FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Silverman, JM Vinko, J Kasliwal, MM Fox, OD Cao, Y Johansson, J Perley, DA Tal, D Wheeler, JC Amanullah, R Arcavi, I Bloom, JS Gal-Yam, A Goobar, A Kulkarni, SR Laher, R Lee, WH Marion, GH Nugent, PE Shivvers, I AF Silverman, Jeffrey M. Vinko, Jozsef Kasliwal, Mansi M. Fox, Ori D. Cao, Yi Johansson, Joel Perley, Daniel A. Tal, David Wheeler, J. Craig Amanullah, Rahman Arcavi, Iair Bloom, Joshua S. Gal-Yam, Avishay Goobar, Ariel Kulkarni, Shrinivas R. Laher, Russ Lee, William H. Marion, G. H. Nugent, Peter E. Shivvers, Isaac TI SN 2000cx and SN 2013bh: extremely rare, nearly twin Type Ia supernovae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; supernovae: individual: SN 2000cx; supernovae: individual: SN 2013bh ID AUTOMATIC IMAGING TELESCOPE; HIGH-VELOCITY FEATURES; LOW-RESOLUTION; LEGACY SURVEY; LIGHT CURVES; WHITE-DWARF; SKY SURVEY; SPECTRA; 2011FE; STAR AB The Type Ia supernova (SN Ia) SN 2000cx was one of the most peculiar transients ever discovered, with a rise to maximum brightness typical of a SN Ia, but a slower decline and a higher photospheric temperature. 13 yr later SN 2013bh (also known as iPTF13abc), a near identical twin, was discovered and we obtained optical and near-infrared photometry and low-resolution optical spectroscopy from discovery until about 1 month past r-band maximum brightness. The spectra of both objects show iron-group elements [Co ii, Ni ii, Fe ii, Fe iii and high-velocity features (HVFs) of Ti ii], intermediate-mass elements (Si ii, Si iii and S ii) and separate normal velocity features (similar to 12 000 km s(-1)) and HVFs (similar to 24 000 km s(-1)) of Ca ii. Persistent absorption from Fe iii and Si iii, along with the colour evolution, implies high blackbody temperatures for SNe 2013bh and 2000cx (similar to 12 000 K). Both objects lack narrow Na i D absorption and exploded in the outskirts of their hosts, indicating that the SN environments were relatively free of interstellar or circumstellar material and may imply that the progenitors came from a relatively old and low-metallicity stellar population. Models of SN 2000cx, seemingly applicable to SN 2013bh, imply the production of up to similar to 1 M-circle dot of Ni-56 and (4.3-5.5) x 10(-3) M-circle dot of fast-moving Ca ejecta. C1 [Silverman, Jeffrey M.; Vinko, Jozsef; Wheeler, J. Craig; Marion, G. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Vinko, Jozsef] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Kasliwal, Mansi M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Fox, Ori D.; Bloom, Joshua S.; Nugent, Peter E.; Shivvers, Isaac] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cao, Yi; Perley, Daniel A.; Kulkarni, Shrinivas R.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Johansson, Joel; Amanullah, Rahman; Goobar, Ariel] Stockholm Univ, Oskar Klein Ctr, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Tal, David; Arcavi, Iair; Gal-Yam, Avishay] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Laher, Russ] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Lee, William H.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Marion, G. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP Silverman, JM (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. EM jsilverman@astro.as.utexas.edu OI Shivvers, Isaac/0000-0003-3373-8047 FU W. M. Keck Foundation; NASA [NNX09AH71G, NNX09AT02G, NNX10AI27G, NNX12AE66G]; CONACyT [INFR-2009-01-122785]; UNAM PAPIIT [IN113810]; UC MEXUS-CONACyT; Alfred P. Sloan Foundation; NSF; US Department of Energy Office of Science; NSF [AST-1302771, AST 11-09801, PHY-1066293]; Hungarian OTKA [NN 107637]; Hubble Fellowship; Carnegie-Princeton Fellowship; CDI from the National Science Foundation [0941742] FX We would like to thank M. Ganeshalingam, P. Kelly and E. Ofek for helpful discussions, J. Caldwell, S. Odewahn and S. Rostopchin for their assistance with some of the observations, as well as the PESSTO and CRTS collaborations for making some of their data on SN 2013bh publicly available. The HET is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universitat Munchen and Georg-August-Universitat Gottingen. The HET is named in honour of its principal benefactors, William P. Hobby and Robert E. Eberly. The Marcario Low Resolution Spectrograph is named for Mike Marcario of High Lonesome Optics who fabricated several optics for the instrument but died before its completion. The LRS is a joint project of the HET partnership and the Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration (NASA); the observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors 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. This work is partially based on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. We thank the RATIR instrument team and the staff of the Observatorio Astronomico Nacional on Sierra San Pedro Martir. RATIR is a collaboration between the University of California, the Universidad Nacional Autonoma de Mexico, NASA Goddard Space Flight Center and Arizona State University, benefiting from the loan of an H2RG detector from Teledyne Scientific and Imaging. RATIR, the automation of the Harold L. Johnson Telescope of the Observatorio Astronomico Nacional on Sierra San Pedro Martir and the operation of both are funded by the partner institutions and through NASA grants NNX09AH71G, NNX09AT02G, NNX10AI27G and NNX12AE66G, CONACyT grants INFR-2009-01-122785, UNAM PAPIIT grant IN113810 and a UC MEXUS-CONACyT grant. The National Energy Research Scientific Computing Center, supported by the Office of Science of the US Department of Energy, provided staff, computational resources and data storage for this project. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the NSF and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. JMS is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. JV is supported by Hungarian OTKA Grant NN 107637. MMK acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. JCW's supernova group at UT Austin is supported by NSF Grant AST 11-09801. Some work on this paper by JCW was done in the hospitable clime of the Aspen Center for Physics that is supported by NSF Grant PHY-1066293.; JSB acknowledges the generous support of a CDI grant (#0941742) from the National Science Foundation. NR 76 TC 7 Z9 7 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 2 BP 1225 EP 1237 DI 10.1093/mnras/stt1647 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 258LP UT WOS:000327461100024 ER PT J AU McKinley, B Briggs, F Gaensler, BM Feain, IJ Bernardi, G Wayth, RB Johnston-Hollitt, M Offringa, AR Arcus, W Barnes, DG Bowman, JD Bunton, JD Cappallo, RJ Corey, BE Deshpande, AA Desouza, L Emrich, D Goeke, R Greenhill, LJ Hazelton, BJ Herne, D Hewitt, JN Kaplan, DL Kasper, JC Kincaid, BB Koenig, R Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Pathikulangara, J Prabu, T Remillard, RA Rogers, AEE Roshi, DA Salah, JE Sault, RJ Shankar, NU Srivani, KS Stevens, J Subrahmanyan, R Tingay, SJ Waterson, M Webster, RL Whitney, AR Williams, A Williams, CL Wyithe, JSB AF McKinley, B. Briggs, F. Gaensler, B. M. Feain, I. J. Bernardi, G. Wayth, R. B. Johnston-Hollitt, M. Offringa, A. R. Arcus, W. Barnes, D. G. Bowman, J. D. Bunton, J. D. Cappallo, R. J. Corey, B. E. Deshpande, A. A. Desouza, L. Emrich, D. Goeke, R. Greenhill, L. J. Hazelton, B. J. Herne, D. Hewitt, J. N. Kaplan, D. L. Kasper, J. C. Kincaid, B. B. Koenig, R. Kratzenberg, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Pathikulangara, J. Prabu, T. Remillard, R. A. Rogers, A. E. E. Roshi, D. A. Salah, J. E. Sault, R. J. Shankar, N. Udaya Srivani, K. S. Stevens, J. Subrahmanyan, R. Tingay, S. J. Waterson, M. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. Wyithe, J. S. B. TI The giant lobes of Centaurus A observed at 118 MHz with the Murchison Widefield Array SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: interferometric; galaxies: active; galaxies: individual: NGC 5128; radio continuum: galaxies ID GALACTIC RADIO-EMISSION; NGC 5128 CENTAURUS; SUPERNOVA REMNANT; SOUTHERN SKY; GALAXIES; SPECTRUM; JET; POLARIZATION; SCALE; INTERFEROMETRY AB We present new wide-field observations of Centaurus A (Cen A) and the surrounding region at 118 MHz with the Murchison Widefield Array (MWA) 32-tile prototype, with which we investigate the spectral-index distribution of Cen A's giant radio lobes. We compare our images to 1.4 GHz maps of Cen A and compute spectral indices using temperature-temperature plots and spectral tomography. We find that the morphologies at 118 MHz and 1.4 GHz match very closely apart from an extra peak in the southern lobe at 118 MHz, which provides tentative evidence for the existence of a southern counterpart to the northern middle lobe of Cen A. Our spatially averaged spectral indices for both the northern and southern lobes are consistent with previous analyses, however we find significant spatial variation of the spectra across the extent of each lobe. Both the spectral-index distribution and the morphology at low radio frequencies support a scenario of multiple outbursts of activity from the central engine. Our results are consistent with inverse-Compton modelling of radio and gamma-ray data that support a value for the lobe age of between 10 and 80 Myr. C1 [McKinley, B.; Briggs, F.; Offringa, A. R.; Waterson, M.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [McKinley, B.; Briggs, F.; Gaensler, B. M.; Wayth, R. B.; Offringa, A. R.; Mitchell, D. A.; Ord, S. M.; Subrahmanyan, R.; Tingay, S. J.; Webster, R. L.; Wyithe, J. S. B.] Australian Natl Univ, ARC Ctr Excellence All Sky Astrophys CAASTRO, Canberra, ACT 2611, Australia. [Gaensler, B. M.; Desouza, L.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Feain, I. J.; Bunton, J. D.; Desouza, L.; Koenig, R.; Pathikulangara, J.; Stevens, J.] CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bernardi, G.] SKA SA, ZA-7405 Cape Town, South Africa. [Wayth, R. B.; Arcus, W.; Emrich, D.; Herne, D.; Lynch, M. J.; Ord, S. M.; Tingay, S. J.; Waterson, M.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Barnes, D. G.] Monash Univ, Monash E Res Ctr, Clayton, Vic 3168, Australia. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Cappallo, R. J.; Corey, B. E.; Kincaid, B. B.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Rogers, A. E. E.; Salah, J. E.; Whitney, A. R.] MIT Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Goeke, R.; Hewitt, J. N.; Morgan, E.; Remillard, R. A.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Mitchell, D. A.; Sault, R. J.; Webster, R. L.; Wyithe, J. S. B.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Roshi, D. A.] Natl Radio Astron Observ, Charlottesville, VA USA. [Roshi, D. A.] Natl Radio Astron Observ, Green Bank, VA USA. [Stevens, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. RP McKinley, B (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. EM ben@mso.anu.edu.au RI Bunton, John/A-4944-2008; Wayth, Randall/B-2444-2013; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Williams, Andrew/K-2931-2013; M, Manjunath/N-4000-2014; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; OI Wayth, Randall/0000-0002-6995-4131; Gaensler, Bryan/0000-0002-3382-9558; Williams, Andrew/0000-0001-9080-0105; M, Manjunath/0000-0001-8710-0730; Emrich, David/0000-0002-4058-1837; Wyithe, Stuart/0000-0001-7956-9758 FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (via the New Zealand Ministry of Economic Development) [MED-E1799]; Victoria University of Wellington (via IBM Shared University Research Grant); Australian Federal government via the Commonwealth Scientific and Industrial Research Organisation (CSIRO); National Collaborative Research Infrastructure Strategy; Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Western Australian State government FX This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753 and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the Commonwealth Scientific and Industrial Research Organisation (CSIRO), National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. We would like to thank P. Leahy for many constructive comments and suggestions that served to improve the manuscript. NR 76 TC 9 Z9 9 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 2 BP 1286 EP 1301 DI 10.1093/mnras/stt1662 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 258LP UT WOS:000327461100030 ER PT J AU Friesen, RK Medeiros, L Schnee, S Bourke, TL Di Francesco, J Gutermuth, R Myers, PC AF Friesen, R. K. Medeiros, L. Schnee, S. Bourke, T. L. Di Francesco, J. Gutermuth, R. Myers, P. C. TI Abundant cyanopolyynes as a probe of infall in the Serpens South cluster-forming region SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrochemistry; stars: formation; ISM: abundances; radio lines: ISM ID MOLECULAR LINE OBSERVATIONS; CARBON-CHAIN MOLECULES; GOULD BELT SURVEY; DARK CLOUD CORES; STARLESS CORES; AQUILA RIFT; DENSE CORES; INTERSTELLAR CLOUDS; CHEMISTRY; AMMONIA AB We have detected bright HC7N J = 21 - 20 emission towards multiple locations in the Serpens South cluster-forming region using the K-Band Focal Plane Array at the Robert C. Byrd Green Bank Telescope. HC7N is seen primarily towards cold filamentary structures that have yet to form stars, largely avoiding the dense gas associated with small protostellar groups and the main central cluster of Serpens South. Where detected, the HC7N abundances are similar to those found in other nearby star-forming regions. Towards some HC7N 'clumps', we find consistent variations in the line centroids relative to NH3 (1,1) emission, as well as systematic increases in the HC7N non-thermal line widths, which we argue reveal infall motions on to dense filaments within Serpens South with minimum mass accretion rates of M similar to 2-5 M-circle dot Myr(-1). The relative abundance of NH3 to HC7N suggests that the HC7N is tracing gas that has been at densities n similar to 10(4) cm(-3) for time-scales t less than or similar to 1-2 x 10(5) yr. Since HC7N emission peaks are rarely co-located with those of either NH3 or continuum, it is likely that Serpens South is not particularly remarkable in its abundance of HC7N, but instead the serendipitous mapping of HC7N simultaneously with NH3 has allowed us to detect HC7N at low abundances in regions where it otherwise may not have been looked for. This result extends the known star-forming regions containing significant HC7N emission from typically quiescent regions, like the Taurus molecular cloud, to more complex, active environments. C1 [Friesen, R. K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Medeiros, L.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Medeiros, L.; Schnee, S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Bourke, T. L.; Myers, P. C.] Harvard Smithsonian Ctr Astrophys, Radio & Geoastron Div, Cambridge, MA 02138 USA. [Di Francesco, J.] Natl Res Council Canada, Radio Astron Program, Victoria, BC V9E 2E7, Canada. [Di Francesco, J.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Gutermuth, R.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Friesen, RK (reprint author), Univ Toronto, Dunlap Inst Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. EM friesen@dunlap.utoronto.ca FU University of Toronto; National Science Foundation FX The authors thank the referee for providing comments that improved the paper. They also thank staff at the National Radio Astronomy Observatory and Robert C. Byrd GBT for their help in obtaining and reducing the KFPA data, particularly G. Langston and J. Masters. They also thank F. Heitsch and H. Kirk for helpful discussions, and additionally thank H. Kirk for providing HNC spectra. RF is a Dunlap Fellow at the Dunlap Institute for Astronomy & Astrophysics, University of Toronto. The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. LM was a summer student at the National Radio Astronomy Observatory, supported by the National Science Foundation Research Experience for Undergraduates programme. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of data from the Herschel Gould Belt survey (HGBS) project (http://gouldbeltherschel.cea.fr). The HGBS is a Herschel Key Programme jointly carried out by SPIRE Specialist Astronomy Group 3 (SAG 3), scientists of several institutes in the PACS Consortium (CEA Saclay, INAF-IFSI Rome and INAF-Arcetri, KU Leuven, MPIA Heidelberg) and scientists of the Herschel Science Center (HSC). NR 60 TC 16 Z9 16 U1 2 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 2 BP 1513 EP 1529 DI 10.1093/mnras/stt1671 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 258LP UT WOS:000327461100048 ER PT J AU Raiteri, CM Villata, M D'Ammando, F Larionov, VM Gurwell, MA Mirzaqulov, DO Smith, PS Acosta-Pulido, JA Agudo, I Arevalo, MJ Bachev, R Benitez, E Berdyugin, A Blinov, DA Borman, GA Bottcher, M Bozhilov, V Carnerero, MI Carosati, D Casadio, C Chen, WP Doroshenko, VT Efimova, YS Efimova, NV Ehgamberdiev, SA Gomez, JL Gonzalez-Morales, PA Hiriart, D Ibryamov, S Jadhav, Y Jorstad, SG Joshi, M Kadenius, V Klimanov, SA Kohli, M Konstantinova, TS Kopatskaya, EN Koptelova, E Kimeridze, G Kurtanidze, OM Larionova, EG Larionova, LV Ligustri, R Lindfors, E Marscher, AP McBreen, B McHardy, IM Metodieva, Y Molina, SN Morozova, DA Nazarov, SV Nikolashvili, MG Nilsson, K Okhmat, DN Ovcharov, E Panwar, N Pasanen, M Peneva, S Phipps, J Pulatova, NG Reinthal, R Ros, JA Sadun, AC Schwartz, RD Semkov, E Sergeev, SG Sigua, LA Sillanpaa, A Smith, N Stoyanov, K Strigachev, A Takalo, LO Taylor, B Thum, C Troitsky, IS Valcheva, A Wehrle, AE Wiesemeyer, H AF Raiteri, C. M. Villata, M. D'Ammando, F. Larionov, V. M. Gurwell, M. A. Mirzaqulov, D. O. Smith, P. S. Acosta-Pulido, J. A. Agudo, I. Arevalo, M. J. Bachev, R. Benitez, E. Berdyugin, A. Blinov, D. A. Borman, G. A. Boettcher, M. Bozhilov, V. Carnerero, M. I. Carosati, D. Casadio, C. Chen, W. P. Doroshenko, V. T. Efimova, Yu. S. Efimova, N. V. Ehgamberdiev, Sh. A. Gomez, J. L. Gonzalez-Morales, P. A. Hiriart, D. Ibryamov, S. Jadhav, Y. Jorstad, S. G. Joshi, M. Kadenius, V. Klimanov, S. A. Kohli, M. Konstantinova, T. S. Kopatskaya, E. N. Koptelova, E. Kimeridze, G. Kurtanidze, O. M. Larionova, E. G. Larionova, L. V. Ligustri, R. Lindfors, E. Marscher, A. P. McBreen, B. McHardy, I. M. Metodieva, Y. Molina, S. N. Morozova, D. A. Nazarov, S. V. Nikolashvili, M. G. Nilsson, K. Okhmat, D. N. Ovcharov, E. Panwar, N. Pasanen, M. Peneva, S. Phipps, J. Pulatova, N. G. Reinthal, R. Ros, J. A. Sadun, A. C. Schwartz, R. D. Semkov, E. Sergeev, S. G. Sigua, L. A. Sillanpaa, A. Smith, N. Stoyanov, K. Strigachev, A. Takalo, L. O. Taylor, B. Thum, C. Troitsky, I. S. Valcheva, A. Wehrle, A. E. Wiesemeyer, H. TI The awakening of BL Lacertae: observations by Fermi, Swift and the GASP-WEBT SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; BL Lacertae objects: general; BL Lacertae objects: individual: BL Lacertae; galaxies: jets ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; GAMMA-RAY; X-RAY; INTRADAY VARIABILITY; RADIO VARIABILITY; LIGHT CURVES; HELICAL JETS; INNER JET; 3C 279 AB Since the launch of the Fermi satellite, BL Lacertae has been moderately active at gamma-rays and optical frequencies until 2011 May, when the source started a series of strong flares. The exceptional optical sampling achieved by the GLAST-AGILE Support Program of the Whole Earth Blazar Telescope in collaboration with the Steward Observatory allows us to perform a detailed comparison with the daily gamma-ray observations by Fermi. Discrete correlation analysis between the optical and gamma-ray emission reveals correlation with a time lag of 0 +/- 1 d, which suggests cospatiality of the corresponding jet emitting regions. A better definition of the time lag is hindered by the daily gaps in the sampling of the extremely fast flux variations. In general, optical flares present more structure and develop on longer time-scales than corresponding gamma-ray flares. Observations at X-rays and at millimetre wavelengths reveal a common trend, which suggests that the region producing the mm and X-ray radiation is located downstream from the optical and gamma-ray-emitting zone in the jet. The mean optical degree of polarization slightly decreases over the considered period and in general it is higher when the flux is lower. The optical electric vector polarization angle (EVPA) shows a preferred orientation of about 15 degrees, nearly aligned with the radio core EVPA and mean jet direction. Oscillations around it increase during the 2011-2012 outburst. We investigate the effects of a geometrical interpretation of the long-term flux variability on the polarization. A helical magnetic field model predicts an evolution of the mean polarization that is in reasonable agreement with the observations. These can be fully explained by introducing slight variations in the compression factor in a transverse shock waves model. C1 [Raiteri, C. M.; Villata, M.; Carnerero, M. I.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. [D'Ammando, F.] Univ Perugia, Dip Fis, I-06123 Perugia, Italy. [D'Ammando, F.] Ist Radioastron, INAF, I-40129 Bologna, Italy. [Larionov, V. M.; Blinov, D. A.; Efimova, N. V.; Jorstad, S. G.; Konstantinova, T. S.; Kopatskaya, E. N.; Larionova, E. G.; Larionova, L. V.; Morozova, D. A.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Larionov, V. M.; Efimova, N. V.; Klimanov, S. A.] Pulkovo Observ, St Petersburg 196140, Russia. [Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mirzaqulov, D. O.; Ehgamberdiev, Sh. A.] Uzbek Acad Sci, Ulugh Beg Astron Inst, Maidanak Observ, Tashkent, Uzbekistan. [Smith, P. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Acosta-Pulido, J. A.; Arevalo, M. J.; Carnerero, M. I.; Gonzalez-Morales, P. A.] IAC, E-38200 Tenerife, Canary Islands, Spain. [Acosta-Pulido, J. A.; Arevalo, M. J.; Carnerero, M. I.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Canary Islands, Spain. [Agudo, I.; Casadio, C.; Gomez, J. L.; Molina, S. N.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Agudo, I.; Jorstad, S. G.; Joshi, M.; Marscher, A. P.; Taylor, B.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Bachev, R.; Ibryamov, S.; Peneva, S.; Semkov, E.; Stoyanov, K.; Strigachev, A.] Bulgarian Acad Sci, Inst Astron, BG-1784 Sofia, Bulgaria. [Benitez, E.; Hiriart, D.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. [Berdyugin, A.; Kadenius, V.; Lindfors, E.; Pasanen, M.; Reinthal, R.; Sillanpaa, A.; Takalo, L. O.] Univ Turku, Dept Phys & Astron, Tuorla Observ, FI-21500 Piikkio, Finland. [Blinov, D. A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. [Borman, G. A.; Efimova, Yu. S.; Nazarov, S. V.; Okhmat, D. N.; Pulatova, N. G.; Sergeev, S. G.] Crimean Astrophys Observ, UA-98409 Crimea, Ukraine. [Boettcher, M.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Boettcher, M.; Jadhav, Y.; Kohli, M.; Phipps, J.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Bozhilov, V.; Metodieva, Y.; Ovcharov, E.; Valcheva, A.] Univ Sofia, Fac Phys, Dept Astron, BG-1164 Sofia, Bulgaria. [Carosati, D.] EPT Observ, E-38780 La Palma, Canary Islands, Spain. [Carosati, D.] TNG Fdn Galileo, INAF, E-38712 La Palma, Canary Islands, Spain. [Chen, W. P.; Koptelova, E.; Panwar, N.] Natl Cent Univ, Grad Inst Astron, Jhongli 320, Taoyuan County, Taiwan. [Doroshenko, V. T.; Koptelova, E.] Moscow MV Lomonosov State Univ, South Stn, Moscow, Russia. [Koptelova, E.] Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. [Kimeridze, G.; Kurtanidze, O. M.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Mt Kanobili, Abastumani, Rep of Georgia. [Kurtanidze, O. M.] Landessternwarte Heidelberg Konigstuhl, D-69117 Heidelberg, Germany. [Ligustri, R.] Circolo Astrofili Talmassons, I-33030 Talmassons, Italy. [Lindfors, E.; Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [McBreen, B.] Univ Coll Dublin, UCD Sch Phys, Dublin 4, Ireland. [McHardy, I. M.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Pulatova, N. G.] Natl Astron Res Inst Thailand, Chiang Mai 50200, Thailand. [Ros, J. A.] Agrupacio Astron Sabadell, E-08200 Sabadell, Spain. [Sadun, A. C.] Univ Colorado Denver, Dept Phys, Denver, CO 80217 USA. [Schwartz, R. D.] Galaxy View Observ, Sequim, WA 98382 USA. [Smith, N.] Cork Inst Technol, Cork, Ireland. [Taylor, B.] Lowell Observ, Flagstaff, AZ 86001 USA. [Thum, C.; Wiesemeyer, H.] IRAM, E-18012 Granada, Spain. [Wehrle, A. E.] Space Sci Inst, Boulder, CO 80301 USA. [Wiesemeyer, H.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Raiteri, CM (reprint author), Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. EM raiteri@oato.inaf.it RI Kurtanidze, Omar/J-6237-2014; Molina, Sol Natalia/F-9968-2015; Agudo, Ivan/G-1701-2015; Larionov, Valeri/H-1349-2013; Morozova, Daria/H-1298-2013; Larionova, Elena/H-7287-2013; Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Grishina, Tatiana/H-6873-2013; Kopatskaya, Evgenia/H-4720-2013; Blinov, Dmitry/G-9925-2013 OI Villata, Massimo/0000-0003-1743-6946; Larionova, Liudmila/0000-0002-0274-1481; Smith, Paul/0000-0002-5083-3663; Raiteri, Claudia Maria/0000-0003-1784-2784; Molina, Sol Natalia/0000-0002-4112-2157; Agudo, Ivan/0000-0002-3777-6182; Larionov, Valeri/0000-0002-4640-4356; Morozova, Daria/0000-0002-9407-7804; Larionova, Elena/0000-0002-2471-6500; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; Grishina, Tatiana/0000-0002-3953-6676; Kopatskaya, Evgenia/0000-0001-9518-337X; Blinov, Dmitry/0000-0003-0611-5784 FU Russian Foundation for Basic Research [12-02-01237-a]; Fermi Guest Investigator grants [NNX08AW56G, NNX09AU10G, NNX12AO93G]; Shota Rustaveli National Science Foundation [FR/639/6-320/12]; Scientific Research Fund of the Bulgarian Ministry of Education and Sciences [DO 02-137 (BIn-13/09)]; Russian RFBR foundation [09-02-00092, 12-02-31193-2]; NASA Fermi Guest Investigator grants [NNX08AV65G, NNX10AO59G, NNX10AU15G, NNX11AO37G, NNX12AO90G]; NSF; BU; Lowell Observatory; UK Science and Technology Facilities Council; INSU/CNRS (France); MPG (Germany); IGN (Spain); MINECO (Spain) [AYA2010-14844]; CEIC (Andalucia) [P09-FQM-4784]; Smithsonian Institution; California Institute of Technology, under National Aeronautics and Space Administration; Academia Sinica FX We thank the referee, Philip Hughes, for useful comments. VTD acknowledges support by the grant of the Russian Foundation for Basic Research 12-02-01237-a. Data from the Steward Observatory spectropolarimetric monitoring project were used. This programme is supported by Fermi Guest Investigator grants NNX08AW56G, NNX09AU10G and NNX12AO93G. This article is partially based on observations made with the IAC80 operated on the island of Tenerife by the Instituto de Astrofisica de Canarias in the Spanish Observatorio del Teide. Many thanks are due to GAS (IAC Support Astronomer Group) and IAC telescope operators for helping with the observations at IAC-80 telescope. The Abastumani team acknowledges financial support of the project FR/639/6-320/12 by the Shota Rustaveli National Science Foundation under contract 31/76. This research was partially supported by Scientific Research Fund of the Bulgarian Ministry of Education and Sciences under grant DO 02-137 (BIn-13/09). The Skinakas Observatory is a collaborative project of the University of Crete, the Foundation for Research and Technology - Hellas, and the Max-Planck-Institut fur Extraterrestrische Physik. St Petersburg University team acknowledges support from Russian RFBR foundation via grants 09-02-00092 and 12-02-31193-2. The research at Boston University (BU) was funded in part by NASA Fermi Guest Investigator grants NNX08AV65G, NNX10AO59G, NNX10AU15G, NNX11AO37G and NNX12AO90G. The PRISM camera at Lowell Observatory was developed by K. Janes et al. at BU and Lowell Observatory, with funding from the NSF, BU and Lowell Observatory. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, with funding from the UK Science and Technology Facilities Council. This paper is partly based on observations carried out at the GermanSpanish Calar Alto Observatory, which is jointly operated by the MPIA and the IAA-CSIC. This paper is partly based on observations carried out at the IRAM 30-m Telescope, which is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). Acquisition and reduction of the MAPCAT and IRAM 30-m data is supported in part by MINECO (Spain) grant and AYA2010-14844, and by CEIC (Andalucia) grant P09-FQM-4784. 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 acknowledge the use of public data from the Swift data archive. This research has made use of Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, with funding from the UK Science and Technology Facilities Council. This paper is partly based on observations carried out at the German-Spanish Calar Alto Observatory, which is jointly operated by the MPIA and the IAA-CSIC. This paper is partly based on observations carried out at the IRAM 30-m Telescope, which is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). Acquisition and reduction of the MAPCAT and IRAM 30-m data is supported in part by MINECO (Spain) grant and AYA2010-14844, and by CEIC (Andalucia) grant P09-FQM-4784.; 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 acknowledge the use of public data from the Swift data archive. This research has made use of; (iii) 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 82 TC 23 Z9 23 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 DEC PY 2013 VL 436 IS 2 BP 1530 EP 1545 DI 10.1093/mnras/stt1672 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 258LP UT WOS:000327461100049 ER PT J AU Roediger, E Kraft, RP Nulsen, P Churazov, E Forman, W Bruggen, M Kokotanekova, R AF Roediger, E. Kraft, R. P. Nulsen, P. Churazov, E. Forman, W. Brueggen, M. Kokotanekova, R. TI Viscous Kelvin-Helmholtz instabilities in highly ionized plasmas SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; instabilities; plasmas; methods: numerical; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID SLOSHING COLD FRONTS; INTRACLUSTER MEDIUM; MAGNETIC-FIELDS; GALAXY CLUSTERS; VIRGO CLUSTER; INTERGALACTIC MEDIUM; CHANDRA OBSERVATION; BUOYANT BUBBLES; HEAT-CONDUCTION; RADIO BUBBLES AB Transport coefficients in highly ionized plasmas like the intracluster medium (ICM) are still ill-constrained. They influence various processes, among them the mixing at shear flow interfaces due to the Kelvin-Helmholtz instability (KHI). The observed structure of potential mixing layers can be used to infer the transport coefficients, but the data interpretation requires a detailed knowledge of the long-term evolution of the KHI under different conditions. Here we present the first systematic numerical study of the effect of constant and temperature-dependent isotropic viscosity over the full range of possible values. We show that moderate viscosities slow down the growth of the KHI and reduce the height of the KHI rolls and their rolling-up. Viscosities above a critical value suppress the KHI. The effect can be quantified in terms of the Reynolds number Re=U lambda nu, where U is the shear velocity, lambda the perturbation length and nu the kinematic viscosity. We derive the critical Re for constant and temperature-dependent Spitzer-like viscosities, an empirical relation for the viscous KHI growth time as a function of Re and density contrast, and describe special behaviours for Spitzer-like viscosities and high density contrasts. Finally, we briefly discuss several astrophysical situations where the viscous KHI could play a role, i.e. sloshing cold fronts, gas stripping from galaxies, buoyant cavities, ICM turbulence and high-velocity clouds. C1 [Roediger, E.; Brueggen, M.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Roediger, E.; Kokotanekova, R.] Univ Bremen, D-28725 Bremen, Germany. [Roediger, E.; Kraft, R. P.; Nulsen, P.; Forman, W.; Kokotanekova, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Churazov, E.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Kokotanekova, R.] Univ Innsbruck, AstroMundus Master Programme, A-6020 Innsbruck, Austria. RP Roediger, E (reprint author), Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. EM eroediger@hs.uni-hamburg.de RI Churazov, Eugene/A-7783-2013; OI Nulsen, Paul/0000-0003-0297-4493; Forman, William/0000-0002-9478-1682 FU Priority Programme 'Physics of the ISM' of the German Research Foundation (DFG); super-computing grants at the John-Neumann Institut at the Forschungszentrum Julich [NIC 5027, 6006]; CfA FX ER acknowledges the support of the Priority Programme 'Physics of the ISM' of the German Research Foundation (DFG), the super-computing grants NIC 5027 and 6006 at the John-Neumann Institut at the Forschungszentrum Julich and the hospitality of CfA during a Visiting Scientist Fellowship. We thank Fulai Guo and Robi Banerjee for helpful discussions. NR 58 TC 14 Z9 14 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 DEC PY 2013 VL 436 IS 2 BP 1721 EP 1740 DI 10.1093/mnras/stt1691 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 258LP UT WOS:000327461100066 ER PT J AU Moreno, J Bluck, AFL Ellison, SL Patton, DR Torrey, P Moster, BP AF Moreno, Jorge Bluck, Asa F. L. Ellison, Sara L. Patton, David R. Torrey, Paul Moster, Benjamin P. TI The dynamics of galaxy pairs in a cosmological setting SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: haloes; galaxies: interactions; galaxies: kinematics and dynamics; large-scale structure of Universe ID DIGITAL SKY SURVEY; SUPERMASSIVE BLACK-HOLES; TRIGGERED STAR-FORMATION; MERGER RATE EVOLUTION; ACTIVE GALACTIC NUCLEI; BRIGHTEST CLUSTER GALAXIES; MASS-METALLICITY RELATION; LAMBDA-CDM COSMOLOGY; GOODS NICMOS SURVEY; DARK-MATTER HALOS AB We use the Millennium Simulation, and an abundance matching framework, to investigate the dynamical behaviour of galaxy pairs embedded in a cosmological context. Our main galaxy-pair sample, selected to have separations r < 250 h(-1) kpc, consists of over 1.3 million pairs at redshift z = 0, with stellar masses greater than 10(10) M-circle dot, probing mass ratios down to 1:1000. We use dark matter halo membership and energy to classify our galaxy pairs. In terms of halo membership, central-satellite pairs tend to be in isolation (in relation to external more massive galaxies), are energetically bound to each other and are also weakly bound to a neighbouring massive galaxy. Satellite-satellite pairs, instead, inhabit regions in close proximity to a more massive galaxy, are energetically unbound and are often bound to that neighbour. We find that 60 per cent of our paired galaxies are bound to both their companion and to a third external object. Moreover, only 9 per cent of our pairs resemble the kind of systems described by idealized binary merger simulations in complete isolation. In sum, we demonstrate the importance of properly connecting galaxy pairs to the rest of the Universe. C1 [Moreno, Jorge; Bluck, Asa F. L.; Ellison, Sara L.