FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Mocz, P Vogelsberger, M Hernquist, L AF Mocz, Philip Vogelsberger, Mark Hernquist, Lars TI A constrained transport scheme for MHD on unstructured static and moving meshes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE MHD; methods: numerical ID MAGNETIC-FIELDS; ACCRETION DISKS; PARTICLE MAGNETOHYDRODYNAMICS; IDEAL MAGNETOHYDRODYNAMICS; INTERSTELLAR GAS; DYNAMICAL STATE; BLACK-HOLES; SIMULATIONS; TURBULENCE; EQUATIONS AB Magnetic fields play an important role in many astrophysical systems and a detailed understanding of their impact on the gas dynamics requires robust numerical simulations. Here we present a new method to evolve the ideal magnetohydrodynamic (MHD) equations on unstructured static and moving meshes that preserves the magnetic field divergence-free constraint to machine precision. The method overcomes the major problems of using a cleaning scheme on the magnetic fields instead, which is non-conservative, not fully Galilean invariant, does not eliminate divergence errors completely, and may produce incorrect jumps across shocks. Our new method is a generalization of the constrained transport (CT) algorithm used to enforce the del . B = 0 condition on fixed Cartesian grids. Preserving del. B = 0 at the discretized level is necessary to maintain the orthogonality between the Lorentz force and B. The possibility of performing CT on a moving mesh provides several advantages over static mesh methods due to the quasi-Lagrangian nature of the former (i.e. the mesh generating points move with the flow), such as making the simulation automatically adaptive and significantly reducing advection errors. Our method preserves magnetic fields and fluid quantities in pure advection exactly. C1 [Mocz, Philip; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vogelsberger, Mark] MIT, Kavli Inst Astrophys & Space Res, Dept Phys, Cambridge, MA 02139 USA. RP Mocz, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pmocz@cfa.harvard.edu OI Mocz, Philip/0000-0001-6631-2566 FU National Science Foundation [DGE-1144152]; NASA [NNX12AC67G]; NSF [AST-1312095] FX This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant no. DGE-1144152. LH acknowledges support from NASA grant NNX12AC67G and NSF award AST-1312095. PM would like to thank Paul Duffell for insightful discussions on the manuscript. NR 29 TC 13 Z9 13 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 JUL 21 PY 2014 VL 442 IS 1 BP 43 EP 55 DI 10.1093/mnras/stu865 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RW UT WOS:000338765400005 ER PT J AU Torrelles, JM Curiel, S Estalella, R Anglada, G Gomez, JF Canto, J Patel, NA Trinidad, MA Girart, JM Carrasco-Gonzalez, C Rodriguez, LF AF Torrelles, J. M. Curiel, S. Estalella, R. Anglada, G. Gomez, J. F. Canto, J. Patel, N. A. Trinidad, M. A. Girart, J. M. Carrasco-Gonzalez, C. Rodriguez, L. F. TI A very young, compact bipolar H2O maser outflow in the intermediate-mass star-forming LkH alpha 234 region SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE masers; stars: formation; ISM: individual objects: LkH alpha 234; ISM: jets and outflows ID LARGE PROPER MOTIONS; STELLAR OBJECTS; PROTOPLANETARY DISKS; CONTINUUM EMISSION; PROTOSTAR CEPHEUS; RADIO-CONTINUUM; MAIN-SEQUENCE; WATER MASERS; AFGL 2591; HH 80-81 AB We report multi-epoch Very Long Baseline Interferometry (VLBI) H2O maser observations towards the compact cluster of young stellar objects (YSOs) close to the Herbig Be star LkH alpha 234. This cluster includes LkH alpha 234 and at least nine more YSOs that are formed within projected distances of similar to 10 arcsec (similar to 9000 au). We detect H2O maser emission towards four of these YSOs. In particular, our VLBI observations (including proper motion measurements) reveal a remarkable very compact (similar to 0.2 arcsec = similar to 180 au), bipolar H2O maser outflow emerging from the embedded YSO Very Large Array (VLA) 2. We estimate a kinematic age of similar to 40 yr for this bipolar outflow, with expanding velocities of similar to 20 km s(-1) and momentum rate. MwVw similar or equal to 10(-4)-10(-3) M-circle dot yr(-1) km s(-1) x (Omega/4 pi), powered by a YSO of a few solar masses. We propose that the outflow is produced by recurrent episodic jet ejections associated with the formation of this YSO. Short-lived episodic ejection events have previously been found towards high-mass YSOs. We show now that this behaviour is also present in intermediatemass YSOs. These short-lived episodic ejections are probably related to episodic increases in the accretion rate, as observed in low-mass YSOs. We predict the presence of an accretion disc associated with VLA 2. If detected, this would represent one of the few known examples of intermediate-mass stars with a disc-YSO-jet system at scales of a few hundred astronomical units. C1 [Torrelles, J. M.] Inst Ciencies Espai CSIC IEEC, E-08028 Barcelona, Spain. [Torrelles, J. M.] Inst Ciencies Cosmos UB IEEC, E-08028 Barcelona, Spain. [Curiel, S.; Canto, J.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Estalella, R.] Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. [Estalella, R.] Univ Barcelona, Inst Ciencies Cosmos IEEC UB, E-08028 Barcelona, Spain. [Anglada, G.; Gomez, J. F.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Patel, N. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Trinidad, M. A.] Univ Guanajuato, Dept Astron, Guanajuato 36000, Mexico. [Girart, J. M.] Inst Ciencies Espai CSIC IEEC, E-08193 Bellaterra, Spain. [Carrasco-Gonzalez, C.; Rodriguez, L. F.] Ctr Radioastron & Astrofis UNAM, Morelia 58089, Michoacan, Mexico. RP Torrelles, JM (reprint author), Inst Ciencies Espai CSIC IEEC, Marti & Franques 1, E-08028 Barcelona, Spain. EM torrelles@ieec.cat RI Girart, Josep/O-1638-2014; Gomez, Jose Francisco/D-8392-2016; OI Girart, Josep/0000-0002-3829-5591; Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 FU MICINN (Spain) [AYA2011-30228-C03]; FEDER funds; CONACyT [61547, 82543]; DGAPA; UNAM; CONACyT (Mexico); CSIC (Spain); AGAUR (Catalonia) [2009SGR1172] FX We are very grateful to Eri Kato for providing us the near- and mid-infrared images shown in this paper (Fig. 1). We thank the referee, Kevin Marvel, for his valuable comments and suggestions on the manuscript. GA, RE, JFG, JMG, and JMT acknowledge the support from MICINN (Spain) AYA2011-30228-C03 grant (co-funded with FEDER funds). JC acknowledges support from CONACyT grant 61547. SC acknowledges the support of DGAPA, UNAM, CONACyT (Mexico), and CSIC (Spain). CC-G and LFR acknowledge the support of DGAPA, UNAM, and CONACyT (Mexico). MAT acknowledges the support from CONACyT grant 82543. JMG, RE, and JMT acknowledge the support from AGAUR (Catalonia) 2009SGR1172 grant. The ICC (UB) is a CSIC-Associated Unit through the ICE (CSIC). NR 63 TC 5 Z9 5 U1 1 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2014 VL 442 IS 1 BP 148 EP 159 DI 10.1093/mnras/stu847 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RW UT WOS:000338765400014 ER PT J AU Faran, T Poznanski, D Filippenko, AV Chornock, R Foley, RJ Ganeshalingam, M Leonard, DC Li, W Modjaz, M Nakar, E Serduke, FJD Silverman, JM AF Faran, T. Poznanski, D. Filippenko, A. V. Chornock, R. Foley, R. J. Ganeshalingam, M. Leonard, D. C. Li, W. Modjaz, M. Nakar, E. Serduke, F. J. D. Silverman, J. M. TI Photometric and spectroscopic properties of Type II-P supernovae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general ID EXPANDING PHOTOSPHERE METHOD; EXTRAGALACTIC DISTANCE SCALE; STANDARDIZED CANDLE METHOD; CORE-COLLAPSE SUPERNOVAE; TO-GAS RATIO; LIGHT-CURVES; PLATEAU SUPERNOVAE; IA SUPERNOVAE; SN 2005CS; DUST EXTINCTION AB We study a sample of 23 Type II plateau supernovae (SNe II-P), all observed with the same set of instruments. Analysis of their photometric evolution confirms that their typical plateau duration is 100 d with little scatter, showing a tendency to get shorter for more energetic SNe. We examine the claimed correlation between the luminosity and the rise time from explosion to plateau. We analyse their spectra, measuring typical ejecta velocities, and confirm that they follow a well-behaved power-law decline. We find indications of high-velocity material in the spectra of six of our SNe. We test different dust-extinction correction methods by asking the following - does the uniformity of the sample increase after the application of a given method? A reasonably behaved underlying distribution should become tighter after correction. No method we tested made a significant improvement. C1 [Faran, T.; Poznanski, D.; Nakar, E.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Filippenko, A. V.; Ganeshalingam, M.; Li, W.; Serduke, F. J. D.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Chornock, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Foley, R. J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, R. J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Ganeshalingam, M.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Leonard, D. C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Modjaz, M.] NYU, CCPP, New York, NY 10003 USA. [Silverman, J. M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Faran, T (reprint author), Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. EM tamar104@gmail.com FU W. M. Keck Foundation; NASA; Alon fellowship for outstanding young researchers; Raymond and Beverly Sackler Chair for young scientists; NSF grants [AST-1009571, AST-1210311]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; Christopher R. Redlich Fund; Richard and Rhoda Goldman Fund; TABASGO Foundation; NSF [AST-0908886, AST-1211916] FX We thank D. Maoz I. Arcavi, and the referee for helpful comments on this manuscript. A. Barth, A. Coil, E. Gates, B. Swift, and D. Wong participated in the many observations that made this work possible, and we thank them for it. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration; it was made possible by the generous financial support of the W. M. Keck Foundation. We wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The Kast spectrograph on the Shane 3 m reflector at Lick Observatory resulted from a generous donation made by Bill and Marina Kast. We also thank the dedicated staffs of the Lick and Keck Observatories for their assistance. This research made use of the Weizmann interactive supernova data repository (www.weizmann.ac.il/astrophysics/wiserep), as well as the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.; KAIT (at Lick Observatory) and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. DP acknowledges support from the Alon fellowship for outstanding young researchers, and the Raymond and Beverly Sackler Chair for young scientists. DCL acknowledges support from NSF grants AST-1009571 and AST-1210311. JMS is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. AVF's group at UC Berkeley has received generous financial assistance from the Christopher R. Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and the NSF (most recently through grants AST-0908886 and AST-1211916). NR 85 TC 31 Z9 31 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 JUL 21 PY 2014 VL 442 IS 1 BP 844 EP 861 DI 10.1093/mnras/stu955 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RW UT WOS:000338765400070 ER PT J AU Bochanski, JJ Willman, B Caldwell, N Sanderson, R West, AA Strader, J Brown, W AF Bochanski, John J. Willman, Beth Caldwell, Nelson Sanderson, Robyn West, Andrew A. Strader, Jay Brown, Warren TI THE MOST DISTANT STARS IN THE MILKY WAY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: halo; Galaxy: stellar content; Galaxy: structure; stars: late-type ID COOL CARBON STARS; DIGITAL SKY SURVEY; SAGITTARIUS DWARF GALAXY; GALACTIC ESCAPE SPEED; STELLAR HALO; ROTATION CURVE; RAVE SURVEY; 2MASS; MASS; DISPERSION AB We report on the discovery of the most distant Milky Way (MW) stars known to date: ULAS J001535.72+015549.6 and ULAS J074417.48+253233.0. These stars were selected as M giant candidates based on their infrared and optical colors and lack of proper motions. We spectroscopically confirmed them as outer halo giants using the MMT/Red Channel spectrograph. Both stars have large estimated distances, with ULAS J001535.72+015549.6 at 274 +/- 74 kpc and ULAS J074417.48+253233.0 at 238 +/- 64 kpc, making them the first MW stars discovered beyond 200 kpc. ULAS J001535.72+015549.6 and ULAS J074417.48+253233.0 are both moving away from the Galactic center at 52 +/- 10 km s(-1) and 24 +/- 10 km s(-1), respectively. Using their distances and kinematics, we considered possible origins such as: tidal stripping from a dwarf galaxy, ejection from the MW's disk, or membership in an undetected dwarf galaxy. These M giants, along with two inner halo giants that were also confirmed during this campaign, are the first to map largely unexplored regions of our Galaxy's outer halo. C1 [Bochanski, John J.; Willman, Beth] Haverford Coll, Haverford, PA 19041 USA. [Caldwell, Nelson; Brown, Warren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sanderson, Robyn] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [West, Andrew A.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Strader, Jay] Michigan State Univ, Michigan State Astron Grp, E Lansing, MI 48824 USA. RP Bochanski, JJ (reprint author), Haverford Coll, 370 Lancaster Ave, Haverford, PA 19041 USA. EM jbochans@haverford.edu OI Sanderson, Robyn/0000-0003-3939-3297 FU NSF [AST-1151462, PHYS-1066293, AST-1109273, AST-1255568]; RCSA's Cottrell Scholarship FX J.J.B. and B.W. thank the NSF for support under grants NSF AST-1151462 and PHYS-1066293. A.A.W acknowledges NSF grants AST-1109273, AST-1255568, and the RCSA's Cottrell Scholarship. We thank Jonathan Hargis, Alis Deason, Wyn Evans, Vasily Belokurov and Kathyrn Johnston for helpful conversations. NR 51 TC 5 Z9 5 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2014 VL 790 IS 1 AR L5 DI 10.1088/2041-8205/790/1/L5 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5ED UT WOS:000339878100005 ER PT J AU Lalitha, S Poppenhaeger, K Singh, KP Czesla, S Schmitt, JHMM AF Lalitha, S. Poppenhaeger, K. Singh, K. P. Czesla, S. Schmitt, J. H. M. M. TI X-RAY EMISSION FROM THE SUPER-EARTH HOST GJ 1214 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: activity; stars: coronae; stars: individual (GJ 1214); stars: late-type; stars: low-mass ID HOT JUPITERS; ESCAPING ATMOSPHERE; HD 189733B; EVOLUTION; EVAPORATION; SYSTEM; STARS; PARAMETERS; RADIATION; COMPANION AB Stellar activity can produce large amounts of high-energy radiation, which is absorbed by the planetary atmosphere leading to irradiation-driven mass loss. We present the detection and an investigation of high-energy emission in a transiting super-Earth host system, GJ 1214, based on XMM-Newton observations. We derive an X-ray luminosity of L-X = 7.4 x10(25) erg s(-1) and a corresponding activity level of log(L-X/L-bol) similar to-5.3. Further, we determine a coronal temperature of about similar to 3.5 MK, which is typical for coronal emission of moderately active low-mass stars. We estimate that GJ 1214 b evaporates at a rate of 1.3x10(10) g s(-1) and has lost a total of approximate to 2-5.6M(circle plus). C1 [Lalitha, S.; Singh, K. P.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Poppenhaeger, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Czesla, S.; Schmitt, J. H. M. M.] Univ Hamburg, D-21029 Hamburg, Germany. RP Lalitha, S (reprint author), Tata Inst Fundamental Res, Homi Bhabha Rd, Bombay 400005, Maharashtra, India. OI Poppenhaeger, Katja/0000-0003-1231-2194 NR 40 TC 6 Z9 7 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 JUL 20 PY 2014 VL 790 IS 1 AR L11 DI 10.1088/2041-8205/790/1/L11 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5ED UT WOS:000339878100011 ER PT J AU Sur, S Pan, LB Scannapieco, E AF Sur, Sharanya Pan, Liubin Scannapieco, Evan TI ALIGNMENT OF THE SCALAR GRADIENT IN EVOLVING MAGNETIC FIELDS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: abundances; magnetic fields; magnetohydrodynamics (MHD); turbulence ID STAGGERED MESH SCHEME; TURBULENT DYNAMO; MAGNETOHYDRODYNAMIC TURBULENCE; HOMOGENEOUS TURBULENCE; INTERGALACTIC METALS; SIMULATIONS; VORTICITY; STRAIN; GAS AB We conduct simulations of turbulent mixing in the presence of a magnetic field, grown by the small-scale dynamo. We show that the scalar gradient field, del C, which must be large for diffusion to operate, is strongly biased perpendicular to the magnetic field, B. This is true both early on, when the magnetic field is negligible, and at late times, when the field is strong enough to back react on the flow. This occurs because del C increases within the plane of a compressive motion, but B increases perpendicular to it. At late times, the magnetic field resists compression, making it harder for scalar gradients to grow and likely slowing mixing. C1 [Sur, Sharanya; Scannapieco, Evan] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Pan, Liubin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sur, S (reprint author), Arizona State Univ, Sch Earth & Space Explorat, POB 876004, Tempe, AZ 85287 USA. EM sharanya.sur@asu.edu; lpan@cfa.harvard.edu; evan.scannapieco@asu.edu FU National Science Foundation [AST11-03608]; NASA [NNX09AD106]; Harvard-Smithsonian Center for Astrophysics; Advanced Computing Center at Arizona State University; Texas Advanced Computing Center (TACC) at The University of Texas at Austin; Extreme Science and Engineering Discovery Environment (XSEDE) [TG-AST130021]; DOE FX S. S. and E. S. were supported by the National Science Foundation under grant AST11-03608 and NASA theory grant NNX09AD106. postdoctoral fellowship at Harvard-Smithsonian Center for Astrophysics. The authors would also like to acknowledge the Advanced Computing Center at Arizona State University (URL: http://a2c2.asu.edu/), the Texas Advanced Computing Center (TACC) at The University of Texas at Austin (URL: http://www.tacc.utexas.edu), and the Extreme Science and Engineering Discovery Environment (XSEDE) for providing HPC resources via grant TG-AST130021 that have contributed to the results reported within this Letter. The FLASH code is developed in part by the DOE-supported Alliances Center for Astrophysical Thermonuclear Flashes (ASC) at the University of Chicago. NR 30 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 JUL 20 PY 2014 VL 790 IS 1 AR L9 DI 10.1088/2041-8205/790/1/L9 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5ED UT WOS:000339878100009 ER PT J AU Ballard, S Chaplin, WJ Charbonneau, D Desert, JM Fressin, F Zeng, L Werner, MW Davies, GR Aguirre, VS Basu, S Christensen-Dalsgaard, J Metcalfe, TS Stello, D Bedding, TR Campante, TL Handberg, R Karoff, C Elsworth, Y Gilliland, RL Hekker, S Huber, D Kawaler, SD Kjeldsen, H Lund, MN Lundkvist, M AF Ballard, Sarah Chaplin, William J. Charbonneau, David Desert, Jean-Michel Fressin, Francois Zeng, Li Werner, Michael W. Davies, Guy R. Aguirre, Victor Silva Basu, Sarbani Christensen-Dalsgaard, Jorgen Metcalfe, Travis S. Stello, Dennis Bedding, Timothy R. Campante, Tiago L. Handberg, Rasmus Karoff, Christoffer Elsworth, Yvonne Gilliland, Ronald L. Hekker, Saskia Huber, Daniel Kawaler, Steven D. Kjeldsen, Hans Lund, Mikkel N. Lundkvist, Mia TI KEPLER-93b: A TERRESTRIAL WORLD MEASURED TO WITHIN 120 km, AND A TEST CASE FOR A NEW SPITZER OBSERVING MODE SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; methods: observational; planetary systems; stars: individual (KOI 69, KIC 3544595) ID TRANSIT TIMING VARIATIONS; STELLAR EVOLUTION CODE; FINE GUIDANCE SENSOR; CIRCLE-PLUS PLANET; EARTH-SIZED PLANET; SOLAR-TYPE STARS; SUN-LIKE STAR; EXTRASOLAR PLANET; SPACE-TELESCOPE; HABITABLE ZONE AB We present the characterization of the Kepler-93 exoplanetary system, based on three years of photometry gathered by the Kepler spacecraft. The duration and cadence of the Kepler observations, in tandem with the brightness of the star, enable unusually precise constraints on both the planet and its host. We conduct an asteroseismic analysis of the Kepler photometry and conclude that the star has an average density of 1.652 +/- 0.006 g cm(-3). Its mass of 0.911 +/- 0.033M(circle dot) renders it one of the lowest-mass subjects of asteroseismic study. An analysis of the transit signature produced by the planet Kepler-93b, which appears with a period of 4.72673978 +/- 9.7 x 10(-7) days, returns a consistent but less precise measurement of the stellar density, 1.72(-0.28)(+0.02) g cm(-3). The agreement of these two values lends credence to the planetary interpretation of the transit signal. The achromatic transit depth, as compared between Kepler and the Spitzer Space Telescope, supports the same conclusion. We observed seven transits of Kepler-93b with Spitzer, three of which we conducted in a new observing mode. The pointing strategy we employed to gather this subset of observations halved our uncertainty on the transit radius ratio R-P/R-star. We find, after folding together the stellar radius measurement of 0.919 +/- 0.011R(circle dot) with the transit depth, a best-fit value for the planetary radius of 1.481 +/- 0.019 R-circle plus. The uncertainty of 120 km on our measurement of the planet's size currently renders it one of the most precisely measured planetary radii outside of the solar system. Together with the radius, the planetary mass of 3.8 +/- 1.5 M-circle plus. corresponds to a rocky density of 6.3 +/- 2.6 g cm(-3). After applying a prior on the plausible maximum densities of similarly sized worlds between 1 and 1.5 R-circle plus, we find that Kepler-93b possesses an average density within this group. C1 [Ballard, Sarah] Univ Washington, Seattle, WA 98195 USA. [Chaplin, William J.; Davies, Guy R.; Campante, Tiago L.; Handberg, Rasmus; Elsworth, Yvonne; Hekker, Saskia] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Chaplin, William J.; Davies, Guy R.; Aguirre, Victor Silva; Christensen-Dalsgaard, Jorgen; Metcalfe, Travis S.; Campante, Tiago L.; Handberg, Rasmus; Karoff, Christoffer; Elsworth, Yvonne; Kjeldsen, Hans; Lund, Mikkel N.; Lundkvist, Mia] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Charbonneau, David; Fressin, Francois; Zeng, Li] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Desert, Jean-Michel] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Werner, Michael W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Metcalfe, Travis S.] Space Sci Inst, Boulder, CO 80301 USA. [Stello, Dennis; Bedding, Timothy R.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Hekker, Saskia] Max Planck Inst Stromungsforsch, D-37077 Gottingen, Germany. [Hekker, Saskia] Univ Amsterdam, Astron Inst, NL-1012 WX Amsterdam, Netherlands. [Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA. [Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. RP Ballard, S (reprint author), Univ Washington, Seattle, WA 98195 USA. EM sarahba@uw.edu OI Zeng, Li/0000-0003-1957-6635; Davies, Guy/0000-0002-4290-7351; Metcalfe, Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965; Bedding, Tim/0000-0001-5222-4661; Basu, Sarbani/0000-0002-6163-3472; Lund, Mikkel Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571; Handberg, Rasmus/0000-0001-8725-4502 FU NASA through the Sagan Fellowship Program; NASA; NASA's Science Mission Directorate; Kepler Participatory Science [NNX12AC77G, NNX09AB53G]; John Templeton Foundation; UK Science and Technology Facilities Council (STFC); NSF [AST-1105930]; NASA [NNX13AE70G, NNX13AE91G, NNX14AB92G]; Danish National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) - European Research Council [267864]; Netherlands Organisation for Scientific Research (NWO); European Research Council under the European Community's Seventh Framework Programme/ERC [338251]; Australian Research Council; International Space Science Institute (ISSI) FX This work was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. It was conducted with 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. We thank the Spitzer team at the Infrared Processing and Analysis Center in Pasadena, California, and in particular Nancy Silbermann for scheduling the Spitzer observations of this program. This work is also based on observations made with Kepler, which was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. The authors would like to thank the many people who generously gave so much their time to make this Mission a success. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. S. Ballard thanks Geoffrey Marcy for helpful discussions about the RV signature of Kepler-93. We acknowledge support through Kepler Participatory Science Awards NNX12AC77G and NNX09AB53G, awarded to D.C. This publication was made possible in part through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. W.J.C., T.L.C., G.R.D., Y.E. and A.M. acknowledge the support of the UK Science and Technology Facilities Council (STFC). S. Basu acknowledges support from NSF grant AST-1105930 and NASA grant NNX13AE70G. Funding for the StellarAstrophysics Centre is provided by The Danish National Research Foundation (grant agreement No. DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement No. 267864). S.H. acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO). The research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 338251 (StellarAges). T.S.M. acknowledges NASA grant NNX13AE91G. D.S. is supported by the Australian Research Council. D.H. acknowledges support by an appointment to the NASA Postdoctoral Program at Ames Research Center administered by Oak Ridge Associated Universities, and NASA grant NNX14AB92G issued through the Kepler Participating Scientist Program. Computational time on Kraken at the National Institute of Computational Sciences was provided through NSF TeraGrid allocation TG-AST090107. We are also grateful for support from the International Space Science Institute (ISSI). NR 108 TC 20 Z9 20 U1 0 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 12 DI 10.1088/0004-637X/790/1/12 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800012 ER PT J AU Civano, F Fabbiano, G Pellegrini, S Kim, DW Paggi, A Feder, R Elvis, M AF Civano, F. Fabbiano, G. Pellegrini, S. Kim, D. -W. Paggi, A. Feder, R. Elvis, M. TI EARLY-TYPE GALAXIES IN THE CHANDRA COSMOS SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; surveys; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY BINARIES; DEEP FIELD-SOUTH; ELLIPTIC GALAXIES; HOT GAS; XMM-COSMOS; LUMINOSITY FUNCTION; STELLAR MASS; HOST-GALAXY; EVOLUTION AB We study a sample of 69 X-ray detected early-type galaxies (ETGs), selected from the Chandra COSMOS survey, to explore the relation between the X-ray luminosity of hot gaseous halos (L-X,L- (gas)) and the integrated stellar luminosity (L-K) of the galaxies, in a range of redshift extending out to z = 1.5. In the local universe, a tight, steep relationship has been established between these two quantities (L-X,L- gas similar to L-K(4.5)), suggesting the presence of largely virialized halos in X-ray luminous systems. We use well-established relations from the study of local universe ETGs, together with the expected evolution of the X-ray emission, to subtract the contribution of low-mass X-ray binary populations from the X-ray luminosity of our sample. Our selection minimizes the presence of active galactic nuclei (AGNs), yielding a sample representative of normal passive COSMOS ETGs; therefore, the resulting luminosity should be representative of gaseous halos, although we cannot exclude other sources such as obscured AGNs or enhanced X-ray emission connected with embedded star formation in the higher-z galaxies. We find that most of the galaxies with estimated L-X < 10(42) erg s(-1) and z < 0.55 follow the L-X,L- gas - L-K relation of local universe ETGs. For these galaxies, the gravitational mass can be estimated with a certain degree of confidence from the local virial relation. However, the more luminous (10(42) erg s(-1) < L-X < 10(43.5) erg s(-1)) and distant galaxies present significantly larger scatter; these galaxies also tend to have younger stellar ages. The divergence from the local L-X,L- gas - L-K relation in these galaxies implies significantly enhanced X-ray emission up to a factor of 100 larger than predicted from the local relation. We discuss the implications of this result for the presence of hidden AGNs, and the evolution of hot halos, in nuclear and star formation feedback. C1 [Civano, F.] Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Civano, F.; Fabbiano, G.; Kim, D. -W.; Paggi, A.; Elvis, M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Civano, F.] Dartmouth Coll, Wilder Lab, Dept Phys & Astron, Hanover, NH 03855 USA. [Pellegrini, S.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Feder, R.] Great Neck South High Sch, Great Neck, NY 11020 USA. RP Civano, F (reprint author), Yale Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA. RI Paggi, Alessandro/C-1219-2017 OI Paggi, Alessandro/0000-0002-5646-2410 FU NASA [11-ADAP11-0218, GO1-12125A, NAS8-03060]; MIUR [2010LY5N2T] FX The authors thank L. Pozzetti for providing the K-band luminosities as a function of time for the Bruzual & Charlot (2003) stellar population models. F.C. acknowledges financial support by the NASA contract 11-ADAP11-0218, S.P. from MIUR grant PRIN 2010-2011, prot. 2010LY5N2T, and A. P. by the NASA grant GO1-12125A. This work was partially supported by NASA contract NAS8-03060 (CXC). NR 68 TC 12 Z9 12 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 JUL 20 PY 2014 VL 790 IS 1 AR 16 DI 10.1088/0004-637X/790/1/16 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800016 ER PT J AU Cohen, O Drake, JJ Glocer, A Garraffo, C Poppenhaeger, K Bell, JM Ridley, AJ Gombosi, TI AF Cohen, O. Drake, J. J. Glocer, A. Garraffo, C. Poppenhaeger, K. Bell, J. M. Ridley, A. J. Gombosi, T. I. TI MAGNETOSPHERIC STRUCTURE AND ATMOSPHERIC JOULE HEATING OF HABITABLE PLANETS ORBITING M-DWARF STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics ( MHD); planets and satellites: atmospheres; planets and satellites: magnetic fields; planets and satellites: terrestrial planets ID MAIN-SEQUENCE STARS; RESISTIVE MHD SIMULATIONS; EARTH-LIKE EXOPLANETS; EJECTION CME ACTIVITY; MASS-LOSS RATES; X-RAY-EMISSION; HOT JUPITERS; OHMIC DISSIPATION; MAGNETIC-FIELD; HD 209458B AB We study the magnetospheric structure and the ionospheric Joule Heating of planets orbiting M-dwarf stars in the habitable zone using a set ofmagnetohydrodynamic models. The stellarwind solution is used to drive amodel for the planetary magnetosphere, which is coupled with a model for the planetary ionosphere. Our simulations reveal that the space environment around close-in habitable planets is extreme, and the stellar wind plasma conditions change from sub-to super-Alfv ' enic along the planetary orbit. As a result, themagnetospheric structure changes dramatically with a bow shock forming in the super-Alfv ' enic sectors, while no bow shock forms in the sub-Alfv ' enic sectors. The planets reside most of the time in the sub-Alfv ' enic sectors with poor atmospheric protection. A significant amount of Joule Heating is provided at the top of the atmosphere as a result of the intense stellar wind. For the steady-state solution, the heating is about 0.1%-3% of the total incoming stellar irradiation, and it is enhanced by 50% for the time-dependent case. The significant Joule Heating obtained here should be considered in models for the atmospheres of habitable planets in terms of the thickness of the atmosphere, the top-side temperature and density, the boundary conditions for the atmospheric pressure, and particle radiation and transport. Here we assume constant ionospheric Pedersen conductance similar to that of the Earth. The conductance could be greater due to the intense EUV radiation leading to smaller heating rates. We plan to quantify the ionospheric conductance in future study. C1 [Cohen, O.; Drake, J. J.; Garraffo, C.; Poppenhaeger, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Glocer, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bell, J. M.] Natl Inst Aerosp, Ctr Planetary Atmospheres & Flight Sci, Hampton, VA 23666 USA. [Ridley, A. J.; Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Glocer, Alex/C-9512-2012; Gombosi, Tamas/G-4238-2011; Ridley, Aaron/F-3943-2011; OI Glocer, Alex/0000-0001-9843-9094; Gombosi, Tamas/0000-0001-9360-4951; Ridley, Aaron/0000-0001-6933-8534; Poppenhaeger, Katja/0000-0003-1231-2194; Cohen, Ofer/0000-0003-3721-0215 FU NASA ESS; NASA ESTO-CT; NSF KDI; DoDMURI; NASA HEC Pleiades system [SMD-13-4076]; NASA [NAS8-03060] FX We thank an unknown referee for comments and suggestions. The work presented here was funded by the Smithsonian Institution Consortium for Unlocking the Mysteries of the Universe grant " Lessons from Mars: Are Habitable Atmospheres on Planets around M Dwarfs Viable?," and by the Smithsonian Institute Competitive Grants Program for Science (CGPS) grant " Can Exoplanets Around Red Dwarfs Maintain Habitable Atmospheres?." Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoDMURI. The simulations were performed on the NASA HEC Pleiades system under award SMD-13-4076. J. J. D. was supported by NASA contract NAS8-03060 to the Chandra X-ray Center during the course of this research and thanks the Director, H. Tananbaum, for continuing support and encouragement. NR 86 TC 24 Z9 24 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 57 DI 10.1088/0004-637X/790/1/57 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800057 ER PT J AU Favre, C Jorgensen, JK Field, D Brinch, C Bisschop, SE Bourke, TL Hogerheijde, MR Frieswijk, WWF AF Favre, Cecile Jorgensen, Jes K. Field, David Brinch, Christian Bisschop, Suzanne E. Bourke, Tyler L. Hogerheijde, Michiel R. Frieswijk, Wilfred W. F. TI DYNAMICAL STRUCTURE OF THE INNER 100 AU OF THE DEEPLY EMBEDDED PROTOSTAR IRAS 16293-2422 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM: individual objects (IRAS 16293-2422); radio lines: ISM; stars: formation ID SUBMILLIMETER-WAVE SPECTRUM; MOLECULAR CLOUD CORES; YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; SOLAR-TYPE PROTOSTAR; LOW-MASS PROTOSTARS; L1551 IRS 5; MILLIMETER-WAVE; CIRCUMSTELLAR DISKS; VIBRATIONAL-STATES AB A fundamental question about the early evolution of low-mass protostars is when circumstellar disks may form. High angular resolution observations of molecular transitions in the (sub)millimeter wavelength windows make it possible to investigate the kinematics of the gas around newly formed stars, for example, to identify the presence of rotation and infall. IRAS 16293-2422 was observed with the extended Submillimeter Array (eSMA) resulting in subarcsecond resolution (0 ''.46 x 0 ''.29, i.e., similar to 55 x 35 AU) images of compact emission from the (CO)-O-17 (3-2) and (CS)-S-34 (7-6) transitions at 337 GHz (0.89 mm). To recover the more extended emission we have combined the eSMA data with SMA observations of the same molecules. The emission of (CO)-O-17 (3-2) and (CS)-S-34 (7-6) both show a velocity gradient oriented along a northeast-southwest direction with respect to the continuum marking the location of one of the components of the binary, IRAS 16293A. Our combined eSMA and SMA observations show that the velocity field on the 50-400AU scales is consistent with a rotating structure. It cannot be explained by simple Keplerian rotation around a single point mass but rather needs to take into account the enclosed envelope mass at the radii where the observed lines are excited. We suggest that IRAS 16293-2422 could be among the best candidates to observe a pseudo-disk with future high angular resolution observations. C1 [Favre, Cecile; Field, David] Univ Aarhus, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Favre, Cecile] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Jorgensen, Jes K.; Brinch, Christian; Bisschop, Suzanne E.] Univ Copenhagen, Niels Bohr Inst, Ctr Star & Planet Format, DK-2100 Copenhagen O, Denmark. [Jorgensen, Jes K.; Brinch, Christian; Bisschop, Suzanne E.] Univ Copenhagen, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark. [Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bourke, Tyler L.] SKA Org, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. [Hogerheijde, Michiel R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Frieswijk, Wilfred W. F.] Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands. RP Favre, C (reprint author), Univ Aarhus, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. EM cfavre@umich.edu RI Brinch, Christian/G-5157-2015; OI Brinch, Christian/0000-0002-5074-7183; Hogerheijde, Michiel/0000-0001-5217-537X FU Smithsonian Institution; Instrument Center for Danish Astrophysics (IDA); Lundbeck foundation; Danish National Research Foundation; Canadian Space Agency; Netherlands Organisation for Scientific Research, NWO [614.061.416]; Academia Sinica FX We thank the entire SMA and eSMA staff who produced such excellent instruments. The development of the eSMA has been facilitated by grant 614.061.416 from the Netherlands Organisation for Scientific Research, NWO. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. We are grateful to Sandrine Bottinelli who was the original proposer of the presented eSMA observations. C.F. thanks Edwin Bergin for enlightening discussions. C.F. also acknowledges the financial support provided by The Instrument Center for Danish Astrophysics (IDA). The research of J.K.J. was supported by a Junior Group Leader Fellowship from the Lundbeck foundation. Research at the Centre for Star and Planet Formation is funded by the Danish National Research Foundation. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. NR 81 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 JUL 20 PY 2014 VL 790 IS 1 AR 55 DI 10.1088/0004-637X/790/1/55 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800055 ER PT J AU Gou, LJ McClintock, JE Remillard, RA Steiner, JF Reid, MJ Orosz, JA Narayan, R Hanke, M Garcia, J AF Gou, Lijun McClintock, Jeffrey E. Remillard, Ronald A. Steiner, James F. Reid, Mark J. Orosz, Jerome A. Narayan, Ramesh Hanke, Manfred Garcia, Javier TI CONFIRMATION VIA THE CONTINUUM-FITTING METHOD THAT THE SPIN OF THE BLACK HOLE IN CYGNUS X-1 IS EXTREME SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; X-rays: binaries; X-rays: individual (Cygnus X-1) ID RAY REFLECTION SPECTRA; LMC X-1; INTERSTELLAR-MEDIUM; MASS-DISTRIBUTION; PLUNGING REGION; ACCRETION DISK; BINARY; STATE; SUZAKU; GALAXY AB In Gou et al., we reported that the black hole primary in the X-ray binary Cygnus X-1 is a near-extreme Kerr black hole with a spin parameter a(*) > 0.95 (3 sigma). We confirm this result while setting a new and more stringent limit: a(*) > 0.983 at the 3 sigma (99.7%) confidence level. The earlier work, which was based on an analysis of all three useful spectra that were then available, was possibly biased by the presence in these spectra of a relatively strong Compton power-law component: the fraction of the thermal seed photons scattered into the power law was f(s) = 23%-31%, while the upper limit for reliable application of the continuum-fitting method is f(s) less than or similar to 25%. We have subsequently obtained six additional spectra of Cygnus X-1 suitable for the measurement of spin. Five of these spectra are of high quality with f(s) in the range 10%-19%, a regime where the continuum-fitting method has been shown to deliver reliable results. Individually, the six spectra give lower limits on the spin parameter that range from a(*) > 0.95 to a(*) > 0.98, allowing us to conservatively conclude that the spin of the black hole is a(*) > 0.983 (3 sigma). C1 [Gou, Lijun] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Gou, Lijun; McClintock, Jeffrey E.; Steiner, James F.; Reid, Mark J.; Narayan, Ramesh; Garcia, Javier] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Remillard, Ronald A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Hanke, Manfred] Univ Erlangen Nurnberg, Remeis Observ, D-96049 Bamberg, Germany. [Hanke, Manfred] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany. RP Gou, LJ (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RI XRAY, SUZAKU/A-1808-2009; OI Narayan, Ramesh/0000-0002-1919-2730; Remillard, Ronald/0000-0003-4815-0481 FU NSFC [Y211541001, 11333005]; NAOC [Y234031001]; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [XDB09000000]; NASA [NNX11AD08G]; NASA Hubble Fellowship [HST-HF-51315.01]; Bundesministerium fur Wirtschaft und Technologie [DLR 50 OR 0701] FX We thank an anonymous referee for many constructive comments and criticisms, particularly those concerning pileup. We are grateful for allocations of Chandra, RXTE, and Swift observing time granted by Director H. Tananbaum and Project Scientists T. Strohmayer and N. Gehrels, respectively. For help in planning the Chandra observations, we thank M. Nowak and N. Schulz. We also thank M. Nowak, J. Wilms, and Bin-Bin Zhang for discussions on X-ray data analysis, R. Smith for calling the effects of dust scattering to our attention, and S. Yamada for reducing the Suzaku data, and J. G. Xiang for reducing the Chandra TE data. This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC) at NASA/Goddard Space Flight Center. For technical support in using the Odyssey cluster, L.J.G. thanks the Harvard FAS Sciences Division Research Computing Group. L.J.G. acknowledges the support of NSFC grant (Y211541001, 11333005) and NAOC grant (Y234031001), and is also supported by the Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences, grant No. XDB09000000, J.E.M. acknowledges support from NASA grant NNX11AD08G, J.F.S. has been supported by NASA Hubble Fellowship grant HST-HF-51315.01, and M.H. acknowledges funding from the Bundesministerium fur Wirtschaft und Technologie under grant No. DLR 50 OR 0701. NR 63 TC 34 Z9 34 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 29 DI 10.1088/0004-637X/790/1/29 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800029 ER PT J AU Haas, M Leipski, C Barthel, P Wilkes, BJ Vegetti, S Bussmann, RS Willner, SP Westhues, C Ashby, MLN Chini, R Clements, DL Fassnacht, CD Horesh, A Klaas, U Koopmans, LVE Kuraszkiewicz, J Lagattuta, DJ Meisenheimer, K Stern, D Wylezalek, D AF Haas, Martin Leipski, Christian Barthel, Peter Wilkes, Belinda J. Vegetti, Simona Bussmann, R. Shane Willner, S. P. Westhues, Christian Ashby, Matthew L. N. Chini, Rolf Clements, David L. Fassnacht, Christopher D. Horesh, Assaf Klaas, Ulrich Koopmans, Leon V. E. Kuraszkiewicz, Joanna Lagattuta, David J. Meisenheimer, Klaus Stern, Daniel Wylezalek, Dominika TI 3C 220.3: A RADIO GALAXY LENSING A SUBMILLIMETER GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: individual (3C 220.3); gravitational lensing: strong; radio continuum: galaxies; submillimeter: galaxies ID SPITZER-SPACE-TELESCOPE; COLD DARK-MATTER; GRAVITATIONAL-LENS; ARRAY CAMERA; MISSION; MASS; SPECTROMETER; PERFORMANCE; POPULATION; B2045+265 AB Herschel Space Observatory photometry and extensive multiwavelength follow-up have revealed that the powerful radio galaxy (PRG) 3C 220.3 at z = 0.685 acts as a gravitational lens for a background submillimeter galaxy (SMG) at z = 2.221. At an observed wavelength of 1 mm, the SMG is lensed into three distinct images. In the observed near infrared, these images are connected by an arc of similar to 1 ''.8 radius forming an Einstein half-ring centered near the radio galaxy. In visible light, only the arc is apparent. 3C 220.3 is the only known instance of strong galaxy-scale lensing by a PRG not located in a galaxy cluster and therefore it offers the potential to probe the dark matter content of the radio galaxy host. Lens modeling rejects a single lens, but two lenses centered on the radio galaxy host A and a companion B, separated by 1 ''.5, provide a fit consistent with all data and reveal faint candidates for the predicted fourth and fifth images. The model does not require an extended common dark matter halo, consistent with the absence of extended bright X-ray emission on our Chandra image. The projected dark matter fractions within the Einstein radii of A (1 ''.02) and B (0 ''.61) are about 0.4 +/- 0.3 and 0.55 +/- 0.3. The mass to i-band light ratios of A and B, M/L-i similar to 8 +/- 4 M-circle dot L-circle dot(-1), appear comparable to those of radio-quiet lensing galaxies at the same redshift in the CfA-Arizona Space Telescope LEns Survey, Lenses Structure and Dynamics, and Strong Lenses in the Legacy Survey samples. The lensed SMG is extremely bright with observed f (250 mu m) = 440 mJy owing to a magnification factor mu similar to 10. The SMG spectrum shows luminous, narrow Civ lambda 1549 angstrom emission, revealing that the SMG houses a hidden quasar in addition to a violent starburst. Multicolor image reconstruction of the SMG indicates a bipolar morphology of the emitted ultraviolet (UV) light suggestive of cones through which UV light escapes a dust-enshrouded nucleus. C1 [Haas, Martin; Westhues, Christian; Chini, Rolf] Ruhr Univ Bochum, Inst Astron, Bochum, Germany. [Leipski, Christian; Klaas, Ulrich; Meisenheimer, Klaus] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Barthel, Peter; Koopmans, Leon V. E.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Wilkes, Belinda J.; Bussmann, R. Shane; Willner, S. P.; Ashby, Matthew L. N.; Kuraszkiewicz, Joanna] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vegetti, Simona] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Chini, Rolf] Univ Catolica Norte, Antofagasta, Chile. [Clements, David L.] Univ London Imperial Coll Sci Technol & Med, London, England. [Fassnacht, Christopher D.] Univ Calif Davis, Davis, CA 95616 USA. [Horesh, Assaf] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Lagattuta, David J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Lagattuta, David J.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Stern, Daniel; Wylezalek, Dominika] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Wylezalek, Dominika] European So Observ, Garching, Germany. RP Haas, M (reprint author), Ruhr Univ Bochum, Inst Astron, Postfach 102148, Bochum, Germany. EM haas@astro.rub.de RI Horesh, Assaf/O-9873-2016 OI Horesh, Assaf/0000-0002-5936-1156 NR 50 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 46 DI 10.1088/0004-637X/790/1/46 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800046 ER PT J AU Kaminski, E Frank, A Carroll, J Myers, P AF Kaminski, Erica Frank, Adam Carroll, Jonathan Myers, Phil TI ON THE ROLE OF AMBIENT ENVIRONMENTS IN THE COLLAPSE OF BONNOR-EBERT SPHERES SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitation; hydrodynamics; ISM: clouds; evolution; methods: numerical; stars: formation ID GRAVITATIONAL COLLAPSE; ISOTHERMAL SPHERES; GAS CLOUDS; DYNAMICS; IMPLEMENTATION; EXTINCTION; ASTROBEAR; CORES; STAR; AMR AB We consider the interaction between a marginally stable Bonnor-Ebert (BE) sphere and the surrounding ambient medium. In particular, we explore how the infall from an evolving ambient medium can trigger the collapse of the sphere using three-dimensional adaptive mesh refinement simulations. We find the resulting collapse dynamics to vary considerably with ambient density. In the highest ambient density cases, infalling material drives a strong compression wave into the cloud. It is the propagation of this wave through the cloud interior that triggers the subsequent collapse. For lower ambient densities, we find the main trigger of collapse to be a quasistatic adjustment of the BE sphere to gravitational settling of the ambient gas. In all cases, we find that the classic "outside-in" collapse mode for super-critical BE spheres is recovered before a protostar (i.e., sink particle) forms. Our work supports scenarios in which BE dynamics naturally begins with either a compression wave or infall dominated phase, and only later assumes the usual outside-in collapse behavior. C1 [Kaminski, Erica; Frank, Adam; Carroll, Jonathan] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Myers, Phil] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kaminski, E (reprint author), Univ Rochester, Dept Phys & Astron, 206 Bausch & Lomb Hall,POB 270171, Rochester, NY 14627 USA. EM erica@pas.rochester.edu; pmyers@cfa.harvard.edu OI Fogerty, Erica/0000-0003-1242-3898 FU Space Telescope Science Institute [HST-AR-12128, HST-AR-12832]; Department of Energy [DE-SC0001063, R17081]; National Science Foundation for the Extreme Science and Engineering Discovery Environment (XSEDE) [OCI-1053575, AST-1109285]; Horton Fellowship FX We are grateful for the support provided by the Space Telescope Science Institute through grants HST-AR-12128 and HST-AR-12832, the Department of Energy through grant numbers DE-SC0001063 and R17081, the National Science Foundation for the Extreme Science and Engineering Discovery Environment (XSEDE) through grant number OCI-1053575 and for grant number AST-1109285. We would also like to thank the University of Rochester's Laboratory for Laser Energetics for funds received by the Horton Fellowship and the University's Center for Integrated Research Computing for providing the supercomputer resources that supported this work. NR 27 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 70 DI 10.1088/0004-637X/790/1/70 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800070 ER PT J AU Lemonias, JJ Schiminovich, D Catinella, B Heckman, TM Moran, SM AF Lemonias, Jenna J. Schiminovich, David Catinella, Barbara Heckman, Timothy M. Moran, Sean M. TI RESOLVED H I IMAGING OF A POPULATION OF MASSIVE H I-RICH GALAXIES WITH SUPPRESSED STAR FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation ID ACTIVE GALACTIC NUCLEI; ARECIBO SDSS SURVEY; FAST ALPHA SURVEY; FRACTION SCALING RELATIONS; SINS/ZC-SINF SURVEY; IRAM LEGACY SURVEY; MOLECULAR GAS; NEUTRAL HYDROGEN; FORMATION EFFICIENCY; ATLAS(3D) PROJECT AB Despite the existence of well-defined relationships between cold gas and star formation, there is evidence that some galaxies contain large amounts of H I that do not form stars efficiently. By systematically assessing the link between HI and star formation within a sample of galaxies with extremely high H I masses (log M-HI/M-circle dot > 10), we uncover a population of galaxies with an unexpected combination of high HI masses and low specific star formation rates that exists primarily at stellar masses greater than log M*/M-circle dot similar to 10.5. We obtained H I maps of 20 galaxies in this population to understand the distribution of the HI and the physical conditions in the galaxies that could be suppressing star formation in the presence of large quantities of H I. We find that all of the galaxies we observed have low H I surface densities in the range in which inefficient star formation is common. The low H I surface densities are likely the main cause of the low specific star formation rates, but there is also some evidence that active galactic nuclei or bulges contribute to the suppression of star formation. The sample's agreement with the global star formation law highlights its usefulness as a tool for understanding galaxies that do not always follow expected relationships. C1 [Lemonias, Jenna J.; Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Catinella, Barbara] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Heckman, Timothy M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Moran, Sean M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Lemonias, JJ (reprint author), Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA. EM jenna@astro.columbia.edu OI Catinella, Barbara/0000-0002-7625-562X FU Australian Research Council Future Fellowship Future Fellowship [FT120100660]; NASA Space Grant; National Science Foundation [AST-1100968]; Alfred P. Sloan Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; Participating Institutions; [HST-GO-12603.02-A] FX We thank Ximena Fernandez and Jacqueline van Gorkom for sharing their expertise and Ted Wyder for providing the GLSB data. We also thank the anonymous referee for useful comments. J.L. was partially supported by HST-GO-12603.02-A and a NASA Space Grant. B.C. is the recipient of an Australian Research Council Future Fellowship (FT120100660).; The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), and in alliance with Ana G. Mendez-Universidad Metropolitana, and the Universities Space Research Association.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. NR 68 TC 4 Z9 4 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 27 DI 10.1088/0004-637X/790/1/27 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800027 ER PT J AU Li, GJ Batygin, K AF Li, Gongjie Batygin, Konstantin TI ON THE SPIN-AXIS DYNAMICS OF A MOONLESS EARTH SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: dynamical evolution and stability ID LONG-TERM EVOLUTION; SUN-LIKE STAR; HABITABLE-ZONE; SOLAR-SYSTEM; OBLIQUITY VARIATIONS; CHAOTIC OBLIQUITY; CLIMATE CHANGES; MARS; PLANETS; DIFFUSION AB The variation of a planet's obliquity is influenced by the existence of satellites with a high mass ratio. For instance, Earth's obliquity is stabilized by the Moon and would undergo chaotic variations in the Moon's absence. In turn, such variations can lead to large-scale changes in the atmospheric circulation, rendering spin-axis dynamics a central issue for understanding climate. The relevant quantity for dynamically forced climate change is the rate of chaotic diffusion. Accordingly, here we re-examine the spin-axis evolution of a Moonless Earth within the context of a simplified perturbative framework. We present analytical estimates of the characteristic Lyapunov coefficient as well as the chaotic diffusion rate and demonstrate that even in absence of the Moon, the stochastic change in Earth's obliquity is sufficiently slow to not preclude long-term habitability. Our calculations are consistent with published numerical experiments and illustrate the putative system's underlying dynamical structure in a simple and intuitive manner. C1 [Li, Gongjie; Batygin, Konstantin] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Li, GJ (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM gli@cfa.harvard.edu NR 34 TC 8 Z9 8 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 69 DI 10.1088/0004-637X/790/1/69 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800069 ER PT J AU Margutti, R Parrent, J Kamble, A Soderberg, AM Foley, RJ Milisavljevic, D Drout, MR Kirshner, R AF Margutti, R. Parrent, J. Kamble, A. Soderberg, A. M. Foley, R. J. Milisavljevic, D. Drout, M. R. Kirshner, R. TI NO X-RAYS FROM THE VERY NEARBY TYPE Ia SN 2014J: CONSTRAINTS ON ITS ENVIRONMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: individual (SN 2014J) ID ACCRETING WHITE-DWARF; LIGHT CURVES; SURFACE DETONATIONS; DEGENERATE CHANNEL; SYMBIOTIC CHANNEL; SUPERNOVA 2011FE; RECURRENT NOVAE; UPPER LIMITS; RS OPHIUCHI; MODELS AB Deep X-ray observations of the post-explosion environment around the very nearby Type Ia SN 2014J (d(L) = 3.5Mpc) reveal no X-ray emission down to a luminosity L-x < 7 x 1036 erg s(-1) (0.3-10 keV) at delta t similar to 20 days after the explosion. We interpret this limit in the context of inverse Compton emission from upscattered optical photons by the supernova shock and constrain the pre-explosion mass-loss rate of the stellar progenitor system to be M < 10(-9) M-circle dot yr(-1) (for wind velocity upsilon(w) = 100 km s(-1)). Alternatively, the SN shock might be expanding into a uniform medium with density n(CSM) < 3 cm (3). These results rule out single-degenerate (SD) systems with steady mass loss until the terminal explosion and constrain the fraction of transferred material lost at the outer Lagrangian point to be <= 1%. The allowed progenitors are (1) white dwarf-white dwarf progenitors, (2) SD systems with unstable hydrogen burning experiencing recurrent nova eruptions with recurrence time t < 300 yr, and (3) stars where the mass loss ceases before the explosion. C1 [Margutti, R.; Parrent, J.; Kamble, A.; Soderberg, A. M.; Milisavljevic, D.; Drout, M. R.; Kirshner, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Foley, R. J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, R. J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. RP Margutti, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Margutti, Raffaella/0000-0003-4768-7586 FU David and Lucile Packard Foundation Fellowship for Science and Engineering; National Science Foundation [AST12-11196] FX We thank the referee for useful comments and a timely report. We thank H. Tananbaum and the entire Chandra team for making the X-ray observations possible. R. M. thanks Lorenzo Sironi, Cristiano Guidorzi, and James Guillochon for many instructive discussions and Georgios Dimitriadis for clarifications about his nova ejection simulations. Support for this work was provided by the David and Lucile Packard Foundation Fellowship for Science and Engineering awarded to A.M.S. R.K. acknowledges support from the National Science Foundation through grant AST12-11196. NR 99 TC 33 Z9 33 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 JUL 20 PY 2014 VL 790 IS 1 AR 52 DI 10.1088/0004-637X/790/1/52 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800052 ER PT J AU Nesvorny, D Kipping, D Terrell, D Feroz, F AF Nesvorny, David Kipping, David Terrell, Dirk Feroz, Farhan TI PHOTO-DYNAMICAL ANALYSIS OF THREE KEPLER OBJECTS OF INTEREST WITH SIGNIFICANT TRANSIT TIMING VARIATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: detection; planets and satellites: dynamical evolution and stability; planets and satellites: individual (KOI-227, KOI-319, KOI-884) ID 1ST 16 MONTHS; II. ANALYSIS; PLANETS; CANDIDATES; EXOMOONS; HUNT; EFFICIENT; SYSTEMS; SEARCH; III. AB KOI-227, KOI-319 and KOI-884 are identified here as (at least) two planet systems. For KOI-319 and KOI-884, the observed Transit Timing Variations (TTVs) of the inner transiting planet are used to detect an outer non-transiting planet. The outer planet in KOI-884 is similar or equal to 2.6 Jupiter masses and has the orbital period just narrow of the 3:1 resonance with the inner planet (orbital period ratio 2.93). The distribution of parameters inferred from KOI-319.01's TTVs is bimodal with either a similar or equal to 1.6 Neptune-mass (M-N) planet wide of the 5:3 resonance (period 80.1 days) or a similar or equal to 1 Saturn-mass planet wide of the 7:3 resonance (period 109.2 days). The radial velocity measurements can be used in this case to determine which of these parameter modes is correct. KOI-227.01's TTVs with large similar or equal to 10 hr amplitude can be obtained for planetary-mass companions in various major resonances. Based on the Bayesian evidence, the current TTV data favor the outer 2:1 resonance with a companion mass similar or equal to 1.5 M-N, but this solution implies a very large density of KOI-227.01. The inner and outer 3:2 resonance solutions with sub-Neptune-mass companions are physically more plausible, but will need to be verified. C1 [Nesvorny, David; Terrell, Dirk] Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Kipping, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Feroz, Farhan] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. RP Nesvorny, D (reprint author), Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA. FU NASA Sagan fellowship FX We thank the Kepler Science Team, especially the DAWG, for making the data used here available. D.M.K. is supported by the NASA Sagan fellowship. NR 38 TC 5 Z9 5 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 JUL 20 PY 2014 VL 790 IS 1 AR 31 DI 10.1088/0004-637X/790/1/31 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800031 ER PT J AU Rigby, JR Bayliss, MB Gladders, MD Sharon, K Wuyts, E Dahle, H AF Rigby, J. R. Bayliss, M. B. Gladders, M. D. Sharon, K. Wuyts, E. Dahle, H. TI ON THE LACK OF CORRELATION BETWEEN Mg II 2796, 2803 angstrom AND Ly alpha EMISSION IN LENSED STAR-FORMING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: star formation; gravitational lensing: strong; ISM: jets and outflows; techniques: spectroscopic ID RCSGA 032727-132609; SPECTROSCOPY; OUTFLOWS; ABSORPTION; SPECTRA; BRIGHT; Z=1.7 AB We examine the Mg II 2796, 2803, Ly alpha, and nebular line emission in five bright star-forming galaxies at 1.66 < z < 1.91 that have been gravitationally lensed by foreground galaxy clusters. All five galaxies show prominent Mg II emission and absorption in a P Cygni profile. We find no correlation between the equivalent widths of Mg II and Lya emission. The Mg II emission has a broader range of velocities than do the nebular emission line profiles; the Mg II emission is redshifted with respect to systemic by 100-200 km s(-1). When present, Ly alpha is even more redshifted. The reddest components of Mg II and Ly alpha emission have tails to 500-600 km s(-1), implying a strong outflow. The lack of correlation in the Mg II and Ly alpha equivalent widths, the differing velocity profiles, and the high ratios of Mg II to nebular line fluxes together suggest that the bulk of Mg II emission does not ultimately arise as nebular line emission, but may instead be reprocessed stellar continuum emission. C1 [Rigby, J. R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Bayliss, M. B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bayliss, M. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gladders, M. D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Gladders, M. D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Sharon, K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Wuyts, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Dahle, H.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. RP Rigby, JR (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. RI Rigby, Jane/D-4588-2012 OI Rigby, Jane/0000-0002-7627-6551 FU Carnegie Observatories, U. Michigan; Carnegie Observatories, U. Chicago; Harvard-Smithsonian Center for Astrophysics FX This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Magellan time for this project was granted by the Carnegie Observatories, U. Michigan, U. Chicago, and the Harvard-Smithsonian Center for Astrophysics. NR 22 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 JUL 20 PY 2014 VL 790 IS 1 AR 44 DI 10.1088/0004-637X/790/1/44 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800044 ER PT J AU Spalding, C Batygin, K AF Spalding, Christopher Batygin, Konstantin TI EARLY EXCITATION OF SPIN-ORBIT MISALIGNMENTS IN CLOSE-IN PLANETARY SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: general; stars: magnetic field ID T-TAURI STARS; MAGNETOCENTRIFUGALLY DRIVEN FLOWS; ACCRETING MAGNETIC PROTOSTARS; HOT JUPITERS; EXOPLANETARY SYSTEMS; PROTOPLANETARY DISKS; STELLAR ROTATION; GIANT PLANETS; YOUNG STARS; MASS STARS AB Continued observational characterization of transiting planets that reside in close proximity to their host stars has shown that a substantial fraction of such objects possess orbits that are inclined with respect to the spin axes of their stars. Mounting evidence for the wide-spread nature of this phenomenon has challenged the conventional notion that large-scale orbital transport occurs during the early epochs of planet formation and is accomplished via planet-disk interactions. However, recent work has shown that the excitation of spin-orbit misalignment between protoplanetary nebulae and their host stars can naturally arise from gravitational perturbations in multi-stellar systems as well as magnetic disk-star coupling. In this work, we examine these processes in tandem. We begin with a thorough exploration of the gravitationally facilitated acquisition of spin-orbit misalignment and analytically show that the entire possible range of misalignments can be trivially reproduced. Moreover, we demonstrate that the observable spin-orbit misalignment only depends on the primordial disk-binary orbit inclination. Subsequently, we augment our treatment by accounting for magnetic torques and show that more exotic dynamical evolution is possible, provided favorable conditions for magnetic tilting. Cumulatively, our results suggest that observed spin-orbit misalignments are fully consistent with disk-driven migration as a dominant mechanism for the origin of close-in planets. C1 [Spalding, Christopher; Batygin, Konstantin] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. [Batygin, Konstantin] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Spalding, C (reprint author), CALTECH, Dept Geol & Planetary Sci, 1200 East Calif Blvd, Pasadena, CA 91125 USA. EM cspaldin@caltech.edu FU ITC Prize Postdoctoral Fellowship at the Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics; CONOCO Graduate Fellowship in Geology at the California Institute of Technology FX We thank the anonymous referee for a careful review of the paper which led to an enhanced manuscript. During the review of this paper, we have become aware that Lai (2014) arrived at similar results simultaneously and independently. K.B. acknowledges the generous support from the ITC Prize Postdoctoral Fellowship at the Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics. C.S. acknowledges the generous support from the CONOCO Graduate Fellowship in Geology at the California Institute of Technology. NR 92 TC 18 Z9 18 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 JUL 20 PY 2014 VL 790 IS 1 AR 42 DI 10.1088/0004-637X/790/1/42 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800042 ER PT J AU Yee, JC Han, C Gould, A Skowron, J Bond, IA Udalski, A Hundertmark, M Monard, LAG Porritt, I Nelson, P Bozza, V Albrow, MD Choi, JY Christie, GW Depoy, DL Gaudi, BS Hwang, KH Jung, YK Lee, CU McCormick, J Natusch, T Ngan, H Park, H Pogge, RW Shin, IG Tan, TG Abe, F Bennett, DP Botzler, CS Freeman, M Fukui, A Fukunaga, D Itow, Y Koshimoto, N Larsen, P Ling, CH Masuda, K Matsubara, Y Muraki, Y Namba, S Ohnishi, K Philpott, L Rattenbury, NJ Saito, T Sullivan, DJ Sumi, T Sweatman, WL Suzuki, D Tristram, PJ Tsurumi, N Wada, K Yamai, N Yock, PCM Yonehara, A Szymanski, MK Ulaczyk, K Kozlowski, S Poleski, R Wyrzykowski, L Kubiak, M Pietrukowicz, P Pietrzynski, G Soszynski, I Bramich, DM Browne, P Jaimes, RF Horne, K Ipatov, S Kains, N Snodgrass, C Steele, IA Street, R Tsapras, Y AF Yee, J. C. Han, C. Gould, A. Skowron, J. Bond, I. A. Udalski, A. Hundertmark, M. Monard, L. A. G. Porritt, I. Nelson, P. Bozza, V. Albrow, M. D. Choi, J. -Y. Christie, G. W. Depoy, D. L. Gaudi, B. S. Hwang, K. -H. Jung, Y. K. Lee, C. -U. McCormick, J. Natusch, T. Ngan, H. Park, H. Pogge, R. W. Shin, I. -G. Tan, T. -G. Abe, F. Bennett, D. P. Botzler, C. S. Freeman, M. Fukui, A. Fukunaga, D. Itow, Y. Koshimoto, N. Larsen, P. Ling, C. H. Masuda, K. Matsubara, Y. Muraki, Y. Namba, S. Ohnishi, K. Philpott, L. Rattenbury, N. J. Saito, To. Sullivan, D. J. Sumi, T. Sweatman, W. L. Suzuki, D. Tristram, P. J. Tsurumi, N. Wada, K. Yamai, N. Yock, P. C. M. Yonehara, A. Szymanski, M. K. Ulaczyk, K. Kozlowski, S. Poleski, R. Wyrzykowski, L. Kubiak, M. Pietrukowicz, P. Pietrzynski, G. Soszynski, I. Bramich, D. M. Browne, P. Jaimes, R. Figuera Horne, K. Ipatov, S. Kains, N. Snodgrass, C. Steele, I. A. Street, R. Tsapras, Y. CA Tan, TG MOA Collaboration OGLE Collaboration ROBONET Collaboration TI MOA-2013-BLG-220Lb: MASSIVE PLANETARY COMPANION TO GALACTIC-DISK HOST SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing: micro; planetary systems ID JUPITER/SATURN ANALOG; MICROLENSING EVENTS; MOA-2011-BLG-293LB; PHOTOMETRY; SYSTEM; DWARF AB We report the discovery of MOA-2013-BLG-220Lb, which has a super-Jupiter mass ratio q = 3.01 +/- 0.02 x 10(-3) relative to its host. The proper motion, mu = 12.5 +/- 1 mas yr(-1), is one of the highest for microlensing planets yet discovered, implying that it will be possible to separately resolve the host within similar to 7 yr. Two separate lines of evidence imply that the planet and host are in the Galactic disk. The planet could have been detected and characterized purely with follow-up data, which has important implications for microlensing surveys, both current and into the Large Synoptic Survey Telescope (LSST) era. C1 [Yee, J. C.; Gould, A.; Gaudi, B. S.; Pogge, R. W.; Poleski, R.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Han, C.; Choi, J. -Y.; Hwang, K. -H.; Jung, Y. K.; Park, H.; Shin, I. -G.] Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea. [Skowron, J.; Udalski, A.; Szymanski, M. K.; Ulaczyk, K.; Kozlowski, S.; Poleski, R.; Wyrzykowski, L.; Kubiak, M.; Pietrukowicz, P.; Pietrzynski, G.; Soszynski, I.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Bond, I. A.; Ling, C. H.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, North Shore Mail Ctr, Auckland, New Zealand. [Hundertmark, M.; Browne, P.; Jaimes, R. Figuera; Horne, K.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Monard, L. A. G.] Klein Karoo Observ, Ctr Backyard Astrophys, Calitzdorp, South Africa. [Porritt, I.] Turitea Observ, Palmerston North, New Zealand. [Nelson, P.] Ellinbank Observ, Ellinbank, Vic, Australia. [Bozza, V.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84081 Baronissi, SA, Italy. [Bozza, V.] Inst Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy. [Albrow, M. D.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand. [Christie, G. W.; Natusch, T.] Auckland Observ, Auckland, New Zealand. [Depoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [McCormick, J.] Farm Cove Observ, Ctr Backyard Astrophys, Auckland, New Zealand. [Natusch, T.] AUT Univ, Inst Radio Astron & Space Res, Auckland, New Zealand. [Tan, T. -G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Abe, F.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Botzler, C. S.; Freeman, M.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1001, New Zealand. [Fukui, A.] Natl Inst Nat Sci, Natl Astron Observ Japan, Okayama Astrophys Observ, Kamogatacho, Okayama 7190232, Japan. [Koshimoto, N.; Namba, S.; Suzuki, D.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Larsen, P.; Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Philpott, L.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [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, Lake Tekapo 8770, New Zealand. [Yamai, N.; Yonehara, A.] Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kyoto 6038555, Japan. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Bramich, D. M.] Qatar Fdn, Qatar Environm & Energy Res Inst, Doha, Qatar. [Jaimes, R. Figuera; Kains, N.] European So Observ, D-85748 Garching, Germany. [Ipatov, S.] Qatar Fdn, Doha, Qatar. [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England. [Street, R.; Tsapras, Y.] La Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Tsapras, Y.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England. RP Yee, JC (reprint author), Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. RI Skowron, Jan/M-5186-2014; Hundertmark, Markus/C-6190-2015; Kozlowski, Szymon/G-4799-2013; Ipatov, Sergei/O-2302-2014; OI Skowron, Jan/0000-0002-2335-1730; Hundertmark, Markus/0000-0003-0961-5231; Kozlowski, Szymon/0000-0003-4084-880X; Ipatov, Sergei/0000-0002-1413-9180; Tan, Thiam-Guan/0000-0001-5603-6895; Snodgrass, Colin/0000-0001-9328-2905 FU Ohio State University; California Institute of Technology (Caltech) - NASA through the Sagan Fellowship Program; Creative Research Initiative Program of the National Research Foundation of Korea [2009-0081561]; NSF [AST 1103471]; NASA [NNX12AB99G]; European Research Council under the European Community's Seventh Framework Programme/ERC [246678]; NPRP [X-019-1-006]; [JSPS23340044]; [JSPS24253004] FX Work by J. C. Yee is supported in part by a Distinguished University Fellowship from The Ohio State University and in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. Work by CH was supported by the Creative Research Initiative Program (2009-0081561) of the National Research Foundation of Korea. Work by A.G. and B.S.G. was supported by NSF grant AST 1103471. Work by A.G., B.S.G., and R.W.P. was supported by NASA grant NNX12AB99G. T.S. acknowledges the support from the grant JSPS23340044 and JSPS24253004. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 246678 to AU. This publication was made possible by NPRP grant X-019-1-006 from the Qatar National Research Fund (a member of Qatar Foundation). NR 26 TC 6 Z9 6 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 14 DI 10.1088/0004-637X/790/1/14 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800014 ER PT J AU Zellem, RT Lewis, NK Knutson, HA Griffith, CA Showman, AP Fortney, JJ Cowan, NB Agol, E Burrows, A Charbonneau, D Deming, D Laughlin, G Langton, J AF Zellem, Robert T. Lewis, Nikole K. Knutson, Heather A. Griffith, Caitlin A. Showman, Adam P. Fortney, Jonathan J. Cowan, Nicolas B. Agol, Eric Burrows, Adam Charbonneau, David Deming, Drake Laughlin, Gregory Langton, Jonathan TI THE 4.5 mu m FULL-ORBIT PHASE CURVE OF THE HOT JUPITER HD 209458b SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; methods: numerical; planets and satellites: general; planets and satellites: individual (HD 209458b); techniques: photometric ID TIDALLY LOCKED EXOPLANETS; SPITZER-SPACE-TELESCOPE; TRANSIT LIGHT-CURVE; ATMOSPHERIC CIRCULATION; EXTRASOLAR PLANET; SECONDARY ECLIPSE; WARM SPITZER; DISEQUILIBRIUM CARBON; HEAT REDISTRIBUTION; THERMAL INVERSIONS AB The hot Jupiter HD 209458b is particularly amenable to detailed study as it is among the brightest transiting exoplanet systems currently known (V-mag = 7.65; K-mag = 6.308) and has a large planet-to-star contrast ratio. HD209458b is predicted to be in synchronous rotation about its host star with a hot spot that is shifted eastward of the substellar point by superrotating equatorial winds. Here we present the first full-orbit observations of HD 209458b, in which its 4.5 mu m emission was recorded with Spitzer/IRAC. Our study revises the previous 4.5 m measurement of HD 209458b's secondary eclipse emission downward by similar to 35% to 0.1391%(+0.0072%)(-0.0069%), changing our interpretation of the properties of its dayside atmosphere. We find that the hot spot on the planet's dayside is shifted eastward of the substellar point by 40 degrees.9 +/- 6 degrees.0, in agreement with circulation models predicting equatorial superrotation. HD 209458b's dayside (T-bright = 1499 +/- 15 K) and nightside (T-bright = 972 +/- 44 K) emission indicate a day-to-night brightness temperature contrast smaller than that observed for more highly irradiated exoplanets, suggesting that the day-to-night temperature contrast may be partially a function of the incident stellar radiation. The observed phase curve shape deviates modestly from global circulation model predictions potentially due to disequilibrium chemistry or deficiencies in the current hot CH4 line lists used in these models. Observations of the phase curve at additional wavelengths are needed in order to determine the possible presence and spatial extent of a dayside temperature inversion, as well as to improve our overall understanding of this planet's atmospheric circulation. C1 [Zellem, Robert T.; Griffith, Caitlin A.; Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Lewis, Nikole K.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Knutson, Heather A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Fortney, Jonathan J.; Laughlin, Gregory] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Cowan, Nicolas B.] Northwestern Univ, Inst Technol, Dept Earth & Planetary Sci, Evanston, IL 60208 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 USA. RP Zellem, RT (reprint author), Univ Arizona, Lunar & Planetary Lab, 1629 East Univ Blvd, Tucson, AZ 85721 USA. EM rzellem@lpl.arizona.edu OI Zellem, Robert/0000-0001-7547-0398 FU NASA Planetary Atmospheres Program; NASA through the Sagan Fellowship Program FX R.Z. and C.A.G. are supported by the NASA Planetary Atmospheres Program.; N.K.L. performed this work in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. NR 91 TC 42 Z9 42 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 53 DI 10.1088/0004-637X/790/1/53 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800053 ER PT J AU Ogburn, MB Roberts, PM Richie, KD Johnson, EG Hines, AH AF Ogburn, Matthew B. Roberts, Paige M. Richie, Kimberly D. Johnson, Eric G. Hines, Anson H. TI Temporal and spatial variation in sperm stores in mature female blue crabs Callinectes sapidus and potential effects on brood production in Chesapeake Bay SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Sperm limitation; Fisheries management; Sex ratio; Callinectes sapidus; Chesapeake Bay ID CHIONOECETES-OPILIO BRACHYURA; MALE MATING HISTORY; OF-SAINT-LAWRENCE; POPULATION-DYNAMICS; SPAWNING STOCK; NORTH-CAROLINA; SEMINAL FLUID; MALE SIZE; RATHBUN; COMPETITION AB Fisheries that selectively harvest males have the potential to diminish the reproductive success of females due to reductions in the transfer of sperm and seminal fluid during mating. The purposes of this study were to investigate variation in sperm and seminal fluid quantities obtained during mating in mature female blue crabs Callinectes sapidus in Chesapeake Bay, USA, and to model potential effects of sperm reduction on lifetime brood production. We explored variation in sperm and seminal fluid quantity with respect to (1) season, (2) location, (3) operational sex ratio (OSR), (4) relative time since mating, and (5) fertilization, and used this information to model brood production. Mature female blue crabs were obtained from targeted or long-term collection efforts. Crabs were characterized by carapace condition, presence of a sperm plug (hardened seminal fluid), and presence of egg masses or egg remnants. They were dissected and processed to determine the quantity of stored sperm and spermathecae weight. Sperm quantity, but not spermathecae weight, of recently mated females varied seasonally and spatially, and was positively correlated with OSR. Females received as many as 3 x 10(9) sperm during mating, which declined to an average of 8 x 10(7) sperm before fertilization of the first brood. Both model simulations and estimates of sperm used for fertilization derived from sperm counts of females with and without evidence of spawning indicated that a reduction in lifetime brood production (sperm limitation) is likely in individual female blue crabs if they survive to a second spawning season. C1 [Ogburn, Matthew B.; Roberts, Paige M.; Richie, Kimberly D.; Johnson, Eric G.; Hines, Anson H.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Johnson, Eric G.] Univ N Florida, Dept Biol, Jacksonville, FL 32224 USA. RP Ogburn, MB (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM ogburnm@si.edu OI Ogburn, Matthew/0000-0001-5417-555X FU NOAA's Chesapeake Bay Office Award [NA11 NMF4570230]; Smithsonian Institution Environmental Studies Program; SERC; Tennenbaum Marine Observatories; Smithsonian Women's Committee; NSF [OCE-9711843, OCE-97155]; Maryland Sea Grant Program; Phillips Seafood, Inc.; Disney Wildlife Conservation Fund FX We thank R. Aguilar, M. Goodison, M. Kramer and many watermen, technicians, and undergraduate interns who have helped with field collections and sample processing since 1996. The manuscript is significantly improved thanks to thoughtful comments from 4 anonymous reviewers. Support for our long-term study of reproductive biology and sperm limitation in blue crabs has been provided by NOAA's Chesapeake Bay Office Award #NA11 NMF4570230, the Smithsonian Institution Environmental Studies Program, the SERC Fellowship Program, Tennenbaum Marine Observatories, the Smithsonian Women's Committee, NSF Awards OCE-9711843 and OCE-97155, the Maryland Sea Grant Program, Phillips Seafood, Inc., and the Disney Wildlife Conservation Fund. NR 53 TC 4 Z9 4 U1 2 U2 14 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 JUL 17 PY 2014 VL 507 BP 249 EP 262 DI 10.3354/meps10869 PG 14 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA AO0EO UT WOS:000340982100019 ER PT J AU Foret, G Eremenko, M Cuesta, J Sellitto, P Barre, J Gaubert, B Coman, A Dufour, G Liu, X Joly, M Doche, C Beekmann, M AF Foret, G. Eremenko, M. Cuesta, J. Sellitto, P. Barre, J. Gaubert, B. Coman, A. Dufour, G. Liu, X. Joly, M. Doche, C. Beekmann, M. TI Ozone pollution: What can we see from space? A case study SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LOWERMOST TROPOSPHERIC OZONE; BOUNDARY-LAYER VENTILATION; GASEOUS DRY DEPOSITION; ATMOSPHERIC COMPOSITION; MONITORING INSTRUMENT; TRANSPORT MODEL; NEXT-GENERATION; DATA ASSIMILATION; CHEMISTRY; SATELLITE AB Due to its impact on environment, tropospheric ozone received particular attention since several decades. Ground-based networks associated with regional chemical transport models are used to monitor and forecast surface ozone concentrations, but coverage, representativeness, and accuracy issues remain important. Recent satellite observations have demonstrated the capacity to probe tropospheric ozone, but there has been no explicit attempt to quantify their ability to measure ozone pollution near ground. We propose here to assess the ability of ozone sounders to detect a photochemical ozone pollution event that is supposed to be a favorable situation for satellite detection. We have chosen ozone pollution event over Europe associated with a warm conveyor belt that efficiently transports photochemically produced ozone upward. Ozone satellite products from Global Ozone Monitoring Experiment-2, Infrared Atmospheric Sounding Interferometer (IASI), and Ozone Monitoring Instrument are analyzed here for their capacity to capture such an event. Also, in situ observations and regional chemical-transport models show increasing ozone concentrations in the continental and Mediterranean boundary layer and further transport to central Europe and Scandinavia associated with upward transport. Satellite observations do not detect high ozone concentrations within the boundary layer due the weak sensitivity near the surface. Nevertheless, we have shown that the IR sounder IASI was able to detect, qualitatively and quantitatively, the ozone plume transported upward by the warm conveyor belt, suggesting that a quantification of upward transport of ozone pollution could be possible using current satellite observations. This should encourage us to further explore approaches more sensitive to surface ozone (such as the multispectral approach) and to prepare the next generation of still more sensitive spaceborne instruments. C1 [Foret, G.; Eremenko, M.; Cuesta, J.; Sellitto, P.; Gaubert, B.; Coman, A.; Dufour, G.; Beekmann, M.] Univ Paris Diderot, Lab Interuniv Syst Atmospher, UMR7583, IPSL,CNRS,Univ Paris Est Creteil, Creteil, France. [Sellitto, P.] Ecole Normale Super, CNRS, Meteorol Dynam Lab, UMR8539,IPSL, Paris, France. [Barre, J.] Natl Ctr Atmospher Res, ACD, NESL, Boulder, CO 80307 USA. [Barre, J.; Joly, M.] CNRM GAME UMR 3589 CNRS Meteo France, Toulouse, France. [Liu, X.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Doche, C.] Meteo France DIRSO DEC FDF, Merignac, France. RP Foret, G (reprint author), Univ Paris Diderot, Lab Interuniv Syst Atmospher, UMR7583, IPSL,CNRS,Univ Paris Est Creteil, Creteil, France. EM foret@lisa.u-pec.fr RI Liu, Xiong/P-7186-2014 OI Liu, Xiong/0000-0003-2939-574X FU European Community's Seventh Framework Programme [SPA.2011.1.5-02, 283576]; project "IASI-TOSCA" (Terre, Ocean, Surfaces continentals, Atmosphere) - CNES FX The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7 THEME [SPA.2011.1.5-02]) under grant agreement n.283576, i.e., the MACC-II project. This study was supported by the project "IASI-TOSCA" (Terre, Ocean, Surfaces continentals, Atmosphere) financed by CNES. This work was granted access to the HPC resources of CCRT under the allocation 2013-6695 made by GENCI (Grand Equipement National de Calcul Intensif). IASI has been developed and built under the responsibility of the Centre National d'Etudes Spatiales (CNES, France). It is flown aboard the MetOp satellites as part of the EUMETSAT Polar System. We acknowledge the support by the data centers ETHER (http://www.pole-ether.fr/) and NOAA CLASS (http://www.class.ncdc.noaa.gov) for providing respectively L1 IASI and GOME-2 data sets, which are originally supplied by EUMETSAT through the Eumetcast system distribution (http://www.eumetsat.int). The Dutch-Finnish OMI instrument is part of the NASA EOS Aura satellite payload. The OMI Project is managed by NIVR and KNMI in the Netherlands. We acknowledge the OMI International Science Team for providing satellite data used in this study. X. Liu is funded by NASA and the Smithsonian Institution. This work is also part of the ADOMOCA-II project funded by the French LEFE program (CHAT/ASSIM). The authors gratefully acknowledge the NOAA Air Resources Laboratory (ARL) for the provision of the HYSPLIT transport and dispersion model and/or READY website (http://www.ready.noaa.gov) used in this publication. RMIB, MeteoSwiss, DWD-MOL, PIMWM, AEMET & KNMI. World Ozone and Ultraviolet Radiation Data Centre (WOUDC) [Data]. Retrieved in 2013, from http://www.woudc.org. The authors acknowledge the strong support of the European Commission, Airbus, and airlines-Lufthansa, Air France, Austrian, and former Sabenato-the MOZAIC program. NR 85 TC 4 Z9 4 U1 2 U2 41 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2014 VL 119 IS 13 AR 2013JD021340 DI 10.1002/2013JD021340 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN2IK UT WOS:000340408000041 ER PT J AU Carter, JL Brezinski, DK Kollar, AD Dutro, JT AF Carter, John L. Brezinski, David K. Kollar, Albert D. Dutro, J. Thomas, Jr. TI BRACHIOPODA TAXONOMY AND BIOSTRATIGRAPHY OF THE REDWALL LIMESTONE (LOWER MISSISSIPPIAN) OF ARIZONA SO ANNALS OF CARNEGIE MUSEUM LA English DT Article DE Biostratigraphy; brachiopods; Mississippian; Redwall Limestone ID GENERA; EAST AB Forty-six species, assignable to 36 brachiopod genera, are recognized, described, and illustrated from the Lower Mississippian Redwall Limestone of northern Arizona. Seven new species are recognized, four of which are named. Named species are: Spinocarinifera (Seminucella) costatula, new species; Magnumbonella ampla, new species; Setigerites gutschicki, new species; and Spirifer redwallensis, new species. The remaining three newly recognized species remain in open nomenclature because study material was too poorly preserved to justify naming. The majority of brachiopod species studied were recovered from the Thunder Springs and Mooney Falls members near the middle of the formation. The basal Whitmore Wash Member and uppermost Horseshoe Mesa Member contain only sparse and poorly preserved brachiopod material. The spotty stratigraphic distribution of collections, which were recovered from largely geographically disparate locations, resulted in the creation of a stratigraphic range chart that exhibits no recognizable segregation into any potential brachiopod zones. Many of the Redwall Limestone's brachiopod species are known from contemporaneous formations elsewhere in the Cordillera or central United States. Biostratigraphically key species such as Marginatia fernglenensis (Weller, 1909), Marginatia burlingtonensis (Hall, 1858), Stegacanthia bowsheri Muir-Wood and Cooper, 1960, Fernglenia vernonensis (Swallow, 1860), Voiseyella novamexicana (Miller, 1881), and Punctospirifer subtexta (White, 1862), indicate that much of the Thunder Springs and Mooney Falls members is correlative with latest Kinderhookian (late Tournaisian) through latest Osagean (early Vis an) formations of the American Midcontinent. These correlations indicate that the Redwall Limestone is temporally equivalent to the Fern Glen-Burlington formations of the central United States. These correlations are consistent with other Redwall forms that are biostratigraphially useful, such as foraminifers. C1 [Carter, John L.] Carnegie Museum Nat Hist, Sect Invertebrate Paleontol, Mt Pleasant, SC 29466 USA. [Brezinski, David K.] Maryland Geol Survey, Carnegie Museum Nat Hist, Sect Invertebrate Paleontol, Baltimore, MD 21218 USA. [Kollar, Albert D.] Carnegie Museum Nat Hist, Sect Invertebrate Paleontol, Pittsburgh, PA 15213 USA. [Dutro, J. Thomas, Jr.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Carter, JL (reprint author), Carnegie Museum Nat Hist, Sect Invertebrate Paleontol, 171 Blalock St, Mt Pleasant, SC 29466 USA. EM rccats13@comcast.net; david.brezinski@maryland.gov; kollara@carnegiemnh.org FU Carnegie Museum of Natural History Graham Netting Field Fund FX We would like to thank Colleen Hyde of the Grand Canyon National Park for access to park collections. John Pojeta of the U. S. National Museum provided help in locating the Grand Canyon National Park collections housed in the USNM. Carnegie Museum of Natural History Graham Netting Field Fund provided for several earlier collecting trips. Special thanks are owed Carla A. Kertis who provided careful and exhausting editing of the manuscript at every level. Norman Samways conducted biometric studies. We would also like to thank an anonymous reviewer for their helpful suggestions. NR 142 TC 0 Z9 0 U1 1 U2 2 PU CARNEGIE MUSEUM NATURAL HISTORY PI PITTSBURGH PA 4400 FORBES AVE, PITTSBURGH, PA 15213 USA SN 0097-4463 EI 1943-6300 J9 ANN CARNEGIE MUS JI Ann. Carnegie Mus. PD JUL 15 PY 2014 VL 82 IS 3 BP 257 EP 289 PG 33 WC Paleontology; Zoology SC Paleontology; Zoology GA AN5JB UT WOS:000340625600005 ER PT J AU Gremillion, KJ Barton, L Piperno, DR AF Gremillion, Kristen J. Barton, Loukas Piperno, Dolores R. TI Reply to Smith: On distinguishing between models, hypotheses, and theoretical frameworks SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 [Gremillion, Kristen J.] Ohio State Univ, Dept Anthropol, Columbus, OH 43210 USA. [Barton, Loukas] Univ Pittsburgh, Dept Anthropol, Pittsburgh, PA 15260 USA. [Piperno, Dolores R.] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. [Piperno, Dolores R.] Smithsonian Trop Res Inst, Panama City, Panama. RP Gremillion, KJ (reprint author), Ohio State Univ, Dept Anthropol, Columbus, OH 43210 USA. EM gremillion.1@osu.edu NR 5 TC 1 Z9 1 U1 0 U2 9 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JUL 15 PY 2014 VL 111 IS 28 BP E2830 EP E2830 DI 10.1073/pnas.1408909111 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AL2WG UT WOS:000338985700004 PM 25157385 ER PT J AU Gremillion, KJ Barton, L Piperno, DR AF Gremillion, Kristen J. Barton, Loukas Piperno, Dolores R. TI Reply to Zeder: Maintaining a diverse scientific toolkit is not an act of faith SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter ID ORIGINS C1 [Gremillion, Kristen J.] Ohio State Univ, Dept Anthropol, Columbus, OH 43210 USA. [Barton, Loukas] Univ Pittsburgh, Dept Anthropol, Pittsburgh, PA 15260 USA. [Piperno, Dolores R.] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. [Piperno, Dolores R.] Smithsonian Trop Res Inst, Panama City, Panama. RP Gremillion, KJ (reprint author), Ohio State Univ, Dept Anthropol, Columbus, OH 43210 USA. EM gremillion.1@osu.edu NR 4 TC 1 Z9 1 U1 0 U2 7 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JUL 15 PY 2014 VL 111 IS 28 BP E2828 EP E2828 DI 10.1073/pnas.1409072111 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AL2WG UT WOS:000338985700002 PM 25157384 ER PT J AU Smith, BD AF Smith, Bruce D. TI Failure of optimal foraging theory to appeal to researchers working on the origins of agriculture worldwide SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. RP Smith, BD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. EM smithb@si.edu NR 5 TC 4 Z9 4 U1 1 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 JUL 15 PY 2014 VL 111 IS 28 BP E2829 EP E2829 DI 10.1073/pnas.1408208111 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AL2WG UT WOS:000338985700003 PM 24979801 ER PT J AU Zeder, MA AF Zeder, Melinda A. TI Alternative to faith-based science SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. RP Zeder, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. EM zederm@si.edu NR 5 TC 5 Z9 5 U1 1 U2 7 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JUL 15 PY 2014 VL 111 IS 28 BP E2827 EP E2827 DI 10.1073/pnas.1408209111 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AL2WG UT WOS:000338985700001 PM 24946802 ER PT J AU Muller, A Schippers, S Phaneuf, RA Scully, SWJ Aguilar, A Cisneros, C Gharaibeh, MF Schlachter, AS McLaughlin, BM AF Mueller, A. Schippers, S. Phaneuf, R. A. Scully, S. W. J. Aguilar, A. Cisneros, C. Gharaibeh, M. F. Schlachter, A. S. McLaughlin, B. M. TI K-shell photoionization of Be-like boron (B+) ions: experiment and theory SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article DE K-shell; photoionization; boron ID PHOTOABSORPTION CROSS-SECTIONS; ELECTRON-IMPACT IONIZATION; DOUBLY-EXCITED RESONANCES; RESOLUTION AUGER-SPECTRA; SINGLE GAS COLLISIONS; R-MATRIX THEORY; ATOMIC IONS; IONIZED BORON; SPECTROSCOPY; FLUORESCENCE AB Absolute cross sections for the K-shell photoionization of Be-like boron ions were measured with the ion-photon merged-beams technique at the Advanced Light Source synchrotron radiation facility. High-resolution spectroscopy with E/Delta E up to 8800 (Delta E similar to 22 meV) covered the energy ranges 193.7-194.7 eV and 209-215 eV. Lifetimes of the strongest resonances are determined with relative uncertainties down to approximately 4% for the broadest resonance. The measured resonance strengths are consistent with 60% 1s(2)2s(2) S-1 ground-state and 40% 1s(2)2s2p P-3(o) metastable-state ions in the primary ion beam and confirmed by comparison with independent absolute photo-recombination heavy-ion storage-ring measurements with B2+ ions using the principle of detailed balance. Experimental determination of the line width for the 1s2s(2)2p P-1(o) resonance gives a value of 47 +/- 2 meV and compares favourably to a theoretical estimate of 47 meV from the R-matrix with pseudo-states (RMPS) method. The measured line widths of the 1s2s2p(2) P-3, D-3 resonances are 10.0 +/- 2 meV and 32 +/- 3 meV, respectively, compared to RMPS theoretical estimates of 9 meV and 34 meV. C1 [Mueller, A.; Schippers, S.] Univ Giessen, Inst Atom & Mol Phys, D-35390 Giessen, Germany. [Phaneuf, R. A.; Scully, S. W. J.; Aguilar, A.; Gharaibeh, M. F.] Univ Nevada, Dept Phys, Reno, NV 89557 USA. [Aguilar, A.; Schlachter, A. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA. [Cisneros, C.] Univ Nacl Autonoma Mexico, Ctr Ciencias Fis, Cuernavaca 62131, Morelos, Mexico. [McLaughlin, B. M.] Queens Univ Belfast, Sch Math & Phys, CTAMOP, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Muller, A (reprint author), Univ Giessen, Inst Atom & Mol Phys, D-35390 Giessen, Germany. EM Alfred.Mueller@iamp.physik.uni-giessen.de; b.mclaughlin@qub.ac.uk RI Muller, Alfred/A-3548-2009; Schippers, Stefan/A-7786-2008 OI Muller, Alfred/0000-0002-0030-6929; Schippers, Stefan/0000-0002-6166-7138 FU Deutsche Forschungsgemeinschaft [Mu 1068/10]; NATO [976362]; US Department of Energy (DOE) [DE-AC03-76SF-00098, DE-FG02-03ER15424]; PAPIT-UNAM, Mexico [IN107912-IN102613]; US National Science Foundation; Queen's University Belfast; National Science Foundation [OCI-1053575]; Office of Science, Office of Basic Energy Sciences, of the US Department of Energy [DE-AC02-05CH11231] FX We acknowledge support by Deutsche Forschungsgemeinschaft under project number Mu 1068/10 and through NATO Collaborative Linkage grant 976362 as well as by the US Department of Energy (DOE) under contract DE-AC03-76SF-00098 and grant DE-FG02-03ER15424. C Cisneros acknowledges support from PAPIT-UNAM IN107912-IN102613, Mexico. B M McLaughlin acknowledges support by the US National Science Foundation through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics, a visiting research fellowship from Queen's University Belfast and the hospitality of AM and SS during a recent visit to Giessen. We thank John C Raymond and Randall K Smith from the Harvard Smithsonian Center for Astrophysics for helpful discussions on the astrophysical applications. The computational work was carried out at the National Energy Research Scientific Computing Center in Oakland, CA, USA, the Kraken XT5 facility at the National Institute for Computational Science (NICS) in Knoxville, TN, USA and at the High Performance Computing Center Stuttgart (HLRS) of the University of Stuttgart, Stuttgart, Germany. We thank Stefan Andersson from Cray Research for his assistance and advice with the implementation and optimization of the parallel R-matrix codes on the Cray-XE6 at HLRS. The Kraken XT5 facility is a resource of the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number OCI-1053575. 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 93 TC 9 Z9 9 U1 0 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 JUL 14 PY 2014 VL 47 IS 13 AR 135201 DI 10.1088/0953-4075/47/13/135201 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AK9WU UT WOS:000338780100003 ER PT J AU McKinney, JC Tchekhovskoy, A Sadowski, A Narayan, R AF McKinney, Jonathan C. Tchekhovskoy, Alexander Sadowski, Aleksander Narayan, Ramesh TI Three-dimensional general relativistic radiation magnetohydrodynamical simulation of super-Eddington accretion, using a new code harmrad with M1 closure SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; black hole physics; gravitation; hydrodynamics; MHD; methods: numerical ID BLACK-HOLE ACCRETION; ADVECTION-DOMINATED ACCRETION; RUNGE-KUTTA SCHEMES; SLIM-DISK MODEL; X-RAY BINARIES; MAGNETIC-FIELD GEOMETRY; HEAT-TRANSFER EQUATIONS; SAGITTARIUS-A-ASTERISK; FLUX-LIMITED DIFFUSION; ACTIVE GALACTIC NUCLEI AB Black hole (BH) accretion flows and jets are dynamic hot relativistic magnetized plasma flows whose radiative opacity can significantly affect flow structure and behaviour. We describe a numerical scheme, tests, and an astrophysically relevant application using the M1 radiation closure within a new 3D general relativistic radiation magnetohydrodynamics (GRRMHD) massively parallel code called harmrad. Our 3D GRRMHD simulation of super-Eddington accretion (about 20 times Eddington) on to a rapidly rotating BH (dimensionless spin j = 0.9375) shows sustained non-axisymmemtric disc turbulence, a persistent electromagnetic jet driven by the Blandford-Znajek effect, a disc wind, and a polar radiation jet. The total accretion efficiency is of the order of 20 per cent, the large-scale electromagnetic jet efficiency is of the order of 10 per cent, the disc wind efficiency is less than 1 per cent, and the total radiative efficiency remains low at only of the order of 1 per cent (of order the Eddington luminosity). However, the radiation jet and the electromagnetic jet both emerge from a geometrically beamed polar region, with super-Eddington isotropic equivalent luminosities. Such simulations with harmrad can enlighten the role of BH spin versus discs in launching jets, help determine the origin of spectral and temporal states in X-ray binaries, help to understand how tidal disruption events work, provide an accurate horizon-scale flow structure for M87 and other active galactic nuclei (AGN), and isolate whether AGN feedback is driven by radiation or by an electromagnetic, thermal, or kinetic wind/jet. For example, the low radiative efficiency and weak BH spin-down rate from our simulation suggest that BH growth over cosmological times to billions of solar masses by redshifts of z similar to 6-8 is achievable even with rapidly rotating BHs and 10 M-aS (TM) BH seeds. C1 [McKinney, Jonathan C.] Univ Maryland, Dept Phys, Joint Space Sci Inst, College Pk, MD 20742 USA. [Tchekhovskoy, Alexander] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Tchekhovskoy, Alexander] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Sadowski, Aleksander; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02134 USA. RP McKinney, JC (reprint author), Univ Maryland, Dept Phys, Joint Space Sci Inst, 1117 John S Toll Bldg 082, College Pk, MD 20742 USA. EM jcm@umd.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NSF [AST1312651]; NASA through Einstein Fellowship Programme [PF3-140115]; NICS Kraken and Nautilus [TG-PHY120005, TG-AST100040, TG-AST080026N]; NASA via High-End Computing (HEC) Program through NASA Advanced Supercomputing (NAS) Division at Ames Research Center FX We thank James M. Stone and Omer Blaes for useful discussions. RN and AS were supported in part by NSF grant AST1312651. AT was supported by NASA through the Einstein Fellowship Programme, grant PF3-140115. We acknowledge NSF support via XSEDE resources, NICS Kraken and Nautilus under grant numbers TG-PHY120005 (JCM), TG-AST100040 (AT), TG-AST080026N (RN and AS), and NASA support via High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center (JCM, AS, and RN) that provided access to the Pleiades supercomputer. NR 192 TC 69 Z9 69 U1 1 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2014 VL 441 IS 4 BP 3177 EP 3208 DI 10.1093/mnras/stu762 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RP UT WOS:000338764700029 ER PT J AU Avila, S Knebe, A Pearce, FR Schneider, A Srisawat, C Thomas, PA Behroozi, P Elahi, PJ Han, JX Mao, YY Onions, J Rodriguez-Gomez, V Tweed, D AF Avila, Santiago Knebe, Alexander Pearce, Frazer R. Schneider, Aurel Srisawat, Chaichalit Thomas, Peter A. Behroozi, Peter Elahi, Pascal J. Han, Jiaxin Mao, Yao-Yuan Onions, Julian Rodriguez-Gomez, Vicente Tweed, Dylan TI SUSSING MERGER TREES: the influence of the halo finder SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: evolution; galaxies: haloes; dark matter ID ACTIVE GALACTIC NUCLEI; DARK-MATTER HALOES; COMPARISON PROJECT; GALAXY FORMATION; BLACK-HOLES; MODELS; SUBHALOES; CLUSTER; LIVES; NOTTS AB Merger tree codes are routinely used to follow the growth and merger of dark matter haloes in simulations of cosmic structure formation. Whereas in Srisawat et. al. we compared the trees built using a wide variety of such codes, here we study the influence of the underlying halo catalogue upon the resulting trees. We observe that the specifics of halo finding itself greatly influences the constructed merger trees. We find that the choices made to define the halo mass are of prime importance. For instance, amongst many potential options different finders select self-bound objects or spherical regions of defined overdensity, decide whether or not to include substructures within the mass returned and vary in their initial particle selection. The impact of these decisions is seen in tree length (the period of time a particularly halo can be traced back through the simulation), branching ratio (essentially the merger rate of subhaloes) and mass evolution. We therefore conclude that the choice of the underlying halo finder is more relevant to the process of building merger trees than the tree builder itself. We also report on some built-in features of specific merger tree codes that (sometimes) help to improve the quality of the merger trees produced. C1 [Avila, Santiago; Knebe, Alexander] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, E-28049 Madrid, Spain. [Avila, Santiago] Univ Autonoma Madrid, UAM CSIC, Inst Fis Teor, E-28049 Madrid, Spain. [Pearce, Frazer R.; Onions, Julian] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Schneider, Aurel; Srisawat, Chaichalit; Thomas, Peter A.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Behroozi, Peter; Mao, Yao-Yuan] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Elahi, Pascal J.] Univ Sydney, Sydney Inst Astron, Sydney, NSW 2016, Australia. [Han, Jiaxin] Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Han, Jiaxin] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Rodriguez-Gomez, Vicente] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tweed, Dylan] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Tweed, Dylan] Shanghai Jiao Tong Univ, Dept Phys & Astron, Ctr Astron & Astrophys, Shanghai 200240, Peoples R China. RP Avila, S (reprint author), Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, Modulo C-15, E-28049 Madrid, Spain. EM santiagoavilaperez@gmail.com RI Knebe, Alexander/N-1815-2014; OI Mao, Yao-Yuan/0000-0002-1200-0820; Schneider, Aurel/0000-0001-7055-8104; Rodriguez-Gomez, Vicente/0000-0002-9495-0079; Knebe, Alexander/0000-0003-4066-8307; Onions, Julian/0000-0001-5192-6856; Pearce, Frazer/0000-0002-2383-9250 FU European Commission through Marie Curie Initial Training Network CosmoComp [PITN-GA-2009-238356]; Universidad Autonoma de Madrid; University of Western Australia; Ministerio de Economia y Competitividad (MINECO) in Spain [AYA2012-31101]; Spanish Ministerio de Ciencia e Innovacion (MICINN) [CSD2009-00064]; Australian Research Council (ARC) [DP130100117, DP140100198]; Giacconi Fellowship through Space Telescope Science Institute under NASA [NAS5-26555]; SSimPL programme; Sydney Institute for Astronomy (SIfA); STFC; The Development and Promotion of Science and Technology Talents Project (DPST), Thailand; Science and Technology Facilities Council [ST/I000976/1]; Weiland Family Stanford Graduate Fellowship; [AYA2009-13936-C06-06]; [FPA2012-39684-C03-02]; [SEV-2012-0249] FX The SUSSING MERGER TREES Workshop was supported by the European Commission's Framework Programme 7, through the Marie Curie Initial Training Network CosmoComp (PITN-GA-2009-238356). This also provided fellowship support for AS.; SA is supported by a PhD fellowship from the Universidad Autonoma de Madrid and the Spanish ministerial grants AYA2009-13936-C06-06, AYA2009-13936-C06-06, FPA2012-39684-C03-02 and SEV-2012-0249. He also acknowledges the support of the University of Western Australia through their Research Collaboration Award 2014 scheme and thanks its International Centre for Radio Astronomy Research (and especially Chris Power) for the hospitality during the final stages of the paper writing.; AK is supported by the Ministerio de Economia y Competitividad (MINECO) in Spain through grant AYA2012-31101 as well as the Consolider-Ingenio 2010 Programme of the Spanish Ministerio de Ciencia e Innovacion (MICINN) under grant MultiDark CSD2009-00064. He also acknowledges support from the Australian Research Council (ARC) grants DP130100117 and DP140100198. He further thanks Belle & Sebastian for tigermilk.; PSB is funded by a Giacconi Fellowship through the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.; PJE is supported by the SSimPL programme and the Sydney Institute for Astronomy (SIfA).; JXH is supported by an STFC Rolling Grant to the Institute for Computational Cosmology, Durham University.; CS is supported by The Development and Promotion of Science and Technology Talents Project (DPST), Thailand.; PAT acknowledges support from the Science and Technology Facilities Council (grant number ST/I000976/1).; YYM received support from the Weiland Family Stanford Graduate Fellowship. NR 27 TC 12 Z9 12 U1 0 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2014 VL 441 IS 4 BP 3488 EP 3501 DI 10.1093/mnras/stu799 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RP UT WOS:000338764700047 ER PT J AU Zapata, LA Arce, HG Brassfield, E Palau, A Patel, N Pineda, JE AF Zapata, Luis A. Arce, Hector G. Brassfield, Erin Palau, Aina Patel, Nimesh Pineda, Jaime E. TI A spider-like outflow in Barnard 5-IRS 1: the transition from a collimated jet to a wide-angle outflow? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: formation; ISM: individual objects: Barnard 5-IRS1; ISM: individual objects: HH 366 VLA 1; ISM: jets and outflows ID DRIVEN MOLECULAR OUTFLOW; HUBBLE-SPACE-TELESCOPE; HERBIG-HARO OBJECTS; PROPER MOTIONS; BIPOLAR OUTFLOWS; YOUNG STARS; CO OUTFLOW; EVOLUTION; EMISSION; IMAGES AB We present line and continuum observations made with the Submillimeter Array of the young stellar object Barnard 5 - IRS1 located in the Perseus molecular cloud. Our (CO)-C-12(2-1) line observations resolve the high-velocity bipolar north-east-south-west outflow associated with this source. We find that the outflowing gas shows different structures at three different velocity regimes, in both lobes, resulting in a spider-like morphology. In addition to the low-velocity, cone-like (wide-angle) lobes that have previously been observed, we report the presence of intermediate-velocity parabolic shells emerging very close to the Class I protostar, as well as high-velocity molecular bullets that appear to be associated with the optical/IR jet emanating from this source. These compact high-velocity features reach radial velocities of about 50 km s(-1) away from the cloud velocity. We interpret that the peculiar spider-like morphology is a result of the molecular material being entrained by a wind with both a collimated jet-like component and a wide-angle component. We suggest that the outflow is in a transitional evolutionary phase between a mostly jet-driven flow and an outflow in which the entrainment is dominated by the wide-angle wind component. We also detect 1300 mu m continuum emission at the position of the protostar, which likely arises from the dusty envelope and disc surrounding the protostar. Finally, we report the detection of (CO)-C-13(2-1) and SO(6(5)-5(4)) emission arising from the outflow and the location of the young stellar object. C1 [Zapata, Luis A.] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Brassfield, Erin; Patel, Nimesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Palau, Aina] Inst Ciencies Espai CSIC IEEC, Fac Ciencies, E-08193 Bellaterra, Catalunya, Spain. [Pineda, Jaime E.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. RP Zapata, LA (reprint author), UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. EM lzapata@crya.unam.mx OI Pineda, Jaime/0000-0002-3972-1978 FU DGAPA; UNAM; CONACyT, Mexico; NSF [AST-0845619]; Spanish MICINN [AYA2011-30228-C03-02]; AGAUR grant (Catalonia) [2009SGR1172]; FEDER FX LAZ acknowledge the financial support from DGAPA, UNAM, and CONACyT, Mexico. HGA acknowledges support from his NSF CAREER award AST-0845619. AP is supported by the Spanish MICINN grant AYA2011-30228-C03-02 (co-funded with FEDER funds) and by the AGAUR grant 2009SGR1172 (Catalonia). NR 46 TC 5 Z9 5 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 JUL 11 PY 2014 VL 441 IS 4 BP 3696 EP 3702 DI 10.1093/mnras/stu810 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RP UT WOS:000338764700066 ER PT J AU Kleint, L Antolin, P Tian, H Judge, P Testa, P De Pontieu, B Martinez-Sykora, J Reeves, KK Wuelser, JP McKillop, S Saar, S Carlsson, M Boerner, P Hurlburt, N Lemen, J Tarbell, TD Title, A Golub, L Hansteen, V Jaeggli, S Kankelborg, C AF Kleint, L. Antolin, P. Tian, H. Judge, P. Testa, P. De Pontieu, B. Martinez-Sykora, J. Reeves, K. K. Wuelser, J. P. McKillop, S. Saar, S. Carlsson, M. Boerner, P. Hurlburt, N. Lemen, J. Tarbell, T. D. Title, A. Golub, L. Hansteen, V. Jaeggli, S. Kankelborg, C. TI DETECTION OF SUPERSONIC DOWNFLOWS AND ASSOCIATED HEATING EVENTS IN THE TRANSITION REGION ABOVE SUNSPOTS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: transition region; sunspots ID IMAGING-SPECTROGRAPH; THERMAL-INSTABILITY; CORONAL LOOPS; SOLAR CORONA; PROMINENCES; FLOWS; OSCILLATIONS; VELOCITIES; TELESCOPE; RAIN AB Interface Region Imaging Spectrograph data allow us to study the solar transition region (TR) with an unprecedented spatial resolution of 0 ''.33. On 2013 August 30, we observed bursts of high Doppler shifts suggesting strong supersonic downflows of up to 200 km s(-1) and weaker, slightly slower upflows in the spectral lines Mg II h and k, C II 1336, Si IV 1394 angstrom, and 1403 angstrom, that are correlated with brightenings in the slitjaw images (SJIs). The bursty behavior lasts throughout the 2 hr observation, with average burst durations of about 20 s. The locations of these short-lived events appear to be the umbral and penumbral footpoints of EUV loops. Fast apparent downflows are observed along these loops in the SJIs and in the Atmospheric Imaging Assembly, suggesting that the loops are thermally unstable. We interpret the observations as cool material falling from coronal heights, and especially coronal rain produced along the thermally unstable loops, which leads to an increase of intensity at the loop footpoints, probably indicating an increase of density and temperature in the TR. The rain speeds are on the higher end of previously reported speeds for this phenomenon, and possibly higher than the free-fall velocity along the loops. On other observing days, similar bright dots are sometimes aligned into ribbons, resembling small flare ribbons. These observations provide a first insight into small-scale heating events in sunspots in the TR. C1 [Kleint, L.; Martinez-Sykora, J.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA. [Kleint, L.; De Pontieu, B.; Martinez-Sykora, J.; Wuelser, J. P.; Boerner, P.; Hurlburt, N.; Lemen, J.; Tarbell, T. D.; Title, A.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Kleint, L.] Univ Appl Sci & Arts Northwestern Switzerland, CH-5210 Windisch, Switzerland. [Antolin, P.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Tian, H.; Testa, P.; Reeves, K. K.; McKillop, S.; Saar, S.; Golub, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Judge, P.] High Altitude Observ NCAR, Boulder, CO 80307 USA. [Carlsson, M.; Hansteen, V.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Jaeggli, S.; Kankelborg, C.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. RP Kleint, L (reprint author), Bay Area Environm Res Inst, 625 2nd St,Ste 209, Petaluma, CA 94952 USA. EM lucia.kleint@fhnw.ch RI Reeves, Katharine/P-9163-2014; OI Antolin, Patrick/0000-0003-1529-4681 FU Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract 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 the Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract. NR 27 TC 17 Z9 17 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 JUL 10 PY 2014 VL 789 IS 2 AR L42 DI 10.1088/2041-8205/789/2/L42 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5DS UT WOS:000339876800017 ER PT J AU Dumusque, X Bonomo, AS Haywood, RD Malavolta, L Segransan, D Buchhave, LA Cameron, AC Latham, DW Molinari, E Pepe, F Udry, S Charbonneau, D Cosentino, R Dressing, CD Figueira, P Fiorenzano, AFM Gettel, S Harutyunyan, A Horne, K Lopez-Morales, M Lovis, C Mayor, M Micela, G Motalebi, F Nascimbeni, V Phillips, DF Piotto, G Pollacco, D Queloz, D Rice, K Sasselov, D Sozzetti, A Szentgyorgyi, A Watson, C AF Dumusque, Xavier Bonomo, Aldo S. Haywood, Raphaelle D. Malavolta, Luca Segransan, Damien Buchhave, Lars A. Cameron, Andrew Collier Latham, David W. Molinari, Emilio Pepe, Francesco Udry, Stephane Charbonneau, David Cosentino, Rosario Dressing, Courtney D. Figueira, Pedro Fiorenzano, Aldo F. M. Gettel, Sara Harutyunyan, Avet Horne, Keith Lopez-Morales, Mercedes Lovis, Christophe Mayor, Michel Micela, Giusi Motalebi, Fatemeh Nascimbeni, Valerio Phillips, David F. Piotto, Giampaolo Pollacco, Don Queloz, Didier Rice, Ken Sasselov, Dimitar Sozzetti, Alessandro Szentgyorgyi, Andrew Watson, Chris TI THE KEPLER-10 PLANETARY SYSTEM REVISITED BY HARPS-N: A HOT ROCKY WORLD AND A SOLID NEPTUNE-MASS PLANET SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (Kepler-10 KOI-072 KIC 11904151); stars: statistics; techniques: photometric; techniques: spectroscopic ID LIMB-DARKENING COEFFICIENTS; MAIN-SEQUENCE STARS; CHAIN MONTE-CARLO; 100 EARTH MASSES; TRANSITING PLANET; EXTRASOLAR PLANETS; MULTIPLE SYSTEM; LIGHT CURVES; SUPER-EARTHS; STELLAR AB Kepler-10b was the first rocky planet detected by the Kepler satellite and confirmed with radial velocity follow-up observations from Keck-HIRES. The mass of the planet was measured with a precision of around 30%, which was insufficient to constrain models of its internal structure and composition in detail. In addition to Kepler-10b, a second planet transiting the same star with a period of 45 days was statistically validated, but the radial velocities were only good enough to set an upper limit of 20 M-circle plus for the mass of Kepler-10c. To improve the precision on the mass for planet b, the HARPS-N Collaboration decided to observe Kepler-10 intensively with the HARPS-N spectrograph on the Telescopio Nazionale Galileo on La Palma. In total, 148 high-quality radial-velocity measurements were obtained over two observing seasons. These new data allow us to improve the precision of the mass determination for Kepler-10b to 15%. With a mass of 3.33 +/- 0.49 M-circle plus and an updated radius of 1.47(-0.02)(+0.03) R-circle plus, Kepler-10b has a density of 5.8 +/- 0.8 g cm(-3), very close to the value predicted by models with the same internal structure and composition as the Earth. We were also able to determine a mass for the 45-day period planet Kepler-10c, with an even better precision of 11%. With a mass of 17.2 +/- 1.9 M-circle plus and radius of 2.35(-0.04)(+0.09) R-circle plus, Kepler-10c has a density of 7.1 +/- 1.0 g cm(-3). Kepler-10c appears to be the first strong evidence of a class of more massive solid planets with longer orbital periods. C1 [Dumusque, Xavier; Buchhave, Lars A.; Latham, David W.; Charbonneau, David; Dressing, Courtney D.; Gettel, Sara; Lopez-Morales, Mercedes; Phillips, David F.; Sasselov, Dimitar; Szentgyorgyi, Andrew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bonomo, Aldo S.; Sozzetti, Alessandro] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, Italy. [Haywood, Raphaelle D.; Cameron, Andrew Collier; Horne, Keith] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Malavolta, Luca; Piotto, Giampaolo] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35122 Padua, Italy. [Malavolta, Luca; Nascimbeni, Valerio; Piotto, Giampaolo] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Segransan, Damien; Pepe, Francesco; Udry, Stephane; Lovis, Christophe; Mayor, Michel; Motalebi, Fatemeh; Queloz, Didier] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Molinari, Emilio; Cosentino, Rosario; Fiorenzano, Aldo F. M.; Harutyunyan, Avet] INAF Fdn Galileo Galilei, E-38712 Brea Baja, Spain. [Molinari, Emilio] INAF IASF, I-20133 Milan, Italy. [Figueira, Pedro] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Micela, Giusi] INAF Osservatorio Astron Palermo, I-90124 Palermo, Italy. [Pollacco, Don] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Queloz, Didier] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Rice, Ken] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Watson, Chris] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. RP Dumusque, X (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM xdumusque@cfa.harvard.edu RI Rice, Ken/H-5084-2011; Figueira, Pedro/J-4916-2013; OI Rice, Ken/0000-0002-6379-9185; Figueira, Pedro/0000-0001-8504-283X; Micela, Giuseppina/0000-0002-9900-4751; Molinari, Emilio/0000-0002-1742-7735; Sozzetti, Alessandro/0000-0002-7504-365X; Cameron, Andrew/0000-0002-8863-7828; Buchhave, Lars A./0000-0003-1605-5666; Piotto, Giampaolo/0000-0002-9937-6387 FU Prodex Program of the Swiss Space Office (SSO); Harvard University Origin of Life Initiative (HUOLI); Scottish Universities Physics Alliance (SUPA); University of Geneva; Smithsonian Astrophysical Observatory (SAO); Italian National Astrophysical Institute (INAF); University of St. Andrews; Queens University Belfast; University of Edinburgh; European Union Seventh Framework Programme (ETAEARTH) [313014]; Swiss National Science Foundation (SNSF) through an Early Postdoc Mobility fellowship; Fundacao para a Ciencia e a Tecnologia (FCT) through the Investigador FCT [IF/01037/2013]; FEDER through the program "Programa Operacional de Factores de Competitividade - COMPETE"; STFC postgraduate research studentship; John Templeton Foundation; Italian Ministero dellIstruzione; Universita e Ricerca (MIUR) within the Piano Operativo Nazionale Ricerca Scientifica, Sviluppo Tecnologico, Alta Formazione [PON 20002006] FX The HARPS-N project was funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origin of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), and the Italian National Astrophysical Institute (INAF), University of St. Andrews, Queens University Belfast, and University of Edinburgh. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under Grant Agreement No. 313014 (ETAEARTH). X. Dumusque would like to thank the Swiss National Science Foundation (SNSF) for its support through an Early Postdoc Mobility fellowship. P. Figueira acknowledges support by Fundacao para a Ciencia e a Tecnologia (FCT) through the Investigador FCT contract of reference IF/01037/2013 and POPH/FSE (EC) by FEDER funding through the program "Programa Operacional de Factores de Competitividade - COMPETE." R. D. Haywood acknowledges support from an STFC postgraduate research studentship. This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This research has made use of the results produced by the PI2S2 Project managed by the Consorzio COMETA, a co-funded project by the Italian Ministero dellIstruzione, Universita e Ricerca (MIUR) within the Piano Operativo Nazionale Ricerca Scientifica, Sviluppo Tecnologico, Alta Formazione (PON 20002006). We would like to thank A. McWilliam, I. Ivans, and C. Sneden for providing us their software that interpolates between atmospheric models. NR 87 TC 64 Z9 64 U1 1 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2014 VL 789 IS 2 AR 154 DI 10.1088/0004-637X/789/2/154 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8JY UT WOS:000338674900063 ER PT J AU Le Chat, G Kasper, JC Cohen, O Spangler, SR AF Le Chat, G. Kasper, J. C. Cohen, O. Spangler, S. R. TI DIAGNOSTICS OF THE SOLAR CORONA FROM COMPARISON BETWEEN FARADAY ROTATION MEASUREMENTS AND MAGNETOHYDRODYNAMIC SIMULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); methods: numerical; Sun: corona; Sun: magnetic fields ID WHOLE SUN MONTH; MAGNETIC-FIELD; ELECTRON-DENSITY; PLASMA STRUCTURE; MASS EJECTIONS; WIND; MODEL; OCCULTATION AB Polarized natural radio sources passing behind the Sun experience Faraday rotation as a consequence of the electron density and magnetic field strength in coronal plasma. Since Faraday rotation is proportional to the product of the density and the component of the magnetic field along the line of sight of the observer, a model is required to interpret the observations and infer coronal structures. Faraday rotation observations have been compared with relatively ad hoc models of the corona. Here for the first time we compare these observations with magnetohydrodynamic (MHD) models of the solar corona driven by measurements of the photospheric magnetic field. We use observations made with the NRAO Very Large Array of 34 polarized radio sources occulted by the solar corona between 5 and 14 solar radii. The measurements were made during 1997 May, and 2005 March and April. We compare the observed Faraday rotation values with values extracted from MHD steady-state simulations of the solar corona. We find that (1) using a synoptic map of the solar magnetic field just one Carrington rotation off produces poorer agreements, meaning that the outer corona changes in the course of one month, even in solar minimum; (2) global MHD models of the solar corona driven by photospheric magnetic field measurements are generally able to reproduce Faraday rotation observations; and (3) some sources show significant disagreement between the model and the observations, which appears to be a function of the proximity of the line of sight to the large-scale heliospheric current sheet. C1 [Le Chat, G.; Kasper, J. C.; Cohen, O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Spangler, S. R.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Le Chat, G.; Kasper, J. C.] NASA, Lunar Sci Inst, Moffett Field, CA USA. RP Le Chat, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gaetan.lechat@obspm.fr RI Kasper, Justin/D-1152-2010; OI Kasper, Justin/0000-0002-7077-930X; Cohen, Ofer/0000-0003-3721-0215 FU NASA ESS; NASA ESTO-CT; NSF KDI; DoD MURI; National Science Foundation [ATM09-56901, AST09-07911] FX Simulation results were obtained using the Space Weather Modeling Framwork, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI. This work was supported at the University of Iowa by grants ATM09-56901 and AST09-07911 from the National Science Foundation. NR 39 TC 1 Z9 1 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2014 VL 789 IS 2 AR 163 DI 10.1088/0004-637X/789/2/163 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8JY UT WOS:000338674900072 ER PT J AU Liu, X Shen, Y Bian, FY Loeb, A Tremaine, S AF Liu, Xin Shen, Yue Bian, Fuyan Loeb, Abraham Tremaine, Scott TI CONSTRAINING SUB-PARSEC BINARY SUPERMASSIVE BLACK HOLES IN QUASARS WITH MULTI-EPOCH SPECTROSCOPY. II. THE POPULATION WITH KINEMATICALLY OFFSET BROAD BALMER EMISSION LINES SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; galaxies: nuclei; line: profiles; quasars: general ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; TERM PROFILE VARIABILITY; DOUBLE-PEAKED EMITTER; LOW-REDSHIFT QSOS; 7TH DATA RELEASE; OJ 287; GALAXY MERGERS; RADIO-LOUD; X-RAY AB A small fraction of quasars have long been known to show bulk velocity offsets (of a few hundred to thousands of km s(-1)) in the broad Balmer lines with respect to the systemic redshift of the host galaxy. Models to explain these offsets usually invoke broad-line region gas kinematics/asymmetry around single black holes (BHs), orbital motion of massive (similar to sub-parsec (sub-pc)) binary black holes (BBHs), or recoil BHs, but single-epoch spectra are unable to distinguish between these scenarios. The line-of-sight (LOS) radial velocity (RV) shifts from long-term spectroscopic monitoring can be used to test the BBH hypothesis. We have selected a sample of 399 quasars with kinematically offset broad H beta lines from the Sloan Digital Sky Survey (SDSS) Seventh Data Release quasar catalog, and have conducted second-epoch optical spectroscopy for 50 of them. Combined with the existing SDSS spectra, the new observations enable us to constrain the LOS RV shifts of broad H beta lines with a rest-frame baseline of a few years to nearly a decade. While previous work focused on objects with extreme velocity offset (> 10(3) km s(-1)), we explore the parameter space with smaller (a few hundred km s(-1)) yet significant offsets (99.7% confidence). Using cross-correlation analysis, we detect significant (99% confidence) radial accelerations in the broad H beta lines in 24 of the 50 objects, of similar to 10-200 km s(-1) yr(-1) with a median measurement uncertainty of similar to 10 km s(-1) yr(-1), implying a high fraction of variability of the broad-line velocity on multi-year timescales. We suggest that 9 of the 24 detections are sub-pc BBH candidates, which show consistent velocity shifts independently measured from a second broad line (either H alpha or Mg II) without significant changes in the broad-line profiles. Combining the results on the general quasar population studied in Paper I, we find a tentative anti-correlation between the velocity offset in the first-epoch spectrum and the average acceleration between two epochs, which could be explained by orbital phase modulation when the time separation between two epochs is a non-negligible fraction of the orbital period of the motion causing the line displacement. We discuss the implications of our results for the identification of sub-pc BBH candidates in offset-line quasars and for the constraints on their frequency and orbital parameters. C1 [Liu, Xin] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Shen, Yue] Carnegie Observ, Pasadena, CA 91101 USA. [Bian, Fuyan] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Bian, Fuyan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Loeb, Abraham] Harvard Univ, Inst Theory & Computat, Cambridge, MA 02138 USA. [Tremaine, Scott] Inst Adv Study, Princeton, NJ 08540 USA. RP Liu, X (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. EM xinliu@astro.ucla.edu RI Tremaine, Scott/M-4281-2015 OI Tremaine, Scott/0000-0002-0278-7180 FU NASA through Hubble Fellowship [HST-HF-51307.01, HST-HF-51314.01]; Space Telescope Science Institute; Association of Universities for Research in Astronomy, Inc., for NASA [NAS 5-26555]; NSF [AST-1312034]; NASA [NNX11AF29G]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We thank Mike Eracleous, Luis Ho, and Alice Shapley for useful discussion, Perry Berlind, Michael Calkins, and Bill Wyatt for assistance with FLWO 1.5 m/FAST queue observations and data retrieval, and Michael Strauss for his support during the course of this work. We also thank an anonymous referee for a prompt and careful report. Support for the work of X.L. and Y.S. was provided by NASA through Hubble Fellowship grant numbers HST-HF-51307.01 and HST-HF-51314.01, respectively, 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 work was supported in part by NSF grant AST-1312034 (A.L.) and NASA grant NNX11AF29G (S.T.).; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. NR 145 TC 19 Z9 19 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2014 VL 789 IS 2 AR 140 DI 10.1088/0004-637X/789/2/140 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8JY UT WOS:000338674900049 ER PT J AU Patnaude, DJ Fesen, RA AF Patnaude, Daniel J. Fesen, Robert A. TI A COMPARISON OF X-RAY AND OPTICAL EMISSION IN CASSIOPEIA A SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Cassiopeia A); radiation mechanisms: thermal ID A SUPERNOVA REMNANT; CORE-COLLAPSE SUPERNOVAE; 3-DIMENSIONAL STRUCTURE; PROPER MOTIONS; HIGH-VELOCITY; LIGHT ECHOES; NOVA REMNANT; EJECTA; EXPANSION; CHANDRA AB Broadband optical and narrowband Si XIII X-ray images of the young Galactic supernova remnant Cassiopeia A (Cas A) obtained over several decades are used to investigate spatial and temporal emission correlations on both large and small angular scales. The data examined consist of optical and near-infrared ground-based and Hubble Space Telescope images taken between 1951 and 2011, and of X-ray images from Einstein, ROSAT, and Chandra taken between 1979 and 2013. We find weak spatial correlations between the remnant's X-ray and optical emission features on large scales, but several cases of good optical/X-ray correlations on small scales for features which have brightened due to recent interactions with the reverse shock. We also find instances (1) where a time delay is observed between the appearance of a feature's optical and X-ray emissions, (2) of displacements of several arcseconds between a feature's X-ray and optical emission peaks, and (3) of regions showing no corresponding X-ray or optical emissions. To explain this behavior, we propose a highly inhomogeneous density model for Cas A's ejecta consisting of small, dense optically emitting knots (n similar to 10(2-3) cm(-3)) and a much lower density (n similar to 0.1-1 cm(-3)) diffuse X-ray emitting component often spatially associated with optical emission knots. The X-ray emitting component is sometimes linked to optical clumps through shock-induced mass ablation generating trailing material leading to spatially offset X-ray/optical emissions. A range of ejecta densities can also explain the observed X-ray/optical time delays since the remnant's approximate to 5000 km s(-1) reverse shock heats dense ejecta clumps to temperatures around 3 x 10(4) K relatively quickly, which then become optically bright while more diffuse ejecta become X-ray bright on longer timescales. Highly inhomogeneous ejecta as proposed here for Cas A may help explain some of the X-ray/optical emission features seen in other young core-collapse supernova remnants. C1 [Patnaude, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fesen, Robert A.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. RP Patnaude, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. FU Chandra X-ray Center [GO8-9065A]; Space Telescope Science Institute [GO-11337.01-A]; NASA [NAS8-03060, GO-8281, 9238, 9890, 10286, 12300]; National Science Foundation [AST-0908237]; Space Telescope Science Institute operated by the Association of Universities for Research in Astronomy, Inc [12674] FX We thank Sidney van den Bergh for making available the extensive Palomar plate collection of Cas A images dating back to 1951 and to Josh Grindlay and the DASCH plate scanning team at CfA/Harvard for their expert help and assistance in scanning these priceless photographic plates. We also thank J. Thorstensen for assistance with applying WCS coordinates to the scanned Palomar plates. We thank Dan Milisavljevic, J. Martin Laming, Roger Chevalier, and the anonymous referee for useful comments during the preparation and revision of this manuscript. D.J.P. acknowledges support from the Chandra X-ray Center through GO8-9065A and from the Space Telescope Science Institute through grant GO-11337.01-A. D.J.P. also acknowledges support through NASA contract NAS8-03060. R.A.F. acknowledges support from the National Science Foundation under grant AST-0908237 and from NASA through grants GO-8281, 9238, 9890, 10286, 12300, and 12674 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. NR 64 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 JUL 10 PY 2014 VL 789 IS 2 AR 138 DI 10.1088/0004-637X/789/2/138 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8JY UT WOS:000338674900047 ER PT J AU Bertrand, C Janzen, DH Hallwachs, W Burns, JM Gibson, JF Shokralla, S Hajibabaei, M AF Bertrand, Claudia Janzen, Daniel H. Hallwachs, Winnie Burns, John M. Gibson, Joel F. Shokralla, Shadi Hajibabaei, Mehrdad TI Mitochondrial and nuclear phylogenetic analysis with Sanger and next-generation sequencing shows that, in Area de Conservacion Guanacaste, northwestern Costa Rica, the skipper butterfly named Urbanus belli (family Hesperiidae) comprises three morphologically cryptic species SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Lepidoptera; Intragenomic variation; Non-metric multi-dimensional scaling; Phylogeny; DNA barcoding ID INTERNAL TRANSCRIBED SPACER; PARASITOID FLIES DIPTERA; DNA BARCODES; WOLBACHIA; ITS2; LEPIDOPTERA; TACHINIDAE; INFERENCE; TAXONOMY; SYSTEM AB Background: Skipper butterflies (Hesperiidae) are a relatively well-studied family of Lepidoptera. However, a combination of DNA barcodes, morphology, and natural history data has revealed several cryptic species complexes within them. Here, we investigate three DNA barcode lineages of what has been identified as Urbanus belli (Hesperiidae, Eudaminae) in Area de Conservacion Guanacaste (ACG), northwestern Costa Rica. Results: Although no morphological traits appear to distinguish among the three, congruent nuclear and mitochondrial lineage patterns show that "Urbanus belli" in ACG is a complex of three sympatric species. A single strain of Wolbachia present in two of the three cryptic species indicates that Urbanus segnestami Burns (formerly Urbanus belliDHJ01), Urbanus bernikerni Burns (formerly Urbanus belliDHJ02), and Urbanus ehakernae Burns (formerly Urbanus belliDHJ03) may be biologically separated by Wolbachia, as well as by their genetics. Use of parallel sequencing through 454-pyrosequencing improved the utility of ITS2 as a phylogenetic marker and permitted examination of the intra-and interlineage relationships of ITS2 variants within the species complex. Interlineage, intralineage and intragenomic compensatory base pair changes were discovered in the secondary structure of ITS2. Conclusion: These findings corroborate the existence of three cryptic species. Our confirmation of a novel cryptic species complex, initially suggested by DNA barcode lineages, argues for using a multi-marker approach coupled with next-generation sequencing for exploration of other suspected species complexes. C1 [Bertrand, Claudia; Gibson, Joel F.; Shokralla, Shadi; Hajibabaei, Mehrdad] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. [Bertrand, Claudia; Gibson, Joel F.; Shokralla, Shadi; Hajibabaei, Mehrdad] Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. [Janzen, Daniel H.; Hallwachs, Winnie] Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. [Burns, John M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Shokralla, Shadi] Mansoura Univ, Dept Microbiol, Mansoura 35516, Egypt. RP Hajibabaei, M (reprint author), Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. EM mhajibab@uoguelph.ca FU U.S. National Science Foundation [BSR 9024770, DEB 9306296, 9400829, 9705072, 0072730, 0515699]; Wege Foundation; International Conservation Fund of Canada; Jessie B. Cox Charitable Trust; Blue Moon Fund; Guanacaste Dry Forest Conservation Fund; Permian Global; University of Pennsylvania; Government of Canada through Genome Canada; Ontario Genomics Institute through the Biomonitoring 2.0 project [OGI-050]; Natural Sciences and Engineering Research Council of Canada; Area de Conservacion Guanacaste FX We gratefully acknowledge the team of ACG parataxonomists [13,60] who found and reared the specimens used in this study, and the team of biodiversity managers who keep the ACG forests that host these butterflies alive. We thank Karie Darrow for preparing Figure 3 and Donald Harvey for dissecting many genitalia. We also thank Teresa Crease and Alex Smith for providing advice and editorial assistance in the early stages of this research. The study has been supported by U.S. National Science Foundation grants BSR 9024770 and DEB 9306296, 9400829, 9705072, 0072730, 0515699, and grants from the Wege Foundation, International Conservation Fund of Canada, Jessie B. Cox Charitable Trust, Blue Moon Fund, Guanacaste Dry Forest Conservation Fund, Permian Global, Area de Conservacion Guanacaste, and University of Pennsylvania (DHJ). This project was funded by the Government of Canada through Genome Canada and the Ontario Genomics Institute (OGI-050) through the Biomonitoring 2.0 project (www.biomonitoring2.org) (MH) and by a Discovery Grant from Natural Sciences and Engineering Research Council of Canada (MH). NR 60 TC 11 Z9 11 U1 0 U2 34 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD JUL 9 PY 2014 VL 14 AR 153 DI 10.1186/1471-2148-14-153 PG 18 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA AM0DI UT WOS:000339513100001 PM 25005355 ER PT J AU Yong, S Perez-Gelabert, DE AF Yong, Sheyla Perez-Gelabert, Daniel E. TI Grasshoppers, Crickets and Katydids (Insecta: Orthoptera) of Cuba: an annotated checklist SO ZOOTAXA LA English DT Article DE Orthoptera; taxonomy; diversity; Cuba; Greater Antilles; West Indies ID SPECIES ORTHOPTERA; MOLE CRICKETS; UNITED-STATES; WEST-INDIES; REVISION; GENUS; GRYLLOTALPIDAE; GRYLLOIDEA; HISPANIOLA; GRYLLIDAE AB An annotated list of the Cuban fauna of Orthoptera is presented. For each species we include details of valid names, synonyms, type specimens (type category, sex, locality and depository), geographic distribution and bibliographic references. Clarifying notes are added, as well as comments on the species considered doubtful. A total of 140 species included in 62 genera, 31 subfamilies and 12 families make up the known Cuban fauna of Orthoptera. The family Episactidae, the acridid subfamily Ommatolampidinae with 3 unknown genera, 3 unknown genera of Tettigoniidae (Conocephalinae) and 1 undescribed new genus of Tetrigidae (Cladonotinae) are here recorded for the first time from Cuba. Syntypes are designated for Hygronemobius histrionicus Zayas. C1 [Perez-Gelabert, Daniel E.] ITIS, Washington, DC 20013 USA. [Perez-Gelabert, Daniel E.] Smithsonian Inst, US Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Yong, S (reprint author), Calle 200,3759-37 & 45,CP 13500, Havana, Cuba. EM gruenes@estudiantes.fbio.uh.cu; perezd@si.edu NR 136 TC 0 Z9 1 U1 3 U2 12 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUL 7 PY 2014 VL 3827 IS 4 BP 401 EP 438 PG 38 WC Zoology SC Zoology GA AK4YN UT WOS:000338430600001 PM 25081171 ER PT J AU Sneed, JM Sharp, KH Ritchie, KB Paul, VJ AF Sneed, Jennifer M. Sharp, Koty H. Ritchie, Kimberly B. Paul, Valerie J. TI The chemical cue tetrabromopyrrole from a biofilm bacterium induces settlement of multiple Caribbean corals SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE biofilm; chemical ecology; coral recruitment; larval settlement; Pseudoalteromonas ID MARINE-INVERTEBRATE LARVAE; ANTIBIOTIC PRODUCTION; MICROBIAL BIOFILMS; METAMORPHOSIS; RECRUITMENT; PSEUDOALTEROMONAS; COMMUNITIES; MUCUS; ALGAE AB Microbial biofilms induce larval settlement for some invertebrates, including corals; however, the chemical cues involved have rarely been identified. Here, we demonstrate the role of microbial biofilms in inducing larval settlement with the Caribbean coral Porites astreoides and report the first instance of a chemical cue isolated from a marine biofilm bacterium that induces complete settlement (attachment and metamorphosis) of Caribbean coral larvae. Larvae settled in response to natural biofilms, and the response was eliminated when biofilms were treated with antibiotics. A similar settlement response was elicited by monospecific biofilms of a single bacterial strain, Pseudoalteromonas sp. PS5, isolated from the surface biofilm of a crustose coralline alga. The activity of Pseudoalteromonas sp. PS5 was attributed to the production of a single compound, tetrabromopyrrole (TBP), which has been shown previously to induce metamorphosis without attachment in Pacific acroporid corals. In addition to inducing settlement of brooded larvae (P. astreoides), TBP also induced larval settlement for two broadcast-spawning species, Orbicella (formerly Montastraea) franksi and Acropora palmata, indicating that this compound may have widespread importance among Caribbean coral species. C1 [Sneed, Jennifer M.; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Sharp, Koty H.] Eckerd Coll, St Petersburg, FL 33711 USA. [Ritchie, Kimberly B.] Mote Marine Lab & Aquarium, Sarasota, FL 34236 USA. RP Sneed, JM (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM sneedj@si.edu FU Mote Protect Our Reef Grant program [POR-2010-29, POR-2011-21, POR-2012-3]; Dart Foundation; Smithsonian Competitive Grants Program for Science; CCRE program [958] FX Funding was provided by Mote Protect Our Reef Grant program (POR-2010-29, POR-2011-21 and POR-2012-3), the Dart Foundation and Smithsonian Competitive Grants Program for Science. This is contribution no. 950 of the Smithsonian Marine Station at Fort Pierce and no. 958 of the CCRE program. NR 30 TC 20 Z9 20 U1 6 U2 70 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 JUL 7 PY 2014 VL 281 IS 1786 AR 20133086 DI 10.1098/rspb.2013.3086 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AI3TA UT WOS:000336784500006 ER PT J AU Anton, SC Potts, R Aiello, LC AF Anton, Susan C. Potts, Richard Aiello, Leslie C. TI Evolution of early Homo: An integrated biological perspective SO SCIENCE LA English DT Review ID GENUS HOMO; TURKANA BASIN; EAST-AFRICA; AUSTRALOPITHECUS-AFARENSIS; CLIMATE-CHANGE; LIFE-HISTORY; SOUTH-AFRICA; KOOBI-FORA; BRAIN SIZE; BODY-SIZE AB Integration of evidence over the past decade has revised understandings about the major adaptations underlying the origin and early evolution of the genus Homo. Many features associated with Homo sapiens, including our large linear bodies, elongated hind limbs, large energy-expensive brains, reduced sexual dimorphism, increased carnivory, and unique life history traits, were once thought to have evolved near the origin of the genus in response to heightened aridity and open habitats in Africa. However, recent analyses of fossil, archaeological, and environmental data indicate that such traits did not arise as a single package. Instead, some arose substantially earlier and some later than previously thought. From similar to 2.5 to 1.5 million years ago, three lineages of early Homo evolved in a context of habitat instability and fragmentation on seasonal, intergenerational, and evolutionary time scales. These contexts gave a selective advantage to traits, such as dietary flexibility and larger body size, that facilitated survival in shifting environments. C1 [Anton, Susan C.] NYU, Dept Anthropol, Ctr Study Human Origins, New York, NY 10003 USA. [Potts, Richard] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20013 USA. [Aiello, Leslie C.] Wenner Gren Fdn, New York, NY 10016 USA. RP Anton, SC (reprint author), NYU, Dept Anthropol, Ctr Study Human Origins, Rufus D Smith Hall,25 Waverly Pl, New York, NY 10003 USA. EM susan.anton@nyu.edu; pottsr@si.edu; laiello@wennergren.org FU Wenner-Gren Foundation for Anthropological Research; New York University; Peter Buck Fund for Human Origins Research; Human Origins Program (Smithsonian) FX We thank the participants of the Wenner-Gren Symposium "Human Biology and the Origin of Homo"; our field and laboratory collaborators for contributing stimulating conversation and ideas; J. B. Clark, who assisted in creating the figures; and E. R. Middleton, who provided bibliographic assistance. Funding provided by the Wenner-Gren Foundation for Anthropological Research (S. C. A. and L. C. A.), New York University (S. C. A.), the Peter Buck Fund for Human Origins Research, and the Human Origins Program (Smithsonian) (R. P.). The authors contributed equally to this work. NR 152 TC 56 Z9 58 U1 30 U2 279 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD JUL 4 PY 2014 VL 345 IS 6192 BP 45 EP + AR 1236828 DI 10.1126/science.1236828 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AK2XU UT WOS:000338284400043 PM 24994657 ER PT J AU Gould, A Udalski, A Shin, IG Porritt, I Skowron, J Han, C Yee, JC Kozlowski, S Choi, JY Poleski, R Wyrzykowski, L Ulaczyk, K Pietrukowicz, P Mroz, P Szymanski, MK Kubiak, M Soszynski, I Pietrzynski, G Gaudi, BS Christie, GW Drummond, J McCormick, J Natusch, T Ngan, H Tan, TG Albrow, M DePoy, DL Hwang, KH Jung, YK Lee, CU Park, H Pogge, RW Abe, F Bennett, DP Bond, IA Botzler, CS Freeman, M Fukui, A Fukunaga, D Itow, Y Koshimoto, N Larsen, P Ling, CH Masuda, K Matsubara, Y Muraki, Y Namba, S Ohnishi, K Philpott, L Rattenbury, NJ Saito, T Sullivan, DJ Sumi, T Suzuki, D Tristram, PJ Tsurumi, N Wada, K Yamai, N Yock, PCM Yonehara, A Shvartzvald, Y Maoz, D Kaspi, S Friedmann, M AF Gould, A. Udalski, A. Shin, I. -G. Porritt, I. Skowron, J. Han, C. Yee, J. C. Kozlowski, S. Choi, J. -Y. Poleski, R. Wyrzykowski, L. Ulaczyk, K. Pietrukowicz, P. Mroz, P. Szymanski, M. K. Kubiak, M. Soszynski, I. Pietrzynski, G. Gaudi, B. S. Christie, G. W. Drummond, J. McCormick, J. Natusch, T. Ngan, H. Tan, T. -G. Albrow, M. DePoy, D. L. Hwang, K. -H. Jung, Y. K. Lee, C. -U. Park, H. Pogge, R. W. Abe, F. Bennett, D. P. Bond, I. A. Botzler, C. S. Freeman, M. Fukui, A. Fukunaga, D. Itow, Y. Koshimoto, N. Larsen, P. Ling, C. H. Masuda, K. Matsubara, Y. Muraki, Y. Namba, S. Ohnishi, K. Philpott, L. Rattenbury, N. J. Saito, To. Sullivan, D. J. Sumi, T. Suzuki, D. Tristram, P. J. Tsurumi, N. Wada, K. Yamai, N. Yock, P. C. M. Yonehara, A. Shvartzvald, Y. Maoz, D. Kaspi, S. Friedmann, M. CA OGLE Team FUN Team Microlensing Follow MOA Team Microlensing Observations Wise Team Wise Observ TI A terrestrial planet in a similar to 1-AU orbit around one member of a similar to 15-AU binary SO SCIENCE LA English DT Article ID MICROLENSING OBSERVATIONS; GALACTIC BULGE; SYSTEMS; STARS; COMPANION; PARALLAX; LENS AB Using gravitational microlensing, we detected a cold terrestrial planet orbiting one member of a binary star system. The planet has low mass (twice Earth's) and lies projected at similar to 0.8 astronomical units (AU) from its host star, about the distance between Earth and the Sun. However, the planet's temperature is much lower, <60 Kelvin, because the host star is only 0.10 to 0.15 solar masses and therefore more than 400 times less luminous than the Sun. The host itself orbits a slightly more massive companion with projected separation of 10 to 15 AU. This detection is consistent with such systems being very common. Straightforward modification of current microlensing search strategies could increase sensitivity to planets in binary systems. With more detections, such binary-star planetary systems could constrain models of planet formation and evolution. C1 [Gould, A.; Yee, J. C.; Poleski, R.; Pietrzynski, G.; Gaudi, B. S.; Pogge, R. W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Udalski, A.; Shin, I. -G.; Skowron, J.; Kozlowski, S.; Choi, J. -Y.; Poleski, R.; Wyrzykowski, L.; Ulaczyk, K.; Pietrukowicz, P.; Mroz, P.; Szymanski, M. K.; Kubiak, M.; Soszynski, I.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Han, C.; Hwang, K. -H.; Jung, Y. K.; Park, H.] Chungbuk Natl Univ, Dept Phys, Cheongju 371763, South Korea. [Porritt, I.] Turitea Observ, Palmerston North, New Zealand. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Christie, G. W.] Auckland Observ, Auckland, New Zealand. [Drummond, J.; Natusch, T.; Ngan, H.] Possum Observ, Patutahi, New Zealand. [McCormick, J.] Farm Cove Observ, Ctr Backyard Astrophys, Auckland, New Zealand. [Natusch, T.] Auckland Univ Technol, Auckland, New Zealand. [Tan, T. -G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Albrow, M.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [DePoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Abe, F.; Fukunaga, D.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Tsurumi, N.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Bond, I. A.; Ling, C. H.] Massey Univ, Inst Informat & Math Sci, Auckland, New Zealand. [Botzler, C. S.; Freeman, M.; Larsen, P.; Rattenbury, N. J.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1001, New Zealand. [Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, Okayama 7190232, Japan. [Koshimoto, N.; Namba, S.; Sumi, T.; Suzuki, D.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, 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, Lake Tekapo 8770, New Zealand. [Yamai, N.; Yonehara, A.] Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kyoto 6038555, Japan. [Shvartzvald, Y.; Maoz, D.; Kaspi, S.; Friedmann, M.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Larsen, P.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Philpott, L.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V6T 1Z4, Canada. RP Han, C (reprint author), Chungbuk Natl Univ, Dept Phys, Cheongju 371763, South Korea. EM cheongho@astroph.chungbuk.ac.kr RI Skowron, Jan/M-5186-2014; Kozlowski, Szymon/G-4799-2013; OI Skowron, Jan/0000-0002-2335-1730; Kozlowski, Szymon/0000-0003-4084-880X; Tan, Thiam-Guan/0000-0001-5603-6895 FU NSF [AST-1103471, AST-1211875]; NASA [NNGX12AB99G, NNX13AF64G]; Ohio State University fellowship; NASA Sagan fellowship; ERC AdG [246678]; IDEAS program; Polish MNiSW [IP2011026771]; Korea NRF CRIP [2009-0081561]; U.S.-Israel BSF; New Zealand Marsden Fund; Israel SF PBC-ICORE [1829/12]; [JSPS23340044]; [JSPS24253004] FX We acknowledge support from NSF AST-1103471 (A. G., B. S. G., and J.C.Y.); NSF AST-1211875 (D. P. B.); NASA NNGX12AB99G (A. G., B. S. G., and R. W. P.); NASA NNX13AF64G (D. P. B.); Ohio State University fellowship and NASA Sagan fellowship (J.C.Y.); ERC AdG 246678 and IDEAS program (A. U.); Polish MNiSW IP2011026771 (S. K.); Korea NRF CRIP 2009-0081561 (C. H.); U.S.-Israel BSF (A. G. and D. M.); JSPS23340044 and JSPS24253004 (T. S.); New Zealand Marsden Fund (P.C.M.Y.); and Israel SF PBC-ICORE 1829/12 (D. M.). Data are available at astroph.chungbuk.ac.kr/similar to cheongho/OB130341/data.html. NR 26 TC 28 Z9 28 U1 2 U2 21 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD JUL 4 PY 2014 VL 345 IS 6192 BP 46 EP 49 DI 10.1126/science.1251527 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AK2XU UT WOS:000338284400044 PM 24994642 ER PT J AU Collins, M AF Collins, Martin TI Adelheid Voskuhl's Androids in the Enlightenment: Mechanics, Artisans, and Cultures of the Self SO HISTORY AND TECHNOLOGY LA English DT Article C1 Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, Washington, DC 20560 USA. RP Collins, M (reprint author), Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, Washington, DC 20560 USA. EM CollinsM@si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0734-1512 EI 1477-2620 J9 HIST TECHNOL JI Hist. Technol. PD JUL 3 PY 2014 VL 30 IS 3 SI SI BP 252 EP 254 DI 10.1080/07341512.2015.1007557 PG 3 WC History SC History GA CA9MS UT WOS:000349248900006 ER PT J AU Loss, SR Will, T Marra, PP AF Loss, Scott R. Will, Tom Marra, Peter P. TI Refining Estimates of Bird Collision and Electrocution Mortality at Power Lines in the United States SO PLOS ONE LA English DT Article ID EAGLE HIERAAETUS-FASCIATUS; RAPTOR ELECTROCUTION; TRANSMISSION-LINES; UTILITY STRUCTURES; AVIAN MORTALITY; RISK; POPULATION; MARKING; CANADA; AREAS AB Collisions and electrocutions at power lines are thought to kill large numbers of birds in the United States annually. However, existing estimates of mortality are either speculative (for electrocution) or based on extrapolation of results from one study to all U.S. power lines (for collision). Because national-scale estimates of mortality and comparisons among threats are likely to be used for prioritizing policy and management strategies and for identifying major research needs, these estimates should be based on systematic and transparent assessment of rigorously collected data. We conducted a quantitative review that incorporated data from 14 studies meeting our inclusion criteria to estimate that between 12 and 64 million birds are killed each year at U.S. power lines, with between 8 and 57 million birds killed by collision and between 0.9 and 11.6 million birds killed by electrocution. Sensitivity analyses indicate that the majority of uncertainty in our estimates arises from variation in mortality rates across studies; this variation is due in part to the small sample of rigorously conducted studies that can be used to estimate mortality. Little information is available to quantify species-specific vulnerability to mortality at power lines; the available literature over-represents particular bird groups and habitats, and most studies only sample and present data for one or a few species. Furthermore, additional research is needed to clarify whether, to what degree, and in what regions populations of different bird species are affected by power line-related mortality. Nonetheless, our data-driven analysis suggests that the amount of bird mortality at U.S. power lines is substantial and that conservation management and policy is necessary to reduce this mortality. C1 [Loss, Scott R.; Marra, Peter P.] Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC USA. [Will, Tom] US Fish & Wildlife Serv, Div Migratory Birds, Midwest Reg Off, Bloomington, MA USA. RP Loss, SR (reprint author), Oklahoma State Univ, Dept Nat Resource Ecol & Management, Stillwater, OK 74078 USA. EM scott.loss@okstate.edu FU U.S. Fish and Wildlife Service FX S.R.L. was supported by a postdoctoral fellowship funded by the U. S. Fish and Wildlife Service through the Smithsonian Institution's Postdoctoral Fellowship program. T.W. participated as a collaborator and co-author throughout the project; however, the U.S. Fish and Wildlife as a larger entity had no role in study design; collection, analysis, and interpretation of data; in writing the report; and in the decision to submit the paper for publication. NR 68 TC 13 Z9 13 U1 6 U2 56 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 3 PY 2014 VL 9 IS 7 AR e101565 DI 10.1371/journal.pone.0101565 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AO3RT UT WOS:000341253400091 PM 24991997 ER PT J AU Deane, RP Paragi, Z Jarvis, MJ Coriat, M Bernardi, G Fender, RP Frey, S Heywood, I Klockner, HR Grainge, K Rumsey, C AF Deane, R. P. Paragi, Z. Jarvis, M. J. Coriat, M. Bernardi, G. Fender, R. P. Frey, S. Heywood, I. Kloeckner, H-R Grainge, K. Rumsey, C. TI A close-pair binary in a distant triple supermassive black hole system SO NATURE LA English DT Article ID ACTIVE GALACTIC NUCLEUS; RADIO-SOURCES; MINOR MERGER; GALAXIES; DISCOVERY; JETS; SCALE; SKY; EVOLUTION; QUASARS AB Galaxies are believed to evolve through merging(1), which should lead to some hosting multiple supermassive black holes(2-4). There are four known triple black hole systems(5-8), with the closest black hole pair being 2.4 kiloparsecs apart (the third component in this system is at 3 kiloparsecs)(7), which is far from the gravitational sphere of influence (about 100 parsecs for a black hole with mass one billion times that of the Sun). Previous searches for compact black hole systems concluded that they were rare(9), with the tightest binary system having a separation of 7 parsecs (ref. 10). Here we report observations of a triple black hole system at redshift z = 0.39, with the closest pair separated by about 140 parsecs and significantly more distant from Earth than any other known binary of comparable orbital separation. The effect of the tight pair is to introduce a rotationally symmetric helical modulation on the structure of the large-scale radio jets, which provides a useful way to search for other tight pairs without needing extremely high resolution observations. As we found this tight pair after searching only six galaxies, we conclude that tight pairs are more common than hitherto believed, which is an important observational constraint for low-frequency gravitational wave experiments(11,12). C1 [Deane, R. P.; Coriat, M.] Univ Cape Town, Dept Astron, Astrophys Cosmol & Grav Ctr, ZA-7701 Cape Town, South Africa. [Deane, R. P.; Coriat, M.; Bernardi, G.] Sq Kilometre Array South Africa, ZA-7405 Cape Town, South Africa. [Paragi, Z.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Jarvis, M. J.; Fender, R. P.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Jarvis, M. J.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Bernardi, G.; Heywood, I.] Rhodes Univ, Dept Phys & Elect, Ctr Radio Astron Tech & Technol, ZA-6140 Grahamstown, South Africa. [Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Frey, S.] Inst Geodesy Cartog & Remote Sensing, Satellite Geodet Observ, H-1592 Budapest, Hungary. [Heywood, I.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Kloeckner, H-R] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Grainge, K.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester, Lancs, England. [Rumsey, C.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. RP Deane, RP (reprint author), Univ Cape Town, Dept Astron, Astrophys Cosmol & Grav Ctr, ZA-7701 Cape Town, South Africa. EM roger.deane@ast.uct.ac.za RI Frey, Sandor/G-4465-2013; OI Frey, Sandor/0000-0003-3079-1889; Paragi, Zsolt/0000-0002-5195-335X FU European Union [RI-261525 NEXPReS]; South African SKA Project (SKA SA); Hungarian Scientific Research Fund [OTKA 104539]; International Space Science Institute FX We thank J. Magorrian, A. Karastergiou, S. Ransom and B. Fanaroff for discussions. The European VLBI Network is a joint facility of European, Chinese, South African and other radio astronomy institutes funded by their national research councils. e-VLBI research infrastructure in Europe was supported by the European Union's Seventh Framework Programme (FP7/2007-2013) under grant agreement number RI-261525 NEXPReS. The financial assistance of the South African SKA Project (SKA SA) towards this research is acknowledged. Opinions expressed and conclusions arrived at are those of the authors and are not necessarily to be attributed to the SKA SA. Z.P. and S.F. acknowledge funding from the Hungarian Scientific Research Fund (OTKA 104539). Z.P. is grateful for funding support from the International Space Science Institute. NR 45 TC 21 Z9 21 U1 0 U2 9 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 JUL 3 PY 2014 VL 511 IS 7507 BP 57 EP U578 DI 10.1038/nature13454 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AK1TN UT WOS:000338199400034 PM 24990745 ER PT J AU Rougerie, R Kitching, IJ Haxaire, J Miller, SE Hausmann, A Hebert, PDN AF Rougerie, Rodolphe Kitching, Ian J. Haxaire, Jean Miller, Scott E. Hausmann, Axel Hebert, Paul D. N. TI Australian Sphingidae - DNA Barcodes Challenge Current Species Boundaries and Distributions SO PLOS ONE LA English DT Article ID LEPIDOPTERA SPHINGIDAE; CRYPTIC DIVERSITY; BIODIVERSITY; MOTH; LIFE; ENDEMISM; TAXONOMY; REVEALS; FAUNA AB Main Objective: We examine the extent of taxonomic and biogeographical uncertainty in a well-studied group of Australian Lepidoptera, the hawkmoths (Sphingidae). Methods: We analysed the diversity of Australian sphingids through the comparative analysis of their DNA barcodes, supplemented by morphological re-examinations and sequence information from a nuclear marker in selected cases. The results from the analysis of Australian sphingids were placed in a broader context by including conspecifics and closely related taxa from outside Australia to test taxonomic boundaries. Results: Our results led to the discovery of six new species in Australia, one case of erroneously synonymized species, and three cases of synonymy. As a result, we establish the occurrence of 75 species of hawkmoths on the continent. The analysis of records from outside Australia also challenges the validity of current taxonomic boundaries in as many as 18 species, including Agrius convolvuli (Linnaeus, 1758), a common species that has gained adoption as a model system. Our work has revealed a higher level of endemism than previously recognized. Most (90%) Australian sphingids are endemic to the continent (45%) or to Australia, the Pacific Islands and the Papuan and Wallacean regions (45%). Only seven species (10%) have ranges that extend beyond this major biogeographical boundary toward SE Asia and other regions of the Old World. Main Conclusions: This study has established that overlooked cryptic diversity and inaccurate species delineation produced significant misconceptions concerning diversity and distribution patterns in a group of insects that is considered well known taxonomically. Because DNA barcoding represents a straightforward way to test taxonomic boundaries, its implementation can improve the accuracy of primary diversity data in biogeography and conservation studies. C1 [Rougerie, Rodolphe; Hebert, Paul D. N.] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. [Kitching, Ian J.] Nat Hist Museum, Dept Life Sci, London SW7 5BD, England. [Haxaire, Jean] Museum Natl Hist Nat Paris, Le Roc, Laplume, France. [Miller, Scott E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Hausmann, Axel] Bavarian State Collect Zool, Sect Lepidoptera, Munich, Germany. RP Rougerie, R (reprint author), INRA, Zool Forestiere UR633, Orleans, France. EM rrougeri@gmail.com RI Rougerie, Rodolphe/D-2930-2009; Hebert, Paul/C-4161-2013; OI Rougerie, Rodolphe/0000-0003-0937-2815; Hebert, Paul/0000-0002-3081-6700; Miller, Scott/0000-0002-4138-1378 FU government of Canada through Genome Canada; Ontario Genomics Institute; Natural Sciences and Engineering Research Council of Canada (NSERC) FX This work was supported by funding from the government of Canada through Genome Canada (www.genomecanada.ca) and the Ontario Genomics Institute (www.ontariogenomics.ca) in support of the International Barcode of Life project (www.iBOL.org), and by the Natural Sciences and Engineering Research Council of Canada (NSERC, www.nserc-crsng.gc.ca). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 57 TC 10 Z9 10 U1 1 U2 21 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 2 PY 2014 VL 9 IS 7 AR e101108 DI 10.1371/journal.pone.0101108 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AO5BA UT WOS:000341354100060 PM 24987846 ER PT J AU Nguyen, TQ Botov, A Le, MD Nophaseud, L Zug, G Bonkowski, M Ziegler, T AF Truong Quang Nguyen Botov, Andreas Minh Duc Le Nophaseud, Liphone Zug, George Bonkowski, Michael Ziegler, Thomas TI A new species of Hemiphyllodactylus (Reptilia: Gekkonidae) from northern Laos SO ZOOTAXA LA English DT Article DE Slender Gecko; karst forest; phylogeny; taxonomy; Luang Prabang Province ID 1860 SQUAMATA GEKKONIDAE; PHYLOGENY; DIVERSITY; BLEEKER; GECKOS; MODEL AB A new species of the genus Hemiphyllodactylus is described from Luang Prabang Province, northern Laos. Hemiphyllodactylus kiziriani sp. nov. is distinguished from the remaining congeners by morphology, coloration, and a significant genetic divergence of greater than 20% (ND2 gene). The new species from Laos is characterized by the following features: SVL of adult males 35.1-40.1 mm, of adult females 36.3-40.8 mm; dorsal scale rows 18-27; ventral scale rows 11-15; chin scales bordering mental and first infralabial distinctly enlarged; digital lamellae formulae 3-4-4-4 (forefoot) and 4-4/5-4/5-4 (hindfoot); femoral pores 0-4, total precloacal pores 10-13 in males, 8-10 pitted precloacal scales in females; cloacal spurs present in both sexes; dorsal trunk pattern dark brown with two rows of irregular transverse bands; dark lateral head stripe distinct; upper zone of flank with a dark brown stripe; caecum and gonadal ducts unpigmented. C1 [Truong Quang Nguyen] Vietnam Acad Sci & Technol, Inst Ecol & Biol Resources, Hanoi, Vietnam. [Truong Quang Nguyen; Bonkowski, Michael; Ziegler, Thomas] Univ Cologne, Inst Zool, Dept Terr Ecol, D-50674 Cologne, Germany. [Botov, Andreas; Ziegler, Thomas] AG Zool Garten Koln, D-50735 Cologne, Germany. [Minh Duc Le] Vietnam Natl Univ, Hanoi Univ Sci, Fac Environm Sci, Hanoi, Vietnam. [Minh Duc Le] Hanoi Natl Univ, Ctr Nat Resources & Environm Studies, Hanoi, Vietnam. [Minh Duc Le] Amer Museum Nat Hist, Dept Herpetol, New York, NY 10024 USA. [Nophaseud, Liphone] Natl Univ Laos, Fac Sci, Viangchan, Laos. [Zug, George] Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Nguyen, TQ (reprint author), Vietnam Acad Sci & Technol, Inst Ecol & Biol Resources, 18 Hoang Quoc Viet, Hanoi, Vietnam. EM nqt2@yahoo.com; andreasbotov@googlemail.com; le.duc.minh@hus.edu.vn; nophasead2007@yahoo.com; zugg@si.edu; m.bonkowski@uni-koeln.de; ziegler@koelnerzoo.de RI Nguyen, Truong/F-3730-2012; Bonkowski, Michael/C-3700-2013 OI Bonkowski, Michael/0000-0003-2656-1183 FU Alexander von Humboldt Foundation [VIE 1143441] FX We are grateful to S. Wayakone, S. Bounphanmy, B. Praxaysombath (National University of Laos, Vientiane), and V. Kanyasone (Provincial Natural Resources and Environment Office of LuangPrabang) for supporting our field research in Laos. Field survey in Luang Prabang was assisted by N. Schneider (Cologne Zoo). Export of collected specimens was done due to the export permit Nr. 141/13 signed by the CITES Management Authority of Lao PDR. T. Q. Nguyen thanks C. X. Le and T. H. Tran (Hanoi) as well as T. Pagel (Cologne) for support of his research. We are grateful to A. Bauer (Villanova), P. David (Paris), and L. L. Grismer (La Sierra) for their reviews of the manuscript. Thanks to E. Sterling (New York) and K. Koy (Berkeley) for providing the map. Field survey in Luang Prabang Province and research of T. Q. Nguyen was funded by the Alexander von Humboldt Foundation (VIE 1143441). NR 22 TC 3 Z9 4 U1 0 U2 4 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUL 2 PY 2014 VL 3827 IS 1 BP 45 EP 56 PG 12 WC Zoology SC Zoology GA AK0OR UT WOS:000338114000004 PM 25081145 ER PT J AU Kidwell, PA AF Kidwell, Peggy Aldrich TI From the Curator's Desk: Online Encyclopedia of Smithsonian Mathematical Instruments SO IEEE ANNALS OF THE HISTORY OF COMPUTING LA English DT News Item C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Kidwell, PA (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. EM kidwellp@si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 1058-6180 EI 1934-1547 J9 IEEE ANN HIST COMPUT JI IEEE Ann. Hist. Comput. PD JUL-SEP PY 2014 VL 36 IS 3 BP 88 EP 89 PG 2 WC Computer Science, Theory & Methods; History & Philosophy Of Science SC Computer Science; History & Philosophy of Science GA AW5MT UT WOS:000346319900011 ER PT J AU Ceruzzi, PE AF Ceruzzi, Paul E. TI Are Historians Failing to Tell the Real Story about the History of Computing? SO IEEE ANNALS OF THE HISTORY OF COMPUTING LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Ceruzzi, PE (reprint author), Smithsonian Inst, Washington, DC 20560 USA. EM ceruzzip@si.edu NR 9 TC 1 Z9 1 U1 1 U2 1 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 1058-6180 EI 1934-1547 J9 IEEE ANN HIST COMPUT JI IEEE Ann. Hist. Comput. PD JUL-SEP PY 2014 VL 36 IS 3 BP 94 EP 95 PG 2 WC Computer Science, Theory & Methods; History & Philosophy Of Science SC Computer Science; History & Philosophy of Science GA AW5MT UT WOS:000346319900016 ER PT J AU Brown, JW Copeland, RS Aarvik, L Miller, SE Rosati, ME Luke, Q AF Brown, J. W. Copeland, R. S. Aarvik, L. Miller, S. E. Rosati, M. E. Luke, Q. TI Host records for fruit-feeding Afrotropical Tortricidae (Lepidoptera) SO AFRICAN ENTOMOLOGY LA English DT Article DE DNA barcode; false codling moth; host plants; Kenya; leaf-rollers; macadamia nut borer; USAID ID FALSE CODLING MOTH; CRYPTOPHLEBIA-LEUCOTRETA MEYRICK; RAVENELIA-MACOWANIANA PAZSCHKE; ACACIA-KARROO HAYNE; SOUTH-AFRICA; DNA BARCODES; LANTANA-CAMARA; NATIVE FRUIT; MACADAMIA; KENYA AB We present host records for the following Afrotropical Tortricidae reared from fruit in Kenya: Idiothauma nr africanum Walsingham, Paraccra mimesa Razowski, Apotoforma nr uncifera Razowski, Eugnosta percnoptila. (Meyrick), Phtheochroa aarviki Razowski & Brown, Actihema hemiacta (Meyrick), Choristoneura dinota (Meyrick), Choristoneura occidentalis (Walsingham), Procrica nr ophiograpta (Meyrick), Metamesia nr episema.(Diakonoff), Epichoristodes acerbella (Walker), Cryptaspasma phycitinana Aarvik, Cryptaspasma subtilis Diakonoff complex, Cryptaspasma caryothia (Meyrick) complex, Cryptaspasma n. sp., Lobesia vanillana (Joannis), Lobesia semosa Diakonoff, Eccopsis nebulana Walsingham, Eccopsis praecedens Walsingham, Afrothreutes madoffei Aarvik, Afroploce nr karsholti Aarvik, Metendothenia balanacma (Meyricic), Endothenia ator Razowski & Brown, Anthozela chrysoxantha Meyridc, Anthozela psychotriae Razowski & Brown, Concinocordis wilsonarum Razowski & Brown, Crocidosema plebejana Zeller, Crocidosema lantana (Busck), Gypsonoma scolopiae Razowski &Brown, Cosmetra nereidopa (Meyrick), Cosmetra sp. 1, Cosmetra sp. 2, Cosmetra sp. 3, Cosmetra podocarpivora Razowski gt Brown, Cosmetra taitana Razowski & Brown, Thaumatotibia leucotreta (Meyrick), Thaumatotibia batrachopa (Meyrick), Thaumatotibia salaciae Razowski & Brown, Cryptophlebia semilunana (Saalmiiller), Cryptophlebia sp. 1, Cryptophlebia peltastica (Meyrick), Cydia connara Razowski & Brown, Cydia sennae Razowski & Brown, Cydia nr choleropa (Meyrick), Fulcrifera crotalariae Razowski & Brown, Fulcrifera nr periculosa (Meyrick), Fulcrifera sp. 1, Fulcrifera sp. 2, Dracontogena continentalis Karisch, Dracontogena solii Aarvik & Karisch, Grapholita limbata Diakonoff, Grapholita mesosocia (Meyridc), Grapholita nr mesosocia (Meyrick), Selania exornata (Diakonoff), Eucosmocydia monitrix (Meyrick), Stenentoma sorindeiae Razowski & Brown, and Thylacogaster garcinivora Razowski & Brown. Nearly 75 % of all our reared tortricids are members of Grapholitini, a tribe that includes numerous pests of fruit worldwide. Approximately 77 % of the reared species are recorded from only one or two different plants species (frequently in the same plant genus). Plant families that support the greatest numbers of tortricid fruit-feeders are Rubiaceae (13 tortricid species), Ochnaceae (11 tortricid species), Sapindaceae (10 tortricid species), Rosaceae (8 tortricid species), Connaraceae (7 tortricid species) and Fabaceae (7 tortricid species). We also review previously reported food plants and provide a few new records for four foliage- and/or fruit-feeding tortricids from the Afrotopical Region, e.g. Goniotorna erratica (Diakonof-f), Taiteccopsis taitana Razowski, Cydia choleropa (Meyrick) and Leguminivora ptychora (Meyrick). Identifications are based on morphology and DNA barcodes (COI). C1 [Brown, J. W.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist, Washington, DC 20013 USA. [Copeland, R. S.] Int Ctr Insect Physiol & Ecol, Nairobi, Kenya. [Copeland, R. S.] Texas A&M Univ, Dept Entomol, College Stn, TX 77843 USA. [Aarvik, L.] Univ Oslo, Nat Hist Museum, NO-0318 Oslo, Norway. [Miller, S. E.; Rosati, M. E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Luke, Q.] E African Herbarium, Nairobi 00100, Kenya. RP Brown, JW (reprint author), ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. OI Miller, Scott/0000-0002-4138-1378 FU Ministry for Foreign Affairs of Finland for the CHIESA Project, Climate Change Impacts on Ecosystem Services and Food Security in Eastern Africa; Government of Canada through Genome Canada; Ontario Genomics Institute; Smithsonian Institution; USAID [PCE-G-00-98-0048-00]; USDA/CSREES/IFAFS [00-52103-9651] FX We are indebted to R. Bagine, formerly of the Kenya Wildlife Service, who was very helpful in granting permission to sample fruits within Kenyan forests. National Museums of Kenya also facilitated all stages of the research. The work of R.S.C. in the Taita Hills was supported with funds from the Ministry for Foreign Affairs of Finland for the CHIESA Project, Climate Change Impacts on Ecosystem Services and Food Security in Eastern Africa. We also thank K. Darrow and L. Helgen of the USNM for invaluable assistance with dissections and preparation of the reared material. DNA sequencing was supported by a grant from the Government of Canada through Genome Canada and the Ontario Genomics Institute in support of the iBOL project, courtesy of P. Hebert, with additional support from the Smithsonian Institution. This work was supported in part by USAID grant no. PCE-G-00-98-0048-00 (in collaboration with the International Centre of Insect Physiology and Ecology and its African Fruit Fly Initiative) and in part by USDA/CSREES/IFAFS grant no. 00-52103-9651, both to R.A. Wharton, Texas A&M University The following provided helpful reviews that enhanced the clarity and quality of the final paper: T Gilligan, USDA, APHIS, PPQ, CPHST, Fort Collins Laboratory, Fort Coffins, Colorado, U.S.A.; and J. Baixeras, Cavanilles Institute of Biodiversity and Evolutionary Biology, University of Valencia, Paterna, Spain. NR 131 TC 7 Z9 7 U1 2 U2 12 PU ENTOMOLOGICAL SOC SOUTHERN AFRICA PI HATFIELD PA PO BOX 13162, HATFIELD 0028, SOUTH AFRICA SN 1021-3589 EI 1026-4914 J9 AFR ENTOMOL JI Afr. Entomol. PD JUL PY 2014 VL 22 IS 2 BP 343 EP 376 PG 34 WC Entomology SC Entomology GA AR5HO UT WOS:000343616000014 ER PT J AU Buffington, ML Forshage, M AF Buffington, Matthew L. Forshage, Mattias TI THE DESCRIPTION OF GARUDELLA BUFFINGTON AND FORSHAGE, NEW GENUS (HYMENOPTERA: FIGITIDAE: EUCOILINAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Kleidotomini; occipital impression; new species; new genus; morphology; Thailand; Laos; Vietnam ID REVISION AB Garudella, a remarkable new genus of eucoiline wasp is described from Thailand, Laos, and the Republic of Congo. Four new species of Garudella are described as well: G. acothonaspis, G. afrotropica, G. algo, and G. alicae. Several autapomorphies distinguish this genus from other eucoiline genera: a distinctly protracted and broadened pronotal plate; a massive, posteriorly protruding propodeum; reduced posterior rim of metapleuron; reduced scutellar foveae and lack of lateral bar ''windows''; and a generally reduced scutellar plate. In addition, the posterior of the head has a distinctly curved occipital impression, resulting in the cuticle surrounding the foramen magnum to be extruded into a neck-like process. The biology of Garudella is unknown, but based on phylogenetic inference from morphology, the presumed host could be a cyclorrhaphous Diptera in a saprophagous environment. C1 [Buffington, Matthew L.] USDA, Smithsonian NMNH, Systemat Entomol Lab, Washington, DC 20013 USA. [Forshage, Mattias] Nat Hist Riksmuseet, Dept Entomol, SE-10405 Stockholm, Sweden. RP Buffington, ML (reprint author), USDA, Smithsonian NMNH, Systemat Entomol Lab, 10th & Constitut Ave NW, Washington, DC 20013 USA. EM matt.buffington@ars.usda.gov; Mattias.Forshage@nrm.se FU Systematic Entomology Lab (USDA-ARS); Smithsonian Institution Short-term Visitor Grants program; NSF [DEB-0542864, EF-0337220] FX We thank Mike Sharkey (University of Kentucky) and Brian Brown (Los Angeles County Museum) for inviting us to collaborate on the cynipoid portion of the TIGER Project. Smithsonian Institution intern Agnes Cororaton helped considerably in mounting and labeling cynipoids collected in the TIGER Project, and her help is greatly appreciated. Taina Litwak (Systematic Entomology Lab, USDA-ARS) produced the fantastic painting found in Figure 1; Sarah King (SI Intern Program) edited Fig. 7. Guilherme Baiao (NHRS) found the Vietnamese Garudella specimens in RMNH, where Kees van Achterberg and Frederique Bakker assisted with guidance and loans. Fritz Gusenleitner and Martin Schwarz (OSML, Linz, Austria) assisted MF with the loan of the first Vietnamese specimen. Funding was provided to MB by the Systematic Entomology Lab (USDA-ARS) and a short-term visitors grant to the USNM for MF was provided by the Smithsonian Institution Short-term Visitor Grants program. Funding for Mike Sharkey and Brian Brown for running Malaise traps in Thailand was provided by NSF grants DEB-0542864 and EF-0337220. USDA is an equal opportunity provider and employer. NR 12 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2014 VL 116 IS 3 BP 225 EP 242 DI 10.4289/0013-8797.116.3.225 PG 18 WC Entomology SC Entomology GA AQ9PL UT WOS:000343187700001 ER PT J AU Buffington, ML Perkovsky, EE Brady, SG AF Buffington, Matthew L. Perkovsky, Evgeny E. Brady, Sean G. TI THE DESCRIPTION OF ROVNOEUCOILA TYMPANOMORPHA BUFFINGTON AND PERKOVSKY, A NEW GENUS AND SPECIES OF FOSSIL EUCOILINE, WITH OBSERVATIONS ON THE ASYNCHRONOUS EVOLUTION OF DIGLYPHOSEMATINI (HYMENOPTERA: FIGITIDAE: EUCOILINAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Rovno amber; amber inclusion; divergence estimation; parasitoid ID CALIBRATION UNCERTAINTY; GALL WASPS; CYNIPOIDEA; PARASITOIDS; FORMICIDAE; CYNIPIDAE; PHYLOGENY; INSECTA; HISTORY; AMBER AB A new genus and species of Eucoilinae, Rovnoeucoila tympanomorpha Buffington and Perkovsky, from a Rovno Amber inclusion, is described. This new taxon differs from extant eucoilines by having a clearly segmented metasoma and singular flagellomere morphology in the antenna. The new taxon is included in the re-analysis of a fossil calibrated, relaxed molecular clock divergence date analysis of Figitidae. The new analysis infers a mean crown group age for Eucoilinae at approximately 10 million years younger than previously estimated. The age of the eucoiline tribe Diglyphosematini does not change substantially in our new dating analysis, and is much younger when compared to the age of its host lineage Agromyzidae (Diptera); we discuss potential implications of this situation within the context of natural enemy selection in biological control projects that include parasitoid Hymenoptera. C1 [Buffington, Matthew L.] USDA, Smithsonian NMNH, Systemat Entomol Lab, Washington, DC 20013 USA. [Perkovsky, Evgeny E.] NAS Ukraine, Schmalhausen Inst Zool, UA-01601 Kiev, Ukraine. [Brady, Sean G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Buffington, ML (reprint author), USDA, Smithsonian NMNH, Systemat Entomol Lab, 10th & Constitut Ave NW, Washington, DC 20013 USA. EM matt.buffington@ars.usda.gov; perkovsk@gmail.com; bradys@si.edu NR 36 TC 2 Z9 3 U1 1 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2014 VL 116 IS 3 BP 243 EP 254 DI 10.4289/0013-8797.116.3.243 PG 12 WC Entomology SC Entomology GA AQ9PL UT WOS:000343187700002 ER PT J AU Cecil, CB DiMichele, WA Elrick, SD AF Cecil, C. Blaine DiMichele, William A. Elrick, Scott D. TI Middle and Late Pennsylvanian cyclothems, American Midcontinent: Ice-age environmental changes and terrestrial biotic dynamics SO COMPTES RENDUS GEOSCIENCE LA English DT Article DE Climate; Coal; Cyclothem; Paleoecology; Pennsylvanian ID CENTRAL APPALACHIAN BASIN; CLIMATE-CHANGE; NORTH-AMERICA; PALEOCLIMATE CONTROLS; PERMIAN PALEOBOTANY; TROPICAL LOWLANDS; GEOLOGICAL TIME; ILLINOIS BASIN; GLACIAL PHASES; PEAT FORMATION AB The Pennsylvanian portion of the Late Paleozoic Ice Age was characterized by stratigraphic repetition of chemical and siliciclastic rocks in the equatorial regions of the Pangean interior. Known as "cyclothems", these stratigraphic successions are a 10(5) yr-record of glacial waxing and waning, superimposed on longer term, 10(6) yr intervals of global warming and cooling and a still longer term trend of increasing equatorial aridity. During periods of maximum ice-minimum sea level, the interior craton was widely exposed. Epicontinental landscapes were initially subjected to dry subhumid climate when first exposed, as sea level fell, but transitioned to humid climates and widespread wetlands during maximum lowstands. During interglacials (ice-minima) seasonally dry vegetation predominated. The wetland and seasonally dry biomes were compositionally distinct and had different ecological and evolutionary dynamics. Published by Elsevier Masson SAS on behalf of Academie des sciences. C1 [Cecil, C. Blaine] US Geol Survey, Rockbridge Baths, VA 24473 USA. [Cecil, C. Blaine; DiMichele, William A.] Smithsonian Inst, NMNH, Dept Paleobiol, Washington, DC 20560 USA. [Elrick, Scott D.] Univ Illinois, Illinois State Geol Survey, Champaign, IL 61820 USA. RP DiMichele, WA (reprint author), Smithsonian Inst, NMNH, Dept Paleobiol, MRC-121, Washington, DC 20560 USA. EM dimichel@si.edu FU U.S. Geological Survey; Smithsonian Institution; State of Illinois FX We thank Sylvie Bourquin for the invitation to submit this paper. Research supported by U.S. Geological Survey, Smithsonian Institution, and State of Illinois. We thank many colleagues for sharing their ideas and expertise. NR 107 TC 9 Z9 9 U1 2 U2 18 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1631-0713 EI 1778-7025 J9 CR GEOSCI JI C. R. Geosci. PD JUL-AUG PY 2014 VL 346 IS 7-8 BP 159 EP 168 DI 10.1016/j.crte.2014.03.008 PG 10 WC Geosciences, Multidisciplinary SC Geology GA AQ1FF UT WOS:000342526600001 ER PT J AU Remo, JL Haubold, HJ AF Remo, John L. Haubold, Hans J. TI Threats from space: 20 years of progress SO BULLETIN OF THE ATOMIC SCIENTISTS LA English DT Article DE asteroid; Chelyabinsk; comet; near-Earth object; NEO; United Nations ID CHELYABINSK; METEORITE; AIRBURST; EARTH AB It has been 20 years since planning began for the 1995 United Nations International Conference on Near-Earth Objects. The conference proceedings established the scientific basis for an international organizational framework to support research and collective actions to mitigate a potential near-Earth object (NEO) threat to the planet. Since that time, researchers have conducted telescope surveys that should, within the coming decade, answer many questions about the size, number, and Earth impact probability of these objects. Space explorations to asteroids and comets have been successfully carried out, including sample recovery. Laboratory experiments and computer simulations at Sandia National Laboratories have analyzed the effects of high-energy-density soft x-ray radiation on meteorites-which might help researchers develop a way to redirect an incoming asteroid by vaporizing a thin layer of its surface. An Action Team on NEOs, established in 2001 in response to recommendations of the Third United Nations Conference on the Exploration and Peaceful Uses of Outer Space, identified the primary components of NEO mitigation and emphasized the value of finding potentially hazardous NEOs as soon as possible. Recommendations from the action team are meant to ensure that all nations are aware of the NEO danger, and to coordinate mitigation activities among nations that could be affected by an impact, as well as those that might play an active role in any eventual deflection or disruption campaign. C1 [Remo, John L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Remo, John L.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Remo, John L.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Remo, John L.] Sandia Natl Labs, Livermore, CA 94550 USA. [Haubold, Hans J.] UN, Off Outer Space Affairs, Vienna, Austria. [Haubold, Hans J.] Ctr Math Sci, Pala, India. [Haubold, Hans J.] UN Basic Space Sci Initiat, Berkeley, CA USA. RP Remo, JL (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 22 TC 1 Z9 1 U1 1 U2 11 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0096-3402 EI 1938-3282 J9 B ATOM SCI JI Bull. Atom. Scient. PD JUL-AUG PY 2014 VL 70 IS 4 BP 85 EP 93 DI 10.1177/0096340214539125 PG 9 WC International Relations; Social Issues SC International Relations; Social Issues GA AP1NN UT WOS:000341837400012 ER PT J AU Crida, A Batygin, K AF Crida, A. Batygin, K. TI Spin-orbit angle distribution and the origin of (mis)aligned hot Jupiters SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites: formation; planets and satellites: dynamical evolution and stability; planet-disk interactions; methods: statistical ID INTERNAL GRAVITY-WAVES; PLANET SCATTERING; TAURUS-AURIGA; YOUNG STARS; MIGRATION; SYSTEMS; MISALIGNMENTS; INSTABILITY; ROTATION; MODEL AB Context. For 61 transiting hot Jupiters, the projection of the angle between the orbital plane and the stellar equator (called the spin-orbit angle) has been measured. For about half of them, a significant misalignment is detected, and retrograde planets have been observed. This challenges scenarios of the formation of hot Jupiters. Aims. In order to better constrain formation models, we relate the distribution of the real spin-orbit angle Psi to the projected one beta. Then, a comparison with the observations is relevant. Methods. We analyse the geometry of the problem to link analytically the projected angle beta to the real spin-orbit angle Psi. The distribution of Psi expected in various models is taken from the literature, or derived with a simplified model and Monte Carlo simulations in the case of the disk-torquing mechanism. Results. An easy formula to compute the probability density function (PDF) of beta knowing the PDF of Psi is provided. All models tested here look compatible with the observed distribution beyond 40 degrees, which is so far poorly constrained by only 18 observations. But only the disk-torquing mechanism can account for the excess of aligned hot Jupiters, provided that the torquing is not always efficient. This is the case if the exciting binaries have semi-major axes as large as similar to 10(4) AU. Conclusions. Based on comparison with the set of observations available today, scattering models and the Kozai cycle with tidal friction models can not be solely responsible for the production of all hot Jupiters. Conversely, the presently observed distribution of the spin-orbit angles is compatible with most hot Jupiters having been transported by smooth migration inside a proto-planetary disk, itself possibly torqued by a companion. C1 [Crida, A.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR 7293, F-06300 Nice, France. [Batygin, K.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Crida, A (reprint author), Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR 7293, F-06300 Nice, France. EM crida@oca.eu FU ITC Prize Postdoctoral Fellowship at the Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics FX K.B. acknowledges the generous support from the ITC Prize Postdoctoral Fellowship at the Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org (Wright et al. 2011). We thank the referee C. Beauge, as well as D. Nesvorny, for comments and suggestions that led to improvement of this article. We further thank S. Tremaine for pointing out a mistake (now corrected) in our Sect. 2.4. NR 50 TC 20 Z9 20 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2014 VL 567 AR A42 DI 10.1051/0004-6361/201323292 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VU UT WOS:000341185300057 ER PT J AU D'Ago, G Paolillo, M Fabbiano, G Puzia, TH Maccarone, TJ Kundu, A Goudfrooij, P Zepf, SE AF D'Ago, G. Paolillo, M. Fabbiano, G. Puzia, T. H. Maccarone, T. J. Kundu, A. Goudfrooij, P. Zepf, S. E. TI Luminosity function of low-mass X-ray binaries in the globular cluster system of NGC 1399 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: binaries; X-rays: galaxies; galaxies: elliptical and lenticular, cD; galaxies: individual: NGC 1399 ID EARLY-TYPE GALAXIES; HUBBLE-SPACE-TELESCOPE; STAR-FORMING GALAXIES; ELLIPTIC GALAXIES; STELLAR MASS; WIDE-FIELD; MILKY-WAY; CHANDRA; CONNECTION; POPULATION AB Aims. We present a study of the faint end of the X-ray luminosity function (XLF) of low-mass X-ray binaries (LMXBs) in the Globular Cluster (GC) system of the cD galaxy NGC 1399. Methods. We performed a stacking experiment on 618 X-ray undetected GCs. in order to verify the Presence of faint LMXBs and to constrain the faint end slope of the GC-LMXBs XLF below the individual detection threshold of 8 x 10(37) erg s(-1) in the 0.5-8 keV band. Results. We obtain a significant X-ray detection for the whole GC sample, as well as for the red and blue GC subpopulations, corresponding to an average luminosity per GC < L-X >(GC) of (3.6 +/- 1.0) x 10(36) erg s(-1), (6.9 +/- 2.1) x 10(36) erg s(-1), and (1.7 +/- 0.9) x 10(36) erg s(-1), respectively, for all GCs, red GCs, and blue GCs. If LMXBs in red and blue GCs have the same average intrinsic luminosity, we derive a red/blue ratio similar or equal to 3 of GCs hosting LMXBs (2.5 +/- 1.0 or 4.1 +/- 2.5 depending on the surveyed region); alternatively, assuming the fractions observed for brighter sources, we measure an average X-ray luminosity of L-X = (4.3 +/- 1.3) x 10(37) erg s(-1) and L-X = (3.4 +/- 1.7) x 10(37) erg s(-1) per red and blue GC-LMXBs, respectively. In the assumption that the XLF follows a power-law distribution, we find that a low luminosity break is required at L-X <= 8 x 10(37) erg s(-1) both in the whole, as well as in the color-selected (red and blue) subsamples. Given the bright-end slopes measured above the X-ray completeness limit, this result is significant at >3 sigma level. Our best estimates for the faint-end slope are beta(L) = -1.39/-1.38/-1.36 for all/red/blue GC-LMXBs. We also find evidence that the luminosity function becomes steeper at luminosities L-X greater than or similar to 3 x 10(39) erg s(-1), as observed in old ellipticals. Conclusions. If most GCs host a single X-ray binary, we conclude that in NGC 1399 the XLF flattens at low luminosities as observed in other nearer galaxies, and we discuss some consequences of this flattening on LMXBs formation scenarios. C1 [D'Ago, G.; Paolillo, M.] Univ Naples Federico II, Dept Phys, I-80126 Naples, Italy. [D'Ago, G.] Univ Salerno, Phys Dept ER Caianiello, I-84084 Fisciano, Italy. [D'Ago, G.] INFN, Grp Collegato Salerno, Sez Napoli, I-84084 Fisciano, Italy. [Paolillo, M.] INFN, Sez Napoli, I-80126 Naples, Italy. [Paolillo, M.] ASI Sci Data Ctr, I-00133 Rome, Italy. [Fabbiano, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Puzia, T. H.] Pontificia Univ Catolica Chile, Inst Astrophys, Santiago 7820436, Chile. [Maccarone, T. J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Maccarone, T. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Kundu, A.] TIFR, Bombay 400005, Maharashtra, India. [Kundu, A.] Eureka Sci Inc, Oakland, CA 94602 USA. [Goudfrooij, P.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Zepf, S. E.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP D'Ago, G (reprint author), Univ Naples Federico II, Dept Phys, Via Cinthia 9, I-80126 Naples, Italy. EM paolillo@na.infn.it RI Paolillo, Maurizio/J-1733-2012; D'Ago, Giuseppe/N-8318-2016 OI Paolillo, Maurizio/0000-0003-4210-7693; D'Ago, Giuseppe/0000-0001-9697-7331 FU University Federico II of Naples; NSF [1066293i] FX M.P. acknowledges support from the FARO 2011 project from the University Federico II of Naples. He also thanks the International Academic Exchange Fund of the "Vicerrectoria Academica" at the Pontificia Universidad Catolica in Santiago, and the Department of Astronomy and Astrophysics for providing travel and lodging support. G.F. is grateful for the hospitality of the Aspen Center for Physics supported by NSF grant No 1066293i. NR 56 TC 1 Z9 1 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2014 VL 567 AR A2 DI 10.1051/0004-6361/201322722 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VU UT WOS:000341185300024 ER PT J AU Desidera, S Bonomo, AS Claudi, RU Damasso, M Biazzo, K Sozzetti, A Marzari, F Benatti, S Gandolfi, D Gratton, R Lanza, AF Nascimbeni, V Andreuzzi, G Affer, L Barbieri, M Bedin, LR Bignamini, A Bonavita, M Borsa, F Calcidese, P Christille, JM Cosentino, R Covino, E Esposito, M Giacobbe, P Harutyunyan, A Latham, D Lattanzi, M Leto, G Lodato, G Lovis, C Maggio, A Malavolta, L Mancini, L Fiorenzano, AFM Micela, G Molinari, E Mordasini, C Munari, U Pagano, L Pedani, M Pepe, F Piotto, G Poretti, E Rainer, M Ribas, I Santos, NC Scandariato, G Silvotti, R Southworth, J Sanchez, RZ AF Desidera, S. Bonomo, A. S. Claudi, R. U. Damasso, M. Biazzo, K. Sozzetti, A. Marzari, F. Benatti, S. Gandolfi, D. Gratton, R. Lanza, A. F. Nascimbeni, V. Andreuzzi, G. Affer, L. Barbieri, M. Bedin, L. R. Bignamini, A. Bonavita, M. Borsa, F. Calcidese, P. Christille, J. M. Cosentino, R. Covino, E. Esposito, M. Giacobbe, P. Harutyunyan, A. Latham, D. Lattanzi, M. Leto, G. Lodato, G. Lovis, C. Maggio, A. Malavolta, L. Mancini, L. Fiorenzano, A. F. Martinez Micela, G. Molinari, E. Mordasini, C. Munari, U. Pagano, L. Pedani, M. Pepe, F. Piotto, G. Poretti, E. Rainer, M. Ribas, I. Santos, N. C. Scandariato, G. Silvotti, R. Southworth, J. Sanchez, R. Zanmar TI The GAPS programme with HARPS-N at TNG IV. A planetary system around XO-2S SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: radial velocities; planetary systems; stars: individual: XO-2S; stars: individual: XO-2N ID RADIAL-VELOCITY MEASUREMENTS; CHAIN MONTE-CARLO; EXTRASOLAR PLANETS; BINARY-SYSTEMS; HOT JUPITERS; HOST STARS; COMPANIONS; EXOPLANETS; SEARCH; II. AB We performed an intensive radial velocity monitoring of XO-2S, the wide companion of the transiting planet-host XO-2N, using HARPS-N at TNG in the framework of the GAPS programme. The radial velocity measurements indicate the presence of a new planetary system formed by a planet that is slightly more massive than Jupiter at 0.48 au and a Saturn-mass planet at 0.13 au. Both planetary orbits are moderately eccentric and were found to be dynamically stable. There are also indications of a long-term trend in the radial velocities. This is the first confirmed case of a wide binary whose components both host planets, one of which is transiting, which makes the XO-2 system a unique laboratory for understanding the diversity of planetary systems. C1 [Desidera, S.; Claudi, R. U.; Marzari, F.; Benatti, S.; Gratton, R.; Nascimbeni, V.; Bedin, L. R.; Bonavita, M.; Munari, U.; Piotto, G.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Bonomo, A. S.; Damasso, M.; Sozzetti, A.; Giacobbe, P.; Lattanzi, M.; Silvotti, R.] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. [Damasso, M.; Calcidese, P.; Christille, J. M.] Osservatorio Astron Reg Autonoma Valle Aosta, I-11020 Nus, Aosta, Italy. [Biazzo, K.; Gandolfi, D.; Lanza, A. F.; Cosentino, R.; Leto, G.; Pagano, L.; Scandariato, G.; Sanchez, R. Zanmar] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Marzari, F.] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35131 Padua, Italy. [Gandolfi, D.] Heidelberg Univ, ZAH, Landessternwarte Konigstuhl, D-69117 Heidelberg, Germany. [Nascimbeni, V.; Barbieri, M.; Malavolta, L.; Piotto, G.] Univ Padua, Dip Fis & Astron Galileo Galilei, I-35122 Padua, Italy. [Andreuzzi, G.; Cosentino, R.; Harutyunyan, A.; Fiorenzano, A. F. Martinez; Molinari, E.; Pedani, M.] Fdn Galileo Galilei INAF, Brena Baja 38712, Spain. [Affer, L.; Maggio, A.; Micela, G.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Bignamini, A.] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Borsa, F.; Poretti, E.; Rainer, M.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Christille, J. M.] Univ Perugia, Dept Phys, I-06123 Perugia, Italy. [Covino, E.] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy. [Esposito, M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Latham, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lodato, G.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Lovis, C.; Malavolta, L.; Pepe, F.] Univ Geneva, Astron Observ, CH-1290 Sauverny, Versoix, Switzerland. [Mancini, L.; Mordasini, C.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Molinari, E.] INAF IASF Milano, I-20133 Milan, Italy. [Ribas, I.] Fac Ciencies, Inst Ciencies Espai CSIC IEEC, Bellaterra 08193, Spain. [Santos, N. C.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Santos, N. C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4150762 Oporto, Portugal. [Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. RP Desidera, S (reprint author), INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. EM silvano.desidera@oapd.inaf.it RI Santos, Nuno/E-9957-2011; Leto, Giuseppe/N-3355-2015; Maggio, Antonio/P-5700-2015; OI Gratton, Raffaele/0000-0003-2195-6805; Sozzetti, Alessandro/0000-0002-7504-365X; Lattanzi, Mario Gilberto/0000-0003-0429-7748; bedin, luigi/0000-0003-4080-6466; Santos, Nuno/0000-0003-4422-2919; Poretti, Ennio/0000-0003-1200-0473; Lanza, Antonino Francesco/0000-0001-5928-7251; Gandolfi, Davide/0000-0001-8627-9628; Munari, Ulisse/0000-0001-6805-9664; Piotto, Giampaolo/0000-0002-9937-6387; Leto, Giuseppe/0000-0002-0040-5011; Molinari, Emilio/0000-0002-1742-7735; Maggio, Antonio/0000-0001-5154-6108; Silvotti, Roberto/0000-0002-1295-8174; Biazzo, Katia/0000-0002-1892-2180; Covino, Elvira/0000-0002-6187-6685; Desidera, Silvano/0000-0001-8613-2589; Barbieri, Mauro/0000-0001-8362-3462; Micela, Giuseppina/0000-0002-9900-4751 FU INAF through the "Progetti Premiali" funding scheme of the Italian Ministry of Education, University, and Research; Regional Government of the Aosta Valley; Town Municipality of Nus; Mont Emilius Community; EU-ESF; Autonomous Region of the Aosta Valley; Italian Ministry of Labour and Social Policy; ASI [I/037/08/0, I/058/10/0]; Fondazione CRT; EU [267251]; Fundacao para a Ciencia e a Tecnologia (FCT, Portugal) [RECI/FIS-AST/0176/2012 (FCOMP-01-0124-FEDER-027493), RECI/FIS-AST/0163/2012 (FCOMP-01-0124-FEDER-027492)]; FCT [IF/00169/2012]; POPH/FSE (EC) - FEDER through the program Programa Operacional de Factores de Competitividade - COMPETE; ERC/EC [239953] FX The GAPS project in Italy acknowledges support from INAF through the "Progetti Premiali" funding scheme of the Italian Ministry of Education, University, and Research. The Aosta Valley Observatory is supported by the Regional Government of the Aosta Valley, the Town Municipality of Nus and the Mont Emilius Community. J.M.C. is supported by a grant of the EU-ESF, the Autonomous Region of the Aosta Valley and the Italian Ministry of Labour and Social Policy. We thank ASI (through contracts I/037/08/0 and I/058/10/0) and the Fondazione CRT for their support to the APACHE Project. D. G. acknowledges support from the EU FP7 under grant agreement No. 267251. N.C.S. acknowledges support from Fundacao para a Ciencia e a Tecnologia (FCT, Portugal) through the FEDER funds in the program COMPETE, as well as through national funds, in the form of grants references RECI/FIS-AST/0176/2012 (FCOMP-01-0124-FEDER-027493), and RECI/FIS-AST/0163/2012 (FCOMP-01-0124-FEDER-027492), and in the form of the Investigador FCT contract reference IF/00169/2012 and POPH/FSE (EC) by the FEDER funding through the program Programa Operacional de Factores de Competitividade - COMPETE. N.C.S. furthermore acknowledges support from the ERC/EC under the FP7 through Starting Grant agreement No. 239953. We thank the TNG staff for help with the observations. NR 34 TC 14 Z9 14 U1 0 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2014 VL 567 AR L6 DI 10.1051/0004-6361/201424339 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VU UT WOS:000341185300154 ER PT J AU Frau, P Girart, JM Zhang, Q Rao, R AF Frau, P. Girart, J. M. Zhang, Q. Rao, R. TI Shaping a high-mass star-forming cluster through stellar feedback The case of the NGC 7538 IRS 1-3 complex SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: individual objects: NGC 7538 IRS 1; ISM: magnetic fields; stars: formation; polarization; submillimeter: ISM; techniques: interferometric ID NGC-7538 MOLECULAR CLOUD; 1333 IRAS 4A; MAGNETIC-FIELDS; PROTOSTELLAR CORES; VLA OBSERVATIONS; METHANOL MASERS; RECOMBINATION LINE; CIRCUMSTELLAR DISK; HII-REGIONS; OUTFLOWS AB Context. NGC 7538 IRS 1-3 is a high-mass star-forming cluster with several detected dust cores, infrared sources, (ultra) compact H II regions, molecular outflows, and masers. In such a complex environment, interactions and feedback among the embedded objects are expected to play a major role in the evolution of the region. Aims. We study the dust, kinematic, and polarimetric properties of the NGC 7538 IRS 1-3 region to investigate the role of the different forces in the formation and evolution of high-mass star-forming clusters. Methods. We performed SMA high angular resolution observations at 880 mu m with the compact configuration. We developed the RATPACKS code to generate synthetic velocity cubes from models of choice to be compared to the observational data. To quantify the stability against gravitational collapse we developed the "mass balance" analysis that accounts for all the energetics on core scales. Results. We detect 14 dust cores from 3.5 M-circle dot to 37 M-circle dot arranged in two larger scale structures: a central bar and a filamentary spiral arm. The spiral arm presents large-scale velocity gradients in (HCO+)-C-13 4-3 and (CO)-O-17 3-2, and magnetic field segments aligned well to the dust main axis. The velocity gradient is reproduced well by a spiral arm expanding at 9 km s(-1) with respect to the central core MM1, which is known to power a large precessing outflow. The energy of the outflow is comparable to the spiral-arm kinetic energy, which dominates gravitational and magnetic energies. In addition, the dynamical ages of the outflow and spiral arm are comparable. On core scales, those embedded in the central bar seem to be unstable against gravitational collapse and prone to forming high-mass stars, while those in the spiral arm have lower masses that seem to be supported by non-thermal motions and magnetic fields. Conclusions. The NGC 7538 IRS 1-3 cluster seems to be dominated by protostellar feedback. The dusty spiral arm appears to be formed in a snowplow fashion owing to the outflow from the MM1 core. We speculate that the external pressure from the redshifted lobe of the outflow could trigger star formation in the spiral arm cores. This scenario would form a small cluster with a few central high-mass stars, surrounded by a number of low-mass stars formed through protostellar feedback. C1 [Frau, P.] CSIC, Inst Ciencia Mat Madrid, Madrid 28049, Spain. [Frau, P.] Observ Astron Nacl, Madrid 28014, Spain. [Girart, J. M.] CSIC IEEC, Fac Ciencies, Inst Ciencies Espai, Bellaterra 08193, Catalonia, Spain. [Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rao, R.] Acad Sinica, Inst Astron & Astrophys, Hilo, HI 96720 USA. RP Frau, P (reprint author), CSIC, Inst Ciencia Mat Madrid, Sor Juana Ines de la Cruz 3, Madrid 28049, Spain. EM pfrau@icmm.csic.es; girart@ice.cat; qzhang@cfa.harvard.edu; rrao@sma.hawaii.edu RI Girart, Josep/O-1638-2014; OI Girart, Josep/0000-0002-3829-5591; Zhang, Qizhou/0000-0003-2384-6589 FU Spanish CONSOLIDER [CSD2009-00038]; Spanish MINECO [AYA2011-30228-C03-02]; Catalan AGAUR [2009SGR1172] FX We thank all members of the SMA staff that made these observations possible. This research made use of NASA's Astrophysics Data System Bibliographic Services (http://adsabs.harvard.edu/), the SIMBAD database, operated at the CDS, Strasbourg, France (http ://simbad.u-strasbg.fr/simbad/), and the Splatalogue database for astronomical spectroscopy (http://www.splatalogue.net). We thank the anonymous referee for the useful comments. PF is supported by the Spanish CONSOLIDER project CSD2009-00038. PF and JMG are supported by the Spanish MINECO AYA2011-30228-C03-02 and Catalan AGAUR 2009SGR1172 grants. NR 69 TC 6 Z9 6 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2014 VL 567 AR A116 DI 10.1051/0004-6361/201423917 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VU UT WOS:000341185300133 ER PT J AU Gallenne, A Kervella, P Merand, A Evans, NR Girard, JHV Gieren, W Pietrzynski, G AF Gallenne, A. Kervella, P. Merand, A. Evans, N. R. Girard, J. H. V. Gieren, W. Pietrzynski, G. TI Searching for visual companions of close Cepheids VLT/NACO lucky imaging of Y Oph, FF Aql, X Sgr, W Sgr, and eta Aql SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation: adaptive optics; techniques: high angular resolution; stars: variables: Cepheids; binaries: visual ID PERIOD-LUMINOSITY RELATIONS; ICCD SPECKLE OBSERVATIONS; BASE-LINE INTERFEROMETRY; ECLIPSING BINARY-SYSTEM; HUBBLE-SPACE-TELESCOPE; PEAK 4-M TELESCOPE; CLASSICAL CEPHEID; GALACTIC CEPHEIDS; INTRINSIC COLORS; STARS AB Aims. High-resolution imaging in several photometric bands can provide color and astrometric information of the wide orbit component of Cepheid stars. Such measurements are needed to understand the age and evolution of pulsating stars. In addition, binary Cepheids have the potential to provide direct and model-independent distances and masses. Methods. We used the NAOS-CONICA adaptive optics instrument (NACO) in the near-infrared to perform a deep search for wide components around the classical Cepheids, Y Oph, FF Aql, X Sgr, W Sgr, and eta Aql, within a field of view of 1,7" x 1.7" (3.4" x 3.4" for eta Aql), Results. We were able to reach contrast Delta N = 5-8 mag and Delta K, = 4-7 mag in the radius range r > 0.2", which enabled us to constrain the presence of wide companions. For Y Oph, FF Aql, X Sgr, W Sgr, and eta Aql at r > 0.2", we ruled out the presence of companions with a spectral type that is earlier than a B7V, A9V, A9V, AIN, and G5V star, respectively. For 0.1" < r < 0.2". no companions earlier than O9V. B3V, B4V, B2V, and B2V star, respectively, are detected. A component is detected close to eta Aql at projected separation p 654.7 +/- 0.9 mas and a position angle PA = 92.8 +/- 0.1 degrees. We estimated its dereddened apparent magnitude to be m 9.34 +/- 0.04 and derived a spectral type that ranges between an F1V and an F6V star. Additional photometric and astrometric measurements are necessary to better constrain this star and check its physical association to the eta Aql system. C1 [Gallenne, A.; Gieren, W.; Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Kervella, P.] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris,UMR 8109, F-92195 Meudon, France. [Merand, A.; Girard, J. H. V.] European So Observ, Santiago 19, Chile. [Evans, N. R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Pietrzynski, G.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Gallenne, A (reprint author), Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion, Chile. EM agallenne@astro-udec.cl FU FONDECYT [3130361]; BASAL Centro de Astrofisica y Tecnologias Afines (CATA) [PFB-06/2007]; Polish National Science Center [MAESTRO 2012/06/A/ST9/00269]; Polish Ministry of Science grant Ideas Plus; "Programme National de Physique Stellaire" (PNPS) of CNRS/INSU, France; ECOS/Conicyt [C13U01]; PHASE; ONERA; Observatoire de Paris; CNRS; University Denis Diderot Paris 7 FX A.G. acknowledges support from FONDECYT grant 3130361. W.G. an G.P. gratefully acknowledge financial support for this work from the BASAL Centro de Astrofisica y Tecnologias Afines (CATA) PFB-06/2007. Support from the Polish National Science Center grant MAESTRO 2012/06/A/ST9/00269 and the Polish Ministry of Science grant Ideas Plus (awarded to G.P.) is also acknowledged. We acknowledge financial support from the "Programme National de Physique Stellaire" (PNPS) of CNRS/INSU, France, and the ECOS/Conicyt grant C13U01. This research received the support of PHASE, the high angular resolution partnership between ONERA, the Observatoire de Paris, CNRS, and University Denis Diderot Paris 7. This work made use of the SIMBAD and VizieR astrophysical database from the CDS, Strasbourg, France and the bibliographic informations from the NASA Astrophysics Data System. Data processing for this work has been done using the Yorick language which is freely available at http://yorick. sourceforgenet/ NR 63 TC 2 Z9 2 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2014 VL 567 AR A60 DI 10.1051/0004-6361/201423872 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VU UT WOS:000341185300125 ER PT J AU Jones, SC Houde, M Harwit, M Kidger, M Kraus, A McCoey, C Marston, A Melnick, G Menten, KM Morris, P Teyssier, D Tolls, V AF Jones, S. C. Houde, M. Harwit, M. Kidger, M. Kraus, A. McCoey, C. Marston, A. Melnick, G. Menten, K. M. Morris, P. Teyssier, D. Tolls, V. TI Polarisation observations of H2O J(K-1) K-1=5(32)-4(41) 620.701 GHz maser emission with Herschel/HIFI in Orion KL SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE magnetic fields; masers; polarisation; ISM: magnetic fields ID WATER MASER; RADIATION; HIFI AB Context. The high intensities and narrow bandwidths exhibited by some astronomical masers make them ideal tools for studying star-forming giant molecular clouds. The water maser transition JK(-1)K(1) = 5(32)-4(41) at 620.701 GHz can only be observed from above Earth's strongly absorbing atmosphere; its emission has recently been detected from space. Aims. We sought to further characterize the star-forming environment of Orion KL by investigating the linear polarisation of a source emitting a narrow 620.701 GHz maser feature with the heterodyne spectrometer HIFI on board the Herschel Space Observatory. Methods. High-resolution spectral datasets were collected over a thirteen month period beginning in 2011 March, to establish not only the linear polarisation but also the temporal variability of the source. Results. Within a 3 sigma uncertainty, no polarisation was detected to an upper limit of approximately 2%. These results are compared with coeval linear polarisation measurements of the 22.235 GHz J(K-1)K(1) = 6(16)-5(23) maser line from the Effelsberg 100-m radio telescope, typically a much stronger maser transition. Although strongly polarised emission is observed for one component of the 22.235 GHz maser at 7.2 km s(-1), a weaker component at the same velocity as the 620.701 GHz maser at 11.7 km s(-1) is much less polarised. C1 [Jones, S. C.; Houde, M.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Houde, M.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Harwit, M.] Cornell Univ, Ctr Radiophys & Space Res, Washington, DC 20024 USA. [Kidger, M.; Marston, A.; Teyssier, D.] European Space Agcy, ESAC, Herschel Sci Ctr, Madrid 28691, Spain. [Kraus, A.; Menten, K. M.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Melnick, G.; Tolls, V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Jones, SC (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. EM sjone7@uwo.ca FU NSERC; Canada Research Chair; Western's Academic Development Fund programs; NASA of JPL [1393122, 1463766] FX We thank D. Neufeld et al. (2013) for alerting us to the presence of the 621 GHz transition prior to publication. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA); Sweden: Chalmers University of Technology - MC2, RSS & GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Partly based on observations with the 100-m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg. M.H.'s research is funded through the NSERC Discovery Grant, Canada Research Chair, and Western's Academic Development Fund programs. The work of M.O.H. has been supported by NASA through awards of JPL subcontracts 1393122 and 1463766 to Cornell University. NR 16 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2014 VL 567 AR A31 DI 10.1051/0004-6361/201323267 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VU UT WOS:000341185300055 ER PT J AU Kacharov, N Bianchini, P Koch, A Frank, MJ Martin, NF van de Ven, G Puzia, TH McDonald, I Johnson, CI Zijlstra, AA AF Kacharov, N. Bianchini, P. Koch, A. Frank, M. J. Martin, N. F. van de Ven, G. Puzia, T. H. McDonald, I. Johnson, C. I. Zijlstra, A. A. TI A study of rotating globular clusters The case of the old, metal-poor globular cluster NGC 4372 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE globular clusters: general; globular clusters: individual: NGC 4372; Galaxy: halo ID HORIZONTAL-BRANCH STARS; STELLAR EVOLUTION DATABASE; AGE-METALLICITY RELATION; COLOR-MAGNITUDE DIAGRAM; WIDE-FIELD IMAGER; DARK-MATTER HALOS; MILKY-WAY; DYNAMICAL MODELS; HOMOGENEOUS PHOTOMETRY; POPULATION SYNTHESIS AB Context. NGC 4372 is a poorly studied old, very metal-poor globular cluster (GC) located in the inner Milky Way halo. Aims. We present the first in-depth study of the kinematic properties and derive the structural parameters of NGC 4372 based on the fit of a Plummer profile and a rotating, physical model. We explore the link between internal rotation to different cluster properties and together with similar studies of more GCs, we put these in the context of globular cluster formation and evolution. Methods. We present radial velocities for 131 cluster member stars measured from high-resolution FLAMES/GIRAFFE observations. Their membership to the GC is additionally confirmed from precise metallicity estimates. We build a velocity dispersion profile and a systemic rotation curve using this kinematic data set. Additionally, we obtain an elliptical number density profile of NGC 4372 based on optical images using a Markov chain Monte Carlo fitting algorithm. From this, we derive the cluster's half-light radius and ellipticity as rh = 3.44' +/- 0.04' and is an element of = 0.08 +/- 0.01. Finally, we give a physical interpretation of the observed morphological and kinematic properties of this GC by fitting an axisymmetric, differentially rotating, dynamical model. Results. Our results show that NGC 4372 has an unusually high ratio of rotation amplitude to velocity dispersion (1.2 vs. 4.5 km s(-1)) for its metallicity. This puts it in line, however, with two other exceptional, very metal-poor GCs: M 15 and NGC 4590. We also find a mild flattening of NGC 4372 in the direction of its rotation. Given its old age, this suggests that the flattening is indeed caused by the systemic rotation rather than tidal interactions with the Galaxy. Additionally, we estimate the dynamical mass of the GC M-dyn = 2.0 +/- 0.5 x 10(5) M-circle dot based on the dynamical model, which constrains the mass-to-light ratio of NGC 4372 between 1.4 and 2.3 M-circle dot/L-circle dot, representative of an old, purely stellar population. C1 [Kacharov, N.; Koch, A.; Frank, M. J.] Heidelberg Univ, Zentrum Astron, Landessternwarte, D-69117 Heidelberg, Germany. [Bianchini, P.; Martin, N. F.; van de Ven, G.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Martin, N. F.] Univ Strasbourg, CNRS, UMR 7550, Observ Astron Strasbourg, F-67000 Strasbourg, France. [Puzia, T. H.] Pontificia Univ Catolica Chile, Inst Astrophys, Santiago, Chile. [McDonald, I.; Zijlstra, A. A.] Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Johnson, C. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kacharov, N (reprint author), Heidelberg Univ, Zentrum Astron, Landessternwarte, Konigstuhl 12, D-69117 Heidelberg, Germany. EM n.kacharov@lsw.uni-heidelberg.de OI Koch, Andreas/0000-0002-9859-4956 FU Deutsche Forschungsgemeinschaft [Ko 4161/1]; Clay Fellowship; FONDECYT Regular Project [1121005]; BASAL Center for Astrophysics and Associated Technologies [PFB-06]; German Research Foundation (DFG) [Sonderforschungsbereich SFB 881]; National Aeronautics and Space Administration; National Science Foundation FX We thank Benjamin Hendricks for valuable discussions. N.K., A. K., and M.J.F. acknowledge the Deutsche Forschungsgemeinschaft for funding through Emmy-Noether grant Ko 4161/1. C.I.J. gratefully acknowledges support through the Clay Fellowship administered by the Smithsonian Astrophysical Observatory. T. H. P. acknowledges support in the form of a FONDECYT Regular Project Grant (No. 1121005) and from BASAL Center for Astrophysics and Associated Technologies (PFB-06). This work was in part supported by Sonderforschungsbereich SFB 881 "The Milky Way System" (subproject A4) of the German Research Foundation (DFG). 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 used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. This research has made use of NASA's Astrophysics Data System. NR 102 TC 15 Z9 15 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2014 VL 567 AR A69 DI 10.1051/0004-6361/201423709 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VU UT WOS:000341185300105 ER PT J AU Pillitteri, I Wolk, SJ Goodman, A Sciortino, S AF Pillitteri, Ignazio Wolk, Scott J. Goodman, Alyssa Sciortino, Salvatore TI Smooth X-ray variability from rho Ophiuchi A plus B A strongly magnetized primary B2 star? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE early-type; stars: activity; stars: magnetic field; stars: individual: rho Ophiuchi; starspots ID COUNTING DETECTOR IMAGES; DRIVEN STELLAR WINDS; THETA(1) ORIONIS-C; CHANDRA SPECTROSCOPY; WAVELET TRANSFORMS; HOT STAR; EMISSION; CLUSTER; CARINA; CLOUD AB X-rays from massive stars are ubiquitous yet not clearly understood. In an XMM-Newton observation devoted to observing the first site of star formation in the p Ophiuchi dark cloud, we detect smoothly variable X-ray emission from the B2IV+B2V system of rho Ophiuchi. We tentatively assign the emission to the primary component. The light curve of the pn camera shows a first phase of low, almost steady rate, then a rise phase of duration of 10 ks, followed by a high rate phase. The variability is seen primarily in the band 1.0-8.0 keV while little variability is detected below 1 keV. The spectral analysis of the three phases reveals the presence of a hot component at 3.0 keV that adds up to two relatively cold components at 0.9 keV and 2.2 keV. We explain the smooth variability with the emergence of an extended active region on the surface of the primary star as being due to its fast rotation (upsilon sin i similar to 315 km s(-1)). We estimate that the region has a diameter in the range 0.5-0.6 R-*. The hard X-ray emission and its variability hint at a magnetic origin, as suggested for a few other late-O through early-B type stars. We also discuss an alternative explanation based on the emergence from occultation of a young (5-10 Myr) low mass companion that is bright and hot in X-rays. C1 [Pillitteri, Ignazio; Sciortino, Salvatore] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Wolk, Scott J.; Goodman, Alyssa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pillitteri, I (reprint author), INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy. EM pilli@astropa.inaf.it RI Goodman, Alyssa/A-6007-2010; Pillitteri, Ignazio/L-1549-2016 OI Goodman, Alyssa/0000-0003-1312-0477; Pillitteri, Ignazio/0000-0003-4948-6550 FU European Union; NASA [NAS8-03060] FX I.P. acknowledges Dr. Mario Guarcello and Dr. Javier Lopez-Santiago for the helpful discussions on the topics of this paper. I.P. acknowledges financial support of the European Union under the project "Astronomy Fellowships in Italy" (AstroFit). S.J.W. was supported by NASA contract NAS8-03060. NR 32 TC 4 Z9 4 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2014 VL 567 AR L4 DI 10.1051/0004-6361/201424243 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VU UT WOS:000341185300152 ER PT J AU Cort, LA AF Cort, Louise Allison TI WHO MADE CHIGUSA? A Tea-leaf Storage Jar's Owners Over Seven Centuries SO ARTS OF ASIA LA English DT Article C1 [Cort, Louise Allison] Freer Gallery Art, Ceram, Washington, DC 20560 USA. [Cort, Louise Allison] Smithsonian Inst, Arthur M Sackler Gallery, Washington, DC 20560 USA. RP Cort, LA (reprint author), Freer Gallery Art, Ceram, Washington, DC 20560 USA. NR 7 TC 0 Z9 0 U1 1 U2 1 PU ARTS ASIA PUBLICATIONS LTD PI KOWLOON PA KOWLOON CENTER-SUITE 1309 29-39 ASHLEY RD, KOWLOON, HONG KONG SN 0004-4083 J9 ART ASIA JI Arts Asia PD JUL-AUG PY 2014 VL 44 IS 4 BP 73 EP 83 PG 11 WC Art; Asian Studies SC Art; Asian Studies GA AO8QA UT WOS:000341618100006 ER PT J AU Barnacka, A Moderski, R Behera, B Brun, P Wagner, S AF Barnacka, Anna Moderski, Rafal Behera, Bagmeet Brun, Pierre Wagner, Stefan TI PKS 1510-089: a rare example of a flat spectrum radio quasar with a very high-energy emission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: jets; galaxies: active; quasars: individual: PKS 1510-089 ID EXTRAGALACTIC BACKGROUND LIGHT; SPACE-TELESCOPE OBSERVATIONS; GAMMA-RAY ABSORPTION; LARGE-AREA TELESCOPE; RELATIVISTIC JET; MULTIWAVELENGTH OBSERVATIONS; RADIATION-FIELDS; 3C 279; BLAZARS; COMPTONIZATION AB Context. The blazar PKS 1510-089 is an example of flat spectrum radio quasars. High-energy emissions from this class of objects are believed to have been produced by IC radiation with seed photons originating from the broad line region. In such a paradigm, a lack of very high-energy emissions is expected because of the Klein-Nishina effect and strong absorption in the broad line region. Recent detection of at least three such blazars by Cherenkov telescopes has forced a revision of our understanding of these objects. Aims. We have aimed to model the observed spectral energy distribution of PKS 1510-089 from the high-energy flares in March 2009. during which very high-energy emission were also detected by H.E.S.S. Methods. We have applied the single zone internal shock scenario to reproduce the multiwavelength spectrum of PKS 1510-089. We have followed the evolution of the electrons as they propagate along the jet and emit synchrotron and IC radiation. We have considered two sources of external photons: the dusty torus and the broad line region. We have also examined the effects of the gamma-gamma absorption of the high-energy photons both in the AGN environment (the broad line region and the dusty torus), as well as while traveling over cosmological distances: the extragalactic background light. Results. We have successfully modeled the observed spectrum of PKS 1510-089. In our model, the highest energy emission is the result of the Comptonization of the infrared photons from the dusty torus, thus avoiding Klein-Nishina regime, while the bulk of the emissions in the GeV range may still be dominated by the Comptonization of radiation coming from the broad line region. C1 [Barnacka, Anna; Moderski, Rafal] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Barnacka, Anna] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brun, Pierre] Ctr Saclay, CEA Irfu, F-91191 Gif Sur Yvette, France. [Behera, Bagmeet] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Wagner, Stefan] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany. RP Barnacka, A (reprint author), Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. EM abarnacka@cfa.harvard.edu FU Polish Ministry of Science and Higher Education [Dec-2011/01/N/ST9/06007]; French national Program for High Energy Astrophysics PNHE; French ANR project CosmoTeV FX We would like to thank the referee the valuable comments. We would like to thank Jeff Grube for help with the Swift/XRT data analysis. This work was supported by the Polish Ministry of Science and Higher Education under Grants No. Dec-2011/01/N/ST9/06007. Part of this work was supported by the French national Program for High Energy Astrophysics PNHE, and the French ANR project CosmoTeV. NR 52 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2014 VL 567 AR A113 DI 10.1051/0004-6361/201322205 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VU UT WOS:000341185300014 ER PT J AU Miotello, A Testi, L Lodato, G Ricci, L Rosotti, G Brooks, K Maury, A Natta, A AF Miotello, A. Testi, L. Lodato, G. Ricci, L. Rosotti, G. Brooks, K. Maury, A. Natta, A. TI Grain growth in the envelopes and disks of Class I protostars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE circumstellar matter; opacity; radiative transfer; protoplanetary disks; stars: protostars; dust, extinction ID YOUNG STELLAR OBJECTS; T-TAURI STARS; MAGNETIC BRAKING CATASTROPHE; GRAVITATING ACCRETION DISCS; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; SIZE DISTRIBUTION; MOLECULAR CLOUDS; PROTOSTELLAR CORES; OHMIC DISSIPATION AB We present new 3 mm ATCA data of two Class I young stellar objects (YSOs) in the Ophiucus star forming region: Elias29 and WL12. For our analysis we compare them with archival 1.1 mm SMA data. In the (u, v) plane the two sources present a similar behavior: a nearly constant non-zero emission at long baselines, which suggests the presence of an unresolved component and an increase of the fluxes at short baselines, related to the presence of an extended envelope. Our data analysis leads to unusually low values of the spectral index alpha(1.1-3) mm, which may indicate that mm-sized dust grains have already formed both in the envelopes and in the disk-like structures at such early stages. To explore the possible scenarios for the interpretation of the sources we perform a radiative transfer modeling using a Monte Carlo code, in order to take into account possible deviations from the Rayleigh-Jeans and optically thin regimes. Comparison between the model outputs and the observations indicates that dust grains may form aggregates up to millimeter size already in the inner regions of the envelopes of Class I YSOs. Moreover, we conclude that the embedded disk-like structures in our two Class I YSOs are probably very compact, in particular in the case of WL12, with outer radii down to tens of AU. C1 [Miotello, A.; Testi, L.] European So Observ, D-85748 Garching, Germany. [Miotello, A.; Lodato, G.