordinates to the MMB catalog between 20 degrees < l < 60 degrees prior to publication. We would also like to thank Julia Kamenetzky and Kimberly Ward-Duong for many useful comments that benefited this paper. B.E.S. was supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1143953. Y.L.S. and B.E.S. were supported in part by the NSF Grants AST-1008577 and AST-1410190. N.J.E. was supported by NSF grant AST-1109116 to the University of Texas at Austin. E.W.R. was supported by a Discovery Grant from NSERC of Canada. NR 145 TC 2 Z9 2 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 MAY 10 PY 2016 VL 822 IS 2 AR 59 DI 10.3847/0004-637X/822/2/59 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6RZ UT WOS:000377204900002 ER PT J AU Gianninas, A Curd, B Fontaine, G Brown, WR Kilic, M AF Gianninas, A. Curd, Brandon Fontaine, G. Brown, Warren R. Kilic, Mukremin TI DISCOVERY OF THREE PULSATING, MIXED-ATMOSPHERE, EXTREMELY LOW-MASS WHITE DWARF PRECURSORS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE asteroseismology; stars: individual (SDSS J075610.71+670424.7, SDSS J114155.56+385003.0, SDSS J115734.46+054645.6); techniques: photometric; white dwarfs ID RED-GIANT STAR; EVOLUTIONARY SEQUENCES; INSTABILITY STRIP; ZZ CETI; BINARY; FRAME; BRIGHT; MODES; RICH AB We report the discovery of pulsations in three mixed-atmosphere, extremely low-mass white dwarf (ELM WD, M <= 0.3M(circle dot)) precursors. Following the recent discoveries of pulsations in both ELM and pre-ELM WDs, we targeted pre-ELM WDs with mixed H/He atmospheres with high-speed photometry. We find significant optical variability in all three observed targets with periods in the range 320-590 s, consistent in timescale with theoretical predictions of p-mode pulsations in mixed-atmosphere approximate to 0.18M(circle dot) He-core pre-ELM WDs. This represents the first empirical evidence that pulsations in pre-ELM WDs can only occur if a significant amount of He is present in the atmosphere. Future, more extensive, timeseries photometry of the brightest of the three new pulsators offers an excellent opportunity to constrain the thickness of the surface H layer, which regulates the cooling timescales for ELM WDs. C1 [Gianninas, A.; Curd, Brandon; Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. [Fontaine, G.] Univ Montreal, Dept Phys, CP 1628, Montreal, PQ H3C 3J7, Canada. [Brown, Warren R.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. 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 OI Gianninas, Alexandros/0000-0002-8655-4308 FU NSF [AST-1312678]; NASA [NNX14AF65G]; Natural Sciences and Engineering Research Council of Canada; Smithsonian Institution FX A.G. and M.K. gratefully acknowledge the support of the NSF under grant AST-1312678, and NASA under grant NNX14AF65G. This work was supported in part by the Natural Sciences and Engineering Research Council of Canada. G.F. also acknowledges the contribution of the Canada Research Chair Program. This work was supported in part by the Smithsonian Institution. NR 30 TC 2 Z9 2 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 MAY 10 PY 2016 VL 822 IS 2 AR L27 DI 10.3847/2041-8205/822/2/L27 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DM2JQ UT WOS:000376173300007 ER PT J AU Miller, SH Breitburg, DL Burrell, RB Keppel, AG AF Miller, Seth H. Breitburg, Denise L. Burrell, Rebecca B. Keppel, Andrew G. TI Acidification increases sensitivity to hypoxia in important forage fishes SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Diel cycling; Estuaries; Menidia; Aquatic surface respiration; Ventilation ID AQUATIC SURFACE RESPIRATION; OCEAN ACIDIFICATION; DISSOLVED-OXYGEN; CLIMATE-CHANGE; O-2 CHEMORECEPTORS; CARBON-DIOXIDE; IMPACTS; ADAPTATION; RESPONSES; WATER AB Hypoxia (low dissolved oxygen [DO]) and CO2-induced acidification are important aquatic stressors that are exacerbated by anthropogenic nutrient inputs and are expected to increase in severity with increasing atmospheric CO2 and higher global temperatures. Understanding how species respond to changes in DO and pH is critical to predicting how climate change will affect estuarine ecosystems, including the extreme shallow margins of these systems, where factors such as respiration, photosynthesis, and tides create daily fluctuations of DO and pH, and strong correlations between the 2 stressors. To determine how acidification affects the sensitivity to hypoxia of 2 important forage fishes, the silversides Menidia menidia and M. beryllina, we recorded opercula ventilation rates, aquatic surface respiration (ASR, where fish breathe in the oxygenated surface layer during hypoxic events), and mortality as we lowered either DO or both DO and pH simultaneously. Fish subjected to low DO and low pH in the laboratory performed ASR and died at higher DO concentrations than fish subjected only to hypoxia. Additionally, fish beat their opercula slower, which may have contributed to the differences in ASR and mortality that we saw. These results indicate acidification can increase mortality under hypoxia not only directly but also indirectly by increasing vulnerability to predation during increased use of ASR. C1 [Miller, Seth H.; Breitburg, Denise L.; Burrell, Rebecca B.; Keppel, Andrew G.] Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. RP Miller, SH (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM millerseth@si.edu FU Smithsonian Postdoctoral Fellowship award; Coastal Ocean Research grant [NA10NOS4780138] FX We thank A. Collier, D. Comba, and W. McBurney for assistance with field collections and laboratory observations. C. Lord and J. Behrens provided useful comments on the manuscript, and A. Reynolds analyzed our alkalinity samples. Fish were collected under a scientific collection permit from the Maryland Department of Natural Resources Fisheries Service. This work was funded by a Smithsonian Postdoctoral Fellowship award to S.H.M. and a NOAA Center for Sponsored Coastal Ocean Research grant (NA10NOS4780138) to D.L.B. NR 45 TC 0 Z9 0 U1 14 U2 35 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD MAY 10 PY 2016 VL 549 BP 1 EP 8 DI 10.3354/meps11695 PG 8 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA DM5GR UT WOS:000376376200001 ER PT J AU Ben Toh, K Ng, CSL Leong, WKG Jaafar, Z Chou, LM AF Ben Toh, Kok Ng, Chin Soon Lionel Leong, Wai-Kit Gavan Jaafar, Zeehan Chou, Loke Ming TI Assemblages and diversity of fishes in Singapore's marinas SO RAFFLES BULLETIN OF ZOOLOGY LA English DT Article; Proceedings Paper CT Biodiversity Research Symposium CY MAY 24, 2014 CL Singapore, SINGAPORE SP Natl Univ Singapore, Natl Pk DE fish diversity; marinas; refugia; modified coastal habitats; Singapore ID COASTAL HABITATS; ENVIRONMENT; ESTUARIES; STRAIT; WATERS; REEFS AB Singapore's coastal environment has been extensively transformed by numerous development projects since the 1960s. However, fish diversity remains relatively high despite the extent of anthropogenic modifications to these environments. The diversity and abundance of fishes supported by recreational marinas in Singapore was examined in this study. Custom-made fish traps were deployed at ONE degrees 15 Marina Club (OMC), Marina at Keppel Bay (MKB) and Raffles Marina (RM). A total of 49 species from 31 families were documented. The average number of fishes caught and the Margalef Diversity index were highest in RM while MKB had the highest evenness and Shannon index. Raffles Marina harbored many estuarine species such as Arius oetik and Etroplus suratensis, while reef-associated species such as chaetodontids and pomacentrids inhabited MKB and OMC. Our findings supplemented ichthyological surveys carried out from 2004 to 2014, which when combined, generated an updated list of over 105 species from 48 families inhabiting recreational marinas in Singapore. The results indicate that marinas in Singapore can support and sustain diverse fish assemblages, and can potentially play important roles for marine conservation in human-modified coastal areas. C1 [Ben Toh, Kok; Ng, Chin Soon Lionel; Leong, Wai-Kit Gavan; Jaafar, Zeehan] Natl Univ Singapore, Dept Biol Sci, 14 Sci Dr 4, Singapore 117543, Singapore. [Ben Toh, Kok; Ng, Chin Soon Lionel; Chou, Loke Ming] Natl Univ Singapore, Trop Marine Sci Inst, 18 Kent Ridge Rd, Singapore 119227, Singapore. [Jaafar, Zeehan] Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, 10th & Constitut Ave NW, Washington, DC 20560 USA. RP Ben Toh, K (reprint author), Natl Univ Singapore, Dept Biol Sci, 14 Sci Dr 4, Singapore 117543, Singapore.; Ben Toh, K (reprint author), Natl Univ Singapore, Trop Marine Sci Inst, 18 Kent Ridge Rd, Singapore 119227, Singapore. EM tmstohkb@nus.edu.sg OI Ng, Lionel/0000-0003-2700-3474 FU National Parks Board [R-154-000-557-490] FX We are grateful to members of the Reef Ecology Laboratory, NUS, for their tireless enthusiasm and assistance with field work. Low Inn Zheng and Toh Tai Chong were instrumental to the completion of the study. We thank Kelvin Lim and Tan Heok Hui for assistance in fish identification, and the staff of Raffles Marina, ONEo15 Marina Club and Marina at Keppel Bay for all help rendered in the course of this study. This study was supported by the National Parks Board (grant number R-154-000-557-490). NR 47 TC 0 Z9 0 U1 0 U2 0 PU NATL UNIV SINGAPORE, SCHOOL BIOLOGICAL SCIENCES PI SINGAPORE PA DEPT ZOOLOGY, KENT RIDGE, SINGAPORE 0511, SINGAPORE SN 0217-2445 J9 RAFFLES B ZOOL JI Raffles Bull. Zool. PD MAY 6 PY 2016 SU 32 BP 85 EP 94 PG 10 WC Zoology SC Zoology GA EJ4UV UT WOS:000393213400006 ER PT J AU Miranda, LS Hirano, YM Mills, CE Falconer, A Fenwick, D Marques, AC Collins, AG AF Miranda, Lucilia S. Hirano, Yayoi M. Mills, Claudia E. Falconer, Audrey Fenwick, David Marques, Antonio C. Collins, Allen G. TI Systematics of stalked jellyfishes (Cnidaria: Staurozoa) SO PEERJ LA English DT Article DE Evolution; Taxonomy; Phylogeny; Medusozoa; Stauromedusae ID PHYLUM-CNIDARIA; PHYLOGENETIC PLACEMENT; MOLECULAR EVIDENCE; NORTHEAST PACIFIC; RDNA DATA; SCYPHOZOA; STAUROMEDUSAE; MODELS; INVERTEBRATES; REASSESSMENT AB Staurozoan classification is highly subjective, based on phylogeny-free inferences, and suborders, families, and genera are commonly defined by homoplasies. Additionally, many characters used in the taxonomy of the group have ontogenetic and intraspecific variation, and demand new and consistent assessments to establish their correct homologies. Consequently, Staurozoa is in need of a thorough systematic revision. The aim of this study is to propose a comprehensive phylogenetic hypothesis for Staurozoa, providing the first phylogenetic classification for the group. According to our working hypothesis based on a combined set of molecular data (mitochondrial markers COI and 16S, and nuclear markers ITS, 18S, and 28S), the traditional suborders Cleistocarpida (animals with claustrum) and Eleutherocarpida (animals without claustrum) are not monophyletic. Instead, our results show that staurozoans are divided into two groups, herein named Amyostaurida and Myostaurida, which can be distinguished by the absence/presence of interradial longitudinal muscles in the peduncle, respectively. We propose a taxonomic revision at the family and genus levels hat preserves the monophyly of taxa. We provide a key for staurozoan genera and discuss the evolution of the main characters used in staurozoan taxonomy. C1 [Miranda, Lucilia S.; Marques, Antonio C.] Univ Sao Paulo, Inst Biociencias, Dept Zool, Sao Paulo, Brazil. [Hirano, Yayoi M.] Nat Hist Museum & Inst, Coastal Branch, Katsuura, Chiba, Japan. [Mills, Claudia E.] Univ Washington, Friday Harbor Labs, Friday Harbor, WA 98250 USA. [Mills, Claudia E.] Univ Washington, Dept Biol, Friday Harbor, WA USA. [Falconer, Audrey] Field Naturalists Club Victoria, Marine Res Grp, Melbourne, Vic, Australia. [Falconer, Audrey] Museum Victoria, Dept Sci, Melbourne, Vic, Australia. [Marques, Antonio C.] Univ Sao Paulo, Ctr Biol Marinha, Sao Paulo, Brazil. [Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Natl Systemat Lab, Natl Marine Fisheries Serv, Washington, DC 20560 USA. RP Miranda, LS (reprint author), Univ Sao Paulo, Inst Biociencias, Dept Zool, Sao Paulo, Brazil. EM mirandals@ib.usp.br RI Marques, Antonio/E-8049-2011; Miranda, Lucilia/L-4930-2015 OI Marques, Antonio/0000-0002-2884-0541; FU FAPESP [2010/07362-7, 2010/52324-6, 2011/50242-5, 2013/50484-4]; CNPq [474672/2007-7, 142270/2010-5, 563106/2010-7, 562143/2010-6, 477156/2011-8, 305805/2013-4, 165066/2014-8, 445444/2014-2]; CAPES/PDSE [16499/12-3]; NSF [AToL EF-0531779] FX This study was supported by FAPESP 2010/07362-7 (LSM), 2010/52324-6 (ACM), 2011/50242-5 (ACM), 2013/50484-4 (ACM); CNPq 474672/2007-7 (ACM), 142270/2010-5 (LSM), 563106/2010-7 (ACM), 562143/2010-6 (ACM), 477156/2011-8 (ACM), 305805/2013-4 (ACM), 165066/2014-8 (LSM), 445444/2014-2 (ACM); CAPES/PDSE: 16499/12-3 (LSM); and NSF Grant AToL EF-0531779 (to P. Cartwright, AGC, and D. Fautin). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 114 TC 6 Z9 6 U1 7 U2 11 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD MAY 5 PY 2016 VL 4 AR e1951 DI 10.7717/peerj.1951 PG 48 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DM7GX UT WOS:000376526900005 PM 27168970 ER PT J AU O'Brien, SJ Koepfli, KP Eizirik, E Johnson, W Driscoll, C Antunes, A Schmidt-Kuntzel, A Marker, L Dobrynin, P AF O'Brien, Stephen J. Koepfli, Klaus Peter Eizirik, Eduardo Johnson, Warren Driscoll, Carlos Antunes, Agostinho Schmidt-Kuntzel, Anne Marker, Laurie Dobrynin, Pavel TI Response to Comment by Faurby, Werdelin and Svenning SO GENOME BIOLOGY LA English DT Article ID PUMA PUMA-CONCOLOR; CHEETAH-LIKE CAT; AMERICAN; FELIDAE; EVOLUTION C1 [O'Brien, Stephen J.; Koepfli, Klaus Peter; Dobrynin, Pavel] St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, 41A Sredniy Ave, St Petersburg 199004, Russia. [O'Brien, Stephen J.] Nova SE Univ, Oceanog Ctr, 8000 N Ocean Dr, Ft Lauderdale, FL 33004 USA. [Koepfli, Klaus Peter] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA. [Eizirik, Eduardo] Pontificia Univ Catolica Rio Grande do Sul, Fac Biociencias, Lab Biol Genom & Mol, Inst Procarivoros, BR-90619900 Porto Alegre, RS, Brazil. [Driscoll, Carlos] NIAAA, Neurogenet Lab, 5625 Fishers Lane, Rockville, MD 20852 USA. [Antunes, Agostinho] Univ Porto, Fac Sci, Dept Biol, Rua Campo, P-4169007 Oporto, Portugal. [Schmidt-Kuntzel, Anne] Cheetah Conservat Fund, Life Technol Conservat Genet Lab, Otjiwarongo 9000, Namibia. [Schmidt-Kuntzel, Anne; Marker, Laurie] Cheetah Conservat Fund, Otjiwarongo 9000, Namibia. RP O'Brien, SJ (reprint author), St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, 41A Sredniy Ave, St Petersburg 199004, Russia.; O'Brien, SJ (reprint author), Nova SE Univ, Oceanog Ctr, 8000 N Ocean Dr, Ft Lauderdale, FL 33004 USA. EM lgdchief@gmail.com RI Eizirik, Eduardo/K-8034-2012; OI Eizirik, Eduardo/0000-0002-9658-0999; Driscoll, Carlos/0000-0003-2392-505X NR 14 TC 0 Z9 0 U1 3 U2 4 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1465-6906 EI 1474-760X J9 GENOME BIOL JI Genome Biol. PD MAY 5 PY 2016 VL 17 AR 90 DI 10.1186/s13059-016-0942-z PG 3 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA DL9KX UT WOS:000375962600003 PM 27150130 ER PT J AU Sun, Y Huang, Y Li, XF Baldwin, CC Zhou, ZC Yan, ZX Crandall, KA Zhang, Y Zhao, XM Wang, M Wong, A Fang, C Zhang, XH Huang, H Lopez, JV Kilfoyle, K Zhang, Y Orti, G Venkatesh, B Shi, Q AF Sun, Ying Huang, Yu Li, Xiaofeng Baldwin, Carole C. Zhou, Zhuocheng Yan, Zhixiang Crandall, Keith A. Zhang, Yong Zhao, Xiaomeng Wang, Min Wong, Alex Fang, Chao Zhang, Xinhui Huang, Hai Lopez, Jose V. Kilfoyle, Kirk Zhang, Yong Orti, Guillermo Venkatesh, Byrappa Shi, Qiong TI Fish-T1K (Transcriptomes of 1,000 Fishes) Project: large-scale transcriptome data for fish evolution studies SO GIGASCIENCE LA English DT Editorial Material DE Fish-T1K; Fish; Transcriptome; RNA; Database; Biodiversity AB Ray-finned fishes (Actinopterygii) represent more than 50 % of extant vertebrates and are of great evolutionary, ecologic and economic significance, but they are relatively underrepresented in 'omics studies. Increased availability of transcriptome data for these species will allow researchers to better understand changes in gene expression, and to carry out functional analyses. An international project known as the "Transcriptomes of 1,000 Fishes" (Fish-T1K) project has been established to generate RNA-seq transcriptome sequences for 1,000 diverse species of ray-finned fishes. The first phase of this project has produced transcriptomes from more than 180 ray-finned fishes, representing 142 species and covering 51 orders and 109 families. Here we provide an overview of the goals of this project and the work done so far. C1 [Sun, Ying; Zhang, Yong] Sun Yat Sen Univ, State Key Lab Biocontrol, Inst Aquat Econ Anim, Guangzhou 510275, Guangdong, Peoples R China. [Sun, Ying; Zhang, Yong] Sun Yat Sen Univ, Guangdong Prov Key Lab Aquat Econ Anim, Sch Life Sci, Guangzhou 510275, Guangdong, Peoples R China. [Sun, Ying; Huang, Yu; Li, Xiaofeng; Zhang, Yong; Zhao, Xiaomeng; Wang, Min; Fang, Chao; Zhang, Xinhui; Shi, Qiong] BGI, Shenzhen Key Lab Marine Genom, Guangdong Prov Key Lab Mol Breeding Marine Econ A, Shenzhen 518083, Peoples R China. [Baldwin, Carole C.] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. [Zhou, Zhuocheng] China Fisheries Assoc, Beijing 100000, Peoples R China. [Yan, Zhixiang] China Natl Genebank, Shenzhen 518083, Peoples R China. [Crandall, Keith A.; Orti, Guillermo] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Wang, Min; Shi, Qiong] BGI Zhenjiang Inst Hydrobiol, Zhenjiang 212000, Peoples R China. [Wong, Alex] BGI Hong Kong, Hong Kong 999077, Hong Kong, Peoples R China. [Huang, Hai] Sanya Sci & Technol Acad Crop Winter Multiplicat, Haikou 572000, Hainan, Peoples R China. [Lopez, Jose V.; Kilfoyle, Kirk] Nova SE Univ, Oceanog Ctr, Ft Lauderdale, FL 33004 USA. [Venkatesh, Byrappa] ASTAR, Inst Mol & Cell Biol, Singapore 138673, Singapore. [Shi, Qiong] Shenzhen Univ, Coll Life Sci, Shenzhen 518060, Peoples R China. RP Sun, Y (reprint author), Sun Yat Sen Univ, State Key Lab Biocontrol, Inst Aquat Econ Anim, Guangzhou 510275, Guangdong, Peoples R China.; Sun, Y (reprint author), Sun Yat Sen Univ, Guangdong Prov Key Lab Aquat Econ Anim, Sch Life Sci, Guangzhou 510275, Guangdong, Peoples R China.; Sun, Y; Shi, Q (reprint author), BGI, Shenzhen Key Lab Marine Genom, Guangdong Prov Key Lab Mol Breeding Marine Econ A, Shenzhen 518083, Peoples R China.; Orti, G (reprint author), George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA.; Venkatesh, B (reprint author), ASTAR, Inst Mol & Cell Biol, Singapore 138673, Singapore. EM ying_sun09@icloud.com; gorti@email.gwu.edu; mcbbv@imcb.a-star.edu.sg; shiqiong@genomics.cn OI Venkatesh, Byrappa/0000-0003-3620-0277 NR 8 TC 2 Z9 2 U1 2 U2 9 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 2047-217X J9 GIGASCIENCE JI GigaScience PD MAY 3 PY 2016 VL 5 AR 18 DI 10.1186/s13742-016-0124-7 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DL5AY UT WOS:000375650300001 PM 27144000 ER PT J AU Kawada, R Buffington, ML AF Kawada, Ricardo Buffington, Matthew L. TI A Scalable and Modular Dome Illumination System for Scientific Microphotography on a Budget SO PLOS ONE LA English DT Article ID MICROSCOPE AB A scalable and modular LED illumination dome for microscopic scientific photography is described and illustrated, and methods for constructing such a dome are detailed. Dome illumination for insect specimens has become standard practice across the field of insect systematics, but many dome designs remain expensive and inflexible with respect to new LED technology. Further, a one-size-fits-all dome cannot accommodate the large breadth of insect size encountered in nature, forcing the photographer to adapt, in some cases, to a less than ideal dome design. The dome described here is scalable, as it is based on a isodecahedron, and the template for the dome is available as a downloaded file from the internet that can be printed on any printer, on the photographer's choice of media. As a result, a photographer can afford, using this design, to produce a series of domes of various sizes and materials, and LED ring lights of various sizes and color temperatures, depending on the need. C1 [Kawada, Ricardo] Fundacao Univ Fed Grande Dourados, Programa Posgrad Entomol & Conservacao Biodiversi, Rodovia Dourados Itahum,Km 12,Cidade Univ, BR-79804970 Dourados, MS, Brazil. [Buffington, Matthew L.] USDA ARS, Systemat Entomol Lab, Natl Museum Nat Hist, Smithsonian Inst, 10th & Constitut Ave NW,MRC 168,POB 30712, Washington, DC 20013 USA. RP Kawada, R (reprint author), Fundacao Univ Fed Grande Dourados, Programa Posgrad Entomol & Conservacao Biodiversi, Rodovia Dourados Itahum,Km 12,Cidade Univ, BR-79804970 Dourados, MS, Brazil. EM hyme.neo@gmail.com FU CNPq [151153/2013-2]; Systematic Entomology Laboratory, ARS-USDA FX RK was funded by a scholarship granted by CNPq, process number 151153/2013-2; MB was funded by the Systematic Entomology Laboratory, ARS-USDA. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 5 TC 1 Z9 1 U1 2 U2 3 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 3 PY 2016 VL 11 IS 5 AR e0153426 DI 10.1371/journal.pone.0153426 PG 20 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DL5KK UT WOS:000375675700009 PM 27138573 ER PT J AU Latmiral, L Armata, F Genoni, MG Pikovski, I Kim, MS AF Latmiral, Ludovico Armata, Federico Genoni, Marco G. Pikovski, Igor Kim, M. S. TI Probing anharmonicity of a quantum oscillator in an optomechanical cavity SO PHYSICAL REVIEW A LA English DT Article ID RADIATION-PRESSURE; PHASE ESTIMATION; MOVING MIRROR; MICROMIRROR; MECHANICS; STATES AB We present a way of measuring with high precision the anharmonicity of a quantum oscillator coupled to an optical field via radiation pressure. Our protocol uses a sequence of pulsed interactions to perform a loop in the phase space of the mechanical oscillator, which is prepared in a thermal state. We show how the optical field acquires a phase depending on the anharmonicity. Remarkably, one only needs small initial cooling of the mechanical motion to probe even small anharmonicities. Finally, by applying tools from quantum estimation theory, we calculate the ultimate bound on the estimation precision posed by quantum mechanics and compare it with the precision obtainable with feasible measurements such as homodyne and heterodyne detection on the cavity field. In particular we demonstrate that homodyne detection is nearly optimal in the limit of a large number of photons of the field and we discuss the estimation precision of small anharmonicities in terms of its signal-to-noise ratio. C1 [Latmiral, Ludovico; Armata, Federico; Kim, M. S.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Quantum Opt & Laser Sci Grp, London SW7 2BW, England. [Genoni, Marco G.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Pikovski, Igor] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Pikovski, Igor] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Latmiral, L; Armata, F (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Quantum Opt & Laser Sci Grp, London SW7 2BW, England. EM ludovico.latmiral@hotmail.it; f.armata@imperial.ac.uk OI Pikovski, Igor/0000-0002-9441-2553 FU EPSRC [EP/J014664/1, EP/K034480/1, EP/K026267/1]; Marie Curie Project [PITN-GA-2012-317232]; NSF FX The authors wish to thank Tommaso Tufarelli for useful discussions on the subject of this paper. M.S.K. acknowledges support from EPSRC through Grants No. EP/J014664/1 and No. EP/K034480/1. F.A. and M.S.K. acknowledge the financial support from the Marie Curie Project No. PITN-GA-2012-317232. M.G.G. acknowledges support from EPSRC through Grant No. EP/K026267/1. I.P. acknowledges support from the NSF through a grant to ITAMP. NR 49 TC 1 Z9 1 U1 3 U2 8 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 MAY 3 PY 2016 VL 93 IS 5 AR 052306 DI 10.1103/PhysRevA.93.052306 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA DL3HC UT WOS:000375523800004 ER PT J AU Temkin, I Printrakoon, C AF Temkin, Ilya Printrakoon, Cheewarat TI Morphology and taxonomy of Isognomon spathulatus (Reeve, 1858), a cryptic bivalve from the mangroves of Thailand SO ZOOTAXA LA English DT Article DE Anatomy; ecology; parapatry; pearls; Pterioidea; speciation ID CILIARY MECHANISMS; EVOLUTION; OYSTERS; INTERRELATIONSHIPS; LAMELLIBRANCHS; COMPETITION; DIVERSITY; EUTAMIAS; MOLLUSCA; MANTLE AB Isognomon spathulatus (Reeve, 1858) is redescribed based on type material and original collections from Kungkrabaen Bay, Thailand. The species agrees with previously described isognomonids in most conchological and anatomical features, but possesses a suite of diagnostic characters, including a comma-shaped outline of the nacreous border, an uncoiled ventral diverticulum of the stomach, and the thickened mantle lobes with granulated cells. This study is the most comprehensive morphological analysis to date for any species of Isognomonidae Woodring, 1925 (1828). It describes and illustrates a number of previously unrecognized or underutilized anatomical characters of potential phylogenetic significance: the morphology of the byssal threads (cross-sectional shape, plumate rootlets, and the shape of adhesive disks), the presence and extent of the interdemibranchial buttresses, the presence of secretory cells in the central zone of the mantle, the shape of the ventral diverticulum of the gastric chamber, the presence of the typhlosolar guard ridge, and the position of the renal pore. A comparison is made between I. spathulatus and morphologically similar Isognomon ephippium (Linnaeus, 1758) with which it has been previously synonymized. Pearls of both species are described and illustrated. Individuals of I. spathulatus inhabit mangroves, where they attach by byssus to prop roots, typically in parapatry with individuals of I. ephippium that occupy adjacent mudflats. The spacial distribution and diverging adaptive strategies (pertaining to physical stabilization and response to predation) displayed by the two isognomonid species are considered in the light of the ecological speciation theory. C1 [Temkin, Ilya] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012,MRC 163, Washington, DC 20013 USA. [Temkin, Ilya] No Virginia Community Coll, Dept Biol, 4001 Wakefield Chapel Rd, Annandale, VA 22003 USA. [Printrakoon, Cheewarat] Kasetsart Univ, Fac Sci, Dept Zool, Anim Systemat & Ecol Special Unit ASESRU, Bangkok 10900, Thailand. RP Temkin, I (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012,MRC 163, Washington, DC 20013 USA.; Temkin, I (reprint author), No Virginia Community Coll, Dept Biol, 4001 Wakefield Chapel Rd, Annandale, VA 22003 USA. EM temkini@si.edu FU NSF-PEET [DEB-9978119]; NSF [DEB-0508311]; Royal Golden Jubilee doctoral fellowship [4.B.MU/44/M.1]; Preproposal Research Fund; Visiting Professor grant, Faculty of Science, Kasetsart University, Bangkok, Thailand FX We thank B.I. Sirenko, A.V. Merkul'ev (the Zoological Institute, Russian Academy of Sciences, St. Petersburg, Russia), K.A. Lutaenko (A.V. Zhirmunsky Institute of Marine Biology, Far East Branch of the Russian Academy of Sciences, Vladivostok, Russia), E. Mekhova, S. Zvonareva, and Y.I. Kantor (A.N. Severtsov Institute of Ecology and Evolution, the Russian Academy of Sciences, Moscow, Russia) for assistance with I. spathulatus records from Vietnam. Kathie Way and A. Salvador (the Natural History Museum, London, United Kingdom) assisted with Reeve's type material; G. Rosenberg (Academy of Natural Sciences of Philadelphia) advised on nomenclatural issues. This study was initiated during the Second International Bivalve Workshop (Chantaburi, Kungkrabaen Bay, Thailand) and supported in part by NSF-PEET DEB-9978119 to R. Bieler and P.M. Mikkelsen. Additional sources of funding included the NSF doctoral dissertation improvement grant DEB-0508311 (to IT), the Royal Golden Jubilee doctoral fellowship (4.B.MU/44/M.1), the Preproposal Research Fund, and the Visiting Professor grant, Faculty of Science, Kasetsart University, Bangkok, Thailand (to CP). NR 122 TC 0 Z9 0 U1 2 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 MAY 2 PY 2016 VL 4107 IS 2 BP 141 EP 174 PG 34 WC Zoology SC Zoology GA DK9UB UT WOS:000375276000002 PM 27394812 ER PT J AU Tornabene, L Valdez, S Erdmann, MV Pezold, FL AF Tornabene, L. Valdez, S. Erdmann, M. V. Pezold, F. L. TI Multi-locus sequence data reveal a new species of coral reef goby (Teleostei: Gobiidae: Eviota), and evidence of Pliocene vicariance across the Coral Triangle SO JOURNAL OF FISH BIOLOGY LA English DT Article DE centre of overlap; dwarfgoby; Indo Australian Archipelago; Indo Malay Archipelago; systematics ID INDO-WEST PACIFIC; HISTORICAL BIOGEOGRAPHY; EVOLUTIONARY HISTORY; MOLECULAR PHYLOGENY; MARINE BIODIVERSITY; FISHES TELEOSTEI; SEA-LEVEL; PATTERNS; DIVERSITY; DISPERSAL AB Here, multi-locus sequence data are coupled with observations of live colouration to recognize a new species, Eviota punyit from the Coral Triangle, Indian Ocean and Red Sea. Relaxed molecular clock divergence time estimation indicates a Pliocene origin for the new species, and the current distribution of the new species and its sister species Eviota sebreei supports a scenario of vicariance across the Indo-Pacific Barrier, followed by subsequent range expansion and overlap in the Coral Triangle. These results are consistent with the 'centre of overlap' hypothesis, which states that the increased diversity in the Coral Triangle is due in part to the overlapping ranges of Indian Ocean and Pacific Ocean faunas. These findings are discussed in the context of other geminate pairs of coral reef fishes separated by the Indo-Pacific Barrier. (C) 2016 The Fisheries Society of the British Isles C1 [Tornabene, L.; Valdez, S.; Pezold, F. L.] Texas A&M Univ Corpus Christi, Coll Sci & Engn, 6300 Ocean Dr, Corpus Christi, TX 78412 USA. [Erdmann, M. V.] Conservat Int Indonesia Marine Program, Jl Dr Muwardi 17, Denpasar 80235, Bali, Indonesia. [Erdmann, M. V.] Calif Acad Sci, Dept Ichthyol, 55 Mus Concourse Dr,Golden Gate Pk, San Francisco, CA 94118 USA. [Tornabene, L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, PO Ox 37012,MRC 159, Washington, DC 20013 USA. RP Tornabene, L (reprint author), Texas A&M Univ Corpus Christi, Coll Sci & Engn, 6300 Ocean Dr, Corpus Christi, TX 78412 USA.; Tornabene, L (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, PO Ox 37012,MRC 159, Washington, DC 20013 USA. EM Luke.Tornabene@gmail.com FU Brunei Darussalam Department of Fisheries (Ministry of Industry and Primary Resources); American Museum of Natural History - Lerner Gray Award; Louis Stokes Alliance for Minority Participation; McNairs Scholars Program at Texas A&M University - Corpus Christi; Paine Family Trust; Walton Family Foundation; Henry Foundation FX We thank the Brunei Darussalam Department of Fisheries (Ministry of Industry and Primary Resources) for sponsoring the biodiversity survey that initially alerted us to the presence of E. punyit; specific thanks are due to P. D. S. S. A. H. Yahya, H. Ibrahim, R. Wahab, Z. Jolkifli and M. H. Juna. We thank G. Ahmadia and G. Allen, who helped collect and photograph many of the comparative specimens used in this study. R. Winterbottom, J. Randall, J. Greenfield and R. Field provided photographs of Eviota. D. Catania and D. Greenfield at California Academy of Sciences provided assistance with deposition of specimens. This project was funded in part by an American Museum of Natural History - Lerner Gray Award (L.T.), the Louis Stokes Alliance for Minority Participation (S.V.), the McNairs Scholars Program at Texas A&M University - Corpus Christi (S.V.), the Paine Family Trust (M.V.E.), the Walton Family Foundation (M.V.E.) and the Henry Foundation (M.V.E.). NR 71 TC 0 Z9 0 U1 3 U2 4 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 MAY PY 2016 VL 88 IS 5 BP 1811 EP 1834 DI 10.1111/jfb.12947 PG 24 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA DX3UL UT WOS:000384300800009 PM 27021219 ER PT J AU Gould, RR AF Gould, Roy R. TI Why does a ball fall?: A new visualization for Einstein's model of gravity SO AMERICAN JOURNAL OF PHYSICS LA English DT Article AB Many physics teachers seek a simple illustration of Einstein's model of gravity, suitable for the introductory physics classroom. In this article, we show that an ordinary wall map of the world can be used to contrast Newton's and Einstein's explanations for why a ball falls when released. Trajectories on the map are analogous to the trajectories of the ball through spacetime, because the geometry of the map is remarkably similar to the geometry of spacetime near Earth's surface. To aid in the pedagogy, we focus on the concept of scale rather than curvature. We show that, contrary to popular visualizations of Einstein's model, it is primarily the warping of time, not space, that causes a ball to fall, and we address the question of why we do not see the distortion of spacetime around us. Finally, we recover Newton's results for the falling ball from our geometrical treatment. (C) 2016 American Association of Physics Teachers. C1 [Gould, Roy R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Gould, RR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Aeronautics and Space Administration [NCC5-261] FX The author thanks Irwin Shapiro, Bruce Gregory, Phil Sadler, and the anonymous reviewers for their helpful suggestions. The author is also grateful to Edwin Taylor and the late John A. Wheeler for a lifetime of inspiration on problems of this sort. This work was supported in part by Grant NCC5-261 from the National Aeronautics and Space Administration. NR 13 TC 2 Z9 2 U1 1 U2 1 PU AMER ASSOC PHYSICS TEACHERS PI COLLEGE PARK PA ONE PHYSICS ELLIPSE, COLLEGE PARK, MD 20740-3845 USA SN 0002-9505 EI 1943-2909 J9 AM J PHYS JI Am. J. Phys. PD MAY PY 2016 VL 84 IS 5 BP 396 EP 402 DI 10.1119/1.4939927 PG 7 WC Education, Scientific Disciplines; Physics, Multidisciplinary SC Education & Educational Research; Physics GA DV6GB UT WOS:000383029700010 ER PT J AU Chazdon, RL Broadbent, EN Rozendaal, DMA Bongers, F Zambrano, AMA Aide, TM Balvanera, P Becknell, JM Boukili, V Brancalion, PHS Craven, D Almeida-Cortez, JS Cabral, GAL de Jong, B Denslow, JS Dent, DH DeWalt, SJ Dupuy, JM Duran, SM Espirito-Santo, MM Fandino, MC Cesar, RG Hall, JS Hernandez-Stefanoni, JL Jakovac, CC Junqueira, AB Kennard, D Letcher, SG Lohbeck, M Martinez-Ramos, M Massoca, P Meave, JA Mesquita, R Mora, F Munoz, R Muscarella, R Nunes, YRF Ochoa-Gaona, S Orihuela-Belmonte, E Pena-Claros, M Perez-Garcia, EA Piotto, D Powers, JS Rodriguez-Velazquez, J Romero-Perez, IE Ruiz, J Saldarriaga, JG Sanchez-Azofeifa, A Schwartz, NB Steininger, MK Swenson, NG Uriarte, M van Breugel, M van der Wal, H Veloso, MDM Vester, H Vieira, ICG Bentos, TV Williamson, GB Poorter, L AF Chazdon, Robin L. Broadbent, Eben N. Rozendaal, Danae M. A. Bongers, Frans Zambrano, Angelica Maria Almeyda Aide, T. Mitchell Balvanera, Patricia Becknell, Justin M. Boukili, Vanessa Brancalion, Pedro H. S. Craven, Dylan Almeida-Cortez, Jarcilene S. Cabral, George A. L. de Jong, Ben Denslow, Julie S. Dent, Daisy H. DeWalt, Saara J. Dupuy, Juan M. Duran, Sandra M. Espirito-Santo, Mario M. Fandino, Maria C. Cesar, Ricardo G. Hall, Jefferson S. Hernandez-Stefanoni, Jose Luis Jakovac, Catarina C. Junqueira, Andre B. Kennard, Deborah Letcher, Susan G. Lohbeck, Madelon Martinez-Ramos, Miguel Massoca, Paulo Meave, Jorge A. Mesquita, Rita Mora, Francisco Munoz, Rodrigo Muscarella, Robert Nunes, Yule R. F. Ochoa-Gaona, Susana Orihuela-Belmonte, Edith Pena-Claros, Marielos Perez-Garcia, Eduardo A. Piotto, Daniel Powers, Jennifer S. Rodriguez-Velazquez, Jorge Romero-Perez, Isabel Eunice Ruiz, Jorge Saldarriaga, Juan G. Sanchez-Azofeifa, Arturo Schwartz, Naomi B. Steininger, Marc K. Swenson, Nathan G. Uriarte, Maria van Breugel, Michiel van der Wal, Hans Veloso, Maria D. M. Vester, Hans Vieira, Ima Celia G. Bentos, Tony Vizcarra Williamson, G. Bruce Poorter, Lourens TI Carbon sequestration potential of second-growth forest regeneration in the Latin American tropics SO SCIENCE ADVANCES LA English DT Article ID ABOVEGROUND BIOMASS; SECONDARY FORESTS; GLOBAL DATABASE; CLIMATE-CHANGE; STOCKS; MAPS; DEFORESTATION; REFORESTATION; REGROWTH; DYNAMICS AB Regrowth of tropical secondary forests following complete or nearly complete removal of forest vegetation actively stores carbon in aboveground biomass, partially counterbalancing carbon emissions from deforestation, forest degradation, burning of fossil fuels, and other anthropogenic sources. We estimate the age and spatial extent of lowland second-growth forests in the Latin American tropics and model their potential aboveground carbon accumulation over four decades. Our model shows that, in 2008, second-growth forests (1 to 60 years old) covered 2.4 million km(2) of land (28.1% of the total study area). Over 40 years, these lands can potentially accumulate a total aboveground carbon stock of 8.48 Pg C (petagrams of carbon) in aboveground biomass via low-cost natural regeneration or assisted regeneration, corresponding to a total CO2 sequestration of 31.09 Pg CO2. This total is equivalent to carbon emissions from fossil fuel use and industrial processes in all of Latin America and the Caribbean from 1993 to 2014. Ten countries account for 95% of this carbon storage potential, led by Brazil, Colombia, Mexico, and Venezuela. We model future land-use scenarios to guide national carbon mitigation policies. Permitting natural regeneration on 40% of lowland pastures potentially stores an additional 2.0 Pg C over 40 years. Our study provides information and maps to guide national-level forest-based carbon mitigation plans on the basis of estimated rates of natural regeneration and pasture abandonment. Coupled with avoided deforestation and sustainable forest management, natural regeneration of second-growth forests provides a low-cost mechanism that yields a high carbon sequestration potential with multiple benefits for biodiversity and ecosystem services. C1 [Chazdon, Robin L.; Rozendaal, Danae M. A.; Boukili, Vanessa] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. [Chazdon, Robin L.] Int Inst Sustainabil, Estr Dona Castorina 124, BR-22460 Rio De Janeiro, Brazil. [Broadbent, Eben N.; Zambrano, Angelica Maria Almeyda] Univ Alabama, Dept Geog, Spatial Ecol & Conservat Lab, Tuscaloosa, AL 35487 USA. [Rozendaal, Danae M. A.] Univ Regina, Dept Biol, 3737 Wascana Pkwy, Regina, SK S4S 0A2, Canada. [Rozendaal, Danae M. A.; Bongers, Frans; Jakovac, Catarina C.; Lohbeck, Madelon; Pena-Claros, Marielos; Poorter, Lourens] Wageningen Univ, Forest Ecol & Forest Management Grp, POB 47, NL-6700 AA Wageningen, Netherlands. [Aide, T. Mitchell] Univ Puerto Rico, Dept Biol, POB 23360, San Juan, PR 00931 USA. [Balvanera, Patricia; Martinez-Ramos, Miguel; Rodriguez-Velazquez, Jorge] Univ Nacl Autonoma Mexico, Inst Invest Ecosistemas & Sustentabi, Morelia 58089, Michoacan, Mexico. [Becknell, Justin M.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Brancalion, Pedro H. S.; Cesar, Ricardo G.] Univ Sao Paulo, Luiz de Queiroz Coll Agr, Dept Forest Sci, Av Padua Dias 11, BR-13418900 Piracicaba, SP, Brazil. [Craven, Dylan; Hall, Jefferson S.; van Breugel, Michiel] Smithsonian Trop Res Inst, SI ForestGEO, Roosevelt Ave 401, Balboa, Panama. [Craven, Dylan] Halle Jena Leipzig, German Ctr Integrat Biodivers Res iDiv, Deutsch Pl 5e, D-04103 Leipzig, Germany. [Craven, Dylan] Univ Leipzig, Inst Biol, Johannisallee 21, D-04103 Leipzig, Germany. [Almeida-Cortez, Jarcilene S.; Cabral, George A. L.] Univ Fed Pernambuco, Dept Bot CCB, BR-50670 Recife, Brazil. [de Jong, Ben; Ochoa-Gaona, Susana; Orihuela-Belmonte, Edith] El Colegio Frontera Sur, Dept Sustainabil Sci, Av Rancho Poligono 2-A, Lerma 24500, Campeche, Mexico. [Denslow, Julie S.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Dent, Daisy H.] Smithsonian Trop Res Inst, Roosevelt Ave 401, Balboa, Panama. [Dent, Daisy H.] Univ Stirling, Biol & Environm Sci, Stirling FK9 4LA, Scotland. [DeWalt, Saara J.] Clemson Univ, Dept Biol Sci, 132 Long Hall, Clemson, SC 29634 USA. [Dupuy, Juan M.; Hernandez-Stefanoni, Jose Luis] Ctr Invest Cient Yucatan, AC Unidad Recursos Nat, Calle 43 130,Colonia Chuburna Hidalgo, Merida 97200, Yucatan, Mexico. [Duran, Sandra M.; Sanchez-Azofeifa, Arturo] Univ Alberta, Earth & Atmospher Sci Dept, Edmonton, AB T6G 2EG, Canada. [Espirito-Santo, Mario M.; Nunes, Yule R. F.; Veloso, Maria D. M.] Univ Estadual Montes Claros, Dept Biol Geral, BR-39401089 Montes Claros, MG, Brazil. [Fandino, Maria C.] Fondo Patrimonio Nat Biodiversidad & Areas Proteg, Calle 72 12-65 Piso 6, Bogota 110231, Colombia. [Jakovac, Catarina C.; Massoca, Paulo; Bentos, Tony Vizcarra; Williamson, G. Bruce] Inst Nacl de Pesquisas da Amazonia, Environm Dynam Res Coordinat, Biol Dynam Forest Fragments Project, BR-69067375 Manaus, Amazonas, Brazil. [Junqueira, Andre B.] Wageningen Univ, Ctr Crop Syst Anal, POB 430, NL-6700 AK Wageningen, Netherlands. [Junqueira, Andre B.] Wageningen Univ, Knowledge Technol & Innovat Grp, POB 8130, NL-6700 EW Wageningen, Netherlands. [Junqueira, Andre B.] Inst Nacl de Pesquisas da Amazonia, Coordenacao Tecnol & Inovacao, Av Andre Araujo 2936, BR-69060001 Manaus, Amazonas, Brazil. [Kennard, Deborah] Colorado Mesa Univ, Dept Phys & Environm Sci, 1100 North Ave, Grand Junction, CO 81501 USA. [Letcher, Susan G.] Purchase Coll SUNY, Dept Environm Studies, 735 Anderson Hill Rd, Purchase, NY 10577 USA. [Lohbeck, Madelon] World Agroforestry Ctr ICRAF, POB 30677-00100, Nairobi, Kenya. [Meave, Jorge A.; Mora, Francisco; Munoz, Rodrigo; Perez-Garcia, Eduardo A.; Romero-Perez, Isabel Eunice] Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Ecol & Recursos Nat, Mexico City 04510, DF, Mexico. [Muscarella, Robert; Schwartz, Naomi B.; Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Muscarella, Robert] Aarhus Univ, Dept Biosci, Sect Ecoinformat & Biodivers, DK-8000 Aarhus, Denmark. [Piotto, Daniel] Univ Fed Bahia, Ctr Formacao Ciencias Agroflorestais, BR-45613204 Itabuna, BA, Brazil. [Powers, Jennifer S.] Univ Minnesota, Dept Ecol Evolut & Behav, Dept Plant Biol, St Paul, MN 55108 USA. [Ruiz, Jorge] Univ Pedagog & Tecnol Colombia, Sch Social Sci, Geog Area, Tunja 150003, Colombia. [Ruiz, Jorge] Univ Calif Santa Barbara, Dept Geog, 4841 Ellison Hall, Santa Barbara, CA 93106 USA. [Saldarriaga, Juan G.] Cr 5 14-05,POB 412, Cota, Cundinamarca, Colombia. [Steininger, Marc K.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Swenson, Nathan G.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [van Breugel, Michiel] Yale NUS Coll, 12 Coll Ave West, Singapore 138610, Singapore. [van Breugel, Michiel] Natl Univ Singapore, Dept Biol Sci, 14 Sci Dr 4, Singapore 117543, Singapore. [van der Wal, Hans] El Colegio Frontera Sur, Dept Agr Sociedad & Ambiente, Unidad Villahermosa, Centro 86280, Tabasco, Mexico. [van der Wal, Hans] Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, NL-1090 Amsterdam, Netherlands. [Vester, Hans] Bonhoeffer Coll, Bruggertstr 60, NL-7545 AX Enschede, Netherlands. [Vieira, Ima Celia G.] Museu Paraense Emilio Goeldi, CP 399, BR-66040170 Belem, Para, Brazil. [Williamson, G. Bruce] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. RP Chazdon, RL (reprint author), Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA.; Chazdon, RL (reprint author), Int Inst Sustainabil, Estr Dona Castorina 124, BR-22460 Rio De Janeiro, Brazil. EM robin.chazdon@uconn.edu RI Brancalion, Pedro/D-6995-2012; Dent, Daisy/L-3549-2016; OI Brancalion, Pedro/0000-0001-8245-4062; Mora Ardila, Francisco/0000-0003-0390-0189; Dent, Daisy/0000-0002-1219-7344; Craven, Dylan/0000-0003-3940-833X; Meave, Jorge A./0000-0002-6241-8803 NR 49 TC 17 Z9 17 U1 36 U2 50 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 2375-2548 J9 SCI ADV JI Sci. Adv. PD MAY PY 2016 VL 2 IS 5 AR e1501639 DI 10.1126/sciadv.1501639 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DR7IK UT WOS:000380073000014 PM 27386528 ER PT J AU Paz, RCR Souza, NP Furtado, PV Brown, JL AF Paz, R. C. R. Souza, N. P. Furtado, P. V. Brown, J. L. TI Estradiol and progesterone fecal metabolites analysis in crab-eating-fox (Cerdocyoun thous) SO ARQUIVO BRASILEIRO DE MEDICINA VETERINARIA E ZOOTECNIA LA English DT Article DE radioimmunoassay; Elisa; estradiol; progesterone; fecal ID ZOO AB In this study, four crab-eating fox females (Cerdocyon thous) maintained at the Federal University of Mato Grosso Zoo, Cuiaba, Brazil, were investigated for 12 months, using feces measurement of estradiol and progesterone concentrations. Fecal collections were performed three times a week for hormone extraction. Two methods of analysis, Elisa (EIA) and Radioimmunoassay (RIA), were used in the measurement of progesterone (P4) and estradiol (E2) metabolites. The aim of this study was to compare and validate two different methods of hormone measurement for C. thous. There were no differences regarding the method used. The Radioimmunoassay technique proved to be more sensitive, however, both showed similar results. C1 [Paz, R. C. R.; Souza, N. P.] Univ Fed Mato Grosso, UFMT, Fac Agron Med Vet & Zootecn, Cuiaba, MT, Brazil. [Furtado, P. V.] PROVET, Lab Endocrinol, Moema, SP, Brazil. [Brown, J. L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA. RP Paz, RCR (reprint author), Univ Fed Mato Grosso, UFMT, Fac Agron Med Vet & Zootecn, Cuiaba, MT, Brazil. EM reginacrpaz@gmail.com FU FAPEMAT; CAPES; SMITHSONIAN CBI FX We thank UFMT Zoo staff for providing a crabeating fox for the experiments. We are also grateful to Sara Putman and Nicole Presley for patient laboratory assistance. This research was funded by FAPEMAT, CAPES and SMITHSONIAN CBI. NR 10 TC 0 Z9 0 U1 0 U2 1 PU ARQUIVO BRASILEIRO MEDICINA VETERINARIA ZOOTECNIA PI MINAS GERAIS PA FEDERAL MINAS GERAIS CAIXA POSTAL 567-BELO HORIZ, MINAS GERAIS, BRAZIL SN 0102-0935 EI 1678-4162 J9 ARQ BRAS MED VET ZOO JI Arq. Bras. Med. Vet. Zootec. PD MAY-JUN PY 2016 VL 68 IS 3 BP 636 EP 640 DI 10.1590/1678-4162-7886 PG 5 WC Veterinary Sciences SC Veterinary Sciences GA DQ6YY UT WOS:000379354600011 ER PT J AU McCormick, MK Taylor, DL Whigham, DF Burnett, RK AF McCormick, Melissa K. Taylor, D. Lee Whigham, Dennis F. Burnett, Robert K., Jr. TI Germination patterns in three terrestrial orchids relate to abundance of mycorrhizal fungi SO JOURNAL OF ECOLOGY LA English DT Article DE Goodyera pubescens; Liparis liliifolia; mycorrhizal limitation; mycorrhizas; orchid; Orchidaceae; plant-soil (below-ground) interactions; seed germination; Tipularia discolor ID BELOW-GROUND VIEWS; ECTOMYCORRHIZAL FUNGI; IN-SITU; SYMBIOTIC GERMINATION; COMMUNITY STRUCTURE; SEEDLING RECRUITMENT; GENETIC DIVERSITY; GOODYERA-REPENS; BOREAL FOREST; GREEN ORCHID AB 1. The spatial distribution of plants, which is often generated by patterns of seed recruitment, is an important determinant of population dynamics, especially for orchids with seeds that must be exposed to appropriate mycorrhizal fungi. 2. We compared the distribution and abundance of target mycorrhizal fungi detected in the soil using DNA-based molecular techniques and germination in seed packets of Goodyera pubescens, Liparis liliifolia and Tipularia discolor. 3. We further examined Tulasnella spp. associated with G. pubescens to determine whether areas with abundant host fungi resulted from multiple genets of the same species or from a single widespread fungal genet. 4. We found that target fungi were more likely to be detected using soil DNA assays than by seed germination. Based on soil DNA, fungi were more widespread than suggested by seed germination, which most often reflected the presence of abundant mycorrhizal fungi in the soil. Fungi were more likely to be abundant close to established orchids. Established plants of G. pubescens that were < 50 cm apart associated with a single abundant fungal genet, while those > 50 cm apart associated with multiple fungal genets. 5. Synthesis. This study demonstrates the importance of using multiple methods to detect the distribution and abundance of target fungi and suggests that fungal 'hot spots' may be keys to the dynamics of orchid populations. C1 [McCormick, Melissa K.; Whigham, Dennis F.; Burnett, Robert K., Jr.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. [Taylor, D. Lee] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. RP McCormick, MK (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM mccormickm@si.edu OI Taylor, Donald/0000-0002-5985-9210; Whigham, Dennis/0000-0003-1488-820X FU NSF [DEB-0316523, REU-0353759]; Frank Bertrum Sherry Endowment at the Smithsonian Institution FX This work was funded by NSF grant DEB-0316523. Microsatellite development was funded by a grant from the Frank Bertrum Sherry Endowment at the Smithsonian Institution to DFW and MKM. RKB was funded by NSF grant REU-0353759. We also wish to thank John P. O'Neill for field and laboratory help and for maintaining fungal collections and the Smithsonian Laboratory of Analytical Biology for DNA sequencing and microsatellite analysis. The manuscript also benefitted from the constructive suggestions of multiple referees. NR 73 TC 2 Z9 2 U1 14 U2 20 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 MAY PY 2016 VL 104 IS 3 BP 744 EP 754 DI 10.1111/1365-2745.12556 PG 11 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA DQ2EO UT WOS:000379014900013 ER PT J AU Inman-Narahari, F Ostertag, R Hubbell, SP Giardina, CP Cordell, S Sack, L AF Inman-Narahari, Faith Ostertag, Rebecca Hubbell, Stephen P. Giardina, Christian P. Cordell, Susan Sack, Lawren TI Density-dependent seedling mortality varies with light availability and species abundance in wet and dry Hawaiian forests SO JOURNAL OF ECOLOGY LA English DT Article DE community compensatory trend; density dependence; determinants of plant community diversity and structure; facilitation; Janzen-Connell hypothesis; regeneration dynamics; seedling ecology; tropical dry forest; tropical wet forest ID TROPICAL TREE SEEDLINGS; RAIN-FOREST; LOCAL NEIGHBORHOOD; NEOTROPICAL FOREST; WOODY SEEDLINGS; SPATIAL-PATTERN; SHADE TOLERANCE; TRADE-OFFS; SURVIVAL; COEXISTENCE AB 1. Conspecific density may contribute to patterns of species assembly through negative density dependence (NDD) as predicted by the Janzen-Connell hypothesis, or through facilitation (positive density dependence; PDD). Conspecific density effects are expected to be more negative in darker and wetter environments due to higher pathogen abundance and more positive in stressful, especially dry, environments (stress-gradient hypothesis). For NDD to contribute to maintaining diversity, it should be apparent at the community-wide scale as a negative correlation between seedling recruitment, growth or survival and conspecific adult abundance (community compensatory trend; CCT). 2. We examined seedling survival in relation to con-and heterospecific adults within 10 m and con-and heterospecific seedlings within 1 m for 13 species within two 4-ha permanent plots located in dry and wet forests in Hawaii. We also examined interactions between conspecific density and light and species' commonness. 3. For all species pooled, adult conspecific effects were positive (PDD) in both dry and wet forests, though they were stronger in the dry forest. In contrast, seedling conspecific effects were negative (NDD), though only significantly so in the wet forest. 4. The strength and direction of density effects varied with understorey light such that seedlings had the highest survival where both adult conspecific density and light were high but the lowest survival where seedling conspecific density and light were high. 5. In the wet forest, the most common species showed positive effects of adult conspecifics, but the less common species showed negative adult conspecific effects. We found mixed evidence for a CCT: seedling survival was positively correlated with basal area, but negatively correlated with tree density (stems ha(-1)). Thus, it remains unclear whether NDD is a diversity-maintaining mechanism in these forests. 6. Synthesis. Overall, we found that positive conspecific effects influenced seedling mortality patterns more than negative interactions did, even in tropical wet forest where NDD is predicted to drive species' abundances. Additionally, the strength and direction of density effects varied with forest type, PAR, and species' abundance, underscoring the need to consider abiotic factors and species' life-history traits in tests of density dependence hypotheses. C1 [Inman-Narahari, Faith; Hubbell, Stephen P.; Sack, Lawren] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, 621 Charles E Young Dr South, Los Angeles, CA 90095 USA. [Ostertag, Rebecca] Univ Hawaii, Dept Biol, 200 W Kawili St, Hilo, HI 96720 USA. [Hubbell, Stephen P.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Box 2072, Balboa, Panama. [Giardina, Christian P.; Cordell, Susan] US Forest Serv, Inst Pacific Isl Forestry, Pacific Southwest Res Stn, USDA, 60 Nowelo St, Hilo, HI 96720 USA. RP Inman-Narahari, F (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, 621 Charles E Young Dr South, Los Angeles, CA 90095 USA. EM finman@hawaii.edu RI Giardina, Christian/C-3120-2011; Sack, Lawren/A-5492-2008 OI Giardina, Christian/0000-0002-3431-5073; Sack, Lawren/0000-0002-7009-7202 FU National Science Foundation [EPSCoR 0554657, 0903833, IOS-0546784]; Smithsonian Tropical Research Institute Center for Tropical Forest Science; University of Hawaii; USDA Forest Service Pacific Southwest Research Station Institute of Pacific Islands Forestry (USFS-IPIF); Catherine H. Beattie grant from the Garden Club of America; Vavra and Pauley Fellowships from the University of California, Los Angeles FX We thank the many field assistants who collected seedling data, especially Molly Murphy, Kahealani Wailani-Nihipali, Kehauwealani Nelson-Kaula and others with the Hawaii Community College Tropical Forest Ecosystem and Agroforestry Management and University of Hawaii at Hilo Pacific Internship Programs for Exploring Science programs. We thank Bernice Hwang, Michael Nullet, Paul Scowcroft and Jodie Schulten for assistance with logistics. We are grateful to Megan Bartlett, Marissa Caringella, Grace John, Rodrigo Mendez-Alonzo, Christine Scoffoni, Daniel J. Johnson, Margaret Metz, Nikhil Inman-Narahari, and anonymous reviewers for comments on draft versions of the manuscript. Financial support was provided by the National Science Foundation (Grants EPSCoR 0554657 and 0903833, and IOS-0546784), the Smithsonian Tropical Research Institute Center for Tropical Forest Science, the University of Hawaii, the USDA Forest Service Pacific Southwest Research Station Institute of Pacific Islands Forestry (USFS-IPIF), a Catherine H. Beattie grant from the Garden Club of America, and Vavra and Pauley Fellowships from the University of California, Los Angeles. We thank the USFS-IPIF and the Hawaii Division of Forestry and Wildlife/Department of Land and Natural Resources for access to the Hawaii Experimental Tropical Forest. NR 54 TC 0 Z9 0 U1 18 U2 27 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 MAY PY 2016 VL 104 IS 3 BP 773 EP 780 DI 10.1111/1365-2745.12553 PG 8 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA DQ2EO UT WOS:000379014900016 ER PT J AU Zemunik, G Turner, BL Lambers, H Laliberte, E AF Zemunik, Graham Turner, Benjamin L. Lambers, Hans Laliberte, Etienne TI Increasing plant species diversity and extreme species turnover accompany declining soil fertility along a long-term chronosequence in a biodiversity hotspot SO JOURNAL OF ECOLOGY LA English DT Article DE beta diversity; determinants of plant community diversity and structure; ecosystem development; non-mycorrhizal plant species; nutrient-impoverished soil; pedogenesis; phosphorus; retrogression; species richness ID 2-MILLION-YEAR DUNE CHRONOSEQUENCE; NUTRIENT-ACQUISITION STRATEGIES; BETA DIVERSITY; ECOSYSTEM RETROGRESSION; PHOSPHORUS LIMITATION; SEED-GERMINATION; COASTAL DUNES; COMMUNITY; GRADIENTS; FORESTS AB 1. Long-term soil chronosequences provide natural soil fertility gradients that can be used to explore linkages between soils and plant community composition and diversity. Well-studied forested soil chronosequences have revealed that local (a) plant diversity increases with greater soil age and declining fertility, but corresponding changes in species turnover and beta (b) diversity have not been explored, particularly in extremely species-rich regions. 2. We quantified changes in plant species diversity and community composition, and identified the edaphic drivers of these changes, along a >2-million year retrogressive dune chronosequence in the south-west Australia biodiversity hotspot. 3. We found greater plant species diversity across all growth forms as soil development proceeded and concentrations of soil nutrients, particularly phosphorus (P), diminished to extremely low levels (surface soil total P concentrations of 6 mg P kg(-1)). Despite the high plant a diversity on older nutrient-impoverished soils, species turnover across the chronosequence was exceptionally high when all growth forms were considered (mean of 1% of species shared between the youngest and oldest soils), and there was complete turnover of woody species along the chronosequence. Such extreme species turnover across the chronosequence reflected large changes in soil chemical properties. In addition, b diversity within individual chronosequence stages increased with declining soil fertility. Shrubs remained the dominant and most speciose growth form throughout the chronosequence. 4. Synthesis. The large increase in plant a diversity and the extreme species turnover associated with declining soil fertility highlight the central role of soil properties in driving plant community assembly during long-term ecosystem development, previously only reported from comparatively species-poor regions. Our finding that plant b diversity increased with declining soil fertility points to a novel mechanism whereby extremely low soil fertility, rather than high productivity, promotes high b diversity. These results suggest that the interaction of an exceptionally diverse plant species pool and nutrient-impoverished soils provides the basis for the maintenance of such high b diversity at extremely low soil fertility. C1 [Zemunik, Graham; Turner, Benjamin L.; Lambers, Hans; Laliberte, Etienne] Univ Western Australia, Sch Plant Biol, Perth, WA 6009, Australia. [Zemunik, Graham; Turner, Benjamin L.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. [Laliberte, Etienne] Univ Montreal, Inst Rech Biol Vegetale, Dept Sci Biol, 4101 Sherbrooke Est, Montreal, PQ H1X 2B1, Canada. RP Zemunik, G (reprint author), Univ Western Australia, Sch Plant Biol, Perth, WA 6009, Australia.; Zemunik, G (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM graham@graduate.uwa.edu.au RI Laliberte, Etienne/B-6855-2008; Lambers, Hans/A-1544-2008; Turner, Benjamin/E-5940-2011; OI Laliberte, Etienne/0000-0002-3167-2622; Lambers, Hans/0000-0002-4118-2272; Turner, Benjamin/0000-0002-6585-0722; Zemunik, Graham/0000-0002-6064-345X FU Paul Hasluck Bequest; DECRA from the Australian Research Council [DE120100352]; University of Western Australia; ARC [DP0985685] FX G.Z. acknowledges the assistance of many helpers and volunteers in conducting the flora surveys. G.Z. was supported by a scholarship from the Paul Hasluck Bequest administered by the Kwongan Foundation. Field sampling and soil analyses were funded by a DECRA (DE120100352) from the Australian Research Council and research grants from The University of Western Australia to E.L. and by an ARC Discovery (DP0985685) to H.L. We acknowledge the Department of Parks and Wildlife (Western Australia) and the Shires of Dandaragan and Coorow for permission to conduct research on land under their administration. NR 74 TC 3 Z9 3 U1 19 U2 38 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 MAY PY 2016 VL 104 IS 3 BP 792 EP 805 DI 10.1111/1365-2745.12546 PG 14 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA DQ2EO UT WOS:000379014900018 ER PT J AU Sanchez-Martinez, G Moreno-Rico, O Smith, DR AF Sanchez-Martinez, Guillermo Moreno-Rico, Onesimo Smith, David R. TI FIRST RECORD AND BIOLOGICAL OBSERVATIONS ON THE WOODWASP Sirex obesus BRADLEY IN AGUASCALIENTES, MEXICO SO AGROCIENCIA LA English DT Article DE Siricidae; Sirex obesus; Pinus teocote; Pinus leiophylla; Ibalia leucospoides; Dendroctonus mexicanus ID UNITED-STATES; HYMENOPTERA; SIRICIDAE; SYMPHYTA AB The woodwasp Sirex obesus Bradley is described from specimens fortuitously captured in Lindgren funnel traps used in studies on the flight of the bark beetle Dendroctonus mexicanus Hopkins and through the direct capture on the bark of trees, in the municipality of San Jose de Gracia, Aguacalientes, Mexico. Pinus leiophylla Schl.et. Chain. and Pinus teocote Schl. et. Chain., weakened by the presence of D. mexicanus, were identified as hosts of S. obesus. The adults of this species emerge and oviposit during October and November. As parasitoids of S. obesus, some specimens of Ibalia leucospoides Hochenwarth (Hymenoptera: Ibaliidae) were collected in the same pine sections where the specimens of S. obesus emerged. This is the first record of the species in the state of Aguascalientes; therefore, more attention should be given to this insect because of its potential risk of invading pine trees and stands in Mexico. C1 [Sanchez-Martinez, Guillermo] INIFAP, Campo Expt Pabellon, Km 32-5,Carretera Aguascalientes Zacatecas, Pabellon De Arteaga 20670, Aguascalientes, Mexico. [Moreno-Rico, Onesimo] Univ Autonoma Aguascalientes, Ctr Ciencias Basicas, Dept Microbiol, Ave Univ 940,Colonia Ciudad Univ, Aguascalientes 20131, Aguascalientes, Mexico. [Smith, David R.] USDA, Systemat Entomol Lab, PSI, ARS,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. RP Sanchez-Martinez, G (reprint author), INIFAP, Campo Expt Pabellon, Km 32-5,Carretera Aguascalientes Zacatecas, Pabellon De Arteaga 20670, Aguascalientes, Mexico. EM omoreno@correo.uaa.mx; dave.smith@ars.usda.gov NR 14 TC 0 Z9 0 U1 2 U2 2 PU COLEGIO POSTGRADUADOS PI MONTECILLO PA CARRETERA MEXICO TEXCOCO KM 36 5, MONTECILLO 56230, ESTADO MEXICO, MEXICO SN 1405-3195 J9 AGROCIENCIA-MEXICO JI Agrociencia PD MAY-JUN PY 2016 VL 50 IS 4 BP 459 EP 469 PG 11 WC Agriculture, Multidisciplinary SC Agriculture GA DQ1IG UT WOS:000378954100007 ER PT J AU Feng, XJ Feakins, SJ Liu, ZG Ponton, C Wang, RZ Karkabi, E Galy, V Berelson, WM Nottingham, AT Meir, P West, AJ AF Feng, Xiaojuan Feakins, Sarah J. Liu, Zongguang Ponton, Camilo Wang, Renee Z. Karkabi, Elias Galy, Valier Berelson, William M. Nottingham, Andrew T. Meir, Patrick West, A. Joshua TI Source to sink: Evolution of lignin composition in the Madre de Dios River system with connection to the Amazon basin and offshore SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article DE lignin phenols; dissolved organic matter (DOM); particulate organic matter (POM); Andes; Amazon; depth profile ID TERRESTRIAL ORGANIC-MATTER; CONTINENTAL-SHELF SEDIMENTS; CUO REACTION-PRODUCTS; LEAF WAX BIOMARKERS; FAGUS-SYLVATICA L.; ELEVATION GRADIENT; PERUVIAN ANDES; TEMPERATURE SENSITIVITY; CHEMICAL-COMPOSITION; OXIDATION-PRODUCTS AB While lignin geochemistry has been extensively investigated in the Amazon River, little is known about lignin distribution and dynamics within deep, stratified river channels or its transformations within soils prior to delivery to rivers. We characterized lignin phenols in soils, river particulate organic matter (POM), and dissolved organic matter (DOM) across a 4 km elevation gradient in the Madre de Dios River system, Peru, as well as in marine sediments to investigate the source-to-sink evolution of lignin. In soils, we found more oxidized lignin in organic horizons relative to mineral horizons. The oxidized lignin signature was maintained during transfer into rivers, and lignin was a relatively constant fraction of bulk organic carbon in soils and riverine POM. Lignin in DOM became increasingly oxidized downstream, indicating active transformation of dissolved lignin during transport, especially in the dry season. In contrast, POM accumulated undegraded lignin downstream during the wet season, suggesting that terrestrial input exceeded in-river degradation. We discovered high concentrations of relatively undegraded lignin in POM at depth in the lower Madre de Dios River in both seasons, revealing a woody undercurrent for its transfer within these deep rivers. Our study of lignin evolution in the soil-river-ocean continuum highlights important seasonal and depth variations of river carbon components and their connection to soil carbon pools, providing new insights into fluvial carbon dynamics associated with the transfer of lignin biomarkers from source to sink. C1 [Feng, Xiaojuan; Liu, Zongguang] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing, Peoples R China. [Feakins, Sarah J.; Ponton, Camilo; Wang, Renee Z.; Karkabi, Elias; Berelson, William M.; West, A. Joshua] Univ So Calif, Dept Earth Sci, Los Angeles, CA 90089 USA. [Galy, Valier] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. [Nottingham, Andrew T.; Meir, Patrick] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland. [Nottingham, Andrew T.] Smithsonian Trop Res Inst, Balboa, Panama. [Meir, Patrick] Australian Natl Univ, Res Sch Biol, Canberra, ACT, Australia. RP Feng, XJ (reprint author), Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing, Peoples R China.; Feakins, SJ (reprint author), Univ So Calif, Dept Earth Sci, Los Angeles, CA 90089 USA. EM xfeng@ibcas.ac.cn; feakins@usc.edu RI galy, valier/I-6185-2012; Feng, Xiaojuan/I-6142-2013; Feakins, Sarah/K-4149-2012 OI Feng, Xiaojuan/0000-0002-0443-0628; Feakins, Sarah/0000-0003-3434-2423 FU U.S. National Science Foundation [1227192]; National Program on Key Basic Research Project [2015CB954201]; National Natural Science Foundation of China [41422304]; USC; Natural Environment Research Council [NE/F002149/1]; ARC [FT110100457]; European Union Marie Curie Fellowship [FP7-2012-329360]; NSF [OCE-0934073] FX This work was supported by funding from the U.S. National Science Foundation award 1227192 to A.J.W. and S.J.F., and by funding from the National Program on Key Basic Research Project (2015CB954201) and National Natural Science Foundation of China (41422304) to X.F. R.Z.W. received support from USC funding for undergraduate research. For the river work, we are grateful to field assistance from M. Torres, A. Robles, and A. Ccahuana, and river navigation by Ernesto. Logistical support was provided by Y. Malhi, J. Huaman, W. Huaraca Huasco, and other collaborators as part of the Andes Biodiversity and Ecosystems Research Group (ABERG; andesresearch.org). Thanks to students who assisted in the laboratory work: E. Rosca, K. McPherson, and G. Li (USC), and technical assistance from Nick Rollins. P.M. and A.N. acknowledge funding from Natural Environment Research Council NE/F002149/1 (soils), ARC FT110100457 to P.M. and European Union Marie Curie Fellowship (FP7-2012-329360) to A.N. Funding for the marine samples is acknowledged from NSF (OCE-0934073) to W.B. We are thankful to the captain and crew of the RN Knorr. We would also like to acknowledge the members of the at-sea and shore-based science party and all contributors to the ANACONDAS project. NR 119 TC 1 Z9 1 U1 22 U2 29 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 EI 2169-8961 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD MAY PY 2016 VL 121 IS 5 BP 1316 EP 1338 DI 10.1002/2016JG003323 PG 23 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA DP7TX UT WOS:000378703200008 ER PT J AU Thompson, EC Chidester, BA Fischer, RA Myers, GI Heinz, DL Prakapenka, VB Campbell, AJ AF Thompson, Elizabeth C. Chidester, Bethany A. Fischer, Rebecca A. Myers, Gregory I. Heinz, Dion L. Prakapenka, Vitali B. Campbell, Andrew J. TI Equation of state of pyrite to 80 GPa and 2400 K SO AMERICAN MINERALOGIST LA English DT Article DE High-pressure; diamond-anvil cell; equation of state; X-ray diffraction ID X-RAY-DIFFRACTION; LASER-HEATING SYSTEM; HIGH-PRESSURE; EARTHS CORE; SULFUR-CONTENT; FES2 PYRITE; OUTER CORE; IRON; ALLOYS; CONSTRAINTS AB The high-cosmic abundance of sulfur is not reflected in the terrestrial crust, implying it is either sequestered in the Earth's interior or was volatilized during accretion. As it has widely been suggested that sulfur could be one of the contributing light elements leading to the density deficit of Earth's core, a robust thermal equation of state of iron sulfide is useful for understanding the evolution and properties of Earth's interior. We performed X-ray diffraction measurements on FeS2 achieving pressures from 15 to 80 GPa and temperatures up to 2400 K using laser-heated diamond-anvil cells. No phase transitions were observed in the pyrite structure over the pressure and temperature ranges investigated. Combining our new P-V-Tdata with previously published room-temperature compression and thermochemical data, we fit a Debye temperature of 624(14) K and determined a Mie-Gruneisen equation of state for pyrite having bulk modulus K-T = 141.2(18) GPa, pressure derivative K-T' = 5.56(24), Gruneisen parameter gamma(0) = 1.41, anharmonic coefficient A(2) = 2.53(27) x 10(-3) J/(K-2.mol), and q = 2.06(27). These findings are compared to previously published equation of state parameters for pyrite from static compression, shock compression, and ab initio studies. This revised equation of state for pyrite is consistent with an outer core density deficit satisfied by 11.4(10) wt% sulfur, yet matching the bulk sound speed of PREM requires an outer core composition of 4.8(19) wt% S. This discrepancy suggests that sulfur alone cannot satisfy both seismological constraints simultaneously and cannot be the only light element within Earth's core, and so the sulfur content needed to satisfy density constraints using our FeS2 equation of state should be considered an upper bound for sulfur in the Earth's core. C1 [Thompson, Elizabeth C.; Chidester, Bethany A.; Fischer, Rebecca A.; Myers, Gregory I.; Heinz, Dion L.; Campbell, Andrew J.] Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA. [Prakapenka, Vitali B.] Univ Chicago, Argonne Natl Lab, GeoSoilEnviroCARS, Argonne, IL 60439 USA. [Fischer, Rebecca A.] Smithsonian Inst, Natl Museum Nat Hist, Santa Cruz, CA 95064 USA. [Fischer, Rebecca A.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. RP Thompson, EC (reprint author), Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA. EM ecthompson@uchicago.edu FU National Science Foundation; American Association of University Women Educational Foundation Dissertation Fellowship; National Science Foundation [EAR-1427123]; DOE-NNSA [DE-NA0001974]; DOE-BES [DE-FG02-99ER45775]; NSF; National Science Foundation-Earth Sciences [EAR-1128799]; Department of Energy-GeoSciences [DE-FG02-94ER14466]; DOE Office of Science [DE-AC02-06CH11357]; NSF [EAR 11-57758]; GSECARS through NSF [EAR -1128799]; DOE [DE-FG0294ER14466] FX We thank the editors and the two reviewers for their helpful comments on the manuscript. This research is supported by National Science Foundation Graduate Research Fellowships to E.C.T. and B.A.C., an American Association of University Women Educational Foundation Dissertation Fellowship to R.A.F., and National Science Foundation Grant no. EAR-1427123 to A.J.C. This work was completed at HPCAT (Sector 16) and GeoSoilEnviroCARS (Sector 13), Advanced Photon Source (APS), Argonne National Laboratory. HPCAT operations are supported by DOE-NNSA under Award No. DE-NA0001974 and DOE-BES under Award No. DE-FG02-99ER45775, with partial instrumentation funding by NSF. GeoSoilEnviroCARS is supported by the National Science Foundation-Earth Sciences (EAR-1128799) and Department of Energy-GeoSciences (DE-FG02-94ER14466). This work was made possible by the generous assistance of the APS beamline scientists at both Sector 13 and Sector 16. The Advanced Photon Source is a U.S. Department of Energy (DOE) Office of Science User Facility operated for the DOE Office of Science by Argonne National Laboratory under Contract No. DE-AC02-06CH11357. Use of the COMPRES-GSECARS gas loading system was supported by COMPRES under NSF Cooperative Agreement EAR 11-57758 and by GSECARS through NSF grant EAR -1128799 and DOE grant DE-FG0294ER14466. This research used resources of the Advanced Photon Source, a U.S. Department of Energy (DOE) Office of Science User Facility operated for the DOE Office of Science by Argonne National Laboratory under Contract No. DE-ACO2-06CH11357. NR 47 TC 0 Z9 0 U1 6 U2 8 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD MAY-JUN PY 2016 VL 101 IS 5-6 BP 1046 EP 1051 DI 10.2138/am-2016-5527 PG 6 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA DP0ND UT WOS:000378185600006 ER PT J AU Wright, DS Yong, L Pierotti, MER McKinnon, JS AF Wright, Daniel Shane Yong, Lengxob Pierotti, Michele E. R. McKinnon, Jeffrey S. TI Male red throat coloration, pelvic spine coloration, and courtship behaviours in threespine stickleback SO EVOLUTIONARY ECOLOGY RESEARCH LA English DT Article DE aggression; colour; Gasterosteus aculeatus; 11-ketotestosterone; pelvic spine; threespine stickleback ID MALE 3-SPINED STICKLEBACK; CULAEA-INCONSTANS KIRTLAND; GASTEROSTEUS-ACULEATUS L; BROOK STICKLEBACK; MATE CHOICE; EVOLUTIONARY SIGNIFICANCE; REDUCTION; ANDROGENS; FISHES; 11-KETOTESTOSTERONE AB Background: In addition to exhibiting red nuptial throat coloration, male threespine sticklebacks (Gasterosteus aculeatus) often possess red coloration on their pelvic spines. Although variation in throat colour has been shown to be associated with male reproductive behaviour, limited research has been devoted to the behavioural correlates of red spine colour. Like the red throat, spine colour might correlate with components of male reproductive behaviour and may also be androgen dependent, with important implications for a potential signalling function. Hypothesis: Spine coloration, like throat coloration, is correlated with components of courtship behaviour, and also with the fish androgen 11-ketotestosterone (11KT). Methods: To examine the role of male throat and spine colour expression in a mating context, we measured the behavioural response of nesting males to conspecific females. We analysed the relationships between throat and spine colours with reproductive behaviours as well as with 11KT. Results: Males with more intensely red throats courted females more vigorously, whereas males with redder spines displayed relatively more aggressive behaviour during courtship. An initial analysis of a subsample of males showed that 11KT was positively associated with spine colour intensity, but not with red throats or any behaviours. Hence throat and spine colour may reflect different components of male reproductive behaviour, and 11KT is a potential mediator of spine coloration in males. C1 [Wright, Daniel Shane; Yong, Lengxob; Pierotti, Michele E. R.; McKinnon, Jeffrey S.] E Carolina Univ, Dept Biol, Greenville, NC USA. [Wright, Daniel Shane] Univ Groningen, Groningen Inst Evolutionary Life Sci GELIFES, Groningen, Netherlands. [Yong, Lengxob] Georgia Inst Technol, Sch Biol, Atlanta, GA 30332 USA. [Pierotti, Michele E. R.] Smithsonian Trop Res Inst, Naos Marine Labs, Panama City, Panama. RP Wright, DS (reprint author), GELIFES Behav Biol, Nijenborgh 7, NL-9747 AG Groningen, Netherlands. EM d.s.wright@rug.nl FU American Museum of Natural History; American Society of Ichthyologists and Herpetologists; Society for the Study of Evolution FX We thank Kaytiana Crane, Samantha Mears, Dhagash Patel, and Drutika Patel for assistance with behavioural trials. Anais Delacruz, George Vuong, Evan Knight, Kevin Shah, Tyson Tran, Christina Webster, Jeremy Willis, and Ben Woodall helped with the maintenance of the fish in the lab. Many thanks to Cindy Kukoly at ECU School of Medicine for providing bench space during the hormonal analyses. The Dolph Schluter lab (University of British Columbia) provided help with the logistics of fish collections. Thanks to the BC Ministry of Natural Resources and the Little Campbell Regional Park for granting us access and permits for fish collection. Funding was provided by the American Museum of Natural History, the American Society of Ichthyologists and Herpetologists, and the Society for the Study of Evolution to L.Y. NR 48 TC 1 Z9 1 U1 8 U2 10 PU EVOLUTIONARY ECOLOGY LTD PI TUCSON PA UNIV ARIZONA, 321 BIOSCIENCES WEST, TUCSON, AZ 85721 USA SN 1522-0613 EI 1937-3791 J9 EVOL ECOL RES JI Evol. Ecol. Res. PD MAY PY 2016 VL 17 IS 3 BP 407 EP 418 PG 12 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA DP0GV UT WOS:000378168300007 ER PT J AU Xu, H Snider, TN Wimer, HF Yamada, SS Yang, T Holmbeck, K Foster, BL AF Xu, H. Snider, T. N. Wimer, H. F. Yamada, S. S. Yang, T. Holmbeck, K. Foster, B. L. TI Multiple essential MT1-MMP functions in tooth root formation, dentinogenesis, and tooth eruption SO MATRIX BIOLOGY LA English DT Article DE Extracellular matrix; Matrix metalloproteinases; Dentin; Bone formation; Periodontal ID RAT DENTAL FOLLICLE; BONE MORPHOGENETIC PROTEIN-2; HORMONE-RELATED PROTEIN; CRE TRANSGENIC MICE; OSTERIX-CRE; MATRIX METALLOPROTEINASES; PERIODONTAL-LIGAMENT; WINCHESTER-SYNDROME; GENE-EXPRESSION; NULL MICE AB Membrane-type matrix metalloproteinase 1 (MT1-MMP) is a transmembrane zinc-endopeptidase that breaks down extracellular matrix components, including several collagens, during tissue development and physiological remodeling. MT1-MMP-deficient mice (MT1-MMP-/-) feature severe defects in connective tissues, such as impaired growth, osteopenia, fibrosis, and conspicuous loss of molar tooth eruption and root formation. In order to define the functions of MT1-MMP during root formation and tooth eruption, we analyzed the development of teeth and surrounding tissues in the absence of MT1-MMP. In situ hybridization showed that MT1-MMP was widely expressed in cells associated with teeth and surrounding connective tissues during development. Multiple defects in dentoalveolar tissues were associated with loss of MT1-MMP. Root formation was inhibited by defective structure and function of Hertwig's epithelial root sheath (HERS). However, no defect was found in creation of the eruption pathway, suggesting that tooth eruption was hampered by lack of alveolar bone modeling/remodeling coincident with reduced periodontal ligament (PDL) formation and integration with the alveolar bone. Additionally, we identified a significant defect in dentin formation and mineralization associated with the loss of MT1-MMP. To segregate these multiple defects and trace their cellular origin, conditional ablation of MT1-MMP was performed in epithelia and mesenchyme. Mice featuring selective loss of MT1-MMP activity in the epithelium were indistinguishable from wild type mice, and importantly, featured a normal HERS structure and molar eruption. In contrast, selective knock-out of MT1-MMP in Osterix-expressing mesenchymal cells, including osteoblasts and odontoblasts, recapitulated major defects from the global knock-out including altered HERS structure, short roots, defective dentin formation and mineralization, and reduced alveolar bone formation, although molars were able to erupt. These data indicate that MT1-MMP activity in the dental mesenchyme, and not in epithelial-derived HERS, is essential for proper tooth root formation and eruption. In summary, our studies point to an indispensable role for MT1-MMP-mediated matrix remodeling in tooth eruption through effects on bone formation, soft tissue remodeling and organization of the follicle/PDL region. (C) 2016 Elsevier B.V. All rights reserved. C1 [Xu, H.] Peking Univ, Dept Pediat Dent, Sch & Hosp Stomatol, Beijing 100871, Peoples R China. [Xu, H.; Foster, B. L.] Natl Inst Arthrit & Musculoskeletal & Skin Dis NI, NIH, Bethesda, MD USA. [Snider, T. N.] Univ Michigan, Dept Orthodont & Pediat Dent, Ann Arbor, MI 48109 USA. [Snider, T. N.] NIH, Med Res Scholars Program, Bldg 10, Bethesda, MD 20892 USA. [Wimer, H. F.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Wimer, H. F.; Yamada, S. S.; Yang, T.; Holmbeck, K.] NIDCR, NIH, Bethesda, MD USA. [Foster, B. L.] Ohio State Univ, Coll Dent, Biosci Div, 4163 Poste Hall,305 W 12th Ave, Columbus, OH 43210 USA. RP Foster, BL (reprint author), Ohio State Univ, Coll Dent, Biosci Div, 4163 Poste Hall,305 W 12th Ave, Columbus, OH 43210 USA. EM foster.1004@osu.edu FU Intramural Research Programs of the National Institute of Arthritis and Musculoskeletal and Skin Diseases (NIAMS); National Institute for Dental and Craniofacial Research (NIDCR) of the National Institutes of Health (NIH, Bethesda, MD); NIAMS/NIH [AR066110]; Peking University School and Hospital of Stomatology; NIH Medical Research Scholars Program (MRSP); NIH; NIH from the Doris Duke Charitable Foundation; American Association for Dental Research; Howard Hughes Medical Institute; Colgate-Palmolive Company FX This research was supported by the Intramural Research Programs of the National Institute of Arthritis and Musculoskeletal and Skin Diseases (NIAMS; to BLF) and the National Institute for Dental and Craniofacial Research (NIDCR; to KH) of the National Institutes of Health (NIH, Bethesda, MD), grant AR066110 from NIAMS/NIH (to BLF), by a 2014-2015 Overseas Research and Personal Training Fund from Peking University School and Hospital of Stomatology (to HX), and by the NIH Medical Research Scholars Program (MRSP)(to TNS). MRSP is a public private partnership supported jointly by the NIH and generous contributions to the Foundation for the NIH from the Doris Duke Charitable Foundation, the American Association for Dental Research, the Howard Hughes Medical Institute, and the Colgate-Palmolive Company, as well as alumni of student research programs and other individual supporters. The authors thank Dr. Pamela G. Robey (NIDCR/NIH) for her support and critical review of the manuscript. NR 92 TC 2 Z9 2 U1 2 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0945-053X EI 1569-1802 J9 MATRIX BIOL JI Matrix Biol. PD MAY-JUL PY 2016 VL 52-54 SI SI BP 266 EP 283 DI 10.1016/j.matbio.2016.01.002 PG 18 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA DP0PC UT WOS:000378190700023 PM 26780723 ER PT J AU Halperin, CT Bishop, RL AF Halperin, Christina T. Bishop, Ronald L. TI Chemical analysis of Late Classic Maya polychrome pottery paints and pastes from Central Peten, Guatemala SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Chemical analysis; LA-ICP-MS; INAA; Ancient Maya; Provincial politics; Polychrome pottery; Paint recipes; Production and exchange; Political-economy ID HEMATITE; SOCIETY AB This paper examines political-economic relationships among Late Classic (ca. 600-900 CE) political centers in the Peten Lakes region, Guatemala, through the chemical analysis of red paints and pastes of polychrome vessels. Chemical analysis of red paints was conducted using Laser Ablation Inductively Coupled Plasma Mass Spectrometry (LA-ICP-MS), and chemical analysis of vessel pastes was conducted using Instrumental Neutron Activation Analysis (INAA). These analyses indicate that a number of political centers along the western shore of Lake Peten Itza, namely Motul de San Jose, Tayasal, and Flores, had access to different polychrome pottery production communities. Nonetheless, inhabitants of these Peten Lakes sites moved between, gifted, or exchanged polychrome pottery with each other, indicating that western Peten Lakes region centers closely interacted with each other. We suggest that these sites may have been part of or allied with the epigraphically known Ik' polity. As such, we find that one of the strengths of 'second-tier' polities, such as the Ik' polity, did not depend on an individual site's size or monumental expression, but on the relationships they forged with other centers. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Halperin, Christina T.] Univ Montreal, Montreal, PQ H3T 1N8, Canada. [Bishop, Ronald L.] Smithsonian Inst, Washington, DC 20560 USA. RP Halperin, CT (reprint author), Univ Montreal, Dept Anthropol, Pavillon Lionel Groulx,3150 Jean Brillant, Montreal, PQ H3T 1N8, Canada. EM christina.halperin@umontreal.ca NR 52 TC 0 Z9 0 U1 2 U2 2 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 MAY PY 2016 VL 69 BP 118 EP 129 DI 10.1016/j.jas.2016.04.007 PG 12 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA DO5KR UT WOS:000377822500012 ER PT J AU Lainhart, W Dutari, LC Rovira, JR Sucupira, IMC Povoa, MM Conn, JE Loaiza, JR AF Lainhart, William Dutari, Larissa C. Rovira, Jose R. Sucupira, Izis M. C. Povoa, Marinete M. Conn, Jan E. Loaiza, Jose R. TI Epidemic and Non-Epidemic Hot Spots of Malaria Transmission Occur in Indigenous Comarcas of Panama SO PLOS NEGLECTED TROPICAL DISEASES LA English DT Article ID PLASMODIUM-FALCIPARUM INFECTION; ANOPHELES-ALBIMANUS DIPTERA; CENTRAL-AMERICA; SPECIES COMPOSITION; ASYMPTOMATIC MALARIA; SOUTHERN MEXICO; BITING ACTIVITY; CULICIDAE; JUXTANUCLEARE; MOSQUITOS AB From 2002-2005, Panama experienced a malaria epidemic that has been associated with El Nino Southern Oscillation weather patterns, decreased funding for malaria control, and landscape modification. Case numbers quickly decreased afterward, and Panama is now in the pre-elimination stage of malaria eradication. To achieve this new goal, the characterization of epidemiological risk factors, foci of transmission, and important anopheline vectors is needed. Of the 24,681 reported cases in these analyses (2000-2014), similar to 62% occurred in epidemic years and similar to 44% in indigenous comarcas (5.9% of Panama's population). Subanalyses comparing overall numbers of cases in epidemic and non-epidemic years identified females, comarcas and some 5-year age categories as those disproportionately affected by malaria during epidemic years. Annual parasites indices (APIs; number of cases per 1,000 persons) for Plasmodium vivax were higher in comarcas compared to provinces for all study years, though P. falciparum APIs were only higher in comarcas during epidemic years. Interestingly, two comarcas report increasing numbers of cases annually, despite national annual decreases. Inclusion of these comarcas within identified foci of malaria transmission confirmed their roles in continued transmission. Comparison of species distribution models for two important anophelines with Plasmodium case distribution suggest An. albimanus is the primary malaria vector in Panama, confirmed by identification of nine P. vivax-infected specimen pools. Future malaria eradication strategies in Panama should focus on indigenous comarcas and include both active surveillance for cases and comprehensive anopheline vector surveys. C1 [Lainhart, William; Conn, Jan E.] SUNY Albany, Sch Publ Hlth, Dept Biomed Sci, Albany, NY USA. [Lainhart, William; Conn, Jan E.] New York State Dept Hlth, Wadsworth Ctr, Albany, NY USA. [Dutari, Larissa C.; Loaiza, Jose R.] Inst Invest Cient & Serv Alta Tecnol, Panama City, Panama. [Rovira, Jose R.; Loaiza, Jose R.] Smithsonian Trop Res Inst, Panama City, Panama. [Sucupira, Izis M. C.; Povoa, Marinete M.] Inst Evandro Chagas, Secao Parasitol, Ananindeua, Para, Brazil. RP Lainhart, W (reprint author), SUNY Albany, Sch Publ Hlth, Dept Biomed Sci, Albany, NY USA.; Lainhart, W (reprint author), New York State Dept Hlth, Wadsworth Ctr, Albany, NY USA. EM wlainhart@gmail.com OI Lainhart, William/0000-0002-9372-6737 FU Secretariat for Science, Technology and Innovation of Panama (SENACYT) [COL11-044, ITE10-015]; National Research Investigator Board (SNI); National Institutes of Health [R01 A154139]; National Institutes of Health Biodefense and Emerging Infectious Disease training fellowship grant [T32 AI05532901] FX This research was supported by the Secretariat for Science, Technology and Innovation of Panama (SENACYT) research grants COL11-044 and ITE10-015 and the National Research Investigator Board (SNI) prize awarded to JRL, and the National Institutes of Health grant R01 A154139 to JEC. The National Institutes of Health Biodefense and Emerging Infectious Disease training fellowship grant T32 AI05532901 provided partial support for WL. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 99 TC 0 Z9 0 U1 1 U2 4 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1935-2735 J9 PLOS NEGLECT TROP D JI Plos Neglect. Trop. Dis. PD MAY PY 2016 VL 10 IS 5 AR e0004718 DI 10.1371/journal.pntd.0004718 PG 21 WC Infectious Diseases; Parasitology; Tropical Medicine SC Infectious Diseases; Parasitology; Tropical Medicine GA DO4QY UT WOS:000377769300059 PM 27182773 ER PT J AU Eckenweber, M Knornschild, M AF Eckenweber, Maria Knornschild, Mirjam TI Responsiveness to conspecific distress calls is influenced by day-roost proximity in bats (Saccopteryx bilineata) SO ROYAL SOCIETY OPEN SCIENCE LA English DT Article DE distress calls; social relevance; location-dependent responsiveness; social call; Chiroptera ID SAC-WINGED BAT; ECHOLOCATION CALLS; PHYLLOSTOMUS-HASTATUS; EMBALLONURID BATS; FEAR SCREAMS; CHIROPTERA; RECOGNITION; RESPONSES; PREDATOR; BIRDS AB Distress calls signal extreme physical distress, e.g. being caught by a predator. In many bat species, distress calls attract conspecifics. Because bats often occupy perennial day-roosts, they might adapt their responsiveness according to the social relevance in which distress calls are broadcast. Specifically, we hypothesized that conspecific distress calls broadcast within or in proximity to the day-roost would elicit a stronger responsiveness than distress calls broadcast at a foraging site. We analysed the distress calls and conducted playback experiments with the greater sac-winged bat, Saccopteryx bilineata, which occupies perennial day-roosts with a stable social group composition. S. bilineata reacted significantly differently depending on the playback's location. Bats were attracted to distress call playbacks within the day-roost and in proximity to it, but showed no obvious response to distress call playbacks at a foraging site. Hence, the bats adapted their responsiveness towards distress calls depending on the social relevance in which distress calls were broadcast. Distress calls within or in proximity to the day-roost are probably perceived as a greater threat and thus have a higher behavioural relevance than distress calls at foraging sites, either because bats want to assess the predation risk or because they engage in mobbing behaviour. C1 [Eckenweber, Maria] Univ Ulm, Evolutionary Ecol & Conservat Genom, D-89069 Ulm, Germany. [Knornschild, Mirjam] Free Univ Berlin, Inst Biol, Anim Behav Lab, Berlin, Germany. [Knornschild, Mirjam] Smithsonian Trop Res Inst, Balboa, Panama. RP Eckenweber, M (reprint author), Univ Ulm, Evolutionary Ecol & Conservat Genom, D-89069 Ulm, Germany. EM mariaeckenweber@gmail.com FU German Baden-Wurttemberg Stiftung, Eliteprogramme; German Adacemic Exchange Service (DAAD) FX This study was supported by the German Baden-Wurttemberg Stiftung, Eliteprogramme for Postdocs (grant issued to M.K.) and by the German Adacemic Exchange Service (DAAD; grant issued to M.E.). NR 43 TC 2 Z9 2 U1 5 U2 6 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 2054-5703 J9 ROY SOC OPEN SCI JI R. Soc. Open Sci. PD MAY PY 2016 VL 3 IS 5 AR UNSP 160151 DI 10.1098/rsos.160151 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DO7NR UT WOS:000377969800022 PM 27293797 ER PT J AU Lima, RAF Muller-Landau, HC Prado, PI Condit, R AF Lima, Renato A. F. Muller-Landau, Helene C. Prado, Paulo I. Condit, Richard TI How do size distributions relate to concurrently measured demographic rates? Evidence from over 150 tree species in Panama SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Barro Colorado Island; demographic equilibrium theory; diameter distribution; El Nino effects; forest structure; population growth; Weibull distribution ID MIXED DIPTEROCARP FOREST; TROPICAL FOREST; EL-NINO; MORTALITY-RATES; DIAMETER DISTRIBUTIONS; SEVERE DROUGHT; RAIN-FOREST; GROWTH; IMPACT; RECRUITMENT AB In stable populations with constant demographic rates, size distributions reflect size-dependent patterns of growth and mortality. However, population growth can also affect size distributions, which may not be aligned with current growth and mortality. Using 25 y of demographic data from the 50-ha Barro Colorado Island plot, we examined how interspecific variation in diameter distributions of over 150 tropical trees relates to growth-diameter and mortality-diameter curves and to population growth rates. Diameter distributions were more skewed in species with faster increases/slower decreases in absolute growth and mortality with diameter and higher population growth rates. The strongest predictor of the diameter distribution shape was the exponent governing the scaling of growth with diameter (partial R-2 = 0.20-0.34), which differed among growth forms, indicating a role of life history variation. However, interspecific variation in diameter distributions was also significantly related to population growth rates (partial R-2 = 0.03-0.23), reinforcing that many populations are not at equilibrium. Consequently, although fitted size distribution parameters were positively related to theoretical predictions based on current size-dependent growth and mortality, there was considerable deviation. These analyses show that temporally variable demographic rates, probably related to cyclic climate variation, are important influences on forest structure. C1 [Lima, Renato A. F.; Prado, Paulo I.] Univ Sao Paulo, Dept Ecol, Lab Ecol Teor, BR-05508090 Sao Paulo, Brazil. [Muller-Landau, Helene C.; Condit, Richard] Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Ancon, Panama. RP Lima, RAF (reprint author), Univ Sao Paulo, Dept Ecol, Lab Ecol Teor, BR-05508090 Sao Paulo, Brazil. EM raflima@usp.br RI Prado, Paulo/G-3353-2012 FU Center for Tropical Forest Science (CTFS); US National Science Foundation; World Wildlife Fund; Earthwatch Center for Field Studies; CAPES [09/53413-5, 2013/08722-5]; Sao Paulo Research Foundation (FAPESP); CNPq [303878/2008-8]; US National Science Foundation [DEB-1046113]; John D. and Catherine T. MacArthur Foundation; Smithsonian Tropical Research Institute FX We thank the Center for Tropical Forest Science (CTFS), especially Stuart Davies, for support. We are grateful to R. Foster, S. Lao, R. Perez, S. Aguilar, A. Hernandez and many field assistants for species identifications, tree measurements and database management. We also thank Nadja Ruger for helpful comments and for providing the digital version of the growth rate estimates of BCI species from Ruger & Condit (2012). The 30 years of monitoring of the BCI plot was funded by the US National Science Foundation, the John D. and Catherine T. MacArthur Foundation, the World Wildlife Fund, the Earthwatch Center for Field Studies and the Smithsonian Tropical Research Institute. RAFL was supported by CAPES and by grants#09/53413-5 and #2013/08722-5, Sao Paulo Research Foundation (FAPESP). PIP was supported by CNPq (grant 303878/2008-8). This manuscript was substantially advanced during the CTFS/SIGEO analytical workshop funded by the US National Science Foundation (DEB-1046113). NR 36 TC 1 Z9 1 U1 0 U2 6 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 EI 1469-7831 J9 J TROP ECOL JI J. Trop. Ecol. PD MAY PY 2016 VL 32 BP 179 EP 192 DI 10.1017/S0266467416000146 PN 3 PG 14 WC Ecology SC Environmental Sciences & Ecology GA DN7YT UT WOS:000377296800001 ER PT J AU Mesa-Cruz, JB Brown, JL Waits, LP Kelly, MJ AF Mesa-Cruz, J. Bernardo Brown, Janine L. Waits, Lisette P. Kelly, Marcella J. TI Non-invasive genetic sampling reveals diet shifts, but little difference in endoparasite richness and faecal glucocorticoids, in Belizean felids inside and outside protected areas SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Belize; diet; endoparasites; faecal glucocorticoids; habitat modification; jaguar; jaguarundi; molecular scatology; ocelot; puma ID JAGUAR PANTHERA-ONCA; OCELOTS LEOPARDUS-PARDALIS; SCAT DETECTION DOGS; PUMA PUMA-CONCOLOR; ADRENOCORTICAL ACTIVITY; SYMPATRIC JAGUARS; STRESS RESPONSES; CENTRAL-AMERICA; DNA; BEHAVIOR AB Many Neotropical felids are threatened with extinction due to direct effects of habitat destruction and/or human persecution. However, indirect and synergistic effects of human-felid conflict remain under-studied and potentially include increased stress and diet shifts that may negatively impact felid health. We hypothesized that faecal glucocorticoid metabolites (FGM) and endoparasite species richness (ESR) would be higher, and diet would shift, for felids outside protected areas where conflict occurs. In north-western Belize, a scat-detector dog located 336 faecal samples, identified to species and individual using DNA analyses. DNA amplification success was substantially higher within protected areas than outside. We detected jaguar, puma, ocelot, jaguarundi and domestic cat. FGMs were higher in puma and jaguarundi than in other felids, while ESR was similar across felids with domestic cats exhibiting the highest number of genera. Diet partitioning occurred among felids, but domestic cats may compete with ocelot and jaguarundi for small prey. Outside of protected areas, large cats shifted their diet to smaller prey and livestock remains were not found. Contrary to our hypotheses, FGM and ESR did not differ inside versus outside protected areas, but sample sizes were low in human-modified areas. We provide a baseline on wild felid adrenal activity, endoparasites and diet and suggest improvements to increase sample sizes outside protected areas. Our research provides a template for expanding non-invasive sampling approaches more widely across the range of Neotropical felids. C1 [Mesa-Cruz, J. Bernardo; Kelly, Marcella J.] Virginia Polytech Inst & State Univ, Dept Fish & Wildlife Conservat, 100 Cheatham Hall, Blacksburg, VA 24061 USA. [Mesa-Cruz, J. Bernardo; Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA. [Waits, Lisette P.] Univ Idaho, Dept Fish & Wildlife Sci, 875 Perimeter Dr, Moscow, ID 83844 USA. RP Mesa-Cruz, JB (reprint author), Virginia Polytech Inst & State Univ, Dept Fish & Wildlife Conservat, 100 Cheatham Hall, Blacksburg, VA 24061 USA.; Mesa-Cruz, JB (reprint author), Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA. EM bmesa@vt.edu FU Conservation, Research, and Education Opportunities (CREO); Cleveland Zoo's Scott Neotropical Fund; Smithsonian Institution; Philadelphia Zoo; Virginia Tech's Graduate School; Department of Fish and Wildlife Conservation at Virginia Tech FX We thank our funding institutions: Conservation, Research, and Education Opportunities (CREO), Cleveland Zoo's Scott Neotropical Fund, Smithsonian Institution, the Philadelphia Zoo, Virginia Tech's Graduate School, and the Department of Fish and Wildlife Conservation at Virginia Tech. We give special thanks to the Lamanai Field Research Center and the Lamanai Outpost Lodge for hosting the team while performing the field survey. We also thank the Belize Zoo and the Tropical Education Center (TEC), the director, Sharon Matola and keeper staff for their collaboration on diet reference sample collection. We thank endocrine laboratory manager, Nicole Presley at SCBI, PackLeader LLC for their training support and detector dog, 'C. J.'. Christine Proctor, Claudia Wultsch, Jennifer Adams and David Montague, provided field and technical support. Julie Golla, Christopher Satter and numerous other field technicians made scat collection surveys possible. We thank laboratory technicians Ankit Patel and Clark De Hart for their assistance in prey remains sorting and parasite processing. We also thank Dr William Hopkins and anonymous reviewers for comments on the manuscript. NR 63 TC 1 Z9 1 U1 5 U2 14 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 EI 1469-7831 J9 J TROP ECOL JI J. Trop. Ecol. PD MAY PY 2016 VL 32 BP 226 EP 239 DI 10.1017/S0266467416000213 PN 3 PG 14 WC Ecology SC Environmental Sciences & Ecology GA DN7YT UT WOS:000377296800005 ER PT J AU Douglas, ST Agueros, MA Covey, KR Cargile, PA Barclay, T Cody, A Howell, SB Kopytova, T AF Douglas, S. T. Agueeros, M. A. Covey, K. R. Cargile, P. A. Barclay, T. Cody, A. Howell, S. B. Kopytova, T. TI K2 ROTATION PERIODS FOR LOW-MASS HYADS AND THE IMPLICATIONS FOR GYROCHRONOLOGY SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations: individual (Hyades); stars: evolution; stars: late-type; stars: low-mass; stars: rotation ID ANGULAR-MOMENTUM EVOLUTION; RADIAL-VELOCITY SURVEY; DIGITAL SKY SURVEY; OPEN-CLUSTER; M-DWARFS; SPECTROSCOPIC ORBITS; LUMINOSITY RELATIONS; HIPPARCOS CATALOG; MAGNETIC-FIELDS; PROPER MOTIONS AB As the closest open cluster to the Sun, the Hyades is an important benchmark for many stellar properties, but its members are also scattered widely over the sky. Previous studies of stellar rotation in the Hyades relied on targeted observations of single stars or data from shallower all-sky variability surveys. The re-purposed Kepler mission, K2, is the first opportunity to measure rotation periods (P-rot) for many Hyads simultaneously while also being sensitive to fully convective M dwarf members. We analyze K2 data for 65 Hyads and present P-rot values for 48. Thirty-seven of these are new measurements, including the first P-rot measurements for fully convective Hyads. For 9 of the 11 stars with P-rot in the literature and this work, the measurements are consistent; we attribute the two discrepant cases to spot evolution. Nearly all stars with masses less than or similar to 0.3 M-circle dot are rapidly rotating, indicating a change in rotation properties at the boundary to full convection. When confirmed and candidate binaries are removed from the mass-period plane, only three rapid rotators with masses greater than or similar to 0.3 M-circle dot remain. This is in contrast to previous results showing that the single-valued mass-period sequence for approximate to 600 Myr old stars ends at approximate to 0.65 M-circle dot when binaries are included. We also find that models of rotational evolution predict faster rotation than is actually observed at approximate to 600 Myr for stars less than or similar to 0.9M(circle dot). The dearth of single rapid rotators more massive than approximate to 0.3M(circle dot) indicates that magnetic braking is more efficient than previously thought, and that age-rotation studies must account for multiplicity. C1 [Douglas, S. T.; Agueeros, M. A.] Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA. [Covey, K. R.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Cargile, P. A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Barclay, T.; Cody, A.; Howell, S. B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kopytova, T.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Kopytova, T.] Heidelberg Univ, Int Max Planck Res Sch Astron & Cosm Phys, IMPRS HD, Bergheimer Str 58, D-69115 Heidelberg, Germany. RP Douglas, ST (reprint author), Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA. OI Douglas, Stephanie/0000-0001-7371-2832; Covey, Kevin/0000-0001-6914-7797; Agueros, Marcel/0000-0001-7077-3664 FU NSF [AST-1255419, AST-1517367, AST-1449476]; NASA Science Mission directorate; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; U.S. Government grant [NAG W-2166]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX S.T.D.. gratefully acknowledges the hospitality of the Kepler/K2 Science Team at NASA Ames Research Center, particularly the advice and support of Geert Barentsen, Knicole Colon, Mike Haas, Mark Messersmith, Fergal Mullally, and Susan. E. Thompson. We thank Sean Matt, Subu Mohanty, and Ansgar Reiners for discussing and sharing their models with us, and Ruth Angus and Dan Foreman-Mackey for useful discussions and advice. We also thank Alisha Kundert for her work on the Hyades catalog and ASAS analysis. M.A.A.. acknowledges support provided by the NSF through grants AST-1255419 and AST-1517367. K.R.C.. acknowledges support provided by the NSF through grant AST-1449476. We thank the anonymous referee for their critique, which improved the paper.; This paper includes data collected by the K2 mission. Funding for the K2 mission is provided by the NASA Science Mission directorate. 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.; The Digitized Sky Survey was produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions.; 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. NR 81 TC 4 Z9 4 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 MAY 1 PY 2016 VL 822 IS 1 AR 47 DI 10.3847/0004-637X/822/1/47 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6AS UT WOS:000377154100047 ER PT J AU Gagne, J Plavchan, P Gao, P Anglada-Escude, G Furlan, E Davison, C Tanner, A Henry, TJ Riedel, AR Brinkworth, C Latham, D Bottom, M White, R Mills, S Beichman, C Johnson, JA Ciardi, DR Wallace, K Mennesson, B von Braun, K Vasisht, G Prato, L Kane, SR Mamajek, EE Walp, B Crawford, TJ Rougeot, R Geneser, CS Catanzarite, J AF Gagne, Jonathan Plavchan, Peter Gao, Peter Anglada-Escude, Guillem Furlan, Elise Davison, Cassy Tanner, Angelle Henry, Todd J. Riedel, Adric R. Brinkworth, Carolyn Latham, David Bottom, Michael White, Russel Mills, Sean Beichman, Chas Johnson, John A. Ciardi, David R. Wallace, Kent Mennesson, Bertrand von Braun, Kaspar Vasisht, Gautam Prato, Lisa Kane, Stephen R. Mamajek, Eric E. Walp, Bernie Crawford, Timothy J. Rougeot, Raphael Geneser, Claire S. Catanzarite, Joseph TI A HIGH-PRECISION NEAR-INFRARED SURVEY FOR RADIAL VELOCITY VARIABLE LOW-MASS STARS USING CSHELL AND A METHANE GAS CELL SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: detection; stars: low-mass; techniques: radial velocities; Supporting material: figure set; machine-readable tables ID YOUNG MOVING GROUPS; ANGULAR-MOMENTUM EVOLUTION; STELLAR KINEMATIC GROUPS; MAIN-SEQUENCE STARS; EXTRA-SOLAR PLANETS; EARTH-SIZED PLANET; FIELD M-DWARFS; VERY-LOW MASS; M-CIRCLE-PLUS; CA-II H AB We present the results of a precise near-infrared (NIR) radial velocity (RV) survey of 32 low-mass stars with spectral types K2-M4 using CSHELL at the NASA InfraRed Telescope Facility in the K band with an isotopologue methane gas cell to achieve wavelength calibration and a novel, iterative RV extraction method. We surveyed 14 members of young (approximate to 25-150 Myr) moving groups, the young field star epsilon. Eridani, and 18 nearby (< 25 pc) low-mass stars and achieved typical single-measurement precisions of 8-15 m s(-1) with a long-term stability of 15-50 m s(-1) over longer baselines. We obtain the best NIR RV constraints to date on 27 targets in our sample, 19 of which were never followed by high-precision RV surveys. Our results indicate that very active stars can display long-term RV variations as low as similar to 25-50 m s(-1) at approximate to 2.3125 mu m, thus constraining the effect of jitter at these wavelengths. We provide the first multiwavelength confirmation of GJ. 876. bc and independently retrieve orbital parameters consistent with previous studies. We recovered RV variabilities for HD. 160934. AB and GJ. 725. AB that are consistent with their known binary orbits, and nine other targets are candidate RV variables with a statistical significance of 3s-5s. Our method, combined with the new iSHELL spectrograph, will yield long-term RV precisions of. 5 m s(-1) in the NIR, which will allow the detection of super-Earths near the habitable zone of mid-M dwarfs. C1 [Gagne, Jonathan] Carnegie Inst Washington DTM, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. [Plavchan, Peter] Missouri State Univ, Dept Phys, 901 S Natl Ave, Springfield, MO 65897 USA. [Gao, Peter] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Anglada-Escude, Guillem] Queen Mary Univ London, Sch Phys & Astron, 327 Mile End Rd, London E1 4NS, England. [Anglada-Escude, Guillem] Univ Hertfordshire, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, Herts, England. [Furlan, Elise; Brinkworth, Carolyn] NASA, Exoplanet Sci Inst, CALTECH, 770 S Wilson Ave, Pasadena, CA 91125 USA. [Davison, Cassy; Henry, Todd J.; White, Russel] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Tanner, Angelle] Mississippi State Univ, Dept Phys & Astron, Hilbun Hall, Starkville, MS 39762 USA. [Riedel, Adric R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Brinkworth, Carolyn] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. [Mills, Sean] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Beichman, Chas] NASA, Exoplanet Sci Inst, CALTECH, Pasadena, CA 91125 USA. [Johnson, John A.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. [Bottom, Michael] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Wallace, Kent; Mennesson, Bertrand; Vasisht, Gautam; Crawford, Timothy J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. [von Braun, Kaspar; Prato, Lisa] Lowell Observ, West Mars Hill Rd, Flagstaff, AZ 86001 USA. [Kane, Stephen R.] San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA. [Mamajek, Eric E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Walp, Bernie] NASA, Stratospher Observ Infrared Astron, Dryden Flight Res Ctr, Mail Stop DAOF, S233,POB 273, Edwards AFB, CA 93523 USA. [Rougeot, Raphael] ESA, European Space Res & Technol Ctr, Keplerlaan 1, NL-2201 Noordwijk, Netherlands. [Catanzarite, Joseph] NASA, Ames Res Ctr, MS 245-3,POB 1, Moffett Field, CA 94035 USA. RP Gagne, J (reprint author), Carnegie Inst Washington DTM, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. EM jgagne@carnegiescience.edu; peterplavchan@missouristate.edu OI Anglada Escude, Guillem/0000-0002-3645-5977; Ciardi, David/0000-0002-5741-3047 FU Engineering Research Council of Canada; iREx postdoctoral fellowship; JPL Research and Technology Development Grant; National Aeronautics and Space Administration (NASA) through the Sagan Fellowship Program FX We thank the anonymous referee who provided valuable comments and suggestions that significantly improved the overall quality of this paper. We thank Jason Wright, Julien Rameau, tienne Artig, David Montes, and Noe AubinCadot for useful comments and discussions, as well as Keeyoon Sung, Sam Crawford, Brian Drouin, Edgardo Garcia-Berrios, Nathan S. Lewis, and S. Lin for precious help in the construction and setup of the methane isotopologue gas cell. We thank the IRTF staff for their collaboration and help throughout this project, in particular John Rayner, Lars Bergknut, Bobby Bus, and the telescope operators. This work was supported in part through an Infrared Processing and Analysis Center (IPAC) fellowship, a grant from the Fond de Recherche Quebecois-Nature et Technologie and the Natural Science, a grant from the Engineering Research Council of Canada, an iREx postdoctoral fellowship, and a JPL Research and Technology Development Grant. This work was performed in part under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by the National Aeronautics and Space Administration (NASA) through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. This research made use of the SIMBAD database and VizieR catalog access tool, operated at the Centre de Donnes Astronomiques de Strasbourg, France (Ochsenbein et al. 2000); data products from the Two Micron All Sky Survey (2MASS; Kirkpatrick et al. 2003; Skrutskie et al. 2006), which is a joint project of the University of Massachusetts and IPAC/Caltech, funded by NASA and the National Science Foundation; the Extrasolar Planets Encyclopaedia (exoplanet. eu), which was developed and is maintained by the exoplanet TEAM; the NASA Exoplanet Archive, which is operated by Caltech, under contract with NASA under the Exoplanet Exploration Program; the NASA/IPAC Infrared Science Archive (IRSA), which is operated by JPL, Caltech, under contract with NASA; the IRTF, which is operated by the University of Hawaii under Cooperative Agreement NNX08AE38A with NASA, Science Mission Directorate, Planetary Astronomy Program. This publication uses observations obtained at IRTF through program numbers 2010B022, 2011A083, 2011B083, 2012A065, 2012B021, 2014A048, 2014B082, and 2015B043, as well as through engineering time in the 2012A and 2012B semesters. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 155 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2016 VL 822 IS 1 DI 10.3847/0004-637X/822/1/40 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6AS UT WOS:000377154100040 ER PT J AU Guillochon, J McCourt, M Chen, X Johnson, MD Berger, E AF Guillochon, James McCourt, Michael Chen, Xian Johnson, Michael D. Berger, Edo TI UNBOUND DEBRIS STREAMS AND REMNANTS RESULTING FROM THE TIDAL DISRUPTIONS OF STARS BY SUPERMASSIVE BLACK HOLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; gravitation; quasars: supermassive black holes ID SAGITTARIUS-A-EAST; X-RAY ECHO; GALACTIC-CENTER; SUPERNOVA-REMNANTS; INTERSTELLAR-MEDIUM; STELLAR DISRUPTION; ACCRETION FLOW; WHITE-DWARFS; ECCENTRIC ORBITS; GIANT PLANETS AB The kinetic energy of a star in orbit about a supermassive black hole is a significant fraction of its rest mass energy when its periapse is comparable to its tidal radius. Upon its destruction, a fraction of this energy is extracted and injected into the stellar debris, half of which becomes unbound from the black hole, with the fastest material moving at similar to 0.03c. In this paper, we present a formalism for determining the fate of these unbound debris streams (UDSs) as they depart from the black hole and interact with the surrounding gas. As the density and velocity varies along the length of a UDS, we find that hydrodynamical drag quickly shapes UDSs into loop-like structures, with the densest portions of the streams leading portions of lower density. As UDSs travel outwards, their drag against the ISM increases quadratically with distance, which causes UDSs to deposit their momentum and energy into the ambient medium before the surrounding shocked ISM has a chance to cool. This sudden injection of similar to 10(50) erg into the ambient medium generates a Sedov-like unbound debris remnant (UDR) that mimics supernova remnants (SNRs) in energetics and appearance, accelerates particles which will produce cosmic rays and synchrotron emission, and provides momentum feedback into the molecular clouds surrounding a black hole. We estimate that a few of these UDRs might be present within a couple degrees of the Galactic Center masquerading as SNRs, and that the UDR scenario is a plausible explanation for Sgr. A. east. C1 [Guillochon, James; McCourt, Michael; Johnson, Michael D.; Berger, Edo] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. [Chen, Xian] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile. RP Guillochon, J (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM jguillochon@cfa.harvard.edu OI McCourt, Michael/0000-0003-4531-7733; Chen, Xian/0000-0003-3950-9317; Guillochon, James/0000-0002-9809-8215 FU Einstein grant [PF3-140108]; National Science Foundation grant [AST-1312651]; NASA [NNX15AK81G]; CONICYT-Chile [ACT1101]; Gordon and Betty Moore Foundation [GBMF-3561] FX We thank MC Miller, D. Finkbeiner, A. Kamble, A. Loeb, L. Lopez, M. MacLeod, EAC. Mills, R. O'Leary, H. Perets, G. Ponti, L. Sironi, P. Slane, and A. Soderberg for useful discussions, and we thank the anonymous referee for their constructive comments. This work was supported by Einstein grant PF3-140108 (J. G.), National Science Foundation grant AST-1312651 and NASA grant NNX15AK81G (M. M.), CONICYT-Chile through Anillo ACT1101 (X. C.), and the Gordon and Betty Moore Foundation GBMF-3561 (M. J.). NR 123 TC 5 Z9 5 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2016 VL 822 IS 1 AR 48 DI 10.3847/0004-637X/822/1/48 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6AS UT WOS:000377154100048 ER PT J AU Herron, CA Burkhart, B Lazarian, A Gaensler, BM McClure-Griffiths, NM AF Herron, C. A. Burkhart, Blakesley Lazarian, A. Gaensler, B. M. McClure-Griffiths, N. M. TI RADIO SYNCHROTRON FLUCTUATION STATISTICS AS A PROBE OF MAGNETIZED INTERSTELLAR TURBULENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: structure; magnetic fields; magnetohydrodynamics (MHD); methods: data analysis; turbulence ID MHD TURBULENCE; MAGNETOHYDRODYNAMIC TURBULENCE; ASTROPHYSICAL IMPLICATIONS; SPECTRAL INDEX; ANISOTROPY; GRADIENTS; EMISSION; FIELD; HI AB We investigate how observations of synchrotron intensity fluctuations can be used to probe the sonic and Alfvenic Mach numbers of interstellar turbulence, based on mock observations performed on simulations of magnetohydrodynamic turbulence. We find that the structure function slope and a diagnostic of anisotropy that we call the integrated quadrupole ratio modulus both depend on the Alfvenic Mach number. However, these statistics also depend on the orientation of the mean magnetic field in the synchrotron emitting region relative to our line of sight, and this creates a degeneracy that cannot be broken by observations of synchrotron intensity alone. We conclude that the polarization of synchrotron emission could be analyzed to break this degeneracy, and suggest that this will be possible with the Square Kilometre Array. C1 [Herron, C. A.; Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Burkhart, Blakesley] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Lazarian, A.] Univ Wisconsin, Dept Astron, 475 N Charter St, Madison, WI 53711 USA. [Gaensler, B. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. [McClure-Griffiths, N. M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. RP Herron, CA (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. EM C.Herron@physics.usyd.edu.au OI Gaensler, Bryan/0000-0002-3382-9558 FU Australian Postgraduate Award; University of Sydney; NASA Einstein Postdoctoral Fellowship; NSF [AST 1212096]; Center for Magnetic Self Organization (CMSO); Australian Research Council [FL100100114]; Dunlap Institute for Astronomy and Astrophysics FX C.A.H. thanks Xiaohui Sun for his help in estimating the sensitivity required to observe synchrotron intensity fluctuations, Geraint Lewis for his supervision, and useful discussions on the real and imaginary parts of the quadrupole ratio, and Christoph Federrath for useful discussions. C.A.H. also thanks Snezana Stanimirovic, Claire Murray, Elijah Bernstein-Cooper, Bob Lindner and Brian Babler for their hospitality and useful discussions whilst at the University of Wisconsin-Madison. C.A.H. acknowledges financial support received via an Australian Postgraduate Award, and a Vice Chancellor's Research Scholarship awarded by the University of Sydney. The research of B.B. is supported by the NASA Einstein Postdoctoral Fellowship. A.L. acknowledges the NSF grant AST 1212096 and the support of the Center for Magnetic Self Organization (CMSO). A.L. acknowledges a distinguished visitor PVE/CAPES appointment at the Physics Graduate Program of the Federal University of Rio Grande do Norte and thanks the INCT INEspao and Physics Graduate Program/UFRN for hospitality. B.M.G. acknowledges the support of the Australian Research Council through grant FL100100114. The Dunlap Institute for Astronomy and Astrophysics is funded through an endowment established by the David Dunlap family and the University of Toronto. NR 42 TC 5 Z9 5 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 MAY 1 PY 2016 VL 822 IS 1 AR 13 DI 10.3847/0004-637X/822/1/13 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6AS UT WOS:000377154100013 ER PT J AU Lotti, S Natalucci, L Mori, K Baganoff, FK Boggs, SE Christensen, FE Craig, WW Hailey, CJ Harrison, FA Hong, J Krivonos, RA Rahoui, F Stern, D Tomsick, JA Zhang, S Zhang, WW AF Lotti, Simone Natalucci, Lorenzo Mori, Kaya Baganoff, Frederick K. Boggs, Steven E. Christensen, Finn E. Craig, William W. Hailey, Charles J. Harrison, Fiona A. Hong, Jaesub Krivonos, Roman A. Rahoui, Farid Stern, Daniel Tomsick, John A. Zhang, Shuo Zhang, William W. TI NUSTAR AND XMM-NEWTON OBSERVATIONS OF 1E1743.1-2843: INDICATIONS OF A NEUTRON STAR LMXB NATURE OF THE COMPACT OBJECT SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: neutron; X-rays: binaries; X-rays: individual (1E1743.1-2843) ID X-RAY BINARIES; GALACTIC PLANE SURVEY; SOURCE 1E 1743.1-2843; EMISSION; ASCA; LIKELIHOOD; DISCOVERY; CATALOG; BURSTS; UKIDSS AB We report on the results of NuSTAR and XMM-Newton observations of the persistent X-ray source 1E1743.1-2843, located in the Galactic Center region. The source was observed between 2012 September and October by NuSTAR and XMM-Newton, providing almost simultaneous observations in the hard and soft X-ray bands. The high X-ray luminosity points to the presence of an accreting compact object. We analyze the possibilities of this accreting compact object being either a neutron star (NS) or a black hole, and conclude that the joint XMM-Newton and NuSTAR spectrum from 0.3 to 40 keV fits a blackbody spectrum with kT similar to 1.8 keV emitted from a hot spot or an equatorial strip on an NS surface. This spectrum is thermally Comptonized by electrons with kT(e) similar to 4.6 keV. Accepting this NS hypothesis, we probe the low-mass X-ray binary (LMXB) or high-mass X-ray binary (HMXB) nature of the source. While the lack of Type-I bursts can be explained in the LMXB scenario, the absence of pulsations in the 2 mHz-49 Hz frequency range, the lack of eclipses and of an IR companion, and the lack of a K-alpha line from neutral or moderately ionized iron strongly disfavor interpreting this source as a HMXB. We therefore conclude that 1E1743.1-2843 is most likely an NS-LMXB located beyond the Galactic Center. There is weak statistical evidence for a soft X-ray excess which may indicate thermal emission from an accretion disk. However, the disk normalization remains unconstrained due to the high hydrogen column density (N-H similar to 1.6 x 10(23) cm(-2)). C1 [Lotti, Simone; Natalucci, Lorenzo] INAF IAPS Roma, Via Fosso Cavaliere 100, I-00133 Rome, Italy. [Mori, Kaya] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. [Baganoff, Frederick K.; Craig, William W.; Hailey, Charles J.; Zhang, Shuo] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Boggs, Steven E.; Craig, William W.; Krivonos, Roman A.; Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. [Christensen, Finn E.] DTU Space, Natl Space Inst, Elektrovej 327, DK-2800 Lyngby, Denmark. [Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Hong, Jaesub] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Krivonos, Roman A.] Russian Acad Sci, Space Res Inst, Profsoyuznaya 84-32, Moscow 117997, Russia. [Rahoui, Farid] Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA. [Rahoui, Farid] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lotti, S (reprint author), INAF IAPS Roma, Via Fosso Cavaliere 100, I-00133 Rome, Italy. EM simone.lotti@iaps.inaf.it RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; lotti, simone/0000-0002-3088-1561 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; ASI/INAF [I/037/12/0]; Russian Science Foundation [14-22-00271] 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). The Italian authors acknowledge the Italian Space Agency (ASI) for financial support by ASI/INAF grant I/037/12/0. R.K. acknowledges support from Russian Science Foundation (grant 14-22-00271). NR 46 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2016 VL 822 IS 1 AR 57 DI 10.3847/0004-637X/822/1/57 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6AS UT WOS:000377154100057 ER PT J AU Padoan, P Pan, LB Haugbolle, T Nordlund, A AF Padoan, Paolo Pan, Liubin Haugbolle, Troels Nordlund, Ake TI SUPERNOVA DRIVING. I. THE ORIGIN OF MOLECULAR CLOUD TURBULENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: kinematics and dynamics; magnetohydrodynamics (MHD); stars: formation; turbulence ID INITIAL MASS FUNCTION; GALACTIC RING SURVEY; CORE-COLLAPSE SUPERNOVAE; STAR-FORMATION RATE; SUPERSONIC ISOTHERMAL TURBULENCE; FULLY-DEVELOPED TURBULENCE; INTERSTELLAR-MEDIUM; MAGNETIC-FIELD; DRIVEN TURBULENCE; SCALING RELATIONS AB Turbulence is ubiquitous in molecular clouds (MCs), but its origin is still unclear because MCs are usually assumed to live longer than the turbulence dissipation time. Interstellar medium (ISM) turbulence is likely driven by supernova (SN) explosions, but it has never been demonstrated that SN explosions can establish and maintain a turbulent cascade inside MCs consistent with the observations. In this work, we carry out a simulation of SN-driven turbulence in a volume of (250 pc)(3), specifically designed to test if SN driving alone can be responsible for the observed turbulence inside MCs. We find that SN driving establishes a velocity scaling consistent with the usual scaling laws of supersonic turbulence, suggesting that previous idealized simulations of MC turbulence, driven with a random, large-scale volume force, were correctly adopted as appropriate models for MC turbulence, despite the artificial driving. We also find that the same scaling laws extend to the interiors of MCs, and that the velocity-size relation of the MCs selected from our simulation is consistent with that of MCs from the Outer-Galaxy Survey, the largest MC sample available. The mass-size relation and the mass and size probability distributions also compare successfully with those of the Outer Galaxy Survey. Finally, we show that MC turbulence is super-Alfvenic with respect to both the mean and rms magnetic-field strength. We conclude that MC structure and dynamics are the natural result of SN-driven turbulence. C1 [Padoan, Paolo] Univ Barcelona, ICREA, IEEC UB, Marti Franques 1, E-08028 Barcelona, Spain. [Padoan, Paolo] Univ Barcelona, Inst Ciencies Cosmos, IEEC UB, Marti Franques 1, E-08028 Barcelona, Spain. [Pan, Liubin] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Haugbolle, Troels; Nordlund, Ake] Univ Copenhagen, Ctr Star & Planet Format, Niels Bohr Inst, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. [Haugbolle, Troels; Nordlund, Ake] Univ Copenhagen, Nat Hist Museum Denmark, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. RP Padoan, P (reprint author), Univ Barcelona, ICREA, IEEC UB, Marti Franques 1, E-08028 Barcelona, Spain.; Padoan, P (reprint author), Univ Barcelona, Inst Ciencies Cosmos, IEEC UB, Marti Franques 1, E-08028 Barcelona, Spain.; Pan, LB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Haugbolle, T; Nordlund, A (reprint author), Univ Copenhagen, Ctr Star & Planet Format, Niels Bohr Inst, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark.; Haugbolle, T; Nordlund, A (reprint author), Univ Copenhagen, Nat Hist Museum Denmark, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. EM ppadoan@icc.ub.edu; lpan@cfa.harvard.edu; haugboel@nbi.ku.dk; aake@nbi.ku.dk OI Padoan, Paolo/0000-0002-5055-5800 FU ERC FP7-PEOPLE-RG grant [PIRG07-GA-2010-261359]; Spanish MINECO [AYA2014-57134-P]; Sapere Aude Starting Grant from The Danish Council for Independent Research; Danish National Research Foundation; University of Copenhagen's programme of excellence FX We are grateful to Christoph Federrath and the anonymous referee for providing useful comments and corrections. Computing resources for this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center, by PRACE through a Tier-0 award providing us access to the computing resource SuperMUC based in Germany at the Leibniz Supercomputing Center, and by the Port d'Informacio Cientifica (PIC), Spain, maintained by a collaboration of the Institut de Fisica d'Altes Energies (IFAE) and the Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas (CIEMAT). P.P. acknowledges support by the ERC FP7-PEOPLE-2010-RG grant PIRG07-GA-2010-261359 and by the Spanish MINECO under project AYA2014-57134-P. T.H. is supported by a Sapere Aude Starting Grant from The Danish Council for Independent Research. Research at Centre for Star and Planet Formation was funded by the Danish National Research Foundation and the University of Copenhagen's programme of excellence. NR 106 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2016 VL 822 IS 1 AR 11 DI 10.3847/0004-637X/822/1/11 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6AS UT WOS:000377154100011 ER PT J AU Rice, TS Goodman, AA Bergin, EA Beaumont, C Dame, TM AF Rice, Thomas S. Goodman, Alyssa A. Bergin, Edwin A. Beaumont, Christopher Dame, T. M. TI A UNIFORM CATALOG OF MOLECULAR CLOUDS IN THE MILKY WAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: general; ISM: clouds; ISM: molecules ID GALACTIC RING SURVEY; LARGE-MAGELLANIC-CLOUD; FAR-OUTER GALAXY; DEEP CO SURVEY; STAR-FORMATION; PHYSICAL-PROPERTIES; 3-DIMENSIONAL DISTRIBUTION; TRIGONOMETRIC PARALLAXES; NEARBY GALAXIES; SOLAR CIRCLE AB The all-Galaxy CO survey of Dame et al. is by far the most uniform, large-scale Galactic CO survey. Using a dendrogram-based decomposition of this survey, we present a catalog of 1064 massive molecular clouds throughout the Galactic plane. This catalog contains 2.5. x 10(8) solar masses, or 25(-5.8)(+10.7)% of the Milky Way's estimated H-2 mass. We track clouds in some spiral arms through multiple quadrants. The power index of Larson's first law, the size-linewidth relation, is consistent with 0.5 in all regions-possibly due to an observational bias-but clouds in the inner Galaxy systematically have significantly (similar to 30%) higher linewidths at a given size, indicating that their linewidths are set in part by the Galactic environment. The mass functions of clouds in the inner Galaxy versus the outer Galaxy are both qualitatively and quantitatively distinct. The inner Galaxy mass spectrum is best described by a truncated power law with a power index of gamma = -1.6 +/- 0.1 and an upper truncation mass of M-0 = (1.0 +/- 0.2) x 10(7) M-circle dot, while the outer Galaxy mass spectrum is better described by a non-truncating power law with gamma = -2.2 +/- 0.1 and an upper mass of M-0 = (1.5 +/- 0.5) x 10(6) M-circle dot, indicating that the inner Galaxy is able to form and host substantially more massive GMCs than the outer Galaxy. Additionally, we have simulated how the Milky Way would appear in CO from extragalactic perspectives, for comparison with CO maps of other galaxies. C1 [Rice, Thomas S.; Bergin, Edwin A.] Univ Michigan, Dept Astron, 311 West Hall,1085 South Univ Ave, Ann Arbor, MI 48109 USA. [Goodman, Alyssa A.; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Beaumont, Christopher] Counsyl, 180 Kimball Way, San Francisco, CA 94080 USA. RP Rice, TS (reprint author), Univ Michigan, Dept Astron, 311 West Hall,1085 South Univ Ave, Ann Arbor, MI 48109 USA. EM tsrice@umich.edu OI Goodman, Alyssa/0000-0003-1312-0477 NR 73 TC 4 Z9 4 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 MAY 1 PY 2016 VL 822 IS 1 AR 52 DI 10.3847/0004-637X/822/1/52 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN6AS UT WOS:000377154100052 ER PT J AU Coughlin, JL Mullally, F Thompson, SE Rowe, JF Burke, CJ Latham, DW Batalha, NM Ofir, A Quarles, BL Henze, CE Wolfgang, A Caldwell, DA Bryson, ST Shporer, A Catanzarite, J Akeson, R Barclay, T Borucki, WJ Boyajian, TS Campbell, JR Christiansen, JL Girouard, FR Haas, MR Howell, SB Huber, D Jenkins, JM Li, J Patil-Sabale, A Quintana, EV Ramirez, S Seader, S Smith, JC Tenenbaum, P Twicken, JD Zamudio, KA AF Coughlin, Jeffrey L. Mullally, F. Thompson, Susan E. Rowe, Jason F. Burke, Christopher J. Latham, David W. Batalha, Natalie M. Ofir, Aviv Quarles, Billy L. Henze, Christopher E. Wolfgang, Angie Caldwell, Douglas A. Bryson, Stephen T. Shporer, Avi Catanzarite, Joseph Akeson, Rachel Barclay, Thomas Borucki, William J. Boyajian, Tabetha S. Campbell, Jennifer R. Christiansen, Jessie L. Girouard, Forrest R. Haas, Michael R. Howell, Steve B. Huber, Daniel Jenkins, Jon M. Li, Jie Patil-Sabale, Anima Quintana, Elisa V. Ramirez, Solange Seader, Shawn Smith, Jeffrey C. Tenenbaum, Peter Twicken, Joseph D. Zamudio, Khadeejah A. TI PLANETARY CANDIDATES OBSERVED BY KEPLER. VII. THE FIRST FULLY UNIFORM CATALOG BASED ON THE ENTIRE 48-MONTH DATA SET (Q1-Q17 DR24) SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; planetary systems; planets and satellites: detection; stars: statistics; surveys; techniques: photometric ID TRANSIT TIMING OBSERVATIONS; FALSE-POSITIVE RATE; SUN-LIKE STARS; ECLIPSING BINARIES; HABITABLE ZONE; LIGHT CURVES; DATA RELEASE; MISSION DATA; LOW-MASS; OCCURRENCE RATES AB We present the seventh Kepler planet candidate (PC) catalog, which is the first catalog to be based on the entire, uniformly processed 48-month Kepler data set. This is the first fully automated catalog, employing robotic vetting procedures to uniformly evaluate every periodic signal detected by the Q1-Q17 Data Release 24 (DR24) Kepler pipeline. While we prioritize uniform vetting over the absolute correctness of individual objects, we find that our robotic vetting is overall comparable to, and in most cases superior to, the human vetting procedures employed by past catalogs. This catalog is the first to utilize artificial transit injection to evaluate the performance of our vetting procedures and to quantify potential biases, which are essential for accurate computation of planetary occurrence rates. With respect to the cumulative Kepler Object of Interest (KOI) catalog, we designate 1478 new KOIs, of which 402 are dispositioned as PCs. Also, 237 KOIs dispositioned as false positives (FPs) in previous Kepler catalogs have their disposition changed to PC and 118 PCs have their disposition changed to FPs. This brings the total number of known KOIs to 8826 and PCs to 4696. We compare the Q1-Q17. DR24 KOI catalog to previous KOI catalogs, as well as ancillary Kepler catalogs, finding good agreement between them. We highlight new PCs that are both potentially rocky and potentially in the habitable zone of their host stars, many of which orbit solar-type stars. This work represents significant progress in accurately determining the fraction of Earth-size planets in the habitable zone of Sun-like stars. The full catalog is publicly available at the NASA Exoplanet Archive. C1 [Coughlin, Jeffrey L.; Mullally, F.; Thompson, Susan E.; Rowe, Jason F.; Burke, Christopher J.; Caldwell, Douglas A.; Catanzarite, Joseph; Campbell, Jennifer R.; Huber, Daniel; Li, Jie; Quintana, Elisa V.; Seader, Shawn; Smith, Jeffrey C.; Tenenbaum, Peter; Twicken, Joseph D.] SETI Inst, 189 Bernardo Ave,Suite 200, Mountain View, CA 94043 USA. [Coughlin, Jeffrey L.; Mullally, F.; Thompson, Susan E.; Rowe, Jason F.; Burke, Christopher J.; Batalha, Natalie M.; Quarles, Billy L.; Henze, Christopher E.; Caldwell, Douglas A.; Bryson, Stephen T.; Catanzarite, Joseph; Barclay, Thomas; Borucki, William J.; Girouard, Forrest R.; Haas, Michael R.; Howell, Steve B.; Jenkins, Jon M.; Li, Jie; Patil-Sabale, Anima; Quintana, Elisa V.; Seader, Shawn; Smith, Jeffrey C.; Tenenbaum, Peter; Twicken, Joseph D.; Zamudio, Khadeejah A.] NASA, Ames Res Ctr, M-S 244-30, Moffett Field, CA 94035 USA. [Latham, David W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Ofir, Aviv] Weizmann Inst Sci, Dept Earth & Planetary Sci, 234 Herzl St, IL-76100 Rehovot, Israel. [Wolfgang, Angie] Univ Calif Santa Cruz, Dept Astron, MS UCO LICK, 1156 High St, Santa Cruz, CA 95064 USA. [Wolfgang, Angie] Penn State Univ, 403 Davey Lab, University Pk, PA 16802 USA. [Shporer, Avi] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Akeson, Rachel; Christiansen, Jessie L.; Ramirez, Solange] CALTECH, NASA Exoplanet Sci Inst, Mail Code 100-22,770 South Wilson Ave, Pasadena, CA 91125 USA. [Barclay, Thomas] Bay Area Environm Res Inst, 625 2nd St,Suite 209, Petaluma, CA 94952 USA. [Boyajian, Tabetha S.] Yale Univ, Dept Astron, 52 Hillhouse Ave, New Haven, CT 06511 USA. [Campbell, Jennifer R.; Patil-Sabale, Anima; Zamudio, Khadeejah A.] Wyle Labs, 1960 East Grand Ave,Suite 900, El Segundo, CA 90245 USA. [Girouard, Forrest R.] Orbital Sci Corp, 2401 East El Segundo Blvd, El Segundo, CA 90245 USA. [Huber, Daniel] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Huber, Daniel] Aarhus Univ, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. RP Coughlin, JL (reprint author), SETI Inst, 189 Bernardo Ave,Suite 200, Mountain View, CA 94043 USA.; Coughlin, JL (reprint author), NASA, Ames Res Ctr, M-S 244-30, Moffett Field, CA 94035 USA. EM jeffrey.l.coughlin@nasa.gov FU Australian Research Council [DE140101364]; National Aeronautics and Space Administration [NNX14AB92G]; NASA; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX We thank the anonymous referee for a careful reading of the paper and comments which greatly helped to improve the readability of the paper. B.Q. gratefully acknowledges support by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. D.H. acknowledges support by the Australian Research Council's Discovery Projects funding scheme (project number DE140101364) and support by the National Aeronautics and Space Administration under grant NNX14AB92G issued through the Kepler Participating Scientist Program. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. The authors acknowledge the efforts of the Kepler Mission team for obtaining the calibrated pixel, light curve, and data validation reports used in this publication, which were generated by the Kepler Mission science pipeline through the efforts of the Kepler Science Operations Center and Science Office. The Kepler Mission is lead by the project office at NASA Ames Research Center. Ball Aerospace built the Kepler photometer and spacecraft which is operated by the mission operations center at LASP. These data products are archived at the NASA Exoplanet Science Institute, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research has made use of NASA's Astrophysics Data System. Some of the data presented in this paper were obtained from the Mikulksi 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 106 TC 16 Z9 16 U1 13 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2016 VL 224 IS 1 AR 12 DI 10.3847/0067-0049/224/1/12 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN4PR UT WOS:000377050200012 ER PT J AU Geller, MJ Hwang, HS Dell'Antonio, IP Zahid, HJ Kurtz, MJ Fabricant, DG AF Geller, Margaret J. Hwang, Ho Seong Dell'Antonio, Ian P. Zahid, Harus Jabran Kurtz, Michael J. Fabricant, Daniel G. TI SHELS: COMPLETE REDSHIFT SURVEYS OF TWO WIDELY SEPARATED FIELDS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology: observations; galaxies: abundances; galaxies: distances and redshifts; galaxies: evolution; large-scale structure of universe; surveys ID DIGITAL SKY SURVEY; VLT DEEP SURVEY; FIBER-FED SPECTROGRAPH; 10K-BRIGHT SPECTROSCOPIC SAMPLE; STAR-FORMATION HISTORIES; MASS ASSEMBLY HISTORY; WEAK-LENSING MAPS; STELLAR MASS; LUMINOSITY FUNCTION; GALAXY EVOLUTION AB The Smithsonian Hectospec Lensing Survey (SHELS) is a complete redshift survey covering two well-separated fields (F1 and F2) of the Deep Lens Survey (DLS). Both fields are more than 94% complete to a Galactic extinction corrected R-0 = 20.2. Here, we describe the redshift survey of the F1 field centered at R.A.(2000) = 00(h)53(m)25(8).3 and decl.(2000) = 12 degrees 33'55"; like F2, the F1 field covers similar to 4 deg(2). The redshift survey of the F1 field includes 9426 new galaxy redshifts measured with Hectospec on the MMT (published here). As a guide to future uses of the combined survey, we compare the mass metallicity relation and the distributions of D(n)4000 as a function of stellar mass and redshift for the two fields. The mass-metallicity relations differ by an insignificant 1.6 sigma. For galaxies in the stellar mass range 10(10)-10(11) M-circle dot, the increase in the star-forming fraction with redshift is remarkably similar in the two fields. The seemingly surprising 31%-38% difference in the overall galaxy counts in F1 and F2 is probably consistent with the expected cosmic variance given the subtleties of the relative systematics in the two surveys. We also review the DLS cluster detections in the two fields: poorer photometric data for F1 precluded secure detection of the single massive cluster at z = 0.35 that we find in SHELS. Taken together, the two fields include 16,055 redshifts for galaxies with R-0 <= 20.2 and 20,754 redshifts for galaxies with R <= 20.6. These dense surveys in two well-separated fields provide a basis for future investigations of galaxy properties and large-scale structure. C1 [Geller, Margaret J.; Kurtz, Michael J.; Fabricant, Daniel G.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Hwang, Ho Seong] Korea Inst Adv Study, Sch Phys, 85 Hoegiro, Seoul 130722, South Korea. [Dell'Antonio, Ian P.] Brown Univ, Dept Phys, Box 1843, Providence, RI 02912 USA. [Zahid, Harus Jabran] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Geller, MJ; Kurtz, MJ; Fabricant, DG (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.; Hwang, HS (reprint author), Korea Inst Adv Study, Sch Phys, 85 Hoegiro, Seoul 130722, South Korea.; Dell'Antonio, IP (reprint author), Brown Univ, Dept Phys, Box 1843, Providence, RI 02912 USA.; Zahid, HJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mgeller@cfa.harvard.edu; hhwang@kias.re.kr; ian@het.brown.edu; zahid@cfa.harvard.edu; mkurtz@cfa.harvard.edu; dfabricant@cfa.harvard.edu OI Geller, Margaret/0000-0002-9146-4876 FU Changbom Park of KIAS; Smithsonian Institution; KIAS FX We appreciate a thoughtful, careful review by the referee that substantially improved this paper. We thank Changbom Park of KIAS for generous support that enabled completion of this project. We thank Kairy Herrera of Brown University for examining images of faint galaxies with superimposed stars to refine the construction of Table 4. We thank Warren Brown for remeasuring two redshifts for two of the objects examined by Kairy Herrera. Scott Kenyon provided advice on numerical methods along with comments on the manuscript. Perry Berlind and Mike Calkins masterfully operated the Hectospec. Susan Tokarz and Sean Moran assisted with the data reduction. The Smithsonian Institution supported the research of Margaret Geller, Ho Seong Hwang, Michael Kurtz, Daniel Fabricant and Jabran Zahid. KIAS supported the research of Ho Seong Hwang. NR 68 TC 4 Z9 4 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 MAY PY 2016 VL 224 IS 1 AR 11 DI 10.3847/0067-0049/224/1/11 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN4PR UT WOS:000377050200011 ER PT J AU Narayan, G Rest, A Tucker, BE Foley, RJ Wood-Vasey, WM Challis, P Stubbs, C Kirshner, RP Aguilera, C Becker, AC Blondin, S Clocchiatti, A Covarrubias, R Damke, G Davis, TM Filippenko, AV Ganeshalingam, M Garg, A Garnavich, PM Hicken, M Jha, SW Krisciunas, K Leibundgut, B Li, W Matheson, T Miknaitis, G Pignata, G Prieto, JL Riess, AG Schmidt, BP Silverman, JM Smith, RC Sollerman, J Spyromilio, J Suntzeff, NB Tonry, JL Zenteno, A AF Narayan, G. Rest, A. Tucker, B. E. Foley, R. J. Wood-Vasey, W. M. Challis, P. Stubbs, C. Kirshner, R. P. Aguilera, C. Becker, A. C. Blondin, S. Clocchiatti, A. Covarrubias, R. Damke, G. Davis, T. M. Filippenko, A. V. Ganeshalingam, M. Garg, A. Garnavich, P. M. Hicken, M. Jha, S. W. Krisciunas, K. Leibundgut, B. Li, W. Matheson, T. Miknaitis, G. Pignata, G. Prieto, J. L. Riess, A. G. Schmidt, B. P. Silverman, J. M. Smith, R. C. Sollerman, J. Spyromilio, J. Suntzeff, N. B. Tonry, J. L. Zenteno, A. TI LIGHT CURVES OF 213 TYPE Ia SUPERNOVAE FROM THE ESSENCE SURVEY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology: observations; methods: data analysis; supernovae: general; surveys ID DIGITAL SKY SURVEY; PHOTOMETRIC STANDARD STARS; HIGH-REDSHIFT SUPERNOVAE; HUBBLE-SPACE-TELESCOPE; SPECTRAL-ENERGY DISTRIBUTION; DARK ENERGY; COSMOLOGICAL CONSTRAINTS; LEGACY SURVEY; DATA RELEASE; SYSTEMATIC UNCERTAINTIES AB The ESSENCE survey discovered 213 Type Ia supernovae at redshifts 0.1 < z < 0.81 between 2002 and 2008. We present their R- and I-band photometry, measured from images obtained using the MOSAIC II camera at the CTIO Blanco, along with rapid-response spectroscopy for each object. We use our spectroscopic follow-up observations to determine an accurate, quantitative classification, and precise redshift. Through an extensive calibration program we have improved the precision of the CTIO Blanco natural photometric system. We use several empirical metrics to measure our internal photometric consistency and our absolute calibration of the survey. We assess the effect of various potential sources of systematic bias on our measured fluxes, and estimate the dominant term in the systematic error budget from the photometric calibration on our absolute fluxes is similar to 1%. C1 [Narayan, G.; Matheson, T.] Natl Opt Astron Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA. [Narayan, G.; Challis, P.; Stubbs, C.; Kirshner, R. P.; Garg, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Narayan, G.; Stubbs, C.; Hicken, M.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. [Rest, A.; Riess, A. G.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Tucker, B. E.; Schmidt, B. P.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Via Cotter Rd, Weston, ACT 2611, Australia. [Foley, R. J.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Wood-Vasey, W. M.; Smith, R. C.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Aguilera, C.; Zenteno, A.] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, Casilla 603, La Serena, Chile. [Becker, A. C.; Covarrubias, R.] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. [Blondin, S.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Inst Astrofis, Casilla 306, Santiago 22, Chile. [Damke, G.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Davis, T. M.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia. [Filippenko, A. V.; Ganeshalingam, M.; Li, W.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Garnavich, P. M.] Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. [Jha, S. W.] Rutgers State Univ, Dept Phys & Astron, POB 849, Piscataway, NJ 08854 USA. [Krisciunas, K.; Suntzeff, N. B.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Leibundgut, B.; Spyromilio, J.] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Miknaitis, G.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Pignata, G.] Univ Andres Bello, Dept Ciencias Fis, Avda Republ 252, Santiago, Santiago Rm, Chile. [Prieto, J. L.] Univ Diego Port, Fac Engn, Astron Nucleus, Ejercito 441, Santiago, Santiago Rm, Chile. [Riess, A. G.] Johns Hopkins Univ, 3400 North Charles St, Baltimore, MD 21218 USA. [Silverman, J. M.] Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. [Sollerman, J.] Stockholm Univ, Alballova, Dept Astron, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Tonry, J. L.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Clocchiatti, A.] Millennium Inst Astrophys, Santiago, Chile. RP Narayan, G (reprint author), Natl Opt Astron Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA.; Narayan, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Narayan, G (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM gnarayan@noao.edu RI Davis, Tamara/A-4280-2008; OI Davis, Tamara/0000-0002-4213-8783; Tucker, Brad/0000-0002-4283-5159; Sollerman, Jesper/0000-0003-1546-6615; Narayan, Gautham/0000-0001-6022-0484; Schmidt, Brian/0000-0001-6589-1287 FU NSF [AST-0507475, AST-0908886, AST-1211916]; Department of Energy; European Southern Observatory, Chile (ESO Programme) [170.A-0519, 176.A-0319]; CONICET (Argentina) [GN-2002B-Q-14, GS-2003B-Q-11, GN-2003B-Q-14, GS-2004B-Q-4, GN-2004B-Q-6, GS-2005B-Q-31, GN-2005B-Q-35]; W. M. Keck Foundation; Danish National Research Foundation; U.S. National Science Foundation [AST-0507475, AST-0443378]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; Ministry of Economy, Development and Tourism [IC120009]; grant Basal CATA PFB 06/09 from CONICYT FX G.N. is supported by NSF award AST-0507475 and the Department of Energy. Based in part on observations obtained at the Cerro Tololo Inter-American Observatory (CTIO), part of the National Optical Astronomy Observatory (NOAO), which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation (NSF); the European Southern Observatory, Chile (ESO Programmes 170.A-0519 and 176.A-0319); 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 NSF (United States), the Particle Physics and Astronomy Research Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil) and CONICET (Argentina) (Programs GN-2002B-Q-14, GS-2003B-Q-11, GN-2003B-Q-14, GS-2004B-Q-4, GN-2004B-Q-6, GS-2005B-Q-31, GN-2005B-Q-35); the Magellan Telescopes at Las Campanas Observatory; the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona; and the F.L. Whipple Observatory, which is operated by the Smithsonian Astrophysical Observatory. 