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Patton, David R.] Trent Univ, Dept Phys & Astron, Peterborough, ON K9J 7B8, Canada. [Torrey, Paul] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Moster, Benjamin P.] Max Planck Inst Astrophys, D-85748 Garching, Germany. RP Moreno, J (reprint author), Univ Victoria, Dept Phys & Astron, Finnerty Rd, Victoria, BC V8P 1A1, Canada. EM moreno@uvic.ca OI Torrey, Paul/0000-0002-5653-0786 FU Canadian Institute for Theoretical Astrophysics; Natural Sciences and Engineering Research Council of Canada FX The authors thank Andrew Benson, Chris Hayward, Florent Renaud, Ravi Sheth and Else Starkenburg for comments on an earlier draft - and the reviewer, Frederic Bournaud, for a very useful and timely report. JM acknowledges partial funding from the Canadian Institute for Theoretical Astrophysics. JM, AB, SE and DP are funded by the Natural Sciences and Engineering Research Council of Canada. NR 201 TC 22 Z9 22 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 DEC PY 2013 VL 436 IS 2 BP 1765 EP 1786 DI 10.1093/mnras/stt1694 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 258LP UT WOS:000327461100069 ER PT J AU Zahid, HJ Torrey, P Kudritzki, RP Kewley, LJ Dave, R Geller, MJ AF Zahid, H. J. Torrey, P. Kudritzki, R. P. Kewley, L. J. Dave, R. Geller, M. J. TI The slow flow model of dust efflux in local star-forming galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: ISM; galaxies: star-formation ID MASS-METALLICITY RELATION; DIGITAL SKY SURVEY; DISTRIBUTED ELECTRON ENERGIES; OXYGEN ABUNDANCE GRADIENT; ACTIVE GALACTIC NUCLEI; LYMAN-BREAK GALAXIES; H II REGIONS; STELLAR MASS; RADIATION PRESSURE; FORMATION RATES AB We develop a dust efflux model of radiation pressure acting on dust grains which successfully reproduces the relation between stellar mass, dust opacity and star formation rate observed in local star-forming galaxies. The dust content of local star-forming galaxies is set by the competition between the physical processes of dust production and dust loss in our model. The dust loss rate is proportional to the dust opacity and star formation rate. Observations of the relation between stellar mass and star formation rate at several epochs imply that the majority of local star-forming galaxies are best characterized as having continuous star formation histories. Dust loss is a consequence of sustained interaction of dust with the radiation field generated by continuous star formation. Dust efflux driven by radiation pressure rather than dust destruction offers a more consistent physical interpretation of the dust loss mechanism. By comparing our model results with the observed relation between stellar mass, dust extinction and star formation rate in local star-forming galaxies, we are able to constrain the time-scale and magnitude of dust loss. The time-scale of dust loss is long and therefore dust is effluxed in a 'slow flow'. Dust loss is modest in low-mass galaxies but massive galaxies may lose up to 70-80 per cent of their dust over their lifetime. Our slow flow model shows that mass-loss driven by dust opacity and star formation may be an important physical process for understanding normal star-forming galaxy evolution. C1 [Zahid, H. J.; Kudritzki, R. P.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Zahid, H. J.; Geller, M. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Torrey, P.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Kudritzki, R. P.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Kewley, L. J.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Dave, R.] Univ Western Cape, ZA-7535 Cape Town, South Africa. [Dave, R.] South African Astron Observ, ZA-7925 Cape Town, South Africa. [Dave, R.] African Inst Math Sci, ZA-7945 Cape Town, South Africa. [Dave, R.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. RP Zahid, HJ (reprint author), Univ Hawaii Manoa, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM jabran@ifa.hawaii.edu OI Torrey, Paul/0000-0002-5653-0786 FU NSF EARLY CAREER AWARD [AST07-48559]; Alexander-von-Humboldt Foundation FX We thank the anonymous reviewer for carefully reading the manuscript and providing constructive comments. This paper benefitted from useful discussions with Brett Andrews, Charlie Conroy, Lars Hernquist, Phil Hopkins, Josh Barnes and Jessica Werk. We are grateful to Rita Tojeiro for help with the VESPA catalogue. HJZ and LJK gratefully acknowledge support by NSF EARLY CAREER AWARD AST07-48559. HJZ enjoyed the hospitality of Margaret Geller and the Smithsonian Astrophysical Observatory during the completion of this work. RPK acknowledges support by the Alexander-von-Humboldt Foundation and the hospitality of the Max-Planck-Institute for Astrophysics in Garching where part of this work was carried out. NR 116 TC 4 Z9 4 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 DEC PY 2013 VL 436 IS 2 BP 1852 EP 1866 DI 10.1093/mnras/stt1699 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 258LP UT WOS:000327461100073 ER PT J AU Zhao, GB Saito, S Percival, WJ Ross, AJ Montesano, F Viel, M Schneider, DP Manera, M Miralda-Escude, J Palanque-Delabrouille, N Ross, NP Samushia, L Sanchez, AG Swanson, MEC Thomas, D Tojeiro, R Yeche, C York, DG AF Zhao, Gong-Bo Saito, Shun Percival, Will J. Ross, Ashley J. Montesano, Francesco Viel, Matteo Schneider, Donald P. Manera, Marc Miralda-Escude, Jordi Palanque-Delabrouille, Nathalie Ross, Nicholas P. Samushia, Lado Sanchez, Ariel G. Swanson, Molly E. C. Thomas, Daniel Tojeiro, Rita Yeche, Christophe York, Donald G. TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: weighing the neutrino mass using the galaxy power spectrum of the CMASS sample SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmological parameters; large-scale structure of Universe ID DIGITAL SKY SURVEY; PROBE WMAP OBSERVATIONS; OBSERVATIONS COSMOLOGICAL INTERPRETATION; PHOTOMETRIC LUMINOUS GALAXIES; DARK-ENERGY CONSTRAINTS; SOUTH-POLE TELESCOPE; ACOUSTIC-OSCILLATIONS; DATA RELEASE; REDSHIFT-SPACE; NONLINEAR EVOLUTION AB We measure the sum of the neutrino particle masses using the three-dimensional galaxy power spectrum of the Sloan Digital Sky Survey III (SDSS-III) Baryon Oscillation Spectroscopic Survey Data Release 9 the constant MASS (CMASS) galaxy sample. Combined with the cosmic microwave background, supernova and additional baryonic acoustic oscillation data, we find upper 95 per cent confidence limits (CL) of the neutrino mass Sigma m(nu) < 0.340 eV within a flat Lambda cold dark matter (Lambda CDM) background, and Sigma m(nu) < 0.821 eV, assuming a more general background cosmological model. The number of neutrino species is measured to be N-eff = 4.308 +/- 0.794 and 4.032(-0.894)(+0.870) for these two cases, respectively. We study and quantify the effect of several factors on the neutrino measurements, including the galaxy power spectrum bias model, the effect of redshift-space distortion, the cut-off scale of the power spectrum and the choice of additional data. The impact of neutrinos with unknown masses on other cosmological parameter measurements is investigated. The fractional matter density and the Hubble parameter are measured to be Omega(M) = 0.2796 +/- 0.0097, H-0 = 69.72(-0.91)(+0.90) km s(-1) Mpc(-1) (flat ACDM) and Omega(M) = 0.2798(-0.0136)(+0.0132) km s(-1) Mpc(-1) (more general background model). Based on a Chevallier-Polarski-Linder parametrization of the equation-of-state w of dark energy, we find that w = -1 is consistent with observations, even allowing for neutrinos. Similarly, the curvature (K) and the running of the spectral index alpha(s) are both consistent with zero. The tensor-to-scalar ratio is constrained down to r < 0.198 (95 per cent CL, flat Lambda CDM) and r < 0.440 (95 per cent CL, more general background model). C1 [Zhao, Gong-Bo; Percival, Will J.; Ross, Ashley J.; Manera, Marc; Samushia, Lado; Thomas, Daniel; Tojeiro, Rita] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Saito, Shun] Chinese Acad Sci, Natl Astron Observatories, Beijing 100012, Peoples R China. [Zhao, Gong-Bo] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Saito, Shun; Ross, Nicholas P.] Lawrence Berkeley Natl Lab, Berkeley, CA 92420 USA. [Montesano, Francesco; Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Viel, Matteo] INAF Osservatorio Astron Trieste, I-34131 Trieste, Italy. [Viel, Matteo] Natl Inst Nucl Phys, Ist Nazl Fis Nucl, I-34127 Trieste, Italy. [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. [Miralda-Escude, Jordi] Inst Catalana Rec & Estudis Avancats, Barcelona 08010, Catalonia, Spain. [Miralda-Escude, Jordi] Univ Barcelona IEEC, Inst Ciencies Cosmos, Barcelona 08028, Catalonia, Spain. [Palanque-Delabrouille, Nathalie; Yeche, Christophe] CEA, IRFU, Ctr Saclay, F-91191 Gif Sur Yvette, France. [Samushia, Lado] Ilia State Univ, Natl Abastumani Astrophys Observ, GE-1060 Tbilisi, Rep of Georgia. [Swanson, Molly E. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [York, Donald G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [York, Donald G.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. RP Zhao, GB (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England. EM gong-bo.zhao@port.ac.uk OI Miralda-Escude, Jordi/0000-0002-2316-8370; Viel, Matteo/0000-0002-2642-5707 FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; ERC-StG cosmoIGM; University of Arizona; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; Harvard University; Instituto de Astrofisica de Canarias; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX We thank Uros Seljak, Kyle Story, Licia Verde and Yvonne Wong for discussions.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the U.S. Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/.; MV is supported by the ERC-StG cosmoIGM.; 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 117 TC 51 Z9 51 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 DEC PY 2013 VL 436 IS 3 BP 2038 EP 2053 DI 10.1093/mnras/stt1710 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 259PY UT WOS:000327540000010 ER PT J AU Marinucci, A Miniutti, G Bianchi, S Matt, G Risaliti, G AF Marinucci, A. Miniutti, G. Bianchi, S. Matt, G. Risaliti, G. TI A Chandra view of the clumpy reflector at the heart of the Circinus galaxy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Galaxies: active; Galaxies: Seyfert ID X-RAY SPECTROSCOPY; COLD MATTER; LINE; IRON; ACIS; EMISSION; RESOLUTION; DISCOVERY; BEPPOSAX; GAS AB We present a spectral and imaging analysis of the X-ray reflecting structure at the heart of the Circinus galaxy, investigating the innermost regions surrounding the central black hole. By studying an archival 200 ks Chandra Advanced CCD Imaging Spectrometer-S observation, we are able to image the extended clumpy structure responsible for both cold reflection of the primary radiation and neutral iron K alpha line emission. We measure an excess of the equivalent width of the iron K alpha line which follows an axisymmetric geometry around the nucleus on a hundred pc scale. Spectra extracted from different regions confirm a scenario in which the dominant mechanism is the reflection of the nuclear radiation from Compton-thick gas. Significant differences in the equivalent width of the iron K alpha emission line (up to a factor of 2) are found. It is argued that these differences are due to different scattering angles with respect to the line of sight rather than to different iron abundances. C1 [Marinucci, A.; Bianchi, S.; Matt, G.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Marinucci, A.; Miniutti, G.] CSIC INTA, Ctr Astrobiol, Dep Astrofis, E-28691 Madrid, Spain. [Marinucci, A.; Miniutti, G.] LAEFF, E-28691 Madrid, Spain. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, G.] INFN Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Marinucci, A (reprint author), Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy. EM marinucci@fis.uniroma3.it RI Bianchi, Stefano/B-4804-2010; Miniutti, Giovanni/L-2721-2014; OI Bianchi, Stefano/0000-0002-4622-4240; Miniutti, Giovanni/0000-0003-0707-4531; Risaliti, Guido/0000-0002-3556-977X FU Fondazione Angelo Della Riccia FX We thank the anonymous referee for comments and suggestions. We also thank Roberto Maiolino for discussions. AM acknowledges Fondazione Angelo Della Riccia for financial support. We would also like to thank Kazushi Iwasawa and Francesco Massaro for suggestions. NR 39 TC 4 Z9 4 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 3 BP 2500 EP 2504 DI 10.1093/mnras/stt1759 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 259PY UT WOS:000327540000043 ER PT J AU van der Horst, AJ Curran, PA Miller-Jones, JCA Linford, JD Gorosabel, J Russell, DM de Ugarte Postigo, A Lundgren, AA Taylor, GB Maitra, D Guziy, S Belloni, TM Kouveliotou, C Jonker, PG Kamble, A Paragi, Z Homan, J Kuulkers, E Granot, J Altamirano, D Buxton, MM Castro-Tirado, A Fender, RP Garrett, MA Gehrels, N Hartmann, DH Kennea, JA Krimm, HA Mangano, V Ramirez-Ruiz, E Romano, P Wijers, RAMJ Wijnands, R Yang, YJ AF van der Horst, A. J. Curran, P. A. Miller-Jones, J. C. A. Linford, J. D. Gorosabel, J. Russell, D. M. de Ugarte Postigo, A. Lundgren, A. A. Taylor, G. B. Maitra, D. Guziy, S. Belloni, T. M. Kouveliotou, C. Jonker, P. G. Kamble, A. Paragi, Z. Homan, J. Kuulkers, E. Granot, J. Altamirano, D. Buxton, M. M. Castro-Tirado, A. Fender, R. P. Garrett, M. A. Gehrels, N. Hartmann, D. H. Kennea, J. A. Krimm, H. A. Mangano, V. Ramirez-Ruiz, E. Romano, P. Wijers, R. A. M. J. Wijnands, R. Yang, Y. J. TI Broad-band monitoring tracing the evolution of the jet and disc in the black hole candidate X-ray binary MAXI J1659-152 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: individual: MAXI J1659-152; X-rays: binaries; X-rays: individual: MAXI J1659-152 ID SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; QUASI-PERIODIC OSCILLATIONS; GX 339-4; COMPACT JET; XTE J1550-564; HARD STATE; FLUX CORRELATION; TIMING ANALYSIS; ACCRETION DISK; LOW/HARD STATE AB MAXI J1659-152 was discovered on 2010 September 25 as a new X-ray transient, initially identified as a gamma-ray burst, but was later shown to be a new X-ray binary with a black hole as the most likely compact object. Dips in the X-ray light curves have revealed that MAXI J1659-152 is the shortest period black hole candidate identified to date. Here we present the results of a large observing campaign at radio, submillimetre, near-infrared (nIR), optical and ultraviolet (UV) wavelengths. We have combined this very rich data set with the available X-ray observations to compile a broad-band picture of the evolution of this outburst. We have performed broad-band spectral modelling, demonstrating the presence of a spectral break at radio frequencies and a relationship between the radio spectrum and X-ray states. Also, we have determined physical parameters of the accretion disc and put them into context with respect to the other parameters of the binary system. Finally, we have investigated the radio-X-ray and nIR/optical/UV-X-ray correlations up to similar to 3 yr after the outburst onset to examine the link between the jet and the accretion disc, and found that there is no significant jet contribution to the nIR emission when the source is in the soft or intermediate X-ray spectral state, consistent with our detection of the jet break at radio frequencies during these states. C1 [van der Horst, A. J.; Altamirano, D.; Wijers, R. A. M. J.; Wijnands, R.; Yang, Y. J.] Univ Amsterdam, Astron Inst, NL-1098 XH Amsterdam, Netherlands. [Curran, P. A.; Miller-Jones, J. C. A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Linford, J. D.; Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Gorosabel, J.; de Ugarte Postigo, A.; Castro-Tirado, A.] CSIC, IAA, E-18008 Granada, Spain. [Gorosabel, J.] Univ Basque Country, EHU, CSIC,ETS Ingn, IAA,Dept Fis Aplicada 1,Unidad Asociada Grp Plane, E-48013 Bilbao, Spain. [Gorosabel, J.] Basque Fdn Sci, Ikerbasque, E-48008 Bilbao, Spain. [Russell, D. M.] IAC, E-38205 Tenerife, Spain. [de Ugarte Postigo, A.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Lundgren, A. A.] Joint ALMA Observ, Santiago, Chile. [Maitra, D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Guziy, S.] Nikolaev Natl Univ, UA-54030 Nikolayev, Ukraine. [Belloni, T. M.] INAF, Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Kouveliotou, C.] NASA, Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.; Kamble, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Paragi, Z.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Homan, J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kuulkers, E.] European Space Astron Ctr ESA ESAC, Sci Operat Dept, E-28691 Madrid, Spain. [Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel. [Buxton, M. M.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Fender, R. P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Garrett, M. A.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Garrett, M. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Gehrels, N.; Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hartmann, D. H.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Mangano, V.; Romano, P.] INAF, Ist Astrofys Spaziale Fis Cosm Palermo, I-90146 Palermo, Italy. [Ramirez-Ruiz, E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP van der Horst, AJ (reprint author), Univ Amsterdam, Astron Inst, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM a.j.vanderhorst@uva.nl RI Curran, Peter/B-5293-2013; Miller-Jones, James/B-2411-2013; OI Curran, Peter/0000-0003-3003-4626; Miller-Jones, James/0000-0003-3124-2814; Wijers, Ralph/0000-0002-3101-1808; Castro-Tirado, A. J./0000-0003-2999-3563; de Ugarte Postigo, Antonio/0000-0001-7717-5085 FU Commonwealth of Australia; CSIRO; European Research Council via Advanced Investigator [247295]; Australian Research Council's Discovery Projects [DP120102393]; Marie Curie Intra European Fellowship within the Seventh European Community Framework Programme [IEF 274805]; European Commission under the Marie Curie Career Integration Grant programme [FP7-PEOPLE-2012CIG 322307]; Dark Cosmology Centre; DNRF; Unidad Asociada IAACSIC; Ikerbasque Foundation for Science; Spanish research programs [AYA2012-39362-C02-02, AYA2011-24780/ESP, AYA200914000-C03-01/ESP, AYA2010-21887-C04-01]; PRIN-INAF; European Research Council FX We greatly appreciate the support from the VLA, WSRT, APEX, ATCA, GMRT, SMARTS, IAC80, 1.23-m CAHA, BOOTES-2 and BOOTES-3 telescopes in their help with scheduling and obtaining these observations. The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under cooperative agreement with the National Science Foundation. The WSRT is operated by ASTRON (Netherlands Institute for Radio Astronomy) with support from the Netherlands foundation for Scientific Research. APEX is a collaboration between the Max-Plank-Institut fur Radioastronomie, the European Southern Observatory and the Onsala Space Observatory. The ATCA is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The GMRT is operated by the National Center for Radio Astrophysics of the Tata Institute of Fundamental Research. The CTIO 1.3-m telescope is operated by the SMARTS consortium. The Centro Astronomico Hispano Aleman (CAHA) at Calar Alto is operated jointly by the Max-Planck Institut fur Astronomie and the Instituto de Astrofisica de Andalucia (CSIC). The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. The IAC80 is operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. The MAXI/GSC data are provided by RIKEN, JAXA and the MAXI team. 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.; AJvdH and RAMJW acknowledge support from the European Research Council via Advanced Investigator Grant no. 247295. PAC and JCAM-J acknowledge support from the Australian Research Council's Discovery Projects funding scheme under grant DP120102393. DMR acknowledges support from a Marie Curie Intra European Fellowship within the Seventh European Community Framework Programme under contract no. IEF 274805. AdUP acknowledges support by the European Commission under the Marie Curie Career Integration Grant programme (FP7-PEOPLE-2012CIG 322307), and the Dark Cosmology Centre, funded by the DNRF. This work was supported by the Unidad Asociada IAACSIC at the group of planetary science of ETSI-UPV/EHU, by the Ikerbasque Foundation for Science, and by Spanish research programs AYA2012-39362-C02-02, AYA2011-24780/ESP, AYA200914000-C03-01/ESP and AYA2010-21887-C04-01. TMB acknowledges support from grant PRIN-INAF 2012. RW acknowledges support from the European Research Council via a Starting Grant. NR 94 TC 12 Z9 12 U1 0 U2 9 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 3 BP 2625 EP 2638 DI 10.1093/mnras/stt1767 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 259PY UT WOS:000327540000053 ER PT J AU Gruppioni, C Pozzi, F Rodighiero, G Delvecchio, I Berta, S Pozzetti, L Zamorani, G Andreani, P Cimatti, A Ilbert, O Le Floc'h, E Lutz, D Magnelli, B Marchetti, L Monaco, P Nordon, R Oliver, S Popesso, P Riguccini, L Roseboom, I Rosario, DJ Sargent, M Vaccari, M Altieri, B Aussel, H Bongiovanni, A Cepa, J Daddi, E Dominguez-Sanchez, H Elbaz, D Schreiber, NF Genzel, R Iribarrem, A Magliocchetti, M Maiolino, R Poglitsch, A Garcia, AP Sanchez-Portal, M Sturm, E Tacconi, L Valtchanov, I Amblard, A Arumugam, V Bethermin, M Bock, J Boselli, A Buat, V Burgarella, D Castro-Rodriguez, N Cava, A Chanial, P Clements, DL Conley, A Cooray, A Dowell, CD Dwek, E Eales, S Franceschini, A Glenn, J Griffin, M Hatziminaoglou, E Ibar, E Isaak, K Ivison, RJ Lagache, G Levenson, L Lu, N Madden, S Maffei, B Mainetti, G Nguyen, HT O'Halloran, B Page, MJ Panuzzo, P Papageorgiou, A Pearson, CP Perez-Fournon, I Pohlen, M Rigopoulou, D Rowan-Robinson, M Schulz, B Scott, D Seymour, N Shupe, DL Smith, AJ Stevens, JA Symeonidis, M Trichas, M Tugwell, KE Vigroux, L Wang, L Wright, G Xu, CK Zemcov, M Bardelli, S Carollo, M Contini, T Le Fevre, O Lilly, S Mainieri, V Renzini, A Scodeggio, M Zucca, E AF Gruppioni, C. Pozzi, F. Rodighiero, G. Delvecchio, I. Berta, S. Pozzetti, L. Zamorani, G. Andreani, P. Cimatti, A. Ilbert, O. Le Floc'h, E. Lutz, D. Magnelli, B. Marchetti, L. Monaco, P. Nordon, R. Oliver, S. Popesso, P. Riguccini, L. Roseboom, I. Rosario, D. J. Sargent, M. Vaccari, M. Altieri, B. Aussel, H. Bongiovanni, A. Cepa, J. Daddi, E. Dominguez-Sanchez, H. Elbaz, D. Schreiber, N. Foerster Genzel, R. Iribarrem, A. Magliocchetti, M. Maiolino, R. Poglitsch, A. Garcia, A. Perez Sanchez-Portal, M. Sturm, E. Tacconi, L. Valtchanov, I. Amblard, A. Arumugam, V. Bethermin, M. Bock, J. Boselli, A. Buat, V. Burgarella, D. Castro-Rodriguez, N. Cava, A. Chanial, P. Clements, D. L. Conley, A. Cooray, A. Dowell, C. D. Dwek, E. Eales, S. Franceschini, A. Glenn, J. Griffin, M. Hatziminaoglou, E. Ibar, E. Isaak, K. Ivison, R. J. Lagache, G. Levenson, L. Lu, N. Madden, S. Maffei, B. Mainetti, G. Nguyen, H. T. O'Halloran, B. Page, M. J. Panuzzo, P. Papageorgiou, A. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Rigopoulou, D. Rowan-Robinson, M. Schulz, B. Scott, D. Seymour, N. Shupe, D. L. Smith, A. J. Stevens, J. A. Symeonidis, M. Trichas, M. Tugwell, K. E. Vigroux, L. Wang, L. Wright, G. Xu, C. K. Zemcov, M. Bardelli, S. Carollo, M. Contini, T. Le Fevre, O. Lilly, S. Mainieri, V. Renzini, A. Scodeggio, M. Zucca, E. TI The Herschel PEP/HerMES Luminosity Function - I. Probing the Evolution of PACS selected Galaxies to z similar or equal to 4 (vol 432, pg 23, 2013) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Correction DE errata; addenda; galaxies: active; galaxies: evolution; galaxies: starburst; cosmology: observations; infrared: galaxies C1 [Gruppioni, C.; Pozzetti, L.; Zamorani, G.; Dominguez-Sanchez, H.; Bardelli, S.; Zucca, E.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Pozzi, F.; Delvecchio, I.] Univ Bologna, Dipartmento Astron, I-40127 Bologna, Italy. [Rodighiero, G.; Marchetti, L.; Franceschini, A.; Mainetti, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Berta, S.; Lutz, D.; Magnelli, B.; Nordon, R.; Popesso, P.; Rosario, D. J.; Schreiber, N. Foerster; Genzel, R.; Poglitsch, A.; Sturm, E.; Tacconi, L.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Andreani, P.; Iribarrem, A.] ESO, D-85748 Garching, Germany. [Ilbert, O.; Boselli, A.; Buat, V.; Burgarella, D.] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Le Floc'h, E.; Riguccini, L.; Sargent, M.; Aussel, H.; Daddi, E.; Bethermin, M.; Chanial, P.; Madden, S.; Panuzzo, P.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Magnelli, B.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Monaco, P.] Univ Trieste, Dipartmento Fis, Sez Astron, I-34131 Trieste, Italy. [Oliver, S.; Roseboom, I.; Smith, A. J.; Wang, L.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Roseboom, I.; Arumugam, V.; Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Bellville, South Africa. [Altieri, B.; Garcia, A. Perez; Sanchez-Portal, M.; Valtchanov, I.] ESA, Herschel Sci Ctr, E-28692 Madrid, Spain. [Bongiovanni, A.; Cepa, J.; Castro-Rodriguez, N.; Perez-Fournon, I.] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Spain. [Iribarrem, A.] Univ Fed Rio de Janeiro, Observ Valongo, BR-21941 Rio De Janeiro, Brazil. [Magliocchetti, M.] INAF, IFSI, I-00133 Rome, Italy. [Maiolino, R.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Amblard, A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bock, J.; Cooray, A.; Dowell, C. D.; Levenson, L.; Lu, N.; Nguyen, H. T.; Schulz, B.; Shupe, D. L.; Xu, C. K.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Castro-Rodriguez, N.; Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain. [Clements, D. L.; O'Halloran, B.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Conley, A.; Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dwek, E.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Eales, S.; Griffin, M.; Papageorgiou, A.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA 389 UCB, Boulder, CO 80309 USA. [Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Isaak, K.] ESA, ESTEC SRE SA, Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands. [Lagache, G.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France. [Lu, N.; Schulz, B.; Shupe, D. L.] CALTECH, Jet Prop Lab, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Maffei, B.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Page, M. J.; Symeonidis, M.; Tugwell, K. E.] Univ Coll London, Mullard Space Sci Lab, Surrey RH5 6NT, England. [Pearson, C. P.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Scott, D.] Univ British Columbia, Dept Phys & Astrophys, Vancouver, BC V6T 1Z1, Canada. [Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Stevens, J. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Trichas, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vigroux, L.] Univ Paris 06, UPMC, CNRS, Inst Astrophys Paris,UMR 7095, F-75014 Paris, France. [Carollo, M.] ETH Honggerberg, Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Contini, T.] Univ Toulouse, CNRS, Inst Rech Astrophys & Plantol, F-31400 Toulouse, France. [Renzini, A.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Scodeggio, M.] INAF IASF Milano, I-20133 Milan, Italy. RP Gruppioni, C (reprint author), Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy. EM carlotta.gruppioni@oabo.inaf.it RI Daddi, Emanuele/D-1649-2012; Bongiovanni, Angel/J-6176-2012; amblard, alexandre/L-7694-2014; Bardelli, Sandro/O-9369-2015; Zucca, Elena/O-9396-2015; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017; OI Daddi, Emanuele/0000-0002-3331-9590; amblard, alexandre/0000-0002-2212-5395; Bardelli, Sandro/0000-0002-8900-0298; Zucca, Elena/0000-0002-5845-8132; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275; Gruppioni, Carlotta/0000-0002-5836-4056 NR 1 TC 4 Z9 4 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 DEC PY 2013 VL 436 IS 3 BP 2875 EP 2876 DI 10.1093/mnras/stt1748 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 259PY UT WOS:000327540000074 ER PT J AU Tyler, JC Collette, BB Broughton, EA AF Tyler, James C. Collette, Bruce B. Broughton, Elisabeth A. TI Northern Range Extension to Georges Bank for Hollardia hollardi (Reticulate Spikefish) (Triacanthodidae, Tetraodontiformes) SO NORTHEASTERN NATURALIST LA English DT Article AB Hollardia hollardi (Reticulate Spikefish) is reported from two specimens caught in lobster traps along the southern edge of Georges Bank, far north of its previously known northern distribution from southern Florida, the Bahamas, and Bermuda. C1 [Tyler, James C.] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20013 USA. [Collette, Bruce B.] Smithsonian Inst, Natl Museum Nat Hist, Natl Marine Fisheries Serv Systemat Lab, Washington, DC 20013 USA. [Broughton, Elisabeth A.] Northeast Fisheries Sci Ctr, Woods Hole Lab, Woods Hole, MA 02543 USA. RP Tyler, JC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, MRC 159,POB 37012, Washington, DC 20013 USA. EM tylerj@si.edu NR 5 TC 0 Z9 0 U1 0 U2 1 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 DEC PY 2013 VL 20 IS 4 BP N33 EP N36 DI 10.1656/045.020.0421 PG 4 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 283EB UT WOS:000329227100006 ER PT J AU Olson, SL AF Olson, Storrs L. TI A Late Pliocene occurrence of the Thick-billed Murre (Alcidae: Uria lomvia) on St. George Island, Pribilofs, Alaska SO PALEONTOLOGICAL JOURNAL LA English DT Article DE Alcidae; murres; Uria; fossil birds; divergence times; Late Pliocene; Pribilofs ID CHARADRIIFORMES; MIOCENE; AVES AB An associated partial skeleton from the Late Pliocene (3.0-2.6 million years) of St. George Island, Pribilofs, Alaska, is identified as the modern Thick-billed Murre (Uria lomvia). This is the oldest occurrence of either modern species of Uria and probably the oldest Cenozoic bird yet known from Alaska. A split between the two modern species of > 3 million years is in accordance with divergence times derived from DNA sequences. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, NHB MRC 116,POB 37012, Washington, DC 20013 USA. EM olsons@si.edu NR 17 TC 2 Z9 2 U1 1 U2 2 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 0031-0301 EI 1555-6174 J9 PALEONTOL J+ JI Paleontol. J. PD DEC PY 2013 VL 47 IS 11 BP 1365 EP 1368 DI 10.1134/S0031030113110129 PG 4 WC Paleontology SC Paleontology GA 278AA UT WOS:000328859200015 ER PT J AU Clough, GW AF Clough, G. Wayne TI Untitled SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD DEC PY 2013 VL 44 IS 8 BP 8 EP 8 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 286QT UT WOS:000329484500002 ER PT J AU Hines, RE Bader, TJ Graves, GR AF Hines, Richard E. Bader, Troy J. Graves, Gary R. TI Chimney Swifts (Chaetura pelagica) Nest in Tree Cavities in Arkansas SO SOUTHEASTERN NATURALIST LA English DT Article AB We report the first records of tree-nesting Chaentra pelagica (Chimney Swifts) in Arkansas from the White River National Wildlife Refuge (WRNWR). These represent the only well-documented reports of tree-nesting swifts for many decades in the lower Mississippi Valley. The WRNWR may support a large population of tree-nesting swifts. C1 [Bader, Troy J.] ARS, USDA, Stuttgart, AR 72160 USA. [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC 116,POB 37012, Washington, DC 20013 USA. EM gravesg@si.edu NR 7 TC 1 Z9 1 U1 4 U2 11 PU HUMBOLDT FIELD RESEARCH INST PI STEUBEN PA PO BOX 9, STEUBEN, ME 04680-0009 USA SN 1528-7092 J9 SOUTHEAST NAT JI Southeast. Nat. PD DEC PY 2013 VL 12 IS 4 BP N18 EP N20 DI 10.1656/058.012.0414 PG 3 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 283EN UT WOS:000329228600003 ER PT J AU Jehl, JR AF Jehl, Joseph R., Jr. TI Ecological Constraints and Phenotypic Accommodation in One-legged Eared Grebes SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article DE Eared Grebe; ecology; phenotypic flexibility; Podiceps nigricollis ID BLACK-NECKED GREBE; PODICEPS-NIGRICOLLIS; UPRIGHT POSTURE; BIPEDAL GAIT; GOAT BORN; MIGRATION; MAMMALS AB An Eared Grebe (Podiceps nigricollis) that lost a leg in an accident increased muscle mass in its intact leg by 28%. This allowed it to forage, run along the surface to take flight, and survive for about a year before dying in a weather-induced downing. Its ultimate survival probably depended on the species' predilection for hypersaline habitats, where passive invertebrates are abundant and can be captured easily on the surface without the need to dive. Similar phenotypic accommodation may have been realized in other similarly impaired Eared Grebes. However, it seems unlikely to be achieved in other grebe species, particularly fish-eating pursuit divers, which require two intact legs and feet for propulsion and underwater maneuverability. C1 Smithsonian Inst, US Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. RP Jehl, JR (reprint author), Smithsonian Inst, US Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. EM grebe5k@cs.com NR 19 TC 0 Z9 0 U1 2 U2 5 PU WILSON ORNITHOLOGICAL SOC PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 1559-4491 EI 1938-5447 J9 WILSON J ORNITHOL JI Wilson J. Ornithol. PD DEC PY 2013 VL 125 IS 4 BP 829 EP 832 PG 4 WC Ornithology SC Zoology GA 285GJ UT WOS:000329381500018 ER PT J AU Moraux, E Artemenko, S Bouvier, J Irwin, J Ibrahimov, M Magakian, T Grankin, K Nikogossian, E Cardoso, C Hodgkin, S Aigrain, S Movsessian, TA AF Moraux, E. Artemenko, S. Bouvier, J. Irwin, J. Ibrahimov, M. Magakian, T. Grankin, K. Nikogossian, E. Cardoso, C. Hodgkin, S. Aigrain, S. Movsessian, T. A. TI The Monitor Project: stellar rotation at 13 Myr I. A photometric monitoring survey of the young open cluster h Persei SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: rotation; stars: low-mass; open clusters and associations: individual: h Per ID LOW-MASS STARS; PRE-MAIN-SEQUENCE; ANGULAR-MOMENTUM EVOLUTION; ORION NEBULA CLUSTER; TIME-SERIES ANALYSIS; SOLAR-LIKE STARS; T-TAURI STARS; CHI-PERSEI; PLANET FORMATION; VARIABILITY AB Aims. We aim at constraining the angular momentum evolution of low-mass stars by measuring their rotation rates when they begin to evolve freely towards the zero-age main sequence (ZAMS), i.e., after the disk accretion phase has stopped. Methods. We conducted a multisite photometric monitoring of the young open cluster h Persei, which has an age of similar to 13 Myr. The observations were done in the I-band using four different telescopes, and the variability study is sensitive to periods from less than 0.2 day to 20 days. Results. Rotation periods are derived for 586 candidate cluster members over the mass range 0.4 <= M/M-circle dot <= 1.4. The rotation period distribution indicates a slightly higher fraction of fast rotators for the lower mass objects, although the lower and upper envelopes of the rotation period distribution, located respectively at similar to 0.2-0.3 d and similar to 10 d, are remarkably flat over the whole mass range. We combine this period distribution with previous results obtained in younger and older clusters to model the angular momentum evolution of low mass stars during the pre-main sequence (PMS) phase. Conclusions. The h Per cluster provides the first statistically robust estimate of the rotational period distribution of solar-type and lower mass stars at the end of the PMS accretion phase (>= 10 Myr). The results are consistent with models that assume significant core-envelope decoupling during the angular momentum evolution to the ZAMS. C1 [Moraux, E.; Bouvier, J.] UJF Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France. [Artemenko, S.; Grankin, K.] Crimean Astrophys Observ, UA-98409 Crimea, Ukraine. [Irwin, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ibrahimov, M.] Uzbek Acad Sci, Ulugh Bek Astron Inst, Tashkent 700052, Uzbekistan. [Magakian, T.; Nikogossian, E.; Movsessian, T. A.] Byurakan Astrophys Observ, Aragatsotn Reg 0213, Armenia. [Cardoso, C.] Osserv Astron Torino, Ist Nazl Astrofis, I-10025 Pino Torinese, Italy. [Hodgkin, S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Aigrain, S.] Univ Oxford, Oxford OX1 3RH, England. RP Moraux, E (reprint author), UJF Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France. EM stelle.moraux@obs.ujf-grenoble.fr OI Artemenko, Svetlana/0000-0001-8856-1758; Grankin, Konstantin/0000-0001-5707-8448 FU EGIDE ECONET 1886YF program; Academy of Science in Armenia and Ukraine; Agence Nationale de la Recherche [ANR-2011-Blanc-SIMI5-6-020-01, ANR-2010-JCJC-0501-1] FX The authors thank B. Reipurth for giving us access to his CFHT data; K. Zwintz for the pulsation analysis of the two fast rotators; A. Scholz for useful discussion about fast rotation from synchronized binaries; F. Mignard for help with the FAMOUS program; and A. Robin for the use of the Besancon Galactic Model. We are also grateful to the CFHT QSO team for service observing and to J.