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Testi, L.; Natta, A.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Testi, L.; Rosotti, G.] Excellence Cluster Universe, D-85748 Garching, Germany. [Ricci, L.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Rosotti, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Brooks, K.] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Maury, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Natta, A.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. RP Miotello, A (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM miotello@mpe.mpg.de OI Brooks, Kate/0000-0001-9373-8992; Rosotti, Giovanni/0000-0003-4853-5736 FU ESO DGDF program; Italian Ministero dell'Istruzione, Universita e Ricerca through the grant Progetti Premiali iALMA FX The authors wish to thank ATNF&CSIRO staff for the support and the hospitality, F. Trotta and F. Testi for their help during the observing session. The authors also thank E. van Dishoeck and the referee, J. Jorgensen, for insightful comments that significantly improved our work. This work was partly supported by the ESO DGDF program and by the Italian Ministero dell'Istruzione, Universita e Ricerca through the grant Progetti Premiali 2012-iALMA. NR 74 TC 21 Z9 21 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2014 VL 567 AR A32 DI 10.1051/0004-6361/201322945 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VU UT WOS:000341185300034 ER PT J AU Bret, A Stockem, A Narayan, R Silva, LO AF Bret, A. Stockem, A. Narayan, R. Silva, L. O. TI Collisionless Weibel shocks: Full formation mechanism and timing SO PHYSICS OF PLASMAS LA English DT Article ID ELECTRON-POSITRON PLASMAS; PARTICLE-ACCELERATION; ASTROPHYSICAL SHOCKS; COSMIC-RAYS; INSTABILITY; WAVES; FILAMENTATION; GENERATION; DYNAMICS; FRONTS AB Collisionless shocks in plasmas play an important role in space physics (Earth's bow shock) and astrophysics (supernova remnants, relativistic jets, gamma-ray bursts, high energy cosmic rays). While the formation of a fluid shock through the steepening of a large amplitude sound wave has been understood for long, there is currently no detailed picture of the mechanism responsible for the formation of a collisionless shock. We unravel the physical mechanism at work and show that an electromagnetic Weibel shock always forms when two relativistic collisionless, initially unmagnetized, plasma shells encounter. The predicted shock formation time is in good agreement with 2D and 3D particle-in-cell simulations of counterstreaming pair plasmas. By predicting the shock formation time, experimental setups aiming at producing such shocks can be optimised to favourable conditions. (C) 2014 AIP Publishing LLC. C1 [Bret, A.] Univ Castilla La Mancha, ETSI Ind, E-13071 Ciudad Real, Spain. [Bret, A.] Inst Invest Energet & Aplicac Ind, Ciudad Real 13071, Spain. [Stockem, A.; Silva, L. O.] Univ Lisbon, Inst Super Tecn, GoLP Inst Plasmas & Fusao Nucl, P-1699 Lisbon, Portugal. [Stockem, A.] Ruhr Univ Bochum, Lehrstuhl Weltraum & Astrophys 4, Inst Theoret Phys, D-44780 Bochum, Germany. [Narayan, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bret, A (reprint author), Univ Castilla La Mancha, ETSI Ind, E-13071 Ciudad Real, Spain. RI Bret, Antoine/C-9112-2009 OI Bret, Antoine/0000-0003-2030-0046 FU European Research Council (ERC) [67841]; FCT (Portugal) [PTDC/FIS/111720/2009, SFRH/BD/38952/2007] FX This work was supported by the European Research Council (ERC-2010-AdG Grant 267841) and FCT (Portugal) Grant Nos. PTDC/FIS/111720/2009 and SFRH/BD/38952/2007. We acknowledge PRACE for providing access to resource SuperMUC based in Germany at the Leibniz research center. The authors gratefully 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). Thanks are due to Martin Lemoine, Laurent Gremillet, and Charles Ruyer for enriching discussions. NR 43 TC 22 Z9 23 U1 4 U2 10 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD JUL PY 2014 VL 21 IS 7 AR 072301 DI 10.1063/1.4886121 PG 5 WC Physics, Fluids & Plasmas SC Physics GA AO2LN UT WOS:000341154100029 ER PT J AU Reynolds, SM Uy, JAC Patricelli, GL Coleman, SW Braun, MJ Borgia, G AF Reynolds, Sheila M. Uy, J. Albert C. Patricelli, Gail L. Coleman, Seth W. Braun, Michael J. Borgia, Gerald TI Tests of the kin selection model of mate choice and inbreeding avoidance in satin bowerbirds SO BEHAVIORAL ECOLOGY LA English DT Article DE bowerbirds; inbreeding avoidance; kin selection; leks; mate choice; outbreeding; relatedness; sexual selection ID MAJOR HISTOCOMPATIBILITY COMPLEX; EXTRA-PAIR PATERNITY; LEK-BREEDING BIRD; GENETIC SIMILARITY; PTILONORHYNCHUS-VIOLACEUS; CROCIDURA-RUSSULA; BIASED DISPERSAL; SOCIAL MATES; COMPATIBILITY; PREFERENCE AB In typically outbreeding species, females can avoid a reduction in offspring fitness by choosing unrelated sires. However, the kin selection model of mate choice suggests that it may be adaptive to mate with relatives to gain inclusive fitness benefits, especially in lekking species. Several studies have shown that females tend to mate with relatives, but the detailed behavioral data necessary to determine whether this reflects an active preference is difficult to acquire. We test the hypotheses that females actively preferred or avoided relatives in mate choice in satin bowerbirds (Ptilonorhynchus violaceus), a lekking species in which comprehensive observations of natural mate choice were obtained using automated video cameras positioned at bowers. We identified specific males that were sampled by individual females and assessed whether relatedness influenced their acceptance or rejection as mates. We found no consistent effect of relatedness on mate choice across years or among multiple stages of mate choice. In 2 of 6 years, females copulated with relatives at or above the half-sibling level significantly more often than expected, but this was attributed to females searching for mates in areas populated by relatives, and not to an active preference for relatives. Furthermore, we found no evidence for inbreeding avoidance through mate choice discrimination or sex-biased dispersal. C1 [Reynolds, Sheila M.; Coleman, Seth W.; Braun, Michael J.; Borgia, Gerald] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA. [Reynolds, Sheila M.; Braun, Michael J.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Suitland, MD 20746 USA. [Uy, J. Albert C.; Patricelli, Gail L.; Braun, Michael J.; Borgia, Gerald] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Uy, J. Albert C.] Univ Miami, Dept Biol, Coral Gables, FL 33146 USA. [Patricelli, Gail L.] Univ Calif Davis, Dept Ecol & Evolut, Davis, CA 95616 USA. RP Reynolds, SM (reprint author), Univ Maryland, Behav Ecol Evolut & Systemat Program, Biol Psychol Bldg, College Pk, MD 20742 USA. EM sheila.reynolds@gmail.com OI Uy, J. Albert C./0000-0002-8437-5525 FU National Science Foundation Animal Behavior Program [0518844]; Smithsonian Institution; University of Maryland FX Funding was provided by the National Science Foundation Animal Behavior Program (0518844) to G. B., the Smithsonian Institution to M. J. Braun, and the University of Maryland, Anne G. Wylie Dissertation Fellowship to S. M. Reynolds. NR 64 TC 3 Z9 3 U1 10 U2 72 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 EI 1465-7279 J9 BEHAV ECOL JI Behav. Ecol. PD JUL-AUG PY 2014 VL 25 IS 4 BP 1005 EP 1014 DI 10.1093/beheco/aru065 PG 10 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA AM7LH UT WOS:000340048200044 ER PT J AU Herman, RDK AF Herman, R. D. K. TI A Shark Going Inland is My Chief: The Island Civilization of Ancient Hawai'i SO JOURNAL OF HISTORICAL GEOGRAPHY LA English DT Book Review C1 [Herman, R. D. K.] Smithsonian Natl Museum Amer Indian, Washington, DC 20560 USA. RP Herman, RDK (reprint author), Smithsonian Natl Museum Amer Indian, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-7488 J9 J HIST GEOGR JI J. Hist. Geogr. PD JUL PY 2014 VL 45 BP 138 EP 139 DI 10.1016/j.jhg.2014.05.020 PG 2 WC Geography; History Of Social Sciences SC Geography; Social Sciences - Other Topics GA AO0FW UT WOS:000340985500033 ER PT J AU Moser, WE Bowerman, J Hovingh, P Pearl, CA Oceguera-Figueroa, A AF Moser, William E. Bowerman, Jay Hovingh, Peter Pearl, Christopher A. Oceguera-Figueroa, Alejandro TI New Host and Distribution Records of the Leech Placobdella sophieae Oceguera-Figueroa et al., 2010 (Hirudinida: Glossiphoniidae) SO COMPARATIVE PARASITOLOGY LA English DT Article DE Rhynchobdellida; Placobdella picta; Placobdella burresonae; Desserobdella; Batracobdella; Taricha granulosa; Rana pretiosa; Rana aurora; Bufo boreas; Anaxyrus boreas ID REDESCRIPTION; VERRILL AB Placobdella sophieae Oceguera-Figueroa et al., 2010 (Hirudinida: Glossiphoniidae) is reported from Oregon, California, and British Columbia for the first time. New hosts reported for P. sophieae include Taricha granulosa (rough-skinned newt), Rana pretiosa (Oregon spotted frog), and Anaxyrus boreas (western toad). Placobdella sophieae exhibits relatively low host specificity and all amphibians occurring in the Pacific Northwest are potential hosts. C1 [Moser, William E.] Smithsonian Inst, Museum Support Ctr, Dept Invertebrate Zool, Natl Museum Nat Hist, Suitland, MD 20746 USA. [Bowerman, Jay] Sunriver Nat Ctr, Sunriver, OR 97707 USA. [Pearl, Christopher A.] US Geol Survey, Forest & Rangeland Ecosyst Sci Ctr, Corvallis, OR 97331 USA. [Oceguera-Figueroa, Alejandro] Univ Nacl Autonoma Mexico, Inst Biol, Lab Hehnintol, Mexico City 04510, DF, Mexico. RP Moser, WE (reprint author), Smithsonian Inst, Museum Support Ctr, Dept Invertebrate Zool, Natl Museum Nat Hist, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM moserw@si.edu; frogs1@sunrivematurecenter.org; phovingh@xmission.com; christopher_pearl@usgs.gov; aoceguera@ib.unam.mx NR 17 TC 1 Z9 1 U1 1 U2 5 PU HELMINTHOLOGICAL SOC WASHINGTON PI LAWRENCE PA C/O ALLEN PRESS INC, 1041 NEW HAMPSHIRE ST, ACCT# 141866, LAWRENCE, KS 66044 USA SN 1525-2647 EI 1938-2952 J9 COMP PARASITOL JI Comp. Parasitol. PD JUL PY 2014 VL 81 IS 2 BP 199 EP 202 PG 4 WC Parasitology; Zoology SC Parasitology; Zoology GA AM9WC UT WOS:000340230700010 ER PT J AU Rose, KC Hamilton, DP Williamson, CE McBride, CG Fischer, JM Olson, MH Saros, JE Allan, MG Cabrol, N AF Rose, Kevin C. Hamilton, David P. Williamson, Craig E. McBride, Chris G. Fischer, Janet M. Olson, Mark H. Saros, Jasmine E. Allan, Mathew G. Cabrol, Nathalie TI Light attenuation characteristics of glacially-fed lakes SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID DISSOLVED ORGANIC-CARBON; ULTRAVIOLET-RADIATION; ALPINE LAKES; VERTICAL-DISTRIBUTION; ABSORPTION-SPECTRUM; MOUNTAIN LAKES; FRESH-WATER; UV; ZOOPLANKTON; MELTWATER AB Transparency is a fundamental characteristic of aquatic ecosystems and is highly responsive to changes in climate and land use. The transparency of glacially-fed lakes may be a particularly sensitive sentinel characteristic of these changes. However, little is known about the relative contributions of glacial flour versus other factors affecting light attenuation in these lakes. We sampled 18 glacially-fed lakes in Chile, New Zealand, and the U. S. and Canadian Rocky Mountains to characterize how dissolved absorption, algal biomass (approximated by chlorophyll a), water, and glacial flour contributed to attenuation of ultraviolet radiation (UVR) and photosynthetically active radiation (PAR, 400-700nm). Variation in attenuation across lakes was related to turbidity, which we used as a proxy for the concentration of glacial flour. Turbidity-specific diffuse attenuation coefficients increased with decreasing wavelength and distance from glaciers. Regional differences in turbidity-specific diffuse attenuation coefficients were observed in short UVR wavelengths (305 and 320nm) but not at longer UVR wavelengths (380nm) or PAR. Dissolved absorption coefficients, which are closely correlated with diffuse attenuation coefficients in most non-glacially-fed lakes, represented only about one quarter of diffuse attenuation coefficients in study lakes here, whereas glacial flour contributed about two thirds across UVR and PAR. Understanding the optical characteristics of substances that regulate light attenuation in glacially-fed lakes will help elucidate the signals that these systems provide of broader environmental changes and forecast the effects of climate change on these aquatic ecosystems. C1 [Rose, Kevin C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Hamilton, David P.; McBride, Chris G.; Allan, Mathew G.] Univ Waikato, Environm Res Inst, Hamilton, New Zealand. [Williamson, Craig E.] Miami Univ, Dept Biol, Oxford, OH 45056 USA. [Fischer, Janet M.; Olson, Mark H.] Franklin & Marshall Coll, Dept Biol, Lancaster, PA 17604 USA. [Saros, Jasmine E.] Univ Maine, Climate Change Inst, Orono, ME USA. [Saros, Jasmine E.] Univ Maine, Sch Biol & Ecol, Orono, ME USA. [Cabrol, Nathalie] NASA, Ames Res Ctr, SETI Inst Carl Sagan Ctr, Mountain View, CA USA. RP Rose, KC (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM kev.c.rose@gmail.com FU National Science Foundation (NSF) Division of Graduate Education (DGE) Integrative Graduate Education Research and Traineeship (IGERT) grant [0903560]; Smithsonian Institution; Franklin and Marshall College; Andrew W. Mellon Foundation through Central Pennsylvania Consortium; Ministry of Business, Employment and Innovation [UOWX0505]; NASA Planetary Lake Lander project [10-ASTEP10-0011] FX K.C.R. and C. E. W. received support from the National Science Foundation (NSF) Division of Graduate Education (DGE) Integrative Graduate Education Research and Traineeship (IGERT) grant 0903560. K. C. R. also received support from the Smithsonian Institution as a Smithsonian Postdoctoral Fellow. J.M.F. and M.H.O. received funding from Franklin and Marshall College and the Andrew W. Mellon Foundation through its grant in support of faculty development within the Central Pennsylvania Consortium. We acknowledge support for the New Zealand component of the study through the Ministry of Business, Employment and Innovation (contract UOWX0505). We thank the Parks Canada Agency for their permission to conduct our research in the national mountain parks of Canada (YNP-2008-1585). Field work on South American lakes (Negra and Lo Encanado) was supported by the NASA Planetary Lake Lander project (grant 10-ASTEP10-0011) and the SETI Institute. We thank Megan Rose, Jeremy Mack, Lucia Acosta, and Erin Overholt for assistance with field work and lab analyses. There are no supporting data for this manuscript. NR 47 TC 4 Z9 4 U1 4 U2 43 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 EI 2169-8961 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD JUL PY 2014 VL 119 IS 7 BP 1446 EP 1457 DI 10.1002/2014JG002674 PG 12 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA AN4FM UT WOS:000340543000013 ER PT J AU Rojas-Sandoval, J Melendez-Ackerman, EJ Fumero-Caban, J Garcia-Bermudez, MA Sustache, J Aragon, S Morales, M Fernandez, DS AF Rojas-Sandoval, Julissa Melendez-Ackerman, Elvia J. Fumero-Caban, Jose Garcia-Bermudez, Miguel A. Sustache, Jose Aragon, Susan Morales, Mariely Fernandez, Denny S. TI Effects of hurricane disturbance and feral goat herbivory on the structure of a Caribbean dry forest SO JOURNAL OF VEGETATION SCIENCE LA English DT Article DE Coppicing; Forest structure; Goat herbivory; Hurricane Georges; Successional status; Tree mortality ID PUERTO-RICO; TROPICAL FOREST; WEST-INDIES; ECOSYSTEMS; VEGETATION; UNGULATE; WINDS; MORTALITY; GILBERT; DAMAGE AB Question: Hurricanes are a major factor influencing forest structure and have been linked to higher incidences of multiple-stemmed trees in Caribbean dry forests relative to the continent. In Sept 1998, category 3 Hurricane Georges passed over Mona Island. This island, unlike others in the Caribbean, has had feral goats for five centuries. In this study we addressed the following questions: (i) what are the short-term (4 mo) and long-term (10 yr) responses of Mona Island's dry forests to hurricane disturbance in terms of forest structure and tree mortality; and (ii) is there any effect of goat exclusion on the recovery process and forest structure after the hurricane? Location: Dry forest of Mona Island, Puerto Rico. Methods: Permanent fenced and unfenced plots established in 1997 and monitored annually until 2008 were used to evaluate the interplay between goat herbivory and hurricane effects on structural dynamics of the tree community. Within these plots, vegetation data collected include species identity, DBH, successional status and hurricane-related tree mortality. Results: We found that vegetation responses to hurricane disturbances may have been influenced by the presence of feral goats through at least two mechanisms. First, goats may have led to changes in forest structure and composition that feed back into the recovery dynamics that follow hurricane events. Second, goat herbivory limits the production of multiple stems, a trait that could be an adaptive response in hurricane-prone areas. Feral goats may lead to alternate successional pathways by keeping this dry forest at early-successional stages much longer than expected, and shifting vegetation communities to an alternate state where smaller, shrubbier and perhaps less palatable species dominate. Conclusions: Differences in structure between Mona Island's dry forest and other tropical dry forests are related to changes in species composition that may have been triggered by introduced goats. Our results highlight the potential complexities that may arise when setting management goals within the context of novel ecosystems. Ultimately, implementation of management goals requires knowing what changes are linked to the ecological integrity of the ecosystem and what cultural values are placed on the current state of the tree community vs its historical condition. C1 [Rojas-Sandoval, Julissa] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Melendez-Ackerman, Elvia J.] Univ Puerto Rico, Dept Environm Sci, Coll Nat Sci, San Juan, PR 00931 USA. [Fumero-Caban, Jose] Univ Puerto Rico, Dept Biol, San Juan, PR 00931 USA. [Garcia-Bermudez, Miguel A.; Sustache, Jose] Commonwealth Puerto Rico, Dept Nat & Environm Resources, San Juan, PR 00936 USA. [Morales, Mariely; Fernandez, Denny S.] Univ Puerto Rico Humacao, Dept Biol, Humacao, PR 00792 USA. [Morales, Mariely; Fernandez, Denny S.] Univ Puerto Rico, Ctr Appl Trop Ecol & Conservat, San Juan, PR 00936 USA. [Aragon, Susan] Clark Univ, Grad Sch Geog, Worcester, MA 01610 USA. RP Rojas-Sandoval, J (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166,POB 37012, Washington, DC 20013 USA. EM julirs07@gmail.com; elmelend@gmail.com; josejfumero@yahoo.com; miguelag@onelinkpr.net; jsustache@drna.gobierno.pr; saragongeo@yahoo.com; mariely.morales@gmail.com; dsfernandez@gmail.com FU NSF-CREST through the Center for Applied Tropical Ecology and Conservation at the University of Puerto Rico [HRD-0206200, HRD 0734826] FX The authors thank Ariel E. Lugo, James D. Ackerman and two anonymous reviewers for helpful comments that significantly improved this manuscript. This study was funded by NSF-CREST (HRD-0206200 and HRD 0734826) through the Center for Applied Tropical Ecology and Conservation at the University of Puerto Rico. NR 48 TC 2 Z9 2 U1 2 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1100-9233 EI 1654-1103 J9 J VEG SCI JI J. Veg. Sci. PD JUL PY 2014 VL 25 IS 4 BP 1069 EP 1077 DI 10.1111/jvs.12160 PG 9 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA AN4QF UT WOS:000340572000017 ER PT J AU Inoue, M Algaba-Marcos, JC Asada, K Blundell, R Brisken, W Burgos, R Chang, CC Chen, MT Doeleman, SS Fish, V Grimes, P Han, J Hirashita, H Ho, PTP Hsieh, SN Huang, T Jiang, H Keto, E Koch, PM Kubo, DY Kuo, CY Liu, B Martin-Cocher, P Matsushita, S Meyer-Zhao, Z Nakamura, M Napier, P Nishioka, H Nystrom, G Paine, S Patel, N Pradel, N Pu, HY Raffin, PA Shen, HY Snow, W Srinivasan, R Wei, TS AF Inoue, M. Algaba-Marcos, J. C. Asada, K. Blundell, R. Brisken, W. Burgos, R. Chang, C-C. Chen, M-T. Doeleman, S. S. Fish, V. Grimes, P. Han, J. Hirashita, H. Ho, P. T. P. Hsieh, S-N. Huang, T. Jiang, H. Keto, E. Koch, P. M. Kubo, D. Y. Kuo, C-Y. Liu, B. Martin-Cocher, P. Matsushita, S. Meyer-Zhao, Z. Nakamura, M. Napier, P. Nishioka, H. Nystrom, G. Paine, S. Patel, N. Pradel, N. Pu, H-Y. Raffin, P. A. Shen, H-Y. Snow, W. Srinivasan, R. Wei, T-S. TI Greenland telescope project: Direct confirmation of black hole with sub-millimeter VLBI SO RADIO SCIENCE LA English DT Article ID GALACTIC-CENTER; M87; JET AB A 12 m diameter radio telescope will be deployed to the Summit Station in Greenland to provide direct confirmation of a Super Massive Black Hole (SMBH) by observing its shadow image in the active galaxy M87. The telescope (Greenland Telescope: GLT) is to become one of the Very Long Baseline Interferometry (VLBI) stations at sub-millimeter (submm) regime, providing the longest baseline >9000 km to achieve an exceptional angular resolution of 20 mu as at 350 GHz, which will enable us to resolve the shadow size of similar to 40 mu as. The triangle with the longest baselines formed by the GLT, the Atacama Large Millimeter/submillimeter Array (ALMA) in Chile, and the Submillimeter Array (SMA) in Hawaii will play a key role for the M87 observations. We have been working on the image simulations based on realistic conditions for a better understanding of the possible observed images. In parallel, retrofitting of the telescope and the site developments are in progress. Based on 3 years of opacity monitoring at 225 GHz, our measurements indicate that the site is excellent for submm observations, comparable to the ALMA site. The GLT is also expected to make single-dish observations up to 1.5 THz. C1 [Inoue, M.; Algaba-Marcos, J. C.; Asada, K.; Chang, C-C.; Chen, M-T.; Han, J.; Hirashita, H.; Ho, P. T. P.; Hsieh, S-N.; Huang, T.; Jiang, H.; Koch, P. M.; Kubo, D. Y.; Kuo, C-Y.; Liu, B.; Martin-Cocher, P.; Matsushita, S.; Meyer-Zhao, Z.; Nakamura, M.; Nishioka, H.; Nystrom, G.; Pradel, N.; Pu, H-Y.; Raffin, P. A.; Shen, H-Y.; Snow, W.; Srinivasan, R.; Wei, T-S.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Blundell, R.; Burgos, R.; Grimes, P.; Keto, E.; Napier, P.; Paine, S.; Patel, N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brisken, W.] Natl Radio Astron Observ, Array Operat Ctr, Socorro, NM 87801 USA. [Doeleman, S. S.; Fish, V.] MIT, Haystack Observ, Westford, MA 01886 USA. RP Inoue, M (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. EM inoue@asiaa.sinica.edu.tw OI Paine, Scott/0000-0003-4622-5857 NR 20 TC 11 Z9 11 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 EI 1944-799X J9 RADIO SCI JI Radio Sci. PD JUL PY 2014 VL 49 IS 7 BP 564 EP 571 DI 10.1002/2014RS005450 PG 8 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA AN2OV UT WOS:000340426100009 ER PT J AU Moini, M O'Halloran, A Peters, AM France, CAM Vicenzi, EP DeWitt, TG Langan, E Walsh, T Speakman, RJ AF Moini, Mehdi O'Halloran, Aoife Peters, Alan M. France, Christine A. M. Vicenzi, Edward P. DeWitt, Tamsen G. Langan, Esther Walsh, Tim Speakman, Robert J. TI Understanding Irregular Shell Formation of Nautilus in Aquaria: Chemical Composition and Structural Analysis SO ZOO BIOLOGY LA English DT Article DE cephalopods; shell formation; black line; isotopic abundances; Mollusca ID ISOTOPE FRACTIONATION; CHAMBER FORMATION; STABLE ISOTOPES; CARBON; POMPILIUS; OXYGEN; MACROMPHALUS; TEMPERATURE; ANIMALS; GROWTH AB Irregular shell formation and black lines on the outside of live chambered nautilus shells have been observed in all adult specimens at aquariums and zoos soon after the organisms enter aquaria. Black lines have also been observed in wild animals at sites of broken shell, but continued growth from that point returns to a normal, smooth structure. In contrast, rough irregular deposition of shell continues throughout residence in aquaria. The composition and reasons for deposition of the black material and mitigation of this irregular shell formation is the subject of the current study. A variety of analytical techniques were used, including stable isotope mass spectrometry (SI-MS), inductively coupled plasma mass spectrometry (ICP-MS), micro x-ray fluorescence (mXRF), X-ray diffraction (XRD), and scanning electron microscopy (SEM) based X-ray microanalysis. Results indicate that the black material contains excess amounts of copper, zinc, and bromine which are unrelated to the Nautilus diet. The combination of these elements and proteins plays an important role in shell formation, growth, and strengthening. Further study will be needed to compare the proteomics of the shell under aquaria versus natural wild environments. The question remains as to whether the occurrence of the black lines indicates normal healing followed by growth irregularities that are caused by stress from chemical or environmental conditions. In this paper we begin to address this question by examining elemental and isotopic differences of Nautilus diet and salt water. The atomic composition and light stable isotopic ratios of the Nautilus shell formed in aquaria verses wild conditions are presented. (C) 2014 Wiley Periodicals, Inc. C1 [Moini, Mehdi] George Washington Univ, Dept Forens Sci, Washington, DC 20052 USA. [O'Halloran, Aoife; France, Christine A. M.; Vicenzi, Edward P.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD USA. [Peters, Alan M.; DeWitt, Tamsen G.; Langan, Esther; Walsh, Tim] Smithsonian Inst, Natl Zoo Anim Care Sci, Washington, DC 20560 USA. [Speakman, Robert J.] Univ Georgia, Ctr Appl Isotope Studies, Athens, GA 30602 USA. RP Peters, AM (reprint author), Natl Zool Pk, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM petersam@si.edu OI Speakman, Robert/0000-0003-2063-154X NR 40 TC 1 Z9 1 U1 3 U2 29 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0733-3188 EI 1098-2361 J9 ZOO BIOL JI Zoo Biol. PD JUL-AUG PY 2014 VL 33 IS 4 BP 285 EP 294 DI 10.1002/zoo.21132 PG 10 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA AN3VX UT WOS:000340517900005 PM 24797217 ER PT J AU Petzinger, C Oftedal, OT Jacobsen, K Murtough, KL Irlbeck, NA Power, ML AF Petzinger, Christina Oftedal, Olav T. Jacobsen, Krista Murtough, Katie L. Irlbeck, Nancy A. Power, Michael L. TI Proximate Composition of Milk of the Bongo (Tragelaphus eurycerus) in Comparison to Other African Bovids and to Hand-Rearing Formulas SO ZOO BIOLOGY LA English DT Article DE lactation; Bovidae; calf; hand-rearing; protein; energy ID DZANGA NATIONAL-PARK; RAIN-FOREST; LACTATION; ANTELOPE; MAMMALS; YIELD; STAGE AB African bovids represent a highly diverse group with divergent neonatal care strategies. The extent to which their milks reflect this diversity is poorly understood. We analyzed milk of the bongo (Tragelaphus eurycerus) to compare its composition to milks of other African bovids and to evaluate bongo milk replacement formulas. Milk samples from three individuals (0 through 300 days postpartum, n = 28) were assayed for dry matter (total solids), crude fat, crude protein, total sugar, ash, calcium, and phosphorus; gross energy was assayed on a subset of samples and compared to calculated values. Nutrient composition changed very little over the lactation period except for day 0 (colostrum) and the last sample (day 300). Bongo milk (days 6-286) contained (mean +/- SEM): 28.1 +/- 0.7% dry matter (71.9 +/- 0.7% water), 12.3 +/- 0.6% fat, 10.6 +/- 0.3% crude protein, 3.6 +/- 0.1% sugar, 1.05 +/- 0.03% ash, 0.26 +/- 0.01% calcium, 0.16 +/- 0.01% phosphorus, and a GE of 1.88 +/- 0.06 kcal/g. The protein content of bongo milk accounts for 33% of energy. High protein energy appears to be typical of Tragelaphines and of African bovids that utilize a "hider" system of postnatal care. The stability of milk composition until day 300 suggests complete weaning may not occur until 9 months rather than at 6 months of age, as commonly assumed. None of the milk replacement formulas previously used for bongos was well matched to bongo milk composition; therefore, a new milk replacement formula is proposed. (C) 2014 Wiley Periodicals, Inc. C1 [Petzinger, Christina; Murtough, Katie L.; Power, Michael L.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Nutr Lab, Washington, DC 20013 USA. [Petzinger, Christina; Murtough, Katie L.; Power, Michael L.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Washington, DC 20013 USA. [Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Jacobsen, Krista] Univ Calif Davis, Davis, CA 95616 USA. [Irlbeck, Nancy A.] Colorado State Univ, Ft Collins, CO 80523 USA. RP Power, ML (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, POB 37012,MRC 5503, Washington, DC 20013 USA. EM powerm@si.edu OI Power, Michael/0000-0002-6120-3528 NR 51 TC 3 Z9 3 U1 2 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0733-3188 EI 1098-2361 J9 ZOO BIOL JI Zoo Biol. PD JUL-AUG PY 2014 VL 33 IS 4 BP 305 EP 313 DI 10.1002/zoo.21139 PG 9 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA AN3VX UT WOS:000340517900007 PM 24978056 ER PT J AU Swanson, DA Rose, TR Mucek, AE Garcia, MO Fiske, RS Mastin, LG AF Swanson, Donald A. Rose, Timothy R. Mucek, Adonara E. Garcia, Michael O. Fiske, Richard S. Mastin, Larry G. TI Cycles of explosive and effusive eruptions at Kilauea Volcano, Hawai'i SO GEOLOGY LA English DT Article ID MAGMA RESERVOIR; KEANAKAKOI ASH; PUNA RIDGE; MAUNA-LOA; SUMMIT; AD; GROUNDWATER; CALIBRATION; CALDERA; VIOLENT AB The subaerial eruptive activity at Kilauea Volcano (Hawaii) for the past 2500 yr can be divided into 3 dominantly effusive and 2 dominantly explosive periods, each lasting several centuries. The prevailing style of eruption for 60% of this time was explosive, manifested by repeated phreatic and phreatomagmatic activity in a deep summit caldera. During dominantly explosive periods, the magma supply rate to the shallow storage volume beneath the summit dropped to only a few percent of that during mainly effusive periods. The frequency and duration of explosive activity are contrary to the popular impression that Kilauea is almost unceasingly effusive. Explosive activity apparently correlates with the presence of a caldera intersecting the water table. The decrease in magma supply rate may result in caldera collapse, because erupted or intruded magma is not replaced. Glasses with unusually high MgO, TiO2, and K2O compositions occur only in explosive tephra (and one related lava flow) and are consistent with disruption of the shallow reservoir complex during caldera formation. Kilauea is a complex, modulated system in which melting rate, supply rate, conduit stability (in both mantle and crust), reservoir geometry, water table, and many other factors interact with one another. The hazards associated with explosive activity at Kilauea's summit would have major impact on local society if a future dominantly explosive period were to last several centuries. The association of lowered magma supply, caldera formation, and explosive activity might characterize other basaltic volcanoes, but has not been recognized. C1 [Swanson, Donald A.] US Geol Survey, Hawaiian Volcano Observ, Hawaii Natl Pk, HI 96718 USA. [Rose, Timothy R.; Fiske, Richard S.] Smithsonian Inst, Museum Nat Hist, Dept Mineral Sci, Washington, DC 20013 USA. [Mucek, Adonara E.; Garcia, Michael O.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Dept Geol & Geophys, Honolulu, HI 96822 USA. [Mastin, Larry G.] US Geol Survey, Cascades Volcano Observ, Vancouver, WA 98683 USA. RP Swanson, DA (reprint author), US Geol Survey, Hawaiian Volcano Observ, Hawaii Natl Pk, Hawaii Natl Pk, HI 96718 USA. FU National Science Foundation [EAR-1118741] FX We thank Dave Clague, Dan Dzurisin, Shaul Hurwitz, and Pete Lipman for insightful manuscript reviews. Tom Wright's comments on a preliminary version were provocative. Dave Sherrod supplied three unpublished 14C ages. Discussions with Frank Trusdell were valuable. Robin Holcomb proposed eruptive cycles that differ from ours but stimulated our thinking. Garcia and Mucek were supported by National Science Foundation grant EAR-1118741. This paper is School of Ocean and Earth Science and Technology (SOEST) contribution 9115. NR 35 TC 9 Z9 9 U1 0 U2 17 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 JUL PY 2014 VL 42 IS 7 BP 631 EP 634 DI 10.1130/G35701.1 PG 4 WC Geology SC Geology GA AM6GJ UT WOS:000339961400022 ER PT J AU Tavares, M Lemaitre, R AF Tavares, Marcos Lemaitre, Rafael TI NEW MORPHOLOGICAL AND DISTRIBUTIONAL INFORMATION ON HOMOLODROMIIDAE AND HOMOLIDAE (DECAPODA: BRACHYURA) FROM THE AMERICAS, WITH DESCRIPTION OF A NEW SPECIES AND COMMENTS ON WESTERN PACIFIC SPECIES SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article DE Decapoda; Dicranodromia galapagensis n. sp.; eastern Pacific; Homolidae; Homolodromiidae; homoloidian and eubrachyuran locking-system; Lamoha williamsi; western Atlantic; western Pacific ID FAMILY HOMOLODROMIIDAE; CRUSTACEA DECAPODA; CRABS DECAPODA; ATLANTIC; EVOLUTION; EDWARDS,A.MILNE; REDESCRIPTION; PHILIPPINES; SPECIMENS; ZONATION AB Seventeen crab species of Homolodromiidae and Homolidae, in seven genera, are recognized in the Atlantic and Pacific coasts of the Americas. The genus Dicranodromia A. Milne-Edwards, 1880, is recorded for the first time from the eastern Pacific with a new species described from the Galapagos Islands. Nine species, five Homolodromiidae and four Homolidae, are taxonomically evaluated and circumscribed based on morphological information, their geographic and bathymetric distribution clarified and updated, and the similarities and differences of each with other members of the families discussed. Photographs, SEM photomicrographs and line drawings for selected species, including notes on habitat, nomenclature, and distinguishing features, are provided. Biramous uropods and complete pleopod formula in males are discovered to occur in juveniles of Homo la minima Guinot and Richer de Forges, 1995, providing evidence that homoloidian and eubrachyuran pleonal locking-system (homoloidian and the eubrachyuran sockets) are not homologous. A checklist of all homolodromiid and homolid species known from both ocean sides of the Americas, with their bathymetric ranges, is presented. The diagnostic characters of one western Pacific species, Lamoha williamsi (Takeda, 1980), are reevaluated. C1 [Tavares, Marcos] Univ Sao Paulo, Museu Zool, BR-04263000 Sao Paulo, Brazil. [Lemaitre, Rafael] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. RP Lemaitre, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM lemaitrr@si.edu RI Museu de Zoologia da USP, MZ-USP/Q-2192-2016 FU CNPq [301806/2010-1]; Petrobras [4600224970] FX We are sincerely grateful to Adam Baldinger (MCZ), Carole Baldwin (USNM) and Fabrizio Scarabino (Direccion Nacional de Recursos Acuaticos, DINARA) for making the type material of Homolodromia paradoxa and the material of Dicranodromia from the Galapagos Islands and Homola minima from Uruguay, respectively, available for study. Many thanks to Rose Gulledge, who prepared all the plates and SEM photomicrographs, and to William Santana who prepared the digitized version of Fig. 8B and 8C. Thanks also to Karen Reed (USNM) and Joana d'Arc (MZUSP) for their kind assistance throughout the execution of this work. MT acknowledges grants CNPq (301806/2010-1) and Petrobras (4600224970) for supporting studies on the systematics of decapod crustaceans. NR 67 TC 1 Z9 1 U1 1 U2 3 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 JUL PY 2014 VL 34 IS 4 BP 504 EP 524 DI 10.1163/1937240X-00002243 PG 21 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AM2RF UT WOS:000339697800011 ER PT J AU Winter, K Holtum, JAM AF Winter, Klaus Holtum, Joseph A. M. TI Facultative crassulacean acid metabolism (CAM) plants: powerful tools for unravelling the functional elements of CAM photosynthesis SO JOURNAL OF EXPERIMENTAL BOTANY LA English DT Review DE C4/CAM; Calandrinia; Clusia; constitutive CAM; crassulacean acid metabolism; inducible CAM; Isoetes; Mesembryanthemum; Portulaca; Talinum ID MESEMBRYANTHEMUM-CRYSTALLINUM L; COMMON ICE PLANT; PORTULACA-OLERACEA L; C-4 SUCCULENT PLANT; CLUSIA-MINOR L; CARBON-ISOTOPE DISCRIMINATION; SUBMERGED AQUATIC PLANTS; UNIFLORA L ASCHERS; SEDUM-ACRE-L; PHOSPHOENOLPYRUVATE CARBOXYLASE AB Facultative crassulacean acid metabolism (CAM) describes the optional use of CAM photosynthesis, typically under conditions of drought stress, in plants that otherwise employ C-3 or C-4 photosynthesis. In its cleanest form, the upregulation of CAM is fully reversible upon removal of stress. Reversibility distinguishes facultative CAM from ontogenetically programmed unidirectional C-3-to-CAM shifts inherent in constitutive CAM plants. Using mainly measurements of 24 h CO2 exchange, defining features of facultative CAM are highlighted in five terrestrial species, Clusia pratensis, Calandrinia polyandra, Mesembryanthemum crystallinum, Portulaca oleracea and Talinum triangulare. For these, we provide detailed chronologies of the shifts between photosynthetic modes and comment on their usefulness as experimental systems. Photosynthetic flexibility is also reviewed in an aquatic CAM plant, Isoetes howellii. Through comparisons of C-3 and CAM states in facultative CAM species, many fundamental biochemical principles of the CAM pathway have been uncovered. Facultative CAM species will be of even greater relevance now that new sequencing technologies facilitate the mapping of genomes and tracking of the expression patterns of multiple genes. These technologies and facultative CAM systems, when joined, are expected to contribute in a major way towards our goal of understanding the essence of CAM. C1 [Winter, Klaus; Holtum, Joseph A. M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Holtum, Joseph A. M.] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld, Australia. RP Winter, K (reprint author), Smithsonian Trop Res Inst, POB 08403-03092, Balboa, Ancon, Panama. EM winterk@si.edu RI Research ID, CTBCC /O-3564-2014 FU Smithsonian Tropical Research Institute; School of Marine and Tropical Biology, James Cook University FX This research was funded by the Smithsonian Tropical Research Institute. JAMH was supported by the School of Marine and Tropical Biology, James Cook University. We gratefully acknowledge the assistance of A. Virgo in preparing the figures. NR 163 TC 30 Z9 30 U1 15 U2 119 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-0957 EI 1460-2431 J9 J EXP BOT JI J. Exp. Bot. PD JUL PY 2014 VL 65 IS 13 SI SI BP 3425 EP 3441 DI 10.1093/jxb/eru063 PG 17 WC Plant Sciences SC Plant Sciences GA AM6DU UT WOS:000339953400010 PM 24642847 ER PT J AU Silvera, K Winter, K Rodriguez, BL Albion, RL Cushman, JC AF Silvera, Katia Winter, Klaus Rodriguez, B. Leticia Albion, Rebecca L. Cushman, John C. TI Multiple isoforms of phosphoenolpyruvate carboxylase in the Orchidaceae (subtribe Oncidiinae): implications for the evolution of crassulacean acid metabolism SO JOURNAL OF EXPERIMENTAL BOTANY LA English DT Article DE Crassulacean acid metabolism; gene duplication; Orchidaceae; Oncidiinae; phosphoenolpyruvate carboxylase; photosynthesis ID LATERAL GENE-TRANSFER; C-4 PHOTOSYNTHESIS; MESEMBRYANTHEMUM-CRYSTALLINUM; PHENOTYPIC PLASTICITY; MAXIMUM-LIKELIHOOD; MOLECULAR-GENETICS; VASCULAR EPIPHYTES; CAM PLANTS; ADAPTATION; EXPRESSION AB Phosphoenolpyruvate carboxylase (PEPC) catalyses the initial fixation of atmospheric CO2 into oxaloacetate and subsequently malate. Nocturnal accumulation of malic acid within the vacuole of photosynthetic cells is a typical feature of plants that perform crassulacean acid metabolism (CAM). PEPC is a ubiquitous plant enzyme encoded by a small gene family, and each member encodes an isoform with specialized function. CAM-specific PEPC isoforms probably evolved from ancestral non-photosynthetic isoforms by gene duplication events and subsequent acquisition of transcriptional control elements that mediate increased leaf-specific or photosynthetic-tissue-specific mRNA expression. To understand the patterns of functional diversification related to the expression of CAM, ppc gene families and photosynthetic patterns were characterized in 11 closely related orchid species from the subtribe Oncidiinae with a range of photosynthetic pathways from C-3 photosynthesis (Oncidium cheirophorum, Oncidium maduroi, Rossioglossum krameri, and Oncidium sotoanum) to weak CAM (Oncidium panamense, Oncidium sphacelatum, Gomesa flexuosa and Rossioglossum insleayi) and strong CAM (Rossioglossum ampliatum, Trichocentrum nanum, and Trichocentrum carthagenense). Phylogenetic analysis revealed the existence of two main ppc lineages in flowering plants, two main ppc lineages within the eudicots, and three ppc lineages within the Orchidaceae. Our results indicate that ppc gene family expansion within the Orchidaceae is likely to be the result of gene duplication events followed by adaptive sequence divergence. CAM-associated PEPC isoforms in the Orchidaceae probably evolved from several independent origins. C1 [Silvera, Katia; Winter, Klaus] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Silvera, Katia; Rodriguez, B. Leticia; Albion, Rebecca L.; Cushman, John C.] Univ Nevada, Dept Biochem & Mol Biol, Reno, NV 89557 USA. RP Silvera, K (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Ancon, Panama. EM katias@ucr.edu FU Smithsonian Tropical Research Institute; US Environmental Protection Agency [MA 91685201]; National Science Foundation NSF [IOB-0543659]; National Institute of Health (NIH) from the INBRE Program of the National Center for Research Resources through Nevada Genomics, Proteomics, and Bioinformatics Centers [P20 RR-016464] FX The authors thank Mark Whitten, Norris H. Williams, and Kurt M. Neubig for providing the Oncidiinae matrix to construct the phylogeny of species used in this study; Pascal-Antoine Christin for invaluable help with Bayesian analyses and for providing additional ppc plant sequences; Mary Jane West-Eberhard for comments and discussions to improve a previous version of the manuscript; Gaspar Silvera for supplying the orchid plant species; Cristina Milsner for assistance with PEPC cloning and sampling; the laboratories of Norm Ellstrand and Louis Santiago at the University of California, Riverside, for greenhouse assistance and support; and L. Santiago, B. Gulle Bilgi, M.A. Cushman, and two anonymous reviewers for helpful comments on the manuscript. This work was partially supported by funding from the Smithsonian Tropical Research Institute (to KS and KW), the US Environmental Protection Agency under the Greater Research Opportunities Graduate Program Agreement no. MA 91685201 (to KS), and the National Science Foundation NSF IOB-0543659 (to JCC). This publication was also made possible by the Panamanian Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT), and by the National Institute of Health (NIH) Grant Number P20 RR-016464 from the INBRE Program of the National Center for Research Resources through its support of the Nevada Genomics, Proteomics, and Bioinformatics Centers. The views expressed in this publication are solely those of the authors and the EPA does not endorse any products or commercial services mentioned in this publication. NR 68 TC 9 Z9 9 U1 2 U2 42 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-0957 EI 1460-2431 J9 J EXP BOT JI J. Exp. Bot. PD JUL PY 2014 VL 65 IS 13 SI SI BP 3623 EP 3636 DI 10.1093/jxb/eru234 PG 14 WC Plant Sciences SC Plant Sciences GA AM6DU UT WOS:000339953400025 PM 24913627 ER PT J AU Winter, K Garcia, M Holtum, JAM AF Winter, Klaus Garcia, Milton Holtum, Joseph A. M. TI Nocturnal versus diurnal CO2 uptake: how flexible is Agave angustifolia? SO JOURNAL OF EXPERIMENTAL BOTANY LA English DT Article DE Agave; biofuel; climate change; crassulacean acid metabolism; C-3 photosynthesis; CO2 response; drought stress; temperature response ID CRASSULACEAN ACID METABOLISM; ELEVATED CO2; ENVIRONMENTAL RESPONSES; BIOFUEL FEEDSTOCK; DELTA-C-13 VALUES; CAM PLANTS; PRODUCTIVITY; TEQUILANA; SEEDLINGS; OPUNTIA AB Agaves exhibit the water-conserving crassulacean acid metabolism (CAM) photosynthetic pathway. Some species are potential biofuel feedstocks because they are highly productive in seasonally dry landscapes. In plants with CAM, high growth rates are often believed to be associated with a significant contribution of C-3 photosynthesis to total carbon gain when conditions are favourable. There has even been a report of a shift from CAM to C-3 in response to overwatering a species of Agave. We investigated whether C-3 photosynthesis can contribute substantially to carbon uptake and growth in young and mature Agave angustifolia collected from its natural habitat in Panama. In well-watered plants, CO2 uptake in the dark contributed about 75% of daily carbon gain. This day/night pattern of CO2 exchange was highly conserved under a range of environmental conditions and was insensitive to intensive watering. Elevated CO2 (800 ppm) stimulated CO2 fixation predominantly in the light. Exposure to CO2-free air at night markedly enhanced CO2 uptake during the following light period, but CO2 exchange rapidly reverted to its standard pattern when CO2 was supplied during the subsequent 24 h. Although A. angustifolia consistently engages in CAM as its principal photosynthetic pathway, its relatively limited photosynthetic plasticity does not preclude it from occupying a range of habitats, from relatively mesic tropical environments in Panama to drier habitats in Mexico. C1 [Winter, Klaus; Garcia, Milton; Holtum, Joseph A. M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Holtum, Joseph A. M.] James Cook Univ, Townsville, Qld 4811, Australia. RP Winter, K (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Ancon, Panama. EM winterk@si.edu RI Research ID, CTBCC /O-3564-2014 FU Smithsonian Tropical Research Institute; JCU School of Marine and Tropical Biology FX The authors acknowledge the contributions of J. Aranda who grew and maintained the plants and A. Virgo who drew the illustrations. The research was supported by funds from the Smithsonian Tropical Research Institute. J.A.M.H. was supported by the JCU School of Marine and Tropical Biology. NR 40 TC 4 Z9 4 U1 5 U2 21 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-0957 EI 1460-2431 J9 J EXP BOT JI J. Exp. Bot. PD JUL PY 2014 VL 65 IS 13 SI SI BP 3695 EP 3703 DI 10.1093/jxb/eru097 PG 9 WC Plant Sciences SC Plant Sciences GA AM6DU UT WOS:000339953400031 PM 24648568 ER PT J AU Paul, VJ Ritson-Williams, R Campbell, J Craft, JD Langdon, C AF Paul, V. J. Ritson-Williams, R. Campbell, J. Craft, J. D. Langdon, C. TI Algal chemical ecology in a changing ocean SO PLANTA MEDICA LA English DT Meeting Abstract CT 55th Annual Meeting of the American-Society-of-Pharmacognosy (ASP) CY AUG 02-06, 2014 CL Oxford, MS SP Amer Soc Pharmacognosy C1 [Paul, V. J.; Ritson-Williams, R.; Campbell, J.; Craft, J. D.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Langdon, C.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. NR 0 TC 0 Z9 0 U1 0 U2 6 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 0032-0943 EI 1439-0221 J9 PLANTA MED JI Planta Med. PD JUL PY 2014 VL 80 IS 10 MA IL11 BP 751 EP 752 PG 2 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA AM3VP UT WOS:000339781200013 ER PT J AU Neufeld, MJ AF Neufeld, Michael J. TI Close Up at a Distance: Mapping, Technology and Politics SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Neufeld, Michael J.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 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 JUL PY 2014 VL 55 IS 3 BP 769 EP 772 PG 4 WC History & Philosophy Of Science SC History & Philosophy of Science GA AM3WI UT WOS:000339783100030 ER PT J AU Sofaer, HR Sillett, TS Langin, KM Morrison, SA Ghalambor, CK AF Sofaer, Helen R. Sillett, T. Scott Langin, Kathryn M. Morrison, Scott A. Ghalambor, Cameron K. TI Partitioning the sources of demographic variation reveals density-dependent nest predation in an island bird population SO ECOLOGY AND EVOLUTION LA English DT Article DE Demography; density dependence; fecundity; island syndrome; nest predation; zero-inflated model ID CLUTCH SIZE; MIGRATORY SONGBIRD; WATERFOWL NESTS; MARKED ANIMALS; LIFE-HISTORY; RED DEER; SURVIVAL; FOOD; ABUNDANCE; DYNAMICS AB Ecological factors often shape demography through multiple mechanisms, making it difficult to identify the sources of demographic variation. In particular, conspecific density can influence both the strength of competition and the predation rate, but density-dependent competition has received more attention, particularly among terrestrial vertebrates and in island populations. A better understanding of how both competition and predation contribute to density-dependent variation in fecundity can be gained by partitioning the effects of density on offspring number from its effects on reproductive failure, while also evaluating how biotic and abiotic factors jointly shape demography. We examined the effects of population density and precipitation on fecundity, nest survival, and adult survival in an insular population of orange-crowned warblers (Oreothlypis celata) that breeds at high densities and exhibits a suite of traits suggesting strong intraspecific competition. Breeding density had a negative influence on fecundity, but it acted by increasing the probability of reproductive failure through nest predation, rather than through competition, which was predicted to reduce the number of offspring produced by successful individuals. Our results demonstrate that density-dependent nest predation can underlie the relationship between population density and fecundity even in a high-density, insular population where intraspecific competition should be strong. C1 [Sofaer, Helen R.; Langin, Kathryn M.; Ghalambor, Cameron K.] Colorado State Univ, Grad Degree Program Ecol & Biol Dept, Ft Collins, CO 80523 USA. [Sillett, T. Scott] Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Morrison, Scott A.] Nature Conservancy, San Francisco, CA 94105 USA. RP Sofaer, HR (reprint author), Colorado State Univ, Dept Fish Wildlife & Conservat Biol, 1474 Campus Delivery, Ft Collins, CO 80523 USA. EM Helen.Sofaer@colostate.edu OI Langin, Kathryn/0000-0002-1799-1942 FU Nature Conservancy; Smithsonian Institution; National Science Foundation; Colorado State University FX This research was funded by The Nature Conservancy, the Smithsonian Institution, the National Science Foundation, and Colorado State University. NR 91 TC 5 Z9 5 U1 6 U2 34 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD JUL PY 2014 VL 4 IS 13 BP 2738 EP 2748 DI 10.1002/ece3.1127 PG 11 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA AL9WT UT WOS:000339494900010 PM 25077023 ER PT J AU Field, DJ Gauthier, JA King, BL Pisani, D Lyson, TR Peterson, KJ AF Field, Daniel J. Gauthier, Jacques A. King, Benjamin L. Pisani, Davide Lyson, Tyler R. Peterson, Kevin J. TI Toward consilience in reptile phylogeny: miRNAs support an archosaur, not lepidosaur, affinity for turtles SO EVOLUTION & DEVELOPMENT LA English DT Article ID SISTER GROUP; EVOLUTION; POSITION; GENOME; SHELL; MICRORNAS; HOMOLOGY; INSIGHTS; SNAKES; ORIGIN AB Understanding the phylogenetic position of crown turtles (Testudines) among amniotes has been a source of particular contention. Recent morphological analyses suggest that turtles are sister to all other reptiles, whereas the vast majority of gene sequence analyses support turtles as being inside Diapsida, and usually as sister to crown Archosauria (birds and crocodilians). Previously, a study using microRNAs (miRNAs) placed turtles inside diapsids, but as sister to lepidosaurs (lizards and Sphenodon) rather than archosaurs. Here, we test this hypothesis with an expanded miRNA presence/absence dataset, and employ more rigorous criteria for miRNA annotation. Significantly, we find no support for a turtle+lepidosaur sister-relationship; instead, we recover strong support for turtles sharing a more recent common ancestor with archosaurs. We further test this result by analyzing a super-alignment of precursor miRNA sequences for every miRNA inferred to have been present in the most recent common ancestor of tetrapods. This analysis yields a topology that is fully congruent with our presence/absence analysis; our results are therefore in accordance with most gene sequence studies, providing strong, consilient molecular evidence from diverse independent datasets regarding the phylogenetic position of turtles. C1 [Field, Daniel J.; Gauthier, Jacques A.; Lyson, Tyler R.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06511 USA. [Field, Daniel J.; Lyson, Tyler R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [King, Benjamin L.] Mt Desert Isl Biol Lab, Salsbury Cove, ME 04672 USA. [Pisani, Davide] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. [Pisani, Davide] Univ Bristol, Sch Biol Sci, Bristol BS8 1UG, Avon, England. [Peterson, Kevin J.] Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. RP Field, DJ (reprint author), Yale Univ, Dept Geol & Geophys, 210 Whitney Ave, New Haven, CT 06511 USA. EM daniel.field@yale.edu; kevin.j.peterson@dartmouth.edu OI King, Benjamin/0000-0001-6463-1336; Field, Daniel/0000-0002-1786-0352 FU NSERC CGS; Lougheed Award of Distinction; Yale Peabody Museum of Natural History; NASA-Ames FX The authors thank K. Kuester for providing an egg of Columba livia, J. Musser and G. Watkins-Colwell for assistance processing the pigeon, A. Heimberg and A. Hsiang for comments, J. Tarver and J. Vinther for laboratory assistance, and G. Wagner for providing lab space. Funding for this project was provided by a NSERC CGS and Lougheed Award of Distinction to D. J. F., and Yale Peabody Museum of Natural History to J. A. G. NASA-Ames supported K. J. P and B. L. K. NR 49 TC 30 Z9 30 U1 8 U2 40 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1520-541X EI 1525-142X J9 EVOL DEV JI Evol. Dev. PD JUL-AUG PY 2014 VL 16 IS 4 BP 189 EP 196 DI 10.1111/ede.12081 PG 8 WC Evolutionary Biology; Developmental Biology; Genetics & Heredity SC Evolutionary Biology; Developmental Biology; Genetics & Heredity GA AL8ZM UT WOS:000339428500003 PM 24798503 ER PT J AU How, MJ Christy, J Roberts, NW Marshall, NJ AF How, Martin J. Christy, John Roberts, Nicholas W. Marshall, N. Justin TI Null point of discrimination in crustacean polarisation vision SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE Polarisation distance; Fiddler crab; Mantis shrimp; Discrimination threshold ID STOMATOPOD CRUSTACEAN; PREDATOR AVOIDANCE; MANTIS SHRIMP; COMPOUND EYES; COLOR-VISION; LIGHT; SENSITIVITY; CUTTLEFISH; CONTRAST; OCTOPUS AB The polarisation of light is used by many species of cephalopods and crustaceans to discriminate objects or to communicate. Most visual systems with this ability, such as that of the fiddler crab, include receptors with photopigments that are oriented horizontally and vertically relative to the outside world. Photoreceptors in such an orthogonal array are maximally sensitive to polarised light with the same fixed e-vector orientation. Using opponent neural connections, this two-channel system may produce a single value of polarisation contrast and, consequently, it may suffer from null points of discrimination. Stomatopod crustaceans use a different system for polarisation vision, comprising at least four types of polarisation-sensitive photoreceptor arranged at 0, 45, 90 and 135 deg relative to each other, in conjunction with extensive rotational eye movements. This anatomical arrangement should not suffer from equivalent null points of discrimination. To test whether these two systems were vulnerable to null points, we presented the fiddler crab Uca heteropleura and the stomatopod Haptosquilla trispinosa with polarised looming stimuli on a modified LCD monitor. The fiddler crab was less sensitive to differences in the degree of polarised light when the e-vector was at -45 deg than when the e-vector was horizontal. In comparison, stomatopods showed no difference in sensitivity between the two stimulus types. The results suggest that fiddler crabs suffer from a null point of sensitivity, while stomatopods do not. C1 [How, Martin J.; Roberts, Nicholas W.] Univ Bristol, Sch Biol Sci, Bristol BS8 1TQ, Avon, England. [How, Martin J.; Marshall, N. Justin] Univ Queensland, Queensland Brain Inst, St Lucia, Qld 4072, Australia. [How, Martin J.; Christy, John] Smithsonian Trop Res Inst, Panama City, Panama. RP How, MJ (reprint author), Univ Bristol, Sch Biol Sci, Bristol Life Sci Bldg,Tyndall Ave, Bristol BS8 1TQ, Avon, England. EM m.how@bristol.ac.uk RI How, Martin/G-1925-2010; OI How, Martin/0000-0001-5135-8828; Roberts, Nicholas/0000-0002-4540-6683 FU US Air Force Office of Scientific Research [FA8655-12-1-2112]; Asian and European Offices of Aerospace Research and Development; Queensland-Smithsonian Fellowship FX M.J.H., N.J.M. and N.W.R. were supported by the US Air Force Office of Scientific Research (grant no. FA8655-12-1-2112) and the Asian and European Offices of Aerospace Research and Development. M.J.H. was also supported by a Queensland-Smithsonian Fellowship award. NR 48 TC 5 Z9 5 U1 10 U2 50 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 JUL PY 2014 VL 217 IS 14 BP 2462 EP 2467 DI 10.1242/jeb.103457 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AL6WG UT WOS:000339273500011 PM 24737768 ER PT J AU Karakaya, C Guzeloglu-Kayisli, O Hobbs, RJ Gerasimova, T Uyar, A Erdem, M Oktem, M Erdem, A Gumuslu, S Ercan, D Sakkas, D Comizzoli, P Seli, E Lalioti, MD AF Karakaya, Cengiz Guzeloglu-Kayisli, Ozlem Hobbs, Rebecca J. Gerasimova, Tsilya Uyar, Asli Erdem, Mehmet Oktem, Mesut Erdem, Ahmet Gumuslu, Seyhan Ercan, Deniz Sakkas, Denny Comizzoli, Pierre Seli, Emre Lalioti, Maria D. TI Follicle-stimulating hormone receptor (FSHR) alternative skipping of exon 2 or 3 affects ovarian response to FSH SO MOLECULAR HUMAN REPRODUCTION LA English DT Review DE FSHR; alternative splicing; cumulus cells; IVF or ICSI; ovarian response ID IN-VITRO FERTILIZATION; SINGLE-NUCLEOTIDE POLYMORPHISMS; HUMAN CHORIONIC-GONADOTROPIN; MESSENGER-RNA TRANSCRIPTS; GENOME-WIDE ASSOCIATION; BOVINE GRANULOSA-CELLS; LUTEINIZING-HORMONE; CHROMOSOME 2P16.3; MOLECULAR-CLONING; GENE-EXPRESSION AB Genes critical for fertility are highly conserved in mammals. Interspecies DNA sequence variation, resulting in amino acid substitutions and post-transcriptional modifications, including alternative splicing, are a result of evolution and speciation. The mammalian follicle-stimulating hormone receptor (FSHR) gene encodes distinct species-specific forms by alternative splicing. Skipping of exon 2 of the human FSHR was reported in women of North American origin and correlated with low response to ovarian stimulation with exogenous follicle-stimulating hormone (FSH). To determine whether this variant correlated with low response in women of different genetic backgrounds, we performed a blinded retrospective observational study in a Turkish cohort. Ovarian response was determined as low, intermediate or high according to retrieved oocyte numbers after classifying patients in four age groups (< 35, 35-37, 38-40, > 40). Cumulus cells collected from 96 women undergoing IVF/ICSI following controlled ovarian hyperstimulation revealed four alternatively spliced FSHR products in seven patients (8%): exon 2 deletion in four patients; exon 3 and exons 2 + 3 deletion in one patient each, and a retention of an intron 1 fragment in one patient. In all others (92%) splicing was intact. Alternative skipping of exons 2, 3 or 2 + 3 were exclusive to low responders and was independent of the use of agonist or antagonist. Interestingly, skipping of exon 3 occurs naturally in the ovaries of domestic cats-a good comparative model for human fertility. We tested the signaling potential of human and cat variants after transfection in HEK293 cells and FSH stimulation. None of the splicing variants initiated cAMP signaling despite high FSH doses, unlike full-length proteins. These data substantiate the occurrence of FSHR exon skipping in a subgroup of low responders and suggest that species-specific regulation of FSHR splicing plays diverse roles in mammalian ovarian function. C1 [Karakaya, Cengiz; Guzeloglu-Kayisli, Ozlem; Gerasimova, Tsilya; Uyar, Asli; Sakkas, Denny; Seli, Emre; Lalioti, Maria D.] Yale Univ, Sch Med, Div Reprod Endocrinol & Infertil, Dept Obstet Gynecol & Reprod Sci, New Haven, CT 06510 USA. [Karakaya, Cengiz; Erdem, Mehmet; Oktem, Mesut; Erdem, Ahmet; Gumuslu, Seyhan; Ercan, Deniz] Gazi Univ, Sch Med, Div Reprod Endocrinol & Infertil, IVF Ctr,Dept Obstet & Gynecol, TR-06500 Ankara, Turkey. [Hobbs, Rebecca J.; Comizzoli, Pierre] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Lalioti, MD (reprint author), FMB329J,330 Cedar St, New Haven, CT 06510 USA. EM maria.lalioti@yale.edu FU National Center for Research Resources (NCRR); National Center for Advancing Translational Science (NCATS) [KL2 RR024138]; National Institute of Health (NIH) [R01HD059909]; Smithsonian Scholarly Studies Program FX This work was supported by the National Center for Research Resources (NCRR) and the National Center for Advancing Translational Science (NCATS) (KL2 RR024138) to M.D.L., by the National Institute of Health (NIH) Award (R01HD059909) to E.S., and by the Smithsonian Scholarly Studies Program to PC. The contents of the article are solely the responsibility of the authors and do not necessarily represent the official view of NIH. NR 82 TC 3 Z9 3 U1 2 U2 12 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1360-9947 EI 1460-2407 J9 MOL HUM REPROD JI Mol. Hum. Reprod. PD JUL PY 2014 VL 20 IS 7 BP 630 EP 643 DI 10.1093/molehr/gau024 PG 14 WC Developmental Biology; Obstetrics & Gynecology; Reproductive Biology SC Developmental Biology; Obstetrics & Gynecology; Reproductive Biology GA AL8XZ UT WOS:000339424400004 PM 24670307 ER PT J AU Ballantine, DL Lozada-Troche, C Ruiz, H AF Ballantine, David L. Lozada-Troche, Chad Ruiz, Hector TI Metapeyssonnelia tangerina (Peyssonneliaceae, Rhodophyta), a new species associated with coral reef habitats in Puerto Rico, Caribbean Sea SO PHYCOLOGICAL RESEARCH LA English DT Article DE Caribbean; Metapeyssonnelia tangerina sp nov; Metapeyssonnelia; Peyssonneliaceae; Puerto Rico; Rhodophyta; small subunit ribosomal DNA; western Atlantic ID RIBOSOMAL-RNA GENE; SP-NOV PEYSSONNELIACEAE; SUBUNIT RDNA SEQUENCES; KILLING RED ALGA; RHODYMENIALES RHODOPHYTA; SSU RDNA; ORD NOV; GIGARTINALES; FAMILIES; REPRESENTATIVES AB A new Metapeyssonnelia species that comprises up to 7% bottom cover at shallow-water reef habitats in southwest Puerto Rico is described herein. It forms conspicuous orange encrustations on hard substrata and does not grow on living coral as does its two Caribbean congeners. The new species possesses conspicuous, to 30 cm in extent, tightly adherent crusts up to 950 mu m thick, only hypobasal calcification, hypothallial cells arranged in broad flabellules and superficial (raised) tetrasporangial and carposporangial nemathecia. Tetrasporangia are pedicellate, borne laterally from cup-like cells that are derived from basal paraphysal cells. Tetrasporangia measure up to 120 mu m long and individual carposporangia to 80 mu m long. The new species differs from other Metapeyssonnelia species developmentally in that perithallial cells at mid thallus height will divide laterally to form a new hypothallium. Small subunit gene sequences relate the new species to the two Metapeyssonnelia species that are previously known from Puerto Rico. C1 [Ballantine, David L.; Lozada-Troche, Chad; Ruiz, Hector] Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00709 USA. [Lozada-Troche, Chad] Univ Puerto Rico, Dept Biol, Cayey, PR USA. [Ballantine, David L.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Ballantine, DL (reprint author), Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00709 USA. EM david.ballantine@upr.edu FU National Oceanographic and Atmospheric Administration Coastal Ocean Programs [NA17OP2919]; Institutional Fund for Research Development at UPR- Cayey FX This paper is a result of research funded by the National Oceanographic and Atmospheric Administration Coastal Ocean Programs under award #NA17OP2919 to the University of Puerto Rico - Mayaguez. The research was also funded in part by the Institutional Fund for Research Development at UPR- Cayey awarded to the second author. NR 29 TC 2 Z9 2 U1 1 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1322-0829 EI 1440-1835 J9 PHYCOL RES JI Phycol. Res. PD JUL PY 2014 VL 62 IS 3 BP 197 EP 205 DI 10.1111/pre.12051 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AM0EW UT WOS:000339517600004 ER PT J AU Hsyu, T Johnson, CI Lee, YW Rich, RM AF Hsyu, Tiffany Johnson, Christian I. Lee, Young-Wook Rich, R. Michael TI Light-Element Chemistry and the Double Red Giant Branch in the Galactic Globular Cluster NGC 288 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID MULTIPLE POPULATIONS; MILKY-WAY; ABUNDANCE VARIATIONS; STARS; SPECTROSCOPY; ENRICHMENT; SAMPLE; I. AB The globular cluster NGC 288 was previously reported to exhibit two distinct red giant branches (RGBs) in the narrowband calcium (HK) and Stromgren b- and y-band passes. In order to investigate this phenomenon further, we obtained moderate resolution (R similar to 18,000) spectra of 27 RGB stars in NGC 288 with the Hydra multifiber spectrograph on the Blanco 4 m telescope at Cerro Tololo Inter-American Observatory (CTIO). From these data we derive iron (<[Fe/HD]> = 1.19; sigma = 0.12), oxygen (<[O/Fe]> = +0.25; sigma = 0.13), and sodium (<[Na/Fe]> = +0.15; sigma = 0.26) abundances using standard equivalent width and spectrum synthesis techniques. Combining these data with those available in the literature indicates that the two giant branches have distinctly different light-element chemistry but do not exhibit a significant spread in [Fe/H]. A new transmission tracing for the CTIO Ca filter, obtained for this project, shows that CN contamination is the primary spectral feature driving the split RGB. Interestingly, the CM leak in the current CTIO Ca filter may be used as an efficient means to search for CN-weak and CN-strong stars in systems with otherwise small Ca abundance variations. C1 [Hsyu, Tiffany; Rich, R. Michael] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Johnson, Christian I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lee, Young-Wook] Yonsei Univ, Ctr Galaxy Evolut Res, Seoul 120749, South Korea. [Lee, Young-Wook] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. RP Hsyu, T (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. EM tiffanyhsyu@ucla.edu; cjohnson@cfa.harvard.edu; ywlee2@yonsei.ac.kr; rmr@astro.ucla.edu FU National Aeronautics and Space Administration; National Science Foundation; Clay Fellowship; National Science Foundation [AST-1003201]; NSF [AST-0709479, AST-12112099]; National Research Foundation of Korea (NRF) of Korea FX We thank the referee for a careful review and thoughtful comments that lead to an improvement of the manuscript. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. We thank the Cerro Tololo Inter-American Observatory (CTIO) staff Daniel Holck and Andrea Kunder for providing the new response curve for the CTIO Ca filter. C. I. J gratefully acknowledges support from the Clay Fellowship, administered by the Smithsonian Astrophysical Observatory. This material is based upon work supported by the National Science Foundation under award No. AST-1003201 to C. I. J; R. M. R acknowledges support from NSF grants AST-0709479 and AST-12112099. Y.-W. L. acknowledges support from National Research Foundation of Korea (NRF) of Korea to Center for Galaxy Evolution Research (CGER). NR 38 TC 4 Z9 4 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2014 VL 126 IS 941 BP 597 EP 604 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM1JQ UT WOS:000339602600001 ER PT J AU Gedan, KB Kellogg, L Breitburg, DL AF Gedan, Keryn B. Kellogg, Lisa Breitburg, Denise L. TI Accounting for Multiple Foundation Species in Oyster Reef Restoration Benefits SO RESTORATION ECOLOGY LA English DT Article DE clearance rate; Crassostrea virginica; ecosystem services; Ischadium recurvum; phytoplankton; top-down control; water quality ID CHESAPEAKE BAY; CRASSOSTREA-VIRGINICA; SALINITY GRADIENT; CURRENT KNOWLEDGE; RIVER ESTUARY; BIODIVERSITY; CONSERVATION; HABITAT; EUTROPHICATION; PHYTOPLANKTON AB Many coastal habitat restoration projects are focused on restoring the population of a single foundation species to recover an entire ecological community. Estimates of the ecosystem services provided by the restoration project are used to justify, prioritize, and evaluate such projects. However, estimates of ecosystem services provided by a single species may vastly under-represent true provisioning, as we demonstrate here with an example of oyster reefs, often restored to improve estuarine water quality. In the brackish Chesapeake Bay, the hooked mussel Ischadium recurvum can have greater abundance and biomass than the focal restoration species, the eastern oyster Crassostrea virginica. We measured the temperature-dependent phytoplankton clearance rates of both bivalves and their filtration efficiency on three size classes of phytoplankton to parameterize an annual model of oyster reef filtration, with and without hooked mussels, for monitored oyster reefs and restoration scenarios in the eastern Chesapeake Bay. The inclusion of filtration by hooked mussels increased the filtration capacity of the habitat greater than 2-fold. Hooked mussels were also twice as effective as oysters at filtering picoplankton (1.5-3 mu m), indicating that they fill a distinct ecological niche by controlling phytoplankton in this size class, which makes up a significant proportion of the phytoplankton load in summer. When mussel and oyster filtration are accounted for in this, albeit simplistic, model, restoration of oyster reefs in a tributary scale restoration is predicted to control 100% of phytoplankton during the summer months. C1 [Gedan, Keryn B.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Gedan, Keryn B.; Breitburg, Denise L.] Smithsonian Environm Res Ctr, Edgewater, MD 20137 USA. [Kellogg, Lisa] Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA. RP Gedan, KB (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA. EM kgedan@umd.edu FU David H. Smith Conservation Research Fellowship; Oyster Recovery Partnership FX For assistance with models and graphics, we thank Virginia Clark and Keira Heggie. For donations of datasets, materials, and equipment, we thank Chris Judy, Sharyn Hedrick, Pat Neale, Mitch Tarnowski, and Odi Zmora. We thank the David H. Smith Conservation Research Fellowship for funding to K. Gedan, the Oyster Recovery Partnership for funding sample collection in the Choptank River, and numerous volunteers for collecting and analyzing those samples. NR 48 TC 4 Z9 4 U1 7 U2 66 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1061-2971 EI 1526-100X J9 RESTOR ECOL JI Restor. Ecol. PD JUL PY 2014 VL 22 IS 4 BP 517 EP 524 DI 10.1111/rec.12107 PG 8 WC Ecology SC Environmental Sciences & Ecology GA AM2EP UT WOS:000339662400012 ER PT J AU Collins, CW Monfort, SL Vick, MM Wolfe, BA Weiss, RB Keefer, CL Songsasen, N AF Collins, C. Wynne Monfort, Steven L. Vick, Mandi M. Wolfe, Barbara A. Weiss, Rachael B. Keefer, Carol L. Songsasen, Nucharin TI Oral and injectable synthetic progestagens effectively manipulate the estrous cycle in the Przewalski's horse (Equus ferus przewalskii) SO ANIMAL REPRODUCTION SCIENCE LA English DT Article DE Estrous synchrony; Equids; Altrenogest; Ovulation induction ID ARTIFICIAL-INSEMINATION; REPRODUCTIVE-PERFORMANCE; ENZYME-IMMUNOASSAY; MARES; OVULATION; ALTRENOGEST; SYNCHRONIZATION; PROGESTERONE; ESTRUS; INDUCTION AB To date, there has been limited research on manipulation of the estrous cycle in endangered equids. The objectives of this study were to assess the efficacy of using combinations of: (a) oral altrenogest and PGF(2)alpha, and (b) injectable altrenogest and PGF(2)alpha for manipulation of ovarian activity in Przewalski's mares. Reproductive cycles were monitored by assessing follicular changes with rectal ultrasound and changes in urinary steroid hormones. In Study 1, five cycling mares were treated with oral altrenogest (n = 11 cycles) for 14 days. In Study 2, cycling mares were treated with oral altrenogest for 12 days (n = 5 cycles; n = 5 mares) or a single injection of biorelease altrenogest (n = 10 cycles; n = 6 mares). In all study groups, PGF(2)alpha was given 2 days before cessation of progestagen treatment. In Study 1, mares responded in six of 11 cycles (54%) where treatment occurred with normal ovarian follicular development post hormone therapy. In Study 2, mares responded in four of five (80%, oral altrenogest) and eight of 10 (80%, injectable altrenogest) cycles with the development of an ovulatory follicle. With the use of injectable altrenogest, there was an obvious suppression of urinary estrogens and progetsagens. These results indicate that manipulation of the estrous cycle of Przewalski's mares can be achieved by administering oral (12 days) or injectable form of altrenogest in conjunction with PGF(2)alpha. Findings in the present study may have long term application for the development of timed artificial insemination as a genetic management tool for this critically endangered equid. (C) 2014 Elsevier B.V. All rights reserved. C1 [Collins, C. Wynne; Monfort, Steven L.; Vick, Mandi M.; Songsasen, Nucharin] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Vick, Mandi M.; Wolfe, Barbara A.; Weiss, Rachael B.] Wilds, Cumberland, OH 43732 USA. [Collins, C. Wynne; Keefer, Carol L.] Univ Maryland, Dept Anim & Avian Sci, College Pk, MD 20742 USA. RP Collins, CW (reprint author), Univ Queensland, Sch Vet Sci, Gatton Campus, Gatton, Qld 4343, Australia. EM w.collins@uq.edu.au FU Morris Animal Foundation [D07Z0-403]; Smithsonian Institution Endowment Funds; Shirley Sichel Endowment Fund FX This research was supported by Morris Animal Foundation (Grant numbers: D07Z0-403); Smithsonian Institution Endowment Funds; and the Shirley Sichel Endowment Fund. NR 47 TC 2 Z9 2 U1 2 U2 18 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 JUL PY 2014 VL 148 IS 1-2 BP 42 EP 52 DI 10.1016/j.anireprosci.2014.03.018 PG 11 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA AL4ZU UT WOS:000339144100005 PM 24856195 ER PT J AU Cranmer, SR AF Cranmer, Steven R. TI ENSEMBLE SIMULATIONS OF PROTON HEATING IN THE SOLAR WIND VIA TURBULENCE AND ION CYCLOTRON RESONANCE SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE plasmas; solar wind; Sun: corona; Sun: heliosphere; turbulence; waves ID KINETIC ALFVEN WAVES; ANISOTROPIC MAGNETOHYDRODYNAMIC TURBULENCE; TEMPERATURE-ANISOTROPY; 1 AU; CORONAL HOLES; MAGNETIC-FIELD; MINOR IONS; VELOCITY DISTRIBUTIONS; DIFFERENTIAL FLOW; PLASMA TURBULENCE AB Protons in the solar corona and heliosphere exhibit anisotropic velocity distributions, violation of magnetic moment conservation, and a general lack of thermal equilibrium with the other particle species. There is no agreement about the identity of the physical processes that energize non-Maxwellian protons in the solar wind, but a traditional favorite has been the dissipation of ion cyclotron resonant Alfven waves. This paper presents kinetic models of how ion cyclotron waves heat protons on their journey from the corona to interplanetary space. It also derives a wide range of new solutions for the relevant dispersion relations, marginal stability boundaries, and nonresonant velocity-space diffusion rates. A phenomenological model containing both cyclotron damping and turbulent cascade is constructed to explain the suppression of proton heating at low alpha-proton differential flow speeds. These effects are implemented in a large-scale model of proton thermal evolution from the corona to 1 AU. A Monte Carlo ensemble of realistic wind speeds, densities, magnetic field strengths, and heating rates produces a filled region of parameter space (in a plane described by the parallel plasma beta and the proton temperature anisotropy ratio) similar to what is measured. The high-beta edges of this filled region are governed by plasma instabilities and strong heating rates. The low-beta edges correspond to weaker proton heating and a range of relative contributions from cyclotron resonance. On balance, the models are consistent with other studies that find only a small fraction of the turbulent power spectrum needs to consist of ion cyclotron waves. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [NNX10AC11G]; NSF SHINE program [AGS-1259519] FX The author gratefully acknowledges Adriaan van Ballegooijen, Lauren Woolsey, Phil Isenberg, Peter Gary, Justin Kasper, and Ben Maruca for many valuable discussions. This work was supported by NASA grant NNX10AC11G and NSF SHINE program grant AGS-1259519. The OMNI solar wind data were obtained from the NASA/GSFC Space Physics Data Facility's OMNIWeb service, and we thank the principal investigators of the IMP 8, Wind, and ACE instruments who provided their data to OMNI. This research made extensive use of NASA's Astrophysics Data System (ADS). NR 202 TC 11 Z9 11 U1 1 U2 11 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 JUL PY 2014 VL 213 IS 1 AR 16 DI 10.1088/0067-0049/213/1/16 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL6HO UT WOS:000339233400016 ER PT J AU Jiang, YF Stone, JM Davis, SW AF Jiang, Yan-Fei Stone, James M. Davis, Shane W. TI AN ALGORITHM FOR RADIATION MAGNETOHYDRODYNAMICS BASED ON SOLVING THE TIME-DEPENDENT TRANSFER EQUATION SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE accretion, accretion disks; magnetohydrodynamics (MHD); methods: numerical; radiative transfer ID DOMINATED ACCRETION DISKS; FLUX-LIMITED DIFFUSION; BLACK-HOLES; VERTICAL STRUCTURE; GALACTIC NUCLEI; GODUNOV METHOD; GAS-PRESSURE; HYDRODYNAMICS; SIMULATIONS; INSTABILITY AB We describe a new algorithm for solving the coupled frequency-integrated transfer equation and the equations of magnetohydrodynamics in the regime that light-crossing time is only marginally shorter than dynamical timescales. The transfer equation is solved in the mixed frame, including velocity-dependent source terms accurate to O(v/c). An operator split approach is used to compute the specific intensity along discrete rays, with upwind monotonic interpolation used along each ray to update the transport terms, and implicit methods used to compute the scattering and absorption source terms. Conservative differencing is used for the transport terms, which ensures the specific intensity (as well as energy and momentum) are conserved along each ray to round-off error. The use of implicit methods for the source terms ensures the method is stable even if the source terms are very stiff. To couple the solution of the transfer equation to the MHD algorithms in the ATHENA code, we perform direct quadrature of the specific intensity over angles to compute the energy and momentum source terms. We present the results of a variety of tests of the method, such as calculating the structure of a non-LTE atmosphere, an advective diffusion test, linear wave convergence tests, and the well-known shadow test. We use new semi-analytic solutions for radiation modified shocks to demonstrate the ability of our algorithm to capture the effects of an anisotropic radiation field accurately. Since the method uses explicit differencing of the spatial operators, it shows excellent weak scaling on parallel computers. C1 [Jiang, Yan-Fei] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stone, James M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Davis, Shane W.] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H4, Canada. RP Jiang, YF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA through Einstein Postdoctoral Fellowship [PF-140109]; Chandra X-ray Center; NASA [NAS8-03060, NNX11AF49G]; NSF [AST-1333612] FX We thank the anonymous referee for helpful comments that improved the paper. Support for this work was provided by NASA through Einstein Postdoctoral Fellowship grant number PF-140109 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060, and by NASA grant NNX11AF49G and NSF grant AST-1333612. NR 52 TC 19 Z9 21 U1 0 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 JUL PY 2014 VL 213 IS 1 AR 7 DI 10.1088/0067-0049/213/1/7 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL6HO UT WOS:000339233400007 ER PT J AU Yan, HJ Stefanon, M Ma, ZY Willner, SP Somerville, R Ashby, MLN Dave, R Perez-Gonzalez, PG Cava, A Wiklind, T Kocevski, D Rafelski, M Kartaltepe, J Cooray, A Koekemoer, AM Grogin, NA AF Yan, Haojing Stefanon, Mauro Ma, Zhiyuan Willner, S. P. Somerville, Rachel Ashby, Matthew L. N. Dave, Romeel Perez-Gonzalez, Pablo G. Cava, Antonio Wiklind, Tommy Kocevski, Dale Rafelski, Marc Kartaltepe, Jeyhan Cooray, Asantha Koekemoer, Anton M. Grogin, Norman A. TI OPTICAL-FAINT, FAR-INFRARED-BRIGHT HERSCHEL SOURCES IN THE CANDELS FIELDS: ULTRA-LUMINOUS INFRARED GALAXIES AT z > 1 AND THE EFFECT OF SOURCE BLENDING SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: starburst; infrared: galaxies; methods: data analysis; submillimeter: galaxies ID STAR-FORMING GALAXIES; HUBBLE-DEEP-FIELD; EXTENDED GROTH STRIP; EXTRAGALACTIC LEGACY SURVEY; SUBMILLIMETER GALAXIES; HIGH-REDSHIFT; PHOTOMETRIC REDSHIFTS; MASSIVE GALAXIES; ALMA SURVEY; MU-M AB The Herschel very wide field surveys have charted hundreds of square degrees in multiple far-IR (FIR) bands. While the Sloan Digital Sky Survey (SDSS) is currently the best resource for optical counterpart identifications over such wide areas, it does not detect a large number of Herschel FIR sources and leaves their nature undetermined. As a test case, we studied seven "SDSS-invisible," very bright 250 mu m sources (S-250 > 55 mJy) in the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey fields where we have a rich multi-wavelength data set. We took a new approach to decompose the FIR sources, using the near-IR or the optical images directly for position priors. This is an improvement over the previous decomposition efforts where the priors are from mid-IR data that still suffer from the problem of source blending. We found that in most cases the single Herschel sources are made of multiple components that are not necessarily at the same redshifts. Our decomposition succeeded in identifying and extracting their major contributors. We show that these are all ultra-luminous infrared galaxies at z similar to 1-2 whose high L-IR is mainly due to dust-obscured star formation. Most of them would not be selected as submillimeter galaxies. They all have complicated morphologies indicative of mergers or violent instability, and their stellar populations are heterogeneous in terms of stellar masses, ages, and formation histories. Their current ultra-luminous infrared galaxy phases are of various degrees of importance in their stellar mass assembly. Our practice provides a promising starting point for developing an automatic routine to reliably study bright Herschel sources. C1 [Yan, Haojing; Stefanon, Mauro; Ma, Zhiyuan] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [Willner, S. P.; Ashby, Matthew L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Somerville, Rachel] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Dave, Romeel] Univ Western Cape, ZA-7535 Cape Town, South Africa. [Perez-Gonzalez, Pablo G.] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain. [Cava, Antonio] Univ Geneva, Observ Geneva, CH-1290 Versoix, Switzerland. [Wiklind, Tommy] Joint ALMA Observ, Santiago, Chile. [Kocevski, Dale] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Rafelski, Marc] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Kartaltepe, Jeyhan] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Koekemoer, Anton M.; Grogin, Norman A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Yan, HJ (reprint author), Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. RI Stefanon, Mauro/F-8708-2016; Perez-Gonzalez, Pablo/J-2871-2016; Cava, Antonio/C-5274-2017; OI Stefanon, Mauro/0000-0001-7768-5309; Perez-Gonzalez, Pablo/0000-0003-4528-5639; Cava, Antonio/0000-0002-4821-1275; Koekemoer, Anton/0000-0002-6610-2048 FU Spitzer RSA [1445905]; NASA [HST-GO-12060, NAS5-26555]; Space Telescope Science Institute; Alfred P. Sloan Foundation; National Aeronautics and Space Administration; National Science Foundation; Department of Energy; Japanese Monbukagakusho; Max Planck Society; Spanish MINECO [AYA2012-31277] FX We thank the anonymous referee for the critical reading and useful comments which helped improve the quality of the paper. We thank M. Bolzonella for providing the latest update of the Hyperz code, C. Peng for the useful discussion of the GALFIT code, R. Siebenmorgen for explaining a number of details of the SK07 models, R. Ivison for allowing the use of the non-public radio map in the EGS field, and E. Laird and K. Nandra for the AEGIS Chandra X-ray catalog that is not yet public. We also thank M. Dickinson, H. Ferguson, J. Newman, and M. Salvato for their useful comments. H.Y., M.S., and Z.M. acknowledge the support of Spitzer RSA 1445905. This work is based on observations made by Herschel, an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. Support for Program number HST-GO-12060 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This work is also based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This work also makes use of the SDSS. 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 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 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, Los Alamos National Laboratory, the Max Planck Institute for Astronomy, the Max Planck Institute for Astrophysics, New Mexico State University, the University of Pittsburgh, Princeton University, the US Naval Observatory, and the University of Washington. This paper has used data obtained by the SHARDS project, funded by the Spanish MINECO grant AYA2012-31277, and based on observations made with the Gran Telescopio Canarias (GTC). NR 106 TC 7 Z9 7 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 JUL PY 2014 VL 213 IS 1 AR 2 DI 10.1088/0067-0049/213/1/2 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL6HO UT WOS:000339233400002 ER PT J AU Ellison, AR Savage, AE DiRenzo, GV Langhammer, P Lips, KR Zamudio, KR AF Ellison, Amy R. Savage, Anna E. DiRenzo, Grace V. Langhammer, Penny Lips, Karen R. Zamudio, Kelly R. TI Fighting a Losing Battle: Vigorous Immune Response Countered by Pathogen Suppression of Host Defenses in the Chytridiomycosis-Susceptible Frog Atelopus zeteki SO G3-GENES GENOMES GENETICS LA English DT Article DE Batrachochytrium dendrobatidis; immunogenomics Atelopus zeteki; acquired immunity immuno-suppression; genetics of immunity; innate immunity; complex genetics; tolerance complex immunity; infection resistance ID FUNGUS BATRACHOCHYTRIUM-DENDROBATIDIS; EMERGING INFECTIOUS-DISEASES; GLOBAL AMPHIBIAN DECLINES; DEADLY CHYTRID FUNGUS; TIME TAQMAN PCR; GENE-EXPRESSION; RNA-SEQ; POPULATION DECLINES; SERINE PROTEASES; REFERENCE GENOME AB The emergence of the disease chytridiomycosis caused by the chytrid fungus Batrachochytrium dendrobatidis (Bd) has been implicated in dramatic global amphibian declines. Although many species have undergone catastrophic declines and/or extinctions, others appear to be unaffected or persist at reduced frequencies after Bd outbreaks. The reasons behind this variance in disease outcomes are poorly understood: differences in host immune responses have been proposed, yet previous studies suggest a lack of robust immune responses to Bd in susceptible species. Here, we sequenced transcriptomes from clutchmates of a highly susceptible amphibian, Atelopus zeteki, with different infection histories. We found significant changes in expression of numerous genes involved in innate and inflammatory responses in infected frogs despite high susceptibility to chytridiomycosis. We show evidence of acquired immune responses generated against Bd, including increased expression of immunoglobulins and major histocompatibility complex genes. In addition, fungal-killing genes had significantly greater expression in frogs previously exposed to Bd compared with Bd-na ve frogs, including chitinase and serine-type proteases. However, our results appear to confirm recent in vitro evidence of immune suppression by Bd, demonstrated by decreased expression of lymphocyte genes in the spleen of infected compared with control frogs. We propose susceptibility to chytridiomycosis is not due to lack of Bd-specific immune responses but instead is caused by failure of those responses to be effective. Ineffective immune pathway activation and timing of antibody production are discussed as potential mechanisms. However, in light of our findings, suppression of key immune responses by Bd is likely an important factor in the lethality of this fungus. C1 [Ellison, Amy R.; Savage, Anna E.; Zamudio, Kelly R.] Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA. [Savage, Anna E.] Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. [DiRenzo, Grace V.; Lips, Karen R.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Langhammer, Penny] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. RP Ellison, AR (reprint author), Cornell Univ, E221 Corson Hall, Ithaca, NY 14853 USA. EM are35@cornell.edu RI Savage, Anna/D-8296-2015; Zamudio, Kelly/R-3533-2016; OI Savage, Anna/0000-0002-4917-8358; Zamudio, Kelly/0000-0001-5107-6206; Lips, Karen/0000-0002-2719-1551; Ellison, Amy/0000-0003-3885-6077 FU National Science Foundation [DEB-0815315, DEB-1120249]; Cornell Center for Vertebrate Genomics; Cornell's Atkinson Center for Sustainable Future FX We thank Vicky Poole and Kevin Murphy of Project Golden Frog and the Maryland Zoo in Baltimore for help in obtaining surplus Atelopus zeteki for research; Steven Bogdanowicz and Jennifer Mosher for advice on Illumina library preparation; Brian Gratwicke for photography; and Brian Lazzaro and Zamudio Lab members for their constructive comments. This study was supported by grants from the National Science Foundation (DEB-0815315 and DEB-1120249), the Cornell Center for Vertebrate Genomics, and Cornell's Atkinson Center for Sustainable Future. NR 102 TC 23 Z9 23 U1 3 U2 72 PU GENETICS SOCIETY AMERICA PI BETHESDA PA 9650 ROCKVILLE AVE, BETHESDA, MD 20814 USA SN 2160-1836 J9 G3-GENES GENOM GENET JI G3-Genes Genomes Genet. PD JUL 1 PY 2014 VL 4 IS 7 BP 1275 EP 1289 DI 10.1534/g3.114.010744 PG 15 WC Genetics & Heredity SC Genetics & Heredity GA AL7PK UT WOS:000339326600009 PM 24841130 ER PT J AU Lemoine, X Zeder, MA Bishop, KJ Rufolo, SJ AF Lemoine, Ximena Zeder, Melinda A. Bishop, Katelyn J. Rufolo, Scott J. TI A new system for computing dentition-based age profiles in Sus scrofa SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Aging; Sus scrofa; Pig; Harvest profiles; Tooth eruption; Tooth wear; Zooarchaeology ID GOATS CAPRA-HIRCUS; TOOTH ERUPTION; MOLAR ERUPTION; WILD BOAR; DOMESTICATION; FUSION; DEATH; WEAR AB Reconstructing demographic profiles is valuable for revealing animal exploitation strategies at archaeological sites. For pig (Sus scrofa), the method presented by Grant (1982) demonstrates a promising technique for estimating age through dental wear pattern analysis. Grant's study is, however, limited as it requires complete or nearly complete mandibles, exclusively uses mandibular teeth, and offers only a relative scale for aging. While some work has been done to establish useful age classes based on tooth eruption and wear patterns in S. scrofa, a systematic study producing a standardized and comprehensive methodology for using tooth wear to age pigs remains to be conducted. The study presented here is part of ongoing research aimed at developing new methods for the construction of S. scrofa demographic profiles based on both dentition and long bone fusion. In this paper, we present the results of a study of eruption and wear patterns in a large modern assemblage of wild boar which provides the basis for a new method for constructing pig harvest profiles and addresses some of the most serious limitations of Grant's earlier study. The utility of this method in detecting subtle differences in pig prey/harvest profiles is demonstrated through its application to three Near Eastern archaeological assemblages from three distinct time periods: Bronze Age Tell Leilan, Halafian Banahilk, and Epipaleolithic Hallan cemi, where residents likely employed widely different pig exploitation strategies. The results of these case studies demonstrate the ability of this method to reliably reconstruct age demography and distinguish age profiles between sites with different animal procurement strategies. This method provides a standardized means of collecting accurate and reliable age data crucial in examining patterns of past pig exploitation. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Lemoine, Ximena; Zeder, Melinda A.; Rufolo, Scott J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. [Bishop, Katelyn J.] Univ Calif Los Angeles, Dept Anthropol, Los Angeles, CA 90024 USA. RP Lemoine, X (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. EM lemoinex@SI.edu FU Wenner-Gren Foundation [Gr. 8619]; Committee for Research and Exploration of the National Geographic Society [9113-13]; Scholarly Studies Humanities Fund of the Smithsonian Institution FX This research has been supported by grants from the Wenner-Gren Foundation (Gr. 8619), the Committee for Research and Exploration of the National Geographic Society (9113-13), and the Scholarly Studies Humanities Fund of the Smithsonian Institution. We would like to express our very great appreciation to Sebastian Payne who not only provided us access to the remarkable collection of wild boar he collected, but put us up in his lovely home while we studied these skeletons. His hospitality and generosity during this study greatly enhanced our work and lifted our spirits. Thanks also go to Rosemary Payne for lending us her study while we conducted this work. We would also like to thank the Zoology Department of the Field Museum of Natural History and the Division of Mammals of the National Museum of Natural History for providing access to the modern museum collections analyzed in this study. Additional thanks go to Anna Goldfield for redrawing tooth-wear patterns in Fig. 1 for this publication. Finally, a special thank you goes to Bruce D. Smith for providing us with the appropriate attire to get through this study. NR 43 TC 6 Z9 6 U1 1 U2 16 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 JUL PY 2014 VL 47 BP 179 EP 193 DI 10.1016/j.jas.2014.04.002 PG 15 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA AL3OE UT WOS:000339037300016 ER PT J AU Lemorini, C Plummer, TW Braun, DR Crittenden, AN Ditchfield, PW Bishop, LC Hertel, F Oliver, JS Marlowe, FW Schoeninger, MJ Potts, R AF Lemorini, Cristina Plummer, Thomas W. Braun, David R. Crittenden, Alyssa N. Ditchfield, Peter W. Bishop, Laura C. Hertel, Fritz Oliver, James S. Marlowe, Frank W. Schoeninger, Margaret J. Potts, Richard TI Old stones' song: Use-wear experiments and analysis of the Oldowan quartz and quartzite assemblage from Kanjera South (Kenya) SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Early Pleistocene; Oldowan archaeological sites; Artifact function; Kenya ID UNDERGROUND-STORAGE ORGANS; INVESTIGATING MICROWEAR POLISHES; HUMAN LIFE-HISTORY; ISOTOPIC EVIDENCE; FALLBACK FOODS; OLDUVAI-GORGE; HOMO-ERECTUS; PLANT FOODS; MORTALITY PROFILES; FLK ZINJANTHROPUS AB Evidence of Oldowan tools by similar to 2.6 million years ago (Ma) may signal a major adaptive shift in hominin evolution. While tool-dependent butchery of large mammals was important by at least 2.0 Ma, the use of artifacts for tasks other than faunal processing has been difficult to diagnose. Here we report on use-wear analysis of similar to 2.0 Ma quartz and quartzite artifacts from Kanjera South, Kenya. A use-wear framework that links processing of specific materials and tool motions to their resultant use-wear patterns was developed. A blind test was then carried out to assess and improve the efficacy of this experimental use-wear framework, which was then applied to the analysis of 62 Oldowan artifacts from Kanjera South. Use-wear on a total of 23 artifact edges was attributed to the processing of specific materials. Use-wear on seven edges (30%) was attributed to animal tissue processing, corroborating zooarchaeological evidence for butchery at the site. Use-wear on 16 edges (70%) was attributed to the processing of plant tissues, including wood, grit-covered plant tissues that we interpret as underground storage organs (USOs), and stems of grass or sedges. These results expand our knowledge of the suite of behaviours carried out in the vicinity of Kanjera South to include the processing of materials that would be 'invisible' using standard archaeological methods. Wood cutting and scraping may represent the production and/or maintenance of wooden tools. Use-wear related to USO processing extends the archaeological evidence for hominin acquisition and consumption of this resource by over 1.5 Ma. Cutting of grasses, sedges or reeds may be related to a subsistence task (e.g., grass seed harvesting, cutting out papyrus culm for consumption) and/or a non-subsistence related task (e.g., production of 'twine,' simple carrying devices, or bedding). These results highlight the adaptive significance of lithic technology for hominins at Kanjera. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Lemorini, Cristina] Univ Roma La Sapienza, Dipartimento Sci Antichita, I-00185 Rome, Italy. [Plummer, Thomas W.] CUNY Queens Coll, Dept Anthropol, Flushing, NY 11367 USA. [Plummer, Thomas W.] CUNY, NYCEP, Flushing, NY 11367 USA. [Braun, David R.] Univ Cape Town, Dept Archaeol, ZA-7701 Rondebosch, South Africa. [Braun, David R.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Braun, David R.] Max Planck Inst Evolutionary Anthropol, Dept Human Evolut, D-04103 Leipzig, Germany. [Crittenden, Alyssa N.] Univ Nevada, Dept Anthropol, Las Vegas, NV 89154 USA. [Ditchfield, Peter W.] Univ Oxford, Res Lab Archaeol & Hist Art, Oxford OX1 3QT, England. [Bishop, Laura C.; Oliver, James S.] Liverpool John Moores Univ, Sch Nat Sci & Psychol, Res Ctr Evolutionary Anthropol & Palaeoecol, Liverpool L3 3AF, Merseyside, England. [Hertel, Fritz] Calif State Univ Northridge, Dept Biol, Northridge, CA 91330 USA. [Oliver, James S.] Illinois State Museum, Dept Anthropol, Springfield, IL 62703 USA. [Marlowe, Frank W.] Univ Cambridge, Dept Archaeol & Anthropol, Div Biol Anthropol, Cambridge CB2 3QG, England. [Schoeninger, Margaret J.] Univ Calif San Diego, Dept Anthropol, San Diego, CA 92093 USA. [Potts, Richard] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20013 USA. [Potts, Richard] Natl Museums Kenya, Dept Earth Sci, Palaeontol Sect, Nairobi, Kenya. RP Plummer, TW (reprint author), CUNY Queens Coll, Dept Anthropol, Flushing, NY 11367 USA. EM cristina.lemorini@uniroma1.it; thomas.plummer@qc.cuny.edu; drbraun76@gmail.com; Alyssa.Crittenden@unlv.edu; peter.ditchfield@rlaha.ox.ac.uk; L.C.Bishop@ljmu.ac.uk; fritz.hertel@csun.edu; J.S.Oliver@2012.ljmu.ac.uk; frank.marlowe@gmail.com; mjschoen@ucsd.edu; POTTSR@si.edu OI Bishop, Laura/0000-0002-4216-8667; , cristina/0000-0002-6998-1615 FU Smithsonian's Human Origins Program; L. S. B. Leakey Foundation; National Geographic Society; National Science Foundation; Wenner-Gren Foundation; Professional Staff Congress-City University of New York Research Award Program; University of California, San Diego FX We are grateful to the Office of the President of Kenya, the National Museums of Kenya for permission to study the Kanjera fossils and artifacts, and the Tanzanian Commission for Science and Technology (COSTECH). The Homa Peninsula field research was conducted through the cooperative agreement between the National Museums of Kenya and the Smithsonian Institution. Logistical support and funding was also provided by the Smithsonian's Human Origins Program. Funding for Kanjera field and laboratory work from the L. S. B. Leakey Foundation, the National Geographic Society, the National Science Foundation, the Wenner-Gren Foundation, and the Professional Staff Congress-City University of New York Research Award Program is gratefully acknowledged. The Tanzanian fieldwork was funded by the National Science Foundation and the University of California, San Diego. We thank Jennifer Parkinson and Frances Forrest for their assistance in conducting the blind test experiments. Finally, we would also like to gratefully acknowledge the Hadza for their participation. NR 126 TC 22 Z9 22 U1 5 U2 30 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD JUL PY 2014 VL 72 BP 10 EP 25 DI 10.1016/j.jhevol.2014.03.002 PG 16 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AL4XZ UT WOS:000339139400002 PM 24726228 ER PT J AU Williams, EM Gordon, AD Richmond, BG AF Williams, E. M. Gordon, A. D. Richmond, B. G. TI Biomechanical strategies for accuracy and force generation during stone tool production SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Dart-thrower's arc; Hand and wrist evolution; Kinematics; Knapping; Oldowan tool making; Wrist anatomy ID OVERARM THROWS; KNUCKLE-WALKING; HUMAN-EVOLUTION; COORDINATION PATTERNS; BASEBALL PLAYERS; DIFFERENT SPEEDS; MIDCARPAL JOINT; FOSSIL EVIDENCE; HAND; WRIST AB Multiple hominin species used and produced stone tools, and the archaeological record provides evidence that stone tool behaviors intensified among later members of the genus Homo. This intensification is widely thought to be the product of cognitive and anatomical adaptations that enabled later Homo taxa to produce stone tools more efficiently relative to earlier hominin species. This study builds upon recent investigations of the knapping motions of modern humans to test whether aspects of our upper limb anatomy contribute to accuracy and/or efficiency. Knapping kinematics were captured from eight experienced knappers using a Vicon motion capture system. Each subject produced a series of Oldowan bifacial choppers under two conditions: with normal wrist mobility and while wearing a brace that reduced wrist extension (similar to 30 degrees-35 degrees), simulating one aspect of the likely primitive hominin condition. Under normal conditions, subjects employed a variant of the proximal-to-distal joint sequence common to throwing activities: subjects initiated down-swing upper limb motion at the shoulder and proceeded distally, increasing peak linear and angular velocities from the shoulder to the elbow to the wrist. At the wrist, subjects utilized the 'dart-thrower's arc,' the most stable plane of radiocarpal motion, during which wrist extension is coupled with radial deviation and flexion with ulnar deviation. With an unrestrained wrist, subjects achieved significantly greater target accuracy, wrist angular velocities, and hand linear velocities compared with the braced condition. Additionally, the modern wrist's ability to reach high degrees of extension (>= 28.5 degrees) following strike may decrease risk of carpal and ligamentous damage caused by hyperextension. These results suggest that wrist extension in humans contributes significantly to stone tool-making performance. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Williams, E. M.] Chatham Univ, Dept Biol, Pittsburgh, PA 15232 USA. [Gordon, A. D.] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Richmond, B. G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, B. G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. RP Williams, EM (reprint author), Chatham Univ, Dept Biol, Buhl Hall,Woodland Rd, Pittsburgh, PA 15232 USA. EM ewilliams2@chatham.edu; agordon@albany.edu; brich@gwu.edu OI Gordon, Adam/0000-0002-1807-4644 FU National Science Foundation [BCS-0903652]; Integrative Graduate Education and Research Traineeship (IGERT) [DGE 9987590, DGE 0801634]; L'Oreal USA Fellowship for Women in Science; Bouchet Dissertation Writing Fellowship (The George Washington University Chapter); George Washington University FX We are very grateful to the knappers that took part in this experiment. We appreciate the assistance provided by Alison Brooks, Peter Lucas, Daniel Schmitt, Dietrich Stout, and Kevin Hatala in preparing this manuscript. We also wish to thank Craig Ratzat at Neolithics.com for his careful selection of raw materials for this project. This research was supported by the National Science Foundation's Doctoral Dissertation Improvement Grant (# BCS-0903652) and Integrative Graduate Education and Research Traineeship (IGERT # DGE 9987590 and # DGE 0801634), The L'Oreal USA Fellowship for Women in Science, The Bouchet Dissertation Writing Fellowship (The George Washington University Chapter), and by The George Washington University's Research Enhancement Fund and Selective Excellence Fund. NR 71 TC 4 Z9 4 U1 2 U2 19 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD JUL PY 2014 VL 72 BP 52 EP 63 DI 10.1016/j.jhevol.2014.03.004 PG 12 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AL4XZ UT WOS:000339139400004 PM 24746547 ER PT J AU Li, R Wen, J AF Li, Rong Wen, Jun TI Phylogeny and biogeography of Asian Schefflera (Araliaceae) based on nuclear and plastid DNA sequence data SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Article DE Araliaceae; Asian Schefflera; biogeography; phylogeny ID CHLOROPLAST DNA; PHILIPPINE ARCHIPELAGO; MOLECULAR PHYLOGENY; MALAYSIAN REGION; CLOSE RELATIVES; RIBOSOMAL DNA; LARGE GENUS; DATA SETS; EVOLUTION; DIVERSIFICATION AB The phylogeny of Asian Schefflera was inferred from sequences of the nuclear ribosomal internal transcribed spacer region, and six plastid regions (the ndhF gene, the trnL-trnF region, the rps16 intron, the atpB-rbcL intergenic spacer, the rpl16 intron, and the psbA-trnH intergenic spacer). Phylogenetic analyses of the combined plastid and internal transcribed spacer data with parsimony and Bayesian methods strongly support the monophyly of Asian Schefflera. The genus is supported to be closely related to Heteropanax and Tetrapanax with the small tropical continental Asian genus Heteropanax as its sister. Within Asian Schefflera, four distinct subclades were identified: (i) the widely distributed Asian Heptapleurum group with no styles in the gynoecium; (ii) the main Agalma group with racemose or spicate inflorescence units with a few umbellate taxa; (iii) the Schefflera hypoleuca group; and (iv) the Schefflera heptaphylla group. In a broader phylogenetic framework of Araliaceae, Asian Schefflera is hypothesized to have originated in continental Asia at 57.41 Mya (95% high posterior density interval of 40.33-76.06 Mya) in the early Tertiary and radiated into the now SE Asia, eastern Himalaya, and E Asia at 46.11 Mya (95% high posterior density interval of 33.02-60.69 Mya). Its subsequent diversification in Asia may have been driven largely by the collision of the Indian plate with the Asian plate in the middle Eocene and the collision of the Australian margin with the Eurasian margin in the early Miocene. C1 [Li, Rong] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650201, Peoples R China. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Wen, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. EM wenj@si.edu FU John D. and Catherine T. MacArthur Foundation; Laboratory of Analytical Biology at the National Museum of Natural History of the Smithsonian Institution; Independent Research Program of the Chinese Academy of Sciences [KSCX2-EW-J-24] FX The study was supported by a grant from the John D. and Catherine T. MacArthur Foundation, the Laboratory of Analytical Biology at the National Museum of Natural History of the Smithsonian Institution, and the Independent Research Program of the Chinese Academy of Sciences (Grant No. KSCX2-EW-J-24). Laboratory assistance was provided by Jeff HUNT, Lei XIE, Xinwei XU, and Yunjuan ZUO. We thank S. OLIVER, M. K. PATHAK, H. KATO, Heng LI, and Yumin SHUI for collecting samples and field assistance. NR 80 TC 7 Z9 8 U1 5 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1674-4918 EI 1759-6831 J9 J SYST EVOL JI J. Syst. Evol. PD JUL PY 2014 VL 52 IS 4 BP 431 EP 449 DI 10.1111/jse.12052 PG 19 WC Plant Sciences SC Plant Sciences GA AL3EE UT WOS:000339007600004 ER PT J AU Dalebout, ML Baker, CS Steel, D Thompson, K Robertson, KM Chivers, SJ Perrin, WF Goonatilake, M Anderson, RC Mead, JG Potter, CW Thompson, L Jupiter, D Yamada, TK AF Dalebout, Merel L. Baker, C. Scott Steel, Debbie Thompson, Kirsten Robertson, Kelly M. Chivers, Susan J. Perrin, William F. Goonatilake, Manori Anderson, R. Charles Mead, James G. Potter, Charles W. Thompson, Lisa Jupiter, Danielle Yamada, Tadasu K. TI Resurrection of Mesoplodon hotaula Deraniyagala 1963: A new species of beaked whale in the tropical Indo-Pacific SO MARINE MAMMAL SCIENCE LA English DT Article DE speciation; taxonomy; species delimitation; mtDNA; nuclear introns; Y-chromosome; morphology; Mesoplodon; beaked whale ID DNA EXTRACTION; ANCIENT DNA; ZIPHIIDAE; PURIFICATION; SEQUENCE; NUCLEAR; CETACEA; DISTINCTIVENESS; PHYLOGEOGRAPHY; DELIMITATION AB We present genetic and morphological evidence supporting the recognition of a previously synonymized species of Mesoplodon beaked whale in the tropical Indo-Pacific, Mesoplodon hotaula. Although the new species is closely-related to the rare ginkgo-toothed beaked whale M. ginkgodens, we show that these two lineages can be differentiated by maternally (mitochondrial DNA), biparentally (autosomal), and paternally (Y chromosome) inherited DNA sequences, as well as by morphological features. The reciprocal monophyly of the mtDNA genealogies and the largely parapatric distribution of these lineages is consistent with reproductive isolation. The new lineage is currently known from at least seven specimens: Sri Lanka (1), Gilbert Islands, Republic of Kiribati (1+), Palmyra Atoll, Northern Line Islands, U. S. A. (3), Maldives (1), and Seychelles (1). The type specimen (Sri Lanka) was described as a new species, M. hotaula, in 1963, but later synonymized with M. ginkgodens. This discovery brings the total number of Mesoplodon species to 15, making it, by far, the most speciose yet least known genus of cetaceans. C1 [Dalebout, Merel L.] Univ New S Wales, Sch Biol Earth & Environm Sci, Sydney, NSW 2052, Australia. [Baker, C. Scott; Steel, Debbie; Thompson, Kirsten] Univ Auckland, Sch Biol Sci, Auckland 1000, New Zealand. [Baker, C. Scott; Steel, Debbie] Oregon State Univ, Hatfield Marine Sci Ctr, Marine Mammal Inst, Newport, OR 97365 USA. [Robertson, Kelly M.; Chivers, Susan J.; Perrin, William F.] NOAA, Southwest Fisheries Sci Ctr, NMFS, La Jolla, CA 92037 USA. [Goonatilake, Manori] Dept Natl Museums, Colombo 7, Sri Lanka. [Anderson, R. Charles] Manta Marine Pvt Ltd, Male, Maldives. [Mead, James G.; Potter, Charles W.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Thompson, Lisa; Jupiter, Danielle] Isl Conservat Soc Fdn Conservat Iles Pointe Larue, Victoria, Seychelles. [Yamada, Tadasu K.] Natl Sci Museum, Shinjuku Ku, Tokyo 1690073, Japan. RP Dalebout, ML (reprint author), Univ New S Wales, Sch Biol Earth & Environm Sci, Sydney, NSW 2052, Australia. EM mereldalebout@gmail.com OI Thompson, Kirsten Freja/0000-0003-4277-3549 FU US Marine Mammal Commission; National Geographic Society FX For collection and access to samples and specimens, we thank Roger V. Grace (Kiribati), NOAA Pacific Islands Regional Office, U. S. Fish and Wildlife Service, and the Nature Conservancy (Palmyra Atoll), New Zealand Department of Conservation field center staff (NZ DoC), John Wang, FormosaCetus, Taiwan, Janette Norman and Wayne Longmore, Museum Victoria, Melbourne, Australia, and Abdullah Asif Waheed, Maldives. We thank the Director General of the Department of Wildlife Conservation of Sri Lanka, and the Director of Departments of the National Museums of Sri Lanka for permission to sample the M. hotaula holotype and tissue-export permits. We thank Bob Pitman, US NMFS Southwest Fisheries Science Center, for discussion regarding color pattern differences, Anton van Helden, National Museum of New Zealand Te Papa Tongarewa for photographs and discussion regarding M. ginkgodens. This manuscript benefitted from comments by Randall Reeves, IUCN Cetacean Specialist Group, and three anonymous reviewers. For additional photographs, we thank Hans Stoffregen and Bryan Williams (NZ DoC). Partial funding for laboratory analyses was provided by grants to CSB from the US Marine Mammal Commission and the National Geographic Society. MLD is a Visiting Fellow at the University of New South Wales, Sydney, Australia. NR 62 TC 12 Z9 15 U1 0 U2 37 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0824-0469 EI 1748-7692 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD JUL PY 2014 VL 30 IS 3 BP 1081 EP 1108 DI 10.1111/mms.12113 PG 28 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA AL4KM UT WOS:000339101800013 ER PT J AU MacPherson, GJ Krot, AN AF MacPherson, Glenn J. Krot, Alexander N. TI The formation of Ca-, Fe-rich silicates in reduced and oxidized CV chondrites: The roles of impact-modified porosity and permeability, and heterogeneous distribution of water ices SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID OXYGEN-ISOTOPIC COMPOSITIONS; ALLENDE DARK INCLUSIONS; EARLY SOLAR-SYSTEM; CARBONACEOUS CHONDRITES; MAGNETIC-SUSCEPTIBILITY; AQUEOUS ALTERATION; ASTEROIDAL ALTERATION; FAYALITE FORMATION; IODINE-XENON; BALI-LIKE AB CV (Vigarano type) carbonaceous chondrites, comprising Allende-like (CVoxA) and Bali-like (CVoxB) oxidized and reduced (CVred) subgroups, experienced differing degrees of fluid-assisted thermal and shock metamorphism. The abundance and speciation of secondary minerals produced during asteroidal alteration differ among the subgroups: (1) ferroan olivine and diopside-hedenbergite solid solution pyroxenes are common in all CVs; (2) nepheline and sodalite are abundant in CVoxA, rare in CVred, and absent in CVoxB; (3) phyllosilicates and nearly pure fayalite are common in CVoxB, rare in CVred, and virtually absent in CVoxA; (4) andradite, magnetite, and Fe-Ni-sulfides are common in oxidized CVs, but rare in reduced CVs; the latter contain kirschsteinite instead. Thus, a previously unrecognized correlation exists between meteorite bulk permeabilities and porosities with the speciation of the Ca-, Fe-rich silicates (pyroxenes, andradite, kirschsteinite) among the CVox and CVred meteorites. The extent of secondary mineralization was controlled by the distribution of water ices, permeability, and porosity, which in turn were controlled by impacts on the asteroidal parent body. More intense shock metamorphism in the region where the reduced CVs originated decreased their porosity and permeability while simultaneously expelling intergranular ices and fluids. The mineralogy, petrography, and bulk chemical compositions of both the reduced and oxidized CV chondrites indicate that mobile elements were redistributed between Ca, Al-rich inclusions, dark inclusions, chondrules, and matrices only locally; there is no evidence for large-scale (>several cm) fluid transport. Published Mn-53-Cr-53 ages of secondary fayalite in CV, CO, and unequilibrated ordinary chondrites, and carbonates in CI, CM, and CR chondrites are consistent with aqueous alteration initiated by heating of water ice-bearing asteroids by decay of Al-26, not shock metamorphism. C1 [MacPherson, Glenn J.] Smithsonian Inst, Dept Mineral Sci, US Natl Museum Nat Hist, Washington, DC 20560 USA. [Krot, Alexander N.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Sch Ocean Earth Sci & Technol, Honolulu, HI 96821 USA. RP MacPherson, GJ (reprint author), Smithsonian Inst, Dept Mineral Sci, US Natl Museum Nat Hist, Washington, DC 20560 USA. EM macphers@si.edu FU NASA [NNX11AD43G, NNX07AJ05G, NNX10AH76G] FX We thank Cari Corrigan and Michael Velbel for very helpful and illuminating discussions. We also thank Larry Grossman and Steve Simon (both at University of Chicago) for very generously loaning us thin sections of Allende CAIs from their collection. The paper benefited from reviews by Neyda Abreu, Lysa Chizmadia, and Associate Editor Ed Scott. This work was supported under NASA grants NNX11AD43G and NNX07AJ05G (GJM, P.I.), and NNX10AH76G (ANK, P.I.). NR 75 TC 11 Z9 11 U1 1 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2014 VL 49 IS 7 BP 1250 EP 1270 DI 10.1111/maps.12316 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AL5FQ UT WOS:000339159300008 ER PT J AU Slater, GJ AF Slater, Graham J. TI Correction to 'Phylogenetic evidence for a shift in the mode of mammalian body size evolution at the Cretaceous-Palaeogene boundary', and a note on fitting macroevolutionary models to comparative paleontological data sets SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE fossils; macroevolution; non-ultrametric; Ornstein-Uhlenbeck; variance-covariance matrix ID TREES AB In this note, I correct two errors from an earlier paper that investigated tempo and mode of mammalian body size evolution across the Cretaceous-Palaeogene boundary. Both errors arose from use of branch length rescaling under the Ornstein-Uhlenbeck process, which I here show to be inappropriate for non-ultrametric trees. Correction of these errors does not change the conclusions of my original study. However, recognition of the underlying problem highlights that comparative methods developed by biologists for examining trait evolution on ultrametric trees may not always be appropriate for paleontological datasets. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Slater, GJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. EM SlaterG@si.edu NR 13 TC 6 Z9 6 U1 3 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X EI 2041-2096 J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD JUL PY 2014 VL 5 IS 7 BP 714 EP 718 DI 10.1111/2041-210X.12201 PG 5 WC Ecology SC Environmental Sciences & Ecology GA AL6MT UT WOS:000339247500015 ER PT J AU Kralj-Fiser, S Celik, T Lokovsek, T Suen, K Siling, R Kuntner, M AF Kralj-Fiser, Simona Celik, Tatjana Lokovsek, Tjasa Suen, Klavdija Siling, Rebeka Kuntner, Matjaz TI Development and growth in synanthropic species: plasticity and constraints SO NATURWISSENSCHAFTEN LA English DT Article DE Arthropod development; Growth patterns; Life history; Nuctenea umbratica; Spider; Urban ecology ID SEXUAL SIZE DIMORPHISM; ORB-WEAVING SPIDER; MANDUCA-SEXTA L; BODY-SIZE; PHENOTYPIC PLASTICITY; NEPHILA-CLAVIPES; TOBACCO HORNWORM; LIFE-HISTORY; ARANEAE; TEMPERATURE AB Urbanization poses serious extinction risks, yet some species thrive in urban environments. This may be due to a pronounced developmental plasticity in these taxa, since phenotypically, plastic organisms may better adjust to unpredictable urban food resources. We studied phenotypic plasticity in Nuctenea umbratica, a common European forest and urban vegetation spider. We subjected spiderlings to low (LF), medium (MF) and high (HF) food treatments and documented their growth and developmental trajectories into adulthood. Spiders from the three treatments had comparable numbers of instars and growth ratios, but differed in developmental periods. Longest developing LF spiders (a (TM) EuroaEuro parts per thousand= 390, a (TM),aEuro parts per thousand= 320 days) had the smallest adults, but MF (a (TM) EuroaEuro parts per thousand= 300, a (TM),aEuro parts per thousand= 240 days) and HF (a (TM) EuroaEuro parts per thousand= 240, a (TM),aEuro parts per thousand= 210 days) spiders reached comparable adult sizes through shorter development. While males and females had comparable instar numbers, females had longer development, higher growth ratios, adult sizes and mass; and while males adjusted their moulting to food availability, female moulting depended on specific mass, not food treatment. We discussed the patterns of Nuctenea sex-specific development and compared our results with published data on two other Holarctic urban colonizers (Larinioides sclopetarius, Zygiella x-notata) exhibiting high plasticity and fast generation turn-over. We conclude that despite relatively unconstrained developmental time in the laboratory enabling Nuctenea to achieve maximal mass and size-main female fitness proxies-their relatively fixed growth ratio and long generation turn-over may explain their lower success in urban environments. C1 [Kralj-Fiser, Simona; Celik, Tatjana; Lokovsek, Tjasa; Kuntner, Matjaz] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, SI-1001 Ljubljana, Slovenia. [Kralj-Fiser, Simona] Univ Primorska, Fac Math Nat Sci & Informat Technol, SI-6000 Koper, Slovenia. [Suen, Klavdija] Univ Ljubljana, Biotech Fac, SI-1000 Ljubljana, Slovenia. [Siling, Rebeka] Inst Water Republ Slovenia, SI-1000 Ljubljana, Slovenia. [Kuntner, Matjaz] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Ctr Behav Ecol & Evolut, Wuhan 430062, Hubei, Peoples R China. RP Kralj-Fiser, S (reprint author), Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Novi Trg 2,POB 306, SI-1001 Ljubljana, Slovenia. EM simonakf@gmail.com FU Slovenian Research Agency [Z1-4194, P1-0236] FX This work was funded by the Slovenian Research Agency (grants Z1-4194 and P1-0236). NR 67 TC 0 Z9 0 U1 3 U2 25 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 EI 1432-1904 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD JUL PY 2014 VL 101 IS 7 BP 565 EP 575 DI 10.1007/s00114-014-1194-y PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AL3BC UT WOS:000338998900006 PM 24898706 ER PT J AU Baber, O Slot, M Celis, G Kitajima, K AF Baber, Ori Slot, Martijn Celis, Gerardo Kitajima, Kaoru TI Diel patterns of leaf carbohydrate concentrations differ between seedlings and mature trees of two sympatric oak species SO BOTANY-BOTANIQUE LA English DT Article DE carbohydrate dynamics; gas exchange; Quercus virginiana; Quercus hemisphaerica; plant ontogeny ID QUERCUS-VIRGINIANA; GAS-EXCHANGE; PLANT-GROWTH; CO2; MORTALITY; STORAGE; LEAVES; VOLUME AB A fundamental aspect of the carbon cycle is the exchange of carbon between plants and the atmosphere. It is, therefore, important to understand factors that affect differences in gas exchange and carbon balance within and among species. Concentrations of nonstructural carbohydrates are often used as a proxy for carbon balance. We determined diel patterns of leaf carbohydrate concentrations in relation to irradiance (sun vs. shade) in seedlings and mature trees of two sympatric oak species (Quercus virginiana Mill. and Quercus hemisphaerica Bartram ex Willd.). For seedlings, we also measured leaf gas exchange. Higher sun exposure significantly increased photosynthesis and carbohydrate concentrations in both species. Carbohydrate concentrations of seedling leaves showed strong diel fluctuations, whereas concentrations in mature tree leaves did not. This contrast might be attributed to faster carbohydrate export from leaves of mature trees. The difference in sink strength between seedlings and adults may be related to the decreasing ratio of leaf mass to plant mass with ontogeny, increasing the demand for carbohydrates per unit leaf mass. Seedlings and mature trees are clearly functionally different and care must be taken when extrapolating results from seedling experiments to mature trees. C1 [Baber, Ori; Slot, Martijn; Celis, Gerardo; Kitajima, Kaoru] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Slot, Martijn; Kitajima, Kaoru] Smithsonian Trop Res Inst, Balboa, Panama. [Kitajima, Kaoru] Kyoto Univ, Grad Sch Agr, Kyoto, Japan. RP Slot, M (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM martijnslot78@gmail.com OI Celis, Gerardo/0000-0003-1265-4063 NR 29 TC 4 Z9 4 U1 0 U2 16 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 1916-2790 EI 1916-2804 J9 BOTANY JI Botany PD JUL PY 2014 VL 92 IS 7 BP 535 EP 540 DI 10.1139/cjb-2014-0032 PG 6 WC Plant Sciences SC Plant Sciences GA AL0SS UT WOS:000338837700008 ER PT J AU Maragkoudakis, A Zezas, A Ashby, MLN Willner, SP AF Maragkoudakis, A. Zezas, A. Ashby, M. L. N. Willner, S. P. TI Aperture effects on spectroscopic galaxy activity classification SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: nuclei; galaxies: Seyfert; galaxies: starburst ID DIGITAL SKY SURVEY; H-II REGIONS; GALACTIC NUCLEI; SEMIEMPIRICAL ANALYSIS; HOST GALAXIES; PARAMETERS; SAMPLE AB Activity classification of galaxies based on long-slit and fibre spectroscopy can be strongly influenced by aperture effects. Here, we investigate how activity classification for 14 nearby galaxies depends on the proportion of the host galaxy's light that is included in the aperture. We use both observed long-slit spectra and simulated elliptical-aperture spectra of different sizes. The degree of change varies with galaxy morphology and nuclear activity type. Starlight removal techniques can mitigate but not remove the effect of host galaxy contamination in the nuclear aperture. Galaxies with extranuclear star formation can show higher [O iii] lambda 5007/H beta ratios with increasing aperture, in contrast to the naive expectation that integrated light will only dilute the nuclear emission lines. We calculate the mean dispersion for the diagnostic line ratios used in the standard BPT diagrams with respect to the central aperture of spectral extraction to obtain an estimate of the uncertainties resulting from aperture effects. C1 [Maragkoudakis, A.; Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Maragkoudakis, A.; Zezas, A.; Ashby, M. L. N.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zezas, A.] Fdn Res & Technol Hellas FORTH, Iraklion 71003, Greece. RP Maragkoudakis, A (reprint author), Univ Crete, Dept Phys, Iraklion 71003, Greece. EM amarag@physics.uoc.gr RI Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X FU 'Maria Michail Manasaki' bequest fellowship; HST [AR-12621-01-A]; NASA [NNX12AN05G]; Chandra [AR1-12011X]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science FX This work was supported by a 'Maria Michail Manasaki' bequest fellowship. AM acknowledges partial support by HST grant AR-12621-01-A. AZ acknowledges partial support by NASA grant NNX12AN05G, and Chandra grant AR1-12011X. We would like to thank the referee for his/her useful comments and suggestions which have improved the clarity of this paper. We also thank observers P. Berlind and M. Calkins for performing the FLWO observations. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, 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 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 29 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 JUL 1 PY 2014 VL 441 IS 3 BP 2296 EP 2308 DI 10.1093/mnras/stu634 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RE UT WOS:000338763600037 ER PT J AU Brorby, M Kaaret, P Prestwich, A AF Brorby, M. Kaaret, P. Prestwich, A. TI X-ray binary formation in low-metallicity blue compact dwarf galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: dwarf; galaxies: star formation; X-rays: galaxies ID STAR-FORMING GALAXIES; METAL-POOR GALAXIES; PRIMORDIAL ABUNDANCE; LUMINOSITY FUNCTIONS; FORMATION RATES; EMISSION; CLUSTERS; UNIVERSE; DISPLACEMENT; EVOLUTION AB X-rays from binaries in small, metal-deficient galaxies may have contributed significantly to the heating and reionization of the early Universe. We investigate this claim by studying blue compact dwarfs (BCDs) as local analogues to these early galaxies. We constrain the relation of the X-ray luminosity function (XLF) to the star formation rate (SFR) using a Bayesian approach applied to a sample of 25 BCDs. The functional form of the XLF is fixed to that found for near-solar metallicity galaxies and is used to find the probability distribution of the normalization that relates X-ray luminosity to SFR. Our results suggest that the XLF normalization for low-metallicity BCDs (12+log(O/H) < 7.7) is not consistent with the XLF normalization for galaxies with near-solar metallicities, at a confidence level 1-5 x 10(- 6). The XLF normalization for the BCDs is found to be 14.5 +/- 4.8 (M-circle dot(-1) yr), a factor of 9.7 +/- 3.2 higher than for near-solar metallicity galaxies. Simultaneous determination of the XLF normalization and power-law index result in estimates of q = 21.2(8.8)(+12.2) (M-circle dot(-1) yr) and alpha = 1.89(-0.30)(+0.41), respectively. Our results suggest a significant enhancement in the population of high-mass X-ray binaries in BCDs compared to the near-solar metallicity galaxies. This suggests that X-ray binaries could have been a significant source of heating in the early Universe. C1 [Brorby, M.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Prestwich, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. 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 through Chandra Award [GO0-11103X]; National Aeronautics Space Administration [NAS8-03060] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO0-11103X 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.; 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 research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 34 TC 22 Z9 22 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 JUL 1 PY 2014 VL 441 IS 3 BP 2346 EP 2353 DI 10.1093/mnras/stu736 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RE UT WOS:000338763600041 ER PT J AU Vidotto, AA Gregory, SG Jardine, M Donati, JF Petit, P Morin, J Folsom, CP Bouvier, J Cameron, AC Hussain, G Marsden, S Waite, IA Fares, R Jeffers, S do Nascimento, JD AF Vidotto, A. A. Gregory, S. G. Jardine, M. Donati, J. F. Petit, P. Morin, J. Folsom, C. P. Bouvier, J. Cameron, A. C. Hussain, G. Marsden, S. Waite, I. A. Fares, R. Jeffers, S. do Nascimento, J. D. TI Stellar magnetism: empirical trends with age and rotation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: polarimetric; stars: activity; stars: evolution; stars: magnetic field; planetary systems; stars: rotation ID PRE-MAIN-SEQUENCE; X-RAY-EMISSION; LOW-MASS STARS; T-TAURI STARS; SUN-LIKE STARS; ORION NEBULA CLUSTER; SOLAR-TYPE STARS; HIGH-RESOLUTION SPECTROSCOPY; LITHIUM DEPLETION; MAGNETOSPHERIC ACCRETION AB We investigate how the observed large-scale surface magnetic fields of low-mass stars (similar to 0.1-2 M-aS (TM)), reconstructed through Zeeman-Doppler imaging, vary with age t, rotation and X-ray emission. Our sample consists of 104 magnetic maps of 73 stars, from accreting pre-main sequence to main-sequence objects (1 Myr a parts per thousand(2) t a parts per thousand(2) 10 Gyr). For non-accreting dwarfs we empirically find that the unsigned average large-scale surface field is related to age as t(-0.655 +/- 0.045). This relation has a similar dependence to that identified by Skumanich, used as the basis for gyrochronology. Likewise, our relation could be used as an age-dating method ('magnetochronology'). The trends with rotation we find for the large-scale stellar magnetism are consistent with the trends found from Zeeman broadening measurements (sensitive to large- and small-scale fields). These similarities indicate that the fields recovered from both techniques are coupled to each other, suggesting that small- and large-scale fields could share the same dynamo field generation processes. For the accreting objects, fewer statistically significant relations are found, with one being a correlation between the unsigned magnetic flux and rotation period. We attribute this to a signature of star-disc interaction, rather than being driven by the dynamo. C1 [Vidotto, A. A.; Gregory, S. G.; Jardine, M.; Cameron, A. C.; Fares, R.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Vidotto, A. A.] Univ Geneva, Observ Geneve, CH-1290 Versoix, Switzerland. [Donati, J. F.; Petit, P.; Folsom, C. P.] Univ Toulouse, CNRS, LATT, F-31400 Toulouse, France. [Morin, J.] CNRS, LUPM, UMR5299, F-34095 Montpellier, France. [Morin, J.] Univ Montpellier 2, F-34095 Montpellier, France. [Bouvier, J.] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. [Hussain, G.] ESO, D-85748 Garching, Germany. [Marsden, S.; Waite, I. A.] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. [Jeffers, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [do Nascimento, J. D.] Univ Fed Rio Grande do Norte, Dep Fis Teor & Exp, BR-59072970 Natal, RN, Brazil. [do Nascimento, J. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vidotto, AA (reprint author), Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. EM aline.vidotto@unige.ch RI do Nascimento, Jose Dias/D-2416-2014; OI do Nascimento, Jose Dias/0000-0001-7804-2145; Petit, Pascal/0000-0001-7624-9222; Morin, Julien/0000-0002-4996-6901; Gregory, Scott/0000-0003-3674-5568; Vidotto, Aline/0000-0001-5371-2675; Marsden, Stephen/0000-0001-5522-8887 FU Royal Astronomical Society Fellowship; Swiss National Science Foundation via an Ambizione Fellowship; Science and Technology Facilities Council (STFC) via an Ernest Rutherford Fellowship [ST/J003255/1]; RF via a consolidated grant [ST/J001651/1]; ANR [Blanc SIMI5-6 020 01] FX AAV acknowledges support from a Royal Astronomical Society Fellowship and from the Swiss National Science Foundation via an Ambizione Fellowship. SGG acknowledges support from the Science and Technology Facilities Council (STFC) via an Ernest Rutherford Fellowship [ST/J003255/1] and RF via a consolidated grant [ST/J001651/1]. JB, PP and CPF acknowledge support from the ANR 2011 Blanc SIMI5-6 020 01 'Toupies: Towards understanding the spin evolution of stars' (http://ipag.osug.fr/Anr_Toupies/). AAV would like to thank Professor Keith Horne and Dr Kate Rowlands for advice in the statistical analysis. NSO/Kitt Peak data used here are produced cooperatively by NSF/NOAO, NASA/GSFC and NOAA/SEL. Partly based on Rotation periods are usually well constrained in the literature. In light of that and that errors are significantly larger for ages, magnetic fields and X-ray luminosities, we have neglected errors in rotation periods. NR 141 TC 58 Z9 58 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2014 VL 441 IS 3 BP 2361 EP 2374 DI 10.1093/mnras/stu728 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RE UT WOS:000338763600043 ER PT J AU Guo, H Zheng, Z Zehavi, I Xu, HJ Eisenstein, DJ Weinberg, DH Bahcall, NA Berlind, AA Comparat, J McBride, CK Ross, AJ Schneider, DP Skibba, RA Swanson, MEC Tinker, JL Tojeiro, R Wake, DA AF Guo, Hong Zheng, Zheng Zehavi, Idit Xu, Haojie Eisenstein, Daniel J. Weinberg, David H. Bahcall, Neta A. Berlind, Andreas A. Comparat, Johan McBride, Cameron K. Ross, Ashley J. Schneider, Donald P. Skibba, Ramin A. Swanson, Molly E. C. Tinker, Jeremy L. Tojeiro, Rita Wake, David A. TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: modelling of the luminosity and colour dependence in the Data Release 10 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: distances and redshifts; galaxies: haloes; galaxies: statistics; cosmology: observations; cosmology: theory; large-scale structure of Universe ID DIGITAL SKY SURVEY; HALO OCCUPATION DISTRIBUTION; 3-POINT CORRELATION-FUNCTION; VLT DEEP SURVEY; RED GALAXIES; REDSHIFT SURVEY; DARK-MATTER; STELLAR MASS; REAL-SPACE; PHOTOMETRIC REDSHIFTS AB We investigate the luminosity and colour dependence of clustering of CMASS galaxies in the Sloan Digital Sky Survey-III Baryon Oscillation Spectroscopic Survey Data Release 10, focusing on projected correlation functions of well-defined samples extracted from the full catalogue of similar to 540 000 galaxies at z similar to 0.5 covering about 6500 deg(2). The halo occupation distribution framework is adopted to model the measurements on small and intermediate scales (from 0.02 to 60 h(-1) Mpc), infer the connection of galaxies to dark matter haloes and interpret the observed trends. We find that luminous red galaxies in CMASS reside in massive haloes of mass M similar to 10(13)-10(14) h(-1) M-aS (TM) and more luminous galaxies are more clustered and hosted by more massive haloes. The strong small-scale clustering requires a fraction of these galaxies to be satellites in massive haloes, with the fraction at the level of 5-8 per cent and decreasing with luminosity. The characteristic mass of a halo hosting on average one satellite galaxy above a luminosity threshold is about a factor of 8.7 larger than that of a halo hosting a central galaxy above the same threshold. At a fixed luminosity, progressively redder galaxies are more strongly clustered on small scales, which can be explained by having a larger fraction of these galaxies in the form of satellites in massive haloes. Our clustering measurements on scales below 0.4 h(-1) Mpc allow us to study the small-scale spatial distribution of satellites inside haloes. While the clustering of luminosity-threshold samples can be well described by a Navarro-Frenk-White profile, that of the reddest galaxies prefers a steeper or more concentrated profile. Finally, we also use galaxy samples of constant number density at different redshifts to study the evolution of luminous red galaxies, and find the clustering to be consistent with passive evolution in the redshift range of 0.5 a parts per thousand(2) z a parts per thousand(2) 0.6. C1 [Guo, Hong; Zheng, Zheng; Xu, Haojie] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Guo, Hong; Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Eisenstein, Daniel J.; McBride, Cameron K.; Swanson, Molly E. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Weinberg, David H.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Bahcall, Neta A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08540 USA. [Berlind, Andreas A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Comparat, Johan] Aix Marseille Univ, CNRS, LAM, UMR 7326, Aix En Provence, France. [Ross, Ashley J.; Tojeiro, Rita] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Skibba, Ramin A.] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA. [Tinker, Jeremy L.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Wake, David A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Wake, David A.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. RP Guo, H (reprint author), Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. EM hong.guo@utah.edu RI Guo, Hong/J-5797-2015 OI Guo, Hong/0000-0003-4936-8247 FU NSF [AST-0907947, AST-1208891]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX We thank Yipeng Jing for kindly providing the simulations used in this paper. We thank Douglas F. Watson for helpful discussions and the anonymous referee for useful comments which improved the presentation of this paper. HG, ZZ, and IZ were supported by NSF grant AST-0907947. ZZ was partially supported by NSF grant AST-1208891.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 102 TC 28 Z9 28 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 JUL 1 PY 2014 VL 441 IS 3 BP 2398 EP 2413 DI 10.1093/mnras/stu763 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RE UT WOS:000338763600047 ER PT J AU Hirsch, B Martinez, D Kurten, EL Brown, DD Carson, WP AF Hirsch, Ben T. Martinez, Daniel Kurten, Erin L. Brown, Danielle D. Carson, Walter P. TI Mammalian Insectivores Exert Top-Down Effects on Azteca Ants SO BIOTROPICA LA English DT Article DE anti-predatory defenses; Azteca; BCI; indirect predation effects; tamandua; top-down effects; trophic interactions ID OCELOT LEOPARDUS-PARDALIS; BARRO-COLORADO ISLAND; JAGUAR PANTHERA-ONCA; PUMA PUMA-CONCOLOR; COSTA-RICA; TROPICAL FOREST; TERMITES NASUTITERMES; ANTEATERS EDENTATA; FELIS-PARDALIS; CAMERA TRAPS AB Insectivorous mammals are hypothesized to reduce the abundance of their insect prey. Using a 14-yr mammal exclusion experiment, we demonstrate for the first time that a widespread and abundant Neotropical mammalian insectivore (Tamandua: Tamandua mexicana) reduced Azteca ant abundance. Azteca ant nests inside mammal exclosures were significantly larger than nests in control plots, where tamanduas were more abundant. These top-down effects were caused not only by direct consumption, but also through non-trophic direct effects, specifically nest damage. In contrast, tamanduas appeared to exert no significant top-down effect on termite prey, which have strong chemical defenses. Our results are consistent with theory that strong defenses against predation can mitigate the top-down effects of predators on some prey species. We argue that predicting the degree of top-down effects caused by predators requires both a quantitative knowledge of prey choice and an understanding of the anti-predator defenses of prey. C1 [Hirsch, Ben T.] Univ Florida, Gainesville, FL 32611 USA. [Hirsch, Ben T.; Martinez, Daniel] Smithsonian Trop Res Inst, Unit 9100, Dpo Aa 340029898, Panama. [Kurten, Erin L.] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Brown, Danielle D.] Western Kentucky Univ, Dept Biol, Bowling Green, KY 42101 USA. [Carson, Walter P.] Univ Pittsburgh, Dept Biol Sci, Pittsburgh, PA 15260 USA. RP Hirsch, B (reprint author), Univ Florida, POB 110430,110 Newins Ziegler Hall, Gainesville, FL 32611 USA. EM hirschb@si.edu FU NSF [DEB-9527729, DEB-0212054]; National Geographic/Waitt grant [W3-08]; Theresa Heinz Environmental Scholars program; NSF; STRI short term fellowship; Max Planck Institute for Ornithology FX We thank Lee Dyer, Peter Morin, and Jonathan Pruitt for helpful comments to an earlier version of this article. We thank Susan Rebellon, Ana Patricia Calderon, Santiago Escobar, and Jose-Alejandro Ramirez for field assistance, and Steve Yanoviak for valuable advice concerning invertebrate sampling. This research was funded by NSF Grants (DEB-9527729 and DEB-0212054) to WPC, a National Geographic/Waitt grant (W3-08) to BTH, a Theresa Heinz Environmental Scholars program grant to ELK, a NSF predoctoral grant and STRI short term fellowship to DDB. We also thank Roland Kays, Martin Wikelski, and the Max Planck Institute for Ornithology for materials and support. NR 71 TC 0 Z9 0 U1 5 U2 30 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 EI 1744-7429 J9 BIOTROPICA JI Biotropica PD JUL PY 2014 VL 46 IS 4 BP 489 EP 494 DI 10.1111/btp.12128 PG 6 WC Ecology SC Environmental Sciences & Ecology GA AK9SD UT WOS:000338766100014 ER PT J AU Kryukova, E Megeath, ST Hora, JL Gutermuth, RA Bontemps, S Kraemer, K Hennemann, M Schneider, N Smith, HA Motte, F AF Kryukova, E. Megeath, S. T. Hora, J. L. Gutermuth, R. A. Bontemps, S. Kraemer, K. Hennemann, M. Schneider, N. Smith, Howard A. Motte, F. TI THE DEPENDENCE OF PROTOSTELLAR LUMINOSITY ON ENVIRONMENT IN THE CYGNUS-X STAR-FORMING COMPLEX SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: stars; stars: formation; stars: luminosity function; mass function; stars: protostars ID YOUNG STELLAR OBJECTS; INITIAL MASS FUNCTION; NEARBY MOLECULAR CLOUDS; SPITZER-SPACE-TELESCOPE; RHO-OPHIUCHI CLOUD; ARRAY CAMERA IRAC; EMBEDDED-CLUSTER; POPULATION; REGION; ORION AB The Cygnus-X star-forming complex is one of the most active regions of low- and high-mass star formation within 2 kpc of the Sun. Using mid-infrared photometry from the IRAC and MIPS Spitzer Cygnus-X Legacy Survey, we have identified over 1800 protostar candidates. We compare the protostellar luminosity functions of two regions within Cygnus-X: CygX-South and CygX-North. These two clouds show distinctly different morphologies suggestive of dissimilar star-forming environments. We find the luminosity functions of these two regions are statistically different. Furthermore, we compare the luminosity functions of protostars found in regions of high and low stellar density within Cygnus-X and find that the luminosity function in regions of high stellar density is biased to higher luminosities. In total, these observations provide further evidence that the luminosities of protostars depend on their natal environment. We discuss the implications this dependence has for the star formation process. C1 [Kryukova, E.; Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Ritter Astrophys Observ, Toledo, OH 43606 USA. [Hora, J. L.; Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gutermuth, R. A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Bontemps, S.; Schneider, N.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Bontemps, S.; Schneider, N.] CNRS, LAB, UMR 5804, F-33270 Floirac, France. [Kraemer, K.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA. [Hennemann, M.; Motte, F.] CEA IRFU CNRS INSU Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM, F-91191 Gif Sur Yvette, France. RP Kryukova, E (reprint author), Univ Toledo, Dept Phys & Astron, Ritter Astrophys Observ, Toledo, OH 43606 USA. EM megeath@physics.utoledo.edu OI Kraemer, Kathleen/0000-0002-2626-7155 FU NASA [NNX12AI55G]; National Aeronautics and Space Administration; National Science Foundation; project "STARFICH" [ANR-11-BS56-010] FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for the work of S.T.M., E.K., R.A.G., J.H., and K.K. was provided by NASA through an award issued by JPL/Caltech. H.A.S. acknowledges partial support for this work from NASA grant NNX12AI55G. 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. N.S. and S.B. acknowledge support by the ANR-11-BS56-010 project "STARFICH" NR 65 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUL PY 2014 VL 148 IS 1 AR 11 DI 10.1088/0004-6256/148/1/11 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK4PF UT WOS:000338405900011 ER PT J AU Rodney, SA Riess, AG Strolger, LG Dahlen, T Graur, O Casertano, S Dickinson, ME Ferguson, HC Garnavich, P Hayden, B Jha, SW Jones, DO Kirshner, RP Koekemoer, AM McCully, C Mobasher, B Patel, B Weiner, BJ Cenko, SB Clubb, KI Cooper, M Filippenko, AV Frederiksen, TF Hjorth, J Leibundgut, B Matheson, T Nayyeri, H Penner, K Trump, J Silverman, JM Vivian, U Bostroem, KA Challis, P Rajan, A Wolff, S Faber, SM Grogin, NA Kocevski, D AF Rodney, Steven A. Riess, Adam G. Strolger, Louis-Gregory Dahlen, Tomas Graur, Or Casertano, Stefano Dickinson, Mark E. Ferguson, Henry C. Garnavich, Peter Hayden, Brian Jha, Saurabh W. Jones, David O. Kirshner, Robert P. Koekemoer, Anton M. McCully, Curtis Mobasher, Bahram Patel, Brandon Weiner, Benjamin J. Cenko, S. Bradley Clubb, Kelsey I. Cooper, Michael Filippenko, Alexei V. Frederiksen, Teddy F. Hjorth, Jens Leibundgut, Bruno Matheson, Thomas Nayyeri, Hooshang Penner, Kyle Trump, Jonathan Silverman, Jeffrey M. Vivian, U. Bostroem, K. Azalee Challis, Peter Rajan, Abhijith Wolff, Schuyler Faber, S. M. Grogin, Norman A. Kocevski, Dale TI TYPE Ia SUPERNOVA RATE MEASUREMENTS TO REDSHIFT 2.5 FROM CANDELS: SEARCHING FOR PROMPT EXPLOSIONS IN THE EARLY UNIVERSE SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: general; supernovae: general; surveys ID CORE-COLLAPSE SUPERNOVAE; DELAY-TIME DISTRIBUTION; ORIGINS DEEP SURVEY; DIGITAL SKY SURVEY; EXTRAGALACTIC LEGACY SURVEY; TELESCOPE ADVANCED CAMERA; GOODS-SOUTH FIELD; GAMMA-RAY BURSTS; II-P SUPERNOVAE; STAR-FORMATION AB dThe Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) was a multi-cycle treasury program on the Hubble Space Telescope (HST) that surveyed a total area of -0.25 deg2 with -900 HST orbits spread across five fields over three years. Within these survey images we discovered 65 supernovae (SNe) of all types, out to z 2.5. We classify -24 of these as Type Ia SNe (SNe Ia) based on host galaxy redshifts and SN photometry (supplemented by grism spectroscopy of six SNe). Here we present a measurement of the volumetric SN Ia rate as a function of redshift, reaching for the first time beyond z =- 2 and putting new constraints on SN Ia progenitor models. Our highest redshift bin includes detections of SNe that exploded when the universe was only -3 Gyr old and near the peak of the cosmic star formation history. This gives the CANDELS high redshift sample unique leverage for evaluating the fraction of SNe Ia that explode promptly after formation (<500 Myr). Combining the CANDELS rates with all available SN Ia rate measurements in the literature we find that this prompt SN Ia fraction is fp = 0.53st=sg.Zc6', consistent with a delay time distribution that follows a simple t-1 power law for all times t > 40 Myr. However, mild tension is apparent between ground-based low-z surveys and space-based high-z surveys. In both CANDELS and the sister HST program CLASH (Cluster Lensing And Supernova Survey with Hubble), we find a low rate of SNe Ia at z > 1. This could be a hint that prompt progenitors are in fact relatively rare, accounting for only 20% of all SN Ia explosions-though further analysis and larger samples will be needed to examine that suggestion. Key words: infrared: general - supernovae: C1 [Rodney, Steven A.; Riess, Adam G.; Graur, Or; Jones, David O.; Wolff, Schuyler] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Riess, Adam G.; Strolger, Louis-Gregory; Dahlen, Tomas; Casertano, Stefano; Ferguson, Henry C.; Koekemoer, Anton M.; Bostroem, K. Azalee; Grogin, Norman A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Graur, Or] Tel Aviv Univ, Dept Astrophys, IL-69978 Tel Aviv, Israel. [Graur, Or] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Dickinson, Mark E.; Matheson, Thomas] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Garnavich, Peter] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Hayden, Brian] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Jha, Saurabh W.; McCully, Curtis; Patel, Brandon] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Kirshner, Robert P.; Challis, Peter] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mobasher, Bahram; Nayyeri, Hooshang; Vivian, U.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Weiner, Benjamin J.; Penner, Kyle] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Clubb, Kelsey I.; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cooper, Michael] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Frederiksen, Teddy F.; Hjorth, Jens] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Leibundgut, Bruno] European So Observ, Garching, Germany. [Leibundgut, Bruno] Tech Univ Munich, D-80290 Munich, Germany. [Trump, Jonathan] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Silverman, Jeffrey M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Rajan, Abhijith] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Faber, S. M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 92064 USA. [Kocevski, Dale] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. RP Rodney, SA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RI Hjorth, Jens/M-5787-2014; OI Hjorth, Jens/0000-0002-4571-2306; Graur, Or/0000-0002-4391-6137; Koekemoer, Anton/0000-0002-6610-2048 NR 117 TC 28 Z9 28 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUL PY 2014 VL 148 IS 1 AR 13 DI 10.1088/0004-6256/148/1/13 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK4PF UT WOS:000338405900013 ER PT J AU Mommert, M Farnocchia, D Hora, JL Chesley, SR Trilling, DE Chodas, PW Mueller, M Harris, AW Smith, HA Fazio, GG AF Mommert, M. Farnocchia, D. Hora, J. L. Chesley, S. R. Trilling, D. E. Chodas, P. W. Mueller, M. Harris, A. W. Smith, H. A. Fazio, G. G. TI PHYSICAL PROPERTIES OF NEAR-EARTH ASTEROID 2011 MD SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE infrared: planetary systems; minor planets, asteroids: individual (2011 MD) ID SPITZER-SPACE-TELESCOPE; RADIATION PRESSURE; YARKOVSKY; FRAGMENTS; NEOWISE AB We report on observations of near-Earth asteroid 2011 MD with the Spitzer Space Telescope. We have spent 19.9 hr of observing time with channel 2 (4.5 mu m) of the Infrared Array Camera and detected the target within the 2 sigma positional uncertainty ellipse. Using an asteroid thermophysical model and a model of nongravitational forces acting upon the object, we constrain the physical properties of 2011 MD, based on the measured flux density and available astrometry data. We estimate 2011 MD to be (6(-2)(+4) ) m in diameter with a geometric albedo of 0.3(-0.2)(+0.4) (uncertainties are 1 sigma). We find the asteroid's most probable bulk density to be (1.1(-0.5)(+0.7) ) g cm(-3), which implies a total mass of (50-350) t and a macroporosity of >= 65%, assuming a material bulk density typical of non-primitive meteorite materials. A high degree of macroporosity suggests that 2011 MD is a rubble-pile asteroid, the rotation of which is more likely to be retrograde than prograde. C1 [Mommert, M.; Trilling, D. E.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Farnocchia, D.; Chesley, S. R.; Chodas, P. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hora, J. L.; Smith, H. A.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mueller, M.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Harris, A. W.] DLR Inst Planetary Res, D-12489 Berlin, Germany. RP Mommert, M (reprint author), No Arizona Univ, Dept Phys & Astron, POB 6010, Flagstaff, AZ 86011 USA. OI Mueller, Michael/0000-0003-3217-5385; Chesley, Steven/0000-0003-3240-6497 FU Arizona's Technology and Research Initiative Fund; Jet Propulsion Laboratory RSA [1367413] FX Some of the computational analyses were run on Northern Arizona University's monsoon computing cluster, funded by Arizona's Technology and Research Initiative Fund. M. Mommert thanks P. Penteado for support on the computational aspects of this work. We thank J. Lee and T. J. Martin-Mur for providing information on the Spitzer ephemeris uncertainties. We thank an anonymous referee for useful suggestions that led to the improvement of this manuscript. The work of D. Farnocchia, S. Chesley, and P. W. Chodas was conducted at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. J. L. Hora and H. A. Smith acknowledge partial support from Jet Propulsion Laboratory RSA #1367413. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 23 TC 6 Z9 6 U1 1 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 JUL 1 PY 2014 VL 789 IS 1 AR L22 DI 10.1088/2041-8205/789/1/L22 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK6UR UT WOS:000338563300022 ER PT J AU Dainou, K Mahy, G Duminil, J Dick, CW Doucet, JL Donkpegan, ASL Pluijgers, M Sinsin, B Lejeune, P Hardy, OJ AF Dainou, K. Mahy, G. Duminil, J. Dick, C. W. Doucet, J-L Donkpegan, A. S. L. Pluijgers, M. Sinsin, B. Lejeune, P. Hardy, O. J. TI Speciation slowing down in widespread and long-living tree taxa: insights from the tropical timber tree genus Milicia (Moraceae) SO HEREDITY LA English DT Article DE Milicia; speciation; phylogeny; phylogeography; Tertiary diversification ID POPULATION-STRUCTURE; EXCELSA MORACEAE; COMPUTER-PROGRAM; PHYLOGENETIC-RELATIONSHIPS; GENETIC DIFFERENTIATION; SPECIES DELIMITATION; POLLINATION SYSTEMS; VEGETATIVE TRAITS; RAIN-FOREST; AFRICA AB The long generation time and large effective size of widespread forest tree species can result in slow evolutionary rate and incomplete lineage sorting, complicating species delimitation. We addressed this issue with the African timber tree genus Milicia that comprises two morphologically similar and often confounded species: M. excelsa, widespread from West to East Africa, and M. regia, endemic to West Africa. We combined information from nuclear microsatellites (nSSRs), nuclear and plastid DNA sequences, and morphological systematics to identify significant evolutionary units and infer their evolutionary and biogeographical history. We detected five geographically coherent genetic clusters using nSSRs and three levels of genetic differentiation. First, one West African cluster matched perfectly with the morphospecies M. regia that formed a monophyletic clade at both DNA sequences. Second, a West African M. excelsa cluster formed a monophyletic group at plastid DNA and was more related to M. regia than to Central African M. excelsa, but shared many haplotypes with the latter at nuclear DNA. Third, three Central African clusters appeared little differentiated and shared most of their haplotypes. Although gene tree paraphyly could suggest a single species in Milicia following the phylogenetic species concept, the existence of mutual haplotypic exclusivity and nonadmixed genetic clusters in the contact area of the two taxa indicate strong reproductive isolation and, thus, two species following the biological species concept. Molecular dating of the first divergence events showed that speciation in Milicia is ancient (Tertiary), indicating that long-living tree taxa exhibiting genetic speciation may remain similar morphologically. C1 [Dainou, K.; Doucet, J-L; Donkpegan, A. S. L.; Pluijgers, M.] Univ Liege, Gembloux Agrobio Tech, Unit Forest & Nat Management, Lab Trop & Subtrop Forestry, B-5030 Gembloux, Belgium. [Dainou, K.; Sinsin, B.] Univ Abomey Calavi, Fac Agron Sci, Lab Appl Ecol, Cotonou, Benin. [Mahy, G.] Univ Liege, Gembloux Agrobio Tech, Biodivers & Landscape Unit, B-5030 Gembloux, Belgium. [Duminil, J.; Hardy, O. J.] Univ Libre Brussels, Fac Sci, Brussels, Belgium. [Duminil, J.] Subreg Off Cent Africa, Forest Genet Resources Programme, Biovers Int, Yaounde, Cameroon. [Dick, C. W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Dick, C. W.] Smithsonian Trop Res Inst, Gamboa, Panama. [Lejeune, P.] Univ Liege, Gembloux Agrobio Tech, Unit Forest & Nat Management, B-5030 Gembloux, Belgium. RP Dainou, K (reprint author), Univ Liege, Gembloux Agrobio Tech, Unit Forest & Nat Management, Lab Trop & Subtrop Forestry, 2 Passage Deportes, B-5030 Gembloux, Belgium. EM kdainou@gmail.com RI Dick, Christopher/A-8744-2008 FU Fund for Scientific Research of Belgium (FNRS) through grants FRFC [2.4.577.10]; FRFC [2.4.576.07] FX We thank the project PPR 10.000 (Gembloux Agro-Bio Tech; University of Liege), the Fonds Leopold III (asbl, Belgium), and the Fund for Scientific Research of Belgium (FNRS) through grants FRFC no. 2.4.577.10 and FRFC no. 2.4.576.07 for their financial support. We are indebted to David Monticelli, Lambert Y Kouadio, Guillaume Koffi, Bonaventure Sonke, Michel Baudoin, Shango Mutambue, Jean-Pierre Mate, Emilien Dubiez, Pierre Proces, Bertin Kasongo, Pat Stoffelen and Georges Mumbere for their various contributions. We also acknowledge the logging companies Pallisco, SFID, Wijma (Cameroon) and Precious Woods Gabon for facilitating field work, and the National Botanical Garden of Belgium (Meise) for permitting sample collection from herbaria. NR 73 TC 6 Z9 6 U1 3 U2 41 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0018-067X EI 1365-2540 J9 HEREDITY JI Heredity PD JUL PY 2014 VL 113 IS 1 BP 74 EP 85 DI 10.1038/hdy.2014.5 PG 12 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA AK3QK UT WOS:000338339600008 PM 24549110 ER PT J AU Cook-Patton, SC Weller, D Rick, TC Parker, JD AF Cook-Patton, Susan C. Weller, Daniel Rick, Torben C. Parker, John D. TI Ancient experiments: forest biodiversity and soil nutrients enhanced by Native American middens SO LANDSCAPE ECOLOGY LA English DT Article DE Land-use legacies; Shell middens; Crassostrea virginica; Forest diversity; Invasion; Nutrient addition; Calcium; Chesapeake Bay, Maryland, USA ID HISTORICAL LAND-USE; PLANT-COMMUNITIES; VASCULAR FLORA; SHELL MIDDENS; ECOSYSTEMS; LANDSCAPE; DIVERSITY; AMAZONIA; EARTHS; LAYER AB The legacy of ancient human practices can affect the diversity and structure of modern ecosystems. Here, we examined how prehistoric refuse dumps ("middens") impacted soil chemistry and plant community composition in forests along the Chesapeake Bay by collecting vegetational and soil nutrient data. The centuries- to millennia-old shell middens had elevated soil nutrients compared to adjacent sites, greater vegetative cover, especially of herb and grass species, and higher species richness. Not only are middens important archaeological resources, they also offer a remarkable opportunity to test ecological hypotheses about nutrient addition over very long time scales. We found no evidence, for example, that elevated nutrients enhanced invasion by non-native species as predicted by the fluctuating resource hypothesis. However, we did find that elevated nutrients shifted community structure from woody species to herbaceous species, as predicted by the structural carbon-nutrient hypothesis. These results highlight the long-lasting effects that humans can have on abiotic and biotic properties of the natural environment, and suggest the potential for modern patterns of species' distributions and abundances to reflect ancient human activities. C1 [Cook-Patton, Susan C.; Parker, John D.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Weller, Daniel] Cornell Univ, Ithaca, NY 14853 USA. [Rick, Torben C.] Smithsonian Inst, Program Human Ecol & Archaeobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Cook-Patton, SC (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM cook-pattons@si.edu RI Parker, John/F-9761-2010 OI Parker, John/0000-0002-3632-7625 FU Smithsonian Institution/SERC; National Museum of Natural History Small Grant; National Geographic Society FX The Smithsonian Institution/SERC supported this work with an internship to D. Weller and a fellowship to S. C. Cook-Patton. Funds from the National Museum of Natural History Small Grant (Rick) and the National Geographic Society (Rick) supported radiocarbon dating. We also thank Tuck Hines, Robert Aguilar, Allison Everett, Midge Kramer and researchers in the SERC Crab Lab who provided logistical support and advice. NR 48 TC 3 Z9 3 U1 1 U2 19 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0921-2973 EI 1572-9761 J9 LANDSCAPE ECOL JI Landsc. Ecol. PD JUL PY 2014 VL 29 IS 6 BP 979 EP 987 DI 10.1007/s10980-014-0033-z PG 9 WC Ecology; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA AK3NP UT WOS:000338331600005 ER PT J AU Cialdella, AM Sede, SM Romaschenko, K Peterson, PM Soreng, RJ Zuloaga, FO Morrone, O AF Cialdella, Ana M. Sede, Silvana M. Romaschenko, Konstantin Peterson, Paul M. Soreng, Robert J. Zuloaga, Fernando O. Morrone, O. TI Phylogeny of Nassella (Stipeae, Pooideae, Poaceae) Based on Analyses of Chloroplast and Nuclear Ribosomal DNA and Morphology SO SYSTEMATIC BOTANY LA English DT Article DE ETS; ITS; morphology; phylogeny; plastid DNA; Stipeae ID NONCODING REGIONS; SEQUENCE; GENUS; CHARACTERS; AMELICHLOA; GRAMINEAE; EVOLUTION; PLANTS; GENES; NRDNA AB The genus Nassella, as currently circumscribed, includes 116-117 American species. It is characterized by florets with a strongly convolute lemma, a conspicuous or inconspicuous crown, and a short palea. Using 53 species of Nassella and 22 outgroup species we conducted phylogenetic analyses to test the monophyly of Nassella and relationships among species. Two plastid (trnT-trnL and rpl32-trnL) and two nuclear ribosomal (ITS and ETS) regions and morphology were used. Our DNA data alone and combined with morphology showed Nassella to be paraphyletic with respect to a monophyletic Amelichloa. Two main clades were recovered: one with species of Nassella distributed in regions of high elevation from Mexico to northwestern Argentina and one composed of the remaining species of Nassella and those of Amelichloa. The latter is mainly concentrated in southern South America in a variety of habitats with generally lower elevation than the other clade. The monophyly of the close relative of Nassella, the South American genus Jarava s. s., was rejected. None of the groups previously circumscribed as subgenera of Stipa, that are now considered to be composed of species in Nassella, were recovered as monophyletic. The close phylogenetic relationship of Nassella and Amelichloa is supported by only one morphological synapomorphy: the lemma margins flat and strongly overlapping. C1 [Cialdella, Ana M.; Sede, Silvana M.; Zuloaga, Fernando O.; Morrone, O.] Inst Bot Darwinion, Buenos Aires, DF, Argentina. [Romaschenko, Konstantin; Peterson, Paul M.; Soreng, Robert J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Cialdella, AM (reprint author), Inst Bot Darwinion, Labarden 200,Casilla Correo 22,B1642HYD San Isidr, Buenos Aires, DF, Argentina. EM anacialdella@darwin.edu.ar RI Romaschenko, Konstantin/K-3096-2014 OI Romaschenko, Konstantin/0000-0002-7248-4193 FU CONICET [PIP 11220100100155]; ANPCyT [PICT 2010-1645]; National Geographic Society [4677-91, 7792-05, 8087-06, 8862-10]; Smithsonian Institution FX This research was supported by CONICET, grant PIP 11220100100155 and ANPCyT, grant PICT 2010-1645; the National Geographic Society, grants number 4677-91, 7792-05, 8087-06, and 8862-10; and the Smithsonian Institution. We are also thankful to the curators and staff of the herbaria mentioned in the text, who allowed the study of the specimens under their care. Finally, we thank the staff of the Darwinion, especially Mrs. Mariana Valente, who kindly helped us to compose Figs. 3 and 4. NR 54 TC 3 Z9 4 U1 1 U2 8 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 EI 1548-2324 J9 SYST BOT JI Syst. Bot. PD JUL-SEP PY 2014 VL 39 IS 3 BP 814 EP 828 DI 10.1600/036364414X681419 PG 15 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA AK4OY UT WOS:000338405200014 ER PT J AU Bulbul, E Markevitch, M Foster, A Smith, RK Loewenstein, M Randall, SW AF Bulbul, Esra Markevitch, Maxim Foster, Adam Smith, Randall K. Loewenstein, Michael Randall, Scott W. TI DETECTION OF AN UNIDENTIFIED EMISSION LINE IN THE STACKED X-RAY SPECTRUM OF GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; elementary particles; line: identification; neutrinos; X-rays: galaxies: clusters ID DWARF SPHEROIDAL GALAXY; XMM-NEWTON SPECTROSCOPY; DECAYING DARK-MATTER; STERILE NEUTRINOS; CHANDRA; SAMPLE; CONSTRAINTS; COSMOLOGY; MODEL; LIGHT AB We detect a weak unidentified emission line at E = (3.55-3.57) +/- 0.03 keV in a stacked XMM-Newton spectrum of 73 galaxy clusters spanning a redshift range 0.01-0.35. When the full sample is divided into three subsamples (Perseus, Centaurus+Ophiuchus+Coma, and all others), the line is seen at >3 sigma statistical significance in all three independent MOS spectra and the PN "all others" spectrum. It is also detected in the Chandra spectra of the Perseus Cluster. However, it is very weak and located within 50-110 eV of several known lines. The detection is at the limit of the current instrument capabilities. We argue that there should be no atomic transitions in thermal plasma at this energy. An intriguing possibility is the decay of sterile neutrino, a long-sought dark matter particle candidate. Assuming that all dark matter is in sterile neutrinos with m(s) = 2 E = 7.1 keV, our detection corresponds to a neutrino decay rate consistent with previous upper limits. However, based on the cluster masses and distances, the line in Perseus is much brighter than expected in this model, significantly deviating from other subsamples. This appears to be because of an anomalously bright line at E = 3.62 keV in Perseus, which could be an Ar XVII dielectronic recombination line, although its emissivity would have to be 30 times the expected value and physically difficult to understand. Another alternative is the above anomaly in the Ar line combined with the nearby 3.51 keV K line also exceeding expectation by a factor of 10-20. Confirmation with Astro-H will be critical to determine the nature of this new line. C1 [Bulbul, Esra; Foster, Adam; Smith, Randall K.; Randall, Scott W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bulbul, Esra; Loewenstein, Michael] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Bulbul, Esra; Loewenstein, Michael] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Markevitch, Maxim] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Loewenstein, Michael] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Bulbul, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ebulbul@cfa.harvard.edu OI Randall, Scott/0000-0002-3984-4337; Smith, Randall/0000-0003-4284-4167 FU Chandra grant [AR0-11020X, GO1-12104X]; NASA ADAP grant [NNX12AF44G]; Chandra X-ray Center through NASA [NAS8-03060]; Smithsonian Institution FX The authors thank Alexey Vikhlinin for extensive discussions, cross-checking the results, and spotting several errors; Douglas Finkbeiner and Serkan Cabi for useful discussions; Christine Jones, Signe Riemer-Sorensen, Alexander Kusenko, and the anonymous referee for useful comments on the draft; and Kevork Abazajian and Shunsaku Horiuchi for providing the limits from their M31 analysis. E.B. also thanks Adrian Batu Gerard for patiently waiting for the submission to be born. E.B. was supported in part by Chandra grant AR0-11020X and GO1-12104X. A.F. and R.S. were supported in part by NASA ADAP grant NNX12AF44G. S.W.R. was supported by the Chandra X-ray Center through NASA contract NAS8-03060 and the Smithsonian Institution. NR 69 TC 218 Z9 218 U1 2 U2 20 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2014 VL 789 IS 1 AR 13 DI 10.1088/0004-637X/789/1/13 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400013 ER PT J AU Dupree, AK Brickhouse, NS Cranmer, SR Berlind, P Strader, J Smith, GH AF Dupree, A. K. Brickhouse, N. S. Cranmer, S. R. Berlind, P. Strader, Jay Smith, Graeme H. TI STRUCTURE AND DYNAMICS OF THE ACCRETION PROCESS AND WIND IN TW Hya SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: individual (TW Hydrae); stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be; stars: winds, outflows ID POWERED STELLAR WINDS; BALMER LINE-PROFILES; MAIN-SEQUENCE STARS; KECK II TELESCOPE; IUE MEGA CAMPAIGN; X-RAY-EMISSION; TAURI STARS; MAGNETOSPHERIC ACCRETION; SPECTRAL VARIABILITY; ECHELLE SPECTROGRAPH AB Time-domain spectroscopy of the classical accreting T Tauri star, TW Hya, covering a decade and spanning the far UV to the near-infrared spectral regions can identify the radiation sources, the atmospheric structure produced by accretion, and properties of the stellar wind. On timescales from days to years, substantial changes occur in emission line profiles and line strengths. Our extensive time-domain spectroscopy suggests that the broad near-IR, optical, and far-uv emission lines, centered on the star, originate in a turbulent post-shock region and can undergo scattering by the overlying stellar wind as well as some absorption from infalling material. Stable absorption features appear in Ha, apparently caused by an accreting column silhouetted in the stellar wind. Inflow of material onto the star is revealed by the near-IR He I 10830 angstrom line, and its free-fall velocity correlates inversely with the strength of the post-shock emission, consistent with a dipole accretion model. However, the predictions of hydrogen line profiles based on accretion stream models are not well-matched by these observations. Evidence of an accelerating warm to hot stellar wind is shown by the near-IR He I line, and emission profiles of C II, C III, C IV, N V, and O VI. The outflow of material changes substantially in both speed and opacity in the yearly sampling of the near-IR He I line over a decade. Terminal outflow velocities that range from 200 km s(-1) to almost 400 km s(-1) in He I appear to be directly related to the amount of post-shock emission, giving evidence for an accretion-driven stellar wind. Calculations of the emission from realistic post-shock regions are needed. C1 [Dupree, A. K.; Brickhouse, N. S.; Cranmer, S. R.; Berlind, P.; Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Smith, Graeme H.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Berlind, P.] Fred L Whipple Observ, Amado, AZ USA. [Strader, Jay] Michigan State Univ, E Lansing, MI 48824 USA. RP Dupree, AK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Cranmer, Steven/0000-0002-3699-3134; Brickhouse, Nancy/0000-0002-8704-4473; Dupree, Andrea/0000-0002-8985-8489 FU NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX We thank the anonymous referee for his/her comments that improved the manuscript. The authors gratefully acknowledge the helpful support from Gemini-S astronomers, the staff at Magellan, and KECK II while acquiring these spectra. Observers at FLWO were a great help on short notice. This research has made use of NASA's Astrophysics Data System Bibliographic Services. Some of the data presented here was 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. We wish to extend special thanks to those of Hawaiian ancestry from whose sacred mountain of Mauna Kea we are privileged to conduct observations. Without their generous hospitality, the Keck results presented in this paper would not have been possible. NR 87 TC 5 Z9 5 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2014 VL 789 IS 1 AR 27 DI 10.1088/0004-637X/789/1/27 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400027 ER PT J AU Faesi, CM Lada, CJ Forbrich, J Menten, KM Bouy, H AF Faesi, Christopher M. Lada, Charles J. Forbrich, Jan Menten, Karl M. Bouy, Herve TI MOLECULAR CLOUD-SCALE STAR FORMATION IN NGC 300 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 300); galaxies: ISM; galaxies: star formation; H II regions; stars: formation ID CO-TO-H-2 CONVERSION FACTOR; MULTIBAND IMAGING PHOTOMETER; FORMATION RATE INDICATORS; SPIRAL-GALAXY NGC-300; GAS DEPLETION TIME; CO J=2-1 SURVEY; NEARBY GALAXIES; MILKY-WAY; FORMATION RATES; FORMATION LAW AB We present the results of a galaxy-wide study of molecular gas and star formation in a sample of 76 H II regions in the nearby spiral galaxy NGC 300. We have measured the molecular gas at 250 pc scales using pointed CO(J = 2-1) observations with the Atacama Pathfinder Experiment telescope. We detect CO in 42 of our targets, deriving molecular gas masses ranging from our sensitivity limit of similar to 10(5) M-circle dot to 7 x 10(5) M-circle dot. We find a clear decline in the CO detection rate with galactocentric distance, which we attribute primarily to the decreasing radial metallicity gradient in NGC 300. We combine Galaxy Evolution Explorer far-ultraviolet, Spitzer 24 mu m, and H alpha narrowband imaging to measure the star formation activity in our sample. We have developed a new direct modeling approach for computing star formation rates (SFRs) that utilizes these data and population synthesis models to derive the masses and ages of the young stellar clusters associated with each of our H II region targets. We find a characteristic gas depletion time of 230 Myr at 250 pc scales in NGC 300, more similar to the results obtained for Milky Way giant molecular clouds than the longer (>2 Gyr) global depletion times derived for entire galaxies and kiloparsec-sized regions within them. This difference is partially due to the fact that our study accounts for only the gas and stars within the youngest star-forming regions. We also note a large scatter in the NGC 300 SFR-molecular gas mass scaling relation that is furthermore consistent with the Milky Way cloud results. This scatter likely represents real differences in giant molecular cloud physical properties such as the dense gas fraction. C1 [Faesi, Christopher M.; Lada, Charles J.; Forbrich, Jan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Forbrich, Jan] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Menten, Karl M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Bouy, Herve] Ctr Astrobiol, INTA CSIC, Dept Astrofis, Villanueva Dela Canada 28691, Spain. RP Faesi, CM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Bouy, Herve/H-2913-2012 OI Bouy, Herve/0000-0002-7084-487X FU National Aeronautics and Space Administration; National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project [NCC5-626]; National Science Foundation Graduate Research Fellowship [DGE-1144152]; Spanish Ramon y Cajal fellowship program [RYC-2009-04497] FX This work is based in part on observations made with the Spitzer Space Telescope, obtained from the NASA/IPAC Infrared Science Archive, both of which are operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. 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 made use of Montage, funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology. Montage is maintained by the NASA/IPAC Infrared Science Archive. C.M.F acknowledges support from a National Science Foundation Graduate Research Fellowship under grant No. DGE-1144152. H. Bouy is funded by the Spanish Ramon y Cajal fellowship program number RYC-2009-04497. NR 78 TC 5 Z9 5 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2014 VL 789 IS 1 AR 81 DI 10.1088/0004-637X/789/1/81 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400081 ER PT J AU La Plante, P Battaglia, N Natarajan, A Peterson, JB Trac, H Cen, R Loeb, A AF La Plante, P. Battaglia, N. Natarajan, A. Peterson, J. B. Trac, H. Cen, R. Loeb, A. TI REIONIZATION ON LARGE SCALES. IV. PREDICTIONS FOR THE 21 cm SIGNAL INCORPORATING THE LIGHT CONE EFFECT SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; intergalactic medium; large-scale structure of universe; methods: numerical ID POWER SPECTRUM; HIGH-REDSHIFT; COSMIC REIONIZATION; 21-CM FLUCTUATIONS; CENTIMETER FLUCTUATIONS; HYDROGEN REIONIZATION; INTERGALACTIC MEDIUM; CLUSTERING WEDGES; EPOCH; SPACE AB We present predictions for the 21 cm brightness temperature power spectrum during the Epoch of Reionization (EoR). We discuss the implications of the "light cone" effect, which incorporates evolution of the neutral hydrogen fraction and 21 cm brightness temperature along the line of sight. Using a novel method calibrated against radiation-hydrodynamic simulations, we model the neutral hydrogen density field and 21 cm signal in large volumes (L = 2 Gpc h(-1)). The inclusion of the light cone effect leads to a relative decrease of about 50% in the 21 cm power spectrum on all scales. We also find that the effect is more prominent at the midpoint of reionization and later. The light cone effect can also introduce an anisotropy along the line of sight. By decomposing the 3D power spectrum into components perpendicular to and along the line of sight, we find that in our fiducial reionization model, there is no significant anisotropy. However, parallel modes can contribute up to 40% more power for shorter reionization scenarios. The scales on which the light cone effect is relevant are comparable to scales where one measures the baryon acoustic oscillation. We argue that due to its large comoving scale and introduction of anisotropy, the light cone effect is important when considering redshift space distortions and future application to the Alcock-Paczynski test for the determination of cosmological parameters. C1 [La Plante, P.; Battaglia, N.; Natarajan, A.; Peterson, J. B.; Trac, H.] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Natarajan, A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Natarajan, A.] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr, Pittsburgh, PA 15260 USA. [Cen, R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Loeb, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP La Plante, P (reprint author), Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. EM plaplant@andrew.cmu.edu RI Trac, Hy/N-8838-2014; Peterson, Jeffrey/O-4794-2014; OI Trac, Hy/0000-0001-6778-3861; Peterson, Jeffrey/0000-0003-1340-818X; La Plante, Paul/0000-0002-4693-0102 FU McWilliams Center for Cosmology Postdoctoral Fellowship; NSF [AST-1009615, AST-1109730, AST-1312991, AST-1108700, AST-0907890]; NASA [NNX12AF91G, NNX08AL43G, NNA09DB30A] FX N.B. and A.N. are supported by a McWilliams Center for Cosmology Postdoctoral Fellowship made possible by Bruce and Astrid McWilliams. A.N. and J.B.P. acknowledge funding from NSF grant AST-1009615. We thank A. Parsons for supplying the data from PAPER and G. Paciga for supplying the data from GMRT. H. T. is supported in part by NSF grants AST-1109730 and AST-1312991. R. C. is supported in part by NSF grant AST-1108700 and NASA grant NNX12AF91G. A. L. is supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A. The simulations were performed at the Pittsburgh Supercomputing Center (PSC) and the Princeton Institute for Computational Science and Engineering (PICSciE). We thank Roberto Gomez and Rick Costa at the PSC and Bill Wichser at PICSciE for invaluable help with computing. NR 52 TC 9 Z9 9 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 JUL 1 PY 2014 VL 789 IS 1 AR 31 DI 10.1088/0004-637X/789/1/31 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400031 ER PT J AU Lee, JJ Park, S Hughes, JP Slane, PO AF Lee, Jae-Joon Park, Sangwook Hughes, John P. Slane, Patrick O. TI X-RAY OBSERVATION OF THE SHOCKED RED SUPERGIANT WIND OF CASSIOPEIA A SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Cas A); ISM: supernova remnants; stars: winds, outflows; X-rays: ISM ID SUPERNOVA-REMNANTS; MASSIVE STARS; CIRCUMSTELLAR MEDIUM; A SUPERNOVA; PROGENITOR; EJECTA; IIB; EXPLOSION; EVOLUTION; EMISSION AB Cas A is a Galactic supernova remnant whose supernova explosion is observed to be of Type IIb from spectroscopy of its light echo. Having its SN type known, observational constraints on the mass-loss history of Cas A's progenitor can provide crucial information on the final fate of massive stars. In this paper, we study X-ray characteristics of the shocked ambient gas in Cas A using the 1 Ms observation carried out with the Chandra X-Ray Observatory and try to constrain the mass-loss history of the progenitor star. We identify thermal emission from the shocked ambient gas along the outer boundary of the remnant. Comparison of measured radial variations of spectroscopic parameters of the shocked ambient gas to the self-similar solutions of Chevalier show that Cas A is expanding into a circumstellar wind rather than into a uniform medium. We estimate a wind density n(H) similar to 0.9 +/- 0.3 cm(-3) at the current outer radius of the remnant (similar to 3 pc), which we interpret as a dense slow wind from a red supergiant (RSG) star. Our results suggest that the progenitor star of Cas A had an initial mass around 16 M-circle dot, and its mass before the explosion was about 5 M-circle dot, with uncertainties of several tens of percent. Furthermore, the results suggest that, among the mass lost from the progenitor star (similar to 11 M-circle dot), a significant amount (more than 6 M-circle dot) could have been via its RSG wind. C1 [Lee, Jae-Joon] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Park, Sangwook] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lee, JJ (reprint author), Korea Astron & Space Sci Inst, Taejon 305348, South Korea. EM leejjoon@kasi.re.kr NR 46 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2014 VL 789 IS 1 AR 7 DI 10.1088/0004-637X/789/1/7 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400007 ER PT J AU Lehmer, BD Berkeley, M Zezas, A Alexander, DM Basu-Zych, A Bauer, FE Brandt, WN Fragos, T Hornschemeier, AE Kalogera, V Ptak, A Sivakoff, GR Tzanavaris, P Yukita, M AF Lehmer, B. D. Berkeley, M. Zezas, A. Alexander, D. M. Basu-Zych, A. Bauer, F. E. Brandt, W. N. Fragos, T. Hornschemeier, A. E. Kalogera, V. Ptak, A. Sivakoff, G. R. Tzanavaris, P. Yukita, M. TI THE X-RAY LUMINOSITY FUNCTIONS OF FIELD LOW-MASS X-RAY BINARIES IN EARLY-TYPE GALAXIES: EVIDENCE FOR A STELLAR AGE DEPENDENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: evolution; Galaxy: stellar content; globular clusters: general; X-rays: binaries; X-rays: galaxies ID GLOBULAR-CLUSTERS; ELLIPTIC GALAXIES; STAR-FORMATION; HOT GAS; SAURON PROJECT; DEEP CHANDRA; POPULATIONS; LMXBS; CATALOG; ENVIRONMENTS AB We present direct constraints on how the formation of low-mass X-ray binary (LMXB) populations in galactic fields depends on stellar age. In this pilot study, we utilize Chandra and Hubble Space Telescope (HST) data to detect and characterize the X-ray point source populations of three nearby early-type galaxies: NGC 3115, 3379, and 3384. The luminosity-weighted stellar ages of our sample span approximate to 3-10 Gyr. X-ray binary population synthesis models predict that the field LMXBs associated with younger stellar populations should be more numerous and luminous per unit stellar mass than older populations due to the evolution of LMXB donor star masses. Crucially, the combination of deep Chandra and HST observations allows us to test directly this prediction by identifying and removing counterparts to X-ray point sources that are unrelated to the field LMXB populations, including LMXBs that are formed dynamically in globular clusters, Galactic stars, and background active galactic nuclei/galaxies. We find that the "young" early-type galaxy NGC 3384 (approximate to 2-5 Gyr) has an excess of luminous field LMXBs (L-X greater than or similar to (5-10) x 10(37) erg s(-1)) per unit K-band luminosity (L-K; a proxy for stellar mass) than the "old" early-type galaxies NGC 3115 and 3379 (approximate to 8-10 Gyr), which results in a factor of approximate to 2-3 excess of L-X/L-K for NGC 3384. This result is consistent with the X-ray binary population synthesis model predictions; however, our small galaxy sample size does not allow us to draw definitive conclusions on the evolution field LMXBs in general. We discuss how future surveys of larger galaxy samples that combine deep Chandra and HST data could provide a powerful new benchmark for calibrating X-ray binary population synthesis models. C1 [Lehmer, B. D.; Tzanavaris, P.; Yukita, M.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Lehmer, B. D.; Berkeley, M.; Basu-Zych, A.; Hornschemeier, A. E.; Ptak, A.; Tzanavaris, P.; Yukita, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Berkeley, M.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Zezas, A.; Sivakoff, G. R.] Univ Crete, Dept Phys, Iraklion, Greece. [Zezas, A.; Fragos, T.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. [Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Basu-Zych, A.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Sivakoff, G. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. RP Lehmer, BD (reprint author), Johns Hopkins Univ, Homewood Campus, Baltimore, MD 21218 USA. RI Sivakoff, Gregory/G-9602-2011; Brandt, William/N-2844-2015; Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016 OI Sivakoff, Gregory/0000-0001-6682-916X; Brandt, William/0000-0002-0167-2453; Zezas, Andreas/0000-0001-8952-676X; Fragos, Tassos/0000-0003-1474-1523 FU Chandra X-ray Center grant [G02-13107A]; Space Telescope Science Institute [GO-12760]; NASA ADP [NNX13AI48G, NNX12AL39G]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024, Gemini-CONICYT 32120003, Anillo ACT1101]; Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo [IC120009]; ADP [NNX10AC99G]; NSERC FX We thank the referee for providing thoughtful comments that have improved the quality of this paper. We thank Zhongli Zhang for providing data. We gratefully acknowledge financial support from Chandra X-ray Center grant G02-13107A, Space Telescope Science Institute grant GO-12760, and NASA ADP grant NNX13AI48G (B.D.L.). F.E.B. acknowledges support from Basal-CATA PFB-06/2007, CONICYT-Chile (grants FONDECYT 1101024, Gemini-CONICYT 32120003, "EMBIGGEN" Anillo ACT1101), and Project IC120009 "Millennium Institute of Astrophysics (MAS)" funded by the Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo. W.N.B. acknowledges ADP grant NNX10AC99G. G.R.S. is supported by an NSERC Discovery Grant. V.K. acknowledges support for this work from NASA ADP grant NNX12AL39G (sub-contract to Northwestern University) NR 63 TC 11 Z9 11 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2014 VL 789 IS 1 AR 52 DI 10.1088/0004-637X/789/1/52 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400052 ER PT J AU Schlafly, EF Green, G Finkbeiner, DP Juric, M Rix, HW Martin, NF Burgett, WS Chambers, KC Draper, PW Hodapp, KW Kaiser, N Kudritzki, RP Magnier, EA Metcalfe, N Morgan, JS Price, PA Stubbs, CW Tonry, JL Wainscoat, RJ Waters, C AF Schlafly, E. F. Green, G. Finkbeiner, D. P. Juric, M. Rix, H. -W. Martin, N. F. Burgett, W. S. Chambers, K. C. Draper, P. W. Hodapp, K. W. Kaiser, N. Kudritzki, R. -P. Magnier, E. A. Metcalfe, N. Morgan, J. S. Price, P. A. Stubbs, C. W. Tonry, J. L. Wainscoat, R. J. Waters, C. TI A MAP OF DUST REDDENING TO 4.5 kpc FROM Pan-STARRS1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: clouds ID DIGITAL SKY SURVEY; MILKY-WAY TOMOGRAPHY; COLOR EXCESS METHOD; INTERSTELLAR EXTINCTION; MOLECULAR CLOUDS; MULTIBAND PHOTOMETRY; 2MASS; SDSS; DISTANCES; DENSITY AB We present a map of the dust reddening to 4.5 kpc derived from Pan-STARRS1 stellar photometry. The map covers almost the entire sky north of declination -30 degrees at a resolution of 7'-14', and is based on the estimated distances and reddenings to more than 500 million stars. The technique is designed to map dust in the Galactic plane, where many other techniques are stymied by the presence of multiple dust clouds at different distances along each line of sight. This reddening-based dust map agrees closely with the Schlegel et al. (SFD) far-infrared emission-based dust map away from the Galactic plane, and the most prominent differences between the two maps stem from known limitations of SFD in the plane. We also compare the map with Planck, finding likewise good agreement in general at high latitudes. The use of optical data from Pan-STARRS1 yields reddening uncertainty as low as 25 mmag E(B - V). C1 [Schlafly, E. F.; Rix, H. -W.; Martin, N. F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Green, G.; Finkbeiner, D. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Finkbeiner, D. P.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Juric, M.] LSST Corp, Tucson, AZ 85721 USA. [Martin, N. F.] CNRS, UMR 7550, Observ Astron Strasbourg, F-67000 Strasbourg, France. [Burgett, W. S.; Chambers, K. C.; Hodapp, K. W.; Kaiser, N.; Kudritzki, R. -P.; Magnier, E. A.; Morgan, J. S.; Tonry, J. L.; Wainscoat, R. J.; Waters, C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Draper, P. W.; Metcalfe, N.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Schlafly, EF (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Green, Gregory/0000-0001-5417-2260; Schlafly, Edward Ford/0000-0002-3569-7421; Draper, Peter W./0000-0002-7204-9802; Chambers, Kenneth /0000-0001-6965-7789; Metcalfe, Nigel/0000-0001-9034-4402 FU German Research Foundation (DFG) [Sonderforschungsbereich SFB 881]; NASA [NNX10AD69G]; NSF [AST-1312891]; CNRS through PICS project [PICS06183]; National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877] FX E.F.S. acknowledges funding by Sonderforschungsbereich SFB 881 "The Milky Way System" subproject A3) of the German Research Foundation (DFG). D.P.F. acknowledges support of NASA grant NNX10AD69G. G.G. and D.P.F. are partially supported by NSF grant AST-1312891. N.F.M. gratefully acknowledges the CNRS for support through PICS project PICS06183. Computation was performed on the GPU Cluster Milky Way at FZ Juelich and on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University.; 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 44 TC 28 Z9 28 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2014 VL 789 IS 1 AR 15 DI 10.1088/0004-637X/789/1/15 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400015 ER PT J AU Van Loo, S Keto, E Zhang, QZ AF Van Loo, Sven Keto, Eric Zhang, Qizhou TI CORE AND FILAMENT FORMATION IN MAGNETIZED, SELF-GRAVITATING ISOTHERMAL LAYERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: structure; methods: numerical; stars: formation ID MOLECULAR CLOUD FORMATION; MAGNETICALLY-DOMINATED CLOUDS; SHOCK-TRIGGERED FORMATION; FREE-FALL TIME; STAR-FORMATION; AMBIPOLAR DIFFUSION; INTERSTELLAR FILAMENTS; INTERNAL STRUCTURE; COMPRESSED LAYERS; LINE-PROFILES AB We examine the role of the gravitational instability in an isothermal, self-gravitating layer threaded by magnetic fields on the formation of filaments and dense cores. Using a numerical simulation, we follow the non-linear evolution of a perturbed equilibrium layer. The linear evolution of such a layer is described in the analytic work of Nagai et al. We find that filaments and dense cores form simultaneously. Depending on the initial magnetic field, the resulting filaments form either a spiderweb-like network (for weak magnetic fields) or a network of parallel filaments aligned perpendicular to the magnetic field lines (for strong magnetic fields). Although the filaments are radially collapsing, the density profile of their central region (up to the thermal scale height) can be approximated by a hydrodynamical equilibrium density structure. Thus, the magnetic field does not play a significant role in setting the density distribution of the filaments. The density distribution outside of the central region deviates from the equilibrium. The radial column density distribution is then flatter than the expected power law of r(-4) and similar to filament profiles observed with Herschel. Our results do not explain the near constant filament width of similar to 0.1pc. However, our model does not include turbulent motions. It is expected that the accretion-driven amplification of these turbulent motions provides additional support within the filaments against gravitational collapse. Finally, we interpret the filamentary network of the massive star forming complex G14.225-0.506 in terms of the gravitational instability model and find that the properties of the complex are consistent with being formed out of an unstable layer threaded by a strong, parallel magnetic field. C1 [Van Loo, Sven; Keto, Eric; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Van Loo, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM svanloo@cfa.harvard.edu OI Van Loo, Sven/0000-0003-4746-8500; Zhang, Qizhou/0000-0003-2384-6589 FU SMA Postdoctoral Fellowship of the Smithsonian Astrophysical Observatory FX We thank Tom Hartquist, Sam Falle, and Phil Myers for useful discussions, Gemma Busquet for providing the observational data of the G14.225-0.506 molecular cloud and the anonymous referee for comments that improved the paper. S. V. L. acknowledges support from the SMA Postdoctoral Fellowship of the Smithsonian Astrophysical Observatory. The simulations for this work were run on the Smithsonian Institution High Performance Cluster (SI/HPC). NR 73 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 JUL 1 PY 2014 VL 789 IS 1 AR 37 DI 10.1088/0004-637X/789/1/37 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400037 ER PT J AU Qurban, MA Krishnakumar, PK Joydas, TV Manikandan, KP Ashraf, TTM Quadri, SI Wafar, M Qasem, A Cairns, SD AF Qurban, Mohammad A. Krishnakumar, P. K. Joydas, T. V. Manikandan, K. P. Ashraf, T. T. M. Quadri, S. I. Wafar, M. Qasem, Ali Cairns, S. D. TI In-situ observation of deep water corals in the northern Red Sea waters of Saudi Arabia SO DEEP-SEA RESEARCH PART I-OCEANOGRAPHIC RESEARCH PAPERS LA English DT Article DE Cold water corals; Azooxanthellate; Dasmosmilia valida; Eguchipsammia fistula; Rhizotrochus typus; Octocorallia; Antipatharia ID MEDITERRANEAN SEA; DIVERSITY; MARGINS; SHELF; ZONE AB Three sites offshore of the Saudi Arabia coast in the northern Red Sea were surveyed in November 2012 to search for deep-water coral (DWC) grounds using a Remotely Operated Vehicle. A total of 156 colonies were positively identified between 400 and 760 m, and were represented by seven species belonging to Scleractinia (3), Alcyonacea (3) and Antipatharia (1). The scleractinians Dasmosmilia valida Marenzeller, 1907, Eguchipsammia fistula (Alcock, 1902) and Rhizotrochus typus Milne-Edwards and Haime, 1848 were identified to species level, while the octocorals Acanthogorgia sp., Chironephthya sp., Pseudopterogorgia sp., and the antipatharian Stichopathes sp., were identified to genus level. Overall, the highest abundance of DWC was observed at Site A1, the closest to the coast. The most abundant species in the study area was D. valida, which lives attached to rocky substrates and represented 42% of the total coral population at site A1. Water column attributes at this depth were quite homogenous with temperature ca. 21.6 degrees C, salinity ca. 40.56, dissolved oxygen ca. 1.75 ml L-1 and current velocity from 0.6 to 34.5 cm s(-1) with a mean value of 9.5 cm s(-1). Interestingly, these DWC can cope with high temperature and salinity, compared to those in other regions. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Qurban, Mohammad A.; Krishnakumar, P. K.; Joydas, T. V.; Manikandan, K. P.; Ashraf, T. T. M.; Quadri, S. I.; Wafar, M.] King Fand Univ Petr & Minerals, Ctr Environm & Water, Res Inst, Dhahran 31261, Saudi Arabia. [Qasem, Ali] Saudi Aramco, Environm Protect Dept, Dhahran, Saudi Arabia. [Cairns, S. D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Qurban, MA (reprint author), King Fand Univ Petr & Minerals, Ctr Environm & Water, Res Inst, PB 391, Dhahran 31261, Saudi Arabia. EM mqurban@kfupm.edu.sa RI Joydas, Thadickal/F-1809-2015; OI Joydas, T.V./0000-0002-6725-4094 NR 44 TC 7 Z9 7 U1 2 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0637 EI 1879-0119 J9 DEEP-SEA RES PT I JI Deep-Sea Res. Part I-Oceanogr. Res. Pap. PD JUL PY 2014 VL 89 BP 35 EP 43 DI 10.1016/j.dsr.2014.04.002 PG 9 WC Oceanography SC Oceanography GA AJ8YG UT WOS:000337993400003 ER PT J AU Soon, W Herrera, VMV Selvaraj, K Traversi, R Usoskin, I Chen, CTA Lou, JY Kao, SJ Carter, RM Pipin, V Severi, M Becagli, S AF Soon, Willie Herrera, Victor M. Velasco Selvaraj, Kandasamy Traversi, Rita Usoskin, Ilya Chen, Chen-Tung Arthur Lou, Jiann-Yuh Kao, Shuh-Ji Carter, Robert M. Pipin, Valery Severi, Mirko Becagli, Silvia TI A review of Holocene solar-linked climatic variation on centennial to millennial timescales: Physical processes, interpretative frameworks and a new multiple cross-wavelet transform algorithm SO EARTH-SCIENCE REVIEWS LA English DT Article DE Solar-climate variations; Solar activity proxies; Wavelet transform ID NORTH-ATLANTIC CLIMATE; NORTHEASTERN UNITED-STATES; TROPICAL PACIFIC-OCEAN; HIGH-RESOLUTION; SOUTHERN-OCEAN; ASIAN MONSOON; ICE CORE; CIRCULATION PATTERNS; SURFACE-TEMPERATURE; COSMOGENIC ISOTOPES AB We report on the existence and nature of Holocene solar and climatic variations on centennial to millennial time-scales. We introduce a new solar activity proxy, based on nitrate (NO) concentration from the Tabs Dome ice core, East Antarctica. We also use a new algorithm for computing multiple-cross wavelet spectra in time-frequency space that is generalized for multiple time series (beyond two). Our results provide a new interpretive framework for relating Holocene solar activity variations on centennial to millennial timescales to co-varying climate proxies drawn from a widespread area around the globe. Climatic proxies used represent variation in the North Atlantic Ocean, Western Pacific Warm Pool, Southern Ocean and the East Asian monsoon regions. Our wavelet analysis identifies fundamental solar modes at 2300-yr (Hallstattzeit), 1000-yr (Eddy), and 500-yr (unnamed) periodicities, leaves open the possibility that the 1500-1800-yr cycle may either be fundamental or derived, and identifies intermediary derived cycles at 700-yr and 300-yr that may mark rectified responses of the Atlantic thermohaline circulation to external solar modulation and pacing. Dating uncertainties suggest that the 1500-yr and 1800-yr cycles described in the literature may represent either the same or two separate cycles, but in either case, and irrespective too of whether it is a fundamental or derived mode in the sense of Dima and Lohmann (2009), the 1500-1800-yr periodicity is widely represented in a large number of paleoclimate proxy records. It is obviously premature to reject possible links between changing solar activity at these multiple scales and the variations that are commonly observed in paleoclimatic records. (C) 2014 Elsevier B.V. All rights reserved. C1 [Soon, Willie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Herrera, Victor M. Velasco] Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City 04510, DF, Mexico. [Selvaraj, Kandasamy; Kao, Shuh-Ji] Xiamen Univ, State Key Lab Marine Environm Sci, Xiamen, Peoples R China. [Traversi, Rita; Severi, Mirko; Becagli, Silvia] Univ Florence, Dept Chem Ugo Schiff, I-50019 Florence, Italy. [Usoskin, Ilya] Univ Oulu, Sodankyla Geophys Observ, Oulu, Finland. [Usoskin, Ilya] Univ Oulu, Dept Phys, Oulu, Finland. [Chen, Chen-Tung Arthur] Natl Sun Yat Sen Univ, Inst Marine Geol & Chem, Kaohsiung 80424, Taiwan. [Lou, Jiann-Yuh] Naval Acad, Dept Marine Sci, Kaohsiung, Taiwan. [Carter, Robert M.] Inst Publ Affairs, Melbourne, Australia. [Pipin, Valery] Russian Acad Sci, Inst Solar Terr Phys, Irkutsk 664033, Russia. RP Soon, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM wsoon@cfa.harvard.edu RI Kao, Shuh-Ji/F-8418-2015; Traversi, Rita/M-7586-2015; Chen, Chen-Tung Arthur/C-8901-2011; Severi, Mirko/J-2508-2012; OI Kao, Shuh-Ji/0000-0002-5054-9099; Traversi, Rita/0000-0002-9790-2195; Severi, Mirko/0000-0003-1511-6762; Becagli, Silvia/0000-0003-3633-4849; Velasco, Victor/0000-0002-0100-8878; Usoskin, Ilya/0000-0001-8227-9081 FU ReSoLVE Center of Excellence (Academy of Finland) [272157]; [CONACyT-180148] FX W.S. thanks Dr. Mihai Dima for his contributions to the scientific knowledge in this manuscript as well as his unselfish sharing of published data. Dr. Mathias Moros is thanked for sharing his data and Dr. Charles Perry is thanked for clarifying the details in Perry and Hsu (2000). We acknowledge the comments by a total of four reviewers that helped to improve the clarity of our paper. W.S. and V.M.V.H. contributed equally to the results in this paper. V.M.V.H. acknowledges the support from CONACyT-180148 grant I.U.'s contribution was done in the framework of the ReSoLVE Center of Excellence (Academy of Finland, project no. 272157). This work is a contribution to TALDICE and HOLOCLIP projects. TALDICE (Tabs Dome Ice Core Project) is a joint European programme, funded by national contributions from Italy, France, Germany, Switzerland and the United Kingdom. Primary logistic support was provided by PNRA at Tabs Dome. HOLOCLIP is a joint research project of ESF PolarCLIMATE programme, funded by national contributions from Italy, France, Germany, Spain, Netherlands, Belgium, and the United Kingdom. This is TALDICE paper n.38 and HOLOCLIP paper n.22. NR 150 TC 26 Z9 26 U1 3 U2 63 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-8252 EI 1872-6828 J9 EARTH-SCI REV JI Earth-Sci. Rev. PD JUL PY 2014 VL 134 BP 1 EP 15 DI 10.1016/j.earscirev.2014.03.003 PG 15 WC Geosciences, Multidisciplinary SC Geology GA AJ7CW UT WOS:000337855800001 ER PT J AU Anderson, MR AF Anderson, Megan R. TI Reaching New Heights: The Effect of an Environmentally Enhanced Outdoor Enclosure on Gibbons in a Zoo Setting SO JOURNAL OF APPLIED ANIMAL WELFARE SCIENCE LA English DT Article DE gibbons; behavior; space utilization; environmental enrichment ID SPACE AB Gibbons have adapted to live in the canopy layer of the rainforest. Gibbons in the wild predominantly spend their time high in the trees resting, traveling, and foraging for food. Comparatively, gibbons in the zoo often rest and search for their food terrestrially. The purpose of this study was to provide these arboreal smaller apes with more opportunities to utilize more vertical space. Six gibbons (4 Nomascus leucogenys and 2 Symphalangus syndactylus) were observed in 2 phases of an observational study. The 1st phase measured space utilization and behaviors of the zoo-housed gibbons in their original outdoor enclosures using instantaneous sampling. The 2nd phase measured the same space usage and behaviors after several modifications were made to the environmental structures in the same outdoor enclosures. A 2-way mixed-model analysis of variance tested the height utilization of the 6 gibbons. The gibbons chose to spend significantly more time outside and at higher heights when the new structures were added. This study shows that given the opportunity, gibbons will exhibit more species-appropriate behaviors. C1 Smithsonian Inst, Natl Zool Pk, Washington, DC 20013 USA. RP Anderson, MR (reprint author), Smithsonian Inst, Natl Zool Pk, MRC 5507, Washington, DC 20013 USA. EM jordanxmegan@hotmail.com NR 15 TC 0 Z9 0 U1 3 U2 32 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 1088-8705 EI 1532-7604 J9 J APPL ANIM WELF SCI JI J. Appl. Anim. Welf. Sci. PD JUL-SEP PY 2014 VL 17 IS 3 BP 216 EP 227 DI 10.1080/10888705.2014.916172 PG 12 WC Veterinary Sciences SC Veterinary Sciences GA AJ8AA UT WOS:000337923000003 PM 24832240 ER PT J AU Comita, LS Queenborough, SA Murphy, SJ Eck, JL Xu, KY Krishnadas, M Beckman, N Zhu, Y AF Comita, Liza S. Queenborough, Simon A. Murphy, Stephen J. Eck, Jenalle L. Xu, Kaiyang Krishnadas, Meghna Beckman, Noelle Zhu, Yan TI Testing predictions of the Janzen-Connell hypothesis: a meta-analysis of experimental evidence for distance- and density-dependent seed and seedling survival SO JOURNAL OF ECOLOGY LA English DT Article DE determinants of plant community diversity and structure; herbivory; maintenance of diversity; natural enemies; pathogens; plant population and community dynamics; review; seed predation; species coexistence; tropical forest ID TROPICAL TREE DIVERSITY; PLANT-SOIL FEEDBACKS; RAIN-FOREST; SPECIES COEXISTENCE; PERENNIAL PLANTS; SPATIAL-PATTERNS; PATHOGENS; RECRUITMENT; MORTALITY; CONSEQUENCES AB 1. The Janzen-Connell hypothesis proposes that specialist natural enemies, such as herbivores and pathogens, maintain diversity in plant communities by reducing survival rates of conspecific seeds and seedlings located close to reproductive adults or in areas of high conspecific density. Variation in the strength of distance- and density-dependent effects is hypothesized to explain variation in plant species richness along climatic gradients, with effects predicted to be stronger in the tropics than the temperate zone and in wetter habitats compared to drier habitats. 2. We conducted a comprehensive literature search to identify peer-reviewed experimental studies published in the 40+ years since the hypothesis was first proposed. Using data from these studies, we conducted a meta-analysis to assess the current weight of evidence for the distance and density predictions of the Janzen-Connell hypothesis. 3. Overall, we found significant support for both the distance- and density-dependent predictions. For all studies combined, survival rates were significantly reduced near conspecifics compared to far from conspecifics, and in areas with high densities of conspecifics compared to areas with low conspecific densities. There was no indication that these results were due to publication bias. 4. The strength of distance and density effects varied widely among studies. Contrary to expectations, this variation was unrelated to latitude, and there was no significant effect of study region. However, we did find a trend for stronger distance and density dependence in wetter sites compared to sites with lower annual precipitation. In addition, effects were significantly stronger at the seedling stage compared to the seed stage. 5. Synthesis. Our study provides support for the idea that distance- and density-dependent mortality occurs in plant communities world-wide. Available evidence suggests that natural enemies are frequently the cause of such patterns, consistent with the Janzen-Connell hypothesis, but additional studies are needed to rule out other mechanisms (e.g. intraspecific competition). With the widespread existence of density and distance dependence clearly established, future research should focus on assessing the degree to which these effects permit species coexistence and contribute to the maintenance of diversity in plant communities. C1 [Comita, Liza S.; Queenborough, Simon A.; Murphy, Stephen J.; Eck, Jenalle L.; Xu, Kaiyang; Krishnadas, Meghna] Ohio State Univ, Dept Evolut Ecol & Organismal Biol, Columbus, OH 43210 USA. [Comita, Liza S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Beckman, Noelle] Ohio State Univ, Math Biosci Inst, Columbus, OH 43210 USA. [Zhu, Yan] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing 100093, Peoples R China. RP Comita, LS (reprint author), Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. EM liza.comita@yale.edu RI Beckman, Noelle/E-5554-2011 OI Beckman, Noelle/0000-0001-5822-0610 NR 65 TC 58 Z9 60 U1 35 U2 252 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 JUL PY 2014 VL 102 IS 4 BP 845 EP 856 DI 10.1111/1365-2745.12232 PG 12 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA AJ9KB UT WOS:000338027500003 ER PT J AU Banin, L Lewis, SL Lopez-Gonzalez, G Baker, TR Quesada, CA Chao, KJ Burslem, DFRP Nilus, R Abu Salim, K Keeling, HC Tan, S Davies, SJ Mendoza, AM Vasquez, R Lloyd, J Neill, DA Pitman, N Phillips, OL AF Banin, Lindsay Lewis, Simon L. Lopez-Gonzalez, Gabriela Baker, Timothy R. Quesada, Carlos A. Chao, Kuo-Jung Burslem, David F. R. P. Nilus, Reuben Abu Salim, Kamariah Keeling, Helen C. Tan, Sylvester Davies, Stuart J. Monteagudo Mendoza, Abel Vasquez, Rodolfo Lloyd, Jon Neill, David A. Pitman, Nigel Phillips, Oliver L. TI Tropical forest wood production: a cross-continental comparison SO JOURNAL OF ECOLOGY LA English DT Article DE Amazon; Asia; carbon; Dipterocarpaceae; dynamics; growth; plant-soil interactions; productivity; soil nutrients; tropical forest ID NET PRIMARY PRODUCTIVITY; RAIN-FOREST; TREE GROWTH; AMAZONIAN FORESTS; NEOTROPICAL FORESTS; NUTRIENT LIMITATION; LITTER PRODUCTION; SOIL-PHOSPHORUS; CARBON-DIOXIDE; EL-NINO AB 1. Tropical forest above-ground wood production (AGWP) varies substantially along environmental gradients. Some evidence suggests that AGWP may vary between regions and specifically that Asian forests have particularly high AGWP. However, comparisons across biogeographic regions using standardized methods are lacking, limiting our assessment of pan-tropical variation in AGWP and potential causes. 2. We sampled AGWP in NW Amazon (17 long-term forest plots) and N Borneo (11 plots), both with abundant year-round precipitation. Within each region, forests growing on a broad range of edaphic conditions were sampled using standardized soil and forest measurement techniques. 3. Plot-level AGWP was 49% greater in Borneo than in Amazonia (9.73 +/- 0.56 vs. 6.53 +/- 0.34 Mg dry mass ha(-1) a(-1), respectively; regional mean +/- 1 SE). AGWP was positively associated with soil fertility (PCA axes, sum of bases and total P). After controlling for the edaphic environment, AGWP remained significantly higher in Bornean plots. Differences in AGWP were largely attributable to differing height-diameter allometry in the two regions and the abundance of large trees in Borneo. This may be explained, in part, by the greater solar radiation in Borneo compared with NW Amazonia. 4. Trees belonging to the dominant SE Asian family, Dipterocarpaceae, gained woody biomass faster than otherwise equivalent, neighbouring non-dipterocarps, implying that the exceptional production of Bornean forests may be driven by floristic elements. This dominant SE Asian family may partition biomass differently or be more efficient at harvesting resources and in converting them to woody biomass. 5. Synthesis. N Bornean forests have much greater AGWP rates than those in NW Amazon when soil conditions and rainfall are controlled for. Greater resource availability and the highly productive dipterocarps may, in combination, explain why Asian forests produce wood half as fast again as comparable forests in the Amazon. Our results also suggest that taxonomic groups differ in their fundamental ability to capture carbon and that different tropical regions may therefore have different carbon uptake capacities due to biogeographic history. C1 [Banin, Lindsay] Bush Estate, Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland. [Banin, Lindsay; Lewis, Simon L.; Lopez-Gonzalez, Gabriela; Baker, Timothy R.; Keeling, Helen C.; Phillips, Oliver L.] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. [Lewis, Simon L.] UCL, Dept Geog, London WC1E 6BT, England. [Quesada, Carlos A.] Inst Nacl de Pesquisas da Amazonia, BR-69060001 Manaus, Amazonas, Brazil. [Chao, Kuo-Jung] Natl Chung Hsing Univ, Coll Agr & Nat Resources, Int Master Program Agr, Taichung 40227, Taiwan. [Burslem, David F. R. P.] Univ Aberdeen, Sch Biol Sci, Aberdeen AB24 3UU, Scotland. [Nilus, Reuben] Forest Res Ctr, Sabah Forestry Dept, Sandakan 90715, Sabah, Malaysia. [Abu Salim, Kamariah] Univ Brunei Darussalam, Fac Sci, BE-1410 Bandar Seri Begawan, Brunei. [Tan, Sylvester] Sarawak Forestry Corp, KCLD, Kuching 93250, Sarawak, Malaysia. [Davies, Stuart J.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Washington, DC 20013 USA. [Monteagudo Mendoza, Abel; Vasquez, Rodolfo] Jardin Bot Missouri, Oxapampa 19231, Pasco, Peru. [Lloyd, Jon] Univ London Imperial Coll Sci Technol & Med, Dept Life Sci, Fac Nat Sci, London SW7 2AZ, England. [Neill, David A.] Univ Estatal Amazonica, Puyo, Pastaza, Ecuador. [Pitman, Nigel] Field Museum, Chicago, IL 60605 USA. [Pitman, Nigel] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. RP Banin, L (reprint author), Bush Estate, Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland. EM Lindsay.banin@gmail.com RI Phillips, Oliver/A-1523-2011; Lloyd, Jonathan/F-8893-2010; OI Phillips, Oliver/0000-0002-8993-6168; Lloyd, Jonathan/0000-0002-5458-9960; Lewis, Simon/0000-0002-8066-6851; Burslem, David/0000-0001-6033-0990 FU RAINFOR network; AMAZONICA project; NERC; Gordon and Betty Moore Foundation; NERC studentship; Henrietta Hutton Grant (RGS-IBG); Dudley Stamp Award (Royal Society); Royal Society University Research Fellowship; European Research Council Advanced Grant; Royal Society Wolfson Research Merit Award FX This work was supported by the RAINFOR network, the AMAZONICA project and funding from NERC and the Gordon and Betty Moore Foundation. L. B. was supported by a NERC studentship with additional funding from Henrietta Hutton Grant (RGS-IBG) and Dudley Stamp Award (Royal Society). S. L. L. was supported by a Royal Society University Research Fellowship. O.L.P. and S. L. L. were supported by a European Research Council Advanced Grant and O.L.P. by a Royal Society Wolfson Research Merit Award. For help in collecting data, we thank J.H. Ovalle, M. M. Solorzano and Antonio Pena Cruz (Peru); R. Sukri and M. Salleh A. B. (Brunei); C. Maycock (Sabah); and L. Chong, R. Shutine and L. K. Kho (Sarawak); for logistical aid and access to the forest plots of Lambir Hills National Park, Sarawak, Malaysia, we thank the Sarawak Forestry Corporation, Malaysia, the Center for Tropical Forest Science - Arnold Arboretum Asia Program of the Smithsonian Tropical Research Institute and Harvard University, USA, and their funding agencies. Additional thanks go to the Economic Planning Unit, Malaysia, for granting L. B. access to conduct research and Rachel Gasior, Martin Gilpin and David Ashley for laboratory assistance. We thank Patrick Meir, Stephen Sitch, Alan Grainger, Geertje van der Heijden, Ron Smith, Joe Wright and an anonymous reviewer for their helpful comments on earlier versions of the manuscript. NR 85 TC 27 Z9 27 U1 6 U2 73 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 JUL PY 2014 VL 102 IS 4 BP 1025 EP 1037 DI 10.1111/1365-2745.12263 PG 13 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA AJ9KB UT WOS:000338027500020 ER PT J AU Cohen, EB Moore, FR Fischer, RA AF Cohen, Emily B. Moore, Frank R. Fischer, Richard A. TI Fuel stores, time of spring, and movement behavior influence stopover duration of Red-eyed Vireo Vireo olivaceus SO JOURNAL OF ORNITHOLOGY LA English DT Article DE Nearctic-Neotropical migrant; Spring migration; Stopover duration; Radio-telemetry; Red-eyed Vireo; Vireo olivaceus ID GULF-OF-MEXICO; MIGRATION STOPOVER; NORTHERN WHEATEARS; ERITHACUS-RUBECULA; OENANTHE-OENANTHE; EUROPEAN ROBINS; FAT DEPOSITION; BIRD MIGRATION; DEPARTURES; MIGRANTS AB Long-distance migration is characterized by periods of flight, when energy stores are consumed, and periods of stopover, when energy stores are replenished. The duration of the migratory period is largely determined by time spent at stopover sites. The time constraints imposed on spring migrants should act to minimize the time spent on migration, yet spring migrants often remain at stopover sites for extended periods. We measured the influence of arrival fuel stores, arrival date, and foraging movement rate on the duration of Red-eyed Vireos (Vireo olivaceus) that remained at stopover sites for more than 1 day. We captured spring migrants in mist-nets as they arrived after crossing the Gulf of Mexico. We released them at an inland site and continuously followed (radio-tracked) their movements until departure. Departure time was confirmed with extensive ground searches and aerial surveys. Migrants remained at the stopover sites from 1 to 8 days (2.80 +/- A 0.14 days). Less than one-third of migrants were transient, leaving the night following release (32 %). Of the migrants that remained more than 1 day, those that arrived with low fuel stores remained longer than those that arrived with more fuel stores. Only migrants arriving early in the spring stayed for extended periods of time (> 5 days). Further, migrants that moved faster within the stopover landscape presumably replenished fuel stores faster because they did not remain as long as migrants that did not move as quickly. When arrival fuel stores, arrival day, and departure day were known, we found multiple factors influenced the length of stay at spring stopover sites. Early spring migrants with low fuel stores that moved slowly through the landscape spent the most time at spring stopover sites. C1 [Cohen, Emily B.; Moore, Frank R.] Univ So Mississippi, Dept Biol Sci, Hattiesburg, MS 39406 USA. [Cohen, Emily B.