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.; A.V.F.'s group at UC Berkeley received additional assistance from NSF grants AST-0908886 and AST-1211916, the TABASGO foundation, and the Christopher R. Redlich fund. The Dark Cosmology Centre is funded by the Danish National Research Foundation. The ESSENCE survey team is very grateful to the scientific and technical staff at the observatories we have been privileged to use.; The survey is supported by the U.S. National Science Foundation through grants AST-0443378 and AST-0507475. The Dark Cosmology Centre is funded by the Danish National Research Foundation.; J.M.S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. A.C. acknowledges support from grant IC120009 awarded to the Millennium Institute of Astrophysics, MAS, by the Ministry of Economy, Development and Tourism, and grant Basal CATA PFB 06/09 from CONICYT. NR 110 TC 0 Z9 0 U1 6 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2016 VL 224 IS 1 AR 3 DI 10.3847/0067-0049/224/1/3 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN4PR UT WOS:000377050200003 ER PT J AU Brown, ME Converse, SJ Chandler, JN Shafer, C Brown, JL Keefer, CL Songsasen, N AF Brown, Megan E. Converse, Sarah J. Chandler, Jane N. Shafer, Charles Brown, Janine L. Keefer, Carol L. Songsasen, Nucharin TI Female gonadal hormones and reproductive behaviors as key determinants of successful reproductive output of breeding whooping cranes (Grus americana) SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Whooping crane; Reproduction; Endocrinology; Glucocorticoids; Behavior; Egg laying ID LUTEINIZING-HORMONE; REINTRODUCED POPULATION; GALLUS-DOMESTICUS; MODEL SELECTION; OVULATORY CYCLE; TURKEY HENS; PROGESTERONE; CORTICOSTERONE; STRESS; TESTOSTERONE AB Reproductive success of endangered whooping cranes (Grus americana) maintained ex situ is poor. As part of an effort to identify potential causes of poor reproductive success in a captive colony, we used non-invasive endocrine monitoring to assess gonadal and adrenal steroids of bird pairs with various reproductive outcomes and evaluated the relationships of hormones and behaviors to reproductive performance. Overall, reproductively successful (i.e., egg laying) females had significantly higher mean estrogen levels but lower mean progestogen concentrations than did unsuccessful females. Other hormones, including glucocorticoids and androgens, were not significantly different between successful and unsuccessful individuals. Observations of specific behaviors such as unison calling, marching, and the number of copulation attempts, along with overall time spent performing reproductive behaviors, were significantly higher in successful pairs. Our findings indicate that overall reproductive performance of whooping crane pairs is linked to female gonadal hormone excretion and reproductive behaviors, but not to altered adrenal hormone production. Published by Elsevier Inc. C1 [Brown, Megan E.; Keefer, Carol L.] Univ Maryland, Dept Anim & Avian Sci, 8127 Regents Dr, College Pk, MD 20742 USA. [Brown, Megan E.; Brown, Janine L.; Songsasen, Nucharin] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA. [Converse, Sarah J.; Chandler, Jane N.; Shafer, Charles] US Geol Survey, Patuxent Wildlife Res Ctr, 12100 Beech Forest Rd, Laurel, MD 20708 USA. RP Songsasen, N (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA. EM songsasenn@si.edu OI Shafer, Charles/0000-0002-1864-2461; Converse, Sarah J/0000-0002-3719-5441 FU Morris Animal Foundation - United States; Cosmos Club FX The authors thank: the Morris Animal Foundation - United States and the Cosmos Club for financial support; the crane crew (B. Clauss, B.A. Clauss, R. Doyle, S. Pegory, A. Lopez, and P. Coontz), and veterinary staff (G. Olsen and C. Caldwell) at the PWRC for its dedication and for providing special assistance to conduct this study; the endocrine lab staff at Smithsonian Conservation Biology Institute (N. Boisseau, N. Parker, N. Prado-Oviedo, S. Putnam, and S. Paris) for technical assistance in endocrine analysis; A. Willis at MP Biomedicals for his assistance during purchase and validation of the two RIA kits; F. Kromm for support and assistance in editing. NR 56 TC 0 Z9 0 U1 6 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0016-6480 EI 1095-6840 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD MAY 1 PY 2016 VL 230 BP 158 EP 165 DI 10.1016/j.ygcen.2016.04.009 PG 8 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA DN4QB UT WOS:000377051200015 PM 27080552 ER PT J AU Lesoway, MP Abouheif, E Collin, R AF Pauline Lesoway, Maryna Abouheif, Ehab Collin, Rachel TI Comparative Transcriptomics of Alternative Developmental Phenotypes in a Marine Gastropod SO JOURNAL OF EXPERIMENTAL ZOOLOGY PART B-MOLECULAR AND DEVELOPMENTAL EVOLUTION LA English DT Article ID NUTRITIVE EGG FORMATION; RNA-SEQ DATA; CALYPTRAEID GASTROPODS; CREPIDULA-DILATATA; LARVAL DEVELOPMENT; MERETRIX-MERETRIX; REFERENCE GENOME; SHELL FORMATION; NORTHERN CHILE; SPADEFOOT TOAD AB Alternative phenotypes are discrete phenotypic differences that develop in response to both genetic and environmental cues. Nutritive embryos, which arrest their development to serve as nutrition for their viable siblings, are an example of an alternative developmental phenotype found in many animal groups. Females of the marine snail, Crepidula navicella, produce broods that consist mainly of nutritive embryos and a small number of viable embryos. In order to better understand the genetic mechanisms that lead to the development of alternative phenotypes in this species, we compared the transcriptomes of viable and nutritive embryos at the earliest stage that we were able to distinguish visually between the two. Using high-throughput Illumina sequencing, we assembled and annotated a de novo transcriptome and compared transcript levels in viable and nutritive embryos. Viable embryos express high levels of transcripts associated with known developmental events, while nutritive embryos express high levels of apoptosis-related transcripts. Gene Ontology term enrichment with GOSeq found that these are associated with the negative regulation of apoptotic processes. This enrichment, combined with morphological evidence, suggests that apoptosis is important in the formation of gastrula-like nutritive embryos. Apoptosis has been implicated in the development of alternative phenotypes in other animal groups, raising the possibility that this mechanism's role in alternative phenotypes is conserved in gastropod development. We suggest possible alternative mechanisms of nutritive embryo development. Most importantly, we contribute further evidence to the hypothesis that nutritive embryos are an alternative developmental phenotype. (C) 2016 Wiley Periodicals, Inc. C1 [Pauline Lesoway, Maryna; Abouheif, Ehab] McGill Univ, Dept Biol, 1205 Ave Docteur Penfield, Montreal, PQ H3A 1B1, Canada. [Pauline Lesoway, Maryna; Collin, Rachel] Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. RP Abouheif, E (reprint author), McGill Univ, Dept Biol, 1205 Ave Docteur Penfield, Montreal, PQ H3A 1B1, Canada.; Collin, R (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM ehab.abouheif@mcgill.ca; collinr@si.edu FU STRI, NSF [IOS-1019727]; Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery; FRQNT FX Grant sponsor: STRI, NSF; Grant number: IOS-1019727; Grant sponsor: Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery; Grant sponsor: FRQNT. NR 79 TC 1 Z9 1 U1 2 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1552-5007 EI 1552-5015 J9 J EXP ZOOL PART B JI J. Exp. Zool. Part B PD MAY PY 2016 VL 326 IS 3 BP 151 EP 167 DI 10.1002/jez.b.22674 PG 17 WC Evolutionary Biology; Developmental Biology; Zoology SC Evolutionary Biology; Developmental Biology; Zoology GA DN6WW UT WOS:000377218200001 PM 27194576 ER PT J AU Escobedo-Morales, LA Mandujano, S Eguiarte, LE Rodriguez-Rodriguez, MA Maldonado, JE AF Escobedo-Morales, Luis A. Mandujano, Salvador Eguiarte, Luis E. Rodriguez-Rodriguez, Marco A. Maldonado, Jesus E. TI First phylogenetic analysis of Mesoamerican brocket deer Mazama pandora and Mazama temama (Cetartiodactyla: Cervidae) based on mitochondrial sequences: Implications for Neotropical deer evolution SO MAMMALIAN BIOLOGY LA English DT Article DE Mazama pandora; Mazama temama; Mesoamerica; mtDNA; Neotropical deer evolution ID AMERICAN BIOTIC INTERCHANGE; CONTROL REGION; CYTOCHROME-B; RED BROCKET; BROWN BROCKET; ARTIODACTYLA; DNA; MAMMALIA; HISTORY; DIVERSIFICATION AB Several recent studies have tried to unravel the complex evolutionary history of Neotropical cervids. However, the two Mesoamerican brocket deer Mazama pandora and M. temama have not been included in these studies and their relationship to other Neotropical cervids remains unclear. Here, we present analyses that included concatenated sequences from the mitochondrial genes ND2, Cytb, and tRNA-Pro-Control region. Our results suggest that both Mesoamerican brocket deer fall within the "red" Glade, more closely related to genus Odocoileus and red brocket deer species, such as South American Mazama americana, M. bororo, M. nana, and M. rufina. We estimated that M. temama diverged from other red brocket deer ca. two MYA. Two hypothesis emerge regarding the relationship of the Yucatan brocket deer M. pandora with respect to the other Neotropical deer. The first one, based on analyses of concatenated sequences from all three genes, implies an early split from a larger Glade that includes Odocoileus and other red Mazama species, with an estimated divergence time dating back to 2.7 MYA. This would suggest isolation on the Yucatan peninsula, limiting the crossing of this species into South America. The second one, based only on Cytb, places M. pandora more closely related to Odocoileus and with an estimated divergence time of ca. 1.9 MYA. This would suggest that the humid tropical forests of Mexico and Central America could have been the most likely place of origin of members of the red brocket deer Glade. Deer colonization into South America occurred after the complete formation of the Panamanian land bridge in the late Pliocene, more than one ancestor of the gray brocket deer Glade crossed into South America, as well as a red brocket deer ancestor and Odocoileus dispersed southward. A posterior event probably occurred when divergent ancestors of M. temama and M. pandora respectively moved northward after the split with South American red brocket deer. Our results add to the growing body of evidence calling for an extensive taxonomic revision of this group, and we concur with previous recommendations that the generic taxonomic designation of Mamma should be applied not only to the red brocket deer but also to all of the species currently recognized under the genus Odocoileus. (C) 2016 Deutsche Gesellschaft fur Saugetierkunde. Published by Elsevier GmbH. All rights reserved. C1 [Escobedo-Morales, Luis A.] Inst Ecol AC, Div Posgrad, Carretera Antigua Coatepec 351, Xalapa 91070, Veracruz, Mexico. [Mandujano, Salvador] Inst Ecol AC, Red Biol & Conservat Vertebrados, Carretera Antigua Coatepec 351, Xalapa 91070, Veracruz, Mexico. [Eguiarte, Luis E.; Rodriguez-Rodriguez, Marco A.] Univ Nacl Autonoma Mexico, Dept Ecol Evolut, Inst Ecol, Apartado Postal 70-275, Mexico City 04510, DF, Mexico. [Maldonado, Jesus E.] Smithsonian Inst, Natl Zool Pk, 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 20008 USA. RP Escobedo-Morales, LA (reprint author), Inst Ecol AC, Div Posgrad, Carretera Antigua Coatepec 351, Xalapa 91070, Veracruz, Mexico. EM laembiol@gmail.com FU Consejo Nacional de Ciencia y Tecnologia (CONACYT); INECOL, Vertebrate Biology and Conservation Department FX We thank F. Cervantes (CNMA), E. Escobedo-Cabrera (ECOCHM), A. Gonzalez-Christen (IIBUV), C. Lorenzo (ECOSCM), L. Leon-Paniagua (MZFC), O. Retana (CMMBMUAC), A. Riechers (CZRMA), N. B. Simmons (AMNH) and R. Timm (KU) for allowing the access to the mammal collections under their charge. R. Pacheco provided hair samples from captive animals from ANIMAYA. Consejo Nacional de Ciencia y Tecnologia (CONACYT) provided a scholarship for LAEM's doctorate degree and Institute de Ecologia, A. C. (INECOL, Vertebrate Biology and Conservation Department) provided logistic and financial support. We also thank R. Fleischer, N. Rotzel and C. Hofman for their support for the laboratory work at the SCBI/Center for Conservation and Evolutionary Genetics. A. Espinosa and A. Guillen (INECOL) provided important suggestions to a previous version of the manuscript. Collecting permits were facilitated to LAEM by Secretaria del Medio Ambiente y Recursos Naturales (SEMARNAT 00503/10 and 06238/11). Thanks to M. Ruiz-Garcia (PUJ) and an anonymous reviewer for their observations that helped to improve this manuscript. NR 67 TC 2 Z9 2 U1 9 U2 10 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 1616-5047 EI 1618-1476 J9 MAMM BIOL JI Mamm. Biol. PD MAY PY 2016 VL 81 IS 3 BP 303 EP 313 DI 10.1016/j.mambio.2016.02.003 PG 11 WC Zoology SC Zoology GA DN1CV UT WOS:000376804800010 ER PT J AU Funk, WC Lovich, RE Hohenlohe, PA Hofman, CA Morrison, SA Sillett, TS Ghalambor, CK Maldonado, JE Rick, TC Day, MD Polato, NR Fitzpatrick, SW Coonan, TJ Crooks, KR Dillon, A Garcelon, DK King, JL Boser, CL Gould, N Andelt, WF AF Funk, W. Chris Lovich, Robert E. Hohenlohe, Paul A. Hofman, Courtney A. Morrison, Scott A. Sillett, T. Scott Ghalambor, Cameron K. Maldonado, Jesus E. Rick, Torben C. Day, Mitch D. Polato, Nicholas R. Fitzpatrick, Sarah W. Coonan, Timothy J. Crooks, Kevin R. Dillon, Adam Garcelon, David K. King, Julie L. Boser, Christina L. Gould, Nicholas Andelt, William F. TI Adaptive divergence despite strong genetic drift: genomic analysis of the evolutionary mechanisms causing genetic differentiation in the island fox (Urocyon littoralis) SO MOLECULAR ECOLOGY LA English DT Article DE conservation genomics; divergent selection; effective population size; genetic drift; population divergence ID EFFECTIVE POPULATION-SIZE; ALLELE FREQUENCY DATA; NATURAL-POPULATIONS; PHYLOGENETIC NETWORKS; DEMOGRAPHIC HISTORY; CALIFORNIA REGION; COMPUTER-PROGRAM; FLORIDA PANTHER; CUTTHROAT TROUT; CONSERVATION AB The evolutionary mechanisms generating the tremendous biodiversity of islands have long fascinated evolutionary biologists. Genetic drift and divergent selection are predicted to be strong on islands and both could drive population divergence and speciation. Alternatively, strong genetic drift may preclude adaptation. We conducted a genomic analysis to test the roles of genetic drift and divergent selection in causing genetic differentiation among populations of the island fox (Urocyon littoralis). This species consists of six subspecies, each of which occupies a different California Channel Island. Analysis of 5293 SNP loci generated using Restriction-site Associated DNA (RAD) sequencing found support for genetic drift as the dominant evolutionary mechanism driving population divergence among island fox populations. In particular, populations had exceptionally low genetic variation, small N-e (range = 2.1-89.7; median = 19.4), and significant genetic signatures of bottlenecks. Moreover, islands with the lowest genetic variation (and, by inference, the strongest historical genetic drift) were most genetically differentiated from mainland grey foxes, and vice versa, indicating genetic drift drives genome-wide divergence. Nonetheless, outlier tests identified 3.6-6.6% of loci as high F-ST outliers, suggesting that despite strong genetic drift, divergent selection contributes to population divergence. Patterns of similarity among populations based on high FST outliers mirrored patterns based on morphology, providing additional evidence that outliers reflect adaptive divergence. Extremely low genetic variation and small Ne in some island fox populations, particularly on San Nicolas Island, suggest that they may be vulnerable to fixation of deleterious alleles, decreased fitness and reduced adaptive potential. C1 [Funk, W. Chris; Ghalambor, Cameron K.] Colorado State Univ, Dept Biol, Grad Degree Program Ecol, 1878 Campus Delivery, Ft Collins, CO 80523 USA. [Lovich, Robert E.] Naval Facil Engn Command Southwest, 1220 Pacific Highway, San Diego, CA 92132 USA. [Hohenlohe, Paul A.; Day, Mitch D.] Univ Idaho, Inst Bioinformat & Evolutionary Studies, Dept Biol Sci, Moscow, ID 83844 USA. [Hofman, Courtney A.] Univ Maryland, Dept Anthropol, College Pk, MD 20742 USA. [Hofman, Courtney A.; Rick, Torben C.] Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Dept Anthropol, Smithsonian Inst, Washington, DC 20013 USA. [Hofman, Courtney A.; Maldonado, Jesus E.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Morrison, Scott A.; Boser, Christina L.] Nature Conservancy, San Francisco, CA 94105 USA. [Sillett, T. Scott] Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, MRC 5503, Washington, DC 20013 USA. [Maldonado, Jesus E.] Natl Museum Nat Hist, Dept Vertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA. [Polato, Nicholas R.] Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14850 USA. [Fitzpatrick, Sarah W.] Michigan State Univ, Kellogg Biol Stn, Dept Integrat Biol, Hickory Corners, MI 49060 USA. [Coonan, Timothy J.] Natl Pk Serv, Channel Islands Natl Pk,1901 Spinnaker Dr, Ventura, CA 93001 USA. [Crooks, Kevin R.; Dillon, Adam; Andelt, William F.] Colorado State Univ, Dept Fish Wildlife & Conservat Biol, 1474 Campus Delivery, Ft Collins, CO 80523 USA. [Garcelon, David K.] Inst Wildlife Studies, POB 1104, Arcata, CA 95518 USA. [King, Julie L.] Catalina Isl Conservancy, POB 2739, Avalon, CA 90704 USA. [Gould, Nicholas] N Carolina State Univ, Fisheries Wildlife & Conservat Biol, Turner House,Box 7646, Raleigh, NC 27695 USA. RP Funk, WC (reprint author), Colorado State Univ, Dept Biol, Grad Degree Program Ecol, 1878 Campus Delivery, Ft Collins, CO 80523 USA. EM Chris.Funk@colostate.edu OI Hofman, Courtney/0000-0002-6808-3370 FU U.S. Department of Defense Legacy Resource Management Program; Nature Conservancy; U.S. National Institutes of Health [P30GM103324] FX We thank Lisa Lyren, Erin Boydston, Francesca Ferrara, and many field assistants who helped collect blood and tissue samples, Tamara Max for helping prepare RAD libraries, and Brian Cypher for providing island fox diet data. We also thank Lisette Waits, Andrew R. Whiteley and three anonymous reviewers for providing helpful suggestions on the manuscript. This research was funded by the U.S. Department of Defense Legacy Resource Management Program, The Nature Conservancy, and the U.S. National Institutes of Health (grant number P30GM103324). This project was approved by the Institutional Animal Care and Use Committee at Colorado State University. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government. NR 108 TC 6 Z9 6 U1 31 U2 63 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 MAY PY 2016 VL 25 IS 10 BP 2176 EP 2194 DI 10.1111/mec.13605 PG 19 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA DN4HF UT WOS:000377024200007 PM 26992010 ER PT J AU Strong, MT AF Strong, Mark T. TI Three New Cyperaceae from the Cuyuni-Mazaruni Region of Guyana (South America) SO NOVON LA English DT Article DE Cephalocarpus; Cyperaceae; Everardia; Guyana; IUCN Red List; Scleria; South America AB Three new species of Cyperaceae are described and illustrated from the Cuyuni-Mazaruni Region of Guyana, South America: Cephalocarpus glabra M. T. Strong, Everardia spongiosa M. T. Strong, and Scleria attenuatifolia M. T. Strong. Comparisons to similar taxa are discussed for each. C1 [Strong, Mark T.] Smithsonian Inst, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. RP Strong, MT (reprint author), Smithsonian Inst, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. EM strongm@si.edu NR 5 TC 0 Z9 0 U1 1 U2 1 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD MAY PY 2016 VL 24 IS 4 BP 401 EP 407 DI 10.3417/2015032 PG 7 WC Plant Sciences SC Plant Sciences GA DN4SL UT WOS:000377057400014 ER PT J AU Hosaka, N Kachi, N Kudoh, H Stuefer, JF Whigham, DF AF Hosaka, Naomi Kachi, Naoki Kudoh, Hiroshi Stuefer, Josef F. Whigham, Dennis F. TI Compensatory growth of the clonal understory tree, Asimina triloba, in response to small-scale disturbances SO PLANT ECOLOGY LA English DT Article DE Clipping; Clonal woody plants; Root sucker; Ramet dynamics; Sprouting ID RAIN-FOREST; PHYSIOLOGICAL INTEGRATION; SEEDLING ESTABLISHMENT; PHYSICAL DISTURBANCE; PLANT-COMMUNITIES; DECIDUOUS FOREST; SHRUB; DEFOLIATION; CANOPY; CARBOHYDRATE AB In hardwood forests, clonal understory trees often develop patches of ramets that are interconnected via root systems. The patches are often partially disturbed by litter falling from the forest canopy, and patterns of damage can vary in size and the number of directly affected ramets. To test the effects of different types of disturbance on recovery and development of patches, we conducted a field experiment using the clonal understory tree, Asimina triloba in a hardwood forest of the northeastern USA. Either single large ramets or many small ramets were cut at their base, which removed about half of the aboveground biomass from each patch. Both types of disturbance did not change new ramet production, and the recovery response of A. triloba was primarily achieved by sprouting of damaged ramets. Three years after the manipulation, total aboveground biomass of disturbed patches recovered to pre-treatment levels without cost in terms of reduced growth or survival of undamaged ramets. These results suggest that A. triloba has the ability to persist under different types of disturbance and regrowth of damaged ramets is probably supported by the translocation of resources stored in root systems. On the other hand, damaged ramets grew less for the first year after the disturbance. New ramets also grew less in disturbed patches than in controls, especially where large ramets were damaged. In A. triloba, damage to large ramets may compromise sexual reproduction, which is limited to large ramets, and have negative impacts on new patch establishment via sexual reproduction. C1 [Hosaka, Naomi; Kachi, Naoki] Tokyo Metropolitan Univ, Dept Biol Sci, Hachioji, Tokyo 1920397, Japan. [Kudoh, Hiroshi] Kyoto Univ, Ctr Ecol Res, Hirano 2-509-3, Otsu, Shiga 5202113, Japan. [Stuefer, Josef F.] Netherlands Org Sci Res, Laan van Nieuw Oost Indie 300, NL-2593 CE The Hague, Netherlands. [Whigham, Dennis F.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. [Hosaka, Naomi] Res Inst Japan Assoc Adv Phytoregulators, Kashiwada Cho 860, Ibaraki 3051211, Japan. RP Hosaka, N (reprint author), Res Inst Japan Assoc Adv Phytoregulators, Kashiwada Cho 860, Ibaraki 3051211, Japan. EM naomi.hosaka@gmail.com OI Whigham, Dennis/0000-0003-1488-820X FU Smithsonian Environmental Research Center FX This research was supported by a Graduate Fellowship and a Pre-doctoral Fellowship to Naomi Hosaka from the Smithsonian Environmental Research Center. We thank Jun-ichirou Suzuki for constructive comments on earlier versions of the manuscript, and Jay O'Neill, Sara Gomez, Laura Dietrich, Dawn Miller, and Reginald Reid for invaluable field assistance. NR 45 TC 0 Z9 0 U1 10 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 MAY PY 2016 VL 217 IS 5 BP 471 EP 480 DI 10.1007/s11258-016-0592-y PG 10 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA DN2LC UT WOS:000376894100001 ER PT J AU Bousquet, MS Ma, JJ Ratnayake, R Havre, PA Yao, J Dang, NH Paul, VJ Carney, TJ Dang, LH Luesch, H AF Bousquet, Michelle S. Ma, Jia Jia Ratnayake, Ranjala Havre, Pamela A. Yao, Jin Dang, Nam H. Paul, Valerie J. Carney, Thomas J. Dang, Long H. Luesch, Hendrik TI Multidimensional Screening Platform for Simultaneously Targeting Oncogenic KRAS and Hypoxia-Inducible Factors Pathways in Colorectal Cancer SO ACS CHEMICAL BIOLOGY LA English DT Article ID NF-KAPPA-B; PROTEIN STABILITY; DRUG DISCOVERY; CELLS REVEALS; TUMOR-GROWTH; K-RAS; HIF-1-ALPHA; ACTIVATION; THERAPY; EXPRESSION AB Colorectal cancer (CRC) is a genetic disease, due to progressive accumulation of mutations in oncogenes and tumor suppressor genes. Large scale genomic sequencing projects revealed >100 mutations in any individual CRC. Many of these mutations are likely passenger mutations, and fewer are driver mutations. Of these, activating mutations in RAS proteins are essential for cancer initiation, progression, and/or resistance to therapy. There has been significant interest in developing drugs targeting mutated cancer gene products or downstream signaling pathways. Due to the number of mutations involved and inherent redundancy in intracellular signaling, drugs targeting one mutation or pathway have been either ineffective or led to rapid resistance. We have devised a strategy whereby multiple cancer pathways may be simultaneously targeted for drug discovery. For proof-of-concept, we targeted the oncogenic KRAS and HIF pathways, since oncogenic KRAS has been shown to be required for cancer initiation and progression, and HIF-1 alpha and HIF-2 alpha are induced by the majority of mutated oncogenes and tumor suppressor genes in CRC. We have generated isogenic cell lines defective in either oncogenic KRAS or both HIF-1 alpha and HIF-2 alpha and subjected them to multiplex genomic, siRNA, and high throughput small molecule screening. We have identified potential drug targets and compounds for preclinical and clinical development. Screening of our marine natural product library led to the rediscovery of the microtubule agent dolastatin 10 and the class I histone deacetylase (HDAC) inhibitor largazole to inhibit oncogenic KRAS and HIF pathways. Largazole was further validated as an antiangiogenic agent in a HIP-dependent manner in human cells and in vivo in zebrafish using a genetic model with activated HIF. Our general strategy, coupling functional genomics with drug susceptibility or chemical-genetic interaction screens, enables the identification of potential drug targets and candidates with requisite selectivity. Molecules prioritized in this manner can easily be validated in suitable zebrafish models due to the genetic tractability of the system. Our multidimensional platform with cellular and organismal components can be extended to larger scale multiplex screens that include other mutations and pathways. C1 [Bousquet, Michelle S.; Ratnayake, Ranjala; Havre, Pamela A.; Dang, Long H.; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Bousquet, Michelle S.; Ratnayake, Ranjala; Havre, Pamela A.; Dang, Long H.; Luesch, Hendrik] Univ Florida, Ctr Nat Prod Drug Discovery & Dev, Gainesville, FL 32610 USA. [Yao, Jin] Univ Florida, Dept Elect & Comp Engn, Gainesville, FL 32610 USA. [Dang, Nam H.; Dang, Long H.] Univ Florida, Dept Med, Gainesville, FL 32610 USA. [Ma, Jia Jia; Carney, Thomas J.; Luesch, Hendrik] ASTAR, Inst Mol & Cell Biol, Singapore 138673, Singapore. [Paul, Valerie J.] Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. [Carney, Thomas J.] Nanyang Technol Univ, Lee Kong Chian Sch Med, S9 Nanyang Dr, Singapore 636921, Singapore. RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA.; Luesch, H (reprint author), Univ Florida, Ctr Nat Prod Drug Discovery & Dev, Gainesville, FL 32610 USA. EM luesch@cop.ufl.edu FU National Institutes of Health [R01CA172310]; Agency for Science, Technology and Research (A*STAR) Singapore; SERI-IMCB Program on Retinal Angiogenic Disease (SIPRAD) FX This research was supported by the National Institutes of Health grant R01CA172310. We are grateful to the Agency for Science, Technology and Research (A*STAR) Singapore for funding through the Research Attachment Programme (M.S.B.) and to the University of Florida (UF) College of Pharmacy and UF Health (D. Guzick) for supporting the sabbatical visit at the IMCB (H.L.). J.J.M. was partly funded by the SERI-IMCB Program on Retinal Angiogenic Disease (SIPRAD). We thank Y. Liu for technical assistance with many experiments. NR 50 TC 2 Z9 2 U1 1 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1554-8929 EI 1554-8937 J9 ACS CHEM BIOL JI ACS Chem. Biol. PD MAY PY 2016 VL 11 IS 5 BP 1322 EP 1331 DI 10.1021/acschembio.5b00860 PG 10 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA DM6OZ UT WOS:000376473600020 PM 26938486 ER PT J AU Katinas, L Hernandez, MP Arambarri, AM Funk, VA AF Katinas, Liliana Hernandez, Marcelo P. Arambarri, Ana M. Funk, Vicki A. TI The origin of the bifurcating style in Asteraceae (Compositae) SO ANNALS OF BOTANY LA English DT Article DE Asteraceae; Calyceraceae; Goodeniaceae; homology; morphology; histochemistry; style evolution; venation ID SECONDARY POLLEN PRESENTATION; NYMPHOIDES MENYANTHACEAE; CENTRAL CHILE; EVOLUTION; ASTERALES; CALYCERACEAE; PHYLOGENY; BIOGEOGRAPHY; MECHANISMS; MORPHOLOGY AB Methods The histochemistry, venation and general morphology of the styles of members of Goodeniaceae, Calyceraceae and early branching lineages of Asteraceae were analysed and put in a phylogenetic framework to discuss the relevance of style features in the evolution of these families. Key Results The location of lipophilic substances allowed differentiation of receptive from non-receptive style papillae, and the style venation in Goodeniaceae and Calyceraceae proved to be distinctive. There were several stages of style evolution from Goodeniaceae to Asteraceae involving connation and elongation of veins, development of bilobation from an initially cup-shaped style, and a redistribution of the receptive and non-receptive papillae. Conclusions These developments resulted in bifurcation in the styles of Asteraceae, with each branch face having a different function, and it is suggested here as a mechanism that promoted outcrossing, which in turn led to the great diversification in the family. C1 [Katinas, Liliana] Museo La Plata, Div Plantas Vasc, La Plata, Buenos Aires, Argentina. [Katinas, Liliana; Hernandez, Marcelo P.; Arambarri, Ana M.] Univ Nacl La Plata, Fac Ciencias Agr & Forestales, Lab Morfol Comparada Espermatofitas LAMCE, RA-1900 La Plata, Buenos Aires, Argentina. [Funk, Vicki A.] Smithsonian Inst, Dept Bot, NMNH, Washington, DC 20560 USA. RP Katinas, L (reprint author), Museo La Plata, Div Plantas Vasc, La Plata, Buenos Aires, Argentina.; Katinas, L (reprint author), Univ Nacl La Plata, Fac Ciencias Agr & Forestales, Lab Morfol Comparada Espermatofitas LAMCE, RA-1900 La Plata, Buenos Aires, Argentina. EM katinas@fcnym.unlp.edu.ar FU Agencia Nacional de Promocion Cientifica y Tecnologica (SECYT); Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET); Universidad Nacional de La Plata (UNLP) FX We acknowledge Jorge Crisci, Raul Pozner and Gisela Sancho for critically reading the manuscript and for providing suggestions on how to improve it. Also, we appreciate the Chief and Handling Editors and the reviewer comments. Mauricio Bonifacino provided the photograph in Fig. 8 and Hugo Calvetti the drawing in Fig. 2. We are also grateful to curators of herbaria BA, LP and US, which provided material for examination. This work was supported by Agencia Nacional de Promocion Cientifica y Tecnologica (SECYT), Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET) and Universidad Nacional de La Plata (UNLP). NR 61 TC 2 Z9 2 U1 1 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-7364 EI 1095-8290 J9 ANN BOT-LONDON JI Ann. Bot. PD MAY PY 2016 VL 117 IS 6 BP 1009 EP 1021 DI 10.1093/aob/mcw033 PG 13 WC Plant Sciences SC Plant Sciences GA DM9AJ UT WOS:000376655400006 PM 27098086 ER PT J AU Beck, PG Prieto, CA Van Reeth, T Tkachenko, A Raskin, G van Winckel, H do Nascimento, JD Salabert, D Corsaro, E Garcia, RA AF Beck, P. G. Allende Prieto, C. Van Reeth, T. Tkachenko, A. Raskin, G. van Winckel, H. do Nascimento, J. -D., Jr. Salabert, D. Corsaro, E. Garcia, R. A. TI The HERMES solar atlas and the spectroscopic analysis of the seismic solar analogue KIC 3241581 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: solar-type; stars: fundamental parameters; methods: observational; techniques: spectroscopic ID CLUSTERS NGC 6791; RED GIANT STARS; LITHIUM DEPLETION; KEPLER-MISSION; STELLAR AGE; ASTEROSEISMOLOGY; TWINS; MASS; ABUNDANCES; PHOTOMETRY AB Context. Solar-analogue stars provide an excellent resource to study the Sun's evolution, i.e. the changes with time in stellar structure, activity, or rotation for solar-like stars. The unparalleled photometric data from the NASA space telescope Kepler allows us to study and characterise solar-like stars through asteroseismology. Aims. We aim to spectroscopically investigate the fundamental parameter and chromospheric activity of solar analogues and twins, based on observations obtained with the HERMES spectrograph and combine them with asteroseismology. Therefore, we need to build a solar atlas for the spectrograph, to provide accurate calibrations of the spectroscopically determined abundances of solar-and late-type stars observed with this instrument and thus perform differential spectroscopic comparisons. Methods. We acquire high-resolution and high signal-to-noise (S/N) spectroscopy to construct three solar reference spectra by observing the reflected light of the asteroids Vesta and Victoria and the jovian moon Europa (100 less than or similar to S/N less than or similar to 450) with the HERMES spectrograph. We then observe the Kepler solar analogue KIC3241581 (S/N similar to 170). For this star, the fundamental spectral parameters are extracted using a differential analysis. Sufficient S/N in the near ultraviolet allows us to investigate the chromospheric magnetic activity in both objects. Results. We constructed three solar spectrum atlases from 385 to 900 nm, obtained with the HERMES spectrograph from observations of two bright asteroids and a jovian moon. A comparison between our solar spectra atlas to the Kurucz and HARPS solar spectrum shows an excellent agreement. KIC3241581 was found to be a long-periodic binary system. The fundamental parameter for the stellar primary component are T-eff = 5689 +/- 11 K, log g = 4.385 +/- 0.005, [Fe/H] = +0.22 +/- 0.01, being in agreement with the published global seismic values, which confirms its status as solar analogue. The chromospheric activity level is compatible with the solar magnetic activity observed during 2014 and 2015. Conclusions. Our solar atlas is an essential tool for the analysis of solar-like stars and to characterise solar analogues and twins with HERMES. The differential analysis, using the presented solar atlas from HERMES observations allows us to obtain the fundamental parameters with very high accuracy. KIC 3241581 is a metal-rich solar analogue with a solar-like activity level in a binary system of unknown period. C1 [Beck, P. G.; Salabert, D.; Corsaro, E.; Garcia, R. A.] Univ Paris Diderot, Lab AIM, Ctr Saclay, CEA,DSM CNRS,IRFU,SAp, F-91191 Gif Sur Yvette, France. [Allende Prieto, C.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Allende Prieto, C.; Corsaro, E.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Van Reeth, T.; Tkachenko, A.; Raskin, G.; van Winckel, H.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium. [do Nascimento, J. -D., Jr.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [do Nascimento, J. -D., Jr.] Univ Fed Rio, Dept Fis Teor & Expt, BR-21941901 Rio De Janeiro, RJ, Brazil. [Corsaro, E.] Inst Astrofis Canarias, Tenerife 38205, Spain. RP Beck, PG (reprint author), Univ Paris Diderot, Lab AIM, Ctr Saclay, CEA,DSM CNRS,IRFU,SAp, F-91191 Gif Sur Yvette, France. EM paul.beck@cea.fr OI Garcia, Rafael/0000-0002-8854-3776 FU ANR (Agence Nationale de la Recherche, France) [ANR-12-BS05-0008]; Fund for Scientific Research of Flanders (FWO), Belgium [G.0B69.13]; European Community [312844, 269194]; CNES grants at CEA FX The observations are based on spectroscopy made with the Mercator Telescope, operated on the island of La Palma by the Flemish Community, at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. PGB acknowledges the ANR (Agence Nationale de la Recherche, France) program IDEE (no ANR-12-BS05-0008) "Interaction Des Etoiles et des Exoplanetes". TVR acknowledges financial support from the Fund for Scientific Research of Flanders (FWO), Belgium, under grant agreement G.0B69.13. AT is a Postdoctoral Fellow of the Fund for Scientific Research (FWO), Flanders, Belgium. E.C. is funded by the European Community's Seventh Framework Programme (FP7/2007/2013) under grant agreement No 312844 (SPACEINN). The research leading to these results received funding from the European Community's Seventh Framework Programme ([FP7/2007-2013]) under grant agreement No. 312844 (SPACEINN) and under grant agreement No. 269194 (IRSES/ASK). PGB also received funding from the CNES grants at CEA. The authors thank Dr. Antonio Garcia for providing us with the archived solar spectra from 2009. We thank the anonymous referee for constructive criticism which helped to improve the paper. NR 55 TC 3 Z9 3 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2016 VL 589 AR A27 DI 10.1051/0004-6361/201425423 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL0JI UT WOS:000375318300039 ER PT J AU Dichiara, S Guidorzi, C Amati, L Frontera, F Margutti, R AF Dichiara, S. Guidorzi, C. Amati, L. Frontera, F. Margutti, R. TI Correlation between peak energy and Fourier power density spectrum slope in gamma-ray bursts SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: general; methods: statistical ID REVERSE-SHOCK EMISSION; STRONG MAGNETIC-FIELDS; PROMPT EMISSION; LIGHT CURVES; PHOTOSPHERIC EMISSION; E-P,E-I-E-ISO CORRELATION; RELATIVISTIC TURBULENCE; LUMINOSITY CORRELATION; OPTICAL POLARIZATION; ICMART MODEL AB Context. The origin of the gamma-ray burst (GRB) prompt emission still defies explanation, in spite of recent progress made, for example, on the occasional presence of a thermal component in the spectrum along with the ubiquitous non-thermal component that is modelled with a Band function. The combination of finite duration and aperiodic modulations make GRBs hard to characterise temporally. Although correlations between GRB luminosity and spectral hardness on one side and time variability on the other side have long been known, the loose and often arbitrary definition of the latter makes the interpretation uncertain. Aims. We characterise the temporal variability in an objective way and search for a connection with rest-frame spectral properties for a number of well-observed GRBs. Methods. We studied the individual power density spectra (PDS) of 123 long GRBs with measured redshift, rest-frame peak energy E-p,E-i of the time-averaged vF(v) spectrum, and well-constrained PDS slope alpha detected with Swift, Fermi and past spacecraft. The PDS were modelled with a power law either with or without a break adopting a Bayesian Markov chain Monte Carlo technique. Results. We find a highly significant E-p,E-i-alpha anti-correlation. The null hypothesis probability is similar to 10(-9). Conclusions. In the framework of the internal shock synchrotron model, the E-p,E-i-alpha anti-correlation can hardly be reconciled with the predicted E-p,E-i alpha Gamma(-2), unless either variable microphysical parameters of the shocks or continual electron acceleration are assumed. Alternatively, in the context of models based on magnetic reconnection, the PDS slope and E-p,E-i are linked to the ejecta magnetisation at the dissipation site, so that more magnetised outflows would produce more variable GRB light curves at short timescales (less than or similar to 1 s), shallower PDS, and higher values of E-p,E-i. C1 [Dichiara, S.; Guidorzi, C.; Frontera, F.] Univ Ferrara, Dept Phys & Earth Sci, Via Saragat 1, I-44122 Ferrara, Italy. [Dichiara, S.] ICRANet, Pzza Repubbl 10, I-65122 Pescara, Italy. [Amati, L.; Frontera, F.] INAF Ist Astrofis Spaziale & Fis Cosm Bologna, Via Gobetti 101, I-40129 Bologna, Italy. [Margutti, R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Margutti, R.] NYU, Dept Phys, 4 Washington Pl, New York, NY 10003 USA. RP Dichiara, S (reprint author), Univ Ferrara, Dept Phys & Earth Sci, Via Saragat 1, I-44122 Ferrara, Italy. EM dichiara@fe.infn.it FU PRIN MIUR project on "Gamma Ray Bursts: from progenitors to physics of the prompt emission process", P.I.F. Frontera [2009 ERC3HT] FX We thank the anonymous referee for helpful comments that improved the paper. S.D., C.G., L.A., F.F. acknowledge support by PRIN MIUR project on "Gamma Ray Bursts: from progenitors to physics of the prompt emission process", P.I.F. Frontera (Prot. 2009 ERC3HT). NR 113 TC 1 Z9 1 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2016 VL 589 AR A97 DI 10.1051/0004-6361/201527635 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL0JI UT WOS:000375318300109 ER PT J AU Faria, JP Santos, NC Figueira, P Mortier, A Dumusque, X Boisse, I Lo Curto, G Lovis, C Mayor, M Melo, C Pepe, F Queloz, D Santerne, A Segransan, D Sousa, SG Sozzetti, A Udry, S AF Faria, J. P. Santos, N. C. Figueira, P. Mortier, A. Dumusque, X. Boisse, I. Lo Curto, G. Lovis, C. Mayor, M. Melo, C. Pepe, F. Queloz, D. Santerne, A. Segransan, D. Sousa, S. G. Sozzetti, A. Udry, S. TI The HARPS search for southern extra-solar planets XL. Searching for Neptunes around metal-poor stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; planetary systems; surveys; stars: individual: HD 87838; techniques: radial velocities ID RADIAL-VELOCITY DATA; MAIN-SEQUENCE STARS; GIANT PLANETS; METALLICITY CORRELATION; BAYESIAN-INFERENCE; STELLAR ACTIVITY; SHORT-PERIOD; HD 41248; MASS; COMPANIONS AB Context. As a probe of the metallicity of proto-planetary disks, stellar metallicity is an important ingredient for giant planet formation, most likely through its effect on the timescales in which rocky or icy planet cores can form. Giant planets have been found to be more frequent around metal-rich stars, in agreement with predictions based on the core-accretion theory. In the metal-poor regime, however, the frequency of planets, especially low-mass planets, and the way it depends on metallicity are still largely unknown. Aims. As part of a planet search programme focused on metal-poor stars, we study the targets from this survey that were observed with HARPS on more than 75 nights. The main goals are to assess the presence of low-mass planets and provide a first estimate of the frequency of Neptunes and super-Earths around metal-poor stars. Methods. We performed a systematic search for planetary companions, both by analysing the periodograms of the radial-velocities and by comparing, in a statistically meaningful way, models with an increasing number of Keplerians. Results. A first constraint on the frequency of planets in our metal-poor sample is calculated considering the previous detection (in our sample) of a Neptune-sized planet around HD 175607 and one candidate planet (with an orbital period of 68.42 d and minimum mass M-p sin i = 11.14 +/- 2.47 M-circle plus) for HD 87838, announced in the present study. This frequency is determined to be close to 13% and is compared with results for solar-metallicity stars. C1 [Faria, J. P.; Santos, N. C.; Figueira, P.; Santerne, A.; Sousa, S. G.] Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Oporto, Portugal. [Faria, J. P.; Santos, N. C.] Univ Porto, Dept Fis & Astron, Fac Ciencias, Rua Campo Alegre, P-4169007 Oporto, Portugal. [Mortier, A.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Dumusque, X.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Boisse, I.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Lo Curto, G.; Melo, C.] European So Observ, Casilla 19001, Santiago 19, Chile. [Lovis, C.; Mayor, M.; Pepe, F.; Queloz, D.; Segransan, D.; Udry, S.] Univ Geneva, Observ Geneve, 51 Chemin Maillettes, CH-1290 Sauverny, Switzerland. [Queloz, D.] Univ Cambridge, JJ Thomson Ave, Cambridge CB3 0HE, England. [Sozzetti, A.] INAF Osservatorio Astrofis Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy. RP Faria, JP (reprint author), Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Oporto, Portugal.; Faria, JP (reprint author), Univ Porto, Dept Fis & Astron, Fac Ciencias, Rua Campo Alegre, P-4169007 Oporto, Portugal. EM joao.faria@astro.up.pt RI Figueira, Pedro/J-4916-2013; OI Figueira, Pedro/0000-0001-8504-283X; Mortier, Annelies/0000-0001-7254-4363 FU Fundacao para a Ciencia e a Tecnologia (FCT) [UID/FIS/04434/2013]; FCT [PTDC/FIS-AST/1526/2014, SFRH/BD/93848/2013, IF/01037/2013, IF/00169/2012, IF/01037/2013CP1191/CT0001]; POPH/FSE (EC) by FEDER; European Union [313014, 627202] FX We would like to thank the referee, Dr. Silvano Desidera, for a careful reading and insightful comments on the paper that helped to improve its quality. This work was supported by Fundacao para a Ciencia e a Tecnologia (FCT) through the research grant UID/FIS/04434/2013. We also acknowledge the support from FCT in the form of grant reference PTDC/FIS-AST/1526/2014. J.P.F. acknowledges the support from FCT through the grant reference SFRH/BD/93848/2013 and thanks Brendon Brewer for his assistance with the diffusive nested sampling code. P.F. and N.C.S. acknowledge support by FCT through Investigador FCT contracts of reference IF/01037/2013 and IF/00169/2012, respectively, and POPH/FSE (EC) by FEDER funding through the program "Programa Operacional de Factores de Competitividade - COMPETE". P.F. further acknowledges support from FCT in the form of an exploratory project of reference IF/01037/2013CP1191/CT0001. A.M. received funding from the European Union Seventh Framework Program (FP7/2007-2013) under grant agreement number 313014 (ETAEARTH). A.S. is supported by the European Union under a Marie Curie Intra-European Fellowship for Career Development with reference FP7-PEOPLE-2013-IEF, number 627202. NR 82 TC 0 Z9 0 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2016 VL 589 AR A25 DI 10.1051/0004-6361/201527522 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL0JI UT WOS:000375318300037 ER PT J AU Goddi, C Ginsburg, A Zhang, Q AF Goddi, C. Ginsburg, A. Zhang, Q. TI Hot ammonia around young O-type stars III. High-mass star formation and hot core activity in W51 Main SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; line: profiles; ISM: kinematics and dynamics; ISM: molecules; stars: protostars; HII regions ID MAGNETIC-FIELDS; DYNAMICAL COLLAPSE; RADIO-CONTINUUM; MOLECULAR CORES; FORMING REGIONS; MASERS; METHANOL; MILLIMETER; EMISSION; OUTFLOW AB Context. This paper is the third in a series of NH3 multilevel imaging studies in well-known, high-mass star-forming regions. The main goal is to characterize kinematics and physical conditions of (hot and dense) circumstellar molecular gas around O-type young stars. Aims. We want to map at subarcsecond resolution highly excited inversion lines of NH3 in the high-mass star-forming region W51 Main (distance = 5.4 kpc), which is an ideal target to constrain theoretical models of high-mass star formation. Methods. Using the Karl Jansky Very Large Array (JVLA), we mapped the hot and dense molecular gas in W51 Main with similar to 0.'' 2-0.'' 3 angular resolution in five metastable (J = K) inversion transitions of ammonia (NH3): (J, K) = (6, 6), (7, 7), (9, 9), (10, 10), and (13, 13). These lines arise from energy levels between similar to 400 K and similar to 1700 K above the ground state. We also made maps of the (free-free) continuum emission at frequencies between 25 and 36 GHz. Results. We have identified and characterized two main centers of high-mass star formation in W51 Main, which excite hot cores and host one or multiple high-mass young stellar objects (YSOs) at their centers: the W51e2 complex and the W51e8 core (similar to 6 '' southward of W51e2). The former breaks down into three further subcores: W51e2-W, which surrounds the well-known hypercompact (HC) HII region, where hot NH3 is observed in absorption, and two additional dusty cores, W51e2-E (similar to 0.'' 8 to the East) and W51e2-NW (similar to 1 '' to the North), where hot NH3 is observed in emission. The velocity maps toward the HC HII region show a clear velocity gradient along the east-west in all lines. The gradient may indicate rotation, although any Keplerian motion must be on smaller scales (<1000 AU) as we do not directly observe a Keplerian velocity profile. The absence of outflow and/or maser activity and the low amount of molecular gas available for accretion (similar to 5 M-circle dot, assuming [NH3]/[H-2] = 10(-7)) with respect to the mass of the central YSO estimated from radio luminosity (>20 M-circle dot), both indicate that the central YSO has already accreted most of its final mass. On the other hand, the nearby W51e2-E, while not showing evidence of rotation, shows signatures of infall in a hot dense core (T similar to 170 K, n(H2) similar to 5 x 10(7) cm(-3)), based on asymmetric spectral profiles (skewed toward the blueshifted component) in optically thick emission lines of NH3. The relatively large amount of hot molecular gas available for accretion (similar to 20 M-circle dot within about half an arcsecond or 2500 AU), along with strong outflow and maser activity, indicates that the main accretion center in the W51e2 complex is W51e2-E rather than W51e2-W. Finally, W51e2-NW and W51e8, although less dense (n(H2) similar to 2 x 10(7) cm(-3) and similar to 3 x 10(6) cm(-3)), are also hot cores (T-gas similar to 140 and 200 K) and contain a significant amount of molecular gas (M-gas similar to 30 M-circle dot and similar to 70 M-circle dot, respectively). We speculate that they may host high-mass YSOs either at a previous evolutionary stage or with a mass that is lower than W51e2-E and W51e2-W. Conclusions. Using high-angular resolution multilevel imaging of highly excited NH3 metastable lines, we characterized the physical and dynamical properties of four individual high-mass young stars forming in the W51 Main clump. C1 [Goddi, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. [Goddi, C.] Leiden Univ, ALLEGRO Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Ginsburg, A.] ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Zhang, Q.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Goddi, C (reprint author), Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.; Goddi, C (reprint author), Leiden Univ, ALLEGRO Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM c.goddi@astro.ru.nl OI Zhang, Qizhou/0000-0003-2384-6589 FU JVLA program [12A-274] FX We thank the anonymous referee for a thorough effort in reviewing the manuscript and a very constructive report. We are grateful to Dr. Vincent Fish for providing the OH proper motion measurements. We are grateful to Riccardo Cesaroni for useful discussions. These data were obtained under JVLA program 12A-274. Spectral line fitting was performed using the pyspeckit package (Ginsburg & Mirocha 2011). NR 34 TC 0 Z9 0 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 MAY PY 2016 VL 589 AR A44 DI 10.1051/0004-6361/201527855 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL0JI UT WOS:000375318300056 ER PT J AU Salabert, D Regulo, C Garcia, RA Beck, PG Ballot, J Creevey, OL Hernandez, FP do Nascimento, JD Corsaro, E Egeland, R Mathur, S Metcalfe, TS Bigot, L Ceillier, T Palle, PL AF Salabert, D. Regulo, C. Garcia, R. A. Beck, P. G. Ballot, J. Creevey, O. L. Hernandez, F. Perez do Nascimento, J. -D., Jr. Corsaro, E. Egeland, R. Mathur, S. Metcalfe, T. S. Bigot, L. Ceillier, T. Palle, P. L. TI Magnetic variability in the young solar analog KIC 10644253 Observations from the Kepler satellite and the HERMES spectrograph SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: oscillations; stars: solar-type; stars: activity; methods: data analysis; methods: observational ID MAIN-SEQUENCE STARS; SUN-LIKE STARS; MODE FREQUENCY-SHIFTS; CA-II H; DIFFERENTIAL ROTATION; ACTIVITY CYCLE; P-MODES; STELLAR ACTIVITY; ACOUSTIC MODES; CHROMOSPHERIC VARIATIONS AB The continuous photometric observations collected by the Kepler satellite over 4 yr provide a wealth of data with an unequalled quantity and quality for the study of stellar evolution of more than 200 000 stars. Moreover, the length of the dataset provides a unique source of information for detecting magnetic activity and associated temporal variability in the acoustic oscillations. In this regards, the Kepler mission was awaited with great expectations. The search for the signature of magnetic activity variability in solar-like pulsations still remained unfruitful more than 2 yr after the end of the nominal mission. Here, however, we report the discovery of temporal variability in the low-degree acoustic frequencies of the young (1 Gyr-old) solar analog KIC 10644253 with a modulation of about 1.5 yr with significant temporal variations for the duration of the Kepler observations. The variations agree with the derived photometric activity. The frequency shifts extracted for KIC 10644253 are shown to result from the same physical mechanisms involved in the inner subsurface layers as in the Sun. In parallel, a detailed spectroscopic analysis of KIC 10644253 is performed based on complementary ground-based, high-resolution observations collected by the HERMES instrument mounted on the Mercator telescope. Its lithium abundance and chromospheric activity S index confirm that KIC 10644253 is a young and more active star than the Sun. C1 [Salabert, D.; Garcia, R. A.; Beck, P. G.; Corsaro, E.; Ceillier, T.] Univ Paris 07, Lab AIM, CEA, DRF CNRS,IRFU,SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France. [Salabert, D.; Creevey, O. L.; Bigot, L.] Univ Cote Azur, Lab Lagrange, Observ Cote Azur, CNRS, Bd Observ,CS 34229, F-06304 Nice 4, France. [Regulo, C.; Hernandez, F. Perez; Corsaro, E.; Palle, P. L.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Regulo, C.; Hernandez, F. Perez; Corsaro, E.; Palle, P. L.] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain. [Ballot, J.] CNRS, Inst Rech Astrophys & Planetol, 14 Ave Edouard Belin, F-31400 Toulouse, France. [Ballot, J.] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France. [do Nascimento, J. -D., Jr.] Univ Fed Rio Grande do Norte, UFRN, Dept Fis, DFTE, CP1641, BR-59072970 Natal, RN, Brazil. [do Nascimento, J. -D., Jr.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Egeland, R.] Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA. [Egeland, R.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Mathur, S.; Metcalfe, T. S.] Space Sci Inst, 4750 Walnut St Suite 205, Boulder, CO 80301 USA. RP Salabert, D (reprint author), Univ Paris 07, Lab AIM, CEA, DRF CNRS,IRFU,SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France.; Salabert, D (reprint author), Univ Cote Azur, Lab Lagrange, Observ Cote Azur, CNRS, Bd Observ,CS 34229, F-06304 Nice 4, France. EM david.salabert@cea.fr OI Garcia, Rafael/0000-0002-8854-3776 FU NASA's Science Mission Directorate; European Community [312844, 269194]; MINECO [AYA2012-39346-C02-02]; CNES GOLF grant; PLATO grant; ANR (Agence Nationale de la Recherche, France) [ANR-12-BS05-0008]; CNPq [PQ 308830/2012-1]; Newkirk Fellowship at the High Altitude Observatory; NASA [NNX12AE17G] FX The authors wish to thank the entire Kepler team, without whom these results would not be possible. Funding for this Discovery mission is provided by NASA's Science Mission Directorate. The ground-based observations are based on spectroscopy made with the Mercator Telescope, operated on the island of La Palma by the Flemish Community, at the Spanish Observatorio del Roque de los Muchachos of the Instituto de AstrofIsica de Canarias. The research leading to these results has received funding from the European Community's Seventh Framework Program ([FP7/2007-2013]) under grant agreement No. 312844 (SPACEINN) and under grant agreement No. 269194 (IRSES/ASK). The research leading to these results has also been supported by grant AYA2012-39346-C02-02 of the Spanish Secretary of State for R&D&i (MINECO). D.S. and R.A.G. acknowledge the financial support from the CNES GOLF and PLATO grants. P.G.B. acknowledges the ANR (Agence Nationale de la Recherche, France) program IDEE (No. ANR-12-BS05-0008) "Interaction Des Etoiles et des Exoplanetes". J.D.N.Jr. acknowledges support from CNPq PQ 308830/2012-1 CNPq PDE Harvard grant. R.E. is supported by the Newkirk Fellowship at the High Altitude Observatory. S.M. acknowledges support from the NASA grant NNX12AE17G. D.S. acknowledges the Observatoire de la Cote d'Azur for support during his stays. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 96 TC 7 Z9 7 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 MAY PY 2016 VL 589 AR A118 DI 10.1051/0004-6361/201527978 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL0JI UT WOS:000375318300130 ER PT J AU Pesendorfer, MB Sillett, TS Koenig, WD Morrison, SA AF Pesendorfer, Mario B. Sillett, T. Scott Koenig, Walter D. Morrison, Scott A. TI Scatter-hoarding corvids as seed dispersers for oaks and pines: A review of a widely distributed mutualism and its utility to habitat restoration SO CONDOR LA English DT Review DE Corvidae; ecosystem engineer; habitat restoration; Pinus; Quercus; scatter-hoarding; seed dispersal ID LONG-DISTANCE DISPERSAL; JAYS CYANOCITTA-CRISTATA; NORTHERN ROCKY-MOUNTAINS; FOOD-STORAGE BEHAVIOR; RECENT CLIMATE-CHANGE; WESTERN SCRUB-JAYS; SANTA-CRUZ ISLAND; WHITEBARK-PINE; BLUE JAYS; CLARKS NUTCRACKER AB Seed dispersal mutualisms with scatter-hoarders play a crucial role in population dynamics of temperate large-seeded trees. These behaviors shape seed dispersal patterns, which can be applied to conservation of populations, communities, and even ecosystems dominated by large-seeded trees. We draw on a growing body of literature to describe the ecological context and consequences of scatter-hoarding as a seed dispersal mechanism. We synthesize the quantitative literature on the interaction between members of the avian family Corvidae (crows, ravens, jays, magpies, and nutcrackers) and nut-bearing trees such as pines (Pinus spp.) and oaks (Quercus spp.) to examine unique aspects of avian scatter-hoarders as seed dispersers. During the scatter-hoarding process, seed selectivity, transportation distance, hoarding frequency, and cache placement affect seed dispersal effectiveness, a measure of the quantity and quality of dispersal. Case studies from around the world highlight the role of corvid seed dispersal in population dynamics of trees, and how the birds' scatter-hoarding behavior can be facilitated for the restoration of oak-and pine-dominated habitats. This mutualism, which provides many plant species with long-distance, high-quality seed dispersal, will likely become even more important for conservation of oak and pine ecosystems as suitable climates shift rapidly in the decades ahead. This ecosystem service provided by corvids could therefore serve as an efficient conservation tool. C1 [Pesendorfer, Mario B.] Univ Nebraska, Sch Biol Sci, Lincoln, NE USA. [Pesendorfer, Mario B.; Sillett, T. Scott] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC USA. [Pesendorfer, Mario B.; Koenig, Walter D.] Cornell Lab Ornithol, Ithaca, NY USA. [Koenig, Walter D.] Cornell Univ, Dept Neurobiol & Behav, Ithaca, NY 14853 USA. [Morrison, Scott A.] Nature Conservancy, San Francisco, CA USA. RP Pesendorfer, MB (reprint author), Univ Nebraska, Sch Biol Sci, Lincoln, NE USA.; Pesendorfer, MB (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC USA.; Pesendorfer, MB (reprint author), Cornell Lab Ornithol, Ithaca, NY USA. EM mario.pesendorfer@yahoo.com OI Pesendorfer, Mario/0000-0002-7994-7090 FU Nature Conservancy; Smithsonian Institution; American Ornithologists' Union; Animal Behavior Society FX This work was supported by The Nature Conservancy and the Smithsonian Institution, as well as by student awards from the American Ornithologists' Union and the Animal Behavior Society. NR 216 TC 4 Z9 4 U1 14 U2 31 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 EI 1938-5129 J9 CONDOR JI Condor PD MAY PY 2016 VL 118 IS 2 BP 215 EP 237 DI 10.1650/CONDOR-15-125.1 PG 23 WC Ornithology SC Zoology GA DN0QO UT WOS:000376769000001 ER PT J AU Gingerich, O AF Gingerich, Owen TI Finding Longitude SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 [Gingerich, Owen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0021-8286 EI 1753-8556 J9 J HIST ASTRON JI J. Hist. Astron. PD MAY PY 2016 VL 47 BP 224 EP 225 PN 2 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA DM8GR UT WOS:000376600000014 ER PT J AU Darroch, SAF Locatelli, ER Mccoy, VE Clark, EG Anderson, RP Tarhan, LG Hull, PM AF Darroch, Simon A. F. Locatelli, Emma R. Mccoy, Victoria E. Clark, Elizabeth G. Anderson, Ross P. Tarhan, Lidya G. Hull, Pincelli M. TI TAPHONOMIC DISPARITY IN FORAMINIFERA AS A PALEO-INDICATOR FOR SEAGRASS SO PALAIOS LA English DT Article ID GREAT-BARRIER-REEF; BENTHIC FORAMINIFERA; SAN-SALVADOR; BOTTOM COMMUNITIES; ARCHAIAS-ANGULATUS; DEATH ASSEMBLAGES; SEDIMENT; ENVIRONMENTS; BAHAMAS; DEGRADATION AB Seagrass meadows are a key component of marine ecosystems that play a variety of prominent geobiological roles in modern coastal environments. However, seagrass itself has low preservation potential, and consequently seagrass meadows are hard to identify in the rock record. In this study we combine observational taphonomic data from a modern sparse seagrass meadow with actualistic taphonomic experiments, in order to test whether taphonomic disparity (i.e., evenness in the distribution of taphonomic grades among multiple individuals) in the larger benthic foraminiferan Archaias angulatus has potential as a paleo-indicator for seagrass dominated communities. Our observational study demonstrates that sparse seagrass meadows possess a higher proportion of both pristine and highly altered tests than non-seagrass settings. Our taphonomic experiments, conducted over a six-month period, demonstrate a greater magnitude of bioerosion and diversity of bioerosion types in foraminifera deployed within sparse seagrass patches, than those deployed in patches without any seagrass cover. Although our experimental results in particular have high variability, these combined approaches provide a link between pattern (high taphonomic disparity) and process (higher rates of bioerosion) in developing the taphonomic signature of seagrass meadows. On the basis of these results we suggest several taphonomic criteria that could be used to identify seagrass meadows in the rock record. These criteria are potentially species-independent, and so may have greater utility as seagrass proxies than invertebrate indicator species that frequently have limited temporal or spatial distributions. C1 [Darroch, Simon A. F.; Locatelli, Emma R.; Mccoy, Victoria E.; Clark, Elizabeth G.; Anderson, Ross P.; Tarhan, Lidya G.; Hull, Pincelli M.] Yale Univ, Dept Geol & Geophys, 210 Whitney Ave, New Haven, CT 06511 USA. [Darroch, Simon A. F.] Smithsonian Inst, POB 37012,MRC 121, Washington, DC 20013 USA. RP Locatelli, ER (reprint author), Yale Univ, Dept Geol & Geophys, 210 Whitney Ave, New Haven, CT 06511 USA. EM emma.locatelli@yale.edu FU Cushman Foundation; Gerace Research Center Student Research Grant FX We would like to thank Tom Rothfus, Erin Rothfus, and all staff at the Gerace Research Centre. SAFD would like to thank Amelinda Webb for invaluable assistance in the field. An earlier version of this manuscript was much improved after constructive comments and criticisms from two anonymous reviewers. This research was made possible through generous funding from the Cushman Foundation (William J. Sliter award), and a Gerace Research Center Student Research Grant (both to SAFD). NR 52 TC 0 Z9 0 U1 3 U2 5 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 EI 1938-5323 J9 PALAIOS JI Palaios PD MAY 1 PY 2016 VL 31 IS 5 BP 242 EP 258 DI 10.2110/palo.2015.046 PG 17 WC Geology; Paleontology SC Geology; Paleontology GA DM8FQ UT WOS:000376597200004 ER PT J AU Deutsch, JI AF Deutsch, James I. TI A 1,000-Year History of Polish Jews SO PUBLIC HISTORIAN LA English DT Art Exhibit Review C1 [Deutsch, James I.] Smithsonian Inst, Washington, DC 20560 USA. RP Deutsch, JI (reprint author), Smithsonian Inst, Washington, DC 20560 USA. 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 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD MAY PY 2016 VL 38 IS 2 BP 84 EP 89 PG 6 WC History SC History GA DM7PG UT WOS:000376551900011 ER PT J AU White, RB AF White, Roger B. TI The Pennsylvania Turnpike: America's First Superhighway SO PUBLIC HISTORIAN LA English DT Art Exhibit Review C1 [White, Roger B.] Natl Museum Amer Hist, Smithsonian Inst, Washington, DC 20001 USA. RP White, RB (reprint author), Natl Museum Amer Hist, Smithsonian Inst, Washington, DC 20001 USA. 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 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD MAY PY 2016 VL 38 IS 2 BP 89 EP 93 PG 5 WC History SC History GA DM7PG UT WOS:000376551900012 ER PT J AU Young, HS Dirzo, R Helgen, KM McCauley, DJ Nunn, CL Snyder, P Veblen, KE Zhao, S Ezenwa, VO AF Young, Hillary S. Dirzo, Rodolfo Helgen, Kristofer M. McCauley, Douglas J. Nunn, Charles L. Snyder, Paul Veblen, Kari E. Zhao, Serena Ezenwa, Vanessa O. TI Large wildlife removal drives immune defence increases in rodents SO FUNCTIONAL ECOLOGY LA English DT Article DE defaunation; ecoimmunology; Kenya Long-term Exclosure Experiment; rodent; wildlife decline ID ECOSYSTEM NUTRIENT DYNAMICS; LARGE HERBIVORES; AFRICAN SAVANNA; PREDATION RISK; TRADE-OFFS; CENTRAL KENYA; TACHYCINETA-BICOLOR; INFECTIOUS-DISEASE; SEASONAL-CHANGES; TREE SWALLOWS AB 1. Anthropogenic disturbances involving land use change, climate disruption, pollution and invasive species have been shown to impact immune function of wild animals. These immune changes have direct impacts on the fitness of impacted animals and, also, potentially indirect effects on other species and on ecological processes, notably involving the spread of infectious disease. Here, we investigate whether the selective loss of large wildlife can also drive changes in immune function of other consumer species. 2. Using a long-standing large-scale exclosure experiment in East Africa, we investigated the effects of selective removal of large wildlife on multiple measures of immune function in the dominant small rodent in the system, the East African pouched mouse, Saccostomus mearnsi. 3. We find support for a general increase in immune function in landscapes where large wildlife has been removed, but with some variation across immune parameters. These changes may be mediated in part by increased pathogen pressure in plots where large wildlife has been removed due to major increases in rodent density in such plots, but other factors such as changes in food resources are also likely involved. 4. Overall, our research reveals that the elimination of large-bodied wildlife - now recognized as another major form of global anthropogenic change - may have cascading effects on immune health, with the potential for these effects to also impact disease dynamics in ecological communities. C1 [Young, Hillary S.; McCauley, Douglas J.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. [Young, Hillary S.; Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Young, Hillary S.; McCauley, Douglas J.; Veblen, Kari E.; Zhao, Serena; Ezenwa, Vanessa O.] Mpala Res Ctr, Box 555, Nanyuki, Kenya. [Dirzo, Rodolfo] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Nunn, Charles L.] Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27708 USA. [Nunn, Charles L.] Duke Univ, Duke Global Hlth Inst, Durham, NC 27708 USA. [Snyder, Paul] Univ Georgia, Coll Vet Med, Odum Sch Ecol, Athens, GA 30602 USA. [Snyder, Paul] Univ Georgia, Coll Vet Med, Dept Infect Dis, Athens, GA 30602 USA. [Snyder, Paul] Oregon State Univ, Dept Integrat Biol, Corvallis, OR 97331 USA. [Veblen, Kari E.] Utah State Univ, Dept Wildland Resources, Logan, UT 84322 USA. [Veblen, Kari E.] Utah State Univ, Ctr Ecol, Logan, UT 84322 USA. RP Young, HS (reprint author), Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA.; Young, HS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA.; Young, HS (reprint author), Mpala Res Ctr, Box 555, Nanyuki, Kenya. EM hillary.young@lifesci.ucsb.edu FU James Smithson Fund of the Smithsonian Institution; Smithsonian Grand Challenges Initiative; National Geographic Society; Woods Institute for the Environment (Stanford University); Smithsonian Institution Women's Committee [SWC 22, 44]; Harvard University Center for the Environment (HUCE Environmental Fellows Program); National Science Foundation [LTREB BSR 97-07477, 03-16402, 08-16453, 12-56004, 12-56034] FX We thank Bernard Agwanda, Benjamin Boyce, Peter Lokeny, Everlyn Ndinda, Ashley Hintz, Melanie Fratto, Margaret Kinnaird and Jacy Hyde for their assistance throughout this project. We also thank the Kenyan Government, Kenya Wildlife Service, National Museums Kenya and Mpala Research Centre for facilitating this research. Financial support for this project came from the James Smithson Fund of the Smithsonian Institution, the Smithsonian Grand Challenges Initiative, the National Geographic Society, the Woods Institute for the Environment (Stanford University), the Smithsonian Institution Women's Committee (SWC 22 and 44), the Harvard University Center for the Environment (HUCE Environmental Fellows Program) and the National Science Foundation (LTREB BSR 97-07477, 03-16402, 08-16453, 12-56004 and 12-56034). All small mammal trapping and sampling were in accordance with Institutional Animal Care and Use permits (Smithsonian Institution IACUC permit # 2009-04). We thank S. Miller, L. Helgen, A. Driskell, D. Lunde and J. Ososky for assistance at the Smithsonian. NR 81 TC 1 Z9 1 U1 14 U2 20 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 EI 1365-2435 J9 FUNCT ECOL JI Funct. Ecol. PD MAY PY 2016 VL 30 IS 5 BP 799 EP 807 DI 10.1111/1365-2435.12542 PG 9 WC Ecology SC Environmental Sciences & Ecology GA DL9DN UT WOS:000375941800014 ER PT J AU Martin, SH Most, M Palmer, WJ Salazar, C McMillan, WO Jiggins, FM Jiggins, CD AF Martin, Simon H. Most, Markus Palmer, William J. Salazar, Camilo McMillan, W. Owen Jiggins, Francis M. Jiggins, Chris D. TI Natural Selection and Genetic Diversity in the Butterfly Heliconius melpomene SO GENETICS LA English DT Article DE background selection; genetic hitchhiking; recombination rate; selective sweeps; effective population size ID SLIGHTLY DELETERIOUS MUTATIONS; RECOMBINATION RATE VARIATION; ADAPTIVE PROTEIN EVOLUTION; MULTILOCUS GENOTYPE DATA; MCDONALD-KREITMAN TEST; DROSOPHILA-MELANOGASTER; POPULATION-GENETICS; MAXIMUM-LIKELIHOOD; POSITIVE SELECTION; SUBDIVIDED POPULATION AB A combination of selective and neutral evolutionary forces shape patterns of genetic diversity in nature. Among the insects, most previous analyses of the roles of drift and selection in shaping variation across the genome have focused on the genus Drosophila. A more complete understanding of these forces will come from analyzing other taxa that differ in population demography and other aspects of biology. We have analyzed diversity and signatures of selection in the neotropical Heliconius butterflies using resequenced genomes from 58 wild-caught individuals of Heliconius melpomene and another 21 resequenced genomes representing 11 related species. By comparing intraspecific diversity and interspecific divergence, we estimate that 31% of amino acid substitutions between Heliconius species are adaptive. Diversity at putatively neutral sites is negatively correlated with the local density of coding sites as well as nonsynonymous substitutions and positively correlated with recombination rate, indicating widespread linked selection. This process also manifests in significantly reduced diversity on longer chromosomes, consistent with lower recombination rates. Although hitchhiking around beneficial nonsynonymous mutations has significantly shaped genetic variation in H. melpomene, evidence for strong selective sweeps is limited overall. We did however identify two regions where distinct haplotypes have swept in different populations, leading to increased population differentiation. On the whole, our study suggests that positive selection is less pervasive in these butterflies as compared to fruit flies, a fact that curiously results in very similar levels of neutral diversity in these very different insects. C1 [Martin, Simon H.; Most, Markus; Jiggins, Chris D.] Univ Cambridge, Dept Zool, Cambridge CB2 3EH, England. [Palmer, William J.; Jiggins, Francis M.] Univ Cambridge, Dept Genet, Cambridge CB2 3EH, England. [Salazar, Camilo] Univ Rosario, Fac Nat Sci & Math, Biol Program, Bogota 111221, Colombia. [McMillan, W. Owen] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. RP Martin, SH (reprint author), Univ Cambridge, Dept Zool, Room S22,Downing St, Cambridge CB2 3EJ, England. EM shm45@cam.ac.uk RI Jiggins, Chris/B-9960-2008; OI Jiggins, Chris/0000-0002-7809-062X; Salazar, Camilo/0000-0001-9217-6588 FU European Research Council [281668, 339873]; John Fell Fund of Oxford University grant; St. John's College, Cambridge; Swiss National Science Foundation Early PostDoc Mobility fellowship [P2EZP3_148773]; Austrian Science Fund Erwin Schrodinger fellowship [J3774-B25]; Convocatoria para Proyectos de Investigacion en Ciencias Basicas [FP44842-103-2015]; Medical Research Council Centenary Award FX We thank the handling editor, David Begun, and two anonymous reviewers, whose comprehensive comments greatly improved this manuscript. Nick Barton and Aylwyn Scally provided helpful comments on an earlier draft. We thank John Davey for advice on the recombination rate analyses and for useful discussions of the results. James Walters provided advice for the analysis of the rate of adaptive substitution, and some of the groundwork for this analysis was performed by Gabriel Jamie and Joseph Harvey. We also thank James Mallet and Lawrence Gilbert for thought-provoking discussions of the life history of Heliconius. Finally, we thank Jenny Barna for computing support. This work was funded by European Research Council grants 281668 to F.M.J. and 339873 to C.D.J. Some sequencing was funded by a John Fell Fund of Oxford University grant to Judith Mank and James Walters. S.H.M. was supported by St. John's College, Cambridge. M.M. was supported by a Swiss National Science Foundation Early PostDoc Mobility fellowship (P2EZP3_148773) and an Austrian Science Fund Erwin Schrodinger fellowship (J3774-B25). C.S. was funded by Convocatoria para Proyectos de Investigacion en Ciencias Basicas-2014 (Colciencias), contract no. FP44842-103-2015. W.J.P was supported by a Medical Research Council Centenary Award. NR 103 TC 0 Z9 0 U1 24 U2 38 PU GENETICS SOCIETY AMERICA PI BETHESDA PA 9650 ROCKVILLE AVE, BETHESDA, MD 20814 USA SN 0016-6731 EI 1943-2631 J9 GENETICS JI Genetics PD MAY PY 2016 VL 203 IS 1 BP 525 EP + DI 10.1534/genetics.115.183285 PG 67 WC Genetics & Heredity SC Genetics & Heredity GA DM0DD UT WOS:000376012100035 PM 27017626 ER PT J AU Schweitzer, CE Karasawa, H Luque, J Feldmann, RM AF Schweitzer, Carrie E. Karasawa, Hiroaki Luque, Javier Feldmann, Rodney M. TI PHYLOGENY AND CLASSIFICATION OF NECROCARCINOIDEA FORSTER, 1968 (BRACHYURA: RANINOIDA) WITH THE DESCRIPTION OF TWO NEW GENERA SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article DE Camarocarcinidae; Cenomanocarcinidae; Necrocarcinidae; Orithopsidae; Paranecrocarcinidae; Phylogeny ID DECAPOD CRUSTACEANS; CRABS CRUSTACEA; FAMILY CRUSTACEA; SOUTH-AMERICA; NORTH-DAKOTA; VAN-STRAELEN; GENUS; REVISION; CENOMANOCARCINIDAE; PODOTREMATA AB Phylogenetic analysis of most species within Necrocarcinoidea based upon 55 adult morphological characters supports the inclusion of 5 families within the superfamily. Two new genera are recognized within Necrocarcinidae, Arcticocarcinus n. gen. and Elektrocarcinus n. gen., and numerous new combinations have resulted. Necrocarcinoidea exhibited diversity peaks in the Albian (Early Cretaceous) and Campanian (Late Cretaceous), and displayed niche partitioning at the family level. Most Paleogene occurrences of Necrocarcinoidea are in carbonate rocks of Northern Europe. C1 [Schweitzer, Carrie E.] Kent State Univ Stark, Dept Geol, 6000 Frank Ave NW, North Canton, OH 44720 USA. [Karasawa, Hiroaki] Mizunami Fossil Museum, Gifu 5096132, Japan. [Luque, Javier] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. [Luque, Javier] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Feldmann, Rodney M.] Kent State Univ, Dept Geol, Kent, OH 44242 USA. RP Feldmann, RM (reprint author), Kent State Univ, Dept Geol, Kent, OH 44242 USA. EM rfeldman@kent.edu 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); Izaak Walton Killam Memorial Scholarship 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 CES and RMF. Field work for collection of comparative material and the species herein described by RMF and CES was funded by NSF grant OPP-9909184 to RMF and K. L. Bice and NSF grant INT-0003058 to RMF and CES. A graduate Scholarship to JL was provided by the Natural Science and Engineering Research Council of Canada (NSERC CGS-D) and the Izaak Walton Killam Memorial Scholarship. G. Schweigert (Staatliches Museum fur Naturkunde, Stuttgart, Germany), M. Nose (BSP), O. Schultz and A. Kroh (Geological and Palaeontological Department of the Naturhistorisches Museum Wien, Vienna, Austria), I. Zorn (Geologische Bundesanstalt Austria, Vienna, Austria), M. Munt and C. Mellish (BM), M. Riley (SM), P. Muller (Termeszettudomanyi Muzeum, Fold-es oslenytar, Budapest, Hungary), S. Charbonnier (MNHN), P. Artal and S. Calzada (Museo Geologico del Seminario de Barcelona, Barcelona, Spain), S. Shelton and J. Martin (SDSM), R. Lemaitre and K. Reed (Crustacea) and K. Hollis and M. Florence (Paleobiology) (USNM), N. S. Rugh and T. Demere (SDSNH), D. Parris and R. Pelligrini (NJSM), G. Rosenberg (ANSP), R. Portell (Florida Museum of Natural History, University of Florida, Gainesville, FL, USA), A. Lord and C. Franz (Paleontology) and the late M. Turkay (Crustacea) (Senckenberg Naturmuseum, Frankfurt, Germany); M. Eriksson (LO), M. Coyne (GSC) 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 (UT), C. Beschin, A. De Angeli, and V. Frisone (Museo Civico "G. Zannato," Montecchio Maggiore (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 (MGUH), and A. E. Sanders (Charleston Museum, Charleston, SC, USA) provided access to their collections or facilitated loans from their institutions. T. Snyder and all of the staff at the Inter-Library Loan service at the KSU library assisted in finding old and obscure literature. G. 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. G. Schweigert (Staatliches Museum fur Naturkunde, Stuttgart, Germany), F. J. Vega (UNAM, Mexico City, Mexico), and an anonymous reviewer provided numerous useful comments. NR 110 TC 1 Z9 1 U1 0 U2 0 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 EI 1937-240X J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD MAY PY 2016 VL 36 IS 3 BP 338 EP 372 DI 10.1163/1937240X-00002432 PG 35 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA DM0SK UT WOS:000376055900009 ER PT J AU Yager, J AF Yager, Jill TI COLLECTING AND PROCESSING REMIPEDES SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article DE anchialine caves; preservation; Sket bottle; troglobitic crustaceans ID SAN-SALVADOR ISLAND; ANCHIALINE CAVE; SURFACE-WATER; SPELEONECTIDAE; BEHAVIOR; BAHAMAS C1 [Yager, Jill] Smithsonian Inst, Museum Support Ctr, Dept Invertebrate Zool, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. RP Yager, J (reprint author), Smithsonian Inst, Museum Support Ctr, Dept Invertebrate Zool, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM jill.yager@gmail.com NR 7 TC 0 Z9 0 U1 1 U2 2 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 EI 1937-240X J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD MAY PY 2016 VL 36 IS 3 BP 405 EP 407 DI 10.1163/1937240X-00002433 PG 3 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA DM0SK UT WOS:000376055900015 ER PT J AU Evans, NR Bond, HE Schaefer, GH Mason, BD Tingle, E Karovska, M Pillitteri, I AF Evans, Nancy Remage Bond, Howard E. Schaefer, Gail H. Mason, Brian D. Tingle, Evan Karovska, Margarita Pillitteri, Ignazio TI HUBBLE SPACE TELESCOPE SNAPSHOT SURVEY FOR RESOLVED COMPANIONS OF GALACTIC CEPHEIDS SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; stars: formation; stars: massive; stars: variables: Cepheids ID LOW-MASS COMPANIONS; CLASSICAL CEPHEID; BINARY CEPHEIDS; STARS; LUMINOSITY; MULTIPLICITY; PARALLAXES; EVOLUTION; CLUSTER; CENSUS AB We have conducted an imaging survey with the Hubble Space Telescope Wide Field Camera 3 (WFC3) of 70 Galactic Cepheids, typically within 1 kpc, with the aim of finding resolved physical companions. The WFC3 field typically covers the 0.1 pc area where companions are expected. In this paper, we identify 39 Cepheids having candidate companions, based on their positions in color magnitude diagrams, and having separations,>=-5" from the Cepheids. We use follow-up observations of 14 of these candidates with XMM-Newton, and of one of them with ROSAT, to separate X-ray-active young stars (probable physical companions) from field stars (chance alignments). Our preliminary estimate, based on the optical and X-ray observations, is that only 3% of the Cepheids in the sample have wide companions. Our survey easily detects resolved main -sequence companions as faint as spectral type K. Thus the fact that the two most probable companions (those of FF Aql and RV Sco) are earlier than type K is not simply a function of the detection limit. We find no physical companions having separations larger than 4000 au in the X-ray survey. Two Cepheids are exceptions in that they do have young companions at significantly larger separations (5 Cep and S Nor), but both belong to a cluster or a loose association, so our working model is that they are not gravitationally bound binary members, but rather cluster/association members. All of these properties provide constraints on both star formation and subsequent dynamical evolution. The low frequency of true physical companions at separations >5" is confirmed by examination of the subset of the nearest Cepheids and also the density of the fields. C1 [Evans, Nancy Remage; Tingle, Evan; Karovska, Margarita; Pillitteri, Ignazio] Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA. [Bond, Howard E.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Bond, Howard E.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Schaefer, Gail H.] Georgia State Univ, Mt Wilson Observ, CHARA Array, Mt Wilson, CA 91023 USA. [Mason, Brian D.] US Naval Observ, 3450 Massachusetts Ave NW, Washington, DC 20392 USA. [Pillitteri, Ignazio] INAF Osservatorio Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA.; Bond, HE (reprint author), Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.; Bond, HE (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM nevans@cfa.harvard.edu; heb11@psu.edu OI Pillitteri, Ignazio/0000-0003-4948-6550 FU STScI [GO-12215.01-A, GO-13368.01-A]; Chandra X-ray Center NASA [NAS8-03060] FX Financial support from STScI grants GO-12215.01-A and GO-13368.01-A and also Chandra X-ray Center NASA Contract NAS8-03060 is gratefully acknowledged. Vizier and SIMBAD were used in the preparation of this study. This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Observatory. NR 42 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2016 VL 151 IS 5 AR 129 DI 10.3847/004-6256/151/5/129 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL4MH UT WOS:000375610400020 ER PT J AU Rodriguez, JE Stassun, KG Lund, MB Siverd, RJ Pepper, J Tang, S Kafka, S Gaudi, BS Conroy, KE Beatty, TG Stevens, DJ Shappee, BJ Kochanek, CS AF Rodriguez, Joseph E. Stassun, Keivan G. Lund, Michael B. Siverd, Robert J. Pepper, Joshua Tang, Sumin Kafka, Stella Gaudi, B. Scott Conroy, Kyle E. Beatty, Thomas G. Stevens, Daniel J. Shappee, Benjamin J. Kochanek, Christopher S. TI AN EXTREME ANALOGUE OF epsilon AURIGAE: AN M-GIANT ECLIPSED EVERY 69 YEARS BY A LARGE OPAQUE DISK SURROUNDING A SMALL HOT SOURCE SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; circumstellar matter; stars: AGB and post-AGB; stars: individual (TYC 2505-672-1); stars: massive ID WHITE-DWARF; CATALOG; SYSTEM; STARS AB We present TYC 2505-672-1 as a newly discovered and remarkable eclipsing system comprising an M-type red giant that undergoes a similar to 3.45 year long, near-total eclipse (depth of similar to 4.5mag) with a very long period of similar to 69.1 years. TYC 2505-672-1 is now the longest-period eclipsing binary system yet discovered, more than twice as long as that of the currently longest-period system, epsilon Aurigae. We show from analysis of the light curve including both our own data and historical data spanning more than 120 years and from modeling of the spectral energy distribution, both before and during eclipse, that the red giant primary is orbited by a moderately hot source (T-eff approximate to 8000 K) that is itself surrounded by an extended, opaque circumstellar disk. From the measured ratio of luminosities, the radius of the hot companion must be in the range of 0.1-0.5 R-circle dot (depending on the assumed radius of the red giant primary), which is an order of magnitude smaller than that for a main sequence A star and 1-2 orders of magnitude larger than that for a white dwarf. The companion is therefore most likely a "stripped red giant" subdwarf-B type star destined to become a He white dwarf. It is, however, somewhat cooler than most sdB stars, implying a very low mass for this "pre-HeWD" star. The opaque disk surrounding this hot source may be a remnant of the stripping of its former hydrogen envelope. However, it is puzzling how this object became stripped, given that it is at present so distant (orbital semimajor axis of similar to 24 au) from the current red giant primary star. Extrapolating from our calculated ephemeris, the next eclipse should begin in early UT 2080 April and end in mid UT 2083 September (eclipse center UT 2081 December 24). In the meantime, radial velocity observations would establish the masses of the components, and high-cadence UV observations could potentially reveal oscillations of the hot companion that would further constrain its evolutionary status. In any case, this system is poised to become an exemplar of a very rare class of systems, even more extreme in several respects than the well studied archetype epsilon Aurigae. C1 [Rodriguez, Joseph E.; Stassun, Keivan G.; Lund, Michael B.; Conroy, Kyle E.] Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr, Nashville, TN 37235 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, 1000 17th Ave North, Nashville, TN 37208 USA. [Siverd, Robert J.] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Santa Barbara, CA 93117 USA. [Pepper, Joshua] Lehigh Univ, Dept Phys, 16 Mem Dr East, Bethlehem, PA 18015 USA. [Tang, Sumin] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Tang, Sumin] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Tang, Sumin] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Kafka, Stella] Amer Assoc Variable Star Observers, 49 Bay State Rd, Cambridge, MA 02138 USA. [Gaudi, B. Scott; Stevens, Daniel J.; Kochanek, Christopher S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Beatty, Thomas G.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Beatty, Thomas G.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, 525 Davey Lab, University Pk, PA 16802 USA. [Shappee, Benjamin J.] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Kochanek, Christopher S.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys CCAPP, 191 W Woodruff Ave, Columbus, OH 43210 USA. RP Rodriguez, JE (reprint author), Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr, Nashville, TN 37235 USA. OI Rodriguez, Joseph/0000-0001-8812-0565 FU NASA [NNG04GO70G, NAS 5-26555]; Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics; NSF CAREER [AST-1056524]; NSF PAARE [AST-1358862]; NSF [AST-0407380, AST-0909073, AST-1313370, AST-0908816, AST-1515927, AST-1515876]; National Aeronautics and Space Administration through the Science Mission Directorate Near-Earth Objects Observations Program [NNG05GF22G]; U.S. National Science Foundation [AST-0909182, AST-1313422]; CCAPP at the Ohio State University; Center for Cosmology and AstroParticle Physics (CCAPP) at OSU; Mt. Cuba Astronomical Foundation; George Skestos, and the Robert Martin Ayers Sciences Fund; NASA - Space Telescope Science Institute [HF-51348.001] FX 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. This work has made use of NASA's Astrophysics Data System and the SIMBAD database operated at CDS, Strasbourg, France.; Work by B.S.G. and D.J.S. was partially supported by NSF CAREER Grant AST-1056524. Work by K.G.S. was supported by NSF PAARE grant AST-1358862.; The DASCH project at Harvard is grateful for partial support from NSF grants AST-0407380, AST-0909073, and AST-1313370.; The CSS survey is funded by the National Aeronautics and Space Administration under Grant No. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Program. The CRTS survey is supported by the U.S. National Science Foundation under grants AST-0909182 and AST-1313422.; Development of ASAS-SN has been supported by NSF grant AST-0908816 and CCAPP at the Ohio State University. ASAS-SN is supported by NSF grant AST-1515927, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, the Mt. Cuba Astronomical Foundation, George Skestos, and the Robert Martin Ayers Sciences Fund.; B.S. is supported by NASA through Hubble Fellowship grant HF-51348.001 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. CSK is supported by NSF grants AST-1515876 and AST-1515927. NR 29 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2016 VL 151 IS 5 AR 123 DI 10.3847/0004-6256/151/5/123 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL4MH UT WOS:000375610400014 ER PT J AU Westhues, C Haas, M Barthel, P Wilkes, BJ Willner, SP Kuraszkiewicz, J Podigachoski, P Leipski, C Meisenheimer, K Siebenmorgen, R Chini, R AF Westhues, Christian Haas, Martin Barthel, Peter Wilkes, Belinda J. Willner, S. P. Kuraszkiewicz, Joanna Podigachoski, Pece Leipski, Christian Meisenheimer, Klaus Siebenmorgen, Ralf Chini, Rolf TI STAR FORMATION IN 3CR RADIO GALAXIES AND QUASARS AT z < 1 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: active; infrared: galaxies; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; PROBE WMAP OBSERVATIONS; COMPACT STEEP-SPECTRUM; PALOMAR-GREEN QUASARS; DIGITAL SKY SURVEY; HIGH-RESOLUTION OBSERVATIONS; SPITZER-SPACE-TELESCOPE; FAR-INFRARED EMISSION; BLACK-HOLE MASS AB Using the Herschel Space Observatory we have observed a representative sample of 87 powerful 3CR sources at redshift z < 1. The far-infrared (FIR, 70-500 mu m) photometry is combined with mid-infrared (MIR) photometry from the Wide-Field Infrared Survey Explorer and cataloged data to analyze the complete spectral energy distributions (SEDs) of each object from optical to radio wavelength. To disentangle the contributions of different components, the SEDs are fitted with a set of templates to derive the luminosities of host galaxy starlight, dust torus emission powered by active galactic nuclei (AGNs), and cool dust heated by stars. The level of emission from relativistic jets is also estimated to isolate the thermal host galaxy contribution. The new data are in line with the orientation-based unification of high-excitation radio-loud AGN, in that the dust torus becomes optically thin longwards of 30 mm. The low-excitation radio galaxies and the MIR-weak sources represent an MIR-and FIR-faint AGN population that is different from the high-excitation MIR-bright objects; it remains an open question whether they are at a later evolutionary state or an intrinsically different population. The derived luminosities for host starlight and dust heated by star formation are converted to stellar masses and star-formation rates (SFR). The host-normalized SFR of the bulk of the 3CR sources is low when compared to other galaxy populations at the same epoch. Estimates of the dust mass yield a 1-100 times lower dust/stellar mass ratio than for the Milky Way, which indicates that these 3CR hosts have very low levels of interstellar matter and explains the low level of star formation. Less than 10% of the 3CR sources show levels of star formation above those of the main sequence of star-forming galaxies. C1 [Westhues, Christian; Haas, Martin; Chini, Rolf] Ruhr Univ Bochum, Astron Inst, Univ Str 150, D-44801 Bochum, Germany. [Barthel, Peter; Podigachoski, Pece] Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands. [Wilkes, Belinda J.; Willner, S. P.; Kuraszkiewicz, Joanna] Harvard Smithsonian Ctr Astrophys, Garden St 60, Cambridge, MA 02138 USA. [Leipski, Christian; Meisenheimer, Klaus] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Siebenmorgen, Ralf] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Chini, Rolf] Univ Catolica Norte, Inst Astron, Ave Angamos 0610,Casilla 1280, Antofagasta, Chile. RP Westhues, C (reprint author), Ruhr Univ Bochum, Astron Inst, Univ Str 150, D-44801 Bochum, Germany. EM christian.westhues@astro.rub.de OI Westhues, Christian/0000-0002-2414-6210; Podigachoski, Pece/0000-0003-3836-710X FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA); NASA; National Aeronautics and Space Administration; National Science Foundation; Alfred P. Sloan Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; University of Chicago; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Korean Scientist Group; Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington; Nordrhein-Westfalische Akademie der Wissenschaften und der Kunste in the framework of the academy program of the Federal Republic of Germany; state Nordrhein-Westfalen; Deutsches Zentrum fur Luft- und Raumfahrt [DLR 50 OR 1106] FX PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); and IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain).; SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, 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).; This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA.; This publication makes use of data products from the Widefield Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.; 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.; Funding for the creation and distribution of the SDSS Archive has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society.; The SDSS Web site is http://www.sdss.org/ The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, the Korean Scientist Group, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.; This work is supported by the Nordrhein-Westfalische Akademie der Wissenschaften und der Kunste in the framework of the academy program of the Federal Republic of Germany and the state Nordrhein-Westfalen, and by Deutsches Zentrum fur Luft- und Raumfahrt (DLR 50 OR 1106). NR 140 TC 3 Z9 3 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2016 VL 151 IS 5 AR 120 DI 10.3847/0004-6256/151/5/120 PG 53 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL4MH UT WOS:000375610400011 ER PT J AU Dauser, T Garcia, J Wilms, J AF Dauser, T. Garcia, J. Wilms, J. TI Relativistic reflection: Review and recent developments in modeling SO ASTRONOMISCHE NACHRICHTEN LA English DT Review DE accretion, accretion disks; black hole physics; line: profiles; X-rays: galaxies ID X-RAY REFLECTION; BLACK-HOLE SPIN; K-ALPHA LINE; ACCRETION DISK; IRON-K; XMM-NEWTON; CYGNUS X-1; SEYFERT-GALAXIES; COLD MATTER; GX 339-4 AB Measuring relativistic reflection is an important tool to study the innermost regions of the an accreting black hole system. In the following we present a brief review on the different aspects contributing to the relativistic reflection. The combined approach is for the first time incorporated in the new "relxill" model. The advantages of this more self-consistent approach are briefly summarized. A special focus is put on the new definition of the intrinsic reflection fraction in the lamp post geometry, which allows to draw conclusions about the primary source of radiation in these system. Additionally the influence of the high energy cutoff of the primary source on the reflection spectrum is motivated, revealing the remarkable capabilities of constraining E-cut by measuring relativistic reflection spectra from NuSTAR, preferably with lower energy coverage. (C) 2016 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim C1 [Dauser, T.; Wilms, J.] Dr Karl Remeis Observ & Erlangen Ctr Astroparticl, Sternwartstr 7, D-96049 Bamberg, Germany. [Garcia, J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Dauser, T (reprint author), Dr Karl Remeis Observ & Erlangen Ctr Astroparticl, Sternwartstr 7, D-96049 Bamberg, Germany. EM thomas.dauser@fau.de RI Wilms, Joern/C-8116-2013 OI Wilms, Joern/0000-0003-2065-5410 NR 53 TC 0 Z9 0 U1 1 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 MAY PY 2016 VL 337 IS 4-5 BP 362 EP 367 DI 10.1002/asna.201612314 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6CJ UT WOS:000375725600004 ER PT J AU McHardy, IM Connolly, SD Peterson, BM Bieryla, A Chand, H Elvis, MS Emmanoulopoulos, D Falco, E Gandhi, P Kaspi, S Latham, D Lira, P McCully, C Netzer, H Uemura, M AF McHardy, I. M. Connolly, S. D. Peterson, B. M. Bieryla, A. Chand, H. Elvis, M. S. Emmanoulopoulos, D. Falco, E. Gandhi, P. Kaspi, S. Latham, D. Lira, P. McCully, C. Netzer, H. Uemura, M. TI The origin of UV-optical variability in AGN and test of disc models: XMM-Newton and ground-based observations of NGC 4395 SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: active; galaxies: individual (NGC 4395, NGC 5548); galaxies: nuclei; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY VARIABILITY; BLACK-HOLE MASS; ACCRETION DISCS; SEYFERT-1 GALAXIES; MR 2251-178; LONG; MCG-6-30-15; EMISSION; NGC-4051 AB The origin of short timescale (weeks/months) variability of AGN, whether due to intrinsic disc variations or reprocessing of X-ray emission by a surrounding accretion disc, has been a puzzle for many years. However recently a number of observational programmes, particularly of NGC 5548 with Swift, have shown that the UV/optical variations lag behind the X-ray variations in a manner strongly supportive of X-ray reprocessing. Somewhat surprisingly, the implied size of the accretion disc is similar to 3 times greater than expected from a standard, smooth, Shakura-Sunyaev thin disc model. Although the difference may be explained by a clumpy accretion disc, it is not clear whether the difference will occur in all AGN or whether it may change as, eg, a function of black hole mass, accretion rate, or disc temperature. Measurements of interband lags for most AGN require long timescale monitoring, which is hard to arrange. However for low mass (<10(6) M-circle dot) AGN, the combination of XMM-Newton EPIC (X-rays) with the optical monitor in fast readout mode allows an X-ray/UV-optical lag to be measured within a single long observation. Here we summarise previous related observations and report on XMM-Newton observations of NGC 4395 (mass 100 times lower, accretion rate similar to 20 times lower than for NGC 5548). We find that the UVW1 lags the X-rays by similar to 470 s. Simultaneous observations at 6 different ground based observatories also allowed the g-band lag (similar to 800 s) to be measured. These observations are in agreement with X-ray reprocessing but initial analysis suggests that, for NGC 4395, they do not differ markedly from the predictions of the standard thin disc model. (C) 2016 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim C1 [McHardy, I. M.; Connolly, S. D.; Emmanoulopoulos, D.; Gandhi, P.] Univ Southampton, Dept Phys & Astron, Univ Rd, Southampton SO17 1BJ, Hants, England. [Peterson, B. M.] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA. [Bieryla, A.; Elvis, M. S.; Falco, E.; Latham, D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Chand, H.] Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263002, India. [Kaspi, S.; Netzer, H.] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. [Kaspi, S.; Netzer, H.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Lira, P.] Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile. [McCully, C.] Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. [Uemura, M.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Kagamiyama 1-3-1, Hiroshima 7398526, Japan. RP McHardy, IM (reprint author), Univ Southampton, Dept Phys & Astron, Univ Rd, Southampton SO17 1BJ, Hants, England. EM imh@soton.ac.uk FU STFC [ST/M001326/1] FX We thank the XMM-Newton operations team for considerable advice and assistance in setting up the observations of NGC4395. We also thank the staff and observers at the McDonald, FLWO, Haleakala, Kanata, Aries, and Wise observatories. IMcH thanks STFC for support under grant ST/M001326/1. NR 33 TC 5 Z9 5 U1 1 U2 3 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 MAY PY 2016 VL 337 IS 4-5 BP 500 EP 506 DI 10.1002/asna.201612337 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6CJ UT WOS:000375725600027 ER PT J AU Roberts, TP Middleton, MJ Sutton, AD Mezcua, M Walton, DJ Heil, LM AF Roberts, T. P. Middleton, M. J. Sutton, A. D. Mezcua, M. Walton, D. J. Heil, L. M. TI ULX behaviour: The ultraluminous state, winds and interesting anomalies SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE accretion, accretion disks; black hole physics; X-rays: binaries ID X-RAY SOURCES; MASS BLACK-HOLE; NGC 5408 X-1; SUPER-EDDINGTON ACCRETION; XMM-NEWTON OBSERVATIONS; HOLMBERG IX X-1; FUNDAMENTAL PLANE; SOLAR MASSES; BROAD-BAND; ESO 243-49 AB Recent evidence - in particular the hard X-ray spectra obtained by NuSTAR, and the large amplitude hard X-ray variability observed when ULXs show soft spectra - reveals that common ultraluminous X-ray source (ULX) behaviour is inconsistent with known sub-Eddington accretion modes, as would be expected for an intermediate-mass black hole (IMBH). Instead, it appears that the majority of ULXs are powered by super-Eddington accretion onto stellar-mass black holes. Here, we will review work that delves deeper into ULX spectral-timing behaviour, demonstrating it remains consistent with the expectations of super-Eddington accretion. One critical missing piece from this picture is the direct detection of the massive, radiatively-driven winds expected from ULXs as atomic emission/absorption line features in ULX spectra; we will show it is very likely these have already been detected as residuals in the soft X-ray spectra of ULXs. Finally, we will discuss ULXs that do not appear to conform to the emerging ULX behaviour patterns. In particular we discuss the implications of the identification of a good IMBH candidate as a background QSO; and the confirmation of an IMBH/ULX candidate in the galaxy NGC 2276 via the radio/X-ray fundamental plane. (C) 2016 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim C1 [Roberts, T. P.] Univ Durham, Ctr Extragalact Astron, Dept Phys, S Rd, Durham DH1 3LE, England. [Middleton, M. J.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Sutton, A. D.] NASA, George C Marshall Space Flight Ctr, Astrophys Off, ZP12, Huntsville, AL 35812 USA. [Mezcua, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Walton, D. J.] NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Walton, D. J.] CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA. [Heil, L. M.] Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. RP Roberts, TP (reprint author), Univ Durham, Ctr Extragalact Astron, Dept Phys, S Rd, Durham DH1 3LE, England. EM t.p.roberts@durham.ac.uk FU STFC [ST/L00075X/1]; NASA Chandra Grant [G05-16099X] FX TPR acknowledges support from STFC as part of the consolidated grant ST/L00075X/1. MM acknowledges financial support from NASA Chandra Grant G05-16099X. All data used is, or will be, public in the relevant mission archives. NR 42 TC 1 Z9 1 U1 1 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 MAY PY 2016 VL 337 IS 4-5 BP 534 EP 540 DI 10.1002/asna.201612343 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL6CJ UT WOS:000375725600033 ER PT J AU Jezkova, T Jaeger, JR Olah-Hemmings, V Jones, KB Lara-Resendiz, RA Mulcahy, DG Riddle, BR AF Jezkova, Tereza Jaeger, Jef R. Olah-Hemmings, Viktoria Jones, K. Bruce Lara-Resendiz, Rafael A. Mulcahy, Daniel G. Riddle, Brett R. TI Range and niche shifts in response to past climate change in the desert horned lizard Phrynosoma platyrhinos SO ECOGRAPHY LA English DT Article ID LAST GLACIAL MAXIMUM; LATE QUATERNARY; HALOTYDEUS-DESTRUCTOR; GENETIC CONSEQUENCES; GREAT-BASIN; ICE AGES; EVOLUTION; CONSERVATISM; ECOLOGY; MODELS AB During climate change, species are often assumed to shift their geographic distributions (geographic ranges) in order to track environmental conditions - niches - to which they are adapted. Recent work, however, suggests that the niches do not always remain conserved during climate change but shift instead, allowing populations to persist in place or expand into new areas. We assessed the extent of range and niche shifts in response to the warming climate after the Last Glacial Maximum (LGM) in the desert horned lizard Phrynosoma platyrhinos, a species occupying the western deserts of North America. We used a phylogeographic approach with mitochondrial DNA sequences to approximate the species range during the LGM by identifying populations that exhibit a genetic signal of population stability versus those that exhibit a signal of a recent (likely post-LGM) geographic expansion. We then compared the climatic niche that the species occupies today with the niche it occupied during the LGM using two models of simulated LGM climate. The genetic analyses indicated that P. platyrhinos persisted within the southern Mojave and Sonoran deserts throughout the latest glacial period and expanded from these deserts northwards, into the western and eastern Great Basin, after the LGM. The climatic niche comparisons revealed that P. platyrhinos expanded its climatic niche after the LGM towards novel, warmer and drier climates that allowed it to persist within the southern deserts. Simultaneously, the species shifted its climatic niche towards greater temperature and precipitation fluctuations after the LGM. We concluded that climatic changes at the end of the LGM promoted both range and niche shifts in this lizard. The mechanism that allowed the species to shift its niche remains unknown, but phenotypic plasticity likely contributes to the species ability to adjust to climate change. C1 [Jezkova, Tereza; Jaeger, Jef R.; Olah-Hemmings, Viktoria; Riddle, Brett R.] Univ Nevada, Sch Life Sci, 4505 South Maryland Pkwy, Las Vegas, NV 89154 USA. [Jezkova, Tereza] Univ Arizona, Dept Ecol & Evolutionary Biol, POB 210088, Tucson, AZ 85721 USA. [Jones, K. Bruce] Desert Res Inst, Div Earth & Ecosyst Sci, 755 East Flamingo Rd, Las Vegas, NV 89119 USA. [Lara-Resendiz, Rafael A.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, 1156 High St, Santa Cruz, CA 95064 USA. [Mulcahy, Daniel G.] Smithsonian Inst, POB 37012,MRC 162, Washington, DC 20013 USA. RP Jezkova, T (reprint author), Univ Nevada, Sch Life Sci, 4505 South Maryland Pkwy, Las Vegas, NV 89154 USA.; Jezkova, T (reprint author), Univ Arizona, Dept Ecol & Evolutionary Biol, POB 210088, Tucson, AZ 85721 USA. EM tjezkova@email.arizona.edu FU Univ. of Nevada; Las Vegas (UNLV) President's Research Award; EPSCoR ACES Grant SFFA [UCCSN 02-123]; Major Research Instrumentation Grant [DBI-0421519]; NIH IRACDA PERT fellowship through the Center for Insect Science at the Univ. of Arizona [K12 GM000708] FX We thank Aaron Ambos, Akira, Matthew Graham, and Randy English for help with sampling; Museum of Vertebrate Zoology, Univ. of California, Berkeley and California Academy of Sciences for loaning of tissue samples; Robert Hijmans, Beth Shapiro, Simon Ho, John McCormack, Eric Waltari, and Robert Boria for valuable advice and information; the Laboratoire des Sciences du Climat et de l'Environnement for collecting and archiving the model data. We thank Kenneth Kozak, Rocky Ward, John Klicka, Mallory Eckstut, Matthew Graham, and Derek Houston for valuable comments on the earlier versions of the manuscript. This work was supported by the Univ. of Nevada, Las Vegas (UNLV) President's Research Award to BRR, JRJ, and TJ, EPSCoR ACES Grant SFFA UCCSN 02-123 to TJ, Major Research Instrumentation Grant DBI-0421519 to UNLV, and an NIH IRACDA PERT fellowship through the Center for Insect Science (K12 GM000708) at the Univ. of Arizona to TJ. NR 84 TC 3 Z9 3 U1 22 U2 41 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0906-7590 EI 1600-0587 J9 ECOGRAPHY JI Ecography PD MAY PY 2016 VL 39 IS 5 BP 437 EP 448 DI 10.1111/ecog.01464 PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA DL4JU UT WOS:000375601700004 PM 27231410 ER PT J AU Fung, T O'Dwyer, JP Rahman, KA Fletcher, CD Chisholm, RA AF Fung, Tak O'Dwyer, James P. Rahman, Kassim Abd. Fletcher, Christine D. Chisholm, Ryan A. TI Reproducing static and dynamic biodiversity patterns in tropical forests: the critical role of environmental variance SO ECOLOGY LA English DT Article DE demographic variance; dynamic model; environmental variance; neutral theory; species-abundance distributions; tropical forests ID RELATIVE SPECIES ABUNDANCE; RAIN-FOREST; NEUTRAL THEORY; ECOLOGICAL COMMUNITIES; EXTINCTION RISK; POPULATION; STOCHASTICITY; TREE; DIVERSITY; MODELS AB Ecological communities are subjected to stochasticity in the form of demographic and environmental variance. Stochastic models that contain only demographic variance (neutral models) provide close quantitative fits to observed species-abundance distributions (SADs) but substantially underestimate observed temporal species-abundance fluctuations. To provide a holistic assessment of whether models with demographic and environmental variance perform better than neutral models, the fit of both to SADs and temporal species-abundance fluctuations at the same time has to be tested quantitatively. In this study, we quantitatively test how closely a model with demographic and environmental variance reproduces total numbers of species, total abundances, SADs and temporal species-abundance fluctuations for two tropical forest tree communities, using decadal data from long-term monitoring plots and considering individuals larger than two size thresholds for each community. We find that the model can indeed closely reproduce these static and dynamic patterns of biodiversity in the two communities for the two size thresholds, with better overall fits than corresponding neutral models. Therefore, our results provide evidence that stochastic models incorporating demographic and environmental variance can simultaneously capture important static and dynamic biodiversity patterns arising in tropical forest communities. C1 [Fung, Tak; Chisholm, Ryan A.] Natl Univ Singapore, Dept Biol Sci, 14 Sci Dr 4, Singapore 117543, Singapore. [O'Dwyer, James P.] Univ Illinois, Sch Integrat Biol, Dept Plant Biol, 505 S Goodwin Ave, Urbana, IL 61801 USA. [Rahman, Kassim Abd.; Fletcher, Christine D.] Forest Res Inst Malaysia, Kepong 52109, Selangor Darul, Malaysia. [Chisholm, Ryan A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Fung, T (reprint author), Natl Univ Singapore, Dept Biol Sci, 14 Sci Dr 4, Singapore 117543, Singapore. EM tfung2000@gmail.com FU National University of Singapore [WBS R-154-000-603-112, R-154-000-560-651]; Templeton World Charity Foundation [TWCF0079/AB47] FX This work was generated using data from the Center for Tropical Forest Science/Smithsonian Institution Global Earth Observatory network. The authors would like to thank Forest Research Institute of Malaysia for managing the Pasoh 50-ha demography plot. The authors would also like to thank Stuart Davies, Richard Condit, and Felix Lim for helpful discussion on the manuscript. In addition, we thank two anonymous reviewers whose comments have resulted in substantial improvements to this study. T. Fung and R. A. Chisholm are supported by the National University of Singapore grants WBS R-154-000-603-112 and R-154-000-560-651. J. P. O'Dwyer acknowledges support from the Templeton World Charity Foundation grant TWCF0079/AB47. NR 60 TC 0 Z9 0 U1 4 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD MAY PY 2016 VL 97 IS 5 BP 1207 EP 1217 DI 10.1890/15-0984.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA DL3XL UT WOS:000375566800010 PM 27349097 ER PT J AU Rushing, CS Marra, PP Dudash, MR AF Rushing, Clark S. Marra, Peter P. Dudash, Michele R. TI Winter habitat quality but not long-distance dispersal influences apparent reproductive success in a migratory bird SO ECOLOGY LA English DT Article DE Aster models; breeding dispersal; carry-over effects; deuterium; long-distance dispersal; natal dispersal; seasonal interactions ID REDSTARTS SETOPHAGA RUTICILLA; GREAT REED WARBLERS; NATAL DISPERSAL; NONBREEDING SEASON; AMERICAN REDSTARTS; BREEDING DISPERSAL; CLIMATE-CHANGE; ARRIVAL DATE; POPULATION; CONSEQUENCES AB Long-distance breeding and natal dispersal play central roles in many ecological and evolutionary processes, including gene flow, population dynamics, range expansion, and individual responses to fluctuating biotic and abiotic conditions. However, the relative contribution of long-distance dispersal to these processes depends on the ability of dispersing individuals to successfully reproduce in their new environment. Unfortunately, due to the difficulties associated with tracking dispersal in the field, relatively little is known about its reproductive consequences. Furthermore, because reproductive success is influenced by a variety of processes, disentangling the influence of each of these processes is critical to understanding the direct consequences of dispersal. In this study, we used stable hydrogen and carbon isotopes to estimate long-distance dispersal and winter territory quality in a migratory bird, the American Redstart (Setophaga ruticilla). We then applied Aster life-history models to quantify the strength of influence of these factors on apparent reproductive success. We found no evidence that male or female reproductive success was lower for long-distance dispersers relative to non-dispersing individuals. In contrast, carry-over effects from the winter season did influence male, but not female, reproductive success. Use of Aster models further revealed that for adult males, winter territory quality influenced the number of offspring produced whereas for yearling males, high-quality winter territories were associated with higher mating and nesting success. These results suggest that although long-distance natal and breeding dispersal carry no immediate reproductive cost for American Redstarts, reproductive success in this species may ultimately be limited by the quality of winter habitat. C1 [Rushing, Clark S.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20013 USA. [Rushing, Clark S.; Dudash, Michele R.] Univ Maryland, Dept Biol, Grad Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA. RP Rushing, CS (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20013 USA.; Rushing, CS (reprint author), Univ Maryland, Dept Biol, Grad Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA. EM rushingc@si.edu FU COSMOS Foundation; American Ornithologists Union; Washington Biologists Field Club; Maryland Ornithological Society; National Science Foundation; BEES/BISI program; University of Maryland; Smithsonian Institution FX Funding was provided by the COSMOS Foundation, the American Ornithologists Union, the Washington Biologists Field Club, the Maryland Ornithological Society and the National Science Foundation. C. S. Rushing was supported by the BEES/BISI program, a Wiley Dissertation Fellowship from the University of Maryland, and a Smithsonian Institution Pre-doctoral fellowship. We thank C. Fenster, C. Geyer, and R. Reynolds for statistical help and comments from S. Sillett, W. Fagan, D. Gruner, D. Hawthorne, W. Koenig, and two anonymous reviewers. NR 49 TC 0 Z9 0 U1 21 U2 31 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD MAY PY 2016 VL 97 IS 5 BP 1218 EP 1227 DI 10.1890/15-1259.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA DL3XL UT WOS:000375566800011 PM 27349098 ER PT J AU Zhang, KM Shen, Y Zhou, XQ Fang, YM Liu, Y Ma, LQ AF Zhang, Kai-Mei Shen, Yu Zhou, Xiao-Qi Fang, Yan-Ming Liu, Ying Ma, Lena Q. TI Photosynthetic electron-transfer reactions in the gametophyte of Pteris multifida reveal the presence of allelopathic interference from the invasive plant species Bidens pilosa SO JOURNAL OF PHOTOCHEMISTRY AND PHOTOBIOLOGY B-BIOLOGY LA English DT Article DE Pteris multifida; Gametophyte; Bidens pilosa; Coreopsis basalis; Photosynthesis; Allelopathy ID AGERATINA-ADENOPHORA; ENERGY-DISSIPATION; SPORE GERMINATION; STRESS; PHOTOINHIBITION; INHIBITION; ROOT; L. AB To date, the response of the fern gametophyte to its environment has received considerable attention. However, studies on the influence of plant invasion on the fern gametophyte are fewer. Allelopathy has been hypothesized to play an important role in biological invasion. Hence, it is necessary to study the allelopathy of invasive plant species to the fern gametophyte and elucidate the mechanisms by which invasive plants cause phytotoxicity. As one of the main invasive plants in China, Bidens pilosa exhibits allelopathic effects on the gametophytic growth of Pteris multifida. The root exudate plays an important role among various allelochemical delivery mechanisms in B. pilosa. The effect invasive plant species has on photosynthesis in native species is poorly understood. To elucidate this effect, the changes in photosynthesis in the gametophytes of P. multifida are analyzed to examine the mechanisms of the root exudates of B. pilosa. Meanwhile, a non-invasive plant, Coreopsis basalis, was also applied to investigate the effects on fluorescence and pigments in P. multifida gametophytes. We found that gametophytes exposed to both B. pilosa and C. basalis had decreased fluorescence parameters in comparison with the control, except for non-photochemical quenching. Furthermore, it was found that these parameters were markedly affected from day 2 to day 10 in the presence of both exudates at a concentration of 25% or above. B. pilosa exudate had a negative dose-dependent effect on chlorophyll a, chlorophyll b, carotenoid, and the total chlorophyll in the gametophyte. The inhibitory effects increased with increasing exudate concentrations of both species, exhibiting the greatest inhibition at day 10. In conclusion, B. pilosa irreversibly affected the photosynthesis of P. mutt-Oda on both PS I and PS II. Root exudates caused the primary damage with respect to the decrease of the acceptors and donors of photon and electron in photosynthetic units and the production and the relative yield of photochemical quantum in PS II. With the effects of exudates, part of the energy is released as heat in chloroplasts. The comparison of invasive and non-invasive plants in allelopathic experiments demonstrated that invasive plants were responsible for the critical damage to the photosynthetic process in local species. (C) 2016 Elsevier B.V. All rights reserved. C1 [Zhang, Kai-Mei; Fang, Yan-Ming; Liu, Ying] Nanjing Forestry Univ, Coinnovat Ctr Sustainable Forestry Southern China, Nanjing 210037, Jiangsu, Peoples R China. [Zhang, Kai-Mei; Shen, Yu; Fang, Yan-Ming; Liu, Ying] Nanjing Forestry Univ, Coll Biol & Environm, Nanjing 210037, Jiangsu, Peoples R China. [Zhang, Kai-Mei] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Shen, Yu] Nanjing Agr Univ, Coll Resources & Environm Sci, Nanjing 210095, Jiangsu, Peoples R China. [Zhou, Xiao-Qi] Griffith Univ, Environm Futures Res Inst, Nathan, Qld 4111, Australia. [Ma, Lena Q.] Nanjing Univ, Sch Environm, State Key Lab Pollut Control & Resource Reuse, Nanjing 210046, Jiangsu, Peoples R China. [Ma, Lena Q.] Univ Florida, Soil & Water Sci Dept, Gainesville, FL 32611 USA. RP Fang, YM (reprint author), Nanjing Forestry Univ, Coinnovat Ctr Sustainable Forestry Southern China, Nanjing 210037, Jiangsu, Peoples R China. EM jwu4@njfu.edu.cn RI Ma, Lena/E-5854-2010 OI Ma, Lena/0000-0002-8463-9957 FU National Natural Science Foundation of China [31200233]; Priority Academic Program Development of Jiangsu Higher Education Institutions (PAPD); Collaborative Innovation Plan of Jiangsu Higher Education; Jiangsu Government; Laboratory of Analytical Biology of the National Museum of Natural History; Laboratory of Analytical Biology of the Smithsonian Institution FX This work was supported by the National Natural Science Foundation of China (31200233), the Priority Academic Program Development of Jiangsu Higher Education Institutions (PAPD), Collaborative Innovation Plan of Jiangsu Higher Education, the Jiangsu Government Scholarship for Overseas Studies and the Laboratories of Analytical Biology of the National Museum of Natural History, the Smithsonian Institution. NR 32 TC 1 Z9 1 U1 9 U2 16 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 1011-1344 J9 J PHOTOCH PHOTOBIO B JI J. Photochem. Photobiol. B-Biol. PD MAY PY 2016 VL 158 BP 81 EP 88 DI 10.1016/j.jphotobiol.2016.02.026 PG 8 WC Biochemistry & Molecular Biology; Biophysics SC Biochemistry & Molecular Biology; Biophysics GA DL2XZ UT WOS:000375499800010 PM 26954232 ER PT J AU Moreno-Bernal, JW Head, J Jaramillo, CA AF Moreno-Bernal, Jorge W. Head, Jason Jaramillo, Carlos A. TI Fossil Crocodilians from the High Guajira Peninsula of Colombia: Neogene faunal change in northernmost South America SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID MIOCENE URUMACO FORMATION; PHYLOGENETIC-RELATIONSHIPS; LOWER PALEOCENE; NORTH-AMERICA; LOWER EOCENE; CROCODYLIA; MORPHOLOGY; VENEZUELA; HISTORY; ORGANS AB The La Guajira Peninsula, Colombia, has a continuous vertebrate fossil record that includes both the late early-early middle Miocene and the Pliocene. Crocodilians from the early to early middle Miocene Jimol and Castilletes formations include gavialoids, recovered from both coastal and shallow marine deposits, and caimanines representing early records of the specialized caimanine taxa Purussaurus and Mourasuchus. Crocodyloid specimens from the Pliocene Ware Formation are assigned to Crocodylus and represent one of the oldest occurrences of the genus in the New World. Records from the La Guajira Peninsula suggest that diverse crocodilian assemblages were already established by the late early Miocene, including several widely distributed lineages that persisted for several million years. Crocodylus is a recent immigrant to South America that occupied habitats left vacant by the extinction of several crocodilian lineages.Citation for this article: Moreno-Bernal, J. W., J. Head, and C. A. Jaramillo. 2016. Fossil crocodilians from the High Guajira Peninsula of Colombia: Neogene faunal change in northernmost South America. Journal of Vertebrate Paleontology. DOI: 10.1080/02724634.2016.1110586. C1 [Moreno-Bernal, Jorge W.; Head, Jason] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA. [Moreno-Bernal, Jorge W.; Jaramillo, Carlos A.] Smithsonian Inst, Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Box 0843-03092, Ancon, Panama. RP Moreno-Bernal, JW (reprint author), Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA.; Moreno-Bernal, JW (reprint author), Smithsonian Inst, Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Box 0843-03092, Ancon, Panama. EM jwmorenob@huskers.unl.edu; jhead2@unl.edu; jaramilloc@si.edu OI Head, Jason/0000-0002-2237-6901 FU Friends of the University of Nebraska State Museum Graduate Student Research Grant (University of Nebraska State Museum); Doris O. and Samuel P. Welles Research Fund (University of California Museum of Paleontology); Smithsonian Institution; National Geographic Society; Anders Foundation; Gregory D. and Jennifer Walston Johnson; Universidad del Norte; University of Zurich; National Science Foundation [EAR 0957679] FX This research formed a component of J.W.M.-B.'s M.S. thesis in the department of Earth and Atmospheric Sciences at the University of Nebraska-Lincoln. We thank J. D. Carrillo, G. Ballen, M. C. Vallejo, and V. Zapata for helping to collect specimens. L. Jimenez helped with the preparation of several specimens in STRI. G. Brown and R. Skolnick (University of Nebraska State Museum, Lincoln, Nebraska) provided assistance for additional preparation of specimens. We thank R. Secord and D. Watkins (University of Nebraska-Lincoln) for discussion, and F. Moreno (University of Rochester, Rochester, New York) and A. Hendy (Florida Museum of Natural History, Gainesville, Florida) for useful comments on the stratigraphy and geochronology of the Cocinetas Basin. For access to comparative specimens, we thank T. Labedtz (University of Nebraska State Museum), P. A. Holroyd (University of California Museum of Paleontology, Berkeley, California), A. Resetar (Field Museum of Natural History, Chicago, Illinois), and M. Calderon (Instituto de Ciencias Naturales, Bogota, Columbia). Research was funded in part by the Friends of the University of Nebraska State Museum Graduate Student Research Grant (University of Nebraska State Museum) and the Doris O. and Samuel P. Welles Research Fund (University of California Museum of Paleontology). The Smithsonian Institution, the National Geographic Society, the Anders Foundation, Gregory D. and Jennifer Walston Johnson, Universidad del Norte, the University of Zurich, and the National Science Foundation (grant EAR 0957679) helped to support this work. Thanks to the communities of Warpana, Patajau, Aulechit, Nazareth, Wososopo, Sillamana, Paraguachon, La Flor de la Guajira, and Ipapura. Thanks to the Colombian National Police (Castilletes base) and the Colombian Army (La Flor de la Guajira and Cerro de la Teta). We express special thanks to our drivers, Grillo, Lalo, and Medardo. NR 85 TC 4 Z9 4 U1 3 U2 3 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD MAY PY 2016 VL 36 IS 3 AR e1110586 DI 10.1080/02724634.2016.1110586 PG 17 WC Paleontology SC Paleontology GA DJ9UG UT WOS:000374557800017 ER PT J AU Worrall, DM Birkinshaw, M Young, AJ AF Worrall, D. M. Birkinshaw, M. Young, A. J. TI X-rays associated with the jet cloud-interacting radio galaxy 3C 277.3 (Coma A): implications for energy deposition SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: individual: (3C 277.3, Coma A); galaxies: ISM; galaxies: jets; radio continuum: galaxies; X-rays: galaxies ID HUBBLE-SPACE-TELESCOPE; OPTICAL SPECTROSCOPIC SURVEY; ACTIVE GALACTIC NUCLEI; HOT-SPOTS; CHANDRA OBSERVATIONS; SNAPSHOT SURVEY; XMM-NEWTON; SKY-SURVEY; B2 SAMPLE; EMISSION AB We report the discovery with Chandra of X-ray-emitting gas associated with the jet cloud interaction in the radio galaxy 3C 277.3 (Coma A), a source that falls in the most important power range for radio-mode feedback in the Universe. This hot gas, heated by the jet, dominates the mass of the cloud which is responsible for an extreme projected deflection of the kpc-scale radio jet. Highly absorbed X-ray emission from the nucleus of 3C 277.3 confirms that the jet lies close to the plane of the sky and so has a large intrinsic deflection. We detect group gas on the scale of the radio lobes, and see X-ray cavities coincident with the brightest radio emission, with the lobes embraced by X-ray enhancements that we argue are the result of shocks. The anti-correlation between the locations of X-ray arms and H a-emitting filaments that are believed to have originated from a merger with one or more gas-rich galaxies suggests that shocks advancing around the lobe are inhibited by the dense colder material. Synchrotron X-ray emission is detected from the upstream edge of a second bright radio knot. X-rays are also detected from the location where an undetected counterjet enters the northern radio hotspot. We suggest that these X-rays are synchrotron radiation from a shock in a small-scale sub-structure. C1 [Worrall, D. M.; Birkinshaw, M.; Young, A. J.] Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England. [Worrall, D. M.; Birkinshaw, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Worrall, DM (reprint author), Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England.; Worrall, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM d.worrall@bristol.ac.uk NR 53 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2016 VL 458 IS 1 BP 174 EP 183 DI 10.1093/mnras/stw277 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ9YI UT WOS:000374568900009 ER PT J AU Dasadia, S Sun, M Morandi, A Sarazin, C Clarke, T Nulsen, P Massaro, F Roediger, E Harris, D Forman, B AF Dasadia, Sarthak Sun, Ming Morandi, Andrea Sarazin, Craig Clarke, Tracy Nulsen, Paul Massaro, Francesco Roediger, Elke Harris, Dan Forman, Bill TI Shocking features in the merging galaxy cluster RXJ0334.2-0111 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: individual: RXJ0334.2-0111; galaxies: clusters: individual: 3C89; galaxies: clusters: intracluster medium; galaxies: jets; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATION; FLUX-LIMITED SAMPLE; TAIL RADIO-SOURCES; X-RAY; COOLING FLOWS; BOW SHOCK; OBSERVATIONAL EVIDENCE; CHANDRA OBSERVATION; EMISSION-LINE AB We present a 66 ks Chandra X-ray observation of the galaxy cluster RXJ0334.2-0111. This deep observation revealed a unique bow shock system associated with a wide angle tail (WAT) radio galaxy and several intriguing substructures. The temperature across the bow shock jumps by a factor of similar to 1.5 (from 4.1 to 6.2 keV), and is consistent with the Mach number M = 1.6(-0.3)(+0.5). A second inner surface brightness edge is a cold front that marks the border between infalling subcluster cool core and the intracluster medium of the main cluster. The temperature across the cold front increases from 1.3(-0.8)(+0.3) to 6.2(-0.6)(+0.6) keV. We find an overpressurized region similar to 250 kpc east of the cold front that is named 'the eastern extension (EE)'. The EE may be a part of the third subcluster in the ongoing merger. We also find a tail shaped feature that originates near the bow shock and may extend up to a distance of similar to 1 Mpc. This feature is also likely overpressurized. The luminous FR-I radio galaxy, 3C89, appears to be the cD galaxy of the infalling subcluster. We estimated 3C89's jet power from jet bending and the possible interaction between the X-ray gas and the radio lobes. A comparison between the shock standoff distance and the Mach number for all known shock front/cold front combinations suggests that the core is continuously shrinking in size by stripping. C1 [Dasadia, Sarthak; Sun, Ming; Morandi, Andrea] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Sarazin, Craig] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Clarke, Tracy] Naval Res Lab, Washington, DC 20375 USA. [Nulsen, Paul] Univ Western Australia, ICRAR, 35 Stirling Hwy, Crawley, WA 6009, Australia. [Massaro, Francesco] Univ Turin, I-10125 Turin, Italy. [Roediger, Elke] Univ Hull, Dept Math & Phys, EA Milne Ctr Astrophys, Kingston Upon Hull HU6 7RX, N Humberside, England. [Harris, Dan; Forman, Bill] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Dasadia, S (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. EM sbd0002@uah.edu RI Massaro, Francesco/L-9102-2016; OI Massaro, Francesco/0000-0002-1704-9850; Morandi, Andrea/0000-0002-5575-3056; Nulsen, Paul/0000-0003-0297-4493 FU National Aeronautics and Space Administration (NASA) [GO2-13160A, GO2-13102A]; NASA [NAS8-03060]; NASA ADAP award [NNX14AI29G]; 6.1 Base funding FX We thank Maxim Markevitch and Marios Chatzikos for discussion and comments. Support for this work was provided by the National Aeronautics and Space Administration (NASA) through Chandra Award GO2-13160A and GO2-13102A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the NASA under contract NAS8-03060. This work was also supported in part by the NASA ADAP award NNX14AI29G. Basic research in radio astronomy at the Naval Research Laboratory is supported by 6.1 Base funding. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. The NRAO VLA Archive Survey image was produced as part of the NRAO VLA Archive Survey, (c) AUI/NRAO. NR 68 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 MAY 1 PY 2016 VL 458 IS 1 BP 681 EP 694 DI 10.1093/mnras/stw291 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ9YI UT WOS:000374568900045 ER PT J AU Hallakoun, N Maoz, D Kilic, M Mazeh, T Gianninas, A Agol, E Bell, KJ Bloemen, S Brown, WR Debes, J Faigler, S Kull, I Kupfer, T Loeb, A Morris, BM Mullally, F AF Hallakoun, N. Maoz, D. Kilic, M. Mazeh, T. Gianninas, A. Agol, E. Bell, K. J. Bloemen, S. Brown, W. R. Debes, J. Faigler, S. Kull, I. Kupfer, T. Loeb, A. Morris, B. M. Mullally, F. TI SDSS J1152+0248: an eclipsing double white dwarf from the Kepler K2 campaign SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; techniques: radial velocities; binaries: eclipsing; stars: individual: SDSS J115219.99+024814.4; white dwarfs ID BINARY NLTT 11748; SUBDWARF-B-STARS; SPECTROSCOPIC ANALYSIS; CSS 41177; HELIUM; COEFFICIENTS; CONSTRAINTS; PROGENITORS; SUPERNOVAE; EVOLUTION AB We report the discovery of the sixth known eclipsing double white dwarf (WD) system, SDSS J1152+0248, with a 2.3968 +/- 0.0003 h orbital period, in data from the Kepler Mission's K2 continuation. Analysing and modelling the K2 data together with ground-based fast photometry, spectroscopy, and radial-velocity measurements, we determine that the primary is a DA-type WD with mass M-1 = 0.47 +/- 0.11M(circle dot), radius R-1 = 0.0197 +/- 0.0035 R-circle dot, and cooling age t(1) = 52 +/- 36 Myr. No lines are detected, to within our sensitivity, from the secondary WD, but it is likely also of type DA. Its central surface brightness, as measured from the secondary eclipse, is 0.31 of the primary's surface brightness. Its mass, radius, and cooling age, respectively, are M-2 = 0.44 +/- 0.09M(circle dot), R-2 = 0.0223(-0.0050)(+0.0064) R-circle dot, and t(2) = 230 +/- 100 Myr. SDSS J1152+0248 is a near twin of the double-lined eclipsing WD system CSS 41177. C1 [Hallakoun, N.; Maoz, D.; Mazeh, T.; Faigler, S.; Kull, I.] Tel Aviv Univ, Sch Phys & Astron, IL-6997801 Tel Aviv, Israel. [Hallakoun, N.] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Kilic, M.; Gianninas, A.] Univ Oklahoma, Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. [Agol, E.; Morris, B. M.] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. [Bell, K. J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Bloemen, S.; Kupfer, T.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands. [Brown, W. R.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Debes, J.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Loeb, A.] Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA. [Mullally, F.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Hallakoun, N; Maoz, D (reprint author), Tel Aviv Univ, Sch Phys & Astron, IL-6997801 Tel Aviv, Israel.; Hallakoun, N (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM naama@wise.tau.ac.il; maoz@astro.tau.ac.il OI Morris, Brett/0000-0003-2528-3409; /0000-0002-0802-9145; Gianninas, Alexandros/0000-0002-8655-4308 FU I-CORE programme of the PBC [1829/12]; Israel Science Foundation; ISF; European Research Council under the EU's Seventh Framework Programme (FP7/ERC Grant) [291352]; NSF [AST-1312678]; NASA [NNX14AF65G]; Raymond and Beverly Sackler Tel-Aviv University - Harvard/ITC Astronomy Programme FX We thank Shai Kaspi for his help with the observations at the Wise Observatory. We are grateful for valuable comments by J. J. Hermes and by the anonymous referee. This work was supported in part by Grant 1829/12 of the I-CORE programme of the PBC and the Israel Science Foundation (DM and TM). DM and TM acknowledge further support by individual grants from the ISF. The research by TM leading to these results has received funding from the European Research Council under the EU's Seventh Framework Programme (FP7/(2007-2013)/ERC Grant Agreement No. 291352). MK, AG and KB gratefully acknowledge the support of the NSF under grant AST-1312678. MK and AG also acknowledge the support of NASA under grant NNX14AF65G. AL acknowledges support by the Raymond and Beverly Sackler Tel-Aviv University - Harvard/ITC Astronomy Programme. 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 de Canarias. The analysis presented in this paper is based on observations obtained with the Apache Point Observatory 3.5-metre telescope, which is owned and operated by the Astrophysical Research Consortium. This paper includes data taken at the McDonald Observatory of The University of Texas at Austin. The authors acknowledge the Texas Advanced Computing Center (TACC)5 at The University of Texas at Austin for providing data base resources that have contributed to the research results reported within this paper. NR 49 TC 4 Z9 4 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2016 VL 458 IS 1 BP 845 EP 854 DI 10.1093/mnras/stw364 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ9YI UT WOS:000374568900059 ER PT J AU Offringa, AR Trott, CM Hurley-Walker, N Johnston-Hollitt, M McKinley, B Barry, N Beardsley, AP Bowman, JD Briggs, F Carroll, P Dillon, JS Ewall-Wice, A Feng, L Gaensler, BM Greenhill, LJ Hazelton, BJ Hewitt, JN Jacobs, DC Kim, HS Kittiwisit, P Lenc, E Line, J Loeb, A Mitchell, DA Morales, MF Neben, AR Paul, S Pindor, B Pober, JC Procopio, P Riding, J Sethi, SK Shankar, NU Subrahmanyan, R Sullivan, IS Tegmark, M Thyagarajan, N Tingay, SJ Wayth, RB Webster, RL Wyithe, JSB AF Offringa, A. R. Trott, C. M. Hurley-Walker, N. Johnston-Hollitt, M. McKinley, B. Barry, N. Beardsley, A. P. Bowman, J. D. Briggs, F. Carroll, P. Dillon, J. S. Ewall-Wice, A. Feng, L. Gaensler, B. M. Greenhill, L. J. Hazelton, B. J. Hewitt, J. N. Jacobs, D. C. Kim, H. -S. Kittiwisit, P. Lenc, E. Line, J. Loeb, A. Mitchell, D. A. Morales, M. F. Neben, A. R. Paul, S. Pindor, B. Pober, J. C. Procopio, P. Riding, J. Sethi, S. K. Shankar, N. U. Subrahmanyan, R. Sullivan, I. S. Tegmark, M. Thyagarajan, N. Tingay, S. J. Wayth, R. B. Webster, R. L. Wyithe, J. S. B. TI Parametrizing Epoch of Reionization foregrounds: a deep survey of low-frequency point-source spectra with the Murchison Widefield Array SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: observational; techniques: interferometric; dark ages, reionization, first stars; radio continuum: general; radio lines: galaxies ID RADIO-TELESCOPE OBSERVATIONS; NORTH CELESTIAL POLE; I POWER SPECTRUM; 21 CM RADIATION; SIMILAR-TO 20; NGC 253; SUPERNOVA-REMNANTS; HYDROGEN REIONIZATION; RECOMBINATION LINES; LOFAR OBSERVATIONS AB Experiments that pursue detection of signals from the Epoch of Reionization (EoR) are relying on spectral smoothness of source spectra at low frequencies. This article empirically explores the effect of foreground spectra on EoR experiments by measuring high-resolution full-polarization spectra for the 586 brightest unresolved sources in one of the Murchison Widefield Array (MWA) EoR fields using 45 h of observation. A novel peeling scheme is used to subtract 2500 sources from the visibilities with ionospheric and beam corrections, resulting in the deepest, confusion-limited MWA image so far. The resulting spectra are found to be affected by instrumental effects, which limit the constraints that can be set on source-intrinsic spectral structure. The sensitivity and power-spectrum of the spectra are analysed, and it is found that the spectra of residuals are dominated by point spread function sidelobes from nearby undeconvolved sources. We release a catalogue describing the spectral parameters for each measured source. C1 [Offringa, A. R.] Netherlands Inst Radio Astron ASTRON, POB 2, NL-7990 AA Dwingeloo, Netherlands. [Trott, C. M.; Hurley-Walker, N.; Tingay, S. J.; Wayth, R. B.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Trott, C. M.; McKinley, B.; Briggs, F.; Gaensler, B. M.; Kim, H. -S.; Lenc, E.; Line, J.; Mitchell, D. A.; Pindor, B.; Procopio, P.; Riding, J.; Tingay, S. J.; Wayth, R. B.; Webster, R. L.; Wyithe, J. S. B.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, POB 600, Wellington 6140, New Zealand. [McKinley, B.; Kim, H. -S.; Line, J.; Pindor, B.; Procopio, P.; Riding, J.; Webster, R. L.; Wyithe, J. S. B.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Barry, N.; Carroll, P.; Hazelton, B. J.; Morales, M. F.; Sullivan, I. S.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Beardsley, A. P.; Bowman, J. D.; Jacobs, D. C.; Kittiwisit, P.; Thyagarajan, N.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Dillon, J. S.; Ewall-Wice, A.; Feng, L.; Hewitt, J. N.; Neben, A. R.; Tegmark, M.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Dillon, J. S.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Gaensler, B. M.; Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Gaensler, B. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Greenhill, L. J.; Loeb, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Mitchell, D. A.] CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia. [Paul, S.; Sethi, S. K.; Shankar, N. U.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Pober, J. C.] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Offringa, AR (reprint author), Netherlands Inst Radio Astron ASTRON, POB 2, NL-7990 AA Dwingeloo, Netherlands. EM offringa@gmail.com RI Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Sethi, Shiv/D-4893-2012; Subrahmanyan, Ravi/D-4889-2012; Udayashankar , N/D-4901-2012; OI Lenc, Emil/0000-0002-9994-1593; Wayth, Randall/0000-0002-6995-4131; Trott, Cathryn/0000-0001-6324-1766; Wyithe, Stuart/0000-0001-7956-9758; /0000-0002-0086-7363; Gaensler, Bryan/0000-0002-3382-9558 FU European Research Council under ERC [LOFARCORE - 339743]; Marsden Fund; Australian Research Council [DE140100316]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Australian Commonwealth Government; NVIDIA at Harvard University FX AO acknowledges financial support from the European Research Council under ERC Advanced Grant LOFARCORE - 339743. MJH acknowledges the support of the Marsden Fund. This research was supported under Australian Research Council's Discovery Early Career Researcher funding scheme (project number DE140100316) and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020).; This scientific work makes use of the NCI National Facility in Canberra, Australia, which is supported by the Australian Commonwealth Government.; 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 operation of the MWA is provided by the Australian Government Department of Industry and Science and Department of Education (National Collaborative Research Infrastructure Strategy: NCRIS), under a contract to Curtin University administered by Astronomy Australia Limited. We acknowledge the iVEC Petabyte Data Store and the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University. NR 71 TC 10 Z9 10 U1 2 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 MAY 1 PY 2016 VL 458 IS 1 BP 1057 EP 1070 DI 10.1093/mnras/stw310 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ9YI UT WOS:000374568900072 ER PT J AU Gonzalez-Rivero, M Bozec, YM Chollett, I Ferrari, R Schonberg, CHL Mumby, PJ AF Gonzalez-Rivero, Manuel Bozec, Yves-Marie Chollett, Iliana Ferrari, Renata Schoenberg, Christine H. L. Mumby, Peter J. TI Asymmetric competition prevents the outbreak of an opportunistic species after coral reef degradation SO OECOLOGIA LA English DT Article DE Disturbance; Population regulation; Transient ecosystems; Marine ecosystems; Porifera ID EXCAVATING SPONGE; LIFE-HISTORY; LONG-TERM; INTERSPECIFIC COMPETITION; SCLERACTINIAN CORALS; POPULATION-DYNAMICS; FIELD EXPERIMENTS; CARIBBEAN CORALS; PHASE-SHIFTS; GROWTH AB Disturbance releases space and allows the growth of opportunistic species, excluded by the old stands, with a potential to alter community dynamics. In coral reefs, abundances of fast-growing, and disturbance-tolerant sponges are expected to increase and dominate as space becomes available following acute coral mortality events. Yet, an increase in abundance of these opportunistic species has been reported in only a few studies, suggesting certain mechanisms may be acting to regulate sponge populations. To gain insights into mechanisms of population control, we simulated the dynamics of the common reef-excavating sponge Cliona tenuis in the Caribbean using an individual-based model. An orthogonal hypothesis testing approach was used, where four candidate mechanisms-algal competition, stock-recruitment limitation, whole and partial mortality-were incorporated sequentially into the model and the results were tested against independent field observations taken over a decade in Belize, Central America. We found that releasing space after coral mortality can promote C. tenuis outbreaks, but such outbreaks can be curtailed by macroalgal competition. The asymmetrical competitive superiority of macroalgae, given by their capacity to pre-empt space and outcompete with the sponge in a size-dependant fashion, supports their capacity to steal the opportunity from other opportunists. While multiple system stages can be expected in coral reefs following intense perturbation macroalgae may prevent the growth of other space-occupiers, such as bioeroding sponges, under low grazing pressure. C1 [Gonzalez-Rivero, Manuel; Bozec, Yves-Marie; Chollett, Iliana; Ferrari, Renata; Mumby, Peter J.] Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia. [Gonzalez-Rivero, Manuel; Bozec, Yves-Marie; Chollett, Iliana; Ferrari, Renata; Mumby, Peter J.] Univ Queensland, Australian Res Council, Ctr Excellence Coral Reef Studies, St Lucia, Qld 4072, Australia. [Gonzalez-Rivero, Manuel; Chollett, Iliana; Mumby, Peter J.] Univ Exeter, Coll Life & Environm Sci, Exeter EX4 4PS, Devon, England. [Schoenberg, Christine H. L.] Univ Western Australia, Oceans Inst, 39 Fairway, Crawley, WA 6009, Australia. [Gonzalez-Rivero, Manuel] Univ Queensland, Global Change Inst, St Lucia, Qld 4072, Australia. [Chollett, Iliana] Smithsonian Inst, Smithsonian Marine Stn, Ft Pierce, FL USA. [Ferrari, Renata] Univ Sydney, Coastal & Marine Ecosyst Grp, Sch Biol Sci, Sydney, NSW, Australia. [Ferrari, Renata] Univ Sydney, Australian Ctr Field Robot, Sydney, NSW, Australia. RP Gonzalez-Rivero, M (reprint author), Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia.; Gonzalez-Rivero, M (reprint author), Univ Queensland, Australian Res Council, Ctr Excellence Coral Reef Studies, St Lucia, Qld 4072, Australia.; Gonzalez-Rivero, M (reprint author), Univ Exeter, Coll Life & Environm Sci, Exeter EX4 4PS, Devon, England.; Gonzalez-Rivero, M (reprint author), Univ Queensland, Global Change Inst, St Lucia, Qld 4072, Australia. EM m.gonzalezrivero@uq.edu.au OI Gonzalez-Rivero, Manuel/0000-0003-0252-584X; Bozec, Yves-Marie/0000-0002-7190-5187; Schonberg, Christine Hanna Lydia/0000-0001-6286-8196 FU Fondo Nacional de Ciencia, Tecnologia e Innovacion; Wildlife Conservation Society; Khaled bin Sultan Living Oceans Foundation; Natural Environment Research Council; ARC FX The authors would like to thank the contribution of five anonymous reviewers and the handling editor, S. Sandin, to the final version of the manuscript. This study was funded by: (1) the Fondo Nacional de Ciencia, Tecnologia e Innovacion to MGR, (2) the Wildlife Conservation Society and Khaled bin Sultan Living Oceans Foundation to R. F., and (3) the Natural Environment Research Council and ARC Laureate Fellowship to P. J. M. We are grateful to the WCS Belize staff and volunteers for their generous field assistance, and to S. O'Farrell, A. Harborne, E. Johnston and C. Doropoulos for editorial comments. NR 91 TC 0 Z9 0 U1 6 U2 14 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD MAY PY 2016 VL 181 IS 1 BP 161 EP 173 DI 10.1007/s00442-015-3541-x PG 13 WC Ecology SC Environmental Sciences & Ecology GA DJ9WM UT WOS:000374564000015 PM 26753672 ER PT J AU Delaney, MA Ward, JM Walsh, TF Chinnadurai, SK Kerns, K Kinsel, MJ Treuting, PM AF Delaney, M. A. Ward, J. M. Walsh, T. F. Chinnadurai, S. K. Kerns, K. Kinsel, M. J. Treuting, P. M. TI Initial Case Reports of Cancer in Naked Mole-rats (Heterocephalus glaber) SO VETERINARY PATHOLOGY LA English DT Article DE adenocarcinoma; cancer; electron microscopy; Heterocephalus glaber; naked mole-rat; neoplasia; neuroendocrine carcinoma; ultrastructure ID 2-YEAR CARCINOGENICITY; LESIONS; MICE; MODEL; DIFFERENTIATION; INSIGHTS; THYMUS; RODENT; TESTIS; SYSTEM AB Naked mole-rats (NMRs; Heterocephalus glaber) are highly adapted, eusocial rodents renowned for their extreme longevity and resistance to cancer. Because cancer has not been formally described in this species, NMRs have been increasingly utilized as an animal model in aging and cancer research. We previously reported the occurrence of several age-related diseases, including putative pre-neoplastic lesions, in zoo-housed NMR colonies. Here, we report for the first time 2 cases of cancer in zoo-housed NMRs. In Case No. 1, we observed a subcutaneous mass in the axillary region of a 22-year-old male NMR, with histologic, immunohistochemical (pancytokeratin positive, rare p63 immunolabeling, and smooth muscle actin negative), and ultrastructural characteristics of an adenocarcinoma possibly of mammary or salivary origin. In Case No. 2, we observed a densely cellular, poorly demarcated gastric mass of polygonal cells arranged in nests with positive immunolabeling for synaptophysin and chromogranin indicative of a neuroendocrine carcinoma in an approximately 20-year-old male NMR. We also include a brief discussion of other proliferative growths and pre-cancerous lesions diagnosed in 1 zoo colony. Although these case reports do not alter the longstanding observation of cancer resistance, they do raise questions about the scope of cancer resistance and the interpretation of biomedical studies in this model. These reports also highlight the benefit of long-term disease investigations in zoo-housed populations to better understand naturally occurring disease processes in species used as models in biomedical research. C1 [Delaney, M. A.; Treuting, P. M.] Univ Washington, Dept Comparat Med, 850 Republ St, Seattle, WA 98109 USA. [Ward, J. M.] Global VetPathol, Montgomery Village, MD USA. [Walsh, T. F.; Kerns, K.] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. [Chinnadurai, S. K.] Chicago Zool Soc & Brookfield Zoo, Brookfield, IL USA. [Kinsel, M. J.] Univ Illinois, Zool Pathol Program, Maywood, IL USA. RP Delaney, MA (reprint author), Univ Washington, Dept Comparat Med, 850 Republ St, Seattle, WA 98109 USA. EM delanm@u.washington.edu NR 22 TC 10 Z9 10 U1 19 U2 23 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0300-9858 EI 1544-2217 J9 VET PATHOL JI Vet. Pathol. PD MAY PY 2016 VL 53 IS 3 BP 691 EP 696 DI 10.1177/0300985816630796 PG 6 WC Pathology; Veterinary Sciences SC Pathology; Veterinary Sciences GA DJ8WB UT WOS:000374492800025 PM 26846576 ER PT J AU Glowacka, H McFarlin, SC Catlett, KK Mudakikwa, A Bromage, TG Cranfield, MR Stoinski, TS Schwartz, GT AF Glowacka, Halszka McFarlin, Shannon C. Catlett, Kierstin K. Mudakikwa, Antoine Bromage, Timothy G. Cranfield, Michael R. Stoinski, Tara S. Schwartz, Gary T. TI Age-related changes in molar topography and shearing crest length in a wild population of mountain Gorillas from Volcanoes National Park, Rwanda SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE tooth wear; dental senescence; aging; Gorilla beringei beringei ID LEMURS LEMUR-CATTA; MAHAFALY SPECIAL RESERVE; TOOTH WEAR; DENTAL TOPOGRAPHY; CHEWING EFFICIENCY; FEEDING ECOLOGY; LIFE-HISTORY; MECHANICAL-PROPERTIES; REPRODUCTIVE SUCCESS; FRACTURE-TOUGHNESS AB ObjectivesGreat ape teeth must remain functional over long lifespans. The molars of the most folivorous apes, the mountain gorillas, must maintain shearing function for 40+ years while the animals consume large quantities of mechanically challenging foods. While other folivorous primates experience dental senescence, which compromises their occlusal surfaces and affects their reproductive success as they age, it is unknown whether dental senescence also occurs in mountain gorillas. In this article, we quantified and evaluated how mountain gorilla molars change throughout their long lifespans. Materials and MethodsWe collected high-resolution replicas of M(1)s (n=15), M(2)s (n=13), and M(3)s (n=11) from a cross-sectional sample of wild mountain gorilla skeletons from the Virunga Volcanoes, ranging in age from 4 to 43 years. We employed dental topographic analyses to track how aspects of occlusal slope, angularity, relief index, and orientation patch count rotated change with age. In addition, we measured the relative length of shearing crests in two- and three-dimensions. ResultsOcclusal topography was found to decrease, while 2D relative shearing crest length increased, and 3D relative crest lengths were maintained with age. DiscussionOur findings indicate that shearing function is maintained throughout the long lifetimes of mountain gorillas. Unlike the dental senescence experienced by other folivorous primates, mountain gorillas do not appear to possess senesced molars despite their long lifetimes, mechanically challenging diets, and decreases in occlusal topography with age. Am J Phys Anthropol 160:3-15, 2016. (c) 2016 Wiley Periodicals, Inc. C1 [Glowacka, Halszka; Catlett, Kierstin K.; Schwartz, Gary T.] Arizona State Univ, Inst Human Origins, Sch Human Evolut & Social Change, Tempe, AZ 85281 USA. [McFarlin, Shannon C.] George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. [McFarlin, Shannon C.] George Washington Univ, Ctr Adv Study Human Paleobiol, Washington, DC 20052 USA. [McFarlin, Shannon C.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. [Mudakikwa, Antoine] Rwanda Dev Board, Tourism & Conservat, Kigali, Rwanda. [Bromage, Timothy G.] NYU, Coll Dent, Dept Biomat & Biomimet, New York, NY 10003 USA. [Bromage, Timothy G.] NYU, Coll Dent, Dept Basic Sci & Craniofacial Biol, New York, NY 10003 USA. [Cranfield, Michael R.] Univ Calif Davis, Mt Gorilla Vet Project, Davis, CA USA. [Stoinski, Tara S.] Dian Fossey Gorilla Fund Int, Atlanta, GA USA. RP Glowacka, H (reprint author), Arizona State Univ, Inst Human Origins, Sch Human Evolut & Social Change, Tempe, AZ 85281 USA. EM halszka.glowacka@asu.edu NR 101 TC 2 Z9 2 U1 7 U2 11 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 MAY PY 2016 VL 160 IS 1 BP 3 EP 15 DI 10.1002/ajpa.22943 PG 13 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA DJ6GY UT WOS:000374310300001 PM 26853974 ER PT J AU Kristensen, LE Brown, JM Wilner, D Salyk, C AF Kristensen, Lars E. Brown, Joanna M. Wilner, David Salyk, Colette TI VELOCITY-RESOLVED HOT WATER EMISSION DETECTED TOWARD HL TAU WITH THE SUBMILLIMETER ARRAY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: jets and outflows; line: profiles; stars: formation; stars: winds, outflows ID YOUNG STELLAR OBJECTS; LOW-MASS PROTOSTARS; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISK; ORGANIC-MOLECULES; REGION; HERSCHEL; VAPOR; LINES; TELESCOPE AB Using the Submillimeter Array (SMA) on Mauna Kea, the (H2O)-O-16 10(2,9)-9(3,6) transition (E-up = 1863 K) at 321.2 GHz has been detected toward the embedded low-mass protostar HL Tau. The line centroid is blueshifted by 20 km s(-1) with respect to the source velocity, and it has a FWHM of 25 km s(-1). The emission is tentatively resolved and extends similar to 3"-4" over the sky (similar to 2 beams), or similar to 500 au at the distance of Taurus. The velocity offset, and to a lesser degree the spatial extent of the emission, show that the line originates in the protostellar jet or wind. This result suggests that at least some water emission observed with Herschel and Spitzer toward embedded sources, and perhaps also disk sources, contains a wind or jet component, which is crucial for interpreting these data. These pathfinder observations done with the SMA open a new window into studying the origin of water emission with e.g., ALMA, thus providing new insights into where water is in protostellar systems. C1 [Kristensen, Lars E.; Brown, Joanna M.; Wilner, David] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Salyk, Colette] Vassar Coll, Dept Phys & Astron, 124 Raymond Ave, Poughkeepsie, NY 12604 USA. RP Kristensen, LE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lkristensen@cfa.harvard.edu RI Kristensen, Lars E/F-4774-2011; OI Kristensen, Lars E/0000-0003-1159-3721; Salyk, Colette/0000-0003-3682-6632 FU Smithsonian Institution; Academia Sinica FX The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The authors would like to thank J. Najita and J. Carr for fruitful discussions on the origin of hot water emission, and M. Gurwell for assistance with the data calibration. NR 40 TC 2 Z9 2 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 MAY 1 PY 2016 VL 822 IS 1 AR L20 DI 10.3847/2041-8205/822/1/L20 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DK8CF UT WOS:000375154100020 ER PT J AU Miller, JM Raymond, J Cackett, E Grinberg, V Nowak, M AF Miller, J. M. Raymond, J. Cackett, E. Grinberg, V. Nowak, M. TI AN ULTRA-FAST X-RAY DISK WIND IN THE NEUTRON STAR BINARY GX 340+0 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; X-rays: binaries ID ACCRETION DISKS; BLACK-HOLES; SPECTRUM; LINES; SPECTROSCOPY; REFLECTION; ABSORPTION; X-1 AB We present a spectral analysis of a brief Chandra/HETG observation of the neutron star low-mass X-ray binary GX 340+0. The high-resolution spectrum reveals evidence of ionized absorption in the Fe K band. The strongest feature, an absorption line at approximately 6.9 keV, is required at the 5 sigma level of confidence via an F-test. Photoionization modeling with XSTAR grids suggests that the line is the most prominent part of a disk wind with an apparent outflow speed of v = 0.04c. This interpretation is preferred at the 4 sigma level over a scenario in which the line is H-like Fe XXVI at a modest redshift. The wind may achieve this speed owing to its relatively low ionization, enabling driving by radiation pressure on lines; in this sense, the wind in GX 340+0 may be the stellar-mass equivalent of the flows in broad absorption line quasars. If the gas has a unity volume filling factor, the mass ouflow rate in the wind is over 10(-5)M(circle dot) yr(-1), and the kinetic power is nearly 10(39) erg s(-1) (or, 5-6 times the radiative Eddington limit for a neutron star). However, geometrical considerations-including a small volume filling factor and low covering factor-likely greatly reduce these values. C1 [Miller, J. M.] Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48109 USA. [Raymond, J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Cackett, E.] Wayne State Univ, Dept Phys & Astron, 666 W Hancock St, Detroit, MI 48201 USA. [Grinberg, V.; Nowak, M.] MIT, Kavli Inst Astrophys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48109 USA. EM jonmm@umich.edu NR 27 TC 2 Z9 2 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 MAY 1 PY 2016 VL 822 IS 1 AR L18 DI 10.3847/2041-8205/822/1/L18 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DK8CF UT WOS:000375154100018 ER PT J AU Montet, BT Johnson, JA Fortney, JJ Desert, JM AF Montet, Benjamin T. Johnson, John Asher Fortney, Jonathan J. Desert, Jean-Michel TI BENCHMARK TRANSITING BROWN DWARF LHS 6343 C: SPITZER SECONDARY ECLIPSE OBSERVATIONS YIELD BRIGHTNESS TEMPERATURE AND MID-T SPECTRAL CLASS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: eclipsing; brown dwarfs; stars: late-type; stars: low-mass ID INFRARED ARRAY CAMERA; LOW-MASS STARS; SPACE-TELESCOPE; PHYSICAL-PROPERTIES; GIANT EXOPLANET; L/T TRANSITION; LIGHT CURVES; EVOLUTION; YOUNG; ATMOSPHERES AB There are no field brown dwarf analogs with measured masses, radii, and luminosities, precluding our ability to connect the population of transiting brown dwarfs with measurable masses and radii and field brown dwarfs with measurable luminosities and atmospheric properties. LHS 6343 C, a weakly irradiated brown dwarf transiting one member of an M+M binary in the Kepler field, provides the first opportunity to probe the atmosphere of a non-inflated brown dwarf with a measured mass and radius. Here, we analyze four Spitzer observations of secondary eclipses of LHS 6343 C behind LHS 6343 A. Jointly fitting the eclipses with a Gaussian process noise model of the instrumental systematics, we measure eclipse depths of 1.06 +/- 0.21 ppt at 3.6 mu m and 2.09 +/- 0.08 ppt at 4.5 mu m, corresponding to brightness temperatures of 1026 +/- 57 K and 1249 +/- 36 K, respectively. We then apply brown dwarf evolutionary models to infer a bolometric luminosity log(L-star/L-circle dot)= -5.16 +/- 0.04. Given the known physical properties of the brown dwarf and the two M dwarfs in the LHS 6343 system, these depths are consistent with models of a 1100 K T dwarf at an age of 5 Gyr and empirical observations of field T5-6 dwarfs with temperatures of 1070 +/- 130 K. We investigate the possibility that the orbit of LHS 6343 C has been altered by the Kozai-Lidov mechanism and propose additional astrometric or Rossiter-McLaughlin measurements of the system to probe the dynamical history of the system. C1 [Montet, Benjamin T.] CALTECH, Cahill Ctr Astron & Astrophys, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91106 USA. [Montet, Benjamin T.; Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Desert, Jean-Michel] Univ Amsterdam, Anton Pannenkoek Astron Inst, NL-1090 GE Amsterdam, Netherlands. RP Montet, BT (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91106 USA.; Montet, BT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM btm@astro.caltech.edu OI Montet, Benjamin/0000-0001-7516-8308 FU NASA; National Science Foundation Graduate Research Fellowship [DGE-1144469]; David and Lucile Packard Foundation; Alfred P. Sloan Foundation FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech.; B.T.M. is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144469. J.A.J. is supported by generous grants from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation. NR 47 TC 0 Z9 0 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 MAY 1 PY 2016 VL 822 IS 1 AR L6 DI 10.3847/2041-8205/822/1/L6 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DK8CF UT WOS:000375154100006 ER PT J AU Sand, DJ Hsiao, EY Banerjee, DPK Marion, GH Diamond, TR Joshi, V Parrent, JT Phillips, MM Stritzinger, MD Venkataraman, V AF Sand, D. J. Hsiao, E. Y. Banerjee, D. P. K. Marion, G. H. Diamond, T. R. Joshi, V. Parrent, J. T. Phillips, M. M. Stritzinger, M. D. Venkataraman, V. TI POST-MAXIMUM NEAR-INFRARED SPECTRA OF SN 2014J: A SEARCH FOR INTERACTION SIGNATURES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Infrared: general; supernovae: general; supernovae: individual (2014J) ID HUBBLE-SPACE-TELESCOPE; IA SUPERNOVA 2014J; PROGENITOR SYSTEM; NEBULAR SPECTRA; CONSTRAINTS; HYDROGEN; SPECTROSCOPY; ABSORPTION; EXPLOSION; COMPANION AB We present near-infrared (NIR) spectroscopic and photometric observations of the nearby Type Ia SN 2014J. The 17 NIR spectra span epochs from +15.3 to +92.5 days after B-band maximum light, while the JHK(s) photometry include epochs from -10 to +71 days. These. data are. used to constrain the progenitor system of SN 2014J utilizing the Pa beta line, following recent suggestions that this phase period and the NIR in particular are excellent for constraining the amount of swept-up hydrogen-rich material associated with a non-degenerate companion star. We find no evidence for Pa beta emission lines in our post-maximum spectra, with a rough hydrogen mass limit of less than or similar to 0.1 M-circle dot, which is consistent with previous limits in SN. 2014J from late-time optical spectra of the H alpha line. Nonetheless, the growing data. set of high-quality NIR spectra holds the promise of very useful hydrogen constraints. C1 [Sand, D. J.] Texas Tech Univ, Dept Phys, Box 41051, Lubbock, TX 79409 USA. [Hsiao, E. Y.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Banerjee, D. P. K.; Joshi, V.; Venkataraman, V.] Phys Res Lab, Astron & Astrophys Div, Ahmadabad 380009, Gujarat, India. [Marion, G. H.] Univ Texas Austin, 1 Univ Stn C1400, Austin, TX 78712 USA. [Diamond, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Parrent, J. T.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Phillips, M. M.] Las Campanas Observ, Carnegie Observ, Casilla 601, Colina El Pino, Chile. [Stritzinger, M. D.] Aarhus Univ, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. RP Sand, DJ (reprint author), Texas Tech Univ, Dept Phys, Box 41051, Lubbock, TX 79409 USA. EM david.sand@ttu.edu OI Hsiao, Eric/0000-0003-1039-2928; Parrent, Jerod/0000-0002-5103-7706; Sand, David/0000-0003-4102-380X FU NSF [AST-1412504, AST-1517649]; Department of Space, Government of India; Danish Agency for Science and Technology and Innovation; National Science Foundation [AST-1008343] FX D.J.S. acknowledges support from NSF grants AST-1412504 and AST-1517649. The research work at the PRL is funded by the Department of Space, Government of India. M.D.S. acknowledges support provided by the Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant. This Letter is partially based on observations carried out by the CSP that were supported by the National Science Foundation under grant No. AST-1008343. We are grateful to Stefano Valenti for his comments. NR 42 TC 2 Z9 2 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 MAY 1 PY 2016 VL 822 IS 1 AR L16 DI 10.3847/2041-8205/822/1/L16 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DK8CF UT WOS:000375154100016 ER PT J AU Ctvrtecka, R Sam, K Miller, SE Weiblen, GD Novotny, V AF Ctvrtecka, Richard Sam, Katerina Miller, Scott E. Weiblen, George D. Novotny, Vojtech TI Fruit sizes and the structure of frugivorous communities in a New Guinea lowland rainforest SO AUSTRAL ECOLOGY LA English DT Article DE Coleoptera; Diptera; Lepidoptera; seed-eating herbivore; seed predation ID PREDISPERSAL SEED PREDATION; PAPUA-NEW-GUINEA; DISPERSAL; LEPIDOPTERA; HOST; DIPTEROCARPACEAE; COLEOPTERA; BEETLES; DEFENSE; DIPTERA AB A community of frugivorous insects was studied by rearing of 25565 individual insects representing three orders (Coleoptera, Lepidoptera and Diptera except Drosophilidae) from 326 woody plant species in a lowland rainforest in Papua New Guinea. Fruits from 19.3% of plant species were not attacked by any insect order, 33.4% of plant species were attacked by a single order, 30% by two orders and 17.2% by all three orders. The likelihood of attack by individual orders was positively correlated so that a higher proportion of plant species than expected suffered either no attack at all or was attacked by all three insect orders. Fruits from most of the plant species exhibited low rates of attack and low densities of insects. One kilogram of fruit was attacked on average by 11 insects, including three to four Coleoptera, six Diptera and one Lepidoptera. Thus, we reared on average one insect from 10 fruits, including one Diptera from 14 fruits, one Coleoptera from 22 fruits and one Lepidoptera from 100 fruits. Only 72 out of the 326 plant species hosted more than one insect per 10 fruits, and only seven species supported a density of greater than one insect per fruit. Our results suggest that specialized insect seed predators are probably too rare to maintain the diversity of vegetation by density-dependent mortality of seeds as suggested by the Janzen-Connell hypothesis. Fruit weight, fruit volume, mesocarp volume, seed volume and fleshiness had no significant effect on the probability that a fruit would be attacked by an insect frugivore. However, fruits attacked by Diptera were significantly larger and had larger volume of both mesocarp and seeds than fruits attacked by Coleoptera and Lepidoptera. C1 [Ctvrtecka, Richard; Sam, Katerina; Novotny, Vojtech] Univ South Bohemia, Fac Sci, Ceske Budejovice, Czech Republic. [Sam, Katerina; Novotny, Vojtech] Acad Sci Czech Republic, Ctr Biol, Ceske Budejovice, Czech Republic. [Miller, Scott E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Weiblen, George D.] Univ Minnesota, Bell Museum, St Paul, MN 55108 USA. [Weiblen, George D.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. [Novotny, Vojtech] New Guinea Binatang Res Ctr, Madang, Papua N Guinea. RP Ctvrtecka, R (reprint author), Univ South Bohemia, Fac Sci, Ceske Budejovice, Czech Republic. EM richard.ctvrtecka@seznam.cz RI Novotny, Vojtech/G-9434-2014; Sam, Katerina/I-2209-2014; OI Novotny, Vojtech/0000-0001-7918-8023; Sam, Katerina/0000-0002-3436-0579; Miller, Scott/0000-0002-4138-1378 FU PNG National Agriculture Research Institute; PNG Forest Research Institute; PNG Department of Environment and Conservation; Czech Science Foundation [13-09979S]; Darwin Initiative for the Survival of Species (UK); Christensen Fund; US National Science Foundation [DEB-0515678, DEB816749]; Government of Canada through Genome Canada; Ontario Genomics Institute [2008-0GIICI-03] FX The present study, as many others in the past 25 years, has benefitted from Roger Kitching's ideas on food webs and from his ecological studies in PNG and elsewhere, as well as from the inspirational and stimulating milieu always prevailing in his lab. This study was undertaken with the support of the PNG National Agriculture Research Institute, PNG Forest Research Institute and PNG Department of Environment and Conservation. We thank New Guinea Research Binatang Center staff and field assistants from Wanang, Ohu and Baitabag villages for technical assistance. Weevil identifications were assisted by Alexander Riedel, Richard Thompson (Baridinae) and Marek Wanat (Apionidae). Fly taxonomy was assisted by Miroslav Bartak (Neriidae), Stepan Kubik (Chloropidae), Rudolf Rozkosny (Stratiomyidae) and Andrew Wittington (Syrphidae). Moth taxonomy was assisted by John Brown (Tortricidae), Don Davis (Tineidae), Lauren Helgen, Jeremy Holloway, Marianne Horak (Phycitinae and Tortricidae), Margaret Rosati, Kevin Tuck (Tortricidae) and Maia Vaswani. We appreciate access to the vital collections of the Natural History Museum, London. Plant taxonomy was assisted by Kipiro Damas and KennethMolem. This study was supported by the Czech Science Foundation (13-09979S), Darwin Initiative for the Survival of Species (UK), the Christensen Fund and the US National Science Foundation (DEB-0515678 and DEB816749). We thank Paul Hebert and colleagues at the Biodiversity Institute of Ontario for their assistance with the barcode library of the local fauna, which was funded by the Government of Canada through Genome Canada and the Ontario Genomics Institute (2008-0GIICI-03). NR 64 TC 1 Z9 1 U1 7 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1442-9985 EI 1442-9993 J9 AUSTRAL ECOL JI Austral Ecol. PD MAY PY 2016 VL 41 IS 3 BP 228 EP 237 DI 10.1111/aec.12326 PG 10 WC Ecology SC Environmental Sciences & Ecology GA DK7CX UT WOS:000375083600001 ER PT J AU Sinsabaugh, RL Turner, BL Talbot, JM Waring, BG Powers, JS Kuske, CR Moorhead, DL Shah, JJF AF Sinsabaugh, Robert L. Turner, Benjamin L. Talbot, Jennifer M. Waring, Bonnie G. Powers, Jennifer S. Kuske, Cheryl R. Moorhead, Daryl L. Shah, Jennifer J. Follstad TI Stoichiometry of microbial carbon use efficiency in soils SO ECOLOGICAL MONOGRAPHS LA English DT Article DE biomass turnover; carbon use efficiency; ecoenzymatic activity; ecological stoichiometry; microbial communities; soil ecology; nutrient use efficiency ID N-P STOICHIOMETRY; TERRESTRIAL ECOSYSTEMS; ORGANIC-MATTER; ECOENZYMATIC STOICHIOMETRY; GROWTH EFFICIENCY; ESCHERICHIA-COLI; BACTERIAL-GROWTH; PLANT INPUTS; COPY-NUMBER; PHOSPHORUS AB The carbon use efficiency (CUE) of microbial communities partitions the flow of C from primary producers to the atmosphere, decomposer food webs, and soil C stores. CUE, usually defined as the ratio of growth to assimilation, is a critical parameter in ecosystem models, but is seldom measured directly in soils because of the methodological difficulty of measuring in situ rates of microbial growth and respiration. Alternatively, CUE can be estimated indirectly from the elemental stoichiometry of organic matter and microbial biomass, and the ratios of C to nutrient-acquiring ecoenzymatic activities. We used this approach to estimate and compare microbial CUE in >2000 soils from a broad range of ecosystems. Mean CUE based on C:N stoichiometry was 0.269 +/- 0.110 (mean +/- SD). A parallel calculation based on C:P stoichiometry yielded a mean CUE estimate of 0.252 +/- 0.125. The mean values and frequency distributions were similar to those from aquatic ecosystems, also calculated from stoichiometric models, and to those calculated from direct measurements of bacterial and fungal growth and respiration. CUE was directly related to microbial biomass C with a scaling exponent of 0.304 (95% CI 0.237-0.371) and inversely related to microbial biomass P with a scaling exponent of -0.234 (95% CI -0.289 to -0.179). Relative to CUE, biomass specific turnover time increased with a scaling exponent of 0.509 (95% CI 0.467-0.551). CUE increased weakly with mean annual temperature. CUE declined with increasing soil pH reaching a minimum at pH 7.0, then increased again as soil pH approached 9.0, a pattern consistent with pH trends in the ratio of fungal : bacteria abundance and growth. Structural equation models that related geographic variables to CUE component variables showed the strongest connections for paths linking latitude and pH to beta-glucosidase activity and soil C:N:P ratios. The integration of stoichiometric and metabolic models provides a quantitative description of the functional organization of soil microbial communities that can improve the representation of CUE in microbial process and ecosystem simulation models. C1 [Sinsabaugh, Robert L.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. [Talbot, Jennifer M.] Boston Univ, Dept Biol, 5 Cummington Mall, Boston, MA 02215 USA. [Waring, Bonnie G.; Powers, Jennifer S.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. [Powers, Jennifer S.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. [Kuske, Cheryl R.] Los Alamos Natl Lab, Biosci Div, POB 1663, Los Alamos, NM 87545 USA. [Moorhead, Daryl L.] Univ Toledo, Dept Environm Sci, 2801 W Bancroft St, Toledo, OH 43606 USA. [Shah, Jennifer J. Follstad] Univ Utah, Environm & Sustainable Studies Program, 260 South Cent Campus Dr, Salt Lake City, UT 84112 USA. RP Sinsabaugh, RL (reprint author), Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. EM rlsinsab@unm.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU NSF CAREER grant [DEB-1053237]; U.S. Department of Energy, Office of Science, Biological and Environmental Research Division FX B. G. Waring and J. S. Powers thank an NSF CAREER grant DEB-1053237 (to J. S. Powers). C. R. Kuske and R. L. Sinsabaugh were supported by a Science Focus Area grant to Los Alamos National Laboratory by the U.S. Department of Energy, Office of Science, Biological and Environmental Research Division. NR 57 TC 0 Z9 0 U1 61 U2 105 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9615 EI 1557-7015 J9 ECOL MONOGR JI Ecol. Monogr. PD MAY PY 2016 VL 86 IS 2 BP 172 EP 189 DI 10.1890/15-2110.1 PG 18 WC Ecology SC Environmental Sciences & Ecology GA DL1EZ UT WOS:000375376400002 ER PT J AU Bacon, CD Molnar, P Antonelli, A Crawford, AJ Montes, C Vallejo-Pareja, MC AF Bacon, Christine D. Molnar, Peter Antonelli, Alexandre Crawford, Andrew J. Montes, Camilo Camila Vallejo-Pareja, Maria TI Quaternary glaciation and the Great American Biotic Interchange SO GEOLOGY LA English DT Article ID INTERTROPICAL CONVERGENCE ZONE; MIDDLE MIOCENE; SOUTH-AMERICA; PACIFIC-OCEAN; LAND MAMMALS; SEA-LEVEL; PANAMA; RECORD; ATLANTIC; ISTHMUS AB Recent geological studies demonstrate that the Isthmus of Panama emerged some 10 m.y. earlier than previously assumed. Although absent today in Panama, Central American savanna environments likely developed in connection with the onset of Northern Hemisphere glaciations. As is widely recognized, most of the mammals crossing the isthmus since 2.5 Ma lived in savannas. Could climate-induced vegetational changes across Panama explain the delayed migration of mammals, rather than terrestrial connectivity? We investigate the congruence between cross-continental mammal migration and climate change through analysis of fossil data and molecular phylogenies. Evidence from fossil findings shows that the vast majority of mammals crossed between South and North America after ca. 3 Ma. By contrast, dated mammal phylogenies suggest that migration events started somewhat earlier, ca. 4-3 Ma, but allowing for biases toward greater ages of molecular than geologic dating and uncertainties in the former, we consider this age range not to be significantly earlier than 3 Ma. We conclude that savanna-like environments developed in response to the vast Laurentide ice sheet at the first Quaternary glaciation triggered the initiation of the Great American Biotic Interchange in mammals. C1 [Bacon, Christine D.; Antonelli, Alexandre] Univ Gothenburg, Dept Biol & Environm Sci, SE-40530 Gothenburg, Sweden. [Bacon, Christine D.; Camila Vallejo-Pareja, Maria] Univ Ind Santander, Dept Biol, CINBIN, Bucaramanga 681011, Colombia. [Molnar, Peter] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Molnar, Peter] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Antonelli, Alexandre] Gothenburg Bot Garden, SE-41319 Gothenburg, Sweden. [Crawford, Andrew J.] Univ Los Andes, Dept Biol Sci, Bogota 111711, Colombia. [Crawford, Andrew J.] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Montes, Camilo] Univ Los Andes, Dept Geosci, Bogota 111711, Colombia. RP Bacon, CD (reprint author), Univ Gothenburg, Dept Biol & Environm Sci, SE-40530 Gothenburg, Sweden.; Bacon, CD (reprint author), Univ Ind Santander, Dept Biol, CINBIN, Bucaramanga 681011, Colombia. OI Montes, Camilo/0000-0002-3553-0787 FU Swedish Research Council [B0569601]; European Research Council [331024, FP/2007-2013]; Wallenberg Academy Fellowship; Uniandes [P12.160422.002/001] FX Bacon and Antonelli were funded by the Swedish (B0569601) and European (331024; FP/2007-2013) Research Councils and a Wallenberg Academy Fellowship. Montes was supported by Uniandes P12.160422.002/001. Molnar thanks the Crafoord Foundation. We thank Kira Lawrence for data on ice rafted debris, and Henry Hooghiemstra, Carlos Jaramillo, and two anonymous reviewers for detailed and constructive suggestions. NR 66 TC 5 Z9 5 U1 7 U2 15 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 EI 1943-2682 J9 GEOLOGY JI Geology PD MAY PY 2016 VL 44 IS 5 BP 375 EP 378 DI 10.1130/G37624.1 PG 4 WC Geology SC Geology GA DK4HG UT WOS:000374877500012 ER PT J AU Pesendorfer, MB Sillett, TS Morrison, SA Kamil, AC AF Pesendorfer, Mario B. Sillett, T. Scott Morrison, Scott A. Kamil, Alan C. TI Context-dependent seed dispersal by a scatter-hoarding corvid SO JOURNAL OF ANIMAL ECOLOGY LA English DT Article DE Aphelocoma; context dependence; Corvidae; Quercus; scatter-hoarding; seed dispersal; species interactions ID ACORN PRODUCTION; CACHING BEHAVIOR; OAK FORESTS; SCRUB-JAYS; PATTERNS; TREES; PREDATION; ECOLOGY; SIZE; COMPETITORS AB Corvids (crows, jays, magpies and nutcrackers) are important dispersers of large-seeded plants. Studies on captive or supplemented birds suggest that they flexibly adjust their scatter-hoarding behaviour to the context of social dynamics and relative seed availability. Because many corvid-dispersed trees show high annual variation in seed production, context-dependent foraging can have strong effects on natural corvid scatter-hoarding behaviour. We investigated how seed availability and social dynamics affected scatter-hoarding in the island scrub jays (Aphelocoma insularis). We quantified rates of scatter-hoarding behaviour and territorial defence of 26 colour-marked birds over a three-year period with variable acorn crops. We tested whether caching parameters were correlated with variation in annual seed production of oaks as predicted by the predator dispersal hypothesis, which states that caching rates and distances should vary with seed abundance in ways that benefit tree fitness. We also tested whether antagonistic interactions with conspecifics would affect scatter-hoarding adversely, as found in experimental studies. Caching behaviour varied with acorn availability. Caching distances correlated positively with annual acorn crop size, increasing by as much as 40% between years. Caching rates declined over time in years with small acorn crops, but increased when crops were large. Acorn foraging and caching rates were also negatively correlated with rates of territorial aggression. Overall foraging rates, however, were not associated with aggression, suggesting that reduced dispersal rates were not simply due to time constraints. Our field results support laboratory findings that caching rates and distances by scatter-hoarding corvids are context-dependent. Furthermore, our results are consistent with predictions of the predator dispersal hypothesis and suggest that large seed crops and social interactions among scatter-hoarders affect dispersal benefits for oaks and other masting tree species. C1 [Pesendorfer, Mario B.; Kamil, Alan C.] Univ Nebraska, Sch Biol Sci, 348 Manter Hall, Lincoln, NE 68588 USA. [Pesendorfer, Mario B.; Sillett, T. Scott] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, MRC 5503, Washington, DC 20013 USA. [Morrison, Scott A.] Nature Conservancy, 201 Mission St, San Francisco, CA 94105 USA. [Pesendorfer, Mario B.] Cornell Lab Ornithol, 159 Sapsucker Woods Rd, Ithaca, NY 14850 USA. RP Pesendorfer, MB (reprint author), Univ Nebraska, Sch Biol Sci, 348 Manter Hall, Lincoln, NE 68588 USA.; Pesendorfer, MB (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, MRC 5503, Washington, DC 20013 USA.; Pesendorfer, MB (reprint author), Cornell Lab Ornithol, 159 Sapsucker Woods Rd, Ithaca, NY 14850 USA. EM mario.pesendorfer@yahoo.com OI Pesendorfer, Mario/0000-0002-7994-7090 FU Nature Conservancy (TNC); U.S. National Park Service; Smithsonian Institution FX This research was funded by The Nature Conservancy (TNC), the U.S. National Park Service, and the Smithsonian Institution. Fieldwork was conducted at the University of California Natural Reserve System's Santa Cruz Island Reserve on property owned and managed by TNC. Comments by Dan Leger, Sabrina Russo, Johannes Knops and Walt Koenig greatly improved the manuscript. We thank Katie Langin for vital input throughout fieldwork and Christie Boser and Lyndal Laughrin for logistical support. Michelle Desrosiers, Elizabeth Donadio, Laura Duval, Claire Giuliano, Cassidy Grattan, Justin Houck, Juan Klavins, Jessica Piispanen and Colin Woolley assisted with data collection. The authors declare no conflict of interest. NR 47 TC 3 Z9 3 U1 9 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8790 EI 1365-2656 J9 J ANIM ECOL JI J. Anim. Ecol. PD MAY PY 2016 VL 85 IS 3 BP 798 EP 805 DI 10.1111/1365-2656.12501 PG 8 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA DK7QS UT WOS:000375121400020 PM 26876417 ER PT J AU Xu, X Liu, FX Chen, J Ono, H Agnarsson, I Li, DQ Kuntner, M AF Xu, Xin Liu, Fengxiang Chen, Jian Ono, Hirotsugu Agnarsson, Ingi Li, Daiqin Kuntner, Matjaz TI Pre-Pleistocene geological events shaping diversification and distribution of primitively segmented spiders on East Asian margins SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE biogeography; Cenozoic; continental islands; dispersal; Kyushu; phylogeography; Ryukyus; vicariance ID DISPERSAL-VICARIANCE ANALYSIS; RYUKYU ARCHIPELAGO; MITOCHONDRIAL-DNA; JAPAN SEA; PALEOGEOGRAPHIC IMPLICATIONS; POPULATION-GROWTH; BIOGEOGRAPHY; PHYLOGEOGRAPHY; EVOLUTION; PHYLOGENY AB Aim Phylogeographical research in the East Asian continent and islands (East Asian Margins, or EAM) suggests predominant Pleistocene over-water dispersal events from continent to islands, but more ancient biogeographical patterns in EAM remain obscure. We explored biogeographical histories and population genetic structures of the primitively segmented spiders, Heptathela and Ryuthela (Liphistiidae), broadly codistributed across EAM islands. To test competing biogeographical hypotheses, we looked for geohistoric events that may have shaped their distributional patterns. Location Kyushu and Ryukyus. Methods We sampled 17 Heptathela and Ryuthela species on 10 out of 12 EAM islands and sequenced fragments of two mitochondrial and three nuclear genes. We performed phylogenetic, network, time-calibrated and biogeographical analyses to identify lineages, estimate their divergence times, and reconstruct ancestral ranges. We also assessed genetic diversity and historic demography of each lineage. Results Phylogenetic origin of Heptathela + Ryuthela is estimated at 26.6-18.4 Ma (95% HPD) when EAM islands became separated from the continent. The crown ages of Heptathela (18.0-10.7 Ma) and Ryuthela (17.8-8.7 Ma) coincide with the formation of Japan Sea and Okinawa Trough respectively. A split within Ryuthela (13.9-6.0 Ma) coincides with the opening of the Kerama Gap, but a split within Heptathela (18.0-10.7 Ma) pre-dates the formation of the Tokara Gap. Speciation within Heptathela and Ryuthela is relatively recent (6.0-0.3 Ma). Population genetic and demographic results suggest interrupted gene flow within and among islands, with most species exhibiting stable past populations. Main conclusions Historic biogeographical reconstructions strongly suggest predominant vicariant origins of EAM island liphistiids. Restricted gene flow following barrier formation is the dominant speciation force in these spiders. As they never seem to cross bodies of water, their past range expansion, successive fragmentation of EAM, and other vicariant events, must have shaped the detected genetic boundaries among and within islands. C1 [Xu, Xin] Hunan Normal Univ, Coll Life Sci, Changsha, Hunan, Peoples R China. [Xu, Xin; Liu, Fengxiang; Chen, Jian; Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Ctr Behav Ecol & Evolut, Wuhan, Peoples R China. [Li, Daiqin] Natl Univ Singapore, Dept Biol Sci, Singapore 117548, Singapore. [Kuntner, Matjaz] Biol Inst ZRC SAZU, Evolutionary Zool Lab, SI-1001 Ljubljana, Slovenia. [Agnarsson, Ingi; Kuntner, Matjaz] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Ono, Hirotsugu] Natl Museum Nat & Sci, Dept Zool, 4-1-1 Amakubo, Tsukuba, Ibaraki 3050005, Japan. [Agnarsson, Ingi] Univ Vermont, Dept Biol, 109 Carrigan Dr,MLS-316, Burlington, VT 05405 USA. RP Kuntner, M (reprint author), ZRC SAZU Inst Biol, Novi Trg 2,POB 306, SI-1001 Ljubljana, Slovenia. EM kuntner@gmail.com RI Li, Daiqin/D-6922-2013; xu, xin/E-5012-2017 OI Li, Daiqin/0000-0001-8269-7734; xu, xin/0000-0001-5632-6622 FU NSFC [31272324]; Singapore Ministry of Education (MOE) AcRF Tier 2 grant [R-154-000-621-112]; Slovenian Research Agency grants [P1-10236, MU-PROM/12-001] FX We thank Zoltan Korsos, Mamoru Toda and Bo Wu for field help, Miquel Arnedo, Matjaz Gregoric, Nina Vidergar and Ren-Chung Cheng for help and/or advice on molecular resources and procedures, and the staff members of the Centre for Behavioural Ecology and Evolution (CBEE, Hubei University) and of the Behavioural Ecology and Sociobiology Lab (DBS, NUS) for all their help and support throughout this study, in particularly Zhanqi Chen, Xiaoguo Jiao, Jie Liu, Yu Peng, Chen Xu, Long Yu and Zengtao Zhang. We value the positive feedback from three anonymous referees. This work was supported by the NSFC grant (31272324), by the Singapore Ministry of Education (MOE) AcRF Tier 2 grant (R-154-000-621-112) and by the Slovenian Research Agency grants (P1-10236 and MU-PROM/12-001). NR 72 TC 1 Z9 1 U1 9 U2 20 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 MAY PY 2016 VL 43 IS 5 BP 1004 EP 1019 DI 10.1111/jbi.12687 PG 16 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA DL2ON UT WOS:000375474800013 ER PT J AU Lany, NK Ayres, MP Stange, EE Sillett, TS Rodenhouse, NL Holmes, RT AF Lany, Nina K. Ayres, Matthew P. Stange, Erik E. Sillett, T. Scott Rodenhouse, Nicholas L. Holmes, Richard T. TI Breeding timed to maximize reproductive success for a migratory songbird: the importance of phenological asynchrony SO OIKOS LA English DT Article ID THROATED BLUE WARBLERS; CLIMATE-CHANGE; PHENOTYPIC PLASTICITY; FOOD AVAILABILITY; TEMPERATE FOREST; DECIDUOUS FOREST; NEST PREDATION; ANNUAL CYCLE; POPULATION; BIRDS AB Phenological advances and trophic mismatches are frequently reported ecological consequences of climate warming. Trophic mismatches occur when phenological responses to environmental conditions differ among trophic levels such that the timing of resource demand by consumers becomes decoupled from supply. We used 25 years of demographic measurements of a migratory songbird (the black-throated blue warbler Setophaga caerulescens) to compare its breeding phenology to the phenology of both its caterpillar prey and the foliage on which caterpillars feed. Caterpillar biomass in this forest did not show a predictable seasonal pulse. Nest initiation by warblers in this northern hardwood forest was therefore not timed to coincide with a peak in food availability for nestlings. Nonetheless, timing of first clutches was strongly associated with spring leaf expansion (slope +/- SE = 0.56 +/- 0.08 days per day of change in leaf phenology, R-2 = 0.66). Warblers adjusted the timing of breeding to early springs mainly by shortening the interval between arrival and clutch initiation, but this likely has limits because recent early springs are approaching the relatively inflexible dates when birds arrive on the breeding grounds. Although the timing of first nests did not match 1:1 with leaf-out phenology, the adjustments in breeding time maximized mean annual reproductive success. Nest predation had the greatest effect on annual reproductive success, but the ability of nesting warblers to appropriately track leaf phenology accounted for effects on annual reproductive success comparable to the influence of variation in caterpillar abundance and conspecific density. Nesting phenology in black-throated blue warblers was generally well matched to the timing of leaf-out, even though the match was not 1:1. Without measurements of reproductive success, these unequal phenological shifts might otherwise have been interpreted as having negative ecological consequences. C1 [Lany, Nina K.; Ayres, Matthew P.; Holmes, Richard T.] Dartmouth Coll, Dept Biol Sci, 78 Coll St,Class 1978 Life Sci Ctr, Hanover, NH 03755 USA. [Stange, Erik E.] Norwegian Inst Nat Res, NO-2624 Lillehammer, Norway. [Sillett, T. Scott] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, MRC 5503, Washington, DC 20013 USA. [Rodenhouse, Nicholas L.] Wellesley Coll, Dept Biol Sci, 106 Cent St, Wellesley, MA 02481 USA. RP Lany, NK (reprint author), Dartmouth Coll, Dept Biol Sci, 78 Coll St,Class 1978 Life Sci Ctr, Hanover, NH 03755 USA. EM nina.k.lany.gr@dartmouth.edu FU US National Science Foundation; Dartmouth College; Wellesley College; Smithsonian Institution; NSF IGERT Fellowship; National Science Foundation FX This research was supported by grants from the US National Science Foundation, and by Dartmouth College, Wellesley College and the Smithsonian Institution. An NSF IGERT Fellowship supported NKL. This paper is a contribution of the Hubbard Brook Ecosystem Study. Hubbard Brook is part of the Long-Term Ecological Research (LTER) network, which is supported by the National Science Foundation. The Hubbard Brook Experimental Forest is operated and maintained by the USDA Forest Service, Northern Research Station, Newtown Square, Pennsylvania, USA. This work was performed under protocols approved by the Institutional Animal Care and Use Committees of Dartmouth College, Wellesley College and the Smithsonian Institution. This manuscript benefitted from comments from T. Wesolowski, K. A. Schmidt and C. Whelan. We thank the many students, field assistants and other colleagues who spent many hours in the field helping to collect the data presented in this paper. NR 66 TC 3 Z9 3 U1 24 U2 35 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 MAY PY 2016 VL 125 IS 5 BP 656 EP 666 DI 10.1111/oik.02412 PG 11 WC Ecology SC Environmental Sciences & Ecology GA DK7EN UT WOS:000375087800007 ER PT J AU Dellape, PM Melo, MC Henry, TJ AF Dellape, Pablo M. Melo, Maria C. Henry, Thomas J. TI A phylogenetic revision of the true bug genus Heraeus (Hemiptera: Rhyparochromidae: Myodochini), with the description of two new genera and 30 new species SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE 32 new taxa; cladistics; Heteroptera; Rhyparochrominae; systematics ID HETEROPTERA RHYPAROCHROMIDAE; GALAPAGOS-ISLANDS; LYGAEIDAE; ARGENTINA; LYGAEOIDEA; STAL; REDESCRIPTION; BRAILOVSKY; ECUADOR; RECORDS AB Prior to this study, the genus Heraeus Stal, 1862 included 14 species, all of which are restricted to the Western Hemisphere. Three species are known from the Nearctic Region, nine from the Neotropical Region, and two mainly tropical elements are distributed in both regions. In this contribution, we consider Heraeus cincticornis Stal, 1874 a junior synonym of Heraeus elegans (Walker, 1873), select a lectotype for Heraeus coquilletti Barber, 1914, and neotype for Lygaeus triguttatus Guerin-Meneville, 1857, and describe 28 new species. In addition, the two new genera, Baranowskiobius gen. nov., to include H. elegans (Baranowskiobius elegans comb. nov.) and two new species, and Paraheraeusgen. nov., to include Heraeus eximius Distant, 1882 (Paraheraeus eximius comb. nov.), are described. Previously described species and new taxa are (re)described and illustrated, including male genitalia. Scanning electron micrographs, general habitus photographs, and distribution maps are included for all species studied. A phylogenetic analysis comprising 46 terminal taxa and 50 morphological characters was performed, and five species groups were hypothesized, including the coquilletti, caliginosus, guttatus, illitus, and plebejus groups. All known species of Heraeus and the new genera are included in the phylogenetic analysis. The type species of the genera Myodocha Latreille, 1807, Orthaea Dallas, 1852, and Paisana Dellape, 2008 are used as out-groups. (C) 2016 The Linnean Society of London, Zoological Journal of the Linnean Society, 2016 C1 [Dellape, Pablo M.; Melo, Maria C.] Univ Nacl La Plata, Fac Ciencias Nat & Museo, Div Entomol, Paseo Bosque S-N,B1900FWA, RA-1900 La Plata, Buenos Aires, Argentina. [Dellape, Pablo M.; Melo, Maria C.] Consejo Nacl Invest Cient & Tecn, Cct La Plata, Argentina. [Henry, Thomas J.] Smithsonian Inst, Natl Museum Nat Hist, ARS, Systemat Entomol Lab,USDA, Washington, DC 20560 USA. RP Dellape, PM (reprint author), Univ Nacl La Plata, Fac Ciencias Nat & Museo, Div Entomol, Paseo Bosque S-N,B1900FWA, RA-1900 La Plata, Buenos Aires, Argentina.; Dellape, PM (reprint author), Consejo Nacl Invest Cient & Tecn, Cct La Plata, Argentina. EM pdellape@fcnym.unlp.edu.ar OI Dellape, Pablo M./0000-0002-6914-1026 FU Consejo Nacional de Investigaciones Cientificas y Tecnicas- CONICET, Argentina FX We are grateful to the following people for kindly lending the specimens used in this study: Randall T. Schuh (AMNH); Mick Webb (BMNH); Keve J. Ribardo (CAS); Diego L. Carpintero (MACN); Michael D. Schwartz (CNC); E. Richard Hoebeke (CUIC); Jerome Constant (IRSN); Axel O. Bachmann (MACN); Carlos Campaner (MZSP); Norman F. Johnson (OSUC); Jane O'Donnell (UCMS); John Grehan (PSUC); Robert Brooks (SEMC); and Mark O'Brien (UMMZ). We also thank R.T.Schuh (AMNH), Ruth Salas (AMNH), and Susan Halbert (FSCA) for their help in looking for the holotype of H.concolor, and Eric Guilbert (MNHN) for help looking for the syntypes of H.triguttatus. This work was funded in part by the Consejo Nacional de Investigaciones Cientificas y Tecnicas- CONICET, Argentina. NR 118 TC 0 Z9 0 U1 4 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 EI 1096-3642 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD MAY PY 2016 VL 177 IS 1 BP 29 EP 134 DI 10.1111/zoj.12362 PG 106 WC Zoology SC Zoology GA DK7KY UT WOS:000375105100002 ER PT J AU Meyer, JL Gunasekera, SP Scott, RM Paul, VJ Teplitski, M AF Meyer, Julie L. Gunasekera, Sarath P. Scott, Raymond M. Paul, Valerie J. Teplitski, Max TI Microbiome shifts and the inhibition of quorum sensing by Black Band Disease cyanobacteria SO ISME JOURNAL LA English DT Article ID WHITE PLAGUE DISEASE; VIBRIO-CHOLERAE AUTOINDUCER; CORAL-ASSOCIATED BACTERIA; GREAT-BARRIER-REEF; ROSEOFILUM-REPTOTAENIUM; INTERACTION NETWORKS; SIGNAL PRODUCTION; CARIBBEAN REEF; HOST-RANGE; COMMUNITIES AB Disruption of the microbiome often correlates with the appearance of disease symptoms in metaorganisms such as corals. In Black Band Disease (BBD), a polymicrobial disease consortium dominated by the filamentous cyanobacterium Roseofilum reptotaenium displaces members of the epibiotic microbiome. We examined both normal surface microbiomes and BBD consortia on Caribbean corals and found that the microbiomes of healthy corals were dominated by Gammaproteobacteria, in particular Halomonas spp., and were remarkably stable across spatial and temporal scales. In contrast, the microbial community structure in black band consortia was more variable and more diverse. Nevertheless, deep sequencing revealed that members of the disease consortium were present in every sampled surface microbiome of Montastraea, Orbicella and Pseudodiploria corals, regardless of the health status. Within the BBD consortium, we identified lyngbic acid, a cyanobacterial secondary metabolite. It strongly inhibited quorum sensing (QS) in the Vibrio harveyi QS reporters. The effects of lyngbic acid on the QS reporters depended on the presence of the CAI-1 receptor CqsS. Lyngbic acid inhibited luminescence in native coral Vibrio spp. that also possess the CAI-1-mediated QS. The effects of this naturally occurring QS inhibitor on bacterial regulatory networks potentially contribute to the structuring of the interactions within BBD consortia. C1 [Meyer, Julie L.; Scott, Raymond M.; Teplitski, Max] Univ Florida, Inst Food & Agr Sci, Genet Inst, Soil & Water Sci Dept, Room 330E,2033 Mowry Rd, Gainesville, FL 32610 USA. [Gunasekera, Sarath P.; Paul, Valerie J.; Teplitski, Max] Smithsonian Marine Stn, Ft Pierce, FL USA. RP Teplitski, M (reprint author), Univ Florida, Inst Food & Agr Sci, Genet Inst, Soil & Water Sci Dept, Room 330E,2033 Mowry Rd, Gainesville, FL 32610 USA. EM maxtep@ufl.edu OI Meyer, Julie/0000-0003-3382-3321 FU Protect Our Reefs Grant [2013-2]; George E Burch Fellowship in Theoretical Medicine; Smithsonian Institution; National Institutes of Health [R01 CA 172310]; Summit Foundation FX This research was supported by Protect Our Reefs Grant 2013-2, a George E Burch Fellowship in Theoretical Medicine and Affiliated Sciences at the Smithsonian Institution and the National Institutes of Health (R01 CA 172310). We are indebted to Dr B Bassler for sharing Vibrio harveyi QS reporters. Logistical support from the Center for Marine Studies, Honduras and funding from the Summit Foundation made possible sample collection off the Honduran coast. We thank E Bartels, C Thacker and C Walker for field assistance. This is a contribution 1007 of the Smithsonian Marine Station and contribution 979 from the Caribbean Coral Reef Ecosystems Program. NR 83 TC 9 Z9 9 U1 18 U2 33 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1751-7362 EI 1751-7370 J9 ISME J JI ISME J. PD MAY PY 2016 VL 10 IS 5 BP 1204 EP 1216 DI 10.1038/ismej.2015.184 PG 13 WC Ecology; Microbiology SC Environmental Sciences & Ecology; Microbiology GA DJ7FL UT WOS:000374377200017 PM 26495995 ER PT J AU Snak, C Vatanparast, M Silva, C Lewis, GP Lavin, M Kajita, T de Queiroz, LP AF Snak, Cristiane Vatanparast, Mohammad Silva, Christian Lewis, Gwilym Peter Lavin, Matt Kajita, Tadashi de Queiroz, Luciano Paganucci TI A dated phylogeny of the papilionoid legume genus Canavalia reveals recent diversification by a pantropical liana lineage SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Ancestral area reconstruction; Biogeography; Diocleae; Isthmus of Panama; Leguminosae; Molecular dating ID DRY TROPICAL FORESTS; NUCLEAR RIBOSOMAL DNA; RAPID DIVERSIFICATION; CLIMATE-CHANGE; PLANT DIVERSITY; WESTERN PANAMA; ANDEAN UPLIFT; SOUTH-AMERICA; MIXED MODELS; EVOLUTION AB Canavalia is a pantropical legume genus of lianas comprising approximately 60 species distributed in a wide range of habitats. In the last taxonomic revision, the genus was divided into four subgenera: Canavalia (Pantropical), Catodonia (Neotropical, excepting one species also found in the Old World), Maunaloa (Hawaiian), and Wenderothia (Neotropical). In this study, we reconstructed the phylogeny of Canavalia using a broad taxon sampling and analyses of nuclear (ETS and ITS) and plastid markers (trnKlmatK). We evaluated the infrageneric classification of the genus and investigated its biogeographical history using molecular dating analyses and ancestral area reconstructions. The phylogenetic analyses resolved subgenus Wenderothia as monophyletic. Subgenus Catodonia needs to be recircumscribed and the relationships between subgenera Canavalia and Maunaloa remain unclear. Canavalia arose during the Miocene with a mean stem age estimate of 13.8 Ma and mean crown age estimate of 8.7 Ma, and most extant species evolved during the Pleistocene. Several climatic and geological events are chronologically coincident with the divergence of the major clades of Canavalia (glacial/interglacial periods, Andes uplift and the formation of Pebas and post-Pebas systems, closure of the Isthmus of Panama, and change in the direction of ocean currents). Ancestral area reconstructions for the early divergence of the genus are equivocal, although, some evidence suggests Canavalia originated in the wet forests of South America and achieved its current pantropical distribution through recent transoceanic dispersal. The evolution of Canavalia is better explained by a series of several processes than by discrete historical events. (C) 2016 Elsevier Inc. All rights reserved. C1 [Snak, Cristiane; Silva, Christian; de Queiroz, Luciano Paganucci] Univ Estadual Feira de Santana, Dept Ciencias Biol, Av Transnordestina S-N, BR-44036900 Feira De Santana, BA, Brazil. [Vatanparast, Mohammad] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. [Vatanparast, Mohammad] Chiba Univ, Grad Sch Sci, Dept Biol, Inage Ku, 1-33 Yayoi Cho, Chiba 2638522, Japan. [Lewis, Gwilym Peter] Royal Bot Gardens, Comparat Plant & Fungal Biol Dept, Richmond TW9 3AB, Surrey, England. [Lavin, Matt] Montana State Univ, Dept Plant Sci & Plant Pathol, Bozeman, MT 59717 USA. [Kajita, Tadashi] Univ Ryukyus, Trop Biosphere Res Ctr, Iriomote Stn, Takketomi, Okinawa 9071541, Japan. RP Snak, C (reprint author), Univ Estadual Feira de Santana, Dept Ciencias Biol, Av Transnordestina S-N, BR-44036900 Feira De Santana, BA, Brazil. EM cristianesnak@gmail.com; vatanparast@gmail.com; christian_da_silva@hotmail.com; g.lewis@kew.org; mlavin@montana.edu; kajita@mail.ryudai.jp; luciano.paganucci@gmail.com FU Programa de Pesquisa em Biodiversidade do Semigrido (PPBIO); Sistema Nacional de Pesquisa em Biodiversidade (SISBIOTA CNPq) [563084/2010-3/FAPESB PES0053/2011]; PRONEX (FAPESB) [PNX0014/2009]; PROTAX (CNPq) [562354/2010-7]; REFLORA (CNPq) [563546/2010-7/FAPESB PES0054/2011]; Environment Research and Technology Development Fund of the Ministry of the Environment, Japan [S-9]; Missouri Botanical Garden; CAPES; SWE CAPES at the Royal Botanic Gardens, Kew FX We thank the curators of the herbaria visited for access to specimens; the herbaria B, BM, CEN, CEPEC, F, G, GH, HUEFS, K, M, MBM, MO, NY, P, and US for the donation of DNA samples; Ariane Barbosa, Domingos Cardoso, Leonardo Borges, Maria Cristina Roberts, and Wallace Sao-Mateus for leaf material of Canavalia; Centro Internacional de Agricultura Tropical (CIAT, Cali, Colombia) for providing seeds of the species of Canavalia from the forage germplasm collection; Alan Graham and Patrick Herendeen for the help with fossils; Alexandre Zuntini for the help with analysis in BioGeoBEARS; Benoit Henry for the photos of C. favieri and C sericea; Jenn Sinasac for the photos of C bicarinata; Kanoa Kimball for the photos of C hawaiiensis; Instituto Chico Mendes de Conservacao da Biodiversidade (ICMBio) for issuing collecting permits. Fieldwork and DNA sequencing were sponsored by the Programa de Pesquisa em Biodiversidade do Semigrido (PPBIO), Sistema Nacional de Pesquisa em Biodiversidade (SISBIOTA CNPq 563084/2010-3/FAPESB PES0053/2011), PRONEX (FAPESB PNX0014/2009), PROTAX (CNPq 562354/2010-7), and REFLORA (CNPq 563546/2010-7/FAPESB PES0054/2011). This study was also supported by the Environment Research and Technology Development Fund (S-9) of the Ministry of the Environment, Japan. C. Snak also thanks the Missouri Botanical Garden for the 2014 Elizabeth E. Bascom Fellowship. This study is part of the first author's PhD thesis developed in the Programa de Pos-Graduacao em Botanica (UEFS) and supported by PhD fellowship grants from CAPES, and SWE CAPES at the Royal Botanic Gardens, Kew. NR 100 TC 1 Z9 1 U1 6 U2 15 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAY PY 2016 VL 98 BP 133 EP 146 DI 10.1016/j.ympev.2016.02.001 PG 14 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA DJ4VT UT WOS:000374206900015 PM 26860339 ER PT J AU Ament-Velasquez, SL Breedy, O Cortes, J Guzman, HM Worheide, G Vargas, S AF Ament-Velasquez, Sandra L. Breedy, Odalisca Cortes, Jorge Guzman, Hector M. Woerheide, Gert Vargas, Sergio TI Homoplasious colony morphology and mito-nuclear phylogenetic discordance among Eastern Pacific octocorals SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Molecular systematics; Octocorals; Eastern Pacific; Mito-nuclear discordance; Colony morphology; Homoplasy ID GENUS PACIFIGORGIA COELENTERATA; TRANSCRIBED SPACER 2; MITOCHONDRIAL-DNA; SEQUENCE ALIGNMENT; MOLECULAR PHYLOGENY; PHENOTYPIC PLASTICITY; SPECIES OCTOCORALLIA; GORGONIAN OCTOCORALS; SOFTWARE PACKAGE; CORALS CNIDARIA AB Octocorals are a diverse and ecologically important group of cnidarians. However, the phylogenetic relationships of many octocoral groups are not well understood and are based mostly on mitochondrial sequence data. In addition, the discovery and description of new gorgonian species displaying unusual or intermediate morphologies and uncertain phylogenetic affinities further complicates the study of octocoral systematics and raises questions about the role played by processes such as plasticity, crypsis, and convergence in the evolution of this group of organisms. Here, we use nuclear (i.e. 28S rDNA) and mitochondrial (mtMutS) markers and a sample of Eastern Pacific gorgonians thought to be remarkable from a morphological point of view to shed light on the morphological diversification among these organisms. Our study reveals the loss of the anastomosed colony morphology in two unrelated lineages of the seafan genus Pacifigorgia and offers strong evidence for the independent evolution of a whip -like morphology in two lineages of Eastern Pacific Leptogorgia. Additionally, our data revealed one instance of mito-nuclear discordance in the genera Leptogorgia and Eugorgia, which may be the results of incomplete lineage sorting or ancient hybridization-introgression events. Our study stresses the importance of comprehensive taxonomic sampling and the use of independent sources of evidence to address the phylogenetic relationships and clarifying the evolution of octocorals. (C) 2016 Elsevier Inc. All rights reserved. C1 [Ament-Velasquez, Sandra L.; Woerheide, Gert; Vargas, Sergio] Univ Munich, Dept Earth & Environm Sci Paleontol & Geobiol, Richard Wagner Str 10, D-80333 Munich, Germany. [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Estruct Microscop, San Jose, Costa Rica. [Breedy, Odalisca; Cortes, Jorge] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica. [Breedy, Odalisca; Guzman, Hector M.] Smithsonian Trop Res Inst, POB 0843-03092, Panama City, Panama. [Woerheide, Gert] Bavarian State Collect Palaeontol & Geol, Richard Wagner Str 10, D-80333 Munich, Germany. [Woerheide, Gert] LMU, GeoBio Ctr, Richard Wagner Str 10, D-80333 Munich, Germany. RP Vargas, S (reprint author), Univ Munich, Dept Earth & Environm Sci Paleontol & Geobiol, Richard Wagner Str 10, D-80333 Munich, Germany. RI Worheide, Gert/C-1080-2008; OI Worheide, Gert/0000-0002-6380-7421; Ament-Velasquez, Sandra Lorena/0000-0003-3371-9292 NR 97 TC 0 Z9 0 U1 5 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAY PY 2016 VL 98 BP 373 EP 381 DI 10.1016/j.ympev.2016.02.023 PG 9 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA DJ4VT UT WOS:000374206900034 PM 26953740 ER PT J AU Mashian, N Loeb, A Sternberg, A AF Mashian, Natalie Loeb, Abraham Sternberg, Amiel TI Spectral distortion of the CMB by the cumulative CO emission from galaxies throughout cosmic history SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE intergalactic medium; cosmic background radiation; cosmology: theory; early Universe ID MICROWAVE BACKGROUND SPECTRUM; COSMOLOGICAL HYDROGEN RECOMBINATION; ENERGY-RELEASE; EARLY UNIVERSE; HOT-MODEL; RADIATION; EVOLUTION; MATTER; WAVES; DISSIPATION AB We show that the cumulative CO emission from galaxies throughout cosmic history distorts the spectrum of the cosmic microwave background at a level that is well above the detection limit of future instruments, such as the Primordial Inflation Explorer. The modelled CO signal has a prominent bump in the frequency interval 100-200 GHz, with a characteristic peak intensity of similar to 2 x 10(-23) W m(-2) Hz(-1) sr(-1). Most of the CO foreground originates from modest redshifts, z similar to 2-5, and needs to be efficiently removed for more subtle distortions from the earlier Universe to be detected. C1 [Mashian, Natalie; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Sternberg, Amiel] Tel Aviv Univ, Raymond & Beverly Sackler Sch Phys & Astron, IL-69978 Tel Aviv, Israel. RP Mashian, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nmashian@physics.harvard.edu FU Raymond and Beverly Sackler Tel Aviv University - Harvard/ITC Astronomy Program; NSF [AST-1312034]; National Science Foundation [DGE1144152] FX This research was supported by the Raymond and Beverly Sackler Tel Aviv University - Harvard/ITC Astronomy Program. This work was supported in part by NSF grant AST-1312034. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE1144152. Any opinion, 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 48 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 MAY 1 PY 2016 VL 458 IS 1 BP L99 EP L103 DI 10.1093/mnrasl/slw027 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ5DF UT WOS:000374226300021 ER PT J AU Nicastro, F Senatore, F Gupta, A Mathur, S Krongold, Y Elvis, M Piro, L AF Nicastro, F. Senatore, F. Gupta, A. Mathur, S. Krongold, Y. Elvis, M. Piro, L. TI Diffuse low-ionization gas in the galactic halo casts doubts on z similar or equal to 0.03 WHIM detections SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE atomic data; line: identification; local interstellar matter; intergalactic medium; quasars: absorption lines; X-rays: ISM ID HOT INTERGALACTIC MEDIUM; X-RAY-ABSORPTION; LINE-OF-SIGHT; INTERSTELLAR-MEDIUM; SCULPTOR WALL; BARYONS; FOREST; ABSORBER AB In this Letter, we demonstrate that the two claims of z similar or equal to 0.03 O VII K alpha absorption lines from Warm Hot Intergalactic Medium (WHIM) along the lines of sight to the blazars H 2356-309 (Buote et al.; Fang et al.) and Mkn 501 (Ren, Fang & Buote) are likely misidentifications of the z = 0 O II K beta line produced by a diffuse Low-Ionization Metal Medium in the Galaxy's interstellar and circum-galactic mediums. We perform detailed modelling of all the available high signal-to-noise Chandra Low Energy Transmission Grating (LETG) and XMM-Newton Reflection Grating Spectrometer (RGS) spectra of H 2356-309 and Mkn 501 and demonstrate that the z similar or equal to 0.03 WHIM absorption along these two sightlines is statistically not required. Our results, however, do not rule out a small contribution from the z similar or equal to 0.03 O VII K alpha absorber along the line of sight to H 2356-309. In our model the temperature of the putative z = 0.031 WHIM filament is T = 3 x 10(5) K and the O VII column density is N-OVII less than or similar to 4 x 10(15) cm(-2), twenty times smaller than the O VIIcolumn density previously reported, and now more consistent with the expectations from cosmological hydrodynamical simulations. C1 [Nicastro, F.; Senatore, F.] Osservatorio Astron Roma INAF, Via Frascati 33, I-00040 Monte Porzio Catone, RM, Italy. [Nicastro, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-04, Cambridge, MA 02138 USA. [Nicastro, F.] Univ Crete, Dept Phys, POB 2208, GR-71003 Iraklion, Greece. [Gupta, A.; Mathur, S.] Ohio State Univ, Dept Astron, 4055 McPherson Lab,140 West 18th Ave, Columbus, OH 43210 USA. [Gupta, A.] Columbus State Community Coll, 550 E Spring St, Columbus, OH 43215 USA. [Mathur, S.] Ctr Cosmol & Astroparticle Phys CCAPP, 191 West Woodruff Ave, Columbus, OH 43210 USA. [Krongold, Y.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Piro, L.] Ist Astrofis & Planetol Spaziali INAF, I-00133 Rome, Italy. RP Nicastro, F (reprint author), Osservatorio Astron Roma INAF, Via Frascati 33, I-00040 Monte Porzio Catone, RM, Italy.; Nicastro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-04, Cambridge, MA 02138 USA.; Nicastro, F (reprint author), Univ Crete, Dept Phys, POB 2208, GR-71003 Iraklion, Greece. EM fabrizio.nicastro@oa-roma.inaf.it FU INAF-PRIN [1.05.01.98.10] FX We thank the anonymous referee for the useful comments that helped improving the Letter. FN and FS acknowledge support from INAF-PRIN grant 1.05.01.98.10. NR 23 TC 2 Z9 2 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 MAY 1 PY 2016 VL 458 IS 1 BP L123 EP L127 DI 10.1093/mnrasl/slw022 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ5DF UT WOS:000374226300026 ER PT J AU Thompson, MA Scicluna, P Kemper, F Geach, JE Dunham, MM Morata, O Ertel, S Ho, PTP Dempsey, J Coulson, I Petitpas, G Kristensen, LE AF Thompson, M. A. Scicluna, P. Kemper, F. Geach, J. E. Dunham, M. M. Morata, O. Ertel, S. Ho, P. T. P. Dempsey, J. Coulson, I. Petitpas, G. Kristensen, L. E. TI Constraints on the circumstellar dust around KIC 8462852 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE circumstellar matter; stars: peculiar; submillimetre: galaxies; submillimetre: stars ID BETA-PICTORIS; DEBRIS DISK; HR 8799; CATALOG; STARS; SCUBA-2; SIGNATURES; SEARCH; SYSTEM AB We present millimetre (Submillimeter Array) and submillimetre (SCUBA-2) continuum observations of the peculiar star KIC 8462852 which displayed several deep and aperiodic dips in brightness during the Kepler mission. Our observations are approximately confusion-limited at 850 mu m and are the deepest millimetre and submillimetre photometry of the star that has yet been carried out. No significant emission is detected towards KIC 8462852. We determine upper limits for dust between a few 10(-6) M-circle plus and 10(-3) M-circle plus for regions identified as the most likely to host occluding dust clumps and a total overall dust budget of <7.7 M-circle plus within a radius of 200 au. Such low limits for the inner system make the catastrophic planetary disruption hypothesis unlikely. Integrating over the Kepler light curve we determine that at least 10(-9) M-circle plus of dust is required to cause the observed Q16 dip. This is consistent with the currently most favoured cometary breakup hypothesis, but nevertheless implies the complete breakup of similar to 30 Comet 1/P Halley type objects. Finally, in the wide SCUBA-2 field of view we identify another candidate debris disc system that is potentially the largest yet discovered. C1 [Thompson, M. A.; Geach, J. E.] Univ Hertfordshire, Sch Phys Astron & Math, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, Herts, England. [Scicluna, P.; Kemper, F.; Morata, O.; Ho, P. T. P.] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. [Dunham, M. M.; Petitpas, G.; Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Ertel, S.] European So Observ, Alonso de Cordova 3107,Casilla 19001, Santiago, Chile. [Ho, P. T. P.; Dempsey, J.; Coulson, I.] East Asian Observ, 660 N Aohoku Pl,Univ Pk, Hilo, HI 96720 USA. RP Thompson, MA (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, Herts, England. EM m.a.thompson@herts.ac.uk RI Kristensen, Lars/F-4774-2011; Kemper, Francisca/D-8688-2011; OI Kristensen, Lars/0000-0003-1159-3721; Kemper, Francisca/0000-0003-2743-8240; Scicluna, Peter/0000-0002-1161-3756 FU Chinese Academy of Sciences [XDB09000000]; Science and Technology Facilities Council of the United Kingdom; Smithsonian Institution; Academia Sinica; UK Science & Technology Facility Council [ST/M001008/1]; Ministry of Science and Technology of Taiwan [MOST104-2628-M-001-004-MY3]; Royal Society; SMA; NASA [NNX13AE54G] FX We would like to thank the anonymous referee for their timely and constructive report. The James Clerk Maxwell Telescope is operated by the East Asian Observatory on behalf of The National Astronomical Observatory of Japan, Academia Sinica Institute of Astronomy and Astrophysics, the Korea Astronomy and Space Science Institute, the National Astronomical Observatories of China and the Chinese Academy of Sciences (Grant No. XDB09000000), with additional funding support from the Science and Technology Facilities Council of the United Kingdom and participating universities in the United Kingdom and Canada. This Letter is based partly on observations obtained with the SMA, a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and funded by the Smithsonian Institution and the Academia Sinica. MAT acknowledges support from the UK Science & Technology Facility Council via grant ST/M001008/1. FK acknowledges the support the Ministry of Science and Technology of Taiwan through grant MOST104-2628-M-001-004-MY3. JEG acknowledges the support of the Royal Society. MMD acknowledges support from the SMA through an SMA Postdoctoral Fellowship, and from NASA through grant NNX13AE54G. NR 30 TC 2 Z9 2 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 MAY 1 PY 2016 VL 458 IS 1 BP L39 EP L43 DI 10.1093/mnrasl/slw008 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ5DF UT WOS:000374226300009 ER PT J AU Boyle, SA Thompson, CL Deluycker, A Alvarez, SJ Alvim, THG Aquino, R Bezerra, BM Boubli, JP Bowler, M Caselli, CB Chagas, RRD Ferrari, SF Fontes, IP Gregory, T Haugaasen, T Heiduck, S Hores, R Lehman, S De Melo, FR Moreira, LS Moura, VS Nagy-Reis, MB Palacios, E Palminteri, S Peres, CA Pinto, L Port-Carvalho, M Rodriguez, A Dos Santos, RR Setz, EZF Shaffer, CA Silva, FE Da Silva, RFS Souza-Alves, JP Trevelin, LC Veiga, LM Vieira, TM Dubose, ME Barnett, AA AF Boyle, Sarah A. Thompson, Cynthia L. Deluycker, Anneke Alvarez, Silvia J. Alvim, Thiago H. G. Aquino, Rolando Bezerra, Bruna M. Boubli, Jean P. Bowler, Mark Caselli, Christini Barbosa Chagas, Renata R. D. Ferrari, Stephen F. Fontes, Isadora P. Gregory, Tremaine Haugaasen, Torbjorn Heiduck, Stefanie Hores, Rose Lehman, Shawn De Melo, Fabiano R. Moreira, Leandro S. Moura, Viviane S. Nagy-Reis, Mariana B. Palacios, Erwin Palminteri, Suzanne Peres, Carlos A. Pinto, Liliam Port-Carvalho, Marcio Rodriguez, Adriana Dos Santos, Ricardo R. Setz, Eleonore Z. F. Shaffer, Christopher A. Silva, Felipe Ennes Da Silva, Rafaela F. Soares Souza-Alves, Joao P. Trevelin, Leonardo C. Veiga, Liza M. Vieira, Tatiana M. Dubose, Mary E. Barnett, Adrian A. TI Geographic Comparison of Plant Genera Used in Frugivory Among the Pitheciids Cacajao, Callicebus, Chiropotes, and Pithecia SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE bearded saki; diet; saki; titi; uacari ID BRAZILIAN ATLANTIC FOREST; NEW-WORLD MONKEYS; FEEDING ECOLOGY; NATIONAL-PARK; SEED DISPERSAL; MELANOCEPHALUS-MELANOCEPHALUS; CHARACTER DISPLACEMENT; HABITAT FRAGMENTATION; PERSONATUS-MELANOCHIR; NEOTROPICAL PRIMATES AB Pitheciids are known for their frugivorous diets, but there has been no broad-scale comparison of fruit genera used by these primates that range across five geographic regions in South America. We compiled 31 fruit lists from data collected from 18 species (three Cacajao, six Callicebus, five Chiropotes, and four Pithecia) at 26 study sites in six countries. Together, these lists contained 455 plant genera from 96 families. We predicted that 1) closely related Chiropotes and Cacajao would demonstrate the greatest similarity in fruit lists; 2) pitheciids living in closer geographic proximity would have greater similarities in fruit lists; and 3) fruit genus richness would be lower in lists from forest fragments than continuous forests. Fruit genus richness was greatest for the composite Chiropotes list, even though Pithecia had the greatest overall sampling effort. We also found that the Callicebus composite fruit list had lower similarity scores in comparison with the composite food lists of the other three genera (both within and between geographic areas). Chiropotes and Pithecia showed strongest similarities in fruit lists, followed by sister taxa Chiropotes and Cacajao. Overall, pitheciids in closer proximity had more similarities in their fruit list, and this pattern was evident in the fruit lists for both Callicebus and Chiropotes. There was no difference in the number of fruit genera used by pitheciids in habitat fragments and continuous forest. Our findings demonstrate that pitheciids use a variety of fruit genera, but phylogenetic and geographic patterns in fruit use are not consistent across all pitheciid genera. This study represents the most extensive examination of pitheciid fruit consumption to date, but future research is needed to investigate the extent to which the trends in fruit genus richness noted here are attributable to habitat differences among study sites, differences in feeding ecology, or a combination of both. Am. J. Primatol. 78: 493-506, 2016. (C) 2015 Wiley Periodicals, Inc. C1 [Boyle, Sarah A.; Dubose, Mary E.] Rhodes Coll, Dept Biol, 2000 North Pkwy, Memphis, TN 38112 USA. [Thompson, Cynthia L.] Grand Valley State Univ, Dept Biomed Sci, Allendale, MI 49401 USA. [Deluycker, Anneke] Smithsonian Mason Sch Conservat, Front Royal, VA USA. [Alvarez, Silvia J.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Alvim, Thiago H. G.] Univ Fed Goias, Res Support Fdn, Jatai, Goias, Brazil. [Aquino, Rolando] Univ Nacl Mayor San Marcos, Lima 14, Peru. [Bezerra, Bruna M.] Univ Fed Pernambuco, Dept Zool, Recife, PE, Brazil. [Boubli, Jean P.] Univ Salford, Manchester, Lancs, England. [Bowler, Mark] San Diego Zoo Global Inst Conservat Res, San Diego, CA USA. [Caselli, Christini Barbosa] Univ Estadual Santa Cruz, Dept Biol Sci, Ilheus, Bahia, Brazil. [Chagas, Renata R. D.; Souza-Alves, Joao P.] Univ Fed Paraiba, Dept Systemat & Ecol, BR-58059900 Joao Pessoa, Paraiba, Brazil. [Ferrari, Stephen F.] Univ Fed Sergipe, Dept Ecol, Sao Cristovao, Sergipe, Brazil. [Fontes, Isadora P.] Municipal Environm Secretariat, Aracaju, Sergipe, Brazil. [Gregory, Tremaine] Ctr Conservat Educ & Sustainabil, Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC USA. [Haugaasen, Torbjorn] Norwegian Univ Life Sci, Dept Ecol & Nat Resource Management, As, Norway. [Heiduck, Stefanie] Deutsches Primatenzentrum, Gottingen, Germany. [Hores, Rose] So Illinois Univ, Dept Anthropol, Carbondale, IL 62901 USA. [Lehman, Shawn] Univ Toronto, Dept Anthropol, Toronto, ON, Canada. [De Melo, Fabiano R.] Univ Fed Goias, Biol Sci Program, Jatai, Goias, Brazil. [Moreira, Leandro S.] Ctr Ecol & Environm Educ Studies, Carangola, Minas Gerais, Brazil. [Moura, Viviane S.] Univ Fed Sergipe, Program Ecol & Conservat, Sao Cristovao, Sergipe, Brazil. [Nagy-Reis, Mariana B.; Setz, Eleonore Z. F.] Univ Estadual Campinas, Inst Biol, Campinas, SP, Brazil. [Palacios, Erwin] Conservat Int Colombia, Bogota, Colombia. [Palminteri, Suzanne] RESOLVE, Washington, DC USA. [Peres, Carlos A.] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England. [Pinto, Liliam] Natl Ctr Amazonian Biodivers Res & Conservat, Chico Mendes Inst Biodivers Conservat, Manaus, Amazonas, Brazil. [Port-Carvalho, Marcio] Sao Paulo Forestry Inst, Sao Paulo, Brazil. [Rodriguez, Adriana; Dos Santos, Ricardo R.] Univ Fed Maranhao, Ctr Agrarian & Environm Sci, Chapadinha, Maranhao, Brazil. [Dos Santos, Ricardo R.] Univ Georgia, Ctr Geospatial Res, Athens, GA 30602 USA. [Shaffer, Christopher A.] Grand Valley State Univ, Dept Anthropol, Allendale, MI 49401 USA. [Silva, Felipe Ennes; Vieira, Tatiana M.] Mamiraua Inst Sustainable Dev, Tefe, Amazonas, Brazil. [Da Silva, Rafaela F. Soares] Museu Paraense Emilio Goeldi, Program Zool, Belem, Para, Brazil. [Trevelin, Leonardo C.; Veiga, Liza M.] Museu Paraense Emilio Goeldi, Dept Zool, Belem, Para, Brazil. [Barnett, Adrian A.] Natl Inst Amazonian Res, Biodivers Unit, Manaus, Amazonas, Brazil. RP Boyle, SA (reprint author), Rhodes Coll, Dept Biol, 2000 North Pkwy, Memphis, TN 38112 USA. EM sarahannboyle@gmail.com RI Bezerra, Bruna/C-6827-2015; Peres, Carlos/B-1276-2013; Haugaasen, Torbjorn/I-2663-2013; Caselli, Christini/F-5737-2017 OI Setz, Eleonore/0000-0001-7638-7086; Peres, Carlos/0000-0002-1588-8765; Haugaasen, Torbjorn/0000-0003-0901-5324; Caselli, Christini/0000-0002-3058-7872 NR 105 TC 1 Z9 1 U1 4 U2 12 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 MAY PY 2016 VL 78 IS 5 SI SI BP 493 EP 506 DI 10.1002/ajp.22422 PG 14 WC Zoology SC Zoology GA DJ0NU UT WOS:000373902000002 PM 26031411 ER PT J AU Gregory, T Bowler, M AF Gregory, Tremaine Bowler, Mark TI Male-Male Affiliation and Cooperation Characterize the Social Behavior of the Large-Bodied Pitheciids, Chiropotes and Cacajao: A Review SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Review DE cooperation; kinship; affiliation; dispersal; large groups ID NEW-WORLD PRIMATES; REPRODUCTIVE STRATEGIES; MULTILEVEL SOCIETIES; WILD CHIMPANZEES; SPIDER-MONKEYS; NATIONAL-PARK; PATTERNS; MELANOCEPHALUS; COMPETITION; POPULATION AB Cooperation and affiliation between males may be key to the evolution of large multimale-multifemale primate groups in some species. Cacajao and Chiropotes form multimale-multifemale groups larger than those of most other platyrrhines (Cacajao: over 150 and Chiropotes: up to 80 individuals), and groups exhibit a high degree of fission-fusion dynamics. In both genera, males engage in affiliative, sex-specific behaviors and form all-male parties. Males in both genera also have conspicuous genitalia but can demonstrate sexual crypsis, or mimicry, wherein testes are retracted, resembling labia. Observed egalitarian interactions among males suggest that there is scramble competition for access to females, and aggression between males is uncommon relative to other social primates. As of yet, there are no genetic data to clarify dispersal patterns, and while relatedness among males would in part explain their affiliative relationships, there is some limited evidence for dispersal by males in Cacajao. In this review of recent studies of male-male social interactions in Chiropotes and Cacajao, we posit that the ability to maintain large groups in these genera may be related to the affiliative and perhaps coalitionary relationships between males, who may or may not be related. Affiliative male-male relationships may allow for monopolization of groups of females and facilitate group cohesion by reducing intragroup aggression; however data on male-male interactions with identified individuals will be required to determine patterns of affiliation, while genetic studies may be the most practical way of determining dispersal patterns for these genera. Am. J. Primatol. 78: 550-560, 2016. (C) 2015 Wiley Periodicals, Inc. C1 [Gregory, Tremaine] Ctr Conservat Educ & Sustainabil, Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC USA. [Bowler, Mark] San Diego Zoo Global Inst Conservat Res, Escondido, CA USA. RP Gregory, T (reprint author), Ctr Conservat Educ & Sustainabil, Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC USA. EM gregoryt@si.edu OI Bowler, Mark/0000-0001-5236-3477 FU Center for Conservation Education and Sustainability FX We would like to thank Liza Veiga for her ground-breaking research in Chiropotes social behavior. We thank Anthony Di Fiore and two anonymous reviewers for their valuable comments and suggestions on drafts of the manuscript. We also thank Sarah Boyle for reviewof a previous draft of this manuscript and Marilyn Norconk for review of the manuscript and the presentation upon which this manuscript is based. MB thanks Matt Anderson, and TG thanks the Center for Conservation Education and Sustainability for support during elaboration of this manuscript. NR 84 TC 1 Z9 1 U1 12 U2 18 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 MAY PY 2016 VL 78 IS 5 SI SI BP 550 EP 560 DI 10.1002/ajp.22404 PG 11 WC Zoology SC Zoology GA DJ0NU UT WOS:000373902000006 PM 25845849 ER PT J AU Shaffer, CA Barnett, AA Gregory, T De Melo, F Moreira, L Alvim, THG Moura, VS Filo, A Cardoso, T Port-Carvalho, M Dos Santos, RR Boyle, SA AF Shaffer, Christopher A. Barnett, Adrian A. Gregory, Tremaine De Melo, Fabiano Moreira, Leandro Alvim, Thiago H. G. Moura, Viviane S. Filo, Anderson Cardoso, Tatiane Port-Carvalho, Marcio Dos Santos, Ricardo Rodrigues Boyle, Sarah A. TI Mixed-Species Associations in Cuxius (Genus Chiropotes) SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE polyspecific association; bearded sakis; Guyana; Brazil; Suriname ID SAGUINUS-FUSCICOLLIS; POLYSPECIFIC ASSOCIATIONS; AMAZONIAN TAMARINS; CALLIMICO-GOELDII; FOREST FRAGMENTS; PRIMATE GROUPS; DIANA MONKEYS; NATIONAL-PARK; RED COLOBUS; PATTERNS AB Polyspecific or mixed-species associations, where two or more species come together to forage and travel as a unit, have been reported in many primate species. These associations appear to offer a number of benefits to the species involved including increased foraging efficiency and decreased risk of predation. While several researchers have suggested that cuxius (genus Chiropotes) form mixed-species associations, previous studies have not identified the circumstances under which cuxius form associations or whether they form associations more often than would be expected by chance. Here we present data on the formation of mixed-species associations by four species of cuxius at eight different sites in Brazil, Suriname, and Guyana. We analyzed data from two of the study sites, (Biological Dynamics of Forest Fragments Project (BDFFP), Brazil and the Upper Essequibo Conservation Concession (UECC), Guyana, to assess whether associations occurred more than would be expected by chance encounters and identify the factors influencing their formation. Cuxius showed a high degree of inter-site variation in the frequency of time spent in association (ranging from 2 to 26% of observation time) and duration of associations (mean duration from 22 min to 2.5 hr). Sapajus apella was the most common association partner at most sites. At BDFFP, cuxius formed associations more frequently but not for longer duration than expected by chance. For much of the year at UECC, associations were not more frequent or longer than chance. However, during the dry season, cuxius formed associations with S. apella significantly more often and for longer duration than predicted by chance. Cuxius at UECC formed associations significantly more often when in smaller subgroups and when foraging for insects, and alarm called significantly less frequently during associations. We suggest cuxius form mixed-species associations at some sites as an adaptive strategy to decrease predation risk and/or increase foraging efficiency. Am. J. Primatol. 78: 583-597, 2016. (C) 2015 Wiley Periodicals, Inc. C1 [Shaffer, Christopher A.] Grand Valley State Univ, Dept Anthropol, Allendale, MI 49401 USA. [Barnett, Adrian A.] Roehampton Univ, Ctr Res Evolutionary & Environm Anthropol, London, England. [Barnett, Adrian A.] Natl Inst Amazonian Res, Biodivers Unit, Manaus, Amazonas, Brazil. [Gregory, Tremaine] Ctr Conservat Educ & Sustainabil, Smithsonian Conservat Biol Inst, Washington, DC USA. [De Melo, Fabiano; Moreira, Leandro; Alvim, Thiago H. G.; Filo, Anderson; Cardoso, Tatiane] Univ Fed Goias, Res Aid Fdn, Goiania, Go, Brazil. [Moura, Viviane S.] Univ Fed Sergipe, Postgrad Program Ecol & Conservat, Sao Cristovao, Sergipe, Brazil. [Port-Carvalho, Marcio] Estacao Expt Bauru, Inst Florestal Sao Paulo, Sao Paulo, SP, Brazil. [Dos Santos, Ricardo Rodrigues] Univ Fed Maranhao, Ctr Ciencias Agr & Ambientais, Chapadinha, MA, Brazil. [Dos Santos, Ricardo Rodrigues] Univ Georgia, Ctr Geospatial Res, Athens, GA 30602 USA. [Boyle, Sarah A.] Rhodes Coll, Dept Biol, Memphis, TN 38112 USA. RP Shaffer, CA (reprint author), Grand Valley State Univ, Dept Anthropol, Allendale, MI 49401 USA. EM shafferc@gvsu.edu FU National Science Foundation [0648678]; Lambda Alpha; Conservation International-Guyana FX Contract grant sponsor: National Science Foundation; contract grant number: 0648678; contract grant sponsor: Lambda Alpha; contract grant sponsor: Conservation International-Guyana NR 71 TC 0 Z9 0 U1 7 U2 11 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 MAY PY 2016 VL 78 IS 5 SI SI BP 583 EP 597 DI 10.1002/ajp.22433 PG 15 WC Zoology SC Zoology GA DJ0NU UT WOS:000373902000009 PM 26031994 ER PT J AU Plotnick, RE Smith, FA Lyons, SK AF Plotnick, Roy E. Smith, Felisa A. Lyons, S. Kathleen TI The fossil record of the sixth extinction SO ECOLOGY LETTERS LA English DT Article DE Body size; extinction; fossils; mammals; range; taphonomy ID MASS EXTINCTION; BODY-SIZE; MAMMALS; FIDELITY; TRAITS; LOSSES; EARTHS; TAXA; RISK AB Comparing the magnitude of the current biodiversity crisis with those in the fossil record is difficult without an understanding of differential preservation. Integrating data from palaeontological databases with information on IUCN status, ecology and life history characteristics of contemporary mammals, we demonstrate that only a small and biased fraction of threatened species (< 9%) have a fossil record, compared with 20% of non-threatened species. We find strong taphonomic biases related to body size and geographic range. Modern species with a fossil record tend to be large and widespread and were described in the 19th century. The expected magnitude of the current extinction based only on species with a fossil record is about half of that of one based on all modern species; values for genera are similar. The record of ancient extinctions may be similarly biased, with many species having originated and gone extinct without leaving a tangible record. C1 [Plotnick, Roy E.] Univ Illinois, Earth & Environm Sci, 845 W Taylor St, Chicago, IL USA. [Smith, Felisa A.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Lyons, S. Kathleen] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, NHB,MRC 121, POB 37012, Washington, DC 20013 USA. RP Plotnick, RE (reprint author), Univ Illinois, Earth & Environm Sci, 845 W Taylor St, Chicago, IL USA. EM plotnick@uic.edu NR 45 TC 5 Z9 5 U1 37 U2 70 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 MAY PY 2016 VL 19 IS 5 BP 546 EP 553 DI 10.1111/ele.12589 PG 8 WC Ecology SC Environmental Sciences & Ecology GA DI8YT UT WOS:000373789100006 PM 26932459 ER PT J AU Harding, LW Gallegos, CL Perry, ES Miller, WD Adolf, JE Mallonee, ME Paerl, HW AF Harding, L. W., Jr. Gallegos, C. L. Perry, E. S. Miller, W. D. Adolf, J. E. Mallonee, M. E. Paerl, H. W. TI Long-Term Trends of Nutrients and Phytoplankton in Chesapeake Bay SO ESTUARIES AND COASTS LA English DT Article DE Estuaries; Chesapeake Bay; Long-term trends; Hydrology; Eutrophication; Water quality; Phytoplankton; Nutrients; Chlorophyll ID CONTIGUOUS UNITED-STATES; NORTH-CAROLINA; COASTAL EUTROPHICATION; SYNOPTIC CLIMATOLOGY; ESTUARINE ECOSYSTEM; PAMLICO SOUND; WATER-QUALITY; RIVER ESTUARY; BIOMASS; CHLOROPHYLL AB Climate effects on hydrology impart high variability to water-quality properties, including nutrient loadings, concentrations, and phytoplankton biomass as chlorophyll-a (chl-a), in estuarine and coastal ecosystems. Resolving long-term trends of these properties requires that we distinguish climate effects from secular changes reflecting anthropogenic eutrophication. Here, we test the hypothesis that strong climatic contrasts leading to irregular dry and wet periods contribute significantly to interannual variability of mean annual values of water-quality properties using in situ data for Chesapeake Bay. Climate effects are quantified using annual freshwater discharge from the Susquehanna River together with a synoptic climatology for the Chesapeake Bay region based on predominant sea-level pressure patterns. Time series of water-quality properties are analyzed using historical (1945-1983) and recent (1984-2012) data for the bay adjusted for climate effects on hydrology. Contemporary monitoring by the Chesapeake Bay Program (CBP) provides data for a period since mid-1984 that is significantly impacted by anthropogenic eutrophication, while historical data back to 1945 serve as historical context for a period prior to severe impairments. The generalized additive model (GAM) and the generalized additive mixed model (GAMM) are developed for nutrient loadings and concentrations (total nitrogen-TN, nitrate + nitrate-NO2 + NO3) at the Susquehanna River and water-quality properties in the bay proper, including dissolved nutrients (NO2 + NO3, orthophosphate-PO4), chl-a, diffuse light attenuation coefficient (K (D) (PAR)), and chl-a/TN. Each statistical model consists of a sum of nonlinear functions to generate flow-adjusted time series and compute long-term trends accounting for climate effects on hydrology. We present results identifying successive periods of (1) eutrophication ca. 1945-1980 characterized by approximately doubled TN and NO2 + NO3 loadings, leading to increased chl-a and associated ecosystem impairments, and (2) modest decreases of TN and NO2 + NO3 loadings from 1981 to 2012, signaling a partial reversal of nutrient over-enrichment. Comparison of our findings with long-term trends of water-quality properties for a variety of estuarine and coastal ecosystems around the world reveals that trends for Chesapeake Bay are weaker than for other systems subject to strenuous management efforts, suggesting that more aggressive actions than those undertaken to date will be required to counter anthropogenic eutrophication of this valuable resource. C1 [Harding, L. W., Jr.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. [Gallegos, C. L.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. [Perry, E. S.] 2000 Kings Landing Rd, Huntingtown, MD 20639 USA. [Miller, W. D.] US Navy, Res Lab, 4555 Overlook Ave SW, Washington, DC 20375 USA. [Adolf, J. E.] Univ Hawaii, Marine Sci Program, 200 W Kawili St, Hilo, HI 96720 USA. [Mallonee, M. E.] US EPA, Chesapeake Bay Program Off, Interstate Commiss Potomac River Basin, 410 Severn Ave, Annapolis, MD 21403 USA. [Paerl, H. W.] Univ North Carolina Chapel Hill, Inst Marine Sci, 3431 Arendell St, Morehead City, NC 28557 USA. RP Harding, LW (reprint author), Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. EM lharding@atmos.ucla.edu OI Gallegos, Charles/0000-0001-5112-0166; Miller, W. David/0000-0002-4940-5987 FU NSF Biological Oceanography Program; NOAA Chesapeake Bay Program Office; North Carolina Department of Environment and Natural Resources; ModMon and FerryMon Projects; Strategic Environmental Defense and Development Program (SERDP) of the Department of Defense FX Our thanks to Dr. Jim Hagy of the EPA Gulf Breeze Laboratory for providing data from his Ph.D. Dissertation and to Dr. Bob Hirsch and his colleagues at the US Geological Survey for providing data on nutrient concentrations and loadings from the Nontidal Monitoring Program. Rich Batiuk and Gary Shenk of the EPA Chesapeake Bay Program provided point-source nutrient estimates and helpful comments on the manuscript. Detailed comments and suggestions by two anonymous reviewers significantly improved the manuscript. LWH was supported by the NSF Biological Oceanography Program and the NOAA Chesapeake Bay Program Office. HWP was supported by the NSF Biological Oceanography Program, the North Carolina Department of Environment and Natural Resources, ModMon and FerryMon Projects, and the Strategic Environmental Defense and Development Program (SERDP) of the Department of Defense. NR 72 TC 4 Z9 4 U1 19 U2 69 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 EI 1559-2731 J9 ESTUAR COAST JI Estuaries Coasts PD MAY PY 2016 VL 39 IS 3 BP 664 EP 681 DI 10.1007/s12237-015-0023-7 PG 18 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA DI2WS UT WOS:000373360500006 ER PT J AU Halabisky, M Moskal, LM Gillespie, A Hannam, M AF Halabisky, Meghan Moskal, L. Monika Gillespie, Alan Hannam, Michael TI Reconstructing semi-arid wetland surface water dynamics through spectral mixture analysis of a time series of Landsat satellite images (1984-2011) SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Time series; Landsat; Wetlands; Hydrology; Hydroperiod; High resolution; OBIA; Object-based image analysis; Hydrograph; Monitoring; Sub-pixel ID PRAIRIE POTHOLE REGION; CLIMATE-CHANGE; FORESTED WETLANDS; UNITED-STATES; NORTH-DAKOTA; CLASSIFICATION; LIDAR; HYDROPERIOD; VARIABILITY; BATHYMETRY AB Wetlands are valuable ecosystems for maintaining biodiversity, but are vulnerable to climate change and land conversion. Despite their importance, wetland hydrology is poorly understood as few tools exist to monitor their hydrologic regime at a landscape scale. This is especially true when monitoring hydrologic change at scales below 30 m, the resolution of one Landsat pixel. To address this, we used spectral mixture analysis (SMA) of a time series of Landsat satellite imagery to reconstruct surface-water hydrographs for 750 wetlands in Douglas County, Washington State, USA, from 1984 to 2011. SMA estimates the fractional abundance of spectra representing physically meaningful materials, known as spectral endmembers, which comprise a mixed pixel, thus providing sub-pixel estimates of surface water extent Endmembers for water and sage steppe were selected directly from each image scene in the Landsat time series, whereas endmembers for salt and wetland vegetation were derived from a mean spectral signature of selected dates spanning the 1984-2011 timeframe. This method worked well (R-2 = 0.99) for even small wetlands (<1800 m(2)) providing a wall-to-wall dataset of reconstructed surface-water hydrographs for wetlands across our study area. We have validated this method only in semi-arid regions. Further research is necessary to extend its validity to other environments. This method can be used to better understand the role of hydrology in wetland ecosystems and as a monitoring tool to identify wetlands undergoing abnormal change. (C) 2016 Elsevier Inc. All rights reserved. C1 [Halabisky, Meghan; Moskal, L. Monika] Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA. [Gillespie, Alan] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Hannam, Michael] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RP Halabisky, M (reprint author), Box 352100, Seattle, WA 98195 USA. EM halabisk@uw.edu RI Hannam, Michael/M-7332-2016; Moskal, L. Monika/F-8715-2010 OI Hannam, Michael/0000-0002-4589-5181; Halabisky, Meghan/0000-0002-1174-2486; Moskal, L. Monika/0000-0003-1563-6506 FU United States Geological Survey, Department of the Interior Northwest Climate Science Center (USGS grant) [GS276A-AUSGS]; University of Washington Precision Forestry Cooperative FX This research was funded by the United States Geological Survey, Department of the Interior Northwest Climate Science Center (USGS grant #GS276A-AUSGS), and the University of Washington Precision Forestry Cooperative. The authors would like to thank Chris Vondrasek and Max Sugarman for their assistance with field work and manual photo interpretation of wetlands and Maureen Ryan and Aaron Johnston for their valuable feedback on this manuscript. Additionally, the authors would like to thank the anonymous reviewers and Associate Editor Tim McVicar for their helpful feedback on an earlier draft. NR 66 TC 3 Z9 3 U1 10 U2 30 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAY PY 2016 VL 177 BP 171 EP 183 DI 10.1016/j.rse.2016.02.040 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA DI5PC UT WOS:000373550100015 ER PT J AU Anderson-Teixeira, KJ Wang, MMH McGarvey, JC LeBauer, DS AF Anderson-Teixeira, Kristina J. Wang, Maria M. H. McGarvey, Jennifer C. LeBauer, David S. TI Carbon dynamics of mature and regrowth tropical forests derived from a pantropical database (TropForC-db) SO GLOBAL CHANGE BIOLOGY LA English DT Review DE biomass; carbon cycle; net ecosystem exchange; productivity; regeneration; secondary; tropical forest ID NET PRIMARY PRODUCTION; AMAZONIAN RAIN-FOREST; ABOVEGROUND BIOMASS ACCUMULATION; NATURAL PLANT-COMMUNITIES; GROSS PRIMARY PRODUCTION; SOUTH-WESTERN NIGERIA; SOIL CO2 EFFLUX; SECONDARY FORESTS; LAND-USE; SHIFTING CULTIVATION AB Tropical forests play a critical role in the global carbon (C) cycle, storing similar to 45% of terrestrial C and constituting the largest component of the terrestrial C sink. Despite their central importance to the global C cycle, their ecosystem-level C cycles are not as well-characterized as those of extra-tropical forests, and knowledge gaps hamper efforts to quantify C budgets across the tropics and to model tropical forest-climate interactions. To advance understanding of C dynamics of pantropical forests, we compiled a new database, the Tropical Forest C database (TropForC-db), which contains data on ground-based measurements of ecosystem-level C stocks and annual fluxes along with disturbance history. This database currently contains 3568 records from 845 plots in 178 geographically distinct areas, making it the largest and most comprehensive database of its type. Using TropForC-db, we characterized C stocks and fluxes for young, intermediate-aged, and mature forests. Relative to existing C budgets of extra-tropical forests, mature tropical broadleaf evergreen forests had substantially higher gross primary productivity (GPP) and ecosystem respiration (R-eco), their autotropic respiration (R-a) consumed a larger proportion (similar to 67%) of GPP, and their woody stem growth (ANPP(stem)) represented a smaller proportion of net primary productivity (NPP, similar to 32%) or GPP (similar to 9%). In regrowth stands, aboveground biomass increased rapidly during the first 20years following stand-clearing disturbance, with slower accumulation following agriculture and in deciduous forests, and continued to accumulate at a slower pace in forests aged 20-100years. Most other C stocks likewise increased with stand age, while potential to describe age trends in C fluxes was generally data-limited. We expect that TropForC-db will prove useful for model evaluation and for quantifying the contribution of forests to the global C cycle. The database version associated with this publication is archived in Dryad (DOI: 10.5061/dryad.t516f) and a dynamic version is maintained at https://github.-com/forc-db. C1 [Anderson-Teixeira, Kristina J.; Wang, Maria M. H.; McGarvey, Jennifer C.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. [Anderson-Teixeira, Kristina J.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci Forest Global Earth Observ, Apartado 0843-03092, Panama City, Panama. [LeBauer, David S.] Univ Illinois, Carl Woese Inst Genom Biol, 1206 W Gregory Dr, Urbana, IL 61801 USA. RP Anderson-Teixeira, KJ (reprint author), Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA.; Anderson-Teixeira, KJ (reprint author), Smithsonian Trop Res Inst, Ctr Trop Forest Sci Forest Global Earth Observ, Apartado 0843-03092, Panama City, Panama. EM teixeirak@si.edu RI LeBauer, David/N-2735-2013 OI LeBauer, David/0000-0001-7228-053X FU DOE [DE-SC0008085, DE-SC0010039]; Smithsonian Women's Committee grant FX We thank all authors of the original studies and data compilations included in this database, their funding agencies, and the various networks that support ground-based measurements of C stocks and fluxes in the tropics, without which this database or the type of integrated analyses conducted here would not be possible. We also acknowledge all authors of previous data compilations, particularly Sebastian Luyssaert, for their key role in synthesizing data upon which this database draws. Thanks to Moein Azimi, Amy C. Bennett, Syed Ashraful Alam, and Markku Larjavaara for help assembling data, to Yadvinder Malhi communication regarding data, to Jens Kattge for helpful discussion, and to Erika Gonzalez-Akre, Adam Miller, and two anonymous reviewers for helpful comments on the manuscript. This research was funded by DOE grants DE-SC0008085 and DE-SC0010039 to KAT, Evan DeLucia, and Benjamin Duval and by a Smithsonian Women's Committee grant to KAT. NR 236 TC 3 Z9 3 U1 24 U2 60 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD MAY PY 2016 VL 22 IS 5 BP 1690 EP 1709 DI 10.1111/gcb.13226 PG 20 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA DH9QL UT WOS:000373130700002 PM 26790568 ER PT J AU Velbel, MA AF Velbel, Michael A. TI Aqueous corrosion of olivine in the Mars meteorite Miller Range (MIL) 03346 during Antarctic weathering: Implications for water on Mars SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID NAKHLITE MARTIAN METEORITES; PRESENT-DAY SERPENTINIZATION; MCMURDO DRY VALLEYS; RAY EXPOSURE AGES; ETCH-PITS; FORSTERITE DISSOLUTION; ALTERATION ASSEMBLAGES; LAFAYETTE METEORITE; MINERAL ASSEMBLAGES; SURFACE CONDITIONS AB Several nakhlites (clinopyroxenite meteorites from Mars) contain olivine phenocrysts with corrosion features identical in size, shape and distribution to the smaller etch-pits of well-characterized weathered terrestrial olivine. Miller Range (MIL) 03346 is an Antarctic nakhlite find, recovered after long exposure to Antarctic conditions. The distribution of discrete olivine etch-pits almost exclusively within a few hundred microns of allocation MIL 03346,171's documentably exposed surface suggests that they formed by terrestrial weathering in Antarctica. The small size of olivine etch-pits in MIL 03346,171 relative to commonly much larger etch-pits in even incipiently weathered terrestrial examples suggests that the duration of its exposure to weathering conditions was short, or the weathering conditions to which it was exposed did not favor olivine corrosion (in the form of etch-pit formation), or both. Time-scales for the formation of etch-pits, estimated from experimentally determined dissolution rates of olivine over a range of pHs, are comparable to the measured terrestrial age of the meteorite and short relative to the time available for possible similar corrosion on Mars. Etch-pits of the observed size on MIL 03346 olivine phenocrysts would be relatively easy to form supraglacially under brief episodic acidic Antarctic conditions, but the terrestrial age of MIL 03346 is long enough that its olivine might have been weathered to the observed state by englacial films of alkaline Antarctic water. The paucity of similar etch-pits in olivine from the interior of MIL 03346 suggests that olivine in this Mars meteorite was exposed to even less aqueous alteration after iddingsitization during its 1.3 billion years on Mars than its exterior was subjected to during its Pleistocene-Holocene exposure to Antarctic weathering conditions. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Velbel, Michael A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Div Meteorites, 10th & Constitut Ave NW, Washington, DC 20560 USA. [Velbel, Michael A.] Michigan State Univ, Dept Geol Sci, 207 Nat Sci Bldg,288 Farm Lane, E Lansing, MI 48824 USA. RP Velbel, MA (reprint author), Michigan State Univ, Dept Geol Sci, 207 Nat Sci Bldg,288 Farm Lane, E Lansing, MI 48824 USA. EM velbel@msu.edu FU NSF [EAR 91-17099, EAR 94-17325, EAR 99-09493]; NASA [NAG 9-1211, NNG05GL77G] FX I thank Susan J. Wentworth, David S. McKay, Ed Vicenzi, Cari Corrigan, Jeff Taylor, Julie Stopar, Lydia Hallis, Theresa Longazo, Lina C. Patino, Lauren M. Spencer, Marc Caffee, Angela R. Donatelle, Daniel R. Snyder, Anna I. Losiak, Benjamin L. Brugman, and Bernard P. Boudreau for helpful discussions; Ewa Danielewicz (Michigan State University Center for Advanced Microscopy) for assistance with some of the scanning electron microscopy; Kunihiko Nishiizumi for the terrestrial age of MIL 03346; the Meteorite Working Group and the staff of the Astromaterials Acquisition and Curation Office at NASA-JSC for samples; Cecilia Satterwhite and Kathleen McBride of the Astromaterials Acquisition and Curation Office at NASA-JSC for detailed allocation and processing information about MIL 03346 in general and MIL 03346,171 in particular; Martin Lee and several anonymous reviewers for their thorough, well-informed, and constructive reviews; and Harley J. Seeley for preparing the image files for publication. Collection, preparation & preliminary petrographic characterization of weathered basalt samples from Hawai'i (Fig. 2) were supported by NSF grants EAR 91-17099 & EAR 94-17325 (R. A. Berner, P. I.). Geochemical characterization of incipiently weathered terrestrially volcanic rocks that served as olivine-corrosion analogs for this study (Figs. 1 and 2) was supported by NSF grant EAR 99-09493 (L. C. Patino, P. I.; M. A. Velbel, co-P. I.). All other aspects of this research were supported by NASA Grants NAG 9-1211 and NNG05GL77G (M. A. Velbel, P. I.). This paper was written during the author's tenure as a Smithsonian Senior Fellow and Research Associate at the Division of Meteorites, Department of Mineral Sciences, National Museum of Natural History, Smithsonian Institution. I am most grateful to Cari Corrigan and Ed Vicenzi for hosting my visits. NR 156 TC 1 Z9 1 U1 5 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY 1 PY 2016 VL 180 BP 126 EP 145 DI 10.1016/j.gca.2016.01.036 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DH1TA UT WOS:000372566600008 ER PT J AU Derryberry, EP Danner, RM Danner, JE Derryberry, GE Phillips, JN Lipshutz, SE Gentry, K Luther, DA AF Derryberry, Elizabeth P. Danner, Raymond M. Danner, Julie E. Derryberry, Graham E. Phillips, Jennifer N. Lipshutz, Sara E. Gentry, Katherine Luther, David A. TI Patterns of Song across Natural and Anthropogenic Soundscapes Suggest That White-Crowned Sparrows Minimize Acoustic Masking and Maximize Signal Content SO PLOS ONE LA English DT Article ID URBAN NOISE; BEHAVIORAL PLASTICITY; VOCAL PERFORMANCE; TRAFFIC NOISE; HIGHER PITCH; BIRD SONG; COMMUNICATION; EVOLUTION; SOUND; CONSEQUENCES AB Soundscapes pose both evolutionarily recent and long-standing sources of selection on acoustic communication. We currently know more about the impact of evolutionarily recent human-generated noise on communication than we do about how natural sounds such as pounding surf have shaped communication signals over evolutionary time. Based on signal detection theory, we hypothesized that acoustic phenotypes will vary with both anthropogenic and natural background noise levels and that similar mechanisms of cultural evolution and/or behavioral flexibility may underlie this variation. We studied song characteristics of white-crowned sparrows (Zonotrichia leucophrys nuttalli) across a noise gradient that includes both anthropogenic and natural sources of noise in San Francisco and Marin counties, California, USA. Both anthropogenic and natural soundscapes contain high amplitude low frequency noise (traffic or surf, respectively), so we predicted that birds would produce songs with higher minimum frequencies in areas with higher amplitude background noise to avoid auditory masking. We also anticipated that song minimum frequencies would be higher than the projected lower frequency limit of hearing based on site-specific masking profiles. Background noise was a strong predictor of song minimum frequency, both within a local noise gradient of three urban sites with the same song dialect and cultural evolutionary history, and across the regional noise gradient, which encompasses 11 urban and rural sites, several dialects, and several anthropogenic and natural sources of noise. Among rural sites alone, background noise tended to predict song minimum frequency, indicating that urban sites were not solely responsible for driving the regional pattern. These findings support the hypothesis that songs vary with local and regional soundscapes regardless of the source of noise. Song minimum frequency from five core study sites was also higher than the lower frequency limit of hearing at each site, further supporting the hypothesis that songs vary to transmit through noise in local soundscapes. Minimum frequencies leveled off at noisier sites, suggesting that minimum frequencies are constrained to an upper limit, possibly to retain the information content of wider bandwidths. We found evidence that site noise was a better predictor of song minimum frequency than territory noise in both anthropogenic and natural soundscapes, suggesting that cultural evolution rather than immediate behavioral flexibility is responsible for local song variation. Taken together, these results indicate that soundscapes shape song phenotype across both evolutionarily recent and long-standing soundscapes. C1 [Derryberry, Elizabeth P.; Danner, Julie E.; Phillips, Jennifer N.; Lipshutz, Sara E.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Danner, Raymond M.; Gentry, Katherine; Luther, David A.] George Mason Univ, Dept Biol, Fairfax, VA 22030 USA. [Derryberry, Graham E.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Luther, David A.] Natl Zoo, Smithsonian Inst, Smithsonian Migratory Bird Ctr, Washington, DC USA. [Danner, Raymond M.] Univ N Carolina, Dept Biol & Marine Biol, Wilmington, NC 28401 USA. RP Derryberry, EP (reprint author), Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. EM ederrybe@tulane.edu FU National Science Foundation [1354763]; National Science Foundation Integrative Organismal Systems [1354756] FX This study was supported by the National Science Foundation, award #1354763 (DAL) and the National Science Foundation Integrative Organismal Systems, award #1354756 (EDP), www.nsf.gov. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 75 TC 1 Z9 1 U1 14 U2 30 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 29 PY 2016 VL 11 IS 4 AR e0154456 DI 10.1371/journal.pone.0154456 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DK8XM UT WOS:000375212600031 PM 27128443 ER PT J AU Gregoric, M Suen, K Cheng, RC Kralj-Fiser, S Kuntner, M AF Gregoric, Matjaz Suen, Klavdija Cheng, Ren-Chung Kralj-Fiser, Simona Kuntner, Matjaz TI Spider behaviors include oral sexual encounters SO SCIENTIFIC REPORTS LA English DT Article ID SPERM COMPETITION; ARANEAE ARANEIDAE; NEPHILID SPIDERS; DROSOPHILA; EMASCULATION; COEVOLUTION; COPULATION; CAEROSTRIS; DIMORPHISM; EVOLUTION AB Several clades of spiders whose females evolved giant sizes are known for extreme sexual behaviors such as sexual cannibalism, opportunistic mating, mate-binding, genital mutilation, plugging, and emasculation. However, these behaviors have only been tested in a handful of size dimorphic spiders. Here, we bring another lineage into the picture by reporting on sexual behavior of Darwin's bark spider, Caerostris darwini. This sexually size dimorphic Madagascan species is known for extreme web gigantism and for producing the world's toughest biomaterial. Our field and laboratory study uncovers a rich sexual repertoire that predictably involves cannibalism, genital mutilation, male preference for teneral females, and emasculation. Surprisingly, C. darwini males engage in oral sexual encounters, rarely reported outside mammals. Irrespective of female's age or mating status males salivate onto female genitalia pre-, during, and post-copulation. While its adaptive significance is elusive, oral sexual contact in spiders may signal male quality or reduce sperm competition. C1 [Gregoric, Matjaz; Suen, Klavdija; Cheng, Ren-Chung; Kralj-Fiser, Simona; Kuntner, Matjaz] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Ljubljana, Slovenia. [Kuntner, Matjaz] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Gregoric, M (reprint author), Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Ljubljana, Slovenia. EM matjaz.gregoric@gmail.com FU Slovenian Research Agency; Explorers Club FX This work was funded by the Slovenian Research Agency and the Explorers Club. We thank the MICET crew in Antananarivo, S. L. Rahanitriniaina and H. Nono Rabarison for help in the field, and T. Celik and T. Lokovsek for analytical and lab help. NR 40 TC 0 Z9 0 U1 8 U2 14 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 APR 29 PY 2016 VL 6 AR 25128 DI 10.1038/srep25128 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DK8MI UT WOS:000375180400001 PM 27126507 ER PT J AU Damaska, A Konstantinov, A AF Damaska, Albert Konstantinov, Alexander TI A new species of Cangshanaltica Konstantinov et al., a moss-inhabiting flea beetle from Thailand (Coleoptera: Chrysomelidae: Galerucinae: Alticini) SO ZOOTAXA LA English DT Editorial Material C1 [Damaska, Albert] Charles Univ Prague, Fac Sci, Dept Zool, Vinicna 7, Prague 12844 2, Czech Republic. [Konstantinov, Alexander] ARS, Systemat Entomol Lab, USDA, Smithsonian Inst,Natl Museum Nat Hist, MRC 168, Washington, DC USA. RP Damaska, A (reprint author), Charles Univ Prague, Fac Sci, Dept Zool, Vinicna 7, Prague 12844 2, Czech Republic.; Konstantinov, A (reprint author), ARS, Systemat Entomol Lab, USDA, Smithsonian Inst,Natl Museum Nat Hist, MRC 168, Washington, DC USA. EM albert.damaska@natur.cuni.cz; alex.konstantinov@ars.usda.gov NR 1 TC 0 Z9 0 U1 4 U2 5 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 29 PY 2016 VL 4107 IS 1 BP 93 EP 97 PG 5 WC Zoology SC Zoology GA DK9TX UT WOS:000375275600007 PM 27394809 ER PT J AU Weider, SZ Nittler, LR Murchie, SL Peplowski, PN Mccoy, TJ Kerber, L Klimczak, C Ernst, CM Goudge, TA Starr, RD Izenberg, NR Klima, RL Solomon, SC AF Weider, Shoshana Z. Nittler, Larry R. Murchie, Scott L. Peplowski, Patrick N. Mccoy, Timothy J. Kerber, Laura Klimczak, Christian Ernst, Carolyn M. Goudge, Timothy A. Starr, Richard D. Izenberg, Noam R. Klima, Rachel L. Solomon, Sean C. TI Evidence from MESSENGER for sulfur- and carbon-driven explosive volcanism on Mercury SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID X-RAY SPECTROMETER; MAGMA VOLATILE CONTENT; SPECTRAL REFLECTANCE; ERUPTION CONDITIONS; PLANETS FORMATION; IMPACT CRATERS; CALORIS BASIN; MARINER 10; SURFACE; EVOLUTION AB Targeted MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) X-Ray Spectrometer measurements of Mercury's largest identified pyroclastic deposit are combined with neutron and reflectance spectroscopy data to constrain the composition of volatiles involved in the eruption that emplaced the pyroclastic material. The deposit, northeast of the Rachmaninoff basin, is depleted in S (relative to Ca and Si) and C, compared with the rest of Mercury's surface. Spectral reflectance measurements of the deposit indicate relatively high overall reflectance and an oxygen-metal charge transfer (OMCT) absorption band at ultraviolet wavelengths. These results are consistent with oxidation of graphite and sulfides during magma ascent, via reaction with oxides in the magma or assimilated country rock, and the formation of S-and C-bearing volatile species. Consumption of graphite during oxidation could account for the elevated reflectance of the pyroclastic material, and the strength of the OMCT band is consistent with similar to 0.03-0.1 wt% FeO in the deposit. C1 [Weider, Shoshana Z.; Nittler, Larry R.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Murchie, Scott L.; Peplowski, Patrick N.; Ernst, Carolyn M.; Izenberg, Noam R.; Klima, Rachel L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Mccoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Kerber, Laura] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Klimczak, Christian] Univ Georgia, Dept Geol, Athens, GA 30602 USA. [Goudge, Timothy A.] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA. [Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. RP Weider, SZ (reprint author), Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. EM sweider@carnegiescience.edu RI Murchie, Scott/E-8030-2015; Ernst, Carolyn/I-4902-2012 OI Murchie, Scott/0000-0002-1616-8751; FU NASA [NAS5-97271, NASW-00002] FX We thank the MESSENGER engineering and instrument teams for the successful operation of the MESSENGER spacecraft and payload. This work 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. We acknowledge Elizabeth Frank, Ellen Crapster-Pregont, and Audrey Vorburger for analysis of the global XRS data set, Malcolm Rutherford for insightful comments, as well as Mikhail Zolotov and David Rothery for helpful reviews. All MESSENGER data used in this paper are publicly available at the NASA Planetary Data System. NR 58 TC 2 Z9 2 U1 5 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD APR 28 PY 2016 VL 43 IS 8 BP 3653 EP 3661 DI 10.1002/2016GL068325 PG 9 WC Geosciences, Multidisciplinary SC Geology GA DP2RQ UT WOS:000378338800005 ER PT J AU Cong, Q Shen, JH Borek, D Robbins, RK Otwinowski, Z Grishin, NV AF Cong, Qian Shen, Jinhui Borek, Dominika Robbins, Robert K. Otwinowski, Zbyszek Grishin, Nick V. TI Complete genomes of Hairstreak butterflies, their speciation, and nucleo-mitochondrial incongruence SO SCIENTIFIC REPORTS LA English DT Article ID DNA-SEQUENCING DATA; REPETITIVE ELEMENTS; READ ALIGNMENT; RNA-SEQ; GENE; GENERATION; IDENTIFICATION; LEPIDOPTERA; DROSOPHILA; EVOLUTION AB Comparison of complete genomes of closely related species enables research on speciation and how phenotype is determined by genotype. Lepidoptera, an insect order of 150,000 species with diverse phenotypes, is well-suited for such comparative genomics studies if new genomes, which cover additional Lepidoptera families are acquired. We report a 729 Mbp genome assembly of the Calycopis cecrops, the first genome from the family Lycaenidae and the largest available Lepidoptera genome. As detritivore, Calycopis shows expansion in detoxification and digestion enzymes. We further obtained complete genomes of 8 Calycopis specimens: 3 C. cecrops and 5 C. isobeon, including a dry specimen stored in the museum for 30 years. The two species differ subtly in phenotype and cannot be differentiated by mitochondrial DNA. However, nuclear genomes revealed a deep split between them. Genes that can clearly separate the two species (speciation hotspots) mostly pertain to circadian clock, mating behavior, transcription regulation, development and cytoskeleton. The speciation hotspots and their function significantly overlap with those we previously found in Pterourus, suggesting common speciation mechanisms in these butterflies. C1 [Cong, Qian; Shen, Jinhui; Borek, Dominika; Otwinowski, Zbyszek; Grishin, Nick V.] Univ Texas SW Med Ctr Dallas, Dept Biophys & Biochem, 5323 Harry Hines Blvd, Dallas, TX 75390 USA. [Robbins, Robert K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012,NHB Stop 105, Washington, DC 20013 USA. [Grishin, Nick V.] Univ Texas SW Med Ctr Dallas, Howard Hughes Med Inst, 5323 Harry Hines Blvd, Dallas, TX 75390 USA. RP Grishin, NV (reprint author), Univ Texas SW Med Ctr Dallas, Dept Biophys & Biochem, 5323 Harry Hines Blvd, Dallas, TX 75390 USA.; Grishin, NV (reprint author), Univ Texas SW Med Ctr Dallas, Howard Hughes Med Inst, 5323 Harry Hines Blvd, Dallas, TX 75390 USA. EM grishin@chop.swmed.edu RI Borek, Dominika/D-2943-2011 OI Borek, Dominika/0000-0002-4321-6253 FU National Institutes of Health [GM094575]; Welch Foundation [I-1505] FX We acknowledge Texas Parks and Wildlife Department (Natural Resources Program Director David H. Riskind) for the permit #08-02Rev that makes research based on material collected in Texas State Parks possible. We thank Lisa N. Kinch, R. Dustin Schaeffer and Raquel Bromberg for critical suggestions and proofreading of the manuscript; John M. Burns and Brian Harris (National Museum of Natural History, Smithsonian Institution, Washington DC), Edward G. Riley (Texas A & M University insect collection, College Station, TX), for facilitating access to the collections under their care and stimulating discussions. Qian Cong is a Howard Hughes Medical Institute International Student Research fellow. This work was supported in part by the National Institutes of Health (GM094575 to NVG) and the Welch Foundation (I-1505 to NVG). NR 82 TC 1 Z9 1 U1 4 U2 12 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 APR 28 PY 2016 VL 6 AR 24863 DI 10.1038/srep24863 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DK5JM UT WOS:000374956200001 PM 27120974 ER PT J AU McMillan, EC Shen, G McCann, JF McLaughlin, BM Stancil, PC AF McMillan, E. C. Shen, G. McCann, J. F. McLaughlin, B. M. Stancil, P. C. TI Rovibrationally resolved photodissociation of SH+ SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article DE 33.80.Gj; 34.20.-b; 95.30.Ky ID INTERSTELLAR CLOUDS; CHEMISTRY; IONS; ABSORPTION; REGIONS; SIH+; CH+ AB Photodissociation cross sections for the SH+ radical are computed from all rovibrational (RV) levels of the ground electronic state X (3)Sigma(-) for wavelengths from threshold to 500 angstrom. The five electronic transitions, 2 (3)Sigma(-) <- X (3)Sigma(-), 3 (3)Sigma(-) <- X (3)Sigma(-), A (3)Pi <- X (3)Sigma(-), 2 (3)Pi <- X (3)Sigma(-), and 3 3P <- X (3)Sigma(-), are treated with a fully quantum-mechanical two-state model, i.e. nonadiabatic couplings between excited states were not included. The photodissociation calculations incorporate adiabatic potentials and transition dipole moment functions computed in the multireference configuration interaction approach along with the Davidson correction (MRCI + Q), but adjusted to match available experimental molecular data and asymptotic atomic limits. Local thermodynamic equilibrium (LTE) photodissociation cross sections were computed which assume a Boltzmann distribution of RV levels in the X (3)Sigma(-) molecular state of the SH+ cation. The LTE cross sections are presented for temperatures in the range 1000-10 000 K. Applications of the current photodissociation cross sections to interstellar gas, photon-dominated regions, and stellar atmospheres are briefly discussed. C1 [McMillan, E. C.; Shen, G.; Stancil, P. C.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [McMillan, E. C.; Shen, G.; Stancil, P. C.] Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. [Shen, G.] Inst Appl Phys & Computat Math, Beijing 100094, Peoples R China. [McCann, J. F.; McLaughlin, B. M.] Queens Univ Belfast, Sch Math & Phys, Ctr Theoret Atom & Mol Phys CTAMOP, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, MS-14, Cambridge, MA 02138 USA. RP Stancil, PC (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.; Stancil, PC (reprint author), Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA.; McLaughlin, BM (reprint author), Queens Univ Belfast, Sch Math & Phys, Ctr Theoret Atom & Mol Phys CTAMOP, Belfast BT7 1NN, Antrim, North Ireland.; McLaughlin, BM (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, MS-14, Cambridge, MA 02138 USA. EM bmclaughlin899@btinternet.com; stancil@physast.uga.edu FU UGA Center for Undergraduate Research Opportunities; NASA through Space Telescope Science Institute [HST-AR-11776.01-A]; NASA [NAS5-26555]; Queen's University Belfast; US National Science Foundation FX ECMcM acknowledges support from the UGA Center for Undergraduate Research Opportunities. GS acknowledges travel support by the International Cooperation and Exchange Foundation of CAEP. PCS acknowledges partial support from HST-AR-11776.01-A which 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 hospitality of the University of Georgia (UGA) is gratefully acknowledged by BMMcL during recent research visits. BMMcL also thanks Queen's University Belfast for the award of a Visiting Research Fellowship (VRF). PCS and BMMcL thank the US National Science Foundation under the visitors program through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics. Grants of computational time at the National Energy Research Scientific Computing Center in Oakland, CA, USA and at the High Performance Computing Center Stuttgart (HLRS) of the University of Stuttgart, Stuttgart, Germany are gratefully acknowledged. NR 37 TC 0 Z9 0 U1 5 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD APR 28 PY 2016 VL 49 IS 8 AR 084001 DI 10.1088/0953-4075/49/8/084001 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA DJ2DV UT WOS:000374014800002 ER PT J AU Chisholm, RA Fung, T Chimalakonda, D O'Dwyer, JP AF Chisholm, Ryan A. Fung, Tak Chimalakonda, Deepthi O'Dwyer, James P. TI Maintenance of biodiversity on islands SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE island biogeography; small-island effect; biodiversity; colonization-extinction balance; niche structure ID SPECIES-AREA RELATIONSHIP; TEMPORAL VARIABILITY; TROPICAL FORESTS; DIVERSITY; MODEL; DISPERSAL; ECOLOGY; NICHE; FRAGMENTATION; DISTRIBUTIONS AB MacArthur and Wilson's theory of island biogeography predicts that island species richness should increase with island area. This prediction generally holds among large islands, but among small islands species richness often varies independently of island area, producing the so-called 'small-island effect' and an overall biphasic species-area relationship (SAR). Here, we develop a unified theory that explains the biphasic island SAR. Our theory's key postulate is that as island area increases, the total number of immigrants increases faster than niche diversity. A parsimonious mechanistic model approximating these processes reproduces a biphasic SAR and provides excellent fits to 100 archipelago datasets. In the light of our theory, the biphasic island SAR can be interpreted as arising from a transition from a niche-structured regime on small islands to a colonization-extinction balance regime on large islands. The first regime is characteristic of classic deterministic niche theories; the second regime is characteristic of stochastic theories including the theory of island biogeography and neutral theory. The data furthermore confirm our theory's key prediction that the transition between the two SAR regimes should occur at smaller areas, where immigration is stronger (i.e. for taxa that are better dispersers and for archipelagos that are less isolated). C1 [Chisholm, Ryan A.; Fung, Tak; Chimalakonda, Deepthi] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. [Chisholm, Ryan A.] Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Ancon, Panama. [O'Dwyer, James P.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP Chisholm, RA (reprint author), Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore.; Chisholm, RA (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Ancon, Panama. EM ryan.chis@gmail.com FU National University of Singapore [WBS R-154-000-603-112, R-154-000-560-651] FX We received financial support from National University of Singapore grant nos. WBS R-154-000-603-112 and R-154-000-560-651. NR 48 TC 1 Z9 1 U1 15 U2 28 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD APR 27 PY 2016 VL 283 IS 1829 AR 20160102 DI 10.1098/rspb.2016.0102 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA DM2EE UT WOS:000376158600010 ER PT J AU Quinn, RA Vermeij, MJA Hartmann, AC d'Auriac, IG Benler, S Haas, A Quistad, SD Lim, YW Little, M Sandin, S Smith, JE Dorrestein, PC Rohwer, F AF Quinn, Robert A. Vermeij, Mark J. A. Hartmann, Aaron C. d'Auriac, Ines Galtier Benler, Sean Haas, Andreas Quistad, Steven D. Lim, Yan Wei Little, Mark Sandin, Stuart Smith, Jennifer E. Dorrestein, Pieter C. Rohwer, Forest TI Metabolomics of reef benthic interactions reveals a bioactive lipid involved in coral defence SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE metabolomics; coral; platelet activating factor; mass spectrometry ID PLATELET-ACTIVATING-FACTOR; PHASE-SHIFTS; CLIMATE-CHANGE; FACTOR PAF; IDENTIFICATION; ALGAE; INVERTEBRATES; INFLAMMATION; COMPETITION; REPERTOIRE AB Holobionts are assemblages of microbial symbionts and their macrobial host. As extant representatives of some of the oldest macro-organisms, corals and algae are important for understanding how holobionts develop and interact with one another. Using untargeted metabolomics, we show that non-self interactions altered the coral metabolome more than self-interactions (i.e. different or same genus, respectively). Platelet activating factor (PAF) and Lyso-PAF, central inflammatory modulators in mammals, were major lipid components of the coral holobionts. When corals were damaged during competitive interactions with algae, PAF increased along with expression of the gene encoding Lyso-PAF acetyltransferase; the protein responsible for converting Lyso-PAF to PAF. This shows that self and non-self recognition among some of the oldest extant holobionts involve bioactive lipids identical to those in highly derived taxa like humans. This further strengthens the hypothesis that major players of the immune response evolved during the pre-Cambrian. C1 [Quinn, Robert A.; Hartmann, Aaron C.; d'Auriac, Ines Galtier; Benler, Sean; Haas, Andreas; Quistad, Steven D.; Lim, Yan Wei; Little, Mark; Rohwer, Forest] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. [Quinn, Robert A.; Dorrestein, Pieter C.] Univ Calif San Diego, Skaggs Sch Pharm & Pharmaceut Sci, Collaborat Mass Spectrometry Innovat Ctr, La Jolla, CA 92093 USA. [Vermeij, Mark J. A.] Carmabi Fdn, Willemstad, Curacao, Neth Antilles. [Vermeij, Mark J. A.] Univ Amsterdam, IBED, Aquat Microbiol, Amsterdam, Netherlands. [Hartmann, Aaron C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Sandin, Stuart; Smith, Jennifer E.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Quinn, RA (reprint author), San Diego State Univ, Dept Biol, San Diego, CA 92182 USA.; Quinn, RA (reprint author), Univ Calif San Diego, Skaggs Sch Pharm & Pharmaceut Sci, Collaborat Mass Spectrometry Innovat Ctr, La Jolla, CA 92093 USA. EM rquinn@ucsd.edu OI Quinn, Robert/0000-0002-9829-3256; Quistad, Steven/0000-0003-4384-8100 FU NSF Partnerships for International Research and Education (PIRE) Grant [124351]; NSF Dimensions Grant [DEB-1046413]; Gordon and Betty Moore Foundation [GBMF-3781]; Canadian Institute for Advanced Research [IMB-ROHW-141679]; Cystic Fibrosis Research Inc. FX This work was supported by NSF Partnerships for International Research and Education (PIRE) Grant (124351; F.R.), NSF Dimensions Grant (DEB-1046413; Edwards and F.R.), the Gordon and Betty Moore Foundation (GBMF-3781; F.R.), the Canadian Institute for Advanced Research (IMB-ROHW-141679) and the Cystic Fibrosis Research Inc. (R.A.Q.). NR 62 TC 1 Z9 1 U1 7 U2 12 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD APR 27 PY 2016 VL 283 IS 1829 AR 20160469 DI 10.1098/rspb.2016.0469 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA DM2EE UT WOS:000376158600021 ER PT J AU Howard, MG McDonald, WJF Forster, PI Kress, WJ Erickson, D Faith, DP Shapcott, A AF Howard, Marion G. McDonald, William J. F. Forster, Paul I. Kress, W. John Erickson, David Faith, Daniel P. Shapcott, Alison TI Patterns of Phylogenetic Diversity of Subtropical Rainforest of the Great Sandy Region, Australia Indicate Long Term Climatic Refugia SO PLOS ONE LA English DT Article ID MULTIPLE SEQUENCE ALIGNMENT; FRASER ISLAND; BIODIVERSITY HOTSPOT; TREES; DIVERSIFICATION; BIOGEOGRAPHY; QUEENSLAND; ENDEMISM; FRAGMENTATION; HETEROGENEITY AB Australia's Great Sandy Region is of international significance containing two World Heritage areas and patches of rainforest growing on white sand. Previous broad-scale analysis found the Great Sandy biogeographic subregion contained a significantly more phylogenetically even subset of species than expected by chance contrasting with rainforest on white sand in Peru. This study aimed to test the patterns of rainforest diversity and relatedness at a finer scale and to investigate why we may find different patterns of phylogenetic evenness compared with rainforests on white sands in other parts of the world. This study focussed on rainforest sites within the Great Sandy and surrounding areas in South East Queensland (SEQ), Australia. We undertook field collections, expanded our three-marker DNA barcode library of SEQ rainforest plants and updated the phylogeny to 95% of the SEQ rainforest flora. We sampled species composition of rainforest in fixed area plots from 100 sites. We calculated phylogenetic diversity (PD) measures as well as species richness (SR) for each rainforest community. These combined with site variables such as geology, were used to evaluate patterns and relatedness. We found that many rainforest communities in the Great Sandy area were significantly phylogenetically even at the individual site level consistent with a broader subregion analysis. Sites from adjacent areas were either not significant or were significantly phylogenetically clustered. Some results in the neighbouring areas were consistent with historic range expansions. In contrast with expectations, sites located on the oldest substrates had significantly lower phylogenetic diversity (PD). Fraser Island was once connected to mainland Australia, our results are consistent with a region geologically old enough to have continuously supported rainforest in refugia. The interface of tropical and temperate floras in part also explains the significant phylogenetic evenness and higher than expected phylogenetic diversity. C1 [Howard, Marion G.; Shapcott, Alison] Univ Sunshine Coast, Fac Sci Hlth Educ, Genecol Res Ctr, Maroochydore, Qld, Australia. [McDonald, William J. F.; Forster, Paul I.] Queensland Herbarium, Queensland Dept Sci Informat Technol & Innovat, Brisbane Bot Gardens, Toowong, Qld, Australia. [Kress, W. John; Erickson, David] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Faith, Daniel P.] Australian Museum, 6-8 Coll St, Sydney, NSW 2000, Australia. RP Shapcott, A (reprint author), Univ Sunshine Coast, Fac Sci Hlth Educ, Genecol Res Ctr, Maroochydore, Qld, Australia. EM ashapcot@usc.edu.au FU Queensland Smithsonian Fellowship; Honours student Marion Howard FX This study was funded by student grant to Honours student Marion Howard; However it built on a previous larger project funded by Queensland Smithsonian Fellowship awarded to AS. NR 61 TC 1 Z9 1 U1 8 U2 15 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 27 PY 2016 VL 11 IS 4 AR e0153565 DI 10.1371/journal.pone.0153565 PG 19 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DK5QZ UT WOS:000374976200030 PM 27119149 ER PT J AU Gorzelak, P Zamora, S AF Gorzelak, Przemyslaw Zamora, Samuel TI Understanding form and function of the stem in early flattened echinoderms (pleurocystitids) using a microstructural approach SO PEERJ LA English DT Article DE Blastozoa; Stereom; Canada; Paleozoic; Palaeoanatomy; Rhombifera; Ordovician ID MIDDLE ORDOVICIAN; RHOMBIFERAN; IMPROBABILITY; ARTICULATIONS; EVOLUTION; CRINOIDS; TISSUES; STALK AB Pleurocystitid rhombiferans are among the most unusual echinoderms whose mode of life has been long debated. These echinoderms are usually interpreted as vagile epibenthic echinoderms, moving over the sea bottom by means of a flexible stem. Although their life habits and posture are reasonably well understood, the mechanisms that control the movement of stem are highly controversial. Specifically, it is unknown whether the stem flexibility was under the control of muscles or ligamentary mutable collagenous tissues (MCTs). Here, we reconstruct palaeoanatomy of the two Ordovician pleurocystitid rhombiferans (Pleurocystites and Amecystis) based on stereom microstructure. We show that the articular facets of columnals in pleurocystitid rhombiferans are composed of fine labyrinthic stereom. Comparison with modern echinoderms suggests that this type of stereom was associated with muscles implying that their stem was a muscular locomotory organ supporting an active mode of life. C1 [Gorzelak, Przemyslaw] Polish Acad Sci, Inst Paleobiol, Dept Biogeol, Warsaw, Poland. [Zamora, Samuel] Inst Geol & Minero Espana, Zaragoza, Spain. [Zamora, Samuel] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Gorzelak, P (reprint author), Polish Acad Sci, Inst Paleobiol, Dept Biogeol, Warsaw, Poland. EM pgorzelak@twarda.pan.pl RI Gorzelak, Przemyslaw/B-6329-2015 OI Gorzelak, Przemyslaw/0000-0001-5706-1881 FU National Science Centre (NCN) [DEC-2011/03/N/ST10/04798]; European Regional Development Fund within the Innovation Economy Operational Programme [POIG.02.02.00-00-025/09]; Ramon y Cajal Grant [RYC-2012-10576]; Spanish Ministry of Economy and Competitiveness [CGL2012-39471, CGL2013-48877] FX This work was funded by the National Science Centre (NCN) grant no DEC-2011/03/N/ST10/04798 and was performed in the NanoFun laboratory co-financed by the European Regional Development Fund within the Innovation Economy Operational Programme POIG.02.02.00-00-025/09. Samuel Zamora is funded by a Ramon y Cajal Grant (RYC-2012-10576) and projects CGL2012-39471 and CGL2013-48877 from the Spanish Ministry of Economy and Competitiveness. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 33 TC 2 Z9 2 U1 0 U2 4 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD APR 25 PY 2016 VL 4 AR UNSP e1820 DI 10.7717/peerj.1820 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DK2MP UT WOS:000374749000001 PM 27168956 ER PT J AU Wood, HM Parkinson, DY Griswold, CE Gillespie, RG Elias, DO AF Wood, Hannah M. Parkinson, Dilworth Y. Griswold, Charles E. Gillespie, Rosemary G. Elias, Damian O. TI Repeated Evolution of Power-Amplified Predatory Strikes in Trap-Jaw Spiders SO CURRENT BIOLOGY LA English DT Article ID SUPERFAMILY PALPIMANOIDEA; ANT ODONTOMACHUS; MANDIBLE STRIKE; BIOMECHANICS; PHYLOGENY; ARANEAE AB Small animals possess intriguing morphological and behavioral traits that allow them to capture prey, including innovative structural mechanisms that produce ballistic movements by amplifying power [1-6]. Power amplification occurs when an organism produces a relatively high power output by releasing slowly stored energy almost instantaneously, resulting in movements that surpass the maximal power output of muscles [7]. For example, trap-jaw, power -amplified mechanisms have been described for several ant genera [5, 8], which have evolved some of the fastest known movements in the animal kingdom [6]. However, power -amplified predatory strikes were not previously known in one of the largest animal classes, the arachnids. Mecysmaucheniidae spiders, which occur only in New Zealand and southern South America, are tiny, cryptic, ground-dwelling spiders that rely on hunting rather than web-building to capture prey [9]. Analysis of high-speed video revealed that power -amplified mechanisms occur in some mecysmaucheniid species, with the fastest species being two orders of magnitude faster than the slowest species. Molecular phylogenetic analysis revealed that power-amplified cheliceral strikes have evolved four times independently within the family. Furthermore, we identified morphological innovations that directly relate to cheliceral function: a highly modified carapace in which the cheliceral muscles are oriented horizontally; modification of a cheliceral sclerite to have muscle attachments; and, in the power-amplified species, a thicker clypeus and clypeal apodemes. These structural innovations may have set the stage for the parallel evolution of ballistic predatory strikes. C1 [Wood, Hannah M.] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Wood, Hannah M.; Griswold, Charles E.] Calif Acad Sci, Entomol Dept, San Francisco, CA 94118 USA. [Wood, Hannah M.; Gillespie, Rosemary G.; Elias, Damian O.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Parkinson, Dilworth Y.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA. RP Wood, HM (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA.; Wood, HM (reprint author), Calif Acad Sci, Entomol Dept, San Francisco, CA 94118 USA.; Wood, HM (reprint author), Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. EM woodh@si.edu FU NSF [1202873, DDIG 0909800, DEB-0613775, DEB-0072713, EAR-0228699]; NSF EAPSI New Zealand grant; Office of Science, Office of Basic Energy Sciences, of the US Department of Energy [DE-AC02-05CH11231] FX Funding for this project came from NSF Postdoctoral Fellowship 1202873, NSF DDIG 0909800, and an NSF EAPSI New Zealand grant to H.M.W. Additional funding came from the following NSF grants: DEB-0613775 to R.G.G. and C.E.G., DEB-0072713 to C.E.G., and EAR-0228699. Support for fieldwork came from the Lindsay Expedition, Exline-Frizzell Funds at California Academy of Sciences, and the Schlinger Foundation. The Advanced Light Source is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the US Department of Energy under contract no. DE-AC02-05CH11231. NR 19 TC 0 Z9 0 U1 8 U2 10 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 EI 1879-0445 J9 CURR BIOL JI Curr. Biol. PD APR 25 PY 2016 VL 26 IS 8 BP 1057 EP 1061 DI 10.1016/j.cub.2016.02.029 PG 5 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA DL0RG UT WOS:000375339700024 PM 27068421 ER PT J AU Kitaura, FS Chuang, CH Liang, Y Zhao, C Tao, CL Rodriguez-Torres, S Eisenstein, DJ Gil-Marin, H Kneib, JP McBride, C Percival, WJ Ross, AJ Sanchez, AG Tinker, J Tojeiro, R Vargas-Magana, M Zhao, GB AF Kitaura, Francisco-Shu Chuang, Chia-Hsun Liang, Yu Zhao, Cheng Tao, Charling Rodriguez-Torres, Sergio Eisenstein, Daniel J. Gil-Marin, Hector Kneib, Jean-Paul McBride, Cameron Percival, Will J. Ross, Ashley J. Sanchez, Ariel G. Tinker, Jeremy Tojeiro, Rita Vargas-Magana, Mariana Zhao, Gong-Bo TI Signatures of the Primordial Universe from Its Emptiness: Measurement of Baryon Acoustic Oscillations from Minima of the Density Field SO PHYSICAL REVIEW LETTERS LA English DT Article ID GALAXY-REDSHIFT-SURVEY; LARGE-SCALE STRUCTURE; DIGITAL SKY SURVEY; COLD DARK-MATTER; PROBE WMAP OBSERVATIONS; DATA RELEASE 7; EXCURSION SET FORMALISM; COSMIC VOIDS; SDSS-III; SPECTROSCOPIC SURVEY AB Sound waves from the primordial fluctuations of the Universe imprinted in the large-scale structure, called baryon acoustic oscillations (BAOs), can be used as standard rulers to measure the scale of the Universe. These oscillations have already been detected in the distribution of galaxies. Here we propose to measure BAOs from the troughs (minima) of the density field. Based on two sets of accurate mock halo catalogues with and without BAOs in the seed initial conditions, we demonstrate that the BAO signal cannot be obtained from the clustering of classical disjoint voids, but it is clearly detected from overlapping voids. The latter represent an estimate of all troughs of the density field. We compute them from the empty circumsphere centers constrained by tetrahedra of galaxies using Delaunay triangulation. Our theoretical models based on an unprecedented large set of detailed simulated void catalogues are remarkably well confirmed by observational data. We use the largest recently publicly available sample of luminous red galaxies from SDSS-III BOSS DR11 to unveil for the first time a > 3 sigma BAO detection from voids in observations. Since voids are nearly isotropically expanding regions, their centers represent the most quiet places in the Universe, keeping in mind the cosmos origin and providing a new promising window in the analysis of the cosmological large-scale structure from galaxy surveys. C1 [Kitaura, Francisco-Shu; Chuang, Chia-Hsun] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany. [Liang, Yu; Zhao, Cheng; Tao, Charling] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China. [Liang, Yu; Zhao, Cheng; Tao, Charling] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Tao, Charling] Aix Marseille Univ, CNRS, IN2P3, CPPM UMR 7346, F-13288 Marseille, France. [Rodriguez-Torres, Sergio] Univ Autonoma Madrid, Inst Fis Teor UAM CSIC, E-28049 Madrid, Spain. [Rodriguez-Torres, Sergio] Campus Int Excellence UAM CSIC, Cantoblanco, E-28049 Madrid, Spain. [Rodriguez-Torres, Sergio] Univ Autonoma Madrid, Dept Fis Teor M8, Cantoblanco, E-28049 Madrid, Spain. [Eisenstein, Daniel J.; McBride, Cameron] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Gil-Marin, Hector] Sorbonne Univ, ILP, 98 Bis Blvd Arago, F-75014 Paris, France. [Gil-Marin, Hector] Univ Paris 06, Lab Phys Nucl & Hautes Energies, 4 Pl Jussieu,Tour 22, F-75005 Paris, France. [Kneib, Jean-Paul] Ecole Polytech Fed Lausanne, Astrophys Lab, CH-1015 Lausanne, Switzerland. [Kneib, Jean-Paul] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Percival, Will J.; Ross, Ashley J.; Zhao, Gong-Bo] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England. [Ross, Ashley J.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. [Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, Postfach 1312,Giessenbachstr, D-85741 Garching, Germany. [Tinker, Jeremy] NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. [Tojeiro, Rita] Univ St Andrews, St Andrews KY16 9SS, Fife, Scotland. [Vargas-Magana, Mariana] Univ Nacl Autonoma Mexico, Inst Fis, Apartado Postal 20-364, Mexico City, DF, Mexico. [Zhao, Gong-Bo] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RP Kitaura, FS (reprint author), Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany. EM kitaura@aip.de OI Gil Marin, Hector/0000-0003-0265-6217 FU Leibniz Society; NSFC [11033003, 11173017]; Sino French CNRS-CAS International Laboratories LIA Origins; FCPPL; STFC; Agence Nationale de la Recherche, as part of the programme Investissements d'avenir [ANR-11-IDEX-0004-02]; Strategic Priority Research Program of the Chinese Academy of Sciences [XDB09000000]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; Tsinghua University through a 985 grant; 973 programme [2013CB834906]; 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 The authors thank Michael Wood-Vasey, Christian Wagner, Marcos Pellejero Ibanez, Juan E. Betancort-Rijo, Anatoly Klypin, Gustavo Yepes, and Francisco Prada for useful discussions. F. S. K. thanks the Leibniz Society for support. Y. L., C. T., and C. Z. acknowledge support from Tsinghua University through a 985 grant, 973 programme 2013CB834906, NSFC Grants No. 11033003 and No. 11173017, Sino French CNRS-CAS International Laboratories LIA Origins, and FCPPL. R. T. thanks the STFC for support. H. G. M. thanks the Labex ILP (Reference No. ANR-10-LABX-63), part of the Idex SUPER, for support, receiving financial state aid managed by the Agence Nationale de la Recherche, as part of the programme Investissements d'avenir under Reference No. ANR-11-IDEX-0004-02. G. Z. is supported by the Strategic Priority Research Program of the Chinese Academy of Sciences Grant No. XDB09000000. The authors are also thankful for the access to computing facilities at Barcelona (MareNostrum), LRZ (Supermuc), AIP (erebos), CCIN2P3 (Quentin Le Boulc'h), and Tsinghua University. 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. 