-C. Cuillandre for the pre-reduction of CFHT data. This work has been supported by the EGIDE ECONET 1886YF program and by bilateral programs with the Academy of Science in Armenia and Ukraine. J. Bouvier and E. Moraux acknowledge funding from the Agence Nationale de la Recherche grants ANR-2011-Blanc-SIMI5-6-020-01 "Toupies: Towards understanding the spin evolution of stars" (http://ipag.osug.fr/Anr_Toupies/) and ANR-2010-JCJC-0501-1 "DESC: Dynamical Evolution of Stellar Clusters" (http://ipag.osug.fr/similar to emoraux/DESC) respectively. NR 68 TC 15 Z9 15 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2013 VL 560 AR A13 DI 10.1051/0004-6361/201321508 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 276MN UT WOS:000328754500013 ER PT J AU Ovelar, MD Min, M Dominik, C Thalmann, C Pinilla, P Benisty, M Birnstiel, T AF Ovelar, M. de Juan Min, M. Dominik, C. Thalmann, C. Pinilla, P. Benisty, M. Birnstiel, T. TI Imaging diagnostics for transitional discs SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE protoplanetary disks; planet-disk interactions; circumstellar matter; methods: observational ID PROTOPLANETARY ACCRETION DISKS; SCATTERED-LIGHT; HD 100546; PRETRANSITIONAL DISKS; CIRCUMSTELLAR DISKS; RADIATIVE-TRANSFER; DUST FILTRATION; INNER REGIONS; SOLID BODIES; GAP EDGES AB Transitional discs are a special type of protoplanetary disc, where planet formation is thought to be taking place. These objects feature characteristic inner cavities and/or gaps of a few tens of AUs in sub-millimetre images of the disc. This signature suggests a localised depletion of matter in the disc that could be caused by planet formation processes. However, recent observations have revealed differences in the structures imaged at different wavelengths in some of these discs. In this paper, we aim to explain these observational differences using self-consistent physical 2D hydrodynamical and dust evolution models of these objects, assuming their morphology is indeed generated by the presence of a planet. We use these models to derive the distribution of gas and dust in a theoretical planet-hosting disc for various planet masses and orbital separations. We then simulate observations of the emitted and scattered light from these models with Very Large Telescope (VLT)/SPHERE-ZIMPOL, Subaru/HiCIAO, VLT/VISIR, and ALMA. We do this by first computing the full resolution images of the models at different wavelengths and then simulating the observations while accounting for the characteristics of each particular instrument. The presence of the planet generates pressure bumps in the gas distribution of the disc, whose characteristics strongly depend on the planet mass and position. These bumps cause large grains to accumulate, while small grains are allowed into inner regions. This spatial differentiation of the grain sizes explains the differences in the observations, since different wavelengths and observing techniques trace different parts of the dust size distribution. Based on this effect, we conclude that the combination of visible/near-infrared polarimetric and sub-mm images is the best strategy to constrain the properties of the unseen planet responsible for the disc structure. C1 [Ovelar, M. de Juan] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Min, M.; Dominik, C.; Thalmann, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Pinilla, P.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Benisty, M.] Inst Planetol & Astrophys Grenoble, F-38400 St Martin Dheres, France. [Birnstiel, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ovelar, MD (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM mjovelar@strw.leidenuniv.nl OI Birnstiel, Tilman/0000-0002-1899-8783 FU EU [284405]; NASA Origins of Solar Systems grant [NNX12AJ04G] FX The authors are grateful to Koen Maaskant, Gijs Mulders, and the "API cookie crew" for helpful and insightful discussions, comments, and suggestions during the course of the study. M.M. acknowledges funding from the EU FP7-2011 under Grant Agreement No. 284405. T.B. acknowledges support from NASA Origins of Solar Systems grant NNX12AJ04G. NR 55 TC 33 Z9 33 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2013 VL 560 AR A111 DI 10.1051/0004-6361/201322218 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 276MN UT WOS:000328754500111 ER PT J AU Schellart, P Nelles, A Buitink, S Corstanje, A Enriquez, JE Falcke, H Frieswijk, W Horandel, JR Horneffer, A James, CW Krause, M Mevius, M Scholten, O ter Veen, S Thoudam, S van den Akker, M Alexov, A Anderson, J Avruch, IM Bahren, L Beck, R Bell, ME Bennema, P Bentum, MJ Bernardi, G Best, P Bregman, J Breitling, F Brentjens, M Broderick, J Bruggen, M Ciardi, B Coolen, A de Gasperin, F de Geus, E de Jong, A de Vos, M Duscha, S Eisloffel, J Fallows, RA Ferrari, C Garrett, MA Griessmeier, J Grit, T Hamaker, JP Hassall, TE Heald, G Hessels, JWT Hoeft, M Holties, HA Iacobelli, M Juette, E Karastergiou, A Klijn, W Kohler, J Kondratiev, VI Kramer, M Kuniyoshi, M Kuper, G Maat, P Macario, G Mann, G Markoff, S McKay-Bukowski, D McKean, JP Miller-Jones, JCA Mol, JD Mulcahy, DD Munk, H Nijboer, R Norden, MJ Orru, E Overeem, R Paas, H Pandey-Pommier, M Pizzo, R Polatidis, AG Renting, A Romein, JW Rottgering, H Schoenmakers, A Schwarz, D Sluman, J Smirnov, O Sobey, C Stappers, BW Steinmetz, M Swinbank, J Tang, Y Tasse, C Toribio, C van Leeuwen, J van Nieuwpoort, R van Weeren, RJ Vermaas, N Vermeulen, R Vocks, C Vogt, C Wijers, RAMJ Wijnholds, SJ Wise, MW Wucknitz, O Yatawatta, S Zarka, P Zensus, A AF Schellart, P. Nelles, A. Buitink, S. Corstanje, A. Enriquez, J. E. Falcke, H. Frieswijk, W. Horandel, J. R. Horneffer, A. James, C. W. Krause, M. Mevius, M. Scholten, O. ter Veen, S. Thoudam, S. van den Akker, M. Alexov, A. Anderson, J. Avruch, I. M. Bahren, L. Beck, R. Bell, M. E. Bennema, P. Bentum, M. J. Bernardi, G. Best, P. Bregman, J. Breitling, F. Brentjens, M. Broderick, J. Brueggen, M. Ciardi, B. Coolen, A. de Gasperin, F. de Geus, E. de Jong, A. de Vos, M. Duscha, S. Eisloeffel, J. Fallows, R. A. Ferrari, C. Garrett, M. A. Griessmeier, J. Grit, T. Hamaker, J. P. Hassall, T. E. Heald, G. Hessels, J. W. T. Hoeft, M. Holties, H. A. Iacobelli, M. Juette, E. Karastergiou, A. Klijn, W. Kohler, J. Kondratiev, V. I. Kramer, M. Kuniyoshi, M. Kuper, G. Maat, P. Macario, G. Mann, G. Markoff, S. McKay-Bukowski, D. McKean, J. P. Miller-Jones, J. C. A. Mol, J. D. Mulcahy, D. D. Munk, H. Nijboer, R. Norden, M. J. Orru, E. Overeem, R. Paas, H. Pandey-Pommier, M. Pizzo, R. Polatidis, A. G. Renting, A. Romein, J. W. Rottgering, H. Schoenmakers, A. Schwarz, D. Sluman, J. Smirnov, O. Sobey, C. Stappers, B. W. Steinmetz, M. Swinbank, J. Tang, Y. Tasse, C. Toribio, C. van Leeuwen, J. van Nieuwpoort, R. van Weeren, R. J. Vermaas, N. Vermeulen, R. Vocks, C. Vogt, C. Wijers, R. A. M. J. Wijnholds, S. J. Wise, M. W. Wucknitz, O. Yatawatta, S. Zarka, P. Zensus, A. TI Detecting cosmic rays with the LOFAR radio telescope SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astroparticle physics; methods: data analysis; instrumentation: interferometers ID EXTENSIVE AIR-SHOWERS; EMISSION; PULSES; SIMULATIONS; CODALEMA; ARRAY AB The low frequency array (LOFAR), is the first radio telescope designed with the capability to measure radio emission from cosmic-ray induced air showers in parallel with interferometric observations. In the first similar to 2 years of observing, 405 cosmic-ray events in the energy range of 10(16)-10(18) eV have been detected in the band from 30-80 MHz. Each of these air showers is registered with up to similar to 1000 independent antennas resulting in measurements of the radio emission with unprecedented detail. This article describes the dataset, as well as the analysis pipeline, and serves as a reference for future papers based on these data. All steps necessary to achieve a full reconstruction of the electric field at every antenna position are explained, including removal of radio frequency interference, correcting for the antenna response and identification of the pulsed signal. C1 [Schellart, P.; Nelles, A.; Buitink, S.; Corstanje, A.; Enriquez, J. E.; Falcke, H.; Horandel, J. R.; Krause, M.; ter Veen, S.; Thoudam, S.; van den Akker, M.; Bahren, L.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Nelles, A.; Falcke, H.; Horandel, J. R.] Nikhef, NL-1098 XG Amsterdam, Netherlands. [Falcke, H.; Frieswijk, W.; Mevius, M.; Bennema, P.; Bentum, M. J.; Bregman, J.; Brentjens, M.; Coolen, A.; de Geus, E.; de Jong, A.; de Vos, M.; Duscha, S.; Fallows, R. A.; Garrett, M. A.; Grit, T.; Hamaker, J. P.; Heald, G.; Hessels, J. W. T.; Holties, H. A.; Klijn, W.; Kondratiev, V. I.; Kuper, G.; Maat, P.; McKean, J. P.; Mol, J. D.; Munk, H.; Nijboer, R.; Norden, M. J.; Orru, E.; Overeem, R.; Pizzo, R.; Polatidis, A. G.; Renting, A.; Romein, J. W.; Schoenmakers, A.; Sluman, J.; Tang, Y.; Toribio, C.; van Leeuwen, J.; van Nieuwpoort, R.; Vermaas, N.; Vermeulen, R.; Vogt, C.; Wijnholds, S. J.; Wise, M. W.; Yatawatta, S.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Falcke, H.; Horneffer, A.; Anderson, J.; Beck, R.; Kohler, J.; Kramer, M.; Kuniyoshi, M.; Mulcahy, D. D.; Sobey, C.; Wucknitz, O.; Zensus, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Buitink, S.; Scholten, O.] Univ Groningen, KVI, NL-9747 AA Groningen, Netherlands. [James, C. W.] Univ Erlangen Nurnberg, ECAP, D-91058 Erlangen, Germany. [Alexov, A.; Hessels, J. W. T.; Markoff, S.; Miller-Jones, J. C. A.; Swinbank, J.; van Leeuwen, J.; Wijers, R. A. M. J.; Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Mevius, M.] Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Garrett, M. A.; Iacobelli, M.; Rottgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Hassall, T. E.; Kramer, M.; Stappers, B. W.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Karastergiou, A.] Univ Oxford, Oxford OX1 3RH, England. [Broderick, J.; Hassall, T. E.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Ciardi, B.] Max Planck Inst Phys & Astrophys, D-85741 Garching, Germany. [Miller-Jones, J. C. A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Best, P.] Univ Edinburgh, Inst Astron, Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, Scotland. [Tasse, C.; Zarka, P.] Observ Paris, CNRS, UMR 8109, LESIA, F-92195 Meudon, France. [Wucknitz, O.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Breitling, F.; Mann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Griessmeier, J.] CNRS, Lab Phys & Chim Environm & Espace, LPC2E, UMR 7328, F-45071 Orleans 02, France. [Avruch, I. M.] SRON Netherlands Insitute Space Res, NL-9700 AV Groningen, Netherlands. [Paas, H.] Univ Groningen, Ctr Informat Technol, NL-9700 AB Groningen, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Bell, M. E.] Univ Sydney, Sydney Inst Astron, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2006, Australia. [Brueggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Kondratiev, V. I.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Bernardi, G.; Smirnov, O.] Rhodes Univ, Dept Phys & Elect, Ctr Radio Astron Tech & Technol RATT, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ferrari, C.; Macario, G.] Univ Nice Sophia Antipolis, CNRS, UMR 7293, Lab Lagrange,Observ Cote Azur, F-06300 Nice, France. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [McKay-Bukowski, D.] Oulu Univ, Sodankyla Geophys Observ, Sodankyla 99600, Finland. [van Nieuwpoort, R.] Netherlands ESci Ctr, NL-1098 XG Amsterdam, Netherlands. [Schwarz, D.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. RP Schellart, P (reprint author), Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. EM P.Schellart@astro.ru.nl RI James, Clancy/G-9178-2015; Miller-Jones, James/B-2411-2013; Ciardi, Benedetta/N-7625-2015; Kondratiev, Vladislav/N-1105-2015; Yatawatta, Sarod/E-6037-2013; OI van Weeren, Reinout/0000-0002-0587-1660; Wijers, Ralph/0000-0002-3101-1808; Buitink, Stijn/0000-0002-6177-497X; James, Clancy/0000-0002-6437-6176; Miller-Jones, James/0000-0003-3124-2814; Kondratiev, Vladislav/0000-0001-8864-7471; Krause, Maria/0000-0001-7595-0914; Schellart, Pim/0000-0002-8324-0880; Swinbank, John/0000-0001-9445-1846; Yatawatta, Sarod/0000-0001-5619-4017; de Gasperin, Francesco/0000-0003-4439-2627 FU Netherlands Research School for Astronomy (NOVA); Samenwerkingsverband Noord-Nederland (SNN); Foundation for Fundamental Research on Matter (FOM); Netherlands Organization for Scientific Research (NWO) [639-041-130]; European Research Council under the European Union [227610]; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX The LOFAR cosmic ray key science project very much acknowledges the scientific and technical support from ASTRON, especially in constructing the LORA particle detectors. We thank the KASCADE Collaboration for providing the scintillator detectors. Furthermore, we acknowledge financial support from the Netherlands Research School for Astronomy (NOVA), the Samenwerkingsverband Noord-Nederland (SNN) and the Foundation for Fundamental Research on Matter (FOM) as well as support from the Netherlands Organization for Scientific Research (NWO), VENI grant 639-041-130. We acknowledge funding from an Advanced Grant of the European Research Council under the European Union's Seventh Framework Program (FP/2007-2013) / ERC Grant Agreement n. 227610. LOFAR, the Low Frequency Array designed and constructed by ASTRON, has facilities in several countries, that are owned by various parties (each with their own funding sources), and that are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. The authors would like to thank both the internal and external referees for carefully reading the manuscript. Chiara Ferrari and Giulia Macario acknowledge financial support by the "Agence Nationale de la Recherche" through grant ANR-09-JCJC-0001-01. NR 20 TC 31 Z9 31 U1 1 U2 9 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2013 VL 560 AR A98 DI 10.1051/0004-6361/201322683 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 276MN UT WOS:000328754500098 ER PT J AU Hong, J Allen, B Grindlay, J Rodrigues, B Ellis, JR Baker, R Barthelmy, S Mao, P Miyasaka, H Apple, J AF Hong, Jaesub Allen, Branden Grindlay, Jonathan Rodrigues, Barbara Ellis, Jon Robert Baker, Robert Barthelmy, Scott Mao, Peter Miyasaka, Hiromasa Apple, Jeff TI Tiled Array of Pixelated CZT Imaging Detectors for ProtoEXIST2 and MIRAX-HXI SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE Astrophysics; semiconductor radiation detectors; telescopes; X-ray detectors ID MISSION AB We have assembled a tiled array (220 cm(2)) of fine pixel (0.6 mm) imaging CZT detectors for a balloon borne wide-field hard X-ray telescope, ProtoEXIST2. ProtoEXIST2 is a prototype experiment for a next generation hard X-ray imager MIRAX-HXI on board Lattes, a spacecraft from the Agencia Espacial Brasilieira. MIRAX will survey the 5 to 200 keV sky of Galactic bulge, adjoining southern Galactic plane and the extragalactic sky with 6' angular resolution. This survey will open a vast discovery space in timing studies of accretion neutron stars and black holes. The ProtoEXIST2 CZT detector plane consists of 64 of 5 mm thick 2 cm 2 cm CZT crystals tiled with a minimal gap. MIRAX will consist of 4 such detector planes, each of which will be imaged with its own coded-aperture mask. We present the packaging architecture and assembly procedure of the ProtoEXIST2 detector. On 2012, Oct 10, we conducted a successful high altitude balloon experiment of the ProtoEXIST1 and 2 telescopes, which demonstrates their technology readiness for space application. During the flight both telescopes performed as well as on the ground. We report the results of ground calibration and the initial results for the detector performance in the balloon flight. C1 [Hong, Jaesub; Allen, Branden; Grindlay, Jonathan; Ellis, Jon Robert] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. [Rodrigues, Barbara] INPE, BR-12227Y01 Sao Jose Dos Campos, SP, Brazil. [Baker, Robert; Barthelmy, Scott] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mao, Peter; Miyasaka, Hiromasa] CALTECH, Pasadena, CA 91125 USA. [Apple, Jeff] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Hong, J (reprint author), Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. EM jaesub@head.cfa.harvard.edu FU NASAGgrants [NNX09AD96G, NNX11AF35G] FX This work was supported by NASAGgrants NNX09AD96G and NNX11AF35G. NR 11 TC 1 Z9 1 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2013 VL 60 IS 6 BP 4610 EP 4617 DI 10.1109/TNS.2013.2283806 PN 2 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 279PI UT WOS:000328971500005 ER PT J AU Ralls, K Sanchez, JN Savage, J Coonan, TJ Hudgens, BR Cypher, BL AF Ralls, Katherine Sanchez, Jessica N. Savage, Jennifer Coonan, Timothy J. Hudgens, Brian R. Cypher, Brian L. TI Social relationships and reproductive behavior of island foxes inferred from proximity logger data SO JOURNAL OF MAMMALOGY LA English DT Article DE estrus; extrapair copulation; home-range overlap; island fox; monogamy; proestrus; proximity loggers; reproductive behavior; social behavior; Urocyon littoralis ID EXTRA-PAIR PATERNITY; UROCYON-LITTORALIS; KIT FOXES; MATING SYSTEM; VULPES-VELOX; SWIFT FOXES; MONOGAMY; MAMMALS; POPULATIONS; ENCOUNTERS AB The social behavior of the smaller fox species is poorly known compared with that of larger and more gregarious canids that can be directly observed. We studied social relationships and reproductive behavior of island foxes (Urocyon littoralis) on San Clemente Island (SCI) and San Miguel Island (SMI), off the coast of Southern California, using proximity logging collars. On both islands, pair members interacted more frequently and spent more time together than other types of dyads. On SCI, a high contact rate identified the same 10 mated pairs that were identified by a high degree of home-range overlap. A high contact rate also identified 3 mated pairs on SMI, 2 of which were associated with large pups 9-10 months old. On SMI, the number of contacts and amount of time that mates spent together per day varied across months and peaked in February, when most conceptions occur. Mates spent much less time together in April to June, the pup-rearing season. More unpaired male female and male male dyads interacted during January and February than in subsequent months. Paired males appeared to guard their mate during the period when she was receptive. The average duration of estrus was approximately 40 h. Paired females were in contact with other males in addition to their mate near the time they were presumably in estrus, and paired males were in contact with other females in addition to their mate. The relatively short duration of estrus, combined with asynchrony of estrus among females, enabled paired males to leave their mate and seek extrapair copulations without risk of cuckoldry. Proximity logging collars provide a new opportunity to learn about these temporal aspects of social and reproductive behavior in canids. C1 [Ralls, Katherine] Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Savage, Jennifer; Coonan, Timothy J.] Channel Isl Natl Pk, Natl Pk Serv, Ventura, CA 93001 USA. [Sanchez, Jessica N.; Hudgens, Brian R.] Inst Wildlife Studies, Arcata, CA 95518 USA. [Sanchez, Jessica N.; Hudgens, Brian R.] Humboldt State Univ, Arcata, CA 95521 USA. [Cypher, Brian L.] Calif State Univ Stanislaus, Endangered Species Recovery Program, Bakersfield, CA 93389 USA. RP Ralls, K (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. EM rallsk@thegrid.net FU Department of Defense Legacy Program; California Department of Fish and Game; Smithsonian Consortium for Understanding and Sustaining a Biodiverse Planet FX We thank M. Booker and the United States Navy for assistance on SCI, P. Alden and the other IWS field crew members for fieldwork on SCI, and the NPS fox technicians for fieldwork on SMI. We are also grateful to J. Ballou for help with data management and preparation of figures; R. Rudolph for help with maps of the study areas; S. Mesnick and N. LaRoche for help with UCINET; and C. Asa for discussions about canid reproduction. G. Roemer provided helpful comments on the manuscript. Funding on SCI was provided through the Department of Defense Legacy Program. Funding on SMI was through grants from the California Department of Fish and Game, and the Smithsonian Consortium for Understanding and Sustaining a Biodiverse Planet. The United States Fish and Wildlife Service granted permission to trap, handle, and radiocollar endangered island foxes on SMI through permit TE086267-0. NR 52 TC 4 Z9 4 U1 8 U2 36 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD DEC PY 2013 VL 94 IS 6 BP 1185 EP 1196 DI 10.1644/13-MAMM-A-057.1 PG 12 WC Zoology SC Zoology GA 280DZ UT WOS:000329010200001 ER PT J AU Sainge, MN Kenfack, D Chuyong, GB AF Sainge, Moses N. Kenfack, David Chuyong, George B. TI Two new species of Afrothismia (Thismiaceae) from southern Cameroon SO KEW BULLETIN LA English DT Article DE Burmanniaceae; Mt Kala; Mt Kupe; myco-heterotrophic plants AB Two new species of Afrothismia are described within the framework of an intended revision of the genus in Cameroon, A. fungiformis from the submontane forest of Mt Kupe and A. pusilla from Mt Kala. The new species are illustrated and the conservation status for both is assessed as Critically Endangered. C1 [Sainge, Moses N.] Trop Plant Explorat Grp TroPEG Cameroon, Ndian Div, Yaounde, Southwest Regio, Cameroon. [Kenfack, David] Smithsonian Inst, Dept Bot, Smithsonian Trop Res Inst, Forest Global Earth Observ ForestGEO, Washington, DC 20013 USA. [Chuyong, George B.] Univ Buea, Dept Bot & Plant Physiol, Buea, Cameroon. RP Sainge, MN (reprint author), Trop Plant Explorat Grp TroPEG Cameroon, Ndian Div, POB 18 Mundemba, Yaounde, Southwest Regio, Cameroon. EM kenfackd@si.edu FU Mohamed Bin Zayed Species Conservation Fund [10251742] FX This study was financially supported by the Mohamed Bin Zayed Species Conservation Fund 2010 (Grant 10251742). Field equipment was provided by IDEAL WILD. Travel expenses for the first author to study specimens at the Missouri Botanical Garden were covered by the Center for Tropical Forest Science (CTFS). The authors are grateful to the Curators of YA, SCA and MO for allowing access to their collections. Special thanks to Dr David Bolger for his logistic support at MO, to the people of Mbulle and Kala villages especially the guides Rei Atabe Epie and Victor Nana for their help during fieldwork and finally, to Alice Tangerini of the Smithsonian National Museum of Natural History for the wonderful illustration. NR 16 TC 1 Z9 1 U1 1 U2 2 PU SPRINGER LONDON LTD PI LONDON PA 236 GRAYS INN RD, 6TH FLOOR, LONDON WC1X 8HL, ENGLAND SN 0075-5974 EI 1874-933X J9 KEW BULL JI Kew Bull. PD DEC PY 2013 VL 68 IS 4 BP 591 EP 597 DI 10.1007/S12225-013-9478-5 PG 7 WC Plant Sciences SC Plant Sciences GA 278QO UT WOS:000328905000005 ER PT J AU Abreu, NM Bullock, ES AF Abreu, Neyda M. Bullock, Emma S. TI Opaque assemblages in CR2 Graves Nunataks (GRA) 06100 as indicators of shock-driven hydrothermal alteration in the CR chondrite parent body SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CM CARBONACEOUS CHONDRITES; FE-NI METAL; TRANSMISSION ELECTRON-MICROSCOPE; AQUEOUS ALTERATION; SOLAR NEBULA; II CHONDRULES; SYSTEM CACO3-MGCO3-FECO3; REFRACTORY INCLUSIONS; PRIMITIVE METEORITES; ANTARCTIC METEORITES AB We have studied the petrologic characteristics of sulfide-metal lodes, polymineralic Fe-Ni nodules, and opaque assemblages in the CR2 chondrite Graves Nunataks (GRA) 06100, one of the most altered CR chondrites. Unlike low petrologic type CR chondrites, alteration of metal appears to have played a central role in the formation of secondary minerals in GRA 06100. Differences in the mineralogy and chemical compositions of materials in GRA 06100 suggest that it experienced higher temperatures than other CR2 chondrites. Mineralogic features indicative of high temperature include: (1) exsolution of Ni-poor and Ni-rich metal from nebular kamacite; (2) formation of sulfides, oxides, and phosphates; (3) changes in the Co/Ni ratios; and (4) carbidization of Fe-Ni metal. The conspicuous absence of pentlandite may indicate that peak temperatures exceeded 600 degrees C. Opaques appear to have been affected by the action of aqueous fluids that resulted in the formation of abundant oxides, Fe-rich carbonates, including endmember ankerite, and the sulfide-silicate-phosphate scorzalite. We suggest that these materials formed via impact-driven metamorphism. Mineralogic features indicative of impact metamorphism include (1) the presence of sulfide-metal lodes; (2) the abundance of polymineralic opaque assemblages with mosaic-like textures; and (3) the presence of suessite. Initial shock metamorphism probably resulted in replacement of nebular Fe-Ni metal in chondrules and in matrix by Ni-rich, Co-rich Fe metal, Al-Ti-Cr-rich alloys, and Fe sulfides, while subsequent hydrothermal alteration produced accessory oxides, phosphates, and Fe carbonates. An extensive network of sulfide-metal veins permitted effective exchange of siderophile elements from pre-existing metal nodules with adjacent chondrules and matrix, resulting in unusually high Fe contents in these objects. C1 [Abreu, Neyda M.] Penn State Univ, Earth Sci Program, Du Bois, PA 15801 USA. [Bullock, Emma S.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Abreu, NM (reprint author), Penn State Univ, Earth Sci Program, Du Bois Campus, Du Bois, PA 15801 USA. EM abreu@psu.edu FU AAS; [NNX11AH10G] FX Funded by NNX11AH10G and AAS grants to NMA. SEM and TEM conducted at the MRI-Penn State. Dr. A. Ruzicka, Dr. L. Keller, and Dr. D. Schrader are thanked for thorough and constructive reviews that greatly improved this manuscript. Dr. S. Singletary is thanked for his contributions to collecting FE-EPMA data. Thanks, for technical assistance, to Mr. M. Angelone, Dr. A. Pesslier, and Dr. T. Clark. Electron microprobe analysis performed at MRI-Penn State, Mineral Sciences-Smithsonian Institution, and ARES-Johnson Space Center. Field-emission EPMA conducted at the Fayetteville State University. Samples provided by MWG. NR 134 TC 7 Z9 7 U1 0 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 DEC PY 2013 VL 48 IS 12 BP 2406 EP 2429 DI 10.1111/maps.12227 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 280IO UT WOS:000329022100003 ER PT J AU Zimbelman, JR Bourke, MC Lorenz, RD AF Zimbelman, J. R. Bourke, M. C. Lorenz, R. D. TI Recent developments in planetary Aeolian studies and their terrestrial analogs SO AEOLIAN RESEARCH LA English DT Review DE Sand dunes; Ripples; Sediment transport; Bedforms; Saltation ID NORTH POLAR-REGION; LARGEST WIND RIPPLES; SALTATION HEIGHT MEASUREMENTS; MEDUSAE FOSSAE FORMATION; SAND TRANSPORT PATHWAYS; MARS ORBITER CAMERA; MERIDIANI-PLANUM; DUNE FIELDS; DUST DEVILS; LAYERED DEPOSITS AB This report summarizes the many advances that have been made in the study of planetary Aeolian processes that have taken place since the first Planetary Dunes Workshop was held in May of 2008, through 2011. Many of the recent studies are facilitated by the wealth and variety of high resolution imaging and spectra data still being returned by multiple spacecraft in orbit and on the surface of Mars, as well as Cassini radar and imaging data for the unique linear dunes on Titan, the large moon of Saturn. The report is divided into seven broad topics: exploring the Martian rock record, the action of the wind, sediment composition, sediment transport, Aeolian bedforms, modification processes, and Titan. Analog studies of terrestrial landforms and processes continue to improve our understanding of the operation of Aeolian processes on other planetary surfaces in each of these topics. Four subjects are likely to see increased emphasis during the coming years: Martian aeolianites, sand compositional diversity, active versus inactive features, and deposition versus erosion. Continued growth of the planetary Aeolian literature is expected as several spacecraft continue to provide high-quality data, including the successful arrival of the Curiosity rover at Mars in August of 2012. Published by Elsevier B.V. C1 [Zimbelman, J. R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Bourke, M. C.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Lorenz, R. D.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA. RP Zimbelman, JR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. EM zimbelmanj@si.edu; mbourke@psi.edu; ralph.lorenz@jhuapl.edu RI Bourke, Mary/I-4387-2012; Lorenz, Ralph/B-8759-2016 OI Bourke, Mary/0000-0002-0424-0322; Lorenz, Ralph/0000-0001-8528-4644 FU NASA [NNX08AK90G] FX The comments and suggestions of Simone Silvestro, Lori Fenton, and the Editor were very helpful during revision of the manuscript. Portions of the work reported here were supported by NASA grant NNX08AK90G (JRZ) from the Mars Data Analysis Program. NR 211 TC 4 Z9 4 U1 2 U2 28 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1875-9637 EI 2212-1684 J9 AEOLIAN RES JI Aeolian Res. PD DEC PY 2013 VL 11 BP 109 EP 126 DI 10.1016/j.aeolia.2013.04.004 PG 18 WC Geography, Physical SC Physical Geography GA 273GT UT WOS:000328524000011 ER PT J AU DeCaluwe, HB Wielebnowski, NC Howard, J Pelican, KM Ottinger, MA AF DeCaluwe, Heather B. Wielebnowski, Nadja C. Howard, JoGayle Pelican, Katharine M. Ottinger, Mary Ann TI Behavioral reactions relate to adrenal activity and temperament in male clouded leopards (Neofelis nebulosa) SO APPLIED ANIMAL BEHAVIOUR SCIENCE LA English DT Article DE Mirror image stimulation test; Behavior tests; Stress; Felids; Anxiety; Fecal hormone monitoring ID CHALLENGE HYPOTHESIS; ECOLOGICAL BASES; TESTOSTERONE; FELIDS; PERSONALITY; RESPONSES; ANXIETY; DOGS AB Due to strong intra-specific aggression and frequent adverse reactions to changes encountered in the captive setting, clouded leopards (Neofelis nebulosa) are particularly difficult to manage as a self-sustaining population in zoos. The aim of this study was to examine the efficacy of behavioral reaction tests in proactively assessing differences in male clouded leopard stress reactivity and temperament. If such tests can be applied to reliably predict which males show stronger adverse behavioral and physiological responses and increased aggression under stressful events, this information can be used for management decisions. Quantitative behavioral and hormonal data were collected before, during, and after a series of brief behavioral reaction tests, which included mirror image stimulation, airhorn, and exposure to unfamiliar people. Keeper questionnaires, validated through correlation with fecal glucocorticoid metabolite concentrations, were used to assess animal temperament ('anxious' vs. 'calm'). Behavioral responses were compared with keeper temperament assessments and fecal androgen metabolite levels to assess individual responses. Results showed that differences in behavior correlated meaningfully and significantly with temperament assessments. During pre-behavior test periods, cats rated as 'anxious' tended to hide in the nest box more often (R-s = 0.80, P = 0.003) and lie down less often (R-s = -0.52, P = 0.04) than those rated as 'calm'. Of the three tests, mirror image stimulation was the most effective in differentiating between 'anxious' and 'calm' cats and identifying potentially aggressive cats. Specifically, 'anxious' cats spent less time interacting with the mirror (R-s =-0.67, P =0.005) while cats with higher mean fecal androgen metabolite levels exhibited the more aggressive behaviors of growling (R-s = 0.60, P = 0.01) and tail flicking (R-s = 0.54, P = 0.03). Our findings demonstrate that behavioral reaction tests may provide a useful indicator of detrimental fear-related and aggressive behaviors in clouded leopards for management decisions. These data also point to potential behavioral neuroendocrine mechanisms that operate in captive felids and contribute to our understanding of the basic biology of these species. (C) 2013 Elsevier B.V. All rights reserved. C1 [DeCaluwe, Heather B.; Ottinger, Mary Ann] Univ Maryland, Dept Anim & Avian Sci, College Pk, MD 20742 USA. [DeCaluwe, Heather B.; Howard, JoGayle] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. [Wielebnowski, Nadja C.] Oregon Zoo, Conservat Res Dept, Portland, OR 97221 USA. [Pelican, Katharine M.] Univ Minnesota, Coll Vet Med, Dept Vet Populat Med, St Paul, MN 55108 USA. RP Pelican, KM (reprint author), Univ Minnesota, Coll Vet Med, Dept Vet Populat Med, 1365 Gortner Ave, St Paul, MN 55108 USA. EM Heather.DeCaluwe@outlook.com; Nadja.Wielebnowski@oregonzoo.org; pelicank@umn.edu; maotting@central.uh.edu FU Association of Zoos and Aquariums [08-801] FX We thank the Conservation Endowment Fund managed by The Association of Zoos and Aquariums (grant # 08-801) for providing financial support for the entire project, as well as the many zookeepers, managers, support staff, and interns at the 12 participating zoological institutions: Alexandria Zoological Park, Audubon Nature Institute, Central Florida Zoo & Botanical Gardens, Cincinnati Zoo & Botanical Garden, Cleveland Metroparks Zoo, Houston Zoo, Minnesota Zoo, Omaha's Henry Doorly Zoo, San Antonio Zoo, Smithsonian Conservation Biology Institute, Zoo Atlanta, and Zoo Miami. NR 32 TC 4 Z9 4 U1 2 U2 63 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1591 EI 1872-9045 J9 APPL ANIM BEHAV SCI JI Appl. Anim. Behav. Sci. PD DEC PY 2013 VL 149 IS 1-4 BP 63 EP 71 DI 10.1016/j.applanim.2013.09.008 PG 9 WC Agriculture, Dairy & Animal Science; Behavioral Sciences; Veterinary Sciences SC Agriculture; Behavioral Sciences; Veterinary Sciences GA 276BW UT WOS:000328724100008 ER PT J AU Williams, SL Davidson, IC Pasari, JR Ashton, GV Carlton, JT Crafton, RE Fontana, RE Grosholz, ED Miller, AW Ruiz, GM Zabin, CJ AF Williams, Susan L. Davidson, Ian C. Pasari, Jae R. Ashton, Gail V. Carlton, James T. Crafton, R. Eliot Fontana, Rachel E. Grosholz, Edwin D. Miller, A. Whitman Ruiz, Gregory M. Zabin, Chela J. TI Managing Multiple Vectors for Marine Invasions in an Increasingly Connected World SO BIOSCIENCE LA English DT Article DE invasive species; marine; vectors; propagule supply; management ID RISK-ASSESSMENT; BALLAST WATER; SPECIES INTRODUCTIONS; BIOLOGICAL INVASIONS; PROPAGULE PRESSURE; EXPERT KNOWLEDGE; AQUARIUM TRADE; CALIFORNIA; SPREAD; MODEL AB Invasive species remain a major environmental problem in the world's oceans. Managing the vectors of introduction is the most effective means of mitigating this problem, but current risk assessments and management strategies are largely focused on species, not on vectors and certainly not on multiple simultaneous vectors. To highlight the issue that multiple vectors contribute to invasions, we analyzed the historical and contemporary contributions of eight maritime vectors to the establishment of nonindigenous species in California, where most species were associated with two to six vectors. Vessel biofouling looms larger than ballast water as a major vector and a management opportunity, but aquaculture risk appears reduced from historic levels. Standardized data on species abundances in each vector are lacking for a robust cross-vector assessment, which could be obtained in a proof-of-concept "vector blitz." Management must shift away from one or two target vectors to coordination across multiple vectors. C1 [Williams, Susan L.; Fontana, Rachel E.] Bodega Bay Marine Lab, Bodega Bay, CA USA. [Williams, Susan L.] Univ Calif Davis, Dept Ecol & Evolut, Davis, CA 95616 USA. [Davidson, Ian C.] Smithsonian Environm Res Ctr, Aquat Bioinvas Res & Policy Inst, Edgewater, MD 21037 USA. [Davidson, Ian C.] Portland State Univ, Environm Sci & Management Dept, Portland, OR 97207 USA. [Pasari, Jae R.] Univ Calif Davis, Bodega Marine Lab, Bodega Bay, CA USA. [Ashton, Gail V.; Zabin, Chela J.] Smithsonian Environm Res Ctr, Tiburon, CA USA. [Carlton, James T.] Williams Coll, Mystic, CT USA. [Carlton, James T.] Williams Myst Maritime Studies Program, Mystic, CT USA. [Crafton, R. Eliot; Fontana, Rachel E.] Univ Calif Davis, Grad Grp, Davis, CA USA. [Fontana, Rachel E.] Natl Sea Grant Knauss Marine Policy, Washington, DC USA. [Grosholz, Edwin D.; Zabin, Chela J.] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA USA. RP Williams, SL (reprint author), Bodega Bay Marine Lab, Bodega Bay, CA USA. EM slwilliams@ucdavis.edu OI Ruiz, Gregory/0000-0003-2499-441X; Davidson, Ian/0000-0002-8729-6048; Miller, Whitman/0000-0003-0484-182X FU California Ocean Protection Council; California Sea Grant Program; Smithsonian Institution; California Ocean Science Trust FX This work was supported by Proposition 84 funds made available to the California Ocean Science Trust by the California Ocean Protection Council, with additional funding from the California Ocean Science Trust, the California Sea Grant Program, and the Smithsonian Institution. We thank many staff members of federal and state agencies for their generous assistance, especially Gary Townsend and Kirsten Ramsey. The Ocean Science Trust staff facilitated and helped shape the work-in particular, Skyli McAfee, Rebecca Gentry, Erin Kramer-Wilt, and Ryan Meyer. We thank Paul Fofonoff, Kim Holzer, and Brian Steves for crucial database support. NR 70 TC 24 Z9 25 U1 13 U2 77 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA SN 0006-3568 EI 1525-3244 J9 BIOSCIENCE JI Bioscience PD DEC PY 2013 VL 63 IS 12 BP 952 EP 966 DI 10.1525/bio.2013.63.12.8 PG 15 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 276AK UT WOS:000328720300010 ER PT J AU Danner, RM Greenberg, RS Danner, JE Kirkpatrick, LT Walters, JR AF Danner, Raymond M. Greenberg, Russell S. Danner, Julie E. Kirkpatrick, Laila T. Walters, Jeffrey R. TI Experimental support for food limitation of a short-distance migratory bird wintering in the temperate zone SO ECOLOGY LA English DT Article DE abundance; body condition; carry-over effects; density dependence; Melospiza georgiana; population limitation; scaled body mass index; short-distance migratory bird; Swamp Sparrow; survival; Winter Food Limitation Hypothesis (WFLH) ID BLACK-CAPPED CHICKADEES; NON-BREEDING SEASON; TIT PARUS-MONTANUS; HABITAT SEGREGATION; NONBREEDING SEASON; NITROGEN LIMITATION; SETOPHAGA-RUTICILLA; ECOSYSTEM RESPONSE; SITE FIDELITY; MIGRANT BIRD AB The Winter Food Limitation Hypothesis (WFLH) states that winter food abundance is a dominant source of population limitation of migratory birds. Evidence is accumulating that long-distance migratory birds wintering in tropical climates have high overwinter survival probabilities and that winter food limitation mainly affects their fitness nonlethally by limiting energetic reserves necessary for successful reproduction. In contrast, the relative roles of direct mortality vs. indirect effects caused by food limitation have not been investigated thoroughly on short-distance migratory birds wintering in temperate zones, where they face thermal challenges. We performed the first test of the WFLH for a temperate migratory bird in the wild on the Swamp Sparrow (Melospiza georgiana), with a replicated plot-wide food supplementation experiment. In contrast to tropical, but consistent with other temperate-wintering migrants, Swamp Sparrows on unmanipulated plots showed relatively low apparent survival across the winter. Following food addition, birds (1) immigrated to experimental plots, which subsequently supported approximate to 50% higher abundances, (2) experienced increases of within-season apparent survival of 8-10%, depending on age/sex class, and (3) had higher-scaled mass index values, all supporting winter food limitation. The last two findings are interrelated because birds with higher scaled mass had higher survival probabilities, further supporting direct effects of winter food limitation. Food limitation of fat reserves might also have indirect effects on reproductive success by limiting migration timing and survival during migration. Increases in scaled mass were higher in females, suggesting that they are disproportionately affected by food limitation, possibly through competition. Based on Robust Design Modeling, we found no support for emigration prior to food addition, indicating that our estimates of mortality are unbiased. C1 [Danner, Raymond M.; Greenberg, Russell S.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Danner, Raymond M.; Danner, Julie E.; Kirkpatrick, Laila T.; Walters, Jeffrey R.] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA. RP Danner, RM (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. EM danner.ray@gmail.com NR 72 TC 5 Z9 5 U1 9 U2 47 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 DEC PY 2013 VL 94 IS 12 BP 2803 EP 2816 DI 10.1890/13-0337.1 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 278ZL UT WOS:000328928300014 PM 24597226 ER PT J AU Pearse, WD Jones, FA Purvis, A AF Pearse, William D. Jones, F. Andrew Purvis, Andy TI Barro Colorado Island's phylogenetic assemblage structure across fine spatial scales and among clades of different ages SO ECOLOGY LA English DT Article DE Barro Colorado Island; Panama; community assembly; community ecology; community phylogenetics; competition; ecophylogenetics; facilitation; habitat filtering; Janzen-Connell effects; phylogenetic scale; spatial scale; tropical forest ID COMMUNITY STRUCTURE; TROPICAL FOREST; ECOLOGICAL COMMUNITIES; NEOTROPICAL FOREST; INTEGRATING PHYLOGENIES; MOLECULAR EVOLUTION; PLANT-COMMUNITIES; DIVERGENCE TIMES; ABSOLUTE RATES; TREE COMMUNITY AB Phylogenetic analyses of assemblage membership provide insight into how ecological communities are structured. However, despite the scale-dependency of many ecological processes, little is known about how assemblage and source pool size definitions can be altered, either alone or together, to provide insight into how ecological diversity is maintained. Moreover, although studies have acknowledged that different clades within an assemblage may be structured by different forces, there has been no attempt to relate the age of a clade to its community phylogenetic structure. Using assemblage phylogenies and spatially explicit data for trees from Barro Colorado Island (BCI), we show that larger assemblages, and assemblages with larger source pools, are more phylogenetically clustered. We argue that this reflects competition, the influence of pathogens, and chance assembly at smaller spatial scales, all operating within the context of wider-scale habitat filtering. A community phylogenetic measure that is based on a null model derived explicitly from trait evolution theory, D, is better able to detect these differences than commonly used measures such as SESMPD and SESMNTD. We also detect a moderate tendency for stronger phylogenetic clustering in younger clades, which suggests that coarse analyses of diverse assemblages may be missing important variation among clades. Our results emphasize the importance of spatial and phylogenetic scale in community phylogenetics and show how varying these scales can help to untangle complex assembly processes. C1 [Pearse, William D.; Purvis, Andy] Univ London Imperial Coll Sci Technol & Med, Dept Life Sci, Ascot SL5 7PY, Berks, England. [Pearse, William D.] NERC Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England. [Jones, F. Andrew] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [Jones, F. Andrew] Smithsonian Trop Res Inst, Unit 0948, Dpo, AA 34002 USA. [Purvis, Andy] Nat Hist Museum, Dept Life Sci, London SW7 5BD, England. RP Pearse, WD (reprint author), Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. EM will.pearse@gmail.com RI Purvis, Andy/A-7529-2008 OI Purvis, Andy/0000-0002-8609-6204 FU National Science Foundation [DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, 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; Celera Foundation FX We are grateful for comments and advice from K. Harms, K. Luckett, C. McInnes, A. Phillimore, A. Pigot, G. Rappaciuolo, and two anonymous reviewers. We are extremely grateful to everyone who assembled the BCI data set. W. D. Pearse was supported by a CASE Ph.D studentship from NERC. The BCI forest dynamics research project was made possible by National Science Foundation grants to Stephen P. Hubbell: DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9615226, DEB-9405933, DEB-9221033, DEB-9100058, DEB-8906869, DEB-8605042, DEB-8206992, DEB-7922197, support from the Center for Tropical Forest Science, the Smithsonian Tropical Research Institute, the John D. and Catherine T. MacArthur Foundation, the Mellon Foundation, the Celera Foundation, and numerous private individuals, and through the hard work of over 100 people from 10 countries over the past two decades. The plot project is part of the Center for Tropical Forest Science, a global network of large-scale demographic tree plots. NR 69 TC 4 Z9 4 U1 7 U2 58 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 DEC PY 2013 VL 94 IS 12 BP 2861 EP 2872 DI 10.1890/12-1676.1 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 278ZL UT WOS:000328928300019 PM 24597231 ER PT J AU Sprenger, M Oelmann, Y Weihermuller, L Wolf, S Wilcke, W Potvin, C AF Sprenger, Matthias Oelmann, Yvonne Weihermueller, Lutz Wolf, Sebastian Wilcke, Wolfgang Potvin, Catherine TI Tree species and diversity effects on soil water seepage in a tropical plantation SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Hydrus-1D; Tree diversity; Mixed-species stands; Seepage; Tropical tree plantation; Water balance model ID EUCALYPTUS-GLOBULUS; FOREST PLANTATIONS; ACACIA-MEARNSII; GRASSLAND PLOTS; COSTA-RICA; PANAMA; BIODIVERSITY; REFORESTATION; PASTURE; EVAPOTRANSPIRATION AB Plant diversity has been shown to influence the water cycle of forest ecosystems by differences in water consumption and the associated effects on groundwater recharge. However, the effects of biodiversity on soil water fluxes remain poorly understood for native tree species plantations in the tropics. Therefore, we estimated soil water fluxes and assessed the effects of tree species and diversity on these fluxes in an experimental native tree species plantation in Sardinilla (Panama). The study was conducted during the wet season 2008 on plots of monocultures and mixtures of three or six tree species. Rainfall and soil water content were measured and evapotranspiration was estimated with the Penman-Monteith equation. Soil water fluxes were estimated using a simple soil water budget model considering water input, output, and soil water and groundwater storage changes and in addition, were simulated using the physically based one-dimensional water flow model Hydrus-1D. In general, the Hydrus simulation did not reflect the observed pressure heads, in that modeled pressure heads were higher compared to measured ones. On the other hand, the results of the water balance equation (WBE) reproduced observed water use patterns well. In monocultures, the downward fluxes through the 200 cm-depth plane were highest below Hura crepitans (6.13 mm day(-1)) and lowest below Luehea seemannii (5.18 mm day(-1)). The average seepage rate in monocultures (+/- SE) was 5.66 +/- 0.18 mm day(-1), and therefore, significantly higher than below six-species mixtures (5.49 +/- 0.04 mm day(-1)) according to overyielding analyses. The three-species mixtures had an average seepage rate of 5.63 +/- 0.12 mm day(-1) and their values did not differ significantly from the average values of the corresponding species in monocultures. Seepage rates were driven by the transpiration of the varying biomass among the plots (r = 0.61, p = 0.017). Thus, a mixture of trees with different growth rates resulted in moderate seepage rates compared to monocultures of either fast growing or slow growing tree species. Our results demonstrate that tree-species specific biomass production and tree diversity are important controls of seepage rates in the Sardinilla plantation during the wet season. (C) 2013 Elsevier B.V. All rights reserved. C1 [Sprenger, Matthias] Univ Koblenz Landau, Inst Integrated Nat Sci, D-56070 Koblenz, Germany. [Oelmann, Yvonne] Univ Tubingen, D-72070 Tubingen, Germany. [Weihermueller, Lutz] Forschungszentrum Julich, Agrosphere Inst, D-52425 Julich, Germany. [Wolf, Sebastian] ETH, Inst Agr Sci, CH-8092 Zurich, Switzerland. [Wolf, Sebastian] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Wilcke, Wolfgang] Univ Bern, Inst Geog, CH-3012 Bern, Switzerland. [Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Potvin, Catherine] McGill Univ, Global Environm & Climate Change Ctr, Montreal, PQ H3A 1B1, Canada. [Potvin, Catherine] Smithsonian Trop Res Inst, Balboa 2072, Panama. RP Sprenger, M (reprint author), Univ Freiburg, Inst Hydrol, Fahnenbergpl 1, D-79098 Freiburg, Germany. EM matthias.sprenger@hydrology.uni-freiburg.de; yvonne.oelmann@uni-tuebingen.de; l.weihermueller@fz-juelich.de; sewolf@ethz.ch; Wolfgang.wilcke@giub.unibe.ch; catherine.potvin@mcgill.ca RI Wolf, Sebastian/B-4580-2010; Sprenger, Matthias/I-6846-2016; Oelmann, Yvonne/J-8730-2016; Wilcke, Wolfgang/P-4620-2016 OI Wolf, Sebastian/0000-0001-7717-6993; Sprenger, Matthias/0000-0003-1221-2767; Oelmann, Yvonne/0000-0003-3513-6568; Wilcke, Wolfgang/0000-0002-6031-4613 FU German Research Foundation [DFG Wi 1601/6-1]; DAAD Promos-Grant; North-South Centre (former Swiss Centre for International Agriculture) of ETH Zurich; Smithsonian Tropical Research Institute (Panama); Natural Sciences and Engineering Council of Canada FX We are grateful to Jose Monteza for maintenance of the experimental plantation and data collection and to Chrystal Healey for installing the piezometers. We thank the Smithsonian Tropical Research Institute, Panama, for its constant support of the Sardinilla Experiment and the processing of research permits. This research was funded by the German Research Foundation (DFG Wi 1601/6-1) which we gratefully acknowledge. Field work of M.S. was funded by the DAAD Promos-Grant. S.W. was funded by the North-South Centre (former Swiss Centre for International Agriculture) of ETH Zurich. C.P. acknowledge the financial support of the Smithsonian Tropical Research Institute (Panama) and a Discovery grant from the Natural Sciences and Engineering Council of Canada. NR 48 TC 5 Z9 5 U1 5 U2 55 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 DEC 1 PY 2013 VL 309 SI SI BP 76 EP 86 DI 10.1016/j.foreco.2013.03.022 PG 11 WC Forestry SC Forestry GA 273HW UT WOS:000328526900009 ER PT J AU Engene, N Paul, VJ Byrum, T Gerwick, WH Thor, A Ellisman, MH AF Engene, Niclas Paul, Valerie J. Byrum, Tara Gerwick, William H. Thor, Andrea Ellisman, Mark H. TI CHEMICALLY RICH SPECIES OF TROPICAL MARINE CYANOBACTERIA OF THE GENUS OKEANIA GEN. NOV (OSCILLATORIALES, CYANOPROKARYOTA) SO JOURNAL OF PHYCOLOGY LA English DT Article DE Lyngbya; Okeania; phylogenetics; secondary metabolites; systematics; taxonomy ID LYNGBYA-MAJUSCULA; SCHIZOTHRIX-CALCICOLA; HARMFUL CYANOBACTERIA; MAXIMUM-LIKELIHOOD; GENETIC DIVERSITY; DRUG DISCOVERY; MICROBIAL MATS; CLIMATE-CHANGE; BIODIVERSITY; INTEGRATION AB An adverse consequence of applying morphology-based taxonomic systems to catalog cyanobacteria, which generally are limited in the number of available morphological characters, is a fundamental underestimation of natural biodiversity. In this study, we further dissect the polyphyletic cyanobacterial genus Lyngbya and delineate the new genus Okeania gen. nov. Okeania is a tropical and subtropical, globally distributed marine group abundant in the shallow-water benthos. Members of Okeania are of considerable ecological and biomedical importance because specimens within this group biosynthesize biologically active secondary metabolites and are known to form blooms in coastal benthic environments. Herein, we describe five species of the genus Okeania: O.hirsuta (type species of the genus), O.plumata, O.lorea, O.erythroflocculosa, and O.comitata, under the provisions of the International Code of Nomenclature for Algae, Fungi, and Plants. All five Okeania species were morphologically, phylogenetically, and chemically distinct. This investigation provides a classification system that is able to identify Okeania spp. and predict their production of bioactive secondary metabolites. C1 [Engene, Niclas; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Byrum, Tara; Gerwick, William H.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biotechnol & Biomed, La Jolla, CA 92093 USA. [Thor, Andrea; Ellisman, Mark H.] Univ Calif San Diego, Natl Ctr Microscopy & Imaging Res, La Jolla, CA 92093 USA. RP Engene, N (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM engenen@si.edu FU Smithsonian Marine Science Network; NMNH Small Grant; Carmabi research station (Curacao); Carrie Bow Cay Field Station (Belize); Mote Marine Laboratory (Summerland Key, FL); Smithsonian Marine Station; Council on International Educational Exchange Research Station (Bonaire); Fogarty International Center [NIH TW006634, NIH NS053398] FX This work was generously supported by the Smithsonian Marine Science Network (NE), and a NMNH Small Grant (VP) supported the collections in Bonaire and Curacao. We gratefully acknowledge Jeff Hunt and Lee Weight at the Laboratories of Analytical Biology of the NMNH for gene sequencing, as well as Hugh Reichardt for general lab assistance. All SEM was done at the USDA Horticultural research laboratory thanks to Julie Piraino. We also thank Amy Wright and Priscilla Winder at Harbor Branch Oceanographic Institute at Florida Atlantic University for usage of LCMS and NMR, as well as Sarath Gunasekera for help with chemical analysis. We are grateful to Athena Economou-Amilli for help with nomenclature. The fieldwork was supported by the Carmabi research station (Curacao), the Carrie Bow Cay Field Station (Belize), the Mote Marine Laboratory (Summerland Key, FL), the Smithsonian Marine Station (Ft. Pierce, FL), and the Council on International Educational Exchange Research Station (Bonaire). We thank Raphael Ritson-Williams, Roger Linington, Marcy Balunas, Brian LaPointe, and Sherry Reed for help with collecting. The field collections were partly supported by the Phycological Society of America's Grants-in-Aid of Research award (NE) MOTE Protect our Reefs Grant program for work in the Florida Keys and the Fogarty International Center funded Panama ICBG program (WHG) (NIH TW006634 and NIH NS053398). We also acknowledge the governments of Panama, Curacao, Belize, and Bonaire for permits to collect cyanobacterial specimens. We also thank Barrett Brooks at the NMNH for help with deposition of type specimens. This is Smithsonian Marine Station at Fort Pierce contribution no. 923 and CCRE contribution no. 943. NR 58 TC 21 Z9 22 U1 1 U2 32 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3646 EI 1529-8817 J9 J PHYCOL JI J. Phycol. PD DEC PY 2013 VL 49 IS 6 BP 1095 EP 1106 DI 10.1111/jpy.12115 PG 12 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 270UD UT WOS:000328343400008 PM 27007630 ER PT J AU Jud, NA Hickey, LJ AF Jud, Nathan A. Hickey, Leo J. TI POTOMACAPNOS APELEUTHERON GEN. ET SP NOV., A NEW EARLY CRETACEOUS ANGIOSPERM FROM THE POTOMAC GROUP AND ITS IMPLICATIONS FOR THE EVOLUTION OF EUDICOT LEAF ARCHITECTURE SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE angiosperm; Cretaceous; eudicot; fossil; Fumarioideae; leaf architecture; Papaveraceae; Potomac Group; Ranunculales ID COMPOUND LEAVES; ECONOMICS SPECTRUM; BASAL ANGIOSPERM; YIXIAN FORMATION; NORTHEAST CHINA; FOSSIL EVIDENCE; PAPAVERACEAE; PHYLOGENY; PLANT; FLOWER AB Premise of the study: Eudicots diverged early in the evolution of flowering plants and now comprise more than 70% of angiosperm species. In spite of the importance of eudicots, our understanding of the early evolution of this clade is limited by a poor fossil record and uncertainty about the order of early phylogenetic branching. The study of Lower Cretaceous fossils can reveal much about the evolution, morphology, and ecology of the eudicots. Methods: Fossils described here were collected from Aptian sediments of the Potomac Group exposed at the Dutch Gap locality in Virginia, USA. Specimens were prepared by degaging, then described and compared with leaves of relevant extant and fossil plants. We conducted a phylogenetic analysis of morphological characters using parsimony while constraining the tree search with the topology found through molecular phylogenetic analyses. Key results: The new species is closely related to ranunculalean eudicots and has leaf architecture remarkably similar to some living Fumarioideae (Papaveraceae). Conclusions: These are the oldest eudicot megafossils from North America, and they show complex leaf architecture reflecting developmental pathways unique to extant eudicots. The morphology and small size of the fossils suggest that they were herbaceous plants, as is seen in other putative early eudicots. The absence of co-occurring tricolpate pollen at Dutch Gap either (1) reflects low preservation probability for pollen of entomophilous herbs or (2) indicates that some leaf features of extant eudicots appeared before the origin of tricolpate pollen. C1 [Jud, Nathan A.] Univ Maryland, Dept Biol Sci, College Pk, MD 20742 USA. [Jud, Nathan A.] Smithsonian Inst, Dept Paleobiol, NHB121, Washington, DC 20013 USA. [Hickey, Leo J.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06520 USA. RP Jud, NA (reprint author), Univ Maryland, Dept Biol Sci, 4140 Plant Sci Bldg, College Pk, MD 20742 USA. EM njud@umd.edu FU University of Maryland Graduate School; Maryland Agricultural Experiment Station; Smithsonian Peter Buck Predoctoral Fellowship FX The authors thank S. L. Wing (Smithsonian) and J. A. Doyle (University of California Berkeley), for valuable discussions, guidance, and comments. We also thank A. Kula (University of Maryland) and B. Atkinson (Oregon State University) for helpful comments on the manuscript. Finally, we thank H. Cochard for her skill in fossil preparation. This research was conducted with support from the University of Maryland Graduate School, the Maryland Agricultural Experiment Station, and a Smithsonian Peter Buck Predoctoral Fellowship for N.A.J. during 2011-2013. NR 95 TC 13 Z9 13 U1 0 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 DEC PY 2013 VL 100 IS 12 BP 2437 EP 2449 DI 10.3732/ajb.1300250 PG 13 WC Plant Sciences SC Plant Sciences GA 269PW UT WOS:000328255400013 PM 24287268 ER PT J AU Karnath, N Prato, L Wasserman, LH Torres, G Skiff, BA Mathieu, RD AF Karnath, N. Prato, L. Wasserman, L. H. Torres, Guillermo Skiff, B. A. Mathieu, R. D. TI ORBITAL PARAMETERS FOR THE TWO YOUNG BINARIES VSB 111 AND VSB 126 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: spectroscopic; stars: pre-main sequence ID CLUSTER NGC 2264; SEQUENCE SPECTROSCOPIC BINARIES; INITIAL MASS FUNCTION; STAR-FORMING REGION; PROPER-MOTION STARS; X-RAY OBSERVATIONS; KECK II TELESCOPE; ECHELLE SPECTROGRAPH; EVOLUTIONARY MODELS; NGC-2264 AB We report orbital parameters for two low-mass, pre-main-sequence, double-lined spectroscopic binaries: VSB 111 and VSB 126. These systems were originally identified as single-lined on the basis of visible-light observations. We obtained high-resolution infrared spectra with the 10 m Keck II telescope, detected absorption lines of the secondary stars, and measured radial velocities of both components in the systems. The visible-light spectra were obtained with the 1.5 m Wyeth reflector at the Oak Ridge Observatory, the 1.5 m Tillinghast reflector at the F. L. Whipple Observatory, and the 4.5 m equivalent Multiple Mirror Telescope. The combination of our visible and infrared observations of VSB 111 leads to a period of 902.1 +/- 0.9 days, an eccentricity of 0.788 +/- 0.008, and a mass ratio of 0.52 +/- 0.05. VSB 126 has a period of 12.9244 +/- 0.0002 days, an eccentricity of 0.18 +/- 0.02, and a mass ratio of 0.29 +/- 0.02. Visible-light photometry, using the 0.8 m telescope at Lowell Observatory, provided rotation periods for the primary stars in both systems: 3.74 +/- 0.02 days for VSB 111 and 5.71 +/- 0.07 days for VSB 126. Both binaries are located in the young, active star-forming cluster NGC 2264 at a distance of similar to 800 pc. The difference in the center-of-mass velocities of the two systems is consistent with the radial velocity gradient seen across NGC 2264. To test the evolutionary models for accuracy and consistency, we compare the stellar properties derived from several sets of theoretical calculations for pre-main-sequence evolution with our dynamical results. C1 [Karnath, N.; Prato, L.; Wasserman, L. H.; Skiff, B. A.] Lowell Observ, Flagstaff, AZ 86001 USA. [Karnath, N.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86001 USA. [Karnath, N.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mathieu, R. D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Karnath, N (reprint author), Lowell Observ, 1400 West Mars Hill Rd, Flagstaff, AZ 86001 USA. EM nicole@lowell.edu; lprato@lowell.edu; lhw@lowell.edu; gtorres@cfa.harvard.edu; bas@lowell.edu; mathieu@astro.wisc.edu FU NSF [AST-1009136, AST-1007992]; NOAO; W. M. Keck Foundation; National Aeronautics and Space Administration FX We are grateful to G. Mace, M. Simon, K. Covey, and J. Patience for useful discussions and comments throughout the progress of this project. We thank Joel Aycock, Gary Puniwai, Gabrelle Saurage, and Cynthia Wilburn for their superb telescope support and Randy Campbell, Al Conrad, Jim Lyke, Barbara Schaefer, and Greg Wirth for their dedicated technical and logistical support. We are grateful to P. Berlind, J. Caruso, R. J. Davis, L. Hartmann, E. Horine, A. Milone, J. Peters, J. Stauffer, R. P. Stefanik, and S. Tokarz for help in obtaining the visible-light spectra of VSB 111 and VSB 126. This work was supported in part by the NSF grant AST-1009136 to L.P.; G.T. acknowledges partial support from NSF grant AST-1007992. 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. Keck telescope time was also granted by NOAO, through the Telescope System Instrumentation Program (TSIP). TSIP is funded by NSF. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This work made use of the SIMBAD database, the VizieR database, the NASA Astrophysics Data System, and the data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the NSF. This publication also made 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. We recognize and acknowledge the significant cultural role that the summit of Mauna Kea plays within the indigenous Hawaiian community and are grateful for the opportunity to conduct observations from this special mountain. NR 64 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2013 VL 146 IS 6 AR 149 DI 10.1088/0004-6256/146/6/149 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262PC UT WOS:000327747700012 ER PT J AU Maciejewski, G Niedzielski, A Wolszczan, A Nowak, G Neuhauser, R Winn, JN Deka, B Adamow, M Gorecka, M Fernandez, M Aceituno, FJ Ohlert, J Errmann, R Seeliger, M Dimitrov, D Latham, DW Esquerdo, GA McKnight, L Holman, MJ Jensen, ELN Kramm, U Pribulla, T Raetz, S Schmidt, TOB Ginski, C Mottola, S Hellmich, S Adam, C Gilbert, H Mugrauer, M Saral, G Popov, V Raetz, M AF Maciejewski, G. Niedzielski, A. Wolszczan, A. Nowak, G. Neuhaeuser, R. Winn, J. N. Deka, B. Adamow, M. Gorecka, M. Fernandez, M. Aceituno, F. J. Ohlert, J. Errmann, R. Seeliger, M. Dimitrov, D. Latham, D. W. Esquerdo, G. A. McKnight, L. Holman, M. J. Jensen, E. L. N. Kramm, U. Pribulla, T. Raetz, St. Schmidt, T. O. B. Ginski, Ch. Mottola, S. Hellmich, S. Adam, Ch. Gilbert, H. Mugrauer, M. Saral, G. Popov, V. Raetz, M. TI CONSTRAINTS ON A SECOND PLANET IN THE WASP-3 SYSTEM SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: individual (WASP-3b); stars: individual (WASP-3) ID ROSSITER-MCLAUGHLIN OBSERVATIONS; TRANSITING EXOPLANET WASP-3B; HOBBY-EBERLY TELESCOPE; OPEN CLUSTERS; ATMOSPHERIC PARAMETERS; ECLIPSING BINARIES; TIMING VARIATIONS; LIGHT CURVES; SPACED DATA; STARS AB There have been previous hints that the transiting planet WASP-3b is accompanied by a second planet in a nearby orbit, based on small deviations from strict periodicity of the observed transits. Here we present 17 precise radial velocity (RV) measurements and 32 transit light curves that were acquired between 2009 and 2011. These data were used to refine the parameters of the host star and transiting planet. This has resulted in reduced uncertainties for the radii and masses of the star and planet. The RV data and the transit times show no evidence for an additional planet in the system. Therefore, we have determined the upper limit on the mass of any hypothetical second planet, as a function of its orbital period. C1 [Maciejewski, G.; Niedzielski, A.; Nowak, G.; Deka, B.; Adamow, M.; Gorecka, M.] Nicholas Copernicus Univ, Ctr Astron, Fac Phys Astron & Informat, PL-87100 Torun, Poland. [Wolszczan, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Wolszczan, A.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Neuhaeuser, R.; Errmann, R.; Seeliger, M.; Raetz, St.; Schmidt, T. O. B.; Ginski, Ch.; Adam, Ch.; Gilbert, H.; Mugrauer, M.] Astrophysikal Inst & Univ Sternwarte, D-07745 Jena, Germany. [Winn, J. N.; McKnight, L.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Fernandez, M.; Aceituno, F. J.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Ohlert, J.] Astron Stiftung Trebur, Michael Adrian Observatorium, D-65468 Trebur, Germany. [Ohlert, J.] Univ Appl Sci, TH Mittelhessen, D-61169 Friedberg, Germany. [Errmann, R.] Abbe Ctr Photon, D-07743 Jena, Germany. [Dimitrov, D.; Popov, V.] Bulgarian Acad Sci, Inst Astron, Sofia 1784, Bulgaria. [Latham, D. W.; Esquerdo, G. A.; Holman, M. J.; Saral, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jensen, E. L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Kramm, U.] Univ Rostock, Inst Phys, D-18051 Rostock, Germany. [Pribulla, T.] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia. [Mottola, S.; Hellmich, S.] German Aerosp Ctr DLR, D-12489 Berlin, Germany. [Saral, G.] Istanbul Univ, Dept Astron & Space Sci, TR-34116 Istanbul, Turkey. [Raetz, M.] Private Observ, D-98587 Herges Hallenberg, Germany. RP Maciejewski, G (reprint author), Nicholas Copernicus Univ, Ctr Astron, Fac Phys Astron & Informat, Grudziadzka 5, PL-87100 Torun, Poland. RI Adamow, Monika/D-1081-2014; Maciejewski, Gracjan/D-6241-2014; Nowak, Grzegorz/H-8234-2014; Dimitrov, Dinko/J-7682-2013; OI Nowak, Grzegorz/0000-0002-7031-7754; Jensen, Eric/0000-0002-4625-7333 FU Polish Ministry of Science and Higher Education [IP2010 023070, 12011 031971, N N203 510938]; Faculty of Physics, Astronomy and Informatics [1627-A]; Polish National Science Centre [UMO-2012/05/N/ST9/03836]; NASA [NNX09AB36G]; Thuringian government [B 515-07010]; German National Science Foundation (Deutsche Forschungsgemeinschaft, DFG) [SPP 1385, NE 515/34-1, NE 515/34-2, NE 515/33-1, NE 515/33-2, NE 515/35-1, NE 515/35-2]; NASA Origins program; MIT UROP office; Kepler mission under NASA; Smithsonian Astrophysical Observatory [NCC2-1390]; DFG [SPP 1385, RE 882/12-1, NE 515/30-1, NE 515/36-1, MU 13-1, NE 515/40-1]; Bulgarian National Science Fund [DO 02-362, DDVU 02/40-2010]; Institute of Astronomy; NAO, Bulgarian Academy of Sciences; PAN/BAN exchange and joint research project "Spectral and photometric studies of variable stars"; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium FX G.M. and G.N. acknowledge the financial support from the Polish Ministry of Science and Higher Education through the Iuventus Plus grants IP2010 023070 and 12011 031971. A.N., G.N., and M.A. are supported by the Polish Ministry of Science and Higher Education grant N N203 510938. G.N. is also supported by the Faculty of Physics, Astronomy and Informatics grant no. 1627-A. M.A. is also supported by the Polish National Science Centre grant no. UMO-2012/05/N/ST9/03836. A.W. is supported by the NASA grant NNX09AB36G. R.N. would like to acknowledge financial support from the Thuringian government (B 515-07010) for the STK CCD camera used in this project. R.N., R.E., S.R., and C.A. would like to thank the German National Science Foundation (Deutsche Forschungsgemeinschaft, 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 & -2, NE 515/33-1 & -2, and NE 515/35-1 & -2. J.N.W. and M.J.H. gratefully acknowledge support from the NASA Origins program and the MIT UROP office. D.W.L. acknowledge partial support from the Kepler mission under NASA Grant and Cooperative Agreement NCC2-1390 with the Smithsonian Astrophysical Observatory. U.K. would like to thank DFG for support in SPP 1385 in project number RE 882/12-1. T.O.B.S. and C.G. would like to thank DFG for support in project NE 515/30-1. M.S. would like to thank DFG for support in project NE 515/36-1. C.G. and M.M. would like to thank DFG for support in project MU 13-1. We would like to thank DFG for travel support to Calar Alto runs in projects NE 515/40-1. D.D. acknowledges the financial support of the projects DO 02-362 and DDVU 02/40-2010 of the Bulgarian National Science Fund, observing grant support from the Institute of Astronomy and NAO, Bulgarian Academy of Sciences, and travel funds from the PAN/BAN exchange and joint research project "Spectral and photometric studies of variable stars." We thank the HET resident astronomers and telescope operators for continuous support. The HET is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universitat Munchen, and Georg-August-Universitat Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. NR 60 TC 11 Z9 11 U1 0 U2 8 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 DEC PY 2013 VL 146 IS 6 AR UNSP 147 DI 10.1088/0004-6256/146/6/147 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262PC UT WOS:000327747700010 ER PT J AU Soffitta, P Barcons, X Bellazzini, R Braga, J Costa, E Fraser, GW Gburek, S Huovelin, J Matt, G Pearce, M Poutanen, J Reglero, V Santangelo, A Sunyaev, RA Tagliaferri, G Weisskopf, M Aloisio, R Amato, E Attina, P Axelsson, M Baldini, L Basso, S Bianchi, S Blasi, P Bregeon, J Brez, A Bucciantini, N Burderi, L Burwitz, V Casella, P Churazov, E Civitani, M Covino, S da Silva, RMC Cusumano, G Dadina, M D'Amico, F De Rosa, A Di Cosimo, S Di Persio, G Di Salvo, T Dovciak, M Elsner, R Eyles, CJ Fabian, AC Fabiani, S Feng, H Giarrusso, S Goosmann, RW Grandi, P Grosso, N Israel, G Jackson, M Kaaret, P Karas, V Kuss, M Lai, D La Rosa, G Larsson, J Larsson, S Latronico, L Maggio, A Maia, J Marin, F Massai, MM Mineo, T Minuti, M Moretti, E Muleri, F O'Dell, SL Pareschi, G Peres, G Pesce, M Petrucci, PO Pinchera, M Porquet, D Ramsey, B Rea, N Reale, F Rodrigo, JM Rozanska, A Rubini, A Rudawy, P Ryde, F Salvati, M de Santiago, VA Sazonov, S Sgro, C Silver, E Spandre, G Spiga, D Stella, L Tamagawa, T Tamborra, F Tavecchio, F Dias, TT van Adelsberg, M Wu, K Zane, S AF Soffitta, Paolo Barcons, Xavier Bellazzini, Ronaldo Braga, Joao Costa, Enrico Fraser, George W. Gburek, Szymon Huovelin, Juhani Matt, Giorgio Pearce, Mark Poutanen, Juri Reglero, Victor Santangelo, Andrea Sunyaev, Rashid A. Tagliaferri, Gianpiero Weisskopf, Martin Aloisio, Roberto Amato, Elena Attina, Primo Axelsson, Magnus Baldini, Luca Basso, Stefano Bianchi, Stefano Blasi, Pasquale Bregeon, Johan Brez, Alessandro Bucciantini, Niccolo Burderi, Luciano Burwitz, Vadim Casella, Piergiorgio Churazov, Eugene Civitani, Marta Covino, Stefano Curado da Silva, Rui Miguel Cusumano, Giancarlo Dadina, Mauro D'Amico, Flavio De Rosa, Alessandra Di Cosimo, Sergio Di Persio, Giuseppe Di Salvo, Tiziana Dovciak, Michal Elsner, Ronald Eyles, Chris J. Fabian, Andrew C. Fabiani, Sergio Feng, Hua Giarrusso, Salvatore Goosmann, Rene W. Grandi, Paola Grosso, Nicolas Israel, Gianluca Jackson, Miranda Kaaret, Philip Karas, Vladimir Kuss, Michael Lai, Dong La Rosa, Giovanni Larsson, Josefin Larsson, Stefan Latronico, Luca Maggio, Antonio Maia, Jorge Marin, Frederic Massai, Marco Maria Mineo, Teresa Minuti, Massimo Moretti, Elena Muleri, Fabio O'Dell, Stephen L. Pareschi, Giovanni