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Fischer, Richard A.] US Army Engn Res & Dev Ctr, Environm Lab, Vicksburg, MS 39180 USA. RP Cohen, EB (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk,POB 37012,MRC 5503, Washington, DC 20013 USA. EM cohene@si.edu FU US Department of Defense Strategic Environmental Research and Development Program; University of Southern Mississippi FX Logistical support was provided by J. Johnson and D. Hudson at Fort Polk and L. Bennett at Louisiana Wildlife and Fisheries. We would especially like to thank the members of the migratory bird research group at USM and all of the hard-working assistants who helped us collect data in the field. Funding for this project was provided by the US Department of Defense Strategic Environmental Research and Development Program and the University of Southern Mississippi. This study was conducted in full compliance with the laws of the United States of America. NR 62 TC 5 Z9 5 U1 1 U2 30 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0021-8375 EI 1439-0361 J9 J ORNITHOL JI J. Ornithol. PD JUL PY 2014 VL 155 IS 3 BP 785 EP 792 DI 10.1007/s10336-014-1067-3 PG 8 WC Ornithology SC Zoology GA AJ6HP UT WOS:000337792500023 ER PT J AU Loss, SR Will, T Marra, PP AF Loss, Scott R. Will, Tom Marra, Peter P. TI Estimation of bird-vehicle collision mortality on US roads SO JOURNAL OF WILDLIFE MANAGEMENT LA English DT Review DE anthropogenic mortality; automobiles; birds; detection probability; roadkill; roads; scavenger removal; systematic review; United States; vehicles ID UNITED-STATES; AVIAN MORTALITY; BARN OWLS; TYTO-ALBA; POPULATIONS; VERTEBRATES; AMPHIBIANS; WILDLIFE; MAMMALS; CANADA AB Roads have numerous direct and indirect ecological impacts on wildlife. Vehicle collisions are a top impact of roads on birds, with tens of millions of birds thought to be killed each year in the United States. However, currently available mortality estimates are extrapolated from a single study. We reviewed the literature and used 20 mortality rates extracted from 13 studies to systematically quantify data-driven estimates of annual U.S. mortality from bird-vehicle collisions. We generated 4 separate estimates along with uncertainty using different subsets of data deemed to be rigorous enough to contribute relatively little bias to estimates. All of our estimates of vehicle mortality are higher than previous U.S. figures. When averaging across model iterations, we estimated that between 89 and 340 million birds die annually from vehicle collisions on U.S. roads. Sensitivity analyses indicated that uncertainty about survey-related biases (scavenger removal and searcher detection of carcasses) contributes the greatest amount of uncertainty to our mortality estimates. Future studies should account for these biases to provide more accurate local estimates of mortality rates and to inform more precise national mortality estimates. We found relatively little information available to quantify regional, seasonal, and taxonomic patterns of vehicle collision risk, and substantial uncertainty remains about whether collisions contribute to large-scale impacts on bird populations. Nonetheless, the large magnitude of bird mortality caused by vehicle collisions combined with evidence that collisions can contribute to local population declines for some species highlights the need for implementation of conservation and management actions to reduce this mortality. Published 2014. This article is a U.S. Government work and is in the public domain in the USA. C1 [Loss, Scott R.; Marra, Peter P.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Will, Tom] US Fish & Wildlife Serv, Div Migratory Birds, Midwest Reg Off, Bloomington, MN 55437 USA. RP Loss, SR (reprint author), Oklahoma State Univ, Dept Nat Resource Ecol & Management, 008C Agr Hall, Stillwater, OK 74078 USA. EM scott.loss@okstate.edu FU U.S. Fish and Wildlife Service through the Smithsonian Institution's Postdoctoral Fellowship program FX We thank J. Rutter and R. Schneider for assisting with data compilation, management, and analysis. S. R. L. was supported by a postdoctoral fellowship funded by the U.S. Fish and Wildlife Service through the Smithsonian Institution's Postdoctoral Fellowship program. The findings and opinions expressed in this paper are those of the authors and do not necessarily reflect the opinions of the U.S. Fish and Wildlife Service, the Smithsonian Institution, or Oklahoma State University. NR 68 TC 18 Z9 18 U1 7 U2 84 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-541X EI 1937-2817 J9 J WILDLIFE MANAGE JI J. Wildl. Manage. PD JUL PY 2014 VL 78 IS 5 BP 763 EP 771 DI 10.1002/jwmg.721 PG 9 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA AJ8PB UT WOS:000337967100002 ER PT J AU Brown, DD Montgomery, RA Millspaugh, JJ Jansen, PA Garzon-Lopez, CX Kays, R AF Brown, D. D. Montgomery, R. A. Millspaugh, J. J. Jansen, P. A. Garzon-Lopez, C. X. Kays, R. TI Selection and spatial arrangement of rest sites within northern tamandua home ranges SO JOURNAL OF ZOOLOGY LA English DT Article DE tamandua; selection; telemetry; accelerometry; Panama; rest site; sleep ID MAMMAL MYRMECOPHAGA-TRIDACTYLA; RESOURCE SELECTION; SLEEPING SITES; UTILIZATION DISTRIBUTIONS; SAGUINUS-FUSCICOLLIS; SEXUAL SEGREGATION; HABITAT SELECTION; PREDATION RISK; PANTHERA-ONCA; TREE HOLES AB The distribution of suitable rest sites is considered to be a key determinant of spatial patterns in animal activity. However, it is not immediately evident which landscape features satisfy rest site requirements or how these sites are configured within the home range. We used Global Positioning System (GPS)/accelerometer telemetry to investigate rest site selection at the home-range scale for northern tamanduas Tamandua mexicana on Barro Colorado Island (BCI), Panama. We developed models specifying each tamandua as the individual experimental unit and averaged coefficients to produce population-level estimates. Tamanduas had on average 17.8 (+/- 8.1) rest sites within their home range and used 1.36 (+/- 0.51) on any given day. These rest sites tended to be located in the core of tamandua home ranges, with active locations associated with the periphery of the home range. Rest sites were positively associated with (1) a high density of Attalea butyracea palm trees; (2) elevation; (3) tall vegetation. There was a slight negative relationship between the distribution of rest sites and slope, and no apparent relationship between rest site selection and relative distance to forest canopy gaps. From focal animal observations, we identified that tamandua rest sites were typically located in trees (90%), with 25% (12 of 49) occurring in palms. We contend that northern tamanduas on BCI selected vegetated arboreal rest sites because of reduced likelihood of detection from terrestrial predators in these sites. Our models identified considerable individual variation in rest site selection, which suggests that the practice of pooling individuals and fitting models at an aggregate level may be inappropriate for certain types of habitat selection research. C1 [Brown, D. D.] Western Kentucky Univ, Dept Biol, Bowling Green, KY 42101 USA. [Montgomery, R. A.; Millspaugh, J. J.] Univ Missouri, Dept Fisheries & Wildlife Sci, Columbia, MO USA. [Montgomery, R. A.] Michigan State Univ, Dept Fisheries & Wildlife, E Lansing, MI 48824 USA. [Jansen, P. A.; Kays, R.] Smithsonian Trop Res Inst, Ancon Panama, Panama. [Jansen, P. A.] Wageningen Univ, Dept Environm Sci, NL-6700 AP Wageningen, Netherlands. [Garzon-Lopez, C. X.] Univ Groningen, Netherlands Community & Conservat Ecol, Groningen, Netherlands. [Garzon-Lopez, C. X.] Ctr Empresarial Potosi, Grp ARCO, Sopo, Colombia. [Kays, R.] North Carolina Museum Nat Sci, Raleigh, NC USA. [Kays, R.] N Carolina State Univ, Dept Fisheries Wildlife & Conservat, Raleigh, NC 27695 USA. RP Brown, DD (reprint author), Western Kentucky Univ, Dept Biol, 1906 Coll Hts Blvd 11080, Bowling Green, KY 42101 USA. EM danielle.brown@wku.edu RI Jansen, Patrick/G-2545-2015; Garzon-Lopez, Carol/G-6251-2014 OI Jansen, Patrick/0000-0002-4660-0314; Garzon-Lopez, Carol/0000-0002-4099-2740 FU Smithsonian Tropical Research Institute FX The authors wish to thank the Smithsonian Tropical Research Institute for funding the acquisition of LiDAR and high-resolution optical imagery of the Barro Colorado Nature Monument as well as Elena Lobo for facilitating the collection of the LiDAR data. They also wish to thank Sergio dos Santos of the Smithsonian Tropical Research Institute for facilitating access to the BCI weather station data. NR 83 TC 1 Z9 1 U1 3 U2 36 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0952-8369 EI 1469-7998 J9 J ZOOL JI J. Zool. PD JUL PY 2014 VL 293 IS 3 BP 160 EP 170 DI 10.1111/jzo.12131 PG 11 WC Zoology SC Zoology GA AJ8QX UT WOS:000337972800003 ER PT J AU Reitzel, K Turner, BL AF Reitzel, Kasper Turner, Benjamin L. TI Quantification of pyrophosphate in soil solution by pyrophosphatase hydrolysis SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Pyrophosphate; Phosphatase; Soil solution; Phosphorus; Tropical forests ID P-31 NMR-SPECTROSCOPY; ORGANIC PHOSPHORUS; MYCORRHIZAL FUNGI; PHOSPHATASE; FRACTIONS; ADDITIONS; EXTRACTS; FORMS; WATER; ACID AB A commercial pyrophosphatase from Saccharomyces cerevisiae selectively hydrolyzed sodium pyrophosphate, but showed no significant activity towards a range of other organic and condensed inorganic phosphorus compounds. Pyrophosphate determined by pyrophosphatase hydrolysis accounted for 38 +/- 12% (mean +/- standard error of 19 sites) of the non-reactive phosphorus in soil solution obtained by centrifugation from a series of lowland tropical rain forest soils. Pyrophosphate concentrations were up to 89 mu g P l(-1) and correlated positively with microbial phosphorus, soil solution pH, and native phosphomonoesterase activity in soil solution, but not with total soil pyrophosphate determined by NaOH-EDTA extraction and solution (31)p NMR spectroscopy. In summary, we identify pyrophosphate as a major constituent of soil solution phosphorus in lowland tropical rain forests, and demonstrate that a commercial pyrophosphatase can be used as a selective tool to quantify trace concentrations of pyrophosphate in soil solution. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Reitzel, Kasper] Univ Southern Denmark, Dept Biol, DK-5230 Odense M, Denmark. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Reitzel, K (reprint author), Univ Southern Denmark, Dept Biol, Campusvej 55, DK-5230 Odense M, Denmark. EM reitzel@biology.sdu.dk RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU Danish Council for Independent Research/Natural Sciences [1637604] FX We thank the Dayana Agudo and Julio Rodruigez for laboratory and field assistance. Kasper Reitzel was funded by grant #1637604 from the Danish Council for Independent Research/Natural Sciences. NR 23 TC 3 Z9 3 U1 3 U2 31 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-0717 J9 SOIL BIOL BIOCHEM JI Soil Biol. Biochem. PD JUL PY 2014 VL 74 BP 95 EP 97 DI 10.1016/j.soilbio.2014.03.001 PG 3 WC Soil Science SC Agriculture GA AJ7BZ UT WOS:000337853500010 ER PT J AU Sekerka, L Windsor, D Dury, G AF Sekerka, Lukas Windsor, Donald Dury, Guillaume TI Cladispa Baly: revision, biology and reassignment of the genus to the tribe Spilophorini (Coleoptera: Chrysomelidae: Cassidinae) SO SYSTEMATIC ENTOMOLOGY LA English DT Article ID PHYLOGENETIC ANALYSES; SUBSTITUTION; MODELS AB The genus, Cladispa Baly 1858, is transferred from the tribe Imatidiini (=Cephaloleiini Chapuis, 1875) to Spilophorini Chapuis, 1875 based on the review of type material, newly collected specimens and molecular phylogenetic analysis. The type species, C.quadrimaculata Baly, 1858, is redescribed, and two new species, C.amboroensis sp.n. from Bolivia (Santa Cruz Department) and C.ecuadorica sp.n. from Ecuador (Pastaza Province), are described and figured. The morphology of C.amboroensis sp.n. immature stages is broadly consistent with other Spilophorini. Field observations document that both C.quadrimaculata and C.amboroensis sp.n. are trophic specialists on Orchideaceae. Keys to Cladispa species and Spilophorini genera are provided. Trophic associations of other Cassidinae and Orchideaceae are discussed. This published work has been registered in ZooBank, http://zoobank.org/urn:lsid:zoobank.org:pub:42A1ECF3-2030-4938-8F3D-FE7EC36F303A C1 [Sekerka, Lukas] Natl Museum, Dept Entomol, CZ-14800 Prague, Czech Republic. [Sekerka, Lukas] Univ South Bohemia, Dept Zool, Fac Sci, Ceske Budejovice, Czech Republic. [Windsor, Donald; Dury, Guillaume] Smithsonian Trop Res Inst, Panama City, Panama. [Dury, Guillaume] McGill Univ, Dept Plant Sci, Quebec City, PQ, Canada. RP Sekerka, L (reprint author), Natl Museum, Dept Entomol, Golcova 1, CZ-14800 Prague, Czech Republic. EM sagrinae@seznam.cz FU Faculty of Science, University of South Bohemia; Ministry of Culture of the Czech Republic (DKRVO, National Museum) FX We thank M. Barclay (BMNH) and S. Konstantinov (USNM) for loaned material used in this study; P. Jolivet (Paris) for clarifying information on the C. quadrimaculata feeding record; A. Murakami (MNKM) and R. Vasquez (Sociedad Boliviana de Botanica) for identification of Xylobium; J. Ledezma (MNKM), J. Aramayo (MNKM), A. Schweining (RLV) and G. Herrera for institutional support and assistance in obtaining collecting and export permits (MMAyA-VMA-DGBAP No 1735/2011, MHNNKM-OF- No 441/2012). The Smithsonian Tropical Research Institute provided logistical support through its imaging laboratory and the services of J. Ceballos. The field study of L. Sekerka in Bolivia was supported by the Faculty of Science, University of South Bohemia. The work was partly supported by the Ministry of Culture of the Czech Republic (DKRVO 2014/13, National Museum, 00023272). NR 29 TC 2 Z9 2 U1 0 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0307-6970 EI 1365-3113 J9 SYST ENTOMOL JI Syst. Entomol. PD JUL PY 2014 VL 39 IS 3 BP 518 EP 530 DI 10.1111/syen.12070 PG 13 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA AJ8TC UT WOS:000337979500011 ER PT J AU Datovo, A Vari, RP AF Datovo, Alessio Vari, Richard P. TI The adductor mandibulae muscle complex in lower teleostean fishes (Osteichthyes: Actinopterygii): comparative anatomy, synonymy, and phylogenetic implications SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE jaw muscles; musculature; myology; Neoteleostei; Teleostei ID WHOLE MITOGENOME SEQUENCES; PECTORAL GIRDLE MUSCLES; CEPHALIC REGION; CHARACIFORM FISHES; CATFISH TELEOSTEI; SILURIFORMES AUTAPOMORPHIES; CRANIAL MORPHOLOGY; CLARIAS-GARIEPINUS; CHEEK MUSCLES; OSTEOLOGY AB Bony fishes of the morphologically diverse infraclass Teleostei include more than 31000 species, encompassing almost one-half of all extant vertebrates. A remarkable anatomical complex in teleosts is the adductor mandibulae, the primary muscle in mouth closure and whose subdivisions vary in number and complexity. Difficulties in recognizing homologies amongst adductor mandibulae subdivisions across the Teleostei have hampered the understanding of the evolution of this system and consequently its application in phylogenetic analyses. The adductor mandibulae in representatives of all lower teleost orders is described, illustrated, and compared based on broad taxonomic sampling complemented by extensive literature information. Muscle division homologies are clarified via the application of a standardized homology-driven anatomical terminology with synonymies provided to the myological terminologies of previous studies. Phylogenetic implications of the observed variations in the adductor mandibulae are discussed and new possible synapomorphies are proposed for the Notacanthiformes, Ostariophysi, Cypriniformes, Siluriphysi, Gymnotiformes, and Alepocephaloidei. New characters corroborate the putative monophyly of the clades Albuliformes plus Notacanthiformes (Elopomorpha), Argentinoidei plus Esocoidei plus Salmonoidei (Protacanthopterygii) and Hemiodontidae plus Parodontidae (Characiformes). We further confirm the validity of characters from the adductor mandibulae previously proposed to support the monophyly of the Esocoidei and the gonorynchiform clade Gonorynchoidei plus Knerioidei. (c) 2014 The Linnean Society of London C1 [Datovo, Alessio] Univ Sao Paulo, Museu Zool, BR-04263000 Sao Paulo, Brazil. [Datovo, Alessio] Univ Sao Paulo, Lab Ictiol Ribeirao Preto, Dept Biol, FFCLRP, BR-14040901 Ribeirao Preto, SP, Brazil. [Datovo, Alessio; Vari, Richard P.] Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Datovo, A (reprint author), Univ Sao Paulo, Lab Ictiol, Museu Zool, Av Nazare 481, BR-04263000 Sao Paulo, Brazil. EM adatovo@gmail.com RI Datovo, Alessio/K-7133-2016; Museu de Zoologia da USP, MZ-USP/Q-2192-2016 FU Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) [2006/56445-7, 2010/18984-9]; Herbert R and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes, National Museum of Natural History, Smithsonian Institution; FAPESP [2004/09219-6, 2009/54931-0, 2011/50282-7] FX Research associated with this study was supported by fellowships from the Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP #2006/56445-7 and #2010/18984-9) and funding from the Herbert R and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes, National Museum of Natural History, Smithsonian Institution. This project was a component of A. D.'s doctoral program in Biologia Comparada at the FFCLRP, Departamento de Biologia, Universidade de Sao Paulo. Claudio Oliveira (LBP) and Scott Schaefer (AMNH) generously loaned important material used in this study. Special thanks are due to Sandra J. Raredon (USNM) for her assistance in photographing various specimens and to Luciana F. Tosin in translating texts from German and editing some images. Ricardo M. C. Castro (LIRP), Flavio A. Bockmann (LIRP), G. David Johnson (USNM), and Monica Toledo-Piza (Instituto de Biociencias, Universidade de Sao Paulo) kindly allowed the use of stereomicroscopic photographic equipment under their care. This paper benefitted from the careful and constructive reviews by Peter Konstantinidis, a second anonymous reviewer, and the Associate Editor. The comprehensive coverage of the literature presented in this study was only possible because of the initiatives of online open-access distribution of classic scientific papers, especially the Biodiversity Heritage Library and the Internet Archive projects. Equipment used in this study was provided by projects from FAPESP (#2004/09219-6, #2009/54931-0, and #2011/50282-7). NR 198 TC 8 Z9 9 U1 0 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 EI 1096-3642 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD JUL PY 2014 VL 171 IS 3 BP 554 EP 622 DI 10.1111/zoj.12142 PG 69 WC Zoology SC Zoology GA AJ9FC UT WOS:000338012000004 ER PT J AU Deluycker, AM AF Deluycker, Anneke M. TI EVOLUTIONARY BIOLOGY AND CONSERVATION OF TITIS, SAKIS, AND UACARIS SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Book Review C1 [Deluycker, Anneke M.] Smithsonian Mason Sch Conservat, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Deluycker, AM (reprint author), Smithsonian Mason Sch Conservat, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 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 JUL PY 2014 VL 154 IS 3 BP 467 EP 468 DI 10.1002/ajpa.22515 PG 3 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AJ4CX UT WOS:000337619200016 ER PT J AU Chisholm, RA Condit, R Abd Rahman, K Baker, PJ Bunyavejchewin, S Chen, YY Chuyong, G Dattaraja, HS Davies, S Ewango, CEN Gunatilleke, CVS Gunatilleke, IAUN Hubbell, S Kenfack, D Kiratiprayoon, S Lin, YC Makana, JR Pongpattananurak, N Pulla, S Punchi-Manage, R Sukumar, R Su, SH Sun, IF Suresh, HS Tan, S Thomas, D Yap, S AF Chisholm, Ryan A. Condit, Richard Abd Rahman, K. Baker, Patrick J. Bunyavejchewin, Sarayudh Chen, Yu-Yun Chuyong, George Dattaraja, H. S. Davies, Stuart Ewango, Corneille E. N. Gunatilleke, C. V. S. Gunatilleke, I. A. U. Nimal Hubbell, Stephen Kenfack, David Kiratiprayoon, Somboon Lin, Yiching Makana, Jean-Remy Pongpattananurak, Nantachai Pulla, Sandeep Punchi-Manage, Ruwan Sukumar, Raman Su, Sheng-Hsin Sun, I-Fang Suresh, H. S. Tan, Sylvester Thomas, Duncan Yap, Sandra TI Temporal variability of forest communities: empirical estimates of population change in 4000 tree species SO ECOLOGY LETTERS LA English DT Article DE Abundance fluctuations; biodiversity; demographic stochasticity; environmental variance; forest dynamics; neutral theory; niche stabilization ID TROPICAL FOREST; NEUTRAL-THEORY; DENSITY-DEPENDENCE; NEOTROPICAL FOREST; TIME-SERIES; LARGE-SCALE; DIVERSITY; DYNAMICS; BIODIVERSITY; ABUNDANCE AB Long-term surveys of entire communities of species are needed to measure fluctuations in natural populations and elucidate the mechanisms driving population dynamics and community assembly. We analysed changes in abundance of over 4000 tree species in 12 forests across the world over periods of 6-28years. Abundance fluctuations in all forests are large and consistent with population dynamics models in which temporal environmental variance plays a central role. At some sites we identify clear environmental drivers, such as fire and drought, that could underlie these patterns, but at other sites there is a need for further research to identify drivers. In addition, cross-site comparisons showed that abundance fluctuations were smaller at species-rich sites, consistent with the idea that stable environmental conditions promote higher diversity. Much community ecology theory emphasises demographic variance and niche stabilisation; we encourage the development of theory in which temporal environmental variance plays a central role. C1 [Chisholm, Ryan A.; Condit, Richard; Hubbell, Stephen] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Chisholm, Ryan A.] Natl Univ Singapore, Dept Biol Sci, Fac Sci, Singapore 117543, Singapore. [Abd Rahman, K.] Forest Res Inst Malaysia, Kepong 52109, Selangor Darul, Malaysia. [Baker, Patrick J.] Univ Melbourne, Dept Forest & Ecosyst Sci, Richmond, Vic 3121, Australia. [Bunyavejchewin, Sarayudh] Dept Natl Pk Wildlife & Plant Conservat, Res Off, Bangkok 10900, Thailand. [Chen, Yu-Yun; Sun, I-Fang] Natl Dong Hwa Univ, Dept Nat Resources & Environm Studies, Hualien 97401, Taiwan. [Chuyong, George] Univ Buea, Dept Bot & Plant Physiol, Buea, Swp, Cameroon. [Dattaraja, H. S.; Pulla, Sandeep; Sukumar, Raman; Suresh, H. S.] Indian Inst Sci, Ctr Ecol Sci, Bangalore 560012, Karnataka, India. [Davies, Stuart; Kenfack, David; Tan, Sylvester] Smithsonian Inst, Smithsonian Inst Global Earth Observ, Ctr Trop Forest Sci, Washington, DC 20013 USA. [Ewango, Corneille E. N.; Makana, Jean-Remy] Wildlife Conservat Soc, Kinshasa, Zaire. [Gunatilleke, C. V. S.; Gunatilleke, I. A. U. Nimal] Univ Peradeniya, Dept Bot, Fac Sci, Peradeniya 20400, Sri Lanka. [Hubbell, Stephen] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Kiratiprayoon, Somboon] Thammasat Univ Rangsit, Fac Sci & Technol, Klongluang, Patumtani, Thailand. [Lin, Yiching] Tunghai Univ, Dept Life Sci, Taichung 40704, Taiwan. [Pongpattananurak, Nantachai] Kasetsart Univ, Dept Forest Biol, Fac Forestry, Bangkok 10900, Thailand. [Punchi-Manage, Ruwan] Univ Gottingen, Dept Ecosyst Modeling, D-37077 Gottingen, Germany. [Su, Sheng-Hsin] Taiwan Forestry Res Inst, Taipei 10066, Taiwan. [Thomas, Duncan] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [Yap, Sandra] Univ Philippines, Inst Biol, Quezon City 1101, Philippines. RP Chisholm, RA (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Ancon, Panama. EM ryan.chis@gmail.com RI Chisholm, Ryan/H-8033-2012; OI Baker, Patrick/0000-0002-6560-7124 NR 49 TC 18 Z9 19 U1 6 U2 75 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 JUL PY 2014 VL 17 IS 7 BP 855 EP 865 DI 10.1111/ele.12296 PG 11 WC Ecology SC Environmental Sciences & Ecology GA AJ2ZP UT WOS:000337534600010 PM 24805976 ER PT J AU Woodman, N Gaffney, SA AF Woodman, Neal Gaffney, Sarah A. TI Can They Dig It? Functional Morphology and Semifossoriality Among Small-Eared Shrews, Genus Cryptotis (Mammalia, Soricidae) SO JOURNAL OF MORPHOLOGY LA English DT Article DE burrowing; Eulipotyphla; fossoriality; insectivora; Neurotrichus; Soricomorpha; Talpidae; Uropsilus ID INTRINSIC HAND PROPORTIONS; FOSSORIAL ADAPTATIONS; CENTRAL-AMERICA; SORICOMORPHA; GUATEMALA; MARSUPIALS; HIGHLANDS; FORELIMB; RODENTS AB Small-eared shrews (Mammalia: Soricidae: Cryptotis), exhibit modifications of the forelimb skeleton that have been interpreted as adaptations for semifossoriality. Most species inhabit remote regions, however, and their locomotory and foraging behaviors remain mostly speculative. To better understand the morphological modifications in the absence of direct observations, we quantified variation in these species by measuring 151 individuals representing 18 species and populations of Cryptotis and two species of moles (Talpidae) for comparison. From our measurements, we calculated 22 indices, most of which have been used previously to characterize substrate use among rodents and other taxa. We analyzed the indices using 1) average percentile ranks, 2) principal components analysis, and 3) cluster analysis. From these analyses, we determined that three basic modes of substrate adaptation are present within Cryptotis: 1) a primarily terrestrial mode, with species that are capable of burrowing, but lack adaptations to increase digging efficiency, 2) a semi-fossorial mode, with species whose forelimbs bones show strong muscle attachment areas and increased mechanical advantage, and 3) an intermediate mode. In addition to identifying new morphological characters and contributing to our understanding of the functional morphology of soricids, these analyses provide additional insight into the ecology of the species of interest. (C) 2014 Wiley Periodicals, Inc. C1 [Woodman, Neal] Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. [Gaffney, Sarah A.] Smith Coll, Dept Biol Sci, Northampton, MA 01063 USA. RP Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. EM woodmann@si.edu OI Woodman, Neal/0000-0003-2689-7373 FU National Science Foundation - Natural History Research Experiences program of the USNM FX Contract grant sponsor: SAG was supported by the National Science Foundation-funded Natural History Research Experiences program of the USNM. NR 42 TC 7 Z9 7 U1 4 U2 12 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 JUL PY 2014 VL 275 IS 7 BP 745 EP 759 DI 10.1002/jmor.20254 PG 15 WC Anatomy & Morphology SC Anatomy & Morphology GA AJ4SR UT WOS:000337666700003 PM 24470078 ER PT J AU Galindo, LA Puillandre, N Strong, EE Bouchet, P AF Galindo, L. A. Puillandre, N. Strong, E. E. Bouchet, P. TI Using microwaves to prepare gastropods for DNA barcoding SO MOLECULAR ECOLOGY RESOURCES LA English DT Article DE DNA damage; PCR optimization; shelled molluscs; tissue preparation; voucher ID EXTRACTION; INVERTEBRATES; SPECIMENS; BACTERIA; SOIL AB Extracting DNA from gastropods presents particular difficulties due to the capacity of the living animal to retract into the shell, resulting in poor penetration of the ethanol into the tissues. Because the shell is essential to establish the link between sequences and traditional taxonomic identity, cracking the shell to facilitate fixation is not ideal. Several methods are currently in routine use to overcome this difficulty, including chemical relaxation, drilling the shell and boiling. Most of these methods are time-consuming, may be safety hazards and constitute a bottleneck in the preparation of large numbers of specimens in the field. We have experimented with a method traditionally used to clean shells that involves placing the living gastropods in a microwave (MW) oven; the electromagnetic radiation very quickly heats both the animal and the water trapped inside the shell, resulting in separation of the muscles that anchor the animal to the shell. Done properly, the body can be removed intact from the shell and the shell voucher is preserved undamaged. To test the method, the bodies of live-collected specimens from two gastropod species were separated from their shell by microwaving and by anesthetizing/drilling. After identical extraction and PCR procedures, the gels showed no difference in DNA quantity or quality, and the resulting sequences are identical within species. The method was then implemented on a large scale during expeditions, resulting in higher percentage of DNA extraction success. The MWs are also effective for quickly and easily removing other molluscs from their shells, that is, bivalves and scaphopods. Workflows implementing the MW technique show a three- to fivefold increase in productivity compared with other methods. C1 [Galindo, L. A.; Puillandre, N.; Bouchet, P.] Museum Natl Hist Nat, Dept Systemat & Evolut, ISyEB Inst UMR CNRS UPMC MNHN EPHE 7205, F-75231 Paris, France. [Strong, E. E.] Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20560 USA. RP Galindo, LA (reprint author), Museum Natl Hist Nat, Serv Systemat Mol, 43 Rue Cuvier, F-75005 Paris, France. EM galindo@mnhn.fr OI Strong, Ellen/0000-0001-7181-4114 NR 27 TC 11 Z9 12 U1 1 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1755-098X EI 1755-0998 J9 MOL ECOL RESOUR JI Mol. Ecol. Resour. PD JUL PY 2014 VL 14 IS 4 BP 700 EP 705 DI 10.1111/1755-0998.12231 PG 6 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA AJ4AM UT WOS:000337611400003 PM 24450943 ER PT J AU Pizano, C Mangan, SA Graham, JH Kitajima, K AF Pizano, Camila Mangan, Scott A. Graham, James H. Kitajima, Kaoru TI Habitat-specific positive and negative effects of soil biota on seedling growth in a fragmented tropical montane landscape SO OIKOS LA English DT Article ID ARBUSCULAR MYCORRHIZAL FUNGI; NEOTROPICAL TREE SEEDLINGS; COMMUNITY STRUCTURE; SHADE TOLERANCE; PLANT; FEEDBACK; MUTUALISTS; PATHOGENS; ABUNDANCE; RESPONSES AB Soil biota, in particular fungi and other microbes, are known to interactively influence plant community structure. However, soil biota effects that can be isolated in a greenhouse experiment may be overridden by other biotic and abiotic factors in the field. Here we conducted parallel greenhouse and field experiments and quantified how soil biota sampled at the habitat level affect the performance of potential host plants within and across neighboring habitat types (pastures, coffee plantations and forest fragments) in a montane region in Colombia. We hypothesized that the direction and strength of soil-biota effects depend on the habitat where soil is sampled, focal plant's life history, and field environmental characteristics (soil nutrients, light). In a greenhouse experiment, we compared growth of 10 plant species with soil from home (where species typically occur) and foreign (where conspecific adults rarely occur) habitats, with or without soil sterilization. In the field, we conducted a reciprocal transplant experiment in which we suppressed soil fungi with the application of fungicide. In the greenhouse experiment, fast-growing pasture grass and pioneer trees performed less well with live soil from their home, compared to foreign habitats, and such home disadvantage was reduced following soil sterilization. Home disadvantage associated with live soil biota was also detectable in the field experiment, although light conditions of grasslands and coffee plantations benefited growth of these fast-growing species. In contrast, coffee and shade-tolerant trees performed similarly or better with their home soils, and showed no response to soil biota suppression. Overall, the species-and-habitat specific soil biota effects detectable in the field experiment were similar in direction and relative strength to those from the greenhouse experiments. Our findings highlight the importance of habitat-level plant-soil interactions and plant life history for the regeneration of natural forests and agricultural production in human-modified landscapes. C1 [Pizano, Camila; Kitajima, Kaoru] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Mangan, Scott A.] Washington Univ, Dept Biol, St Louis, MO 63130 USA. [Mangan, Scott A.] Smithsonian Trop Res Inst, Balboa, Panama. [Graham, James H.] Univ Florida, Citrus Res & Educ Ctr, Lake Alfred, FL 33850 USA. RP Pizano, C (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM pizanoc@ufl.edu FU Compton Foundation; Univ. of Florida Program for Studies in Tropical Conservation; Aerolineas Aeropobre; Compton Fellowship FX This study was funded by the Compton Fellowship granted by the Compton Foundation and the Univ. of Florida Program for Studies in Tropical Conservation to CP, and by Aerolineas Aeropobre. We are grateful to Jorge Botero and Gabriel Cadena for their critical institutional support, and Hector Vargas for his help with the set up and harvesting of greenhouse and field experiments. We are also grateful to the farmers that allowed us to carry out this work on their land and provided relevant information, and to W. van der Putten who significantly improved this manuscript. The authors declare no conflict of interest. NR 50 TC 4 Z9 4 U1 11 U2 87 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 JUL PY 2014 VL 123 IS 7 BP 846 EP 856 DI 10.1111/oik.01032 PG 11 WC Ecology SC Environmental Sciences & Ecology GA AJ5RP UT WOS:000337744900010 ER PT J AU Almeida, C Ortega, H Higginbotham, S Spadafora, C Arnold, AE Coley, PD Kursar, TA Gerwick, WH Cubilla-Rios, L AF Almeida, C. Ortega, H. Higginbotham, S. Spadafora, C. Arnold, A. E. Coley, P. D. Kursar, T. A. Gerwick, W. H. Cubilla-Rios, L. TI Chemical and bioactive natural products from Microthyriaceae sp., an endophytic fungus from a tropical grass SO LETTERS IN APPLIED MICROBIOLOGY LA English DT Article DE antiparasitic activity; endophytic fungi; integrasone B; sterigmatocystin ID STERIGMATOCYSTIN; INTEGRASE; DIVERSITY; MICROORGANISMS; HOST AB In screening for natural products with antiparasitic activity, an endophytic fungus, strain F2611, isolated from above-ground tissue of the tropical grass Paspalum conjugatum (Poaceae) in Panama, was chosen for bioactive principle elucidation. Cultivation on malt extract agar (MEA) followed by bioassay-guided chromatographic fractionation of the extract led to the isolation of the new polyketide integrasone B (1) and two known mycotoxins, sterigmatocystin (2) and secosterigmatocystin (3). Sterigmatocystin (2) was found to be the main antiparasitic compound in the fermentation extract of this fungus, possessing potent and selective antiparasitic activity against Trypanosoma cruzi, the cause of Chagas disease, with an IC50 value of 0 center dot 13moll-1. Compounds 2 and 3 showed high cytotoxicity against Vero cells (IC50 of 0 center dot 06 and 0 center dot 97moll-1, respectively). The new natural product integrasone B (1), which was co-purified from the active fractions, constitutes the second report of a natural product possessing an epoxyquinone with a lactone ring and exhibited no significant biological activity. Strain F2611 represents a previously undescribed taxon within the Microthyriaceae (Dothideomycetes, Ascomycota). C1 [Almeida, C.; Ortega, H.; Cubilla-Rios, L.] Univ Panama, Fac Nat Exact Sci & Technol, Lab Trop Bioorgan Chem, Panama City, Panama. [Almeida, C.; Ortega, H.; Higginbotham, S.; Coley, P. D.; Kursar, T. A.; Cubilla-Rios, L.] Smithsonian Trop Res Inst, Panama City, Panama. [Almeida, C.] Univ Lisbon, Fac Ciencias, Ctr Biodiversidade Genom Integrat & Func BioFIG, Lisbon, Portugal. [Spadafora, C.] City Knowledge, Natl Secretariat Sci Technol & Innovat, Inst Adv Sci Invest & High Technol Serv, Panama City, Panama. [Arnold, A. E.] Univ Arizona, Sch Plant Sci, Tucson, AZ USA. [Coley, P. D.; Kursar, T. A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Gerwick, W. H.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biotechnol & Biomed, La Jolla, CA 92093 USA. [Gerwick, W. H.] Univ Calif San Diego, Scripps Inst Oceanog, Skaggs Sch Pharm & Pharmaceut Sci, La Jolla, CA 92093 USA. RP Almeida, C (reprint author), Edificio ICAT TecLabs,Campus FCUL, P-1749016 Lisbon, Portugal. EM celsoguerreiro@gmail.com; luis.cubilla@up.ac.pa OI Almeida, Celso/0000-0002-5935-612X; Spadafora, Carmenza/0000-0002-3002-9467 FU US NIH [2 U01 TW006634-06]; College of Agriculture and Life Sciences at the University of Arizona; National Institute of Mental Health's Psychoactive Drug Screening Program [HHSN-271-2008-00025-C] FX This work was supported by a US NIH grant for the International Cooperative Biodiversity Groups program (ICBG-Panama; 2 U01 TW006634-06). We thank Malkanthi Gunatilaka and Douglas Mahana for DNA sequencing, and the College of Agriculture and Life Sciences at the University of Arizona for logistical and financial support. We thank Mathieu Metifiot (Center for Cancer Research, NCI/NIH, USA) for providing the HIV integrase assays. We thank Panama's Autoridad Nacional del Ambiente for facilitating this research. The Ki determinations and antagonist functional data were generously provided by the National Institute of Mental Health's Psychoactive Drug Screening Program, Contract # HHSN-271-2008-00025-C (NIMH PDSP) directed by Bryan L. Roth MD, PhD at the University of North Carolina at Chapel Hill and Jamie Driscol at NIMH, Bethesda, MD, USA. NR 25 TC 2 Z9 2 U1 2 U2 37 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0266-8254 EI 1472-765X J9 LETT APPL MICROBIOL JI Lett. Appl. Microbiol. PD JUL PY 2014 VL 59 IS 1 BP 58 EP 64 DI 10.1111/lam.12245 PG 7 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA AJ3ZU UT WOS:000337609000008 PM 24612068 ER PT J AU Torres, IC Turner, BL Reddy, KR AF Torres, Isabela C. Turner, Benjamin L. Reddy, K. Ramesh TI The Chemical Nature of Phosphorus in Subtropical Lake Sediments SO AQUATIC GEOCHEMISTRY LA English DT Article DE Phosphorus; Sediment; Solution P-31 NMR spectroscopy; Sequential fractionation; Polyphosphate; Subtropical; Florida ID SOIL ORGANIC PHOSPHORUS; P-31 NMR; INORGANIC PHOSPHORUS; BIOGENIC PHOSPHORUS; HYPEREUTROPHIC LAKE; EUTROPHIC LAKES; FLORIDA LAKES; WETLAND SOILS; TROPHIC STATE; POLYPHOSPHATE AB The phosphorus (P) composition of sediment profiles in three subtropical lakes of contrasting trophic state in Florida, USA, was determined by sequential fractionation and solution P-31 NMR spectroscopy. Sediment from Lake Annie, an oligo-mesotrophic sinkhole with moderately acidic sediment (pH 5.4; loss on ignition 58 %), contained higher total P concentrations than sediment from eutrophic Lake Okeechobee (pH 7.7, loss on ignition 36 %) and hyper-eutrophic Lake Apopka (pH 7.5, loss on ignition 69 %). The chemical nature of sediment P varied markedly among the three lakes, suggesting the predominance of different diagenetic processes. Lake Okeechobee sediment was dominated by inorganic P, indicating the dominance of abiotic reactions; Lake Annie sediment contained abundant organic P throughout the sediment profile, indicating the importance of organic P stabilization at acidic pH; Lake Apopka contained almost half of its sediment P in microbial biomass, indicating the importance of biotic processes in regulating P dynamics. Solution P-31 NMR spectroscopy of NaOH-EDTA extracts revealed that organic P occurred mainly as phosphomonoesters in all lakes. However, sediment from Lake Apopka also contained abundant phosphodiesters and was the only lake to contain detectable concentrations of polyphosphate, perhaps due to a combination of alternating redox conditions and high concentrations of inorganic phosphate and organic carbon. Organic P concentrations determined by sequential fractionation and solution P-31 NMR spectroscopy were similar for all lakes when microbial P was included in values for sequential fractionation. We conclude that the chemical nature of sediment P varies markedly depending on trophic state and can provide important information on the dominant processes controlling P cycling in subtropical lakes. C1 [Torres, Isabela C.; Reddy, K. Ramesh] Univ Florida, Soil & Water Sci Dept, Wetland Biogeochem Lab, Gainesville, FL 32611 USA. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, 0843-03092 Apartado, Balboa, Ancon, Panama. EM TurnerBL@si.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU USDA-CREES National Research Initiative [2004-35107-14918] FX This work was funded in part by funded by a grant from the USDA-CREES National Research Initiative (No. 2004-35107-14918). We thank Matt Fisher, Jason Smith, Andrea Albertin, and Kathleen McKee for assistance in the field, and Yu Wang, Jeremy Bright, and Alex Blumenfeld for laboratory support. NR 69 TC 10 Z9 11 U1 3 U2 33 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1380-6165 EI 1573-1421 J9 AQUAT GEOCHEM JI Aquat. Geochem. PD JUL PY 2014 VL 20 IS 4 BP 437 EP 457 DI 10.1007/s10498-014-9228-9 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AI6KN UT WOS:000336983000004 ER PT J AU Chin, SW Shaw, J Haberle, R Wen, J Potter, D AF Chin, Siew-Wai Shaw, Joey Haberle, Rosemarie Wen, Jun Potter, Dan TI Diversification of almonds, peaches, plums and cherries - Molecular systematics and biogeographic history of Prunus (Rosaceae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Boreotropical flora; Intercontinental disjunction; Rosaceae; Prunus; Biogeography; Phylogeny ID DISPERSAL-VICARIANCE ANALYSIS; EASTERN NORTH-AMERICA; DNA-SEQUENCES; PHYLOGENETIC ANALYSIS; LIKELIHOOD APPROACH; WASHINGTON-STATE; BRITISH-COLUMBIA; DIVERGENCE TIMES; MADDENIA CLADE; ABSOLUTE RATES AB Most previous molecular phylogenetic studies of Prunus have been conducted primarily with crop species and their close relatives. As the center of crop diversity of the genus is in Eurasia, the geographic origin of Prunus has inevitably been inferred to be Eurasia as well. The lesser-known tropical Prunus species have not been well represented in previous phylogenetic reconstructions; therefore, their effects on inferences about the phylogenetic structure and geographic origin of Prunus are uncertain. In this study, we examined the phylogeny of Prunus, including an expanded sampling of species from tropical regions in Southeast Asia and the Americas, using sequences from four plastid markers and the nuclear ribosomal ITS region. A penalized likelihood method was used to estimate the absolute age of Prunus and the timing of infrageneric cladogenic events. The geographic origin of Prunus and ancestral sites of cladogenesis were inferred using the Bayes-DIVA approach. Our results indicate that the modern genus appeared similar to 61 Myr in eastern Asia and that diversification of all major lineages may have been triggered by the global warming period of the early Eocene. In addition, our molecular dating estimates suggest that the crown clade that includes the temperate deciduous crop species is older than the one that includes the tropical evergreen species, while incongruence between plastid and nuclear phylogenies suggests that the latter lineage originated via an ancient hybridization event. The most recent common ancestor (MRCA) of the temperate crop species was a component of the continuous boreotropical forests of the Northern Hemisphere, while the MRCA of the tropical species represented the last remains of the boreotropical elements and subsequently radiated throughout the Old and New World tropics from refugial areas at lower latitudes. Complex biogeographic histories leading to the present global distribution of the genus were driven by several geologic events, climatic oscillations, and independent dispersals across continents via the Bering and the North Atlantic Land Bridges during different geologic time periods. (C) 2014 Elsevier Inc. All rights reserved. C1 [Chin, Siew-Wai; Potter, Dan] Univ Calif Davis, Dept Plant Sci, Davis, CA 95616 USA. [Shaw, Joey] Univ Tennessee, Dept Biol & Environm Sci, Chattanooga, TN 37403 USA. [Haberle, Rosemarie] Pacific Lutheran Univ, Dept Biol, Tacoma, WA 98447 USA. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Chin, SW (reprint author), Univ Calif Davis, Dept Plant Sci, MS2, Davis, CA 95616 USA. EM csiewwai@ucdavis.edu FU NSF [DEB 0515431] FX The study is part of S-W Chin's doctoral dissertation at the University of California, Davis. We thank Elizabeth Widjaja (Herbarium Bogoriense) for assistance with fieldwork in Indonesia. This work was supported by NSF grant number DEB 0515431. NR 88 TC 17 Z9 19 U1 11 U2 76 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 JUL PY 2014 VL 76 BP 34 EP 48 DI 10.1016/j.ympev.2014.02.024 PG 15 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA AI4FJ UT WOS:000336820800005 PM 24631854 ER PT J AU Johnson, AEM Freeman, EW Colgin, M McDonough, C Songsasen, N AF Johnson, Amy E. M. Freeman, Elizabeth W. Colgin, Mark McDonough, Caitlin Songsasen, Nucharin TI Induction of ovarian activity and ovulation in an induced ovulator, the maned wolf (Chrysocyon brachyurus), using GnRH agonist and recombinant LH SO THERIOGENOLOGY LA English DT Article DE Maned wolf; Induced ovulator; Ovarian steroid; Canid reproduction; Estrus induction ID LAPAROSCOPIC ARTIFICIAL-INSEMINATION; LUTEINIZING-HORMONE; DESLORELIN IMPLANTS; ESTRUS INDUCTION; DOMESTIC CAT; ASSISTED REPRODUCTION; CLOUDED LEOPARD; FELIDS; GONADOTROPIN; BITCHES AB Assisted reproductive techniques, such as ovarian manipulation and artificial insemination, are useful for enhancing genetic management of threatened wildlife maintained ex situ. In this study, we used noninvasive fecal hormone monitoring to investigate (1) the influence of pairing with a male on endocrine responses of female maned wolves (Chrysocyon brachyurus) to a GnRH agonist (deslorelin) and (2) the efficiency of recombinant LH (reLH) on ovulation induction in females housed alone. Deslorelin (2.1 mg Ovuplant) was given to females that were either paired with a male (n = 4) or housed alone (n = 7); the implant was removed 7 to 11 days postimplantation. Three of seven singleton females were injected with reLH (0.0375 mg) on the day of implant removal, whereas the remaining females (n = 4) did not receive the additional treatment. Fecal samples were collected 5 to 7 days/wk from all females starting 11 days prior to hormone insertion until at least 70 days post implant removal for a total of 11 hormone treatment cycles. Fecal estrogen and progestagen metabolites were extracted and analyzed by enzyme immunoassay. Evidence of ovulation, demonstrated by a surge of estrogen followed by a significant rise in progestagen, occurred in all paired females. Three of the four singleton females that did not receive reLH treatment exhibited no rise in progestagen after an estrogen surge. All singleton females treated with reLH exhibited a rise in fecal progestagen after injection, indicating ovulation. In conclusion, deslorelin is effective at inducing ovarian activity and ovulation in paired female maned wolves; however, exogenous reLH is needed to induce ovulation in females housed alone. The findings obtained from this study serve as a foundation for future application of artificial insemination to enhance genetic management of this threatened species ex situ. Published by Elsevier Inc. C1 [Johnson, Amy E. M.; McDonough, Caitlin; Songsasen, Nucharin] Natl Zool Park, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Johnson, Amy E. M.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Freeman, Elizabeth W.] George Mason Univ, New Century Coll, Fairfax, VA 22030 USA. [Colgin, Mark] AspenBio Pharma Inc, Venaxis Inc, Castle Rock, CO USA. RP Songsasen, N (reprint author), Natl Zool Park, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. EM songsasenn@si.edu OI Johnson, Amy/0000-0002-9288-1305 FU Morris Animal Foundation; George Mason University FX This study was supported by the Morris Animal Foundation. We also thank George Mason University for supporting a portion of the graduate student stipend for A.E.M. Johnson. The authors thank animal care and veterinary staff from the White Oak Conservation Center, Fossil Rim Wildlife Center, Houston Zoological Park, Dickerson Park Zoo and the Smithsonian Conservation Biology Institute for their assistance in this project. Finally, we are extremely grateful to AspenBio Pharma for kindly providing recombinant LH for this study. NR 42 TC 3 Z9 3 U1 2 U2 23 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 JUL 1 PY 2014 VL 82 IS 1 BP 71 EP 79 DI 10.1016/j.theriogenology.2014.03.009 PG 9 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA AI6SA UT WOS:000337006100010 PM 24742964 ER PT J AU Tennyson, J Bernath, PF Brown, LR Campargue, A Csaszar, AG Daumont, L Gamache, RR Hodges, JT Naumenko, OV Polyansky, OL Rothman, LS Vandaele, AC Zobov, NF Denes, N Fazliev, AZ Furtenbacher, T Gordon, IE Hu, SM Szidarovszky, T Vasilenko, IA AF Tennyson, Jonathan Bernath, Peter F. Brown, Linda R. Campargue, Alain Csaszar, Attila G. Daumont, Ludovic Gamache, Robert R. Hodges, Joseph T. Naumenko, Olga V. Polyansky, Oleg L. Rothman, Laurence S. Vandaele, Ann Carine Zobov, Nikolai F. Denes, Nora Fazliev, Alexander Z. Furtenbacher, Tibor Gordon, Iouli E. Hu, Shui-Ming Szidarovszky, Tamas Vasilenko, Irina A. TI IUPAC critical evaluation of the rotational-vibrational spectra of water vapor. Part IV. Energy levels and transition wavenumbers for (D2O)-O-16, (D2O)-O-17, and (D2O)-O-18 SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Water vapor; Transition wavenumbers; Atmospheric physics; Energy levels; Spectroscopic information system ID LASER-ABSORPTION SPECTROSCOPY; HETERODYNE FREQUENCY MEASUREMENTS; LORENTZ-BROADENING COEFFICIENTS; FOURIER-TRANSFORM SPECTRUM; TRIPLY DEUTERATED AMMONIA; INTERSTELLAR HEAVY-WATER; LINE-SHIFT COEFFICIENTS; HOT EMISSION-SPECTRA; LONG PATH SPECTRA; D2O LOW-PRESSURE AB This paper is the fourth of a series of papers reporting critically evaluated rotational-vibrational line positions, transition intensities, pressure dependences, and energy levels, with associated critically reviewed assignments and uncertainties, for all the main isotopologues of water. This paper presents energy level and transition data for the following doubly and triply substituted isotopologues of water: (D2O)-O-16, (D2O)-O-17, and (D2O)-O-18. The MARVEL (Measured Active Rotational-Vibrational Energy Levels) procedure is used to determine the levels, the lines, and their self-consistent uncertainties for the spectral regions 0-14 016, 0-7969, and 0-9108 cm(-1) for (D2O)-O-16, (D2O)-O-17, and (D2O)-O-18, respectively. For (D2O)-O-16, (D2O)-O-17, and (D2O)-O-18, 53 534, 600, and 12 167 lines are considered, respectively, from spectra recorded in absorption at room temperature and in emission at elevated temperatures. The number of validated energy levels is 12 269, 338, and 3351 for (D2O)-O-16, (D2O)-O-17, and (D2O)-O-18, respectively. The energy levels have been checked against the ones determined, with an average accuracy of about 0.03 cm(-1), from variational rovibrational computations employing exact kinetic energy operators and an accurate potential energy surface. Furthermore, the rovibrational labels of the energy levels have been validated by an analysis of the computed wavefunctions using the rigid-rotor decomposition (RRD) scheme. The extensive list of MARVEL lines and levels obtained is deposited in the Supplementary Material of this paper, in a distributed information system applied to water, W@DIS, and on the official MARVEL website, where they can easily be retrieved. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Tennyson, Jonathan; Polyansky, Oleg L.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Bernath, Peter F.] Old Dominion Univ, Norfolk, VA USA. [Brown, Linda R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Campargue, Alain] Univ Grenoble Alpes, CNRS, Grenoble, France. [Csaszar, Attila G.; Denes, Nora; Furtenbacher, Tibor; Szidarovszky, Tamas] Eotvos Lorand Univ, Inst Chem, MTA ELTE Res Grp Complex Chem Syst, Budapest, Hungary. [Daumont, Ludovic] Univ Reims, Reims, France. [Gamache, Robert R.] Univ Massachusetts, Lowell, MA USA. [Hodges, Joseph T.] NIST, Gaithersburg, MD 20899 USA. [Naumenko, Olga V.; Polyansky, Oleg L.; Fazliev, Alexander Z.; Vasilenko, Irina A.] Russian Acad Sci, Inst Atmospher Opt, Tomsk, Russia. [Rothman, Laurence S.; Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vandaele, Ann Carine] Inst Aeron Spatiale Belgique, B-1180 Brussels, Belgium. [Zobov, Nikolai F.] Russian Acad Sci, Inst Appl Phys, Nizhnii Novgorod 603600, Russia. [Hu, Shui-Ming] Univ Sci & Technol China, Hefei 230026, Peoples R China. RP Tennyson, J (reprint author), UCL, Dept Phys & Astron, Mortimer St, London WC1E 6BT, England. EM j.tennyson@ucl.ac.uk RI Tennyson, Jonathan/I-2222-2012; Csaszar, Attila/A-5241-2009; Bernath, Peter/B-6567-2012; Hu, Shuiming/C-4287-2008; Szidarovszky, Tamas/E-4376-2015; OI Tennyson, Jonathan/0000-0002-4994-5238; Bernath, Peter/0000-0002-1255-396X; Hu, Shuiming/0000-0002-1565-8468; Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 FU International Union of Pure and Applied Chemistry [2004-035-1-100]; UK Natural Environment Research Council; ERC Advanced Investigator [267219]; Royal Society; Scientific Research Fund of Hungary [OTKA NK83583]; Russian Foundation for Basic Research; Belgian Federal Science Policy Office [EV/35/3A, SD/AT/01A, PRODEX 1514901NLSFe(IC)]; Belgian National Fund for Scientific Research (FRFC contracts); Communaute de Belgique (Action de Recherche Concertees); COST Action CoDECS [CM1002]; NASA AURA mission [NNX11AF91G] FX We all thank the International Union of Pure and Applied Chemistry for funding under project 2004-035-1-100 (A database of water transitions from experiment and theory). In addition, this work has received partial support from the UK Natural Environment Research Council, ERC Advanced Investigator Project 267219, the Royal Society, the Scientific Research Fund of Hungary (Grant OTKA NK83583), the Russian Foundation for Basic Research, the Belgian Federal Science Policy Office (contracts EV/35/3A, SD/AT/01A, PRODEX 1514901NLSFe(IC)), the Belgian National Fund for Scientific Research (FRFC contracts), the Communaute de Belgique (Action de Recherche Concertees), the COST Action CoDECS (CM1002), and the NASA AURA mission, under the grant NNX11AF91G. Part of the research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contracts and grants with NASA. Alain Campargue and Ludovic Daumont are grateful for the financial support provided by the Programme National LEFE (CHAT) of CNRS (INSU). Semen Mikhailenko is thanked for providing part of the D216O dataset used during this study. We thank Christina Puzzarini for help deperturbing the published frequencies given in 13CaPu. NR 161 TC 28 Z9 33 U1 11 U2 66 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUL PY 2014 VL 142 BP 93 EP 108 DI 10.1016/j.jqsrt.2014.03.019 PG 16 WC Optics; Spectroscopy SC Optics; Spectroscopy GA AI2RR UT WOS:000336706300010 ER PT J AU Zapata, S Cardona, A Montes, C Valencia, V Vervoort, J Reiners, P AF Zapata, S. Cardona, A. Montes, C. Valencia, V. Vervoort, J. Reiners, P. TI Provenance of the Eocene Soebi Blanco formation, Bonaire, Leeward Antilles: Correlations with post-Eocene tectonic evolution of northern South America SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Provenance; Caribbean plate; Conglomerates; Leeward Antilles; Paleogeography ID OCEANIC PLATEAU; CARIBBEAN PLATE; ZIRCON GEOCHRONOLOGY; BRITISH-COLUMBIA; SANTA-MARTA; COLOMBIA; VENEZUELA; ANDES; ARC; CONSTRAINTS AB Middle to upper Eocene fluvial strata in the island of Bonaire contain detrital components that were tracked to Precambrian to Triassic massifs in northern Colombia and Venezuela. These detrital components confirm previous hypothesis suggesting that Bonaire and the Leeward Antilles were attached to South American basement massifs (SABM). These are composed of different fragmented South American blocks (Paraguana, Falcon, Maracaibo, Guajira, Perija, and Santa Marta) representing an Eocene, rightlaterally displaced tectonic piercing point along the southern Caribbean plate margin. U-Pb LA-ICP-MS from the metamorphic boulders of the Soebi Blanco Formation in Bonaire yield Grenvillian peaks ages (1000-1200 Ma), while detrital zircons recovered from the sandy matrix of the conglomerates contain populations with peaks of 1000 Ma-1200 Ma, 750-950 Ma, and 200-300 Ma. These populations match with geochronological data reported for the northern South American massifs. Thermochronological results from the metamorphic clasts yield Paleocene middle Eocene ages (65-50 Ma) that confirm a regional-scale cooling event in this time. These data imply a land connection between the SABM and the Leeward Antilles in late Eocene times, followed by a significant strike slip right-lateral displacement and transtensional basin opening starting in latest Eocene times. The succession of Eocene tectonic events recorded by the Soebi Blanco Formation and adjacent basins is a major tracer of the oblique convergence of the Caribbean plate against the South American margin. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Zapata, S.] Comorac Geolog Ares, Bogota, Colombia. [Cardona, A.] Univ Nacl Colombia Sede Medellin, Dept Proc & Energia, Medellin, Colombia. [Montes, C.] Univ Los Andes, Dept Geociencias, Bogota, Colombia. [Valencia, V.; Vervoort, J.] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA. [Reiners, P.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Zapata, S.] Smithsonian Trop Res Inst, Bogota, Colombia. RP Zapata, S (reprint author), Comorac Geolog Ares, Calle 44a 53-96, Bogota, Colombia. EM szapatah@gmail.com OI Montes, Camilo/0000-0002-3553-0787 FU COLCIENCIAS; Smithsonian Tropical Research Institute (STRI); environmental authorities of Bonaire FX We thank the Smithsonian Tropical Research Institute (STRI) and the environmental authorities of Bonaire for their support during several phases of the project. C. Jaramillo, Bayona, G., N. Hoyos, Londono, L and C. Echeverri are acknowledged for their discussions and continuous support. S. Zapata thanks COLCIENCIAS for its support as a young researchers fellowship. U. Ukchowdh, E. Abdel and G. Canizalez helped with sample preparations and lab analyses. Finally we also thank the environmental authorities of Bonaire for their support and guidance. NR 80 TC 2 Z9 3 U1 0 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD JUL PY 2014 VL 52 BP 179 EP 193 DI 10.1016/j.jsames.2014.02.009 PG 15 WC Geosciences, Multidisciplinary SC Geology GA AH9LU UT WOS:000336464700012 ER PT J AU Schuh, MA Banda, JM Bernasconi, PN Angryk, RA Martens, PCH AF Schuh, M. A. Banda, J. M. Bernasconi, P. N. Angryk, R. A. Martens, P. C. H. TI A Comparative Evaluation of Automated Solar Filament Detection SO SOLAR PHYSICS LA English DT Article DE Automated feature finding; Filaments; Quantitative comparative evaluation AB We present a comparative evaluation for automated filament detection in H alpha solar images. By using metadata produced by the Advanced Automated Filament Detection and Characterization Code (AAFDCC) module, we adapted our trainable feature recognition (TFR) module to accurately detect regions in solar images containing filaments. We first analyze the AAFDCC module's metadata and then transform it into labeled datasets for machine-learning classification. Visualizations of data transformations and classification results are presented and accompanied by statistical findings. Our results confirm the reliable event reporting of the AAFDCC module and establishes our TFR module's ability to effectively detect solar filaments in H alpha solar images. C1 [Schuh, M. A.; Banda, J. M.; Angryk, R. A.] Montana State Univ, Dept Comp Sci, Bozeman, MT 59717 USA. [Bernasconi, P. N.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Martens, P. C. H.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Martens, P. C. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schuh, MA (reprint author), Montana State Univ, Dept Comp Sci, 357 EPS, Bozeman, MT 59717 USA. EM michael.schuh@cs.montana.edu; juan.banda@cs.montana.edu; pietro.bernasconi@jhuapl.edu; angryk@cs.montana.edu; martens@physics.montana.edu RI Bernasconi, Pietro/H-2224-2016; OI Bernasconi, Pietro/0000-0002-0787-8954; Banda, Juan/0000-0001-8499-824X FU NASA [NNX09AB03G]; [NNH08ZDA001N-SDOSC solicitation]; [NNX11AM13A]; [NNH11ZHA003C solicitation] FX This research and development project was supported by two NASA Grant Awards: No. NNX09AB03G, funded from the NNH08ZDA001N-SDOSC solicitation, and No. NNX11AM13A, funded from the NNH11ZHA003C solicitation. We would also like to thank our internal reviewers as well as the Big Bear Solar Observatory/New Jersey Institute of Technology and the Global High Resolution Ha Network for providing and maintaining the ftp image data archive. NR 27 TC 9 Z9 9 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD JUL PY 2014 VL 289 IS 7 BP 2503 EP 2524 DI 10.1007/s11207-014-0495-9 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE7TI UT WOS:000334201400007 ER PT J AU Kobelski, AR Saar, SH Weber, MA McKenzie, DE Reeves, KK AF Kobelski, Adam R. Saar, Steven H. Weber, Mark A. McKenzie, David E. Reeves, Katharine K. TI Calibrating Data from the Hinode/X-Ray Telescope and Associated Uncertainties SO SOLAR PHYSICS LA English DT Article DE Corona; Instrumentation and data management ID MISSION; XRT AB The X-Ray Telescope (XRT) onboard the Hinode satellite, launched 23 September 2006 by the Japan Aerospace Exploration Agency (JAXA), is a joint mission of Japan, the United States, and the United Kingdom to study the solar corona. In particular, XRT was designed to study solar plasmas with temperatures between 1 and 10 MK with a parts per thousand aEuro parts per thousand 1aEuro(3) pixels (a parts per thousand aEuro parts per thousand 2aEuro(3) resolution). Prior to analysis, the data product from this instrument must be properly calibrated and data values quantified to accurately assess the information contained within. We present here the standard methods of calibration for these data. The calibration was performed on an empirical basis that uses the least complicated correction that accurately describes the data while suppressing spurious features. By analyzing the uncertainties remaining in the data after calibration, we conclude that the procedure is successful, because the remaining uncertainty after calibration is dominated by photon noise. This calibration software is available in the SolarSoft software library. C1 [Kobelski, Adam R.; McKenzie, David E.] Montana State Univ, Bozeman, MT 59717 USA. [Saar, Steven H.; Weber, Mark A.; Reeves, Katharine K.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kobelski, AR (reprint author), Montana State Univ, POB 173840, Bozeman, MT 59717 USA. EM kobelski@solar.physics.montana.edu RI Reeves, Katharine/P-9163-2014 FU NASA [NNM07AB07C]; Smithsonian Astrophysical Observatory; JAXA; NAOJ (Japan); STFC (U.K.); NASA (Norway); ESA (Norway); NSC (Norway) FX Hinode is a Japanese mission developed and launched by ISAS/JAXA, collaborating with NAOJ as a domestic partner, and with NASA and STFC (UK) as international partners. Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/JAXA. This team mainly consists of scientists from institutes in the partner countries. Support for the post-launch operation is provided by JAXA and NAOJ (Japan), STFC (U.K.), NASA, ESA, and NSC (Norway). This work was supported by NASA under contract NNM07AB07C with the Smithsonian Astrophysical Observatory. NR 7 TC 10 Z9 10 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD JUL PY 2014 VL 289 IS 7 BP 2781 EP 2802 DI 10.1007/s11207-014-0487-9 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE7TI UT WOS:000334201400021 ER PT J AU Kenworthy, WJ Gallegos, CL Costello, C Field, D di Carlo, G AF Kenworthy, W. J. Gallegos, C. L. Costello, Charles Field, Donald di Carlo, Giuseppe TI Dependence of eelgrass (Zostera marina) light requirements on sediment organic matter in Massachusetts coastal bays: Implications for remediation and restoration SO MARINE POLLUTION BULLETIN LA English DT Article DE Eelgrass; Zostera marina; Light requirements; Water quality; Nitrogen loading; USA; Massachusetts ID SUBMERSED AQUATIC VEGETATION; OPTICAL WATER-QUALITY; SEAGRASS DEPTH LIMITS; ABSORPTION-COEFFICIENTS; SPECTRAL ABSORPTION; NUTRIENT ENRICHMENT; WAQUOIT BAY; HABITAT REQUIREMENTS; MESOCOSM EXPERIMENTS; POSITIVE FEEDBACKS AB Using a calibrated bio-optical model we determined that the optical water quality conditions in several nitrogen-impaired embayments and in one unimpaired system were within the range of values known to support eelgrass growth. We also used the model to identify a range of light requirements for eelgrass (Zostera marina). Higher eelgrass light requirements, expressed as a percentage of surface-incident irradiance, corresponded with higher sediment organic matter content. These results corroborated findings by previous studies which indicate a generalized relationship: seagrasses growing in turbid conditions with poorer water and sediment quality have higher light requirements than those growing in less degraded conditions. The mechanistic reason for the variation in light requirements is still not completely explained and cannot be attributed to a single independent variable. Varying light requirement have important implications for eelgrass protection and should be considered when setting restoration targets for eelgrass in water quality and nitrogen remediation programs. Published by Elsevier Ltd. C1 [Kenworthy, W. J.; Field, Donald; di Carlo, Giuseppe] NOAA, Ctr Coastal Fisheries & Habitat Res, NCCOS, NOS, Beaufort, NC 28516 USA. [Gallegos, C. L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Costello, Charles] Massachusetts Dept Environm Protect, Div Watershed Management, Boston, MA 02108 USA. RP Gallegos, CL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM jud.kenworthy@gmail.com; gallegosc@si.edu; charles.costello@state.ma.us; don.fleld@noaa.gov; Giuseppe.dicarlo@gmail.com OI Gallegos, Charles/0000-0001-5112-0166 FU Massachusetts Department of Environmental Protection [2007-03/CAP]; Center for Coastal Fisheries and Habitat Research; NCCOS; NOS; NOAA FX Funding for this work was provided by contract 2007-03/CAP from the Massachusetts Department of Environmental Protection to the Smithsonian Institution. Additional funding for W.J. Kenworthy, G. Di Carlo and D. Field was provided by the Center for Coastal Fisheries and Habitat Research, NCCOS, NOS, NOAA. We thank S. L. Benson and E. A. L. Milton for assistance with field and laboratory work, and Mary Kay Fox of the Waquoit Bay National Estuarine Research Reserve for access to laboratory space. We thank Jessie Jarvis for assistance with sediment organic matter and grain size analysis. We also thank Amit Malhotra of the Center for Coastal Fisheries and Habitat Research for assistance in collecting and processing Kinematic Global Positioning System data. NR 86 TC 8 Z9 8 U1 6 U2 42 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-326X EI 1879-3363 J9 MAR POLLUT BULL JI Mar. Pollut. Bull. PD JUN 30 PY 2014 VL 83 IS 2 BP 446 EP 457 DI 10.1016/j.marpolbul.2013.11.006 PG 12 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA AK4PH UT WOS:000338406100009 PM 24308994 ER PT J AU Schmidt, LK Zimmermann, A Elsenbeer, H AF Schmidt, Lena Katharina Zimmermann, Alexander Elsenbeer, Helmut TI Ant mounds as a source of sediment in a tropical rainforest? SO HYDROLOGICAL PROCESSES LA English DT Article DE ant mounds; soil erosion; sediment output; zoogeomorphology ID OVERLAND-FLOW; EASTERN SPAIN; SOIL; CATCHMENT; COMMUNITY; TRANSPORT; EROSION; LOSSES; WATER AB In Lutzito catchment on Barro Colorado Island, Panama, extraordinarily high suspended-sediment yields of 1-2Mgha-1year-1 were generated despite the dense forest cover coinciding with erosion-resistant soils. We hypothesized that ant mounding activity is an important zoogeomorphological mechanism in this area, providing relevant quantities of easily transportable material at the soil surface. To test this hypothesis, all ant mound material was collected collected for dry mass determination from thirty 4m2 plots installed in the study area every 1-3days during the 39-day sampling period. Additionally, three ground-nesting ant species responsible for mounds in the study area, Ectatomma ruidum, Trachymyrmex cornetzi and Strumigenys marginiventris, were identified. On the basis of the total of 1.38kg of material collected in the wet season of 2011, the estimate for the whole 8months wet season amounts to 725kgha-1. As this value is in the same order of magnitude as sediment output, it shows that ants may act as important ecosystem engineers and contribute to sediment production here by providing large quantities of fine-grained, readily erodible material at the soil surface for subsequent transport to the streambed. Copyright (c) 2014 John Wiley & Sons, Ltd. C1 [Schmidt, Lena Katharina; Zimmermann, Alexander; Elsenbeer, Helmut] Univ Potsdam, Inst Earth & Environm Sci, D-14476 Potsdam, Germany. [Elsenbeer, Helmut] Smithsonian Trop Res Inst, Panama City, Panama. RP Schmidt, LK (reprint author), Univ Potsdam, Inst Earth & Environm Sci, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany. EM leschmid@uni-potsdam.de RI Zimmermann, Alexander/B-6831-2011 FU Smithsonian Tropical Research Institute, Panama FX This research was funded by Smithsonian Tropical Research Institute, Panama, with a short-term fellowship awarded to Katharina Schmidt. We thank Joe Wright for his help and advice and Steven Yanoviak for his help with species identification. H. E. acknowledges STRI's support during his sabbaticals on BCI. Finally, we thank Artemi Cerda and an anonymous reviewer for their constructive comments on an earlier version of this manuscript. NR 27 TC 0 Z9 0 U1 1 U2 19 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0885-6087 EI 1099-1085 J9 HYDROL PROCESS JI Hydrol. Process. PD JUN 30 PY 2014 VL 28 IS 13 BP 4156 EP 4160 DI 10.1002/hyp.10222 PG 5 WC Water Resources SC Water Resources GA AJ8SG UT WOS:000337977100014 ER PT J AU Touchon, JC Wojdak, JM AF Touchon, Justin C. Wojdak, Jeremy M. TI Plastic Hatching Timing by Red-Eyed Treefrog Embryos Interacts with Larval Predator Identity and Sublethal Predation to Affect Prey Morphology but Not Performance SO PLOS ONE LA English DT Article ID SWIMMING PERFORMANCE; TRADE-OFFS; BEHAVIORAL PLASTICITY; PHENOTYPIC PLASTICITY; AGALYCHNIS-CALLIDRYAS; HABITAT COMPLEXITY; MULTIPLE PREDATORS; DRAGONFLY STRIKES; NONLETHAL INJURY; OPPOSITE SHIFTS AB Many animals respond to predation risk by altering their morphology, behavior, or life-history. We know a great deal about the cues prey respond to and the changes to prey that can be induced by predation risk, but less is known about how plastic responses to predators may be affected by separate plastic responses occurring earlier in life, particularly during the embryonic period. Embryos of a broad array of taxa can respond to egg- or larval-stage risks by altering hatching timing, which may alter the way organisms respond to future predators. Using the red-eyed treefrog (Agalychnis callidryas), a model for understanding the effects of plasticity across life-stages, we assessed how the combined effects of induced variation in the timing of embryo hatching and variation in the larval predator community impacted tadpole morphology, pigmentation and swimming performance. We found that A. callidryas tadpoles developed deeper tail muscles and fins and darker pigmentation in response to fish predators, either when alone or in diverse community with other predators. Tadpoles altered morphology much less so to dragonfly naiads or water bugs. Interestingly, morphological responses to predators were also affected by induced differences in hatching age, with early and late-hatched tadpoles exhibiting different allometric relationships between tail height and body length in different predator environments. Beyond induced morphological changes, fish predators often damaged tadpoles' tails without killing them (i.e., sublethal predation), but these tadpoles swam equally quickly to those with fully intact tails. This was due to the fact that tadpoles with more damaged tails increased tail beats to achieve equal swimming speed. This study demonstrates that plastic phenotypic responses to predation risk can be influenced by a complex combination of responses to both the embryo and larval environments, but also that prey performance can be highly resilient to sublethal predation. C1 [Touchon, Justin C.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Touchon, Justin C.] Smithsonian Trop Res Inst, Balboa, Panama. [Wojdak, Jeremy M.] Radford Univ, Dept Biol, Radford, VA 24142 USA. RP Touchon, JC (reprint author), Boston Univ, Dept Biol, 5 Cummington St, Boston, MA 02215 USA. EM justintouchon@gmail.com FU Research Opportunity Award from the National Science Foundation; NSF [DEB-0717220, DEB-0716923]; Radford University; Smithsonian Tropical Research Institute; [IIA-1064566] FX JMW was supported by a Research Opportunity Award from the National Science Foundation, stemming from NSF grant DEB-0717220 to James Vonesh. JCT was partially supported by NSF grant DEB-0716923 to Karen Warkentin and by IIA-1064566 to JCT. Radford University and the Smithsonian Tropical Research Institute also provided funding or support. NR 61 TC 4 Z9 4 U1 0 U2 25 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUN 26 PY 2014 VL 9 IS 6 AR e100623 DI 10.1371/journal.pone.0100623 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AK2WP UT WOS:000338280800048 PM 24967896 ER PT J AU Launius, RD AF Launius, Roger D. TI Neil Armstrong: A Life of Flight SO NATURE LA English DT Book Review C1 [Launius, Roger D.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. EM launiusr@si.edu NR 1 TC 0 Z9 0 U1 0 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 JUN 26 PY 2014 VL 510 IS 7506 BP 472 EP 472 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AJ6LK UT WOS:000337806300024 ER PT J AU Norrbom, AL Neder, LE AF Norrbom, Allen L. Estela Neder, Lilia TI New neotropical species of Trupanea (Diptera: Tephritidae) with unusual wing patterns SO ZOOTAXA LA English DT Article DE Diptera; Tephritidae; Tephritinae; taxonomy; host plant; Asteraceae AB Four species of Trupanea Shrank (Diptera: Tephritidae) with unusual wing patterns are described from the Neotropical Region: T. dimorphica (Argentina), T. fasciata (Argentina), T. polita (Argentina and Bolivia), and T. trivittata (Argentina). Celidosphenella Hendel, 1914 and Melanotrypana Hering, 1944 are considered new synonyms of Trupanea, and the following species are transferred from Celidosphenella to Trupanea: Acinia bella Blanchard, 1852; Acanthiophilus benoisti Seguy, 1933; Tephritis diespasmena Schiner, 1868; Celidosphenella maculata Hendel, 1914; Sphenella poecila Schiner, 1868; Trypanea simulata Malloch, 1933; Trupanea stonei Stuardo, 1946; and Trypanea vidua Hering, 1942. Aphyllocladus spartioides Wedd. (Asteraceae: Mutisieae) is reported as a probable host plant for Trupanea dimorphica. C1 [Norrbom, Allen L.] USDA ARS, Systemat Entomol Lab, Smithsonian Inst, Washington, DC 20013 USA. [Estela Neder, Lilia] Univ Nacl Jujuy, CONICET, Inst Biol Altura, RA-4600 San Salvador De Jujuy, Jujuy, Argentina. RP Norrbom, AL (reprint author), USDA ARS, Systemat Entomol Lab, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM allen.norrbom@ars.usda.gov; leneder@inbial.unju.edu.ar NR 21 TC 1 Z9 1 U1 0 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUN 24 PY 2014 VL 3821 IS 4 BP 443 EP 456 PG 14 WC Zoology SC Zoology GA AJ5AH UT WOS:000337692000003 PM 24989757 ER PT J AU Vazquez-Bader, AR Gracia, A Lemaitre, R AF Vazquez-Bader, Ana Rosa Gracia, Adolfo Lemaitre, Rafael TI A new species of Munidopsis Whiteaves, 1874 (Crustacea: Anomura: Galatheoidea: Munidopsidae) from the Gulf of Mexico and Caribbean Sea SO ZOOTAXA LA English DT Article DE Crustacea; Decapoda; Anomura; Galatheoidea; Munidopsidae; squat lobster; Munidopsis; new species; Anoplonotus group; Gulf of Mexico; western Caribbean ID DECAPODA ANOMURA; SQUAT LOBSTERS; GALATHEIDAE AB A new species of squat lobster, Munidopsis shulerae sp. nov., from the Gulf of Mexico and western Caribbean, is fully described and illustrated. This new species is named in honor of the late Barbara Shuler Mayo (1945-1988), who first recognized this new taxon in her 1974 unpublished doctoral dissertation, but never formalized it. This new species is placed in the Anoplonotus group based on the presence of simple, narrow rostrum, spineless eyes, fused sternites 3 and 4, well-marked carapace regions, unarmed pleonal tergites, and smooth dactyls of pereopods 2-4. Among western Atlantic congeners, M. shulerae sp. nov. is most similar to M. polita (Smith, 1883), from which it can be distinguished by the straight shape of the rostrum with a tuberculate dorsal carina extending to the epigastric region, coarse ornamentation of the carapace, and a conspicuous submarginal protuberance on each side of the carapace between the antennal and ocular peduncles. C1 [Vazquez-Bader, Ana Rosa; Gracia, Adolfo] Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Lab Ecol Pesquera Crustaceos, UNAM,CU, Mexico City 04510, DF, Mexico. [Lemaitre, Rafael] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Suitland, MD 20746 USA. RP Vazquez-Bader, AR (reprint author), Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Lab Ecol Pesquera Crustaceos, UNAM,CU, Univ 3000, Mexico City 04510, DF, Mexico. EM ana-rosav@hotmail.com; gracia@unam.mx; lemaitrr@si.edu FU Direccion General de Asuntos del Personal Academico, UNAM [IN223109-3] FX At UMML we thank Drs. Nancy Voss and Julio Garcia-Gomez for help in attempting to locate specimens used by Barbara Shuler Mayo. The help of Mary K. Wicksten in locating specimens of this new species is gratefully acknowledged. Rose Gulledge assisted in the electronic preparation of the figures. We are grateful to Magaly Galvan Palmerin for her assistance in taking photos. This study was partially supported by a grant (IN223109-3) of the Direccion General de Asuntos del Personal Academico, UNAM. We also thank the crew of the R/V Justo Sierra that participated in research cruises. NR 33 TC 4 Z9 5 U1 0 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUN 23 PY 2014 VL 3821 IS 3 BP 354 EP 362 PG 9 WC Zoology SC Zoology GA AJ5AE UT WOS:000337691600004 PM 24989749 ER PT J AU Glowska, E Milensky, CM AF Glowska, Eliza Milensky, Christopher M. TI New species of the genus Picobia (Cheyletoidea: Syringophilidae) parasitizing tyrannid birds (Passeriformes: Tyrannidae) SO ZOOTAXA LA English DT Article DE Quill mites; Syringophilidae; tyrannid birds; systematics; ectoparasites ID QUILL MITES; ACARI SYRINGOPHILIDAE AB Three new quill mite species of the genus Picobia Haller (Cheyletoidea: Syringophilidae) are described from 6 host species of the family Tyrannidae (Passeriformes), P. ochoi sp. nov. from Tolmomyias sulphurescens (Spix) (Guyana), P. schmidti sp. nov. from Lophotriccus pileatus (Tschudi) (type host) (Peru) and Hemitriccus margaritaceiventer (Orbigny & Lafresnaye) (Guyana), and P. myiopagi sp. nov. from Myiopagis gaimardii (Orbigny) (type host) (Guyana), M. sub-placens (Sclater) (Peru) and Elaenia ruficeps Pelzeln (Guyana). C1 [Glowska, Eliza] Adam Mickiewicz Univ, Fac Biol, Dept Anim Morphol, PL-61614 Poznan, Poland. [Milensky, Christopher M.] Smithsonian Inst, Div Birds, Washington, DC 20013 USA. RP Glowska, E (reprint author), Adam Mickiewicz Univ, Fac Biol, Dept Anim Morphol, Umultowska 89, PL-61614 Poznan, Poland. EM glowska@amu.edu.pl NR 11 TC 4 Z9 4 U1 1 U2 4 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUN 23 PY 2014 VL 3821 IS 3 BP 373 EP 383 PG 11 WC Zoology SC Zoology GA AJ5AE UT WOS:000337691600006 PM 24989751 ER PT J AU Harasewych, MG AF Harasewych, M. G. TI Attenuiconus marileeae, a new species of cone (Gastropoda: Conidae: Puncticulinae) from Curacao SO NAUTILUS LA English DT Article DE Deep Reef; Curasub; bottles; predation AB Attenuiconus marileeae new species is described from deep reefs off southeastern Curacao. It resembles A. attenuatus, A. honkeri, and A. aureonimbosus in size and general proportion of the shell, but is readily distinguished on the basis of its distinctive color pattern, which consists of a vivid orange-red base color with three bands of irregular, white flammules. Attenuiconus marileeae was collected at substantially greater depths than any of its Caribbean congeners. Only A. aureonimbosus, from the northeastern Gulf of Mexico, inhabits comparable depths. Like all species of Attenuiconus, nearly all specimens A. marileeae have one or more major repaired breaks indicative of unsuccessful attacks by crustaceans. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012, Washington, DC 20013 USA. EM Harasewych@si.edu NR 14 TC 1 Z9 1 U1 0 U2 1 PU BAILEY-MATTHEWS SHELL MUSEUM PI SANIBEL PA C/O DR JOSE H LEAL, ASSOCIATE/MANAGING EDITOR, 3075 SANIBEL-CAPTIVA RD, SANIBEL, FL 33957 USA SN 0028-1344 J9 NAUTILUS JI Nautilus PD JUN 20 PY 2014 VL 128 IS 2 BP 55 EP 58 PG 4 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA AQ9PV UT WOS:000343188700004 ER PT J AU Walters-Conte, KB Le Johnson, D Johnson, WE O'Brien, SJ Pecon-Slattery, J AF Walters-Conte, Kathryn B. Le Johnson, Diana Johnson, Warren E. O'Brien, Stephen J. Pecon-Slattery, Jill TI The dynamic proliferation of CanSINEs mirrors the complex evolution of Feliforms SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Incomplete lineage sorting; SINEs; Carnivora; Speciation; transposable elements; Adaptation; Feliformia; Felidae ID LINKED MYOTUBULAR MYOPATHY; RNA-DERIVED RETROPOSONS; ORDER CARNIVORA; REPETITIVE ELEMENTS; SINE INSERTION; ALU REPEATS; GENOMIC DIVERSITY; DOMESTIC DOG; DNA-SEQUENCE; FAMILY AB Background: Repetitive short interspersed elements (SINEs) are retrotransposons ubiquitous in mammalian genomes and are highly informative markers to identify species and phylogenetic associations. Of these, SINEs unique to the order Carnivora (CanSINEs) yield novel insights on genome evolution in domestic dogs and cats, but less is known about their role in related carnivores. In particular, genome-wide assessment of CanSINE evolution has yet to be completed across the Feliformia (cat-like) suborder of Carnivora. Within Feliformia, the cat family Felidae is composed of 37 species and numerous subspecies organized into eight monophyletic lineages that likely arose 10 million years ago. Using the Felidae family as a reference phylogeny, along with representative taxa from other families of Feliformia, the origin, proliferation and evolution of CanSINEs within the suborder were assessed. Results: We identified 93 novel intergenic CanSINE loci in Feliformia. Sequence analyses separated Feliform CanSINEs into two subfamilies, each characterized by distinct RNA polymerase binding motifs and phylogenetic associations. Subfamily I CanSINEs arose early within Feliformia but are no longer under active proliferation. Subfamily II loci are more recent, exclusive to Felidae and show evidence for adaptation to extant RNA polymerase activity. Further, presence/absence distributions of CanSINE loci are largely congruent with taxonomic expectations within Feliformia and the less resolved nodes in the Felidae reference phylogeny present equally ambiguous CanSINE data. SINEs are thought to be nearly impervious to excision from the genome. However, we observed a nearly complete excision of a CanSINEs locus in puma (Puma concolor). In addition, we found that CanSINE proliferation in Felidae frequently targeted existing CanSINE loci for insertion sites, resulting in tandem arrays. Conclusions: We demonstrate the existence of at least two SINE families within the Feliformia suborder, one of which is actively involved in insertional mutagenesis. We find SINEs are powerful markers of speciation and conclude that the few inconsistencies with expected patterns of speciation likely represent incomplete lineage sorting, species hybridization and SINE-mediated genome rearrangement. C1 [Walters-Conte, Kathryn B.] Amer Univ, Dept Biol, Washington, DC 20016 USA. [Le Johnson, Diana] George Washington Univ, Dept Biol Sci, Washington, DC 20009 USA. [Johnson, Warren E.; Pecon-Slattery, Jill] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [O'Brien, Stephen J.] St Petersburg State Univ, Dobzhansky Ctr Genome Bioinformat, St Petersburg 199034, Russia. RP Walters-Conte, KB (reprint author), Amer Univ, Dept Biol, 101 Hurst Hall 4440 Massachusetts Ave, Washington, DC 20016 USA. EM kwalt@american.edu RI Johnson, Warren/D-4149-2016; OI Johnson, Warren/0000-0002-5954-186X; O'Brien, Stephen J./0000-0001-7353-8301 FU National Science Foundation Doctoral Dissertation Improvement Grant [DEB-0909922]; National Institutes of Health [N01-CO-12400]; Intramural Research Program of the NIH; NCI; Center for Cancer Research; National Cancer Institute; The George Washington University Facilitation Fund FX The authors thank Joan Pontius, Marc Allard, Carrie McCracken, Victor David and Nicole Crumpler for technical assistance and expertise. This project was funded through the National Science Foundation Doctoral Dissertation Improvement Grant (DEB-0909922) and The George Washington University Facilitation Fund. This project was also supported with federal funds from the National Cancer Institute, National Institutes of Health, under contract N01-CO-12400. This research was supported (in part) by the Intramural Research Program of the NIH, NCI, Center for Cancer Research. The content of this publication does not necessarily reflect the views or policies of the Department of Health and Human Services, nor does its mention of trade names, commercial products, or organizations imply endorsement by the U.S. Government. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of manuscript. This work was completed in the Department of Biology at The George Washington University and in the Laboratory of Genomic Diversity at National Cancer Institute, USA. NR 101 TC 2 Z9 2 U1 0 U2 21 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD JUN 20 PY 2014 VL 14 AR 137 DI 10.1186/1471-2148-14-137 PG 15 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA AK5HG UT WOS:000338454700001 PM 24947429 ER PT J AU Archambault, S Arlen, T Aune, T Beilicke, M Benbow, W Bird, R Bottcher, M Bouvier, A Buckley, JH Bugaev, V Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Dickherber, R Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fortson, L Furniss, A Galante, N Gall, D Garson, AI Gillanders, GH Griffin, S Grube, J Gusbar, C Gyuk, G Hanna, D Holder, J Hughes, G Kaaret, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Lamerato, A Lang, MJ Li, K Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Millis, J Moriarty, P Mukherjee, R Nieto, D De Bhroithe, AO Ong, RA Orr, M Otte, AN Park, N Perkins, JS Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Reynolds, PT Richards, GT Roache, E Roustazadeh, P Saxon, DB Sembroski, GH Senturk, GD Skole, C Staszak, D Telezhinsky, I Tesic, G Theiling, M Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Weinstein, A Welsing, R Williams, DA Zitzer, B AF Archambault, S. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bird, R. Boettcher, M. Bouvier, A. Buckley, J. H. Bugaev, V. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Dickherber, R. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fortson, L. Furniss, A. Galante, N. Gall, D. Garson, A. III. Gillanders, G. H. Griffin, S. Grube, J. Gusbar, C. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Lamerato, A. Lang, M. J. Li, K. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Millis, J. Moriarty, P. Mukherjee, R. Nieto, D. De Bhroithe, A. O'Faolain Ong, R. A. Orr, M. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Reynolds, P. T. Richards, G. T. Roache, E. Roustazadeh, P. Saxon, D. B. Sembroski, G. H. Senturk, G. D. Skole, C. Staszak, D. Telezhinsky, I. Tesic, G. Theiling, M. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Weinstein, A. Welsing, R. Williams, D. A. Zitzer, B. TI TEST OF MODELS OF THE COSMIC INFRARED BACKGROUND WITH MULTIWAVELENGTH OBSERVATIONS OF THE BLAZAR 1ES 1218+30.4 IN 2009 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; BL Lacertae objects: individual (1ES1218+30.4); cosmic background radiation; diffuse radiation; galaxies: jets; gamma rays: galaxies ID GAMMA-RAY OBSERVATIONS; EXTRAGALACTIC MAGNETIC-FIELDS; ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; X-RAY; TEV BLAZARS; PARTICLE-ACCELERATION; VERITAS OBSERVATIONS; TIMING EXPLORER; STRONG FLARES AB We present the results of a multi-wavelength campaign targeting the blazar 1ES 1218+30.4 with observations with the 1.3 m McGraw-Hill optical telescope, the Rossi X-ray Timing Explorer (RXTE), the Fermi Gamma-Ray Space Telescope, and the Very Energetic Radiation Imaging Telescope Array System (VERITAS). The RXTE and VERITAS observations were spread over a 13 day period and revealed clear evidence for flux variability, and a strong X-ray and gamma-ray flare on 2009 February 26 (MJD 54888). The campaign delivered a well-sampled broadband energy spectrum with simultaneous RXTE and VERITAS very high energy (VHE, > 100 GeV) observations, as well as contemporaneous optical and Fermi observations. The 1ES 1218+30.4 broadband energy spectrum-the first with simultaneous X-ray and VHE gamma-ray energy spectra-is of particular interest as the source is located at a high cosmological redshift for a VHE source (z = 0.182), leading to strong absorption of VHE gamma rays by photons from the optical/infrared extragalactic background light (EBL) via gamma VHE +gamma EBL -> e(+) e(-)pair-creation processes. We model the data with a one-zone synchrotron self-Compton (SSC) emission model and with the extragalactic absorption predicted by several recent EBL models. We find that the observations are consistent with the SSC scenario and all the EBL models considered in this work. We discuss observational and theoretical avenues to improve on the EBL constraints. C1 [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Arlen, T.; Aune, T.; Ong, R. A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Garson, A. III.; Krawczynski, H.; Li, K.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bird, R.; Collins-Hughes, E.; Khassen, Y.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Boettcher, M.; Gusbar, C.; Gyuk, G.; Lamerato, A.; Roustazadeh, P.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Ciupik, L.; Grube, J.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Errando, M.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Federici, S.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Skole, C.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam Golm, Germany. [Gall, D.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Holder, J.; Saxon, D. B.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Saxon, D. B.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Majumdar, P.] Saha Inst Nucl Phys, Kolkata 700064, India. [McArthur, S.; Park, N.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Nieto, D.; Senturk, G. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Perkins, J. S.] NASA, GSFC, CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, GSFC, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland, Baltimore, MD 21250 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. RP Archambault, S (reprint author), McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. RI Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755; Cui, Wei/0000-0002-6324-5772; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. NR 72 TC 1 Z9 1 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2014 VL 788 IS 2 AR 158 DI 10.1088/0004-637X/788/2/158 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200061 ER PT J AU Barnacka, A Geller, MJ Dell'antonio, IP Benbow, W AF Barnacka, Anna Geller, Margaret J. Dell'antonio, Ian P. Benbow, Wystan TI STRONG GRAVITATIONAL LENSING AS A TOOL TO INVESTIGATE THE STRUCTURE OF JETS AT HIGH ENERGIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; galaxies: structure; gamma rays: general; gravitational lensing: strong ID GAMMA-RAY FLARE; ACTIVE GALACTIC NUCLEI; SPACE-TELESCOPE OBSERVATIONS; SYNCHROTRON-PROTON BLAZAR; DARK-MATTER SUBSTRUCTURE; M87 JET; TIME-DELAY; RADIO-SOURCES; EMISSION; VARIABILITY AB The components of blazar jets that emit radiation span a factor of 1010 in scale. The spatial structure of these emitting regions depends on the observed energy. Photons emitted at different sites cross the lens plane at different distances from the mass-weighted center of the lens. Thus there are differences in magnification ratios and time delays between the images of lensed blazars observed at different energies. When the lens structure and redshift are known from optical observations, these constraints can elucidate the structure of the source at high energies. At these energies, current technology is inadequate to resolve these sources, and the observed light curve is thus the sum of the images. Durations of gamma-ray flares are short compared with typical time delays; thus both the magnification ratio and the time delay can be measured for the delayed counterparts. These measurements are a basis for localizing the emitting region along the jet. To demonstrate the power of strong gravitational lensing, we build a toy model based on the best studied and the nearest relativistic jet M87. C1 [Barnacka, Anna; Geller, Margaret J.; Benbow, Wystan] 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. 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 NR 80 TC 7 Z9 7 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 20 PY 2014 VL 788 IS 2 AR 139 DI 10.1088/0004-637X/788/2/139 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200042 ER PT J AU Caputi, KI Michalowski, MJ Krips, M Geach, JE Ashby, MLN Huang, JS Fazio, GG Koekemoer, AM Popping, G Spaans, M Castellano, M Dunlop, JS Fontana, A Santini, P AF Caputi, K. I. Michalowski, M. J. Krips, M. Geach, J. E. Ashby, M. L. N. Huang, J. -S. Fazio, G. G. Koekemoer, A. M. Popping, G. Spaans, M. Castellano, M. Dunlop, J. S. Fontana, A. Santini, P. TI PdBI COLD DUST IMAGING OF TWO EXTREMELY RED H - [4.5] > 4 GALAXIES DISCOVERED WITH SEDS AND CANDELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: high-redshift; infrared: galaxies; submillimeter: galaxies ID DEEP-FIELD-SOUTH; EXTRAGALACTIC LEGACY SURVEY; SPITZER-SPACE-TELESCOPE; SQUARE DEGREE SURVEY; S-SELECTED GALAXIES; GREATER-THAN 4; SUBMILLIMETER GALAXIES; SOURCE COUNTS; STELLAR MASS; K-S AB We report Plateau de Bure Interferometer (PdBI) 1.1mmcontinuum imaging toward two extremely redH-[ 4.5] > 4 (AB) galaxies at z > 3, which we have previously discovered making use of Spitzer SEDS and Hubble Space Telescope CANDELS ultra-deep images of the Ultra Deep Survey field. One of our objects is detected on the PdBI map with a 4.3s significance, corresponding to S. (1.1 mm) = 0.78 +/- 0.18 mJy. By combining this detection with the Spitzer 8 and 24 mu m photometry for this source, and SCUBA2 flux density upper limits, we infer that this galaxy is a composite active galactic nucleus/star-forming system. The infrared (IR)-derived star formation rate is SFR approximate to 200 +/- 100M circle dot yr(-1), which implies that this galaxy is a higher-redshift analogue of the ordinary ultra-luminous infrared galaxies more commonly found at z similar to 2-3. In the field of the other target, we find a tentative 3.1 sigma detection on the PdBI 1.1 mm map, but 3.7 arcsec away of our target position, so it likely corresponds to a different object. In spite of the lower significance, the PdBI detection is supported by a close SCUBA2 3.3 sigma detection. No counterpart is found on either the deep SEDS or CANDELS maps, so, if real, the PdBI source could be similar in nature to the submillimeter source GN10. We conclude that the analysis of ultra-deep near-and mid-IR images offers an efficient, alternative route to discover new sites of powerful star formation activity at high redshifts. C1 [Caputi, K. I.; Popping, G.; Spaans, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Michalowski, M. J.; Dunlop, J. S.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Krips, M.] IRAM, F-38406 St Martin Dheres, France. [Geach, J. E.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Ashby, M. L. N.; Huang, J. -S.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Castellano, M.; Fontana, A.; Santini, P.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. RP Caputi, KI (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. EM karina@astro.rug.nl OI Castellano, Marco/0000-0001-9875-8263; Popping, Gergo/0000-0003-1151-4659; Santini, Paola/0000-0002-9334-8705; Koekemoer, Anton/0000-0002-6610-2048 NR 45 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 JUN 20 PY 2014 VL 788 IS 2 AR 126 DI 10.1088/0004-637X/788/2/126 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200029 ER PT J AU Hada, K Giroletti, M Kino, M Giovannini, G D'Ammando, F Cheung, CC Beilicke, M Nagai, H Doi, A Akiyama, K Honma, M Niinuma, K Casadio, C Orienti, M Krawczynski, H Gomez, JL Sawada-Satoh, S Koyama, S Cesarini, A Nakahara, S Gurwell, MA AF Hada, K. Giroletti, M. Kino, M. Giovannini, G. D'Ammando, F. Cheung, C. C. Beilicke, M. Nagai, H. Doi, A. Akiyama, K. Honma, M. Niinuma, K. Casadio, C. Orienti, M. Krawczynski, H. Gomez, J. L. Sawada-Satoh, S. Koyama, S. Cesarini, A. Nakahara, S. Gurwell, M. A. TI A STRONG RADIO BRIGHTENING AT THE JET BASE OF M 87 DURING THE ELEVATED VERY HIGH ENERGY GAMMA-RAY STATE IN 2012 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (M 87); galaxies: jets; gamma rays: galaxies; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; SUPERMASSIVE BLACK-HOLE; M87 JET; TEV EMISSION; GALAXY M87; SCHWARZSCHILD RADII; RELATIVISTIC JETS; VLBI OBSERVATIONS; UNIFIED SCHEMES AB We report our intensive, high angular resolution radio monitoring observations of the jet in M 87 with the VLBI Exploration of Radio Astrometry (VERA) and the European VLBI Network (EVN) from 2011 February to 2012 October, together with contemporaneous high-energy (100 MeV< E < 100 GeV)gamma-ray light curves obtained by the Fermi Large Area Telescope. During this period (specifically from 2012 February to 2012 March), an elevated level of the M 87 flux is reported at very high energy (VHE; E > 100 GeV). rays by VERITAS. We detected a remarkable (up to similar to 70%) increase of the radio flux density from the unresolved jet base (radio core) with VERA at 22 and 43 GHz coincident with the VHE activity. Meanwhile, we confirmed with EVN at 5 GHz that the peculiar knot, HST-1, which is an alternative favored gamma-ray production site located at greater than or similar to 120 pc from the nucleus, remained quiescent in terms of its flux density and structure. These results in the radio bands strongly suggest that the VHE gamma-ray activity in 2012 originates in the jet base within 0.03 pc or 56 Schwarzschild radii (the VERA spatial resolution of 0.4 mas at 43 GHz) from the central supermassive black hole. We further conducted VERA astrometry for the M 87 core at six epochs during the flaring period, and detected core shifts between 22 and 43 GHz, a mean value of which is similar to that measured in the previous astrometric measurements. We also discovered a clear frequency-dependent evolution of the radio core flare at 43, 22, and 5 GHz; the radio flux density increased more rapidly at higher frequencies with a larger amplitude, and the light curves clearly showed a time-lag between the peaks at 22 and 43 GHz, the value of which is constrained to be within similar to 35-124 days. This indicates that a new radio-emitting component was created near the black hole in the period of the VHE event, and then propagated outward with progressively decreasing synchrotron opacity. By combining the obtained core shift and time-lag, we estimated an apparent speed of the newborn component propagating through the opaque region between the cores at 22 and 43 GHz. We derived a sub-luminal speed (less than similar to 0.2c) for this component. This value is significantly slower than the super-luminal (similar to 1.1c) features that appeared from the core during the prominent VHE flaring event in 2008, suggesting that stronger VHE activity can be associated with the production of a higher Lorentz factor jet in M 87. C1 [Hada, K.; Giroletti, M.; Giovannini, G.; D'Ammando, F.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Hada, K.; Akiyama, K.; Honma, M.; Sawada-Satoh, S.; Koyama, S.] Natl Astron Observ Japan, Mizusawa VLBI Observ, Tokyo 1818588, Japan. [Kino, M.] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea. [Kino, M.; Koyama, S.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. [Giovannini, G.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Cheung, C. C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Beilicke, M.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Beilicke, M.; Krawczynski, H.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Nagai, H.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Akiyama, K.; Koyama, S.] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Honma, M.; Niinuma, K.] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan. [Casadio, C.; Gomez, J. L.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Cesarini, A.] Univ Trent, Dept Phys, I-38050 Trento, Italy. [Nakahara, S.] Kagoshima Univ, Fac Sci, Kagoshima, Kagoshima 8900065, Japan. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Yamaguchi Univ, Grad Sch Sci & Engn, Yamaguchi 7538512, Japan. RP Hada, K (reprint author), INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. OI Giovannini, Gabriele/0000-0003-4916-6362; Cesarini, Andrea/0000-0002-8611-8610; Akiyama, Kazunori/0000-0002-9475-4254; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; D'Ammando, Filippo/0000-0001-7618-7527 FU Japan Society for the Promotion of Science (JSPS); KAKENHI [24340042, 24540240, 24540242, 25120007, 26800109]; European Union [RI-261525 NEXPReS]; Smithsonian Institution; Academia Sinica; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX We thank the anonymous referee for the review and suggestions for improving the paper. We are grateful to E. Torresi for reading and helpful comments on the manuscript. The VERA is operated by Mizusawa VLBI Observatory, a branch of National Astronomical Observatory of Japan. K. H. thanks K. M. Shibata, T. Jike, and all of the rest of the staff who helped with operations of the VERA observations presented in this paper. K. H. is supported by the Japan Society for the Promotion of Science (JSPS) Research Fellowship Program for Young Scientists. Part of this work was done with the contribution of the Italian Ministry of Foreign Affairs and University and Research for the collaboration project between Italy and Japan. This work was partially supported by KAKENHI (24340042, 24540240, 24540242, 25120007, and 26800109). e-VLBI research infrastructure in Europe is supported by the European Union's Seventh Framework Programme (FP7/2007-2013) under grant agreement No. RI-261525 NEXPReS. The European VLBI Network is a joint facility of European, Chinese, South African, and other radio astronomy institutes funded by their national research councils. 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.; 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 68 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 JUN 20 PY 2014 VL 788 IS 2 AR 165 DI 10.1088/0004-637X/788/2/165 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200068 ER PT J AU Hunter, TR Brogan, CL Cyganowski, CJ Young, KH AF Hunter, T. R. Brogan, C. L. Cyganowski, C. J. Young, K. H. TI SUBARCSECOND IMAGING OF THE NGC 6334 I(N) PROTOCLUSTER: TWO DOZEN COMPACT SOURCES AND A MASSIVE DISK CANDIDATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; H II regions; ISM: individual objects (NGC 6334 I(N)); ISM: kinematics and dynamics; stars: formation; stars: protostars ID STAR-FORMING REGIONS; HYPERCOMPACT HII-REGIONS; H-II REGIONS; SPATIALLY-RESOLVED CHEMISTRY; EXTENDED GREEN OBJECTS; METHANOL MASER SURVEY; YOUNG STELLAR OBJECT; HIGH-RESOLUTION; RADIO-CONTINUUM; WATER MASER AB Using the Submillimeter Array (SMA) and Karl G. Jansky Very Large Array, we have imaged the massive protocluster NGC 6334 I(N) at high angular resolution (0".5 similar to 650 AU) from 6 cm to 0.87 mm, detecting 18 new compact continuum sources. Three of the new sources are coincident with previously identified H2O masers. Together with the previously known sources, these data bring the number of likely protocluster members to 25 for a protostellar density of similar to 700 pc(-3). Our preliminary measurement of the Q-parameter of the minimum spanning tree is 0.82-close to the value for a uniform volume distribution. All of the (nine) sources with detections at multiple frequencies have spectral energy distributions consistent with dust emission, and two (SMA 1b and SMA 4) also have long wavelength emission consistent with a central hypercompact H II region. Thermal spectral line emission, including CH3CN, is detected in six sources: LTE model fitting of CH3CN (J = 12-11) yields temperatures of 72-373 K, confirming the presence of multiple hot cores. The fitted LSR velocities range from -3.3 to -7.0 kms(-1), with an unbiased mean square deviation of 2.05 km s(-1), implying a protocluster dynamical mass of 410 +/- 260M circle dot. From analysis of a wide range of hot core molecules, the kinematics of SMA 1b are consistent with a rotating, infalling Keplerian disk of diameter 800 AU and enclosed mass of 10-30 M circle dot that is perpendicular (within 1 degrees) to the large-scale bipolar outflow axis. A companion to SMA 1b at a projected separation of (0".45 (590 AU; SMA 1d), which shows no evidence of spectral line emission, is also confirmed. Finally, we detect one 218.4400 GHz and several 229.7588 GHz Class-I CH3OH masers. C1 [Hunter, T. R.; Brogan, C. L.] NRAO, Charlottesville, VA 22903 USA. [Cyganowski, C. J.; Young, K. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cyganowski, C. J.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. RP Hunter, TR (reprint author), NRAO, 520 Edgemont Rd, Charlottesville, VA 22903 USA. EM thunter@nrao.edu OI Hunter, Todd/0000-0001-6492-0090 NR 136 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 20 PY 2014 VL 788 IS 2 AR 187 DI 10.1088/0004-637X/788/2/187 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200090 ER PT J AU Jian, HY Lin, LW Chiueh, T Lin, KY Liu, HB Merson, A Baugh, C Huang, JS Chen, CW Foucaud, S Murphy, DNA Cole, S Burgett, W Kaiser, N AF Jian, Hung-Yu Lin, Lihwai Chiueh, Tzihong Lin, Kai-Yang Liu, Hauyu Baobab Merson, Alex Baugh, Carlton Huang, Jia-Sheng Chen, Chin-Wei Foucaud, Sebastien Murphy, David N. A. Cole, Shaun Burgett, William Kaiser, Nick TI PROBABILITY FRIENDS-OF-FRIENDS (PFOF) GROUP FINDER: PERFORMANCE STUDY AND OBSERVATIONAL DATA APPLICATIONS ON PHOTOMETRIC SURVEYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: groups: general; large-scale structure of universe; methods: data analysis ID GALAXY REDSHIFT SURVEY; GROUP-FINDING ALGORITHM; LARGE-SCALE STRUCTURE; DIGITAL SKY SURVEY; MEDIUM-DEEP SURVEY; COLD DARK MATTER; PAN-STARRS; CLUSTER SURVEY; RED-SEQUENCE; GROUP CATALOG AB In tandem with observational data sets, we utilize realistic mock catalogs, based on a semi-analytic galaxy formation model, constructed specifically for Pan-STARRS1 Medium Deep Surveys to assess the performance of the Probability Friends-of-Friends (PFOF) group finder, and aim to develop a grouping optimization method applicable to surveys like Pan-STARRS1. Producing mock PFOF group catalogs under a variety of photometric redshift accuracies (s.z/(1+ zs)), we find that catalog purities and completenesses from " good" (s.z/(1+ zs) +/- 0.01) to " poor" (s.z/(1+ zs) +/- 0.07) photo-zs gradually degrade from 77% and 70% to 52% and 47%, respectively. A " subset optimization" approach is developed by using spectroscopic-redshift group data from the target field to train the group finder for application to that field and demonstrated using zCOSMOS groups for PFOF searches within PS1 Medium Deep Field04 (PS1MD04) and DEEP2 EGS groups in PS1MD07. With four data sets spanning the photo-z accuracy range from 0.01 to 0.06, we find purities and completenesses agree with their mock analogs. Further tests are performed via matches to X-ray clusters. We find PFOF groups match +/- 85% of X-ray clusters identified in COSMOS and PS1MD04, lending additional support to the reliability of the detection algorithm. In the end, we demonstrate, by separating red and blue group galaxies in the EGS and PS1MD07 group catalogs, that the algorithm is not biased with respect to specifically recovering galaxies by color. The analyses suggest the PFOF algorithm shows great promise as a reliable group finder for photometric galaxy surveys of varying depth and coverage. C1 [Jian, Hung-Yu; Chiueh, Tzihong] Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. [Lin, Lihwai; Lin, Kai-Yang; Liu, Hauyu Baobab; Chen, Chin-Wei; Foucaud, Sebastien] Acad Sin, Inst Astron & Astrophys, Taipei 106, Taiwan. [Chiueh, Tzihong] Natl Taiwan Univ, Ctr Theoret Sci, Taipei 106, Taiwan. [Chiueh, Tzihong] Natl Taiwan Univ, LeCosPa, Taipei 106, Taiwan. [Merson, Alex] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Merson, Alex; Baugh, Carlton; Cole, Shaun] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Huang, Jia-Sheng] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Huang, Jia-Sheng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Foucaud, Sebastien] Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 11677, Taiwan. [Murphy, David N. A.] Pontificia Univ Catolica Chile, Dept Astron & Astrophys, Santiago 7820436, Chile. [Burgett, William; Kaiser, Nick] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Jian, HY (reprint author), Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. EM hyj@phys.ntu.edu.tw RI Baugh, Carlton/A-8482-2012; OI Baugh, Carlton/0000-0002-9935-9755; CHIUEH, TZI-HONG/0000-0003-2654-8763 FU National Science Council of Taiwan [NSC101-2811-M-002-075, NSC992112- M-001-003-MY3, NSC101-2112-M-001-011-MY2, NSC101-2628-M-008-002]; NSF [AST-95-09298, AST-0071048, AST-0507428, AST-0507483]; NASA LTSA grant [NNG04GC89G] FX We thank R. Bower, M. Takada, and M. Oguri for helpful discussions on our algorithm and PFOF applications, and P. Price for the valuable comments. We also thank Brian F. Gerke for providing us with the DEEP2 group catalogs for the PFOF training. The work is supported in part by the National Science Council of Taiwan under the grants NSC101-2811-M-002-075, NSC992112- M-001-003-MY3, NSC101-2112-M-001-011-MY2, and NSC101-2628-M-008-002. This research is Based on zCOSMOS observations carried out using the Very Large Telescope at the ESO Paranal Observatory under Programme ID LP175. A0839. Funding for the DEEP2 Galaxy Redshift Survey has been provided by NSF grants AST-95-09298, AST-0071048, AST-0507428, and AST-0507483 as well as NASA LTSA grant NNG04GC89G. 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, theMax Planck Institute forAstronomyHeidelberg and theMax Planck Institute for Extraterrestrial Physics Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant No. AST-1238877, and theUniversity of Maryland, and Eotvos Lorand University (ELTE). PS1 images and catalogs will be made available through a Pan-STARRS PS1 data release by STScI. We close with thanks to the Hawaiian people for the use of their sacred mountain. NR 77 TC 9 Z9 9 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2014 VL 788 IS 2 AR 109 DI 10.1088/0004-637X/788/2/109 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200012 ER PT J AU Lu, RS Broderick, AE Baron, F Monnier, JD Fish, VL Doeleman, SS Pankratius, V AF Lu, Ru-Sen Broderick, Avery E. Baron, Fabien Monnier, John D. Fish, Vincent L. Doeleman, Sheperd S. Pankratius, Victor TI IMAGING THE SUPERMASSIVE BLACK HOLE SHADOW AND JET BASE OF M87 WITH THE EVENT HORIZON TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; galaxies: jets; submillimeter: galaxies; techniques: high angular resolution; techniques: interferometric ID SAGITTARIUS A-ASTERISK; HIGH-FREQUENCY VLBI; S ACCRETION FLOW; GALACTIC-CENTER; OPTICAL INTERFEROMETRY; STRUCTURAL SIMILARITY; SCHWARZSCHILD RADII; LINE INTERFEROMETRY; RELATIVISTIC JETS; MILLIMETER-VLBI AB The Event Horizon Telescope (EHT) is a project to assemble a Very Long Baseline Interferometry (VLBI) network of millimeter wavelength dishes that can resolve strong field general relativistic signatures near a supermassive black hole. As planned, the EHT will include enough dishes to enable imaging of the predicted black hole "shadow," a feature caused by severe light bending at the black hole boundary. The center of M87, a giant elliptical galaxy, presents one of the most interesting EHT targets as it exhibits a relativistic jet, offering the additional possibility of studying jet genesis on Schwarzschild radius scales. Fully relativistic models of the M87 jet that fit all existing observational constraints now allow horizon-scale images to be generated. We perform realistic VLBI simulations of M87 model images to examine the detectability of the black shadow with the EHT, focusing on a sequence of model images with a changing jet mass load radius. When the jet is launched close to the black hole, the shadow is clearly visible both at 230 and 345 GHz. The EHT array with a resolution of 20-30 mu as resolution (similar to 2-4 Schwarzschild radii) is able to image this feature independent of any theoretical models and we show that imaging methods used to process data from optical interferometers are applicable and effective for EHT data sets. We demonstrate that the EHT is also capable of tracing real-time structural changes on a few Schwarzschild radii scales, such as those implicated by very high-energy flaring activity of M87. While inclusion of ALMA in the EHT is critical for shadow imaging, the array is generally robust against loss of a station. C1 [Lu, Ru-Sen; Fish, Vincent L.; Doeleman, Sheperd S.; Pankratius, Victor] MIT, Haystack Observ, Westford, MA 01886 USA. [Broderick, Avery E.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Broderick, Avery E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Baron, Fabien] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Monnier, John D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Doeleman, Sheperd S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lu, RS (reprint author), MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. EM rslu@haystack.mit.edu FU National Science Foundation; NSF [AST-1310896, AST-1211539]; Gordon & Betty Moore Foundation [GMBF-3561]; Perimeter Institute for Theoretical Physics; Natural Sciences and Engineering Research Council of Canada through a Discovery Grant; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research and Innovation FX We thank the anonymous referee for suggestions that improved the quality of the paper. High frequency VLBI work at MIT Haystack Observatory is supported by grants from the National Science Foundation. This work is also supported through NSF grants AST-1310896, AST-1211539. We acknowledge support from the Gordon & Betty Moore Foundation through award GMBF-3561. A.E.B. receives financial support from 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. We thank Dr. Keiichi Asada for providing information for the Greenland Telescope and Dr. Michael Johnson for useful comments. NR 64 TC 35 Z9 35 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2014 VL 788 IS 2 AR 120 DI 10.1088/0004-637X/788/2/120 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200023 ER PT J AU Raymond, JC McCauley, PI Cranmer, SR Downs, C AF Raymond, J. C. McCauley, P. I. Cranmer, S. R. Downs, C. TI THE SOLAR CORONA AS PROBED BY COMET LOVEJOY (C/2011 W3) SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: individual (C/2011 W3); plasmas; solar wind; Sun: corona; waves ID MAGNETIC-FIELD; ALFVEN WAVES; DENSITY-FLUCTUATIONS; EXTREME-ULTRAVIOLET; SUNGRAZING COMETS; ATOMIC DATABASE; POLAR PLUMES; MHD WAVES; WIND; HELIOSPHERE AB Extreme-ultraviolet images of Comet Lovejoy (C/2011 W3) from the Atmospheric Imaging Assembly show striations related to the magnetic field structure in both open and closed magnetic regions. The brightness contrast implies coronal density contrasts of at least a factor of six between neighboring flux tubes over scales of a few thousand kilometers. These density structures imply variations in the Alfven speed on a similar scale. They will drastically affect the propagation and dissipation of Alfven waves, and that should be taken into account in models of coronal heating and solar wind acceleration. In each striation, the cometary emission moves along the magnetic field and broadens with time. The speed and the rate of broadening are related to the parallel and perpendicular components of the velocities of the cometary neutrals when they become ionized. We use a magnetohydrodynamic model of the coronal magnetic field and the theory of pickup ions to compare the measurements with theoretical predictions, in particular with the energy lost to Alfven waves as the cometary ions isotropize. C1 [Raymond, J. C.; McCauley, P. I.; Cranmer, S. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Downs, C.] Predict Sci Inc, San Diego, CA 92121 USA. RP Raymond, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI McCauley, Patrick/P-7747-2015; OI McCauley, Patrick/0000-0002-1450-7350; Cranmer, Steven/0000-0002-3699-3134 FU NSF SHINE [AGS-1259519]; NASA [SPH02H1701R]; Lockheed Martin for NASA [NNG04EA00]; NASA Heliophysics Theory Program FX Patrick McCauley was supported by NSF SHINE grant AGS-1259519 and NASA grant SPH02H1701R for SDO/AIA to the Smithsonian Astrophysical Observatory. SDO is a NASA satellite and the AIA instrument team is led by Lockheed Martin, with SAO as a major subcontractor. Cooper Downs was supported by a subcontract from Lockheed Martin for NASA contract NNG04EA00, and by NASA Heliophysics Theory Program. MHD simulations were conducted on the NASA Pleiades and NSF Ranger supercomputers. This work benefitted from discussions at the workshop on the Science of Near-Sun Comets at the International Space Sciences Institute. NR 67 TC 11 Z9 11 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2014 VL 788 IS 2 AR 152 DI 10.1088/0004-637X/788/2/152 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200055 ER PT J AU Sliski, DH Kipping, DM AF Sliski, David H. Kipping, David M. TI A HIGH FALSE POSITIVE RATE FOR KEPLER PLANETARY CANDIDATES OF GIANT STARS USING ASTERODENSITY PROFILING SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; methods: data analysis; planetary systems; planets and satellites: general; techniques: photometric ID LIGHT-CURVE; TRANSIT DETECTION; II. ANALYSIS; ASTEROSEISMOLOGY; VALIDATION; EFFICIENT; ECCENTRICITIES; AMPLITUDES; PARAMETERS; EXOPLANETS AB Asterodensity profiling (AP) is a relatively new technique for studying transit light curves. By comparing the mean stellar density derived from the transit light curve to that found through an independent method, AP provides information on several useful properties such as orbital eccentricity and blended light. We present an AP survey of 41 Kepler Objects of Interest (KOIs), with a single transiting candidate, for which the target star's mean stellar density has been measured using asteroseismology. The ensemble distribution of the AP measurements for the 31 dwarf stars in our sample shows excellent agreement with the spread expected if the KOIs were genuine and have realistic eccentricities. In contrast, the same test for the 10 giants in our sample reveals significant incompatibility at > 4 sigma confidence. While extreme eccentricities could be invoked, this hypothesis requires four of the KOIs to contact their host star at periastron passage, including the recently claimed confirmation of Kepler-91b. After carefully examining several hypotheses, we conclude that the most plausible explanation is that the transiting objects orbit a different star to that measured with asteroseismology-cases we define as false-positives. Based on the AP distribution, we estimate a false-positive rate (FPR) for Kepler's giant stars with a single transiting object of FPR similar or equal to 70% +/- 30%. C1 [Sliski, David H.; Kipping, David M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sliski, DH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dsliski@cfa.harvard.edu NR 54 TC 25 Z9 25 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2014 VL 788 IS 2 AR 148 DI 10.1088/0004-637X/788/2/148 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200051 ER PT J AU Kubiczek, K Renner, SC Bohm, SM Kalko, EKV Wells, K AF Kubiczek, Katrin Renner, Swen C. Boehm, Stefan M. Kalko, Elisabeth K. V. Wells, Konstans TI Movement and ranging patterns of the Common Chaffinch in heterogeneous forest landscapes SO PEERJ LA English DT Article DE Animal tracking; Bird movement capacity; Habitat use; Landscape heterogeneity; Hierarchical habitat selection; Multilevel hierarchical regression ID YELLOWSTONE-NATIONAL-PARK; FRINGILLA-COELEBS; HABITAT SELECTION; ANIMAL MOVEMENT; HOME RANGES; BEHAVIOR; BIRDS; MODELS; TERRITORIES; SCALE AB The partitioning of production forests into discretely managed forest stands confronts animals with diversity in forest attributes at scales from point-level tree assemblages to distinct forest patches and range-level forest cover. We have investigated the movement and ranging patterns of male Common Chaffinches, Fringilla coelebs, in heterogeneous forest production landscapes during spring and summer in south-western Germany. We radio-tracked a total of 15 adult males, each for up to six days, recording locations at 10-min intervals. We then performed point-level tree surveys at all tracking locations and classified forest stand attributes for the areal covering of birds' ranges. Movement distances were shortest in beech forest stands and longer in spruce-mixed and non-spruce conifer stands. Movement distances increased with stand age in beech stands but not in others, an effect that was only detectable in a multilevel hierarchical model. We found negligible effects of point-level tree assemblages and temperature on movement distances. Daily range estimates were from 0.01 to 8.0 hectare (median of 0.86 ha) with no evident impact of forest attributes on ranging patterns but considerable intra-individual variation in range sizes over consecutive days. Most daily ranges covered more than one forest stand type. Our results show that forest management impacts the movement behaviour of chaffinches in heterogeneous production forest. Although point-level effects of movement distances are weak compared with stand-level effects in this study, the hierarchical organization of forest is an important aspect to consider when analysing fine-scale movement and might exert more differentiated effects on bird species that are more sensitive to habitat changes than the chaffinch. C1 [Kubiczek, Katrin; Renner, Swen C.; Boehm, Stefan M.; Kalko, Elisabeth K. V.; Wells, Konstans] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Renner, Swen C.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Wells, Konstans] Univ Adelaide, Sch Earth & Environm Sci, Inst Environm, Adelaide, SA, Australia. RP Renner, SC (reprint author), Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. EM swen.renner@uni-ulm.de RI Wells, Konstans/A-7232-2010; OI Wells, Konstans/0000-0003-0377-2463; Renner, Swen/0000-0002-6893-4219 FU DFG priority programme 'Biodiversity Exploratories' [1374, KA 1241/15-1] FX This study benefited from the infrastructure of the DFG priority programme 1374 'Biodiversity Exploratories' (KA 1241/15-1). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 50 TC 1 Z9 1 U1 1 U2 15 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD JUN 19 PY 2014 VL 2 AR e368 DI 10.7717/peerj.368 PG 18 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AY5KI UT WOS:000347610600001 PM 25024900 ER PT J AU Ade, PAR Aikin, RW Barkats, D Benton, SJ Bischoff, CA Bock, JJ Brevik, JA Buder, I Bullock, E Dowell, CD Duband, L Filippini, JP Fliescher, S Golwala, SR Halpern, M Hasselfield, M Hildebrandt, SR Hilton, GC Hristov, VV Irwin, KD Karkare, KS Kaufman, JP Keating, BG Kernasovskiy, SA Kovac, JM Kuo, CL Leitch, EM Lueker, M Mason, P Netterfield, CB Nguyen, HT O'Brient, R Ogburn, RW Orlando, A Pryke, C Reintsema, CD Richter, S Schwarz, R Sheehy, CD Staniszewski, ZK Sudiwala, RV Teply, GP Tolan, JE Turner, AD Vieregg, AG Wong, CL Yoon, KW AF Ade, P. A. R. Aikin, R. W. Barkats, D. Benton, S. J. Bischoff, C. A. Bock, J. J. Brevik, J. A. Buder, I. Bullock, E. Dowell, C. D. Duband, L. Filippini, J. P. Fliescher, S. Golwala, S. R. Halpern, M. Hasselfield, M. Hildebrandt, S. R. Hilton, G. C. Hristov, V. V. Irwin, K. D. Karkare, K. S. Kaufman, J. P. Keating, B. G. Kernasovskiy, S. A. Kovac, J. M. Kuo, C. L. Leitch, E. M. Lueker, M. Mason, P. Netterfield, C. B. Nguyen, H. T. O'Brient, R. Ogburn, R. W. Orlando, A. Pryke, C. Reintsema, C. D. Richter, S. Schwarz, R. Sheehy, C. D. Staniszewski, Z. K. Sudiwala, R. V. Teply, G. P. Tolan, J. E. Turner, A. D. Vieregg, A. G. Wong, C. L. Yoon, K. W. CA BICEP2 Collaboration TI Detection of B-Mode Polarization at Degree Angular Scales by BICEP2 SO PHYSICAL REVIEW LETTERS LA English DT Article ID MICROWAVE BACKGROUND POLARIZATION; PROBE WMAP OBSERVATIONS; INFLATIONARY UNIVERSE SCENARIO; SPT-SZ SURVEY; POWER SPECTRA; SYMMETRY-BREAKING; PHASE-TRANSITION; CMB POLARIMETRY; GRAVITY-WAVES; ANISOTROPY AB We report results from the BICEP2 experiment, a cosmic microwave background (CMB) polarimeter specifically designed to search for the signal of inflationary gravitational waves in the B-mode power spectrum around l similar to 80. The telescope comprised a 26 cm aperture all-cold refracting optical system equipped with a focal plane of 512 antenna coupled transition edge sensor 150 GHz bolometers each with temperature sensitivity of approximate to 300 mu K-CMB root s. BICEP2 observed from the South Pole for three seasons from 2010 to 2012. A low-foreground region of sky with an effective area of 380 square deg was observed to a depth of 87 nK deg in Stokes Q and U. In this paper we describe the observations, data reduction, maps, simulations, and results. We find an excess of B-mode power over the base lensed-ACDM expectation in the range 30 < l < 150, inconsistent with the null hypothesis at a significance of > 5 sigma. Through jackknife tests and simulations based on detailed calibration measurements we show that systematic contamination is much smaller than the observed excess. Cross correlating against WMAP 23 GHz maps we find that Galactic synchrotron makes a negligible contribution to the observed signal. We also examine a number of available models of polarized dust emission and find that at their default parameter values they predict power similar to(5-10)x smaller than the observed excess signal (with no significant cross-correlation with our maps). However, these models are not sufficiently constrained by external public data to exclude the possibility of dust emission bright enough to explain the entire excess signal. Cross correlating BICEP2 against 100 GHz maps from the BICEP1 experiment, the excess signal is confirmed with 3 sigma significance and its spectral index is found to be consistent with that of the CMB, disfavoring dust at 1.7 sigma. The observed B-mode power spectrum is well fit by a lensed-ACDM + tensor theoretical model with tensor-to-scalar ratio r = 0.20(-0.05)(+0.07), with r = 0 disfavored at 7.0 sigma. Accounting for the contribution of foreground, dust will shift this value downward by an amount which will be better constrained with upcoming data sets. C1 [Ade, P. A. R.; Sudiwala, R. V.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aikin, R. W.; Bock, J. J.; Brevik, J. A.; Filippini, J. P.; Golwala, S. R.; Hildebrandt, S. R.; Hristov, V. V.; Lueker, M.; Mason, P.; Staniszewski, Z. K.; Teply, G. P.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Barkats, D.] Joint ALMA Observ, Santiago, Chile. [Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Bischoff, C. A.; Buder, I.; Karkare, K. S.; Kovac, J. M.; Richter, S.; Vieregg, A. G.; Wong, C. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bock, J. J.; Dowell, C. D.; Hildebrandt, S. R.; Nguyen, H. T.; O'Brient, R.; Staniszewski, Z. K.; Turner, A. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bullock, E.; Pryke, C.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Duband, L.] CEA, Serv Basses Temp, F-38054 Grenoble, France. [Fliescher, S.; Pryke, C.; Schwarz, R.; Sheehy, C. D.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Halpern, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Hilton, G. C.; Irwin, K. D.; Reintsema, C. D.] NIST, Boulder, CO 80305 USA. [Irwin, K. D.; Kernasovskiy, S. A.; Kuo, C. L.; Ogburn, R. W.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Irwin, K. D.; Kuo, C. L.; Ogburn, R. W.; Yoon, K. W.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Kaufman, J. P.; Keating, B. G.; Orlando, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Leitch, E. M.; Orlando, A.; Sheehy, C. D.; Vieregg, A. G.] Univ Chicago, Chicago, IL 60637 USA. [Netterfield, C. B.] Canadian Inst Adv Res, Toronto, ON M5G 1Z8, Canada. RP Ade, PAR (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. EM jmkovac@cfa.harvard.edu; pryke@physics.umn.edu OI Orlando, Angiola/0000-0001-8004-5054; Karkare, Kirit/0000-0002-5215-6993; Barkats, Denis/0000-0002-8971-1954 FU U.S. National Science Foundation [ANT-0742818, ANT-1044978, ANT-0742592, ANT-1110087]; NASA APRA [06-ARPA206-0040, 10-SAT10-0017]; SAT programs; Gordon and Betty Moore Foundation at Caltech; Canada Foundation for Innovation grant; W. M. Keck Foundation; FAS Science Division Research Computing Group at Harvard University; U.S. Department of Energy Office of Science FX BICEP2 was supported by the U.S. National Science Foundation under Grants No. ANT-0742818 and No. ANT-1044978 (Caltech and Harvard) and ANT-0742592 and ANT-1110087 (Chicago and Minnesota). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and Grants No. 06-ARPA206-0040 and No. 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The receiver development was supported in part by a grant from the W. M. Keck Foundation. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. Department of Energy Office of Science. Tireless administrative support was provided by Irene Coyle and Kathy Deniston. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. We thank all those who have contributed past efforts to the BICEP-Keck Array series of experiments, including the BICEP1 and Keck Array teams. We thank all those in the astrophysics community who have contributed feedback on the public preprint of this paper, and particularly two anonymous referees for their detailed and constructive recommendations. This work would not have been possible without the late Andrew Lange, whom we sorely miss. NR 103 TC 793 Z9 794 U1 11 U2 82 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JUN 19 PY 2014 VL 112 IS 24 AR 241101 DI 10.1103/PhysRevLett.112.241101 PG 25 WC Physics, Multidisciplinary SC Physics GA AO0MN UT WOS:000341003800002 PM 24996078 ER PT J AU Fortenberry, RC Huang, XC McCarthy, MC Crawford, TD Lee, TJ AF Fortenberry, Ryan C. Huang, Xinchuan McCarthy, Michael C. Crawford, T. Daniel Lee, Timothy J. TI Fundamental Vibrational Frequencies and Spectroscopic Constants of cis- and trans-HOCS, HSCO, and Isotopologues via Quartic Force Fields SO JOURNAL OF PHYSICAL CHEMISTRY B LA English DT Article ID SHELL HARTREE-FOCK; CORRELATED MOLECULAR CALCULATIONS; GAUSSIAN-BASIS SETS; ELECTRON-AFFINITIES; WAVE-FUNCTIONS; CHEMISTRY; ENERGIES; INTERMEDIATE; GRADIENTS; HYDROGEN AB Highly accurate, coupled-cluster-based quartic force fields (QFFs) have been employed recently to provide spectroscopic reference for a myriad of molecules. Here, we are extending the same approach to provide vibrational and rotational spectroscopic reference data for the sulfur analogues of HOCO, HSCO, and HOCS, in both the cis and trans conformations as well as the D and S-34 isotopologues of each system. The resulting energies corroborate previous computations showing that trans-HSCO is the lowest-energy isomer for this system. The vibrational frequencies are computed with both second-order vibrational perturbation theory (VPT2) and vibrational configuration interaction (VCI) methods. The VPT2 and VCI QFF frequencies largely agree with one another to better than 5.0 cm(-1) (often better than 1.0 cm(-1)) and are also consistent with the type of behavior exhibited in previous studies. As such, the reference data provided here should assist in analysis of environments in which these sulfur systems may be found, including the interstellar medium, combustion flames, or laboratory simulations of either. C1 [Fortenberry, Ryan C.] Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA. [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. [McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Crawford, T. Daniel] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA. [Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Fortenberry, RC (reprint author), Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA. EM rfortenberry@georgiasouthern.edu; Timothy.J.Lee@nasa.gov RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013; Crawford, Thomas/A-9271-2017; OI Crawford, Thomas/0000-0002-7961-7016; McCarthy, Michael/0000-0001-9142-0008 FU RCF; NASA; Georgia Southern University; NASA [NNX13AE59G, 10-APRA10-0167]; NSF [CHE-1058420]; NASA/SETI Institute [NNX12AG96A]; NSF Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) Award [CHE-0741927]; NASA's Laboratory Astrophysics 'Carbon in the Galaxy' Consortium Grant [NNH10ZDA001N] FX The authors would like to acknowledge the following sources of funding: RCF, the NASA Postdoctoral Program administered by Oak Ridge Associated Universities, as well as Georgia Southern University for start-up funds; M.C.M., NASA Award NNX13AE59G; T.D.C., NSF Award CHE-1058420; XI I., NASA/SETI Institute Cooperative Agreement NNX12AG96A; T.J.L., NASA Grant 10-APRA10-0167; R.C.F. and T.D.C., NSF Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) Award CHE-0741927; and R.C.F., X.H., and T.J.L., NASA's Laboratory Astrophysics 'Carbon in the Galaxy' Consortium Grant (NNH10ZDA001N). NR 52 TC 5 Z9 5 U1 3 U2 12 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1520-6106 J9 J PHYS CHEM B JI J. Phys. Chem. B PD JUN 19 PY 2014 VL 118 IS 24 SI SI BP 6498 EP 6510 DI 10.1021/jp412362h PG 13 WC Chemistry, Physical SC Chemistry GA AJ6FC UT WOS:000337784100017 PM 24635494 ER PT J AU Fang, W Tu, H Li, Y Huang, JS Shu, CG AF Fang, Wei Tu, Hong Li, Ying Huang, Jiasheng Shu, Chenggang TI Full investigation on the dynamics of power-law kinetic quintessence SO PHYSICAL REVIEW D LA English DT Article ID ACCELERATING UNIVERSE; COSMOLOGICAL CONSTANT; SUPERNOVAE AB We give a full investigation on the dynamics of power-law kinetic quintessence LdX;._Vd._d- X _ X2 by considering the potential related parameter Gd VV00 V02 _ as a function of another potential parameter.d V0.V3= 2, which correspondingly extends the analysis of the dynamical system of our Universe from two dimensional to three dimensional. In addition to the critical points found in previous papers, we find a new de Sitter- like dominant attractor ( cp6) and give its stable condition using the center manifold theorem. For the dark energy dominant solution ( cp6 and cp7), it could be distinguished from canonical quintessence and tachyon models since the sound speed c2s 0 or c2s 1. For the scaling solution ( cp8), it is very interesting that the sound speed c2s 1= 5, while it behaves as ordinary matter. We therefore point out that the power- law kinetic quintessence should have different signatures on the cold dark matter power spectrum and the cosmic microwave background both at early time, when this scalar field is an early dark energy with O. being non- negligible at high redshift, and at late time, when it drives the accelerating expansion. We still do not know whether there are any degeneracies of the impacts between these two epoches. They are expected to be investigated in future. C1 [Fang, Wei; Tu, Hong] Shanghai Normal Univ, Dept Phys, Shanghai 200234, Peoples R China. [Fang, Wei; Tu, Hong; Shu, Chenggang] Shanghai Key Lab Astrophys, Shanghai 200234, Peoples R China. [Fang, Wei; Huang, Jiasheng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Li, Ying] Shanghai Ocean Univ, Coll Informat Technol, Shanghai 201306, Peoples R China. RP Fang, W (reprint author), Shanghai Normal Univ, Dept Phys, 100 Guilin Rd, Shanghai 200234, Peoples R China. EM wfang@shnu.edu.cn NR 48 TC 1 Z9 1 U1 2 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD JUN 18 PY 2014 VL 89 IS 12 AR 123514 DI 10.1103/PhysRevD.89.123514 PG 9 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AK6IS UT WOS:000338531900003 ER PT J AU Cook-Patton, SC Maynard, L Lemoine, NP Shue, J Parker, JD AF Cook-Patton, Susan C. Maynard, Lauren Lemoine, Nathan P. Shue, Jessica Parker, John D. TI Cascading effects of a highly specialized beech-aphid-fungus interaction on forest regeneration SO PEERJ LA English DT Article DE Seedling survival; Grylloprociphilus imbricator; Scorias spongiosa; Forest regeneration; Fagus grandifolia; Specialist herbivore; Indirect interactions ID TROPICAL FORESTS; COEXISTENCE; INVASIONS; HERBIVORY; ECOLOGY; HISTORY AB Specialist herbivores are thought to often enhance or maintain plant diversity within ecosystems, because they prevent their host species from becoming competitively dominant. In contrast, specialist herbivores are not generally expected to have negative impacts on non-hosts. However, we describe a cascade of indirect interactions whereby a specialist sooty mold (Scorias spongiosa) colonizes the honeydew from a specialist beech aphid (Grylloprociphilus imbricator), ultimately decreasing the survival of seedlings beneath American beech trees (Fagus grandifolia). A common garden experiment indicated that this mortality resulted from moldy honeydew impairing leaf function rather than from chemical or microbial changes to the soil. In addition, aphids consistently and repeatedly colonized the same large beech trees, suggesting that seedling-depauperate islands may form beneath these trees. Thus this highly specialized three-way beech-aphid-fungus interaction has the potential to negatively impact local forest regeneration via a cascade of indirect effects. C1 [Cook-Patton, Susan C.; Maynard, Lauren; Shue, Jessica; Parker, John D.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Lemoine, Nathan P.] Florida Int Univ, Miami, FL 33199 USA. RP Cook-Patton, SC (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM cook-pattons@si.edu RI Parker, John/F-9761-2010 OI Parker, John/0000-0002-3632-7625 FU Washington Biologists Field Club; NSF-REU [DBI 156799] FX A grant from the Washington Biologists Field Club to SCC and JDP, and an NSF-REU grant to JDP (DBI 156799) supported this research. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 27 TC 0 Z9 0 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 JUN 17 PY 2014 VL 2 AR e442 DI 10.7717/peerj.442 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AY5KG UT WOS:000347610300008 PM 25024911 ER PT J AU Meyer, JL Paul, VJ Teplitski, M AF Meyer, Julie L. Paul, Valerie J. Teplitski, Max TI Community Shifts in the Surface Microbiomes of the Coral Porites astreoides with Unusual Lesions SO PLOS ONE LA English DT Article ID WHITE PLAGUE DISEASE; REEF-BUILDING CORAL; BACTERIAL COMMUNITIES; MONTASTRAEA-FAVEOLATA; CLIMATE-CHANGE; SP NOV.; INFECTIOUS-DISEASES; PHAGE THERAPY; RED-SEA; ENDOZOICOMONAS AB Apical lesions on Porites astreoides were characterized by the appearance of a thin yellow band, which was preceded by bleaching of the coral tissues and followed by a completely denuded coral skeleton, which often harbored secondary macroalgal colonizers. These characteristics have not been previously described in Porites and do not match common Caribbean coral diseases. The lesions were observed only in warmer months and at shallow depths on the fore reef in Belize. Analysis of the microbial community composition based on the V4 hypervariable region of 16S ribosomal RNA genes revealed that the surface microbiomes associated with nonsymptomatic corals were dominated by the members of the genus Endozoicomonas, consistent with other studies. Comparison of the microbiomes of nonsymptomatic and lesioned coral colonies sampled in July and September revealed two distinct groups, inconsistently related to the disease state of the coral, but showing some temporal signal. The loss of Endozoicomonas was characteristic of lesioned corals, which also harbored potential opportunistic pathogens such as Alternaria, Stenotrophomonas, and Achromobacter. The presence of lesions in P. astreoides coincided with a decrease in the relative abundance of Endozoicomonas, rather than the appearance of specific pathogenic taxa. C1 [Meyer, Julie L.; Teplitski, Max] Univ Florida, Inst Food & Agr Sci, Dept Soil & Water Sci, Gainesville, FL 32611 USA. [Paul, Valerie J.; Teplitski, Max] Smithsonian Marine Stn, Ft Pierce, FL USA. RP Teplitski, M (reprint author), Univ Florida, Inst Food & Agr Sci, Dept Soil & Water Sci, Gainesville, FL 32611 USA. EM maxtep@ufl.edu RI Meyer, Julie/D-1021-2010 OI Meyer, Julie/0000-0003-3382-3321 FU George E. Burch Fellowship in Theoretical Medicine and Affiliated Sciences at the Smithsonian Institution; National Geographic Society Committee for Research Exploration grant [9184-12] FX Support for this research was provided by the George E. Burch Fellowship in Theoretical Medicine and Affiliated Sciences at the Smithsonian Institution; M.T. was a 2012 recipient of this fellowship. Funding for sample collection was provided by the National Geographic Society Committee for Research Exploration grant # 9184-12. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 76 TC 19 Z9 19 U1 1 U2 34 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUN 17 PY 2014 VL 9 IS 6 AR e100316 DI 10.1371/journal.pone.0100316 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AK5YM UT WOS:000338503400104 PM 24937478 ER PT J AU Heinze, CR Freeman, LM Martin, CR Power, ML Fascetti, AJ AF Heinze, Cailin R. Freeman, Lisa M. Martin, Camilia R. Power, Michael L. Fascetti, Andrea J. TI Comparison of the nutrient composition of commercial dog milk replacers with that of dog milk SO JAVMA-JOURNAL OF THE AMERICAN VETERINARY MEDICAL ASSOCIATION LA English DT Article ID POLYUNSATURATED FATTY-ACIDS; ALPHA-LINOLENIC ACID; DOCOSAHEXAENOIC ACID; NEURAL DEVELOPMENT; RETINAL FUNCTIONS; LACTATION; PUPPIES; GESTATION; KITTENS; INFANTS AB Objective-To compare the nutrient composition of commercially available dog milk replacers with that of dog milk. Design-Prospective, cross-sectional study. Sample-5 dog milk samples and 15 samples of commercial dog milk replacers. Procedures-Dog milk and milk replacers were analyzed for concentrations of total protein, essential amino acids, sugars, total fat, essential fatty acids, calcium, and phosphorus. Energy density was calculated. Results from milk replacers were compared with the range of the concentration of each nutrient in milk samples from mature dogs as well as the National Research Council (NRC) recommendations for puppy growth. Results-Milk replacers varied widely in caloric density and concentration of nutrients such as calcium, protein, and fat. Calcium concentration was lower in 14 of 15 milk replacers than in the dog milk samples. Docosahexaenoic acid was undetectable in 12 of 15 milk replacers but present in all dog milk samples. All milk replacers had numerous essential nutrients outside of the range of the dog milk samples, and many had concentrations of amino acids, essential fatty acids, calcium, and phosphorus less than the NRC minimal requirement or recommended allowance. Compared with NRC recommendations, some dog milk samples had concentrations of total protein, linoleic acid, calcium, or phosphorus less than the recommended allowance. Conclusions and Clinical Relevance-Results suggested that there was substantial variation in nutrient composition of 15 dog milk replacers and that some products were closer approximations of dog milk than others. Nearly all products would benefit from more appropriate calcium, amino acids, and essential fatty acids concentrations and better feeding directions. C1 [Heinze, Cailin R.; Freeman, Lisa M.] Tufts Univ, Cummings Sch Vet Med, Dept Clin Sci, North Grafton, MA 01536 USA. [Martin, Camilia R.] Beth Israel Deaconess Med Ctr, Dept Neonatol, Boston, MA 02215 USA. [Power, Michael L.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Washington, DC USA. [Fascetti, Andrea J.] Univ Calif Davis, Sch Vet Med, Dept Mol Biosci, Davis, CA 95616 USA. RP Heinze, CR (reprint author), Tufts Univ, Cummings Sch Vet Med, Dept Clin Sci, North Grafton, MA 01536 USA. EM cailin.heinze@tufts.edu FU Nestle Purina PetCare FX Supported by a grant from Nestle Purina PetCare. NR 38 TC 1 Z9 1 U1 2 U2 16 PU AMER VETERINARY MEDICAL ASSOC PI SCHAUMBURG PA 1931 N MEACHAM RD SUITE 100, SCHAUMBURG, IL 60173-4360 USA SN 0003-1488 EI 1943-569X J9 JAVMA-J AM VET MED A JI JAVMA-J. Am. Vet. Med. Assoc. PD JUN 15 PY 2014 VL 244 IS 12 BP 1413 EP 1422 PG 10 WC Veterinary Sciences SC Veterinary Sciences GA CA6CK UT WOS:000348995800023 PM 24871064 ER PT J AU Verhoeven, JTA Laanbroek, HJ Rains, MC Whigham, DF AF Verhoeven, Jos T. A. Laanbroek, Hendrikus J. Rains, Mark C. Whigham, Dennis F. TI Effects of increased summer flooding on nitrogen dynamics in impounded mangroves SO JOURNAL OF ENVIRONMENTAL MANAGEMENT LA English DT Article DE Mangrove; Nitrogen cycling; Hydroperiod; Water management; Mosquito control; Avicennia ID INDIAN RIVER LAGOON; AVICENNIA-GERMINANS; SALT-MARSH; FLORIDA; FOREST; ECOSYSTEMS; DENITRIFICATION; LIMITATION; SEDIMENTS; SALINITY AB Mangroves are important for coastal protection, carbon sequestration and habitat provision for plants and animals in the tropics and subtropics. Mangroves are threatened by habitat destruction and sea level rise, but management activities such as impounding for mosquito control can also have negative effects. We studied the effects of Rotational Impoundment Management (RIM) on nitrogen dynamics in impoundments dominated by three types of Black mangrove (Avicennia germinans) stands along the Indian River Lagoon (Florida). RIM, designed for noxious insect control, involves pumping estuarine water into impoundments in this area during spring and summer to raise water levels by 30 cm. We compared aspects of the nitrogen cycle before and after the start of the RIM and measured the same variables in an impoundment without RIM management. RIM led to the accumulation of ammonium in the substrate which coincided with a lowering of nitrification rates and decreased denitrification rates. Salt pan habitats dominated by dwarf mangroves became less saline following RIM initiation. Shoot growth of mangroves increased in response to higher nitrogen availability and lower pore water salinity. Mangrove responses were greatest in areas with dwarf and sparse mangrove cover. Overall, RIM resulted in lower nitrification and denitrification leading to lower nitrogen losses and increased Black mangrove growth, all benefits of RIM beyond those associated with noxious insect control. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Verhoeven, Jos T. A.; Laanbroek, Hendrikus J.] Univ Utrecht, Inst Environm Biol, NL-3584 CH Utrecht, Netherlands. [Verhoeven, Jos T. A.; Laanbroek, Hendrikus J.; Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MA 21037 USA. [Laanbroek, Hendrikus J.] Netherlands Inst Ecol NIOO KNAW, Dept Microbial Ecol, NL-6700 AB Wageningen, Netherlands. [Rains, Mark C.] Univ S Florida, Sch Geosci, Tampa, FL 33620 USA. RP Verhoeven, JTA (reprint author), Univ Utrecht, Inst Environm Biol, Padualaan 8, NL-3584 CH Utrecht, Netherlands. EM j.t.a.verhoeven@uu.nl; r.laanbroek@nioo.knaw.nl; mrains@usf.edu; whighamd@si.edu RI Library, Library/A-4320-2012; Laanbroek, Hendrikus J./C-3830-2008; OI Library, Library/0000-0002-3835-159X; Laanbroek, Hendrikus J./0000-0003-2400-3399; Whigham, Dennis/0000-0003-1488-820X FU Smithsonian Marine Science Network (Smithsonian Marine Station at Fort Pierce, Florida) [945]; Smithsonian Environmental Research Center, Utrecht University; Netherlands Institute of Ecology and the University of South Florida FX The research was supported by grants from the Smithsonian Marine Science Network (Smithsonian Marine Station at Fort Pierce, Florida, Contribution No. 945.) and by resources of the Smithsonian Environmental Research Center, Utrecht University, The Netherlands, the Netherlands Institute of Ecology and the University of South Florida. We thank Gerrit Rouwenhorst, Paul van der Ven, Christina Stinger and Jay O'Neill for assistance with the field work and analytical processing of samples. Special thanks to Dr. Valerie Paul, Woody Lee and other staff at the Smithsonian Marine Station at Fort Pierce for their great help and support. This is publication number 5592 of the Netherlands Institute of Ecology (NIOO-KNAW) and publication number yyyy of the Smithsonian Marine Station at Fort Pierce. NR 41 TC 3 Z9 3 U1 2 U2 37 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0301-4797 EI 1095-8630 J9 J ENVIRON MANAGE JI J. Environ. Manage. PD JUN 15 PY 2014 VL 139 BP 217 EP 226 DI 10.1016/j.jenvman.2014.02.035 PG 10 WC Environmental Sciences SC Environmental Sciences & Ecology GA AJ7HG UT WOS:000337867200023 PM 24751377 ER PT J AU Hong, T AF Hong, Terry TI Colorless Tsukuru Tazaki and His Years of Pilgrimage SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20013 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20013 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 15 PY 2014 VL 139 IS 11 BP 87 EP 87 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA AI7MD UT WOS:000337074000110 ER PT J AU Riley, SM AF Riley, Sheila M. TI Dirty Work SO LIBRARY JOURNAL LA English DT Book Review C1 [Riley, Sheila M.] Smithsonian Inst Libs, Washington, DC 20560 USA. RP Riley, SM (reprint author), Smithsonian Inst Libs, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 15 PY 2014 VL 139 IS 11 BP 89 EP 89 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA AI7MD UT WOS:000337074000119 ER PT J AU Buzas-Stephens, P Livsey, DN Simms, AR Buzas, MA AF Buzas-Stephens, Pamela Livsey, Daniel N. Simms, Alexander R. Buzas, Martin A. TI Estuarine foraminifera record Holocene stratigraphic changes and Holocene climate changes in ENSO and the North American monsoon: Baffin Bay, Texas SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Holocene climate change; Foraminifera; El Nino-Southern Oscillation; North American monsoon; Baffin Bay,Texas ID SEA-LEVEL; EL-NINO; LATE QUATERNARY; VARIABILITY; LAKE; OSCILLATION; AGE; USA; UK AB During the last Quaternary sea level fall (120- ka), Baffin Bay was formed by the down-cutting of the Los Olmos, San Fernando, and Petronila Creeks of south Texas. When sea level rose, this incised valley was then filled with mixed siliciclastic/carbonate sediments that record coastal environmental change over the past 10 Icy. Previous sedimentological and seismic analysis shows that Baffin Bay contains atypical depositional environments as a result of its semi-arid climate setting and isolation from the Gulf of Mexico. Three prominent stratigraphic surfaces can be recognized within the bay deposits, and are chronostratigraphically constrained using radiocarbon dates. The purpose of the present study is to use foraminifera to create a separate account of change and to determine if foraminiferal data corroborate sedimentological evidence for sea level and climate fluctuations. Foraminifera were sampled at 20 cm intervals from a 14.4 m dated core and from surface and subsurface sediments of five cores along a dip transect. Multiple discriminate analysis was used to compare sections of the core by species proportions, and clearly delineates three different foraminiferal communities: deltaic, open-bay, and hypersaline. Breaks between these communities coincide with two of the surfaces observed in the core, one at about 8.0 Icy and the other around 5.5 ky. Rapid sea level rise at the 8.0 ky flooding surface corresponds with a shift from a deltaic to an open-bay foraminiferal assemblage, while faunal change across the 5.5 ky surface is due to the formation of a large barrier island (Padre Island) and the onset of more arid climate conditions. Prior to the isolation of Baffin Bay at 55 Icy, foraminiferal assemblages do not correspond to climate change records, perhaps because open circulation with the Gulf of Mexico tempered regional climate effects on bay salinity. After 5.5 ky, changes in foraminiferal assemblages correspond to independently derived records of the El Niflo-Southern Oscillation and North American monsoon. Foraminiferal analysis supports sedimentological interpretations in that assemblages and sediments track climate change. (C) 2014 Elsevier B.V. All rights reserved. C1 [Buzas-Stephens, Pamela] Midwestern State Univ, Dept Geosci, Wichita Falls, TX 76308 USA. [Livsey, Daniel N.; Simms, Alexander R.] Univ Calif Santa Barbara, Dept Earth Sci, Santa Barbara, CA 93106 USA. [Buzas, Martin A.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Buzas-Stephens, P (reprint author), Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. EM pamela.stephens@colorado.edu; dnl@umail.ucsb.edu; asimms@geol.ucsb.edu; BUZASM@si.edu FU Petroleum Research Fund of the American Chemical Society [44868-GB8]; NSF [EAR-0921963]; NSF Graduate Research Fellowship [DGE-1144085] FX This work was made possible by a supplemental summer grant from the Petroleum Research Fund of the American Chemical Society (grant number 44868-GB8), and was also partially supported by an NSF grant EAR-0921963 and an NSF Graduate Research Fellowship grant DGE-1144085. The authors also wish to thank the editor and reviewers for their constructive comments which have served to strengthen this paper. NR 60 TC 4 Z9 4 U1 1 U2 19 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 15 PY 2014 VL 404 BP 44 EP 56 DI 10.1016/j.palaeo.2014.03.031 PG 13 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA AH7ZP UT WOS:000336354200005 ER PT J AU McLaughlin, BM Bizau, JM Cubaynes, D Al Shorman, MM Guilbaud, S Sakho, I Blancard, C Gharaibeh, MF AF McLaughlin, B. M. Bizau, J. M. Cubaynes, D. Al Shorman, M. M. Guilbaud, S. Sakho, I. Blancard, C. Gharaibeh, M. F. TI K-shell photoionization of B-like oxygen (O3+) ions: experiment and theory SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article DE photoionization; K-shell; oxygen ions; experiment; theory ID BORON ISOELECTRONIC SEQUENCE; X-RAY-ABSORPTION; R-MATRIX THEORY; AUTOIONIZATION RATES; ATOMIC OXYGEN; CROSS-SECTIONS; CONFIGURATION-INTERACTION; OSCILLATOR-STRENGTHS; 1S2P(4) STATES; AUGER-SPECTRA AB Absolute cross sections for the K-shell photoionization of boron-like (B-like) O3+ ions were measured by employing the ion-photon merged-beam technique at the SOLEIL synchrotron-radiation facility in Saint-Aubin, France. High-resolution spectroscopy with E/Delta E approximate to 5000 (approximate to 110 meV, full width half maximum) was achieved with photon energy from 540 up to 600 eV. Several theoretical approaches, including R-matrix, multi-configuration Dirac-Fock and screening constant by unit nuclear charge were used to identify and characterize the strong 1s -> 2p and the weaker 1s -> 3p resonances observed in the K-shell spectra of this ion. The trend of the integrated oscillator strength and autoionization width (natural line width) of the strong 1s -> 2p resonances along the first few ions of the B-like sequence is discussed. C1 [McLaughlin, B. M.] Queens Univ Belfast, Sch Math & Phys, Ctr Theoret Atom Mol & Opt Phys, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Bizau, J. M.; Cubaynes, D.; Al Shorman, M. M.; Guilbaud, S.] Univ Paris 11, CNRS UMR 8214, Inst Sci Mol Orsay, F-91405 Orsay, France. [Bizau, J. M.; Cubaynes, D.] Synchrotron SOLEIL LOrme Merisiers, F-91192 Gif Sur Yvette, France. [Sakho, I.] Univ Assane Seck Ziguinchor, UFR Sci & Technol, Dept Phys, Ziguinchor, Senegal. [Blancard, C.] CEA DAM DIF, F-91297 Arpajon, France. [Gharaibeh, M. F.] Jordan Univ Sci & Technol, Dept Phys, Irbid 22110, Jordan. RP McLaughlin, BM (reprint author), Queens Univ Belfast, Sch Math & Phys, Ctr Theoret Atom Mol & Opt Phys, David Bates Bldg,7 Coll Pk, Belfast BT7 1NN, Antrim, North Ireland. EM b.mclaughlin@qub.ac.uk; jean-marc.bizau@u-psud.fr FU Scientific Research Support Fund, Jordan [Bas/2/02/2010]; US National Science Foundation; Queen's University Belfast; National Science Foundation [OCI-1053575]; Oak Ridge Leadership Computing Facility at the Oak Ridge National Laboratory - Office of Science of the US Department of Energy [DE-AC05-00OR22725] FX The experimental measurements were performed on the PLEIADES beam line, at the SOLEIL Synchrotron radiation facility in Saint-Aubin, France. The authors would like to thank the SOLEIL staff and, in particular C Miron the local contact of the PLEIADES beam line during the experiment for their helpful assistance. MFG acknowledges funding from the Scientific Research Support Fund, Jordan, for supporting a research visit to SOLEIL, under contract number Bas/2/02/2010. BMM acknowledges support from the US National Science Foundation through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics, the RTRA network Triangle de la Physique and a visiting research fellowship from Queen's University Belfast. We thank John C Raymond and Randall K Smith at the Harvard-Smithsonian Center for Astrophysics for discussions on the astrophysical applications. The computational work was carried out at the National Energy Research Scientific Computing Center in Oakland, CA, USA, the Kraken XT5 facility at the National Institute for Computational Science (NICS) in Knoxville, TN, USA and at the High Performance Computing Center Stuttgart (HLRS) of the University of Stuttgart, Stuttgart, Germany. Stefan Andersson from Cray Research is acknowledged for his advice and assistance with the implementation of the parallel R-matrix codes on the Cray-XE6 at HLRS. The Kraken XT5 facility is a resource of the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number OCI-1053575. 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. NR 73 TC 8 Z9 8 U1 0 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD JUN 14 PY 2014 VL 47 IS 11 AR 115201 DI 10.1088/0953-4075/47/11/115201 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AI1NZ UT WOS:000336619100008 ER PT J AU Tiansawat, P Davis, AS Berhow, MA Zalamea, PC Dalling, JW AF Tiansawat, Pimonrat Davis, Adam S. Berhow, Mark A. Zalamea, Paul-Camilo Dalling, James W. TI Investment in Seed Physical Defence Is Associated with Species' Light Requirement for Regeneration and Seed Persistence: Evidence from Macaranga Species in Borneo SO PLOS ONE LA English DT Article ID TROPICAL RAIN-FOREST; CHEMICAL DEFENSE; MECHANICAL DEFENSE; SOIL; DISPERSAL; PREDATION; PLANTS; TREE; RESISTANCE; HERBIVORY AB The seed stage is often critical in determining the regeneration success of plants. Seeds must survive an array of seed predators and pathogens and germinate under conditions favourable for seedling establishment. To maximise recruitment success plants protect seeds using a diverse set of chemical and physical defences. However, the relationship between these defence classes, and their association with other life history traits, is not well understood. Data on seed coat thickness and fracture resistance, and the abundance and diversity of potential defensive compounds were collected for 10 tree species of Macaranga from Borneo. The data were used to test whether there is a trade-off in physical versus chemical defence investment, and to determine how investment varies with seed mass, and light requirement for regeneration. Across species there was no correlation between seed coat thickness and abundance of potential defensive compounds, indicating the absence of a direct trade-off between defence classes. While chemical defences were not correlated to other traits, physical defences were positively correlated with light requirement for regeneration. For a subset of five Macaranga species we evaluated the relative investment in chemical and physical defence to seed persistence in the soil, measured as the time to half initial seed viability (seed half-life). Half-life was negatively related to the ratio of potential defensive compound abundance to seed coat thickness, suggesting that species with long persistence invested in physical defence more than stored chemical defences. These results indicate that investment in seed defences are associated with species' light requirements for regeneration, rather than scaling positively with seed mass. Furthermore, chemical defences, although highly variable among species, do not appear to be critical to long term persistence of Macaranga seeds, and may be important in defending seeds from natural enemies distinct from those found in the soil. C1 [Tiansawat, Pimonrat; Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Davis, Adam S.] ARS, Global Change & Photosynthesis Res Unit, United Dept Agr, Urbana, IL USA. [Berhow, Mark A.] ARS, Natl Ctr Agr Utilizat Res, United Dept Agr, Peoria, IL USA. [Zalamea, Paul-Camilo; Dalling, James W.] Smithsonian Trop Res Inst, Ancon, Panama. RP Tiansawat, P (reprint author), Chiang Mai Univ, Dept Biol, Chiang Mai 50000, Thailand. EM tiansawat@yahoo.co.th OI Tiansawat, Pimonrat/0000-0003-1354-1247 FU Center of Tropical Forest Science; Royal Thai Government; National Science Foundation [1120205] FX The funding for this work was provided by the Center of Tropical Forest Science (2010 Research Grant) to PT, the Royal Thai Government to PT and The National Science Foundation Grant 1120205 to JWD and ASD. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 64 TC 4 Z9 4 U1 2 U2 22 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUN 13 PY 2014 VL 9 IS 6 AR e99691 DI 10.1371/journal.pone.0099691 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AK2VQ UT WOS:000338278100067 PM 24927025 ER PT J AU Sterrenburg, FAS De Haan, M Herwig, WE Hargraves, PE AF Sterrenburg, Frithjof A. S. De Haan, Myriam Herwig, Wulf E. Hargraves, Paul E. TI Typification and taxonomy of Gyrosigma tenuissimum (W. Sm.) JW Griffith & Henfr., comparison with Gyrosigma coelophilum N. Okamoto & Nagumo and description of two new taxa: Gyrosigma tenuissimum var. gundulae var. nov and Gyrosigma baculum sp nov (Pleurosigmataceae, Bacillariophyta) SO PHYTOTAXA LA English DT Article DE Gyrosigma tenuissimum; Gyrosigma coelophilum; Gyrosigma tenuissimum var. gundulae; Gyrosigma baculum; typification ID GENERA GYROSIGMA AB Gyrosigma tenuissimum (W.Sm.) J.W. Griffith & Henfr. was examined in the original material and an emended description is presented. Its protologue contains an error of taxonomic significance: in the type material, the valve and raphe sternum do not show the considerable flexure described and illustrated in Smith (1853). A comparison with Gyrosigma coelophilum N. Okamoto & Nagumo revealed that the latter, although similar in several characters, differs sufficiently in others to warrant separate specific status. Descriptions of two new taxa are given: Gyrosigma tenuissimum var. gundulae var. nov. and Gyrosigma baculum sp. nov. Both show very fine longitudinal striae at or beyond the limit of ordinary light microscopy and are practically non-sigmoid. C1 [De Haan, Myriam] Bot Garden, Dept Bryophytes Thallophytes, BE-1860 Meise, Belgium. [Hargraves, Paul E.] Florida Atlantic Univ, Harbor Branch Oceanog Inst, Ft Pierce, FL USA. [Hargraves, Paul E.] Smithsonian Inst Marine Stn, Ft Pierce, FL USA. RP Sterrenburg, FAS (reprint author), Stn Weg 158, Heiloo, Netherlands. EM fass@wxs.nl; myriam.dehaan@br.fgov.be; WEHerwig@arcor.de; Dr.Pharg@gmail.com FU Florida Fish and Wildlife Conservation Commission via the Fish and Wildlife Research Institute (FWC ) [06135]; State of Florida's Save Our Seas specialty license plate program FX David Williams, NHM London and reviewers are thanked for helpful suggestions. Manfred Ruppel, Goethe Universitat, Frankfurt am Main, Germany, kindly made SEM photomicrographs of G. tenuissimum in our own samples. Wulf Herwig thanks Rosa Trobajo for the sample from Alfacs Bay. Personal discussion with Noriko Okamoto led to a consensus regarding the taxonomic status of Gyrosigma coelophilum vs. Gyrosigma tenuissimum. Paul Hargraves acknowledges the following assistance: The Florida field work was done by Kristen S. Davis and Patrick Monaghan. Julie Piraino provided excellent assistance with SEM photomicrographs of G. tenuissimum var. gundulae. Financial support was provided by Florida Fish and Wildlife Conservation Commission via the Fish and Wildlife Research Institute (FWC Agreement No., 06135), and the State of Florida's Save Our Seas specialty license plate program. This paper is contribution 1922 of Harbor Branch Oceanographic Institute at Florida Atlantic University, and contribution 952 of the Smithsonian Marine Station, Fort Pierce. NR 22 TC 2 Z9 2 U1 2 U2 3 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 13 PY 2014 VL 172 IS 2 BP 71 EP 80 PG 10 WC Plant Sciences SC Plant Sciences GA AJ2OR UT WOS:000337497800002 ER PT J AU Gonzalez, DAC Ibanez, A AF Gonzalez, Daniel Adolfo Caceres Ibanez, Alicia TI Pitcairnia albifolia (Bromeliaceae), a new species from the Talamanca Mountains in Veraguas Province, Panama SO PHYTOTAXA LA English DT Article C1 [Gonzalez, Daniel Adolfo Caceres] Univ Autonoma Chiriqui, UCH Herbarium, Chiriqui, Panama. [Gonzalez, Daniel Adolfo Caceres] Herbarium Senckenbergianum, Frankfurt, Germany. [Ibanez, Alicia] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Gonzalez, DAC (reprint author), Univ Autonoma Chiriqui, UCH Herbarium, Chiriqui, Panama. EM consultoria.caceres@gmail.com; ibaneza@si.edu FU US National Institutes of Health through the International Cooperative Biodiversity Groups (ICBG) program FX The authors wish to thank the curators of the herbaria B, CR, FR, INB, MO, NY, PMA, SCZ, SEL, UCH, USJ, and WU for allowing access to their collections; the Autoridad Nacional del Ambiente (ANAM) for facilitating this research through issuing the collecting permit (SE/P-19-09); the Smithsonian Tropical Research Institute (STRI) for supporting all logistical aspects of this work; and the US National Institutes of Health for funding the fieldwork through the International Cooperative Biodiversity Groups (ICBG) program. NR 12 TC 0 Z9 0 U1 0 U2 1 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 11 PY 2014 VL 172 IS 1 BP 46 EP 50 PG 5 WC Plant Sciences SC Plant Sciences GA AJ2OQ UT WOS:000337497600006 ER PT J AU Connolly, SR MacNeil, MA Caley, J Knowlton, N Cripps, E Hisano, M Thibaut, LM Bhattacharya, BD Benedetti-Cecchi, L Brainard, RE Brandt, A Bulleri, F Ellingsen, KE Kaiser, S Kroncke, I Linse, K Maggi, E O'Hara, TD Plaisance, L Poore, GCB Sarkar, SK Satpathy, KK Schuckel, U Williams, A Wilson, RS AF Connolly, Sean R. MacNeil, M. Aaron Caley, Julian Knowlton, Nancy Cripps, Ed Hisano, Mizue Thibaut, Loic M. Bhattacharya, Bhaskar D. Benedetti-Cecchi, Lisandro Brainard, Russell E. Brandt, Angelika Bulleri, Fabio Ellingsen, Kari E. Kaiser, Stefanie Kroencke, Ingrid Linse, Katrin Maggi, Elena O'Hara, Timothy D. Plaisance, Laetitia Poore, Gary C. B. Sarkar, Santosh K. Satpathy, Kamala K. Schueckel, Ulrike Williams, Alan Wilson, Robin S. TI Commonness and rarity in the marine biosphere SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE metacommunities; marine macroecology; species coexistence; Poisson-lognormal distribution ID SPECIES-ABUNDANCE DISTRIBUTIONS; NEUTRAL THEORY; COMMUNITY STRUCTURE; GLOBAL CORRELATIONS; REJECT NEUTRALITY; MULTIPLE SCALES; CORAL-REEFS; DIVERSITY; MODELS; BIODIVERSITY AB Explaining patterns of commonness and rarity is fundamental for understanding and managing biodiversity. Consequently, a key test of biodiversity theory has been how well ecological models reproduce empirical distributions of species abundances. However, ecological models with very different assumptions can predict similar species abundance distributions, whereas models with similar assumptions may generate very different predictions. This complicates inferring processes driving community structure from model fits to data. Here, we use an approximation that captures common features of "neutral" biodiversity models-which assume ecological equivalence of species-to test whether neutrality is consistent with patterns of commonness and rarity in the marine biosphere. We do this by analyzing 1,185 species abundance distributions from 14 marine ecosystems ranging from intertidal habitats to abyssal depths, and from the tropics to polar regions. Neutrality performs substantially worse than a classical nonneutral alternative: empirical data consistently show greater heterogeneity of species abundances than expected under neutrality. Poor performance of neutral theory is driven by its consistent inability to capture the dominance of the communities' most-abundant species. Previous tests showing poor performance of a neutral model for a particular system often have been followed by controversy about whether an alternative formulation of neutral theory could explain the data after all. However, our approach focuses on common features of neutral models, revealing discrepancies with a broad range of empirical abundance distributions. These findings highlight the need for biodiversity theory in which ecological differences among species, such as niche differences and demographic trade-offs, play a central role. C1 [Connolly, Sean R.; Hisano, Mizue; Thibaut, Loic M.] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. [Connolly, Sean R.; Hisano, Mizue; Thibaut, Loic M.] James Cook Univ, Australian Res Council Ctr Excellence Coral Reef, Townsville, Qld 4811, Australia. [MacNeil, M. Aaron; Caley, Julian] Australian Inst Marine Sci, Townsville, Qld 4810, Australia. [Knowlton, Nancy; Plaisance, Laetitia] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Cripps, Ed] Univ Western Australia, Sch Math & Stat, Perth, WA 6009, Australia. [Bhattacharya, Bhaskar D.; Sarkar, Santosh K.] Univ Calcutta, Dept Marine Sci, Kolkata 700019, W Bengal, India. [Benedetti-Cecchi, Lisandro; Bulleri, Fabio; Maggi, Elena] Univ Pisa, Dipartimento Biol, I-56126 Pisa, Italy. [Brainard, Russell E.] NOAA, Coral Reef Ecosyst Div, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA. [Brandt, Angelika] Univ Hamburg, Bioctr Grindel, D-20146 Hamburg, Germany. [Brandt, Angelika] Univ Hamburg, Zool Museum, D-20146 Hamburg, Germany. [Ellingsen, Kari E.] Norwegian Inst Nat Res, FRAM High North Res Ctr Climate & Environm, N-9296 Tromso, Norway. [Kaiser, Stefanie] German Ctr Marine Biodivers Res, D-26382 Wilhelmshaven, Germany. [Kroencke, Ingrid; Schueckel, Ulrike] Marine Res Dept, D-26382 Wilhelmshaven, Germany. [Linse, Katrin] British Antarctic Survey, Cambridge CB3 0ET, England. [O'Hara, Timothy D.; Poore, Gary C. B.; Wilson, Robin S.] Museum Victoria, Melbourne, Vic 3001, Australia. [Satpathy, Kamala K.] Indira Gandhi Ctr Atom Res, Environm & Safety Div, Kalpakkam 603102, Tamil Nadu, India. [Williams, Alan] Commonwealth Sci & Ind Res Org, Marine & Atmospher Res, Marine Labs, Hobart, Tas 7001, Australia. RP Connolly, SR (reprint author), James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. EM Sean.connolly@jcu.edu.au; knowlton@si.edu RI Williams, Alan/C-6999-2012; MacNeil, M. Aaron/E-8196-2017; OI MacNeil, M. Aaron/0000-0001-8406-325X; Connolly, Sean/0000-0003-1537-0859 FU Ministry for Science and Technology; German Research Foundation (Deutsche Forschungsgemeinschaft); Australian Research Council FX U.S. acknowledges S. Ehrich and A. Sell for providing ship time. The authors thank all participants in the Census of Marine Life project, particularly S. Campana, M. Sogin, K. Stocks, and L. A. Zettler. They also thank R. Etienne for providing advice for obtaining numerical solutions of the fission speciation neutral model, and J. Rosindell and S. Cornell for sharing simulated neutral community data from their spatially explicit neutral model. The authors thank T. Hughes for comments on an early version of the manuscript. K. E. E. acknowledges The Norwegian Oil and Gas Association for permitting use of data. A. B. acknowledges the support of the Ministry for Science and Technology and the German Research Foundation (Deutsche Forschungsgemeinschaft) for support of the Antarctic benthic deep-sea biodiversity (ANDEEP) and ANDEEP-System Coupling (SYSTCO) expeditions, as well as five PhD positions. A. B. also thanks the Alfred-Wegener-Institute for Polar and Marine Research for logistic help, as well as the crew of the vessel and all pickers, sorters and identifiers of the extensive deep-sea material. The Census of Marine Life funded the assembly of the metadataset. Analysis of the data was made possible by funding from the Australian Research Council (to S.R.C.). NR 42 TC 29 Z9 29 U1 5 U2 86 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JUN 10 PY 2014 VL 111 IS 23 BP 8524 EP 8529 DI 10.1073/pnas.1406664111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AI6IJ UT WOS:000336976000060 PM 24912168 ER PT J AU Aliu, E Aune, T Behera, B Beilicke, M Benbow, W Berger, K Bird, R Bouvier, A Buckley, JH Bugaev, V Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Dumm, J Dwarkadas, VV Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fleischhack, H Fortin, P Fortson, L Furniss, A Galante, N Gillanders, GH Gotthelf, EV Griffin, S Griffiths, ST Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Johnson, CA Kaaret, P Kargaltsev, O Kertzman, M Khassen, Y Kieda, D Krennrich, F Lang, MJ Madhavan, AS Maier, G McArthur, S McCann, A Millis, J Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Pandel, D Park, N Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Rajotte, J Reyes, LC Reynolds, PT Richards, GT Roache, E Roberts, M Sembroski, GH Shahinyan, K Smith, AW Staszak, D Telezhinsky, I Tucci, JV Tyler, J Vincent, S Wakely, SP Weinstein, A Welsing, R Wilhelm, A Williams, DA Zitzer, B AF Aliu, E. Aune, T. Behera, B. Beilicke, M. Benbow, W. Berger, K. Bird, R. Bouvier, A. Buckley, J. H. Bugaev, V. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Dumm, J. Dwarkadas, V. V. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fleischhack, H. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Gotthelf, E. V. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Johnson, C. A. Kaaret, P. Kargaltsev, O. Kertzman, M. Khassen, Y. Kieda, D. Krennrich, F. Lang, M. J. Madhavan, A. S. Maier, G. McArthur, S. McCann, A. Millis, J. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Pandel, D. Park, N. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Rajotte, J. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Roberts, M. Sembroski, G. H. Shahinyan, K. Smith, A. W. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Vincent, S. Wakely, S. P. Weinstein, A. Welsing, R. Wilhelm, A. Williams, D. A. Zitzer, B. TI SPATIALLY RESOLVING THE VERY HIGH ENERGY EMISSION FROM MGRO J2019+37 WITH VERITAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : stars; pulsars : individual (PSR J2021+3651); supernovae : individual (CTB 87) ID GAMMA-RAY EMISSION; PULSAR WIND NEBULA; GALACTIC PLANE; PSR J2021+3651; CYGNUS REGION; DISCOVERY; MILAGRO; STARS; HESS; ASSOCIATIONS AB We present very high energy (VHE) imaging of MGRO J2019+37 obtained with the VERITAS observatory. The bright extended (similar to 2 degrees) unidentified Milagro source is located toward the rich star formation region Cygnus-X. MGRO J2019+37 is resolved into two VERITAS sources. The faint, point-like source VER J2016+371 overlaps CTB 87, a filled-center remnant (SNR) with no evidence of a supernova remnant shell at the present time. Its spectrum is well fit in the 0.65-10 TeV energy range by a power-law model with photon index 2.3 +/- 0.4. VER J2019+378 is a bright extended (similar to 1 degrees) source that likely accounts for the bulk of the Milagro emission and is notably coincident with PSR J2021+3651 and the star formation region Sh 2-104. Its spectrum in the range 1-30 TeV is well fit with a power-law model of photon index 1.75 +/- 0.3, among the hardest values measured in the VHE band, comparable to that observed near Vela-X. We explore the unusual spectrum and morphology in the radio and X-ray bands to constrain possible emission mechanisms for this source. C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Aune, T.; Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Behera, B.; Chen, X.; Federici, S.; Fleischhack, H.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Beilicke, M.; Buckley, J. H.; Bugaev, V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Bouvier, A.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Chen, X.; Federici, S.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Univ Coll Galway, Sch Phys, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Dwarkadas, V. V.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Humensky, T. B.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kargaltsev, O.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Krennrich, F.; Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Millis, J.; Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Pandel, D.] Grand Valley State Univ, Dept Phys, Allendale, MI 49401 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Roberts, M.] Eureka Sci Inc, Oakland, CA 94602 USA. [Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. RP Aliu, E (reprint author), Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. EM ealiu@astro.columbia.edu; nahee@uchicago.edu RI Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755; Cui, Wei/0000-0002-6324-5772; Roberts, Mallory/0000-0002-9396-9720; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U. K; ESA Member States and NASA; Natural Sciences and Engineering Research Council FX The authors would like to thank Jules Halpern for many useful discussions and help in obtaining and interpreting the Swift data. This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by STFC in the U. K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has made use of data 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 research presented in this paper has used data from the Canadian Galactic Plane Survey, a Canadian project with international partners, supported by the Natural Sciences and Engineering Research Council. NR 56 TC 13 Z9 14 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2014 VL 788 IS 1 AR 78 DI 10.1088/0004-637X/788/1/78 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200078 ER PT J AU Bartschat, K Sadeghpour, HR AF Bartschat, Klaus Sadeghpour, H. R. TI HYPERFINE-CHANGING TRANSITIONS IN He-3 II AND OTHER ONE-ELECTRON IONS BY ELECTRON SCATTERING SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; atomic processes; dark ages, reionization, first stars; early universe; radio lines : general ID HYDROGEN; COLLISIONS AB We consider the spin-exchange (SE) cross-section in electron scattering from He-3 II, which drives the hyperfine-changing 3.46 cm (8.665 GHz) line transition. Both the analytical quantum defect method-applicable at very low energies-and accurate R-matrix techniques for electron-He+ scattering are employed to obtain SE cross-sections. The quantum defect theory is also applied to electron collisions with other one-electron ions in order to demonstrate the utility of the method and derive scaling relations. At very low energies, the hyperfine-changing cross-sections due to e-He+ scattering are much larger in magnitude than for electron collisions with neutral hydrogen, hinting at large rate constants for equilibration. Specifically, we obtain rate coefficients of K(10K) = 1.10 x 10(-6) cm(3) s(-1) and K(100 K) = 3.49 x 10(-7) cm(3) s(-1). C1 [Bartschat, Klaus] Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. [Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Bartschat, K (reprint author), Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. EM klaus.bartschat@drake.edu; hrs@cfa.harvard.edu FU United States National Science Foundation [PHY-1068140]; Harvard University; Harvard-Smithsonian Center for Astrophysics FX This work was supported by the United States National Science Foundation under grant No. PHY-1068140 (K. B.) and through a grant to the Institute for Theoretical Atomic,Molecular, and Optical Physics at Harvard University and the Harvard-Smithsonian Center for Astrophysics. NR 19 TC 1 Z9 1 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2014 VL 788 IS 1 AR 69 DI 10.1088/0004-637X/788/1/69 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200069 ER PT J AU Bechter, EB Crepp, JR Ngo, H Knutson, HA Batygin, K Hinkley, S Muirhead, PS Johnson, JA Howard, AW Montet, BT Matthews, CT Morton, TD AF Bechter, Eric B. Crepp, Justin R. Ngo, Henry Knutson, Heather A. Batygin, Konstantin Hinkley, Sasha Muirhead, Philip S. Johnson, John Asher Howard, Andrew W. Montet, Benjamin T. Matthews, Christopher T. Morton, Timothy D. TI WASP-12b AND HAT-P-8b ARE MEMBERS OF TRIPLE STAR SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; stars: individual (WASP-12, HAT-P-8); techniques: high angular resolution; techniques: photometric ID EXOPLANET HOST STARS; ROSSITER-MCLAUGHLIN OBSERVATIONS; TRANSITING EXTRASOLAR PLANET; SPIN-ORBIT ALIGNMENT; LOW-MASS STELLAR; HOT JUPITERS; GIANT PLANETS; ADAPTIVE OPTICS; C/O RATIO; M DWARFS AB We present high spatial resolution images that demonstrate that WASP-12b and HAT-P-8b orbit the primary stars of hierarchical triple star systems. In each case, two distant companions with colors and brightnesses consistent with Mdwarfs co-orbit the hot Jupiter planet host as well as one another. Our adaptive optics images spatially resolve the secondary around WASP-12, previously identified by Bergfors et al. and Crossfield et al. into two distinct sources separated by 84.3 +/- 0.6 mas (21 +/- 3 AU). We find that the secondary to HAT-P-8, also identified by Bergfors et al., is in fact composed of two stars separated by 65.3 +/- 0.5 mas (15 +/- 1 AU). Our follow-up observations demonstrate physical association through common proper motion. HAT-P-8 C has a particularly low mass, which we estimate to be 0.18 +/- 0.02 M-circle dot using photometry. Due to their hierarchy, WASP-12 BC and HAT-P-8 BC will enable the first dynamical mass determination for hot Jupiter stellar companions. These previously well studied planet hosts now represent higher-order multi-star systems with potentially complex dynamics, underscoring the importance of diffraction-limited imaging and providing additional context for understanding the migrant population of transiting hot Jupiters. C1 [Bechter, Eric B.; Crepp, Justin R.; Matthews, Christopher T.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Ngo, Henry; Knutson, Heather A.; Batygin, Konstantin; Johnson, John Asher] CALTECH, Dept Planetary Sci, Pasadena, CA 91125 USA. [Hinkley, Sasha; Muirhead, Philip S.; Montet, Benjamin T.; Morton, Timothy D.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Muirhead, Philip S.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Bechter, EB (reprint author), Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. EM ebechter@nd.edu RI Howard, Andrew/D-4148-2015; Muirhead, Philip/H-2273-2014; OI Howard, Andrew/0000-0001-8638-0320; Muirhead, Philip/0000-0002-0638-8822; Montet, Benjamin/0000-0001-7516-8308; Ngo, Henry/0000-0001-5172-4859 FU W.M. Keck Foundation; David and Lucile Packard Foundation; Alfred P. Sloan Foundation; National Science Foundation [DGE1144469] FX This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. 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. J.A.J. is supported by generous grants from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation. B. T. M. is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE1144469. NR 56 TC 16 Z9 16 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2014 VL 788 IS 1 AR 2 DI 10.1088/0004-637X/788/1/2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200002 ER PT J AU Beiersdorfer, P Trabert, E Lepson, JK Brickhouse, NS Golub, L AF Beiersdorfer, Peter Traebert, Elmar Lepson, Jaan K. Brickhouse, Nancy S. Golub, Leon TI HIGH-RESOLUTION LABORATORY MEASUREMENTS OF CORONAL LINES IN THE 198-218 angstrom REGION SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; line&COLFAML identification; stars&COLFAML coronae; Sun&COLFAML corona; X-rays&COLFAML stars ID BEAM ION-TRAP; SOFT-X-RAY; EXTREME-ULTRAVIOLET REGION; AN ATOMIC DATABASE; ELECTRON-BEAM; EMISSION-LINES; CHARGED IONS; FE-XIII; WAVELENGTH MEASUREMENTS; ACTIVE-REGION AB We present high-resolution laboratory measurements of the emission from various ions of C, N, O, F, Ne, S, Ar, Fe, and Ni in the extreme ultraviolet wavelength band centered around the lambda 211 Fe XIV channel of the Atmospheric Imaging Assembly on the Solar Dynamics Observatory. While all of the strong iron lines in this region are well known, we note many weaker lines of iron that are not yet identified. The high resolution of our measurements also allows us to resolve several lines in Fe XI, Fe XII, and Fe XIII between 200 and 205 angstrom, whose identities were in question based on a disagreement between different databases. The spectra of the elements other than iron are much less known, and we find a multitude of lines that are not yet in the databases. For example, the CHIANTI database clearly disagrees with the NIST data listings on several of the argon lines we observe and also it contains only about half of the observed sulfur lines. C1 [Beiersdorfer, Peter; Traebert, Elmar] Lawrence Livermore Natl Lab, Div Phys, Livermore, CA 94550 USA. [Traebert, Elmar] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany. [Lepson, Jaan K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brickhouse, Nancy S.; Golub, Leon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Beiersdorfer, P (reprint author), Lawrence Livermore Natl Lab, Div Phys, Livermore, CA 94550 USA. FU Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; Solar and Heliospherical Physics Program of the National Aeronautics and Space Administration [NNH10AN31I]; German Research Association (DFG) [Tr171/18, Tr171/19] FX This work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344 and was supported by the Solar and Heliospherical Physics Program of the National Aeronautics and Space Administration under award NNH10AN31I. E.T. acknowledges support from the German Research Association (DFG; grants Tr171/18 and Tr171/19). NR 57 TC 11 Z9 12 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2014 VL 788 IS 1 AR 25 DI 10.1088/0004-637X/788/1/25 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200025 ER PT J AU Beky, B Holman, MJ Kipping, DM Noyes, RW AF Beky, Bence Holman, Matthew J. Kipping, David M. Noyes, Robert W. TI STELLAR ROTATION-PLANETARY ORBIT PERIOD COMMENSURABILITY IN THE HAT-P-11 SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: activity; stars: individual (HAT-P-11, Kepler-17); stars: rotation ID SUPER-NEPTUNE HAT-P-11B; COROT SPACE MISSION; TRANSITING EXOPLANETS; MAGNETIC ACTIVITY; HOT JUPITERS; TAU-BOOTIS; STAR; STARSPOTS; KEPLER; FIELD AB A number of planet host stars have been observed to rotate with a period equal to an integer multiple of the orbital period of their close planet. We expand this list by analyzing Kepler data of HAT-P-11 and finding a period ratio of 6:1. In particular, we present evidence for a long-lived spot on the stellar surface that is eclipsed by the planet in the same position four times, every sixth transit. We also identify minima in the out-of-transit light curve and confirm that their phase with respect to the stellar rotation is mostly stationary for the 48 month time frame of the observations, confirming the proposed rotation period. For comparison, we apply our methods to Kepler-17 and confirm the findings of Bonomo & Lanza that the period ratio is not exactly 8:1 in that system. Finally, we provide a hypothesis on how interactions between a star and its planet could possibly result in an observed commensurability for systems where the stellar differential rotation profile happens to include a period at some latitude that is commensurable to the planetary orbit. C1 [Beky, Bence; Holman, Matthew J.; Kipping, David M.; Noyes, Robert W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Beky, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bbeky@cfa.harvard.edu FU NASA [NNX09AB28G]; Origins program [NNX09AB33G, NNX13A124G]; NASA Carl Sagan Fellowships; FAS Science Division Research Computing Group at Harvard University FX Work by B.B. and M.J.H. was supported by NASA under grant NNX09AB28G from the Kepler Participating Scientist Program and grants NNX09AB33G and NNX13A124G under the Origins program. D.M.K. is funded by the NASA Carl Sagan Fellowships. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. The MCMC computations in this paper were run on the Odyssey 2.0 cluster supported by the FAS Science Division Research Computing Group at Harvard University. B.B. is grateful for discussions with John A. Johnson, Ruth Murray-Clay, Claire Moutou, and Joshua N. Winn. NR 45 TC 12 Z9 12 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 10 PY 2014 VL 788 IS 1 AR 1 DI 10.1088/0004-637X/788/1/1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200001 ER PT J AU Carr, JS Najita, JR AF Carr, John S. Najita, Joan R. TI THE OH ROTATIONAL POPULATION AND PHOTODISSOCIATION OF H2O IN DG Tauri SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; infrared : stars; circumstellar matter; protoplanetary disks; stars : pre-main sequence ID MOLECULAR SPECTROSCOPIC DATABASE; FAR-ULTRAVIOLET CONTINUUM; YOUNG CIRCUMSTELLAR DISKS; 4TH POSITIVE EMISSION; PROTOPLANETARY DISKS; ORGANIC-MOLECULES; DISSOCIATION DYNAMICS; LINEAR-MOLECULES; PROMPT EMISSION; LAMBDA-DOUBLETS AB We analyze the OH rotational emission in the Spitzer Space Telescope mid- infrared spectrum of the T Tauri star DG Tau. OH is observed in emission from upper level energies of 1900 K to 28,000 K. The rotational diagram cannot be fit with any single combination of temperature and column density and has slopes that correspond to excitation temperatures ranging from 200 K to 6000 K. The relative A-doublet population within each rotational level is not equal, showing that the OH population is not in thermal equilibrium. The symmetric A-doublet state is preferred in all rotational states, with an average of 0.5 for the population ratio of the anti-symmetric to symmetric state. We show that the population distribution of the high rotational lines and the A-doublet ratio are consistent with the formation of OH following the photo- dissociation of H2O by FUV photons in the second absorption band of water (similar to 1150-1400 angstrom), which includes Ly alpha. Other processes, OH formation from either photo-dissociation of water in the first absorption band (1450-1900 angstrom) or the reaction O(D-1) + H-2, or collisional excitation, cannot explain the observed emission in the high rotational states but could potentially contribute to the population of lower rotational levels. These results demonstrate that the photo-dissociation of water is active in DG Tau and support the idea that the hot rotational OH emission commonly observed in Classical T Tauri stars is due to the dissociation of H2O by FUV radiation. C1 [Carr, John S.] Naval Res Lab, Washington, DC 20375 USA. [Najita, Joan R.] Natl Opt Astron Observ, Tucson, AZ 85716 USA. [Najita, Joan R.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Carr, JS (reprint author), Naval Res Lab, Code 7211, Washington, DC 20375 USA. FU NASA; Naval Research Laboratory; Institute for Theory and Computation at the Harvard-Smithsonian Center for Astrophysics 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. Basic research in infrared astrophysics at the Naval Research Laboratory is supported by 6.1 base funding. J.N. gratefully acknowledges support from the Institute for Theory and Computation at the Harvard-Smithsonian Center for Astrophysics. NR 72 TC 1 Z9 1 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2014 VL 788 IS 1 AR 66 DI 10.1088/0004-637X/788/1/66 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200066 ER PT J AU Dittmann, JA Soderberg, AM Chomiuk, L Margutti, R Goss, WM Milisavljevic, D Chevalier, RA AF Dittmann, J. A. Soderberg, A. M. Chomiuk, L. Margutti, R. Goss, W. M. Milisavljevic, D. Chevalier, R. A. TI A MID-LIFE CRISIS? SUDDEN CHANGES IN RADIO AND X-RAY EMISSION FROM SUPERNOVA 1970G SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: evolution; stars: low-mass; supernovae: individual (1970G) ID LUMINOUS BLUE VARIABLES; MASS-LOSS; IBC SUPERNOVA; SN 1970G; EVOLUTION; PROGENITORS; M101; MODULATIONS; RECOVERY; REMNANTS AB Supernovae (SNe) provide a backdrop from which we can probe the end state of stellar evolution in the final years before the progenitor star explodes. As the shock from the SN expands, the timespan of mass-loss history we are able to probe also extends, providing insight to rapid timescale processes that govern the end state of massive stars. While SNe transition into remnants on timescales of decades to centuries, observations of this phase are currently limited. Here, we present observations of SN 1970G, serendipitously observed during the monitoring campaign of SN 2011fe, which shares the same host galaxy. Utilizing the new Jansky Very Large Array (VLA) upgrade and a deep X-ray exposure taken by Chandra, we are able to recover this middle-aged SN and distinctly resolve it from the H II cloud with which it is associated. We find that the flux density of SN 1970G has changed significantly since it was last observed-the X-ray luminosity has increased by a factor of similar to 3, while we observe a significantly lower radio flux of only 27.5 mu Jy at 6.75 GHz, a level only detectable through the upgrades now in operation at the Jansky VLA. These changes suggest that SN 1970G has entered a new stage of evolution toward an SN remnant, and we may be detecting the turn-on of the pulsar wind nebula. Deep radio observations of additional middle-aged SNe with the improved radio facilities will provide a statistical census of the delicate transition period between SN and remnant. C1 [Dittmann, J. A.; Soderberg, A. M.; Margutti, R.; Milisavljevic, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chomiuk, L.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Goss, W. M.] Natl Radio Astron Observ, Domenici Sci Operat Ctr, Socorro, NM 87801 USA. [Chevalier, R. A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Dittmann, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jdittmann@cfa.harvard.edu OI Dittmann, Jason/0000-0001-7730-2240 NR 43 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 10 PY 2014 VL 788 IS 1 AR 38 DI 10.1088/0004-637X/788/1/38 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200038 ER PT J AU Kelly, BC Becker, AC Sobolewska, M Siemiginowska, A Uttley, P AF Kelly, Brandon C. Becker, Andrew C. Sobolewska, Malgosia Siemiginowska, Aneta Uttley, Phil TI FLEXIBLE AND SCALABLE METHODS FOR QUANTIFYING STOCHASTIC VARIABILITY IN THE ERA OF MASSIVE TIME-DOMAIN ASTRONOMICAL DATA SETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : statistical ID ACTIVE GALACTIC NUCLEI; MULTIVARIATE CARMA PROCESSES; REVERBERATION MAPPING DATA; DAMPED RANDOM-WALK; X-RAY VARIABILITY; OPTICAL VARIABILITY; QUASAR VARIABILITY; LIGHT CURVES; BLACK-HOLE; AUTOREGRESSIVE MODELS AB We present the use of continuous-time autoregressive moving average (CARMA) models as a method for estimating the variability features of a light curve, and in particular its power spectral density (PSD). CARMA models fully account for irregular sampling and measurement errors, making them valuable for quantifying variability, forecasting and interpolating light curves, and variability-based classification. We show that the PSD of a CARMA model can be expressed as a sum of Lorentzian functions, which makes them extremely flexible and able to model a broad range of PSDs. We present the likelihood function for light curves sampled from CARMA processes, placing them on a statistically rigorous foundation, and we present a Bayesian method to infer the probability distribution of the PSD given the measured light curve. Because calculation of the likelihood function scales linearly with the number of data points, CARMA modeling scales to current and future massive time-domain data sets. We conclude by applying our CARMA modeling approach to light curves for an X-ray binary, two active galactic nuclei, a long-period variable star, and an RR Lyrae star in order to illustrate their use, applicability, and interpretation. C1 [Kelly, Brandon C.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Becker, Andrew C.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Sobolewska, Malgosia] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Siemiginowska, Aneta] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Uttley, Phil] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. RP Kelly, BC (reprint author), Univ Calif Santa Barbara, Dept Phys, Broida Hall, Santa Barbara, CA 93106 USA. NR 65 TC 24 Z9 24 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2014 VL 788 IS 1 AR 33 DI 10.1088/0004-637X/788/1/33 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200033 ER PT J AU Lopez, LA Castro, D Slane, PO Ramirez-Ruiz, E Badenes, C AF Lopez, Laura A. Castro, Daniel Slane, Patrick O. Ramirez-Ruiz, Enrico Badenes, Carles TI IDENTIFICATION OF A JET-DRIVEN SUPERNOVA REMNANT IN THE SMALL MAGELLANIC CLOUD: POSSIBLE EVIDENCE FOR THE ENHANCEMENT OF BIPOLAR EXPLOSIONS AT LOW METALLICITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: supernova remnants; Magellanic Clouds; X-rays: ISM ID GAMMA-RAY BURSTS; CORE-COLLAPSE SUPERNOVAE; STAR-FORMATION HISTORY; IA SUPERNOVA; IBC SUPERNOVA; H I; PROGENITORS; EMISSION; BINARIES; W49B AB Recent evidence has suggested that the supernova remnant (SNR) 0104-72.3 in the Small Magellanic Cloud (SMC) may be the result of a "prompt" Type Ia SN on the basis of enhanced iron abundances and its association with a star-forming region. In this paper, we present evidence that SNR 0104-72.3 arose from a jet-driven bipolar core-collapse (CC) SN. Specifically, we use serendipitous Chandra data of SNR 0104-72.3 taken because of its proximity to the calibration source SNR E0102-72.3. We analyze 56 Advanced CCD Imaging Spectrometer (ACIS) observations of SNR 0104-72.3 to produce imaging and spectra with an effective exposure of 528.6 ks. We demonstrate that SNR 0104-72.3 is highly elliptical relative to other nearby young SNRs, suggesting a CC SN origin. Furthermore, we compare ejecta abundances derived from spectral fits to nucleosynthetic yields of Type Ia and CC SNe, and we find that the iron, neon, and silicon abundances are consistent with either a spherical CC SN of a 18-20 M-circle dot progenitor or an aspherical CC SN of a 25 M-circle dot progenitor. We show that the star formation history at the site of SNR 0104-72.3 is also consistent with a CC origin. Given the bipolar morphology of the SNR, we favor the aspherical CC SN scenario. This result may suggest jet-driven SNe occur frequently in the low-metallicity environment of the SMC, consistent with the observational and theoretical work on broad-line Type Ic SNe and long-duration gamma-ray bursts. C1 [Lopez, Laura A.; Castro, Daniel] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ramirez-Ruiz, Enrico] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95060 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. RP Lopez, LA (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave,37-664H, Cambridge, MA 02139 USA. EM lopez@space.mit.edu OI Badenes, Carles/0000-0003-3494-343X FU NASA through the Einstein Fellowship Program [PF1-120085]; MIT Pappalardo Fellowship in Physics; David and Lucile Packard Foundation; NSF [AST-0847563]; NASA through the Smithsonian Astrophysical Observatory [SV3-73016]; NASA [NAS8-03060] FX We acknowledge helpful discussions with J.-J. Lee in writing this paper. Support for L.A.L. was provided by NASA through the Einstein Fellowship Program, grant PF1-120085, and the MIT Pappalardo Fellowship in Physics. E.R.R. acknowledges support from the David and Lucile Packard Foundation and NSF grant AST-0847563. D.C. and P.O.S. acknowledge support for this work provided by NASA through the Smithsonian Astrophysical Observatory contract SV3-73016 to MIT for support of the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. NR 61 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 JUN 10 PY 2014 VL 788 IS 1 AR 5 DI 10.1088/0004-637X/788/1/5 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200005 ER PT J AU Miller, JM Raymond, J Kallman, TR Maitra, D Fabian, AC Proga, D Reynolds, CS Reynolds, MT Degenaar, N King, AL Cackett, EM Kennea, JA Beardmore, A AF Miller, J. M. Raymond, J. Kallman, T. R. Maitra, D. Fabian, A. C. Proga, D. Reynolds, C. S. Reynolds, M. T. Degenaar, N. King, A. L. Cackett, E. M. Kennea, J. A. Beardmore, A. TI CHANDRA SPECTROSCOPY OF MAXI J1305-704: DETECTION OF AN INFALLING BLACK HOLE DISK WIND? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics ID X-RAY BINARIES; LY-ALPHA LINE; ACCRETION DISK; INTERSTELLAR-MEDIUM; GRO J1655-40; ABSORPTION; RADIATION; DRIVEN; JETS; SUPPRESSION AB We report on a high-resolution Chandra/HETG X-ray spectrum of the transient X-ray binary MAXI J1305-704. A rich absorption complex is detected in the Fe L band, including density-sensitive lines from Fe XX, Fe XXI, and Fe XXII. Spectral analysis over three wavelength bands with a large grid of XSTAR photoionization models generally requires a gas density of n >= 10(17) cm(-3). Assuming a luminosity of L = 10(37) erg s(-1), fits to the 10-14 angstrom band constrain the absorbing gas to lie within r = (3.9 +/- 0.7) x 10(3) km from the central engine, or about r = 520 +/- 90 (M/5M(circle dot)) r(g), where r(g) = GM/c(2). At this small distance from the compact object, gas in stable orbits should have a gravitational redshift of z = v/c similar or equal to (3 +/- 1) x 10(-3) (M/5M(circle dot)), and any tenuous inflowing gas should have a free-fall velocity of v/c similar or equal to (6 +/- 1) x 10(-2) (M/5M(circle dot))(1/2). The best-fit single-zone photoionization models measure a redshift of v/c = (2.6-3.2) x 10(-3.) Models with two absorbing zones provide significantly improved fits, and the additional zone is measured to have a redshift of v/c = (4.6-4.9) x 10(-2) (models including two zones suggest slightly different radii and may point to lower densities). Thus, the observed shifts are broadly consistent with those expected at the photoionization radius. The absorption spectrum revealed in MAXI J1305-704 may be best explained in terms of a "failed wind" like those predicted in some recent numerical simulations of black hole accretion flows. The robustness of the velocity shifts was explored through detailed simulations with the Chandra/MARX ray-tracing package and analysis of the zeroth-order ACIS-S3 spectrum. These tests are particularly important given the anomalously large angle between the source and the optical axis in this observation. The simulations and ACIS spectrum suggest that the shifts are not instrumental; however, strong caution is warranted. We discuss our results in the context of accretion flows in stellar-mass black holes and active galactic nuclei, as well as the potential role of failed winds in emerging connections between disk outflows and black hole state transitions. C1 [Miller, J. M.; Maitra, D.; Reynolds, M. T.; Degenaar, N.; King, A. L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Raymond, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greedbelt, MD 20771 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Proga, D.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Cackett, E. M.] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48201 USA. [Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Beardmore, A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM jonmm@umich.edu FU Chandra Guest Observer Program; Swift; NASA through Hubble Postdoctoral Fellowship grant from the Space Telescope Science Institute [HST-HF-51287.01-A]; Swift at the University of Leicester; UK Space Agency FX We gratefully acknowledge comments from the anonymous referee that improved the clarity and content of this paper. We thank Harvey Tananbaum and Chandra for executing this observation. We are indebted to Mateusz Ruszkowski for lending computing cluster clock cycles to this project. We acknowledge Mike Nowak, David Huenemoerder, John Davis, John Houck, Norbert Schulz, and Jonathan McDowell for helpful discussions. J.M.M. gratefully acknowledges support from the Chandra Guest Observer Program and Swift. N.D. is supported by NASA through Hubble Postdoctoral Fellowship grant number HST-HF-51287.01-A from the Space Telescope Science Institute. A.P.B. acknowledges funding for Swift at the University of Leicester by the UK Space Agency. NR 57 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 JUN 10 PY 2014 VL 788 IS 1 AR 53 DI 10.1088/0004-637X/788/1/53 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200053 ER PT J AU Oberg, KI Lauck, T Graninger, D AF Oeberg, Karin I. Lauck, Trish Graninger, Dawn TI COMPLEX ORGANIC MOLECULES DURING LOW-MASS STAR FORMATION: PILOT SURVEY RESULTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; astrochemistry; circumstellar matter; ISM : molecules; molecular processes; stars : formation; stars : protostars ID SPITZER SPECTROSCOPIC SURVEY; YOUNG STELLAR OBJECTS; HOT-CORE; PROTOSTAR IRAS-16293-2422; CHEMISTRY; ICES; GRAIN; GAS; ENVELOPE; SPECTRA AB Complex organic molecules (COMs) are known to be abundant toward some low-mass young stellar objects (YSOs), but how these detections relate to typical COM abundance are not yet understood. We aim to constrain the frequency distribution of COMs during low-mass star formation, beginning with this pilot survey of COM lines toward six embedded YSOs using the IRAM 30m Telescope. The sample was selected from the Spitzer c2d ice sample and covers a range of ice abundances. We detect multiple COMs, including CH3CN, toward two of the YSOs, and tentatively toward a third. Abundances with respect to CH3OH vary between 0.7% and 10%. This sample is combined with previous COM observations and upper limits to obtain a frequency distributions of CH3CN, HCOOCH3, CH3OCH3, and CH3CHO. We find that for all molecules more than 50% of the sample have detections or upper limits of 1%-10% with respect to CH3OH. Moderate abundances of COMs thus appear common during the early stages of low-mass star formation. A larger sample is required, however, to quantify the COM distributions, as well as to constrain the origins of observed variations across the sample. C1 [Oeberg, Karin I.; Graninger, Dawn] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lauck, Trish] Univ Virginia, Charlottesville, VA 22904 USA. RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM koberg@cfa.harvard.edu NR 37 TC 8 Z9 8 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 10 PY 2014 VL 788 IS 1 AR 68 DI 10.1088/0004-637X/788/1/68 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200068 ER PT J AU Walton, DJ Risaliti, G Harrison, FA Fabian, AC Miller, JM Arevalo, P Ballantyne, DR Boggs, SE Brenneman, LW Christensen, FE Craig, WW Elvis, M Fuerst, F Gandhi, P Grefenstette, BW Hailey, CJ Kara, E Luo, B Madsen, KK Marinucci, A Matt, G Parker, ML Reynolds, CS Rivers, E Ross, RR Stern, D Zhang, WW AF Walton, D. J. Risaliti, G. Harrison, F. A. Fabian, A. C. Miller, J. M. Arevalo, P. Ballantyne, D. R. Boggs, S. E. Brenneman, L. W. Christensen, F. E. Craig, W. W. Elvis, M. Fuerst, F. Gandhi, P. Grefenstette, B. W. Hailey, C. J. Kara, E. Luo, B. Madsen, K. K. Marinucci, A. Matt, G. Parker, M. L. Reynolds, C. S. Rivers, E. Ross, R. R. Stern, D. Zhang, W. W. TI NuSTAR AND XMM-NEWTON OBSERVATIONS OF NGC 1365: EXTREME ABSORPTION VARIABILITY AND A CONSTANT INNER ACCRETION DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies : active; X-rays : individual (NGC 1365) ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; X-RAY REVERBERATION; GALAXY SWIFT J2127.4+5654; PHOTON IMAGING CAMERA; SPECTRAL VARIABILITY; IRON-K; SEYFERT-GALAXIES; BEPPOSAX OBSERVATIONS; COMPTON REFLECTION AB We present a spectral analysis of four coordinated NuSTAR+ XMM-Newton observations of the Seyfert galaxy NGC 1365. These exhibit an extreme level of spectral variability, which is primarily due to variable line-of-sight absorption, revealing relatively unobscured states in this source for the first time. Despite the diverse range of absorption states, each of the observations displays the same characteristic signatures of relativistic reflection from the inner accretion disk. Through time-resolved spectroscopy, we find that the strength of the relativistic iron line and the Compton reflection hump relative to the intrinsic continuum are well correlated, which is expected if they are two aspects of the same broadband reflection spectrum. We apply self-consistent disk reflection models to these time-resolved spectra in order to constrain the inner disk parameters, allowing for variable, partially covering absorption to account for the vastly different absorption states that were observed. Each of the four observations is treated independently to test the consistency of the results obtained for the black hole spin and the disk inclination, which should not vary on observable timescales. We find both the spin and the inclination determined from the reflection spectrum to be consistent, confirming that NGC 1365 hosts a rapidly rotating black hole; in all cases the dimensionless spin parameter is constrained to be a* > 0.97 (at 90% statistical confidence or better). C1 [Walton, D. J.; Harrison, F. A.; Fuerst, F.; Grefenstette, B. W.; Madsen, K. K.; Rivers, E.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Risaliti, G.] INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, G.; Brenneman, L. W.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabian, A. C.; Elvis, M.; Parker, M. L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Arevalo, P.] Pontificia Univ Catolica Chile, Inst Astrfis, Santiago 22, Chile. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Luo, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Marinucci, A.; Matt, G.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Reynolds, C. S.] Univ Maryland, Joint Space Sci Inst JSI, College Pk, MD 20742 USA. [Ross, R. R.] Coll Holy Cross, Dept Phys, Worcester, MA 01610 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Walton, DJ (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Risaliti, Guido/0000-0002-3556-977X FU NASA [NNG08FD60C]; XMM-Newton; ESA Member States; Conicyt [ACT 1101]; STFC [ST/J00369711] FX The authors would like to thank the referee for providing useful feedback, which helped improve the manuscript. This research has made use of data obtained with the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA, and XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. We thank both the XMM-Newton and the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these coordinated observations. This research was supported under NASA grant No. NNG08FD60C and has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA). P.A. acknowledges financial support from Conicyt ACT 1101, and P.G. acknowledges support from STFC (grant reference ST/J00369711). NR 102 TC 32 Z9 32 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2014 VL 788 IS 1 AR 76 DI 10.1088/0004-637X/788/1/76 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200076 ER PT J AU Usman, SM Murray, SS Hickox, RC Brodwin, M AF Usman, S. M. Murray, S. S. Hickox, R. C. Brodwin, M. TI OBSCURATION BY GAS AND DUST IN LUMINOUS QUASARS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: nuclei; infrared: galaxies; quasars: general; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; DEEP FIELD-SOUTH; ULTRALUMINOUS INFRARED GALAXIES; IRAC SHALLOW SURVEY; APPROXIMATE-TO 2; X-RAY; TYPE-2 QUASARS; II QUASARS; RADIO GALAXIES AB We explore the connection between absorption by neutral gas and extinction by dust in mid-infrared (IR) selected luminous quasars. We use a sample of 33 quasars at redshifts 0.7 < z less than or similar to 3 in the 9 deg(2) Bootes multiwavelength survey field that are selected using Spitzer Space Telescope Infrared Array Camera colors and are well-detected as luminous X-ray sources (with > 150 counts) in Chandra observations. We divide the quasars into dust-obscured and unobscured samples based on their optical to mid-IR color, and measure the neutral hydrogen column density N-H through fitting of the X-ray spectra. We find that all subsets of quasars have consistent power law photon indices G approximate to 1.9 that are uncorrelated with N-H. We classify the quasars as gas-absorbed or gas-unabsorbed if NH > 1022 cm(-2) or N-H < 1022 cm-2, respectively. Of 24 dust-unobscured quasars in the sample, only one shows clear evidence for significant intrinsic N-H, while 22 have column densities consistent with N-H < 1022 cm(-2). In contrast, of the nine dust-obscured quasars, six show evidence for intrinsic gas absorption, and three are consistent with N-H < 1022 cm(-2). We conclude that dust extinction in IR-selected quasars is strongly correlatedwith significant gas absorption as determined through X-ray spectral fitting. These results suggest that obscuring gas and dust in quasars are generally co-spatial, and confirm the reliability of simple mid-IR and optical photometric techniques for separating quasars based on obscuration. C1 [Usman, S. M.; Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. RP Usman, SM (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. EM Shawn.Usman@jhu.edu FU NASA through ADAP award [NNX12AE38G]; National Science Foundation [1211096]; NASA [NAS8-03060] FX This work was supported by NASA through ADAP award NNX12AE38G and by the National Science Foundation through grant number 1211096. 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. This work is based on observations with the Chandra X-Ray Telescope, which is operated by SAO under a contract with NASA NAS8-03060. NR 41 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 10 PY 2014 VL 788 IS 1 AR L3 DI 10.1088/2041-8205/788/1/L3 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI8CV UT WOS:000337134100013 ER PT J AU Yang, Q Wang, YJ Labandeira, CC Shih, CK Ren, D AF Yang, Qiang Wang, Yongjie Labandeira, Conrad C. Shih, Chungkun Ren, Dong TI Mesozoic lacewings from China provide phylogenetic insight into evolution of the Kalligrammatidae (Neuroptera) SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Jiulongshan formation; Yixian formation; Mouthparts; Wing eyespots; Phylogenetic analysis; Classification ID INNER-MONGOLIA; INSECTA; FAMILY; DAOHUGOU; GENERA; RECORD AB Background: The Kalligrammatidae are distinctive, large, conspicuous, lacewings found in Eurasia from the Middle Jurassic to mid Early Cretaceous. Because of incomplete and often inadequate fossil preservation, an absence of detailed morphology, unclear relationships, and unknown evolutionary trends, the Kalligrammatidae are poorly understood. Results: We describe three new subfamilies, four new genera, twelve new species and four unassigned species from the late Middle Jurassic Jiulongshan and mid Early Cretaceous Yixian Formations of China. These kalligrammatid taxa exhibit diverse morphological characters, such as mandibulate mouthparts in one major clade and siphonate mouthparts in the remaining four major clades, the presence or absence of a variety of distinctive wing markings such as stripes, wing spots and eyespots, as well as multiple major wing shapes. Based on phylogenetic analyses, the Kalligrammatidae are divided into five principal clades: Kalligrammatinae Handlirsch, 1906, Kallihemerobiinae Ren & Engel, 2008, Meioneurinae subfam. nov., Oregrammatinae subfam. nov. and Sophogrammatinae subfam. nov., each of which is accorded subfamily-level status. Our results show significant morphological and evolutionary differentiation of the Kalligrammatidae family during a 40 million-year-interval of the mid Mesozoic. Conclusion: A new phylogeny and classification of five subfamilies and their constituent genera is proposed for the Kalligrammatidae. These diverse, yet highly specialized taxa from northeastern China suggest that eastern Eurasia likely was an important diversification center for the Kalligrammatidae. Kalligrammatids possess an extraordinary morphological breadth and panoply of adaptations during the mid-Mesozoic that highlight our conclusion that their evolutionary biology is much more complex than heretofore realized. C1 [Yang, Qiang; Wang, Yongjie; Labandeira, Conrad C.; Shih, Chungkun; Ren, Dong] Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Yang, Qiang] Shijiazhuang Univ Econ, Geosci Museum, Shijiazhuang 050031, Peoples R China. RP Wang, YJ (reprint author), Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. EM wangyjosmy@gmail.com; rendong@mail.cnu.edu.cn FU National Basic Research Program of China (973 Program) [2012CB821906)]; National Natural Science Foundation of China [31230065, 31272352, 31301905, 41372013, 41272006]; Great Wall Scholar and KEY project of Beijing Municipal Commission of Education [KZ201310028033]; Program for Changjiang Scholars and Innovative Research Team in University [IRT13081]; China Postdoctoral Science Foundation [2012T50113]; Ph.D. Programs Foundation of Ministry of Education of China [20131108120005]; Beijing Municipal Natural Science Foundation [5132008]; Doctoral Scientific Research Foundation of Shijiazhuang University of Economics [BQ201326] FX We sincerely thank Prof. Michael S. Engel (Kansas University, Kansas, USA), the editor, and two anonymous reviewers for their helpful comments and suggestions. We also express our thanks to Ms. Wenying Wu for the preparation of a previous version of photo for the specimen (CNU-NEU-NN2009-033). This research is supported by the National Basic Research Program of China (973 Program) (grant 2012CB821906), the National Natural Science Foundation of China (grants 31230065, 31272352, 31301905, 41372013 and 41272006), Great Wall Scholar and KEY project of Beijing Municipal Commission of Education (grant KZ201310028033), Program for Changjiang Scholars and Innovative Research Team in University (IRT13081), China Postdoctoral Science Foundation (grant 2012T50113), Ph.D. Programs Foundation of Ministry of Education of China (grant 20131108120005), the Beijing Municipal Natural Science Foundation (grant 5132008), and the Doctoral Scientific Research Foundation of Shijiazhuang University of Economics (BQ201326). Finnegan Marsh assisted in the placement and formatting of the figures. This is contribution 258 from the Evolution of Terrestrial Ecosystems Consortium of the National Museum of Natural History, in Washington, D. C. NR 44 TC 13 Z9 13 U1 0 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 JUN 9 PY 2014 VL 14 AR 126 DI 10.1186/1471-2148-14-126 PG 30 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA AM0DE UT WOS:000339512700001 PM 24912379 ER PT J AU Thomas, DB Nascimbene, PC Dove, CJ Grimaldi, DA James, HF AF Thomas, Daniel B. Nascimbene, Paul C. Dove, Carla J. Grimaldi, David A. James, Helen F. TI Seeking carotenoid pigments in amber-preserved fossil feathers SO SCIENTIFIC REPORTS LA English DT Article ID RAMAN; PLUMAGE; DOMINICAN AB Plumage colours bestowed by carotenoid pigments can be important for visual communication and likely have a long evolutionary history within Aves. Discovering plumage carotenoids in fossil feathers could provide insight into the ecology of ancient birds and non-avian dinosaurs. With reference to a modern feather, we sought chemical evidence of carotenoids in six feathers preserved in amber (Miocene to mid-Cretaceous) and in a feather preserved as a compression fossil (Eocene). Evidence of melanin pigmentation and microstructure preservation was evaluated with scanning electron and light microscopies. We observed fine microstructural details including evidence for melanin pigmentation in the amber and compression fossils, but Raman spectral bands did not confirm the presence of carotenoids in them. Carotenoids may have been originally absent from these feathers or the pigments may have degraded during burial; the preservation of microstructure may suggest the former. Significantly, we show that carotenoid plumage pigments can be detected without sample destruction through an amber matrix using confocal Raman spectroscopy. C1 [Thomas, Daniel B.; Dove, Carla J.; James, Helen F.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Nascimbene, Paul C.; Grimaldi, David A.] Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA. RP Thomas, DB (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. EM d.b.thomas@massey.ac.nz FU Peter Buck Postdoctoral Fellowship FX We thank James Zigras and Jim Kane for loaning amber specimens to AMNH, Matthew Carrano (NMNH) for helpful comments, Scott Whittaker (NMNH) for SEM training, Finnegan Marsh and Mark Florence (NMNH) for access to fossil feathers. DBT was funded by a Peter Buck Postdoctoral Fellowship, administered by NMNH. NR 19 TC 10 Z9 10 U1 2 U2 33 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 JUN 9 PY 2014 VL 4 AR 5226 DI 10.1038/srep05226 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AI5JB UT WOS:000336900900001 PM 24909554 ER PT J AU Britz, R Ruber, L Johnson, GD AF Britz, R. Rueber, L. Johnson, G. D. TI Reinventing the disc: a reminder to give credit to past giants SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article C1 [Britz, R.] Nat Hist Museum, Dept Life Sci, London SW7 5BD, England. [Rueber, L.] Nat Hist Museum Burgergemeinde Bern, CH-3005 Bern, Switzerland. [Johnson, G. D.] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. RP Britz, R (reprint author), Nat Hist Museum, Dept Life Sci, Cromwell Rd, London SW7 5BD, England. EM r.britz@nhm.ac.uk OI Ruber, Lukas/0000-0003-0125-008X NR 6 TC 1 Z9 1 U1 1 U2 6 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 JUN 7 PY 2014 VL 281 IS 1784 AR 20132920 DI 10.1098/rspb.2013.2920 PG 3 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AG4IJ UT WOS:000335382700004 PM 24759853 ER PT J AU Saarinen, JJ Boyer, AG Brown, JH Costa, DP Ernest, SKM Evans, AR Fortelius, M Gittleman, JL Hamilton, MJ Harding, LE Lintulaakso, K Lyons, SK Okie, JG Sibly, RM Stephens, PR Theodor, J Uhen, MD Smith, FA AF Saarinen, Juha J. Boyer, Alison G. Brown, James H. Costa, Daniel P. Ernest, S. K. Morgan Evans, Alistair R. Fortelius, Mikael Gittleman, John L. Hamilton, Marcus J. Harding, Larisa E. Lintulaakso, Kari Lyons, S. Kathleen Okie, Jordan G. Sibly, Richard M. Stephens, Patrick R. Theodor, Jessica Uhen, Mark D. Smith, Felisa A. TI Patterns of maximum body size evolution in Cenozoic land mammals: eco-evolutionary processes and abiotic forcing SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE body size; maximum size frequency; mammals; Cenozoic; evolution; macroecology ID COPES RULE; FOSSIL MAMMALS; TRENDS AB There is accumulating evidence that macroevolutionary patterns of mammal evolution during the Cenozoic follow similar trajectories on different continents. This would suggest that such patterns are strongly determined by global abiotic factors, such as climate, or by basic eco-evolutionary processes such as filling of niches by specialization. The similarity of pattern would be expected to extend to the history of individual clades. Here, we investigate the temporal distribution of maximum size observed within individual orders globally and on separate continents. While the maximum size of individual orders of large land mammals show differences and comprise several families, the times at which orders reach their maximum size over time show strong congruence, peaking in the Middle Eocene, the Oligocene and the Plio-Pleistocene. The Eocene peak occurs when global temperature and land mammal diversity are high and is best explained as a result of niche expansion rather than abiotic forcing. Since the Eocene, there is a significant correlation between maximum size frequency and global temperature proxy. The Oligocene peak is not statistically significant and may in part be due to sampling issues. The peak in the Plio-Pleistocene occurs when global temperature and land mammal diversity are low, it is statistically the most robust one and it is best explained by global cooling. We conclude that the macroevolutionary patterns observed are a result of the interplay between eco-evolutionary processes and abiotic forcing. C1 [Saarinen, Juha J.; Fortelius, Mikael; Lintulaakso, Kari] Univ Helsinki, Dept Geosci & Geog, Helsinki, Finland. [Boyer, Alison G.] Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN USA. [Brown, James H.; Hamilton, Marcus J.; Harding, Larisa E.; Okie, Jordan G.; Smith, Felisa A.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Hamilton, Marcus J.] Univ New Mexico, Dept Anthropol, Albuquerque, NM 87131 USA. [Costa, Daniel P.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Ernest, S. K. Morgan] Utah State Univ, Dept Biol, Logan, UT 84322 USA. [Ernest, S. K. Morgan] Utah State Univ, Ctr Ecol, Logan, UT 84322 USA. [Evans, Alistair R.] Monash Univ, Sch Biol Sci, Clayton, Vic 3800, Australia. [Gittleman, John L.; Stephens, Patrick R.] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Hamilton, Marcus J.] Santa Fe Inst, Santa Fe, NM 87501 USA. [Lyons, S. Kathleen] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Okie, Jordan G.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Sibly, Richard M.] Univ Reading, Sch Biol Sci, Reading, Berks, England. [Theodor, Jessica] Univ Calgary, Dept Biol Sci, Calgary, AB T2N 1N4, Canada. [Uhen, Mark D.] George Mason Univ, Dept Atmospher Ocean & Earth Sci, Fairfax, VA 22030 USA. RP Saarinen, JJ (reprint author), Univ Helsinki, Dept Geosci & Geog, Helsinki, Finland. EM juha.saarinen@helsinki.fi RI Evans, Alistair/D-4239-2011; Ernest, SK Morgan/O-2532-2015; OI Evans, Alistair/0000-0002-4078-4693; Ernest, SK Morgan/0000-0002-6026-8530; Sibly, Richard/0000-0001-6828-3543 FU National Science Foundation Grant Integrating Macroecological Pattern and Processes across Scales, Research Coordination Network [DEB 0541625]; Finnish Graduate School of Geology FX This study was supported by National Science Foundation Grant Integrating Macroecological Pattern and Processes across Scales, Research Coordination Network DEB 0541625 (to F. A. S., S. K. L. and S. K. M. E., principal investigators). The work of J.S. was funded by the Finnish Graduate School of Geology. NR 28 TC 3 Z9 3 U1 3 U2 31 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD JUN 7 PY 2014 VL 281 IS 1784 AR 20132049 DI 10.1098/rspb.2013.2049 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AG4IJ UT WOS:000335382700001 PM 24741007 ER PT J AU Chang, D Duda, TF AF Chang, Dan Duda, Thomas F., Jr. TI Application of community phylogenetic approaches to understand gene expression: differential exploration of venom gene space in predatory marine gastropods SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID DUPLICATE GENES; RAPID EVOLUTION; CIS-ELEMENTS; CONUS; DIVERGENCE; PATTERNS; SNAILS; DIVERSIFICATION; TRANSCRIPTOME; FAMILIES AB Background: Predatory marine gastropods of the genus Conus exhibit substantial variation in venom composition both within and among species. Apart from mechanisms associated with extensive turnover of gene families and rapid evolution of genes that encode venom components ('conotoxins'), the evolution of distinct conotoxin expression patterns is an additional source of variation that may drive interspecific differences in the utilization of species' 'venom gene space'. To determine the evolution of expression patterns of venom genes of Conus species, we evaluated the expression of A-superfamily conotoxin genes of a set of closely related Conus species by comparing recovered transcripts of A-superfamily genes that were previously identified from the genomes of these species. We modified community phylogenetics approaches to incorporate phylogenetic history and disparity of genes and their expression profiles to determine patterns of venom gene space utilization. Results: Less than half of the A-superfamily gene repertoire of these species is expressed, and only a few orthologous genes are coexpressed among species. Species exhibit substantially distinct expression strategies, with some expressing sets of closely related loci ('under-dispersed' expression of available genes) while others express sets of more disparate genes ('over-dispersed' expression). In addition, expressed genes show higher d(N)/d(S) values than either unexpressed or ancestral genes; this implies that expression exposes genes to selection and facilitates rapid evolution of these genes. Few recent lineage-specific gene duplicates are expressed simultaneously, suggesting that expression divergence among redundant gene copies may be established shortly after gene duplication. Conclusions: Our study demonstrates that venom gene space is explored differentially by Conus species, a process that effectively permits the independent and rapid evolution of venoms in these species. C1 [Chang, Dan; Duda, Thomas F., Jr.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Chang, Dan; Duda, Thomas F., Jr.] Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA. [Chang, Dan] Univ Michigan, Dept Stat, Ann Arbor, MI 48109 USA. [Duda, Thomas F., Jr.] Smithsonian Trop Res Inst, Balboa, Panama. RP Chang, D (reprint author), 1156 High Str Mail Stop EEBiol, Santa Cruz, CA 95064 USA. EM changdan@umich.edu FU EEB Block Grants from Rackham Graduate School of University of Michigan; NSF [IOS-0718379] FX We thank J-P Bingham from the University of Hawaii for providing venom duct samples of C. quercinus. We acknowledge colleagues at the University of Michigan, including Jianzhi Zhang, Taehwan Lee, Earl Werner, Lori Isom and Wenfeng Qian, and Gang Chen at the University of Rhode Island, as well as the editor and two anonymous reviewers for their valuable comments on our manuscript. This study is supported by EEB Block Grants from Rackham Graduate School of University of Michigan awarded to DC and an NSF research grant (IOS-0718379) awarded to TFD. NR 54 TC 3 Z9 3 U1 0 U2 8 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD JUN 5 PY 2014 VL 14 AR 123 DI 10.1186/1471-2148-14-123 PG 12 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA AK3HF UT WOS:000338313400001 PM 24903151 ER PT J AU Darnell, AM Graf, JA Somers, MJ Slotow, R Gunther, MS AF Darnell, Angela M. Graf, Jan A. Somers, Michael J. Slotow, Rob Gunther, Micaela Szykman TI Space Use of African Wild Dogs in Relation to Other Large Carnivores SO PLOS ONE LA English DT Article ID HLUHLUWE-UMFOLOZI PARK; KRUGER-NATIONAL-PARK; LYCAON-PICTUS; SOUTH-AFRICA; INTERSPECIFIC COMPETITION; HUNTING BEHAVIOR; SPOTTED HYAENAS; IMFOLOZI-PARK; PANTHERA-LEO; PACK SIZE AB Interaction among species through competition is a principle process structuring ecological communities, affecting behavior, distribution, and ultimately the population dynamics of species. High competition among large African carnivores, associated with extensive diet overlap, manifests in interactions between subordinate African wild dogs (Lycaon pictus) and dominant lions (Panthera leo) and spotted hyenas (Crocuta crocuta). Using locations of large carnivores in Hluhluwe-iMfolozi Park, South Africa, we found different responses from wild dogs to their two main competitors. Wild dogs avoided lions, particularly during denning, through a combination of spatial and temporal avoidance. However, wild dogs did not exhibit spatial or temporal avoidance of spotted hyenas, likely because wild dog pack sizes were large enough to adequately defend their kills. Understanding that larger carnivores affect the movements and space use of other carnivores is important for managing current small and fragmented carnivore populations, especially as reintroductions and translocations are essential tools used for the survival of endangered species, as with African wild dogs. C1 [Darnell, Angela M.; Gunther, Micaela Szykman] Humboldt State Univ, Dept Wildlife, Arcata, CA 95521 USA. [Graf, Jan A.; Slotow, Rob] Univ KwaZulu Natal, Sch Life Sci, Durban, South Africa. [Somers, Michael J.] Univ Pretoria, Ctr Wildlife Management, Ctr Invas Biol, ZA-0002 Pretoria, South Africa. [Gunther, Micaela Szykman] Smithsonian Conservat Biol Inst, Front Royal, VA USA. RP Darnell, AM (reprint author), Humboldt State Univ, Dept Wildlife, Arcata, CA 95521 USA. EM ange.darnell@gmail.com RI Somers, Michael/A-1523-2008; OI /0000-0002-5836-8823 FU Smithsonian Institution Undersecretary for Science Endowment Funds; American Zoo and Aquarium Association Conservation Endowment Fund; Humboldt State University Sponsored Program Foundation; University of Pretoria, Green Trust; Bateleurs and Wildlife Conservation Trust; NRF, NSF; University of KwaZulu-Natal; Walt Disney Foundation and MGM; Wild about Cats; Hluhluwe Tourism Association; THRIP; Grand Hotel grants FX Funding for this project was provided by the Smithsonian Institution Undersecretary for Science Endowment Funds, the American Zoo and Aquarium Association Conservation Endowment Fund, and Humboldt State University Sponsored Program Foundation (MSG); University of Pretoria, The Green Trust (WWF-SA), and Bateleurs and Wildlife Conservation Trust (KZN) (MS); NRF, NSF, University of KwaZulu-Natal, Walt Disney Foundation and MGM, Wild about Cats, and Hluhluwe Tourism Association (RS); and THRIP (N. Ferguson) and Grand Hotel grants (C. Packer). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 78 TC 6 Z9 6 U1 11 U2 83 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUN 4 PY 2014 VL 9 IS 6 AR e98846 DI 10.1371/journal.pone.0098846 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AK4YO UT WOS:000338430700086 PM 24896638 ER PT J AU Kuntner, M Naparus, M Li, DQ Coddington, JA AF Kuntner, Matjaz Naparus, Magdalena Li, Daiqin Coddington, Jonathan A. TI Phylogeny Predicts Future Habitat Shifts Due to Climate Change SO PLOS ONE LA English DT Article ID RANGE EXPANSION; BIODIVERSITY; IMPACTS; DRIVEN; DISTRIBUTIONS; POPULATIONS; EXTINCTIONS; DIVERSITY; EVOLUTION; PATTERNS AB Background: Taxa may respond differently to climatic changes, depending on phylogenetic or ecological effects, but studies that discern among these alternatives are scarce. Here, we use two species pairs from globally distributed spider clades, each pair representing two lifestyles (generalist, specialist) to test the relative importance of phylogeny versus ecology in predicted responses to climate change. Methodology: We used a recent phylogenetic hypothesis for nephilid spiders to select four species from two genera (Nephilingis and Nephilengys) that match the above criteria, are fully allopatric but combined occupy all subtropical-tropical regions. Based on their records, we modeled each species niche spaces and predicted their ecological shifts 20, 40, 60, and 80 years into the future using customized GIS tools and projected climatic changes. Conclusions: Phylogeny better predicts the species current ecological preferences than do lifestyles. By 2080 all species face dramatic reductions in suitable habitat (54.8-77.1%) and adapt by moving towards higher altitudes and latitudes, although at different tempos. Phylogeny and life style explain simulated habitat shifts in altitude, but phylogeny is the sole best predictor of latitudinal shifts. Models incorporating phylogenetic relatedness are an important additional tool to predict accurately biotic responses to global change. C1 [Kuntner, Matjaz] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Ljubljana, Slovenia. [Kuntner, Matjaz; Li, Daiqin] Hubei Univ, Coll Life Sci, Ctr Behav Ecol & Evolut, Wuhan, Hubei, Peoples R China. [Kuntner, Matjaz; Coddington, Jonathan A.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Naparus, Magdalena] Univ Bucharest, Ctr Landscape Terr Informat Syst CeLTIS, Bucharest, Romania. [Naparus, Magdalena] Tular Cave Lab, Kranj, Slovenia. [Li, Daiqin] Natl Univ Singapore, Dept Biol Sci, Singapore 117548, Singapore. RP Kuntner, M (reprint author), Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Ljubljana, Slovenia. EM kuntner@gmail.com RI Aljancic, Magdalena/O-4801-2014; Li, Daiqin/D-6922-2013 OI Li, Daiqin/0000-0001-8269-7734 FU Raffles Museum for Biodiversity Research (RMBR); Slovenian Research Agency [P10236, BI-US/09-12-016, MU-PROM/12-001]; NSFC [31272324]; Singapore Ministry of Education (MOE) AcRF [R-154-000-476-112] FX This research was supported in part by a Raffles Museum for Biodiversity Research (RMBR) Short-term Fellowship and the grants P10236, BI-US/09-12-016 and MU-PROM/12-001 from the Slovenian Research Agency to M. K. and by the NSFC grant (31272324) and Singapore Ministry of Education (MOE) AcRF grant (R-154-000-476-112) to D. L. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 52 TC 4 Z9 4 U1 7 U2 41 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUN 3 PY 2014 VL 9 IS 6 AR e98907 DI 10.1371/journal.pone.0098907 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AI5ML UT WOS:000336911400109 PM 24892737 ER PT J AU Adamski, D Landry, JF Nazari, V AF Adamski, David Landry, Jean-Francois Nazari, Vazrick TI THREE NEW SPECIES OF LEAF-MINING GELECHIIDAE (LEPIDOPTERA) FROM CANADA AND NORTHEASTERN UNITED STATES SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY LA English DT Article DE chaetotaxy; DNA barcode; Gelechiidae; leaf-miners; taxonomy ID HOLARCTIC TELEIODINI LEPIDOPTERA AB Three new species of leaf-mining Gelechiidae are described: Xenolechia ceanothiae Priest, whose larvae feed on Ceanothus americanus L. (Rhamnaceae); Gnorimoschema shepherdiae Priest, on Shepherdia canadensis (L.) Nutt. (Elaeagnaceae); and Scrobipalpula manierreorum Priest, on Eurybia (Aster) macrophylla (L.) Cassini (Asteraceae). Their leaf mines were initially discovered in the understory in Michigan forests. Barcoding revealed additional records for two of these species from several regions of Canada. Photographs of the imagos and illustrations of the male and female genitalia, larval and pupal chaetotaxal maps are provided. Scanning electron micrographs of selected features of the larva for each species supplement illustrations. Comparative diagnoses of adult morphological characters are presented to distinguish the new species from other North American congeners. Photographs of the leaf-mines for each species are also included. DNA barcodes for each species are shown to be distinct from related North American congeners. The first occurrence of Gnorimosthema vibei Wolff in North America is confirmed by barcoded specimens from Kuujjuarapik in northern Quebec, Canada. C1 [Adamski, David] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Landry, Jean-Francois; Nazari, Vazrick] Agr & Agri Food Canada, CEF, Ottawa, ON K1A 0C6, Canada. RP Adamski, D (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012,NHB E526,MRC 168, Washington, DC 20013 USA. EM adamskid@si.edu; landryjf@agr.gc.ca; nazariv@agr.gc.ca FU Huron Mountains Wildlife Foundation; Government of Canada through Genome Canada; Ontario Genomics Institute; NSERC; Canada Foundation for Innovation; Ontario Ministry of Research and Innovation; AAFC (Science and Innovation Branch) FX RJP is most grateful to David Gosling, former, and Kerry Woods, Research Director, Huron Mountains Wildlife Foundation for support of this research; William and Anne Manierre for sharing their vast knowledge of the Huron Mountain holdings, guidance to various habitats, personal friendship, encouragement, and hospitality during his visits; and to Wayne Thorpe for his sharing of the historical knowledge of the Huron Mountain Club and his assistance with logistics.; We thank Peter Huemer, Tyroler Landesmuseen, Innsbruck, Austria, Marko Mutanen, University of Oulu, Finland, Helena Wirta, University of Helsinki, Finland, Jeremy deWaard, Alex Smith, and Paul Hebert for granting us permission to use BOLD sequences based on specimens from their collection or under their care. We thank Ole Karsholt, Zoological Museum, University of Copenhagen, for unpublished information about Gnorimoschema vibei. Paul Hebert generously agreed that BIO specimens designated as paratypes be deposited in the CNC. DNA barcoding was enabled, in part, by funding from the Government of Canada through Genome Canada, and the Ontario Genomics Institute in support of the International Barcode of Life Project. NSERC, the Canada Foundation for Innovation, the Ontario Ministry of Research and Innovation, and AAFC (Science and Innovation Branch) also provided support. NR 28 TC 1 Z9 1 U1 1 U2 3 PU LEPIDOPTERISTS SOC PI LOS ANGELES PA 900 EXPOSITION BLVD, LOS ANGELES, CA 90007-4057 USA SN 0024-0966 J9 J LEPID SOC JI J. Lepid. Soc. PD JUN 2 PY 2014 VL 68 IS 2 BP 101 EP 123 PG 23 WC Entomology SC Entomology GA AI4XZ UT WOS:000336871200004 ER PT J AU Long, KS Kuntz, KD Blair, WP Godfrey, L Plucinsky, PP Soria, R Stockdale, C Winkler, PF AF Long, Knox S. Kuntz, Kip D. Blair, William P. Godfrey, Leith Plucinsky, Paul P. Soria, Roberto Stockdale, Christopher Winkler, P. Frank TI A DEEP CHANDRA ACIS SURVEY OF M83 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: individual (M83); galaxies: ISM; ISM: supernova remnants; supernovae: individual (SN1923A); X-rays: binaries; X-rays: general; X-rays: individual (M83) ID X-RAY BINARIES; HUBBLE-SPACE-TELESCOPE; BLACK-HOLE; CENTRAL REGION; STAR-FORMATION; INTERSTELLAR-MEDIUM; SUPERNOVA-REMNANTS; SOURCE POPULATION; SPIRAL-GALAXIES; SOURCE CATALOG AB We have obtained a series of deep X-ray images of the nearby galaxy M83 using Chandra, with a total exposure of 729 ks. Combining the new data with earlier archival observations totaling 61 ks, we find 378 point sources within the D-25 contour of the galaxy. We find 80 more sources, mostly background active galactic nuclei (AGNs), outside of the D25 contour. Of the X-ray sources, 47 have been detected in a new radio survey of M83 obtained using the Australia Telescope Compact Array. Of the X-ray sources, at least 87 seem likely to be supernova remnants (SNRs), based on a combination of their properties in X-rays and at other wavelengths. We attempt to classify the point source population of M83 through a combination of spectral and temporal analysis. As part of this effort, we carry out an initial spectral analysis of the 29 brightest X-ray sources. The soft X-ray sources in the disk, many of which are SNRs, are associated with the spiral arms, while the harder X-ray sources, mostly X-ray binaries (XRBs), do not appear to be. After eliminating AGNs, foreground stars, and identified SNRs from the sample, we construct the cumulative luminosity function (CLF) of XRBs brighter than 8 x 10(35) erg s(-1). Despite M83's relatively high star formation rate, the CLF indicates that most of the XRBs in the disk are low mass XRBs. C1 [Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kuntz, Kip D.; Blair, William P.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Godfrey, Leith; Soria, Roberto] Curtin Univ Technol, Curtin Inst Radio Astron, Bentley, WA 6102, Australia. [Godfrey, Leith] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Plucinsky, Paul P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stockdale, Christopher] Marquette Univ, Dept Phys, Milwaukee, WI 53201 USA. [Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. RP Long, KS (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM long@stsci.edu; kuntz@pha.jhu.edu; wpb@pha.jhu.edu; leith.godfrey@icrar.org; plucinsky@cfa.harvard.edu; roberto.soria@icrar.org; christopher.stockdale@marquette.edu; winkler@middlebury.edu OI Long, Knox/0000-0002-4134-864X; Blair, William/0000-0003-2379-6518 FU National Aeronautics and Space Administration [GO1-12115]; NASA [NAS8-03060]; National Science Foundation [AST-0908566]; [GO1-12115C] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra grant No. GO1-12115, issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. W.P.B. and K.K. acknowledge Chandra grant No. GO1-12115C to Johns Hopkins University. P.F.W. also acknowledges financial support from the National Science Foundation through grant AST-0908566, and the hospitality of the Research School of Astronomy and Astrophysics, Australian National University, during a portion of the work presented here. NR 84 TC 8 Z9 8 U1 0 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 2014 VL 212 IS 2 AR 21 DI 10.1088/0067-0049/212/2/21 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD3PZ UT WOS:000350993000004 ER PT J AU Robison, HW McAllister, CT Breinholt, JW Crandall, KA AF Robison, Henry W. McAllister, Chris T. Breinholt, Jesse W. Crandall, Keith A. TI STATUS, DISTRIBUTION, AND GENETICS OF BLAIR'S FENCING CRAYFISH, FAXONELLA BLAIRI (DECAPODA: CAMBARIDAE) SO SOUTHWESTERN NATURALIST LA English DT Article ID OSAGE BURROWING CRAYFISH; OKLAHOMA; ARKANSAS; RECORDS; HISTORY AB During a multi-year study of the rare Blair's fencing crayfish (Faxonella blairi Hayes and Reimer), we made 87 collections in 10 counties throughout the West Gulf Coastal Plain of southwestern Arkansas. Intensive searches throughout these counties revealed the presence of 36 new populations of F. blairi in Little River, Miller, and Sevier counties. In each of these counties, F. blairi was found to be a locally abundant crayfish. New county records from museum collections were documented for Columbia and Howard counties, Arkansas, and Cass County, Texas. Additionally, we surveyed genetic variation in F. blairi and found them to be a monophyletic group with a sister relationship to Faxonella clypeata but with clear genetic distinctiveness from this sister taxon. There was modest genetic variation within Arkansas, and this genetic variation was greater than that across Arkansas, Oklahoma, and Texas for F. blairi. Faxonella blairi should be considered as currently stable due to its more widespread distribution than previously believed and general abundance throughout its range in southwestern Arkansas. C1 [Robison, Henry W.] Southern Arkansas Univ, Dept Biol, Magnolia, AR 71754 USA. [McAllister, Chris T.] Eastern Oklahoma State Coll, Div Sci & Math, Idabel, OK 74745 USA. [Breinholt, Jesse W.] Brigham Young Univ, Dept Biol, Provo, UT 84602 USA. [Crandall, Keith A.] George Washington Univ, Computat Biol Inst, Ashburn, VA 20147 USA. [Crandall, Keith A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP McAllister, CT (reprint author), Eastern Oklahoma State Coll, Div Sci & Math, Idabel, OK 74745 USA. EM cmcallister@se.edu OI Crandall, Keith/0000-0002-0836-3389 NR 19 TC 0 Z9 0 U1 0 U2 2 PU SOUTHWESTERN ASSOC NATURALISTS PI SAN MARCOS PA SOUTHWEST TEXAS STATE UNIV, DEPT BIOLOGY, 601 UNIVERSITY DR, SAN MARCOS, TX 78666 USA SN 0038-4909 EI 1943-6262 J9 SOUTHWEST NAT JI Southw. Natural. PD JUN PY 2014 VL 59 IS 2 BP 244 EP 250 DI 10.1894/F12-JHK-09.1 PG 7 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CC8YX UT WOS:000350655600012 ER PT J AU Matson, JO Ordonez-Garza, N Woodman, N Bulmer, W Eckerlin, RP Hanson, JD AF Matson, John O. Ordonez-Garza, Nicte Woodman, Neal Bulmer, Walter Eckerlin, Ralph P. Hanson, J. Delton TI SMALL MAMMALS FROM THE CHELEMHA CLOUD FOREST RESERVE, ALTA VERAPAZ, GUATEMALA SO SOUTHWESTERN NATURALIST LA English DT Article ID HIGHLANDS; SORICIDAE; SHREWS; SORICOMORPHA; POPULATIONS AB We surveyed the small mammals of remnant mixed hardwood-coniferous cloud forest at elevations ranging from 2,100-2,300 m in the Chelemha Cloud Forest Reserve, Alta Verapaz, Guatemala. Removal-trapping using a combination of live traps, snap traps, and pitfall traps for 6 days in January 2007 resulted in 175 captures of 15 species of marsupials, shrews, and rodents. This diversity of small mammals is the highest that we have recorded from a single locality of the 10 visited during eight field seasons in the highlands of Guatemala. Based on captures, the most abundant species in the community of small mammals is Peromyscus grandis (n = 50), followed by Handleyomys rhabdops (n = 27), Heteromys desmarestianus (n = 18), Reithrodontomys mexicanus (n = 17), Handleyomys saturatior (n = 16), Sorex veraepacis (n = 15), and Scotinomys teguina (n = 13). The remaining eight species were represented by one to five individuals. C1 [Matson, John O.] San Jose State Univ, Dept Biol Sci, San Jose, CA 95192 USA. [Ordonez-Garza, Nicte] Texas Tech Univ, Dept Biol Sci, Lubbock, TX 79409 USA. [Woodman, Neal] Smithsonian Inst, Natl Museum Nat Hist, US Geol Survey, Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. [Bulmer, Walter; Eckerlin, Ralph P.] No Virginia Community Coll, Div Nat Sci, Annandale, VA 22003 USA. [Hanson, J. Delton] Res & Testing Lab, Lubbock, TX 79416 USA. RP Matson, JO (reprint author), San Jose State Univ, Dept Biol Sci, San Jose, CA 95192 USA. EM johnomatson@gmail.com OI Woodman, Neal/0000-0003-2689-7373 FU Virginia Community College System Professional Development Grant; Northern Virginia Community College Educational Foundation; Department of Biological Sciences, San Jose State University, California; United States Geological Survey Patuxent Wildlife Research Center, Maryland; R. Baker of the Natural Sciences Research Laboratory at The Museum of Texas Tech University, Lubbock; NIH FX We thank the personnel of Reserva Privada Chelemha-Union para Proteger el Bosque Nuboso for allowing us to sample small mammals on their reserve. We thank F. Herrera of Consejo Nacional de Areas Protegidas, Guatemala, for providing collecting permits and other valuable assistance during the 2007 field season. We thank A. Gardner for his suggestions and comments on the manuscript. Partial funding was provided by the Virginia Community College System Professional Development Grant and Northern Virginia Community College Educational Foundation to WB and RPE, the Department of Biological Sciences, San Jose State University, California to JOM, and the United States Geological Survey Patuxent Wildlife Research Center, Maryland, to NW. Additional funds were provided to JDH by R. Baker of the Natural Sciences Research Laboratory at The Museum of Texas Tech University, Lubbock, and an NIH grant to C. Fulhorst at the University of Texas Medical Branch, Galveston. NR 25 TC 2 Z9 2 U1 0 U2 3 PU SOUTHWESTERN ASSOC NATURALISTS PI SAN MARCOS PA SOUTHWEST TEXAS STATE UNIV, DEPT BIOLOGY, 601 UNIVERSITY DR, SAN MARCOS, TX 78666 USA SN 0038-4909 EI 1943-6262 J9 SOUTHWEST NAT JI Southw. Natural. PD JUN PY 2014 VL 59 IS 2 BP 258 EP 262 DI 10.1894/F14-TAL-60.1 PG 5 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CC8YX UT WOS:000350655600014 ER PT J AU Torres, JM Curet, LA Rice-Snow, S Castor, MJ Castor, AK AF Torres, Joshua M. Curet, L. Antonio Rice-Snow, Scott Castor, Melissa J. Castor, Andrew K. TI OF FLESH AND STONE: LABOR INVESTMENT AND REGIONAL SOCIOPOLITICAL IMPLICATIONS OF PLAZA/BATEY CONSTRUCTION AT THE CEREMONIAL CENTER OF TIBES (A.D. 600-A.D. 1200), PUERTO RICO SO LATIN AMERICAN ANTIQUITY LA English DT Article ID ORGANIZATION; ARCHAEOLOGY; COMMUNITY; MONUMENTALITY; MESOAMERICA; ENERGETICS; IDEOLOGY; HAWAII; POWER; PERU AB Ceremonial architecture of late precontact (A.D. 600-1500) societies of Puerto Rico consists of stone-lined plazas and ball courts (bateys). Archaeologists use these structures to signify the onset of hierarchical "chiefly" polities and to interpret their regional organization. Problematically, little consideration is given to the costs of their physical construction and the associated organizational implications at local and regional scales. In this paper, we use data gathered through geoarchaelogical field investigations to develop labor estimates for the plaza and bateys at the site of Tibes one of the largest precolumbian ceremonial centers in Puerto Rico. The estimates provide a basis for addressing how these features were constructed at the site and are considered within the broader organizational contexts of incipient polities in the island's south-central region between A.D. 600 and A.D. 1200. C1 [Torres, Joshua M.] Natl Pk Serv, St Croix, VI 00820 USA. [Curet, L. Antonio] Smithsonian Inst, Natl Museum Amer Indian, Cultural Ctr, Suitland, MD 20746 USA. [Rice-Snow, Scott; Castor, Melissa J.; Castor, Andrew K.] Ball State Univ, Dept Geol Sci, Muncie, IN 47306 USA. RP Torres, JM (reprint author), Natl Pk Serv, 2100 Church St 100 Christiansted, St Croix, VI 00820 USA. EM joshua_torres@nps.gov; CuretA@si.edu; ricesnow@bsu.edu NR 110 TC 1 Z9 1 U1 0 U2 0 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 1045-6635 J9 LAT AM ANTIQ JI Lat. Am. Antiq. PD JUN PY 2014 VL 25 IS 2 BP 125 EP 151 PG 27 WC Archaeology SC Archaeology GA CA4QZ UT WOS:000348890900003 ER PT J AU Kanzaki, N Giblin-Davis, RM Ye, W Herre, EA Center, BJ AF Kanzaki, N. Giblin-Davis, R. M. Ye, W. Herre, E. A. Center, B. J. TI PARASITODIPLOGASTER SPECIES ASSOCIATED WITH PHARMACOSYCEA FIGS IN PANAMA SO JOURNAL OF NEMATOLOGY LA English DT Meeting Abstract C1 [Kanzaki, N.; Giblin-Davis, R. M.; Ye, W.; Center, B. J.] Univ Florida, Ft Lauderdale Res & Educ Ctr, Davie, FL 33314 USA. [Kanzaki, N.] Forestry & Forest Prod Res Inst, Forest Pathol Lab, Tsukuba, Ibaraki 3058687, Japan. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. NR 0 TC 0 Z9 0 U1 1 U2 4 PU SOC NEMATOLOGISTS PI MARCELINE PA PO BOX 311, MARCELINE, MO 64658 USA SN 0022-300X J9 J NEMATOL JI J. Nematol. PD JUN PY 2014 VL 46 IS 2 BP 184 EP 184 PG 1 WC Zoology SC Zoology GA AW5EW UT WOS:000346299700180 ER PT J AU Touwaide, A AF Touwaide, Alain TI Communities of Learned Experience: Epistolary Medicine in the Renaissance. SO RENAISSANCE QUARTERLY LA English DT Book Review C1 [Touwaide, Alain] Inst Preservat Med Tradit, Washington, DC 20560 USA. [Touwaide, Alain] Smithsonian Inst, Washington, DC 20560 USA. RP Touwaide, A (reprint author), Inst Preservat Med Tradit, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0034-4338 EI 1935-0236 J9 RENAISSANCE QUART JI Renaiss. Q. PD SUM PY 2014 VL 67 IS 2 BP 575 EP U528 DI 10.1086/677425 PG 2 WC Medieval & Renaissance Studies SC Arts & Humanities - Other Topics GA AU5CM UT WOS:000345624700021 ER PT J AU Zuckerman, MK Garofalo, EM Frohlich, B Ortner, DJ AF Zuckerman, Molly K. Garofalo, Evan M. Frohlich, Bruno Ortner, Donald J. TI Anemia or scurvy: A pilot study on differential diagnosis of porous and hyperostotic lesions using differential cranial vault thickness in subadult humans SO INTERNATIONAL JOURNAL OF PALEOPATHOLOGY LA English DT Article DE Scurvy; Anemia; Cribra orbitalia; Porotic hyperostosis; Cranial vault thickness; Fuzzy landmarks ID ARCHAEOLOGICAL SITES; BONE-GROWTH; POPULATION; DEFICIENCY; BRITAIN AB Metabolic disorders, such as scurvy, manifested in human skeletal remains provide insight into health, nutrition, and environmental quality in past populations. Porous cranial vault lesions are often used to diagnose metabolic conditions in subadult remains, but overlapping gross lesion expressions have led to over-diagnosis of anemia and under-diagnosis of scurvy. Studies by Ortner and colleagues have suggested that specific porous cranial lesions are pathognomonic of scurvy, but additional diagnostic tools are necessary. In this technical report, we offer a preliminary assessment of cranial vault thickness (CVT) at the site of porous lesions ( sensu lato porotic hyperostosis, cribra orbitalia) as a method for distinguishing between scurvy and anemia in subadult crania. Computed Tomography (CT) was used to measure CVT at various landmarks associated with porotic hyperostosis and cribra orbitalia, complemented by lesion scores, from scorbutic (N = 11), anemic (N = 3), and non-pathological (N = 28) subadult crania used as a control group. Results indicate that CVT consistently distinguishes scorbutic from non-pathological individuals, while anemic individuals overlap with both - likely a function of small sample size in this study. Despite current limitations, CVT has the potential to be an objective diagnostic tool for distinguishing scurvy and expanding reconstructions of nutritional adequacy over the life course in past populations. (C) 2014 Elsevier Inc. All rights reserved. C1 [Zuckerman, Molly K.] Mississippi State Univ, Cobb Inst Archaeol, Dept Anthropol & Middle Eastern Cultures, Mississippi State, MS 39762 USA. [Garofalo, Evan M.] Univ Maryland, Sch Med, Dept Anat & Neurobiol, Baltimore, MD 21201 USA. [Frohlich, Bruno; Ortner, Donald J.] Natl Museum Nat Hist, Smithsonian Inst, Dept Phys Anthropol, Washington, DC 20560 USA. RP Zuckerman, MK (reprint author), Mississippi State Univ, Cobb Inst Archaeol, Dept Anthropol & Middle Eastern Cultures, POB AR, Mississippi State, MS 39762 USA. EM mkz12@msstate.edu; egarofalo@stapa.umm.edu; frohlich@si.edu OI Garofalo, Evan/0000-0002-5792-2239; Zuckerman, Molly/0000-0001-8967-3321 NR 24 TC 5 Z9 5 U1 2 U2 7 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 2014 VL 5 BP 27 EP 33 DI 10.1016/j.ijpp.2014.02.001 PG 7 WC Paleontology; Pathology SC Paleontology; Pathology GA AT2PO UT WOS:000344776900004 ER PT J AU Gingerich, O AF Gingerich, Owen TI INFINITESIMAL How a Dangerous Mathematical Theory Shaped the Modern World SO AMERICAN SCHOLAR LA English DT Book Review C1 [Gingerich, Owen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU PHI BETA KAPPA SOC PI WASHINGTON PA 1785 MASSACHUSETTS AVENUE, N W FOURTH FL,, WASHINGTON, DC 20036 USA SN 0003-0937 EI 2162-2892 J9 AM SCHOLAR JI Am. Sch. PD SUM PY 2014 VL 83 IS 3 BP 109 EP 111 PG 3 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA AS3ZS UT WOS:000344214100040 ER PT J AU Hintz, ES AF Hintz, Eric S. TI Tesla: Inventor of the Electrical Age. SO BUSINESS HISTORY REVIEW LA English DT Book Review C1 [Hintz, Eric S.] Smithsonian Inst, Lemelson Ctr, Washington, DC 20560 USA. RP Hintz, ES (reprint author), Smithsonian Inst, Lemelson Ctr, 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 2014 VL 88 IS 2 BP 394 EP 396 DI 10.1017/S0007680514000129 PG 4 WC Business; History Of Social Sciences SC Business & Economics; Social Sciences - Other Topics GA AS4CR UT WOS:000344221500014 ER PT J AU Kaeppler, AL AF Kaeppler, Adrienne L. TI SISTER MALIA TU'IFUA DESCENDANT OF CHIEFS, DAUGHTER OF GOD SO JOURNAL OF THE POLYNESIAN SOCIETY LA English DT Article DE Tonga; Marist sisters; Second World War; women's development; dance AB This portrait of Sister Tu'ifua (1924-2007), explores the life of high-ranking Halakihe'umata Tu'ifua from her inauspicious birth in Lapaha, Tonga, to her profession in becoming a Roman Catholic nun and her subsequent work for the church. The account details several features of her early life: her love of dancing and performing, her interaction with American servicemen during the Second World War, and her reason for becoming a nun. It then follows Sister Tu'ifua's career: teaching children, development work with Tongan women and, latterly, her international role and work for the betterment of the poorest of Tongan people. C1 [Kaeppler, Adrienne L.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Kaeppler, AL (reprint author), Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, MRC 112,10th & Constitut Ave NW, Washington, DC 20560 USA. EM KAEPPLEA@si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU POLYNESIAN SOC INC PI AUCKLAND PA C/O MAORI STUDIES, UNIV AUCKLAND, PRIVATE BAG, AUCKLAND 92019, NEW ZEALAND SN 0032-4000 EI 2230-5955 J9 J POLYNESIAN SOC JI J. Polyn. Soc. PD JUN PY 2014 VL 123 IS 2 SI SI BP 169 EP 183 PG 15 WC Anthropology SC Anthropology GA AR6JH UT WOS:000343689400005 ER PT J AU Stassun, KG Feiden, GA Torres, G AF Stassun, Keivan G. Feiden, Gregory A. Torres, Guillermo TI Empirical tests of pre-main-sequence stellar evolution models with eclipsing binaries SO NEW ASTRONOMY REVIEWS LA English DT Article ID LOW-MASS STARS; ORION NEBULA CLUSTER; EQUATION-OF-STATE; HIGH-RESOLUTION SPECTROSCOPY; OBSERVED LUMINOSITY SPREAD; MULTICOLOR OPTICAL SURVEY; UPPER CENTAURUS-LUPUS; TY CORONAE AUSTRALIS; M-DWARF STARS; BROWN DWARFS AB We examine the performance of standard pre-main-sequence (PMS) stellar evolution models against the accurately measured properties of a benchmark sample of 26 PMS stars in 13 eclipsing binary (EB) systems having masses 0.04-4.0 M-circle dot and nominal ages approximate to 1-20 Myr. We provide a definitive compilation of all fundamental properties for the EBs, with a careful and consistent reassessment of observational uncertainties. We also provide a definitive compilation of the various PMS model sets, including physical ingredients and limits of applicability. No set of model isochrones is able to successfully reproduce all of the measured properties of all of the EBs. In the H-R diagram, the masses inferred for the individual stars by the models are accurate to better than 10% at >= 1 M-circle dot, but below 1 M-circle dot they are discrepant by 50-100%. Adjusting the observed radii and temperatures using empirical relations for the effects of magnetic activity helps to resolve the discrepancies in a few cases, but fails as a general solution. We find evidence that the failure of the models to match the data is linked to the triples in the EB sample; at least half of the EBs possess tertiary companions. Excluding the triples, the models reproduce the stellar masses to better than similar to 10% in the H-R diagram, down to 0.5 M-circle dot, below which the current sample is fully contaminated by tertiaries. We consider several mechanisms by which a tertiary might cause changes in the EB properties and thus corrupt the agreement with stellar model predictions. We show that the energies of the tertiary orbits are comparable to that needed to potentially explain the scatter in the EB properties through injection of heat, perhaps involving tidal interaction. It seems from the evidence at hand that this mechanism, however it operates in detail, has more influence on the surface properties of the stars than on their internal structure, as the lithium abundances are broadly in good agreement with model predictions. The EBs that are members of young clusters appear individually coeval to within 20%, but collectively show an apparent age spread of similar to 50%, suggesting true age spreads in young clusters. However, this apparent spread in the EB ages may also be the result of scatter in the EB properties induced by tertiaries. (C) 2014 Elsevier B.V. All rights reserved. C1 [Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Feiden, Gregory A.] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Stassun, KG (reprint author), Vanderbilt Univ, Dept Phys & Astron, 1807 Stn B, Nashville, TN 37235 USA. EM keivan.stassun@vanderbilt.edu; gregory.a.feiden@gmail.com; gtorres@cfa.harvard.edu RI Feiden, Gregory/F-1505-2015 OI Feiden, Gregory/0000-0002-2012-7215 FU NSF grants [AST-1009810, AST-0849736, AST-1007992, AST-0908345] FX KGS acknowledges NSF grants AST-1009810 and AST-0849736. GT acknowledges partial support from NSF grant AST-1007992. GAF acknowledges NSF grant AST-0908345 and the William H. Neukom 1964 Institute for Computational Science at Dartmouth College, which both supported the development of the magnetic Dartmouth stellar evolution code. This research has made use of NASA's Astrophysics Data System, the SIMBAD database and the VizieR catalog access tool, both operated at CDS, Strasbourg, France, and the ROSAT data archive tools hosted by the High Energy Astrophysics Science Archive Research Center (HEASARC) at NASA's Goddard Space Flight Center. The research has also made use of data obtained from the Chandra Data Archive and the Chandra Source Catalog, and software provided by the Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa. We thank Scott Wolk for his assistance in the use of those tools. NR 148 TC 23 Z9 23 U1 2 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 EI 1872-9630 J9 NEW ASTRON REV JI New Astron. Rev. PD JUN-AUG PY 2014 VL 60-61 BP 1 EP 28 DI 10.1016/j.newar.2014.06.001 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR1SN UT WOS:000343365000001 ER PT J AU Ernst, CH Creque, TR Orr, JM Hartsell, TD Laemmerzahl, AF AF Ernst, Carl H. Creque, Terry R. Orr, John M. Hartsell, Traci D. Laemmerzahl, Arndt F. TI Operating Body Temperatures in a Snake Community of Northern Virginia SO NORTHEASTERN NATURALIST LA English DT Article ID EASTERN WORM SNAKE; CARPHOPHIS-AMOENUS; GARTER SNAKES; THAMNOPHIS AB Thermal data were collected from 15 of 16 species of snakes found at the Mason Neck National Wildlife Refuge, Fairfax County, VA. Data recorded at each capture included the date, 24-hour military time, body temperature (BT), air temperature (AT), ground-surface temperature (ST), water temperature (WT) if in water, and the snake's activity (under cover, moving on land, basking, foraging, climbing, swimming, courting/mating). The purpose of this study was to determine the potential range of operating body temperature (OBT) of the individual species. The range of OBT is interpreted as the snake's operating temperature at its current environmental temperatures (ET), which can be used in comparisons with similar data from other North American regions, and represents the first such report from the Mid-Atlantic Region. The mean and ranges of BT, AT, ST, and WT are presented for the eight snakes with 20 or more records: Carphophis amoenus (n = 238), Coluber constrictor (204), Nerodia sipedon (67), Thamnophis sirtalis (55), Diadophis punctatus (54), Pantherophis alleghaniensis (43), Thamnophis sauritus (26), and Agkistrodon contortrix (24). New thermal records are reported for several of these species. The ranges of BT during activities are also reported. New temperature records are also reported for Virginia valeriae (n = 16 encounters), Storeria dekayi (12), Opheodrys aestivus (6), Lampropeltis calligaster (6), and Regina septemvittata (2). C1 [Ernst, Carl H.] Smithsonian Inst, Div Amphibians & Reptiles, Washington, DC 20013 USA. [Creque, Terry R.; Orr, John M.] George Mason Univ, Dept Environm Sci & Publ Policy, Fairfax, VA 22030 USA. [Hartsell, Traci D.] Homeland Secur Invest, Lorton, VA 20598 USA. [Laemmerzahl, Arndt F.] George Mason Univ, Biol Program, Fairfax, VA 22030 USA. RP Ernst, CH (reprint author), Smithsonian Inst, Div Amphibians & Reptiles, Mrc 162,POB 37012, Washington, DC 20013 USA. EM chernst@frontiernet.net NR 41 TC 2 Z9 3 U1 7 U2 25 PU HUMBOLDT FIELD RESEARCH INST PI STEUBEN PA PO BOX 9, STEUBEN, ME 04680-0009 USA SN 1092-6194 EI 1938-5307 J9 NORTHEAST NAT JI Northeast. Nat PD JUN PY 2014 VL 21 IS 2 BP 247 EP 258 DI 10.1656/045.021.0205 PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AQ0QP UT WOS:000342488100007 ER PT J AU Curet, LA AF Curet, L. Antonio TI The Taino: Phenomena, Concepts, and Terms SO ETHNOHISTORY LA English DT Article ID HISTORY; CHIEFDOMS AB The Taino term and concept has traditionally been used as a designation of some form of cultural identity for the groups that occupied the Greater Antilles at the time of contact. This perspective assumes that these groups shared a cultural background because of a common ancestry. However, this position has been questioned in recent years, and many problems with the concept have been brought to light. This article presents the history of the concept and discusses three recent studies that have proposed new ways to approach the problem. It ends by presenting the implications of this new perspective for future research, their limitations, how they may be misapplied, and to what extent they are applicable in different situations. C1 Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. RP Curet, LA (reprint author), Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. NR 82 TC 0 Z9 0 U1 1 U2 5 PU DUKE UNIV PRESS PI DURHAM PA 905 W MAIN ST, STE 18-B, DURHAM, NC 27701 USA SN 0014-1801 EI 1527-5477 J9 ETHNOHISTORY JI Ethnohistory PD SUM PY 2014 VL 61 IS 3 BP 467 EP 495 DI 10.1215/00141801-2681759 PG 29 WC Anthropology; History SC Anthropology; History GA AN4ST UT WOS:000340579500004 ER PT J AU Bouley, S Craddock, RA AF Bouley, Sylvain Craddock, Robert A. TI Age dates of valley network drainage basins and subbasins within Sabae and Arabia Terrae, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID DIGITAL ELEVATION MODELS; MARTIAN HIGHLANDS; EVOLUTION; PRECIPITATION; CHRONOLOGY; LANDSCAPE; MARINERIS; INCISION; DEPOSITS; SURFACE AB The precise timing of valley network drainage basin formation is critical to understanding the history of water and climate on Mars. To determine whether there are any variations in ages within separate drainage basins and subbasins that may reflect local or regional variations in climate or resetting from resurfacing (e.g., impact ejecta or lava flows), we dated 27 basins and subbasins in Sabaea and Arabia Terrae. The age-dating basin technique we employed allowed sufficient precision to give accurate ages and shows that fluvial activity within the basins and subbasins ceased at approximately the same time around the Early Hesperian/Late Hesperian transition. Our results support the hypothesis that valley networks formed during a unique "fluvial optimum" that may have shut off gradually because of a global climate change that affected all areas simultaneously on Mars. C1 [Bouley, Sylvain] GEOPS Geosci Paris Sud, UMR 8148, Orsay, France. [Craddock, Robert A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Craddock, RA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM craddockb@si.edu FU NASA's Mars Data Analysis Program [NNX09AI40G] FX Ross Irwin provided the shapefiles from his previous study that became the basis for the study proposed here. This research was supported by NASA's Mars Data Analysis Program, grant NNX09AI40G. NR 45 TC 1 Z9 1 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN PY 2014 VL 119 IS 6 BP 1302 EP 1310 DI 10.1002/2013JE004571 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN4CK UT WOS:000340535000010 ER PT J AU Arvidson, RE Bellutta, P Calef, F Fraeman, AA Garvin, JB Gasnault, O Grant, JA Grotzinger, JP Hamilton, VE Heverly, M Iagnemma, KA Johnson, JR Lanza, N Le Mouelic, S Mangold, N Ming, DW Mehta, M Morris, RV Newsom, HE Renno, N Rubin, D Schieber, J Sletten, R Stein, NT Thuillier, F Vasavada, AR Vizcaino, J Wiens, RC AF Arvidson, R. E. Bellutta, P. Calef, F. Fraeman, A. A. Garvin, J. B. Gasnault, O. Grant, J. A. Grotzinger, J. P. Hamilton, V. E. Heverly, M. Iagnemma, K. A. Johnson, J. R. Lanza, N. Le Mouelic, S. Mangold, N. Ming, D. W. Mehta, M. Morris, R. V. Newsom, H. E. Renno, N. Rubin, D. Schieber, J. Sletten, R. Stein, N. T. Thuillier, F. Vasavada, A. R. Vizcaino, J. Wiens, R. C. TI Terrain physical properties derived from orbital data and the first 360 sols of Mars Science Laboratory Curiosity rover observations in Gale Crater SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID CHEMCAM INSTRUMENT SUITE; SURFACE-PROPERTIES; LASER-ABLATION; MISSION; UNIT AB Physical properties of terrains encountered by the Curiosity rover during the first 360 sols of operations have been inferred from analysis of the scour zones produced by Sky Crane Landing System engine plumes, wheel touch down dynamics, pits produced by Chemical Camera (ChemCam) laser shots, rover wheel traverses over rocks, the extent of sinkage into soils, and the magnitude and sign of rover-based slippage during drives. Results have been integrated with morphologic, mineralogic, and thermophysical properties derived from orbital data, and Curiosity-based measurements, to understand the nature and origin of physical properties of traversed terrains. The hummocky plains (HP) landing site and traverse locations consist of moderately to well-consolidated bedrock of alluvial origin variably covered by slightly cohesive, hard-packed basaltic sand and dust, with both embedded and surface-strewn rock clasts. Rock clasts have been added through local bedrock weathering and impact ejecta emplacement and form a pavement-like surface in which only small clasts (<5 to 10 cm wide) have been pressed into the soil during wheel passages. The bedded fractured (BF) unit, site of Curiosity's first drilling activity, exposes several alluvial-lacustrine bedrock units with little to no soil cover and varying degrees of lithification. Small wheel sinkage values (<1 cm) for both HP and BF surfaces demonstrate that compaction resistance countering driven-wheel thrust has been minimal and that rover slippage while traversing across horizontal surfaces or going uphill, and skid going downhill, have been dominated by terrain tilts and wheel-surface material shear modulus values. C1 [Arvidson, R. E.; Fraeman, A. A.; Stein, N. T.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Bellutta, P.; Calef, F.; Heverly, M.; Vasavada, A. R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Garvin, J. B.] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. [Gasnault, O.] Univ Toulouse UPS OMP, CNRS, IRAP, Toulouse, France. [Grant, J. A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Grotzinger, J. P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Hamilton, V. E.] SW Res Inst, Boulder, CO USA. [Iagnemma, K. A.] MIT, Dept Mech Engn, Cambridge, MA 02139 USA. [Johnson, J. R.] Johns Hopkins Appl Phys Lab, Laurel, MD USA. [Lanza, N.; Wiens, R. C.] Los Alamos Natl Lab, Los Alamos, NM USA. [Le Mouelic, S.; Mangold, N.; Thuillier, F.] CNRS, UMR6112, LPGN, Nantes, France. [Le Mouelic, S.; Mangold, N.; Thuillier, F.] Univ Nantes, Nantes, France. [Ming, D. W.; Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Mehta, M.; Vizcaino, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Newsom, H. E.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Renno, N.] Univ Michigan, Ann Arbor, MI 48109 USA. [Rubin, D.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Schieber, J.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. [Sletten, R.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. RP Arvidson, RE (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. EM arvidson@wunder.wustl.edu RI Johnson, Jeffrey/F-3972-2015; OI Gasnault, Olivier/0000-0002-6979-9012 FU NASA FX We thank NASA for support for our work on MSL and CRISM, and we thank the science and engineering teams associated with the Mars Science Laboratory, HiRISE, CRISM, and THEMIS for planning and acquisition of the data used in this paper. Data are available from the NASA Planetary Data System Geosciences Node (http://pds-geosciences.wustl.edu/). NR 50 TC 11 Z9 11 U1 0 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN PY 2014 VL 119 IS 6 BP 1322 EP 1344 DI 10.1002/2013JE004605 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN4CK UT WOS:000340535000012 ER PT J AU Weller, DE Baker, ME AF Weller, Donald E. Baker, Matthew E. TI CROPLAND RIPARIAN BUFFERS THROUGHOUT CHESAPEAKE BAY WATERSHED: SPATIAL PATTERNS AND EFFECTS ON NITRATE LOADS DELIVERED TO STREAMS SO JOURNAL OF THE AMERICAN WATER RESOURCES ASSOCIATION LA English DT Article DE watersheds; geospatial analysis; nonpoint source pollution; watershed management; nitrate nitrogen; riparian buffer; cropland; flow-path analysis; Chesapeake Bay ID LAND-COVER; COASTAL-PLAIN; DISCHARGES; NITROGEN; MODELS; QUALITY; AGRICULTURE; RESTORATION; PHOSPHORUS; CHALLENGES AB We used statistical models to provide the first empirical estimates of riparian buffer effects on the cropland nitrate load to streams throughout the Chesapeake Bay watershed. For each of 1,964 subbasins, we quantified the 1990 prevalence of cropland and riparian buffers. Cropland was considered buffered if the topographic flow path connecting it to a stream traversed a streamside forest or wetland. We applied a model that predicts stream nitrate concentration based on physiographic province and the watershed proportions of unbuffered and buffered cropland. We used another model to predict annual streamflow based on precipitation and temperature, and then multiplied the predicted flows and concentrations to estimate 1990 annual nitrate loads. Across the entire Chesapeake watershed, croplands released 92.3 Gg of nitrate nitrogen, but 19.8 Gg of that was removed by riparian buffers. At most, 29.4 Gg more might have been removed if buffer gaps were restored so that all cropland was buffered. The other 43.1 Gg of cropland load cannot be addressed with riparian buffers. The Coastal Plain physiographic province provided 52% of the existing buffer reduction of Bay-wide nitrate loads and 36% of potential additional removal from buffer restoration in cropland buffer gaps. Existing and restorable nitrate removal in buffers were lower in the other three major provinces because of less cropland, lower buffer prevalence, and lower average buffer nitrate removal efficiency. C1 [Weller, Donald E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Baker, Matthew E.] Univ Maryland Baltimore Cty, Dept Geog & Environm Syst, Baltimore, MD 21250 USA. RP Weller, DE (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM wellerd@si.edu RI Baker, Matthew/I-2839-2014; OI Baker, Matthew/0000-0001-5069-0204; Weller, Donald/0000-0002-7629-5437 FU U.S. Environmental Protection Agency [R-82868401]; Watershed Classification Program (USEPA) [R-831369]; CICEET, the Cooperative Institute for Coastal and Estuarine Environmental Technology FX Support for this research was provided in part by grants from the U.S. Environmental Protection Agency's Science to Achieve Results (STAR) Estuarine and Great Lakes (EaGLes) Program to the Atlantic Slope Consortium (USEPA Agreement #R-82868401) and the Watershed Classification Program (USEPA Agreement #R-831369). Although the research described in this article has been funded by the U.S. Environmental Protection Agency, it has not been subjected to the Agency's required peer and policy review and therefore does not necessarily reflect the views of the Agency, and no official endorsement should be inferred. Further support was provided by CICEET, the Cooperative Institute for Coastal and Estuarine Environmental Technology. The stream data were collected with support from NSF (BSR-89-05219, DEB-92-06811, and DEB-93-17968), NOAA (NA66RG0129), the Governor's Research Council of Maryland, the government of Charles County Maryland, and the Smithsonian Institution Environmental Sciences Program. David L. Correll and Thomas E. Jordan led the stream sampling program. Tom Jordan, Meghan Williams, and three anonymous reviewers provided helpful comments on the manuscript. Molly Van Appledorn helped develop the ArcGIS Toolbox and calculated land cover metrics for the Chesapeake Watershed. Richard Vogel and Ian Wilson provided the data underlying their 1998 regional discharge model, and Gary Shenk provided results from the Chesapeake Bay Program watershed model. NR 52 TC 7 Z9 8 U1 6 U2 28 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1093-474X EI 1752-1688 J9 J AM WATER RESOUR AS JI J. Am. Water Resour. Assoc. PD JUN PY 2014 VL 50 IS 3 BP 696 EP 712 DI 10.1111/jawr.12207 PG 17 WC Engineering, Environmental; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA AN3CQ UT WOS:000340462900012 ER PT J AU Escovar, JE Gonzalez, R Quinones, ML Wilkerson, RC Ruiz, F Harrison, BA AF Eduardo Escovar, Jesus Gonzalez, Ranulfo Quinones, Martha L. Wilkerson, Richard C. Ruiz, Fredy Harrison, Bruce A. TI Morphology of the larvae, male genitalia and DNA sequences of Anopheles (Kerteszia) pholidotus (Diptera: Culicidae) from Colombia SO MEMORIAS DO INSTITUTO OSWALDO CRUZ LA English DT Article DE Kerteszia; Anopheles pholidotus; male genitalia; DNA sequences ID MALARIA VECTOR; SOUTHEASTERN BRAZIL; SUBGENUS KERTESZIA; CHARACTERS; PACIFIC AB Since 1984, Anopheles (Kerteszia) lepidotus has been considered a mosquito species that is involved in the transmission of malaria in Colombia, after having been incriminated as such with epidemiological evidence from a malaria outbreak in Cunday-Villarrica, Tolima. Subsequent morphological analyses of females captured in the same place and at the time of the outbreak showed that the species responsible for the transmission was not An. lepidotus, but rather Anopheles pholidotus. However, the associated morphological stages and DNA sequences of An. pholidotus from the foci of Cunday-Villarrica had not been analysed. Using samples that were caught recently from the outbreak region, the purpose of this study was to provide updated and additional information by analysing the morphology of female mosquitoes, the genitalia of male mosquitoes and fourth instar larvae of An. pholidotus, which was confirmed with DNA sequences of cytochrome oxidase I and rDNA internal transcribed spacer. A total of 1,596 adult females were collected in addition to 37 larval collections in bromeliads. Furthermore, 141 adult females, which were captured from the same area in the years 1981-1982, were analysed morphologically. Ninety-five DNA sequences were analysed for this study. Morphological and molecular analyses showed that the species present in this region corresponds to An. pholidotus. Given the absence of An. lepidotus, even in recent years, we consider that the species of mosquitoes that was previously incriminated as the malaria vector during the outbreak was indeed An. pholidotus, thus ending the controversy. C1 [Eduardo Escovar, Jesus; Quinones, Martha L.] Univ Nacl Colombia, Bogota, Cundinamarca, Colombia. [Eduardo Escovar, Jesus] Univ Salle, Bogota, Cundinamarca, Colombia. [Gonzalez, Ranulfo] Univ Valle, Fac Nat & Exact Sci, Valle, Colombia. [Wilkerson, Richard C.; Ruiz, Fredy] Smithsonian Inst, Museum Support Ctr, Walter Reed Biosystemat Unit, Suitland, MD USA. [Harrison, Bruce A.] Western Carolina Univ, Coll Hlth & Human Sci, Clemmons, NC USA. RP Escovar, JE (reprint author), Univ Nacl Colombia, Bogota, Cundinamarca, Colombia. EM jeescobar@unisalle.edu.co FU COLCIENCIAS [110145921478] FX COLCIENCIAS (110145921478) NR 28 TC 4 Z9 4 U1 0 U2 3 PU FUNDACO OSWALDO CRUZ PI RIO DE JANEIRO, RJ PA AV BRASIL 4365, 21045-900 RIO DE JANEIRO, RJ, BRAZIL SN 0074-0276 EI 1678-8060 J9 MEM I OSWALDO CRUZ JI Mem. Inst. Oswaldo Cruz PD JUN PY 2014 VL 109 IS 4 BP 473 EP 479 DI 10.1590/0074-0276130596 PG 7 WC Parasitology; Tropical Medicine SC Parasitology; Tropical Medicine GA AN3LE UT WOS:000340488700012 PM 25075785 ER PT J AU Rooney, TO Bastow, ID Keir, D Mazzarini, F Movsesian, E Grosfils, EB Zimbelman, JR Ramsey, MS Ayalew, D Yirgu, G AF Rooney, Tyrone O. Bastow, Ian D. Keir, Derek Mazzarini, Francesco Movsesian, Emily Grosfils, Eric B. Zimbelman, James R. Ramsey, Michael S. Ayalew, Dereje Yirgu, Gezahegn TI The protracted development of focused magmatic intrusion during continental rifting SO TECTONICS LA English DT Article ID MAIN-ETHIOPIAN-RIFT; EAST-AFRICAN RIFT; GEOCHEMICAL EVIDENCE; EXTENSION DIRECTION; VELOCITY STRUCTURE; CRUSTAL STRUCTURE; MAGNETIC-ANOMALIES; VOLCANIC PROVINCE; BASIN DEVELOPMENT; OCEAN TRANSITION AB The transition from mechanical thinning toward focused magmatic intrusion during continental rifting is poorly constrained; the tectonically active Main Ethiopian Rift (MER) provides an ideal study locale to address this issue. The presence of linear magmatic-tectonic belts in the relatively immature central MER may indicate that the transition from mechanical to magmatic rifting is more spatially distributed and temporally protracted than has previously been assumed. Here we examine lava geochemistry and vent distribution of a Pliocene-Quaternary linearmagmatic chain along the western margin of the central MER-the Akaki Magmatic Zone. Our results show limited variability in parental magma that evolve in a complex polybaric fractionation system that has not changed significantly over the past 3 Ma. Our results suggest the following: (1) channeling of plume material and the localization of shear-or topography-induced porosity modulates melt intrusion into the continental lithosphere. (2) Pre-existing lithospheric structures may act as catalysts for intrusion of magmas into the lithospheric mantle. (3) The midcrustal to upper crustal strain regime dictates the surface orientation of volcanic vents. Therefore, although linear magmatic belts like those in the central MER may young progressively toward the rift axis and superficially resemble oceanic style magmatism, they actually represent prebreakup magmatism on continental crust. The oldest linear magmatic belts observed seismically and magnetically at the edge of the ocean basins thus may not, as is often assumed, actually mark the onset of seafloor spreading. C1 [Rooney, Tyrone O.; Movsesian, Emily] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA. [Bastow, Ian D.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London, England. [Keir, Derek] Univ Southampton, Natl Oceanog Ctr Southampton, Southampton, Hants, England. [Mazzarini, Francesco] Ist Nazl Geofis & Vulcanol, Pisa, Italy. [Grosfils, Eric B.] Pomona Coll, Dept Geol, Claremont, CA 91711 USA. [Zimbelman, James R.] Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 315, Washington, DC 20560 USA. [Ramsey, Michael S.] Univ Pittsburgh, Dept Geol & Planetary Sci, Pittsburgh, PA 15260 USA. [Ayalew, Dereje] Univ Addis Ababa, Sch Earth Sci, Addis Ababa, Ethiopia. RP Rooney, TO (reprint author), Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA. EM rooneyt@MSU.EDU RI Rooney, Tyrone/B-4594-2010; Mazzarini, Francesco/L-1369-2015; OI Mazzarini, Francesco/0000-0002-3864-6558; Keir, Derek/0000-0001-8787-8446 FU NASA Planetary Geology and Geophysics grant [NNX11AQ82G] FX This work was supported by NASA Planetary Geology and Geophysics grant NNX11AQ82G. W. Nelson and A. Mekonnen assisted with the field sample collection. We thank Giacomo Corti and an anonymous reviewer for comments that improved the manuscript. T.O.R. thanks Tanya Furman for many fruitful discussions on the nature of magmatism in the Ethiopian Rift. Brandon Chiasera, Kaitlyn Trestrail, Paul Mohr, and Susan Krans are thanked for proof-reading. We thank Margaret Rusmore for careful editorial handling. NR 112 TC 12 Z9 12 U1 3 U2 21 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0278-7407 EI 1944-9194 J9 TECTONICS JI Tectonics PD JUN PY 2014 VL 33 IS 6 BP 875 EP 897 DI 10.1002/2013TC003514 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN0CD UT WOS:000340248700001 ER PT J AU Marrow, JC Padilla, LR Hayek, LAC Bush, M Murray, S AF Marrow, Judilee C. Padilla, Luis R. Hayek, Lee-Ann C. Bush, Mitch Murray, Suzan TI COMPARISON OF ANTIBODY RESPONSE TO A NON-ADJUVANTED, LIVE CANARYPOX-VECTORED RECOMBINANT RABIES VACCINE AND A KILLED, ADJUVANTED RABIES VACCINE IN ELD'S DEER (RUCERVUS ELDI THAMIN) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Cervid; Eld's deer; rabies; Rucervus eldi thamin; vaccination ID MATERNAL ANTIBODIES; VIRUS AB Captive Eld's deer (Rucervus eldi thamin) were evaluated for the presence of rabies virus-neutralizing antibodies using a rapid fluorescent focus inhibition after vaccination with either a live canarypox-vectored recombinant rabies vaccine or a killed monovalent rabies vaccine. Twelve deer were vaccinated with 1.0 ml of killed, adjuvanted, monovalent rabies vaccine at 5-33 mo of age then annually thereafter, and 14 deer were vaccinated with 1.0 ml nonadjuvanted, live canarypox-vectored rabies vaccine at 3-15 mo of age then annually thereafter. Banked serum was available or collected prospectively from deer at 6 mo and 1 yr after initial vaccination, then collected annually. Rabies virus-neutralizing antibodies considered adequate (>0.5 IU/ml) were present in 20/34 samples vaccinated with canarypox-vectored rabies vaccine and in 12/14 samples vaccinated with killed adjuvanted rabies vaccine. Poor seroconversion was noted in deer less than 6 mo of age vaccinated with the canarypox-vectored rabies vaccine. C1 [Marrow, Judilee C.; Padilla, Luis R.; Bush, Mitch] Species Survival Ctr, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Marrow, Judilee C.; Murray, Suzan] Smithsonian Conservat Biol Inst, Smithsonian Inst Natl Zool Pk, Washington, DC 20008 USA. [Hayek, Lee-Ann C.] Smithsonian Inst, Washington, DC 20013 USA. RP Marrow, JC (reprint author), Binder Pk Zoo, 7400 Div Dr, Battle Creek, MI 49014 USA. EM judileemarrowdvm@gmail.com NR 18 TC 0 Z9 0 U1 0 U2 8 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 2014 VL 45 IS 2 BP 315 EP 320 PG 6 WC Veterinary Sciences SC Veterinary Sciences GA AM2AF UT WOS:000339649800013 PM 25000692 ER PT J AU Najera, F Brown, J Kaufman, K Schwartz, R Goodrowe, K Asaithanmakul, W Aitken-Palmer, C Kongprom, U Wildt, DE Bush, M AF Najera, Fernando Brown, Janine Kaufman, Krystle Schwartz, Rick Goodrowe, Karen Asaithanmakul, Wisit Aitken-Palmer, Copper Kongprom, Urarikha Wildt, David E. Bush, Mitchell TI SWIMMER SYNDROME IN A CLOUDED LEOPARD (NEOFELIS NEBULOSA) CUB SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Clouded leopard; cub; felid; Neofelis nebulosa; swimmer syndrome ID PECTUS EXCAVATUM; CATS; DOGS AB A 32-day-old, hand-reared, captive-born female clouded leopard (Neofelis nebulosa) cub presented as being unable to stand, ambulate, or adduct both hind limbs. The cub exhibited hyperextension of both tarsal joints and a flattened thorax, which limited mobility to "swimmer-like'' movements. Neither congenital defects nor neurologic deficits were observed during the medical examination. Radiographic examination showed the thorax was compressed dorsoventrally, but no other skeletal abnormalities were detected. Based on clinical signs, the condition was more consistent with swimmer syndrome, which has been described in young offspring of several domestic species. Over the course of 3 wk, affected limbs were treated by intensive physiotherapy, corrective bandages were applied, and thermotherapy was used to improve circulation, which resulted in a complete recovery and development of subsequent normal ambulation. It is concluded that early diagnosis and treatment of this condition led to the resolution of clinical signs, resulting in normal development of the clouded leopard cub reported here. C1 [Najera, Fernando; Kaufman, Krystle; Asaithanmakul, Wisit; Kongprom, Urarikha] Khao Kheow Open Zoo, Thailand Clouded Leopard Consortium, Sriracha 20110, Chonburi, Thailand. [Najera, Fernando; Brown, Janine; Aitken-Palmer, Copper; Wildt, David E.; Bush, Mitchell] Smithsonian Conservat Biol Inst, Ctr Species Survival, Dept Reprod Sci, Front Royal, VA 22630 USA. [Najera, Fernando; Goodrowe, Karen] Point Defiance Zoo & Aquarium, Tacoma, WA 98407 USA. [Najera, Fernando; Schwartz, Rick] Nashville Zoo Grassmere, Nashville, TN 37211 USA. RP Najera, F (reprint author), Thailand Clouded Leopard Consortium, POB 2311, Gig Harbor, WA 98335 USA. EM borneanwildcatvet@gmail.com NR 12 TC 0 Z9 0 U1 1 U2 9 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 2014 VL 45 IS 2 BP 386 EP 388 DI 10.1638/2012-0289R2.1 PG 3 WC Veterinary Sciences SC Veterinary Sciences GA AM2AF UT WOS:000339649800024 PM 25000703 ER PT J AU Steeil, JC Schumacher, J George, RH Bulman, F Baine, K Cox, S AF Steeil, James C. Schumacher, Juergen George, Robert H. Bulman, Frank Baine, Katherine Cox, Sherry TI PHARMACOKINETICS OF CEFOVECIN (CONVENIA (R)) IN WHITE BAMBOO SHARKS (CHILOSCYLLIUM PLAGIOSUM) AND ATLANTIC HORSESHOE CRABS (LIMULUS POLYPHEMUS) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Cefovecin; Chiloscyllium plagiosum; horseshoe crab; Limulus polyphemus; pharmacokinetics; white bamboo shark ID CEPHALOSPORIN; SPECTRUM; CATS; DOGS AB Cefovecin was administered to six healthy adult white bamboo sharks (Chiloscyllium plagiosum) and six healthy adult Atlantic horseshoe crabs (Limulus polyphemus) to determine its pharmacokinetics in these species. A single dose of cefovecin at 8 mg/kg was administered subcutaneously in the epaxial region of the bamboo sharks and in the proximal articulation of the lateral leg of the horseshoe crabs. Blood and hemolymph samples were collected at various time points from bamboo sharks and Atlantic horseshoe crabs. High performance liquid chromatography was performed to determine plasma levels of cefovecin. The terminal half-life of cefovecin in Atlantic horseshoe crabs was 37.70 +/- 9.04 hr and in white bamboo sharks was 2.02 +/- 4.62 hr. Cefovecin concentrations were detected for 4 days in white bamboo sharks and for 14 days in Atlantic horseshoe crabs. No adverse effects associated with cefovecin administration were seen in either species. C1 [Steeil, James C.; Schumacher, Juergen; Baine, Katherine] Univ Tennessee, Coll Vet Med, Dept Small Anim Clin Sci, Knoxville, TN 37996 USA. [Cox, Sherry] Univ Tennessee, Coll Vet Med, Dept Biomed & Diagnost Sci, Knoxville, TN 37996 USA. [George, Robert H.; Bulman, Frank] Ripleys Aquarium Smokies, Gatlinburg, TN 37738 USA. RP Steeil, JC (reprint author), Smithsonian Natl Zool Pk, Dept Anim Hlth, 3001 Connecticut Ave, Washington, DC 20013 USA. EM jamste7@gmail.com OI Schumacher, Juergen/0000-0003-3973-7248; Cox, Sherry/0000-0002-5184-900X FU Faculty Education Advancement and Research Fund, College of Veterinary Medicine, The University of Tennessee FX The authors thank Ms. Amanda Gudgel and the aquarists at Ripley's Aquarium of the Smokies for their technical assistance and Pfizer Animal Health for providing the Convenia (cefovecin) used in this study. This study was funded by the Faculty Education Advancement and Research Fund, College of Veterinary Medicine, The University of Tennessee. NR 10 TC 3 Z9 3 U1 1 U2 15 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 EI 1937-2825 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD JUN PY 2014 VL 45 IS 2 BP 389 EP 392 DI 10.1638/2013-0061R2.1 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA AM2AF UT WOS:000339649800025 PM 25000704 ER PT J AU Martinez-Melendez, N Martinez-Camilo, R Perez-Farrera, MA Skog, LE Barrie, F AF Martinez-Melendez, Nayely Martinez-Camilo, Ruben Angel Perez-Farrera, Miguel Skog, Laurence E. Barrie, Fred TI A new species of Alsobia (Gesneriaceae) from Chiapas, Mexico SO REVISTA MEXICANA DE BIODIVERSIDAD LA Spanish DT Article DE Episcia; Episcieae; endemic species; Selva El Ocote biosphere reserve ID EPISCIEAE GESNERIACEAE; NDHF SEQUENCES AB Alsobia chiapensis, a new species from Chiapas, Mexico is described and illustrated. It differs from its 2 congeners by a relatively larger corolla and shorter limb; linear-lanceolate calyx lobes; and petiole less than a third of the length of the leaf blade. The new species shares characteristics found in other species of Alsobia such as fimbriate margins on the corolla lobes, and stolons. C1 [Martinez-Melendez, Nayely; Martinez-Camilo, Ruben; Angel Perez-Farrera, Miguel] Univ Ciencias & Artes Chiapas, Fac Ciencias Biol, Herbario Eizi Matuda, Tuxtla Gutierrez 29039, Chiapas, Mexico. [Skog, Laurence E.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Barrie, Fred] Missouri Bot Garden, St Louis, MO 63166 USA. [Martinez-Camilo, Ruben] Colegio La Frontera Sur, Unidad San Cristobal de Las Casas, San Cristobal Las Casas 29290, Chiapas, Mexico. RP Martinez-Melendez, N (reprint author), Univ Ciencias & Artes Chiapas, Fac Ciencias Biol, Herbario Eizi Matuda, Libramiento Norte Poniente 1150, Tuxtla Gutierrez 29039, Chiapas, Mexico. EM nayely.martinez@unicach.mx NR 14 TC 1 Z9 1 U1 1 U2 4 PU INST BIOLOGIA, UNIV NACIONAL AUTONOMA MEXICO PI MEXICO PA APARTADO POSTAL 70-233, MEXICO, D F 00000, MEXICO SN 1870-3453 J9 REV MEX BIODIVERS JI Rev. Mex. Biodivers. PD JUN PY 2014 VL 85 IS 2 BP 343 EP 348 DI 10.7550/rmb.32633 PG 6 WC Biodiversity Conservation SC Biodiversity & Conservation GA AM3UX UT WOS:000339779400001 ER PT J AU Miller, MJ AF Miller, Matthew J. TI A distinctive avian assemblage (Aves: Passeriformes) in Western Darien, Panama is uncovered through a disease surveillance program SO REVISTA DE BIOLOGIA TROPICAL LA English DT Article DE community composition; Darien; rare birds; beta-diversity ID WHITE-SAND FORESTS; BETA-DIVERSITY; BIRDS; TREE; PHYLOGEOGRAPHY; SIMILARITY; AMERICA AB Basic knowledge about the distribution of flora and fauna is lacking for most tropical areas. Improving our knowledge of the tropical biota will help address contemporary global problems, including emerging tropical diseases. Less appreciated is the role that applied studies can have in improving our understanding of basic biological patterns and processes in the tropics. Here, I describe a novel avifauna assemblage uncovered in Western Darien province in the Republic of Panama that was uncovered during a vector-borne disease surveillance program. I compared the passerine bird species composition at 16 sites using records from recent ornithological expeditions sponsored by the Smithsonian Tropical Research Institute in Central and Eastern Panama. Based on the results of a Mantel test, geographic distance did not correlate with pairwise distinctiveness of sites. Instead, based on an index of distinctiveness modified from the Chao-Jaccard index, most sites were more or less similarly distinctive, with one site, Aruza Abajo, significantly more distinctive than the rest. I found that the distinctiveness of this site was due not only to the presence of several rare and range-restricted taxa, but also to the absence of taxa that are common elsewhere. This finding provides more evidence of high species composition turnover (beta-diversity) in the Panamanian biota, which appears to be driven by a combination of soil and climate differences over narrow distances. C1 Smithsonian Trop Res Inst, Panama City, Panama. RP Miller, MJ (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama. EM millerma@si.edu OI Miller, Matthew/0000-0002-2939-0239 FU NIH/NSF "Ecology and Evolution of Infectious Diseases" award from the Fogarty International Center [3R01-TW005869-05S1]; inter-agency award from the US Centers for Disease Control FX I would like to thank Panama's Environmental Ministry (ANAM) for over 10 years of consistent support of scientific collecting in Panama. More than a dozen Latin American students and interns have dedicated their time to helping the STRI Bird Collection grow, and I am indebted to them. The STRI Bird Collection received supported from an NIH/NSF "Ecology and Evolution of Infectious Diseases" award from the Fogarty International Center 3R01-TW005869-05S1 and an inter-agency award from the US Centers for Disease Control ("Effect of Anthropogenic Climate Change on the Ecology of Zoonotic and Vector-borne Diseases"). Prior to 2007, the LSU Museum of Vertebrate Zoology, UNLV Marjorie Barrick Museum, University of Alaska Museum, and the US National Museum sponsored collecting trips in concert with STRI that form the basis of some of the data analyzed here. S. Weaver, University of Texas Medical Branch, provided information regarding his team's ongoing research on equine encephalitic virus in Eastern Panama. J. Touchon, J. Loaiza, A. Crawford, and two anonymous reviewers, provided helpful comments on the manuscript. NR 22 TC 0 Z9 0 U1 1 U2 2 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, 00000, COSTA RICA SN 0034-7744 EI 2215-2075 J9 REV BIOL TROP JI Rev. Biol. Trop. PD JUN PY 2014 VL 62 IS 2 BP 711 EP 717 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AL7GJ UT WOS:000339301800025 PM 25102652 ER PT J AU Schwadron, NA Gorby, M Torok, T Downs, C Linker, J Lionello, R Mikic, Z Riley, P Giacalone, J Chandran, B Germaschewski, K Isenberg, PA Lee, MA Lugaz, N Smith, S Spence, HE Desai, M Kasper, J Kozarev, K Korreck, K Stevens, M Cooper, J MacNeice, P AF Schwadron, Nathan A. Gorby, Matt Torok, Tibor Downs, Cooper Linker, Jon Lionello, Roberto Mikic, Zoran Riley, Pete Giacalone, Joe Chandran, Ben Germaschewski, Kai Isenberg, Phil A. Lee, Martin A. Lugaz, Noe Smith, Sonya Spence, Harlan E. Desai, Mihir Kasper, Justin Kozarev, Kamen Korreck, Kelly Stevens, Mike Cooper, John MacNeice, Peter TI Synthesis of 3-D Coronal-Solar Wind Energetic Particle Acceleration Modules SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID WHOLE SUN MONTH; MAGNETIC-FIELD; MASS EJECTION; 1 AU; FLARES C1 [Schwadron, Nathan A.; Chandran, Ben; Germaschewski, Kai; Isenberg, Phil A.; Lee, Martin A.; Lugaz, Noe; Smith, Sonya; Spence, Harlan E.] Univ New Hampshire, Durham, NH 03824 USA. [Gorby, Matt] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Torok, Tibor; Downs, Cooper; Lionello, Roberto; Mikic, Zoran] Predict Sci Inc, San Diego, CA USA. [Linker, Jon; Riley, Pete] Predict Sci Inc, Morristown, NJ USA. [Giacalone, Joe] Univ Arizona, Tucson, AZ 85721 USA. [Spence, Harlan E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Desai, Mihir] Southwest Res Inst, San Antonio, TX USA. [Kasper, Justin] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Kozarev, Kamen; Korreck, Kelly; Stevens, Mike] Smithsonian Astrophys Observ, Washington, DC USA. [Cooper, John] NASA, Space Phys Data Facil, Washington, DC USA. [Cooper, John] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Heliophys Sci Div, Washington, DC USA. [MacNeice, Peter] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Washington, DC USA. RP Schwadron, NA (reprint author), Univ New Hampshire, Durham, NH 03824 USA. RI Lugaz, Noe/C-1284-2008; Kasper, Justin/D-1152-2010; OI Lugaz, Noe/0000-0002-1890-6156; Kasper, Justin/0000-0002-7077-930X; Riley, Pete/0000-0002-1859-456X FU C-SWEPA (NASA) [NNX13AI75G]; EMMREM [NNX07AC14G]; Sun-2-Ice (NSF) projects [AGS1135432]; DREAM (NASA) [NNX10AB17A]; DREAM2 (NASA) [NNX14AG13A] FX We thank all those who made C-SWEPA (NASA grant NNX13AI75G) possible. This work was also funded EMMREM (grant NNX07AC14G), Sun-2-Ice (NSF grant AGS1135432) projects, DREAM (NASA grant NNX10AB17A), and DREAM2 (NASA grant NNX14AG13A). NR 27 TC 3 Z9 3 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD JUN PY 2014 VL 12 IS 6 BP 323 EP 328 DI 10.1002/2014SW001086 PG 6 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AM0CG UT WOS:000339509900001 ER PT J AU Porter, JA Townsend, LW Spence, H Golightly, M Schwadron, N Kasper, J Case, AW Blake, JB Zeitlin, C AF Porter, Jamie A. Townsend, Lawrence W. Spence, Harlan Golightly, Michael Schwadron, Nathan Kasper, Justin Case, Anthony W. Blake, John B. Zeitlin, Cary TI Radiation environment at the Moon: Comparisons of transport code modeling and measurements from the CRaTER instrument SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID NUCLEAR FRAGMENTATION MODEL; SPECTRUM; SPACE AB The Cosmic Ray Telescope for the Effects of Radiation (CRaTER), an instrument carried on the Lunar Reconnaissance Orbiter spacecraft, directly measures the energy depositions by solar and galactic cosmic radiations in its silicon wafer detectors. These energy depositions are converted to linear energy transfer (LET) spectra. High LET particles, which are mainly high-energy heavy ions found in the incident cosmic ray spectrum, or target fragments and recoils produced by protons and heavier ions, are of particular importance because of their potential to cause significant damage to human tissue and electronic components. Aside from providing LET data useful for space radiation risk analyses for lunar missions, the observed LET spectra can also be used to help validate space radiation transport codes, used for shielding design and risk assessment applications, which is a major thrust of this work. In this work the Monte Carlo transport code HETC-HEDS (High-Energy Transport Code-Human Exploration and Development in Space) is used to estimate LET contributions from the incident primary ions and their charged secondaries produced by nuclear collisions as they pass through the three pairs of silicon detectors. Also in this work, the contributions to the LET of the primary ions and their charged secondaries are analyzed and compared with estimates obtained using the deterministic space radiation code HZETRN 2010, developed at NASA Langley Research Center. LET estimates obtained from the two transport codes are compared with measurements of LET from the CRaTER instrument during the mission. Overall, a comparison of the LET predictions of the HETC-HEDS code to the predictions of the HZETRN code displays good agreement. The code predictions are also in good agreement with the CRaTER LET measurements above 15 keV/mu m but differ from the measurements for smaller values of LET. A possible reason for this disagreement between measured and calculated spectra below 15 keV/mu m is an inadequate representation of the light ion spectra in HETC-HEDS and HZETRN code calculations. It is also clear from the results of this work that Vavilov distributions need to be incorporated into the HETC-HJEDS code before it will be able to recreate the observed LET spectra measured by the CRaTER instrument. C1 [Porter, Jamie A.; Townsend, Lawrence W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. [Spence, Harlan; Golightly, Michael; Schwadron, Nathan] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Kasper, Justin] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Case, Anthony W.] Harvard Smithsonian Ctr Astrophys, Div High Energy Astrophys, Cambridge, MA 02138 USA. [Blake, John B.] Aerosp Corp, El Segundo, CA 90245 USA. [Zeitlin, Cary] Southwest Res Inst, Space & Engn Div, Boulder, CO USA. RP Porter, JA (reprint author), Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. EM jander40@utk.edu RI Kasper, Justin/D-1152-2010 OI Kasper, Justin/0000-0002-7077-930X FU University of Tennessee [11-107]; University of New Hampshire; University of New Hampshire under the NASA CRaTER [NNG11PA03C] FX The CRaTER data for this paper are available for download at http://geo. pds.nasa.gov/missions/lro/. The HETCHEDS and HZETRN data are available upon request from the first author. This work was supported at University of Tennessee under agreement 11-107 with the University of New Hampshire and at the University of New Hampshire under the NASA CRaTER contract NNG11PA03C. The authors wish to thank Joe Mazur of the Aerospace Corporation for his contributions to the early analytical phases of this work. NR 27 TC 0 Z9 0 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD JUN PY 2014 VL 12 IS 6 BP 329 EP 336 DI 10.1002/2013SW000994 PG 8 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AM0CG UT WOS:000339509900002 ER PT J AU Giorgi, JA Lima, MS Vandenberg, NJ AF Giorgi, Jose Adriano Lima, Mauricio Silva Vandenberg, Natalia J. TI THE FIRST RECORD OF BRUMOIDES FOUDRASII (MULSANT) (COLEOPTERA: COCCINELLIDAE: CHILOCORINI) FROM SOUTH AMERICA, WITH NOTES ON ITS BIOLOGY SO COLEOPTERISTS BULLETIN LA English DT Editorial Material ID PSEUDOCOCCIDAE C1 [Giorgi, Jose Adriano] Fed Univ Para, Fac Ciencias Biol, BR-68372040 Altamira, PA, Brazil. [Lima, Mauricio Silva] Univ Fed Rural Pernambuco, Dept Agron, BR-52171900 Recife, PE, Brazil. [Vandenberg, Natalia J.] USDA, Systemat Entomol Lab, ARS, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Giorgi, JA (reprint author), Fed Univ Para, Fac Ciencias Biol, Rua Jose Porfirio 2515, BR-68372040 Altamira, PA, Brazil. EM coccinellid@gmail.com; mauriciosilvadelima@gmail.com; Natalia.Vandenberg@ars.usda.gov NR 12 TC 1 Z9 1 U1 0 U2 0 PU COLEOPTERISTS SOC PI ATHENS PA UNIV GEORGIA, 413 BIOLOGICAL SCIENCES BUILDING, ATHENS, GA 30602-2603 USA SN 0010-065X EI 1938-4394 J9 COLEOPTS BULL JI Coleopt. Bull. PD JUN PY 2014 VL 68 IS 2 BP 336 EP 338 PG 3 WC Entomology SC Entomology GA AL2UY UT WOS:000338982200021 ER PT J AU Weichenthal, S Villeneuve, PJ Burnett, RT van Donkelaar, A Martin, RV Jones, RR DellaValle, CT Sandler, DP Ward, MH Hoppin, JA AF Weichenthal, Scott Villeneuve, Paul J. Burnett, Richard T. van Donkelaar, Aaron Martin, Randall V. Jones, Rena R. DellaValle, Curt T. Sandler, Dale P. Ward, Mary H. Hoppin, Jane A. TI Long-Term Exposure to Fine Particulate Matter: Association with Nonaccidental and Cardiovascular Mortality in the Agricultural Health Study Cohort SO ENVIRONMENTAL HEALTH PERSPECTIVES LA English DT Article ID EXTENDED FOLLOW-UP; HARVARD 6 CITIES; AIR-POLLUTION; DISEASE; RISK AB Background: Few studies have examined the relationship between long-term exposure to ambient fine particulate matter (PM2.5) and nonaccidental mortality in rural populations. Objective: We examined the relationship between PM2.5 and nonaccidental and cardiovascular mortality in the U.S. Agricultural Health Study cohort. Methods: The cohort (n = 83,378) included farmers, their spouses, and commercial pesticide applicators residing primarily in Iowa and North Carolina. Deaths occurring between enrollment (1993-1997) and 30 December 2009 were identified by record linkage. Six-year average (2001-2006) remote-sensing derived estimates of PM2.5 were assigned to participants' residences at enrollment, and Cox proportional hazards models were used to estimate hazard ratios (HR) in relation to a 10-mu g/m(3) increase in PM2.5 adjusted for individual-level covariates. Results: In total, 5,931 nonaccidental and 1,967 cardiovascular deaths occurred over a median follow-up time of 13.9 years. PM2.5 was not associated with nonaccidental mortality in the cohort as a whole (HR = 0.95; 95% CI: 0.76, 1.20), but consistent inverse relationships were observed among women. Positive associations were observed between ambient PM2.5 and cardiovascular mortality among men, and these associations were strongest among men who did not move from their enrollment address (HR = 1.63; 95% 0.94, 2.84). In particular, cardiovascular mortality risk in men was significantly increased when analyses were limited to nonmoving participants with the most precise exposure geocoding (HR = 1.87; 95% CI: 1.04, 3.36). Conclusions: Rural PM2.5 may be associated with cardiovascular mortality in men; however, similar associations were not observed among women. Further evaluation is required to explore these sex differences. C1 [Weichenthal, Scott] Hlth Canada, Air Hlth Sci Div, Ottawa, ON K1A 0K9, Canada. [Weichenthal, Scott] Univ Montreal, Dept Occupat & Environm Hlth, Montreal, PQ, Canada. [Villeneuve, Paul J.; Burnett, Richard T.] Hlth Canada, Populat Studies Div, Ottawa, ON K1A 0K9, Canada. [Villeneuve, Paul J.] Carleton Univ, Inst Hlth Sci Technol & Policy, Ottawa, ON K1S 5B6, Canada. [van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jones, Rena R.; DellaValle, Curt T.; Ward, Mary H.] NCI, Occupat & Environm Epidemiol Branch, Div Canc Epidemiol & Genet, NIH, Bethesda, MD 20892 USA. [Sandler, Dale P.; Hoppin, Jane A.] NIEHS, Epidemiol Branch, NIH, US Dept HHS, Res Triangle Pk, NC 27709 USA. RP Weichenthal, S (reprint author), Hlth Canada, 269 Laurier Ave West,AL 4903C, Ottawa, ON K1A 0K9, Canada. EM scott.weichenthal@hc-sc.gc.ca RI Martin, Randall/C-1205-2014; OI Martin, Randall/0000-0003-2632-8402; Sandler, Dale/0000-0002-6776-0018 FU Health Canada; Intramural Research Program of the National Institutes of Health; National Institute of Environmental Health Sciences [Z01-ES025041]; National Cancer Institute [Z01-CP010119]; Natural Sciences and Engineering Research Council (NSERC) FX This work was supported by Health Canada and the Intramural Research Program of the National Institutes of Health, National Institute of Environmental Health Sciences (Z01-ES025041) and National Cancer Institute (Z01-CP010119). R.M. and A.v.D. were supported by Health Canada and the Natural Sciences and Engineering Research Council (NSERC). NR 30 TC 23 Z9 26 U1 4 U2 35 PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE PI RES TRIANGLE PK PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233, RES TRIANGLE PK, NC 27709-2233 USA SN 0091-6765 EI 1552-9924 J9 ENVIRON HEALTH PERSP JI Environ. Health Perspect. PD JUN PY 2014 VL 122 IS 6 BP 609 EP 615 DI 10.1289/ehp.1307277 PG 7 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA AL1ZW UT WOS:000338926500024 PM 24633320 ER PT J AU Schwartz, DA AF Schwartz, Daniel A. TI Invited Review Article: The Chandra X-ray Observatory SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Review ID CCD IMAGING SPECTROMETER; HIGH-RESOLUTION CAMERA; TRANSMISSION GRATING SPECTROMETER; FLIGHT CONTAMINATION MONITOR; CHARGE-TRANSFER INEFFICIENCY; ASTROPHYSICS FACILITY AXAF; IRIDIUM OPTICAL-CONSTANTS; ACTIVE GALACTIC NUCLEI; REFLECTANCE MEASUREMENTS; SUPERNOVA REMNANT AB The Chandra X-ray Observatory is an orbiting x-ray telescope facility. It is one of the National Aeronautics and Space Administration's four "Great Observatories" that collectively have carried out astronomical observations covering the infrared through gamma-ray portion of the electromagnetic spectrum. Chandra is used by astronomers world-wide to acquire imaging and spectroscopic data over a nominal 0.1-10 keV (124-1.24 angstrom) range. We describe the three major parts of the observatory: the telescope, the spacecraft systems, and the science instruments. This article will emphasize features of the design and development driven by some of the experimental considerations unique to x-ray astronomy. We will update the on-orbit performance and present examples of the scientific highlights. (C) 2014 AIP Publishing LLC. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Schwartz, DA (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM das@cfa.harvard.edu FU NASA MSFC [NAS8-03060] FX The Chandra Observatory is the result of Riccardo Giacconi's vision for x-ray astronomy. The director of the Chandra X-ray Center, Harvey Tananbaum, and the MSFC Project Scientist, Martin Weisskopf, are most responsible for uniting the scientific community, NASA, and the principle contractors into the team supporting and implementing this mission. The exquisite quality of the Chandra images is due largely to the telescope scientist, the late Leon VanSpeybroeck. The astronomical community owes a great debt to more than a thousand people at NASA, Northrop Grumman and its subcontractors, and SAO, and to the instrument developers at SAO, MIT, PSU, the Max-Planck Institut fur extraterrestrische Physik (MPE), and the Space Research Institute of the Netherlands (SRON) who worked on the AXAF (now Chandra) project. This review has benefited from information and material originally prepared by the NASA/MSFC Project Science team, the SAO mission support team, the Chandra X-ray Observatory Center, and the Northrop Grumman development and flight operations teams. This research has made use of NASA's Astrophysics Data System Bibliographic Services. The Chandra X-ray Observatory is operated by SAO under Contract No. NAS8-03060 from the NASA MSFC. Reference herein to any specific commercial product, process, or service by trade name, trademark, or manufacturer, or otherwise does not constitute or imply its endorsement by NASA or SAO. NR 132 TC 4 Z9 4 U1 1 U2 3 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 2014 VL 85 IS 6 AR 061101 DI 10.1063/1.4881695 PG 40 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA AL3FB UT WOS:000339010500001 PM 24985792 ER PT J AU Hershler, R Landye, JJ Liu, HP De la Maza-Benignos, M Ornelas, P Carson, EW AF Hershler, Robert Landye, J. Jerry Liu, Hsiu-Ping De la Maza-Benignos, Mauricio Ornelas, Pavel Carson, Evan W. TI NEW SPECIES AND RECORDS OF CHIHUAHUAN DESERT SPRINGSNAILS, WITH A NEW COMBINATION FOR TRYONIA BRUNEI SO WESTERN NORTH AMERICAN NATURALIST LA English DT Article ID NORTH-AMERICAN SOUTHWEST; PHYLOGENETIC-RELATIONSHIPS; GASTROPODS RISSOOIDEA; BIOGEOGRAPHY; HYDROBIIDAE; MEXICO; GENUS AB This is the last in a series of papers clarifying the taxonomy of a critically imperiled assemblage of Cochliopid gastropods (Tryonia sensu lato) that inhibit thermal springs in the Chihuahuan Desert (Mexico and United States). We describe 2 new narrowly endemic species of Tryonia from Chihuahua, both of which appear to have been recently,extirpated, and we provide new records for 4 congeners (also from Chihuahua) and for a species of Pseudotryonia (from Durango). The 2 new species of Tryonia differ from closely similar regional congeners in shell and penial characters. On the basis of new anatomical data, we also transfer T brunet Taylor, 1987 to the genus Juttamia and provide evidence that this species, which was endemic to the Phantom Lake spring complex in west Texas, became extinct sometime after 1984. Our findings provide additional insight into the complex biogeographic history of the Chihuahuan Desert cochliopids and further document the recent decline of regional spring-dwelling biota as a result of groundwater mining. C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Liu, Hsiu-Ping] Metropolitan State Univ Denver, Dept Biol, Denver, CO 80217 USA. [De la Maza-Benignos, Mauricio; Ornelas, Pavel] Pronatuia Noreste AC, Monterrey 64710, NL, Mexico. [Carson, Evan W.] Univ New Mexico, Dept Biol & Museum Southwestern Biol, Albuquerque, NM 87131 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Box 37012,NHB W-305,MRC 163, Washington, DC 20013 USA. EM hershlerr@si.edu FU National Science Foundation [GB-6477x]; Secretaria de Industria y Cornercio [5803] FX JJEs early collections were made under the auspices of a National Science Foundation grant to W.L. Minckley (GB-6477x) and a collecting permit from the Secretaria de Industria y Cornercio (#5803). More recent fieldwork was supported by awards (to RH) from the Smithsonian Biodiversity Program; collecting permits were provided by La Secretaria de Relaciones Exteriores (DAN 01874, 03358) and facilitated by Angelica Narvaez (U.S. Embassy Mexico City, Office of Environment, Science and Technology Affairs) We thank Andrew Simons and Jonathan Slaght (BellMNH) and Artie L. Metcalf (UTEP) for loans of material under their care, and Douglas Nelson (UMMZ) for providing copies of Robert Rush Miller's field notes. Various individuals assisted with fieldwork, including Phil Hines, William G. Kepner, Sandra Tyler Landye, Charles 0. Minckley, Saundra King Mincldey, W.L. Minckley, Donna Portz, Dwight W. Taylor, Sandra Willoughby, and Darrell Wong. Yolanda Villacampa measured shells and prepared scanning electron micrographs, and Karolyn Darrow inked the anatomical drawings. The DigitalGlobe satellite image of the Julimes area was purchased from Digital Data Services, Inc. (Lakewood, CO). NR 29 TC 2 Z9 2 U1 0 U2 6 PU BRIGHAM YOUNG UNIV PI PROVO PA 290 LIFE SCIENCE MUSEUM, PROVO, UT 84602 USA SN 1527-0904 EI 1944-8341 J9 WEST N AM NATURALIST JI West. North Am. Naturalist PD JUN PY 2014 VL 74 IS 1 BP 47 EP 65 PG 19 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AL2QO UT WOS:000338970400004 ER PT J AU Ims, JJ Sofaer, HR Sillett, TS Ghalambor, CK AF Ims, Jessica J. Sofaer, Helen R. Sillett, T. Scott Ghalambor, Cameron K. TI TEMPERATURE DOES NOT AFFECT THE TIMING OF FIRST NEST DEPARTURE IN ORANGE-CROWNED WARBLERS SO WESTERN NORTH AMERICAN NATURALIST LA English DT Article ID DAILY ROOSTING TIMES; INCUBATION BEHAVIOR; LATITUDINAL VARIATION; AMBIENT-TEMPERATURE; STURNUS-VULGARIS; BREEDING-SEASON; EGG TEMPERATURE; PREDATION RISK; ENERGETIC COST; TREE SWALLOWS AB Acr. Organisms often respond to variation in temperature by altering their behavior, but the sensitivity of each behavioral trait depends on the degree to which temperature affects its costs and benefits. Here, we tested whether a little-studied trait, the timing of the first nest departure in the morning, varied in response to ambient temperature at sunrise, sunrise time, and nesting stage (incubation vs. nestling) in female Orange-crowned Warblers breeding on Santa Catalina Island, California. We found that the time of first nest departure was significantly correlated with sunrise time but was not affected by ambient temperature at sunrise. Compared with the nestling period, first nest departure times tended to be later and more variable during incubation, but the causes of these patterns remain to be explored in future studies of avian early-morning behavior C1 [Ims, Jessica J.; Sofaer, Helen R.; Ghalambor, Cameron K.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Sofaer, Helen R.; Ghalambor, Cameron K.] Colorado State Univ, Grad Degree Program Ecol, Ft Collins, CO 80523 USA. [Sillett, T. Scott] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. RP Sofaer, HR (reprint author), Colorado State Univ, Dept Fish Wildlife & Conservat Biol, 1474 Campus Delivery, Ft Collins, CO 80523 USA. FU Nature Conservancy, the Smithsonian Institution; American Ornithologists' Union Graduate Research Award; Frank M. Chapman Memorial Grant from the American Museum of Natural History FX This work was supported by The Nature Conservancy, the Smithsonian Institution, an American Ornithologists' Union Graduate Research Award (HRS), and a Frank M. Chapman Memorial Grant from the American Museum of Natural History (HRS). Logistical support was provided by the Catalina Island Conservancy. We appreciate the field assistants who assisted with data collection and the undergraduate students who transcribed our nest videos. Comments from 2 anonymotth reviewers improved this manuscript. NR 41 TC 0 Z9 0 U1 2 U2 6 PU BRIGHAM YOUNG UNIV PI PROVO PA 290 LIFE SCIENCE MUSEUM, PROVO, UT 84602 USA SN 1527-0904 EI 1944-8341 J9 WEST N AM NATURALIST JI West. North Am. Naturalist PD JUN PY 2014 VL 74 IS 1 BP 66 EP 70 PG 5 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AL2QO UT WOS:000338970400005 ER PT J AU Hollister, LS Bindi, L Yao, N Poirier, GR Andronicos, CL MacPherson, GJ Lin, C Distler, VV Eddy, MP Kostin, A Kryachko, V Steinhardt, WM Yudovskaya, M Eiler, JM Guan, YB Clarke, JJ Steinhardt, PJ AF Hollister, Lincoln S. Bindi, Luca Yao, Nan Poirier, Gerald R. Andronicos, Christopher L. MacPherson, Glenn J. Lin, Chaney Distler, Vadim V. Eddy, Michael P. Kostin, Alexander Kryachko, Valery Steinhardt, William M. Yudovskaya, Marina Eiler, John M. Guan, Yunbin Clarke, Jamil J. Steinhardt, Paul J. TI Impact-induced shock and the formation of natural quasicrystals in the early solar system SO NATURE COMMUNICATIONS LA English DT Article ID FORMING ALLOY SYSTEM; PHASE-EQUILIBRIA; ORDINARY CHONDRITES; SOLIDIFICATION; METAMORPHISM; METEORITES; DIAGRAM; COPPER AB The discovery of a natural quasicrystal, icosahedrite (Al63Cu24Fe13), accompanied by khatyrkite (CuAl2) and cupalite (CuAl) in the CV3 carbonaceous chondrite Khatyrka has posed a mystery as to what extraterrestrial processes led to the formation and preservation of these metal alloys. Here we present a range of evidence, including the discovery of high-pressure phases never observed before in a CV3 chondrite, indicating that an impact shock generated a heterogeneous distribution of pressures and temperatures in which some portions reached at least 5GPa and 1,200 degrees C. The conditions were sufficient to melt Al-Cu-bearing minerals, which then rapidly solidified into icosahedrite and other Al-Cu metal phases. The meteorite also contains heretofore unobserved phases of iron-nickel and iron sulphide with substantial amounts of Al and Cu. The presence of these phases in Khatyrka provides further proof that the Al-Cu alloys are natural products of unusual processes that occurred in the early solar system. C1 [Hollister, Lincoln S.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Bindi, Luca] Univ Florence, Dipartimento Sci Terra, I-50121 Florence, Italy. [Yao, Nan; Poirier, Gerald R.] Princeton Univ, Princeton Inst Sci & Technol Mat, Princeton, NJ 08544 USA. [Andronicos, Christopher L.] Purdue Univ, Div Earth & Atmospher Sci, W Lafayette, IN 47907 USA. [MacPherson, Glenn J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20013 USA. [Lin, Chaney; Steinhardt, Paul J.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Distler, Vadim V.; Kryachko, Valery; Yudovskaya, Marina] Russian Acad Sci, Inst Geol Ore Deposits Petrog Mineral & Geochem I, Moscow 119017, Russia. [Eddy, Michael P.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Kostin, Alexander] BHP Billiton, Geosci Technol, Houston, TX 77056 USA. [Steinhardt, William M.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Eiler, John M.; Guan, Yunbin] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Clarke, Jamil J.] Hitachi High Technol Amer Inc, Gaithersburg, MD 20878 USA. [Steinhardt, Paul J.] Princeton Univ, Princeton Ctr Theoret Sci, Princeton, NJ 08544 USA. RP Steinhardt, PJ (reprint author), Princeton Univ, Dept Phys, Jadwin Hall, Princeton, NJ 08544 USA. EM steinh@princeton.edu RI Yudovskaya, Marina/K-3980-2013 FU National Science Foundation-MRSEC program through New York University [DMR-0820341]; Princeton Center for Complex Materials [DMR-0819860]; NASA [NNX11AD43G] FX L.B. thanks M.I.U.R., P.R.I.N. 2009 project 'Structure, microstructure and properties of minerals', the 'MEMA', Centro di Microscopia Elettronica e Microanalisi, Florence, Italy, and 'CRIST', Centro di Cristallografia Strutturale, Sesto Fiorentino, Florence, Italy. This work was supported in part by the National Science Foundation-MRSEC program through New York University (DMR-0820341; P.J.S.), through the Princeton Center for Complex Materials (DMR-0819860; N.Y.) and NASA grant NNX11AD43G (G.J.M.). The expedition to Chukotka was supported by a grant from an anonymous donor to Princeton University (P.J.S., Principal Investigator). NR 27 TC 7 Z9 7 U1 4 U2 36 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD JUN PY 2014 VL 5 AR 4040 DI 10.1038/ncomms5040 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AL0SR UT WOS:000338837600002 PM 24925481 ER PT J AU Mueller, T Dressler, G Tucker, CJ Pinzon, JE Leimgruber, P Dubayah, RO Hurtt, GC Bohning-Gaese, K Fagan, WF AF Mueller, Thomas Dressler, Gunnar Tucker, Compton J. Pinzon, Jorge E. Leimgruber, Peter Dubayah, Ralph O. Hurtt, George C. Boehning-Gaese, Katrin Fagan, William F. TI Human Land-Use Practices Lead to Global Long-Term Increases in Photosynthetic Capacity SO REMOTE SENSING LA English DT Article DE NDVI; land-use; anthropogenic biomes; anthromes; global change; GIMMS3g ID NDVI DATA SETS; TIME-SERIES; VEGETATION INDEX; SATELLITE DATA; SOUTH-AMERICA; TRENDS; MODIS; CLIMATE; COVER; PRODUCTIVITY AB Long-term trends in photosynthetic capacity measured with the satellite-derived Normalized Difference Vegetation Index (NDVI) are usually associated with climate change. Human impacts on the global land surface are typically not accounted for. Here, we provide the first global analysis quantifying the effect of the earth's human footprint on NDVI trends. Globally, more than 20% of the variability in NDVI trends was explained by anthropogenic factors such as land use, nitrogen fertilization, and irrigation. Intensely used land classes, such as villages, showed the greatest rates of increase in NDVI, more than twice than those of forests. These findings reveal that factors beyond climate influence global long-term trends in NDVI and suggest that global climate change models and analyses of primary productivity should incorporate land use effects. C1 [Mueller, Thomas; Fagan, William F.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Mueller, Thomas; Boehning-Gaese, Katrin] Senckenberg Gesell Nat Forsch, Biodivers & Climate Res Ctr, D-60325 Frankfurt, Germany. [Mueller, Thomas; Boehning-Gaese, Katrin] Goethe Univ Frankfurt, Dept Biol Sci, D-60438 Frankfurt, Germany. [Mueller, Thomas; Leimgruber, Peter] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Dressler, Gunnar] UFZ Helmholtz Ctr Environm Res, Dept Ecol Modeling, D-04318 Leipzig, Germany. [Tucker, Compton J.; Pinzon, Jorge E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dubayah, Ralph O.; Hurtt, George C.] Univ Maryland, Dept Geog Sci, College Pk, MD 20771 USA. [Hurtt, George C.; Fagan, William F.] Natl Socioenvironm Synth Ctr SESYNC, Annapolis, MD 21401 USA. RP Mueller, T (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA. EM muellert@gmail.com; gunnar.dressler@gmail.com; compton.j.tucker@nasa.gov; jorge.e.pinzon@nasa.gov; leimgruberp@si.edu; dubayah@umd.edu; gchurtt@umd.edu; katrin.boehning-gaese@senckenberg.de; bfagan@umd.edu RI Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 FU NSF ABI [1062411]; Robert Bosch Foundation; National Socio-Environmental Synthesis Center (SESYNC) - National Science Foundation [DBI-1052875] FX WFF and TM were supported by NSF ABI award 1062411 and TM was supported by the Robert Bosch Foundation. This work was also supported by the National Socio-Environmental Synthesis Center (SESYNC) under funding received from the National Science Foundation DBI-1052875. NR 45 TC 8 Z9 8 U1 1 U2 13 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD JUN PY 2014 VL 6 IS 6 BP 5717 EP 5731 DI 10.3390/rs6065717 PG 15 WC Remote Sensing SC Remote Sensing GA AK9RB UT WOS:000338763300048 ER PT J AU Bartalucci, I Mazzotta, P Bourdin, H Vikhlinin, A AF Bartalucci, I. Mazzotta, P. Bourdin, H. Vikhlinin, A. TI Chandra ACIS-I particle background: an analytical model SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; instrumentation: detectors; X-rays: general ID DEEP FIELD-SOUTH; X-RAY; XMM-NEWTON AB Aims. Imaging and spectroscopy of X-ray extended sources require a proper characterisation of a spatially unresolved background signal. This background includes sky and instrumental components, each of which are characterised by its proper spatial and spectral behaviour. While the X-ray sky background has been extensively studied in previous work, here we analyse and model the instrumental background of the ACIS-I detector on board the Chandra X-ray observatory in very faint mode. Methods. Caused by interaction of highly energetic particles with the detector, the ACIS-I instrumental background is spectrally characterised by the superimposition of several fluorescence emission lines onto a continuum. To isolate its flux from any sky component, we fitted an analytical model of the continuum to observations performed in very faint mode with the detector in the stowed position shielded from the sky, and gathered over the eight-year period starting in 2001. The remaining emission lines were fitted to blank-sky observations of the same period. We found 11 emission lines. Analysing the spatial variation of the amplitude, energy and width of these lines has further allowed us to infer that three lines of these are presumably due to an energy correction artefact produced in the frame store. Results. We provide an analytical model that predicts the instrumental background with a precision of 2% in the continuum and 5% in the lines. We use this model to measure the flux of the unresolved cosmic X-ray background in the Chandra deep field south. We obtain a flux of 10.2(-0.4)(+0.5) x 10(-13) erg cm(-2) deg(-2) s(-1) for the [1-2] keV band and (3.8 +/- 0.2) x 10(-12) erg cm(-2) deg(-2) s(-1) for the [2-8] keV band. C1 [Bartalucci, I.; Mazzotta, P.; Bourdin, H.] Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy. [Mazzotta, P.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bartalucci, I (reprint author), Univ Roma Tor Vergata, Dept Phys, Via Ric Sci 1, I-00133 Rome, Italy. EM bartalucci@roma2.infn.it RI Mazzotta, Pasquale/B-1225-2016 OI Mazzotta, Pasquale/0000-0002-5411-1748 FU PRIN-INAF; ASI-INAF [I/009/10/0]; NASA [G02-13153X, MNX14AC22G] FX We thank Maxim Markevitch and the anonymous referee for their comments and suggestions, which significantly improved the quality of the paper. I.B. thanks the Harvard-Smithsonian Centre for Astrophysics, where this work was initiated, for its hospitality. I.B., P.M., and H.B. acknowledge support by grants PRIN-INAF2013 and ASI-INAF I/009/10/0. P.M. acknowledge support by NASA grants G02-13153X and MNX14AC22G. NR 14 TC 12 Z9 12 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR A25 DI 10.1051/0004-6361/201423443 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500098 ER PT J AU Iacobelli, M Burkhart, B Haverkorn, M Lazarian, A Carretti, E Staveley-Smith, L Gaensler, BM Bernardi, G Kesteven, MJ Poppi, S AF Iacobelli, M. Burkhart, B. Haverkorn, M. Lazarian, A. Carretti, E. Staveley-Smith, L. Gaensler, B. M. Bernardi, G. Kesteven, M. J. Poppi, S. TI Galactic interstellar turbulence across the southern sky seen through spatial gradients of the polarization vector SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: general; ISM: magnetic fields; ISM: structure; radio lines: general; radio continuum: ISM ID RADIO-CONTINUUM SURVEY; LINEAR-POLARIZATION; MILKY-WAY; VERTICAL STRUCTURE; MAGNETIC-FIELDS; STAR-FORMATION; FREE-ELECTRONS; INNER GALAXY; IONIZED-GAS; OUTER SCALE AB Aims. Radio synchrotron polarization maps of the Galaxy can be used to infer the properties of interstellar turbulence in the diffuse magneto-ionic medium (MIM). In this paper, we investigate the normalized spatial gradient of linearly polarized synchrotron emission (vertical bar del P vertical bar/vertical bar P vertical bar) as a tracer of turbulence, the relationship of the gradient to the sonic Mach number of the MIM, and changes in morphology of the gradient as a function of Galactic position in the southern sky. Methods. We used data from the S-band Polarization All Sky Survey (S-PASS) to image the normalized spatial gradient of the linearly polarized synchrotron emission (vertical bar del P vertical bar/vertical bar P vertical bar) in the entire southern sky at 2.3 GHz. The spatial gradient of linear polarization reveals rapid changes in the density and magnetic fluctuations in the MIM due to magnetic turbulence as a function of Galactic position. We made comparisons of these data to ideal MHD numerical simulations. To constrain the sonic Mach number (M-s), we applied a high-order moments analysis to the observations and to the simulated diffuse, isothermal ISM with ideal magneto-hydrodynamic turbulence. Results. We find that polarization gradient maps reveal elongated structures, which we associate with turbulence in the MIM. Our analysis indicates that turbulent MIM is in a generally transonic regime. This result for the turbulent regime is more general than the ones deduced by the analysis of electron density variation data, because it is based on the stochastic imprints of the Faraday rotation effect, which is also sensitive to the magnetic field fluctuations. Filamentary structures are seen with typical widths down to the angular resolution, and the observed morphologies closely match numerical simulations and, in some cases, H alpha contours. The vertical bar del P vertical bar/vertical bar P vertical bar intensity is found to be approximately log-normal distributed. No systematic variations in the sonic Mach number are observed as a function of Galactic coordinates, which is consistent with turbulence in the WIM, as inferred by the analysis of H alpha data. We conclude that the sonic Mach number of the diffuse MIM appears to be spatially uniform towards the Galactic plane and the Sagittarius-Carina arm, but local variations induced by nearby extended objects are also found. C1 [Iacobelli, M.; Haverkorn, M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Iacobelli, M.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Haverkorn, M.] Radboud Univ Nijmegen, NL-6525 AJ Nijmegen, Netherlands. [Burkhart, B.; Lazarian, A.] Univ Wisconsin, Dept Astron, Madison, WI 53711 USA. [Carretti, E.; Kesteven, M. J.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Staveley-Smith, L.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Staveley-Smith, L.] CAASTRO ARC Ctr Excellence All Sky Astrophys, Sydney, NSW, Australia. [Gaensler, B. M.] Univ Sydney, Sch Phys A29, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Poppi, S.] INAF Osservatorio Astron Cagliari, I-09047 Selargius, Italy. RP Iacobelli, M (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM iacobelli@strw.leidenuniv.nl RI Staveley-Smith, Lister/A-1683-2011; OI Staveley-Smith, Lister/0000-0002-8057-0294; Carretti, Ettore/0000-0002-3973-8403; Poppi, Sergio/0000-0002-4698-2607; Gaensler, Bryan/0000-0002-3382-9558 FU European Union [239490]; Netherlands Organization for Scientific Research (NWO) [639.042.915]; NSF [AST 1212096]; Center for Magnetic Self-Organization in Laboratory and Astrophysical Plasmas (CMSO); Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; Australian Research Council through an Australian Laureate Fellowship [FL100100114]; Commonwealth of Australia FX The authors thank the referee, Steven Spangler, for providing detailed comments and helpful suggestions in the preparation of the final manuscript. This work has been carried out in the framework of the S-band Polarisation All Sky Survey collaboration (S-PASS). The Parkes Radio Telescope is part of the Australia Telescope National Facility, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The research leading to these results has received funding from the European Union's Seventh Framework Programme (FP7/2007-2013) under grant agreement number 239490. This work is part of the research programme 639.042.915; which is (partly) financed by the Netherlands Organization for Scientific Research (NWO). Support for B.B. and A.L. comes from the NSF grant AST 1212096, and the Center for Magnetic Self-Organization in Laboratory and Astrophysical Plasmas (CMSO). B.B. acknowledges Vilas Associate Awards and the hospitality of the International Institute of Physics (Natal). Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. B.M.G. acknowledges support from the Australian Research Council through an Australian Laureate Fellowship (FL100100114). NR 81 TC 11 Z9 11 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR A5 DI 10.1051/0004-6361/201322982 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500050 ER PT J AU Kim, DW Protopapas, P Bailer-Jones, CAL Byun, YI Chang, SW Marquette, JB Shin, MS AF Kim, Dae-Won Protopapas, Pavlos Bailer-Jones, Coryn A. L. Byun, Yong-Ik Chang, Seo-Won Marquette, Jean-Baptiste Shin, Min-Su TI The EPOCH Project I. Periodic variable stars in the EROS-2 LMC database SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: variables: general; Magellanic Clouds; methods: data analysis ID LARGE-MAGELLANIC-CLOUD; GRAVITATIONAL LENSING EXPERIMENT.; OGLE-III CATALOG; HUBBLE-SPACE-TELESCOPE; R-CORONAE-BOREALIS; TIME-SERIES DATA; DETECTING VARIABILITY; MACHO PROJECT; LYRAE STARS; CANDIDATES AB The EPOCH (EROS-2 periodic variable star classification using machine learning) project aims to detect periodic variable stars in the EROS-2 light curve database. In this paper, we present the first result of the classification of periodic variable stars in the EROS-2 LMC database. To classify these variables, we first built a training set by compiling known variables in the Large Magellanic Cloud area from the OGLE and MACHO surveys. We crossmatched these variables with the EROS-2 sources and extracted 22 variability features from 28 392 light curves of the corresponding EROS-2 sources. We then used the random forest method to classify the EROS-2 sources in the training set. We designed the model to separate not only delta Scuti stars, RR Lyraes, Cepheids, eclipsing binaries, and long-period variables, the superclasses, but also their subclasses, such as RRab, RRc, RRd, and RRe for RR Lyraes, and similarly for the other variable types. The model trained using only the superclasses shows 99% recall and precision, while the model trained on all subclasses shows 87% recall and precision. We applied the trained model to the entire EROS-2 LMC database, which contains about 29 million sources, and found 117 234 periodic variable candidates. Out of these 117 234 periodic variables, 55 285 have not been discovered by either OGLE or MACHO variability studies. This set comprises 1906 delta Scuti stars, 6607 RR Lyraes, 638 Cepheids, 178 Type II Cepheids, 34 562 eclipsing binaries, and 11 394 long-period variables. C1 [Kim, Dae-Won; Bailer-Jones, Coryn A. L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Protopapas, Pavlos] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Byun, Yong-Ik; Chang, Seo-Won] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Byun, Yong-Ik; Chang, Seo-Won] Yonsei Univ, Univ Observ, Seoul 120749, South Korea. [Marquette, Jean-Baptiste] Inst Astrophys, UPMC CNRS, UMR7095, F-75014 Paris, France. [Shin, Min-Su] Univ Oxford, Dept Phys, Oxford OX1 3PU, England. RP Kim, DW (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM kim@mpia.de FU CEA; CNRS through the IN2P3 institute; CNRS through the INSU institute; "Programme National de Physique Stellaire" (PNPS) of the CNRS/INSU, France; NRF [2012R1A1A2006924] FX The EROS-2 project was funded by the CEA and the CNRS through the IN2P3 and INSU institutes. J.B.M. acknowledges financial support from "Programme National de Physique Stellaire" (PNPS) of the CNRS/INSU, France. Work at Yonsei was supported by NRF grant 2012R1A1A2006924. The analysis in this paper has been performed using the Odyssey cluster supported by the FAS Research Computing Group at Harvard. NR 56 TC 13 Z9 13 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR A43 DI 10.1051/0004-6361/201323252 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500071 ER PT J AU Lombardi, M Bouy, H Alves, J Lada, CJ AF Lombardi, Marco Bouy, Herve Alves, Joao Lada, Charles J. TI Herschel-Planck dust optical-depth and column-density maps I. Method description and results for Orion SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; dust, extinction; ISM: structure; ISM: individual objects: Orion molecular cloud ID FIELD EXTINCTION MAPS; NEAR-INFRARED OBSERVATIONS; MOLECULAR CLOUDS; NEBULA CLUSTER; STAR-FORMATION; SUPERSONIC TURBULENCE; INTERSTELLAR DUST; TRAPEZIUM CLUSTER; SIZE DISTRIBUTION; BURNING LIMIT AB We present high-resolution, high dynamic range column-density and color-temperature maps of the Orion complex using a combination of Planck dust-emission maps, Herschel dust-emission maps, and 2MASS NIR dust-extinction maps. The column-density maps combine the robustness of the 2MASS NIR extinction maps with the resolution and coverage of the Herschel and Planck dust-emission maps and constitute the highest dynamic range column-density maps ever constructed for the entire Orion complex, covering 0.01 mag < A(K) < 30 mag, or 2 x 10(20) cm(-2) < N < 5 x 10(23) cm(-2). We determined the ratio of the 2.2 mu m extinction coefficient to the 850 mu m opacity and found that the values obtained for both Orion A and B are significantly lower than the predictions of standard dust models, but agree with newer models that incorporate icy silicate-graphite conglomerates for the grain population. We show that the cloud projected probability distribution function, over a large range of column densities, can be well fitted by a simple power law. Moreover, we considered the local Schmidt-law for star formation, and confirm earlier results, showing that the protostar surface density Sigma(*) follows a simple law Sigma(*) proportional to Sigma(beta)(gas), with beta similar to 2. C1 [Lombardi, Marco] Univ Milan, Dept Phys, I-20133 Milan, Italy. [Bouy, Herve] INTA CSIC, Ctr Astrobiol, Madrid 28691, Spain. [Alves, Joao] Univ Vienna, A-1180 Vienna, Austria. [Lombardi, Marco; Lada, Charles J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lombardi, M (reprint author), Univ Milan, Dept Phys, Via Celoria 16, I-20133 Milan, Italy. EM marco.lombardi@unimi.it RI Bouy, Herve/H-2913-2012; OI Bouy, Herve/0000-0002-7084-487X; LOMBARDI, MARCO/0000-0002-3336-4965; Alves, Joao/0000-0002-4355-0921 FU ESA Member States; NASA; Ramon y Cajal fellowship program [RYC-2009-04497]; Faculty of the European Space Astronomy Centre (ESAC) FX 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. We are grateful to H. Roussel for her help with Scanamorphos. H. Bouy is funded by the Ramon y Cajal fellowship program number RYC-2009-04497. J. Alves acknowledges support from the Faculty of the European Space Astronomy Centre (ESAC). NR 66 TC 39 Z9 39 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR A45 DI 10.1051/0004-6361/201323293 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500075 ER PT J AU Santos, NC Mortier, A Faria, JP Dumusque, X Adibekyan, VZ Delgado-Mena, E Figueira, P Benamati, L Boisse, I Cunha, D da Silva, JG Lo Curto, G Lovis, C Martins, JHC Mayor, M Melo, C Oshagh, M Pepe, F Queloz, D Santerne, A Segransan, D Sozzetti, A Sousa, SG Udry, S AF Santos, N. C. Mortier, A. Faria, J. P. Dumusque, X. Adibekyan, V. Zh. Delgado-Mena, E. Figueira, P. Benamati, L. Boisse, I. Cunha, D. da Silva, J. Gomes Lo Curto, G. Lovis, C. Martins, J. H. C. Mayor, M. Melo, C. Oshagh, M. Pepe, F. Queloz, D. Santerne, A. Segransan, D. Sozzetti, A. Sousa, S. G. Udry, S. TI The HARPS search for southern extra-solar planets XXXV. The interesting case of HD 41248: stellar activity, no planets? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; stars: individual: HD 41248; stars: solar-type; stars: activity; stars: abundances surveys ID METAL-POOR STARS; DIFFERENTIAL ROTATION; GIANT PLANETS; BOLOMETRIC CORRECTIONS; MAGNETIC CYCLES; CORALIE SURVEY; HOT-JUPITER; MASS; METALLICITY; EXOPLANETS AB Context. The search for planets orbiting metal-poor stars is of utmost importance for our understanding of planet formation models. However, no dedicated searches have been conducted so far for very low mass planets orbiting such objects. Only a few cases of low-mass planets orbiting metal-poor stars are thus known. Amongst these, HD 41248 is a metal-poor, solar-type star on the orbit of which a resonant pair of super-Earth-like planets has been announced. This detection was based on 62 radial velocity measurements obtained with the HARPS spectrograph (public data). Aims. We present a new planet search program that is using the HARPS spectrograph to search for Neptunes and super-Earths that orbit a sample of metal-poor FGK dwarfs. We then present a detailed analysis of 162 additional radial velocity measurements of HD 41248, obtained within this program, with the goal of confirming the existence of the proposed planetary system. Methods. We analysed the precise radial velocities, obtained with the HARPS spectrograph, together with several stellar activity diagnostics and line profile indicators. Results. A careful analysis shows no evidence for the planetary system. One of the signals, with a period of similar to 25 days, is shown to be related to the rotational period of the star, and is clearly seen in some of the activity proxies. We were unable to convincingly retrieve the remaining signal (P similar to 18 days) in the new dataset. Conclusions. We discuss possible causes for the complex (evolving) signals observed in the data of HD 41248, proposing that they might be explained by the appearance and disappearance of active regions on the surface of a star with strong differential rotation, or by a combination of the sparse data sampling and active region evolution. C1 [Santos, N. C.; Mortier, A.; Faria, J. P.; Adibekyan, V. Zh.; Delgado-Mena, E.; Figueira, P.; Benamati, L.; Cunha, D.; da Silva, J. Gomes; Martins, J. H. C.; Oshagh, M.; Santerne, A.; Sousa, S. G.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Santos, N. C.; Faria, J. P.; Benamati, L.; Cunha, D.; da Silva, J. Gomes; Martins, J. H. C.; Oshagh, M.; Sousa, S. G.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4169007 Oporto, Portugal. [Dumusque, X.; Lovis, C.; Mayor, M.; Pepe, F.; Queloz, D.; Segransan, D.; Udry, S.] Univ Geneva, Observ Geneve, CH-1290 Sauverny, Switzerland. [Dumusque, X.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lo Curto, G.; Melo, C.] European So Observ, Santiago, Chile. [Sousa, S. G.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Sozzetti, A.] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, Italy. [Boisse, I.] Aix Marseille Univ, CNRS, LAM Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. [Queloz, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Santos, NC (reprint author), Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Oporto, Portugal. EM nuno@astro.up.pt RI Santos, Nuno/E-9957-2011; Cunha, Diana/B-1274-2011; Figueira, Pedro/J-4916-2013; Sousa, Sergio/I-7466-2013; Delgado Mena, Elisa/M-9178-2013; Melo, Claudio/O-2797-2013; Adibekyan, Vardan/I-5026-2013; OI Sozzetti, Alessandro/0000-0002-7504-365X; Santos, Nuno/0000-0003-4422-2919; Santerne, Alexandre/0000-0002-3586-1316; Mortier, Annelies/0000-0001-7254-4363; Cunha, Diana/0000-0002-6775-0493; Figueira, Pedro/0000-0001-8504-283X; Sousa, Sergio/0000-0001-9047-2965; Delgado Mena, Elisa/0000-0003-4434-2195; Oshagh, Mahmoudreza/0000-0002-0715-8789; Faria, Joao/0000-0002-6728-244X; Adibekyan, Vardan/0000-0002-0601-6199; Melo, Claudio/0000-0002-6090-8446 FU Fundacao para a Ciencia e a Tecnologia (FCT, Portugal) through FEDER [PTDC/CTE-AST/120251/2010 (COMPETE reference FCOMP-01-0124-FEDER-019884), RECI/FIS-AST/0176/2012 (FCOMP-01-0124-FEDER-027493), RECI/FIS-AST/0163/2012 (FCOMP-01-0124-FEDER-027492)]; European Research Council/European Community [239953]; FCT [IF/00169/2012, IF/01037/2013]; POPH/FSE (EC); FEDER funding through the program Programa Operacional de Factores de Competitividade - COMPETE; Swiss National Science Foundation FX We would like to thank N. Lanza for fruitful discussions. We acknowledge support from Fundacao para a Ciencia e a Tecnologia (FCT, Portugal) through FEDER funds in program COMPETE, as well as through national funds, in the form of grants reference PTDC/CTE-AST/120251/2010 (COMPETE reference FCOMP-01-0124-FEDER-019884), RECI/FIS-AST/0176/2012 (FCOMP-01-0124-FEDER-027493), and RECI/FIS-AST/0163/2012 (FCOMP-01-0124-FEDER-027492). This work was supported by the European Research Council/European Community under the FP7 through Starting Grant agreement number 239953. N.C.S. and P.F. were supported by FCT through the Investigador FCT contract references IF/00169/2012 and IF/01037/2013 and POPH/FSE (EC) by FEDER funding through the program Programa Operacional de Factores de Competitividade - COMPETE. X. Dumusque was supported by the Swiss National Science Foundation. This work made use of the SIMBAD database. NR 77 TC 27 Z9 27 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR A35 DI 10.1051/0004-6361/201423808 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500141 ER PT J AU Schulze, S Malesani, D Cucchiara, A Tanvir, NR Kruhler, T Postigo, AD Leloudas, G Lyman, J Bersier, D Wiersema, K Perley, DA Schady, P Gorosabel, J Anderson, JP Castro-Tirado, AJ Cenko, SB De Cia, A Ellerbroek, LE Fynbo, JPU Greiner, J Hjorth, J Kann, DA Kaper, L Klose, S Levan, AJ Martin, S O'Brien, PT Page, KL Pignata, G Rapaport, S Sanchez-Ramirez, R Sollerman, J Smith, IA Sparre, M Thone, CC Watson, DJ Xu, D Bauer, EE Bayliss, M Bjornsson, G Bremer, M Cano, Z Covino, S D'Elia, V Frail, DA Geier, S Goldoni, P Hartoog, OE Jakobsson, P Korhonen, H Lee, KY Milvang-Jensen, B Nardini, M Guelbenzu, AN Oguri, M Pandey, SB Petitpas, G Rossi, A Sandberg, A Schmidl, S Tagliaferri, G Tilanus, RPJ Winters, JM Wright, D Wuyts, E AF Schulze, S. Malesani, D. Cucchiara, A. Tanvir, N. R. Kruhler, T. de Ugarte Postigo, A. Leloudas, G. Lyman, J. Bersier, D. Wiersema, K. Perley, D. A. Schady, P. Gorosabel, J. Anderson, J. P. Castro-Tirado, A. J. Cenko, S. B. De Cia, A. Ellerbroek, L. E. Fynbo, J. P. U. Greiner, J. Hjorth, J. Kann, D. A. Kaper, L. Klose, S. Levan, A. J. Martin, S. O'Brien, P. T. Page, K. L. Pignata, G. Rapaport, S. Sanchez-Ramirez, R. Sollerman, J. Smith, I. A. Sparre, M. Thoene, C. C. Watson, D. J. Xu, D. Bauer, E. E. Bayliss, M. Bjornsson, G. Bremer, M. Cano, Z. Covino, S. D'Elia, V. Frail, D. A. Geier, S. Goldoni, P. Hartoog, O. E. Jakobsson, P. Korhonen, H. Lee, K. Y. Milvang-Jensen, B. Nardini, M. Guelbenzu, A. Nicuesa Oguri, M. Pandey, S. B. Petitpas, G. Rossi, A. Sandberg, A. Schmidl, S. Tagliaferri, G. Tilanus, R. P. J. Winters, J. M. Wright, D. Wuyts, E. TI GRB 120422A/SN 2012bz: Bridging the gap between low- and high-luminosity gamma-ray bursts SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: individual: GRB 120422A; supernovae: individual: SN 2012bz; dust, extinction; galaxies: ISM; galaxies: individual: GRB 120422A ID MASS-METALLICITY RELATION; CORE-COLLAPSE SUPERNOVAE; COSMIC STAR-FORMATION; DIGITAL SKY SURVEY; 25 APRIL 1998; HOST GALAXIES; LIGHT CURVES; 980425/SN 1998BW; LY-ALPHA; PHOTOMETRIC REDSHIFTS AB Context. At low redshift, a handful of gamma-ray bursts (GRBs) have been discovered with luminosities that are substantially lower (L-iso less than or similar to 10(48.5) erg s(-1)) than the average of more distant ones (L-iso greater than or similar to 10(49.5) erg s(-1)). It has been suggested that the properties of several low-luminosity (low-L) GRBs are due to shock break-out, as opposed to the emission from ultrarelativistic jets. This has led to much debate about how the populations are connected. Aims. The burst at redshift z = 0.283 from 2012 April 22 is one of the very few examples of intermediate-L GRBs with a gamma-ray luminosity of L-iso similar to 10(49.6-49.9) erg s(-1) that have been detected up to now. With the robust detection of its accompanying supernova SN 2012bz, it has the potential to answer important questions on the origin of low-and high-L GRBs and the GRB-SN connection. Methods. We carried out a spectroscopy campaign using medium-and low-resolution spectrographs with 6-10-m class telescopes, which covered a time span of 37.3 days, and a multi-wavelength imaging campaign, which ranged from radio to X-ray energies over a duration of similar to 270 days. Furthermore, we used a tuneable filter that is centred at H alpha to map star-formation in the host and the surrounding galaxies. We used these data to extract and model the properties of different radiation components and fitted the spectral energy distribution to extract the properties of the host galaxy. Results. Modelling the light curve and spectral energy distribution from the radio to the X-rays revealed that the blast wave expanded with an initial Lorentz factor of Gamma(0) similar to 50, which is a low value in comparison to high-L GRBs, and that the afterglow had an exceptionally low peak luminosity density of less than or similar to 2 x 10(30) erg s(-1) Hz(-1) in the sub-mm. Because of the weak afterglow component, we were able to recover the signature of a shock break-out in an event that was not a genuine low-L GRB for the first time. At 1.4 hr after the burst, the stellar envelope had a blackbody temperature of k(B)T similar to 16 eV and a radius of similar to 7 x 10(13) cm (both in the observer frame). The accompanying SN 2012bz reached a peak luminosity of M-V = -19.7 mag, which is 0.3 mag more luminous than SN 1998bw. The synthesised nickel mass of 0.58 M-circle dot, ejecta mass of 5.87 M-circle dot, and kinetic energy of 4.10x10(52) erg were among the highest for GRB-SNe, which makes it the most luminous spectroscopically confirmed SN to date. Nebular emission lines at the GRB location were visible, which extend from the galaxy nucleus to the explosion site. The host and the explosion site had close-to-solar metallicity. The burst occurred in an isolated star-forming region with an SFR that is 1/10 of that in the galaxy's nucleus. Conclusions. While the prompt gamma-ray emission points to a high-L GRB, the weak afterglow and the low Gamma(0) were very atypical for such a burst. Moreover, the detection of the shock break-out signature is a new quality for high-L GRBs. So far, shock break-outs were exclusively detected for low-L GRBs, while GRB 120422A had an intermediate L-iso of similar to 10(49.6-49.9) erg s(-1). Therefore, we conclude that GRB 120422A was a transition object between low-and high-L GRBs, which supports the failed-jet model that connects low-L GRBs that are driven by shock break-outs and high-L GRBs that are powered by ultra-relativistic jets. C1 [Schulze, S.; Bauer, E. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago, Chile. [Schulze, S.; Bjornsson, G.; Cano, Z.; Jakobsson, P.] Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Schulze, S.; Bjornsson, G.; Cano, Z.; Jakobsson, P.] Univ Iceland, IS-107 Reykjavik, Iceland. [Malesani, D.; Kruhler, T.; de Ugarte Postigo, A.; Leloudas, G.; Fynbo, J. P. U.; Hjorth, J.; Sparre, M.; Watson, D. J.; Xu, D.; Geier, S.; Milvang-Jensen, B.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Cucchiara, A.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Tanvir, N. R.; Wiersema, K.; O'Brien, P. T.; Page, K. L.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [de Ugarte Postigo, A.; Gorosabel, J.; Castro-Tirado, A. J.; Sanchez-Ramirez, R.; Thoene, C. C.] CSIC, IAA, E-18008 Granada, Spain. [Leloudas, G.] Stockholm Univ, Oskar Klein Ctr, Dept Phys, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden. [Lyman, J.; Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Perley, D. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Schady, P.; Greiner, J.; Kann, D. A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Anderson, J. P.] Univ Chile, Dept Astron, Santiago, Chile. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. B.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [De Cia, A.; Xu, D.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, Fac Phys, IL-76100 Rehovot, Israel. [Ellerbroek, L. E.; Kaper, L.; Hartoog, O. E.] Univ Amsterdam, NL-1098 XH Amsterdam, Netherlands. [Kann, D. A.; Klose, S.; Guelbenzu, A. Nicuesa; Rossi, A.; Schmidl, S.] Thuringer Landessternwarte Tautenburg, Tautenburg, Germany. [Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Kruhler, T.; Anderson, J. P.; Martin, S.] European So Observ, Santiago 19, Chile. [Pignata, G.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Rapaport, S.] Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Sollerman, J.; Lee, K. Y.; Sandberg, A.] Stockholm Univ, Oskar Klein Ctr, Dept Astron, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden. [Smith, I. A.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. [Bayliss, M.; Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, M.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Covino, S.; Tagliaferri, G.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Bremer, M.; Winters, J. M.] Inst Radioastron Millimetr IRAM, F-38406 St Martin Dheres, France. [D'Elia, V.] ASI Sci Data Ctr, I-00133 Rome, Italy. [Frail, D. A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Geier, S.] Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain. [Goldoni, P.] Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France. [Korhonen, H.] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio 21500, Finland. [Nardini, M.] Univ Milano Bicocca, I-20126 Milan, Italy. [Oguri, M.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Oguri, M.] Univ Tokyo, Kavli IPMU, WPI, Chiba 2778583, Japan. [Pandey, S. B.] Aryabhatta Res & Observat Sci, Naini Tal 263129, India. [Tilanus, R. P. J.] Joint Astron Ctr, James Clerk Maxwell Telescope, Hilo, HI 96720 USA. [Tilanus, R. P. J.] Netherlands Org Sci Res, NL-2509 AC The Hague, Netherlands. [Wright, D.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Wuyts, E.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Wuyts, E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Bauer, E. E.] Space Sci Inst, Boulder, CO 80301 USA. [Gorosabel, J.] Univ Pais Vasco UPV EHU, Unidad Asociada Grp Ciencia Planetarias UPV EHU I, Dept Fis Aplicada 1, Bilbao 48013, Spain. [Gorosabel, J.] Basque Fdn Sci, Ikerbasque, Bilbao 48008, Spain. [D'Elia, V.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. RP Schulze, S (reprint author), Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago, Chile. EM sschulze@astro.puc.cl RI Oguri, Masamune/C-6230-2011; Hjorth, Jens/M-5787-2014; Sparre, Martin/C-2424-2015; Watson, Darach/E-4521-2015; Jakobsson, Pall/L-9950-2015; Korhonen, Heidi/E-3065-2016; Rossi, Andrea/N-4674-2015; OI Schulze, Steve/0000-0001-6797-1889; de Ugarte Postigo, Antonio/0000-0001-7717-5085; Covino, Stefano/0000-0001-9078-5507; Sanchez-Ramirez, Ruben/0000-0002-7158-5099; Kruehler, Thomas/0000-0002-8682-2384; Tagliaferri, Gianpiero/0000-0003-0121-0723; D'Elia, Valerio/0000-0002-7320-5862; Sollerman, Jesper/0000-0003-1546-6615; Castro-Tirado, A. J./0000-0003-2999-3563; Hjorth, Jens/0000-0002-4571-2306; Sparre, Martin/0000-0002-9735-3851; Watson, Darach/0000-0002-4465-8264; Jakobsson, Pall/0000-0002-9404-5650; Korhonen, Heidi/0000-0003-0529-1161; Rossi, Andrea/0000-0002-8860-6538; Thone, Christina/0000-0002-7978-7648 FU Icelandic Research Fund; University of Iceland Research Fund; Dark Cosmology Centre; CONICYT through FONDECYT [3140534, 3110142]; Basal-CATA [PFB-06/2007]; Iniciativa Cientifica Milenio grant (Millennium Center for Supernova Science) [P10-064-F]; "Millennium Institute of Astrophysics (MAS)" of Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo de Chile [IC120009]; "Fondo de Innovacion para la Competitividad, del Ministerio de Economia, Foment y Turismo de Chile"; CONICYT-Chile FONDECYT [1101024]; Instrument Center for Danish Astrophysics; European Commission under the Marie Curie Intra-European Fellowship Programme; ERC-StG [EGGS-278202]; UK Space Agency; Swedish Research Council [623-2011-7117]; UK Science and Technology Facilities Council; Spanish research project [AYA2012-39362-C02-02, AYA2009-14000-C03-01, AYA2012-39727-C03-01]; European Commission under the Marie Curie Career Integration Grant programme [FP7-PEOPLE-2012-CIG 322307]; DFG cluster of excellence "Origin and Structure of the Universe" - Thuringer Landessternwarte Tautenburg; Thuringer Landessternwarte Tautenburg; Alexander von Humboldt Foundation of Germany; DFG [KL 766/16-1, HA 1850/28-1]; Thuringer Ministerium fur Bildung, Wissenschaft und Kultur [FKZ 12010-514]; Danish National Research Foundation; Spitzer/NASA grant RSA [1287913]; NSF [GN-2012A-Q-9, GN-2012A-Q-39, GN-2012B-Q-5, GS-2012A-Q-30, GS-2012A-Q-38]; Nordic Optical Telescope (NOT); Instituto de Astrofisica de Canarias [P45-002, ITP10-04]; Gran Telescopio Canarias (GTC) in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias in the island of La Palma; Magellan [CN2012A-059]; TRAM Plateau de Bure Interferometer; James Clerk Maxwell Telescope [M12AI12]; XMM-Newton, an ESA science mission; ESA Member States; NASA; W.M. Keck Foundation; Science and Technology Facilities Council of the United Kingdom; National Research Council of Canada; Netherlands Organisation for Scientific Research; Canada Foundation for Innovation; Smithsonian Institution; Academia Sinica; INSU/CNRS (France); MPG (Germany); IGN (Spain); Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; James S. McDonnell Foundation; Associates of the California Institute of Technology; University of Chicago; state of California, Illinois; state of California, Maryland; National Science Foundation; Alfred P. Sloan Foundation; US Department of Energy Office of Science FX We thank Shri Kulkarni (Caltech) for obtaining the Keck spectrum. S.S. thanks Tsvi Piran (The Hebrew University, Israel), Nir Sapir, Eli Waxman (Weizmann Institute of Science, Israel), Milena Butane (Universidad Andres Bello, Chile), Maryam Modjaz (New York University, USA), and the anonymous referee for many productive and valuable discussions. S.S. acknowledges support by a Grant of Excellence from the Icelandic Research Fund, from the University of Iceland Research Fund, from the Dark Cosmology Centre, where part of this study was performed, and from CONICYT through FONDECYT grant 3140534. We acknowledge support from Basal-CATA PFB-06/2007 (FEB, SS), Iniciativa Cientifica Milenio grant P10-064-F (Millennium Center for Supernova Science), by Project IC120009 "Millennium Institute of Astrophysics (MAS)" of Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo de Chile, with input from "Fondo de Innovacion para la Competitividad, del Ministerio de Economia, Foment y Turismo de Chile" (F.E.B., G.P., J.A.R., S.S.), CONICYT-Chile FONDECYT 1101024 (FEB). J.A.P. acknowledges support by CONICYT through FONDECYT grant 3110142. D.M. acknowledges the Instrument Center for Danish Astrophysics for support. T.K. and H.K. acknowledge support by the European Commission under the Marie Curie Intra-European Fellowship Programme in FP7. J.P.U.F., B.M.J., and D.X. acknowledge support from the ERC-StG grant EGGS-278202. K.L.P. acknowledges financial support by the UK Space Agency for the Swift project. G.L. is supported by the Swedish Research Council through grant No. 623-2011-7117. J.L. acknowledges the UK Science and Technology Facilities Council for research studentship support. The research activity of AdUP, C.T., and J.G. is supported by Spanish research project AYA2012-39362-C02-02. A.d.U.P. acknowledges support by the European Commission under the Marie Curie Career Integration Grant programme (FP7-PEOPLE-2012-CIG 322307). A.J.C.T. acknowledges support front the Spanish research project AYA2009-14000-C03-01 and AYA2012-39727-C03-01 D.A.K. acknowledges support by the DFG cluster of excellence "Origin and Structure of the Universe" and funding by the Thuringer Landessternwarte Tautenburg. A. R. acknowledges support by the Thuringer Landessternwarte Tautenburg. P.S. acknowledges support through the Sofja Kovalevskaja Award from the Alexander von Humboldt Foundation of Germany. A.N.G. and S.K. acknowledge support by DFG KL 766/16-1. S. Schmidl acknowledges support by the Thuringer Ministerium fur Bildung, Wissenschaft und Kultur under FKZ 12010-514. The Dark Cosmology Centre is funded by the Danish National Research Foundation. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This research has made use of the GHostS database (www.grbhosts.org), which is partly funded by Spitzer/NASA grant RSA Agreement No. 1287913. Based in part on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, as part of the program 089.A-0067, the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc.; , under a co-operative agreement with the NSF on behalf of the Gemini partnership, as part of the programs GN-2012A-Q-9, GN-2012A-Q-39, GN-2012B-Q-5, GS-2012A-Q-30, GS-2012A-Q-38, GS-2012A-Q-30, and GN-2012B-Q-5, the Nordic Optical Telescope (NOT), 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, as part of the program P45-002 (PI: Jakobsson) and ITP10-04 (PI: Kotak, QUB), the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma, with Magellan as part of CN2012A-059, with the TRAM Plateau de Bure Interferometer, the James Clerk Maxwell Telescope, as part of the program M12AI12, with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. 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 United Kingdom Infrared Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK The lames Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the National Research Council of Canada, and the Netherlands Organisation for Scientific Research. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. 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. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). 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.sdss3org/.; 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 216 TC 23 Z9 23 U1 3 U2 15 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 2014 VL 566 AR A102 DI 10.1051/0004-6361/201423387 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500092 ER PT J AU Wu, YW Sato, M Reid, MJ Moscadelli, L Zhang, B Xu, Y Brunthaler, A Menten, KM Dame, TM Zheng, XW AF Wu, Y. W. Sato, M. Reid, M. J. Moscadelli, L. Zhang, B. Xu, Y. Brunthaler, A. Menten, K. M. Dame, T. M. Zheng, X. W. TI Trigonometric parallaxes of star-forming regions in the Sagittarius spiral arm SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrometry; Galaxy: structure; Galaxy: kinematics and dynamics; masers; stars: formation ID II METHANOL MASERS; GIANT MOLECULAR CLOUD; MILKY-WAY; WATER MASER; FUNDAMENTAL PARAMETERS; GALACTIC ROTATION; VLBI ASTROMETRY; INFRARED SURVEY; BESSEL SURVEY; IRAS SOURCES AB We report measurements of parallaxes and proper motions of ten high-mass star-forming regions in the Sagittarius spiral arm of the Milky Way as part of the BeSSeL Survey with the VLBA. Combining these results with eight others from the literature, we investigated the structure and kinematics of the arm between Galactocentric azimuths beta approximate to -2 degrees. and 65 degrees. We found that the spiral pitch angle is 7 degrees.3 +/- 1 degrees.5; the arm's half-width, defined as the rms deviation from the fitted spiral, is approximate to 0.2 kpc; and the nearest portion of the Sagittarius arm is 1.4 +/- 0.2 kpc from the Sun. Unlike for adjacent spiral arms, we found no evidence for significant peculiar motions of sources in the Sagittarius arm opposite to Galactic rotation. C1 [Wu, Y. W.; Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Wu, Y. W.; Sato, M.; Zhang, B.; Brunthaler, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Wu, Y. W.] Chinese Acad Sci, Grad Univ, Beijing 100049, Peoples R China. [Reid, M. J.; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Moscadelli, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Zheng, X. W.] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. RP Wu, YW (reprint author), Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. EM ywwu@pmo.ac.cn OI Moscadelli, Luca/0000-0002-8517-8881 FU Chinese NSF [NSF 11133008, NSF 11073054, NSF 11203082, NSF 10921063, NSF 11233007, BK2012494]; Key Laboratory for Radio Astronomy, CAS; ERC Advanced Investigator Grant GLOSTAR [247078] FX This work was supported by the Chinese NSF through grants NSF 11133008, NSF 11073054, NSF 11203082, NSF 10921063, NSF 11233007, BK2012494, and the Key Laboratory for Radio Astronomy, CAS. This work was partially funded by the ERC Advanced Investigator Grant GLOSTAR (247078). We are grateful to James Urquhart for providing the ATLASGAL FITS files. We also acknowledge John D. Hunter, the creator of the Python matplotlib, which was used extensively for our figures. Facilities: VLBA. NR 80 TC 27 Z9 27 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR A17 DI 10.1051/0004-6361/201322765 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500036 ER PT J AU O'Malley, RC Power, ML AF O'Malley, Robert C. Power, Michael L. TI The energetic and nutritional yields from insectivory for Kasekela chimpanzees SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Pan troglodytes; Faunivory; Tool use; Diet; Tanzania; Feeding rate; Ants; Termites ID PAN-TROGLODYTES-SCHWEINFURTHII; GOMBE NATIONAL-PARK; WILD CHIMPANZEES; CULTURAL VARIATION; COMMON ANCESTOR; EDIBLE INSECTS; LAETOLIL BEDS; PLANT FOODS; TOOL USE; ANTS AB Insectivory is hypothesized to be an important source of macronutrients, minerals, and vitamins for chimpanzees (Pan troglodytes), yet nutritional data based on actual intake are lacking. Drawing on observations from 2008 to 2010 and recently published nutritional assays, we determined the energy, macronutrient and mineral yields for termite-fishing (Macrotermes), ant-dipping (Dorylus), and antfishing (Camponotus) by the Kasekela chimpanzees of Gombe National Park, Tanzania. We also estimated the yields from consumption of weaver ants (Oecophylla) and termite alates (Macrotermes and Pseudacanthotermes). On days when chimpanzees were observed to prey on insects, the time spent in insectivorous behavior ranged from <1 min to over 4 h. After excluding partial bouts and those of <1 min duration, ant-dipping bouts were of significantly shorter duration than the other two forms of tool-assisted insectivory but provided the highest mass intake rate. Termite-fishing bouts were of significantly longer duration than ant-dipping and had a lower mass intake rate, but provided higher mean and maximum mass yields. Ant-fishing bouts were comparable to termite-fishing bouts in duration but had significantly lower mass intake rates. Mean and maximum all-day yields from termite-fishing and antdipping contributed to or met estimated recommended intake (ERI) values for a broad array of minerals. The mean and maximum all-day yields of other insects consistently contributed to the ERI only for manganese. All forms of insectivory provided small but probably non-trivial amounts of fat and protein. We conclude that different forms of insectivoly have the potential to address different nutritional needs for Kasekela chimpanzees. Other than honeybees, insects have received little attention as potential foods for hominins. Our results suggest that ants and (on a seasonal basis) termites would have been viable sources of fat, high-quality protein and minerals for extinct hominins employing Pan-like subsistence technology in East African woodlands. (C) 2014 Elsevier Ltd. All rights reserved. C1 [O'Malley, Robert C.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Power, Michael L.] Smithsonian Conservat Biol Inst, Nutr Lab, Washington, DC 20008 USA. [Power, Michael L.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Washington, DC 20008 USA. RP O'Malley, RC (reprint author), George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. EM omalleyrc@gmail.com; PowerM@si.edu OI Power, Michael/0000-0002-6120-3528 FU Tanzania Wildlife Research Institute; Tanzania National Parks, Gombe National Park; Jane Goodall Institute-Tanzania; University of Southern California; International Summer Field Research Award; Dissertation Research and Writing Award; Jane Goodall Center Research Award; Integrative and Evolutionary Biology Research Award; Gold Family Fellowship FX Samson Pindu provided invaluable assistance in the field. Dr. Craig Stanford provided welcome mentoring and support during Robert O'Malley's dissertation research. Michael Jakubasz provided training for the nutritional assays. Dr. Francisco Hita Garcia, Dr. Caspar Schoning, and Dr. Rudolf Scheffrahn shared their expertise in insect identification. Three anonymous reviewers provided helpful comments and critiques that greatly improved this manuscript. We thank the Tanzania Wildlife Research Institute, the Tanzania National Parks, Gombe National Park and the Jane Goodall Institute-Tanzania for their permission and support for this research, conducted under COSTECH permit #2009-229-ER-2007-188. Finally, we thank Dr. W.C. McGrew for co-chairing 'The Other Faunivory' symposium held at the 2012 American Association of Physical Anthropologists meeting in Portland, Oregon. Robert O'Malley's research was funded by the University of Southern California through a Joint Initiative Merit Fellowship, International Summer Field Research Award, a Dissertation Research and Writing Award, a Jane Goodall Center Research Award, an Integrative and Evolutionary Biology Research Award, and a Gold Family Fellowship. This research complied with all US institutional requirements and regulations of the Republic of Tanzania regarding the ethical treatment of primate research subjects in the field. NR 98 TC 5 Z9 5 U1 3 U2 30 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD JUN PY 2014 VL 71 SI SI BP 46 EP 58 DI 10.1016/j.jhevol.2013.09.014 PG 13 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AL0NZ UT WOS:000338824900007 PM 24698197 ER PT J AU Zhou, SL Dong, WP Chen, XQ Zhang, XC Wen, J Schneider, H AF Zhou, Shiliang Dong, Wenpan Chen, Xiaoqing Zhang, Xianchun Wen, Jun Schneider, Harald TI How many species of bracken (Pteridium) are there? Assessing the Chinese brackens using molecular evidence SO TAXON LA English DT Article DE chloroplast; microsatellite; phylogeny; phylogeography; Pteridium; taxonomy ID AQUILINUM L. KUHN; TAXONOMIC STATUS; MATING SYSTEM; CHLOROPLAST DNA; FERNS PTERIDIUM; CAINOZOIC FERNS; NEW-ZEALAND; DENNSTAEDTIACEAE; PHYLOGEOGRAPHY; DELIMITATION AB Pteridium (the bracken) is a genus of common and widely distributed ferns throughout the world. The variation patterns of morphology in the genus are highly complex and no consensus has been reached among taxonomists regarding the number of species as well as subdivision of the variable species. To address the question of how many species and subspecies of Pteridium occur in Asia, 75 populations were sampled in Bolivia, China, Japan, Malaysia, Mexico and Peru. Sequence data of three chloroplast DNA regions, rps4-trnSGGA, rpl16 and trnSGCU-trnGUCC and the genotype data of three microsatellite loci were collected. The newly generated sequence data combined with the sequences already available from GenBank for samples from all over the world were subjected to several phylogenetic analyses and species delimitation tests. The results support recognition of two diploid species, P. aquilinum in the Northern Hemisphere and Africa and P. esculentum in South America and Australia. Evidence was found to recognize one Asian tetraploid species, P. semihastatum. The Eurasian occurrences of P. aquilinum can be further subdivided into subsp. aquilinum occurring in Africa, Europe and Asia Minor; subsp. japonicum occurring from East Asia to eastern Europe; subsp. wightianum occurring from central China to Malesia (Malay Peninsula, New Caledonia, New Zealand) and northern Australia. The North American subsp. latiusculum was also found in India. Some local "species" recorded in Flora of China likely represent hybrids between subsp. japonicum and subsp. wightianum. C1 [Zhou, Shiliang; Dong, Wenpan; Chen, Xiaoqing; Zhang, Xianchun; Wen, Jun; Schneider, Harald] Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Schneider, Harald] Nat Hist Museum, London SW7 BD, England. RP Wen, J (reprint author), Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. EM wenj@si.edu; h.schneider@nhm.ac.uk RI 董, 文攀/D-1297-2015; Dong, Wenpan/C-8167-2013; Schneider, Harald/B-6681-2008 OI Schneider, Harald/0000-0002-4548-7268 FU Ministry of Science and Technology [2012BAC01B05-6, 2011FY120200, 2012AA021602]; National Natural Science Foundation of China [31270239, 31110103911] FX We thank Gerry Moore, John A. Thomson and Ching-I Peng for help in solving nomenclatural problems. This work was supported in part by the Ministry of Science and Technology (2012BAC01B05-6, 2011FY120200 & 2012AA021602) and the National Natural Science Foundation of China (31270239 & 31110103911). NR 84 TC 5 Z9 5 U1 3 U2 21 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 JUN PY 2014 VL 63 IS 3 BP 509 EP 521 PG 13 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA AK9OE UT WOS:000338755600003 ER PT J AU Gonzalez-Astudillo, V Aguirre, AA AF Gonzalez-Astudillo, Viviana Aguirre, A. Alonso TI News from the IAEH SO ECOHEALTH LA English DT News Item C1 [Gonzalez-Astudillo, Viviana] Univ Queensland, Sch Vet Sci, Gatton, Qld, Australia. [Aguirre, A. Alonso] Smithsonian Mason Sch Conservat, Front Royal, VA USA. [Aguirre, A. Alonso] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. RP Gonzalez-Astudillo, V (reprint author), Univ Queensland, Sch Vet Sci, Gatton, Qld, Australia. EM v.gonzalezastudillo@uq.edu.au NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1612-9202 EI 1612-9210 J9 ECOHEALTH JI EcoHealth PD JUN PY 2014 VL 11 IS 2 BP 152 EP 153 DI 10.1007/s10393-014-0932-0 PG 2 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AK2EE UT WOS:000338231100001 PM 24740800 ER PT J AU Zatsarinny, O Bartschat, K Babaeva, NY Kushner, MJ AF Zatsarinny, Oleg Bartschat, Klaus Babaeva, Natalia Yu Kushner, Mark J. TI Electron collisions with cesium atoms-benchmark calculations and application to modeling an excimer-pumped alkali laser SO PLASMA SOURCES SCIENCE & TECHNOLOGY LA English DT Article DE electron-cesium collisions; cross section; elastic scattering; excitation; ionization; momentum transfer; excimer-pumped alkali laser ID TOTAL CROSS-SECTIONS; CS SCATTERING; POLARIZED ELECTRONS; ELASTIC-SCATTERING; SHAPE RESONANCES; IONIZATION; POTASSIUM AB The B-spline R-matrix (BSR) with pseudostates method is employed to describe electron collisions with cesium atoms. Over 300 states are kept in the close-coupling expansion, including a large number of pseudostates to model the effect of the Rydberg spectrum and, most importantly, the ionization continuum on the results for transitions between the discrete physical states of interest. Predictions for elastic scattering, momentum transfer, excitation and ionization are presented for incident energies up to 200 eV and compared with results from previous calculations and available experimental data. In a second step, the results are used to model plasma formation in an excimer-pumped alkali laser operating on the Cs (6(2)P(3/2),(1/2) -> 6(2)S(1/2)) (852 nm and 894 nm) transitions. At sufficiently high operating temperature of a Cs-Ar containing quartz cell, pump power, and repetition rate, plasma formation in excess of 10(14)-10(15)cm(-3) occurs. This may reduce laser output power by electron collisional mixing of the upper and lower laser levels. C1 [Zatsarinny, Oleg; Bartschat, Klaus] Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. [Bartschat, Klaus] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Babaeva, Natalia Yu; Kushner, Mark J.] Univ Michigan, Dept Elect Engn & Comp Sci, Ann Arbor, MI 48109 USA. RP Zatsarinny, O (reprint author), Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. EM oleg.zatsarinny@drake.edu; klaus.bartschat@drake.edu; nbabaeva@umich.edu; mjkush@umich.edu RI Kushner, Mark/D-4547-2015 FU NSF [PHY-1068140, PHY-1212450]; XSEDE allocation [PHY-090031]; DoD High Energy Laser Multidisciplinary Research Initiative (NYB, MJK) FX This work was supported by the NSF under grants No PHY-1068140, PHY-1212450, and the XSEDE allocation PHY-090031 (OZ, KB), and by the DoD High Energy Laser Multidisciplinary Research Initiative (NYB, MJK). NR 32 TC 3 Z9 3 U1 3 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0963-0252 EI 1361-6595 J9 PLASMA SOURCES SCI T JI Plasma Sources Sci. Technol. PD JUN PY 2014 VL 23 IS 3 AR 035011 DI 10.1088/0963-0252/23/3/035011 PG 7 WC Physics, Fluids & Plasmas SC Physics GA AJ7QS UT WOS:000337891900013 ER PT J AU Stanford, D Bradley, B AF Stanford, Dennis Bradley, Bruce TI On thin ice: problems with Stanford and Bradley's proposed Solutrean colonisation of North America Reply SO ANTIQUITY LA English DT Editorial Material ID RADIOCARBON-DATES; VARIABILITY C1 [Stanford, Dennis] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. [Bradley, Bruce] Univ Exeter, Dept Archaeol, Exeter EX4 4QE, Devon, England. RP Stanford, D (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, 10th & Constitut Ave NW, Washington, DC 20560 USA. NR 19 TC 1 Z9 1 U1 2 U2 7 PU ANTIQUITY PI YORK PA KINGS MANOR, YORK YO1 7EP, ENGLAND SN 0003-598X EI 1745-1744 J9 ANTIQUITY JI Antiquity PD JUN PY 2014 VL 88 IS 340 BP 614 EP 621 PG 8 WC Anthropology; Archaeology SC Anthropology; Archaeology GA AJ4LE UT WOS:000337647000019 ER PT J AU Sackett, LC Seglund, A Guralnick, RP Mazzella, MN Wagner, DM Busch, JD Martin, AP AF Sackett, Loren C. Seglund, Amy Guralnick, Robert P. Mazzella, Maxwell N. Wagner, David M. Busch, Joseph D. Martin, Andrew P. TI Evidence for two subspecies of Gunnison's prairie dogs (Cynomys gunnisoni), and the general importance of the subspecies concept SO BIOLOGICAL CONSERVATION LA English DT Article DE Prairie dog; Genetic variation; Ecological differentiation; lntraspecific taxonomy; Subspecies; Evolutionary divergence ID ZAPUS-HUDSONIUS-PREBLEI; ENDANGERED SPECIES ACT; MITOCHONDRIAL-DNA; POPULATION-STRUCTURE; CYTOCHROME-B; HYBRID ZONE; INTROGRESSIVE HYBRIDIZATION; GENETIC DIFFERENTIATION; MAXIMUM-LIKELIHOOD; MICROSATELLITE DNA AB Accurate taxonomy is essential for conservation, but subspecies-level systematics can be hampered both by a lack of consensus on what constitutes a subspecies and by discordance among data types (e.g., genetics vs. morphology). Here we provide a framework for evaluating subspecies using multidimensional criteria, and suggest that taxa must satisfy multiple criteria to qualify as subspecies. As a case study, we use the Gunnison's prairie dog (Cynomys gunnisoni), a species for which there has been disagreement regarding the existence of subspecies due to inconsistent application of criteria for defining subspecies. To explicitly test the hypothesis that two subspecies exist, we generated five predictions that could be evaluated with genetic data, while also using morphological and ecological criteria. We sampled 838 Gunnison's prairie dogs from across the species range and performed a series of genetic analyses using 16 microsatellite and two mitochondrial loci (cytochrome b and the control region). We compared subspecies morphology and quantitatively evaluated whether abiotic and biotic habitat characteristics encountered by each subspecies differed. Genetic results from all five predictions supported the existence of two distinct subspecies within the confines of a proposed revision in the boundary between subspecies. The subspecies differed marginally in morphology and significantly in their habitats, suggesting ecological differentiation. Our results, which are in line with historical descriptions of morphologically distinct subspecies, suggest the subspecies should be recognized. This work provides support for the utility of integrating multiple data and analysis types to inform systematics and conservation. (c) 2014 Elsevier Ltd. All rights reserved. C1 [Sackett, Loren C.; Guralnick, Robert P.; Mazzella, Maxwell N.; Martin, Andrew P.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. [Seglund, Amy] Colorado Pk & Wildlife, Montrose, CO 81401 USA. [Guralnick, Robert P.] Univ Colorado, Museum Nat Hist, Boulder, CO 80309 USA. [Wagner, David M.; Busch, Joseph D.] No Arizona Univ, Ctr Microbial Genet & Genom, Flagstaff, AZ 86011 USA. RP Sackett, LC (reprint author), Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. EM Loren.Sackett@Colorado.edu FU Colorado Parks and Wildlife [IA-SWG-1658-10] FX We are grateful to Abbey Paulson for assisting in generation of GIS maps in ArcMap and to Nic Kooyers for feedback on the mixed models. Many field assistants were instrumental in completing this project, especially Erin Arnold Pikcilingis and Sarah Hale. Colorado Parks and Wildlife helped in the collection of samples from Colorado. We would like to thank Colorado Parks and Wildlife, Dave Cagle and the AZDGF, Andrea Chavez and the BLM, Jim Stuart and the NMDGF, Cel Gachupin and the Zia DNR, Bob Salter and the Santo Domingo DNR, Stuart Perea and the Jicarilla Apache Nation, Dave Mikesic and the Navajo Nation DFW, and the National Park Service for permission to live-trap prairie dogs. Paula Martin provided information about previous relocation sites in NM and CO. Prairie Dog Pals allowed us to obtain samples from prairie dogs in their holding facility, and Kenny Bader provided a sample from Petrified Forest NP. Many anonymous private landowners graciously provided access to their land for trapping. Funding for this project was provided by Colorado Parks and Wildlife grant #IA-SWG-1658-10. We thank Alan Templeton, Eliecer Gutierrez, Tony Apa, Dan Tripp, Patrik Nosil, John Hoogland, Bryan Carstens and an anonymous reviewer for useful comments that improved this manuscript. NR 120 TC 9 Z9 9 U1 3 U2 35 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 JUN PY 2014 VL 174 BP 1 EP 11 DI 10.1016/j.biocon.2014.03.010 PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AJ4MP UT WOS:000337650800001 ER PT J AU Deutsch, JI AF Deutsch, James I. TI The Battle for the Bs: 1950s Hollywood and the rebirth of low-budget cinema SO HISTORICAL JOURNAL OF FILM RADIO AND TELEVISION LA English DT Book 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 ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0143-9685 EI 1465-3451 J9 HIST J FILM RADIO TV JI Hist. J. Film Radio Telev. PD JUN PY 2014 VL 34 IS 2 BP 289 EP 290 DI 10.1080/01439685.2014.914664 PG 2 WC Film, Radio, Television SC Film, Radio & Television GA AJ4AY UT WOS:000337612800014 ER PT J AU Ocampo, EH Menone, ML Iturburu, FG Nunez, JD Baeza, JA AF Ocampo, Emiliano H. Menone, Mirta L. Iturburu, Fernando G. Nunez, Jesus D. Antonio Baeza, J. TI Effect of the endosymbiotic pea crab Calyptraeotheres garthi on the metabolic rate and oxidative status of the slipper limpet Crepidula cachimilla SO INVERTEBRATE BIOLOGY LA English DT Article DE oxidative stress; oxygen consumption; Pinnotheridae ID OXYGEN-CONSUMPTION; ANTIOXIDANT RESPONSES; ENERGY BUDGETS; STRESS; PARASITISM; ARGENTINA; INFECTION; EXPOSURE; PINNOTHERIDAE; MITOCHONDRIA AB Parasites may induce metabolic changes and imbalances in the redox status of hosts. This study tested the effect of parasites on the O2 consumption rate (O2-CR) of hosts, and explored the link between O2-CR and oxidative stress in parasitized hosts. We used the symbiotic pea crab Calyptraeotheres garthi and its slipper limpet host Crepidula cachimilla as models. The O2-CR of long-term (3months) infested limpets was 2.5 times greater than that of long-term uninfested limpets. Also, the O2-CR of limpets stripped of crabs 24h before measurements was intermediate between that of long-term infested and uninfested limpets. These results indicate a parasitic relationship between C. garthi and Cr. cachimilla, and suggest that the effect of the parasite on the metabolic rate of limpets is reversible. Lastly, the activity of two antioxidant enzymes (CAT and GST) as well as lipid peroxidation did not vary between infested and uninfested limpets. Thus, increased O2-CR is not necessarily coupled with oxidative stress in pea crab-parasitized slipper limpets. C1 [Ocampo, Emiliano H.; Nunez, Jesus D.] Univ Nacl Mar del Plata, CONICET, Inst Invest Marinas & Costeras, Lab Invertebrados, RA-7600 Buenos Aires, DF, Argentina. [Menone, Mirta L.; Iturburu, Fernando G.] Univ Nacl Mar del Plata, CONICET, Inst Invest Marinas & Costeras, Lab Ecotoxicol, RA-7600 Buenos Aires, DF, Argentina. [Antonio Baeza, J.] Clemson Univ, Dept Biol Sci, Clemson, SC 29632 USA. [Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Antonio Baeza, J.] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Coquimbo 1780000, Chile. RP Ocampo, EH (reprint author), Univ Nacl Mar del Plata, CONICET, Inst Invest Marinas & Costeras, Lab Invertebrados, RA-7600 Buenos Aires, DF, Argentina. EM eocampo@mdp.edu.ar FU CONICET [PIP 2008 112-384 200-801-02190]; Universidad Nacional de Mar del Plata [EXA 515/10] FX We are grateful to Juan Pablo Busalmen and Luciana Robuschi for their assistance with the use of the O2-sensing system, Emiliano Pisani for providing phytoplankton, Samuel Silva for help in collecting limpets, and Nicolas Chiaradia for help in taking photographs. We are indebted to Juan Timi and two anonymous reviewers for their suggestions, which improved this manuscript. We also thank Enrique Morsan and colleagues of the Instituto de Biologia Marina y Pesquera, Almirante Storni for their hospitality during sampling. The present work was partially supported by PIP 2008 112-384 200-801-02190 (CONICET) and EXA 515/10 (Universidad Nacional de Mar del Plata). E.O. received scholarship support from CONICET. This is contribution number 942 of the Smithsonian Marine Station at Fort Pierce, Smithsonian Institution. NR 49 TC 2 Z9 2 U1 2 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 2014 VL 133 IS 2 BP 170 EP 179 DI 10.1111/ivb.12050 PG 10 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA AJ2ZA UT WOS:000337532900007 ER PT J AU Hood, WR Kessler, DS Oftedal, OT AF Hood, W. R. Kessler, D. S. Oftedal, O. T. TI Milk composition and lactation strategy of a eusocial mammal, the naked mole-rat SO JOURNAL OF ZOOLOGY LA English DT Article DE milk composition; naked mole-rat; proximate composition; mineral composition; evaporative water loss; bone mineralization ID HETEROCEPHALUS-GLABER; WATER-BALANCE; LITTER SIZE; AD-LIBITUM; RODENT; CALCIUM; GROWTH; YOUNG; BATHYERGIDAE; TEMPERATURE AB The reproductive female, or queen, in a eusocial colony must allocate sufficient nutrients to reproduction to maintain a high rate of reproductive output. In mammals, the energetic costs of lactation greatly exceed those of pregnancy, and thus, lactation should be exceptionally costly for a eusocial queen, such as the naked mole-rat Heterocephalus glaber. We predicted that naked mole-rat milk would be energy- and nutrient-dense. Naked mole-rat milk averaged 17.2% dry matter, 4.5% fat, 4.8% protein, 5.7% sugar and 1.1% ash; and per gram contained 3.0mg calcium, 1.1mg phosphorus, 0.44mg magnesium and 0.54mg potassium. Other than elevated protein and low sugar in colostrum, the composition of milk did not change over the course of lactation. Naked mole-rats not only had the lowest energy content of milk (3.9kJg-1) reported for any rodent but also appeared to be an outlier from a trend for milk dry matter, fat and energy concentrations to be inversely related to body mass in rodents. The dilute nature of naked mole-rat milk indicates that an unusually large amount of milk (equivalent to about half of body mass) must be produced daily to sustain the energy needs of an average litter (12 young). Sustaining high water throughput during lactation may be necessary to meet expected water needs of the offspring but may limit the queen to foods that are high in moisture. The concentrations of macrominerals in milk were within the range described for other rodents, except that the Ca:P ratio of milk (2.8:1) was unusually high. Given a lifespan that can exceed 30 years, large average litter size and several litters per year, the lifetime lactation output of a mole-rat queen must be phenomenal and warrants further study. C1 [Hood, W. R.] Auburn Univ, Dept Biol Sci, Auburn, AL 36849 USA. [Kessler, D. S.] Smithsonian Natl Zool Pk, Washington, DC USA. [Oftedal, O. T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Hood, WR (reprint author), Auburn Univ, Dept Biol Sci, 101 Life Sci Bldg, Auburn, AL 36849 USA. EM wrhood@auburn.edu NR 59 TC 0 Z9 0 U1 2 U2 29 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0952-8369 EI 1469-7998 J9 J ZOOL JI J. Zool. PD JUN PY 2014 VL 293 IS 2 BP 108 EP 118 DI 10.1111/jzo.12126 PG 11 WC Zoology SC Zoology GA AJ2WP UT WOS:000337525500006 ER PT J AU Cushman, KC Muller-Landau, HC Condit, RS Hubbell, SP AF Cushman, K. C. Muller-Landau, Helene C. Condit, Richard S. Hubbell, Stephen P. TI Improving estimates of biomass change in buttressed trees using tree taper models SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE above-ground biomass; Barro Colorado Island; forest dynamics; permanent sample plot; tropical forest ID TROPICAL FORESTS; CARBON SINK; BALANCE; PLOT AB Repeat censuses of tree plots are key tools for investigating forest carbon fluxes. Current measurement procedures for trees with buttresses or trunk irregularities - trees that account for a large fraction of tropical forest biomass -introduce substantial systematic error in plot-level estimates of biomass change. The diameters of buttressed trees are measured above the standard height of 13m, and the measurement heights on individual trees are often moved upwards as buttresses grow. Because tree trunks taper (diameter decreases with height), biomass growth in buttressed individuals tends to be underestimated. Methods have been introduced to correct biomass growth estimates in individual trees for increases in measurement height; however, these methods change the distribution of effective measurement heights over time, introducing biases in plot-level estimates of biomass change. In this study, we developed and applied new methods to measure and model trunk taper, and to use taper models to correct estimates of AGB change for changing measurement heights. We measured trunk taper above buttresses in 190 stems on Barro Colorado Island, Panama (BCI), a site where more than half of forest biomass is in trees measured above standard height. We compared proposed taper models to see which best described our measured taper data, then used the best taper model to correct for changing measurement heights in the historical plot data. Specifically, for all diameter measurements taken above 13m, we calculated equivalent diameters at 13m and substituted these into allometric equations to examine biomass change over time. We found that measured taper was best fit by an exponential model with a rate parameter that varied with measured diameter (tree size), height of measurement (buttress height) and species. Whereas uncorrected data show a decrease in biomass of 021% year-1 between 1985 and 2010 on BCI, taper-corrected data show an increase of 018% year-1. The novel correction method presented here converts all measured diameters to one standard effective measurement height. This corrects for biases at the plot level and provides a stronger foundation for measuring biomass change in tropical forests. C1 [Cushman, K. C.; Muller-Landau, Helene C.; Condit, Richard S.; Hubbell, Stephen P.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Hubbell, Stephen P.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. RP Cushman, KC (reprint author), Smithsonian Trop Res Inst, Roosevelt Ave, Balboa, Ancon, Panama. EM cushman.kc@gmail.com FU Smithsonian Institution internship; National Science Foundation [DEB-1046113, DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9405933, DEB-9221033, DEB-9100058, DEB-8906869, DEB-8605042, DEB-8206992, DEB-7922197]; Center for Tropical Forest Science; Smithsonian Tropical Research Institute; John D. and Catherine T. MacArthur Foundation; Mellon Foundation; Small World Institute Fund FX We thank Pablo Ramos and Paulino Villareal for assistance with fieldwork and gratefully acknowledge the financial support of a Smithsonian Institution internship for KCC. This manuscript was advanced at a workshop funded by the National Science Foundation (DEB-1046113). The BCI forest dynamics research project was made possible by National Science Foundation grants to Stephen P. Hubbell: DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9615226, DEB-9405933, DEB-9221033, DEB-9100058, DEB-8906869, DEB-8605042, DEB-8206992, DEB-7922197, support from the Center for Tropical Forest Science, the Smithsonian Tropical Research Institute, the John D. and Catherine T. MacArthur Foundation, the Mellon Foundation, the Small World Institute Fund, and numerous private individuals, and through the hard work of over 100 people from 10 countries over the past three decades. The plot project is part of the Center for Tropical Forest Science, a global network of large-scale demographic tree plots. HCM designed the study, KCC collected the taper data, RC and SPH contributed the forest plot data, KCC and HCM analysed the data, KCC and HCM wrote the paper, and RC provided comments on a draft. NR 32 TC 9 Z9 9 U1 2 U2 29 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X EI 2041-2096 J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD JUN PY 2014 VL 5 IS 6 BP 573 EP 582 DI 10.1111/2041-210X.12187 PG 10 WC Ecology SC Environmental Sciences & Ecology GA AJ5UK UT WOS:000337754500009 ER PT J AU Lambert, O Bianucci, G Beatty, BL AF Lambert, Olivier Bianucci, Giovanni Beatty, Brian L. TI Bony outgrowths on the jaws of an extinct sperm whale support macroraptorial feeding in several stem physeteroids SO NATURWISSENSCHAFTEN LA English DT Article DE Cetacea; Physeteroidea; Buccal exostoses; Feeding; Macroraptorial ID GARDNERS-SYNDROME; EXOSTOSES; CETACEA; MIOCENE; PREVALENCE; ODONTOCETI; LESIONS; PERU AB Several extinct sperm whales (stem Physeteroidea) were recently proposed to differ markedly in their feeding ecology from the suction-feeding modern sperm whales Kogia and Physeter. Based on cranial, mandibular, and dental morphology, these Miocene forms were tentatively identified as macroraptorial feeders, able to consume proportionally large prey using their massive teeth and robust jaws. However, until now, no corroborating evidence for the use of teeth during predation was available. We report on a new specimen of the stem physeteroid Acrophyseter, from the late middle to early late Miocene of Peru, displaying unusual bony outgrowths along some of the upper alveoli. Considering their position and outer shape, these are identified as buccal maxillary exostoses. More developed along posterior teeth and in tight contact with the high portion of the dental root outside the bony alveoli, the exostoses are hypothesized to have developed during powerful bites; they may have worked as buttresses, strengthening the teeth when facing intense occlusal forces. These buccal exostoses further support a raptorial feeding technique for Acrophyseter and, indirectly, for other extinct sperm whales with a similar oral apparatus (Brygmophyseter, Livyatan, Zygophyseter). With a wide size range, these Miocene stem physeteroids were major marine macropredators, occupying ecological niches nowadays mostly taken by killer whales. C1 [Lambert, Olivier] Inst Royal Sci Nat Belgique, Direct Operat Terre & Hist Vie, B-1000 Brussels, Belgium. [Bianucci, Giovanni] Univ Pisa, Dipartimento Sci Terra, I-56126 Pisa, Italy. [Beatty, Brian L.] NYIT Coll Osteopath Med, Old Westbury, NY 11568 USA. [Beatty, Brian L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Beatty, Brian L.] Virginia Museum Nat Hist, Martinsville, VA 24112 USA. RP Lambert, O (reprint author), Inst Royal Sci Nat Belgique, Direct Operat Terre & Hist Vie, 29 Rue Vautier, B-1000 Brussels, Belgium. EM olivier.lambert@naturalsciences.be OI Lambert, Olivier/0000-0003-0740-5791 FU MIUR [PRIN 2012YJSBM]; SYNT HESYS grant [BE-TAF-2842]; Belgian Federal Science Policy Office FX We thank W Aguirre, E Diaz, R Salas-Gismondi, and M Urbina for giving us access to the specimen and for its final preparation. Constructive comments from C de Muizon, ND Pyenson, and two anonymous reviewers considerably enhanced the quality of the article. This work was financially supported by MIUR grant (PRIN 2012YJSBM, resp. GB), SYNT HESYS grant (BE-TAF-2842, GB), and Return Grant of the Belgian Federal Science Policy Office (2012-April 2013, OL). NR 22 TC 7 Z9 7 U1 1 U2 13 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 EI 1432-1904 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD JUN PY 2014 VL 101 IS 6 BP 517 EP 521 DI 10.1007/s00114-014-1182-2 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AJ3WD UT WOS:000337597700009 PM 24821119 ER PT J AU Tananbaum, H Weisskopf, MC Tucker, W Wilkes, B Edmonds, P AF Tananbaum, H. Weisskopf, M. C. Tucker, W. Wilkes, B. Edmonds, P. TI Highlights and discoveries from the Chandra X-ray Observatory SO REPORTS ON PROGRESS IN PHYSICS LA English DT Review DE X-ray Observatory; Chandra; NASA ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; DEEP FIELD-SOUTH; STAR-FORMATION RATE; SUPERNOVA REMNANT G292.0+1.8; GALAXY CLUSTER 1E-0657-56; INTERACTION CROSS-SECTION; CORE-COLLAPSE SUPERNOVAE; ABSORPTION-LINE QUASARS; XMM-NEWTON OBSERVATIONS AB Within 40 years of the detection of the first extra-solar x-ray source in 1962, NASA's Chandra X-ray Observatory has achieved an increase in sensitivity of 10 orders of magnitude, comparable to the gain in going from naked-eye observations to the most powerful optical telescopes over the past 400 years. Chandra is unique in its capabilities for producing sub-arcsecond x-ray images with 100-200 eV energy resolution for energies in the range 0.08= 2 cm diameter) and measured its diameter at 1.3 m height, and then used these data to estimate liana aboveground biomass. An initial liana survey was completed in 1997-1999 and then repeated in 2012, using identical methods. Liana abundance in the plots increased by an average of 1.00% +/- 0.88% per year, leading to a highly significant (t = 6.58, df = 35, P < 0.00001) increase in liana stem numbers. Liana biomass rose more slowly over time (0.32% +/- 1.37% per year) and the mean difference between the two sampling intervals was nonsignificant (t = 1.46, df = 35, P = 0.15; paired t tests). Liana size distributions shifted significantly (chi(2) = 191, df = 8, P < 0.0001; Chi-square test for independence) between censuses, mainly as a result of a nearly 40% increase in the number of smaller (2-3 cm diameter) lianas, suggesting that lianas recruited rapidly during the study. We used long-term data on rainfall and forest dynamics from our study site to test hypotheses about potential drivers of change in liana communities. Lianas generally increase with rainfall seasonality, but we found no significant trends over time (1997-2012) in five rainfall parameters (total annual rainfall, dry-season rainfall, wet-season rainfall, number of very dry months, CV of monthly rainfall). However, rates of tree mortality and recruitment have increased significantly over time in our plots, and general linear mixed-effect models suggested that lianas were more abundant at sites with higher tree mortality and flatter topography. Rising concentrations of atmospheric CO2, which may stimulate liana growth, might also have promoted liana increases. Our findings clearly support the view that lianas are increasing in abundance in old-growth tropical forests, possibly in response to accelerating forest dynamics and rising CO2 concentrations. The aboveground biomass of trees was lowest in plots with abundant lianas, suggesting that lianas could reduce forest carbon storage and potentially alter forest dynamics if they continue to proliferate. C1 [Laurance, William F.; Magrach, Ainhoa; Campbell, Mason; Edwards, Will; Laurance, Susan G.] James Cook Univ, Ctr Trop Environm & Sustainabil Sci, Cairns, Qld 4878, Australia. [Laurance, William F.; Magrach, Ainhoa; Campbell, Mason; Edwards, Will; Laurance, Susan G.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4878, Australia. [Andrade, Ana S.; Camargo, Jose L. C.; Valsko, Jefferson J.; Lovejoy, Thomas E.] Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, BR-69060000 Manaus, Amazonas, Brazil. [Andrade, Ana S.; Camargo, Jose L. C.; Valsko, Jefferson J.; Lovejoy, Thomas E.] Smithsonian Trop Res Inst, BR-69060000 Manaus, Amazonas, Brazil. [Fearnside, Philip M.] Natl Inst Amazonian Res INPA, Dept Ecol, BR-69060000 Manaus, Amazonas, Brazil. [Lovejoy, Thomas E.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. RP Laurance, WF (reprint author), James Cook Univ, Ctr Trop Environm & Sustainabil Sci, Cairns, Qld 4878, Australia. EM bill.laurance@jcu.edu.au RI James Cook University, TESS/B-8171-2012; Research ID, CTBCC /O-3564-2014; Camargo, Jose Luis/C-3137-2015; Laurance, Susan/G-6021-2011; Magrach, Ainhoa/B-1038-2012; OI Laurance, Susan/0000-0002-2831-2933; Magrach, Ainhoa/0000-0003-2155-7556; Edwards, Will/0000-0001-8981-7479; Fearnside, Philip/0000-0003-3672-9082 FU Conservation, Food and Health Foundation; Australian Research Council; U.S. National Science Foundation; NASA Long-term Biosphere-Atmosphere Experiment in the Amazon; A. W. Mellon Foundation; MacArthur Foundation; World Wildlife Fund-US; National Institute for Amazonian Research; Smithsonian Institution FX We thank Stefan Schnitzer and two anonymous referees for commenting on the manuscript. Support was provided by the Conservation, Food and Health Foundation, Australian Research Council, U.S. National Science Foundation, NASA Long-term Biosphere-Atmosphere Experiment in the Amazon, A. W. Mellon Foundation, MacArthur Foundation, World Wildlife Fund-US, National Institute for Amazonian Research, and Smithsonian Institution. This is publication number 628 in the Biological Dynamics of Forest Fragments Project (BDFFP) technical series. NR 65 TC 23 Z9 24 U1 10 U2 83 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD JUN PY 2014 VL 95 IS 6 BP 1604 EP 1611 PG 8 WC Ecology SC Environmental Sciences & Ecology GA AI9AQ UT WOS:000337218500018 PM 25039224 ER PT J AU Cook-Patton, SC Agrawal, AA AF Cook-Patton, Susan C. Agrawal, Anurag A. TI Exotic plants contribute positively to biodiversity functions but reduce native seed production and arthropod richness SO ECOLOGY LA English DT Article DE arthropod richness; biodiversity; biomass; Dryden, New York, USA; exotic plants; invasion; mono- vs. polyculture; native plants; old-field habitat; plant-insect interactions; seed production ID VEGETATIONAL DIVERSITY; SPECIES-DIVERSITY; ENEMY RELEASE; COMMUNITIES; INVASIONS; COMPLEMENTARITY; MAINTENANCE; MECHANISMS; IMPACTS; HYPOTHESIS AB Although exotic plants comprise a substantial portion of floristic biodiversity, their contributions to community and ecosystem processes are not well understood. We manipulated plant species richness in old-field communities to compare the impacts of native vs. exotic species on plant biomass, seed production, and arthropod community structure. Plants within diverse communities, regardless of whether they were native or exotic, had higher biomass and seed production than in monocultures and displayed positive complementarity. Increasing native or exotic plant richness also enhanced the richness of arthropods on plants, but exotics attracted fewer arthropod species for a given arthropod abundance than did natives. Additionally, when exotic and native plants grew together, exotics suppressed seed production of native species. Thus, exotic plants appear to contribute positively to some biodiversity functions, but may impact native communities over longer time frames by reducing native seed production and recruiting fewer arthropod species. C1 [Cook-Patton, Susan C.; Agrawal, Anurag A.] Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA. RP Cook-Patton, SC (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM cook-pattons@si.edu FU Cornell's IGERT in Biogeochemistry and Environmental Biocomplexity; [NSF-DEB 1118783] FX We thank A. C. Erwin, A. P. Hastings, L. Schunk, and S. H. McArt for field assistance, P. Kotanen for Elymus seeds, J. Simonis for statistical advice, and B. Blossey, L. J. Martin, S. H. McArt, J. Sparks, and A. Agrawal's lab for invaluable discussion. We thank reviewers for their comments on earlier versions of the manuscript. This work was supported by a grant from Cornell's IGERT in Biogeochemistry and Environmental Biocomplexity to S. C. Cook-Patton and NSF-DEB 1118783 to A. A. Agrawal. NR 46 TC 5 Z9 5 U1 5 U2 43 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD JUN PY 2014 VL 95 IS 6 BP 1642 EP 1650 PG 9 WC Ecology SC Environmental Sciences & Ecology GA AI9AQ UT WOS:000337218500022 PM 25039228 ER PT J AU Smith, TB Glynn, PW Mate, JL Toth, LT Gyory, J AF Smith, Tyler B. Glynn, Peter W. Mate, Juan L. Toth, Lauren T. Gyory, Joanna TI A depth refugium from catastrophic coral bleaching prevents regional extinction SO ECOLOGY LA English DT Article DE coral bleaching; coral mortality; depth refuge; eastern Tropical Pacific; El Nino-Southern Oscillation; extinction; Holocene; Millepora; refuge ID EL-NINO; CLIMATE-CHANGE; OXIDATIVE STRESS; REEF; RECORD; PANAMA; MORTALITY; WINNERS; BARRIER; FISHES AB Species intolerant of changing climate might avoid extinction within refugia buffered from extreme conditions. Refugia have been observed in the fossil record but are not well documented or understood on ecological time scales. Using a 37-year record from the eastern Pacific across the two most severe El Nino events on record (1982-1983 and 1997-1998) we show how an exceptionally thermally sensitive reef-building hydrocoral, Millepora intricata, twice survived catastrophic bleaching in a deeper-water refuge (>11 m depth). During both events, M. intricata was extirpated across its range in shallow water, but showed recovery within several years, while two other hydrocorals without deep-water populations were driven to regional extinction. Evidence from the subfossil record in the same area showed shallow-water persistence of abundant M. intricata populations from 5000 years ago, through severe El Nino-Southern Oscillation cycles, suggesting a potential depth refugium on a millennial timescale. Our data confirm the deep refuge hypothesis for corals under thermal stress. C1 [Smith, Tyler B.; Gyory, Joanna] Univ Virgin Isl, Ctr Marine & Environm Studies, St Thomas, VI 00802 USA. [Glynn, Peter W.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Mate, Juan L.] Smithsonian Trop Res Inst, Panama City, Panama. [Toth, Lauren T.] Florida Inst Technol, Melbourne, FL 32901 USA. RP Smith, TB (reprint author), Univ Virgin Isl, Ctr Marine & Environm Studies, St Thomas, VI 00802 USA. EM tsmith@uvi.edu FU Biological Oceanography Program of the U.S. National Science Foundation; STRI Pre-doctoral Fellowship; University of Miami; Lana Vento Charitable Trust; NSF Virgin Islands Experimental Program to Stimulate Competitive Research; Smithsonian Institution Marine Science Network; Geological Society of America; American Museum of Natural History's Lerner Gray Fund FX We thank the Smithsonian Tropical Research Institute (STRI) and the crew of the R. V. Urraca for field logistics and support; I. Bethancourt, A. Correa, A. Domingo, I. Enochs, D. Manzello, P. Fong, R. Muthukrishnan, for field assistance; I. Enochs, J. Martens, and B. Riegl for satellite image processing and bathymetry files; R. B. Aronson and I. G. Macintyre for support on the coring project; and H. Cheng for conducting U-series dating on the cores. We also thank two anonymous reviewers for comments that improved the manuscript. Funding was provided by the Biological Oceanography Program of the U.S. National Science Foundation (to P. W. Glynn), a STRI Pre-doctoral Fellowship, the University of Miami Alumni and Maytag Fellowships, the Lana Vento Charitable Trust (to T. B. Smith), the NSF Virgin Islands Experimental Program to Stimulate Competitive Research (to J. Gyory and T. B. Smith), and the Smithsonian Institution Marine Science Network, Geological Society of America, and American Museum of Natural History's Lerner Gray Fund (L. T. Toth). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. The Autoridad Nacional de Ambiente de Panama (ANAM) granted the necessary permits to conduct coral research in the Gulf of Chiriqui, Panama NR 42 TC 10 Z9 10 U1 2 U2 36 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD JUN PY 2014 VL 95 IS 6 BP 1663 EP 1673 PG 11 WC Ecology SC Environmental Sciences & Ecology GA AI9AQ UT WOS:000337218500024 PM 25039230 ER PT J AU Geeta, R Lohmann, LG Magallon, S Faith, DP Hendry, A Crandall, K de Meester, L Webb, CO Prieur-Richard, AH Mimura, M Conti, E Cracraft, J Forest, F Jaramillo, C Donoghue, M Yahara, T AF Geeta, R. Lohmann, Lucia G. Magallon, Susana Faith, Daniel P. Hendry, Andrew Crandall, Keith de Meester, Luc Webb, Campbell O. Prieur-Richard, Anne-Helene Mimura, Makiko Conti, Elena Cracraft, Joel Forest, Felix Jaramillo, Carlos Donoghue, Michael Yahara, Tetsukazu TI Biodiversity only makes sense in the light of evolution SO JOURNAL OF BIOSCIENCES LA English DT Article DE Ecosystem services; evolutionary potential; evosystem services; sustainable use ID RESISTANCE; PERSPECTIVE; DIVERSITY; INDIA; RICE C1 [Geeta, R.] Univ Delhi, Dept Bot, Delhi 110007, India. [Lohmann, Lucia G.] Univ Sao Paulo, Dept Bot, BR-05508090 Sao Paulo, Brazil. [Magallon, Susana] Univ Nacl Autonoma Mexico, Inst Biol, Dept Bot, Mexico City 04510, DF, Mexico. [Faith, Daniel P.] Australian Museum, Sydney, NSW 2010, Australia. [Hendry, Andrew] McGill Univ, Redpath Museum, Montreal, PQ H3A 2K6, Canada. [Hendry, Andrew] McGill Univ, Dept Biol, Montreal, PQ H3A 2K6, Canada. [Crandall, Keith] George Washington Univ, Computat Biol Inst, Ashburn, VA 20147 USA. [de Meester, Luc] Lab Aquat Ecol & Evolutionary Biol, B-3000 Louvain, Belgium. [Webb, Campbell O.] Arnold Arboretum Harvard Univ, Boston, MA 02131 USA. [Prieur-Richard, Anne-Helene] MNHN, DIVERSITAS, F-75231 Paris 05, France. [Mimura, Makiko] Tamagawa Univ, Div Genet & Cell Biol, Machida, Tokyo 1948610, Japan. [Conti, Elena] Univ Zurich, Inst Systemat Bot, CH-8008 Zurich, Switzerland. [Conti, Elena] Univ Zurich, Bot Garden, CH-8008 Zurich, Switzerland. [Cracraft, Joel] Amer Museum Nat Hist, Dept Ornithol, New York, NY 10024 USA. [Forest, Felix] Royal Bot Gardens, Jodrell Lab, Richmond TW9 3DS, Surrey, England. [Jaramillo, Carlos] Smithsonian Trop Res Inst, Panama City, Panama. [Donoghue, Michael] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. [Yahara, Tetsukazu] Kyushu Univ, Dept Biol, Higashi Ku, Fukuoka 8128581, Japan. RP Geeta, R (reprint author), Univ Delhi, Dept Bot, Delhi 110007, India. EM rgeeta53@gmail.com RI Conti, Elena/G-3720-2010; U-ID, Kyushu/C-5291-2016; De Meester, Luc/F-3832-2015; OI De Meester, Luc/0000-0001-5433-6843; Crandall, Keith/0000-0002-0836-3389 NR 33 TC 2 Z9 3 U1 4 U2 51 PU INDIAN ACAD SCIENCES PI BANGALORE PA C V RAMAN AVENUE, SADASHIVANAGAR, P B #8005, BANGALORE 560 080, INDIA SN 0250-5991 EI 0973-7138 J9 J BIOSCIENCES JI J. Biosci. PD JUN PY 2014 VL 39 IS 3 BP 333 EP 337 DI 10.1007/s12038-014-9427-y PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AJ0HZ UT WOS:000337332900001 PM 24845496 ER PT J AU Gutstein, CS Cozzuol, MA Pyenson, ND AF Simon Gutstein, Carolina Alberto Cozzuol, Mario Pyenson, Nicholas D. TI The Antiquity of Riverine Adaptations in Iniidae (Cetacea, Odontoceti) Documented by a Humerus from the Late Miocene of the Ituzaingo Formation, Argentina SO ANATOMICAL RECORD-ADVANCES IN INTEGRATIVE ANATOMY AND EVOLUTIONARY BIOLOGY LA English DT Article DE Iniidae; late Miocene; south America; scapula; sternum; Ituzaingo formation ID DOLPHIN INIA-GEOFFRENSIS; EVOLUTIONARY HISTORY; EXTANT CETACEANS; WHALE PHYLOGENY; NORTH-CAROLINA; CYTOCHROME-B; AMAZON; MORPHOLOGY; LINEAGES; IDENTIFICATION AB "River dolphins" are a paraphyletic group of toothed whales (Odontoceti) that represent independent secondary invasions of freshwater habitats. Different "river dolphin" lineages display suites of convergent morphological specializations that commonly reflect adaptations to riverine and freshwater environments, such as longirostry, reduced orbits, and wide, paddle-like flippers. One lineage, the Iniidae, is presently endemic to South America, and includes several extinct Neogene taxa along with their sole extant genus, Inia (the Amazon River dolphin). We report here a humerus recovered from the late Miocene deposits of the Ituzaingo Formation in the Parana Basin of Argentina. The specimen exhibits diagnostic features of the family Iniidae, including a scapular-sternal joint of the humerus, which is a unique anatomical connection among mammals. This joint permits enhanced parasagittal adduction of the flipper as a control surface, relative to other odontocetes, providing Inia with a high degree of maneuverability in its structurally complex and heterogenous riverine habitat. This unique anatomical connection, here documented from the late Miocene (similar to 9 million years-6.5 million years old), not only provides the oldest diagnostic record for Iniidae, but it also indicates a similar habitat use for this lineage, a finding coincident with the current paleoenvironmental interpretation for the Ituzaingo Formation. (C) 2014 Wiley Periodicals, Inc. C1 [Simon Gutstein, Carolina] Univ Chile, Dept Biol, Lab Ontogenia & Filogenia, Fac Ciencias, Santiago 7800003, Chile. [Simon Gutstein, Carolina; Pyenson, Nicholas D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Alberto Cozzuol, Mario] Univ Fed Minas Gerais, Dept Zool, Inst Ciencias Biol, BR-31270910 Belo Horizonte, MG, Brazil. [Pyenson, Nicholas D.] Burke Museum Nat & Culture, Dept Mammal, Seattle, WA USA. [Pyenson, Nicholas D.] Burke Museum Nat & Culture, Dept Paleontol, Seattle, WA USA. RP Gutstein, CS (reprint author), Univ Chile, Dept Biol, Las Palmeras 3425, Santiago 7800003, Chile. EM sgcarolina@gmail.com RI Cozzuol, Mario/H-8302-2012; OI Cozzuol, Mario/0000-0003-3645-0401; Gutstein, Carolina/0000-0002-0823-2434 FU CONICYT, Becas Chile, Departamento de Postgrado y Postitulo of the Vicerrectoria de Asuntos Academicos of Universidad de Chile; NMNH Small Grant Award; NMNH Office of the Director; Smithsonian Institution's Remington Kellogg Fund; National Geographic Society Committee on Research Exploration [8903-11, 9019-11] FX Grant sponsor: CONICYT, Becas Chile, Departamento de Postgrado y Postitulo of the Vicerrectoria de Asuntos Academicos of Universidad de Chile (C. S. G.); Grant sponsor: NMNH Small Grant Award; Grant sponsor: NMNH Office of the Director; Grant sponsor: The Smithsonian Institution's Remington Kellogg Fund; Grant sponsor: National Geographic Society Committee on Research Exploration (N.D.P); Grant number: 8903-11, 9019-11; Grant sponsor: (CSG). NR 53 TC 4 Z9 4 U1 3 U2 12 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 JUN PY 2014 VL 297 IS 6 BP 1096 EP 1102 DI 10.1002/ar.22901 PG 7 WC Anatomy & Morphology SC Anatomy & Morphology GA AI7DJ UT WOS:000337042100008 PM 24585575 ER PT J AU Johnson, AEM Freeman, EW Wildt, DE Songsasen, N AF Johnson, Amy E. M. Freeman, Elizabeth W. Wildt, David E. Songsasen, Nucharin TI Spermatozoa from the maned wolf (Chrysocyon brachyurus) display typical canid hyper-sensitivity to osmotic and freezing-induced injury, but respond favorably to dimethyl sulfoxide SO CRYOBIOLOGY LA English DT Article DE Maned wolf; Osmotic stress; Sperm cryopreservation; Glycerol; Dimethyl sulfoxide; Cooling ID MEXICAN GRAY WOLVES; BLACK-FOOTED FERRET; SPERM QUALITY; BOAR SPERM; PERMEABILITY CHARACTERISTICS; REPRODUCTIVE TECHNOLOGIES; MEMBRANE-PERMEABILITY; STALLION SPERMATOZOA; AVIAN SPERMATOZOA; TOLERANCE LIMITS AB We assessed the influences of medium osmolality, cryoprotectant and cooling and warming rate on maned wolf (Cluysocyon brachyurus) spermatozoa. Ejaculates were exposed to Ham's F10 medium (isotonic control) or to this medium plus NaCl (350-1000 mOsm), sucrose (369 and 479 mOsm), 1 M glycerol (1086 mOsm) or dimethyl sulfoxide (Me2SO, 1151 mOsm) for 10 min. Each sample then was diluted back into Ham's medium and assessed for sperm motility and plasma membrane integrity. Although glycerol and Me2SO had no influence (P > 0.05), NaCl and sucrose solutions affected sperm motility (P < 0.05), but not membrane integrity. Motility of sperm exposed to <600 mOsm NaCl or sucrose was less (P < 0.05) than fresh ejaculate, but comparable (P> 0.05) to the control. As osmolality of the NaCl solution increased, motility decreased to <5%. In a separate study, ejaculates were diluted in Test Yolk Buffer containing 1 M glycerol or Me2SO and cooled from 5 degrees C to -120 degrees C at -57.8 degrees C, -124.2 degrees C or -67.0 degrees C/min, frozen in LN2, thawed in a water bath for 30s at 37 degrees C or 10 s at 50 degrees C, and then assessed for motility, plasma- and acrosomal membrane integrity. Cryopreservation markedly (P < 0.05) reduced sperm motility by 70% compared to fresh samples. Higher (P < 0.05) post-thaw motility (20.0 +/- 1.9% versus 13.5 +/- 2.1%) and membrane integrity (51.2 +/- 1.7% versus 41.5 +/- 2.2%) were observed in samples cryopreserved in Me2- SO than in glycerol. Cooling rates influenced survival of sperm cryopreserved in glycerol with -57.8 degrees C/min being advantageous (P < 0.05). The findings demonstrate that although maned wolf spermatozoa are similar to domestic dog sperm in their sensitivity to osmotic-induced motility damage, the plasma membranes tolerate dehydration, and the cells respond favorably to Me2SO as a cryoprotectant. Published by Elsevier Inc. C1 [Johnson, Amy E. M.; Wildt, David E.; Songsasen, Nucharin] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. [Johnson, Amy E. M.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Freeman, Elizabeth W.] George Mason Univ, New Century Coll, Fairfax, VA 22030 USA. RP Songsasen, N (reprint author), Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM songsasenn@si.edu OI Johnson, Amy/0000-0002-9288-1305 FU Morris Animal Foundation FX This study was supported by the Morris Animal Foundation. The Maned Wolf SSP played a key role in recruiting and organizing participating institutions. The authors thank: staff from the White Oak Conservation Center, Houston Zoo, Connecticut's Beardsley Zoo, Sedgwick County Zoo, Louisville Zoo, Natural Science Center of Greensboro, Dickerson Park Zoo and the Smithsonian Conservation Biology Institute for participating; and Dr. Luis Padilla, Dr. Erika Wilson-Lipanovich, Lara Mouttham, Tatiana Motheo and Ainjil Bills for technical assistance. NR 67 TC 3 Z9 5 U1 0 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0011-2240 EI 1090-2392 J9 CRYOBIOLOGY JI Cryobiology PD JUN PY 2014 VL 68 IS 3 BP 361 EP 370 DI 10.1016/j.cryobiol.2014.04.004 PG 10 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA AI5CX UT WOS:000336884100009 PM 24731851 ER PT J AU Hultgren, KM AF Hultgren, Kristin M. TI Variable effects of symbiotic snapping shrimps on their sponge hosts SO MARINE BIOLOGY LA English DT Article ID DWELLING ALPHEID SHRIMP; CARIBBEAN CORAL-REEFS; COMMUNITY STRUCTURE; SEA-ANEMONES; MUTUALISM; PLANT; COEVOLUTION; MORPHOLOGY; PREDATION; HABITATS AB Mutualistic relationships are ubiquitous in tropical coral reefs, but the costs and benefits to partner species are often poorly known. In Caribbean coral reefs, several species of snapping shrimp (Synalpheus spp.) dwell exclusively in marine sponges, which serve as both habitat and food source. A paired experimental design was used to examine the effects of Synalpheus occupancy on predation, morphology, and growth of their sponge host Lissodendoryx colombiensis in Bocas del Toro, Panama (9.351A degrees N, 82.258A degrees W) in June 2009. Shrimp occupancy significantly decreased consumption of sponges by a predatory sea star (Oreaster reticulatus) and also affected sponge morphology; sponges grown without shrimps decreased in canal size, in both the laboratory and the field. Shrimp occupancy had more ambiguous effects on sponge growth. In laboratory experiments, shrimp occupancy benefited sponge growth, although all sponges experienced overall decreases in mass. In field experiments, there were no significant differences in growth between occupied and empty sponges. However, the benefits of shrimp occupancy on sponge growth were negatively correlated with overall increases in sponge size; sponges that decreased in mass during the experiment benefited more from shrimp occupancy than sponges that increased in mass. These costs and benefits suggest that Synalpheus has variable effects on sponges: positive effects on sponges in the presence of predators, and/or when sponges are decreasing in mass (e.g., during periods of physical stress), but a negative effect on sponges during periods of active sponge growth. C1 [Hultgren, Kristin M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Hultgren, KM (reprint author), Seattle Univ, 901 12th Ave, Seattle, WA 98122 USA. EM hultgrenk@seattleu.edu FU Smithsonian Marine Science Network FX The Smithsonian Marine Science Network provided funding for this study. This study could not have been completed without the patience and help of the staff at the Smithsonian's Bocas del Toro marine station and the advice and help of J. Emmett Duffy. This study was greatly improved by advice from J. Pawlik, M. E. Hay, and J. Wulff. M. McGrew and C. Freeman provided invaluable assistance in the field. This manuscript was also greatly improved by the comments of Martin Thiel, Tripp Macdonald, and several anonymous reviewers. All experiments and collections were conducted in compliance with the current laws of Panama. NR 52 TC 0 Z9 0 U1 1 U2 30 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD JUN PY 2014 VL 161 IS 6 BP 1217 EP 1227 DI 10.1007/s00227-014-2412-z PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AI4AG UT WOS:000336806700001 ER PT J AU Miller, AW Ruiz, GM AF Miller, A. Whitman Ruiz, Gregory M. TI Arctic shipping and marine invaders SO NATURE CLIMATE CHANGE LA English DT Editorial Material ID INVASION; RISK C1 [Miller, A. Whitman; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Miller, AW (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd,POB 28, Edgewater, MD 21037 USA. EM millerw@si.edu OI Ruiz, Gregory/0000-0003-2499-441X; Miller, Whitman/0000-0003-0484-182X NR 20 TC 21 Z9 21 U1 6 U2 34 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X EI 1758-6798 J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD JUN PY 2014 VL 4 IS 6 BP 413 EP 416 PG 5 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AI8EC UT WOS:000337138700007 ER PT J AU Dudley, R AF Dudley, Robert TI Drunks and Monkeys SO SCIENTIST LA English DT Article C1 [Dudley, Robert] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Panama City, Panama. RP Dudley, R (reprint author), Univ Calif Berkeley, Berkeley, CA 94720 USA. NR 0 TC 0 Z9 0 U1 1 U2 3 PU LABX MEDIA GROUP PI MIDLAND PA PO BOX 216, 478 BAY ST, MIDLAND, ONTARIO L4R 1K9, CANADA SN 0890-3670 EI 1547-0806 J9 SCIENTIST JI Scientist PD JUN PY 2014 VL 28 IS 6 BP 70 EP 70 PG 1 WC Information Science & Library Science; Multidisciplinary Sciences SC Information Science & Library Science; Science & Technology - Other Topics GA AI5WS UT WOS:000336940900018 ER PT J AU Garvin, HM Sholts, SB Mosca, LA AF Garvin, Heather M. Sholts, Sabrina B. Mosca, Laurel A. TI Sexual Dimorphism in Human Cranial Trait Scores: Effects of Population, Age, and Body Size SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE sex estimation; ordinal scores; non-metric traits; Walker method; forensic anthropology ID GREATER SCIATIC NOTCH; FORENSIC ANTHROPOLOGY; AMERICAN WHITES; LONG BONES; STATURE; MORPHOLOGY; COLLECTION; HOMINIDS; INDIANS; NEGROES AB Sex estimation from the skull is commonly performed by physical and forensic anthropologists using a five-trait scoring system developed by Walker. Despite the popularity of this method, validation studies evaluating its accuracy across a variety of samples are lacking. Furthermore, it remains unclear what other intrinsic or extrinsic variables are related to the expression of these traits. In this study, cranial trait scores and postcranial measurements were collected from four diverse population groups (U.S. Whites, U.S. Blacks, medieval Nubians, and Arikara Native Americans) following Walker's protocols (total n=499). Univariate and multivariate analyses were utilized to evaluate the accuracy of these traits in sex estimation, and to test for the effects of population, age, and body size on trait expressions. Results revealed significant effects of population on all trait scores. Sample-specific correct sex classification rates ranged from 74% to 94%, with an overall accuracy of 85% for the pooled sample. Classification performance varied among the traits (best for glabella and mastoid scores and worst for nuchal scores). Furthermore, correlations between traits were weak or nonsignificant, suggesting that different factors may influence individual traits. Some traits displayed correlations with age and/or postcranial size that were significant but weak, and within-population analyses did not reveal any consistent relationships between these traits across all groups. These results indicate that neither age nor body size plays a large role in trait expression, and thus does not need to be incorporated into sex estimation methods. Am J Phys Anthropol 154:259-269, 2014. (c) 2014 Wiley Periodicals, Inc. C1 [Garvin, Heather M.; Mosca, Laurel A.] Mercyhurst Univ, Dept Anthropol Archaeol, Erie, PA 16546 USA. [Garvin, Heather M.; Mosca, Laurel A.] Mercyhurst Univ, Dept Appl Forens Sci, Erie, PA 16546 USA. [Sholts, Sabrina B.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Garvin, HM (reprint author), Mercyhurst Univ, 501 E 38th St, Erie, PA 16546 USA. EM HMGarvin@gmail.com FU NSF Doctoral Dissertation Improvement Grant [BCS-1061313]; Sigma Xi GIAR [G20101015155040] FX Grant sponsor: NSF Doctoral Dissertation Improvement Grant; Grant number: BCS-1061313; Grant sponsor: Sigma Xi GIAR; Grant number: G20101015155040. NR 48 TC 10 Z9 11 U1 1 U2 28 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 JUN PY 2014 VL 154 IS 2 BP 259 EP 269 DI 10.1002/ajpa.22502 PG 11 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AH9VM UT WOS:000336492900009 PM 24595622 ER PT J AU Pobiner, B AF Pobiner, Briana TI SHAPING HUMANITY: HOW SCIENCE, ART, AND IMAGINATION HELP US UNDERSTAND OUR ORIGINS SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Book Review C1 [Pobiner, Briana] Smithsonian Inst, Natl Museum Amer Hist, Dept Anthropol, Washington, DC 20560 USA. RP Pobiner, B (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Anthropol, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 2 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD JUN PY 2014 VL 154 IS 2 BP 317 EP 317 DI 10.1002/ajpa.22508 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AH9VM UT WOS:000336492900017 ER PT J AU Graves, GR AF Graves, Gary R. TI Historical decline and probable extinction of the Jamaican Golden Swallow Tachycineta euchrysea euchrysea SO BIRD CONSERVATION INTERNATIONAL LA English DT Article ID WINTERING POPULATIONS; PREDATION; BEHAVIOR AB The endemic Jamaican subspecies of the Golden Swallow Tachycineta euchrysea euchrysea has been rare and locally distributed since its discovery in 1847. By the 1950s, its geographic range had contracted to a small region along the northern frontier of Cockpit Country. The last unequivocal sight records occurred in the early 1980s, raising strong concern about the swallow's conservation status. I conducted an island-wide search for the swallow from 1994 through 2012. Standardised censuses of aerial insectivores at 1,281 sites, including the last redoubts of the Golden Swallow in Trelawny Parish, revealed no evidence of the species. These surveys and the absence of documented sight records during the past three decades suggest that the Jamaican race of the Golden Swallow is close to extinction if not already extinct. The cause of the population decline is unknown but is most likely linked to chronic predation by introduced mammalian predators, particularly the arboreal black rat Rattus rattus C1 [Graves, Gary R.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, MRC 116, Washington, DC 20013 USA. [Graves, Gary R.] Univ Copenhagen, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark. RP Graves, GR (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, MRC 116, POB 37012, Washington, DC 20013 USA. RI publist, CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017 FU Alexander Wetmore fund of the Smithsonian Institution; James Bond fund of the Smithsonian Institution FX Brian Schmidt was an indispensable participant in the aerial insectivore censuses and supplied the base maps. Kim Bostwick (Cornell University Museum of Vertebrates), Mike Brooke (Cambridge University Museum of Zoology), Ben Marks (Field Museum), Brad Millen (Royal Ontario Museum), Robert Prys-Jones and Hein van Grouw (Natural History Museum, formerly British Museum of Natural History), Tony Parker (National Museums Liverpool), Jeremiah Trimble (Museum of Comparative Zoology, Harvard University), and Paul Sweet, Tom Trombone and Mary LeCroy (American Museum of Natural History) provided information on swallow specimens in their care. Catherine Levy and Jim Wiley provided additional information about the Golden Swallow in Jamaica. Susan Koenig and Mike Schwartz (Windsor Research Centre) and Catherine Levy (Kingston) provided critical logistical support. Nick Gotelli gave advice on EcoSim. Catherine Levy, Susan Koenig, Justin Proctor, Jason Townsend, and three anonymous reviewers critiqued earlier drafts of the manuscript. Ellen Alers (Smithsonian Institution Archives) and Catherine Levy helped with W. T. March correspondence. Leslie Overstreet of the Joseph F. Cullman 3rd Library of Natural History (Smithsonian Institution Libraries) provided a digital scan of the Gosse lithograph. This paper is dedicated to Errol Francis (1950-2011) for his contributions to Jamaican science. I am grateful to them all. Fieldwork was supported by the Alexander Wetmore and the James Bond funds of the Smithsonian Institution. NR 60 TC 1 Z9 1 U1 0 U2 11 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0959-2709 EI 1474-0001 J9 BIRD CONSERV INT JI Bird Conserv. Int. PD JUN PY 2014 VL 24 IS 2 BP 239 EP 251 DI 10.1017/S095927091300035X PG 13 WC Ornithology SC Zoology GA AI1IG UT WOS:000336603600010 ER PT J AU Chollett, I Canty, SWJ Box, SJ Mumby, PJ AF Chollett, Iliana Canty, Steven W. J. Box, Stephen J. Mumby, Peter J. TI Adapting to the impacts of global change on an artisanal coral reef fishery SO ECOLOGICAL ECONOMICS LA English DT Article DE Small-scale fisheries; Fuel price; Wave exposure; Climate change; Emission scenarios; Economic scenarios; Adaptation ID SOCIAL-ECOLOGICAL SYSTEMS; SMALL-SCALE FISHERIES; CLIMATE-CHANGE; SPECIES DISTRIBUTIONS; MODELS; MANAGEMENT; SUSTAINABILITY; EXPLOITATION; COMMUNITIES; HONDURAS AB When assessing future changes in fishing, research has focused on changes in the availability of the resource. Fishers' behaviour, however, also defines fishing activity, and is susceptible not only to changes in weather but also to changes in the economy, which can be faster and more ubiquitous. Using a novel modelling approach and spatially explicit predictors we identified the current drivers of artisanal fishing activity and predicted how it is likely to change in 2025 and 2035 under two climate and two economic scenarios. The model is effective at explaining the activity of fishers (AUC = 0.84) and suggests that economic variables overwhelm the importance of climate variables in influencing the decisions of fishers in our case study area (Utila, Honduras). Although future changes in the overall incidence of fishing activity are modest, decreases in the number of accessible fishing grounds with projected increases in fuel prices will increase localised fishing effort depleting fish resources near the port. Compelling adaptation strategies in the area require the intervention of the market chain to make the sale price of fish more responsive to fuel price fluctuations and changes in fishing behaviour to improve fuel efficiency, including the revival of traditional ways of fishing. (C) 2014 Elsevier B.V. All rights reserved. C1 [Chollett, Iliana; Mumby, Peter J.] Univ Exeter, Marine Spatial Ecol Lab, Coll Life & Environm Sci, Exeter EX4 4PS, Devon, England. [Chollett, Iliana; Mumby, Peter J.] Univ Queensland, Sch Biol Sci, Marine Spatial Ecol Lab, Brisbane, Qld 4072, Australia. [Canty, Steven W. J.] Ctr Estudios Marinos, Tegucigalpa, Honduras. [Box, Stephen J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Chollett, I (reprint author), Univ Exeter, Marine Spatial Ecol Lab, Coll Life & Environm Sci, Exeter EX4 4PS, Devon, England. EM i.c.chollett-ordaz@exeter.ac.uk; steve_canty@utilaecology.org; boxs@si.edu; p.j.mumby@uq.edu.au FU European Union [244161]; Pew Laureate Fellowship [2008-000330-010]; ARC Laureate Fellowship [FL0992179]; Summit Foundation [504502] FX The research leading to these results has received funding from the European Union 7th Framework programme (P7/2007-2013) under grant agreement no. 244161, Pew (grant 2008-000330-010) and ARC Laureate Fellowships (FL0992179) to PJM and the Summit Foundation (grant 504502) and Smithsonian Marine Station at Fort Pierce contribution number 949 to SJB. We are grateful to the Caribbean Community Climate Change Centre, particularly Timo Baur, for assisting in the provision of climate change data, and to Alice Rogers and two reviewers for their comments on the manuscript. NR 49 TC 5 Z9 5 U1 5 U2 48 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-8009 EI 1873-6106 J9 ECOL ECON JI Ecol. Econ. PD JUN PY 2014 VL 102 BP 118 EP 125 DI 10.1016/j.ecolecon.2014.03.010 PG 8 WC Ecology; Economics; Environmental Sciences; Environmental Studies SC Environmental Sciences & Ecology; Business & Economics GA AI2OK UT WOS:000336697600015 ER PT J AU Graves, GR AF Graves, Gary R. TI WESTERN MARSH HARRIER PREYS ON HERRING GULL SO JOURNAL OF RAPTOR RESEARCH LA English DT Letter DE Western Marsh Harrier; Circus aeruginosus; Herring Gull; Larus argentatus; predation ID CIRCUS-AERUGINOSUS; DIET; BEHAVIOR; FOOD C1 [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Graves, Gary R.] Univ Copenhagen, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC 116,POB 37012, Washington, DC 20013 USA. EM gravesg@si.edu RI publist, CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017 NR 8 TC 0 Z9 0 U1 5 U2 12 PU RAPTOR RESEARCH FOUNDATION INC PI HASTINGS PA 14377 117TH STREET SOUTH, HASTINGS, MN 55033 USA SN 0892-1016 EI 2162-4569 J9 J RAPTOR RES JI J. Raptor Res. PD JUN PY 2014 VL 48 IS 2 BP 191 EP 192 PG 2 WC Ornithology SC Zoology GA AI0RF UT WOS:000336556400011 ER PT J AU Le Borgne, JF Poretti, E Klotz, A Denoux, E Smith, HA Kolenberg, K Szabo, R Bryson, S Audejean, M Buil, C Caron, J Conseil, E Corp, L Drillaud, C de France, T Graham, K Hirosawa, K Klotz, AN Kugel, F Loughney, D Menzies, K Rodriguez, M Ruscitti, PM AF Le Borgne, J. F. Poretti, E. Klotz, A. Denoux, E. Smith, H. A. Kolenberg, K. Szabo, R. Bryson, S. Audejean, M. Buil, C. Caron, J. Conseil, E. Corp, L. Drillaud, C. de France, T. Graham, K. Hirosawa, K. Klotz, A. N. Kugel, F. Loughney, D. Menzies, K. Rodriguez, M. Ruscitti, P. M. TI Historical vanishing of the Blazhko effect of RR Lyr from the GEOS and Kepler surveys SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; stars: individual: RR Lyrae; stars: oscillations; stars: variables: RR Lyrae ID TAROT TELESCOPES; STARS; PERIOD; LIGHT; BEHAVIOR; CYCLE AB RR Lyr is one of the most studied variable stars. Its light curve has been regularly monitored since the discovery of its periodic variability in 1899. The analysis of all observed maxima allows us to identify two primary pulsation states, defined as pulsation over a long (P-0 longer than 0.56684 d) and a short (P-0 shorter than 0.56682 d) primary pulsation period. These states alternate with intervals of 13-16 yr, and are well defined after 1943. The 40.8-d periodical modulations of the amplitude and the period (i.e. the Blazhko effect) were noticed in 1916. We provide homogeneous determinations of the Blazhko period in the different primary pulsation states. The Blazhko period does not follow the variations of P-0 and suddenly diminished from 40.8 d to around 39.0 d in 1975. The monitoring of these periodicities deserved, and still deserves, a continuous and intensive observational effort. For this purpose, we have built dedicated, transportable and autonomous small instruments, Very Tiny Telescopes (VTTs), to observe the times of maximum brightness of RR Lyr. As immediate results, the VTTs recorded the last change of the P-0 state in mid-2009 and extended the time coverage of the Kepler observations, thus recording a maximum O - C amplitude of the Blazhko effect at the end of 2008, followed by the historically smallest O - C amplitude in late 2013. This decrease is still ongoing and the VTTs are ready to monitor the expected increase in the next few years. C1 [Le Borgne, J. F.; Poretti, E.; Klotz, A.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Le Borgne, J. F.; Poretti, E.; Klotz, A.] CNRS, IRAP, F-31400 Toulouse, France. [Le Borgne, J. F.; Poretti, E.; Klotz, A.; Denoux, E.; Corp, L.; Klotz, A. N.] GEOS, F-28300 Bailleau Leveque, France. [Poretti, E.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Smith, H. A.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Kolenberg, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kolenberg, K.