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 119 TC 6 Z9 6 U1 2 U2 3 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 25 PY 2016 VL 116 IS 17 AR 171301 DI 10.1103/PhysRevLett.116.171301 PG 8 WC Physics, Multidisciplinary SC Physics GA DK5MI UT WOS:000374963600003 PM 27176512 ER PT J AU Ritson-Williams, R Arnold, SN Paul, VJ AF Ritson-Williams, Raphael Arnold, Suzanne N. Paul, Valerie J. TI Patterns of larval settlement preferences and post-settlement survival for seven Caribbean corals SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Facilitation; Coral recruitment; Resilience; Larval ecology; Crustose coralline algae ID MARINE INVERTEBRATE LARVAE; MONTASTRAEA-ANNULARIS; SCLERACTINIAN CORALS; RECRUITMENT FAILURE; ACROPORA-PALMATA; PLANULA LARVAE; VIRGIN-ISLANDS; ST-JOHN; METAMORPHOSIS; POPULATION AB Caribbean coral reefs continue to decline in coral cover; however, recruitment is a natural process that could increase coral abundance. Benthic habitats that increase coral recruitment are a key factor for coral persistence, but very little is known about habitat selectivity for larvae of most species of corals. The larval settlement preferences and post-settlement survival of 3 brooding and 4 broadcast spawning coral species were compared in this study. The crustose coralline algae Titanoderma prototypum and Hydrolithon boergesenii facilitated larval settlement more than the biofilm control for the broadcast spawning corals but not for the majority of the brooding corals. In paired choice experiments, the larvae of all 7 corals preferred T. prototypum over Paragoniolithon solubile, and 6 of them preferred H. boergesenii over Pa. solubile, the exception being larvae of Porites astreoides. All corals equally preferred T. prototypum and H. boergesenii, except Pseudodiploria strigosa, which preferred T. prototypum, and Acropora palmata, which preferred H. boergesenii. Some recruits from the 3 brooding corals survived longer than 1 yr in the field, but of the 4 spawning corals, only P. strigosa had 2 recruits that survived >1 yr. Corals that spawned their gametes had increased settlement in the presence of a few species of coralline algae, but corals that brooded their larvae settled on biofilms and had much greater post-settlement survival, suggesting that the recruitment of brooding corals will dominate on reefs without facilitating species of crustose coralline algae. C1 [Ritson-Williams, Raphael; Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Arnold, Suzanne N.] Univ Maine, Sch Marine Sci, Darling Marine Ctr, Walpole, ME 04573 USA. [Ritson-Williams, Raphael] Univ Hawaii Manoa, 2538 McCarthy Mall, Honolulu, HI 96822 USA. RP Ritson-Williams, R (reprint author), Smithsonian Marine Stn, Ft Pierce, FL 34949 USA.; Ritson-Williams, R (reprint author), Univ Hawaii Manoa, 2538 McCarthy Mall, Honolulu, HI 96822 USA. EM rrw33@hawaii.edu FU Hunterdon Oceanographic Research fund; Caribbean Coral Reef Ecosystems (CCRE) program at the Smithsonian Institution FX Special thanks to Nikki Fogarty and Robert Steneck for their help and advice during many field trips. Thanks to Karen Arthur, Scott Jones, Nathan Kirk, Kathy Morrow and Lorae Simpson for counting thousands of larvae and to Mike Carpenter, Klaus Ruetzler, Zach Foltz and Scott Jones for facilitating our research at Carrie Bow Cay. The Belize Fisheries Department graciously provided us with research permits. Funding was provided by the Hunterdon Oceanographic Research fund and the Caribbean Coral Reef Ecosystems (CCRE) program at the Smithsonian Institution. This manuscript is contribution 1029 of the Smithsonian Marine Station at Fort Pierce and 988 of the CCRE program. NR 50 TC 2 Z9 2 U1 22 U2 27 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD APR 21 PY 2016 VL 548 BP 127 EP 138 DI 10.3354/meps11688 PG 12 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA DM5GF UT WOS:000376375000009 ER PT J AU Buddhachat, K Thitaram, C Brown, JL Klinhom, S Bansiddhi, P Penchart, K Ouitavon, K Sriaksorn, K Pa-in, C Kanchanasaka, B Somgird, C Nganvongpanit, K AF Buddhachat, Kittisak Thitaram, Chatchote Brown, Janine L. Klinhom, Sarisa Bansiddhi, Pakkanut Penchart, Kitichaya Ouitavon, Kanita Sriaksorn, Khanittha Pa-in, Chalermpol Kanchanasaka, Budsabong Somgird, Chaleamchat Nganvongpanit, Korakot TI Use of handheld X-ray fluorescence as a non-invasive method to distinguish between Asian and African elephant tusks SO SCIENTIFIC REPORTS LA English DT Article ID BONE TISSUE; IVORY IDENTIFICATION; BAYESIAN-ANALYSIS; DNA; CONTAMINATION; LEAD; TRADE; SEX; ACCUMULATION; OSTEOCALCIN AB We describe the use of handheld X-ray fluorescence, for elephant tusk species identification. Asian (n = 72) and African (n = 85) elephant tusks were scanned and we utilized the species differences in elemental composition to develop a functional model differentiating between species with high precision. Spatially, the majority of measured elements (n = 26) exhibited a homogeneous distribution in cross-section, but a more heterologous pattern in the longitudinal direction. Twenty-one of twenty four elements differed between Asian and African samples. Data were subjected to hierarchical cluster analysis followed by a stepwise discriminant analysis, which identified elements for the functional equation. The best equation consisted of ratios of Si, S, Cl, Ti, Mn, Ag, Sb and W, with Zr as the denominator. Next, Bayesian binary regression model analysis was conducted to predict the probability that a tusk would be of African origin. A cut-off value was established to improve discrimination. This Bayesian hybrid classification model was then validated by scanning an additional 30 Asian and 41 African tusks, which showed high accuracy (94%) and precision (95%) rates. We conclude that handheld XRF is an accurate, non-invasive method to discriminate origin of elephant tusks provides rapid results applicable to use in the field. C1 [Buddhachat, Kittisak; Nganvongpanit, Korakot] Chiang Mai Univ, Fac Vet Med, Dept Vet Biosci & Publ Hlth, Anim Bone & Joint Res Lab, Chiang Mai 50100, Thailand. [Thitaram, Chatchote; Klinhom, Sarisa; Bansiddhi, Pakkanut; Somgird, Chaleamchat; Nganvongpanit, Korakot] Chiang Mai Univ, Fac Vet Med, Ctr Excellence Elephant Res & Educ, Chiang Mai 50100, Thailand. [Thitaram, Chatchote] Maesa Elephant Camp, 119-9 Tapae Rd, Chiang Mai 50100, Thailand. [Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA. [Penchart, Kitichaya; Ouitavon, Kanita; Sriaksorn, Khanittha] Dept Natl Pk Wildlife & Plant Conservat, Wildlife Conservat Off, Wildlife Res Div, DNP Wildlife Forens Sci Unit DNP WIFOS, 61 Phaholyothin Rd, Chatuchak Bangkok 10900, Thailand. [Pa-in, Chalermpol; Kanchanasaka, Budsabong] Dept Natl Pk Wildlife & Plant Conservat, Wildlife Res Div, Wildlife Conservat Off, 61 Phaholyothin Rd, Chatuchak Bangkok 10900, Thailand. RP Nganvongpanit, K (reprint author), Chiang Mai Univ, Fac Vet Med, Dept Vet Biosci & Publ Hlth, Anim Bone & Joint Res Lab, Chiang Mai 50100, Thailand.; Nganvongpanit, K (reprint author), Chiang Mai Univ, Fac Vet Med, Ctr Excellence Elephant Res & Educ, Chiang Mai 50100, Thailand. EM korakot.n@cmu.ac.th FU Center of Excellence in Elephant Research and Education, Faculty of Veterinary Medicine, Chiang Mai University, Chiang Mai, Thailand; Faculty of Veterinary Medicine, Chiang Mai University, Chiang Mai, Thailand FX The authors are grateful for research funding from the Center of Excellence in Elephant Research and Education, Faculty of Veterinary Medicine, Chiang Mai University, Chiang Mai, Thailand and Faculty of Veterinary Medicine, Chiang Mai University, Chiang Mai, Thailand, and Mr. Choochart Kalmapijit, Maesa Elephant Camp, Chiang Mai for use of the Asian ivory samples. NR 45 TC 1 Z9 1 U1 4 U2 10 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 APR 21 PY 2016 VL 6 AR 24845 DI 10.1038/srep24845 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DJ8YA UT WOS:000374499200001 PM 27097717 ER PT J AU Sutikna, T Tocheri, MW Morwood, MJ Saptomo, EW Jatmiko Awe, RD Wasisto, S Westaway, KE Aubert, M Li, B Zhao, JX Storey, M Alloway, BV Morley, MW Meijer, HJM van den Bergh, GD Grun, R Dosseto, A Brumm, A Jungers, WL Roberts, RG AF Sutikna, Thomas Tocheri, Matthew W. Morwood, Michael J. Saptomo, E. Wahyu Jatmiko Awe, Rokus Due Wasisto, Sri Westaway, Kira E. Aubert, Maxime Li, Bo Zhao, Jian-xin Storey, Michael Alloway, Brent V. Morley, Mike W. Meijer, Hanneke J. M. van den Bergh, Gerrit D. Gruen, Rainer Dosseto, Anthony Brumm, Adam Jungers, William L. Roberts, Richard G. TI Revised stratigraphy and chronology for Homo floresiensis at Liang Bua in Indonesia SO NATURE LA English DT Article ID NORTHERN AUSTRALIA; LATE PLEISTOCENE; HUMAN OCCUPATION; QUATERNARY GEOCHRONOLOGY; SOUTHEAST-ASIA; HOMININ; LUMINESCENCE; ARCHAEOLOGY; FELDSPAR; AGE C1 [Sutikna, Thomas; Morwood, Michael J.; Saptomo, E. Wahyu; Jatmiko; Awe, Rokus Due; Li, Bo; Alloway, Brent V.; Morley, Mike W.; van den Bergh, Gerrit D.; Roberts, Richard G.] Univ Wollongong, Sch Earth & Environm Sci, Ctr Archaeol Sci, Wollongong, NSW 2522, Australia. [Sutikna, Thomas; Saptomo, E. Wahyu; Jatmiko; Awe, Rokus Due; Wasisto, Sri] Pusat Penelitian Arkeol Nas, Jakarta 12510, Indonesia. [Tocheri, Matthew W.] Lakehead Univ, Dept Anthropol, Thunder Bay, ON P7B 5E1, Canada. [Tocheri, Matthew W.; Meijer, Hanneke J. M.] Smithsonian Inst, Dept Anthropol, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20013 USA. [Westaway, Kira E.] Macquarie Univ, Dept Environm Sci, Traps MQ Luminescence Dating Facil, Sydney, NSW 2109, Australia. [Aubert, Maxime] Griffith Univ, Pl Evolut & Rock Art Heritage Unit, Res Ctr Human Evolut, Gold Coast, Qld 4222, Australia. [Aubert, Maxime; Brumm, Adam] Univ Wollongong, Sch Earth & Environm Sci, Wollongong, NSW 2522, Australia. [Zhao, Jian-xin] Univ Queensland, Sch Earth Sci, Brisbane, Qld 4072, Australia. [Storey, Michael] Nat Hist Museum Denmark, Sect Earth & Planetary Syst Sci, QUADLAB, DK-1350 Copenhagen, Denmark. [Alloway, Brent V.] Victoria Univ Wellington, Sch Geog Environm & Earth Sci, Wellington 6012, New Zealand. [Meijer, Hanneke J. M.] Univ Bergen, Univ Museum Bergen, Dept Nat Hist, N-5007 Bergen, Norway. [Gruen, Rainer; Brumm, Adam] Griffith Univ, Environm Futures Res Inst, Res Ctr Human Evolut, Brisbane, Qld 4111, Australia. [Gruen, Rainer] Australian Natl Univ, Res Sch Earth Sci, GPO Box 4, Canberra, ACT 0200, Australia. [Dosseto, Anthony] Univ Wollongong, Sch Earth & Environm Sci, GeoQuEST Res Ctr, Wollongong, NSW 2522, Australia. [Jungers, William L.] SUNY Stony Brook, Med Ctr, Dept Anat Sci, Stony Brook, NY 11794 USA. [Jungers, William L.] Assoc Vahatra, BP 3972, Antananarivo 101, Madagascar. RP Sutikna, T; Roberts, RG (reprint author), Univ Wollongong, Sch Earth & Environm Sci, Ctr Archaeol Sci, Wollongong, NSW 2522, Australia.; Sutikna, T (reprint author), Pusat Penelitian Arkeol Nas, Jakarta 12510, Indonesia.; Tocheri, MW (reprint author), Lakehead Univ, Dept Anthropol, Thunder Bay, ON P7B 5E1, Canada.; Tocheri, MW (reprint author), Smithsonian Inst, Dept Anthropol, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20013 USA. EM thomasutikna@gmail.com; tocherim@gmail.com; rgrob@uow.edu.au RI Meijer, Hanneke/A-1912-2013; Grun, Rainer/A-1437-2012; Zhao, Jian-xin/A-5938-2008; OI Meijer, Hanneke/0000-0001-7066-6869; Grun, Rainer/0000-0003-1366-3674; Zhao, Jian-xin/0000-0002-2413-6178; Storey, Michael/0000-0002-3126-4637; Tocheri, Matthew/0000-0001-7600-8998; Li, Bo/0000-0003-4186-4828 FU Australian Research Council (ARC) [DP0770234]; Waitt Foundation/National Geographic Society [2121-2]; Smithsonian Scholarly Studies Program; Peter Buck Fund for Human Origins Research; Smithsonian's Human Origins Program; University of Wollongong (UOW); ARC [DP1093049, DE140100254, DE130101560, FT14010038]; UOW postgraduate scholarship; Canada Research Chair; ARC Australian Laureate Fellowship [FL130100116]; Victoria University of Wellington Science Faculty Research Grant [201255]; Villum Foundation FX The 2007-2014 excavations at Liang Bua were supported by an Australian Research Council (ARC) Discovery Project grant to M.J.M. (DP0770234), a Waitt Foundation/National Geographic Society grant to M.W.T. and T.S. (No. 2121-2) and a Smithsonian Scholarly Studies Program award to M.W.T. Additional funding was provided by the Peter Buck Fund for Human Origins Research, the Smithsonian's Human Origins Program, the University of Wollongong (UOW) and the ARC (DP1093049 to K.E.W.). T.S. is supported by a UOW postgraduate scholarship, M.W.T. by a Canada Research Chair, M.A. and A.B. by ARC Discovery Early Career Researcher Awards (DE140100254 and DE130101560, respectively), B.L. by an ARC Future Fellowship (FT14010038), R.G.R. by an ARC Australian Laureate Fellowship (FL130100116) and B.V.A. by a Victoria University of Wellington Science Faculty Research Grant (201255). QUADLAB is funded by the Villum Foundation. Fieldwork was authorised by Pusat Penelitian Arkeologi Nasional (Jakarta, Indonesia) and Pemerintah Daerah Kabupaten Manggarai (Flores, Nusa Tenggara Timur). We also thank I Made Geria, V.N. Sene, R. Potts, P. Goldberg, K. Douka, G. Veatch, V. Rossi, A. Metallo, L. Kinsley, Y. Jafari, T. Lachlan, A. D. Nguyen, D. Yurnaldi, R. Setiawan, I Dewa Kompiang and the entire Liang Bua Team from Teras, Golo Manuk and Bere. NR 63 TC 13 Z9 14 U1 24 U2 49 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 APR 21 PY 2016 VL 532 IS 7599 BP 366 EP + DI 10.1038/nature17179 PG 18 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DJ7WU UT WOS:000374424700031 PM 27027286 ER PT J AU Israel, GL Esposito, P Rea, N Zelati, FC Tiengo, A Campana, S Mereghetti, S Castillo, GAR Gots, D Burgay, M Possenti, A Zane, S Turolla, R Perna, R Cannizzaro, G Pons, J AF Israel, G. L. Esposito, P. Rea, N. Zelati, F. Coti Tiengo, A. Campana, S. Mereghetti, S. Castillo, G. A. Rodriguez Goets, D. Burgay, M. Possenti, A. Zane, S. Turolla, R. Perna, R. Cannizzaro, G. Pons, J. TI The discovery, monitoring and environment of SGR J1935+2154 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: magnetars; stars: neutron; X-rays: bursts; X-rays: individual: SGR J1935+2154 ID X-RAY-EMISSION; PHOTON IMAGING CAMERA; XMM-NEWTON; SWIFT J1834.9-0846; SUPERNOVA-REMNANTS; RRAT J1819-1458; NEUTRON-STARS; MAGNETAR; PLANE; TELESCOPE AB We report on the discovery of a new member of the magnetar class, SGR J1935+2154, and on its timing and spectral properties measured by an extensive observational campaign carried out between 2014 July and 2015 March with Chandra and XMM-Newton (11 pointings). We discovered the spin period of SGR J1935+2154 through the detection of coherent pulsations at a period of about 3.24 s. The magnetar is slowing down at a rate of (P) over dot = 1.43(1) x 10(-11) s s(-1) and with a decreasing trend due to a negative (P) over dot of -3.5(7) x 10(-19) s s(-2). This implies a surface dipolar magnetic field strength of similar to 2.2 x 10(14) G, a characteristic age of about 3.6 kyr and a spin-down luminosity L-sd similar to 1.7 x 10(34) erg s(-1). The source spectrum is well modelled by a blackbody with temperature of about 500 eV plus a power-law component with photon index of about 2. The source showed a moderate long-term variability, with a flux decay of about 25 per cent during the first four months since its discovery, and a re-brightening of the same amount during the second four months. The X-ray data were also used to study the source environment. In particular, we discovered a diffuse emission extending on spatial scales from about 1 arcsec up to at least 1 arcmin around SGR J1935+2154 both in Chandra and XMM-Newton data. This component is constant in flux (at least within uncertainties) and its spectrum is well modelled by a power-law spectrum steeper than that of the pulsar. Though a scattering halo origin seems to be more probable we cannot exclude that part, or all, of the diffuse emission is due to a pulsar wind nebula. C1 [Israel, G. L.; Castillo, G. A. Rodriguez] INAF, Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. [Esposito, P.] INAF, Ist Astrofis Spaziale & Fis Cosm Milano, Via E Bassini 15, I-20133 Milan, Italy. [Esposito, P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Rea, N.; Zelati, F. Coti] Univ Amsterdam, Astron Inst Anton Pannekoek, Postbus 94249, NL-1090 GE Amsterdam, Netherlands. [Rea, N.] Inst Ciencias Espacio ICE CSIC IEEC, Carrer Can Magrans S-N, E-02193 Barcelona, Spain. [Zelati, F. Coti] Univ Insubria, Via Valleggio 11, I-22100 Como, Italy. [Zelati, F. Coti; Campana, S.] INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, LC, Italy. [Tiengo, A.; Mereghetti, S.] INAF Ist Astrofis Spaziale & Fis Cosm, Via E Bassini 15, I-20133 Milan, Italy. [Tiengo, A.] IUSS Ist Univ Super, Piazza Vittoria 15, I-27100 Pavia, Italy. [Tiengo, A.] INFN Ist Nazl Fis Nucl, Sez Pavia, Via A Bassi 6, I-27100 Pavia, Italy. [Goets, D.] AIM CEA Irfu Serv Astrophys, F-91191 Gif Sur Yvette, France. [Burgay, M.; Possenti, A.] Osservatorio Astron Cagliari, Via Sci 5, I-09047 Cagliari, Italy. [Zane, S.; Turolla, R.] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. [Turolla, R.] Univ Padua, Dipartimento Fis & Astron, Via F Marzolo 8, I-35131 Padua, Italy. [Perna, R.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Cannizzaro, G.] Univ Roma La Sapienza, Piazzale Aldo Moro 5, I-00185 Rome, Italy. [Pons, J.] Univ Alacant, Dept Fis Aplicada, Ap Correus 99, E-03080 Alacant, Spain. RP Israel, GL (reprint author), INAF, Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. EM gianluca@oa-roma.inaf.it RI PONS, JOSE/D-4687-2012; OI PONS, JOSE/0000-0003-1018-8126; Rodriguez Castillo, Guillermo Andres/0000-0003-3952-7291; Esposito, Paolo/0000-0003-4849-5092; Rea, Nanda/0000-0003-2177-6388 FU ESA Member States; NASA; Commonwealth of Australia; NWO Vidi Grant; European COST Action [MP1304]; [AYA2012-39303]; [SGR2014-1073] FX The scientific results reported in this article are based on observations obtained with the Chandra X-ray Observatory and XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application package CIAO, and of softwares and tools provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. This research is based on observations with the NASA/UK/ASI Swift mission. We thank N. Schartel for approving the XMM-Newton 2014 November observation through the Director's Discretionary Time program and the staff of the XMM-Newton Science Operation Center for performing the Target of Opportunity observations. Similarly, we thank B. Wilkes for approving the Chandra 2014 August observation through the Director's Discretionary Time program and the Chandra staff for performing the Target of Opportunity observations. We thank the Swift duty scientists and science planners for making these observations possible. The Parkes radio telescope is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The authors warmly thank Phil Edwards for the prompt scheduling of the observations and John Reynolds for releasing part of the telescope time of his project. We thanks Jules Halpern for useful comments. NR is supported by an NWO Vidi Grant, and by grants AYA2012-39303 and SGR2014-1073. This work is partially supported by the European COST Action MP1304 (NewCOMPSTAR). NR 44 TC 4 Z9 4 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 21 PY 2016 VL 457 IS 4 BP 3448 EP 3456 DI 10.1093/mnras/stw008 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI6CE UT WOS:000373586000004 ER PT J AU Sartori, LF Schawinski, K Koss, M Treister, E Maksym, WP Keel, WC Urry, CM Lintott, CJ Wong, OI AF Sartori, Lia F. Schawinski, Kevin Koss, Michael Treister, Ezequiel Maksym, W. Peter Keel, William C. Urry, C. Megan Lintott, Chris J. Wong, O. Ivy TI Extended X-ray emission in the IC 2497-Hanny's Voorwerp system: energy injection in the gas around a fading AGN SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; quasars: general; quasars: individual: IC 2497; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; ACCRETING BLACK-HOLES; HANNYS VOORWERP; GALAXY ZOO; DOMINATED ACCRETION; BINARIES; QUASAR; EVENTS; GROWTH; STARBURSTS AB We present deep Chandra X-ray observations of the core of IC 2497, the galaxy associated with Hanny's Voorwerp and hosting a fading AGN. We find extended soft X-ray emission from hot gas around the low intrinsic luminosity (unobscured) AGN (L-bol similar to 10(42)-10(44) erg s(-1)). The temperature structure in the hot gas suggests the presence of a bubble or cavity around the fading AGN (E-bub similar to 10(54)-10(55) erg). A possible scenario is that this bubble is inflated by the fading AGN, which after changing accretion state is now in a kinetic mode. Other possibilities are that the bubble has been inflated by the past luminous quasar (L-bol similar to 10(46) erg s(-1)), or that the temperature gradient is an indication of a shock front from a superwind driven by the AGN. We discuss the possible scenarios and the implications for the AGN-host galaxy interaction, as well as an analogy between AGN and X-ray binaries lifecycles. We conclude that the AGN could inject mechanical energy into the host galaxy at the end of its lifecycle, and thus provide a source for mechanical feedback, in a similar way as observed for X-ray binaries. C1 [Sartori, Lia F.; Schawinski, Kevin; Koss, Michael] Swiss Fed Inst Technol, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [Treister, Ezequiel] Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion, Chile. [Maksym, W. Peter] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Keel, William C.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Urry, C. Megan] Yale Ctr Astron & Astrophys, Dept Phys, POB 208120, New Haven, CT 06520 USA. [Lintott, Chris J.] Oxford Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. [Wong, O. Ivy] Univ Western Australia, ICRAR, M468,35 Stirling Highway, Crawley, WA 6009, Australia. RP Sartori, LF; Schawinski, K (reprint author), Swiss Fed Inst Technol, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. EM lia.sartori@phys.ethz.ch; kevin.schawinski@phys.ethz.ch OI Schawinski, Kevin/0000-0001-5464-0888; Maksym, Walter/0000-0002-2203-7889; Urry, Meg/0000-0002-0745-9792 FU Swiss National Science Foundation Professorship grant [PP00P2_138979/1]; SNSF Ambizione grant [PZ00P2_154799/1]; Australian Research Council FX LFS, KS and MK gratefully acknowledge support from Swiss National Science Foundation Professorship grant PP00P2_138979/1 and MK support from SNSF Ambizione grant PZ00P2_154799/1. LS thanks Claudio Ricci and Hans Moritz Gunther for useful discussions. OIW acknowledges a Super Science Fellowship from the Australian Research Council. NR 36 TC 0 Z9 0 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 21 PY 2016 VL 457 IS 4 BP 3629 EP 3636 DI 10.1093/mnras/stw230 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI6CE UT WOS:000373586000016 ER PT J AU Haywood, RD Cameron, AC Unruh, YC Lovis, C Lanza, AF Llama, J Deleuil, M Fares, R Gillon, M Moutou, C Pepe, F Pollacco, D Queloz, D Segransan, D AF Haywood, R. D. Cameron, A. Collier Unruh, Y. C. Lovis, C. Lanza, A. F. Llama, J. Deleuil, M. Fares, R. Gillon, M. Moutou, C. Pepe, F. Pollacco, D. Queloz, D. Segransan, D. TI The Sun as a planet-host star: proxies from SDO images for HARPS radial-velocity variations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: radial velocities; Sun: activity; Sun: faculae, plages; Sun: granulation; sunspots; planets and satellites: detection ID EXTRA-SOLAR PLANETS; STELLAR ACTIVITY; CHROMOSPHERIC ACTIVITY; INTEGRATED SUNLIGHT; APPARENT VELOCITY; MAGNETIC CYCLES; GLIESE 581; SEARCH; EARTH; SYSTEM AB The Sun is the only star whose surface can be directly resolved at high resolution, and therefore constitutes an excellent test case to explore the physical origin of stellar radial-velocity (RV) variability. We present HARPS observations of sunlight scattered off the bright asteroid 4/Vesta, from which we deduced the Sun's activity-driven RV variations. In parallel, the Helioseismic and Magnetic Imager instrument on board the Solar Dynamics Observatory provided us with simultaneous high spatial resolution magnetograms, Dopplergrams and continuum images of the Sun in the Fe I 6173 angstrom line. We determine the RV modulation arising from the suppression of granular blueshift in magnetized regions and the flux imbalance induced by dark spots and bright faculae. The rms velocity amplitudes of these contributions are 2.40 and 0.41 m s(-1), respectively, which confirms that the inhibition of convection is the dominant source of activity-induced RV variations at play, in accordance with previous studies. We find the Doppler imbalances of spot and plage regions to be only weakly anticorrelated. Light curves can thus only give incomplete predictions of convective blueshift suppression. We must instead seek proxies that track the plage coverage on the visible stellar hemisphere directly. The chromospheric flux index R'(HK) derived from the HARPS spectra performs poorly in this respect, possibly because of the differences in limb brightening/darkening in the chromosphere and photosphere. We also find that the activity-driven RV variations of the Sun are strongly correlated with its full-disc magnetic flux density, which may become a useful proxy for activity-related RV noise. C1 [Haywood, R. D.; Cameron, A. Collier; Llama, J.; Fares, R.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Haywood, R. D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Unruh, Y. C.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Lovis, C.; Pepe, F.; Queloz, D.; Segransan, D.] Observ Geneva, 51 Chdes Maillettes, CH-1290 Sauverny, Switzerland. [Lanza, A. F.; Fares, R.] INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy. [Llama, J.] Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA. [Deleuil, M.; Moutou, C.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Gillon, M.] Univ Liege, Inst Astrophys & Geophys, Allee 6 Aout 17,Bat B5C, B-4000 Liege, Belgium. [Pollacco, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Haywood, RD (reprint author), Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.; Haywood, RD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rhaywood@cfa.harvard.edu OI Cameron, Andrew/0000-0002-8863-7828; Llama, Joseph/0000-0003-4450-0368; Lanza, Antonino Francesco/0000-0001-5928-7251 FU STFC studentship [ST/J500744/1]; John Templeton Foundation; STFC [ST/J001651/1, ST/M001296/1]; NASA Origins of the Solar System grant [NNX13AH79G] FX We wish to thank the referee for their thoughtful comments, which have greatly helped improve the analysis presented in this paper. RDH gratefully acknowledges STFC studentship grant number ST/J500744/1, and 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. ACC and RF acknowledge support from STFC consolidated grants numbers ST/J001651/1 and ST/M001296/1. JL acknowledges support from NASA Origins of the Solar System grant No. NNX13AH79G and from STFC grant ST/M001296/1. The Solar Dynamics Observatory was launched by NASA on 2011 February 11, as part of the Living With A Star programme. This research has made use of NASA's Astrophysics Data System Bibliographic Services. We also used data from Haywood et al. (2016). NR 56 TC 13 Z9 13 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 21 PY 2016 VL 457 IS 4 BP 3637 EP 3651 DI 10.1093/mnras/stw187 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI6CE UT WOS:000373586000017 ER PT J AU Parrent, JT Howell, DA Fesen, RA Parker, S Bianco, FB Dilday, B Sand, D Valenti, S Vinko, J Berlind, P Challis, P Milisavljevic, D Sanders, N Marion, GH Wheeler, JC Brown, P Calkins, ML Friesen, B Kirshner, R Pritchard, T Quimby, R Roming, P AF Parrent, J. T. Howell, D. A. Fesen, R. A. Parker, S. Bianco, F. B. Dilday, B. Sand, D. Valenti, S. Vinko, J. Berlind, P. Challis, P. Milisavljevic, D. Sanders, N. Marion, G. H. Wheeler, J. C. Brown, P. Calkins, M. L. Friesen, B. Kirshner, R. Pritchard, T. Quimby, R. Roming, P. TI Comparative analysis of SN 2012dn optical spectra: days-14 to+114 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; supernovae: individual: SN 2012dn ID IA SUPERNOVA SPECTRA; HUBBLE-SPACE-TELESCOPE; LOW-DENSITY PHOTOSPHERES; HIGH-VELOCITY FEATURES; MASS WHITE-DWARF; DELAYED-DETONATION MODELS; BOLOMETRIC LIGHT CURVES; HOST-GALAXY PROPERTIES; GAMMA-RAY BURST; H II REGIONS AB SN 2012dn is a super-Chandrasekhar mass candidate in a purportedly normal spiral (SAcd) galaxy, and poses a challenge for theories of type Ia supernova diversity. Herewe utilize the fast and highly parametrized spectrum synthesis tool, SYNAPPS, to estimate relative expansion velocities of species inferred from optical spectra obtained with six facilities. As with previous studies of normal SN Ia, we find that both unburned carbon and intermediate-mass elements are spatially coincident within the ejecta near and below 14 000 km s(-1). Although the upper limit on SN 2012dn's peak luminosity is comparable to some of the most luminous normal SN Ia, we find a progenitor mass exceeding similar to 1.6 M-circle dot is not strongly favoured by leading merger models since these models do not accurately predict spectroscopic observations of SN 2012dn and more normal events. In addition, a comparison of light curves and host-galaxy masses for a sample of literature and Palomar Transient Factory SN Ia reveals a diverse distribution of SN Ia subtypes where carbon-rich material remains unburned in some instances. Such events include SN 1991T, 1997br, and 1999aa where trace signatures of C III at optical wavelengths are presumably detected. C1 [Parrent, J. T.; Challis, P.; Milisavljevic, D.; Sanders, N.; Kirshner, R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Parrent, J. T.; Howell, D. A.; Valenti, S.] Global Telescope Network, Las Cumbres Observ, Goleta, CA 93117 USA. [Parrent, J. T.; Fesen, R. A.; Valenti, S.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Howell, D. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93117 USA. [Parker, S.] Parkdale Observ, Backyard Observ Supernova Search, Canterbury 7495, New Zealand. [Bianco, F. B.; Calkins, M. L.] NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. [Dilday, B.] Grav Jack, 23505 E Appleway Ave 200, Liberty Lake, WA 99019 USA. [Sand, D.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Vinko, J.] Univ Szeged, Dept Opt & Quantum Elect, Dom Ter 9, H-6720 Szeged, Hungary. [Vinko, J.; Marion, G. H.; Wheeler, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Berlind, P.] FL Whipple Observ, 670 Mt Hopkins Rd,POB 97, Amado, AZ 85645 USA. [Brown, P.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, 4242 TAMU, College Stn, TX 77843 USA. [Friesen, B.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks, Norman, OK 73019 USA. [Pritchard, T.; Roming, P.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Quimby, R.] San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA. [Quimby, R.] Univ Tokyo, UTIAS, Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan. [Roming, P.] SW Res Inst, Dept Space Sci, 6220 Culebra Rd, San Antonio, TX 78238 USA. RP Parrent, JT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Parrent, JT; Howell, DA (reprint author), Global Telescope Network, Las Cumbres Observ, Goleta, CA 93117 USA.; Parrent, JT (reprint author), Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA.; Howell, DA (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93117 USA. EM jparrent@cfa.harvard.edu; ahowell@lcogt.net FU Las Cumbres Observatory Global Telescope Network; Office of Science of the US Department of Energy [DE-AC02-05CH11231]; National Science Foundation [AST-1211196]; Hungarian OTKA [NN 107637] FX This work was supported by the Las Cumbres Observatory Global Telescope Network. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231, and a grant from the National Science Foundation: AST-1211196. JV is supported by Hungarian OTKA Grant NN 107637. NR 236 TC 3 Z9 3 U1 2 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 21 PY 2016 VL 457 IS 4 BP 3702 EP 3723 DI 10.1093/mnras/stw239 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI6CE UT WOS:000373586000022 ER PT J AU Brorby, M Kaaret, P Prestwich, A Mirabel, IF AF Brorby, M. Kaaret, P. Prestwich, A. Mirabel, I. F. TI Enhanced X-ray emission from Lyman break analogues and a possible L-X-SFR-metallicity plane SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: starburst; X-rays: binaries; X-rays: galaxies ID ULTRAVIOLET-LUMINOUS GALAXIES; COMPACT DWARF GALAXIES; STAR-FORMING GALAXIES; METAL-POOR GALAXIES; LOCAL UNIVERSE; INTERSTELLAR-MEDIUM; FORMATION RATES; HIGH-REDSHIFT; SKY SURVEY; ABUNDANCE AB The source of energetic photons that heated and reionized the early Universe remains uncertain. Early galaxies had low metallicity and recent population synthesis calculations suggest that the number and luminosity of high-mass X-ray binaries are enhanced in star-forming galaxies with low metallicity, offering a potentially important and previously overlooked source of heating and reionization. Lyman break analogue (LBA) galaxies are local galaxies that strongly resemble the high-redshift, star-forming Lyman break galaxies and have been suggested as local analogues to these metal-deficient galaxies found in the early Universe. We studied a sample of 10 LBAs in order to measure the relation between star formation rate and X-ray luminosity. We found that for LBAs with metallicities in the range 12 + log(10)(O/H) = 8.15-8.80, the L-X -SFR relation was log(10)(L-X/SFR [erg s(-1) M-circle dot(-1) yr]) = 39.85(+/- 0.10) in the 0.5-8 keV band with a dispersion of s = 0.25 dex. This is an enhancement of nearly a factor of 2 in the L0.5-8 keV-SFR relation relative to results for nearby, near-solar metallicity galaxies. The enhancement is significant at the 98.2 per cent level (2.4 sigma). Our enhanced L-X/SFR relation is consistent with themetallicity-dependent predicted value from population synthesis models. We discuss the possibility of an L-X-SFR-metallicity plane for star-forming galaxies. These results are important to our understanding of reionization and the formation of early galaxies. C1 [Brorby, M.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Prestwich, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Mirabel, I. F.] UBA CONICET, IAFE, CC 67,Suc 28,C1428ZAA, Buenos Aires, DF, Argentina. [Mirabel, I. F.] IRFU DSM Serv Astrophys, CEA Saclay, F-91191 Gif Sur Yvette, France. RP Brorby, M (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. EM matthew-brorby@uiowa.edu FU National Aeronautics and Space Administration [G04-15085X, NAS8-03060] FX We thank the anonymous referee for helpful comments and suggestions that greatly improved the manuscript. The scientific results reported in this article are based on observations made by the Chandra X-ray Observatory. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G04-15085X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. NR 50 TC 4 Z9 4 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 21 PY 2016 VL 457 IS 4 BP 4081 EP 4088 DI 10.1093/mnras/stw284 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI6CE UT WOS:000373586000050 ER PT J AU Aravena, M Spilker, JS Bethermin, M Bothwell, M Chapman, SC de Breuck, C Furstenau, RM Gonzalez-Lopez, J Greve, TR Litke, K Ma, J Malkan, M Marrone, DP Murphy, EJ Stark, A Strandet, M Vieira, JD Weiss, A Welikala, N Wong, GF Collier, JD AF Aravena, M. Spilker, J. S. Bethermin, M. Bothwell, M. Chapman, S. C. de Breuck, C. Furstenau, R. M. Gonzalez-Lopez, J. Greve, T. R. Litke, K. Ma, J. Malkan, M. Marrone, D. P. Murphy, E. J. Stark, A. Strandet, M. Vieira, J. D. Weiss, A. Welikala, N. Wong, G. F. Collier, J. D. TI A survey of the cold molecular gas in gravitationally lensed star-forming galaxies at z > 2 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: star-burst; cosmology: observations ID CO-TO-H-2 CONVERSION FACTOR; HUBBLE-DEEP-FIELD; SOUTH-POLE TELESCOPE; LUMINOUS SUBMILLIMETER GALAXIES; FREE-FREE EMISSION; DUST MASS RATIOS; C II EMISSION; HIGH-REDSHIFT; INTERSTELLAR-MEDIUM; SCALING RELATIONS AB Using the Australia Telescope Compact Array, we conducted a survey of CO J = 1 - 0 and J = 2 - 1 line emission towards strongly lensed high-redshift dusty star-forming galaxies (DSFGs) previously discovered with the South Pole Telescope (SPT). Our sample comprises 17 sources that had CO-based spectroscopic redshifts obtained with the Atacama Large Millimeter/submillimeter Array and the Atacama Pathfinder Experiment. We detect all sources with known redshifts in either CO J = 1 - 0 or J = 2 - 1. 12 sources are detected in the 7-mm continuum. The derived CO luminosities imply gas masses in the range (0.5-11) x 10(10) M-circle dot and gas depletion time-scales t(dep) < 200 Myr, using a CO to gas mass conversion factor alpha(CO) = 0.8 M-circle dot (K km s(-1) pc(2))(-1). Combining the CO luminosities and dust masses, along with a fixed gas-to-dust ratio, we derive alpha(CO) factors in the range 0.4-1.8 M-circle dot (K km s-1 pc2)-1, similar to what is found in other starbursting systems. We find small scatter in alpha(CO) values within the sample, even though inherent variations in the spatial distribution of dust and gas in individual cases could bias the dust-based alpha(CO) estimates. We find that lensing magnification factors based on the CO linewidth to luminosity relation (mu(CO)) are highly unreliable, but particularly when mu < 5. Finally, comparison of the gas and dynamical masses suggest that the average molecular gas fraction stays relatively constant at z = 2-5 in the SPT DSFG sample. C1 [Aravena, M.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Av Ejercito 441, Santiago 8370191, Chile. [Spilker, J. S.; Litke, K.; Marrone, D. P.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [Bethermin, M.; de Breuck, C.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Bothwell, M.] Univ Cambridge, Cavendish Lab, JJ Thompson Ave, Cambridge CB3 0HA, England. [Chapman, S. C.] Dalhousie Univ, Halifax, NS B3H 3J5, Canada. [Furstenau, R. M.; Vieira, J. D.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Furstenau, R. M.; Vieira, J. D.] Univ Illinois, Dept Phys, 1002 W Green St, Urbana, IL 61801 USA. [Gonzalez-Lopez, J.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860,Casilla 306, Santiago, Chile. [Greve, T. R.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Ma, J.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Murphy, E. J.] CALTECH, Ctr Infrared Proc & Anal, MC 220-6, Pasadena, CA 91125 USA. [Stark, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Strandet, M.; Weiss, A.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Welikala, N.] Univ Oxford, Dept Phys & Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. [Wong, G. F.; Collier, J. D.] Univ Western Sydney, Locked Bag 1797, Penrith, NSW 2751, Australia. [Wong, G. F.; Collier, J. D.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, POB 76, Epping, NSW 2121, Australia. RP Aravena, M (reprint author), Univ Diego Portales, Fac Ingn, Nucleo Astron, Av Ejercito 441, Santiago 8370191, Chile. EM manuel.aravenaa@mail.udp.cl OI De Breuck, Carlos/0000-0002-6637-3315 FU FONDECYT [1140099]; US National Science Foundation [AST-1312950]; NRAO [SOSPA1-006]; Commonwealth of Australia; National Science Foundation [ANT-0638937]; Kavli Foundation; Gordon and Betty Moore Foundation; [PHY-1125897] FX MA acknowledges partial support from FONDECYT through grant 1140099. JSS, DPM and JDV acknowledge support from the US National Science Foundation under grant no. AST-1312950. JSS acknowledges support through award SOSPA1-006 from the NRAO. The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The SPT is supported by the National Science Foundation through grant ANT-0638937, with partial support through PHY-1125897, the Kavli Foundation and the Gordon and Betty Moore Foundation. NR 130 TC 8 Z9 8 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 21 PY 2016 VL 457 IS 4 BP 4406 EP 4420 DI 10.1093/mnras/stw275 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI6CE UT WOS:000373586000074 ER PT J AU Walker, DL Longmore, SN Bastian, N Kruijssen, JMD Rathborne, JM Galvan-Madrid, R Liu, HB AF Walker, D. L. Longmore, S. N. Bastian, N. Kruijssen, J. M. D. Rathborne, J. M. Galvan-Madrid, R. Liu, H. B. TI Comparing young massive clusters and their progenitor clouds in the Milky Way SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: formation; ISM: clouds; Galaxy: centre; Galaxy: disc; open clusters and associations: general ID GIANT MOLECULAR CLOUD; GALACTIC PLANE SURVEY; STAR-FORMING REGION; CENTER DUST RIDGE; STELLAR CLUSTERS; DYNAMICAL EVOLUTION; INITIAL CONDITIONS; CONTINUUM OBSERVATIONS; GLOBULAR-CLUSTERS; STARBURST CLUSTER AB Young massive clusters (YMCs) have central stellar mass surface densities exceeding 10(4) M-circle dot pc(-2). It is currently unknown whether the stars formed at such high (proto) stellar densities. We compile a sample of gas clouds in the Galaxy which have sufficient gas mass within a radius of a few parsecs to form a YMC, and compare their radial gas mass distributions to the stellar mass distribution of Galactic YMCs. We find that the gas in the progenitor clouds is distributed differently than the stars in YMCs. The mass surface density profiles of the gas clouds are generally shallower than the stellar mass surface density profiles of the YMCs, which are characterized by prominent dense core regions with radii similar to 0.1 pc, followed by a power-law tail. On the scale of YMC core radii, we find that there are no known clouds with significantly more mass in their central regions when compared to Galactic YMCs. Additionally, we find that models in which stars form from very dense initial conditions require surface densities that are generally higher than those seen in the known candidate YMC progenitor clouds. Our results show that the quiescent, less evolved clouds contain less mass in their central regions than in the highly star-forming clouds. This suggests an evolutionary trend in which clouds continue to accumulate mass towards their centres after the onset of star formation. We conclude that a conveyor-belt scenario for YMC formation is consistent with the current sample of Galactic YMCs and their progenitor clouds. C1 [Walker, D. L.; Longmore, S. N.; Bastian, N.] Liverpool John Moores Univ, Astrophys Res Inst, IC2,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England. [Walker, D. L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Kruijssen, J. M. D.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. [Kruijssen, J. M. D.] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany. [Rathborne, J. M.] CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia. [Galvan-Madrid, R.] UNAM, Inst Radioastron & Astrofis, Apdo Postal 3-72 Xangari, Morelia 58089, Michoacan, Mexico. [Liu, H. B.] 3 Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. RP Walker, DL; Longmore, SN; Bastian, N (reprint author), Liverpool John Moores Univ, Astrophys Res Inst, IC2,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England.; Walker, DL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM daniel.walker@cfa.harvard.edu; S.N.Longmore@ljmu.ac.uk; N.J.Bastian@ljmu.ac.uk NR 80 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 APR 21 PY 2016 VL 457 IS 4 BP 4536 EP 4545 DI 10.1093/mnras/stw313 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI6CE UT WOS:000373586000083 ER PT J AU Archer, A Benbow, W Bird, R Buchovecky, M Buckley, JH Bugaev, V Byrum, K Cardenzana, JV Cerruti, M Chen, X Ciupik, L Collins-Hughes, E Connolly, MP Eisch, JD Falcone, A Feng, Q Finley, JP Fleischhack, H Flinders, A Fortson, L Furniss, A Gillanders, GH Griffin, S Grube, J Gyuk, G Hakansson, N Hanna, D Holder, J Humensky, TB Hutten, M Johnson, CA Kaaret, P Kar, P Kelley-Hoskins, N Kertzman, M Kieda, D Krause, M Krennrich, F Kumar, S Lang, MJ McArthur, S McCann, A Meagher, K Millis, J Moriarty, P Mukherjee, R Nieto, D Ong, RA Park, N Pelassa, V Pohl, M Popkow, A Pueschel, E Quinn, J Ragan, K Ratliff, G Reynolds, PT Richards, GT Roache, E Rousselle, J Santander, M Sembroski, GH Shahinyan, K Smith, AW Staszak, D Telezhinsky, I Tucci, JV Tyler, J Vassiliev, VV Wakely, SP Weiner, OM Weinstein, A Wilhelm, A Williams, DA Zitzer, B Yusef-Zadeh, F AF Archer, A. Benbow, W. Bird, R. Buchovecky, M. Buckley, J. H. Bugaev, V. Byrum, K. Cardenzana, J. V. Cerruti, M. Chen, X. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Eisch, J. D. Falcone, A. Feng, Q. Finley, J. P. Fleischhack, H. Flinders, A. Fortson, L. Furniss, A. Gillanders, G. H. Griffin, S. Grube, J. Gyuk, G. Hakansson, N. Hanna, D. Holder, J. Humensky, T. B. Huetten, M. Johnson, C. A. Kaaret, P. Kar, P. Kelley-Hoskins, N. Kertzman, M. Kieda, D. Krause, M. Krennrich, F. Kumar, S. Lang, M. J. McArthur, S. McCann, A. Meagher, K. Millis, J. Moriarty, P. Mukherjee, R. Nieto, D. Ong, R. A. Park, N. Pelassa, V. Pohl, M. Popkow, A. Pueschel, E. Quinn, J. Ragan, K. Ratliff, G. Reynolds, P. T. Richards, G. T. Roache, E. Rousselle, J. Santander, M. Sembroski, G. H. Shahinyan, K. Smith, A. W. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Vassiliev, V. V. Wakely, S. P. Weiner, O. M. Weinstein, A. Wilhelm, A. Williams, D. A. Zitzer, B. Yusef-Zadeh, F. TI TEV GAMMA-RAY OBSERVATIONS OF THE GALACTIC CENTER RIDGE BY VERITAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; gamma rays: general; supernovae: individual (G0.9+0.1) ID SGR-A-ASTERISK; SAGITTARIUS B2 CLOUD; CENTER BLACK-HOLE; HIGH-ENERGY; CENTER REGION; MOLECULAR CLOUDS; CHANDRA OBSERVATIONS; STELLAR CLUSTERS; EMISSION; TELESCOPE AB The Galactic Center ridge has been observed extensively in the past by both GeV and TeV gamma-ray instruments revealing a wealth of structure, including a diffuse component and the point sources G0.9+0.1 (a composite supernova remnant) and Sgr A* (believed to be associated with the supermassive black hole located at the center of our Galaxy). Previous very high energy (VHE) gamma-ray observations with the H.E.S.S.. experiment have also detected an extended TeV gamma-ray component along the Galactic plane in the >300 GeV gamma-ray regime. Here we report on observations of the Galactic Center ridge from 2010 to 2014 by the VERITAS telescope array in the >2 TeV energy range. From these observations we (1) provide improved measurements of the differential energy spectrum for Sgr A* in the >2 TeV gamma-ray regime, (2) provide a detection in the >2 TeV gamma-ray emission from the composite SNR G0.9+0.1 and an improved determination of its multi-TeV gamma-ray energy spectrum, and. (3) report on the detection of VER J1746-289, a localized enhancement of >2 TeV gamma-ray emission along the Galactic plane. C1 [Archer, A.; Buckley, J. H.; Bugaev, V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Pelassa, V.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bird, R.; Collins-Hughes, E.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Buchovecky, M.; Ong, R. A.; Popkow, A.; Rousselle, J.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA. [Cardenzana, J. V.; Eisch, J. D.; Krennrich, F.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Chen, X.; Fleischhack, H.; Huetten, M.; Kelley-Hoskins, N.; Krause, M.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] DESY, Platanenallee 6, D-15738 Zeuthen, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.; Ratliff, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway, Ireland. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Feng, Q.; Finley, J. P.; McArthur, S.; Sembroski, G. H.; Tucci, J. V.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. [Flinders, A.; Kar, P.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Furniss, A.] Calif State Univ East Bay, Dept Phys, Hayward, CA 94542 USA. [Griffin, S.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. [Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Humensky, T. B.; Nieto, D.; Weiner, O. M.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Kaaret, P.] Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Meagher, K.; Richards, G. T.] Georgia Inst Technol, Sch Phys, 837 State St NW, Atlanta, GA 30332 USA. [Meagher, K.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, 837 State St NW, Atlanta, GA 30332 USA. [Millis, J.] Anderson Univ, Dept Phys, 1100 East 5th St, Anderson, IN 46012 USA. [Mukherjee, R.; Santander, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Sci, Cork, Ireland. [Smith, A. W.] Univ Maryland, College Pk, MD 20742 USA. [Smith, A. W.] NASA, Goddard Space Flight Ctr, College Pk, MD 20742 USA. [Yusef-Zadeh, F.] Northwestern Univ, Dept Phys & Astron, CIERA, Evanston, IL 60208 USA. RP Smith, AW (reprint author), Univ Maryland, College Pk, MD 20742 USA.; Smith, AW (reprint author), NASA, Goddard Space Flight Ctr, College Pk, MD 20742 USA. EM asmith44@umd.edu OI Chen, Xuhui/0000-0002-9745-0248; Krause, Maria/0000-0001-7595-0914 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Cycle 7 Fermi Guest Investigator program [NNH13ZDA001N] 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 and by NSERC in Canada. 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.; A.W.S. acknowledges support through the Cycle 7 Fermi Guest Investigator program, grant number NNH13ZDA001N. NR 58 TC 2 Z9 2 U1 3 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 20 PY 2016 VL 821 IS 2 AR 129 DI 10.3847/0004-637X/821/2/129 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700058 ER PT J AU Bai, XN AF Bai, Xue-Ning TI TOWARD A GLOBAL EVOLUTIONARY MODEL OF PROTOPLANETARY DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; magnetohydrodynamics (MHD); methods: numerical ID YOUNG STELLAR OBJECTS; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; PROTOSTELLAR ACCRETION DISKS; VERTICAL SHEAR INSTABILITY; WIND-DRIVEN ACCRETION; SCALE MAGNETIC-FIELDS; X-RAY IONIZATION; T TAURI STARS; MAGNETOROTATIONAL-INSTABILITY; CIRCUMSTELLAR DISKS AB A global picture of the evolution. of protoplanetary disks (PPDs) is key to understanding almost every aspect of planet formation, where standard alpha-disk models have been continually employed for their simplicity. In the meantime, disk mass loss has been conventionally attributed to photoevaporation, which controls disk dispersal. However, a paradigm shift toward accretion driven by magnetized disk winds has taken place in recent years, thanks to studies of non-ideal magnetohydrodynamic effects in PPDs. I present a framework of global PPD evolution aiming to incorporate these advances, highlighting the role of wind-driven accretion and wind mass loss. Disk evolution is found to be largely dominated by wind-driven processes, and viscous spreading is suppressed. The timescale of disk evolution is controlled primarily by the amount of external magnetic flux threading the disks, and how rapidly the disk loses the flux. Rapid disk dispersal can be achieved if the disk is able to hold most of its magnetic flux during the evolution. In addition, because wind launching requires a sufficient level of ionization at the disk surface (mainly via external far-UV (FUV) radiation), wind kinematics is also affected by the FUV penetration depth and disk geometry. For a typical disk lifetime of a few million years, the disk loses approximately the same amount of mass through the wind as through accretion onto the protostar, and most of the wind mass loss proceeds from the outer disk via a slow wind. Fractional wind mass loss increases with increasing disk lifetime. Significant wind mass loss likely substantially enhances the dust-to-gas mass ratio and promotes planet formation. C1 [Bai, Xue-Ning] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. RP Bai, XN (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM xbai@cfa.harvard.edu FU Institute for Theory and Computation at Harvard University FX I thank Kees Dullemond and Antonella Natta for encouraging me to work on this project, Jonathan Williams for informing me about the new results from the ALMA survey of PPDs in the Lupus clouds, and Sean Andrews for useful discussions. I also thank Jeremy Goodman, Antonella Natta, Kees Dullemond, and an anonymous referee for carefully reading the manuscript and providing useful feedback that improved this paper. This work is supported by Institute for Theory and Computation at Harvard University. NR 101 TC 2 Z9 2 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 APR 20 PY 2016 VL 821 IS 2 AR 80 DI 10.3847/0004-637X/821/2/80 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700009 ER PT J AU Bower, GC Deller, A Demorest, P Brunthaler, A Falcke, H Moscibrodzka, M O'Leary, RM Eatough, RP Kramer, M Lee, KJ Spitler, L Desvignes, G Rushton, AP Doeleman, S Reid, MJ AF Bower, Geoffrey C. Deller, Adam Demorest, Paul Brunthaler, Andreas Falcke, Heino Moscibrodzka, Monika O'Leary, Ryan M. Eatough, Ralph P. Kramer, Michael Lee, K. J. Spitler, Laura Desvignes, Gregory Rushton, Anthony P. Doeleman, Sheperd Reid, Mark J. TI THE PROPER MOTION OF THE GALACTIC CENTER PULSAR RELATIVE TO SAGITTARIUS A (vol 798, 120, 2015) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Bower, Geoffrey C.] Acad Sinica, Inst Astron & Astrophys, 645 N Aohoku Pl, Hilo, HI 96720 USA. [Deller, Adam; Falcke, Heino] ASTRON, POB 2, NL-7990 AA Dwingeloo, Netherlands. [Demorest, Paul] NRAO, 520 Edgemont Rd, Charlottesville, VA 22903 USA. [Brunthaler, Andreas; Falcke, Heino; Eatough, Ralph P.; Kramer, Michael; Lee, K. J.; Spitler, Laura; Desvignes, Gregory] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Falcke, Heino; Moscibrodzka, Monika] Radboud Univ Nijmegen, Inst Math Astrophys & Particle Phys IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands. [O'Leary, Ryan M.] Univ Colorado, JILA, 440 UCB, Boulder, CO 80309 USA. [O'Leary, Ryan M.] NIST, 440 UCB, Boulder, CO 80309 USA. [Kramer, Michael] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Rushton, Anthony P.] Univ Oxford, Dept Phys, Astrophys, Keble Rd, Oxford OX1 3RH, England. [Rushton, Anthony P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Doeleman, Sheperd] MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. [Doeleman, Sheperd; Reid, Mark J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Bower, GC (reprint author), Acad Sinica, Inst Astron & Astrophys, 645 N Aohoku Pl, Hilo, HI 96720 USA. EM gbower@asiaa.sinica.edu.tw NR 1 TC 0 Z9 0 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2016 VL 821 IS 2 AR 133 DI 10.3847/0004-637X/821/2/133 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700062 ER PT J AU Bryan, ML Knutson, HA Howard, AW Ngo, H Batygin, K Crepp, JR Fulton, BJ Hinkley, S Isaacson, H Johnson, JA Marcy, GW Wright, JT AF Bryan, Marta L. Knutson, Heather A. Howard, Andrew W. Ngo, Henry Batygin, Konstantin Crepp, Justin R. Fulton, B. J. Hinkley, Sasha Isaacson, Howard Johnson, John A. Marcy, Geoffry W. Wright, Jason T. TI STATISTICS OF LONG PERIOD GAS GIANT PLANETS IN KNOWN PLANETARY SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; methods: statistical; techniques: radial velocities ID EXTRA-SOLAR PLANETS; EXOPLANET HOST STARS; SPIN-ORBIT MISALIGNMENT; LOW-MASS COMPANIONS; METAL-RICH STARS; SUN-LIKE STARS; HOT JUPITERS; M-DWARF; RADIAL-VELOCITY; HARPS SEARCH AB We conducted a Doppler survey at Keck combined with NIRC2 K-band adaptive optics (AO) imaging to search for massive, long-period companions to 123 known exoplanet systems with one or two planets detected using the radial velocity ( RV) method. Our survey is sensitive to Jupiter-mass planets out to 20 au for a majority of stars in our sample, and we report the discovery of eight new long-period planets, in addition to 20 systems with statistically significant RV trends that indicate the presence of an outer companion beyond 5 au. We combine our RV observations with AO imaging to determine the range of allowed masses and orbital separations for these companions, and account for variations in our sensitivity to companions among stars in our sample. We estimate the total occurrence rate of companions in our sample to be 52 +/- 5% over the range 1-20 M-Jup and 5-20 au. Our data also suggest a declining frequency for gas giant planets in these systems beyond 3-10 au, in contrast to earlier studies that found a rising frequency for giant planets in the range 0.01-3 au. This suggests either that the frequency of gas giant planets peaks between 3 and 10 au, or that outer companions in these systems have a different semi-major axis distribution than the overall population of gas giant planets. Our results also suggest that hot gas giants may be more likely to have an outer companion than cold gas giants. We find that planets with an outer companion have higher average eccentricities than their single counterparts, suggesting that dynamical interactions between planets may play an important role in these systems. C1 [Bryan, Marta L.] CALTECH, Cahill Ctr Astron & Astrophys, 1200 East Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. [Knutson, Heather A.; Ngo, Henry; Batygin, Konstantin] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Howard, Andrew W.; Fulton, B. J.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Hinkley, Sasha] Univ Exeter, Dept Astron, Exeter, Devon, England. [Isaacson, Howard; Marcy, Geoffry W.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Johnson, John A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Wright, Jason T.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. RP Bryan, ML (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, 1200 East Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. OI Wright, Jason/0000-0001-6160-5888; Ngo, Henry/0000-0001-5172-4859; Isaacson, Howard/0000-0002-0531-1073; Fulton, Benjamin/0000-0003-3504-5316 FU NASA [NNX14AD24G] FX We thank David Hogg and Ben Montet for helpful conversations. This work was supported by NASA grant NNX14AD24G, and was based on observations at the W.M. Keck Observatory granted by the University of Hawaii, the University of California, the California Institute of Technology, Yale University, and NASA. We thank the observers who contributed to the measurements reported here and acknowledge the efforts of the Keck Observatory staff. We extend special thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. NR 143 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 APR 20 PY 2016 VL 821 IS 2 AR 89 DI 10.3847/0004-637X/821/2/89 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700018 ER PT J AU Chomiuk, L Soderberg, AM Chevalier, RA Bruzewski, S Foley, RJ Parrent, J Strader, J Badenes, C Fransson, C Kamble, A Margutti, R Rupen, MP Simon, JD AF Chomiuk, Laura Soderberg, Alicia M. Chevalier, Roger A. Bruzewski, Seth Foley, Ryan J. Parrent, Jerod Strader, Jay Badenes, Carles Fransson, Claes Kamble, Atish Margutti, Raffaella Rupen, Michael P. Simon, Joshua D. TI A DEEP SEARCH FOR PROMPT RADIO EMISSION FROM THERMONUCLEAR SUPERNOVAE WITH THE VERY LARGE ARRAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; circumstellar matter; radio continuum: stars; supernovae: general; supernovae: individual (SN 2012cg) ID X-RAY-EMISSION; RESOLUTION SPECTROSCOPIC SEARCH; CHANDRASEKHAR-MASS PROGENITOR; CORE-COLLAPSE SUPERNOVAE; HUBBLE-SPACE-TELESCOPE; BVRI LIGHT CURVES; IA SUPERNOVA; WHITE-DWARF; SYMBIOTIC STARS; SN 2011FE AB Searches for circumstellar material around Type Ia supernovae (SNe Ia) are some of the most powerful tests of the nature of SN Ia progenitors, and radio observations provide a particularly sensitive probe of this material. Here, we report radio observations for SNe. Ia and their lower-luminosity thermonuclear cousins. We present the largest, most sensitive, and spectroscopically diverse study of prompt (Delta t less than or similar to 1 years) radio observations of 85 thermonuclear SNe, including 25 obtained by our team with the unprecedented depth of the Karl G. Jansky Very Large Array. With these observations, SN 2012cg joins SN 2011fe and SN 2014J as an SN. Ia with remarkably deep radio limits and excellent temporal coverage (six epochs, spanning 5-216 days after explosion, implying <(M)over dot>/v(w) less than or similar to 5 x 10(-9) M-circle dot yr(-1)/100 km s(-1), assuming epsilon(B) = 0.1 and epsilon(e) = 0.1). All observations yield non-detections, placing strong constraints on the presence of circumstellar material. We present analytical models for the temporal and spectral evolution of prompt radio emission from thermonuclear SNe as expected from interaction with either wind-stratified or uniform density media. These models allow us to constrain the progenitor mass loss rates, with limits in the range of <(M)over dot> less than or similar to 10(-9) - 10(-4) M-circle dot yr(-1), assuming a wind velocity of v(w) = 100 km s(-1). We compare our radio constraints with measurements of Galactic symbiotic binaries to conclude that less than or similar to 10% of thermonuclear SNe have red giant companions. C1 [Chomiuk, Laura; Bruzewski, Seth; Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Soderberg, Alicia M.; Parrent, Jerod; Kamble, Atish] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Chevalier, Roger A.] Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA. [Foley, Ryan J.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Foley, Ryan J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 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. [Fransson, Claes] Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden. [Margutti, Raffaella] NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. [Rupen, Michael P.] Natl Res Council Canada, Herzberg Astron Program, Domin Radio Astrophys Observ, POB 248, Penticton, BC V2A 6J9, Canada. [Rupen, Michael P.] Natl Res Council Canada, Astrophys Program, Domin Radio Astrophys Observ, POB 248, Penticton, BC V2A 6J9, Canada. [Simon, Joshua D.] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. RP Chomiuk, L (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM chomiuk@pa.msu.edu OI Fransson, Claes/0000-0001-8532-3594; Badenes, Carles/0000-0003-3494-343X; Parrent, Jerod/0000-0002-5103-7706 FU National Science Foundation [PHY-1066293]; Alfred P. Sloan Foundation; Packard Foundation Fellowships; NSF [AST-0807727, AST-1412980, AST-1518052] FX The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We are grateful to J. McMullin, C. Chandler, J. Wrobel, and G. van Moorsel for their work in commissioning the VLA and scheduling these observations promptly. This work was performed in part at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1066293. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We are also grateful to David Bishop, who maintains the "Latest SNe" webpage as a member of the Astronomy Section of the Rochester Academy of Science. L.C. is a Jansky Fellow of the National Radio Astronomy Observatory. R.J.F. and A.M.S. gratefully acknowledge support from the Alfred P. Sloan Foundation. J.S. and A.M.S. are supported by Packard Foundation Fellowships. This research was supported in part by NSF grants AST-0807727 (R.C.), AST-1412980 (L.C., S.B., and C.B.), and AST-1518052 (R.J.F.). NR 235 TC 6 Z9 6 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 APR 20 PY 2016 VL 821 IS 2 AR 119 DI 10.3847/0004-637X/821/2/119 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700048 ER PT J AU Faesi, CM Lada, CJ Forbrich, J AF Faesi, Christopher M. Lada, Charles J. Forbrich, Jan TI RESOLVING GIANT MOLECULAR CLOUDS IN NGC 300: A FIRST LOOK WITH THE SUBMILLIMETER ARRAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 300); galaxies: ISM; ISM: clouds; ISM: molecules; radio lines: galaxies; techniques: interferometric ID STAR-FORMATION; LOCAL GROUP; MILKY-WAY; GALAXY; M33; MASS; TURBULENCE; NGC-300; REGIONS; ORIGIN AB We present the first high angular resolution study of giant molecular clouds (GMCs) in the nearby spiral galaxy NGC 300, based on observations from the Submillimeter Array (SMA). We target eleven 500 pc sized regions of active star formation within the galaxy in the (CO)-C-12(J = 2-1) line at 40 pc spatial and 1 km s(-1) spectral resolution and identify 45 individual GMCs. We characterize the physical properties of these GMCs, and find that they are similar to GMCs in the disks of the Milky Way and other nearby spiral galaxies. For example, the GMC mass spectrum in our sample has a slope of 1.80 +/- 0.07. Twelve clouds are spatially resolved by our observations, of which ten have virial mass estimates that agree to within a factor of two with mass estimates derived directly from (CO)-C-12 integrated intensity, suggesting that the majority of these GMCs are bound. The resolved clouds show consistency with Larson's fundamental relations between size, linewidth, and mass observed in the Milky Way. We find that the linewidth scales with the size as Delta V proportional to R0.52+0.20, and the median surface density in the subsample is 54 M-circle dot pc(-2). We detect (CO)-C-13 in four GMCs and find a mean (CO)-C-12/(CO)-C-13 flux ratio of 6.2. Our interferometric observations recover between 30% and 100% of the integrated intensity from the APEX single dish (CO)-C-12 observations of Faesi et al., suggesting the presence of low-mass GMCs and/or diffuse gas below our sensitivity limit. The fraction of APEX emission recovered increases with the SMA total intensity, as well as with the star formation rate. C1 [Faesi, Christopher M.; Lada, Charles J.; Forbrich, Jan] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Forbrich, Jan] Univ Vienna, A-1010 Vienna, Austria. RP Faesi, CM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Science Foundation [DGE-1144152] FX The authors owe their deepest gratitude to Nimesh Patel for tireless guidance on the use of MIR-IDL and MIRIAD for SMA data reduction and imaging. We also wish to thank Erik Rosolowsky for helpful discussions on the application of CPROPS to this data set. We acknowledge the anonymous referee for extremely helpful comments that greatly improved the quality of this manuscript. In addition, we thank Eric Keto for assistance in obtaining the observations leading to this paper. C.M.F acknowledges support from a National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144152. NR 38 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 APR 20 PY 2016 VL 821 IS 2 AR 125 DI 10.3847/0004-637X/821/2/125 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700054 ER PT J AU Krips, M Martin, S Peck, AB Sakamoto, K Neri, R Gurwell, M Petitpas, G Zhao, JH AF Krips, M. Martin, S. Peck, A. B. Sakamoto, K. Neri, R. Gurwell, M. Petitpas, G. Zhao, Jun-Hui TI SMA OBSERVATIONS OF THE EXTENDED (CO)-C-12(J=6-5) EMISSION IN THE STARBURST GALAXY NGC 253 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 253); galaxies: ISM; galaxies: starburst; ISM: molecules; submillimeter: galaxies ID DENSE MOLECULAR GAS; STAR-FORMATION; ARP 220; SUBMILLIMETER ARRAY; J=6-5 OBSERVATIONS; NUCLEAR STARBURST; ALMA OBSERVATIONS; GALACTIC NUCLEUS; CLOUD COMPLEXES; HERSCHEL-SPIRE AB We present observations of the (CO)-C-12(J = 6-5) line and 686 GHz continuum emission in NGC 253 with the Submillimeter Array at an angular resolution of similar to 4 '' The (CO)-C-12(J = 6-5) emission is clearly detected along the disk and follows the distribution of the lower 12CO line transitions with little variation of the line ratios. A large velocity gradient analysis suggests a two-temperature model of the molecular gas in the disk, likely dominated by a combination of low-velocity shocks and the disk-wide photodissociation regions. Only marginal (CO)-C-12(J = 6-5) emission is detected in the vicinity of the expanding shells at the eastern and western edges of the disk. While the eastern shell contains gas even warmer (T-kin > 300 K) than the hot gas component (T-kin = 300 K) of the disk, the western shell is surrounded by gas much cooler (T-kin = 60 K) than the eastern shell but somewhat hotter than the cold gas component of the disk (for similar H-2 and CO column densities), indicative of different (or differently efficient) heating mechansisms. The continuum emission at 686 GHz in the disk agrees well in shape and size with that at lower (sub) millimeter frequencies, exhibiting a spectral index consistent with thermal dust emission. We find dust temperatures of similar to 10-30 K and largely optically thin emission. However, our fits suggest a second (more optically thick) dust component at higher temperatures (T-d > 60 K), similar to the molecular gas. We estimate a global dust mass of similar to 10(6) M-circle dot for the disk, translating into a gas-to-dust mass ratio of a few hundred, consistent with other nearby active galaxies. C1 [Krips, M.; Martin, S.; Neri, R.] Inst Radio Astron Millimetr, 300 Rue Piscine,Domaine Univ, F-38406 St Martin Dheres, France. [Martin, S.] European So Observ, Avda Alonso de Cordova 3107, Santiago 19, Chile. [Peck, A. B.] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. [Sakamoto, K.] Acad Sinica, Inst Astron & Astrophys, Tainan, Taiwan. [Gurwell, M.; Petitpas, G.; Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Krips, M (reprint author), Inst Radio Astron Millimetr, 300 Rue Piscine,Domaine Univ, F-38406 St Martin Dheres, France. EM krips@iram.fr; smartin@iram.fr; apeck@nrao.edu; ksakamoto@asiaa.sinica.edu.tw; neri@iram.fr; mgurwell@cfa.harvard.edu; gpetitpa@cfa.harvard.edu; jzhao@cfa.harvard.edu OI Gurwell, Mark/0000-0003-0685-3621; Martin Ruiz, Sergio/0000-0001-9281-2919 FU Smithsonian Institution; Academia Sinica; [NSC 102-2119-M-001-001-MY3] FX The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This paper makes use of the following ALMA data: ADS/JAO. ALMA#2011.0.00172.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. K.S. was supported by the grant NSC 102-2119-M-001-001-MY3. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities Inc. We thank the anonymous referee for thorough and constructive comments. NR 73 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 APR 20 PY 2016 VL 821 IS 2 AR 112 DI 10.3847/0004-637X/821/2/112 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700041 ER PT J AU Newton, ER Irwin, J Charbonneau, D Berta-Thompson, ZK Dittmann, JA West, AA AF Newton, Elisabeth R. Irwin, Jonathan Charbonneau, David Berta-Thompson, Zachory K. Dittmann, Jason A. West, Andrew A. TI THE ROTATION AND GALACTIC KINEMATICS OF MID M DWARFS IN THE SOLAR NEIGHBORHOOD SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: kinematics and dynamics; stars: low-mass; stars: rotation; starspots ID LOW-MASS STARS; NEARBY M-DWARFS; FULLY CONVECTIVE STARS; FIELD M-DWARFS; STELLAR VELOCITY DISTRIBUTION; HIGH-RESOLUTION SPECTROSCOPY; ANGULAR-MOMENTUM EVOLUTION; SCALE MAGNETIC TOPOLOGIES; GENEVA-COPENHAGEN SURVEY; VOLUME-LIMITED SAMPLE AB Rotation is a directly observable stellar property, and it drives magnetic field generation and activity through a magnetic dynamo. Main-sequence stars with masses below approximately 0.35 M. (mid-to-late M dwarfs) are fully convective, and are expected to have a different type of dynamo mechanism than solar-type stars. Measurements of their rotation rates provide insight into these mechanisms, but few rotation periods are available for these stars at field ages. Using photometry from the MEarth Project, we measure rotation periods for 387 nearby, mid-to-late M dwarfs in the northern hemisphere, finding periods from 0.1 to 140 days. The typical rotator has stable, sinusoidal photometric modulations at a semi-amplitude of 0.5%-1%. We find no period-amplitude relation for stars below 0.25 M-circle dot and an anticorrelation between period and amplitude for higher-mass M dwarfs. We highlight the existence of older, slowly rotating stars without Ha emission that nevertheless have strong photometric variability. We use parallaxes, proper motions, radial velocities, photometry, and near-infrared metallicity estimates to further characterize the population of rotators. The Galactic kinematics of our sample is consistent with the local population of G and K dwarfs, and rotators have metallicities characteristic of the solar neighborhood. We use the W space velocities and established age-velocity relations to estimate that stars with P < 10 days have ages of on average <2 Gyr, and that those with P > 70 days have ages of about 5 Gyr. The period distribution is dependent on mass: as the mass decreases, the slowest rotators at a given mass have longer periods, and the fastest rotators have shorter periods. We find a lack of stars with intermediate rotation periods, and the gap between the fast and slow rotators is larger for lower masses. Our data are consistent with a scenario in which these stars maintain rapid rotation for several gigayears, then spin down quickly, reaching periods of around 100 days by a typical age of 5 Gyr. C1 [Newton, Elisabeth R.; Irwin, Jonathan; Charbonneau, David; Dittmann, Jason A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Berta-Thompson, Zachory K.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Berta-Thompson, Zachory K.] MIT, Dept Phys, Cambridge, MA 02139 USA. [West, Andrew A.] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. RP Newton, ER (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI West, Andrew/0000-0002-5805-6715; Dittmann, Jason/0000-0001-7730-2240; Newton, Elisabeth/0000-0003-4150-841X FU National Science Foundation [AST-0807690, AST-1109468, AST-1004488]; David and Lucile Packard Foundation Fellowship for Science and Engineering; John Templeton Foundation; NSF Graduate Research Fellowship; MIT Torres Fellowship for Exoplanet Research; NSF grants [AST-1109273, AST-1255568]; Research Corporation for Science Advancement's Cottrell Scholarship; NASA; NSF; Sloan Digital Sky Survey (SDSS); NASA's Astrophysics Data System (ADS) FX The MEarth project acknowledges funding from the National Science Foundation under grants AST-0807690, AST-1109468, and AST-1004488 (Alan T. Waterman Award) and the David and Lucile Packard Foundation Fellowship for Science and Engineering. This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed here are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. E.R.N. was supported by the NSF Graduate Research Fellowship, and Z.K.B.-T. by the MIT Torres Fellowship for Exoplanet Research. A.A.W. acknowledges the support of NSF grants AST-1109273 and AST-1255568 and the Research Corporation for Science Advancement's Cottrell Scholarship.; This research has made use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF; the Sloan Digital Sky Survey (SDSS); NASA's Astrophysics Data System (ADS); and the SIMBAD database and VizieR catalog access tool, at CDS, Strasbourg, France. NR 151 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 20 PY 2016 VL 821 IS 2 AR 93 DI 10.3847/0004-637X/821/2/93 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700022 ER PT J AU Pons, E Elvis, M Civano, F Watson, MG AF Pons, E. Elvis, M. Civano, F. Watson, M. G. TI NARROW-LINE X-RAY-SELECTED GALAXIES IN THE CHANDRA-COSMOS FIELD. I. OPTICAL SPECTROSCOPIC CATALOG SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; galaxies: general; surveys; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; EVOLUTION SURVEY COSMOS; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; HOST GALAXIES; EMISSION; SAMPLE; AGN; 1ST; CLASSIFICATION AB The COSMOS survey is a large and deep survey with multiwavelength observations of sources from X-rays to the UV, allowing an extensive study of their properties. The central 0.9 deg(2) of the COSMOS field have been observed by Chandra with a sensitivity up to 1.9 x 10(-16) erg cm(-2) s(-1) in the full (0.5-10 keV) band. Photometric and spectroscopic identification of the Chandra-COSMOS (C-COSMOS) sources is available from several catalogs and campaigns. Despite the fact that the C-COSMOS galaxies have a reliable spectroscopic redshift in addition to a spectroscopic classification, the emission-line properties of this sample have not yet been measured. We present here the creation of an emission-line catalog of 453 narrow-line sources from the C-COSMOS spectroscopic sample. We have performed spectral fitting for the more common lines in galaxies ([O II] lambda 3727, [Ne III] lambda 3869, H beta, [O III] lambda lambda 4959, 5007, H alpha, and [N II] lambda lambda 6548, 6584). These data provide an optical classification for 151 (i.e., 33%) of the C-COSMOS narrow-line galaxies based on emission-line diagnostic diagrams. C1 [Pons, E.; Watson, M. G.] Univ Leicester, Leicester, Leics, England. [Pons, E.; Elvis, M.; Civano, F.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Civano, F.] Yale Univ, New Haven, CT USA. RP Pons, E (reprint author), Univ Leicester, Leicester, Leics, England.; Pons, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [617876]; ESA Member States FX This work was supported in part by NASA Grant 617876.; The scientific results reported in this article are based on observations made by the Chandra X-ray Observatory from NASA, and also in part by XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. NR 45 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 APR 20 PY 2016 VL 821 IS 2 AR 130 DI 10.3847/0004-637X/821/2/130 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700059 ER PT J AU Schlafly, EF Meisner, AM Stutz, AM Kainulainen, J Peek, JEG Tchernyshyov, K Rix, HW Finkbeiner, DP Covey, KR Green, GM Bell, EF Burgett, WS Chambers, KC Draper, PW Flewelling, H Hodapp, KW Kaiser, N Magnier, EA Martin, NF Metcalfe, N Wainscoat, RJ Waters, C AF Schlafly, E. F. Meisner, A. M. Stutz, A. M. Kainulainen, J. Peek, J. E. G. Tchernyshyov, K. Rix, H-W Finkbeiner, D. P. Covey, K. R. Green, G. M. Bell, E. F. Burgett, W. S. Chambers, K. C. Draper, P. W. Flewelling, H. Hodapp, K. W. Kaiser, N. Magnier, E. A. Martin, N. F. Metcalfe, N. Wainscoat, R. J. Waters, C. TI THE OPTICAL-INFRARED EXTINCTION CURVE AND ITS VARIATION IN THE MILKY WAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: clouds; ISM: structure ID DIGITAL SKY SURVEY; ULTRAVIOLET EXTINCTION; INTERSTELLAR EXTINCTION; MOLECULAR CLOUDS; DUST EMISSION; COLOR-EXCESS; SHAPES; LAW; EVOLUTION; APOGEE AB The dust extinction curve is a critical component of many observational programs and an important diagnostic of the physics of the interstellar medium. Here we present new measurements of the dust extinction curve and its variation toward tens of thousands of stars, a hundred-fold larger sample than in existing detailed studies. We use data from the APOGEE spectroscopic survey in combination with ten-band photometry from Pan-STARRS1, the Two Micron All-Sky Survey, and Wide-field Infrared Survey Explorer. We find that the extinction curve in the optical through infrared is well characterized by a one-parameter family of curves described by R(V). The extinction curve is more uniform than suggested in past works, with sigma(R(V)) = 0.18, and with less than one percent of sight lines having R(V) > 4. Our data and analysis have revealed two new aspects of Galactic extinction: first, we find significant, wide-area variations in R(V) throughout the Galactic plane. These variations are on scales much larger than individual molecular clouds, indicating that R(V) variations must trace much more than just grain growth in dense molecular environments. Indeed, we find no correlation between R(V) and dust column density up to E(B - V) approximate to 2. Second, we discover a strong relationship between R(V) and the far-infrared dust emissivity. C1 [Schlafly, E. F.; Stutz, A. M.; Kainulainen, J.; Rix, H-W; Martin, N. F.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Schlafly, E. F.; Meisner, A. M.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, One Cyclotron Rd, Berkeley, CA 94720 USA. [Meisner, A. M.] Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Peek, J. E. G.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Tchernyshyov, K.] Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. [Finkbeiner, D. P.; Green, G. M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Finkbeiner, D. P.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. [Covey, K. R.] Western Washington Univ, Dept Phys & Astron, 516 High St, Bellingham, WA 98225 USA. [Bell, E. F.] Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. [Burgett, W. S.] GMTO Corp, 251 S Lake Ave,Suite 300, Pasadena, CA 91101 USA. [Chambers, K. C.; Flewelling, H.; Hodapp, K. W.; Kaiser, N.; Magnier, E. A.; Wainscoat, R. J.; Waters, C.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Draper, P. W.; Metcalfe, N.] Univ Durham, Dept Phys, S Rd, Durham DH1 3LE, England. [Martin, N. F.] CNRS, Observ Astron Strasbourg, UMR 7550, 11 Rue Univ, F-67000 Strasbourg, France. RP Schlafly, EF (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.; Schlafly, EF (reprint author), Univ Calif Berkeley, Lawrence Berkeley Natl Lab, One Cyclotron Rd, Berkeley, CA 94720 USA. OI Schlafly, Edward Ford/0000-0002-3569-7421; Peek, Joshua/0000-0003-4797-7030; Green, Gregory/0000-0001-5417-2260; Stutz, Amelia/0000-0003-2300-8200; Covey, Kevin/0000-0001-6914-7797; Bell, Eric/0000-0002-5564-9873 FU NASA through Hubble Fellowship by the Space Telescope Science Institute [HST-HF2-51367.001-A]; NASA [NAS 5-26555, NNX10AD69G]; German Research Foundation (DFG) [Sonderforschungsbereich SFB 881]; NSF [AST-1312891]; Deutsche Forschungsgemeinschaft [1573]; CNRS through PICS project [PICS06183]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877]; University of Maryland; Eotvos Lorand University (ELTE) FX ES acknowledges support for this work provided by NASA through Hubble Fellowship grant HST-HF2-51367.001-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, and funding from Sonderforschungsbereich SFB 881 "The Milky Way System" (subproject A3) of the German Research Foundation (DFG). DF acknowledges support of NASA grant NNX10AD69G. GMG and DPF are partially supported by NSF grant AST-1312891. The work of JK was supported by the Deutsche Forschungsgemeinschaft priority program 1573 ("Physics of the ISM"). NFM gratefully acknowledges the CNRS for support through PICS project PICS06183.; 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 Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). NR 76 TC 4 Z9 4 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 20 PY 2016 VL 821 IS 2 AR 78 DI 10.3847/0004-637X/821/2/78 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700007 ER PT J AU van Ballegooijen, AA Asgari-Targhi, M AF van Ballegooijen, A. A. Asgari-Targhi, M. TI HEATING AND ACCELERATION OF THE FAST SOLAR WIND BY ALFVEN WAVE TURBULENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); solar wind; Sun: corona; Sun: magnetic fields; turbulence; waves ID POLAR CORONAL HOLES; STRONG IMBALANCED TURBULENCE; LOW-FREQUENCY WAVES; MAGNETOHYDRODYNAMIC TURBULENCE; MAGNETIC-FIELD; FLUX TUBES; INTERPLANETARY MEDIUM; STELLAR ATMOSPHERES; TRANSITION REGION; MHD TURBULENCE AB We present numerical simulations of reduced magnetohydrodynamic (RMHD) turbulence in a magnetic flux tube at the center of a polar coronal hole. The model for the background atmosphere is a solution of the momentum equation. and includes the effects of wave pressure on the solar wind outflow. Alfven waves are launched at the coronal base. and reflect at various heights owing. to variations in Alfven speed and outflow velocity. The turbulence is driven by nonlinear interactions between the counterpropagating Alfven waves. Results are presented for two models of the background atmosphere. In the first model the plasma density and Alfven speed vary smoothly with height, resulting in minimal wave reflections and low-energy dissipation rates. We find that the dissipation rate is insufficient to maintain the temperature of the background atmosphere. The standard phenomenological formula for the dissipation rate significantly overestimates the rate derived from our RMHD simulations, and a revised formula is proposed. In the second model we introduce additional density variations along the flux tube with a correlation length of 0.04 R-circle dot and with relative amplitude of 10%. These density variations simulate the effects of compressive MHD waves on the Alfven waves. We find that such variations significantly enhance the wave reflection and thereby the turbulent dissipation rates, producing enough heat to maintain the background atmosphere. We conclude that interactions between Alfven and compressive waves may play an important role in the turbulent heating of the fast solar wind. C1 [van Ballegooijen, A. A.; Asgari-Targhi, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP van Ballegooijen, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI van Ballegooijen, Adriaan/0000-0002-5622-3540 FU NASA [NNM07AB07C]; LMSAL [SP02H1701R] FX We thank the referee for providing detailed comments that helped improve the paper. We are most grateful to Alex Voss from the School of Computer Science at the University of St. Andrews for his support with the computational work. We thank Steve Cranmer for his thorough reading of the manuscript and helpful comments. We also thank Hui Tian for pointing out recent observations relevant to our work. We are grateful to Benjamin Chandran for providing more information about the modeling results of Perez & Chandran (2013). Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and NSC (Norway). This project was supported under contract NNM07AB07C from NASA to the Smithsonian Astrophysical Observatory (SAO) and SP02H1701R from LMSAL to SAO. This research has made use of NASA's Astrophysical Data System. NR 114 TC 2 Z9 2 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 APR 20 PY 2016 VL 821 IS 2 AR 106 DI 10.3847/0004-637X/821/2/106 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700035 ER PT J AU Yee, JC Johnson, JA Skowron, J Gould, A Pineda, JS Eastman, J Vanderburg, A Howard, A AF Yee, Jennifer C. Johnson, John Asher Skowron, Jan Gould, Andrew Pineda, J. Sebastian Eastman, Jason Vanderburg, Andrew Howard, Andrew TI TWO STARS TWO WAYS: CONFIRMING A MICROLENSING BINARY LENS SOLUTION WITH A SPECTROSCOPIC MEASUREMENT OF THE ORBIT SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; binaries: spectroscopic; gravitational lensing: micro; techniques: radial velocities ID GLOBULAR-CLUSTER; EVENT; PLANET; MASS; OGLE-2005-BLG-169; CONFIRMATION; CONSTRAINTS; RESOLUTION; SYSTEM AB Light curves of microlensing events involving stellar binaries and planetary systems can provide information about the orbital elements of the system due to orbital modulations of the caustic structure. Accurately measuring the orbit in either the stellar or planetary case requires detailed modeling of subtle deviations in the light curve. At the same time, the natural, Cartesian parameterization of a microlensing binary is partially degenerate with the microlens parallax. Hence, it is desirable to perform independent tests of the predictions of microlens orbit models using radial velocity (RV) time series of the lens binary system. To this end, we present 3.5 years of RV monitoring of the binary lens system OGLE-2009-BLG-020 L, for which Skowron et al. constrained all internal parameters of the 200-700 day orbit. Our RV measurements reveal an orbit that is consistent with the predictions of the microlens light curve analysis, thereby providing the first confirmation of orbital elements inferred from microlensing events. C1 [Yee, Jennifer C.; Johnson, John Asher; Eastman, Jason; Vanderburg, Andrew] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Skowron, Jan] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. [Gould, Andrew] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA. [Pineda, J. Sebastian] CALTECH, Dept Astron, 1200 East Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. [Howard, Andrew] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. RP Yee, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jyee@cfa.harvard.edu; jjohnson@cfa.harvard.edu; jason.eastman@cfa.harvard.edu; avanderburg@cfa.harvard.edu RI Skowron, Jan/M-5186-2014; OI Skowron, Jan/0000-0002-2335-1730; Pineda, J. Sebastian/0000-0002-4489-0135; Vanderburg, Andrew/0000-0001-7246-5438 FU NASA through the Sagan Fellowship Program - NASA Exoplanet Science Institute; NSF [AST 1103471]; NASA [NNX12AB99G]; National Science Foundation [DGE-1144469, DGE 1144152]; W.M. Keck Foundation FX The authors would like to thank Josh Simon, Ian Czekala, Alicia Soderberg, and Atish Kamble for their assistance in obtaining RV data from Magellan. Work by JCY was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. AG was supported by NSF grant AST 1103471 and NASA grant NNX12AB99G. JSP was supported by a grant from the National Science Foundation Graduate Research Fellowship under grant no. DGE-1144469. AV is supported by the National Science Foundation Graduate Research Fellowship, Grant No. DGE 1144152.; This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. 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 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 35 TC 2 Z9 2 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 APR 20 PY 2016 VL 821 IS 2 AR 121 DI 10.3847/0004-637X/821/2/121 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700050 ER PT J AU You, B Straub, O Czerny, B Sobolewska, M Rozanska, A Bursa, M Dovciak, M AF You, Bei Straub, Odele Czerny, Bozena Sobolewska, Malgosia Rozanska, Agata Bursa, Michal Dovciak, Michal TI TESTING WIND AS AN EXPLANATION FOR THE SPIN PROBLEM IN THE CONTINUUM-FITTING METHOD SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; X-rays: binaries ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; X-RAY BINARIES; MICROQUASAR GRS 1915+105; ACCRETION DISK WINDS; LMC X-3; NUMERICAL-SIMULATION; CYGNUS X-1; COSMOLOGICAL EVOLUTION; DOMINATED ACCRETION AB The continuum-fitting method is one of the two most advanced methods of determining the black hole spin in accreting X-ray binary systems. There are, however, still some unresolved issues with the underlying disk models. One of these issues manifests as an apparent decrease in spin for increasing source luminosity. Here, we perform a few simple tests to establish whether outflows from the disk close to the inner radius can address this problem. We employ four different parametric models to describe the wind and compare these to the apparent decrease in spin with luminosity measured in the sources LMC X-3 and GRS 1915+105. Wind models in which parameters do not explicitly depend on the accretion rate cannot reproduce the spin measurements. Models with mass accretion rate dependent outflows, however, have spectra that emulate the observed ones. The assumption of a wind thus effectively removes the artifact of spin decrease. This solution is not unique; the same conclusion can be obtained using a truncated inner disk model. To distinguish among the valid models, we will need high-resolution X-ray data and a realistic description of the Comptonization in the wind. C1 [You, Bei; Czerny, Bozena; Sobolewska, Malgosia; Rozanska, Agata] N Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. [Straub, Odele] Univ Oxford, Dept Phys, Astrophys, Keble Rd, Oxford OX1 3RH, England. [Straub, Odele] Univ Paris Diderot, Observ Paris, LUTH, CNRS,UMR 8102, F-92190 Meudon, France. [Czerny, Bozena] Ctr Theoret Phys, Al Lotnikow 32-46, PL-02668 Warsaw, Poland. [Sobolewska, Malgosia] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Bursa, Michal; Dovciak, Michal] Acad Sci Czech Republic, Astron Inst, Bocni 2 1401, Prague 14131, Czech Republic. RP You, B (reprint author), N Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. EM youbeiyb@gmail.com; odelest@protonmail.com; bcz@camk.edu.pl; malgosia@camk.edu.pl; agata@camk.edu.pl; bursa@astro.cas.cz; dovciak@asu.cas.cz RI Dovciak, Michal/F-4258-2014; Bursa, Michal/G-9004-2014 OI Dovciak, Michal/0000-0003-0079-1239; FU European Union Seventh Framework Program [312789]; Ministry of Science and Higher Education grant [W30/7.PR/2013]; Polish National Science Center grant [2011/03/B/ST9/03281, 2013/08/A/ST9/00795] FX Our warmest and most heartfelt thanks go to R. Remillard and J. F. Steiner, who shared their data for this study. We thank F. Yuan for his helpful comments. Furthermore, we are greatly indebted to the anonymous referee whose to-the-point comments and suggestions helped to significantly improve the manuscript. The project has received funding from the European Union Seventh Framework Program (FP7/2007-2013) under grant agreement No. 312789. This work was also supported by the Ministry of Science and Higher Education grant W30/7.PR/2013 and the Polish National Science Center grants No. 2011/03/B/ST9/03281 and No. 2013/08/A/ST9/00795. NR 129 TC 1 Z9 1 U1 3 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 20 PY 2016 VL 821 IS 2 AR 104 DI 10.3847/0004-637X/821/2/104 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700033 ER PT J AU Zahid, HJ Damjanov, I Geller, MJ Hwang, HS Fabricant, DG AF Zahid, H. Jabran Damjanov, Ivana Geller, Margaret J. Hwang, Ho Seong Fabricant, Daniel G. TI THE STELLAR MASS FUNDAMENTAL PLANE AND COMPACT QUIESCENT GALAXIES AT z < 0.6 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: structure ID DIGITAL SKY SURVEY; SIMILAR-TO 2; HUBBLE-SPACE-TELESCOPE; HIGH-SPECTRAL-RESOLUTION; STAR-FORMING GALAXIES; SIZE EVOLUTION; ELLIPTIC GALAXIES; INTERMEDIATE REDSHIFT; NUMBER DENSITY; PHOTOMETRIC REDSHIFTS AB We examine the evolution of the relation between stellar mass surface density, velocity dispersion, and half-light radius-the stellar mass fundamental plane (MFP)-for quiescent galaxies at z < 0.6. We measure the local relation from galaxies in the Sloan Digital Sky Survey and the intermediate redshift relation from similar to 500 quiescent galaxies with stellar masses 10 less than or similar to log(M*/M-circle dot) less than or similar to 11.5. Nearly half of the quiescent galaxies in our intermediate redshift sample are compact. After accounting for important selection and systematic effects, the velocity dispersion distribution of galaxies at intermediate redshifts is similar to that of galaxies in the local universe. Galaxies at z < 0.6 appear to be smaller (less than or similar to 0.1 dex) than galaxies in the local sample. The orientation of the stellar MFP is independent of redshift for massive quiescent galaxies at z < 0.6 and the zero-point evolves by similar to 0.04 dex. Compact quiescent galaxies fall on the same relation as the extended objects. We confirm that compact quiescent galaxies are the tail of the size and mass distribution of the normal quiescent galaxy population. C1 [Zahid, H. Jabran; Damjanov, Ivana; Geller, Margaret J.; Fabricant, Daniel G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Hwang, Ho Seong] Korea Inst Adv Study, Sch Phys, 85 Hoegiro, Seoul 130722, South Korea. RP Zahid, HJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM zahid@cfa.harvard.edu OI Geller, Margaret/0000-0002-9146-4876 FU Clay Postdoctoral Fellowship; Harvard College Observatory Menzel Fellowship; Natural Sciences and Engineering Research Council of Canada Postdoctoral Fellowship (NSERC) [PDF-421224-2012]; Smithsonian Institution; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX H.J.Z. gratefully acknowledges the generous support of the Clay Postdoctoral Fellowship. I.D. is supported by the Harvard College Observatory Menzel Fellowship and the Natural Sciences and Engineering Research Council of Canada Postdoctoral Fellowship (NSERC PDF-421224-2012). M.J.G. is supported by the Smithsonian Institution. This research has made use of NASA's Astrophysics Data System Bibliographic Services.; 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 76 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 APR 20 PY 2016 VL 821 IS 2 AR 101 DI 10.3847/0004-637X/821/2/101 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700030 ER PT J AU Zucker, C Walker, LM Johnson, K Gallagher, S Alatalo, K Tzanavaris, P AF Zucker, Catherine Walker, Lisa May Johnson, Kelsey Gallagher, Sarah Alatalo, Katherine Tzanavaris, Panayiotis TI HIERARCHICAL FORMATION IN ACTION: CHARACTERIZING ACCELERATED GALAXY EVOLUTION IN COMPACT GROUPS USING WHOLE-SKY WISE DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: groups: general; galaxies: interactions ID INFRARED-EMISSION; AROMATIC FEATURES; STAR-CLUSTERS; GREEN VALLEY; ULTRAVIOLET; HYPERLEDA; SPITZER; SAMPLE; ATLAS; SWIFT AB Compact groups provide an environment to study the growth of galaxies amid multiple prolonged interactions. With their dense galaxy concentrations and relatively low velocity dispersions, compact groups mimic the conditions of hierarchical galaxy assembly. Compact group galaxies are known to show a bimodality in Spitzer IRAC infrared color space: galaxies are preferentially either quiescent with low specific star formation rates (SSFRs) or prolifically forming stars-galaxies with moderate levels of specific star formation are rare. Previous Spitzer IRAC studies identifying this "canyon" have been limited by small number statistics. We utilize whole-sky Wide-field Infrared Survey Explorer (WISE) data to study 163 compact groups, thereby tripling our previous sample and including more galaxies with intermediate mid-IR colors indicative of moderate SSFRs. We define a distinct WISE. mid-IR color space (log [f(12)/f(4.6)]) versus (log [f(22)/f(3.4)]) that we use to identify canyon galaxies from the larger sample. We confirm that compact group galaxies show a bimodal distribution in the mid-infrared and identify 37 canyon galaxies with reliable photometry and intermediate mid-IR colors. Morphologically, we find that the canyon harbors a large population of both Sa-Sbc and E/S0 type galaxies, and that they fall on the optical red sequence rather than the green valley. Finally, we provide a catalog of WISE. photometry for 567 of 652 galaxies selected from the sample of 163 compact groups. C1 [Zucker, Catherine; Johnson, Kelsey] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Zucker, Catherine] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Walker, Lisa May] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Gallagher, Sarah] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Gallagher, Sarah] Univ Western Ontario, Ctr Planetary & Space Explorat, London, ON N6A 3K7, Canada. [Alatalo, Katherine] Carnegie Observ, Pasadena, CA 91101 USA. [Alatalo, Katherine] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Tzanavaris, Panayiotis] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Mail Code 662, Greenbelt, MD 20771 USA. [Tzanavaris, Panayiotis] Univ Maryland Baltimore Cty, CRESST, 1000 Hilltop Circle, Baltimore, MD 21250 USA. [Tzanavaris, Panayiotis] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Zucker, C (reprint author), Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.; Zucker, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM catherine.zucker@cfa.harvard.edu OI Zucker, Catherine/0000-0002-2250-730X; Alatalo, Katherine/0000-0002-4261-2326 FU National Aeronautics and Space Administration; Alfred P. Sloan Foundation; U.S. Department of Energy Office of Science; Virginia Space Grant Consortium; University of Virginia College of Arts and Sciences; Natural Sciences and Engineering Research Council of Canada FX This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.; Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS Web site is www.sdss.org.; C.S.Z. would like to sincerely thank the anonymous referee for their thorough feedback throughout the review process. She would also like to thank the Virginia Space Grant Consortium and the University of Virginia College of Arts and Sciences for support.; S.C.G. thanks the Natural Sciences and Engineering Research Council of Canada for support. NR 32 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 APR 20 PY 2016 VL 821 IS 2 AR 113 DI 10.3847/0004-637X/821/2/113 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DN5JM UT WOS:000377102700042 ER PT J AU Ballen, GA Urbano-Bonilla, A Maldonado-Ocampo, JA AF Ballen, Gustavo A. Urbano-Bonilla, Alexander Maldonado-Ocampo, Javier A. TI Description of a new species of the genus Chaetostoma from the Orinoco River drainage with comments on Chaetostoma milesi Fowler, 1941 (Siluriformes: Loricariidae) SO ZOOTAXA LA English DT Article DE Ancistrini; taxonomy; Hemiancistrus platyrhynchus; Andes; northern South America ID ARMORED CATFISHES; CENTRAL PERU; HYPOSTOMINAE; GENERA; PHYLOGENY; ECUADOR; ANDES AB Chaetostoma joropo n. sp. is described from the piedmont of the Orinoco River drainage in Colombia. The new species has been long confused with Chaetostoma milesi, a species with similar overall morphology and color pattern that is restricted to the Magdalena-Cauca River Basin. We diagnose the new species on the basis of morphology as well as a precise description of the color pattern. Chaetostoma joropo n. sp. is also easily distinguished from C. formosae the most similar species and other species inhabiting the Orinoco River drainage in Colombia. Data on ontogenetic variation and sexual dimorphism are provided, as well as natural history notes and remarks on the usage of the name Chaetostoma milesi for specimens from both the Orinoco and Magdalena-Cauca drainages. A discussion on the usage of the name Chaetostoma platyrhynchus is also provided given its current instability in the literature. C1 [Ballen, Gustavo A.] Univ Sao Paulo, Museu Zool, Sao Paulo, SP, Brazil. [Ballen, Gustavo A.] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Ancon, Panama. [Ballen, Gustavo A.; Urbano-Bonilla, Alexander; Maldonado-Ocampo, Javier A.] Pontificia Univ Javeriana, Fac Ciencias, Dept Biol, Lab Ictiol, Bogota, Colombia. [Urbano-Bonilla, Alexander] Inst Invest Recursos Biol Alexander von Humboldt, Bogota, Colombia. [Maldonado-Ocampo, Javier A.] Pontificia Univ Javeriana, Fac Ciencias, Dept Biol, Unidad Ecol & Sistemat UNESIS, Bogota, Colombia. RP Ballen, GA (reprint author), Univ Sao Paulo, Museu Zool, Sao Paulo, SP, Brazil.; Ballen, GA (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Ancon, Panama.; Ballen, GA; Urbano-Bonilla, A; Maldonado-Ocampo, JA (reprint author), Pontificia Univ Javeriana, Fac Ciencias, Dept Biol, Lab Ictiol, Bogota, Colombia.; Urbano-Bonilla, A (reprint author), Inst Invest Recursos Biol Alexander von Humboldt, Bogota, Colombia.; Maldonado-Ocampo, JA (reprint author), Pontificia Univ Javeriana, Fac Ciencias, Dept Biol, Unidad Ecol & Sistemat UNESIS, Bogota, Colombia. EM gaballench@gmail.com; bio.ictiologia@gmail.com; maldonadoj@javeriana.edu.co RI Museu de Zoologia da USP, MZ-USP/Q-2192-2016 FU Pontificia Universidad Javeriana [5211411]; University Vienna, Department of Integrative Zoology; Department of Morphology, Universidade Estadual Paulista-UNESP-; Instituto de Investigacion de Recursos Biologicos Alexander von Humboldt; Oleoducto Bicentenario [4400000166]; FAPESP [2014/11558-5] FX Funding to conduct field work along the Orinoco River Basin piedmont was provided by the Pontificia Universidad Javeriana (project No 5211411), University Vienna, Department of Integrative Zoology, and Department of Morphology, Universidade Estadual Paulista-UNESP-, Instituto de Investigacion de Recursos Biologicos Alexander von Humboldt and Oleoducto Bicentenario (project No. 4400000166); and through a doctoral grant by FAPESP to GAB (process 2014/11558-5). John Lundberg (ANSP), Saul Prada (MPUJ), and Francisco Villa (CZUT) are acknowledged for the access to collections or loan of specimens. GAB acknowledges Sandra Reinales and Carlos Sarmiento for their skillful advice on data analysis, and Tulio Teixeira for information about collections of Chaetostoma from Peru housed at MZUSP. AU-B acknowledges fishermen Juan de Dios Ocampo and Josue Ocampo, Anton Lamboj and Oliver Lucanus who facilitated and participated in the fieldwork at the Serrania de La Macarena. The comments from two anonymous reviewers are also acknowledged for helping to improve the quality of the manuscript. Donald Taphorn is acknowledged for kindly reviewing the English of the manuscript. NR 45 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD APR 20 PY 2016 VL 4105 IS 2 BP 181 EP 197 PG 17 WC Zoology SC Zoology GA DK9SR UT WOS:000375272100006 PM 27394772 ER PT J AU Kunder, A Rich, RM Koch, A Storm, J Nataf, DM De Propris, R Walker, AR Bono, G Johnson, CI Shen, JT Li, ZY AF Kunder, Andrea Rich, R. M. Koch, A. Storm, J. Nataf, D. M. De Propris, R. Walker, A. R. Bono, G. Johnson, C. I. Shen, Juntai Li, Z. -Y. TI BEFORE THE BAR: KINEMATIC DETECTION OF A SPHEROIDAL METAL-POOR BULGE COMPONENT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: bulge; Galaxy: evolution; Galaxy: formation; Galaxy: halo; Galaxy: kinematics and dynamics; Galaxy: structure ID RR-LYRAE STARS; BAADE-WESSELINK METHOD; METALLICITY DISTRIBUTION FUNCTION; GRAVITATIONAL LENSING EXPERIMENT; OLD GALACTIC BULGE; WAY STELLAR HALO; MILKY-WAY; ABSOLUTE MAGNITUDES; RADIAL-VELOCITIES; VY SERPENTIS AB We present 947 radial velocities of RR Lyrae variable stars in four fields located toward the Galactic bulge, observed within the data from the ongoing Bulge RR Lyrae Radial Velocity Assay (BRAVA-RR). We show that these RR Lyrae stars (RRLs) exhibit hot kinematics and null or negligible rotation and are therefore members of a separate population from the bar/pseudobulge that currently dominates the mass and luminosity of the inner Galaxy. Our RRLs predate these structures. and have metallicities, kinematics, and spatial distribution that are consistent with a "classical" bulge, although we cannot yet completely rule out the possibility that they are the metal-poor tail of a more metal-rich ([Fe/H] similar to -1 dex) halo-bulge population. The complete catalog of radial velocities for the BRAVA-RR stars is also published electronically. C1 [Kunder, Andrea; Storm, J.] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany. [Rich, R. M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Koch, A.] Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England. [Nataf, D. M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [De Propris, R.] Univ Turku, Finnish Ctr Astron ESO, Turku 2150, Finland. [Walker, A. R.] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, Casilla 603, La Serena, Chile. [Bono, G.] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy. [Bono, G.] Rome Astron Observ, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. [Johnson, C. I.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Shen, Juntai; Li, Z. -Y.] Chinese Acad Sci, Key Lab Res Galaxies & Cosmol, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China. RP Kunder, A (reprint author), Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany. OI Kunder, Andrea/0000-0002-2808-1370 FU National Science Foundation [NSF PHY11-25915, AST-1413755]; German Research Foundation (DFG) [Sonderforschungsbereich SFB 881]; Clay Fellowship; 973 Program of China [2014CB845700]; National Natural Science Foundation of China [11333003, 11322326]; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [XDB09000000]; Newton Advanced Fellowship - Royal Society; Newton Fund FX We thank the Australian Astronomical Observatory, which have made these observations possible. This research was supported in part by the National Science Foundation under grant No. NSF PHY11-25915. This work was supported by Sonderforschungsbereich SFB 881 "The Milky Way System" (subprojects A4, A5, A8) of the German Research Foundation (DFG). R.M.R. acknowledges support from grant AST-1413755 from the National Science Foundation. C.I.J. gratefully acknowledges support from the Clay Fellowship, administered by the Smithsonian Astrophysical Observatory. The research presented here is partially supported by the 973 Program of China under grant No. 2014CB845700, by the National Natural Science Foundation of China under grant Nos. 11333003 and 11322326, and by the Strategic Priority Research Program "The Emergence of Cosmological Structures" (No. XDB09000000) of the Chinese Academy of Sciences. J.S. acknowledges support from a Newton Advanced Fellowship awarded by the Royal Society and the Newton Fund. This work made use of the facilities of the Center for High Performance Computing at Shanghai Astronomical Observatory. NR 67 TC 8 Z9 8 U1 3 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 20 PY 2016 VL 821 IS 2 AR L25 DI 10.3847/2041-8205/821/2/L25 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ6OD UT WOS:000374331900006 ER PT J AU Migliori, G Siemiginowska, A Sobolewska, M Loh, A Corbel, S Ostorero, L Stawarz, L AF Migliori, G. Siemiginowska, A. Sobolewska, M. Loh, A. Corbel, S. Ostorero, L. Stawarz, L. TI FIRST DETECTION IN GAMMA-RAYS OF A YOUNG RADIO GALAXY: FERMI-LAT OBSERVATIONS OF THE COMPACT SYMMETRIC OBJECT PKS 1718-649 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual (PKS 1718, 649); galaxies: jets; gamma rays: galaxies; radiation mechanisms: non-thermal ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; SOURCE PMN J1603-4904; STEEP-SPECTRUM; X-RAY; SOURCE CATALOG; JET EMISSION; GHZ; VIEW; SKY AB We report the gamma-ray detection of a young radio galaxy, PKS 1718-649, belonging to the class of compact symmetric objects (CSOs), with the Large Area Telescope (LAT) on board the Fermi satellite. The third Fermi Gamma-ray LAT catalog (3FGL) includes an unassociated gamma-ray source, 3FGL J1728.0-6446, located close to PKS 1718-649. Using the latest Pass 8 calibration, we confirm that the best-fit 1 sigma position of the gamma-ray source is compatible with the radio location of PKS 1718-649. Cross-matching of the gamma-ray source position with the positions of blazar sources from several catalogs yields negative results. Thus, we conclude that PKS 1718-649 is the most likely counterpart to the unassociated LAT source. We obtain a detection test statistics TS similar to 36 (>5 sigma) with a best-fit photon spectral index Gamma = 2.9 +/- 0.3 and a 0.1-100 GeV photon flux density F0.1-100 (GeV) = (11.5 +/- 0.3) x 10(-9) ph cm(-2) s(-1). We argue that the linear size (similar to 2 pc), the kinematic age (similar to 100 years), and the source distance (z = 0.014) make PKS 1718-649 an ideal candidate for gamma-ray detection in the framework of the model proposing that the most compact and the youngest CSOs can efficiently produce GeV radiation via inverse-Compton scattering of the ambient photon fields by the radio lobe non-thermal electrons. Thus, our detection of the source in gamma-rays establishes young radio galaxies as a distinct class of extragalactic high-energy emitters and yields a unique insight on the physical conditions in compact radio lobes interacting with the interstellar medium of the host galaxy. C1 [Migliori, G.; Loh, A.; Corbel, S.] Univ Paris Diderot, CEA DSM SAp, Lab AIM, CEA IRFU,CNRS INSU, F-91191 Gif Sur Yvette, France. [Siemiginowska, A.; Sobolewska, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Sobolewska, M.] Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. [Corbel, S.] Univ Orleans, Stn Radioastron Nancay, Observ Paris, CNRS INSU, F-18330 Nancay, France. [Ostorero, L.] Univ Turin, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy. [Ostorero, L.] Ist Nazl Fis Nucl, Via P Giuria 1, I-10125 Turin, Italy. [Stawarz, L.] Jagiellonian Univ, Astron Observ, Ul Orla 171, PL-30244 Krakow, Poland. RP Migliori, G (reprint author), Univ Paris Diderot, CEA DSM SAp, Lab AIM, CEA IRFU,CNRS INSU, F-91191 Gif Sur Yvette, France. EM giulia.migliori@cea.fr FU UnivEarthS Labex program of Sorbonne Paris Cite [ANR10LABX0023, ANR11I-DEX000502]; Polish NSC grant [DEC-2012/04/A/ST9/00083]; INFN InDark, MIUR PRIN "Fisica Astroparticellare Teorica"; "Origin and Detection of Galactic and Extragalactic Cosmic Rays" from UniTo and Compagnia di San Paolo; NASA [NAS8-39073]; Chandra [GO4-15099X, GO0-11133X] FX We are grateful to the anonymous referee for comments that helped to improve the paper. The authors thank P. Grandi for sharing the data of Figure 2 and J. Ballet, F. D'Ammando, and F. Massaro for useful suggestions. G.M. and S.C. acknowledge the financial support from the UnivEarthS Labex program of Sorbonne Paris Cite (ANR10LABX0023 and ANR11I-DEX000502). L.S. was supported by Polish NSC grant DEC-2012/04/A/ST9/00083. L.O. acknowledges the grants: INFN InDark, MIUR PRIN2012 "Fisica Astroparticellare Teorica," and "Origin and Detection of Galactic and Extragalactic Cosmic Rays" from UniTo and Compagnia di San Paolo. This research is funded in part by NASA contract NAS8-39073. Partial support was provided by the Chandra grants GO4-15099X and GO0-11133X. NR 51 TC 2 Z9 2 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 APR 20 PY 2016 VL 821 IS 2 AR L31 DI 10.3847/2041-8205/821/2/L31 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ6OD UT WOS:000374331900012 ER PT J AU Williams, PKG Berger, E AF Williams, P. K. G. Berger, E. TI NO PRECISE LOCALIZATION FOR FRB 150418: CLAIMED RADIO TRANSIENT IS AGN VARIABILITY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; intergalactic medium; radio continuum: general; scattering ID RAY BURST AFTERGLOWS; INTERSTELLAR SCINTILLATION; 5 GHZ; ALGORITHM; EMISSION; GALAXIES; PLASMA; I. AB Keane et al. have recently claimed to have obtained the first precise localization for a fast radio burst (FRB) thanks to the identification of a contemporaneous fading slow (similar to week-timescale) radio transient. They use this localization to pinpoint the FRB to a galaxy at z approximate to 0.49 that exhibits no discernible star formation activity. We argue that the transient is not genuine and that the host candidate, WISE J071634.59-190039.2, is instead a radio variable: the available data did not exclude this possibility; a random radio variable consistent with the observations is not unlikely to have a redshift compatible with the FRB dispersion measure; and the proposed transient light curve is better explained as a scintillating steady source, perhaps also showing an active galactic nucleus (AGN) flare, than a synchrotron-emitting blastwave. The radio luminosity of the host candidate implies that it is an AGN and we present new late-time Very Large Array observations showing that the galaxy is indeed variable at a level consistent with the claimed transient. Therefore the claimed precise localization and redshift determination for FRB 150418 cannot be justified. C1 [Williams, P. K. G.; Berger, E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Williams, PKG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pwilliams@cfa.harvard.edu OI Williams, Peter/0000-0003-3734-3587 NR 40 TC 31 Z9 31 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 APR 20 PY 2016 VL 821 IS 2 AR L22 DI 10.3847/2041-8205/821/2/L22 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DJ6OD UT WOS:000374331900003 ER PT J AU Cameron, SA Lim, HC Lozier, JD Duennes, MA Thorp, R AF Cameron, Sydney A. Lim, Haw Chuan Lozier, Jeffrey D. Duennes, Michelle A. Thorp, Robbin TI Test of the invasive pathogen hypothesis of bumble bee decline in North America SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Bombus; Microsporidia; Nosema bombi; pollinator; conservation ID EMERGING INFECTIOUS-DISEASES; MULTIPLE SEQUENCE ALIGNMENT; NOSEMA-BOMBI MICROSPORIDIA; PHYLOGENETIC NETWORKS; SPECIAL FOCUS; HYMENOPTERA; POPULATIONS; APIDAE; SPP.; WILD AB Emergent fungal diseases are critical factors in global biodiversity declines. The fungal pathogen Nosema bombi was recently found to be widespread in declining species of North American bumble bees (Bombus), with circumstantial evidence suggesting an exotic introduction from Europe. This interpretation has been hampered by a lack of knowledge of global genetic variation, geographic origin, and changing prevalence patterns of N. bombi in declining North American populations. Thus, the temporal and spatial emergence of N. bombi and its potential role in bumble bee decline remain speculative. We analyze Nosema prevalence and genetic variation in the United States and Europe from 1980, before an alleged introduction in the early 1990s, to 2011, extracting Nosema DNA from Bombus natural history collection specimens from across this time period. Nosema bombi prevalence increased significantly from low detectable frequency in the 1980s to significantly higher frequency in the mid-to late-1990s, corresponding to a period of reported massive infectious outbreak of N. bombi in commercial bumble bee rearing stocks in North America. Despite the increased frequency, we find no conclusive evidence of an exotic N. bombi origin based on genetic analysis of global Nosema populations; the widespread Nosema strain found currently in declining United States bumble bees was present in the United States before commercial colony trade. Notably, the US N. bombi is not detectably different from that found predominantly throughout Western Europe, with both regions characterized by low genetic diversity compared with high levels of diversity found in Asia, where commercial bee breeding activities are low or nonexistent. C1 [Cameron, Sydney A.; Lim, Haw Chuan; Duennes, Michelle A.] Univ Illinois, Dept Entomol, 320 Morrill Hall, Urbana, IL 61801 USA. [Lozier, Jeffrey D.] Univ Alabama, Dept Biol Sci, Tuscaloosa, AL 35487 USA. [Thorp, Robbin] Univ Calif Davis, Dept Entomol & Nematol, Davis, CA 95616 USA. [Lim, Haw Chuan] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Duennes, Michelle A.] Univ Calif Riverside, Dept Entomol, Riverside, CA 92521 USA. RP Cameron, SA (reprint author), Univ Illinois, Dept Entomol, 320 Morrill Hall, Urbana, IL 61801 USA. EM scameron@life.illinois.edu FU National Institute of Food and Agriculture, US Department of Agriculture, Agriculture and Food Research Initiative Grant [2010-65104-05992] FX We especially thank L. McIntyre, as well as R. McClure, A. Hudson, and M. Honkanen for DNA extractions of museum samples. We are indebted to P. and A. Rasmont for hosting field collections in France. We also thank J. Strange for Alaska specimens, the many curators from the institutions listed in Table S1, Alvaro Hernandez and Chris Wright for technical support at the University of Illinois W. M. Keck Center, and J. Whitfield for critical reading of the manuscript and helpful discussions. This research was supported by the National Institute of Food and Agriculture, US Department of Agriculture, Agriculture and Food Research Initiative Grant 2010-65104-05992 (to S.A.C., J.D.L., and R.T.). NR 58 TC 1 Z9 1 U1 28 U2 57 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD APR 19 PY 2016 VL 113 IS 16 BP 4386 EP 4391 DI 10.1073/pnas.1525266113 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DJ7LV UT WOS:000374393800050 PM 27044096 ER PT J AU Savage, AE Terrell, KA Gratwicke, B Mattheus, NM Augustine, L Fleischer, RC AF Savage, Anna E. Terrell, Kimberly A. Gratwicke, Brian Mattheus, Nichole M. Augustine, Lauren Fleischer, Robert C. TI Reduced immune function predicts disease susceptibility in frogs infected with a deadly fungal pathogen SO CONSERVATION PHYSIOLOGY LA English DT Article DE Amphibian; bacterial killing ability; Batrachochytrium dendrobatidis; chytridiomycosis; immune response; Lithobates yavapaiensis ID BATRACHOCHYTRIUM-DENDROBATIDIS; COMPLEMENT-SYSTEM; CHYTRID FUNGUS; POPULATION DECLINES; LITORIA-CAERULEA; SERUM COMPLEMENT; LEOPARD FROG; LIFE-HISTORY; CHYTRIDIOMYCOSIS; SKIN AB The relationship between amphibian immune function and disease susceptibility is of primary concern given current worldwide declines linked to the pathogenic fungus Batrachochytrium dendrobatidis (Bd). We experimentally infected lowland leopard frogs (Lithobates yavapaiensis) with Bd to test the hypothesis that infection causes physiological stress and stimulates humoral and cell-mediated immune function in the blood. We measured body mass, the ratio of circulating neutrophils to lymphocytes (a known indicator of physiological stress) and plasma bacterial killing ability (BKA; a measure of innate immune function). In early exposure (1-15 days post-infection), stress was elevated in Bd-positive vs. Bd-negative frogs, whereas other metrics were similar between the groups. At later stages (29-55 days post-infection), stress was increased in Bd-positive frogs with signs of chytridiomycosis compared with both Bd-positive frogs without disease signs and uninfected control frogs, which were similar to each other. Infection decreased growth during the same period, demonstrating that sustained resistance to Bd is energetically costly. Importantly, BKA was lower in Bd-positive frogs with disease than in those without signs of chytridiomycosis. However, neither group differed from Bd-negative control frogs. The low BKA values in dying frogs compared with infected individuals without disease signs suggests that complement activity might signify different immunogenetic backgrounds or gene-by-environment interactions between the host, Bd and abiotic factors. We conclude that protein complement activity might be a useful predictor of Bd susceptibility and might help to explain differential disease outcomes in natural amphibian populations. C1 [Savage, Anna E.; Mattheus, Nichole M.; Fleischer, Robert C.] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, 3001 Connecticut Ave NW, Washington, DC 20008 USA. [Terrell, Kimberly A.; Gratwicke, Brian] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, 3001 Connecticut Ave NW, Washington, DC 20008 USA. [Augustine, Lauren] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Anim Care Sci, 3001 Connecticut Ave NW, Washington, DC 20008 USA. [Savage, Anna E.] Univ Cent Florida, Dept Biol, 4110 Libra Dr, Orlando, FL 32816 USA. [Terrell, Kimberly A.] Memphis Zoo, Dept Res & Conservat, 2000 Prentiss Pl, Memphis, TN 38104 USA. RP Savage, AE (reprint author), Univ Cent Florida, Dept Biol, 4110 Libra Dr, Orlando, FL 32816 USA. EM anna.savage@ucf.edu FU Smithsonian Institution Competitive Grants Program for Science; Smithsonian's Center for Conservation and Evolutionary Genetics; Smithsonian Institution Molecular Evolution Postdoctoral Fellowship; Smith Postdoctoral Fellowship FX This work was supported by a Smithsonian Institution Competitive Grants Program for Science grant to A.E.S., B.G. and R.C.F., the Smithsonian's Center for Conservation and Evolutionary Genetics, a Smithsonian Institution Molecular Evolution Postdoctoral Fellowship to A.E.S., and a Smith Postdoctoral Fellowship to K.A.T. NR 74 TC 2 Z9 2 U1 16 U2 29 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 2051-1434 J9 CONSERV PHYSIOL JI Conserv. Physiol. PD APR 15 PY 2016 VL 4 AR cow011 DI 10.1093/conphys/cow011 PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences; Physiology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Physiology GA DK8VS UT WOS:000375207000001 PM 27293759 ER PT J AU Erwin, DH AF Erwin, Douglas H. TI Eric, evolution and bodyplans SO DEVELOPMENTAL BIOLOGY LA English DT Editorial Material C1 [Erwin, Douglas H.] Smithsonian Inst, MRC 121, Dept Paleobiol, POB 37012, Washington, DC 20013 USA. RP Erwin, DH (reprint author), Smithsonian Inst, MRC 121, Dept Paleobiol, POB 37012, Washington, DC 20013 USA. EM Erwind@si.edu NR 5 TC 0 Z9 0 U1 3 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0012-1606 EI 1095-564X J9 DEV BIOL JI Dev. Biol. PD APR 15 PY 2016 VL 412 SU 2 BP S33 EP S34 DI 10.1016/j.ydbio.2016.01.024 PG 2 WC Developmental Biology SC Developmental Biology GA DK9II UT WOS:000375243700008 PM 26845576 ER PT J AU Grocke, SB Cottrell, E de Silva, S Kelley, KA AF Grocke, Stephanie B. Cottrell, Elizabeth de Silva, Shanaka Kelley, Katherine A. TI The role of crustal and eruptive processes versus source variations in controlling the oxidation state of iron in Central Andean magmas SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Central Andean volcanic zone; crustal assimilation; oxygen fugacity; subduction; wet chemistry ID AUCANQUILCHA VOLCANIC CLUSTER; FE-TI OXIDES; OXYGEN FUGACITY; NORTHERN CHILE; TRACE-ELEMENT; REDOX STATES; GEODYNAMIC IMPLICATIONS; SILICATE LIQUIDS; SUBDUCTION ZONES; LASCAR VOLCANO AB The composition of the continental crust is closely tied to subduction zone magmatism. Elevated oxygen fugacity (fO(2)) plays a central role in fostering crystallization of oxide minerals and thereby aids in generating the calc-alkaline trend of iron depletion that characterizes the continents. Along continental margins, arc magmas erupt through continental crust and often undergo extensive differentiation that may modify magmatic fO(2). The importance of the subducting slab and mantle wedge relative to the effects of this differentiation on the fO(2) recorded by continental arc magmas remains relatively unconstrained. Here, we focus on the effect of differentiation on magmatic fO(2) using a suite of 14 samples from the Central Volcanic Zone (CVZ) of the Andes where the continental crust is atypically thick (60-80 km). The samples range in composition from similar to 55 to 74 wt% SiO2 and represent the Neogene history of the arc. Samples are basaltic andesite to rhyolite and span a range of radiogenic isotopic compositions (Sr-87/Sr-86 = similar to 0.705-0.712) that represent 30 to 100% crustal assimilation. We use several proxies to estimate the 102 recorded by lavas, pumice, and scoria: (1) whole rock Fe3+/Sigma Fe ratios, (2) Fe3+/Sigma Fe ratios in quartz-hosted melt inclusions, and (3) Fe-Ti oxide oxygen-barometry. Comparison of the fO(2) calculated from bulk Fe3+/Sigma Fe ratios (post-eruptive) with that derived from Fe-Ti oxides or melt inclusion Fe3+/Sigma Fe ratios (pre-eruptive), enables us to quantify the effect of syn- or post eruptive alteration, and to select rocks for bulk analysis appropriate for the determination of pre-eruptive magmatic fO(2) using a strict criterion developed here. Across our sample suite, and in context with samples from the literature, we do not find evidence for systematic oxidation due to crystal fractionation or crustal contamination. Less evolved samples, ranging from 55 to 61 wt% SiO2, record a range of >3 orders of magnitude in fO(2), spanning the fO(2) range recorded by all samples in our suite. Among these less evolved magmas, we find that those erupted from volcanic centers located closer to the trench, closer to the Benioff Zone, and with more geochemical evidence of subducted components in the mantle source (elevated La/Nb) result in magmas that record systematically higher fO(2). We conclude that the slab/mantle source can exert greater control on magmatic fO(2) than processes occurring in even the thickest continental crust. Thus, the fO(2) of arc magmas, and hence their calc-alkaline nature, may be inherited from the mantle. (C) 2016 Elsevier B.V. All rights reserved. C1 [Grocke, Stephanie B.; Cottrell, Elizabeth] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Grocke, Stephanie B.; de Silva, Shanaka] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Kelley, Katherine A.] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 20882 USA. RP Grocke, SB (reprint author), Smithsonian Inst, Mineral Sci, NHB 119,10TH & Constitut Ave NW, Washington, DC 20560 USA. EM GrockeS@si.edu RI de Silva, Shanaka/A-4630-2011 OI de Silva, Shanaka/0000-0002-0310-5516 FU U.S. Department of Energy [DE-AC02-98CH10886]; NSF [EAR 0838536, 0908324]; Smithsonian FX We would like to thank two anonymous reviewers for providing insightful comments that significantly improved this manuscript, and Tamsin Mather for editorial handling. We appreciate assistance from T. Gooding with sample preparation, M. Brounce with wet chemistry, and T. Rose with the electron microprobe. Use of the National Synchrotron Light Source, Brookhaven National Laboratory, was supported by the U.S. Department of Energy, under contract DE-AC02-98CH10886. We acknowledge support from NSF grants EAR 0838536 and 0908324, and Smithsonian's Pre-Doctoral Fellowship and Global Volcanism Programs. NR 86 TC 2 Z9 2 U1 2 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD APR 15 PY 2016 VL 440 BP 92 EP 104 DI 10.1016/j.epsl.2016.01.026 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DH7AF UT WOS:000372942600010 ER PT J AU Somgird, C Sripiboon, S Mahasawangkul, S Boonprasert, K Brown, JL Stout, TAE Colenbrander, B Thitaram, C AF Somgird, Chaleamchat Sripiboon, Supaphen Mahasawangkul, Sittidet Boonprasert, Khajohnpat Brown, Janine L. Stout, Tom A. E. Colenbrander, Ben Thitaram, Chatchote TI Differential testosterone response to GnRH-induced LH release before and after musth in adult Asian elephant (Elephas maximus) bulls SO THERIOGENOLOGY LA English DT Article DE GnRH agonist; Hypothalamo-pituitary-gonadal (HPG) axis; Musth; Asian elephant (Elephas maximus); Testosterone; LH ID TESTICULAR GONADOTROPIN RECEPTORS; MALE AFRICAN ELEPHANTS; LOXODONTA-AFRICANA; SERUM TESTOSTERONE; DEVELOPMENTAL-CHANGES; LUTEINIZING-HORMONE; BEHAVIOR; ENDOCRINOLOGY; ESTRADIOL; DOMINANCE AB Bull elephants exhibit marked increases in testosterone secretion during musth, and studies have shown a heightened sensitivity of the testis to GnRH-stimulated testosterone production in musth compared to nonmusth males. However, activity of the hypothalamo-pituitary-gonadal axis before or soon after musth has not been studied in detail. The aim of this study was to evaluate LH and testosterone responses to GnRH challenge in nine adult Asian elephant (Elephas maximus) bulls during three periods relative to musth: premusth, postmusth, and nonmusth. Bulls were administered 80 mu g of a GnRH agonist, and blood was collected before and after injection to monitor serum hormone concentrations. The same bulls were injected with saline 2 weeks before each GnRH challenge and monitored using the same blood collection protocol. All bulls responded to GnRH, but not saline, with an increase in LH and testosterone during all three periods. The mean peak LH (1.76 +/- 0.19 ng/mL; P < 0.001) and testosterone (6.71 +/- 1.62 ng/mL; P = 0.019) concentrations after GnRH were higher than the respective baselines (0.57 +/- 0.07 ng/mL, 3.05 +/- 0.60 ng/mL). Although basal- and GnRH-induced LH secretion were similar across the stages, evaluation of the area under the curve in GnRH-treated bulls indicated that the testosterone response was greatest during premusth (2.84 +/- 0.76 area units; P = 0.019) compared to postmusth (2.02 +/- 0.63 area units), and nonmusth (2.01 +/- 0.46 area units). This confirms earlier reports that GnRH stimulates LH release and subsequent testosterone production in bull elephants. Furthermore, although the hypothalamo-pituitary-gonadal axis is active throughout the year, the testis appears to be more responsive to LH in terms of testosterone production in the period leading up to musth, compared to the nonmusth and postmusth periods. This heightened sensitivity, perhaps as a result of LH receptor up -regulation, may prime the testis for maximal testosterone production, leading to the physiological and behavioral changes associated with musth. (C) 2016 Elsevier Inc. All rights reserved. C1 [Somgird, Chaleamchat; Thitaram, Chatchote] Chiang Mai Univ, Fac Vet Med, Dept Compan Anim & Wildlife Clin, Chiang Mai 50000, Thailand. [Somgird, Chaleamchat; Sripiboon, Supaphen; Thitaram, Chatchote] Chiang Mai Univ, Ctr Excellence Elephant Res & Educ, Chiang Mai 50000, Thailand. [Mahasawangkul, Sittidet; Boonprasert, Khajohnpat] Forest Ind Org, Natl Elephant Inst, Thai Elephant Conservat Ctr, Lampang, Thailand. [Brown, Janine L.] Smithsonian Inst, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Stout, Tom A. E.; Colenbrander, Ben] Univ Utrecht, Fac Vet Med, CM, Utrecht, Netherlands. [Stout, Tom A. E.] Univ Pretoria, Fac Vet Sci, ZA-0002 Pretoria, South Africa. [Sripiboon, Supaphen] Kasetsart Univ, Fac Vet Med, Kamphaeng Saen Campus, Nakhon Pathom 73140, Thailand. RP Somgird, C; Thitaram, C (reprint author), Chiang Mai Univ, Fac Vet Med, Dept Compan Anim & Wildlife Clin, Chiang Mai 50000, Thailand.; Somgird, C; Thitaram, C (reprint author), Chiang Mai Univ, Ctr Excellence Elephant Res & Educ, Chiang Mai 50000, Thailand. EM chaleamchat.s@cmu.ac.th; chatchote.thitaram@cmu.ac.th FU National Research Council of Thailand (NRCT), Royal Thai Government scholarship; Asia-Link Program, Europe Aid Co-operation Office FX The authors thank the 1) National Research Council of Thailand (NRCT), Royal Thai Government scholarship and 2) Asia-Link Program, Europe Aid Co-operation Office for funding this research, the National Elephant Institute for allowing the study of the elephants, and the mahouts and staff at the Thai Elephant Conservation for their kind help. NR 33 TC 0 Z9 0 U1 8 U2 11 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0093-691X EI 1879-3231 J9 THERIOGENOLOGY JI Theriogenology PD APR 15 PY 2016 VL 85 IS 7 BP 1225 EP 1232 DI 10.1016/j.theriogenology.2015.12.003 PG 8 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA DH8HW UT WOS:000373035100004 PM 26774889 ER PT J AU Chen, J Shen, SZ Li, XH Xu, YG Joachimski, MM Bowring, SA Erwin, DH Yuan, DX Chen, B Zhang, H Wang, Y Cao, CQ Zheng, QF Mu, L AF Chen, Jun Shen, Shu-zhong Li, Xian-hua Xu, Yi-gang Joachimski, Michael M. Bowring, Samuel A. Erwin, Douglas H. Yuan, Dong-xun Chen, Bo Zhang, Hua Wang, Yue Cao, Chang-qun Zheng, Quan-feng Mu, Lin TI High-resolution SIMS oxygen isotope analysis on conodont apatite from South China and implications for the end-Permian mass extinction SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE SIMS; Oxygen isotope; Conodont apatite; South China; Climate warming; End-Permian mass extinction ID LARGE IGNEOUS PROVINCES; PALEOZOIC ICE-AGE; TRIASSIC BOUNDARY; BIOGENIC APATITES; OCEAN ACIDIFICATION; CHANGHSINGIAN STAGE; STRATOTYPE SECTION; SIBERIAN TRAPS; CARBON-CYCLE; POINT GSSP AB Understanding the interplay of climatic and biological events in deep time requires resolving the precise timing and pattern of paleotemperature changes and their temporal relationship with carbon cycle variations and biodiversity fluctuations. In situ oxygen isotope analyses of conodont apatite from South China enables us to reconstruct high-resolution seawater temperature records across the Permian-Triassic boundary (PTB) intervals in the upper slope (Meishan), lower slope (Shangsi), and carbonate platform (Daijiagou and Liangfengya) settings. Constrained by the latest high-precision geochronological dates and high-resolution conodont biozones, we can establish the temporal and spatial patterns of seawater temperature changes and assess their potential connections with the carbon cycle disruption and biodiversity decline. We find a rapid warming of similar to 10 degrees C during the latest Permian-earliest Triassic that postdated the onset of the negative shift in delta C-13(carb) by similar to 81 kyr (thousand years), the abrupt decline in delta C-13(carb) by similar to 32 kyr and the onset of mass extinction by similar to 23 kyr, which contradicts previous claims that the extreme temperature rise started immediately before or coincided with the onset of mass extinction. Our new evidence indicates that climate warming was most likely not a direct cause for the main pulse of the end-Permian mass extinction (EPME), but rather a later participant or a catalyst that increased the pace of the biodiversity decline. In addition, a prominent cooling is recorded in the earliest Changhsingian, with the main phase (a drop of similar to 8 degrees C in similar to 0.2 Ma) confined to the lower part of the Clarkina wangi zone and synchronous with the positive limb of the carbon isotope excursion (CIE) around the Wuchiapingian-Changhsingian boundary (WCB) in Meishan and Shangsi. Further long-term and high-resolution studies from other sections are needed to confirm the full contexts and underlying dynamics of the WCB "cooling event". (C) 2015 Elsevier B.V. All rights reserved. C1 [Chen, Jun; Xu, Yi-gang] Chinese Acad Sci, Guangzhou Inst Geochem, State Key Lab Isotope Geochem, 511 Kehua St, Guangzhou 510640, Guangdong, Peoples R China. [Shen, Shu-zhong; Yuan, Dong-xun; Chen, Bo; Zhang, Hua; Wang, Yue; Cao, Chang-qun] Chinese Acad Sci, Nanjing Inst Geol & Palaeontol, State Key Lab Palaeobiol & Stratig, Nanjing 210008, Jiangsu, Peoples R China. [Li, Xian-hua] Chinese Acad Sci, Inst Geol & Geophys, State Key Lab Lithospher Evolut, Beijing 100029, Peoples R China. [Joachimski, Michael M.] Univ Erlangen Nurnberg, GeoZentrum Nordbayern, Schlossgarten 5, D-91054 Erlangen, Germany. [Bowring, Samuel A.] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Erwin, Douglas H.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121, Washington, DC 20013 USA. [Zheng, Quan-feng] Chinese Acad Sci, Nanjing Inst Geol & Palaeontol, Key Lab Econ Stratig & Palaeogeog, Nanjing 210008, Jiangsu, Peoples R China. [Mu, Lin] Chinese Acad Sci, Nanjing Inst Geol & Palaeontol, Dept Invertebrate Palaeontol, Nanjing 210008, Jiangsu, Peoples R China. RP Chen, J (reprint author), Chinese Acad Sci, Guangzhou Inst Geochem, State Key Lab Isotope Geochem, 511 Kehua St, Guangzhou 510640, Guangdong, Peoples R China. EM junchen@gig.ac.cn RI Joachimski, Michael/B-9477-2011; Xu, Yi-Gang/E-9539-2010; Shen, Shuzhong/D-8214-2011; OI Shen, Shuzhong/0000-0001-8380-0692; CHEN, Jun/0000-0003-3291-5400; Yuan, Dongxun/0000-0001-9249-0569 FU National Natural Science Foundation of China [41290260, 41203008]; National Basic Research Program of China [2011CB808900]; State Key Laboratory of Isotope Geochemistry [SKLIG-QD-12-02]; State Key Laboratory of Palaeobiology and Stratigraphy [123111, 20131101]; National Science Foundation [EAR-0807475] FX We thank G.Q. Tang, Y. Liu, X.X. Ling, and H.X. Ma for assistance with the SIMS analyses. We are also grateful to Zivile Zigaite and Charles Henderson for their constructive reviews and Jisuo Jin for his editorial handling. This research was supported by the National Natural Science Foundation of China (41290260, 41203008), National Basic Research Program of China (2011CB808900), State Key Laboratory of Isotope Geochemistry (SKLIG-QD-12-02), and State Key Laboratory of Palaeobiology and Stratigraphy (123111, 20131101). S.A. Bowring's participation was supported by the National Science Foundation (EAR-0807475). This is contribution No. IS-2162 from GIGCAS. NR 89 TC 4 Z9 6 U1 17 U2 39 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 APR 15 PY 2016 VL 448 SI SI BP 26 EP 38 DI 10.1016/j.palaeo.2015.11.025 PG 13 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA DH3GY UT WOS:000372676700003 ER PT J AU Porterfield, JP Baraban, JH Troy, TP Ahmed, M McCarthy, MC Morgan, KM Daily, JW Nguyen, TL Stanton, JF Ellison, GB AF Porterfield, Jessica P. Baraban, Joshua H. Troy, Tyler P. Ahmed, Musahid McCarthy, Michael C. Morgan, Kathleen M. Daily, John W. Thanh Lam Nguyen Stanton, John F. Ellison, G. Barney TI Pyrolysis of the Simplest Carbohydrate, Glycolaldehyde (CHO-CH2OH), and Glyoxal in a Heated Microreactor SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID INITIATED OXIDATION; UNIMOLECULAR DECOMPOSITION; SUBMILLIMETER SPECTRUM; INFRARED-SPECTRA; MATRIX-ISOLATION; MICRO-REACTOR; GAS-PHASE; OH; MECHANISM; IONIZATION AB Both glycolaldehyde and glyoxal were pyrolyzed in a set of flash-pyrolysis microreactors. The pyrolysis products resulting from CHO-CH2OH and HCO-CHO were detected and identified by vacuum ultraviolet (VUV) photoionization mass spectrometry. Complementary product identification was provided by argon matrix infrared absorption spectroscopy. Pyrolysis pressures in the microreactor were about 100 Torr, and contact times with the microreactors were roughly 100 mu s. At 1200 K, the products of glycolaldehyde pyrolysis are H atoms, CO, CH2=O, CH2=C=O, and HCO-CHO. Thermal decomposition of HCO-CHO was studied with pulsed 118.2 nm photoionization mass spectrometry and matrix infrared absorption. Under these conditions, glyoxal undergoes pyrolysis to H atoms and CO. Tunable VUV photoionization mass spectrometry provides a lower bound for the ionization energy (IE)(CHO-CH2OH) >= 9.95 +/- 0.05 eV. The gas-phase heat of formation of glycolaldehyde was established by a sequence of calorimetric experiments. The experimental result is Delta H-f(298)(CHO-CH2OH) = -75.8 +/- 1.3 kcal mol(-1). Fully ab initio, coupled cluster calculations predict Delta H-f(0)(CHO-CH2OH) of -73.1 +/- 0.5 kcal mol(-1) and Delta H-f(298)(CHO-CH2OH) of -76.1 +/- 0.5 kcal mol(-1). The coupled-cluster singles doubles and noniterative triples correction calculations also lead to a revision of the geometry of CHO-CH2OH. We find that the O-H bond length differs substantially from earlier experimental estimates, due to unusual zero-point contributions to the moments of inertia. C1 [Porterfield, Jessica P.; Baraban, Joshua H.; Ellison, G. Barney] Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA. [Daily, John W.] Univ Colorado, Dept Mech Engn, Ctr Combust & Environm Res, Boulder, CO 80309 USA. [Troy, Tyler P.; Ahmed, Musahid] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Chem Sci, Berkeley, CA 94720 USA. [McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Morgan, Kathleen M.] Xavier Univ Louisiana, Dept Chem, New Orleans, LA 70125 USA. [Thanh Lam Nguyen; Stanton, John F.] Univ Texas Austin, Dept Chem, Austin, TX 78712 USA. RP Ellison, GB (reprint author), Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA. EM barney@jila.colorado.edu RI Ahmed, Musahid/A-8733-2009 FU National Science Foundation [CBET-1403979]; Robert A. Welch Foundation [F-1283]; United States Department of Energy, Basic Energy Sciences [DE-FG02-07ER15884]; Office of Energy Research, Office of Basic Energy Sciences, and Chemical Sciences Division of the U.S. Department of Energy [DE-AC02- 05CH11231] FX The National Science Foundation (CBET-1403979) has provided support for J.P.P, J.H.B, J.W.D, and G.B.E. We would like to acknowledge National Science Foundation (CHE-1361874) to K.M.M. and CHE-1361031 to J.F.S. Thermal analysis measurements were performed with assistance from S. Akbarian-Tefaghi at the Univ. of New Orleans, Advanced Materials Research Institute FACS user facility. J.F.S. and T.L.N. acknowledge support from the Robert A. Welch Foundation (Grant No. F-1283) and the United States Department of Energy, Basic Energy Sciences (DE-FG02-07ER15884). M.A. and T.P.T. and the Advanced Light Source are supported by the Director, Office of Energy Research, Office of Basic Energy Sciences, and Chemical Sciences Division of the U.S. Department of Energy under Contract No. DE-AC02- 05CH11231. We thank Prof. K. B. Wiberg for several helpful comments. NR 87 TC 0 Z9 0 U1 11 U2 29 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD APR 14 PY 2016 VL 120 IS 14 BP 2161 EP 2172 DI 10.1021/acs.jpca.6b00652 PG 12 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA DJ7ZH UT WOS:000374431200001 PM 26979134 ER PT J AU Hawkins, MTR Leonard, JA Helgen, KM McDonough, MM Rockwood, LL Maldonado, JE AF Hawkins, Melissa T. R. Leonard, Jennifer A. Helgen, Kristofer M. McDonough, Molly M. Rockwood, Larry L. Maldonado, Jesus E. TI Evolutionary history of endemic Sulawesi squirrels constructed from UCEs and mitogenomes sequenced from museum specimens SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Wallacea; Ultraconserved elements; Species tree; Sciuridae; Ancient introgression ID SPECIES-TREE ANALYSIS; ULTRACONSERVED ELEMENTS; MAXIMUM-LIKELIHOOD; PHYLOGENETIC-RELATIONSHIPS; ANCIENT HYBRIDIZATION; PARTITIONING SCHEMES; TARGET CAPTURE; DNA PHYLOGENY; CYTOCHROME-B; SEA LEVELS AB Background: The Indonesian island of Sulawesi has a complex geological history. It is composed of several landmasses that have arrived at a near modern configuration only in the past few million years. It is the largest island in the biodiversity hotspot of Wallacea-an area demarcated by the biogeographic breaks between Wallace's and Lydekker's lines. The mammal fauna of Sulawesi is transitional between Asian and Australian faunas. Sulawesi's three genera of squirrels, all endemic (subfamily Nannosciurinae: Hyosciurus, Rubrisciurus and Prosciurillus), are of Asian origin and have evolved a variety of phenotypes that allow a range of ecological niche specializations. Here we present a molecular phylogeny of this radiation using data from museum specimens. High throughput sequencing technology was used to generate whole mitochondrial genomes and a panel of nuclear ultraconserved elements providing a large genome-wide dataset for inferring phylogenetic relationships. Results: Our analysis confirmed monophyly of the Sulawesi taxa with deep divergences between the three endemic genera, which predate the amalgamation of the current island of Sulawesi. This suggests lineages may have evolved in allopatry after crossing Wallace's line. Nuclear and mitochondrial analyses were largely congruent and well supported, except for the placement of Prosciurillus murinus. Mitochondrial analysis revealed paraphyly for Prosciurillus, with P. murinus between or outside of Hyosciurus and Rubrisciurus, separate from other species of Prosciurillus. A deep but monophyletic history for the four included species of Prosciurillus was recovered with the nuclear data. Conclusions: The divergence of the Sulawesi squirrels from their closest relatives dated to similar to 9.7-12.5 million years ago (MYA), pushing back the age estimate of this ancient adaptive radiation prior to the formation of the current conformation of Sulawesi. Generic level diversification took place around 9.7 MYA, opening the possibility that the genera represent allopatric lineages that evolved in isolation in an ancient proto-Sulawesian archipelago. We propose that incongruence between phylogenies based on nuclear and mitochondrial sequences may have resulted from biogeographic discordance, when two allopatric lineages come into secondary contact, with complete replacement of the mitochondria in one species. C1 [Hawkins, Melissa T. R.; McDonough, Molly M.; Maldonado, Jesus E.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC 20008 USA. [Hawkins, Melissa T. R.; Helgen, Kristofer M.; McDonough, Molly M.; Maldonado, Jesus E.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, MRC 108, POB 37012, Washington, DC 20013 USA. [Hawkins, Melissa T. R.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Leonard, Jennifer A.] CSIC, EBD, Conservat & Evolutionary Genet Grp, Seville 41092, Spain. [Rockwood, Larry L.] George Mason Univ, Dept Biol, Fairfax, VA 22030 USA. RP Hawkins, MTR (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC 20008 USA.; Hawkins, MTR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, MRC 108, POB 37012, Washington, DC 20013 USA. EM mtroberts2@gmail.com RI Leonard, Jennifer/A-7894-2010; CSIC, EBD Donana/C-4157-2011 OI Leonard, Jennifer/0000-0003-0291-7819; CSIC, EBD Donana/0000-0003-4318-6602 FU Smithsonian Conservation Biology Institute's Center for Conservation and Evolutionary Genetics; Smithsonian Institution's Grand Challenges Award Program; Smithsonian Institution's Small Grants Program; Spanish Research Council; Department of Biology (George Mason University); American Society of Mammalogists FX This project would not have been possible without the support of many. This includes Nancy Rotzel McInerney, Robert Fleischer and the Smithsonian Conservation Biology Institute's Center for Conservation and Evolutionary Genetics. Travis Glenn and Brant Faircloth provided training and guidance for the UCEs. Klaus-Peter Koepfli provided guidance in species tree and divergence dating analyses. Paul Frandsen performed the partitioning analysis on the UCE dataset. Anna Cornellas assisted with various aspects of library preparation. Anang Achmadi, Jake Esselstyn, and Kevin Rowe provided several critical samples from Sulawesi. Lawrence Flynn provided expertise and guidance regarding fossil calibrations. Funding for this project came from the Smithsonian Institution's Grand Challenges Award Program (JEM, KMH), the Smithsonian Institution's Small Grants Program (KMH, JEM and MTRH), the American Society of Mammalogists Grants-in-Aid, and travel award (MTRH, JEM, KMH), the Spanish Research Council (JAL, JEM) and the Department of Biology (George Mason University, to MTRH and LLR). Museum specimens were sampled from a variety of collections, including the National Museum of Natural History, Smithsonian Institution, Washington, DC (R. Thorington, D. Lunde, E. Langan, N. Edmison, S. Peurach, and L. Gordon), American Museum of Natural History, New York (R. Voss, and E. Westwig), and Museum Zoologicum Bogoriense, Research Center for Biology, Indonesia Institute of Sciences, Cibinong, Indonesia (A. Achmadi). Logistical support was provided by the Laboratorio de Ecologia Molecular, Estacion Biologica de Donana, CSIC (LEM-EBD). Two anonymous reviewers and the associate editor provided valuable feedback that improved the quality of this manuscript. NR 90 TC 2 Z9 2 U1 10 U2 27 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD APR 14 PY 2016 VL 16 AR 80 DI 10.1186/s12862-016-0650-z PG 16 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA DJ3TK UT WOS:000374129300001 PM 27075887 ER PT J AU Dubernet, ML Antony, BK Ba, YA Babikov, YL Bartschat, K Boudon, V Braams, BJ Chung, HK Daniel, F Delahaye, F Del Zanna, G de Urquijo, J Dimitrijevic, MS Domaracka, A Doronin, M Drouin, BJ Endres, CP Fazliev, AZ Gagarin, SV Gordon, IE Gratier, P Heiter, U Hill, C Jevremovic, D Joblin, C Kasprzak, A Krishnakumar, E Leto, G Loboda, PA Louge, T Maclot, S Marinkovic, BP Markwick, A Marquart, T Mason, HE Mason, NJ Mendoza, C Mihajlov, AA Millar, TJ Moreau, N Mulas, G Pakhomov, Y Palmeri, P Pancheshnyi, S Perevalov, VI Piskunov, N Postler, J Quinet, P Quintas-Sanchez, E Ralchenko, Y Rhee, YJ Rixon, G Rothman, LS Roueff, E Ryabchikova, T Sahal-Brechot, S Scheier, P Schlemmer, S Schmitt, B Stempels, E Tashkun, S Tennyson, J Tyuterev, VG Vujcic, V Wakelam, V Walton, NA Zatsarinny, O Zeippen, CJ Zwolf, CM AF Dubernet, M. L. Antony, B. K. Ba, Y. A. Babikov, Yu L. Bartschat, K. Boudon, V. Braams, B. J. Chung, H-K Daniel, F. Delahaye, F. Del Zanna, G. de Urquijo, J. Dimitrijevic, M. S. Domaracka, A. Doronin, M. Drouin, B. J. Endres, C. P. Fazliev, A. Z. Gagarin, S. V. Gordon, I. E. Gratier, P. Heiter, U. Hill, C. Jevremovic, D. Joblin, C. Kasprzak, A. Krishnakumar, E. Leto, G. Loboda, P. A. Louge, T. Maclot, S. Marinkovic, B. P. Markwick, A. Marquart, T. Mason, H. E. Mason, N. J. Mendoza, C. Mihajlov, A. A. Millar, T. J. Moreau, N. Mulas, G. Pakhomov, Yu Palmeri, P. Pancheshnyi, S. Perevalov, V. I. Piskunov, N. Postler, J. Quinet, P. Quintas-Sanchez, E. Ralchenko, Yu Rhee, Y-J Rixon, G. Rothman, L. S. Roueff, E. Ryabchikova, T. Sahal-Brechot, S. Scheier, P. Schlemmer, S. Schmitt, B. Stempels, E. Tashkun, S. Tennyson, J. Tyuterev, Vl G. Vujcic, V. Wakelam, V. Walton, N. A. Zatsarinny, O. Zeippen, C. J. Zwoelf, C. M. TI The virtual atomic and molecular data centre (VAMDC) consortium SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article DE databases; atoms; molecules; spectroscopy; kinetic data; astrophysics ID LOW-ENERGY-ELECTRON; LINE-DATA-BASE; IRRADIATION EXPERIMENTS RELEVANT; STIMULATED RAMAN-SPECTROSCOPY; HIGH-RESOLUTION SPECTROSCOPY; R-MATRIX METHOD; CW-CAVITY RING; ION IRRADIATION; CROSS-SECTIONS; COLLISIONAL DATABASE AB The Virtual Atomic and Molecular Data Centre (VAMDC) Consortium is a worldwide consortium which federates atomic and molecular databases through an e-science infrastructure and an organisation to support this activity. About 90% of the inter-connected databases handle data that are used for the interpretation of astronomical spectra and for modelling in many fields of astrophysics. Recently the VAMDC Consortium has connected databases from the radiation damage and the plasma communities, as well as promoting the publication of data from Indian institutes. This paper describes how the VAMDC Consortium is organised for the optimal distribution of atomic and molecular data for scientific research. It is noted that the VAMDC Consortium strongly advocates that authors of research papers using data cite the original experimental and theoretical papers as well as the relevant databases. C1 [Dubernet, M. L.; Ba, Y. A.; Delahaye, F.; Dimitrijevic, M. S.; Doronin, M.; Moreau, N.; Quintas-Sanchez, E.; Roueff, E.; Sahal-Brechot, S.; Zeippen, C. J.; Zwoelf, C. M.] Univ Paris 06, Univ Sorbonne, CNRS, LERMA,Observ Paris,PSL Res Univ, 5 Pl Janssen, F-92190 Meudon, France. [Antony, B. K.] Indian Sch Mines, Dept Appl Phys, Dhanbad 826004, Bihar, India. [Babikov, Yu L.; Fazliev, A. Z.; Perevalov, V. I.; Tashkun, S.] Russian Acad Sci, Inst Atmospher Opt, Zuev Sq 1, Tomsk 634021, Russia. [Babikov, Yu L.] Tomsk State Univ, Tomsk 634050, Russia. [Bartschat, K.; Zatsarinny, O.] Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. [Boudon, V.] Univ Bourgogne Franche Comte, CNRS, UMR 6303, Lab Interdisciplinaire Carnot Bourgogne, 9 Ave Alain Savary,BP 47 870, F-21078 Dijon, France. [Braams, B. J.; Chung, H-K] IAEA, Vienna Int Ctr, Div Phys & Chem Sci, Nucl Data Sect, A-1400 Vienna, Austria. [Daniel, F.; Schmitt, B.] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France. [Del Zanna, G.; Mason, H. E.] Ctr Math Sci, DAMTP, Wilberforce Rd, Cambridge CB3 0WA, England. [de Urquijo, J.] Univ Nacl Autonoma Mexico, Inst Ciencias Fis, POB 48-3, Cuernavaca 62251, Morelos, Mexico. [Dimitrijevic, M. S.; Jevremovic, D.; Vujcic, V.] Astron Observ, Volgina 7, Belgrade 11060, Serbia. [Domaracka, A.; Maclot, S.] UCN, ENSICAEN, CNRS, CIMAP,UMR 6252,CEA, Bd Henri Becquerel,BP 5133, F-14070 Caen 5, France. [Drouin, B. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Endres, C. P.