Peres, Giovanni Pesce, Melissa Petrucci, Pierre-Olivier Pinchera, Michele Porquet, Delphine Ramsey, Brian Rea, Nanda Reale, Fabio Rodrigo, Juana Maria Rozanska, Agata Rubini, Alda Rudawy, Pawel Ryde, Felix Salvati, Marco de Santiago, Valdivino Alexandre, Jr. Sazonov, Sergey Sgro, Carmelo Silver, Eric Spandre, Gloria Spiga, Daniele Stella, Luigi Tamagawa, Toru Tamborra, Francesco Tavecchio, Fabrizio Dias, Teresa Teixeira van Adelsberg, Matthew Wu, Kinwah Zane, Silvia TI XIPE: the X-ray imaging polarimetry explorer SO EXPERIMENTAL ASTRONOMY LA English DT Article DE Astronomy; X-ray; Polarimetry ID GAS PIXEL DETECTOR; ACCRETING BLACK-HOLES; SOLAR-FLARES; GALACTIC-CENTER; NEUTRON-STARS; CRAB-NEBULA; COMPTON-SCATTERING; QUANTUM-GRAVITY; POLARIZATION MEASUREMENTS; CHANDRA OBSERVATIONS AB X-ray polarimetry, sometimes alone, and sometimes coupled to spectral and temporal variability measurements and to imaging, allows a wealth of physical phenomena in astrophysics to be studied. X-ray polarimetry investigates the acceleration process, for example, including those typical of magnetic reconnection in solar flares, but also emission in the strong magnetic fields of neutron stars and white dwarfs. It detects scattering in asymmetric structures such as accretion disks and columns, and in the so-called molecular torus and ionization cones. In addition, it allows fundamental physics in regimes of gravity and of magnetic field intensity not accessible to experiments on the Earth to be probed. Finally, models that describe fundamental interactions (e.g. quantum gravity and the extension of the Standard Model) can be tested. We describe in this paper the X-ray Imaging Polarimetry Explorer (XIPE), proposed in June 2012 to the first ESA call for a small mission with a launch in 2017. The proposal was, unfortunately, not selected. To be compliant with this schedule, we designed the payload mostly with existing items. The XIPE proposal takes advantage of the completed phase A of POLARIX for an ASI small mission program that was cancelled, but is different in many aspects: the detectors, the presence of a solar flare polarimeter and photometer and the use of a light platform derived by a mass production for a cluster of satellites. XIPE is composed of two out of the three existing JET-X telescopes with two Gas Pixel Detectors (GPD) filled with a He-DME mixture at their focus. Two additional GPDs filled with a 3-bar Ar-DME mixture always face the Sun to detect polarization from solar flares. The Minimum Detectable Polarization of a 1 mCrab source reaches 14 % in the 2-10 keV band in 10(5) s for pointed observations, and 0.6 % for an X10 class solar flare in the 15-35 keV energy band. The imaging capability is 24 arcsec Half Energy Width (HEW) in a Field of View of 14.7 arcmin x 14.7 arcmin. The spectral resolution is 20 % at 6 keV and the time resolution is 8 mu s. The imaging capabilities of the JET-X optics and of the GPD have been demonstrated by a recent calibration campaign at PANTER X-ray test facility of the Max-Planck-Institut fur extraterrestrische Physik (MPE, Germany). XIPE takes advantage of a low-earth equatorial orbit with Malindi as down-link station and of a Mission Operation Center (MOC) at INPE (Brazil). The data policy is organized with a Core Program that comprises three months of Science Verification Phase and 25 % of net observing time in the following 2 years. A competitive Guest Observer program covers the remaining 75 % of the net observing time. C1 [Soffitta, Paolo; Costa, Enrico; De Rosa, Alessandra; Di Cosimo, Sergio; Di Persio, Giuseppe; Fabiani, Sergio; Muleri, Fabio; Rubini, Alda] IAPS INAF, I-00133 Rome, Italy. [Barcons, Xavier] Inst Fis Cantabria CSIC UC, Santander 39005, Spain. [Bellazzini, Ronaldo; Bregeon, Johan; Brez, Alessandro; Kuss, Michael; Latronico, Luca; Minuti, Massimo; Pesce, Melissa; Pinchera, Michele; Sgro, Carmelo; Spandre, Gloria] INFN Pisa, I-56127 Pisa, Italy. [Braga, Joao; D'Amico, Flavio; de Santiago, Valdivino Alexandre, Jr.] INPE Div Astrofs, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [Fraser, George W.] Univ Leicester, Dept Phys & Astron, Space Res Ctr, Leicester LE1 7RH, Leics, England. [Gburek, Szymon] Polish Acad Sci, Space Res Ctr, Solar Phys Div, PL-51622 Wroclaw, Poland. [Huovelin, Juhani] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland. [Matt, Giorgio; Bianchi, Stefano; Tamborra, Francesco] Univ Studi Roma Tre, Dipartimento Fis E Amaldi, I-00146 Rome, Italy. [Pearce, Mark; Axelsson, Magnus; Jackson, Miranda; Larsson, Josefin; Larsson, Stefan; Moretti, Elena; Ryde, Felix] Royal Inst Technol, Dept Phys, KTH, Stockholm, Sweden. [Pearce, Mark; Axelsson, Magnus; Jackson, Miranda; Larsson, Josefin; Larsson, Stefan; Moretti, Elena; Ryde, Felix] AlbaNova Univ Ctr, Oskar Klein Ctr Cosmoparticle Phys, Stockholm, Sweden. [Poutanen, Juri] Univ Oulu, Dept Phys, Astron Div, Oulu 90014, Finland. [Reglero, Victor; Rodrigo, Juana Maria] Univ Valencia Astron & Astrofis, Inst Ciencias Mat, Burjassot 46100, Spain. [Santangelo, Andrea] Iniversitat Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Sunyaev, Rashid A.; Churazov, Eugene] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Tagliaferri, Gianpiero; Basso, Stefano; Civitani, Marta; Covino, Stefano; Pareschi, Giovanni; Spiga, Daniele; Tavecchio, Fabrizio] INAF Osservatorio Astron Brera, I-23807 Merate, Lc, Italy. [Weisskopf, Martin; Elsner, Ronald; O'Dell, Stephen L.; Ramsey, Brian] NASA Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Attina, Primo] Thales Alenia Space Italia S P A, I-10146 Turin, Italy. [Baldini, Luca; Massai, Marco Maria] Univ Pisa, Dipartimento Fis, I-56127 Pisa, Italy. [Baldini, Luca; Massai, Marco Maria] INFN Pisa, Dipartimento Fis, I-56127 Pisa, Italy. [Aloisio, Roberto; Amato, Elena; Blasi, Pasquale; Bucciantini, Niccolo; Salvati, Marco] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Burderi, Luciano] Univ Cagliari, Dipartimento Fis, I-09042 Cagliari, Italy. [Burwitz, Vadim] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Burwitz, Vadim] Panter Xray Test Facil, D-82061 Neuried, Germany. [Casella, Piergiorgio; Israel, Gianluca; Stella, Luigi] INAF Osservatorio Astrofis Roma, I-00040 Rome, Italy. [Curado da Silva, Rui Miguel; Maia, Jorge; Dias, Teresa Teixeira] Univ Coimbra, Dept Fis, P-3004516 Coimbra, Portugal. [Cusumano, Giancarlo; Giarrusso, Salvatore; La Rosa, Giovanni; Mineo, Teresa] INAF IASF Palermo, I-90146 Palermo, Italy. [Dadina, Mauro; Grandi, Paola] INAF IASF Bologna, I-40129 Bologna, Italy. [Di Salvo, Tiziana; Peres, Giovanni; Reale, Fabio] Univ Studi Palermo, DiFC, I-90123 Palermo, Italy. [Dovciak, Michal; Karas, Vladimir] Acad Sci Czech Republic, Astron Inst, Prague 14131, Czech Republic. [Eyles, Chris J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Feng, Hua] Tsinghua Univ, Dept Engn Phys, Beijing 100084, Peoples R China. [Feng, Hua] Tsinghua Univ, Ctr Astrophys, Beijing 100084, Peoples R China. [Fabian, Andrew C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Goosmann, Rene W.; Grosso, Nicolas; Marin, Frederic; Porquet, Delphine] Observ Astronom Strasbourg, F-67000 Strasbourg, France. [Kaaret, Philip] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Lai, Dong] Cornell Univ, Ithaca, NY 14853 USA. [Maggio, Antonio] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Petrucci, Pierre-Olivier] UJF Grenoble 1, IPAG, CNRS INSU, UMR 5274, F-38041 Grenoble, France. [Rea, Nanda] Fac Ciencies, CSIC IEEC, Inst Space Sci, Barcelona 08193, Spain. [Rozanska, Agata] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Rudawy, Pawel] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Sazonov, Sergey] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [Sazonov, Sergey] Moscow Phys Tech Inst, Dolgoprudnyi 141700, Russia. [Silver, Eric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tamagawa, Toru] RIKEN, Wako, Saitama 3510198, Japan. [van Adelsberg, Matthew] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Wu, Kinwah; Zane, Silvia] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Soffitta, P (reprint author), IAPS INAF, Via Fosso Cavaliere 100, I-00133 Rome, Italy. EM paolo.soffitta@iaps.inaf.it RI Bianchi, Stefano/B-4804-2010; Karas, Vladimir/C-1559-2013; Dovciak, Michal/F-4258-2014; Barcons, Xavier/L-3335-2014; Marin, Frederic/A-3737-2015; Churazov, Eugene/A-7783-2013; Rea, Nanda/I-2853-2015; Maia, Jorge/K-1344-2015; Aloisio, Roberto/I-9533-2012; Blasi, Pasquale/O-9345-2015; Amato, Elena/P-2938-2015; Maggio, Antonio/P-5700-2015; Poutanen, Juri/H-6651-2016; Sgro, Carmelo/K-3395-2016; OI Bianchi, Stefano/0000-0002-4622-4240; Karas, Vladimir/0000-0002-5760-0459; Dovciak, Michal/0000-0003-0079-1239; Barcons, Xavier/0000-0003-1081-8861; Rea, Nanda/0000-0003-2177-6388; Maia, Jorge/0000-0002-9314-1763; Aloisio, Roberto/0000-0003-0161-5923; Blasi, Pasquale/0000-0003-2480-599X; Amato, Elena/0000-0002-9881-8112; Maggio, Antonio/0000-0001-5154-6108; Poutanen, Juri/0000-0002-0983-0049; Curado da Silva, Rui Miguel/0000-0002-9961-965X; Spiga, Daniele/0000-0003-1163-7843; Burderi, Luciano/0000-0001-5458-891X; Pareschi, Giovanni/0000-0003-3967-403X; Dias, Teresa/0000-0001-5101-4902; Bucciantini, Niccolo'/0000-0002-8848-1392; Porquet, Delphine/0000-0001-9731-0352; GIARRUSSO, SALVATORE/0000-0002-0738-2940; O'Dell, Stephen/0000-0002-1868-8056; Mineo, Teresa/0000-0002-4931-8445; Soffitta, Paolo/0000-0002-7781-4104; Dadina, Mauro/0000-0002-7858-7564; Cusumano, Giancarlo/0000-0002-8151-1990; Pesce-Rollins, Melissa/0000-0003-1790-8018; Grandi, Paola/0000-0003-1848-6013; Costa, Enrico/0000-0003-4925-8523; Israel, GianLuca/0000-0001-5480-6438; Sgro', Carmelo/0000-0001-5676-6214; PERES, Giovanni/0000-0002-6033-8180; Reale, Fabio/0000-0002-1820-4824; /0000-0003-0065-2933; Axelsson, Magnus/0000-0003-4378-8785; Casella, Piergiorgio/0000-0002-0752-3301; Moretti, Elena/0000-0001-5477-9097; Covino, Stefano/0000-0001-9078-5507; Baldini, Luca/0000-0002-9785-7726; Tagliaferri, Gianpiero/0000-0003-0121-0723; Tavecchio, Fabrizio/0000-0003-0256-0995 FU ASI; INAF; INFN FX This work is partially funded by ASI, INAF and INFN. NR 148 TC 34 Z9 34 U1 10 U2 40 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 EI 1572-9508 J9 EXP ASTRON JI Exp. Astron. PD DEC PY 2013 VL 36 IS 3 BP 523 EP 567 DI 10.1007/s10686-013-9344-3 PG 45 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 269BB UT WOS:000328214000005 ER PT J AU Allured, R McEntaffer, RT AF Allured, Ryan McEntaffer, Randall T. TI Analytical alignment tolerances for off-plane reflection grating spectroscopy SO EXPERIMENTAL ASTRONOMY LA English DT Article DE Diffraction gratings; X-ray spectroscopy; Alignment tolerances AB Future NASA X-ray Observatories will shed light on a variety of high-energy astrophysical phenomena. Off-plane reflection gratings can be used to provide high throughput and spectral resolution in the 0.3-1.5 keV band, allowing for unprecedented diagnostics of energetic astrophysical processes. A grating spectrometer consists of multiple aligned gratings intersecting the converging beam of a Wolter-I telescope. Each grating will be aligned such that the diffracted spectra overlap at the focal plane. Misalignments will degrade both spectral resolution and effective area. In this paper we present an analytical formulation of alignment tolerances that define grating orientations in all six degrees of freedom. We verify our analytical results with raytrace simulations to fully explore the alignment parameter space. We also investigate the effect of misalignments on diffraction efficiency. C1 [Allured, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McEntaffer, Randall T.] Univ Iowa, Iowa City, IA USA. RP Allured, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rallured@cfa.harvard.edu FU NASA [NNX12AF23G] FX The authors acknowledge support from NASA Strategic Astrophysics Technology grant, NNX12AF23G. The commercial software PCGrate-S(X) v.6.1 (c) (I.I.G. Inc.) was also crucial in the completion of this work. NR 11 TC 8 Z9 8 U1 0 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 EI 1572-9508 J9 EXP ASTRON JI Exp. Astron. PD DEC PY 2013 VL 36 IS 3 BP 661 EP 677 DI 10.1007/s10686-013-9349-y PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 269BB UT WOS:000328214000009 ER PT J AU Park, MG Kim, S Shin, EY Yih, W Coats, DW AF Park, Myung Gil Kim, Sunju Shin, Eun-Young Yih, Wonho Coats, D. Wayne TI Parasitism of harmful dinoflagellates in Korean coastal waters SO HARMFUL ALGAE LA English DT Article DE Amoebophrya; Biological control; Genetic diversity; Harmful algal blooms; Host specificity; Parvilucifera infectans ID SP-NOV PERKINSOZOA; GENETIC DIVERSITY; AMOEBOPHRYA SP; RED-TIDE; HOST-SPECIFICITY; CHESAPEAKE BAY; 2 STRAINS; IN-VITRO; GYMNODINIUM-SANGUINEUM; POPULATION-DYNAMICS AB Two parasites of dinoflagellates, the perkinsid Parvilucifera infectans and the parasitic dinoflagellate Amoebophrya ceratii, are known to infect numerous dinoflagellate hosts, including some toxic and harmful algal bloom species. These parasites have received particular attention, due to growing interest in developing "natural" biological approaches for controlling harmful red tides. Nonetheless, few published accounts of dinoflagellate parasitism are available for coastal waters of Asia, although that region is strongly influenced by dinoflagellate red tides. In this paper, our goals were (1) to review available information (i.e. distribution and seasonality) on Amoebophrya that infect dinoflagellates of Korean coastal waters, providing novel observation where possible, (2) set data (i.e. biology and genetic diversity) for Korean Amoebophrya within a global context, and (3) discuss the implications of available findings on the potential use of Amoebophrya as a biological control agent of harmful dinoflagellates. (C) 2013 Elsevier B.V. All rights reserved. C1 [Park, Myung Gil] Chonnam Natl Univ, LOHABE, Dept Oceanog, Kwangju 500757, South Korea. [Kim, Sunju] Chonnam Natl Univ, Res Inst Basic Sci, Kwangju 500757, South Korea. [Shin, Eun-Young] Microalgal Taxon Inst Korea, Seoul 135839, South Korea. [Yih, Wonho] Kunsan Natl Univ, Dept Oceanog, Gunsan 573701, South Korea. [Coats, D. Wayne] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Park, MG (reprint author), Chonnam Natl Univ, LOHABE, Dept Oceanog, Kwangju 500757, South Korea. EM mpark@chonnam.ac.kr; sunjukim75@gmail.com FU Mid-career Researcher Program through NRF; Ministry of Science, ICU and Future Planning [2011-0015820]; Long-term change of structure and function in marine ecosystems of Korea program of KIMST/MOF; National Research Foundation of Korea; Korean Government (Ministry of Science, ICT and Future Planning) [NRF-C1ABA001-2010-0020700] FX This work was supported in part by Mid-career Researcher Program through NRF grant funded by the Ministry of Science, ICU and Future Planning (2011-0015820) (M.G.P.) and Long-term change of structure and function in marine ecosystems of Korea program of KIMST/MOF and the National Research Foundation of Korea Grant funded by the Korean Government (Ministry of Science, ICT and Future Planning) (NRF-C1ABA001-2010-0020700) (W.Y.). NR 96 TC 13 Z9 13 U1 0 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1568-9883 EI 1878-1470 J9 HARMFUL ALGAE JI Harmful Algae PD DEC PY 2013 VL 30 SU 1 SI SI BP S62 EP S74 DI 10.1016/j.hal.2013.10.007 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 270FU UT WOS:000328305100007 ER PT J AU Strong, EE Bouchet, P AF Strong, Ellen E. Bouchet, Philippe TI Cryptic yet colorful: anatomy and relationships of a new genus of Cerithiidae (Caenogastropoda, Cerithioidea) from coral reef drop-offs SO INVERTEBRATE BIOLOGY LA English DT Article DE anatomy; DNA; phylogeny; systematics; Bittiinae ID PHYLOGENETIC TREES; SPECIES RICHNESS; PROSOBRANCHIA; MORPHOLOGY; SEQUENCES; UTILITY AB Cerithium koperbergi is a rare gastropod of the family Cerithiidae from the tropical Indo-West Pacific. The species has a small, unusual shell and often inhabits deeper water, fore-reef habitats that are atypical for the genus. Anatomical investigations reveal that it possesses a combination of features heretofore considered diagnostic of two main cerithiid subfamilies: Cerithiinae and Bittiinae. While the shell is bittiine, the animal lacks mesopodial pedal glands and possesses a seminal receptacle (vs. a spermatophore bursa) in the lateral lamina of the oviduct, which are considered to be cerithiine features. Re-evaluation of the anatomy of Bittium reticulatum, the type species of Bittium, indicates the defining anatomical difference in oviduct anatomy between the two subfamilies does not stand up to closer scrutiny. Partial mitochondrial cytochrome c oxidase I (COI) sequences support the interpretation that C. koperbergi is a species complex around the western Pacific rim comprising three divergent mitochondrial lineages. Bayesian analysis of partial mitochondrial COI and 16S rRNA sequences confirm the placement of the C. koperbergi complex within a monophyletic Bittiinae, despite the apparent absence of a unifying anatomical feature. Species in the C. koperbergi complex are here united in Pictorium nov. gen. and two species are described as new. It is hypothesized that features of the midgut may be diagnostic of the Bittiinae, but more comparative data are needed. C1 [Strong, Ellen E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Bouchet, Philippe] Museum Natl Hist Nat, F-75005 Paris, France. RP Strong, EE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. EM stronge@si.edu FU Total Foundation; Stavros Niarchos Foundation; French Ministry of Foreign Affairs FX The bulk of the MNHN material used in this study was collected primarily during the LI-FOU 2000, PANGLAO 2004, and SANTO 2006 marine biodiversity surveys. These expeditions were made possible by grants from the Total Foundation, Stavros Niarchos Foundation, and the French Ministry of Foreign Affairs, and in-kind support from Institut de Recherche pour le Developpement (IRD) and University of San Carlos, Cebu City (USC). We thank Stefano Schiaparelli and Marco Oliverio for their skilful contribution to sampling in the field, and Philippe Maestrati for coordinating the post-expedition family sorting. In addition, we thank the following for assistance with specimens under their care: Frank Wesselingh (Naturalis) for photos of the type of Cerithium koperbergi; Robert Moolenbeek (ZMA) for the loan of material from the former Schepman collection and the Siboga Expedition; Virginie Heros and Barbara Buge (MNHN), Ian Loch and Alison Miller (AM), Paul Callomon and Gary Rosenberg (ANSP), and Shirley Slack-Smith and Aaron Cosgrove-Wilke (WAM) for research support during visits and assistance with loans of specimens. We are also grateful to Taiji Kurozumi for photos of specimens of Pictorium koperbergi from Okinawa; Manuel Amorim and Paulo Granja of Deep'N Reef Shells for providing us with a specimen of P. versicolor trawled in Mozambique; and He Jing of shellspecimen. net for specimens of P. versicolor from the South China Sea. We are also grateful to Marilyn Schotte (USNM) for preparing the histological sections and for inking the anatomical drawings, and especially to Andrea Ormos and Robin Turner (Laboratories for Analytical Biology, USNM) for generating the molecular sequences. For assistance in the field collecting marine cerithiids, ES is grateful to Kenneth Hayes and Norine Yeung (University of Hawaii), and to Stephanie Clark and Phil Colman (Australia). Thanks as well to Serge Gofas (University of Malaga) for collecting specimens of Bittium latreillii and B. simplex in Spain. The comments of two anonymous referees improved the quality of the manuscript. NR 37 TC 2 Z9 2 U1 2 U2 9 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 DEC PY 2013 VL 132 IS 4 BP 326 EP 351 DI 10.1111/ivb.12031 PG 26 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 264SG UT WOS:000327900200005 ER PT J AU Yeshurun, R Bar-Oz, G Nadel, D AF Yeshurun, Reuven Bar-Oz, Guy Nadel, Dani TI The social role of food in the Natufian cemetery of Raqefet Cave, Mount Carmel, Israel SO JOURNAL OF ANTHROPOLOGICAL ARCHAEOLOGY LA English DT Article DE Epipaleolithic; Burial; Foodways; Mount Carmel; Zooarchaeology; Contextual taphonomy; Feasting ID SOUTHERN LEVANT; CUT MARKS; HAMMERSTONE PERCUSSION; FAUNAL ANALYSIS; SITE STRUCTURE; BONE SURFACES; LONG BONES; PATTERNS; GAZELLE; ASSEMBLAGES AB The archaeology of mortuary practices and related foodways in the Late Natufian (LN; ca. 14,000/13,500-11,700 BP) sheds light on the communal activities of the last hunter-gatherers in the Mediterranean Levant. We present a detailed analysis of the fauna from the LN cemetery of Ragefet Cave (Mount Carmel, Israel). Taphonomic evidence indicates that the animal bones are butchery and consumption leftovers. While the patterns of animal exploitation are reminiscent of Natufian habitation sites, the remains do not reflect the typical recurring post-discard damage resulting from continuous or repeating habitations in those sites. Hence the fauna is interpreted as the leftovers of punctuated, short-term events, rather than 'ordinary' Natufian household trash. Taking into account the special depositional context and site characteristics, we interpret the fauna as the intentionally-gathered and buried remains of simple funerary feasts. Elaborate mortuary behavior and symbolic role of food refuse were recently suggested at the contemporaneous cave of Hilazon Tachtit (Israel). The new data from Ragefet Cave probably reflect a somewhat different type of communal meals, adding to the diversity and complexity of pre-agricultural life-ways in the Levant. (C) 2013 Elsevier Inc. All rights reserved. C1 [Yeshurun, Reuven; Bar-Oz, Guy; Nadel, Dani] Univ Haifa, Zinman Inst Archaeol, IL-31905 Haifa, Israel. [Yeshurun, Reuven] Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. RP Yeshurun, R (reprint author), Univ Haifa, Zinman Inst Archaeol, IL-31905 Haifa, Israel. EM ryeshuru@research.haifa.ac.il; guybar@research.haifa.ac.il; dnadel@research.haifa.ac.il NR 139 TC 6 Z9 6 U1 2 U2 18 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0278-4165 EI 1090-2686 J9 J ANTHROPOL ARCHAEOL JI J. Anthropol. Archaeol. PD DEC PY 2013 VL 32 IS 4 BP 511 EP 526 DI 10.1016/j.jaa.2013.09.002 PG 16 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 269IB UT WOS:000328233900010 ER PT J AU Hirschmann, M Naab, T Dave, R Oppenheimer, BD Ostriker, JP Somerville, RS Oser, L Genzel, R Tacconi, LJ Forster-Schreiber, NM Burkert, A Genel, S AF Hirschmann, Michaela Naab, Thorsten Dave, Romeel Oppenheimer, Benjamin D. Ostriker, Jeremiah P. Somerville, Rachel S. Oser, Ludwig Genzel, Reinhard Tacconi, Linda J. Foerster-Schreiber, Natascha M. Burkert, Andreas Genel, Shy TI The effect of metal enrichment and galactic winds on galaxy formation in cosmological zoom simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: evolution; galaxies: formation; galaxies: general; galaxies: kinematics and dynamics; galaxies: stellar content ID MASS-METALLICITY RELATION; STAR-FORMING GALAXIES; COLD DARK-MATTER; TULLY-FISHER RELATION; SUPERNOVA ENERGY FEEDBACK; MOVING-MESH COSMOLOGY; LAMBDA-CDM COSMOLOGY; CENTRAL BLACK-HOLES; DIGITAL SKY SURVEY; INSIDE-OUT GROWTH AB We investigate the differential effects of metal cooling and galactic stellar winds on the cosmological formation of individual galaxies with three sets of cosmological, hydrodynamical zoom simulations of 45 haloes in the mass range 10(11) < M-halo < 10(13) M-circle dot. Models including both galactic winds and metal cooling (i) suppress early star formation at z greater than or similar to 1 and predict reasonable star formation histories for galaxies in present-day haloes of less than or similar to 10(12) M-circle dot, (ii) produce galaxies with high cold gas fractions (30-60 per cent) at high redshift, (iii) significantly reduce the galaxy formation efficiencies for haloes (M-halo less than or similar to 10(12) M-circle dot) at all redshifts in overall good agreement with recent observational data and constraints from abundance matching, (iv) result in high-redshift galaxies with reduced circular velocities in agreement with the observed Tully-Fisher relation at z similar to 2 and (v) significantly increase the sizes of low-mass galaxies (M-stellar less than or similar to 3 x 10(10) M-circle dot) at high redshift resulting in a weak size evolution - a trend in agreement with observations. However, the low-redshift (z < 0.5) star formation rates of more massive galaxies are higher than observed (up to 10 times). No tested model predicts the observed size evolution for low-mass and high-mass galaxies simultaneously. Without winds the sizes of low-mass galaxies evolve rapidly, and with winds the size evolution of massive galaxies is too weak. Due to the delayed onset of star formation in the wind models, the metal enrichment of gas and stars is delayed and agrees well with observational constraints. Metal cooling and stellar winds are both found to increase the ratio of in situ formed to accreted stars - the relative importance of dissipative versus dissipationless assembly. For halo masses below similar to 10(12) M-circle dot, this is mainly caused by less stellar accretion and compares well to predictions from semi-analytical models and but differs from abundance matching models as the in situ formed fractions of stellar mass are still too low in the simulations. For higher masses, however, the fraction of in situ stars is overpredicted due to the unrealistically high star formation rates at low redshifts. C1 [Hirschmann, Michaela] INAF Astron Observ Trieste, I-34143 Trieste, Italy. [Naab, Thorsten; Oser, Ludwig] Max Planck Inst Astrophys, D-85740 Garching, Germany. [Dave, Romeel] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Dave, Romeel] S African Astron Observ, ZA-7925 Cape Town, South Africa. [Oppenheimer, Benjamin D.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Oppenheimer, Benjamin D.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA, Boulder, CO 80309 USA. [Ostriker, Jeremiah P.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Ostriker, Jeremiah P.; Oser, Ludwig] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Somerville, Rachel S.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Genzel, Reinhard; Tacconi, Linda J.; Foerster-Schreiber, Natascha M.; Burkert, Andreas] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. [Burkert, Andreas] Univ Sternwarte Munchen, D-81679 Munich, Germany. [Genel, Shy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hirschmann, M (reprint author), INAF Astron Observ Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy. EM mhirsch@oats.inaf.it OI Genel, Shy/0000-0002-3185-1540 FU European Research Council under European Community [202781]; DFG cluster of excellence 'Origin and Structure of the Universe'; Leibniz Supercomputing Centre [pr32re] FX MH acknowledges financial support from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 202781. TN acknowledges support from the DFG cluster of excellence 'Origin and Structure of the Universe'. Computer resources for this project have been provided by the Leibniz Supercomputing Centre under the grant no. pr32re. We thank the referee, Fabio Governato, for a careful and constructive reading of our paper. NR 175 TC 41 Z9 41 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 DEC PY 2013 VL 436 IS 4 BP 2929 EP 2949 DI 10.1093/mnras/stt1770 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263HL UT WOS:000327798100005 ER PT J AU Vogelsberger, M Genel, S Sijacki, D Torrey, P Springel, V Hernquist, L AF Vogelsberger, Mark Genel, Shy Sijacki, Debora Torrey, Paul Springel, Volker Hernquist, Lars TI A model for cosmological simulations of galaxy formation physics SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; cosmology: theory ID SMOOTHED PARTICLE HYDRODYNAMICS; ACTIVE GALACTIC NUCLEI; COLD DARK-MATTER; ADAPTIVE MESH REFINEMENT; COSMIC STAR-FORMATION; MASSIVE BLACK-HOLES; TULLY-FISHER RELATION; TO-LIGHT RATIOS; STELLAR MASS; MOVING-MESH AB We present a new comprehensive model of the physics of galaxy formation designed for large-scale hydrodynamical simulations of structure formation using the moving-mesh code arepo. Our model includes primordial and metal-line cooling with self-shielding corrections, stellar evolution and feedback processes, gas recycling, chemical enrichment, a novel subgrid model for the metal loading of outflows, black hole (BH) seeding, BH growth and merging procedures, quasar- and radio-mode feedback, and a prescription for radiative electromagnetic (EM) feedback from active galactic nuclei (AGN). Our stellar evolution and chemical enrichment scheme follows nine elements (H, He, C, N, O, Ne, Mg, Si, Fe) independently. Stellar feedback is realized through kinetic outflows. The metal mass loading of outflows can be adjusted independently of the wind mass loading. This is required to simultaneously reproduce the stellar mass content of low-mass haloes and their gas oxygen abundances. Radiative EM AGN feedback is implemented assuming an average spectral energy distribution and a luminosity-dependent scaling of obscuration effects. This form of feedback suppresses star formation more efficiently than continuous thermal quasar-mode feedback alone, but is less efficient than mechanical radio-mode feedback in regulating star formation in massive haloes. We contrast simulation predictions for different variants of our galaxy formation model with key observations, allowing us to constrain the importance of different modes of feedback and their uncertain efficiency parameters. We identify a fiducial best match model and show that it reproduces, among other things, the cosmic star formation history, the stellar mass function, the stellar mass-halo mass relation, g-, r-, i- and z-band SDSS galaxy luminosity functions, and the Tully-Fisher relation. We can achieve this success only if we invoke very strong forms of stellar and AGN feedback such that star formation is adequately reduced in both low- and high-mass systems. In particular, the strength of radio-mode feedback needs to be increased significantly compared to previous studies to suppress efficient cooling in massive, metal-enriched haloes. C1 [Vogelsberger, Mark; Genel, Shy; Sijacki, Debora; Torrey, Paul; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sijacki, Debora] Kavli Inst Cosmol, Cambridge, England. [Sijacki, Debora] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, ARI, Zentrum Astron, D-69120 Heidelberg, Germany. RP Vogelsberger, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mvogelsberger@cfa.harvard.edu OI Torrey, Paul/0000-0002-5653-0786; Genel, Shy/0000-0002-3185-1540 FU PRACE project [RA0844]; NASA through Hubble Fellowship [HST-HF-51317.01]; DFG [SFB 881]; European Research Council under ERC-StG grant [EXAGAL-308037]; FAS Science Division Research Computing Group at Harvard University; Stampede supercomputer at the Texas Advanced Computing Center; Magny Cluster at HITS; CURIE supercomputer at CEA/France as part of PRACE project [RA0844] FX The simulations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University, the Stampede supercomputer at the Texas Advanced Computing Center, the Magny Cluster at HITS and the CURIE supercomputer at CEA/France as part of PRACE project RA0844. We thank Simeon Bird, Laura Blecha, Charlie Conroy, Daniel Eisenstein, Claude-Andre Faucher-Giguere, Chris Hayward, Dusan Keres, Lisa Kewley, Bence Kocsis, Federico Marinacci, Diego Munoz, Dylan Nelson, Rudiger Pakmor, Christoph Pfrommer, Ewald Puchwein, Vicente Rodriguez-Gomez, Laura Sales, Rob Simcoe, Gregory Snyder, Joshua Suresh, Rob Wiersma, Dandan Xu and Jabran Zahid for useful discussions. MV acknowledges support from NASA through Hubble Fellowship grant HST-HF-51317.01. VS acknowledges support through SFB 881 'The Milky Way System' of the DFG, and through the European Research Council under ERC-StG grant EXAGAL-308037. NR 237 TC 175 Z9 175 U1 0 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 4 BP 3031 EP 3067 DI 10.1093/mnras/stt1789 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263HL UT WOS:000327798100012 ER PT J AU Yeates, AR Munoz-Jaramillo, A AF Yeates, A. R. Munoz-Jaramillo, A. TI Kinematic active region formation in a three-dimensional solar dynamo model SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Sun: interior; Sun: magnetic fields; Sun: photosphere; sunspots ID BIPOLAR MAGNETIC REGIONS; ADAPTIVE MESH REFINEMENT; CONVECTION ZONE; FLUX-TRANSPORT; SPHERICAL GEOMETRY; CYCLE; FIELD; TUBES; SUN; SURFACE AB We propose a phenomenological technique for modelling the emergence of active regions within a three-dimensional, kinematic dynamo framework. By imposing localized velocity perturbations, we create emergent flux tubes out of toroidal magnetic field at the base of the convection zone, leading to the eruption of active regions at the solar surface. The velocity perturbations are calibrated to reproduce observed active region properties (including the size and flux of active regions, and the distribution of tilt angle with latitude), resulting in a more consistent treatment of flux-tube emergence in kinematic dynamo models than artificial flux deposition. We demonstrate how this technique can be used to assimilate observations and drive a kinematic three-dimensional model, and use it to study the characteristics of active region emergence and decay as a source of poloidal field. We find that the poloidal components are strongest not at the solar surface, but in the middle convection zone, in contrast with the common assumption that the poloidal source is located near the solar surface. We also find that, while most of the energy is contained in the lower convection zone, there is a good correlation between the evolution of the surface and interior magnetic fields. C1 [Yeates, A. R.] Univ Durham, Dept Math Sci, Durham DH1 3LE, England. [Munoz-Jaramillo, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Munoz-Jaramillo, A.] Univ Corp Atmospher Res, Boulder, CO 80307 USA. [Munoz-Jaramillo, A.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. RP Yeates, AR (reprint author), Univ Durham, Dept Math Sci, South Rd, Durham DH1 3LE, England. EM anthony.yeates@durham.ac.uk; amunoz@cfa.harvard.edu RI Yeates, Anthony/D-1338-2014; OI Yeates, Anthony/0000-0002-2728-4053; Munoz-Jaramillo, Andres/0000-0002-4716-0840 FU University of Utah; NASA; University of St Andrews FX AM-J is grateful to David Kieda for his support and sponsorship at the University of Utah. AM-J is supported by the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Programme, administered by the UCAR Visiting Scientist Programmes. Numerical simulations used the STFC and SRIF funded UKMHD cluster at the University of St Andrews. Figs 5( a) and 10 used the NCAR VAPOR visualization software (www.vapor.ucar.edu). Magnetogram data from NSO/KP were produced cooperatively by NSF/NSO, NASA/GSFC and NOAA/SEL, and SOLIS data are produced cooperatively by NSF/NSO and NASA/LWS. NR 52 TC 11 Z9 12 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 DEC PY 2013 VL 436 IS 4 BP 3366 EP 3379 DI 10.1093/mnras/stt1818 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263HL UT WOS:000327798100037 ER PT J AU Hermes, JJ Montgomery, MH Gianninas, A Winget, DE Brown, WR Harrold, ST Bell, KJ Kenyon, SJ Kilic, M Castanheira, BG AF Hermes, J. J. Montgomery, M. H. Gianninas, A. Winget, D. E. Brown, Warren R. Harrold, Samuel T. Bell, Keaton J. Kenyon, Scott J. Kilic, Mukremin Castanheira, Barbara G. TI A new class of pulsating white dwarf of extremely low mass: the fourth and fifth members SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Stars: individual: SDSS J161431; 28+191219; 4; Stars: individual: SDSS J222859; 93+362359; 6; Stars: oscillations; white dwarfs; Galaxy: stellar content ID ZZ-CETI STARS; STELLAR ASTROPHYSICS MESA; INSTABILITY STRIP; SPECTROSCOPIC ANALYSIS; CONVECTIVE EFFICIENCY; MILLISECOND PULSAR; MERGER SYSTEMS; BLUE EDGE; DISCOVERY; MODES AB We report the discovery of two new pulsating extremely low-mass (ELM) white dwarfs (WDs), SDSS J161431.28+191219.4 (hereafter J1614) and SDSS J222859.93+362359.6 (hereafter J2228). Both WDs have masses < 0.25 M-circle dot and thus likely harbour helium cores. Spectral fits indicate these are the two coolest pulsating WDs ever found. J1614 has T-eff = 8880 +/- 170 K and log g = 6.66 +/- 0.14, which corresponds to a similar to 0.19 M-circle dot WD. J2228 is considerably cooler, with a T-eff = 7870 +/- 120 K and log g = 6.03 +/- 0.08, which corresponds to an similar to 0.16 M-circle dot WD, making it the coolest and lowest mass pulsating WD known. There are multiple ELM WDs with effective temperatures between the warmest and coolest known ELM pulsators that do not pulsate to observable amplitudes, which questions the purity of the instability strip for low-mass WDs. In contrast to the CO-core ZZ Ceti stars, which are believed to represent a stage in the evolution of all such WDs, ELM WDs may not all evolve as a simple cooling sequence through an instability strip. Both stars exhibit long-period variability (1184-6235 s) consistent with non-radial g-mode pulsations. Although ELM WDs are preferentially found in close binary systems, both J1614 and J2228 do not exhibit significant radial-velocity variability, and are perhaps in low-inclination systems or have low-mass companions. These are the fourth and fifth pulsating ELM WDs known, all of which have hydrogen-dominated atmospheres, establishing these objects as a new class of pulsating WD. C1 [Hermes, J. J.; Montgomery, M. H.; Winget, D. E.; Harrold, Samuel T.; Bell, Keaton J.; Castanheira, Barbara G.