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Szabo, R.] MTA CSFK, Konkoly Observ, H-1121 Budapest, Hungary. [Bryson, S.] NASA Ames Res Ctr, Mountain View, CA 94035 USA. [Audejean, M.] Observ Chinon, F-37500 Chinon, France. [Buil, C.] Observ Castanet Tolosan, F-31320 Castanet Tolosan, France. [Caron, J.; Kugel, F.] Observ Chante Perdrix, F-04150 Banon, France. [Conseil, E.; Drillaud, C.] Observ Strasbourg, AFOEV, F-67000 Strasbourg, France. [Corp, L.; de France, T.; Graham, K.; Menzies, K.] AAVSO, Cambridge, MA 02138 USA. [Hirosawa, K.] VSOLJ, Tsukuba, Ibaraki 3050035, Japan. [Loughney, D.] British Astron Assoc, Variable Star Sect BAA VSS, London W1J 0DU, England. [Ruscitti, P. M.] Osservatorio Astron B Occhialini, I-67041 Aielli, AQ, Italy. RP Le Borgne, JF (reprint author), Univ Toulouse, UPS OMP, IRAP, Toulouse, France. EM jleborgne@irap.omp.eu OI Poretti, Ennio/0000-0003-1200-0473; Szabo, Robert/0000-0002-3258-1909 FU NASA's Science Mission Directorate; Hungarian Academy of Science; Hungarian OTKA grant [K83790]; KTIA [URKUT_10-1-2011-0019]; European Community [269194]; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences FX Funding for the Kepler Discovery Mission is provided by NASA's Science Mission Directorate. The Kepler Team and the Kepler Guest Observer Office are recognized for helping to make this mission and these data possible. EP acknowledges Observatoire Midi-Pyrenees for the two-month grant allocated in 2013 October and November, which allowed him to work at the Institut de Recherche en Astrophysique et Planetologie in Toulouse, France. The present study has used the SIMBAD data base operated at the Centre de Donnees Astronomiques (Strasbourg, France) and the GEOS RR Lyr data base hosted by IRAP (OMP-UPS, Toulouse, France). This study has been supported by the Lendulet-2009 Young Researchers Programme of the Hungarian Academy of Science, the Hungarian OTKA grant K83790 and the KTIA URKUT_10-1-2011-0019 grant. The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 269194 (IRSES/ASK). RSz was supported by the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. The basic ideas of the VTT project have been sketched during several GEOS meetings, and fruitful discussions with R. Boninsegna, M. Dumont, J. Fabregat, F. Fumagalli, D. Husar, J. Remis, J. Vandenbroere and J. M. Vilalta are gratefully acknowledged. NR 39 TC 9 Z9 9 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 JUN PY 2014 VL 441 IS 2 BP 1435 EP 1443 DI 10.1093/mnras/stu671 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH9WC UT WOS:000336494800039 ER PT J AU Keto, E Burkert, A AF Keto, Eric Burkert, Andreas TI From filaments to oscillating starless cores SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; radiative transfer; ISM: clouds; ISM: kinematics and dynamics ID MOLECULAR CLOUD CORES; DYNAMICAL STATE; DARK CLOUD; BARNARD 68; EMISSION; GLOBULE AB Long-wavelength sonic oscillations are observed or inferred in many of the small, dark molecular clouds, the starless cores, that are the precursors to protostars. The oscillations provide significant internal energy and the time-scale for their dissipation may control the rate of star formation in starless cores. Despite their importance, their origin is unknown. We explore one hypothesis that the oscillations develop as a starless core forms from a filament. We model this process with a numerical hydrodynamic simulation and generate synthetic molecular line observations with a radiative transfer simulation. Comparison with actual observations shows general agreement suggesting that the proposed mechanism is viable. C1 [Keto, Eric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02420 USA. [Burkert, Andreas] Univ Munich, D-81679 Munich, Germany. RP Keto, E (reprint author), Harvard Smithsonian Ctr Astrophys, 160 Garden St, Cambridge, MA 02420 USA. EM keto@cfa.harvard.edu FU German Science Foundation [1573] FX AB thanks the Harvard-Smithsonian Center for Astrophysics for their hospitality during multiple visits. The research of AB is supported by the priority programme 1573 'Physics of the Interstellar Medium' of the German Science Foundation. NR 33 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 PY 2014 VL 441 IS 2 BP 1468 EP 1473 DI 10.1093/mnras/stu379 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH9WC UT WOS:000336494800042 ER PT J AU Parker, ML Walton, DJ Fabian, AC Risaliti, G AF Parker, M. L. Walton, D. J. Fabian, A. C. Risaliti, G. TI PCA of PCA: principal component analysis of partial covering absorption in NGC 1365 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: individual: NGC 1365; galaxies: individual: MCG-6-30-15; galaxies: Seyfert ID RAY SPECTRAL VARIABILITY; XMM-NEWTON; BLACK-HOLE; MCG-6-30-15; REFLECTION; DISCOVERY; LAGS; LINE AB We analyse 400 ks of XMM-Newton data on the active galactic nucleus NGC 1365 using principal component analysis (PCA) to identify model-independent spectral components. We find two significant components and demonstrate that they are qualitatively different from those found in MCG-6-30-15 using the same method. As the variability in NGC 1365 is known to be due to changes in the parameters of a partial covering neutral absorber, this shows that the same mechanism cannot be the driver of variability in MCG-6-30-15. By examining intervals where the spectrum shows relatively low absorption we separate the effects of intrinsic source variability, including signatures of relativistic reflection, from variations in the intervening absorption. We simulate the principal components produced by different physical variations, and show that PCA provides a clear distinction between absorption and reflection as the drivers of variability in AGN spectra. The simulations are shown to reproduce the PCA spectra of both NGC 1365 and MCG-6-30-15, and further demonstrate that the dominant cause of spectral variability in these two sources requires a qualitatively different mechanism. C1 [Parker, M. L.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Walton, D. J.] CALTECH, Pasadena, CA 91125 USA. [Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Parker, ML (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM mlparker@ast.cam.ac.uk OI Risaliti, Guido/0000-0002-3556-977X FU Science and Technology Facilities Council (STFC) FX The authors would like to thank the anonymous referee for their helpful comments. MLP acknowledges financial support from the Science and Technology Facilities Council (STFC). NR 24 TC 8 Z9 8 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 PY 2014 VL 441 IS 2 BP 1817 EP 1824 DI 10.1093/mnras/stu712 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH9WC UT WOS:000336494800066 ER PT J AU Hartman, JD Bakos, GA Torres, G Kovacs, G Johnson, JA Howard, AW Marcy, GW Latham, DW Bieryla, A Buchhave, LA Bhatti, W Beky, B Csubry, Z Penev, K De Val-Borro, M Noyes, RW Fischer, DA Esquerdo, GA Everett, M Szklenar, T Zhou, G Bayliss, D Shporer, A Fulton, BJ Sanchis-Ojeda, R Falco, E Lazar, J Papp, I Sari, P AF Hartman, J. D. Bakos, G. A. Torres, G. Kovacs, G. Johnson, J. A. Howard, A. W. Marcy, G. W. Latham, D. W. Bieryla, A. Buchhave, L. A. Bhatti, W. Beky, B. Csubry, Z. Penev, K. De Val-Borro, M. Noyes, R. W. Fischer, D. A. Esquerdo, G. A. Everett, M. Szklenar, T. Zhou, G. Bayliss, D. Shporer, A. Fulton, B. J. Sanchis-Ojeda, R. Falco, E. Lazar, J. Papp, I. Sari, P. TI HAT-P-44b, HAT-P-45b, AND HAT-P-46b: THREE TRANSITING HOT JUPITERS IN POSSIBLE MULTI-PLANET SYSTEMS SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HAT-P-44, HAT-P-45, HAT-P-46); techniques: photometric; techniques: spectroscopic ID ECCENTRIC ORBIT; GIANT PLANETS; BRIGHT STAR; LONG-PERIOD; MULTIPLANET SYSTEMS; KEPLER FIELD; HOST STARS; K-DWARF; SEARCH; STELLAR AB We report the discovery by the HATNet survey of three new transiting extrasolar planets orbiting moderately bright (V = 13.2, 12.8, and 11.9) stars. The planets have orbital periods of 4.3012, 3.1290, and 4.4631 days, masses of 0.35, 0.89, and 0.49 M-J, and radii of 1.24, 1.43, and 1.28 R-J. The stellar hosts have masses of 0.94, 1.26, and 1.28 M-circle dot . Each system shows significant systematic variations in its residual radial velocities, indicating the possible presence of additional components. Based on its Bayesian evidence, the preferred model for HAT-P-44 consists of two planets, including the transiting component, with the outer planet having a period of 872 days, eccentricity of 0.494 +/- 0.081, and a minimum mass of 4.0 M-J. Due to aliasing we cannot rule out alternative solutions for the outer planet having a period of 220 days or 438 days. For HAT-P-45, at present there is not enough data to justify the additional free parameters included in a multi-planet model; in this case a single-planet solution is preferred, but the required jitter of 22.5 +/- 6.3 m s(-1) is relatively high for a star of this type. For HAT-P-46 the preferred solution includes a second planet having a period of 78 days and a minimum mass of 2.0 M-J, however the preference for this model over a single-planet model is not very strong. While substantial uncertainties remain as to the presence and/or properties of the outer planetary companions in these systems, the inner transiting planets are well characterized with measured properties that are fairly robust against changes in the assumed models for the outer planets. Continued radial velocity monitoring is necessary to fully characterize these three planetary systems, the properties of which may have important implications for understanding the formation of hot Jupiters. C1 [Hartman, J. D.; Bakos, G. A.; Bhatti, W.; Csubry, Z.; Penev, K.; De Val-Borro, M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Torres, G.; Latham, D. W.; Bieryla, A.; Beky, B.; Noyes, R. W.; Esquerdo, G. A.; Falco, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kovacs, G.] Konkoly Observ Budapest, Budapest, Hungary. [Kovacs, G.] Univ N Dakota, Dept Phys & Astrophys, Grand Forks, ND 58202 USA. [Johnson, J. A.; Shporer, A.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Howard, A. W.; Fulton, B. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Fischer, D. A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Everett, M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Szklenar, T.; Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, H-1461 Budapest, Hungary. [Zhou, G.; Bayliss, D.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Shporer, A.] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Shporer, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Sanchis-Ojeda, R.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Hartman, JD (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. EM jhartman@astro.princeton.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Penev, Kaloyan/0000-0003-4464-1371; Buchhave, Lars A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166 FU NASA [NNG04GN74G, NNX08AF23G, NNX13AJ15G, NNX09AB29G, NNX09AF59G, N154Hr, N108Hr]; NSF [AST-1108686]; Kepler Mission under NASA [NCC2-1390]; Hungarian Scientific Research Foundation (OTKA) [K-81373]; NOAO [A284Hr] FX HATNet operations have been funded in part by NASA grants NNG04GN74G, NNX08AF23G, and NNX13AJ15G. J.D.H., G.A.B., and W.B. received partial support from NSF grant AST-1108686. G.A.B., Z.C., and K. P. acknowledge partial support from NASA grant NNX09AB29G. G.T. acknowledges partial support from NASA grant NNX09AF59G. We acknowledge partial support also from the Kepler Mission under NASA Co-operative Agreement NCC2-1390 (PI: D.W.L.). G.K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-81373. This research has made use of Keck telescope time granted through NOAO (program A284Hr) and NASA (N154Hr, N108Hr). This paper uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope. Data presented in this paper are based on observations obtained at the HAT station at the Submillimeter Array of SAO, and the HAT station at the Fred Lawrence Whipple Observatory of SAO. We also thank Mount Stromlo Observatory and Siding Spring Observatory for granting us time on the ANU 2.3 m telescope. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at http://www.exoplanets.org. NR 68 TC 10 Z9 10 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUN PY 2014 VL 147 IS 6 AR 128 DI 10.1088/0004-6256/147/6/128 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6TC UT WOS:000336262600004 ER PT J AU Janes, K Barnes, SA Meibom, S Hoq, S AF Janes, Kenneth Barnes, Sydney A. Meibom, Soren Hoq, Sadia TI OPEN CLUSTERS IN THE KEPLER FIELD. II. NGC 6866 SO ASTRONOMICAL JOURNAL LA English DT Article DE Hertzsprung-Russell and C-M diagrams; methods: data analysis; open clusters and associations: individual (NGC 6866) ID COLOR-MAGNITUDE DIAGRAMS; VARIABLE-STARS; CCD PHOTOMETRY; PARAMETERS; ISOCHRONES; AGE AB We have developed a maximum-likelihood procedure to fit theoretical isochrones to the observed cluster color-magnitude diagrams of NGC 6866, an open cluster in the Kepler spacecraft field of view. The Markov chain Monte Carlo algorithm permits exploration of the entire parameter space of a set of isochrones to find both the best solution and the statistical uncertainties. For clusters in the age range of NGC 6866 with few, if any, red giant members, a purely photometric determination of the cluster properties is not well-constrained. Nevertheless, based on our UBVRI photometry alone, we have derived the distance, reddening, age, and metallicity of the cluster and established estimates for the binary nature and membership probability of individual stars. We derive the following values for the cluster properties: (m - M)(v) = 10.98 +/- 0.24, E(B - V) = 0.16 +/- 0.04 (so the distance = 1250 pc), age = 705 +/- 170 Myr, and Z = 0.014 +/- 0.005. C1 [Janes, Kenneth; Hoq, Sadia] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Barnes, Sydney A.] Leibniz Inst Astrophys, Potsdam, Germany. [Meibom, Soren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barnes, Sydney A.] Space Sci Inst, Boulder, CO 80301 USA. RP Janes, K (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. FU Boston University; Lowell Observatory; Barnes family; LoMonaco family; NASA [NNX09AH18A] FX We acknowledge the financial and technical support from Boston University and the Lowell Observatory. S.A.B is grateful for financial support from the Barnes and LoMonaco families and thanks the Flagstaff Public Library for providing a serene working environment during a crucial phase of this work. S.M. acknowledges support from NASA cooperative agreement NNX09AH18A (the Kepler Cluster Study). NR 20 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 JUN PY 2014 VL 147 IS 6 AR 139 DI 10.1088/0004-6256/147/6/139 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6TC UT WOS:000336262600015 ER PT J AU Kraus, AL Shkolnik, EL Allers, KN Liu, MC AF Kraus, Adam L. Shkolnik, Evgenya L. Allers, Katelyn N. Liu, Michael C. TI A STELLAR CENSUS OF THE TUCANA-HOROLOGIUM MOVING GROUP SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: spectroscopic; open clusters and associations: individual (Tucana-Horologium); stars: activity; stars: kinematics and dynamics; stars: low-mass; stars: pre-main sequence ID LOW-MASS STARS; LITHIUM DEPLETION BOUNDARY; TW-HYDRAE ASSOCIATION; DIGITAL SKY SURVEY; ETA-CHAMAELEONTIS CLUSTER; GALAXY-EVOLUTION-EXPLORER; BROWN DWARF CANDIDATES; MAIN-SEQUENCE STARS; NEARBY YOUNG STARS; BETA-PICTORIS AB We report the selection and spectroscopic confirmation of 129 new late-type (SpT = K3-M6) members of the Tucana-Horologium moving group, a nearby (d similar to 40 pc), young (tau similar to 40 Myr) population of comoving stars. We also report observations for 13 of the 17 known Tuc-Hor members in this spectral type range, and that 62 additional candidates are likely to be unassociated field stars; the confirmation frequency for new candidates is therefore 129/191 = 67%. We have used radial velocities, Ha emission, and Li-6708 absorption to distinguish between contaminants and bona fide members. Our expanded census of Tuc-Hor increases the known population by a factor of similar to 3 in total and by a factor of similar to 8 for members with SpT >= K3, but even so, the K-M dwarf population of Tuc-Hor is still markedly incomplete. Our expanded census allows for a much more detailed study of Tuc-Hor than was previously feasible. The spatial distribution of members appears to trace a two-dimensional sheet, with a broad distribution in X and Y, but a very narrow distribution (+/- 5 pc) in Z. The corresponding velocity distribution is very small, with a scatter of +/- 1.1 km s(-1) about the mean UVW velocity for stars spanning the entire 50 pc extent of Tuc-Hor. We also show that the isochronal age (tau similar to 20-30 Myr) and the lithium depletion boundary age (tau similar to 40 Myr) disagree, following the trend in other pre-main-sequence populations for isochrones to yield systematically younger ages. The H alpha emission line strength follows a trend of increasing equivalent width with later spectral type, as is seen for young clusters. We find that moving group members have been depleted of measurable lithium for spectral types of K7.0-M4.5. None of our targets have significant infrared excesses in the WISE W3 band, yielding an upper limit on warm debris disks of F < 0.7%. Finally, our purely kinematic and color-magnitude selection procedure allows us to test the efficiency and completeness for activity-based selection of young stars. We find that 60% of K-M dwarfs in Tuc-Hor do not have ROSAT counterparts and would have been omitted in X-ray-selected samples. In contrast, GALEX UV-selected samples using a previously suggested criterion for youth achieve completeness of 77% and purity of 78%, and we suggest new SpT-dependent selection criteria that will yield > 95% completeness for tau similar to 40 Myr populations with GALEX data available. C1 [Kraus, Adam L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Kraus, Adam L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shkolnik, Evgenya L.] Lowell Observ, Flagstaff, AZ 86001 USA. [Allers, Katelyn N.] Bucknell Univ, Dept Phys & Astron, Lewisburg, PA 17837 USA. [Liu, Michael C.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. RP Kraus, AL (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. FU Clay fellowship FX The authors thank Jason Curtis for obtaining many excellent observations as part of a time trade, Jason Wright for useful suggestions regarding the optimal map projection for plotting stars on the celestial sphere, and the anonymous referee for a helpful and thorough critique of the paper. A.L.K. was supported in part by a Clay fellowship. NR 92 TC 41 Z9 41 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUN PY 2014 VL 147 IS 6 AR 146 DI 10.1088/0004-6256/147/6/146 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6TC UT WOS:000336262600022 ER PT J AU Lacy, CHS Torres, G Fekel, FC Muterspaugh, MW AF Lacy, Claud H. Sandberg Torres, Guillermo Fekel, Francis C. Muterspaugh, Matthew W. TI ABSOLUTE PROPERTIES OF THE ECLIPSING BINARY STAR AP ANDROMEDAE SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; binaries: spectroscopic; stars: fundamental parameters; stars: individual (AP And) ID SPECTROSCOPIC BINARIES; BOLOMETRIC CORRECTIONS; RADIAL-VELOCITIES; Y-2 ISOCHRONES; LIGHT CURVES; EXTINCTION; TELESCOPE; ACCURACY; MODELS; ORBITS AB AP And is a well-detached F5 eclipsing binary star for which only a very limited amount of information was available before this publication. We have obtained very extensive measurements of the light curve (19,097 differential V magnitude observations) and a radial velocity curve (83 spectroscopic observations) which allow us to fit orbits and determine the absolute properties of the components very accurately: masses of 1.277 +/- 0.004 and 1.251 +/- 0.004 M-circle dot, radii of 1.233 +/- 0.006 and 1.1953 +/- 0.005 R-circle dot, and temperatures of 6565 +/- 150 K and 6495 +/- 150 K. The distance to the system is about 400 +/- 30 pc. Comparison with the theoretical properties of the stellar evolutionary models of the Yonsei-Yale series of Yi et al. shows good agreement between the observations and the theory at an age of about 500 Myr and a slightly sub-solar metallicity. C1 [Lacy, Claud H. Sandberg] Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fekel, Francis C.; Muterspaugh, Matthew W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. RP Lacy, CHS (reprint author), Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. EM clacy@uark.edu; gtorres@cfa.harvard.edu; fekel@evans.tsuniv.edu; matthew1@coe.tsuniv.edu OI Lacy, Claud/0000-0002-0455-679X FU NSF [AST-1007992]; NSF through Major Research Instrumentation Program [1039522]; state of Tennessee through Centers of Excellence programs FX The authors wish to thank Bill Neely who operates and maintains the NFO WebScope for the Consortium, and who handles preliminary processing of the images and their distribution. Thanks also to University of Arkansas undergraduate student Craig Heinrich for initial analysis of the URSA photometry and preliminary radial velocities. We thank P. Berlind, Z. Berta, M. L. Calkins, G. A. Esquerdo, G. Furesz, D. W. Latham, R. P. Stefanik, and S. Tang for help with the spectroscopic observations of AP And on Mount Hopkins, as well as R. J. Davis and J. Mink for maintaining the echelle databases at the CfA. G. T. acknowledges partial support through NSF grant AST-1007992. The research at Tennessee State University was made possible by NSF support through grant 1039522 of the Major Research Instrumentation Program. In addition, astronomy at Tennessee State University is supported by the state of Tennessee through its Centers of Excellence programs. We wish to thank an anonymous referee of this article for suggestions that improved the clarity of our paper and expanded some of our discussion. NR 54 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 JUN PY 2014 VL 147 IS 6 AR 148 DI 10.1088/0004-6256/147/6/148 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6TC UT WOS:000336262600024 ER PT J AU Zhou, G Bayliss, D Penev, K Bakos, GA Hartman, JD Jordan, A Mancini, L Mohler, M Csubry, Z Ciceri, S Brahm, R Rabus, M Buchhave, L Henning, T Suc, V Espinoza, N Beky, B Noyes, RW Schmidt, B Butler, RP Shectman, S Thompson, I Crane, J Sato, B Csak, B Lazar, J Papp, I Sari, P Nikolov, N AF Zhou, G. Bayliss, D. Penev, K. Bakos, G. A. Hartman, J. D. Jordan, A. Mancini, L. Mohler, M. Csubry, Z. Ciceri, S. Brahm, R. Rabus, M. Buchhave, L. Henning, T. Suc, V. Espinoza, N. Beky, B. Noyes, R. W. Schmidt, B. Butler, R. P. Shectman, S. Thompson, I. Crane, J. Sato, B. Csak, B. Lazar, J. Papp, I. Sari, P. Nikolov, N. TI HATS-5b: A TRANSITING HOT SATURN FROM THE HATSouth SURVEY SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: individual (HATS-5, GSC 5897-00933); techniques: photometric; techniques: spectroscopic ID HUBBLE-SPACE-TELESCOPE; EXTRASOLAR PLANET; TRANSMISSION SPECTRUM; ATMOSPHERIC HAZE; GIANT PLANETS; OKAYAMA HIDES; IODINE CELLS; HOST STARS; SUBARU HDS; STELLAR AB We report the discovery of HATS-5b, a transiting hot Saturn orbiting a G-type star, by the HATSouth survey. HATS-5b has a mass of Mp approximate to 0.24 M-J, radius of R-p approximate to 0.91 R-J, and transits its host star with a period of P approximate to 4.7634 days. The radius of HATS-5b is consistent with both theoretical and empirical models. The host star has a V-band magnitude of 12.6, mass of 0.94 M-circle dot, and radius of 0.87 R-circle dot. The relatively high scale height of HATS-5b and the bright, photometrically quiet host starmake this planet a favorable target for future transmission spectroscopy follow-up observations. We reexamine the correlations in radius, equilibrium temperature, and metallicity of the close-in gas giants and find hot Jupiter-mass planets to exhibit the strongest dependence between radius and equilibrium temperature. We find no significant dependence in radius and metallicity for the close-in gas giant population. C1 [Zhou, G.; Bayliss, D.; Schmidt, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Penev, K.; Bakos, G. A.; Hartman, J. D.; Csubry, Z.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Penev, K.; Bakos, G. A.; Hartman, J. D.; Csubry, Z.; Beky, B.; Noyes, R. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jordan, A.; Brahm, R.; Rabus, M.; Suc, V.; Espinoza, N.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 7820436, Chile. [Mancini, L.; Mohler, M.; Ciceri, S.; Henning, T.; Csak, B.; Nikolov, N.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Buchhave, L.] Univ Copenhagen, Niels Bohr Inst, DK-1168 Copenhagen, Denmark. [Butler, R. P.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Shectman, S.; Thompson, I.; Crane, J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Sato, B.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. [Nikolov, N.] Univ Exeter, Sch Phys, Astrophys Grp, Exeter EX4 4QL, Devon, England. RP Zhou, G (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. EM george.zhou@anu.edu.au RI Butler, Robert/B-1125-2009; OI Jordan, Andres/0000-0002-5389-3944; Penev, Kaloyan/0000-0003-4464-1371; Schmidt, Brian/0000-0001-6589-1287; Buchhave, Lars A./0000-0003-1605-5666; Nikolov, Nikolay/0000-0002-6500-3574; Hartman, Joel/0000-0001-8732-6166 FU NSF MRI grant [NSF/AST-0723074]; NASA [NNX12AH91H]; ARC Laureate Fellowship Grant [FL0992131]; FONDECYT project [1130857, BASAL CATA PFB-06]; Millennium Institute of Astrophysics (MAS) [IC120009]; Millennium Science Initiative [P10-022-F]; FONDECYT postdoctoral fellowship [3120097]; CONICYT-PCHA/Doctorado Nacional and Fondecyt project [1130857]; Robert Martin Ayers Sciences Fund; Chilean Ministry of Economy; [NSF/AST-1108686]; [P087. A-9014(A), P088. A-9008(A), P089. A-9008(A), P087. C-0508(A), and P089. A-9006(A)] FX Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074, operations are supported by NASA grant NNX12AH91H, and follow-up observations receive partial support from grant NSF/AST-1108686. Work at the Australian National University is supported by ARC Laureate Fellowship Grant FL0992131. Follow-up observations with the ESO 2.2 m/FEROS instrument were performed under MPI guaranteed time (P087.A-9014(A), P088. A-9008(A), P089. A-9008(A)) and Chilean time (P087.C-0508(A)). A. J. acknowledges support from FONDECYT project 1130857, BASAL CATA PFB-06, and projects IC120009 "Millennium Institute of Astrophysics (MAS)" and P10-022-F of the Millennium Science Initiative, Chilean Ministry of Economy. V. S. acknowledges support form BASAL CATA PFB-06. M. R. acknowledges support from FONDECYT postdoctoral fellowship No3120097. R. B. and N. E. acknowledge support from CONICYT-PCHA/Doctorado Nacional and Fondecyt project 1130857. This work is based on observations made with ESO Telescopes at the La Silla Observatory under program IDs P087. A-9014(A), P088. A-9008(A), P089. A-9008(A), P087. C-0508(A), and P089. A-9006(A). We acknowledge the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund, and the SIMBAD database, operated at CDS, Strasbourg, France. Operations at the MPG/ESO 2.2 m telescope are jointly performed by the Max Planck Gesellschaft and the European Southern Observatory. The imaging system GROND has been built by the high-energy group of MPE in collaboration with the LSW Tautenburg and ESO. We thank Rgis Lachaume for his technical assistance during the observations at the MPG/ESO 2.2 m telescope. Australian access to the Magellan Telescopes was supported through the National Collaborative Research Infrastructure Strategy of the Australian Federal Government. We thank Albert Jahnke, Toni Hanke (HESS), and Peter Conroy (MSO) for their contributions to the HATSouth project. NR 60 TC 8 Z9 8 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 JUN PY 2014 VL 147 IS 6 AR 144 DI 10.1088/0004-6256/147/6/144 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6TC UT WOS:000336262600020 ER PT J AU Aliu, E Archambault, S Aune, T Behera, B Beilicke, M Benbow, W Berger, K Bird, R Buckley, JH Bugaev, V Cardenzana, JV Cerruti, M Chen, X Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Dumm, J Dwarkadas, VV Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fleischhack, H Fortin, P Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Kaaret, P Kertzman, M Khassen, Y Kieda, D Krennrich, F Kumar, S Lang, MJ Madhavan, AS Maier, G McCann, AJ Meagher, K Millis, J Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Pandel, D Park, N Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Rajotte, J Ratliff, G Reyes, LC Reynolds, PT Richards, GT Roache, E Rousselle, J Sembroski, GH Shahinyan, K Sheidaei, F Smith, AW Staszak, D Telezhinsky, I Tsurusaki, K Tucci, JV Tyler, J Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Ward, JE Weinstein, A Welsing, R Wilhelm, A AF Aliu, E. Archambault, S. Aune, T. Behera, B. Beilicke, M. Benbow, W. Berger, K. Bird, R. Buckley, J. H. Bugaev, V. Cardenzana, J. V. Cerruti, M. Chen, X. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Dumm, J. Dwarkadas, V. V. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fleischhack, H. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krennrich, F. Kumar, S. Lang, M. J. Madhavan, A. S. Maier, G. McCann, A. J. Meagher, K. Millis, J. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Pandel, D. Park, N. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Rajotte, J. Ratliff, G. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Rousselle, J. Sembroski, G. H. Shahinyan, K. Sheidaei, F. Smith, A. W. Staszak, D. Telezhinsky, I. Tsurusaki, K. Tucci, J. V. Tyler, J. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Ward, J. E. Weinstein, A. Welsing, R. Wilhelm, A. TI INVESTIGATING THE TeV MORPHOLOGY OF MGRO J1908+06 WITH VERITAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: general; gamma-ray burst: individual (MGRO J1908+06, VER J1907+062); pulsars: individual (PSR J1907+0602); ISM: supernova remnants ID PULSAR WIND NEBULA; GAMMA-RAY EMISSION; GALACTIC PLANE; PSR J1907+0602; REMNANT; G40.5-0.5; MILAGRO; ARRAY AB We report on deep observations of the extended TeV gamma-ray source MGRO J1908+06 made with the VERITAS very high energy gamma-ray observatory. Previously, the TeV emission has been attributed to the pulsar wind nebula (PWN) of the Fermi-LAT pulsar PSR J1907+0602. We detect MGRO J1908+06 at a significance level of 14 standard deviations (14 sigma) and measure a photon index of 2.20 +/- 0.10(stat) +/- 0.20(sys). The TeV emission is extended, covering the region near PSR J1907+0602 and also extending toward SNR G40.5-0.5. When fitted with a two-dimensional Gaussian, the intrinsic extension has a standard deviation of sigma(src) = 0 degrees.44 +/- 0 degrees.02. In contrast to other TeV PWNe of similar age in which the TeV spectrum softens with distance from the pulsar, the TeV spectrum measured near the pulsar location is consistent with that measured at a position near the rim of G40.5-0.5, 0 degrees.33 away. C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Aune, T.; Ong, R. A.; Popkow, A.; Rousselle, J.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Behera, B.; Chen, X.; Federici, S.; Fleischhack, H.; Maier, G.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.; Wilhelm, A.] DESY, D-15738 Zeuthen, Germany. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Ward, J. E.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Collins-Hughes, E.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cardenzana, J. V.; Humensky, T. B.; Krennrich, F.; Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Federici, S.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.; Ratliff, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Hughes, G.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Dwarkadas, V. V.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Furniss, A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Furniss, A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Gall, D.; Griffiths, S. T.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Kieda, D.; Sheidaei, F.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [McCann, A. J.; Otte, A. N.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Meagher, K.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Meagher, K.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Pandel, D.] Grand Valley State Univ, Dept Phys, Allendale, MI 49401 USA. [Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Aliu, E (reprint author), Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. RI Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755; Cui, Wei/0000-0002-6324-5772; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation and the Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K FX We thank Ji Yang of the Chinese Academy of Sciences' Purple Mountain Observatory for providing the CO maps and the anonymous referee for providing useful comments. This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 40 TC 3 Z9 3 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2014 VL 787 IS 2 AR 166 DI 10.1088/0004-637X/787/2/166 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700071 ER PT J AU Andrews, SM Chandler, CJ Isella, A Birnstiel, T Rosenfeld, KA Wilner, DJ Perez, LM Ricci, L Carpenter, JM Calvet, N Corder, SA Deller, AT Dullemond, CP Greaves, JS Harris, RJ Henning, T Kwon, W Lazio, J Linz, H Mundy, LG Sargent, AI Storm, S Testi, L AF Andrews, Sean M. Chandler, Claire J. Isella, Andrea Birnstiel, T. Rosenfeld, K. A. Wilner, D. J. Perez, L. M. Ricci, L. Carpenter, J. M. Calvet, N. Corder, S. A. Deller, A. T. Dullemond, C. P. Greaves, J. S. Harris, R. J. Henning, Th. Kwon, W. Lazio, J. Linz, H. Mundy, L. G. Sargent, A. I. Storm, S. Testi, L. TI RESOLVED MULTIFREQUENCY RADIO OBSERVATIONS OF GG Tau SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; protoplanetary disks; radio continuum: planetary systems; stars: individual (GG Tau) ID PROTOPLANETARY ACCRETION DISKS; YOUNG STELLAR OBJECTS; STAR-FORMING REGION; DUST GRAIN-SIZE; CIRCUMSTELLAR DISKS; CIRCUMBINARY DISK; TRANSITION DISK; TEMPERATURE-GRADIENT; MILLIMETER EMISSION; OPTICAL-CONSTANTS AB We present subarcsecond resolution observations of continuum emission associated with the GG Tau quadruple star system at wavelengths of 1.3, 2.8, 7.3, and 50 mm. These data confirm that the GG Tau A binary is encircled by a circumbinary ring at a radius of 235 AU with a FWHM width of similar to 60 AU. We find no clear evidence for a radial gradient in the spectral shape of the ring, suggesting that the particle size distribution is spatially homogeneous on angular scales greater than or similar to 0 ''.1. A central point source, likely associated with the primary component (GG Tau Aa), exhibits a composite spectrum from dust and free-free emission. Faint emission at 7.3 mm is observed toward the low-mass star GG Tau Ba, although its origin remains uncertain. Using these measurements of the resolved, multifrequency emission structure of the GG Tau A system, models of the far-infrared to radio spectrum are developed to place constraints on the grain size distribution and dust mass in the circumbinary ring. The non-negligible curvature present in the ring spectrum implies a maximum particle size of 1-10 mm, although we are unable to place strong constraints on the distribution shape. The corresponding dust mass is 30-300 M-circle plus, at a temperature of 20-30 K. We discuss how this significant concentration of relatively large particles in a narrow ring at a large radius might be produced in a local region of higher gas pressures (i.e., a particle "trap") located near the inner edge of the circumbinary disk. C1 [Andrews, Sean M.; Birnstiel, T.; Rosenfeld, K. A.; Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chandler, Claire J.; Perez, L. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Isella, Andrea; Ricci, L.; Carpenter, J. M.; Sargent, A. I.] CALTECH, Pasadena, CA 91125 USA. [Calvet, N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Corder, S. A.] Joint ALMA Observ, Santiago, Chile. [Deller, A. T.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Dullemond, C. P.] Heidelberg Univ, Ctr Astron, Heidelberg, Germany. [Greaves, J. S.] Univ St Andrews, St Andrews KY16 9SS, Fife, Scotland. [Harris, R. J.] Univ Illinois, Dept Astronony, Urbana, IL 61810 USA. [Henning, Th.; Linz, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kwon, W.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Lazio, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA. [Mundy, L. G.; Storm, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Testi, L.] European So Observ, Garching, Germany. [Testi, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. RP Andrews, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sandrews@cfa.harvard.edu OI Dullemond, Cornelis/0000-0002-7078-5910; Deller, Adam/0000-0001-9434-3837 FU NASA [NNX12AJ04G]; NSF [AST-1109334]; National Science Foundation; CARMA partner universities FX We thank Mark Reid for valuable discussions about data modeling and an anonymous referee for helpful suggestions. S.M.A. and T.B. acknowledge support from NASA Origins of Solar Systems grant NNX12AJ04G. A.I., L.M.P., and J.M.C. acknowledge support from NSF award AST-1109334. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. The VLA is run by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 97 TC 14 Z9 14 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2014 VL 787 IS 2 AR 148 DI 10.1088/0004-637X/787/2/148 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700053 ER PT J AU Battersby, C Ginsburg, A Bally, J Longmore, S Dunham, M Darling, J AF Battersby, Cara Ginsburg, Adam Bally, John Longmore, Steve Dunham, Miranda Darling, Jeremy TI THE ONSET OF MASSIVE STAR FORMATION: THE EVOLUTION OF TEMPERATURE AND DENSITY STRUCTURE IN AN INFRARED DARK CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; H II regions; ISM: kinematics and dynamics; radio lines: ISM; stars: formation ID GALACTIC RING SURVEY; REMNANT 3C 391; LARGE ARRAY OBSERVATIONS; HI-GAL SURVEY; MOLECULAR CLOUDS; PHYSICAL-PROPERTIES; METHANOL MASERS; FORMING REGIONS; SUPERNOVA-REMNANTS; INITIAL CONDITIONS AB We present new NH3 (1, 1), (2, 2), and (4, 4) observations from the Karl G. Jansky Very Large Array compiled with work in the literature to explore the range of conditions observed in young, massive star-forming regions. To sample the effects of evolution independent from those of distance/resolution, abundance, and large-scale environment, we compare clumps in different evolutionary stages within a single infrared dark cloud (IRDC), G32.02+0.06. We find that the early stages of clustered star formation are characterized by dense, parsec-scale filamentary structures interspersed with complexes of dense cores (<0.1 pc cores clustered in complexes separated by similar to 1 pc) with masses from about 10 to 100 M-circle dot. The most quiescent core is the most extended while the star forming cores are denser and more compact, showing very similar column density structure before and shortly after the onset of massive star formation, with peak surface densities Sigma greater than or similar to 1 g cm(-2). Quiescent cores and filaments show smoothly varying temperatures from 10 to 20 K, rising to over 40 K in star-forming cores. We calculate virial parameters for 16 cores and find that the level of support provided by turbulence is generally insufficient to support them against gravitational collapse (alpha(vir) similar to 0.6). The star-forming filaments show smooth velocity fields, punctuated by discontinuities at the sites of active star formation. We discuss the massive molecular filament (M similar to 10(5) M-circle dot, length >60 pc) hosting the IRDC, hypothesizing that it may have been shaped by previous generations of massive stars. C1 [Battersby, Cara] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Battersby, Cara; Ginsburg, Adam; Bally, John; Darling, Jeremy] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Ginsburg, Adam] European So Observ, D-85748 Garching, Germany. [Longmore, Steve] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Dunham, Miranda] Yale Univ, Dept Astron, New Haven, CT 06520 USA. RP Battersby, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Ginsburg, Adam/0000-0001-6431-9633; Darling, Jeremy/0000-0003-2511-2060 FU National Science Foundation [AST-9800334, AST-0098562, AST-0100793, AST-0228993, AST-0507657]; Italian Space Agency [I/038/080/0] FX We thank the referee for comments which have improved the quality of this manuscript. We thank Rick White and the MAGPIS team for their assistance understanding continuum fluxes of the free-free source. We thank Roberto Galvan Madrid for comments on an early draft of this paper. This work has made use of the GLIMPSE and MIPSGAL surveys, and we thank those teams for their help and support. We would like to thank the staff at VLA for their assistance. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This publication makes use of molecular line data from the Boston University-FCRAO Galactic Ring Survey (GRS). The GRS is a joint project of Boston University and Five College Radio Astronomy Observatory, funded by the National Science Foundation under grants AST-9800334, AST-0098562, AST-0100793, AST-0228993, and AST-0507657. This work has made use of ds9 and the Goddard Space Flight Center's IDL Astronomy Library. Data processing and map production of the Herschel data has been possible thanks to generous support from the Italian Space Agency via contract I/038/080/0. Data presented in this paper were also analyzed using The Herschel interactive processing environment (HIPE), a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS, and SPIRE consortia. NR 91 TC 14 Z9 14 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2014 VL 787 IS 2 AR 113 DI 10.1088/0004-637X/787/2/113 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700018 ER PT J AU Deck, KM Agol, E Holman, MJ Nesvorny, D AF Deck, Katherine M. Agol, Eric Holman, Matthew J. Nesvorny, David TI TTVFast: AN EFFICIENT AND ACCURATE CODE FOR TRANSIT TIMING INVERSION PROBLEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: dynamical evolution and stability; planets and satellites: fundamental parameters; methods: numerical ID N-BODY PROBLEM; SYMPLECTIC CORRECTORS; EXTRASOLAR PLANETS; STELLAR SPIN; SYSTEM; MAPS; PAIR; MASS; EXOPLANETS; ORBITS AB Transit timing variations (TTVs) have proven to be a powerful technique for confirming Kepler planet candidates, for detecting non-transiting planets, and for constraining the masses and orbital elements of multi-planet systems. These TTV applications often require the numerical integration of orbits for computation of transit times (as well as impact parameters and durations); frequently tens of millions to billions of simulations are required when running statistical analyses of the planetary system properties. We have created a fast code for transit timing computation, TTVFast, which uses a symplectic integrator with a Keplerian interpolator for the calculation of transit times. The speed comes at the expense of accuracy in the calculated times, but the accuracy lost is largely unnecessary, as transit times do not need to be calculated to accuracies significantly smaller than the measurement uncertainties on the times. The time step can be tuned to give sufficient precision for any particular system. We find a speed-up of at least an order of magnitude relative to dynamical integrations with high precision using a Bulirsch-Stoer integrator. C1 [Deck, Katherine M.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Deck, Katherine M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Agol, Eric] Univ Washington, Dept Phys & Astron, Seattle, WA 98195 USA. [Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nesvorny, David] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. RP Deck, KM (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. OI /0000-0002-0802-9145 FU NSF Graduate Research Fellowship; NSF Career grant [AST 0645416]; NASA Origins of Solar Systems Grant [12-OSS12-0011]; NASA from the Kepler Participating Scientist Program [NNX09AB28G]; Origins program [NNX09AB33G, NNX13A124G]; NSF [AST-1008890]; NASA Astrobiology Institute's Virtual Planetary Laboratory - NASA [NNH05ZDA001C] FX We acknowledge Dan Fabrycky for testing our code and the Kepler TTV team for helpful suggestions. K.M.D. acknowledges the support of an NSF Graduate Research Fellowship. E.A. acknowledges funding by NSF Career grant AST 0645416, NASA Astrobiology Institute's Virtual Planetary Laboratory, supported by NASA under cooperative agreement NNH05ZDA001C, and NASA Origins of Solar Systems Grant 12-OSS12-0011. Work by K.M.D and M.J.H. was supported by NASA under grant NNX09AB28G from the Kepler Participating Scientist Program and grants NNX09AB33G and NNX13A124G under the Origins program. D.N. acknowledges support from NSF AST-1008890. NR 35 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 2014 VL 787 IS 2 AR 132 DI 10.1088/0004-637X/787/2/132 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700037 ER PT J AU Graham, ML Sand, DJ Valenti, S Howell, DA Parrent, J Halford, M Zaritsky, D Bianco, F Rest, A Dilday, B AF Graham, M. L. Sand, D. J. Valenti, S. Howell, D. A. Parrent, J. Halford, M. Zaritsky, D. Bianco, F. Rest, A. Dilday, B. TI CLUES TO THE NATURE OF SN 2009ip FROM PHOTOMETRIC AND SPECTROSCOPIC EVOLUTION TO LATE TIMES SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: mass-loss; stars: variables: general; supernovae: individual (2009ip) ID BINARY INTERACTION; SUPERNOVA 1988Z; CORE-COLLAPSE; II SUPERNOVAE; 2012 OUTBURST; STAR; CONSTRAINTS; PROGENITOR; LUMINOSITY; EXPLOSION AB We present time series photometric and spectroscopic data for the transient SN 2009ip from the start of its outburst in 2012 September until 2013 November. These data were collected primarily with the new robotic capabilities of the Las Cumbres Observatory Global Telescope Network, a specialized facility for time domain astrophysics, and includes supporting high-resolution spectroscopy from the Southern Astrophysical Research Telescope, Kitt Peak National Observatory, and Gemini Observatory. Based on our nightly photometric monitoring, we interpret the strength and timing of fluctuations in the light curve as interactions between fast-moving ejecta and an inhomogeneous circumstellar material (CSM) produced by past eruptions of this massive luminous blue variable (LBV) star. Our time series of spectroscopy in 2012 reveals that, as the continuum and narrow Ha flux from CSM interactions declines, the broad component of Ha persists with supernova (SN)-like velocities that are not typically seen in LBVs or SN impostor events. At late times, we find that SN 2009ip continues to decline slowly, at less than or similar to 0.01 mag day(-1), with small fluctuations in slope similar to Type IIn supernovae (SNe IIn) or SN impostors but no further LBV-like activity. The late-time spectrum features broad calcium lines similar to both late-time SNe and SN impostors. In general, we find that the photometric and spectroscopic evolution of SN 2009ip is more similar to SNe IIn than either continued eruptions of an LBV star or SN impostors but we cannot rule out a nonterminal explosion. In this context, we discuss the implications for episodic mass loss during the late stages of massive star evolution. C1 [Graham, M. L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Sand, D. J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Valenti, S.; Howell, D. A.; Parrent, J.] Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA. [Valenti, S.; Howell, D. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Parrent, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Halford, M.; Zaritsky, D.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Bianco, F.] NYU, Dept Phys, New York, NY 10003 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Dilday, B.] North Idaho Coll, Coeur Dalene, ID 83814 USA. RP Graham, ML (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM melissagraham@berkeley.edu FU Gemini Observatory [GS-2013A-Q-62]; Canadian Space Agency FX This research is based on observations obtained at the Gemini Observatory (PI: Howell, program GS-2013A-Q-62), 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).; This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. NR 50 TC 24 Z9 25 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2014 VL 787 IS 2 AR 163 DI 10.1088/0004-637X/787/2/163 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700068 ER PT J AU Keane, JT Pascucci, I Espaillat, C Woitke, P Andrews, S Kamp, I Thi, WF Meeus, G Dent, WRF AF Keane, J. T. Pascucci, I. Espaillat, C. Woitke, P. Andrews, S. Kamp, I. Thi, W. -F. Meeus, G. Dent, W. R. F. TI HERSCHEL EVIDENCE FOR DISK FLATTENING OR GAS DEPLETION IN TRANSITIONAL DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; infrared: stars; protoplanetary disks; stars: pre-main sequence ID T-TAURI STARS; HIGH-RESOLUTION SPECTROSCOPY; MAIN-SEQUENCE STARS; LOW-MASS STARS; YOUNG STELLAR OBJECTS; NE-II EMISSION; PLANET-FINDING CAMPAIGN; AURIGA MOLECULAR CLOUD; X-RAY SURVEY; PROTOPLANETARY DISKS AB Transitional disks are protoplanetary disks characterized by reduced near- and mid-infrared emission, with respect to full disks. This characteristic spectral energy distribution indicates the presence of an optically thin inner cavity within the dust disk believed to mark the disappearance of the primordial massive disk. We present new Herschel Space Observatory PACS spectra of [OI] 63.18 mu m for 21 transitional disks. Our survey complements the larger Herschel GASPS program ("Gas in Protoplanetary Systems") by quadrupling the number of transitional disks observed with PACS in this wavelength. [OI] 63.18 mu m traces material in the outer regions of the disk, beyond the inner cavity of most transitional disks. We find that transitional disks have [OI] 63.18 mu m line luminosities similar to 2 times fainter than their full disk counterparts. We self-consistently determine various stellar properties (e.g., bolometric luminosity, FUV excess, etc.) and disk properties (e.g., disk dust mass, etc.) that could influence the [OI] 63.18 mu m line luminosity, and we find no correlations that can explain the lower [OI] 63.18 mu m line luminosities in transitional disks. Using a grid of thermo-chemical protoplanetary disk models, we conclude that either transitional disks are less flared than full disks or they possess lower gas-to-dust ratios due to a depletion of gas mass. This result suggests that transitional disks are more evolved than their full disk counterparts, possibly even at large radii. C1 [Keane, J. T.; Pascucci, I.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Espaillat, C.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Woitke, P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Andrews, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kamp, I.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Thi, W. -F.] Univ Grenoble 1, CNRS INSU, Inst Planetol & Astrophys IPAG UMR 5274, F-38041 Grenoble, France. [Meeus, G.] Univ Autonoma Madrid, Dept Fis Teor, Madrid 28049, Spain. [Dent, W. R. F.] ALMA SCO, Santiago, Chile. RP Keane, JT (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. FU NASA/JPL FX I.P., J.T.K., C.E., and S.A. acknowledge NASA/JPL for funding support. J.T.K. and I.P. thank Elisabetta Rigliaco for helpful discussions on mass accretion rate estimates. The authors would also like to thank the referee, Kees Dullemond, for a very constructive review. NR 142 TC 17 Z9 17 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2014 VL 787 IS 2 AR 153 DI 10.1088/0004-637X/787/2/153 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700058 ER PT J AU Lunnan, R Chornock, R Berger, E Laskar, T Fong, W Rest, A Sanders, NE Challis, PM Drout, MR Foley, RJ Huber, ME Kirshner, RP Leibler, C Marion, GH McCrum, M Milisavljevic, D Narayan, G Scolnic, D Smartt, SJ Smith, KW Soderberg, AM Tonry, JL Burgett, WS Chambers, KC Flewelling, H Hodapp, KW Kaiser, N Magnier, EA Price, PA Wainscoat, RJ AF Lunnan, R. Chornock, R. Berger, E. Laskar, T. Fong, W. Rest, A. Sanders, N. E. Challis, P. M. Drout, M. R. Foley, R. J. Huber, M. E. Kirshner, R. P. Leibler, C. Marion, G. H. McCrum, M. Milisavljevic, D. Narayan, G. Scolnic, D. Smartt, S. J. Smith, K. W. Soderberg, A. M. Tonry, J. L. Burgett, W. S. Chambers, K. C. Flewelling, H. Hodapp, K. W. Kaiser, N. Magnier, E. A. Price, P. A. Wainscoat, R. J. TI HYDROGEN-POOR SUPERLUMINOUS SUPERNOVAE AND LONG-DURATION GAMMA-RAY BURSTS HAVE SIMILAR HOST GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: dwarf; galaxies: star formation; supernovae: general ID MASS-METALLICITY RELATION; CORE-COLLAPSE SUPERNOVAE; DIGITAL SKY SURVEY; PULSATIONAL PAIR-INSTABILITY; HUBBLE-SPACE-TELESCOPE; STAR-FORMING GALAXIES; GOODS-NORTH FIELD; IC SUPERNOVAE; LIGHT CURVES; LUMINOUS SUPERNOVAE AB We present optical spectroscopy and optical/near-IR photometry of 31 host galaxies of hydrogen-poor superluminous supernovae (SLSNe), including 15 events from the Pan-STARRS1 Medium Deep Survey. Our sample spans the redshift range 0.1 less than or similar to z less than or similar to 1.6, and is the first comprehensive host galaxy study of this specific subclass of cosmic explosions. Combining the multi-band photometry and emission-line measurements, we determine the luminosities, stellar masses, star formation rates, and metallicities. We find that, as a whole, the hosts of SLSNe are a low-luminosity (< M-B > approximate to -17.3 mag), low stellar mass (< M-*> approximate to 2 x 10(8) M-circle dot) population, with a high median specific star formation rate (< sSFR > approximate to 2Gyr(-1)). The median metallicity of our spectroscopic sample is low, 12 + log(O/H) approximate to 8.35 approximate to 0.45Z(circle dot), although at least one host galaxy has solar metallicity. The host galaxies of H-poor SLSNe are statistically distinct from the hosts of GOODS core-collapse SNe (which cover a similar redshift range), but resemble the host galaxies of long-duration gamma-ray bursts (LGRBs) in terms of stellar mass, SFR, sSFR, and metallicity. This result indicates that the environmental causes leading to massive stars forming either SLSNe or LGRBs are similar, and in particular that SLSNe are more effectively formed in low metallicity environments. We speculate that the key ingredient is large core angular momentum, leading to a rapidly spinning magnetar in SLSNe and an accreting black hole in LGRBs. C1 [Lunnan, R.; Chornock, R.; Berger, E.; Laskar, T.; Fong, W.; Sanders, N. E.; Challis, P. M.; Drout, M. R.; Foley, R. J.; Kirshner, R. P.; Leibler, C.; Marion, G. H.; Milisavljevic, D.; Narayan, G.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Foley, R. J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, R. J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Huber, M. E.; Tonry, J. L.; Burgett, W. S.; Chambers, K. C.; Flewelling, H.; Hodapp, K. W.; Kaiser, N.; Magnier, E. A.; Wainscoat, R. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Leibler, C.] UCSC, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Smartt, S. J.; Smith, K. W.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7, Antrim, North Ireland. [Scolnic, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Lunnan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rlunnan@cfa.harvard.edu RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Lunnan, Ragnhild/0000-0001-9454-4639; Narayan, Gautham/0000-0001-6022-0484; Chambers, Kenneth /0000-0001-6965-7789; Flewelling, Heather/0000-0002-1050-4056 FU National Aeronautics and Space Administration [NNX08AR22G]; National Science Foundation [AST-1238877, AST-1009749, AST-1211196]; NASA [GO-13022, GO-13326, NAS5-26555]; FAS Science Division Research Computing Group at Harvard University FX We thank the staffs at PS1, MMT, and Magellan for their assistance with performing these observations, and Andy Monson for help with processing the FourStar data. 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). Support for programs number GO-13022 and GO-13326 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. 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 between the Smithsonian Institution and the University of Arizona. This paper includes data based on observations made with the NASA/ESA Hubble Space Telescope and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). 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 research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. Some of the computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. Partial support for this work was provided by National Science Foundation grants AST-1009749 and AST-1211196. NR 123 TC 47 Z9 47 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2014 VL 787 IS 2 AR 138 DI 10.1088/0004-637X/787/2/138 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700043 ER PT J AU Masson, S McCauley, P Golub, L Reeves, KK DeLuca, EE AF Masson, Sophie McCauley, Patrick Golub, Leon Reeves, Katharine K. DeLuca, Edward E. TI DYNAMICS OF THE TRANSITION CORONA SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: magnetic fields; Sun: UV radiation ID 3-DIMENSIONAL MAGNETIC RECONNECTION; QUASI-SEPARATRIX LAYERS; X-RAY; ACTIVE-REGION; SOLAR CORONA; NULL-POINT; FLARE EMISSIONS; MODEL; TOPOLOGY; FIELD AB Magnetic reconnection between the open and closed magnetic fields in the corona is believed to play a crucial role in the corona/heliosphere coupling. At large scale, the exchange of open/closed connectivity is expected to occur in pseudo-streamer (PS) structures. However, there is neither clear observational evidence of how such coupling occurs in PSs, nor evidence for how the magnetic reconnection evolves. Using a newly developed technique, we enhance the off-limb magnetic fine structures observed with the Atmospheric Imaging Assembly and identify a PS-like feature located close to the northern coronal hole. We first identify that the magnetic topology associated with the observation is a PS, null-point (NP) related topology bounded by the open field. By comparing the magnetic field configuration with the EUV emission regions, we determined that most of the magnetic flux associated with plasma emission are small loops below the PS basic NP and open field bounding the PS topology. In order to interpret the evolution of the PS, we referred to a three-dimensional MHD interchange reconnection modeling the exchange of connectivity between small closed loops and the open field. The observed PS fine structures follow the dynamics of the magnetic field before and after reconnecting at the NP obtained by the interchange model. Moreover, the pattern of the EUV plasma emission is the same as the shape of the expected plasma emission location derived from the simulation. These morphological and dynamical similarities between the PS observations and the results from the simulation strongly suggest that the evolution of the PS, and in particular the opening/closing of the field, occurs via interchange/slipping reconnection at the basic NP of the PS. Besides identifying the mechanism at work in the large-scale coupling between the open and closed fields, our results highlight that interchange reconnection in PSs is a gradual physical process that differs from the impulsive reconnection of the solar-jet model. C1 [Masson, Sophie] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Masson, Sophie] Catholic Univ Amer, Washington, DC 20064 USA. [McCauley, Patrick; Golub, Leon; Reeves, Katharine K.; DeLuca, Edward E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Masson, S (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM sophie.masson@nasa.gov RI Reeves, Katharine/P-9163-2014; McCauley, Patrick/P-7747-2015; DeLuca, Edward/L-7534-2013 OI Reeves, Katharine/0000-0002-6903-6832; Golub, Leon/0000-0001-9638-3082; McCauley, Patrick/0000-0002-1450-7350; DeLuca, Edward/0000-0001-7416-2895 FU Lockheed-Martin [SP02H1701R]; NASA TRT Program; NASA SRT Program; NASA Postdoctoral Program FX The authors thank the referees for the pertinent comments that helped to improve the manuscript, as well as J. Klimchuck and G. Aulanier for helpful discussions. This work partially supported under contract SP02H1701R from Lockheed-Martin to SAO. The work of Sophie Masson was supported by the NASA TR&T and SR&T Programs. S.M. gratefully acknowledges support from the NASA Postdoctoral Program, administrated by Oak Ridge Associated University through a contract with NASA, during her stay at NASA Goddard Space Flight Center. NR 51 TC 8 Z9 8 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2014 VL 787 IS 2 AR 145 DI 10.1088/0004-637X/787/2/145 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700050 ER PT J AU Paggi, A Fabbiano, G Kim, DW Pellegrini, S Civano, F Strader, J Luo, B AF Paggi, Alessandro Fabbiano, Giuseppina Kim, Dong-Woo Pellegrini, Silvia Civano, Francesca Strader, Jay Luo, Bin TI ACTIVE GALACTIC NUCLEUS FEEDBACK IN THE HOT HALO OF NGC 4649 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 4649); galaxies: ISM; ISM: jets and outflows; X-rays: galaxies; X-rays: ISM ID X-RAY BINARIES; EARLY-TYPE GALAXIES; DEEP CHANDRA OBSERVATION; SUPERMASSIVE BLACK-HOLE; DARK-MATTER HALO; ELLIPTIC GALAXY; JET POWER; PERSEUS CLUSTER; RADIO-SOURCES; RADIATIVE EFFICIENCY AB Using the deepest available Chandra observations of NGC 4649, we find strong evidences of cavities, ripples, and ring-like structures in the hot interstellar medium that appear to be morphologically related with the central radio emission. These structures show no significant temperature variations in correspondence with higher pressure regions (0.5 kpc < r < 3 kpc). On the same spatial scale, a discrepancy between the mass profiles obtained from stellar dynamic and Chandra data represents the telltale evidence of a significant nonthermal pressure component in this hot gas, which is related to the radio jet and lobes. On a larger scale we find agreement between the mass profile obtained from Chandra data and planetary nebulae and globular cluster dynamics. The nucleus of NGC 4649 appears to be extremely radiatively inefficient, with highly sub-Bondi accretion flow. Consistent with this finding, the jet power evaluated from the observed X-ray cavities implies that a small fraction of the accretion power calculated for the Bondi mass accretion rate emerges as kinetic energy. Comparing the jet power to radio and nuclear X-ray luminosity, the observed cavities show behavior similar to those of other giant elliptical galaxies. C1 [Paggi, Alessandro; Fabbiano, Giuseppina; Kim, Dong-Woo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pellegrini, Silvia] Univ Bologna, Dept Astron, I-40127 Bologna, Italy. [Civano, Francesca] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Civano, Francesca] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Luo, Bin] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Paggi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM apaggi@cfa.harvard.edu RI Paggi, Alessandro/C-1219-2017; OI Paggi, Alessandro/0000-0002-5646-2410; Kim, Dong-Woo/0000-0002-7386-944X FU NASA [NAS8-03060, 11-ADAP11-0218]; NASA Chandra [G01-12110X]; Smithsonian Institute Competitive Grants Program for Science; MIUR grant PRIN, project "The Chemical and Dynamical Evolution of the Milky Way and Local Group Galaxies," [2010LY5N2T] FX We acknowledge useful comments and suggestions by our anonymous referee. This work was partially supported by NASA contract NAS8-03060 (CXC), and NASA Chandra grant G01-12110X. D.W.K. acknowledges partial support from Smithsonian Institute 2014 Competitive Grants Program for Science. 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. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa. NR 79 TC 2 Z9 2 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2014 VL 787 IS 2 AR 134 DI 10.1088/0004-637X/787/2/134 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700039 ER PT J AU Psaltis, D Ouml;zel, F Chakrabarty, D AF Psaltis, Dimitrios Oezel, Feryal Chakrabarty, Deepto TI PROSPECTS FOR MEASURING NEUTRON-STAR MASSES AND RADII WITH X-RAY PULSE PROFILE MODELING SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitation; stars: neutron ID BURST OSCILLATIONS; LIGHT CURVES; MILLISECOND PULSARS; SAX-J1808.4-3658; APPROXIMATION; CONSTRAINTS; COMPACTNESS; J0437-4715; EQUATION; BOUNDS AB Modeling the amplitudes and shapes of the X-ray pulsations observed from hot, rotating neutron stars provides a direct method for measuring neutron-star properties. This technique constitutes an important part of the science case for the forthcoming NICER and proposed LOFT X-ray missions. In this paper, we determine the number of distinct observables that can be derived from pulse profile modeling and show that using only bolometric pulse profiles is insufficient for breaking the degeneracy between inferred neutron-star radius and mass. However, we also show that for moderately spinning (300-800 Hz) neutron stars, analysis of pulse profiles in two different energy bands provides additional constraints that allow a unique determination of the neutron-star properties. Using the fractional amplitudes of the fundamental and the second harmonic of the pulse profile in addition to the amplitude and phase difference of the spectral color oscillations, we quantify the signal-to-noise ratio necessary to achieve a specified measurement precision for neutron star radius. We find that accumulating 106 counts in a pulse profile is sufficient to achieve a less than or similar to 5% uncertainty in the neutron star radius, which is the level of accuracy required to determine the equation of state of neutron-star matter. Finally, we formally derive the background limits that can be tolerated in the measurements of the various pulsation amplitudes as a function of the system parameters. C1 [Psaltis, Dimitrios; Oezel, Feryal] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Psaltis, Dimitrios; Oezel, Feryal] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Oezel, Feryal] Harvard Univ, Radcliffe Inst Adv Study, Cambridge, MA 02138 USA. [Chakrabarty, Deepto] MIT, Dept Phys, Cambridge, MA 02139 USA. [Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Psaltis, D (reprint author), Univ Arizona, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA. EM dpsaltis@email.arizona.edu; fozel@email.arizona.edu; deepto@mit.edu FU NSF [AST-1108753]; NSF CAREER award [AST-0746549]; Chandra Theory grant [TM2-13002X]; Radcliffe Institute for Advanced Study at Harvard University FX We thank the NICER and LOFT science teams for many discussions on ray tracing in neutron-star spacetimes. This work was supported in part by NSF grant AST-1108753, NSF CAREER award AST-0746549, and Chandra Theory grant TM2-13002X. F.O. gratefully acknowledges support from the Radcliffe Institute for Advanced Study at Harvard University. D.P. and F.O. thank the Institute for Theory and Computation at Harvard University for their hospitality during the time that this work was completed. NR 28 TC 30 Z9 30 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2014 VL 787 IS 2 AR 136 DI 10.1088/0004-637X/787/2/136 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700041 ER PT J AU Woolsey, LN Cranmer, SR AF Woolsey, Lauren N. Cranmer, Steven R. TI TURBULENCE-DRIVEN CORONAL HEATING AND IMPROVEMENTS TO EMPIRICAL FORECASTING OF THE SOLAR WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); solar wind; Sun: corona; Sun: magnetic fields; turbulence; waves ID MAGNETIC-FIELDS; MAGNETOHYDRODYNAMIC TURBULENCE; STREAMER BELTS; STELLAR WINDS; ALFVEN WAVES; MODEL; ACCELERATION; HOLES; FLUX; INTERPLANETARY AB Forecasting models of the solar wind often rely on simple parameterizations of the magnetic field that ignore the effects of the full magnetic field geometry. In this paper, we present the results of two solar wind prediction models that consider the full magnetic field profile and include the effects of Alfven waves on coronal heating and wind acceleration. The one-dimensional magnetohydrodynamic code ZEPHYR self-consistently finds solar wind solutions without the need for empirical heating functions. Another one-dimensional code, introduced in this paper (The Efficient Modified-Parker-Equation-Solving Tool, TEMPEST), can act as a smaller, stand-alone code for use in forecasting pipelines. TEMPEST is written in Python and will become a publicly available library of functions that is easy to adapt and expand. We discuss important relations between the magnetic field profile and properties of the solar wind that can be used to independently validate prediction models. ZEPHYR provides the foundation and calibration for TEMPEST, and ultimately we will use these models to predict observations and explain space weather created by the bulk solar wind. We are able to reproduce with both models the general anticorrelation seen in comparisons of observed wind speed at 1 AU and the flux tube expansion factor. There is significantly less spread than comparing the results of the two models than between ZEPHYR and a traditional flux tube expansion relation. We suggest that the new code, TEMPEST, will become a valuable tool in the forecasting of space weather. C1 [Woolsey, Lauren N.; Cranmer, Steven R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Woolsey, LN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Cranmer, Steven/0000-0002-3699-3134 FU National Science Foundation Graduate Research Fellowship [DGE-1144152]; NSF SHINE program [AGS-1259519]; Harvard Astronomy Department FX This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1144152 and by the NSF SHINE program under grant No. AGS-1259519. The authors obtained the OMNI solar wind data from the GSFC/SPDF OMNIWeb interface and thank David McComas and Ruth Skoug (ACE/SWEPAM) and Charles Smith and Norman Ness (ACE/MAG) for providing the majority of the OMNI measurements used in this paper. L. N.W. also thanks the Harvard Astronomy Department for the student travel grant and Loomis fund. NR 55 TC 6 Z9 6 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 2014 VL 787 IS 2 AR 160 DI 10.1088/0004-637X/787/2/160 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700065 ER PT J AU Krediet, CJ Meyer, JL Gimbrone, N Yanong, R Berzins, I Alagely, A Castro, H Ritchie, KB Paul, VJ Teplitski, M AF Krediet, Cory J. Meyer, Julie L. Gimbrone, Nicholas Yanong, Roy Berzins, Ilze Alagely, Ali Castro, Herman Ritchie, Kim B. Paul, Valerie J. Teplitski, Max TI Interactions between the tropical sea anemone Aiptasia pallida and Serratia marcescens, an opportunistic pathogen of corals SO ENVIRONMENTAL MICROBIOLOGY REPORTS LA English DT Article ID CAENORHABDITIS-ELEGANS; VIBRIO-CORALLIILYTICUS; ACROPORA-PALMATA; CELL BIOLOGY; VIRULENCE; DISEASE; SYMBIOSIS; MUCUS; MODEL; HOST AB Coral reefs are under increasing stress caused by global and local environmental changes, which are thought to increase the susceptibility of corals to opportunistic pathogens. In the absence of an easily culturable model animal, the understanding of the mechanisms of disease progression in corals remains fairly limited. In the present study, we tested the susceptibility of the tropical sea anemone Aiptasia pallida to an opportunistic coral pathogen (Serratia marcescens). A.pallida was susceptible to S. marcescensPDL100 and responded to this opportunistic coral pathogen with darkening of the tissues and retraction of tentacles, followed by complete disintegration of polyp tissues. Histological observations revealed loss of zooxanthellae and structural changes in eosinophilic granular cells in response to pathogen infection. A screen of S.marcescens mutants identified a motility and tetrathionate reductase mutants as defective in virulence in the A.pallida infection model. In co-infections with the wild-type strain, the tetrathionate reductase mutant was less fit within the surface mucopolysaccharide layer of the host coral Acropora palmata. C1 [Krediet, Cory J.; Teplitski, Max] Univ Florida IFAS, Sch Nat Resources & Environm, Interdisciplinary Ecol Grad Program, Gainesville, FL 32610 USA. [Meyer, Julie L.; Gimbrone, Nicholas; Alagely, Ali; Castro, Herman; Ritchie, Kim B.; Teplitski, Max] Univ Florida IFAS, Soil & Water Sci Dept, Gainesville, FL 32610 USA. [Yanong, Roy] Univ Florida IFAS, Sch Forest Resources & Conservat, Trop Aquaculture Lab, Ruskin, FL 33570 USA. [Berzins, Ilze] Aquat & Exot Anim Vet Serv LLC, Minneapolis, MN 55416 USA. [Ritchie, Kim B.] Mote Marine Lab, Sarasota, FL 34236 USA. [Paul, Valerie J.; Teplitski, Max] Smithsonian Marine Stn, Ft Pierce, FL USA. RP Teplitski, M (reprint author), Univ Florida IFAS, Sch Nat Resources & Environm, Interdisciplinary Ecol Grad Program, Gainesville, FL 32610 USA. EM maxtep@ufl.edu RI Meyer, Julie/D-1021-2010 OI Meyer, Julie/0000-0003-3382-3321 FU Protect Our Reefs; George E. Burch Fellowship in Theoretical and Applied Medicine at the Smithsonian Institution FX This work was supported by a grant from 'Protect Our Reefs', a program managed by Mote Marine Laboratory, with the proceeds from the state-wide sales of Protect Our Reefs specialty license plates and administered through a peer-reviewed mechanism and Dart Foundation funding. We thank W. Hoffman (Smithsonian Marine Ecosystems Exhibit) for sharing A. palmata colonies reared and maintained at the St. Lucie County Aquarium). We are grateful to Noretta Perry (Florida Fish and Wildlife Commission) for assistance with the histology (sectioning and staining), and to Ross Whetstone for the identification of the ttr mutants. M.T. is supported by the George E. Burch Fellowship in Theoretical and Applied Medicine at the Smithsonian Institution. This is contribution # 941 the Smithsonian Marine Station, Ft. Pierce. NR 29 TC 1 Z9 1 U1 0 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1758-2229 J9 ENV MICROBIOL REP JI Environ. Microbiol. Rep. PD JUN PY 2014 VL 6 IS 3 BP 287 EP 292 DI 10.1111/1758-2229.12151 PG 6 WC Environmental Sciences; Microbiology SC Environmental Sciences & Ecology; Microbiology GA AG9VQ UT WOS:000335768400009 PM 24983533 ER PT J AU Jovanovic, B Guzman, HM AF Jovanovic, Boris Guzman, Hector M. TI EFFECTS OF TITANIUM DIOXIDE ( TiO2) NANOPARTICLES ON CARIBBEAN REEF- BUILDING CORAL ( MONTASTRAEA FAVEOLATA) SO ENVIRONMENTAL TOXICOLOGY AND CHEMISTRY LA English DT Article DE Titanium dioxide nanoparticles; Coral; Zooxanthellae; Toxicology ID ELEVATED-TEMPERATURE; GENE-EXPRESSION; ZOOXANTHELLAE; STRESS; HSP70; PHOTOINHIBITION; ANNULARIS; GROWTH; WATER AB Increased use of manufactured titanium dioxide nanoparticles (nano-TiO2) is causing a rise in their concentration in the aquatic environment, including coral reef ecosystems. Caribbean mountainous star coral (Montastraea faveolata) has frequently been used as a model species to study gene expression during stress and bleaching events. Specimens of M. faveolata were collected in Panama and exposed for 17 d to nano-TiO2 suspensions (0.1mgL(-1) and 10mgL(-1)). Exposure to nano-TiO2 caused significant zooxanthellae expulsion in all the colonies, without mortality. Induction of the gene for heat-shock protein 70 (HSP70) was observed during an early stage of exposure (day 2), indicating acute stress. However, there was no statistical difference in HSP70 expression on day 7 or 17, indicating possible coral acclimation and recovery from stress. No other genes were significantly upregulated. Inductively coupled plasma mass spectrometry analysis revealed that nano-TiO2 was predominantly trapped and stored within the posterior layer of the coral fragment (burrowing sponges, bacterial and fungal mats). The bioconcentration factor in the posterior layer was close to 600 after exposure to 10mgL(-1) of nano-TiO2 for 17 d. The transient increase in HSP70, expulsion of zooxanthellae, and bioaccumulation of nano-TiO2 in the microflora of the coral colony indicate the potential of such exposure to induce stress and possibly contribute to an overall decrease in coral populations. Environ Toxicol Chem 2014;33:1346-1353. (c) 2014 SETAC C1 [Jovanovic, Boris] Univ Munich, Fac Vet Med, Dept Fish Dis & Fisheries Biol, Munich, Germany. [Guzman, Hector M.] Smithsonian Trop Res Inst, Balboa, Panama. RP Jovanovic, B (reprint author), Univ Munich, Fac Vet Med, Dept Fish Dis & Fisheries Biol, Munich, Germany. EM nanoaquatox@gmail.com OI Jovanovic, Boris/0000-0003-3970-805X FU Smithsonian Tropical Research Institute Short-Term Fellowship Program FX The present study was partially funded by the Smithsonian Tropical Research Institute Short-Term Fellowship Program. We are grateful to C. Guevara and A. Croquer, who collected coral specimens, and to the Government of Panama for providing the necessary permits to collect and export the specimens. We also thank R. Niessner and C. Sternkopf from the Institute of Hydrochemistry, Technical University of Munich, Germany, who advised on and performed the ICP-MS analysis, as well as H. Duran from TOBB University of Ankara, Turkey, who helped with TiO2 dry powder characterization. In addition, we thank G. Goetz from the National Oceanic and Atmospheric Administration (NOAA) in Seattle (WA, USA) for bioinformatics support. NR 33 TC 9 Z9 9 U1 3 U2 33 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0730-7268 EI 1552-8618 J9 ENVIRON TOXICOL CHEM JI Environ. Toxicol. Chem. PD JUN PY 2014 VL 33 IS 6 BP 1346 EP 1353 DI 10.1002/etc.2560 PG 8 WC Environmental Sciences; Toxicology SC Environmental Sciences & Ecology; Toxicology GA AH2FM UT WOS:000335936900021 PM 24677278 ER PT J AU Neufeld, MJ AF Neufeld, Michael J. TI First Mission to Pluto: Policy, Politics, Science, and Technology in the Origins of New Horizons, 1989-2003 SO HISTORICAL STUDIES IN THE NATURAL SCIENCES LA English DT Article DE Pluto; New Horizons; NASA; JPL; APL; Alan Stern; Daniel Goldin; Robert Staehle AB The complex and contested origins of the New Horizons mission to Pluto, launched by NASA in 2006, provides a window on how space science policy has been formulated in the United States before and after the turn of the twenty-first century, and how the shifting network of institutions that support and shape space science have changed since 1989. Those decades have so far been little studied except by policy scholars seeking lessons from the NASA Administrator Daniel Goldin's attempt to force a small-spacecraft technological revolution on space science in the 1990s. The New Horizons case study reveals a shift in the balance of power around 2000 among the important players in the field, increasing the influence of non-NASA actors notably Congress, science groups, and planetary-exploration lobbies. In addition, the origins of New Horizons reveal how contingent the emergence of a particular space science mission can be. C1 Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, Washington, DC 20013 USA. RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, MRC 311 POB 37012, Washington, DC 20013 USA. EM neufeldm@si.edu NR 115 TC 1 Z9 1 U1 1 U2 14 PU UNIV CALIFORNIA PRESS PI OAKLAND PA 155 GRAND AVE, SUITE 400, OAKLAND, CA 94612-3758 USA SN 1939-1811 EI 1939-182X J9 HIST STUD NAT SCI JI Hist. Stud. Nat. Sci. PD JUN PY 2014 VL 44 IS 3 BP 234 EP 276 DI 10.1525/hsns.2014.44.3.234 PG 43 WC History & Philosophy Of Science SC History & Philosophy of Science GA AH6IU UT WOS:000336235400002 ER PT J AU Foley, DH Linton, YM Ruiz-Lopez, JF Conn, JE Sallum, MAM Povoa, MM Bergo, ES Oliveira, TMP Sucupira, I Wilkerson, RC AF Foley, Desmond H. Linton, Yvonne-Marie Freddy Ruiz-Lopez, J. Conn, Jan E. Sallum, Maria Anice M. Povoa, Marinete M. Bergo, Eduardo S. Oliveira, Tatiane M. P. Sucupira, Izis Wilkerson, Richard C. TI Geographic distribution, evolution, and disease importance of species within the Neotropical Anopheles albitarsis Group (Diptera, Culicidae) SO JOURNAL OF VECTOR ECOLOGY LA English DT Article DE Mosquito; ecological niche models; malaria; phylogenetics; SEEVA; Albitarsis Group ID COMPARATIVE SUSCEPTIBILITY; PLASMODIUM-FALCIPARUM; CONSERVATION GENETICS; POPULATION HISTORY; MALARIA VECTORS; NICHE MODELS; PHYLOGEOGRAPHY; BRAZIL; SPECIATION; TRANSMISSION AB The Anopheles albitarsis group of mosquitoes comprises eight recognized species and one mitochondrial lineage. Our knowledge of malaria vectorial importance and the distribution and evolution of these taxa is incomplete. We constructed ecological niche models (ENMs) for these taxa and used hypothesized phylogenetic relationships and ENMs to investigate environmental and ecological divergence associated with speciation events. Two major clades were identified, one north (Clade 1) and one south (Clade 2) of the Amazon River that likely is or was a barrier to mosquito movement. Clade 1 species occur more often in higher average temperature locations than Clade 2 species, and taxon splits within Clade 1 corresponded with a greater divergence of variables related to precipitation than was the case within Clade 2. Comparison of the ecological profiles of sympatric species and sister species support the idea that phylogenetic proximity is related to ecological similarity. Anopheles albitarsis I, An. janconnae, and An. marajoara ENMs had the highest percentage of their predicted suitable habitat overlapping distribution models of Plasmodium falciparum and P. vivax, and warrant additional studies of the transmission potential of these species. Phylogenetic proximity may be related to malaria vectorial importance within the Albitarsis Group. C1 [Foley, Desmond H.; Linton, Yvonne-Marie; Wilkerson, Richard C.] Walter Reed Army Inst Res, Div Entomol, Silver Spring, MD 20910 USA. [Freddy Ruiz-Lopez, J.] Museum Support Ctr, Smithsonian Inst, Walter Reed Biosystemat Unit, Suitland, MD 20746 USA. [Freddy Ruiz-Lopez, J.] Univ Antioquia, PECET, Medellin, Colombia. [Conn, Jan E.] New York State Dept Hlth, Wadsworth Ctr, Albany, NY 12159 USA. [Conn, Jan E.] SUNY Albany, Sch Publ Hlth, Dept Biomed Sci, Albany, NY 12222 USA. [Sallum, Maria Anice M.; Oliveira, Tatiane M. P.] Univ Sao Paulo, Fac Saude Publ, Dept Epidemiol, BR-05508 Sao Paulo, Brazil. [Povoa, Marinete M.; Sucupira, Izis] Inst Evandro Chagas, Ananindeua, Para, Brazil. [Bergo, Eduardo S.] Superintendencia Controle Endemias Estado Sao Paul, Sao Paulo, Brazil. RP Foley, DH (reprint author), Walter Reed Army Inst Res, Div Entomol, 503 Robert Grant Ave, Silver Spring, MD 20910 USA. EM foleydes@si.edu RI Oliveira, Tatiane/O-6518-2014; Sallum, Maria/B-8537-2012; OI BERGO, EDUARDO/0000-0003-4928-0368; Conn, Jan/0000-0002-5301-7020; Foley, Desmond/0000-0001-7525-4601 FU Global Emerging Infections Surveillance and Response System (a Division of the Armed Forces Health Surveillance Center - AFHSC/Div of GEIS Ops) [P0149_13_WR]; National Institute of Health, USA [R01 AI50139-02]; Foundation for Research Support of the State of Sao Paulo, FAPESP [2011/20397-7]; National Research Council Research Associateship Award at the Walter Reed Army Institute of Research FX This investigation received financial support from the Global Emerging Infections Surveillance and Response System (a Division of the Armed Forces Health Surveillance Center - AFHSC/Div of GEIS Ops) (grant P0149_13_WR to DHF); from the National Institute of Health, USA (grant R01 AI50139-02 to JEC); and from the Foundation for Research Support of the State of Sao Paulo, FAPESP (Processo no. 2011/20397-7 to MAMS). This manuscript was prepared while YML held a National Research Council Research Associateship Award at the Walter Reed Army Institute of Research. We thank Simon Hay, Carlos Guerra, Catherine Moyes, and Peter Gething of the Malaria Atlas Project for access to malaria models. This research was performed under a Memorandum of Understanding between the Walter Reed Army Institute of Research and the Smithsonian Institution, with institutional support provided by both organizations. The published material reflects the views of the authors and should not be construed to represent those of the Department of the Army or the Department of Defense. NR 33 TC 6 Z9 6 U1 0 U2 18 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 2014 VL 39 IS 1 BP 168 EP 181 DI 10.1111/j.1948-7134.2014.12084.x PG 14 WC Entomology SC Entomology GA AH3XJ UT WOS:000336059300021 PM 24820570 ER PT J AU Anderson, L Aubourg, E Bailey, S Beutler, F Bhardwaj, V Blanton, M Bolton, AS Brinkmann, J Brownstein, JR Burden, A Chuang, CH Cuesta, AJ Dawson, KS Eisenstein, DJ Escoffier, S Gunn, JE Guo, H Ho, S Honscheid, K Howlett, C Kirkby, D Lupton, RH Manera, M Maraston, C McBride, CK Mena, O Montesano, F Nichol, RC Nuza, SE Olmstead, MD Padmanabhan, N Palanque-Delabrouille, N Parejko, J Percival, WJ Petitjean, P Prada, F Price-Whelan, AM Reid, B Roe, NA Ross, AJ Ross, NP Sabiu, CG Saito, S Samushia, L Sanchez, AG Schlegel, DJ Schneider, DP Scoccola, CG Seo, HJ Skibba, RA Strauss, MA Swanson, MEC Thomas, D Tinker, JL Tojeiro, R Magana, MV Verde, L Wake, DA Weaver, BA Weinberg, DH White, M Xu, XY Yeche, C Zehavi, I Zhao, GB AF Anderson, Lauren Aubourg, Eric Bailey, Stephen Beutler, Florian Bhardwaj, Vaishali Blanton, Michael Bolton, Adam S. Brinkmann, J. Brownstein, Joel R. Burden, Angela Chuang, Chia-Hsun Cuesta, Antonio J. Dawson, Kyle S. Eisenstein, Daniel J. Escoffier, Stephanie Gunn, James E. Guo, Hong Ho, Shirley Honscheid, Klaus Howlett, Cullan Kirkby, David Lupton, Robert H. Manera, Marc Maraston, Claudia McBride, Cameron K. Mena, Olga Montesano, Francesco Nichol, Robert C. Nuza, Sebastian E. Olmstead, Matthew D. Padmanabhan, Nikhil Palanque-Delabrouille, Nathalie Parejko, John Percival, Will J. Petitjean, Patrick Prada, Francisco Price-Whelan, Adrian M. Reid, Beth Roe, Natalie A. Ross, Ashley J. Ross, Nicholas P. Sabiu, Cristiano G. Saito, Shun Samushia, Lado Sanchez, Ariel G. Schlegel, David J. Schneider, Donald P. Scoccola, Claudia G. Seo, Hee-Jong Skibba, Ramin A. Strauss, Michael A. Swanson, Molly E. C. Thomas, Daniel Tinker, Jeremy L. Tojeiro, Rita Magana, Mariana Vargas Verde, Licia Wake, David A. Weaver, Benjamin A. Weinberg, David H. White, Martin Xu, Xiaoying Yeche, Christophe Zehavi, Idit Zhao, Gong-Bo TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Data Releases 10 and 11 Galaxy samples SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmological parameters; cosmology: observations; dark energy; distance scale; large-scale structure of Universe ID DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; POWER-SPECTRUM ANALYSIS; HUBBLE-SPACE-TELESCOPE; LARGE-SCALE STRUCTURE; SURVEY IMAGING DATA; COSMOLOGICAL IMPLICATIONS; CENT DISTANCE; III/BOSS GALAXIES; REDSHIFT SURVEY AB We present a one per cent measurement of the cosmic distance scale from the detections of the baryon acoustic oscillations (BAO) in the clustering of galaxies from the Baryon Oscillation Spectroscopic Survey, which is part of the Sloan Digital Sky Survey III. Our results come from the Data Release 11 (DR11) sample, containing nearly one million galaxies and covering approximately 8500 square degrees and the redshift range 0.2 < z < 0.7. We also compare these results with those from the publicly released DR9 and DR10 samples. Assuming a concordance A cold dark matter (ACDM) cosmological model, the DR11 sample covers a volume of 13 Gpc(3) and is the largest region of the Universe ever surveyed at this density. We measure the correlation function and power spectrum, including density- field reconstruction of the BAO feature. The acoustic features are detected at a significance of over 7s in both the correlation function and power spectrum. Fitting for the position of the acoustic features measures the distance relative to the sound horizon at the drag epoch, r(d), which has a value of r(d,fid) = 149.28 Mpc in our fiducial cosmology. We find D-V = (1264 +/- 25 Mpc)(r(d)/r(d,fid)) at z = 0.32 and D-V = (2056 +/- 20 Mpc)(r(d)/r(d,fid)) at z = 0.57. At 1.0 per cent, this latter measure is the most precise distance constraint ever obtained from a galaxy survey. Separating the clustering along and transverse to the line of sight yields measurements at z = 0.57 of D-A = (1421 +/- 20 Mpc)(r(d)/r(d,fid)) and H = (96.8 +/- 3.4 kms(-1) Mpc(-1))(r(d),(fid)/r(d)). Our measurements of the distance scale are in good agreement with previous BAO measurements and with the predictions from cosmic microwave background data for a spatially flat CDM model with a cosmological constant. C1 [Anderson, Lauren; Bhardwaj, Vaishali] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Aubourg, Eric; Magana, Mariana Vargas] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, APC,Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France. [Bailey, Stephen; Beutler, Florian; Bhardwaj, Vaishali; Palanque-Delabrouille, Nathalie; Reid, Beth; Roe, Natalie A.; Ross, Nicholas P.; Schlegel, David J.; White, Martin] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Blanton, Michael; Tinker, Jeremy L.; Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Bolton, Adam S.; Brownstein, Joel R.; Dawson, Kyle S.; Guo, Hong; Olmstead, Matthew D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Brinkmann, J.] Apache Point Observ, Sunspot, NM 88349 USA. [Burden, Angela; Howlett, Cullan; Manera, Marc; Maraston, Claudia; Nichol, Robert C.; Percival, Will J.; Ross, Ashley J.; Samushia, Lado; Thomas, Daniel; Tojeiro, Rita; Zhao, Gong-Bo] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Chuang, Chia-Hsun; Prada, Francisco; Scoccola, Claudia G.] Univ Autonoma Madrid, Inst Fis Teor UAM CSIC, E-28049 Madrid, Spain. [Cuesta, Antonio J.; Padmanabhan, Nikhil; Parejko, John] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Cuesta, Antonio J.] Univ Barcelona, IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain. [Eisenstein, Daniel J.; McBride, Cameron K.; Swanson, Molly E. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Escoffier, Stephanie] Aix Marseille Univ, CPPM, CNRS IN2P3, Marseille 07, France. [Gunn, James E.; Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Ho, Shirley; Lupton, Robert H.; Xu, Xiaoying] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Honscheid, Klaus] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Honscheid, Klaus; Seo, Hee-Jong; Weinberg, David H.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Kirkby, David] UC Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Manera, Marc] UCL, London WC1E 6BT, England. [Mena, Olga] Univ Valencia, IFIC, CSIC, E-46071 Valencia, Spain. [Montesano, Francesco; Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Nuza, Sebastian E.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Palanque-Delabrouille, Nathalie; Yeche, Christophe] CEA, Ctr Saclay, IRFU, F-91191 Gif Sur Yvette, France. [Petitjean, Patrick] Univ Paris 06, Inst Astrophys Paris, CNRS UMR7095, F-75014 Paris, France. [Prada, Francisco] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain. [Prada, Francisco] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Price-Whelan, Adrian M.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Reid, Beth; White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Ross, Nicholas P.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Sabiu, Cristiano G.] Korea Inst Adv Study, Seoul 130722, South Korea. [Saito, Shun] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Todai Inst Adv Study, Chiba 2778582, Japan. [Samushia, Lado] Ilia State Univ, Natl Abastumani Astrophys Observ, GE-1060 Tbilisi, Rep of Georgia. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Scoccola, Claudia G.] IAC, E-38200 Tenerife, Spain. [Scoccola, Claudia G.; Verde, Licia] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. [Seo, Hee-Jong] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA. [Seo, Hee-Jong] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Skibba, Ramin A.] Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA. [Verde, Licia] ICREA, E-08028 Barcelona, Spain. [Verde, Licia] ICC UB Univ Barcelona, E-08028 Barcelona, Spain. [Wake, David A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Wake, David A.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [White, Martin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Zhao, Gong-Bo] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RP Anderson, L (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM djschlegel@lbl.gov; mwhite@berkeley.edu RI Ho, Shirley/P-3682-2014; Guo, Hong/J-5797-2015; White, Martin/I-3880-2015; OI Ho, Shirley/0000-0002-1068-160X; Guo, Hong/0000-0003-4936-8247; White, Martin/0000-0001-9912-5070; Escoffier, Stephanie/0000-0002-2847-7498; Kirkby, David/0000-0002-8828-5463; Beutler, Florian/0000-0003-0467-5438; Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470; Verde, Licia/0000-0003-2601-8770 FU Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; NASA Office of Space Science; Office of Science of the US Department of Energy [DE-AC02-05CH11231]; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.; We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science.; 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. NR 130 TC 332 Z9 332 U1 9 U2 36 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 PY 2014 VL 441 IS 1 BP 24 EP 62 DI 10.1093/mnras/stu523 PG 39 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6OC UT WOS:000336249300002 ER PT J AU Seeliger, M Dimitrov, D Kjurkchieva, D Mallonn, M Fernandez, M Kitze, M Casanova, V Maciejewski, G Ohlert, JM Schmidt, JG Pannicke, A Puchalski, D Gogus, E Guver, T Bilir, S Ak, T Hohle, MM Schmidt, TOB Errmann, R Jensen, E Cohen, D Marschall, L Saral, G Bernt, I Derman, E Galan, C Neuhauser, R AF Seeliger, M. Dimitrov, D. Kjurkchieva, D. Mallonn, M. Fernandez, M. Kitze, M. Casanova, V. Maciejewski, G. Ohlert, J. M. Schmidt, J. G. Pannicke, A. Puchalski, D. Gogus, E. Guver, T. Bilir, S. Ak, T. Hohle, M. M. Schmidt, T. O. B. Errmann, R. Jensen, E. Cohen, D. Marschall, L. Saral, G. Bernt, I. Derman, E. Galan, C. Neuhaeuser, R. TI Transit timing analysis in the HAT-P-32 system SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planets and satellites: individual: HAT-P-32b; stars: individual: HAT-P-32; planetary systems ID HOT JUPITER; LIGHT CURVES; PLANETS; CONSTRAINTS; PHOTOMETRY; JITTER; STARS; ORBIT; TIME; I. AB We present the results of 45 transit observations obtained for the transiting exoplanet HATP-32b. The transits have been observed using several telescopes mainly throughout the YETI (Young Exoplanet Transit Initiative) network. In 25 cases, complete transit light curves with a timing precision better than 1.4 min have been obtained. These light curves have been used to refine the system properties, namely inclination i, planet-to-star radius ratio R-p/R-s, and the ratio between the semimajor axis and the stellar radius a/R-s. First analyses by Hartman et al. suggests the existence of a second planet in the system, thus we tried to find an additional body using the transit timing variation (TTV) technique. Taking also the literature data points into account, we can explain all mid-transit times by refining the linear ephemeris by 21 ms. Thus, we can exclude TTV amplitudes of more than similar to 1.5min. C1 [Seeliger, M.; Kitze, M.; Schmidt, J. G.; Pannicke, A.; Hohle, M. M.; Schmidt, T. O. B.; Errmann, R.; Neuhaeuser, R.] Inst Astrophys, D-07745 Jena, Germany. [Seeliger, M.; Kitze, M.; Schmidt, J. G.; Pannicke, A.; Hohle, M. M.; Schmidt, T. O. B.; Errmann, R.; Neuhaeuser, R.] Univ Observ Jena, D-07745 Jena, Germany. [Dimitrov, D.] Bulgarian Acad Sci, Inst Astron, BU-1784 Sofia, Bulgaria. [Dimitrov, D.] Bulgarian Acad Sci, NAO, BU-1784 Sofia, Bulgaria. [Kjurkchieva, D.] Univ Shumen, Shumen 9700, Bulgaria. [Mallonn, M.; Bernt, I.] Leibnitz Inst Astrophys Potsdam, D-14482 Potsdam, Germany. [Fernandez, M.; Casanova, V.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Maciejewski, G.; Puchalski, D.; Galan, C.] N Copernicus Univ, Ctr Astron, Fac Phys Astron & Informat, PL-87100 Torun, Poland. [Ohlert, J. M.] Astron Stiftung Trebur, Michael Adrian Observ, D-65468 Trebur, Germany. [Ohlert, J. M.] Univ Appl Sci, Tech Hsch Mittelhessen, D-61169 Friedberg, Germany. [Gogus, E.] Sabanci Univ, TR-34956 Istanbul, Turkey. [Guver, T.; Bilir, S.; Ak, T.] Istanbul Univ, Dept Astron & Space Sci, Fac Sci, TR-34119 Istanbul, Turkey. [Errmann, R.] Univ Jena, Abbe Ctr Photonis, D-07743 Jena, Germany. [Jensen, E.; Cohen, D.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Marschall, L.] Gettysburg Coll Observ, Dept Phys, Gettysburg, PA 17325 USA. [Saral, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Saral, G.; Derman, E.] Ankara Univ, Dept Astron & Space Sci, TR-06100 Ankara, Turkey. RP Seeliger, M (reprint author), Inst Astrophys, Schillergaesschen 2-3, D-07745 Jena, Germany. EM martin.seeliger@uni-jena.de RI bilir, selcuk/I-8827-2014; Maciejewski, Gracjan/D-6241-2014; Galan, Cezary/N-5556-2015; Dimitrov, Dinko/J-7682-2013; OI Guver, Tolga/0000-0002-3531-9842 FU Deutsche Forschungsgemeinschaft (DFG), Collaborative Research Center Sonderforschungsbereich SFB TR 7 'Gravitationswellenastronomie'; DFG, Priority Programme SPP 1385 on the First ten Million years of the Solar system [NE 515/34-1, NE 515/34-2]; Polish Ministry of Science and Higher Education [IP2011 031971]; Thuringian government [B 515-07010]; Bulgarian Scientific Foundation [DO 02-362, DO 02-85, DDVU 02/40-2010]; Shumen University [RD-08-261]; TUBITAK National Observatory (TUG) [12BT100-324-0] FX MS would like to thank the referee for the helpful comments on the paper draft. All the participating observatories appreciate the logistic and financial support of their institutions and in particular their technical workshops. MS would also like to thank all participating YETI telescopes for their observations. MMH, JGS, AP and RN would like to thank the Deutsche Forschungsgemeinschaft (DFG) for support in the Collaborative Research Center Sonderforschungsbereich SFB TR 7 'Gravitationswellenastronomie'. RE, MK and RN would like to thank the DFG for support in the Priority Programme SPP 1385 on the First ten Million years of the Solar system in projects NE 515/34-1 and -2. GM and DP acknowledge the financial support from the Polish Ministry of Science and Higher Education through the luventus Plus grant IP2011 031971. RN would like to acknowledge financial support from the Thuringian government (B 515-07010) for the STK CCD camera (Jena 0.6 m) used in this project. The research of DD and DK was supported partly by funds of projects DO 02-362, DO 02-85 and DDVU 02/40-2010 of the Bulgarian Scientific Foundation, as well as project RD-08-261 of Shumen University. We also wish to thank the TUBITAK National Observatory (TUG) for supporting this work through project number 12BT100-324-0 using the T100 telescope. NR 42 TC 6 Z9 6 U1 0 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2014 VL 441 IS 1 BP 304 EP 315 DI 10.1093/mnras/stu567 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6OC UT WOS:000336249300020 ER PT J AU Nelson, BE Ford, EB Wright, JT Fischer, DA von Braun, K Howard, AW Payne, MJ Dindar, S AF Nelson, Benjamin E. Ford, Eric B. Wright, Jason T. Fischer, Debra A. von Braun, Kaspar Howard, Andrew W. Payne, Matthew J. Dindar, Saleh TI The 55 Cancri planetary system: fully self-consistent N-body constraints and a dynamical analysis SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; techniques: radial velocities; planets and satellites: dynamical evolution and stability ID CHAIN MONTE-CARLO; TRANSITING SUPER-EARTH; MEAN MOTION RESONANCE; DIFFERENTIAL EVOLUTION; EXTRASOLAR PLANETS; MASS; PRECISION; SEARCH; SPECTROMETER; INTEGRATIONS AB We present an updated study of the planets known to orbit 55 Cancri A using 1 418 high-precision radial velocity observations from four observatories (Lick, Keck, Hobby-Eberly Telescope, Harlan J. Smith Telescope) and transit time/durations for the inner-most planet, 55 Cancri 'e' (Winn et al. 2011). We provide the first posterior sample for the masses and orbital parameters based on self-consistent N-body orbital solutions for the 55 Cancri planets, all of which are dynamically stable (for at least 10(8) yr). We apply a GPU version of Radial velocity Using N-body Differential evolution Markov Chain Monte Carlo (RUN DMC; Nelson, Ford & Payne) to perform a Bayesian analysis of the radial velocity and transit observations. Each of the planets in this remarkable system has unique characteristics. Our investigation of high-cadence radial velocities and priors based on space-based photometry yields an updated mass estimate for planet 'e' (8.09 +/- 0.26 M-circle plus), which affects its density (5.51+/-(1.32)(1.00) g cm(-3)) and inferred bulk composition. Dynamical stability dictates that the orbital plane of planet 'e' must be aligned to within 60 degrees of the orbital plane of the outer planets (which we assume to be coplanar). The mutual interactions between the planets 'b' and 'c' may develop an apsidal lock about 180 degrees. We find 36-45 per cent of all our model systems librate about the anti-aligned configuration with an amplitude of 51 degrees +/-(6 degrees)(10 degrees). Other cases showed short-term perturbations in the libration of (omega) over bar (b) - (omega) over bar (c), circulation, and nodding, but we find the planets are not in a 3: 1 mean-motion resonance. A revised orbital period and eccentricity for planet 'd' pushes it further towards the closest known Jupiter analogue in the exoplanet population. C1 [Nelson, Benjamin E.; Ford, Eric B.; Wright, Jason T.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, Davey Lab 525, University Pk, PA 16802 USA. [Nelson, Benjamin E.; Ford, Eric B.; Wright, Jason T.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Nelson, Benjamin E.; Ford, Eric B.; Payne, Matthew J.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [von Braun, Kaspar] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Payne, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dindar, Saleh] Univ Florida, Dept Comp & Informat Sci & Engn, Gainesville, FL 32611 USA. RP Nelson, BE (reprint author), Penn State Univ, Ctr Exoplanets & Habitable Worlds, Davey Lab 525, University Pk, PA 16802 USA. EM benelson@psu.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Nelson, Benjamin/0000-0003-3010-2334; Wright, Jason/0000-0001-6160-5888 FU NASA [NNX09AB35G, NNX09AM41G]; University of Florida High Performance Computing Center; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium FX We would like to thank our referee Sean Raymond for his helpful comments on the manuscript. B.E.N. thanks Eric Feigelson and Brad Hansen for insightful discussions of that helped strengthen the paper. We thank Geoff Marcy and the entire of the California Planet Survey team for their long-term commitment to high-precision RVs for the 55 Cancri system. We also thank Stan Dermott for his contribution to this project. This research was supported by NASA Origins of Solar Systems grant NNX09AB35G and NASA Applied Information Systems Research Programme grant NNX09AM41G. The authors acknowledge the University of Florida High Performance Computing Center for providing computational resources and support that have contributed to the results reported within this paper. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. We extend special thanks to those of Hawai'ian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. NR 43 TC 23 Z9 23 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 PY 2014 VL 441 IS 1 BP 442 EP 451 DI 10.1093/mnras/stu450 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6OC UT WOS:000336249300031 ER PT J AU McKernan, B Ford, KES Kocsis, B Lyra, W Winter, LM AF McKernan, B. Ford, K. E. S. Kocsis, B. Lyra, W. Winter, L. M. TI Intermediate- mass black holes in AGN discs - II. Model predictions and observational constraints SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion accretion discs; planets and satellites: formation; planet-disc interactions; protoplanetary discs; galaxies: active; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; COMPACT BINARY INSPIRALS; WAVE STANDARD SIRENS; X-RAY-EMISSION; GAS PILE-UP; PROTOPLANETARY DISKS; GLOBULAR-CLUSTERS; ACCRETION DISK; GRAVITATIONAL-RADIATION; NUMERICAL SIMULATIONS AB If intermediate-mass black holes (IMBHs) grow efficiently in gas discs around supermassive black holes, their host active galactic nucleus (AGN) discs should exhibit myriad observational signatures. Gap-opening IMBHs in AGN discs can exhibit spectral features and variability analogous to gapped protoplanetary discs. Agap-opening IMBH in the innermost disc imprints ripples and oscillations on the broad Fe K alpha line which may be detectable with future X-ray missions. A non-gap-opening IMBH will accrete and produce a soft X-ray excess relative to continuum emission. An IMBH on a retrograde orbit in an AGN disc will not open a gap and will generate soft X-rays from a bow-shock 'headwind'. Accreting IMBH in a large cavity can generate ULX-like X-ray luminosities and LINER-like optical line ratios from local ionized gas. We propose that many LINERs house a weakly accreting MBH binary in a large central disc cavity and will be luminous sources of gravitational waves (GW). IMBHs in galactic nuclei may also be detected via intermittent observational signatures including: UV/X-ray flares due to tidal disruption events, asymmetric X-ray intensity distributions as revealed by AGN transits, quasi-periodic oscillations and underluminous Type Ia supernovae. GW emitted during IMBH inspiral and collisions may be detected with eLISA and LIGO, particularly from LINERs. We summarize observational signatures and compare to current data where possible or suggest future observations. C1 [McKernan, B.; Ford, K. E. S.] CUNY, Dept Sci, Borough Manhattan Community Coll, New York, NY 10007 USA. [McKernan, B.; Ford, K. E. S.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [McKernan, B.; Ford, K. E. S.] CUNY, Grad Ctr, New York, NY 10016 USA. [McKernan, B.; Ford, K. E. S.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Kocsis, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kocsis, B.] Inst Adv Study, Princeton, NJ 08540 USA. [Lyra, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lyra, W.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Winter, L. M.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA. RP McKernan, B (reprint author), CUNY, Dept Sci, Borough Manhattan Community Coll, New York, NY 10007 USA. EM bmckernan@amnh.org RI Kocsis, Bence/C-3061-2013 OI Kocsis, Bence/0000-0002-4865-7517 FU NSF PAARE [AST-1153335]; W.M. Keck Foundation Fund of the Institute for Advanced Study; NASA [NNX11AF29G]; National Science Foundation [AST10-09802]; NASA through the Sagan Fellowship Program; [NASA-APRA08-0117] FX We thank the referee for a report that helped us condense and focus this paper. We acknowledge very useful discussions with Tahir Yaqoob, Stephan Rosswog, Zoltan Haiman, Ari Laor, Hagai Perets, Kayhan Gultekin and Mordecai Mac Low. BM and KESF acknowledge support from NASA-APRA08-0117 and NSF PAARE AST-1153335. BK was supported in part by the W.M. Keck Foundation Fund of the Institute for Advanced Study and NASA grant NNX11AF29G. WL acknowledges support by the National Science Foundation under grant no. AST10-09802. This work was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. NR 99 TC 6 Z9 6 U1 0 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2014 VL 441 IS 1 BP 900 EP 909 DI 10.1093/mnras/stu553 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6OC UT WOS:000336249300070 ER PT J AU Ramiaramanantsoa, T Moffat, AFJ Chene, AN Richardson, ND Henrichs, HF Desforges, S Antoci, V Rowe, JF Matthews, JM Kuschnig, R Weiss, WW Sasselov, D Rucinski, SM Guenther, DB AF Ramiaramanantsoa, Tahina Moffat, Anthony F. J. Chene, Andre-Nicolas Richardson, Noel D. Henrichs, Huib F. Desforges, Sebastien Antoci, Victoria Rowe, Jason F. Matthews, Jaymie M. Kuschnig, Rainer Weiss, Werner W. Sasselov, Dimitar Rucinski, Slavek M. Guenther, David B. TI MOST detects corotating bright spots on the mid-O-type giant xi Persei SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; stars: massive; stars: rotation; starspots ID IUE MEGA CAMPAIGN; EARLY-TYPE STARS; SHORT-TERM VARIABILITY; BETA-CEPHEI STARS; WIND VARIABILITY; MASSIVE STARS; INTERACTION REGIONS; STELLAR WINDS; MAIN-SEQUENCE; PHOTOMETRY AB We have used the MOST (Microvariability and Oscillations of STars) microsatellite to obtain four weeks of contiguous high-precision broad-band visual photometry of the O7.5III(n)((f)) star xi Persei in 2011 November. This star is well known from previous work to show prominent DACs (discrete absorption components) on time-scales of about 2 d from UV spectroscopy and non-radial pulsation with one (l = 3) p-mode oscillation with a period of 3.5 h from optical spectroscopy. Our MOST-orbit (101.4min) binned photometry fails to reveal any periodic light variations above the 0.1 mmag 3 sigma noise level for periods of a few hours, while several prominent Fourier peaks emerge at the 1 mmag level in the two-day period range. These longer period variations are unlikely due to pulsations, including gravity modes. From our simulations based upon a simple spot model, we deduce that we are seeing the photometric modulation of several corotating bright spots on the stellar surface. In our model, the starting times (random) and lifetimes (up to several rotations) vary from one spot to another yet all spots rotate at the same period of 4.18 d, the best-estimated rotation period of the star. This is the first convincing reported case of corotating bright spots on an O star, with important implications for drivers of the DACs (resulting from corotating interaction regions) with possible bright-spot generation via a breakout at the surface of a global magnetic field generated by a subsurface convection zone. C1 [Ramiaramanantsoa, Tahina; Moffat, Anthony F. J.; Richardson, Noel D.; Desforges, Sebastien] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Chene, Andre-Nicolas] Northern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. [Chene, Andre-Nicolas] Univ Valparaiso, Dept Fis & Astron, Playa Ancha, Chile. [Chene, Andre-Nicolas] Univ Concepcion, Dept Astron, Concepcion, Chile. [Henrichs, Huib F.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Antoci, Victoria] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Matthews, Jaymie M.; Kuschnig, Rainer] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Guenther, David B.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada. RP Ramiaramanantsoa, T (reprint author), Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada. EM tahina@astro.umontreal.ca FU NSERC (Canada); FQRNT (Quebec); Chilean Centro de Astrofisica FONDAP [15010003]; Chilean Centro de Excelencia en Astrofisica y Tecnologias Afines (CATA); Comite Mixto ESO-Gobierno de Chile; GEMINI-CONICYT [32110005]; Danish National Research Foundation; ASTERISK project; European Research Council [267864]; Austrian Space Agency; Austrian Science Fund; CRAQ (Centre de Recherche en Astrophysique du Quebec) FX We gratefully acknowledge useful conversations with Paul Charbonneau, Nicole St-Louis, Stan Owocki and, Alex Fullerton in relation to this project. DBG, JMM, AFJM, and SMR are supported by NSERC (Canada), with additional support to AFJM from FQRNT (Quebec). ANC gratefully acknowledges support from the Chilean Centro de Astrofisica FONDAP no. 15010003 and the Chilean Centro de Excelencia en Astrofisica y Tecnologias Afines (CATA). ANC also received support from the Comite Mixto ESO-Gobierno de Chile and GEMINI-CONICYT no. 32110005. VA acknowledges the Stellar Astrophysics Centre (SAC) funded by the Danish National Research Foundation. VA also received support from the ASTERISK project (ASTERoseismic Investigations with SONG and Kelper) funded by the European Research Council (Grant agreement no.: 267864). RK and WWW are supported by the Austrian Space Agency and the Austrian Science Fund. NDR acknowledges his CRAQ (Centre de Recherche en Astrophysique du Quebec) fellowship. NR 68 TC 11 Z9 11 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 PY 2014 VL 441 IS 1 BP 910 EP 917 DI 10.1093/mnras/stu619 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6OC UT WOS:000336249300071 ER PT J AU Ogrean, GA Bruggen, M van Weeren, R Rottgering, H Simionescu, A Hoeft, M Croston, JH AF Ogrean, G. A. Brueggen, M. van Weeren, R. Roettgering, H. Simionescu, A. Hoeft, M. Croston, J. H. TI Multiple density discontinuities in the merging galaxy cluster CIZA J2242.8+5301 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE shock waves; galaxies: clusters: individual: CIZA J2242.8+5301; X-rays: galaxies: clusters ID DIFFUSIVE SHOCK ACCELERATION; X-RAY OBSERVATIONS; RADIO RELICS; PARTICLE-ACCELERATION; FRONTS; SIMULATIONS; UNIVERSE; MERGER; WAVES AB CIZA J2242.8+5301, a merging galaxy cluster at z = 0.19, hosts a double-relic system and a faint radio halo. Radio observations at frequencies ranging from a few MHz to several GHz have shown that the radio spectral index at the outer edge of the northern relic corresponds to a shock of Mach number 4.6(-0.9)(+1.3), under the assumptions of diffusive shock acceleration of thermal particles in the test-particle regime. Here, we present results from new Chandra observations of the cluster. The Chandra surface brightness profile across the northern relic only hints to a surface brightness discontinuity (<2 sigma detection). Nevertheless, our reanalysis of archival Suzaku data indicates a temperature discontinuity across the relic that is consistent with a Mach number of 2.54(-0.43)(+0.64), in agreement with previously published results. This confirms that the Mach number at the shock traced by the northern relic is much weaker than predicted from the radio. Puzzlingly, in the Chandra data we also identify additional inner small density discontinuities both on and off the merger axis. Temperature measurements on both sides of the discontinuities do not allow us to undoubtedly determine their nature, although a shock front interpretation seems more likely. We speculate that if the inner density discontinuities are indeed shock fronts, then they are the consequence of violent relaxation of the dark matter cores of the clusters involved in the merger. C1 [Ogrean, G. A.; Brueggen, M.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [van Weeren, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Roettgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Simionescu, A.] Japan Aerosp Explorat Agcy, Sagamihara, Kanagawa 2298510, Japan. [Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Ogrean, GA (reprint author), Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. EM gogrean@hs.uni-hamburg.de RI XRAY, SUZAKU/A-1808-2009; OI van Weeren, Reinout/0000-0002-0587-1660 FU Deutsche Forschungsgemeinschaft (DFG) [FOR 1254]; NASA through Einstein Postdoctoral Fellowship [PF2-130104]; Chandra X-ray Center; NASA [NAS8-03060] FX We thank the referee for constructive comments that significantly improved the manuscript. GAO thanks M. Markevitch for his help with the Chandra background analysis. GAO, MB and MH acknowledge support by the research group FOR 1254 funded by the Deutsche Forschungsgemeinschaft (DFG). RJvW acknowledges support provided by NASA through Einstein Postdoctoral Fellowship grant number PF2-130104 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. MB acknowledges allocations 5056 and 5984 on supercomputers at the NIC of the Forschungszentrum Julich. The scientific results reported in this article are based on observations made by the Chandra X-ray Observatory. NR 31 TC 18 Z9 18 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 PY 2014 VL 440 IS 4 BP 3416 EP 3425 DI 10.1093/mnras/stu537 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6AT UT WOS:000336213800039 ER PT J AU Mayor, JR Wright, SJ Schuur, EAG Brooks, ME Turner, BL AF Mayor, Jordan R. Wright, S. Joseph Schuur, Edward A. G. Brooks, Mollie E. Turner, Benjamin L. TI Stable nitrogen isotope patterns of trees and soils altered by long-term nitrogen and phosphorus addition to a lowland tropical rainforest SO BIOGEOCHEMISTRY LA English DT Article DE Ecosystem ecology; Gigante Fertilization Experiment; Mass balance mixing models; Panama; Stoichiometry ID NATURAL N-15 ABUNDANCE; POTASSIUM ADDITION; MICROBIAL BIOMASS; MYCORRHIZAL FUNGI; ORGANIC NITROGEN; MONTANE FOREST; MIXING MODELS; PLANT; PREFERENCES; DELTA-N-15 AB Foliar nitrogen (N) isotope ratios (delta N-15) are used as a proxy for N-cycling processes, including the "openness" of the N cycle and the use of distinct N sources, but there is little experimental support for such proxies in lowland tropical forest. To address this, we examined the delta N-15 values of soluble soil N and canopy foliage of four tree species after 13 years of factorial N and P addition to a mature lowland rainforest. We hypothesized that N addition would lead to N-15-enriched soil N forms due to fractionating losses, whereas P addition would reduce N losses as the plants and microbes adjusted their stoichiometric demands. Chronic N addition increased the concentration and delta N-15 value of soil nitrate and delta N-15 in live and senesced leaves in two of four tree species, but did not affect ammonium or dissolved organic N. Phosphorus addition significantly increased foliar delta N-15 in one tree species and elicited significant N x P interactions in two others due to a reduction in foliar delta N-15 enrichment under N and P co-addition. Isotope mixing models indicated that three of four tree species increased their use of nitrate relative to ammonium following N addition, supporting the expectation that tropical trees use the most available form of mineral N. Previous observations that anthropogenic N deposition in this tropical region have led to increasing foliar delta N-15 values over decadal time-scales is now mechanistically linked to greater usage of N-15-enriched nitrate. C1 [Mayor, Jordan R.; Wright, S. Joseph; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Schuur, Edward A. G.; Brooks, Mollie E.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. RP Mayor, JR (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM clavulina@gmail.com RI Turner, Benjamin/E-5940-2011; Wright, Stuart/M-3311-2013 OI Turner, Benjamin/0000-0002-6585-0722; Wright, Stuart/0000-0003-4260-5676 FU National Science Foundation's International Research Fellowship Program [OISE-1012703] FX Support for J.M. was provided by the National Science Foundation's International Research Fellowship Program (OISE-1012703) and in-kind support from the Smithsonian Tropical Research Institute's Fellowship Program. We thank Julio Rodriquez, Dayana Agudo, Helene Mueller-Landau, Luis Ramos, Rueben Hernandez, Sarah Dale, and Tania Romero for their contributions, and the Republic of Panama for providing access to their natural resources for scientific research. We thank Grace Crummer, Jason Curtis, and Kathy Curtis for their contributions at the University of Florida. JM, BT, and JW designed the experiment and wrote the manuscript; TS contributed analytical ideas and logistical support, MB contributed a statistical method. The manuscript was improved due to the untiring efforts of three anonymous reviewers. NR 75 TC 10 Z9 11 U1 8 U2 103 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-2563 EI 1573-515X J9 BIOGEOCHEMISTRY JI Biogeochemistry PD JUN PY 2014 VL 119 IS 1-3 BP 293 EP 306 DI 10.1007/s10533-014-9966-1 PG 14 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA AH3MR UT WOS:000336028400019 ER PT J AU Diefendorf, AF Freeman, KH Wing, SL AF Diefendorf, Aaron F. Freeman, Katherine H. Wing, Scott L. TI A comparison of terpenoid and leaf fossil vegetation proxies in Paleocene and Eocene Bighorn Basin sediments SO ORGANIC GEOCHEMISTRY LA English DT Article DE Terpenoids; n-Alkanes; Biomarkers; Lipids; Paleoecology; Preservation; Alteration; Paleogene; Wyoming ID POLYCYCLIC AROMATIC-HYDROCARBONS; PETROLEUM SOURCE ROCKS; VICTORIAN BROWN-COAL; WILLWOOD FORMATION; EARLY DIAGENESIS; THERMAL MAXIMUM; TRITERPENOID HYDROCARBONS; DEPOSITIONAL ENVIRONMENT; ALLUVIAL PALEOSOLS; AUSTRALIAN COALS AB Plant-derived terpenoids, long recognized as biomarkers, can help reveal the major taxonomic groups of land plants present in ancient environments, even if rocks and sediments do not preserve plant macro-or microfossils. Previous studies have used simple di-to triterpenoid ratios to reconstruct floral changes in the geologic past, but few have compared terpenoid ratios with estimates of floral composition from fossils. Further, reconstructions have not taken into account differences in biomarker production (i.e. concentration relative to leaf biomass) between different types of plants. Here, we have examined terpenoids from early Cenozoic fluvial rocks from the Bighorn Basin (Wyoming, USA), where fossil flora has been studied in detail. We analyzed the distributions of diterpenoids, triterpenoids and n-alkanes from leaf wax in a total of 43 samples from 15 stratigraphic horizons of late Paleocene (63 Ma) to early Eocene (53 Ma) in age. In nearly all samples, triterpenoids, derived from angiosperms, were significantly lower in abundance than conifer-specific diterpenoids, a finding that contrasted with plant fossil evidence for the same rocks. This suggests that di-to triterpenoid ratios severely underestimate the abundance of angiosperms in paleovegetation. Angiosperms dominated n-alkane production among modern plants, and we propose a new paleovegetation proxy based on the ratio of diterpenoids (conifers) to n-alkanes (angiosperms), corrected for lipid production estimated from extant vegetation. Using diterpenoids and alkanes, we infer the composition of paleovegetation to be similar to that inferred from plant fossils. Although the approach works well for the Bighorn Basin, we stress the new paleovegetation proxy will need to be evaluated for other time periods, communities, paleogeography and depositional environments with pollen or megafossil data available. (C) 2014 Elsevier Ltd. All rights C1 [Diefendorf, Aaron F.] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA. [Freeman, Katherine H.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Wing, Scott L.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP Diefendorf, AF (reprint author), Univ Cincinnati, Dept Geol, POB 210013, Cincinnati, OH 45221 USA. EM aaron.diefendorf@uc.edu RI Freeman, Katherine/H-5140-2011; OI Freeman, Katherine/0000-0002-3350-7671; Wing, Scott/0000-0002-2954-8905 FU National Science Foundation [EAR-0844212]; Pennsylvania State University Biogeochemical Research Initiative for Education (BRIE); National Science Foundation IGERT [DGE-9972759]; Geological Society of America FX We thank R. Secord for assistance with determining sediment ages in context of the Bighorn Basin chronostratigraphy. We also thank L. Eccles, K. Mueller and H. Graham for laboratory assistance, E. Diefendorf for sample collection assistance and D. Walizer for instrumentation assistance. We thank P. Medeiros for support with the interpretation of terpenoid mass spectra and E. Currano for stratigraphic and floral information. We also thank J. Rullkotter, E. Freimuth and an anonymous reviewer for helpful comments. The research was supported by the National Science Foundation Grant EAR-0844212 (to K. H. F.), fellowship awards from The Pennsylvania State University Biogeochemical Research Initiative for Education (BRIE) funded by the National Science Foundation IGERT Grant DGE-9972759, and a Geological Society of America Student Research Grant (to A. F. D.). NR 98 TC 7 Z9 7 U1 0 U2 27 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0146-6380 J9 ORG GEOCHEM JI Org. Geochem. PD JUN PY 2014 VL 71 BP 30 EP 42 DI 10.1016/j.orggeochem.2014.04.004 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AH1TB UT WOS:000335902800004 ER PT J AU Gregory, T Mullett, A Norconk, MA AF Gregory, Tremaine Mullett, Amanda Norconk, Marilyn A. TI Strategies for Navigating Large Areas: A GIS Spatial Ecology Analysis of the Bearded Saki Monkey, Chiropotes sagulatus, in Suriname SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE ridge travel; repeated-travel areas; line density; neotropics; platyrrhines ID DIETARY ADAPTATIONS; COGNITIVE MAPS; NATIONAL-PARK; CONSERVATION; BEHAVIOR; TRAVEL; EVOLUTION; PATTERNS; PRIMATES; CACAJAO AB Animals with long day paths and large home ranges expend a considerable amount of energy on travel. Studies have shown that in the interest of reducing energy expenditure, animals selectively navigate the landscape using a variety of strategies. However, these studies have generally focused on terrestrial animals. Here we present data on an exceedingly mobile arboreal animal, bearded saki monkeys, in a topographically variable landscape in Suriname. Using ArcMap and Google Earth, we explore two potential navigation strategies: the nonrandom use of travel areas and the use of ridges in slope navigation. Over a year of data collection, bearded sakis were found to use relatively long travel paths daily, use some areas more intensely than others for travel, and when travel paths were converted to strings of points, 40.3% and 63.9% of the points were located on (50m from the main ridgeline) or near (100m from the main ridgeline) ridge tops, respectively. Thus in a habitat of high relief we found support for intensive use of ridge tops or slopes close to ridge tops by bearded sakis. Selective habitat use may be related to surveying tree crowns for fruit by large, fast moving groups of bearded sakis or monitoring the presence of potential predators. Am. J. Primatol. 76:586-595, 2014. (c) 2013 Wiley Periodicals, Inc. C1 [Gregory, Tremaine] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat Educ & Sustainabil, Washington, DC 20013 USA. [Mullett, Amanda] Kent State Univ, Dept Geog, Kent, OH 44242 USA. [Norconk, Marilyn A.] Kent State Univ, Dept Anthropol, Kent, OH 44242 USA. [Norconk, Marilyn A.] Kent State Univ, Dept Biomed Sci, Kent, OH 44242 USA. RP Gregory, T (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat Educ & Sustainabil, Washington, DC 20013 USA. EM gregoryt@si.edu FU Suriname's Foundation for Nature Conservation (STINASU); Kent State University's Graduate Student Senate, Departments of Anthropology and Geography FX Contract grant sponsor: Suriname's Foundation for Nature Conservation (STINASU); contract grant sponsor: Kent State University's Graduate Student Senate, Departments of Anthropology and Geography. NR 57 TC 1 Z9 1 U1 5 U2 41 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 EI 1098-2345 J9 AM J PRIMATOL JI Am. J. Primatol. PD JUN PY 2014 VL 76 IS 6 BP 586 EP 595 DI 10.1002/ajp.22251 PG 10 WC Zoology SC Zoology GA AG5WU UT WOS:000335490200007 PM 24375420 ER PT J AU Savage, AE Kiemnec-Tyburczy, KM Ellison, AR Fleischer, RC Zamudio, KR AF Savage, Anna E. Kiemnec-Tyburczy, Karen M. Ellison, Amy R. Fleischer, Robert C. Zamudio, Kelly R. TI Conservation and divergence in the frog immunome: pyrosequencing and de novo assembly of immune tissue transcriptomes SO GENE LA English DT Article DE Anura; Neobatrachia; RNA-seq; Immune system; Functional genomics ID DEADLY CHYTRID FUNGUS; EGG-WHITE LYSOZYME; BATRACHOCHYTRIUM-DENDROBATIDIS; XENOPUS-TROPICALIS; PROTEIN EVOLUTION; AMPHIBIAN XENOPUS; GENE-EXPRESSION; RANID FROGS; CLASS-II; SELECTION AB Background: Frogs are a diverse group of vertebrates for which limited genomic resources are available. Natural frog populations face a multitude of threats, including habitat degradation, infectious disease, and environmental change. Characterizing the functional genomics of anuran tissues in general - and the immune system in particular - will enhance our knowledge of genetic and epigenetic responses to environmental threats and inform conservation and recovery efforts. Results: To increase the number of species with genomic datasets and characterize gene expression in immune-related tissues, we sequenced the transcriptomes of three tissues from two frogs (Espadarana prosoblepon and Lithobates yavapaiensis) on the Roche 454 GS FLX platform. Our sequencing produced 8881 E. prosoblepon and 5428 L. yavapaiensis annotated gene products after de novo assembly and Gene Ontology classification. Transcripts of the innate and acquired immune system were expressed in all three tissues. Inflammatory response and acquired immunity transcripts were significantly more diverged between E. prosoblepon and L. yavapaiensis compared to innate immunity and immune system development transcripts. Immune-related transcripts did not show an overall elevated rate of functional evolution, with the exception of glycosyl proteases, which include lysozymes, central bacterial and fungal-killing enzymes of the innate immune system. Conclusions: The three frog transcriptomes provide more than 600 Mbp of new genomic data, and will serve as a valuable framework for future comparative studies of non-model anurans. Additionally, we show that immune gene divergence varies by functional group and that transcriptome studies can be useful in comparing rates of evolutionary change across gene families. (C) 2014 Elsevier B.V. All rights reserved. C1 [Savage, Anna E.; Fleischer, Robert C.] Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. [Savage, Anna E.; Kiemnec-Tyburczy, Karen M.; Ellison, Amy R.; Zamudio, Kelly R.] Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA. RP Savage, AE (reprint author), Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. EM savagea@si.edu; kmk877@humboldt.edu; are35@cornell.edu; fleischerr@si.edu; kelly.zamudio@cornell.edu RI Savage, Anna/D-8296-2015; Zamudio, Kelly/R-3533-2016; OI Savage, Anna/0000-0002-4917-8358; Zamudio, Kelly/0000-0001-5107-6206; Ellison, Amy/0000-0003-3885-6077 FU National Science Foundation [DEB-0815315, DEB-1120249]; Cornell Center for Vertebrate Genomics; Cornell Center for Comparative and Population Genomics Fellowship; Smithsonian Institution Molecular Evolution Postdoctoral Fellowship FX We thank Karen Lips for assistance with specimen collection, Steve Bogdanowicz for library preparation, Jacob Crawford, Francisco Pina-Martins and Dan hut for assistance with programming, and Autoridad Nacional del Ambiente, Panama and Arizona Game and Fish Department for scientific collecting permits. This study was supported by the National Science Foundation (DEB-0815315 and DEB-1120249), a grant from the Cornell Center for Vertebrate Genomics, a Cornell Center for Comparative and Population Genomics Fellowship, and a Smithsonian Institution Molecular Evolution Postdoctoral Fellowship. NR 68 TC 15 Z9 16 U1 0 U2 38 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1119 EI 1879-0038 J9 GENE JI Gene PD JUN 1 PY 2014 VL 542 IS 2 BP 98 EP 108 DI 10.1016/j.gene.2014.03.051 PG 11 WC Genetics & Heredity SC Genetics & Heredity GA AG7YB UT WOS:000335633600002 PM 24680726 ER PT J AU Nash, DM Haygarth, PM Turner, BL Condron, LM McDowell, RW Richardson, AE Watkins, M Heaven, MW AF Nash, David M. Haygarth, Philip M. Turner, Benjamin L. Condron, Leo M. McDowell, Richard W. Richardson, Alan E. Watkins, Mark Heaven, Michael W. TI Using organic phosphorus to sustain pasture productivity: A perspective SO GEODERMA LA English DT Review DE Phosphorus; Organic; Pasture; Transformations; Inositol; Enzymes ID NUCLEAR-MAGNETIC-RESONANCE; P-31 NMR-SPECTROSCOPY; NAOH-EDTA EXTRACTION; MYOINOSITOL HEXAPHOSPHATE; POTENTIAL BIOAVAILABILITY; CHEMICAL NATURE; ANIMAL MANURES; DESORPTION CHARACTERISTICS; INOSITOL HEXAKISPHOSPHATE; SEQUENTIAL FRACTIONATION AB Organic phosphorus (P) in grazed pastures/grasslands could sustain production systems that historically relied on inorganic P fertiliser. Interactions between inorganic P, plants and soils have been studied extensively. However, less is known about the transformation of organic P to inorganic orthophosphate. This paper investigates what is known about organic P in pasture/grassland soils used for agriculture, as well as the research needed to utilise organic P for sustainable plant production. Organic P comprises > 50% of total soil P in agricultural systems depending on location, soil type and land use. Organic P hydrolysis and release of orthophosphate by phosphatase enzymatic activity is affected by a range of factors including: (a) the chemical nature of the organic P and its ability to interact with the soil matrix; (b) microorganisms that facilitate mineralisation; (c) soil mineralogy; (d) soil water electrolytes; and (e) soil physicochemical properties. Current biogeochemical knowledge of organic P processing in soil limits our ability to develop management strategies that promote the use of organic P in plant production. Information is particularly needed on the types and sources of organic Pin grassland systems and the factors affecting the activity of enzymes that mineralise organic P. Integrated approaches analysing the soil matrix, soil water and soil biology are suggested to address this knowledge gap. (C) 2013 The Authors. Published by Elsevier B.V. All rights reserved. C1 [Nash, David M.; Watkins, Mark; Heaven, Michael W.] Victorian Dept Environm & Primary Ind Ellinbank, Ellinbank, Vic 3821, Australia. [Haygarth, Philip M.] Univ Lancaster, Lancaster Environm Ctr, Ctr Sustainable Water Management, Lancaster LA1 4YW, England. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Condron, Leo M.] Lincoln Univ, Fac Agr & Life Sci, Christchurch 7647, New Zealand. [McDowell, Richard W.] AgRes Invermay Agr Ctr, Mosgiel 9053, New Zealand. [Richardson, Alan E.] CSIRO Plant Ind, Canberra, ACT 2601, Australia. RP Nash, DM (reprint author), Victorian Dept Environm & Primary Ind Ellinbank, RMB 2460 Hazeldean Rd, Ellinbank, Vic 3821, Australia. EM david.nash@depi.vic.gov.au RI Turner, Benjamin/E-5940-2011; Richardson, Alan/I-1903-2012; Heaven, Michael/N-7442-2015; OI Turner, Benjamin/0000-0002-6585-0722; Heaven, Michael/0000-0002-7281-9643; Watkins, Mark/0000-0001-8568-0110; McDowell, Richard/0000-0003-3911-4825 NR 119 TC 21 Z9 22 U1 13 U2 129 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 PY 2014 VL 221 BP 11 EP 19 DI 10.1016/j.geoderma.2013.12.004 PG 9 WC Soil Science SC Agriculture GA AG3CJ UT WOS:000335293100002 ER PT J AU Lovelock, CE Feller, IC Reef, R Ruess, RW AF Lovelock, Catherine E. Feller, Ilka C. Reef, Ruth Ruess, Roger W. TI Variable effects of nutrient enrichment on soil respiration in mangrove forests SO PLANT AND SOIL LA English DT Article DE Soil CO2 efflux; Nitrogen; Phosphorus; Avicennia; Rhizophora; Growth; Salinity; Carbon cycling ID VS. PHOSPHORUS LIMITATION; CARBON ALLOCATION; AVICENNIA-MARINA; RHIZOPHORA-MANGLE; LITTER DECOMPOSITION; SALINITY TOLERANCE; MICROBIAL ACTIVITY; FUNCTIONAL TRAITS; ROOT RESPIRATION; CLIMATE-CHANGE AB Mangrove forests are globally important sites of carbon burial that are increasingly exposed to nutrient pollution. Here we assessed the response of soil respiration, an important component of forest carbon budgets, to nutrient enrichment over a wide range of mangrove forests. We assessed the response of soil respiration to nutrient enrichment using fertilization experiments within 22 mangrove forests over ten sites. We used boosted regression tree (BRT) models to determine the importance of environmental and plant factors for soil respiration and its responsiveness to fertilizer treatments. Leaf area index explained the largest proportion of variation in soil respiration rates (LAI, 45.9 %) followed by those of site, which had a relative influence of 39.9 % in the BRT model. Nutrient enrichment enhanced soil respiration only in nine out of 22 forests. Soil respiration in scrub forests showed a positive response to nutrient addition more frequently than taller fringing forests. The response of soil respiration to nutrient enrichment varied with changes in specific leaf area (SLA) and stem extension, with relative influences of 14.4 %, 13.6 % in the BRT model respectively. Soil respiration in mangroves varied with LAI, but other site specific factors also influenced soil respiration and its response to nutrient enrichment. Strong enhancements in aboveground growth but moderate increases in soil respiration with nutrient enrichment indicated that nutrient enrichment of mangrove forests has likely increased net ecosystem production. C1 [Lovelock, Catherine E.; Reef, Ruth] Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia. [Feller, Ilka C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Ruess, Roger W.] Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK 99775 USA. RP Lovelock, CE (reprint author), Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia. EM c.lovelock@uq.edu.au RI Lovelock, Catherine/G-7370-2012; OI Lovelock, Catherine/0000-0002-2219-6855; Feller, Ilka/0000-0002-6391-1608 FU National Science Foundation [DEB 99-81309]; WISC award from the American Association for the Advancement; New Zealand Foundation for Research, Science and Technology [C01X0024, C01X0215, C01X0307]; Smithsonian's Marine Science Network; Smithsonian Marine Station at Fort Pierce; Caribbean Coral Reef Ecosystems Program; Australian Research Council [LP0561498, DP0774491] FX This study was supported by the National Science Foundation under Grant DEB 99-81309, a WISC award from the American Association for the Advancement, the New Zealand Foundation for Research, Science and Technology (C01X0024, C01X0215, and C01X0307), the Smithsonian's Marine Science Network, the Smithsonian Marine Station at Fort Pierce, the Caribbean Coral Reef Ecosystems Program and Australian Research Council awards LP0561498 and DP0774491. I thank Marilyn Ball and the taff of Carrie Bow Cay Research Station and Pelican Beach Resort, Belize. Thanks are also extended to the many people who helped in the field, including Fernanda Adame, Dianne Allen, Don Cahoon, Anne Chamberlain, Beth Clegg, Bettina Engelbrecht, Sharon Ewe, Ray Feller, Jane Halliday, Nicole Hancock, Helen Penrose, Brian Sorrell, Ann Maree Schwarz, and Rachel Tenni. NR 85 TC 9 Z9 9 U1 13 U2 99 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 JUN PY 2014 VL 379 IS 1-2 BP 135 EP 148 DI 10.1007/s11104-014-2036-6 PG 14 WC Agronomy; Plant Sciences; Soil Science SC Agriculture; Plant Sciences GA AG1HQ UT WOS:000335166300010 ER PT J AU Weider, SZ Nittler, LR Starr, RD McCoy, TJ Solomon, SC AF Weider, Shoshana Z. Nittler, Larry R. Starr, Richard D. McCoy, Timothy J. Solomon, Sean C. TI Variations in the abundance of iron on Mercury's surface from MESSENGER X-Ray Spectrometer observations SO ICARUS LA English DT Article DE Mercury, surface; Spectroscopy ID SILICATE FRACTIONATION; REGOLITH; FLUORESCENCE; ORIGIN; REFLECTANCE; CONSTRAINTS; EVOLUTION; VOLCANISM; ELEMENTS; PLANETS AB We present measurements of Mercury's surface composition from the analysis of MESSENGER X-Ray Spectrometer data acquired during 55 large solar flares, which each provide a statistically significant detection of Fe X-ray fluorescence. The Fe/Si data display a clear dependence on phase angle, for which the results are empirically corrected. Mercury's surface has a low total abundance of Fe, with a mean Fe/Si ratio of similar to 0.06 (equivalent to similar to 1.5 wt% Fe). The absolute Fe/Si values are subject to a number of systematic uncertainties, including the phase-angle correction and possible mineral mixing effects. Individual Fe/Si measurements have an intrinsic error of similar to 10%. Observed Fe/Si values display small variations (significant at two standard deviations) from the planetary average value across large regions in Mercury's southern hemisphere. Larger differences are observed between measured Fe/Si values from more spatially resolved footprints on volcanic smooth plains deposits in the northern hemisphere and from those in surrounding terrains. Fe is most likely contained as a minor component in sulfide phases (e.g., troilite, niningerite, daubreelite) and as Fe metal, rather than within mafic silicates. Variations in surface reflectance (i.e., differences in overall reflectance and spectral slope) across Mercury are unlikely to be caused by variations in the abundance of Fe. (C) 2014 Elsevier Inc. All rights reserved. C1 [Weider, Shoshana Z.; Nittler, Larry R.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. RP Weider, SZ (reprint author), Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. EM sweider@ciw.edu FU NASA [NAS5-97271, NASW-00002] FX We thank the MESSENGER team for the development and operation of the MESSENGER spacecraft. We also thank two anonymous reviewers for constructive comments. This work is supported by the NASA Discovery Program under contract NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. NR 70 TC 23 Z9 23 U1 0 U2 19 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUN PY 2014 VL 235 BP 170 EP 186 DI 10.1016/j.icarus.2014.03.002 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG3BU UT WOS:000335291600014 ER PT J AU Beck, RMD Travouillon, KJ Aplin, KP Godthelp, H Archer, M AF Beck, Robin M. D. Travouillon, Kenny J. Aplin, Ken P. Godthelp, Henk Archer, Michael TI The Osteology and Systematics of the Enigmatic Australian Oligo-Miocene Metatherian Yalkaparidon (Yalkaparidontidae; Yalkaparidontia; ?Australidelphia; Marsupialia) SO JOURNAL OF MAMMALIAN EVOLUTION LA English DT Article DE Yalkaparidon; Zalambdodont; Marsupialia; Metatheria; Australidelphia; Riversleigh ID TERTIARY ZALAMBDODONT MARSUPIALS; FOSSIL MAMMAL NECROLESTES; ANDEAN MAIN RANGE; PHYLOGENETIC-RELATIONSHIPS; CLADISTIC-ANALYSIS; LATE PALEOCENE; SOUTH-AMERICA; PALEOGENE METATHERIANS; DIDELPHID MARSUPIALS; CRANIAL ANATOMY AB We provide the first detailed description of the osteology of the enigmatic Oligo-Miocene Australian metatherian Yalkaparidon. This taxon exhibits a number of unusual craniodental apomorphies but appears to be plesiomorphic within Metatheria in retaining four molars, rather than three as previously reported. We demonstrate that the only known skull of Yalkaparidon almost certainly represents a single individual. We also tentatively refer a number of isolated tarsals to the genus. Maximum parsimony analyses of a 258 character morphological matrix (with information from the tarsals described here either included or excluded) place Yalkaparidon within the superordinal clade Australidelphia, but Bayesian analyses of the same matrix are less well resolved, placing Yalkaparidon within Marsupialia but without unequivocally supporting australidelphian affinities. Bayesian analyses of a total evidence matrix that combines the morphological data with 9 kb of sequence data from five nuclear protein-coding genes (APOB, BRCA1, IRBP, RAG1 and VWF), 78 indels, and 53 retroposon insertion characters are similarly poorly resolved and do not clarify the supraordinal relationships of Yalkaparidon beyond suggesting that it is probably a member of Marsupialia. However, if the tarsal remains are correctly attributed to Yalkaparidon, then membership of Australidelphia seems likely, as these specimens exhibit characteristic australidelphian apomorphies. We conclude that the ordinal status of Yalkaparidon remains justified based on current evidence, and we present a revised diagnosis for Yalkaparidontia. We maintain the two currently recognized species, Y. coheni and Y. jonesi, but present revised specific diagnoses. We suggest a revised phylogenetic definition for Marsupialia, and provide phylogenetic definitions for Eomarsupialia (the clade comprising all extant Australian marsupial orders) and for the clade comprising Dasyuromorphia, Peramelemorphia, and Notoryctemorphia to the exclusion of Diprotodontia; we propose the name Agreodontia for the latter clade. C1 [Beck, Robin M. D.; Travouillon, Kenny J.; Godthelp, Henk; Archer, Michael] Univ New S Wales, Sch Biol Earth & Environm Sci, Sydney, NSW 2052, Australia. [Beck, Robin M. D.; Aplin, Ken P.] Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. [Travouillon, Kenny J.] Univ Queensland, Sch Earth Sci, St Lucia, Qld 4072, Australia. [Aplin, Ken P.] Smithsonian Inst, Div Mammals, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Beck, RMD (reprint author), Univ New S Wales, Sch Biol Earth & Environm Sci, Sydney, NSW 2052, Australia. EM robin.beck@unsw.edu.au RI Travouillon, Kenny/A-2400-2011; OI Travouillon, Kenny/0000-0003-1734-4742; Archer, Michael/0000-0002-0304-4039 FU Leverhulme Trust [SAS/30110]; University of New South Wales; National Science Foundation [DEB-0743039]; Australian Research Council [DE120100957, DP0453262, LP0453664, LP0989969, LP100200486]; Robert Day Postdoctoral Fellowship at the University of Queensland; XSTRATA Community Partnership Program (North Queensland); Phil Creaser and the CREATE Fund; Queensland National Parks and Wildlife Service; Environment Australia; Queensland Museum; Riversleigh Society Inc.; Outback at Isa; Mount Isa City Council FX Financial support for RMDB's research on Yalkaparidon has been provided by the Leverhulme Trust (via Study Abroad Studentship SAS/30110), Phil Creaser and the CREATE fund at the University of New South Wales (via a CREATE scholarship), the National Science Foundation (via grant DEB-0743039, in collaboration with Rob Voss at the American Museum of Natural History), and the Australian Research Council (via Discovery Early Career Researcher Award DE120100957). KJT is supported by the Robert Day Postdoctoral Fellowship at the University of Queensland. Additional support for research at Riversleigh has come from the Australian Research Council (DP0453262, LP0453664, LP0989969, and LP100200486 grants to MA), the XSTRATA Community Partnership Program (North Queensland), the University of New South Wales, Phil Creaser and the CREATE Fund, the Queensland National Parks and Wildlife Service, Environment Australia, the Queensland Museum, the Riversleigh Society Inc., Outback at Isa, Mount Isa City Council, and private supporters including K. and M. Pettit, E. Clark, M. Beavis, and M. Dickson. We also thank the hundreds of volunteers, staff and postgraduate students of the University of New South Wales who have assisted in field work at Riversleigh. We thank Drs Brook and Tveshor for x-raying several mandibles for us. We are grateful to the editor-in-chief John Wible and an anonymous reviewer for their thorough and constructive reviews. NR 155 TC 7 Z9 9 U1 0 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1064-7554 EI 1573-7055 J9 J MAMM EVOL JI J. Mamm. Evol. PD JUN PY 2014 VL 21 IS 2 BP 127 EP 172 DI 10.1007/s10914-013-9236-3 PG 46 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA AF8AU UT WOS:000334938200001 ER PT J AU Boerner, PF Testa, P Warren, H Weber, MA Schrijver, CJ AF Boerner, P. F. Testa, P. Warren, H. Weber, M. A. Schrijver, C. J. TI Photometric and Thermal Cross-calibration of Solar EUV Instruments SO SOLAR PHYSICS LA English DT Article DE Atomic data; Chromosphere; Corona; EUV; Instrumentation; Transition region ID DIFFERENTIAL EMISSION MEASURE; X-RAY LINES; ATOMIC DATA; HINODE; REGION; ASTROPHYSICS; DATABASE; CHIANTI; CORONA; EIT AB We present an assessment of the accuracy of the calibration measurements and atomic physics models that go into calculating the SDO/AIA response as a function of wavelength and temperature. The wavelength response is tested by convolving SDO/EVE and Hinode/EIS spectral data with the AIA effective area functions and by comparing the predictions with AIA observations. For most channels, the AIA intensities summed over the disk agree with the corresponding measurements derived from the current version (V2) of the EVE data to within the estimated 25 % calibration error. This agreement indicates that the AIA effective areas are generally stable in time. The AIA 304 channel, however, does show degradation by a factor of almost 3 from May 2010 through September 2011, when the throughput apparently reached a minimum. We also found some inconsistencies in the 335 passband, possibly due to higher-order contamination of the EVE data. The intensities in the AIA 193 channel agree to within the uncertainties with the corresponding measurements from EIS full CCD observations. Analysis of high-resolution X-ray spectra of the solar-like corona of Procyon and of EVE spectra allowed us to investigate the accuracy and completeness of the CHIANTI database in the AIA shorter wavelength passbands. We found that in the 94 channel, the spectral model significantly underestimates the plasma emission owing to a multitude of missing lines. We derived an empirical correction for the AIA temperature responses by performing differential emission measure (DEM) inversion on a broad set of EVE spectra and adjusting the AIA response functions so that the count rates predicted by the full-disk DEMs match the observations. C1 [Boerner, P. F.; Schrijver, C. J.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Testa, P.; Weber, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Warren, H.] Naval Res Lab, Washington, DC 20375 USA. RP Boerner, PF (reprint author), Lockheed Martin Solar & Astrophys Lab, A021S,Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA. EM boerner@lmsal.com; ptesta@cfa.harvard.edu; harry.warren@nrl.navy.mil; mweber@cfa.harvard.edu; schrijver@lmsal.com FU NASA [NNG04EA00C] FX The authors thank the members of the EVE team for providing helpful advice and excellent data. 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 NASA under contract NNG04EA00C. NR 29 TC 22 Z9 22 U1 0 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD JUN PY 2014 VL 289 IS 6 BP 2377 EP 2397 DI 10.1007/s11207-013-0452-z PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AB1FE UT WOS:000331536100025 ER PT J AU Rutzler, K Piantoni, C van Soest, RWM Diaz, MC AF Rutzler, Klaus Piantoni, Carla van Soest, Rob W. M. Diaz, M. Cristina TI Diversity of sponges (Porifera) from cryptic habitats on the Belize barrier reef near Carrie Bow Cay SO ZOOTAXA LA English DT Article DE Taxonomy; morphology; distribution; Caribbean; submarine caves; coral rubble; mangrove; new species; associations ID CARIBBEAN CORAL-REEF; WESTERN ATLANTIC; SOUTHWESTERN ATLANTIC; EXCAVATING SPONGES; SHALLOW-WATER; NEW-ZEALAND; DEMOSPONGIAE; POECILOSCLERIDA; HADROMERIDA; ASTROPHORIDA AB The Caribbean barrier reef near Carrie Bow Cay, Belize, has been a focus of Smithsonian Institution (Washington) reef and mangrove investigations since the early 1970s. Systematics and biology of sponges (Porifera) were addressed by several researchers but none of the studies dealt with cryptic habitats, such as the shaded undersides of coral rubble, reef crevices, and caves, although a high species diversity was recognized and samples were taken for future reference and study. This paper is the result of processing samples taken between 1972 and 2012. In all, 122 species were identified, 14 of them new (including one new genus). The new species are Tetralophophora (new genus) mesoamericana, Geodia cribrata, Placospongia caribica, Prosuberites carriebowensis, Timea diplasterina, Timea oxyasterina, Rhaphidhistia belizensis, Wigginsia curlewensis, Phorbas aurantiacus, Myrmekioderma laminatum, Niphates arenata, Siphonodictyon occultum, Xestospongia purpurea, and Aplysina sciophila. We determined that about 75 of the 122 cryptic sponge species studied (61%) are exclusive members of the sciophilic community, 47 (39 %) occur in both, light-exposed and shaded or dark habitats. Since we estimate the previously known sponge population of Carrie Bow reefs and mangroves at about 200 species, the cryptic fauna makes up 38 % of total diversity. C1 [Rutzler, Klaus; Piantoni, Carla] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Piantoni, Carla] Univ Sao Paulo, Inst Biociencias, BR-05508900 Sao Paulo, Brazil. [van Soest, Rob W. M.] Nat Biodivers Ctr, Dept Marine Zool, NL-2333 CR Leiden, Netherlands. [Diaz, M. Cristina] Museo Marino Margarita, Macanao, Edo Nueva Espar, Venezuela. RP Rutzler, K (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM ruetzler@si.edu; carla.piantoni@gmail.com; rob.vansoest@naturalis.nl; crisdiaz@ix.netcom.com RI Piantoni, Carla/K-2986-2015 OI Piantoni, Carla/0000-0002-1201-0041 NR 191 TC 13 Z9 13 U1 2 U2 21 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 29 PY 2014 VL 3805 IS 1 BP 1 EP 129 PG 129 WC Zoology SC Zoology GA AI5IU UT WOS:000336900100001 ER PT J AU Buchhave, LA Bizzarro, M Latham, DW Sasselov, D Cochran, WD Endl, M Isaacson, H Juncher, D Marcy, GW AF Buchhave, Lars A. Bizzarro, Martin Latham, David W. Sasselov, Dimitar Cochran, William D. Endl, Michael Isaacson, Howard Juncher, Diana Marcy, Geoffrey W. TI Three regimes of extrasolar planet radius inferred from host star metallicities SO NATURE LA English DT Article ID SUPER-EARTHS; KEPLER PLANETS; GIANT PLANETS; MASS PLANETS; MIGRATION; NEPTUNES; PARAMETERS; EXOPLANETS; SYSTEMS; RANGE AB Approximately half of the extrasolar planets (exoplanets) with radii less than four Earth radii are in orbits with short periods(1). Despite their sheer abundance, the compositions of such planets are largely unknown. The available evidence suggests that they range in composition from small, high-density rocky planets to low-density planets consisting of rocky cores surrounded by thick hydrogen and helium gas envelopes. Here we report the metallicities (that is, the abundances of elements heavier than hydrogen and helium) of more than 400 stars hosting 600 exoplanet candidates, and find that the exoplanets can be categorized into three populations defined by statistically distinct (similar to 4.5 sigma) metallicity regions. We interpret these regions as reflecting the formation regimes of terrestrial-like planets (radii less than 1.7 Earth radii), gas dwarf planets with rocky cores and hydrogen-helium envelopes (radii between 1.7 and 3.9 Earth radii) and ice or gas giant planets (radii greater than 3.9 Earth radii). These transitions correspond well with those inferred from dynamical mass estimates(2,3), implying that host star metallicity, which is a proxy for the initial solids inventory of the protoplanetary disk, is a key ingredient regulating the structure of planetary systems. C1 [Buchhave, Lars A.; Latham, David W.; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, Lars A.; Bizzarro, Martin; Juncher, Diana] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Cochran, William D.; Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Isaacson, Howard; Marcy, Geoffrey W.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Juncher, Diana] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. RP Buchhave, LA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lbuchhave@cfa.harvard.edu RI Bizzarro, Martin/I-8701-2012; OI Bizzarro, Martin/0000-0001-9966-2124; Buchhave, Lars A./0000-0003-1605-5666 FU Harvard Origins of Life Initiative; Danish National Research Foundation [DNRF97]; European Research Council [616027- STARDUST2ASTEROIDS]; Kepler Mission under NASA [NCC2-1390, NNX11AB99A, NNX13AB58A]; Smithsonian Astrophysical Observatory FX L.A.B. acknowledges support from the Harvard Origins of Life Initiative. M. B. acknowledges funding from the Danish National Research Foundation (grant number DNRF97) and from the European Research Council under ERC Consolidator grant agreement 616027- STARDUST2ASTEROIDS. D.W.L. acknowledges support from the Kepler Mission under NASA Cooperative Agreements NCC2-1390, NNX11AB99A and NNX13AB58A with the Smithsonian Astrophysical Observatory, and thanks the observers who helped obtain the TRES observations reported here, especially R. Stefanik, G. Esquerdo, P. Berlind and M. Calkins. NR 29 TC 65 Z9 66 U1 1 U2 17 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 29 PY 2014 VL 509 IS 7502 BP 593 EP + DI 10.1038/nature13254 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AH9JC UT WOS:000336457100043 PM 24870544 ER PT J AU Zhang, HL Aharonovich, I Glenn, DR Schalek, R Magyar, AP Lichtman, JW Hu, EL Walsworth, RL AF Zhang, Huiliang Aharonovich, Igor Glenn, David R. Schalek, Richard Magyar, Andrew P. Lichtman, Jeff W. Hu, Evelyn L. Walsworth, Ronald L. TI Silicon-Vacancy Color Centers in Nanodiamonds: Cathodoluminescence Imaging Markers in the Near Infrared SO SMALL LA English DT Article DE cathodoluminescence; nanodiamond; Silicon vacancy (Si-V); correlated cathodoluminescence and secondary electron microscopy; charge state ID CHEMICAL-VAPOR-DEPOSITION; FLUORESCENT NANODIAMONDS; HIGH-RESOLUTION; ELECTRON-BEAM; LIVING CELLS; DIAMOND; MICROSCOPY; EMISSION; SPIN C1 [Zhang, Huiliang; Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Aharonovich, Igor; Magyar, Andrew P.; Hu, Evelyn L.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Glenn, David R.; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schalek, Richard; Lichtman, Jeff W.] Harvard Univ, Dept Mol & Cellular Biol, Cambridge, MA 02138 USA. [Schalek, Richard; Lichtman, Jeff W.; Walsworth, Ronald L.] Harvard Univ, Ctr Brain Sci, Cambridge, MA 02138 USA. [Aharonovich, Igor] Univ Technol Sydney, Sch Phys & Adv Mat, Broadway, NSW 2007, Australia. RP Walsworth, RL (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM rwalsworth@cfa.harvard.edu RI Zhang, Huiliang/A-1630-2014; OI Aharonovich, Igor/0000-0003-4304-3935 FU NSF; DARPA; Australian research council [DE130100592] FX We acknowledge the financial support from the NSF and DARPA. Dr Aharonovich is the recipient of an Australian research council discovery early career research award (project number DE130100592). We thank Mary Chessey and Jean-Christophe Jaskula for helpful technical assistance. NR 46 TC 9 Z9 10 U1 2 U2 70 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 1613-6810 EI 1613-6829 J9 SMALL JI Small PD MAY 28 PY 2014 VL 10 IS 10 BP 1908 EP 1913 DI 10.1002/smll.201303582 PG 6 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA AI1KX UT WOS:000336611000004 PM 24596272 ER PT J AU Robins, JH Tintinger, V Aplin, KP Hingston, M Matisoo-Smith, E Penny, D Lavery, SD AF Robins, Judith H. Tintinger, Vernon Aplin, Ken P. Hingston, Melanie Matisoo-Smith, Elizabeth Penny, David Lavery, Shane D. TI Phylogenetic Species Identification in Rattus Highlights Rapid Radiation and Morphological Similarity of New Guinean Species SO PLOS ONE LA English DT Article ID NUCLEAR GENE-SEQUENCES; ANCIENT DNA; CHROMOSOME EVOLUTION; AUSTRALIAN RATTUS; BLACK RATS; MITOCHONDRIAL; DELIMITATION; EXTRACTION; TAXONOMY; REVEALS AB The genus Rattus is highly speciose, the taxonomy is complex, and individuals are often difficult to identify to the species level. Previous studies have demonstrated the usefulness of phylogenetic approaches to identification in Rattus but some species, especially among the endemics of the New Guinean region, showed poor resolution. Possible reasons for this are simple misidentification, incomplete gene lineage sorting, hybridization, and phylogenetically distinct lineages that are unrecognised taxonomically. To assess these explanations we analysed 217 samples, representing nominally 25 Rattus species, collected in New Guinea, Asia, Australia and the Pacific. To reduce misidentification problems we sequenced museum specimens from earlier morphological studies and recently collected tissues from samples with associated voucher specimens. We also reassessed vouchers from previously sequenced specimens. We inferred combined and separate phylogenies from two mitochondrial DNA regions comprising 550 base pair D-loop sequences and both long (655 base pair) and short (150 base pair) cytochrome oxidase I sequences. Our phylogenetic species identification for 17 species was consistent with morphological designations and current taxonomy thus reinforcing the usefulness of this approach. We reduced misidentifications and consequently the number of polyphyletic species in our phylogenies but the New Guinean Rattus clades still exhibited considerable complexity. Only three of our eight New Guinean species were monophyletic. We found good evidence for either incomplete mitochondrial lineage sorting or hybridization between species within two pairs, R. leucopus/R. cf. verecundus and R. steini/R. praetor. Additionally, our results showed that R. praetor, R. niobe and R. verecundus each likely encompass more than one species. Our study clearly points to the need for a revised taxonomy of the rats of New Guinea, based on broader sampling and informed by both morphology and phylogenetics. The remaining taxonomic complexity highlights the recent and rapid radiation of Rattus in the Australo-Papuan region. C1 [Robins, Judith H.; Hingston, Melanie; Lavery, Shane D.] Univ Auckland, Sch Biol Sci, Auckland 1, New Zealand. [Robins, Judith H.; Tintinger, Vernon] Univ Auckland, Dept Anthropol, Auckland 1, New Zealand. [Aplin, Ken P.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. [Matisoo-Smith, Elizabeth] Univ Otago, Dept Anat, Dunedin, New Zealand. [Penny, David] Massey Univ, Inst Fundamental Sci, Palmerston North, New Zealand. [Lavery, Shane D.] Univ Auckland, Inst Marine Sci, Auckland 1, New Zealand. RP Robins, JH (reprint author), Univ Auckland, Sch Biol Sci, Auckland 1, New Zealand. EM j.robins@auckland.ac.nz OI Hingston, Melanie/0000-0002-2960-6212 FU University of Auckland; Marsden Fund of New Zealand [UOA510] FX The University of Auckland and the Marsden Fund of New Zealand, Project Number UOA510. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 57 TC 5 Z9 5 U1 0 U2 23 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 27 PY 2014 VL 9 IS 5 AR e98002 DI 10.1371/journal.pone.0098002 PG 18 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AI5NG UT WOS:000336914100028 PM 24865350 ER PT J AU Schuetz, MJA Kessler, EM Vandersypen, LMK Cirac, JI Giedke, G AF Schuetz, M. J. A. Kessler, E. M. Vandersypen, L. M. K. Cirac, J. I. Giedke, G. TI Nuclear spin dynamics in double quantum dots: Multistability, dynamical polarization, criticality, and entanglement SO PHYSICAL REVIEW B LA English DT Article ID SINGLE-ELECTRON SPIN; TRAPPED IONS; STEADY-STATE; RESONANCE; SYSTEM; DRIVEN; MANIPULATION; COMPUTATION; FIELD; BITS AB We theoretically study the nuclear spin dynamics driven by electron transport and hyperfine interaction in an electrically defined double quantum dot in the Pauli-blockade regime. We derive a master-equation-based framework and show that the coupled electron-nuclear system displays an instability towards the buildup of large nuclear spin polarization gradients in the two quantum dots. In the presence of such inhomogeneous magnetic fields, a quantum interference effect in the collective hyperfine coupling results in sizable nuclear spin entanglement between the two quantum dots in the steady state of the evolution. We investigate this effect using analytical and numerical techniques, and demonstrate its robustness under various types of imperfections. C1 [Schuetz, M. J. A.; Cirac, J. I.; Giedke, G.] Max Planck Inst Quantum Opt, D-85748 Garching, Germany. [Kessler, E. M.] Harvard Univ, Dept Phys, Cambridge, MA 02318 USA. [Kessler, E. M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02318 USA. [Vandersypen, L. M. K.] Delft Univ Technol, Kavli Inst NanoSci, NL-2600 GA Delft, Netherlands. RP Schuetz, MJA (reprint author), Max Planck Inst Quantum Opt, Hans Kopfermann Str 1, D-85748 Garching, Germany. RI Kessler, Eric Matthias/E-6981-2012 OI Kessler, Eric Matthias/0000-0001-9959-538X FU DFG [SFB 631]; Cluster of Excellence NIM; European Commission [265522]; Harvard Quantum Optics Center; Institute for Theoretical Atomic and Molecular Physics; Dutch Foundation for Fundamental Research on Matter (FOM) FX M.J.A.S., J.I.C., and G.G. acknowledge support by the DFG within SFB 631, the Cluster of Excellence NIM, and the project MALICIA within the 7th Framework Programme for Research of the European Commission, under FET-Open Grant No. 265522. E.M.K. acknowledges support by the Harvard Quantum Optics Center and the Institute for Theoretical Atomic and Molecular Physics. L.M.K.V. acknowledges support by the Dutch Foundation for Fundamental Research on Matter (FOM). NR 121 TC 5 Z9 5 U1 1 U2 23 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 EI 1550-235X J9 PHYS REV B JI Phys. Rev. B PD MAY 27 PY 2014 VL 89 IS 19 AR 195310 DI 10.1103/PhysRevB.89.195310 PG 32 WC Physics, Condensed Matter SC Physics GA AI1YF UT WOS:000336650500005 ER PT J AU Legates, DR Eschenbach, W Soon, W AF Legates, David R. Eschenbach, Willis Soon, Willie TI Arctic albedo changes are small compared with changes in cloud cover in the tropics SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 [Legates, David R.] Univ Delaware, Dept Geog, Newark, DE 19716 USA. [Legates, David R.] Univ Delaware, Dept Appl Econ & Stat, Newark, DE 19716 USA. [Soon, Willie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Legates, DR (reprint author), Univ Delaware, Dept Geog, Newark, DE 19716 USA. EM legates@udel.edu NR 4 TC 1 Z9 1 U1 2 U2 20 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAY 27 PY 2014 VL 111 IS 21 BP E2157 EP E2158 DI 10.1073/pnas.1404997111 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AH8TO UT WOS:000336411300001 PM 24821819 ER PT J AU Rocha, LA Aleixo, A Allen, G Almeda, F Baldwin, CC Barclay, MVL Bates, JM Bauer, AM Benzoni, F Berns, CM Berumen, ML Blackburn, DC Blum, S Bolanos, F Bowie, RCK Britz, R Brown, RM Cadena, CD Carpenter, K Ceriaco, LM Chakrabarty, P Chaves, G Choat, JH Clements, KD Collette, BB Collins, A Coyne, J Cracraft, J Daniel, T de Carvalho, MR de Queiroz, K Di Dario, F Drewes, R Dumbacher, JP Engilis, A Erdmann, MV Eschmeyer, W Feldman, CR Fisher, BL Fjeldsa, J Fritsch, PW Fuchs, J Getahun, A Gill, A Gomon, M Gosliner, T Graves, GR Griswold, CE Guralnick, R Hartel, K Helgen, KM Ho, H Iskandar, DT Iwamoto, T Jaafar, Z James, HF Johnson, D Kavanaugh, D Knowlton, N Lacey, E Larson, HK Last, P Leis, JM Lessios, H Liebherr, J Lowman, M Mahler, DL Mamonekene, V Matsuura, K Mayer, GC Mays, H McCosker, J McDiarmid, RW McGuire, J Miller, MJ Mooi, R Mooi, RD Moritz, C Myers, P Nachman, MW Nussbaum, RA Foighil, DO Parenti, LR Parham, JF Paul, E Paulay, G Perez-Eman, J Perez-Matus, A Poe, S Pogonoski, J Rabosky, DL Randall, JE Reimer, JD Robertson, DR Rodel, MO Rodrigues, MT Roopnarine, P Ruber, L Ryan, MJ Sheldon, F Shinohara, G Short, A Simison, WB Smith-Vaniz, WF Springer, VG Stiassny, M Tello, JG Thompson, CW Trnski, T Tucker, P Valqui, T Vecchione, M Verheyen, E Wainwright, PC Wheeler, TA White, T Will, K Williams, JT Williams, G Wilson, EO Winker, K Winterbottom, R Witt, CC AF Rocha, L. A. Aleixo, A. Allen, G. Almeda, F. Baldwin, C. C. Barclay, M. V. L. Bates, J. M. Bauer, A. M. Benzoni, F. Berns, C. M. Berumen, M. L. Blackburn, D. C. Blum, S. Bolanos, F. Bowie, R. C. K. Britz, R. Brown, R. M. Cadena, C. D. Carpenter, K. Ceriaco, L. M. Chakrabarty, P. Chaves, G. Choat, J. H. Clements, K. D. Collette, B. B. Collins, A. Coyne, J. Cracraft, J. Daniel, T. de Carvalho, M. R. de Queiroz, K. Di Dario, F. Drewes, R. Dumbacher, J. P. Engilis, A., Jr. Erdmann, M. V. Eschmeyer, W. Feldman, C. R. Fisher, B. L. Fjeldsa, J. Fritsch, P. W. Fuchs, J. Getahun, A. Gill, A. Gomon, M. Gosliner, T. Graves, G. R. Griswold, C. E. Guralnick, R. Hartel, K. Helgen, K. M. Ho, H. Iskandar, D. T. Iwamoto, T. Jaafar, Z. James, H. F. Johnson, D. Kavanaugh, D. Knowlton, N. Lacey, E. Larson, H. K. Last, P. Leis, J. M. Lessios, H. Liebherr, J. Lowman, M. Mahler, D. L. Mamonekene, V. Matsuura, K. Mayer, G. C. Mays, H., Jr. McCosker, J. McDiarmid, R. W. McGuire, J. Miller, M. J. Mooi, R. Mooi, R. D. Moritz, C. Myers, P. Nachman, M. W. Nussbaum, R. A. Foighil, D. O. Parenti, L. R. Parham, J. F. Paul, E. Paulay, G. Perez-Eman, J. Perez-Matus, A. Poe, S. Pogonoski, J. Rabosky, D. L. Randall, J. E. Reimer, J. D. Robertson, D. R. Roedel, M. -O. Rodrigues, M. T. Roopnarine, P. Rueber, L. Ryan, M. J. Sheldon, F. Shinohara, G. Short, A. Simison, W. B. Smith-Vaniz, W. F. Springer, V. G. Stiassny, M. Tello, J. G. Thompson, C. W. Trnski, T. Tucker, P. Valqui, T. Vecchione, M. Verheyen, E. Wainwright, P. C. Wheeler, T. A. White, T. Will, K. Williams, J. T. Williams, G. Wilson, E. O. Winker, K. Winterbottom, R. Witt, C. C. TI Specimen collection: An essential tool SO SCIENCE LA English DT Letter C1 [Rocha, L. A.; Almeda, F.; Blackburn, D. C.; Blum, S.; Daniel, T.; Drewes, R.; Dumbacher, J. P.; Eschmeyer, W.; Fisher, B. L.; Fritsch, P. W.; Gosliner, T.; Griswold, C. E.; Iwamoto, T.; Kavanaugh, D.; Lowman, M.; McCosker, J.; Mooi, R.; Roopnarine, P.; Simison, W. B.; Williams, G.] Calif Acad Sci, San Francisco, CA 94118 USA. [Aleixo, A.] Museu Paraense Emilio Goeldi, BR-66040170 Belem, Para, Brazil. [Allen, G.] Western Australian Museum, Perth, WA 6986, Australia. [Baldwin, C. C.; de Queiroz, K.; Graves, G. R.; Helgen, K. M.; Jaafar, Z.; James, H. F.; Johnson, D.; Knowlton, N.; McDiarmid, R. W.; Parenti, L. R.; Springer, V. G.; Williams, J. T.] Smithsonian Inst, Washington, DC 20560 USA. [Barclay, M. V. L.; Britz, R.] Nat Hist Museum, London SW7 5BD, England. [Bates, J. M.] Field Museum Nat Hist, Chicago, IL 60605 USA. [Bauer, A. M.] Villanova Univ, Villanova, PA 19085 USA. [Benzoni, F.] Univ Milano Bicocca, I-20126 Milan, Italy. [Berns, C. M.] Utica Coll, Utica, NY 13502 USA. [Berumen, M. L.] King Abdullah Univ Sci & Technol, Thuwal 23955, Saudi Arabia. [Bolanos, F.; Chaves, G.] Univ Costa Rica, San Jose 115012060, Costa Rica. [Lacey, E.; McGuire, J.; Nachman, M. W.; Will, K.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Brown, R. M.; Short, A.] Univ Kansas, Lawrence, KS 66045 USA. [Cadena, C. D.] Univ Los Andes, Bogota 4976, Colombia. [Carpenter, K.] Old Dominion Univ, Norfolk, VA 23529 USA. [Ceriaco, L. M.] Museu Nacl Hist Nat & Ciencia, P-7005638 Lisbon, Portugal. [Chakrabarty, P.; Sheldon, F.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Choat, J. H.] James Cook Univ, Townsville, Qld 4811, Australia. [Bowie, R. C. K.; Clements, K. D.] Univ Auckland, Auckland 1142, New Zealand. [Collette, B. B.; Collins, A.; Vecchione, M.] NOAA Systemat Lab, Washington, DC 20013 USA. [Coyne, J.] Univ Chicago, Chicago, IL 60637 USA. [Cracraft, J.; Stiassny, M.; Tello, J. G.] Amer Museum Nat Hist, New York, NY 10024 USA. [de Carvalho, M. R.; Rodrigues, M. T.] Univ Sao Paulo, BR-05508090 Sao Paulo, Brazil. [Di Dario, F.] Univ Fed Rio de Janeiro, BR-27965045 Macae, RJ, Brazil. [Engilis, A., Jr.; Mahler, D. L.; Wainwright, P. C.] Univ Calif Davis, Davis, CA 95616 USA. [Erdmann, M. V.] Conservat Int, Denpasar 80235, Bali, Indonesia. [Feldman, C. R.] Univ Nevada, Reno, NV 89557 USA. [Fjeldsa, J.] Nat Hist Museum Denmark, DK-2100 Copenhagen, Denmark. [Fuchs, J.] Museum Natl Hist Nat, F-75005 Paris, France. [Getahun, A.] Univ Addis Ababa, Addis Ababa 1176, Ethiopia. [Gill, A.] Univ Sydney, Sydney, NSW 2006, Australia. [Gomon, M.] Museum Victoria, Melbourne, Vic 3001, Australia. [Guralnick, R.] Univ Colorado, Boulder, CO 80309 USA. [Hartel, K.; Wilson, E. O.] Harvard Univ, Cambridge, MA 02138 USA. [Ho, H.] Natl Museum Marine Biol & Aquarium, Pingtung 944, Taiwan. [Iskandar, D. T.] Inst Teknol Bandung, Bandung 40132, Indonesia. [Jaafar, Z.] Natl Univ Singapore, Singapore 117543, Singapore. [Larson, H. K.] Museum & Art Gallery Northern Terr, Darwin, NT 0820, Australia. [Last, P.; Pogonoski, J.; White, T.] CSIRO Marine & Atmospher Res, Hobart, Tas 7000, Australia. [Leis, J. M.] Australian Museum, Sydney, NSW 2010, Australia. [Lessios, H.; Miller, M. J.; Robertson, D. R.] Smithsonian Trop Res Inst, Balboa 084303092, Panama. [Liebherr, J.] Cornell Univ, Ithaca, NY 14853 USA. [Mamonekene, V.] Univ Marien Ngouabi, Brazzaville, Congo. [Matsuura, K.; Shinohara, G.] Natl Museum Nat & Sci, Tsukuba, Ibaraki 3050005, Japan. [Mayer, G. C.] Univ Wisconsin Parkside, Kenosha, WI 53141 USA. [Mays, H., Jr.] Cincinnati Museum Ctr, Cincinnati, OH 45203 USA. [Mooi, R. D.] Manitoba Museum, Winnipeg, MB R3B 0N2, Canada. [Moritz, C.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Myers, P.; Nussbaum, R. A.; Foighil, D. O.; Rabosky, D. L.; Thompson, C. W.; Tucker, P.] Univ Michigan, Ann Arbor, MI 48109 USA. [Parham, J. F.] Calif State Univ Fullerton, Fullerton, CA 92831 USA. [Paul, E.] Ornithol Council, Chevy Chase, MD 20815 USA. [Paulay, G.; Smith-Vaniz, W. F.] Univ Florida, Gainesville, FL 32611 USA. [Perez-Eman, J.] Cent Univ Venezuela, Caracas 1041, Venezuela. [Perez-Matus, A.] Pontificia Univ Catolica Chile, Santiago 6513677, Chile. [Poe, S.; Ryan, M. J.; Witt, C. C.] Univ New Mexico, Albuquerque, NM 87131 USA. [Randall, J. E.] Bernice P Bishop Museum, Honolulu, HI 96817 USA. [Reimer, J. D.] Univ Ryukyus, Nishihara, Okinawa 9030213, Japan. [Roedel, M. -O.] Museum Nat Kunde, D-10115 Berlin, Germany. [Rueber, L.] Nat Hist Museum Burgergemeinde Bern, CH-3005 Bern, Switzerland. [Tello, J. G.] Long Isl Univ, Brooklyn, NY 11201 USA. [Trnski, T.] Auckland Museum, Auckland 1142, New Zealand. [Valqui, T.] Ctr Ornitol & Biodiversidad, Lima 33, Peru. [Verheyen, E.] Royal Belgian Inst Nat Sci, B-1000 Brussels, Belgium. [Wheeler, T. A.] McGill Univ, Montreal, PQ H9X 3V9, Canada. [Winker, K.] Univ Alaska Museum, Fairbanks, AK 99775 USA. [Winterbottom, R.] Royal Ontario Museum, Toronto, ON M5S 2C6, Canada. RP Rocha, LA (reprint author), Calif Acad Sci, San Francisco, CA 94118 USA. EM LRocha@calacademy.org RI Moritz, Craig/A-7755-2012; Witt, Christopher/D-8587-2012; Aleixo, Alexandre/L-3135-2013; publist, CMEC/C-3010-2012; Pogonoski, John /E-1710-2017; publicationpage, cmec/B-4405-2017; White, William/B-9748-2009; Fjeldsa, Jon/A-9699-2013; Leis, Jeffrey/E-7502-2012; Benzoni, Francesca/G-1304-2010; Rocha, Luiz/C-5107-2011; Wheeler, Terry/A-9466-2011; Rabosky, Daniel/G-4530-2015; Berumen, Michael/F-7745-2011; Rodrigues, Miguel/F-8174-2012; Jaafar, Zeehan/I-1248-2012; Chakrabarty, Prosanta/E-3307-2010; Winker, Kevin/M-2042-2014 OI Chaves, Gerardo/0000-0002-4301-6569; Bowie, Rauri/0000-0001-8328-6021; Clements, Kendall/0000-0001-8512-5977; Witt, Christopher/0000-0003-2781-1543; White, William/0000-0001-9705-2453; Fjeldsa, Jon/0000-0003-0790-3600; Benzoni, Francesca/0000-0001-8906-1309; Wheeler, Terry/0000-0002-7260-0350; Berumen, Michael/0000-0003-2463-2742; Winker, Kevin/0000-0002-8985-8104 NR 13 TC 41 Z9 45 U1 12 U2 115 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 23 PY 2014 VL 344 IS 6186 BP 814 EP 815 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AH6IL UT WOS:000336233800019 PM 24855245 ER PT J AU Cook-Patton, SC LaForgia, M Parker, JD AF Cook-Patton, Susan C. LaForgia, Marina Parker, John D. TI Positive interactions between herbivores and plant diversity shape forest regeneration SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE diversity; forest ecosystem; survival; herbivory; Odocoileus virginianus ID SPECIES-DIVERSITY; ASSOCIATIONAL RESISTANCE; TROPHIC COMPLEXITY; TROPICAL FORESTS; FUNCTIONAL-ROLE; BIODIVERSITY; TREE; CONSEQUENCES; ECOSYSTEMS; PRODUCTIVITY AB The effects of herbivores and diversity on plant communities have been studied separately but rarely in combination. We conducted two concurrent experiments over 3 years to examine how tree seedling diversity, density and herbivory affected forest regeneration. One experiment factorially manipulated plant diversity (one versus 15 species) and the presence/absence of deer (Odocoileus virginianus). We found that mixtures outperformed monocultures only in the presence of deer. Selective browsing on competitive dominants and associational protection from less palatable species appear responsible for this herbivore-driven diversity effect. The other experiment manipulated monospecific plant density and found little evidence for negative density dependence. Combined, these experiments suggest that the higher performance in mixture was owing to the acquisition of positive interspecific interactions rather than the loss of negative intraspecific interactions. Overall, we emphasize that realistic predictions about the consequences of changing biodiversity will require a deeper understanding of the interaction between plant diversity and higher trophic levels. If we had manipulated only plant diversity, we would have missed an important positive interaction across trophic levels: diverse seedling communities better resist herbivores, and herbivores help to maintain seedling diversity. C1 [Cook-Patton, Susan C.; LaForgia, Marina; Parker, John D.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Cook-Patton, SC (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM cook-pattons@si.edu RI Parker, John/F-9761-2010 OI Parker, John/0000-0002-3632-7625 FU Smithsonian Scholarly Studies; Smithsonian Postdoctoral Fellowship FX A Smithsonian Scholarly Studies grant to J.D.P. and a Smithsonian Postdoctoral Fellowship to S.C.C. supported this work. NR 50 TC 10 Z9 10 U1 5 U2 89 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD MAY 22 PY 2014 VL 281 IS 1783 AR 20140261 DI 10.1098/rspb.2014.0261 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AF0NP UT WOS:000334411600026 PM 24718763 ER PT J AU Ortega-Jimenez, VM Sapir, N Wolf, M Variano, EA Dudley, R AF Ortega-Jimenez, Victor M. Sapir, Nir Wolf, Marta Variano, Evan A. Dudley, Robert TI Into turbulent air: size-dependent effects of von Karman vortex streets on hummingbird flight kinematics and energetics SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Calypte anna; flight energetics; stability; turbulence; vortex shedding; wingbeat kinematics ID ANNAS HUMMINGBIRDS; HOVERING HUMMINGBIRDS; OXYGEN-CONSUMPTION; WIND-TUNNEL; PERFORMANCE; BEHAVIOR; CANOPY; TROUT; COSTS; WAKES AB Animal fliers frequently move through a variety of perturbed flows during their daily aerial routines. However, the extent to which these perturbations influence flight control and energetic expenditure is essentially unknown. Here, we evaluate the kinematic and metabolic consequences of flight within variably sized vortex shedding flows using five Anna's hummingbirds feeding from an artificial flower in steady control flow and within vortex wakes produced behind vertical cylinders. Tests were conducted at three horizontal airspeeds (3, 6 and 9 m s(-1)) and using three different wake-generating cylinders (with diameters equal to 38, 77 and 173% of birds' wing length). Only minimal effects on wing and body kinematics were demonstrated for flight behind the smallest cylinder, whereas flight behind the medium-sized cylinder resulted in significant increases in the variances of wingbeat frequency, and variances of body orientation, especially at higher airspeeds. Metabolic rate was, however, unchanged relative to that of unperturbed flight. Hummingbirds flying within the vortex street behind the largest cylinder exhibited highest increases in variances of wingbeat frequency, and of body roll, pitch and yaw amplitudes at all measured airspeeds. Impressively, metabolic rate under this last condition increased by up to 25% compared with control flights. Cylinder wakes sufficiently large to interact with both wings can thus strongly affect stability in flight, eliciting compensatory kinematic changes with a consequent increase in flight metabolic costs. Our findings suggest that vortical flows frequently encountered by aerial taxa in diverse environments may impose substantial energetic costs. C1 [Ortega-Jimenez, Victor M.; Sapir, Nir; Wolf, Marta; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Variano, Evan A.] Univ Calif Berkeley, Dept Civil & Environm Engn, Berkeley, CA 94720 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. RP Ortega-Jimenez, VM (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM vortega@berkeley.edu OI Sapir, Nir/0000-0002-2477-0515; Ortega-Jimenez, Victor Manuel/0000-0003-0024-5086 FU AFOSR [13RSA030]; University of California MEXUS-CONACYT program; Swedish Research Council FX This work was supported by AFOSR #13RSA030, the University of California MEXUS-CONACYT program, and the Swedish Research Council. NR 41 TC 15 Z9 15 U1 5 U2 30 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD MAY 22 PY 2014 VL 281 IS 1783 AR 20140180 DI 10.1098/rspb.2014.0180 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AF0NP UT WOS:000334411600022 PM 24671978 ER PT J AU Ackermann, M Ajello, M Albert, A Allafort, A Baldini, L Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Bissaldi, E Bonamente, E Bottacini, E Bouvier, A Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cecchi, C Charles, E Chekhtman, A Chen, Q Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S D'Ammando, F de Angelis, A de Palma, F Dermer, CD Desiante, R Digel, SW Di Venere, L Silva, EDE Drell, PS Drlica-Wagner, A Favuzzi, C Fegan, SJ Focke, WB Franckowiak, A Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Hadasch, D Hayashida, M Hays, E Horan, D Hughes, RE Inoue, Y Jackson, MS Jogler, T Johannesson, G Johnson, WN Kamae, T Kawano, T Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Lemoine-Goumard, M Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Mayer, M Mazziotta, MN McEnery, JE Michelson, PF Mizuno, T Moiseev, AA Monte, C Monzani, ME Moretti, E Morselli, A Moskalenko, IV Murgia, S Murphy, R Nemmen, R Nuss, E Ohno, M Ohsugi, T Okumura, A Omodei, N Orienti, M Orlando, E Ormes, JF Paneque, D Panetta, JH Perkins, JS Pesce-Rollins, M Petrosian, V Piron, F Pivato, G Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Ritz, S Schulz, A Sgro, C Siskind, EJ Spandre, G Spinelli, P Takahashi, H Takeuchi, Y Tanaka, Y Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Tosti, G Troja, E Tronconi, V Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Werner, M Winer, BL Wood, DL Wood, KS Wood, M Yang, Z AF Ackermann, M. Ajello, M. Albert, A. Allafort, A. Baldini, L. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Bissaldi, E. Bonamente, E. Bottacini, E. Bouvier, A. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cecchi, C. Charles, E. Chekhtman, A. Chen, Q. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. D'Ammando, F. de Angelis, A. de Palma, F. Dermer, C. D. Desiante, R. Digel, S. W. Di Venere, L. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Fegan, S. J. Focke, W. B. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Hadasch, D. Hayashida, M. Hays, E. Horan, D. Hughes, R. E. Inoue, Y. Jackson, M. S. Jogler, T. Johannesson, G. Johnson, W. N. Kamae, T. Kawano, T. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lemoine-Goumard, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Mayer, M. Mazziotta, M. N. McEnery, J. E. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Moretti, E. Morselli, A. Moskalenko, I. V. Murgia, S. Murphy, R. Nemmen, R. Nuss, E. Ohno, M. Ohsugi, T. Okumura, A. Omodei, N. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Perkins, J. S. Pesce-Rollins, M. Petrosian, V. Piron, F. Pivato, G. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Ritz, S. Schulz, A. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Takahashi, H. Takeuchi, Y. Tanaka, Y. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Tosti, G. Troja, E. Tronconi, V. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Werner, M. Winer, B. L. Wood, D. L. Wood, K. S. Wood, M. Yang, Z. TI HIGH-ENERGY GAMMA-RAY EMISSION FROM SOLAR FLARES: SUMMARY OF FERMI LARGE AREA TELESCOPE DETECTIONS AND ANALYSIS OF TWO M-CLASS FLARES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: flares; Sun: X-rays, gamma rays ID STOCHASTIC ACCELERATION; PARTICLE-ACCELERATION; EGRET; CALIBRATION; ELECTRONS; COMPTON; SHOCKS; WAVES; GRO AB We present the detections of 18 solar flares detected in high-energy gamma-rays (above 100 MeV) with the Fermi Large Area Telescope (LAT) during its first 4 yr of operation. This work suggests that particle acceleration up to very high energies in solar flares is more common than previously thought, occurring even in modest flares, and for longer durations. Interestingly, all these flares are associated with fairly fast coronal mass ejections (CMEs). We then describe the detailed temporal, spatial, and spectral characteristics of the first two long-lasting events: the 2011 March 7 flare, a moderate (M3.7) impulsive flare followed by slowly varying gamma-ray emission over 13 hr, and the 2011 June 7 M2.5 flare, which was followed by gamma-ray emission lasting for 2 hr. We compare the Fermi LAT data with X-ray and proton data measurements from GOES and RHESSI. We argue that the gamma-rays are more likely produced through pion decay than electron bremsstrahlung, and we find that the energy spectrum of the proton distribution softens during the extended emission of the 2011 March 7 flare. This would disfavor a trapping scenario for particles accelerated during the impulsive phase of the flare and point to a continuous acceleration process at play for the duration of the flares. CME shocks are known for accelerating the solar energetic particles (SEPs) observed in situ on similar timescales, but it might be challenging to explain the production of gamma-rays at the surface of the Sun while the CME is halfway to the Earth. A stochastic turbulence acceleration process occurring in the solar corona is another likely scenario. Detailed comparison of characteristics of SEPs and gamma-ray-emitting particles for several flares will be helpful to distinguish between these two possibilities. C1 [Ackermann, M.; Mayer, M.; Schulz, A.] DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Albert, A.; Hughes, R. E.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA. [Allafort, A.; Bechtol, K.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chen, Q.; Chiang, J.; Claus, R.; Digel, S. W.; Di Venere, L.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Inoue, Y.; Jogler, T.; Kamae, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Allafort, A.; Bechtol, K.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chen, Q.; Chiang, J.; Claus, R.; Desiante, R.; Digel, S. W.; Di Venere, L.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Inoue, Y.; Jogler, T.; Kamae, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.] Ist Nazl Fis Nucl, I-56127 Pisa, Italy. [Barbiellini, G.; Desiante, R.; Longo, F.] Ist Nazl Fis Nucl, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.; Tronconi, V.] Univ Padua, Dipartimento Fis Astron G Galilei, I-35131 Padua, Italy. [Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bissaldi, E.; Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Bissaldi, E.; Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Bouvier, A.; Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Brandt, T. J.; Guiriec, S.; Hays, E.; McEnery, J. E.; Moiseev, A. A.; Nemmen, R.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, Lab Leprince Ringuet, CNRS, IN2P3, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.] CSIC, Inst Ciencies Espai, IEEE, E-08193 Barcelona, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Ist Nazl Astrofis, Osservatorio Astron Roma, I-00040 Rome, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univ & Particules Montpellier, CNRS, IN2P3, F-34095 Montpellier, France. [Conrad, J.; Larsson, S.; Yang, Z.] Univ Stockholm, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Jackson, M. S.; Larsson, S.; Moretti, E.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden. [D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Murphy, R.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Fukazawa, Y.; Kawano, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Grenier, I. A.] Univ Paris Diderot, CEA Saclay, Lab AIM, Serv Astrophys,CEA IRFU CNRS, F-91191 Gif Sur Yvette, France. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Jackson, M. S.; Moretti, E.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, GAHEC, F-31100 Toulouse, France. [Larsson, S.] Univ Stockholm, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Lemoine-Goumard, M.; Lott, B.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Moiseev, A. A.; Perkins, J. S.] Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Ohno, M.; Tanaka, Y.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Okumura, A.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Takeuchi, Y.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Vianello, G.] Consorzio Interuniv Fis Spaziale, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartmento Fis, I-00133 Rome, Italy. [Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA. RP Ackermann, M (reprint author), DESY, D-15738 Zeuthen, Germany. EM vahep@stanford.edu; allafort@stanford.edu; nico.giglietto@ba.infn.it; nicola.omodei@stanford.edu; tanaka@astro.isas.jaxa.jp RI Di Venere, Leonardo/C-7619-2017; Bissaldi, Elisabetta/K-7911-2016; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Orlando, E/R-5594-2016; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016 OI Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Di Venere, Leonardo/0000-0003-0703-824X; Giordano, Francesco/0000-0002-8651-2394; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Inoue, Yoshiyuki/0000-0002-7272-1136; Bastieri, Denis/0000-0002-6954-8862; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Bissaldi, Elisabetta/0000-0001-9935-8106; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; FU National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden FX The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT, as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States; the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy; the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK), and Japan Aerospace Exploration Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden. NR 31 TC 16 Z9 16 U1 1 U2 22 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 2014 VL 787 IS 1 AR 15 DI 10.1088/0004-637X/787/1/15 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200015 ER PT J AU Albertsson, T Indriolo, N Kreckel, H Semenov, D Crabtree, KN Henning, T AF Albertsson, T. Indriolo, N. Kreckel, H. Semenov, D. Crabtree, K. N. Henning, Th. TI FIRST TIME-DEPENDENT STUDY OF H-2 AND H-3(+) ORTHO-PARA CHEMISTRY IN THE DIFFUSE INTERSTELLAR MEDIUM: OBSERVATIONS MEET THEORETICAL PREDICTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; cosmic rays; ISM: clouds; ISM: molecules; methods: numerical; molecular processes ID RAY IONIZATION RATE; MOLECULAR-HYDROGEN; PROTOPLANETARY DISKS; PRESTELLAR CORES; SELECTION-RULES; GALACTIC-CENTER; DARK CLOUDS; D-3(+) IONS; RECOMBINATION; GAS AB The chemistry in the diffuse interstellar medium (ISM) initiates the gradual increase of molecular complexity during the life cycle of matter. A key molecule that enables build-up of new molecular bonds and new molecules via proton donation is H-3(+). Its evolution is tightly related to molecular hydrogen and thought to be well understood. However, recent observations of ortho and para lines of H-2 and H-3(+) in the diffuse ISM showed a puzzling discrepancy in nuclear spin excitation temperatures and populations between these two key species. H-3(+), unlike H2, seems to be out of thermal equilibrium, contrary to the predictions of modern astrochemical models. We conduct the first time-dependent modeling of the para-fractions of H-2 and H-3(+) in the diffuse ISM and compare our results to a set of line-of-sight observations, including new measurements presented in this study. We isolate a set of key reactions for H-3(+) and find that the destruction of the lowest rotational states of H-3(+) by dissociative recombination largely controls its ortho/para ratio. A plausible agreement with observations cannot be achieved unless a ratio larger than 1:5 for the destruction of (1, 1)- and (1, 0)-states of H-3(+) is assumed. Additionally, an increased cosmic-ray ionization rate to 10(-15) s(-1) further improves the fit whereas variations of other individual physical parameters, such as density and chemical age, have only a minor effect on the predicted ortho/para ratios. Thus, our study calls for new laboratory measurements of the dissociative recombination rate and branching ratio of the key ion H-3(+) under interstellar conditions. C1 [Albertsson, T.; Semenov, D.; Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Indriolo, N.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Kreckel, H.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Crabtree, K. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Albertsson, T (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. RI Kreckel, Holger/F-4969-2010; Semenov, Dmitry/B-7446-2012; OI Semenov, Dmitry/0000-0002-3913-7114; Indriolo, Nick/0000-0001-8533-6440 FU European Community [238258]; NASA [1465490]; European Research Council [StG 307163]; Deutsche Forschungsgemeinschaft [SPP 1385] FX We would like to thank the anonymous referees for their useful comments that helped improve this paper. We also thank Ben McCall for contributing his expertise and valuable comments to this paper. This research made use of NASA's Astrophysics Data System. T.A. acknowledges funding from the European Community's Seventh Framework Programme [FP7/2007-2013] under grant agreement No. 238258. N.I. is funded by NASA Research Support Agreement No. 1465490 provided through JPL. H.K. was supported by the European Research Council under grant agreement No. StG 307163. D.S. acknowledges support by the Deutsche Forschungsgemeinschaft through SPP 1385: "The first ten million years of the Solar System-a planetary materials approach" (SE 1962/1-3). K.N.C. has been supported by a CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory. NR 85 TC 9 Z9 9 U1 2 U2 20 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 2014 VL 787 IS 1 AR 44 DI 10.1088/0004-637X/787/1/44 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200044 ER PT J AU Brown, WR Geller, MJ Kenyon, SJ AF Brown, Warren R. Geller, Margaret J. Kenyon, Scott J. TI MMT HYPERVELOCITY STAR SURVEY. III. THE COMPLETE SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; Galaxy: halo; Galaxy: kinematics and dynamics; stars: early-type; stars: individual ( SDSS J111136.44+005856.44, J114146.45+044217.29, J215629.02+005444.18) ID MASSIVE BLACK-HOLE; DIGITAL SKY SURVEY; MILKY-WAY HALO; HORIZONTAL-BRANCH STARS; DYNAMICALLY EJECTED RUNAWAY; GALACTIC ESCAPE SPEED; DWARF MERGER SYSTEMS; WHITE-DWARF; TRIGONOMETRIC PARALLAXES; VELOCITY DISTRIBUTIONS AB We describe our completed spectroscopic survey for unbound hypervelocity stars (HVSs) ejected from the Milky Way. Three new discoveries bring the total number of unbound late B-type stars to 21. We place new constraints on the nature of the stars and on their distances using moderate resolution MMT spectroscopy. Half of the stars are fast rotators; they are certain 2.5-4 M-circle dot main sequence stars at 50-120 kpc distances. Correcting for stellar lifetime, our survey implies that unbound 2.5-4M(circle dot) stars are ejected from the Milky Way at a rate of 1.5 x 10(-6) yr(-1). These unbound HVSs are likely ejected continuously over the past 200 Myr and do not share a common flight time. The anisotropic spatial distribution of HVSs on the sky remains puzzling. Southern hemisphere surveys like SkyMapper will soon allow us to map the all-sky distribution of HVSs. Future proper motion measurements with Hubble Space Telescope and Gaia will provide strong constraints on origin. Existing observations are all consistent with HVS ejections from encounters with the massive black hole in the Galactic center. C1 [Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Brown, WR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM wbrown@cfa.harvard.edu; mgeller@cfa.harvard.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X FU Smithsonian Institution FX We thank A. Milone, J. McAfee, S. Gottilla, and E. Martin for their assistance with observations obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. We thank the referee for constructive comments that improved this paper. This project makes use of data products from the Sloan Digital Sky Survey, which is managed by the Astrophysical Research Consortium for the Participating Institutions. This research makes use of NASA's Astrophysics Data System Bibliographic Services. This work was supported by the Smithsonian Institution. NR 108 TC 27 Z9 27 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 89 DI 10.1088/0004-637X/787/1/89 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200089 ER PT J AU Burke, MJ Jourdain, E Roques, JP Evans, DA AF Burke, Mark J. Jourdain, Elisabeth Roques, Jean-Pierre Evans, Daniel A. TI THE HARD X-RAY CONTINUUM OF CEN A OBSERVED WITH INTEGRAL SPI SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (NGC 5128); galaxies: active; galaxies: elliptical and lenticular, cD; gamma rays: galaxies; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; HIGH-ENERGY EMISSION; CENTAURUS-A; GALAXY CENTAURUS; BLACK-HOLE; GAMMA-RAYS; BL-LAC; SPECTRA; REFLECTION; BLAZARS AB We revisit the average hard X-ray spectrum from the active galactic nucleus (AGN) of Centaurus A (Cen A) using 10 yr worth of observations with INTEGRAL SPI. This source has the highest flux observed from any AGNs in the SPI bandpass (23 keV-8 MeV). The 10 year light curve of Cen A is presented, and hardness ratios confirm that the spectral shape changes very little despite the luminosity varying by a factor of a few. Primarily, we establish the presence of a reflection component in the average spectrum by demonstrating an excess between 20 and 60 keV, from extending the spectral shape observed at low energy to the SPI regime. The excess in Chandra HETGS and INTEGRAL SPI data is well described by reflection of the dominant power-law spectrum from a neutral, optically thick atmosphere. We find that the reprocessed emission contributes 20%-25% of the 23-100 keV flux. The existence of a cutoff at tens to hundreds of kiloelectron volts remains controversial. Using simulated spectra, we demonstrate that a high energy cutoff reproduces the observed spectral properties of Cen A more readily than a simple power law. However, we also show that such a cutoff is probably underestimated when neglecting (even modest) reflection, and for Cen A would be at energies > 700 keV, with a confidence of > 95%. This is atypically high for thermal Comptonizing plasmas observed in AGNs, and we propose that we are in fact modeling the more gradual change in spectral shape expected of synchrotron self-Compton spectra. C1 [Burke, Mark J.; Jourdain, Elisabeth; Roques, Jean-Pierre] CNRS, IRAP, F-31028 Toulouse 4, France. [Evans, Daniel A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Burke, MJ (reprint author), CNRS, IRAP, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France. EM mburke@irap.omp.eu FU CNES FX The INTEGRAL SPI project is supported under the responsibility and leadership of CNES. We are grateful to ASI, CEA, CNES, DLR, ESA, INTA, NASA, and OSTC for support. NR 45 TC 5 Z9 5 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 50 DI 10.1088/0004-637X/787/1/50 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200050 ER PT J AU Graninger, DM Herbst, E Ouml;berg, KI Vasyunin, AI AF Graninger, Dawn M. Herbst, Eric Oeberg, Karin I. Vasyunin, Anton I. TI THE HNC/HCN RATIO IN STAR-FORMING REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: molecules; stars: formation ID GAS-GRAIN CHEMISTRY; DENSE INTERSTELLAR CLOUDS; HCN/HNC ABUNDANCE RATIO; MONTE-CARLO TREATMENT; ROTATIONAL-EXCITATION; MOLECULAR CLOUDS; CHEMICAL-MODEL; HCN; HNC; CORES AB HNC and HCN, typically used as dense gas tracers in molecular clouds, are a pair of isomers that have great potential as a temperature probe because of temperature dependent, isomer-specific formation and destruction pathways. Previous observations of the HNC/HCN abundance ratio show that the ratio decreases with increasing temperature, something that standard astrochemical models cannot reproduce. We have undertaken a detailed parameter study on which environmental characteristics and chemical reactions affect the HNC/HCN ratio and can thus contribute to the observed dependence. Using existing gas and gas-grain models updated with new reactions and reaction barriers, we find that in static models the H + HNC gas-phase reaction regulates the HNC/HCN ratio under all conditions, except for very early times. We quantitatively constrain the combinations of H abundance and H + HNC reaction barrier that can explain the observed HNC/HCN temperature dependence and discuss the implications in light of new quantum chemical calculations. In warm-up models, gas-grain chemistry contributes significantly to the predicted HNC/HCN ratio and understanding the dynamics of star formation is therefore key to model the HNC/HCN system. C1 [Graninger, Dawn M.; Oeberg, Karin I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Herbst, Eric] Univ Virginia, Dept Chem, Charlottesville, VA 22901 USA. [Vasyunin, Anton I.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Herbst, Eric] Univ Virginia, Dept Phys & Astron, Charlottesville, VA 22903 USA. RP Graninger, DM (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM dgraninger@cfa.harvard.edu RI Vasyunin, Anton/N-9112-2016 OI Vasyunin, Anton/0000-0003-1684-3355 FU National Science Foundation; NASA Exobiology and Evolutionary Biology program through Rensselaer Polytechnic Institute; European Research Council (ERC) [PALs 320620] FX E.H. acknowledges the support of the National Science Foundation for his astrochemistry program. He also acknowledges support from the NASA Exobiology and Evolutionary Biology program through a subcontract from Rensselaer Polytechnic Institute. A. Vasyunin acknowledges the financial support of the European Research Council (ERC; project PALs 320620) NR 47 TC 14 Z9 14 U1 2 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 74 DI 10.1088/0004-637X/787/1/74 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200074 ER PT J AU Kostov, VB McCullough, PR Carter, JA Deleuil, M Diaz, RF Fabrycky, DC Hebrard, G Hinse, TC Mazeh, T Orosz, JA Tsvetanov, ZI Welsh, WF AF Kostov, V. B. McCullough, P. R. Carter, J. A. Deleuil, M. Diaz, R. F. Fabrycky, D. C. Hebrard, G. Hinse, T. C. Mazeh, T. Orosz, J. A. Tsvetanov, Z. I. Welsh, W. F. TI KEPLER-413B: A SLIGHTLY MISALIGNED, NEPTUNE-SIZE TRANSITING CIRCUMBINARY PLANET (vol 784, pg 14, 2014) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Kostov, V. B.; McCullough, P. R.; Tsvetanov, Z. I.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Kostov, V. B.; McCullough, P. R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Carter, J. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Deleuil, M.; Diaz, R. F.] Lab Astrophys Marseille, F-13388 Marseille 13, France. [Fabrycky, D. C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Hebrard, G.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Hebrard, G.] Univ Aix Marseille, Observ Haute Provence, F-04870 St Michel lObservatoire, France. [Hebrard, G.] CNRS, F-04870 St Michel lObservatoire, France. [Hinse, T. C.] Korea Astron & Space Sci Inst KASI, Adv Astron & Space Sci Div, Taejon 305348, South Korea. [Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Mazeh, T.] Tel Aviv Univ, Dept Astron & Astrophys, IL-69978 Tel Aviv, Israel. [Orosz, J. A.; Welsh, W. F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Kostov, VB (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. EM vkostov@pha.jhu.edu NR 1 TC 4 Z9 4 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 20 PY 2014 VL 787 IS 1 AR 93 DI 10.1088/0004-637X/787/1/93 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200093 ER PT J AU Landi, E Testa, P AF Landi, E. Testa, P. TI THE TEMPERATURE OF QUIESCENT STREAMERS DURING SOLAR CYCLES 23 AND 24 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: evolution ID WIND SCALING LAW; R-CIRCLE-DOT; X-RAY STAR; EMISSION MEASURE; SUMER TELESCOPE; ATOMIC DATABASE; ACTIVE REGIONS; QUIET REGIONS; MAGNETIC-FLUX; INNER CORONA AB Recent in-situ determinations of the temporal evolution of the charge state distribution in the fast and slow solar wind have shown a general decrease in the degree of ionization of all the elements in the solar wind along solar cycles 23 and 24. Such a decrease has been interpreted as a cooling of the solar corona which occurred during the decline and minimum phase of solar cycle 23 from 2000 to 2010. In the present work, we investigate whether spectroscopic determinations of the temperature of the quiescent streamers show signatures of coronal plasma cooling during cycles 23 and 24. We measure the coronal electron density and thermal structure at the base of 60 quiescent streamers observed from 1996 to 2013 by SOHO/SUMER and Hinode/EIS and find that both quantities do now show any significant dependence on the solar cycle. We argue that if the slow solar wind is accelerated from the solar photosphere or chromosphere, the measured decrease in the in-situ wind charge state distribution might be due to an increased efficiency in the wind acceleration mechanism at low altitudes. If the slow wind originates from the corona, a combination of density and wind acceleration changes may be responsible for the in-situ results. C1 [Landi, E.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Testa, P.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Landi, E (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. FU NASA [NNX11AC20G, NNX10AF29G] FX The work of E.L. was supported by NASA grant NNX11AC20G; the work of P.T. is supported by NASA grants NNX11AC20G and NNX10AF29G. We thank the referee for very useful comments that helped improve the original manuscript. NR 60 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 20 PY 2014 VL 787 IS 1 AR 33 DI 10.1088/0004-637X/787/1/33 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200033 ER PT J AU Marinucci, A Matt, G Miniutti, G Guainazzi, M Parker, ML Brenneman, L Fabian, AC Kara, E Arevalo, P Ballantyne, DR Boggs, SE Cappi, M Christensen, FE Craig, WW Elvis, M Hailey, CJ Harrison, FA Reynolds, CS Risaliti, G Stern, DK Walton, DJ Zhang, W AF Marinucci, A. Matt, G. Miniutti, G. Guainazzi, M. Parker, M. L. Brenneman, L. Fabian, A. C. Kara, E. Arevalo, P. Ballantyne, D. R. Boggs, S. E. Cappi, M. Christensen, F. E. Craig, W. W. Elvis, M. Hailey, C. J. Harrison, F. A. Reynolds, C. S. Risaliti, G. Stern, D. K. Walton, D. J. Zhang, W. TI THE BROADBAND SPECTRAL VARIABILITY OF MCG-6-30-15 OBSERVED BY NUSTAR AND XMM-NEWTON SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: Seyfert; X-rays: individual (MCG-6-30-015) ID ACTIVE GALACTIC NUCLEI; 1 GALAXY MCG-6-30-15; X-RAY VARIABILITY; K-ALPHA LINE; PHOTON IMAGING CAMERA; DUSTY WARM ABSORBER; BLACK-HOLE; IRON LINE; SUZAKU OBSERVATIONS; SEYFERT-1 GALAXIES AB MCG-6-30-15, at a distance of 37 Mpc (z = 0.008), is the archetypical Seyfert 1 galaxy showing very broad Fe K alpha emission. We present results from a joint NuSTAR and XMM-Newton observational campaign that, for the first time, allows a sensitive, time-resolved spectral analysis from 0.35 keV up to 80 keV. The strong variability of the source is best explained in terms of intrinsic X-ray flux variations and in the context of the light-bending model: the primary, variable emission is reprocessed by the accretion disk, which produces secondary, less variable, reflected emission. The broad Fe K alpha profile is, as usual for this source, well explained by relativistic effects occurring in the innermost regions of the accretion disk around a rapidly rotating black hole. We also discuss the alternative model in which the broadening of the Fe K alpha is due to the complex nature of the circumnuclear absorbing structure. Even if this model cannot be ruled out, it is disfavored on statistical grounds. We also detected an occultation event likely caused by broad-line region clouds crossing the line of sight. C1 [Marinucci, A.; Matt, G.] Univ Rome, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Marinucci, A.; Miniutti, G.] ESAC, Dep Astrofis, Ctr Astrobiol CSIC INTA, Madrid, Spain. [Guainazzi, M.] European Space Astron Ctr ESA, E-28080 Madrid, Spain. [Parker, M. L.; Fabian, A. C.; Kara, E.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Brenneman, L.; Elvis, M.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Arevalo, P.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 22, Chile. [Arevalo, P.] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Cappi, M.] IASF Bologna, INAF, I-40129 Bologna, Italy. [Christensen, F. E.] Danish Tech Univ, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Craig, W. W.; Hailey, C. J.; Walton, D. J.] Columbia Univ, New York, NY 10027 USA. [Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Stern, D. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Marinucci, A (reprint author), Univ Rome, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy. RI Miniutti, Giovanni/L-2721-2014; Boggs, Steven/E-4170-2015; Cappi, Massimo/F-4813-2015; OI Miniutti, Giovanni/0000-0003-0707-4531; Boggs, Steven/0000-0001-9567-4224; Cappi, Massimo/0000-0001-6966-8920; Risaliti, Guido/0000-0002-3556-977X FU Fondazione Angelo Della Riccia.; Italian Space Agency [ASI/INAF I/037/12/0-011/13]; European Union Seventh Framework Programme (FP7) [312789]; Anillo [ACT1101]; NASA [NNG08FD60C]; California Institute of Technology; National Aeronautics and Space Administration.; NuSTAR Operations, Software, and Calibration; NuSTAR Data Analysis Software (NuSTARDAS); ASI Science Data Center (ASDC, Italy); California Institute of Technology (USA) FX A. M. acknowledges financial support from Fondazione Angelo Della Riccia. A. M. and G. M. acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. A. M., G. Matt, G. Miniutti, A. C. F., and E. K. acknowledge financial support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789. P. A. acknowledges financial support from Anillo ACT1101. 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). NR 76 TC 26 Z9 26 U1 3 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 MAY 20 PY 2014 VL 787 IS 1 AR 83 DI 10.1088/0004-637X/787/1/83 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200083 ER PT J AU Mudd, D Mathur, S Guainazzi, M Piconcelli, E Bianchi, S Komossa, S Vignali, C Lanzuisi, G Nicastro, F Fiore, F Maiolino, R AF Mudd, Dale Mathur, Smita Guainazzi, Matteo Piconcelli, Enrico Bianchi, Stefano Komossa, S. Vignali, Cristian Lanzuisi, Giorgio Nicastro, Fabrizio Fiore, Fabrizio Maiolino, Roberto TI XMM-NEWTON OBSERVATIONS OF THREE INTERACTING LUMINOUS INFRARED GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: interactions; galaxies: nuclei; galaxies: starburst; infrared: galaxies; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; X-RAY-EMISSION; SUPERMASSIVE BLACK-HOLES; DIGITAL SKY SURVEY; COMPLEX HOT ISM; SIMILAR-TO 2; FORMATION RATES; OPTICAL CLASSIFICATION; CHEMICAL ENRICHMENT AB We investigate the X-ray properties of three interacting luminous infrared galaxy systems. In one of these systems, IRAS 18329+5950, we resolve two separate sources. A second and third source, IRAS 19354+4559 and IRAS 20550+1656, have only a single X-ray source detected. We compare the observed emission to point-spread function (PSF) profiles and determine that they are all consistent with the PSF, albeit with large uncertainties for some of our sources. We then model the spectra to determine soft (0.5-2 keV) and hard (2-10 keV) luminosities for the resolved sources and compare these to relationships found in the literature between infrared and X-ray luminosities for starburst galaxies. We obtain luminosities (0.5-10 keV) ranging from 1.7 to 7.3x10(41) erg s(-1) for our systems. These X-ray luminosities are consistent with predictions for star-formation-dominated sources and thus are most likely due to starbursts, but we cannot conclusively rule out active galactic nuclei. C1 [Mudd, Dale; Mathur, Smita] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Mathur, Smita] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Guainazzi, Matteo] ESA, European Space Astron Ctr, E-28691 Madrid, Spain. [Piconcelli, Enrico; Nicastro, Fabrizio] Osservatorio Astron Roma INAF, I-00040 Monte Porzio Catone, RM, Italy. [Bianchi, Stefano] Univ Roma Tre, Dipartimento Fis, I-00416 Rome, Italy. [Komossa, S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Vignali, Cristian] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Lanzuisi, Giorgio] INAF Ist Astrofis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy. [Nicastro, Fabrizio] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fiore, Fabrizio] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Maiolino, Roberto] Univ Cambridge, Dept Phys, Cambridge CB3 0HE, England. [Maiolino, Roberto] Kavli Inst Cosmol, Cambridge CB3 0HA, England. RP Mudd, D (reprint author), Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. EM mudd@astronomy.ohio-state.edu RI Lanzuisi, Giorgio/K-4378-2013; Vignali, Cristian/J-4974-2012; Bianchi, Stefano/B-4804-2010; OI Lanzuisi, Giorgio/0000-0001-9094-0984; Vignali, Cristian/0000-0002-8853-9611; Bianchi, Stefano/0000-0002-4622-4240; Nicastro, Fabrizio/0000-0002-6896-1364; piconcelli, enrico/0000-0001-9095-2782; Mudd, Dale/0000-0003-2371-4121; Fiore, Fabrizio/0000-0002-4031-4157 NR 83 TC 0 Z9 0 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 40 DI 10.1088/0004-637X/787/1/40 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200040 ER PT J AU Park, H Han, C Gould, A Udalski, A Sumi, T Fouque, P Choi, JY Christie, G Depoy, DL Dong, S Gaudi, BS Hwang, KH Jung, YK Kavka, A Lee, CU Monard, LAG Natusch, T Ngan, H Pogge, RW Shin, IG Yee, JC Szymanski, MK Kubiak, M Soszynski, I Pietrzynski, G Poleski, R Ulaczyk, K Pietrukowicz, P Kozlowski, S Skowron, J Wyrzykowski, L Abe, F Bennett, DP Bond, IA Botzler, CS Chote, P Freeman, M Fukui, A Fukunaga, D Harris, P Itow, Y Koshimoto, N Ling, CH Masuda, K Matsubara, Y Muraki, Y Namba, S Ohnishi, K Rattenbury, NJ Saito, T Sullivan, DJ Sweatman, WL Suzuki, D Tristram, PJ Wada, K Yamai, N Yock, PCM Yonehara, A AF Park, H. Han, C. Gould, A. Udalski, A. Sumi, T. Fouque, P. Choi, J. -Y. Christie, G. Depoy, D. L. Dong, Subo Gaudi, B. S. Hwang, K. -H. Jung, Y. K. Kavka, A. Lee, C. -U. Monard, L. A. G. Natusch, T. Ngan, H. Pogge, R. W. Shin, I. -G. Yee, J. C. Szymanski, M. K. Kubiak, M. Soszynski, I. Pietrzynski, G. Poleski, R. Ulaczyk, K. Pietrukowicz, P. Kozlowski, S. Skowron, J. Wyrzykowski, L. Abe, F. Bennett, D. P. Bond, I. A. Botzler, C. S. Chote, P. Freeman, M. Fukui, A. Fukunaga, D. Harris, P. Itow, Y. Koshimoto, N. Ling, C. H. Masuda, K. Matsubara, Y. Muraki, Y. Namba, S. Ohnishi, K. Rattenbury, N. J. Saito, To. Sullivan, D. J. Sweatman, W. L. Suzuki, D. Tristram, P. J. Wada, K. Yamai, N. Yock, P. C. M. Yonehara, A. CA FUN Collaboration OGLE Collaboration MOA Collaboration TI OGLE-2012-BLG-0455/MOA-2012-BLG-206: MICROLENSING EVENT WITH AMBIGUITY IN PLANETARY INTERPRETATIONS CAUSED BY INCOMPLETE COVERAGE OF PLANETARY SIGNAL SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing: micro; planets and satellites: general ID GRAVITATIONAL BINARY-LENS; DIFFERENCE IMAGE-ANALYSIS; GALACTIC BULGE; PHOTOMETRY; SYSTEMS; MASS; PERTURBATIONS AB Characterizing a microlensing planet is done by modeling an observed lensing light curve. In this process, it is often confronted that solutions of different lensing parameters result in similar light curves, causing difficulties in uniquely interpreting the lens system, and thus understanding the causes of different types of degeneracy is important. In this work, we show that incomplete coverage of a planetary perturbation can result in degenerate solutions even for events where the planetary signal is detected with a high level of statistical significance. We demonstrate the degeneracy for an actually observed event OGLE-2012-BLG-0455/MOA-2012-BLG-206. The peak of this high-magnification event (A(max) similar to 400) exhibits very strong deviation from a point-lens model with Delta chi(2) greater than or similar to 4000 for data sets with a total of 6963 measurements. From detailed modeling of the light curve, we find that the deviation can be explained by four distinct solutions, i.e., two very different sets of solutions, each with a twofold degeneracy. While the twofold (so-called close/wide) degeneracy is well understood, the degeneracy between the radically different solutions is not previously known. The model light curves of this degeneracy differ substantially in the parts that were not covered by observation, indicating that the degeneracy is caused by the incomplete coverage of the perturbation. It is expected that the frequency of the degeneracy introduced in this work will be greatly reduced with the improvement of the current lensing survey and follow-up experiments and the advent of new surveys. C1 [Park, H.; Han, C.; Choi, J. -Y.; Hwang, K. -H.; Jung, Y. K.; Shin, I. -G.] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Chongju 371763, South Korea. [Gould, A.; Gaudi, B. S.; Kavka, A.; Pogge, R. W.; Yee, J. C.; Poleski, R.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Udalski, A.; Szymanski, M. K.; Kubiak, M.; Soszynski, I.; Pietrzynski, G.; Poleski, R.; Ulaczyk, K.; Pietrukowicz, P.; Kozlowski, S.; Skowron, J.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Sumi, T.; Koshimoto, N.; Namba, S.; Suzuki, D.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Fouque, P.] Univ Toulouse, CNRS, IRAP, F-31400 Toulouse, France. [Christie, G.; Natusch, T.; Ngan, H.] Auckland Observ, Auckland, New Zealand. [Depoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Dong, Subo] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Monard, L. A. G.] Kleinkaroo Observ, Calitzdorp, South Africa. [Monard, L. A. G.] Bronberg Observ, Pretoria, South Africa. [Natusch, T.] AUT Univ, Inst Radiophys & Space Res, Auckland, New Zealand. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Abe, F.; Fukunaga, D.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Bond, I. A.; Ling, C. H.; Sweatman, W. L.] Massey Univ, North Shore Mail Ctr, Inst Informat & Math Sci, Auckland, New Zealand. [Botzler, C. S.; Freeman, M.; Rattenbury, N. J.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1001, New Zealand. [Chote, P.; Harris, P.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand. [Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Saito, To.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan. [Tristram, P. J.] Mt John Univ Observ, Lake Tekapo 8770, New Zealand. [Yamai, N.; Yonehara, A.] Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kyoto 6038555, Japan. RP Park, H (reprint author), Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Chongju 371763, South Korea. RI Skowron, Jan/M-5186-2014; Kozlowski, Szymon/G-4799-2013 OI Skowron, Jan/0000-0002-2335-1730; Kozlowski, Szymon/0000-0003-4084-880X FU Creative Research Initiative Program of the National Research Foundation of Korea [2009-0081561]; NSF [AST-1103471, AST-0807444]; NASA [NNX12AB99G]; European Research Council under the European Community's Seventh Framework Programme (FP7)/ERC [246678]; JSPS [JSPS23540339, JSPS19340058]; IAS; NASA through the Sagan Fellowship Program; [JSPS22403003]; [JSPS23340064]; [JSPS24253004]; [JSPS23340044] FX Work by C.H. was supported by the Creative Research Initiative Program (2009-0081561) of the National Research Foundation of Korea. A.G. and B.S.G. acknowledge support from NSF AST-1103471. B.S.G., A.G., and R.W.P. acknowledge support from NASA grant NNX12AB99G. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 246678 to A.U. The MOA experiment was supported by grants JSPS22403003 and JSPS23340064. T.S. acknowledges the support from the grant JSPS24253004. T.S. is supported by the grant JSPS23340044. Y.M. acknowledges support from JSPS grants JSPS23540339 and JSPS19340058. S.D. was supported through a Ralph E. and Doris M. Hansmann Membership at the IAS and NSF grant AST-0807444. Work by J.C.Y. was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. NR 33 TC 2 Z9 2 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 71 DI 10.1088/0004-637X/787/1/71 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200071 ER PT J AU Quinn, SN White, RJ Latham, DW Buchhave, LA Torres, G Stefanik, RP Berlind, P Bieryla, A Calkins, MC Esquerdo, GA Furesz, G Geary, JC Szentgyorgyi, AH AF Quinn, Samuel N. White, Russel J. Latham, David W. Buchhave, Lars A. Torres, Guillermo Stefanik, Robert P. Berlind, Perry Bieryla, Allyson Calkins, Michael C. Esquerdo, Gilbert A. Furesz, Gabor Geary, John C. Szentgyorgyi, Andrew H. TI HD 285507b: AN ECCENTRIC HOT JUPITER IN THE HYADES OPEN CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations: individual (Hyades, Melotte 25); planets and satellites: detection; planets and satellites: dynamical evolution and stability; planet-star interactions; stars: individual (HD 285507) ID SINGLE-PLANET SYSTEMS; T-TAURI STAR; GIANT PLANETS; STELLAR POPULATIONS; RADIAL-VELOCITIES; TRANSIT SURVEYS; MASS STARS; EVOLUTION; ROTATION; EXOPLANETS AB We report the discovery of the first hot Jupiter in the Hyades open cluster. HD 285507b orbits a V = 10.47 K4.5V dwarf (M-* = 0.734M(circle dot) ; R-* = 0.656R(circle dot)) in a slightly eccentric (e = 0.086(-0.019)(+0.018)) orbit with a period of 6.0881(-0.0018) (+0.0019) days. The induced stellar radial velocity corresponds to a minimum companion mass ofM(P) sin i = 0.917 +/- 0.033M(Jup). Line bisector spans and stellar activity measures show no correlation with orbital phase, and the radial velocity amplitude is independent of wavelength, supporting the conclusion that the variations are caused by a planetary companion. Follow-up photometry indicates with high confidence that the planet does not transit. HD 285507b joins a small but growing list of planets in open clusters, and its existence lends support to a planet formation scenario in which a high stellar space density does not inhibit giant planet formation and migration. We calculate the circularization timescale for HD 285507b to be larger than the age of the Hyades, which may indicate that this planet's non-zero eccentricity is the result of migration via interactions with a third body. We also demonstrate a significant difference between the eccentricity distributions of hot Jupiters that have had time to tidally circularize and those that have not, which we interpret as evidence against Type II migration in the final stages of hot Jupiter formation. Finally, the dependence of the circularization timescale on the planetary tidal quality factor, Q(P), allows us to constrain the average value for hot Jupiters to be logQ(P) = 6.14(-0.25)(+0.41). C1 [Quinn, Samuel N.; White, Russel J.