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Gagarin, S. V.; Loboda, P. A.] Russian Fed Nucl Ctr All Russian Inst Tech Phys R, Snezhinsk, Russia. [Gordon, I. E.; Rothman, L. S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, MS50,60 Garden St, Cambridge, MA 02138 USA. [Gratier, P.; Wakelam, V.] Univ Bordeaux, LAB, UMR 5804, F-33270 Florac, France. [Gratier, P.; Wakelam, V.] CNRS, LAB, UMR 5804, F-33270 Florac, France. [Heiter, U.; Marquart, T.; Piskunov, N.; Stempels, E.] Uppsala Univ, Dept Phys & Astron, Box 516, SE-75120 Uppsala, Sweden. [Hill, C.; Tennyson, J.] UCL, Dept Phys & Astron, Mortimer St, London WC1E 6BT, England. [Joblin, C.; Louge, T.; Mulas, G.] Univ Toulouse, UPS OMP, CNRS, Inst Rech Astrophys & Planetol, 9 Av Colonel Roche, F-31028 Toulouse 4, France. [Kasprzak, A.] Observ Paris, SRCV, 61 Av Denfert Rochereau, F-75014 Paris, France. [Krishnakumar, E.] Tata Inst Fundamental Res, Dept Nucl & Atom Phys, Homi Bhabha Rd, Bombay 400005, Maharashtra, India. [Leto, G.] INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy. [Loboda, P. A.] Natl Res Nucl Univ, Moscow Engn Phys Inst MEPhI, Moscow, Russia. [Maclot, S.] Univ Caen Normandie, Esplanade Paix, CS 14032, F-14032 Caen 5, France. [Marinkovic, B. P.; Mihajlov, A. A.] Univ Belgrade, Inst Phys Belgrade, POB 57, Belgrade 11001, Serbia. [Markwick, A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. [Mason, N. J.] Open Univ, Dept Phys Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England. [Mendoza, C.] IVIC, Ctr Fis, POB 20632, Caracas 1020A, Venezuela. [Millar, T. J.] Queens Univ Belfast, Sch Math & Phys, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland. [Mulas, G.] Osservatorio Astron Cagliari, Ist Nazl AstroFis, Via Sci 5, I-09047 Selargius, CA, Italy. [Pakhomov, Yu; Ryabchikova, T.] RAS, Inst Astron, Pyatnitskaya 48, Moscow 119017, Russia. [Palmeri, P.; Quinet, P.] Univ Mons, Phys Atom & Astrophys, B-7000 Mons, Belgium. [Pancheshnyi, S.] ABB Corp Res, Segelhofstr 1K, CH-5405 Baden, Switzerland. [Postler, J.; Scheier, P.] Univ Innsbruck, Inst Ion Phys & Appl Phys, Technikerstr 25-3, A-6020 Innsbruck, Austria. [Quinet, P.] Univ Liege, IPNAS, B-4000 Liege, Belgium. [Ralchenko, Yu] NIST, Atom Spect Grp, Gaithersburg, MD 20899 USA. [Rhee, Y-J] Korea Atom Energy Res Inst, Nucl Data Ctr, Taejon 305353, South Korea. [Rixon, G.; Walton, N. A.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Schlemmer, S.] Univ Cologne, Inst Phys 1, zulpicher Str 77, D-50937 Kln, Germany. [Tyuterev, Vl G.] Univ Reims, GSMA, UMR CNRS 7331, Reims, France. [Vujcic, V.] Univ Belgrade, Fac Org Sci, Jove Ilica 33, Belgrade 11000, Serbia. RP Dubernet, ML (reprint author), Univ Paris 06, Univ Sorbonne, CNRS, LERMA,Observ Paris,PSL Res Univ, 5 Pl Janssen, F-92190 Meudon, France. EM marie-lise.dubernet@obspm.fr RI Tennyson, Jonathan/I-2222-2012; Scheier, Paul/E-3088-2010; Tashkun, Sergey/E-8682-2014; Marinkovic, Bratislav/D-3589-2012; Babikov, Yurii/E-8686-2014; Antony, Bobby Kachappilly/H-5302-2015; Pakhomov, Yury/B-5172-2014; OI Tennyson, Jonathan/0000-0002-4994-5238; Marinkovic, Bratislav/0000-0002-6904-6360; Antony, Bobby Kachappilly/0000-0003-2073-9681; Leto, Giuseppe/0000-0002-0040-5011; Wakelam, Valentine/0000-0001-9676-2605; Mulas, Giacomo/0000-0003-0602-6669; Millar, Tom/0000-0001-5178-3656 FU VAMDC project; SUP@VAMDC project [INFRA-2008-1.2.2, 239108, 313284]; Paris Astronomical Data Center; UK Science and Technology Facilities Council (STFC) [ST/M007731/1, ST/M007774/1, ST/M007766/1]; NASA; UK STFC; SOLID (First European SOLar Irradiance Data Exploitation), a collaborative SPACE Project under the Seventh Framework Programme (FP7) of the European Commission [313188]; Russian Foundation for Basic Research, RFBR grant [14-07-00863]; NASA Planetary Atmospheres Grant [NNX13AI59G]; ERC Advanced Investigator Project [267219]; United States National Science Foundation [PHY-1403245, PHY-1520970]; Dept. of Science and Technology (DST), Govt. of India; Austrian Science Fund (FWF) [P26635]; Nano-IBCT COST Action MP1002 (Nano-scale Insights into Ion Beam Cancer Therapy); LIA SAMIA; Tomsk State University D Mendeleev funding program; Ministry of Education, Science and Technological Development of Republic of Serbia [III44002, 176002, 171020]; XSEDE supercomputer allocation [PHY-090031] FX Support for VAMDC has been provided through the VAMDC and the SUP@VAMDC projects funded under the 'Combination of Collaborative Projects and Coordination and Support Actions' Funding Scheme of The Seventh Framework Program. Call topic: INFRA-2008-1.2.2 and INFRA-2012 Scientific Data Infrastructure. Grant Agreement numbers: 239108 and 313284. In addition we acknowledge support from Paris Astronomical Data Center. The UK nodes acknowledge support from the UK Science and Technology Facilities Council (STFC) under grants ST/M007731/1, ST/M007774/1 and ST/M007766/1. Portions of the research described in this paper were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The NIST ASD development is supported in part by NASA. GDZ and HEM work on CHIANTI has been supported by the UK STFC and SOLID (First European SOLar Irradiance Data Exploitation), a collaborative SPACE Project under the Seventh Framework Programme (FP7/2007-2013) of the European Commission under Grant Agreement N 313188. The Spectr-W3 project activities are currently supported in part by the Russian Foundation for Basic Research, RFBR grant Nr. 14-07-00863. LSR and IEG wish to thank the support from NASA Planetary Atmospheres Grant NNX13AI59G. ExoMol is supported by ERC Advanced Investigator Project 267219. ZB and KB acknowledge support from the United States National Science Foundation under grants PHY-1403245 and PHY-1520970, and by the XSEDE supercomputer allocation PHY-090031. AD and SM thank P Rousseau and B A Huber for fruitful discussions, Quentin Marie for the preparing of the RADAM-ION database website structure and Universite de Caen Normandie for hosting the website. BA is supported by the Dept. of Science and Technology (DST), Govt. of India. Part of this research was supported by the Austrian Science Fund (FWF): P26635. Support from Nano-IBCT COST Action MP1002 (Nano-scale Insights into Ion Beam Cancer Therapy) is also acknowledged. YLB and VGT acknowledge support from LIA SAMIA and from Tomsk State University D Mendeleev funding program. Belgrade node activities and the corresponding research are supported by projects III44002, 176002 and 171020 of the Ministry of Education, Science and Technological Development of Republic of Serbia. NR 162 TC 10 Z9 10 U1 10 U2 29 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD APR 14 PY 2016 VL 49 IS 7 AR 074003 DI 10.1088/0953-4075/49/7/074003 PG 18 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA DH6OS UT WOS:000372911000003 ER PT J AU Ziska, LH Pettis, JS Edwards, J Hancock, JE Tomecek, MB Clark, A Dukes, JS Loladze, I Polley, HW AF Ziska, Lewis H. Pettis, Jeffery S. Edwards, Joan Hancock, Jillian E. Tomecek, Martha B. Clark, Andrew Dukes, Jeffrey S. Loladze, Irakli Polley, H. Wayne TI Rising atmospheric CO2 is reducing the protein concentration of a floral pollen source essential for North American bees SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE bee health; carbon dioxide; Solidago canadensis; planetary health; pollen; protein ID APIS-MELLIFERA L.; HONEY-BEE; ELEVATED CO2; HUMAN-NUTRITION; PLANT-TISSUES; HYMENOPTERA; APIDAE; DIET; METAANALYSIS; TRANSPIRATION AB At present, there is substantive evidence that the nutritional content of agriculturally important food crops will decrease in response to rising levels of atmospheric carbon dioxide, C-a. However, whether C-a-induced declines in nutritional quality are also occurring for pollinator food sources is unknown. Flowering late in the season, goldenrod (Solidago spp.) pollen is a widely available autumnal food source commonly acknowledged by apiarists to be essential to native bee (e.g. Bombus spp.) and honeybee (Apis mellifera) health and winter survival. Using floral collections obtained from the Smithsonian Natural History Museum, we quantified C-a-induced temporal changes in pollen protein concentration of Canada goldenrod (Solidago canadensis), the most widespread Solidago taxon, from hundreds of samples collected throughout the USA and southern Canada over the period 1842-2014 (i.e. a C-a from approx. 280 to 398 ppm). In addition, we conducted a 2 year in situ trial of S. canadensis populations grown along a continuous C-a gradient from approximately 280 to 500 ppm. The historical data indicated a strong significant correlation between recent increases in Ca and reductions in pollen protein concentration (r(2) = 0.81). Experimental data confirmed this decrease in pollen protein concentration, and indicated that it would be ongoing as C-a continues to rise in the near term, i.e. to MO ppm (r(2) = 0.88). While additional data are needed to quantify the subsequent effects of reduced protein concentration for Canada goldenrod on bee health and population stability, these results are the first to indicate that increasing C-a can reduce protein content of a floral pollen source widely used by North American bees. C1 [Ziska, Lewis H.; Tomecek, Martha B.] USDA ARS, Crop Syst & Global Change Lab, Beltsville, MD 20705 USA. [Pettis, Jeffery S.] USDA ARS, Bee Res Lab, Beltsville, MD 20705 USA. [Edwards, Joan; Hancock, Jillian E.] Williams Coll, Dept Biol, Williamstown, MA 01267 USA. [Clark, Andrew] Smithsonian Inst, US Natl Herbarium, MRC 166,POB 37012, Washington, DC 20013 USA. [Dukes, Jeffrey S.] Purdue Univ, Dept Forestry & Nat Resources, W Lafayette, IN 47097 USA. [Dukes, Jeffrey S.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47097 USA. [Loladze, Irakli] Bryan Coll Hlth Sci, Bryan Med Ctr, Lincoln, NE 68506 USA. [Polley, H. Wayne] USDA ARS, Grassland Soil & Water Res Lab, Temple, TX 76502 USA. RP Ziska, LH (reprint author), USDA ARS, Crop Syst & Global Change Lab, Beltsville, MD 20705 USA. EM l.ziska@ars.usda.gov RI Dukes, Jeffrey/C-9765-2009; OI Dukes, Jeffrey/0000-0001-9482-7743; Loladze, Irakli/0000-0001-7615-7803 NR 58 TC 3 Z9 3 U1 25 U2 46 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD APR 13 PY 2016 VL 283 IS 1828 AR 20160414 DI 10.1098/rspb.2016.0414 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA DL9LU UT WOS:000375965600008 ER PT J AU Galvan-Quesada, S Doadrio, I Alda, F Perdices, A Reina, RG Varela, MG Hernandez, N Mendoza, AC Bermingham, E Dominguez-Dominguez, O AF Galvan-Quesada, Sesangari Doadrio, Ignacio Alda, Fernando Perdices, Anabel Gisela Reina, Ruth Garcia Varela, Martin Hernandez, Natividad Campos Mendoza, Antonio Bermingham, Eldredge Dominguez-Dominguez, Omar TI Molecular Phylogeny and Biogeography of the Amphidromous Fish Genus Dormitator Gill 1861 (Teleostei: Eleotridae) SO PLOS ONE LA English DT Article ID FRESH-WATER FISHES; CENTRAL-AMERICAN ISTHMUS; REEF FISH; EVOLUTIONARY HISTORY; POPULATION-STRUCTURE; ATLANTIC-OCEAN; LIFE-HISTORY; FAT SLEEPER; PHYLOGEOGRAPHY; DIVERGENCE AB Species of the genus Dormitator, also known as sleepers, are representatives of the amphidromous freshwater fish fauna that inhabit the tropical and subtropical coastal environments of the Americas and Western Africa. Because of the distribution of this genus, it could be hypothesized that the evolutionary patterns in this genus, including a pair of geminate species across the Central American Isthmus, could be explained by vicariance following the break-up of Gondwana. However, the evolutionary history of this group has not been evaluated. We constructed a time-scaled molecular phylogeny of Dormitator using mitochondrial (Cytochrome b) and nuclear (Rhodopsin and beta-actin) DNA sequence data to infer and date the cladogenetic events that drove the diversification of the genus and to relate them to the biogeographical history of Central America. Two divergent lineages of Dormitator were recovered: one that included all of the Pacific samples and another that included all of the eastern and western Atlantic samples. In contrast to the Pacific lineage, which showed no phylogeographic structure, the Atlantic lineage was geographically structured into four clades: Cameroon, Gulf of Mexico, West Cuba and Caribbean, showing evidence of potential cryptic species. The separation of the Pacific and Atlantic lineages was estimated to have occurred similar to 1 million years ago (Mya), whereas the four Atlantic clades showed mean times of divergence between 0.2 and 0.4 Mya. The splitting times of Dormitator between ocean basins are similar to those estimated for other geminate species pairs with shoreline estuarine preferences, which may indicate that the common evolutionary histories of the different clades are the result of isolation events associated with the closure of the Central American Isthmus and the subsequent climatic and oceanographic changes. C1 [Galvan-Quesada, Sesangari] Univ Michoacana, Programa Inst Doctorado Ciencias Biol, Morelia, Michoacan, Mexico. [Galvan-Quesada, Sesangari; Campos Mendoza, Antonio; Dominguez-Dominguez, Omar] Univ Michoacana, Fac Biol, Lab Biol Acuat, Morelia, Michoacan, Mexico. [Doadrio, Ignacio; Perdices, Anabel] CSIC, Museo Nacl Ciencias Nat, Dept Biodiversidad & Biol Evolut, E-28006 Madrid, Spain. [Alda, Fernando; Perdices, Anabel; Gisela Reina, Ruth; Bermingham, Eldredge] Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. [Garcia Varela, Martin] Univ Nacl Autonoma Mexico, Inst Biol, Mexico City 04510, DF, Mexico. [Hernandez, Natividad] Inst Med Trop Pedro Kouri, Apartado 601, Havana, Cuba. [Alda, Fernando] Louisiana State Univ, Dept Biol Sci, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Bermingham, Eldredge] Patricia & Phillip Frost Museum Sci, Miami, FL USA. RP Galvan-Quesada, S (reprint author), Univ Michoacana, Programa Inst Doctorado Ciencias Biol, Morelia, Michoacan, Mexico.; Galvan-Quesada, S; Dominguez-Dominguez, O (reprint author), Univ Michoacana, Fac Biol, Lab Biol Acuat, Morelia, Michoacan, Mexico. EM galygq@hotmail.com; goodeido@yahoo.com.mx FU CIC-UMSNH; PIFI-UMSNH program (Mexico); PAPIIT-UNAM [IN207213]; CONACyT [179048, 216640]; Museo Nacional de Ciencias Naturales-CSIC; Spanish Ministry of Economy and Competitiveness (Spain) [CGL2013-41375-P]; Smithsonian Tropical Research Institute (Panama) FX The authors are grateful for the following financial support for this research: CIC-UMSNH (2010, 2011) and PIFI-UMSNH program (Mexico) to ODD; PAPIIT-UNAM No. IN207213 and CONACyT No. 179048 (Mexico) to MGV; Museo Nacional de Ciencias Naturales-CSIC and Spanish Ministry of Economy and Competitiveness No. CGL2013-41375-P (Spain) to ID; Smithsonian Tropical Research Institute (Panama) to EB; CONACyT PhD scholarship No. 216640 granted to SGQ. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 90 TC 0 Z9 0 U1 6 U2 11 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 13 PY 2016 VL 11 IS 4 AR e0153538 DI 10.1371/journal.pone.0153538 PG 26 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DJ3UC UT WOS:000374131200105 PM 27074006 ER PT J AU Pineda, J Cho, W Starczak, V Govindarajan, AF Guzman, HM Girdhar, Y Holleman, RC Churchill, J Singh, H Ralston, DK AF Pineda, Jesus Cho, Walter Starczak, Victoria Govindarajan, Annette F. Guzman, Hector M. Girdhar, Yogesh Holleman, Rusty C. Churchill, James Singh, Hanumant Ralston, David K. TI A crab swarm at an ecological hotspot: patchiness and population density from AUV observations at a coastal, tropical seamount SO PEERJ LA English DT Article DE Swarms; Ecological hotspot; Patchiness; Panama; Eastern Pacific; Seamount; Pleuroncodes planipes; Hypoxic environment; Anomuran crabs ID PLEURONCODES-PLANIPES CRUSTACEA; BAJA-CALIFORNIA-SUR; UNDERWATER VEHICLES; CORAL-REEFS; WEST-COAST; PACIFIC; DECAPODA; ANOMURA; MEXICO; GALATHEIDAE AB A research cruise to Hannibal Bank, a seamount and an ecological hotspot in the coastal eastern tropical Pacific Ocean off Panama, explored the zonation, biodiversity, and the ecological processes that contribute to the seamount's elevated biomass. Here we describe the spatial structure of a benthic anomuran red crab population, using submarine video and autonomous underwater vehicle (AUV) photographs. High density aggregations and a swarm of red crabs were associated with a dense turbid layer 4-10 m above the bottom. The high density aggregations were constrained to 355-385 m water depth over the Northwest flank of the seamount, although the crabs also occurred at lower densities in shallower waters (similar to 280 m) and in another location of the seamount. The crab aggregations occurred in hypoxic water, with oxygen levels of 0.04 ml/l. Barcoding of Hannibal red crabs, and pelagic red crabs sampled in a mass stranding event in 2015 at a beach in San Diego, California, USA, revealed that the Panamanian and the Californian crabs are likely the same species, Pleuroncodes planipes, and these findings represent an extension of the southern endrange of this species. Measurements along a 1.6 km transect revealed three high density aggregations, with the highest density up to 78 crabs/m(2), and that the crabs were patchily distributed. Crab density peaked in the middle of the patch, a density structure similar to that of swarming insects. C1 [Pineda, Jesus; Starczak, Victoria; Govindarajan, Annette F.] Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA. [Cho, Walter] Point Loma Nazarene Univ, Dept Biol, San Diego, CA USA. [Guzman, Hector M.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Girdhar, Yogesh; Holleman, Rusty C.; Singh, Hanumant; Ralston, David K.] Woods Hole Oceanog Inst, Dept Appl Ocean Phys & Engn, Woods Hole, MA 02543 USA. [Holleman, Rusty C.] San Francisco Estuary Inst, Richmond, CA USA. [Churchill, James] Woods Hole Oceanog Inst, Dept Phys Oceanog, Woods Hole, MA 02543 USA. RP Pineda, J (reprint author), Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA. EM jpinedaa@hotmail.com FU Dalio Foundation, Inc, through the Woods Hole Oceanographic Institution FX This work was sponsored by a grant from the Dalio Foundation, Inc, through the Woods Hole Oceanographic Institution. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 68 TC 0 Z9 0 U1 7 U2 7 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD APR 12 PY 2016 VL 4 AR e1770 DI 10.7717/peerj.1770 PG 23 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DJ4GN UT WOS:000374163500001 PM 27114859 ER PT J AU Zhao, GB Wang, YT Ross, AJ Shandera, S Percival, WJ Dawson, KS Kneib, JP Myers, AD Brownstein, JR Comparat, J Delubac, T Gao, PY Hojjati, A Koyama, K McBride, CK Meza, A Newman, JA Palanque-Delabrouille, N Pogosian, L Prada, F Rossi, G Schneider, DP Seo, HJ Tao, CL Wang, DD Yeche, C Zhang, HY Zhang, YC Zhou, X Zhu, FZ Zou, H AF Zhao, Gong-Bo Wang, Yuting Ross, Ashley J. Shandera, Sarah Percival, Will J. Dawson, Kyle S. Kneib, Jean-Paul Myers, Adam D. Brownstein, Joel R. Comparat, Johan Delubac, Timothee Gao, Pengyuan Hojjati, Alireza Koyama, Kazuya McBride, Cameron K. Meza, Andres Newman, Jeffrey A. Palanque-Delabrouille, Nathalie Pogosian, Levon Prada, Francisco Rossi, Graziano Schneider, Donald P. Seo, Hee-Jong Tao, Charling Wang, Dandan Yeche, Christophe Zhang, Hanyu Zhang, Yuecheng Zhou, Xu Zhu, Fangzhou Zou, Hu TI The extended Baryon Oscillation Spectroscopic Survey: a cosmological forecast SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE dark energy; large-scale structure of Universe ID DIGITAL SKY SURVEY; SDSS-III; ACOUSTIC-OSCILLATIONS; NON-GAUSSIANITY; NEUTRINO MASS; DATA SETS; GALAXIES; QUASARS; FOREST; CONSTRAINTS AB We present a science forecast for the extended Baryon Oscillation Spectroscopic Survey (eBOSS) survey. Focusing on discrete tracers, we forecast the expected accuracy of the baryonic acoustic oscillation (BAO), the redshift-space distortion (RSD) measurements, the fNL parameter quantifying the primordial non-Gaussianity, the dark energy and modified gravity parameters. We also use the line-of-sight clustering in the Lyman a forest to constrain the total neutrino mass. We find that eBOSS luminous red galaxies, emission line galaxies and clustering quasars can achieve a precision of 1, 2.2 and 1.6 per cent, respectively, for spherically averaged BAO distance measurements. Using the same samples, the constraint on fob is expected to be 2.5, 3.3 and 2.8 per cent, respectively. For primordial non-Gaussianity, eBOSS alone can reach an accuracy of a (f(NL)) similar to 10-15. eBOSS can at most improve the dark energy figure of merit by a factor of 3 for the Chevallier-Polarski-Linder parametrization, and can well constrain three eigenmodes for the general equation-of-state parameter. eBOSS can also significantly improve constraints on modified gravity parameters by providing the RSD information, which is highly complementary to constraints obtained from weak lensing measurements. A principal component analysis shows that eBOSS can measure the eigenmodes of the effective Newton's constant to 2 per cent precision; this is a factor of 10 improvement over that achievable without eBOSS. Finally, we derive the eBOSS constraint (combined with Planck, Dark Energy Survey and BOSS) on the total neutrino mass, sigma (Em(upsilon)) = 0.03 eV (68 per cent CL), which in principle makes it possible to distinguish between the two scenarios of neutrino mass hierarchies. C1 [Zhao, Gong-Bo; Wang, Yuting; Gao, Pengyuan; Wang, Dandan; Zhang, Hanyu; Zhang, Yuecheng; Zhou, Xu; Zou, Hu] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Zhao, Gong-Bo; Wang, Yuting; Ross, Ashley J.; Percival, Will J.; Koyama, Kazuya] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England. [Ross, Ashley J.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Shandera, Sarah; Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Shandera, Sarah] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Dawson, Kyle S.; Brownstein, Joel R.] Univ Utah, Dept Phys & Astron, 115 S 1400 E, Salt Lake City, UT 84112 USA. [Kneib, Jean-Paul; Delubac, Timothee] Ecole Polytech Fed Lausanne, Astrophys Lab, CH-1015 Lausanne, Switzerland. [Kneib, Jean-Paul] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Comparat, Johan; Prada, Francisco] Univ Autonoma Madrid, Inst Fis Teor, UAM CSIC, E-28049 Madrid, Spain. [Hojjati, Alireza] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Hojjati, Alireza; Pogosian, Levon] Simon Fraser Univ, Dept Phys, Burnaby, BC V5A 1S6, Canada. [McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Meza, Andres] Univ Andres Bello, Dept Ciencias Fis, Avda Republ 220, Santiago, Chile. [Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, 3941 OHara St, Pittsburgh, PA 15260 USA. [Newman, Jeffrey A.] Univ Pittsburgh, PITT PACC, 3941 OHara St, Pittsburgh, PA 15260 USA. [Palanque-Delabrouille, Nathalie; Yeche, Christophe] IRFU SPP, Ctr Saclay, CEA, F-91191 Gif Sur Yvette, France. [Prada, Francisco] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain. [Prada, Francisco] Inst Astrofis Andalucia CSIC, E-18080 Granada, Spain. [Rossi, Graziano] Sejong Univ, Dept Astron & Space Sci, Seoul 143747, South Korea. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Seo, Hee-Jong] Ohio Univ, Dept Phys & Astron, 251B Clippinger Labs, Athens, OH 45701 USA. [Tao, Charling] CNRS IN2P3 Luminy, Ctr Phys Particules Marseille, Case 907, F-13288 Marseille 9, France. [Tao, Charling] Univ Mediterranee, Case 907, F-13288 Marseille 9, France. [Tao, Charling] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Tao, Charling] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China. [Zhu, Fangzhou] Yale Univ, Dept Phys, New Haven, CT 06511 USA. RP Zhao, GB (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.; Zhao, GB (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England. EM gbzhao@nao.cas.cn RI Gao, Peng/F-3114-2012; OI Gao, Peng/0000-0002-4963-2282; Meza, Andres/0000-0002-9460-7828 FU Strategic Priority Research Program 'The Emergence of Cosmological Structures' of the Chinese Academy of Sciences [XDB09000000]; 1000 Young Talents program in China; NSFC [11403034]; NSERC; STFC [ST/K00090/1]; European Research Council [646702]; National Research Foundation of Korea (NRF) through NRF-SGER [2014055950]; Alfred P. Sloan Foundation; US Department of Energy Office of Science; Center for High Performance Computing at the University of Utah; Brazilian Participation Group; Carnegie Institution for Science; Carnegie Mellon University; Chilean Participation Group; French Participation Group; Harvard-Smithsonian Center for Astrophysics; Instituto de Astrofisica de Canarias; Johns Hopkins University; Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo; Lawrence Berkeley National Laboratory; Leibniz Institut fur Astrophysik Potsdam (AIP); Max-Planck-Institut fur Astronomic (MPIA Heidelberg); Max-Planck-Institut fur Astrophysik (MPA Garching); Max-Planck-Institut fur Extraterrestrische Physik (MPE); National Astronomical Observatory of China; New Mexico State University; New York University; University of Notre Dame; Observatario Nacional/MCTI; Ohio State University; Pennsylvania State University; Shanghai Astronomical Observatory; United Kingdom Participation Group; Universidad Nacional Autonoma de Mexico; University of Arizona; University of Colorado Boulder; University of Oxford; University of Portsmouth; University of Utah; University of Virginia; University of Washington; University of Wisconsin; Vanderbilt University; Yale University FX G-BZ and YW are supported by the Strategic Priority Research Program 'The Emergence of Cosmological Structures' of the Chinese Academy of Sciences Grant No. XDB09000000. G-BZ is supported by the 1000 Young Talents program in China. YW is supported by the NSFC grant no. 11403034. AH and LP are supported by NSERC. KK is supported by the STFC through the consolidated grant ST/K00090/1, and the European Research Council through grant 646702 (CosTesGrav). GR is supported by the National Research Foundation of Korea (NRF) through NRF-SGER 2014055950.r Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the US Department of Energy Office of Science and the Participating Institutions. SDSSIV acknowledges support and resources from the Center for High Performance Computing at the University of Utah. The SDSS web site is www.sdss.org.r SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofisica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut fur Astrophysik Potsdam (AIP), Max-Planck-Institut fur Astronomic (MPIA Heidelberg), Max-Planck-Institut fur Astrophysik (MPA Garching), Max-Planck-Institut fur Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observatario Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autonoma de Mexico, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University and Yale University. NR 70 TC 18 Z9 18 U1 5 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 APR 11 PY 2016 VL 457 IS 3 BP 2377 EP 2390 DI 10.1093/mnras/stw135 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI6BJ UT WOS:000373583900008 ER PT J AU Henshaw, JD Longmore, SN Kruijssen, JMD Davies, B Bally, J Barnes, A Battersby, C Burton, M Cunningham, MR Dale, JE Ginsburg, A Immer, K Jones, PA Kendrew, S Mills, EAC Molinari, S Moore, TJT Ott, J Pillai, T Rathborne, J Schilke, P Schmiedeke, A Testi, L Walker, D Walsh, A Zhang, Q AF Henshaw, J. D. Longmore, S. N. Kruijssen, J. M. D. Davies, B. Bally, J. Barnes, A. Battersby, C. Burton, M. Cunningham, M. R. Dale, J. E. Ginsburg, A. Immer, K. Jones, P. A. Kendrew, S. Mills, E. A. C. Molinari, S. Moore, T. J. T. Ott, J. Pillai, T. Rathborne, J. Schilke, P. Schmiedeke, A. Testi, L. Walker, D. Walsh, A. Zhang, Q. TI Molecular gas kinematics within the central 250 pc of the Milky Way SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: formation; ISM: clouds; ISM: kinematics and dynamics; ISM: structure-Galaxy: centre; galaxies: ISM ID GALACTIC PLANE SURVEY; HIGH-RESOLUTION OBSERVATIONS; CENTER CLOUD G0.253+0.016; MASSIVE STAR-FORMATION; CENTER DUST RIDGE; 1720 MHZ MASERS; SGR A-ASTERISK; LARGE-SCALE; CENTER REGION; BARRED POTENTIALS AB Using spectral line observations of HNCO, N2H+, and HNC, we investigate the kinematics of dense gas in the central similar to 250 pc of the Galaxy. We present SCOUSE (Semi -automated multi-COmponent Universal Spectral-line fitting Engine), a line-fitting algorithm designed to analyse large volumes of spectral line data efficiently and systematically. Unlike techniques which do not account for complex line profiles, SCOUSE accurately describes the {l, b, v(LsR)} distribution of Central Molecular Zone (CMZ) gas, which is asymmetric about Sgr A* in both position and velocity. Velocity dispersions range from 2.6 km s(-1) < a < 53.1 km s (1) A median dispersion of 9.8 km s 1, translates to a Mach number, M-3D > 28. The gas is distributed throughout several 'streams', with projected lengths similar to 100-250 pc. We link the streams to individual clouds and sub-regions, including Sgr C, the 20 and 50 km s 1 clouds, the dust ridge, and Sgr B2. Shell-like emission features can be explained by the projection of independent molecular clouds in Sgr C and the newly identified conical profile of Sgr B2 in {l, b, vi sR} space. These features have previously invoked supernova-driven shells and cloud-cloud collisions as explanations. We instead caution against structure identification in velocity-integrated emission maps. Three geometries describing the 3D structure of the CMZ are investigated: (i) two spiral arms; (ii) a closed elliptical orbit; (iii) an open stream. While two spiral arms and an open stream qualitatively reproduce the gas distribution, the most recent parametrization of the closed elliptical orbit does not. Finally, we discuss how proper motion measurements of masers can distinguish between these geometries, and suggest that this effort should be focused on the 20 km s(-1) and 50 km s(-1) clouds and Sgr C. C1 [Henshaw, J. D.; Longmore, S. N.; Davies, B.; Barnes, A.; Moore, T. J. T.; Walker, D.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Kruijssen, J. M. D.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. [Kruijssen, J. M. D.] Heidelberg Univ, Zentrum Astronomie, Astron Rechen Inst, Monchhofstr 12-14, D-69120 Heidelberg, Germany. [Bally, J.] Univ Colorado, Dept Astrophys & Planetary Sci, UCB 389, Boulder, CO 80309 USA. [Battersby, C.; Zhang, Q.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Burton, M.; Cunningham, M. R.; Jones, P. A.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Dale, J. E.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Ginsburg, A.; Immer, K.; Testi, L.] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Kendrew, S.] Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. [Mills, E. A. C.; Ott, J.] Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA. [Molinari, S.] INAF Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere 100, I-00133 Rome, Italy. [Pillai, T.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Rathborne, J.] CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia. [Schilke, P.; Schmiedeke, A.] Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. [Walsh, A.] Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia. RP Henshaw, JD (reprint author), Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. EM j.d.henshaw@ljmu.ac.uk RI Molinari, Sergio/O-4095-2016; OI Molinari, Sergio/0000-0002-9826-7525; Cunningham, Maria/0000-0001-7020-6176; Zhang, Qizhou/0000-0003-2384-6589; Kendrew, Sarah/0000-0002-7612-0469 FU Commonwealth of Australia; Australian Research Council (ARC); UNSW, Sydney; Monash Universities; CSIRO; Gliese Fellowship FX We thank the anonymous referee for their comments which have helped to improve the clarity of this paper. JDH would like to thank Paola Caselli and Cormac Purcell for discussions which have helped to improve the implementation of SCOUSE, and Jens Kauffmann for providing comments which have helped to improve the presentation of the paper. The data were obtained using the Mopra radio telescope, a 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 (UNSW) digital filter bank (the UNSW-MOPS) used for the observations with Mopra was provided with support from the Australian Research Council (ARC), UNSW, Sydney and Monash Universities, as well as the CSIRO. JMDK is funded by a Gliese Fellowship. NR 106 TC 9 Z9 9 U1 5 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 11 PY 2016 VL 457 IS 3 BP 2675 EP 2702 DI 10.1093/mnras/stw121 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI6BJ UT WOS:000373583900030 ER PT J AU Haider, M Steinhauser, D Vogelsberger, M Genel, S Springel, V Torrey, P Hernquist, L AF Haider, M. Steinhauser, D. Vogelsberger, M. Genel, S. Springel, V. Torrey, P. Hernquist, L. TI Large-scale mass distribution in the Illustris simulation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: haloes; dark matter; large-scale structure of Universe ID GALAXY FORMATION PHYSICS; HOT INTERGALACTIC MEDIUM; COSMOLOGICAL SIMULATIONS; LOW-REDSHIFT; BLACK-HOLES; HYDRODYNAMICAL SIMULATIONS; MISSING BARYONS; AGN FEEDBACK; MOVING MESH; COSMIC TIME AB Observations at low redshifts thus far fail to account for all of the baryons expected in the Universe according to cosmological constraints. A large fraction of the baryons presumably resides in a thin and warm-hot medium between the galaxies, where they are difficult to observe due to their low densities and high temperatures. Cosmological simulations of structure formation can be used to verify this picture and provide quantitative predictions for the distribution of mass in different large-scale structure components. Here we study the distribution of baryons and dark matter at different epochs using data from the Illustris simulation. We identify regions of different dark matter density with the primary constituents of large-scale structure, allowing us to measure mass and volume of haloes, filaments and voids. At redshift zero, we find that 49 per cent of the dark matter and 23 per cent of the baryons are within haloes more massive than the resolution limit of 2 x 10(8) M-circle dot. The filaments of the cosmic web host a further 45 per cent of the dark matter and 46 per cent of the baryons. The remaining 31 per cent of the baryons reside in voids. The majority of these baryons have been transported there through active galactic nuclei feedback. We note that the feedback model of Illustris is too strong for heavy haloes, therefore it is likely that we are overestimating this amount. Categorizing the baryons according to their density and temperature, we find that 17.8 per cent of them are in a condensed state, 21.6 per cent are present as cold, diffuse gas, and 53.9 per cent are found in the state of a warm-hot intergalactic medium. C1 [Haider, M.; Steinhauser, D.] Univ Innsbruck, Inst Astro & Teilchenphys, Technikerstr 25-8, A-6020 Innsbruck, Austria. [Vogelsberger, M.; Torrey, P.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Genel, S.] Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA. [Springel, V.] Heidelberg Inst Theoret Studies, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany. [Springel, V.] Heidelberg Univ, Zentrum Astron, Astron Recheninst, Monchhofstr 12-14, D-69120 Heidelberg, Germany. [Torrey, P.] CALTECH, TAPIR, Mailcode 350-17, Pasadena, CA 91125 USA. [Hernquist, L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Haider, M (reprint author), Univ Innsbruck, Inst Astro & Teilchenphys, Technikerstr 25-8, A-6020 Innsbruck, Austria. EM markus.haider@uibk.ac.at FU office of the vice rector for research of the University of Innsbruck [DB: 194272]; doctoral school - Computational Interdisciplinary Modelling FWF DK-plus [W1227]; Austrian Federal Ministry of Science, Research and Economy, UniInfrastrukturprogramm of the Focal Point Scientific Computing at the University of Innsbruck; NASA through Hubble Fellowship - STScI [HST-HF2-51341.001-A]; NASA [NAS5-26555]; European Research Council through ERC-StG grant [EXAGAL-308037] FX MH and DS thank their colleagues at the Institute for Astro- and Particle Physics at the University of Innsbruck for usefull discussions, especially Francine Marleau, Dominic Clancy, Rebecca Habas and Matteo Bianconi. DS acknowledges the research grant from the office of the vice rector for research of the University of Innsbruck (project DB: 194272) and the doctoral school - Computational Interdisciplinary Modelling FWF DK-plus (W1227). This work was supported by the Austrian Federal Ministry of Science, Research and Economy as part of the UniInfrastrukturprogramm of the Focal Point Scientific Computing at the University of Innsbruck. SG acknowledges support provided by NASA through Hubble Fellowship grant HST-HF2-51341.001-A awarded by the STScI, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. VS acknowledges support through the European Research Council through ERC-StG grant EXAGAL-308037. NR 47 TC 2 Z9 2 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 11 PY 2016 VL 457 IS 3 BP 3024 EP 3035 DI 10.1093/mnras/stw077 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI6BJ UT WOS:000373583900056 ER PT J AU Chiu, I Dietrich, JP Mohr, J Applegate, DE Benson, BA Bleem, LE Bayliss, MB Bocquet, S Carlstrom, JE Capasso, R Desai, S Gangkofner, C Gonzalez, AH Gupta, N Hennig, C Hoekstra, H von der Linden, A Liu, J McDonald, M Reichardt, CL Saro, A Schrabback, T Strazzullo, V Stubbs, CW Zenteno, A AF Chiu, I. Dietrich, J. P. Mohr, J. Applegate, D. E. Benson, B. A. Bleem, L. E. Bayliss, M. B. Bocquet, S. Carlstrom, J. E. Capasso, R. Desai, S. Gangkofner, C. Gonzalez, A. H. Gupta, N. Hennig, C. Hoekstra, H. von der Linden, A. Liu, J. McDonald, M. Reichardt, C. L. Saro, A. Schrabback, T. Strazzullo, V. Stubbs, C. W. Zenteno, A. TI Detection of enhancement in number densities of background galaxies due to magnification by massive galaxy clusters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; galaxies: clusters: individual; cosmology: observations; large-scale structure of Universe ID WEAK-LENSING MASSES; SOUTH-POLE TELESCOPE; DARK-MATTER HALOS; DIGITAL SKY SURVEY; K-BAND PROPERTIES; PHOTOMETRIC REDSHIFTS; COSMIC MAGNIFICATION; LUMINOSITY FUNCTION; IMAGE-ANALYSIS; SHEAR AB We present a detection of the enhancement in the number densities of background galaxies induced from lensing magnification and use it to test the Sunyaev-Zel'dovich effect (SZE-) inferred masses in a sample of 19 galaxy clusters with median redshift z similar or equal to 0.42 selected from the South Pole Telescope SPT-SZ survey. These clusters are observed by the Megacam on the Magellan Clay Telescope though gri filters. Two background galaxy populations are selected for this study through their photometric colours; they have median redshifts zmedian similar or equal to 0.9 (low-z background) and z(median) similar or equal to 1.8 (high-z background). Stacking these populations, we detect the magnification bias effect at 3.3 sigma and 1.3 sigma for the low-and high-z backgrounds, respectively. We fit Navarro, Frenk and White models simultaneously to all observed magnification bias profiles to estimate the multiplicative factor. that describes the ratio of the weak lensing mass to the mass inferred from the SZE observable-mass relation. We further quantify systematic uncertainties in. resulting from the photometric noise and bias, the cluster galaxy contamination and the estimations of the background properties. The resulting. for the combined background populations with 1 sigma uncertainties is 0.83 +/- 0.24(stat) +/- 0.074(sys), indicating good consistency between the lensing and the SZE-inferred masses. We use our best-fitting eta to predict the weak lensing shear profiles and compare these predictions with observations, showing agreement between the magnification and shear mass constraints. This work demonstrates the promise of using the magnification as a complementary method to estimate cluster masses in large surveys. C1 [Chiu, I.; Dietrich, J. P.; Mohr, J.; Bocquet, S.; Capasso, R.; Desai, S.; Gangkofner, C.; Gupta, N.; Hennig, C.; Liu, J.; Saro, A.; Strazzullo, V.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Chiu, I.; Dietrich, J. P.; Mohr, J.; Bocquet, S.; Capasso, R.; Desai, S.; Gangkofner, C.; Gupta, N.; Hennig, C.; Liu, J.; Saro, A.] Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany. [Mohr, J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Applegate, D. E.; Schrabback, T.] Argelander Inst Astron, Auf Hugel 71, D-53121 Bonn, Germany. [Benson, B. A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.] Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Bleem, L. E.] Univ Chicago, Dept Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Bleem, L. E.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA. [Bayliss, M. B.; Stubbs, C. W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Bayliss, M. B.; Stubbs, C. W.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Hoekstra, H.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [von der Linden, A.] Stanford Univ, KIPAC, 452 Lomita Mall, Stanford, CA 94305 USA. [von der Linden, A.] Stanford Univ, Dept Phys, 452 Lomita Mall, Stanford, CA 94305 USA. [von der Linden, A.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. [McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Zenteno, A.] Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. RP Chiu, I; Dietrich, JP; Mohr, J (reprint author), Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany.; Chiu, I; Dietrich, JP; Mohr, J (reprint author), Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany.; Mohr, J (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. EM inonchiu@usm.lmu.de; dietrich@usm.lmu.de; jmohr@USM.LMU.de OI Dietrich, Jorg/0000-0002-8134-9591; Stern, Corvin/0000-0003-4406-6127; Hoekstra, Henk/0000-0002-0641-3231 FU DFG Cluster of Excellence 'Origin and Structure of the Universe'; Transregio programme 'The Dark Universe' [TR33]; German Federal Ministry of Economics and Technology (BMWi) through DLR [50 OR 1210, 50 OR 1308, 50 OR 1407]; Australian Research Council's Discovery Projects scheme [DP150103208]; National Science Foundation [ANT-0638937]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation FX We acknowledge the support by the DFG Cluster of Excellence 'Origin and Structure of the Universe' and the Transregio programme TR33 'The Dark Universe'. DA and TS acknowledge support from the German Federal Ministry of Economics and Technology (BMWi) provided through DLR under projects 50 OR 1210, 50 OR 1308, and 50 OR 1407. CR acknowledges support from the Australian Research Council's Discovery Projects scheme (DP150103208). The South Pole Telescope is supported by the National Science Foundation through grant ANT-0638937. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation and the Gordon and Betty Moore Foundation. Optical imaging data were obtained with Megacam on the 6.5 m Magellan Clay Telescope. NR 64 TC 4 Z9 4 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 11 PY 2016 VL 457 IS 3 BP 3050 EP 3065 DI 10.1093/mnras/stw190 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI6BJ UT WOS:000373583900058 ER PT J AU Avrett, E Tian, H Landi, E Curdt, W Wuelser, JP AF Avrett, E. Tian, H. Landi, E. Curdt, W. Wuelser, J. -P. TI MODELING THE CHROMOSPHERE OF A SUNSPOT AND THE QUIET SUN (vol 811, 87, 2015) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Avrett, E.; Tian, H.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Landi, E.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Curdt, W.] Max Planck Inst Sonnensyst Forsch, Gottingen, Germany. [Wuelser, J. -P.] Lockheed Martin Adv Techonol Ctr, Palo Alto, CA USA. RP Avrett, E (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2016 VL 821 IS 1 AR 70 DI 10.3847/0004-637X/821/1/70 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI9GB UT WOS:000373809000070 ER PT J AU Barnacka, A Geller, MJ Dell'Antonio, IP Zitrin, A AF Barnacka, Anna Geller, Margaret J. Dell'Antonio, Ian P. Zitrin, Adi TI THE STRUCTURE OF THE STRONGLY LENSED GAMMA-RAY SOURCE B2 0218+35 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; galaxies: jets; gamma rays: general; gravitational lensing: strong; quasars: individual (B2 0218+35) ID HUBBLE-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; RELATIVISTIC MAGNETIC RECONNECTION; EXTENDED RADIO JETS; EARLY-TYPE GALAXIES; X-RAY; PARTICLE-ACCELERATION; GRAVITATIONAL LENSES; PAIR PLASMAS AB Strong gravitational lensing is a powerful tool for resolving the high-energy universe. We combine the temporal resolution of Fermi-LAT, the angular resolution of radio telescopes, and the independently and precisely known Hubble constant from the analysis by the Planck collaboration, to resolve the spatial origin of gamma-ray flares in the strongly lensed source B2. 0218+35. The lensing model achieves 1 mas spatial resolution of the source at gamma-ray energies. The data imply that the gamma-ray flaring sites are separate from the radio core: the bright gamma-ray flare (MJD: 56160-56280) occurred 51 +/- 8pc from the 15 GHz radio core, toward the central engine. This displacement is significant at the similar to 3 sigma level, and is limited primarily by the precision of the Hubble constant. B2. 0218+35 is the first source where the position of the gamma-ray emitting region relative to the radio core can be resolved. We discuss the potential of an ensemble of strongly lensed high-energy sources for elucidating the physics of distant variable sources based on data from Chandra and SKA. C1 [Barnacka, Anna; Geller, Margaret J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barnacka, Anna] Jagiellonian Univ, Astron Observ, Krakow, Poland. [Dell'Antonio, Ian P.] Brown Univ, Dept Phys, Providence, RI 02912 USA. [Zitrin, Adi] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RP Barnacka, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-20, Cambridge, MA 02138 USA. EM abarnacka@cfa.harvard.edu OI Barnacka, Anna/0000-0001-5655-4158; Geller, Margaret/0000-0002-9146-4876 FU NASA; Smithsonian Institution FX AB is supported by NASA through Einstein Postdoctoral Fellowship. MJG is supported by the Smithsonian Institution. NR 120 TC 2 Z9 2 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2016 VL 821 IS 1 AR 58 DI 10.3847/0004-637X/821/1/58 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI9GB UT WOS:000373809000058 ER PT J AU Drout, MR Milisavljevic, D Parrent, J Margutti, R Kamble, A Soderberg, AM Challis, P Chornock, R Fong, W Frank, S Gehrels, N Graham, ML Hsiao, E Itagaki, K Kasliwal, M Kirshner, RP Macomb, D Marion, GH Norris, J Phillips, MM AF Drout, M. R. Milisavljevic, D. Parrent, J. Margutti, R. Kamble, A. Soderberg, A. M. Challis, P. Chornock, R. Fong, W. Frank, S. Gehrels, N. Graham, M. L. Hsiao, E. Itagaki, K. Kasliwal, M. Kirshner, R. P. Macomb, D. Marion, G. H. Norris, J. Phillips, M. M. TI THE DOUBLE-PEAKED SN 2013ge: A TYPE Ib/c SN WITH AN ASYMMETRIC MASS EJECTION OR AN EXTENDED PROGENITOR ENVELOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (SN 2013ge) ID CORE-COLLAPSE SUPERNOVAE; GAMMA-RAY BURSTS; NEUTRINO-DRIVEN EXPLOSIONS; RADIO OBSERVATIONS REVEAL; LIGHT CURVES; IA SUPERNOVAE; IBC SUPERNOVA; IC SUPERNOVAE; SHOCK BREAKOUT; CASSIOPEIA-A AB We present extensive multiwavelength (radio to X-ray) observations of the Type Ib/c supernova (SN Ib/c) SN 2013ge from -13 to +457 days relative to maximum light, including a series of optical spectra and Swift UV-optical photometry beginning 2-4 days post-explosion. This data set makes SN 2013ge one of the best-observed normal SNe Ib/c at early times-when the light curve is particularly sensitive to the progenitor configuration and mixing of radioactive elements-and reveals two distinct light curve components in the UV bands. The first component rises over 4-5 days and is visible for the first week post-explosion. Spectra of the first component have blue continua and show a plethora of moderately high. velocity (similar to 15,000 km s(-1)) but narrow (similar to 3500 km s(-1)) spectroscopic features, indicating that the line-forming region is restricted. The explosion parameters estimated for the bulk explosion (M-ej similar to 2-3 M-circle dot; E-K similar to (1-2) x 10(51) erg) are standard for SNe Ib/c, and there is evidence for weak He features at early times-in an object that. would have otherwise been classified as Type Ic. In addition, SN 2013ge exploded in a low-metallicity environment (similar to 0.5 Z(circle dot)), and we have obtained some of the deepest radio and X-ray limits for an SN Ib/c to date, which constrain the progenitor mass-loss rate to be (M) over dot < 4 x 10(-6) M-circle dot yr(-1). We are left with two distinct progenitor scenarios for SN 2013ge, depending on our interpretation of the early emission. If the first component is cooling envelope emission, then the progenitor of SN 2013ge either possessed an extended (greater than or similar to 30 R-circle dot) envelope or ejected a portion of its envelope in the final less than or similar to 1 yr before core. collapse. Alternatively, if the first component is due to outwardly mixed Ni-56, then our observations are consistent with the asymmetric ejection of a distinct clump of nickel-rich material at high velocities. Current models for the collision of an. SN. shock with a binary companion cannot reproduce both the timescale and luminosity of the early emission in SN 2013ge. Finally, the spectra of the first component of SN 2013ge are similar to those of the rapidly declining SN 2002bj. C1 [Drout, M. R.; Milisavljevic, D.; Parrent, J.; Margutti, R.; Kamble, A.; Soderberg, A. M.; Challis, P.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chornock, R.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Clippinger Lab 251B, Athens, OH 45701 USA. [Fong, W.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Frank, S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Graham, M. L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hsiao, E.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Hsiao, E.; Phillips, M. M.] Las Campanas Observ, Carnegie Observ, Colina El Pino, Chile. [Itagaki, K.] Itagaki Astron Observ, Yamagata, Yamagata 9902492, Japan. [Kasliwal, M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Macomb, D.; Norris, J.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. [Marion, G. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Drout, MR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mdrout@cfa.harvard.edu OI Parrent, Jerod/0000-0002-5103-7706; Margutti, Raffaella/0000-0003-4768-7586 FU NSF Graduate Research Fellowship; Gary and Cynthia Bengier; NSF [AST-1211916, AST-9987045]; Danish Agency for Science and Technology and Innovation through a Sapere Aude Level 2 grant; NSF Telescope System Instrumentation Program (TSIP); Ohio Board of Regents; Ohio State University Office of Research FX We thank the anonymous referee for numerous comments that improved this manuscript. M.R.D. thanks L. Z. Kelley, D. Kasen, and E. Ramirez-Ruiz for useful discussions. We thank N. Morrell for obtaining some of the observations reported here. M.R.D. is supported in part by the NSF Graduate Research Fellowship. M.L.G.'s position in the supernova research group at UC Berkeley is supported by Gary and Cynthia Bengier and NSF grant AST-1211916. E.Y.H. acknowledges the generous support provided by the Danish Agency for Science and Technology and Innovation through a Sapere Aude Level 2 grant.; This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Some observations reported here were obtained at the MMT observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This paper uses data taken with the MODS spectrographs built with funding from NSF grant AST-9987045 and the NSF Telescope System Instrumentation Program (TSIP), with additional funds from the Ohio Board of Regents and the Ohio State University Office of Research. NR 160 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2016 VL 821 IS 1 AR 57 DI 10.3847/0004-637X/821/1/57 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI9GB UT WOS:000373809000057 ER PT J AU Fausnaugh, MM Denney, KD Barth, AJ Bentz, MC Bottorff, MC Carini, MT Croxall, KV De Rosa, G Goad, MR Horne, K Joner, MD Kaspi, S Kim, M Klimanov, SA Kochanek, CS Leonard, DC Netzer, H Peterson, BM Schnulle, K Sergeev, SG Vestergaard, M Zheng, WK Zu, Y Anderson, MD Arevalo, P Bazhaw, C Borman, GA Boroson, TA Brandt, WN Breeveld, AA Brewer, BJ Cackett, EM Crenshaw, DM Dalla Bonta, E De Lorenzo-Caceres, A Dietrich, M Edelson, R Efimova, NV Ely, J Evans, PA Filippenko, AV Flatland, K Gehrels, N Geier, S Gelbord, JM Gonzalez, L Gorjian, V Grier, CJ Grupe, D Hall, PB Hicks, S Horenstein, D Hutchison, T Im, M Jensen, JJ Jones, J Kaastra, J Kelly, BC Kennea, JA Kim, SC Korista, KT Kriss, GA Lee, JC Lira, P MacInnis, F Manne-Nicholas, ER Mathur, S McHardy, IM Montouri, C Musso, R Nazarov, SV Norris, RP Nousek, JA Okhmat, DN Pancoast, A Papadakis, I Parks, JR Pei, L Pogge, RW Pott, JU Rafter, SE Rix, HW Saylor, DA Schimoia, JS Siegel, M Spencer, M Starkey, D Sung, HI Teems, KG Treu, T Turner, CS Uttley, P Villforth, C Weiss, Y Woo, JH Yan, H Young, S AF Fausnaugh, M. M. Denney, K. D. Barth, A. J. Bentz, M. C. Bottorff, M. C. Carini, M. T. Croxall, K. V. De Rosa, G. Goad, M. R. Horne, Keith Joner, M. D. Kaspi, S. Kim, M. Klimanov, S. A. Kochanek, C. S. Leonard, D. C. Netzer, H. Peterson, B. M. Schnuelle, K. Sergeev, S. G. Vestergaard, M. Zheng, W. -K. Zu, Y. Anderson, M. D. Arevalo, P. Bazhaw, C. Borman, G. A. Boroson, T. A. Brandt, W. N. Breeveld, A. A. Brewer, B. J. Cackett, E. M. Crenshaw, D. M. Dalla Bonta, E. De Lorenzo-Caceres, A. Dietrich, M. Edelson, R. Efimova, N. V. Ely, J. Evans, P. A. Filippenko, A. V. Flatland, K. Gehrels, N. Geier, S. Gelbord, J. M. Gonzalez, L. Gorjian, V. Grier, C. J. Grupe, D. Hall, P. B. Hicks, S. Horenstein, D. Hutchison, T. Im, M. Jensen, J. J. Jones, J. Kaastra, J. Kelly, B. C. Kennea, J. A. Kim, S. C. Korista, K. T. Kriss, G. A. Lee, J. C. Lira, P. MacInnis, F. Manne-Nicholas, E. R. Mathur, S. McHardy, I. M. Montouri, C. Musso, R. Nazarov, S. V. Norris, R. P. Nousek, J. A. Okhmat, D. N. Pancoast, A. Papadakis, I. Parks, J. R. Pei, L. Pogge, R. W. Pott, J. -U. Rafter, S. E. Rix, H. -W. Saylor, D. A. Schimoia, J. S. Siegel, M. Spencer, M. Starkey, D. Sung, H. -I. Teems, K. G. Treu, T. Turner, C. S. Uttley, P. Villforth, C. Weiss, Y. Woo, J. -H. Yan, H. Young, S. TI SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. III. OPTICAL CONTINUUM EMISSION AND BROADBAND TIME DELAYS IN NGC 5548 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 5548); galaxies: nuclei; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; AGN MONITORING PROJECT; DIGITAL SKY SURVEY; DAMPED RANDOM-WALK; BLACK-HOLE MASSES; COSMIC ORIGINS SPECTROGRAPH; QUASI-STELLAR OBJECTS; DRIVEN DISK WINDS; LINE REGION; X-RAY AB We present ground-based optical photometric monitoring data for NGC 5548, part of an extended multiwavelength reverberation mapping campaign. The light curves have nearly daily cadence from 2014 January to July in nine filters (BVRI and ugriz). Combined with ultraviolet data from the Hubble Space Telescope and Swift, we confirm significant time delays between the continuum bands as a function of wavelength, extending the wavelength coverage from 1158 angstrom to the z band (similar to 9160 angstrom). We find that the lags at wavelengths longer than the V band are equal to or greater than the lags of high-ionization-state emission lines (such as He II lambda 1640 and lambda 4686), suggesting that the continuum-emitting source is of a physical size comparable to the inner broad-line region (BLR). The trend of lag with wavelength is broadly consistent with the prediction for continuum reprocessing by an accretion disk with tau proportional to lambda(4/3). However, the lags also imply a disk radius that is 3 times larger than the prediction from standard thin-disk theory, assuming that the bolometric luminosity is 10% of the Eddington luminosity (L = 0.1L(Edd)). Using optical spectra from the Large Binocular Telescope, we estimate the bias of the interband continuum lags due to BLR emission observed in the filters. We find that the bias for filters with high levels of BLR contamination (similar to 20%) can be important for the shortest continuum lags. and likely has a significant impact on the u and U bands owing to Balmer continuum emission. C1 [Fausnaugh, M. M.; Denney, K. D.; Croxall, K. V.; De Rosa, G.; Kochanek, C. S.; Peterson, B. M.; Zu, Y.; Grier, C. J.; Mathur, S.; Pogge, R. W.; Schimoia, J. S.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. [Denney, K. D.; Croxall, K. V.; De Rosa, G.; Kochanek, C. S.; Peterson, B. M.; Mathur, S.; Pogge, R. W.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA. [Barth, A. J.; Pei, L.] Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA. [Bentz, M. C.; Anderson, M. D.; Bazhaw, C.; Crenshaw, D. M.; Horenstein, D.; Jones, J.; Manne-Nicholas, E. R.; Norris, R. P.; Parks, J. R.; Saylor, D. A.; Teems, K. G.; Turner, C. S.] Georgia State Univ, Dept Phys & Astron, 25 Pk Pl,Suite 605, Atlanta, GA 30303 USA. [Bottorff, M. C.; Hutchison, T.; MacInnis, F.; Musso, R.] Southwestern Univ, Dept Phys FJS 149, Fountainwood Observ, 1011 E Univ Ave, Georgetown, TX 78626 USA. Western Kentucky Univ, Dept Phys & Astron, 1906 Coll Hts Blvd 11077, Bowling Green, KY 42101 USA. [De Rosa, G.; Ely, J.; Kriss, G. A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Goad, M. R.; Evans, P. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Univ St Andrews, SUPA Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Joner, M. D.; Spencer, M.] Brigham Young Univ, Dept Phys & Astron, N283 ESC, Provo, UT 84602 USA. [Kaspi, S.; Netzer, H.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Kaspi, S.; Rafter, S. E.; Weiss, Y.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Kim, M.; Kim, S. C.; Lee, J. C.; Sung, H. -I.] Korea Astron & Space Sci Inst, Seoul, South Korea. [Klimanov, S. A.; Efimova, N. V.] Pulkovo Observ, St Petersburg 196140, Russia. San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Schnuelle, K.; Pott, J. -U.; Rix, H. -W.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Sergeev, S. G.; Borman, G. A.; Nazarov, S. V.; Okhmat, D. N.] Crimean Astrophys Observ, P-O Nauchny, Crimea 298409, Russia. [Vestergaard, M.; Jensen, J. J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. [Vestergaard, M.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [Zheng, W. -K.; Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Zu, Y.] Carnegie Mellon Univ, Dept Phys, 5000 Forbes Ave, Pittsburgh, PA 15213 USA. [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Gran Bretana N 1111, Valparaiso, Chile. [Boroson, T. A.; Kennea, J. A.; Siegel, M.] Las Cumbres Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA. [Brandt, W. N.; Grier, C. J.; Nousek, J. A.] Penn State Univ, Eberly Coll Sci, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Brandt, W. N.; Grier, C. J.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA. [Breeveld, A. A.] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. [Brewer, B. J.] Univ Auckland, Dept Stat, Private Bag 92019, Auckland 1142, New Zealand. [Cackett, E. M.] Wayne State Univ, Dept Phys & Astron, 666 W Hancock St, Detroit, MI 48201 USA. [Dalla Bonta, E.] Univ Padua, Dipartimento Fis & Astron G Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy. [Dalla Bonta, E.] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Dietrich, M.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Dietrich, M.] Worcester State Univ, Dept Earth Environm & Phys, 486 Chandler St, Worcester, MA 01602 USA. [Edelson, R.; Young, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Geier, S.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Geier, S.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Geier, S.] Gran Telescopio Canarias GRANTECAN, E-38205 Tenerife, Spain. [Gelbord, J. M.] Spectral Sci Inc, 4 Fourth Ave, Burlington, MA 01803 USA. [Gelbord, J. M.] Eureka Sci Inc, 2452 Delmer St,Suite 100, Oakland, CA 94602 USA. [Gorjian, V.] CALTECH, Jet Prop Lab, MS 169-327,4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Grupe, D.] Morehead State Univ, Ctr Space Sci, 235 Martindale Dr, Morehead, KY 40351 USA. [Hall, P. B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Im, M.; Woo, J. -H.] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul, South Korea. [Kaastra, J.] SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CC Utrecht, Netherlands. [Kaastra, J.] Univ Utrecht, Dept Phys & Astron, POB 80000, NL-3508 Utrecht, Netherlands. [Kaastra, J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Kelly, B. C.; Treu, T.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Korista, K. T.] Western Michigan Univ, Dept Phys, 1120 Everett Tower, Kalamazoo, MI 49008 USA. [Kriss, G. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Lira, P.] Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile. [McHardy, I. M.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Montouri, C.] Univ Insubria, DiSAT, Via Valleggio 11, I-22100 Como, Italy. [Pancoast, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Papadakis, I.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. [Papadakis, I.] Univ Crete, Inst Theoret & Computat Phys, GR-71003 Iraklion, Greece. [Papadakis, I.] Fdn Res & Technol, IESL, GR-71110 Iraklion, Greece. [Rafter, S. E.] Univ Haifa, Fac Nat Sci, Dept Phys, IL-31905 Haifa, Israel. [Schimoia, J. S.] Univ Fed Rio Grande do Sul, Inst Fis, Campus Vale, Porto Alegre, RS, Brazil. [Treu, T.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Uttley, P.] Univ Amsterdam, Astron Inst Anton Pannekoek, Postbus 94249, NL-1090 GE Amsterdam, Netherlands. [Villforth, C.] Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England. [Yan, H.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. RP Fausnaugh, MM (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. RI Lira, Paulina/G-8536-2016; Papadakis, Iossif/C-3235-2011; OI Zu, Ying/0000-0001-6966-6925; Vestergaard, Marianne/0000-0001-9191-9837; Im, Myungshin/0000-0002-8537-6714; Barth, Aaron/0000-0002-3026-0562 FU National Science Foundation (NSF) [AST-9987045]; NSF [AST-1108693, AST-1008882, AST-1412693, AST-1211916, AST-1302093, AST-0618209, AST-1009756, AST-1009571, AST-1210311, AST-1412315]; Ohio Board of Regents; Ohio State University Office of Research; UK Science and Technology Facilities Council; NASA through Space Telescope Science Institute [GO-13330]; NASA [NAS5-26555, NNX13AC26G, NNX13AC63G, NNX13AE99G, NNH13CH61C]; TABASGO Foundation; Christopher R. Redlich Fund; NSF CAREER grant [AST-1253702]; HHMI; NSERC; Creative Initiative program of the National Research Foundation of Korea (NRFK) - Korean government (MSIP) [2008-0060544]; NWO, the Netherlands Organization for Scientific Research; UC Center for Galaxy Evolution; Fondecyt [1120328]; UCSB Dean's Fellowship; NASA Einstein Fellowship; CNPq, National Council for Scientific and Technological Development (Brazil); Packard Foundation; Danish National Research Foundation; Danish Council for Independent Research [DFF-400200275]; National Research Foundation of Korea (NRF) grant - Korean government [2010-0027910]; Padua University [60A02-5857/13, 60A02-5833/14, 60A02-4434/15, CPDA133894]; STFC grant [ST/M001296/1] FX This paper used data obtained with the MODS spectrographs built with funding from National Science Foundation (NSF) grant AST-9987045 and the NSF Telescope System Instrumentation Program (TSIP), with additional funds from the Ohio Board of Regents and the Ohio State University Office of Research. This paper made use of the mods IDL spectral data reduction pipeline developed in part with funds provided by NSF Grant AST-1108693.; The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council.; Support for HST program number GO-13330 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. M.M.F., G.D.R., B.M.P., C.J.G., and R.W.P. are grateful for the support of the NSF through grant AST-1008882 to The Ohio State University. A.J.B. and L.P. have been supported by NSF grant AST-1412693. A.V.F. and W.-K.Z. are grateful for financial assistance from NSF grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. M.C. Bentz gratefully acknowledges support through NSF CAREER grant AST-1253702 to Georgia State University. M.C. Bottorff acknowledges HHMI for support through an undergraduate science education grant to Southwestern University. K.D.D. is supported by an NSF Fellowship awarded under grant AST-1302093. R.E. gratefully acknowledges support from NASA under awards NNX13AC26G, NNX13AC63G, and NNX13AE99G. J.M.G. gratefully acknowledges support from NASA under award NNH13CH61C. P.B.H. is supported by NSERC. M.I. acknowledges support from the Creative Initiative program, No. 2008-0060544, of the National Research Foundation of Korea (NRFK) funded by the Korean government (MSIP). M.D.J. acknowledges NSF grant AST-0618209 used for obtaining the 0.91 m telescope at WMO. SRON is financially supported by NWO, the Netherlands Organization for Scientific Research. B.C.K. is partially supported by the UC Center for Galaxy Evolution. C.S.K. acknowledges the support of NSF grant AST-1009756. D.C.L. acknowledges support from NSF grants AST-1009571 and AST-1210311, under which part of this research (photometric observations collected at MLO) was carried out. We thank Nhieu Duong, Harish Khandrika, Richard Mellinger, J. Chuck Horst, Steven Armen, and Eddie Garcia for assistance with the MLO observations. P.L. acknowledges support from Fondecyt grant # 1120328. A.P. acknowledges support from an NSF graduate fellowship, a UCSB Dean's Fellowship, and a NASA Einstein Fellowship. J. S.S. acknowledges CNPq, National Council for Scientific and Technological Development (Brazil) for partial support and The Ohio State University for warm hospitality. T.T. has been supported by NSF grant AST-1412315. T.T. and B.C.K. acknowledge support from the Packard Foundation in the form of a Packard Research Fellowship to T.T.; also, T.T. thanks the American Academy in Rome and the Observatory of Monteporzio Catone for kind hospitality. The Dark Cosmology Centre is funded by the Danish National Research Foundation. M.V. gratefully acknowledges support from the Danish Council for Independent Research via grant no. DFF-400200275. J.-H.W. acknowledges support by the National Research Foundation of Korea (NRF) grant funded by the Korean government (No. 2010-0027910). E.D.B. is supported by Padua University through grants 60A02-5857/13, 60A02-5833/14, 60A02-4434/15, and CPDA133894. K.H. acknowledges support from STFC grant ST/M001296/1. S.A.K. thanks Dr. I. A. Rakhimov, the director of Svetloe Observatory, for his support and hospitality. NR 113 TC 16 Z9 16 U1 7 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2016 VL 821 IS 1 AR 56 DI 10.3847/0004-637X/821/1/56 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI9GB UT WOS:000373809000056 ER PT J AU Liu, HB Lai, SP Hasegawa, Y Hirano, N Rao, R Li, IH Fukagawa, M Girart, JM Carrasco-Gonzalez, C Rodriguez, LF AF Liu, Hauyu Baobab Lai, Shih-Ping Hasegawa, Yasuhiro Hirano, Naomi Rao, Ramprasad Li, I-Hsiu Fukagawa, Misato Girart, Josep M. Carrasco-Gonzalez, Carlos Rodriguez, Luis F. TI DETECTION OF LINEARLY POLARIZED 6.9 mm CONTINUUM EMISSION FROM THE CLASS 0 YOUNG STELLAR OBJECT NGC 1333 IRAS4A SO ASTROPHYSICAL JOURNAL LA English DT Article DE evolution; ISM: individual objects (NGC 1333 IRAS4A); stars: formation ID UNDERSTANDING RADIO POLARIMETRY; PROTOSTELLAR DISK FORMATION; MAGNETIC-FIELD STRUCTURE; STAR-FORMING CORES; KEPLERIAN DISK; PROTOPLANETARY DISKS; MOLECULAR OUTFLOW; GRAIN ALIGNMENT; ENVELOPE; 4A AB We report new Karl G. Jansky Very Large Array (JVLA), 0 ''.5 angular resolution observations of linearly polarized continuum emission at 6.9 mm, toward the class 0 young stellar object NGC 1333 IRAS4A. This target source is a collapsing dense molecular core that. was resolved at short wavelengths to have an hourglass shaped B-field configuration. We compare these 6.9 mm observations with previous polarization Submillimeter Array observations at 0.88 mm, which have a comparable angular resolution (similar to 0 ''.7). We find that at the same resolution, the observed polarization position angles at 6.9 mm are slightly deviated from those observed at 0.88 mm. Due to the lower optical depth of the emission at 6.9 mm, and the potential effect of dust grain growth, the new JVLA observations are likely probing B-field alignments in regions interior to those sampled by the previous polarization observations at higher frequencies. Our understanding can be improved with more sensitive observations, and with observations for the more extended spatial scales. C1 [Liu, Hauyu Baobab; Hirano, Naomi; Rao, Ramprasad; Li, I-Hsiu] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. [Liu, Hauyu Baobab] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Lai, Shih-Ping] Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan. [Lai, Shih-Ping] Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan. [Hasegawa, Yasuhiro; Fukagawa, Misato] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Hasegawa, Yasuhiro] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Girart, Josep M.] CSIC IEEC, Inst Ciencies Espai, Campus UAB,Carrer de Can Magrans S-N, E-08193 Cerdanyola Del Valles, Catalonia, Spain. [Girart, Josep M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Carrasco-Gonzalez, Carlos; Rodriguez, Luis F.] UNAM, Inst Radioastron & Astrofis, AP 3-72, Morelia 58089, Michoacan, Mexico. RP Liu, HB (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan.; Liu, HB (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM hyliu@asiaa.sinica.edu.tw OI Li, Jennifer/0000-0002-0311-2812; Girart, Josep Miquel/0000-0002-3829-5591 FU ASIAA; MoST grant [104-2119-M-001-016]; MICINN (Spain) [AYA2014-57369-C3-1-P]; MECD (Spain) [PRX15/00435]; UNAM-DGAPA-PAPIIT [IA101214]; JPL/Caltech FX H.B.L. is grateful for support from ASIAA. We are extremely grateful to our referee Charles Hull,for the very useful comments. H.B.L. thanks Dr. Steve Myers for the information about polarization calibration sources, and thanks Drs. Akimasa Kataoka, Francisca Kemper, Hiroyuki Hirashita, and Michihiro Takami for useful suggestions. N.H. is supported by the MoST grant 104-2119-M-001-016. J.M.G. acknowledges support from the MICINN (Spain) AYA2014-57369-C3-1-P grant and the MECD (Spain) PRX15/00435 travel grant. C.C.-G. acknowledges support by UNAM-DGAPA-PAPIIT, grant number IA101214. Y.H. is currently supported by JPL/Caltech. NR 52 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 APR 10 PY 2016 VL 821 IS 1 AR 41 DI 10.3847/0004-637X/821/1/41 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI9GB UT WOS:000373809000041 ER PT J AU Su, YY Buote, DA Gastaldello, F van Weeren, R AF Su, Yuanyuan Buote, David A. Gastaldello, Fabio van Weeren, Reinout TI CHANDRA OBSERVATION OF ABELL 1142: A COOL-CORE CLUSTER LACKING A CENTRAL BRIGHTEST CLUSTER GALAXY? SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: clusters: individual (Abell 1142); galaxies: clusters: intracluster medium; galaxies: individual (NGC 3492, IC 664); galaxies: ISM ID ACTIVE GALACTIC NUCLEI; X-RAY SPECTROSCOPY; HOT GAS; REDSHIFT SURVEY; XMM-NEWTON; VELOCITY DISPERSIONS; TEMPERATURE RELATION; CENTRAL METALLICITY; DYNAMICAL-FRICTION; SCALING RELATIONS AB Abell 1142 is a low-mass galaxy cluster at low redshift containing two comparable brightest cluster galaxies (BCGs) resembling a scaled-down version of the Coma Cluster. Our Chandra analysis reveals an X-ray emission peak, roughly 100 kpc away from either BCG, which we identify as the cluster center. The emission center manifests itself as a second beta-model surface brightness component distinct from that of the cluster on larger scales. The center is also substantially cooler and more metal-rich than the surrounding intracluster medium (ICM), which makes Abell 1142 appear to be a cool-core cluster. The redshift distribution of its member galaxies indicates that Abell 1142 may contain two subclusters, each of which contain one BCG. The BCGs are merging at a relative velocity of approximate to 1200 km s(-1). This ongoing merger may have shock-heated the ICM from approximate to 2 keV to above 3 keV, which would explain the anomalous L-X-T-X scaling relation for this system. This merger may have displaced the metal-enriched "cool core" of either of the subclusters from the BCG. The southern BCG consists of three individual galaxies residing within a radius of 5 kpc in projection. These galaxies should rapidly sink into the subcluster center due to the dynamical friction of a cuspy cold dark matter halo. C1 [Su, Yuanyuan; van Weeren, Reinout] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Su, Yuanyuan; Buote, David A.] Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA. [Gastaldello, Fabio] INAF IASF Milano, Via E Bassini 15, I-20133 Milan, Italy. RP Su, YY (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Su, YY (reprint author), Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA. EM yuanyuan.su@cfa.harvard.edu OI Gastaldello, Fabio/0000-0002-9112-0184; van Weeren, Reinout/0000-0002-0587-1660 FU National Aeronautics and Space Administration through the Astrophysics Data Analysis Program [NNX13AF14G]; NASA [GO2-13159X, NAS8-03060]; National Aeronautics and Space Administration; National Science Foundation; Alfred P. Sloan Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We are thankful for helpful discussions with William Forman, Manoj Kaplinghat, Tiziana Venturi, and Ralph Kraft. D.A.B. and Y.S. gratefully acknowledge partial support from the National Aeronautics and Space Administration under grant No. NNX13AF14G issued through the Astrophysics Data Analysis Program. Partial support for this work was also provided by NASA through Chandra Award No. GO2-13159X 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. 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. 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. This paper is dedicated to the loving memory of Y. S.'s late grandfather Hua Li. NR 76 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 APR 10 PY 2016 VL 821 IS 1 AR 40 DI 10.3847/0004-637X/821/1/40 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI9GB UT WOS:000373809000040 ER PT J AU Dupree, AK Avrett, EH Kurucz, RL AF Dupree, A. K. Avrett, E. H. Kurucz, R. L. TI CHROMOSPHERIC MODELS AND THE OXYGEN ABUNDANCE IN GIANT STARS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE line: formation; stars: abundances; stars: atmospheres; stars: chromospheres ID METAL-POOR STARS; RICH OPEN CLUSTER; UV LEGACY SURVEY; TURN-OFF STARS; LINE FORMATION; GLOBULAR-CLUSTERS; OMEGA-CENTAURI; CHEMICAL ABUNDANCES; FORMATION SCENARIOS; NEUTRAL OXYGEN AB Realistic stellar atmospheric models of two typical metal-poor giant stars in Omega Centauri, which include a chromosphere (CHR), influence the formation of optical lines of O I: the forbidden lines (lambda 6300, lambda 6363) and the infrared triplet (lambda lambda 7771-7775). One-dimensional semi-empirical non-local thermodynamic equilibrium (LTE) models are constructed based on observed Balmer lines. A full non-LTE formulation is applied for evaluating the line strengths of O I, including photoionization by the Lyman continuum and photoexcitation by Ly alpha and Ly beta. Chromospheric models (CHR) yield forbidden oxygen transitions that are stronger than those in radiative/convective equilibrium (RCE) models. The triplet oxygen lines from high levels also appear stronger than those produced in an RCE model. The inferred oxygen abundance from realistic CHR models for these two stars is decreased by factors of similar to 3 as compared to values derived from RCE models. A lower oxygen abundance suggests that intermediate-mass AGB stars contribute to the observed abundance pattern in globular clusters. A change in the oxygen abundance of metal-poor field giants could affect models of deep mixing episodes on the red giant branch. Changes in the oxygen abundance can impact other abundance determinations that are critical to astrophysics, including chemical tagging techniques and galactic chemical evolution. C1 [Dupree, A. K.; Avrett, E. H.; Kurucz, R. L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Dupree, AK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dupree@cfa.harvard.edu OI Dupree, Andrea/0000-0002-8985-8489 NR 51 TC 3 Z9 3 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 APR 10 PY 2016 VL 821 IS 1 AR L7 DI 10.3847/2041-8205/821/1/L7 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI9HA UT WOS:000373812000007 ER PT J AU Miller, JM Raymond, J Fabian, AC Gallo, E Kaastra, J Kallman, T King, AL Proga, D Reynolds, CS Zoghbi, A AF Miller, J. M. Raymond, J. Fabian, A. C. Gallo, E. Kaastra, J. Kallman, T. King, A. L. Proga, D. Reynolds, C. S. Zoghbi, A. TI THE ACCRETION DISK WIND IN THE BLACK HOLE GRS 1915+105 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; X-rays: binaries ID X-RAY BINARIES; INNER DISK; MASS; SPIN; OUTFLOWS; CORONAE; JETS; GAS; SPECTROSCOPY; SIMULATIONS AB We report on a 120 ks Chandra/HETG spectrum of the black hole GRS 1915+105. The observation was made during an extended and bright soft state in 2015 June. An extremely rich disk wind absorption spectrum is detected, similar to that observed at lower sensitivity in 2007. The very high resolution of the third-order spectrum reveals four components to the disk wind in the Fe K band alone; the fastest has a blueshift of v = 0.03c. Broadened re-emission from the wind is also detected in the first-order spectrum, giving rise to clear accretion disk P Cygni profiles. Dynamical modeling of the re-emission spectrum gives wind launching radii of r similar or equal to 10(2-4) GM/c(2). Wind density values of n similar or equal to 10(13-16) cm(-3) are then required by the ionization parameter formalism. The small launching radii, high density values, and inferred high mass outflow rates signal a role for magnetic driving. With simple, reasonable assumptions, the wind properties constrain the magnitude of the emergent magnetic field to be B similar or equal to 10(3-4) G if the wind is driven via magnetohydrodynamic (MHD) pressure from within the disk. and B similar or equal to 10(4-5) G if the wind is driven by magnetocentrifugal acceleration. The MHD estimates are below upper limits predicted by the canonical alpha-disk model. We discuss these results in terms of fundamental disk physics and black hole accretion modes. C1 [Miller, J. M.; Gallo, E.; Zoghbi, A.] Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48109 USA. [Raymond, J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 OHA, England. [Kaastra, J.] SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. [Kaastra, J.] Univ Utrecht, Dept Phys & Astron, POB 80000, NL-3508 TA Utrecht, Netherlands. [Kallman, T.] NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. [King, A. L.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Proga, D.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48109 USA. EM jonmm@umich.edu RI Zoghbi, Abderahmen/A-8445-2017 OI Zoghbi, Abderahmen/0000-0002-0572-9613 NR 41 TC 4 Z9 4 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 10 PY 2016 VL 821 IS 1 AR L9 DI 10.3847/2041-8205/821/1/L9 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI9HA UT WOS:000373812000009 ER PT J AU Newton, ER Irwin, J Charbonneau, D Berta-Thompson, ZK Dittmann, JA AF Newton, Elisabeth R. Irwin, Jonathan Charbonneau, David Berta-Thompson, Zachory K. Dittmann, Jason A. TI THE IMPACT OF STELLAR ROTATION ON THE DETECTABILITY OF HABITABLE PLANETS AROUND M DWARFS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: low-mass; stars: rotation ID MAIN-SEQUENCE STARS; EXTRA-SOLAR PLANETS; NEARBY M DWARFS; LOW-MASS STARS; M-CIRCLE-PLUS; HARPS SEARCH; SUPER-EARTHS; GLIESE 581; TRIGONOMETRIC PARALLAXES; RADIAL-VELOCITIES AB Stellar activity and rotation frustrate the detection of exoplanets through the radial velocity technique. This effect is particularly of concern for M dwarfs, which can remain magnetically active for billions of years. We compile rotation periods for late-type stars and for the M dwarf planet-host sample in order to investigate the rotation periods of older field stars across the main sequence. We show that for stars with masses between 0.25 and 0.5 M-circle dot (M4V-M1V), the stellar rotation period typical of field stars coincides with the orbital periods of planets in the habitable zone. This will pose a fundamental challenge to the discovery and characterization of potentially habitable planets around early M dwarfs. Due to the longer rotation periods reached by mid. M dwarfs and the shorter orbital period at which the planetary habitable zone is found, stars with masses between 0.1 and 0.25 M-circle dot (M6V-M4V) offer better opportunities for the detection of habitable planets via radial velocities. C1 [Newton, Elisabeth R.; Irwin, Jonathan; Charbonneau, David; Dittmann, Jason A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Berta-Thompson, Zachory K.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Berta-Thompson, Zachory K.] MIT, Dept Phys, Cambridge, MA 02139 USA. RP Newton, ER (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Dittmann, Jason/0000-0001-7730-2240; Newton, Elisabeth/0000-0003-4150-841X FU National Science Foundation [AST-0807690, AST-1109468, AST-1004488]; David and Lucile Packard Foundation Fellowship for Science and Engineering; John Templeton Foundation; NSF Graduate Research Fellowship; MIT Torres Fellowship for Exoplanet Research; NASA; NSF; NASA Astrophysics Data System (ADS) FX The MEarth project acknowledges funding from the National Science Foundation under grants AST-0807690, AST-1109468, and AST-1004488 (Alan T. Waterman Award) and the David and Lucile Packard Foundation Fellowship for Science and Engineering. This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed here are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. E.R.N. was supported by the NSF Graduate Research Fellowship, and Z.K.B.-T. by the MIT Torres Fellowship for Exoplanet Research. This research has made use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF; NASA Astrophysics Data System (ADS); and the SIMBAD database and VizieR catalog access tool, at CDS, Strasbourg, France. NR 79 TC 5 Z9 5 U1 3 U2 18 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 2016 VL 821 IS 1 AR L19 DI 10.3847/2041-8205/821/1/L19 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI9HA UT WOS:000373812000019 ER PT J AU Ortiz, OO Baldini, RM Berguido, G Croat, TB AF Ortiz, Orlando O. Baldini, Riccardo M. Berguido, Guido Croat, Thomas B. TI New species of Anthurium (Araceae) from Chucanti Nature Reserve, eastern Panama SO PHYTOTAXA LA English DT Article DE Taxonomy; Flora of Panama; Daricn; Xialophyllium; Polyneurium ID CENTRAL-AMERICA AB In the present paper we describe two new endemic species of Anthurium, discovered during field trips to study the Araceae flora of the Chucanti Nature Reserve (Reserva Natural Chucanti) located in the province of Darien, Panama. Anthurium annularum sp. nov., a member of section Xialophyllium, is principally characterized by its hemiepiphytic climbing habit, stems with ring-shaped nodes with short internodes alternating with much longer internodes, a yellow-green spadix and pale green globose berries which are nearly translucent toward the base. A. chucantiense sp. nov., a member of section Polyneurium, is characterized by its epiphytic habit, short internodes at stem apex, terete petioles, blades with obscure primary lateral veins, greenish to pale orange spadix and narrowly ovoid, and bluntly pointed red-orange berries. C1 [Ortiz, Orlando O.] Univ Panama, Herbario PMA, Estafeta Univ, Panama City, Panama. [Ortiz, Orlando O.] Univ Panama, Programa Maestria Ciencias Biol, Estafeta Univ, Panama City, Panama. [Baldini, Riccardo M.] Univ Florence, Dept Biol, I-50121 Florence, Italy. [Baldini, Riccardo M.] Univ Florence, Trop Herbarium FT, I-50121 Florence, Italy. [Baldini, Riccardo M.] Smithsonian Trop Res Insitute, Panama City, Panama. [Berguido, Guido] Adopt Panama Rainforest Assoc ADOPTA, POB 0801-00051, Panama City, Panama. [Croat, Thomas B.] Missouri Bot Garden, POB 299, St Louis, MO 63166 USA. RP Ortiz, OO (reprint author), Univ Panama, Herbario PMA, Estafeta Univ, Panama City, Panama.; Ortiz, OO (reprint author), Univ Panama, Programa Maestria Ciencias Biol, Estafeta Univ, Panama City, Panama. EM ortizopma@gmail.com OI Ortiz, Orlando Oriel/0000-0002-7805-0046 FU Missouri Botanical Garden FX We offer our gratitude to the Missouri Botanical Garden for funding the Herbarium work through the Alwyn Gentry Fellowship (O.O.O.). We are also very grateful to the curators of the following herbaria: PMA, MO and SCZ for allowing us to access to their collections. We would like to thank Alicia Ibanez and Rodolfo Flores for providing information about flora and vegetation of Chucanti; Professor Mireya Correa, Director of PMA, botanists and herbarium workers Lucila Guillen and Vielka Murillo (PMA) for providing excellent images of the holotypes and Dr. Carlos Ramos, Dean of the Faculty of Natural Sciences and Technology, for providing facilities and other support. Special thanks go to Dr. Peter C. Boyce and Dr. Alberto Sidney Taylor Blake for their revisions and suggestions. NR 36 TC 1 Z9 1 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1179-3155 EI 1179-3163 J9 PHYTOTAXA JI Phytotaxa PD APR 5 PY 2016 VL 255 IS 1 BP 47 EP 56 DI 10.11646/phytotaxa.255.1.4 PG 10 WC Plant Sciences SC Plant Sciences GA DT9GL UT WOS:000381804700004 ER PT J AU Thompson, RC Wann, L Narula, N Narula, J Sutherland, ML Sutherland, J Allam, A France, C Frohlich, B AF Thompson, Randall C. Wann, L. Narula, Navneet Narula, Jagat Sutherland, M. Linda Sutherland, James Allam, Adel France, Christine Frohlich, Bruno CA Study Grp Horus TI ASSESSMENT OF MISSING LINKS IN ATHEROGENESIS: PILOT STUDY OF GREAT APES AND HUMANS SO JOURNAL OF THE AMERICAN COLLEGE OF CARDIOLOGY LA English DT Meeting Abstract CT 65th Annual Scientific Session and Expo of the American-College-of-Cardiology (ACC) CY APR 02-04, 2016 CL Chicago, IL SP Amer Coll Cardiol C1 St Lukes Mid Amer Heart Inst, Kansas City, MO USA. Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0735-1097 EI 1558-3597 J9 J AM COLL CARDIOL JI J. Am. Coll. Cardiol. PD APR 5 PY 2016 VL 67 IS 13 SU S MA 1230-263 BP 1766 EP 1766 PG 1 WC Cardiac & Cardiovascular Systems SC Cardiovascular System & Cardiology GA DK8PH UT WOS:000375188702612 ER PT J AU van Donkelaar, A Martin, RV Brauer, M Hsu, NC Kahn, RA Levy, RC Lyapustin, A Sayer, AM Winker, DM AF van Donkelaar, Aaron Martin, Randall V. Brauer, Michael Hsu, N. Christina Kahn, Ralph A. Levy, Robert C. Lyapustin, Alexei Sayer, Andrew M. Winker, David M. TI Global Estimates of Fine Particulate Matter using a Combined Geophysical-Statistical Method with Information from Satellites, Models, and Monitors SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID AEROSOL OPTICAL DEPTH; GEOGRAPHICALLY WEIGHTED REGRESSION; UNITED-STATES; CARBONACEOUS AEROSOLS; EXPOSURE ASSESSMENT; NORTH-AMERICA; MODIS; PRODUCTS; PM2.5; LAND AB We estimated global fine particulate matter (PM2.5) concentrations using information from satellite-, simulation- and monitor-based sources by applying a Geographically Weighted Regression (GWR) to global geophysically based satellite-derived PM2.5 estimates. Aerosol optical depth from multiple satellite products (MISR, MODIS Dark Target, MODIS and SeaWiFS Deep Blue, and MODIS MAIAC) was combined with simulation (GEOS-Chem) based upon their relative uncertainties as determined using ground-based sun photometer (AERONET) observations for 1998-2014. The GWR predictors included simulated aerosol composition and land use information. The resultant PM2.5 estimates were highly consistent (R-2 = 0.81) with out-of-sample cross-validated PM2.5 concentrations from monitors. The global population-weighted annual average PM2.5 concentrations were 3-fold higher than the 10 mu g/m(3) WHO guideline, driven by exposures in Asian and African regions. Estimates in regions with high contributions from mineral dust were associated with higher uncertainty, resulting from both sparse ground-based monitoring, and challenging conditions for retrieval and simulation. This approach demonstrates that the addition of even sparse ground-based measurements to more globally continuous PM2.5 data sources can yield valuable improvements to PM2.5 characterization on a global scale. C1 [van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Brauer, Michael] Univ British Columbia, Sch Populat & Publ Hlth, 2206 East Mall, Vancouver, BC V6T 1Z3, Canada. [Hsu, N. Christina; Kahn, Ralph A.; Levy, Robert C.; Lyapustin, Alexei; Sayer, Andrew M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lyapustin, Alexei; Sayer, Andrew M.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Greenbelt, MD 20771 USA. [Winker, David M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP van Donkelaar, A (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. EM Aaron.van.Donkelaar@dal.ca RI Sayer, Andrew/H-2314-2012; Levy, Robert/M-7764-2013; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI Sayer, Andrew/0000-0001-9149-1789; Levy, Robert/0000-0002-8933-5303; Martin, Randall/0000-0003-2632-8402; FU Natural Science and Engineering Research Council of Canada; NASA MEaSUREs program; NASA EOS program FX We are grateful to the MODIS, MISR, SeaWiFS, CALIOP, and AERONET teams that have made this work possible through the creation, validation, and public release of their data products, as well as Compute Canada for computing resources. This work was supported by the Natural Science and Engineering Research Council of Canada. SeaWiFS and MODIS Deep Blue data set development was supported by the NASA MEaSUREs and EOS programs, respectively. NR 52 TC 14 Z9 14 U1 30 U2 51 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD APR 5 PY 2016 VL 50 IS 7 BP 3762 EP 3772 DI 10.1021/acs.est.5b05833 PG 11 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA DI7CD UT WOS:000373655800055 PM 26953851 ER PT J AU El Gamal, A Agarwal, V Diethelm, S Rahman, I Schorn, MA Sneed, JM Louie, GV Whalen, KE Mincer, TJ Noel, JP Paul, VJ Moore, BS AF El Gamal, Abrahim Agarwal, Vinayak Diethelm, Stefan Rahman, Imran Schorn, Michelle A. Sneed, Jennifer M. Louie, Gordon V. Whalen, Kristen E. Mincer, Tracy J. Noel, Joseph P. Paul, Valerie J. Moore, Bradley S. TI Biosynthesis of coral settlement cue tetrabromopyrrole in marine bacteria by a uniquely adapted brominase-thioesterase enzyme pair SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE natural products; biosynthesis; halogenation; enzymology ID TRYPTOPHAN 7-HALOGENASE PRNA; CARRIER PROTEIN; HALOGENASE PLTA; CHLORINATION; STREPTOMYCES; ORGANISMS; MECHANISM AB Halogenated pyrroles (halopyrroles) are common chemical moieties found in bioactive bacterial natural products. The halopyrrole moieties of mono-and dihalopyrrole-containing compounds arise from a conserved mechanism in which a proline-derived pyrrolyl group bound to a carrier protein is first halogenated and then elaborated by peptidic or polyketide extensions. This paradigm is broken during the marine pseudoalteromonad bacterial biosynthesis of the coral larval settlement cue tetrabromopyrrole (1), which arises from the substitution of the proline-derived carboxylate by a bromine atom. To understand the molecular basis for decarboxylative bromination in the biosynthesis of 1, we sequenced two Pseudoalteromonas genomes and identified a conserved four-gene locus encoding the enzymes involved in its complete biosynthesis. Through total in vitro reconstitution of the biosynthesis of 1 using purified enzymes and biochemical interrogation of individual biochemical steps, we show that all four bromine atoms in 1 are installed by the action of a single flavin-dependent halogenase: Bmp2. Tetrabromination of the pyrrole induces a thioesterase-mediated offloading reaction from the carrier protein and activates the biosynthetic intermediate for decarboxylation. Insights into the tetrabrominating activity of Bmp2 were obtained from the high-resolution crystal structure of the halogenase contrasted against structurally homologous halogenase Mpy16 that forms only a dihalogenated pyrrole in marinopyrrole biosynthesis. Structure-guided mutagenesis of the proposed substrate- binding pocket of Bmp2 led to a reduction in the degree of halogenation catalyzed. Our study provides a biogenetic basis for the biosynthesis of 1 and sets a firm foundation for querying the biosynthetic potential for the production of 1 in marine (meta) genomes. C1 [El Gamal, Abrahim; Agarwal, Vinayak; Diethelm, Stefan; Rahman, Imran; Schorn, Michelle A.; Moore, Bradley S.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Oceans & Human Hlth, La Jolla, CA 92093 USA. [Sneed, Jennifer M.; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Louie, Gordon V.; Noel, Joseph P.] Salk Inst Biol Studies, Howard Hughes Med Inst, La Jolla, CA 92037 USA. [Louie, Gordon V.; Noel, Joseph P.] Salk Inst Biol Studies, Jack H Skirball Ctr Chem Biol & Prote, 10010 N Torrey Pines Rd, La Jolla, CA 92037 USA. [Whalen, Kristen E.; Mincer, Tracy J.] Woods Hole Oceanog Inst, Marine Chem & Geochem, Woods Hole, MA 02543 USA. [Moore, Bradley S.] Univ Calif San Diego, Skaggs Sch Pharm & Pharmaceut Sci, La Jolla, CA 92093 USA. RP Moore, BS (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Ctr Oceans & Human Hlth, La Jolla, CA 92093 USA.; Moore, BS (reprint author), Univ Calif San Diego, Skaggs Sch Pharm & Pharmaceut Sci, La Jolla, CA 92093 USA. EM bsmoore@ucsd.edu FU US National Science Foundation [OCE-1313747]; US National Institutes of Health (NIH) [P01-ES021921, R01-AI47818, R21-AI119311]; Mote Protect Our Reef Grant Program [POR-2012-3]; Dart Foundation; Smithsonian Competitive Grants Program for Science; Howard Hughes Medical Institute; NIH Marine Biotechnology Training Grant Predoctoral Fellowship [T32-GM067550]; Helen Hay Whitney Foundation Postdoctoral Fellowship; Swiss National Science Foundation Postdoctoral Fellowship FX We thank our colleague B. M. Duggan at University of California, San Diego for assistance in acquiring NMR data. This work was jointly supported by US National Science Foundation Grant OCE-1313747 (to B.S.M.) and US National Institutes of Health (NIH) Grants P01-ES021921 and R01-AI47818 (to B.S.M.) and R21-AI119311 (to K.E.W. and T.J.M.), the Mote Protect Our Reef Grant Program (POR-2012-3), the Dart Foundation, the Smithsonian Competitive Grants Program for Science (V.J.P.), the Howard Hughes Medical Institute (J.P.N.), NIH Marine Biotechnology Training Grant Predoctoral Fellowship T32-GM067550 (to A.E.), a Helen Hay Whitney Foundation Postdoctoral Fellowship (to V.A.), and a Swiss National Science Foundation Postdoctoral Fellowship (to S.D.). NR 31 TC 2 Z9 2 U1 10 U2 29 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD APR 5 PY 2016 VL 113 IS 14 BP 3797 EP 3802 DI 10.1073/pnas.1519695113 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DI2UI UT WOS:000373354000043 PM 27001835 ER PT J AU Boyce, CK DiMichele, WA AF Boyce, C. Kevin DiMichele, William A. TI Arborescent lycopsid productivity and lifespan: Constraining the possibilities SO REVIEW OF PALAEOBOTANY AND PALYNOLOGY LA English DT Article DE Carboniferous; Lepidodendron; Lepidophloios; Oldest palm; Sigillaria; Stigmaria ID LAND PLANT EVOLUTION; ATMOSPHERIC CARBON-DIOXIDE; FOSSIL RECORD; CARBONIFEROUS PLANTS; SWAMP-FOREST; PHOTOSYNTHETIC CAPACITY; RHIZOMORPHIC LYCOPSIDS; GROWTH ARCHITECTURE; PHANEROZOIC TIME; FLOOD TOLERANCE AB One of the most enigmatic components of early terrestrial vegetation was the arborescent lycopsids. Because of the sheer abundance of their biomass in many wetland environments of the Late Paleozoic, they may have been an important variable in the global carbon cycle and climate. However, their unusual structure has invited extraordinary interpretations regarding their biology. One idea that has persisted in the literature for over forty years is that these trees had extremely short lifespans, on the order of ten years. Such an accelerated lifecycle would require growth rates twenty times higher than modern angiosperm trees (and at least 60 times higher than modem lycopsids). Here, we evaluate the morphology and anatomy of lycopsid trees-including aerenchyma, phloem, leaf base distributions, leaf structure, rootlet anatomy, and the demography of the preserved fossils with comparison to modern plants with some similarity of overall form, most notably the palms. The environmental context of lycopsid trees also is considered in the light of the vegetation of modem water-saturated substrates. It is concluded that such rapid growth would violate all known physiological mechanisms. One hypothetical mechanism that had been proposed to provide for increased carbon fixation, a unique photosynthetic pathway, could not have been viable in these plants and there is no accounting for the increases in nitrogen and phosphorous uptake that would be necessary to sustain enormous rates of carbon fixation. Of the various aspects of lycopsid anatomy and ecology that might militate against this conclusion that productivity was not high, no line of evidence requires a uniquely rapid growth rate for the arborescent lycopsids and several lines of evidence seem to prohibit it. Thus, we conclude that the lifespans of arborescent lycopsids most likely were measured in centuries rather than years. These trees should not be expected to have been unique outliers with physiological function completely distinct from all other tracheophytes. Furthermore, they require no special consideration in the evaluation of Paleozoic biogeochemical cycling. Finally, the conclusion that lycopsid lifespans were an order of magnitude longer than previous expectations invites reconsideration of many other aspects of their ontogeny, physiology, and structure. (C) 2015 Elsevier B.V. All rights reserved. C1 [Boyce, C. Kevin] Stanford Univ, Dept Geol Sci, Stanford, CA 94305 USA. [DiMichele, William A.] NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC USA. RP Boyce, CK (reprint author), Stanford Univ, Dept Geol Sci, Stanford, CA 94305 USA. EM ckboyce@stanford.edu FU National Science Foundation [EAR1024041] FX The authors thank T.L. Phillips, H.W. Pfefferkorn, R.M. Bateman, H. Kerp, and T.L. Rintoul for helpful discussions on many of the matters covered in this paper, as well as three anonymous reviewers; however, the authors bear sole responsibility for the ideas expressed here. This research was supported by National Science Foundation Grant #EAR1024041 (C.K.B). NR 163 TC 2 Z9 2 U1 4 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0034-6667 EI 1879-0615 J9 REV PALAEOBOT PALYNO JI Rev. Palaeobot. Palynology PD APR PY 2016 VL 227 BP 97 EP 110 DI 10.1016/j.revpalbo.2015.10.007 PG 14 WC Plant Sciences; Paleontology SC Plant Sciences; Paleontology GA EH6QH UT WOS:000391898500009 ER PT J AU DeRoo, CT McEntaffer, RL Miles, DM Peterson, TJ Marlowe, H Tutt, JH Donovan, BD Menz, B Burwitz, V Hartner, G Allured, R Smith, RK Gunther, R Yanson, A Vacanti, G Ackermann, M AF DeRoo, Casey T. McEntaffer, Randall L. Miles, Drew M. Peterson, Thomas J. Marlowe, Hannah Tutt, James H. Donovan, Benjamin D. Menz, Benedikt Burwitz, Vadim Hartner, Gisela Allured, Ryan Smith, Randall K. Guenther, Ramses Yanson, Alex Vacanti, Giuseppe Ackermann, Marcelo TI Line spread functions of blazed off-plane gratings operated in the Littrow mounting SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS LA English DT Article DE x-ray spectroscopy; off-plane gratings; x-ray diffraction; grating fabrication ID X-RAY OPTICS; NANOIMPRINT LITHOGRAPHY; FABRICATION AB Future soft x-ray (10 to 50 angstrom) spectroscopy missions require higher effective areas and resolutions to perform critical science that cannot be done by instruments on current missions. An x-ray grating spectrometer employing off-plane reflection gratings would be capable of meeting these performance criteria. Off-plane gratings with blazed groove facets operating in the Littrow mounting can be used to achieve excellent throughput into orders achieving high resolutions. We have fabricated two off-plane gratings with blazed groove profiles via a technique that uses commonly available microfabrication processes, is easily scaled for mass production, and yields gratings customized for a given mission architecture. Both fabricated gratings were tested in the Littrow mounting at the Max Planck Institute for Extraterrestrial Physics (MPE) PANTER x-ray test facility to assess their performance. The line spread functions of diffracted orders were measured, and a maximum resolution of 800 +/- 20 is reported. In addition, we also observe evidence of a blaze effect from measurements of relative efficiencies of the diffracted orders. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI. C1 [DeRoo, Casey T.; McEntaffer, Randall L.; Miles, Drew M.; Peterson, Thomas J.; Marlowe, Hannah; Tutt, James H.; Donovan, Benjamin D.] Univ Iowa, Dept Phys & Astron, 210 Van Allen Hall, Iowa City, IA 52242 USA. [Menz, Benedikt; Burwitz, Vadim; Hartner, Gisela] MPI Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Allured, Ryan; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Guenther, Ramses; Yanson, Alex; Vacanti, Giuseppe] Cosine Sci & Comp BV, JH Oortweg 19, NL-2333 CH Leiden, Netherlands. [Ackermann, Marcelo] Cosine Res BV, JH Oortweg 19, NL-2333 CH Leiden, Netherlands. RP DeRoo, CT (reprint author), Univ Iowa, Dept Phys & Astron, 210 Van Allen Hall, Iowa City, IA 52242 USA. EM casey-deroo@uiowa.edu NR 20 TC 1 Z9 1 U1 0 U2 0 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 2329-4124 EI 2329-4221 J9 J ASTRON TELESC INST JI J. Astron. Telesc. Instrum. Syst. PD APR PY 2016 VL 2 IS 2 AR 025001 DI 10.1117/1.JATIS.2.2.025001 PG 15 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA DV7OV UT WOS:000383126900002 ER PT J AU Erskine, DJ Edelstein, J Wishnow, EH Sirk, M Muirhead, PS Muterspaugh, MW Lloyd, JP Ishikawa, Y McDonald, EA Shourt, WV Vanderburg, AM AF Erskine, David J. Edelstein, Jerry Wishnow, Edward H. Sirk, Martin Muirhead, Philip S. Muterspaugh, Matthew W. Lloyd, James P. Ishikawa, Yuzo McDonald, Eliza A. Shourt, William V. Vanderburg, Andrew M. TI High-resolution broadband spectroscopy using externally dispersed interferometry at the Hale telescope: Part 1, data analysis and results SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS LA English DT Article DE dispersed interferometry; Doppler radial velocimetry; high-resolution spectroscopy ID MICHELSON INTERFEROMETER; RADIAL VELOCIMETRY; SPECTROGRAPHS; EFFICIENT; SPECTRUM AB High-resolution broadband spectroscopy at near-infrared wavelengths (950 to 2450 nm) has been performed using externally dispersed interferometry (EDI) at the Hale telescope at Mt. Palomar. Observations of stars were performed with the "TEDI" interferometer mounted within the central hole of the 200-in. primary mirror in series with the comounted TripleSpec near-infrared echelle spectrograph. These are the first multidelay EDI demonstrations on starlight, as earlier measurements used a single delay or laboratory sources. We demonstrate very high (10x) resolution boost, from original 2700 to 27,000 with current set of delays (up to 3 cm), well beyond the classical limits enforced by the slit width and detector pixel Nyquist limit. Significantly, the EDI used with multiple delays rather than a single delay as used previously yields an order of magnitude or more improvement in the stability against native spectrograph point spread function (PSF) drifts along the dispersion direction. We observe a dramatic (20x) reduction in sensitivity to PSF shift using our standard processing. A recently realized method of further reducing the PSF shift sensitivity to zero is described theoretically and demonstrated in a simple simulation which produces a 350x times reduction. We demonstrate superb rejection of fixed pattern noise due to bad detector pixels-EDI only responds to changes in pixel intensity synchronous to applied dithering. This part 1 describes data analysis, results, and instrument noise. A section on theoretical photon limited sensitivity is in a companion paper, part 2. (C) 2016 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Erskine, David J.] Lawrence Livermore Natl Lab, Mailstop L-487,7000 East Ave, Livermore, CA 94550 USA. [Edelstein, Jerry; Wishnow, Edward H.; Sirk, Martin; Ishikawa, Yuzo; McDonald, Eliza A.; Shourt, William V.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. [Muirhead, Philip S.] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. [Muterspaugh, Matthew W.] Tennessee State Univ, Boswell Sci Hall, Nashville, TN 37209 USA. [Lloyd, James P.] Cornell Univ, Carl Sagan Inst, Dept Astron, Space Sci 230, Ithaca, NY 14853 USA. [Vanderburg, Andrew M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-10, Cambridge, MA 02138 USA. RP Erskine, DJ (reprint author), Lawrence Livermore Natl Lab, Mailstop L-487,7000 East Ave, Livermore, CA 94550 USA. EM erskine1@llnl.gov RI Muirhead, Philip/H-2273-2014 OI Muirhead, Philip/0000-0002-0638-8822 NR 24 TC 1 Z9 1 U1 4 U2 4 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 2329-4124 EI 2329-4221 J9 J ASTRON TELESC INST JI J. Astron. Telesc. Instrum. Syst. PD APR PY 2016 VL 2 IS 2 AR 025004 DI 10.1117/1.JATIS.2.2.025004 PG 36 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA DV7OV UT WOS:000383126900005 ER PT J AU Culley, TM Huebner, CD Novy, A AF Culley, Theresa M. Huebner, Cynthia D. Novy, Ari TI Regional and Local Genetic Variation in Japanese Stiltgrass (Microstegium vimineum) SO INVASIVE PLANT SCIENCE AND MANAGEMENT LA English DT Article DE Genetic structure; invasive; local dispersal; microsatellites ID CANOPY DECIDUOUS FORESTS; MULTILOCUS GENOTYPE DATA; CENTRAL HARDWOOD FOREST; INVASIVE GRASS; C-4 GRASS; ENVIRONMENTAL GRADIENTS; POPULATION-STRUCTURE; PLANT-COMMUNITIES; SHADE-TOLERANT; VARIABLE LIGHT AB Nonnative M. vimineum has been expanding rapidly in the eastern United States, where it can negatively affect plant communities. Locally, the species is assumed to spread from roadsides into nearby forests, where it can form dense populations after disturbances, especially in light gaps. Using microsatellite markers, we quantified patterns of genetic variation and structure among populations at nine sites in West Virginia. We then examined patterns of local dispersal within each population, focusing on subpopulations along the roadside, those coalescing nearby along the forest edge, and subpopulations in the interior forest. We found that levels of genetic variation of M. vimineum were relatively low overall across populations but with genetic structure present among populations (F-st = 0.60). Within populations, subpopulations along the roadside were genetically variable, containing 4 to 22 unique, multilocus genotypes. Many of these genotypes were also identified in the adjacent forest, consistent with local, diffusive spread from the roadway. However, several genotypes in the interior forest were unique to the population, indicating that dispersal from other sites may also occur. Overall, it appears that genetic diversity and structure in M. vimineum reflects a variety of processes, including localized dispersal and long-distance migration. Nomenclature: Japanese stiltgrass, Microstegium vimineum (Trin.) A. Camus. C1 [Culley, Theresa M.] Univ Cincinnati, Dept Biol Sci, 614 Rieveschl Hall, Cincinnati, OH 45221 USA. US Forest Serv, USDA, Northern Res Stn, 180 Canfield St, Morgantown, WV 26505 USA. US Bot Garden, 245 First St SW, Washington, DC 20024 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Culley, TM (reprint author), Univ Cincinnati, Dept Biol Sci, 614 Rieveschl Hall, Cincinnati, OH 45221 USA. EM theresa.culley@uc.edu FU Northern Research Station, U.S. Department of Agriculture, Forest Service, Morgantown, WV [10-JV11242303-047] FX The authors thank L. Chaney for field collection of samples, as well as S. Stancheva, S. Yadav, and S. Albers for assistance with the genetic analysis of the PRD and WVU populations. We thank several anonymous reviewers for their valuable comments. This research was funded by the Northern Research Station, U.S. Department of Agriculture, Forest Service, Morgantown, WV, with Joint Venture Agreement 10-JV11242303-047. NR 64 TC 0 Z9 0 U1 7 U2 7 PU WEED SCI SOC AMER PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 1939-7291 EI 1939-747X J9 INVAS PLANT SCI MANA JI Invasive Plant Sci. Manag. PD APR-JUN PY 2016 VL 9 IS 2 BP 96 EP 111 DI 10.1614/IPSM-D-15-00055.1 PG 16 WC Plant Sciences SC Plant Sciences GA DS2EM UT WOS:000380561300002 ER PT J AU Hong, T AF Hong, Terry TI A Greater Music SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20024 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20024 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR PY 2016 VL 141 IS 13 BP 77 EP 77 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA DT0ME UT WOS:000381176900075 ER PT J AU Hong, T AF Hong, Terry TI The Boat Rocker SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR PY 2016 VL 141 IS 13 BP 81 EP 81 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA DT0ME UT WOS:000381176900092 ER PT J AU Joshi, AR Dinerstein, E Wikramanayake, E Anderson, ML Olson, D Jones, BS Seidensticker, J Lumpkin, S Hansen, MC Sizer, NC Davis, CL Palminteri, S Hahn, NR AF Joshi, Anup R. Dinerstein, Eric Wikramanayake, Eric Anderson, Michael L. Olson, David Jones, Benjamin S. Seidensticker, John Lumpkin, Susan Hansen, Matthew C. Sizer, Nigel C. Davis, Crystal L. Palminteri, Suzanne Hahn, Nathan R. TI Tracking changes and preventing loss in critical tiger habitat SO SCIENCE ADVANCES LA English DT Article ID ROADS AB The global population of wild tigers remains dangerously low at fewer than 3500 individuals. Habitat loss, along with poaching, can undermine the international target recovery of doubling the number of wild tigers by 2022. Using a new satellite-based monitoring system, we analyzed 14 years of forest loss data within the 76 landscapes (ranging from 278 to 269,983 km(2)) that have been prioritized for conservation of wild tigers. Our analysis provides an update of the status of tiger habitat and describes new applications of technology to detect precisely where forest loss is occurring in order to curb future habitat loss. Across the 76 landscapes, forest loss was far less than anticipated (79,597 +/- 22,629 km(2), 7.7% of remaining habitat) over the 14-year study period (2001-2014). Habitat loss was unevenly distributed within a subset of 29 landscapes deemed most critical for doubling wild tiger populations: 19 showed little change (1.5%), whereas 10 accounted for more than 98% (57,392 +/- 16,316 km(2)) of habitat loss. Habitat loss in source population sites within 76 landscapes ranged from no loss to 435 +/- 124 km(2) ((x) over bar = 24 km(2), SD = 89, total = 1676 +/- 476 km(2)). Doubling the tiger population by 2022 requires moving beyond tracking annual changes in habitat. We highlight near-real-time forest monitoring technologies that provide alerts of forest loss at relevant spatial and temporal scales to prevent further erosion. C1 [Joshi, Anup R.] Univ Minnesota, Conservat Biol Program, St Paul, MN 55108 USA. [Dinerstein, Eric; Wikramanayake, Eric; Anderson, Michael L.; Olson, David; Seidensticker, John; Lumpkin, Susan; Palminteri, Suzanne; Hahn, Nathan R.] RESOLVE, Biodivers & Wildlife Solut Program, 1255 23rd St NW, Washington, DC 20037 USA. [Jones, Benjamin S.] Stanford Univ, Stanford, CA 94305 USA. [Seidensticker, John] Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Hansen, Matthew C.] Univ Maryland, College Pk, MD 20742 USA. [Sizer, Nigel C.; Davis, Crystal L.] World Resources Inst, 10 G St, Washington, DC 20002 USA. RP Joshi, AR (reprint author), Univ Minnesota, Conservat Biol Program, St Paul, MN 55108 USA. EM joshi002@umn.edu NR 27 TC 0 Z9 0 U1 9 U2 16 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 2375-2548 J9 SCI ADV JI Sci. Adv. PD APR PY 2016 VL 2 IS 4 AR e1501675 DI 10.1126/sciadv.1501675 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DR7IB UT WOS:000380072100030 PM 27051881 ER PT J AU Morris, JT Barber, DC Callaway, JC Chambers, R Hagen, SC Hopkinson, CS Johnson, BJ Megonigal, P Neubauer, SC Troxler, T Wigand, C AF Morris, James T. Barber, Donald C. Callaway, John C. Chambers, Randy Hagen, Scott C. Hopkinson, Charles S. Johnson, Beverly J. Megonigal, Patrick Neubauer, Scott C. Troxler, Tiffany Wigand, Cathleen TI Contributions of organic and inorganic matter to sediment volume and accretion in tidal wetlands at steady state SO EARTHS FUTURE LA English DT Article ID SEA-LEVEL RISE; MARSH VERTICAL ACCRETION; MISSISSIPPI RIVER DELTA; BULK-DENSITY; SPARTINA-ALTERNIFLORA; SALT-MARSHES; FRESH-WATER; FOREST SOILS; DECOMPOSITION; BAY AB A mixing model derived from first principles describes the bulk density ( BD) of intertidal wetland sediments as a function of loss on ignition (LOI). The model assumes that the bulk volume of sediment equates to the sum of self-packing volumes of organic and mineral components or BD = 1/[LOI/k(1) + (1-LOI)/k(2)], where k(1) and k(2) are the self-packing densities of the pure organic and inorganic components, respectively. The model explained 78% of the variability in total BD when fitted to 5075 measurements drawn from 33 wetlands distributed around the conterminous United States. The values of k(1) and k(2) were estimated to be 0.085 +/- 0.0007 g cm(-3) and 1.99 +/- 0.028 g cm(-3), respectively. Based on the fitted organic density (k(1)) and constrained by primary production, the model suggests that the maximum steady state accretion arising from the sequestration of refractory organic matter is <= 0.3 cm yr(-1). Thus, tidal peatlands are unlikely to indefinitely survive a higher rate of sea-level rise in the absence of a significant source of mineral sediment. Application of k(2) to a mineral sediment load typical of East and eastern Gulf Coast estuaries gives a vertical accretion rate from inorganic sediment of 0.2 cm yr(-1). Total steady state accretion is the sum of the parts and therefore should not be greater than 0.5 cm yr(-1) under the assumptions of the model. Accretion rates could deviate from this value depending on variation in plant productivity, root: shoot ratio, suspended sediment concentration, sediment-capture efficiency, and episodic events. C1 [Morris, James T.] Univ South Carolina, Dept Biol Sci, Belle W Baruch Inst Marine & Coastal Sci, Columbia, SC 29208 USA. [Barber, Donald C.] Bryn Mawr Coll, Dept Geol, Bryn Mawr, PA 19010 USA. [Callaway, John C.] Univ Calif San Francisco, Dept Environm Sci, San Francisco, CA 94143 USA. [Chambers, Randy] Coll William & Mary, Keck Environm Field Lab, Williamsburg, VA USA. [Hagen, Scott C.] Louisiana State Univ, Dept Civil & Environm Engn, Baton Rouge, LA 70803 USA. [Hagen, Scott C.] Louisiana State Univ, Ctr Computat & Technol, Baton Rouge, LA 70803 USA. [Hopkinson, Charles S.] Univ Georgia, Dept Marine Sci, Athens, GA 30602 USA. [Johnson, Beverly J.] Bates Coll, Dept Geol, Lewiston, ME 04240 USA. [Megonigal, Patrick] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. [Neubauer, Scott C.] Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. [Troxler, Tiffany] Florida Int Univ, Dept Biol Sci, Southeast Environm Res Ctr, Miami, FL 33199 USA. [Wigand, Cathleen] US EPA, Atlantic Ecol Div, Off Res & Dev, Natl Hlth & Environm Effects Res Lab, Narragansett, RI USA. RP Morris, JT (reprint author), Univ South Carolina, Dept Biol Sci, Belle W Baruch Inst Marine & Coastal Sci, Columbia, SC 29208 USA. EM morris@biol.sc.edu FU NOAA [NA10NOS4780146]; NSF DEB [1052636, 0620409, 9910514, 1237517, 1127958, 0950090, 1457100, 1355059]; NSF EAR [1322859, 1322658]; NSF [OCE-1238212]; NICCR [DE-FC02-06ER64298]; NASA [NNH14AY67]; Bates College Student Research Fund; Bryn Mawr College Summer Science Research Program; Conservation International; IUCN; IOC-UNESCO FX This research was supported by NOAA grant NA10NOS4780146, NSF DEB grants 1052636, 0620409, 9910514, 1237517, 1127958, 0950090, 1457100 and 1355059, NSF EAR grants 1322859 and 1322658, NSF OCE-1238212, NICCR grant DE-FC02-06ER64298, NASA grant NNH14AY67, the Bates College Student Research Fund, the Bryn Mawr College Summer Science Research Program, and the Blue Carbon Initiative coordinated by Conservation International, IUCN, and IOC-UNESCO. NR 89 TC 5 Z9 5 U1 25 U2 38 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2328-4277 J9 EARTHS FUTURE JI Earth Future PD APR PY 2016 VL 4 IS 4 BP 110 EP 121 DI 10.1002/2015EF000334 PG 12 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA DR1MD UT WOS:000379668700002 PM 27819012 ER PT J AU Park, T Fitzgerald, EMG Evans, AR AF Park, Travis Fitzgerald, Erich M. G. Evans, Alistair R. TI Ultrasonic hearing and echolocation in the earliest toothed whales SO BIOLOGY LETTERS LA English DT Article DE evolution; fossil; Oligocene; Odontoceti; Cetacea; cochlea ID INNER-EAR; ODONTOCETI; RADIATION; OLIGOCENE; CETACEANS; EVOLUTION; PETROSAL AB The evolution of biosonar (production of high-frequency sound and reception of its echo) was a key innovation of toothed whales and dolphins (Odontoceti) that facilitated phylogenetic diversification and rise to ecological predominance. Yet exactly when high-frequency hearing first evolved in odontocete history remains a fundamental question in cetacean biology. Here, we show that archaic odontocetes had a cochlea specialized for sensing high-frequency sound, as exemplified by an Oligocene xenorophid, one of the earliest diverging stem groups. This specialization is not as extreme as that seen in the crown Glade. Paired with anatomical correlates for high-frequency signal production in Xenorophidae, this is strong evidence that the most archaic toothed whales possessed a functional biosonar system, and that this signature adaptation of odontocetes was acquired at or soon after their origin. C1 [Park, Travis; Evans, Alistair R.] Monash Univ, Sch Biol Sci, Melbourne, Vic 3004, Australia. [Park, Travis; Fitzgerald, Erich M. G.; Evans, Alistair R.] Museum Victoria, Geosci, Melbourne, Vic, Australia. [Fitzgerald, Erich M. G.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Park, T (reprint author), Monash Univ, Sch Biol Sci, Melbourne, Vic 3004, Australia.; Park, T (reprint author), Museum Victoria, Geosci, Melbourne, Vic, Australia. EM travis.park@monash.edu OI Evans, Alistair/0000-0002-4078-4693; Park, Travis/0000-0002-9492-8859 FU Australian Postgraduate Award FX T.P. received an Australian Postgraduate Award. NR 17 TC 5 Z9 5 U1 43 U2 58 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 APR 1 PY 2016 VL 12 IS 4 AR 20160060 DI 10.1098/rsbl.2016.0060 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA DN8GR UT WOS:000377317700016 ER PT J AU Cheng, BS Grosholz, ED AF Cheng, Brian S. Grosholz, Edwin D. TI Environmental stress mediates trophic cascade strength and resistance to invasion SO ECOSPHERE LA English DT Article DE biotic resistance; climate change; consumer stress; environmental stress model; estuarine gradient; indirect effect; invasion; Ostrea lurida; range limit; tri-trophic interaction; trophic cascade; trophic sensitivity ID UROSALPINX-CINEREA SAY; FOOD-WEB STRUCTURE; CLIMATE-CHANGE; BIOTIC RESISTANCE; TOP-DOWN; WARMING STRENGTHENS; OYSTER DRILL; BOTTOM-UP; TEMPERATURE; COMMUNITY AB Although much attention has focused on the drivers of trophic cascade strength among systems (e.g., habitat type, body size, predator, and prey thermy) comparatively little is known of how trophic cascades change within systems, especially with respect to gradients in environmental stress. To address this, we measured the strength of a trophic cascade across an estuarine stress gradient and tested the predictions of "consumer stress model" that suggests sensitivity to stress is greater in mobile consumers relative to sessile prey. We used field observations and experimental manipulations within a central California estuary (Tomales Bay), where higher water temperatures in summer/fall and lower salinity during winter/spring may differentially affect predators (native crabs), meso-consumers (invasive oyster drills), and sessile prey (native oysters). Our results demonstrate that sites with high environmental stress (warmer and lower salinity waters) excluded top predators from the food web, which facilitated high densities of oyster drills and resulted in low oyster survival. In contrast, less stressful sites (cooler and higher salinity waters) had high crab densities leading to reduced oyster drill survival and high oyster survival (an indirect positive effect). Observational data from 14 field sites along both margins of Tomales Bay are consistent with the results of experimental manipulations. This study highlights the importance of environmental stress in mediating within system trophic cascade strength by altering top predator abundance. Our results support the predictions of the consumer stress model and suggest that increasing environmental stress (warming and variable salinity regimes) as a result of climate change may decouple species interactions. Furthermore, warming and extreme low salinities may indirectly intensify the negative effects of non-native species by reducing the biotic resistance provided by native predators. C1 [Cheng, Brian S.; Grosholz, Edwin D.] Univ Calif Davis, Bodega Marine Lab, 2099 Westside Rd, Bodega Bay, CA 94923 USA. [Cheng, Brian S.; Grosholz, Edwin D.] Univ Calif Davis, Dept Environm Sci & Policy, One Shields Ave, Davis, CA 95616 USA. [Cheng, Brian S.] Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. RP Cheng, BS (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM bscheng@gmail.com OI Cheng, Brian/0000-0003-1679-8398 FU National Park Service George Melendez Wright Climate Change Fellowship; National Estuarine Research Reserve System Graduate Research Fellowship; National Science Foundation GK-12 Fellowship; California Sea Grant Program [R/ENV-203] FX We thank J. Couture, S. Covello, C. Knight, C. Norton, D. Hooper, H. Long, K. Griffith, A. Deck, C. Coleman-Hulburt, and L. Komoroske for lab and field assistance. We thank B. Becker and S. Allen for access to sites and logistical support. We also thank M. Whalen and S. Burgess for statistical consulting. Special thanks to J. Largier and M. Robart for BOON time-series data. E. Sanford, J. Stachowicz, M. Whalen, and N. Fangue provided insightful comments on earlier versions of this manuscript. This project was supported by grants from the National Park Service George Melendez Wright Climate Change Fellowship (BSC), National Estuarine Research Reserve System Graduate Research Fellowship (BSC), National Science Foundation GK-12 Fellowship (BSC), and the California Sea Grant Program (Grant #R/ENV-203 to EDG). Species graphics courtesy of T. Saxby, Integration and Application Network, University of Maryland Center for Environmental Science (http://ian.umces.edu/imagelibrary/) and S. Dana, Information and Educational Technology, University of California, Davis. This manuscript is a contribution from the Bodega Marine Laboratory, University of California, Davis. NR 70 TC 2 Z9 2 U1 17 U2 31 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD APR PY 2016 VL 7 IS 4 AR e01247 DI 10.1002/ecs2.1247 PG 13 WC Ecology SC Environmental Sciences & Ecology GA DN6VA UT WOS:000377213400003 ER PT J AU Chaboo, CS Chamorro, ML Scholler, M AF Chaboo, Caroline S. Chamorro, Maria Lourdes Schoeller, Matthias TI CATALOGUE OF KNOWN IMMATURE STAGES OF CAMPTOSOMATE LEAF BEETLES (COLEOPTERA, CHRYSOMELIDAE, CRYPTOCEPHALINAE AND LAMPROSOMATINAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Morphology; egg; larva; pupa; myrmecophily; Camptosomata; life history ID ANOMOEA-FLAVOKANSIENSIS COLEOPTERA; 1ST INSTAR LARVA; LIFE-HISTORY; CHLAMISUS CRIBRIPENNIS; NEOCHLAMISUS KARREN; 1ST-INSTAR LARVA; HOST-SPECIFICITY; NATURAL-HISTORY; CADMUS ERICHSON; EGG BURSTERS AB Lack of syntheses of knowledge on immature stages of insects impedes accurate understanding of their diversity, biology and evolution. Literature describing known immature stages of case-bearing chrysomelids is catalogued, i.e., 358 species of Cryptocephalinae Gyllenhal and 13 species of Lamprosomatinae Lacordaire. The catalogue covers the world fauna including fossils, and reviews information on eggs, larvae, pupae, host plants, distribution, host ants (for myrmecophiles), and parasitoids and predators. This synthesis should stimulate efforts to discover and study immatures, and generate new hypotheses about the evolution in these two sister clades of leaf beetles. C1 [Chaboo, Caroline S.] Univ Kansas, Div Entomol, 1501 Crestline Dr,Suite 140, Lawrence, KS 66045 USA. [Chamorro, Maria Lourdes] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, MRC 168,POB 37012, Washington, DC 20013 USA. [Schoeller, Matthias] Humboldt Univ, Fac Life Sci, Lentzeallee 55-57, D-14195 Berlin, Germany. RP Chaboo, CS (reprint author), Univ Kansas, Div Entomol, 1501 Crestline Dr,Suite 140, Lawrence, KS 66045 USA. EM cschaboo@ku.edu FU NSF-EPSCOR [66928]; U.S. Department of Agriculture (U.S.D.A.) FX This research was supported by the authors' respective institutions and NSF-EPSCOR grant #66928 to C.S. Chaboo. The research of Lourdes Chamorro is supported by the U.S. Department of Agriculture (U.S.D.A.); USDA is an equal opportunity provider and employer. In this project, assembling literature was a challenge so we are grateful to the following for helping us track down certain works: Alexander Konstantinov and Vladimir Blagoderov for part of the Russian literature and translations; Dashdondog Narangarvuu for part of the literature on Mongolian species; Davide Sassi and Stefano Zoia for part of Italian literature, and Michael Schmitt for part of the German literature. We are indebted to the following reviewers: Federico A. Agrain, Patrice Bouchard, Matthew Buffington, Vivian Flinte, Douglas Yanega, three anonymous reviewers, and the managing editors of the journal who provided valuable comments on the final version of the manuscript. NR 490 TC 2 Z9 2 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 2016 VL 118 IS 2 BP 150 EP 217 DI 10.4289/0013-8797.118.1.150 PG 68 WC Entomology SC Entomology GA DN0NH UT WOS:000376760100002 ER PT J AU Chamorro, ML Persson, J Torres-Santana, CW Keularts, J Scheffer, SJ Lewis, ML AF Chamorro, M. Lourdes Persson, Joshua Torres-Santana, Christian W. Keularts, Jeff Scheffer, Sonja J. Lewis, Matthew L. TI MOLECULAR AND MORPHOLOGICAL TOOLS TO DISTINGUISH SCYPHOPHORUS ACUPUNCTATUS GYLLENHAL, 1838 (CURCULIONIDAE: DRYOPHTHORINAE): A NEW WEEVIL PEST OF THE ENDANGERED CENTURY PLANT, AGAVE EGGERSIANA FROM ST. CROIX, US VIRGIN ISLANDS SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE larval morphology; Palm weevils; COI; EF1a; conservation; Endangered Species Act; West Indies; Scyphophorus yuccae; Sphenophorus cubensis ID BAYESIAN PHYLOGENETIC INFERENCE; COLEOPTERA-CURCULIONIDAE; LARVAL; CHARACTERS; MRBAYES; HOST AB The agave snout weevil (AGW) or sisal weevil, Scyphophorus acupunctatus Gyllenhal is here reported for the first time in St. Croix, U.S. Virgin Islands (USVI) where it threatens Agave eggersiana Trel., a USVI endemic and endangered century-plant. We provide molecular, morphological, and behavioral characters to successfully distinguish the two known Scyphophorus species at all developmental stages. We identified seven new larval characters on the mandibles and characters relating to the chaetotaxy of the labrum and labio-maxillary complex as well as new, putatively informative characters for weevil systematics: chitinized arm of mentum (postlabial strut or postlabial bracon) and the presence of 4 ventral malar setae, instead of 5. In the pupae, the difference in number and placement of rostral setae were also found to be diagnostic. We analyzed two genes, mtCO1 and EF1a, to confirm the identity of the immatures. Phylogenetic analysis of both genes separately and together suggests a clear pattern of substantial phylogeographic structure with specimens clustering by geographic location and this pattern strongly suggests the presence of cryptic species or allopatrically diverged populations. We provide management recommendations for the protection of Agave eggersiana against the threat posed by ASW. We also report, for the first time, the presence of Sphenophorus cubensis (Buchanan) in St. Croix and Scyphophorus yuccae Horn in Panama on Hesperoyucca whipplei (Torr.) Trel. (Asparagaceae: Agavoideae). C1 [Chamorro, M. Lourdes] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. [Persson, Joshua] George Mason Univ, Fairfax, VA 22030 USA. [Torres-Santana, Christian W.] US Forest Serv, Int Inst Trop Forestry, USDA, 1201 Calle Ceiba, San Juan, PR 00926 USA. [Torres-Santana, Christian W.] Fdn Luis Munoz Marin, Arboretum Parque Dona Ines, RR 2,Buzon 5, San Juan, PR 00926 USA. [Keularts, Jeff] Univ Virgin Isl, St Croix Campus,RR1 Box 10000, Kingshill, VI 00850 USA. [Scheffer, Sonja J.] ARS, Systemat Entomol Lab, USDA, Beltsville, MD USA. RP Chamorro, ML (reprint author), ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM lourdes.chamorro@ars.usda.gov NR 58 TC 0 Z9 0 U1 3 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 2016 VL 118 IS 2 BP 218 EP 243 DI 10.4289/0013-8797.118.2.218 PG 26 WC Entomology SC Entomology GA DN0NH UT WOS:000376760100003 ER PT J AU Davis, DR Graves, GR AF Davis, Donald R. Graves, Gary R. TI A NEW LEAFMINING MOTH (CAMERARIA COTINIVORA, LEPIDOPTERA: GRACILLARIIDAE) OF THE AMERICAN SMOKETREE (COTINUS OBOVATUS) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE American smoketree; Cameraria cotinivora; Cameraria guttifinitella; Cotinus obovatus; Gracillariidae; leafminer; taxonomy ID SCHINUS-TEREBINTHIFOLIUS-RADDI AB Fieldwork in the Ozark Mountains of the central United States by GRG over the last decade involving the American smoketree, Cotinus obovatus Raf. (Anacardiaceae), has resulted in the discovery of a previously unknown moth species belonging to the genus Cameraria (Lepidoptera: Gracillariidae). The larva of this species mines the leaf mesophyll of this tree, creating serpentine mines most visible from the upper (adaxial) surface of the leaf. The most closely related species to Cameraria cotinivora, n. sp. is Cameraria guttifinitella (Clemens), a common leafminer of poison ivy, Toxicodendron radicans (L.) Kuntze (Anacardiaceae). Illustrations of both species are provided as well as a COI analysis of their genetic relationship. C1 [Davis, Donald R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012,MRC 168, Washington, DC 20013 USA. [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012,MRC 116, Washington, DC 20013 USA. [Graves, Gary R.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark. RP Davis, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012,MRC 168, Washington, DC 20013 USA.; Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012,MRC 116, Washington, DC 20013 USA.; Graves, GR (reprint author), Univ Copenhagen, Nat Hist Museum Denmark, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark. EM davisd@si.edu; gravesg@si.edu RI publicationpage, cmec/B-4405-2017 FU government of Canada through Genome Canada; Ontario Genomics Institute; Alexander Wetmore Fund; Smithsonian Institution; Smoketree Trust FX We are indebted to Vichai Malikul, Young Sohn, Donald Harvey, and Karolyn Darrow of the Department of Entomology, Smithsonian Institution, for the illustrations, graphics, and the preparation of plates used in this publication. Donald Harvey and Margaret Rosati also assisted in preparing the neighbor-joining tree (figure 12). We especially thank Margaret Rosati, Department of Entomology, Smithsonian Institution, for her assistance in assembling the barcode tree data. We thank Jean F. Landry, Agriculture Canada, Camiel Doorenweerd and Erik van Nieukerken, Naturalis Biodiversity Center, Leiden, The Netherlands, and Carlos Lopez-Vaamonde, INRA Orleans, Unite de Recherche en Zoologie Forestiere, France for their permission to use their barcode data, and to Paul Hebert and Jeremy deWaard of the Biodiversity Institute of Ontario, University of Guelph, Canada, for providing barcode data. Financial support for DNA barcoding was provided by the government of Canada through Genome Canada and the Ontario Genomics Institute in support of the International Barcode of Life project. Mignon Davis assisted with data capture and specimen curation. GRG was supported by the Alexander Wetmore Fund, Smithsonian Institution, and by the Smoketree Trust. Finally we thank Erik van Nieukerken and Jurate De Prins for their reviews of this paper. NR 18 TC 0 Z9 0 U1 1 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2016 VL 118 IS 2 BP 244 EP 253 PG 10 WC Entomology SC Entomology GA DN0NH UT WOS:000376760100004 ER PT J AU Kula, RR AF Kula, Robert R. TI CARDIOCHILINAE AND ICHNEUTINAE (HYMENOPTERA: BRACONIDAE) OF KONZA PRAIRIE SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE biodiversity; conservation; Flint Hills; gallery forest; Great Plains; Kansas; Nearctic; new species; parasitoid; tallgrass prairie; taxonomy ID WASPS HYMENOPTERA; GENERA; ICHNEUMONOIDEA; REVISION; HALIDAY; TRIBE; RNA AB The results of a survey of Cardiochilinae and Ichneutinae (Hymenoptera: Braconidae) at Konza Prairie near Manhattan, Kansas are reported. Eleven sites representing prairie and woodland/wetland areas, including gallery forest, were sampled in 2001 and 2005 using Malaise traps and a canopy trap. Selected sites were also sampled haphazardly using pan traps and a sweep net. Six species of Cardiochilinae and two species of Ichneutinae were collected. Cardiochilines were collected at woodland/wetland sites only except a single specimen collected at a prairie site. Both species of Ichneutinae were collected at woodland/wetland sites and prairie sites. Cardiochiles floridanus (Ashmead) (n=3) and Cardiochiles minutus (Cresson) (n=4) were the most abundant species of Cardiochilinae in 2001 and 2005, respectively. Paroligoneurus newharti Kula, new species, the most abundant species of Ichneutinae in 2001 and only ichneutine collected in 2005, is described. Cardiochiles insculptus Mao and Cardiochiles minutus (Cresson) are reported from Kansas for the first time. C1 [Kula, Robert R.] ARS, Systemat Entomol Lab, Beltsville Agr Res Ctr, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. RP Kula, RR (reprint author), ARS, Systemat Entomol Lab, Beltsville Agr Res Ctr, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM Robert.Kula@ars.usda.gov NR 45 TC 0 Z9 0 U1 1 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2016 VL 118 IS 2 BP 273 EP 288 DI 10.4289/0013-8797.118.2.273 PG 16 WC Entomology SC Entomology GA DN0NH UT WOS:000376760100007 ER PT J AU Smith, DR AF Smith, David R. TI Pristiphora subbifida (Thomson) (Hymenoptera: Tenthredinidae), a Palearctic Sawfly New to North America SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material C1 [Smith, David R.] ARS, Systemat Entomol Lab, Natl Museum Nat Hist, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, Natl Museum Nat Hist, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM sawfly2@aol.com NR 5 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2016 VL 118 IS 2 BP 297 EP 299 DI 10.4289/0013-8797.118.2.297 PG 3 WC Entomology SC Entomology GA DN0NH UT WOS:000376760100009 ER PT J AU Smith, DR Monjaras-Barrera, JI Aguilar-Hernandez, JC Quinones-Dena, H AF Smith, David R. Irving Monjaras-Barrera, Jose Cupertino Aguilar-Hernandez, Jose Quinones-Dena, Hector TI New Host and Distribution Records for Zadiprion rohweri (Middleton) (Hymenoptera: Diprionidae), a Pinyon Pine Sawfly SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material ID GENUS C1 [Smith, David R.] ARS, Systemat Entomol Lab, Natl Museum Nat Hist, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. [Irving Monjaras-Barrera, Jose; Cupertino Aguilar-Hernandez, Jose; Quinones-Dena, Hector] Univ Autonoma Agr Antonio Narro, Dept Parasitol, Calzada Antonio Narro 1923, Saltillo 25315, Coahuila, Mexico. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, Natl Museum Nat Hist, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA.; Monjaras-Barrera, JI; Aguilar-Hernandez, JC; Quinones-Dena, H (reprint author), Univ Autonoma Agr Antonio Narro, Dept Parasitol, Calzada Antonio Narro 1923, Saltillo 25315, Coahuila, Mexico. EM sawfly2@aol.com; Irving_032@hotmail.com; che_1703@hotmail.com; hectorqd68@gmail.com NR 7 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2016 VL 118 IS 2 BP 300 EP 301 DI 10.4289/0013-8797.118.2.300 PG 2 WC Entomology SC Entomology GA DN0NH UT WOS:000376760100010 ER PT J AU Naiman, JP AF Naiman, J. P. TI AstroBlend: An astrophysical visualization package for Blender SO ASTRONOMY AND COMPUTING LA English DT Article DE Miscellaneous; Methods: numerical ID GALAXY SIMULATIONS; MILKY-WAY; CODE; HYDRODYNAMICS; ASTRONOMY; CLUSTERS; FEEDBACK; DRIVEN AB The rapid growth in scale and complexity of both computational and observational astrophysics over the past decade necessitates efficient and intuitive methods for examining and visualizing large datasets. Here, I present AstroBlend, an open-source Python library for use within the three dimensional modeling software, Blender, While Blender has been a popular open-source software among animators and visual effects artists, in recent years it has also become a tool for visualizing astrophysical datasets. AstroBlend combines the three dimensional capabilities of Blender with the analysis tools of the widely used astrophysical toolset, yt, to afford both computational and observational astrophysicists the ability to simultaneously analyze their data and create informative and appealing visualizations. The introduction of this package includes a description of features, work flow, and various example visualizations. A website - www.astroblend.com - has been developed which includes tutorials, and a gallery of example images and movies, along with links to downloadable data, three dimensional artistic models, and various other resources. (C) 2016 Elsevier B.V. All rights reserved. C1 [Naiman, J. P.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. RP Naiman, JP (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM jill.naiman@cfa.harvard.edu FU NSF [AST-1402480] FX The author would like to acknowledge illuminating discussions with Matthew Turk, Morgan MacLeod, Melinda Soares-Furtado and Enrico Ramirez-Ruiz. In addition, the thorough comments of one anonymous reviewer and the extensive input of another, Dr. Rhys Taylor were invaluable. This work is supported by an NSF grant AST-1402480. NR 34 TC 0 Z9 0 U1 3 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2213-1337 EI 2213-1345 J9 ASTRON COMPUT JI Astron. Comput. PD APR PY 2016 VL 15 BP 50 EP 60 DI 10.1016/j.ascom.2016.02.002 PG 11 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA DM7LV UT WOS:000376543000005 ER PT J AU Thomas, DB James, HF AF Thomas, Daniel B. James, Helen F. TI Nondestructive Raman spectroscopy confirms carotenoid-pigmented plumage in the Pink-headed Duck SO AUK LA English DT Article DE Anseriformes; coloration; feather; pigmentation; Raman spectroscopy; Rhodonessa ID COLORATION; WATERFOWL; BIRDS; EVOLUTION; ANATIDAE; FEATHERS AB A small group of pigment classes is responsible for the wide range of plumage colors in modern birds. Yellow, pink, and other "warm" feather colors of many species are attributed to carotenoid pigments, a plumage trait that has an uneven distribution across modern bird species. Carotenoid plumage pigments are especially rare among fowl (superorder Galloanseres), and until recently, the Pink-eared Duck (Malacorhynchus membranaceus) from Australia provided the only evidence that any species of waterfowl (order Anseriformes) exhibits carotenoid-pigmented plumage. We analyzed a Pink-headed Duck (Rhodonessa caryophyllacea) study skin using Raman spectroscopy, without plucking or otherwise damaging the specimen. Raman spectra confirmed that the pink feathers of Rhodonessa are pigmented with carotenoids. Spectra from Rhodonessa were similar to those from Malacorhynchus, which suggests that the same carotenoid is the primary plumage pigment in both species. Moreover, spectra from Rhodonessa were similar to spectra from other taxa pigmented with ketocarotenoids. Malacorhynchus and Rhodonessa are distant relatives within Anseriformes, so these findings indicate multiple evolutionary origins of plumage carotenoids within the waterfowl or (less likely) many losses of plumage carotenoids from duck species. Our results show that pigment chemistry can be studied in precious ornithological specimens without damaging the specimens, and provide new evidence that the (apparently extinct) Rhodonessa possessed what is evolutionarily an extremely rare trait among waterfowl. C1 [Thomas, Daniel B.] Massey Univ, Inst Nat & Math Sci, Auckland, New Zealand. [Thomas, Daniel B.; James, Helen F.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Thomas, DB (reprint author), Massey Univ, Inst Nat & Math Sci, Auckland, New Zealand.; Thomas, DB (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. EM d.b.thomas@massey.ac.nz FU Peter Buck Postdoctoral Fellowship; Wetmore Fund, Division of Birds, Smithsonian Institution FX D.B.T. was funded by a Peter Buck Postdoctoral Fellowship, provided by NMNH. Instrument rental was funded by the Wetmore Fund, Division of Birds, Smithsonian Institution. NR 33 TC 0 Z9 0 U1 2 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 2016 VL 133 IS 2 BP 147 EP 154 DI 10.1642/AUK-15-152.1 PG 8 WC Ornithology SC Zoology GA DN0QY UT WOS:000376770100003 ER PT J AU Ma, YP Chen, MM Wei, JX Zhao, L Liu, PL Dai, SL Wen, J AF Ma, Yue-Ping Chen, Meng-Meng Wei, Jiang-Xue Zhao, Liang Liu, Pei-Liang Dai, Si-Lan Wen, Jun TI Origin of Chrysanthemum cultivars - Evidence from nuclear low-copy LFY gene sequences SO BIOCHEMICAL SYSTEMATICS AND ECOLOGY LA English DT Article DE Chrysanthemum cultivars; Origin; Allopolyploidy; LFY gene ID BAYESIAN PHYLOGENETIC INFERENCE; HOMEOTIC GENE; FLORICAULA/LEAFY HOMOLOG; LEAFY; FLOWER; ARABIDOPSIS; EVOLUTION; ANGIOSPERMS; EXPRESSION; ALIGNMENT AB The chrysanthemums (Chrysanthemum x morifolium Ramat.) are a well-known group of traditional ornamental flowers in China and have been cultivated all over the world. Yet the origin of chrysanthemum cultivars has been highly debated. In this study we employ the nuclear low-copy LFY gene to study the evolutionary history of chrysanthemum cultivars. The structure of the LFY gene in all Chrysanthemum species examined is highly conserved with three exons and two introns. The length of the LFY gene in Chrysanthemum varied from 2, 887 to 3, 348 bp. The two introns exhibited high levels of variation in length and sequence composition at the intraspecific and interspecific levels. Phylogenetic analysis of the whole LFY sequences of Chrysanthemum resulted in topologies that contained three major clades. The LFY sequences from the same cultivars are present in two or three clades, supporting that hybridization and allopolyploidy were important mechanisms in the origins of different chrysanthemums. Our results suggest that different cultivars had different ancestors. Chrysanthemum indicum, C. zawadskii and C. nankingense were likely the direct ancestors of most chrysanthemum cultivars examined. Chrysanthemum vestitum is a putative ancestor for some cultivars, and may have indirectly involved in the development of the chrysanthemum cultivars. Sequences of the LFY gene are informative to shed insights into the origin of chrysanthemum cultivars and show great potential as a phylogenetic marker to decipher the phylogeny of Chrysanthemum and its close relatives. Published by Elsevier Ltd. C1 [Ma, Yue-Ping; Chen, Meng-Meng; Wei, Jiang-Xue] Northeastern Univ, Coll Life & Hlth Sci, Shenyang 110004, Peoples R China. [Zhao, Liang; Liu, Pei-Liang] Northwest A&F Univ, Coll Life Sci, Yangling 712100, Shaanxi, Peoples R China. [Dai, Si-Lan] Beijing Forestry Univ, Coll Landscape Architecture, Beijing 100083, Peoples R China. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. RP Dai, SL (reprint author), Beijing Forestry Univ, Coll Landscape Architecture, Beijing 100083, Peoples R China.; Wen, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. EM silandai@sina.com; wenj@si.edu FU National Natural Science Foundation of China [31470699, 31300158]; Fundamental Research Funds for the Central Universities [130420003, QN2012020, 2452015406]; Laboratories of Analytical Biology of the National Museum of Natural History, the Smithsonian Institution; China Scholarship Council FX This work was supported by the National Natural Science Foundation of China (No. 31470699, 31300158), the Fundamental Research Funds for the Central Universities (No. 130420003, QN2012020, 2452015406) and the Laboratories of Analytical Biology of the National Museum of Natural History, the Smithsonian Institution. The China Scholarship Council was gratefully acknowledged for financial support of Yueping Ma's research visit to the Smithsonian Institution. NR 37 TC 0 Z9 0 U1 2 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0305-1978 EI 1873-2925 J9 BIOCHEM SYST ECOL JI Biochem. Syst. Ecol. PD APR PY 2016 VL 65 BP 129 EP 136 DI 10.1016/j.bse.2016.02.010 PG 8 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA DK0JN UT WOS:000374599200018 ER PT J AU Cornelius, ML Buffington, ML Talamas, EJ Gates, MW AF Cornelius, Mary L. Buffington, Matthew L. Talamas, Elijah J. Gates, Michael W. TI Impact of the Egg Parasitoid, Gryon pennsylvanicum (Hymenoptera: Scelionidae), on Sentinel and Wild Egg Masses of the Squash Bug (Hemiptera: Coreidae) in Maryland SO ENVIRONMENTAL ENTOMOLOGY LA English DT Article DE biological control; egg parasitism; egg predation; pest management ID YELLOW VINE DISEASE; LEPTOGLOSSUS-OCCIDENTALIS HEIDEMANN; ANASA-TRISTIS HEMIPTERA; MARMORATED STINK BUG; TRISSOLCUS-BASALIS; ASHMEAD HYMENOPTERA; BIOLOGICAL-CONTROL; NATURAL ENEMIES; NEZARA-VIRIDULA; POPULATION-DYNAMICS AB Seasonal changes in egg parasitism and predation rates on sentinel (laboratory-reared) and wild (naturally occurring) egg masses of the squash bug, Anasa tristis (De Geer), were evaluated in squash fields in Maryland from June through September in 2013 and 2014. Rates of egg parasitism were significantly higher on wild egg masses than on sentinel egg masses. Squash bug nymphal emergence was significantly higher on sentinel egg masses than on wild egg masses. Between the first week of July and the first week of September of both survey years, squash bug nymphs emerged from 24.2% of wild eggs compared with 46.2% of sentinel eggs and parasitoids emerged from 55.7% of wild eggs compared with only 21.8% of sentinel eggs. Sentinel egg masses significantly underestimated the rate of natural egg parasitism. The egg parasitoid, Gryon pennsylvanicum (Ashmead), was responsible for over 99% of parasitism of squash bug eggs. There was a significant negative correlation between parasitoid emergence and nymphal emergence, suggesting that parasitoids were able to suppress squash bug populations. The average rate of parasitoid emergence peaked on wild egg masses on the fifth week of July at 72.8%, whereas the average rate of nymphal emergence from wild egg masses was < 20% from the fifth week of July until the first week of September. These results demonstrate that G. pennsylvanicum was able to efficiently track wild squash bug eggs throughout the season and that it has the potential to be an effective biological control agent of the squash bug in Maryland. C1 [Cornelius, Mary L.] USDA ARS, Invas Insect Biocontrol & Behav Lab, Beltsville Agr Res Ctr, 10300 Baltimore Ave,Bldg 007, Beltsville, MD 20705 USA. [Buffington, Matthew L.; Talamas, Elijah J.; Gates, Michael W.] USDA ARS, Systemat Entomol Lab, Natl Museum Nat Hist, Smithsonian Inst, 10th & Constitut Ave NW,MRC 168, Washington, DC 20560 USA. RP Cornelius, ML (reprint author), USDA ARS, Invas Insect Biocontrol & Behav Lab, Beltsville Agr Res Ctr, 10300 Baltimore Ave,Bldg 007, Beltsville, MD 20705 USA. EM mary.cornelius@ars.usda.gov; matt.buffington@ARS.USDA.GOV; elijah.talamas@ars.usda.gov; michael.gates@ars.usda.gov NR 45 TC 2 Z9 2 U1 0 U2 2 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0046-225X EI 1938-2936 J9 ENVIRON ENTOMOL JI Environ. Entomol. PD APR PY 2016 VL 45 IS 2 BP 367 EP 375 DI 10.1093/ee/nvv228 PG 9 WC Entomology SC Entomology GA DM5JO UT WOS:000376385000011 PM 26759367 ER PT J AU Murtagh, F Kurtz, MJ AF Murtagh, Fionn Kurtz, Michael J. TI The Classification Society's Bibliography Over Four Decades: History and Content Analysis SO JOURNAL OF CLASSIFICATION LA English DT Article DE Cluster analysis; Data analysis; Data analytics; Correspondence analysis; Search; Retrieval; Bibliography ID CLUSTER-ANALYSIS AB The Classification Literature Automated Search Service, an annual bibliography based on citation of one or more of a set of around 80 book or journal publications, ran from 1972 to 2012. We analyze here the years 1994 to 2012. The Classification Society's Service, as it was termed, was produced by the Classification Society. In earlier decades it was distributed as a diskette or CD with the Journal of Classification. Among our findings are the following: an enormous increase in scholarly production in this area post approximately 2000; and another big increase in quantity of publications from approximately 2004. The over 93,000 bibliographic records used is the basis for determining the research disciplines that we analyze. We make all this data available for download, formatted in text and in XML, with an accompanying Apache Lucene/Solr search interface. C1 [Murtagh, Fionn] Univ London, London SE14 6NW, England. [Kurtz, Michael J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Murtagh, F (reprint author), Univ London, Dept Comp, London SE14 6NW, England. EM fmurtagh@acm.org NR 15 TC 0 Z9 0 U1 4 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0176-4268 EI 1432-1343 J9 J CLASSIF JI J. Classif. PD APR PY 2016 VL 33 IS 1 BP 6 EP 29 DI 10.1007/s00357-016-9196-4 PG 24 WC Mathematics, Interdisciplinary Applications; Psychology, Mathematical SC Mathematics; Psychology GA DM7BP UT WOS:000376508200002 ER PT J AU Ceruzzi, PE AF Ceruzzi, Paul E. TI Moore's Law: The Life of Gordon Moore, Silicon Valley's Quiet Revolutionary SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Ceruzzi, Paul E.] Smithsonian Inst, Natl Air & Space Museum, Space Hist Dept, Washington, DC 20560 USA. RP Ceruzzi, PE (reprint author), Smithsonian Inst, Natl Air & Space Museum, Space Hist Dept, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 8 U2 8 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X EI 1097-3729 J9 TECHNOL CULT JI Technol. Cult. PD APR PY 2016 VL 57 IS 2 BP 499 EP 500 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA DM6OP UT WOS:000376472600029 ER PT J AU Almeida, D Maldonado, E Khan, I Silva, L Gilbert, MTP Zhang, GJ Jarvis, ED O'Brien, SJ Johnson, WE Antunes, A AF Almeida, Daniela Maldonado, Emanuel Khan, Imran Silva, Liliana Gilbert, M. Thomas P. Zhang, Guojie Jarvis, Erich D. O'Brien, Stephen J. Johnson, Warren E. Antunes, Agostinho TI Whole-Genome Identification, Phylogeny, and Evolution of the Cytochrome P450 Family 2 (CYP2) Subfamilies in Birds SO GENOME BIOLOGY AND EVOLUTION LA English DT Article DE avian genomes; cytochrome P450 (CYPs); substrate recognition sites (SRS); heme binding areas (HEM); positive selection ID AMINO-ACID SITES; DETECTING POSITIVE SELECTION; SUBSTRATE RECOGNITION SITES; ADAPTIVE EVOLUTION; MAXIMUM-LIKELIHOOD; MOLECULAR EVOLUTION; STATISTICAL-METHODS; CODON-SUBSTITUTION; SEQUENCE ALIGNMENT; DRUG-METABOLISM AB The cytochrome P450 (CYP) superfamily defends organisms from endogenous and noxious environmental compounds, and thus is crucial for survival. However, beyond mammals the molecular evolution of CYP2 subfamilies is poorly understood. Here, we characterized the CYP2 family across 48 avian whole genomes representing all major extant bird clades. Overall, 12 CYP2 subfamilies were identified, including the first description of the CYP2F, CYP2G, and several CYP2AF genes in avian genomes. Some of the CYP2 genes previously described as being lineage-specific, such as CYP2K and CYP2W, are ubiquitous to all avian groups. Furthermore, we identified a large number of CYP21 copies, which have been associated previously with water reabsorption. We detected positive selection in the avian CYP2C, CYP2D, CYP2H, CYP2J, CYP2K, and CYP2AC subfamilies. Moreover, we identified new substrate recognition sites (SRSO, SRS2 SRS3, and 51353.1) and heme binding areas that influence CYP2 structure and function of functional importance as under significant positive selection. Some of the positively selected sites in avian CYP2D are located within the same SRS1 region that was previously linked with the metabolism of plant toxins. Additionally, we find that selective constraint variations in some avian CYP2 subfamilies are consistently associated with different feeding habits (CYP2H and CYP21), habitats (CYP2D, CYP2H, CYP2J, and CYP2K), and migratory behaviors (CYP2D, CYP2H, and CYP2J). Overall, our findings indicate that there has been active enzyme site selection on CYP2 subfamilies and differential selection associated with different life history traits among birds. C1 [Almeida, Daniela; Maldonado, Emanuel; Khan, Imran; Silva, Liliana; Antunes, Agostinho] Univ Porto, Interdisciplinary Ctr Marine & Environm Res, CIIMAR CIMAR, Rua Campo Alegre 823, P-4100 Oporto, Portugal. [Almeida, Daniela; Khan, Imran; Silva, Liliana; Antunes, Agostinho] Univ Porto, Fac Sci, Dept Biol, Rua Campo Alegre 823, P-4100 Oporto, Portugal. [Gilbert, M. Thomas P.