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Hermes, J. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Gianninas, A.; Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Brown, Warren R.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Hermes, JJ (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. EM jjhermes@astro.as.utexas.edu RI Alexandros, Gianninas/B-8352-2016; OI Alexandros, Gianninas/0000-0002-8655-4308; Kenyon, Scott/0000-0003-0214-609X FU NSF [AST-0909107]; Norman Hackerman Advanced Research Program [003658-0252-2009]; NASA [NNX12AC96G]; CNPq; FAPERGS-Pronex-Brazil FX We acknowledge the anonymous referee for valuable suggestions that greatly improved this manuscript. JJH, MHM and DEW acknowledge the support of the NSF under grant AST-0909107 and the Norman Hackerman Advanced Research Program under grant 003658-0252-2009. MHM additionally acknowledges the support of NASA under grant NNX12AC96G. BGC thanks the support from CNPq and FAPERGS-Pronex-Brazil. The authors are grateful to the essential assistance of the McDonald Observatory support staff, especially Dave Doss and John Kuehne, and to Fergal Mullally for developing some of the data analysis pipeline used here. NR 55 TC 35 Z9 35 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 DEC PY 2013 VL 436 IS 4 BP 3573 EP 3580 DI 10.1093/mnras/stt1835 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263HL UT WOS:000327798100053 ER PT J AU LaMassa, SM Urry, CM Cappelluti, N Civano, F Ranalli, P Glikman, E Treister, E Richards, G Ballantyne, D Stern, D Comastri, A Cardamone, C Schawinski, K Bohringer, H Chon, G Murray, SS Green, P Nandra, K AF LaMassa, Stephanie M. Urry, C. Megan Cappelluti, Nico Civano, Francesca Ranalli, Piero Glikman, Eilat Treister, Ezequiel Richards, Gordon Ballantyne, David Stern, Daniel Comastri, Andrea Cardamone, Carie Schawinski, Kevin Boehringer, Hans Chon, Gayoung Murray, Stephen S. Green, Paul Nandra, Kirpal TI Finding rare AGN: XMM-Newton and Chandra observations of SDSS Stripe 82 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE catalogues; surveys; galaxies: active; quasars: general; quasars: supermassive black holes; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; POINT-SOURCE CATALOG; DIGITAL SKY SURVEY; RAY SOURCE CATALOG; HIGHEST REDSHIFT QUASARS; X-RAY; NUMBER COUNTS; LUMINOSITY FUNCTION; COSMOS FIELD AB We have analysed the XMM-Newton and Chandra data overlapping similar to 16.5 deg(2) of Sloan Digital Sky Survey Stripe 82, including similar to 4.6 deg(2) of proprietary XMM-Newton data that we present here. In total, 3362 unique X-ray sources are detected at high significance. We derive the XMM-Newton number counts and compare them with our previously reported Chandra logN-logS relations and other X-ray surveys. The Stripe 82 X-ray source lists have been matched to multiwavelength catalogues using a maximum likelihood estimator algorithm. We discovered the highest redshift (z = 5.86) quasar yet identified in an X-ray survey. We find 2.5 times more high-luminosity (L-x >= 10(45) erg s(-1)) AGN than the smaller area Chandra and XMM-Newton survey of COSMOS and 1.3 times as many identified by XBootes. Comparing the high-luminosity active galactic nuclei (AGN) we have identified with those predicted by population synthesis models, our results suggest that this AGN population is a more important component of cosmic black hole growth than previously appreciated. Approximately a third of the X-ray sources not detected in the optical are identified in the infrared, making them candidates for the elusive population of obscured high-luminosity AGN in the early universe. C1 [LaMassa, Stephanie M.; Urry, C. Megan; Glikman, Eilat] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Cappelluti, Nico; Ranalli, Piero; Comastri, Andrea] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Cappelluti, Nico] Univ Maryland Baltimore Coll, Ctr Space Sci & Technol, Dept Phys, Baltimore, MD 21250 USA. [Civano, Francesca; Murray, Stephen S.; Green, Paul] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Civano, Francesca] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ranalli, Piero] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, GR-15236 Athens, Greece. [Treister, Ezequiel] Univ Concepcion, Concepcion, Chile. [Richards, Gordon] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Ballantyne, David] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cardamone, Carie] Brown Univ, Harriet W Sheridan Ctr Teaching & Learning, Providence, RI 02912 USA. [Schawinski, Kevin] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. [Boehringer, Hans; Chon, Gayoung; Nandra, Kirpal] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP LaMassa, SM (reprint author), Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, POB 208120, New Haven, CT 06520 USA. EM stephanie.lamassa@yale.edu RI Ranalli, Piero/K-6363-2013; Comastri, Andrea/O-9543-2015; OI Ranalli, Piero/0000-0003-3956-755X; Comastri, Andrea/0000-0003-3451-9970; Cappelluti, Nico/0000-0002-1697-186X; Schawinski, Kevin/0000-0001-5464-0888; Urry, Meg/0000-0002-0745-9792 FU National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX 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.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the U.S. Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/. NR 90 TC 21 Z9 21 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 DEC PY 2013 VL 436 IS 4 BP 3581 EP 3601 DI 10.1093/mnras/stt1837 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263HL UT WOS:000327798100054 ER PT J AU Penna, RF Narayan, R Sadowski, A AF Penna, Robert F. Narayan, Ramesh Sadowski, Aleksander TI General relativistic magnetohydrodynamic simulations of Blandford-Znajek jets and the membrane paradigm SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; black hole physics; gravitation; MHD ID MAGNETICALLY DRIVEN ACCRETION; BLACK-HOLE SPIN; ADVECTION-DOMINATED ACCRETION; ACTIVE GALACTIC NUCLEI; ELECTRODYNAMICS; FLOWS; DISKS; FIELD; POWER; MAGNETOSPHERES AB Recently it has been observed that the scaling of jet power with black hole spin in Galactic X-ray binaries is consistent with the predictions of the Blandford-Znajek (BZ) jet model. These observations motivate us to revisit the BZ model using general relativistic magnetohydrodynamic simulations of magnetized jets from accreting (h/r similar to 0.3), spinning (0 < a(*) < 0.98) black holes. We have three main results. First, we quantify the discrepancies between the BZ jet power and our simulations: assuming maximum efficiency and uniform fields on the horizon leads to an similar to 10 per cent overestimate of jet power, while ignoring the accretion disc leads to a further similar to 50 per cent overestimate. Simply reducing the standard BZ jet power prediction by 60 per cent gives a good fit to our simulation data. Our second result is to show that the membrane formulation of the BZ model correctly describes the physics underlying simulated jets: torques, dissipation and electromagnetic fields on the horizon. This provides intuitive yet rigorous pictures for the black hole energy extraction process. Third, we compute the effective resistance of the load region and show that the load and the black hole achieve near perfect impedance matching. Taken together, these results increase our confidence in the BZ model as the correct description of jets observed from astrophysical black holes. C1 [Penna, Robert F.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Penna, Robert F.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Penna, Robert F.; Narayan, Ramesh; Sadowski, Aleksander] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Penna, RF (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. EM rpenna@cfa.harvard.edu; rnarayan@cfa.harvard.edu; asadowski@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU Pappalardo Fellowship in Physics at MIT; NASA [NNX11AE16G] FX We thank Jon McKinney and Sasha Tchekhovskoy for discussions. RFP was supported in part by a Pappalardo Fellowship in Physics at MIT. RN and AS were supported in part by NASA grant NNX11AE16G. NR 47 TC 36 Z9 36 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 DEC PY 2013 VL 436 IS 4 BP 3741 EP 3758 DI 10.1093/mnras/stt1860 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263HL UT WOS:000327798100067 ER PT J AU Sadowski, A Narayan, R Penna, R Zhu, YC AF Sadowski, Aleksander Narayan, Ramesh Penna, Robert Zhu, Yucong TI Energy, momentum and mass outflows and feedback from thick accretion discs around rotating black holes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion accretion discs; black hole physics; relativistic processes; methods: numerical; galaxies: jets ID ACTIVE GALACTIC NUCLEI; ADVECTION-DOMINATED ACCRETION; MAGNETICALLY DRIVEN ACCRETION; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; ULTRA-FAST OUTFLOWS; M-BH-SIGMA; GALAXY FORMATION; COOLING FLOWS; HOST GALAXIES; DIFFUSION-COEFFICIENTS AB Using long-duration general relativistic magnetohydrodynamic simulations of radiatively inefficient accretion discs, the energy, momentum and mass outflow rates from such systems are estimated. Outflows occur via two fairly distinct modes: a relativistic jet and a subrelativistic wind. The jet power depends strongly on the black hole spin and on the magnetic flux at the horizon. Unless these are very small, the energy output in the jet dominates over that in the wind. For a rapidly spinning black hole accreting in the magnetically arrested limit, it is confirmed that jet power exceeds the total rate of accretion of rest mass energy. However, because of strong collimation, the jet probably does not have a significant feedback effect on its immediate surroundings. The power in the wind is more modest and shows a weaker dependence on black hole spin and magnetic flux. Nevertheless, because the wind subtends a large solid angle, it is expected to provide efficient feedback on a wide range of scales inside the host galaxy. Empirical formulae are obtained for the energy and momentum outflow rates in the jet and the wind. C1 [Sadowski, Aleksander; Narayan, Ramesh; Penna, Robert; Zhu, Yucong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02134 USA. RP Sadowski, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02134 USA. EM asadowski@cfa.harvard.edu; rnarayan@cfa.harvard.edu; rpenna@cfa.harvard.edu; yzhu@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA [NNX11AE16G]; NSF via XSEDE; NASA via High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division FX AS and RN were supported in part by NASA grant NNX11AE16G. We acknowledge NSF support via XSEDE resources and NASA support via High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division. NR 115 TC 40 Z9 41 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 DEC PY 2013 VL 436 IS 4 BP 3856 EP 3874 DI 10.1093/mnras/stt1881 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263HL UT WOS:000327798100074 ER PT J AU Hines, J Hammrich, A Steiner, D Gessner, MO AF Hines, Jes Hammrich, Arne Steiner, Daniel Gessner, Mark O. TI A field facility to simulate climate warming and increased nutrient supply in shallow aquatic ecosystems SO OECOLOGIA LA English DT Article DE Enclosure; Global change; Lake; Multiple stressors; Mesocosm; Nitrogen loading; Climate warming; Wetland ID GLOBAL NITROGEN-CYCLE; LONG-TERM DATA; FRESH-WATER; ELEVATED CO2; LAKE; EUTROPHICATION; COMMUNITIES; ENRICHMENT; RESPONSES; IMPACTS AB Global warming and excess nitrogen deposition can exert strong impacts on aquatic populations, communities, and ecosystems. However, experimental data to establish clear cause-and-effect relationships in naturally complex field conditions are scarce in aquatic environments. Here, we describe the design and performance of a unique outdoor enclosure facility used to simulate warming, increased nitrogen supply, and both factors combined in a littoral freshwater wetland dominated by common reed, Phragmites australis. The experimental system effectively simulated a 2.8 A degrees C climate warming scenario over an extended period, capturing the natural temperature variations in the wetland at diel and seasonal scales with only small deviations. Excess nitrogen supply enhanced nitrate concentrations especially in winter when it was associated with increased concentration of ammonium and dissolved organic carbon. Nitrogen also reduced dissolved oxygen concentrations, particularly in the summer. Importantly, by stimulating biological activity, warming enhanced the nitrogen uptake capacity of the wetland during the winter, emphasizing the need for multifactorial global change experiments that examine both warming and nitrogen loading in concert. Establishing similar experiments across broad environmental gradients holds great potential to provide robust assessments of the impacts of climate change on shallow aquatic ecosystems. C1 [Hines, Jes; Hammrich, Arne; Steiner, Daniel; Gessner, Mark O.] Eawag Swiss Fed Inst Aquat Sci & Technol, Dept Aquat Ecol, Dubendorf, Switzerland. [Hines, Jes; Hammrich, Arne; Steiner, Daniel; Gessner, Mark O.] Eawag Swiss Fed Inst Aquat Sci & Technol, Dept Aquat Ecol, Kastanienbaum, Switzerland. [Hines, Jes; Gessner, Mark O.] Leibniz Inst Freshwater Ecol & Inland Fisheries I, Dept Expt Limnol, Stechlin, Germany. [Hines, Jes] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Hammrich, Arne; Gessner, Mark O.] ETH, Inst Integrat Biol IBZ, Zurich, Switzerland. [Gessner, Mark O.] Berlin Inst Technol TU Berlin, Dept Ecol, Berlin, Germany. RP Hines, J (reprint author), Leibniz Inst Freshwater Ecol & Inland Fisheries I, Dept Expt Limnol, Alte Fischerhutte 2, Stechlin, Germany. EM hinesj@si.edu; gessner@igb-berlin.de RI Hines, Jes/L-7668-2016 OI Hines, Jes/0000-0002-9129-5179 FU Swiss National Science Foundation [SNF 32-63701.00, 3100A0-108441]; Swiss State Secretariat for Education and Research through the Euro-limpacs project under FP7 of the EU Commission; AEW Energie AG FX We are grateful to N. Buesing, M. Brosed, M.J. Daigo, M. da Silva Moretti, C. K. Dang, M. Doring, F. Erb, R. Fankhauser, M. Filippini, S. Flury, A. Frainer, P. Gaumann, S. Grob, A. H. Hines, D. Hohmann, S. Kamara, S. Kapelli, N. Kodama, A. Ivanovski, P. Madej, R. Illi and the AUA lab, A. Raffainer, M. Reyes, I. Ronning, M. Schindler, J. Sierra, A. Stockli, N. Tschopp, Wenjing Xu, and numerous others for support, data, assistance with the design, and installation and/or operation of the facility. We also thank the Canton of Argovia for permission to access the site and data provision, the Fisheries Sports Club Hallwilersee-Meisterschwanden for access to electricity, and the AEW Energie AG for partial sponsoring of electricity supply. This research was funded by the Swiss National Science Foundation (SNF 32-63701.00 and 3100A0-108441) and the Swiss State Secretariat for Education and Research through the Euro-limpacs project supported under FP7 of the EU Commission. NR 50 TC 8 Z9 8 U1 7 U2 66 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 DEC PY 2013 VL 173 IS 4 BP 1169 EP 1178 DI 10.1007/s00442-013-2720-x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 268ZR UT WOS:000328210000002 PM 23836092 ER PT J AU Baldeck, CA Kembel, SW Harms, KE Yavitt, JB John, R Turner, BL Chuyong, GB Kenfack, D Thomas, DW Madawala, S Gunatilleke, N Gunatilleke, S Bunyavejchewin, S Kiratiprayoon, S Yaacob, A Supardi, MNN Valencia, R Navarrete, H Davies, SJ Hubbell, SP Dalling, JW AF Baldeck, Claire A. Kembel, Steven W. Harms, Kyle E. Yavitt, Joseph B. John, Robert Turner, Benjamin L. Chuyong, George B. Kenfack, David Thomas, Duncan W. Madawala, Sumedha Gunatilleke, Nimal Gunatilleke, Savitri Bunyavejchewin, Sarayudh Kiratiprayoon, Somboon Yaacob, Adzmi Supardi, Mohd. N. Nur Valencia, Renato Navarrete, Hugo Davies, Stuart J. Hubbell, Stephen P. Dalling, James W. TI A taxonomic comparison of local habitat niches of tropical trees SO OECOLOGIA LA English DT Article DE Community assembly; Phylogenetic community structure; Phylogenetic signal; Niche overlap; Tropical forest ID PHYLOGENETIC STRUCTURE; ECOLOGICAL COMMUNITIES; CONSERVATION BIOLOGY; NEOTROPICAL FOREST; DIVERSITY; EVOLUTION; SIGNAL; PLOT; DISTRIBUTIONS; ASSOCIATIONS AB The integration of ecology and evolutionary biology requires an understanding of the evolutionary lability in species' ecological niches. For tropical trees, specialization for particular soil resource and topographic conditions is an important part of the habitat niche, influencing the distributions of individual species and overall tree community structure at the local scale. However, little is known about how these habitat niches are related to the evolutionary history of species. We assessed the relationship between taxonomic rank and tree species' soil resource and topographic niches in eight large (24-50 ha) tropical forest dynamics plots. Niche overlap values, indicating the similarity of two species' distributions along soil or topographic axes, were calculated for all pairwise combinations of co-occurring tree species at each study site. Congeneric species pairs often showed greater niche overlap (i.e., more similar niches) than non-congeneric pairs along both soil and topographic axes, though significant effects were found for only five sites based on Mantel tests. No evidence for taxonomic effects was found at the family level. Our results indicate that local habitat niches of trees exhibit varying degrees of phylogenetic signal at different sites, which may have important ramifications for the phylogenetic structure of these communities. C1 [Baldeck, Claire A.] Univ Illinois, Program Ecol Evolut & Conservat Biol, Urbana, IL 61801 USA. [Baldeck, Claire A.; Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Kembel, Steven W.] Univ Quebec, Dept Sci Biol, Montreal, PQ H3C 3P8, Canada. [Harms, Kyle E.; Turner, Benjamin L.; Davies, Stuart J.; Dalling, James W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Yavitt, Joseph B.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. [John, Robert] Indian Inst Sci Educ & Res, Nadia 741252, W Bengal, India. [Chuyong, George B.] Univ Buea, Dept Plant & Anim Sci, Buea, Cameroon. [Kenfack, David; Davies, Stuart J.] Harvard Univ, Ctr Trop Forest Sci, Arnold Arboretum Asia Program, Cambridge, MA 02138 USA. [Thomas, Duncan W.] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [Madawala, Sumedha; Gunatilleke, Nimal; Gunatilleke, Savitri] Univ Peradeniya, Dept Bot, Fac Sci, Peradeniya 20400, Sri Lanka. [Bunyavejchewin, Sarayudh] Natl Pk Wildlife & Plant Conservat Dept, Bangkok 10900, Thailand. [Kiratiprayoon, Somboon] Thammasat Univ Rangsit, Fac Sci & Technol, Klongluang 12121, Patumtani, Thailand. [Yaacob, Adzmi] Univ Teknol MARA, Fac Plantat & Agrotechnol, Shah Alam 40450, Selangor, Malaysia. [Supardi, Mohd. N. Nur] Forest Res Inst Malaysia, Div Forest Environm, Kepong 52109, Selangor Darul, Malaysia. [Valencia, Renato; Navarrete, Hugo] Pontificia Univ Catolica Ecuador, Lab Ecol Plantas & Herbario QCA, Escuela Ciencias Biol, Quito, Ecuador. [Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. RP Baldeck, CA (reprint author), Univ Illinois, Dept Plant Biol, 265 Morrill Hall,505 S Goodwin Ave, Urbana, IL 61801 USA. EM baldeck2@life.illinois.edu RI Turner, Benjamin/E-5940-2011; OI Turner, Benjamin/0000-0002-6585-0722; Kembel, Steven/0000-0001-5224-0952 NR 40 TC 11 Z9 11 U1 1 U2 34 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 DEC PY 2013 VL 173 IS 4 BP 1491 EP 1498 DI 10.1007/s00442-013-2709-5 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 268ZR UT WOS:000328210000030 PM 23851985 ER PT J AU Yang, J Zuo, YX Lou, Z Cheng, JQ Zhang, QZ Shi, SC Huang, JS Yao, QJ Wang, Z AF Yang, Ji Zuo, Ying-Xi Lou, Zheng Cheng, Jing-Quan Zhang, Qi-Zhou Shi, Sheng-Cai Huang, Jia-Sheng Yao, Qi-Jun Wang, Zhong TI Conceptual design studies of the 5m terahertz antenna for Dome A, Antarctica SO RESEARCH IN ASTRONOMY AND ASTROPHYSICS LA English DT Article DE Dome A, Antarctica; antennas; astronomy; telescopes; terahertz ID SITE AB As the highest, coldest and driest place in Antarctica, Dome A provides exceptionally good observing conditions for ground-based observations over terahertz wavebands. The 5m Dome A Terahertz Explorer (DATE5) has been proposed to explore new terahertz windows, primarily over wavelengths between 350 and 200 mu m. DATE5 will be an open-air, fully-steerable telescope that can function by unmanned operation with remote control. The telescope will be able to endure the harsh polar environment, including high altitude, very low temperature and very low air pressure. The unique specifications, including high accuracies for surface shape and pointing and fully automatic year-around remote operation, along with a stringent limit on the periods of on-site assembly, testing and maintenance, bring a number of challenges to the design, construction, assembly and operation of this telescope. This paper introduces general concepts related to the design of the DATE5 antenna. Beginning from an overview of the environmental and operational limitations, the design specifications and requirements of the DATE5 antenna are listed. From these, major aspects on the conceptual design studies, including the antenna optics, the backup structure, the panels, the subreflector, the mounting and the antenna base structure, are explained. Some critical issues of performance are justified through analyses that use computational fluid dynamics, thermal analysis and de-icing studies, and the proposed approaches for test operation and on-site assembly. Based on these studies, we conclude that the specifications of the DATE5 antenna can generally be met by using enhanced technological approaches. C1 [Yang, Ji; Zuo, Ying-Xi; Lou, Zheng; Cheng, Jing-Quan; Shi, Sheng-Cai; Yao, Qi-Jun] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. [Yang, Ji; Zuo, Ying-Xi; Lou, Zheng; Cheng, Jing-Quan; Shi, Sheng-Cai; Yao, Qi-Jun] Chinese Acad Sci, Key Lab Radio Astron, Nanjing 210008, Jiangsu, Peoples R China. [Zhang, Qi-Zhou; Huang, Jia-Sheng; Wang, Zhong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yang, J (reprint author), Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. EM jqcheng@pmo.ac.cn FU CAS (Chinese Academy of Sciences)/SAFEA (State Administration of Foreign Experts Affairs); National Natural Science Foundation of China [10921063, 11190014] FX This work related to the DATE5 telescope was initiated from discussions among the Cosmic Star Formation Research Partner Team, which was supported by the CAS (Chinese Academy of Sciences)/SAFEA (State Administration of Foreign Experts Affairs) International Partnership Program for Creative Research Teams by International Collaboration. This partner team includes Yu Gao, Lin Yan, Edward Tong, Ruiqing Mao, Longlong Feng, Hongchi Wang, Zhibo Jiang, Ye Xu and Xianzhong Zheng. The authors have benefitted from many stimulating discussions with Robert Wilson, Jiansheng Chen, Steve Padin, Karl Menten, Xiangqun Cui, Lifan Wang, Huigeng Yang and Wenlei Shan. This work has been supported by the National Natural Science Foundation of China (Grant Nos. 10921063 and 11190014). NR 18 TC 16 Z9 22 U1 0 U2 11 PU NATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES PI BEIJING PA 20A DATUN RD, CHAOYANG, BEIJING, 100012, PEOPLES R CHINA SN 1674-4527 J9 RES ASTRON ASTROPHYS JI Res. Astron. Astrophys. PD DEC PY 2013 VL 13 IS 12 BP 1493 EP 1508 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 264KI UT WOS:000327875500010 ER PT J AU Batygin, K Adams, FC AF Batygin, Konstantin Adams, Fred C. TI MAGNETIC AND GRAVITATIONAL DISK-STAR INTERACTIONS: AN INTERDEPENDENCE OF PMS STELLAR ROTATION RATES AND SPIN-ORBIT MISALIGNMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; planets and satellites: formation; protoplanetary disks; stars: formation; stars: pre-main sequence ID T-TAURI STARS; MAGNETOCENTRIFUGALLY DRIVEN FLOWS; ANGULAR-MOMENTUM TRANSPORT; INTERMEDIATE-MASS STARS; MAIN-SEQUENCE STAR; HOT JUPITERS; MAGNETOSPHERIC ACCRETION; PLANET SCATTERING; YOUNG STARS; MAGNETOHYDRODYNAMIC SIMULATIONS AB The presence of giant gaseous planets that reside in close proximity to their host stars, i.e., hot Jupiters, may be a consequence of large-scale radial migration through the protoplanetary nebulae. Within the framework of this picture, significant orbital obliquities characteristic of a substantial fraction of such planets can be attributed to external torques that perturb the natal disks out of alignment with the spin axes of their host stars. Therefore, the acquisition of orbital obliquity likely exhibits sensitive dependence on the physics of disk-star interactions. Here, we analyze the primordial excitation of spin-orbit misalignment of Sun-like stars in light of disk-star angular momentum transfer. We begin by calculating the stellar pre-main-sequence rotational evolution, accounting for spin-up due to gravitational contraction and accretion as well as spin-down due to magnetic star-disk coupling. We devote particular attention to angular momentum transfer by accretion, and show that while generally subdominant to gravitational contraction, this process is largely controlled by the morphology of the stellarmagnetic field (that is, specific angular momentum accreted by stars with octupole-dominated surface fields is smaller than that accreted by dipole-dominated stars by an order of magnitude). Subsequently, we examine the secular spin-axis dynamics of disk-bearing stars, accounting for the time-evolution of stellar and disk properties, and demonstrate that misalignments are preferentially excited in systems where stellar rotation is not overwhelmingly rapid. Moreover, we show that the excitation of spin-orbit misalignment occurs impulsively through an encounter with a resonance between the stellar precession frequency and the disk-torquing frequency. Cumulatively, the model developed herein opens up a previously unexplored avenue toward understanding star-disk evolution and its consequences in a unified manner. C1 [Batygin, Konstantin] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Adams, Fred C.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Adams, Fred C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Batygin, K (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM kbatygin@cfa.harvard.edu; fca@umich.edu FU ITC Prize Postdoctoral Fellowship at the Institute for Theory and Computation; Harvard-Smithsonian Center for Astrophysics; NASA [NNX11AK87G] FX We thank the referee, Scott Gregory, for providing an exceptionally helpful and thorough report that resulted in a substantial improvement of the manuscript. K. B. acknowledges generous support from the ITC Prize Postdoctoral Fellowship at the Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics. F. C. A. acknowledges support from NASA Origins grant NNX11AK87G. NR 120 TC 29 Z9 29 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 169 DI 10.1088/0004-637X/778/2/169 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800084 ER PT J AU Becker, JC Batygin, K AF Becker, Juliette C. Batygin, Konstantin TI DYNAMICAL MEASUREMENTS OF THE INTERIOR STRUCTURE OF EXOPLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: dynamical evolution and stability; planets and satellites: interiors ID MULTIPLE-PLANET SYSTEMS; GIANT PLANETS; SOLAR-SYSTEM; HOT JUPITERS; LOW-MASS; CLOSE ENCOUNTERS; TIDAL EVOLUTION; LIGHT CURVES; HARPS SEARCH; ORBIT AB Giant gaseous planets often reside on orbits in sufficient proximity to their host stars for the planetary quadrupole gravitational field to become non-negligible. In presence of an additional planetary companion, a precise characterization of the system's orbital state can yield meaningful constraints on the transiting planet's interior structure. However, such methods can require a very specific type of system. This paper explores the dynamic range of applicability of these methods and shows that interior structure calculations are possible for a wide array of orbital architectures. The HAT-P-13 system is used as a case study, and the implications of perturbations arising from a third distant companion on the feasibility of an interior calculation are discussed. We find that the method discussed here is likely to be useful in studying other planetary systems, allowing the possibility of an expanded survey of the interiors of exoplanets. C1 [Becker, Juliette C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Batygin, Konstantin] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Becker, JC (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM jbecker@caltech.edu OI Becker, Juliette/0000-0002-7733-4522 FU ITC Prize Postdoctoral Fellowship FX We thank John Johnson for his careful review of the manuscript and helpful suggestions. We would additionally like to thank Greg Laughlin for useful conversations. K. Batygin acknowledges the generous support of the ITC Prize Postdoctoral Fellowship. We also thank the anonymous referee for their insightful report. NR 66 TC 5 Z9 5 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 DEC 1 PY 2013 VL 778 IS 2 AR 100 DI 10.1088/0004-637X/778/2/100 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800015 ER PT J AU Foley, RJ Mandel, K AF Foley, Ryan J. Mandel, Kaisey TI CLASSIFYING SUPERNOVAE USING ONLY GALAXY DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: general; methods: statistical; supernovae: general ID DIGITAL SKY SURVEY; CORE-COLLAPSE SUPERNOVAE; GAMMA-RAY BURSTS; IA SUPERNOVAE; HOST GALAXIES; DATA RELEASE; SN 2008HA; SDSS-III; REDSHIFT; RATES AB We present a new method for probabilistically classifying supernovae (SNe) without using SN spectral or photometric data. Unlike all previous studies to classify SNe without spectra, this technique does not use any SN photometry. Instead, the method relies on host-galaxy data. We build upon the well-known correlations between SN classes and host-galaxy properties, specifically that core-collapse SNe rarely occur in red, luminous, or early-type galaxies. Using the nearly spectroscopically complete Lick Observatory Supernova Search sample of SNe, we determine SN fractions as a function of host-galaxy properties. Using these data as inputs, we construct a Bayesian method for determining the probability that an SN is of a particular class. This method improves a common classification figure of merit by a factor of >2, comparable to the best light-curve classification techniques. Of the galaxy properties examined, morphology provides the most discriminating information. We further validate this method using SN samples from the Sloan Digital Sky Survey and the Palomar Transient Factory. We demonstrate that this method has wide-ranging applications, including separating different subclasses of SNe and determining the probability that an SN is of a particular class before photometry or even spectra can. Since this method uses completely independent data from light-curve techniques, there is potential to further improve the overall purity and completeness of SN samples and to test systematic biases of the light-curve techniques. Further enhancements to the host-galaxy method, including additional host-galaxy properties, combination with light-curve methods, and hybrid methods, should further improve the quality of SN samples from past, current, and future transient surveys. C1 [Foley, Ryan J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, Ryan J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Mandel, Kaisey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Foley, RJ (reprint author), Univ Illinois, Dept Astron, 1002 West Green St, Urbana, IL 61801 USA. FU NSF [AST-1211196]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX Supernova research at Harvard is supported in part by NSF grant AST-1211196.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration, including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 45 TC 7 Z9 7 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 167 DI 10.1088/0004-637X/778/2/167 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800082 ER PT J AU Jordan, A Espinoza, N Rabus, M Eyheramendy, S Sing, DK Desert, JM Bakos, GA Fortney, JJ Lopez-Morales, M Maxted, PFL Triaud, AHMJ Szentgyorgyi, A AF Jordan, Andres Espinoza, Nestor Rabus, Markus Eyheramendy, Susana Sing, David K. Desert, Jean-Michel Bakos, Gaspar A. Fortney, Jonathan J. Lopez-Morales, Mercedes Maxted, Pierre F. L. Triaud, Amaury H. M. J. Szentgyorgyi, Andrew TI A GROUND-BASED OPTICAL TRANSMISSION SPECTRUM OF WASP-6b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: atmospheres; techniques: spectroscopic ID HUBBLE-SPACE-TELESCOPE; EXOPLANET HD 189733B; ASTRONOMICAL TIME-SERIES; EXTRASOLAR PLANET; TRANSIT SPECTROPHOTOMETRY; SPITZER OBSERVATIONS; SODIUM-ABSORPTION; ATMOSPHERIC HAZE; LIGHT CURVES; MU-M AB We present a ground-based optical transmission spectrum of the inflated sub-Jupiter-mass planet WASP-6b. The spectrum was measured in 20 spectral channels from 480 nm to 860 nm using a series of 91 spectra over a complete transit event. The observations were carried out using multi-object differential spectrophotometry with the Inamori-Magellan Areal Camera and Spectrograph on the Baade Telescope at Las Campanas Observatory. We model systematic effects on the observed light curves using principal component analysis on the comparison stars and allow for the presence of short and long memory correlation structure in our Monte Carlo Markov Chain analysis of the transit light curves for WASP-6. The measured transmission spectrum presents a general trend of decreasing apparent planetary size with wavelength and lacks evidence for broad spectral features of Na and K predicted by clear atmosphere models. The spectrum is consistent with that expected for scattering that is more efficient in the blue, as could be caused by hazes or condensates in the atmosphere of WASP-6b. WASP-6b therefore appears to be yet another massive exoplanet with evidence for a mostly featureless transmission spectrum, underscoring the importance that hazes and condensates can have in determining the transmission spectra of exoplanets. C1 [Jordan, Andres; Espinoza, Nestor; Rabus, Markus] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Santiago 7820436, Chile. [Eyheramendy, Susana] Pontificia Univ Catolica Chile, Dept Estadist, Fac Matemat, Santiago 7820436, Chile. [Sing, David K.