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Latham, David W.; Buchhave, Lars A.; Torres, Guillermo; Stefanik, Robert P.; Berlind, Perry; Bieryla, Allyson; Calkins, Michael C.; Esquerdo, Gilbert A.; Furesz, Gabor; Geary, John C.; Szentgyorgyi, Andrew H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. RP Quinn, SN (reprint author), Georgia State Univ, Dept Phys & Astron, 25 Pk Pl NE Suite 605, Atlanta, GA 30303 USA. OI Buchhave, Lars A./0000-0003-1605-5666 FU National Aeronautics and Space Administration (NASA) [NNX11AC32G]; NSF Graduate Research Fellowship [DGE-1051030]; NASA's Kepler mission [NNX11AB99A]; Smithsonian Astrophysical Observatory; NSF [AST-1007992] FX We thank Josh Winn, Tsevi Mazeh, and an anonymous referee for insightful comments and discussion, and Greg Feiden for producing a Dartmouth isochrone appropriate for our analysis. This research has made use of The Extrasolar Planets Encyclopaedia. The material herein is based upon work supported by the National Aeronautics and Space Administration (NASA) under grant No. NNX11AC32G issued through the Origins of Solar Systems program. S.N.Q. is supported by an NSF Graduate Research Fellowship, grant DGE-1051030. D.W.L. acknowledges partial support from NASA's Kepler mission under cooperative agreement NNX11AB99A with the Smithsonian Astrophysical Observatory. G.T. acknowledges partial support from NSF grant AST-1007992. NR 83 TC 22 Z9 22 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2014 VL 787 IS 1 AR 27 DI 10.1088/0004-637X/787/1/27 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200027 ER PT J AU Sankrit, R Raymond, JC Bautista, M Gaetz, TJ Williams, BJ Blair, WP Borkowski, KJ Long, KS AF Sankrit, Ravi Raymond, John C. Bautista, Manuel Gaetz, Terrance J. Williams, Brian J. Blair, William P. Borkowski, Kazimierz J. Long, Knox S. TI SPITZER IRS OBSERVATIONS OF THE XA REGION IN THE CYGNUS LOOP SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; ISM: abundances; ISM: individual objects (Cygnus Loop); ISM: supernova remnants ID SPACE-TELESCOPE; INFRARED SPECTROGRAPH; INTERSTELLAR-MEDIUM; ATOMIC DATABASE; EMISSION-LINES; SHOCK-WAVE; SPECTROSCOPY; EXCITATION; RAY; DUST AB We report on spectra of two positions in the XA region of the Cygnus Loop supernova remnant obtained with the InfraRed Spectrograph on the Spitzer Space Telescope. The spectra span the 10-35 mu m wavelength range, which contains a number of collisionally excited forbidden lines. These data are supplemented by optical spectra obtained at the Whipple Observatory and an archival UV spectrum from the International Ultraviolet Explorer. Coverage from the UV through the IR provides tests of shock wave models and tight constraints on model parameters. Only lines from high ionization species are detected in the spectrum of a filament on the edge of the remnant. The filament traces a 180 km s(-1) shock that has just begun to cool, and the oxygen to neon abundance ratio lies in the normal range found for Galactic H II regions. Lines from both high and low ionization species are detected in the spectrum of the cusp of a shock-cloud interaction, which lies within the remnant boundary. The spectrum of the cusp region is matched by a shock of about 150 km s(-1) that has cooled and begun to recombine. The post-shock region has a swept-up column density of about 1.3 x 10(18) cm(-2), and the gas has reached a temperature of 7000-8000 K. The spectrum of the Cusp indicates that roughly half of the refractory silicon and iron atoms have been liberated from the grains. Dust emission is not detected at either position. C1 [Sankrit, Ravi] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Raymond, John C.; Gaetz, Terrance J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Bautista, Manuel] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Williams, Brian J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Borkowski, Kazimierz J.] N Carolina State Univ, Raleigh, NC 27607 USA. [Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Sankrit, R (reprint author), NASA, Ames Res Ctr, SOFIA Sci Ctr, M-S N211-3, Moffett Field, CA 94035 USA. OI Blair, William/0000-0003-2379-6518 FU JPL Award [1278412]; North Carolina State University, Raleigh; USRA at the SOFIA Science Center; NASA [NAS8-03060]; Chandra X-ray Center FX This work was supported in part by the JPL Award 1278412 to the University of California, Berkeley, and North Carolina State University, Raleigh. We thank the anonymous referee for several useful suggestions, one of which led to Figure 9, providing a visual comparison of model predictions with observations. RS acknowledges support from USRA at the SOFIA Science Center. T.J.G. acknowledges support under NASA contract NAS8-03060 with the Chandra X-ray Center. NR 49 TC 5 Z9 5 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 2014 VL 787 IS 1 AR 3 DI 10.1088/0004-637X/787/1/3 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200003 ER PT J AU Sironi, L Giannios, D AF Sironi, Lorenzo Giannios, Dimitrios TI RELATIVISTIC PAIR BEAMS FROM TeV BLAZARS: A SOURCE OF REPROCESSED GeV EMISSION RATHER THAN INTERGALACTIC HEATING SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: general; instabilities; intergalactic medium; plasmas; radiation mechanisms: non-thermal ID EXTRAGALACTIC MAGNETIC-FIELDS; PARTICLE-ACCELERATION; COSMOLOGICAL IMPACT; COSMIC VOIDS; 2-STREAM INSTABILITY; COLLISIONLESS SHOCKS; WEIBEL INSTABILITY; BACKGROUND LIGHT; PIC SIMULATIONS; ELECTRON-BEAM AB The interaction of TeV photons from blazars with the extragalactic background light produces a relativistic beam of electron-positron pairs streaming through the intergalactic medium (IGM). The fate of the beam energy is uncertain. By means of two-and three-dimensional particle-in-cell simulations, we study the nonlinear evolution of dilute ultra-relativistic pair beams propagating through the IGM. We explore a wide range of beam Lorentz factors.gamma(b) >> 1 and beam-to-plasma density ratios a << 1, so that our results can be extrapolated to the extreme parameters of blazar-induced beams (gamma(b) similar to 10(6) and a similar to 10 (15), for powerful blazars). For cold beams, we show that the oblique instability governs the early stages of evolution, but its exponential growth terminates-due to self-heating of the beam in the transverse direction-when only a negligible fraction similar to (a/gamma(b))(1/3) similar to 10(-7) of the beam energy has been transferred to the IGM plasma. Further relaxation of the beam proceeds through quasi-longitudinal modes, until the momentum dispersion in the direction of propagation saturates at Delta Pb,vertical bar vertical bar /gamma bm(e)c similar to 0.2. This corresponds to a fraction similar to 10% of the beam energy-irrespective of gamma(b) or a-being ultimately transferred to the IGM plasma (as compared to the heating efficiency of similar to 50% predicted by one-dimensional models, which cannot properly account for the transverse broadening of the beam). For the warm beams generated by TeV blazars, the development of the longitudinal relaxation is suppressed, since the initial dispersion in beam momentum is already Delta Pb0,vertical bar vertical bar /gamma bm(e)c >= 1. Here, the fraction of beam energy ultimately deposited into the IGM is only similar to a gamma(b) similar to 10(-9). It follows that most of the beam energy is still available to power the GeV emission produced by inverse Compton up-scattering of the cosmic microwave background by the beam pairs. C1 [Sironi, Lorenzo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sironi, Lorenzo; Giannios, Dimitrios] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. RP Sironi, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lsironi@cfa.harvard.edu; dgiannio@purdue.edu FU NASA through Einstein Postdoctoral Fellowship [PF1-120090]; Chandra X-ray Center FX We thank A. Bret, M. Dieckmann, and the anonymous referee for insightful comments. L. S. is supported by NASA through Einstein Postdoctoral Fellowship grant number PF1-120090 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. The simulations were performed on XSEDE resources under contract No. TG-AST120010, and on NASA High-End Computing (HEC) resources through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 56 TC 24 Z9 24 U1 2 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 MAY 20 PY 2014 VL 787 IS 1 AR 49 DI 10.1088/0004-637X/787/1/49 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200049 ER PT J AU Smith, RK Foster, AR Edgar, RJ Brickhouse, NS AF Smith, Randall K. Foster, Adam R. Edgar, Richard J. Brickhouse, Nancy S. TI RESOLVING THE ORIGIN OF THE DIFFUSE SOFT X-RAY BACKGROUND SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: bubbles; radiation mechanisms: general; Sun: particle emission; X-rays: diffuse background ID WIND CHARGE-TRANSFER; SOLAR-WIND; LOCAL BUBBLE; EMISSION; SPECTROMETER; COLLISIONS; IONS; GAS AB The ubiquitous diffuse soft (1/4 keV) X-ray background was one of the earliest discoveries of X-ray astronomy. At least some of the emission may arise from charge exchange between solar wind ions and neutral atoms in the heliosphere, but no detailed models have been fit to the available data. Here, we report on a new model for charge exchange in the solar wind, which, when combined with a diffuse hot plasma component, filling the Local Cavity provides a good fit to the only available high-resolution soft X-ray and extreme ultraviolet spectra using plausible parameters for the solar wind. The implied hot plasma component is in pressure equilibrium with the local cloud that surrounds the solar system, creating for the first time a self-consistent picture of the local interstellar medium. C1 [Smith, Randall K.; Foster, Adam R.; Edgar, Richard J.; Brickhouse, Nancy S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Smith, RK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Brickhouse, Nancy/0000-0002-8704-4473; Smith, Randall/0000-0003-4284-4167 FU NASA [NNX09AC71G, TM1-12004X] FX We thank John Raymond and Brad Wargelin for discussions and Jeffrey Morgenthaler for the original DXS data analysis and calibration, and most particularly the DXS PI Wilton Sanders, without whom this work would not have been possible. This work was funded by NASA ADP NNX09AC71G and Chandra grant TM1-12004X. NR 22 TC 14 Z9 14 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 2014 VL 787 IS 1 AR 77 DI 10.1088/0004-637X/787/1/77 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200077 ER PT J AU van Ballegooijen, AA Asgari-Targhi, M Berger, MA AF van Ballegooijen, A. A. Asgari-Targhi, M. Berger, M. A. TI ON THE RELATIONSHIP BETWEEN PHOTOSPHERIC FOOTPOINT MOTIONS AND CORONAL HEATING IN SOLAR ACTIVE REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); Sun: corona; Sun: magnetic fields; turbulence ID ALFVEN-WAVE TURBULENCE; AB-INITIO APPROACH; MAGNETIC-FIELD; MAGNETOHYDRODYNAMIC TURBULENCE; TRANSITION REGION; MHD-TURBULENCE; ENERGY-RELEASE; PARKER PROBLEM; BRIGHT POINTS; SCALING LAWS AB Coronal heating theories can be classified as either direct current (DC) or alternating current (AC) mechanisms, depending on whether the coronal magnetic field responds quasi-statically or dynamically to the photospheric footpoint motions. In this paper we investigate whether photospheric footpoint motions with velocities of 1-2 km s(-1) can heat the corona in active regions, and whether the corona responds quasi-statically or dynamically to such motions (DC versus AC heating). We construct three-dimensional magnetohydrodynamic models for the Alfven waves and quasi-static perturbations generated within a coronal loop. We find that in models where the effects of the lower atmosphere are neglected, the corona responds quasi-statically to the footpoint motions (DC heating), but the energy flux into the corona is too low compared to observational requirements. In more realistic models that include the lower atmosphere, the corona responds more dynamically to the footpoint motions (AC heating) and the predicted heating rates due to Alfven wave turbulence are sufficient to explain the observed hot loops. The higher heating rates are due to the amplification of Alfven waves in the lower atmosphere. We conclude that magnetic braiding is a highly dynamic process. C1 [van Ballegooijen, A. A.; Asgari-Targhi, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Berger, M. A.] Univ Exeter, SECAM, Exeter EX4 4QF, Devon, England. RP van Ballegooijen, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS-15, Cambridge, MA 02138 USA. OI van Ballegooijen, Adriaan/0000-0002-5622-3540 FU UK's Engineering and Physical Sciences Research Council [EP/I034327/1]; NASA [NNM07AB07C]; LMSAL [SP02H1701R] FX We thank the anonymous referee for his/her comments which helped to improve this paper. We thank James Klimchuk for discussions that motivated this work. We also thank Stephen Cranmer for discussions and 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, which was funded by the UK's Engineering and Physical Sciences Research Council (EP/I034327/1). This project is supported under contract NNM07AB07C from NASA to the Smithsonian Astrophysical Observatory (SAO) and SP02H1701R from LMSAL to SAO. NR 85 TC 27 Z9 27 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 20 PY 2014 VL 787 IS 1 AR 87 DI 10.1088/0004-637X/787/1/87 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH2AX UT WOS:000335924200087 ER PT J AU Caldwell, N Strader, J Romanowsky, AJ Brodie, JP Moore, B Diemand, J Martizzi, D AF Caldwell, Nelson Strader, Jay Romanowsky, Aaron J. Brodie, Jean P. Moore, Ben Diemand, Jurg Martizzi, Davide TI A GLOBULAR CLUSTER TOWARD M87 WITH A RADIAL VELOCITY <-1000 km s(-1): THE FIRST HYPERVELOCITY CLUSTER SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: clusters: individual (Virgo); galaxies: individual (M87); galaxies: kinematics and dynamics; galaxies: star clusters: general; globular clusters: general ID SUPERMASSIVE BLACK-HOLES; DIGITAL SKY SURVEY; MILKY-WAY HALO; VIRGO CLUSTER; STAR-CLUSTERS; STELLAR-SYSTEMS; NEARBY GALAXIES; GALACTIC-CENTER; MASS; KINEMATICS AB We report the discovery of an object near M87 in the Virgo Cluster with an extraordinary blueshift of -1025 km s(-1), offset from the systemic velocity by >2300 km s(-1). Evaluation of photometric and spectroscopic data provides strong evidence that this object is a distant massive globular cluster, which we call HVGC-1 in analogy to Galactic hypervelocity stars. We consider but disfavor more exotic interpretations, such as a system of stars bound to a recoiling black hole. The odds of observing an outlier as extreme as HVGC-1 in a virialized distribution of intracluster objects are small; it appears more likely that the cluster was (or is being) ejected from Virgo following a three-body interaction. The nature of the interaction is unclear, and could involve either a subhalo or a binary supermassive black hole at the center of M87. C1 [Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Romanowsky, Aaron J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Romanowsky, Aaron J.; Brodie, Jean P.] Univ Calif Observ, Santa Cruz, CA 95064 USA. [Moore, Ben; Diemand, Jurg] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland. [Martizzi, Davide] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Caldwell, N (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM caldwell@cfa.harvard.edu RI Diemand, Juerg/G-9448-2011 FU NSF [AST-1211995, AST-1109878] FX Data are from MMT and CFHT. Help was provided by SAO/OIR TDC. Support by NSF/AST-1211995 and AST-1109878. NR 42 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 20 PY 2014 VL 787 IS 1 AR L11 DI 10.1088/2041-8205/787/1/L11 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH3PE UT WOS:000336035800011 ER PT J AU Prieto, JL Rest, A Bianco, FB Matheson, T Smith, N Walborn, NR Hsiao, EY Chornock, R Alvarez, LP Campillay, A Contreras, C Gonzalez, C James, D Knapp, GR Kunder, A Margheim, S Morrell, N Phillips, MM Smith, RC Welch, DL Zenteno, A AF Prieto, J. L. Rest, A. Bianco, F. B. Matheson, T. Smith, N. Walborn, N. R. Hsiao, E. Y. Chornock, R. Paredes Alvarez, L. Campillay, A. Contreras, C. Gonzalez, C. James, D. Knapp, G. R. Kunder, A. Margheim, S. Morrell, N. Phillips, M. M. Smith, R. C. Welch, D. L. Zenteno, A. TI LIGHT ECHOES FROM eta CARINAE'S GREAT ERUPTION: SPECTROPHOTOMETRIC EVOLUTION AND THE RAPID FORMATION OF NITROGEN-RICH MOLECULES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; stars: evolution; stars: individual (Eta Carinae); stars: mass-loss ID LARGE-MAGELLANIC-CLOUD; HOMUNCULUS NEBULA; CASSIOPEIA-A; SUPERNOVA; SPECTROSCOPY; VARIABLES; SPECTRUM; TRANSIENTS; ASYMMETRY; DISCOVERY AB We present follow-up optical imaging and spectroscopy of one of the light echoes of eta Carinae's nineteenth century Great Eruption discovered by Rest et al. By obtaining images and spectra at the same light echo position between 2011 and 2014, we follow the evolution of the Great Eruption on a 3 yr timescale. We find remarkable changes in the photometric and spectroscopic evolution of the echo light. The i-band light curve shows a decline of similar to 0.9 mag in similar to 1 yr after the peak observed in early 2011 and a flattening at later times. The spectra show a pure-absorption early G-type stellar spectrum at peak, but a few months after peak the lines of the Ca II triplet develop strong P-Cygni profiles and we see the appearance of [Ca II] 7291, 7324 doublet in emission. These emission features and their evolution in time resemble those observed in the spectra of some Type IIn supernovae and supernova impostors. Most surprisingly, starting similar to 300 days after peak brightness, the spectra show strong molecular transitions of CN at greater than or similar to 6800 angstrom. The appearance of these CN features can be explained if the ejecta are strongly nitrogen enhanced, as is observed in modern spectroscopic studies of the bipolar Homunculus nebula. Given the spectroscopic evolution of the light echo, velocities of the main features, and detection of strong CN, we are likely seeing ejecta that contributes directly to the Homunculus nebula. C1 [Prieto, J. L.; Knapp, G. R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Rest, A.; Walborn, N. R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Bianco, F. B.] NYU, Dept Phys, New York, NY 10012 USA. [Bianco, F. B.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10012 USA. [Matheson, T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Smith, N.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Hsiao, E. Y.; Campillay, A.; Contreras, C.; Gonzalez, C.; Morrell, N.; Phillips, M. M.] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Chornock, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Paredes Alvarez, L.; James, D.; Smith, R. C.; Zenteno, A.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. [Contreras, C.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Kunder, A.] Leibniz Inst Astrophys Potsdam, D-14482 Potsdam, Germany. [Margheim, S.] Southern Operat Ctr, Gemini Observ, La Serena, Chile. [Welch, D. L.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. RP Prieto, JL (reprint author), Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane, Princeton, NJ 08544 USA. FU Hubble Space Telescope programs [GO-12577, AR-12851, GO-13486]; NSF [AST-1312221]; U.S. DoE (Spain); NSF (Spain); MECD (Spain); STFC (UK); HEFCE (England); NCSA (Brazil); KICP (Brazil); FINEP (Brazil); FAPERJ (Brazil); CNPq (Brazil); GRF FX We thank H. Bond, J. Dolence, J. Murphy, and R. Wing for discussions. We thank R. Foley for help in one of the LCO runs. We are indebted to the staff of Las Campanas, CTIO, LCOGT, and Gemini observatories for their assistance. This work was supported by the Hubble Space Telescope programs GO-12577, AR-12851, and GO-13486, and by NSF grant AST-1312221. This work makes use of observations from the LCOGT network. This Letter is based in part on observations obtained at the Gemini Observatory, which is operated by AURA, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the NSF (USA), the NRC (Canada), CONICYT (Chile), the ARC (Australia), CNPq (Brazil), and CONICET (Argentina). This project used data obtained with the Dark Energy Camera (DECam), which was constructed by the Dark Energy Survey (DES) collaborating institutions. Funding for DES, including DECam, has been provided by the U.S. DoE, NSF, MECD (Spain), STFC (UK), HEFCE (England), NCSA, KICP, FINEP, FAPERJ, CNPq (Brazil), the GRF-sponsored cluster of excellence "Origin and Structure of the Universe" and the DES collaborating institutions. NR 46 TC 6 Z9 6 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 20 PY 2014 VL 787 IS 1 AR L8 DI 10.1088/2041-8205/787/1/L8 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH3PE UT WOS:000336035800008 ER PT J AU Winebarger, AR Cirtain, J Golub, L DeLuca, E Savage, S Alexander, C Schuler, T AF Winebarger, Amy R. Cirtain, Jonathan Golub, Leon DeLuca, Edward Savage, Sabrina Alexander, Caroline Schuler, Timothy TI DISCOVERY OF FINELY STRUCTURED DYNAMIC SOLAR CORONA OBSERVED IN THE Hi-C TELESCOPE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: corona ID LOOPS; MOSS AB In the Summer of 2012, the High-resolution Coronal Imager (Hi-C) flew on board a NASA sounding rocket and collected the highest spatial resolution images ever obtained of the solar corona. One of the goals of the Hi-C flight was to characterize the substructure of the solar corona. We therefore examine how the intensity scales from AIA resolution to Hi-C resolution. For each low-resolution pixel, we calculate the standard deviation in the contributing high-resolution pixel intensities and compare that to the expected standard deviation calculated from the noise. If these numbers are approximately equal, the corona can be assumed to be smoothly varying, i.e., have no evidence of substructure in the Hi-C image to within Hi-C's ability to measure it given its throughput and readout noise. A standard deviation much larger than the noise value indicates the presence of substructure. We calculate these values for each low-resolution pixel for each frame of the Hi-C data. On average, 70% of the pixels in each Hi-C image show no evidence of substructure. The locations where substructure is prevalent is in the moss regions and in regions of sheared magnetic field. We also find that the level of substructure varies significantly over the roughly 160 s of the Hi-C data analyzed here. This result indicates that the finely structured corona is concentrated in regions of heating and is highly time dependent. C1 [Winebarger, Amy R.; Cirtain, Jonathan; Savage, Sabrina; Alexander, Caroline] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Golub, Leon; DeLuca, Edward] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schuler, Timothy] SUNY Coll Buffalo, Buffalo, NY 14222 USA. RP Winebarger, AR (reprint author), NASA, George C Marshall Space Flight Ctr, ZP 13, Huntsville, AL 35812 USA. EM amy.r.winebarger@nasa.gov RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Golub, Leon/0000-0001-9638-3082 FU NASA FX We thank the referee for many important observations and comments. We acknowledge the High-resolution Coronal Imager instrument grant funded by NASA's Low Cost Access to Space program. MSFC/NASA led the mission, and partners include the Smithsonian Astrophysical Observatory in Cambridge, MA; Lockheed Martin's Solar Astrophysical Laboratory in Palo Alto, Calif.; the University of Central Lancashire in Lancashire, England; and the Lebedev Physical Institute of the Russian Academy of Sciences in Moscow. NR 10 TC 5 Z9 5 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 20 PY 2014 VL 787 IS 1 AR L10 DI 10.1088/2041-8205/787/1/L10 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH3PE UT WOS:000336035800010 ER PT J AU MacLean, EL Hare, B Nunn, CL Addessi, E Amici, F Anderson, RC Aureli, F Baker, JM Bania, AE Barnard, AM Boogert, NJ Brannon, EM Bray, EE Bray, J Brent, LJN Burkart, JM Call, J Cantlon, JF Cheke, LG Clayton, NS Delgado, MM DiVincenti, LJ Fujita, K Herrmann, E Hiramatsu, C Jacobs, LF Jordan, KE Laude, JR Leimgruber, KL Messer, EJE Moura, ACD Ostojic, L Picard, A Platt, ML Plotnik, JM Range, F Reader, SM Reddy, RB Sandel, AA Santos, LR Schumann, K Seed, AM Sewall, KB Shaw, RC Slocombe, KE Su, YJ Takimoto, A Tan, JZ Tao, R van Schaik, CP Viranyi, Z Visalberghi, E Wade, JC Watanabe, A Widness, J Young, JK Zentall, TR Zhao, YN AF MacLean, Evan L. Hare, Brian Nunn, Charles L. Addessi, Elsa Amici, Federica Anderson, Rindy C. Aureli, Filippo Baker, Joseph M. Bania, Amanda E. Barnard, Allison M. Boogert, Neeltje J. Brannon, Elizabeth M. Bray, Emily E. Bray, Joel Brent, Lauren J. N. Burkart, Judith M. Call, Josep Cantlon, Jessica F. Cheke, Lucy G. Clayton, Nicola S. Delgado, Mikel M. DiVincenti, Louis J. Fujita, Kazuo Herrmann, Esther Hiramatsu, Chihiro Jacobs, Lucia F. Jordan, Kerry E. Laude, Jennifer R. Leimgruber, Kristin L. Messer, Emily J. E. Moura, Antonio C. de A. Ostojic, Ljerka Picard, Alejandra Platt, Michael L. Plotnik, Joshua M. Range, Friederike Reader, Simon M. Reddy, Rachna B. Sandel, Aaron A. Santos, Laurie R. Schumann, Katrin Seed, Amanda M. Sewall, Kendra B. Shaw, Rachael C. Slocombe, Katie E. Su, Yanjie Takimoto, Ayaka Tan, Jingzhi Tao, Ruoting van Schaik, Carel P. Viranyi, Zsoia Visalberghi, Elisabetta Wade, Jordan C. Watanabe, Arii Widness, Jane Young, Julie K. Zentall, Thomas R. Zhao, Yini TI The evolution of self-control SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE psychology; behavior; comparative methods; inhibitory control; executive function ID RELATIVE BRAIN SIZE; FOOD-STORING BIRDS; UP PRIMATE BRAIN; COMPARATIVE PSYCHOLOGY; SOCIAL COGNITION; INTELLIGENCE HYPOTHESIS; PREFRONTAL CORTEX; SPATIAL MEMORY; NEOCORTEX SIZE; CULTURAL INTELLIGENCE AB Cognition presents evolutionary research with one of its greatest challenges. Cognitive evolution has been explained at the proximate level by shifts in absolute and relative brain volume and at the ultimate level by differences in social and dietary complexity. However, no study has integrated the experimental and phylogenetic approach at the scale required to rigorously test these explanations. Instead, previous research has largely relied on various measures of brain size as proxies for cognitive abilities. We experimentally evaluated these major evolutionary explanations by quantitatively comparing the cognitive performance of 567 individuals representing 36 species on two problem-solving tasks measuring self-control. Phylogenetic analysis revealed that absolute brain volume best predicted performance across species and accounted for considerably more variance than brain volume controlling for body mass. This result corroborates recent advances in evolutionary neurobiology and illustrates the cognitive consequences of cortical reorganization through increases in brain volume. Within primates, dietary breadth but not social group size was a strong predictor of species differences in self-control. Our results implicate robust evolutionary relationships between dietary breadth, absolute brain volume, and self-control. These findings provide a significant first step toward quantifying the primate cognitive phenome and explaining the process of cognitive evolution. C1 [MacLean, Evan L.; Hare, Brian; Nunn, Charles L.; Bray, Joel; Platt, Michael L.; Tan, Jingzhi] Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27708 USA. [Platt, Michael L.] Duke Univ, Dept Neurobiol, Durham, NC 27708 USA. [Brannon, Elizabeth M.] Duke Univ, Dept Psychol & Neurosci, Durham, NC 27708 USA. [Hare, Brian; Brannon, Elizabeth M.; Brent, Lauren J. N.; Platt, Michael L.] Duke Univ, Ctr Cognit Neurosci, Durham, NC 27708 USA. [Brent, Lauren J. N.; Platt, Michael L.] Duke Univ, Duke Inst Brain Sci, Durham, NC 27708 USA. [Addessi, Elsa; Visalberghi, Elisabetta] CNR, Ist Sci & Tecnol Cogniz, I-00197 Rome, Italy. [Amici, Federica; Call, Josep; Herrmann, Esther; Schumann, Katrin] Max Planck Inst Evolutionary Anthropol, Dept Dev & Comparat Psychol, D-04103 Leipzig, Germany. [Anderson, Rindy C.; Sewall, Kendra B.] Duke Univ, Dept Biol, Durham, NC 27704 USA. [Aureli, Filippo] Univ Veracruzana, Inst Neuroetol, Xalapa 91190, Veracruz, Mexico. [Aureli, Filippo] Liverpool John Moores Univ, Res Ctr Evolutionary Anthropol & Palaeoecol, Liverpool L3 3AF, Merseyside, England. [Baker, Joseph M.] Stanford Univ, Sch Med, Ctr Interdisciplinary Brain Sci Res, Stanford, CA 94305 USA. [Baker, Joseph M.; Messer, Emily J. E.] Stanford Univ, Sch Med, Dept Psychiat & Behav Sci, Stanford, CA 94305 USA. [Bania, Amanda E.] Smithsonian Natl Zool Pk, Ctr Anim Care Sci, Washington, DC 20008 USA. [Barnard, Allison M.; Cantlon, Jessica F.] Univ Rochester, Seneca Pk Zoo, Dept Brain & Cognit Sci, Rochester, NY 14620 USA. [DiVincenti, Louis J.] Univ Rochester, Seneca Pk Zoo, Dept Comparat Med, Rochester, NY 14620 USA. [Boogert, Neeltje J.; Seed, Amanda M.; Tao, Ruoting] Univ St Andrews, Dept Psychol & Neurosci, St Andrews KY16 9JP, Scotland. [Bray, Emily E.] Univ Penn, Dept Psychol, Philadelphia, PA 19104 USA. [Burkart, Judith M.; van Schaik, Carel P.] Univ Zurich, Anthropol Inst & Museum, CH-8057 Zurich, Switzerland. [Cheke, Lucy G.; Clayton, Nicola S.; Ostojic, Ljerka; Plotnik, Joshua M.; Shaw, Rachael C.; Watanabe, Arii] Univ Cambridge, Dept Psychol, Cambridge CB2 3EB, England. [Delgado, Mikel M.; Jacobs, Lucia F.] Univ Calif Berkeley, Dept Psychol, Berkeley, CA 94720 USA. [Jacobs, Lucia F.] Univ Calif Berkeley, Helen Wills Neurosci Inst, Berkeley, CA 94720 USA. [Fujita, Kazuo; Hiramatsu, Chihiro; Takimoto, Ayaka] Kyoto Univ, Grad Sch Letters, Kyoto 6068501, Japan. [Jordan, Kerry E.] Utah State Univ, Dept Psychol, Logan, UT 84322 USA. [Young, Julie K.] Utah State Univ, Wildland Resources, Logan, UT 84322 USA. [Laude, Jennifer R.; Wade, Jordan C.] Univ Kentucky, Dept Psychol, Lexington, KY 40506 USA. [Leimgruber, Kristin L.; Santos, Laurie R.; Widness, Jane] Yale Univ, Dept Psychol, New Haven, CT 06520 USA. [Moura, Antonio C. de A.] Univ Fed Paraiba, Dept Engn & Meio Ambiente, BR-58059900 Joao Pessoa, Paraiba, Brazil. [Picard, Alejandra; Slocombe, Katie E.] Univ York, Dept Psychol, York YO10 5DD, N Yorkshire, England. [Plotnik, Joshua M.] Think Elephants Int, Stone Ridge, NY 12484 USA. [Range, Friederike; Viranyi, Zsoia] Univ Vet Med Vienna, Messerli Res Inst, A-1210 Vienna, Austria. [Range, Friederike] Wolf Sci Ctr, A-2115 Ernstbrunn, Austria. [Reader, Simon M.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Reddy, Rachna B.; Sandel, Aaron A.] Univ Michigan, Dept Anthropol, Ann Arbor, MI 48109 USA. [Su, Yanjie; Zhao, Yini] Peking Univ, Dept Psychol, Beijing 100871, Peoples R China. RP MacLean, EL (reprint author), Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27708 USA. EM maclean@duke.edu RI Reader, Simon/B-9075-2011; Burkart, Judith/P-6357-2014; Addessi, Elsa/B-8329-2015; Slocombe, Katie/B-8788-2016; OI MacLean, Evan/0000-0001-7595-662X; Shaw, Rachael/0000-0002-4831-8283; Reader, Simon/0000-0002-3785-1357; Burkart, Judith/0000-0002-6229-525X; Slocombe, Katie/0000-0002-7310-1887; addessi, elsa/0000-0002-5553-7732; Amici, Federica/0000-0003-3539-1067; Visalberghi, Elisabetta/0000-0001-7407-5468; Brent, Lauren/0000-0002-1202-1939; Messer, Emily/0000-0002-8242-133X; Range, Friederike/0000-0003-3127-5536 FU National Evolutionary Synthesis Center (NESCent); National Science Foundation (NSF) [EF-0905606]; NSF [BCS-0923791, DGE-1106401, NSF-BCS-27552, NSF-BCS-25172]; National Natural Science Foundation of China [31170995]; National Basic Research Program (973 Program) [2010CB833904]; Newton International Fellowship from the Royal Society; British Academy; James S. McDonnell Foundation [220020242]; National Institutes of Mental Health [R01-MH096875, R01-MH089484]; Duke Institute for Brain Sciences Incubator Award; Duke Center for Interdisciplinary Decision Sciences Fellowship; Programma Nazionale per la Ricerca-Consiglio Nazionale delle Ricerche (CNR) Aging Program; Japan Society for the Promotion of Science (JSPS) [20220004]; European Community [012-984 NESTPathfinder, 043318]; Humboldt Research Fellowship [1138999]; NSF Electrical, Communications, and Cyber Systems [1028319]; NSF; JSPS [21264]; Austrian Science Fund (FWF) [P21244-B17]; European Research Council (ERC) under the European Union [311870]; Vienna Science and Technology Fund Project [CS11-026]; National Institutes of Health [5 R03 HD070649-02]; Royal Canin; [10J04395] FX We thank Natalie Cooper and Sunil Suchindran for statistical advice; Jeff Stevens and two anonymous reviewers for comments on drafts of this manuscript; and Ikuma Adachi, Nathan Emery, Daniel Haun, Marc Hauser, Ludwig Huber, Al Kamil, Chris Krupenye, Luke Matthews, Collin McCabe, Alexandra Rosati, Kara Schroepfer, Jeff Stevens, Tara Stoinski, Michael Tomasello, and Victoria Wobber for their helpful discussion during the workshops from which this research emerged. F. Aureli and F. Amici thank Iber Rodriguez Castillo, Roberto Pacheco Mendez, Fernando Victoria Arceo, Liesbeth Sterck, Barbara Tiddi, and all the animal keepers at the facilities where the data were collected for support and cooperation. K.E.S. and A.P. thank Steve Nichols and the staff at The Parrot Zoo. This work was supported by the National Evolutionary Synthesis Center (NESCent) through support of a working group led by C.L.N. and B.H. NESCent is supported by the National Science Foundation (NSF) EF-0905606. For training in phylogenetic comparative methods, we thank the AnthroTree Workshop (supported by NSF BCS-0923791). Y.S. thanks the National Natural Science Foundation of China (Project 31170995) and National Basic Research Program (973 Program: 2010CB833904). E.E.B. thanks the Duke Vertical Integration Program and the Duke Undergraduate Research Support Office. J.M.P. was supported by a Newton International Fellowship from the Royal Society and the British Academy. L.R.S. thanks the James S. McDonnell Foundation for Award 220020242. L.J.N.B. and M.L.P. acknowledge the National Institutes of Mental Health (R01-MH096875 and R01-MH089484), a Duke Institute for Brain Sciences Incubator Award (to M.L.P.), and a Duke Center for Interdisciplinary Decision Sciences Fellowship (to L.J.N.B.). E.V. and E.A. thank the Programma Nazionale per la Ricerca-Consiglio Nazionale delle Ricerche (CNR) Aging Program 2012-2014 for financial support, Roma Capitale-Museo Civico di Zoologia and Fondazione Bioparco for hosting the Istituto di Scienze e Tecnologie della Cognizione-CNR Unit of Cognitive Primatology and Primate Centre, and Massimiliano Bianchi and Simone Catarinacci for assistance with capuchin monkeys. K.F. thanks the Japan Society for the Promotion of Science (JSPS) for Grant-in-Aid for Scientific Research 20220004. F. Aureli thanks the Stages in the Evolution and Development of Sign Use project (Contract 012-984 NESTPathfinder) and the Integrating Cooperation Research Across Europe project (Contract 043318), both funded by the European Community's Sixth Framework Programme (FP6/2002-2006). F. Amici was supported by Humboldt Research Fellowship for Post-doctoral Researchers (Humboldt ID 1138999). L.F.J. and M.M.D. acknowledge NSF Electrical, Communications, and Cyber Systems Grant 1028319 (to L.F.J.) and an NSF Graduate Fellowship (to M. M. D.). C.H. thanks Grant-in-Aid for JSPS Fellows (10J04395). A.T. thanks Research Fellowships of the JSPS for Young Scientists (21264). F.R. and Z.V. acknowledge Austrian Science Fund (FWF) Project P21244-B17, the European Research Council (ERC) under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement 311870 (to F. R.), Vienna Science and Technology Fund Project CS11-026 (to Z.V.), and many private sponsors, including Royal Canin for financial support and the Game Park Ernstbrunn for hosting the Wolf Science Center. S.M.R. thanks the Natural Sciences and Engineering Research Council (Canada). J.K.Y. thanks the US Department of Agriculture-Wildlife Services-National Wildlife Research Center. J.F.C.; thanks the James S. McDonnell Foundation and Alfred P. Sloan Foundation. E.L.M. and B.H. thank the Duke Lemur Center and acknowledge National Institutes of Health Grant 5 R03 HD070649-02 and NSF Grants DGE-1106401, NSF-BCS-27552, and NSF-BCS-25172. This is Publication 1265 of the Duke Lemur Center. NR 201 TC 89 Z9 89 U1 30 U2 178 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 20 PY 2014 VL 111 IS 20 BP E2140 EP E2148 DI 10.1073/pnas.1323533111 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AH5KP UT WOS:000336168100011 PM 24753565 ER PT J AU Ziemke, JR Olsen, MA Witte, JC Douglass, AR Strahan, SE Wargan, K Liu, X Schoeberl, MR Yang, K Kaplan, TB Pawson, S Duncan, BN Newman, PA Bhartia, PK Heney, MK AF Ziemke, J. R. Olsen, M. A. Witte, J. C. Douglass, A. R. Strahan, S. E. Wargan, K. Liu, X. Schoeberl, M. R. Yang, K. Kaplan, T. B. Pawson, S. Duncan, B. N. Newman, P. A. Bhartia, P. K. Heney, M. K. TI Assessment and applications of NASA ozone data products derived from Aura OMI/MLS satellite measurements in context of the GMI chemical transport model SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPICAL TROPOSPHERIC OZONE; VARIATIONAL STATISTICAL-ANALYSIS; 1997-1998 EL-NINO; COLUMN OZONE; INTERANNUAL VARIABILITY; MONITORING INSTRUMENT; RECURSIVE FILTERS; NUMERICAL ASPECTS; MLS MEASUREMENTS; ARCTIC OZONE AB Measurements from the Ozone Monitoring Instrument (OMI) and Microwave Limb Sounder (MLS), both on board the Aura spacecraft, have been used to produce daily global maps of column and profile ozone since August 2004. Here we compare and evaluate three strategies to obtain daily maps of tropospheric and stratospheric ozone from OMI and MLS measurements: trajectory mapping, direct profile retrieval, and data assimilation. Evaluation is based on an assessment that includes validation using ozonesondes and comparisons with the Global Modeling Initiative (GMI) chemical transport model. We investigate applications of the three ozone data products from near-decadal and interannual time scales to day-to-day case studies. Interannual changes in zonal mean tropospheric ozone from all of the products in any latitude range are of the order 1-2 Dobson units while changes (increases) over the 8 year Aura record investigated vary by 2-4 Dobson units. It is demonstrated that all of the ozone products can measure and monitor exceptional tropospheric ozone events including major forest fire and pollution transport events. Stratospheric ozone during the Aura record has several anomalous interannual events including split stratospheric warmings in the Northern Hemisphere extratropics that are well captured using the data assimilation ozone profile product. Data assimilation with continuous daily global coverage and vertical ozone profile information is the best of the three strategies at generating a global tropospheric and stratospheric ozone product for science applications. C1 [Ziemke, J. R.; Olsen, M. A.] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA. [Ziemke, J. R.; Olsen, M. A.; Douglass, A. R.; Strahan, S. E.; Wargan, K.; Pawson, S.; Duncan, B. N.; Newman, P. A.; Bhartia, P. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Witte, J. C.; Wargan, K.; Heney, M. K.] Sci Syst & Applicat Inc, Lanham, MD USA. [Strahan, S. E.] Univ Space Res Assoc, Columbia, MD USA. [Liu, X.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schoeberl, M. R.] Sci & Technol Corp, Lanham, MD USA. [Yang, K.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Kaplan, T. B.] INNOVIM, Greenbelt, MD USA. RP Ziemke, JR (reprint author), Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA. EM jerald.r.ziemke@gsfc.nasa.gov RI Douglass, Anne/D-4655-2012; Liu, Xiong/P-7186-2014; Bhartia, Pawan/A-4209-2016; Pawson, Steven/I-1865-2014; Duncan, Bryan/A-5962-2011; OI Liu, Xiong/0000-0003-2939-574X; Bhartia, Pawan/0000-0001-8307-9137; Pawson, Steven/0000-0003-0200-717X; Wargan, Krzysztof/0000-0002-3795-2983 FU NASA [NNH07ZDA001N-AST] FX The authors thank the Aura MLS and OMI instrument and algorithm teams for the extensive satellite measurements used in this study. We also thank the Editor and three reviewers for valuable comments that were very beneficial in improving the paper. OMI is a Dutch-Finnish contribution to the Aura mission. Funding for this research was provided in part by NASA NNH07ZDA001N-AST. NR 57 TC 10 Z9 10 U1 4 U2 23 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 19 PY 2014 VL 119 IS 9 BP 5671 EP 5699 DI 10.1002/2013JD020914 PG 29 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AK3QS UT WOS:000338340400042 ER PT J AU Mulcahy, DG Martinez-Gomez, JE Aguirre-Leon, G Cervantes-Pasqualli, JA Zug, GR AF Mulcahy, Daniel G. Martinez-Gomez, Juan E. Aguirre-Leon, Gustavo Cervantes-Pasqualli, Juan A. Zug, George R. TI Rediscovery of an Endemic Vertebrate from the Remote Islas Revillagigedo in the Eastern Pacific Ocean: The Clarion Nightsnake Lost and Found SO PLOS ONE LA English DT Article ID CONSERVATION STATUS; HYPSIGLENA-TORQUATA; LIZARD; MEXICO; BIOGEOGRAPHY; CALIFORNIA; COLUBRIDAE; REPTILES; TREE AB Vertebrates are currently going extinct at an alarming rate, largely because of habitat loss, global warming, infectious diseases, and human introductions. Island ecosystems are particularly vulnerable to invasive species and other ecological disturbances. Properly documenting historic and current species distributions is critical for quantifying extinction events. Museum specimens, field notes, and other archived materials from historical expeditions are essential for documenting recent changes in biodiversity. The Islas Revillagigedo are a remote group of four islands, 700-1100 km off the western coast of mainland Mexico. The islands are home to many endemic plants and animals recognized at the specific-and subspecific-levels, several of which are currently threatened or have already gone extinct. Here, we recount the initial discovery of an endemic snake Hypsiglena ochrorhyncha unaocularus Tanner on Isla Clarion, the later dismissal of its existence, its absence from decades of field surveys, our recent rediscovery, and recognition of it as a distinct species. We collected two novel complete mitochondrial (mt) DNA genomes and up to 2800 base-pairs of mtDNA from several other individuals, aligned these with previously published mt-genome data from samples throughout the range of Hypsiglena, and conducted phylogenetic analyses to infer the biogeographic origin and taxonomic status of this population. We found the Isla Clarion population to be most closely related to populations in the Sonora-Sinaloa state border area of mainland Mexico and Isla Santa Catalina, in the Gulf of California. Based on genetics, morphology, and geographic distributions, we also recognize these two other lineages as distinct species. Our study shows the importance of museum specimens, field notes, and careful surveys to accurately document biodiversity and brings these island endemics (Clarion and Santa Catalina nightsnakes) and mainland population near the Sonora-Sinaloa state border to the attention of conservation biologists currently monitoring biodiversity in these fragile subtropical ecosystems. C1 [Mulcahy, Daniel G.; Zug, George R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Martinez-Gomez, Juan E.; Aguirre-Leon, Gustavo; Cervantes-Pasqualli, Juan A.] Red Interacc Multitrof, Asociac Civil, Inst Ecol, Xalapa, Veracruz, Mexico. RP Mulcahy, DG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM MulcahyD@si.edu RI Martinez-Gomez, Juan/F-3585-2010 FU Smithsonian-NMNH; Island Endemics Foundation; INECOL FX This research was funded by Smithsonian-NMNH grants awarded to GRZ and DGM, RW McDiarmid and DGM, and funds by the Island Endemics Foundation and INECOL were awarded to JEMG. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 46 TC 1 Z9 2 U1 4 U2 23 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 16 PY 2014 VL 9 IS 5 AR e97682 DI 10.1371/journal.pone.0097682 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM1NZ UT WOS:000339614800062 PM 24837300 ER PT J AU Kerr, KA Christy, JH Joly-Lopez, Z Luque, J Collin, R Guichard, F AF Kerr, Kecia A. Christy, John H. Joly-Lopez, Zoe Luque, Javier Collin, Rachel Guichard, Frederic TI Reproducing on Time When Temperature Varies: Shifts in the Timing of Courtship by Fiddler Crabs SO PLOS ONE LA English DT Article ID RECENT CLIMATE-CHANGE; ADAPTIVE SIGNIFICANCE; BEHAVIORAL THERMOREGULATION; INTERTIDAL CRABS; WAVELET ANALYSIS; MARINE SYSTEMS; TROPHIC LEVELS; TIDAL REGIMES; WARMING WORLD; UCA-PUGILATOR AB Many species reproduce when conditions are most favorable for the survival of young. Numerous intertidal fish and invertebrates release eggs or larvae during semilunar, large amplitude, nocturnal tides when these early life stages are best able to escape predation by fish that feed near the shore during the day. Remarkably, some species, including the fiddler crabs Uca terpsichores and Uca deichmanni, maintain this timing throughout the year as temperature, and thus the rate of embryonic development, vary. The mechanisms that allow such precision in the timing of the production of young are poorly known. A preliminary study suggested that when temperature decreases, U. terpsichores mate earlier in the tidal amplitude cycle such that larvae are released at the appropriate time. We tested this idea by studying the timing of courtship in U. terpsichores and U. deichmanni as temperature varied annually during two years, at 5 locations that differed in the temperature of the sediment where females incubate their eggs. Uca terpsichores courted earlier at locations where sediment temperature declined seasonally but not where sediment temperature remained elevated throughout the year. In contrast, clear shifts in courtship timing were not observed for U. deichmanni despite variation in sediment temperature. We discuss other mechanisms by which this species may maintain reproductive timing. These two species are likely to be affected differently by changes in the frequency and intensity of cold periods that are expected to accompany climate change. C1 [Kerr, Kecia A.; Joly-Lopez, Zoe; Guichard, Frederic] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Kerr, Kecia A.; Christy, John H.; Luque, Javier; Collin, Rachel] Smithsonian Trop Res Inst, Panama City, Panama. [Kerr, Kecia A.; Collin, Rachel; Guichard, Frederic] McGill Univ, McGill STRI Neotrop Environm Opt NEO, Montreal, PQ, Canada. [Luque, Javier] Univ Alberta, Dept Biol Sci, Edmonton, AB, Canada. RP Kerr, KA (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM kecia.kerr@mail.mcgill.ca RI Guichard, Frederic/B-6188-2015; OI Guichard, Frederic/0000-0002-7369-482X; Luque, Javier/0000-0002-4391-5951; Collin, Rachel/0000-0001-5103-4460 FU Society of Integrative and Comparative Biology; McGill Neotropical Environment Option; Natural Sciences and Engineering Research Council of Canada; Quebec- Ocean FX This work was funded by a Society of Integrative and Comparative Biology Grant-in-Aid of Research to K. K.; a McGill Neotropical Environment Option Grant-in-Aid of Research to K.K.; the Natural Sciences and Engineering Research Council of Canada (Research grant to F.G. and PGSD to K.K.); and Quebec- Ocean funding of F.G. and K.K. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 79 TC 5 Z9 5 U1 2 U2 44 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 15 PY 2014 VL 9 IS 5 AR e97593 DI 10.1371/journal.pone.0097593 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AI3UI UT WOS:000336789500083 PM 24832079 ER PT J AU Talbot, J Lewis, SL Lopez-Gonzalez, G Brienen, RJW Monteagudo, A Baker, TR Feldpausch, TR Malhi, Y Vanderwel, M Murakami, AA Arroyo, LP Chao, KJ Erwin, T van der Heijden, G Keeling, H Killeen, T Neill, D Vargas, PN Gutierrez, GAP Pitman, N Quesada, CA Silveira, M Stropp, J Phillips, OL AF Talbot, Joey Lewis, Simon L. Lopez-Gonzalez, Gabriela Brienen, Roe J. W. Monteagudo, Abel Baker, Timothy R. Feldpausch, Ted R. Malhi, Yadvinder Vanderwel, Mark Murakami, Alejandro Araujo Arroyo, Luzmila P. Chao, Kuo-Jung Erwin, Terry van der Heijden, Geertje Keeling, Helen Killeen, Tim Neill, David Nunez Vargas, Percy Gutierrez, Germaine Alexander Parada Pitman, Nigel Quesada, Carlos Alberto Silveira, Marcos Stropp, Juliana Phillips, Oliver L. TI Methods to estimate aboveground wood productivity from long-term forest inventory plots SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Biomass; Carbon; Census interval; Diameter; Recruitment; Tropical forest ID NET PRIMARY PRODUCTIVITY; TROPICAL FORESTS; TREE MORTALITY; CARBON STORAGE; RAIN-FOREST; GROWTH; DENSITY; HEIGHT; RECRUITMENT; ALLOMETRY AB Forest inventory plots are widely used to estimate biomass carbon storage and its change over time. While there has been much debate and exploration of the analytical methods for calculating biomass, the methods used to determine rates of wood production have not been evaluated to the same degree. This affects assessment of ecosystem fluxes and may have wider implications if inventory data are used to parameterise biospheric models, or scaled to large areas in assessments of carbon sequestration. Here we use a dataset of 35 long-term Amazonian forest inventory plots to test different methods of calculating wood production rates. These address potential biases associated with three issues that routinely impact the interpretation of tree measurement data: (1) changes in the point of measurement (POM) of stem diameter as trees grow over time; (2) unequal length of time between censuses; and (3) the treatment of trees that pass the minimum diameter threshold ("recruits"). We derive corrections that control for changing POM height, that account for the unobserved growth of trees that die within census intervals, and that explore different assumptions regarding the growth of recruits during the previous census interval. For our dataset we find that annual aboveground coarse wood production (AGWP; in Mg ha(-1) year(-1) of dry matter) is underestimated on average by 9.2% if corrections are not made to control for changes in POM height. Failure to control for the length of sampling intervals results in a mean underestimation of 2.7% in annual AGWP in our plots for a mean interval length of 3.6 years. Different methods for treating recruits result in mean differences of up to 8.1% in AGWP. In general, the greater the length of time a plot is sampled for and the greater the time elapsed between censuses, the greater the tendency to underestimate wood production. We recommend that POM changes, census interval length, and the contribution of recruits should all be accounted for when estimating productivity rates, and suggest methods for doing this. (C) 2014 Elsevier B.V. All rights reserved. C1 [Talbot, Joey; Lewis, Simon L.; Lopez-Gonzalez, Gabriela; Brienen, Roe J. W.; Baker, Timothy R.; Chao, Kuo-Jung; Keeling, Helen; Phillips, Oliver L.] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. [Lewis, Simon L.] UCL, Dept Geog, London WC1E 6BT, England. [Monteagudo, Abel] Jardin Bot Missouri, Oxapampa, Pasco, Peru. [Feldpausch, Ted R.] Univ Exeter, Coll Life & Environm Sci, Exeter, Devon, England. [Malhi, Yadvinder] Univ Oxford, Sch Geog & Environm, Environm Change Inst, Oxford OX1 3QY, England. [Vanderwel, Mark] Microsoft Res, Computat Ecol & Environm Sci Grp, Cambridge CB1 2FB, England. [Vanderwel, Mark] Univ Florida, Dept Biol, Gainesville, FL USA. [Murakami, Alejandro Araujo; Arroyo, Luzmila P.; Killeen, Tim; Gutierrez, Germaine Alexander Parada] Muse Hist Nat Noel Kempff Mercado, Santa Cruz, Bolivia. [Chao, Kuo-Jung] Natl Chung Hsing Univ, Taipei, Taiwan. [Erwin, Terry] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [van der Heijden, Geertje] Univ Wisconsin, Milwaukee, WI 53201 USA. [van der Heijden, Geertje] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Neill, David] Univ Estatal Amazon, Puyo, Pastaza, Ecuador. [Nunez Vargas, Percy] Univ Nacl San Antonio Abad Cusco, Cuzco 921, Peru. [Pitman, Nigel] Duke Univ, Nicholas Sch Environm, Ctr Trop Conservat, Durham, NC 27708 USA. [Quesada, Carlos Alberto] Inst Nacl de Pesquisas da Amazonia, BR-69060011 Manaus, AM, Brazil. [Silveira, Marcos] Univ Fed Acre, Museu Univ, Depto Ctr Ciencias Nat, BR-69910900 Rio Branco, AC, Brazil. [Stropp, Juliana] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy. RP Talbot, J (reprint author), Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. EM gyjt@leeds.ac.uk RI Phillips, Oliver/A-1523-2011; Feldpausch, Ted/D-3436-2009; Silveira, Marcos/H-7906-2013; OI Phillips, Oliver/0000-0002-8993-6168; Feldpausch, Ted/0000-0002-6631-7962; Silveira, Marcos/0000-0003-0485-7872; Lopez-Gonzalez, Gabriela/0000-0002-0814-8830; Lewis, Simon/0000-0002-8066-6851 FU European Union; UK Natural Environment Research Council; Gordon and Betty Moore Foundation; NERC from UNEP-WCMC; NERC Research Fellowship; Royal Society University Research Fellowship; ERC Advanced Grant "Tropical Forests in the Changing Earth System"; Royal Society Wolfson Research Merit Award FX Data collection has been supported by grants from the European Union, the UK Natural Environment Research Council, and the Gordon and Betty Moore Foundation, including grants held by Jon Lloyd. JT is supported by a NERC PhD Studentship with CASE sponsorship from UNEP-WCMC. RJWB is supported by a NERC Research Fellowship; SLL is supported by a Royal Society University Research Fellowship; OLP and SLL are supported by an ERC Advanced Grant "Tropical Forests in the Changing Earth System", and OLP by a Royal Society Wolfson Research Merit Award. We thank Rodolfo Vasquez Martinez and Nallaret Davila Cardozo for contributing their botanical expertise, Sue Grahame and Georgia Pickavance for their work with the ForestPlots.net database, Joana Ricardo for work supporting RAINFOR collaborators, Lera Miles and Drew Purves for advice, and the many colleagues and field assistants who have contributed to the development of the RAINFOR network. NR 38 TC 19 Z9 19 U1 2 U2 45 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 2014 VL 320 BP 30 EP 38 DI 10.1016/j.foreco.2014.02.021 PG 9 WC Forestry SC Forestry GA AH4PN UT WOS:000336110600005 ER PT J AU Kessler, EM Komar, P Bishof, M Jiang, L Sorensen, AS Ye, J Lukin, MD AF Kessler, E. M. Komar, P. Bishof, M. Jiang, L. Sorensen, A. S. Ye, J. Lukin, M. D. TI Heisenberg-Limited Atom Clocks Based on Entangled Qubits SO PHYSICAL REVIEW LETTERS LA English DT Article ID FREQUENCY STANDARDS; PHASE; STABILITY; METROLOGY AB We present a quantum-enhanced atomic clock protocol based on groups of sequentially larger Greenberger-Horne-Zeilinger (GHZ) states that achieves the best clock stability allowed by quantum theory up to a logarithmic correction. Importantly the protocol is designed to work under realistic conditions where the drift of the phase of the laser interrogating the atoms is the main source of decoherence. The simultaneous interrogation of the laser phase with a cascade of GHZ states realizes an incoherent version of the phase estimation algorithm that enables Heisenberg-limited operation while extending the coherent interrogation time beyond the laser noise limit. We compare and merge the new protocol with existing state of the art interrogation schemes, and identify the precise conditions under which entanglement provides an advantage for clock stabilization: it allows a significant gain in the stability for short averaging time. C1 [Kessler, E. M.; Komar, P.; Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Kessler, E. M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Bishof, M.; Ye, J.] Univ Colorado, Dept Phys, Natl Inst Stand & Technol, JILA, Boulder, CO 80309 USA. [Jiang, L.] Yale Univ, Dept Appl Phys, New Haven, CT 06520 USA. [Sorensen, A. S.] Niels Bohr Inst, Danish Natl Res Fdn Ctr Quantum Opt, QUANTOP, DK-2100 Copenhagen, Denmark. RP Kessler, EM (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Ye, Jun/C-3312-2011; Kessler, Eric Matthias/E-6981-2012; Sorensen, Anders/L-1868-2013; Jiang, Liang/A-9847-2008 OI Kessler, Eric Matthias/0000-0001-9959-538X; Sorensen, Anders/0000-0003-1337-9163; Jiang, Liang/0000-0002-0000-9342 FU NSF; CUA; ITAMP; HQOC; JILA PFC; NIST; DARPA QUSAR; Alfred P. Sloan Foundation; Quiness programs; ARO MURI; ERC grant QIOS [306576]; NDSEG; NSF GRFP FX We are grateful to Till Rosenband, Vladan Vuletic, and Johannes Borregaard for enlightening discussions. This work was supported by NSF, CUA, ITAMP, HQOC, JILA PFC, NIST, DARPA QUSAR, the Alfred P. Sloan Foundation, the Quiness programs, ARO MURI, and the ERC grant QIOS (Grant No. 306576); M. B. acknowledges support from NDSEG and NSF GRFP. E. M. K. and P. K. contributed equally to this work. NR 34 TC 22 Z9 22 U1 1 U2 35 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 MAY 15 PY 2014 VL 112 IS 19 AR 190403 DI 10.1103/PhysRevLett.112.190403 PG 5 WC Physics, Multidisciplinary SC Physics GA AH1NV UT WOS:000335888700001 PM 24877919 ER PT J AU Baldwin, CC Johnson, GD AF Baldwin, Carole C. Johnson, G. David TI Connectivity across the Caribbean Sea: DNA Barcoding and Morphology Unite an Enigmatic Fish Larva from the Florida Straits with a New Species of Sea Bass from Deep Reefs off Curacao SO PLOS ONE LA English DT Article ID IDENTIFICATION; TELEOSTEI; SERRANIDAE; DIVERSITY; EPINEPHELINAE; GOBIIDAE; HISTORY; GENUS AB Integrative taxonomy, in which multiple disciplines are combined to address questions related to biological species diversity, is a valuable tool for identifying pelagic marine fish larvae and recognizing the existence of new fish species. Here we combine data from DNA barcoding, comparative morphology, and analysis of color patterns to identify an unusual fish larva from the Florida Straits and demonstrate that it is the pelagic larval phase of a previously undescribed species of Liopropoma sea bass from deep reefs off Curacao, southern Caribbean. The larva is unique among larvae of the teleost family Serranidae, Tribe Liopropomini, in having seven elongate dorsal-fin spines. Adults of the new species are similar to the golden bass, Liopropoma aberrans, with which they have been confused, but they are distinct genetically and morphologically. The new species differs from all other western Atlantic liopropomins in having IX, 11 dorsal-fin rays and in having a unique color pattern-most notably the predominance of yellow pigment on the dorsal portion of the trunk, a pale to white body ventrally, and yellow spots scattered across both the dorsal and ventral portions of the trunk. Exploration of deep reefs to 300 m using a manned submersible off Curacao is resulting in the discovery of numerous new fish species, improving our genetic databases, and greatly enhancing our understanding of deep-reef fish diversity in the southern Caribbean. Oh the mother and child reunion is only a moment away. Paul Simon. C1 [Baldwin, Carole C.; Johnson, G. David] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Baldwin, CC (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. EM baldwinc@si.edu FU Consortium for Understanding and Sustaining a Biodiverse Planet; National Geographic Society's Committee for Research and Exploration [9102-12]; Evelyn Axelrod Endowment Fund for systematic ichthyology FX Funding for the Smithsonian Institution's Deep Reef Observation Project was provided internally by the Consortium for Understanding and Sustaining a Biodiverse Planet and by National Geographic Society's Committee for Research and Exploration to CCB (Grant # 9102-12). Additional funding for this study was provided to both authors through the generous support of the Herbert R. and Evelyn Axelrod Endowment Fund for systematic ichthyology. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 42 TC 13 Z9 13 U1 0 U2 17 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 13 PY 2014 VL 9 IS 5 AR e97661 DI 10.1371/journal.pone.0097661 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AH8EY UT WOS:000336369200131 PM 24825118 ER PT J AU Conway, KW Baldwin, C White, MD AF Conway, Kevin W. Baldwin, Carole White, Macaulay D. TI Cryptic Diversity and Venom Glands in Western Atlantic Clingfishes of the Genus Acyrtus (Teleostei: Gobiesocidae) SO PLOS ONE LA English DT Article ID CRYPTOBENTHIC FISH ASSEMBLAGES; GOBIIDAE; PACIFIC; TRIPTERYGIIDAE; ENNEANECTES; EVOLUTION AB Examination of genetic data (mitochondrial cytochrome c oxidase I) for western Atlantic clingfishes revealed two distinct lineages within a group of individuals originally identified as Acyrtus artius. Subsequent investigation of preserved voucher specimens was conducted to reconcile the genetic data and the existing classification, which is based on morphology. In addition to discovering that one of the genetic lineages is an undescribed species, which we describe as Acyrtus lanthanum, new species, we found that the nominal species Acyrtus artius has a putative venom gland associated with the subopercle that has been overlooked since the species was described nearly 60 years ago. The new species lacks the subopercular gland as does Acyrtus rubiginosus, but one is present in the related Arcos nudus. Venom glands have not been reported previously for the Gobiesocidae, and the venom gland described herein for Acyrtus and Arcos represents the first example in teleost fishes of a venom gland associated with the subopercle. C1 [Conway, Kevin W.] Texas A&M Univ, Dept Wildlife & Fisheries Sci & Biodivers Res & T, College Stn, TX 77843 USA. [Baldwin, Carole] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [White, Macaulay D.] Texas A&M Univ, Dept Wildlife & Fisheries Sci, Undergrad Degree Program, College Stn, TX 77843 USA. RP Conway, KW (reprint author), Texas A&M Univ, Dept Wildlife & Fisheries Sci & Biodivers Res & T, College Stn, TX 77843 USA. EM kevin.conway@tamu.edu FU National Science Foundation [IOS 1256793]; Texas A&M Agrilife Research [TEX09452]; Smithsonian Institution Caribbean Coral Reef Ecosystems (CCRE) Program FX This research was funded by National Science Foundation (IOS 1256793 to KWC), Texas A&M Agrilife Research (TEX09452 to KWC), and several Smithsonian Institution Caribbean Coral Reef Ecosystems (CCRE) Program grants (to CCB). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 54 TC 5 Z9 5 U1 0 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 2014 VL 9 IS 5 AR e97664 DI 10.1371/journal.pone.0097664 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AH8EY UT WOS:000336369200132 PM 24825326 ER PT J AU Mah, CL Foltz, DW AF Mah, Christopher L. Foltz, David W. TI New taxa and taxonomic revisions to the Poraniidae (Valvatacea; Asteroidea) with Comments on Feeding Biology SO ZOOTAXA LA English DT Article ID SEA-STARS; SEQUENCE ALIGNMENT; ECHINODERMATA; ODONTASTERIDAE; ASSEMBLAGES; PHYLOGENY; LARVAE; GULF AB New molecular phylogenetic data and new specimens provide the basis for a revision of the family Poraniidae. We present molecular phylogenetic data for five out of 11 genera in the Poraniidae including a newly discovered taxon from the North Pacific. Bathyporania ascendens nov. gen., nov. sp., is described from Davidson Seamount (35 degrees 43 ' N, 122 degrees 43 ' W). Another newly discovered poraniid taxon, Clavaporania fitchorum nov. gen., nov. sp. is described from south of Macquarie Island (56 degrees 21 ' S, 158 degrees 28 ' E) but was not included in the analysis. Revision of the Poraniidae has been undertaken. We present two new genera and reinstate the previously synonymized genus Glabraster and return Culcitopsis to genus level. The genus Porania sensu Clark (1993) and Clark and Downey (1992) is not monophyletic. Porania, Poraniomorpha and Poraniopsis are revised. In situ feeding observations of Bathyporania are described and compared with other poraniid feeding accounts. C1 [Mah, Christopher L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Foltz, David W.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. RP Mah, CL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. FU NSF [DEB-1036358] FX The authors are grateful to several individuals for their assistance with specimens and specimen collections. We are grateful to Jim Barry, Lonny Lundsten, and the crews and staff at the Monterey Bay Aquarium Research Institute for collection of Bathyporania. Lara Atkinson, South Africa Egagasini Offshore Node (SAEON) collected South African specimens for morphological examination. Martha Nizinski and Cheryl Ames, National Marine Fisheries Service (NMFS), provided and assisted with specimens from the North Atlantic. Jerry Hoff, NMFS provided assistance with locating locality data from the North Pacific. Museum specimen assistance was provided by Bob Van Syoc and Chrissy Piotrowski (CASIZ), Paul Greenhall, Tim Coffer and Linda Ward (USNM) and Marc Eleaume and Nadia Ameziane (MNHN in Paris). We are grateful to Peter Schuchert at the Museum d'histoire naturelle in Geneva, Switzerland for images of the Poraniopsis mira lectotype. James W. Halk and Scott D. Fatland assisted with the molecular work. Funding was provided by NSF award DEB-1036358 to Foltz and Mah. NR 221 TC 3 Z9 3 U1 1 U2 8 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 2014 VL 3795 IS 3 BP 327 EP 372 PG 46 WC Zoology SC Zoology GA AG8EK UT WOS:000335651400007 PM 24870481 ER PT J AU Young, HS Dirzo, R Helgen, KM McCauley, DJ Billeter, SA Kosoy, MY Osikowicz, LM Salkeld, DJ Young, TP Dittmar, K AF Young, Hillary S. Dirzo, Rodolfo Helgen, Kristofer M. McCauley, Douglas J. Billeter, Sarah A. Kosoy, Michael Y. Osikowicz, Lynn M. Salkeld, Daniel J. Young, Truman P. Dittmar, Katharina TI Declines in large wildlife increase landscape-level prevalence of rodent-borne disease in Africa SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Kenya; dilution effect ID INFECTIOUS-DISEASE; SMALL MAMMALS; LYME-DISEASE; SPECIES-DIVERSITY; COMMUNITY COMPOSITION; FLEAS SIPHONAPTERA; LARGE HERBIVORES; EXTINCTION RISK; BARTONELLA SPP.; HOST DIVERSITY AB Populations of large wildlife are declining on local and global scales. The impacts of this pulse of size-selective defaunation include cascading changes to smaller animals, particularly rodents, and alteration of many ecosystem processes and services, potentially involving changes to prevalence and transmission of zoonotic disease. Understanding linkages between biodiversity loss and zoonotic disease is important for both public health and nature conservation programs, and has been a source of much recent scientific debate. In the case of rodent-borne zoonoses, there is strong conceptual support, but limited empirical evidence, for the hypothesis that defaunation, the loss of large wildlife, increases zoonotic disease risk by directly or indirectly releasing controls on rodent density. We tested this hypothesis by experimentally excluding large wildlife from a savanna ecosystem in East Africa, and examining changes in prevalence and abundance of Bartonella spp. infection in rodents and their flea vectors. We found no effect of wildlife removal on per capita prevalence of Bartonella infection in either rodents or fleas. However, because rodent and, consequently, flea abundance doubled following experimental defaunation, the density of infected hosts and infected fleas was roughly twofold higher in sites where large wildlife was absent. Thus, defaunation represents an elevated risk in Bartonella transmission to humans (bartonellosis). Our results (i) provide experimental evidence of large wildlife defaunation increasing landscape-level disease prevalence, (ii) highlight the importance of susceptible host regulation pathways and host/vector density responses in biodiversity-disease relationships, and (iii) suggest that rodent-borne disease responses to large wildlife loss may represent an important context where this relationship is largely negative. C1 [Young, Hillary S.; McCauley, Douglas J.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Young, Hillary S.; Dirzo, Rodolfo; McCauley, Douglas J.] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Salkeld, Daniel J.] Stanford Univ, Woods Inst Environm, Stanford, CA 94305 USA. [Young, Hillary S.; Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Billeter, Sarah A.; Kosoy, Michael Y.; Osikowicz, Lynn M.] Ctr Dis Control & Prevent, Div Vector Borne Infect Dis, Natl Ctr Infect Dis, Ft Collins, CO 80521 USA. [Salkeld, Daniel J.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Young, Truman P.] Univ Calif Davis, Dept Plant Sci, Davis, CA 95616 USA. [Dittmar, Katharina] SUNY Buffalo, Dept Biol Sci, Buffalo, NY 14260 USA. RP Dirzo, R (reprint author), Stanford Univ, Dept Biol, Stanford, CA 94305 USA. EM rdirzo@stanford.edu FU James Smithson Fund of the Smithsonian Institution; National Geographic Society; National Science Foundation [BSR-97-07477, 03-16402, 08-16453, 12-56034, DEB-09-09670, DEB-1213740]; Natural Sciences and Engineering Council of Canada; African Elephant Program of the US Fish and Wildlife Service [98210-0-G563]; Woods Institute for the Environment; Smithsonian Institution Women's Committee FX We thank Cara Brook, Ralph Eckerlin, Jackson Ekadeli, Frederick Erii, Lauren Gillespie, Lauren Helgen, Ashley Hintz, Helen Kafka, Felicia Keesing, John Lochikuya, Margaret Kinnaird, Peter Lokeny, Darrin Lunde, Scott Miller, Mathew Namoni, Everlyn Ndinda, John Ososky, John Montenieri, Jack Silange, Michael Hastriter, and Michael Whiting for help in this project. Financial support for this project came from the James Smithson Fund of the Smithsonian Institution, the National Geographic Society, the National Science Foundation (Long Term Research in Environmental Biology Grants BSR-97-07477, 03-16402, 08-16453, 12-56034, DEB-09-09670, and DEB-1213740), the Natural Sciences and Engineering Council of Canada, the African Elephant Program of the US Fish and Wildlife Service (Grant 98210-0-G563), the Woods Institute for the Environment, and the Smithsonian Institution Women's Committee. Vector images were provided courtesy of the Integration and Application Network, University of Maryland Center for Environmental Science (http://ian.umces.edu/imagelibrary). NR 68 TC 25 Z9 26 U1 12 U2 132 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 13 PY 2014 VL 111 IS 19 BP 7036 EP 7041 DI 10.1073/pnas.1404958111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AH0GS UT WOS:000335798000068 PM 24778215 ER PT J AU Ackermann, M Ajello, M Allafort, A Antolini, E Barbiellini, G Bastieri, D Bellazzini, R Bissaldi, E Bonamente, E Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cavazzuti, E Cecchi, C Chaves, RCG Chekhtman, A Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S D'Ammando, F De Palma, F Dermer, CD Silva, EDE Donato, D Drell, PS Favuzzi, C Finke, J Focke, WB Franckowiak, A Fukazawa, Y Fusco, P Gargano, F Gasparrini, D Gehrels, N Giglietto, N Giordano, F Giroletti, M Godfrey, G Grenier, IA Guiriec, S Hayashida, M Hewitt, JW Horan, D Hughes, RE Iafrate, G Johnson, AS Knoedlseder, J Kuss, M Lande, J Larsson, S Latronico, L Longo, F Loparco, F Lovellette, MN Lubrano, P Mayer, M Mazziotta, MN McEnery, JE Michelson, PF Mizuno, T Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nemmen, R Nuss, E Ohsugi, T Orienti, M Orlando, E Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Porter, TA Raino, S Razzano, M Reimer, A Reimer, O Sanchez, DA Schulz, A Sgro, C Siskind, EJ Spandre, G Spinelli, P Stawarz, L Takahashi, H Takahashi, T Thayer, JG Thayer, JB Thompson, DJ Tinivella, M Torres, DF Tosti, G Troja, E Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Werner, M Winer, BL Wood, DL Wood, KS Aleksic, J Ansoldi, S Antonelli, LA Antoranz, P Babic, A Bangale, P de Almeida, UB Barrio, JA Gonzalez, JB Bednarek, W Berger, K Bernardini, E Biland, A Blanch, O Bock, RK Bonnefoy, S Bonnoli, G Borracci, F Bretz, T Carmona, E Carosi, A Fidalgo, DC Colin, P Colombo, E Contreras, JL Cortina, J Covino, S Da Vela, P Dazzi, F De Angelis, A De Caneva, G De Lotto, B Mendez, CD Doert, M Dominguez, A Prester, DD Dorner, D Doro, M Einecke, S Eisenacher, D Elsaesser, D Farina, E Ferenc, D Fonseca, MV Font, L Frantzen, K Fruck, C Lopez, RJG Garczarczyk, M Terrats, DG Gaug, M Giavitto, G Godinovic, N Munoz, AG Gozzini, SR Hadasch, D Herrero, A Hildebrand, D Hose, J Hrupec, D Idec, W Kadenius, V Kellermann, H Knoetig, ML Kodani, K Konno, Y Krause, J Kubo, H Kushida, J La Barbera, A Lelas, D Lewandowska, N Lindfors, E Lombardi, S Lopez, M Lopez-Coto, R Lopez-Oramas, A Lorenz, E Lozano, I Makariev, M Mallot, K Maneva, G Mankuzhiyil, N Mannheim, K Maraschi, L Marcote, B Mariotti, M Martinez, M Mazin, D Menzel, U Meucci, M Miranda, JM Mirzoyan, R Moralejo, A Munar-Adrover, P Nakajima, D Niedzwiecki, A Nishijima, K Nilsson, K Nowak, N Orito, R Overkemping, A Paiano, S Palatiello, M Paneque, D Paoletti, R Paredes, JM Paredes-Fortuny, X Partini, S Persic, M Prada, F Moroni, PGP Prandini, E Preziuso, S Puljak, I Reinthal, R Rhode, W Ribo, M Rico, J Garcia, JR Rugamer, S Saggion, A Saito, T Saito, K Salvati, M Satalecka, K Scalzotto, V Scapin, V Schultz, C Schweizer, T Shore, SN Sillanpaa, A Sitarek, J Snidaric, I Sobczynska, D Spanier, F Stamatescu, V Stamerra, A Steinbring, T Storz, J Sun, S Suric, T Takalo, L Takami, H Tavecchio, F Temnikov, P Terzic, T Tescaro, D Teshima, M Thaele, J Tibolla, O Toyama, T Treves, A Vogler, P Wagner, RM Zandanel, F Zanin, R Aller, MF Angelakis, E Blinov, DA Djorgovski, SG Drake, AJ Efimova, NV Gurwell, MA Homan, DC Jordan, B Kopatskaya, EN Kovalev, YY Kurtanidze, OM Lahteenmaki, A Larionov, VM Lister, ML Nieppola, E Nikolashvili, MG Ros, E Savolainen, T Sigua, LA Tornikoski, M AF Ackermann, M. Ajello, M. Allafort, A. Antolini, E. Barbiellini, G. Bastieri, D. Bellazzini, R. Bissaldi, E. Bonamente, E. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cavazzuti, E. Cecchi, C. Chaves, R. C. G. Chekhtman, A. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. D'Ammando, F. De Palma, F. Dermer, C. D. do Couto e Silva, E. Donato, D. Drell, P. S. Favuzzi, C. Finke, J. Focke, W. B. Franckowiak, A. Fukazawa, Y. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Giglietto, N. Giordano, F. Giroletti, M. Godfrey, G. Grenier, I. A. Guiriec, S. Hayashida, M. Hewitt, J. W. Horan, D. Hughes, R. E. Iafrate, G. Johnson, A. S. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Mayer, M. Mazziotta, M. N. McEnery, J. E. Michelson, P. F. Mizuno, T. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nemmen, R. Nuss, E. Ohsugi, T. Orienti, M. Orlando, E. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Porter, T. A. Raino, S. Razzano, M. Reimer, A. Reimer, O. Sanchez, D. A. Schulz, A. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Stawarz, L. Takahashi, H. Takahashi, T. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Werner, M. Winer, B. L. Wood, D. L. Wood, K. S. Aleksic, J. Ansoldi, S. Antonelli, L. A. Antoranz, P. Babic, A. Bangale, P. de Almeida, U. Barres Barrio, J. A. Becerra Gonzalez, J. Bednarek, W. Berger, K. Bernardini, E. Biland, A. Blanch, O. Bock, R. K. Bonnefoy, S. Bonnoli, G. Borracci, F. Bretz, T. Carmona, E. Carosi, A. Fidalgo, D. Carreto Colin, P. Colombo, E. Contreras, J. L. Cortina, J. Covino, S. Da Vela, P. Dazzi, F. De Angelis, A. De Caneva, G. De Lotto, B. Mendez, C. Delgado Doert, M. Dominguez, A. Prester, D. Dominis Dorner, D. Doro, M. Einecke, S. Eisenacher, D. Elsaesser, D. Farina, E. Ferenc, D. Fonseca, M. V. Font, L. Frantzen, K. Fruck, C. Lopez, R. J. Garcia Garczarczyk, M. Terrats, D. Garrido Gaug, M. Giavitto, G. Godinovic, N. Munoz, A. Gonzalez Gozzini, S. R. Hadasch, D. Herrero, A. Hildebrand, D. Hose, J. Hrupec, D. Idec, W. Kadenius, V. Kellermann, H. Knoetig, M. L. Kodani, K. Konno, Y. Krause, J. Kubo, H. Kushida, J. La Barbera, A. Lelas, D. Lewandowska, N. Lindfors, E. Lombardi, S. Lopez, M. Lopez-Coto, R. Lopez-Oramas, A. Lorenz, E. Lozano, I. Makariev, M. Mallot, K. Maneva, G. Mankuzhiyil, N. Mannheim, K. Maraschi, L. Marcote, B. Mariotti, M. Martinez, M. Mazin, D. Menzel, U. Meucci, M. Miranda, J. M. Mirzoyan, R. Moralejo, A. Munar-Adrover, P. Nakajima, D. Niedzwiecki, A. Nishijima, K. Nilsson, K. Nowak, N. Orito, R. Overkemping, A. Paiano, S. Palatiello, M. Paneque, D. Paoletti, R. Paredes, J. M. Paredes-Fortuny, X. Partini, S. Persic, M. Prada, F. Moroni, P. G. Prada Prandini, E. Preziuso, S. Puljak, I. Reinthal, R. Rhode, W. Ribo, M. Rico, J. Garcia, J. Rodriguez Ruegamer, S. Saggion, A. Saito, T. Saito, K. Salvati, M. Satalecka, K. Scalzotto, V. Scapin, V. Schultz, C. Schweizer, T. Shore, S. N. Sillanpaeae, A. Sitarek, J. Snidaric, I. Sobczynska, D. Spanier, F. Stamatescu, V. Stamerra, A. Steinbring, T. Storz, J. Sun, S. Suric, T. Takalo, L. Takami, H. Tavecchio, F. Temnikov, P. Terzic, T. Tescaro, D. Teshima, M. Thaele, J. Tibolla, O. Toyama, T. Treves, A. Vogler, P. Wagner, R. M. Zandanel, F. Zanin, R. Aller, M. F. Angelakis, E. Blinov, D. A. Djorgovski, S. G. Drake, A. J. Efimova, N. V. Gurwell, M. A. Homan, D. C. Jordan, B. Kopatskaya, E. N. Kovalev, Y. Y. Kurtanidze, O. M. Laehteenmaeki, A. Larionov, V. M. Lister, M. L. Nieppola, E. Nikolashvili, M. G. Ros, E. Savolainen, T. Sigua, L. A. Tornikoski, M. CA Fermi Large Area Telescope Collab MAGIC Collaboration TI MULTIFREQUENCY STUDIES OF THE PECULIAR QUASAR 4C+21.35 DURING THE 2010 FLARING ACTIVITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; gamma rays: general; quasars: general; quasars: individual (4C +21.35); radiation mechanisms: non-thermal ID RAY BRIGHT BLAZARS; BLACK-HOLE MASS; EXTRAGALACTIC BACKGROUND LIGHT; SPECTRUM RADIO QUASARS; LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS; GAMMA-RAY; GALACTIC NUCLEI; X-RAY; EMISSION-LINE AB The discovery of rapidly variable Very High Energy ( VHE; E > 100 GeV). - ray emission from 4C + 21.35 ( PKS 1222+ 216) by MAGIC on 2010 June 17, triggered by the high activity detected by the Fermi Large Area Telescope ( LAT) in high energy ( HE; E > 100 MeV). - rays, poses intriguing questions on the location of the. - ray emitting region in this flat spectrum radio quasar. We present multifrequency data of 4C + 21.35 collected from centimeter to VHE during 2010 to investigate the properties of this source and discuss a possible emission model. The first hint of detection at VHE was observed by MAGIC on 2010 May 3, soon after a gamma- ray flare detected by Fermi-LAT that peaked on April 29. The same emission mechanism may therefore be responsible for both the HE and VHE emission during the 2010 flaring episodes. Two optical peaks were detected on 2010 April 20 and June 30, close in time but not simultaneous with the two gamma- ray peaks, while no clear connection was observed between the X-ray and gamma- ray emission. An increasing flux density was observed in radio and mm bands from the beginning of 2009, in accordance with the increasing gamma- ray activity observed by Fermi-LAT, and peaking on 2011 January 27 in the mm regime ( 230 GHz). We model the spectral energy distributions ( SEDs) of 4C + 21.35 for the two periods of the VHE detection and a quiescent state, using a one-zone model with the emission coming from a very compact region outside the broad line region. The three SEDs can be fit with a combination of synchrotron self-Compton and external Compton emission of seed photons from a dust torus, changing only the electron distribution parameters between the epochs. The fit of the optical/UV part of the spectrum for 2010 April 29 seems to favor an inner disk radius of < six gravitational radii, as one would expect from a prograde-rotating Kerr black hole. C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.; Bernardini, E.; De Caneva, G.; Gozzini, S. R.; Mallot, K.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Allafort, A.; Caliandro, G. A.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Godfrey, G.; Johnson, A. S.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Porter, T. A.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Allafort, A.; Caliandro, G. A.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Godfrey, G.; Johnson, A. S.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Porter, T. A.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Antolini, E.; Bonamente, E.; Cecchi, C.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Antolini, E.; Bonamente, E.; Cecchi, C.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Barbiellini, G.; Iafrate, G.; Longo, F.; Snidaric, I.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Bissaldi, E.; Longo, F.; Persic, M.; Snidaric, I.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Dazzi, F.; Doro, M.; Mariotti, M.; Paiano, S.; Prandini, E.; Saggion, A.; Scalzotto, V.; Schultz, C.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Dazzi, F.; Doro, M.; Mariotti, M.; Paiano, S.; Prandini, E.; Saggion, A.; Scalzotto, V.; Schultz, C.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bissaldi, E.; Persic, M.] Univ Trieste, I-34127 Trieste, Italy. [Brigida, M.; De Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; De Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Horan, D.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cavazzuti, E.; Cutini, S.; Gasparrini, D.] ASI, Sci Data Ctr, I-00044 Rome, Italy. [Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, CEA IRFU,CNRS,Lab AIM, F-91191 Gif Sur Yvette, France. [Chekhtman, A.] George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Rome, Italy. 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Dominis; Ferenc, D.; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Suric, T.; Terzic, T.] Univ Rijeka, Rudjer Boskov Inst, Croatian MAGIC Consortium, HR-10000 Zagreb, Croatia. [Babic, A.; Prester, D. Dominis; Ferenc, D.; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Suric, T.; Terzic, T.] Univ Split, HR-10000 Zagreb, Croatia. [Bangale, P.; de Almeida, U. Barres; Bock, R. K.; Borracci, F.; Colin, P.; Fruck, C.; Hose, J.; Kellermann, H.; Knoetig, M. L.; Krause, J.; Lorenz, E.; Mazin, D.; Menzel, U.; Mirzoyan, R.; Nakajima, D.; Nowak, N.; Paneque, D.; Garcia, J. Rodriguez; Schweizer, T.; Sun, S.; Teshima, M.; Toyama, T.; Wagner, R. M.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Barrio, J. A.; Bonnefoy, S.; Contreras, J. L.; Fonseca, M. V.; Lopez, M.; Lozano, I.; Satalecka, K.; Scapin, V.] Univ Complutense, E-28040 Madrid, Spain. [Becerra Gonzalez, J.; Berger, K.; Colombo, E.; Lopez, R. J. 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Garrido; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiac, Bellaterra 08193, Spain. [Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain. [Kadenius, V.; Lindfors, E.; Nilsson, K.; Reinthal, R.; Takalo, L.] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland. [Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nishijima, K.; Orito, R.; Saito, T.; Saito, K.; Takami, H.] Kyoto Univ, Div Phys & Astron, Japanese MAGIC Consortium, Kyoto 6068501, Japan. [Makariev, M.; Maneva, G.; Temnikov, P.] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria. [Marcote, B.; Munar-Adrover, P.; Paredes, J. M.; Paredes-Fortuny, X.; Ribo, M.; Zanin, R.] Univ Barcelona ICC IEEC, E-08028 Barcelona, Spain. [Moroni, P. G. Prada; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy. [Moroni, P. G. Prada; Shore, S. N.] INFN Pisa, I-56126 Pisa, Italy. [Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Angelakis, E.; Kovalev, Y. Y.; Ros, E.; Savolainen, T.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Blinov, D. A.; Efimova, N. V.; Larionov, V. M.] Pulkovo Observ, St Petersburg 196140, Russia. [Djorgovski, S. G.; Drake, A. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Efimova, N. V.; Kopatskaya, E. N.; Larionov, V. M.] St Petersburg State Univ, Astron Inst, St Petersburg 199034, Russia. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Homan, D. C.] Denison Univ, Dept Phys, Granville, OH 43023 USA. [Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Kovalev, Y. Y.] Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Kurtanidze, O. M.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Abastumani, Rep of Georgia. [Kurtanidze, O. M.] Kazan Fed Univ, Engelhardt Astron Observ, Tatarstan, Russia. [Laehteenmaeki, A.; Nieppola, E.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Nieppola, E.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikio, Finland. [Ros, E.] Univ Valencia, E-46010 Valencia, Spain. [Larionov, V. M.] St Petersburg Branch, Isaac Newton Inst Chile, St Petersburg, Russia. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM dammando@ira.inaf.it; justin.finke@nrl.navy.mil; davide.donato-1@nasa.gov; tterzic@uniri.hr; jbecerragonzalez@gmail.com RI Fonseca Gonzalez, Maria Victoria/I-2004-2015; Contreras Gonzalez, Jose Luis/K-7255-2014; Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Temnikov, Petar/L-6999-2016; Maneva, Galina/L-7120-2016; Makariev, Martin/M-2122-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Barrio, Juan/L-3227-2014; Martinez Rodriguez, Manel/C-2539-2017; Cortina, Juan/C-2783-2017; Ribo, Marc/B-3579-2015; Antoranz, Pedro/H-5095-2015; Miranda, Jose Miguel/F-2913-2013; Delgado, Carlos/K-7587-2014; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Blinov, Dmitry/G-9925-2013; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; Stamatescu, Victor/C-9945-2016; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Fernandez, Ester/K-9734-2014; Lopez Moya, Marcos/L-2304-2014; GAug, Markus/L-2340-2014; Font, Lluis/L-4197-2014; Moralejo Olaizola, Abelardo/M-2916-2014; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Babic, Ana/B-9599-2014; Lahteenmaki, Anne/L-5987-2013; Reimer, Olaf/A-3117-2013; Kovalev, Yuri/J-5671-2013; Kurtanidze, Omar/J-6237-2014; Rico, Javier/K-8004-2014; OI Bonnoli, Giacomo/0000-0003-2464-9077; Doro, Michele/0000-0001-9104-3214; Stamerra, Antonio/0000-0002-9430-5264; Prandini, Elisa/0000-0003-4502-9053; Becerra Gonzalez, Josefa/0000-0002-6729-9022; Caraveo, Patrizia/0000-0003-2478-8018; Giordano, Francesco/0000-0002-8651-2394; Prada Moroni, Pier Giorgio/0000-0001-9712-9916; LA BARBERA, ANTONINO/0000-0002-5880-8913; Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; De Lotto, Barbara/0000-0003-3624-4480; Sgro', Carmelo/0000-0001-5676-6214; Savolainen, Tuomas/0000-0001-6214-1085; SPINELLI, Paolo/0000-0001-6688-8864; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Bissaldi, Elisabetta/0000-0001-9935-8106; Temnikov, Petar/0000-0002-9559-3384; Torres, Diego/0000-0002-1522-9065; Barrio, Juan/0000-0002-0965-0259; Cortina, Juan/0000-0003-4576-0452; Iafrate, Giulia/0000-0002-6185-8292; Antoranz, Pedro/0000-0002-3015-3601; Miranda, Jose Miguel/0000-0002-1472-9690; Delgado, Carlos/0000-0002-7014-4101; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Blinov, Dmitry/0000-0003-0611-5784; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; Stamatescu, Victor/0000-0001-9030-7513; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Lopez Moya, Marcos/0000-0002-8791-7908; GAug, Markus/0000-0001-8442-7877; Font, Lluis/0000-0003-2109-5961; Moralejo Olaizola, Abelardo/0000-0002-1344-9080; Morselli, Aldo/0000-0002-7704-9553; Babic, Ana/0000-0001-9549-9710; Reimer, Olaf/0000-0001-6953-1385; Kovalev, Yuri/0000-0001-9303-3263; Rico, Javier/0000-0003-4137-1134; Ros, Eduardo/0000-0001-9503-4892; Angelakis, Emmanouil/0000-0001-7327-5441; Covino, Stefano/0000-0001-9078-5507; Paredes, Josep M./0000-0002-1566-9044; Gasparrini, Dario/0000-0002-5064-9495; Tavecchio, Fabrizio/0000-0003-0256-0995; Persic, Massimo/0000-0003-1853-4900; Dominguez, Alberto/0000-0002-3433-4610; Bastieri, Denis/0000-0002-6954-8862; Farina, Emanuele Paolo/0000-0002-6822-2254; Ribo, Marc/0000-0002-9931-4557; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Ahnen, Max Ludwig/0000-0003-1000-0082 FU CPAN [CSD2007- 00042]; MultiDark [CSD2009-00064] FX MAGIC Collaboration would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de losMuchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. Thisworkwas also supported by the CPAN CSD2007- 00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence "Origin and Structure of the Universe," by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. We thank the Swift team for making these observations possible, the duty scientists, and science planners. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2009, AJ, 137, 3718). The MOJAVE project is supported under NASA-Fermi grant 11-Fermi11-0019. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work made use of the Swinburne University of Technology software correlator (Deller et al. 2011, PASP, 123, 275), developed as part of the Australian Major National Research Facilities Programme and operated under license. The OVRO 40-m monitoring program is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST-1109911. This paper is partly based on observations with the 100m telescope of the MPIfR ( Max-Planck-Institut fur Radioastronomie) at Effelsberg and the Medicina telescope operated by INAF-Istituto di Radioastronomia. We acknowledge A. Orlati, S. Righini, and the Enhanced Single-dish Control System (ESCS) Development Team. We acknowledge financial contribution from agreement ASI-INAF I/009/10/0. 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. Data from the Steward Observatory spectropolarimetric monitoring project were used. This program is supported by Fermi Guest Investigator grants NNX08AW56G, NNX09AU10G, and NNX12AO93G. The St. Petersburg University team acknowledges support from Russian RFBR foundation, grants 12-02-00452 and 12-02-31193. The Abastumani team acknowledges financial support of the project FR/638/6-320/12 by the Shota Rustaveli National Science Foundation under contract 31/77. The Metsahovi team acknowledges support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). E. R. was partially supported by the Spanish MINECO projectsAYA2009-13036-C02-02 and AYA2012-38491-C02-01 and by the Generalitat Valenciana project PROMETEO/2009/104, as well as by the COST MP0905 action " Black Holes in a Violent Universe." Y.Y.K. was partly supported by the Russian Foundation for Basic Research (project 13-02-12103) and the Dynasty Foundation. We thank the anonymous referee for useful comments and suggestions. J.F. would like to thank J. Steiner for useful discussions regarding the black hole spin of 4C+21.35. F. D. thanks P. Smith for useful discussions about the polarimetric observations of 4C +21.35. NR 88 TC 12 Z9 12 U1 2 U2 37 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 2014 VL 786 IS 2 AR 157 DI 10.1088/0004-637X/786/2/157 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500080 ER PT J AU Barber, SD Kilic, M Brown, WR Gianninas, A AF Barber, Sara D. Kilic, Mukremin Brown, Warren R. Gianninas, A. TI DUSTY WDs IN THE WISE ALL SKY SURVEY boolean AND SDSS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: planetary systems; infrared: stars; white dwarfs ID POLLUTED WHITE-DWARFS; EXCESS INFRARED RADIATION; EXTRASOLAR MINOR PLANET; FINAL MASS RELATION; DEBRIS DISKS; BROWN DWARF; CATALOG; ACCRETION; SYSTEMS; BRIGHT AB A recent cross-correlation between the Sloan Digital Sky Survey (SDSS) Data Release 7 White Dwarf Catalog with the Wide-Field Infrared Survey Explorer (WISE) all-sky photometry at 3.4, 4.6, 12, and 22 mu m performed by Debes et al. resulted in the discovery of 52 candidate dusty white dwarfs (WDs). However, the 6 '' WISE beam allows for the possibility that many of the excesses exhibited by these WDs may be due to contamination from a nearby source. We present MMT + SAOWide-Field InfraRed Camera J- and H-band imaging observations (0 ''.5-1 ''.5 point spread function) of 16 of these candidate dusty WDs and confirm that four have spectral energy distributions (SEDs) consistent with a dusty disk and are not accompanied by a nearby source contaminant. The remaining 12 WDs have contaminated WISE photometry and SEDs inconsistent with a dusty disk when the contaminating sources are not included in the photometry measurements. We find the frequency of disks around single WDs in the WISE boolean AND SDSS sample to be 2.6%-4.1%. One of the four new dusty WDs has a mass of 1.04M(circle dot) (progenitor mass 5.4M(circle dot)) and its discovery offers the first confirmation that massive WDs (and their massive progenitor stars) host planetary systems. C1 [Barber, Sara D.; Kilic, Mukremin; Gianninas, A.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Brown, Warren R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Barber, SD (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. EM barber@nhn.ou.edu RI Alexandros, Gianninas/B-8352-2016 OI Alexandros, Gianninas/0000-0002-8655-4308 NR 46 TC 12 Z9 12 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 2014 VL 786 IS 2 AR 77 DI 10.1088/0004-637X/786/2/77 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500001 ER PT J AU Battersby, C Bally, J Dunham, M Ginsburg, A Longmore, S Darling, J AF Battersby, Cara Bally, John Dunham, Miranda Ginsburg, Adam Longmore, Steve Darling, Jeremy TI THE COMPARISON OF PHYSICAL PROPERTIES DERIVED FROM GAS AND DUST IN A MASSIVE STAR-FORMING REGION SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; evolution; ISM: abundances; ISM: molecules; stars: formation ID INFRARED-DARK CLOUDS; GALACTIC PLANE; PROTOSTELLAR CORES; INITIAL CONDITIONS; NH3 OBSERVATIONS; METHANOL MASERS; COLUMN DENSITY; DATA REDUCTION; AMMONIA; HERSCHEL AB We explore the relationship between gas and dust in a massive star-forming region by comparing the physical properties derived from each. We compare the temperatures and column densities in a massive star-forming Infrared Dark Cloud (G32.02+ 0.05), which shows a range of evolutionary states, from quiescent to active. The gas properties were derived using radiative transfer modeling of the (1,1), (2,2), and (4,4) transitions of NH3 on the Karl G. Jansky Very Large Array, while the dust temperatures and column densities were calculated using cirrus-subtracted, modified blackbody fits to Herschel data. We compare the derived column densities to calculate an NH3 abundance, XNH3 = 4.6 x 10(-8). In the coldest star-forming region, we find that the measured dust temperatures are lower than the measured gas temperatures (mean and standard deviations T-dust,T-avg similar to 11.6 +/- 0.2 K versus T-gas,(avg) similar to 15.2 +/- 1.5 K), which may indicate that the gas and dust are not well-coupled in the youngest regions (similar to 0.5Myr) or that these observations probe a regime where the dust and/or gas temperature measurements are unreliable. Finally, we calculate millimeter fluxes based on the temperatures and column densities derived from NH3, which suggest that millimeter dust continuum observations of massive star-forming regions, such as the Bolocam Galactic Plane Survey or ATLASGAL, can probe hot cores, cold cores, and the dense gas lanes from which they form, and are generally not dominated by the hottest core. C1 [Battersby, Cara; Bally, John; Ginsburg, Adam; Darling, Jeremy] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Battersby, Cara] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dunham, Miranda] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Ginsburg, Adam] European So Observ, D-85748 Garching, Germany. [Longmore, Steve] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. RP Battersby, C (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, UCB 389, Boulder, CO 80309 USA. OI Darling, Jeremy/0000-0003-2511-2060; Ginsburg, Adam/0000-0001-6431-9633 FU National Science Foundation [AST-9800334, AST-0098562, AST-0100793, AST-0228993, AST-0507657]; Italian Space Agency [I/038/080/0] FX We thank the referee for helpful comments which have helped to improve the quality of this manuscript. We thank Hugo Martel and Neal Evans for assistance comparing our results with their cluster-scale simulations. This work has made use of the GLIMPSE and MIPSGAL surveys, and we thank those teams for their help and support. We would like to thank the staff at VLA for their assistance. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This publication makes use of molecular line data from the Boston University-FCRAO Galactic Ring Survey (GRS). The GRS is a joint project of Boston University and Five College Radio Astronomy Observatory, funded by the National Science Foundation under grants AST-9800334, AST-0098562, AST-0100793, AST-0228993, and AST-0507657. This work has made use of ds9 and the Goddard Space Flight Center's IDL Astronomy Library. Data processing and map production of the Herschel data has been possible thanks to generous support from the Italian Space Agency via contract I/038/080/0. Data presented in this paper were also analyzed using The Herschel Interactive Processing Environment (HIPE), a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS, and SPIRE consortia. NR 46 TC 12 Z9 12 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 2014 VL 786 IS 2 AR 116 DI 10.1088/0004-637X/786/2/116 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500040 ER PT J AU Drake, JJ Braithwaite, J Kashyap, V Gunther, HM Wright, NJ AF Drake, Jeremy J. Braithwaite, Jonathan Kashyap, Vinay Guenther, H. Moritz Wright, Nicholas J. TI BURN OUT OR FADE AWAY? ON THE X-RAY AND MAGNETIC DEATH OF INTERMEDIATE MASS STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: activity; stars: coronae; stars: magnetic field; Sun: activity; Sun: corona; X-rays: stars ID HERBIG-AE/BE STARS; A-TYPE STARS; MAIN-SEQUENCE STARS; ACTIVITY-ROTATION RELATIONSHIP; DARKEST BRIGHT STAR; BETA-PICTORIS; TW HYDRAE; HR 4796A; DIFFERENTIAL ROTATION; CIRCUMSTELLAR DISK AB The nature of the mechanisms apparently driving X-rays from intermediate mass stars lacking strong convection zones or massive winds remains poorly understood, and the possible role of hidden, lower mass close companions is still unclear. A 20 ks Chandra HRC-I observation of HR 4796A, an 8 Myr old main sequence A0 star devoid of close stellar companions, has been used to search for a signature or remnant of magnetic activity from the Herbig Ae phase. X-rays were not detected and the X-ray luminosity upper limit was L-X <= 1.3 x 10(27) erg s(-1). The result is discussed in the context of various scenarios for generating magnetic activity, including rotational shear and subsurface convection. A dynamo driven by natal differential rotation is unlikely to produce observable X rays, chiefly because of the difficulty in getting the dissipated energy up to the surface of the star. A subsurface convection layer produced by the ionization of helium could host a dynamo that should be effective throughout the main sequence but can only produce X-ray luminosities of the order 10(25) erg s(-1). This luminosity lies only moderately below the current detection limit for Vega. Our study supports the idea that X-ray production in Herbig Ae/Be stars is linked largely to the accretion process rather than the properties of the underlying star, and that early A stars generally decline in X-ray luminosity at least 100,000 fold in only a few million years. C1 [Drake, Jeremy J.; Kashyap, Vinay; Guenther, H. Moritz; Wright, Nicholas J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Braithwaite, Jonathan] Argelander Inst Astron, D-53121 Bonn, Germany. [Wright, Nicholas J.] Univ Hertfordshire, STRI, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, MS-3,60 Garden St, Cambridge, MA 02138 USA. EM jdrake@cfa.harvard.edu OI Gunther, Hans Moritz/0000-0003-4243-2840 FU Chandra [GO7-8006X]; NASA [NAS8-03060] FX J.J.D. and V.K. thank the NASA AISRP for providing financial assistance for the development of the PINTofALE package. This work was partially funded by Chandra grant GO7-8006X. J.J.D. and V. K. were funded by NASA contract NAS8-03060 to the Chandra X-ray Center during the course of this research and thank the Director, H. Tananbaum, for continuing support and encouragement. NR 75 TC 5 Z9 5 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 136 DI 10.1088/0004-637X/786/2/136 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500059 ER PT J AU Fouesneau, M Johnson, LC Weisz, DR Dalcanton, JJ Bell, EF Bianchi, L Caldwell, N Gouliermis, DA Guhathakurta, P Kalirai, J Larsen, SS Rix, HW Seth, AC Skillman, ED Williams, BF AF Fouesneau, Morgan Johnson, L. Clifton Weisz, Daniel R. Dalcanton, Julianne J. Bell, Eric F. Bianchi, Luciana Caldwell, Nelson Gouliermis, Dimitrios A. Guhathakurta, Puragra Kalirai, Jason Larsen, Soren S. Rix, Hans-Walter Seth, Anil C. Skillman, Evan D. Williams, Benjamin F. TI THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY. V. AGES AND MASSES OF THE YEAR 1 STELLAR CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M31); galaxies: star clusters: general; methods: data analysis; techniques:photometric ID SMALL-MAGELLANIC-CLOUD; DISRUPTION TIME-SCALES; MASSIVE STAR-CLUSTERS; ANTENNAE GALAXIES; GLOBULAR-CLUSTERS; SPIRAL GALAXIES; RADIATIVE OPACITIES; FORMATION HISTORY; YOUNG CLUSTERS; EVOLUTION AB We present ages and masses for 601 star clusters in M31 from the analysis of the six filter integrated light measurements from near-ultraviolet to near-infrared wavelengths, made as part of the Panchromatic Hubble Andromeda Treasury (PHAT). We derive the ages and masses using a probabilistic technique, which accounts for the effects of stochastic sampling of the stellar initialmass function. Tests on synthetic data show that this method, in conjunction with the exquisite sensitivity of the PHAT observations and their broad wavelength baseline, provides robust age and mass recovery for clusters ranging from similar to 102 to 2 x 10(6) M-circle dot. We find that the cluster age distribution is consistent with being uniform over the past 100 Myr, which suggests a weak effect of cluster disruption within M31. The age distribution of older (> 100 Myr) clusters falls toward old ages, consistent with a power-law decline of index - 1, likely from a combination of fading and disruption of the clusters. We find that the mass distribution of the whole sample can be well described by a single power law with a spectral index of - 1.9 +/- 0.1 over the range of 10(3)-3 x 10(5)M circle dot. However, if we subdivide the sample by galactocentric radius, we find that the age distributions remain unchanged. However, the mass spectral index varies significantly, showing best-fit values between - 2.2 and -1.8, with the shallower slope in the highest star formation intensity regions. We explore the robustness of our study to potential systematics and conclude that the cluster mass function may vary with respect to environment. C1 [Fouesneau, Morgan; Johnson, L. Clifton; Weisz, Daniel R.; Dalcanton, Julianne J.; Williams, Benjamin F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Weisz, Daniel R.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA. [Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bianchi, Luciana] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gouliermis, Dimitrios A.] Heidelberg Univ, Inst Theoret Phys, Zentrum Astron, D-69120 Heidelberg, Germany. [Gouliermis, Dimitrios A.; Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Guhathakurta, Puragra] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Kalirai, Jason] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Larsen, Soren S.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Seth, Anil C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Skillman, Evan D.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. RP Fouesneau, M (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA. EM mfouesn@uw.edu OI Seth, Anil/0000-0003-0248-5470; Gouliermis, Dimitrios/0000-0002-2763-0075; Johnson, Lent/0000-0001-6421-0953; Bell, Eric/0000-0002-5564-9873 FU German Research Foundation (DFG) [1659/3-1]; NASA through Hubble Fellowship - Space Telescope Science Institute [HST-HF-51331.01]; NASA [HST GO-12055] FX The authors acknowledge the efforts of the entire PHAT collaboration in this project. Also, the authors thank Nate Bastian for his prompt and useful referee report. D. G. kindly acknowledges financial support by the German Research Foundation (DFG) through grant GO 1659/3-1. Support for D.R.W. is provided by NASA through Hubble Fellowship grants HST-HF-51331.01 awarded by the Space Telescope Science Institute. This paper is based on observations taken with the NASA/ESA Hubble Space Telescope. Support for this work was provided by NASA through grant number HST GO-12055 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555. NR 67 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 MAY 10 PY 2014 VL 786 IS 2 AR 117 DI 10.1088/0004-637X/786/2/117 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500041 ER PT J AU Hanneman, WJ Reeves, KK AF Hanneman, Will J. Reeves, Katharine K. TI THERMAL STRUCTURE OF CURRENT SHEETS AND SUPRA-ARCADE DOWNFLOWS IN THE SOLAR CORONA SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: coronal mass ejections (CMEs); Sun: flares ID X-RAY TELESCOPE; QUANTITATIVE EXAMINATION; RECONNECTION OUTFLOWS; PATCHY RECONNECTION; EXTREME-ULTRAVIOLET; ATOMIC DATABASE; FLARE PLASMA; EMISSION; XRT; RECONSTRUCTION AB After the peak intensity of many large solar flares, magnetic and thermodynamic processes give rise to a phenomenon known as supra-arcade downflows (SADs). SADs are sunward flowing density depletions, often observed in post-flare plasma sheets. Some models have suggested that the plasma in the dark lanes is heated to temperatures of 20-80 MK, which is much hotter than temperatures of the surrounding plasma. In this work, we use data from the Atmospheric Imaging Assembly on the Solar Dynamics Observatory and the X-Ray Telescope on the Hinode satellite to determine the thermal structure of SADs in the solar corona. We examine four flares that took place on 2011 October 22, 2012 January 14, 2012 January 16, and 2012 January 27. Differential emission measures are calculated for each flare and we compare the temperatures in the SADs to those of the surrounding plasma. We find that the SADs are hotter than the background, but cooler than the surrounding plasma in most cases, with only 1 out of the 11 SADs examined here having a slightly higher temperature than its surroundings. C1 [Hanneman, Will J.; Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hanneman, Will J.] Univ Southampton, Southampton SO17 1BJ, Hants, England. RP Hanneman, WJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 58, Cambridge, MA 02138 USA. EM whanneman@cfa.harvard.edu; kreeves@cfa.harvard.edu RI Reeves, Katharine/P-9163-2014 FU Lockheed-Martin [SP02H1701R]; NASA [NNM07AB07C, NNX13AG54G] FX The authors would like to thank the anonymous referee for helpful comments that improved this paper, and P. Jibben, S. Saar, and M. Weber for help with the XRT point-spread function. This paper was part of a master's thesis from the University of Southampton. Will Hanneman would like to thank J. Drake and P. Charles for maintaining the connection between the University of Southampton and the Harvard-Smithsonian Center for Astrophysics. Travel to the AAS meeting and part of K. K. Reeves contribution supported under contract SP02H1701R from Lockheed-Martin to SAO. K. K. Reeves is also supported under contract NNM07AB07C from NASA to SAO and NASA grant NNX13AG54G. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and the NSC (Norway). This work has benefited from the use of NASA's Astrophysics Data System. NR 47 TC 11 Z9 11 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 95 DI 10.1088/0004-637X/786/2/95 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500019 ER PT J AU Lee, CF Hirano, N Zhang, QZ Shang, H Ho, PTP Krasnopolsky, R AF Lee, Chin-Fei Hirano, Naomi Zhang, Qizhou Shang, Hsien Ho, Paul T. P. Krasnopolsky, Ruben TI ALMA RESULTS OF THE PSEUDODISK, ROTATING DISK, AND JET IN THE CONTINUUM AND HCO+ IN THE PROTOSTELLAR SYSTEM HH 212 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; ISM: individual objects (HH 212); ISM: jets and outflows; stars: formation ID MAGNETIC BRAKING; KEPLERIAN DISK; STAR-FORMATION; OUTFLOW; EMISSION; ENVELOPE; COLLAPSE; HH-212; CORES; GAS AB HH 212 is a nearby (400 pc) Class 0 protostellar system showing several components that can be compared with theoretical models of core collapse. We have mapped it in the 350 GHz continuum and HCO+ J = 4-3 emission with ALMA at up to similar to 0 ''.4 resolution. A flattened envelope and a compact disk are seen in the continuum around the central source, as seen before. The HCO+ kinematics shows that the flattened envelope is infalling with small rotation (i.e., spiraling) into the central source, and thus can be identified as a pseudodisk in the models of magnetized core collapse. Also, the HCO+ kinematics shows that the disk is rotating and can be rotationally supported. In addition, to account for the missing HCO+ emission at low-redshifted velocity, an extended infalling envelope is required, with its material flowing roughly parallel to the jet axis toward the pseudodisk. This is expected if it is magnetized with an hourglass B-field morphology. We have modeled the continuum and HCO+ emission of the flattened envelope and disk simultaneously. We find that a jump in density is required across the interface between the pseudodisk and the disk. A jet is seen in HCO+ extending out to similar to 500 AU away from the central source, with the peaks upstream of those seen before in SiO. The broad velocity range and high HCO+ abundance indicate that the HCO+ emission traces internal shocks in the jet. C1 [Lee, Chin-Fei; Hirano, Naomi; Shang, Hsien; Ho, Paul T. P.; Krasnopolsky, Ruben] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Zhang, Qizhou; Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lee, CF (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM cflee@asiaa.sinica.edu.tw OI Zhang, Qizhou/0000-0003-2384-6589 FU National Science Council of Taiwan [NSC 101-2119-M-001-002-MY3]; Academia Sinica (Career Development Award) FX This paper makes use of the following ALMA data: ADS/JAO. ALMA#2011.0.00647. 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. These data were made available to C.-F.L., as part of his ALMA proposal 2011.0.00122.S (PI: C.-F.L.), which requested observations duplicating those of proposal 2011.0.00647.S. C.-F.L. acknowledges grants from the National Science Council of Taiwan (NSC 101-2119-M-001-002-MY3) and the Academia Sinica (Career Development Award). NR 40 TC 22 Z9 22 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 114 DI 10.1088/0004-637X/786/2/114 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500038 ER PT J AU McCully, C Jha, SW Foley, RJ Chornock, R Holtzman, JA Balam, DD Branch, D Filippenko, AV Frieman, J Fynbo, J Galbany, L Ganeshalingam, M Garnavich, PM Graham, ML Hsiao, EY Leloudas, G Leonard, DC Li, WD Riess, AG Sako, M Schneider, DP Silverman, JM Sollerman, J Steele, TN Thomas, RC Wheeler, JC Zheng, C AF McCully, Curtis Jha, Saurabh W. Foley, Ryan J. Chornock, Ryan Holtzman, Jon A. Balam, David D. Branch, David Filippenko, Alexei V. Frieman, Joshua Fynbo, Johan Galbany, Lluis Ganeshalingam, Mohan Garnavich, Peter M. Graham, Melissa L. Hsiao, Eric Y. Leloudas, Giorgos Leonard, Douglas C. Li, Weidong Riess, Adam G. Sako, Masao Schneider, Donald P. Silverman, Jeffrey M. Sollerman, Jesper Steele, Thea N. Thomas, Rollin C. Wheeler, J. Craig Zheng, Chen TI HUBBLE SPACE TELESCOPE AND GROUND-BASED OBSERVATIONS OF THE TYPE Iax SUPERNOVAE SN 2005hk AND SN 2008A SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (SN 2002cx, SN 2005hk, SN 2008A) ID DELAYED-DETONATION MODEL; LATE-TIME SPECTRA; MASS WHITE-DWARF; LIGHT CURVES; DARK ENERGY; FAINT TYPE; THERMONUCLEAR SUPERNOVAE; FACTORY OBSERVATIONS; NEBULAR SPECTRA; HIPASS CATALOG AB We present Hubble Space Telescope (HST) and ground-based optical and near-infrared observations of SN 2005hk and SN 2008A, typical members of the Type Iax class of supernovae (SNe). Here we focus on late-time observations, where these objects deviate most dramatically from all other SN types. Instead of the dominant nebular emission lines that are observed in other SNe at late phases, spectra of SNe 2005hk and 2008A show lines of Fe II, Ca II, and Fe I more than a year past maximum light, along with narrow [ Fe II] and [ Ca II] emission. We use spectral features to constrain the temperature and density of the ejecta, and find high densities at late times, with n(e) greater than or similar to 10(9) cm(-3). Such high densities should yield enhanced cooling of the ejecta, making these objects good candidates to observe the expected "infrared catastrophe," a generic feature of SN Ia models. However, our HST photometry of SN 2008A does not match the predictions of an infrared catastrophe. Moreover, our HST observations rule out a "complete deflagration" that fully disrupts the white dwarf for these peculiar SNe, showing no evidence for unburned material at late times. Deflagration explosion models that leave behind a bound remnant can match some of the observed properties of SNe Iax, but no published model is consistent with all of our observations of SNe 2005hk and 2008A. C1 [McCully, Curtis; Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Foley, Ryan J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, Ryan J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Holtzman, Jon A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Balam, David D.] Herzberg Inst Astrophys, Dominion Astrophys Observ, Victoria, BC V9E 2E7, Canada. [Branch, David] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Filippenko, Alexei V.; Silverman, Jeffrey M.; Steele, Thea N.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Frieman, Joshua] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Frieman, Joshua] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Frieman, Joshua] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Fynbo, Johan; Leloudas, Giorgos; Sollerman, Jesper] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Galbany, Lluis] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Bellaterra, Barcelona, Spain. [Galbany, Lluis] Inst Super Tecn, Ctr Multidisciplinar Astrofis, P-1049001 Lisbon, Portugal. [Ganeshalingam, Mohan] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Garnavich, Peter M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Graham, Melissa L.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Graham, Melissa L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Graham, Melissa L.; Hsiao, Eric Y.] Las Campanas Observ, Carnegie Observ, Atacama, Chile. [Leloudas, Giorgos] Stockholm Univ, Oskar Klein Ctr, Dept Phys, SE-10691 Stockholm, Sweden. [Leonard, Douglas C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Riess, Adam G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Sako, Masao] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Silverman, Jeffrey M.; Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Sollerman, Jesper] Stockholm Univ, Dept Astron, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Thomas, Rollin C.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Zheng, Chen] Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Zheng, Chen] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. RP McCully, C (reprint author), Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. EM cmccully@physics.rutgers.edu RI Galbany, Lluis/A-8963-2017; OI Galbany, Lluis/0000-0002-1296-6887; Sollerman, Jesper/0000-0003-1546-6615; McCully, Curtis/0000-0001-5807-7893 FU Rutgers University through NASA/HST [GO-11133.01, GO-11590.01]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; NSF [AST-1109801, AST-1211916]; Swedish Research Council [623-2011-7117]; Gary and Cynthia Bengier; Richard and Rhoda Goldman Fund; TABASGO Foundation; NASA/HST [GO-10877, AR-12623]; Space Telescope Science Institute; NASA; Alfred P. Sloan Foundation; Participating Institutions; NSF; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX This research at Rutgers University was supported through NASA/HST grants GO-11133.01 and GO-11590.01, along with U. S. Department of Energy (DOE) grant DE-FG02-08ER41562, and National Science Foundation (NSF) CAREER award AST-0847157 to S.W.J., and a G Lambda Lambda NN Fellowship to C.M.J. M. S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. The research of J.C.W. is supported in part by NSF Grant AST-1109801. G. L. is supported by the Swedish Research Council through grant No. 623-2011-7117. A.V.F. and his group at UC Berkeley are funded by Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, NSF grant AST-1211916, the TABASGO Foundation, and NASA/HST grants GO-10877 and AR-12623.; Support for HST programs GO-10877, GO-11133, GO-11590, and AR-12623 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.; Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the University of California, the California Institute of Technology, and NASA, made possible by the generous financial support of the W. M. Keck Foundation. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community, and we are most privileged to have the opportunity to explore the universe from this mountain.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the NSF, the U.S. Department of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max- Planck-Institute for Astronomy (MPIA), the Max- Planck- Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 116 TC 17 Z9 17 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 134 DI 10.1088/0004-637X/786/2/134 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500057 ER PT J AU Mommert, M Hora, JL Farnocchia, D Chesley, SR Vokrouhlicky, D Trilling, DE Mueller, M Harris, AW Smith, HA Fazio, GG AF Mommert, M. Hora, J. L. Farnocchia, D. Chesley, S. R. Vokrouhlicky, D. Trilling, D. E. Mueller, M. Harris, A. W. Smith, H. A. Fazio, G. G. TI CONSTRAINING THE PHYSICAL PROPERTIES OF NEAR-EARTH OBJECT 2009 BD SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: planetary systems; minor planets, asteroids: individual (2009 BD) ID THERMAL-INFRARED OBSERVATIONS; SPITZER-SPACE-TELESCOPE; RADIATION PRESSURE; ASTEROIDAL FRAGMENTS; YARKOVSKY; POPULATION; TARGET; RADAR; MISSION; HAYABUSA AB We report on Spitzer Space Telescope Infrared Array Camera observations of near-Earth object 2009 BD that were carried out in support of the NASA Asteroid Robotic Retrieval Mission concept. We did not detect 2009 BD in 25 hr of integration at 4.5 mu m. Based on an upper-limit flux density determination from our data, we present a probabilistic derivation of the physical properties of this object. The analysis is based on the combination of a thermophysical model with an orbital model accounting for the non-gravitational forces acting upon the body. We find two physically possible solutions. The first solution shows 2009 BD as a 2.9 +/- 0.3 m diameter rocky body (rho = 2.9 +/- 0.5 g cm(-3)) with an extremely high albedo of 0.85(-0.10)(+0.20) that is covered with regolith-like material, causing it to exhibit a low thermal inertia (Gamma = 30(-10)(+20) SI units). The second solution suggests 2009 BD to be a 4 +/- 1 m diameter asteroid with pv = 0.45(-0.15)(+0.35) that consists of a collection of individual bare rock slabs (Gamma = 2000 +/- 1000 SI units, rho = 1.7(-0.4)(+0.7) g cm(-3)). We are unable to rule out either solution based on physical reasoning. 2009 BD is the smallest asteroid for which physical properties have been constrained, in this case using an indirect method and based on a detection limit, providing unique information on the physical properties of objects in the size range smaller than 10 m. C1 [Mommert, M.; Trilling, D. E.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Hora, J. L.; Smith, H. A.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Farnocchia, D.; Chesley, S. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vokrouhlicky, D.] Charles Univ Prague, Inst Astron, CZ-18000 Prague 8, Czech Republic. [Mueller, M.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Harris, A. W.] DLR Inst Planetary Res, D-12489 Berlin, Germany. RP Mommert, M (reprint author), No Arizona Univ, Dept Phys & Astron, POB 6010, Flagstaff, AZ 86011 USA. EM michael.mommert@nau.edu OI Mueller, Michael/0000-0003-3217-5385 FU NASA Postdoctoral Program at the Jet Propulsion Laboratory; California Institute of Technology; Grant Agency of the Czech Republic [P209-13- 01308S]; Propulsion Laboratory RSA [1367413] FX The authors of this work thank Tom Soifer, Director of the Spitzer Space Telescope, for the time allocation to observe 2009 BD. We also would like to thank Paul Chodas for his support and many informative conversations. We thank an anonymous referee for useful suggestions that improved this manuscript. D. Farnocchia was supported for this research by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. The work of S. Chesley was conducted at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. The work of D. Vokrouhlicky was partially supported by the Grant Agency of the Czech Republic (grant P209-13- 01308S). J. L. Hora and H. A. Smith acknowledge partial support from Jet Propulsion Laboratory RSA No. 1367413. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 71 TC 7 Z9 7 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 148 DI 10.1088/0004-637X/786/2/148 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500071 ER PT J AU Oesch, PA Bouwens, RJ Illingworth, GD Labbe, I Smit, R Franx, M van Dokkum, PG Momcheva, I Ashby, MLN Fazio, GG Huang, JS Willner, SP Gonzalez, V Magee, D Trenti, M Brammer, GB Skelton, RE Spitler, LR AF Oesch, P. A. Bouwens, R. J. Illingworth, G. D. Labbe, I. Smit, R. Franx, M. van Dokkum, P. G. Momcheva, I. Ashby, M. L. N. Fazio, G. G. Huang, J. -S. Willner, S. P. Gonzalez, V. Magee, D. Trenti, M. Brammer, G. B. Skelton, R. E. Spitler, L. R. TI THE MOST LUMINOUS z similar to 9-10 GALAXY CANDIDATES YET FOUND: THE LUMINOSITY FUNCTION, COSMIC STAR-FORMATION RATE, AND THE FIRST MASS DENSITY ESTIMATE AT 500 Myr* SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: luminosity function, mass function ID ULTRA-DEEP FIELD; HUBBLE-SPACE-TELESCOPE; LYMAN-BREAK GALAXIES; EXTRAGALACTIC LEGACY SURVEY; HIGH-REDSHIFT GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; EMISSION-LINE GALAXIES; GOODS-SOUTH FIELD; FAINT-END SLOPES; EXTREMELY RED H AB We present the discovery of four surprisingly bright (H-160 similar to 26-27 mag AB) galaxy candidates at z similar to 9-10 in the complete HST CANDELS WFC3/IR GOODS-N imaging data, doubling the number of z similar to 10 galaxy candidates that are known, just similar to 500 Myr after the big bang. Two similarly bright sources are also detected in a reanalysis of the GOODS-S data set. Three of the four galaxies in GOODS-N are significantly detected at 4.5 sigma-6.2 sigma in the very deep Spitzer/IRAC 4.5 mu m data, as is one of the GOODS-S candidates. Furthermore, the brightest of our candidates (at z = 10.2 +/- 0.4) is robustly detected also at 3.6 mu m (6.9 sigma), revealing a flat UV spectral energy distribution with a slope beta = -2.0 +/- 0.2, consistent with demonstrated trends with luminosity at high redshift. Thorough testing and use of grism data excludes known low-redshift contamination at high significance, including single emission-line sources, but as-yet unknown low redshift sources could provide an alternative solution given the surprising luminosity of these candidates. Finding such bright galaxies at z similar to 9-10 suggests that the luminosity function for luminous galaxies might evolve in a complex way at z > 8. The cosmic star formation rate density still shows, however, an order-of-magnitude increase from z similar to 10 to z similar to 8 since the dominant contribution comes from low-luminosity sources. Based on the IRAC detections, we derive galaxy stellar masses at z similar to 10, finding that these luminous objects are typically 10(9) M-circle dot. This allows for a first estimate of the cosmic stellar mass density at z similar to 10 resulting in log(10) P* = 4.7(-0.8)(+0.5) M-circle dot Mpc(-3) for galaxies brighter than MUV similar to -18. The remarkable brightness, and hence luminosity, of these z similar to 9-10 candidates will enable deep spectroscopy to determine their redshift and nature, and highlights the opportunity for the James Webb Space Telescope to map the buildup of galaxies at redshifts much earlier than z similar to 10. C1 [Oesch, P. A.; Illingworth, G. D.; Magee, D.] Univ Calif Santa Cruz, UCO, Lick Observ, Santa Cruz, CA 95064 USA. [Oesch, P. A.; van Dokkum, P. G.; Momcheva, I.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Bouwens, R. J.; Labbe, I.; Smit, R.; Franx, M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Ashby, M. L. N.; Fazio, G. G.; Huang, J. -S.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gonzalez, V.] Univ Calif Riverside, Riverside, CA 92507 USA. [Trenti, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Trenti, M.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Brammer, G. B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Skelton, R. E.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Spitler, L. R.] Macquarie Univ, Fac Sci, Dept Phys & Astron, N Ryde, NSW 2109, Australia. [Spitler, L. R.] Australian Astron Observ, N Ryde, NSW 1670, Australia. RP Oesch, PA (reprint author), Univ Calif Santa Cruz, UCO, Lick Observ, 1156 High St, Santa Cruz, CA 95064 USA. EM pascal.oesch@yale.edu RI Gonzalez, Valentino/I-5279-2016; Skelton, Rosalind/S-1845-2016; OI Skelton, Rosalind/0000-0001-7393-3336; Oesch, Pascal/0000-0001-5851-6649 FU NASA through Hubble Fellowship [HF-51278.01]; Space Telescope Science Institute; NASA [NAS 5-26555, NAG5-7697, HSTGO-11563, HST-GO-12177, JPL1416188/1438944]; ERC [HIGHZ 227749]; NWO vrij competitie [600.065.140.11N211]; National Science Foundation [PHY-1066293] FX We thank the anonymous referee for very helpful feedback that improved the paper. We also thank Jason Jaacks, Sandro Tacchella, and Kristian Finlator for providing us with the predictions of their models. Support for this work was provided by NASA through Hubble Fellowship grant HF-51278.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Additionally, this work was supported by NASA grant NAG5-7697, NASA grant HSTGO-11563, NASA grant HST-GO-12177, NASA grant JPL1416188/1438944, ERC grant HIGHZ 227749, and NWO vrij competitie grant 600.065.140.11N211. This work was further supported in part by the National Science Foundation under grant PHY-1066293 and the Aspen Center for Physics. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. NR 98 TC 97 Z9 97 U1 2 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 MAY 10 PY 2014 VL 786 IS 2 AR 108 DI 10.1088/004-637X/786/2/108 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500032 ER PT J AU Puzia, TH Paolillo, M Goudfrooij, P Maccarone, TJ Fabbiano, G Angelini, L AF Puzia, Thomas H. Paolillo, Maurizio Goudfrooij, Paul Maccarone, Thomas J. Fabbiano, Giuseppina Angelini, Lorella TI WIDE-FIELD HUBBLE SPACE TELESCOPE OBSERVATIONS OF THE GLOBULAR CLUSTER SYSTEM IN NGC 1399 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: individual (NGC 1399); galaxies: star clusters: general; globular clusters: general ID EARLY-TYPE GALAXIES; ACS-VIRGO CLUSTER; SURFACE-BRIGHTNESS PROFILES; LARGE-MAGELLANIC-CLOUD; NEARBY DWARF GALAXIES; MASSIVE STAR-CLUSTERS; POINT-SPREAD FUNCTION; HALF-LIGHT RADII; STRUCTURAL PARAMETERS; FORNAX CLUSTER AB We present a comprehensive high spatial resolution imaging study of globular clusters (GCs) in NGC 1399, the central giant elliptical cD galaxy in the Fornax galaxy cluster, conducted with the Advanced Camera for Surveys (ACS) aboard the Hubble Space Telescope (HST). Using a novel technique to construct drizzled point-spread function libraries for HST/ACS data, we accurately determine the fidelity of GC structural parameter measurements from detailed artificial star cluster experiments and show the superior robustness of the GC half-light radius, r(h), compared with other GC structural parameters, such as King core and tidal radius. The measurement of r(h) for the major fraction of the NGC 1399 GC system reveals a trend of increasing r(h) versus galactocentric distance, R-gal, out to about 10 kpc and a flat relation beyond. This trend is very similar for blue and red GCs, which are found to have a mean size ratio of r(h),(red)/r(h),(blue) = 0.82 +/- 0.11 at all galactocentric radii from the core regions of the galaxy out to similar to 40 kpc. This suggests that the size difference between blue and red GCs is due to internal mechanisms related to the evolution of their constituent stellar populations. Modeling the mass density profile of NGC 1399 shows that additional external dynamical mechanisms are required to limit the GC size in the galaxy halo regions to r(h) approximate to 2 pc. We suggest that this may be realized by an exotic GC orbit distribution function, an extended dark matter halo, and/or tidal stress induced by the increased stochasticity in the dwarf halo substructure at larger galactocentric distances. We compare our results with the GC r(h) distribution functions in various galaxies and find that the fraction of extended GCs with r(h) >= 5 pc is systematically larger in late-type galaxies compared with GC systems in early-type galaxies. This is likely due to the dynamically more violent evolution of early-type galaxies. We match our GC r(h) measurements with radial velocity data from the literature and split the resulting sample at the median r(h) value into compact and extended GCs. We find that compact GCs show a significantly smaller line-of-sight velocity dispersion, = 225 +/- 25 km s(-1), than their extended counterparts, = 317 +/- 21 km s(-1). Considering the weaker statistical correlation in the GC r(h) color and the GC r(h)-R-gal relations, the more significant GC size-dynamics relation appears to be astrophysically more relevant and hints at the dominant influence of the GC orbit distribution function on the evolution of GC structural parameters. C1 [Puzia, Thomas H.] Pontificia Univ Catolica Chile, Natl Res Council Canada, Santiago 7820436, Chile. [Puzia, Thomas H.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Paolillo, Maurizio] Univ Naples Federico II, Dept Phys Sci, I-80126 Naples, Italy. [Paolillo, Maurizio] Ist Nazl Fis Nucl, Dept Phys Sci, Napoli Unit, I-80126 Naples, Italy. [Paolillo, Maurizio] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy. [Goudfrooij, Paul] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Maccarone, Thomas J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Fabbiano, Giuseppina] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Angelini, Lorella] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. RP Puzia, TH (reprint author), Pontificia Univ Catolica Chile, Natl Res Council Canada, Ave Vicuna Mackenna 4860, Santiago 7820436, Chile. EM tpuzia@astro.puc.cl RI Paolillo, Maurizio/J-1733-2012 OI Paolillo, Maurizio/0000-0003-4210-7693 FU NASA [NAS5-26555]; FONDECYT [1121005]; BASAL Center for Astrophysics and Associated Technologies [PFB-06]; National Research Council of Canada; University of Napoli Federico II; Chandra X-ray Center (CXC) [NAS8-03060] FX Support for HST program GO- 10129 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. This research was supported by FONDECYT Regular Project grant 1121005 and BASAL Center for Astrophysics and Associated Technologies (PFB-06). T. H. P. is thankful for the hospitality and support during his visits at the University of Napoli Federico II, where parts of this work were completed; he also gratefully acknowledges support in the form of a Plaskett Research Fellowship from the National Research Council of Canada. M. P. acknowledges financial support from the FARO 2011 project of the University of Napoli Federico II. This work was partially supported by the Chandra X-ray Center (CXC), which is operated by the Smithsonian Astrophysical Observatory (SAO) under NASA contract NAS8-03060. We are grateful to Anton Koekemoer and Andy Fruchter for their technical support and useful discussions on the MultiDrizzle code and to Chien Y. Peng for his help with the implementation and testing of the modified GALFIT routine. We thank TomRichtler and Ylva Schuberth for providing their radial velocity measurements ahead of publication, as well as Luis Ho and Zhao-Yu Li for kindly making available to us their latest NGC 1399 surface brightness profile measurements from the Carnegie-Irvine Galaxy Survey, again prior to publication. Avon Huxor has very kindly supplied M31 GC data prior to publication. We are grateful to the referee, Bill Harris, for providing a thoughtful and constructive report that helped improve the presentation of the results. We thank Jeremy Webb, Mark Gieles, Andres Jordan, Eric Peng, Chunyan Jiang, Stephen Zepf, and Arunav Kundu for valuable discussions and providing data in electronic format. Some of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. 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. Figures 2 and 3 were created with the help of the ESA/ESO/NASA Photoshop FITS Liberator. This research has made use of NASA's Astrophysics Data System. Facility: HST(ACS) NR 171 TC 22 Z9 22 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 MAY 10 PY 2014 VL 786 IS 2 AR 78 DI 10.1088/0004-637X/786/2/78 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500002 ER PT J AU Sobolewska, MA Siemiginowska, A Kelly, BC Nalewajko, K AF Sobolewska, M. A. Siemiginowska, A. Kelly, B. C. Nalewajko, K. TI STOCHASTIC MODELING OF THE FERMI/LAT gamma-RAY BLAZAR VARIABILITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; BL Lacertae objects: general; galaxies: active; galaxies: jets; gamma rays: galaxies ID ACTIVE GALACTIC NUCLEI; DAMPED RANDOM-WALK; OPTICAL VARIABILITY; TIMING PROPERTIES; TERM VARIABILITY; TEV VARIABILITY; BLACK-HOLES; HARD STATE; COMPONENTS; GALAXIES AB We study the gamma-ray variability of 13 blazars observed with the Fermi/Large Area Telescope (LAT). These blazars have the most complete light curves collected during the first four years of the Fermi sky survey. We model them with the Ornstein-Uhlenbeck (OU) process or a mixture of the OU processes. The OU process has power spectral density (PSD) proportional to 1/f(alpha) with alpha changing at a characteristic timescale, tau(0), from 0 (tau >> tau(0)) to 2 (tau << tau(0)). The PSD of the mixed OU process has two characteristic timescales and an additional intermediate region with 0 < alpha < 2. We show that the OU model provides a good description of the Fermi/LAT light curves of three blazars in our sample. For the first time, we constrain a characteristic gamma-ray timescale of variability in two BL Lac sources, 3C 66A and PKS 2155-304 (tau(0) similar or equal to 25 days and tau 0 similar or equal to 43 days, respectively, in the observer's frame), which are longer than the soft X-ray timescales detected in blazars and Seyfert galaxies. We find that the mixed OU process approximates the light curves of the remaining 10 blazars better than the OU process. We derive limits on their long and short characteristic timescales, and infer that their Fermi/LAT PSD resemble power-law functions. We constrain the PSD slopes for all but one source in the sample. We find hints for sub-hour Fermi/LAT variability in four flat spectrum radio quasars. We discuss the implications of our results for theoretical models of blazar variability. C1 [Sobolewska, M. A.; Siemiginowska, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sobolewska, M. A.] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Kelly, B. C.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93107 USA. [Nalewajko, K.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Nalewajko, K.] NIST, Boulder, CO 80309 USA. RP Sobolewska, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM malgosia@camk.edu.pl FU Fermi grant [NNX11AO45G]; NASA [NAS8-03060]; Polish National Science Center [2011/03/B/ST9/03281]; NASA through Einstein Postdoctoral Fellowship [PF3-140112] FX This research made use of data obtained with the Fermi Gamma-Ray Observatory. The authors thank Mitch Begelman and James Chiang for discussions and comments, and the anonymous referee for reviewing our manuscript. Partial support for this work was provided by the Fermi grant NNX11AO45G and by NASA contract NAS8-03060. M.A.S. was partially supported by the Polish National Science Center grant No. 2011/03/B/ST9/03281. K.N. was supported by NASA through Einstein Postdoctoral Fellowship grant No. PF3-140112 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. NR 38 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 143 DI 10.1088/0004-637X/786/2/143 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500066 ER PT J AU Starikova, S Jones, C Forman, WR Vikhlinin, A Kurtz, MJ Geller, MJ Fabricant, DG Murray, SS Dell'Antonio, IP AF Starikova, Svetlana Jones, Christine Forman, William R. Vikhlinin, Alexey Kurtz, Michael J. Geller, Margaret J. Fabricant, Daniel G. Murray, Stephen S. Dell'Antonio, Ian P. TI COMPARISON OF GALAXY CLUSTERS SELECTED BY WEAK-LENSING, OPTICAL SPECTROSCOPY, AND X-RAYS IN THE DEEP LENS SURVEY F2 FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; gravitational lensing: weak; X-rays: galaxies: clusters ID DIGITAL SKY SURVEY; FIBER-FED SPECTROGRAPH; DARK-MATTER; LUMINOSITY FUNCTION; REDSHIFT SURVEYS; DATA RELEASE; CATALOG; CHANDRA; SAMPLE; COSMOLOGY AB We compare galaxy clusters selected in Chandra and XMM-Newton X-ray observations of the 4 deg(2) Deep Lens Survey (DLS) F2 field to the cluster samples previously selected in the same field from a sensitive weak-lensing shear map derived from the DLS and from a detailed galaxy redshift survey-the Smithsonian Hectospec Lensing Survey (SHELS). Our Chandra and XMM-Newton observations cover 1.6 deg(2) of the DLS F2 field, including all 12 weak-lensing peaks above a signal-to-noise ratio of 3.5, along with 16 of the 20 SHELS clusters with published velocity dispersions > 500 km s(-1). We detect 26 extended X-ray sources in this area and confirm 23 of them as galaxy clusters using the optical imaging. Approximately 75% of clusters detected in either X-ray or spectroscopic surveys are found in both; these follow the previously established scaling relations between velocity dispersion, L-X, and T-X. A lower percentage, 60%, of clusters are in common between X-ray and DLS samples. With the exception of a high false-positive rate in the DLS weak-lensing search (5 out of 12 DLS candidates appear to be false), differences between the three cluster detection methods can be attributed primarily to observational uncertainties and intrinsic scatter between different observables and cluster mass. C1 [Starikova, Svetlana; Jones, Christine; Forman, William R.; Vikhlinin, Alexey; Kurtz, Michael J.; Fabricant, Daniel G.; Murray, Stephen S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vikhlinin, Alexey] Space Res Inst IKI, Moscow, Russia. [Geller, Margaret J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Dell'Antonio, Ian P.] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Starikova, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Forman, William/0000-0002-9478-1682 FU NASA [NAS8-03060, NNX12AE35G]; Smithsonian Consortium for Unlocking the Mysteries of the Universe FX Support for this work was provided by the NASA contract NAS8-03060, NASA Grant NNX12AE35G, and the Smithsonian Consortium for Unlocking the Mysteries of the Universe. NR 67 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 125 DI 10.1088/0004-637X/786/2/125 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500049 ER PT J AU Tian, H DeLuca, E Reeves, KK McKillop, S De Pontieu, B Martinez-Sykora, J Carlsson, M Hansteen, V Kleint, L Cheung, M Golub, L Saar, S Testa, P Weber, M Lemen, J Title, A Boerner, P Hurlburt, N Tarbell, TD Wuelser, JP Kankelborg, C Jaeggli, S McIntosh, SW AF Tian, H. DeLuca, E. Reeves, K. K. McKillop, S. De Pontieu, B. Martinez-Sykora, J. Carlsson, M. Hansteen, V. Kleint, L. Cheung, M. Golub, L. Saar, S. Testa, P. Weber, M. Lemen, J. Title, A. Boerner, P. Hurlburt, N. Tarbell, T. D. Wuelser, J. P. Kankelborg, C. Jaeggli, S. McIntosh, S. W. TI HIGH-RESOLUTION OBSERVATIONS OF THE SHOCK WAVE BEHAVIOR FOR SUNSPOT OSCILLATIONS WITH THE INTERFACE REGION IMAGING SPECTROGRAPH SO ASTROPHYSICAL JOURNAL LA English DT Article DE line: profiles; Sun: chromosphere; Sun: oscillations; Sun: transition region; waves ID RUNNING PENUMBRAL WAVES; TRANSITION REGION; DYNAMIC FIBRILS; SPECTROSCOPIC OBSERVATIONS; MAGNETOACOUSTIC SHOCKS; NUMERICAL SIMULATIONS; PROPAGATING WAVES; ATOMIC DATABASE; UMBRAL FLASHES; CORONAL LOOPS AB We present the first results of sunspot oscillations from observations by the Interface Region Imaging Spectrograph. The strongly nonlinear oscillation is identified in both the slit-jaw images and the spectra of several emission lines formed in the transition region and chromosphere. We first apply a single Gaussian fit to the profiles of the Mg II 2796.35 angstrom, C II 1335.71 angstrom, and Si IV 1393.76 angstrom lines in the sunspot. The intensity change is similar to 30%. The Doppler shift oscillation reveals a saw tooth pattern with an amplitude of similar to 10 km s(-1) in Si IV. The Si IV oscillation lags those of C II and Mg II by similar to 6 and similar to 25 s, respectively. The line width suddenly increases as the Doppler shift changes from redshift to blueshift. However, we demonstrate that this increase is caused by the superposition of two emission components. We then perform detailed analysis of the line profiles at a few selected locations on the slit. The temporal evolution of the line core is dominated by the following behavior: a rapid excursion to the blue side, accompanied by an intensity increase, followed by a linear decrease of the velocity to the red side. The maximum intensity slightly lags the maximum blueshift in Si IV, whereas the intensity enhancement slightly precedes the maximum blueshift in Mg II. We find a positive correlation between the maximum velocity and deceleration, a result that is consistent with numerical simulations of upward propagating magnetoacoustic shock waves. C1 [Tian, H.; DeLuca, E.; Reeves, K. K.; McKillop, S.; Golub, L.; Saar, S.; Testa, P.; Weber, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [De Pontieu, B.; Martinez-Sykora, J.; Kleint, L.; Cheung, M.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Martinez-Sykora, J.; Kleint, L.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Carlsson, M.; Hansteen, V.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Kleint, L.] NASA, Ames Res Ctr, Moffett Field, CA 94305 USA. [Kankelborg, C.; Jaeggli, S.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [McIntosh, S. W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. RP Tian, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hui.tian@cfa.harvard.edu RI Reeves, Katharine/P-9163-2014; DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Carlsson, Mats/0000-0001-9218-3139 FU NASA [NNG09FA40C]; Lockheed Martin Independent Research Program; European Research Council [291058]; LMSAL [8100002705] 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 the Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract. This work is supported by NASA under contract NNG09FA40C (IRIS) and the Lockheed Martin Independent Research Program, the European Research Council grant agreement No. 291058, and contract 8100002705 from LMSAL to SAO. H. T. thanks Luc Rouppe van der Voort and Jorrit Leenaarts for useful discussion. NR 56 TC 35 Z9 35 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 137 DI 10.1088/0004-637X/786/2/137 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500060 ER PT J AU Utsumi, Y Miyazaki, S Geller, MJ Dell'Antonio, IP Oguri, M Kurtz, MJ Hamana, T Fabricant, DG AF Utsumi, Yousuke Miyazaki, Satoshi Geller, Margaret J. Dell'Antonio, Ian P. Oguri, Masamune Kurtz, Michael J. Hamana, Takashi Fabricant, Daniel G. TI REDUCING SYSTEMATIC ERROR IN WEAK LENSING CLUSTER SURVEYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; gravitational lensing: weak; techniques: image processing ID DARK-MATTER HALOS; SHEAR-SELECTED CLUSTERS; FIBER-FED SPECTROGRAPH; BONN DEEP SURVEY; GALAXY CLUSTERS; REDSHIFT SURVEYS; SUPRIME-CAM; HECTOSPEC; GABODS; SHELS AB Weak lensing provides an important route toward collecting samples of clusters of galaxies selected by mass. Subtle systematic errors in image reduction can compromise the power of this technique. We use the B-mode signal to quantify this systematic error and to test methods for reducing this error. We show that two procedures are efficient in suppressing systematic error in the B-mode: (1) refinement of the mosaic CCD warping procedure to conform to absolute celestial coordinates and (2) truncation of the smoothing procedure on a scale of 10'. Application of these procedures reduces the systematic error to 20% of its original amplitude. We provide an analytic expression for the distribution of the highest peaks in noise maps that can be used to estimate the fraction of false peaks in the weak-lensing kappa-signal-to-noise ratio (S/N) maps as a function of the detection threshold. Based on this analysis, we select a threshold S/N=4.56 for identifying an uncontaminated set of weak-lensing peaks in two test fields covering a total area of similar to 3 deg(2). Taken together these fields contain seven peaks above the threshold. Among these, six are probable systems of galaxies and one is a superposition. We confirm the reliability of these peaks with dense redshift surveys, X-ray, and imaging observations. The systematic error reduction procedures we apply are general and can be applied to future large-area weak-lensing surveys. Our high-peak analysis suggests that with an S/N threshold of 4.5, there should be only 2.7 spurious weak-lensing peaks even in an area of 1000 deg2, where we expect similar to 2000 peaks based on our Subaru fields. C1 [Utsumi, Yousuke; Miyazaki, Satoshi; Hamana, Takashi] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Utsumi, Yousuke] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Miyazaki, Satoshi] Grad Univ Adv Studies, Mitaka, Tokyo 1818588, Japan. [Geller, Margaret J.; Kurtz, Michael J.; Fabricant, Daniel G.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Dell'Antonio, Ian P.] Brown Univ, Dept Phys, Providence, RI 02912 USA. [Oguri, Masamune] Univ Tokyo, Univ Kavli IPMU, WPI, Kavli Inst Phys & Math, Kashiwa, Chiba 2778583, Japan. [Oguri, Masamune] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. RP Utsumi, Y (reprint author), Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. EM yutsumi@naoj.org RI Oguri, Masamune/C-6230-2011; OI Utsumi, Yousuke/0000-0001-6161-8988 FU Japan Society for the Promotion of Science (JSPS) through JSPS Research Fellowships for Young Scientists; Department of Astronomical Sciences of the Graduate University for Advanced Studies (SOKENDAI) through Research incentive; Smithsonian Institution; FIRST program "Subaru Measurements of Images and Redshifts (SuMIRe)," World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan; JSPS [23740161] FX Y.U. acknowledges financial support from the Japan Society for the Promotion of Science (JSPS) through JSPS Research Fellowships for Young Scientists and from the Department of Astronomical Sciences of the Graduate University for Advanced Studies (SOKENDAI) through Research incentive.; The Smithsonian Institution supports the research of M.G., D.G.F., and M.J.K.; This work was also supported in part by the FIRST program "Subaru Measurements of Images and Redshifts (SuMIRe)," World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and Grant-in-Aid for Scientific Research from the JSPS (23740161). NR 53 TC 8 Z9 8 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2014 VL 786 IS 2 AR 93 DI 10.1088/0004-637X/786/2/93 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH1MI UT WOS:000335884500017 ER PT J AU Guillochon, J Loeb, A MacLeod, M Ramirez-Ruiz, E AF Guillochon, James Loeb, Abraham MacLeod, Morgan Ramirez-Ruiz, Enrico TI POSSIBLE ORIGIN OF THE G2 CLOUD FROM THE TIDAL DISRUPTION OF A KNOWN GIANT STAR BY SGR A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE black hole physics; galaxies : active; gravitation ID SUPERMASSIVE BLACK-HOLE; STELLAR ASTROPHYSICS MESA; SAGITTARIUS A-ASTERISK; GALACTIC-CENTER; GAS CLOUD; HYDRODYNAMICAL SIMULATIONS; PROPER MOTIONS; CENTRAL PARSEC; DYNAMICS; GALAXY AB The discovery of the gas cloud G2 on a near-radial orbit about Sgr A* has prompted much speculation on its origin. In this Letter, we propose that G2 formed out of the debris stream produced by the removal of mass from the outer envelope of a nearby giant star. We perform hydrodynamical simulations of the returning tidal debris stream with cooling and find that the stream condenses into clumps that fall periodically onto Sgr A*. We propose that one of these clumps is the observed G2 cloud, with the rest of the stream being detectable at lower Br gamma. emissivity along a trajectory that would trace from G2 to the star that was partially disrupted. By simultaneously fitting the orbits of S2, G2, and similar to 2000 candidate stars, and by fixing the orbital plane of each candidate star to G2 (as is expected for a tidal disruption), we find that several stars have orbits that are compatible with the notion that one of them was tidally disrupted to produce G2. If one of these stars were indeed disrupted, it last encountered Sgr A* hundreds of years ago and has likely encountered Sgr A* repeatedly. However, while these stars are compatible with the giant disruption scenario given their measured positions and proper motions, their radial velocities are currently unknown. If one of these stars' radial velocity is measured to be compatible with a disruptive orbit, it would strongly suggest that its disruption produced G2. C1 [Guillochon, James; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [MacLeod, Morgan; Ramirez-Ruiz, Enrico] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. 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 Guillochon, James/0000-0002-9809-8215 FU Einstein [PF3-140108]; NSF; NSF GFRP; [AST-1312034] FX We thank L. Meyer and S. Gillessen for assistance in interpreting the observational data. This work was supported by Einstein grant PF3-140108 (J.G.), NSF grant AST-1312034 (A.L.), and NSF GFRP (M.M.). NR 44 TC 24 Z9 24 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 2014 VL 786 IS 2 AR L12 DI 10.1088/2041-8205/786/2/L12 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0QB UT WOS:000335824100003 ER PT J AU van Weeren, RJ Intema, HT Lal, DV Andrade-Santos, F Bruggen, M de Gasperin, F Forman, WR Hoeft, M Jones, C Nuza, SE Rottgering, HJA Stroe, A AF van Weeren, R. J. Intema, H. T. Lal, D. V. Andrade-Santos, F. Brueggen, M. de Gasperin, F. Forman, W. R. Hoeft, M. Jones, C. Nuza, S. E. Rottgering, H. J. A. Stroe, A. TI A DISTANT RADIO MINI-HALO IN THE PHOENIX GALAXY CLUSTER SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: clusters: individual (SPT-CL J2344-4243); galaxies: clusters: intracluster medium; large-scale structure of universe; radiation mechanisms: non-thermal; X-rays: galaxies: clusters ID COOLING FLOW CLUSTERS; LUMINOUS CLUSTER; IMAGING SURVEY; SOUTHERN SKY; COLD FRONTS; COSMIC-RAYS; EMISSION; CORES; DISCOVERY; MINIHALOS AB We report the discovery of extended radio emission in the Phoenix cluster (SPT-CL J2344-4243, z = 0.596) with the Giant Metrewave Radio Telescope (GMRT) at 610 MHz. The diffuse emission extends over a region of at least 400-500 kpc and surrounds the central radio source of the Brightest Cluster Galaxy, but does not appear to be directly associated with it. We classify the diffuse emission as a radio mini-halo, making it the currently most distant mini-halo known. Radio mini-halos have been explained by synchrotron emitting particles re-accelerated via turbulence, possibly induced by gas sloshing generated from a minor merger event. Chandra observations show a non-concentric X-ray surface brightness distribution, which is consistent with this sloshing interpretation. The mini-halo has a flux density of 17 +/- 5 mJy, resulting in a 1.4 GHz radio power of (10.4 +/- 3.5) x 10(24) WHz(-1). The combined cluster emission, which includes the central compact radio source, is also detected in a shallow GMRT 156 MHz observation and together with the 610 MHz data we compute a spectral index of -0.84 +/- 0.12 for the overall cluster radio emission. Given that mini-halos typically have steeper radio spectra than cluster radio galaxies, this spectral index should be taken as an upper limit for the mini-halo. C1 [van Weeren, R. J.; Andrade-Santos, F.; Forman, W. R.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Intema, H. T.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Lal, D. V.] TIFR, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Brueggen, M.; de Gasperin, F.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Hoeft, M.] Thuringer Landessternwarte Tautenburg, D-21029 Tautenburg, Germany. [Nuza, S. E.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Rottgering, H. J. A.; Stroe, A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP van Weeren, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rvanweeren@cfa.harvard.edu RI Intema, Huib/D-1438-2012; OI Intema, Huib/0000-0002-5880-2730; de Gasperin, Francesco/0000-0003-4439-2627; van Weeren, Reinout/0000-0002-0587-1660; Forman, William/0000-0002-9478-1682 FU Einstein Postdoctoral [PF2-130104]; Chandra X-Ray Center; Smithsonian Astrophysical Observatory for NASA [NAS8-03060]; National Radio Astronomy Observatory; Deutsche Forschungsgemeinschaf; DFG NU [332/2-1]; Smithsonian Institution; [FOR 1254] FX 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. H. T. I. acknowledges support from the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. M. B. and M. H. acknowledge support by the research group FOR 1254 funded by the Deutsche Forschungsgemeinschaft: " Magnetisation of interstellar and intergalactic media: the prospects of low-frequency radio observations." S. E. N. is supported by the DFG NU 332/2-1. W. R. F., C. J., and F. A.-S. acknowledge support from the Smithsonian Institution. We thank Annalisa Bonafede and Julie Hlavacek-Larrondo for commenting on an earlier version of this Letter. NR 35 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 10 PY 2014 VL 786 IS 2 AR L17 DI 10.1088/2041-8205/786/2/L17 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0QB UT WOS:000335824100008 ER PT J AU Doppler, J Mendez-Bermudez, JA Feist, J Dietz, O Krimer, DO Makarov, NM Izrailev, FM Rotter, S AF Doppler, J. Mendez-Bermudez, J. A. Feist, J. Dietz, O. Krimer, D. O. Makarov, N. M. Izrailev, F. M. Rotter, S. TI Reflection resonances in surface-disordered waveguides: strong higher-order effects of the disorder SO NEW JOURNAL OF PHYSICS LA English DT Article DE scattering mechanisms; coherent transport; transmission through waveguides; surface and disorder scattering; localization effects; nano-wires ID RANDOM-MATRIX THEORY; ROUGH BOUNDARIES; QUANTUM TRANSPORT; LIGHT-SCATTERING; LOCALIZATION; FILMS; CONDUCTIVITY; POLARITONS; TRANSITION; PARTICLES AB We study coherent wave scattering through waveguides with a step-like surface disorder and find distinct enhancements in the reflection coefficients at well-defined resonance values. Based on detailed numerical and analytical calculations, we can unambiguously identify the origin of these reflection resonances to be higher-order correlations in the surface disorder profile which are typically neglected in similar studies of the same system. A remarkable feature of this new effect is that it relies on the longitudinal correlations in the step profile, although individual step heights are random and thus completely uncorrelated. The corresponding resonances are very pronounced and robust with respect to ensemble averaging, and lead to an enhancement of wave reflection by more than one order of magnitude. C1 [Doppler, J.; Krimer, D. O.; Rotter, S.] Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria. [Mendez-Bermudez, J. A.; Izrailev, F. M.] Benemerita Univ Autonoma Puebla, Inst Fis, Puebla 72570, Mexico. [Feist, J.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Feist, J.] Univ Autonoma Madrid, Dept Fis Teor Mat Condensada, E-28049 Madrid, Spain. [Dietz, O.] Humboldt Univ, Inst Phys, Berlin, Germany. [Makarov, N. M.] Benemerita Univ Autonoma Puebla, Inst Ciencias, Puebla 72050, Mexico. RP Doppler, J (reprint author), Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria. EM joerg.doppler@tuwien.ac.at; stefan.rotter@tuwien.ac.at RI Feist, Johannes/J-7394-2012; Rotter, Stefan/E-1997-2011 OI Feist, Johannes/0000-0002-7972-0646; Rotter, Stefan/0000-0002-4123-1417 FU Vienna Science and Technology Fund (WWTF) [MA09-030]; Austrian Science Fund (FWF) [SFB IR-ON F25-14, SFB NextLite F49-10, I 1142-N27]; Vienna Scientific Cluster (VSC); NSF; European Research Council [290981]; VIEP-BUAP [IZMF-EXC13-G, MEBJ-EXC13-I.]; CONACYT [N-133375]; SEP-CONACYT (Mexico) [CB-2011-01-166382] FX The authors are grateful to U Kuhl, M Liertzer, M Rendon, H-J Stockmann, and S Wimberger for fruitful discussions. J D and S R acknowledge support by the Vienna Science and Technology Fund (WWTF) through project MA09-030 and by the Austrian Science Fund (FWF) through Projects No. SFB IR-ON F25-14, No. SFB NextLite F49-10, and No. I 1142-N27 (GePartWave), as well as computational resources by the Vienna Scientific Cluster (VSC). J F acknowledges support by the NSF through a grant to ITAMP and by the European Research Council under Grant No. 290981 (PLASMONANOQUANTA). F.M.I. and J.A.M.-B. acknowledge the VIEP-BUAP grants IZMF-EXC13-G and MEBJ-EXC13-I. F.M.I. also acknowledges partial support from CONACYT Grant No. N-133375. N.M.M acknowledges support from the SEP-CONACYT (Mexico) under Grant No. CB-2011-01-166382. NR 74 TC 2 Z9 2 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD MAY 9 PY 2014 VL 16 AR 053026 DI 10.1088/1367-2630/16/5/053026 PG 25 WC Physics, Multidisciplinary SC Physics GA AL0VB UT WOS:000338843900006 ER PT J AU Vogelsberger, M Genel, S Springel, V Torrey, P Sijacki, D Xu, D Snyder, G Bird, S Nelson, D Hernquist, L AF Vogelsberger, M. Genel, S. Springel, V. Torrey, P. Sijacki, D. Xu, D. Snyder, G. Bird, S. Nelson, D. Hernquist, L. TI Properties of galaxies reproduced by a hydrodynamic simulation SO NATURE LA English DT Article ID MOVING-MESH COSMOLOGY; COLD DARK-MATTER; LY-ALPHA SYSTEMS; STAR-FORMATION; POWER SPECTRUM; RADIAL-DISTRIBUTION; SCALING RELATIONS; MASSIVE GALAXIES; DWARF GALAXIES; LOCAL UNIVERSE AB Previous simulations of the growth of cosmic structures have broadly reproduced the 'cosmic web' of galaxies that we see in the Universe, but failed to create a mixed population of elliptical and spiral galaxies, because of numerical inaccuracies and incomplete physical models. Moreover, they were unable to track the small-scale evolution of gas and stars to the present epoch within a representative portion of the Universe. Here we report a simulation that starts 12 million years after the Big Bang, and traces 13 billion years of cosmic evolution with 12 billion resolution elements in a cube of 106.5 megaparsecs a side. It yields a reasonable population of ellipticals and spirals, reproduces the observed distribution of galaxies in clusters and characteristics of hydrogen on large scales, and at the same time matches the 'metal' and hydrogen content of galaxies on small scales. C1 [Vogelsberger, M.] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Genel, S.; Torrey, P.; Nelson, D.; Hernquist, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Springel, V.; Xu, D.] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, V.] Heidelberg Univ, Zentrum Astron, ARI, D-69120 Heidelberg, Germany. [Sijacki, D.] Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Sijacki, D.] Inst Astron, Cambridge CB3 0HA, England. [Snyder, G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Bird, S.] Inst Adv Study, Princeton, NJ 08540 USA. RP Vogelsberger, M (reprint author), MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. EM mvogelsb@mit.edu OI Torrey, Paul/0000-0002-5653-0786; Bird, Simeon/0000-0001-5803-5490; Genel, Shy/0000-0002-3185-1540 FU DFG Research Centre SFB-881; European Research Council [ERC-StG EXAGAL-308037]; HST [HST-AR-12856.01-A]; NASA from the Space Telescope Science Institute [12856, NAS 5-26555]; NASA [NNX12AC67G]; NSF [AST-1312095, AST-0907969]; Alexander von Humboldt Foundation; GCS [pr85je]; NASA Office of Space Science [NNX13AC07G]; [9,352]; [9,425]; [9,488]; [9,575]; [9,793]; [9,978]; [10,086]; [10,189]; [10,258]; [10,340]; [10,530]; [11,359]; [11,563]; [12,060]; [12,061]; [12,062]; [12,099]; [12,177] FX V. S. acknowledges support from the DFG Research Centre SFB-881 'The Milky Way System' through project A1, and from the European Research Council under ERC-StG EXAGAL-308037. G. S. acknowledges support from the HST grants programme, no. HST-AR-12856.01-A. Support for program no. 12856 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. L. H. acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. D. X. acknowledges support from the Alexander von Humboldt Foundation. S. B. was supported by NSF grant AST-0907969. The Illustris simulation was run on 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 GCS-project pr85je. Further simulations were run on the Harvard Odyssey and CfA/ITC clusters, the Ranger and Stampede supercomputers at the Texas Advanced Computing Center through XSEDE, and the Kraken supercomputer at Oak Rridge National Laboratory through XSEDE. Figure 1b is based on observations made with the NASA/ESA Hubble Space Telescope. These data were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). These observations were associated with programs 9,352, 9,425, 9,488, 9,575, 9,793, 9,978, 10,086, 10,189, 10,258, 10,340, 10,530, 11,359, 11,563, 12,060, 12,061, 12,062, 12,099 and 12,177, and compiled for the Hubble eXtreme Deep Field data release version 1.0 (http://archive.stsci.edu/prepds/xdf/). 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. NR 75 TC 173 Z9 173 U1 2 U2 26 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 8 PY 2014 VL 509 IS 7499 BP 177 EP + DI 10.1038/nature13316 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AG5JC UT WOS:000335454300029 PM 24805343 ER PT J AU Hovers, E Ekshtain, R Greenbaum, N Malinsky-Buller, A Nir, N Yeshurun, R AF Hovers, Erella Ekshtain, Ravid Greenbaum, Noam Malinsky-Buller, Ariel Nir, Nadav Yeshurun, Reuven TI Islands in a stream? Reconstructing site formation processes in the late Middle Paleolithic site of 'Ein Qashish, northern Israel SO QUATERNARY INTERNATIONAL LA English DT Article; Proceedings Paper CT Israel-Science-Foundation Workshop on Opportunities, Problems and Future Directions in the Study of Open-Air Middle Paleolithic Sites CY NOV, 2012 CL Tel Hai Coll, ISRAEL SP Israel Sci Fdn HO Tel Hai Coll ID SEDIMENT CONSOLIDATION; OLDUVAI GORGE; BONE; ASSEMBLAGES; TAPHONOMY; IDENTIFICATION; TRANSPORT; RECORD; PALIMPSESTS; ORIENTATION AB Information retrieved from open-air sites is necessary for a more complete reconstruction of Middle Paleolithic behaviors, which is currently often based mainly on data from caves and rockshelters. However, open-air sites present methodological and analytical challenges that differ from those encountered in cave sites. Being essentially an integral part of their paleo-landscape, open-air sites are affected by localized as well as landscape-scale processes that need to be distinguished from the anthropogenic signatures. 'Ein Qashish is an open-air late Middle Paleolithic occurrence located in the Yizra'el Valley just east of Mt. Carmel, situated on the Pleistocene floodplain of the Qishon stream. The site is found at the interface of the sediments deposited by the Qishon stream, which drains the Yizra'el Valley, and paleo-Wadi Qashish, which flowed off Mt. Carmel. Artifacts and bones are dispersed over a vertical distance of some 90 cm. Observations in geological trenches located at variable distances from the excavated area indicate that this cluster of finds occurred at a circumscribed locality on the landscape rather than as a part of a continuous distribution on the paleo-surface. We 'reverse-engineer' site formation processes, starting with the latest (post-depositional), moving to earlier (syn-depositional) processes, and relate them to their most likely causative agents through the examination of a series of explicit models. GIS techniques were applied in order to parse the variable lines of information, which include lithic and faunal taphonomy, size distributions and spatial and stratigraphic dispersal of objects, fabric analysis and OSL results. We discuss the implications of the results for distinguishing anthropogenic from non-anthropogenic effects and for reconstructing the timeline of depositional events that led to the current distribution of artifacts. Insights into these questions inform our understanding of human activities at the site, suggesting that the excavation samples the margins of an occupation horizon where activities focused on knapping and resource processing rather than task-specific behaviors such as hunting. (C) 2014 Elsevier Ltd and INQUA. All rights reserved. C1 [Hovers, Erella; Ekshtain, Ravid; Malinsky-Buller, Ariel; Nir, Nadav] Hebrew Univ Jerusalem, Inst Archaeol, Jerusalem, Israel. [Greenbaum, Noam] Univ Haifa, Dept Geog & Environm Studies, IL-31999 Haifa, Israel. [Yeshurun, Reuven] Univ Haifa, Zinman Inst Archaeol, IL-31999 Haifa, Israel. [Yeshurun, Reuven] Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. RP Hovers, E (reprint author), Hebrew Univ Jerusalem, Inst Archaeol, Jerusalem, Israel. EM hovers@mscc.huji.ac.il OI Hovers, Erella/0000-0002-7855-6573 NR 97 TC 5 Z9 5 U1 0 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1040-6182 EI 1873-4553 J9 QUATERN INT JI Quat. Int. PD MAY 8 PY 2014 VL 331 BP 216 EP 233 DI 10.1016/j.quaint.2014.01.028 PG 18 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA AG9NK UT WOS:000335746000017 ER PT J AU Dunne, JA Labandeira, CC Williams, RJ AF Dunne, Jennifer A. Labandeira, Conrad C. Williams, Richard J. TI Highly resolved early Eocene food webs show development of modern trophic structure after the end-Cretaceous extinction SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE food webs; Messel Shale; early Eocene; network structure; niche model; trophic organization ID RED QUEEN; TERRESTRIAL COMMUNITIES; ECOLOGICAL NETWORKS; MASS EXTINCTION; CLIMATE; RECORD; DIVERSIFICATION; PARASITOIDS; ROBUSTNESS; RICHNESS AB Generalities of food web structure have been identified for extant ecosystems. However, the trophic organization of ancient ecosystems is unresolved, as prior studies of fossil webs have been limited by low-resolution, highuncertainty data. We compiled highly resolved, well-documented feeding interaction data for 700 taxa from the 48 million-year-old latest early Eocene Messel Shale, which contains a species assemblage that developed after an interval of protracted environmental and biotal change during and following the endCretaceous extinction. We compared the network structure of Messel lake and forest foodwebs to extantwebs using analyses that account for scaledependence of structure with diversity and complexity. The Messel lake web, with 94 taxa, displays unambiguous similarities in structure to extant webs. While the Messel forest web, with 630 taxa, displays differences compared to extant webs, they appear to result from high diversity and resolution of insect-plant interactions, rather than substantive differences in structure. The evidence presented here suggests that modern trophic organization developed along with the modern Messel biota during an 18 Myr interval of dramatic post-extinction change. Our study also has methodological implications, as the Messel forest web analysis highlights limitations of current food web data and models. C1 [Dunne, Jennifer A.] Santa Fe Inst, Santa Fe, NM 87501 USA. [Dunne, Jennifer A.] Pacific Ecoinformat & Computat Ecol Lab, Berkeley, CA 94703 USA. [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA. [Williams, Richard J.] Microsoft Res, Cambridge CB3 0FB, England. RP Dunne, JA (reprint author), Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. EM jdunne@santafe.edu FU Santa Fe Institute; Thaw Trust; Packard Foundation; Intel Research; NSF [DBI-0234980, DBI-0850373] FX This work was supported by the Santa Fe Institute, Thaw Trust, Packard Foundation, Intel Research, NSF DBI-0234980 to J.A.D. and NSF DBI-0850373 to J.A.D. and R.J.W. The funders had no role in study design, data collection and analysis, decision to publish or preparation of the manuscript. NR 67 TC 10 Z9 10 U1 3 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 MAY 7 PY 2014 VL 281 IS 1782 AR 20133280 DI 10.1098/rspb.2013.3280 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AF0NA UT WOS:000334410100019 PM 24648225 ER PT J AU O'Dea, A Shaffer, ML Doughty, DR Wake, TA Rodriguez, FA AF O'Dea, Aaron Shaffer, Marian Lynne Doughty, Douglas R. Wake, Thomas A. Rodriguez, Felix A. TI Evidence of size-selective evolution in the fighting conch from prehistoric subsistence harvesting SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Strombus pugilis; Caribbean; pre-Columbian; fossil; artisanal harvesting; fisheries-induced evolution ID BOCAS DEL TORO; BASE-LINE; CARIBBEAN FISHERIES; STROMBUS-GIGAS; SOUTH-AFRICA; CORAL-REEFS; STONE-AGE; PANAMA; EXPLOITATION; SEA AB Intensive size-selective harvesting can drive evolution of sexual maturity at smaller body size. Conversely, prehistoric, low-intensity subsistence harvesting is not considered an effective agent of size-selective evolution. Uniting archaeological, palaeontological and contemporary material, we show that size at sexual maturity in the edible conch Strombus pugilis declined significantly from pre-human (approx. 7 ka) to prehistoric times (approx. 1 ka) and again to the present day. Size at maturity also fell from early-to late-prehistoric periods, synchronous with an increase in harvesting intensity as other resources became depleted. A consequence of declining size at maturity is that early prehistoric harvesters would have received two-thirds more meat per conch than contemporary harvesters. After exploring the potential effects of selection biases, demographic shifts, environmental change and habitat alteration, these observations collectively implicate prehistoric subsistence harvesting as an agent of size-selective evolution with long-term detrimental consequences. We observe that contemporary populations that are protected from harvesting are slightly larger at maturity, suggesting that halting or even reversing thousands of years of size-selective evolution may be possible. C1 [O'Dea, Aaron; Shaffer, Marian Lynne; Rodriguez, Felix A.] Smithsonian Trop Res Inst, Balboa, Panama. [Shaffer, Marian Lynne] Univ Wisconsin, Cofrin Ctr Biodivers, Green Bay, WI 54311 USA. [Doughty, Douglas R.] Inst Trop Ecol & Conservat, Gainesville, FL 32605 USA. [Wake, Thomas A.] Univ Calif Los Angeles, Cotsen Inst Archaeol, Zooarchaeol Lab, Los Angeles, CA 90095 USA. RP O'Dea, A (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Panama. EM odeaa@si.edu FU National System of Investigators (SNI) of the National Research of the National Secretariat for Science, Technology and Innovation of Panama (SENACYT); SENACYT; Academic Program of the Smithsonian Tropical Research Institute FX This research was supported by the National System of Investigators (SNI) of the National Research of the National Secretariat for Science, Technology and Innovation of Panama (SENACYT) to A.O. SENACYT also provided financial support to T. A. W. and T. Mendizabal for excavation and analysis of material. The Academic Program of the Smithsonian Tropical Research Institute awarded a fellowship to M.L.S. NR 58 TC 5 Z9 5 U1 4 U2 45 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 7 PY 2014 VL 281 IS 1782 AR 20140159 DI 10.1098/rspb.2014.0159 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AF0NA UT WOS:000334410100028 PM 24648229 ER PT J AU Lemoine, NP Burkepile, DE Parker, JD AF Lemoine, Nathan P. Burkepile, Deron E. Parker, John D. TI Variable effects of temperature on insect herbivory SO PEERJ LA English DT Article DE Climate change; Hierarchical model; Thermal response curve; Lepidoptera; Coleoptera; Hymenoptera ID MULTIPLE ALLELOCHEMICALS; WARMING STRENGTHENS; THERMAL REGIMES; CLIMATE-CHANGE; ELEVATED CO2; PLANT; GROWTH; CONSEQUENCES; COMMUNITIES; PERFORMANCE AB Rising temperatures can influence the top-down control of plant biomass by increasing herbivore metabolic demands. Unfortunately, we know relatively little about the effects of temperature on herbivory rates for most insect herbivores in a given community. Evolutionary history, adaptation to local environments, and dietary factors may lead to variable thermal response curves across different species. Here we characterized the effect of temperature on herbivory rates for 21 herbivore-plant pairs, encompassing 14 herbivore and 12 plant species. We show that overall consumption rates increase with temperature between 20 and 30 degrees C but do not increase further with increasing temperature. However, there is substantial variation in thermal responses among individual herbivore-plant pairs at the highest temperatures. Over one third of the herbivore-plant pairs showed declining consumption rates at high temperatures, while an approximately equal number showed increasing consumption rates. Such variation existed even within herbivore species, as some species exhibited idiosyncratic thermal response curves on different host plants. Thus, rising temperatures, particularly with respect to climate change, may have highly variable effects on plant-herbivore interactions and, ultimately, top-down control of plant biomass. C1 [Lemoine, Nathan P.; Burkepile, Deron E.] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. [Parker, John D.] Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA. RP Lemoine, NP (reprint author), Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. EM lemoine.nathan@gmail.com RI Parker, John/F-9761-2010 OI Parker, John/0000-0002-3632-7625 FU FIU FX Work was supported by a Presidential Fellowship from FIU (NL). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 39 TC 12 Z9 12 U1 8 U2 46 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 6 PY 2014 VL 2 AR e376 DI 10.7717/peerj.376 PG 18 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AY5JB UT WOS:000347607300002 PM 24860701 ER PT J AU Blume, D AF Blume, D. TI Three-body bound states in a harmonic waveguide with cylindrical symmetry SO PHYSICAL REVIEW A LA English DT Article ID RESONANTLY-INTERACTING PARTICLES; FEW-BODY SYSTEMS; ULTRACOLD GASES; SCATTERING AB Highly elongated quasi-one-dimensional cold-atom samples have been studied extensively over the past years experimentally and theoretically. This work determines the energy spectrum of two identical fermions and a third distinguishable particle as functions of the mass ratio kappa and the free-space s-wave scattering length a(3D) between the identical fermions and the distinguishable third particle in a cylindrically symmetric waveguide whose symmetry axis is chosen to be along the z axis. We focus on the regime where the mass of the identical fermions is equal to or larger than that of the third distinguishable particle. Our theoretical framework accounts explicitly for the motion along the transverse confinement direction. In the regime where excitations in the transverse direction are absent (i. e., for states with projection quantum number M-rel = 0), we determine the binding energies for states with odd parity in z. These full three-dimensional energies deviate significantly from those obtained within a strictly one-dimensional framework when the s-wave scattering length is of the order of or smaller than the oscillator length in the confinement direction. If transverse excitations are present, we predict the existence of a class of universal three-body bound states with | M-rel| = 1 and positive parity in z. These bound states arise on the positive s-wave scattering length side if the mass ratio kappa is sufficiently large. Implications of our results for ongoing cold-atom experiments are discussed. C1 [Blume, D.] Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. [Blume, D.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Blume, D (reprint author), Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. FU NSF [PHY-1205443]; National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University; Smithsonian Astrophysical Observatory FX D. B. is grateful to J. Shertzer for extensive discussions involving the symmetry of the Hamiltonian and for preliminary calculations of effective hyperradial potential curves using a four-dimensional finite-element analysis. D. B. also thanks D. Rakshit and S. E. Gharashi for helpful discussions, and acknowledges support by the NSF through Grant No. PHY-1205443. This work was additionally supported by the National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory. NR 40 TC 1 Z9 1 U1 2 U2 9 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD MAY 5 PY 2014 VL 89 IS 5 AR 053603 DI 10.1103/PhysRevA.89.053603 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AH4LY UT WOS:000336100500006 ER PT J AU Carvalho, MR Wilf, P Barrios, H Windsor, DM Currano, ED Labandeira, CC Jaramillo, CA AF Carvalho, Monica R. Wilf, Peter Barrios, Hector Windsor, Donald M. Currano, Ellen D. Labandeira, Conrad C. Jaramillo, Carlos A. TI Insect Leaf-Chewing Damage Tracks Herbivore Richness in Modern and Ancient Forests SO PLOS ONE LA English DT Article ID LAGUNA DEL HUNCO; TROPICAL FOREST; FEEDING DAMAGE; CLIMATE-CHANGE; MIDDLE EOCENE; NORTH-AMERICA; FOSSIL RECORD; RAIN-FOREST; PLANT; ASSOCIATIONS AB The fossil record demonstrates that past climate changes and extinctions significantly affected the diversity of insect leaf-feeding damage, implying that the richness of damage types reflects that of the unsampled damage makers, and that the two are correlated through time. However, this relationship has not been quantified for living leaf-chewing insects, whose richness and mouthpart convergence have obscured their value for understanding past and present herbivore diversity. We hypothesized that the correlation of leaf-chewing damage types (DTs) and damage maker richness is directly observable in living forests. Using canopy access cranes at two lowland tropical rainforest sites in Panama to survey 24 host-plant species, we found significant correlations between the numbers of leaf chewing insect species collected and the numbers of DTs observed to be made by the same species in feeding experiments, strongly supporting our hypothesis. Damage type richness was largely driven by insect species that make multiple DTs. Also, the rank-order abundances of DTs recorded at the Panama sites and across a set of latest Cretaceous to middle Eocene fossil floras were highly correlated, indicating remarkable consistency of feeding-mode distributions through time. Most fossil and modern host-plant pairs displayed high similarity indices for their leaf-chewing DTs, but informative differences and trends in fossil damage composition became apparent when endophytic damage was included. Our results greatly expand the potential of insect-mediated leaf damage for interpreting insect herbivore richness and compositional heterogeneity from fossil floras and, equally promisingly, in living forests. C1 [Carvalho, Monica R.; Wilf, Peter] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Carvalho, Monica R.] Cornell Univ, Dept Plant Biol, Ithaca, NY USA. [Barrios, Hector] Univ Panama, Programa Maestri Entomol, Panama City, Panama. [Windsor, Donald M.; Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Currano, Ellen D.] Miami Univ, Dept Geol & Environm Earth Sci, Oxford, OH 45056 USA. [Labandeira, Conrad C.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Univ Maryland, BEES Program, College Pk, MD 20742 USA. RP Carvalho, MR (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM mjr383@cornell.edu FU David and Lucile Packard Fellowship; NSF [DEB-0919071] FX This study was funded by a David and Lucile Packard Fellowship, with additional support from NSF DEB-0919071 (PW). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 42 TC 14 Z9 14 U1 1 U2 18 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 2 PY 2014 VL 9 IS 5 AR e94950 DI 10.1371/journal.pone.0094950 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AI1ZS UT WOS:000336655700021 PM 24788720 ER PT J AU Paxton, KL Cohen, EB Paxton, EH Nemeth, Z Moore, FR AF Paxton, Kristina L. Cohen, Emily B. Paxton, Eben H. Nemeth, Zoltan Moore, Frank R. TI El Nino-Southern Oscillation Is Linked to Decreased Energetic Condition in Long-Distance Migrants SO PLOS ONE LA English DT Article ID NORTH-ATLANTIC OSCILLATION; MIGRATORY BIRD; SPRING MIGRATION; REPRODUCTIVE SUCCESS; SETOPHAGA-RUTICILLA; BREEDING GROUNDS; REGIONAL-SCALE; ARRIVAL DATE; SONGBIRD; CLIMATE AB Predicting how migratory animals respond to changing climatic conditions requires knowledge of how climatic events affect each phase of the annual cycle and how those effects carry-over to subsequent phases. We utilized a 17-year migration dataset to examine how El Nino-Southern Oscillation climatic events in geographically different regions of the Western hemisphere carry-over to impact the stopover biology of several intercontinental migratory bird species. We found that migratory birds that over-wintered in South America experienced significantly drier environments during El Nino years, as reflected by reduced Normalized Difference Vegetation Index (NDVI) values, and arrived at stopover sites in reduced energetic condition during spring migration. During El Nino years migrants were also more likely to stopover immediately along the northern Gulf coast of the southeastern U. S. after crossing the Gulf of Mexico in small suboptimal forest patches where food resources are lower and migrant density often greater than larger more contiguous forests further inland. In contrast, NDVI values did not differ between El Nino and La Nina years in Caribbean-Central America, and we found no difference in energetic condition or use of coastal habitats for migrants en route from Caribbean-Central America wintering areas. Birds over-wintering in both regions had consistent median arrival dates along the northern Gulf coast, suggesting that there is a strong drive for birds to maintain their time program regardless of their overall condition. We provide strong evidence that not only is the stopover biology of migratory landbirds influenced by events during the previous phase of their life-cycle, but where migratory birds over-winter determines how vulnerable they are to global climatic cycles. Increased frequency and intensity of ENSO events over the coming decades, as predicted by climatic models, may disproportionately influence long-distance migrants over-wintering in South America. C1 [Paxton, Kristina L.; Moore, Frank R.] Univ So Mississippi, Dept Biol Sci, Hattiesburg, MS 39406 USA. [Cohen, Emily B.] Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC USA. [Paxton, Eben H.] US Geol Survey, Pacific Isl Ecosyst Res Ctr, Honolulu, HI USA. [Nemeth, Zoltan] Univ Calif Davis, Dept Neurobiol Physiol & Behav, Davis, CA 95616 USA. RP Paxton, KL (reprint author), Univ So Mississippi, Dept Biol Sci, Hattiesburg, MS 39406 USA. EM kpaxton@hawaii.edu OI Paxton, Eben/0000-0001-5578-7689 FU National Science Foundation [DEB 0554754, IBN 0078189, IOS 844703] FX Funding for this research was provided by National Science Foundation grants to FRM (DEB 0554754, IBN 0078189, IOS 844703). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 70 TC 6 Z9 6 U1 6 U2 49 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 2 PY 2014 VL 9 IS 5 AR e95383 DI 10.1371/journal.pone.0095383 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AI1ZS UT WOS:000336655700028 PM 24788978 ER PT J AU Fisher, MM Reddy, KR Turner, BL Keenan, LW AF Fisher, Millard M. Reddy, K. Ramesh Turner, Benjamin L. Keenan, Lawrence W. TI Millennial-Scale Phosphorus Transformations during Diagenesis in a Subtropical Peatland SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL LA English DT Article ID P-31 NMR-SPECTROSCOPY; MAGNETIC-RESONANCE-SPECTROSCOPY; ORGANIC PHOSPHORUS; FLORIDA EVERGLADES; LAKE-SEDIMENTS; NUTRIENT ACCUMULATION; WETLAND SOILS; INOSITOL PHOSPHATES; TROPHIC STATE; RATES AB The record of ecosystem history preserved in wetland soils is often used to set ecosystem restoration targets but is complicated by diagenetic changes. We examined changes in the forms of soil P in a 4000-yr-old subtropical peat deposit in Florida using sequential fractionation and solution P-31 nuclear magnetic resonance spectroscopy. By combining information on changes in soil P composition with C-14 dates, our aim was to estimate the long-term rate of P storage in a subtropical peatland. Diagenesis caused a decline in labile compounds and an accumulation of recalcitrant compounds. For example, stable P forms determined by sequential fractionation increased from 23% of total P in surface peat to 48 to 73% of total P at a depth of 1.5 m. In contrast, fulvic-acid bound P declined with increasing depth at a rate of 37 to 65 mg P kg(-1) yr(-1). Solution 31P nuclear magnetic resonance (NMR) spectroscopy showed that the majority of the extractable organic P occurred as phosphodiesters, which declined markedly with depth, indicating recycling of labile organic P in surface sediments. Carbon-14 dating at two soil coring stations indicated a long-term P accretion rate of 1.71 mg P m(-2) yr(-1) at both stations, a rate approximately 20-fold lower than previous estimates of long-term P accretion in this wetland. Recently deposited material undergoes rapid biogeochemical transformations that complicate associations between soil properties and extrinsic factors such as nutrient loading. We conclude that studies of P accretion based only on approximately <200-yr-old peat will tend to overestimate long-term sequestration rate of the ecosystem. C1 [Fisher, Millard M.; Keenan, Lawrence W.] St Johns River Water Management Dist, Palatka, FL 32178 USA. [Reddy, K. Ramesh] Univ Florida, Dept Soil & Water Sci, Gainesville, FL 32611 USA. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Fisher, MM (reprint author), St Johns River Water Management Dist, 4049 Reid St, Palatka, FL 32178 USA. EM millard3@gmail.com RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU St. Johns River Water Management District, Palatka, FL FX We thank Ms. Yu Wang for laboratory support throughout this project and Mr. Ken Snyder for assistance with field work. We also thank two anonymous reviewers, whose helpful comments greatly improved the clarity and focus of this manuscript. This work was supported through funding from the St. Johns River Water Management District, Palatka, FL. NR 50 TC 0 Z9 0 U1 0 U2 10 PU SOIL SCI SOC AMER PI MADISON PA 677 SOUTH SEGOE ROAD, MADISON, WI 53711 USA SN 0361-5995 EI 1435-0661 J9 SOIL SCI SOC AM J JI Soil Sci. Soc. Am. J. PD MAY-JUN PY 2014 VL 78 IS 3 BP 1087 EP 1096 DI 10.2136/sssaj2013.08.0364 PG 10 WC Soil Science SC Agriculture GA AO7WU UT WOS:000341564100038 ER PT J AU Thomson, OA Cavosie, AJ Moser, DE Barker, I Radovan, HA French, BM AF Thomson, Olivia A. Cavosie, Aaron J. Moser, Desmond E. Barker, Ivan Radovan, Henri A. French, Bevan M. TI Preservation of detrital shocked minerals derived from the 1.85 Ga Sudbury impact structure in modern alluvium and Holocene glacial deposits SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Article ID PLANAR DEFORMATION FEATURES; ARCHEAN SPHERULE LAYER; SOUTH-AFRICA; VREDEFORT DOME; U-PB; METAMORPHOSED ZIRCON; STRUCTURE ONTARIO; METEORITE IMPACT; IGNEOUS COMPLEX; MAGMATIC ZIRCON AB Detrital shocked minerals can provide valuable residual records of eroded impact structures. Recent studies have reported shocked minerals in modern alluvium in a subtropical climate from the deeply eroded 2.02 Ga Vredefort Dome impact basin in South Africa. To evaluate the detrital shocked mineral record at a large impact structure in a temperate setting with a Holocene glacial erosional history, we investigated similar to 4000 detrital zircons and similar to 20,000 quartz grains at the less-eroded 1.85 Ga Sudbury Basin in Ontario, Canada, for the presence of shocked sand grains. Modern alluvium from rivers within and outside the basin, and Holocene glaciofluvial sands (eskers and outwash deltas) across the basin were investigated for shocked minerals. Shocked zircon and/or quartz were found in all modern rivers and most Holocene glacial deposits within, but not outside, the basin. Petrography and scanning electron microscopy (SEM; back scattered electron [BSE]; cathodoluminescence [CL]) imaging and analysis (energy-dispersive X-ray spectroscopy [EDS], electron backscatter diffraction [EBSD]) were used to document shock microstructures. Of the total detrital zircons surveyed, similar to 3% (118/3978) were identified as shocked; Holocene samples contained higher average percentages of shocked zircon (63/1361, or 4.6%, with a high of 29%) compared to modern alluvium (55/2617, or 2.1%, with a high of 6%). EBSD analysis revealed a range of shock microstructures, including planar fractures, deformation microtwins, and crystal plastic deformation. At Sudbury, detrital shocked quartz is rare compared to zircon; only 15 grains (similar to 0.08%) were identified, all with decorated planar deformation features (PDFs). These results demonstrate that a detrital shocked mineral record exists at a large impact basin that is in a "youthful" stage of erosion, despite its age. In addition to modern alluvium, our results also identify glaciofluvial eskers and deltas as reservoirs for detrital shocked minerals; glacial episodes thus enhance the dispersal and preservation of shocked detritus in sedimentary systems. Despite physical differences, the observation that the two largest Precambrian impact basins continue to contribute detrital shocked minerals 2 b.y. after impact suggests that a shocked mineral record of impacts on early Earth should reside in Precambrian siliciclastic rocks. C1 [Thomson, Olivia A.; Cavosie, Aaron J.] Univ Puerto Rico, Dept Geol, Mayaguez, PR 00681 USA. [Cavosie, Aaron J.] Univ Wisconsin, Dept Geosci, WiscSIMS, Madison, WI 53706 USA. [Moser, Desmond E.; Barker, Ivan] Univ Western Ontario, Dept Earth Sci, London, ON N6A 5B7, Canada. [Radovan, Henri A.] Univ Puerto Rico, Dept Phys, Mayaguez, PR 00681 USA. [French, Bevan M.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP Thomson, OA (reprint author), Univ Puerto Rico, Dept Geol, POB 9000, Mayaguez, PR 00681 USA. EM olivia.thomson@upr.edu OI Cavosie, Aaron/0000-0001-6819-6810 FU National Science Foundation [EAR-0838300]; NASA Astrobiology Institute; Simon Kattenhorn FX Thomson thanks the Planetary Geology Division of the Geological Society of America for receiving the 2011 Eugene M. Shoemaker impact cratering award. Cavosie graciously acknowledges support from the National Science Foundation (EAR-0838300) and the NASA Astrobiology Institute. Lisa Cupelli, Chris Mattson, and Timmons Erickson assisted with sample collection at the Sudbury impact structure. We thank Jose Almodovar and Dayanidi Ortiz for providing access to laboratory facilities. The staff of the Ontario Geological Survey office in Sudbury is thanked for providing publication resources. Thanks also go to Simon Kattenhorn and Raiza Quintero for their support. We thank Associate Editor Uwe Reimold and two anonymous reviewers for insightful and productive comments. NR 90 TC 11 Z9 11 U1 2 U2 19 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0016-7606 EI 1943-2674 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD MAY-JUN PY 2014 VL 126 IS 5-6 BP 720 EP 737 DI 10.1130/B30958.1 PG 18 WC Geosciences, Multidisciplinary SC Geology GA AO2YF UT WOS:000341193400007 ER PT J AU Osazuwa-Peters, OL Wright, SJ Zanne, AE AF Osazuwa-Peters, Oyomoare L. Wright, S. Joseph Zanne, Amy E. TI RADIAL VARIATION IN WOOD SPECIFIC GRAVITY OF TROPICAL TREE SPECIES DIFFERING IN GROWTH-MORTALITY STRATEGIES SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE aboveground biomass; growth-mortality trade-off; Panama; wood density ID MECHANICAL-PROPERTIES; FUNCTIONAL TRAITS; DENSITY; FOREST; AGE; CONSEQUENCES; RECRUITMENT; ALLOMETRY; GRADIENTS; AMAZONIA AB Premise of the study: Wood specific gravity (WSG) mediates an interspecific trade-off between growth and mortality and is a key measure for estimating carbon stocks. Most studies use species mean values to represent WSG, despite variation at different levels of biological organization. We examined sources of variation in WSG across four nested scales (segments within cores, cores within trees, trees within species, and species), compared the pattern of radial variation in WSG among species differing in growth strategies, and investigated the effect of WSG radial variation on aboveground biomass estimates. Methods: We took two perpendicular cores from six individuals each of 20 tropical tree species representing a broad range of mean WSGs and growth-mortality strategies in a lowland tropical moist forest in Panama. Cores were divided into 1-cm segments, and WSG was determined for each segment. Key results: The bulk of the total variance in WSG was dominated by interspecies variation (88%), whereas variation due to measurement error, segments within cores, and cores within trees (8%) was minimal. Radial variation in WSG, defined as change in WSG with increasing distance from the pith, was significant in 17 of the 20 species and included significant monotonic increases in 6 species and nonmonotonic patterns in 11 species. Radial variation in WSG resulted in a small but significant bias in aboveground biomass estimates. Conclusions: Radial variation in WSG is related to a species' growth strategy and, though minimal compared with interspecific variation in WSG, can cause a downward bias when not incorporated into aboveground biomass estimates. C1 [Osazuwa-Peters, Oyomoare L.] Univ Missouri, Dept Biol, St Louis, MO 63121 USA. [Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Panama. [Zanne, Amy E.] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Zanne, Amy E.] Missouri Bot Garden, Ctr Conservat & Sustainable Dev, St Louis, MO 63166 USA. RP Osazuwa-Peters, OL (reprint author), Univ Missouri, Dept Biol, One Univ Blvd, St Louis, MO 63121 USA. EM oletkd@mail.umsl.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU Whitney Harris World Ecology Center FX The authors thank Whitney Harris World Ecology Center for providing research funds; I. Jimenez for contributions to the statistical analysis; H. Muller-Landau for providing the integral solution for area-weighted mean estimates of wood specific gravity; N. Osazuwa-Peters, S. Bernal, O. Hernandez, and R. Gonzalez for providing invaluable field and technical assistance; J. Aibueku for financial support; and D. Kenfack for logistical support. M. C. Wiemann and three anonymous reviewers provided valuable comments on the manuscript. NR 47 TC 3 Z9 3 U1 1 U2 14 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 MAY PY 2014 VL 101 IS 5 BP 803 EP 811 DI 10.3732/ajb.1400040 PG 9 WC Plant Sciences SC Plant Sciences GA AN2YY UT WOS:000340453200007 PM 24793318 ER PT J AU Williamson, CE Brentrup, JA Zhang, J Renwick, WH Hargreaves, BR Knoll, LB Overholt, EP Rose, KC AF Williamson, Craig E. Brentrup, Jennifer A. Zhang, Jing Renwick, William H. Hargreaves, Bruce R. Knoll, Lesley B. Overholt, Erin P. Rose, Kevin C. TI Lakes as sensors in the landscape: Optical metrics as scalable sentinel responses to climate change SO LIMNOLOGY AND OCEANOGRAPHY LA English DT Article ID DISSOLVED ORGANIC-CARBON; ABSORPTION SPECTRAL SLOPES; ULTRAVIOLET-RADIATION; BOREAL LAKES; TEMPERATE LAKES; SOLAR-RADIATION; WATER CLARITY; GLOBAL CHANGE; MATTER; ECOSYSTEM AB As the lowest point in the surrounding landscape, lakes act as sensors in the landscape to provide insights into the response of both terrestrial and aquatic ecosystems to climate change. Here a novel suite of climate forcing optical indices (CFOI) from lakes across North America is found to respond to changes in air temperature, precipitation, and solar radiation at timescales ranging from a single storm event to seasonal changes to longer-term interdecadal trends with regression r(2) values ranging from 0.73 to 0.89. These indices are based on two optical metrics of dissolved organic carbon (DOC) quality: DOC specific absorbance (a*(320)) and spectral slope (S275-295), where the ratio a*(320) to S275-295 gives a composite climate forcing index. These indices of DOC quality are more responsive to climate forcing than is DOC concentration. A similar relationship between the component indices a*(320) and S275-295 is observed across a wide range of lake types. A conceptual model is used to examine the similarities and differences in DOC-related mechanisms and ecological consequences due to increased temperature vs. precipitation. While both warmer and wetter conditions increase thermal stratification, these two types of climate forcing will have opposite effects on water transparency as well as many ecological consequences, including oxygen depletion, the balance between autotrophy and heterotrophy, and depth distributions of phytoplankton and zooplankton. C1 [Williamson, Craig E.; Brentrup, Jennifer A.; Overholt, Erin P.] Miami Univ, Dept Biol, Oxford, OH 45056 USA. [Zhang, Jing] Miami Univ, Dept Stat, Oxford, OH 45056 USA. [Renwick, William H.] Miami Univ, Dept Geog, Oxford, OH 45056 USA. [Hargreaves, Bruce R.] Lehigh Univ, Dept Earth & Environm Sci, Bethlehem, PA 18015 USA. [Knoll, Lesley B.] Lacawac Sanctuary, Lake Ariel, PA USA. [Rose, Kevin C.] Smithsonian Environm Res Ctr, Edgewater, MD USA. RP Williamson, CE (reprint author), Miami Univ, Dept Biol, Oxford, OH 45056 USA. EM craig.williamson@miamiOH.edu FU National Science Foundation grants from the Division of Environmental Biology (DEB) [0734277]; DEB Integrated Research Challenges in Environmental Biology [0552283]; Division of Graduate Education [0903560] FX We thank Wiebke Boeing, Janet Fischer, Evelyn Gaiser, Weston Nowlin, John Melack, Mark Olson, Jasmine Saros, and Hilary Swain for help and logistics in collecting water samples that contributed to the 35 lake data set and the late Robert E. Moeller for contributing to earlier discussions regarding indices to look at the shifting balance between hydraulic flushing and photobleaching. Comments from two anonymous reviewers improved an earlier version of this manuscript. We also thank the GLEON for providing forums at their meetings for presenting and discussing some of the ideas presented here with the broader limnological community as well as for travel support for some of the coauthors who attended these meetings. This work was supported in part by National Science Foundation grants from the Division of Environmental Biology (DEB)-0734277, DEB Integrated Research Challenges in Environmental Biology-0552283, and the Division of Graduate Education-0903560. NR 62 TC 20 Z9 20 U1 5 U2 51 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-3590 EI 1939-5590 J9 LIMNOL OCEANOGR JI Limnol. Oceanogr. PD MAY PY 2014 VL 59 IS 3 BP 840 EP 850 DI 10.4319/lo.2014.59.3.0840 PG 11 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA AM5MQ UT WOS:000339904300016 ER PT J AU Anderson, GE Gaensler, BM Kaplan, DL Slane, PO Muno, MP Posselt, B Hong, J Murray, SS Steeghs, DTH Brogan, CL Drake, JJ Farrell, SA Benjamin, RA Chakrabarty, D Drew, JE Finley, JP Grindlay, JE Lazio, TJW Lee, JC Mauerhan, JC van Kerkwijk, MH AF Anderson, Gemma E. Gaensler, B. M. Kaplan, David L. Slane, Patrick O. Muno, Michael P. Posselt, Bettina Hong, Jaesub Murray, Stephen S. Steeghs, Danny T. H. Brogan, Crystal L. Drake, Jeremy J. Farrell, Sean A. Benjamin, Robert A. Chakrabarty, Deepto Drew, Janet E. Finley, John P. Grindlay, Jonathan E. Lazio, T. Joseph W. Lee, Julia C. Mauerhan, Jon C. van Kerkwijk, Marten H. TI CHASING THE IDENTIFICATION OF ASCA GALACTIC OBJECTS (ChIcAGO): AN X-RAY SURVEY OF UNIDENTIFIED SOURCES IN THE GALACTIC PLANE. I. SOURCE SAMPLE AND INITIAL RESULTS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE surveys; X-rays: binaries; X-rays: galaxies; X-rays: general; X-rays: stars ID XMM-NEWTON OBSERVATIONS; H-II-REGIONS; PULSAR WIND NEBULA; ALL-SKY SURVEY; SUPERNOVA REMNANT G349.7+0.2; MASSIVE STAR-FORMATION; MAIN-SEQUENCE STARS; M IR-EXCESS; SOURCE CATALOG; INFRARED COUNTERPART AB We present the Chasing the Identification of ASCA Galactic Objects (ChIcAGO) survey, which is designed to identify the unknown X-ray sources discovered during the ASCA Galactic Plane Survey (AGPS). Little is known about most of the AGPS sources, especially those that emit primarily in hard X-rays (2-10 keV) within the F-x similar to 10(-13) to 10(-11) erg cm(-2) s(-1) X-ray flux range. In ChIcAGO, the subarcsecond localization capabilities of Chandra have been combined with a detailed multiwavelength follow-up program, with the ultimate goal of classifying the >100 unidentified sources in the AGPS. Overall to date, 93 unidentified AGPS sources have been observed with Chandra as part of the ChIcAGO survey. A total of 253 X-ray point sources have been detected in these Chandra observations within 3' of the original ASCA positions. We have identified infrared and optical counterparts to the majority of these sources, using both new observations and catalogs from existing Galactic plane surveys. X-ray and infrared population statistics for the X-ray point sources detected in the Chandra observations reveal that the primary populations of Galactic plane X-ray sources that emit in the F-x similar to 10(-13) to 10(-11) erg cm(-2) s(-1) flux range are active stellar coronae, massive stars with strong stellar winds that are possibly in colliding wind binaries, X-ray binaries, and magnetars. There is also another primary population that is still unidentified but, on the basis of its X-ray and infrared properties, likely comprises partly Galactic sources and partly active galactic nuclei. C1 [Anderson, Gemma E.; Gaensler, B. M.; Farrell, Sean A.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Kaplan, David L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Slane, Patrick O.; Hong, Jaesub; Drake, Jeremy J.; Grindlay, Jonathan E.; Lee, Julia C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Muno, Michael P.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Posselt, Bettina] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Steeghs, Danny T. H.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Brogan, Crystal L.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Benjamin, Robert A.] Univ Wisconsin, Dept Phys, Whitewater, WI 53190 USA. [Chakrabarty, Deepto] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Chakrabarty, Deepto] MIT, Dept Phys, Cambridge, MA 02139 USA. [Drew, Janet E.] Univ Hertfordshire, STRI, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Finley, John P.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Lazio, T. Joseph W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mauerhan, Jon C.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [van Kerkwijk, Marten H.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Anderson, GE (reprint author), Univ Oxford, Dept Phys, Denys Wilkinson Bldg, Oxford OX1 3RH, England. EM gemma.anderson@astro.ox.ac.uk RI Lee, Julia/G-2381-2015; OI Lee, Julia/0000-0002-7336-3588; Anderson, Gemma/0000-0001-6544-8007; Posselt, Bettina/0000-0003-2317-9747; Gaensler, Bryan/0000-0002-3382-9558; Drew, Janet/0000-0003-1192-7082; Kaplan, David/0000-0001-6295-2881 FU Australian Postgraduate Award; Australian Laureate Fellowship through ARC [FL100100114]; NASA [NAS8-03060, NAS8-39073, GO90155X]; STFC Advanced Fellowship; Commonwealth of Australia under the International Science Linkages program; Commonwealth of Australia; Australian Research Council; Science Foundation for Physics within the University of Sydney; NFS FX G.E.A. acknowledges the support of an Australian Postgraduate Award. B.M.G. acknowledges the support of an Australian Laureate Fellowship through ARC grant FL100100114. P.O.S. acknowledges partial support from NASA contract NAS8-03060. D.T.H.S. acknowledges a STFC Advanced Fellowship. J.J.D. was supported by NASA contract NAS8-39073 to the Chandra X-ray Center (CXC). Support for this work was also provided by NASA through Chandra award number GO90155X issued by the CXC, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA. The access to major research facilities program is supported by the Commonwealth of Australia under the International Science Linkages program. This research makes use of data obtained with the Chandra X-ray Observatory and software provided by the CXC in the application packages CIAO. The ATCA is part of the Australia Telescope, funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The MOST is operated with the support of the Australian Research Council and the Science Foundation for Physics within the University of Sydney. Observing time on the 6.5 m Baade Magellan Telescope, located at Las Campanas Observatory, was allocated through the Harvard-Smithsonian Center for Astrophysics and the Massachusetts Institute of Technology. 2MASS is a joint project of the University of Massachusetts and the IPAC/Caltech, funded by NASA and the NFS. GLIMPSE survey data are part of the Spitzer Legacy Program. The Spitzer Space Telescope is operated by JPL/Caltech under a contract with NASA. This research has made use of NASA's Astrophysics Data System. NR 189 TC 2 Z9 2 U1 0 U2 4 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 2014 VL 212 IS 1 DI 10.1088/0067-0049/212/1/13 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL6HG UT WOS:000339232600013 ER PT J AU Ashby, MLN Stanford, SA Brodwin, M Gonzalez, AH Martinez-Manso, J Bartlett, JG Benson, BA Bleem, LE Crawford, TM Dey, A Dressler, A Eisenhardt, PRM Galametz, A Jannuzi, BT Marrone, DP Mei, S Muzzin, A Pacaud, F Pierre, M Stern, D Vieira, JD AF Ashby, M. L. N. Stanford, S. A. Brodwin, M. Gonzalez, A. H. Martinez-Manso, J. Bartlett, J. G. Benson, B. A. Bleem, L. E. Crawford, T. M. Dey, A. Dressler, A. Eisenhardt, P. R. M. Galametz, A. Jannuzi, B. T. Marrone, D. P. Mei, S. Muzzin, A. Pacaud, F. Pierre, M. Stern, D. Vieira, J. D. TI THE SPITZER SOUTH POLE TELESCOPE DEEP FIELD: SURVEY DESIGN AND INFRARED ARRAY CAMERA CATALOGS (vol 209, 16, 2013) SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Correction C1 [Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Gonzalez, A. H.; Martinez-Manso, J.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Bartlett, J. G.] Univ Paris Diderot, CEA IRFU, Observ Paris, Sorbonne Paris Cite,CNRS IN2P3, F-75205 Paris 13, France. [Benson, B. A.; Bleem, L. E.; Crawford, T. M.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Crawford, T. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Dey, A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Dressler, A.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Eisenhardt, P. R. M.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Galametz, A.] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Jannuzi, B. T.; Marrone, D. P.] Univ Arizona, Dept Astron, Tucson, AZ 85719 USA. [Jannuzi, B. T.; Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA. [Mei, S.] Observ Paris, GEPI, Sect Meudon, F-92190 Meudon, France. [Mei, S.] Univ Paris Denis Diderot, F-75205 Paris 13, France. [Mei, S.] Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Muzzin, A.] Leiden Univ, Leiden Observ, NL-9513 RA Leiden, Netherlands. [Pacaud, F.] Argelander Inst Astron, D-53121 Bonn, Germany. [Pierre, M.] AIM IRFU DSM CEA, Serv Astrophys, F-91190 Gif Sur Yvette, France. [Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. RP Ashby, MLN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mashby@cfa.harvard.edu NR 1 TC 2 Z9 2 U1 0 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 MAY PY 2014 VL 212 IS 1 AR 16 DI 10.1088/0067-0049/212/1/16 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL6HG UT WOS:000339232600016 ER PT J AU Garcia, P Bronfman, L Nyman, LA Dame, TM Luna, A AF Garcia, P. Bronfman, L. Nyman, Lars-Ake Dame, T. M. Luna, A. TI GIANT MOLECULAR CLOUDS AND MASSIVE STAR FORMATION IN THE SOUTHERN MILKY WAY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: spiral; Galaxy: structure; ISM: clouds; stars: massive ID H-II REGIONS; 21-CENTIMETER ABSORPTION MEASUREMENTS; RECOMBINATION LINE EMISSION; DISCRETE-SOURCE SPECTRA; 1ST GALACTIC QUADRANT; INNER GALAXY; NEUTRAL HYDROGEN; SPIRAL STRUCTURE; METHANOL MASERS; OUTER GALAXY AB The Columbia University-Universidad de Chile CO Survey of the southern Milky Way is used to separate the CO(1-0) emission of the fourth Galactic quadrant within the solar circle into its dominant components, giant molecular clouds (GMCs). After the subtraction of an axisymmetric model of the CO background emission in the inner southern Galaxy, 92 GMCs are identified, and for 87 of them the twofold distance ambiguity is solved. Their total molecular mass is M(H-2) = 1.14 +/- 0.05 x 10(8) M-circle dot, accounting for around 40% of the molecular mass estimated from an axisymmetric analysis of the H2 volume density in the Galactic disk, M(H-2)(disk) = 3.03 x 10(8) M-circle dot. The large-scale spiral structure in the southern Galaxy, within the solar circle, is traced by the GMCs in our catalog; three spiral arm segments, the Centaurus, Norma, and 3 kpc expanding arm, are analyzed. After fitting a logarithmic spiral arm model to the arms, tangent directions at 310 degrees, 330 degrees, and 338 degrees, respectively, are found, consistent with previous values from the literature. A complete CS(2-1) survey toward IRAS point-like sources with far-IR colors characteristic of ultracompact H II regions is used to estimate the massive star formation rate per unit H-2 mass (MSFR) and the massive star formation efficiency (is an element of) for GMCs. The average MSFR for GMCs is 0.41 +/- 0.06 L-circle dot/M-circle dot, and for the most massive clouds in the Norma arm it is 0.58 +/- 0.09 L-circle dot/M-circle dot. Massive star formation efficiencies of GMCs are, on average, 3% of their available molecular mass. C1 [Garcia, P.; Bronfman, L.] Univ Chile, Dept Astron, Santiago, Chile. [Garcia, P.] Univ Cologne, Inst Phys, D-50937 Cologne, Germany. [Nyman, Lars-Ake] JAO, Santiago 3107, Chile. [Nyman, Lars-Ake] ESO, Santiago 3107, Chile. [Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Luna, A.] INAOE Mexico, Puebla, Mexico. RP Garcia, P (reprint author), Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile. EM pablo@ph1.uni-koeln.de; aluna@inaoep.mx RI Bronfman, Leonardo/H-9544-2013 OI Bronfman, Leonardo/0000-0002-9574-8454 FU Basal Center for Astrophysics and Associated Technologies [PFB-06] FX We gratefully acknowledge Professor Patrick Thaddeus for his seminal contributions to this work. We thank Hector Alvarez for his early help with the analysis. We remember Professor Jorge May (deceased) for his unconditional dedication to this project. P.G. and L.B. acknowledge support from Basal Center for Astrophysics and Associated Technologies PFB-06. NR 106 TC 23 Z9 23 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 MAY PY 2014 VL 212 IS 1 AR 2 DI 10.1088/0067-0049/212/1/2 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL6HG UT WOS:000339232600002 ER PT J AU Rose, KC Winslow, LA Read, JS Read, EK Solomon, CT Adrian, R Hanson, PC AF Rose, Kevin C. Winslow, Luke A. Read, Jordan S. Read, Emily K. Solomon, Christopher T. Adrian, Rita Hanson, Paul C. TI Improving the precision of lake ecosystem metabolism estimates by identifying predictors of model uncertainty SO LIMNOLOGY AND OCEANOGRAPHY-METHODS LA English DT Article ID DISSOLVED-OXYGEN; GAS-EXCHANGE; FRESH-WATER; CARBON; RADIATION AB Diel changes in dissolved oxygen are often used to estimate gross primary production (GPP) and ecosystem respiration (ER) in aquatic ecosystems. Despite the widespread use of this approach to understand ecosystem metabolism, we are only beginning to understand the degree and underlying causes of uncertainty for metabolism model parameter estimates. Here, we present a novel approach to improve the precision and accuracy of ecosystem metabolism estimates by identifying physical metrics that indicate when metabolism estimates are highly uncertain. Using datasets from seventeen instrumented GLEON (Global Lake Ecological Observatory Network) lakes, we discovered that many physical characteristics correlated with uncertainty, including PAR (photosynthetically active radiation, 400-700 nm), daily variance in Schmidt stability, and wind speed. Low PAR was a consistent predictor of high variance in GPP model parameters, but also corresponded with low ER model parameter variance. We identified a threshold (30% of clear sky PAR) below which GPP parameter variance increased rapidly and was significantly greater in nearly all lakes compared with variance on days with PAR levels above this threshold. The relationship between daily variance in Schmidt stability and GPP model parameter variance depended on trophic status, whereas daily variance in Schmidt stability was consistently positively related to ER model parameter variance. Wind speeds in the range of similar to 0.8-3 m s(-1) were consistent predictors of high variance for both GPP and ER model parameters, with greater uncertainty in eutrophic lakes. Our findings can be used to reduce ecosystem metabolism model parameter uncertainty and identify potential sources of that uncertainty. C1 [Rose, Kevin C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Winslow, Luke A.; Hanson, Paul C.] Univ Wisconsin, Ctr Limnol, Madison, WI 53706 USA. [Read, Jordan S.] US Geol Survey, Ctr Integrated Data Analyt, Middleton, WI USA. [Read, Emily K.] Cary Inst Ecosyst Studies, Millbrook, NY USA. [Solomon, Christopher T.] McGill Univ, Dept Nat Resource Sci, Quebec City, PQ, Canada. [Adrian, Rita] Leibniz Inst Freshwater Ecol & Inland Fisheries, Berlin, Germany. RP Rose, KC (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM kev.c.rose@gmail.com RI Solomon, Chris/E-6284-2014; OI Solomon, Chris/0000-0002-2850-4257; Read, Jordan/0000-0002-3888-6631 FU European Union [244121]; DFG [AD 91/13-1] FX Data collection and contributions to GLEON were generously supported by individuals and organizations including Michael Vanni and Susanna Scott (Acton); Evelyn Gaiser, Hilary Swain, and the Archbold Biological Station (Annie); Peter Staehr (Castle, Gribsoe, Hampensoe, Vedstedsoe); the North Temperate Lakes (NTL) Long Term Ecological Research (LTER) site and the NTL Microbial Observatory (Crystal Bog, Mendota, North Sparkling Bog, Sparkling, Trout, and Trout Bog); Elizabeth Ryder, Elvira de Eyto, and the Marine Institute, Co. Mayo, Ireland (Feeagh); Leibniz-Institute of Freshwater Ecology and Inland Fisheries (Muggelsee), RA was funded by the European Union Project REFRESH (Contract: 244121) and the DFG project LakeRisk (AD 91/13-1); David Hamilton and Chris McBride (Rotorua); Guangwei Zhu (Taihu); and Chih-Yu Chiu (Yuan Yang). This research emerged from discussions amongst authors at GLEON meetings and workshops. High-throughput computing resources were provided by the HTCondor project at the University of Wisconsin Madison. The authors thank Sudeep Chandra, Ulrike Scharfenberger, and the anonymous reviewers for providing thoughtful comments that improved the manuscript. NR 33 TC 8 Z9 8 U1 3 U2 22 PU AMER SOC LIMNOLOGY OCEANOGRAPHY PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA SN 1541-5856 J9 LIMNOL OCEANOGR-METH JI Limnol. Oceanogr. Meth. PD MAY PY 2014 VL 12 BP 303 EP 312 DI 10.4319/lom.2014.12.303 PG 10 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA AM0PM UT WOS:000339547700002 ER PT J AU Hayward, BW Figueira, BO Sabaa, AT Buzas, MA AF Hayward, Bruce W. Figueira, Brigida O. Sabaa, Ashwaq T. Buzas, Martin A. TI Multi-year life spans of high salt marsh agglutinated foraminifera from New Zealand SO MARINE MICROPALEONTOLOGY LA English DT Article DE High salt marsh foraminifera; Life spans; Live depths ID NATIONAL WILDLIFE REFUGE; SEA-LEVEL CHANGE; BENTHIC FORAMINIFERA; INTERTIDAL FORAMINIFERA; POPULATION-DYNAMICS; ENGLAND; ESTUARY; RECORD; ASSOCIATIONS; ASSEMBLAGES AB The depth-related density profiles of live and dead foraminiferal tests were studied in eleven cores (four with replicate cores) from above mean high water spring level in four high salt marshes in the temperate South Island of New Zealand. The species most tolerant of high elevation and low salinity in New Zealand, Trochamminita salsa, was strongly dominant in most cores but two other species, Haplophragmoides wilberti and Trochammina inflata, occurred in sufficient numbers in several cores to allow analysis. We found that the highest salt marsh foraminifera live at variable depths, sometimes in low numbers down to 30 cm at least. T. salsa appears to occur at greater depths (maximum densities between 5 and 13 cm) than H. wilberti and T. inflata (maximum densities in upper 5 cm). No strong evidence was observed for significant seasonal blooms of these agglutinated species in these highest marsh cores that are only inundated by the tide for a matter of hours a few times per year. Using the size of the total live stock in each core, the downcore density profile of dead tests and the relatively constant sediment accumulation rates we calculated estimates for the mean life spans of these high marsh foraminiferal species by two slightly different methods. Before accepting these life span estimates we compared the actual depth profiles of dead test density in each core with modelled downcore test density profiles based on ideal conditions of constant sedimentation rates, constant livestock numbers, constant live depth distributions and no taphonomic loss. Estimates from three of our cores are rejected because their dead test profiles suggest significant taphonomic loss in the intervals of interest. Estimates from the remaining eight cores indicate that the highest salt marsh foraminifera in temperate New Zealand have mean life spans of 1.3-13 years, with means of 5.5 years for T. salsa, 4.5 years for T. inflata and 3 years for H. wilberti - showing progressively shorter life spans at lower elevations in less stressful environments. These life span estimates are considerably longer than the majority reported for foraminifera from less harsh conditions but help explain how highest marsh foraminifera survive and grow in this extreme environment. (C) 2014 Published by Elsevier B.V. C1 [Hayward, Bruce W.; Figueira, Brigida O.; Sabaa, Ashwaq T.] Geomarine Res, Auckland, New Zealand. [Buzas, Martin A.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Hayward, BW (reprint author), Geomarine Res, 49 Swainston Rd, Auckland, New Zealand. EM b.hayward@geomarine.org.nz FU New Zealand Foundation for Research Science and Technology FX This paper is a by-product of studies funded by the New Zealand Foundation for Research Science and Technology. We thank Hugh Grenfell for his assistance with field work and Andrew Berkeley and Richard Jordan for their helpful reviews of the manuscript. We thank Atun Zawadzki, Geraldine Jacobsen and Jack Goralewski of the Australian Nuclear Science and Technology Organisation for their assistance with the lead and caesium isotope measurements for age models on Waikawa and Whanganui cores. NR 55 TC 3 Z9 3 U1 1 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-8398 EI 1872-6186 J9 MAR MICROPALEONTOL JI Mar. Micropaleontol. PD MAY PY 2014 VL 109 BP 54 EP 65 DI 10.1016/j.marmicro.2014.03.002 PG 12 WC Paleontology SC Paleontology GA AJ7IZ UT WOS:000337871700005 ER PT J AU Etterson, MA Greenberg, R Hollenhorst, T AF Etterson, Matthew A. Greenberg, Russell Hollenhorst, Tom TI Landscape and regional context differentially affect nest parasitism and nest predation for Wood Thrush in central Virginia, USA SO CONDOR LA English DT Article DE MCestimate; competing risks; edge effects; Wood Thrush; Hylocichla mustelina; nest predation; nest parasitism ID EFFECTIVE MESH SIZE; REPRODUCTIVE SUCCESS; FOREST FRAGMENTATION; MIGRATORY BIRDS; SONGBIRDS; EDGE; MULTISCALE; SELECTION; EXPOSURE; FAILURE AB Many empirical studies have shown that forest-breeding songbirds, and Neotropical migrants in particular, suffer greater rates of nest predation and nest parasitism in smaller forest patches and in fragmented landscapes. To compare the performance of different metrics of spatial habitat configuration resulting from deforestation, we studied nest predation and nest parasitism rates at 200 Wood Thrush (Hylocichla mustelina) nests in eight forest fragments ranging from 82 to 9,171 ha in central Virginia, USA. We analyzed nest parasitism rates using logistic regression and we analyzed daily nest predation rates under a multistate competing risks design. For both analyses we compared the performance of 16 covariates, 11 of which related to the spatial configuration of habitat (e.g., patch size, distance to edge, percent core forest in proximity to nest) and 5 of which were unrelated to habitat (e.g., year, serial date, nest height). Distance to agriculture gained the greatest support in analyses of nest predation and suggested that elevated predation rates are manifest primarily within 50 m of edges; at 5, 10, and 20 m, respectively, the estimated predation rates were 87%, 76%, and 68%. In contrast, biogeographic region received the greatest support in analyses of nest parasitism, which also showed increasing rates of Brown-headed Cowbird (Molothrus ater) parasitism with percent agricultural land and road density within 500 m of a nest. Among regions, the greatest difference seemed to be a virtual absence of nest parasitism along the Blue Ridge in the absence of disturbance (agriculture or road incursion) whereas the other two biogeographic regions showed 20-50% rates of nest parasitism as background rates. Interactive models between spatial configuration metrics and region gained little support from nest predation analyses, but considerable support from the nest parasitism analyses, suggesting regional context plays a more important role in nest parasitism than in nest predation at these central Virginia sites. C1 [Etterson, Matthew A.; Hollenhorst, Tom] US EPA, Off Res & Dev, Natl Hlth & Environm Effects Res Lab, Mid Continent Ecol Div, Duluth, MN 55804 USA. [Greenberg, Russell] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Etterson, MA (reprint author), US EPA, Off Res & Dev, Natl Hlth & Environm Effects Res Lab, Mid Continent Ecol Div, Duluth, MN 55804 USA. EM etterson.matthew@epa.gov FU Smithsonian Migratory Bird Center FX Funding for field work was provided by the Smithsonian Migratory Bird Center. Traynor Biasiolli, Francesca May, and Wanda San Jule assisted greatly with nest discovery and monitoring. Lisa Petit provided invaluable guidance in designing the sampling regime. G. Shriver and M. Starus provided valuable comments that greatly improved an earlier version of this manuscript. The views expressed in this paper are those of the authors and do not necessarily reflect the views or policies of the U.S. Environmental Protection Agency. NR 43 TC 8 Z9 8 U1 6 U2 49 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 2014 VL 116 IS 2 BP 205 EP 214 DI 10.1650/CONDOR-13-045.1 PG 10 WC Ornithology SC Zoology GA AK0ID UT WOS:000338095200006 ER PT J AU Reef, R Feller, IC Lovelock, CE AF Reef, Ruth Feller, Ilka C. Lovelock, Catherine E. TI Mammalian herbivores in Australia transport nutrients from terrestrial to marine ecosystems via mangroves SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE elemental composition; flying fox; kangaroos; Macropus spp; nutrient subsidy; Pteropus sp; roost; stable isotopes; tree growth; vector ID FOX PTEROPUS-ALECTO; WESTERN-AUSTRALIA; RHIZOPHORA-MANGLE; ORGANIC-MATTER; PACIFIC SALMON; FOOD WEBS; AVICENNIA-GERMINANS; NORTHERN-TERRITORY; CARBON ALLOCATION; FLYING-FOXES AB Nutrient subsidies from one ecosystem to another serve a critical link among ecosystems. The transfer of materials across the terrestrial-to-marine boundary is considered to be driven by hydrological connectivity, but animal movement can provide another pathway for nutrient transfers. In two separate studies we assessed the role mammals (bats and kangaroos) play in alleviating nutrient limitation in mangrove forests in Australia. At Lizard Island, we measured tree growth and foliar elemental and isotopic composition of trees growing within and outside a large flying fox roost. In Western Australia, we measured foliar elemental and isotopic composition of trees within two forests frequented by kangaroos that feed in spinifex grasslands and shelter in the shade of the mangroves. We compared those with mangroves from adjacent forests that are not frequented by kangaroos. We show that at both locations, the mangroveforest receives terrestrial nutrient subsidies through animal movement. At Lizard Island dominant mangrove species were significantly enriched in nitrogen within the bat roost, as evidenced by higher foliar N concentrations (by up to 150%), N:P and N:C ratios in trees within the roost compared with trees outside the roost. The isotopic signature of foliar N was significantly enriched in 15N by 1-3% within the roost, further suggesting that the source of the N enrichment was the bat roost. Growth rates of mangroves within the roost were nearly six times higher than trees outside the roost. In the arid coast of Western Australia, we show elevated foliar N-15 abundance of up to 3 parts per thousand in mangroves where kangaroos shelter relative to trees where they do not. Thus, this study presents two examples for mammalian herbivore mediated localized transport of nutrients from terrestrial to marine ecosystems, consequently affecting mangrove tree growth, productivity and forest structure. C1 [Reef, Ruth; Lovelock, Catherine E.] Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia. [Feller, Ilka C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Reef, R (reprint author), Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia. EM r.reef@uq.edu.au RI Lovelock, Catherine/G-7370-2012; OI Lovelock, Catherine/0000-0002-2219-6855; Feller, Ilka/0000-0002-6391-1608 FU ARC awards [DP0774491, DP1096749, DE120101706] FX This study was funded by ARC awards DP0774491, DP1096749 and DE120101706. We thank H. Penrose for assistance in the field and N. Santini and F. Adame for helpful comments on the manuscript. We thank R. Kelley for the photo of the euro. NR 66 TC 4 Z9 4 U1 3 U2 39 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 2014 VL 30 BP 179 EP 188 DI 10.1017/S0266467414000054 PN 3 PG 10 WC Ecology SC Environmental Sciences & Ecology GA AJ5XC UT WOS:000337762600001 ER PT J AU Young, HS McCauley, DJ Pollock, A Dirzo, R AF Young, Hillary S. McCauley, Douglas J. Pollock, Amanda Dirzo, Rodolfo TI Differential plant damage due to litterfall in palm-dominated forest stands in a Central Pacific atoll SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Cocos nucifera; diversity; island; litterfall; palm; regeneration ID SCALE PHYSICAL DISTURBANCE; TROPICAL MOIST FOREST; RAIN-FOREST; SEEDLING MORTALITY; MECHANICAL DAMAGE; TREE SEEDLINGS; ESTABLISHMENT; FRAGMENTS; PANAMA; DIVERSITY AB High densities of palms are common in many tropical forests. In some cases, the dominance of palms has been associated with a depauperate understorey and high rates of native seedling mortality. A variety of different potential mechanisms has been suggested to explain the sustained palm dominance in the understorey and canopy of these forests. Working in a Cocos nucifera-dominated wet tropical forest at Palmyra Atoll in the central Pacific, we examine how litterfall from this pantropical, and economically important palm, impacts seedling survival. We compare rates of litterfall, and rates of litterfall-associated damage, between forest stands dominated by C. nucifera (coconut palm) and forest stands with low abundance of C. nucifera. To assess litterfall damage we survey damage to both artificial seedlings (n = 711), outplanted real seedlings of two species (with and without protection via caging; n = 204), and standing rates of litterfall damage. We find that rates of large-litterfall damage were an average of five times higher in sites with high densities of C. nucifera. Associated with these increases we observe that levels of physical damage to artificial model seedlings caused by litterfall over a 4-mo period increased from 4.9% in sites with low abundance of C. nucifera to 16.1% in sites with high abundance of C. nucifera. Extrapolated to annual rates, litterfall damage of this magnitude exceeds the average levels observed in other published studies. Living native seedlings also showed more than 300% higher levels of mortality in forest stands with high densities of C. nucifera, a difference that was greatly reduced when protected by caging from litterfall. In contrast, uncaged C. nucifera seedlings actually had slightly higher survivorship in habitats dominated by conspecifics. We suggest that litterfall damage may be an important mechanism by which this tropical palm reaches and maintains near monodominance in many coastal and insular habitats. C1 [Young, Hillary S.; Dirzo, Rodolfo] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Young, Hillary S.] Smithsonian Inst, Div Vertebrate Zool, Washington, DC 20013 USA. [McCauley, Douglas J.] Stanford Univ, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. [Pollock, Amanda] US Fish & Wildlife Serv, Honolulu, HI USA. RP Young, HS (reprint author), Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. EM hyoung@fas.harvard.edu FU National Science Foundation; National Geographic Society and US Fish and Wildlife Service; Palmyra Atoll National Wildlife Refuge under a Special Use Permit FX We thank the National Science Foundation, National Geographic Society and US Fish and Wildlife Service for their support of this research. This research was done within the Palmyra Atoll National Wildlife Refuge under a Special Use Permit issued by the US Fish and Wildlife Service. We thank J. Wible, L. Anderegg, A. Briggs, W. Anderegg, G. Carroll, P. DeSalles, Z. Drozdz, C. Hanson, J. McCallen, L. Palumbi, T. Robbins and J. Tam for their assistance in the field. We thank Len Gillman and Markus Eichhorn for their careful reviews of this manuscript. NR 29 TC 3 Z9 3 U1 0 U2 9 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 2014 VL 30 BP 231 EP 236 DI 10.1017/S026646741400008X PN 3 PG 6 WC Ecology SC Environmental Sciences & Ecology GA AJ5XC UT WOS:000337762600006 ER PT J AU Clarke, EM Thompson, RC Allam, AH Wann, LS Lombardi, GP Sutherland, ML Sutherland, JD Cox, SL Soliman, MAT Abd El-Maksoud, G Badr, I Miyamoto, MI Frohlich, B El-Din, AHN Stewart, AFR Narula, J Zink, AR Finch, CE Michalik, DE Thomas, GS AF Clarke, Emily M. Thompson, Randall C. Allam, Adel H. Wann, L. Samuel Lombardi, Guido P. Sutherland, M. Linda Sutherland, James D. Cox, Samantha L. Soliman, Muhammad Al-Tohamy Abd El-Maksoud, Gomaa Badr, Ibrahem Miyamoto, Michael I. Frohlich, Bruno El-Din, Abdel-Halim Nur Stewart, Alexandre F. R. Narula, Jagat Zink, Albert R. Finch, Caleb E. Michalik, David E. Thomas, Gregory S. TI Is atherosclerosis fundamental to human aging? Lessons from ancient mummies SO JOURNAL OF CARDIOLOGY LA English DT Review DE Mummies; Atherosclerosis; Aging; Paleopathology; Coronary artery disease ID CORONARY HEART-DISEASE; HUMAN LIFE-SPAN; EGYPTIAN MUMMIES; CARDIOVASCULAR-DISEASE; RISK; INFLAMMATION; INFECTION; HORUS; ASSOCIATION; INFLUENZA AB Case reports from Johan Czermak, Marc Ruffer, and others a century or more ago demonstrated ancient Egyptians had atherosclerosis three millennia ago. The Horus study team extended their findings, demonstrating that atherosclerosis was prevalent among 76 ancient Egyptian mummies and among 61 mummies from each of the ancient cultures of Peru, the American Southwest, and the Aleutian Islands. These findings challenge the assumption that atherosclerosis is a modern disease caused by present day risk factors. An extensive autopsy of an ancient Egyptian teenage male weaver named Nakht found that he was infected with four parasites: Schistosoma haematobium, Taenia species, Trichinella spiralis, and Plasmodium falciparum. Modern day patients with chronic inflammatory disease such as rheumatoid arthritis, systemic lupus erythematosus, and human immunodeficiency virus experience premature atherosclerosis. Could the burden of chronic inflammatory disease have been a risk factor for atherosclerosis in these ancient cultures? The prevalence of atherosclerosis in four diverse ancient cultures is consistent with atherosclerosis being fundamental to aging. The impact of risk factors in modern times, and potentially in ancient times, suggests a strong gene-environmental interplay: human genes provide a vulnerability to atherosclerosis, the environment determines when and if atherosclerosis becomes manifest clinically. (C) 2014 Japanese College of Cardiology. Published by Elsevier Ltd. All rights reserved. C1 [Clarke, Emily M.] Univ Calif Los Angeles, Los Angeles, CA USA. [Thompson, Randall C.] St Lukes Mid Amer Heart Inst, Kansas City, MO USA. [Thompson, Randall C.] Univ Missouri, Sch Med, Kansas City, MO 64108 USA. [Allam, Adel H.] Al Azhar Med Sch, Cairo, Egypt. [Wann, L. Samuel] Columbia St Marys Healthcare, Milwaukee, WI USA. [Lombardi, Guido P.] Univ Peruana Cayetano Heredia, Lab Paleopatol, Catedra Pedro Weiss, Lima, Peru. [Sutherland, M. Linda] Newport Diagnost Ctr, Newport Beach, CA USA. [Sutherland, James D.] Saddleback Mem, Laguna Hills, CA USA. [Cox, Samantha L.] Univ Cambridge, Cambridge, England. [Soliman, Muhammad Al-Tohamy] Natl Res Ctr, Giza, Egypt. [Abd El-Maksoud, Gomaa] Cairo Univ, Cairo, Egypt. [Badr, Ibrahem] Inst Restorat, Alexandria, Egypt. [Miyamoto, Michael I.] Miss Internal Med Grp, Mission Viejo, CA USA. [Frohlich, Bruno] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [El-Din, Abdel-Halim Nur] Univ Sci & Technol, 6TH Of October City, Egypt. [Stewart, Alexandre F. R.] Univ Ottawa, Inst Heart, Ottawa, ON, Canada. [Narula, Jagat] Mt Sinai, New York, NY USA. [Zink, Albert R.] European Acad, Inst Mummies & Iceman, Bolzano, Italy. [Finch, Caleb E.] Univ So Calif, Los Angeles, CA USA. [Michalik, David E.] Miller Childrens Hosp, Long Beach, CA USA. [Thomas, Gregory S.] Univ Calif Irvine, Irvine, CA USA. Long Beach Mem, MemorialCare Heart & Vasc Inst, Long Beach, CA 90806 USA. RP Thomas, GS (reprint author), Long Beach Mem, 2801 Atlantic Ave, Long Beach, CA 90806 USA. EM gthomas1@memorialcare.org RI Zink, Albert/P-4024-2015; Al-Tohamy, Muhammad/B-4273-2016; OI Zink, Albert/0000-0002-1461-747X; Al-Tohamy, Muhammad/0000-0001-9368-2570; Stewart, Alexandre/0000-0003-2673-9164 FU National Endowment for the Humanities [HJ-50069-12]; Paleocardiology Foundation; Siemens; National Bank of Egypt; St Luke's Hospital Foundation of Kansas City FX Funding for the Horus study was provided by the National Endowment for the Humanities (#HJ-50069-12), the Paleocardiology Foundation, Siemens, the National Bank of Egypt, and the St Luke's Hospital Foundation of Kansas City. NR 51 TC 8 Z9 8 U1 2 U2 4 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0914-5087 EI 1876-4738 J9 J CARDIOL JI J. Cardiol. PD MAY-JUN PY 2014 VL 63 IS 5-6 BP 329 EP 334 DI 10.1016/j.jjcc.2013.12.012 PG 6 WC Cardiac & Cardiovascular Systems SC Cardiovascular System & Cardiology GA AJ3FI UT WOS:000337551500002 PM 24582386 ER PT J AU Ose, GA Hogsette, JA AF Ose, Gregory A. Hogsette, Jerome A. TI Spatial Distribution, Seasonality and Trap Preference of Stable Fly, Stomoxys Calcitrans L. (Diptera: Muscidae), Adults on a 12-Hectare Zoological Park SO ZOO BIOLOGY LA English DT Article DE alsynite fiberglass; sticky traps; UV light; cloth target; cylinder traps ID FLIES DIPTERA; BITING FLIES; ABUNDANCE; FLORIDA; POPULATIONS; CATTLE; DAIRY; NZI AB Although this study was originally designed to compare the efficacy of two different stable fly traps within 10 sites at a 12-ha zoological park, seasonal and spatial population distribution data were simultaneously collected. The two traps included an Alsynite fiberglass cylindrical trap (AFT) and a blue-black cloth target modified into a cylindrical trap (BCT). Both traps were covered with sticky sleeves to retain the attracted flies. Paired trap types were placed at sites that were 20-100 m apart. Distance between trap pairs within sites ranged from 1 to 2 m, and was limited by exhibit design and geography. Both trap types reflect/refract ultraviolet (UV) light which attracts adult S. calcitrans. During this 15-week study, AFTs captured significantly more stable flies than the BCTs at 8 of the 10 sites. Of the 12,557 stable flies found on the traps, 80% and 20% were captured by AFTs and BCTs, respectively. The most attractive trap site at the zoo was at the goat exhibit where most stable flies were consistently captured throughout the study. This exhibit was 100m from the other exhibits, next to a small lake, and adjacent to a field containing pastured exotic ungulates, rhea and ostrich. Stable fly populations peaked in early June then slowly decreased as the last trapping date approached. We believe this to be the first seasonality data collected at a zoological park. Results demonstrate the use of urban zoos by stable flies and the need to develop environmentally friendly stable fly management systems for zoos. Published 2014. This article is a U.S. Government work and is in the public domain in the USA. C1 [Ose, Gregory A.] Univ Nebraska, Dept Entomol, Lincoln, NE 68583 USA. [Ose, Gregory A.] Smithsonian Natl Zool Pk, Ctr Anim Care Sci, Washington, DC USA. [Hogsette, Jerome A.] ARS, USDA, Ctr Med Agr & Vet Entomol, Gainesville, FL 32608 USA. RP Hogsette, JA (reprint author), ARS, USDA, Ctr Med Agr & Vet Entomol, Gainesville, FL 32608 USA. EM jerry.hogsette@ars.usda.gov NR 30 TC 1 Z9 1 U1 1 U2 25 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0733-3188 EI 1098-2361 J9 ZOO BIOL JI Zoo Biol. PD MAY-JUN PY 2014 VL 33 IS 3 BP 228 EP 233 DI 10.1002/zoo.21126 PG 6 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA AJ4XC UT WOS:000337681700009 PM 24740859 ER PT J AU Stauderman, S AF Stauderman, Sarah TI COMPENDIUM OF IMAGE ERRORS IN ANALOGUE VIDEO SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Book Review C1 [Stauderman, Sarah] Smithsonian Inst Arch, Washington, DC 20013 USA. RP Stauderman, S (reprint author), Smithsonian Inst Arch, MRC 507,POB 37012, Washington, DC 20013 USA. EM Staudermans@si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0197-1360 EI 1945-2330 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD MAY PY 2014 VL 53 IS 2 BP 140 EP 141 DI 10.1179/0197136014Z.0000000030 PG 2 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA AI7KE UT WOS:000337067600004 ER PT J AU Dangremond, EM Feller, IC AF Dangremond, Emily M. Feller, Ilka C. TI Functional traits and nutrient limitation in the rare mangrove Pelliciera rhizophorae SO AQUATIC BOTANY LA English DT Article DE Pelliciera rhizophorae; Functional traits; Nutrient limitation; Mangrove; Panama ID AVICENNIA-GERMINANS; RESORPTION; GROWTH; PANAMA; ENRICHMENT; LEAVES; PHOTOSYNTHESIS; ESTUARIES; HERBIVORY; PATTERNS AB Nutrient limitation is a major factor structuring mangrove forests, with nitrogen (N) and phosphorus (P) limitation causing stunted growth forms around the world. The rare mangrove Pelliciera rhizophorae exists in both fringe and dwarf forms on both coasts of Panama, but the reasons for the differences in growth form are unknown. Nutrient content, functional traits and herbivory were measured in fringe and dwarf trees from 14 populations on the Pacific and Caribbean coasts of Panama. Dwarf trees had a mean N of 1.51% on the Caribbean and 1.37% on the on the Pacific, lower than the 1.58% N fringe trees had on both coasts. Dwarf trees also had lower P concentrations (Caribbean: 0.10%, Pacific: 0.11%) in their green leaves than fringe trees (Caribbean: 0.12%, Pacific: 0.13%), indicating nutrient limitation may be responsible for the dwarf growth form of this species. Additionally, Caribbean trees had higher rates of P resorption (70.97-72.65%) compared to Pacific trees (58.87-60.8%) and lower P content in senescent leaves, suggesting Caribbean trees are P limited relative to Pacific trees. Dwarf trees allocate biomass differently than fringe trees, with smaller stem length to stem biomass, and leaf weight, shoot weight, and leaf area ratios. Dwarf trees experience less herbivory than fringe trees, which may be a result of lower leaf nutrient content. This is the first study to examine nutrients and growth traits in P. rhizophorae, and the only study to date comparing nutrients and growth traits in mangroves from both the Caribbean and Pacific coasts of Panama. (c) 2014 Elsevier B.V. All rights reserved. C1 [Dangremond, Emily M.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Dangremond, Emily M.; Feller, Ilka C.] Smithsonian Environm Res Ctr, Edgewater, MD 21307 USA. RP Dangremond, EM (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21307 USA. EM dangremonde@si.edu OI Feller, Ilka/0000-0002-6391-1608 FU Smithsonian Marine Science Network; National Science Foundation Graduate Research Fellowship Program FX The authors thank the Smithsonian Marine Science Network for funding and the staff of the Smithsonian Tropical Research Institue (STRI) in Bocas del Toro and Punta Galeta, Panama for logistical and field support. We also thank the government of Panama for permission to use study sites. The authors thank Jaime Polania and Eric Brown for field assistance, and Anne Chamberlain, Lisa Duckett, Sierra Flynn and Dianna Samuelson for laboratory support. Wayne Sousa, Paul Fine, Perry de Valpine and three anonymous reviewers greatly improved previous versions. EMD was supported by the National Science Foundation Graduate Research Fellowship Program. NR 31 TC 1 Z9 1 U1 1 U2 24 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3770 EI 1879-1522 J9 AQUAT BOT JI Aquat. Bot. PD MAY PY 2014 VL 116 BP 1 EP 7 DI 10.1016/j.aquabot.2013.12.007 PG 7 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA AI5ZX UT WOS:000336950700001 ER PT J AU Alves, J Lombardi, M Lada, CJ AF Alves, Joao Lombardi, Marco Lada, Charles J. TI 2MASS wide-field extinction maps SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: structure; ISM: clouds; dust, extinction; ISM: general ID DENSITY PROBABILITY-DISTRIBUTION; TURBULENT MAGNETIZED CLOUDS; STAR-FORMING REGIONS; MOLECULAR CLOUDS; COLUMN-DENSITY; ISOTHERMAL TURBULENCE; INTERSTELLAR CLOUDS; CORONAE-AUSTRALIS; H-I; GAS AB We present a near-infrared extinction map of a large region (similar to 870 deg(2)) covering the isolated Corona Australis complex of molecular clouds. We reach a 1-sigma error of 0.02 mag in the K-band extinction with a resolution of 3 arcmin over the entire map. We find that the Corona Australis cloud is about three times as large as revealed by previous CO and dust emission surveys. The cloud consists of a 45 pc long complex of filamentary structure from the well known star forming Western-end (the head, N >= 10(23) cm(-2)) to the diffuse Eastern-end (the tail, N <= 10(21) cm(-2)). Remarkably, about two thirds of the complex both in size and mass lie beneath A(v) similar to 1 mag. We find that the probability density function (PDF) of the cloud cannot be described by a single log-normal function. Similar to prior studies, we found a significant excess al., high column densities, but a log-normal + power-law tail fit does not work well at low column densities. We show that at low column densities near the peak of the observed PDF, both the amplitude and shape of the PDF are dominated by noise in the extinction measurements making it impractical to derive the intrinsic cloud PDF below A(K) < 0.15 mag. Above A(K) similar to 0.15 mag, essentially the molecular component of the cloud, the PDF appears to be best described by a power-law with index -3, but could also described as the tail of a broad and relatively low amplitude, log-normal PDF that peaks at very low column densities. C1 [Alves, Joao] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Lombardi, Marco] Univ Milan, Dept Phys, I-20133 Milan, Italy. [Lada, Charles J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Alves, J (reprint author), Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria. EM joao.alves@univie.ac.at OI LOMBARDI, MARCO/0000-0002-3336-4965; Alves, Joao/0000-0002-4355-0921 FU Austrian Science Fund (FWF); NASA ORIGINS [NAG 5-13041] FX It is a pleasure to acknowledge discussions with Paolo Padoan, Jouni Kainulainen, and Alyssa Goodman. We also want to thank the anonymous referee for comments that subtantially improved the paper. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013). This publication is supported by the Austrian Science Fund (FWF). This research has made use of the 2MASS archive, provided by 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. C.J.L. acknowledges support from NASA ORIGINS Grant NAG 5-13041. NR 56 TC 16 Z9 16 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2014 VL 565 AR A18 DI 10.1051/0004-6361/201322159 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900018 ER PT J AU Poppenhaeger, K Wolk, SJ AF Poppenhaeger, K. Wolk, S. J. TI Indications for an influence of hot Jupiters on the rotation and activity of their host stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: activity; stars: coronae; planet-star interactions; X-rays: stars; binaries: general ID EXTRASOLAR GIANT PLANETS; X-RAY-EMISSION; STELLAR ROTATION; CORONAL PROPERTIES; TIDAL DISSIPATION; MAGNETIC ACTIVITY; TAU-BOOTIS; HD 189733; PERIOD; GYROCHRONOLOGY AB Context. The magnetic activity of planet-hosting stars is an important factor for estimating the atmospheric stability of close-in exoplanets and the age of their host stars. It has long been speculated that close-in exoplanets can influence the stellar activity level. However, testing for tidal or magnetic interaction effects in samples of planet-hosting stars is difficult because stellar activity hinders exoplanet detection, so that stellar samples with detected exoplanets show a bias toward low activity for small exoplanets. Aims. We aim to test whether exoplanets in close orbits influence the stellar rotation and magnetic activity of their host stars. Methods. We developed a novel approach to test for systematic activity-enhancements in planet-hosting stars. We use wide (several 100 AU) binary systems in which one of the stellar components is known to have an exoplanet, while the second stellar component does not have a detected planet and therefore acts as a negative control. We use the stellar coronal X-ray emission as an observational proxy for magnetic activity and analyze observations performed with Chandra and XMM-Newton. Results. We find that in two systems for which strong tidal interaction can be expected the planet-hosting primary displays a much higher magnetic activity level than the planet-free secondary. In three systems for which weaker tidal interaction can be expected the activity levels of the two stellar components agree with each other. Conclusions. Our observations indicate that the presence of Hot Jupiters may inhibit the spin-down of host stars with thick outer convective layers. Possible causes for this effect include a transfer of angular momentum from the planetary orbit to the stellar rotation through tidal interaction, or differences during the early evolution of the system, where the host star may decouple from the protoplanetary disk early because of a gap opened by the forming Hot Jupiter. C1 [Poppenhaeger, K.; Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Poppenhaeger, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kpoppenhaeger@cfa.harvard.edu OI Poppenhaeger, Katja/0000-0003-1231-2194 FU NASA FX This work was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. NR 46 TC 37 Z9 37 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2014 VL 565 AR L1 DI 10.1051/0004-6361/201423454 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900133 ER PT J AU Sanna, A Cesaroni, R Moscadelli, L Zhang, Q Menten, KM Molinari, S Garatti, ACO De Buizer, JM AF Sanna, A. Cesaroni, R. Moscadelli, L. Zhang, Q. Menten, K. M. Molinari, S. Garatti, A. Caratti O. De Buizer, J. M. TI A subarcsecond study of the hot molecular core in G023.01-00.41 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: kinematics and dynamics; instrumentation: high angular resolution; stars individual: G23.01-0.41; stars: formation ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; GALACTIC PLANE; MASSIVE STARS; HI-GAL; OUTFLOWS; EMISSION; G23.01-0.41; PROTOSTARS; ACCRETION AB Context. Searching for disk-outflow systems in massive star-forming regions is a key to assessing the main physical processes in the recipe of massive star formation. Aims. We have selected a hot molecular core (HMC) in the high-mass star-forming region G023.011-00.41, where VLBI multi-epoch observations of water and methanol masers have suggested the existence of rotation and expansion within 2000 AU of its center. Our piu-pose is to image the thermal line and continuum emission at millimeter was to establish the physical parameters and velocity field of the gas in the region. Methods. We performed SMA observations at 1.3 mm with both the most extended and compact array configurations, providing subarcsecond and high sensitivity maps of various molecular lines, including both hot-core and outflow tracers. We also reconstructed the spectral energy distribution of the region from millimeter to near infrared wavelengths, using the Herschel/Hi-GAL maps, as well as archival data. Results. From the spectral energy distribution, we derive a bolometric luminosity of similar to 4 x 10(4) L-circle dot. Our interferometric observations reveal that the distribution of dense gas and dust in the HMC is significantly flattened and extends up to a radius of 8000 AU from the center of radio continuum and maser emission in the region. The equatorial plane of this HMC is strictly perpendicular to the elongation of the collimated bipolar outflow, as imaged on scales of similar to 0.1-0.5 pc in the main CO isotopomers, as well as in the SiO(5-4) line. In the innermost LIMC regions (less than or similar to 1000 AU), the velocity.field traced by the CH3CN (12(K)-11(K)) line emission shows that molecular gas is both expanding along the outflow direction following a Hubble law and rotating about the outflow axis, in agreement with the (3D) velocity field traced by methanol masers. The velocity field associated with rotation indicates a dynamical mass of similar to 19 M-circle dot at the center of the core. The latter is likely to be concentrated in a single O9.5 ZAMS star, consistent with the estimated bolometric luminosity of G023.01-00.41. The physical properties of the CO (2-1) outflow emission, such as its momentum rate 6 x 10(-3) M-circle dot km s(-1) yr(-1) and its outflow rate 2 x 10(-4) M circle dot yr(-1), support our estimates of the luminosity (and mass) of the embedded young stellar object. C1 [Sanna, A.; Menten, K. M.; Garatti, A. Caratti O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Cesaroni, R.; Moscadelli, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Molinari, S.] INAF IFSI, I-00133 Rome, Italy. [De Buizer, J. M.] NASA, Stratospher Observ Infrared Astron USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Sanna, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM asanna@mpifr-bonn.mpg.de RI Molinari, Sergio/O-4095-2016; OI Molinari, Sergio/0000-0002-9826-7525; Moscadelli, Luca/0000-0002-8517-8881; Cesaroni, Riccardo/0000-0002-2430-5103; Caratti o Garatti, Alessio/0000-0001-8876-6614; Zhang, Qizhou/0000-0003-2384-6589 FU European Research Council for the ERC Advanced [247078]; National Aeronautics and Space Administration FX Comments from the anonymous referee, which helped improving our paper, are gratefully acknowledged. Financial support by the European Research Council for the ERC Advanced Grant GLOSTAR (ERC-2009-AdG, Grant Agreement no. 247078) is gratefully acknowledged. This research made use of the myXCLASS program (https//www.astro.uni-koeln.de/projects/schilke/XCLASS), which accesses the CDMS (http//www.cdms.de) and JPL (http://spec.jpl.nasa.gov) molecular databases. 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. NR 37 TC 9 Z9 9 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2014 VL 565 AR A34 DI 10.1051/0004-6361/201323129 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900034 ER PT J AU Ueta, T Ladjal, D Exter, KM Otsuka, M Szczerba, R Siodmiak, N Aleman, I van Hoof, PAM Kastner, JH Montez, R McDonald, I Wittkowski, M Sandin, C Ramstedt, S De Marco, O Villaver, E Chu, YH Vlemmings, W Izumiura, H Sahai, R Lopez, JA Balick, B Zijlstra, A Tielens, AGGM Rattray, RE Behar, E Blackman, EG Hebden, K Hora, JL Murakawa, K Nordhaus, J Nordon, R Yamamura, I AF Ueta, T. Ladjal, D. Exter, K. M. Otsuka, M. Szczerba, R. Siodmiak, N. Aleman, I. van Hoof, P. A. M. Kastner, J. H. Montez, R., Jr. McDonald, I. Wittkowski, M. Sandin, C. Ramstedt, S. De Marco, O. Villaver, E. Chu, Y-H Vlemmings, W. Izumiura, H. Sahai, R. Lopez, J. A. Balick, B. Zijlstra, A. Tielens, A. G. G. M. Rattray, R. E. Behar, E. Blackman, E. G. Hebden, K. Hora, J. L. Murakawa, K. Nordhaus, J. Nordon, R. Yamamura, I. TI The Herschel Planetary Nebula Survey (HerPlaNS) I. Data overview and analysis demonstration with NGC 6781 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE infrared: stars; planetary nebulae: general; stars: winds, outflows; stars: mass-loss; planetary nebulae: individual: NGC 6781; circumstellar matter ID GIANT BRANCH STARS; OPTICAL RECOMBINATION LINES; FAR-INFRARED SPECTROSCOPY; INTERMEDIATE-MASS STARS; EXCITATION ATOMIC GAS; HELIX-NEBULA; EVOLVED STARS; CHEMICAL ABUNDANCES; INTERSTELLAR-MEDIUM; MAGELLANIC-CLOUD AB Context. This is the first of a series of investigations into far-IR characteristics of 11 planetary nebulae (PNe) under the Herschel Space Observatory open time 1 program, Herschel Planetary Nebula Survey (HerPlaNS). Aims. Using the HerPlaNS data set, we look into the PN energetics and variations of the physical conditions within the target nebulae. In the present work, we provide an overview of the survey, data acquisition and processing, and resulting data products. Methods. We performed (1) PACS/SPIRE broadband imaging to determine the spatial distribution of the cold dust component in the target PNe and (2) PACS/SPIRE spectral-energy-distribution and line spectroscopy to determine the spatial distribution of the gas component in the target PNe. Results. For the case of NGC 6781, the broadband maps confirm the nearly pole-on barrel structure of the amorphous carbon-rich dust shell and the surrounding halo having temperatures of 26-40 K. The PACS/SPIRE multiposition spectra show spatial variations of far-.IR lines that reflect the physical stratification of the nebula. We demonstrate that spatially resolved far-IR line diagnostics yield the (T-e, n(e)) profiles, from which distributions of ionized, atomic, and molecular gases can be determined. Direct comparison of the dust and gas column mass maps constrained by the HerPlaNS data allows to construct an empirical gas-to-dust mass ratio map, which shows a range of ratios with the median of 195 +/- 110. The present analysis yields estimates of the total mass of the shell to be 0.86 M-circle dot, consisting of 0.54 M-circle dot of ionized gas, 0.12 M-circle dot of atomic gas, 0.2 M-circle dot of molecular gas, and 4 x 10(-3) M-circle dot of dust grains. These estimates' also suggest that the central star of about 1.5 M-circle dot initial mass is terminating its PN evolution onto the white dwarf cooling track. Conclusions. The HerPlaNS data provide various diagnostics for both the dust and gas components in a spatially resolved manner. In the forthcoming papers of the HerPlaNS series we will explore the HerPlaNS data set fully for the entire sample of 11 PNe. C1 [Ueta, T.; Ladjal, D.; Rattray, R. E.] Univ Denver, Dept Phys & Astron, Denver, CO 80210 USA. [Ueta, T.; Yamamura, I.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Exter, K. M.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Otsuka, M.] Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. [Szczerba, R.; Siodmiak, N.] N Copernicus Astron Ctr, PL-87100 Torun, Poland. [Aleman, I.; Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Hoof, P. A. M.] Royal Observ Belgium, B-1180 Brussels, Belgium. [Kastner, J. H.] Rochester Inst Technol, Rochester, NY 14623 USA. [Montez, R., Jr.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [McDonald, I.; Zijlstra, A.; Hebden, K.] Jodrell Batik Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Wittkowski, M.] ESO, D-85748 Garching, Germany. [Sandin, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Ramstedt, S.] Uppsala Univ, Div Astron & Space Phys, Dept Phys & Astron, S-75120 Uppsala, Sweden. [De Marco, O.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Villaver, E.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. [Chu, Y-H] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Vlemmings, W.] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. [Izumiura, H.] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan. [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lopez, J. A.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 22800, Baja California, Mexico. [Balick, B.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Behar, E.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Blackman, E. G.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14618 USA. [Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murakawa, K.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Nordhaus, J.] Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 USA. [Nordon, R.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. RP Ueta, T (reprint author), Univ Denver, Dept Phys & Astron, 2112 E Wesley Ave, Denver, CO 80210 USA. EM tueta@du.edu RI Aleman, Isabel/F-3251-2012; OI /0000-0002-2700-9916; Wittkowski, Markus/0000-0002-7952-9550 FU NASA by jet Propulsion Laboratory, Caltech; NASA by jet Propulsion Laboratory, Ladjal; NASA by jet Propulsion Laboratory, Kastner; NASA by jet Propulsion Laboratory, Sahai; Japan Society for the Promotion of Science (JSPS); Belgian Federal Science Policy Office via the PRODEX Programme of ESA; Polish NCN [2011/01/B/ST9/02031]; European Research Council via the advanced-ERC [246976]; Dutch Science Agency (NWO) via the Dutch Astrochemistry Network; NASA FX This work is based on observations made with the Herschel Space Observatory, a European Space Agency (ESA) Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by jet Propulsion Laboratory, Caltech Ladjal, Kastner, Sahai), the Japan Society for the Promotion of Science (JSPS) through a FY2013 long-term invitation fellowship program (Ueta), the Belgian Federal Science Policy Office via the PRODEX Programme of ESA (Exter, van Hoof), the Polish NCN through a grant 2011/01/B/ST9/02031 (Szczerba, Siodmiak), and the European Research Council via the advanced-ERC grant 246976 and the Dutch Science Agency (NWO) via the Dutch Astrochemistry Network and the Spinoza prize (Aleman, Tielens). The authors thank M. A. Guerrero for sharing the NOT optical images of NGC 6781 with us. Also, H. Monteiro's generosity is appreciated for the reproduction of one of his figures (Fig. 3 of Schwarz & Monteiro 2006). Sahai acknowledges that his contribution to the research described here was carried out at the JPE/Caltech, under a contract with NASA. Finally, Ueta also acknowledges the hospitality of the members of the Laboratory of Infrared Astrophysics at ISAS/JAXA during his sabbatical stay as a JSPS invitation fellow. NR 84 TC 7 Z9 7 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2014 VL 565 AR A36 DI 10.1051/0004-6361/201423395 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3AN UT WOS:000336730900036 ER PT J AU Benson, RBJ Campione, NE Carrano, MT Mannion, PD Sullivan, C Upchurch, P Evans, DC AF Benson, Roger B. J. Campione, Nicolas E. Carrano, Matthew T. Mannion, Philip D. Sullivan, Corwin Upchurch, Paul Evans, David C. TI Rates of Dinosaur Body Mass Evolution Indicate 170 Million Years of Sustained Ecological Innovation on the Avian Stem Lineage SO PLOS BIOLOGY LA English DT Article ID CRETACEOUS-PALEOGENE BOUNDARY; ADAPTIVE RADIATION; SIZE EVOLUTION; MORPHOLOGICAL DISPARITY; STABILIZING SELECTION; SPECIES-DIVERSITY; CHARACTER CHANGE; RED QUEEN; MAMMALS; EXTINCTION AB Large-scale adaptive radiations might explain the runaway success of a minority of extant vertebrate clades. This hypothesis predicts, among other things, rapid rates of morphological evolution during the early history of major groups, as lineages invade disparate ecological niches. However, few studies of adaptive radiation have included deep time data, so the links between extant diversity and major extinct radiations are unclear. The intensively studied Mesozoic dinosaur record provides a model system for such investigation, representing an ecologically diverse group that dominated terrestrial ecosystems for 170 million years. Furthermore, with 10,000 species, extant dinosaurs (birds) are the most speciose living tetrapod clade. We assembled composite trees of 614-622 Mesozoic dinosaurs/birds, and a comprehensive body mass dataset using the scaling relationship of limb bone robustness. Maximum-likelihood modelling and the node height test reveal rapid evolutionary rates and a predominance of rapid shifts among size classes in early (Triassic) dinosaurs. This indicates an early burst niche-filling pattern and contrasts with previous studies that favoured gradualistic rates. Subsequently, rates declined in most lineages, which rarely exploited new ecological niches. However, feathered maniraptoran dinosaurs (including Mesozoic birds) sustained rapid evolution from at least the Middle Jurassic, suggesting that these taxa evaded the effects of niche saturation. This indicates that a long evolutionary history of continuing ecological innovation paved the way for a second great radiation of dinosaurs, in birds. We therefore demonstrate links between the predominantly extinct deep time adaptive radiation of non-avian dinosaurs and the phenomenal diversification of birds, via continuing rapid rates of evolution along the phylogenetic stem lineage. This raises the possibility that the uneven distribution of biodiversity results not just from large-scale extrapolation of the process of adaptive radiation in a few extant clades, but also from the maintenance of evolvability on vast time scales across the history of life, in key lineages. C1 [Benson, Roger B. J.] Univ Oxford, Dept Earth Sci, Oxford OX1 3PR, England. [Campione, Nicolas E.] Uppsala Univ, Dept Earth Sci Palaeobiol, Uppsala, Sweden. [Campione, Nicolas E.] Uppsala Univ, Dept Organismal Biol Evolut & Dev, Uppsala, Sweden. [Campione, Nicolas E.; Evans, David C.] Univ Toronto, Dept Ecol & Evolutionary Biol, Toronto, ON, Canada. [Carrano, Matthew T.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Mannion, Philip D.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London, England. [Sullivan, Corwin] Chinese Acad Sci, Inst Vertebrate Paleontol & Paleoanthropol, Key Lab Vertebrate Evolut & Human Origins, Beijing, Peoples R China. [Upchurch, Paul] UCL, Dept Earth Sci, London, England. [Evans, David C.] Royal Ontario Museum, Dept Nat Hist, Toronto, ON M5S 2C6, Canada. RP Benson, RBJ (reprint author), Univ Oxford, Dept Earth Sci, Oxford OX1 3PR, England. EM roger.benson@earth.ox.ac.uk RI Upchurch, Paul/C-1654-2008; Carrano, Matthew/C-7601-2011; OI Carrano, Matthew/0000-0003-2129-1612; Campione, Nicolas/0000-0002-4205-9794; Benson, Roger/0000-0001-8244-6177 FU Leverhulme Research Grant [RPG-129]; Imperial College Junior Research Fellowship FX Parts of this project were supported by a Leverhulme Research Grant (to Paul Upchurch) RPG-129. PDM is funded by an Imperial College Junior Research Fellowship. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 95 TC 57 Z9 57 U1 10 U2 69 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1545-7885 J9 PLOS BIOL JI PLoS. Biol. PD MAY PY 2014 VL 12 IS 5 AR e1001853 DI 10.1371/journal.pbio.1001853 PG 11 WC Biochemistry & Molecular Biology; Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics GA AI6GD UT WOS:000336969200004 PM 24802911 ER PT J AU Ryan, MJ AF Ryan, Michael J. TI When seeing is deceiving: a comment on Kelley and Kelley SO BEHAVIORAL ECOLOGY LA English DT Editorial Material ID SIGNALS C1 [Ryan, Michael J.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Ryan, MJ (reprint author), Univ Texas Austin, Dept Integrat Biol, 1 Univ Stn C0990, Austin, TX 78712 USA. EM mryan@utexas.edu NR 8 TC 1 Z9 1 U1 2 U2 10 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 EI 1465-7279 J9 BEHAV ECOL JI Behav. Ecol. PD MAY-JUN PY 2014 VL 25 IS 3 BP 466 EP 467 DI 10.1093/beheco/aru036 PG 2 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA AH9TQ UT WOS:000336486100007 ER PT J AU Martinson, EO Jander, KC Peng, YQ Chen, HH Machado, CA Arnold, AE Herre, EA AF Martinson, Ellen O. Jander, K. Charlotte Peng, Yan-Qiong Chen, Huan-Huan Machado, Carlos A. Arnold, A. Elizabeth Allen Herre, Edward TI Relative investment in egg load and poison sac in fig wasps: Implications for physiological mechanisms underlying seed and wasp production in figs SO ACTA OECOLOGICA-INTERNATIONAL JOURNAL OF ECOLOGY LA English DT Article DE Figs; Pollinator wasps; Parasitic wasps; Poison sac; Eggs; Galls; Reproductive investment; Mutualism ID NON-POLLINATING WASPS; NEW-WORLD; HISTORICAL BIOGEOGRAPHY; HOST-SPECIFICITY; EVOLUTION; MUTUALISM; FICUS; HYMENOPTERA; CHALCIDOIDEA; COEVOLUTION AB Fig pollinating wasps and most non-pollinator wasps apply secretions from their poison sacs into oviposited flowers that appear necessary to the formation of the galls that their developing offspring consume. Thus, both eggs and poison sac secretions appear to be essential for wasp reproduction, but the relative investment in each is unknown. We measured relative investment in poison sac and egg production in pollinating and non-pollinating wasps associated with seven species of monoecious Panamanian figs representing both active and passive pollination syndromes. We then collected similar data for four fig hosts in China, where some wasp species in the genus Eupristina have lost the ability to pollinate ("cheaters"). All wasps examined possessed large poison sacs, and we found a strong positive correlation between poison sac size and absolute egg production. In the Panamanian species, the relative poison sac to egg investment was highest in the externally ovipositing non-pollinator-wasps, followed by active pollinators, then by passive pollinators. Further, pollinator wasps of fig species with demonstrated host sanctions against "cheating" wasps showed higher investment in the poison sac than wasps of species without sanctions. In the Chinese samples, relative investment in the poison sac was indistinguishable between pollinators and "cheaters" associated with the same fig species. We suggest that higher relative investment in poison sac across fig wasp species reflects higher relative difficulty in initiating formation of galls and subsequently obtaining resources from the fig. We discuss the implications for the stability of the fig-wasp mutualism, and for the ability of non-pollinators to exploit this mutualism. Published by Elsevier Masson SAS. C1 [Martinson, Ellen O.; Arnold, A. Elizabeth] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. [Jander, K. Charlotte] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. [Peng, Yan-Qiong; Chen, Huan-Huan] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Key Lab Trop Forest Ecol, Kunming, Peoples R China. [Machado, Carlos A.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Allen Herre, Edward] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Herre, EA (reprint author), Smithsonian Trop Res Inst, Balboa, Ancon, Panama. EM herrea@si.edu RI Machado, Carlos/B-8855-2009 OI Machado, Carlos/0000-0003-1546-7415 FU National Science Foundation; Smithsonian Institute; Yale University FX We gratefully acknowledge the National Science Foundation for supporting this research (NSF Graduate Research Fellowship to EOS), as well as the Smithsonian Institute (Predoctoral Fellowship to EOS; laboratory and facilities support to EAH and KCJ), Yale University (KCJ). We thank the Smithsonian Tropical Research Institute for logistical support and the government of Panama for permission to carry out this research. We are grateful to A. Gomez for technical assistance and S. Jansen-Gonzalez, R.A.S. Pereira, F. Kjellberg, J.J. Van Alphen, and V. Martinson for helpful discussion, and R.M. Borges, Finn Kjellberg, and two anonymous reviewers for useful comments on previous drafts. NR 64 TC 7 Z9 7 U1 2 U2 19 PU GAUTHIER-VILLARS/EDITIONS ELSEVIER PI PARIS PA 23 RUE LINOIS, 75015 PARIS, FRANCE SN 1146-609X EI 1873-6238 J9 ACTA OECOL JI Acta Oecol.-Int. J. Ecol. PD MAY PY 2014 VL 57 SI SI BP 58 EP 66 DI 10.1016/j.actao.2013.07.009 PG 9 WC Ecology SC Environmental Sciences & Ecology GA AH5SI UT WOS:000336191000009 ER PT J AU Errmann, R Torres, G Schmidt, TOB Seeliger, M Howard, AW Maciejewski, G Neuhauser, R Meibom, S Kellerer, A Dimitrov, DP Dincel, B Marka, C Mugrauer, M Ginski, C Adam, C Raetz, S Schmidt, JG Hohle, MM Berndt, A Kitze, M Trepl, L Moualla, M Eisenbeiss, T Fiedler, S Dathe, A Graefe, C Pawellek, N Schreyer, K Kjurkchieva, DP Radeva, VS Yotov, V Chen, WP Hu, SCL Wu, ZY Zhou, X Pribulla, T Budaj, J Vanko, M Kundra, E Hambalek, L Krushevska, V Bukowiecki, L Nowak, G Marschall, L Terada, H Tomono, D Fernandez, M Sota, A Takahashi, H Oasa, Y Briceno, C Chini, R Broeg, CH AF Errmann, R. Torres, G. Schmidt, T. O. B. Seeliger, M. Howard, A. W. Maciejewski, G. Neuhaeuser, R. Meibom, S. Kellerer, A. Dimitrov, D. P. Dincel, B. Marka, C. Mugrauer, M. Ginski, Ch Adam, Ch Raetz, St Schmidt, J. G. Hohle, M. M. Berndt, A. Kitze, M. Trepl, L. Moualla, M. Eisenbeiss, T. Fiedler, S. Dathe, A. Graefe, Ch. Pawellek, N. Schreyer, K. Kjurkchieva, D. P. Radeva, V. S. Yotov, V. Chen, W. P. Hu, S. C. -L. Wu, Z. -Y. Zhou, X. Pribulla, T. Budaj, J. Vanko, M. Kundra, E. Hambalek, L. Krushevska, V. Bukowiecki, L. Nowak, G. Marschall, L. Terada, H. Tomono, D. Fernandez, M. Sota, A. Takahashi, H. Oasa, Y. Briceno, C. Chini, R. Broeg, C. H. TI Investigation of a transiting planet candidate in Trumpler 37: An astrophysical false positive eclipsing spectroscopic binary star SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE open clusters and associations: individual (Trumpler 37); binaries: eclipsing; binaries: spectroscopic; planetary systems; stars: fundamental parameters; stars: late-type ID INTERMEDIATE-MASS STARS; SKY SURVEY 2MASS; INITIAL CONDITIONS; EXTRASOLAR PLANET; FORMING REGIONS; CEPHEUS OB2; ACCRETION; EVOLUTION; SPECTRA; SPECTROGRAPH AB We report our investigation of the first transiting planet candidate from the YETI project in the young (approximate to 4 Myr old) open cluster Trumpler 37. The transit-like signal detected in the lightcurve of F8V star 2M21385603+5711345 repeats every 1.364894 + 0.000015 days, and has a depth of 54.5 + 0.8 mmag in R. Membership in the cluster is supported by its mean radial velocity and location in the color-magnitude diagram, while the Li diagnostic and proper motion are inconclusive in this regard. Follow-up photometric monitoring and adaptive optics imaging allow us to rule out many possible blend scenarios, but our radial-velocity measurements show it to be an eclipsing single-lined spectroscopic binary with a late-type (mid-M) stellar companion, rather than one of planetary nature. The estimated mass of the companion is 0.15-0.44 M. The search for planets around very young stars such as those targeted by the YETI survey remains of critical importance to understand the early stages of planet formation and evolution. ((c) 2014 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) C1 [Errmann, R.; Schmidt, T. O. B.; Seeliger, M.; Neuhaeuser, R.; Dincel, B.; Marka, C.; Mugrauer, M.; Ginski, Ch; Adam, Ch; Raetz, St; Schmidt, J. G.; Hohle, M. M.; Berndt, A.; Kitze, M.; Trepl, L.; Moualla, M.; Eisenbeiss, T.; Fiedler, S.; Dathe, A.; Pawellek, N.; Schreyer, K.] Inst Astrophys, D-07745 Jena, Germany. [Errmann, R.; Schmidt, T. O. B.; Seeliger, M.; Neuhaeuser, R.; Dincel, B.; Marka, C.; Mugrauer, M.; Ginski, Ch; Adam, Ch; Raetz, St; Schmidt, J. G.; Hohle, M. M.; Berndt, A.; Kitze, M.; Trepl, L.; Moualla, M.; Eisenbeiss, T.; Fiedler, S.; Dathe, A.; Pawellek, N.; Schreyer, K.] Univ Sternwarte, D-07745 Jena, Germany. [Errmann, R.] Univ Jena, Abbe Ctr Photon, D-07743 Jena, Germany. [Torres, G.; Meibom, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howard, A. W.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Maciejewski, G.; Bukowiecki, L.] Nicholas Copernicus Univ, Ctr Astron, Fac Phys, PL-87100 Torun, Poland. [Kellerer, A.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Kellerer, A.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Dimitrov, D. P.] Inst Astron, Sofia 1784, Bulgaria. [Dimitrov, D. P.] NAO, Sofia 1784, Bulgaria. [Graefe, Ch.] Univ Kiel, D-24098 Kiel, Germany. [Kjurkchieva, D. P.; Radeva, V. S.; Yotov, V.] Univ Shumen, Shumen 9700, Bulgaria. [Chen, W. P.; Hu, S. C. -L.] Natl Cent Univ, Grad Inst Astron, Jhongli 32001, Taiwan. [Hu, S. C. -L.] Taipei Astron Museum, Taipei 11160, Taiwan. [Wu, Z. -Y.; Zhou, X.] Chinese Acad Sci, Key Lab Opt Astron, NAO, Beijing 100012, Peoples R China. [Pribulla, T.; Budaj, J.; Vanko, M.; Kundra, E.; Hambalek, L.] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia. [Budaj, J.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Krushevska, V.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine. [Nowak, G.] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Nowak, G.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Marschall, L.] Gettysburg Coll Observ, Dept Phys, Gettysburg, PA 17325 USA. [Terada, H.; Tomono, D.] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Fernandez, M.; Sota, A.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Takahashi, H.] Univ Tokyo, Inst Astron, Tokyo 1810015, Japan. [Oasa, Y.] Saitama Univ, Dept Astron & Earth Sci, Sakura Ku, Saitama 3388570, Japan. [Briceno, C.] Ctr Invest Astron, Merida 5101, Venezuela. [Briceno, C.] Cerro Tololo Interamer Observ CTIO, La Serena, Chile. [Chini, R.] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany. [Chini, R.] Univ Catolica Norte, Inst Astron, Antofagasta, Chile. [Broeg, C. H.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. RP Errmann, R (reprint author), Inst Astrophys, Schillergasschen 2-3, D-07745 Jena, Germany. EM ronny.errmann@uni-jena.de RI Maciejewski, Gracjan/D-6241-2014; Howard, Andrew/D-4148-2015; Nowak, Grzegorz/H-8234-2014; Dimitrov, Dinko/J-7682-2013 OI Howard, Andrew/0000-0001-8638-0320; Nowak, Grzegorz/0000-0002-7031-7754; FU DFG [SPP 1385, NE 515 / 34-1, 34-2, SCHR 665 / 7-1, MU 2695 / 13-1, NE 515 / 35-1, 35-2, NE 515 / 33-1, 33-2]; Bulgarian National Science Fund [DDVU 02/40-2010]; Chinese National Natural Science Foundation grant [11373033]; National Nature Science Foundation of China [U1231113]; Chinese Academy of Science [U1231113]; Chinese National Natural Science Foundation [11073032]; National Basic Research Program of China (973 Program) [2014CB845704, 2013CB834902]; VEGA Grant of the Slovak Academy of Sciences [2/0143/13]; Thuringian government [B 515-07010] FX RN, MK, and RE would like to thank DFG for support in the Priority Programme SPP 1385 on the "First Ten Million Years of the Solar System" in project NE 515 / 34-1 and 34-2. BD, JGS, MMH, LT, TE, and RN thank DFG in SFB TR 7 in TPs C2, C7, and B9. CM and KS thank DFG in project SCHR 665 / 7-1. CG and MM thank DFG in project MU 2695 / 13-1. CA thanks DFG in project NE 515 / 35-1 and 35-2 in SPP 1385. SR and TR thanks DFG in project NE 515 / 33-1 and 33-2 in SPP 1385. NP thanks DFG in project KR 2164 / 10-1. DD acknowledges the partial financial support of the project DDVU 02/40-2010 of the Bulgarian National Science Fund. Wu, Z.Y. was supported by the Chinese National Natural Science Foundation grant No. 11373033. This work was also supported by the joint fund of Astronomy of the National Nature Science Foundation of China and the Chinese Academy of Science, under Grant U1231113. Zhou, X. was supported by the Chinese National Natural Science Foundation grands No. 11073032, and by the National Basic Research Program of China (973 Program), No. 2014CB845704, and 2013CB834902.; This work has been supported by a VEGA Grant 2/0143/13 of the Slovak Academy of Sciences. We would like to acknowledge financial support from the Thuringian government (B 515-07010) for the STK CCD camera used in this project. 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 52 TC 6 Z9 6 U1 0 U2 5 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD MAY PY 2014 VL 335 IS 4 BP 345 EP 356 DI 10.1002/asna.201412047 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8JV UT WOS:000335665600001 ER PT J AU Comizzoli, P AF Comizzoli, Pierre TI Saving Species Through Cryobiology - Filling the Gap Between Technology and Ecology SO IN VITRO CELLULAR & DEVELOPMENTAL BIOLOGY-ANIMAL LA English DT Meeting Abstract C1 [Comizzoli, Pierre] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC USA. EM comizzolip@si.edu NR 0 TC 0 Z9 0 U1 1 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1071-2690 EI 1543-706X J9 IN VITRO CELL DEV-AN JI In Vitro Cell. Dev. Biol.-Anim. PD MAY PY 2014 VL 50 SU 1 BP S1 EP S1 PG 1 WC Cell Biology; Developmental Biology SC Cell Biology; Developmental Biology GA AH8KN UT WOS:000336386800002 ER PT J AU Hagedorn, M AF Hagedorn, Mary TI Coral Cryopreservation Offsetting Climate Change on Reefs SO IN VITRO CELLULAR & DEVELOPMENTAL BIOLOGY-ANIMAL LA English DT Meeting Abstract C1 [Hagedorn, Mary] Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. EM hagedornm@si.edu NR 0 TC 0 Z9 0 U1 0 U2 9 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1071-2690 EI 1543-706X J9 IN VITRO CELL DEV-AN JI In Vitro Cell. Dev. Biol.-Anim. PD MAY PY 2014 VL 50 SU 1 BP S2 EP S2 PG 1 WC Cell Biology; Developmental Biology SC Cell Biology; Developmental Biology GA AH8KN UT WOS:000336386800004 ER PT J AU Font-Ribera, A Kirkby, D Busca, N Miralda-Escude, J Ross, NP Slosar, A Rich, J Aubourg, E Bailey, S Bhardwaj, V Bautista, J Beutler, F Bizyaev, D Blomqvist, M Brewington, H Brinkmann, J Brownstein, JR Carithers, B Dawson, KS Delubac, T Ebelke, G Eisenstein, DJ Ge, J Kinemuchi, K Lee, KG Malanushenko, V Malanushenko, E Marchante, M Margala, D Muna, D Myers, AD Noterdaeme, P Oravetz, D Palanque-Delabrouille, N Paris, I Petitjean, P Pieri, MM Rossi, G Schneider, DP Simmons, A Viel, M Yeche, C York, DG AF Font-Ribera, Andreu Kirkby, David Busca, Nicolas Miralda-Escude, Jordi Ross, Nicholas P. Slosar, Arze Rich, James Aubourg, Eric Bailey, Stephen Bhardwaj, Vaishali Bautista, Julian Beutler, Florian Bizyaev, Dmitry Blomqvist, Michael Brewington, Howard Brinkmann, Jon Brownstein, Joel R. Carithers, Bill Dawson, Kyle S. Delubac, Timothee Ebelke, Garrett Eisenstein, Daniel J. Ge, Jian Kinemuchi, Karen Lee, Khee-Gan Malanushenko, Viktor Malanushenko, Elena Marchante, Moses Margala, Daniel Muna, Demitri Myers, Adam D. Noterdaeme, Pasquier Oravetz, Daniel Palanque-Delabrouille, Nathalie Paris, Isabelle Petitjean, Patrick Pieri, Matthew M. Rossi, Graziano Schneider, Donald P. Simmons, Audrey Viel, Matteo Yeche, Christophe York, Donald G. TI Quasar-Lyman a forest cross-correlation from BOSS DR11: Baryon Acoustic Oscillations SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE Lyman alpha forest; baryon acoustic oscillations; redshift surveys; dark energy experiments ID DIGITAL SKY SURVEY; LY-ALPHA FOREST; DATA RELEASE 9; 9TH DATA RELEASE; SPECTROSCOPIC SURVEY; SDSS-III; TARGET SELECTION; DARK ENERGY; POWER-SPECTRUM; SUPERNOVAE AB We measure the large-scale cross-correlation of quasars with the Ly alpha forest absorption, using over 164,000 quasars from Data Release 11 of the SDSS-III Baryon Oscillation Spectroscopic Survey. We extend the previous study of roughly 60,000 quasars from Data Release 9 to larger separations, allowing a measurement of the Baryonic Acoustic Oscillation (BAO) scale along the line of sight cl(H(z = 2.36) r(s)) = 9.0 +/- 0.3 and across the line of sight DA(z = 2.36) / r(s) = 10.8 +/- 0.4, consistent with CMB and other BAO data. Using the best fit value of the sound horizon from Planck data (r(s) = 147.49 Mpc), we can translate these results to a measurement of the Hubble parameter of H(z = 2.36) = 226 +/- 8km s(-1)Mpc(-1) and of the angular diameter distance of DA(z = 2.36) = 1590 +/- 60 Mpc. The measured cross-correlation function and an update of the code to fit the BAO scale (baofit) are made publicly available. C1 [Font-Ribera, Andreu] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland. [Font-Ribera, Andreu; Ross, Nicholas P.; Bailey, Stephen; Bhardwaj, Vaishali; Beutler, Florian; Carithers, Bill] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Kirkby, David; Blomqvist, Michael; Margala, Daniel] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Busca, Nicolas; Aubourg, Eric; Bautista, Julian] Univ Paris 07, CNRS IN2P3, CEA, Observ Paris,APC, Paris, France. [Miralda-Escude, Jordi] Inst Ciencies Cosmos IEEC UB, Barcelona 08028, Catalonia, Spain. [Miralda-Escude, Jordi] Inst Catalana Recerca & Estudis Avancats, Barcelona 08010, Catalonia, Spain. [Ross, Nicholas P.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Slosar, Arze] Brookhaven Natl Lab, Upton, NY 11375 USA. [Bhardwaj, Vaishali; Bizyaev, Dmitry; Kinemuchi, Karen; Marchante, Moses; Oravetz, Daniel; Simmons, Audrey] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Brewington, Howard; Brinkmann, Jon; Ebelke, Garrett; Malanushenko, Viktor; Malanushenko, Elena] Apache Point Observ, Sunspot, NM 88349 USA. [Brewington, Howard; Brinkmann, Jon; Ebelke, Garrett; Malanushenko, Viktor; Malanushenko, Elena] New Mexico State Univ, Sunspot, NM 88349 USA. [Brownstein, Joel R.; Dawson, Kyle S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Rich, James; Delubac, Timothee; Palanque-Delabrouille, Nathalie; Rossi, Graziano; Yeche, Christophe] CEA, Ctr Saclay, IRFU, F-91191 Gif Sur Yvette, France. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ge, Jian] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Lee, Khee-Gan] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Muna, Demitri] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron 3905, Laramie, WY 82071 USA. [Noterdaeme, Pasquier; Petitjean, Patrick] CNRS UPMC, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. [Paris, Isabelle] Univ Chile, Dept Astron, Santiago, Chile. [Pieri, Matthew M.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Viel, Matteo] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Viel, Matteo] Ist Nazl Fis Nucl, I-34127 Trieste, Italy. [York, Donald G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60615 USA. [York, Donald G.] Univ Chicago, Fermi Inst, Chicago, IL 60615 USA. RP Font-Ribera, A (reprint author), Univ Zurich, Inst Theoret Phys, Winterthurerstr 190, CH-8057 Zurich, Switzerland. EM font@physik.uzh.ch FU Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; Spanish grant [AYA2012-33938]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX This research used resources of the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. DK would like to thank CEA Saclay for their hospitality and productive environment during his sabbatical. JM is supported in part by Spanish grant AYA2012-33938.; 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.sdssRorg/. Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 47 TC 65 Z9 66 U1 3 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD MAY PY 2014 IS 5 AR 027 DI 10.1088/1475-7516/2014/05/027 PG 26 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AH4JC UT WOS:000336092200029 ER PT J AU Yeshurun, R Bar-Oz, G Weinstein-Evron, M AF Yeshurun, Reuven Bar-Oz, Guy Weinstein-Evron, Mina TI Intensification and sedentism in the terminal Pleistocene Natufian sequence of el-Wad Terrace (Israel) SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Epipaleolithic; Levant; Zooarchaeology; Broad-spectrum revolution; Mobility; Contextual taphonomy ID BROAD-SPECTRUM REVOLUTION; MOUNT-CARMEL; SOUTHERN LEVANT; EPIPALAEOLITHIC SITE; RAQEFET CAVE; CUT MARKS; ARCHAEOLOGICAL EVIDENCE; HAMMERSTONE PERCUSSION; PALEOLITHIC DEMOGRAPHY; GAZELLA-GAZELLA AB Measuring subsistence intensification in the archaeofaunal record has provided strong evidence for socioeconomic shifts related to sedentarization in the terminal Pleistocene Mediterranean Basin, but the precise timing and scale of the intensification trend and its place in the evolution of settled societies remain contentious. New archaeofaunal data from the key Natufian sequence of el-Wad Terrace (Mount Carmel, Israel, ca. 15.0-11.7 ka [thousands of years ago]) is used here to clarify and contextualize paleoeconomy and mobility trends in the latest Pleistocene Levant, representing the culmination of Epipaleolithic subsistence strategies. Taphonomic variables serve as supplementary indicators of habitation function and occupation intensity along the sequence. At el-Wad, a very broad range of animals, mostly small to medium in size, were captured and consumed. Consumption leftovers were discarded in intensively occupied domestic spaces and suffered moderate attrition. The Early (ca. 15.0-13.7/13.0 ka) and Late (ca. 13.7/13.0-11.7 ka) Natufian phases display some differences in prey exploitation and taphonomic markers of occupation intensity, corresponding with other archaeological signals. We further set the intra-Natufian taxonomic and demographic trends in perspective by considering the earlier Epipaleolithic sequence of the same region, the Israeli coastal plain. Consequently, we show that the Early Natufian record constituted an important dietary shift related to greater occupation intensity and sedentarization, rather than a gradual development, and that the Late Natufian record appears to be maintaining, if not amplifying, many of these novel signals. These conclusions are important for understanding the mode and tempo of the transition to settled life in human evolution. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Yeshurun, Reuven; Bar-Oz, Guy; Weinstein-Evron, Mina] Univ Haifa, Zinman Inst Archaeol, IL-3498838 Haifa, Israel. [Yeshurun, Reuven] Smithsonian Inst, Program Human Ecol & Archaeobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Yeshurun, R (reprint author), Univ Haifa, Zinman Inst Archaeol, IL-3498838 Haifa, Israel. EM ryeshuru@research.haifa.ac.il; guybar@research.haifa.ac.il; evron@research.haifa.ac.il FU Hecht Scholarship; Wolf Foundation Scholarship; Carmel Research Center Grant; Smithsonian Institution; Wenner-Gren Foundation; Care Foundation; Faculty of Humanities, University of Haifa; Dan David Foundation FX This paper is based on R.Y.'s doctoral research at the University of Haifa, generously funded by the Graduate Studies Authority, the Hecht Scholarship, the Wolf Foundation Scholarship and the Carmel Research Center Grant. The manuscript was written during his Fulbright post-doctoral fellowship in the Smithsonian Institution. We thank D. Kaufman for his help throughout this research and for commenting on a previous draft and A. Regev for graphic assistance. The paper greatly benefitted from the helpful comments and suggestions by the editors and two anonymous reviewers. The renewed excavation at el-Wad Terrace is sponsored by the Wenner-Gren Foundation, the Care Foundation and the Faculty of Humanities, University of Haifa. Thanks are also due to the Dan David Foundation and to Sarah and Avie Arenson for their support. NR 163 TC 10 Z9 10 U1 2 U2 16 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD MAY PY 2014 VL 70 BP 16 EP 35 DI 10.1016/j.jhevol.2014.02.011 PG 20 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA AH4RT UT WOS:000336116400002 PM 24661906 ER PT J AU Prothero, DR Campbell, KE Beatty, BL Frailey, CD AF Prothero, Donald R. Campbell, Kenneth E., Jr. Beatty, Brian L. Frailey, Carl D. TI NEW LATE MIOCENE DROMOMERYCINE ARTIODACTYL FROM THE AMAZON BASIN: IMPLICATIONS FOR INTERCHANGE DYNAMICS SO JOURNAL OF PALEONTOLOGY LA English DT Article ID SEA-LEVEL; PANAMA; CLOSURE; STRATIGRAPHY; BIOGEOGRAPHY; CIRCULATION; LANDSCAPE; EVOLUTION; ATLANTIC; MAMMALIA AB A new dromomerycine palaeomerycid artiodactyl, Surameryx acrensis new genus new species, from upper Miocene deposits of the Amazon Basin documents the first and only known occurrence of this Northern Hemisphere group in South America. Osteological characters place the new taxon among the earliest known dromomerycine artiodactyls, most similar to Barbouromeryx trigonocorneus, which lived in North America during the early to middle Miocene, 20-16 Ma. Although it has long been assumed that the Great American Biotic Interchange (GABI) began with the closure of the Isthmus of Panama in the late Pliocene, or ca. 3.0-2.5 Ma, the presence of this North American immigrant in Amazonia is further evidence that terrestrial connections between North America and South America through Panama existed as early as the early late Miocene, or ca. 9.5 Ma. This early interchange date was previously indicated by approximately coeval specimens of proboscideans, peccaries, and tapirs in South America and ground sloths in North America. Although palaeomerycids apparently never flourished in South America, proboscideans thrived there until the end of the Pleistocene, and peccaries and tapirs diversified and still live there today. C1 [Prothero, Donald R.; Campbell, Kenneth E., Jr.] Nat Hist Museum Los Angeles Cty, Los Angeles, CA 90007 USA. [Beatty, Brian L.] Coll Osteopath Med, New York Inst Technol, Old Westbury, NY 11568 USA. [Beatty, Brian L.] Smithsonian Inst, United States Natl Museum, Washington, DC 20560 USA. [Beatty, Brian L.] Virginia Museum Nat Hist, Martinsville, VA 24112 USA. [Frailey, Carl D.] Johnson Cty Community Coll, Dept Sci, Overland Pk, KS 66210 USA. RP Prothero, DR (reprint author), Nat Hist Museum Los Angeles Cty, 900 Exposition Blvd, Los Angeles, CA 90007 USA. EM donaldprothero@att.net; kcampbell@nhm.org; bbeatty@nyit.edu; cfrailey@jccc.edu NR 76 TC 4 Z9 4 U1 2 U2 10 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 EI 1937-2337 J9 J PALEONTOL JI J. Paleontol. PD MAY PY 2014 VL 88 IS 3 BP 434 EP 443 DI 10.1666/13-022 PG 10 WC Paleontology SC Paleontology GA AH5IQ UT WOS:000336162300003 ER PT J AU John Pojeta, ML AF John Pojeta, Mary Lou TI Presentation of the Pojeta Award of the Paleontological Society to John and Mary Lou Pojeta RESPONSE SO JOURNAL OF PALEONTOLOGY LA English DT Editorial Material C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP John (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 EI 1937-2337 J9 J PALEONTOL JI J. Paleontol. PD MAY PY 2014 VL 88 IS 3 BP 629 EP 630 PG 2 WC Paleontology SC Paleontology GA AH5IQ UT WOS:000336162300024 ER PT J AU DiMattina, M Gordon, JD Botes, A Celia, G Payson, M Graves-Herring, J AF DiMattina, Michael Gordon, John David Botes, Awie Celia, Gerald Payson, Mark Graves-Herring, Jennifer TI Follicular and Estradiol Parameters That Improve Success with Natural Cycle in Vitro Fertilization SO JOURNAL OF REPRODUCTIVE MEDICINE LA English DT Article DE assisted reproductive technologies; in vitro fertilization; in vitro oocyte maturation; infertility; natural cycle IVF; unstimulated IVF ID CUMULATIVE PREGNANCY RATES; OVARIAN STIMULATION; UNSTIMULATED IVF; EMBRYO-TRANSFER; EXPERIENCE; OPINIONS; SART AB OBJECTIVE: To describe clinical thresholds for follicle size and estradiol levels to optimize success with natural cycle in vitro fertilization (NCIVF). STUDY DESIGN: Descriptive cohort of candidates for stimulated IVF, <43 years old, with regular menstrual cycles, regardless of ovarian reserve or fertility treatment NCIVF, defined as oocyte retrieval, fertilization and embryo transfer after human chorionic gonadotropin (hCG) trigger without luteinizing hormone (LH) suppression or ovarian stimulation medications. RESULTS: A total of 422 patients underwent 821 NCIVF cycles. Clinical pregnancy rates per cycle start, retrieval, and transfer were 13%, 17%, and 32%, respectively, for all patients and 19%, 25%, and 49% for patients <30 years old. The threshold estradiol level on day of hCG was 101 pg/mL; below that level no clinical pregnancies occurred. Likewise, a mean follicular diameter >15 mm was the optimal, threshold for hCG trigger, Anti-Miillerian hormone and follicle-stimulating hormone levels did not predict success in NCIVF, and no statistical difference in clinical pregnancy rates between day 3 or day 5 embryo transfer was observed. CONCLUSION: NCIVF is an effective therapy for infertile patients regardless of their ovarian reserve. Cycle cancellation due to a premature LH surge can be reduced, without sacrificing success, by triggering smaller follicles above a threshold level of estradiol. C1 [DiMattina, Michael] Domin Fertil, Arlington, VA 22204 USA. Smithsonian Conservat Biol Inst, Dept Reprod Med, Washington, DC USA. Inova Fairfax Hosp Womens Ctr, Falls Church, VA USA. RP DiMattina, M (reprint author), Domin Fertil, 46 South Glebe Rd, Arlington, VA 22204 USA. EM mikedima@mac.com NR 22 TC 2 Z9 2 U1 0 U2 0 PU SCI PRINTERS & PUBL INC PI ST LOUIS PA PO DRAWER 12425 8342 OLIVE BLVD, ST LOUIS, MO 63132 USA SN 0024-7758 EI 1943-3565 J9 J REPROD MED JI J. Reprod. Med. PD MAY-JUN PY 2014 VL 59 IS 5-6 BP 267 EP 273 PG 7 WC Obstetrics & Gynecology SC Obstetrics & Gynecology GA AH8WS UT WOS:000336419500016 PM 24937968 ER PT J AU Gregory, T Rueda, FC Deichmann, J Kolowski, J Alonso, A AF Gregory, Tremaine Rueda, Farah Carrasco Deichmann, Jessica Kolowski, Joseph Alonso, Alfonso TI Arboreal camera trapping: taking a proven method to new heights SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE camera trap; canopy research methods; Lower Urubamba; Peruvian Amazon AB 1. Although camera trapping has been shown to be a highly effective non-invasive tool for wildlife monitoring, the technique has not yet been widely applied to studies of arboreal species. Despite the unique challenges that camera trapping in the canopy poses, its versatility and relatively non-invasive nature, combined with recent technological improvements on the cameras themselves, make camera trapping a highly useful tool for arboreal research. 2. We present data on the methodology and effectiveness of arboreal camera trapping during the first 6 months of a year-long study in the Lower Urubamba Region of Peru investigating animal use of natural crossing points (i.e. branches) over a natural gas pipeline clearing. We placed Reconyx PC800 Hyperfire cameras in 25 crossing points of 13 distinct natural canopy 'bridges' at a mean height of 26.8m. 3. After 6 months of data collection, we logged 1522 photoevents, recording 20 mammal, 23 bird and four reptile species. An analysis of animal passing events in front of the cameras over time did not suggest any negative response to camera presence. While we found that cameras in the canopy are triggered more frequently by non-target stimuli (e.g. leaves) than cameras on the ground, we demonstrated significantly reduced false triggering following leaf removal within 1.5 m of the camera. 4. Our results suggest that arboreal camera trapping can provide robust documentation of a diversity of vertebrate species engaged in a variety of activities, and we provide recommendations for other researchers interested in using in this method. This is the most extensive arboreal camera trapping study to date in terms of the length of the study period, the number of cameras being used and the height of the cameras in the trees. Therefore, lessons provided from this experience can be used to improve the design of future arboreal camera trap studies. C1 [Gregory, Tremaine; Rueda, Farah Carrasco; Deichmann, Jessica; Kolowski, Joseph; Alonso, Alfonso] Smithsonian Conservat Biol Inst, Ctr Conservat Educ & Sustainabil, Washington, DC 20013 USA. [Rueda, Farah Carrasco] Univ Florida, Sch Nat Resources & Environm, Gainesville, FL 32611 USA. RP Gregory, T (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat Educ & Sustainabil, Natl Zool Pk, Washington, DC 20013 USA. EM gregoryt@si.edu OI Carrasco-Rueda, Farah/0000-0003-1686-2249 FU Repsol Exploracion Peru FX We thank five anonymous reviewers for their valuable comments on previous drafts of this manuscript. We thank Stanford W. Gregory, Jr. for camera tree mount design support, Sophia Celino, Guillermo Joo Novoa, Matthijs Schuring and Drew Hart for valuable support in photoprocessing, and Sulema Castro, Tatiana Pacheco, and Marcel Costa for administrative and logistics support. For identification of mammals and birds, we thank Louise Emmons, Robert Voss, Daniel Lane and Grace Servat. We also thank our field nurses, support staff and local guides from the communities of Camisea and Shivankoreni. This is contribution 16 of the Peru Biodiversity Program. We thank Repsol Exploracion Peru for financial and logistical support. This research was conducted under the Peruvian government's Direccion General Forestal y de Fauna Silvestre Resolucion Directoral No. 0221-2011-AG-DGFFS-DGEFFS, No. 0197-2012-AG-DGFFS-DGEFFS and No. 0265-2012-AG-DGFFS-DGEFFS. NR 19 TC 14 Z9 15 U1 7 U2 60 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X EI 2041-2096 J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD MAY PY 2014 VL 5 IS 5 BP 443 EP 451 DI 10.1111/2041-210X.12177 PG 9 WC Ecology SC Environmental Sciences & Ecology GA AH9YA UT WOS:000336500500005 ER PT J AU Fleming, CH Calabrese, JM Mueller, T Olson, KA Leimgruber, P Fagan, WF AF Fleming, Christen H. Calabrese, Justin M. Mueller, Thomas Olson, Kirk A. Leimgruber, Peter Fagan, William F. TI Non-Markovian maximum likelihood estimation of autocorrelated movement processes SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE autocorrelation function; characteristic scale; home range; irregular sampling; Mongolian gazelle; movement ecology; Procapra gutturosa; satellite collar movement data; time series; tracking data gaps ID CORRELATED RANDOM-WALK; ANIMAL MOVEMENT; HOME-RANGE; TELEMETRY DATA; SPACED DATA; MODELS; PATTERNS; SYSTEMS AB By viewing animal movement paths as realizations of a continuous stochastic process, we introduce a rigorous likelihood method for estimating the statistical parameters of movement processes. This method makes no assumption of a hidden Markov property, places no special emphasis on the sampling rate, is insensitive to irregular sampling and data gaps, can produce reasonable estimates with limited sample sizes and can be used to assign AIC values to a vast array of qualitatively different models of animal movement at the individual and population levels. To develop our approach, we consider the likelihood of the first two cumulants of stochastic processes, the mean and autocorrelation functions. Together, these measures provide a considerable degree of information regarding searching, foraging, migration and other aspects of animal movement. As a specific example, we develop the likelihood analyses necessary to contrast performance of animal movement models based on Brownian motion, the Ornstein-Uhlenbeck process and a generalization of the Ornstein-Uhlenbeck process that includes ballistic bouts. We then show how our framework also provides a new and more accurate approach to home-range estimation when compared to estimators that neglect autocorrelation in the movement path. We apply our methods to a data set on Mongolian gazelles (Procapra gutturosa) to identify the movement behaviours and their associated time and length scales that characterize the movement of each individual. Additionally, we show that gazelle annual ranges are vastly larger than those of other non-migratory ungulates. C1 [Fleming, Christen H.; Calabrese, Justin M.; Mueller, Thomas; Olson, Kirk A.; Leimgruber, Peter] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA. [Fleming, Christen H.; Mueller, Thomas; Fagan, William F.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Fleming, CH (reprint author), Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. EM chris.h.fleming@gmail.com RI Calabrese, Justin/B-9131-2012; Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 FU US National Science Foundation ABI [1062411] FX The project was funded by the US National Science Foundation ABI 1062411. We thank Caroline Wick for editorial assistance. NR 48 TC 11 Z9 11 U1 3 U2 30 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X EI 2041-2096 J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD MAY PY 2014 VL 5 IS 5 BP 462 EP 472 DI 10.1111/2041-210X.12176 PG 11 WC Ecology SC Environmental Sciences & Ecology GA AH9YA UT WOS:000336500500007 ER PT J AU Zarowiecki, M Linton, YM Post, RJ Bangs, MJ Htun, PT Hlaing, T Seng, CM Baimai, V Ding, TH Sochantha, T Walton, C AF Zarowiecki, Magdalena Linton, Yvonne-Marie Post, Rory J. Bangs, Michael J. Htun, Pe Than Hlaing, Thaung Seng, Chang Moh Baimai, Visut Trung Ho Ding Sochantha, Tho Walton, Catherine TI Repeated landmass reformation limits diversification in the widespread littoral zone mosquito Anopheles sundaicus sensu lato in the Indo-Oriental Region SO MOLECULAR ECOLOGY LA English DT Article DE isolation with migration; biogeography; speciation; Anopheles epiroticus; mannose phosphate isomerase (Mpi); vicariance ID SOUTH-EAST ASIA; MITOCHONDRIAL-DNA; CELLIA SUNDAICUS; COMPARATIVE PHYLOGEOGRAPHY; ECOLOGICAL SPECIATION; DIPTERA-CULICIDAE; RAIN-FORESTS; GENE FLOW; POPULATION; COMPLEX AB Southeast Asia harbours abundant biodiversity, hypothesized to have been generated by Pliocene and Pleistocene climatic and environmental change. Vicariance between the island of Borneo, the remaining Indonesian archipelago and mainland Southeast Asia caused by elevated sea levels during interglacial periods has been proposed to lead to diversification in the littoral zone mosquito Anopheles (Cellia) sundaicus (Rodenwaldt) sensu lato. To test this biogeographical hypothesis, we inferred the population history and assessed gene flow of A.sundaicus s.l. sampled from 18 populations across its pan-Asian species range, using sequences from mitochondrial cytochrome c oxidase subunit 1 (CO1), the internal transcribed spacer 2 (ITS2) and the mannose phosphate isomerase (Mpi) gene. A hypothesis of ecological speciation for A.sundaicus involving divergent adaptation to brackish and freshwater larval habitats was also previously proposed, based on a deficiency of heterozygotes for Mpi allozyme alleles in sympatry. This hypothesis was not supported by Mpi sequence data, which exhibited no fixed differences between brackish and freshwater larval habitats. Mpi and CO1 supported the presence of up to eight genetically distinct population groupings. Counter to the hypothesis of three allopatric species, divergence was often no greater between Borneo, Sumatra/Java and the Southeast Asian mainland than it was between genetic groupings within these landmasses. An isolation-with-migration (IM) model indicates recurrent gene flow between the current major landmasses. Such gene flow would have been possible during glacial periods when the current landmasses merged, presenting opportunities for dispersal along expanding and contracting coastlines. Consequently, Pleistocene climatic variation has proved a homogenizing, rather than diversifying, force for A.sundaicus diversity. C1 [Zarowiecki, Magdalena] Wellcome Trust Sanger Inst, Parasite Genom Grp, Cambridge CB10 1SA, England. [Linton, Yvonne-Marie] Smithsonian Inst Museum Support Ctr, Walter Reed Biosystemat Unit, Suitland, MD 20746 USA. [Linton, Yvonne-Marie] Walter Reed Army Inst Res, Entomol Branch, Silver Spring, MD 20910 USA. [Post, Rory J.] Liverpool John Moores Univ, Sch Nat Sci & Psychol, Liverpool L3 3AF, Merseyside, England. [Bangs, Michael J.] Int SOS, Publ Hlth & Malaria Control, Kuala Kencana 99920, Papua, Indonesia. [Htun, Pe Than; Hlaing, Thaung] Minist Hlth, Dept Hlth, Natl Malaria Control Programme, Nay Pyi Taw, Myanmar. [Seng, Chang Moh] World Hlth Org Cambodia, Phnom Penh, Cambodia. [Baimai, Visut] Mahidol Univ, Dept Biol, Fac Sci, Bangkok 10400, Thailand. [Trung Ho Ding] Natl Inst Malariol Parasitol & Entomol, Hanoi, Vietnam. [Sochantha, Tho] Natl Ctr Malaria Control Parasitol & Entomol, Phnom Penh, Cambodia. [Walton, Catherine] Univ Manchester, Fac Life Sci, Manchester M13 9PL, Lancs, England. RP Zarowiecki, M (reprint author), Wellcome Trust Sanger Inst, Parasite Genom Grp, Wellcome Trust Genome Campus, Cambridge CB10 1SA, England. EM mz3@sanger.ac.uk OI Zarowiecki, Magdalena/0000-0001-6102-7731 FU Natural History Museum (NHM), London FX The authors wish to thank the Natural History Museum (NHM), London, for funding the PhD study of MZZ. Most of the work was carried out while MZZ, YML and RP were at NHM. We would like to thank U Sein Minh, U Thi Ha and other staff at the Department of Medical Research in Lower Myanmar for help with fieldwork and Dr. Erling Pedersen for providing specimens from Simeulue. This manuscript was prepared in part while YML held a National Research Council Research Associateship Award at the Walter Reed Army Institute of Research. The material to be published reflects the views of the authors and should not be construed to represent those of the US Department of the Army or the US Department of Defence. NR 75 TC 2 Z9 2 U1 2 U2 16 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 2014 VL 23 IS 10 BP 2573 EP 2589 DI 10.1111/mec.12761 PG 17 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA AH0KN UT WOS:000335808900015 PM 24750501 ER PT J AU Farmer, EA AF Farmer, Erica A. TI Codifying Consensus and Constructing Boundaries: Setting the Limits of Appellation d'origine contrOLEE PROTection in bordeaux, france SO POLAR-POLITICAL AND LEGAL ANTHROPOLOGY REVIEW LA English DT Article DE appellation d'origine controlee; boundaries; communal rights; wine; intellectual property; geographical indications; traditional knowledge AB Legal geographical indication (GI) regimes are increasingly considered a promising tool to protect cultural heritage from outside appropriation. Yet such regimes have origins in a much more specific context: the structures and practices of wine-making in the elite wine regions of France. This article examines the relationships between different types of communities and structures involved in boundary-making under the prototypical GI system, appellation d'origine controlee (AOC), in its place of origin, Bordeaux. Here, legal boundaries are simultaneously reinforced, created, and defined by the values and priorities of the society that created them. In this article I consider geographical indications in Bordeaux not only as communal rights but as communal emanations, both to highlight the idiosyncrasies of AOC as a legal system and some of the problems and possibilities status suggests for the future of intellectual property rights. C1 Smithsonian Inst, Washington, DC 20560 USA. RP Farmer, EA (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 19 TC 0 Z9 0 U1 1 U2 6 PU WILEY PERIODICALS, INC PI SAN FRANCISCO PA ONE MONTGOMERY ST, SUITE 1200, SAN FRANCISCO, CA 94104 USA SN 1081-6976 EI 1555-2934 J9 POLAR-POLIT LEG ANTH JI Polar PD MAY PY 2014 VL 37 IS 1 BP 126 EP 144 DI 10.1111/plar.12054 PG 19 WC Anthropology SC Anthropology GA AG5KY UT WOS:000335459100009 ER PT J AU Asgari-Targhi, M van Ballegooijen, AA Imada, S AF Asgari-Targhi, M. van Ballegooijen, A. A. Imada, S. TI COMPARISON OF EXTREME ULTRAVIOLET IMAGING SPECTROMETER OBSERVATIONS OF SOLAR CORONAL LOOPS WITH ALFVEN WAVE TURBULENCE MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); Sun: corona; Sun: magnetic fields ID ACTIVE-REGION LOOPS; SPECTROSCOPIC OBSERVATIONS; FLUX TUBES; NONTHERMAL VELOCITIES; MAGNETIC-FIELDS; EMISSION-LINES; MOTIONS; HINODE; TEMPERATURE; SPICULES AB The observed non-thermal widths of coronal emission lines could be due to Alfven wave turbulence. To test this idea, we examine and analyze the dynamics of an active region observed on 2012 September 7. We use spectral line profiles of Fe XII, Fe XIII, Fe XV, and Fe XVI obtained by the Extreme-ultraviolet Imaging Spectrometer on the it Hinode spacecraft. The observations show non-thermal velocities, Doppler outflows, and intensities for loops in this active region. The observed non-thermal velocities are compared with predictions from models for Alfven wave turbulence in the observed coronal loops. This modeling takes into account the relationship between the width of the coronal emission lines and the orientation of the coronal loops with respect to the line-of-sight direction. We find that in order to produce the observed line widths we need to introduce a random parallel-flow component in addition to the perpendicular velocity due to Alfven waves. The observed widths are consistent with photospheric footpoint velocities in the range 0.3-1.5 km s(-1). We conclude that the Alfven wave turbulence model is a strong candidate for explaining how the observed loops are heated. C1 [Asgari-Targhi, M.; van Ballegooijen, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Imada, S.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan. RP Asgari-Targhi, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 15, Cambridge, MA 02138 USA. OI van Ballegooijen, Adriaan/0000-0002-5622-3540 FU UK's Engineering and Physical Sciences Research Council [EP/I034327/1]; JSPS; NASA [NNM07AB07C]; LMSAL [SP02H1701R] FX We thank the anonymous referee for detailed comments that helped to improve this paper. We thank John Raymond for discussions and 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, which was funded by the UK's Engineering and Physical Sciences Research Council (EP/I034327/1). M.A.T. was in part supported by JSPS Postdoctral Fellowship for North American and European Researchers. She is most grateful to Kanya Kusano at Nagoya University for hosting her visit. This project is supported under contract NNM07AB07C from NASA to the Smithsonian Astrophysical Observatory (SAO) and SP02H1701R from LMSAL to SAO. NR 66 TC 12 Z9 12 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 2014 VL 786 IS 1 AR 28 DI 10.1088/0004-637X/786/1/28 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700028 ER PT J AU Becerra, F Escala, A AF Becerra, Fernando Escala, Andres TI THE INTERSTELLAR MEDIUM AND STAR FORMATION IN LOCAL GALAXIES: VARIATIONS OF THE STAR FORMATION LAW IN SIMULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: structure; ISM: general; methods: numerical; stars: formation ID ADAPTIVE MESH REFINEMENT; INITIAL MASS FUNCTION; GLOBAL SCHMIDT LAW; GALACTIC DISKS; MOLECULAR CLOUDS; FORMATION CRITERIA; FORMING GALAXIES; STELLAR FEEDBACK; NEARBY GALAXIES; GAS AB We use the adaptive mesh refinement code Enzo to model the interstellar medium (ISM) in isolated local disk galaxies. The simulation includes a treatment for star formation and stellar feedback. We get a highly supersonic turbulent disk, which is fragmented at multiple scales and characterized by a multi-phase ISM. We show that a Kennicutt-Schmidt relation only holds when averaging over large scales. However, values of star formation rates and gas surface densities lie close in the plot for any averaging size. This suggests an intrinsic relation between stars and gas at cell-size scales, which dominates over the global dynamical evolution. To investigate this effect, we develop a method to simulate the creation of stars based on the density field from the snapshots, without running the code again. We also investigate how the star formation law is affected by the characteristic star formation timescale, the density threshold, and the efficiency considered in the recipe. We find that the slope of the law varies from similar to 1.4 for a free-fall timescale, to similar to 1.0 for a constant depletion timescale. We further demonstrate that a power law is recovered just by assuming that the mass of the new stars is a fraction of the mass of the cell m(star) = is an element of rho(gas)Delta x(3), with no other physical criteria required. We show that both efficiency and density threshold do not affect the slope, but the right combination of them can adjust the normalization of the relation, which in turn could explain a possible bi-modality in the law. C1 [Becerra, Fernando; Escala, Andres] Univ Chile, Dept Astron, Santiago, Chile. [Becerra, Fernando] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Becerra, F (reprint author), Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile. EM fbecerra@cfa.harvard.edu RI Escala, Andres /J-6618-2016 FU Programa Nacional de Becas de Postgrado [D-22100632]; Center for Astrophysics and Associated Technologies CATA [PFB 06]; Anillo de Ciencia y Tecnologia [ACT1101]; Proyecto Regular Fondecyt [1130458] FX We thank the anonymous referee for helpful suggestions and comments that improved the paper. F.B. acknowledges support from Programa Nacional de Becas de Postgrado (grant D-22100632). A.E. acknowledges partial support from the Center for Astrophysics and Associated Technologies CATA (PFB 06), Anillo de Ciencia y Tecnologia (Project ACT1101), and Proyecto Regular Fondecyt (grant 1130458). The simulation was performed using the HPC clustersMarkarian (FONDECYT 11090216) and Levque (ECM-02). The analysis and plots were carried out with the publicly available tool yt (Turk et al. 2011). NR 79 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 2014 VL 786 IS 1 AR 56 DI 10.1088/0004-637X/786/1/56 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700056 ER PT J AU Brandt, TD Kuzuhara, M McElwain, MW Schlieder, JE Wisniewski, JP Turner, EL Carson, J Matsuo, T Biller, B Bonnefoy, M Dressing, C Janson, M Knapp, GR Moro-Martin, A Thalmann, C Kudo, T Kusakabe, N Hashimoto, J Abe, L Brandner, W Currie, T Egner, S Feldt, M Golota, T Goto, M Grady, CA Guyon, O Hayano, Y Hayashi, M Hayashi, S Henning, T Hodapp, KW Ishii, M Iye, M Kandori, R Kwon, J Mede, K Miyama, S Morino, JI Nishimura, T Pyo, TS Serabyn, E Suenaga, T Suto, H Suzuki, R Takami, M Takahashi, Y Takato, N Terada, H Tomono, D Watanabe, M Yamada, T Takami, H Usuda, T Tamura, M AF Brandt, Timothy D. Kuzuhara, Masayuki McElwain, Michael W. Schlieder, Joshua E. Wisniewski, John P. Turner, Edwin L. Carson, J. Matsuo, T. Biller, B. Bonnefoy, M. Dressing, C. Janson, M. Knapp, G. R. Moro-Martin, A. Thalmann, C. Kudo, T. Kusakabe, N. Hashimoto, J. Abe, L. Brandner, W. Currie, T. Egner, S. Feldt, M. Golota, T. Goto, M. Grady, C. A. Guyon, O. Hayano, Y. Hayashi, M. Hayashi, S. Henning, T. Hodapp, K. W. Ishii, M. Iye, M. Kandori, R. Kwon, J. Mede, K. Miyama, S. Morino, J. -I. Nishimura, T. Pyo, T. -S. Serabyn, E. Suenaga, T. Suto, H. Suzuki, R. Takami, M. Takahashi, Y. Takato, N. Terada, H. Tomono, D. Watanabe, M. Yamada, T. Takami, H. Usuda, T. Tamura, M. TI THE MOVING GROUP TARGETS OF THE SEEDS HIGH-CONTRAST IMAGING SURVEY OF EXOPLANETS AND DISKS: RESULTS AND OBSERVATIONS FROM THE FIRST THREE YEARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; brown dwarfs; open clusters and associations: general; stars: activity; stars: imaging; stars: low-mass; stars: planetary systems ID TW-HYDRAE ASSOCIATION; LATE-TYPE STARS; LOW-MASS STARS; MAIN-SEQUENCE STARS; STELLAR KINEMATIC GROUPS; YOUNG SOLAR ANALOGS; ALL-SKY SURVEY; EXTRASOLAR GIANT PLANETS; GENEVA-COPENHAGEN SURVEY; ADAPTIVE OPTICS SURVEY AB We present results from the first three years of observations of moving group (MG) targets in the Strategic Exploration of Exoplanets and Disks with Subaru (SEEDS) high-contrast imaging survey of exoplanets and disks using the Subaru telescope. We achieve typical contrasts of similar to 10(5) at 1 '' and similar to 10(6) beyond 2 '' around 63 proposed members of nearby kinematic MGs. We review each of the kinematic associations to which our targets belong, concluding that five, beta Pictoris (similar to 20 Myr), AB Doradus (similar to 100 Myr), Columba (similar to 30 Myr), Tucana-Horogium (similar to 30 Myr), and TW Hydrae (similar to 10 Myr), are sufficiently well-defined to constrain the ages of individual targets. Somewhat less than half of our targets are high-probability members of one of these MGs. For all of our targets, we combine proposed MG membership with other age indicators where available, including Ca II HK emission, X-ray activity, and rotation period, to produce a posterior probability distribution of age. SEEDS observations discovered a substellar companion to one of our targets,. And, a late B star. We do not detect any other substellar companions, but do find seven new close binary systems, of which one still needs to be confirmed. A detailed analysis of the statistics of this sample, and of the companion mass constraints given our age probability distributions and exoplanet cooling models, will be presented in a forthcoming paper. C1 [Brandt, Timothy D.; Turner, Edwin L.; Janson, M.; Knapp, G. R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Kuzuhara, Masayuki] Tokyo Inst Technol, Tokyo 152, Japan. [McElwain, Michael W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Schlieder, Joshua E.; Carson, J.; Biller, B.; Bonnefoy, M.; Brandner, W.; Feldt, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Matsuo, T.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Univ WPI, Tokyo 1138654, Japan. [Carson, J.] Coll Charleston, Charleston, SC 29401 USA. [Matsuo, T.] Kyoto Univ, Dept Astron, Kyoto, Japan. [Dressing, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Moro-Martin, A.] CAB CSIC INTA, Dept Astrophys, Madrid, Spain. [Thalmann, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Kudo, T.; Egner, S.; Golota, T.; Guyon, O.; Hayano, Y.; Hayashi, S.; Ishii, M.; Nishimura, T.; Pyo, T. -S.; Takato, N.; Terada, H.; Tomono, D.; Takami, H.; Usuda, T.] Subaru Telescope, Hilo, HI USA. [Kusakabe, N.; Hashimoto, J.; Iye, M.; Kandori, R.; Kwon, J.; Morino, J. -I.; Suto, H.; Suzuki, R.; Tamura, M.] Natl Astron Observ Japan, Tokyo, Japan. [Abe, L.] Lab Hippolyte Fizeau, Nice, France. [Currie, T.] Univ Toronto, Toronto, ON, Canada. [Goto, M.] Univ Sternwarte, Munich, Germany. [Grady, C. A.] Eureka Sci, Oakland, CA USA. [Hayashi, M.; Takahashi, Y.; Tamura, M.] Univ Tokyo, Tokyo, Japan. [Hodapp, K. W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Kwon, J.; Suenaga, T.] Grad Univ Adv Studies, Dept Astron Sci, Tokyo, Japan. [Miyama, S.] Hiroshima Univ, Higashihiroshima 724, Japan. [Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido, Japan. [Yamada, T.] Tohoku Univ, Astron Inst, Sendai, Miyagi 980, Japan. RP Brandt, TD (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016 OI Watanabe, Makoto/0000-0002-3656-4081 NR 237 TC 27 Z9 27 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 1 DI 10.1088/0004-637X/786/1/1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700001 ER PT J AU Broekhoven-Fiene, H Matthews, BC Harvey, PM Gutermuth, RA Huard, TL Tothill, NFH Nutter, D Bourke, TL DiFrancesco, J Jorgensen, JK Allen, LE Chapman, NL Dunham, MM Merin, B Miller, JF Terebey, S Peterson, DE Stapelfeldt, KR AF Broekhoven-Fiene, Hannah Matthews, Brenda C. Harvey, Paul M. Gutermuth, Robert A. Huard, Tracy L. Tothill, Nicholas F. H. Nutter, David Bourke, Tyler L. DiFrancesco, James Jorgensen, Jes K. Allen, Lori E. Chapman, Nicholas L. Dunham, Michael M. Merin, Bruno Miller, Jennifer F. Terebey, Susan Peterson, Dawn E. Stapelfeldt, Karl R. TI THE Spitzer SURVEY OF INTERSTELLAR CLOUDS IN THE GOULD BELT. VI. THE AURIGA-CALIFORNIA MOLECULAR CLOUD OBSERVED WITH IRAC AND MIPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: general; ISM: clouds; stars: formation ID YOUNG STELLAR OBJECTS; ARRAY CAMERA IRAC; T-TAURI STARS; C2D SURVEY; SPACE-TELESCOPE; NEARBY; PERSEUS; POPULATION; DISTRIBUTIONS; LUMINOSITIES AB We present observations of the Auriga-California Molecular Cloud (AMC) at 3.6, 4.5, 5.8, 8.0, 24, 70, and 160 mu m observed with the IRAC and MIPS detectors as part of the Spitzer Gould Belt Legacy Survey. The total mapped areas are 2.5 deg(2) with IRAC and 10.47 deg(2) with MIPS. This giant molecular cloud is one of two in the nearby Gould Belt of star-forming regions, the other being the Orion A Molecular Cloud (OMC). We compare source counts, colors, and magnitudes in our observed region to a subset of the SWIRE data that was processed through our pipeline. Using color-magnitude and color-color diagrams, we find evidence for a substantial population of 166 young stellar objects (YSOs) in the cloud, many of which were previously unknown. Most of this population is concentrated around the LkH alpha 101 cluster and the filament extending from it. We present a quantitative description of the degree of clustering and discuss the relative fraction of YSOs in earlier (Class I and F) and later (Class II) classes compared to other clouds. We perform simple SED modeling of the YSOs with disks to compare the mid-IR properties to disks in other clouds and identify 14 classical transition disk candidates. Although the AMC is similar in mass, size, and distance to the OMC, it is forming about 15-20 times fewer stars. C1 [Broekhoven-Fiene, Hannah; Matthews, Brenda C.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Matthews, Brenda C.; DiFrancesco, James] Natl Res Council Herzberg Astron Astrophys, Victoria, BC V9E 2E7, Canada. [Harvey, Paul M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Gutermuth, Robert A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Huard, Tracy L.; Miller, Jennifer F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Huard, Tracy L.] Univ Western Sydney, Sch Comp Engn & Math, Penrith, NSW 2751, Australia. [Tothill, Nicholas F. H.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Nutter, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bourke, Tyler L.; Miller, Jennifer F.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Jorgensen, Jes K.] Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Jorgensen, Jes K.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Allen, Lori E.] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Chapman, Nicholas L.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Chapman, Nicholas L.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Dunham, Michael M.] ESAC ESA, Herschel Sci Ctr, E-28691 Madrid, Spain. [Merin, Bruno] Space Sci Inst, Boulder, CO 80301 USA. [Terebey, Susan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Broekhoven-Fiene, H (reprint author), Univ Victoria, Dept Phys & Astron, POB 3055, Victoria, BC V8W 3P6, Canada. RI Tothill, Nicholas/M-6379-2016 OI Tothill, Nicholas/0000-0002-9931-5162 FU NSERC Discovery Grant; NASA - California Institute of Technology [NCC5-626] FX We thank the referee whose comments and suggestions greatly helped improve the paper and its clarity. H.B.F. gratefully acknowledges research support from an NSERC Discovery Grant. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy. github. com. This research also made use of Montage, funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology. Montage is maintained by the NASA/IPAC Infrared Science Archive. NR 39 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 37 DI 10.1088/0004-637X/786/1/37 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700037 ER PT J AU Del Moro, A Mullaney, JR Alexander, DM Comastri, A Bauer, FE Treister, E Stern, D Civano, F Ranalli, P Vignali, C Aird, JA Ballantyne, DR Balokovic, M Boggs, SE Brandt, WN Christensen, FE Craig, WW Gandhi, P Gilli, R Hailey, CJ Harrison, FA Hickox, RC LaMassa, SM Lansbury, GB Luo, B Puccetti, S Urry, M Zhang, WW AF Del Moro, A. Mullaney, J. R. Alexander, D. M. Comastri, A. Bauer, F. E. Treister, E. Stern, D. Civano, F. Ranalli, P. Vignali, C. Aird, J. A. Ballantyne, D. R. Balokovic, M. Boggs, S. E. Brandt, W. N. Christensen, F. E. Craig, W. W. Gandhi, P. Gilli, R. Hailey, C. J. Harrison, F. A. Hickox, R. C. LaMassa, S. M. Lansbury, G. B. Luo, B. Puccetti, S. Urry, M. Zhang, W. W. TI NuSTAR J033202-2746.8: DIRECT CONSTRAINTS ON THE COMPTON REFLECTION IN A HEAVILY OBSCURED QUASAR AT z approximate to 2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; infrared: galaxies; quasars: general; quasars: individual (NuSTAR J033202-2746.8); X-rays: galaxies ID DEEP FIELD-SOUTH; ACTIVE GALACTIC NUCLEI; RAY SPECTRAL PROPERTIES; HARD X-RAYS; XMM-NEWTON OBSERVATIONS; STAR-FORMING GALAXIES; POINT-SOURCE CATALOGS; LINE RADIO GALAXIES; MS SOURCE CATALOGS; SWIFT-BAT SURVEY AB We report Nuclear Spectroscopic Telescope Array (NuSTAR) observations of NuSTAR J033202-2746.8, a heavily obscured, radio-loud quasar detected in the Extended Chandra Deep Field-South, the deepest layer of the NuSTAR extragalactic survey (similar to 400 ks, at its deepest). NuSTAR J033202-2746.8 is reliably detected by NuSTAR only at E > 8 keV and has a very flat spectral slope in the NuSTAR energy band (Gamma = 0.55(-0.64)(+0.62); 3-30 keV). Combining the NuSTAR data with extremely deep observations by Chandra and XMM-Newton (4 Ms and 3 Ms, respectively), we constrain the broad-band X-ray spectrum of NuSTAR J033202-2746.8, indicating that this source is a heavily obscured quasar (N-H = 5.6(-0.8)(+0.9) x 10(23) cm(-2)) with luminosity L10-40 keV approximate to 6.4 x 10(44) erg s(-1). Although existing optical and near-infrared (near-IR) data, as well as follow-up spectroscopy with the Keck and VLT telescopes, failed to provide a secure redshift identification for NuSTAR J033202-2746.8, we reliably constrain the redshift z = 2.00 +/- 0.04 from the X-ray spectral features (primarily from the iron K edge). The NuSTAR spectrum shows a significant reflection component (R = 0.55(-0.37)(+0.44)), which was not constrained by previous analyses of Chandra and XMM-Newton data alone. The measured reflection fraction is higher than the R similar to 0 typically observed in bright radio-loud quasars such as NuSTAR J033202-2746.8, which has L-1.4 GHz approximate to 10(27) W Hz(-1). Constraining the spectral shape of active galactic nuclei (AGNs), including bright quasars, is very important for understanding the AGN population, and can have a strong impact on the modeling of the X-ray background. Our results show the importance of NuSTAR in investigating the broad-band spectral properties of quasars out to high redshift. C1 [Del Moro, A.; Mullaney, J. R.; Alexander, D. M.; Aird, J. A.; Gandhi, P.; Lansbury, G. B.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Mullaney, J. R.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Comastri, A.; Vignali, C.; Gilli, R.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Civano, F.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ranalli, P.] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, Inst Astron, Penteli 15236, Greece. [Vignali, C.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Balokovic, M.; Harrison, F. A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [LaMassa, S. M.; Urry, M.] Yale Univ, Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA. [Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Puccetti, S.] INAF Osservatorio Astronomico Roma, I-00040 Monte Porzio Catone, Italy. [Zhang, W. W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Del Moro, A (reprint author), Univ Durham, Dept Phys, S Rd, Durham DH1 3LE, England. EM agnese.del-moro@durham.ac.uk RI Ranalli, Piero/K-6363-2013; Vignali, Cristian/J-4974-2012; Boggs, Steven/E-4170-2015; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Ranalli, Piero/0000-0003-3956-755X; Vignali, Cristian/0000-0002-8853-9611; Boggs, Steven/0000-0001-9567-4224; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Alexander, David/0000-0002-5896-6313 FU UK Science and Technology Facilities Council (STFC) [ST/I001573/I, ST/K501979/1, ST/J003697/1]; Leverhulme Trust; ASI/INAF [I/037/12/0-011/13]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024]; Anillo [ACT1101]; FONDECYT [1120061]; Caltech NuSTAR [44A-1092750]; NASA ADP [NNX10AC99G]; NASA [NNG08FD60C]; National Aeronautics and Space Administration; ESO Telescopes at the La Silla Paranal Observatory under the program [ID 092.A-0452] FX We thank the anonymous referee for careful reading and for the helpful comments, which helped improving this manuscript. We gratefully acknowledge financial support from the UK Science and Technology Facilities Council (STFC, ST/I001573/I, ADM and DMA; ST/K501979/1, GBL; ST/J003697/1, PG) and the Leverhulme Trust (D.M.A. and J.R.M.). A.C., C.V., R.G., and P.R. thank the ASI/INAF grant I/037/12/0-011/13. F.E.B. acknowledges support from Basal-CATA (PFB-06/2007) and CONICYT-Chile (FONDECYT 1101024 and Anillo grant ACT1101) and E.T. acknowledges the FONDECYT grant 1120061. W.N.B. and B.L. thank Caltech NuSTAR subcontract 44A-1092750 and NASA ADP grant NNX10AC99G. M.B. acknowledges the International Fulbright Science and Technology Award. 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). This work also used observations made with ESO Telescopes at the La Silla Paranal Observatory under the program ID 092.A-0452. NR 111 TC 19 Z9 19 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 16 DI 10.1088/0004-637X/786/1/16 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700016 ER PT J AU Kenyon, SJ Currie, T Bromley, BC AF Kenyon, Scott J. Currie, Thayne Bromley, Benjamin C. TI FOMALHAUT b AS A CLOUD OF DUST: TESTING ASPECTS OF PLANET FORMATION THEORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: detection; planets and satellites: formation; planets and satellites: physical evolution; planets and satellites: rings ID KUIPER-BELT OBJECTS; TRANS-NEPTUNIAN OBJECTS; GIANT IMPACT ORIGIN; BETA-PICTORIS DISK; IRREGULAR SATELLITES; SIZE DISTRIBUTION; SOLAR-SYSTEM; DEBRIS DISKS; PLUTO-CHARON; COLLISIONAL FRAGMENTATION AB We consider the ability of three models-impacts, captures, and collisional cascades-to account for a bright cloud of dust in Fomalhaut b. Our analysis is based on a novel approach to the power-law size distribution of solid particles central to each model. When impacts produce debris with (1) little material in the largest remnant and (2) a steep size distribution, the debris has enough cross-sectional area to match observations of Fomalhaut b. However, published numerical experiments of impacts between 100 km objects suggest this outcome is unlikely. If collisional processes maintain a steep size distribution over a broad range of particle sizes (300 mu m to 10 km), Earth-mass planets can capture enough material over 1-100 Myr to produce a detectable cloud of dust. Otherwise, capture fails. When young planets are surrounded by massive clouds or disks of satellites, a collisional cascade is the simplest mechanism for dust production in Fomalhaut b. Several tests using Hubble Space Telescope or James Webb Space Telescope data-including measuring the expansion/elongation of Fomalhaut b, looking for trails of small particles along Fomalhaut b's orbit, and obtaining low resolution spectroscopy-can discriminate among these models. C1 [Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Currie, Thayne] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 1A1, Canada. [Bromley, Benjamin C.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM skenyon@cfa.harvard.edu; currie@astro.utoronto.ca; bromley@physics.utah.edu OI Kenyon, Scott/0000-0003-0214-609X FU NASA [NNX10AF35G, NNX11AM37G] FX Comments from M. Geller and a thoughtful referee improved our presentation. Portions of this project were supported by the NASA Astrophysics Theory and Origins of Solar Systems programs through grant NNX10AF35G and the NASA Outer Planets Program through grant NNX11AM37G. NR 123 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 70 DI 10.1088/0004-637X/786/1/70 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700070 ER PT J AU Piso, AMA Youdin, AN AF Piso, Ana-Maria A. Youdin, Andrew N. TI ON THE MINIMUM CORE MASS FOR GIANT PLANET FORMATION AT WIDE SEPARATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: atmospheres; planets and satellites: formation; planets and satellites: gaseous planets ID GRAVITATIONAL-INSTABILITY; PROTOPLANETARY DISKS; PROTOSTELLAR DISKS; GASEOUS ENVELOPE; GAS; ACCRETION; EVOLUTION; MODELS; GROWTH; ATMOSPHERES AB In the core accretion hypothesis, giant planets form by gas accretion onto solid protoplanetary cores. The minimum (or critical) core mass to form a gas giant is typically quoted as 10 M-circle plus. The actual value depends on several factors: the location in the protoplanetary disk, atmospheric opacity, and the accretion rate of solids. Motivated by ongoing direct imaging searches for giant planets, this study investigates core mass requirements in the outer disk. To determine the fastest allowed rates of gas accretion, we consider solid cores that no longer accrete planetesimals, as this would heat the gaseous envelope. Our spherical, two-layer atmospheric cooling model includes an inner convective region and an outer radiative zone that matches onto the disk. We determine the minimum core mass for a giant planet to form within a typical disk lifetime of 3 Myr. The minimum core mass declines with disk radius, from similar to 8.5M(circle plus) at 5 AU to similar to 3.5M(circle plus) at 100 AU, with standard interstellar grain opacities. Lower temperatures in the outer disk explain this trend, while variations in disk density are less influential. At all distances, a lower dust opacity or higher mean molecular weight reduces the critical core mass. Our non-self-gravitating, analytic cooling model reveals that self-gravity significantly affects early atmospheric evolution, starting when the atmosphere is only similar to 10% as massive as the core. C1 [Piso, Ana-Maria A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Youdin, Andrew N.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Youdin, Andrew N.] NIST, Boulder, CO 80309 USA. RP Piso, AMA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Youdin, Andrew/0000-0002-3644-8726 FU NASA ATP; NASA OSS [NNX10AF35G]; NASA OPR grant at the CfA [NNX11AM37G]; NSF AST [1313021]; NASA OSS at JILA [NNX13AI58G] FX We thank the referee for a thorough report and Ruth Murray-Clay for detailed feedback and skillful proofreading. We appreciate valuable comments from Eugene Chiang and Scott Kenyon. A.N.Y. thanks Phil Armitage for stimulating conversations. A.N.Y. acknowledges support from the NASA ATP and OSS grant NNX10AF35G and the NASA OPR grant NNX11AM37G while at the CfA, and from the NSF AST grant 1313021 and the NASA OSS grant NNX13AI58G while at JILA. NR 52 TC 24 Z9 24 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 21 DI 10.1088/0004-637X/786/1/21 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700021 ER PT J AU Schlafly, EF Green, G Finkbeiner, DP Rix, HW Bell, EF Burgett, WS Chambers, KC Draper, PW Hodapp, KW Kaiser, N Magnier, EA Martin, NF Metcalfe, N Price, PA Tonry, JL AF Schlafly, E. F. Green, G. Finkbeiner, D. P. Rix, H. -W. Bell, E. F. Burgett, W. S. Chambers, K. C. Draper, P. W. Hodapp, K. W. Kaiser, N. Magnier, E. A. Martin, N. F. Metcalfe, N. Price, P. A. Tonry, J. L. TI A LARGE CATALOG OF ACCURATE DISTANCES TO MOLECULAR CLOUDS FROM PS1 PHOTOMETRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: clouds ID STAR-FORMING REGIONS; NUMBER DENSITY DISTRIBUTION; MILKY-WAY TOMOGRAPHY; DIGITAL SKY SURVEY; INTERSTELLAR EXTINCTION; CEPHEUS FLARE; MONOCEROS R2; ORION NEBULA; H2O MASERS; DUST AB Distance measurements to molecular clouds are important but are often made separately for each cloud of interest, employing very different data and techniques. We present a large, homogeneous catalog of distances to molecular clouds, most of which are of unprecedented accuracy. We determine distances using optical photometry of stars along lines of sight toward these clouds, obtained from PanSTARRS-1. We simultaneously infer the reddenings and distances to these stars, tracking the full probability distribution function using a technique presented in Green et al. We fit these star-by-star measurements using a simple dust screen model to find the distance to each cloud. We thus estimate the distances to almost all of the clouds in the Magnani et al. catalog, as well as many other well-studied clouds, including Orion, Perseus, Taurus, Cepheus, Polaris, California, and Monoceros R2, avoiding only the inner Galaxy. Typical statistical uncertainties in the distances are 5%, though the systematic uncertainty stemming from the quality of our stellar models is about 10%. The resulting catalog is the largest catalog of accurate, directly measured distances to molecular clouds. Our distance estimates are generally consistent with available distance estimates from the literature, though in some cases the literature estimates are off by a factor of more than two. C1 [Schlafly, E. F.; Rix, H. -W.; Martin, N. F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Green, G.; Finkbeiner, D. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Finkbeiner, D. P.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bell, E. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Burgett, W. S.; Chambers, K. C.; Hodapp, K. W.; Kaiser, N.; Magnier, E. A.; Tonry, J. L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Draper, P. W.; Metcalfe, N.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Martin, N. F.] CNRS, Observ Astron Strasbourg, UMR 7550, F-67000 Strasbourg, France. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Schlafly, EF (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. OI Chambers, Kenneth /0000-0001-6965-7789; Metcalfe, Nigel/0000-0001-9034-4402; Bell, Eric/0000-0002-5564-9873; Schlafly, Edward Ford/0000-0002-3569-7421; Green, Gregory/0000-0001-5417-2260 FU DFG [SFB 881]; NSF [AST-1312891]; CNRS [PICS06183]; National Aeronautics and Space Administration [NNX08AR22G]; National Science Foundation [AST-1238877] FX E.S. acknowledges support from the DFG grant SFB 881 (A3). G.M.G. and D.P.F. are partially supported by NSF grant AST-1312891. N.F.M. gratefully acknowledges the CNRS for support through PICS project PICS06183. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.; 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 Net-work 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 70 TC 51 Z9 51 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2014 VL 786 IS 1 AR 29 DI 10.1088/0004-637X/786/1/29 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH0LF UT WOS:000335810700029 ER PT J AU Bocxlaer, B Albrecht, C Stauffer, JR AF Van Bocxlaer, Bert Albrecht, Christian Stauffer, Jay R., Jr. TI Growing population and ecosystem change increase human schistosomiasis around Lake Malawi SO TRENDS IN PARASITOLOGY LA English DT Editorial Material DE global health; schistosomiasis; bilharzia; ecosystem change; population densities; sedimentation; eutrophication; parasite transmission; Bulinus ID SOFT-SEDIMENT GASTROPODS; CAPE MACLEAR; RESISTANCE; DISEASES; FISHES AB Multiple anthropogenic environmental stressors with reinforcing effects to the deterioration of ecosystem stability can obscure links between ecosystem change and the prevalence of infectious diseases. Incomplete understanding may lead to ineffective public health and disease control strategies, as appears to be the case with increased urogenital schistosomiasis in humans around Lake Malawi over recent decades. Sedimentation and eutrophication help explain historical changes in intermediate host range and parasite transmission. Hence, control strategies should account for abiotic changes. C1 [Van Bocxlaer, Bert] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Van Bocxlaer, Bert] Univ Ghent, Dept Geol & Soil Sci, B-9000 Ghent, Belgium. [Albrecht, Christian] Univ Giessen, Dept Anim Ecol & Systemat, D-35392 Giessen, Germany. [Stauffer, Jay R., Jr.] Penn State Univ, Dept Ecosyst Sci & Management, University Pk, PA 16802 USA. RP Bocxlaer, B (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. EM vanboodaerb@si.edu RI Van Bocxlaer, Bert/N-1965-2016 OI Van Bocxlaer, Bert/0000-0003-2033-326X NR 15 TC 1 Z9 1 U1 2 U2 12 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1471-4922 EI 1471-5007 J9 TRENDS PARASITOL JI Trends Parasitol. PD MAY PY 2014 VL 30 IS 5 BP 217 EP 220 DI 10.1016/j.pt.2014.02.006 PG 4 WC Parasitology SC Parasitology GA AH3IJ UT WOS:000336016600002 ER PT J AU Brady, SG Fisher, BL Schultz, TR Ward, PS AF Brady, Sean G. Fisher, Brian L. Schultz, Ted R. Ward, Philip S. TI The rise of army ants and their relatives: diversification of specialized predatory doryline ants SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID DIVERGENCE TIME-ESTIMATION; HYMENOPTERA-FORMICIDAE; PSEUDOMYRMECINAE HYMENOPTERA; EVOLUTIONARY TRANSITIONS; RELAXED PHYLOGENETICS; TERMINAL TAXA; LEPTANILLOIDINAE; INFERENCE; TAXONOMY; FOSSILS AB Background: Army ants are dominant invertebrate predators in tropical and subtropical terrestrial ecosystems. Their close relatives within the dorylomorph group of ants are also highly specialized predators, although much less is known about their biology. We analyzed molecular data generated from 11 nuclear genes to infer a phylogeny for the major dorylomorph lineages, and incorporated fossil evidence to infer divergence times under a relaxed molecular clock. Results: Because our results indicate that one subfamily and several genera of dorylomorphs are non-monophyletic, we propose to subsume the six previous dorylomorph subfamilies into a single subfamily, Dorylinae. We find the monophyly of Dorylinae to be strongly supported and estimate the crown age of the group at 87 (74-101) million years. Our phylogenetic analyses provide only weak support for army ant monophyly and also call into question a previous hypothesis that army ants underwent a fundamental split into New World and Old World lineages. Outside the army ants, our phylogeny reveals for the first time many old, distinct lineages in the Dorylinae. The genus Cerapachys is shown to be non-monophyletic and comprised of multiple lineages scattered across the Dorylinae tree. We recover, with strong support, novel relationships among these Cerapachys like clades and other doryline genera, but divergences in the deepest parts of the tree are not well resolved. We find the genus Sphinctomyrmex, characterized by distinctive abdominal constrictions, to consist of two separate lineages with convergent morphologies, one inhabiting the Old World and the other the New World tropics. Conclusions: While we obtain good resolution in many parts of the Dorylinae phylogeny, relationships deep in the tree remain unresolved, with major lineages joining each other in various ways depending upon the analytical method employed, but always with short internodes. This may be indicative of rapid radiation in the early history of the Dorylinae, but additional molecular data and more complete species sampling are needed for confirmation. Our phylogeny now provides a basic framework for comparative biological analyses, but much additional study on the behavior and morphology of doryline species is needed, especially investigations directed at the non-army ant taxa. C1 [Brady, Sean G.; Schultz, Ted R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Fisher, Brian L.] Calif Acad Sci, Dept Entomol, San Francisco, CA 94118 USA. [Ward, Philip S.] Univ Calif Davis, Dept Entomol & Nematol, Davis, CA 95616 USA. RP Brady, SG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. EM bradys@si.edu OI Fisher, Brian/0000-0002-4653-3270 FU National Science Foundation Ant AToL (Assembling the Tree of Life) [EF-0431330, DEB-0743542] FX We thank S. Berghoff, P. Buenavente, S. Chatchumnan, S. De Greef, D. A. Donoso, K. Eguchi, E. Estrella, C. Felix, E. M. Fisher, W. Freund, J. Gadau, H. Gilberth, Z. Guang, N. R. Gunawardene, R. Harin'Hala, M. E. Irwin, S. Khonglasae, S. Lacau, J. Longino, E. Marais, D. Mezger, J. S. Noyes, W. Okeka, D. M. Olson, H. G. Robertson, M. Sanetra, E. F. Santos, C. P. Scott-Santos, S. Singtong, R. R. Snelling, P. Tamtip, A. L. Wild, S. K. Yamane, and S. P. Yanoviak for collecting some of the specimens used this study; M. Kweskin for computational support; P. Armstrong, M. Kweskin, and H. Zhao for assistance generating molecular sequences; E. Okonski for museum collection assistance; M. Borowiec and two anonymous reviewers for helpful and insightful comments that improved the quality of the manuscript. This work was supported by the National Science Foundation Ant AToL (Assembling the Tree of Life) grant EF-0431330 and grant DEB-0743542. NR 80 TC 30 Z9 31 U1 1 U2 30 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 1 PY 2014 VL 14 AR 93 DI 10.1186/1471-2148-14-93 PG 14 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA AG7LB UT WOS:000335598400001 PM 24886136 ER PT J AU Cohen, EB Hostetler, JA Royle, JA Marra, PP AF Cohen, Emily B. Hostetler, Jeffrey A. Royle, J. Andrew Marra, Peter P. TI Estimating migratory connectivity of birds when re- encounter probabilities are heterogeneous SO ECOLOGY AND EVOLUTION LA English DT Article DE Bird Banding Laboratory; migratory connectivity; multistate model; Nearctic-Neotropical Migrant; re-encounter probability ID BAND-RECOVERY DATA; COMMON TERNS; CAPTURE-RECAPTURE; MARKED INDIVIDUALS; MIGRANT SONGBIRD; WINTER QUARTERS; ROSEATE TERNS; PROGRAM MARK; ABUNDANCE; MOVEMENT AB Understanding the biology and conducting effective conservation of migratory species requires an understanding of migratory connectivity - the geographic linkages of populations between stages of the annual cycle. Unfortunately, for most species, we are lacking such information. The North American Bird Banding Laboratory (BBL) houses an extensive database of marking, recaptures and recoveries, and such data could provide migratory connectivity information for many species. To date, however, few species have been analyzed for migratory connectivity largely because heterogeneous re-encounter probabilities make interpretation problematic. We accounted for regional variation in re-encounter probabilities by borrowing information across species and by using effort covariates on recapture and recovery probabilities in a multistate capture-recapture and recovery model. The effort covariates were derived from recaptures and recoveries of species within the same regions. We estimated the migratory connectivity for three tern species breeding in North America and over-wintering in the tropics, common (Sterna hirundo), roseate (Sterna dougallii), and Caspian terns (Hydroprogne caspia). For western breeding terns, model-derived estimates of migratory connectivity differed considerably from those derived directly from the proportions of re-encounters. Conversely, for eastern breeding terns, estimates were merely refined by the inclusion of re-encounter probabilities. In general, eastern breeding terns were strongly connected to eastern South America, and western breeding terns were strongly linked to the more western parts of the nonbreeding range under both models. Through simulation, we found this approach is likely useful for many species in the BBL database, although precision improved with higher re-encounter probabilities and stronger migratory connectivity. We describe an approach to deal with the inherent biases in BBL banding and re-encounter data to demonstrate that this large dataset is a valuable source of information about the migratory connectivity of the birds of North America. C1 [Cohen, Emily B.; Hostetler, Jeffrey A.; Marra, Peter P.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Royle, J. Andrew] US Geol Survey, Patuxent Wildlife Res Ctr, Laurel, MD USA. RP Cohen, EB (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, POB 37012 MRC 5503, Washington, DC 20013 USA. EM cohenE@si.edu RI Hostetler, Jeffrey/A-3345-2011; OI Hostetler, Jeffrey/0000-0003-3669-1758; Royle, Jeffrey/0000-0003-3135-2167 FU US Geological Survey; US Fish and Wildlife Service; Upper Midwest and Great Lakes Landscape Conservation Cooperative FX Funding was provided from US Geological Survey, US Fish and Wildlife Service, and the Upper Midwest and Great Lakes Landscape Conservation Cooperative. NR 63 TC 8 Z9 11 U1 0 U2 31 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD MAY PY 2014 VL 4 IS 9 BP 1659 EP 1670 DI 10.1002/ece3.1059 PG 12 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA AG2SQ UT WOS:000335267000013 PM 24967083 ER PT J AU McFrederick, QS Wcislo, WT Hout, MC Mueller, UG AF McFrederick, Quinn S. Wcislo, William T. Hout, Michael C. Mueller, Ulrich G. TI Host species and developmental stage, but not host social structure, affects bacterial community structure in socially polymorphic bees SO FEMS MICROBIOLOGY ECOLOGY LA English DT Article DE facultative sociality; microbiota; pollinator conservation; bee-associated bacteria ID GUT MICROBIOTA; BUMBLE BEES; HONEY-BEE; MEGALOPTA-GENALIS; SWEAT BEES; ECUADORIA HYMENOPTERA; GEN. NOV.; DIVERSITY; HALICTIDAE; WOLBACHIA AB Social transmission and host developmental stage are thought to profoundly affect the structure of bacterial communities associated with honey bees and bumble bees, but these ideas have not been explored in other bee species. The halictid bees Megalopta centralis and M.genalis exhibit intrapopulation social polymorphism, which we exploit to test whether bacterial communities differ by host social structure, developmental stage, or host species. We collected social and solitary Megalopta nests and sampled bees and nest contents from all stages of host development. To survey these bacterial communities, we used 16S rRNA gene 454 pyrosequencing. We found no effect of social structure, but found differences by host species and developmental stage. Wolbachia prevalence differed between the two host species. Bacterial communities associated with different developmental stages appeared to be driven by environmentally acquired bacteria. A Lactobacillus kunkeei clade bacterium that is consistently associated with other bee species was dominant in pollen provisions and larval samples, but less abundant in mature larvae and pupae. Foraging adults appeared to often reacquire L.kunkeei clade bacteria, likely while foraging at flowers. Environmental transmission appears to be more important than social transmission for Megalopta bees at the cusp between social and solitary behavior. C1 [McFrederick, Quinn S.] Calif State Univ Fresno, Dept Biol, Fresno, CA 93740 USA. [McFrederick, Quinn S.; Mueller, Ulrich G.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Panama. [Hout, Michael C.] New Mexico State Univ, Dept Psychol, Las Cruces, NM 88003 USA. RP McFrederick, QS (reprint author), Calif State Univ Fresno, Dept Biol, 2555 East San Ramon Ave MS-73, Fresno, CA 93740 USA. EM qmcfrederick@csufresno.edu FU National Science Foundation [PRFB-1003133, DEB-0919519] FX This material is based on work supported by National Science Foundation grant PRFB-1003133 awarded to Q.S.M. and grant DEB-0919519 awarded to U.G.M. We thank the Smithsonian Tropical Research Institute for logistical support and the government of Panama for collecting and export permits. The authors have no conflict of interest to declare in relation to this work. NR 56 TC 12 Z9 12 U1 6 U2 37 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0168-6496 EI 1574-6941 J9 FEMS MICROBIOL ECOL JI FEMS Microbiol. Ecol. PD MAY PY 2014 VL 88 IS 2 BP 398 EP 406 DI 10.1111/1574-6941.12302 PG 9 WC Microbiology SC Microbiology GA AG4OA UT WOS:000335398400015 PM 24579829 ER PT J AU Jha, S Bacon, CM Philpott, SM Mendez, VE Laderach, P Rice, RA AF Jha, Shalene Bacon, Christopher M. Philpott, Stacy M. Mendez, V. Ernesto Laederach, Peter Rice, Robert A. TI Shade Coffee: Update on a Disappearing Refuge for Biodiversity SO BIOSCIENCE LA English DT Article DE agriculture; agroforestry; corridor; ecosystem services; tropical ecology ID WESTERN EL-SALVADOR; CENTRAL-AMERICA; FAIR TRADE; AGRICULTURAL INTENSIFICATION; ECOSYSTEM SERVICES; PRODUCTION SYSTEMS; CLIMATE-CHANGE; BERRY BORER; COSTA-RICA; LAND-USE AB In the past three decades, coffee cultivation has gained widespread attention for its crucial role in supporting local and global biodiversity. In this synthetic Overview, we present newly gathered data that summarize how global patterns in coffee distribution and shade vegetation have changed and discuss implications for biodiversity, ecosystem services, and livelihoods. Although overall cultivated coffee area has decreased by 8% since 1990, coffee production and agricultural intensification have increased in many places and shifted globally, with production expanding in Asia while contracting in Africa. Ecosystem services such as pollination, pest control, climate regulation, and nutrient sequestration are generally greater in shaded coffee farms, but many coffee-growing regions are removing shade trees from their management. Although it is clear that there are ecological and socioeconomic benefits associated with shaded coffee, we expose the many challenges and future research priorities needed to link sustainable coffee management with sustainable livelihoods. C1 [Jha, Shalene] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. [Bacon, Christopher M.] Santa Clara Univ, Dept Environm Studies & Sci, Santa Clara, CA 95053 USA. [Philpott, Stacy M.] Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. [Mendez, V. Ernesto] Univ Vermont, Environm Program, Agroecol & Rural Livelihoods Grp, Burlington, VT 05405 USA. [Mendez, V. Ernesto] Univ Vermont, Plant & Soil Sci Dept, Burlington, VT 05405 USA. [Laederach, Peter] Ctr Int Agr Trop, Managua, Nicaragua. [Rice, Robert A.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC USA. RP Jha, S (reprint author), Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. EM sjha@austin.utexas.edu RI Philpott, Stacy/F-2330-2011; OI Bacon, Christopher/0000-0002-2534-6900 NR 84 TC 22 Z9 22 U1 15 U2 124 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0006-3568 EI 1525-3244 J9 BIOSCIENCE JI Bioscience PD MAY PY 2014 VL 64 IS 5 BP 416 EP 428 DI 10.1093/biosci/biu038 PG 13 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AG5AG UT WOS:000335430900009 ER PT J AU Riley, SM AF Riley, Sheila M. TI The Ice Cream Queen of Orchard Street SO LIBRARY JOURNAL LA English DT Book Review C1 [Riley, Sheila M.] Smithsonian Inst Libs, Washington, DC 20560 USA. RP Riley, SM (reprint author), Smithsonian Inst Libs, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 2 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 1 PY 2014 VL 139 IS 8 BP 66 EP 66 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA AG3DN UT WOS:000335296100046 ER PT J AU Hong, T AF Hong, Terry TI Everything I Never Told You SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20013 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20013 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 1 PY 2014 VL 139 IS 8 BP 69 EP 69 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA AG3DN UT WOS:000335296100059 ER PT J AU Vargas, S Guzman, HM Breedy, O Worheide, G AF Vargas, Sergio Guzman, Hector M. Breedy, Odalisca Woerheide, Gert TI Molecular phylogeny and DNA barcoding of tropical eastern Pacific shallow-water gorgonian octocorals SO MARINE BIOLOGY LA English DT Article ID GENUS PACIFIGORGIA COELENTERATA; MIXED MODELS; REVISION; DIVERSITY; SEQUENCES; ANTHOZOA; PLEXAURIDAE; MORPHOLOGY; CNIDARIA; VERRILL AB The octocoral fauna inhabiting the shallow waters (< 50 m) of the eastern Pacific has been the subject of renewed interest, and the taxonomy of the most important genera in the region has been reviewed and clarified. Many new species have been described, significantly increasing the known biological diversity of the region. Despite their importance as potential sister-groups of Caribbean octocorals, the phylogenetic relationships of eastern Pacific octocorals remain poorly studied. Here, using partial mitochondrial MutS and igr1-COI sequences, we provide a phylogenetic assessment of a broad sample of eastern Pacific shallow-water octocorals and investigate their phylogenetic relationships with Caribbean gorgonians. We corroborate the monophyly of Pacifigorgia, Leptogorgia and Eugorgia and provide evidence of a close relationship between Swiftia and Psammogorgia, currently placed in Plexauridae. In addition, the phylogenies obtained here provide insights into the historical biogeography and phylogenetic diversity of the eastern Pacific octocoral assemblages and on character evolution among this diverse faunal assemblage. Finally, we evaluate the classification power of DNA barcoding for identifying species of shallow-water eastern Pacific octocorals and assess the use of a nuclear intron (SRP54) to supplement traditional mitochondrial barcodes in this group of organisms. C1 [Vargas, Sergio; Woerheide, Gert] Univ Munich, Dept Earth & Environm Sci Paleontol & Geobiol, D-80333 Munich, Germany. [Guzman, Hector M.; Breedy, Odalisca] Smithsonian Trop Res Inst, Panama City, Panama. [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica. [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Estruct Microscop, San Jose, Costa Rica. [Woerheide, Gert] Bavarian State Collect Palaeontol & Geol, D-80333 Munich, Germany. [Woerheide, Gert] LMU, GeoBioctr, 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. EM s.vargas@lrz.uni-muenchen.de RI Vargas, Sergio/A-5678-2011; Worheide, Gert/C-1080-2008 OI Vargas, Sergio/0000-0001-8704-1339; Worheide, Gert/0000-0002-6380-7421 FU Secretaria Nacional de Ciencia y Tecnologia de Panama (SENACYT); Smithsonian Tropical Research Institute; DFG [SPP 1158, Wo896/9-1] FX We thank Carlos Guevara for support during field collection campaigns. The Autoridad Nacional del Ambiente (ANA M) provided the permits for collecting and exporting the specimens. The project was partially sponsored by the Secretaria Nacional de Ciencia y Tecnologia de Panama (SENACYT) and the Smithsonian Tropical Research Institute. SV acknowledges financial support from the DFG SPP 1158 "Antarktisforschung" through grants Wo896/9-1,2 to G. Worheide. Natalie Villalobos Trigueros and Malena Vargas Villalobos were crucial to the realization of this study, and SV is indebted to them because of their unconditional support. The manuscript benefits from the comments of two anonymous reviewers and the editor, we appreciate their careful and detailed work. NR 39 TC 3 Z9 3 U1 2 U2 22 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD MAY PY 2014 VL 161 IS 5 BP 1027 EP 1038 DI 10.1007/s00227-014-2396-8 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AF7ZW UT WOS:000334935500006 ER PT J AU Abarca, D Adowski, AS Sironi, L AF Abarca, David Adowski, Aleksander S. Sironi, Lorenzo TI Simulating the effect of the Sgr A* accretion flow on the appearance of G2 after pericentre SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; black hole physics; methods: numerical ID CENTER CLOUD G2; ADVECTION-DOMINATED ACCRETION; GALACTIC-CENTER; SAGITTARIUS-A; BLACK-HOLE; GAS CLOUD; GRMHD SIMULATIONS; MODELS; PASSAGE; GALAXY AB We study the dynamical interaction of the G2 cloud with the accretion flow around Sgr A* by means of 3D, hydrodynamic simulations. We show the effects of the rotating accretion flow on the evolution of G2 by projecting the cloud density on to the plane of the sky, and extracting position-velocity diagrams. We study a number of possible orientations of the cloud orbit with respect to the disc. We find that once the centre of mass of the cloud has crossed the pericentre, the differences between models become significant. Models with the cloud counterrotating with respect to the disc are expected to reach higher blueshifted line-of-sight velocities. The spatial extent of the emission depends strongly on the cloud-to-disc inclination angle. Future imaging and spectroscopy of G2 emission will shed light both on the structure of the Sgr A* disc and on the properties of the cloud. C1 [Abarca, David; Adowski, Aleksander S.; Sironi, Lorenzo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02134 USA. RP Abarca, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02134 USA. EM david.abarca@post.harvard.edu FU NASA grant [NNX11AE16G]; NASA through Einstein Postdoctoral Fellowship - Chandra X-ray Center [PF1-120090]; NASA [NAS8-03060] FX AS is supported in part by NASA grant NNX11AE16G. LS is supported by NASA through Einstein Postdoctoral Fellowship grant number PF1-120090 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. We thank Ramesh Narayan and Maciek Wielgus for helpful discussions. NR 30 TC 9 Z9 9 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2014 VL 440 IS 2 BP 1125 EP 1137 DI 10.1093/mnras/stu244 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5GO UT WOS:000334742200014 ER PT J AU Suutarinen, AN Kristensen, LE Mottram, JC Fraser, HJ van Dishoeck, EF AF Suutarinen, A. N. Kristensen, L. E. Mottram, J. C. Fraser, H. J. van Dishoeck, E. F. TI Water and methanol in low-mass protostellar outflows: gas-phase synthesis, ice sputtering and destruction SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrochemistry; stars: formation; ISM: jets and outflows; ISM: molecules ID STAR-FORMING REGIONS; YOUNG STELLAR OBJECTS; TIME DIGIT HERSCHEL; CO LINE FORMATION; INTERSTELLAR ICES; SHOCK-WAVES; ROTATIONAL-EXCITATION; SPECTROSCOPIC SURVEY; THERMAL-DESORPTION; BIPOLAR OUTFLOWS AB Water in outflows from protostars originates either as a result of gas-phase synthesis from atomic oxygen at T greater than or similar to 200 K, or from sputtered ice mantles containing water ice. We aim to quantify the contribution of the two mechanisms that lead to water in outflows, by comparing observations of gas-phase water to methanol (a grain surface product) towards three low-mass protostars in NGC 1333. In doing so, we also quantify the amount of methanol destroyed in outflows. To do this, we make use of James Clerk Maxwell Telescope and Herschel-Heterodyne Instrument for the Far-Infrared data of H2O, CH3OH and CO emission lines and compare them to radex non-local thermodynamic equilibrium excitation simulations. We find up to one order of magnitude decrease in the column density ratio of CH3OH over H2O as the velocity increases in the line wings up to similar to 15 km s(-1). An independent decrease in X(CH3OH) with respect to CO of up to one order of magnitude is also found in these objects. We conclude that gas-phase formation of H2O must be active at high velocities (above 10 km s(-1) relative to the source velocity) to re-form the water destroyed during sputtering. In addition, the transition from sputtered water at low velocities to form water at high velocities must be gradual. We place an upper limit of two orders of magnitude on the destruction of methanol by sputtering effects. C1 [Suutarinen, A. N.; Fraser, H. J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mottram, J. C.; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Suutarinen, AN (reprint author), Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. EM aleksi.suutarinen@iki.fi RI Kristensen, Lars/F-4774-2011; OI Kristensen, Lars/0000-0003-1159-3721; Suutarinen, Aleksi/0000-0001-5635-6418 FU European Community [238258]; Netherlands Research School for Astronomy (NOVA) FX ANS acknowledges financial support by the European Community FP7-ITN Marie-Curie Programme (grant agreement 238258). Astrochemistry in Leiden is supported by the Netherlands Research School for Astronomy (NOVA) by a Spinoza grant and by the European Community's Seventh Framework Programme FP7/2007-2013 under grant agreement 238258 (LASSIE). 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, Univ. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; the Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. The authors thank the referee for their helpful comments and questions. NR 75 TC 11 Z9 11 U1 1 U2 10 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 PY 2014 VL 440 IS 2 BP 1844 EP 1855 DI 10.1093/mnras/stu406 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5GO UT WOS:000334742200067 ER PT J AU Fragoso, GM Neale, PJ Kana, TM Pritchard, AL AF Fragoso, Glaucia M. Neale, Patrick J. Kana, Todd M. Pritchard, Alicia L. TI Kinetics of Photosynthetic Response to Ultraviolet and Photosynthetically Active Radiation in Synechococcus WH8102 (CYANOBACTERIA) SO PHOTOCHEMISTRY AND PHOTOBIOLOGY LA English DT Article ID UV-B RADIATION; REACTION-CENTER SUBUNITS; PHOTOSYSTEM-II; MARINE PICOCYANOBACTERIA; DUNALIELLA-TERTIOLECTA; SHORT-TERM; SP WH7803; PCC 6803; LIGHT; PHYTOPLANKTON AB The picoplanktonic cyanobacteria, Synechococcus spp., (Nageli) are important contributors to global ocean primary production that can be stressed by solar radiation, both in the photosynthetically active (PAR) and ultraviolet (UV) range. We studied the responses of PSII quantum yield (active fluorescence), carbon fixation (C-14 assimilation) and oxygen evolution (membrane inlet mass spectrometry) in Synechococcus WH8102 under moderate UV and PAR. PSII quantum yield decreased during exposure to moderate UV and UV+PAR, with response to the latter being faster (6.4 versus 2.8min, respectively). Repair processes were also faster when UV+PAR exposure was followed by moderate PAR (1.68min response time) than when UV was followed by very low PAR (10.5min response time). For the UV+PAR treatment, the initial decrease in quantum yield was followed by a 50% increase ("rebound") after 7min exposure, showing an apparent photoprotection induction. While oxygen uptake increased with PAR, it did not change under UV, suggesting that this oxygen-dependent mechanism of photoprotection, which may be acting as an electron sink, is not an important strategy against UV. We used propyl gallate, an antioxidant, to test for plastid terminal oxidase (ptox) or ptox-like enzymes activity, but it caused nonspecific and toxic effects on Synechococcus WH8102. C1 [Fragoso, Glaucia M.; Neale, Patrick J.; Pritchard, Alicia L.] Smithsonian Environm Res Ctr, Edgewater, MD USA. [Kana, Todd M.] Univ Maryland, Ctr Environm Sci, Cambridge, MD USA. RP Fragoso, GM (reprint author), Univ Southampton Waterfront Campus, Natl Oceanog Ctr Southampton, European Way, Southampton SO14 3ZH, Hants, England. EM glaucia.fragoso@noc.soton.ac.uk RI Fragoso, Glaucia/P-9725-2016 FU NASA [NNX09AM85G]; NSF [OCE-0727488] FX This research was supported by NASA grant NNX09AM85G to Brian Thomas, Patrick J. Neale and Adrian Melott and NSF grant OCE-0727488 to Todd Kana. The authors thank Erica Kiss (UMCES, Horn Point Laboratory), who assisted with the MIMS experiments and Emily Roberts for constructive comments and criticisms throughout the development of this manuscript. NR 51 TC 4 Z9 4 U1 0 U2 31 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0031-8655 EI 1751-1097 J9 PHOTOCHEM PHOTOBIOL JI Photochem. Photobiol. PD MAY PY 2014 VL 90 IS 3 BP 522 EP 532 DI 10.1111/php.12202 PG 11 WC Biochemistry & Molecular Biology; Biophysics SC Biochemistry & Molecular Biology; Biophysics GA AG2QN UT WOS:000335261300007 PM 24175996 ER PT J AU Fleming, CH Calabrese, JM Mueller, T Olson, KA Leimgruber, P Fagan, WF AF Fleming, Chris H. Calabrese, Justin M. Mueller, Thomas Olson, Kirk A. Leimgruber, Peter Fagan, William F. TI From Fine-Scale Foraging to Home Ranges: A Semivariance Approach to Identifying Movement Modes across Spatiotemporal Scales SO AMERICAN NATURALIST LA English DT Article DE variogram regression; variogram; continuous movement models; semivariance function; autocorrelation function; movement modes; characteristic timescales ID STATE-SPACE MODELS; ANIMAL MOVEMENT; MONGOLIAN GAZELLES; RANDOM-WALKS; PROCAPRA-GUTTUROSA; WAVELET ANALYSES; SAMPLING RATE; POPULATION; MECHANISMS; PATTERNS AB Understanding animal movement is a key challenge in ecology and conservation biology. Relocation data often represent a complex mixture of different movement behaviors, and reliably decomposing this mix into its component parts is an unresolved problem in movement ecology. Traditional approaches, such as composite random walk models, require that the timescales characterizing the movement are all similar to the usually arbitrary data-sampling rate. Movement behaviors such as long-distance searching and fine-scale foraging, however, are often intermixed but operate on vastly different spatial and temporal scales. An approach that integrates the full sweep of movement behaviors across scales is currently lacking. Here we show how the semivariance function (SVF) of a stochastic movement process can both identify multiple movement modes and solve the sampling rate problem. We express a broad range of continuous-space, continuous-time stochastic movement models in terms of their SVFs, connect them to relocation data via variogram regression, and compare them using standard model selection techniques. We illustrate our approach using Mongolian gazelle relocation data and show that gazelle movement is characterized by ballistic foraging movements on a 6-h timescale, fast diffusive searching with a 10-week timescale, and asymptotic diffusion over longer timescales. C1 [Fleming, Chris H.; Calabrese, Justin M.; Mueller, Thomas; Olson, Kirk A.; Leimgruber, Peter] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Fleming, Chris H.; Mueller, Thomas; Fagan, William F.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. Senckenberg Gesell Nat Forsch, Biodivers & Climate Res Ctr, D-60325 Frankfurt, Germany. RP Calabrese, JM (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Front Royal, VA 22630 USA. EM calabresej@si.edu RI Calabrese, Justin/B-9131-2012; Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 FU National Science Foundation [ABI-1062411, DEB-0743385, DEB-0743557] FX We thank S. Bewick for helpful comments on the manuscript and J. Blanke for sharing his composite RW code. We are also grateful to the Ministry of Environment and Green Development of Mongolia for granting permission to capture and collar gazelles. This work was supported by National Science Foundation grants ABI-1062411, DEB-0743385, and DEB-0743557. NR 42 TC 22 Z9 23 U1 7 U2 68 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 EI 1537-5323 J9 AM NAT JI Am. Nat. PD MAY 1 PY 2014 VL 183 IS 5 BP E154 EP E167 DI 10.1086/675504 PG 14 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA AE9MR UT WOS:000334332400002 PM 24739204 ER PT J AU Lin, HW Chen, YT Lacerda, P Ip, WH Holman, M Protopapas, P Chen, WP Burgett, WS Chambers, KC Flewelling, H Huber, ME Jedicke, R Kaiser, N Magnier, EA Metcalfe, N Price, PA AF Lin, H. W. Chen, Y. T. Lacerda, P. Ip, W. H. Holman, M. Protopapas, P. Chen, W. P. Burgett, W. S. Chambers, K. C. Flewelling, H. Huber, M. E. Jedicke, R. Kaiser, N. Magnier, E. A. Metcalfe, N. Price, P. A. TI PAN-STARRS 1 OBSERVATIONS OF THE UNUSUAL ACTIVE CENTAUR P/2011 S1(GIBBS) SO ASTRONOMICAL JOURNAL LA English DT Article DE comets: general; Kuiper belt objects: individual (Centaur asteroid) ID COMET 29P/SCHWASSMANN-WACHMANN 1; JUPITER-FAMILY COMETS; KUIPER-BELT OBJECTS; DUST RELEASE RATES; 2060 CHIRON; PHOTOMETRIC CALIBRATION; OUTBURST ACTIVITY; 17P/HOLMES; CO; SCHWASSMANN-WACHMANN-1 AB P/2011 S1 (Gibbs) is an outer solar system comet or active Centaur with a similar orbit to that of the famous 29P/Schwassmann-Wachmann 1. P/2011 S1 (Gibbs) has been observed by the Pan-STARRS 1 (PS1) sky survey from 2010 to 2012. The resulting data allow us to perform multi-color studies of the nucleus and coma of the comet. Analysis of PS1 images reveals that P/2011 S1 (Gibbs) has a small nucleus <4 km radius, with colors g(P1) - r(P1) = 0.5 +/- 0.02, r(P1) - i(P1) = 0.12 +/- 0.02, and i(P1) - z(P1) = 0.46 +/- 0.03. The comet remained active from 2010 to 2012, with a model-dependent mass-loss rate of similar to 100 kg s(-1). The mass-loss rate per unit surface area of P/2011 S1 (Gibbs) is as high as that of 29P/Schwassmann-Wachmann 1, making it one of the most active Centaurs. The mass-loss rate also varies with time from similar to 40 kg s(-1) to 150 kg s(-1). Due to its rather circular orbit, we propose that P/2011 S1 (Gibbs) has 29P/Schwassmann-Wachmann 1-like outbursts that control the outgassing rate. The results indicate that it may have a similar surface composition to that of 29P/Schwassmann-Wachmann 1. Our numerical simulations show that the future orbital evolution of P/2011 S1 (Gibbs) is more similar to that of the main population of Centaurs than to that of 29P/Schwassmann-Wachmann 1. The results also demonstrate that P/2011 S1 (Gibbs) is dynamically unstable and can only remain near its current orbit for roughly a thousand years. C1 [Lin, H. W.; Ip, W. H.; Chen, W. P.] Natl Cent Univ, Inst Astron, Taoyuan 32001, Taiwan. [Chen, Y. T.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Lacerda, P.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Holman, M.; Protopapas, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burgett, W. S.; Chambers, K. C.; Flewelling, H.; Huber, M. E.; Jedicke, R.; Kaiser, N.; Magnier, E. A.; Metcalfe, N.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Lin, HW (reprint author), Natl Cent Univ, Inst Astron, Taoyuan 32001, Taiwan. EM edlin@gm.astro.ncu.edu.tw OI Lin, Hsing Wen/0000-0001-7737-6784; Chambers, Kenneth /0000-0001-6965-7789; Metcalfe, Nigel/0000-0001-9034-4402 FU NSC [NSC 102-2119-M-008-001, NSC 101-2119-M-008-007-MY3]; Ministry of Education under the 5500 Program NCU; National Aeronautics and Space Administration under Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877] FX This work was supported in part by NSC grants NSC 102-2119-M-008-001 and NSC 101-2119-M-008-007-MY3 and the Ministry of Education under the 5500 Program NCU.; The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, and the University of Maryland. NR 41 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2014 VL 147 IS 5 AR 114 DI 10.1088/0004-6256/147/5/114 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3DO UT WOS:000334591900021 ER PT J AU Masters, KL Springob, CM Huchra, JP AF Masters, Karen L. Springob, Christopher M. Huchra, John P. TI 2MTF. I. THE TULLY-FISHER RELATION IN THE TWO MICRON ALL SKY SURVEY J, H, AND K BANDS (vol 135, pg 1738, 2008) SO ASTRONOMICAL JOURNAL LA English DT Correction C1 [Masters, Karen L.; Huchra, John P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Springob, Christopher M.] Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. [Springob, Christopher M.] Naval Res Lab, Remote Sensing Div Code 7213, Washington, DC 20375 USA. RP Masters, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM karen.masters@port.ac.uk NR 1 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 2014 VL 147 IS 5 AR 124 DI 10.1088/0004-6256/147/5/124 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3DO UT WOS:000334591900031 ER PT J AU Modjaz, M Blondin, S Kirshner, RP Matheson, T Berlind, P Bianco, FB Calkins, ML Challis, P Garnavich, P Hicken, M Jha, S Liu, YQ Marion, GH AF Modjaz, M. Blondin, S. Kirshner, R. P. Matheson, T. Berlind, P. Bianco, F. B. Calkins, M. L. Challis, P. Garnavich, P. Hicken, M. Jha, S. Liu, Y. Q. Marion, G. H. TI OPTICAL SPECTRA OF 73 STRIPPED-ENVELOPE CORE-COLLAPSE SUPERNOVAE SO ASTRONOMICAL JOURNAL LA English DT Article DE supernovae: general; surveys ID GAMMA-RAY BURSTS; IC SN 2007GR; RICH CIRCUMSTELLAR MEDIUM; IA SUPERNOVAE; X-RAY; IB/C SUPERNOVAE; LIGHT CURVES; MASSIVE STARS; PROGENITOR STARS; HOST GALAXIES AB We present 645 optical spectra of 73 supernovae (SNe) of Types IIb, Ib, Ic, and broad-lined Ic. All of these types are attributed to the core collapse of massive stars, with varying degrees of intact H and He envelopes before explosion. The SNe in our sample have a mean redshift < cz > = 4200 km s(-1). Most of these spectra were gathered at the Harvard-Smithsonian Center for Astrophysics (CfA) between 2004 and 2009. For 53 SNe, these are the first published spectra. The data coverage ranges from mere identification (1-3 spectra) for a few SNe to extensive series of observations (10-30 spectra) that trace the spectral evolution for others, with an average of 9 spectra per SN. For 44 SNe of the 73 SNe presented here, we have well-determined dates of maximum light to determine the phase of each spectrum. Our sample constitutes the most extensive spectral library of stripped-envelope SNe to date. We provide very early coverage (as early as 30 days before V-band max) for photospheric spectra, as well as late-time nebular coverage when the innermost regions of the SN are visible (as late as 2 yr after explosion, while for SN 1993J, we have data as late as 11.6 yr). This data set has homogeneous observations and reductions that allow us to study the spectroscopic diversity of these classes of stripped SNe and to compare these to SNe-gamma-ray bursts. We undertake these matters in follow-up papers. C1 [Modjaz, M.; Bianco, F. B.; Liu, Y. Q.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Blondin, S.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. [Kirshner, R. P.; Challis, P.; Hicken, M.; Marion, G. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Matheson, T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Berlind, P.; Calkins, M. L.] FL Whipple Observ, Amado, AZ 85645 USA. [Garnavich, P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Jha, S.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. RP Modjaz, M (reprint author), NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. EM mmodjaz@nyu.edu FU Hubble Fellowship [HST-HF-51277.01-A]; STScI; NASA [NAS5-26555]; NYU ADVANCE Women-in-Science Travel Grant; NSF ADVANCE-PAID [HRD-0820202]; National Science Foundation [AST06-06772, AST09-07903, AST-1211196, PHY99-07949, PHY11-25915]; Rutgers University in part by NSF CAREER [AST-084715]; James Arthur fellowship at the CCPP NYU FX M.M. acknowledges support from Hubble Fellowship grant HST-HF-51277.01-A, awarded by STScI, which is operated by AURA under NASA contract NAS5-26555, and from the NYU ADVANCE Women-in-Science Travel Grant funded by the NSF ADVANCE-PAID award Number HRD-0820202, during which part of this work was performed. Supernova research at Harvard University, including the CfA Supernova Archive, has been supported in part by the National Science Foundation grants AST06-06772, AST09-07903, and AST-1211196. R. P. K. is grateful to the John Simon Guggenheim Foundation and was supported by NSF grants PHY99-07949 and NSF PHY11-25915 to the Kavli Institute for Theoretical Physics. S.W.J. is supported at Rutgers University in part by NSF CAREER award AST-084715, and F. B. B. is supported by a James Arthur fellowship at the CCPP NYU. NR 163 TC 41 Z9 41 U1 0 U2 7 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 2014 VL 147 IS 5 AR 99 DI 10.1088/0004-6256/147/5/99 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3DO UT WOS:000334591900006 ER PT J AU Paggi, A Milisavljevic, D Masetti, N Jimenez-Bailon, E Chavushyan, V D'Abrusco, R Massaro, F Giroletti, M Smith, HA Margutti, R Tosti, G Martinez-Galarza, JR Oti-Floranes, H Landoni, M Grindlay, JE Funk, S AF Paggi, A. Milisavljevic, D. Masetti, N. Jimenez-Bailon, E. Chavushyan, V. D'Abrusco, R. Massaro, F. Giroletti, M. Smith, H. A. Margutti, R. Tosti, G. Martinez-Galarza, J. R. Oti-Floranes, H. Landoni, M. Grindlay, J. E. Funk, S. TI OPTICAL SPECTROSCOPIC OBSERVATIONS OF gamma-RAY BLAZAR CANDIDATES. I. PRELIMINARY RESULTS SO ASTRONOMICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; galaxies: active; radiation mechanisms: non-thermal ID BL LACERTAE OBJECTS; DIGITAL-SKY-SURVEY; LARGE-AREA TELESCOPE; EXTRAGALACTIC RADIO-SOURCES; ACTIVE GALACTIC NUCLEI; DATA RELEASE; CLUSTERING ENVIRONMENTS; DETECTED BLAZARS; SIMPLIFIED VIEW; SOURCE CATALOG AB A significant fraction (similar to 30%) of the gamma-ray sources listed in the second Fermi/LAT (2FGL) catalog is still of unknown origin, being not yet associated with counterparts at lower energies. Using the available information at lower energies and optical spectroscopy on the selected counterparts of these gamma-ray objects, we can pinpoint their exact nature. Here, we present a pilot project pointing to assess the effectiveness of the several classification methods developed to select gamma-ray blazar candidates. To this end, we report optical spectroscopic observations of a sample of five gamma-ray blazar candidates selected on the basis of their infrared Wide-field Infrared Survey Explorer (WISE) colors or of their low-frequency radio properties. Blazars come in two main classes, BL Lac objects and FSRQs, showing similar optical spectra except for the stronger emission lines of the latter. For three of our sources, the almost featureless optical spectra obtained confirm their BL Lac nature, while for the source WISEJ022051.24+250927.6 we observe emission lines with equivalent width EW similar to 31 angstrom, identifying it as a FSRQ with z = 0.48. The source WISEJ064459.38+603131.7, although not featuring a clear radio counterpart, shows a blazar-like spectrum with weak emission lines with EW similar to 7 angstrom, yielding a redshift estimate of z = 0.36. In addition, we report optical spectroscopic observations of four WISE sources associated with known gamma-ray blazars without a firm classification or redshift estimate. For the latter sources, we confirm a BL Lac classification, with a tentative redshift estimate for the source WISEJ100800.81+062121.2 of z = 0.65. C1 [Paggi, A.; Milisavljevic, D.; D'Abrusco, R.; Smith, H. A.; Margutti, R.; Martinez-Galarza, J. R.; Landoni, M.; Grindlay, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Masetti, N.; Giroletti, M.] INAF, Ist Astrofis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy. [Jimenez-Bailon, E.; Oti-Floranes, H.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. [Chavushyan, V.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico. [Massaro, F.; Funk, S.] SLAC Natl Lab, Menlo Pk, CA 94025 USA. [Massaro, F.; Funk, S.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Landoni, M.] INAF, Osservatorio Astron Brera, I-23807 Merate, Italy. [Landoni, M.] Ist Nazl Fis Nucl, Sede Milano Bicocca, I-20126 Milan, Italy. RP Paggi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Funk, Stefan/B-7629-2015; D'Abrusco, Raffaele/L-2767-2016; Massaro, Francesco/L-9102-2016; Paggi, Alessandro/C-1219-2017 OI Funk, Stefan/0000-0002-2012-0080; D'Abrusco, Raffaele/0000-0003-3073-0605; Massaro, Francesco/0000-0002-1704-9850; Paggi, Alessandro/0000-0002-5646-2410 FU NASA [NNX12AO97G, NNX13AP20G]; ASI/INAF [I/005/12/0]; CONACyT (Mexico) [129204, 151494]; 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; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX We acknowledge useful comments and suggestions from our anonymous referee. We are grateful to E. Falco for his valuable support and for the enjoyable nightly discussions at the MMT telescope. This work is supported by the NASA grant NNX12AO97G. The work at SAO is partially supported by the NASA grant NNX13AP20G. The work by G. T. is supported by the ASI/INAF contract I/005/12/0. E.J.-B. acknowledges funding by CONACyT research grant 129204 (Mexico). V. C. acknowledges funding by CONACyT research grant 151494 (Mexico). TOPCAT11 (Taylor 2005) has been used in this work for the preparation and manipulation of the tabular data and the images. The WENSS project was a collaboration between the Netherlands Foundation for Research in Astronomy and Leiden Observatory. We acknowledge the WENSS team, consisting 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. 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. This research has made use of software provided by the Chandra X-Ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa. 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. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions.; The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. The United Kingdom Infrared Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK. NR 73 TC 18 Z9 18 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2014 VL 147 IS 5 AR 112 DI 10.1088/0004-6256/147/5/112 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF3DO UT WOS:000334591900019 ER PT J AU Schrader, DL Nagashima, K Krot, AN Ogliore, RC Hellebrand, E AF Schrader, Devin L. Nagashima, Kazuhide Krot, Alexander N. Ogliore, Ryan C. Hellebrand, Eric TI Variations in the O-isotope composition of gas during the formation of chondrules from the CR chondrites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID EARLY SOLAR-SYSTEM; OXYGEN-ISOTOPE; CARBONACEOUS CHONDRITES; MAGNESIAN CHONDRULES; II CHONDRULES; PROTOPLANETARY DISK; ION MICROPROBE; PARENT BODIES; NEBULAR GAS; CONSTRAINTS AB To better understand the environment of chondrule formation and constrain the O-isotope composition of the ambient gas in the Renazzo-like carbonaceous (CR) chondrite chondrule-forming region, we studied the mineralogy, petrology, and in situ O-isotope compositions of olivine in 11 barred olivine (BO) chondrules and pyroxene and silica in three type I porphyritic chondrules from the CR chondrites Gao-Guenie (b), Graves Nunataks (GRA) 95229, Pecora Escarpment (PCA) 91082, and Shisr 033. BO chondrules experienced a higher degree of melting than porphyritic chondrules, and therefore, it has been hypothesized that they more accurately recorded the O-isotope composition of the gas in chondrule-forming regions. We studied the O-isotope composition of silica as it has been hypothesized to have formed via direct condensation from the gas. BO chondrules constitute similar to 4% of the total CR chondrule population by volume. On a three-isotope oxygen diagram (delta O-17 vs. delta O-18), olivine phenocrysts in type I and type II BO chondrules plot along similar to slope-1 line; with the exception of a type II BO chondrule that plots along similar to slope-0.5 line. Olivine phenocrysts in type I and type II BO chondrules have similar but more restricted ranges of Delta O-17 values (similar to 3.8 parts per thousand to similar to 1.3 parts per thousand and similar to-0.8 parts per thousand to similar to+1.4 parts per thousand, respectively) than those in type I and type II porphyritic chondrules (similar to-4.6 parts per thousand to similar to 0.3 parts per thousand and similar to 1.8 parts per thousand to similar to+0.9 parts per thousand, respectively). The observation that olivine grains in type I BO chondrules have similar chemical and O-isotope compositions to those of olivine in their porphyritic counterparts argues against the hypothesis that olivine grains in type I porphyritic chondrules are xenocrysts and represent relict fragments of early formed planetesimals. The compositional and O-isotope data suggest that BO chondrules experienced more extensive, but incomplete exchange with the ambient gas than porphyritic chondrules. We suggest that CR chondrules formed from relatively O-16-enriched solids in the presence of relatively O-16-depleted gaseous H2O. The O-isotope compositions of chondrule olivine likely result from differences in the O-isotope composition of both the chondrule precursors and the ambient gas during chondrule formation. The inferred O-isotope composition of this gas (Delta O-17 ranges from similar to 3 parts per thousand to +3 parts per thousand) is inconsistent with a high abundance of water from the outer Solar System, which has been predicted to be isotopically heavy. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Schrader, Devin L.; Nagashima, Kazuhide; Krot, Alexander N.; Ogliore, Ryan C.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Hellebrand, Eric] Univ Hawaii Manoa, Sch Ocean Earth Sci & Technol, Dept Geol & Geophys, Honolulu, HI 96822 USA. RP Schrader, DL (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, POB 37012,MRC 119, Washington, DC 20013 USA. EM schraderd@si.edu RI Schrader, Devin/H-6293-2012 OI Schrader, Devin/0000-0001-5282-232X FU NASA [NNX11AJ51G, NNX08AH77G, NNX10AH76G, NNX07AM62G] FX The authors are grateful to the ANSMET, JSC, MWG, NIPR, Smithsonian Institution, M. Farmer, J. Schrader, and E. Olson for samples. We thank M. Chaussidon, who kindly provided the 313 orthopyroxene standard, and J. Valley and N. Kita, who kindly provided the UVVQ-1 quartz standard. We also thank G. Huss and J. Davidson for helpful comments and discussions. Constructive comments by J. T. Wasson, an anonymous reviewer, and the Associate Editor T. R. Ireland significantly improved the quality of the manuscript. This research was funded in part by NASA grants, NNX11AJ51G (Q.-Z. Yin, PI), NNX08AH77G (K. Nagashima, PI), NNX10AH76G (A. N. Krot, PI), and NNX07AM62G (R. C. Ogliore). NR 97 TC 11 Z9 11 U1 0 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 2014 VL 132 BP 50 EP 74 DI 10.1016/j.gca.2014.01.034 PG 25 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AF6NP UT WOS:000334832100004 ER PT J AU Mingo, B Hardcastle, MJ Croston, JH Dicken, D Evans, DA Morganti, R Tadhunter, C AF Mingo, B. Hardcastle, M. J. Croston, J. H. Dicken, D. Evans, D. A. Morganti, R. Tadhunter, C. TI An X-ray survey of the 2 Jy sample - I. Is there an accretion mode dichotomy in radio-loud AGN? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; RADIATIVELY INEFFICIENT ACCRETION; OPTICALLY SELECTED QUASARS; GIGAHERTZ-PEAKED SPECTRUM; CENTRAL CLUSTER GALAXIES; XMM-NEWTON OBSERVATIONS; BL-LACERTAE OBJECTS; MASSIVE BLACK-HOLES; LESS-THAN 0.3; STELLAR POPULATIONS AB We carry out a systematic study of the X-ray emission from the active nuclei of the 0.02 < z < 0.7 2 Jy sample, using Chandra and XMM-Newton observations. We combine our results with those from mid-infrared, optical emission-line and radio observations, and add them to those of the 3CRR sources. We show that the low-excitation objects in our samples show signs of radiatively inefficient accretion. We study the effect of the jet-related emission on the various luminosities, confirming that it is the main source of soft X-ray emission for our sources. We also find strong correlations between the accretion-related luminosities, and identify several sources whose optical classification is incompatible with their accretion properties. We derive the bolometric and jet kinetic luminosities for the samples and find a difference in the total Eddington rate between the low- and high-excitation populations, with the former peaking at similar to 1 per cent and the latter at similar to 20 per cent Eddington. Our results are consistent with a simple Eddington switch when the effects of environment on radio luminosity and black hole mass calculations are considered. The apparent independence of jet kinetic power and radiative luminosity in the high-excitation population in our plots supports a model in which jet production and radiatively efficient accretion are not strongly correlated in high-excitation objects, though they have a common underlying mechanism. C1 [Mingo, B.; Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Mingo, B.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1SJ, Hants, England. [Dicken, D.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Evans, D. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morganti, R.] Netherlands Fdn Res Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Morganti, R.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Tadhunter, C.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. RP Mingo, B (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. EM bmingo@extragalactic.info OI Hardcastle, Martin/0000-0003-4223-1117 FU University of Hertfordshire; ESA Member States; NASA FX BM thanks the University of Hertfordshire for a PhD studentship. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. It has also made use of new and archival data from Chandra and software provided by the Chandra X-ray Center (CXC) in the application package CIAO. We thank Dr B. Punsly for giving us access to his data for Fig. 13. We also thank the anonymous referee for the useful comments. NR 109 TC 19 Z9 19 U1 0 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2014 VL 440 IS 1 BP 269 EP 297 DI 10.1093/mnras/stu263 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4OD UT WOS:000334691900023 ER PT J AU Torres, MAP Jonker, PG Britt, CT Johnson, CB Hynes, RI Greiss, S Steeghs, D Maccarone, TJ Ozel, F Bassa, C Nelemans, G AF Torres, M. A. P. Jonker, P. G. Britt, C. T. Johnson, C. B. Hynes, R. I. Greiss, S. Steeghs, D. Maccarone, T. J. Oezel, F. Bassa, C. Nelemans, G. TI Identification of 23 accreting binaries in the Galactic Bulge Survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; black hole physics; techniques: radial velocities; binaries: close; stars: neutron; X-rays: binaries ID X-RAY BINARIES; SPECTROGRAPH WAVELENGTH CALIBRATION; TIME-RESOLVED SPECTROSCOPY; RESOLUTION SPECTRAL ATLAS; SW SEXTANTIS STARS; T-TAURI STARS; BLACK-HOLE; CATACLYSMIC VARIABLES; EMISSION-LINES; NEUTRON-STAR AB We present the identification of optical counterparts to 23 GBS X-ray sources. All sources are classified as accreting binaries according to the emission-line characteristics inferred from medium-resolution spectroscopy. To distinguish accreting binaries from chromospherically active objects, we develop criteria based on H alpha and He i lambda lambda 5786, 6678 emission-line properties available in the literature. The spectroscopic properties and photometric variability of each object is discussed and a classification is given where possible. At least 12 of the 23 systems show an accretion-dominated optical spectrum and another 6 show stellar absorption features in addition to emission lines indicating that they are probably accreting binaries in quiescence or in a low accretion rate state. Two sources are confirmed to be eclipsing: CX207 and CX794. CX207 is likely a magnetic cataclysmic variable (CV), while CX794 is a nova-like CV in the period gap. Finally, the large broadening (2100 km s(-1) FWHM) of the H alpha emission lines in CX446 and CX1004 suggests that they are also high-inclination or even eclipsing systems. Whether the compact object is a white dwarf in an eclipsing CV, a neutron star or a black hole in a high-inclination low-mass X-ray binary remains to be established. C1 [Torres, M. A. P.; Jonker, P. G.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. [Jonker, P. G.; Nelemans, G.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 AJ Nijmegen, Netherlands. [Britt, C. T.; Johnson, C. B.; Hynes, R. I.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Britt, C. T.; Maccarone, T. J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Greiss, S.; Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Oezel, F.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Bassa, C.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Nelemans, G.] Katholieke Univ Leuven, Inst Astron, B-3001 Louvain, Belgium. RP Torres, MAP (reprint author), SRON Netherlands Inst Space Res, SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM M.Torres@sron.nl RI Nelemans, Gijs/D-3177-2012 OI Nelemans, Gijs/0000-0002-0752-2974 FU VIDI grant from the Netherlands Organization for Scientific Research; STFC through an Advanced Fellowship [PP/D005914/1]; National Science Foundation [AST-0908789]; [ST/I001719/1] FX We are thankful to Marina Rejkuba (ESO) for supporting our service mode observations with VIMOS. We are grateful to Eva Ratti, Oliwia Madej and Marianne Heida and for helping in the preparation of the VIMOS masks. We also thank Victoria Gabb and Monique Villar for assistance with Mosaic-II data analysis and Lauren Gossen for assistance at the Blanco telescope. PGJ acknowledges support from a VIDI grant from the Netherlands Organization for Scientific Research. DS acknowledges support from STFC through an Advanced Fellowship (PP/D005914/1) as well as grant ST/I001719/1 RIH, CTB and CBJ acknowledge support from the National Science Foundation under Grant no. AST-0908789. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 100 TC 8 Z9 8 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2014 VL 440 IS 1 BP 365 EP 386 DI 10.1093/mnras/stu170 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4OD UT WOS:000334691900030 ER PT J AU Bietenholz, MF De Colle, F Granot, J Bartel, N Soderberg, AM AF Bietenholz, M. F. De Colle, F. Granot, J. Bartel, N. Soderberg, A. M. TI Radio limits on off-axis GRB afterglows and VLBI observations of SN 2003gk SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: individual: (SN 2003gk); radio continuum: general ID GAMMA-RAY-BURST; IBC SUPERNOVAE; PHYSICAL PARAMETERS; LUMINOSITY FUNCTION; IC SUPERNOVAE; 1993J VLBI; JET; EMISSION; SIMULATIONS; DISCOVERY AB We report on a Very Large Array survey for late-time radio emission from 59 supernovae (SNe) of the Type I b/c, which is associated with long-duration gamma-ray bursts (GRBs). An 'off-axis' GRB burst (i. e. whose relativistic jet points away from us) is expected to have late-time radio emission even in the absence of significant prompt gamma-ray emission. From our sample, we detected only SN 2003gk with an 8.4 GHz flux density of 2260 +/- 130 mu Jy. Our subsequent very long baseline interferometry (VLBI) observations of SN 2003gk, at an age of similar to 8 yr, allowed us to determine its radius to be (2.4 +/- 0.4) x 10(17) cm, or 94 +/- 15 light days. This radius rules out relativistic expansion as expected for an off-axis GRB jet, and instead suggests an expansion speed of similar to 10 000 km s(-1) typical for non-relativistic core-collapse SNe. We attribute the late-onset radio emission to interaction of the ejecta with a dense shell caused by episodic mass-loss from the progenitor. In addition, we present new calculations for the expected radio light curves from GRB jets at various angles to the line of sight, and compare these to our observed limits on the flux densities of the remainder of our SN sample. From this comparison, we can say that only a fraction of broadlined Type I b/c SNe have a radio-bright jet similar to those seen for GRB afterglows at cosmological distances. However, we also find that for a reasonable range of parameters, as might be representative of the actual population of GRB events rather than the detected bright ones, the radio emission from the GRB jets can be quite faint, and that at present, radio observations do not place strong constraints on off-axis GRB jets. C1 [Bietenholz, M. F.] Hartebeesthoek Radio Observ, ZA-1740 Krugersdorp, South Africa. [Bietenholz, M. F.; Bartel, N.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [De Colle, F.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel. [Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bietenholz, MF (reprint author), Hartebeesthoek Radio Observ, POB 443, ZA-1740 Krugersdorp, South Africa. EM mbieten@yorku.ca OI De Colle, Fabio/0000-0002-3137-4633 FU National Research Foundation (NRF) of South Africa; NSERC; DGAPA-PAPIIT-UNAM [IA101413-2]; National Aeronautics and Space Administration FX Research at Hartebeesthoek Radio Astronomy Observatory was partly supported by National Research Foundation (NRF) of South Africa. Research at York University was partly supported by NSERC. FDC acknowledges support from the DGAPA-PAPIIT-UNAM grant IA101413-2. The National Radio Astronomy Observatory (NRAO) is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), and in alliance with Ana G. Mendez Universidad Metropolitana and the Universities Space Research Association. We have made use of NASA's Astrophysics Data System Bibliographic Services, the HyperLeda data base and 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 89 TC 6 Z9 6 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 MAY PY 2014 VL 440 IS 1 BP 821 EP 832 DI 10.1093/mnras/stu246 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF4OD UT WOS:000334691900064 ER PT J AU Negrello, M Hopwood, R Dye, S da Cunha, E Serjeant, S Fritz, J Rowlands, K Fleuren, S Bussmann, RS Cooray, A Dannerbauer, H Gonzalez-Nuevo, J Lapi, A Omont, A Amber, S Auld, R Baes, M Buttiglione, S Cava, A Danese, L Dariush, A De Zotti, G Dunne, L Eales, S Ibar, E Ivison, RJ Kim, S Leeuw, L Maddox, S Michalowski, MJ Massardi, M Pascale, E Pohlen, M Rigby, E Smith, DJB Sutherland, W Temi, P Wardlow, J AF Negrello, M. Hopwood, R. Dye, S. da Cunha, E. Serjeant, S. Fritz, J. Rowlands, K. Fleuren, S. Bussmann, R. S. Cooray, A. Dannerbauer, H. Gonzalez-Nuevo, J. Lapi, A. Omont, A. Amber, S. Auld, R. Baes, M. Buttiglione, S. Cava, A. Danese, L. Dariush, A. De Zotti, G. Dunne, L. Eales, S. Ibar, E. Ivison, R. J. Kim, S. Leeuw, L. Maddox, S. Michalowski, M. J. Massardi, M. Pascale, E. Pohlen, M. Rigby, E. Smith, D. J. B. Sutherland, W. Temi, P. Wardlow, J. TI Herschel-ATLAS: deep HST/WFC3 imaging of strongly lensed submillimetre galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: strong; galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation; infrared: galaxies; submillimetre: galaxies ID SCIENCE DEMONSTRATION PHASE; EXTRAGALACTIC SURVEY; LUMINOSITY FUNCTIONS; INFRARED-EMISSION; HIGH-REDSHIFT; SIMPLE-MODEL; BLACK-HOLES; DUST; EVOLUTION; STELLAR AB We report on deep near-infrared observations obtained with the Wide Field Camera-3 (WFC3) onboard the Hubble Space Telescope (HST) of the first five confirmed gravitational lensing events discovered by the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). We succeed in disentangling the background galaxy from the lens to gain separate photometry of the two components. The HST data allow us to significantly improve on previous constraints of the mass in stars of the lensed galaxy and to perform accurate lens modelling of these systems, as described in the accompanying paper by Dye et al. We fit the spectral energy distributions of the background sources from near-IR to millimetre wavelengths and use the magnification factors estimated by Dye et al. to derive the intrinsic properties of the lensed galaxies. We find these galaxies to have star-formations rates (SFR) similar to 400-2000 M-circle dot yr(-1), with similar to(6-25) x 10(10) M-circle dot of their baryonic mass already turned into stars. At these rates of star formation, all remaining molecular gas will be exhausted in less than similar to 100 Myr, reaching a final mass in stars of a few 10(11) M-circle dot. These galaxies are thus proto-ellipticals caught during their major episode of star formation, and observed at the peak epoch (z similar to 1.5-3) of the cosmic star formation history of the Universe. C1 [Negrello, M.; Buttiglione, S.; De Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. [Dye, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [da Cunha, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Serjeant, S.; Amber, S.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Fritz, J.; Baes, M.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Rowlands, K.] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Fleuren, S.; Sutherland, W.] Univ London, Sch Math Sci, London E1 4NS, England. [Bussmann, R. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bussmann, R. S.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Cooray, A.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dannerbauer, H.] Univ Vienna, Inst Astron, A-1160 Vienna, Austria. [Gonzalez-Nuevo, J.] Inst Fis Cantabria CSIC UC, E-39005 Santander, Spain. [Lapi, A.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Lapi, A.; Danese, L.; De Zotti, G.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Omont, A.] Univ Paris 06, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Omont, A.] CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Auld, R.; Dariush, A.; Eales, S.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Cava, A.] Univ Geneva, Observ Geneve, CH-1290 Versoix, Switzerland. [Dunne, L.; Maddox, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Ibar, E.] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile. [Ivison, R. J.] European So Observ, D-85748 Garching, Germany. [Ivison, R. J.; Michalowski, M. J.] Univ Edinburgh, Inst Astron, Scottish Univ Phys Alliance, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Kim, S.] Catholic Univ Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Leeuw, L.] UNISA, Coll Grad Studies, ZA-0003 Unisa, South Africa. [Massardi, M.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [Rigby, E.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Smith, D. J. B.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. RP Negrello, M (reprint author), Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. EM mattia.negrello@oapd.inaf.it RI Wardlow, Julie/C-9903-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Ivison, R./G-4450-2011; Cava, Antonio/C-5274-2017; OI Baes, Maarten/0000-0002-3930-2757; Maddox, Stephen/0000-0001-5549-195X; Dye, Simon/0000-0002-1318-8343; Wardlow, Julie/0000-0003-2376-8971; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Smith, Daniel/0000-0001-9708-253X; Ivison, R./0000-0001-5118-1313; Cava, Antonio/0000-0002-4821-1275; De Zotti, Gianfranco/0000-0003-2868-2595 FU STFC [PP/D002400/1, ST/G002533/1]; ASI/INAF [I/072/09/0]; PRIN-INAF; Spanish Ministerio de Ciencia e Innovacion [AYA2010-21766-C03-01]; Spanish CSIC; European Social Fund; National Aeronautics and Space Administration FX This work was supported by STFC (grants PP/D002400/1 and ST/G002533/1), by ASI/INAF agreement I/072/09/0, by PRIN-INAF 2012 project 'Looking into the dust-obscured phase of galaxy formation through cosmic zoom lenses in the Herschel Astrophysical Large Area Survey' and, in part, by the Spanish Ministerio de Ciencia e Innovacion (project AYA2010-21766-C03-01). JGN acknowledges financial support from the Spanish CSIC for a JAE-DOC fellowship, co-funded by the European Social Fund. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The Herschel-ATLAS is a project with Herschel, which is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS website is http://www.h-atlas.org/. This publication makes use of data products from the WISE, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 61 TC 26 Z9 26 U1 0 U2 15 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2014 VL 440 IS 3 BP 1999 EP 2012 DI 10.1093/mnras/stu413 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5HG UT WOS:000334744000009 ER PT J AU Dye, S Negrello, M Hopwood, R Nightingale, JW Bussmann, RS Amber, S Bourne, N Cooray, A Dariush, A Dunne, L Eales, SA Gonzalez-Nuevo, J Ibar, E Ivison, RJ Maddox, S Valiante, E Smith, M AF Dye, S. Negrello, M. Hopwood, R. Nightingale, J. W. Bussmann, R. S. Amber, S. Bourne, N. Cooray, A. Dariush, A. Dunne, L. Eales, S. A. Gonzalez-Nuevo, J. Ibar, E. Ivison, R. J. Maddox, S. Valiante, E. Smith, M. TI Herschel-ATLAS: modelling the first strong gravitational lenses SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: structure ID EARLY-TYPE GALAXIES; DARK-MATTER HALOES; SPECTROSCOPICALLY SELECTED SAMPLE; INITIAL MASS FUNCTION; DENSITY PROFILE; ACS SURVEY; SPHEROIDAL GALAXIES; LENSING STATISTICS; SWELLS SURVEY; DRY MERGERS AB We have determined the mass density radial profiles of the first five strong gravitational lens systems discovered by the Herschel Astrophysical Terahertz Large Area Survey. We present an enhancement of the semilinear lens inversion method of Warren & Dye which allows simultaneous reconstruction of several different wavebands and apply this to dual-band imaging of the lenses acquired with the Hubble Space Telescope. The five systems analysed here have lens redshifts which span a range 0.22 <= z <= 0.94. Our findings are consistent with other studies by concluding that: (1) the logarithmic slope of the total mass density profile steepens with decreasing redshift; (2) the slope is positively correlated with the average total projected mass density of the lens contained within half the effective radius and negatively correlated with the effective radius; (3) the fraction of dark matter contained within half the effective radius increases with increasing effective radius and increases with redshift. C1 [Nightingale, J. W.; Bourne, N.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Negrello, M.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Hopwood, R.; Dariush, A.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Bussmann, R. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bussmann, R. S.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Amber, S.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Bourne, N.; Ivison, R. J.] Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Cooray, A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Dunne, L.; Maddox, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand. [Eales, S. A.; Valiante, E.; Smith, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Gonzalez-Nuevo, J.] Inst Fis Cantabria CSIC UC, Santander 39005, Spain. [Ibar, E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. RP Dye, S (reprint author), Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD, England. EM simon.dye@nottingham.ac.uk RI Gonzalez-Nuevo, Joaquin/I-3562-2014; Ivison, R./G-4450-2011; OI Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Ivison, R./0000-0001-5118-1313; Maddox, Stephen/0000-0001-5549-195X; Dye, Simon/0000-0002-1318-8343 FU NASA/ESA Hubble Space Telescope under the HST programme [12194]; ASI/INAF [I/072/09/0]; PRIN-INAF; Spanish Ministerio de Ciencia e Innovacion [AYA2010-21766-C03-01]; Spanish CSIC; European Social Fund FX The work in this paper is based on observations made with the NASA/ESA Hubble Space Telescope under the HST programme #12194. MN acknowledges financial support from ASI/INAF Agreement I/072/09/0 and from PRIN-INAF 2012 project: 'Looking into the dust-obscured phase of galaxy formation through cosmic zoom lenses in the Herschel Astrophysical Large Area Survey'. JGN acknowledges financial support from the Spanish Ministerio de Ciencia e Innovacion, project AYA2010-21766-C03-01, and the Spanish CSIC for a JAE-DOC fellowship, co-funded by the European Social Fund. We thank Martin Baes and Michal Michalowski for constructive comments on this paper. We would also like to thank Adam Moss for technical discussions regarding the MCMC analysis contained herein. NR 80 TC 22 Z9 22 U1 0 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2014 VL 440 IS 3 BP 2013 EP 2025 DI 10.1093/mnras/stu305 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5HG UT WOS:000334744000010 ER PT J AU Drew, JE Gonzalez-Solares, E Greimel, R Irwin, MJ Yoldas, AK Lewis, J Barentsen, G Eisloffel, J Farnhill, HJ Martin, WE Walsh, JR Walton, NA Mohr-Smith, M Raddi, R Sale, SE Wright, NJ Groot, P Barlow, MJ Corradi, RLM Drake, JJ Fabregat, J Frew, DJ Gansicke, BT Knigge, C Mampaso, A Morris, RAH Naylor, T Parker, QA Phillipps, S Ruhland, C Steeghs, D Unruh, YC Vink, JS Wesson, R Zijlstra, AA AF Drew, J. E. Gonzalez-Solares, E. Greimel, R. Irwin, M. J. Yoldas, A. Kupcu Lewis, J. Barentsen, G. Eisloeffel, J. Farnhill, H. J. Martin, W. E. Walsh, J. R. Walton, N. A. Mohr-Smith, M. Raddi, R. Sale, S. E. Wright, N. J. Groot, P. Barlow, M. J. Corradi, R. L. M. Drake, J. J. Fabregat, J. Frew, D. J. Gaensicke, B. T. Knigge, C. Mampaso, A. Morris, R. A. H. Naylor, T. Parker, Q. A. Phillipps, S. Ruhland, C. Steeghs, D. Unruh, Y. C. Vink, J. S. Wesson, R. Zijlstra, A. A. TI The VST Photometric H alpha Survey of the Southern Galactic Plane and Bulge (VPHAS plus ) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; stars: general; H II regions; planetary nebulae: general; Galaxy: bulge; Galaxy: disc ID V458 VULPECULAE; DATA RELEASE; UVEX SURVEY; SKY SURVEY; MILKY-WAY; IPHAS; NEBULAE; CATALOG; OBJECTS; STARS AB The VST Photometric H alpha Survey of the Southern Galactic Plane and Bulge (VPHAS+) is surveying the southern Milky Way in u, g, r, i and H alpha at similar to 1 arcsec angular resolution. Its footprint spans the Galactic latitude range -5(o) < b < +5 degrees at all longitudes south of the celestial equator. Extensions around the Galactic Centre to Galactic latitudes +/- 10 degrees bring in much of the Galactic bulge. This European Southern Observatory public survey, begun on 2011 December 28, reaches down to similar to 20th magnitude (10 Sigma) and will provide single-epoch digital optical photometry for similar to 300 million stars. The observing strategy and data pipelining are described, and an appraisal of the segmented narrow-band H alpha filter in use is presented. Using model atmospheres and library spectra, we compute main-sequence (u - g), (g - r), (r - i) and (r - H alpha) stellar colours in the Vega system. We report on a preliminary validation of the photometry using test data obtained from two pointings overlapping the Sloan Digital Sky Survey. An example of the (u - g, g - r) and (r - H alpha, r - i) diagrams for a full VPHAS+ survey field is given. Attention is drawn to the opportunities for studies of compact nebulae and nebular morphologies that arise from the image quality being achieved. The value of the u band as the means to identify planetary-nebula central stars is demonstrated by the discovery of the central star of NGC 2899 in survey data. Thanks to its excellent imaging performance, the VLT Survey Telescope (VST)/OmegaCam combination used by this survey is a perfect vehicle for automated searches for reddened early-type stars, and will allow the discovery and analysis of compact binaries, white dwarfs and transient sources. C1 [Drew, J. E.; Barentsen, G.; Farnhill, H. J.; Martin, W. E.; Mohr-Smith, M.; Wright, N. J.; Ruhland, C.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Gonzalez-Solares, E.; Irwin, M. J.; Yoldas, A. Kupcu; Lewis, J.; Walton, N. A.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Greimel, R.] Graz Univ, Inst Phys, IGAM, A-8010 Graz, Austria. [Eisloeffel, J.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Walsh, J. R.] ESO Headquarters, D-85748 Garching, Germany. [Raddi, R.; Gaensicke, B. T.; Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Sale, S. E.] Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England. [Groot, P.] Radboud Univ Nijmegen, Afd Sterrenkunde, Fac NWI, NL-6500 GL Nijmegen, Netherlands. [Barlow, M. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Corradi, R. L. M.; Mampaso, A.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabregat, J.] Univ Valencia, Astron Observ, E-46980 Paterna, Spain. [Frew, D. J.; Parker, Q. A.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia. [Knigge, C.; Phillipps, S.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Morris, R. A. H.] Univ Bristol, Sch Phys, Bristol BS8 1TL, Avon, England. [Naylor, T.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Unruh, Y. C.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Dept Phys, London SW7 2AZ, England. [Vink, J. S.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Wesson, R.] European So Observ, Santiago, Chile. [Zijlstra, A. A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Drew, JE (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. EM j.drew@herts.ac.uk RI Barlow, Michael/A-5638-2009; Gaensicke, Boris/A-9421-2012; Naylor, Tim /A-9465-2015; Fabregat, Juan/F-9066-2016; Groot, Paul/K-4391-2016; OI Drew, Janet/0000-0003-1192-7082; Barlow, Michael/0000-0002-3875-1171; Gaensicke, Boris/0000-0002-2761-3005; Fabregat, Juan/0000-0002-5986-9347; Groot, Paul/0000-0002-4488-726X; Unruh, Yvonne/0000-0001-8217-6998 FU European Southern Observatory [177.D-3023]; Robert Martin Ayers Sciences Fund; NASA; NSF; Science & Technology Facilities Council of the UK (STFC) [ST/J001335/1]; European Research Council under the European Union [320964]; UK STFC [ST/I001719/1]; Spanish grants [AYA2007-66804, AYA2012-35330]; Royal Astronomical Society; European Commission FX This paper makes use of public survey data (programme 177.D-3023) obtained via queue observing at the European Southern Observatory. In respect of the H alpha filter, we would very much like to thank Bernard Muschielok for the benefit of his expertise and support in connection with its laboratory testing, and Jean-Louis Lizon for his steady hand in correcting some minor surface defects. The referee of this paper is thanked for constructive comments that improved its content.; This research made use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund. Many elements of the data analysis contained in this work have been eased greatly by the TOPCAT package created and maintained by Mark Taylor (Taylor 2005). The pipeline reduction also makes significant use of data from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF.; JED and GB acknowledge the support of a grant from the Science & Technology Facilities Council of the UK (STFC, ref ST/J001335/1). The research leading to these results has also benefitted from funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement n. 320964 (WDTracer). BTG was also supported in part by the UK STFC (ST/I001719/1). RLMC and AMR acknowledge funding from the Spanish AYA2007-66804 and AYA2012-35330 grants. HJF and MM-S both acknowledge STFC postgraduate studentships. NJW is in receipt of a Royal Astronomical Society Fellowship. RW acknowledges funding from the Marie Curie Actions of the European Commission (FP7-COFUND). NR 66 TC 40 Z9 40 U1 0 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2014 VL 440 IS 3 BP 2036 EP 2058 DI 10.1093/mnras/stu394 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5HG UT WOS:000334744000012 ER PT J AU Kipping, DM AF Kipping, David M. TI Characterizing distant worlds with asterodensity profiling SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE asteroseismology; methods: analytical; techniques: photometric; eclipses; planets and satellites: fundamental parameters ID KEPLER PLANET CANDIDATES; TRANSITING EXTRASOLAR PLANETS; LIGHT-CURVE; ECCENTRICITY DISTRIBUTION; ORBITAL ECCENTRICITIES; TIMING OBSERVATIONS; MULTIPLE SYSTEM; HOST STARS; DETECTABILITY; EXOMOON AB Eclipsing systems, such as transiting exoplanets, allow one to measure the mean stellar density of the host star under various idealized assumptions. Asterodensity profiling (AP) compares this density to an independently determined value in order to check the validity of the assumptions and ultimately derive useful parameters. Several physical effects can cause said assumptions to become invalid, with the most well-known example being the so-called photoeccentric effect. In this work, we provide analytic expressions for five other effects which induce AP deviations: the photoblend, -spot, -timing, -duration and -mass effects. We find that these effects can easily reproduce large AP deviations and so we caution that extracting the eccentricity distribution is only viable with careful consideration of the prior distributions for these other effects. We also re-investigate the photoeccentric effect and derive a single-domain minimum eccentricity expression and the parameter range for which analytic formulae are valid. The latter result shows that the assumptions underlying the analytic model for the photoeccentric effect break down for close-in, highly eccentric planets, meaning that extreme care must be taken in this regime. Finally, we demonstrate that contaminated light fraction can be solved for, indicating that AP could be a potent tool for planet validation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu FU NASA Sagan Fellowship FX DMK would like to thank D. Sliski, S. Ballard and J. Irwin for very helpful conversations in the preparation of this work. Thanks to the anonymous reviewers for their constructive comments. DMK is supported by the NASA Sagan Fellowship. NR 46 TC 25 Z9 25 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 PY 2014 VL 440 IS 3 BP 2164 EP 2184 DI 10.1093/mnras/stu318 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5HG UT WOS:000334744000020 ER PT J AU Tojeiro, R Ross, AJ Burden, A Samushia, L Manera, M Percival, WJ Beutler, F Brinkmann, J Brownstein, JR Cuesta, AJ Dawson, K Eisenstein, DJ Ho, S Howlett, C McBride, CK Montesano, F Olmstead, MD Parejko, JK Reid, B Sanchez, AG Schlegel, DJ Schneider, DP Tinker, JL Magana, MV White, M AF Tojeiro, Rita Ross, Ashley J. Burden, Angela Samushia, Lado Manera, Marc Percival, Will J. Beutler, Florian Brinkmann, J. Brownstein, Joel R. Cuesta, Antonio J. Dawson, Kyle Eisenstein, Daniel J. Ho, Shirley Howlett, Cullan McBride, Cameron K. Montesano, Francisco Olmstead, Matthew D. Parejko, John K. Reid, Beth Sanchez, Ariel G. Schlegel, David J. Schneider, Donald P. Tinker, Jeremy L. Magana, Mariana Vargas White, Martin TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: galaxy clustering measurements in the low-redshift sample of Data Release 11 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; cosmology: observations; distance scale; large-scale structure of Universe ID DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; POWER-SPECTRUM ANALYSIS; 1ST DATA RELEASE; MEASURING D-A; ACOUSTIC-OSCILLATIONS; SYSTEMATIC UNCERTAINTIES; STELLAR SPECTRA; SUPERNOVAE; DISTANCE AB We present the distance measurement to z = 0.32 using the eleventh data release (DR) of the Sloan Digital Sky Survey-III Baryon Acoustic Oscillation Survey (BOSS). We use 313 780 galaxies of the low-redshift (LOWZ) sample over 7341 square degrees to compute D-V = (1264 +/- 25)(r(d)/r(d),(fid)) - a sub 2 per cent measurement - using the baryon acoustic feature measured in the galaxy two-point correlation function and power spectrum. We compare our results to those obtained in DR10. We study observational systematics in the LOWZ sample and quantify potential effects due to photometric offsets between the northern and southern Galactic caps. We find the sample to be robust to all systematic effects found to impact on the targeting of higher redshift BOSS galaxies and that the observed north-south tensions can be explained by either limitations in photometric calibration or by sample variance, and have no impact on our final result. Our measurement, combined with the baryonic acoustic scale at z = 0.57, is used in Anderson et al. to constrain cosmological parameters. C1 [Tojeiro, Rita; Ross, Ashley J.; Burden, Angela; Samushia, Lado; Percival, Will J.; Howlett, Cullan] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Manera, Marc] UCL, London WC1E 6BT, England. [Beutler, Florian; Reid, Beth; Schlegel, David J.; White, Martin] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Brinkmann, J.; Dawson, Kyle; Olmstead, Matthew D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Brownstein, Joel R.] Apache Point Observ, Sunspot, NM 88349 USA. [Cuesta, Antonio J.; Parejko, John K.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Cuesta, Antonio J.] Univ Barcelona, IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain. [Eisenstein, Daniel J.; McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Shirley; Magana, Mariana Vargas] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Montesano, Francisco; Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Reid, Beth] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Tinker, Jeremy L.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [White, Martin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Tojeiro, R (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg,Burnaby Rd, Portsmouth PO1 3FX, Hants, England. EM rita.tojeiro@port.ac.uk RI White, Martin/I-3880-2015; OI White, Martin/0000-0001-9912-5070; Beutler, Florian/0000-0003-0467-5438; Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470 FU European Research Council; Science & Technology Facilities Council; ICG; SEPNet; University of Portsmouth; 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; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX RT is thankful for support from the European Research Council and the Science & Technology Facilities Council. Numerical computations were done on the Sciama High Performance Compute (HPC) cluster which is supported by the ICG, SEPNet and the University of Portsmouth.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, 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 62 TC 45 Z9 45 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 PY 2014 VL 440 IS 3 BP 2222 EP 2237 DI 10.1093/mnras/stu371 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5HG UT WOS:000334744000024 ER PT J AU Marinucci, A Matt, G Kara, E Miniutti, G Elvis, M Arevalo, P Ballantyne, DR Balokovic, M Bauer, F Brenneman, L Boggs, SE Cappi, M Christensen, FE Craig, WW Fabian, AC Fuerst, F Hailey, CJ Harrison, FA Risaliti, G Reynolds, CS Stern, DK Walton, DJ Zhang, W AF Marinucci, A. Matt, G. Kara, E. Miniutti, G. Elvis, M. Arevalo, P. Ballantyne, D. R. Balokovic, M. Bauer, F. Brenneman, L. Boggs, S. E. Cappi, M. Christensen, F. E. Craig, W. W. Fabian, A. C. Fuerst, F. Hailey, C. J. Harrison, F. A. Risaliti, G. Reynolds, C. S. Stern, D. K. Walton, D. J. Zhang, W. TI Simultaneous NuSTAR and XMM-Newton 0.5-80 keV spectroscopy of the narrow-line Seyfert 1 galaxy SWIFT J2127.4+5654 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; galaxies: active; galaxies: individual: SWIFT J2127.4+5654; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; HIGH-ENERGY OBSERVATIONS; PHOTON IMAGING CAMERA; RAY-EMITTING REGION; X-RAY; IRON K; BEPPOSAX OBSERVATIONS; REVERBERATION LAGS; COSMIC EVOLUTION AB We present a broad-band spectral analysis of the joint XMM-Newton and Nuclear Spectroscopic Telescope Array observational campaign of the narrow-line Seyfert 1 SWIFT J2127.4+5654, consisting of 300 ks performed during three XMM-Newton orbits. We detect a relativistic broadened iron K alpha line originating from the innermost regions of the accretion disc surrounding the central black hole, from which we infer an intermediate spin of a = 0.58(-0.17)(+0.11). The intrinsic spectrum is steep (Gamma = 2.08 +/- 0.01) as commonly found in narrow-line Seyfert 1 galaxies, while the cutoff energy (Ec = 108(-10)(+11)kev) falls within the range observed in broad-line Seyfert 1 galaxies. We measure a low-frequency lag that increases steadily with energy, while at high frequencies, there is a clear lag following the shape of the broad Fe K emission line. Interestingly, the observed Fe K lag in SWIFT J2127.4+5654 is not as broad as in other sources that have maximally spinning black holes. The lag amplitude suggests a continuum-to-reprocessor distance of about 10-20 r(g). These timing results independently support an intermediate black hole spin and a compact corona. C1 [Marinucci, A.; Matt, G.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. [Kara, E.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Miniutti, G.] Ctr Astrobiol CSIC INTA, Dep Astrofis, E-28691 Madrid, Spain. [Miniutti, G.] ESAC, E-28691 Madrid, Spain. [Elvis, M.; Brenneman, L.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Arevalo, P.; Bauer, F.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 22, Chile. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Balokovic, M.; Fuerst, F.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Cappi, M.] IASF Bologna, INAF, I-40129 Bologna, Italy. [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Risaliti, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Stern, D. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Marinucci, A (reprint author), Univ Roma Tre, Dipartimento Fis, Via Vasca Navale 84, I-00146 Rome, Italy. EM marinucci@fis.uniroma3.it RI Miniutti, Giovanni/L-2721-2014; Boggs, Steven/E-4170-2015; Cappi, Massimo/F-4813-2015; OI Miniutti, Giovanni/0000-0003-0707-4531; Boggs, Steven/0000-0001-9567-4224; Cappi, Massimo/0000-0001-6966-8920; Risaliti, Guido/0000-0002-3556-977X FU Italian Space Agency [ASI/INAFI/037/12/0-011/13]; European Union [312789]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024]; Anillo ACT1101; International Fulbright Science and Technology Award; NASA [NNG08FD60C]; National Aeronautics and Space Administration FX We thank the referee for her/his comments and suggestions that greatly improved the paper. AM thanks Javier Garcia and Thomas Dauser for the efforts in producing XILLVER and RELXILL tables to use in this paper. AM and GM acknowledge financial support from Italian Space Agency under grant ASI/INAFI/037/12/0-011/13 and from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789. PA and FB acknowledge support from Basal-CATA PFB-06/2007 (FEB), CONICYT-Chile FONDECYT 1101024 (FEB) and Anillo ACT1101 (FEB, PA). MB acknowledges support from the International Fulbright Science and Technology Award. 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). NR 69 TC 47 Z9 47 U1 1 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 PY 2014 VL 440 IS 3 BP 2347 EP 2356 DI 10.1093/mnras/stu404 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5HG UT WOS:000334744000033 ER PT J AU Saro, A Liu, J Mohr, JJ Aird, KA Ashby, MLN Bayliss, M Benson, BA Bleem, LE Bocquet, S Brodwin, M Carlstrom, JE Chang, CL Chiu, I Cho, HM Clocchiatti, A Crawford, TM Crites, AT de Haan, T Desai, S Dietrich, JP Dobbs, MA Dolag, K Dudley, JP Foley, RJ Gangkofner, D George, EM Gladders, MD Gonzalez, AH Halverson, NW Hennig, C Hlavacek-Larrondo, J Holzapfel, WL Hrubes, JD Jones, C Keisler, R Lee, AT Leitch, EM Lueker, M Luong-Van, D Mantz, A Marrone, DP McDonald, M McMahon, JJ Mehl, J Meyer, SS Mocanu, L Montroy, TE Murray, SS Nurgaliev, D Padin, S Patej, A Pryke, C Reichardt, CL Rest, A Ruel, J Ruhl, JE Saliwanchik, BR Sayre, JT Schaffer, KK Shirokoff, E Spieler, HG Stalder, B Staniszewski, Z Stark, AA Story, K van Engelen, A Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zahn, O Zenteno, A AF Saro, A. Liu, J. Mohr, J. J. Aird, K. A. Ashby, M. L. N. Bayliss, M. Benson, B. A. Bleem, L. E. Bocquet, S. Brodwin, M. Carlstrom, J. E. Chang, C. L. Chiu, I. Cho, H. M. Clocchiatti, A. Crawford, T. M. Crites, A. T. de Haan, T. Desai, S. Dietrich, J. P. Dobbs, M. A. Dolag, K. Dudley, J. P. Foley, R. J. Gangkofner, D. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. Hennig, C. Hlavacek-Larrondo, J. Holzapfel, W. L. Hrubes, J. D. Jones, C. Keisler, R. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. Mantz, A. Marrone, D. P. McDonald, M. McMahon, J. J. Mehl, J. Meyer, S. S. Mocanu, L. Montroy, T. E. Murray, S. S. Nurgaliev, D. Padin, S. Patej, A. Pryke, C. Reichardt, C. L. Rest, A. Ruel, J. Ruhl, J. E. Saliwanchik, B. R. Sayre, J. T. Schaffer, K. K. Shirokoff, E. Spieler, H. G. Stalder, B. Staniszewski, Z. Stark, A. A. Story, K. van Engelen, A. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zahn, O. Zenteno, A. TI Constraints on the CMB temperature evolution using multiband measurements of the Sunyaev-Zel'dovich effect with the South Pole Telescope SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; cosmic background radiation; cosmology: observations; cosmology: theory; submillimetre: general ID MICROWAVE BACKGROUND TEMPERATURE; PARTICLE HYDRODYNAMICS SIMULATIONS; 720 SQUARE DEGREES; GALAXY CLUSTERS; RADIATION TEMPERATURE; HIGH-REDSHIFT; T-CMB; COSMOLOGY; CATALOG; DEG(2) AB The adiabatic evolution of the temperature of the cosmic microwave background (CMB) is a key prediction of standard cosmology. We study deviations from the expected adiabatic evolution of the CMB temperature of the form T(z) = T-0(1 + z)(1 - alpha) using measurements of the spectrum of the Sunyaev-Zel'dovich effect with the South Pole Telescope (SPT). We present a method for using the ratio of the Sunyaev-Zel'dovich signal measured at 95 and 150 GHz in the SPT data to constrain the temperature of the CMB. We demonstrate that this approach provides unbiased results using mock observations of clusters from a new set of hydrodynamical simulations. We apply this method to a sample of 158 SPT-selected clusters, spanning the redshift range 0.05 < z < 1.35, and measure alpha = 0.017(-0.028)(+0.030), consistent with the standard model prediction of alpha = 0. In combination with other published results, we find alpha = 0.005 +/- 0.012, an improvement of similar to 10 per cent over published constraints. This measurement also provides a strong constraint on the effective equation of state in models of decaying dark energy w(eff) =-0.994 +/- 0.010. C1 [Saro, A.; Liu, J.; Mohr, J. J.; Bocquet, S.; Chiu, I.; Desai, S.; Dietrich, J. P.; Dolag, K.; Gangkofner, D.; Hennig, C.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Saro, A.; Liu, J.; Mohr, J. J.; Bocquet, S.; Chiu, I.; Desai, S.; Dietrich, J. P.; Dolag, K.; Gangkofner, D.; Hennig, C.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Ashby, M. L. N.; Bayliss, M.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, M.; Nurgaliev, D.; Patej, A.; Ruel, J.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Benson, B. A.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Keisler, R.; Leitch, E. M.; Mantz, A.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Inst Astrofis, Macul Santiago 7820436, Chile. [de Haan, T.; Dobbs, M. A.; Dudley, J. P.; van Engelen, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, R. J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Hlavacek-Larrondo, J.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Hlavacek-Larrondo, J.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Lueker, M.; Padin, S.; Shirokoff, E.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Saro, A (reprint author), Univ Munich, Dept Phys, Scheinerstr 1, D-81679 Munich, Germany. EM saro@usm.lmu.de RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Dietrich, Jorg/0000-0002-8134-9591; Stern, Corvin/0000-0003-4406-6127; Stark, Antony/0000-0002-2718-9996 FU DFG [TR33]; National Science Foundation [ANT-0638937]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NASA [PF2-130094]; NSF [AST-1009012, DGE-1144152, AST-1009649, MRI-0723073]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs programme; Canadian Institute for Advanced Research FX The Munich SPT group is supported by the DFG through TR33 'The Dark Universe' and the Cluster of Excellence 'Origin and Structure of the Universe'. The South Pole Telescope programme 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, by the Kavli Foundation and the Gordon and Betty Moore Foundation and by NASA grant number PF2-130094. Galaxy cluster research at Harvard is supported by NSF grants AST-1009012 and DGE-1144152. Galaxy cluster research at SAO is supported in part by NSF grants AST-1009649 and MRI-0723073. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs programme, and the Canadian Institute for Advanced Research. NR 48 TC 19 Z9 19 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 MAY PY 2014 VL 440 IS 3 BP 2610 EP 2615 DI 10.1093/mnras/stu575 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5HG UT WOS:000334744000053 ER PT J AU Keto, E Rawlings, J Caselli, P AF Keto, Eric Rawlings, Jonathan Caselli, Paola TI Chemistry and radiative transfer of water in cold, dense clouds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrochemistry; radiative transfer; ISM: abundances; ISM: individual objects: L1544; ISM: molecules ID STARLESS CORES; DARK CLOUDS; VAPOR; ABUNDANCE; DEPLETION; EMISSION; DYNAMICS; OUTFLOW; PLANETS; REGIONS AB The Herschel Space Observatory's recent detections of water vapour in the cold, dense cloud L1544 allow a direct comparison between observations and chemical models for oxygen species in conditions just before star formation. We explain a chemical model for gas-phase water, simplified for the limited number of reactions or processes that are active in extreme cold (< 15 K). In this model, water is removed from the gas phase by freezing on to grains and by photodissociation. Water is formed as ice on the surface of dust grains from O and OH and released into the gas phase by photodesorption. The reactions are fast enough with respect to the slow dynamical evolution of L1544 that the gas-phase water is in equilibrium for the local conditions throughout the cloud. We explain the paradoxical radiative transfer of the H2O (1(10)-1(01)) line. Despite discouragingly high optical depth caused by the large Einstein A coefficient, the subcritical excitation in the cold, rarefied H-2 causes the line brightness to scale linearly with column density. Thus, the water line can provide information on the chemical and dynamical processes in the darkest region in the centre of a cold, dense cloud. The inverse P-Cygni profile of the observed water line generally indicates a contracting cloud. This profile is reproduced with a dynamical model of slow contraction from unstable quasi-static hydrodynamic equilibrium (an unstable Bonnor-Ebert sphere). C1 [Keto, Eric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02420 USA. [Rawlings, Jonathan] UCL, London, England. [Caselli, Paola] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. RP Keto, E (reprint author), Harvard Smithsonian Ctr Astrophys, 160 Garden St, Cambridge, MA 02420 USA. EM keto@cfa.harvard.edu; jcr@star.ucl.ac.uk; p.caselli@leeds.ac.uk FU European Research Council (ERC) [PALs 320620]; UK Science and Technology Funding Council; Submillimeter Array Telescope FX The authors acknowledge Simon Bruderer, Fabien Daniel, Michiel Hogerheijde, Joe Mottram and Floris van der Tak for interesting discussions on the radiative transfer of water. PC acknowledges the financial support of the European Research Council (ERC; project PALs 320620) and the successive rolling grants awarded by the UK Science and Technology Funding Council. JR acknowledges the financial support of the Submillimeter Array Telescope. NR 42 TC 16 Z9 16 U1 0 U2 10 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 PY 2014 VL 440 IS 3 BP 2616 EP 2624 DI 10.1093/mnras/stu426 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5HG UT WOS:000334744000054 ER PT J AU Sanchez, AG Montesano, F Kazin, EA Aubourg, E Beutler, F Brinkmann, J Brownstein, JR Cuesta, AJ Dawson, KS Eisenstein, DJ Ho, S Honscheid, K Manera, M Maraston, C McBride, CK Percival, WJ Ross, AJ Samushia, L Schlegel, DJ Schneider, DP Skibba, R Thomas, D Tinker, JL Tojeiro, R Wake, DA Weaver, BA White, M Zehavi, I AF Sanchez, Ariel G. Montesano, Francesco Kazin, Eyal A. Aubourg, Eric Beutler, Florian Brinkmann, Jon Brownstein, Joel R. Cuesta, Antonio J. Dawson, Kyle S. Eisenstein, Daniel J. Ho, Shirley Honscheid, Klaus Manera, Marc Maraston, Claudia McBride, Cameron K. Percival, Will J. Ross, Ashley J. Samushia, Lado Schlegel, David J. Schneider, Donald P. Skibba, Ramin Thomas, Daniel Tinker, Jeremy L. Tojeiro, Rita Wake, David A. Weaver, Benjamin A. White, Martin Zehavi, Idit TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological implications of the full shape of the clustering wedges in the data release 10 and 11 galaxy samples SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmological parameters; large-scale structure of Universe ID DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; MICROWAVE BACKGROUND ANISOTROPIES; POWER-SPECTRUM ANALYSIS; SOUTH-POLE TELESCOPE; PROBING DARK ENERGY; SPT-SZ SURVEY; ACOUSTIC-OSCILLATIONS; REDSHIFT SURVEYS; PARAMETER CONSTRAINTS AB We explore the cosmological implications of the angle-averaged correlation function, xi(s), and the clustering wedges, xi(perpendicular to)(s) and xi()(s), of the LOWZ and CMASS galaxy samples from Data Releases 10 and 11 of the Sloan Digital Sky Survey III (SDSS-III) Baryon Oscillation Spectroscopic Survey. Our results show no significant evidence for a deviation from the standard Lambda cold dark matter model. The combination of the information from our clustering measurements with recent data from the cosmic microwave background is sufficient to constrain the curvature of the Universe to (k) = 0.0010 +/- 0.0029, the total neutrino mass to Sigma m(nu) < 0.23 eV (95 per cent confidence level), the effective number of relativistic species to N-eff = 3.31 +/- 0.27 and the dark energy equation of state to w(DE) = -1.051 +/- 0.076. These limits are further improved by adding information from Type Ia supernovae and baryon acoustic oscillations from other samples. In particular, this data set combination is completely consistent with a time-independent dark energy equation of state, in which case we find w(DE) = -1.024 +/- 0.052. We explore the constraints on the growth rate of cosmic structures assuming f(z) = (m)(z)(gamma) and obtain gamma = 0.69 +/- 0.15, consistent with the predictions of general relativity of gamma = 0.55. C1 [Sanchez, Ariel G.; Montesano, Francesco] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Kazin, Eyal A.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Kazin, Eyal A.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Aubourg, Eric] Univ Paris Diderot, APC, CNRS IN2P3, CEA IRFU,Observ Paris,Sorbonne Paris Cite, Paris, France. [Beutler, Florian; Schlegel, David J.; White, Martin] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Brinkmann, Jon] Apache Point Observ, Sunspot, NM 88349 USA. [Brownstein, Joel R.; Dawson, Kyle S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Cuesta, Antonio J.] Univ Barcelona, Inst Ciencies Cosmos, IEEC UB, E-08028 Barcelona, Spain. [Cuesta, Antonio J.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Eisenstein, Daniel J.; McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Shirley] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Ho, Shirley] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Honscheid, Klaus] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Honscheid, Klaus] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Manera, Marc] UCL, London WC1E 6BT, England. [Manera, Marc; Maraston, Claudia; Percival, Will J.; Ross, Ashley J.; Samushia, Lado; Thomas, Daniel; Tojeiro, Rita] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Samushia, Lado] Ilia State Univ, Natl Abastumani Astrophys Observ, GE-1060 Tbilisi, Rep of Georgia. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Skibba, Ramin] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Tinker, Jeremy L.; Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Wake, David A.] Univ Wisconsin Madison, Dept Astron, Madison, WI 53706 USA. [Wake, David A.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. RP Sanchez, AG (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312,Giessenbachstr, D-85741 Garching, Germany. EM arielsan@mpe.mpg.de RI White, Martin/I-3880-2015; OI White, Martin/0000-0001-9912-5070; Beutler, Florian/0000-0003-0467-5438; Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470 FU Trans-regional Collaborative Research Centre TR33 'The Dark Universe' of the German Research Foundation (DFG); Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; ICG; SEPNet; University of Portsmouth; ESA Member States; NASA; NASA Office of Space Science FX We would like to thank the referee, Will Sutherland, for his careful reading of our manuscript and his suggestions to improve the quality of the publication. AGS would like to thank Ximena Mazzalay for useful discussions. AGS and FM acknowledge support from the Trans-regional Collaborative Research Centre TR33 'The Dark Universe' of the German Research Foundation (DFG). EK is supported by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020.; Numerical computations for the PTHALOS mocks were done on the Sciama High Performance Compute (HPC) cluster which is supported by the ICG, SEPNet and the University of Portsmouth.; This work is based on observations obtained with Planck (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA and Canada. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. NR 111 TC 45 Z9 45 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 MAY PY 2014 VL 440 IS 3 BP 2692 EP 2713 DI 10.1093/mnras/stu342 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AF5HG UT WOS:000334744000060 ER PT J AU Kornis, MS Carlson, J Lehrer-Brey, G Vander Zanden, MJ AF Kornis, Matthew S. Carlson, Jedchada Lehrer-Brey, Gabrielle Vander Zanden, M. Jake TI Experimental evidence that ecological effects of an invasive fish are reduced at high densities SO OECOLOGIA LA English DT Article DE Species interactions; Invasive species; Round goby; Density impact relationship; Great Lakes ID GOBIES NEOGOBIUS-MELANOSTOMUS; GREAT-LAKES TRIBUTARIES; ROUND GOBY; INTERSPECIFIC COMPETITION; FIELD EXPERIMENTS; MOTTLED SCULPIN; COTTUS-BAIRDI; INTERFERENCE COMPETITION; BIOLOGICAL INVASIONS; DREISSENA-POLYMORPHA AB Understanding the relationship between invasive species density and ecological impact is a pressing topic in ecology, with implications for environmental management and policy. Although it is widely assumed that invasive species impact will increase with density, theory suggests interspecific competition may diminish at high densities due to increased intraspecific interactions. To test this theory, we experimentally examined intra- and interspecific interactions between a globally invasive fish, round goby (Neogobius melanostomus), and three native species at different round goby densities in a tributary of the Laurentian Great Lakes. Eighteen 2.25 m(2) enclosures were stocked with native fish species at natural abundances, while round gobies were stocked at three different densities: 0 m(-2), 2.7 m(-2), and 10.7 m(-2). After 52 days, native fish growth rate was significantly reduced in the low density goby treatment, while growth in the high density goby treatment mirrored the goby-free treatment for two of three native species. Invertebrate density and gut content weight of native fishes did not differ among treatments. Conversely, gut content weight and growth of round gobies were lower in the high goby density treatment, suggesting interactions between round gobies and native fishes are mediated by interference competition amongst gobies. Our experiment provides evidence that invasive species effects may diminish at high densities, possibly due to increased intraspecific interactions. This is consistent with some ecological theory, and cautions against the assumption that invasive species at moderate densities have low impact. C1 [Kornis, Matthew S.; Carlson, Jedchada; Lehrer-Brey, Gabrielle; Vander Zanden, M. Jake] Univ Wisconsin, Ctr Limnol, Madison, WI 53706 USA. RP Kornis, MS (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM kornism@si.edu FU University of Wisconsin Sea Grant Institute, federal Grant [NA06OAR4170011, R/AI-3] FX We thank Hans Martin for assistance with enclosure construction and with invertebrate analysis. We also thank Mary Szela for granting permission to use her land for the experiment. Bobbi Peckarsky, John Magnuson, and two anonymous reviewers provided valuable assistance in framing our arguments. Tammi Paoli assisted with acquiring permits. Erika Nilsson, Patrik Stenroth, Scott Higgins, and Ryan Batt assisted with specimen collection and enclosure extraction. This work was funded by a grant from the University of Wisconsin Sea Grant Institute, federal Grant Number NA06OAR4170011 project number R/AI-3, to M.J.V.Z. NR 67 TC 13 Z9 13 U1 10 U2 70 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 2014 VL 175 IS 1 BP 325 EP 334 DI 10.1007/s00442-014-2899-5 PG 10 WC Ecology SC Environmental Sciences & Ecology GA AF4OB UT WOS:000334691600030 PM 24532212 ER PT J AU Ceron-Souza, I Turner, BL Winter, K Medina, E Bermingham, E Feliner, GN AF Ceron-Souza, Ivania Turner, Benjamin L. Winter, Klaus Medina, Ernesto Bermingham, Eldredge Feliner, Gonzalo N. TI Reproductive phenology and physiological traits in the red mangrove hybrid complex (Rhizophora mangle and R-racemosa) across a natural gradient of nutrients and salinity SO PLANT ECOLOGY LA English DT Article DE Introgressive hybridization; Salinity tolerance; Nutrient limitation; Flowering time; Microsatellites; Water-use efficiency ID MULTILOCUS GENOTYPE DATA; SUNFLOWER HELIANTHUS-ANNUUS; ADAPTIVE INTROGRESSION; LOUISIANA IRISES; KANDELIA-CANDEL; PHOTOSYNTHESIS; PATTERNS; GROWTH; DELTA-N-15; INFERENCE AB Factors modulating introgressive hybridization between the red mangrove species Rhizophora mangle and R. racemosa in spatially defined sites are poorly understood. To investigate this, we evaluated the reproductive phenology and the nutrient and physiological traits in those two species and their F-1 hybrids genotyped with microsatellite data across a natural hybrid zone from the Pacific coast of Panama. We found no evidence that reproductive phenology represents a barrier to gene flow, because R. mangle and the F-1 hybrids produced flowers and propagules throughout the annual cycle, while R. racemosa flowered only in the dry season. Soil nutrient concentrations decreased landward, while soil salinity varied only slightly. Foliar nutrients and delta N-15 signatures varied according to the soil nutrient gradient, but only foliar phosphorus and carbon varied among species. In contrast, two structural variables (height and trunk diameter) and leaf variables related to salinity tolerance (Na, Cl:Na, K:Na, cation:anion) and water-use efficiency (i.e., delta C-13) differed among species, suggesting higher salinity tolerance for R. mangle and F-1 hybrids compared with R. racemosa. We conclude that parental species and F-1 hybrids differ in salinity tolerance and water-use efficiency, which could be associated with adaptive evolution of the red mangrove hybrid complex. C1 [Turner, Benjamin L.; Winter, Klaus; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Ceron-Souza, Ivania] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [Medina, Ernesto] IVIC, Ctr Ecol, Caracas 1020A, Venezuela. [Feliner, Gonzalo N.] CSIC, Real Jardin Bot, E-28014 Madrid, Spain. RP Ceron-Souza, I (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM iviceron@gmail.com RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU BBVA Foundation in Spain; Secretaria Nacional de Ciencia; Tecnologia e Innovacion-SENACYT [FID-0927]; Smithsonian Tropical Research Institute-STRI in Panama FX This study was supported by grants from the BBVA Foundation in Spain, Secretaria Nacional de Ciencia, Tecnologia e Innovacion-SENACYT (FID-0927) and Smithsonian Tropical Research Institute-STRI in Panama. The authors thank to Autoridad Nacional del Ambiente-ANAM in Panama for study permits and logistic support in the province of Anton-Cocle; J. Chavarria, G. Jaramillo, G. J. Jaramillo, L. Jaramillo, S. Martinez and L. Rodriguez for field assistance; D. Agudo for laboratory support; J. Touchon and S. Dennis for their suggestions in the statistical analysis and L. Santiago for his comments to improve the manuscript. NR 63 TC 3 Z9 3 U1 1 U2 29 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 2014 VL 215 IS 5 BP 481 EP 493 DI 10.1007/s11258-014-0315-1 PG 13 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA AF0OM UT WOS:000334413900001 ER PT J AU Slater, GJ Pennell, MW AF Slater, Graham J. Pennell, Matthew W. TI Robust Regression and Posterior Predictive Simulation Increase Power to Detect Early Bursts of Trait Evolution SO SYSTEMATIC BIOLOGY LA English DT Article DE Adaptive Radiations; Early Burst; Posterior Predictive Simulations; Quantitative Characters ID MORPHOLOGICAL DIVERSIFICATION; ECOLOGICAL OPPORTUNITY; PHENOTYPIC DIVERSIFICATION; STABILIZING SELECTION; PHYLOGENETIC SIGNAL; ADAPTIVE RADIATIONS; LIMITING SIMILARITY; MODEL SELECTION; FOSSIL RECORD; RANDOM-WALKS AB A central prediction of much theory on adaptive radiations is that traits should evolve rapidly during the early stages of a clade's history and subsequently slowdown in rate as niches become saturated-a so-called "Early Burst." Although a common pattern in the fossil record, evidence for early bursts of trait evolution in phylogenetic comparative data has been equivocal at best. We show here that this may not necessarily be due to the absence of this pattern in nature. Rather, commonly used methods to infer its presence perform poorly when when the strength of the burst-the rate at which phenotypic evolution declines-is small, and when some morphological convergence is present within the clade. We present two modifications to existing comparative methods that allow greater power to detect early bursts in simulated datasets. First, we develop posterior predictive simulation approaches and show that they outperform maximum likelihood approaches at identifying early bursts at moderate strength. Second, we use a robust regression procedure that allows for the identification and down-weighting of convergent taxa, leading to moderate increases in method performance. We demonstrate the utility and power of these approach by investigating the evolution of body size in cetaceans. Model fitting using maximum likelihood is equivocal with regards the mode of cetacean body size evolution. However, posterior predictive simulation combined with a robust node height test return low support for Brownian motion or rate shift models, but not the early burst model. While the jury is still out on whether early bursts are actually common in nature, our approach will hopefully facilitate more robust testing of this hypothesis. We advocate the adoption of similar posterior predictive approaches to improve the fit and to assess the adequacy of macroevolutionary models in general. [Adaptive Radiations, Early Burst, Posterior Predictive Simulations, Quantitative Characters]. C1 [Slater, Graham J.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Slater, Graham J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Slater, Graham J.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Pennell, Matthew W.] Univ Idaho, Inst Bioinformat & Evolutionary Studies, Moscow, ID 83844 USA. [Pennell, Matthew W.] Natl Evolutionary Synth Ctr, Durham, NC 27705 USA. RP Slater, GJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM SlaterG@si.edu FU National Science Foundation [DEB 0918748, DEB 1208912]; Peter Buck Smithsonian Institution post-doctoral fellowship; National Evolutionary Synthesis Center; University of Idaho FX G.J.S. was supported in part by National Science Foundation grant DEB 0918748 to Michael Alfaro and Luke Harmon, and in part by a Peter Buck Smithsonian Institution post-doctoral fellowship. M. W. P. was funded by a National Evolutionary Synthesis Center Graduate Fellowship, a Bioinformatics and Computational Biology Graduate Fellowship from the University of Idaho, and a National Science Foundation grant DEB 1208912 to Luke Harmon. NR 95 TC 22 Z9 22 U1 3 U2 25 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1063-5157 EI 1076-836X J9 SYST BIOL JI Syst. Biol. PD MAY PY 2014 VL 63 IS 3 BP 293 EP 308 DI 10.1093/sysbio/syt066 PG 16 WC Evolutionary Biology SC Evolutionary Biology GA AF5KO UT WOS:000334752600002 PM 24149077 ER PT J AU Souto, T Deichmann, JL Nunez, C Alonso, A AF Souto, Tamia Deichmann, Jessica L. Nunez, Cecilia Alonso, Alfonso TI Classifying conservation targets based on the origin of motivation: implications over the success of community-based conservation projects SO BIODIVERSITY AND CONSERVATION LA English DT Article DE Motivators for conservation; Participation; Indigenous and local people; Conservation target; Biodiversity conservation; Project design ID HUMAN-WILDLIFE CONFLICT; CONCEPTUAL-FRAMEWORK; HUMAN-NEEDS; LIVELIHOODS; PRIORITIES; FORESTS; RISK AB Community-based conservation (CBC) projects represent one approach to biodiversity conservation when working with indigenous and local people. This method aims to achieve conservation and development goals simultaneously, however whether both types of goals can be met or whether competition between the two precludes success is an issue of much discussion. Conservation targets are one of the most important elements upon which a conservation project is built. We propose that one way to link biodiversity conservation with human development goals is to consider people's needs and interests in the selection of the conservation target. Here, we present three categories of conservation targets that vary according to the origin of motivation that drives indigenous and local people to conserve the target. According to the type of target selected, the level of participation, integration of traditional ecological knowledge, level of external intervention and long-term sustainability will vary. We encourage conservation practitioners to understand the motivations that lead indigenous and local people to participate in conservation projects, and to develop and design CBC projects from these incentives. C1 [Souto, Tamia; Deichmann, Jessica L.; Nunez, Cecilia; Alonso, Alfonso] Natl Zool Pk, Ctr Conservat Educ & Sustainabil, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. RP Souto, T (reprint author), Natl Zool Pk, Ctr Conservat Educ & Sustainabil, Smithsonian Conservat Biol Inst, MRC 0705, Washington, DC 20013 USA. EM soutot@si.edu; deichmannj@si.edu; cecilianunez@gmail.com; alonsoa@si.edu FU Smithsonian Conservation Biology Institute; Repsol Exploracion Peru FX We are very grateful to the Miaria and Nuevo Mundo communities in Peru, and the CCES team in Lima and Washington DC for rich discussions and logistical support. This work was supported by the Smithsonian Conservation Biology Institute and Repsol Exploracion Peru. This is contribution # 24 of the CCES Peru Biodiversity Program. NR 28 TC 2 Z9 3 U1 10 U2 54 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 EI 1572-9710 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD MAY PY 2014 VL 23 IS 5 BP 1331 EP 1337 DI 10.1007/s10531-014-0659-9 PG 7 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AE3SX UT WOS:000333898600015 ER PT J AU Campbell, JE Fourqurean, JW AF Campbell, Justin E. Fourqurean, James W. TI Ocean acidification outweighs nutrient effects in structuring seagrass epiphyte communities SO JOURNAL OF ECOLOGY LA English DT Article DE climate change; determinants of plant community diversity and structure; CO2; filamentous algae; eutrophication; coralline algae; Thalassia testudinum; CCA; carbon dioxide; plant-climate interactions ID FLORIDA BAY; THALASSIA-TESTUDINUM; COASTAL ECOSYSTEMS; ZOSTERA-MARINA; CARBONATE ENVIRONMENT; MACROALGAL BLOOMS; INORGANIC CARBON; CLIMATE-CHANGE; CO2; ENRICHMENT AB Developing a framework for assessing interactions between multiple anthropogenic stressors remains an important goal in environmental research. In coastal ecosystems, the relative effects of aspects of global climate change (e.g. CO2 concentrations) and localized stressors (e.g. eutrophication), in combination, have received limited attention. Using a long-term (11month) field experiment, we examine how epiphyte assemblages in a tropical seagrass meadow respond to factorial manipulations of dissolved carbon dioxide (CO2(aq)) and nutrient enrichment. In situ CO2(aq) manipulations were conducted using clear, open-top chambers, which replicated carbonate parameter forecasts for the year 2100. Nutrient enrichment consisted of monthly additions of slow-release fertilizer, nitrogen (N) and phosphorus (P), to the sediments at rates equivalent to theoretical maximum rates of anthropogenic loading within the region (1.54gNm(-2)d(-1) and 0.24gPm(-2)d(-1)). Epiphyte community structure was assessed on a seasonal basis and revealed declines in the abundance of coralline algae, along with increases in filamentous algae under elevated CO2(aq). Surprisingly, nutrient enrichment had no effect on epiphyte community structure or overall epiphyte loading. Interactions between CO2(aq) and nutrient enrichment were not detected. Furthermore, CO2(aq)-mediated responses in the epiphyte community displayed strong seasonality, suggesting that climate change studies in variable environments should be conducted over extended time-scales. Synthesis. The observed responses indicate that for certain locations, global stressors such as ocean acidification may take precedence over local eutrophication in altering the community structure of seagrass epiphyte assemblages. Given that nutrient-driven algal overgrowth is commonly cited as a widespread cause of seagrass decline, our findings highlight that alternate climate change forces may exert proximate control over epiphyte community structure. C1 [Campbell, Justin E.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Fourqurean, James W.] Florida Int Univ, Dept Biol Sci, Marine Sci Program, Miami, FL 33199 USA. [Fourqurean, James W.] Florida Int Univ, Southeast Environm Res Ctr, Miami, FL 33199 USA. RP Campbell, JE (reprint author), Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. EM campbellju@si.edu OI Fourqurean, James/0000-0002-0811-8500 FU National Science Foundation [DBI-0620409]; Florida International University FX We thank Dr. Patrick Rice and the Florida Keys Community College for logistical support. Jennifer Sweatman, Bryan Dewsbury, Nathan Lemoine and Thomas Frankovich provided assistance in the field. This work was supported by the National Science Foundation through the Florida Coastal Everglades Long-Term Ecological Research Program under Grant No. DBI-0620409, and a Graduate School Doctoral Evidence Acquisition Fellowship awarded to J.E.C by Florida International University. This is contribution number 654 from the Southeast Environmental Research Center at FIU. The authors declare no conflict of interest. NR 62 TC 11 Z9 11 U1 3 U2 103 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 2014 VL 102 IS 3 BP 730 EP 737 DI 10.1111/1365-2745.12233 PG 8 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA AF3CE UT WOS:000334588300019 ER PT J AU de Silva, P Jaramillo, C Bernal, XE AF de Silva, Priyanka Jaramillo, Cesar Bernal, Ximena E. TI Feeding Site Selection by Frog-Biting Midges (Diptera: Corethrellidae) on Anuran Hosts SO JOURNAL OF INSECT BEHAVIOR LA English DT Article DE Biting behavior; blood feeding; skin characteristics; mouthparts; optimal foraging ID AEDES-AEGYPTI L; CARBON-DIOXIDE; ANOPHELES-ARABIENSIS; DEFENSIVE BEHAVIOR; MOSQUITOS DIPTERA; SPECIES DIPTERA; TUNGARA FROG; BLOOD; CULICIDAE; SUCCESS AB A critical challenge of obtaining a blood meal resides in selecting a feeding site at the host. We investigate the feeding sites of species of frog-biting midges (Corethrella spp) on tungara frogs, Engystomops pustulosus (Cope), and two species of treefrogs, Dendropsophus ebraccatus (Cope) and Dendropsophus microcephalus (Cope). To investigate the differences in midge feeding sites, we performed field observations, histological sections of the frogs and examined the mouthparts of the midges. Feeding sites are predicted by the vascular properties of the skin in different body areas of the frogs. According to optimal foraging theory, the midges should feed on host body areas that maximize blood intake. Contrary to optimal foraging theory predictions, however, their feeding sites correspond to body areas with high intensity host defensive behavior. C1 [de Silva, Priyanka] Texas Tech Univ, Dept Biol Sci, Lubbock, TX 79409 USA. [Jaramillo, Cesar] Univ Panama, Dept Histol & Neuroanat Humana, Fac Med, Panama City, Panama. [Jaramillo, Cesar; Bernal, Ximena E.] Smithsonian Trop Res Inst, Balboa, Panama. [Bernal, Ximena E.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. RP de Silva, P (reprint author), Texas Tech Univ, Dept Biol Sci, POB 43131, Lubbock, TX 79409 USA. EM priyanka.desilva@ttu.edu FU National Science Foundation (NSF) [IOS-1258039] FX We are thankful to Lewis Held for his help and advice with the midge dissections and Art Borkent for his suggestions that helped improve this work. We are also grateful to two anonymous reviewers that provided valuable comments to improve this manuscript. The Smithsonian Tropical Research Institute provided critical logistic support. We are also thankful to the ANAM (Autoridad Nacional del Ambiente, Panama) which provided the required permits to collect and export specimens (No. SE/A-50-09, No. SEX/A-60-09). This work was supported by the National Science Foundation (NSF) grant IOS-1258039 to X.E.B. NR 59 TC 4 Z9 5 U1 2 U2 11 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0892-7553 EI 1572-8889 J9 J INSECT BEHAV JI J. Insect Behav. PD MAY PY 2014 VL 27 IS 3 BP 302 EP 316 DI 10.1007/s10905-013-9428-y PG 15 WC Entomology SC Entomology GA AE3PT UT WOS:000333889100002 ER PT J AU Breed, WG Leigh, CM Aplin, KP Shahin, AAB Avenant, NL AF Breed, William G. Leigh, Chris M. Aplin, Ken P. Shahin, Adel A. B. Avenant, Nico L. TI Morphological Diversity and Evolution of the Spermatozoon in the Mouse-Related Clade of Rodents SO JOURNAL OF MORPHOLOGY LA English DT Article DE sperm evolution; Spalacidae; Dipodidae; Pedetidae; Heteromyidae ID SPERM COMPETITION; MUROID RODENTS; MURINE RODENTS; SIZE; DIVERSIFICATION; PHYLOGENY AB Most species in the three highly speciose families of the mouse-related clade of rodents, the Muridae, Cricetidae, and Nesomyidae (superfamily Muroidea), have a highly complex sperm head in which there is an apical hook but there are few data available for the other related families of these rodents. In the current study, using light and electron microscopies, we investigated the structure of the spermatozoon in representative species of four other families within the mouse-related clade, the Dipodidae, Spalacidae, Pedetidae, and Heteromyidae, that diverged at or near the base of the muroid lineage. Our results indicate that a diverse array of sperm head shapes and tail lengths occurs but none of the species in the families Spalacidae, Dipodidae, or Pedetidae has a sperm head with an apical hook. By contrast, a rostrally extending apical hook is present in spermatozoa of members of the Family Heteromyidae which also invariably have comparatively long sperm tails. These findings suggest that the hook-shaped sperm head in the murid, cricetid, and nesomyid rodents evolved after divergence of this lineage from its common ancestor with the other families of the mouse-related clade, and that separate, and independent, convergent evolution of a similar sperm head form, and long sperm tail, occurred in the Heteromyidae. J. Morphol. 275:540-547, 2014. (c) 2013 Wiley Periodicals, Inc. C1 [Breed, William G.; Leigh, Chris M.] Univ Adelaide, Sch Med Sci, Discipline Anat & Pathol, Adelaide, SA 5005, Australia. [Aplin, Ken P.] Smithsonian Inst, Div Mammals, Natl Museum Nat Hist, Washington, DC 20013 USA. [Shahin, Adel A. B.] Menia Univ, Dept Zool, Fac Sci, El Minia 61519, Egypt. [Avenant, Nico L.] Natl Museum, Dept Mammal, Bloemfontein, South Africa. RP Breed, WG (reprint author), Univ Adelaide, Sch Med Sci, Discipline Anat & Pathol, Adelaide, SA 5005, Australia. EM bill.breed@adelaide.edu.au NR 40 TC 3 Z9 3 U1 2 U2 10 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 MAY PY 2014 VL 275 IS 5 BP 540 EP 547 DI 10.1002/jmor.20236 PG 8 WC Anatomy & Morphology SC Anatomy & Morphology GA AE4UX UT WOS:000333981600007 PM 24338943 ER PT J AU Baker, TR Pennington, RT Magallon, S Gloor, E Laurance, WF Alexiades, M Alvarez, E Araujo, A Arets, EJMM Aymard, G de Oliveira, AA Amaral, I Arroyo, L Bonal, D Brienen, RJW Chave, J Dexter, KG Di Fiore, A Eler, E Feldpausch, TR Ferreira, L Lopez-Gonzalez, G van der Heijden, G Higuchi, N Honorio, E Huamantupa, I Killeen, TJ Laurance, S Leano, C Lewis, SL Malhi, Y Marimon, BS Marimon, BH Mendoza, AM Neill, D Penuela-Mora, MC Pitman, N Prieto, A Quesada, CA Ramirez, F Angulo, HR Rudas, A Ruschel, AR Salomao, RP de Andrade, AS Silva, JNM Silveira, M Simon, MF Spironello, W ter Steege, H Terborgh, J Toledo, M Torres-Lezama, A Vasquez, R Vieira, ICG Vilanova, E Vos, VA Phillips, OL AF Baker, Timothy R. Pennington, R. Toby Magallon, Susana Gloor, Emanuel Laurance, William F. Alexiades, Miguel Alvarez, Esteban Araujo, Alejandro Arets, Eric J. M. M. Aymard, Gerardo de Oliveira, Atila Alves Amaral, Ieda Arroyo, Luzmila Bonal, Damien Brienen, Roel J. W. Chave, Jerome Dexter, Kyle G. Di Fiore, Anthony Eler, Eduardo Feldpausch, Ted R. Ferreira, Leandro Lopez-Gonzalez, Gabriela van der Heijden, Geertje Higuchi, Niro Honorio, Euridice Huamantupa, Isau Killeen, Tim J. Laurance, Susan Leano, Claudio Lewis, Simon L. Malhi, Yadvinder Marimon, Beatriz Schwantes Marimon Junior, Ben Hur Monteagudo Mendoza, Abel Neill, David Cristina Penuela-Mora, Maria Pitman, Nigel Prieto, Adriana Quesada, Carlos A. Ramirez, Fredy Ramirez Angulo, Hirma Rudas, Agustin Ruschel, Ademir R. Salomao, Rafael P. de Andrade, Ana Segalin Silva, J. Natalino M. Silveira, Marcos Simon, Marcelo F. Spironello, Wilson ter Steege, Hans Terborgh, John Toledo, Marisol Torres-Lezama, Armando Vasquez, Rodolfo Guimaraes Vieira, Ima Celia Vilanova, Emilio Vos, Vincent A. Phillips, Oliver L. TI Fast demographic traits promote high diversification rates of Amazonian trees SO ECOLOGY LETTERS LA English DT Article DE generation time; tropical forest; Diversity; traits; turnover ID SPECIES RICHNESS; ECOLOGICAL LIMITS; DIVERGENCE TIMES; LIFE-HISTORY; DIVERSITY; EVOLUTION; PATTERNS; FORESTS; CLIMATE; CLADES AB The Amazon rain forest sustains the world's highest tree diversity, but it remains unclear why some clades of trees are hyperdiverse, whereas others are not. Using dated phylogenies, estimates of current species richness and trait and demographic data from a large network of forest plots, we show that fast demographic traits - short turnover times - are associated with high diversification rates across 51 clades of canopy trees. This relationship is robust to assuming that diversification rates are either constant or decline over time, and occurs in a wide range of Neotropical tree lineages. This finding reveals the crucial role of intrinsic, ecological variation among clades for understanding the origin of the remarkable diversity of Amazonian trees and forests. C1 [Baker, Timothy R.; Gloor, Emanuel; Brienen, Roel J. W.; Feldpausch, Ted R.; Lopez-Gonzalez, Gabriela; Honorio, Euridice; Lewis, Simon L.; Phillips, Oliver L.] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. [Pennington, R. Toby; Dexter, Kyle G.] Royal Bot Garden Edinburgh, Edinburgh EH3 5LR, Midlothian, Scotland. [Magallon, Susana] Univ Nacl Autonoma Mexico, Inst Biol, Mexico City 04510, DF, Mexico. [Laurance, William F.; Laurance, Susan] James Cook Univ, Ctr Trop Environm & Sustainabil Sci TESS, Cairns, Qld 4878, Australia. [Laurance, William F.; Laurance, Susan] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4878, Australia. [Alexiades, Miguel] Univ Kent, Sch Anthropol & Conservat, Canterbury CT2 7NR, Kent, England. [Alvarez, Esteban] Univ Tolima, Fac Ingn Forestal, Ibaque, Colombia. [Araujo, Alejandro; Arroyo, Luzmila] Museo Hist Nat Noel Kempff Mercado, Santa Cruz, Bolivia. [Arets, Eric J. M. M.] Univ Wageningen & Res Ctr, Alterra, NL-6708 PB Wageningen, Netherlands. [Aymard, Gerardo] Herbario Univ PORT, Guanare, Venezuela. [de Oliveira, Atila Alves; Amaral, Ieda; Eler, Eduardo; Spironello, Wilson] Inst Nacl de Pesquisas da Amazonia, Projeto TEAM Manaus, BR-69067375 Manaus, Amazonas, Brazil. [Bonal, Damien] UMR EEF INRA Univ Lorraine, INRA, F-54280 Champenoux, France. [Chave, Jerome] CNRS, F-31062 Toulouse, France. [Chave, Jerome] Univ Toulouse 3, UMR EDB 5174, F-31062 Toulouse, France. [Dexter, Kyle G.] Univ Edinburgh, Sch GeoSci, Edinburgh EH9 3JW, Midlothian, Scotland. [Di Fiore, Anthony] Univ Texas Austin, Dept Anthropol, Austin, TX 78712 USA. [Ferreira, Leandro; Salomao, Rafael P.; Guimaraes Vieira, Ima Celia] Museu Paraense Emilio Goeldi, BR-66040170 Belem, Para, Brazil. [van der Heijden, Geertje] Univ Wisconsin, Sch Freshwater Sci, Milwaukee, WI 53201 USA. [van der Heijden, Geertje] Smithsonian Trop Res Inst, Panama City, Panama. [Higuchi, Niro; Quesada, Carlos A.] Inst Nacl de Pesquisas da Amazonia, BR-69067375 Manaus, Amazonas, Brazil. [Honorio, Euridice] Inst Invest Amazonia Peruana, Iquitos, Peru. [Huamantupa, Isau] Univ Nacl San Antonio Abad Cusco, Herbario CUZ, Cuzco, Peru. [Killeen, Tim J.] Conservat Int, Arlington, VA USA. [Leano, Claudio; Toledo, Marisol] Inst Boliviano Invest Forestal, Santa Cruz, Bolivia. [Lewis, Simon L.] Univ London Univ Coll, Dept Geog, London WC1E 6BT, England. [Malhi, Yadvinder] Univ Oxford, Sch Geog & Environm, Environm Change Inst, Oxford OX1 3QY, England. [Marimon, Beatriz Schwantes; Marimon Junior, Ben Hur] Univ Estado Mato Grosso, BR-78690000 Nova Xavantina, Brazil. [Monteagudo Mendoza, Abel; Vasquez, Rodolfo] Jardin Bot Missouri, Oxapampa, Peru. [Neill, David] Univ Estatal Amazonica, Puyo, Ecuador. [Cristina Penuela-Mora, Maria] Univ Nacl Colombia, Sede Amazonia, Leticia, Colombia. [Pitman, Nigel; Terborgh, John] Duke Univ, Nicholas Sch Environm, Ctr Trop Conservat, Durham, NC 27705 USA. [Prieto, Adriana; Rudas, Agustin] Univ Nacl Colombia, Inst Ciencias Nat, Bogota, Colombia. [Ramirez, Fredy] Univ Nacl Amazonia Peruana, Iquitos, Peru. [Ramirez Angulo, Hirma; Torres-Lezama, Armando; Vilanova, Emilio] Univ Los Andes, INDEFOR, Merida, Venezuela. [Ruschel, Ademir R.] Embrapa Amazonia Oriental, BR-66095100 Belem, Para, Brazil. [de Andrade, Ana Segalin] Inst Nacl de Pesquisas da Amazonia, PDBFF, BR-69067375 Manaus, Amazonas, Brazil. [Silva, J. Natalino M.] Univ Fed Rural Amazonia, BR-66077830 Belem, Para, Brazil. [Silva, J. Natalino M.] Inst Floresta Trop, BR-66025660 Belem, Para, Brazil. [Silveira, Marcos] Univ Fed Acre, Museu Univ, BR-69920900 Rio Branco, Brazil. [Simon, Marcelo F.] Embrapa Recursos Genet & Biotecnol, BR-70770900 Brasilia, DF, Brazil. [ter Steege, Hans] Naturalis Biodivers Ctr, NL-2333 CR Leiden, Netherlands. [ter Steege, Hans] Univ Utrecht, Ecol & Biodivers Grp, Dept Biol, NL-3508 TB Utrecht, Netherlands. [Vos, Vincent A.] Univ Autonoma Beni, Riberalta, Bolivia. RP Baker, TR (reprint author), Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. EM t.r.baker@leeds.ac.uk RI Arets, Eric/C-1050-2008; James Cook University, TESS/B-8171-2012; Research ID, CTBCC /O-3564-2014; Laurance, Susan/G-6021-2011; Honorio Coronado, Euridice/K-3412-2015; Marimon, Beatriz/J-6389-2012; ter Steege, Amaz/B-5866-2011; Phillips, Oliver/A-1523-2011; Feldpausch, Ted/D-3436-2009; Silveira, Marcos/H-7906-2013; Marimon Junior, Ben Hur/E-7330-2013 OI Arets, Eric/0000-0001-7209-9028; Vos, Vincent Antoine/0000-0002-0388-8530; Lewis, Simon/0000-0002-8066-6851; Laurance, Susan/0000-0002-2831-2933; Honorio Coronado, Euridice/0000-0003-2314-590X; ter Steege, Amaz/0000-0002-8738-2659; Phillips, Oliver/0000-0002-8993-6168; Feldpausch, Ted/0000-0002-6631-7962; Silveira, Marcos/0000-0003-0485-7872; FU Gordon and Betty Moore Foundation; National Environmental Research Council [NE/I028122/1, NE/F005806/1]; European Commission [282664, 283080]; Royal Society; National Geographic Society; Tropenbos International; European Commission; NASA Longterm Biosphere-Atmosphere Project in Amazonia (LBA); Brazilian National Council for Scientific and Technological Development (CNPq) [558069/2009-6]; projeto INCT Processo [574008/2008-0]; National Institute for Amazonian Research (INPA), Brazil; Tropical Ecology Assessment and Monitoring (TEAM) Network, a collaboration among Conservation International; Missouri Botanical Garden; Smithsonian Institution; Wildlife Conservation Society; French ANR [CEBA: ANR-10-LABX-0025, TULIP: ANR-10-LABX-0041]; European Research Council project 'Tropical Forests in the Changing Earth System' FX This analysis is based on contributions to the RAINFOR network and ForestPlots. net database (http://www.forestplots.net), and supported by the Gordon and Betty Moore Foundation, National Environmental Research Council (grant numbers NE/I028122/1, NE/F005806/1), the European Commission [FP 5, 6 & 7 including the AMAZALERT (282664) and GEOCARBON (283080) projects)] and the Royal Society. Additional funding for fieldwork was provided by the National Geographic Society, Tropenbos International, European Commission, NASA Longterm Biosphere-Atmosphere Project in Amazonia (LBA), Brazilian National Council for Scientific and Technological Development (CNPq) including the long-term ecological research program CNPq/PELD Sitio 15 Transicao Cerrado - Floresta Amazonica (558069/2009-6) and projeto INCT Processo 574008/2008-0, the National Institute for Amazonian Research (INPA), Brazil and the Tropical Ecology Assessment and Monitoring (TEAM) Network, a collaboration among Conservation International, the Missouri Botanical Garden, the Smithsonian Institution, and the Wildlife Conservation Society, and partially funded by these institutions, the Gordon and Betty Moore Foundation and Investissement d'Avenir grants of the French ANR (CEBA: ANR-10-LABX-0025; TULIP: ANR-10-LABX-0041), as well as other donors. OP, SL and GL-G are supported by the European Research Council project 'Tropical Forests in the Changing Earth System'. We thank Tiina Saarkinen for assisting with clade ages for Fabaceae, David Greenberg for valuable discussions and Rick Condit for advice using lmerBayes. NR 48 TC 17 Z9 17 U1 4 U2 91 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 2014 VL 17 IS 5 BP 527 EP 536 DI 10.1111/ele.12252 PG 10 WC Ecology SC Environmental Sciences & Ecology GA AD9EW UT WOS:000333568600001 PM 24589190 ER PT J AU Cavanaugh, KC Gosnell, JS Davis, SL Ahumada, J Boundja, P Clark, DB Mugerwa, B Jansen, PA O'Brien, TG Rovero, F Sheil, D Vasquez, R Andelman, S AF Cavanaugh, Kyle C. Gosnell, J. Stephen Davis, Samantha L. Ahumada, Jorge Boundja, Patrick Clark, David B. Mugerwa, Badru Jansen, Patrick A. O'Brien, Timothy G. Rovero, Francesco Sheil, Douglas Vasquez, Rodolfo Andelman, Sandy TI Carbon storage in tropical forests correlates with taxonomic diversity and functional dominance on a global scale SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE Aboveground carbon storage; tropical forest; functional dominance; Africa; functional diversity; biodiversity; Neotropics; Asia; taxonomic diversity; niche complementarity ID ECOSYSTEM FUNCTION; SPECIES RICHNESS; PLANT DIVERSITY; WOOD DENSITY; ABOVEGROUND BIOMASS; AMAZONIAN FOREST; SPATIAL-PATTERNS; MULTIPLE TRAITS; PRODUCTIVITY; BIODIVERSITY AB Aim We examined (1) the relationships between aboveground tropical forest C storage, biodiversity and environmental drivers and (2) how these relationships inform theory concerning ecosystem function and biodiversity. Experiments have shown that there is a positive relationship between biodiversity and ecosystem functioning, but intense debate exists on the underlying mechanisms. While some argue that mechanisms such as niche complementarity increase ecosystem function, others argue that these relationships are a selection effect. Location Eleven tropical forests in the Americas, Africa and Asia. Methods We analysed the correlates of biodiversity and carbon storage in tropical forests using data from 59 1-ha tree plots from a standardized global tropical forest biodiversity-monitoring network. We examined taxonomic and functional diversity, aboveground C storage and environmental variables in order to determine the relationships between biodiversity and carbon storage in natural (non-plantation) tropical forests. Results We found that aboveground C storage in tropical forests increased with both taxonomic diversity and functional dominance, specifically the dominance of genera with large maximum diameters, after potential environmental drivers were accounted for (final model R-2 = 0.38, P < 0.001). Main conclusions Our results suggest that niche complementarity and the selection effect are not mutually exclusive: they both play a role in structuring tropical forests. While previous studies have documented relationships between diversity and C storage, these have largely been conducted on small scales in biomes that are relatively species poor compared with tropical forests (e.g. grasslands and temperate or boreal forests). Our results demonstrate that these positive biodiversity-ecosystem functioning relationships are also present in hyperdiverse systems on spatial scales relevant to conservation and management. This insight can be used to inform the conservation and management of tropical forests, which play a critical role in the global carbon cycle and are some of the biologically richest ecosystems on the planet. C1 [Cavanaugh, Kyle C.] Smithsonian Inst, Edgewater, MD 21037 USA. [Cavanaugh, Kyle C.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Gosnell, J. Stephen; Davis, Samantha L.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Ahumada, Jorge; Andelman, Sandy] Conservat Int, Trop Ecol Assessment & Monitoring Network, Moore Ctr Ecosyst Sci & Econ, Arlington, VA USA. [Clark, David B.] Univ Missouri, St Louis, MO 63121 USA. [Mugerwa, Badru; Sheil, Douglas] MUST, ITFC, Kabale, Uganda. [Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Jansen, Patrick A.] Wageningen Univ, Resource Ecol Grp, NL-6700 AA Wageningen, Netherlands. [O'Brien, Timothy G.] Wildlife Conservat Soc, Bronx, NY 10460 USA. [Rovero, Francesco] MUSE Museo Sci, Trop Biodivers Sect, I-38123 Trento, Italy. [Sheil, Douglas] So Cross Univ, Sch Environm Sci & Engn, Lismore, NSW 2480, Australia. [Sheil, Douglas] Ctr Int Forestry Res, Bogor 16000, Indonesia. [Vasquez, Rodolfo] Jardin Bot Missouri, Oxapampa, Pasco, Peru. RP Cavanaugh, KC (reprint author), Smithsonian Inst, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM cavanaughk@si.edu RI Sheil, Douglas/A-3867-2015; Jansen, Patrick/G-2545-2015 OI Sheil, Douglas/0000-0002-1166-6591; Jansen, Patrick/0000-0002-4660-0314 FU Gordon and Betty Moore Foundation; NASA [TE08-0037, TE11-0100]; SERNANP-PNYCh; National Science Foundation Dimensions of Biodiversity grant [1050680] FX All data in this publication were provided by the TEAM Network, a collaboration between Conservation International, the Missouri Botanical Garden, 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 Darley Calderado Leal Matos, Johanna Hurtado, Richard Condit, Leandro Valle Ferreira, Ieda Amaral, Nurul Winarni, Meyner Nusalawo, Emanuel Martin, David Kenfack, Christine Dawn Fletcher, Jean Claude Andrianantenaina and all the field staff at the following TEAM sites for their hard and invaluable work: Bukit Barisan, Barro Colorado Island, Bwindi Impenetrable Forest, Caxiuana, Manaus, Nouabale Ndoki, Pasoh Forest Reserve, Ranomafana, Udzungwa, Volcan Barva and Yanachaga Chimillen National Park. Fieldwork for the Costa Rican plots was partially supported by NASA grants TE08-0037 and TE11-0100. Thanks to SERNANP-PNYCh for their support. This research was supported by a Graduate Distributed Seminar Series made possible by a National Science Foundation Dimensions of Biodiversity grant (1050680) to SA and Julia Parish. NR 59 TC 24 Z9 26 U1 6 U2 99 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 MAY PY 2014 VL 23 IS 5 BP 563 EP 573 DI 10.1111/geb.12143 PG 11 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA AD7BV UT WOS:000333417100005 ER PT J AU Polishook, D Moskovitz, N Binzel, RP DeMeo, FE Vokrouhlicky, D Zizka, J Oszkiewicz, D AF Polishook, David Moskovitz, Nicholas Binzel, Richard P. DeMeo, Francesca E. Vokrouhlicky, David Zizka, Jindrich Oszkiewicz, Dagmara TI Observations of "fresh" and weathered surfaces on asteroid pairs and their implications on the rotational-fission mechanism SO ICARUS LA English DT Article DE Asteroids; Asteroids rotation; Asteroids surfaces; Rotational dynamics; Spectroscopy ID NEAR-EARTH ASTEROIDS; MAIN BELT ASTEROIDS; SPIN RATE DISTRIBUTION; RUBBLE-PILE ASTEROIDS; BINARY ASTEROIDS; SPECTRAL PROPERTIES; ORDINARY CHONDRITE; SOURCE REGIONS; ORIGIN; ENCOUNTERS AB The rotational-fission of a "rubble-pile" structured asteroid can result in an "asteroid pair" - two unbound asteroids sharing nearly identical heliocentric orbits. Models suggest that this mechanism exposes material from below the progenitor surface that previously had never have been exposed to the weathering conditions of space. Therefore, the surfaces of asteroid pairs offer the opportunity to observe non-weathered "fresh" spectra. Here we report near-infrared spectroscopic observations of 31 asteroids in pairs. In order to search for spectral indications of fresh surfaces we analyze their spectral slopes, parameters of their li.tm absorption band and taxonomic classification. Additionally, through backward dynamical integration we estimate the time elapsed since the disintegration of the pairs' progenitors. Analyzing the 19 ordinary chondrite-like (S-complex) objects in our sample, we find two Q-type Asteroids (19289 and 54827) that are the first of their kind to be observed in the main-belt of asteroids over the full visible and near-infrared range. This solidly demonstrates that the Q-type taxonomy is not limited to the NEA population. The pairs in our sample present a range of fresh and weathered surfaces with no clear evidence for a correlation with the ages of the pairs. However, our sample includes "old" pairs (2 x 10(6) >= age >= 1 x 10(6) years) that present relatively low, meteoritic-like spectral slopes (<0.2% per mu m). This illustrates a timescale of at least similar to 2 myr before an object develops high spectral slope that is typical for S-type asteroids. We discuss three mechanisms that explain the existence of weathered pairs with young dynamical ages and find that the "secondary fission" model (Jacobson, S.-A., Scheeres, D.-J. [2011]. Icarus 214, 161-178) is the most robust with our observations. In this mechanism an additional and subsequent fission of the secondary component contributes the lion share of fresh material that re-settles on the primary's surface and recoats it with fresh material. If the secondary breaks loose from the vicinity of the primary before its "secondary fission", this main source of fresh dust is avoided. We prefer this secondary fission model since (i) the secondary members in our sample present "fresh" parameters that tend to be "fresher" than their weathered primaries; (ii) most of the fresh pairs in our sample have low size ratios between the secondary and the primary; (iii) 33% of the primaries in our sample are fresh, similar to the prediction set by the secondary fission model (Jacobson, S.-A., Scheeres, D.-J. [2011]. Icarus 214, 161178); (iv) known satellites orbit two of the pairs in our sample with low size ratio (D-2/D-1) and fresh surface; (v) there is no correlation between the weathering state and the primary shape as predicted by other models. (C) 2014 Elsevier Inc. All rights reserved. C1 [Polishook, David; Moskovitz, Nicholas; Binzel, Richard P.; DeMeo, Francesca E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [DeMeo, Francesca E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vokrouhlicky, David; Zizka, Jindrich] Charles Univ Prague, Inst Astron, CZ-18000 Prague 8, Czech Republic. [Oszkiewicz, Dagmara] Adam Mickiewicz Univ, Fac Phys, Astron Observ Inst, PL-60286 Poznan, Poland. RP Polishook, D (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM davidpol@mit.edu FU AXA research fund; National Science Foundation Astronomy; Astrophysics Postdoctoral fellowship program; RPB acknowledges NASA Near-Earth Object Observation program [NNX10AG27G]; National Science Foundation [0907766, 6920422]; NASA [NNX12AL26G]; Hubble Fellowship [HST-HF-51319.01-A]; Space Telescope Science Institute; Czech Grant Agency [209/12/0229]; Polish National Science Center [2012/04/S/ST9/00022] FX We thank Seth Jacobson, Kevin Walsh, Paul Sanchez and Stephen Wolters for fruitful discussions, Bobby Bus for his help with the IRTF observations and data, Petr Pravec for sharing with us his pre-published data and Brad S. Cenko for his observations at the Lick Observatory. We thank Vishnu Reddy and Mark Willman for their useful reviews. DP is grateful to the AXA research fund for their generous postdoctoral fellowship. NM would like to acknowledge support from the National Science Foundation Astronomy and Astrophysics Postdoctoral fellowship program. RPB acknowledges NASA Near-Earth Object Observation program support through Grant NNX10AG27G. FED acknowledges support by the National Science Foundation under Grant 0907766 and by NASA under Grant NNX12AL26G and through Hubble Fellowship Grant HST-HF-51319.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under Contract NAS 526555. The work of DV and JZ was supported by the Czech Grant Agency (Grant 209/12/0229). DO was supported by Polish National Science Center, Grant Number NCN 2012/04/S/ST9/00022. This study was supported by the National Science Foundation under Grant 6920422. 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. Observations reported here were obtained at the InfraRed Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement NCC 5-538 with NASA, Science Mission Directorate, Planetary Astronomy Program. This paper also includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile and 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 Institut de Astrofisica de Canarias. We appreciate the Hawaiian, Chilean, Californian, Spanish and Israeli people for allowing us to use their sacred mountains for astronomy. NR 85 TC 8 Z9 8 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAY 1 PY 2014 VL 233 BP 9 EP 26 DI 10.1016/j.icarus.2014.01.014 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE1KX UT WOS:000333729300002 ER PT J AU Breedy, O Guzman, HM AF Breedy, Odalisca Guzman, Hector M. TI A new species of alcyonacean octocoral from the Peruvian zoogeographic region SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article DE Peruvian zoogeographic region; biodiversity; Octocorallia; eastern Pacific; plexaurids; marine protected area; octocorals; new species; Psammogorgia ID COELENTERATA; GORGONIIDAE; ECOSYSTEM; REVISION; FUTURE AB The first record of the plexaurid genus Psammogorgia from the shallow waters of Peru is reported here. A new species (Psammogorgia hookeri sp. nov.) is described from Isla San Gallan, Paracas National Reserve. The new species was morphologically analysed using light microscopy and scanning electron microscopy. It is distinguished from the others in the genus by its small size; prominent calyces with wide lips around polyp apertures and without a special type of sclerites, but with a concentration of irregular, thorny spindles and wart-clubs around the calyx rim; coenenchymal sclerites that do not reach more than 0.2mm long; the occurrence of conspicuous star-like radiates; and the colour of the colony and coenenchymal sclerites, which is coral red. The results increase species richness within a genus that has not been studied for more than a century, and contribute to the establishment of characters for further morphological studies. Additionally, the new species adds value to existing protected areas and to the octocoral biodiversity records for the Peruvian region and the eastern Pacific. C1 [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, Ctr Invest Estruct Microscop, San Jose, Costa Rica. [Breedy, Odalisca; Guzman, Hector M.] Smithsonian Trop Res Inst, Panama City, Panama. RP Breedy, O (reprint author), Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, Ctr Invest Estruct Microscop, POB 11501-2060, San Jose, Costa Rica. EM odaliscab@gmail.com FU Vicerrectoria de Investigacion; Universidad de Costa Rica; Smithsonian Tropical Research Institute in Panama FX This project was partially funded by the Vicerrectoria de Investigacion, Universidad de Costa Rica, and the Smithsonian Tropical Research Institute in Panama. NR 22 TC 2 Z9 2 U1 0 U2 7 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0025-3154 EI 1469-7769 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD MAY PY 2014 VL 94 IS 3 BP 493 EP 498 DI 10.1017/S0025315413001835 PG 6 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AD9CD UT WOS:000333561300006 ER PT J AU Touchton, JM Seddon, N Tobias, JA AF Touchton, Janeene M. Seddon, Nathalie Tobias, Joseph A. TI Captive Rearing Experiments Confirm Song Development without Learning in a Tracheophone Suboscine Bird SO PLOS ONE LA English DT Article ID LONG-TAILED MANAKIN; SEXUAL SELECTION; VOCAL DISTINCTIVENESS; EVOLUTION; SONGBIRDS; REPERTOIRES; DIVERGENCE; PASSERINE; ANTBIRDS; DRIVE AB The origin of vocal learning in animals has long been the subject of debate, but progress has been limited by uncertainty regarding the distribution of learning mechanisms across the tree of life, even for model systems such as birdsong. In particular, the importance of learning is well known in oscine songbirds, but disputed in suboscines. Members of this diverse group (similar to 1150 species) are generally assumed not to learn their songs, but empirical evidence is scarce, with previous studies restricted to the bronchophone (non-tracheophone) clade. Here, we conduct the first experimental study of song development in a tracheophone suboscine bird by rearing spotted antbird (Hylophylax naevioides) chicks in soundproofed aviaries. Individuals were raised either in silence with no tutor or exposed to standardized playback of a heterospecific tutor. All individuals surviving to maturity took a minimum of 79 days to produce a crystallized version of adult song, which in all cases was indistinguishable from wild song types of their own species. These first insights into song development in tracheophone suboscines suggest that adult songs are innate rather than learnt. Given that empirical evidence for song learning in suboscines is restricted to polygamous and lek-mating species, whereas tracheophone suboscines are mainly monogamous with long-term social bonds, our results are consistent with the view that sexual selection promotes song learning in birds. C1 [Touchton, Janeene M.] Smithsonian Trop Res Inst, Balboa, Panama. [Touchton, Janeene M.] Max Planck Inst Ornithol, Radolfzell am Bodensee, Germany. [Seddon, Nathalie; Tobias, Joseph A.] Univ Oxford, Dept Zool, Edward Grey Inst, Oxford OX1 3PS, England. RP Touchton, JM (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM touchtonj@gmail.com OI Tobias, Joseph/0000-0003-2429-6179 FU Royal Society [ATJCZRJ2]; Smithsonian Institution Fellowship FX This research was funded by a Royal Society Research Grant (ATJCZRJ2) to J.A.T., a Royal Society Research Fellowship to N.S., and a Smithsonian Institution Fellowship to J.M.T. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 61 TC 5 Z9 6 U1 8 U2 33 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 30 PY 2014 VL 9 IS 4 AR e95746 DI 10.1371/journal.pone.0095746 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AL1WP UT WOS:000338917300017 PM 24788343 ER PT J AU Larson, G Piperno, DR Allaby, RG Purugganan, MD Andersson, L Arroyo-Kalin, M Barton, L Vigueira, CC Denham, T Dobney, K Doust, AN Gepts, P Gilbert, MTP Gremillion, KJ Lucas, L Lukens, L Marshall, FB Olsen, KM Pires, JC Richerson, PJ de Casas, RR Sanjur, OI Thomas, MG Fuller, DQ AF Larson, Greger Piperno, Dolores R. Allaby, Robin G. Purugganan, Michael D. Andersson, Leif Arroyo-Kalin, Manuel Barton, Loukas Vigueira, Cynthia Climer Denham, Tim Dobney, Keith Doust, Andrew N. Gepts, Paul Gilbert, M. Thomas P. Gremillion, Kristen J. Lucas, Leilani Lukens, Lewis Marshall, Fiona B. Olsen, Kenneth M. Pires, J. Chris Richerson, Peter J. Rubio de Casas, Rafael Sanjur, Oris I. Thomas, Mark G. Fuller, Dorian Q. TI Current perspectives and the future of domestication studies SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Editorial Material DE evolution; selection; agriculture; human ecology; human history ID CORE AREA HYPOTHESIS; LOW ATMOSPHERIC CO2; AGRICULTURAL ORIGINS; ANIMAL DOMESTICATION; PLANT DOMESTICATION; RESEQUENCING REVEALS; MAIZE DOMESTICATION; CROP DOMESTICATION; MOLECULAR EVIDENCE; FERTILE CRESCENT AB It is difficult to overstate the cultural and biological impacts that the domestication of plants and animals has had on our species. Fundamental questions regarding where, when, and how many times domestication took place have been of primary interest within a wide range of academic disciplines. Within the last two decades, the advent of new archaeological and genetic techniques has revolutionized our understanding of the pattern and process of domestication and agricultural origins that led to our modern way of life. In the spring of 2011, 25 scholars with a central interest in domestication representing the fields of genetics, archaeobotany, zooarchaeology, geoarchaeology, and archaeology met at the National Evolutionary Synthesis Center to discuss recent domestication research progress and identify challenges for the future. In this introduction to the resulting Special Feature, we present the state of the art in the field by discussing what is known about the spatial and temporal patterns of domestication, and controversies surrounding the speed, intentionality, and evolutionary aspects of the domestication process. We then highlight three key challenges for future research. We conclude by arguing that although recent progress has been impressive, the next decade will yield even more substantial insights not only into how domestication took place, but also when and where it did, and where and why it did not. C1 [Larson, Greger] Univ Durham, Dept Archaeol, Durham Evolut & Ancient DNA, Durham DH1 3LE, England. [Piperno, Dolores R.] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. [Piperno, Dolores R.; Sanjur, Oris I.] Smithsonian Trop Res Inst, Balboa, Panama. [Allaby, Robin G.] Univ Warwick, Sch Life Sci, Coventry CV4 7AL, W Midlands, England. [Purugganan, Michael D.] NYU, Dept Biol, New York, NY 10003 USA. [Andersson, Leif] Uppsala Univ, Dept Med Biochem & Microbiol, SE-75123 Uppsala, Sweden. [Andersson, Leif] Swedish Univ Agr Sci, Dept Anim Breeding & Genet, SE-75007 Uppsala, Sweden. [Arroyo-Kalin, Manuel; Lucas, Leilani; Fuller, Dorian Q.] UCL, Inst Anthropol, London WC1H 0PY, England. [Barton, Loukas] Univ Pittsburgh, Ctr Comparat Archaeol, Dept Anthropol, Pittsburgh, PA 15260 USA. [Vigueira, Cynthia Climer; Olsen, Kenneth M.] Washington Univ, Dept Biol, St Louis, MO 63130 USA. [Marshall, Fiona B.] Washington Univ, Dept Anthropol, St Louis, MO 63130 USA. [Denham, Tim] Australian Natl Univ, Coll Arts & Social Sci, Sch Archaeol & Anthropol, Canberra, ACT 0200, Australia. [Dobney, Keith] Univ Aberdeen, Dept Archaeol, Aberdeen AB24 3UF, Scotland. [Doust, Andrew N.] Oklahoma State Univ, Dept Bot, Stillwater, OK 74078 USA. [Gepts, Paul] Univ Calif Davis, Sect Crop & Ecosyst Sci, Dept Plant Sci MS1, Davis, CA 95616 USA. [Richerson, Peter J.] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. [Gilbert, M. Thomas P.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, DK-1350 Copenhagen, Denmark. Univ Copenhagen, Nat Hist Museum Denmark, Sect Evolutionary Genom, DK-1350 Copenhagen, Denmark. [Gremillion, Kristen J.] Ohio State Univ, Dept Anthropol, Columbus, OH 43210 USA. [Lukens, Lewis] Univ Guelph, Dept Plant Agr, Guelph, ON N1G 2W1, Canada. [Pires, J. Chris] Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA. [Rubio de Casas, Rafael] Univ Granada, Fac Ciencias, Dept Ecol, E-18071 Granada, Spain. [Thomas, Mark G.] UCL, Res Dept Genet Evolut & Environm, London WC1E 6BT, England. RP Larson, G (reprint author), Univ Durham, Dept Archaeol, Durham Evolut & Ancient DNA, Durham DH1 3LE, England. EM greger.larson@durham.ac.uk RI Gilbert, Marcus/A-8936-2013; Thomas, Mark/A-2219-2012 OI Gilbert, Marcus/0000-0002-5805-7195; Thomas, Mark/0000-0002-2452-981X NR 112 TC 74 Z9 74 U1 17 U2 177 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 29 PY 2014 VL 111 IS 17 BP 6139 EP 6146 DI 10.1073/pnas.1323964111 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AG1TL UT WOS:000335199000026 PM 24757054 ER PT J AU Gremillion, KJ Barton, L Piperno, DR AF Gremillion, Kristen J. Barton, Loukas Piperno, Dolores R. TI Particularism and the retreat from theory in the archaeology of agricultural origins SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE evolutionary theory; behavioral ecology ID BROAD-SPECTRUM REVOLUTION; OPTIMAL FORAGING THEORY; CULTURAL-EVOLUTION; NICHE CONSTRUCTION; HUNTER-GATHERERS; FOOD-PRODUCTION; PLANT DOMESTICATION; NORTH-AMERICA; LOWER YANGTZE; DIET BREADTH AB The introduction of new analytic methods and expansion of research into previously untapped regions have greatly increased the scale and resolution of data relevant to the origins of agriculture (OA). As a result, the recognition of varied historical pathways to agriculture and the continuum of management strategies have complicated the search for general explanations for the transition to food production. In this environment, higher-level theoretical frameworks are sometimes rejected on the grounds that they force conclusions that are incompatible with real-world variability. Some of those who take this position argue instead that OA should be explained in terms of local and historically contingent factors. This retreat from theory in favor of particularism is based on the faulty beliefs that complex phenomena such as agricultural origins demand equally complex explanations and that explanation is possible in the absence of theoretically based assumptions. The same scholars who are suspicious of generalization are reluctant to embrace evolutionary approaches to human behavior on the grounds that they are ahistorical, overly simplistic, and dismissive of agency and intent. We argue that these criticisms are misplaced and explain why a coherent theory of human behavior that acknowledges its evolutionary history is essential to advancing understanding of OA. Continued progress depends on the integration of human behavior and culture into the emerging synthesis of evolutionary developmental biology that informs contemporary research into plant and animal domestication. C1 [Gremillion, Kristen J.] Ohio State Univ, Dept Anthropol, Columbus, OH 43210 USA. [Barton, Loukas] Univ Pittsburgh, Dept Anthropol, Pittsburgh, PA 15260 USA. [Piperno, Dolores R.] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. [Piperno, Dolores R.] Smithsonian Trop Res Inst, Panama City, Panama. RP Gremillion, KJ (reprint author), Ohio State Univ, Dept Anthropol, Columbus, OH 43210 USA. EM gremillion.1@osu.edu NR 114 TC 29 Z9 29 U1 2 U2 50 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 29 PY 2014 VL 111 IS 17 BP 6171 EP 6177 DI 10.1073/pnas.1308938110 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AG1TL UT WOS:000335199000031 PM 24753601 ER PT J AU Chan, CK Lin, GD Yelin, SF Lukin, MD AF Chan, Ching-Kit Lin, Guin-Dar Yelin, Susanne F. Lukin, Mikhail D. TI Quantum interference between independent reservoirs in open quantum systems SO PHYSICAL REVIEW A LA English DT Article ID DECOHERENCE AB When a quantum system interacts with multiple reservoirs, the environmental effects are usually treated in an additive manner. We show that this assumption breaks down for non-Markovian environments that have finite memory times. Specifically, we demonstrate that quantum interferences between independent environments can qualitatively modify the dynamics of the physical system. We illustrate this effect with a two-level system coupled to two structured photonic reservoirs, discuss its origin using a nonequilibrium diagrammatic technique, and show an example when the application of this interference can result in an improved dark state preparation in a Lambda system. C1 [Chan, Ching-Kit; Lin, Guin-Dar; Yelin, Susanne F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Chan, Ching-Kit; Lin, Guin-Dar; Yelin, Susanne F.; Lukin, Mikhail D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Lin, Guin-Dar] Natl Taiwan Univ, Dept Phys, Taipei 10617, Taiwan. [Yelin, Susanne F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. RP Chan, CK (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. OI LIN, GUIN-DAR/0000-0002-2243-9490 FU NSF; CUA; ITAMP; AFOSR; MURI; Croucher Foundation FX We thank Tony Lee and Shenshen Wang for very helpful discussions. This work is supported by NSF, CUA, ITAMP, AFOSR, and MURI. C.K.C. is supported by the Croucher Foundation. NR 47 TC 9 Z9 9 U1 4 U2 18 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD APR 25 PY 2014 VL 89 IS 4 AR 042117 DI 10.1103/PhysRevA.89.042117 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AH0CT UT WOS:000335787400001 ER PT J AU Karadjian, G Martinsen, E Duval, L Chavatte, JM Landau, I AF Karadjian, Gregory Martinsen, Ellen Duval, Linda Chavatte, Jean-Marc Landau, Irene TI Haemoproteus ilanpapernai n. sp (Apicomplexa, Haemoproteidae) in Strix seloputo from Singapore: morphological description and reassignment of molecular data SO PARASITE LA English DT Article DE Haemoproteus ilanpapernai n. sp.; Strix seloputo; Singapore; cyt b; co1 ID PARASITES; IDENTIFICATION AB Haemoproteus ilanpapernai Karadjian and Landau n. sp. from the Spotted Wood Owl, Strix seloputo, in Singapore is described from material from Ilan Paperna's collection of slides. The species was previously identified as Haemoproteus syrnii (Mayer, 1910). However, comparisons between the material from Strix seloputo and our own material from Strix aluco, the type host of H. syrnii, revealed morphological and molecular differences. H. ilanpapernai n. sp. differs morphologically from H. syrnii by the much smaller size of the gametocytes, the different position of the mature gametocytes in the erythrocyte (apical, subapical, or lateral in H. ilanpapernai vs. always lateral in H. syrnii), the effect on the erythrocyte nucleus (frequently tilted in H. ilanpapernai but not displaced laterally vs. straight and displaced laterally in H. syrnii) and characters of the pigment (aggregated in the gametocytes of H. ilanpapernai vs. dispersed in H. syrnii). A molecular analysis showed that the two species differ by 2.9% at the cyt b and 3.1% at the COI genes. C1 [Karadjian, Gregory; Duval, Linda; Landau, Irene] CNRS, MCAM MNHN, UMR 7245, F-75231 Paris 05, France. [Martinsen, Ellen] Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. [Chavatte, Jean-Marc] Malaria Reference Ctr, Natl Publ Hlth Lab, Minist Hlth, Singapore 169612, Singapore. RP Landau, I (reprint author), CNRS, MCAM MNHN, UMR 7245, 61 Rue Buffon,CP 52, F-75231 Paris 05, France. EM landau@mnhn.fr OI Chavatte, Jean-Marc/0000-0002-0003-541X FU Labex BCDiv (Biological and Cultural Diversities), Museum National d'Histoire Naturelle, Paris FX The slides from Ilan Paperna's collection were deposited in the collections of The Museum National d'Histoire Naturelle de Paris, through the courtesy of Prof. Jaap van Rijn, Director of the Department of Animal Sciences, The Robert H. Smith Faculty of Agriculture, Food and Environment, Rehovot, Israel. LD was supported by a postdoctoral fellowship from the Labex BCDiv (Biological and Cultural Diversities), Museum National d'Histoire Naturelle, Paris. NR 13 TC 0 Z9 0 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1252-607X EI 1776-1042 J9 PARASITE JI Parasite PD APR 24 PY 2014 VL 21 AR 17 DI 10.1051/parasite/2014018 PG 5 WC Parasitology SC Parasitology GA AG5HB UT WOS:000335449000001 PM 24759652 ER PT J AU Lahrz, M Lemeshko, M Sengstock, K Becker, C Mathey, L AF Lahrz, M. Lemeshko, M. Sengstock, K. Becker, C. Mathey, L. TI Detecting quadrupole interactions in ultracold Fermi gases SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATION; MANY-BODY PHYSICS; OPTICAL LATTICES; MOLECULES; ATOMS; TRANSITION AB We propose to detect quadrupole interactions of neutral ultracold atoms via their induced mean-field shift. We consider a Mott insulator state of spin-polarized atoms in a two-dimensional optical square lattice. The quadrupole moments of the atoms are aligned by an external magnetic field. As the alignment angle is varied, the mean-field shift shows a characteristic angular dependence, which constitutes the defining signature of the quadrupole interaction. For the P-3(2) states of Yb and Sr atoms, we find a frequency shift of the order of tens of Hertz, which can be realistically detected in experiment with current technology. We compare our results to the mean-field shift of a spin-polarized quasi-two-dimensional Fermi gas in continuum. C1 [Lahrz, M.; Sengstock, K.; Becker, C.; Mathey, L.] Univ Hamburg, Zentrum Opt Quantentechnol, D-22761 Hamburg, Germany. [Lahrz, M.; Sengstock, K.; Becker, C.; Mathey, L.] Univ Hamburg, Inst Laserphys, D-22761 Hamburg, Germany. [Lemeshko, M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Lemeshko, M.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Sengstock, K.; Becker, C.; Mathey, L.] Hamburg Ctr Ultrafast Imaging, D-22761 Hamburg, Germany. RP Lahrz, M (reprint author), Univ Hamburg, Zentrum Opt Quantentechnol, D-22761 Hamburg, Germany. RI Mathey, Ludwig/A-9644-2009; Becker, Christoph/E-5304-2017 FU Deutsche Forschungsgemeinschaft through the SFB 925; Hamburg Centre for Ultrafast Imaging; Landesexzellenzinitiative Hamburg; Joachim Herz Stiftung FX We gratefully acknowledge discussions with Florian Schreck, Yoshiro Takahashi, Wen-Min Huang, Eite Tiesinga, and Alexander Pikovski. We acknowledge support from the Deutsche Forschungsgemeinschaft through the SFB 925 and the Hamburg Centre for Ultrafast Imaging, and from the Landesexzellenzinitiative Hamburg, which is supported by the Joachim Herz Stiftung. NR 38 TC 7 Z9 7 U1 2 U2 11 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD APR 23 PY 2014 VL 89 IS 4 AR 043616 DI 10.1103/PhysRevA.89.043616 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AG3LM UT WOS:000335319300008 ER PT J AU Jacobs, B Johnson, NL Wahl, D Schall, M Maseko, BC Lewandowski, A Raghanti, MA Wicinski, B Butti, C Hopkins, WD Bertelsen, MF Walsh, T Roberts, JR Reep, RL Hof, PR Sherwood, CC Manger, PR AF Jacobs, Bob Johnson, Nicholas L. Wahl, Devin Schall, Matthew Maseko, Busisiwe C. Lewandowski, Albert Raghanti, Mary A. Wicinski, Bridget Butti, Camilla Hopkins, William D. Bertelsen, Mads F. Walsh, Timothy Roberts, John R. Reep, Roger L. Hof, Patrick R. Sherwood, Chet C. Manger, Paul R. TI Comparative neuronal morphology of the cerebellar cortex in afrotherians, carnivores, cetartiodactyls, and primates SO FRONTIERS IN NEUROANATOMY LA English DT Article DE dendrite; morphometry; Golgi method; brain evolution; cerebellum ID QUANTITATIVE DENDRITIC ANALYSIS; ELEPHANT ELEPHAS-MAXIMUS; HUMPBACK WHALE SONG; GRANULAR LAYER; PURKINJE-CELLS; ASIAN ELEPHANT; MOTOR CONTROL; LUGARO CELL; HUMAN-BRAIN; FUNCTIONAL IMPLICATIONS AB Although the basic morphological characteristics of neurons in the cerebellar cortex have been documented in several species, virtually nothing is known about the quantitative morphological characteristics of these neurons across different taxa. To that end, the present study investigated cerebellar neuronal morphology among eight different, large-brained mammalian species comprising a broad phylogenetic range: afrotherians (African elephant, Florida manatee), carnivores (Siberian tiger, clouded leopard), cetartiodactyls (humpback whale, giraffe) and primates (human, common chimpanzee). Specifically, several neuron types (e.g., stellate, basket, Lugaro, Golgi, and granule neurons; N = 317) of the cerebellar cortex were stained with a modified rapid Golgi technique and quantified on a computer-assisted microscopy system. There was a 64-fold variation in brain mass across species in our sample (from clouded leopard to the elephant) and a 103-fold variation in cerebellar volume. Most dendritic measures tended to increase with cerebellar volume. The cerebellar cortex in these species exhibited the trilaminate pattern common to all mammals. Morphologically, neuron types in the cerebellar cortex were generally consistent with those described in primates (Fox et al., 1967) and rodents (Palay and Chan-Palay 1974), although there was substantial quantitative variation across species. In particular, Lugaro neurons in the elephant appeared to be disproportionately larger than those in other species. To explore potential quantitative differences in dendritic measures across species, MARSplines analyses were used to evaluate whether species could be differentiated from each other based on dendritic characteristics alone. Results of these analyses indicated that there were significant differences among all species in dendritic measures. C1 [Jacobs, Bob; Johnson, Nicholas L.; Wahl, Devin; Schall, Matthew] Colorado Coll, Lab Quantitat Neuromorphol, Colorado Springs, CO 80903 USA. [Maseko, Busisiwe C.; Manger, Paul R.] Univ Witwatersrand, Sch Anat Sci, Fac Hlth Sci, Johannesburg, South Africa. [Lewandowski, Albert] Cleveland Metropk Zoo, Cleveland, OH USA. [Raghanti, Mary A.] Kent State Univ, Dept Anthropol, Kent, OH 44242 USA. [Wicinski, Bridget; Butti, Camilla; Hof, Patrick R.] Icahn Sch Med Mt Sinai, Fishberg Dept Neurosci, New York, NY USA. [Wicinski, Bridget; Butti, Camilla; Hof, Patrick R.] Icahn Sch Med Mt Sinai, Friedman Brain Inst, New York, NY USA. [Hopkins, William D.] Yerkes Natl Primate Res Ctr, Div Dev & Cognit Neurosci, Atlanta, GA USA. [Bertelsen, Mads F.] Copenhagen Zoo, Ctr Zoo & Wild Anim Hlth, Frederiksberg, Denmark. [Walsh, Timothy; Roberts, John R.] Smithsonian Natl Zool Pk, Washington, DC USA. [Reep, Roger L.] Univ Florida, Dept Physiol Sci, Gainesville, FL 32610 USA. [Sherwood, Chet C.] George Washington Univ, Dept Anthropol, Washington, DC USA. RP Jacobs, B (reprint author), Colorado Coll, Lab Quantitat Neuromorphol, 14 E Cache La Poudre, Colorado Springs, CO 80903 USA. EM bjacobs@coloradocollege.edu OI Wahl, Devin/0000-0003-2794-0185; Bertelsen, Mads/0000-0001-9201-7499 FU Colorado College's divisional research funds; James S. McDonnell Foundation [22002078, 220020293]; National Science Foundation [BCS-0827531]; South African National Research Foundation [FA2005033100004] FX Partial support for this work was provided by Colorado College's divisional research funds (Bob Jacobs), the James S. McDonnell Foundation (grant 22002078, to Chet C. Sherwood, Patrick R. Hof; grant 220020293 to Chet C. Sherwood), National Science Foundation (BCS-0827531 to Chet C. Sherwood), and the South African National Research Foundation (Paul R. Manger; FA2005033100004). We would also like to thank the Danish Cardiovascular Research Program, especially Emil Toft-Brondum, for allowing us to obtain the specimens of giraffe brains. NR 134 TC 13 Z9 13 U1 2 U2 29 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1662-5129 J9 FRONT NEUROANAT JI Front. Neuroanat. PD APR 23 PY 2014 VL 8 AR 24 DI 10.3389/fnana.2014.00024 PG 27 WC Anatomy & Morphology; Neurosciences SC Anatomy & Morphology; Neurosciences & Neurology GA AF8VR UT WOS:000334994200001 PM 24795574 ER PT J AU Roberts, P Delson, E Miracle, P Ditchfield, P Roberts, RG Jacobs, Z Blinkhorn, J Ciochon, RL Fleagle, JG Frost, SR Gilbert, CC Gunnell, GF Harrison, T Korisettar, R Petraglia, MD AF Roberts, Patrick Delson, Eric Miracle, Preston Ditchfield, Peter Roberts, Richard G. Jacobs, Zenobia Blinkhorn, James Ciochon, Russell L. Fleagle, John G. Frost, Stephen R. Gilbert, Christopher C. Gunnell, Gregg F. Harrison, Terry Korisettar, Ravi Petraglia, Michael D. TI Continuity of mammalian fauna over the last 200,000 y in the Indian subcontinent SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Kurnool; fossil mammals; OSL dating; Theropithecus ID LATE PLEISTOCENE; SUPER-ERUPTION; ARABIAN PENINSULA; SOUTHERN-INDIA; SAUDI-ARABIA; NAFUD DESERT; EXTINCTIONS; DISPERSAL; AFRICA; TOBA AB Mammalian extinction worldwide during the Late Pleistocene has been a major focus for Quaternary biochronology and paleoecology. These extinctions have been variably attributed to the impacts of climate change and human interference. However, until relatively recently, research has been largely restricted to the Americas, Europe, and Australasia. We present the oldest Middle-Late Pleistocene stratified and numerically dated faunal succession for the Indian subcontinent from the Billasurgam cave complex. Our data demonstrate continuity of 20 of 21 identified mammalian taxa from at least 100,000 y ago to the present, and in some cases up to 200,000 y ago. Comparison of this fossil record to contemporary faunal ranges indicates some geographical redistribution of mammalian taxa within India. We suggest that, although local extirpations occurred, the majority of taxa survived or adapted to substantial ecological pressures in fragmented habitats. Comparison of the Indian record with faunal records from Southeast and Southwest Asia demonstrates the importance of interconnected mosaic habitats to long-term faunal persistence across the Asian tropics. The data presented here have implications for mammalian conservation in India today, where increasing ecological circumscription may leave certain taxa increasingly endangered in the most densely populated region of the world. C1 [Roberts, Patrick; Ditchfield, Peter; Petraglia, Michael D.] Univ Oxford, Sch Archaeol, Res Lab Archaeol & Hist Art, Oxford OX1 3QY, England. [Delson, Eric] Amer Museum Nat Hist, Dept Vertebrate Paleontol, New York, NY 10024 USA. [Delson, Eric] CUNY Herbert H Lehman Coll, Dept Anthropol, Bronx, NY 10468 USA. [Delson, Eric; Gilbert, Christopher C.; Gunnell, Gregg F.] CUNY, Grad Ctr, PhD Program Anthropol, New York, NY 10016 USA. [Delson, Eric; Gilbert, Christopher C.; Gunnell, Gregg F.; Harrison, Terry] New York Consortium Evolutionary Primatol, New York, NY 10024 USA. [Miracle, Preston] Univ Cambridge, Dept Archaeol, Cambridge CB2 3DZ, England. [Roberts, Richard G.; Jacobs, Zenobia] Univ Wollongong, Sch Earth & Environm Sci, Ctr Archaeol Sci, Wollongong, NSW 2522, Australia. [Blinkhorn, James] Univ Bordeaux 1, Lab Prehist Actuel Culture Environm & Anthropol, F-33405 Talence, France. [Ciochon, Russell L.] Univ Iowa, Dept Anthropol, Iowa City, IA 52242 USA. [Ciochon, Russell L.] Univ Iowa, Museum Nat Hist, Iowa City, IA 52242 USA. [Fleagle, John G.] SUNY Stony Brook, Sch Med, Stony Brook, NY USA. [Frost, Stephen R.] Univ Oregon, Dept Anthropol, Eugene, OR 97132 USA. [Gilbert, Christopher C.] CUNY Hunter Coll, Dept Anthropol, New York, NY 10065 USA. [Gunnell, Gregg F.] Duke Lemur Ctr, Div Fossil Primates, Durham, NC 27705 USA. [Harrison, Terry] NYU, Dept Anthropol, Ctr Study Human Origins, New York, NY 10003 USA. [Korisettar, Ravi] Karnatak Univ, Dr DC Pavate Chair Art & Archaeol, Dharwad 580003, Karnataka, India. [Petraglia, Michael D.] Smithsonian Inst, Human Origins Program, Washington, DC 20560 USA. RP Petraglia, MD (reprint author), Univ Oxford, Sch Archaeol, Res Lab Archaeol & Hist Art, S Parks Rd, Oxford OX1 3QY, England. EM michael.petraglia@rlaha.ox.ac.uk OI Gilbert, Christopher/0000-0001-8768-3171 FU British Academy; Leverhulme Trust; European Research Council [295719]; Australian Research Council FX We thank Miriam Belmaker, John de Vos, and Chris Stimpson for suggestions regarding faunal continuity in the Levant, Southeast Asia, and the Arabian Peninsula, respectively. We thank the Archaeological Survey of India for permission to conduct the fieldwork and the international team for their contributions to the excavations. This work was supported by grants from the British Academy, the Leverhulme Trust, and European Research Council Grant 295719 (to M. D. P.), and the Australian Research Council (to R.G.R.). NR 45 TC 12 Z9 12 U1 4 U2 14 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 22 PY 2014 VL 111 IS 16 BP 5848 EP 5853 DI 10.1073/pnas.1323465111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AF4OV UT WOS:000334694000038 PM 24711426 ER PT J AU Pyenson, ND Gutstein, CS Parham, JF Le Roux, JP Chavarria, CC Little, H Metallo, A Rossi, V Valenzuela-Toro, AM Velez-Juarbe, J Santelli, CM Rogers, DR Cozzuol, MA Suarez, ME AF Pyenson, Nicholas D. Gutstein, Carolina S. Parham, James F. Le Roux, Jacobus P. Chavarria, Catalina Carreno Little, Holly Metallo, Adam Rossi, Vincent Valenzuela-Toro, Ana M. Velez-Juarbe, Jorge Santelli, Cara M. Rogers, David Rubilar Cozzuol, Mario A. Suarez, Mario E. TI Repeated mass strandings of Miocene marine mammals from Atacama Region of Chile point to sudden death at sea SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE taphonomy; strandings; fossil record; harmful algal blooms ID CETACEANS CENOZOIC DRIVERS; NORTH PACIFIC-OCEAN; SOUTHERN CALIFORNIA; PISCO FORMATION; MODERN WHALES; MORTALITY; NEOGENE; COASTAL; RECORD; PRESERVATION AB Marine mammal mass strandings have occurred for millions of years, but their origins defy singular explanations. Beyond human causes, mass strandings have been attributed to herding behaviour, large-scale oceanographic fronts and harmful algal blooms (HABs). Because algal toxins cause organ failure in marine mammals, HABs are the most common mass stranding agent with broad geographical and widespread taxonomic impact. Toxin-mediated mortalities in marine food webs have the potential to occur over geological timescales, but direct evidence for their antiquity has been lacking. Here, we describe an unusually dense accumulation of fossil marine vertebrates from Cerro Ballena, a Late Miocene locality in Atacama Region of Chile, preserving over 40 skeletons of rorqual whales, sperm whales, seals, aquatic sloths, walrus-whales and predatory bony fish. Marine mammal skeletons are distributed in four discrete horizons at the site, representing a recurring accumulation mechanism. Taphonomic analysis points to strong spatial focusing with a rapid death mechanism at sea, before being buried on a barrier-protected supratidal flat. In modern settings, HABs are the only known natural cause for such repeated, multispecies accumulations. This proposed agent suggests that upwelling zones elsewhere in the world should preserve fossil marine vertebrate accumulations in similar modes and densities. C1 [Pyenson, Nicholas D.; Gutstein, Carolina S.; Little, Holly; Velez-Juarbe, Jorge] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Pyenson, Nicholas D.] Burke Museum Nat Hist & Culture, Dept Mammal, Seattle, WA 98195 USA. [Pyenson, Nicholas D.] Burke Museum Nat Hist & Culture, Dept Paleontol, Seattle, WA 98195 USA. [Gutstein, Carolina S.; Valenzuela-Toro, Ana M.; Rogers, David Rubilar; Suarez, Mario E.] Univ Chile, Fac Ciencias, Dept Biol, Lab Ontogenia & Filogenia, Santiago 3425, Chile. [Parham, James F.] Calif State Univ Fullerton, Dept Geol Sci, John D Cooper Archaeol & Paleontol Ctr, Fullerton, CA 92834 USA. [Chavarria, Catalina Carreno] Univ Chile, Fac Ciencias Fis, Dept Geol, Santiago, Chile. [Chavarria, Catalina Carreno] Univ Chile, Matemat & Andean Geothermal Ctr, Santiago, Chile. [Metallo, Adam; Rossi, Vincent] Smithsonian Inst, Digitizat Program Off 3D Lab, Landover, MD 20785 USA. [Valenzuela-Toro, Ana M.; Suarez, Mario E.] Univ Chile, Fac Ciencias, Dept Ecol, Lab Ecofisiol, Santiago 3425, Chile. [Velez-Juarbe, Jorge] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Rogers, David Rubilar] Museo Nacl Hist Nat, Area Paleontol, Santiago, Chile. [Cozzuol, Mario A.] Univ Fed Minas Gerais, Inst Ciencias Biol, Dept Zool, Belo Horizonte, MG, Brazil. RP Pyenson, ND (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA. EM pyensonn@si.edu RI Le Roux, Jacobus/A-9765-2008; Cozzuol, Mario/H-8302-2012; OI Le Roux, Jacobus/0000-0003-0173-4471; Cozzuol, Mario/0000-0003-3645-0401; Gutstein, Carolina/0000-0002-0823-2434; Santelli, Cara/0000-0001-8617-0008 FU Sacyr Chile S.A.; CONICYT; Becas Chile; Departamento de Postgrado y Postitulo of the Vicerrectoria de Asuntos Academicos of Universidad de Chile; National Museum of Natural History (NMNH); NMNH Office of the Director; Smithsonian Institution's Remington Kellogg Fund; National Geographic Society Committee [8903-11, 9019-11]; U-REDES (Universidad de Chile) [Domeyko II UR-C12/1] FX Excavation work was conducted under CMN permit no. 5979 to M. E. S. and was financed by Sacyr Chile S.A. Funding from CONICYT, Becas Chile, Departamento de Postgrado y Postitulo of the Vicerrectoria de Asuntos Academicos of Universidad de Chile supported C. S. G. This work was also funded by a National Museum of Natural History (NMNH) Small Grant Award, discretionary funding from NMNH Office of the Director, the Smithsonian Institution's Remington Kellogg Fund, two National Geographic Society Committee on Research Exploration grants (8903-11, 9019-11) to N.D.P. and by U-REDES (Domeyko II UR-C12/1, Universidad de Chile) to A. O. Vargas. NR 56 TC 20 Z9 20 U1 8 U2 70 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 22 PY 2014 VL 281 IS 1781 AR 20133316 DI 10.1098/rspb.2013.3316 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AC6NL UT WOS:000332640400024 PM 24573855 ER PT J AU Tsangaras, K Siracusa, MC Nikolaidis, N Ishida, Y Cui, P Vielgrader, H Helgen, KM Roca, AL Greenwood, AD AF Tsangaras, Kyriakos Siracusa, Matthew C. Nikolaidis, Nikolas Ishida, Yasuko Cui, Pin Vielgrader, Hanna Helgen, Kristofer M. Roca, Alfred L. Greenwood, Alex D. TI Hybridization Capture Reveals Evolution and Conservation across the Entire Koala Retrovirus Genome SO PLOS ONE LA English DT Article ID ANCIENT DNA; PHASCOLARCTOS-CINEREUS; MITOCHONDRIAL-DNA; LEUKEMIA-VIRUS; REAL-TIME; PROTEIN; ESCAPE; SELECTION; PRESSURE; GENETICS AB The koala retrovirus (KoRV) is the only retrovirus known to be in the midst of invading the germ line of its host species. Hybridization capture and next generation sequencing were used on modern and museum DNA samples of koala (Phascolarctos cinereus) to examine ca. 130 years of evolution across the full KoRV genome. Overall, the entire proviral genome appeared to be conserved across time in sequence, protein structure and transcriptional binding sites. A total of 138 polymorphisms were detected, of which 72 were found in more than one individual. At every polymorphic site in the museum koalas, one of the character states matched that of modern KoRV. Among non-synonymous polymorphisms, radical substitutions involving large physiochemical differences between amino acids were elevated in env, potentially reflecting anti-viral immune pressure or avoidance of receptor interference. Polymorphisms were not detected within two functional regions believed to affect infectivity. Host sequences flanking proviral integration sites were also captured; with few proviral loci shared among koalas. Recently described variants of KoRV, designated KoRV-B and KoRV-J, were not detected in museum samples, suggesting that these variants may be of recent origin. C1 [Tsangaras, Kyriakos] Leibniz Inst Zoo & Wildlife Res, Dept Wildlife Dis, Berlin, Germany. [Siracusa, Matthew C.; Nikolaidis, Nikolas; Cui, Pin; Greenwood, Alex D.] Calif State Univ Fullerton, Dept Biol Sci, Fullerton, CA 92634 USA. [Siracusa, Matthew C.; Nikolaidis, Nikolas; Cui, Pin; Greenwood, Alex D.] Calif State Univ Fullerton, Ctr Appl Biotechnol Studies, Fullerton, CA 92634 USA. [Ishida, Yasuko; Roca, Alfred L.] Univ Illinois, Dept Anim Sci, Urbana, IL USA. [Vielgrader, Hanna] Zoo Vienna, Vienna, Austria. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Greenwood, AD (reprint author), Calif State Univ Fullerton, Dept Biol Sci, Fullerton, CA 92634 USA. EM greenwood@izw-berlin.de FU California State University, Fullerton; HHMI; Smithsonian Institution; National Institute of General Medical Sciences (NIGMS) [R01GM092706] FX NN was supported by start-up funds and a state-mini grant from California State University, Fullerton and a Faculty-Student research Grant from California State University, Fullerton. MS was supported by an HHMI scholarship. KH was supported by the Smithsonian Institution. The project described was supported by Grant Number R01GM092706 from the National Institute of General Medical Sciences (NIGMS). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. The Vienna Zoo is a public entity, e.g. a state funded zoo. NR 51 TC 19 Z9 19 U1 0 U2 28 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 21 PY 2014 VL 9 IS 4 AR e95633 DI 10.1371/journal.pone.0095633 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AG2DX UT WOS:000335227400094 PM 24752422 ER PT J AU Dikow, T Grimaldi, DA AF Dikow, Torsten Grimaldi, David A. TI Robber flies in Cretaceous ambers (Insecta: Diptera: Asilidae) SO AMERICAN MUSEUM NOVITATES LA English DT Article AB Cretaceous fossils of Asilidae are reviewed, and two new taxa from Burmese and Raritan (New Jersey) ambers are described. The first robber fly from Burmese amber, Burmapogon bruckschi, new genus and species, is described based on specimens of both sexes. A scientific name is provided for the previously described but unnamed fossil assassin fly from Raritan amber, Cretagaster raritanensis, new genus and species, preserved as a fragmentary specimen. The amber fossils are placed phylogenetically within Asilidae. Specifically, Burmapogon is postulated to be a representative of the clade comprised of (Brachyrhopalinae + Stichopogoninae), while Cretagaster is a member of the Leptogastrinae and postulated to be an extinct sister group to (Acronychini + Leptogastrini). C1 [Dikow, Torsten] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Grimaldi, David A.] Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA. RP Dikow, T (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, 10th St & Constitut Ave NW, Washington, DC 20560 USA. FU U.S. National Science Foundation REVSYS Grant [DEB 0919333]; John D. and Catherine T. MacArthur Foundation of the Biodiversity Synthesis Group of the Encyclopedia of Life FX We thank Dan Bickel (Australian Museum, Sydney) for making us aware of the male Burmese amber specimen, and Klaus-Peter Brucksch for making it available to our study through purchase by the AMNH. James Zigras kindly loaned the sole asilid in his extensive Burmese amber collection for study. We thank the two anynonymous reviewers and the editor for their suggestions that improved the manuscript. The Burmese amber specimens were purchased by the AMNH with generous funds provided by Robert Goelet, Chairman Emeritus of the AMNH. This project is funded by a U.S. National Science Foundation REVSYS Grant (DEB 0919333; PI Torsten Dikow, Co-PI David Yeates). Any opinions, findings, and conclusions or recommendations expressed in this manuscript are those of the authors and do not necessarily reflect the views of the National Science Foundation. Partial funding is also provided by the John D. and Catherine T. MacArthur Foundation funding of the Biodiversity Synthesis Group of the Encyclopedia of Life. NR 23 TC 5 Z9 5 U1 1 U2 4 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0082 EI 1937-352X J9 AM MUS NOVIT JI Am. Mus. Novit. PD APR 21 PY 2014 IS 3799 BP 1 EP 19 PG 19 WC Biodiversity Conservation; Zoology SC Biodiversity & Conservation; Zoology GA AF8NW UT WOS:000334973900001 ER PT J AU Albrecht, S Winn, JN Torres, G Fabrycky, DC Setiawan, J Gillon, M Jehin, E Triaud, A Queloz, D Snellen, I Eggleton, P AF Albrecht, Simon Winn, Joshua N. Torres, Guillermo Fabrycky, Daniel C. Setiawan, Johny Gillon, Michael Jehin, Emmanuel Triaud, Amaury Queloz, Didier Snellen, Ignas Eggleton, Peter TI THE BANANA PROJECT. V. MISALIGNED AND PRECESSING STELLAR ROTATION AXES IN CV VELORUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; stars: early-type; stars: formation; stars: individual (CV Velorum, DI Herculis, EP Crucis); stars: kinematics and dynamics; stars: rotation; techniques: spectroscopic ID SPIN-ORBIT MISALIGNMENT; INTERNAL GRAVITY-WAVES; PULSATING B-STARS; DI HERCULIS; ECLIPSING BINARY; APSIDAL MOTION; GENERAL-RELATIVITY; TIDAL-EVOLUTION; DWARF COMPANION; HOT JUPITERS AB As part of the Binaries Are Not Always Neatly Aligned project (BANANA), we have found that the eclipsing binary CV Velorum has misaligned rotation axes. Based on our analysis of the Rossiter-McLaughlin effect, we find sky-projected spin-orbit angles of beta(p) = -52 degrees +/- 6 degrees and beta(s) = 3 degrees +/- 7 degrees for the primary and secondary stars (B2.5V + B2.5V, P = 6.9 days). We combine this information with several measurements of changing projected stellar rotation speeds (v sin i(star)) over the last 30 yr, leading to a model in which the primary star's obliquity is approximate to 65 degrees, and its spin axis precesses around the total angular momentum vector with a period of about 140 yr. The geometry of the secondary star is less clear, although a significant obliquity is also implicated by the observed time variations in the v sin i(star). By integrating the secular tidal evolution equations backward in time, we find that the system could have evolved from a state of even stronger misalignment similar to DI Herculis, a younger but otherwise comparable binary. C1 [Albrecht, Simon; Winn, Joshua N.; Triaud, Amaury] MIT, Dept Phys, Cambridge, MA 02139 USA. [Albrecht, Simon; Winn, Joshua N.; Triaud, Amaury] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Setiawan, Johny] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Setiawan, Johny] Embassy Republ Indonesia, D-10557 Berlin, Germany. [Gillon, Michael; Jehin, Emmanuel] Univ Liege, Inst Astrophys & Geophys, Liege, Belgium. [Triaud, Amaury; Queloz, Didier] Univ Geneva, Astron Observ, CH-1290 Sauverny, Switzerland. [Queloz, Didier] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Snellen, Ignas] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [Eggleton, Peter] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. RP Albrecht, S (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. OI Triaud, Amaury/0000-0002-5510-8751; Fabrycky, Daniel/0000-0003-3750-0183 FU Rubicon fellowship from the Netherlands Organisation for Scientific Research (NWO); NASA Origins award [NNX09AB33G]; NSF [1108595]; Belgian Fund for Scientific Research (FNRS); Swiss National Science Fundation (SNF); Swiss National Science Foundation [PBGEP2-14559] FX We thank the anonymous referee for timely suggestions, which improved the manuscript. We thank Kadri Yakut and Conny Aerts for providing us with a digital version of the Clausen & Gronbech (1977) photometry, as well as their own CORALIE spectra and comments on the manuscript. S. A. acknowledges support during part of this project by a Rubicon fellowship from the Netherlands Organisation for Scientific Research (NWO). Work by S. A. and J.N.W. was supported by NASA Origins award NNX09AB33G and NSF grant no. 1108595. TRAPPIST is a project funded by the Belgian Fund for Scientific Research (FNRS) with the participation of the Swiss National Science Fundation (SNF). M. G. and E.J. are FNRS Research Associates. A. H.M.J. Triaud received funding from of a fellowship provided by the Swiss National Science Foundation under grant number PBGEP2-14559. This research has made use of the following web resources: simbad.u-strasbg.fr, adswww.harvard.edu, http://arxiv.org NR 45 TC 17 Z9 17 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 20 PY 2014 VL 785 IS 2 AR 83 DI 10.1088/0004-637X/785/2/83 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800002 ER PT J AU Bennett, DP Batista, V Bond, IA Bennett, CS Suzuki, D Beaulieu, JP Udalski, A Donatowicz, J Bozza, V Abe, F Botzler, CS Freeman, M Fukunaga, D Fukui, A Itow, Y Koshimoto, N Ling, CH Masuda, K Matsubara, Y Muraki, Y Namba, S Ohnishi, K Rattenbury, NJ Saito, T Sullivan, DJ Sumi, T Sweatman, WL Tristram, PJ Tsurumi, N Wada, K Yock, PCM Albrow, MD Bachelet, E Brillant, S Caldwell, JAR Cassan, A Cole, AA Corrales, E Coutures, C Dieters, S Prester, DD Fouque, P Greenhill, J Horne, K Koo, JR Kubas, D Marquette, JB Martin, R Menzies, JW Sahu, KC Wambsganss, J Williams, A Zub, M Choi, JY DePoy, DL Dong, SB Gaudi, BS Gould, A Han, C Henderson, CB McGregor, D Lee, CU Pogge, RW Shin, IG Yee, JC Szymanski, MK Skowron, J Poleski, R Kozllowski, S Wyrzykowski, L Kubiak, M Pietrukowicz, P Pietrzynski, G Soszynski, I Ulaczyk, K Tsapras, Y Street, RA Dominik, M Bramich, DM Browne, P Hundertmark, M Kains, N Snodgrass, C Steele, IA Dekany, I Gonzalez, OA Heyrovsky, D Kandori, R Kerins, E Lucas, PW Minniti, D Nagayama, T Rejkuba, M Robin, AC Saito, R AF Bennett, D. P. Batista, V. Bond, I. A. Bennett, C. S. Suzuki, D. Beaulieu, J. -P. Udalski, A. Donatowicz, J. Bozza, V. Abe, F. Botzler, C. S. Freeman, M. Fukunaga, D. Fukui, A. Itow, Y. Koshimoto, N. Ling, C. H. Masuda, K. Matsubara, Y. Muraki, Y. Namba, S. Ohnishi, K. Rattenbury, N. J. Saito, To. Sullivan, D. J. Sumi, T. Sweatman, W. L. Tristram, P. J. Tsurumi, N. Wada, K. Yock, P. C. M. Albrow, M. D. Bachelet, E. Brillant, S. Caldwell, J. A. R. Cassan, A. Cole, A. A. Corrales, E. Coutures, C. Dieters, S. Prester, D. Dominis Fouque, P. Greenhill, J. Horne, K. Koo, J. -R. Kubas, D. Marquette, J. -B. Martin, R. Menzies, J. W. Sahu, K. C. Wambsganss, J. Williams, A. Zub, M. Choi, J. Y. DePoy, D. L. Dong, Subo Gaudi, B. S. Gould, A. Han, C. Henderson, C. B. McGregor, D. Lee, C. -U. Pogge, R. W. Shin, I. -G. Yee, J. C. Szymanski, M. K. Skowron, J. Poleski, R. Kozllowski, S. Wyrzykowski, L. Kubiak, M. Pietrukowicz, P. Pietrzynski, G. Soszynski, I. Ulaczyk, K. Tsapras, Y. Street, R. A. Dominik, M. Bramich, D. M. Browne, P. Hundertmark, M. Kains, N. Snodgrass, C. Steele, I. A. Dekany, I. Gonzalez, O. A. Heyrovsky, D. Kandori, R. Kerins, E. Lucas, P. W. Minniti, D. Nagayama, T. Rejkuba, M. Robin, A. C. Saito, R. CA MOA Collaboration PLANET Collaboration FUN Collaboration OGLE Collaboration RoboNet Collaboration TI MOA-2011-BLG-262Lb: A SUB-EARTH-MASS MOON ORBITING A GAS GIANT PRIMARY OR A HIGH VELOCITY PLANETARY SYSTEM IN THE GALACTIC BULGE SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing: micro; planetary systems ID GRAVITATIONAL LENSING EXPERIMENT; FREE-FLOATING PLANET; MAGNIFICATION MICROLENSING EVENTS; SNOW LINE; EXTRASOLAR PLANETS; MAIN-SEQUENCE; STELLAR-MASS; BROWN DWARF; OGLE-III; JUPITER/SATURN ANALOG AB We present the first microlensing candidate for a free-floating exoplanet-exomoon system, MOA-2011-BLG-262, with a primary lens mass of M-host similar to 4 Jupitermasses hosting a sub-Earthmassmoon. The argument for an exomoon hinges on the system being relatively close to the Sun. The data constrain the product M-L pi(rel) where ML is the lens system mass and prel is the lens-source relative parallax. If the lens system is nearby (large pi(rel)), then ML is small (a few Jupiter masses) and the companion is a sub-Earth-mass exomoon. The best-fit solution has a large lens-source relative proper motion, mu(rel) = 19.6 +/- 1.6 mas yr(-1), which would rule out a distant lens system unless the source star has an unusually high proper motion. However, data from the OGLE collaboration nearly rule out a high source proper motion, so the exoplanet+exomoon model is the favored interpretation for the best fit model. However, there is an alternate solution that has a lower proper motion and fits the data almost as well. This solution is compatible with a distant (so stellar) host. A Bayesian analysis does not favor the exoplanet+exomoon interpretation, so Occam's razor favors a lens system in the bulge with host and companion masses of M-host = 0.12(-0.06)(+0.19) M-circle dot and m(comp) = 18(-10)(+28) M-circle plus, at a projected separation of a(perpendicular to) = 0.84(-0.14)(+0.25) AU. The existence of this degeneracy is an unlucky accident, so current microlensing experiments are in principle sensitive to exomoons. In some circumstances, it will be possible to definitively establish the mass of such lens systems through the microlensing parallax effect. Future experiments will be sensitive to less extreme exomoons. C1 [Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Batista, V.; Gaudi, B. S.; Gould, A.; McGregor, D.; Pogge, R. W.; Yee, J. C.; Poleski, R.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Batista, V.; Beaulieu, J. -P.; Cassan, A.; Corrales, E.; Coutures, C.; Kubas, D.; Marquette, J. -B.] UPMC, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Bond, I. A.; Ling, C. H.; Sweatman, W. L.] Massey Univ, Inst Nat & Math Sci, Auckland 0745, New Zealand. [Bennett, C. S.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Bennett, C. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Suzuki, D.; Koshimoto, N.; Namba, S.; Sumi, T.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Udalski, A.; Szymanski, M. K.; Skowron, J.; Poleski, R.; Kozllowski, S.; Wyrzykowski, L.; Kubiak, M.; Pietrukowicz, P.; Pietrzynski, G.; Soszynski, I.; Ulaczyk, K.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Donatowicz, J.] Vienna Univ Technol, A-1040 Vienna, Austria. [Bozza, V.] Univ Salerno, Dipartimento Fis, I-84084 Fisciano, Italy. [Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy. [Abe, F.; Fukunaga, D.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Tsurumi, N.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Botzler, C. S.; Freeman, M.; Rattenbury, N. J.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1001, New Zealand. [Fukui, A.] Natl Astron Observ, Okayama Astrophys Observ, Okayama 7190232, 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 6140, New Zealand. [Tristram, P. J.] Mt John Univ Observ, Lake Tekapo 8770, New Zealand. [Albrow, M. D.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand. [Bachelet, E.; Fouque, P.] Univ Toulouse, CNRS, IRAP, F-31400 Toulouse, France. [Brillant, S.; Gonzalez, O. A.; Rejkuba, M.] European So Observ, Santiago 19, Chile. [Caldwell, J. A. R.] McDonald Observ, Fort Davis, TX 79734 USA. [Cole, A. A.; Dieters, S.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Prester, D. Dominis] Univ Rijeka, Dept Phys, Rijeka 51000, Croatia. [Horne, K.; Dominik, M.; Browne, P.; Hundertmark, M.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Koo, J. -R.; Choi, J. Y.; Han, C.; Shin, I. -G.] Chungbuk Natl Univ, Dept Phys, Chongju 371763, South Korea. [Martin, R.; Williams, A.] Perth Observ, Perth, WA 6076, Australia. [Menzies, J. W.] S African Astron Observ, ZA-7925 Cape Town, South Africa. [Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Wambsganss, J.; Zub, M.] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. [DePoy, D. L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Dong, Subo] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Tsapras, Y.; Street, R. A.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Tsapras, Y.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England. [Bramich, D. M.; Kains, N.] ESO Headquarters, D-85748 Munich, Germany. [Bramich, D. M.] Qatar Fdn, Qatar Environm & Energy Res Inst, Doha, Qatar. [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England. [Dekany, I.; Minniti, D.; Saito, R.] Pontificia Univ Catolica Chile, Santiago 22, Chile. [Heyrovsky, D.] Charles Univ Prague, Inst Theoret Phys, Prague 18000, Czech Republic. [Kandori, R.; Nagayama, T.] Nagoya Univ, Grad Sch Sci, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Kerins, E.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Lucas, P. W.] Univ Hertfordshire, Hatfield AL10 9AB, Herts, England. [Robin, A. C.] Univ Franche Comte, UTINAM, CNRS, Observ Besancon Inst,UMR 6213, F-25010 Besancon, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bennett, DP (reprint author), Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. EM bennett@nd.edu RI Skowron, Jan/M-5186-2014; Heyrovsky, David/A-2031-2015; Williams, Andrew/K-2931-2013; Hundertmark, Markus/C-6190-2015; Saito, Roberto/L-6722-2016; OI Skowron, Jan/0000-0002-2335-1730; Heyrovsky, David/0000-0002-5198-5343; Williams, Andrew/0000-0001-9080-0105; Hundertmark, Markus/0000-0003-0961-5231; Dominik, Martin/0000-0002-3202-0343; Cole, Andrew/0000-0003-0303-3855; Rejkuba, Marina/0000-0002-6577-2787; Snodgrass, Colin/0000-0001-9328-2905 FU JSPS [JSPS23340044, JSPS24253004]; NASA Keck PI Data Award; W. M. Keck Foundation; NSF [AST 110347, AST-0807444]; NASA [NNX12AB99G]; Ralph E. and Doris M. Hansmann Membership at the IAS; California Institute of Technology (Caltech); NASA through the Sagan Fellowship Program; European Research Council under the European Community's Seventh Framework Programme (FP7)/ERC [246678]; Czech Science Foundation grant GACR [P209/10/1318]; NPRP grant from the Qatar National Research Fund (a member of the Qatar Foundation) [NPRP-09-476-1-78]; [NASA-NNX12AF54G]; [JPL-RSA 1453175]; [NSF AST-1211875]; [JSPS18253002]; [JSPS20340052] FX D.P.B. was supported by grants NASA-NNX12AF54G, JPL-RSA 1453175 and NSF AST-1211875. This MOA project is supported by the grants JSPS18253002 and JSPS20340052. T. S. acknowledges the financial support from the JSPS, JSPS23340044, JSPS24253004. This work was partially supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. B. S. G. and A. G. were supported by NSF grant AST 110347. B. S. G., A. G., R. P. G. were supported by NASA grant NNX12AB99G. S. D. was partly supported through a Ralph E. and Doris M. Hansmann Membership at the IAS and by NSF grant AST-0807444. Work by J.C.Y. was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 246678 to A. U. D. H. was supported by Czech Science Foundation grant GACR P209/10/1318. D. M. B., M. D., K. H., C. S., R. A. S., M. H. and Y.T. are supported by NPRP grant NPRP-09-476-1-78 from the Qatar National Research Fund (a member of the Qatar Foundation). NR 95 TC 28 Z9 28 U1 1 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2014 VL 785 IS 2 AR 155 DI 10.1088/0004-637X/785/2/155 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800074 ER PT J AU Hendricks, B Koch, A Lanfranchi, GA Boeche, C Walker, M Johnson, CI Penarrubia, J Gilmore, G AF Hendricks, Benjamin Koch, Andreas Lanfranchi, Gustavo A. Boeche, Corrado Walker, Matthew Johnson, Christian I. Penarrubia, Jorge Gilmore, Gerard TI THE METAL-POOR KNEE IN THE FORNAX DWARF SPHEROIDAL GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: dwarf; galaxies: evolution; galaxies: individual (Fornax); galaxies: star formation ID MULTIELEMENT ABUNDANCE MEASUREMENTS; CA II TRIPLET; STAR-FORMATION HISTORY; CHEMICAL EVOLUTION; GLOBULAR-CLUSTERS; METALLICITY DISTRIBUTION; LOCAL GROUP; MILKY-WAY; ELEMENTAL ABUNDANCES; SATELLITE GALAXIES AB We present alpha-element abundances of Mg, Si, and Ti for a large sample of field stars in two outer fields of the Fornax dwarf spheroidal (dSph) galaxy, obtained with Very Large Telescope/GIRAFFE (R similar to 16,000). Due to the large fraction of metal-poor (MP) stars in our sample, we are able to follow the a-element evolution from [Fe/H] approximate to -2.5 continuously to [Fe/H] approximate to -0.7. For the first time we are able to resolve the turnover from the Type II supernovae (SNe) dominated, alpha-enhanced plateau down to subsolar [alpha/Fe] values, due to the onset of SNe Ia, and thus to trace the chemical enrichment efficiency of the galaxy. Our data support the general concept of an a-enhanced plateau at early epochs, followed by a well-defined "knee" caused by the onset of SNe Ia, and finally a second plateau with sub-solar [a/Fe] values. We find the position of this knee to be at [Fe/H] approximate to -1.9 and therefore significantly more MP than expected from comparison with other dSphs and standard evolutionary models. Surprisingly, this value is rather comparable to the knee in Sculptor, a dSph similar to 10 times less luminous than Fornax. Using chemical evolution models, we find that the position of the knee and the subsequent plateau at the sub-solar level can hardly be explained unless the galaxy experienced several discrete star formation (SF) events with a drastic variation in SF efficiency, while a uniform SF can be ruled out. One possible evolutionary scenario is that Fornax experienced one or several major accretion events from gas-rich systems in the past, so that its current stellar mass is not indicative of the chemical evolution environment at ancient times. If Fornax is the product of several smaller buildings blocks, this may also have implications for the understanding of the formation process of dSphs in general. C1 [Hendricks, Benjamin; Koch, Andreas] Heidelberg Univ, Zentrum Astron, Landessternwarte, D-69117 Heidelberg, Germany. [Lanfranchi, Gustavo A.] Univ Cruzeiro Sul, Nucleo Astrofis Teor, BR-01506000 Sao Paulo, Brazil. [Boeche, Corrado] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, D-69120 Heidelberg, Germany. [Walker, Matthew] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Johnson, Christian I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Penarrubia, Jorge] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Gilmore, Gerard] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. RP Hendricks, B (reprint author), Heidelberg Univ, Zentrum Astron, Landessternwarte, Konigstuhl 12, D-69117 Heidelberg, Germany. EM ben.hendricks@lsw.uni-heidelberg.de RI Walker, Matthew/P-1777-2014; OI Walker, Matthew/0000-0003-2496-1925; Koch, Andreas/0000-0002-9859-4956 FU German Research Foundation (DFG) [Ko 4161/1]; DFG [Sonderforschungsbereich SFB 881]; CNPq [308677/2012-9]; Clay Fellowship; European Union FP7 program through ERC [320360] FX B. Hendricks thanks M. Frank and N. Kacharov for many fruitful discussions. B.H. and A.K. acknowledge the German Research Foundation (DFG) for funding from Emmy-Noether grant Ko 4161/1. This work was in part supported by Sonderforschungsbereich SFB 881 "The Milky Way System" (subproject A5) of the DFG. G. A. L acknowledges Brazilian agency CNPq, proj. 308677/2012-9. C.I.J. acknowledges support through the Clay Fellowship administered by the Smithsonian Astrophysical Observatory. This work was partly supported by the European Union FP7 program through ERC grant number 320360. NR 61 TC 19 Z9 19 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2014 VL 785 IS 2 AR 102 DI 10.1088/0004-637X/785/2/102 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800021 ER PT J AU Knutson, HA Fulton, BJ Montet, BT Kao, M Ngo, H Howard, AW Crepp, JR Hinkley, S Bakos, GA Batygin, K Johnson, JA Morton, TD Muirhead, PS AF Knutson, Heather A. Fulton, Benjamin J. Montet, Benjamin T. Kao, Melodie Ngo, Henry Howard, Andrew W. Crepp, Justin R. Hinkley, Sasha Bakos, Gaspar A. Batygin, Konstantin Johnson, John Asher Morton, Timothy D. Muirhead, Philip S. TI FRIENDS OF HOT JUPITERS. I. A RADIAL VELOCITY SEARCH FOR MASSIVE, LONG-PERIOD COMPANIONS TO CLOSE-IN GAS GIANT PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; instrumentation: adaptive optics; planetary systems techniques: radial velocities ID SPIN-ORBIT ALIGNMENT; SOLAR-TYPE STARS; ROSSITER-MCLAUGHLIN OBSERVATIONS; TRANSITING EXOPLANET WASP-3B; INFRARED-EMISSION SPECTRUM; HIGH-PRECISION PHOTOMETRY; LIGHT-CURVE PROJECT; CHAIN MONTE-CARLO; BRIGHT F-STAR; LOW-DENSITY AB In this paper we search for distant massive companions to known transiting gas giant planets that may have influenced the dynamical evolution of these systems. We present new radial velocity observations for a sample of 51 planets obtained using the Keck HIRES instrument, and find statistically significant accelerations in fifteen systems. Six of these systems have no previously reported accelerations in the published literature: HAT-P-10, HAT-P-22, HAT-P-29, HAT-P-32, WASP-10, and XO-2. We combine our radial velocity fits with Keck NIRC2 adaptive optics (AO) imaging data to place constraints on the allowed masses and orbital periods of the companions responsible for the detected accelerations. The estimated masses of the companions range between 1-500MJup, with orbital semi-major axes typically between 1-75 AU. A significant majority of the companions detected by our survey are constrained to have minimum masses comparable to or larger than those of the transiting planets in these systems, making them candidates for influencing the orbital evolution of the inner gas giant. We estimate a total occurrence rate of 51% +/- 10% for companions with masses between 1-13M(Jup) and orbital semi-major axes between 1-20AU in our sample. We find no statistically significant difference between the frequency of companions to transiting planets with misaligned or eccentric orbits and those with well-aligned, circular orbits. We combine our expanded sample of radial velocity measurements with constraints from transit and secondary eclipse observations to provide improved measurements of the physical and orbital characteristics of all of the planets included in our survey. C1 [Knutson, Heather A.; Ngo, Henry; Johnson, John Asher] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Fulton, Benjamin J.; Howard, Andrew W.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Montet, Benjamin T.; Kao, Melodie; Hinkley, Sasha; Morton, Timothy D.; Muirhead, Philip S.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Montet, Benjamin T.; Batygin, Konstantin; Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Bakos, Gaspar A.; Morton, Timothy D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Muirhead, Philip S.] Boston Univ, Dept Astron, Boston, MA 02215 USA. RP Knutson, HA (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM hknutson@caltech.edu RI Muirhead, Philip/H-2273-2014; Howard, Andrew/D-4148-2015; OI Muirhead, Philip/0000-0002-0638-8822; Howard, Andrew/0000-0001-8638-0320; Montet, Benjamin/0000-0001-7516-8308; Ngo, Henry/0000-0001-5172-4859 FU University of Hawaii; University of California; California Institute of Technology; National Science Foundation [DGE-1144469]; David and Lucille Packard Foundation; Alfred P. Sloan Foundation; NASA [HST-HF-51326.01, NAS 5-26555]; STScI; NSF [AST-1203023]; [NSFAST-1108686] FX We thank Jason Wright and Joshua Winn for their thoughtful input on early drafts of this paper. This work was based on observations at the W.M. Keck Observatory granted by the University of Hawaii, the University of California, and the California Institute of Technology. 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. B. T. M. is supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1144469. J.A.J. and G. B. are supported by grants from the David and Lucille Packard Foundation and the Alfred P. Sloan Foundation. P. S. M. acknowledges support for this work from the Hubble Fellowship Program, provided by NASA through Hubble Fellowship grant HST-HF-51326.01-A awarded by the STScI, which is operated by the AURA, Inc., for NASA, under contract NAS 5-26555. S. H. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1203023. G. B. acknowledges support from grant NSFAST-1108686. NR 209 TC 85 Z9 85 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2014 VL 785 IS 2 AR 126 DI 10.1088/0004-637X/785/2/126 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800045 ER PT J AU Li, GJ Naoz, S Kocsis, B Loeb, A AF Li, Gongjie Naoz, Smadar Kocsis, Bence Loeb, Abraham TI ECCENTRICITY GROWTH AND ORBIT FLIP IN NEAR-COPLANAR HIERARCHICAL THREE-BODY SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries (including multiple): close; celestial mechanics; planets and satellites: dynamical evolution and stability ID PLANET-PLANET SCATTERING; SUPERMASSIVE BLACK-HOLES; X-RAY OUTBURST; TIDAL DISRUPTION; KOZAI MECHANISM; HOT JUPITERS; TRIPLE STARS; EXTRASOLAR PLANETS; SECULAR EVOLUTION; STELLAR BINARIES AB The secular dynamical evolution of a hierarchical three-body system in which a distant third object orbits around a binary has been studied extensively, demonstrating that the inner orbit can undergo large eccentricity and inclination oscillations. It was shown before that starting with a circular inner orbit, large mutual inclination (40. -140.) can produce long timescale modulations that drive the eccentricity to extremely large values and can flip the orbit. Here, we demonstrate that starting with an almost coplanar configuration, for eccentric inner and outer orbits, the eccentricity of the inner orbit can still be excited to high values, and the orbit can flip by similar to 180 degrees, rolling over its major axis. The similar to 180 degrees. flip criterion and the flip timescale are described by simple analytic expressions that depend on the initial orbital parameters. With tidal dissipation, this mechanism can produce counter-orbiting exoplanetary systems. In addition, we also show that this mechanism has the potential to enhance the tidal disruption or collision rates for different systems. Furthermore, we explore the entire e(1) and i(0) parameter space that can produce flips. C1 [Li, Gongjie; Naoz, Smadar; Kocsis, Bence; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Kocsis, Bence] Inst Adv Study, Princeton, NJ 08540 USA. RP Li, GJ (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM gli@cfa.harvard.edu RI Kocsis, Bence/C-3061-2013; OI Kocsis, Bence/0000-0002-4865-7517; Naoz, Smadar/0000-0002-9802-9279 FU NASA through an Einstein Post-doctoral Fellowship; Chandra X-ray Center; NASA [PF2-130096]; W. M. Keck Foundation Fund of the Institute for Advanced Study; NASA grant [NNX11AF29G]; NSF grant [AST-1312034] FX We thank Konstantin Batygin, Matt Holman, Josh Winn, and Boaz Katz for useful remarks. S.N. is supported by NASA through an Einstein Post-doctoral Fellowship awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract PF2-130096. B.K. was supported in part by the W. M. Keck Foundation Fund of the Institute for Advanced Study and NASA grant NNX11AF29G. A.L. was supported in part by NSF grant AST-1312034. NR 71 TC 46 Z9 46 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 2014 VL 785 IS 2 AR 116 DI 10.1088/0004-637X/785/2/116 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800035 ER PT J AU Mezcua, M Fabbiano, G Gladstone, JC Farrell, SA Soria, R AF Mezcua, M. Fabbiano, G. Gladstone, J. C. Farrell, S. A. Soria, R. TI REVEALING THE NATURE OF THE ULX AND X-RAY POPULATION OF THE SPIRAL GALAXY NGC 4088 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; black hole physics; ISM: jets and outflows; radio continuum: general X-rays:binaries ID MASS BLACK-HOLE; QUASI-PERIODIC OSCILLATIONS; ULTRACOMPACT HII-REGIONS; ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; ESO 243-49 HLX-1; NEARBY GALAXIES; RADIO-EMISSION; XMM-NEWTON; LUMINOSITY FUNCTION AB We present the first Chandra and Swift X-ray study of the spiral galaxy NGC 4088 and its ultraluminous X-ray source (ULX N4088-X1). We also report very long baseline interferometry (VLBI) observations at 1.6 and 5 GHz performed quasi-simultaneously with the Swift and Chandra observations, respectively. Fifteen X-ray sources are detected by Chandra within the D25 ellipse of NGC 4088, from which we derive the X-ray luminosity function (XLF) of this galaxy. We find the XLF is very similar to those of star-forming galaxies and estimate a star-formation rate of 4.5M(circle dot) yr(-1). The Chandra detection of the ULX yields its most accurate X-ray position, which is spatially coincident with compact radio emission at 1.6 GHz. The ULX Chandra X-ray luminosity, L0.2-10.0 keV = 3.4 x 10(39) erg s(-1), indicates that N4088-X1 could be located at the high-luminosity end of the high-mass X-ray binary (HMXB) population of NGC 4088. The estimates of the black hole (BH) mass and ratio of radio to X-ray luminosity of N4088-X1 rule out a supermassive BH nature. The Swift X-ray spectrum of N4088-X1 is best described by a thermal Comptonization model and presents a statistically significant high-energy cutoff. We conclude that N4088-X1 is most likely a stellar remnant BH in an HMXB, probably fed by Roche lobe overflow, residing in a super-Eddington ultraluminous state. The 1.6 GHz VLBI source is consistent with radio emission from possible ballistic jet ejections in this state. C1 [Mezcua, M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Mezcua, M.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Fabbiano, G.] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. [Gladstone, J. C.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Farrell, S. A.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Soria, R.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. RP Mezcua, M (reprint author), Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. EM mmezcua@iac.es FU Chandra X-Ray Center (CXC); NASA [NAS8-03060]; Chandra Director Discretionary Time grant [DD2-13063X]; NSERC; Australian Research Council; Australian Research Council [DP120102393]; [AYA2011-25527]; [DP110102889] FX This work was partially supported by the Chandra X-Ray Center (CXC), which is operated by the Smithsonian Astrophysical Observatory (SAO) under NASA contract NAS8-03060, and by Chandra Director Discretionary Time grant DD2-13063X. M. M. acknowledges financial support from AYA2011-25527. J.C.G. would like to acknowledge Avadh Bhatia Fellowship, the Alberta Ingenuity New Faculty Award, and the financial support from NSERC Discovery Grants. S. A. F. is the recipient of an Australian Research Council Postdoctoral Fellowship, funded by grant DP110102889. RS acknowledges support from the Australian Research Council's Discovery Projects funding scheme (project number DP120102393). NR 104 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 APR 20 PY 2014 VL 785 IS 2 AR 121 DI 10.1088/0004-637X/785/2/121 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800040 ER PT J AU Ranjan, S Charbonneau, D Desert, JM Madhusudhan, N Deming, D Wilkins, A Mandell, AM AF Ranjan, Sukrit Charbonneau, David Desert, Jean-Michel Madhusudhan, Nikku Deming, Drake Wilkins, Ashlee Mandell, Avi M. TI ATMOSPHERIC CHARACTERIZATION OF FIVE HOT JUPITERS WITH THE WIDE FIELD CAMERA 3 ON THE HUBBLE SPACE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; techniques: photometric; techniques: spectroscopic ID NICMOS TRANSMISSION SPECTROSCOPY; EXTRASOLAR PLANET ATMOSPHERE; COLLISION-INDUCED ABSORPTION; INFRARED-EMISSION SPECTRUM; SECONDARY ECLIPSE; HD 189733B; TEMPERATURE INVERSION; EXOPLANET ATMOSPHERES; MODEL ATMOSPHERES; THERMAL EMISSION AB We probe the structure and composition of the atmospheres of five hot Jupiter exoplanets using the Hubble Space Telescope Wide Field Camera 3 (WFC3) instrument. We use the G141 grism (1.1-1.7 mu m) to study TrES-2b, TrES-4b, and CoRoT-1b in transit; TrES-3b in secondary eclipse; and WASP-4b in both. This wavelength region includes a predicted absorption feature from water at 1.4 mu m, which we expect to be nondegenerate with the other molecules that are likely to be abundant for hydrocarbon-poor (e. g., solar composition) hot Jupiter atmospheres. We divide our wavelength regions into 10 bins. For each bin we produce a spectrophotometric light curve spanning the time of transit or eclipse. We correct these light curves for instrumental systematics without reference to an instrument model. For our transmission spectra, our mean 1 sigma precision per bin corresponds to variations of 2.1, 2.8, and 3.0 atmospheric scale heights for TrES-2b, TrES-4b, and CoRoT-1b, respectively. We find featureless spectra for these three planets. We are unable to extract a robust transmission spectrum for WASP-4b. For our dayside emission spectra, our mean 1 sigma precision per bin corresponds to a planet-to-star flux ratio of 1.5 x 10(-4) and 2.1 x 10(-4) for WASP-4b and TrES-3b, respectively. We combine these estimates with previous broadband measurements and conclude that for both planets isothermal atmospheres are disfavored. We find no signs of features due to water. We confirm that WFC3 is suitable for studies of transiting exoplanets, but in staring mode multivisit campaigns are necessary to place strong constraints on water abundance. C1 [Ranjan, Sukrit; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Desert, Jean-Michel] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Madhusudhan, Nikku] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA. [Deming, Drake; Wilkins, Ashlee] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mandell, Avi M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Desert, Jean-Michel] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Ranjan, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sranjan@cfa.harvard.edu OI Ranjan, Sukrit/0000-0002-5147-9053 FU NASA through Space Telescope Science Institute; NASA [NAS 5-26555]; National Science Foundation Graduate Research Fellowship [DGE-1144152]; California Institute of Technology (Caltech); NASA through the Sagan Fellowship Program grant; Yale University through the YCAA postdoctoral prize fellowship; [HST-GO-12181] FX Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute (STScI). These observations are associated with program HST-GO-12181. Support for this program was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1144152. This work was also performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program grant awarded to J.-M.D. N.M. acknowledges support from Yale University through the YCAA postdoctoral prize fellowship. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org; the SIMBAD database, operated at CDS, Strasbourg, France; NASA's Astrophysics Data System Bibliographic Services; and SAOImage DS9, developed by Smithsonian Astrophysical Observatory. The authors are grateful to Z. Berta-Thompson and J. Carter for many fruitful discussions, to the STScI HST help team for their assistance, and to an anonymous referee whose comments strengthened the paper. NR 69 TC 15 Z9 15 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2014 VL 785 IS 2 AR 148 DI 10.1088/0004-637X/785/2/148 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800067 ER PT J AU Spilker, JS Marrone, DP Aguirre, E Aravena, M Ashby, MLN Bethermin, M Bradford, CM Bothwell, MS Brodwin, M Carlstrom, JE Chapman, SC Crawford, TM de Breuck, C Fassnacht, CD Gonzalez, AH Greve, TR Gullberg, B Hezaveh, Y Holzapfel, WL Husband, K Ma, J Malkan, M Murphy, EJ Reichardt, CL Rotermund, KM Stalder, B Stark, AA Strandet, M Vieira, JD Weiss, A Welikala, N AF Spilker, J. S Marrone, D. P. Aguirre, E. Aravena, M. Ashby, M. L. N. Bethermin, M. Bradford, C. M. Bothwell, M. S. Brodwin, M. Carlstrom, J. E. Chapman, S. C. Crawford, T. M. de Breuck, C. Fassnacht, C. D. Gonzalez, A. H. Greve, T. R. Gullberg, B. Hezaveh, Y. Holzapfel, W. L. Husband, K. Ma, J. Malkan, M. Murphy, E. J. Reichardt, C. L. Rotermund, K. M. Stalder, B. Stark, A. A. Strandet, M. Vieira, J. D. Weiss, A. Welikala, N. TI THE REST-FRAME SUBMILLIMETER SPECTRUM OF HIGH-REDSHIFT, DUSTY, STAR-FORMING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: ISM; galaxies: star formation; ISM: molecules ID DENSE MOLECULAR GAS; SOUTH-POLE TELESCOPE; ULTRALUMINOUS INFRARED GALAXIES; DIFFUSE INTERSTELLAR-MEDIUM; CLOVERLEAF QUASAR; APM 08279+5255; CONVERSION FACTOR; HERSCHEL-SPIRE; LINE EMISSION; ARP 220 AB We present the average rest-frame spectrum of high-redshift dusty, star-forming galaxies from 250 to 770 GHz. This spectrum was constructed by stacking Atacama Large Millimeter/submillimeter Array (ALMA) 3 mm spectra of 22 such sources discovered by the South Pole Telescope and spanning z = 2.0-5.7. In addition to multiple bright spectral features of (CO)-C-12, [C I], and H2O, we also detect several faint transitions of (CO)-C-13, HCN, HNC, HCO+, and CN, and use the observed line strengths to characterize the typical properties of the interstellar medium of these high-redshift starburst galaxies. We find that the (CO)-C-13 brightness in these objects is comparable to that of the only otherz > 2 star-forming galaxy in which (CO)-C-13 has been observed. We show that the emission from the high-critical density molecules HCN, HNC, HCO+, and CN is consistent with a warm, dense medium with T-kin similar to 55K and n(H2) >= 10(5.5) cm(-3). High molecular hydrogen densities are required to reproduce the observed line ratios, and we demonstrate that alternatives to purely collisional excitation are unlikely to be significant for the bulk of these systems. We quantify the average emission from several species with no individually detected transitions, and find emission from the hydride CH and the linear molecule CCH for the first time at high redshift, indicating that these molecules may be powerful probes of interstellar chemistry in high-redshift systems. These observations represent the first constraints on many molecular species with rest-frame transitions from 0.4 to 1.2 mm in star-forming systems at high redshift, and will be invaluable in making effective use of ALMA in full science operations. C1 [Spilker, J. S; Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Aguirre, E.] Univ Penn, Philadelphia, PA 19104 USA. [Aravena, M.] European So Observ, Casilla 19001, Vitacura Santia, Chile. [Aravena, M.] Univ Diego Port, Fac Ingn, Santiago, Chile. [Ashby, M. L. N.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bethermin, M.] Univ Paris Diderot, CEA Saclay, CEA DSM Irfu CNRS, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bothwell, M. S.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HA, England. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Carlstrom, J. E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Chapman, S. C.; Rotermund, K. M.] Dalhousie Univ, Halifax, NS, Canada. [de Breuck, C.; Gullberg, B.] European So Observ, D-85748 Garching, Germany. [Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Gonzalez, A. H.; Husband, K.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Hezaveh, Y.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Holzapfel, W. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Husband, K.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Malkan, M.] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Murphy, E. J.] Carnegie Inst Sci, Pasadena, CA 91101 USA. [Strandet, M.; Weiss, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Welikala, N.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France. RP Spilker, JS (reprint author), Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. EM jspilker@as.arizona.edu RI Aravena, Manuel/O-2361-2014; Holzapfel, William/I-4836-2015; OI Bethermin, Matthieu/0000-0002-3915-2015; Stark, Antony/0000-0002-2718-9996; Marrone, Daniel/0000-0002-2367-1080; Reichardt, Christian/0000-0003-2226-9169; De Breuck, Carlos/0000-0002-6637-3315 FU U.S. National Science Foundation [AST-1312950]; National Science Foundation [ANT-0638937]; Kavli Foundation; Gordon and Betty Moore Foundation; Commonwealth of Australia; [PHY-1125897] FX This material is based on work supported by the U.S. National Science Foundation under grant No. AST-1312950. 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. This paper makes use of the following ALMA data: ADS/JAO.ALMA2011.0.00957.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. 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 Commonwealth of Australia for operation as a National Facility managed by CSIRO. This research has made use of NASA's Astrophysics Data System. NR 119 TC 18 Z9 18 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2014 VL 785 IS 2 AR 149 DI 10.1088/0004-637X/785/2/149 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800068 ER PT J AU Wellons, S Zhu, YC Psaltis, D Narayan, R McClintock, JE AF Wellons, Sarah Zhu, Yucong Psaltis, Dimitrios Narayan, Ramesh McClintock, Jeffrey E. TI A HIGH-FREQUENCY DOPPLER FEATURE IN THE POWER SPECTRA OF SIMULATED GRMHD BLACK HOLE ACCRETION DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; X-rays: binaries ID X-RAY BINARIES; ADVECTION-DOMINATED ACCRETION; QUASI-PERIODIC OSCILLATIONS; LENS-THIRRING PRECESSION; MAGNETOHYDRODYNAMIC SIMULATIONS; GENERAL-RELATIVITY; PLUNGING REGION; MODEL; VARIABILITY; SYSTEMS AB Black hole binaries exhibit a wide range of variability phenomena, from large-scale state changes to broadband noise and quasi-periodic oscillations, but the physical nature of much of this variability is poorly understood. We examine the variability properties of three GRMHD simulations of thin accretion disks around black holes of varying spin, producing light curves and power spectra as would be seen by observers. We find that the simulated power spectra show a broad feature at high frequency, which increases in amplitude with the inclination of the observer. We show that this high-frequency feature is a product of the Doppler effect and that its location is a function of the mass and spin of the black hole. This Doppler feature demonstrates that power spectral properties of the accretion disk can be tied to, and potentially used to determine, physical properties of the black hole. C1 [Wellons, Sarah; Zhu, Yucong; Narayan, Ramesh; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Psaltis, Dimitrios] Univ Arizona, Dept Astron, Tucson, AZ USA. RP Wellons, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM swellons@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU National Science Foundation Graduate Research Fellowship [DGE1144152]; National Science Foundation [OCI-1053575, AST1312651]; NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center; NSF CAREER award [AST-0746549] FX S.W. is supported by the National Science Foundation Graduate Research Fellowship under grant number DGE1144152. Resources supporting this work were provided by the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number OCI-1053575, and the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. This material is based upon work supported by National Science Foundation grant number AST1312651 to R.N. D. P. was partially supported by NSF CAREER award AST-0746549. NR 40 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 20 PY 2014 VL 785 IS 2 AR 142 DI 10.1088/0004-637X/785/2/142 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800061 ER PT J AU Wiklind, T Conselice, CJ Dahlen, T Dickinson, ME Ferguson, HC Grogin, NA Guo, YC Koekemoer, AM Mobasher, B Mortlock, A Fontana, A Dave, R Yan, HJ Acquaviva, V Ashby, MLN Barro, G Caputi, KI Castellano, M Dekel, A Donley, JL Fazio, GG Giavalisco, M Grazian, A Hathi, NP Kurczynski, P Lu, Y McGrath, EJ de Mello, DF Peth, M Safarzadeh, M Stefanon, M Targett, T AF Wiklind, Tommy Conselice, Christopher J. Dahlen, Tomas Dickinson, Mark E. Ferguson, Henry C. Grogin, Norman A. Guo, Yicheng Koekemoer, Anton M. Mobasher, Bahram Mortlock, Alice Fontana, Adriano Dave, Romeel Yan, Haojing Acquaviva, Viviana Ashby, Matthew L. N. Barro, Guillermo Caputi, Karina I. Castellano, Marco Dekel, Avishai Donley, Jennifer L. Fazio, Giovanni G. Giavalisco, Mauro Grazian, Andrea Hathi, Nimish P. Kurczynski, Peter Lu, Yu McGrath, Elizabeth J. de Mello, Duilia F. Peth, Michael Safarzadeh, Mohammad Stefanon, Mauro Targett, Thomas TI PROPERTIES OF SUBMILLIMETER GALAXIES IN THE CANDELS GOODS-SOUTH FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: photometry ID HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; HUBBLE-DEEP-FIELD; COSMOLOGICAL HYDRODYNAMIC SIMULATIONS; ULTRALUMINOUS INFRARED GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; EXTRAGALACTIC LEGACY SURVEY; X-RAY-PROPERTIES; SIMILAR-TO 2 AB We derive physical properties of 10 submillimeter galaxies located in the CANDELS coverage of the GOODS-S field. The galaxies were first identified as submillimeter sources with the LABOCA bolometer and subsequently targeted for 870 mu m continuum observation with ALMA. The high angular resolution of the ALMA imaging allows secure counterparts to be identified in the CANDELS multiband data set. The CANDELS data provide deep photometric data from UV through near-infrared wavelengths. Using synthetic spectral energy distributions, we derive photometric redshifts, stellar masses, extinction, ages, and the star formation history. The redshift range is z = 1.65-4.76, with two of the galaxies located atz > 4. Two submillimeter galaxy (SMG) counterparts have stellar masses 2-3 orders of magnitude lower than the rest. The remaining SMG counterparts have stellar masses around 1x10 M-11(circle dot). The stellar population in the SMGs is typically older than the expected duration of the submillimeter phase, suggesting that the star formation history of SMGs is more complex than a single burst. Non-parametric morphology indices suggest that the SMG counterparts are among the most asymmetric systems compared with galaxies of the same stellar mass and redshift. The Hubble Space Telescope images show that three of the SMGs are associated with ongoing mergers. The remaining counterparts are isolated. Estimating the dust and molecular gas mass from the submillimeter fluxes, and comparing with our stellar masses shows that the gas mass fraction of SMGs is similar to 28% and that the final stellar mass is likely to be similar to(1-2) x 10 (11) M-circle dot. C1 [Wiklind, Tommy] Joint ALMA Observ, European So Observ, Santiago, Chile. [Conselice, Christopher J.; Mortlock, Alice] Univ Nottingham, Dept Phys & Astron, Nottingham NG7 2RD, England. [Dahlen, Tomas; Ferguson, Henry C.; Grogin, Norman A.; Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Dickinson, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Guo, Yicheng; Barro, Guillermo] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 95064 USA. [Fontana, Adriano; Castellano, Marco; Grazian, Andrea] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Dave, Romeel] Univ Western Cape, ZA-7535 Bellville, Cape Town, South Africa. [Dave, Romeel] S African Astron Observ, ZA-7925 Cape Town, South Africa. [Dave, Romeel] African Inst Math Sci, ZA-7945 Cape Town, South Africa. [Yan, Haojing; Stefanon, Mauro] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [Acquaviva, Viviana] CUNY, Dept Phys, Coll Technol, Brooklyn, NY 11201 USA. [Ashby, Matthew L. N.; Fazio, Giovanni G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Caputi, Karina I.] Univ Groningen, Kapteyn Astron Inst, Groningen, Netherlands. [Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, Ctr Astrophys & Planetary Sci, IL-91904 Jerusalem, Israel. [Donley, Jennifer L.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Giavalisco, Mauro] Univ Massachusetts, Dept Phys & Astron, Amherst, MA 01003 USA. [Hathi, Nimish P.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, Marseille, France. [Kurczynski, Peter] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08852 USA. [Lu, Yu] Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [McGrath, Elizabeth J.] Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA. [de Mello, Duilia F.] Catholic Univ Amer, Dept Phys & Astron, Washington, DC 20064 USA. [Peth, Michael; Safarzadeh, Mohammad] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Targett, Thomas] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh, Midlothian, Scotland. [Targett, Thomas] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. RP Wiklind, T (reprint author), Joint ALMA Observ, European So Observ, 3107 Alonso de Cordova, Santiago, Chile. EM twiklind@alma.cl RI Stefanon, Mauro/F-8708-2016; Hathi, Nimish/J-7092-2014; OI Stefanon, Mauro/0000-0001-7768-5309; Hathi, Nimish/0000-0001-6145-5090; Castellano, Marco/0000-0001-9875-8263; fontana, adriano/0000-0003-3820-2823; Koekemoer, Anton/0000-0002-6610-2048 FU NASA [NAS5-26555] FX This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is based in part on observations with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA, and also on the Very Large Telescope, operated by the European Southern Observatory. NR 101 TC 17 Z9 18 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2014 VL 785 IS 2 AR 111 DI 10.1088/0004-637X/785/2/111 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG9KA UT WOS:000335736800030 ER PT J AU Evans, NR Pillitteri, I Wolk, S Guinan, E Engle, S Bond, HE Schaefer, GH Karovska, M DePasquale, J Tingle, E AF Evans, Nancy Remage Pillitteri, Ignazio Wolk, Scott Guinan, Edward Engle, Scott Bond, Howard E. Schaefer, Gail H. Karovska, Margarita DePasquale, Joseph Tingle, Evan TI X-RAY DETECTION OF THE CLUSTER CONTAINING THE CEPHEID S MUS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE open clusters and associations: individual (ASCC 69); stars: low-mass; stars: variables: Cepheids; X-rays:stars ID DISTANCE SCALE; LUMINOSITY; EMISSION; STARS AB The galactic Cepheid S Muscae has recently been added to the important list of Cepheids linked to open clusters, in this case the sparse young cluster ASCC 69. Low-mass members of a young cluster are expected to have rapid rotation and X-ray activity, making X-ray emission an excellent way to discriminate them from old field stars. We have made an XMM-Newton observation centered on S Mus and identified a population of X-ray sources whose near-IR Two Micron All Sky Survey counterparts lie at locations in the J, (J - K) color-magnitude diagram consistent with cluster membership at the distance of S Mus. Their median energy and X-ray luminosity are consistent with young cluster members as distinct from field stars. These strengthen the association of S Mus with the young cluster, making it a potential Leavitt law (period-luminosity relation) calibrator. C1 [Evans, Nancy Remage; Pillitteri, Ignazio; Wolk, Scott; Karovska, Margarita; DePasquale, Joseph; Tingle, Evan] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Pillitteri, Ignazio] Osserv Astron Palermo, INAF, I-90134 Palermo, Italy. [Guinan, Edward; Engle, Scott] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Bond, Howard E.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schaefer, Gail H.] CHARA Array Georgia State, Mt Wilson, CA 91023 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA. EM nevans@cfa.harvard.edu 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 [NAS8-03060]; HST [GO-12215.01-A] FX We thank an anonymous referee for comments that improved the presentation of the Letter. Support for this work was also provided from the Chandra X-ray Center NASA contract NAS8-03060 and by HST grant GO-12215.01-A. Vizier and SIMBAD were used in the preparation of this study. NR 14 TC 1 Z9 1 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 2014 VL 785 IS 2 AR L25 DI 10.1088/2041-8205/785/2/L25 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE9VR UT WOS:000334359800006 ER PT J AU Kipping, DM Bastien, FA Stassun, KG Chaplin, WJ Huber, D Buchhave, LA AF Kipping, D. M. Bastien, F. A. Stassun, K. G. Chaplin, W. J. Huber, D. Buchhave, L. A. TI FLICKER AS A TOOL FOR CHARACTERIZING PLANETS THROUGH ASTERODENSITY PROFILING SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: activity; stars: solar-type; techniques: photometric ID CANDIDATE HOST STARS; FIELD STARS; ASTEROSEISMOLOGY; OSCILLATIONS; ROTATION; AGES; VARIABILITY AB Variability in the time series brightness of a star on a timescale of 8 hr, known as "flicker," has been previously demonstrated to serve as a proxy for the surface gravity of a star by Bastien et al. Although surface gravity is crucial for stellar classification, it is the mean stellar density that is most useful when studying transiting exoplanets, due to its direct impact on the transit light curve shape. Indeed, an accurate and independent measure of the stellar density can be leveraged to infer subtle properties of a transiting system, such as the companion's orbital eccentricity via asterodensity profiling (AP). We here calibrate flicker to the mean stellar density of 439 Kepler targets with asteroseismology, allowing us to derive a new empirical relation given by log(10)(rho star (kg m(- 3))) = 5.413 - 1.850 log(10)(F-8 (ppm)). The calibration is valid for stars with 4500 < T-eff < 6500 K, KP < 14, and flicker estimates corresponding to stars with 3.25 < log g star < 4.43. Our relation has a model error in the stellar density of 31.7% and so has similar to 8 times lower precision than that from asteroseismology but is applicable to a sample similar to 40 times greater. Flicker therefore provides an empirical method to enable AP on hundreds of planetary candidates from present and future missions. C1 [Kipping, D. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bastien, F. A.; Stassun, K. G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Stassun, K. G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Chaplin, W. J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Chaplin, W. J.] Aarhus Univ, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huber, D.] SETI Inst, Mountain View, CA 94043 USA. [Buchhave, L. A.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu OI Buchhave, Lars A./0000-0003-1605-5666; Stassun, Keivan/0000-0002-3481-9052 FU NASA Sagan Fellowship; NASA Harriet Jenkins Fellowship; Vanderbilt Provost Graduate Fellowship; UK Science and Technology Facilities Council; NASA Postdoctoral Program at Ames Research Center; Kepler Participating Scientist Program FX D.M.K. is supported by the NASA Sagan Fellowships. F. A. B. is supported by the NASA Harriet Jenkins Fellowship and a Vanderbilt Provost Graduate Fellowship. W.J.C. acknowledges financial support from the UK Science and Technology Facilities Council. D. H. acknowledges support by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA, and support by the Kepler Participating Scientist Program. We thank the anaon. NR 33 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2014 VL 785 IS 2 AR L32 DI 10.1088/2041-8205/785/2/L32 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE9VR UT WOS:000334359800013 ER PT J AU Yamaguchi, H Badenes, C Petre, R Nakano, T Castro, D Enoto, T Hiraga, JS Hughes, JP Maeda, Y Nobukawa, M Safi-Harb, S Slane, PO Smith, RK Uchida, H AF Yamaguchi, Hiroya Badenes, Carles Petre, Robert Nakano, Toshio Castro, Daniel Enoto, Teruaki Hiraga, Junko S. Hughes, John P. Maeda, Yoshitomo Nobukawa, Masayoshi Safi-Harb, Samar Slane, Patrick O. Smith, Randall K. Uchida, Hiroyuki TI DISCRIMINATING THE PROGENITOR TYPE OF SUPERNOVA REMNANTS WITH IRON K-SHELL EMISSION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: abundances; ISM: supernova remnants; X-rays: ISM ID X-RAY-EMISSION; LARGE-MAGELLANIC-CLOUD; XMM-NEWTON OBSERVATIONS; IA SUPERNOVA; SHOCKED EJECTA; RCW 86; CHANDRA; SPECTROSCOPY; EXPLOSION; SUZAKU AB Supernova remnants (SNRs) retain crucial information about both their parent explosion and circumstellar material left behind by their progenitor. However, the complexity of the interaction between supernova ejecta and ambient medium often blurs this information, and it is not uncommon for the basic progenitor type (Ia or core-collapse) of well-studied remnants to remain uncertain. Here we present a powerful new observational diagnostic to discriminate between progenitor types and constrain the ambient medium density of SNRs using solely Fe K-shell X-ray emission. We analyze all extant Suzaku observations of SNRs and detect Fe K alpha emission from 23 young or middle-aged remnants, including five first detections (IC 443, G292.0+ 1.8, G337.2-0.7, N49, and N63A). The Fe Ka centroids clearly separate progenitor types, with the Fe-rich ejecta in Type Ia remnants being significantly less ionized than in core-collapse SNRs. Within each progenitor group, the Fe Ka luminosity and centroid are well correlated, with more luminous objects having more highly ionized Fe. Our results indicate that there is a strong connection between explosion type and ambient medium density, and suggest that Type Ia supernova progenitors do not substantially modify their surroundings at radii of up to several parsecs. We also detect a K-shell radiative recombination continuum of Fe in W49B and IC 443, implying a strong circumstellar interaction in the early evolutionary phases of these core-collapse remnants. C1 [Yamaguchi, Hiroya; Petre, Robert; Enoto, Teruaki] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yamaguchi, Hiroya] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Yamaguchi, Hiroya; Slane, Patrick O.; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 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. [Badenes, Carles] Univ Pittsburgh, Pittsburgh, PA 15260 USA. [Nakano, Toshio; Hiraga, Junko S.] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Castro, Daniel] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. [Enoto, Teruaki] RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Maeda, Yoshitomo] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Nobukawa, Masayoshi] Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. [Safi-Harb, Samar] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. RP Yamaguchi, H (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM hiroya.yamaguchi@nasa.gov RI XRAY, SUZAKU/A-1808-2009; OI Enoto, Teruaki/0000-0003-1244-3100 NR 51 TC 27 Z9 27 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 20 PY 2014 VL 785 IS 2 AR L27 DI 10.1088/2041-8205/785/2/L27 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE9VR UT WOS:000334359800008 ER PT J AU Ortega, HE Shen, YYC TenDyke, K Rios, N Cubilla-Rios, L AF Ortega, Humberto. E. Shen, Young Yongchun TenDyke, Karen Rios, Nivia Cubilla-Rios, Luis TI Polyhydroxylated macrolide isolated from the endophytic fungus Pestalotiopsis mangiferae SO TETRAHEDRON LETTERS LA English DT Article DE Hyptis dilatata; Pestalotiopsis mangiferae; Polyhydroxylated macrolide; Listeria monocytogenes; Bacillus cereus; Antibacterial activity ID PENICILLIUM-SP; EPIDEMIOLOGY; PATHOGENESIS; METABOLITES; LACTONE; XYOLIDE; ORIGIN AB A new polyhydroxylated macrolide, named mangiferaelactone (1) was isolated from a solid culture of the endophytic fungus Pestalotiopsis manguiferae, together with ten known compounds [(65,1'S)-LL-P880 alpha; (6S,1'S,2'R)-LL-P880 beta; (1'S,2'R)-LL-880 gamma; (1'R)-dehydropestalotin; (-)-5-carboxylmellein; (-)-5-methylmellein: (-)-5-hydroxylmethylmellein; arabenoic acid; 5,6-dihydro-4-methoxy-2H-pyran-2-one; and the (-)-2-hexylidene-3-methylsuccinic acid]. P. manguiferae was isolated from Hyptis dilatata, a small shrub common in the central region of Panama. The structure of compound 1 was elucidated by a combination of spectroscopic methods (IR. MS, optical rotation. 1D and 2D NMR spectroscopy). The absolute configuration of 1 was established as 4R,7R.8R.9S by application of vibrational circular dichroism (VCD). Compound 1 showed a minimum inhibitory concentration (MIC) of 1.6863 mg/mL against Listeria monocytogenes, and 0.5529 mg/mL against Bacillus cereus. No activity was observed for compound 1 against Plasmodium falciparum or Trypanosoma cruzi; likewise, no cytotoxic activity was observed against A2058 and H522-T1 cells. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Ortega, Humberto. E.; Cubilla-Rios, Luis] Univ Panama, Fac Nat Exact Sci & Technol, Lab Trop Bioorgan Chem, Panama City, Panama. [Ortega, Humberto. E.; Cubilla-Rios, Luis] Smithsonian Trop Res Inst, Panama City, Panama. [Shen, Young Yongchun; TenDyke, Karen] Eisai Inc, Andover, MA 01810 USA. [Rios, Nivia] Univ Panama, Dept Microbiol, Panama City, Panama. 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 SENACYT Grant [COL10-060] FX This work was supported by SENACYT Grant (COL10-060). We express our thanks to Dr. C. Spadafora for conducting the P. falciparum and T. cruzi bioassays, and to the personnel of Panama's Autoridad Nacional del Ambiente for facilitating this research. NR 22 TC 7 Z9 8 U1 1 U2 22 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0040-4039 J9 TETRAHEDRON LETT JI Tetrahedron Lett. PD APR 16 PY 2014 VL 55 IS 16 BP 2642 EP 2645 DI 10.1016/j.tetlet.2014.03.012 PG 4 WC Chemistry, Organic SC Chemistry GA AW1JC UT WOS:000346044800014 ER PT J AU Harasewych, MG AF Harasewych, M. G. TI On the authorship and primary type of Cerion incanum (Gastropoda: Cerionidae) SO NAUTILUS LA English DT Article DE Pupa incana; authorship; neotype; Florida Keys ID FLORIDA AB Although the author of the species Ceylon incanum (originally proposed as Pupa incana) has been cited as Binney, 1851, a review of his multiple uses of the name do not satisfy the criteria of availability set forth by the International Code of Zoological Nomenclature (Article 12), until the publication of illustrations of three shells labelled Pupa incana in 1857. In a separately authored paper published as part of Binney's multi-volume work on the Terrestrial Mollusks of the United States, Leidy published detailed descriptions and illustrations of several organ systems of Pupa incana in 1851. Thus, the authorship of Pupa incana must be attributed to Leidy, 1851, rather than to Binney. As Leidy did not retain the dissected tissues, there is no surviving type material for Pupa incana Leidy. A neotype is designated for Pupa incana Leidy, 1851, from the subsequently designated type locality in order to provide an objective standard of reference for this species-group taxon that may be used to evaluate the relationship of the nominotypical subspecies to three subsequently described subspecies, as well as to two introduced Bahamian species with which it is documented to have hybridized. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012, Washington, DC 20013 USA. EM Harasewych@si.edu NR 20 TC 2 Z9 2 U1 0 U2 2 PU BAILEY-MATTHEWS SHELL MUSEUM PI SANIBEL PA C/O DR JOSE H LEAL, ASSOCIATE/MANAGING EDITOR, 3075 SANIBEL-CAPTIVA RD, SANIBEL, FL 33957 USA SN 0028-1344 J9 NAUTILUS JI Nautilus PD APR 16 PY 2014 VL 128 IS 1 BP 18 EP 21 PG 4 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA AQ9PU UT WOS:000343188600003 ER PT J AU Rebollar, EA Hughey, MC Harris, RN Domangue, RJ Medina, D Ibanez, R Belden, LK AF Rebollar, Eria A. Hughey, Myra C. Harris, Reid N. Domangue, Rickie J. Medina, Daniel Ibanez, Roberto Belden, Lisa K. TI The Lethal Fungus Batrachochytrium dendrobatidis Is Present in Lowland Tropical Forests of Far Eastern Panama SO PLOS ONE LA English DT Article ID POPULATION DECLINES; CHYTRID FUNGUS; AFFECTS PREVALENCE; COSTA-RICA; NEW-WORLD; CHYTRIDIOMYCOSIS; AMPHIBIANS; FROGS; INFECTION; CONSERVATION AB The fungal disease chytridiomycosis, caused by Batrachochytrium dendrobatidis (Bd), is one of the main causes of amphibian population declines and extinctions all over the world. In the Neotropics, this fungal disease has caused catastrophic declines in the highlands as it has spread throughout Central America down to Panama. In this study, we determined the prevalence and intensity of Bd infection in three species of frogs in one highland and four lowland tropical forests, including two lowland regions in eastern Panama in which the pathogen had not been detected previously. Bd was present in all the sites sampled with a prevalence ranging from 15-34%, similar to other Neotropical lowland sites. The intensity of Bd infection on individual frogs was low, ranging from average values of 0.11-24 zoospore equivalents per site. Our work indicates that Bd is present in anuran communities in lowland Panama, including the Darien province, and that the intensity of the infection may vary among species from different habitats and with different life histories. The population-level consequences of Bd infection in amphibian communities from the lowlands remain to be determined. Detailed studies of amphibian species from the lowlands will be essential to determine the reason why these species are persisting despite the presence of the pathogen. C1 [Rebollar, Eria A.; Harris, Reid N.] James Madison Univ, Dept Biol, Harrisonburg, VA 22807 USA. [Hughey, Myra C.; Medina, Daniel; Belden, Lisa K.] Virginia Tech, Dept Biol Sci, Blacksburg, VA USA. [Domangue, Rickie J.] James Madison Univ, Dept Math & Stat, Harrisonburg, VA 22807 USA. [Ibanez, Roberto] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Rebollar, EA (reprint author), James Madison Univ, Dept Biol, Harrisonburg, VA 22807 USA. EM ea.rebollar@gmail.com RI Rebollar, Eria/B-2044-2015 FU National Science Foundation [DEB-1136640, DEB-1136602] FX The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. This project was funded by the National Science Foundation Dimensions of Biodiversity program, under grants DEB-1136640 to Lisa K. Belden and DEB-1136602 to Reid N. Harris (http://www.nsf.gov/). NR 50 TC 10 Z9 11 U1 3 U2 28 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 16 PY 2014 VL 9 IS 4 AR e95484 DI 10.1371/journal.pone.0095484 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AI4VW UT WOS:000336863900149 PM 24740162 ER PT J AU McCormick, BT Herzog, M Yang, J Edmonds, M Mather, TA Carn, SA Hidalgo, S Langmann, B AF McCormick, Brendan T. Herzog, Michael Yang, Jian Edmonds, Marie Mather, Tamsin A. Carn, Simon A. Hidalgo, Silvana Langmann, Baerbel TI A comparison of satellite- and ground-based measurements of SO2 emissions from Tungurahua volcano, Ecuador SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OZONE MONITORING INSTRUMENT; SULFUR-DIOXIDE EMISSIONS; SOUFRIERE-HILLS VOLCANO; AIR-QUALITY; PLUME; FLUX; CLIMATE; TRANSPORT; NICARAGUA; DEPLETION C1 [McCormick, Brendan T.] Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [McCormick, Brendan T.; Edmonds, Marie] Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England. [Herzog, Michael; Yang, Jian] Univ Cambridge, Dept Geog, Cambridge CB2 3EN, England. [Mather, Tamsin A.] Univ Oxford, Dept Earth Sci, Oxford OX1 3PR, England. [Carn, Simon A.] Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA. [Hidalgo, Silvana] Escuela Politec Nacl, Inst Geofis, Quito, Ecuador. [Langmann, Baerbel] Univ Hamburg, Inst Geophys, Hamburg, Germany. RP McCormick, BT (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM mccormickb@si.edu RI Mather, Tamsin/A-7604-2011 OI Mather, Tamsin/0000-0003-4259-7303 FU National Centre for Earth Observation; UK's Natural Environment Research Council; NERC NCEO Dynamic Earth and Geohazards group; NASA [NNX09AJ40G, NNX10AG60G, NNX11AF42G]; Isaac Newton Trust at the University of Cambridge FX B.T.M. acknowledges funding from the National Centre for Earth Observation, part of the UK's Natural Environment Research Council, and latterly the Deep Carbon Observatory and the Smithsonian Institution. B. T. M., M. E., and T. A. M. are supported by and contribute to the NERC NCEO Dynamic Earth and Geohazards group. S. A. C. acknowledges funding from NASA through grants NNX09AJ40G (Aura Validation), NNX10AG60G (Atmospheric Chemistry Modeling and Analysis Program), and NNX11AF42G (Aura Science Team). J.Y. was funded by the Isaac Newton Trust at the University of Cambridge for the duration of this project. The authors thank Anja Schmidt and two anonymous reviewers for their thorough and constructive comments. We acknowledge the Goddard Earth Sciences Data and Information Services Center for making OMI SO2 data publicly available. NR 79 TC 10 Z9 10 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 16 PY 2014 VL 119 IS 7 BP 4264 EP 4285 DI 10.1002/2013JD019771 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AF7PZ UT WOS:000334908300036 ER PT J AU Pawlak, M Moiseyev, N Sadeghpour, HR AF Pawlak, M. Moiseyev, N. Sadeghpour, H. R. TI Highly excited Rydberg states of a rubidium atom: Theory versus experiments SO PHYSICAL REVIEW A LA English DT Article ID ALKALI-METAL; MOLECULES AB There has been increasing interest in the energy spectrum of highly excited Rydberg states. The energy spectra of the s, p, and d highly excited Rydberg states of a rubidium atom have been measured by different groups. However, there is a discrepancy between the reported data concerning the energy levels of highly excited s and d states of Rb. We address this issue by performing accurate calculations of Rb(ns, np, nd) energy levels using the parametric one-electron valence potential [Marinescu, Sadeghpour, and Dalgarno, Phys. Rev. A 49, 982 (1994)] with spin-orbit coupling. We compare results with reference data from the National Institute of Standards and Technology and from available experiments. This enables us to recommend energy levels of highly excited Rydberg states of Rb that can be used as reference values. C1 [Pawlak, M.; Moiseyev, N.] Technion Israel Inst Technol, Schulich Fac Chem, IL-32000 Haifa, Israel. [Pawlak, M.] Nicholas Copernicus Univ, Fac Chem, PL-87100 Torun, Poland. [Moiseyev, N.] Technion Israel Inst Technol, Fac Phys, IL-32000 Haifa, Israel. [Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Pawlak, M (reprint author), Technion Israel Inst Technol, Schulich Fac Chem, IL-32000 Haifa, Israel. EM teomar@chem.umk.pl RI Pawlak, Mariusz/F-3073-2014 OI Pawlak, Mariusz/0000-0002-2200-8287 FU "Mobility Plus" program - Polish Ministry of Science and Higher Education; ISF [298/11]; NSF FX M.P. acknowledges support by the "Mobility Plus" program financed by the Polish Ministry of Science and Higher Education. N.M. acknowledges ISF Grant No. 298/11 for partial support. Support from the NSF for ITAMP is acknowledged. NR 39 TC 4 Z9 4 U1 3 U2 19 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD APR 16 PY 2014 VL 89 IS 4 AR 042506 DI 10.1103/PhysRevA.89.042506 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AH0CS UT WOS:000335787300005 ER PT J AU Kessler, EM Lovchinsky, I Sushkov, AO Lukin, MD AF Kessler, E. M. Lovchinsky, I. Sushkov, A. O. Lukin, M. D. TI Quantum Error Correction for Metrology SO PHYSICAL REVIEW LETTERS LA English DT Article ID NUCLEAR-MAGNETIC-RESONANCE; BRAIN ACTIVITY MAP; ENHANCED METROLOGY; DIAMOND; SPIN; CIRCUITS; SYSTEMS; MEMORY; LIMIT AB We propose and analyze a new approach based on quantum error correction (QEC) to improve quantum metrology in the presence of noise. We identify the conditions under which QEC allows one to improve the signal-to-noise ratio in quantum-limited measurements, and we demonstrate that it enables, in certain situations, Heisenberg-limited sensitivity. We discuss specific applications to nanoscale sensing using nitrogen-vacancy centers in diamond in which QEC can significantly improve the measurement sensitivity and bandwidth under realistic experimental conditions. C1 [Kessler, E. M.; Lovchinsky, I.; Sushkov, A. O.; Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Kessler, E. M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Sushkov, A. O.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. RP Kessler, EM (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Kessler, Eric Matthias/E-6981-2012 OI Kessler, Eric Matthias/0000-0001-9959-538X FU NSF; CUA; HQOC; ITAMP; Defense Advanced Research Projects Agency (QuASAR Program); NDSEG FX We thank Alex Retzker, Janek Kolodynski, and Luis Davidovich for enlightening discussions. This work was supported by NSF, CUA, HQOC, ITAMP, the Defense Advanced Research Projects Agency (QuASAR Program), and NDSEG (IL). NR 35 TC 53 Z9 53 U1 0 U2 35 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 16 PY 2014 VL 112 IS 15 AR 150802 DI 10.1103/PhysRevLett.112.150802 PG 5 WC Physics, Multidisciplinary SC Physics GA AH0NH UT WOS:000335816200005 PM 24785020 ER PT J AU Ngatia, LW Reddy, KR Nair, PKR Pringle, RM Palmer, TM Turner, BL AF Ngatia, Lucy W. Reddy, K. Ramesh Nair, P. K. Ramachandran Pringle, Robert M. Palmer, Todd M. Turner, Benjamin L. TI Seasonal patterns in decomposition and nutrient release from East African savanna grasses grown under contrasting nutrient conditions SO AGRICULTURE ECOSYSTEMS & ENVIRONMENT LA English DT Article DE Aboveground biomass; East Africa; Nutrient cycling; N release; P release; Savanna ID PLANT LITTER DECOMPOSITION; LEAF-LITTER; NITROGEN-MINERALIZATION; CHEMICAL-COMPOSITION; SEMIARID ECOSYSTEM; N MINERALIZATION; LIGNIN CONTROL; DYNAMICS; FORESTS; KENYA AB Litter decomposition and nutrient release is one of the key biogeochemical processes that regulate plant productivity and nutrient cycling in African savanna ecosystems. We examined the influence of nitrogen and phosphorus additions on grass decomposition and nutrient release rates in an Acacia savanna ecosystem in central Kenya. Grass was clipped from a factorial nitrogen x phosphorus experiment and decomposed in a common plot that had not received fertilizer. After 20 weeks, including one dry season and one wet season, 50-65% of carbon, 68-75% of nitrogen and 73-83% of phosphorus had been released from the litter. Decomposition was slow in the dry season (mass loss 1-2% wk(-1)) compared to the wet season (7-11% wk(-1)). Wet season decomposition was more rapid for grasses that had been fertilized with nitrogen, even though tissue nitrogen was not significantly different from the control grass, indicating that factors other than litter nitrogen concentration influenced decomposition rates under nitrogen enrichment. Surprisingly, nutrient loss from decomposing litter was relatively high during the dry season, suggesting a role for dew in leaching nutrients from dry litter. We conclude that seasonal rain and nitrogen addition (but not phosphorus addition) accelerate decomposition of grass litter, but that nutrient leaching during the dry season can be considerable. (C) 2014 Elsevier B.V. All rights reserved. C1 [Ngatia, Lucy W.; Reddy, K. Ramesh; Nair, P. K. Ramachandran] Univ Florida, Dept Soil & Water Sci, Gainesville, FL 32611 USA. [Ngatia, Lucy W.; Pringle, Robert M.; Palmer, Todd M.] Mpala Res Ctr, Nanyuki, Kenya. [Nair, P. K. Ramachandran] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA. [Pringle, Robert M.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Palmer, Todd M.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Reddy, KR (reprint author), POB 110290,2181 McCarty Hall A, Gainesville, FL 32611 USA. EM krr@ufl.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU University of Florida; Swiss National Centre of Competence in Research (NCCR); Smithsonian Tropical Research Institute - Levinson Fellowship FX Funding for the research was provided by the University of Florida, the Swiss National Centre of Competence in Research (NCCR) and a Smithsonian Tropical Research Institute - Levinson Fellowship. We thank Elkanah Korir for field assistance, the Mpala Research Centre for logistical support, CETRAD and the University of Nairobi for providing access to laboratories, James Colee for statistical support, the Wetland Biogeochemistry Laboratory for analytical support, and the Office of the President in Kenya for allowing us to conduct this research in Kenya. Jacob R. Goheen provided helpful comments on the paper. NR 60 TC 2 Z9 2 U1 1 U2 33 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-8809 EI 1873-2305 J9 AGR ECOSYST ENVIRON JI Agric. Ecosyst. Environ. PD APR 15 PY 2014 VL 188 BP 12 EP 19 DI 10.1016/j.agee.2014.02.004 PG 8 WC Agriculture, Multidisciplinary; Ecology; Environmental Sciences SC Agriculture; Environmental Sciences & Ecology GA AI2PI UT WOS:000336700100002 ER PT J AU Pyenson, ND Kelley, NP Parham, JF AF Pyenson, Nicholas D. Kelley, Neil P. Parham, James F. TI Marine tetrapod macroevolution: Physical and biological drivers on 250 Ma of invasions and evolution in ocean ecosystems SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Special issue; Evolutionary drivers ID CETACEANS CENOZOIC DRIVERS; FOSSIL CALIBRATIONS; STRANDING RECORD; RIVER DOLPHINS; TOOTHED WHALES; RORQUAL WHALES; NORTH PACIFIC; MIDDLE EOCENE; DIVERSITY; RADIATION AB The dominant consumers in today's ocean ecosystems are marine mammals, including cetaceans, sirenians, and pinnipeds, and other marine carnivorans. The ecological dominance of marine mammals can be traced back to at least seven independent transitions during the Cenozoic, when different lineages of terrestrial mammals underwent land to sea evolutionary transformations. However, the evolution of marine mammals represents only the most recent set of marine invasions by tetrapods over the past 250 Ma. During the Mesozoic, over a dozen different reptile lineages (e.g., mosasaurs, ichthyosaurs, turtles, snakes) evolved obligate marine lineages, including a few lineages that persist to today, such as sea turtles. Birds, which are phylogenetically nested among diapsid reptiles, have also repeatedly adapted to marine life since the Cretaceous. Attempts to understand the common patterns of marine tetrapod evolution, and the processes that have shaped them, have largely been limited to individual groups. Placed in a broad comparative view from the Mesozoic to the Cenozoic eras, the macroevolution of marine tetrapods reveals evolutionary drivers at different scales, along with morphological parallels, unique evolutionary innovations, and the strong influence of historical constraints. Major physical, environmental drivers appear to be responsible for some patterns in marine tetrapod evolution at some temporal and geographic scales, but these drivers are not unique causes, as biological drivers (e.g., escalation) likely also play a role. The culmination of this trophic ascendancy has been dramatically altered by human hunting (especially of marine mammals), underscoring the need for historical datasets that extend into deep time to understand the ecological history of marine tetrapods. Published by Elsevier B.V. C1 [Pyenson, Nicholas D.; Kelley, Neil P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Pyenson, Nicholas D.] Burke Museum Nat Hist & Culture, Dept Mammal, Seattle, WA 98195 USA. [Pyenson, Nicholas D.] Burke Museum Nat Hist & Culture, Dept Paleontol, Seattle, WA 98195 USA. [Kelley, Neil P.] Vanderbilt Univ, Dept Earth & Environm Sci, Nashville, TN 37240 USA. [Parham, James F.] Calif State Univ Fullerton, Dept Geol Sci, John D Cooper Archaeol & Paleontol Ctr, Fullerton, CA 92834 USA. RP Pyenson, ND (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA. EM pyensonn@si.edu FU Biodiversity Synthesis Center at the Field Museum of Natural History, in Chicago; Smithsonian Institution; Remington Kellogg Fund; Peter S. Buck Postdoctoral Fellowship at the Smithsonian's National Museum of Natural History FX This particular research collaboration started as an Encyclopedia of Life synthesis meeting in 2009 on the evolution and diversity of marine tetrapods, funded by the Biodiversity Synthesis Center at the Field Museum of Natural History, in Chicago. This meeting lead to a symposium on the "Physical Drivers of Marine Tetrapod Evolution," convened at the 2010 Annual Meeting of the Society of Vertebrate Paleontology in Pittsburgh. We thank all of the participants at both the EOL BioSynC meeting and SVP symposium for their contributions and patience. This manuscript was written with support from the Smithsonian Institution and its Remington Kellogg Fund to NDP. NPK was supported by a Peter S. Buck Postdoctoral Fellowship at the Smithsonian's National Museum of Natural History. This is Paleobiology Database publication no. 198. NR 124 TC 17 Z9 17 U1 5 U2 82 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 2014 VL 400 SI SI BP 1 EP 8 DI 10.1016/j.palaeo.2014.02.018 PG 8 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA AG0OF UT WOS:000335114100001 ER PT J AU Velez-Juarbe, J AF Velez-Juarbe, Jorge TI Ghost of seagrasses past: Using sirenians as a proxy for historical distribution of seagrasses SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Sirenia; Seagrasses; Physical drivers; Evolution; Paleobiogeography ID STABLE-ISOTOPE ANALYSIS; EASTERN PACIFIC-OCEAN; CARIBBEAN REGION; FOSSIL SIRENIA; WEST ATLANTIC; LATE MIOCENE; ENVIRONMENTAL-CHANGE; MANATEES TRICHECHUS; ECOLOGICAL CHANGE; MIDDLE EOCENE AB Seagrasses are a notable component of shallow marine habitats, especially in tropical and subtropical regions. Their fossil record extends back to the Mesozoic, but it is relatively poor and fragmentary, with large temporal and geographical gaps. As a result, very little is known about the paleobiogeography of these plants and how physical drivers, such as climatic or oceanic events, have affected their distribution. One approach is to infer the past distribution of seagrasses using fossils of organisms dependent of seagrasses with more complete records as proxies. Seagrass consumers, such as sirenians (seacows, manatees and dugongs), are much better represented in the fossil record than seagrasses are. The characteristically dense bones of sirenians together with the fact that they are usually found in marginal marine environments increases the potential for preservation and recognition of their fossils. The long evolutionary history of sirenians, extending throughout most of the last 50 Ma, together with their diet permits the use of their fossils as a proxy for inferring the paleobiogeography of seagrasses. Here I looked at the fossil record of sirenians and seagrasses from the Eocene, through the Miocene epochs. This comparison produced several inferences about seagrass paleobiogeography and how physical drivers, such as climate change, ocean currents and tectonic events, have been influential in their distribution: 1) seagrasses were well-established in the Western Atlantic-Caribbean prior to the middle Eocene, making possible at least two instances of trans-Atlantic sirenian dispersal events, either with the aid of Tethyan currents or along the nearly continuous Northern Atlantic coastline that was present in the Eocene; 2) climatic cooling during the early Oligocene seemed to have limited the extent of seagrasses and sirenians, although these groups recovered and further diversified and expanded their distributions by the late Oligocene in tandem with a climatic warming event; 3) by the Miocene, seagrasses and sirenians reached the southern Western Atlantic and the Eastern Pacific aided by the presence of the Central American Seaway, achieving a distribution similar to, and sometimes, surpassing that of today. The fossil record of sirenians can provide a broad overview of seagrass paleobiogeography through time. However, several aspects, such as when sirenians and seagrasses arrived to Australia and the seemingly late arrival of seagrasses to South America and the Eastern Pacific, still need further investigation. (C) 2013 Elsevier B.V. All rights reserved. C1 [Velez-Juarbe, Jorge] Howard Univ, Dept Anat, Lab Evolutionary Biol, Washington, DC 20059 USA. [Velez-Juarbe, Jorge] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Velez-Juarbe, J (reprint author), Univ Florida, Florida Museum Nat Hist, 1659 Museum Rd,POB 117800, Gainesville, FL 32611 USA. EM velezjuarbe@gmail.com FU WBHR-LSAMP Bridge to the Doctorate Program at Howard University; National Museum of Natural History; Smithsonian Institution; NSF EAR [0929117] FX D. P. Domning and I. Koretsky are gratefully acknowledged for comments on an earlier version of this manuscript. I wish to thank the editors N. D. Pyenson, N. Kelley and J. F. Parham for their comments and patience. This manuscript benefited greatly from comments and corrections from an anonymous reviewer and B. L Beatty. Lastly, many thanks to my wife T. Pineda-Enriquez for her patience and comments on the affinities of UPRMP 2767 and insight regarding ophiuroid habitats. Financial support has been provided in part by the WBHR-LSAMP Bridge to the Doctorate Program at Howard University, a predoctoral fellowship at the National Museum of Natural History, Smithsonian Institution and by NSF EAR grant no. 0929117 to D. P. Domning. NR 104 TC 16 Z9 16 U1 3 U2 55 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 2014 VL 400 SI SI BP 41 EP 49 DI 10.1016/j.palaeo.2013.05.012 PG 9 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA AG0OF UT WOS:000335114100005 ER PT J AU Gutstein, CS Figueroa-Bravo, CP Pyenson, ND Yury-Yanez, RE Cozzuol, MA Canals, M AF Gutstein, Carolina S. Figueroa-Bravo, Constanza P. Pyenson, Nicholas D. Yury-Yanez, Roberto E. Cozzuol, Mario A. Canals, Mauricio TI High frequency echolocation, ear morphology, and the marine-freshwater transition: A comparative study of extant and extinct toothed whales SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE River dolphins; Odontoceti; Periotic; Ecomorphology; Evolution; Neogene ID TUCUXI SOTALIA-FLUVIATILIS; CETACEAN STRANDING RECORD; BOTOS INIA-GEOFFRENSIS; RIVER DOLPHINS; TURSIOPS-TRUNCATUS; SOUTHERN ARGENTINA; PHOCOENA-PHOCOENA; CYTOCHROME-B; MIOCENE; EVOLUTION AB This study compares the bony ear morphology of freshwater and marine odontocetes (toothed whales). Odontocetes are unique among marine mammals in two important respects: I) they use echolocation; 2) at least three lineages have independently evolved obligate freshwater habits from marine ancestries. Freshwater odontocetes include the so-called "river dolphins," a paraphyletic group that each evolved convergent external morphological characters that distinguish them from oceanic dolphins (Delphinoidea). In addition to their convergent external morphology, "river dolphins" all have echolocation that use one peak (narrow-band) frequency around 100 kHz, compared to oceanic delphinoids which use a two peak (bimodal) frequency ranging from 40 to 140 kHz. The differences in echolocation suggest that the sensory systems responsible for detecting these different sound frequencies should also differ, although quantitative assessments of the cetacean hearing system remain understudied and taxonomically undersampled. To test if ear bone morphology reflects underlying environmentally driven differences in echolocation ability, we assembled a dataset of odontocete periotics (n = 114) from extant and fossil species. We examined 18 external and three internal linear periotic measurements, the latter of which were examined using cone-beam scanning tomography. Results from multivariate canonical ordination analyses show that periotic height, periotic thickness and pars cochlearis width collectively explain the largest amount of interspecific variation in our dataset Because these particular ear bone measurements correspond to acoustic hearing ranges, we propose that they are also proxies for environmental preference (i.e., marine, freshwater and intermediate habitats) and may be useful for deciphering environmental preferences of extinct odontocetes. (c) 2014 Elsevier B.V. All rights reserved. C1 [Gutstein, Carolina S.; Canals, Mauricio] Univ Chile, Fac Ciencias, Dept Ecol, Lab Ecofisiol, Santiago, Chile. [Gutstein, Carolina S.; Figueroa-Bravo, Constanza P.] Univ Chile, Dept Biol, Fac Ciencias, Lab Ontogenia & Filogenia,Red Paleontol U Chile, Santiago, Chile. [Gutstein, Carolina S.; Pyenson, Nicholas D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Pyenson, Nicholas D.] Burke Museum Nat & Culture, Dept Mammal, Seattle, WA 98195 USA. [Pyenson, Nicholas D.] Burke Museum Nat & Culture, Dept Paleontol, Seattle, WA 98195 USA. [Yury-Yanez, Roberto E.] Univ Chile, Fac Ciencias, Lab Zool Vertebrados, Santiago, Chile. [Cozzuol, Mario A.] Univ Fed Minas Gerais, Inst Ciencias Biol, Dept Zool, BR-31270910 Belo Horizonte, MG, Brazil. RP Gutstein, CS (reprint author), Univ Chile, Fac Ciencias, Dept Ecol, Lab Ecofisiol, Las Palmeras 3425, Santiago, Chile. EM sgcarolina@gmail.com; fbconstanza@gmail.com; pyensonn@si.edu; robyury@ug.uchile.cl; cozzuol@icb.ufmg.br; mcanals@uchile.cl RI Cozzuol, Mario/H-8302-2012; OI Cozzuol, Mario/0000-0003-3645-0401; Gutstein, Carolina/0000-0002-0823-2434 FU CONICYT; Becas Chile; Departamento de Postgrado y Postitulo of the Vicerrectoria de Asuntos Academicos of Universidad de Chile; Smithsonian Institution's Remington Kellogg Fund; NMNH Small Grant Award; National Geographic Society Committee on Research Exploration grant [8903-11]; master's degree CONICYT-Chile scholarship from the Programa de Formacion de Capital Humano Avanzado FX We thank two anonymous reviewers and special issue guest editors Neil P. Kelley and James F. Parham for insightful and thorough comments that greatly improved the quality of this manuscript. This paper represents part of a Ph.D. dissertation (CSG) completed at Facultad de Ciencias, Universidad de Chile. This work would not be possible without assistance from collection managers and curators of many collections in different countries: from Chile, David Rubilar-Rogers from MNHN in Santiago; from Brazil, Miriam Marmontel at Instituto Mamiraua in Tefe, Paulo C. Simoes-Lopes at UFSC in Florianopolis, and Danilo Saraiva at Museo de Ciencias Naturais (Pontificia Universidade Catolica) in Belo Horizonte; from Argentina, Alejandro Kramarz at MACN in Buenos Aires and Marcelo Reguero at MLP in La Plata; from France, Christine Argot from MNHN in Paris; from the United Kingdom, Richard Sabin at the Natural History Museum, London; from the U.S.A., David Bohaska (Paleobiology) and Charles Potter (Vertebrate Zoology) at the Smithsonian Institution's NMNH, in Washington D.C., and Stephen Godfrey at the Calvert Marine Museum, in Maryland. We wish to thank Rodrigo Passoni (Cefalo-X, Florianopolis, Brazil) for the permission and care to perform the cone-beam tomography at his clinic. We also thank David Rubilar-Rogers who read and improved prior versions of this manuscript and Paulo Simoes-Lopes and Jorge Velez-Juarbe for helpful discussions about periotic morphology. We also thank the conveners of the "Physical Drivers and Marine Tetrapod Evolution" symposium at the 2010 Society of Vertebrate Paleontology annual meeting. C.S.G was funded by CONICYT, Becas Chile, Departamento de Postgrado y Postitulo of the Vicerrectoria de Asuntos Academicos of Universidad de Chile and the Smithsonian Institution's Remington Kellogg Fund. This manuscript was also written with support from a NMNH Small Grant Award, the Smithsonian Institution's Remington Kellogg Fund and a National Geographic Society Committee on Research Exploration grant (8903-11) to N.D.P. RE.Y.-Y. was funded by a master's degree CONICYT-Chile scholarship from the Programa de Formacion de Capital Humano Avanzado. This paper is Caldera Paleontology Project contribution No. 2. NR 102 TC 6 Z9 6 U1 16 U2 92 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 2014 VL 400 SI SI BP 62 EP 74 DI 10.1016/j.palaeo.2014.01.026 PG 13 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA AG0OF UT WOS:000335114100007 ER PT J AU Cavanaugh, KC Kellner, JR Forde, AJ Gruner, DS Parker, JD Rodriguez, W Feller, IC AF Cavanaugh, Kyle C. Kellner, James R. Forde, Alexander J. Gruner, Daniel S. Parker, John D. Rodriguez, Wilfrid Feller, Ilka C. TI Reply to Giri and Long: Freeze-mediated expansion of mangroves does not depend on whether expansion is emergence or reemergence SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 [Cavanaugh, Kyle C.; Parker, John D.; Rodriguez, Wilfrid; Feller, Ilka C.] Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA. [Cavanaugh, Kyle C.; Kellner, James R.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Forde, Alexander J.] Univ Maryland, Grad Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA. [Gruner, Daniel S.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. RP Cavanaugh, KC (reprint author), Smithsonian Environm Res Ctr, Smithsonian Inst, POB 28, Edgewater, MD 21037 USA. EM cavanaughk@si.edu RI Gruner, Daniel/A-5166-2010; Parker, John/F-9761-2010; OI Gruner, Daniel/0000-0002-3153-4297; Parker, John/0000-0002-3632-7625; Feller, Ilka/0000-0002-6391-1608 NR 5 TC 1 Z9 1 U1 2 U2 8 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 15 PY 2014 VL 111 IS 15 BP E1449 EP E1449 DI 10.1073/pnas.1401809111 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AE8YI UT WOS:000334288600002 PM 24851264 ER PT J AU Archer, GJ Ash, RD Bullock, ES Walker, RJ AF Archer, G. J. Ash, R. D. Bullock, E. S. Walker, R. J. TI Highly siderophile elements and Re-187-Os-187 isotopic systematics of the Allende meteorite: Evidence for primary nebular processes and late-stage alteration SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID EARLY SOLAR-SYSTEM; ALUMINUM-RICH INCLUSIONS; RARE-EARTH ELEMENTS; CARBONACEOUS CHONDRITES; TRACE-ELEMENTS; PLATINUM-GROUP; REFRACTORY INCLUSIONS; MASS-SPECTROMETRY; OSMIUM; CHONDRULES AB The abundances of highly siderophile elements (HSE) Re, Os, Ir, Ru, Pt, and Pd, as well as Re-187-Os-187 isotopic systematics were determined for calcium-aluminum-rich inclusions (CAIs), chondrules, and matrix, separated from the CV3 carbonaceous chondrite Allende. Consistent with prior studies, CAIs are characterized by significant depletions in Pd relative to the other HSE, while the other HSE are in generally bulk chondritic relative abundances. The depletions in Pd can be linked with initial formation of CAIs via condensation, or subsequent processing by evaporative processes. Chondrules generally have relative HSE patterns similar to CAIs, although they have lower absolute abundances. Palladium depletions in chondrules may reflect solid metal-liquid metal fractionation at the time of formation, or alternatively, be the result of processes that acted on precursor materials. Matrix samples have nearly chondritic absolute abundances of all HSE measured. Consequently, matrix is the only major chondritic component examined here that shows no relative depletion in Pd. Mass balance suggests the existence of an unidentified Pd-rich carrier, although it is possible that the dataset presented here is too limited to represent typical HSE abundances of some chondritic components (e. g., chondrules). The Re-187-Os-187 isotopic systematics of only six out of twenty-four Allende chondritic components analyzed plot within uncertainties of a 4568 Ma primordial reference isochron. The deviations from the expected isochron most likely reflect late-stage, open-system behavior within the last 2 billion years, and, in some cases, could even have resulted from terrestrial alteration. The open-system behavior is most readily observed in small, millimeter-size sub-samples of Allende, consistent with Re and/or Os mobility on that scale. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Archer, G. J.; Ash, R. D.; Walker, R. J.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Bullock, E. S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Archer, GJ (reprint author), Univ Maryland, Dept Geol, College Pk, MD 20742 USA. EM garcher@umd.edu RI Walker, Richard/K-6869-2016 OI Walker, Richard/0000-0003-0348-2407 FU NASA [NNX10AG94G] FX Samples for this study were provided by the U.S. National Museum of Natural History (Smithsonian Institution, Washington, DC). Glenn MacPherson is acknowledged for aiding in sample selection and separation, as well as providing insight into CAIs and the Allende chondrite. Thanks go to Igor Puchtel, Jingao Liu, Miriam Sharp, Nick Sharp, Emily Worsham, Katherine Bermingham, James Day, and Mathieu Touboul for their help in the lab. James Farquhar provided valuable comments that improved this manuscript. This work was supported by NASA grant NNX10AG94G. We thank Toni Schulz and an anonymous reviewer for their thorough and constructive reviews. We also thank our associate editor, Christian Koeberl, for his comments. NR 87 TC 9 Z9 9 U1 2 U2 13 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 APR 15 PY 2014 VL 131 BP 402 EP 414 DI 10.1016/j.gca.2013.12.032 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AD5YS UT WOS:000333330100025 ER PT J AU Womack, CC Crabtree, KN McCaslin, L Martinez, O Field, RW Stanton, JF McCarthy, MC AF Womack, Caroline C. Crabtree, Kyle N. McCaslin, Laura Martinez, Oscar, Jr. Field, Robert W. Stanton, John F. McCarthy, Michael C. TI Gas-Phase Structure Determination of Dihydroxycarbene, One of the Smallest Stable Singlet Carbenes SO ANGEWANDTE CHEMIE-INTERNATIONAL EDITION LA English DT Article DE atmospheric chemistry; carbenes; microwave spectroscopy; reactive intermediates; structure elucidation ID CRIEGEE INTERMEDIATE CH2OO; TRANSFORM MICROWAVE SPECTROMETER; HO-C-OH; PHOTOELECTRON-SPECTROSCOPY; ROTATIONAL SPECTRUM; DICARBOXYLIC-ACIDS; CARBON-DIOXIDE; OXALIC-ACID; BASIS-SETS; TRIPLET AB Carbenes are reactive molecules of the form (RC)-C-1..R-2 that play a role in topics ranging from organic synthesis to gas-phase oxidation chemistry. We report the first experimental structure determination of dihydroxycarbene (HOC..OH), one of the smallest stable singlet carbenes, using a combination of microwave rotational spectroscopy and high-level coupled-cluster calculations. The semi-experimental equilibrium structure derived from five isotopic variants of HOC..OH contains two very short CO single bonds (ca. 1.32 angstrom). Detection of HOC..OH in the gas phase firmly establishes that it is stable to isomerization, yet it has been underrepresented in discussions of the CH2O2 chemical system and its atmospherically relevant isomers: formic acid and the Criegee intermediate CH2OO. C1 [Womack, Caroline C.; Field, Robert W.] MIT, Dept Chem, Cambridge, MA 02139 USA. [Crabtree, Kyle N.; Martinez, Oscar, Jr.; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McCaslin, Laura; Stanton, John F.] Univ Texas Austin, Dept Chem & Biochem, Austin, TX 78712 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmccarthy@cfa.harvard.edu RI Womack, Caroline/C-7818-2016; OI McCarthy, Michael/0000-0001-9142-0008 FU NSF [CHE1058063]; Robert A. Welch Foundation of Houston, Texas [F-1283]; US Department of Energy, Office of Basic Energy Sciences [DE-FG02-07ER15884]; Dreyfus Foundation Environmental Postdoctoral Fellowship; Smithsonian Astrophysical Observatory FX The experimental work at the Center for Astrophysics was supported by the NSF (grant number CHE1058063). The theoretical studies were supported by the Robert A. Welch Foundation (grant number F-1283) of Houston, Texas, and the US Department of Energy, Office of Basic Energy Sciences (contract number DE-FG02-07ER15884). C.C.W. acknowledges support from a Dreyfus Foundation Environmental Postdoctoral Fellowship. K.N.C. was supported by a CfA postdoctoral fellowship from the Smithsonian Astrophysical Observatory. We would like to offer our thanks to E. S. Palmer for technical assistance and to J. H. Kroll for helpful discussions. NR 59 TC 6 Z9 6 U1 2 U2 40 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 1433-7851 EI 1521-3773 J9 ANGEW CHEM INT EDIT JI Angew. Chem.-Int. Edit. PD APR 14 PY 2014 VL 53 IS 16 BP 4089 EP 4092 DI 10.1002/anie.201311082 PG 4 WC Chemistry, Multidisciplinary SC Chemistry GA AE6TB UT WOS:000334127800004 PM 24623525 ER PT J AU Kwan, JC Liu, YX Ratnayake, R Hatano, R Kuribara, A Morimoto, C Ohnuma, K Paul, VJ Ye, T Luesch, H AF Kwan, Jason C. Liu, Yanxia Ratnayake, Ranjala Hatano, Ryo Kuribara, Akiko Morimoto, Chiko Ohnuma, Kei Paul, Valerie J. Ye, Tao Luesch, Hendrik TI Grassypeptolides as Natural Inhibitors of Dipeptidyl Peptidase 8 and T-Cell Activation SO CHEMBIOCHEM LA English DT Article DE dipeptidyl peptidases; grassypeptolides; immunochemistry; natural products; protease inhibition ID CYANOBACTERIAL PEPTIDES; ELASTASE INHIBITORS; CYCLIC-PEPTIDES; ACTIVE-SITE; DPP-IV; ISOINDOLINE; SCAFFOLDS; PROTEASES; BINDING; LOOP AB Natural products made by marine cyanobacteria are often highly modified peptides and depsipeptides that have the potential to act as inhibitors for proteases. In the interests of finding new protease inhibition activity and selectivity, grassypeptolide A (1) was screened against a panel of proteases and found to inhibit DPP8 selectively over DPP4. Grassypeptolides were also found to inhibit IL-2 production and proliferation in activated T-cells, consistent with a putative role of DPP8 in the immune system. These effects were also observed in Jurkat cells, and DPP activity in Jurkat cell cytosol was shown to be inhibited by grassypeptolides. In silico docking suggests two possible binding modes of grassypeptolidesat the active site of DPP8 and at one of the entrances to the internal cavity. Collectively these results suggest that grassypeptolides might be useful tool compounds in the study of DPP8 function. C1 [Kwan, Jason C.; Liu, Yanxia; Ratnayake, Ranjala; Luesch, Hendrik] Univ Florida, Coll Pharm, Dept Med Chem, Gainesville, FL 32610 USA. [Liu, Yanxia; Ratnayake, Ranjala; Luesch, Hendrik] Univ Florida, CNPD3, Gainesville, FL 32610 USA. [Hatano, Ryo; Kuribara, Akiko; Morimoto, Chiko; Ohnuma, Kei] Univ Tokyo, Inst Med Sci, Adv Clin Res Ctr, Div Clin Immunol,Minato Ku, Tokyo 1088639, Japan. [Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Ye, Tao] Hong Kong Polytech Univ, Dept Appl Biol & Chem Technol, Kowloon, Hong Kong, Peoples R China. RP Luesch, H (reprint author), Univ Florida, Coll Pharm, Dept Med Chem, 1345 Ctr Dr, Gainesville, FL 32610 USA. EM luesch@cop.ufl.edu RI Kwan, Jason/F-9589-2010 OI Kwan, Jason/0000-0001-9933-1536 FU National Institutes of Health, NIGMS [P41GM086210]; National Institutes of Health, NCI [R01CA172310] FX This research was supported in part by the National Institutes of Health, NIGMS grant P41GM086210 and NCI grant R01CA172310. We wish to thank Christian Rummey for kindly providing the homology model of DPP8. We would also like to thank Nam Dang for helpful discussions. This is contribution 940 from the Smithsonian Marine Station at Fort Pierce. NR 36 TC 7 Z9 7 U1 2 U2 22 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 1439-4227 EI 1439-7633 J9 CHEMBIOCHEM JI ChemBioChem PD APR 14 PY 2014 VL 15 IS 6 BP 799 EP 804 DI 10.1002/cbic.201300762 PG 6 WC Biochemistry & Molecular Biology; Chemistry, Medicinal SC Biochemistry & Molecular Biology; Pharmacology & Pharmacy GA AE4PW UT WOS:000333966100004 PM 24591193 ER PT J AU Bonafede, A Intema, HT Bruggen, M Girardi, M Nonino, M Kantharia, N van Weeren, RJ Rottgering, HJA AF Bonafede, A. Intema, H. T. Brueggen, M. Girardi, M. Nonino, M. Kantharia, N. van Weeren, R. J. Roettgering, H. J. A. TI EVIDENCE FOR PARTICLE RE-ACCELERATION IN THE RADIO RELIC IN THE GALAXY CLUSTER PLCKG287.0+32.9 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; galaxies: clusters: individual (PLCKG287.0+32.9); magnetic fields; methods: observational; shock waves; radiation mechanisms: non-thermal ID ACTIVE GALACTIC NUCLEI; X-RAY LUMINOSITY; SHOCK-WAVES; LOW-FREQUENCY; COSMIC-RAYS; GAMMA-RAY; COSMOLOGICAL SIMULATIONS; DATA REDUCTION; HALOS; ACCELERATION AB Radio relics are diffuse radio sources observed in galaxy clusters, probably produced by shock acceleration during cluster-cluster mergers. Their large size, of the order of 1 Mpc, indicates that the emitting electrons need to be (re) accelerated locally. The usually invoked diffusive shock acceleration models have been challenged by recent observations and theory. We report the discovery of complex radio emission in the Galaxy cluster PLCKG287.0+32.9, which hosts two relics, a radio halo, and several radio filamentary emission. Optical observations suggest that the cluster is elongated, likely along an intergalactic filament, and displays a significant amount of substructure. The peculiar features of this radio relic are that (1) it appears to be connected to the lobes of a radio galaxy and (2) the radio spectrum steepens on either side of the radio relic. We discuss the origins of these features in the context of particle re-acceleration. C1 [Bonafede, A.; Brueggen, M.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Intema, H. T.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Girardi, M.] Univ Trieste, Sez Astron, Dipartimento Fis, I-34143 Trieste, Italy. [Girardi, M.; Nonino, M.] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Kantharia, N.] TIFR, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Roettgering, H. J. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Bonafede, A (reprint author), Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. RI Intema, Huib/D-1438-2012; OI Intema, Huib/0000-0002-5880-2730; Nonino, Mario/0000-0001-6342-9662; van Weeren, Reinout/0000-0002-0587-1660 FU research group FOR [1254]; Deutsche Forschungsgemeinschaft; NASA [PF2-130104, NAS8-03060]; Chandra X-ray Center FX We thank F. Vazza and T. Jones for useful discussions. A.B. and M.B. acknowledge support by the research group FOR 1254, funded by the Deutsche Forschungsgemeinschaft: "Magnetization of interstellar and intergalactic media: the prospects of low-frequency radio observations." The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank the staff of the GMRT who made these observation possible. GMRT is run by the National Center for Astrophysics of the Tata Institute of Fundamental Research. R.J.v.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 research made use of the NASA/IPAC Extragalactic Data Base (NED), which is operated by the JPL, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 62 TC 16 Z9 16 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 1 DI 10.1088/0004-637X/785/1/1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300001 ER PT J AU Cook, BA Williams, PKG Berger, E AF Cook, B. A. Williams, P. K. G. Berger, E. TI TRENDS IN ULTRACOOL DWARF MAGNETISM. II. THE INVERSE CORRELATION BETWEEN X-RAY ACTIVITY AND ROTATION AS EVIDENCE FOR A BIMODAL DYNAMO SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; stars: activity; stars: low-mass; stars: rotation ID LOW-MASS STARS; SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; MAIN-SEQUENCE STARS; H-ALPHA EMISSION; L FIELD DWARFS; ALL-SKY SURVEY; BROWN DWARF; SOLAR NEIGHBORHOOD; RADIO-EMISSION; LARGE-SCALE AB Observations of magnetic activity indicators in solar-type stars exhibit a relationship with rotation with an increase until a "saturation" level and a moderate decrease in activity in the very fastest rotators ("supersaturation"). While X-ray data have suggested that this relationship is strongly violated in ultracool dwarfs (UCDs; spectral type greater than or similar to M7), the limited number of X-ray detections has prevented firm conclusions. In this paper, we analyze the X-ray activity-rotation relation in 38 UCDs. Our sample represents the largest catalog of X-ray active UCDs to date, including seven new and four previously unpublished Chandra observations presented in a companion paper. We identify a substantial number of rapidly rotating UCDs with X-ray activity extending two orders of magnitude below the expected saturation level and measure a "supersaturation"-type anticorrelation between rotation and X-ray activity. The scatter in UCD X-ray activity at a fixed rotation is similar to 3 times larger than that in earlier-type stars. We discuss several mechanisms that have been proposed to explain the data, including centrifugal stripping of the corona, and find them to be inconsistent with the observed trends. Instead, we suggest that an additional parameter correlated with both X-ray activity and rotation is responsible for the observed effects. Building on the results of Zeeman-Doppler imaging of UCD magnetic fields and our companion study of radio/X-ray flux ratios, we argue that this parameter is the magnetic field topology, and that the large scatter in UCD X-ray fluxes reflects the presence of two dynamo modes that produce distinct topologies. C1 [Cook, B. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Williams, P. K. G.; Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cook, BA (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. EM bacook@princeton.edu FU National Science Foundation REU; Department of Defense ASSURE programs under NSF [1262851]; Smithsonian Institution; National Science Foundation [AST-1008361]; National Aeronautics and Space Administration through Chandra Award [GO2-13007A]; National Aeronautics Space Administration [NAS8-03060] FX B.A.C. thanks Jonathan McDowell and Marie Machacek for their advice and comments on drafts of this work. We also thank the anonymous referee for helpful, constructive comments. This work is supported in part by the National Science Foundation REU and Department of Defense ASSURE programs under NSF grant No. 1262851 and by the Smithsonian Institution. E.B. and P.K.G.W. acknowledge support for this work from the National Science Foundation through grant AST-1008361, and from the National Aeronautics and Space Administration through Chandra Award Number GO2-13007A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and NASA's Astrophysics Data System. NR 98 TC 17 Z9 17 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 10 DI 10.1088/0004-637X/785/1/10 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300010 ER PT J AU Lansbury, GB Alexander, DM Del Moro, A Gandhi, P Assef, RJ Stern, D Aird, J Ballantyne, DR Balokovic, M Bauer, FE Boggs, SE Brandt, WN Christensen, FE Craig, WW Elvis, M Grefenstette, BW Hailey, CJ Harrison, FA Hickox, RC Koss, M LaMassa, SM Luo, B Mullaney, JR Teng, SH Urry, CM Zhang, WW AF Lansbury, G. B. Alexander, D. M. Del Moro, A. Gandhi, P. Assef, R. J. Stern, D. Aird, J. Ballantyne, D. R. Balokovic, M. Bauer, F. E. Boggs, S. E. Brandt, W. N. Christensen, F. E. Craig, W. W. Elvis, M. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Hickox, R. C. Koss, M. LaMassa, S. M. Luo, B. Mullaney, J. R. Teng, S. H. Urry, C. M. Zhang, W. W. TI NuSTAR OBSERVATIONS OF HEAVILY OBSCURED QUASARS AT z similar to 0.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; HARD X-RAY; SEYFERT 2 GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; RESOLUTION SPECTRAL TEMPLATES; XMM-NEWTON OBSERVATIONS; COMPTON-THICK QUASARS; MU-M; TYPE-2 QUASARS AB We present NuSTAR hard X-ray observations of three Type 2 quasars at z approximate to 0.4-0.5, optically selected from the Sloan Digital Sky Survey. Although the quasars show evidence for being heavily obscured, Compton-thick systems on the basis of the 2-10 keV to [O III] luminosity ratio and multiwavelength diagnostics, their X-ray absorbing column densities (N-H) are poorly known. In this analysis, (1) we study X-ray emission at > 10 keV, where X-rays from the central black hole are relatively unabsorbed, in order to better constrain N-H. (2) We further characterize the physical properties of the sources through broad-band near-UV to mid-IR spectral energy distribution analyses. One of the quasars is detected with NuSTAR at > 8 keV with a no-source probability of < 0.1%, and its X-ray band ratio suggests near Compton-thick absorption with N-H greater than or similar to 5 Chi 10(23) cm(-2). The other two quasars are undetected, and have low X-ray to mid-IR luminosity ratios in both the low-energy (2-10 keV) and high-energy (10-40 keV) X-ray regimes that are consistent with extreme, Compton-thick absorption (N-H greater than or similar to 10(24) cm(-2)). We find that for quasars at z similar to 0.5, NuSTAR provides a significant improvement compared to lower energy (< 10 keV) Chandra and XMM-Newton observations alone, as higher column densities can now be directly constrained. C1 [Lansbury, G. B.; Alexander, D. M.; Del Moro, A.; Gandhi, P.; Aird, J.; Mullaney, J. R.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Assef, R. J.] Univ Diego Port, Nucl Astron Fac Ingn, Santiago, Chile. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ballantyne, D. R.] Georgia Inst Technol, Ctr Relativist Astrophys, Sch Phys, Atlanta, GA 30332 USA. [Balokovic, M.; Grefenstette, B. W.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Koss, M.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [LaMassa, S. M.; Urry, C. M.] Yale Univ, Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA. [Teng, S. H.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lansbury, GB (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. EM g.b.lansbury@durham.ac.uk RI Boggs, Steven/E-4170-2015; Koss, Michael/B-1585-2015; Brandt, William/N-2844-2015; OI Urry, Meg/0000-0002-0745-9792; Boggs, Steven/0000-0001-9567-4224; Koss, Michael/0000-0002-7998-9581; Brandt, William/0000-0002-0167-2453; Alexander, David/0000-0002-5896-6313 FU Science and Technology Facilities Council (STFC) [ST/K501979/1, ST/I001573/1, ST/J003697/1]; Leverhulme Trust; Gemini-CONICYT [32120009]; NSF AST [1008067]; International Fulbright Science and Technology Award; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024, Anillo ACT1101]; Caltech NuSTAR [44A-1092750]; NASA ADP [NNX10AC99G]; NASA ADAP [NNX12AE38G]; National Science Foundation [1211096]; Swiss National Science Foundation [PP00P2_ 138979/1]; NASA [NNG08FD60C]; National Aeronautics and Space Administration; ASI Science Data Center (ASDC, Italy); California Institute of Technology (USA) FX We acknowledge financial support from the Science and Technology Facilities Council (STFC) grants ST/K501979/1 (G.B.L.), ST/I001573/1 (D.M.A. and A.D.M.) and ST/J003697/1 (P.G.), the Leverhulme Trust (D.M.A. and J.R.M.), Gemini-CONICYT grant 32120009 (R.J.A.), NSF AST award 1008067 (D.R.B.), the International Fulbright Science and Technology Award (M.B.), Basal-CATA PFB-06/2007 (F.E.B.), CONICYT-Chile grant FONDECYT 1101024 (F.E.B.), CONICYT-Chile grant Anillo ACT1101 (F.E.B.), Caltech NuSTAR subcontract 44A-1092750 (W.N.B. and B.L.), NASA ADP grant NNX10AC99G (W.N.B.and B.L.), NASA ADAP award NNX12AE38G (R.C.H.), National Science Foundation grant 1211096 (R.C.H.), and Swiss National Science Foundation grant PP00P2_ 138979/1 (M.K.). We thank the referee for the constructive comments, which helped improve our study. 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). NR 88 TC 28 Z9 28 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 17 DI 10.1088/0004-637X/785/1/17 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300017 ER PT J AU Lanz, L Hayward, CC Zezas, A Smith, HA Ashby, MLN Brassington, N Fazio, GG Hernquist, L AF Lanz, Lauranne Hayward, Christopher C. Zezas, Andreas Smith, Howard A. Ashby, Matthew L. N. Brassington, Nicola Fazio, Giovanni G. Hernquist, Lars TI SIMULATED GALAXY INTERACTIONS AS PROBES OF MERGER SPECTRAL ENERGY DISTRIBUTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies COLFAML; interactions; galaxies COLFAML; star formation; hydrodynamics; methods COLFAML; numerical; methods COLFAML; observational; radiative transfer ID MOVING-MESH COSMOLOGY; SMOOTHED PARTICLE HYDRODYNAMICS; STAR-FORMATION RATES; NEARBY GALAXIES; BLACK-HOLES; SUBMILLIMETER GALAXIES; MAJOR MERGERS; DUST MASS; STARBURSTS; SAMPLE AB We present the first systematic comparison of ultraviolet-millimeter spectral energy distributions (SEDs) of observed and simulated interacting galaxies. Our sample is drawn from the Spitzer Interacting Galaxy Survey and probes a range of galaxy interaction parameters. We use 31 galaxies in 14 systems which have been observed with Herschel, Spitzer, GALEX, and 2MASS. We create a suite of GADGET-3 hydrodynamic simulations of isolated and interacting galaxies with stellar masses comparable to those in our sample of interacting galaxies. Photometry for the simulated systems is then calculated with the sunrise radiative transfer code for comparison with the observed systems. For most of the observed systems, one or more of the simulated SEDs match reasonably well. The best matches recover the infrared luminosity and the star formation rate of the observed systems, and the more massive systems preferentially match SEDs from simulations of more massive galaxies. The most morphologically distorted systems in our sample are best matched to the simulated SEDs that are close to coalescence, while less evolved systems match well with the SEDs over a wide range of interaction stages, suggesting that an SED alone is insufficient for identifying the interaction stage except during the most active phases in strongly interacting systems. This result is supported by our finding that the SEDs calculated for simulated systems vary little over the interaction sequence. C1 [Lanz, Lauranne; Zezas, Andreas; Smith, Howard A.; Ashby, Matthew L. N.; Fazio, Giovanni G.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lanz, Lauranne] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Hayward, Christopher C.] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany. [Zezas, Andreas] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Zezas, Andreas] Univ Crete, Inst Theoret & Computat Phys, Iraklion 71003, Crete, Greece. [Zezas, Andreas] Fdn Res & Technol Hellas, Iraklion 71110, Crete, Greece. [Brassington, Nicola] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. RP Lanz, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM llanz@ipac.caltech.edu RI Hayward, Christopher/I-4756-2012; Zezas, Andreas/C-7543-2011; OI Hayward, Christopher/0000-0003-4073-3236; Zezas, Andreas/0000-0001-8952-676X; Lanz, Lauranne/0000-0002-3249-8224 FU NASA [NNX12AI55G, NAS5-98034]; JPL RSA [717437, 717353]; Klaus Tschira Foundation; National Science Foundation [PHY-1066293] FX The simulations in this paper were performed on the Odyssey cluster supported by the FAS Research Computing Group at Harvard University. L.L.and H.A.S.acknowledge partial support from NASA grant NNX12AI55G and JPL RSA contracts 717437 and 717353.C.C.H.is grateful to the Klaus Tschira Foundation for financial support and acknowledges the hospitality of the Aspen Center for Physics, which is supported by the National Science Foundation Grant No.PHY-1066293. This work was based on archival data obtained from the Spitzer Science Archive, the Mikulski Archive for Space Telescopes (MAST), the Swift data archive, and the Herschel Science Archive.Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Spitzer is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA.GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034.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 71 TC 16 Z9 16 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 2014 VL 785 IS 1 AR 39 DI 10.1088/0004-637X/785/1/39 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300039 ER PT J AU McNamara, BR Russell, HR Nulsen, PEJ Edge, AC Murray, NW Main, RA Vantyghem, AN Combes, F Fabian, AC Salome, P Kirkpatrick, CC Baum, SA Bregman, JN Donahue, M Egami, E Hamer, S O'Dea, CP Oonk, JBR Tremblay, G Voit, GM AF McNamara, B. R. Russell, H. R. Nulsen, P. E. J. Edge, A. C. Murray, N. W. Main, R. A. Vantyghem, A. N. Combes, F. Fabian, A. C. Salome, P. Kirkpatrick, C. C. Baum, S. A. Bregman, J. N. Donahue, M. Egami, E. Hamer, S. O'Dea, C. P. Oonk, J. B. R. Tremblay, G. Voit, G. M. TI A 10(10) SOLAR MASS FLOW OF MOLECULAR GAS IN THE A1835 BRIGHTEST CLUSTER GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies COLFAML; active; galaxies COLFAML; clusters COLFAML; general; galaxies COLFAML; clusters COLFAML; individual (A1835); galaxies COLFAML; star formation; ISM COLFAML; jets and outflows; ISM COLFAML; molecules ID ACTIVE GALACTIC NUCLEI; RAY-LUMINOUS CLUSTERS; COOLING-FLOW; STAR-FORMATION; BLACK-HOLES; H-ALPHA; SPITZER OBSERVATIONS; CONVERSION FACTOR; BUOYANT BUBBLES; PERSEUS CLUSTER AB We report ALMA Early Science observations of the A1835 brightest cluster galaxy (BCG) in the CO (3-2) and CO (1-0) emission lines. We detect 5 Chi 10(10)M(circle dot) of molecular gas within 10 kpc of the BCG. Its ensemble velocity profile width of similar to 130 km s(-1) FWHM is too narrow for the molecular clouds to be supported in the galaxy by dynamic pressure. The gas may instead be supported in a rotating, turbulent disk oriented nearly face-on. Roughly 10(10)M(circle dot) of molecular gas is projected 3-10 kpc to the northwest and to the east of the nucleus with line-of-sight velocities lying between -250 km s(-1) and +480 km s(-1) with respect to the systemic velocity. The high-velocity gas may be either inflowing or outflowing. However, the absence of high-velocity gas toward the nucleus that would be expected in a steady inflow, and its bipolar distribution on either side of the nucleus, are more naturally explained as outflow. Star formation and radiation from the active galactic nucleus (AGN) are both incapable of driving an outflow of this magnitude. The location of the high-velocity gas projected behind buoyantly rising X-ray cavities and favorable energetics suggest an outflow driven by the radio AGN. If so, the molecular outflow may be associated with a hot outflow on larger scales reported by Kirkpatrick and colleagues. The molecular gas flow rate of approximately 200M(circle dot) yr (1) is comparable to the star formation rate of 100-180M(circle dot) yr (1) in the central disk. How radio bubbles would lift dense molecular gas in their updrafts, how much gas will be lost to the BCG, and how much will return to fuel future star formation and AGN activity are poorly understood. Our results imply that radio-mechanical (radio-mode) feedback not only heats hot atmospheres surrounding elliptical galaxies and BCGs, but it is able to sweep higher density molecular gas away from their centers. C1 [McNamara, B. R.; Russell, H. R.; Main, R. A.; Vantyghem, A. N.; Kirkpatrick, C. C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada. [McNamara, B. R.; Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Edge, A. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Murray, N. W.; Hamer, S.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Combes, F.; Salome, P.] Observ Paris, F-75014 Paris, France. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Baum, S. A.; O'Dea, C. P.] Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA. [Bregman, J. N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Donahue, M.; Voit, G. M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Egami, E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Oonk, J. B. R.] Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands. [Tremblay, G.] European So Observ, D-85748 Garching, Germany. RP McNamara, BR (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. OI Edge, Alastair/0000-0002-3398-6916; Voit, Gerard/0000-0002-3514-0383 FU Canadian Space Agency Space Science Enhancement Program; Natural Sciences and Engineering Research Council of Canada; STFC [ST/I001573/1]; NASA [NAS8-03060]; [2011.0.00374] FX B.R.M. thanks Tom Jones and Christine Jones for helpful comments. H.R.R. and B.R.M. acknowledge generous financial support from the Canadian Space Agency Space Science Enhancement Program. B.R.M., R.A.M., H.R.R., and A.N.V. acknowledge support from the Natural Sciences and Engineering Research Council of Canada. A.C.E. acknowledges support from STFC grant ST/I001573/1. P.E.J.N. is supported by NASA grant NAS8-03060. We thank the ALMA scientific support staff members Adam Leroy and Stephane Leon. The paper makes use of the following ALMA data: ADS/JAO. ALMA No. 2011.0.00374. S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), 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. This paper is dedicated to Jim Pisano, who helped make ALMA the marvelous facility it is. NR 64 TC 29 Z9 29 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 2014 VL 785 IS 1 AR 44 DI 10.1088/0004-637X/785/1/44 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300044 ER PT J AU Meng, Y Lin, J Zhang, L Reeves, KK Zhang, QS Yuan, F AF Meng, Y. Lin, J. Zhang, L. Reeves, K. K. Zhang, Q. S. Yuan, F. TI AN MHD MODEL FOR MAGNETAR GIANT FLARES SO ASTROPHYSICAL JOURNAL LA English DT Article DE instabilities; magnetic reconnection; magnetohydrodynamics (MHD); stars: flare; stars: magnetic field; stars: neutron ID CORONAL MASS EJECTIONS; CRUSTAL PLATE-TECTONICS; SOFT GAMMA-REPEATERS; X-RAY PULSAR; FLUX-ROPE MODELS; SOLAR ERUPTIONS; NEUTRON-STARS; SGR 1900+14; PARTICLE-ACCELERATION; RADIATIVE MECHANISM AB Giant flares on soft gamma-ray repeaters that are thought to take place on magnetars release enormous energy in a short time interval. Their power can be explained by catastrophic instabilities occurring in the magnetic field configuration and the subsequent magnetic reconnection. By analogy with the coronal mass ejection events on the Sun, we develop a theoretical model via an analytic approach for magnetar giant flares. In this model, the rotation and/or displacement of the crust causes the field to twist and deform, leading to flux rope formation in the magnetosphere and energy accumulation in the related configuration. When the energy and helicity stored in the configuration reach a threshold, the system loses its equilibrium, the flux rope is ejected outward in a catastrophic way, and magnetic reconnection helps the catastrophe develop to a plausible eruption. By taking SGR 1806-20 as an example, we calculate the free magnetic energy released in such an eruptive process and find that it is more than 10(47) erg, which is enough to power a giant flare. The released free magnetic energy is converted into radiative energy, kinetic energy, and gravitational energy of the flux rope. We calculated the light curves of the eruptive processes for the giant flares of SGR 1806-20, SGR 0526-66, and SGR 1900+14, and compared them with the observational data. The calculated light curves are in good agreement with the observed light curves of giant flares. C1 [Meng, Y.; Lin, J.; Zhang, Q. S.] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Yunnan, Peoples R China. [Meng, Y.] Univ Chinese Acad Sci, Beijing 100039, Peoples R China. [Zhang, L.] Yunnan Univ, Dept Phys, Kunming 650091, Yunnan, Peoples R China. [Reeves, K. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zhang, Q. S.] Chinese Acad Sci, Yunnan Astron Observ, Key Lab Struct & Evolut Celestial Objects, Kunming 650011, Yunnan, Peoples R China. [Yuan, F.] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. RP Meng, Y (reprint author), Chinese Acad Sci, Yunnan Observ, POB 110, Kunming 650011, Yunnan, Peoples R China. EM mengy@ynao.ac.cn; jlin@ynao.ac.cn RI Reeves, Katharine/P-9163-2014; LIN, JUN/B-9890-2017 FU Program 973 [2011CB811403, 2013CBA01503]; NSFC [11273055, 11333007, 11121062, 11133005]; CAS [KJCX2-EW-T07, XDB09000000]; NSF [AGS-1156076] FX We are grateful to K. Hurley for providing the observational data used in this paper, and to Z. Dai and Y. Yuan for valuable discussions and suggestions. Helpful advice and suggestions for using the observational data given by D.M. Palmer are highly appreciated. We appreciate the referee for constructive advice and comments for improving this work as well. This work was supported by Program 973 grants 2011CB811403 and 2013CBA01503, NSFC grants 11273055 and 11333007, and CAS grants KJCX2-EW-T07 and XDB09000000. F.Y. was supported by the NSFC grants 11121062 and 11133005. K.K.R. is supported by NSF grant AGS-1156076 to the Smithsonian Astrophysical Observatory. NR 79 TC 6 Z9 8 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 62 DI 10.1088/0004-637X/785/1/62 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300062 ER PT J AU Palau, A Estalella, R Girart, JM Fuente, A Fontani, F Commercon, B Busquet, G Bontemps, S Sanchez-Monge, A Zapata, LA Zhang, QZ Hennebelle, P di Francesco, J AF Palau, Aina Estalella, Robert Girart, Josep M. Fuente, Asuncion Fontani, Francesco Commercon, Benoit Busquet, Gemma Bontemps, Sylvain Sanchez-Monge, Alvaro Zapata, Luis A. Zhang, Qizhou Hennebelle, Patrick di Francesco, James TI FRAGMENTATION OF MASSIVE DENSE CORES DOWN TO less than or similar to 1000 AU: RELATION BETWEEN FRAGMENTATION AND DENSITY STRUCTURE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies COLFAML; star clusters COLFAML; general; radio continuum COLFAML; ISM; stars COLFAML; formation; techniques COLFAML; high angular resolution ID HIGH ANGULAR RESOLUTION; MOLECULAR CLOUD CORES; STAR-FORMING REGIONS; (PROTO)STAR IRAS 20126+4104; FAR-INFRARED OBSERVATIONS; RIMMED GLOBULE IC1396N; MILLIMETER CONTINUUM; CYGNUS-X; HIERARCHICAL FRAGMENTATION; SUBMILLIMETER OBSERVATIONS AB In order to shed light on the main physical processes controlling fragmentation of massive dense cores, we present a uniform study of the density structure of 19 massive dense cores, selected to be at similar evolutionary stages, for which their relative fragmentation level was assessed in a previous work. We inferred the density structure of the 19 cores through a simultaneous fit of the radial intensity profiles at 450 and 850 mu m (or 1.2 mm in two cases) and the spectral energy distribution, assuming spherical symmetry and that the density and temperature of the cores decrease with radius following power-laws. Even though the estimated fragmentation level is strictly speaking a lower limit, its relative value is significant and several trends could be explored with our data. We find a weak (inverse) trend of fragmentation level and density power-law index, with steeper density profiles tending to show lower fragmentation, and vice versa. In addition, we find a trend of fragmentation increasing with density within a given radius, which arises from a combination of flat density profile and high central density and is consistent with Jeans fragmentation. We considered the effects of rotational-to-gravitational energy ratio, non-thermal velocity dispersion, and turbulence mode on the density structure of the cores, and found that compressive turbulence seems to yield higher central densities. Finally, a possible explanation for the origin of cores with concentrated density profiles, which are the cores showing no fragmentation, could be related with a strong magnetic field, consistent with the outcome of radiation magnetohydrodynamic simulations. C1 [Palau, Aina; Girart, Josep M.] Inst Ciencies Espai CSIC IEEC, Fac Ciencies, E-08193 Bellaterra, Catalunya, Spain. [Estalella, Robert] Univ Barcelona, Inst Ciencies Cosmos, Dept Astron Meteorol IEEC UB, E-08028 Barcelona, Spain. [Fuente, Asuncion] Observ Astron Nacl, E-28803 Madrid, Spain. [Fontani, Francesco; Sanchez-Monge, Alvaro] INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Commercon, Benoit; Hennebelle, Patrick] Ecole Normale Super, Observ Paris, Lab Radioastron, UMR CNRS 8112, F-75231 Paris 05, France. [Commercon, Benoit] Univ Lyon, Ecole Normale Super Lyon, CRAL, UMR CNRS 5574, F-69364 Lyon 07, France. [Busquet, Gemma] INAF Ist Astrofis & Planetol Spaziali, Area Rec Tor Vergata, I-00133 Rome, Italy. [Bontemps, Sylvain] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Bontemps, Sylvain] CNRS, LAB, UMR 5804, F-33270 Floirac, France. [Sanchez-Monge, Alvaro] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Zapata, Luis A.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [di Francesco, James] Univ Victoria, Dept Phys & Astron, STN CSC, Victoria, BC V8W 3P6, Canada. [di Francesco, James] Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. RP Palau, A (reprint author), Inst Ciencies Espai CSIC IEEC, Fac Ciencies, Campus UAB,Torre C5 Parell, E-08193 Bellaterra, Catalunya, Spain. EM palau@ieec.uab.es RI Girart, Josep/O-1638-2014; Fuente, Asuncion/G-1468-2016; OI Girart, Josep/0000-0002-3829-5591; Fuente, Asuncion/0000-0001-6317-6343; Zhang, Qizhou/0000-0003-2384-6589 NR 115 TC 11 Z9 11 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 42 DI 10.1088/0004-637X/785/1/42 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300042 ER PT J AU Patra, N Kral, P Sadeghpour, HR AF Patra, N. Kral, P. Sadeghpour, H. R. TI NUCLEATION AND STABILIZATION OF CARBON-RICH STRUCTURES IN INTERSTELLAR MEDIA SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; astrochemistry; infrared: ISM; ISM: molecules; planetary nebulae: general; methods: numerical; molecular processes ID POLYCYCLIC AROMATIC-HYDROCARBONS; MOLECULAR-DYNAMICS; REFLECTION NEBULAE; DARK CLOUDS; BANDS; C-60; SPACE; NANOPARTICLES; NAPHTHALENE; FULLERENES AB We study the conditions under which carbon clusters of different sizes form and stabilize. We describe the approach to equilibrium by simulating tenuous carbon gas dynamics to long times. First, we use reactive molecular dynamics simulations to describe the nucleation of long chains, large clusters, and complex cage structures in carbon- and hydrogen-rich interstellar gas phases. We study how temperature, particle density, the presence of hydrogen, and carbon inflow affect the nucleation of molecular moieties with different characteristics, in accordance with astrophysical conditions. We extend the simulations to densities that are orders of magnitude lower than current laboratory densities, to temperatures that are relevant to circumstellar environments of planetary nebulae, and microsecond formation times. We correlate cluster size distributions from the simulations with thermodynamic equilibrium at low temperatures and gas densities, where entropy plays a significant role. C1 [Patra, N.; Kral, P.] Univ Illinois, Dept Chem, Chicago, IL 60607 USA. [Kral, P.] Univ Illinois, Dept Phys, Chicago, IL 60607 USA. [Patra, N.; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Patra, N (reprint author), Univ Illinois, Dept Chem, Chicago, IL 60607 USA. EM npatra2@uic.edu; pkral@uic.edu; hrs@cfa.harvard.edu FU SAO Fellowship; Smithsonian Grand Challenges Award FX N.P. acknowledges support from the SAO Fellowship. The authors are grateful for the allocation of computer time on the Kraken Cluster at the NSF-XSEDE and Odyssey Clusters at Harvard University where parts of the simulations were conducted. Financial support was provided by a Smithsonian Grand Challenges Award. NR 38 TC 3 Z9 3 U1 0 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 6 DI 10.1088/0004-637X/785/1/6 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300006 ER PT J AU Teng, SH Brandt, WN Harrison, FA Luo, B Alexander, DM Bauer, FE Boggs, SE Christensen, FE Comastri, A Craig, WW Fabian, AC Farrah, D Fiore, F Gandhi, P Grefenstette, BW Hailey, CJ Hickox, RC Madsen, KK Ptak, AF Rigby, JR Risaliti, G Saez, C Stern, D Veilleux, S Walton, DJ Wik, DR Zhang, WW AF Teng, Stacy H. Brandt, W. N. Harrison, F. A. Luo, B. Alexander, D. M. Bauer, F. E. Boggs, S. E. Christensen, F. E. Comastri, A. Craig, W. W. Fabian, A. C. Farrah, D. Fiore, F. Gandhi, P. Grefenstette, B. W. Hailey, C. J. Hickox, R. C. Madsen, K. K. Ptak, A. F. Rigby, J. R. Risaliti, G. Saez, C. Stern, D. Veilleux, S. Walton, D. J. Wik, D. R. Zhang, W. W. TI NuSTAR REVEALS AN INTRINSICALLY X-RAY WEAK BROAD ABSORPTION LINE QUASAR IN THE ULTRALUMINOUS INFRARED GALAXY MARKARIAN 231 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; quasars: individual (Mrk 231); X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; ADVECTION-DOMINATED ACCRETION; DIGITAL SKY SURVEY; XMM-NEWTON; SEYFERT-GALAXIES; CHANDRA SURVEY; EMISSION-LINE; LOCAL ULIRGS; ENERGY-DISTRIBUTIONS AB We present high-energy (3-30 keV) NuSTAR observations of the nearest quasar, the ultraluminous infrared galaxy (ULIRG) Markarian 231 (Mrk 231), supplemented with new and simultaneous low-energy (0.5-8 keV) data from Chandra. The source was detected, though at much fainter levels than previously reported, likely due to contamination in the large apertures of previous non-focusing hard X-ray telescopes. The full band (0.5-30 keV) X-ray spectrum suggests the active galactic nucleus (AGN) in Mrk 231 is absorbed by a patchy and Compton-thin (N-H similar to 1.2(-0.3)(+0.3) Chi 10(23) cm(-2)) column. The intrinsic X-ray luminosity (L0.5-30 keV similar to 1.0 Chi 10(43) erg s(-1)) is extremely weak relative to the bolometric luminosity where the 2-10 keV to bolometric luminosity ratio is similar to 0.03% compared to the typical values of 2%-15%. Additionally, Mrk 231 has a low X-ray-to-optical power law slope (alpha(OX) similar to -1.7). It is a local example of a low-ionization broad absorption line quasar that is intrinsically X-ray weak. The weak ionizing continuum may explain the lack of mid-infrared [O Iv], [Ne v], and [Ne vI] fine-structure emission lines which are present in sources with otherwise similar AGN properties. We argue that the intrinsic X-ray weakness may be a result of the super-Eddington accretion occurring in the nucleus of this ULIRG, and may also be naturally related to the powerful wind event seen in Mrk 231, a merger remnant escaping from its dusty cocoon. C1 [Teng, Stacy H.; Rigby, J. R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Harrison, F. A.; Grefenstette, B. W.; Madsen, K. K.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Alexander, D. M.; Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Comastri, A.] INAF Osserv Astron Bologna, I-40127 Bologna, Italy. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Fabian, A. C.] Inst Astron, Cambridge CB3 0HA, England. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Fiore, F.] Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Ptak, A. F.; Wik, D. R.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Risaliti, G.] INAF Osserv Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Veilleux, S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. RP Teng, SH (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. EM stacy.h.teng@nasa.gov RI Rigby, Jane/D-4588-2012; Boggs, Steven/E-4170-2015; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; OI Rigby, Jane/0000-0002-7627-6551; Boggs, Steven/0000-0001-9567-4224; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Risaliti, Guido/0000-0002-3556-977X; Alexander, David/0000-0002-5896-6313; Fiore, Fabrizio/0000-0002-4031-4157 FU NASA [NNG08FD60C]; California Institute of Technology; National Aeronautics and Space Administration; NuSTAR Data Analysis Software (NuSTARDAS); ASI Science Data Center (ASDC, Italy); California Institute of Technology (USA); ESA Member States; USA (NASA); Jet Propulsion Laboratory, Caltech; Jet Propulsion Laboratory, Caltech, under contract with NASA; NASA Postdoctoral Program (NPP) Fellowship; California Institute of Technology (Caltech) NuSTAR [44A-1092750]; NASA ADP [NNX10AC99G]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024, Anillo ACT1101]; ASI/INAF [I/037/12/0011/13]; STFC [ST/J003697/1] FX We are grateful to the anonymous referee for providing useful comments which improved our manuscript. We thank Wayne Baumgartner, Bret Lehmer, Richard Mushotzky, Jeremy Schnittman, Tahir Yaqoob, and Andreas Zezas for useful discussions. We would also like to thank Lee Armus who provided useful comments in the early planning phase of the NuSTAR ULIRG program. We also thank Roberto Maiolino, David Rupke, and Eckhard Sturm who are co-investigators of the Chandra program. 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 scientific results reported in this article are based in part on observations made by the Chandra X-Ray Observatory and data obtained from the Chandra Data Archive published previously in cited articles. This work, in part, made use of observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). We made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, Caltech, under contract with NASA. S.H.T. is supported by a NASA Postdoctoral Program (NPP) Fellowship. W.N.B. and B.L. acknowledge support by California Institute of Technology (Caltech) NuSTAR subcontract 44A-1092750 and NASA ADP grant NNX10AC99G. F.E.B. acknowledges support from Basal-CATA (PFB-06/2007) and CONICYT-Chile (under grants FONDECYT 1101024 and Anillo ACT1101). A.C. acknowledges support from ASI/INAF grant I/037/12/0011/13. P.G. acknowledges support from STFC grant reference ST/J003697/1. NR 97 TC 34 Z9 34 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2014 VL 785 IS 1 AR 19 DI 10.1088/0004-637X/785/1/19 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG8AE UT WOS:000335639300019 ER EF