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, DK-1168 Copenhagen, Denmark. [Zhang, Guojie] BGI Shenzhen, China Natl GeneBank, Shenzhen, Peoples R China. [Zhang, Guojie] Univ Copenhagen, Dept Biol, Ctr Social Evolut, Copenhagen, Denmark. [Jarvis, Erich D.] Duke Univ, Med Ctr Durham, Dept Neurobiol, Durham, NC 27706 USA. [Jarvis, Erich D.] Howard Hughes Med Inst, Chevy Chase, MD USA. [O'Brien, Stephen J.] St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, St Petersburg 199034, Russia. [O'Brien, Stephen J.] Nova SE Univ, Oceanog Ctr, Ft Lauderdale, FL 33314 USA. [Johnson, Warren E.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC USA. RP Antunes, A (reprint author), Univ Porto, Interdisciplinary Ctr Marine & Environm Res, CIIMAR CIMAR, Rua Campo Alegre 823, P-4100 Oporto, Portugal.; Antunes, A (reprint author), Univ Porto, Fac Sci, Dept Biol, Rua Campo Alegre 823, P-4100 Oporto, Portugal. EM aantunes@ciimar.up.pt OI Maldonado, Emanuel/0000-0002-0084-6116; Almeida, Daniela/0000-0002-9874-933X FU Fundacao para a Ciencia e a Tecnologia (FCT) [SFRH/BD/79766/2011, SFRH/BD/48518/2008]; Howard Hughes Medical Institute (HHMI); Russian Ministry of Science Mega-grant [11.G34.31.0068]; Strategic Funding through national fund by FCT [UID/Multi/04423/2013]; Strategic Funding through national fund by European Regional Development Fund (ERDF) [PT2020]; FCT [PTDC/AAG-GLO/6887/2014] FX We owe special thanks to Tibisay Escalona, Aldo Barreiro, Rui Borges, and Rosalina Goulao for their helpful discussions and support. The authors are thankful to the Associate Editor Dr Jose Pereira-Leal and the anonymous reviewers for their valuable comments and suggestions. D.A. and I.K. were funded with a PhD grant from Fundacao para a Ciencia e a Tecnologia (FCT) (SFRH/BD/79766/2011 and SFRH/BD/48518/2008, respectively) E.D.J. was supported by the Howard Hughes Medical Institute (HHMI). S.J.O. was supported as Principal Investigator by Russian Ministry of Science Mega-grant no. 11.G34.31.0068. A.A. was partially supported by the Strategic Funding UID/Multi/04423/2013 through national funds provided by FCT and European Regional Development Fund (ERDF) in the framework of the programme PT2020, and the FCT project PTDC/AAG-GLO/6887/2014. NR 83 TC 0 Z9 0 U1 12 U2 17 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1759-6653 J9 GENOME BIOL EVOL JI Genome Biol. Evol. PD APR PY 2016 VL 8 IS 4 BP 1115 EP 1131 DI 10.1093/gbe/evw041 PG 17 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA DM1SL UT WOS:000376126400013 PM 26979796 ER PT J AU Neufeld, M AF Neufeld, Michael TI NASA'S PLUTO MISSION SO PHYSICS TODAY LA English DT Article AB As spectacular pictures slowly trickle back from an enormously distant New Horizons spacecraft, which shot through the Pluto-Charon system on 14 July 2015, it is easy to think that this mission was inevitable-the capstone to the US's pioneering exploration of the solar system. But it took 17 difficult years to get from the first proposal to launch day, 19 January 2006. On the way, there were many changes of course and three outright cancellations. Far from being inevitable, the Pluto mission was saved from oblivion several times by dogged advocacy, protests by scientists and the public, political intervention by Senator Barbara Mikulski (D-MD), and a timely endorsement by the National Academies. C1 [Neufeld, Michael] Smithsonian Natl Air & Space Museum, Space Hist Dept, Washington, DC USA. RP Neufeld, M (reprint author), Smithsonian Natl Air & Space Museum, Space Hist Dept, Washington, DC USA. NR 1 TC 0 Z9 0 U1 5 U2 10 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0031-9228 EI 1945-0699 J9 PHYS TODAY JI Phys. Today PD APR PY 2016 VL 69 IS 4 BP 41 EP 47 PG 7 WC Physics, Multidisciplinary SC Physics GA DL7YU UT WOS:000375857100021 ER PT J AU Baez, GP AF Baez, Gabriela Perez TI THE INTERDISCIPLINARY DOCUMENTATION OF THE FLORA OF LA VENTOSA AND ASSOCIATED LEXICON AND KNOWLEDGE: A PILOT FOR THE NATIONAL ETHNOBOTANICAL HERBARIUM ONLINE SO TAXON LA English DT Editorial Material C1 [Baez, Gabriela Perez] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. RP Baez, GP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD APR PY 2016 VL 65 IS 2 BP 425 EP 426 PG 2 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA DL7LZ UT WOS:000375823500057 ER PT J AU Wang, C Shih, CK Ren, D AF Wang Chen Shih Chungkun Ren Dong TI Three-Dimensional Reconstruction of Fossil Insects within Their Ecosystems SO ACTA GEOLOGICA SINICA-ENGLISH EDITION LA English DT Editorial Material C1 [Wang Chen; Shih Chungkun; Ren Dong] Capital Normal Univ, Coll Life Sci, Key Lab Insect Evolut & Environm Changes, Beijing 100048, Peoples R China. [Shih Chungkun] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Ren, D (reprint author), Capital Normal Univ, Coll Life Sci, Key Lab Insect Evolut & Environm Changes, Beijing 100048, Peoples R China. EM rendong@mail.cnu.edu.cn NR 0 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1000-9515 EI 1755-6724 J9 ACTA GEOL SIN-ENGL JI Acta Geol. Sin.-Engl. Ed. PD APR PY 2016 VL 90 IS 2 BP 771 EP 772 DI 10.1111/1755-6724.12713 PG 2 WC Geosciences, Multidisciplinary SC Geology GA DK1WL UT WOS:000374705600034 ER PT J AU Howard, JG Lynch, C Santymire, RM Marinari, PE Wildt, DE AF Howard, J. G. Lynch, C. Santymire, R. M. Marinari, P. E. Wildt, D. E. TI Recovery of gene diversity using long-term cryopreserved spermatozoa and artificial insemination in the endangered black-footed ferret SO ANIMAL CONSERVATION LA English DT Article DE black-footed ferret; reproduction; artificial insemination; cryopreserved sperm; gene diversity; genetic management ID MUSTELA-PUTORIUS-FURO; TAILED PRAIRIE DOG; CAPTIVE POPULATIONS; RESOURCE BANKS; NIGRIPES; CONSERVATION; STRATEGIES; EFFICACY; HEALTH AB One of the most significant challenges in the recovery of threatened species is the ability to maintain genetic diversity, avoid inbreeding and sustain population health and reproduction. Assisted reproductive techniques, including artificial insemination (AI), have been touted for decades as approaches that could contribute to the demographic and genetic management of rare species. Here, we report the first successful integration of AI with frozen semen into a formal recovery program and the positive impact on genetic diversity for the critically endangered black-footed ferret Mustela nigripes. Techniques developed in the taxonomically related domestic ferret Mustela putorius furo and Siberian polecat Mustela eversmannii were applied over time to selected black-footed ferrets, including semen banking from six of the last 18 survivors. After evaluation, processing and storage in liquid nitrogen (-196 degrees C/-321 degrees F), for as long as 20 years, sperm samples were thawed and transabdominally inseminated into the uterine horns of female conspecifics. Eight black-footed ferret offspring were produced using thawed sperm samples (including after two decades of cryopreservation) with inseminates containing as few as 3.4 x 10(6) motile spermatozoa. The incorporation of these offspring and/or their descendants into the ex situ breeding program prevented heterozygosity loss in the population and actually enhanced gene diversity (GD) significantly by 0.2% and lowered measures of inbreeding by 5.8%. This study demonstrates the utility and genetic diversity benefits of applying AI with cryopreserved spermatozoa 20 generations removed from the contemporary population for a wild animal revival program. C1 [Howard, J. G.; Santymire, R. M.; Marinari, P. E.; Wildt, D. E.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Lynch, C.] Riverbanks Zoo & Garden, Anim Care Dept, Columbia, SC USA. [Lynch, C.; Santymire, R. M.] Lincoln Pk Zoo, Conservat & Sci Dept, Chicago, IL USA. RP Wildt, DE (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. EM wildtd@si.edu NR 48 TC 9 Z9 9 U1 36 U2 51 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1367-9430 EI 1469-1795 J9 ANIM CONSERV JI Anim. Conserv. PD APR PY 2016 VL 19 IS 2 BP 102 EP 111 DI 10.1111/acv.12229 PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA DJ9WL UT WOS:000374563900002 ER PT J AU Wildt, DE Lynch, C Santymire, RM Marinari, PE AF Wildt, D. E. Lynch, C. Santymire, R. M. Marinari, P. E. TI Recovery of gene diversity using long-term cryopreserved spermatozoa and artificial insemination in the endangered black-footed ferret: response to commentaries SO ANIMAL CONSERVATION LA English DT Editorial Material ID GENOME RESOURCE BANKING; CONSERVATION C1 [Wildt, D. E.; Santymire, R. M.; Marinari, P. E.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Lynch, C.] Riverbanks Zoo & Garden, Dept Anim Care, Columbia, SC USA. [Lynch, C.; Santymire, R. M.] Lincoln Pk Zoo, Dept Conservat & Sci, Lincoln, IL USA. RP Wildt, DE (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. EM wildtd@si.edu NR 11 TC 1 Z9 1 U1 4 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1367-9430 EI 1469-1795 J9 ANIM CONSERV JI Anim. Conserv. PD APR PY 2016 VL 19 IS 2 BP 118 EP 119 DI 10.1111/acv.12277 PG 2 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA DJ9WL UT WOS:000374563900006 ER PT J AU Neale, PJ Thomas, BC AF Neale, Patrick J. Thomas, Brian C. TI Solar Irradiance Changes and Phytoplankton Productivity in Earth's Ocean Following Astrophysical Ionizing Radiation Events SO ASTROBIOLOGY LA English DT Article DE Algae; Photosynthesis; UV radiation; Supernovae; Radiative transfer ID GAMMA-RAY BURSTS; ULTRAVIOLET-RADIATION; OZONE DEPLETION; PHOTOSYNTHESIS; INHIBITION; SEA; TEMPERATURE; ABSORPTION; SUPERNOVAE; EXPOSURE AB Two atmospheric responses to simulated astrophysical ionizing radiation events significant to life on Earth are production of odd-nitrogen species, especially NO2, and subsequent depletion of stratospheric ozone. Ozone depletion increases incident short-wavelength ultraviolet radiation (UVB, 280-315nm) and longer (>600nm) wavelengths of photosynthetically available radiation (PAR, 400-700nm). On the other hand, the NO2 haze decreases atmospheric transmission in the long-wavelength UVA (315-400nm) and short-wavelength PAR. Here, we use the results of previous simulations of incident spectral irradiance following an ionizing radiation event to predict changes in terran productivity focusing on photosynthesis of marine phytoplankton. The prediction is based on a spectral model of photosynthetic response, which was developed for the dominant genera in central regions of the ocean (Synechococcus and Prochlorococcus), and on remote-sensing-based observations of spectral water transparency, temperature, wind speed, and mixed layer depth. Predicted productivity declined after a simulated ionizing event, but the effect integrated over the water column was small. For integrations taking into account the full depth range of PAR transmission (down to 0.1% of utilizable PAR), the decrease was at most 2-3% (depending on strain), with larger effects (5-7%) for integrations just to the depth of the surface mixed layer. The deeper integrations were most affected by the decreased utilizable PAR at depth due to the NO2 haze, whereas shallower integrations were most affected by the increased surface UV. Several factors tended to dampen the magnitude of productivity responses relative to increases in surface-damaging radiation, for example, most inhibition in the modeled strains is caused by UVA and PAR, and the greatest relative increase in damaging exposure is predicted to occur in the winter when UV and productivity are low. Astrobiology 16, 245-258. C1 [Neale, Patrick J.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. [Thomas, Brian C.] Washburn Univ, Dept Phys & Astron, Topeka, KS 66621 USA. RP Neale, PJ (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM nealep@si.edu OI Thomas, Brian/0000-0001-9091-0830 FU National Aeronautics and Space Administration [NNX09AM85G, NNX14AK22G] FX Dirk Aurin, NASA, for generously sharing his Matlab script for processing the QAA v6 algorithms. Cedric Fichot for assistance with attenuation coefficients. This work has been supported by the National Aeronautics and Space Administration under grant numbers NNX09AM85G and NNX14AK22G, through the Astrobiology: Exobiology and Evolutionary Biology Program. Computational time was provided by the High Performance Computing Environment (HiPACE) at Washburn University; thanks to Steve Black for assistance with computing resources. NR 44 TC 2 Z9 2 U1 2 U2 8 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD APR PY 2016 VL 16 IS 4 BP 245 EP 258 DI 10.1089/ast.2015.1360 PG 14 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA DK1CF UT WOS:000374649400001 PM 27027533 ER PT J AU Abdul-Masih, M Prsa, A Conroy, K Bloemen, S Boyajian, T Doyle, LR Johnston, C Kostov, V Latham, DW Matijevic, G Shporer, A Southworth, J AF Abdul-Masih, Michael Prsa, Andrej Conroy, Kyle Bloemen, Steven Boyajian, Tabetha Doyle, Laurance R. Johnston, Cole Kostov, Veselin Latham, David W. Matijevic, Gal Shporer, Avi Southworth, John TI KEPLER ECLIPSING BINARY STARS. VIII. IDENTIFICATION OF FALSE POSITIVE ECLIPSING BINARIES AND RE-EXTRACTION OF NEW LIGHT CURVES SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; catalogs; methods: analytical; methods: data analysis; methods: statistical; techniques: photometric ID DATA RELEASE; CATALOG; I. AB The Kepler mission has provided unprecedented, nearly continuous photometric data of similar to 200,000 objects in the similar to 105 deg(2) field of view (FOV) from the beginning of science operations in May of 2009 until the loss of the second reaction wheel in May of 2013. The Kepler Eclipsing Binary Catalog contains information including but not limited to ephemerides, stellar parameters, and analytical approximation fits for every known eclipsing binary system in the Kepler FOV. Using target pixel level data collected from Kepler in conjunction with the Kepler Eclipsing Binary Catalog, we identify false positives among eclipsing binaries, i.e., targets that are not eclipsing binaries themselves, but are instead contaminated by eclipsing binary sources nearby on the sky and show eclipsing binary signatures in their light curves. We present methods for identifying these false positives and for extracting new light curves for the true source of the observed binary signal. For each source, we extract three separate light curves for each quarter of available data by optimizing the signal-to-noise ratio, the relative percent eclipse depth, and the flux eclipse depth. We present 289 new eclipsing binaries in the Kepler FOV that were not targets for observation, and these have been added to the catalog. An online version of this catalog with downloadable content and visualization tools is maintained at http://keplerEBs.villanova.edu. C1 [Abdul-Masih, Michael; Prsa, Andrej; Johnston, Cole; Matijevic, Gal] Villanova Univ, Dept Astrophys & Planetary Sci, 800 E Lancaster, Villanova, PA 19085 USA. [Abdul-Masih, Michael] Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA. [Conroy, Kyle] Vanderbilt Univ, Dept Phys & Astron, VU Stn B 1807, Nashville, TN 37235 USA. [Bloemen, Steven] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Boyajian, Tabetha] Yale Univ, JW Gibbs Lab, 260 Whitney Ave, New Haven, CT 06511 USA. [Doyle, Laurance R.] Principia Coll, IMoP, Elsah, IL 62028 USA. [Doyle, Laurance R.] SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA. [Kostov, Veselin] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Latham, David W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Shporer, Avi] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Southworth, John] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. RP Abdul-Masih, M (reprint author), Villanova Univ, Dept Astrophys & Planetary Sci, 800 E Lancaster, Villanova, PA 19085 USA. OI Boyajian, Tabetha/0000-0001-9879-9313; Latham, David/0000-0001-9911-7388 FU NASA GO grant [14-K2GO1_2-0057]; Kepler mission via NASA [NNX13AB58A, NNX11AB99A]; Smithsonian Astrophysical Observatory; Theodore Dunham, Jr. Grant of the Fund for Astrophysical Research; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; NASAs Science Mission Directorate FX We gratefully acknowledge support from NASA GO grant 14-K2GO1_2-0057. D.W.L. gratefully acknowledges support from the Kepler mission via NASA Cooperative Agreements NNX13AB58A and NNX11AB99A with the Smithsonian Astrophysical Observatory. The high-performance computational facility used for this work was sponsored in part by the Theodore Dunham, Jr. Grant of the Fund for Astrophysical Research. All of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-Hubble Space Telescope data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. Funding for this Discovery Mission is provided by NASAs Science Mission Directorate. NR 17 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD APR PY 2016 VL 151 IS 4 AR 101 DI 10.3847/0004-6256/151/4/101 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL4LV UT WOS:000375609100014 ER PT J AU Crespo, NA Massaro, F Milisavljevic, D Landoni, M Chavushyan, V Patino-Alvarez, V Masetti, N Jimenez-Bailon, E Strader, J Chomiuk, L Katagiri, H Kagaya, M Cheung, CC Paggi, A D'Abrusco, R Ricci, F La Franca, F Smith, HA Tosti, G AF Crespo, N. Alvarez Massaro, F. Milisavljevic, D. Landoni, M. Chavushyan, V. Patino-Alvarez, V. Masetti, N. Jimenez-Bailon, E. Strader, J. Chomiuk, L. Katagiri, H. Kagaya, M. Cheung, C. C. Paggi, A. D'Abrusco, R. Ricci, F. La Franca, F. Smith, Howard A. Tosti, G. TI OPTICAL SPECTROSCOPIC OBSERVATIONS OF GAMMA-RAY BLAZAR CANDIDATES. VI. FURTHER OBSERVATIONS FROM TNG, WHT, OAN, SOAR, AND MAGELLAN TELESCOPES SO ASTRONOMICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; galaxies: active; quasars: general; radiation mechanisms: non-thermal ID ALL-SKY SURVEY; ACTIVE GALACTIC NUCLEI; RADIO-SOURCES; SOURCE CATALOG; SAMPLE; COUNTERPARTS; EMISSION; OBJECTS; GHZ; MHZ AB Blazars, one of the most extreme classes of active galaxies, constitute so far the largest known population of.-ray sources, and their number is continuously growing in the Fermi catalogs. However, in the latest release of the Fermi catalog there is still a large fraction of sources that are classified as blazar candidates of uncertain type (BCUs) for which optical spectroscopic observations are necessary to confirm their nature and their associations. In addition, about one-third of the gamma-ray point sources listed in the Third Fermi-LAT Source Catalog (3FGL) are still unassociated and lacking an assigned lower-energy counterpart. Since 2012 we have been carrying out an optical spectroscopic campaign to observe blazar candidates to confirm their nature. In this paper, the sixth of the series, we present optical spectroscopic observations for 30 gamma-ray blazar candidates from different observing programs we carried out with the Telescopio Nazionale Galileo, William Herschel Telescope, Observatorio Astronomico Nacional, Southern Astrophysical Research Telescope, and Magellan. Telescopes. We found that 21 out of 30 sources investigated are BL Lac objects, while the remaining targets are classified as flat-spectrum radio quasars showing the typical broad emission lines of normal quasi-stellar objects. We conclude that our selection of gamma-ray blazar. candidates based on their multifrequency properties continues to be a successful way to discover potential low-energy counterparts of the Fermi. unidentified gamma-ray sources and to confirm the nature of BCUs. C1 [Crespo, N. Alvarez; Massaro, F.] Univ Turin, Dipartimento Fis, Via Pietro Giuria 1, I-10125 Turin, Italy. [Crespo, N. Alvarez; Massaro, F.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Milisavljevic, D.; Paggi, A.; Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Landoni, M.] INAF Osservatorio Astron Brera, Via Emilio Bianchi 46, I-23807 Merate, Italy. [Chavushyan, V.; Patino-Alvarez, V.] Inst Nacl Astrofis Opt & Electr, Apartado Postal 51-216, Puebla 72000, Mexico. [Masetti, N.] INAF Ist Astrofis Spaziale & Fis Cosm Bologna, Via Gobetti 101, I-40129 Bologna, Italy. [Masetti, N.] Univ Andres Bello, Dept Ciencias Fis, Fernandez Concha 700, Santiago, Chile. [Jimenez-Bailon, E.] Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 877, Ensenada 22800, Baja California, Mexico. [Strader, J.; Chomiuk, L.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Katagiri, H.; Kagaya, M.] Ibaraki Univ, Coll Sci, 2-1-1 Bunkyo, Mito, Ibaraki 3108512, Japan. [Cheung, C. C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [D'Abrusco, R.] Univ Naples Federico II, Dept Phys Sci, Via Cinthia 9, I-80126 Naples, Italy. [Ricci, F.; La Franca, F.] Univ Rome Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy. [Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. RP Crespo, NA (reprint author), Univ Turin, Dipartimento Fis, Via Pietro Giuria 1, I-10125 Turin, Italy. RI D'Abrusco, Raffaele/L-2767-2016; Massaro, Francesco/L-9102-2016; Paggi, Alessandro/C-1219-2017; OI D'Abrusco, Raffaele/0000-0003-3073-0605; Massaro, Francesco/0000-0002-1704-9850; Paggi, Alessandro/0000-0002-5646-2410; Ricci, Federica/0000-0001-5742-5980; La Franca, Fabio/0000-0002-1239-2721 FU NASA [NNX12AO97G, NNX13AP20G, NNX14AJ61G, DPR S-15633-Y]; NASA/JPL grant [RSA 1369566]; ASI/INAF contract [I/005/12/0]; CONACyT (Mexico) [151494]; Packard Foundation; National Aeronautics and Space Administration; National Science Foundation; Australian Research Council; Science Foundation for Physics within the University of Sydney; 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 We thank the anonymous referee for useful comments that led to improvements in the paper. We are grateful to Dr. Mendez Alvarez, Dr. Dominguez, Dr. Karjalainen, Dr. Riddick, Dr. Skillen at WHT, and Dr. Boschin at TNG for their help in. scheduling, preparing,. and performing the observations. This investigation is supported by. NASA grants NNX12AO97G, NNX13AP20G, and NNX14AJ61G. H.A.S. acknowledges partial support from NASA/JPL grant RSA 1369566. The work by G.T. is supported by the ASI/INAF contract I/005/12/0. V.C. and V.P.-A. are supported by the CONACyT research grant 151494 (Mexico). Work by C.C.C. at NRL is supported in part by NASA DPR S-15633-Y. J.S. is supported by a Packard Foundation Fellowship.r Based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministerio da Ciencia, Tecnologia, e Inovacao (MCTI) ada Republica Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). Part of this work is based on archival data, software, or online services provided by the ASI Science Data Center. This research has made use of data obtained from the high-energy Astrophysics Science Archive Research Center (HEASARC) provided by NASA's Goddard Space Flight Center; the SIMBAD database operated at CDS, Strasbourg, France; and. the NASA/IPAC Extragalactic Database (NED), operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Part of this work is based on the NVSS (NRAO VLA Sky Survey): The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under contract with the National Science Foundation and on the VLA low-frequency Sky Survey (VLSS). The Molonglo Observatory site manager, Duncan Campbell-Wilson, and the staff, Jeff Webb, Michael White, and John Barry, are responsible for the smooth operation of Molonglo Observatory Synthesis Telescope (MOST) and the day-to-day observing program of SUMSS. The SUMSS survey is dedicated to Michael Large, whose expertise and vision made the project possible. The MOST is operated by the School of Physics with the support of the Australian Research Council and the Science Foundation for Physics within the University of Sydney. 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 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 USNOFS Image and Catalogue Archive operated by the United States Naval Observatory, Flagstaff Station (http://www.nofs.navy.mil/data/fchpix/). 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/.; r 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. The WENSS project was a collaboration between the Netherlands Foundation for Research in Astronomy and the Leiden Observatory. We acknowledge the WENSS team,. which consisted of Ger de Bruyn, Yuan Tang, Roeland Rengelink, George Miley, Huub Rottgering, Malcolm Bremer, Martin Bremer, Wim Brouw, Ernst Raimond, and David Fullagar, for the extensive work aimed at producing the WENSS catalog, and. TOPCAT16 (Taylor 2005) for the preparation and manipulation of the tabular data and the images. The Aladin Java applet17 was used to create the finding charts reported in this paper (Bonnarel et al. 2000). It can be started from the CDS (Strasbourg-France), from the CFA (Harvard-USA), from the ADAC (Tokyo-Japan), from the IUCAA (Pune-India), from the UKADC (Cambridge-UK), or from the CADC (Victoria-Canada).r The Molonglo Observatory site manager, Duncan Campbell-Wilson, and the staff, Jeff Webb, Michael White and John Barry, are responsible for the smooth operation of Molonglo Observatory Synthesis Telescope (MOST) and the day-to-day observing programme of SUMSS. The SUMSS survey is dedicated to Michael Large whose expertise and vision made the project possible. The MOST is operated by the School of Physics with the support of the Australian Research Council and the Science Foundation for Physics within the University of Sydney. NR 53 TC 5 Z9 5 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD APR PY 2016 VL 151 IS 4 AR 95 DI 10.3847/0004-6256/151/4/95 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL4LV UT WOS:000375609100008 ER PT J AU Evans, NR Pillitteri, I Wolk, S Karovska, M Tingle, E Guinan, E Engle, S Bond, HE Schaefer, GH Mason, BD AF Evans, Nancy Remage Pillitteri, Ignazio Wolk, Scott Karovska, Margarita Tingle, Evan Guinan, Edward Engle, Scott Bond, Howard E. Schaefer, Gail H. Mason, Brian D. TI RESOLVED COMPANIONS OF CEPHEIDS: TESTING THE CANDIDATES WITH X-RAY OBSERVATIONS SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; stars: formation; stars: massive; stars: variables: Cepheids ID COUNTING DETECTOR IMAGES; WAVELET TRANSFORMS; MASSIVE STARS; BINARY STARS; ALPHA-PERSEI; OPEN CLUSTER; S-MUSCAE; MULTIPLICITY; EVOLUTION; POLARIS AB We have made XMM-Newton observations of 14 Galactic Cepheids that have candidate resolved (>= 5") companion stars based on our earlier HST Wide Field Camera 3 (WFC3) imaging survey. Main-sequence stars that are young enough to be physical companions of Cepheids are expected to be strong X-ray producers in contrast to field stars. XMM-Newton exposures were set to detect essentially all companions hotter than spectral type M0 (corresponding to 0.5 M-circle dot). The large majority of our candidate companions were not detected in X-rays, and hence are not confirmed as young companions. One resolved candidate (S Nor #4) was unambiguously detected, but the Cepheid is a member of a populous cluster. For this reason, it is likely that S. Nor #4 is a cluster member rather than a gravitationally bound companion. Two further Cepheids (S Mus and R Cru) have X-ray emission that might be produced by either the Cepheid or the candidate resolved companion. A subsequent Chandra observation of S Mus shows that the X-rays are at the location of the Cepheid/spectroscopic binary. R Cru and also V659 Cen (also X-ray bright) have possible companions closer than 5" (the limit for this study) which are the likely sources of X-rays. One final X-ray detection (V473 Lyr) has no known optical companion, so the prime suspect is the Cepheid itself. It is a unique Cepheid with a variable amplitude. The 14 stars that we observed with XMM constitute 36% of the 39 Cepheids found to have candidate companions in our HST/WFC3 optical survey. No young probable binary companions were found with separations of >= 5" or 4000 au. C1 [Evans, Nancy Remage; Pillitteri, Ignazio; Wolk, Scott; Karovska, Margarita; Tingle, Evan] Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA. [Pillitteri, Ignazio] INAF Osservatorio Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy. [Guinan, Edward; Engle, Scott] Villanova Univ, Dept Astron & Astrophys, 800 Lancaster Ave, Villanova, PA 19085 USA. [Bond, Howard E.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Bond, Howard E.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Schaefer, Gail H.] Georgia State Univ, CHARA Array, Mt Wilson, CA 91023 USA. [Mason, Brian D.] US Naval Observ, 3450 Massachusetts Ave NW, Washington, DC 20392 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA.; Bond, HE (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.; Bond, HE (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.; Schaefer, GH (reprint author), Georgia State Univ, CHARA Array, Mt Wilson, CA 91023 USA. EM nevans@cfa.harvard.edu; heb11@psu.edu; schaefer@chara-array.org RI Pillitteri, Ignazio/L-1549-2016; OI Pillitteri, Ignazio/0000-0003-4948-6550; Wolk, Scott/0000-0002-0826-9261 FU Chandra X-ray Center NASA Contract [NAS8-03060]; [HST GO-13369.001-A] FX Support for this work was also provided from the Chandra X-ray Center NASA Contract NAS8-03060. Funding was provided from HST GO-13369.001-A (to NRE and IP). Vizier and SIMBAD were used in the preparation of this study. Comments from an anonymous referee improved the clarity of the presentation. NR 34 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD APR PY 2016 VL 151 IS 4 AR 108 DI 10.3847/0004-6256/151/4/108 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DL4LV UT WOS:000375609100021 ER PT J AU Albornoz, FE Lambers, H Turner, BL Teste, FP Laliberte, E AF Albornoz, Felipe E. Lambers, Hans Turner, Benjamin L. Teste, Francois P. Laliberte, Etienne TI Shifts in symbiotic associations in plants capable of forming multiple root symbioses across a long-term soil chronosequence SO ECOLOGY AND EVOLUTION LA English DT Article DE Arbuscular mycorrhizal fungi; chronosequence; ectomycorrhizal fungi; nitrogen fixation; pedogenesis; phosphorus; rhizobia ID ARBUSCULAR-MYCORRHIZAL FUNGI; 2-MILLION-YEAR DUNE CHRONOSEQUENCE; NUTRIENT-ACQUISITION STRATEGIES; ECTOMYCORRHIZAL FUNGI; NITROGEN-FIXATION; PHOSPHORUS UPTAKE; ORGANIC MATERIAL; SALIX REPENS; HOST-PLANT; GROWTH AB Changes in soil nutrient availability during long-term ecosystem development influence the relative abundances of plant species with different nutrient-acquisition strategies. These changes in strategies are observed at the community level, but whether they also occur within individual species remains unknown. Plant species forming multiple root symbioses with arbuscular mycorrhizal (AM) fungi, ectomycorrhizal (ECM) fungi, and nitrogen-(N) fixing microorganisms provide valuable model systems to examine edaphic controls on symbioses related to nutrient acquisition, while simultaneously controlling for plant host identity. We grew two co-occurring species, Acacia rostellifera (N-2-fixing and dual AM and ECM symbioses) and Melaleuca systena (AM and ECM dual symbioses), in three soils of contrasting ages (c. 0.1, 1, and 120 ka) collected along a long-term dune chronosequence in southwestern Australia. The soils differ in the type and strength of nutrient limitation, with primary productivity being limited by N (0.1 ka), co-limited by N and phosphorus (P) (1 ka), and by P (120 ka). We hypothesized that (i) within-species root colonization shifts from AM to ECM with increasing soil age, and that (ii) nodulation declines with increasing soil age, reflecting the shift from N to P limitation along the chronosequence. In both species, we observed a shift from AM to ECM root colonization with increasing soil age. In addition, nodulation in A. rostellifera declined with increasing soil age, consistent with a shift from N to P limitation. Shifts from AM to ECM root colonization reflect strengthening P limitation and an increasing proportion of total soil P in organic forms in older soils. This might occur because ECM fungi can access organic P via extracellular phosphatases, while AM fungi do not use organic P. Our results show that plants can shift their resource allocation to different root symbionts depending on nutrient availability during ecosystem development. C1 [Albornoz, Felipe E.; Lambers, Hans; Turner, Benjamin L.; Teste, Francois P.; Laliberte, Etienne] Univ Western Australia, Sch Plant Biol, 35 Stirling Highway, Perth, WA 6009, Australia. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. [Teste, Francois P.] IMASL CONICET, Grp Estudios Ambientales, Av Ejercito Andes 950, RA-5700 San Luis, Argentina. [Teste, Francois P.] Univ Nacl San Luis, Av Ejercito Andes 950, RA-5700 San Luis, Argentina. [Laliberte, Etienne] Univ Montreal, Inst Rech Biol Vegetale, Dept Sci Biol, 4101 Sherbrooke Est, Montreal, PQ H1X 2B2, Canada. RP Albornoz, FE (reprint author), Univ Western Australia, Sch Plant Biol, 35 Stirling Highway, Perth, WA 6009, Australia. EM felipe.albornozramirez@research.uwa.edu.au RI Turner, Benjamin/E-5940-2011; Laliberte, Etienne/B-6855-2008; Lambers, Hans/A-1544-2008 OI Turner, Benjamin/0000-0002-6585-0722; Laliberte, Etienne/0000-0002-3167-2622; Lambers, Hans/0000-0002-4118-2272 FU Australian Research Council (ARC) [DE120100352, DP0985685]; UWA; Chilean Government; ANZ Holsworth Wildlife Research Endowment; University of Western Australia FX Funding was provided by the Australian Research Council (ARC) through a DECRA (DE120100352) to EL and a Discovery Project (DP0985685) to HL and a UWA Research and Development Award granted to FPT. We also acknowledge financial support to FA through the "Becas Chile" scholarship from the Chilean Government, the ANZ Holsworth Wildlife Research Endowment, and the University of Western Australia. NR 79 TC 1 Z9 1 U1 16 U2 38 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 2016 VL 6 IS 8 BP 2368 EP 2377 DI 10.1002/ece3.2000 PG 10 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA DJ9YD UT WOS:000374568300011 PM 27066229 ER PT J AU Sheets, EA Cohen, CS Ruiz, GM Da Rocha, RM AF Sheets, Elizabeth A. Cohen, C. Sarah Ruiz, Gregory M. Da Rocha, Rosana M. TI Investigating the widespread introduction of a tropical marine fouling species SO ECOLOGY AND EVOLUTION LA English DT Article DE Ascidian; biological introduction; Botrylloides nigrum; chimerism; Panama Canal; population genetics ID ASCIDIAN BOTRYLLUS-SCHLOSSERI; BIOLOGICAL INVASIONS; POPULATION-GENETICS; CIONA-INTESTINALIS; MITOCHONDRIAL-DNA; MEDITERRANEAN COAST; STATISTICAL-METHOD; DIDEMNUM-VEXILLUM; SHIP MOVEMENTS; NORTH-AMERICA AB Little is known about the number and rate of introductions into terrestrial and marine tropical regions, and if introduction patterns and processes differ from temperate latitudes. Botryllid ascidians (marine invertebrate chordates) are an interesting group to study such introduction differences because several congeners have established populations across latitudes. While temperate botryllid invasions have been repeatedly highlighted, the global spread of tropical Botrylloides nigrum (Herdman, 1886) has been largely ignored. We sampled B. nigrum from 16 worldwide warm water locations, including around the Panama Canal, one of the largest shipping hubs in the world and a possible introduction corridor. Using mitochondrial (COI) and nuclear (ANT) markers, we discovered a single species with low genetic divergence and diversity that has established in the Atlantic, Pacific, Indo-Pacific, and Mediterranean Oceans. The Atlantic Ocean contained the highest diversity and multilocus theta estimates and may be a source for introductions to other regions. A high frequency of one mitochondrial haplotype was detected in Pacific populations that may represent a recent introduction in this region. In comparison to temperate relatives, B. nigrum displayed lower (but similar to temperate Botrylloides violaceus) genetic divergence and diversity at both loci that may represent a more recent global spread or differences in introduction pressures in tropical regions. Additionally, chimeras (genetically distinct individuals sharing a single body) were detected in three populations by the mitochondrial locus and validated using cloning, and these individuals contained new haplotype diversity not detected in any other colonies. C1 [Sheets, Elizabeth A.; Cohen, C. Sarah] San Francisco State Univ, Dept Biol, Romberg Tiburon Ctr Environm Studies, 3150 Paradise Dr, Tiburon, CA 94920 USA. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, 627 Contees Wharf Rd, Edgewater, MD 21037 USA. [Da Rocha, Rosana M.] Univ Fed Parana, Dept Zool, CP 19020, BR-81531980 Curitiba, Parana, Brazil. RP Cohen, CS (reprint author), San Francisco State Univ, Dept Biol, Romberg Tiburon Ctr Environm Studies, 3150 Paradise Dr, Tiburon, CA 94920 USA. EM sarahcoh@sfsu.edu OI Ruiz, Gregory/0000-0003-2499-441X FU National Science Foundation [FSML 0435033]; Brazilian National Council for Scientific and Technological Development [CNPq 200914/2008-1] FX National Science Foundation, (Grant/Award Number: FSML 0435033) Brazilian National Council for Scientific and Technological Development, (Grant/Award Number: CNPq 200914/2008-1). NR 112 TC 2 Z9 2 U1 11 U2 18 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 2016 VL 6 IS 8 BP 2453 EP 2471 DI 10.1002/ece3.2065 PG 19 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA DJ9YD UT WOS:000374568300018 PM 27066231 ER PT J AU Zhao, JL Xia, YM Cannon, CH Kress, WJ Li, QJ AF Zhao, Jian-Li Xia, Yong-Mei Cannon, Charles H. Kress, W. John Li, Qing-Jun TI Evolutionary diversification of alpine ginger reflects the early uplift of the Himalayan-Tibetan Plateau and rapid extrusion of Indochina SO GONDWANA RESEARCH LA English DT Article DE The late Eocene; The early Oligocene; The Oligocene/Miocene boundary; Alpine ginger; Roscoea ID DISPERSAL-VICARIANCE ANALYSIS; MULTIPLE SEQUENCE ALIGNMENT; MAXIMUM-LIKELIHOOD; AILAO SHAN; HISTORICAL BIOGEOGRAPHY; PHYLOGENETIC NETWORKS; DNA POLYMORPHISM; CHLOROPLAST DNA; BANANA FAMILY; MIXED MODELS AB The evolutionary diversifications of many taxonomic groups, especially those with limited dispersal ability, are often driven by key geological events, such as tectonic drift, continental collisions, and uplifts of mountains. Here, we use full range geographic sampling to create a dated molecular phylogeny for two genera of alpine gingers (Cautleya and Roscoea) in the Pan-Himalaya, and test the correlations between evolutionary diversification of this group and major geological events in the studied region. Our results revealed that the origination of their common ancestor and evolutionary split between the two genera occurred during the middle Eocene and the late Eocene to the early Oligocene, corresponding well to the proposed two early uplifts of the Himalayan-Tibetan Plateau. Roscoea species, the highest elevation gingers known, were then divided into distinct Himalayan and Indochinese clades, simultaneous with the rapid extrusion of Indochina and accompanied by the third Himalayan uplift around the Oligocene/Miocene boundary. This study highlights the importance of evolutionary diversification of plants as an independent line of evidence to reflect tectonic events in the Himalayan Indochinese region. (C) 2015 The Authors. Published by Elsevier B.V. on behalf of International Association for Gondwana Research. This is an open access article under the CC BY-NC-ND license (http://creativecommons.org/licenses/by-nc-nd/4.0/). C1 [Zhao, Jian-Li; Xia, Yong-Mei; Cannon, Charles H.; Kress, W. John; Li, Qing-Jun] Chinese Acad Sci, Key Lab Trop Forest Ecol, Xishuangbanna Trop Bot Garden, Mengla 666303, Yunnan, Peoples R China. [Cannon, Charles H.] Texas Tech Univ, Dept Biol Sci, Box 43131,Flint & Main St, Lubbock, TX 79409 USA. [Kress, W. John] Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, MRC-166,POB 7012, Washington, DC 20013 USA. RP Li, QJ (reprint author), Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Mengla 666303, Yunnan, Peoples R China. EM qjli@xtbg.ac.cn FU National Natural Science Foundation of China [U1202261]; National Basic Research Program of China (973 Program) [2007CB411603]; CAS [XTBG-T01, F01] FX We thank Ram P. Chaudhary and Mohandass Dharmalingam for sampling in Nepal; Laboratory of Plant Phylogenetics and Conservation, Xishuangbanna Tropical Botanical Garden, Chinese Academy of Sciences for part lab work; Jianquan Liu and Kangshan Mao at Sichuan University for critical comments on the manuscript; Yong-Li Fan at Xishuangbanna Tropical Botanical Garden, Chinese Academy of Sciences for providing plant photographs; and CIPRES Science Gateway for computation resources. We also thank Robert E. Ricklefs, University of Missouri at St. Louis; David Woodruff, UC San Diego; An Yin, University of California at Los Angeles; Paul Tapponnier, Nanyan Technological University, Singapore; and Kendrick L. Marr, Royal British Columbia Museum, Canada; Jun Wen, Smithsonian Institution, for their comments and suggestions. This research was supported by the National Natural Science Foundation of China (U1202261), the National Basic Research Program of China (973 Program No. 2007CB411603), and the CAS 135 Program (XTBG-T01, F01). NR 83 TC 3 Z9 3 U1 7 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1342-937X EI 1878-0571 J9 GONDWANA RES JI Gondwana Res. PD APR PY 2016 VL 32 BP 232 EP 241 DI 10.1016/j.gr.2015.02.004 PG 10 WC Geosciences, Multidisciplinary SC Geology GA DJ7WY UT WOS:000374425100015 ER PT J AU Ball, T Chandler-Ezell, K Dickau, R Duncan, N Hart, TC Iriarte, J Lentfer, C Logan, A Lu, HY Madella, M Pearsall, DM Piperno, DR Rosen, AM Vrydaghs, L Weisskopf, A Zhang, JP AF Ball, Terry Chandler-Ezell, Karol Dickau, Ruth Duncan, Neil Hart, Thomas C. Iriarte, Jose Lentfer, Carol Logan, Amanda Lu, Houyuan Madella, Marco Pearsall, Deborah M. Piperno, Dolores R. Rosen, Arlene M. Vrydaghs, Luc Weisskopf, Alison Zhang, Jianping TI Phytoliths as a tool for investigations of agricultural origins and dispersals around the world SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Phytoliths; Crop plants; Diagnostic criteria ID MAIZE ZEA-MAYS; DIAGNOSTIC OPAL PHYTOLITHS; WHEAT TRITICUM-MONOCOCCUM; MILLET PANICUM-MILIACEUM; ORYZA-SATIVA POACEAE; BALSAS RIVER VALLEY; STARCH GRAINS; INFLORESCENCE PHYTOLITHS; REPRODUCTIVE STRUCTURES; NEOLITHIC CATALHOYUK AB Agricultural origins and dispersals are subjects of fundamental importance to archaeology as well as many other scholarly disciplines. These investigations are world-wide in scope and require significant amounts of paleobotanical data attesting to the exploitation of wild progenitors of crop plants and subsequent domestication and spread. Accordingly, for the past few decades the development of methods for identifying the remains of wild and domesticated plant species has been a focus of paleoethnobotany. Phytolith analysis has increasingly taken its place as an important independent contributor of data in all areas of the globe, and the volume of literature on the subject is now both very substantial and disseminated in a range of international journals. In this paper, experts who have carried out the hands-on work review the utility and importance of phytolith analysis in documenting the domestication and dispersals of crop plants around the world. It will serve as an important resource both to paleoethnobotanists and other scholars interested in the development and spread of agriculture. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Ball, Terry] Brigham Young Univ, Provo, UT 84602 USA. [Chandler-Ezell, Karol] Stephen F Austin State Univ, Dept Social & Cultural Anal, SFA Stn, LAN 351,POB 13047, Nacogdoches, TX 75962 USA. [Dickau, Ruth] HD Analyt Solut, 952 Oxford St West, London, ON N6H 1V3, Canada. [Duncan, Neil] Univ Cent Florida, Dept Anthropol, Orlando, FL 32816 USA. [Hart, Thomas C.] Univ Texas Austin, Dept Anthropol, Environm Archaeol Lab, Austin, TX 78712 USA. [Iriarte, Jose] Univ Exeter, Dept Archaeol, Exeter EX4 4QJ, Devon, England. [Lentfer, Carol] Univ Queensland, Sch Social Sci, Brisbane St Lucia, Qld 4072, Australia. [Lentfer, Carol] Univ Liege, Dept Sci Hist, Australia & Serv Prehist, B-4000 Liege, Belgium. [Logan, Amanda] Northwestern Univ, Dept Anthropol, Evanston, IL 60208 USA. [Lu, Houyuan; Zhang, Jianping] Chinese Acad Sci, Inst Geol & Geophys, Key Lab Cenozo Geol & Environm, Beijing 100029, Peoples R China. [Madella, Marco] Univ Pompeu Fabra, CaSEs Res Grp, ICREA, Barcelona, Spain. [Madella, Marco] IMF CSIC, Barcelona, Spain. [Pearsall, Deborah M.] Univ Missouri, Columbia, MO 65211 USA. [Piperno, Dolores R.] Smithsonian Trop Res Inst, Panama City, Panama. [Piperno, Dolores R.] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Washington, DC USA. [Rosen, Arlene M.] Univ Texas Austin, Dept Anthropol, Austin, TX 78712 USA. [Vrydaghs, Luc] Univ Libre Bruxelles, Ctr Rech Archeol & Patrimoine, Brussels, Belgium. [Vrydaghs, Luc] Res Team Archaeo & Paleoenvironm Sci, Brussels, Belgium. [Weisskopf, Alison] UCL, Inst Archaeol, London, England. RP Piperno, DR (reprint author), Smithsonian Trop Res Inst, Panama City, Panama.; Piperno, DR (reprint author), Smithsonian Natl Museum Nat Hist, Dept Anthropol, Washington, DC USA. EM pipernod@si.edu OI Iriarte, Jose/0000-0002-8155-5360 NR 150 TC 7 Z9 7 U1 15 U2 21 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 2016 VL 68 BP 32 EP 45 DI 10.1016/j.jas.2015.08.010 PG 14 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA DL7LX UT WOS:000375823300005 ER PT J AU Piperno, DR AF Piperno, Dolores R. TI Phytolith radiocarbon dating in archaeological and paleoecological research: a case study of phytoliths from modern Neotropical plants and a review of the previous dating evidence SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Review DE Carbon 14 phytolith dating; Modern plants; Archaeological and paleoecological; phytolith dates ID CARBON-ISOTOPE SIGNATURES; COASTAL ECUADOR; OCCLUDED CARBON; CLIMATE-CHANGE; VEGETATION; RECONSTRUCTION; ADAPTATION; DYNAMICS; POLLEN; SOILS AB Recent carbon-14 studies of phytoliths from modern plants collected from extra-tropical regions of the world have yielded dates that are too old by several hundred to thousands of years. These findings have prompted questions about the suitability of phytolith-derived carbon for dating in archaeological and paleo-environmental research. In this paper, phytolith C-14 ages are determined from a number of modern Neotropical plant taxa collected between 1964 and 2013. The specimens studied are maize (Zea mays L.), two squash species (Cucurbita ecuadorensis H.C.Cutler & Whitaker and C ficifolia Bouche), and two trees common in Neotropical forest, Hirtella americana L. and Socratea durissima (Oersted) H. Uendl. They represent families, genera, and species that are well-represented in Neotropical archaeological and paleoecological sediments. Every phytolith sample returned a post-bomb C-14 phytolith age reflecting collection after 1955, with the exception of a herbarium specimen that was treated with chemicals containing radiocarbon-dead carbon. The phytolith dates do not indicate a source of extraneous old or young carbon occurring on the surfaces or inside of phytoliths that bias their ages. Such findings are also reflected by previous phytolith C-14 studies of ancient Neotropical sites. Possible reasons for the differences in results between these and other studies and varying interpretations of soil and sediment phytolith C-14 analyses by different investigators are discussed. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Piperno, Dolores R.] Smithsonian Trop Res Inst, Balboa, Panama. [Piperno, Dolores R.] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Washington, DC USA. RP Piperno, DR (reprint author), Smithsonian Trop Res Inst, Balboa, Panama.; Piperno, DR (reprint author), Smithsonian Natl Museum Nat Hist, Dept Anthropol, Washington, DC USA. EM pipernod@si.edu FU Small Grant award from the Smithsonian National Museum of Natural History, Washington; Smithsonian Tropical Research Institute, Panama FX Supported by a Small Grant award from the Smithsonian National Museum of Natural History, Washington and the Smithsonian Tropical Research Institute, Panama. I thank Thomas Hart for the invitation to participate in this special issue. NR 38 TC 7 Z9 7 U1 5 U2 11 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 2016 VL 68 BP 54 EP 61 DI 10.1016/j.jas.2015.06.002 PG 8 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA DL7LX UT WOS:000375823300007 ER PT J AU Zapico, SC Ubelaker, DH AF Zapico, Sara C. Ubelaker, Douglas H. TI Relationship Between Mitochondrial DNA Mutations and Aging. Estimation of Age-at-death SO JOURNALS OF GERONTOLOGY SERIES A-BIOLOGICAL SCIENCES AND MEDICAL SCIENCES LA English DT Article DE Age; Free radicals; mtDNA mutations; HV2; Dentin ID ASPARTIC-ACID RACEMIZATION; TOOTH CEMENTUM ANNULATION; CHRONOLOGICAL AGE; OXIDATIVE STRESS; 4977-BP DELETION; SKELETAL-MUSCLE; MTDNA; DAMAGE; QUANTIFICATION; ACCUMULATION AB Some studies have pointed to the relationship between mitochondrial DNA ( mtDNA) mutations and age in different tissues, which are potentially interesting in aging research and in forensic identification because they could help to improve the estimation of age-at-death. The present study aims to evaluate the mutations in mtDNA from dentin and pulp and their relation with age. Healthy erupted third molars were extracted from individuals from two Spanish populations, aged 20-70. When analyzing the amplification of hypervariable region 2 of the mtDNA by real-time polymerase chain reaction, a negative strong linear correlation was found between the mtDNA amplification and age in dentin from both populations. In contrast, a significant correlation between mtDNA amplification and age in pulp was not discovered, probably due to the majority of the mitochondria are placed in dentin. A difference in mtDNA damage between these two populations was also detected, indicating the role of ancestry as a component. The findings from this research enrich the current studies related to aging and mitochondrial damage and provide a new quantitative tool for estimating the age-at-death that, in combination with traditional age markers, could improve identification accuracy in forensic cases. C1 [Zapico, Sara C.; Ubelaker, Douglas H.] Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, MRC 112,10th & Constitut Ave,NW,POB 37012, Washington, DC 20013 USA. RP Zapico, SC (reprint author), Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, MRC 112,10th & Constitut Ave,NW,POB 37012, Washington, DC 20013 USA. EM saiczapico@gmail.com FU Smithsonian Institution FX This work was supported by Peter Buck Award postdoctoral fellowship from Smithsonian Institution. NR 38 TC 0 Z9 0 U1 6 U2 7 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1079-5006 EI 1758-535X J9 J GERONTOL A-BIOL JI J. Gerontol. Ser. A-Biol. Sci. Med. Sci. PD APR PY 2016 VL 71 IS 4 BP 445 EP 450 DI 10.1093/gerona/glv115 PG 6 WC Geriatrics & Gerontology; Gerontology SC Geriatrics & Gerontology GA DJ4ZA UT WOS:000374215400005 PM 26286606 ER PT J AU Osuri, AM Ratnam, J Varma, V Alvarez-Loayza, P Astaiza, JH Bradford, M Fletcher, C Ndoundou-Hockemba, M Jansen, PA Kenfack, D Marshall, AR Ramesh, BR Rovero, F Sankaran, M AF Osuri, Anand M. Ratnam, Jayashree Varma, Varun Alvarez-Loayza, Patricia Hurtado Astaiza, Johanna Bradford, Matt Fletcher, Christine Ndoundou-Hockemba, Mireille Jansen, Patrick A. Kenfack, David Marshall, Andrew R. Ramesh, B. R. Rovero, Francesco Sankaran, Mahesh TI Contrasting effects of defaunation on aboveground carbon storage across the global tropics SO NATURE COMMUNICATIONS LA English DT Article ID FOREST BIOMASS; ATLANTIC FOREST; TREE RECRUITMENT; SEED DISPERSAL; WOOD DENSITY; CONSEQUENCES; BUSHMEAT; ANTHROPOCENE; REGENERATION; WORLDWIDE AB Defaunation is causing declines of large-seeded animal-dispersed trees in tropical forests worldwide, but whether and how these declines will affect carbon storage across this biome is unclear. Here we show, using a pan-tropical data set, that simulated declines of large-seeded animal-dispersed trees have contrasting effects on aboveground carbon stocks across Earth's tropical forests. In our simulations, African, American and South Asian forests, which have high proportions of animal-dispersed species, consistently show carbon losses (2-12%), but Southeast Asian and Australian forests, where there are more abiotically dispersed species, show little to no carbon losses or marginal gains (+/- 1%). These patterns result primarily from changes in wood volume, and are underlain by consistent relationships in our empirical data (similar to 2,100 species), wherein, large-seeded animal-dispersed species are larger as adults than small-seeded animal-dispersed species, but are smaller than abiotically dispersed species. Thus, floristic differences and distinct dispersal mode-seed size-adult size combinations can drive contrasting regional responses to defaunation. C1 [Osuri, Anand M.; Ratnam, Jayashree; Varma, Varun; Sankaran, Mahesh] Tata Inst Fundamental Res, Natl Ctr Biol Sci, GKVK Campus,Bellary Rd, Bangalore 560065, Karnataka, India. [Osuri, Anand M.] Nat Conservat Fdn, 3076-5 4 Cross,Gokulam Pk, Mysore 570002, Karnataka, India. [Alvarez-Loayza, Patricia] Duke Univ, Ctr Trop Conservat, Durham, NC 27705 USA. [Hurtado Astaiza, Johanna] Org Trop Studies, La Selva Biol Stn, Puerto Viejo de Sarapiqui, Heredia, Costa Rica. [Bradford, Matt] CSIRO Land & Water, Trop Forest Res Ctr, POB 780, Atherton, Qld 4883, Australia. [Fletcher, Christine] Forest Res Inst Malaysia FRIM, Kepong 52109, Selangor Darul, Malaysia. [Ndoundou-Hockemba, Mireille] Wildlife Conservat Soc WCS Congo Program, BP 14537, Brazzaville, Congo. [Jansen, Patrick A.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Apartado 0843-03092, Panama City, Panama. [Jansen, Patrick A.] Wageningen Univ, Dept Environm Sci, Box 47, NL-6700 AA Wageningen, Netherlands. [Kenfack, David] Smithsonian Inst, Dept Bot, CTFS ForestGEO, NMNH MRC 166, POB 37012, Washington, DC 20013 USA. [Marshall, Andrew R.] Univ York, Dept Environm, CIRCLE, York YO10 5DD, N Yorkshire, England. [Marshall, Andrew R.] Flamingo Land Ltd, Kirby Misperton YO17 6UX, N Yorkshire, England. [Ramesh, B. R.] Inst Francais Pondichery, 11 St Louis St, Pondicherry 605001, India. [Rovero, Francesco] MUSE Sci Museum Trento, Corso Lavoro Sci 3, I-38122 Trento, Italy. [Sankaran, Mahesh] Univ Leeds, Sch Biol, Leeds LS2 9JT, W Yorkshire, England. RP Osuri, AM (reprint author), Tata Inst Fundamental Res, Natl Ctr Biol Sci, GKVK Campus,Bellary Rd, Bangalore 560065, Karnataka, India.; Osuri, AM (reprint author), Nat Conservat Fdn, 3076-5 4 Cross,Gokulam Pk, Mysore 570002, Karnataka, India. EM moanand@gmail.com RI Bradford, Matt/D-3389-2011; OI Varma, Varun/0000-0002-0289-6125 FU Gordon and Betty Moore Foundation; CSIRO; Terrestrial Ecosystem Research Network (TERN); University of Buea; WWF-Cameroon; Ministry of Forest and Wildlife, Cameroon; Smithsonian Tropical Research Institute; Ministry of Environment and Forestry-Republic of Indonesia; Bukit Barisan Selatan National Park; Wildlife Conservation Society-Indonesia Program; Forest Research Institute Malaysia; Organization for Tropical Studies; La Selva Biological Station; Wildlife Conservation Society; Leverhulme Trust; MUSE-Science Museum of Trento (Italy); Tanzania National Parks; SERNANP; Servicio Nacional de Areas Protegidas del Peru; Department of Science and Technology, Government of India [SERB/SR/SO/PS/78/2012]; Rufford Small Grants for Nature Conservation; National Centre for Biological Sciences; Nature Conservation Foundation; Karnataka Forest Department FX This study includes data obtained from the Tropical Ecology Assessment and Monitoring (TEAM) open data Network and open data sets published by Commonwealth Scientific and Industrial Research Organisation (CSIRO) and Institut Francais de Pondichery (IFP). TEAM is a collaboration between Conservation International, the Smithsonian Institution and the Wildlife Conservation Society, and partially funded by these institutions, the Gordon and Betty Moore Foundation and other donors. We thank Jorge Ahumada, Dan Metcalfe, Andrew Ford, Helen Murphy, Moses Sainge, Peter Mambo, George Chuyong, Duncan Thomas, Richard Condit, Rolando Perez, Salomon Aguilar, Meyner Nusalawo, William Marthy, Patrick Boundja, Sarah Yoga, Pebou Stevy, Poka Tecle, Emanuel H. Martin, Simon Lewis, Jon Lovett, Pantaleo Munishi, John Terborgh, Fernando Cornejo, M.H. Swaminath, Santoshgouda V. Patil, Dasappa, Raphael Pelissier, P. Dilip Venugopal, S. Aravajy, Claire Elouard, S. Ramalingam and all field technicians for helping establish and maintain the tree plots used in this study. We acknowledge CSIRO, Terrestrial Ecosystem Research Network (TERN), University of Buea, WWF-Cameroon, Ministry of Forest and Wildlife, Cameroon, Smithsonian Tropical Research Institute, Ministry of Environment and Forestry-Republic of Indonesia, Bukit Barisan Selatan National Park, Wildlife Conservation Society-Indonesia Program, Forest Research Institute Malaysia, Organization for Tropical Studies, La Selva Biological Station, Wildlife Conservation Society, Leverhulme Trust (c/o Valuing the Arc project), MUSE-Science Museum of Trento (Italy), Tanzania National Parks, SERNANP, Servicio Nacional de Areas Protegidas del Peru, Department of Science and Technology, Government of India (SERB/SR/SO/PS/78/2012), Rufford Small Grants for Nature Conservation, National Centre for Biological Sciences, Nature Conservation Foundation and Karnataka Forest Department for funding, institutional support and research permits. We thank William Bond, T.R. Shankar Raman and Hari Sridhar for comments on the manuscript. A.M.O. thanks James Maccarthy, Patrick Boundja and William Marthy for advising on and facilitating use of TEAM data. A.M.O. was supported by a fellowship from National Centre for Biological Sciences. NR 56 TC 3 Z9 3 U1 13 U2 26 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD APR PY 2016 VL 7 AR 11351 DI 10.1038/ncomms11351 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DK1OQ UT WOS:000374682800001 PM 27108957 ER PT J AU Rojas-Sandoval, J Melendez-Ackerman, EJ Angles-Alcazar, D AF Rojas-Sandoval, Julissa Melendez-Ackerman, Elvia J. Angles-Alcazar, Daniel TI Assessing the impact of grass invasion on the population dynamics of a threatened Caribbean dry forest cactus SO BIOLOGICAL CONSERVATION LA English DT Article DE Biological invasion; Columnar cacti; Demography; Elasticity; Invasive grasses; Invasive plants; Matrix dimension; Matrix population models ID PACHYCEREUS-PECTEN-ABORIGINUM; INTEGRAL PROJECTION MODELS; EXOTIC PLANT INVASIONS; MATRIX DIMENSIONALITY; BIOLOGICAL INVASIONS; NORTHWESTERN MEXICO; NITROGEN DYNAMICS; ALIEN PLANTS; COMPETITION; FIRE AB The negative impact of invasive plants on native species has been well documented, but little is known about the specific role that invaders play on the population decline of native species. Here we used demographic models to evaluate how the alien grass Megathyrsus maximus affects the population dynamics of the native cactus Harrisia portoricensis. Demographic data gathered for H. portoricensis in grass-invaded and non-invaded areas were used to construct matrix projection models. Our demographic analysis includes numerical simulations, life table response experiments, life-cycle parameters and a systematic evaluation of the effects of matrix dimensionality. Results revealed that, while positive A values can be achieved in grass-free areas dominated by native vegetation, population growth rates of H. portoricensis are reduced in grass-invaded areas (lambda = 0.88-0.91). Models predicted that H. portoricensis populations in grass-invaded areas might become extinct in the next 14-59 years, suggesting that the long-term persistence of this cactus may be linked to the fate of the grass invasion. Overall, our data show that the conversion of native forests into grass-dominated areas is having detrimental impacts on the population dynamics of native species, creating novel regeneration barriers that native species cannot surpass. Under this scenario, management strategies designed for the conservation of H. portoricensis should consider grass eradication and control policies and long-term monitoring of populations. The information derived from this work may help us understand the mechanisms by which invasive species are gaining dominance over native species, which is crucial for managing and predicting biological invasions. (C) 2016 Elsevier Ltd All rights reserved. C1 [Rojas-Sandoval, Julissa] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Room W526b,POB 37012, Washington, DC 20013 USA. [Rojas-Sandoval, Julissa; Melendez-Ackerman, Elvia J.] Univ Puerto Rico, Ctr Appl Trop Ecol & Conservat, POB 70377, San Juan, PR 00936 USA. [Melendez-Ackerman, Elvia J.] Univ Puerto Rico, Coll Nat Sci, Dept Environm Sci, POB 70377, San Juan, PR 00931 USA. [Angles-Alcazar, Daniel] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Angles-Alcazar, Daniel] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. RP Rojas-Sandoval, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Room W526b,POB 37012, Washington, DC 20013 USA. EM julirs07@gmail.com FU NSF-CREST through the Center for Applied Tropical Ecology and Conservation (CATEC) from The University of Puerto Rico [HRD-0206200, HRD 0734826] FX We thank J.M. Nassar, J.D. Ackerman and R.L. Tremblay for helpful comments on earlier versions of this manuscript. We also thank R. Rodriguez, C. Sanfiorenzo and J.J. Fumero who assisted collecting demographic data. This research was funded by the NSF-CREST (HRD-0206200 and HRD 0734826) through the Center for Applied Tropical Ecology and Conservation (CATEC) from The University of Puerto Rico. NR 61 TC 0 Z9 0 U1 11 U2 21 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD APR PY 2016 VL 196 BP 156 EP 164 DI 10.1016/j.biocon.2016.02.015 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA DL1AW UT WOS:000375365300018 ER PT J AU Ubernickel, K Simon, R Kalko, EKV Tschapka, M AF Uebernickel, Kirstin Simon, Ralph Kalko, Elisabeth K. V. Tschapka, Marco TI Sensory challenges for trawling bats: Finding transient prey on water surfaces SO JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA LA English DT Article ID ECHOLOCATION SIGNALS; NOCTILIO-LEPORINUS; MYOTIS-DAUBENTONII; BEHAVIOR; SENSITIVITY; INFORMATION; DASYCNEME; DISTANCE; FLIGHT; SONAR AB Bats are able to identify obstacles and prey objects based exclusively on acoustic information acquired via echolocation. To assess the echo information potentially available to the trawling bat Noctilio leporinus, prey objects were ensonified with artificial bat calls and deduced echo target strengths (TS) of the reflected signals. The artificial calls consisted either of constant frequency (CF) or frequency modulated (FM) sounds. Detection distances were calculated for call intensities of N. leporinus emitted in the field and in confined space. Measurements of a transient target consisting of a brief water splash and subsequently expanding water ripples revealed that concentrically expanding water ripples can provide sufficiently loud echoes to be detected by trawling bats. Experiments with stationary targets revealed differences in TS depending on the type of signal used (CF or FM). A calculated maximum detection distance between 4.5 and 13.7m for all measured targets indicates that prey detection in this very loud calling species occurs much earlier than suggested by estimations based on modifications in echolocation or flight behavior. (C) 2016 Acoustical Society of America. C1 [Uebernickel, Kirstin; Tschapka, Marco] Univ Ulm, Inst Evolutionary Ecol & Conservat Genom, Albert Einstein Allee 11, D-89069 Ulm, Germany. [Simon, Ralph] Univ Erlangen Nurnberg, Dept Sensor Technol, D-91054 Erlangen, Germany. [Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.; Tschapka, Marco] Smithsonian Trop Res Inst, Balboa, Panama. RP Ubernickel, K (reprint author), Univ Ulm, Inst Evolutionary Ecol & Conservat Genom, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM kirstin.uebernickel@uni-ulm.de FU ChiRoPing project, IST contract [215370] FX We want to thank K. Hochradel and A. T. Ruiz Ruiz for advice regarding the acoustic calculations, K. Jung, H.-U. Schnitzler, W. P. Stilz, and the ChiRoPing consortium for many fruitful discussions and A. Grinnell for helpful comments on earlier drafts. This study was funded through the ChiRoPing project, IST contract number 215370. NR 30 TC 0 Z9 0 U1 2 U2 6 PU ACOUSTICAL SOC AMER AMER INST PHYSICS PI MELVILLE PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA SN 0001-4966 EI 1520-8524 J9 J ACOUST SOC AM JI J. Acoust. Soc. Am. PD APR PY 2016 VL 139 IS 4 BP 1914 EP 1922 DI 10.1121/1.4944756 PG 9 WC Acoustics; Audiology & Speech-Language Pathology SC Acoustics; Audiology & Speech-Language Pathology GA DK5QN UT WOS:000374974900044 PM 27106338 ER PT J AU Riley, KN Browne, RA Erwin, TL AF Riley, Kathryn N. Browne, Robert A. Erwin, Terry L. TI Results from two sampling techniques for carabid beetles (Coleoptera: Carabidae) in temporarily flooded and terra firme rainforest of western Amazonia SO STUDIES ON NEOTROPICAL FAUNA AND ENVIRONMENT LA English DT Article DE Flight intercept trap (FIT); Neotropics; Ecuador; hand sampling; trapping methods; Tiputini Biodiversity Station (TBS); inundation forests; Insecta; species assemblages; diversity ID SPECIES RICHNESS ESTIMATORS; FLIGHT INTERCEPT TRAP; ASSEMBLAGES COLEOPTERA; TROPICAL FOREST; PITFALL TRAPS; ARTHROPOD ASSEMBLAGES; DWELLING COLEOPTERA; SUCCESSION GRADIENT; BRAZILIAN AMAZON; INSECT DIVERSITY AB Carabidae beetles (Coleoptera) were sampled by flight intercept traps (FITs) and hand sampling in the understory of a lowland rainforest in eastern Ecuador. Sampling occurred in June and July of 2011 and 2012 at 24 sites within temporarily flooded forest (FP) and non-flooded terra firme (TF) forest. A total of 674 Carabidae (excluding Cicindelinae) individuals, representing 18 tribes, 50 genera and 133 morphospecies, were collected. Significantly more individuals were collected by hand compared to FITs, particularly by hand in FP forests. After correction through sample-based rarefaction there are no significant differences in species richness between sampling methods and forest types. Ordination and dissimilarity analysis show FITs and hand sampling target different portions of the Carabidae community. Understanding sampling biases for various sampling methods and how it may be affected by forest type will result in more accurate and efficient surveys in tropical forests. C1 [Riley, Kathryn N.; Browne, Robert A.] Wake Forest Univ, Dept Biol, Winston Salem, NC 27109 USA. [Erwin, Terry L.] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Riley, KN (reprint author), Wake Forest Univ, Dept Biol, Winston Salem, NC 27109 USA. EM rilekn8@wfu.edu FU Wake Forest University; Richter Scholarship Program; Smithsonian Institution's National Museum of Natural History FX Financial support was provided by Wake Forest University, the Richter Scholarship Program and the Smithsonian Institution's National Museum of Natural History. NR 122 TC 0 Z9 0 U1 3 U2 3 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 2016 VL 51 IS 1 BP 78 EP 95 DI 10.1080/01650521.2016.1164473 PG 18 WC Zoology SC Zoology GA DK4IN UT WOS:000374881300010 ER PT J AU Fourie, NH Brown, JL Jolly, CJ Phillips-Conroy, JE Rogers, J Bernstein, RM AF Fourie, Nicolaas H. Brown, Janine L. Jolly, Clifford J. Phillips-Conroy, Jane E. Rogers, Jeffrey Bernstein, Robin M. TI Sources of variation in hair cortisol in wild and captive non-human primates SO ZOOLOGY LA English DT Article DE Cortisol; Hair cortisol analysis; Stress; Primates; Chronic stress ID CHIMPANZEES PAN-TROGLODYTES; ARCHAEOLOGICAL HAIR; SALIVARY CORTISOL; ANABOLIC-STEROIDS; BODY REGION; STRESS; BABOONS; AGE; CORTICOSTEROIDS; POPULATIONS AB Hair cortisol analysis is a potentially powerful tool for evaluating adrenal function and chronic stress. However, the technique has only recently been applied widely to studies of wildlife, including primates, and there are numerous practical and technical factors that should be considered to ensure good quality data and the validity of results and conclusions. Here we report on various intrinsic and extrinsic sources of variation in hair cortisol measurements in wild and captive primates. Hair samples from both wild and captive primates revealed that age and sex can affect hair cortisol concentrations; these effects need to be controlled for when making comparisons between individual animals or populations. Hair growth rates also showed considerable inter-specific variation among a number of primate species. We describe technical limitations of hair analyses and variation in cortisol concentrations as a function of asynchronous hair growth, anatomical site of collection, and the amount and numbers of hair/s used for cortisol extraction. We discuss these sources of variation and their implications for proper study design and interpretation of results. Published by Elsevier GmbH. C1 [Fourie, Nicolaas H.; Bernstein, Robin M.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, 2110 G St NW, Washington, DC 20052 USA. [Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. [Jolly, Clifford J.] NYU, Dept Anthropol, Rufus D Smith Hall,25 Waverly Pl, New York, NY 10003 USA. [Phillips-Conroy, Jane E.] Washington Univ, Sch Med, Dept Anat & Neurobiol, 660 South Euclid Ave, St Louis, MO 63110 USA. [Phillips-Conroy, Jane E.] Washington Univ, Dept Anthropol, McMillan Hall,Room 112,One Brookings Dr, St Louis, MO 63130 USA. [Rogers, Jeffrey] Baylor Coll Med, Human Genome Sequencing Ctr, 1 Baylor Plaza, Houston, TX 77030 USA. [Rogers, Jeffrey] Baylor Coll Med, Dept Mol & Human Genet, 1 Baylor Plaza, Houston, TX 77030 USA. [Bernstein, Robin M.] Univ Colorado, Dept Anthropol, 1350 Pleasant St, Boulder, CO 80309 USA. RP Fourie, NH (reprint author), NIH, Biobehav Branch, Div Intramural Res, Bethesda, MD 20892 USA. EM fourienh@mail.nih.gov OI Fourie, Nicolaas/0000-0002-5167-8570 FU San Diego Zoo; Center for the Advanced Study of Hominid Paleobiology at the George Washington University; Lewis Cotlow Grant FX We would like to thank Jean-Yves Robert and Dr. Benoit Quintard from the Museum de Besancon for arranging for the collection of Papio papio samples. We would like to thank Dr. Antoinette Kotze, Dr. Adrian Tordif and Mark Howitt from the National Zoological Gardens in South Africa for providing wild Papio ursinus samples from their collections and projects, and the Tanzanian National Parks Authority (TANAPA) for providing permission to conduct research in Mikumi National Park. We would like to thank the San Diego Zoo for its support in this research. We would also like to thank Dr. Rui Diogo for allowing the collection of hair samples in the course of his research. We would also like to thank Sarah Putman from the Smithsonian's Conservation Research Center for her support and advice. We would like to thank Michael Holland for his assistance in the laboratory. The research was supported with funds provided by the Center for the Advanced Study of Hominid Paleobiology at the George Washington University and through a Lewis Cotlow Grant. The opinions expressed herein and the interpretation and reporting of these data are the responsibility of the authors and in no way should be seen as an official recommendation, interpretation, or policy of the National Institutes of Health or the United States Government. The research presented in this paper was conducted as part of Dr. Fourie's doctoral research at the George Washington University before joining the NINR. NR 57 TC 0 Z9 0 U1 10 U2 11 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 0944-2006 J9 ZOOLOGY JI Zoology PD APR PY 2016 VL 119 IS 2 BP 119 EP 125 DI 10.1016/j.zool.2016.01.001 PG 7 WC Zoology SC Zoology GA DJ7AQ UT WOS:000374364700005 PM 26884274 ER PT J AU Beaty, LE Emmering, QC Bernal, XE AF Beaty, Lynne E. Emmering, Quinn C. Bernal, Ximena E. TI Mixed Sex Effects on the Second-toFourth Digit Ratio of Tungara Frogs (Engystomops pustulosus) and Cane Toads (Rhinella marina) SO ANATOMICAL RECORD-ADVANCES IN INTEGRATIVE ANATOMY AND EVOLUTIONARY BIOLOGY LA English DT Article DE allometry; amphibia; asymmetry; digit ratio (2D:4D); indicator traits; sexual dimorphism ID LENGTH RATIO; COSTA-RICA; DIMORPHISM; 2D4D; EVOLUTION; ECOLOGY; 2D-4D; 2D/4D; 2ND AB Sexual dimorphism in the ratio of digit lengths has been correlated to behavioral, physiological, and morphological traits in a variety of taxa. While sexual dimorphism in the second-to-fourth digit length ratio (2D:4D) is a well-established indicator of prenatal androgen exposure in mammals, investigations into the patterns of 2D: 4D and the drivers of such variation in other taxa are lacking. We used linear mixed effects models to gain a mechanistic understanding of the factors that drive variation in the scaling relationship between the lengths of the second and fourth digits in two species of anurans: tungara frogs (Engystomops pustulosus) and cane toads (Rhinella marina). We found evidence for sexual dimorphism of the 2D: 4D scaling relationship on the front feet of tungara frogs, with female frogs having a larger ratio than males resulting from a relatively longer second digit on females. To our knowledge, this mammal-like pattern of sex differences in digit ratio has not yet been reported for anurans. However, given the reduced number of digits on the front feet of anurans, and uncertainty about which digit was lost during evolutionary history, this apparent sexual dimorphism in the front feet of tungara frogs should be treated with caution. In contrast, we found no evidence of sexual dimorphism in 2D: 4D on either the front or rear feet of cane toads. This study highlights ambiguities in 2D: 4D across taxa and suggests that further research is needed to evaluate the effect of androgens on 2D: 4D in animals other than placental mammals. (C) 2016 Wiley Periodicals, Inc. C1 [Beaty, Lynne E.] Oklahoma State Univ, Dept Integrat Biol, 501 Life Sci West, Stillwater, OK 74078 USA. [Emmering, Quinn C.] Fed Energy Regulatory Commiss, Washington, DC USA. [Bernal, Ximena E.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. [Bernal, Ximena E.] Smithsonian Trop Res Inst, Gamboa, Panama. RP Beaty, LE (reprint author), Oklahoma State Univ, Dept Integrat Biol, 501 Life Sci West, Stillwater, OK 74078 USA. EM lynne.beaty@okstate.edu FU DoD, Air Force Office of Scientific Research, National Defense Science and Engineering Graduate (NDSEG) Fellowship [32 CFR 168a]; NSF [IOS 1433990] FX Grant sponsor: The DoD, Air Force Office of Scientific Research, National Defense Science and Engineering Graduate (NDSEG) Fellowship; Grant number: 32 CFR 168a (LEB); Grant sponsor: NSF grant; Grant number: IOS 1433990 (XEB). NR 37 TC 1 Z9 1 U1 1 U2 4 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 2016 VL 299 IS 4 BP 421 EP 427 DI 10.1002/ar.23322 PG 7 WC Anatomy & Morphology SC Anatomy & Morphology GA DJ7FU UT WOS:000374378100003 PM 26815928 ER PT J AU Alvarado-Gomez, JD Hussain, GAJ Cohen, O Drake, JJ Garraffo, C Grunhut, J Gombosi, TI AF Alvarado-Gomez, J. D. Hussain, G. A. J. Cohen, O. Drake, J. J. Garraffo, C. Grunhut, J. Gombosi, T. I. TI Simulating the environment around planet-hosting stars I. Coronal structure SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: coronae; stars: magnetic field; stars: late-type; stars: individual: HD 1237; stars: individual: HD 22049; stars: individual: HD 147513 ID STELLAR MAGNETIC-FIELDS; X-RAY; EXTREME-ULTRAVIOLET; EPSILON-ERIDANI; ACTIVE STARS; MASS-LOSS; EXTRASOLAR PLANETS; NEAR-ULTRAVIOLET; ATOMIC DATABASE; ALFVENIC WAVES AB We present the results of a detailed numerical simulation of the circumstellar environment around three exoplanet-hosting stars. A modern global magnetohydrodynamic model is considered that includes Alfven wave dissipation as a self-consistent coronal heating mechanism. This paper contains the description of the numerical set-up, evaluation procedure, and the simulated coronal structure of each system (HD 1237, HD 22049, and HD 147513). The simulations are driven by surface magnetic field maps, recovered with the observational technique of Zeeman-Doppler imaging. A detailed comparison of the simulations is performed, where two di ff erent implementations of this mapping routine are used to generate the surface field distributions. Quantitative and qualitative descriptions of the coronae of these systems are presented, including synthetic high-energy emission maps in the extreme ultraviolet (EUV) and soft X-ray (SXR) ranges. Using the simulation results, we are able to recover similar trends as in previous observational studies, including the relation between the magnetic flux and the coronal X-ray emission. Furthermore, for HD 1237 we estimate the rotational modulation of the high-energy emission that is due to the various coronal features developed in the simulation. We obtain variations during a single stellar rotation cycle of up to 15% for the EUV and SXR ranges. The results presented here will be used in a follow-up paper to self-consistently simulate the stellar winds and inner astrospheres of these systems. C1 [Alvarado-Gomez, J. D.; Hussain, G. A. J.; Grunhut, J.] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Alvarado-Gomez, J. D.] Univ Munich, Univ Sternwarte Munchen, Scheinerstr 1, D-81679 Munich, Germany. [Hussain, G. A. J.] Univ Toulouse, Inst Rech Astrophys & Planetol, UPS OMP, F-31400 Toulouse, France. [Cohen, O.; Drake, J. J.; Garraffo, C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, 2455 Hayward St, Ann Arbor, MI 48109 USA. RP Alvarado-Gomez, JD (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.; Alvarado-Gomez, JD (reprint author), Univ Munich, Univ Sternwarte Munchen, Scheinerstr 1, D-81679 Munich, Germany. EM jalvarad@eso.org RI Gombosi, Tamas/G-4238-2011; OI Gombosi, Tamas/0000-0001-9360-4951; Alvarado Gomez, Julian David/0000-0001-5052-3473; Cohen, Ofer/0000-0003-3721-0215 FU DFG Cluster of Excellence "Origin and Structure of the Universe" FX This work was carried out using the SWMF/BATSRUS tools developed at The University of Michigan Center for Space Environment Modeling (CSEM) and made available through the NASA Community Coordinated Modeling Center (CCMC). We acknowledge the support by the DFG Cluster of Excellence "Origin and Structure of the Universe". We are grateful for the support by A. Krukau through the Computational Center for Particle and Astrophysics (C2PAP). NR 90 TC 5 Z9 5 U1 2 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 APR PY 2016 VL 588 AR A28 DI 10.1051/0004-6361/201527832 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI0SQ UT WOS:000373207800040 ER PT J AU Faria, JP Haywood, RD Brewer, BJ Figueira, P Oshagh, M Santerne, A Santos, NC AF Faria, J. P. Haywood, R. D. Brewer, B. J. Figueira, P. Oshagh, M. Santerne, A. Santos, N. C. TI Uncovering the planets and stellar activity of CoRoT-7 using only radial velocities SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; planetary systems; stars: individual: CoRoT-7; techniques: radial velocities ID EXTRA-SOLAR PLANETS; STARS; MASS; ROTATION; SYSTEM AB Stellar activity can induce signals in the radial velocities of stars, complicating the detection of orbiting low-mass planets. We present a method to determine the number of planetary signals present in radial-velocity datasets of active stars, using only radial-velocity observations. Instead of considering separate fits with different number of planets, we use a birth-death Markov chain Monte Carlo algorithm to infer the posterior distribution for the number of planets in a single run. In a natural way, the marginal distributions for the orbital parameters of all planets are also inferred. This method is applied to HARPS data of CoRoT-7. We confidently recover the orbits of both CoRoT-7b and CoRoT-7c although the data show evidence for the presence of additional signals. C1 [Faria, J. P.; Figueira, P.; Oshagh, M.; Santerne, A.; Santos, N. C.] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, Rua Estrelas, P-4150762 Oporto, Portugal. [Faria, J. P.; Santos, N. C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, Rua Campo Alegre, P-4169007 Oporto, Portugal. [Haywood, R. D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Brewer, B. J.] Univ Auckland, Dept Stat, Private Bag 92019, Auckland 1142, New Zealand. [Oshagh, M.] Univ Gottingen, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany. RP Faria, JP (reprint author), Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, Rua Estrelas, P-4150762 Oporto, Portugal.; Faria, JP (reprint author), Univ Porto, Fac Ciencias, Dept Fis & Astron, Rua Campo Alegre, P-4169007 Oporto, Portugal. EM joao.faria@astro.up.pt RI Figueira, Pedro/J-4916-2013 OI Figueira, Pedro/0000-0001-8504-283X FU Fundacao para a Ciencia e a Tecnologia (FCT) [UID/FIS/04434/2013, PTDC/FIS-AST/1526/2014]; FCT [SFRH/BD/93848/2013, IF/01037/2013CP1191/CT0001]; John Templeton Foundation; Fast Start grant from the Royal Society of New Zealand; FCT through Investigador FCT contracts [IF/01037/2013, IF/00169/2012]; POPH/FSE (EC) by FEDER through program Programa Operacional de Factores de Competitividade - COMPETE; Deutsche Forschungsgemeinschft (DFG, German Research Foundation) [OS 508/1-1]; European Union under a Marie Curie Intra-European Fellowship for Career Development [627202] FX The work presented here grew directly from a collaboration that started at the Astro Hack Week 2015. We thank Andrew Collier Cameron for insightful discussions. We acknowledge the excellent open-source Python packages made available to the community (in particular DAFT and George). This work was supported by Fundacao para a Ciencia e a Tecnologia (FCT) through the research grant UID/FIS/04434/2013 and the grant PTDC/FIS-AST/1526/2014. J.P.F. acknowledges support from FCT through the grant reference SFRH/BD/93848/2013. R.D.H. gratefully acknowledges 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. B.J.B. is supported by a Fast Start grant from the Royal Society of New Zealand. P.F. and N.C.S. acknowledge support by FCT through Investigador FCT contracts (IF/01037/2013 and IF/00169/2012, respectively), and POPH/FSE (EC) by FEDER funding through the program Programa Operacional de Factores de Competitividade - COMPETE. P.F. further acknowledges support from FCT in the form of an exploratory project of reference IF/01037/2013CP1191/CT0001. M.O. acknowledges research funding from the Deutsche Forschungsgemeinschft (DFG, German Research Foundation) - OS 508/1-1. A.S. is supported by the European Union under a Marie Curie Intra-European Fellowship for Career Development with reference FP7-PEOPLE-2013-IEF, No. 627202. NR 37 TC 6 Z9 6 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2016 VL 588 AR A31 DI 10.1051/0004-6361/201527899 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI0SQ UT WOS:000373207800043 ER PT J AU Gatuzz, E Garcia, JA Kallman, TR Mendoza, C AF Gatuzz, Efrain Garcia, Javier A. Kallman, Timothy R. Mendoza, Claudio TI Oxygen, neon, and iron X-ray absorption in the local interstellar medium SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: general; ISM: atoms; ISM: abundances; ISM: structure; X-rays: ISM ID HOT INTERGALACTIC MEDIUM; XMM-NEWTON OBSERVATION; K ABSORPTION; PHYSICAL-PROPERTIES; ATOMIC OXYGEN; SCULPTOR WALL; SPECTROSCOPY; BINARIES; SPECTRUM; EDGE AB Aims. We present a detailed study of X-ray absorption in the local interstellar medium by analyzing the X-ray spectra of 24 galactic sources obtained with the Chandra High Energy Transmission Grating Spectrometer and the XMM-Newton Reflection Grating Spectrometer. Methods. By modeling the continuum with a simple broken power-law and by implementing the new ISMabs X-ray absorption model, we have estimated the total H, O, Ne, and Fe column densities towards the observed sources. Results. We have determined the absorbing material distribution as a function of source distance and galactic latitude-longitude. Conclusions. Direct estimates of the fractions of neutrally, singly, and doubly ionized species of O, Ne, and Fe reveal the dominance of the cold component, thus indicating an overall low degree of ionization. Our results are expected to be sensitive to the model used to describe the continuum in all sources. C1 [Gatuzz, Efrain] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Gatuzz, Efrain] Cent Univ Venezuela, Fac Ciencias, Escuela Fis, POB 20632, Caracas 1020A, Venezuela. [Gatuzz, Efrain; Mendoza, Claudio] Inst Venezolano Invest Cient, Ctr Fis, POB 20632, Caracas 1020A, Venezuela. [Garcia, Javier A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Kallman, Timothy R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gatuzz, E (reprint author), Max Planck Inst Astrophys, D-85741 Garching, Germany.; Gatuzz, E (reprint author), Cent Univ Venezuela, Fac Ciencias, Escuela Fis, POB 20632, Caracas 1020A, Venezuela.; Gatuzz, E (reprint author), Inst Venezolano Invest Cient, Ctr Fis, POB 20632, Caracas 1020A, Venezuela. EM egatuzz@mpa-garching.mpg.de NR 43 TC 2 Z9 2 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2016 VL 588 AR A111 DI 10.1051/0004-6361/201527752 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI0SQ UT WOS:000373207800123 ER PT J AU Giroletti, M Massaro, F D'Abrusco, R Lico, R Burlon, D Hurley-Walker, N Johnston-Hollitt, M Morgan, J Pavlidou, V Bell, M Bernardi, G Bhat, R Bowman, JD Briggs, F Cappallo, RJ Corey, BE Deshpande, AA Ewall-Rice, A Emrich, D Gaensler, BM Goeke, R Greenhill, LJ Hazelton, BJ Hindson, L Kaplan, DL Kasper, JC Kratzenberg, E Feng, L Jacobs, D Kudryavtseva, N Lenc, E Lonsdale, CJ Lynch, MJ McKinley, B McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Offringa, AR Ord, SM Pindor, B Prabu, T Procopio, P Riding, J Rogers, AEE Roshi, A Shankar, NU Srivani, KS Subrahmanyan, R Tingay, SJ Waterson, M Wayth, RB Webster, RL Whitney, AR Williams, A Williams, CL AF Giroletti, M. Massaro, F. D'Abrusco, R. Lico, R. Burlon, D. Hurley-Walker, N. Johnston-Hollitt, M. Morgan, J. Pavlidou, V. Bell, M. Bernardi, G. Bhat, R. Bowman, J. D. Briggs, F. Cappallo, R. J. Corey, B. E. Deshpande, A. A. Ewall-Rice, A. Emrich, D. Gaensler, B. M. Goeke, R. Greenhill, L. J. Hazelton, B. J. Hindson, L. Kaplan, D. L. Kasper, J. C. Kratzenberg, E. Feng, L. Jacobs, D. Kudryavtseva, N. Lenc, E. Lonsdale, C. J. Lynch, M. J. McKinley, B. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Offringa, A. R. Ord, S. M. Pindor, B. Prabu, T. Procopio, P. Riding, J. Rogers, A. E. E. Roshi, A. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Tingay, S. J. Waterson, M. Wayth, R. B. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. TI High-energy sources at low radio frequency: the Murchison Widefield Array view of Fermi blazars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE BL Lacertae objects: general; catalogs; gamma rays: galaxies; quasars: general; radiation mechanisms: non-thermal; radio continuum: galaxies ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; SOURCE CATALOG; SKY SURVEY; RAY CONNECTION; IMAGING SURVEY; SOUTHERN SKY; LOFAR; SUMSS; GHZ AB Context. Low-frequency radio arrays are opening a new window for the study of the sky, both to study new phenomena and to better characterize known source classes. Being flat-spectrum sources, blazars are so far poorly studied at low radio frequencies. Aims. We characterize the spectral properties of the blazar population at low radio frequency, compare the radio and high-energy properties of the gamma-ray blazar population, and search for radio counterparts of unidentified gamma-ray sources. Methods. We cross-correlated the 6100 deg(2) Murchison Widefield Array Commissioning Survey catalogue with the Roma blazar catalogue, the third catalogue of active galactic nuclei detected by Fermi-LAT, and the unidentified members of the entire third catalogue of gamma-ray sources detected by Fermi-LAT. When available, we also added high-frequency radio data from the Australia Telescope 20 GHz catalogue. Results. We find low-frequency counterparts for 186 out of 517 (36%) blazars, 79 out of 174 (45%) gamma-ray blazars, and 8 out of 73 (11%) gamma-ray blazar candidates. The mean low-frequency (120-180 MHz) blazar spectral index is = 0.57 +/- 0.02: blazar spectra are flatter than the rest of the population of low-frequency sources, but are steeper than at similar to GHz frequencies. Low-frequency radio flux density and gamma-ray energy flux display a mildly significant and broadly scattered correlation. Ten unidentified gamma-ray sources have a (probably fortuitous) positional match with low radio frequency sources. Conclusions. Low-frequency radio astronomy provides important information about sources with a flat radio spectrum and high energy. However, the relatively low sensitivity of the present surveys still misses a significant fraction of these objects. Upcoming deeper surveys, such as the GaLactic and Extragalactic All-Sky MWA (GLEAM) survey, will provide further insight into this population. C1 [Giroletti, M.] INAF Osservatorio Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. [Massaro, F.] Univ Turin, Dept Phys, Via Pietro Giuria 1, I-10125 Turin, Italy. [D'Abrusco, R.] Univ Naples Federico II, Dept Phys Sci, Via Cinthia 9, I-80126 Naples, Italy. [Lico, R.] Univ Bologna, Dipartimento Fis & Astron, Via Ranzani 1, I-40127 Bologna, Italy. [Burlon, D.; Gaensler, B. M.; Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Burlon, D.; Briggs, F.; Gaensler, B. M.; Lenc, E.; Mitchell, D. A.; Ord, S. M.; Subrahmanyan, R.; Tingay, S. J.; Wayth, R. B.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Dublin, Ireland. [Hurley-Walker, N.; Morgan, J.; Bhat, R.; Emrich, D.; Kudryavtseva, N.; Lynch, M. J.; Ord, S. M.; Tingay, S. J.; Waterson, M.; Wayth, R. B.; Williams, A.] Curtin Univ Technol, ICRAR, Bentley, WA 6102, Australia. [Johnston-Hollitt, M.; Hindson, L.] Victoria Univ Wellington, Sch Chem & Phys Sci, POB 600, Wellington 6140, New Zealand. [Pavlidou, V.] Univ Crete, Iraklion 71003, Greece. [Pavlidou, V.] Fdn Res & Technol Hellas, Iraklion 71003, Greece. [Bell, M.; Mitchell, D. A.] CSIRO Astron & Space Sci CASS, POB 76, Epping, NSW 1710, Australia. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Bowman, J. D.; Jacobs, D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, R. J.; Corey, B. E.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Rogers, A. E. E.; Whitney, A. R.] MIT Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Ewall-Rice, A.; Goeke, R.; Feng, L.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Gaensler, B. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Kudryavtseva, N.] Tallinn Univ Technol, Inst Cybernet, Akad Tee 21, EE-12618 Tallinn, Estonia. [McKinley, B.; Pindor, B.; Procopio, P.; Riding, J.; Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Offringa, A. R.] Netherlands Inst Radio Astron ASTRON, POB 2, NL-7990 AA Dwingeloo, Netherlands. [Roshi, A.] Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22903 USA. [Roshi, A.] Natl Radio Astron Observ, Greenbank, VA 22903 USA. [Waterson, M.] SKA Org, Macclesfield SK11 9DL, Cheshire, England. RP Giroletti, M (reprint author), INAF Osservatorio Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. EM giroletti@ira.inaf.it RI Udayashankar , N/D-4901-2012; Subrahmanyan, Ravi/D-4889-2012; Pavlidou, Vasiliki/C-2944-2011; Wayth, Randall/B-2444-2013; D'Abrusco, Raffaele/L-2767-2016; Massaro, Francesco/L-9102-2016; Deshpande, Avinash/D-4868-2012 OI Pavlidou, Vasiliki/0000-0002-0870-1368; Lenc, Emil/0000-0002-9994-1593; Kudryavtseva, Nadia/0000-0002-1372-0942; Wayth, Randall/0000-0002-6995-4131; D'Abrusco, Raffaele/0000-0003-3073-0605; Massaro, Francesco/0000-0002-1704-9850; FU Curtin University; Sydney Institute for Astrophysics; PRIN-INAF; NVIDIA at Harvard University FX M.G. acknowledges financial support and kind hospitality during his visits at Curtin University and Sydney Institute for Astrophysics. We acknowledge financial contribution from grant PRIN-INAF-2011. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France, and of NASA's Astrophysics Data System. 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 operation of the MWA is provided by the Australian Government Department of Industry and Science and Department of Education (National Collaborative Research Infrastructure Strategy: NCRIS), under a contract to Curtin University administered by Astronomy Australia Limited. We acknowledge the iVEC Petabyte Data Store and the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University. The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. NR 37 TC 3 Z9 3 U1 1 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2016 VL 588 AR A141 DI 10.1051/0004-6361/201527817 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI0SQ UT WOS:000373207800153 ER PT J AU Guidi, G Tazzari, M Testi, L de Gregorio-Monsalvo, I Chandler, CJ Perez, L Isella, A Natta, A Ortolani, S Henning, T Corder, S Linz, H Andrews, S Wilner, D Ricci, L Carpenter, J Sargent, A Mundy, L Storm, S Calvet, N Dullemond, C Greaves, J Lazio, J Deller, A Kwon, W AF Guidi, G. Tazzari, M. Testi, L. de Gregorio-Monsalvo, I. Chandler, C. J. Perez, L. Isella, A. Natta, A. Ortolani, S. Henning, Th. Corder, S. Linz, H. Andrews, S. Wilner, D. Ricci, L. Carpenter, J. Sargent, A. Mundy, L. Storm, S. Calvet, N. Dullemond, C. Greaves, J. Lazio, J. Deller, A. Kwon, W. TI Dust properties across the CO snowline in the HD 163296 disk from ALMA and VLA observations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: pre-main sequence; protoplanetary disks; instrumentation: interferometers; submillimeter: stars ID T-TAURI STARS; PROTOPLANETARY DISKS; GRAIN-GROWTH; CIRCUMSTELLAR DISKS; PLANET FORMATION; SOLAR NEBULA; HL TAU; MILLIMETER WAVELENGTHS; ACCRETION DISKS; CQ TAURI AB Context. To characterize the mechanisms of planet formation it is crucial to investigate the properties and evolution of protoplanetary disks around young stars, where the initial conditions for the growth of planets are set. The high spatial resolution of Atacama Large Millimeter/submillimeter Array (ALMA) and Karl G. Jansky Very Large Array (VLA) observations now allows the study of radial variations of dust properties in nearby resolved disks and the investigation of the early stages of grain growth in disk midplanes. Aims. Our goal is to study grain growth in the well-studied disk of the young, intermediate-mass star HD 163296 where dust processing has already been observed and to look for evidence of growth by ice condensation across the CO snowline, which has already been identified in this disk with ALMA. Methods. Under the hypothesis of optically thin emission, we compare images at different wavelengths from ALMA and VLA to measure the opacity spectral index across the disk and thus the maximum grain size. We also use a Bayesian tool based on a two-layer disk model to fit the observations and constrain the dust surface density. Results. The measurements of the opacity spectral index indicate the presence of large grains and pebbles (>= 1 cm) in the inner regions of the disk (inside similar to 50 AU) and smaller grains, consistent with ISM sizes, in the outer disk (beyond 150 AU). Re-analyzing ALMA Band 7 science verification data, we find (radially) unresolved excess continuum emission centered near the location of the CO snowline at similar to 90 AU. Conclusions. Our analysis suggests a grain size distribution consistent with an enhanced production of large grains at the CO snowline and consequent transport to the inner regions. Our results combined with the excess in infrared scattered light suggests there is a structure at 90 AU involving the whole vertical extent of the disk. This could be evidence of small scale processing of dust at the CO snowline. C1 [Guidi, G.; Testi, L.; Natta, A.] Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. [Guidi, G.] Univ Florence, Dipartimento Fis & Astron, I-50121 Florence, Italy. [Tazzari, M.; Testi, L.; de Gregorio-Monsalvo, I.] ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Tazzari, M.; Testi, L.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [de Gregorio-Monsalvo, I.; Corder, S.] Joint ALMA Observ JAO, Alonso Cordova 3107 Vitacura, Santiago, Chile. [Chandler, C. J.; Perez, L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Isella, A.] Rice Univ, Dept Phys & Astron, 6100 Main St, Houston, TX 77005 USA. [Natta, A.] Dublin Inst Adv Studies, Sch Cosm Phys, 31 Fitzwilliams Pl, Dublin 2, Ireland. [Ortolani, S.] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy. [Ortolani, S.] Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Henning, Th.; Linz, H.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Andrews, S.; Wilner, D.; Ricci, L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Carpenter, J.; Sargent, A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Mundy, L.; Storm, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Calvet, N.] Univ Michigan, Dept Astron, 830 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA. [Dullemond, C.] Heidelberg Univ, Inst Theoret Astrophys, Albert Ueberle Str 2, D-69120 Heidelberg, Germany. [Greaves, J.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Lazio, J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Deller, A.] Netherlands Inst Radio Astron ASTRON, NL-7991 Dwingeloo, Netherlands. [Kwon, W.] Korea Astron & Space Sci Inst, 776 Daedeok Daero, Daejeon 34055, South Korea. RP Guidi, G (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. EM guidi@arcetri.astro.it OI Dullemond, Cornelis/0000-0002-7078-5910 FU Italian Ministero dell'Istruzione, Universita e Ricerca [CUP C52I13000140001]; National Aeronautics and Space Administration FX This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.000010.SV. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. We are grateful to Antonio Garufi for many discussions and for sharing his infrared polarization images. We thank Sebastian Stammler for insightful discussions on the effect of the CO snowline on dust and for showing us the results of his simulations in advance of publication. We thank the anonymous referee for the helpful comments. Part 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. The fits have been carried out on the computing facilities of the Computational Center for Particle and Astrophysics (C2PAP) as part of the approved project "Dust evolution in protoplanetary disks". M.T. and L.T. are grateful for the experienced support by F. Beaujean (C2PAP). This work was partly supported by the Italian Ministero dell'Istruzione, Universita e Ricerca through the grant Progetti Premiali 2012 - iALMA (CUP C52I13000140001). NR 65 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2016 VL 588 AR A112 DI 10.1051/0004-6361/201527516 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI0SQ UT WOS:000373207800124 ER PT J AU Hansen, TT Andersen, J Nordstrom, B Beers, TC Placco, VM Yoon, J Buchhave, LA AF Hansen, T. T. Andersen, J. Nordstroem, B. Beers, T. C. Placco, V. M. Yoon, J. Buchhave, L. A. TI The role of binaries in the enrichment of the early Galactic halo III. Carbon-enhanced metal-poor stars - CEMP-s stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Galaxy: formation; Galaxy: halo; stars: chemically peculiar; binaries: spectroscopic; ISM: structure ID ASYMPTOTIC GIANT BRANCH; NEAR-INFRARED SPECTROSCOPY; ROCHE-LOBE OVERFLOW; LOW-METALLICITY; HAMBURG/ESO SURVEY; ORBITAL ELEMENTS; MASSIVE STARS; PROCESS NUCLEOSYNTHESIS; HORIZONTAL-BRANCH; ROTATING STARS AB Context. Detailed spectroscopic studies of metal-poor halo stars have highlighted the important role of carbon-enhanced metal-poor (CEMP) stars in understanding the early production and ejection of carbon in the Galaxy and in identifying the progenitors of the CEMP stars among the first stars formed after the Big Bang. Recent work has also classified the CEMP stars by absolute carbon abundance, A(C), into high- and low-C bands, mostly populated by binary and single stars, respectively. Aims. Our aim is to determine the frequency and orbital parameters of binary systems among the CEMP-s stars, which exhibit strong enhancements of neutron-capture elements associated with the s-process. This allows us to test whether local mass transfer from a binary companion is necessary and sufficient to explain their dramatic carbon excesses. Methods. We have systematically monitored the radial velocities of a sample of 22 CEMP-s stars for several years with similar to monthly, high-resolution, low S/N echelle spectra obtained at the Nordic Optical Telescope (NOT) at La Palma, Spain. From these spectra, radial velocities with an accuracy of approximate to 100 m s(-1) were determined by cross-correlation with optimised templates. Results. Eighteen of the 22 stars exhibit clear orbital motion, yielding a binary frequency of 82 +/- 10%, while four stars appear to be single (18 +/- 10%). We thus confirm that the binary frequency of CEMP-s stars is much higher than for normal metal-poor giants, but not 100% as previously claimed. Secure orbits are determined for eleven of the binaries and provisional orbits for six long-period systems (P > 3000 days), and orbital circularisation timescales are discussed. Conclusions. The conventional scenario of local mass transfer from a former asymptotic giant branch (AGB) binary companion does appear to account for the chemical composition of most CEMP-s stars. However, the excess of C and s-process elements in some single CEMP-s stars was apparently transferred to their natal clouds by an external (distant) source. This finding has important implications for our understanding of carbon enrichment in the early Galactic halo and some high-redshift damped lyman alpha (DLA) systems, and of the mass loss from extremely metal-poor AGB stars. C1 [Hansen, T. T.] Heidelberg Univ, ZAH, Landessternwarte, Konigstuhl 12, D-69117 Heidelberg, Germany. [Hansen, T. T.] Carnegie Inst Washington Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Andersen, J.; Nordstroem, B.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. [Andersen, J.; Nordstroem, B.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Beers, T. C.; Placco, V. M.; Yoon, J.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Beers, T. C.; Placco, V. M.; Yoon, J.] Univ Notre Dame, JINA Ctr Evolut Elements, Notre Dame, IN 46556 USA. [Buchhave, L. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, L. A.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. RP Hansen, TT (reprint author), Heidelberg Univ, ZAH, Landessternwarte, Konigstuhl 12, D-69117 Heidelberg, Germany.; Hansen, TT (reprint author), Carnegie Inst Washington Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. EM thansen@carnegiescience.edu OI Hansen, Terese/0000-0001-6154-8983 FU German Research Foundation (DFG) [Sonderforschungsbereich SFB 881]; Danish Natural Science Research Council; Carlsberg Foundation; Physics Frontier Center/Joint Institute or Nuclear Astrophysics (JINA) [PHY 08-22648]; Physics Frontier Center/JINA Center for the Evolution of the Elements (JINA-CEE) - US National Science Foundation [PHY 14-30152] FX This paper is based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. We thank numerous NOT staff members and students for readily and very efficiently obtaining most of the many observations for us in service mode. We also thank Carlo Abate for clarifying the response of his modelled binary systems to the different modes of angular-momentum loss. Finally, we thank the anonymous referee for a very careful and incisive report that led to substantive clarifications, revisions, and improvements in the paper. This work was supported by Sonderforschungsbereich SFB 881 "The Milky Way System" (subproject A4) of the German Research Foundation (DFG). J.A. and B.N. gratefully acknowledge financial support from the Danish Natural Science Research Council and the Carlsberg Foundation. T.C.B., V.M.P., and J.Y. acknowledge partial support for this work from grants PHY 08-22648; Physics Frontier Center/Joint Institute or Nuclear Astrophysics (JINA), and PHY 14-30152; Physics Frontier Center/JINA Center for the Evolution of the Elements (JINA-CEE), awarded by the US National Science Foundation. NR 79 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2016 VL 588 AR A3 DI 10.1051/0004-6361/201527409 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI0SQ UT WOS:000373207800015 ER PT J AU Kama, M Bruderer, S Carney, M Hogerheijde, M van Dishoeck, EF Fedele, D Baryshev, A Boland, W Gusten, R Aikutalp, A Choi, Y Endo, A Frieswijk, W Karska, A Klaassen, P Koumpia, E Kristensen, L Leurini, S Nagy, Z Beaupuits, JPP Risacher, C van der Marel, N van Kempen, TA van Weeren, RJ Wyrowski, F Yildiz, UA AF Kama, M. Bruderer, S. Carney, M. Hogerheijde, M. van Dishoeck, E. F. Fedele, D. Baryshev, A. Boland, W. Guesten, R. Aikutalp, A. Choi, Y. Endo, A. Frieswijk, W. Karska, A. Klaassen, P. Koumpia, E. Kristensen, L. Leurini, S. Nagy, Z. Beaupuits, J. -P. Perez Risacher, C. van der Marel, N. van Kempen, T. A. van Weeren, R. J. Wyrowski, F. Yildiz, U. A. TI Observations and modelling of CO and [CI] in protoplanetary disks First detections of [CI] and constraints on the carbon abundance SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE surveys; protoplanetary disks; submillimeter: planetary systems ID T-TAURI STARS; HERBIG AE/BE STARS; MAIN-SEQUENCE STARS; HD 100546; YOUNG STARS; GAS-RICH; CIRCUMSTELLAR DISKS; VLBA DETERMINATION; TRANSITIONAL DISK; ISO SPECTROSCOPY AB Context. The gas-solid budget of carbon in protoplanetary disks is related to the composition of the cores and atmospheres of the planets forming in them. The principal gas-phase carbon carriers CO, C-0, and C+ can now be observed regularly in disks. Aims. The gas-phase carbon abundance in disks has thus far not been well characterized observationally. We obtain new constraints on the [C]/[H] ratio in a large sample of disks, and compile an overview of the strength of [CI] and warm CO emission. Methods. We carried out a survey of the CO 6-5 line and the [CI] 1-0 and 2-1 lines towards 37 disks with the APEX telescope, and supplemented it with [CII] data from the literature. The data are interpreted using a grid of models produced with the DALI disk code. We also investigate how well the gas-phase carbon abundance can be determined in light of parameter uncertainties. Results. The CO6-5 line is detected in 13 out of 33 sources, [CI] 1-0 in 6 out of 12, and [CI] 2-1 in 1 out of 33. With separate deep integrations, the first unambiguous detections of the [CI] 1-0 line in disks are obtained, in TW Hya and HD 100546. Conclusions. Gas-phase carbon abundance reductions of a factor of 5-10 or more can be identified robustly based on CO and [CI] detections, assuming reasonable constraints on other parameters. The atomic carbon detection towards TW Hya confirms a factor of 100 reduction of [C]/[H](gas) in that disk, while the data are consistent with an ISM-like carbon abundance for HD 100546. In addition, BP Tau, T Cha, HD 139614, HD 141569, and HD 100453 are either carbon-depleted or gas-poor disks. The low [CI] 2-1 detection rates in the survey mostly reflect insufficient sensitivity for T Tauri disks. The Herbig Ae/Be disks with CO and [CII] upper limits below the models are debris-disk-like systems. An increase in sensitivity of roughly order of magnitude compared to our survey is required to obtain useful constraints on the gas-phase [C]/[H] ratio in most of the targeted systems. C1 [Kama, M.; Carney, M.; Hogerheijde, M.; van Dishoeck, E. F.; Boland, W.; Frieswijk, W.; Klaassen, P.; Kristensen, L.; van der Marel, N.; van Kempen, T. A.; van Weeren, R. J.; Yildiz, U. A.] Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Bruderer, S.; Fedele, D.; Karska, A.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Baryshev, A.; Risacher, C.] SRON Netherlands Inst Space Res, NL-3584 Utrecht, Netherlands. [Baryshev, A.; Aikutalp, A.; Choi, Y.; Koumpia, E.; Nagy, Z.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. [Boland, W.] NOVA, JH Oort Bldg,POB 9513, NL-2300 RA Leiden, Netherlands. [Guesten, R.; Leurini, S.; Beaupuits, J. -P. Perez; Risacher, C.; Wyrowski, F.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Endo, A.] Delft Univ Technol, Kavli Inst Nanosci, Lorentzweg 1, NL-2628 CJ Delft, Netherlands. [Frieswijk, W.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Karska, A.] Adam Mickiewicz Univ, Fac Phys, Astron Observ Inst, Sloneczna 36, PL-60286 Poznan, Poland. [Klaassen, P.] Royal Observ, UK Astron Technol Ctr, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Kristensen, L.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Nagy, Z.] Univ Toledo, Dept Phys & Astron, 2801 West Bancroft St, Toledo, OH 43606 USA. [Yildiz, U. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Kama, M (reprint author), Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM mkama@strw.leidenuniv.nl RI Fedele, Davide/L-8688-2013; Yildiz, Umut/C-5257-2011; Karska, Agata/O-5311-2016; Kristensen, Lars E/F-4774-2011; OI Fedele, Davide/0000-0001-6156-0034; Yildiz, Umut/0000-0001-6197-2864; Karska, Agata/0000-0001-8913-925X; Kristensen, Lars E/0000-0003-1159-3721; Kama, Mihkel/0000-0003-0065-7267; van Weeren, Reinout/0000-0002-0587-1660 FU Royal Netherlands Academy of Arts and Sciences (KNAW); Netherlands Research School for Astronomy (NOVA); European Union A-ERC grant [291141 CHEMPLAN]; Foundation for Polish Science (FNP); Polish National Science Center [2013/11/N/ST9/00400]; NASA - Chandra X-ray Center [PF2-130104]; NASA [NAS8-03060]; Netherlands Organization for Scientific Research (NWO) [600.063.310.10] FX We thank the anonymous referee for constructive comments which helped to improve the paper, Arnaud Belloche and the APEX staff for assistance during the observations, and Matthijs van der Wiel for discussing his SPIRE observations with us. This work is supported by a Royal Netherlands Academy of Arts and Sciences (KNAW) professor prize, the Netherlands Research School for Astronomy (NOVA), and by the European Union A-ERC grant 291141 CHEMPLAN. A.K. acknowledges support from the Foundation for Polish Science (FNP) and the Polish National Science Center grant 2013/11/N/ST9/00400. R.J.W. is supported by NASA through the Einstein Postdoctoral grant number PF2-130104 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. This publication is based on data acquired with the Atacama Pathfinder Experiment (APEX). APEX is a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. CHAMP+ was constructed with support from the Netherlands Organization for Scientific Research (NWO), grant 600.063.310.10. NR 112 TC 10 Z9 10 U1 4 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 APR PY 2016 VL 588 AR A108 DI 10.1051/0004-6361/201526791 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI0SQ UT WOS:000373207800120 ER PT J AU Malavolta, L Nascimbeni, V Piotto, G Quinn, SN Borsato, L Granata, V Bonomo, AS Marzari, F Bedin, LR Rainer, M Desidera, S Lanza, AF Poretti, E Sozzetti, A White, RJ Latham, DW Cunial, A Libralato, M Nardiello, D Boccato, C Claudi, RU Cosentino, R Covino, E Gratton, R Maggio, A Micela, G Molinari, E Pagano, I Smareglia, R Affer, L Andreuzzi, G Aparicio, A Benatti, S Bignamini, A Borsa, F Damasso, M Di Fabrizio, L Harutyunyan, A Esposito, M Fiorenzano, AFM Gandolfi, D Giacobbe, P Hernandez, JIG Maldonado, J Masiero, S Molinaro, M Pedani, M Scandariato, G AF Malavolta, L. Nascimbeni, V. Piotto, G. Quinn, S. N. Borsato, L. Granata, V. Bonomo, A. S. Marzari, F. Bedin, L. R. Rainer, M. Desidera, S. Lanza, A. F. Poretti, E. Sozzetti, A. White, R. J. Latham, D. W. Cunial, A. Libralato, M. Nardiello, D. Boccato, C. Claudi, R. U. Cosentino, R. Covino, E. Gratton, R. Maggio, A. Micela, G. Molinari, E. Pagano, I. Smareglia, R. Affer, L. Andreuzzi, G. Aparicio, A. Benatti, S. Bignamini, A. Borsa, F. Damasso, M. Di Fabrizio, L. Harutyunyan, A. Esposito, M. Fiorenzano, A. F. M. Gandolfi, D. Giacobbe, P. Gonzalez Hernandez, J. I. Maldonado, J. Masiero, S. Molinaro, M. Pedani, M. Scandariato, G. TI The GAPS programme with HARPS-N at TNG XI. Pr 0211 in M44: the first multi-planet system in an open cluster SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: radial velocities; techniques: photometric; planetary systems ID EXTRA-SOLAR PLANETS; STELLAR EVOLUTION DATABASE; HOT JUPITERS; SUBSTELLAR COMPANIONS; CIRCUMSTELLAR DISKS; MULTIPLANET SYSTEMS; STAR-CLUSTERS; GIANT PLANETS; MASS STARS; HYADES AB Context. Open cluster (OC) stars share the same age and metallicity, and, in general, their age and mass can be estimated with higher precision than for field stars. For this reason, OCs are considered an important laboratory to study the relation between the physical properties of the planets and those of their host stars, and the evolution of planetary systems. However, only a handful of planets have been discovered around OC main-sequence stars so far, all of them in single-planet systems. For this reason we started an observational campaign within the GAPS collaboration to search for and characterize planets in OCs Aims. We monitored the Praesepe member Pr 0211 to improve our knowledge of the eccentricity of the hot Jupiter (HJ) that is already known to orbit this star and search for additional intermediate-mass planets. An eccentric orbit for the HJ would support a planet-planet scattering process rather than a disk-driven migration after its formation. Methods. From 2012 to 2015, we collected 70 radial velocity (RV) measurements with HARPS-N and 36 with TRES of Pr 0211. Simultaneous photometric observations were carried out with the robotic STELLA telescope to characterize the stellar activity. We discovered a long-term trend in the RV residuals that we show as being due to the presence of a second, massive, outer planet. Orbital parameters for the two planets are derived by simultaneously fitting RVs and photometric light curves, with the activity signal modelled as a series of sinusoids at the rotational period of the star and its harmonics. Results. We confirm that Pr 0211b has a nearly circular orbit (e = 0.02 +/- 0.01), with an improvement of a factor two with respect to the previous determination of its eccentricity, and estimate that Pr 0211c has a mass M(p)sin i = 7.9 +/- 0.2 M-J, a period P > 3500 days and a very eccentric orbit (e > 0 : 60). This kind of peculiar system may be typical of open clusters if the planet-planet scattering phase, which lead to the formation of HJs, is caused by stellar encounters rather than by unstable primordial orbits. Pr 0211 is the first multi-planet system discovered around an OC star. C1 [Malavolta, L.; Piotto, G.; Borsato, L.; Granata, V.; Marzari, F.; Bedin, L. R.; Cunial, A.; Libralato, M.; Nardiello, D.] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Vicolo Osservatorio 2, I-35122 Padua, Italy. [Malavolta, L.; Nascimbeni, V.; Piotto, G.; Borsato, L.; Granata, V.; Bedin, L. R.; Desidera, S.; Cunial, A.; Libralato, M.; Nardiello, D.; Boccato, C.; Claudi, R. U.; Gratton, R.; Benatti, S.; Masiero, S.] Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Quinn, S. N.; White, R. J.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Lanza, A. F.; Pagano, I.; Scandariato, G.] Osserv Astrofis Catania, INAF, Via S Sofia 78, I-95123 Catania, Italy. [Rainer, M.; Poretti, E.; Borsa, F.] Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy. [Bonomo, A. S.; Sozzetti, A.; Damasso, M.; Giacobbe, P.] Osserv Astron Torino, INAF, Via Osservatorio 20, I-10025 Pino Torinese, Italy. [Latham, D. W.; Cosentino, R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Cosentino, R.; Andreuzzi, G.; Di Fabrizio, L.; Harutyunyan, A.; Fiorenzano, A. F. M.; Pedani, M.] Fdn Galileo Galilei, INAF, Rambla Jose Ana Fernandez Perez 7, Brena Baja 38712, TF, Spain. [Covino, E.; Molinari, E.; Esposito, M.] Osserv Astron Capodimonte, INAF, Salita Moiariello 16, I-80131 Naples, Italy. [Maggio, A.; Micela, G.; Affer, L.; Maldonado, J.] Osserv Astron Palermo, INAF, Piazza Parlamento 1, I-90134 Palermo, Italy. [Molinari, E.] IASF Milano, INAF, Via Bassini 15, I-20133 Milan, Italy. [Smareglia, R.; Bignamini, A.; Molinaro, M.] Osserv Astron Trieste, INAF, Via Tiepolo 11, I-34143 Trieste, Italy. [Andreuzzi, G.] Osserv Astron Roma, INAF, Sede Monteporzio Catone, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. [Aparicio, A.; Gonzalez Hernandez, J. I.] Inst Astrofis Canarias, Calle Via Lactea S-N, Tenerife 38205, Spain. [Aparicio, A.; Gonzalez Hernandez, J. I.] Univ La Laguna, Dept Astrofis, Tenerife 38200, Spain. [Gandolfi, D.] Univ Turin, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy. [Gandolfi, D.] Heidelberg Univ, Zentrum Astron, Landessternwarte Konigstuhl, Konigstuhl 12, D-69117 Heidelberg, Germany. RP Malavolta, L (reprint author), Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Vicolo Osservatorio 2, I-35122 Padua, Italy. EM luca.malavolta@unipd.it OI Malavolta, Luca/0000-0002-6492-2085; Lanza, Antonino Francesco/0000-0001-5928-7251; Gandolfi, Davide/0000-0001-8627-9628 FU INAF through the "Progetti Premiali" funding scheme of the Italian Ministry of Education, University, and Research; European Union [313014]; INAF-OAPd [19/2013, 42/2013]; Spanish Ministry of Economy and Competitiveness (MINECO) [RYC-2013-14875]; Spanish ministry [AYA2014-56359-P] FX GAPS acknowledges support from INAF through the "Progetti Premiali" funding scheme of the Italian Ministry of Education, University, and Research. L.M. acknowledges the financial support provided by the European Union Seventh Framework Programme (FP7/2007-2013) under Grant agreement number 313014 (ETAEARTH). V.N. acknowledges partial support from INAF-OAPd through the grant "Analysis of HARPS-N data in the framework of GAPS project" (#19/2013) and "Studio preparatorio per le osservazioni della missione ESA/CHEOPS" (#42/2013). J.I.G.H. acknowledges financial support from the Spanish Ministry of Economy and Competitiveness (MINECO) under the 2013 Ramon y Cajal program MINECO RYC-2013-14875, and the Spanish ministry project MINECO AYA2014-56359-P. We made use of the SIMBAD database and VizieR catalogue access tool, operated at the CDS, Strasbourg, France. We wish to thank the anonymous referee for the valuable comments and suggestions. NR 92 TC 9 Z9 9 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2016 VL 588 AR A118 DI 10.1051/0004-6361/201527933 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI0SQ UT WOS:000373207800130 ER PT J AU Tazzari, M Testi, L Ercolano, B Natta, A Isella, A Chandler, CJ Perez, LM Andrews, S Wilner, DJ Ricci, L Henning, T Linz, H Kwon, W Corder, SA Dullemond, CP Carpenter, JM Sargent, AI Mundy, L Storm, S Calvet, N Greaves, JA Lazio, J Deller, AT AF Tazzari, M. Testi, L. Ercolano, B. Natta, A. Isella, A. Chandler, C. J. Perez, L. M. Andrews, S. Wilner, D. J. Ricci, L. Henning, T. Linz, H. Kwon, W. Corder, S. A. Dullemond, C. P. Carpenter, J. M. Sargent, A. I. Mundy, L. Storm, S. Calvet, N. Greaves, J. A. Lazio, J. Deller, A. T. TI Multiwavelength analysis for interferometric (sub-)mm observations of protoplanetary disks Radial constraints on the dust properties and the disk structure SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; planetary systems; protoplanetary disks ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; CIRCUMSTELLAR DISKS; GRAIN-GROWTH; MILLIMETER WAVELENGTHS; OPTICAL-PROPERTIES; SIZE DISTRIBUTION; TRANSITION DISK; ACCRETION DISKS; FORMING REGION AB Context. The growth of dust grains from sub-mu m to mm and cm sizes is the first step towards the formation of planetesimals. Theoretical models of grain growth predict that dust properties change as a function of disk radius, mass, age, and other physical conditions. High angular resolution observations at several (sub-)mm wavelengths constitute the ideal tool with which to directly probe the bulk of dust grains and to investigate the radial distribution of their properties. Aims. We lay down the methodology for a multiwavelength analysis of (sub-) mm and cm continuum interferometric observations to self-consistently constrain the disk structure and the radial variation of the dust properties. The computational architecture is massively parallel and highly modular. Methods. The analysis is based on the simultaneous fit in the uv-plane of observations at several wavelengths with a model for the disk thermal emission and for the dust opacity. The observed flux density at the different wavelengths is fitted by posing constraints on the disk structure and on the radial variation of the grain size distribution. Results. We apply the analysis to observations of three protoplanetary disks (AS 209, FT Tau, DR Tau) for which a combination of spatially resolved observations in the range similar to 0.88 mm to similar to 10 mm is available from SMA, CARMA, and VLA. In these disks we find evidence of a decrease in the maximum dust grain size, a(max), with radius. We derive large a(max) values up to 1 cm in the inner disk 15 AU <= R <= 30 AU and smaller grains with a(max) similar to 1 mm in the outer disk (R greater than or similar to 80 AU). Our analysis of the AS 209 protoplanetary disk confirms previous literature results showing a(max) decreasing with radius. Conclusions. Theoretical studies of planetary formation through grain growth are plagued by the lack of direct information on the radial distribution of the dust grain size. In this paper we develop a multiwavelength analysis that will allow this missing quantity to be constrained for statistically relevant samples of disks and to investigate possible correlations with disk or stellar parameters. C1 [Tazzari, M.; Testi, L.] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Tazzari, M.; Testi, L.; Ercolano, B.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Testi, L.; Natta, A.] INAF Osservatorio Astrofis Arcetri, Largo Fermi 5, I-50125 Florence, Italy. [Ercolano, B.] Univ Sternwarte Munchen, Scheinerstr 1, D-81679 Munich, Germany. [Natta, A.] Dublin Inst Adv Studies, Sch Cosm Phys, 31 Fitzwilliam Pl, Dublin 2, Ireland. [Isella, A.] Rice Univ, Dept Phys & Astron, 6100 Main St, Houston, TX 77005 USA. [Chandler, C. J.; Perez, L. M.] Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA. [Andrews, S.; Wilner, D. J.; Ricci, L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Henning, T.; Linz, H.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Kwon, W.] Korea Astron & Space Sci Inst, 776 Daedeok Daero, Daejeon 34055, South Korea. [Corder, S. A.] Joint ALMA Observ JAO, Ave Alonso de Cordova 3107, Santiago, Chile. [Dullemond, C. P.] Heidelberg Univ, Inst Theoret Astrophys, Albert Ueberle Str 2, D-69120 Heidelberg, Germany. [Carpenter, J. M.; Sargent, A. I.] CALTECH, Dept Astron, MC 249-17, Pasadena, CA 91125 USA. [Mundy, L.; Storm, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Calvet, N.] Univ Michigan, Dept Astron, 830 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA. [Greaves, J. A.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Lazio, J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Deller, A. T.] Netherlands Inst Radio Astron ASTRON, NL-7990 Dwingeloo, Netherlands. RP Tazzari, M (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.; Tazzari, M (reprint author), Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. EM mtazzari@eso.org OI Tazzari, Marco/0000-0003-3590-5814; Deller, Adam/0000-0001-9434-3837 FU DFG cluster of excellence Origin and Structure of the Universe; NSF [AST-1109334/1535809]; NASA Origins of Solar Systems program [NNX14AD26G]; Italian Ministero dell' Istruzione, Universita e Ricerca through Progetti Premiali - iALMA [CUP C52I13000140001] FX M.T. and L.T. acknowledge support by the DFG cluster of excellence Origin and Structure of the Universe (http://www.universe-cluster.de). A. I. acknowledges support from the NSF award AST-1109334/1535809 and from the NASA Origins of Solar Systems program through the award number NNX14AD26G. The fits have been carried out on the computing facilities of the Computational Center for Particle and Astrophysics (C2PAP) as part of the approved project "Dust evolution in protoplanetary disks". M.T. and L.T. are grateful for the experienced support from F. Beaujean (C2PAP). M.T. thanks I. Jimenez-Serra, P. Papadopoulos, C. Manara and L. Loreta for the precious support throughout this work. Figures have been generated using the Python-based matplotlib package (Hunter 2007). Staircase plots of PDFs have been generated with a user-modified version of the Python-based triangle package (Foreman-Mackey et al. 2014). Plots of the residuals have been generated with APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This work was partly supported by the Italian Ministero dell' Istruzione, Universita e Ricerca through the grant Progetti Premiali 2012 - iALMA (CUP C52I13000140001). NR 82 TC 7 Z9 7 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 APR PY 2016 VL 588 AR A53 DI 10.1051/0004-6361/201527423 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI0SQ UT WOS:000373207800065 ER PT J AU Ribeiro, SP Basset, Y AF Ribeiro, Servio P. Basset, Yves TI Effects of sclerophylly and host choice on gall densities and herbivory distribution in an Australian subtropical forest SO AUSTRAL ECOLOGY LA English DT Article DE canopy-understorey gradient; gall density; hypothesis of harsh environment; Lamington National Park; leaf herbivory; plant-herbivore interactions; sclerophyllous habitats ID SPECIES RICHNESS; RAIN-FOREST; ADAPTIVE SIGNIFICANCE; TROPICAL FOREST; LEAF STRUCTURE; PLANT; GRADIENTS; INSECTS; PATTERNS; AGE AB We hypothesize that upper canopies contrast with the understorey vegetation in gall density and survival because of greater mortality in the latter. We expect that high sclerophylly rates in the upper canopy leaves are a main cause of such pattern, and more important than other environmental traits, for instance related to altitude. The study was conducted in Lamington National Park, Queensland, Australia. Four independent vertical cylindrical transects through the forest canopy and one equivalent, horizontal understorey transect (20m long and 1m in diameter) were sampled at different altitude (300, 700, 900 and 1100m above sea level) during two seasons. Total and damaged leaves were counted, and galls were collected and opened to determine if they were alive or what may have been the cause of death. Sclerophylly was estimated as specific foliar mass. Out of 72 sampled plant species, 29 presented galls, of which the greatest densities were concentrated on seven host species. A significant increase in sclerophylly with increasing canopy stratum height was observed, but had no direct effect on gall distribution. Total and live galls were more abundant in the canopy than in the understorey for all altitudes but 300m, where a specific infestation on saplings of the canopy tree Arytera divaricata occurred. We found a positive gall establishment and survivorship in the upper canopy, along with a decrease in chewing herbivory, which resulted in decreasing risks of gall death by herbivory. An overall high sclerophylly rate in both canopy and understorey and the total number of galled host species suggest that the plant community studied is prone to gall establishment and evolution. However, a few hosts species with extreme infestation, such as A.divaricata and Ficus watkinsiana, override the community-wide effect of sclerophylly. Our results emphasize how scarce and patchy distributed galls are. C1 [Ribeiro, Servio P.] ICEB Univ Fed Ouro Preto, Lab Evolutionary Ecol Canopy Insects, Dept Biodivers Evolut & Environm, Ouro Preto, Minas Gerais, Brazil. [Basset, Yves] Smithsonian Trop Res Inst, Panama City, Panama. [Basset, Yves] Univ Panama, Maestria Entomol, Panama City, Panama. [Basset, Yves] Univ South Bohemia, Fac Biol, Ceske Budejovice, Czech Republic. RP Ribeiro, SP (reprint author), ICEB Univ Fed Ouro Preto, Lab Evolutionary Ecol Canopy Insects, Dept Biodivers Evolut & Environm, Ouro Preto, Minas Gerais, Brazil. EM spribeiro@iceb.ufop.br RI Basset, Yves/B-6642-2014 FU Queensland Government Smart State Grant; Griffith University; Queensland Museum; Queensland Herbarium; Natural Resource Management Queensland; Queensland National Parks Association; Global Canopy Programme (Oxford); Fundacao de Amparo a Pesquisa de Minas Gerais; Brazilian Council for Science and Technology, CNPq; Czech Science Foundation [41-14-36068G] FX We thank Roger Kitching for organizing the IBISCA-Queensland programme and for reviewing the text. Further Roger has been and still is an inspiration to S. R. and Y. B. over a number of years. Sarah Boulter reviewed the text and helped with field work. We thank also Milton Barbosa for climbing and field services. We are also grateful to Stefan Curtis, Jankees van der Have, Sarah Maunsell, Daniel Pamin and Kalsum Mohd Yusah for contributions to the field work. The project was funded by a Queensland Government Smart State Grant operated by the Department of State Development, with additional support from Griffith University, the Queensland Museum, Queensland Herbarium, Natural Resource Management Queensland, the Queensland National Parks Association and the Global Canopy Programme (Oxford). The British Foreign and Commonwealth Office in Brazil provided M. B. the climbing gear; the Universidade Federal de Ouro Preto and the Post-Graduate Programme in Ecology of Tropical Biomes provided M. B. the training in climbing techniques. Fundacao de Amparo a Pesquisa de Minas Gerais and the Brazilian Council for Science and Technology, CNPq, funded S. P. R. Y. B. is member of the Sistema Nacional de Investigacion of the SENACYT in Panama, and was supported by Czech Science Foundation GACR grant 41-14-36068G. NR 40 TC 0 Z9 0 U1 7 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1442-9985 EI 1442-9993 J9 AUSTRAL ECOL JI Austral Ecol. PD APR PY 2016 VL 41 IS 2 BP 219 EP 226 DI 10.1111/aec.12329 PG 8 WC Ecology SC Environmental Sciences & Ecology GA DJ6EA UT WOS:000374301600011 ER PT J AU Pinson, JB Schuettpelz, E AF Pinson, Jerald B. Schuettpelz, Eric TI Unraveling the origin of the Appalachian gametophyte, Vittaria appalachiana SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Appalachian Mountains; nuclear DET1; hybridization; independent gametophytes; leptosporangiate ferns; plastid genes; polyploidy; Pteridaceae ID EASTERN UNITED-STATES; INDEPENDENT FERN GAMETOPHYTES; MATERNAL INHERITANCE; PTERIDACEAE; PHYLOGENY; DISPERSAL; HYMENOPHYLLACEAE; CHLOROPLAST; PROPAGULES; EVOLUTION AB PREMISE OF STUDY: Ferns and lycophytes are distinct among plants in producing two free-living life stages: a long-lived sporophyte phase and a (usually) short-lived gametophyte phase. Notably, however, some species have perennial, vegetatively reproducing gametophytes. Vittaria appalachiana is one of just three species in which mature sporophytes are unknown. It has a wide range throughout the Appalachian Mountains and Plateau, where it reproduces asexually via gemmae. The origin of V. appalachiana, however, has long been a mystery, with most previous studies suggesting it may have resulted from hybridization of two closely related Vittaria species (V. graminifolia and V. lineata). METHODS: A four-gene plastid data set including 32 samples of six Vittaria species, plus samples of five outgroup species, was analyzed to uncover phylogenetic relationships. Additional analyses of nuclear DET1 gene sequences allowed for the examination of hypotheses involving a hybrid origin for V. appalachiana. KEY RESULTS: In the plastid phylogeny, V. appalachiana is well supported as monophyletic, but is embedded within V. graminifolia. With the exception of a single aberrant allele, this result is mirrored in the nuclear tree. CONCLUSIONS: Through analyses of plastid and nuclear data sets, this study demonstrates that a hybrid origin for V. appalachiana is unlikely. Instead, it appears that this species emerged from within the V. graminifolia lineage. Further work is needed to fully elucidate the genetic structure within this group. C1 [Pinson, Jerald B.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Schuettpelz, Eric] Smithsonian Inst, Dept Bot, MRC 166 POB 37012, Washington, DC 20013 USA. RP Pinson, JB (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM jbp4166@ufl.edu OI Schuettpelz, Eric/0000-0003-3891-9904 FU U. S. National Science Foundation [DEB-1145925, DEB-1405181] FX The authors thank Marcel Van Tuinen and Brian Arbogast for their valuable input on an earlier version of this manuscript as well as two anonymous reviewers for their comments and suggestions. Sally Chambers, Michael Kessler, Fernando Matos, Joel Nitta, Jefferson Prado, Tom Ranker, Carl Rothfels, and Michael Sundue kindly provided silica-dried material for analysis. The acquisition of new material was facilitated by the U. S. National Park Service, the Kentucky Department of Parks, the U. S. Department of Agriculture, the Georgia Department of Natural Resources, the West Virginia Department of Parks and Recreation, the Ohio Division of Natural Areas and Preserves, Panama Rocks, Rock City Park, and the Kentucky State Nature Preserves Commission. Layne Huiet shared unpublished primer sequences. Funding for this research was provided in part by the U. S. National Science Foundation (grants DEB-1145925 and DEB-1405181 to E.S.). NR 46 TC 3 Z9 3 U1 1 U2 2 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 APR PY 2016 VL 103 IS 4 BP 668 EP 676 DI 10.3732/ajb.1500522 PG 9 WC Plant Sciences SC Plant Sciences GA DJ3ZA UT WOS:000374144000011 PM 27033317 ER PT J AU Binder, B Williams, BF Kong, AKH Gaetz, TJ Plucinsky, PP Skillman, ED Dolphin, A AF Binder, B. Williams, B. F. Kong, A. K. H. Gaetz, T. J. Plucinsky, P. P. Skillman, E. D. Dolphin, A. TI Recurring X-ray outbursts in the supernova impostor SN 2010da in NGC 300 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: early-type; stars: massive; X-rays: binaries X-rays: individual: SN 2010da ID STAR-FORMATION HISTORIES; LUMINOUS BLUE VARIABLES; ETA-CARINAE; MILKY-WAY; BINARIES; EMISSION; GALAXY; TRANSIENTS; CLUSTERS; I. AB We present new observations of the 'supernova impostor' SN 2010da using the Chandra X-ray Observatory and the Hubble Space Telescope. During the initial 2010 outburst, the 0.3-10 keV luminosity was observed by Swift to be similar to 5 x 10(38) erg s(-1) and faded by a factor of similar to 25 in a four month period. Our two new Chandra observations show a factor of similar to 10 increase in the 0.35-8 keV X-ray luminosity, from similar to 4 x 10(36) to 4 x 10(37) erg s(-1) in similar to 6 months, and the X-ray spectrum is consistent in both observations with a power-law with a photon index of I" similar to 0. We find evidence of X-ray spectral state changes: when SN 2010da is in a high-luminosity state, the X-ray spectrum is harder (I" similar to 0) compared to the low-luminosity state (I" similar to 1.2 +/- A 0.8). Using our Hubble observations, we fit the colour-magnitude diagram of the coeval stellar population to estimate a time since formation of the SN 2010da progenitor system of a parts per thousand(2)5 Myr. Our observations are consistent with SN 2010da being a high-mass X-ray binary (HMXB) composed of a neutron star and a luminous blue variable-like companion, although we cannot rule out the possibility that SN 2010da is an unusually X-ray bright massive star. The a parts per thousand(2)5 Myr age is consistent with the theoretically predicted delay time between the formation of a massive binary and the onset of the HMXB phase. It is possible that the initial 2010 outburst marked the beginning of X-ray production in the system, making SN 2010da possibly the first massive progenitor binary ever observed to evolve into an HMXB. C1 [Binder, B.; Williams, B. F.] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. [Kong, A. K. H.] Natl Tsing Hua Univ, Dept Phys, Inst Astron, Hsinchu 30013, Taiwan. [Gaetz, T. J.; Plucinsky, P. P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Skillman, E. D.] Univ Minnesota, Dept Astron, 116 Church St SE, Minneapolis, MN 55455 USA. [Dolphin, A.] Raytheon Co, Tucson, AZ 85734 USA. RP Binder, B (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM bbinder@uw.edu FU National Aeronautics and Space Administration through Chandra Award by the Chandra X-ray Observatory Center [G04-15088X]; National Aeronautics and Space Administration [NAS8-03060]; NASA [NAS8-03060]; National Aeronautics and Space Administration FX We would like to thank the anonymous referee for suggestions that helped improve this manuscript. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G04-15088X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics and Space Administration under contract NAS8-03060. TJG and PPP acknowledge support under NASA contract NAS8-03060. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France. NR 70 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 APR 1 PY 2016 VL 457 IS 2 BP 1636 EP 1643 DI 10.1093/mnras/stw119 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI6AB UT WOS:000373580500040 ER PT J AU Cuesta, AJ Vargas-Magana, M Beutler, F Bolton, AS Brownstein, JR Eisenstein, DJ Gil-Marin, H Ho, S McBride, CK Maraston, C Padmanabhan, N Percival, WJ Reid, BA Ross, AJ Ross, NP Sanchez, AG Schlegel, DJ Schneider, DP Thomas, D Tinker, J Tojeiro, R Verde, L White, M AF Cuesta, Antonio J. Vargas-Magana, Mariana Beutler, Florian Bolton, Adam S. Brownstein, Joel R. Eisenstein, Daniel J. Gil-Marin, Hector Ho, Shirley McBride, Cameron K. Maraston, Claudia Padmanabhan, Nikhil Percival, Will J. Reid, Beth A. Ross, Ashley J. Ross, Nicholas P. Sanchez, Ariel G. Schlegel, David J. Schneider, Donald P. Thomas, Daniel Tinker, Jeremy Tojeiro, Rita Verde, Licia White, Martin TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the correlation function of LOWZ and CMASS galaxies in Data Release 12 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; POWER-SPECTRUM ANALYSIS; FINAL DATA; DISTANCE MEASUREMENTS; SAMPLE; TELESCOPE; SCALE; I.; RECONSTRUCTION; CONSTRAINTS AB We present distance scale measurements from the baryon acoustic oscillation signal in the constant stellar mass and low-redshift sample samples from the Data Release 12 of the Baryon Oscillation Spectroscopic Survey. The total volume probed is 14.5 Gpc(3), a 10 per cent increment from Data Release 11. From an analysis of the spherically averaged correlation function, we infer a distance to z = 0.57 of Mpc and a distance to z = 0.32 of Mpc assuming a cosmology in which Mpc. From the anisotropic analysis, we find an angular diameter distance to z = 0.57 of Mpc and a distance to z = 0.32 of 981 +/- 20 Mpc, a 1.5 and 2.0 per cent measurement, respectively. The Hubble parameter at z = 0.57 is km s(-1) Mpc(-1) and its value at z = 0.32 is 79.2 +/- 5.6 km s(-1) Mpc(-1), a 3.7 and 7.1 per cent measurement, respectively. These cosmic distance scale constraints are in excellent agreement with a I > cold dark matter model with cosmological parameters released by the recent Planck 2015 results. C1 [Cuesta, Antonio J.; Verde, Licia] Univ Barcelona IEEC UB, Inst Ciencies Cosmos ICCUB, Marti & Franques 1, E-02028 Barcelona, Spain. [Vargas-Magana, Mariana] Univ Nacl Autonoma Mexico, Inst Fis, POB 20-364, Mexico City 01000, DF, Mexico. [Vargas-Magana, Mariana; Ho, Shirley] Carnegie Mellon Univ, Dept Phys, Bruce & Astrid McWilliams Ctr, 5000 Forbes Ave, Pittsburgh, PA 15213 USA. [Vargas-Magana, Mariana; Ho, Shirley] Carnegie Mellon Univ, Dept Phys, 5000 Forbes Ave, Pittsburgh, PA 15217 USA. [Beutler, Florian; Reid, Beth A.; Schlegel, David J.; White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Beutler, Florian; Reid, Beth A.; Schlegel, David J.; White, Martin] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Bolton, Adam S.; Brownstein, Joel R.] Univ Utah, Dept Phys & Astron, 115 S 1400 E, Salt Lake City, UT 84112 USA. [Eisenstein, Daniel J.; McBride, Cameron K.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Gil-Marin, Hector; Maraston, Claudia; Percival, Will J.; Thomas, Daniel] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England. [Padmanabhan, Nikhil] Yale Univ, Dept Phys, 260 Whitney Ave, New Haven, CT 06520 USA. [Ross, Ashley J.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. [Ross, Nicholas P.] Univ Edinburgh, Royal Observ, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ross, Nicholas P.] Drexel Univ, Dept Phys, 3141 Chestnut St, Philadelphia, PA 19104 USA. [Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [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. [Tinker, Jeremy] CUNY, Dept Phys, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. [Tojeiro, Rita] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Verde, Licia] Passeig Lluis Co, ICREA, E-2308010 Barcelona, Spain. [Verde, Licia] Harvard Univ, Radcliffe Inst Adv Study, Cambridge, MA 02138 USA. [Verde, Licia] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [White, Martin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. RP Cuesta, AJ (reprint author), Univ Barcelona IEEC UB, Inst Ciencies Cosmos ICCUB, Marti & Franques 1, E-02028 Barcelona, Spain. EM ajcuesta@icc.ub.edu RI White, Martin/I-3880-2015; Gil Marin, Hector/B-2013-2017; OI White, Martin/0000-0001-9912-5070; Gil Marin, Hector/0000-0003-0265-6217; Beutler, Florian/0000-0003-0467-5438; Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470; Verde, Licia/0000-0003-2601-8770 FU European Research Council under the European Community [FP7-IDEAS-Phys.LSS 240117]; Spanish MINECO of ICCUB (Unidad de Excelencia 'Maria de Maeztu') [AYA2014-58747-P, MDM-2014-0369]; ESA; NASA; Alfred P. Sloan Foundation; National Science Foundation; US 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; Office of Science of the US Department of Energy [DEAC02-05CH11231]; Science, Technology and Facilities Council [ST/I001204/1] FX AJC and LV are supported by supported by the European Research Council under the European Community's Seventh Framework Programme FP7-IDEAS-Phys.LSS 240117. Funding for this work was partially provided by the Spanish MINECO under projects AYA2014-58747-P and MDM-2014-0369 of ICCUB (Unidad de Excelencia 'Maria de Maeztu').; Based on observations obtained with Planck (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada.; 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, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.; This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department of Energy under Contract no. DEAC02-05CH11231. Power spectrum computations were supported by the facilities and staff of the UK Sciama High Performance Computing cluster supported by SEPNet and the University of Portsmouth. Power spectrum calculations, and fitting made use of the COSMOS/Universe supercomputer, a UK-CCC facility supported by HEFCE and STFC in cooperation with CGI/Intel.; The Science, Technology and Facilities Council is acknowledged for support through the Survey Cosmology and Astrophysics consolidated grant, ST/I001204/1. NR 59 TC 26 Z9 26 U1 4 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 1 PY 2016 VL 457 IS 2 BP 1770 EP 1785 DI 10.1093/mnras/stw066 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI6AB UT WOS:000373580500052 ER PT J AU Spingola, C Dallacasa, D Orienti, M Giroletti, M McKean, JP Cheung, CC Hovatta, T Ciprini, S D'Ammando, F Falco, E Larsson, S Max-Moerbeck, W Ojha, R Readhead, ACS Richards, JL Scargle, J AF Spingola, C. Dallacasa, D. Orienti, M. Giroletti, M. McKean, J. P. Cheung, C. C. Hovatta, T. Ciprini, S. D'Ammando, F. Falco, E. Larsson, S. Max-Moerbeck, W. Ojha, R. Readhead, A. C. S. Richards, J. L. Scargle, J. TI Radio follow-up of the gamma-ray flaring gravitational lens JVAS B0218+357 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: strong; quasars: individual: JVAS B0218+357 ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; BLAZAR PKS 1830-211; ALL-SKY SURVEY; SUPERLUMINAL MOTION; SYSTEM B0218+357; BRIGHT BLAZARS; EINSTEIN RING; TIME-DELAY; VARIABILITY AB We present results on multifrequency Very Long Baseline Array (VLBA) monitoring observations of the double-image gravitationally lensed blazar JVAS B0218+357. Multi-epoch observations started less than one month after the gamma-ray flare detected in 2012 by the Large Area Telescope on board Fermi, and spanned a 2-month interval. The radio light curves did not reveal any significant flux density variability, suggesting that no clear correlation between the high-energy and low-energy emission is present. This behaviour was confirmed also by the long-term Owens Valley Radio Observatory monitoring data at 15 GHz. The milliarcsecond-scale resolution provided by the VLBA observations allowed us to resolve the two images of the lensed blazar, which have a core-jet structure. No significant morphological variation is found by the analysis of the multi-epoch data, suggesting that the region responsible for the gamma-ray variability is located in the core of the active galactic nuclei, which is opaque up to the highest observing frequency of 22 GHz. C1 [Spingola, C.; Dallacasa, D.; D'Ammando, F.] Univ Bologna, Dipartmento Astron, Via Ranzani 1, I-40127 Bologna, Italy. [Spingola, C.; Dallacasa, D.; Orienti, M.; Giroletti, M.; D'Ammando, F.] INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. [Spingola, C.; McKean, J. P.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. [McKean, J. P.] Netherlands Inst Radio Astron ASTRON, POB 2, NL-7990 AA Dwingeloo, Netherlands. [Cheung, C. C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Hovatta, T.] Aalto Univ Metsahovi Radio Observ, Metsahovintie 114, FI-02540 Kylmala, Finland. [Ciprini, S.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy. [Ciprini, S.] Ist Nazl Astrofis, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Roma, Italy. [Falco, E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Larsson, S.] KTH Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, S.] AlbaNova, Oscar Klein Ctr, SE-10691 Stockholm, Sweden. [Larsson, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Max-Moerbeck, W.] Natl Radio Astron Observ, POB 0, Socorro, NM 87801 USA. [Ojha, R.