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Desert, Jean-Michel] Univ Colorado, CASA, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Desert, Jean-Michel] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Bakos, Gaspar A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Lopez-Morales, Mercedes; Szentgyorgyi, Andrew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maxted, Pierre F. L.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Triaud, Amaury H. M. J.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Triaud, Amaury H. M. J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Jordan, A (reprint author), Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile. OI Sing, David /0000-0001-6050-7645; Fortney, Jonathan/0000-0002-9843-4354; Jordan, Andres/0000-0002-5389-3944 FU FONDECYT [1130857]; BASAL CATA [PFB-06]; Millennium Science Initiative; Chilean Ministry of Economy [Nucleus P10-022-F]; Vicerrectoria de Investigacion (VRI), Pontificia Universidad Cat olica de Chile (proyecto investigacion interdisciplinaria; CONICYT-PCHA/Doctorado Nacional; FONDECYT postdoctoral fellowship [3120097]; STFC consolidated grant [ST/J0016/1]; NASA through the Sagan Exoplanet Fellowship program; Swiss National Science Foundation fellow [PBGEP2-145594] FX A.J. acknowledges support from FONDECYT project 1130857, BASAL CATA PFB-06, and the Millennium Science Initiative, Chilean Ministry of Economy (Nucleus P10-022-F). A.J., S.E., and N.E. acknowledge support from the Vicerrectoria de Investigacion (VRI), Pontificia Universidad Cat olica de Chile (proyecto investigacion interdisciplinaria 25/2011). N.E. is supported by CONICYT-PCHA/Doctorado Nacional, and M.R. is supported by FONDECYT postdoctoral fellowship 3120097. D.K.S.acknowledges support from STFC consolidated grant ST/J0016/1. J.-M.D.acknowledges funding from NASA through the Sagan Exoplanet Fellowship program administered by the NASA Exoplanet Science Institute (NExScI). A.H.M.J.T. is a Swiss National Science Foundation fellow under grant number PBGEP2-145594. NR 59 TC 25 Z9 25 U1 3 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 DEC 1 PY 2013 VL 778 IS 2 AR 184 DI 10.1088/0004-637X/778/2/184 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800098 ER PT J AU Lada, CJ Lombardi, M Roman-Zuniga, C Forbrich, J Alves, JF AF Lada, Charles J. Lombardi, Marco Roman-Zuniga, Carlos Forbrich, Jan Alves, Joao F. TI SCHMIDT'S CONJECTURE AND STAR FORMATION IN MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: star formation; ISM: clouds; stars: formation ID YOUNG STELLAR OBJECTS; NEARBY GALAXIES; FORMATION LAW; PRESTELLAR CORES; FORMATION RATES; MILKY-WAY; DENSE GAS; EXTINCTION; TURBULENCE; HERSCHEL AB We investigate Schmidt's conjecture (i.e., that the star formation rate (SFR) scales in a power-law fashion with the gas density) for four well-studied local molecular clouds (giant molecular clouds, GMCs). Using the Bayesian methodology, we show that a local Schmidt scaling relation of the form Sigma(*)(A(K)) = kappa A(K)(beta) (protostars pc(-2)) exists within (but not between) GMCs. Further, we find that the Schmidt scaling law does not by itself provide an adequate description of star formation activity in GMCs. Because the total number of protostars produced by a cloud is given by the product of Sigma(*)(A(K)) and S'(> A(K)), the differential surface area distribution function, integrated over the entire cloud, the cloud's structure plays a fundamental role in setting the level of its star formation activity. For clouds with similar functional forms of S*(AK), observed differences in their total SFRs are primarily due to the differences in S'(>A(K)) between the clouds. The coupling of Sigma(*)(A(K)) with the measured S'(>A(K)) in these clouds also produces a steep jump in the SFR and protostellar production above A(K) similar to 0.8 mag. Finally, we show that there is no global Schmidt law that relates the SFR and gas mass surface densities between GMCs. Consequently, the observed Kennicutt-Schmidt scaling relation for disk galaxies is likely an artifact of unresolved measurements of GMCs and not a result of any underlying physical law of star formation characterizing the molecular gas. C1 [Lada, Charles J.; Forbrich, Jan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lombardi, Marco] Univ Milan, Dept Phys, I-20133 Milan, Italy. [Roman-Zuniga, Carlos] Univ Nacl Autonoma Mexico, Inst Astron, Unidad Acad Ensenada, Ensenada 22860, Baja California, Mexico. [Forbrich, Jan; Alves, Joao F.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. RP Lada, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM clada@cfa.harvard.edu; marco.lombardi@unimi.it; croman@astrosen.unam.mx; jan.forbrich@univie.ac.at; joao.alves@univie.ac.at RI Roman-Zuniga, Carlos/F-6602-2016; OI Roman-Zuniga, Carlos/0000-0001-8600-4798; LOMBARDI, MARCO/0000-0002-3336-4965; Alves, Joao/0000-0002-4355-0921 FU CONACYT [152160]; DGAPA-PAPIIT-UNAM Mexico [IA101812] FX We thank Bruce Elmegreen, Neal Evans, and Chris McKee for carefully reading an earlier draft of this paper and providing comments and suggestions which resulted in improvements to this final version. We acknowledge comments from an anonymous referee which led to refinements in our arguments and improved the overall presentation of the paper. We are grateful to Mark Reid and Leo Blitz for informative discussions. One of us (C.R.Z.) gratefully acknowledges support from the following programs: CONACYT 152160 and DGAPA-PAPIITUNAM IA101812 Mexico. NR 41 TC 35 Z9 35 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 DEC 1 PY 2013 VL 778 IS 2 AR UNSP 133 DI 10.1088/0004-637X/778/2/133 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800048 ER PT J AU Moe, M Di Stefano, R AF Moe, Maxwell Di Stefano, Rosanne TI THE CLOSE BINARY PROPERTIES OF MASSIVE STARS IN THE MILKY WAY AND LOW-METALLICITY MAGELLANIC CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; binaries: spectroscopic; galaxies: stellar content; Magellanic Clouds; stars: early-type; stars: statistics ID GRAVITATIONAL LENSING EXPERIMENT; X-RAY BINARIES; SOLAR-TYPE STARS; DENSE STELLAR REGIONS; IA SUPERNOVAE; CHEMICAL-COMPOSITION; SPECTROSCOPIC BINARIES; GLOBULAR-CLUSTERS; FORMATION HISTORY; VISUAL BINARIES AB In order to understand the rates and properties of Type Ia and Type Ib/c supernovae, X-ray binaries, gravitational wave sources, and gamma-ray bursts as a function of galactic environment and cosmic age, it is imperative that we measure how the close binary properties of O- and B-type stars vary with metallicity. We have studied eclipsing binaries with early B main-sequence primaries in three galaxies with different metallicities: the Large and Small Magellanic Clouds (LMC and SMC, respectively) and the Milky Way (MW). The observed fractions of early B stars that exhibit deep eclipses 0.25 < Delta m (mag) < 0.65 and orbital periods 2 < P (days) < 20 in the MW, LMC, and SMC span a narrow range of (0.7-1.0)%, which is a model-independent result. After correcting for geometrical selection effects and incompleteness toward low-mass companions, we find for early B stars in all three environments (1) a close binary fraction of (22 +/- 5)% across orbital periods 2 < P (days) < 20 and mass ratios q = M-2/M-1 > 0.1, (2) an intrinsic orbital period distribution slightly skewed toward shorter periods relative to a distribution that is uniform in log P, (3) a mass-ratio distribution weighted toward low-mass companions, and (4) a small, nearly negligible excess fraction of twins with q > 0.9. Our fitted parameters derived for the MW eclipsing binaries match the properties inferred from nearby, early-type spectroscopic binaries, which further validates our results. There are no statistically significant trends with metallicity, demonstrating that the close binary properties of massive stars do not vary across metallicities -0.7 < log(Z/Z(circle dot)) < 0.0 beyond the measured uncertainties. C1 [Moe, Maxwell; Di Stefano, Rosanne] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Moe, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-10, Cambridge, MA 02138 USA. EM mmoe@cfa.harvard.edu FU NSF [AST-1211843]; NASA [NNX12AE39G] FX We acknowledge support from NSF grant AST-1211843 and NASA grant NNX12AE39G. M. M. thanks Tsevi Mazeh, Ian Czekala, and Tanmoy Laskar for enlightening discussions of eclipsing binaries and statistics. NR 88 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR UNSP 95 DI 10.1088/0004-637X/778/2/95 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800010 ER PT J AU Ouchi, M Ellis, R Ono, Y Nakanishi, K Kohno, K Momose, R Kurono, Y Ashby, MLN Shimasaku, K Willner, SP Fazio, GG Tamura, Y Iono, D AF Ouchi, Masami Ellis, Richard Ono, Yoshiaki Nakanishi, Kouichiro Kohno, Kotaro Momose, Rieko Kurono, Yasutaka Ashby, M. L. N. Shimasaku, Kazuhiro Willner, S. P. Fazio, G. G. Tamura, Yoichi Iono, Daisuke TI AN INTENSELY STAR-FORMING GALAXY AT z similar to 7 WITH LOW DUST AND METAL CONTENT REVEALED BY DEEP ALMA AND HST OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: formation; galaxies: high-redshift ID UV LUMINOSITY FUNCTION; HIGH-REDSHIFT GALAXIES; LYMAN-BREAK GALAXIES; LY-ALPHA EMITTERS; SPECTRAL ENERGY-DISTRIBUTIONS; EARLY RELEASE SCIENCE; STELLAR POPULATIONS; C-II; MU-M; SUBMILLIMETER GALAXY AB We report deep ALMA observations complemented by associated Hubble Space Telescope (HST) imaging for a luminous (m(UV) = 25) galaxy, "Himiko," at a redshift of z = 6.595. The galaxy is remarkable for its high star formation rate, 100 M-circle dot yr(-1), which has been securely estimated from our deep HST and Spitzer photometry, and the absence of any evidence for strong active galactic nucleus activity or gravitational lensing magnification. Our ALMA observations probe an order of magnitude deeper than previous IRAM observations, yet fail to detect a 1.2 mm dust continuum, indicating a flux of < 52 mu Jy, which is comparable to or weaker than that of local dwarf irregulars with much lower star formation rates. We likewise provide a strong upper limit for the flux of [C II] 158 mu m, L-[C II] < 5.4 x 10(7) L-circle dot, which is a diagnostic of the hot interstellar gas that is often described as a valuable probe for early galaxies. In fact, our observations indicate that Himiko lies off the local L-[C II]-star formation rate scaling relation by a factor of more than 30. Both aspects of our ALMA observations suggest that Himiko is a unique object with a very low dust content and perhaps nearly primordial interstellar gas. Our HST images provide unique insight into the morphology of this remarkable source, highlighting an extremely blue core of activity and two less extreme associated clumps. Himiko is undergoing a triple major merger event whose extensive ionized nebula of Lya emitting gas, discovered in our earlier work with Subaru, is powered by star formation and the dense circumgalactic gas. We are likely witnessing an early massive galaxy during a key period of its mass assembly close to the end of the reionization era. C1 [Ouchi, Masami; Ono, Yoshiaki; Momose, Rieko] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Ouchi, Masami] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Ellis, Richard] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Nakanishi, Kouichiro] Grad Univ Adv Studies SOKENDAI, Mitaka, Tokyo 1818588, Japan. [Nakanishi, Kouichiro; Kurono, Yasutaka] Joint ALMA Observ, Santiago 7630355, Chile. [Kohno, Kotaro; Tamura, Yoichi] Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Kohno, Kotaro; Shimasaku, Kazuhiro] Univ Tokyo, Res Ctr Early Universe WPI, Bunkyo Ku, Tokyo 1130033, Japan. [Ashby, M. L. N.; Willner, S. P.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shimasaku, Kazuhiro] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Iono, Daisuke] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Ouchi, M (reprint author), Univ Tokyo, Inst Cosm Ray Res, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778582, Japan. EM ouchims@icrr.u-tokyo.ac.jp FU NASA STScI [GO 12265]; World Premier International Research Center Initiative (WPI Initiative); MEXT, Japan; KAKENHI [23244025]; Japan Society for the Promotion of Science (JSPS); ADS/JAO.ALMA [2011.0.00115.S]; NASA [NAS 5-26555]; [12265] FX We are grateful to Pratika Dayal, Andrea Ferrara, Rob Kennicutt, Kyoungsoo Lee, Masao Mori, Dominik Riechers, Dimitra Rigopoulou, Daniel Schaerer, Masayuki Umemura, Fabian Walter, and Chris Willott for their useful comments and discussions. We thank the ALMA observatory and HST support staff for their invaluable help that made these pioneering observations possible. The HST reduction was supported by a NASA STScI grant GO 12265. This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and KAKENHI (23244025) Grant-in-Aid for Scientific Research (A) through Japan Society for the Promotion of Science (JSPS). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00115.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC, and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program #12265. Support for program #12265 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 work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 87 TC 70 Z9 70 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 DEC 1 PY 2013 VL 778 IS 2 AR 102 DI 10.1088/0004-637X/778/2/102 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800017 ER PT J AU Raymond, JC Ghavamian, P Williams, BJ Blair, WP Borkowski, KJ Gaetz, TJ Sankrit, R AF Raymond, John C. Ghavamian, Parviz Williams, Brian J. Blair, William P. Borkowski, Kazimierz J. Gaetz, Terrance J. Sankrit, Ravi TI GRAIN DESTRUCTION IN A SUPERNOVA REMNANT SHOCK WAVE SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: individual objects (Cygnus Loop); ISM: supernova remnants; shock waves; ultraviolet: ISM ID LARGE-MAGELLANIC-CLOUD; COSMIC ORIGINS SPECTROGRAPH; CYGNUS-LOOP; DUST DESTRUCTION; INTERSTELLAR-MEDIUM; CHEMICAL-COMPOSITION; NONRADIATIVE SHOCKS; ELEMENTS HYDROGEN; INFRARED-EMISSION; OPTICAL-EMISSION AB Dust grains are sputtered away in the hot gas behind shock fronts in supernova remnants (SNRs), gradually enriching the gas phase with refractory elements. We have measured emission in C IV lambda 1550 from C atoms sputtered from dust in the gas behind a non-radiative shock wave in the northern Cygnus Loop. Overall, the intensity observed behind the shock agrees approximately with predictions from model calculations that match the Spitzer 24 mu m and the X-ray intensity profiles. Thus, these observations confirm the overall picture of dust destruction in SNR shocks and the sputtering rates used in models. However, there is a discrepancy in that the C IV intensity 10 '' behind the shock is too high compared with the intensities at the shock and 25 '' behind it. Variations in the density, hydrogen neutral fraction, and the dust properties over parsec scales in the pre-shock medium limit our ability to test dust destruction models in detail. C1 [Raymond, John C.; Gaetz, Terrance J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ghavamian, Parviz] Towson Univ, Dept Phys Astron & Geosci, Towson, MD 21252 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, Dept Phys, Raleigh, NC 27695 USA. [Sankrit, Ravi] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. RP Raymond, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jraymond@cfa.harvard.edu FU NASA [NAS8-03060]; [HST-GO-12885]; [HST-GO-12545.08] FX This work was performed under grant HST-GO-12885 to the Smithsonian Astrophysical Observatory. P.G was supported under grant HST-GO-12545.08 and T.J.G. acknowledges support under NASA contract NAS8-03060. NR 53 TC 9 Z9 9 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 161 DI 10.1088/0004-637X/778/2/161 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800076 ER PT J AU Shen, Y McBride, CK White, M Zheng, Z Myers, AD Guo, H Kirkpatrick, JA Padmanabhan, N Parejko, JK Ross, NP Schlegel, DJ Schneider, DP Streblyanska, A Swanson, MEC Zehavi, I Pan, K Bizyaev, D Brewington, H Ebelke, G Malanushenko, V Malanushenko, E Oravetz, D Simmons, A Snedden, S AF Shen, Yue McBride, Cameron K. White, Martin Zheng, Zheng Myers, Adam D. Guo, Hong Kirkpatrick, Jessica A. Padmanabhan, Nikhil Parejko, John K. Ross, Nicholas P. Schlegel, David J. Schneider, Donald P. Streblyanska, Alina Swanson, Molly E. C. Zehavi, Idit Pan, Kaike Bizyaev, Dmitry Brewington, Howard Ebelke, Garrett Malanushenko, Viktor Malanushenko, Elena Oravetz, Daniel Simmons, Audrey Snedden, Stephanie TI CROSS-CORRELATION OF SDSS DR7 QUASARS AND DR10 BOSS GALAXIES: THE WEAK LUMINOSITY DEPENDENCE OF QUASAR CLUSTERING AT z similar to 0.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; cosmology: observations; galaxies: active; large-scale structure of universe; quasars: general; surveys ID DIGITAL-SKY-SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; SUPERMASSIVE BLACK-HOLES; HALO OCCUPATION DISTRIBUTION; ACTIVE GALACTIC NUCLEI; DARK-MATTER HALOES; PHOTOMETRICALLY CLASSIFIED QUASARS; QSO REDSHIFT SURVEY; DATA RELEASE 9; LARGE-SCALE STRUCTURE AB We present the measurement of the two-point cross-correlation function (CCF) of 8198 Sloan Digital Sky Survey Data Release 7 quasars and 349,608 Data Release 10 CMASS galaxies from the Baryonic Oscillation Spectroscopic Survey at 0.3 < z < 0.9. The CCF can be reasonably well fit by a power-law model.QG(r) = (r/r0)-. on projected scales of rp = 2-25 h(-1) Mpc with r(0) = 6.61 +/- 0.25 h(-1) Mpc and gamma = 1.69 +/- 0.07. We estimate a quasar linear bias of b(Q) = 1.38 +/- 0.10 at < z > = 0.53 from the CCF measurements, which corresponds to a characteristic host halo mass of similar to 4 x 10(12) h(-1) M-circle dot, compared with a similar to 10(13) h(-1) M-circle dot characteristic host halo mass for CMASS galaxies. Based on the clustering measurements, most quasars at (z) over barz similar to 0.5 are not the descendants of their higher luminosity counterparts at higher redshift, which would have evolved into more massive and more biased systems at low redshift. We divide the quasar sample in luminosity and constrain the luminosity dependence of quasar bias to be dbQ/d logL = 0.20 +/- 0.34 or 0.11 +/- 0.32 (depending on different luminosity divisions) for quasar luminosities -23.5 > Mi (z = 2) > -25.5, implying a weak luminosity dependence of clustering for luminous quasars at (z) over barz similar to 0.5. We compare our measurements with theoretical predictions, halo occupation distribution (HOD) models, and mock catalogs. These comparisons suggest that quasars reside in a broad range of host halos. The host halo mass distributions significantly overlap with each other for quasars at different luminosities, implying a poor correlation between halo mass and instantaneous quasar luminosity. We also find that the quasar HOD parameterization is largely degenerate such that different HODs can reproduce the CCF equally well, but with different satellite fractions and host halo mass distributions. These results highlight the limitations and ambiguities in modeling the distribution of quasars with the standard HOD approach. C1 [Shen, Yue; McBride, Cameron K.; Swanson, Molly E. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shen, Yue] Carnegie Observ, Pasadena, CA 91101 USA. [White, Martin; Kirkpatrick, Jessica A.; Ross, Nicholas P.; Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [White, Martin; Kirkpatrick, Jessica A.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [White, Martin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Zheng, Zheng] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Guo, Hong; Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Padmanabhan, Nikhil; Parejko, John K.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Streblyanska, Alina] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Streblyanska, Alina] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Pan, Kaike; Bizyaev, Dmitry; Brewington, Howard; Ebelke, Garrett; Malanushenko, Viktor; Malanushenko, Elena; Oravetz, Daniel; Simmons, Audrey; Snedden, Stephanie] Apache Point Observ, Sunspot, NM 88349 USA. RP Shen, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. RI Guo, Hong/J-5797-2015; White, Martin/I-3880-2015 OI Guo, Hong/0000-0003-4936-8247; White, Martin/0000-0001-9912-5070 NR 139 TC 33 Z9 34 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR UNSP 98 DI 10.1088/0004-637X/778/2/98 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800013 ER PT J AU Sironi, L Giannios, D AF Sironi, Lorenzo Giannios, Dimitrios TI A LATE-TIME FLATTENING OF LIGHT CURVES IN GAMMA-RAY BURST AFTERGLOWS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; radiation mechanisms: non-thermal; shock waves ID COMPACT OBJECT MERGERS; MASSIVE BLACK-HOLE; PARTICLE-ACCELERATION; TIDAL DISRUPTION; RADIO AFTERGLOW; ELECTROMAGNETIC COUNTERPARTS; ASTROPHYSICAL SHOCKS; GIANT FLARE; GRB 970508; SIMULATIONS AB The afterglow emission from gamma-ray bursts (GRBs) is usually interpreted as synchrotron radiation from relativistic electrons accelerated at the GRB external shock. We investigate the temporal decay of the afterglow emission at late times, when the bulk of the shock-accelerated electrons are non-relativistic (the "deep Newtonian phase," as denoted by Huang and Cheng). We assume that the electron spectrum in the deep Newtonian phase is a power-law distribution in momentum with slope p, as dictated by the theory of Fermi acceleration in non-relativistic shocks. For a uniform circumburst medium, the deep Newtonian phase begins at t(DN) similar to 3 epsilon(5/6)(e,-1)t(ST), where t(ST) marks the transition of the blast wave to the non-relativistic, spherically symmetric Sedov-Taylor (ST) solution, and epsilon(e) = 0.1 epsilon(e,-1) quantifies the amount of shock energy transferred to the electrons. For typical parameters, the deep Newtonian stage starts similar to 0.5 to several years after the GRB. The radio flux in this phase decays as F-nu proportional to t(-3(p+1)/10) proportional to t(-(0.9 divided by 1.2)), for a power-law slope 2 < p < 3. This is shallower than the scaling F-nu proportional to t(-3(5p-7)/10) proportional to t(-(0.9 divided by 2.4)) derived by Frail et al., which only applies if the GRB shock is non-relativistic, but the electron distribution still peaks at ultra-relativistic energies (a regime that is relevant for a narrow time interval, and only if t(DN) greater than or similar to t(ST), namely, epsilon(e) greater than or similar to 0.03). We discuss how the deep Newtonian phase can be reliably used for GRB calorimetry, and we comment on the good detection prospects of trans-relativistic blast waves at 0.1 divided by 10 GHz with the Karl G. Jansky Very Large Array and LOw-Frequency ARray. C1 [Sironi, Lorenzo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Giannios, Dimitrios] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. EM lsironi@cfa.harvard.edu; dgiannio@purdue.edu FU NASA [PF1-120090]; Chandra X-ray Center; Smithsonian Astrophysical Observatory for NASA [NAS8-03060] FX We thank D. Frail, J. Granot, R. Margutti, E. Ramirez-Ruiz, A. van der Horst, and the anonymous referee for insightful comments and suggestions. L.S. is grateful to H. J. van Eerten for help in using the Afterglow Library. 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. NR 54 TC 9 Z9 9 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 DEC 1 PY 2013 VL 778 IS 2 AR UNSP 107 DI 10.1088/0004-637X/778/2/107 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800022 ER PT J AU Sun, XD Hoeksema, JT Liu, Y Aulanier, G Su, YN Hannah, IG Hock, RA AF Sun, Xudong Hoeksema, J. Todd Liu, Yang Aulanier, Guillaume Su, Yingna Hannah, Iain G. Hock, Rachel A. TI HOT SPINE LOOPS AND THE NATURE OF A LATE-PHASE SOLAR FLARE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: flares; Sun: magnetic fields; Sun: UV radiation ID CORONAL MASS EJECTIONS; QUASI-SEPARATRIX LAYERS; UNSTABLE FLUX ROPES; MAGNETIC-FIELD; ACTIVE-REGION; X-RAY; 3 DIMENSIONS; RECONNECTION; TOPOLOGY; MODEL AB The fan-spine magnetic topology is believed to be responsible for many curious features in solar explosive events. A spine field line links distinct flux domains, but direct observation of such a feature has been rare. Here we report a unique event observed by the Solar Dynamic Observatory where a set of hot coronal loops (over 10 MK) connected to a quasi-circular chromospheric ribbon at one end and a remote brightening at the other. Magnetic field extrapolation suggests that these loops are partly tracers of the evolving spine field line. Continuous slipping-and null-point-type reconnections were likely at work, energizing the loop plasma and transferring magnetic flux within and across the fan quasi-separatrix layer. We argue that the initial reconnection is of the "breakout" type, which then transitioned to a more violent flare reconnection with an eruption from the fan dome. Significant magnetic field changes are expected and indeed ensued. This event also features an extreme-ultraviolet (EUV) late phase, i.e., a delayed secondary emission peak in warm EUV lines (about 2-7 MK). We show that this peak comes from the cooling of large post-reconnection loops beside and above the compact fan, a direct product of eruption in such topological settings. The long cooling time of the large arcades contributes to the long delay; additional heating may also be required. Our result demonstrates the critical nature of cross-scale magnetic coupling-topological change in a sub-system may lead to explosions on a much larger scale. C1 [Sun, Xudong; Hoeksema, J. Todd; Liu, Yang] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Aulanier, Guillaume] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92190 Meudon, France. [Su, Yingna] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hannah, Iain G.] Univ Glasgow, SUPA Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Hock, Rachel A.] Air Force Res Lab, Space Vehicle Directorate, Kirtland AFB, NM 87116 USA. RP Sun, XD (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. EM xudong@sun.stanford.edu RI Hannah, Iain/F-1972-2011; Sun, Xudong/M-3245-2013 OI Hannah, Iain/0000-0003-1193-8603; Sun, Xudong/0000-0003-4043-616X FU NASA [NAS5-02139]; NASA contract from LMSAL [SP02H1701R] FX We are grateful to T. Wiegelmann for the NLFFF extrapolation model and J. A. Klimchuk for the EBTEL model. We thank J. Qiu, Q.-R. Chen, W. Liu, C.-L. Shen, A. Malanushenko, and K. Liu for discussion and help on the data analysis. X. Sun, J. T. Hoeksema, and Y. Liu are supported by NASA contract NAS5-02139 (HMI) to Stanford University. Y.-N. S. is supported by NASA contract SP02H1701R from LMSAL to SAO. The SDO data are courtesy of NASA and the AIA, EVE, and HMI science teams. We acknowledge the use of GOES, Hinode, RHESSI, and STEREO data. Magnetic field lines are visualized with VAPOR (http://www.vapor.ucar.edu). The curve fitting is performed with MPFIT (http://purl.com/net/mpfit). NR 101 TC 38 Z9 38 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 DEC 1 PY 2013 VL 778 IS 2 AR 139 DI 10.1088/0004-637X/778/2/139 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800054 ER PT J AU Trichas, M Green, PJ Constantin, A Aldcroft, T Kalfountzou, E Sobolewska, M Hyde, AK Zhou, HY Kim, DW Haggard, D Kelly, BC AF Trichas, Markos Green, Paul J. Constantin, Anca Aldcroft, Tom Kalfountzou, Eleni Sobolewska, Malgosia Hyde, Ashley K. Zhou, Hongyan Kim, Dong-Woo Haggard, Daryl Kelly, Brandon C. TI EMPIRICAL LINKS BETWEEN XRB AND AGN ACCRETION USING THE COMPLETE z < 0.4 SPECTROSCOPIC CSC/SDSS CATALOG SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: Seyfert; quasars: emission lines; quasars: supermassive black holes; X-rays: binaries; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; X-RAY-BRIGHT; CHANDRA MULTIWAVELENGTH PROJECT; OPTICALLY NORMAL GALAXIES; SUPERMASSIVE BLACK-HOLES; SEYFERT-GALAXIES; HELLAS2XMM SURVEY; LOCAL UNIVERSE; HOST GALAXIES AB Striking similarities have been seen between accretion signatures of Galactic X-ray binary (XRB) systems and active galactic nuclei (AGNs). XRB spectral states show a V-shaped correlation between X-ray spectral hardness and Eddington ratio as they vary, and some AGN samples reveal a similar trend, implying analogous processes at vastly larger masses and timescales. To further investigate the analogies, we have matched 617 sources from the Chandra Source Catalog to Sloan Digital Sky Survey spectroscopy, and uniformly measured both X-ray and optical spectral characteristics across a broad range of AGN and galaxy types. We provide useful tabulations of X-ray spectral slope for broad-and narrow-line AGNs, star-forming and passive galaxies, and composite systems, also updating relationships between optical (Ha and [O III]) line emission and X-ray luminosity. We further fit broadband spectral energy distributions with a variety of templates to estimate bolometric luminosity. Our results confirm a significant trend in AGNs between X-ray spectral hardness and Eddington ratio expressed in X-ray luminosity, albeit with significant dispersion. The trend is not significant when expressed in the full bolometric or template-estimated AGN luminosity. We also confirm a relationship between the X-ray/ optical spectral slope aox and Eddington ratio, but it may not follow the trend predicted by analogy with XRB accretion states. C1 [Trichas, Markos] EADS Astrium, Stevenage SG1 2AS, Herts, England. [Trichas, Markos; Green, Paul J.; Aldcroft, Tom; Sobolewska, Malgosia; Kim, Dong-Woo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Constantin, Anca] James Madison Univ, PHCH, Dept Phys & Astron, Harrisonburg, VA 22807 USA. [Kalfountzou, Eleni] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys, Hatfield AL10 9AB, Herts, England. [Hyde, Ashley K.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, London SW7 2AZ, England. [Zhou, Hongyan] Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Peoples R China. [Haggard, Daryl] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys, Evanston, IL 60208 USA. [Kelly, Brandon C.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93107 USA. RP Trichas, M (reprint author), EADS Astrium, Gunnels Wood Rd, Stevenage SG1 2AS, Herts, England. EM markos.trichas@astrium.eads.net RI Zhou, Hai/B-7331-2009; OI Constantin, Anca/0000-0002-2441-1619 FU National Aeronautics and Space Administration through Chandra Award [AR0-11018A, AR1-12016X]; Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; US Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Awards Numbered AR0-11018A and AR1-12016X, 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 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.Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSSWeb 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-PlanckInstitute 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 60 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 DEC 1 PY 2013 VL 778 IS 2 AR UNSP 188 DI 10.1088/0004-637X/778/2/188 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800102 ER PT J AU Tripathi, D Reeves, KK Gibson, SE Srivastava, A Joshi, NC AF Tripathi, Durgesh Reeves, Katharine K. Gibson, Sarah E. Srivastava, Abhishek Joshi, Navin C. TI SDO/AIA OBSERVATIONS OF A PARTIALLY ERUPTING PROMINENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: atmosphere; Sun: corona; Sun: coronal mass ejections; Sun: filaments, prominences; Sun: magnetic fields; Sun: UV radiation ID CORONAL MASS EJECTIONS; MAGNETIC-FLUX ROPE; EMISSION; DOWNFLOW; FLARE; MODEL AB We report an observation of a partially erupting prominence and its associated dynamical plasma processes based on observations recorded by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory. The prominence first went through a slow rise (SR) phase followed by a fast rise (FR) phase. The SR phase began after a couple of small brightenings were seen toward the footpoints. When the prominence had transitioned from SR to FR, it had already become kinked. The prominence shows strong brightening at the central kink location during the start of FR. We interpret this as an internal magnetic reconnection occurring at a vertical current sheet forming between the two legs of the erupting prominence (flux rope). The brightening at the central kink location is seen in all EUV channels of AIA. The contributions of differential emission at higher temperatures are larger compared to that for typical coronal temperatures supporting a reconnection scenario at the central kink location. The plasma above the brightening location is ejected as a hot plasmoid-like structure embedded in a coronal mass ejection, and those below the brightening move down in the form of blobs moving toward the Sun's surface. The unique time resolution of the AIA has allowed these eruptive aspects, including SR-to-FR, kinking, central current sheet formation, plasmoid-like eruption, and filament "splitting," to be observed in a single event, providing strong and comprehensive evidence in favor of the model of partially erupting flux ropes. C1 [Tripathi, Durgesh] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Reeves, Katharine K.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Gibson, Sarah E.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Srivastava, Abhishek; Joshi, Navin C.] Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263129, India. RP Tripathi, D (reprint author), Interuniv Ctr Astron & Astrophys, Pune Univ Campus, Pune 411007, Maharashtra, India. RI Tripathi, Durgesh/D-9390-2012; Reeves, Katharine/P-9163-2014 OI Tripathi, Durgesh/0000-0003-1689-6254; FU DST under the Fast Track Scheme [SERB/F/3369/2012-2013]; Lockheed-Martin [SP02H1701R]; NSF SHINE grant [AGS-1156076]; National Science Foundation FX We acknowledge the suggestions of the referee which improved our manuscript. We thank Yuhong Fan for reviewing the article and providing comments. D.T. acknowledges the support from DST under the Fast Track Scheme (SERB/F/3369/2012-2013). K. K. R. acknowledges support from the contract SP02H1701R from Lockheed-Martin to SAO and the NSF SHINE grant AGS-1156076 to SAO. The National Center for Atmospheric Research is funded by the National Science Foundation. The AIA data are courtesy of SDO (NASA) and the AIA consortium. The STEREO SECCHI data are produced by an international consortium of the Naval Research Laboratory (USA), the Lockheed Martin Solar and Astrophysics Lab (USA), the NASA Goddard Space Flight Center (USA), the Rutherford Appleton Laboratory (UK), the University of Birmingham (UK), the Max-Planck-Institut fur Sonnensystem-forschung (Germany), the Centre Spatiale de Liege (Belgium), the Institut d'Optique Theorique et Appliquee (France), and the Institut d'Astrophysique Spatiale (France). NR 39 TC 14 Z9 14 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR UNSP 142 DI 10.1088/0004-637X/778/2/142 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800057 ER PT J AU Willis, S Marengo, M Allen, L Fazio, GG Smith, HA Carey, S AF Willis, S. Marengo, M. Allen, L. Fazio, G. G. Smith, H. A. Carey, S. TI A WIDE-FIELD NEAR- AND MID-INFRARED CENSUS OF YOUNG STARS IN NGC 6334 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (NGC 6334); stars: formation ID LARGE-MAGELLANIC-CLOUD; NEAR-INFRARED OBSERVATIONS; SPITZER-SPACE-TELESCOPE; INTERSTELLAR CLOUDS; MOLECULAR CLOUDS; STELLAR OBJECTS; MILKY-WAY; FORMATION RATES; AGB STARS; IRAC AB This paper presents a study of the rate and efficiency of star formation in the NGC 6334 star-forming region. We obtained observations at J, H, and Ks taken with the NOAO Extremely Wide-Field Infrared Imager and combined them with observations taken with the Infrared Array Camera (IRAC) on the Spitzer Space Telescope at wavelengths = 3.6, 4.5, 5.8, and 8.0 mu m. We also analyzed previous observations taken at 24 mu m using the Spitzer MIPS camera as part of the MIPSGAL survey. We have produced a point source catalog with > 700,000 entries. We have identified 2283 young stellar object (YSO) candidates, 375 Class I YSOs, and 1908 Class II YSOs using a combination of existing IRAC-based color classification schemes that we have extended and validated to the nearIR for use with warm Spitzer data. We have identified multiple new sites of ongoing star formation activity along filamentary structures extending tens of parsecs beyond the central molecular ridge of NGC 6334. By mapping the extinction, we derived an estimate for the gas mass, 2.2 x 105 M-circle dot. The heavy concentration of protostars along the dense filamentary structures indicates that NGC 6334 may be undergoing a "mini-starburst" event with SSFR > 8.2M(circle dot) Myr-1 pc-2 and SFE > 0.10. We have used these estimates to place NGC 6334 in the Kennicutt-Schmidt diagram to help bridge the gap between observations of local low-mass star-forming regions and star formation in other galaxies. C1 [Willis, S.; Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50010 USA. [Allen, L.