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Ojha, R.] Univ Maryland Baltimore Cty, 1000 Hilltop Circle, Baltimore, MD 21250 USA. [Ojha, R.] Catholic Univ Amer, 620 Michigan Ave NE, Washington, DC 20064 USA. [Readhead, A. C. S.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Richards, J. L.] Purdue Univ, Dept Phys & Astron, 525 Northwestern Ave, W Lafayette, IN 47907 USA. [Scargle, J.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Spingola, C; Dallacasa, D (reprint author), Univ Bologna, Dipartmento Astron, Via Ranzani 1, I-40127 Bologna, Italy.; Spingola, C; Dallacasa, D; Orienti, M (reprint author), INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy.; Spingola, C (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. EM spingola@astro.rug.nl; ddallaca@ira.inaf.it; orienti@ira.inaf.it OI Spingola, Cristiana/0000-0002-2231-6861 FU National Aeronautics and Space Administration; NASA Guest Investigator programme [13-FERMI13-0009]; Royal Swedish Academy Crafoord Foundation; NASA [NNX08AW31G, NNX11A043G]; NSF [AST-0808050, AST-1109911]; NASA through Fermi Guest Investigator grants [NNH09ZDA001N, NNH10ZDA001N, NNH12ZDA001N, NNH13ZDA001N-FERMI] FX The VLBA is operated by the US National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under a cooperative agreement by Associated University, Inc., under contract with the National Science Foundation. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.; CCC was supported at NRL by NASA Guest Investigator programme 13-FERMI13-0009. SL was supported by the Royal Swedish Academy Crafoord Foundation. We thank the NRAO Schedsoc for approving our request and Mark Claussen for facilitating the VLBA scheduling. The OVRO 40-m monitoring programme is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST-1109911.; This research was funded in part by NASA through Fermi Guest Investigator grants NNH09ZDA001N, NNH10ZDA001N, NNH12ZDA001N, NNH13ZDA001N-FERMI. This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 44 TC 4 Z9 4 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 1 PY 2016 VL 457 IS 2 BP 2263 EP 2271 DI 10.1093/mnras/stw136 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI6AB UT WOS:000373580500086 ER PT J AU Lefcheck, JS Brandl, SJ Reynalds, PL Smyth, AR Meyer, ST AF Lefcheck, Jonathan S. Brandl, Simon J. Reynalds, Pamela L. Smyth, Ashley R. Meyer, Sebastian T. TI Extending Rapid Ecosystem Function Assessments to Marine Ecosystems: A Reply to Meyer SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Letter ID BIODIVERSITY; DIVERSITY C1 [Lefcheck, Jonathan S.; Reynalds, Pamela L.; Smyth, Ashley R.] Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA. [Brandl, Simon J.] Smithsonian Environm Res Ctr, Tennenbaum Marine Observ Network, POB 28, Edgewater, MD 21037 USA. [Reynalds, Pamela L.] Univ Calif Davis, Davis, CA 95616 USA. [Meyer, Sebastian T.] Tech Univ Munich, Ctr Food & Life Sci Weihenstephan, Dept Ecol & Ecosyst Management, Terr Ecol Res Grp, Hans Carl von Carlowitz Pl 2, D-85354 Frelsing, Germany. RP Lefcheck, JS (reprint author), Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA. EM jslefche@vims.edu OI Lefcheck, Jonathan/0000-0002-8787-1786; Brandl, Simon/0000-0002-6649-2496 NR 12 TC 1 Z9 1 U1 3 U2 16 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD APR PY 2016 VL 31 IS 4 BP 251 EP 253 DI 10.1016/j.tree.2016.02.002 PG 3 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA DJ4TC UT WOS:000374199900001 PM 26922421 ER PT J AU Tilley, A Carter, E Wassermann, S Lopez-Angarita, J AF Tilley, Alexander Carter, Elliott Wassermann, Sophia Lopez-Angarita, Juliana TI Enhancing management effectiveness of invasive lionfish using distance sampling and detection probability SO AQUATIC CONSERVATION-MARINE AND FRESHWATER ECOSYSTEMS LA English DT Article DE coral; reef; conservation evaluation; ecological status; fish; alien species ID INDO-PACIFIC LIONFISH; PTEROIS SPP.; RED LIONFISH; CORAL-REEFS; ATLANTIC; DENSITY; SCORPAENIDAE; PREDATION; ABUNDANCE; TRANSECT AB 1. Invasive lionfish Pterois volitans and Pterois miles are one of the greatest threats to coral reef fisheries in the Caribbean. Management currently relies solely on removal, however, there is little understanding of spatial ecology of lionfish to inform management strategies and thus, increase their effectiveness. 2. The use of detection probability and population density estimates from distance sampling as a method to: (a) estimate spatial and depth variations in detectability of lionfish to prioritize removal efforts; (b) reduce costs related to removal in the Caribbean; and (c) provide quantifiable baseline data against which management success can be measured was evaluated. 3. Underwater visual transect surveys were conducted at varying depths at four coral reef sites in the Turks and Caicos Islands using perpendicular distance sampling. Detection functions were fitted to distance data from 299 lionfish sightings across 37 transects to explore variation in detectability among survey sites and depths. 4. Lionfish were detected with a 15.9% (12.2- 20.6%) (mean 95% CI) probability across all sampling. Detection probability was significantly higher in depths < 15 m, however, lionfish density and mean size increased with depth. Population density on South Caicos reefs was estimated at 1679 (1140.4- 2473.1) individuals per km2. Increased detection probability in shallower depths implies caution is needed in assessing management success at depth, and that removal methods and effort should be related specifically to depth and habitat factors. 5. Distance sampling is an effective method for accurate estimation of lionfish population density and detection probability, providing metrics by which to identify priority management areas, and track population changes along with the success of removal efforts. As a result its integration into initial planning and continued monitoring aspects of lionfish management throughout the Caribbean is recommended. Copyright # 2015 John Wiley & Sons, Ltd. C1 [Tilley, Alexander; Lopez-Angarita, Juliana] Fdn Talking Oceans, Bogota, Colombia. [Tilley, Alexander] Smithsonian Marine Stn, Ft Pierce, FL USA. [Tilley, Alexander; Carter, Elliott; Wassermann, Sophia] Ctr Marine Resource Studies, Sch Field Studies, South Caicos, Turks & Caicos, England. [Carter, Elliott; Wassermann, Sophia] Davidson Coll, 204 Ridge Rd, Davidson, NC 28036 USA. [Lopez-Angarita, Juliana] Univ York, Dept Environm, York YO10 5DD, N Yorkshire, England. RP Tilley, A (reprint author), Fdn Talking Oceans, Bogota, Colombia. EM alex@talking-oceans.org OI Tilley, Alexander/0000-0002-6363-0945; Lopez-Angarita, Juliana/0000-0002-8725-0795 NR 41 TC 0 Z9 0 U1 29 U2 51 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1052-7613 EI 1099-0755 J9 AQUAT CONSERV JI Aquat. Conserv.-Mar. Freshw. Ecosyst. PD APR PY 2016 VL 26 IS 2 BP 279 EP 288 DI 10.1002/aqc.2549 PG 10 WC Environmental Sciences; Marine & Freshwater Biology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA DJ1IT UT WOS:000373957200006 ER PT J AU Broderick, AE Fish, VL Johnson, MD Rosenfeld, K Wang, C Doeleman, SS Akiyama, K Johannsen, T Roy, AL AF Broderick, Avery E. Fish, Vincent L. Johnson, Michael D. Rosenfeld, Katherine Wang, Carlos Doeleman, Sheperd S. Akiyama, Kazunori Johannsen, Tim Roy, Alan L. TI MODELING SEVEN YEARS OF EVENT HORIZON TELESCOPE OBSERVATIONS WITH RADIATIVELY INEFFICIENT ACCRETION FLOW MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; Galaxy: center; submillimeter: general; techniques: high angular resolution; techniques: interferometric ID SAGITTARIUS-A-ASTERISK; MASSIVE BLACK-HOLE; SCATTER-BROADENED IMAGE; GALACTIC-CENTER; STELLAR ORBITS; YOUNG STARS; LINEAR-POLARIZATION; SGR J1745-29; SIMULATIONS; DISK AB An initial three-station version of the Event Horizon Telescope, a millimeter-wavelength very-along baseline interferometer, has observed Sagittarius A* (Sgr A*) repeatedly from 2007 to 2013, resulting in the measurement of a variety of interferometric quantities. Of particular importance is that there is now a large set of closure phases measured over a number of independent observing epochs. We analyze these observations within the context of a realization of semi-analytic radiatively inefficient disk models, implicated by the low luminosity of Sgr. A*. We find a broad consistency among the various observing epochs and between different interferometric data types, with the latter providing significant support for this class of model of Sgr. A*. The new data significantly tighten existing constraints on the spin magnitude and its orientation within this model context, finding a spin magnitude of a = 0.10(0.10)(0.10)(+0.30)(+0.56), an inclination with respect to the line of sight of theta = 60 degrees(+5 degrees)(+10 degrees)(8 degrees)(13 degrees), and a position angle of xi = 156 degrees(+10 degrees)(+14 degrees)(-17 degrees)(-27 degrees) east of north. These are in good agreement with previous analyses. Notably, the previous 180 degrees degeneracy in the position angle has now been conclusively broken by the inclusion of the closure-aphase measurements. A reflection degeneracy in the inclination remains, permitting two localizations of the spin vector orientation, one of which is in agreement with the orbital angular momentum of the infrared gas cloud G2 and the clockwise disk of young stars. This may support a relationship between Sgr. A*'s accretion flow and these larger-scale features. C1 [Broderick, Avery E.; Johannsen, Tim] Perimeter Inst Theoret Phys, 31 Caroline St North, Waterloo, ON N2L 2Y5, Canada. [Broderick, Avery E.; Wang, Carlos; Johannsen, Tim] Univ Waterloo, Dept Phys & Astron, 200 Univ Ave West, Waterloo, ON N2L 3G1, Canada. [Fish, Vincent L.; Doeleman, Sheperd S.; Akiyama, Kazunori] MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. [Johnson, Michael D.; Rosenfeld, Katherine; Doeleman, Sheperd S.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Akiyama, Kazunori] Natl Astron Observ Japan, Osawa 2-21-1, Mitaka, Tokyo 1818588, Japan. [Akiyama, Kazunori] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. [Johannsen, Tim] Univ Toronto, Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada. [Roy, Alan L.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. RP Broderick, AE (reprint author), Perimeter Inst Theoret Phys, 31 Caroline St North, Waterloo, ON N2L 2Y5, Canada.; Broderick, AE (reprint author), Univ Waterloo, Dept Phys & Astron, 200 Univ Ave West, Waterloo, ON N2L 3G1, Canada. FU Perimeter Institute for Theoretical Physics; Natural Sciences and Engineering Research Council of Canada; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research and Innovation FX A.E.B. receives financial support from the Perimeter Institute for Theoretical Physics and the Natural Sciences and Engineering Research Council of Canada through a Discovery Grant. 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 Research and Innovation. NR 63 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2016 VL 820 IS 2 AR 137 DI 10.3847/0004-637X/820/2/137 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI8HE UT WOS:000373741300056 ER PT J AU Fish, VL Johnson, MD Doeleman, SS Broderick, AE Psaltis, D Lu, RS Akiyama, K Alef, W Algaba, JC Asada, K Beaudoin, C Bertarini, A Blackburn, L Blundell, R Bower, GC Brinkerink, C Cappallo, R Chael, AA Chamberlin, R Chan, CK Crew, GB Dexter, J Dexter, M Dzib, SA Falcke, H Freund, R Friberg, P Greer, CH Gurwell, MA Ho, PTP Honma, M Inoue, M Johannsen, T Kim, J Krichbaum, TP Lamb, J Leon-Tavares, J Loeb, A Loinard, L MacMahon, D Marrone, DP Moran, JM Moscibrodzka, M Ortiz-Leon, GN Oyama, T Ouml;zel, F Plambeck, RL Pradel, N Primiani, RA Rogers, AEE Rosenfeld, K Rottmann, H Roy, AL Ruszczyk, C Smythe, DL SooHoo, J Spilker, J Stone, J Strittmatter, P Tilanus, RPJ Titus, M Vertatschitsch, L Wagner, J Wardle, JFC Weintroub, J Woody, D Wright, M Yamaguchi, P Young, A Young, KH Zensus, JA Ziurys, LM AF Fish, Vincent L. Johnson, Michael D. Doeleman, Sheperd S. Broderick, Avery E. Psaltis, Dimitrios Lu, Ru-Sen Akiyama, Kazunori Alef, Walter Algaba, Juan Carlos Asada, Keiichi Beaudoin, Christopher Bertarini, Alessandra Blackburn, Lindy Blundell, Ray Bower, Geoffrey C. Brinkerink, Christiaan Cappallo, Roger Chael, Andrew A. Chamberlin, Richard Chan, Chi-Kwan Crew, Geoffrey B. Dexter, Jason Dexter, Matt Dzib, Sergio A. Falcke, Heino Freund, Robert Friberg, Per Greer, Christopher H. Gurwell, Mark A. Ho, Paul T. P. Honma, Mareki Inoue, Makoto Johannsen, Tim Kim, Junhan Krichbaum, Thomas P. Lamb, James Leon-Tavares, Jonathan Loeb, Abraham Loinard, Laurent MacMahon, David Marrone, Daniel P. Moran, James M. Moscibrodzka, Monika Ortiz-Leon, Gisela N. Oyama, Tomoaki Oezel, Feryal Plambeck, Richard L. Pradel, Nicolas Primiani, Rurik A. Rogers, Alan E. E. Rosenfeld, Katherine Rottmann, Helge Roy, Alan L. Ruszczyk, Chester Smythe, Daniel L. SooHoo, Jason Spilker, Justin Stone, Jordan Strittmatter, Peter Tilanus, Remo P. J. Titus, Michael Vertatschitsch, Laura Wagner, Jan Wardle, John F. C. Weintroub, Jonathan Woody, David Wright, Melvyn Yamaguchi, Paul Young, Andre Young, Ken H. Zensus, J. Anton Ziurys, Lucy M. TI PERSISTENT ASYMMETRIC STRUCTURE OF SAGITTARIUS A* ON EVENT HORIZON SCALES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; submillimeter: general; techniques: high angular resolution; techniques: interferometric ID SUPERMASSIVE BLACK-HOLE; SCATTER-BROADENED IMAGE; BASE-LINE INTERFEROMETRY; S ACCRETION FLOW; NO-HAIR THEOREM; CENTER CLOUD G2; GALACTIC-CENTER; GRMHD SIMULATIONS; VLBI OBSERVATIONS; TELESCOPE OBSERVATIONS AB The Galactic Center black hole Sagittarius. A* (Sgr A*) is a prime observing target for the Event Horizon Telescope (EHT), which can resolve the 1.3 mm emission from this source on angular scales comparable to that of the general relativistic shadow. Previous EHT observations have used visibility amplitudes to infer the morphology of the millimeter-wavelength emission. Potentially much richer source information is contained in the phases. We report on 1.3 mm phase information on Sgr. A* obtained with the EHT on a total of 13 observing nights over four years. Closure phases, which are the sum of visibility phases along a closed triangle of interferometer baselines, are used because they are robust against phase corruptions introduced by instrumentation and the rapidly variable atmosphere. The median closure phase on a triangle including telescopes in California, Hawaii, and Arizona is nonzero. This result conclusively demonstrates that the millimeter emission is asymmetric on scales of a few Schwarzschild radii and can be used to break 180 degrees rotational ambiguities inherent from amplitude data alone. The stability of the sign of the closure phase over most observing nights indicates persistent asymmetry in the image of Sgr. A* that is not obscured by refraction due to interstellar electrons along the line of sight. C1 [Fish, Vincent L.; Doeleman, Sheperd S.; Lu, Ru-Sen; Akiyama, Kazunori; Beaudoin, Christopher; Cappallo, Roger; Crew, Geoffrey B.; Rogers, Alan E. E.; Ruszczyk, Chester; Smythe, Daniel L.; SooHoo, Jason; Titus, Michael] MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. [Johnson, Michael D.; Doeleman, Sheperd S.; Blackburn, Lindy; Blundell, Ray; Chael, Andrew A.; Gurwell, Mark A.; Loeb, Abraham; Moran, James M.; Primiani, Rurik A.; Rosenfeld, Katherine; Vertatschitsch, Laura; Weintroub, Jonathan; Yamaguchi, Paul; Young, Andre; Young, Ken H.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Broderick, Avery E.; Johannsen, Tim] Perimeter Inst Theoret Phys, 31 Caroline St North, Waterloo, ON N2L 2Y5, Canada. [Broderick, Avery E.; Johannsen, Tim] Univ Waterloo, Dept Phys & Astron, 200 Univ Ave West, Waterloo, ON N2L 3G1, Canada. [Psaltis, Dimitrios; Chan, Chi-Kwan; Freund, Robert; Greer, Christopher H.; Kim, Junhan; Marrone, Daniel P.; Oezel, Feryal; Spilker, Justin; Stone, Jordan; Strittmatter, Peter; Ziurys, Lucy M.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [Psaltis, Dimitrios; Chan, Chi-Kwan; Freund, Robert; Greer, Christopher H.; Kim, Junhan; Marrone, Daniel P.; Oezel, Feryal; Spilker, Justin; Stone, Jordan; Strittmatter, Peter; Ziurys, Lucy M.] Univ Arizona, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA. [Lu, Ru-Sen; Alef, Walter; Bertarini, Alessandra; Dzib, Sergio A.; Falcke, Heino; Krichbaum, Thomas P.; Loinard, Laurent; Rottmann, Helge; Roy, Alan L.; Wagner, Jan; Zensus, J. Anton] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Akiyama, Kazunori; Honma, Mareki; Oyama, Tomoaki] Natl Astron Observ Japan, Osawa 2-21-1, Mitaka, Tokyo 1818588, Japan. [Akiyama, Kazunori] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. [Algaba, Juan Carlos; Wagner, Jan] Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 305348, South Korea. [Algaba, Juan Carlos; Asada, Keiichi; Ho, Paul T. P.; Inoue, Makoto] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. [Bertarini, Alessandra] Univ Bonn, Inst Geodesy & Geoinformat, D-53113 Bonn, Germany. [Bower, Geoffrey C.] Acad Sinica, Inst Astron & Astrophys, 645 N Aohoku Pl, Hilo, HI 96720 USA. [Brinkerink, Christiaan; Falcke, Heino; Moscibrodzka, Monika; Tilanus, Remo P. J.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. [Chamberlin, Richard] CALTECH, Submillimeter Observ, 111 Nowelo St, Hilo, HI 96720 USA. [Dexter, Jason] Max Planck Inst Extraterr Phys, Giessenbachstr 1, Garching, Germany. [Dexter, Matt; MacMahon, David; Plambeck, Richard L.; Wright, Melvyn] Univ Calif Berkeley, Dept Astron, Radio Astron Lab, 501 Campbell, Berkeley, CA 94720 USA. [Dzib, Sergio A.; Loinard, Laurent; Ortiz-Leon, Gisela N.] Univ Nacl Autonoma Mexico, Inst Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Falcke, Heino] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Friberg, Per] James Clerk Maxwell Telescope, East Asia Observ, 660 N Aohoku Pl, Hilo, HI 96720 USA. [Honma, Mareki] Grad Univ Adv Studies, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Johannsen, Tim] Univ Toronto, Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada. [Lamb, James; Woody, David] CALTECH, Owens Valley Radio Observ, 100 Leighton Lane, Big Pine, CA 93513 USA. [Leon-Tavares, Jonathan] Inst Nacl Astrofis Opt & Electr, Apartado Postal 51 & 216, Puebla 72000, Mexico. [Leon-Tavares, Jonathan] Univ Ghent, Sterrenkundig Observ, Krijgslaan 281-S9, B-9000 Ghent, Belgium. [Pradel, Nicolas] Auckland Univ Technol, 55 Wellesley St East, Auckland Cent, New Zealand. [Tilanus, Remo P. J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Wardle, John F. C.] Brandeis Univ, Dept Phys, Waltham, MA 02454 USA. RP Fish, VL (reprint author), MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. EM vfish@haystack.mit.edu OI Kim, Junhan/0000-0002-4274-9373; Akiyama, Kazunori/0000-0002-9475-4254; Stone, Jordan/0000-0003-0454-3718; Moran, James/0000-0002-3882-4414 FU National Science Foundation (NSF); Gordon AMP; Betty Moore Foundation [GBMF-3561]; NSF University Radio Observatories program; NSF; CARMA partner universities; Perimeter Institute for Theoretical Physics; Natural Sciences and Engineering Research Council of Canada; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research and Innovation; MEXT/JSPS KAKENHI; DGAPA, Mexico; UNAM, Mexico; CONACyT, Mexico FX The EHT is supported by multiple grants from the National Science Foundation (NSF) and a grant from the Gordon & Betty Moore Foundation (GBMF-3561) to SSD. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics. The ARO is partially supported through the NSF University Radio Observatories program. The JCMT was operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK, the Netherlands Organisation for Scientific Research, and the National Research Council of Canada. Funding for ongoing CARMA development and operations was supported by the NSF and CARMA partner universities. A.E.B. receives financial support from the Perimeter Institute for Theoretical Physics and the Natural Sciences and Engineering Research Council of Canada through a Discovery Grant. 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. M.H. acknowledges support from MEXT/JSPS KAKENHI. L.L. and G.N.O.L. acknowledge the financial support of DGAPA, UNAM, and CONACyT, Mexico. The EHT gratefully acknowledges equipment donations from Xilinx Inc. NR 80 TC 11 Z9 11 U1 3 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 APR 1 PY 2016 VL 820 IS 2 AR 90 DI 10.3847/0004-637X/820/2/90 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI8HE UT WOS:000373741300009 ER PT J AU Kipping, DM Torres, G Henze, C Teachey, A Isaacson, H Petigura, E Marcy, GW Buchhave, LA Chen, J Bryson, ST Sandford, E AF Kipping, D. M. Torres, G. Henze, C. Teachey, A. Isaacson, H. Petigura, E. Marcy, G. W. Buchhave, L. A. Chen, J. Bryson, S. T. Sandford, E. TI A TRANSITING JUPITER ANALOG SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: detection; stars: individual (KIC-3239945, KOI-490, Kepler-167); techniques: photometric ID MULTI-PLANET SYSTEMS; KEPLER INPUT CATALOG; GIANT PLANETS; FALSE POSITIVES; HABITABLE ZONE; SNOW-LINE; EXTRASOLAR PLANETS; BLEND SCENARIOS; HOST STARS; EXOPLANET AB Decadal-long radial velocity surveys have recently started to discover analogs to the most influential planet of our solar system, Jupiter. Detecting and characterizing these worlds is expected to shape our understanding of our uniqueness in the cosmos. Despite the great successes of recent transit surveys, Jupiter analogs represent a terra incognita, owing to the strong intrinsic bias of this method against long orbital periods. We here report on the first validated transiting Jupiter analog, Kepler-167e (KOI-490.02), discovered using Kepler archival photometry orbiting the K4-dwarf KIC-3239945. With a radius of (0.91 +/- 0.02) R-J, a low orbital eccentricity (0.06(-0.04)(+0.10)), and an equilibrium temperature of(131 +/- 3) K, Kepler-167e bears many of the basic hallmarks of Jupiter. Kepler-167e is accompanied by three Super-Earths on compact orbits, which we also validate, leaving a large cavity of transiting worlds around the habitable-zone. With two transits and continuous photometric coverage, we are able to uniquely and precisely measure the orbital period of this post snow-line planet (1071.2323 +/- 0.0006d), paving the way for follow-up of this K = 11.8 mag target. C1 [Kipping, D. M.; Teachey, A.; Chen, J.; Sandford, E.] Columbia Univ, Dept Astron, 550 W 120th St, New York, NY 10027 USA. [Torres, G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Henze, C.; Bryson, S. T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Isaacson, H.; Petigura, E.; Marcy, G. W.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Buchhave, L. A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. RP Kipping, DM (reprint author), Columbia Univ, Dept Astron, 550 W 120th St, New York, NY 10027 USA. EM dkipping@astro.columbia.edu OI Isaacson, Howard/0000-0002-0531-1073 FU NASA [NNX14AB83G, NNX15AF09G] FX This work made use of the Michael Dodds Computing Facility and the Pleiades supercomputer at NASA Ames. G.T. acknowledges partial support for this work from NASA grant NNX14AB83G (Kepler Participating Scientist Program). D.M.K. acknowledges partial support from NASA grant NNX15AF09G (NASA ADAP Program). This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org, and the corner.py code by Dan Foreman-Mackey at github.com/dfm/corner.py. We offer our thanks and praise to the extraordinary scientists, engineers, and individuals who have made the Kepler mission possible. Finally, the authors wish to extend special thanks to those of Hawaiian 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 74 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 APR 1 PY 2016 VL 820 IS 2 AR 112 DI 10.3847/0004-637X/820/2/112 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI8HE UT WOS:000373741300031 ER PT J AU Laporte, N Infante, L Iribarren, PT Zheng, W Molino, A Bauer, FE Bina, D Broadhurst, T Chilingarian, I Garcia, S Kim, S Marques-Chaves, R Moustakas, J Pello, R Perez-Fournon, I Shu, X Streblyanska, A Zitrin, A AF Laporte, N. Infante, L. Troncoso Iribarren, P. Zheng, W. Molino, A. Bauer, F. E. Bina, D. Broadhurst, Tom Chilingarian, I. Garcia, S. Kim, S. Marques-Chaves, R. Moustakas, J. Pello, R. Perez-Fournon, I. Shu, X. Streblyanska, A. Zitrin, A. TI YOUNG GALAXY CANDIDATES IN THE HUBBLE FRONTIER FIELDS. III. MACS. J0717.5+3745 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: individual (MACS. J0717.5+3745); galaxies: high-redshift; gravitational lensing: strong ID STAR-FORMATION RATE; LYMAN-BREAK GALAXIES; ULTRA-DEEP FIELD; SIMILAR-TO 8; SPECTRAL ENERGY-DISTRIBUTIONS; UV LUMINOSITY FUNCTION; HIGH-REDSHIFT GALAXIES; FORMATION RATE DENSITY; EARLY RELEASE SCIENCE; DWARF/L-DWARF BINARIES AB In this paper we present the results of our search for and study of z >= 6 galaxy candidates behind the third Frontier Fields (FFs) cluster, MACS. J0717.5+ 3745, and its parallel field, combining data from Hubble and Spitzer. We select 39 candidates using the Lyman break technique, for which the clear non-detection in optical make the extreme mid-z interlopers hypothesis unlikely. We also take benefit from z >= 6 samples selected using the previous FF data sets of Abell 2744 and MACS. 0416 to improve the constraints on the properties of very high redshift objects. We compute the redshift and the physical properties such emission lines properties, star formation rate, reddening, and stellar mass for all FF objects from their spectral energy distribution using templates including nebular emission lines. We study the relationship between several physical properties and confirm the trend already observed in previous surveys for evolution of star formation rate with galaxy mass and between the size and the UV luminosity of our candidates. The analysis of the evolution of the UV luminosity function with redshift seems more compatible with an evolution of density. Moreover, no robust z >= 8.5 object is selected behind the cluster field and few z similar to 9 candidates have been selected in the two previous data sets from this legacy survey, suggesting a strong evolution in the number density of galaxies between z similar to 8 and 9. Thanks to the use of the lensing cluster, we study the evolution of the star formation rate density produced by galaxies with L > 0.03 L-star, and confirm the strong decrease observed between z similar to 8 and 9. C1 [Laporte, N.; Infante, L.; Troncoso Iribarren, P.; Bauer, F. E.; Kim, S.] Pontificia Univ Catolica Chile, Inst Astrofis, Vicuna Mackenna 4860, Santiago 7820436, Chile. [Laporte, N.; Infante, L.; Troncoso Iribarren, P.; Bauer, F. E.; Garcia, S.] Pontificia Univ Catolica Chile, Ctr Astroingn, Fac Fis, Vicuna Mackenna 4860, Santiago 7820436, Chile. [Troncoso Iribarren, P.; Garcia, S.; Kim, S.] Pontificia Univ Catolica Chile, Ctr Astroingn, Vicuna Mackenna 4860, Santiago 7820436, Chile. [Zheng, W.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Molino, A.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Cidade Univ, BR-05508090 Sao Paulo, Brazil. [Molino, A.] Inst Astrofis Andalucia CSIC, Glorieta Astron S-N, E-18008 Granada, Spain. [Bauer, F. E.] Millennium Inst Astrophys, Vicuna Mackenna 4860, Santiago 7820436, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Bina, D.; Pello, R.] CNRS, IRAP, 14 Ave Edouard Belin, F-31400 Toulouse, France. [Broadhurst, Tom] Univ Basque Country UPV EHU, Dept Theoret Phys, Bilbao, Spain. [Broadhurst, Tom] Basque Fdn Sci, Ikerbasque, Bilbao, Spain. [Chilingarian, I.] Smithsonian Astrophys Observ, 60 Garden St MS09, Cambridge, MA 02138 USA. [Chilingarian, I.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, 13 Univ Sky Prospect, Moscow 119992, Russia. [Marques-Chaves, R.; Perez-Fournon, I.; Streblyanska, A.] IAC, E-38200 Tenerife, Spain. [Marques-Chaves, R.; Perez-Fournon, I.; Streblyanska, A.] ULL, Dept Astrofis, E-38205 Tenerife, Spain. [Moustakas, J.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Shu, X.] Univ Sci & Technol China, Dept Astron, CAS Key Lab Res Galaxies & Cosmol, Hefei 230026, Anhui, Peoples R China. [Shu, X.] CEA Saclay, DSM Irfu Serv Astrophys, F-91191 Gif Sur Yvette, France. [Zitrin, A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RP Laporte, N (reprint author), Pontificia Univ Catolica Chile, Inst Astrofis, Vicuna Mackenna 4860, Santiago 7820436, Chile.; Laporte, N (reprint author), Pontificia Univ Catolica Chile, Ctr Astroingn, Fac Fis, Vicuna Mackenna 4860, Santiago 7820436, Chile. RI Chilingarian, Igor/N-5117-2016; Shu, Xinwen/D-7294-2017 OI Chilingarian, Igor/0000-0002-7924-3253; Shu, Xinwen/0000-0002-7020-4290 FU CONICYT-Chile [Basal-CATA PFB-06/2007]; Gemini-CONICYT [32120003]; EMBIGGEN [Anillo ACT1101]; FONDECYT [1141218, 3160122, 3140542]; "Millennium Institute of Astrophysics (MAS)" of the Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo [IC120009]; French Agence Nationale de la Recherche [ANR-09-BLAN-0234]; Brazilian funding agency FAPESP [2014/11806-9]; Space Telescope Science Institute (STScI) [AR-13279]; NASA [NAS 5-26555]; Smithsonian Astrophysical Observatory Telescope Data Center; Russian Federation [MD-7355.2015.2]; Russian Foundation for Basic Research [15-32-21062, 15-52-15050]; HST Frontier Fields program FX The authors thank the anonymous referee for the useful comments that strongly improved the quality of the paper. We acknowledge support from CONICYT-Chile grants Basal-CATA PFB-06/2007 (NL, LI, FEB, and SK), Gemini-CONICYT #32120003 (NL), "EMBIGGEN" Anillo ACT1101 (FEB), FONDECYT 1141218 (FEB), FONDECYT Postdoctorado 3160122 (NL), 3140542 (PT) and Project IC120009 "Millennium Institute of Astrophysics (MAS)" of the Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo (FEB), and the French Agence Nationale de la Recherche bearing the reference ANR-09-BLAN-0234 (RP, DB). A.M. acknowledges the financial support of the Brazilian funding agency FAPESP (Postdoc fellowship-process number 2014/11806-9). This work was supported by award AR-13279 from the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. I.C. acknowledges the support from Smithsonian Astrophysical Observatory Telescope Data Center and from the grants MD-7355.2015.2 by the research council of the president of the Russian Federation, 15-32-21062 and 15-52-15050 by the Russian Foundation for Basic Research. This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. The HST image mosaics were produced by the Frontier Fields Science Data Products Team at STScI. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This work utilizes gravitational lensing models produced by PIs Bradac, Ebeling, Merten & Zitrin, Sharon, and Williams funded as part of the HST Frontier Fields program conducted by STScI. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. The lens models were obtained from the Mikulski Archive for Space Telescopes (MAST). NR 139 TC 6 Z9 6 U1 6 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 2016 VL 820 IS 2 AR 98 DI 10.3847/0004-637X/820/2/98 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI8HE UT WOS:000373741300017 ER PT J AU Ma, YK Ng, CY Bucciantini, N Slane, PO Gaensler, BM Temim, T AF Ma, Y. K. Ng, C-Y. Bucciantini, N. Slane, P. O. Gaensler, B. M. Temim, T. TI RADIO POLARIZATION OBSERVATIONS OF THE SNAIL: A CRUSHED PULSAR WIND NEBULA IN G327.1-1.1 WITH A HIGHLY ORDERED MAGNETIC FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (G327.1-1.1); ISM: supernova remnants; radio continuum: ISM ID SUPERNOVA REMNANT G327.1-1.1; X-RAY-EMISSION; IGR J11014-6103; EVOLUTION; CHANDRA; CONSTRAINTS; MODEL; JET AB Pulsar wind nebulae (PWNe) are suggested to be acceleration sites of cosmic rays in the Galaxy. While the magnetic field plays an important role in the acceleration process, previous observations of magnetic field configurations of PWNe are rare, particularly for evolved systems. We present a radio polarization study of the "Snail" PWN inside the supernova remnant G327.1-1.1 using the Australia Telescope Compact Array. This PWN is believed to have been recently crushed by the supernova (SN) reverse shock. The radio morphology is composed of a main circular body with a finger-like protrusion. We detected a strong linear polarization signal from the emission, which reflects a highly ordered magnetic field in the PWN and is in contrast to the turbulent environment with a tangled magnetic field generally expected from hydrodynamical simulations. This could suggest that the characteristic turbulence scale is larger than the radio beam size. We built a toy model to explore this possibility, and found that a simulated PWN with a turbulence scale of about one-eighth to one-sixth of the nebula radius and a pulsar wind filling factor of 50%-75% provides the best match to observations. This implies substantial mixing between the SN ejecta and pulsar wind material in this system. C1 [Ma, Y. K.; Ng, C-Y.] Univ Hong Kong, Dept Phys, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China. [Bucciantini, N.] INAF Osservatorio Astrofis Arcetri, Lgo E Fermi 5, I-50125 Florence, Italy. [Bucciantini, N.] INFN Sez Firenze, Via G Sansone 1, I-50019 Florence, Italy. [Slane, P. O.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Gaensler, B. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Temim, T.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. [Temim, T.] Univ Maryland, CRESST, College Pk, MD 20742 USA. RP Ng, CY (reprint author), Univ Hong Kong, Dept Phys, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China. EM ncy@bohr.physics.hku.hk OI /0000-0002-5847-2612; Gaensler, Bryan/0000-0002-3382-9558; Temim, Tea/0000-0001-7380-3144 FU Commonwealth of Australia; Australian Research Council; Science Foundation for Physics within the University of Sydney; ECS grant of Hong Kong Government [HKU 709713P]; NASA [NAS8-03060] FX The authors thank J. Lim for fruitful discussions. We also thank an anonymous referee for helpful comments and suggestions which improved the paper. 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. MOST is operated by The University of Sydney with support from the Australian Research Council and the Science Foundation for Physics within the University of Sydney. This work is supported by ECS grant of Hong Kong Government under HKU 709713P. P.O.S. acknowledges partial support from NASA Contract NAS8-03060. NR 40 TC 1 Z9 1 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2016 VL 820 IS 2 AR 100 DI 10.3847/0004-637X/820/2/100 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI8HE UT WOS:000373741300019 ER PT J AU Mackenzie, C Pichara, K Protopapas, P AF Mackenzie, Cristobal Pichara, Karim Protopapas, Pavlos TI CLUSTERING-BASED FEATURE LEARNING ON VARIABLE STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; stars: statistics ID TIME-SERIES CLASSIFICATION; RECURRENT NEURAL-NETWORKS; LARGE-MAGELLANIC-CLOUD; LIGHT CURVES; BOLTZMANN MACHINES; ALGORITHM; SELECTION; DATABASE; VARIABILITY; CANDIDATES AB The success of automatic classification of variable stars depends strongly on the lightcurve representation. Usually, lightcurves are represented as a vector of many descriptors designed by astronomers called features. These descriptors are expensive in terms of computing, require substantial research effort to develop, and do not guarantee a good classification. Today, lightcurve representation is not entirely automatic; algorithms must be designed and manually tuned up for every survey. The amounts of data that will be generated in the future mean astronomers must develop scalable and automated analysis pipelines. In this work we present a feature learning algorithm designed for variable objects. Our method works by extracting a large number of lightcurve subsequences from a given set, which are then clustered to find common local patterns in the time series. Representatives of these common patterns are then used to transform lightcurves of a labeled set into a new representation that can be used to train a classifier. The proposed algorithm learns the features from both labeled and unlabeled lightcurves, overcoming the bias using only labeled data. We test our method on data sets from the Massive Compact Halo Object survey and the Optical Gravitational Lensing Experiment; the results show that our classification performance is as good as and in some cases better than the performance achieved using traditional statistical features, while the computational cost is significantly lower. With these promising results, we believe that our method constitutes a significant step toward the automation of the lightcurve classification pipeline. C1 [Mackenzie, Cristobal; Pichara, Karim] Pontificia Univ Catolica Chile, Dept Comp Sci, Alameda 340, Santiago, Chile. [Pichara, Karim; Protopapas, Pavlos] Harvard Univ, Inst Appl Computat Sci, Cambridge, MA 02138 USA. [Pichara, Karim] Millennium Inst Astrophys, Santiago, Chile. [Protopapas, Pavlos] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Mackenzie, C (reprint author), Pontificia Univ Catolica Chile, Dept Comp Sci, Alameda 340, Santiago, Chile. FU Vicerrectoria de Investigacion (VRI) from Pontificia Universidad Catolica de Chile; Institute of Applied Computer Science at Harvard University; Chilean Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cientifica Milenio [P07-021-F] FX This work is supported by Vicerrectoria de Investigacion (VRI) from Pontificia Universidad Catolica de Chile, Institute of Applied Computer Science at Harvard University, and the Chilean Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cientifica Milenio through grant P07-021-F, awarded to The Milky Way Millennium Nucleus. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 63 TC 1 Z9 1 U1 3 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 2016 VL 820 IS 2 AR 138 DI 10.3847/0004-637X/820/2/138 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI8HE UT WOS:000373741300057 ER PT J AU Marion, GH Brown, PJ Vinko, J Silverman, JM Sand, DJ Challis, P Kirshner, RP Wheeler, JC Berlind, P Brown, WR Calkins, ML Camacho, Y Dhungana, G Foley, RJ Friedman, AS Graham, ML Howell, DA Hsiao, EY Irwin, JM Jha, SW Kehoe, R Macri, LM Maeda, K Mandel, K McCully, C Pandya, V Rines, KJ Wilhelmy, S Zheng, WK AF Marion, G. H. Brown, Peter J. Vinko, Jozsef Silverman, Jeffrey M. Sand, David J. Challis, Peter Kirshner, Robert P. Wheeler, J. Craig Berlind, Perry Brown, Warren R. Calkins, Michael L. Camacho, Yssavo Dhungana, Govinda Foley, Ryan J. Friedman, Andrew S. Graham, Melissa L. Howell, D. Andrew Hsiao, Eric Y. Irwin, Jonathan M. Jha, Saurabh W. Kehoe, Robert Macri, Lucas M. Maeda, Keiichi Mandel, Kaisey McCully, Curtis Pandya, Viraj Rines, Kenneth J. Wilhelmy, Steven Zheng, Weikang TI SN. 2012cg: EVIDENCE FOR INTERACTION BETWEEN A NORMAL SN Ia AND A NON-DEGENERATE BINARY COMPANION SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (2012cg) ID OBSERVATORY SUPERNOVA SEARCH; HOBBY-EBERLY TELESCOPE; HIGH-VELOCITY FEATURES; LIGHT CURVES; CIRCUMSTELLAR MATERIAL; VIRGO CLUSTER; PHOTOMETRY PROGRAM; SODIUM-ABSORPTION; SPIRAL GALAXIES; PROGENITORS AB We report evidence for excess blue light from the Type Ia supernova (Sn Ia) SN. 2012cg at 15 and 16 days before maximum B-band brightness. The emission is consistent with predictions for the impact of the supernova on a non-degenerate binary companion. This is the first evidence for emission from a companion to a normal SN. Ia. Sixteen days before maximum light, the B - V color of SN. 2012cg is 0.2 mag bluer than for other normal SN. Ia. At later times, this supernova has a typical SN. Ia light curve, with extinction-corrected MB = -19.62 +/- 0.02 mag and Delta m(15)(B)= 0.86 +/- 0.02. Our data set is extensive, with photometry in seven filters from five independent sources. Early spectra also show the effects of blue light, and high-velocity features are observed at early times. Near maximum, the spectra are normal with a silicon velocity v(Si) = -10,500 km s(-1). Comparing the early data with models by Kasen favors a main-sequence companion of about six solar masses. It is possible that many other SN Ia have main-sequence companions that have eluded detection because the emission from the impact is fleeting and faint. C1 [Marion, G. H.; Vinko, Jozsef; Silverman, Jeffrey M.; Wheeler, J. Craig] Univ Texas Austin, 1 Univ Stn C1400, Austin, TX 78712 USA. [Marion, G. H.; Challis, Peter; Kirshner, Robert P.; Berlind, Perry; Brown, Warren R.; Calkins, Michael L.; Friedman, Andrew S.; Irwin, Jonathan M.; Mandel, Kaisey] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Brown, Peter J.; Macri, Lucas M.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, 4242 TAMU, College Stn, TX 77843 USA. [Vinko, Jozsef] Univ Szeged, Dept Opt & Quantum Elect, Domter 9, H-6720 Szeged, Hungary. [Sand, David J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Camacho, Yssavo; Jha, Saurabh W.; Pandya, Viraj] Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. [Camacho, Yssavo] Lehigh Univ, Dept Phys, 16 Mem Dr East, Bethlehem, PA 18015 USA. [Dhungana, Govinda; Kehoe, Robert] So Methodist Univ, Dept Phys, Dallas, TX 75275 USA. [Foley, Ryan J.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Foley, Ryan J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. [Friedman, Andrew S.] MIT, Ctr Theoret Phys, Cambridge, MA 02139 USA. [Friedman, Andrew S.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Graham, Melissa L.; Zheng, Weikang] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Howell, D. Andrew; McCully, Curtis] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA. [Howell, D. Andrew] Univ Calif Santa Barbara, Dept Phys, Broida Hall,Mail Code 9530, Santa Barbara, CA 93106 USA. [Hsiao, Eric Y.] Las Campanas Observ, Carnegie Observ, Casilla 601, Colina El Pino, Chile. [Hsiao, Eric Y.] Aarhus Univ, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Maeda, Keiichi] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan. [Pandya, Viraj] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Rines, Kenneth J.; Wilhelmy, Steven] Western Washington Univ, Dept Phys & Astron, 516 High St, Bellingham, WA 98225 USA. [Maeda, Keiichi] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan. RP Marion, GH (reprint author), Univ Texas Austin, 1 Univ Stn C1400, Austin, TX 78712 USA.; Marion, GH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ghmarion@gmail.com RI Friedman, Andrew/I-4691-2013; OI Friedman, Andrew/0000-0003-1334-039X; Sand, David/0000-0003-4102-380X FU Hungarian OTKA grant [NN-107637]; NSF [AST-1109801, AST-1211196, AST-156854]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; National Science Foundation [NSF PHY-1125915, AST-1008343]; NSF Graduate Research Fellowship; NASA Graduate Research Program Fellowship; NSF STS postdoctoral fellowship [SES-1056580]; NASA through Space Telescope Science Institute [GO-12540]; NASA [NAS5-26555, NNX10A196H, UTA13-000844]; NASA's Astrophysics Data Analysis Program [NNX13AF35G]; Danish Agency for Science, Technology and Innovation through a Sapere Aude Level 2 grant; NSF CAREER award [AST-0847157]; NSF REU grant [PHY-1263280]; JSPS KAKENHI [26800100]; MEXT WPI Initiative, Japan FX J.V. is supported by Hungarian OTKA grant NN-107637. J.C.W., G.H.M., J.M.S. and the U.T. supernova group are supported by NSF grant AST-1109801. J.M.S. is also supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. The CfA Supernova Program is supported by NSF grants AST-1211196 and AST-156854 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. A.S.F. acknowledges support from a NSF Graduate Research Fellowship, a NASA Graduate Research Program Fellowship, and a NSF STS postdoctoral fellowship under award SES-1056580. We acknowledge the work of C. Klein, D. L. Starr, and J. S. Bloom on the PAIRITEL mosaic data reduction pipeline. Additional support comes from program GO-12540, 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. ROTSE data analysis was supported by NASA grant NNX10A196H subaward UTA13-000844.; G.H.M. is a visiting Astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. P. J. Brown and the Swift Optical/Ultraviolet Supernova Archive are supported by NASA's Astrophysics Data Analysis Program through grant NNX13AF35G. E.Y.H. acknowledges the support provided by the National Science Foundation under grant no. AST-1008343 and by the Danish Agency for Science, Technology and Innovation through a Sapere Aude Level 2 grant. This research at Rutgers University was supported by NSF CAREER award AST-0847157 to S.W.J., and NSF REU grant PHY-1263280 for Y.C. The work by K. Maeda is supported by JSPS KAKENHI (26800100) and MEXT WPI Initiative, Japan. This paper includes data gathered with the 6.5 m Magellan Telescopes located at the Las Campanas Observatory, Chile. This work makes use of observations from the LCOGT network. The authors make frequent use of David Bishop's excellent webpage listing recent supernovae and valuable references associated with them: www.rochesterastronomy.org/snimages/. NR 95 TC 16 Z9 16 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2016 VL 820 IS 2 AR 92 DI 10.3847/0004-637X/820/2/92 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI8HE UT WOS:000373741300011 ER PT J AU Villanueva, S Eastman, JD Gaudi, BS AF Villanueva, S., Jr. Eastman, J. D. Gaudi, B. S. TI THE DEDICATED MONITOR OF EXOTRANSITS (DEMONEX): SEVEN TRANSITS OF XO-4b SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; planetary systems; stars: individual (XO-4); techniques: photometric; techniques: radial velocities ID SPITZER-SPACE-TELESCOPE; JUPITER-MASS COMPANION; SPIN-ORBIT ANGLE; EXTRASOLAR PLANETS; Y-2 ISOCHRONES; MCLAUGHLIN; SYSTEM; STAR; EXOPLANETS; VELOCITY AB The DEdicated MONitor of EXotransits (DEMONEX) was a 20-inch robotic and automated telescope to monitor bright stars hosting transiting exoplanets to discover new planets and improve constraints on the properties of known transiting planetary systems. We present results for the misaligned hot Jupiter XO-4b containing seven new transits from the DEMONEX telescope, including three full and four partial transits. We combine these data with archival light curves and archival radial velocity measurements to derive the host star mass M-* = 1.293(-0.029)(+0.030) M-circle dot and radius R-* = 1.554(-0.030)(+0.042) R-circle dot, the planet mass M-P = 1.615(-0.099)(+0.10) M-J and radius R-P = 1.317(-0.029)(+0.040) R-J, and a refined ephemeris of P = 4.1250687 +/- 0.0000024 days and T-0 = 2, 4547, 58.18978 +/- 0.00024 BJD(TDB). We include archival Rossiter-McLaughlin measurements of XO-4 to infer the stellar spin-planetary orbit alignment of lambda = -40.0(-7.5)(+8.8) degrees. We test the effects of including various detrend parameters, theoretical and empirical mass-radius relations, and Rossiter-McLaughlin models. We infer that detrending against CCD position and time or airmass can improve data quality. but can have significant effects on the inferred values of many parameters-most significantly R-P/R-* and the observed central transit times T-C. In the case of R-P/R-* we find that the systematic uncertainty due to detrending can be three times that of the quoted statistical uncertainties. The choice of mass-radius relation has little effect on our inferred values of the system parameters. The choice of Rossiter-McLaughlin models can have significant effects on the inferred values of v sin I-* and the stellar spin-planet orbit angle lambda. C1 [Villanueva, S., Jr.; Gaudi, B. S.] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA. [Eastman, J. D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Villanueva, S (reprint author), Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA. EM svillan@astronomy.ohio-state.edu FU National Science Foundation [DGE-1343012, AST-1056524] FX S.V. is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1343012. B.S.G. is supported by National Science Foundation CAREER Grant AST-1056524. NR 43 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 APR 1 PY 2016 VL 820 IS 2 AR 87 DI 10.3847/0004-637X/820/2/87 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DI8HE UT WOS:000373741300006 ER PT J AU McClain, CR Barry, JP Eernisse, D Horton, T Judge, J Kakui, K Mah, C Waren, A AF McClain, Craig R. Barry, James P. Eernisse, Douglas Horton, Tammy Judge, Jenna Kakui, Keiichi Mah, Chris Waren, Anders TI Multiple processes generate productivity-diversity relationships in experimental wood-fall communities SO ECOLOGY LA English DT Article DE connectivity; deep sea; diversity; energy; productivity; resource availability ID SPECIES-ENERGY RELATIONSHIPS; FOOD-CHAIN LENGTH; BETA-DIVERSITY; INDIVIDUALS HYPOTHESIS; SCALE-DEPENDENCE; BIRD COMMUNITIES; SPATIAL SCALE; RICHNESS; ABUNDANCE; BIODIVERSITY AB Energy availability has long been recognized as a predictor of community structure, and changes in both terrestrial and marine productivity under climate change necessitate a deeper understanding of this relationship. The productivity-diversity relationship (PDR) is well explored in both empirical and theoretical work in ecology, but numerous questions remain. Here, we test four different theories for PDRs (More-Individuals Hypothesis, Resource-Ratio Theory, More Specialization Theory, and the Connectivity-Diversity Hypothesis) with experimental deep-sea wood falls. We manipulated productivity by altering wood-fall sizes and measured responses after 5 and 7 years. In November 2006, 32 Acacia sp. logs were deployed at 3203 m in the Northeast Pacific Ocean (Station Deadwood: 36.154098 degrees N, 122.40852 degrees W). Overall, we found a significant increase in diversity with increased wood-fall size for these communities. Increases in diversity with wood-fall size occurred because of the addition of rare species and increases of overall abundance, although individual species responses varied. We also found that limited dispersal helped maintain the positive PDR relationship. Our experiment suggests that multiple interacting mechanisms influence PDRs. C1 [McClain, Craig R.] Duke Univ, Dept Biol, Box 90338, Durham, NC 27708 USA. [Barry, James P.] Monterey Bay Aquarium Res Inst, 7700 Sandholdt Rd, Moss Landing, CA 95039 USA. [Eernisse, Douglas] Calif State Univ Fullerton, Dept Biol Sci, Fullerton, CA 92834 USA. [Horton, Tammy] Univ Southampton, Natl Oceanog Ctr, Ocean Biogeochem & Ecosyst, Waterfront Campus,European Way, Southampton SO14 3ZH, Hants, England. [Judge, Jenna] Univ Calif Berkeley, Dept Integrat Biol, 3040 Valley Life Sci Bldg, Berkeley, CA 94720 USA. [Kakui, Keiichi] Hokkaido Univ, Fac Sci, Dept Biol Sci, Sapporo, Hokkaido 0600810, Japan. [Mah, Chris] Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, 10th & Constitut Ave NW, Washington, DC 20560 USA. [Waren, Anders] Swedish Museum Nat Hist, Dept Zool, Box 50007, SE-10405 Stockholm, Sweden. RP McClain, CR (reprint author), Duke Univ, Dept Biol, Box 90338, Durham, NC 27708 USA. EM craig.mcclain@duke.edu RI Kakui, Keiichi/D-6108-2015; OI Kakui, Keiichi/0000-0003-4630-9065; McClain, Craig/0000-0003-0574-428X FU National Evolutionary Synthesis Center (NSF) [EF-0905606]; Monterey Bay Aquarium Research Institute [200002, 900703, 900608]; David and Lucile Packard Foundation FX We thank Karl Evans, Tom Webb, and Solange Brault for input on the analyses. Janet Voight provided invaluable assistance with the experimental design, taxonomic identification, and review of the manuscript. Tom Webb, Jeff Nekola, Morgan Ernest, and Dan McGlinn provided helpful comments on earlier versions of the manuscript. The crew of the RV Western Flyer and ROV Doc Ricketts were invaluable for their help in deployment and retrieval. We also thank C. Lovera, K. Buck, P. Whaling, and D. Honig for providing help with processing of the retrieved logs. C. R. McClain was supported by the National Evolutionary Synthesis Center (NSF #EF-0905606). This work was also supported by the Monterey Bay Aquarium Research Institute (projects 200002, 900703, 900608) and the David and Lucile Packard Foundation. Michelle Gaither-McClain provided editorial assistance and loving patience with the first author. NR 54 TC 3 Z9 3 U1 10 U2 27 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD APR PY 2016 VL 97 IS 4 BP 885 EP 898 DI 10.1890/15-1669.1 PG 14 WC Ecology SC Environmental Sciences & Ecology GA DJ0VS UT WOS:000373923100008 PM 27220205 ER PT J AU Kaspari, M Clay, NA Lucas, J Revzen, S Kay, A Yanoviak, SP AF Kaspari, Michael Clay, Natalie A. Lucas, Jane Revzen, Shai Kay, Adam Yanoviak, Stephen P. TI Thermal adaptation and phosphorus shape thermal performance in an assemblage of rainforest ants SO ECOLOGY LA English DT Article DE ants; boundary layer; community; ectotherms; functional traits; phosphorus; thermal adaptation; thermal tolerance; tradeoffs; tropical forest; vertical stratification ID HEAT-SHOCK PROTEINS; GLOBAL ANALYSIS; BODY-SIZE; TEMPERATURE; TOLERANCE; EVOLUTION; ECTOTHERMS; BIOGEOGRAPHY; PHYSIOLOGY; COMMUNITY AB We studied the Thermal Performance Curves (TPCs) of 87 species of rainforest ants and found support for both the Thermal Adaptation and Phosphorus Tolerance hypotheses. TPCs relate a fitness proxy (here, worker speed) to environmental temperature. Thermal Adaptation posits that thermal generalists (ants with flatter, broader TPCs) are favored in the hotter, more variable tropical canopy compared to the cooler, less variable litter below. As predicted, species nesting in the forest canopy 1) had running speeds less sensitive to temperature; 2) ran over a greater range of temperatures; and 3) ran at lower maximum speeds. Tradeoffs between tolerance and maximum performance are often invoked for constraining the evolution of thermal generalists. There was no evidence that ant species traded off thermal tolerance for maximum speed, however. Phosphorus Tolerance is a second mechanism for generating ectotherms able to tolerate thermal extremes. It posits that ants active at high temperatures invest in P rich machinery to buffer their metabolism against thermal extremes. Phosphorus content in ant tissue varied three fold, and as predicted, temperature sensitivity was lower and thermal range was higher in P rich species. Combined, we show how the vertical distribution of hot and variable vs. cooler and stable microclimates in a single forest contribute to a diversity of TPCs and suggest that a widely varying P stoichiometry among these ants may drive some of these differences. C1 [Kaspari, Michael; Clay, Natalie A.; Lucas, Jane] Univ Oklahoma, Dept Biol, Grad Program Ecol & Evolut, Norman, OK 73019 USA. [Kaspari, Michael; Clay, Natalie A.; Lucas, Jane] Smithsonian Trop Res Inst, Balboa, Panama. [Kay, Adam] Univ St Thomas, Dept Biol, St Paul, MN 55105 USA. [Yanoviak, Stephen P.] Univ Louisville, Dept Biol, Louisville, KY 40292 USA. [Revzen, Shai] Univ Michigan, Dept Elect Engn & Comp Sci, Ann Arbor, MI 48109 USA. RP Kaspari, M (reprint author), Univ Oklahoma, Dept Biol, Grad Program Ecol & Evolut, Norman, OK 73019 USA.; Kaspari, M (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM mkaspari@ou.edu OI Kaspari, Michael/0000-0002-9717-5768 FU NSF [DEB 0842038, EF 1065844, DEB 1252614] FX Our work benefited from discussions with Ray Huey, Jon Harrison, and Dan Hahn and five anonymous reviewers. Funding was provided by grants from the NSF (DEB 0842038) to A.D. Kay and M. Kaspari, (EF 1065844) to M. Kaspari, and (DEB 1252614) to SP Yanoviak. NR 56 TC 1 Z9 1 U1 21 U2 30 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD APR PY 2016 VL 97 IS 4 BP 1038 EP 1047 DI 10.1890/15-1225.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA DJ0VS UT WOS:000373923100022 PM 27220219 ER PT J AU Picq, S McMillan, WO Puebla, O AF Picq, Sophie McMillan, W. Owen Puebla, Oscar TI Population genomics of local adaptation versus speciation in coral reef fishes (Hypoplectrus spp, Serranidae) SO ECOLOGY AND EVOLUTION LA English DT Article DE Fish; local adaptation; marine; RAD sequencing; speciation ID MULTILOCUS GENOTYPE DATA; MARINE SPECIES FLOCK; COLOR MORPHS; HAMLETS HYPOPLECTRUS; CICHLID FISH; ATLANTIC COD; DE-NOVO; DIVERGENCE; MARKERS; SCALE AB Are the population genomic patterns underlying local adaptation and the early stages of speciation similar? Addressing this question requires a system in which (i) local adaptation and the early stages of speciation can be clearly identified and distinguished, (ii) the amount of genetic divergence driven by the two processes is similar, and (iii) comparisons can be repeated both taxonomically (for local adaptation) and geographically (for speciation). Here, we report just such a situation in the hamlets (Hypoplectrus spp), brightly colored reef fishes from the wider Caribbean. Close to 100,000 SNPs genotyped in 126 individuals from three sympatric species sampled in three repeated populations provide genome-wide levels of divergence that are comparable among allopatric populations (F-st estimate=0.0042) and sympatric species (F-st estimate=0.0038). Population genetic, clustering, and phylogenetic analyses reveal very similar patterns for local adaptation and speciation, with a large fraction of the genome undifferentiated (F-st estimate approximate to 0), a very small proportion of F-st outlier loci (0.05-0.07%), and remarkably few repeated outliers (1-3). Nevertheless, different loci appear to be involved in the two processes in Hypoplectrus, with only 7% of the most differentiated SNPs and outliers shared between populations and species comparisons. In particular, a tropomyosin (Tpm4) and a previously identified hox (HoxCa) locus emerge as candidate loci (repeated outliers) for local adaptation and speciation, respectively. We conclude that marine populations may be locally adapted notwithstanding shallow levels of genetic divergence, and that from a population genomic perspective, this process does not appear to differ fundamentally from the early stages of speciation. C1 [Picq, Sophie; Puebla, Oscar] GEOMAR Helmholtz Ctr Ocean Res Kiel, Evolutionary Ecol Marine Fishes, Dusternbrooker Weg 20, D-24105 Kiel, Germany. [Picq, Sophie; Puebla, Oscar] Univ Kiel, Fac Math & Nat Sci, Christian Albrechts Pl 4, D-24118 Kiel, Germany. [McMillan, W. Owen; Puebla, Oscar] Smithsonian Trop Res Inst, Panama City 084303092, Panama. RP Puebla, O (reprint author), GEOMAR Helmholtz Ctr Ocean Res Kiel, Evolutionary Ecol Marine Fishes, Dusternbrooker Weg 20, D-24105 Kiel, Germany. EM oscar.puebla@mail.mcgill.ca FU Smithsonian Institution Scholarly Studies FX Smithsonian Institution Scholarly Studies (Grant/Award Number: 'Smithsonian Institution Scholarly Studies'). NR 82 TC 3 Z9 3 U1 19 U2 50 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 2016 VL 6 IS 7 BP 2109 EP 2124 DI 10.1002/ece3.2028 PG 16 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA DJ2RE UT WOS:000374052000019 PM 27099711 ER PT J AU Ripperger, S Josic, D Hierold, M Koelpin, A Weigel, R Hartmann, M Page, R Mayer, F AF Ripperger, Simon Josic, Darija Hierold, Martin Koelpin, Alexander Weigel, Robert Hartmann, Markus Page, Rachel Mayer, Frieder TI Automated proximity sensing in small vertebrates: design of miniaturized sensor nodes and first field tests in bats SO ECOLOGY AND EVOLUTION LA English DT Article DE Automated data collection; digital telemetry; encounter logging; sensor network; social interactions ID SOCIAL NETWORK ANALYSIS; DECISION-MAKING; INFORMATION-TRANSFER; FORAGING BEHAVIOR; CONTACT NETWORKS; GROUP-DYNAMICS; MOLOSSID BATS; WILD BIRDS; EARED BATS; TRANSMISSION AB Social evolution has led to a stunning diversity of complex social behavior, in particular in vertebrate taxa. Thorough documentation of social interactions is crucial to study the causes and consequences of sociality in gregarious animals. Wireless digital transceivers represent a promising tool to revolutionize data collection for the study of social interactions in terms of the degree of automation, data quantity, and quality. Unfortunately, devices for automated proximity sensing via direct communication among animal-borne sensors are usually heavy and do not allow for the investigation of small animal species, which represent the majority of avian and mammalian taxa. We present a lightweight animal-borne sensor node that is built from commercially available components and uses a sophisticated scheme for energy-efficient communication, with high sampling rates at relatively low power consumption. We demonstrate the basic functionality of the sensor node under laboratory conditions and its applicability for the study of social interactions among free-ranging animals. The first field tests were performed on two species of bats in temperate and tropical ecosystems. At <2g, this sensor node is light enough to observe a broad spectrum of taxa including small vertebrates. Given our specifications, the system was especially sensitive to changes in distance within the short range (up to a distance of 4m between tags). High spatial resolution at short distances enables the evaluation of interactions among individuals at a fine scale and the investigation of close contacts. This technology opens new avenues of research, allowing detailed investigation of events associated with social contact, such as mating behavior, pathogen transmission, social learning, and resource sharing. Social behavior that is not easily observed becomes observable, for example, in animals living in burrows or in nocturnal animals. A switch from traditional methods to the application of digital transceiver chips in proximity sensing offers numerous advantages in addition to an enormous increase in data quality and quantity. For future applications, the platform allows for the integration of additional sensors that may collect physiological or environmental data. Such information complements social network studies and may allow for a deeper understanding of animal ecology and social behavior. C1 [Ripperger, Simon; Josic, Darija; Mayer, Frieder] Museum Nat Kunde, Leibniz Inst Evolut & Biodivers Sci, Invalidenstr 43, D-10115 Berlin, Germany. [Hierold, Martin; Koelpin, Alexander; Weigel, Robert] Univ Erlangen Nurnberg, Inst Elect Engn, D-91054 Erlangen, Germany. [Hartmann, Markus] Univ Erlangen Nurnberg, Informat Technol Commun Elect, D-91054 Erlangen, Germany. [Page, Rachel] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. [Mayer, Frieder] Berlin Brandenburg Inst Adv Biodivers Res, Berlin, Germany. RP Ripperger, S (reprint author), Museum Nat Kunde, Leibniz Inst Evolut & Biodivers Sci, Invalidenstr 43, D-10115 Berlin, Germany. EM simon.ripperger@mfn-berlin.de OI Hartmann, Markus/0000-0002-4503-3098 FU Deutsche Forschungsgemeinschaft [FOR 1508] FX Deutsche Forschungsgemeinschaft (Grant/Award Number: 'FOR 1508'). NR 56 TC 0 Z9 0 U1 8 U2 18 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 2016 VL 6 IS 7 BP 2179 EP 2189 DI 10.1002/ece3.2040 PG 11 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA DJ2RE UT WOS:000374052000025 PM 27069579 ER PT J AU Schrader, CM Cohen, BA Donovan, JJ Vicenzi, EP AF Schrader, Christian M. Cohen, Barbara A. Donovan, John J. Vicenzi, Edward P. TI Ni/S/Cl systematics and the origin of impact-melt glasses in Martian meteorite Elephant Moraine 79001 SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID X-RAY SPECTROMETER; SHOCK METAMORPHISM; GUSEV CRATER; MERIDIANI-PLANUM; SOIL COMPONENT; MARS; SHERGOTTITE; OLIVINE; A79001; ROCKS AB Martian meteorite Elephant Moraine A79001 (EET 79001) has received considerable attention for the unusual composition of its shock melt glass, particularly its enrichment in sulfur relative to the host shergottite. It has been hypothesized that Martian regolith was incorporated into the melt or, conversely, that the S-enrichment stems from preferential melting of sulfide minerals in the host rock during shock. We present results from an electron microprobe study of EET 79001 including robust measurements of major and trace elements in the shock melt glass (S, Cl, Ni, Co, V, and Sc) and minerals in the host rock (Ni, Co, and V). We find that both S and major element abundances can be reconciled with previous hypotheses of regolith incorporation and/or excess sulfide melt. However, trace element characteristics of the shock melt glass, particularly Ni and Cl abundances relative to S, cannot be explained either by the incorporation of regolith or sulfide minerals. We therefore propose an alternative hypothesis whereby, prior to shock melting, portions of EET 79001 experienced acid-sulfate leaching of the mesostasis, possibly groundmass feldspar, and olivine, producing Al-sulfates that were later incorporated into the shock melt, which then quenched to glass. Such activity in the Martian near-surface is supported by observations from the Mars Exploration Rovers and laboratory experiments. Our preimpact alteration model, accompanied by the preferential survival of olivine and excess melting of feldspar during impact, explains the measured trace element abundances better than either the regolith incorporation or excess sulfide melting hypothesis does. C1 [Schrader, Christian M.; Cohen, Barbara A.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Schrader, Christian M.] Bowdoin Coll, Dept Geol, Brunswick, ME 04011 USA. [Donovan, John J.] Univ Oregon, Dept Chem, Eugene, OR 97403 USA. [Vicenzi, Edward P.] Museum Conservat Inst, Smithsonian Inst, Suitland, MD 20746 USA. RP Cohen, BA (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM barbara.a.cohen@nasa.gov FU NASA Postdoctoral Program; Mars Fundamental Research Program grant FX We thank the NASA Postdoctoral Program for funding salary and travel for the first author, and the Antarctic Meteorite Working Group for approving our sample request. Joel Hurowitz, Hap McSween, Paul Warren, Erin Walton, and several anonymous reviewers provided helpful reviews and editor Mike Zolensky encouraged us through several revisions. This research was supported by a Mars Fundamental Research Program grant to B. A. Cohen and used NASA's Astrophysics Data System (ADS). NR 61 TC 0 Z9 0 U1 2 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD APR PY 2016 VL 51 IS 4 BP 663 EP 680 DI 10.1111/maps.12612 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DJ2QT UT WOS:000374050800003 ER PT J AU Woodman, N AF Woodman, Neal TI Pranked by Audubon: Constantine S. Rafinesque's description of John James Audubon's imaginary Kentucky mammals SO ARCHIVES OF NATURAL HISTORY LA English DT Article DE cryptozoology; eccentric naturalist; hoax; mouse; Peromyscus leucopus; Sciurus niger rufiventer ID MOUSE AB The North American naturalist Constantine S. Rafinesque spent much of the year 1818 engaged in a solo journey down the Ohio River Valley to explore parts of what was then the western United States. Along the way, he visited a number of fellow naturalists, and he spent more than a week at the Henderson, Kentucky, home of artist and ornithologist John James Audubon. During the succeeding two years, Rafinesque published descriptions of new species that resulted from his expedition, including eleven species of fishes that eventually proved to have been invented by Audubon as a prank on the credulous naturalist. Less well known are a number of "wild rats" described by Rafinesque that include one recognized species (Musculus leucopus) and ten other, imaginary "species" fabricated by Audubon (Gerbillus leonurus, G. megalops, Spalax trivittata, Cricetus fasciatus, Sorex cerulescens, S. melanotis, Musculus nigricans, Lemmus albovittatus, L. talpoides, Sciurus ruber). Rafinesque's unpublished sketches of these animals provide important insight regarding the supposed nature of the animals invented by Audubon and ultimately published by Rafinesque. C1 [Woodman, Neal] Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, MRC-111,POB 37012, Washington, DC 20013 USA. RP Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, MRC-111,POB 37012, Washington, DC 20013 USA. EM woodmann@si.edu OI Woodman, Neal/0000-0003-2689-7373 NR 51 TC 0 Z9 0 U1 5 U2 7 PU EDINBURGH UNIV PRESS PI EDINBURGH PA THE TUN-HOLYROOD RD, 12 2F JACKSONS ENTRY, EDINBURGH EH8 8PJ, SCOTLAND SN 0260-9541 EI 1755-6260 J9 ARCH NAT HIST JI Arch. Nat. Hist. PD APR PY 2016 VL 43 IS 1 BP 95 EP 108 DI 10.3366/anh.2016.0349 PG 14 WC History & Philosophy Of Science; Multidisciplinary Sciences SC History & Philosophy of Science; Science & Technology - Other Topics GA DI3SB UT WOS:000373417700008 ER PT J AU Marcowith, A Bret, A Bykov, A Dieckmann, ME Drury, LO Lembege, B Lemoine, M Morlino, G Murphy, G Pelletier, G Plotnikov, I Reville, B Riquelme, M Sironi, L Novo, AS AF Marcowith, A. Bret, A. Bykov, A. Dieckmann, M. E. Drury, L. O'C Lembege, B. Lemoine, M. Morlino, G. Murphy, G. Pelletier, G. Plotnikov, I. Reville, B. Riquelme, M. Sironi, L. Novo, A. Stockem TI The microphysics of collisionless shock waves SO REPORTS ON PROGRESS IN PHYSICS LA English DT Review DE shocks; plasma instabilities; particle acceleration ID GAMMA-RAY-BURSTS; ENERGY COSMIC-RAYS; MAGNETIC-FIELD AMPLIFICATION; HIGH-MACH-NUMBER; QUASI-PERPENDICULAR SHOCKS; ELECTRON-POSITRON PLASMAS; SUPERNOVA REMNANT SHOCKS; IN-CELL SIMULATIONS; EARTHS BOW SHOCK; BALMER-DOMINATED SHOCKS AB Collisionless shocks, that is shocks mediated by electromagnetic processes, are customary in space physics and in astrophysics. They are to be found in a great variety of objects and environments: magnetospheric and heliospheric shocks, supernova remnants, pulsar winds and their nebulae, active galactic nuclei, gamma-ray bursts and clusters of galaxies shock waves. Collisionless shock microphysics enters at different stages of shock formation, shock dynamics and particle energization and/or acceleration. It turns out that the shock phenomenon is a multi-scale non-linear problem in time and space. It is complexified by the impact due to high-energy cosmic rays in astrophysical environments. This review adresses the physics of shock formation, shock dynamics and particle acceleration based on a close examination of available multi-wavelength or in situ observations, analytical and numerical developments. A particular emphasis is made on the different instabilities triggered during the shock formation and in association with particle acceleration processes with regards to the properties of the background upstream medium. It appears that among the most important parameters the background magnetic field through the magnetization and its obliquity is the dominant one. The shock velocity that can reach relativistic speeds has also a strong impact over the development of the micro-instabilities and the fate of particle acceleration. Recent developments of laboratory shock experiments has started to bring some new insights in the physics of space plasma and astrophysical shock waves. A special section is dedicated to new laser plasma experiments probing shock physics. C1 [Marcowith, A.] Univ Montpellier, CNRS, Lab Univers & Particules Montpellier, Pl E Bataillon, F-34095 Montpellier, France. [Bret, A.] Univ Castilla La Mancha, ETSI Ind, E-13071 Ciudad Real, Spain. [Bret, A.] Inst Invest Energt & Aplicac Ind, Campus Univ Ciudad Real, Ciudad Real 13071, Spain. [Bykov, A.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Bykov, A.] St Petersburg State Politecn Univ, St Petersburg, Russia. [Bykov, A.] Int Space Sci Inst, Bern, Switzerland. [Dieckmann, M. E.] Linkpings Univ, Dept Sci & Technol ITN, Campus Norrkping, SE-60174 Norrkoping, Sweden. [Drury, L. O'C] Dublin Inst Adv Studies, Sch Cosm Phys, 31 Fitzwilliam Pl, Dublin 2, Ireland. [Lembege, B.] IPSL, UVSQ, LATMOS, CNRS, 11 Bd Alembert, F-78280 Guyancourt, France. [Lemoine, M.] UPMC, CNRS, Inst Astrophys Paris, 98 Bis Blvd Arago, F-75014 Paris, France. [Morlino, G.] Gran Sasso Sci Inst, Ist Nazl Fis Nucl, Viale F Crispi 7, I-67100 Laquila, Italy. [Morlino, G.] Osserv Astrofis Arcetri, INAF, Lgo E Fermi 5, I-50125 Florence, Italy. [Murphy, G.] Niels Bohr Inst, Niels Bohr Int Acad, Blegdamsvej 17, DK-2100 Copenhagen, Denmark. [Pelletier, G.; Plotnikov, I.] IPAG, UMR 5274, F-38041 Grenoble, France. [Plotnikov, I.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Plotnikov, I.] Inst Rech Astrophys & Planetol, CNRS, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France. [Reville, B.] Queens Univ Belfast, Dept Phys & Astron, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland. [Riquelme, M.] Univ Chile, Dept Phys, FCFM, Santiago, Chile. [Sironi, L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Novo, A. Stockem] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum Astrophys 4, D-44801 Bochum, Germany. RP Marcowith, A (reprint author), Univ Montpellier, CNRS, Lab Univers & Particules Montpellier, Pl E Bataillon, F-34095 Montpellier, France. EM Alexandre.Marcowith@umontpellier.fr RI Dieckmann, Mark Eric/C-8591-2009; Riquelme, Mario/H-2235-2016; Bykov, Andrei/E-3131-2014 OI Dieckmann, Mark Eric/0000-0003-4055-0552; FU ISSI; french ANR MACH project; Ministerio de Educacion y Ciencia, Spain [ENE2013-45661-C2-1-P]; Junta de Comunidades de Castilla-La Mancha, Spain [PEII-2014-008-P] FX This review is issued from a working group hosted by the international space science institute (ISSI) in Bern Switzerland. The authors acknowledge supports by ISSI. AM acknowledges the support by the french ANR MACH project. ACB acknowledges the support by Grant ENE2013-45661-C2-1-P from the Ministerio de Educacion y Ciencia, Spain and Grant PEII-2014-008-P from the Junta de Comunidades de Castilla-La Mancha, Spain. NR 460 TC 7 Z9 7 U1 13 U2 36 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0034-4885 EI 1361-6633 J9 REP PROG PHYS JI Rep. Prog. Phys. PD APR PY 2016 VL 79 IS 4 AR 046901 DI 10.1088/0034-4885/79/4/046901 PG 49 WC Physics, Multidisciplinary SC Physics GA DI0VZ UT WOS:000373216700006 PM 27007555 ER PT J AU Eastwood, G Loaiza, JR Pongsiri, MJ Sanjur, OI Pecor, JE Auguste, AJ Kramer, LD AF Eastwood, Gillian Loaiza, Jose R. Pongsiri, Montira J. Sanjur, Oris I. Pecor, James E. Auguste, Albert J. Kramer, Laura D. TI Enzootic Arbovirus Surveillance in Forest Habitat and Phylogenetic Characterization of Novel Isolates of Gamboa Virus in Panama SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE LA English DT Article ID VENEZUELAN EQUINE ENCEPHALITIS; AEDEOMYIA-SQUAMIPENNIS; YELLOW-FEVER; MOSQUITOS DIPTERA; CULICIDAE; AMERICA; IDENTIFICATION; BUNYAVIRUSES; TRANSMISSION; DIVERSITY AB Landscape changes occurring in Panama, a country whose geographic location and climate have historically supported arbovirus transmission, prompted the hypothesis that arbovirus prevalence increases with degradation of tropical forest habitats. Investigations at four variably degraded sites revealed a diverse array of potential mosquito vectors, several of which are known vectors of arbovirus pathogens. Overall, 675 pools consisting of 25,787 mosquitoes and representing 29 species from nine genera (collected at ground and canopy height across all habitats) were screened for cytopathic viruses on Vero cells. We detected four isolates of Gamboa virus (family: Bunyaviridae; genus: Ortho-bunyavirus) from pools of Aedeomyia squamipennis captured at canopy level in November 2012. Phylogenetic characterization of complete genome sequences shows the new isolates to be closely related to each other with strong evidence of reassortment among the M segment of Panamanian Gamboa isolates and several other viruses of this group. At the site yielding viruses, Soberania National Park in central Panama, 18 mosquito species were identified, and the predominant taxa included A. squamipennis, Coquillettidia nigricans, and Mansonia titillans. C1 [Eastwood, Gillian; Kramer, Laura D.] New York State Dept Hlth, Wadsworth Ctr, Slingerlands, NY USA. [Loaiza, Jose R.] Inst Invest Cient & Serv Alta Tecnol INDICASAT, Ciudad Del Saber, Panama. [Pongsiri, Montira J.] US EPA, Washington, DC 20460 USA. Smithsonian Trop Res Inst, Panama City, Panama. Walter Reed Biosystemat Unit, Suitland, MD USA. [Auguste, Albert J.] Univ Texas Med Branch, Dept Pathol, Keiller Bldg, Galveston, TX 77555 USA. [Sanjur, Oris I.] Smithsonian Trop Res Inst, Mol Biol & Evolut Labs, Ancon, Panama. [Pecor, James E.] Walter Reed Army Med Ctr, Walter Reed Army Inst Res, Dept Entomol, Washington, DC 20307 USA. RP Eastwood, G (reprint author), Univ Texas Med Branch, Dept Pathol, Keiller Bldg, Galveston, TX 77555 USA. EM gieastwo@utmb.edu; jloaiza@indicasat.org.pa; pongsiri.montira@epa.gov; sanjuro@si.edu; pecorj@si.edu; ajlaugus@utmb.edu; laura.kramer@health.ny.gov FU Robert E. Shope International Fellowship Award - American Society of Tropical Medicine and Hygiene; James W. McLaughlin Endowment fund; National Research Investigator Board (SNI) of the Secretariat for Science, Technology and Innovation of Panama (SENACYT); U.S. Environmental Protection Agency [DW33-92296801-0] FX Funding for this project was provided via the Robert E. Shope International Fellowship Award granted by the American Society of Tropical Medicine and Hygiene to Gillian Eastwood in 2012. Gillian Eastwood and Albert J. Auguste are also funded by the James W. McLaughlin Endowment fund. Jose R. Loaiza is funded by the National Research Investigator Board (SNI) of the Secretariat for Science, Technology and Innovation of Panama (SENACYT). The U.S. Environmental Protection Agency project "Mosquito Species Diversity and Landscape Change DW33-92296801-0" awarded to Montira Pongsiri covered the costs of mosquito sampling at Las Pavas, Achiote, and Barro Colorado Island, and some of the laboratory supplies and reagents used at NYSDOH. NR 45 TC 0 Z9 0 U1 3 U2 3 PU AMER SOC TROP MED & HYGIENE PI MCLEAN PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA SN 0002-9637 EI 1476-1645 J9 AM J TROP MED HYG JI Am. J. Trop. Med. Hyg. PD APR PY 2016 VL 94 IS 4 BP 786 EP 793 DI 10.4269/ajtmh.15-0445 PG 8 WC Public, Environmental & Occupational Health; Tropical Medicine SC Public, Environmental & Occupational Health; Tropical Medicine GA DI1FQ UT WOS:000373242400015 PM 26834200 ER PT J AU Schwartz, GE Rivera, N Lee, SW Harrington, JM Hower, JC Levine, KE Vengosh, A Hsu-Kim, H AF Schwartz, Grace E. Rivera, Nelson Lee, Sung-Woo Harrington, James M. Hower, James C. Levine, Keith E. Vengosh, Avner Hsu-Kim, Heileen TI Leaching potential and redox transformations of arsenic and selenium in sediment microcosms with fly ash SO APPLIED GEOCHEMISTRY LA English DT Article DE Coal combustion residuals; Water quality; Solid waste disposal ID FIRED POWER-PLANTS; COAL ASH; CONTAMINATED SOIL; ENVIRONMENTAL IMPACTS; SPECIATION; REDUCTION; TENNESSEE; KINGSTON; METALS; BEHAVIOR AB The unintended release of coal ash to the environment is a concern due to the enrichment of contaminants such as arsenic (As) and selenium (Se) in this solid waste material. Current risk assessments of coal ash disposal focus on pH as the primary driver of leaching from coal ash. However, redox speciation of As and Se is a major factor for their mobilization potential and has received much less attention for risk assessments, particularly in disposal scenarios where coal ash will likely be exposed to microbially-driven redox gradients. The aim of this study was to demonstrate the differences of aerobic and anaerobic conditions for the leaching of As and Se from coal ash. Batch sediment-ash slurry microcosms were performed to mimic an ash spill scenario and were monitored for changes in As and Se speciation and mobilization potential. The results showed that the dissolved As concentrations were up to 50 times greater in the anaerobic microcosms relative to the aerobic microcosms during the two week incubation. This trend was consistent with As redox speciation determined by X-ray absorption spectroscopy, which indicated that 55% of the As in the solid phase at the end of the experiment was present as As(III) (a more leachable form of arsenic relative to As(V)). In the aerobic microcosms, only 13% of the As was As(III) and the rest was As(V). More than half of the Se was present as Se(IV) in the original fly ash and in the aerobic microcosms, while in the anaerobic microcosms Se was gradually transformed to less soluble Se(0) species. Likewise, dissolved Se concentrations were up to 25 times greater in the aerobic microcosms relative to anaerobic conditions. While the overall observations of As and Se mobilization potential from coal ash were consistent with expectations for aqueous and solid phase speciation of these elements, the findings directly show the relevance of these processes for coal ash disposal. These results highlight the need to select appropriate environmental parameters to include in risk assessments as well as provide potential geochemical monitoring tools through the use of dissolved Se/As ratios to determine the redox conditions of ash storage and spill sites. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Schwartz, Grace E.; Rivera, Nelson; Lee, Sung-Woo; Hsu-Kim, Heileen] Duke Univ, Dept Civil & Environm Engn, 121 Hudson Hall, Durham, NC 27708 USA. [Harrington, James M.; Levine, Keith E.] RTI Int, Analyt Sci, 3040 East Cornwallis Dr, Res Triangle Pk, NC 27709 USA. [Hower, James C.] Univ Kentucky, Ctr Appl Energy Res, 2540 Res Pk Dr, Lexington, KY 40511 USA. [Vengosh, Avner] Duke Univ, Nicholas Sch Environm, Div Earth & Ocean Sci, Durham, NC 27708 USA. [Schwartz, Grace E.] Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. RP Hsu-Kim, H (reprint author), Duke Univ, Dept Civil & Environm Engn, 121 Hudson Hall, Durham, NC 27708 USA. EM hsukim@duke.edu RI Hsu-Kim, Heileen/A-5409-2008 OI Hsu-Kim, Heileen/0000-0003-0675-4308 FU National Science Foundation [CBET-1235661]; Environmental Research and Education Foundation FX We thank the Tennessee Valley Authority, Restoration Services, and Environmental Services for their assistance with field sample collection. We also thank Kaitlyn Porter for her assistance with ICP-MS measurements. This work was supported by the National Science Foundation (CBET-1235661). G. Schwartz was also partly supported by a doctoral scholarship from the Environmental Research and Education Foundation. NR 51 TC 3 Z9 3 U1 9 U2 33 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0883-2927 J9 APPL GEOCHEM JI Appl. Geochem. PD APR PY 2016 VL 67 BP 177 EP 185 DI 10.1016/j.apgeochem.2016.02.013 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DH3XU UT WOS:000372720900016 ER PT J AU Andrews, SM Wilner, DJ Zhu, ZH Birnstiel, T Carpenter, JM Perez, LM Bai, XN Oberg, KI Hughes, AM Isella, A Ricci, L AF Andrews, Sean M. Wilner, David J. Zhu, Zhaohuan Birnstiel, Tilman Carpenter, John M. Perez, Laura M. Bai, Xue-Ning Oeberg, Karin I. Hughes, A. Meredith Isella, Andrea Ricci, Luca TI RINGED SUBSTRUCTURE AND A GAP AT 1 au IN THE NEAREST PROTOPLANETARY DISK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planet-disk interactions; protoplanetary disks; stars: individual (TW Hydrae) ID LOW-MASS PLANETS; VERTICAL MAGNETIC-FIELDS; TW HYA DISK; ACCRETION DISKS; ALMA OBSERVATIONS; SCATTERED-LIGHT; DUST PARTICLES; DENSITY WAVES; OUTER REGIONS; SOLAR NEBULA AB We present long baseline Atacama Large Millimeter/submillimeter Array (ALMA) observations of the 870 mu m continuum emission from the nearest gas-rich protoplanetary disk, around TW Hya, that trace millimeter-sized particles down to spatial scales as small as 1 au (20 mas). These data reveal a series of concentric ring-shaped substructures in the form of bright zones and narrow dark annuli (1-6 au) with modest contrasts (5%-30%). We associate these features with concentrations of solids that have had their inward radial drift slowed or stopped, presumably at local gas pressure maxima. No significant non-axisymmetric structures are detected. Some of the observed features occur near temperatures that may be associated with the condensation fronts of major volatile species, but the relatively small brightness contrasts may also be a consequence of magnetized disk evolution (the so-called zonal flows). Other features, particularly a narrow dark annulus located only 1 au from the star, could indicate interactions between the disk and young planets. These data signal that ordered substructures on similar to au scales can be common, fundamental factors in disk evolution and that high-resolution microwave imaging can help characterize them during the epoch of planet formation. C1 [Andrews, Sean M.; Wilner, David J.; Bai, Xue-Ning; Oeberg, Karin I.; Ricci, Luca] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Zhu, Zhaohuan] Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane,Peyton Hall, Princeton, NJ 08544 USA. [Birnstiel, Tilman] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Carpenter, John M.] Joint ALMA Observ JAO, Alonso Cordova 3107, Vitacura Santiago Chile, Chile. [Perez, Laura M.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Hughes, A. Meredith] Wesleyan Univ, Dept Astron, Van Vleck Observ, 96 Foss Hill Dr, Middletown, CT 06457 USA. [Isella, Andrea] Rice Univ, Dept Phys & Astron, 6100 Main St, Houston, TX 77005 USA. RP Andrews, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sandrews@cfa.harvard.edu OI Birnstiel, Tilman/0000-0002-1899-8783 FU DFG [KL 1469/13-1] FX We thank Ian Czekala for advice on the figures, the NRAO/NAASC staff for their assistance with the data calibration, and Ilse Cleeves and Ruobing Dong for helpful conversations. This research greatly benefited from the Astropy (Astropy Collaboration et al. 2013) and Matplotlib (Hunter 2007) software packages. This Letter makes use of the following ALMA data: ADS/JAO. ALMA#2015.1.00686. S, ADS/JAO. ALMA#2011.1.00399. S, and ADS/JAO. ALMA#2013.1.00198. S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory (NRAO) is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. T.B. acknowledges support from the DFG through grant (KL 1469/13-1). NR 55 TC 24 Z9 25 U1 2 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 1 PY 2016 VL 820 IS 2 AR L40 DI 10.3847/2041-8205/820/2/L40 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH8ZL UT WOS:000373085300018 ER PT J AU Pillitteri, I Wolk, SJ Megeath, ST AF Pillitteri, I. Wolk, S. J. Megeath, S. T. TI A STAR-FORMING RING AROUND kappa Ori 250 pc FROM THE SUN SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: activity; stars: formation; stars: individual (Orion A, L1641, Kappa Ori) ID YOUNG STELLAR OBJECTS; PARSEC EVOLUTIONARY TRACKS; SPACE-TELESCOPE SURVEY; LYNDS 1641; MASSIVE STARS; POPULATION; MONOCEROS; ROSETTE; REGIONS; CLUSTER AB X-rays are a powerful probe of activity in early stages of star formation. They allow us to identify young stars even after they have lost the IR signatures of circumstellar disks and provide constraints on their distance. Here, we report on XMM-Newton observations that detect 121 young stellar objects (YSOs) in two fields between L1641 S and kappa Ori. These observations extend the Survey of Orion. A with XMM and Spitzer (SOXS). The YSOs are contained in a ring of gas and dust apparent at millimeter wavelengths, and in far-IR and near-IR surveys. The X-ray luminosity function of the YSOs detected in the two fields indicates a distance of 250-280 pc, much closer than the Orion. A cloud and similar to distance estimates of kappa Ori. We propose that the ring is a 5-8 pc diameter shell that has been swept up by kappa Ori. This ring contains several groups of stars detected by Spitzer and WISE including one surrounding the Herbig Ae/Be stars V1818. Ori. In this interpretation, the kappa Ori ring is one of several shells swept up by massive stars within the Orion Eridanus Superbubble and is unrelated to the southern portion of Orion. A/L1641 S. C1 [Pillitteri, I.; Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Pillitteri, I.] INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy. [Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA. RP Pillitteri, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Pillitteri, I (reprint author), INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy. EM ipillitt@cfa.harvard.edu RI Pillitteri, Ignazio/L-1549-2016 OI Pillitteri, Ignazio/0000-0003-4948-6550 FU NASA [NAS8-03060] FX S.T.M. acknowledges useful discussions with Noel Richardson and Adolf Witt. S.J.W. was supported by NASA contract NAS8-03060. NR 29 TC 0 Z9 0 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 1 PY 2016 VL 820 IS 2 AR L28 DI 10.3847/2041-8205/820/2/L28 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH8ZL UT WOS:000373085300006 ER PT J AU Kuchta, SR Haughey, M Wynn, AH Jacobs, JF Highton, R AF Kuchta, Shawn R. Haughey, Michael Wynn, Addison H. Jacobs, Jeremy F. Highton, Richard TI Ancient river systems and phylogeographical structure in the spring salamander, Gyrinophilus porphyriticus SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Appalachian River; cytochrome b; distance-based redundancy analysis; Gyrinophilus; Plethodontidae; phylogeography; RAG-1; stream capture; Teays River ID SPECIES ENSATINA-ESCHSCHOLTZII; PLETHODONTID SALAMANDERS; HISTORICAL BIOGEOGRAPHY; PHYLOGENETIC ANALYSIS; GENE GENEALOGIES; DIVERGENCE DATES; CALIFORNIA NEWT; TARICHA-TOROSA; EVOLUTION; DIVERSIFICATION AB AimThe river drainages of the Appalachian Mountains have experienced a dynamic history as glacial cycles, stream capture and other geological processes have led to the fragmentation and fusion of formerly isolated palaeodrainages. Some ancient rivers have gone extinct, including portions of the great Teays River. Here we investigate the contribution of contemporary and historical drainages to patterns of phylogeographical structure in the spring salamander complex, Gyrinophilus porphyriticus. LocationEastern North America, USA. MethodsSampling spanned the range of the G. porphyriticus complex, and included representative samples of the cave species of Gyrinophilus as well. Molecular sequence data included the mitochondrial DNA locus cytochrome b and the nuclear locus recombination-activating gene 1 (RAG-1). Time-calibrated phylogenies were inferred, and Bayes-LAGRANGE was used to reconstruct ancestral distributions. Contemporary and historical river influences on patterns of genetic diversity were tested using distance-based redundancy analysis (db-RDA). ResultsThe G. porphyriticus complex originated prior to the Pleistocene glacial cycles, and historical river systems explained more genetic variation than did contemporary drainages or geographical distance. Patterns of genetic variation suggest that extinct or remodelled palaeodrainages, including the Teays River, played an important role in structuring contemporary patterns of genetic variation. Main conclusionsThe hydrogeological history of eastern North American drainage basins has been instrumental in structuring patterns of regional biodiversity in freshwater species. Here we show that hydrological remodelling has also left its genetic signature in the semi-aquatic spring salamander complex, G. porphyriticus. Historical drainages accounted for the largest fraction of phylogeographical structure, more so than did contemporary drainages or geographical distance, with spatial and temporal patterns of variation associated with the extinct Teays River. C1 [Kuchta, Shawn R.; Haughey, Michael] Ohio Univ, Dept Biol Sci, Ohio Ctr Ecol & Evolutionary Studies, Athens, OH 45701 USA. [Wynn, Addison H.; Jacobs, Jeremy F.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Highton, Richard] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Kuchta, SR (reprint author), Oho Univ, Dept Biol Sci, Ohio Ctr Ecol & Evolutionary Studies, 107 Irvine, Athens, OH 45701 USA. EM kuchta@ohio.edu FU Ohio University, Program to Aid in Career Exploration (PACE); Honors Tutorial College (HTC) FX Financial support was provided to S.R.K. by Ohio University, including the Program to Aid in Career Exploration (PACE) and the Honors Tutorial College (HTC). We thank Ashley Brown and Elizabeth Makley for their assistance in the DNA lab, and Paul Converse, Maggie Hantak, and Tom Radomski for their comments on drafts of the manuscript. We thank Ronald A. Brandon, John R. MacGregor, David M. Sever, R. Wayne Van Devender, and the many other people who provided specimens and helped with fieldwork. NR 56 TC 2 Z9 2 U1 8 U2 23 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 APR PY 2016 VL 43 IS 4 BP 639 EP 652 DI 10.1111/jbi.12668 PG 14 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA DH9ZH UT WOS:000373154000001 ER PT J AU Riley, SM AF Riley, Sheila M. TI Three-Martini Lunch SO LIBRARY JOURNAL LA English DT Book Review C1 [Riley, Sheila M.] Smithsonian Inst Libs, Washington, DC USA. RP Riley, SM (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR 1 PY 2016 VL 141 IS 6 BP 87 EP 87 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA DI1JF UT WOS:000373251700109 ER PT J AU Thurman, TJ Barrett, RDH AF Thurman, Timothy J. Barrett, Rowan D. H. TI The genetic consequences of selection in natural populations SO MOLECULAR ECOLOGY LA English DT Review DE evolution; genetics; meta-analysis; natural populations; natural selection; selection coefficient ID FISHERS GEOMETRICAL MODEL; FITNESS TRADE-OFFS; TIME-SERIES DATA; PHENOTYPIC SELECTION; DIRECTIONAL SELECTION; LOCAL ADAPTATION; MOVING OPTIMUM; BENEFICIAL MUTATIONS; MOLECULAR EVOLUTION; ADAPTIVE EVOLUTION AB The selection coefficient, s, quantifies the strength of selection acting on a genetic variant. Despite this parameter's central importance to population genetic models, until recently we have known relatively little about the value of s in natural populations. With the development of molecular genetic techniques in the late 20th century and the sequencing technologies that followed, biologists are now able to identify genetic variants and directly relate them to organismal fitness. We reviewed the literature for published estimates of natural selection acting at the genetic level and found over 3000 estimates of selection coefficients from 79 studies. Selection coefficients were roughly exponentially distributed, suggesting that the impact of selection at the genetic level is generally weak but can occasionally be quite strong. We used both nonparametric statistics and formal random-effects meta-analysis to determine how selection varies across biological and methodological categories. Selection was stronger when measured over shorter timescales, with the mean magnitude of s greatest for studies that measured selection within a single generation. Our analyses found conflicting trends when considering how selection varies with the genetic scale (e.g., SNPs or haplotypes) at which it is measured, suggesting a need for further research. Besides these quantitative conclusions, we highlight key issues in the calculation, interpretation, and reporting of selection coefficients and provide recommendations for future research. C1 [Thurman, Timothy J.; Barrett, Rowan D. H.] McGill Univ, Redpath Museum, Sherbrooke St West, Montreal, PQ H3A 1B1, Canada. [Thurman, Timothy J.; Barrett, Rowan D. H.] McGill Univ, Dept Biol, Sherbrooke St West, Montreal, PQ H3A 1B1, Canada. [Thurman, Timothy J.] Smithsonian Trop Res Inst, Panama City, Panama. RP Thurman, TJ (reprint author), McGill Univ, Redpath Museum, Sherbrooke St West, Montreal, PQ H3A 1B1, Canada.; Thurman, TJ (reprint author), McGill Univ, Dept Biol, Sherbrooke St West, Montreal, PQ H3A 1B1, Canada.; Thurman, TJ (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM timothy.thurman@mail.mcgill.ca FU STRI-McGill-NEO fellowship; Canada Research Chair; Natural Science and Engineering Research Council FX We thank J. Anderson, W. Eanes, P. Gerbault, Z. Gompert, J. Prunier and S. Taylor for providing data, K. Gotanda for access to the preliminary database of Siepielski et al. 2013, and J. Hadfield and S. Diamond for answering questions about MCMCglmm. S. Otto, P. Nosil and W.O. McMillan provided helpful comments on an earlier version of this manuscript. S. Otto also co-authored Appendix S1 (Supporting information). We thank L. Bernatchez, A. Eyre-Walker and two anonymous reviewers for helpful comments that improved this manuscript. This work was supported by a STRI-McGill-NEO fellowship to T.J.T. and funding from a Canada Research Chair and a Natural Science and Engineering Research Council Discovery grant to R.D.H.B. NR 98 TC 7 Z9 7 U1 34 U2 60 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 2016 VL 25 IS 7 BP 1429 EP 1448 DI 10.1111/mec.13559 PG 20 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA DH9GN UT WOS:000373104500004 PM 26836758 ER PT J AU Collins, CG Wright, SJ Wurzburger, N AF Collins, Courtney G. Wright, S. Joseph Wurzburger, Nina TI Root and leaf traits reflect distinct resource acquisition strategies in tropical lianas and trees SO OECOLOGIA LA English DT Article DE Economic spectrum; Trade-offs; Mycorrhiza; Specific root length; Specific leaf area ID PLANT FUNCTIONAL TRAITS; BARRO-COLORADO ISLAND; LIFE-SPAN; MYCORRHIZAL COLONIZATION; AMAZONIAN FORESTS; GLOBAL PATTERNS; TRADE-OFFS; COMMUNITY; GROWTH; ECOSYSTEMS AB In Neotropical forests, lianas are increasing in abundance relative to trees. This increased species richness may reflect a positive response to global change factors including increased temperature, atmospheric CO2, habitat fragmentation, and drought severity; however, questions remain as to the specific mechanisms facilitating the response. Previous work suggests that lianas may gain an ecological advantage over trees through leaf functional traits that offer a quick return on investment of resources, although it is unknown whether this pattern extends to root traits and relationships with fungal or bacterial symbionts belowground. We sampled confamilial pairs of liana and tree species and quantified morphological and chemical traits of leaves and fine roots, as well as root symbiont abundance, to determine whether functional traits associated with resource acquisition differed between the two. Compared to trees, lianas possessed higher specific leaf area, specific root length, root branching intensity, and root nitrogen (N) and phosphorus (P) concentrations, and lower leaf and root tissue density, leaf and root carbon (C), root diameter, root C:P and N:P, and mycorrhizal colonization. Our study provides new evidence that liana leaf and root traits are characterized by a rapid resource acquisition strategy relative to trees. These liana functional traits may facilitate their response to global change, raising questions about how increased liana dominance might affect ecosystem processes of Neotropical forests. C1 [Collins, Courtney G.; Wurzburger, Nina] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Collins, CG (reprint author), Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. EM courtneygrace125@gmail.com RI Wright, Stuart/M-3311-2013; OI Wright, Stuart/0000-0003-4260-5676; Collins, Courtney/0000-0001-5455-172X FU University of Georgia; Odum School of Ecology; Smithsonian Tropical Research Institute FX We thank Rufino Gonzalez and Oldemar Valdez for field assistance and plant identification, Rick Lankau for statistical advice, Stefan Schnitzer for liana species information, Tom Maddox and Ben Turner for chemical analyses, Shialoh Wilson, Tierney O'Sullivan and Dina Abdulhadi for assistance in the lab, Kelly Andersen for comments and logistical support, and Teresa Bohner and Jake Allgeier for assistance with graphics. Funding was provided by the University of Georgia and the Odum School of Ecology, and research was conducted under a short term fellowship at the Smithsonian Tropical Research Institute. NR 82 TC 2 Z9 2 U1 13 U2 49 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD APR PY 2016 VL 180 IS 4 BP 1037 EP 1047 DI 10.1007/s00442-015-3410-7 PG 11 WC Ecology SC Environmental Sciences & Ecology GA DI0KV UT WOS:000373186100012 PM 26254258 ER PT J AU George, TS Hinsinger, P Turner, BL AF George, Timothy S. Hinsinger, Philippe Turner, Benjamin L. TI Phosphorus in soils and plants - facing phosphorus scarcity SO PLANT AND SOIL LA English DT Editorial Material DE Ecosystemdynamics; Environmental impact; Phosphorus acquisition; Phosphorus forms; Phosphorus cycling; Phosphorus utilization; Phosphorus signalling; Sustainable use and management ID SECURITY; ISSUES AB Introduction Phosphorus is a fundamental nutrient for primary productivity of ecosystems and agricultural production, but its misuse impacts agricultural sustainability and has important environmental consequences. Access to global reserves of phosphate rock is politically sensitive and economically challenging. Phosphorus accumulates in agricultural soils, representing a financial loss to farmers and increasing the risk of loss to water. The challenges facing phosphorus sustainability are varied, but many solutions are to be found in the plant-soil system. Scope This special issue arises from the 5th International Symposium on Phosphorus in Soils and Plants (PSP5), held in Montpellier, France. Articles highlighted here discuss ways to tackle food security, improve phosphorus sustainability by understanding the imbalanced phosphorus cycle, use technology to reduce phosphorus demand and recycle phosphorus in waste products, and consider how efforts to increase phosphorus efficiency interact with other sustainability challenges. Conclusions The challenges associated with P sustainability are tackled from many different directions, including plant genetics, soil microbiology, novel imaging and modelling techniques, the development of new technologies, and an improved understanding of how these technologies interact with agronomic management. Integration of the various approaches will be necessary to deliver a truly effective solution to the challenge of attaining phosphorus sustainability. C1 [George, Timothy S.] James Hutton Inst, Dundee DD2 5DA, Scotland. [Hinsinger, Philippe] INRA, UMR Eco&Sols, Pl Viala, F-34060 Montpellier, France. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. RP George, TS (reprint author), James Hutton Inst, Dundee DD2 5DA, Scotland. EM tim.george@hutton.ac.uk RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 NR 11 TC 1 Z9 1 U1 31 U2 92 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0032-079X EI 1573-5036 J9 PLANT SOIL JI Plant Soil PD APR PY 2016 VL 401 IS 1-2 BP 1 EP 6 DI 10.1007/s11104-016-2846-9 PG 6 WC Agronomy; Plant Sciences; Soil Science SC Agriculture; Plant Sciences GA DH7CC UT WOS:000372947800001 ER PT J AU Galbany, J Stoinski, TS Abavandimwe, D Breuer, T Rutkowski, W Batista, NV Ndagijimana, F McFarlin, SC AF Galbany, Jordi Stoinski, Tara S. Abavandimwe, Didier Breuer, Thomas Rutkowski, William Batista, Nicholas V. Ndagijimana, Felix McFarlin, Shannon C. TI Validation of Two Independent Photogrammetric Techniques for Determining Body Measurements of Gorillas SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE photogrammetry; parallel laser; distance meter; gorilla ID DIGITAL PHOTOGRAMMETRY; WESTERN GORILLAS; BERINGEI-BERINGEI; LIFE-HISTORY; WILD; GROWTH; CHIMPANZEES; SWELLINGS; BABOONS; SIZE AB The ability to accurately measure morphological characteristics of wild primates in the field is challenging, yet critical for understanding fundamental aspects of their biology and behavior. Recent studies have shown that digital photogrammetry can be used to non-invasively measure morphological traits of wild primates, as it allows for the determination of geometric properties of objects remotely from photographic images. We report here on a rare opportunity to test this methodology by comparing measurements obtained directly from living great apes to those obtained from photographs. We test the accuracy and precision of two independent photogrammetric techniques, employing the use of parallel lasers and a distance meter, respectively, for obtaining measurements of static objects and captive western lowland gorillas (Gorilla gorilla gorilla) (n = 4) at Zoo Atlanta. For static objects, the mean percent error between corresponding measurements collected by the same observer directly versus using photogrammetry was 0.49-0.74% for the parallel laser method and 0.62-0.76% for the distance meter method. For gorillas, mean percent error between corresponding direct and remote measurements was 2.72-5.20% for the parallel laser method and 2.20-7.51% for the distance meter method. Correlations between direct measurements and corresponding parallel laser and distance meter measurements of gorillas were highly significant with R-2 values and slopes approaching 1.0 (parallel lasers: R-2 = 0.9989, P < 0.0001; distance-meter: R-2 = 0.9990, P < 0.0001). Further, variation between measurements of the same targets collected repeatedly by the same observer, and between different observers, was uniformly low across methods (CV, range = 0.003-0.013). While errors are slightly higher for the distance meter technique, both methods show great promise for addressing a wide range of questions requiring the non-invasive collection of morphological data from wild primates. (C) 2015 Wiley Periodicals, Inc. C1 [Galbany, Jordi; McFarlin, Shannon C.] George Washington Univ, Ctr Adv Study Human Paleobiol, Dept Anthropol, 800 22nd St NW,Ste 6000, Washington, DC 20052 USA. [Stoinski, Tara S.; Abavandimwe, Didier; Ndagijimana, Felix] Dian Fossey Gorilla Fund Int, Atlanta, GA USA. [Stoinski, Tara S.] Zoo Atlanta, Atlanta, GA USA. [Breuer, Thomas] Wildlife Conservat Soc, Global Conservat Program, Bronx, NY USA. [Rutkowski, William] George Washington Univ, Dept Phys, 800 22nd St NW,Ste 6000, Washington, DC 20052 USA. [Batista, Nicholas V.] George Washington Univ, Dept Mech & Aerosp Engn, 800 22nd St NW,Ste 6000, Washington, DC 20052 USA. [McFarlin, Shannon C.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. RP Galbany, J (reprint author), George Washington Univ, Ctr Adv Study Human Paleobiol, Dept Anthropol, 800 22nd St NW,Ste 6000, Washington, DC 20052 USA. EM jgalbany@gwu.edu FU Leakey Foundation; Wenner Gren Foundation; Center & Institute Facilitating Fund and Signature Program; Columbian College of Arts and Sciences; National Science Foundation [BCS 1520221] FX Contract grant sponsor: The Leakey Foundation; contract grant sponsor: The Wenner Gren Foundation; contract grant sponsor: Center & Institute Facilitating Fund and Signature Program funding to the Center for the Advanced Study of Human Paleobiology, The George Washington University; contract grant sponsor: Columbian College of Arts and Sciences; contract grant sponsor: National Science Foundation; contract grant number: BCS 1520221. NR 54 TC 1 Z9 1 U1 5 U2 10 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 APR PY 2016 VL 78 IS 4 BP 418 EP 431 DI 10.1002/ajp.22511 PG 14 WC Zoology SC Zoology GA DH0QQ UT WOS:000372489100003 ER PT J AU Kearns, AM Joseph, L White, LC Austin, JJ Baker, C Driskell, AC Malloy, JF Omland, KE AF Kearns, Anna M. Joseph, Leo White, Lauren C. Austin, Jeremy J. Baker, Caitlin Driskell, Amy C. Malloy, John F. Omland, Kevin E. TI Norfolk Island Robins are a distinct endangered species: ancient DNA unlocks surprising relationships and phenotypic discordance within the Australo-Pacific Robins SO CONSERVATION GENETICS LA English DT Article DE Ancient DNA; Conservation genetics; Endangered species; Insular speciation; Norfolk Island; Pacific ID NINOX-NOVAESEELANDIAE-UNDULATA; MOLECULAR SYSTEMATICS; PHYLOGENETIC ANALYSES; EVOLUTIONARY HISTORY; MAXIMUM-LIKELIHOOD; CONSERVATION; PETROICIDAE; PLUMAGE; BIRDS; AVES AB Uncertain taxonomy hinders the effective prioritization of taxa for conservation. This problem is acute for understudied island populations in the southwest Pacific Ocean, which are increasingly threatened by habitat loss, predation and climate change. Here, we offer the first test of taxonomic limits and phylogenetic affinities of the iconic Pacific Robin radiation (Petroica multicolor) in order to prioritize the conservation of its nominotypical subspecies, the endangered Norfolk Island Robin (P. m. multicolor). We integrate phylogenetic analyses of ancient DNA and quantitative measures of plumage and morphometric variation to show that the Norfolk Island Robin should be recognized as a distinct species. Phenotypic and genetic datasets contradict the longstanding treatment of Pacific Robins (including Norfolk Island Robins) and Scarlet Robins (P. boodang) as a single species. Instead, we show that Norfolk Island Robins are deeply divergent from Scarlet Robins and have more genetic similarity to Red-capped Robins (P. goodenovii) than to other Pacific Robins. This finding is unrepresentative of the current taxonomic and conservation status of the Norfolk Island Robin, which we propose should be recognised as an endemic endangered species. Our study clearly shows that in the absence of contemporary tissues, ancient DNA approaches using historical museum specimens can address taxonomic questions that morphological traits are unable to resolve. Further, it highlights the need for similar studies of other threatened Norfolk fauna with uncertain taxonomic status in order to ensure appropriate conservation prioritization. C1 [Kearns, Anna M.; Malloy, John F.; Omland, Kevin E.] Univ Maryland Baltimore Cty, Dept Biol Sci, 1000 Hilltop Circle, Baltimore, MD 21250 USA. [Kearns, Anna M.] Univ Oslo, Nat Hist Museum, POB 1172, N-0318 Oslo, Norway. [Joseph, Leo] CSIRO Natl Res Collect Australia, Australian Natl Wildlife Collect, GPO Box 1700, Canberra, ACT 2601, Australia. [White, Lauren C.; Austin, Jeremy J.] Univ Adelaide, Australian Ctr Ancient DNA, Sch Earth & Environm Sci, N Terrace, Adelaide, SA 5005, Australia. [White, Lauren C.; Austin, Jeremy J.] Univ Adelaide, Inst Environm, N Terrace, Adelaide, SA 5005, Australia. [Austin, Jeremy J.] Museum Victoria, Dept Sci, Carlton Gardens, Melbourne, Vic 3000, Australia. [Baker, Caitlin] Harvard Univ, Dept Organism & Evolutionary Biol, Museum Comparat Zool, 26 Oxford St, Cambridge, MA 02138 USA. [Baker, Caitlin; Driskell, Amy C.] Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Washington, DC 20013 USA. RP Kearns, AM (reprint author), Univ Maryland Baltimore Cty, Dept Biol Sci, 1000 Hilltop Circle, Baltimore, MD 21250 USA.; Kearns, AM (reprint author), Univ Oslo, Nat Hist Museum, POB 1172, N-0318 Oslo, Norway. EM anna.m.kearns@gmail.com RI Joseph, Leo/F-9235-2010; OI Kearns, Anna/0000-0002-8502-7442 FU NSF [DEB-1119506]; Australian Biological Resources Study Churchill Fellowship FX We thank the following institutions, collectors, collection managers, staff and curators for the specimens or sequences used in this study: Paul Sweet, Thomas Trombone, Lydia Garetano, Peter Capainolo and Chris Filardi at the American Museum of Natural History, Jean Woods at the Delaware Museum of Natural History, A. Townsend Peterson, Michael Andersen and Mark Robbins at the Kansas University Natural History Museum, David Steadman, Andrew Kratter and Tom Webber at the Ornithology Division of the Florida Museum of Natural History, Robb Brumfield and Donna Dittmann at the Louisiana State University Museum of Natural Sciences, Robert Palmer at the Australian National Wildlife Collection and Susanne Metcalfe at CSIRO Ecosystem Sciences, Gaynor Dolman at the Western Australian Museum, Joanna Sumner at the Museum of Victoria, Aude Thierry, Tammy Steeves and Jim Briskie at the University of Canterbury, and Sharon Birks at the University of Washington Burke Museum. We thank David Yeates, Kerensa McElroy and two anonymous reviewers for helpful comments. Allen Kearns helped measure specimens. Analyses were run on the UMBC High Performance Computing Facility and CIPRES. This research was funded by NSF grant DEB-1119506 to K. E. Omland and an Australian Biological Resources Study Churchill Fellowship to A. M. Kearns. NR 66 TC 1 Z9 1 U1 1 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 EI 1572-9737 J9 CONSERV GENET JI Conserv. Genet. PD APR PY 2016 VL 17 IS 2 BP 321 EP 335 DI 10.1007/s10592-015-0783-4 PG 15 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA DG7QI UT WOS:000372278400007 ER PT J AU Hedrick, PW Hoeck, PEA Fleischer, RC Farabaugh, S Masuda, BM AF Hedrick, Philip W. Hoeck, Paquita E. A. Fleischer, Robert C. Farabaugh, Susan Masuda, Bryce M. TI The influence of captive breeding management on founder representation and inbreeding in the 'AlalA, the Hawaiian crow SO CONSERVATION GENETICS LA English DT Article DE Ancestry; Genetic drift; Inbreeding; Inbreeding depression; Pedigree ID DEPRESSION; PEDIGREES; MEXICAN AB The 'AlalA (Corvus hawaiiensis), or the Hawaiian crow, was historically only found on the island of Hawai'i, declined greatly in the twentieth century, and was last seen in the wild in 2002. A captive breeding program was initiated in the 1970s and 113 individuals were in captivity in 2014. All of the present day individuals are descended from nine founders. From pedigree analysis, 50 % of the initial ancestry was from a single founder pair and as of 2014, 45 % of the ancestry was still from this pair. Six other founders have also contributed substantially to the population and managed breeding has increased and evened out their contributions in recent years. Managed breeding has also kept the inbreeding level at the relatively low level of 0.120 in 2014. However, for most of the history of the population, all of the inbreeding was from the single founder pair and in 2014, 76 % of the inbreeding was still from this pair. As a result, the high inbreeding depression previously seen in this population appears to descend from this single pair. Breeding management to maximize founder genome equivalents, which takes into account loss of variation from genetic drift, could increase the genetic representation from the founders, particularly if ancestry from the single founder with only one living descendant is increased. C1 [Hedrick, Philip W.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. [Hoeck, Paquita E. A.; Farabaugh, Susan] San Diego Zoo Global, Inst Conservat Res, 15600 San Pasqual Valley Rd, Escondido, CA 92027 USA. [Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, 3001 Connecticut Ave NW, Washington, DC 20008 USA. [Masuda, Bryce M.] San Diego Zoo Global, Inst Conservat Res, POB 39, Volcano, HI 96785 USA. RP Hedrick, PW (reprint author), Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. EM philip.hedrick@asu.edu FU Ullman Professorship; U.S. Fish and Wildlife Service; Hawai'i Division of Forestry and Wildlife; Moore Family Foundation; Marisla Foundation; San Diego Zoo Global FX PWH was partially supported by the Ullman Professorship. Funding was provided by the U.S. Fish and Wildlife Service, Hawai'i Division of Forestry and Wildlife, Moore Family Foundation, Marisla Foundation, several anonymous donors, and the San Diego Zoo Global. PWH thanks Bob Lacy for his assistance in calculating individual inbreeding coefficients. Thank you to Rich Fredrickson for assistance with some of the figures. Many thanks to the staff and interns at the captive breeding facilities on Maui (Maui Bird Conservation Center) and Hawai'i (Keauhou Bird Conservation Center) and particularly to Marla Kuhn, Tracey Goltz, and Lisa Komarczyk for their efforts. We appreciate comments by Fern Duvall on early captive breeding and Jolene Sutton and several anonymous reviewers on the manuscript. NR 31 TC 1 Z9 1 U1 13 U2 25 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 EI 1572-9737 J9 CONSERV GENET JI Conserv. Genet. PD APR PY 2016 VL 17 IS 2 BP 369 EP 378 DI 10.1007/s10592-015-0788-z PG 10 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA DG7QI UT WOS:000372278400011 ER PT J AU Corrales, A Mangan, SA Turner, BL Dalling, JW AF Corrales, Adriana Mangan, Scott A. Turner, Benjamin L. Dalling, James W. TI An ectomycorrhizal nitrogen economy facilitates monodominance in a neotropical forest SO ECOLOGY LETTERS LA English DT Article DE Decomposition; Juglandaceae; mycorrhizal networks; mycorrhizal symbiosis; Panama; stable isotopes ID TROPICAL RAIN-FORESTS; MYCORRHIZAL FUNGI; TEMPERATE FORESTS; SEEDLING SURVIVAL; SOIL COMMUNITY; CARBON STORAGE; NEW-CALEDONIA; NETWORKS; PLANTS; FEEDBACK AB Tropical forests are renowned for their high diversity, yet in many sites a single tree species accounts for the majority of the individuals in a stand. An explanation for these monodominant forests remains elusive, but may be linked to mycorrhizal symbioses. We tested three hypotheses by which ectomycorrhizas might facilitate the dominance of the tree, Oreomunnea mexicana, in montane tropical forest in Panama. We tested whether access to ectomycorrhizal networks improved growth and survival of seedlings, evaluated whether ectomycorrhizal fungi promote seedling growth via positive plant-soil feedback, and measured whether Oreomunnea reduced inorganic nitrogen availability. We found no evidence that Oreomunnea benefits from ectomycorrhizal networks or plant-soil feedback. However, we found three-fold higher soil nitrate and ammonium concentrations outside than inside Oreomunnea-dominated forest and a correlation between soil nitrate and Oreomunnea abundance in plots. Ectomycorrhizal effects on nitrogen cycling might therefore provide an explanation for the monodominance of ectomycorrhizal tree species worldwide. C1 [Corrales, Adriana; Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Mangan, Scott A.] Washington Univ, Dept Biol, Campus Box 1137, St Louis, MO 63130 USA. [Mangan, Scott A.; Turner, Benjamin L.; Dalling, James W.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. RP Corrales, A (reprint author), Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. EM adricorrales33@gmail.com RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU Smithsonian Tropical Research Institute predoctoral Fellowship; Graduate College at University of Illinois; COLCIENCIAS [497-2009]; Government of Panama (SENACYT) grant [COLO08-003] FX Funding from the Smithsonian Tropical Research Institute predoctoral Fellowship and the Graduate College at University of Illinois are gratefully acknowledged. We thank COLCIENCIAS (497-2009) for providing financial support to AC. Forest plot work was supported by the Government of Panama (SENACYT) grant (COLO08-003). We thank Katie Heineman, Carlos Espinosa, Cecilia Prada, Camilo Zalamea and Carolina Sarmiento for their help during the development of project; Mike Masters, Dayana Agudo and Aleksandra Bielnicka for help with resin bag and isotopic analysis, Pedro Caballero, Fredy Miranda, Jan Miranda and Evidelio Garcia for help with fieldwork and logistic support, and Leho Tedersoo and four anonymous reviewers for thoughtful reviews of this manuscript. NR 49 TC 9 Z9 9 U1 13 U2 52 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 APR PY 2016 VL 19 IS 4 BP 383 EP 392 DI 10.1111/ele.12570 PG 10 WC Ecology SC Environmental Sciences & Ecology GA DH2YZ UT WOS:000372654800004 PM 26833573 ER PT J AU Smith, BD AF Smith, Bruce D. TI Neo-Darwinism, niche construction theory, and the initial domestication of plants and animals SO EVOLUTIONARY ECOLOGY LA English DT Article DE Domestication; Origins of agriculture; Niche construction theory; Standard evolutionary theory; Neo-Darwinism ID EASTERN NORTH-AMERICA; EVOLUTIONARY-THEORY NEED; FOOD-PRODUCTION; AGRICULTURAL ORIGINS; ARCHAEOLOGY; BIOLOGY; FORESTS; RETHINK; COMPLEX AB The initial domestication of plants and animals and the subsequent emergence of agricultural economies, which began independently more than 10,000 years ago in a number of different world regions, represent a major evolutionary transition in earth history. It is these domesticates, and the agricultural economies based on them, that have formed the lever with which humans have substantially modified the earth's terrestrial ecosystems over the past ten millennia. General explanations for this transition from hunting and gathering to food production economies formulated over the past 40 years have been based on standard evolutionary theory (SET) and employ the assumption of unidirectional adaptation-that environments change and species adapt. Here I compare these proposed SET-based externalist explanations for domestication with a recently formulated alternative developed from niche construction theory (NCT). Archaeological and paleoenvironmental records from two independent centers of domestication in the Americas-eastern North America and the Neotropics of northern South America, are found to support the NCT-based explanatory approach but not the SET explanations, underscoring the limitations of externalist SET approaches and the need for broader conceptualization of the processes that direct evolutionary change in order to gain a better general understanding of initial domestication as well as other major evolutionary transitions. C1 [Smith, Bruce D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, 10th & Constitut, Washington, DC 20560 USA. [Smith, Bruce D.] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. RP Smith, BD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, 10th & Constitut, Washington, DC 20560 USA.; Smith, BD (reprint author), Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. EM smithb@si.edu NR 57 TC 3 Z9 3 U1 14 U2 34 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 APR PY 2016 VL 30 IS 2 SI SI BP 307 EP 324 DI 10.1007/s10682-015-9797-0 PG 18 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA DH4KA UT WOS:000372753400008 ER PT J AU Zeder, MA AF Zeder, Melinda A. TI Domestication as a model system for niche construction theory SO EVOLUTIONARY ECOLOGY LA English DT Article DE Domestication; Niche Construction Theory; Co-evolution; Ecological Inheritance; Cooperation; Extended Evolutionary Synthesis ID HUMAN BEHAVIORAL ECOLOGY; FOOD-PRODUCTION; AGRICULTURAL ORIGINS; ANIMAL DOMESTICATION; SOUTHWEST ASIA; EVOLUTIONARY CONSEQUENCES; DEVELOPMENTAL PLASTICITY; PUNCTUATED EQUILIBRIUM; PLANT CULTIVATION; NEAR-EAST AB Niche Construction Theory (NCT) provides a powerful conceptual framework for understanding how and why humans and target species entered into domesticatory relationships that have transformed Earth's biota, landforms, and atmosphere, and shaped the trajectory of human cultural development. NCT provides fresh perspective on how niche-constructing behaviors of humans and plants and animals promote co-evolutionary interactions that alter selection pressures and foster genetic responses in domesticates. It illuminates the role of niche-altering activities in bequeathing an ecological inheritance that perpetuates the co-evolutionary relationships leading to domestication, especially as it pertains to traditional ecological knowledge and the transmission of learned behaviors aimed at enhancing returns from local environments. NCT also provides insights into the contexts and mechanisms that promote cooperative interactions in both humans and target species needed to sustain niche-constructing activities, ensuring that these activities produce an ecological inheritance in which domesticates play an increasing role. A NCT perspective contributes to on-going debates in the social sciences over explanatory frameworks for domestication, in particular as they pertain to issues of reciprocal causation, co-evolution, and the role of human intentionality. Reciprocally, domestication provides a model system for evaluating on-going debates in evolutionary biology concerning the impact of niche construction, phenotypic plasticity, extra-genetic inheritance, and developmental bias in shaping the direction and tempo of evolutionary change. C1 [Zeder, Melinda A.] Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Dept Anthropol, 10th & Constitut NW, Washington, DC 20013 USA. [Zeder, Melinda A.] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. RP Zeder, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Dept Anthropol, 10th & Constitut NW, Washington, DC 20013 USA.; Zeder, MA (reprint author), Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. EM zederm@si.edu NR 165 TC 5 Z9 5 U1 37 U2 55 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 APR PY 2016 VL 30 IS 2 SI SI BP 325 EP 348 DI 10.1007/s10682-015-9801-8 PG 24 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA DH4KA UT WOS:000372753400009 ER PT J AU Chapman, CA DeLuycker, A Reyna-Hurtado, RA Serio-Silva, JC Smith, TB Strier, KB Goldberg, TL AF Chapman, Colin A. DeLuycker, Anneke Reyna-Hurtado, Rafael A. Serio-Silva, Juan Carlos Smith, Thomas B. Strier, Karen B. Goldberg, Tony L. TI Safeguarding biodiversity: what is perceived as working, according to the conservation community? SO ORYX LA English DT Article DE Biodiversity loss; conservation approach; development; evaluation of success ID PROTECTED AREAS; ECOSYSTEMS; LOCATION; COLLAPSE; SUCCESS; FORESTS; CLIMATE; AFRICA AB Dramatic increases in human populations and per capita consumption, climate change, overexploitation of marine and freshwater resources, and deforestation have caused a litany of negative consequences for biodiversity. Such doom-and-gloom scenarios are widely known, frequently cited and frankly depressing. Although accurate assessments of threats have clear value for intervention planning, we believe there is also a need to reflect on successes. Such reflection provides balance to negative scenarios and may shift attention towards constructive, positive action. Here we use a systematic evaluation of.. success stories provided by conservation scientists and practitioners to explore the characteristics of the projects perceived as being associated with success. Success was deemed to have occurred for 19.4% of the projects simply because an event had occurred (e.g. a law was passed) and for 36.1% of projects quantitative data indicated success (e.g. censuses demonstrated population increase). However, for most projects (63.9%) there was no evaluation and success was defined by the subjective opinion of the respondent. Conservation community members viewed successful projects most often as those being long-term (88%), small in spatial scale (52%), with a relatively low budget (68%), and involving a protectionist approach alone or in combination with another approach. These results highlight the subjectivity of definitions of success in conservation but also the characteristics of conservation efforts that the conservation community perceives as indicative of success. C1 [Chapman, Colin A.] McGill Univ, Sch Environm, Montreal, PQ, Canada. [Chapman, Colin A.] McGill Univ, Dept Anthropol, Montreal, PQ, Canada. [Chapman, Colin A.] Wildlife Conservat Soc, Bronx, NY USA. [DeLuycker, Anneke] Smithsonian Conservat Biol Inst, Smithsonian Mason Sch Conservat, Front Royal, VA USA. [Reyna-Hurtado, Rafael A.] El Colegio Frontera Sur, Campeche, Mexico. [Serio-Silva, Juan Carlos] Inst Ecol AC, Red Biol & Conservac Vertebrados, Xalapa, Veracruz, Mexico. [Smith, Thomas B.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA. [Smith, Thomas B.] Univ Calif Los Angeles, Ctr Trop Res, Inst Environm & Sustainabil, Los Angeles, CA USA. [Strier, Karen B.] Univ Wisconsin, Dept Anthropol, Madison, WI 53706 USA. [Goldberg, Tony L.] Univ Wisconsin, Dept Pathobiol Sci, Madison, WI 53706 USA. RP Chapman, CA (reprint author), McGill Univ, Sch Environm, Montreal, PQ, Canada.; Chapman, CA (reprint author), McGill Univ, Dept Anthropol, Montreal, PQ, Canada.; Chapman, CA (reprint author), Wildlife Conservat Soc, Bronx, NY USA. EM colin.chapman@mcgill.ca FU Canada Research Chairs Program; Natural Science and Engineering Research Council of Canada; Infectious Disease Programme; UK Economic and Social Research Council FX Funding for the research was provided by the Canada Research Chairs Program, Natural Science and Engineering Research Council of Canada, Infectious Disease Programme, and the UK Economic and Social Research Council. We thank John Oates, Tom Struhsaker, Valerie Schoof and Tyler Bonnell for helpful comments. We would like to give special thanks to all the people who contributed their stories to our project. NR 36 TC 1 Z9 1 U1 8 U2 26 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0030-6053 EI 1365-3008 J9 ORYX JI Oryx PD APR PY 2016 VL 50 IS 2 BP 302 EP 307 DI 10.1017/S0030605314000738 PG 6 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA DH1DZ UT WOS:000372525900024 ER PT J AU Marvin, DC Asner, GP Schnitzer, SA AF Marvin, David C. Asner, Gregory P. Schnitzer, Stefan A. TI Liana canopy cover mapped throughout a tropical forest with high-fidelity imaging spectroscopy SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Carnegie Airborne Observatory; Hyperspectral imaging; Panama; Support vector machine ID BARRO-COLORADO ISLAND; REDUCE CARBON ACCUMULATION; TREE GROWTH; RAIN-FOREST; AMAZONIAN BOLIVIA; PANAMA; BIOMASS; LEAF; CLASSIFICATION; PATTERNS AB Increasing size and abundance of lianas relative to trees are pervasive changes in Neotropical forests that may lead to reduced forest carbon stocks. Yet the liana growth form is chronically understudied in large-scale tropical forest censuses, resulting in few data on the scale, cause, and impact of increasing lianas. Satellite and airborne remote sensing provide potential tools to map and monitor lianas at much larger spatial and rapid temporal scales than are possible with plot-based forest censuses. We combined high-resolution airborne imaging spectroscopy and a ground-based tree canopy census to investigate whether tree canopies supporting lianas could be discriminated from tree canopies with no liana coverage. Using support vector machine algorithms, we achieved accuracies of nearly 90% in discriminating the presence-absence of lianas, and low error (15.7% RMSE) when predicting liana percent canopy cover. When applied to the full image of the study site, our model had a 4.1% false-positive error rate as validated against an independent plot-level dataset of liana canopy cover. Using the derived liana cover classification map, we show that 6.1%-10.2% of the 1823 ha study site has high-to-severe (50-100%) liana canopy cover. Given that levels of liana infestation are increasing in Neotropical forests and can result in high tree mortality, the extent of high-to-severe liana canopy cover across the landscape may have broad implications for ecosystem function and forest carbon storage. The ability to accurately map landscape-scale liana infestation is crucial to quantifying their effects on forest function and uncovering the mechanisms underlying their increase. (C) 2015 Elsevier Inc. All rights reserved. C1 [Marvin, David C.; Asner, Gregory P.] Carnegie Inst Sci, Dept Global Ecol, 260 Panama St, Stanford, CA 94305 USA. [Marvin, David C.] Univ Michigan, Dept Ecol & Evolutionary Biol, 830 N Univ Ave, Ann Arbor, MI 48109 USA. [Schnitzer, Stefan A.] Marquette Univ, Dept Biol Sci, POB 1881, Milwaukee, WI 53201 USA. [Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama. RP Marvin, DC (reprint author), Carnegie Inst Sci, Dept Global Ecol, 260 Panama St, Stanford, CA 94305 USA. EM dmarvin@camegiescience.edu; gpa@carnegiescience.edu; S1@marquette.edu OI Marvin, David/0000-0002-2938-9027 FU John D. and Catherine T. MacArthur Foundation; NASA Earth and Space Science Fellowship Program; National Science Foundation [NSF-DEB 0613666, NSF-DEB 0845071, NSF-DEB 101943]; University of Michigan Department of Ecology and Evolutionary Biology; University of Michigan Rackham Graduate School; Grantham Foundation for the Protection of the Environment grant; Avatar Alliance Foundation; National Science Foundation (NSF Graduate Research Fellowship) FX We thank B. Fadrique, J. Malcomb, A. Quebbeman, S. Senkewitz, G. Williams, and M. Zapata for their assistance with field work and tree crown digitization. N. Vaughn, C. Anderson, R. Martin, D. Knapp, J.B. Feret, and P. Brodrick assisted with collection, processing, and analysis of remotely sensed data. R. Burnham, I. Ibanez, C. Dick, and K. Bergen gave helpful comments on the manuscript. Logistical support was provided by H. Muller-Landau, M. Solano, and the Smithsonian Tropical Research Institute. This study was supported by the John D. and Catherine T. MacArthur Foundation, the NASA Earth and Space Science Fellowship Program (to DCM), the National Science Foundation (NSF-DEB 0613666, NSF-DEB 0845071, and NSF-DEB 101943 to SAS, and a NSF Graduate Research Fellowship to DCM), the University of Michigan Department of Ecology and Evolutionary Biology (to DCM), and the University of Michigan Rackham Graduate School (to DCM). Airborne data collection was supported by a Grantham Foundation for the Protection of the Environment grant (to GPA). The Carnegie Airborne Observatory is supported by the John D. and Catherine T. MacArthur Foundation, Avatar Alliance Foundation, Mary Anne Nyburg Baker and G. Leonard Baker Jr., and William R. Hearst III. NR 65 TC 3 Z9 3 U1 6 U2 18 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD APR PY 2016 VL 176 BP 98 EP 106 DI 10.1016/j.rse.2015.12.028 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA DG9DO UT WOS:000372383200008 ER PT J AU Kirk, MF Altman, SJ Santillan, EFU Bennett, PC AF Kirk, Matthew F. Altman, Susan J. Santillan, Eugenio-Felipe U. Bennett, Philip C. TI Interplay between microorganisms and geochemistry in geological carbon storage SO INTERNATIONAL JOURNAL OF GREENHOUSE GAS CONTROL LA English DT Article DE Carbon trapping; Porous media; Subsurface microbiology; Bioenergetics; Capnophile; Bioreactor experiments ID HIGH-PRESSURE; GEOBACILLUS-STEAROTHERMOPHILUS; MICROBIAL DIVERSITY; SUPERCRITICAL CO2; CALCIUM-CARBONATE; SALINE AQUIFERS; DEEP SUBSURFACE; WATER-QUALITY; DIOXIDE; INACTIVATION AB Researchers at the Center for Frontiers of Subsurface Energy Security (CFSES) have conducted laboratory and modeling studies to better understand the interplay between microorganisms and geochemistry for geological carbon storage (GCS). We provide evidence of microorganisms adapting to high pressure CO2 conditions and identify factors that may influence survival of cells to CO2 stress. Factors that influenced the ability of cells to survive exposure to high-pressure CO2 in our experiments include mineralogy, the permeability of cell walls and/or membranes, intracellular buffering capacity, and whether cells live planktonically or within biofilm. Column experiments show that, following exposure to acidic water, biomass can remain intact in porous media and continue to alter hydraulic conductivity. Our research also shows that geochemical changes triggered by CO2 injection can alter energy available to populations of subsurface anaerobes and that microbial feedbacks on this effect can influence carbon storage. Our research documents the impact of CO2 on microorganisms and in turn, how subsurface microorganisms can influence GCS. We conclude that microbial presence and activities can have important implications for carbon storage and that microorganisms should not be overlooked in further GCS research. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Kirk, Matthew F.] Kansas State Univ, Dept Geol, Manhattan, KS 66506 USA. [Altman, Susan J.] Sandia Natl Labs, Dept Geochem, Albuquerque, NM 87185 USA. [Santillan, Eugenio-Felipe U.; Bennett, Philip C.] Univ Texas Austin, Dept Geol Sci, Jackson Sch Geosci, Austin, TX USA. [Santillan, Eugenio-Felipe U.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RP Altman, SJ (reprint author), Sandia Natl Labs, POB 5800 MS0754, Albuquerque, NM 87185 USA. EM sjaltma@sandia.gov FU Center for Frontiers of Subsurface Energy Security, an Energy Frontier Research Center - U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-SC0001114]; U.S. Department of Energy's National Nuclear Security Administration [DE-AC04-94AL85000] FX This material is based upon work supported as part of the Center for Frontiers of Subsurface Energy Security, an Energy Frontier Research Center funded by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences under Award Number DE-SC0001114. Sandia National Laboratories is a multi-program laboratory managed and operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Corporation, for the U.S. Department of Energy's National Nuclear Security Administration under contract DE-AC04-94AL85000. Matthew Kirk conducted the laboratory and modeling work presented in this paper while at Sandia National Laboratories. NR 83 TC 1 Z9 1 U1 6 U2 13 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1750-5836 EI 1878-0148 J9 INT J GREENH GAS CON JI Int. J. Greenh. Gas Control PD APR PY 2016 VL 47 BP 386 EP 395 DI 10.1016/j.ijggc.2016.01.041 PG 10 WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Energy & Fuels; Engineering, Environmental SC Science & Technology - Other Topics; Energy & Fuels; Engineering GA DG3SB UT WOS:000371989100034 ER PT J AU Lohan, KMP Fleischer, RC Carney, KJ Holzer, KK Ruiz, GM AF Lohan, K. M. Pagenkopp Fleischer, R. C. Carney, K. J. Holzer, K. K. Ruiz, G. M. TI Amplicon-Based Pyrosequencing Reveals High Diversity of Protistan Parasites in Ships' Ballast Water: Implications for Biogeography and Infectious Diseases SO MICROBIAL ECOLOGY LA English DT Article DE Chesapeake Bay; Non-indigenous; Non-native; Parasite; Protist; Metabarcode; Harbor ID RIBOSOMAL-RNA SEQUENCES; MARINE; COMMUNITIES; TRANSPORT; TAXONOMY; ECOSYSTEMS; ECOLOGY; LABYRINTHULOMYCOTA; CLASSIFICATION; MICROORGANISMS AB Ships' ballast water (BW) commonly moves macroorganisms and microorganisms across the world's oceans and along coasts; however, the majority of these microbial transfers have gone undetected. We applied high-throughput sequencing methods to identify microbial eukaryotes, specifically emphasizing the protistan parasites, in ships' BW collected from vessels calling to the Chesapeake Bay (Virginia and Maryland, USA) from European and Eastern Canadian ports. We utilized tagged-amplicon 454 pyrosequencing with two general primer sets, amplifying either the V4 or V9 domain of the small subunit (SSU) of the ribosomal RNA (rRNA) gene complex, from total DNA extracted from water samples collected from the ballast tanks of bulk cargo vessels. We detected a diverse group of protistan taxa, with some known to contain important parasites in marine systems, including Apicomplexa (unidentified apicomplexans, unidentified gregarines, Cryptosporidium spp.), Dinophyta (Blastodinium spp., Euduboscquella sp., unidentified syndinids, Karlodinium spp., Syndinium spp.), Perkinsea (Parvilucifera sp.), Opisthokonta (Ichthyosporea sp., Pseudoperkinsidae, unidentified ichthyosporeans), and Stramenopiles (Labyrinthulomycetes). Further characterization of groups with parasitic taxa, consisting of phylogenetic analyses for four taxa (Cryptosporidium spp., Parvilucifera spp., Labyrinthulomycetes, and Ichthyosporea), revealed that sequences were obtained from both known and novel lineages. This study demonstrates that high-throughput sequencing is a viable and sensitive method for detecting parasitic protists when present and transported in the ballast water of ships. These data also underscore the potential importance of human-aided dispersal in the biogeography of these microbes and emerging diseases in the world's oceans. C1 [Lohan, K. M. Pagenkopp; Fleischer, R. C.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Lohan, K. M. Pagenkopp; Carney, K. J.; Holzer, K. K.; Ruiz, G. M.] Smithsonian Environm Res Ctr, Marine Invas Lab, POB 28, Edgewater, MD 21037 USA. RP Lohan, KMP (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA.; Lohan, KMP (reprint author), Smithsonian Environm Res Ctr, Marine Invas Lab, POB 28, Edgewater, MD 21037 USA. EM lohank@si.edu OI Ruiz, Gregory/0000-0003-2499-441X; Lohan, Katrina/0000-0003-3885-7985; Holzer, Kimberly/0000-0002-3582-0880 FU Center for Conservation and Evolutionary Genetics and a Smithsonian Institution Next Generation Sequencing Small Grant; US Coast Guard; Smithsonian MarineGEO Postdoctoral Fellowship FX The crews of the various cargo ships, the facilities within the Ports of Baltimore and Hampton Roads, and agents T. Parker Host and Capes Shipping Agencies enabled vessel and tank access. Rebecca Dikow assisted with interpreting some phylogenetic analyses and access to computers. Rebecca Dikow, Carly Woltz, and three anonymous reviewers provided useful feedback on the content of this manuscript. Taylor and Joel Callicrate assisted with file formatting. Nancy Rotzel McInerney provided logistical support at CCEG. We thank Roche-454 for providing a GS Junior to CCEG, and assistance with protocols. This project was funded by the Center for Conservation and Evolutionary Genetics and a Smithsonian Institution Next Generation Sequencing Small Grant. Sample collection was supported by funding from the US Coast Guard. Pagenkopp Lohan was funded by a Smithsonian MarineGEO Postdoctoral Fellowship. NR 67 TC 1 Z9 1 U1 10 U2 24 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0095-3628 EI 1432-184X J9 MICROB ECOL JI Microb. Ecol. PD APR PY 2016 VL 71 IS 3 BP 530 EP 542 DI 10.1007/s00248-015-0684-6 PG 13 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA DG7LO UT WOS:000372266000003 ER PT J AU Richardson, ML Keathley, CP Peterson, CL AF Richardson, Matthew L. Keathley, Craig P. Peterson, Cheryl L. TI Breeding system of the critically endangered Lakela's Mint and influence of plant height on pollinators and seed output SO POPULATION ECOLOGY LA English DT Article DE Agamospermy; Apis mellifera; Bombus impatiens; Cross-pollination; Dicerandra immaculata; Self-pollination ID INTRODUCED HONEY-BEES; FLORAL DISPLAY SIZE; POLLEN-LIMITATION; FLOWERING PLANTS; MATING SYSTEMS; FLORIDA SCRUB; FRUIT-SET; REPRODUCTION; LIMITS; PATTERNS AB Understanding reproductive systems of rare plants is critical for conservation efforts. Lakela's Mint, Dicerandra immaculata Lakela var. immaculata, is an endangered plant endemic to an approximately 4.8-km long area in Florida, USA. We used an experimental garden and three populations of Lakela's Mint to determine: (1) what is the breeding system (autonomous, asexual, self-fertile, cross-fertile) and are insects necessary for reproduction; (2) which native and nonnative insect species visit flowers and is the frequency of visits to a plant influenced by its height; (3) does the number of flowers visited within a plant by individual insects differ among native and nonnative insect species and due to plant height; and (4) is seed output influenced by plant height? Our results indicate that the breeding system of Lakela's Mint was facultative outcrossing. Insect-pollinated flowers produced more seeds than flowers that reproduced autonomously or asexually. The honey bee Apis mellifera L., a nonnative species, was the most frequent visitor to plants and visited more flowers within plants than native pollinators, but its behavior was not influenced by plant height. Native pollinators such as Bombus impatiens Cresson were attracted more frequently to shorter plants, but visited fewer flowers than on taller plants. Despite having fewer total and pollinated flowers, shorter plants had a higher output of intact seeds than taller plants, which could be due to differences in efficiency between native and nonnative pollinators or other factors. Our results add insight into factors influencing seed output and interactions between pollinators and rare plants. C1 [Richardson, Matthew L.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Sustainabil, Washington, DC 20560 USA. [Keathley, Craig P.] EI Pont Nemours & Co, Stine Haskell Res Ctr, Newark, DE 19711 USA. [Peterson, Cheryl L.] Rare Plant Conservat Program, Bok Tower Gardens,1151 Tower Blvd, Lake Wales, FL 33853 USA. RP Peterson, CL (reprint author), Rare Plant Conservat Program, Bok Tower Gardens,1151 Tower Blvd, Lake Wales, FL 33853 USA. EM cpeterson@boktower.org FU state of Florida Department of Agriculture and Consumer Services Division of Plant Industry [20160, 21009] FX We thank M. Watson, M. Bell, R. Bell, G. Bupp, and J. Thompson for assistance in the field, Harbor Branch Oceanographic Institute and St. Lucie and Indian River County land managers for site access, and three anonymous reviewers for their constructive comments. This research was funded in part by grants from the state of Florida Department of Agriculture and Consumer Services Division of Plant Industry (contracts #20160 and #21009) to Bok Tower Gardens. Research was conducted under Harvesting Permits #1086, 1141, 1157, and 1184 from the State of Florida Department of Agriculture and Consumer Services Division of Plant Industry. NR 50 TC 1 Z9 1 U1 8 U2 21 PU SPRINGER JAPAN KK PI TOKYO PA CHIYODA FIRST BLDG EAST, 3-8-1 NISHI-KANDA, CHIYODA-KU, TOKYO, 101-0065, JAPAN SN 1438-3896 EI 1438-390X J9 POPUL ECOL JI Popul. Ecol. PD APR PY 2016 VL 58 IS 2 BP 277 EP 284 DI 10.1007/s10144-015-0531-0 PG 8 WC Ecology SC Environmental Sciences & Ecology GA DG6CF UT WOS:000372169100005 ER PT J AU Barclay, RS Wing, SL AF Barclay, Richard S. Wing, Scott L. TI Improving the Ginkgo CO2 barometer: Implications for the early Cenozoic atmosphere SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE stomatal index; Ginkgo biloba; improved response curve; total diffusivity; carbon dioxide; greenhouse climate ID STOMATAL FREQUENCY-RESPONSE; LIVING FOSSIL GINKGO; PAST 2 CENTURIES; CARBON-DIOXIDE; LEAVES; INCREASE; RECORD; CLIMATE; PLEISTOCENE; BOUNDARY AB Stomatal properties of fossil Ginkgo have been used widely to infer the atmospheric concentration of CO2 in the geological past (paleo-pCO(2)). Many of these estimates of paleo-pCO2 have relied on the inverse correlation between pCO(2) and stomatal index (SI the proportion of epidermal cells that are stomata) observed in recent Ginkgo biloba, and therefore depend on the accuracy of this relationship. The SI-pCO(2) relationship in G. biloba has not been well documented, however. Here we present new measurements of SI for leaves of G. biloba that grew under pCO(2) from 290 to 430 ppm. We prepared and imaged all specimens using a consistent procedure and photo-documented each count. As in prior studies, we found a significant inverse relationship between SI and pCO(2), however, the relationship is more linear, has a shallower slope, and a lower correlation coefficient than previously reported. We examined leaves of G. biloba grown under pCO(2) of 1500 ppm, but found they had highly variable SI and a large proportion of malformed stomata. We also measured stomatal dimensions, stomatal density, and the carbon isotope composition of G. biloba leaves in order to test a mechanistic model for inferring pCO(2). This model overestimated observed pCO(2), performing less well than the SI method between 290 and 430 ppm. We used our revised SI-pCO(2) response curve, and new observations of selected fossils, to estimate late Cretaceous and Cenozoic pCO(2) from fossil Ginkgo adiantoides. All but one of the new estimates is below 800 ppm, and together they show little long-term change in pCO(2) or relation to global temperature. The low Paleogene pCO(2) levels indicated by the Ginkgo SI proxy are not consistent with the high pCO(2) inferred by some climate and carbon cycle models. We cannot currently resolve the discrepancy, but greater agreement between proxy data and models may come from a better understanding of the stomatal response of G. biloba to elevated pCO(2), better counts and measurements of fossil Ginkgo, or models that can simulate greenhouse climates at lower pCO(2). (C) 2016 Elsevier B.V. All rights reserved. C1 [Barclay, Richard S.; Wing, Scott L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, 10th & Constitut, Washington, DC 20560 USA. RP Barclay, RS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, 10th & Constitut, Washington, DC 20560 USA. EM barclay.rich@gmail.com FU Peter Buck Postdoctoral Fellowship at the Smithsonian's National Museum of Natural History in Washington FX Robert Webster and Joe Kirkbride provided access and permission to sample herbarium specimens at the National Arboretum Herbarium (NA). Rusty Russell provided permission and Deborah Bell provided access to sample in the National Museum of Natural History Herbarium (US - Smithsonian Institution). Shusheng Hu facilitated the specimen loan from the Yale Peabody Museum. Emily Martin helped sample living trees in the "Ginkgo Grove" at the Blandy Experimental Farm near Boyce, VA. Access and sampling permission at Blandy were provided by Kyle Haynes, Research Assistant Professor in the Department of Environmental Sciences at the University of Virginia. We thank Jennifer McElwain of University College Dublin for providing Ginkgo biloba leaves from the experiment of Haworth et al. (2013). NMNH volunteer Sal Bosco prepared and mounted most of the Ginkgo specimens. We thank Odile Madden from the Museum Conservation Institute (Smithsonian Institution) for suggesting imaging Ginkgo specimens with an environmental SEM. Volunteer Pam Hamilton spent hundreds of hours taking SEM images at NMNH and also helped test the stomatal measurement approaches; without her efforts this project would not have been completed. Intern Rebecca Blader (Paleobiology) helped initiate the SEM imaging project. Scott Whittaker and Caitlin Baker provided training in the operation of the Zeiss environmental SEM at the National Museum of Natural History. International summer interns Nicolas Perez (Colombia) and Rolf Svenning (Denmark) in the Paleobiology Department at NMNH were pivotal in preparing samples for carbon isotope measurement at the Isotope Ratio Mass Spectrometry lab of the Museum Conservation Institute, under the direction of Christine France. Funding for RSB comes from a Peter Buck Postdoctoral Fellowship at the Smithsonian's National Museum of Natural History in Washington, NR 58 TC 2 Z9 2 U1 4 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD APR 1 PY 2016 VL 439 BP 158 EP 171 DI 10.1016/j.epsl.2016.01.012 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DG1QX UT WOS:000371843700016 ER PT J AU Bernatsky, S Smargiassi, A Barnabe, C Svenson, LW Brand, A Martin, RV Hudson, M Clarke, AE Fortin, PR van Donkelaar, A Edworthy, S Belisle, P Joseph, L AF Bernatsky, Sasha Smargiassi, Audrey Barnabe, Cheryl Svenson, Lawrence W. Brand, Allan Martin, Randall V. Hudson, Marie Clarke, Ann E. Fortin, Paul R. van Donkelaar, Aaron Edworthy, Steven Belisle, Patrick Joseph, Lawrence TI Fine particulate air pollution and systemic autoimmune rheumatic disease in two Canadian provinces SO ENVIRONMENTAL RESEARCH LA English DT Article DE Systemic lupus erythematosus (SLE); Autoimmune diseases; Environmental factors ID LUPUS-ERYTHEMATOSUS; DNA-DAMAGE; EXPOSURE; MATTER; RISK; POPULATION; PARTICLES; ARTHRITIS; ASSOCIATIONS; PREVALENCE AB Objective: To estimate the degree to which fine particulate (PM2.5) air pollution is associated with systemic autoimmune rheumatic diseases (SARDs). Methods: We used population-based administrative data from Alberta (1993-2007) and Quebec (19892011). SARD algorithms included >= 2 physician billing codes, or >= 1 rheumatology billing code, or 1 hospitalization diagnostic code (for systemic lupus, Sjogren's Syndrome, scleroderma, polymyositis, dermatomyositis, or undifferentiated connective tissue disease). Bayesian hierarchical latent class regression models estimated the probability that any given resident was a SARD case, based on the algorithms. Mean 2001-2006 residential ambient PM2.5 levels were assigned using satellite-derived data for dissemination area regions in Alberta and CLSC regions in Quebec. The sum of individual level probabilities provided the estimated total cases per region in each province, according to age, sex, urban-versus-rural residence, income, and PM2.5 levels. In Alberta, we ran separate models for First-Nations (FN) and non-First Nations subgroups. Bayesian logistic regression modeling generated odds ratio (OR) estimates for being a SARD case, accounting concurrently for demographics, as well as an interaction term between age and sex. Results: Our data suggested that the probability of being a SARD case was higher among females versus males and for residents aged >45 versus younger, with the highest ORs for older females. Independently, the odds of being a SARDs case increased with PM2.5 levels in both provinces. Conclusion: Our data suggest that PM2.5 exposure may be associated with an increased risk of SARDs. (C) 2015 Elsevier Inc. All rights reserved. C1 [Bernatsky, Sasha; Clarke, Ann E.; Joseph, Lawrence] McGill Univ, Dept Epidemiol Biostat & Occupat Hlth, Purvis Hall 1020 Pine Ave West, Montreal, PQ H3A 1A2, Canada. [Bernatsky, Sasha; Belisle, Patrick; Joseph, Lawrence] McGill Univ, Royal Victoria Hosp, Ctr Hlth, Div Clin Epidemiol, V Pavil 687,Pine Ave West, Montreal, PQ H3A 1A1, Canada. [Smargiassi, Audrey; Brand, Allan] Univ Montreal, Ecole Sante Publ, Dept Sante Environm & Sante Travail, Pavillon Marguerite dYouville,CP 6128, Montreal, PQ, Canada. [Smargiassi, Audrey] Inst Natl Sante Publ Quebec, 190 Cremazie Blvd E, Montreal, PQ H2P 1E2, Canada. [Barnabe, Cheryl; Edworthy, Steven] Univ Calgary, Dept Med, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada. [Barnabe, Cheryl; Svenson, Lawrence W.; Edworthy, Steven] Univ Calgary, Dept Community Hlth Sci, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada. [Martin, Randall V.; van Donkelaar, Aaron] Dalhousie Univ, Dept Phys & Atmospher Sci, 6310 Coburg Rd POB 15000, Halifax, NS B3H 4R2, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Hudson, Marie] McGill Univ, Dept Med, 1001 Decarie Blvd,Mail Drop D05-2214, Montreal, PQ H4A 3J1, Canada. [Hudson, Marie] McGill Univ, Jewish Gen Hosp, Div Rheumatol, 3755 Cote Ste Catherine Rd, Montreal, PQ H3T 1E2, Canada. [Clarke, Ann E.] McGill Univ, Ctr Hlth, Div Allergy & Clin Immunol, 1547 Ave Pins, Montreal, PQ H3G 1B3, Canada. [Fortin, Paul R.] Univ Laval, Div Rheumatol, Dept Med, Bur 4633, Pavilion Ferdinand Vandry 1050,Ave Med, Quebec City, PQ G1V 0A6, Canada. [Svenson, Lawrence W.] Alberta Minist Hlth, Surveillance & Assessment Branch, 10025 Jasper Ave, Edmonton, AB T5J 1S6, Canada. [Svenson, Lawrence W.] Univ Alberta, Canada Sch Publ Hlth, 11405 87 Ave NW, Edmonton, AB T6G 1C9, Canada. [Svenson, Lawrence W.] Univ Calgary, Canada Dept Community Hlth Sci, 2500 Hosp Dr NW, Calgary, AB T2N 1N4, Canada. RP Bernatsky, S (reprint author), McGill Univ, Ctr Hlth, Div Clin Epidemiol, 687 Pine Ave West, Bldg V2-09, Montreal, PQ H3A 1A1, Canada. EM sasha.bernatsky@mcgill.ca RI Martin, Randall/C-1205-2014 OI Martin, Randall/0000-0003-2632-8402 FU Canadian Institutes of Health Research [CAP-120355] FX This study was funded by the Canadian Institutes of Health Research, CAP-120355. NR 42 TC 4 Z9 4 U1 4 U2 13 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0013-9351 EI 1096-0953 J9 ENVIRON RES JI Environ. Res. PD APR PY 2016 VL 146 BP 85 EP 91 DI 10.1016/j.envres.2015.12.021 PG 7 WC Environmental Sciences; Public, Environmental & Occupational Health SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health GA DF2TE UT WOS:000371196000011 PM 26724462 ER PT J AU Weichenthal, S Crouse, DL Pinault, L Godri-Pollitt, K Lavigne, E Evans, G van Donkelaar, A Martin, RV Burnett, RT AF Weichenthal, Scott Crouse, Daniel L. Pinault, Lauren Godri-Pollitt, Krystal Lavigne, Eric Evans, Greg van Donkelaar, Aaron Martin, Randall V. Burnett, Rick T. TI Oxidative burden of fine particulate air pollution and risk of cause-specific mortality in the Canadian Census Health and Environment Cohort (CanCHEC) SO ENVIRONMENTAL RESEARCH LA English DT Article DE PM2.5; Oxidative potential; Mortality; Lung cancer ID LONG-TERM EXPOSURE; LINING FLUID ANTIOXIDANTS; CARDIOVASCULAR MORTALITY; SPATIAL VARIATION; LUNG-CANCER; MATTER; STRESS; GLUTATHIONE; DISEASE; GENERATION AB Backround: Fine particulate air pollution (PM2.5) is known to contribute to cardiorespiratory mortality but it is not clear how PM2.5 oxidative burden (i.e. the ability of PM2.5 to cause oxidative stress) may influence long-term mortality risk. Methods: We examined the relationship between PM2.5 oxidative burden and cause-specific mortality in Ontario, Canada. Integrated PM2.5 samples were collected from 30 provincial monitoring sites between 2012 and 2013. The oxidative potential (% depletion/mu g) of regional PM2.5 was measured as the ability of filter extracts to deplete antioxidants (glutathione and ascorbate) in a synthetic respiratory tract lining fluid. PM2.5 oxidative burden was calculated as the product of PM2.5 mass concentrations and regional estimates of oxidative potential. In total, this study included 193,300 people who completed the Canadian long-form census in 1991 and who lived within 5 km of a site where oxidative potential was measured. Deaths occurring between 1991 and 2009 were identified through record linkages and Cox proportional hazard models were used to estimate hazard ratios (and 95% confidence intervals) for interquartile changes in exposure adjusting for individual-level covariates and indirect-adjustment for smoking and obesity. Results: Glutathione-related oxidative burden was associated with cause-specific mortality. For lung cancer specifically, this metric was associated with a 12% (95% CI: 5.0-19) increased risk of mortality whereas a 5.0% (95% CI: 0.1, 10) increase was observed for PM2.5. Indirect adjustment for smoking and obesity decreased the lung cancer hazard ratio for glutathione-related oxidative burden but it remained significantly elevated (HR=1.07, 95% CI: 1.005, 1.146). Ascorbate-related oxidative burden was not associated with mortality. Conclusions: Our findings suggest that glutathione-related oxidative burden may be more strongly associated with lung cancer mortality than PM2.5 mass concentrations. Crown Copyright (C) 2015 Published by Elsevier Inc. C1 [Weichenthal, Scott; Lavigne, Eric; Burnett, Rick T.] Hlth Canada, Ottawa, ON K1A 0K9, Canada. [Crouse, Daniel L.] Univ New Brunswick, Fredericton, NB, Canada. [Godri-Pollitt, Krystal] Univ Massachusetts, Amherst, MA 01003 USA. [Evans, Greg] Univ Toronto, Toronto, ON, Canada. [van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Halifax, NS, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Pinault, Lauren] STAT Canada, Ottawa, ON, Canada. RP Weichenthal, S (reprint author), Hlth Canada, Air Hlth Sci Div, 269 Laurier Ave West, Ottawa, ON K1A 0K9, Canada. EM scott.weichenthal@hc-sc.gc.ca RI Lavigne, Eric/E-2948-2013; Martin, Randall/C-1205-2014; OI Lavigne, Eric/0000-0001-6146-9839; Martin, Randall/0000-0003-2632-8402; Evans, Greg/0000-0002-9641-4499 FU Health Canada FX We would like to thank Farhan Mansoor for conducting the oxidative burden analysis and Christie McMann, Tim Shin, and Hongyu You for their help in compiling oxidative burden data. We would also like to thank Luc White (Environment Canada) and the Ontario. Ministry of the Environment and Climate Change for their help in collecting PM2.5 filters for oxidative burden analyses. This work was funded by Health Canada. NR 53 TC 1 Z9 1 U1 6 U2 28 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0013-9351 EI 1096-0953 J9 ENVIRON RES JI Environ. Res. PD APR PY 2016 VL 146 BP 92 EP 99 DI 10.1016/j.envres.2015.12.013 PG 8 WC Environmental Sciences; Public, Environmental & Occupational Health SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health GA DF2TE UT WOS:000371196000012 PM 26745732 ER PT J AU Rushing, CS Ryder, TB Scarpignato, AL Saracco, JF Marra, PP AF Rushing, Clark S. Ryder, Thomas B. Scarpignato, Amy L. Saracco, James F. Marra, Peter P. TI Using demographic attributes from long-term monitoring data to delineate natural population structure SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE Andrewartha & Birch; Breeding Bird Survey; conservation planning; demography; hierarchical clustering; local population; monitoring; natural population; population dynamics ID BREEDING BIRD SURVEY; CONSERVATION BIOLOGY; DYNAMICS; PRODUCTIVITY; EXTINCTION; ECOLOGY AB The concept of natural' populations is a foundation of modern ecology and conservation, with a large body of theoretical literature using these discrete demographic units to understand population dynamics and prioritize conservation strategies. To date, there are currently no objective methods for empirically delineating large-scale population boundaries using demographic data. We present a novel approach for using large-scale, citizen-science monitoring data to quantify geographic structure in trend and abundance and identify distinct natural populations. We demonstrate this approach by delineating populations of eight passerine species using data collected as part of the North American Breeding Bird Survey. Our approach was able to identify geographic structure in both trend and abundance and to delineate distinct populations for all eight species. An independent validation of three species indicated this demographic variation was reflected in underlying vital rates.Synthesis and applications. Natural populations are biologically based alternatives to the traditional geographically defined units that can improve the ability of researchers and managers to quantify spatial variation in population dynamics. Our analysis of natural population structure in breeding songbirds demonstrates that species can show substantial geographic variation in population attributes and underlying demography. We recommend managers define spatial units using natural populations when setting regional population objectives for both single and multispecies conservation plans. Natural populations are biologically based alternatives to the traditional geographically defined units that can improve the ability of researchers and managers to quantify spatial variation in population dynamics. Our analysis of natural population structure in breeding songbirds demonstrates that species can show substantial geographic variation in population attributes and underlying demography. We recommend managers define spatial units using natural populations when setting regional population objectives for both single and multispecies conservation plans. C1 [Rushing, Clark S.; Ryder, Thomas B.; Scarpignato, Amy L.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Migratory Bird Ctr, MRC 5503 POB 37012, Washington, DC 20013 USA. [Saracco, James F.] Inst Bird Populat, POB 1346, Point Reyes Stn, CA 94956 USA. RP Rushing, CS (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Migratory Bird Ctr, MRC 5503 POB 37012, Washington, DC 20013 USA. EM rushingc@si.edu FU Smithsonian James Smithson Postdoctoral Fellowship; Strategic Environmental Research and Defense Program; U.S. Fish and Wildlife Service FX We thank S. Sillett, J. Hostetler, A-L. Harrison, T. Wilbert, G. Siriwardena and three anonymous reviewers for comments that strengthened earlier drafts of this paper. CSR was supported by a Smithsonian James Smithson Postdoctoral Fellowship. This work was made possible by the support from the Strategic Environmental Research and Defense Program and the U.S. Fish and Wildlife Service. NR 49 TC 1 Z9 1 U1 5 U2 13 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 2016 VL 53 IS 2 BP 491 EP 500 DI 10.1111/1365-2664.12579 PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA DE9LN UT WOS:000370959100021 ER PT J AU Carry, B Solano, E Eggl, S DeMeo, FE AF Carry, B. Solano, E. Eggl, S. DeMeo, F. E. TI Spectral properties of near-Earth and Mars-crossing asteroids using Sloan photometry SO ICARUS LA English DT Article DE Near-Earth objects; Asteroids, composition; Photometry ID DIGITAL-SKY-SURVEY; JOVIAN TROJAN ASTEROIDS; MOVING OBJECT CATALOG; SURFACE-COMPOSITION; MAIN-BELT; TAXONOMIC CLASSIFICATION; PHYSICAL-CHARACTERIZATION; ORBITAL DISTRIBUTION; SPECTROSCOPIC SURVEY; DYNAMICAL FAMILIES AB The nature and origin of the asteroids orbiting in near-Earth space, including those on a potentially hazardous trajectory, is of both scientific interest and practical importance. We aim here at determining the taxonomy of a large sample of near-Earth and Mars-crosser asteroids and analyze the distribution of these classes with orbit. We use this distribution to identify the source regions of near-Earth objects and to study the strength of planetary encounters to refresh asteroid surfaces. We measure the photometry of these asteroids over four filters at visible wavelengths on images taken by the Sloan Digital Sky Survey (SDSS). These colors are used to classify the asteroids into a taxonomy consistent with the widely used Bus-DeMeo taxonomy (DeMeo et al. [2009]. Icarus 202, 160-180) based on visible and near-infrared spectroscopy. We report here on the taxonomic classification of 206 near-Earth and 776 Mars-crosser asteroids determined from SDSS photometry, representing an increase of 40% and 663% of known taxonomy classifications in these populations. Using the source region mapper by Greenstreet et al. (Greenstreet, S., Ngo, H., Gladman, B. [2012]. Icarus, 217, 355-366), we compare for the first time the taxonomic distribution among near-Earth and main-belt asteroids of similar diameters. Both distributions agree at the few percent level for the inner part of the main belt and we confirm this region as a main source of near-Earth objects. The effect of planetary encounters on asteroid surfaces are also studied by developing a simple model of forces acting on a surface grain during planetary encounter, which provides the minimum distance at which a close approach should occur to trigger resurfacing events. By integrating numerically the orbit of the 519 S-type and 46 Q-type asteroids in our sample back in time for 500,000 years and monitoring their encounter distance with Venus, Earth, Mars, and Jupiter, we seek to understand the conditions for resurfacing events. The population of Q-type is found to present statistically more encounters with Venus and the Earth than S-types, although both S- and Q-types present the same amount of encounters with Mars. (C) 2016 Elsevier Inc. All rights reserved. C1 [Carry, B.; Eggl, S.] Univ Lille, Univ Paris 06, Univ Sorbonne, PSL Res Univ,IMCCE,Observ Paris,CNRS, Lille, France. [Carry, B.] ESA, European Space Astron Ctr, POB 78, Madrid 28691, Spain. [Solano, E.] Ctr Astrobiol INTA CSIC, Dept Astrofis, POB 78, E-28691 Madrid, Spain. [Solano, E.] Spanish Virtual Observ, Madrid, Spain. [DeMeo, F. E.] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [DeMeo, F. E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 16, Cambridge, MA 02138 USA. RP Carry, B (reprint author), Univ Lille, Univ Paris 06, Univ Sorbonne, PSL Res Univ,IMCCE,Observ Paris,CNRS, Lille, France. EM benoit.carry@oca.eu RI Solano, Enrique/C-2895-2017 FU European Commission [H2020-PROTEC-2014, 640351]; Spanish MICINN [AyA2008-02156, AyA2011-24052]; Region Ile de France; project Equip@Meso of the programme Investissements dAvenir by Agence Nationale pour la Recherche [ANR-10-EQPX-29-01]; National Science Foundation [0907766]; National Aeronautics and Space Administration; Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society FX We thanks S. Greenstreet for providing the source region mapper extended to include Mars-crosser space. We acknowledge support from the Faculty of the European Space Astronomy Centre (ESAC) for B. Carry's visit. S. Eggl would like to acknowledge the support of the European Commission H2020-PROTEC-2014 Grant No. 640351 (NEOShield-2). This publication makes use of the NEAs Precovery Service, developed under the Spanish Virtual Observatory project (Centro de Astrobiologia, INTA-CSIC) supported from the Spanish MICINN through grants AyA2008-02156 and AyA2011-24052. This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements dAvenir supervised by the Agence Nationale pour la Recherche. This material is based upon work supported, in part, by the National Science Foundation under Grant 0907766. 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.; This publication makes use of data products from the Wide field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Funding for the creation and distribution of the SDSS Archive has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/. NR 108 TC 3 Z9 3 U1 2 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 APR PY 2016 VL 268 BP 340 EP 354 DI 10.1016/j.icarus.2015.12.047 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DD9AN UT WOS:000370218100023 ER PT J AU Averianov, A Sues, HD AF Averianov, Alexander Sues, Hans-Dieter TI Troodontidae (Dinosauria: Theropoda) from the Upper Cretaceous of Uzbekistan SO CRETACEOUS RESEARCH LA English DT Article DE Dinosauria; Theropoda; Troodontidae; Cretaceous; Uzbekistan ID STENONYCHOSAURUS-INEQUALIS SAURISCHIA; REPUBLIC-OF-CHINA; OLDMAN FORMATION; NORTHERN ALASKA; INFORMATION; EVOLUTION; MONGOLIA; FORMOSUS; ALBERTA; ORIGIN AB To date three taxa of troodontid theropod dinosaurs have been recognized from Upper Cretaceous strata in two regions of the Kyzylkum Desert in Uzbekistan. The Cenomanian Khodzhakul Formation in the southwestern Kyzylkum Desert has yielded isolated serrated teeth and some postcranial bones of an indeterminate troodontid. In the central Kyzylkum Desert troodontids are known from the Cenomanian Dzharakuduk Formation (Urbacodon itemirensis) and the Turonian Bissekty Formation (Urbacodon sp.). Urbacodon itemirensis is known from a single dentary whereas Urbacodon sp. is represented by isolated teeth, maxilla and dentary fragments, a partial braincase, and some postcranial bones. The troodontid affinities of Urbacodon are supported by several synapomorphies: presence of a subotic recess; reduced basal tubera placed directly under the occipital condyle; maxilla participating in the margin of the external naris; nutrient foramina on dentary situated within a deep lateral groove; dentary without distinct interdental plates; large number of small dentary and maxillary teeth; teeth constricted between root and crown; anterior dentary teeth smaller, more numerous, more closely spaced than those in the middle of the tooth row, and implanted in a groove; posterior dorsal vertebrae with tall and posterodorsally tapering neural spines; and presence of a midline sulcus on the neural arches of distal caudals. Among Troodontidae, Urbacodon resembles Byronosaurus, Gobivenator, and Xixiasaurus in the absence of serrations on the tooth crowns and having premaxillary teeth that are D-shaped in cross-section. However, phylogenetic analysis did not recover a Glade of Asiatic troodontids with unserrated teeth. Published by Elsevier Ltd. C1 [Averianov, Alexander] Russian Acad Sci, Inst Zool, Univ Skaya Nab 1, St Petersburg 199034, Russia. [Averianov, Alexander] St Petersburg State Univ, Geol Fac, Dept Sedimentary Geol, 16 Liniya VO 29, St Petersburg 199178, Russia. [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. RP Sues, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM dzharakuduk@mail.ru; suesh@si.edu RI Averianov, Alexander/M-8490-2013 OI Averianov, Alexander/0000-0001-5948-0799 FU National Science Foundation [EAR-9804771, EAR-0207004]; National Geographic Society [5901-97, 6281-98]; Navoi Mining and Metallurgy Combinat; Russian Scientific Fund [14-14-00015] FX Fieldwork in Uzbekistan was facilitated by and conducted in cooperation with the Zoological Institute of the National Academy of Sciences of Uzbekistan, particularly D.A. Azimov and Y.A. Chikin. For their efforts in the field, scientific expertise, and camaraderie, we thank A.V. Abramov, J.D. Archibald, G.O. Cherepanov, I.G. Danilov, S. Dominguez, N. Morris, C.M. Redman, A.S. Resvyi, C. Skrabec, P.P. Skutschas, E.V. Syromyatnikova, and DJ. Ward. M. Pinsdorf skillfully prepared ZIN PH 2308/16. The field work in 1997-2006 was funded by the National Science Foundation (EAR-9804771 and EAR-0207004 to J.D. Archibald and H.-D. Sues), the National Geographic Society (5901-97 and 6281-98 to J.D. Archibald and H.-D. Sues), and the Navoi Mining and Metallurgy Combinat. The laboratory research by AA is supported by the Russian Scientific Fund (14-14-00015). Two anonymous reviewers provided helpful comments on a draft of the manuscript. NR 52 TC 1 Z9 1 U1 3 U2 19 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0195-6671 EI 1095-998X J9 CRETACEOUS RES JI Cretac. Res. PD APR PY 2016 VL 59 BP 98 EP 110 DI 10.1016/j.cretres.2015.11.005 PG 13 WC Geology; Paleontology SC Geology; Paleontology GA DB5PP UT WOS:000368566400006 ER PT J AU Sues, HD Averianov, A AF Sues, Hans-Dieter Averianov, Alexander TI Therizinosauroidea (Dinosauria: Theropoda) from the Upper Cretaceous of Uzbekistan SO CRETACEOUS RESEARCH LA English DT Article DE Dinosauria; Theropoda; Therizinosauroidea; Cretaceous; Uzbekistan ID REPUBLIC-OF-CHINA; FALCARIUS-UTAHENSIS; NORTHWESTERN CHINA; NORTH-AMERICA; MANIRAPTORA; AFFINITIES; BRAINCASE; ANATOMY AB Skeletal remains of indeterminate therizinosauroid dinosaurs are present in the Cenomanian Khodzhakul Formation and common in the Turonian Bissekty Formation of Uzbekistan. At least two taxa are present in the Bissekty Formation based on different frontal and humerus morphotypes. Phylogenetic analysis based on a dataset with 348 morphological characters and including all known therizinosaurian taxa places the Bissekty taxa as derived non-therizinosaurid therizinosauroids. The Bissekty therizinosauroids are more derived than Alxasaurus elesitaiensis in the extensive pneumatization of the postcranial axial skeleton, the absence of teeth in the anterior portion of the dentary, the weak development or even absence of pits for the collateral ligaments on the manual phalanges, and the sub triangular medial aspect of the distal end of the humerus, with the entepicondyle positioned well medial to the ulnar condyle. They are less derived than Therizinosauridae in the presence of a basisphenoid recess, the absence of pneumatic openings on the anterior caudal vertebrae, the distal end of metacarpal III not being ginglymoid in dorsal view, and the separation of the femoral head from the neck of that bone by a raised ventral rim. Published by Elsevier Ltd. C1 [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. [Averianov, Alexander] Russian Acad Sci, Inst Zool, Univ Skaya Nab 1, St Petersburg 199034, Russia. [Averianov, Alexander] St Petersburg State Univ, Geol Fac, Dept Sedimentary Geol, 16 Liniya VO 29, St Petersburg 199178, Russia. RP Sues, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM suesh@si.edu; dzharakuduk@mail.ru RI Averianov, Alexander/M-8490-2013; OI Averianov, Alexander/0000-0001-5948-0799; Sues, Hans-Dieter/0000-0002-9911-7254 FU National Science Foundation [EAR-9804771, EAR-0207004]; National Geographic Society [5901-97, 6281-98]; Navoi Mining and Metallurgy Combinat; Russian Scientific Fund [14-14-00015] FX Fieldwork in Uzbekistan was facilitated by and conducted in cooperation with the Zoological Institute of the National Academy of Sciences of Uzbekistan, particularly D.A. Azimov and Y.A. Chikin. For their efforts in the field, scientific expertise, and camaraderie, we thank A.V. Abramov, J.D. Archibald, G.O. Cherepanov, I.G. Danilov, S. Dominguez, C. King, N. Morris, C.M. Redman, A.S. Resvyi, C. Skrabec, P.P. Skutschas, E.V. Syromyatnikova, and D.J. Ward. We thank M. Machalski and D. Madzia for helpful comments on a draft of the manuscript. The field work in 1997-2006 was funded by the National Science Foundation (EAR-9804771 and EAR-0207004 to J.D. Archibald and H.-D. Sues), the National Geographic Society (5901-97 and 6281-98 to J.D. Archibald and H.-D. Sues), and the Navoi Mining and Metallurgy Combinat. The laboratory research by AA is supported by the Russian Scientific Fund (14-14-00015). NR 35 TC 2 Z9 2 U1 1 U2 6 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0195-6671 EI 1095-998X J9 CRETACEOUS RES JI Cretac. Res. PD APR PY 2016 VL 59 BP 155 EP 178 DI 10.1016/j.cretres.2015.11.003 PG 24 WC Geology; Paleontology SC Geology; Paleontology GA DB5PP UT WOS:000368566400011 ER PT J AU Reich, PB Sendall, KM Stefanski, A Wei, XR Rich, RL Montgomery, RA AF Reich, Peter B. Sendall, Kerrie M. Stefanski, Artur Wei, Xiaorong Rich, Roy L. Montgomery, Rebecca A. TI Boreal and temperate trees show strong acclimation of respiration to warming SO NATURE LA English DT Article ID LEAF RESPIRATION; THERMAL-ACCLIMATION; PLANT RESPIRATION; CLIMATE; PHOTOSYNTHESIS; FEEDBACKS; NITROGEN; POPULATIONS; VEGETATION; RESPONSES AB Plant respiration results in an annual flux of carbon dioxide (CO2) to the atmosphere that is six times as large as that due to the emissions from fossil fuel burning, so changes in either will impact future climate. As plant respiration responds positively to temperature, a warming world may result in additional respiratory CO2 release, and hence further atmospheric warming(1,2). Plant respiration can acclimate to altered temperatures, however, weakening the positive feedback of plant respiration to rising global air temperature(3-7), but a lack of evidence on long-term (weeks to years) acclimation to climate warming in field settings currently hinders realistic predictions of respiratory release of CO2 under future climatic conditions. Here we demonstrate strong acclimation of leaf respiration to both experimental warming and seasonal temperature variation for juveniles of ten North American tree species growing for several years in forest conditions. Plants grown and measured at 3.4 degrees C above ambient temperature increased leaf respiration by an average of 5% compared to plants grown and measured at ambient temperature; without acclimation, these increases would have been 23%. Thus, acclimation eliminated 80% of the expected increase in leaf respiration of non-acclimated plants. Acclimation of leaf respiration per degree temperature change was similar for experimental warming and seasonal temperature variation. Moreover, the observed increase in leaf respiration per degree increase in temperature was less than half as large as the average reported for previous studies(4,7), which were conducted largely over shorter time scales in laboratory settings. If such dampening effects of leaf thermal acclimation occur generally, the increase in respiration rates of terrestrial plants in response to climate warming may be less than predicted, and thus may not raise atmospheric CO2 concentrations as much as anticipated. C1 [Reich, Peter B.; Sendall, Kerrie M.; Stefanski, Artur; Wei, Xiaorong; Rich, Roy L.; Montgomery, Rebecca A.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. [Reich, Peter B.] Univ Western Sydney, Hawkesbury Inst Environm, Penrith, NSW 2753, Australia. [Wei, Xiaorong] Northwest A&F Univ, State Key Lab Soil Eros & Dryland Farming Loess P, Yangling 712100, Peoples R China. [Rich, Roy L.] Smithsonian Environm Res Ctr, Edgewater, MD 20137 USA. RP Reich, PB (reprint author), Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA.; Reich, PB (reprint author), Univ Western Sydney, Hawkesbury Inst Environm, Penrith, NSW 2753, Australia. EM preich@umn.edu FU US Department of Energy, Office of Science, Office of Biological and Environmental Research award [DE-FG02-07ER64456]; Minnesota Agricultural Experiment Station [MIN-42-030, MIN-42-060]; Minnesota Department of Natural Resources; College of Food, Agricultural, and Natural Resources Sciences; Wilderness Research Foundation; University of Minnesota FX This research was supported by the US Department of Energy, Office of Science, Office of Biological and Environmental Research award DE-FG02-07ER64456; Minnesota Agricultural Experiment Station MIN-42-030 and MIN-42-060; the Minnesota Department of Natural Resources; and the College of Food, Agricultural, and Natural Resources Sciences and Wilderness Research Foundation, University of Minnesota. Assistance with experimental operation and data collection was provided by K. Rice, C. Buschena, C. Zhao, H. Jihua and numerous summer interns. NR 31 TC 13 Z9 13 U1 41 U2 88 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 31 PY 2016 VL 531 IS 7596 BP 633 EP + DI 10.1038/nature17142 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DH8EX UT WOS:000373027400037 PM 26982730 ER PT J AU Vieira, LM Almeida, ACS Winston, JE AF Vieira, Leandro M. Almeida, Ana C. S. Winston, Judith E. TI Taxonomy of intertidal cheilostome Bryozoa of Maceio, northeastern Brazil. Part 1: Suborders Inovicellina, Malacostegina and Thalamoporellina SO ZOOTAXA LA English DT Article DE Alagoas; Atlantic; Biodiversity; bryozoans; new species ID SUBTROPICAL WESTERN ATLANTIC; CONTINENTAL-SHELF; GENUS; SOUTH AB Thirteen cheilostome bryozoan species from intertidal habitats of Maceio, Alagoas State, Brazil, are reported here. We describe four new species: Aetea cultrata n. sp., Biflustra marcusi n. sp., Biflustra sphinx n. sp. and Jellyella brasiliensis n. sp. Two other species of Inovicellina, Aetea arcuata Winston & Hayward, 2012, and Aetea curta Jullien, 1888, and four species of Malacostegina, Arbocuspis bellula (Hincks, 1881), Arbocuspis bicornis (Hincks, 1881), Arbocuspis ramosa (Osburn, 1940), and Jellyella tuberculata (Bosc, 1802), are reported on drift algae. Three species of Thalamoporellina are found for the first time in Maceio, Labioporella tuberculata Winston, Vieira & Woollacoot, 2014, Steginoporella magnilabris (Busk, 1854) and Thalamoporella floridana Osburn, 1940. C1 [Vieira, Leandro M.; Almeida, Ana C. S.] Univ Fed Pernambuco, Ctr Ciencias Biol, Dept Zool, Lab Estudos Bryozoa, BR-50670810 Recife, PE, Brazil. [Almeida, Ana C. S.] Univ Fed Bahia, Museu Zool, BR-40170290 Salvador, BA, Brazil. [Winston, Judith E.] Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. RP Vieira, LM (reprint author), Univ Fed Pernambuco, Ctr Ciencias Biol, Dept Zool, Lab Estudos Bryozoa, BR-50670810 Recife, PE, Brazil. EM leandromanzoni@hotmail.com RI Vieira, Leandro/B-7712-2011; OI Manzoni Vieira, Leandro/0000-0001-8661-8861; Almeida, Ana Carolina/0000-0003-4899-1483 FU FAPESP through the Graduate Program in Zoology of the Departamento de Zoologia - IBUSP [06/05141-8] FX This study is part of the L.M. Vieira's Master dissertation conducted between 2006-2008 and supported by FAPESP (Proc. 06/05141-8) through the Graduate Program in Zoology of the Departamento de Zoologia - IBUSP. Thanks to Alvaro E. Migotto, for discussion and remarks on an early version of this paper. Thanks to Monica D. Correia (UFAL, Brazil), Hilda H. Sovierzoski (UFAL, Brazil), Victor R. Cedro (UFAL, Brazil) and Alvaro G.A. Borba Jr. for help with sampling specimens. JoAnn Sanner and Mary E. Spencer Jones provided help with comparative specimens. Thanks to D.P. Gordon, J.-G. Harmelin and O. Reverter-Gil, who provided useful comments to improve the text. Setor de Comunidade Bentonicas of Universidade Federal de Alagoas (UFAL), the Natural History Museum's Zoology Department (London) and the National Museum of Natural History, Smithsonian Institution (USA) provided logistical support for L.M. Vieira during this study. We also thank Centro de Pesquisa Goncalo Moniz (FIOCRUZ/BA) for SEM images. NR 105 TC 0 Z9 0 U1 1 U2 4 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 30 PY 2016 VL 4097 IS 1 BP 59 EP 83 PG 25 WC Zoology SC Zoology GA DK9ON UT WOS:000375260700003 PM 27394525 ER PT J AU Sedlacek, JA Kim, E Rittenhouse, ST Weck, PF Sadeghpour, HR Shaffer, JP AF Sedlacek, J. A. Kim, E. Rittenhouse, S. T. Weck, P. F. Sadeghpour, H. R. Shaffer, J. P. TI Electric Field Cancellation on Quartz by Rb Adsorbate-Induced Negative Electron Affinity SO PHYSICAL REVIEW LETTERS LA English DT Article ID SILICON DIOXIDE; SURFACE-STATES; LIQUID-HELIUM; RYDBERG ATOMS; ALPHA-QUARTZ; VAPOR; DIAMOND; SYSTEMS; CESIUM; LAYERS AB We investigate the (0001) surface of single crystal quartz with a submonolayer of Rb adsorbates. Using Rydberg atom electromagnetically induced transparency, we investigate the electric fields resulting from Rb adsorbed on the quartz surface, and measure the activation energy of the Rb adsorbates. We show that the adsorbed Rb induces negative electron affinity (NEA) on the quartz surface. The NEA surface allows low energy electrons to bind to the surface and cancel the electric field from the Rb adsorbates. Our results will be important for integrating Rydberg atoms into hybrid quantum systems, as fundamental probes of atom-surface interactions, and for studies of 2D electron gases bound to surfaces. C1 [Sedlacek, J. A.; Shaffer, J. P.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Kim, E.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. [Rittenhouse, S. T.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Rittenhouse, S. T.] US Naval Acad, Dept Phys, Annapolis, MD 21402 USA. [Weck, P. F.] Sandia Natl Labs, POB 5800, Albuquerque, NM 87185 USA. [Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Shaffer, JP (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. EM shaffer@nhn.ou.edu FU U.S. Department of Energy's National Nuclear Security Administration [DE-AC04-94AL85000]; DARPA Quasar program by a grant through ARO [60181-PH-DRP]; AFOSR [FA9550-12-1-0282]; NSF [PHY-1104424, NSF PHY-1516421]; NSF grant through ITAMP at the Harvard-Smithsonian Center for Astrophysics FX Sandia National Laboratories is a multiprogram laboratory managed and operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Corporation, for the U.S. Department of Energy's National Nuclear Security Administration under Contract No. DE-AC04-94AL85000. This work was supported by the DARPA Quasar program by a grant through ARO (Grant No. 60181-PH-DRP), AFOSR (Grant No. FA9550-12-1-0282), NSF (Grants No. PHY-1104424) and No. NSF PHY-1516421) and an NSF grant through ITAMP at the Harvard-Smithsonian Center for Astrophysics. The authors thank Tilman Pfau for useful discussions. NR 67 TC 6 Z9 6 U1 4 U2 13 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 MAR 30 PY 2016 VL 116 IS 13 AR 133201 DI 10.1103/PhysRevLett.116.133201 PG 7 WC Physics, Multidisciplinary SC Physics GA DH9EP UT WOS:000373099500006 PM 27081976 ER PT J AU Harding, LW Mallonee, ME Perry, ES Miller, WD Adolf, JE Gallegos, CL Paerl, HW AF Harding, Lawrence W., Jr. Mallonee, Michael E. Perry, Elgin S. Miller, W. David Adolf, Jason E. Gallegos, Charles L. Paerl, Hans W. TI Variable climatic conditions dominate recent phytoplankton dynamics in Chesapeake Bay SO SCIENTIFIC REPORTS LA English DT Article ID PERFORMANCE LIQUID-CHROMATOGRAPHY; PARTIALLY STRATIFIED ESTUARY; RIVER FLOW; SYNOPTIC CLIMATOLOGY; PRIMARY PRODUCTIVITY; FLORAL COMPOSITION; NORTH-CAROLINA; WATER-QUALITY; EUTROPHICATION; COASTAL AB Variable climatic conditions strongly influence phytoplankton dynamics in estuaries globally. Our study area is Chesapeake Bay, a highly productive ecosystem providing natural resources, transportation, and recreation for nearly 16 million people inhabiting a 165,000-km(2) watershed. Since World War II, nutrient over-enrichment has led to multiple ecosystem impairments caused by increased phytoplankton biomass as chlorophyll-a (chl-a). Doubled nitrogen (N) loadings from 1945-1980 led to increased chl-a, reduced water clarity, and low dissolved oxygen (DO), while decreased N loadings from 1981-2012 suggest modest improvement. The recent 30+ years are characterized by high inter-annual variability of chl-a, coinciding with irregular dry and wet periods, complicating the detection of long-term trends. Here, we synthesize time-series data for historical and recent N loadings (TN, NO2 + NO3), chl-a, floral composition, and net primary productivity (NPP) to distinguish secular changes caused by nutrient over-enrichment from spatio-temporal variability imposed by climatic conditions. Wet years showed higher chl-a, higher diatom abundance, and increased NPP, while dry years showed lower chl-a, lower diatom abundance, and decreased NPP. Our findings support a conceptual model wherein variable climatic conditions dominate recent phytoplankton dynamics against a backdrop of nutrient over-enrichment, emphasizing the need to separate these effects to gauge progress toward improving water quality in estuaries. C1 [Harding, Lawrence W., Jr.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. [Mallonee, Michael E.] US EPA, Interstate Commiss Potomac River Basin, Chesapeake Bay Program Off, 410 Severn Ave, Annapolis, MD 21403 USA. [Miller, W. David] US Naval Res Lab, 4555 Overlook Ave SW, Washington, DC 20375 USA. [Adolf, Jason E.] Univ Hawaii, Marine Sci Program, 200 W Kawili St, Hilo, HI 96720 USA. [Gallegos, Charles L.] Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. [Paerl, Hans W.] Univ North Carolina Chapel Hill, Inst Marine Sci, 3431 Arendell St, Morehead City, NC 28557 USA. RP Harding, LW (reprint author), Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. EM lharding@atmos.ucla.edu OI Gallegos, Charles/0000-0001-5112-0166; Miller, W. David/0000-0002-4940-5987 FU National Science Foundation (NSF) Land Margin Ecosystem Research, Biocomplexity, Biological Oceanography, Microbial Observatory, and Small Grants for Environmental Research (SGER) programs; Atlantic Coast Environmental Indicators Consortium (ACE-INC) - EPA; Atlantic Coast Environmental Indicators Consortium (ACE-INC) - National Aeronautics and Space Administration (NASA); NASA SeaWiFS Program; SIMBIOS Program; Chesapeake Bay Program Office of the National Oceanic and Atmospheric Administration (NOAA) FX The Authors acknowledge support from the Chesapeake Bay Program of the US Environmental Protection Agency (EPA) for providing water-quality and cell-counts data; grants from the National Science Foundation (NSF) Land Margin Ecosystem Research, Biocomplexity, Biological Oceanography, Microbial Observatory, and Small Grants for Environmental Research (SGER) programs; the Atlantic Coast Environmental Indicators Consortium (ACE-INC) supported by EPA and the National Aeronautics and Space Administration (NASA); NASA SeaWiFS and SIMBIOS Programs; and the Chesapeake Bay Program Office of the National Oceanic and Atmospheric Administration (NOAA). NR 60 TC 0 Z9 0 U1 5 U2 20 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 MAR 30 PY 2016 VL 6 AR 23773 DI 10.1038/srep23773 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DH8MW UT WOS:000373048400001 PM 27026279 ER PT J AU Brusatte, SL Averianov, A Sues, HD Muir, A Butler, IB AF Brusatte, Stephen L. Averianov, Alexander Sues, Hans-Dieter Muir, Amy Butler, Ian B. TI New tyrannosaur from the mid-Cretaceous of Uzbekistan clarifies evolution of giant body sizes and advanced senses in tyrant dinosaurs SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE dinosaur; Tyrannosauroidea; Uzbekistan; phylogenetics; evolution ID REPUBLIC-OF-CHINA; NORTH-AMERICA; THEROPODA; ANATOMY; OSTEOLOGY; ASIA; ALIORAMUS; BRAINCASE; POSITION; BEHAVIOR AB Tyrannosaurids-the familiar group of carnivorous dinosaurs including Tyrannosaurus and Albertosaurus-were the apex predators in continental ecosystems in Asia and North America during the latest Cretaceous (ca. 80-66 million years ago). Their colossal sizes and keen senses are considered key to their evolutionary and ecological success, but little is known about how these features developed as tyrannosaurids evolved from smaller basal tyrannosauroids that first appeared in the fossil record in the Middle Jurassic (ca. 170 million years ago). This is largely because of a frustrating 20+ million-year gap in the mid-Cretaceous fossil record, when tyrannosauroids transitioned from small-bodied hunters to gigantic apex predators but from which no diagnostic specimens are known. We describe the first distinct tyrannosauroid species from this gap, based on a highly derived braincase and a variety of other skeletal elements from the Turonian (ca. 90-92 million years ago) of Uzbekistan. This taxon is phylogenetically intermediate between the oldest basal tyrannosauroids and the latest Cretaceous forms. It had yet to develop the giant size and extensive cranial pneumaticity of T. rex and kin but does possess the highly derived brain and inner ear characteristic of the latest Cretaceous species. Tyrannosauroids apparently developed huge size rapidly during the latest Cretaceous, and their success in the top predator role may have been enabled by their brain and keen senses that first evolved at smaller body size. C1 [Brusatte, Stephen L.; Muir, Amy; Butler, Ian B.] Univ Edinburgh, Sch GeoSci, Edinburgh EH9 3FE, Midlothian, Scotland. [Averianov, Alexander] Russian Acad Sci, Zool Inst, St Petersburg 199034, Russia. [Averianov, Alexander] St Petersburg State Univ, Dept Sedimentary Geol, St Petersburg 199178, Russia. [Sues, Hans-Dieter] Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20560 USA. RP Brusatte, SL (reprint author), Univ Edinburgh, Sch GeoSci, Edinburgh EH9 3FE, Midlothian, Scotland. EM Stephen.Brusatte@ed.ac.uk RI Averianov, Alexander/M-8490-2013 OI Averianov, Alexander/0000-0001-5948-0799 FU Marie Curie Career Integration Grant [EC630652]; University of Edinburgh; National Science Foundation (NSF) [DDIG DEB-1110357]; NSF [EAR-9804771, EAR-0207004]; National Geographic Society [5901-97, 6281-98]; Russian Scientific Fund Project [14-14-00015] FX We thank many colleagues for discussion about tyrannosauroids: R. Benson, T. Carr, P. Currie, T. Holtz, J. Horner, M. Loewen, J. Lu, P. Makovicky, M. Norell, K. Padian, P. Sereno, T. Williamson, and X. Xu. T. Marshall skillfully prepared the drawing used in Fig. 1. S.L.B. is supported by Marie Curie Career Integration Grant EC630652 and the University of Edinburgh, and his trip to St. Petersburg was supported by National Science Foundation (NSF) DDIG DEB-1110357. A.A. and H.-D.S. acknowledge support for fieldwork from NSF EAR-9804771 and EAR-0207004 and Grants 5901-97 and 6281-98 from the National Geographic Society. A.A. was supported by the Russian Scientific Fund Project 14-14-00015. NR 47 TC 1 Z9 1 U1 15 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 MAR 29 PY 2016 VL 113 IS 13 BP 3447 EP 3452 DI 10.1073/pnas.1600140113 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DH6BQ UT WOS:000372876400035 PM 26976562 ER PT J AU Martin, ES AF Martin, Emily S. TI The distribution and characterization of strike-slip faults on Enceladus SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE tectonics; Saturnian satellites; Enceladus; fractures and faults ID SATURNS MOON ENCELADUS; NONSYNCHRONOUS ROTATION; TECTONIC PATTERNS; GROWTH MECHANICS; ECHELON CRACKS; TIGER STRIPES; ICE SHELL; HEAT-FLUX; EUROPA; STRESS AB Strike-slip faulting is typically characterized by lateral offsets on icy satellites of the outer solar system. However, strike-slip faults on Enceladus lack these typical lateral offsets and instead are marked by the presence of tailcracks or en echelon cracks. These features are used here to develop the first near-global distribution of strike-slip faults on Enceladus. Strike-slip faults on Enceladus fall into three broad categories: tectonic terrain boundaries, reactivated linear features, and primary strike-slip faults. All three types of strike-slip faults are found predominantly, or within close proximity to, the antipodal cratered terrains on the Saturnian and anti-Saturnian hemispheres. Stress modeling suggests that strike-slip faulting on Enceladus is not controlled by nonsynchronous rotation, as on Europa, suggesting a fundamentally different process driving Enceladus's strike-slip faulting. The motion along strike-slip faults at tectonic terrain boundaries suggests large-scale northward migration of the ice shell on the leading hemisphere of Enceladus, occurring perpendicular to the opening direction of the tiger stripes in the south polar terrain. C1 [Martin, Emily S.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Martin, Emily S.] Univ Idaho, Dept Geol Sci, Moscow, ID 83843 USA. RP Martin, ES (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.; Martin, ES (reprint author), Univ Idaho, Dept Geol Sci, Moscow, ID 83843 USA. EM martines@si.edu FU NASA [NNX11AP30H] FX This work was funded by NASA Earth and Space Science Fellowship grant NNX11AP30H. E.S.M. would like to acknowledge Simon Kattenhorn, D. Alex Patthoff, and Jennifer Whitten for helpful discussion and two anonymous reviewers for their comments which served to significantly improve this manuscript. The data used are listed in the references, tables, supporting information, and The CEPS Data Repository at http://airandspace.si.edu/CEPSData. NR 57 TC 0 Z9 0 U1 3 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 28 PY 2016 VL 43 IS 6 BP 2456 EP 2464 DI 10.1002/2016GL067805 PG 9 WC Geosciences, Multidisciplinary SC Geology GA DK1TM UT WOS:000374697200015 ER PT J AU Cui, P Lober, U Alquezar-Planas, DE Ishida, Y Courtiol, A Timms, P Johnson, RN Lenz, D Helgen, KM Roca, AL Hartman, S Greenwood, AD AF Cui, Pin Loeber, Ulrike Alquezar-Planas, David E. Ishida, Yasuko Courtiol, Alexandre Timms, Peter Johnson, Rebecca N. Lenz, Dorina Helgen, Kristofer M. Roca, Alfred L. Hartman, Stefanie Greenwood, Alex D. TI Comprehensive profiling of retroviral integration sites using target enrichment methods from historical koala samples without an assembled reference genome SO PEERJ LA English DT Article DE Integration sites; Retroviral endogenization; KoRV; Target enrichment; Clustering ID ENDOGENOUS RETROVIRUSES; WIDE ANALYSIS; SEQUENCE DATA; ANCIENT DNA; EVOLUTION; SELECTION; SOFTWARE; REVEALS; INVASION; PLATFORM AB Background. Retroviral integration into the host germline results in permanent viral colonization of vertebrate genomes. The koala retrovirus (KoRV) is currently invading the germline of the koala (Phascolarctos cinereus) and provides a unique opportunity for studying retroviral endogenization. Previous analysis of KoRV integration patterns in modern koalas demonstrate that they share integration sites primarily if they are related, indicating that the process is currently driven by vertical transmission rather than infection. However, due to methodological challenges, KoRV integrations have not been comprehensively characterized. Results. To overcome these challenges, we applied and compared three target enrichment techniques coupled with next generation sequencing (NGS) and a newly customized sequence-clustering based computational pipeline to determine the integration sites for 10 museum Queensland and New South Wales (NSW) koala samples collected between the 1870s and late 1980s. A secondary aim of this study sought to identify common integration sites across modern and historical specimens by comparing our dataset to previously published studies. Several million sequences were processed, and the KoRV integration sites in each koala were characterized. Conclusions. Although the three enrichment methods each exhibited bias in integration site retrieval, a combination of two methods, Primer Extension Capture and hybridization capture is recommended for future studies on historical samples. Moreover, identification of integration sites shows that the proportion of integration sites shared between any two koalas is quite small. C1 [Cui, Pin; Loeber, Ulrike; Alquezar-Planas, David E.; Greenwood, Alex D.] Leibniz Inst Zoo & Wildlife Res, Dept Wildlife Dis, Berlin, Germany. [Loeber, Ulrike; Hartman, Stefanie] Univ Potsdam, Inst Biochem & Biol, Potsdam, Germany. [Ishida, Yasuko; Roca, Alfred L.] Univ Illinois, Dept Anim Sci, Urbana, IL USA. [Courtiol, Alexandre] Leibniz Inst Zoo & Wildlife Res, Dept Evolutionary Ecol, Berlin, Germany. [Timms, Peter] Univ Sunshine Coast, Sippy Downs, Qld 4556, Australia. [Johnson, Rebecca N.] Australian Museum, Australian Ctr Wildlife Genom, 6-8 Coll St, Sydney, NSW 2000, Australia. [Lenz, Dorina] Leibniz Inst Zoo & Wildlife Res, Dept Evolutionary Genet, Berlin, Germany. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Helgen, Kristofer M.] Free Univ Berlin, Dept Vet Med, Berlin, Germany. RP Greenwood, AD (reprint author), Leibniz Inst Zoo & Wildlife Res, Dept Wildlife Dis, Berlin, Germany. EM greenwood@izw-berlin.de OI Courtiol, Alexandre/0000-0003-0637-2959 FU National Institute of General Medical Sciences (NIGMS) [R01GM092706]; Morris Animal Foundation [D14ZO-94]; China Scholarship Council; interdisciplinary training initiative "Evolution across Scales" - Volkswagen foundation [83459]; Deutscher Akademischer Austauschdienst-DAAD FX YI, ALR, KMH and ADG were supported by Grant Number R01GM092706 from the National Institute of General Medical Sciences (NIGMS). ADG was additionally supported by a grant from the Morris Animal Foundation, grant number D14ZO-94. PC was supported by a fellowship from the China Scholarship Council. UL was supported by the interdisciplinary training initiative "Evolution across Scales", funded by the Volkswagen foundation (Grant Number 83459). DEAP was supported by a scholarship from the Deutscher Akademischer Austauschdienst-DAAD. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 60 TC 1 Z9 1 U1 2 U2 6 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 28 PY 2016 VL 4 AR e1847 DI 10.7717/peerj.1847 PG 29 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DJ4EW UT WOS:000374159200007 PM 27069793 ER PT J AU Crabtree, KN Martin-Drumel, MA Brown, GG Gaster, SA Hall, TM McCarthy, MC AF Crabtree, Kyle N. Martin-Drumel, Marie-Aline Brown, Gordon G. Gaster, Sydney A. Hall, Taylor M. McCarthy, Michael C. TI Microwave spectral taxonomy: A semi-automated combination of chirped-pulse and cavity Fourier-transform microwave spectroscopy SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID ROTATIONAL SPECTROSCOPY; MILLIMETER; SPECTROMETER; MOLECULES; CHEMISTRY; STATES; C3S AB Because of its structural specificity, rotational spectroscopy has great potential as an analytical tool for characterizing the chemical composition of complex gas mixtures. However, disentangling the individual molecular constituents of a rotational spectrum, especially if many of the lines are entirely new or unknown, remains challenging. In this paper, we describe an empirical approach that combines the complementary strengths of two techniques, broadband chirped-pulse Fourier transform microwave spectroscopy and narrowband cavity Fourier transform microwave spectroscopy, to characterize and assign lines. This procedure, called microwave spectral taxonomy, involves acquiring a broadband rotational spectrum of a rich mixture, categorizing individual lines based on their relative intensities under series of assays, and finally, linking rotational transitions of individual chemical compounds within each category using double resonance techniques. The power of this procedure is demonstrated for two test cases: a stable molecule with a rich spectrum, 3,4-difluorobenzaldehyde, and products formed in an electrical discharge through a dilute mixture of C2H2 and CS2, in which spectral taxonomy has enabled the identification of propynethial, HC(S) CCH. (C) 2016 AIP Publishing LLC. C1 [Crabtree, Kyle N.] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA. [Martin-Drumel, Marie-Aline; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Martin-Drumel, Marie-Aline; McCarthy, Michael C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Brown, Gordon G.; Gaster, Sydney A.; Hall, Taylor M.] Coker Coll, Hartsville, SC 29550 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; McCarthy, MC (reprint author), Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu OI Crabtree, Kyle/0000-0001-5629-5192; Martin-Drumel, Marie-Aline/0000-0002-5460-4294 FU NSF [CHE-1213200, 1213560]; Smithsonian Astrophysical Observatory FX M.C.M. and M.-A.M.-D. acknowledge support from NSF Grant No. CHE-1213200. M.-A.M.-D. was partially supported by a Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory. G.G.B. acknowledges the support of NSF Award No. 1213560. NR 34 TC 3 Z9 3 U1 7 U2 14 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD MAR 28 PY 2016 VL 144 IS 12 AR 124201 DI 10.1063/1.4944072 PG 12 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA DI6XV UT WOS:000373644400023 PM 27036440 ER PT J AU Martin-Drumel, MA McCarthy, MC Patterson, D McGuire, BA Crabtree, KN AF Martin-Drumel, Marie-Aline McCarthy, Michael C. Patterson, David McGuire, Brett A. Crabtree, Kyle N. TI Automated microwave double resonance spectroscopy: A tool to identify and characterize chemical compounds SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID FOURIER-TRANSFORM SPECTROSCOPY; MULTIDIMENSIONAL NMR; SPECTROMETER; SPECTRA AB Owing to its unparalleled structural specificity, rotational spectroscopy is a powerful technique to unambiguously identify and characterize volatile, polar molecules. We present here a new experimental approach, automated microwave double resonance (AMDOR) spectroscopy, to rapidly determine the rotational constants of these compounds without a priori knowledge of elemental composition or molecular structure. This task is achieved by rapidly acquiring the classical (frequency vs. intensity) broadband spectrum of a molecule using chirped-pulse Fourier transform microwave (FTMW) spectroscopy and subsequently analyzing it in near real-time using complementary cavity FTMW detection and double resonance. AMDOR measurements provide a unique "barcode" for each compound from which rotational constants can be extracted. To illustrate the power of this approach, AMDOR spectra of three aroma compounds - trans-cinnamaldehyde, alpha-, and beta-ionone - have been recorded and analyzed. The prospects to extend this approach to mixture characterization and purity assessment are described. (C) 2016 AIP Publishing LLC. C1 [Martin-Drumel, Marie-Aline; McCarthy, Michael C.; McGuire, Brett A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Martin-Drumel, Marie-Aline; McCarthy, Michael C.] Harvard Univ, Sch Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02138 USA. [Patterson, David] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [McGuire, Brett A.] Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22903 USA. [Crabtree, Kyle N.] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA. RP Crabtree, KN (reprint author), Univ Calif Davis, Dept Chem, Davis, CA 95616 USA. EM kncrabtree@ucdavis.edu OI Crabtree, Kyle/0000-0001-5629-5192; Martin-Drumel, Marie-Aline/0000-0002-5460-4294 FU NSF [CHE-1213200] FX The authors thank E. S. Palmer and P. Antonucci for technical assistance. M.C.M. and M.A.M.-D. acknowledge support from NSF Grant No. CHE-1213200. B.A.M. thanks A. J. Remijan for his support. NR 29 TC 3 Z9 3 U1 1 U2 6 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD MAR 28 PY 2016 VL 144 IS 12 AR 124202 DI 10.1063/1.4944089 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA DI6XV UT WOS:000373644400024 PM 27036441 ER PT J AU McCarthy, MC Martinez, O McGuire, BA Crabtree, KN Martin-Drumel, MA Stanton, JF AF McCarthy, Michael C. Martinez, Oscar, Jr. McGuire, Brett A. Crabtree, Kyle N. Martin-Drumel, Marie-Aline Stanton, John F. TI Isotopic studies of trans- and cis-HOCO using rotational spectroscopy: Formation, chemical bonding, and molecular structures SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CO REACTANT COMPLEX; HIGH-PRESSURE RANGE; INDUCED FLUORESCENCE MEASUREMENTS; DOUBLE-RESONANCE SPECTROSCOPY; MICROWAVE SPECTROSCOPY; INFRARED-SPECTRA; ATOM EXCHANGE; RATE-CONSTANT; BASIS-SETS; PLUS CO AB HOCO is an important intermediate in combustion and atmospheric processes because the OH + CO -> H + CO2 reaction represents the final step for the production of CO2 in hydrocarbon oxidation, and theoretical studies predict that this reaction proceeds via various intermediates, the most important being this radical. Isotopic investigations of trans- and cis-HOCO have been undertaken using Fourier transform microwave spectroscopy and millimeter-wave double resonance techniques in combination with a supersonic molecular beam discharge source to better understand the formation, chemical bonding, and molecular structures of this radical pair. We find that trans-HOCO can be produced almost equally well from either OH + CO or H + CO2 in our discharge source, but cis-HOCO appears to be roughly two times more abundant when starting from H + CO2. Using isotopically labelled precursors, the OH + (CO)-O-18 reaction predominately yields (HOCO)-O-18 for both isomers, but (HOCO)-O-18 is observed as well, typically at the level of 10%-20% that of (HOCO)-O-18; the opposite propensity is found for the (OH)-O-18 + CO reaction. DO + (CO)-O-18 yields similar ratios between (DOCO)-O-18 and (DOCO)-O-18 as those found for OH + (CO)-O-18, suggesting that some fraction of HOCO (or DOCO) may be formed from the back-reaction H + CO2, which, at the high pressure of our gas expansion, can readily occur. The large C-13 Fermi-contact term (a(F)) for trans- and cis-(HOCO)-C-13 implicates significant unpaired electronic density in a sigma-type orbital at the carbon atom, in good agreement with theoretical predictions. By correcting the experimental rotational constants for zero-point vibration motion calculated theoretically using second-order vibrational perturbation theory, precise geometrical structures have been derived for both isomers. (C) 2016 AIP Publishing LLC. C1 [McCarthy, Michael C.; Martinez, Oscar, Jr.; McGuire, Brett A.; Crabtree, Kyle N.; Martin-Drumel, Marie-Aline] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [McCarthy, Michael C.; Martinez, Oscar, Jr.; McGuire, Brett A.; Crabtree, Kyle N.; Martin-Drumel, Marie-Aline] Harvard Univ, Sch Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02138 USA. [McGuire, Brett A.] Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22901 USA. [Stanton, John F.] Univ Texas Austin, Dept Chem & Biochem, 1 Univ Stn A5300, Austin, TX 78712 USA. [Martinez, Oscar, Jr.] US Air Force, Res Lab, Space Vehicles Directorate, Kirtland AFB, NM 87117 USA. [Crabtree, Kyle N.] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; McCarthy, MC (reprint author), Harvard Univ, Sch Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu OI Crabtree, Kyle/0000-0001-5629-5192; Martin-Drumel, Marie-Aline/0000-0002-5460-4294 FU U.S. National Science Foundation [CHE-1012743, CHE-1361031]; Smithsonian Astrophysical Observatory; Robert A. Welch Foundation of Houston, Texas [F-1283]; U.S. Department of Energy, Office of Basic Energy Sciences [DE-FG02-07ER15884] FX The authors thank C. A. Gottlieb, G. B. Ellison, and D. J. Nesbitt for helpful discussions. The work in Cambridge is supported by the U.S. National Science Foundation (Grant No. CHE-1012743). B. A. McGuire thanks A. J. Remijan for his support. K. N. Crabtree was supported by a CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory. The work in Austin is supported by the Robert A. Welch Foundation (Grant No. F-1283) of Houston, Texas, the U.S. National Science Foundation (Grant No. CHE-1361031) and the U.S. Department of Energy, Office of Basic Energy Sciences (Contract No. DE-FG02-07ER15884). NR 78 TC 2 Z9 2 U1 6 U2 17 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD MAR 28 PY 2016 VL 144 IS 12 AR 124304 DI 10.1063/1.4944070 PG 11 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA DI6XV UT WOS:000373644400028 PM 27036445 ER PT J AU Shen, XL Bourg, NA McShea, WJ Turner, BL AF Shen, Xiaoli Bourg, Norman A. McShea, William J. Turner, Benjamin L. TI Long-Term Effects of White-Tailed Deer Exclusion on the Invasion of Exotic Plants: A Case Study in a Mid-Atlantic Temperate Forest SO PLOS ONE LA English DT Article ID DECIDUOUS FORESTS; BIRD POPULATIONS; UNDERSTORY; PENNSYLVANIA; BIODIVERSITY; VEGETATION; USA; INTRODUCTIONS; DIVERSITY; HERBIVORE AB Exotic plant invasions and chronic high levels of herbivory are two of the major biotic stressors impacting temperate forest ecosystems in eastern North America, and the two problems are often linked. We used a 4-ha deer exclosure maintained since 1991 to examine the influence of a generalist herbivore, white-tailed deer (Odocoileus virginianus), on the abundance of four exotic invasive (Rosa multiflora, Berberis thunbergii, Rubus phoenicolasius and Microstegium vimineum) and one native (Cynoglossum virginianum) plant species, within a 25.6-ha mature temperate forest dynamics plot in Virginia, USA. We identified significant predictors of the abundance of each focal species using generalized linear models incorporating 10 environmental and landscape variables. After controlling for those predictors, we applied our models to a 4-ha deer exclusion site and a 4-ha reference site, both embedded within the larger plot, to test the role of deer on the abundance of the focal species. Slope, edge effects and soil pH were the most frequent predictors of the abundance of the focal species on the larger plot. The abundance of C. virginianum, known to be deer-dispersed, was significantly lower in the exclosure. Similar patterns were detected for B. thunbergii, R. phoenicolasius and M. vimineum, whereas R. multiflora was more abundant within the exclosure. Our results indicate that chronic high deer density facilitates increased abundances of several exotic invasive plant species, with the notable exception of R. multiflora. We infer that the invasion of many exotic plant species that are browse-tolerant to whitetailed deer could be limited by reducing deer populations. C1 [Shen, Xiaoli; Bourg, Norman A.; McShea, William J.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA USA. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Shen, Xiaoli] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing, Peoples R China. [Bourg, Norman A.] US Geol Survey, Natl Res Program, Eastern Branch, 959 Natl Ctr, Reston, VA 22092 USA. RP Shen, XL (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA USA.; Shen, XL (reprint author), Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing, Peoples R China. EM xlshen.pku@gmail.com RI Turner, Benjamin/E-5940-2011; OI Turner, Benjamin/0000-0002-6585-0722; Bourg, Norman/0000-0002-7443-1992 FU Smithsonian Global Earth Observatory initiative; Smithsonian Institution; HSBC; National Zoo; Earthwatch Foundation FX The Smithsonian Global Earth Observatory initiative (http://www.forestgeo.si.edu/), the Smithsonian Institution (http://www.si.edu/), and the HSBC Climate Partnership (http://www.theclimategroup.org/programs/hsbc-climate-partnership/) provided the funding for establishing the SCBI Large Forest Dynamics Plot. The Friends of the National Zoo (https://nationalzoo.si.edu/JoinFONZ/Join/) and Earthwatch Foundation (http://earthwatch.org/) supported the original exclosure fence installation. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 60 TC 1 Z9 2 U1 18 U2 46 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAR 28 PY 2016 VL 11 IS 3 AR e0151825 DI 10.1371/journal.pone.0151825 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DH5EH UT WOS:000372807800021 PM 27019356 ER PT J AU McLaughlin, BM Ballance, CP Schippers, S Hellhund, J Kilcoyne, ALD Phaneuf, RA Muller, A AF McLaughlin, B. M. Ballance, C. P. Schippers, S. Hellhund, J. Kilcoyne, A. L. D. Phaneuf, R. A. Mueller, A. TI Photoionization of tungsten ions: experiment and theory for W2+ and W3+ SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article DE photoionization cross sections; tungsten ions; large scale ID R-MATRIX METHOD; ELECTRON-SCATTERING; CROSS-SECTION; IONIZATION; EXCITATION AB Experimental and theoretical results are reported for single-photon single ionization of W2+ and W3+ tungsten ions. Experiments were performed at the photon-ion merged-beam setup of the Advanced Light Source in Berkeley. Absolute cross sections and detailed energy scans were measured over an energy range 20-90 eV at a bandwidth of 100 meV. Broad peak features with widths typically around 5 eV have been observed with almost no narrow resonances present in the investigated energy range. Theoretical results were obtained from a Dirac-Coulomb R-matrix approach. The calculations were carried out for the lowest-energy terms of the investigated tungsten ions with levels 5s(2)5p(6)5d(4) D-5(J) = 0, 1, 2, 3, 4 for W2+ and 5s(2)5p(6)5d(3) F-4(J') J' = 3 2, 5 2, 7 2, 9 2 for W3+. Assuming a statistically weighted distribution of ions in the initial ground-term levels there is good agreement of theory and experiment for W3+ ions. However, for W2+ ions at higher energies there is a factor of approximately two difference between experimental and theoretical cross sections. C1 [McLaughlin, B. M.; Ballance, C. P.] Queens Univ Belfast, CTAMOP, Sch Math & Phys, David Bates Bldg,7 Coll Pk, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, MS-14, Cambridge, MA 02138 USA. [Schippers, S.; Hellhund, J.; Mueller, A.] Univ Giessen, Inst Atom & Mol Phys, D-35392 Giessen, Germany. [Schippers, S.] Univ Giessen, Inst Phys 1, D-35392 Giessen, Germany. [Kilcoyne, A. L. D.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA. [Hellhund, J.; Phaneuf, R. A.] Univ Nevada, Dept Phys, Reno, NV 89557 USA. RP McLaughlin, BM (reprint author), Queens Univ Belfast, CTAMOP, Sch Math & Phys, David Bates Bldg,7 Coll Pk, Belfast BT7 1NN, Antrim, North Ireland.; McLaughlin, BM (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, MS-14, Cambridge, MA 02138 USA.; Muller, A (reprint author), Univ Giessen, Inst Atom & Mol Phys, D-35392 Giessen, Germany. EM bmclaughlin899@btinternet.com; Alfred.Mueller@iamp.physik.uni-giessen.de RI Muller, Alfred/A-3548-2009; Kilcoyne, David/I-1465-2013; Schippers, Stefan/A-7786-2008 OI Muller, Alfred/0000-0002-0030-6929; Schippers, Stefan/0000-0002-6166-7138 FU Deutsche Forschungsgemeinschaft (DFG) [Mu 1068/20]; NASA; NSF grants through Auburn University; US National Science Foundation; Office of Science of the US Department of Energy [DE-AC05-00OR22725]; Office of Science, Office of Basic Energy Sciences, of the US Department of Energy [DE-AC02-05CH11231] FX The Giessen group acknowledges support by Deutsche Forschungsgemeinschaft (DFG) under project number Mu 1068/20. C P Ballance was supported by NASA and NSF grants through Auburn University. B M McLaughlin acknowledges support by the US National Science Foundation through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics, under the visitors program, Queen's University Belfast for the award of a visiting research fellowship (VRF). The computational work was carried out at the National Energy Research Scientific Computing Center in Oakland, CA, USA and at the High Performance Computing Center Stuttgart (HLRS) of the University of Stuttgart, Stuttgart, Germany. This research also used resources of the Oak Ridge Leadership Computing Facility at the Oak Ridge National Laboratory, which is supported by the Office of Science of the US Department of Energy under Contract No. DE-AC05-00OR22725. The Advanced Light Source is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the US Department of Energy under Contract No. DE-AC02-05CH11231. NR 41 TC 1 Z9 1 U1 4 U2 10 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 2016 VL 49 IS 6 AR 065201 DI 10.1088/0953-4075/49/6/065201 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA DG0UW UT WOS:000371782200028 ER PT J AU Mecke, S Kieckbusch, M O'Shea, M Kaiser, H AF Mecke, Sven Kieckbusch, Max O'Shea, Mark Kaiser, Hinrich TI First Record of the Poorly Known Skink Sphenomorphus oligolepis (Boulenger, 1914) (Reptilia: Squamata: Scincidae) from Seram Island, Maluku Province, Indonesia SO ASIAN HERPETOLOGICAL RESEARCH LA English DT Article DE Scincidae; Lygosominae; Sphenomorphus oligolepis; new record; Seram; Maluku Islands; Indonesia; Wallacea ID VARANIDAE; SERPENTES AB Based on four specimens discovered in the collection of The Natural History Museum, London, United Kingdom, we present a new distribution record for the skink Sphenomorphus oligolepis for Seram Island, Maluku Province, Indonesia. This find constitutes the westernmost record for the species and extends its range by over 800 km. The species was heretofore only known from apparently isolated mainland New Guinean populations. C1 [Mecke, Sven; Kieckbusch, Max] Univ Marburg, Fac Biol, Dept Anim Evolut & Systemat & Zool Collect Marbur, Karl von Frisch Str 8, D-35032 Marburg, Germany. [O'Shea, Mark] Wolverhampton Univ, Fac Sci & Engn, Wulfruna St, Wolverhampton WV1 1LY, W Midlands, England. [O'Shea, Mark] West Midland Safari Pk, Bewdley DY12 1LF, Worcs, England. [Kaiser, Hinrich] Victor Valley Coll, Dept Biol, 18422 Bear Valley Rd, Victorville, CA 92395 USA. [Kaiser, Hinrich] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Mecke, S (reprint author), Univ Marburg, D-35032 Marburg, Germany. EM meckes@staff.uni-marburg.de FU Harvard University FX We are indebted to Patrick Campbell (BMNH) for his hospitality and the loan of specimens. We thank Jose Rosado and Joseph Martinez (MCZ), and Pumehana Imada and Allen Allison (BPBM) for access to specimens photographed by one of us (MOS). We also thank Ronald Lilley (The Indonesian Nature Foundation) for providing some of the cited literature, Glenn Shea (The University of Sydney) for providing unpublished data of Sphenomorphus oligolepis, and Thomas Beitz for the photographs of the S. oligolepis specimens from Seram (Figure 2). We are very grateful to George R. Zug (USNM) and an anonymous reviewer for their helpful comments on earlier versions of the manuscript. Travel funds to visit the MCZ were provided by an Ernst Mayr Grant from Harvard University to MOS. NR 15 TC 0 Z9 0 U1 1 U2 1 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 2095-0357 J9 ASIAN HERPETOL RES JI Asian Herpetol. Res. PD MAR 25 PY 2016 VL 7 IS 1 BP 64 EP 68 PG 5 WC Zoology SC Zoology GA DJ3CY UT WOS:000374083600010 ER PT J AU Wilf, P Zhang, SP Chikkerur, S Little, SA Wing, SL Serre, T AF Wilf, Peter Zhang, Shengping Chikkerur, Sharat Little, Stefan A. Wing, Scott L. Serre, Thomas TI Computer vision cracks the leaf code SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE leaf architecture; leaf venation; computer vision; sparse coding; paleobotany ID ANGIOSPERM PHYLOGENY; IMAGE FEATURES; CLASSIFICATION; DISTANCE; PLANTS; SHAPE AB Understanding the extremely variable, complex shape and venation characters of angiosperm leaves is one of the most challenging problems in botany. Machine learning offers opportunities to analyze large numbers of specimens, to discover novel leaf features of angiosperm clades that may have phylogenetic significance, and to use those characters to classify unknowns. Previous computer vision approaches have primarily focused on leaf identification at the species level. It remains an open question whether learning and classification are possible among major evolutionary groups such as families and orders, which usually contain hundreds to thousands of species each and exhibit many times the foliar variation of individual species. Here, we tested whether a computer vision algorithm could use a database of 7,597 leaf images from 2,001 genera to learn features of botanical families and orders, then classify novel images. The images are of cleared leaves, specimens that are chemically bleached, then stained to reveal venation. Machine learning was used to learn a codebook of visual elements representing leaf shape and venation patterns. The resulting automated system learned to classify images into families and orders with a success rate many times greater than chance. Of direct botanical interest, the responses of diagnostic features can be visualized on leaf images as heat maps, which are likely to prompt recognition and evolutionary interpretation of a wealth of novel morphological characters. With assistance from computer vision, leaves are poised to make numerous new contributions to systematic and paleobotanical studies. C1 [Wilf, Peter; Little, Stefan A.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Zhang, Shengping; Serre, Thomas] Brown Univ, Dept Cognit Linguist & Psychol Sci, Brown Inst Brain Sci, Providence, RI 02912 USA. [Zhang, Shengping] Harbin Inst Technol, Sch Comp Sci & Technol, Weihai 264209, Shandong, Peoples R China. [Chikkerur, Sharat] Microsoft, Azure Machine Learning, Cambridge, MA 02142 USA. [Little, Stefan A.] Univ Paris 11, Lab Ecol Systemat & Evolut, Bat 425, F-91405 Orsay, France. [Wing, Scott L.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Wilf, P (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.; Zhang, SP; Serre, T (reprint author), Brown Univ, Dept Cognit Linguist & Psychol Sci, Brown Inst Brain Sci, Providence, RI 02912 USA.; Zhang, SP (reprint author), Harbin Inst Technol, Sch Comp Sci & Technol, Weihai 264209, Shandong, Peoples R China. EM pwilf@psu.edu; s.zhang@hit.edu.cn; thomas_serre@brown.edu OI Wing, Scott/0000-0002-2954-8905 FU David and Lucile Packard Foundation; National Science Foundation [IIS-1252951]; Defense Advanced Research Projects Agency Young Investigator Award [N66001-14-1-4037]; Office of Naval Research Grant [N000141110743]; Brown Center for Computation and Visualization; National Natural Science Foundation of China [61300111, 61133003] FX We thank A. Young and J. Kissell for image preparations, the anonymous reviewers for helpful comments, Y. Guo for software, A. Rozo for book scanning, and D. Erwin for assistance with the Axelrod collection. We acknowledge financial support from the David and Lucile Packard Foundation (P. W.); National Science Foundation Early Career Award IIS-1252951, Defense Advanced Research Projects Agency Young Investigator Award N66001-14-1-4037, Office of Naval Research Grant N000141110743, and the Brown Center for Computation and Visualization (T. S.); and National Natural Science Foundation of China Grant 61300111 and Key Program Grant 61133003 (to S.Z.). NR 38 TC 3 Z9 4 U1 5 U2 21 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 MAR 22 PY 2016 VL 113 IS 12 BP 3305 EP 3310 DI 10.1073/pnas.1524473113 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DH0QH UT WOS:000372488200058 PM 26951664 ER PT J AU Mezcua, M Prieto, MA Fernandez-Ontiveros, JA Tristram, KRW AF Mezcua, M. Prieto, M. A. Fernandez-Ontiveros, J. A. Tristram, K. R. W. TI The nuclear dust lane of Circinus: collimation without a torus SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: high angular resolution; astrometry; galaxies: nuclei; galaxies: Seyfert; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; SEYFERT 2 GALAXIES; CORONAL-LINE REGION; CENTRAL PARSECS; X-RAY; SPECTROPOLARIMETRY; RADIATION; NGC-1068; VLT; AGN AB In some AGN, nuclear dust lanes connected to kpc-scale dust structures provide all the extinction required to obscure the nucleus, challenging the role of the dusty torus proposed by the Unified Model. In this letter, we show the pc-scale dust and ionized gas maps of Circinus constructed using sub-arcsec-accuracy registration of infrared VLT AO images with optical Hubble Space Telescope images. We find that the collimation of the ionized gas does not require a torus but is caused by the distribution of dust lanes of the host galaxy on similar to 10 pc scales. This finding questions the presumed torus morphology and its role at parsec scales, as one of its main attributes is to collimate the nuclear radiation, and is in line with interferometric observations which show that most of the pc-scale dust is in the polar direction. We estimate that the nuclear dust lane in Circinus provides 1/3 of the extinction required to obscure the nucleus. This constitutes a conservative lower limit to the obscuration at the central parsecs, where the dust filaments might get optically thicker if they are the channels that transport material from similar to 100 pc scales to the centre. C1 [Mezcua, M.] Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada. [Mezcua, M.] Harvard Smithsonian Ctr Astrophys CfA, 60 Garden St, Cambridge, MA 02138 USA. [Mezcua, M.; Prieto, M. A.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Prieto, M. A.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Fernandez-Ontiveros, J. A.] IAPS, INAF, Via Fosso del Cavaliere 100, I-00133 Rome, Italy. [Tristram, K. R. W.] European So Observ, Alonso de Cordova 3107,Casilla 19001, Santiago, Chile. RP Mezcua, M (reprint author), Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada.; Mezcua, M (reprint author), Harvard Smithsonian Ctr Astrophys CfA, 60 Garden St, Cambridge, MA 02138 USA.; Mezcua, M (reprint author), Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. EM marmezcua.astro@gmail.com; aprieto@iac.es OI Tristram, Konrad/0000-0001-8281-5059 FU NASA Chandra Grant [G05-16099X] FX The authors thank the referee L. Burtscher, for his valuable comments which have helped improve this manuscript, and M. Elvis for insightful discussion. MM acknowledges support from the NASA Chandra Grant G05-16099X. NR 39 TC 0 Z9 0 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 21 PY 2016 VL 457 IS 1 BP L94 EP L98 DI 10.1093/mnrasl/slv209 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO9GY UT WOS:000378094600020 ER PT J AU Nicholl, M Smartt, SJ AF Nicholl, M. Smartt, S. J. TI Seeing double: the frequency and detectability of double-peaked superluminous supernova light curves SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; supernovae: individual: LSQ14bdq ID LUMINOUS SUPERNOVAE; SHOCK BREAKOUT; EMISSION; GALAXIES; MASS; DISCOVERY; TRANSIENT; MAGNETAR; WIND AB The discovery of double-peaked light curves in some superluminous supernovae (SLSNe) offers an important new clue to their origins. We examine the published photometry of all Type Ic SLSNe, finding 14 objectswith constraining data or limits around the time of explosion. Of these, eight (including the already identified SN 2006oz and LSQ14bdq) show plausible flux excess at the earliest epochs, which deviate by 2-9 sigma from polynomial fits to the rising light curves. Simple scaling of the LSQ14bdq data show that they are all consistent with a similar double-peaked structure. PS1-10pm provides multicolour UV data indicating a temperature of T-bb = 25000 +/- 5000 K during the early 'bump' phase. We find that a double-peak cannot be excluded in any of the other six objects, and that this behaviour may be ubiquitous. The homogeneity of the observed bumps is unexpected for interaction-powered models. Enginepowered models can explain the observations if all progenitors have extended radii or the central engine drives shock breakout emission several days after the supernova explosion. C1 [Nicholl, M.; Smartt, S. J.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Nicholl, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Nicholl, M (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.; Nicholl, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM matt.nicholl@cfa.harvard.edu FU European Research Council: EU [291222] FX We thank Edo Berger, Jeff Cooke, Dan Kasen, Brian Metzger, Bob Nichol and Tony Piro for helpful discussion. Funded by the European Research Council: EU(FP7/2007-2013) Grant no. [291222]. NR 35 TC 6 Z9 6 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 21 PY 2016 VL 457 IS 1 BP L79 EP L83 DI 10.1093/mnrasl/slv210 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DO9GY UT WOS:000378094600017 ER PT J AU Kieckbusch, M Mecke, S Hartmann, L Ehrmantraut, L O'Shea, M Kaiser, H AF Kieckbusch, Max Mecke, Sven Hartmann, Lukas Ehrmantraut, Lisa O'Shea, Mark Kaiser, Hinrich TI An inconspicuous, conspicuous new species of Asian pipesnake, genus Cylindrophis (Reptilia: Squamata: Cylindrophiidae), from the south coast of Jawa Tengah, Java, Indonesia, and an overview of the tangled taxonomic history of C. ruffus (Laurenti, 1768) SO ZOOTAXA LA English DT Article DE Cylindrophis subocularis sp nov.; C. ruffus; Serpentes; Cylindrophiidae; Asian pipesnakes; species complex; morphology; Central Java; Indonesia; Greater Sunda Islands ID BENT-TOED GECKO; SERPENTES; SNAKES; GEKKONIDAE; REDESCRIPTION; COLLECTION; COLUBRIDAE; SUMATRA; ORIGIN AB We describe a new species of Cylindrophis currently known only from Grabag, Purworejo Regency, Jawa Tengah Province (Central Java), Java, Indonesia. Cylindrophis subocularis sp. nov. can be distinguished from all congeners by the presence of a single, eponymous subocular scale between the 3rd and 4th or 4th and 5th supralabial, preventing contact between the 4 th or 5 th supralabial and the orbit, and by having the prefrontal in narrow contact with or separated from the orbit. We preface our description with a detailed account of the tangled taxonomic history of the similar and putatively wide-ranging species C. ruffus, which leads us to (1) remove the name Scytale scheuchzeri from the synonymy of C. ruffus, (2) list the taxon C. rufa var. javanica as species inquirenda, and (3) synonymize C. mirzae with C. ruffus. We provide additional evidence to confirm that the type locality of C. ruffus is Java. Cylindrophis subocularis sp. nov. is the second species of Asian pipesnake from Java. C1 [Kieckbusch, Max; Mecke, Sven; Hartmann, Lukas; Ehrmantraut, Lisa] Univ Marburg, Fac Biol, Dept Anim Evolut & Systemat & Zool Collect Marbur, Karl Von Frisch Str 8, D-35032 Marburg, Germany. [O'Shea, Mark] Wolverhampton Univ, Fac Sci & Engn, Wulfruna St, Wolverhampton WV1 1LY, W Midlands, England. [O'Shea, Mark] West Midland Safari Pk, Bewdley DY12 1LF, Worcs, England. [Kaiser, Hinrich] Victor Valley Coll, Dept Biol, 18422 Bear Valley Rd, Victorville, CA 92395 USA. [Kaiser, Hinrich] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Kieckbusch, M (reprint author), Univ Marburg, Fac Biol, Dept Anim Evolut & Systemat & Zool Collect Marbur, Karl Von Frisch Str 8, D-35032 Marburg, Germany. EM kieckbus@students.uni-marburg.de FU AMNH collection study grant FX For the loans of specimens and for access to collections under their care during our visits, we are very grateful to Esther Dondorp (RMNH); Georg Gassner, Silke Schweiger, and Heinz Grillitsch (NMW); and Frank Tillack and Mark-Oliver Rodel (ZMB). Further important material for comparison was provided by Lauren Vonnahme, David A. Dickey, David A. Kizirian, and Christopher J. Raxworthy (AMNH); Andreas Schmitz (MHNG); Markus Auer and Raffael Ernst (MTKD); Stefan T. Hertwig (NHM); Urs Wuest and Denis Vallan (NMB); Linda Acker and Gunther Kohler (SMF); Jakob Hallermann (ZMH); and Kelvin Lim (ZRC). We are very grateful to Harry W. Greene (Cornell University, Ithaca, USA), John C. Murphy (FMHN), Marinus S. Hoogmoed (MPEG), Roy W. McDiarmid (USNM), George R. Zug (USNM), Frank Tillack, Gernot Vogel, and an anonymous reviewer for their helpful comments on earlier versions of the manuscript. SM thanks Glenn Shea (AM) for fruitful discussions regarding scale characteristics and pholidotic aberrations. We thank Britta Doring (Philipps-Universitat Marburg, Germany) for contributing to data collection. Many thanks to Felix Mader who prepared the drawings in Figs. 4 & 6, and to Gunther Kohler who provided the photograph on which the illustration in Fig. 6 is based. We further thank Linda Acker, Aaron M. Bauer (Villanova University, Villanova, USA), Esther Dondorp, Georg Gassner, Heinz Grillitsch, Gunther Kohler, Silke Schweiger, and Frank Tillack for providing some of the literature cited below. This study was supported by an AMNH collection study grant to SM. This paper is contribution No. 19 from the Tropical Research Initiative at Victor Valley College. NR 95 TC 1 Z9 1 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 21 PY 2016 VL 4093 IS 1 BP 1 EP 25 PG 25 WC Zoology SC Zoology GA DK9NT UT WOS:000375258300001 PM 27394478 ER PT J AU Slepian, Z Eisenstein, DJ AF Slepian, Zachary Eisenstein, Daniel J. TI A simple analytic treatment of linear growth of structure with baryon acoustic oscillations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmology: theory; large-scale structure of Universe ID MICROWAVE BACKGROUND ANISOTROPIES; COSMOLOGICAL PERTURBATION-THEORY; LARGE-SCALE STRUCTURE; PROBING DARK ENERGY; EXPANDING UNIVERSE; REDSHIFT SURVEYS; POWER-SPECTRUM; MATTER; RADIATION; FLUCTUATIONS AB In linear perturbation theory, all information about the growth of structure is contained in the Green's function, or equivalently, transfer function. These functions are generally computed using numerical codes or by phenomenological fitting formula anchored in accurate analytic results in the limits of large and small scale. Here, we present a framework for analytically solving all scales, in particular the intermediate scales relevant for the baryon acoustic oscillations (BAO). We solve for the Green's function and transfer function using spherically averaged overdensities and the approximation that the density of the coupled baryon-photon fluid is constant interior to the sound horizon. C1 [Slepian, Zachary; Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Slepian, Z; Eisenstein, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM zslepian@fas.harvard.edu; deisenstein@cfa.harvard.edu FU National Science Foundation [DGE-1144152]; US Department of Energy [DE-SC0013718] FX ZS thanks Aaron Bray, Anthony Challinor, George Efstathiou, Douglas Finkbeiner, Lehman Garrison, Margaret Geller, Avi Loeb, Ramesh Narayan, Stephen Portillo, David Spergel, and Alexander Wiegand for many valuable discussions, and Meredith MacGregor, Philip Mocz, and Stephen Portillo for careful reads of the manuscript. ZS especially thanks Yuan-Sen Ting for an extensive and rigorous set of comments, Harry Desmond for helpful suggestions on the broader context of the work, and the anonymous referee for comments that improved the presentation of the work. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under Grant no. DGE-1144152; DJE is supported by grant DE-SC0013718 from the US Department of Energy. NR 50 TC 0 Z9 0 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 21 PY 2016 VL 457 IS 1 BP 24 EP 37 DI 10.1093/mnras/stv2889 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH2FM UT WOS:000372599600003 ER PT J AU Payne, MJ Veras, D Holman, MJ Gansicke, BT AF Payne, Matthew J. Veras, Dimitri Holman, Matthew J. Gaensicke, Boris T. TI Liberating exomoons in white dwarf planetary systems SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; celestial mechanics; minor planets, asteroids: general; Moon; planets and satellites: dynamical evolution and stability; white dwarfs ID POST-MAIN-SEQUENCE; STELLAR MASS-LOSS; GREAT ESCAPE; BROWN DWARF; ROCKY PLANETESIMALS; INFRARED EXCESS; BINARY-SYSTEMS; DEBRIS DISKS; EVOLUTION; STARS AB Previous studies indicate that more than a quarter of all white dwarf (WD) atmospheres are polluted by remnant planetary material, with some WDs being observed to accrete the mass of Pluto in 10(6) yr. The short sinking time-scale for the pollutants indicates that the material must be frequently replenished. Moons may contribute decisively to this pollution process if they are liberated from their parent planets during the post-main-sequence evolution of the planetary systems. Here, we demonstrate that gravitational scattering events amongst planets in WD systems easily trigger moon ejection. Repeated close encounters within tenths of planetary Hill radii are highly destructive to even the most massive, close-in moons. Consequently, scattering increases both the frequency of perturbing agents in WD systems, as well as the available mass of polluting material in those systems, thereby enhancing opportunities for collision and fragmentation and providing more dynamical pathways for smaller bodies to reach the WD. Moreover, during intense scattering, planets themselves have pericentres with respect to the WD of only a fraction of an astronomical unit, causing extreme Hill-sphere contraction, and the liberation of moons into WD-grazing orbits. Many of our results are directly applicable to exomoons orbiting planets around main-sequence stars. C1 [Payne, Matthew J.; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA. [Veras, Dimitri; Gaensicke, Boris T.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Payne, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA.; Veras, D (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM mpayne@cfa.harvard.edu; d.veras@warwick.ac.uk RI Gaensicke, Boris/A-9421-2012 OI Gaensicke, Boris/0000-0002-2761-3005 FU Royal Society [IE140641]; NASA Origins of Solar Systems Program [NNX13A124G, NNX10AH40G, 1312645088477]; BSF [2012384]; European Union through ERC [320964]; Institute for Theory and Computation at the Harvard-Smithsonian Center for Astrophysics FX All authors gratefully acknowledge the Royal Society, whose funding (grant number IE140641) supported the research leading to these results. MJP also acknowledges Smithsonian 2015 CGPS/Pell Grant, NASA Origins of Solar Systems Program grant NNX13A124G, NASA Origins of Solar Systems Program grant NNX10AH40G via sub-award agreement 1312645088477, and BSF Grant Number 2012384. DV and BTG also benefited by support from the European Union through ERC grant number 320964. DV further acknowledges support from the Institute for Theory and Computation at the Harvard-Smithsonian Center for Astrophysics. NR 93 TC 12 Z9 12 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 21 PY 2016 VL 457 IS 1 BP 217 EP 231 DI 10.1093/mnras/stv2966 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH2FM UT WOS:000372599600015 ER PT J AU Narayan, R Zhu, YC Psaltis, D Sadowski, A AF Narayan, Ramesh Zhu, Yucong Psaltis, Dimitrios Sadowski, Aleksander TI HEROIC: 3D general relativistic radiative post-processor with comptonization for black hole accretion discs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; MHD; radiative transfer; stars: black holes; galaxies: nuclei ID X-RAY BINARIES; ACTIVE GALACTIC NUCLEI; MONTE-CARLO CODE; SUPER-EDDINGTON ACCRETION; MAGNETOHYDRODYNAMIC SIMULATIONS; NUMERICAL SIMULATIONS; PLUNGING REGION; KERR SPACETIME; M1 CLOSURE; SPECTRA AB We describe Hybrid Evaluator for Radiative Objects Including Comptonization (HEROIC), an upgraded version of the relativistic radiative post-processor code HERO described in a previous paper, but which now Includes Comptonization. HEROIC models Comptonization via the Kompaneets equation, using a quadratic approximation for the source function in a short characteristics radiation solver. It employs a simple form of accelerated lambda iteration to handle regions of high scattering opacity. In addition to solving for the radiation field, HEROIC also solves for the gas temperature by applying the condition of radiative equilibrium. We present benchmarks and tests of the Comptonization module in HEROIC with simple 1D and 3D scattering problems. We also test the ability of the code to handle various relativistic effects using model atmospheres and accretion flows in a black hole space-time. We present two applications of HEROIC to general relativistic magnetohydrodynamics simulations of accretion discs. One application is to a thin accretion disc around a black hole. We find that the gas below the photosphere in the multidimensional HEROIC solution is nearly isothermal, quite different from previous solutions based on 1D plane parallel atmospheres. The second application is to a geometrically thick radiation-dominated accretion disc accreting at 11 times the Eddington rate. Here, the multidimensional HEROIC solution shows that, for observers who are on axis and look down the polar funnel, the isotropic equivalent luminosity could be more than 10 times the Eddington limit, even though the spectrum might still look thermal and show no signs of relativistic beaming. C1 [Narayan, Ramesh; Zhu, Yucong] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Psaltis, Dimitrios] Univ Arizona, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Sadowski, Aleksander] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rnarayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NSF [AST1312651]; NASA [TCAN NNX14AB47G, NAS8-03060]; NASA through Einstein Postdoctotral Fellowship - Chandra X-ray Center [PF4-150126]; NSF via XSEDE [TG-AST080026N] FX The authors thank Jonathan McKinney and an anonymous referee for helpful comments and suggestions. RN and YZ were supported in part by NSF grant AST1312651. RN also received partial support under NASA grant TCAN NNX14AB47G. AS acknowledges support by NASA through Einstein Postdoctotral Fellowship number PF4-150126 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. AS also thanks the Harvard-Smithsonian Center for Astrophysics for hospitality. The authors acknowledge computational support from NSF via XSEDE resources (grant TG-AST080026N), and from NASA via the High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 88 TC 4 Z9 4 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 21 PY 2016 VL 457 IS 1 BP 608 EP 628 DI 10.1093/mnras/stv2979 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH2FM UT WOS:000372599600043 ER PT J AU Nicastro, F Senatore, F Gupta, A Guainazzi, M Mathur, S Krongold, Y Elvis, M Piro, L AF Nicastro, F. Senatore, F. Gupta, A. Guainazzi, M. Mathur, S. Krongold, Y. Elvis, M. Piro, L. TI X-ray detection of warm ionized matter in the Galactic halo SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Galaxy: abundances; Galaxy: disc; Galaxy: halo; local interstellar matter; galaxies: ISM; X-rays: ISM ID HOT INTERGALACTIC MEDIUM; ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; MULTIPHASE INTERSTELLAR-MEDIUM; BINARY 4U 0614+091; ABSORPTION SPECTROSCOPY; SCULPTOR WALL; K ABSORPTION; OXYGEN IONS; ATOMIC DATA; SIGHT LINE AB We report on a systematic investigation of the cold and mildly ionized gaseous baryonic metal components of our Galaxy, through the analysis of high-resolution Chandra and XMM-Newton spectra of two samples of Galactic and extragalactic sources. The comparison between lines of sight towards sources located in the disc of our Galaxy and extragalactic sources allows us for the first time to clearly distinguish between gaseous metal components in the disc and halo of our Galaxy. We find that a warm ionized metal medium (WIMM) permeates a large volume above and below the Galaxy's disc, perhaps up to the circum-galactic space. This halo WIMM imprints virtually the totality of the OI and OII absorption seen in the spectra of our extragalactic targets, has a temperature of T-WIMM(Halo) = 2900 +/- 900 K, a density < nH >(Halo)(WIMM) = 0.023 +/- 0.009 cm(-3) and a metallicity Z(WIMM)(Halo) = (0.4 +/- 0.1) Z(circle dot). Consistently with previous works, we also confirm that the disc of the Galaxy contains at least two distinct gaseous metal components, one cold and neutral (the CNMM: cold neutral metal medium) and one warm and mildly ionized, with the same temperature of the haloWIMM, but higher density (< nH >(Disc)(WIMM) = 0.09 +/- 0.03 cm(-3)) and metallicity (Z(WIMM)(Disc) = 0.8 +/- 0.1 Z(circle dot)). By adopting a simple disc+sphere geometry for the Galaxy, we estimate masses of the CNMM and the total (disc + halo) WIMM of M-CNMM less than or similar to 8 x 10(8) M-circle dot and M-WIMM similar or equal to 8.2 x 10(9) M-circle dot. C1 [Nicastro, F.; Senatore, F.] Osservatorio Astronom Roma INAF, Via Frascati 33, I-00040 Monte Porzio Catone, RM, Italy. [Nicastro, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-04, Cambridge, MA 02138 USA. [Nicastro, F.] Univ Crete, Iraklion 71003, Greece. [Senatore, F.] Univ Roma Tor Vergata, Via Orazio Raimondo 18, I-00173 Rome, Italy. [Gupta, A.; Mathur, S.] Ohio State Univ, Columbus, OH 43210 USA. [Gupta, A.] Columbus State Community Coll, Columbus, OH 43215 USA. [Guainazzi, M.] ESA, European Space Astron Ctr, E-28691 Madrid, Spain. [Mathur, S.] Ohio State Univ, CCAPP, Columbus, OH 43210 USA. [Krongold, Y.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Piro, L.] Ist Astrofs & Planetol Spaziali INAF, I-00133 Rome, Italy. RP Nicastro, F (reprint author), Osservatorio Astronom Roma INAF, Via Frascati 33, I-00040 Monte Porzio Catone, RM, Italy.; Nicastro, F; Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-04, Cambridge, MA 02138 USA.; Nicastro, F (reprint author), Univ Crete, Iraklion 71003, Greece.; Mathur, S (reprint author), Ohio State Univ, Columbus, OH 43210 USA.; Mathur, S (reprint author), Ohio State Univ, CCAPP, Columbus, OH 43210 USA. EM fabrizio.nicastro@oa-roma.inaf.it; smita@astronomy.ohio-state.edu; melvis@cfa.harvard.edu FU INAF-PRIN grant [1.05.01.98.10] FX We thank the anonymous referee for the useful comments that helped improving the paper, and Ehud Behar for providing wavelength, oscillator strengths and transition probabilities of inner-shell transitions of C, O and Ne. FN acknowledges support from INAF-PRIN grant 1.05.01.98.10. 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 MAR 21 PY 2016 VL 457 IS 1 BP 676 EP 694 DI 10.1093/mnras/stv2923 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH2FM UT WOS:000372599600047 ER PT J AU Bozza, V Shvartzvald, Y Udalski, A Novati, SC Bond, IA Han, C Hundertmark, M Poleski, R Pawlak, M Szymanski, MK Skowron, J Mroz, P Kozlowski, S Wyrzykowski, L Pietrukowicz, P Soszynski, I Ulaczyk, K Beichman, C Bryden, G Carey, S Fausnaugh, M Gaudi, BS Gould, A Henderson, CB Pogge, RW Wibking, B Yee, JC Zhu, W Abe, F Asakura, Y Barry, RK Bennett, DP Bhattacharya, A Donachie, M Freeman, M Fukui, A Hirao, Y Inayama, K Itow, Y Koshimoto, N Li, MCA Ling, CH Masuda, K Matsubara, Y Muraki, Y Nagakane, M Nishioka, T Ohnishi, K Oyokawa, H Rattenbury, N Saito, T Sharan, A Sullivan, DJ Sumi, T Suzuki, D Tristram, PJ Wakiyama, Y Yonehara, A Choi, JY Park, H Jung, YK Shin, IG Albrow, MD Park, BG Kim, SL Lee, CU Cha, SM Kim, DJ Lee, Y Dominik, M Jorgensen, UG Andersen, MI Bramich, DM Burgdorf, MJ Ciceri, S D'Ago, G Evans, DF Jaimes, RF Gu, SH Hinse, TC Kains, N Kerins, E Korhonen, H Kuffmeier, M Mancini, L Popovas, A Rabus, M Rahvar, S Rasmussen, RT Scarpetta, G Skottfelt, J Snodgrass, C Southworth, J Surdej, J Unda-Sanzana, E von Essen, C Wang, YB Wertz, O Maoz, D Friedmann, M Kaspi, S AF Bozza, V. Shvartzvald, Y. Udalski, A. Novati, S. Calchi Bond, I. A. Han, C. Hundertmark, M. Poleski, R. Pawlak, M. Szymanski, M. K. Skowron, J. Mroz, P. Kozlowski, S. Wyrzykowski, L. Pietrukowicz, P. Soszynski, I. Ulaczyk, K. Beichman, C. Bryden, G. Carey, S. Fausnaugh, M. Gaudi, B. S. Gould, A. Henderson, C. B. Pogge, R. W. Wibking, B. Yee, J. C. Zhu, W. Abe, F. Asakura, Y. Barry, R. K. Bennett, D. P. Bhattacharya, A. Donachie, M. Freeman, M. Fukui, A. Hirao, Y. Inayama, K. Itow, Y. Koshimoto, N. Li, M. C. A. Ling, C. H. Masuda, K. Matsubara, Y. Muraki, Y. Nagakane, M. Nishioka, T. Ohnishi, K. Oyokawa, H. Rattenbury, N. Saito, To. Sharan, A. Sullivan, D. J. Sumi, T. Suzuki, D. Tristram, P. J. Wakiyama, Y. Yonehara, A. Choi, J. -Y. Park, H. Jung, Y. K. Shin, I. -G. Albrow, M. D. Park, B. -G. Kim, S. -L. Lee, C. -U. Cha, S. -M. Kim, D. -J. Lee, Y. Dominik, M. Jorgensen, U. G. Andersen, M. I. Bramich, D. M. Burgdorf, M. J. Ciceri, S. D'Ago, G. Evans, D. F. Jaimes, R. Figuera Gu, S. -H. Hinse, T. C. Kains, N. Kerins, E. Korhonen, H. Kuffmeier, M. Mancini, L. Popovas, A. Rabus, M. Rahvar, S. Rasmussen, R. T. Scarpetta, G. Skottfelt, J. Snodgrass, C. Southworth, J. Surdej, J. Unda-Sanzana, E. von Essen, C. Wang, Y. -B. Wertz, O. Maoz, D. Friedmann, M. Kaspi, S. CA OGLE Grp SPITZER Team MOA Grp KMTNet Grp MiNDSTEp WISE Grp TI SPITZER OBSERVATIONS OF OGLE-2015-BLG-1212 REVEAL A NEW PATH TOWARD BREAKING STRONG MICROLENS DEGENERACIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; Galaxy: bulge; gravitational lensing: micro; planets and satellites: detection; space vehicles ID GRAVITATIONAL LENSING EXPERIMENT; GALACTIC BULGE; OGLE-III; BINARY; EVENTS; SATELLITE; PARALLAXES; PHOTOMETRY; SYSTEMS; STARS AB Spitzer microlensing parallax observations of OGLE-2015-BLG-1212 decisively break. a degeneracy between planetary and binary solutions that is somewhat ambiguous when only ground-based data are considered. Only eight viable models survive out of an initial set of 32 local minima in the parameter space. These models clearly indicate that the lens is a stellar binary system possibly located within the bulge of our Galaxy, ruling out the planetary alternative. We argue that several types of discrete degeneracies can be broken via such space-based parallax observations. C1 [Bozza, V.; Novati, S. Calchi; D'Ago, G.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo II 132, I-84084 Fisciano, SA, Italy. [Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy. [Shvartzvald, Y.; Bryden, G.; Henderson, C. B.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Udalski, A.; Poleski, R.; Pawlak, M.; Szymanski, M. K.; Skowron, J.; Mroz, P.; Kozlowski, S.; Wyrzykowski, L.; Pietrukowicz, P.; Soszynski, I.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. [Novati, S. Calchi; D'Ago, G.; Scarpetta, G.] IIASS, Via G Pellegrino 19, I-84019 Vietri Sul Mare, SA, Italy. [Novati, S. Calchi; Beichman, C.] NASA, Exoplanet Sci Inst, CALTECH, MS 100-22, Pasadena, CA 91125 USA. [Bond, I. A.; Ling, C. H.] Massey Univ, Inst Informat & Math Sci, North Shore Mail Ctr, Private Bag 102-904, Auckland, New Zealand. [Han, C.; Bhattacharya, A.; Choi, J. -Y.; Park, H.; Jung, Y. K.; Shin, I. -G.] Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea. [Hundertmark, M.; Jorgensen, U. G.; Korhonen, H.; Kuffmeier, M.; Popovas, A.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark. [Hundertmark, M.; Jorgensen, U. G.; Korhonen, H.; Kuffmeier, M.; Popovas, A.; Skottfelt, J.] Univ Copenhagen, Ctr Star & Planet Format, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark. [Poleski, R.; Fausnaugh, M.; Gaudi, B. S.; Gould, A.; Henderson, C. B.; Pogge, R. W.; Wibking, B.; Zhu, W.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. [Ulaczyk, K.] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England. [Carey, S.] CALTECH, Ctr Sci, Spitzer, MS 220-6, Pasadena, CA USA. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Abe, F.; Asakura, Y.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Nishioka, T.; Oyokawa, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Barry, R. K.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bennett, D. P.; Suzuki, D.] NASA, Lab Exoplanets & Stellar Astrophys, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bhattacharya, A.; Wakiyama, Y.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Donachie, M.; Freeman, M.; Li, M. C. A.; Rattenbury, N.; Sharan, A.] Univ Auckland, Dept Phys, Private Bag 92019, Auckland, New Zealand. [Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, 3037-5 Honjo, Asakuchi, Okayama 7190232, Japan. [Hirao, Y.; Koshimoto, N.; Nagakane, M.; Sumi, T.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Inayama, K.; Yonehara, A.] Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kyoto 6038555, Japan. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Saito, To.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan. [Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand. [Tristram, P. J.] Mt John Univ Observ, POB 56, Lake Tekapo 8770, New Zealand. [Albrow, M. D.] Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch 8020, New Zealand. [Cha, S. -M.; Kim, D. -J.; Lee, Y.] Kyung Hee Univ, Sch Space Res, Yongin 446701, South Korea. [Park, B. -G.; Lee, C. -U.; Kim, D. -J.] Korea Astron & Space Sci Inst, Daejon 305348, South Korea. [Dominik, M.; Jaimes, R. Figuera] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Andersen, M. I.] Univ Copenhagen, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. [Bramich, D. M.] Qatar Fdn, HBKU, QEERI, Doha, Qatar. [Burgdorf, M. J.] Univ Hamburg, Inst Meteorol, Bundesstr 55, D-20146 Hamburg, Germany. [Ciceri, S.; Mancini, L.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Evans, D. F.; Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Jaimes, R. Figuera] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Gu, S. -H.; Wang, Y. -B.] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China. [Kains, N.; Kerins, E.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. [Korhonen, H.] Finnish Ctr Astron ESO FINCA, Vaisalantie 20, FI-21500 Piikkio, Finland. [Rabus, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile. [Rahvar, S.] Sharif Univ Technol, Dept Phys, POB 11155-9161, Tehran, Iran. [Rasmussen, R. T.; von Essen, C.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Skottfelt, J.] Open Univ, Dept Phys Sci, Ctr Elect Imaging, Milton Keynes MK7 6AA, Bucks, England. [Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England. [Surdej, J.; Wertz, O.] Inst Astrophys & Geophys, Allee 6 Aout 17,Bat B5c, B-4000 Liege, Belgium. [Unda-Sanzana, E.] Univ Antofagasta, Fac Ciencias Basicas, Unidad Astronomia, Avda U Antofagasta, Antofagasta 02800, Chile. [Maoz, D.; Friedmann, M.; Kaspi, S.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. RP Bozza, V (reprint author), Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo II 132, I-84084 Fisciano, SA, Italy.; Bozza, V (reprint author), Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy. RI Korhonen, Heidi/E-3065-2016; Hundertmark, Markus/C-6190-2015; D'Ago, Giuseppe/N-8318-2016; Skowron, Jan/M-5186-2014; OI Tronsgaard, Rene/0000-0003-1001-0707; Korhonen, Heidi/0000-0003-0529-1161; Hundertmark, Markus/0000-0003-0961-5231; D'Ago, Giuseppe/0000-0001-9697-7331; Skowron, Jan/0000-0002-2335-1730; Dominik, Martin/0000-0002-3202-0343; Wang, Yi-Bo/0000-0002-5172-8558 FU National Science Centre, Poland [MAESTRO 2014/14/A/ST9/00121]; Creative Research Initiative Program of National Research Foundation of Korea [2009-0081561]; JPL grant [1500811]; NSF AST [1516842]; NASA through the Sagan Fellowship Program; JSPS [JSPS23103002, JSPS24253004, JSPS26247023]; [JSPS25103508]; [JSPS23340064] FX The OGLE Team thanks Profs. M. Kubiak and G. Pietrzynski, former members of the OGLE team, for their contribution to the collection of the OGLE photometric data over the past years. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U.; Work by C.H. was supported by Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea.; J.C.Y., A.G., and S.C.N. acknowledge support by JPL grant 1500811. Work by W.Z. and A.G. was supported by NSF AST 1516842.; Work by J.C.Y. was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute.; T.S. acknowledges the financial support from the JSPS, JSPS23103002, JSPS24253004, and JSPS26247023. The MOA project is supported by grants JSPS25103508 and JSPS23340064. NR 40 TC 5 Z9 5 U1 3 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 2016 VL 820 IS 1 AR 79 DI 10.3847/0004-637X/820/1/79 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH4WT UT WOS:000372787000078 ER PT J AU Dijkstra, M Sethi, S Loeb, A AF Dijkstra, Mark Sethi, Shiv Loeb, Abraham TI 3-cm FINE STRUCTURE MASERS: A UNIQUE SIGNATURE OF SUPERMASSIVE BLACK HOLE FORMATION VIA DIRECT COLLAPSE IN THE EARLY UNIVERSE SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; cosmology: observations; dark ages, reionization, first stars; masers; radiative transfer; radio lines: general ID RESONANCE-LINE RADIATION; EQUATION-OF-STATE; H-II REGIONS; ACTIVE GALACTIC NUCLEI; EXTREMELY OPAQUE MEDIA; ATOMIC COOLING HALOES; LY-ALPHA EMITTERS; HIGH-REDSHIFT; ASTROPHYSICAL MASERS; INTERGALACTIC MEDIUM AB The direct collapse black hole (DCBH) scenario describes the isothermal collapse of a pristine gas cloud directly into a massive, M-BH = 10(4) - 10(6) M-circle dot black hole. In this paper we show that large H I column densities of primordial gas at T similar to 10(4) K with low molecular abundance-which represent key aspects of the DCBH scenario-provide optimal conditions for the pumping of the 2p-level of atomic hydrogen by trapped Ly alpha photons. This Ly alpha pumping mechanism gives rise to an inverted level population of the 2s(1/2) - 2p(3/2) transition, and therefore also gives rise to stimulated fine structure emission at lambda = 3.04 cm (rest-frame). We show that simplified models of the DCBH scenario amplify the CMB by up to a factor of similar to 10(5), above which the maser saturates. Hyperfine splitting of the 3 cm transition gives rise to a characteristic broad (FWHM similar to tens of MHz in the observers frame) asymmetric line profile. This signal subtends an angular scale of similar to 1-10 mas, which translates to a flux of similar to 0.3-3 mu Jy, which is detectable with ultra-deep surveys being planned with SKA1-MID. While challenging, as the signal is visible for a fraction of the collapse time of the cloud, the matching required physical conditions imply that a detection of the redshifted 3-cm emission line could provide direct evidence for the DCBH scenario. C1 [Dijkstra, Mark] Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, NO-0315 Oslo, Norway. [Sethi, Shiv] Raman Res Inst, CV Raman Ave, Bangalore 560080, Karnataka, India. [Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA USA. RP Dijkstra, M (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, NO-0315 Oslo, Norway.; Sethi, S (reprint author), Raman Res Inst, CV Raman Ave, Bangalore 560080, Karnataka, India. EM mark.dijkstra@astro.uio.no; sethi@rri.res.in RI Sethi, Shiv/D-4893-2012 FU NSF [AST-1312034] FX M.D. thanks the Raman Research Institute for their hospitality during a visit that initiated this project. The authors thank Jonathan Pritchard, Max Gronke, Lluis Mas-Ribas for useful discussions, and Jens Chluba for helpful correspondence. This work was supported in part by NSF-grant AST-1312034 (for A.L.). NR 81 TC 3 Z9 3 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 20 PY 2016 VL 820 IS 1 AR 10 DI 10.3847/0004-637X/820/1/10 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH4WT UT WOS:000372787000010 ER PT J AU Ganot, N Gal-Yam, A Ofek, EO Sagiv, I Waxman, E Lapid, O Kulkarni, SR Ben-Ami, S Kasliwal, MM Chelouche, D Rafter, S Behar, E Laor, A Poznanski, D Nakar, E Maoz, D Trakhtenbrot, B Neill, JD Barlow, TA Martin, CD Gezari, S Arcavi, I Bloom, JS Nugent, PE Sullivan, M AF Ganot, Noam Gal-Yam, Avishay Ofek, Eran. O. Sagiv, Ilan Waxman, Eli Lapid, Ofer Kulkarni, Shrinivas R. Ben-Ami, Sagi Kasliwal, Mansi M. Chelouche, Doron Rafter, Stephen Behar, Ehud Laor, Ari Poznanski, Dovi Nakar, Ehud Maoz, Dan Trakhtenbrot, Benny Neill, James D. Barlow, Thomas A. Martin, Christofer D. Gezari, Suvi Arcavi, Iair Bloom, Joshua S. Nugent, Peter E. Sullivan, Mark CA ULTRASAT Sci Team WTTH Consortium GALEX Sci Team Palomar Transient Factory TI THE DETECTION RATE OF EARLY UV EMISSION FROM SUPERNOVAE: A DEDICATED GALEX/PTF SURVEY AND CALIBRATED THEORETICAL ESTIMATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general ID CORE-COLLAPSE SUPERNOVAE; GAMMA-RAY BURSTS; II-P SUPERNOVAE; DENSE MASS-LOSS; SHOCK-BREAKOUT; LIGHT-CURVES; LUMINOUS SUPERNOVAE; FOLLOW-UP; STELLAR ENVELOPES; RED SUPERGIANT AB The radius and surface composition of an exploding massive star, as well as the explosion energy per unit mass, can be measured using early UV observations of core-collapse supernovae (SNe). We present the first results from a simultaneous GALEX/PTF search for early ultraviolet (UV) emission from SNe. Six SNe II and one Type II superluminous SN (SLSN-II) are clearly detected in the GALEX near-UV (NUV) data. We compare our detection rate with theoretical estimates based on early, shock-cooling UV light curves calculated from models that fit existing Swift and GALEX observations well, combined with volumetric SN rates. We find that our observations are in good agreement with calculated rates assuming that red supergiants (RSGs) explode with fiducial radii of 500 R-circle dot, explosion energies of 10(51) erg, and ejecta masses of 10M(circle dot). Exploding blue supergiants and Wolf-Rayet stars are poorly constrained. We describe how such observations can be used to derive the progenitor radius, surface composition, and explosion energy per unit mass of such SN events, and we demonstrate why UV observations are critical for such measurements. We use the fiducial RSG parameters to estimate the detection rate of SNe during the shock-cooling phase (<1 day after explosion) for several ground-based surveys (PTF, ZTF, and LSST). We show that the proposed wide-field UV explorer ULTRASAT mission is expected to find >85 SNe per year (similar to 0.5 SN per deg(2)), independent of host galaxy extinction, down to an NUV detection limit of 21.5 mag AB. Our pilot GALEX/PTF project thus convincingly demonstrates that a dedicated, systematic SN survey at the NUV band is a compelling method to study how massive stars end their life. C1 [Ganot, Noam; Gal-Yam, Avishay; Ofek, Eran. O.; Sagiv, Ilan; Waxman, Eli; Lapid, Ofer] Weizmann Inst Sci, Fac Phys, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Kulkarni, Shrinivas R.; Kasliwal, Mansi M.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Ben-Ami, Sagi] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Chelouche, Doron; Rafter, Stephen] Univ Haifa, Dept Phys, Fac Nat Sci, IL-31905 Haifa, Israel. [Behar, Ehud; Laor, Ari] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Poznanski, Dovi; Nakar, Ehud; Maoz, Dan] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Trakhtenbrot, Benny] ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [Neill, James D.; Barlow, Thomas A.; Martin, Christofer D.] CALTECH, 1200 East Calif Blvd,MC 278-17, Pasadena, CA 91125 USA. [Gezari, Suvi] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Arcavi, Iair] Las Cumbres Observ Global Telescope, 6740 Cortona Dr,Suite 102, Goleta, CA 93111 USA. [Bloom, Joshua S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Sullivan, Mark] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Arcavi, Iair] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. RP Ganot, N (reprint author), Weizmann Inst Sci, Fac Phys, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. EM noam.ganot@gmail.com OI Sullivan, Mark/0000-0001-9053-4820; Trakhtenbrot, Benny/0000-0002-3683-7297 FU Israeli Space Agency (ISA); Ministry of Science, Technology and Space (MOS); EU via ERC grant [307260]; ISF; Kimmel award FX This research was supported by grants from the Israeli Space Agency (ISA) and the Ministry of Science, Technology and Space (MOS). Additional funding was provided by the EU via ERC grant 307260, the ISF, and a Kimmel award. NR 69 TC 1 Z9 1 U1 2 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 2016 VL 820 IS 1 AR 57 DI 10.3847/0004-637X/820/1/57 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH4WT UT WOS:000372787000056 ER PT J AU Garnavich, PM Tucker, BE Rest, A Shaya, EJ Olling, RP Kasen, D Villar, A AF Garnavich, P. M. Tucker, B. E. Rest, A. Shaya, E. J. Olling, R. P. Kasen, D. Villar, A. TI SHOCK BREAKOUT AND EARLY LIGHT CURVES OF TYPE II-P SUPERNOVAE OBSERVED WITH KEPLER SO ASTROPHYSICAL JOURNAL LA English DT Article DE shock waves; stars: mass-loss; supernovae: general; supernovae: individual (KSN2011a, KSN2011d, SN1999ig) ID CORE-COLLAPSE SUPERNOVAE; RED SUPERGIANTS; PROGENITOR; EMISSION; WIND AB We discovered two transient events in the Kepler field with light curves that strongly suggest they are type. II-P supernovae (SNe II-P). Using the fast cadence of the Kepler observations we precisely estimate the rise time to maximum for KSN2011a and KSN2011d as 10.5 +/- 0.4 and 13.3 +/- 0.4 rest-frame days, respectively. Based on fits to idealized analytic models, we find the progenitor radius of KSN2011a (280 +/- 20 R-circle dot) to be significantly smaller than that for KSN2011d (490 +/- 20 R-circle dot), but both have similar explosion energies of 2.0 +/- 0.3 x 10(51) erg. The rising light curve of KSN2011d is an excellent match to that predicted by simple models of exploding red supergiants (RSG). However, the early rise of KSN2011a is faster than the models predict, possibly due to the supernova shock wave moving into pre-existing wind or mass-loss from the RSG. A mass-loss rate of 10(-4)M(circle dot) yr(-1) from the RSG can explain the fast rise without impacting the optical flux at maximum light or the shape of the post-maximum light curve. No shock breakout emission is seen in KSN2011a, but this is likely due to the circumstellar interaction suspected in the fast rising light curve. The early light curve of KSN2011d does show excess emission consistent with model predictions of a shock breakout. This is the first optical detection of a shock breakout from a SNe II-P. C1 [Garnavich, P. M.] Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. [Tucker, B. E.] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Via Cotter Rd, Weston, ACT 2611, Australia. [Tucker, B. E.; Kasen, D.] Univ Calif Berkeley, Dept Phys & Astron, Berkeley, CA 94720 USA. [Rest, A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Shaya, E. J.; Olling, R. P.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Kasen, D.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Villar, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Garnavich, PM (reprint author), Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. FU Kepler grants [NNX12AC89G, NNX11AG95G]; DOE office of nuclear physics early career award FX This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work was partly supported by Kepler grants NNX12AC89G and NNX11AG95G. D.K. is supported by a DOE office of nuclear physics early career award. NR 26 TC 9 Z9 9 U1 3 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 20 PY 2016 VL 820 IS 1 AR 23 DI 10.3847/0004-637X/820/1/23 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH4WT UT WOS:000372787000023 ER PT J AU Houde, M Hull, CLH Plambeck, RL Vaillancourt, JE Hildebrand, RH AF Houde, Martin Hull, Charles L. H. Plambeck, Richard L. Vaillancourt, John E. Hildebrand, Roger H. TI DISPERSION OF MAGNETIC FIELDS IN MOLECULAR CLOUDS. IV. ANALYSIS OF INTERFEROMETRY DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: magnetic fields; polarization; turbulence ID AMBIPOLAR DIFFUSION SCALE; ION SPECTRA; POLARIZATION; POLARIMETRY; TURBULENCE; REGIONS; DUST; CORE; M51 AB We expand on the dispersion analysis of polarimetry maps toward applications to interferometry data. We show how the filtering of low spatial frequencies can be accounted for within the idealized Gaussian turbulence model, initially introduced for single-dish data analysis, to recover reliable estimates for correlation lengths of magnetized turbulence, as well as magnetic field strengths (plane-of-the-sky component) using the Davis-Chandrasekhar-Fermi method. We apply our updated technique to TADPOL/CARMA data obtained on W3(OH), W3 Main, and DR21(OH). For W3(OH), our analysis yields a turbulence correlation length delta similar or equal to 19 mpc, a ratio of turbulent-to-total magnetic energy < B-t(2)> / < B-2 > similar or equal to 0.58 and a magnetic field strength B-0 similar to 1.1 mG; for W3 Main delta similar or equal to 22 mpc, < B-t(2)> / < B-2 > similar or equal to 0.74 and B similar to 0.7 mG; while for DR21(OH) delta similar or equal to 12 mpc, < B-t(2)> / < B-2 > similar or equal to 0.70 and B-0 similar or equal to 1.2 mG. C1 [Houde, Martin] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Houde, Martin] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Hull, Charles L. H.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Plambeck, Richard L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Plambeck, Richard L.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Vaillancourt, John E.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hildebrand, Roger H.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Hildebrand, Roger H.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Hildebrand, Roger H.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. RP Houde, M (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.; Houde, M (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. FU NSERC Discovery Grant; Canada Research Chair; Canada Foundation for Innovation; Ontario Innovation Trust; Western's Academic Development Fund programs; National Science Foundation; CARMA partner universities FX M.H.'s research is funded through the NSERC Discovery Grant, Canada Research Chair, Canada Foundation for Innovation, Ontario Innovation Trust, and Western's Academic Development Fund programs. CARMA development and operations were funded by the National Science Foundation and the CARMA partner universities. NR 36 TC 4 Z9 4 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 2016 VL 820 IS 1 AR 38 DI 10.3847/0004-637X/820/1/38 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH4WT UT WOS:000372787000038 ER PT J AU LaMassa, SM Ricarte, A Glikman, E Urry, CM Stern, D Yaqoob, T Lansbury, GB Civano, F Boggs, SE Brandt, WN Chen, CTJ Christensen, FE Craig, WW Hailey, CJ Harrison, F Hickox, RC Koss, M Ricci, C Treister, E Zhang, W AF LaMassa, Stephanie M. Ricarte, Angelo Glikman, Eilat Urry, C. Megan Stern, Daniel Yaqoob, Tahir Lansbury, George B. Civano, Francesca Boggs, Steve E. Brandt, W. N. Chen, Chien-Ting J. Christensen, Finn E. Craig, William W. Hailey, Chuck J. Harrison, Fiona Hickox, Ryan C. Koss, Michael Ricci, Claudio Treister, Ezequiel Zhang, Will TI PEERING THROUGH THE DUST: NuSTAR OBSERVATIONS OF TWO FIRST-2MASS RED QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; infrared: galaxies; quasars: individual (F2M 0380+3759, F2M 1227+3214); X-rays: individual (F2M 0830+3759, F2M 1227+3214) ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; XMM-NEWTON OBSERVATIONS; DIGITAL SKY SURVEY; RAY SPECTRAL MODEL; WIDE-FIELD SURVEY; X-RAY; REDDENED QUASARS; COSMOS FIELD; SEYFERT-GALAXIES AB Some reddened quasars appear to be transitional objects in the paradigm of merger-induced black hole growth/galaxy evolution, where a heavily obscured nucleus starts to be unveiled by powerful quasar winds evacuating the surrounding cocoon of dust and gas. Hard X-ray observations are able to peer through this gas and dust, revealing the properties of circumnuclear obscuration. Here, we present NuSTAR and XMM-Newton/Chandra observations of FIRST-2MASS-selected red quasars F2M 0830+3759 and F2M 1227+3214. We find that though F2M 0830 +3759 is moderately obscured (N-H,(Z) = (2.1 +/- 0.2) x 10(22) cm(-2)) and F2M 1227+3214 is mildly absorbed (N-H,(Z) = 3.4(- 0.7)(+0.8) x 10(21) cm(-2)) along the line of sight, heavier global obscuration may be present in both sources, with N-H,(S) = 3.7(- 2.6)(+4.1) x 10(23) cm(-2) and <5.5 x 10(23) cm(-2) for F2M 0830+3759 and F2M 1227+3214, respectively. F2M 0830+3759 also has an excess of soft X-ray emission below 1 keV, which is well accommodated by a model where 7% of the intrinsic X-ray emission from the active galactic nucleus (AGN) is scattered into the line of sight. While F2M 1227+3214 has a dust-to-gas ratio (E(B - V)/N-H) consistent with the Galactic value, the value of E(B - V)/N-H for F2M 0830+3759 is lower than the Galactic standard, consistent with the paradigm that the dust resides on galactic scales while the X-ray reprocessing gas originates within the dust sublimation zone of the broad-line region. The X-ray and 6.1 mu m luminosities of these red quasars are consistent with the empirical relations derived for high-luminosity, unobscured quasars, extending the parameter space of obscured AGNs previously observed by NuSTAR to higher luminosities. C1 [LaMassa, Stephanie M.; Urry, C. Megan; Civano, Francesca] Yale Ctr Astron & Astrophys, Dept Phys, POB 208120, New Haven, CT 06520 USA. [LaMassa, Stephanie M.; Urry, C. Megan; Civano, Francesca] Yale Univ, Dept Phys, POB 208121, New Haven, CT 06520 USA. [LaMassa, Stephanie M.; Zhang, Will] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ricarte, Angelo] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Glikman, Eilat] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-221, Pasadena, CA 91109 USA. [Yaqoob, Tahir] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. [Lansbury, George B.] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England. [Civano, Francesca; Hickox, Ryan C.] Dartmouth Coll, Dept Phys & Astron, 6127 Wilder Lab, Hanover, NH 03755 USA. [Civano, Francesca] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Boggs, Steve E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brandt, W. N.; Chen, Chien-Ting J.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Brandt, W. N.; Chen, Chien-Ting J.] Penn State Univ, Inst Gravitat & Cosmos, 525 Davey Lab, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, 525 Davey Lab, University Pk, PA 16802 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, Chuck J.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. [Harrison, Fiona] CALTECH, Cahill Ctr Astron & Astrophys, 1216 E Calif Blvd, Pasadena, CA 91125 USA. [Koss, Michael] ETH, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [Ricci, Claudio] Pontificia Univ Catolica Chile, Inst Astrofis, Vicuna Mackenna 4860, Santiago 7820436, Chile. [Treister, Ezequiel] Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion, Chile. RP LaMassa, SM (reprint author), Yale Ctr Astron & Astrophys, Dept Phys, POB 208120, New Haven, CT 06520 USA. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Urry, Meg/0000-0002-0745-9792 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; Gruber Science Fellowship; Cottrell College Award through the Research Corporation for Science Advancement; Caltech NuSTAR subcontract [44A-1092750]; NASA ADP grant [NNX10AC99G]; NASA through ADAP award [NNX12AE38G]; National Science Foundation [1211096, 1515364]; Sloan Research Fellowship; Dartmouth Class of Faculty Fellowship; CONICYT-Chile grants ["EMBIGGEN" Anillo ACT1101, FONDECYT 1141218, Basal-CATA PFB-06/2007] FX We thank the referee for a careful reading of this manuscript and helpful comments. 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). AR is supported by the Gruber Science Fellowship. EG acknowledges the generous support of the Cottrell College Award through the Research Corporation for Science Advancement. WNB acknowledges support from Caltech NuSTAR subcontract 44A-1092750 and NASA ADP grant NNX10AC99G. RCH acknowledges support from NASA through ADAP award NNX12AE38G, the National Science Foundation through grant nos. 1211096 and 1515364, a Sloan Research Fellowship, and a Dartmouth Class of 1962 Faculty Fellowship. CR acknowledges financial support from the CONICYT-Chile grants "EMBIGGEN" Anillo ACT1101, FONDECYT 1141218, Basal-CATA PFB-06/2007. NR 108 TC 3 Z9 3 U1 2 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 20 PY 2016 VL 820 IS 1 AR 70 DI 10.3847/0004-637X/820/1/70 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH4WT UT WOS:000372787000069 ER PT J AU Neben, AR Hewitt, JN Bradley, RF Dillon, JS Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Corey, BE Deshpande, AA Goeke, R Greenhill, LJ Hazelton, BJ Johnston-Hollitt, M Kaplan, DL Lonsdale, CJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Prabu, T Shankar, NU Srivani, KS Subrahmanyan, R Tingay, SJ Wayth, RB Webster, RL Williams, A Williams, CL AF Neben, Abraham R. Hewitt, Jacqueline N. Bradley, Richard F. Dillon, Joshua S. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Corey, B. E. Deshpande, A. A. Goeke, R. Greenhill, L. J. Hazelton, B. J. Johnston-Hollitt, M. Kaplan, D. L. Lonsdale, C. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Prabu, T. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Tingay, S. J. Wayth, R. B. Webster, R. L. Williams, A. Williams, C. L. TI BEAM-FORMING ERRORS IN MURCHISON WIDEFIELD ARRAY PHASED ARRAY ANTENNAS AND THEIR EFFECTS ON EPOCH OF REIONIZATION SCIENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dark ages, reionization, first stars; instrumentation: interferometers; methods: statistical; techniques: interferometric ID 21 CM EPOCH; POWER SPECTRUM MEASUREMENTS; LOW-FREQUENCY ARRAY; DYNAMIC-RANGE; FIELD; PRECISION; CALIBRATION; COSMOLOGY; DEMONSTRATOR; SENSITIVITY AB Accurate antenna beam models are critical for radio observations aiming to isolate the redshifted 21 cm spectral line emission from the Dark Ages and the Epoch of Reionization (EOR) and unlock the scientific potential of 21 cm cosmology. Past work has focused on characterizing mean antenna beam models using either satellite signals or astronomical sources as calibrators, but antenna-to-antenna variation due to imperfect instrumentation has remained unexplored. We characterize this variation for the Murchison Widefield Array (MWA) through laboratory measurements and simulations, finding typical deviations of the order of +/- 10%-20% near the edges of the main lobe and in the sidelobes. We consider the ramifications of these results for image-and power spectrum-based science. In particular, we simulate visibilities measured by a 100 m baseline and find that using an otherwise perfect foreground model, unmodeled beam-forming errors severely limit foreground subtraction accuracy within the region of Fourier space contaminated by foreground emission (the "wedge"). This region likely contains much of the cosmological signal, and accessing it will require measurement of per-antenna beam patterns. However, unmodeled beam-forming errors do not contaminate the Fourier space region expected to be free of foreground contamination (the "EOR window"), showing that foreground avoidance remains a viable strategy. C1 [Neben, Abraham R.; Hewitt, Jacqueline N.; Dillon, Joshua S.; Goeke, R.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Bradley, Richard F.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. [Bradley, Richard F.] Natl Radio Astron Obs, Charlottesville, VA USA. [Dillon, Joshua S.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Dillon, Joshua S.] Berkeley Ctr Cosmol Phys, Berkeley, CA USA. [Bernardi, G.] SKA SA, ZA-7405 Cape Town, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, R. J.; Corey, B. E.; Lonsdale, C. J.; McWhirter, S. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [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. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Mitchell, D. A.] CSIRO Astron & Space Sci CASS, POB 76, Epping, NSW 1710, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Ord, S. M.; Tingay, S. J.; Wayth, R. B.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Mitchell, D. A.; Ord, S. M.; Wayth, R. B.; Webster, R. L.; Williams, A.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. RP Neben, AR (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RI Wayth, Randall/B-2444-2013; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Subrahmanyan, Ravi/D-4889-2012 OI Wayth, Randall/0000-0002-6995-4131; FU NSF [AST-0821321]; Marble Astrophysics Fund; MIT School of Science; U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF grant) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; 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); Australian Federal government via the Commonwealth Scientific and Industrial Research Organisation (CSIRO); Australian Federal government via National Collaborative Research Infrastructure Strategy; Australian Federal government via Education Investment Fund; Australian Federal government via Australia India Strategic Research Fund; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University; University of Western Australia - Western Australian State government FX This work was supported by NSF grant AST-0821321, the Marble Astrophysics Fund, and the MIT School of Science. We thank Aaron Ewall-Wice and Hamdi Mani for assistance in running these experiments, Steve Burns for debugging beam-former issues, and Danny Jacobs, Nithyanandan Thyagarajan, and Lu Feng for helpful discussions.; 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 U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant 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 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 Commonwealth Scientific and Industrial Research Organisation (CSIRO), 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 62 TC 4 Z9 4 U1 8 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 MAR 20 PY 2016 VL 820 IS 1 AR 44 DI 10.3847/0004-637X/820/1/44 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH4WT UT WOS:000372787000043 ER PT J AU Parrent, JT Milisavljevic, D Soderberg, AM Parthasarathy, M AF Parrent, J. T. Milisavljevic, D. Soderberg, A. M. Parthasarathy, M. TI LINE IDENTIFICATIONS OF TYPE I SUPERNOVAE: ON THE DETECTION OF Si II FOR THESE HYDROGEN-POOR EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general ID CORE-COLLAPSE SUPERNOVA; GAMMA-RAY BURST; LIGHT CURVES; SUPERLUMINOUS SUPERNOVAE; OPTICAL-SPECTRA; MAXIMUM-LIGHT; SN 2011FE; RADIATIVE-TRANSFER; H-ALPHA; EMISSION AB Here we revisit line identifications of type I supernovae (SNe I) and highlight trace amounts of unburned hydrogen as an important free parameter for the composition of the progenitor. Most one-dimensional stripped-envelope models of supernovae indicate that observed features near 6000-6400 angstrom in type. I spectra are due to more than Si II lambda 6355. However, while an interpretation of conspicuous Si II lambda 6355 can approximate 6150 angstrom absorption features for all SNe Ia during the first month of free expansion, similar identifications applied to 6250 angstrom features of SNe Ib and Ic have not been as successful. When the corresponding synthetic spectra are compared with high-quality timeseries observations, the computed spectra are frequently too blue in wavelength. Some improvement can be achieved with Fe II lines that contribute redward of 6150 angstrom; however, the computed spectra either remain too blue or the spectrum only reaches a fair agreement when the rise-time to peak brightness of the model conflicts with observations by a factor of two. This degree of disagreement brings into question the proposed explosion scenario. Similarly, a detection of strong Si II lambda 6355 in the spectra of broadlined Ic and super-luminous events of type I/R is less convincing despite numerous model spectra used to show otherwise. Alternatively, we suggest 6000-6400 angstrom features are possibly influenced by either trace amounts of hydrogen or blueshifted absorption and emission in H alpha, the latter being an effect which is frequently observed in the spectra of hydrogen-rich, SNe II. C1 [Parrent, J. T.; Milisavljevic, D.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Parthasarathy, M.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. RP Parrent, JT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Parrent, Jerod/0000-0002-5103-7706 FU Scientific Schools of Russia [3458.2010.2]; RFBR [10-02-00249] FX This work was made possible by contributions to the Supernova Spectrum Archive (Richardson et al. 2001) and the Weizmann Interactive Supernova data REPository (WISeREP Yaron & Gal-Yam 2012), as well as David Bishop's Latest Supernovae page (Gal-Yam et al. 2013). This work has also made use of the Sternberg Astronomical Institute Supernova Light Curve Catalog, which is supported by grants of "Scientific Schools of Russia (3458.2010.2)," RFBR (10-02-00249). NR 124 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 MAR 20 PY 2016 VL 820 IS 1 AR 75 DI 10.3847/0004-637X/820/1/75 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH4WT UT WOS:000372787000074 ER PT J AU Rubin, A Gal-Yam, A De Cia, A Horesh, A Khazov, D Ofek, EO Kulkarni, SR Arcavi, I Manulis, I Yaron, O Vreeswijk, P Kasliwal, MM Ben-Ami, S Perley, DA Cao, Y Cenko, SB Rebbapragada, UD Wozniak, PR Filippenko, AV Clubb, KI Nugent, PE Pan, YC Badenes, C Howell, DA Valenti, S Sand, D Sollerman, J Johansson, J Leonard, DC Horst, JC Armen, SF Fedrow, JM Quimby, RM Mazzali, P Pian, E Sternberg, A Matheson, T Sullivan, M Maguire, K Lazarevic, S AF Rubin, Adam Gal-Yam, Avishay De Cia, Annalisa Horesh, Assaf Khazov, Danny Ofek, Eran O. Kulkarni, S. R. Arcavi, Iair Manulis, Ilan Yaron, Ofer Vreeswijk, Paul Kasliwal, Mansi M. Ben-Ami, Sagi Perley, Daniel A. Cao, Yi Cenko, S. Bradley Rebbapragada, Umaa D. Wozniak, P. R. Filippenko, Alexei V. Clubb, K. I. Nugent, Peter E. Pan, Y-C. Badenes, C. Howell, D. Andrew Valenti, Stefano Sand, David Sollerman, J. Johansson, Joel Leonard, Douglas C. Horst, J. Chuck Armen, Stephen F. Fedrow, Joseph M. Quimby, Robert M. Mazzali, Paulo Pian, Elena Sternberg, Assaf Matheson, Thomas Sullivan, M. Maguire, K. Lazarevic, Sanja TI TYPE II SUPERNOVA ENERGETICS AND COMPARISON OF LIGHT CURVES TO SHOCK-COOLING MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general ID P SUPERNOVAE; LUMINOUS SUPERNOVAE; CORE-COLLAPSE; PHOTOSPHERIC PHASE; LOW-RESOLUTION; IA SUPERNOVAE; RISE-TIME; FOLLOW-UP; MASS-LOSS; BREAKOUT AB During the first few days after explosion, Type II supernovae (SNe) are dominated by relatively simple physics. Theoretical predictions regarding early-time SN light curves in the ultraviolet (UV) and optical bands are thus quite robust. We present, for the first time, a sample of 57 R-band SN II light curves that are well-monitored during their rise, with > 5 detections during the first 10 days after discovery, and a well-constrained time of explosion to within 1-3 days. We show that the energy per unit mass (E/M) can be deduced to roughly a factor of five by comparing early-time optical data to the 2011 model of Rabinak & Waxman, while the progenitor radius cannot be determined based on R-band data alone. We find that SN II explosion energies span a range of E/M = (0.2-20) x 10(51) erg/(10 M-circle dot), and have a mean energy per unit mass of < E/M > = 0.85 x 10(51) erg/(10 M-circle dot), corrected for Malmquist bias. Assuming a small spread in progenitor masses, this indicates a large intrinsic diversity in explosion energy. Moreover, E/M is positively correlated with the amount of Ni-56 produced in the explosion, as predicted by some recent models of core-collapse SNe. We further present several empirical correlations. The peak magnitude is correlated with the decline rate (Delta m(15)), the decline rate is weakly correlated with the rise time, and the rise time is not significantly correlated with the peak magnitude. Faster declining SNe are more luminous and have longer rise times. This limits the possible power sources for such events. C1 [Rubin, Adam; Gal-Yam, Avishay; De Cia, Annalisa; Horesh, Assaf; Khazov, Danny; Ofek, Eran O.; Manulis, Ilan; Yaron, Ofer; Vreeswijk, Paul] Weizmann Inst Sci, Dept Particle Phys & Astrophys, 234 Herzl St, Rehovot, Israel. [Kulkarni, S. R.; Perley, Daniel A.; Cao, Yi] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Kulkarni, S. R.] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. [Arcavi, Iair; Howell, D. Andrew; Valenti, Stefano] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA. [Arcavi, Iair] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Kasliwal, Mansi M.] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA. Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Perley, Daniel A.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA. [Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Rebbapragada, Umaa D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Wozniak, P. R.] Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA. [Filippenko, Alexei V.; Clubb, K. I.; Nugent, Peter E.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Pan, Y-C.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Badenes, C.] Univ Pittsburgh, Dept Phys & Astron, 3941 OHara St, Pittsburgh, PA 15260 USA. [Badenes, C.] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, 3941 OHara St, Pittsburgh, PA 15260 USA. [Howell, D. Andrew] Univ Calif Santa Barbara, Dept Phys, Broida Hall,Mail Code 9530, Santa Barbara, CA 93106 USA. [Sand, David] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Sollerman, J.] Stockholm Univ, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [Johansson, Joel] Stockholm Univ, Oskar Klein Ctr, Dept Phys, SE-10691 Stockholm, Sweden. [Leonard, Douglas C.; Horst, J. Chuck; Armen, Stephen F.; Fedrow, Joseph M.; Quimby, Robert M.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Fedrow, Joseph M.] Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 6068502, Japan. [Quimby, Robert M.] Univ Tokyo, UTIAS, Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan. [Mazzali, Paulo] Liverpool John Moores Univ, IC2, Astrophys Res Inst, Liverpool Sci Pk,146 Browlow Hill, Liverpool L3 5RF, Merseyside, England. [Mazzali, Paulo; Sternberg, Assaf] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. [Pian, Elena] Inst Space Astrophys & Cosm Phys, INAF, Via P Gobetti 101, I-40129 Bologna, Italy. [Pian, Elena] Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy. [Sternberg, Assaf] Tech Univ Munich, Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Matheson, Thomas] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. [Sullivan, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Maguire, K.] ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Lazarevic, Sanja] Univ Belgrade, Fac Math, Dept Astron, Belgrade, Serbia. RP Rubin, A (reprint author), Weizmann Inst Sci, Dept Particle Phys & Astrophys, 234 Herzl St, Rehovot, Israel. EM adam.rubin@weizmann.ac.il RI Horesh, Assaf/O-9873-2016; OI Horesh, Assaf/0000-0002-5936-1156; Sollerman, Jesper/0000-0003-1546-6615; Wozniak, Przemyslaw/0000-0002-9919-3310; Sullivan, Mark/0000-0001-9053-4820 FU EU/FP7 via ERC [307260]; Quantum universe I-CORE Program by the Israeli Committee for Planning and Budgeting; Israel Science Foundation (ISF); Minerva grant; ISF grant; Weizmann-UK "making connections" program; Kimmel award; ARCHES award; Willner Family Leadership Institute Ilan Gluzman (Secaucus, NJ); Weizmann-UK; I-CORE Program of the Planning and Budgeting Committee; EU/FP7-ERC [615929]; NSF [AST-1009571, AST-1210311, AST-1211916]; Christopher R. Redlich Fund; TABASGO Foundation; W.M. Keck Foundation; Robert Martin Ayers Sciences Fund; US Department of Energy, Laboratory Directed Research and Development program; ISF; Royal Society; US Government; Minerva; European Community FX A.G.Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum universe I-CORE Program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF); by Minerva and ISF grants; by the Weizmann-UK "making connections" program; and by Kimmel and ARCHES awards. E.O.O. is the incumbent of the Arye Dissentshik career development chair and is grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus, NJ), ISF, Minerva, Weizmann-UK, and the I-CORE Program of the Planning and Budgeting Committee and the ISF. M. S. acknowledges support from the Royal Society and EU/FP7-ERC grant No. [615929]. K. M. is grateful for a Marie Curie Intra-European Fellowship, within the 7th European Community Framework Programme (FP7). D.C.L., S.F.A., J.C.H., and J.M.F. are supported by NSF grants AST-1009571 and AST-1210311, under which part of this research (photometry data collected at MLO) was carried out. The supernova research of A.V.F.'s group at U.C. Berkeley presented herein is supported by Gary & Cynthia Bengier, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916.; Research at Lick Observatory is partially supported by a generous gift from Google. 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 observatory was made possible by the generous financial support of the W.M. Keck Foundation. 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 de Canarias. This research has made use of the APASS database, located at the AAVSO web site. Funding for APASS has been provided by the Robert Martin Ayers Sciences Fund. A portion of this work was carried out at the Jet Propulsion Laboratory under a Research and Technology Development Grant, under contract with the National Aeronautics and Space Administration. US Government Support is acknowledged. LANL participation in iPTF is supported by the US Department of Energy as part of the Laboratory Directed Research and Development program. NR 75 TC 8 Z9 8 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 MAR 20 PY 2016 VL 820 IS 1 AR 33 DI 10.3847/0004-637X/820/1/33 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DH4WT UT WOS:000372787000033 ER PT J AU do Nascimento, JD Vidotto, AA Petit, P Folsom, C Castro, M Marsden, SC Morin, J de Mello, GFP Meibom, S Jeffers, SV Guinan, E Ribas, I AF do Nascimento, J. -D., Jr. Vidotto, A. A. Petit, P. Folsom, C. Castro, M. Marsden, S. C. Morin, J. Porto de Mello, G. F. Meibom, S. Jeffers, S. V. Guinan, E. Ribas, I. TI MAGNETIC FIELD AND WIND OF KAPPA CETI: TOWARD THE PLANETARY HABITABILITY OF THE YOUNG SUN WHEN LIFE AROSE ON EARTH SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: individual (HD 20630, HIP 15457); stars: magnetic field; stars: winds, outflows ID SOLAR-TYPE STARS; ACTIVE STARS; TIME; EVOLUTION; ZONES; EXOPLANETS; GEODYNAMO; DEPLETION; EMISSION; MISSION AB We report magnetic field measurements for kappa(1) Cet, a proxy of the young Sun when life arose on Earth. We carry out an analysis of the magnetic properties determined from spectropolarimetric observations and reconstruct the large-scale surface magnetic field to derive the magnetic environment, stellar winds, and particle flux permeating the interplanetary medium around kappa(1) Cet. Our results show a closer magnetosphere and mass-loss rate of M = 9.7 x 10(-13) M-circle dot yr(-1), i.e., a factor of 50 times larger than the current solar wind mass-loss rate, resulting in a larger interaction via space weather disturbances between the stellar wind and a hypothetical young-Earth analogue, potentially affecting the planet's habitability. Interaction of the wind from the young Sun with the planetary ancient magnetic field may have affected the young Earth and its life conditions. C1 [do Nascimento, J. -D., Jr.; Meibom, S.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [do Nascimento, J. -D., Jr.; Castro, M.] Univ Fed Rio G Norte, UFRN, Dept Fis, CP 1641, BR-59072970 Natal, RN, Brazil. [Vidotto, A. A.] Observ Geneva, 51 Ch Maillettes, CH-1290 Chavannes Des Bois, Switzerland. [Petit, P.] Univ Toulouse, UPS OMP, Inst R Astrop & Planetol, Toulouse, France. [Petit, P.] CNRS, IRAP, 14 Ave E Belin, F-31400 Toulouse, France. [Folsom, C.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Marsden, S. C.] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. [Morin, J.] Univ Montpellier, LUPM UMR5299, F-34095 Montpellier, France. [Porto de Mello, G. F.] Univ Fed Rio de Janeiro, Obs Valongo, L do Pedro Antonio 43, BR-20080090 Rio de Janeiro, RJ, Brazil. [Jeffers, S. V.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Guinan, E.] Villanova Univ, Dept Astron, Villanova, PA 19085 USA. [Ribas, I.] Inst Ciencies Espai CSIC IEEC, Carrer Can Magrans S-N,Campus UAB, E-08193 Barcelona, Spain. [Vidotto, A. A.] Univ Dublin Trinity Coll, Sch Phys, Dublin 2, Ireland. RP do Nascimento, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jdonascimento@cfa.harvard.edu OI Petit, Pascal/0000-0001-7624-9222; Morin, Julien/0000-0002-4996-6901; Vidotto, Aline/0000-0001-5371-2675 FU CNPq PQ grant; Swiss National Supercomputing Centre [s516]; DiRAC (National E-Infrastructure) Data Analytic system at the University of Cambridge, on behalf of the STFC DiRAC HPC Facility [ST/K001590/1]; STFC [ST/H008861/1, ST/H00887X/1]; STFC DiRAC Operations [ST/K00333X/1]; ANR [SIMI5-6 020 01 Toupies]; Spanish Ministry of Economy and Competitiveness (MINECO); Fondo Europeo de Desarrollo Regional (FEDER) [ESP2013-48391-C4-1-R, ESP2014-57495-C2-2-R] FX The authors wish to thank the TBL team. J.D.N. acknowledges CNPq PQ grant and A.A.V. acknowledges the support by the Swiss National Supercomputing Centre (ID s516) and DiRAC (National E-Infrastructure) Data Analytic system at the University of Cambridge, on behalf of the STFC DiRAC HPC Facility funded by ST/K001590/1, STFC (ST/H008861/1, ST/H00887X/1), and STFC DiRAC Operations (ST/K00333X/1). C.P.F was supported by the grant ANR 2011 Blanc SIMI5-6 020 01 Toupies. I.R. acknowledges support from the Spanish Ministry of Economy and Competitiveness (MINECO) and the Fondo Europeo de Desarrollo Regional (FEDER) through grants ESP2013-48391-C4-1-R and ESP2014-57495-C2-2-R. NR 48 TC 7 Z9 7 U1 3 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 MAR 20 PY 2016 VL 820 IS 1 AR L15 DI 10.3847/2041-8205/820/1/L15 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DG8RT UT WOS:000372352000015 ER EF