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Fazio, G. G.; Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Carey, S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Willis, S (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50010 USA. EM swillis@cfa.harvard.edu FU NASA [NNX12AI55G, NNX10AD68G, JPL-RSA 1369565] FX We acknowledge the assistance of Robert Gutermuth, Vallia Antoniou, Andres Guzman, and Rafael Martinez during the preparation of this manuscript. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. S.W. acknowledges partial support from NASA grants NNX12AI55G and NNX10AD68G, and JPL-RSA 1369565. NR 69 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR UNSP 96 DI 10.1088/0004-637X/778/2/96 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800011 ER PT J AU Ackermann, M Ajello, M Allafort, A Atwood, WB Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Belfiore, A Bellazzini, R Bernieri, E Bissaldi, E Bloom, ED Bonamente, E Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Burnett, TH Buson, S Caliandro, GA Cameron, RA Campana, R Caraveo, PA Casandjian, JM Cavazzuti, E Cecchi, C Charles, E Chaves, RCG Chekhtman, A Cheung, CC Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Cominsky, LR Conrad, J Cutini, S D'Ammando, F De Angelis, A De Palma, F Dermer, CD Desiante, R Digel, SW Di Venere, L Drell, PS Drlica-Wagner, A Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Fortin, P Franckowiak, A Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giommi, P Giordano, F Giroletti, M Godfrey, G Gomez-Vargas, GA Grenier, IA Guiriec, S Hadasch, D Hanabata, Y Harding, AK Hayashida, M Hays, E Hewitt, J Hill, AB Horan, D Hughes, RE Jogler, T Johannesson, G Johnson, AS Johnson, TJ Johnson, WN Kamae, T Kataoka, J 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 Massaro, E Mayer, M Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mizuno, T Moiseev, AA Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nemmen, R Nuss, E Ohsugi, T Okumura, A Orienti, M Ormes, JF Paneque, D Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Porter, TA Raino, S Razzano, M Reimer, A Reimer, O Reposeur, T Ritz, S Romani, RW Roth, M Parkinson, PMS Schulz, A Sgro, C Siskind, EJ Smith, DA Spandre, G Spinelli, P Stawarz, L Strong, AW Suson, DJ Takahashi, H Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Torres, DF Tosti, G Troja, E Uchiyama, Y Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Werner, M Winer, BL Wood, KS Wood, M AF Ackermann, M. Ajello, M. Allafort, A. Atwood, W. B. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Belfiore, A. Bellazzini, R. Bernieri, E. Bissaldi, E. Bloom, E. D. Bonamente, E. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Burnett, T. H. Buson, S. Caliandro, G. A. Cameron, R. A. Campana, R. Caraveo, P. A. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Charles, E. Chaves, R. C. G. Chekhtman, A. Cheung, C. C. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Cominsky, L. R. Conrad, J. Cutini, S. D'Ammando, F. De Angelis, A. De Palma, F. Dermer, C. D. Desiante, R. Digel, S. W. Di Venere, L. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Fortin, P. Franckowiak, A. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Godfrey, G. Gomez-Vargas, G. A. Grenier, I. A. Guiriec, S. Hadasch, D. Hanabata, Y. Harding, A. K. Hayashida, M. Hays, E. Hewitt, J. Hill, A. B. Horan, D. Hughes, R. E. Jogler, T. Johannesson, G. Johnson, A. S. Johnson, T. J. Johnson, W. N. Kamae, T. Kataoka, J. Kawano, T. Knodlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lemoine-Goumard, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Massaro, E. Mayer, M. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nemmen, R. Nuss, E. Ohsugi, T. Okumura, A. Orienti, M. Ormes, J. F. Paneque, D. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Porter, T. A. Raino, S. Razzano, M. Reimer, A. Reimer, O. Reposeur, T. Ritz, S. Romani, R. W. Roth, M. Parkinson, P. M. Saz Schulz, A. Sgro, C. Siskind, E. J. Smith, D. A. Spandre, G. Spinelli, P. Stawarz, Lukasz Strong, A. W. Suson, D. J. Takahashi, H. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Uchiyama, Y. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Werner, M. Winer, B. L. Wood, K. S. Wood, M. TI THE FIRST FERMI-LAT CATALOG OF SOURCES ABOVE 10 GeV SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; gamma rays: general ID LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; PULSAR WIND NEBULA; BLIND FREQUENCY SEARCHES; NANCAY RADIO TELESCOPE; SUPERNOVA REMNANT; SPACE-TELESCOPE; MILLISECOND PULSARS; CRAB PULSAR; MULTIWAVELENGTH OBSERVATIONS AB We present a catalog of gamma-ray sources at energies above 10 GeV based on data from the Large Area Telescope (LAT) accumulated during the first 3 yr of the Fermi Gamma-ray Space Telescope mission. The first Fermi catalog of > 10 GeV sources (1FHL) has 514 sources. For each source we present location, spectrum, a measure of variability, and associations with cataloged sources at other wavelengths. We found that 449 (87%) could be associated with known sources, of which 393 (76% of the 1FHL sources) are active galactic nuclei. Of the 27 sources associated with known pulsars, we find 20 (12) to have significant pulsations in the range > 10 GeV (> 25 GeV). In this work we also report that, at energies above 10 GeV, unresolved sources account for 27% +/- 8% of the isotropic. gamma-ray background, while the unresolved Galactic population contributes only at the few percent level to the Galactic diffuse background. We also highlight the subset of the 1FHL sources that are best candidates for detection at energies above 50-100 GeV with current and future ground-based gamma-ray observatories. C1 [Ackermann, M.; Buehler, R.; Mayer, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Allafort, A.; Bechtol, K.; Bloom, E. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Funk, S.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Okumura, A.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Allafort, A.; Bechtol, K.; Bloom, E. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Funk, S.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Okumura, A.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; 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. [Atwood, W. B.; Belfiore, A.; Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Belfiore, A.; Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Desiante, R.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Belfiore, A.] Univ Pavia, I-27100 Pavia, Italy. [Belfiore, A.; Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, 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. [Bernieri, E.] Ist Nazl Fis Nucl, Lab Nazl Frascati, I-00044 Frascati, Roma, Italy. [Bernieri, E.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. [Bissaldi, E.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Bissaldi, E.] Univ Trieste, I-34127 Trieste, Italy. [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. [Brandt, T. J.; Ferrara, E. C.; Gehrels, N.; Guiriec, S.; Harding, A. K.; Hays, E.; Hewitt, J.; McEnery, J. E.; Nemmen, R.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brigida, M.; De Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; De Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [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.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Burnett, T. H.; Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Campana, R.] INAF IASF Bologna, I-40129 Bologna, Italy. [Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Giommi, P.] ASI, Sci Data Ctr, I-00044 Frascati, Roma, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Cheung, C. C.; Dermer, C. D.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Roma, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, F-34095 Montpellier, France. [Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Conrad, J.; Larsson, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.; Larsson, S.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, 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.; Drlica-Wagner, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [De Angelis, A.; Drlica-Wagner, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Fortin, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Gomez-Vargas, G. A.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. [Gomez-Vargas, G. A.] Univ Autonoma Madrid, Inst Fis Teor IFT UAM CSIC, E-28049 Madrid, Spain. [Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Hanabata, Y.; Hayashida, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Johnson, T. J.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Kawano, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Knodlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knodlseder, J.] Univ Toulouse, GAHEC, IRAP, UPS OMP, F-31028 Toulouse, France. [Paneque, D.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Lemoine-Goumard, M.; Lott, B.; Mehault, J.; Reposeur, T.; Smith, D. A.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, IN2P3, CNRS, F-33175 Gradignan, France. [Massaro, E.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA. [Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Murgia, S.] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA. [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. [Parkinson, P. M. Saz] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Stawarz, Lukasz] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Stawarz, Lukasz] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Schulz, A.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Torres, D. F.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain. [Gomez-Vargas, G. A.] ICREA, E-08010 Barcelona, Spain. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM digel@stanford.edu; fortin@veritas.sao.arizona.edu; dpaneque@mppmu.mpg.de RI Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Gomez-Vargas, German/C-7138-2015; Campana, Riccardo/F-5272-2015; 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; Bissaldi, Elisabetta/K-7911-2016; Torres, Diego/O-9422-2016; Di Venere, Leonardo/C-7619-2017; OI orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; Campana, Riccardo/0000-0002-4794-5453; 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; Bissaldi, Elisabetta/0000-0001-9935-8106; Torres, Diego/0000-0002-1522-9065; Di Venere, Leonardo/0000-0003-0703-824X; giommi, paolo/0000-0002-2265-5003; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Hill, Adam/0000-0003-3470-4834; Bastieri, Denis/0000-0002-6954-8862; Pesce-Rollins, Melissa/0000-0003-1790-8018 NR 131 TC 85 Z9 87 U1 1 U2 25 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2013 VL 209 IS 2 AR UNSP 34 DI 10.1088/0067-0049/209/2/34 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266YG UT WOS:000328059500016 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 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies: clusters: general; infrared: galaxies; surveys ID IRAC SHALLOW SURVEY; GALAXY CLUSTERS; SUNYAEV-ZELDOVICH; SPACE-TELESCOPE; MASS FRACTIONS; SKY; PERFORMANCE; MODEL; GAS; CALIBRATION AB The Spitzer South Pole Telescope Deep Field (SSDF) is a wide-area survey using Spitzer's Infrared Array Camera (IRAC) to cover 94 deg(2) of extragalactic sky, making it the largest IRAC survey completed to date outside the Milky Way midplane. The SSDF is centered at (alpha, delta) = (23:30, -55:00), in a region that combines observations spanning a broad wavelength range from numerous facilities. These include millimeter imaging from the South Pole Telescope, far-infrared observations from Herschel/SPIRE, X-ray observations from the XMM XXL survey, near-infrared observations from the VISTA Hemisphere Survey, and radio-wavelength imaging from the Australia Telescope Compact Array, in a panchromatic project designed to address major outstanding questions surrounding galaxy clusters and the baryon budget. Here we describe the Spitzer/IRAC observations of the SSDF, including the survey design, observations, processing, source extraction, and publicly available data products. In particular, we present two band-merged catalogs, one for each of the two warm IRAC selection bands. They contain roughly 5.5 and 3.7 million distinct sources, the vast majority of which are galaxies, down to the SSDF 5 sigma sensitivity limits of 19.0 and 18.2 Vega mag (7.0 and 9.4 mu Jy) at 3.6 and 4.5 mu m, respectively. 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, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA IRFU, 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.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Muzzin, A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Pacaud, F.] Argelander Inst Astron, D-53121 Bonn, Germany. [Pierre, M.] CEA, DSM, AIM IRFU, 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 OI Marrone, Daniel/0000-0002-2367-1080 FU NASA [1439357]; U. S. Department of Energy, National Nuclear Security Administration [DE-AC52-07NA27344]; Deutches Zenturm fur Luft-und Raumfahrt (DLR) [50 OR 1117] 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 contract with the National Aeronautics and Space Administration (NASA). Support was provided by NASA through contract number 1439357 issued by JPL/Caltech. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. Lawrence Livermore National Laboratory is operated by Lawrence Livermore National Security, LLC, for the U. S. Department of Energy, National Nuclear Security Administration under Contract DE-AC52-07NA27344. F.P. acknowledges support from grant 50 OR 1117 of the Deutches Zenturm fur Luft-und Raumfahrt (DLR). We thank Dave Nair for his efforts in characterizing a preliminary reduction of the SSDF images. We also thank Richard G. Arendt, who kindly computed the Milky Way star count models shown in Figure 8. NR 45 TC 16 Z9 16 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2013 VL 209 IS 2 AR UNSP 22 DI 10.1088/0067-0049/209/2/22 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266YG UT WOS:000328059500004 ER PT J AU Kaminski, T Gottlieb, CA Young, KH Menten, KM Patel, NA AF Kaminski, T. Gottlieb, C. A. Young, K. H. Menten, K. M. Patel, N. A. TI AN INTERFEROMETRIC SPECTRAL LINE AND IMAGING SURVEY OF VY CANIS MAJORIS IN THE 345 GHz BAND SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astrochemistry; circumstellar matter; line: identification; stars: individual (VY CMa); supergiants; surveys ID SIO MASER EMISSION; LATE-TYPE STARS; 3-DIMENSIONAL MORPHOLOGY; CIRCUMSTELLAR ENVELOPE; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; J=5-4 TRANSITION; DUST SHELLS; SUBMILLIMETER; KINEMATICS AB A spectral line survey of the oxygen-rich red supergiant VY Canis Majoris was made between 279 and 355 GHz with the Submillimeter Array (SMA). Two hundred twenty-three spectral features from 19 molecules (not counting isotopic species of some of them) were observed, including the rotational spectra of TiO, TiO2, and AlCl for the first time in this source. The parameters and an atlas of all spectral features are presented. Observations of each line with a synthesized beam of similar to 0 ''.9, reveal the complex kinematics and morphology of the nebula surrounding VY CMa. Many of the molecules are observed in high-lying rotational levels or in excited vibrational levels. From these, it was established that the main source of the submillimeter-wave continuum (dust) and the high-excitation molecular gas (the star) are separated by about 0 ''.15. Apparent coincidences between the molecular gas observed with the SMA, and some of the arcs and knots observed at infrared wavelengths and in the optical scattered light by the Hubble Space Telescope are identified. The observations presented here provide important constraints on the molecular chemistry in oxygen-dominated circumstellar environments and a deeper picture of the complex circumstellar environment of VY CMa. C1 [Kaminski, T.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Gottlieb, C. A.; Young, K. H.; Patel, N. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kaminski, T (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM kaminski@mpifr.de NR 43 TC 12 Z9 12 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2013 VL 209 IS 2 AR UNSP 38 DI 10.1088/0067-0049/209/2/38 PG 47 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266YG UT WOS:000328059500020 ER PT J AU Prud'homme, G Dobbin, NA Sun, L Burnett, RT Martin, RV Davidson, A Cakmak, S Villeneuve, PJ Lamsal, LN van Donkelaar, A Peters, PA Johnson, M AF Prud'homme, Genevieve Dobbin, Nina A. Sun, Liu Burnett, Richard T. Martin, Randall V. Davidson, Andrew Cakmak, Sabit Villeneuve, Paul J. Lamsal, Lok N. van Donkelaar, Aaron Peters, Paul A. Johnson, Markey TI Comparison of remote sensing and fixed-site monitoring approaches for examining air pollution and health in a national study population SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Air pollution; Satellite remote sensing; Regulatory monitoring; Asthma; Allergy; Population health; Epidemiology ID LONG-TERM EXPOSURE; FINE PARTICULATE MATTER; AMERICAN-CANCER-SOCIETY; NITROGEN-DIOXIDE; CHILDHOOD ASTHMA; PUBLIC-HEALTH; CARDIOVASCULAR-DISEASE; UNITED-STATES; PROMISED LAND; QUALITY AB Satellite remote sensing (RS) has emerged as a cutting edge approach for estimating ground level ambient air pollution. Previous studies have reported a high correlation between ground level PM2.5 and NO2 estimated by RS and measurements collected at regulatory monitoring sites. The current study examined associations between air pollution and adverse respiratory and allergic health outcomes using multi-year averages of NO2 and PM2.5 from RS and from regulatory monitoring. RS estimates were derived using satellite measurements from OMI, MODIS, and MISR instruments. Regulatory monitoring data were obtained from Canada's National Air Pollution Surveillance Network. Self-reported prevalence of doctor-diagnosed asthma, current asthma, allergies, and chronic bronchitis were obtained from the Canadian Community Health Survey (a national sample of individuals 12 years of age and older). Multi-year ambient pollutant averages were assigned to each study participant based on their six digit postal code at the time of health survey, and were used as a marker for long-term exposure to air pollution. RS derived estimates of NO2 and PM2.5 were associated with 6-10% increases in respiratory and allergic health outcomes per interquartile range (3.97 mu g m(-3) for PM2.5 and 1.03 ppb for NO2) among adults (aged 20-64) in the national study population. Risk estimates for air pollution and respiratory/allergic health outcomes based on RS were similar to risk estimates based on regulatory monitoring for areas where regulatory monitoring data were available (within 40 km of a regulatory monitoring station). RS derived estimates of air pollution were also associated with adverse health outcomes among participants residing outside the catchment area of the regulatory monitoring network (p < 0.05). The consistency between risk estimates based on RS and regulatory monitoring as well as the associations between air pollution and health among participants living outside the catchment area for regulatory monitoring suggest that RS can provide useful estimates of long-term ambient air pollution in epidemiologic studies. This is particularly important in rural communities and other areas where monitoring and modeled air pollution data are limited or unavailable. Crown Copyright (C) 2013 Published by Elsevier Ltd. All rights reserved. C1 [Prud'homme, Genevieve; Dobbin, Nina A.; Sun, Liu; Johnson, Markey] Hlth Canada, Air Hlth Sci Div, Ottawa, ON K1A 0K9, Canada. [Burnett, Richard T.; Cakmak, Sabit; Villeneuve, Paul J.] Hlth Canada, Populat Studies Div, Ottawa, ON K1A 0K9, Canada. [Martin, Randall V.; van Donkelaar, Aaron] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Davidson, Andrew] Agr & Agri Food Canada, Earth Observat Serv, Ottawa, ON, Canada. [Davidson, Andrew] Carleton Univ, Dept Geog & Environm Studies, Ottawa, ON K1S 5B6, Canada. [Villeneuve, Paul J.] Carleton Univ, Inst Hlth Sci Technol & Policy, Ottawa, ON K1S 5B6, Canada. [Villeneuve, Paul J.] Univ Toronto, Dalla Lana Sch Publ Hlth, Toronto, ON, Canada. [Lamsal, Lok N.] Univ Space Res Assoc, Columbia, MD USA. [Lamsal, Lok N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Peters, Paul A.] STAT Canada, Hlth Anal Div, Ottawa, ON, Canada. RP Johnson, M (reprint author), Hlth Canada, Water & Air Qual Bur, Air Hlth Sci Div, 269 Laurier Ave West,Room 4-039, Ottawa, ON K1A 0K9, Canada. EM markey.johnson@hc-sc.gc.ca RI Mashamba-Thompson, Tivani /B-6087-2014; Martin, Randall/C-1205-2014; OI Martin, Randall/0000-0003-2632-8402; Cakmak, Sabit/0000-0001-9921-2107; Peters, Paul/0000-0001-5225-2005 NR 90 TC 4 Z9 5 U1 2 U2 51 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2013 VL 80 BP 161 EP 171 DI 10.1016/j.atmosenv.2013.07.020 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 267JV UT WOS:000328094800017 ER PT J AU Engel-Cox, J Oanh, NTK van Donkelaar, A Martin, RV Zell, E AF Engel-Cox, Jill Nguyen Thi Kim Oanh van Donkelaar, Aaron Martin, Randall V. Zell, Erica TI Toward the next generation of air quality monitoring: Particulate Matter SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Particulate matter; Aerosols; Monitoring; Policy; Indicators ID POLLUTION EXPOSURE; GLOBAL BURDEN; LAND; REGRESSION; OUTDOOR; DISEASE; MODELS; PM10 AB Fine particulate matter is one of the key global pollutants affecting human health. Satellite and ground-based monitoring technologies as well as chemical transport models have advanced significantly in the past 50 years, enabling improved understanding of the sources of fine particles, their chemical composition, and their effect on human and environmental health. The ability of air pollution to travel across country and geographic boundaries makes particulate matter a global problem. However, the variability in monitoring technologies and programs and poor data availability make global comparison difficult. This paper summarizes fine particle monitoring, models that integrate ground-based and satellite-based data, and communications, then recommends steps for policymakers and scientists to take to expand and improve local and global indicators of particulate matter air pollution. One of the key set of recommendations to improving global indicators is to improve data collection by basing particulate matter monitoring design and stakeholder communications on the individual country, its priorities, and its level of development, while at the same time creating global data standards for inter-country comparisons. When there are good national networks that produce consistent quality data that is shared openly, they serve as the foundation for better global understanding through data analysis, modeling, health impact studies, and communication. Additionally, new technologies and systems should be developed to expand personal air quality monitoring and participation of non-specialists in crowd-sourced data collections. Finally, support to the development and improvement of global multi-pollutant indicators of the health and economic effects of air pollution is essential to addressing improvement of air quality around the world. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Engel-Cox, Jill] Battelle Mem Inst, Columbus, OH 43201 USA. [Nguyen Thi Kim Oanh] Asian Inst Technol, Klongluang 12120, Pathumthani, Thailand. [van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Halifax, NS B3H 4R2, Canada. [Zell, Erica] Battelle Mem Inst, Arlington, VA 22201 USA. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Engel-Cox, J (reprint author), Battelle Mem Inst, 505 King Ave, Columbus, OH 43201 USA. EM engelcoxj@battelle.org RI Martin, Randall/C-1205-2014 OI Martin, Randall/0000-0003-2632-8402 NR 44 TC 23 Z9 23 U1 7 U2 52 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2013 VL 80 BP 584 EP 590 DI 10.1016/j.atmosenv.2013.08.016 PG 7 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 267JV UT WOS:000328094800064 ER PT J AU Durkan, TH Yeung, NW Meyer, WM Hayes, KA Cowie, RH AF Durkan, Torsten H. Yeung, Norine W. Meyer, Wallace M., III Hayes, Kenneth A. Cowie, Robert H. TI Evaluating the efficacy of land snail survey techniques in Hawaii: implications for conservation throughout the Pacific SO BIODIVERSITY AND CONSERVATION LA English DT Article DE Gastropoda; Inventory; Micromolluscs; Mollusca; Sampling methods ID MOLLUSK COMMUNITIES; FRENCH-POLYNESIA; SPECIES RICHNESS; DIVERSITY; DECLINE; PULMONATA; FORESTS; FAUNAS; SAMOA AB Terrestrial micromolluscs (snails with an adult maximum shell dimension < 5 mm) constitute a considerable proportion of the land snail fauna of the Pacific. However, micromolluscs are often underestimated in biological surveys because of size bias. It has been argued that visual searches are preferable on Pacific islands because: (1) size biases are limited based on the understanding that most native Pacific island land snails are very small, and (2) amount of labor is less than other methods such as soil surveys and adequate for inventory purposes (though not for abundance assessments). To test whether visual surveys and soil surveys were accurately recording all taxa, land snail inventories were completed in three forest reserves (5 sampling sites in each) on the island of Oahu, Hawaii. Visual surveys involved 30-min visual search in a 10 m(2) site; soil surveys involved sieving leaf litter and topsoil from four 0.3 m(2) quadrats and extracting snails with the aid of a microscope. The data indicate a size and microhabitat bias associated with both techniques. Visual surveys consistently collected large arboreal and litter-dwelling species but missed a significant portion of micromolluscs, while soil surveys collected micromolluscs but missed larger snails. Because of such biases, employing both methods is critical for collecting all taxa at a survey location. As such, we recommend that future land snail surveys on Pacific Islands incorporate both survey techniques. Obtaining a complete inventory is critical if we are to understand species distributions and patterns of diversity and make well-informed conservation recommendations. C1 [Durkan, Torsten H.; Yeung, Norine W.; Hayes, Kenneth A.; Cowie, Robert H.] Univ Hawaii, Pacific Biosci Res Ctr, Honolulu, HI 96822 USA. [Yeung, Norine W.; Hayes, Kenneth A.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Meyer, Wallace M., III] Pomona Coll, Dept Biol, Claremont, CA 91711 USA. [Hayes, Kenneth A.] Howard Univ, Dept Biol, Washington, DC 20059 USA. RP Hayes, KA (reprint author), Howard Univ, Dept Biol, 415 Coll St NW,EE Just Hall 332, Washington, DC 20059 USA. EM kenneth.hayes@howard.edu FU Oahu Army Natural Resource Program grant; National Science Foundation [DEB-1120906]; University of Hawaii FX We thank Dylan Ressler, Patrick Curry, David Sischo, Jaynee Kim, Kelsey Coleman, Taryn Takebayashi, Celeste Yee, Vince Costello and Stephanie Joe for assistance in the field and lab. T.H. Durkan and N.W. Yeung were supported by an Oahu Army Natural Resource Program grant (PI Yeung). This work was also supported by National Science Foundation grant DEB-1120906 to K.A. Hayes and a University of Hawaii Undergraduate Research Opportunities Program grant to T.H. Durkan. We thank the Division of Forestry and Wildlife (Department of Land and Natural Resources) for permits. NR 26 TC 5 Z9 5 U1 4 U2 14 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 DEC PY 2013 VL 22 IS 13-14 BP 3223 EP 3232 DI 10.1007/s10531-013-0580-7 PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 257OV UT WOS:000327395300014 ER PT J AU Athanasiadis, A Ballantine, DL Ruiz, H AF Athanasiadis, Athanasios Ballantine, David L. Ruiz, Hector TI Hydrolithon abyssophila sp nov. (Hydrolithoideae, Corallinales), a bisporic coralline from the insular shelf edge of Puerto Rico and the Virgin Islands (US) SO BOTANICA MARINA LA English DT Article DE Caribbean Sea; Hydrolithon; mesophotic zone; Porolithon; taxonomy; uninucleate bispores ID MASTOPHOROIDEAE CORALLINALES; RHODOPHYTA; FOSLIE; NUCLEAR AB A new species of Hydrolithon is described from mesophotic habitats, between 30 and at least 76 m depth, off La Parguera, Puerto Rico, and St Thomas, Virgin Islands (Caribbean Sea). Its encrusting thallus covers corals and rocks. Hydrolithon abyssophila sp. nov. is distinctive in developing bisporangia that are about twice as large as its congeners and in lacking both perithallial protuberances and trichocytes in horizontal or vertical groups. It reproduces primarily by uninucleate bispores that presumably recycle the parental phase. Unfertilized carpogonia were observed in one collection suggesting the rare occurrence of gametophytic reproduction in the species. C1 [Athanasiadis, Athanasios] Univ Gothenburg, SE-40530 Gothenburg, Sweden. [Ballantine, David L.; Ruiz, Hector] Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00681 USA. [Ballantine, David L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Athanasiadis, A (reprint author), Univ Gothenburg, POB 461, SE-40530 Gothenburg, Sweden. EM Athanasios.Athanasiadis@bioenv.gu.se FU Captain Stenholms Foundation; The Royal Society of Arts and Sciences in Goteborg; National Oceanographic and Atmospheric Administration Coastal Ocean Program [NA17OP2919, NA06NOS4780190] FX Financial support for the field and laboratory work was provided through grants from the Captain Stenholms Foundation and The Royal Society of Arts and Sciences in Goteborg to Athanasios Athanasiadis. David L. Ballantine and Hector Ruiz acknowledge funding by the National Oceanographic and Atmospheric Administration Coastal Ocean Program under award #NA17OP2919 and (in part) #NA06NOS4780190 to the University of Puerto Rico - Mayaguez. We also thank three anonymous referees for their helpful comments. NR 32 TC 2 Z9 2 U1 1 U2 4 PU WALTER DE GRUYTER GMBH PI BERLIN PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY SN 0006-8055 EI 1437-4323 J9 BOT MAR JI Bot. Marina PD DEC PY 2013 VL 56 IS 5-6 BP 495 EP 505 DI 10.1515/bot-2013-0019 PG 11 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 269UM UT WOS:000328267600009 ER PT J AU Alba-Mejia, L Caillaud, D Montenegro, OL Sanchez-Palomino, P Crofoot, MC AF Alba-Mejia, Lilian Caillaud, Damien Montenegro, Olga L. Sanchez-Palomino, Pedro Crofoot, Margaret C. TI Spatiotemporal Interactions Among Three Neighboring Groups of Free-Ranging White-Footed Tamarins (Saguinus leucopus) in Colombia SO INTERNATIONAL JOURNAL OF PRIMATOLOGY LA English DT Article DE Home range overlap; Radio-telemetry; Spatial attraction; Territoriality ID HOME-RANGE; CALLITHRIX-JACCHUS; COMMON MARMOSETS; BLUE MONKEYS; PATTERNS; PRIMATES; DEFENSE; MYSTAX; FOREST; SIZE AB Successful conservation requires an understanding of animal movement patterns and space use. Such data are hard to obtain, however, when difficult terrain, nocturnal habits, or lack of habituation make direct observation impractical. White-footed tamarins (Saguinus leucopus) are small primates endemic to Colombia that are in danger of extinction due to habitat loss, fragmentation, and the illegal pet trade. Here, we report the results of the first study to use radio-tracking to investigate white-footed tamarin ranging behavior. We recorded the movements of three neighboring tamarin groups simultaneously for 3 month using radio-telemetry. Home range sizes (estimated using both minimum convex polygon and fixed kernel contour methods) were substantially larger than reported in previous studies that did not use remote-tracking. Monte Carlo resampling procedures revealed that home range size differed significantly among the three groups but that the mean daily path length did not. As in other tamarin species, the degree of range overlap between neighboring social groups was high, ranging from 27 to 81%. Using a randomization test, we showed that the observed mean distance between groups was significantly lower than expected by chance for two of the three group dyads. This pattern of intergroup "attraction," in conjunction with substantial range overlap and high population density, implies that the Bellavista Forest, one of the few remaining habitats of Saguinus leucopus, may be saturated, and promoting habitat restoration should be a priority for the conservation of this species. C1 [Alba-Mejia, Lilian; Montenegro, Olga L.; Sanchez-Palomino, Pedro] Univ Nacl Colombia, Grp Conservac & Manejo Vida Silvestre, Inst Ciencias Nat, Bogota 11001000, Colombia. [Alba-Mejia, Lilian; Crofoot, Margaret C.] Smithsonian Trop Res Inst, Panama City, Panama. [Caillaud, Damien] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Caillaud, Damien] Dian Fossey Gorilla Fund Int, Atlanta, GA 30315 USA. [Crofoot, Margaret C.] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, D-78315 Radolfzell am Bodensee, Germany. [Crofoot, Margaret C.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. RP Crofoot, MC (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama. EM crofootm@si.edu FU regional environmental government authority CORPOCALDAS (Corporacion Autonoma Regional de Caldas); Margot Marsh Foundation; Wildlife Conservation Society; Fundacion Biodiversa Colombia; Colciencias (Programa Jovenes Investigadores e Innovadores "Virginia Gutierrez de Pineda"); Grupo en Conservacion y Manejo de Vida Silvestre (Universidad Nacional de Colombia); Smithsonian Tropical Research Institute; Max Planck Institute for Ornithology; NSF [DEB-0749097] FX We thank the regional environmental government authority CORPOCALDAS (Corporacion Autonoma Regional de Caldas) for permission to conduct this research and for financial support. We also thank Luis Soto (Proyecto Titi Foundation) for training in the capture and radio collaring of tamarins, and Asociacion de Veterinarios de Vida Silvestre and the staff from Centro de Rehabilitacion de Fauna Silvestre del Oriente de Caldas (CRFSOC) for technical support. We thank Andres, Efrain, Amilvia, Jose, Willy, and the family Carvajal Betancur for their support during the field work. We thank Oscar Ospina, Nestor Roncancio, Adriana Bilgray, and Oris Acevedo for logistical support; Vanessa Perez, Jesualdo Fuentes, and Egbert Leigh for helpful suggestions; and Ryan Chisolm for statistical advice. We also thank the anonymous reviewers whose comments have improved this manuscript. Funding for this project was provided by the Margot Marsh Foundation, the Wildlife Conservation Society, Fundacion Biodiversa Colombia, Colciencias (Programa Jovenes Investigadores e Innovadores "Virginia Gutierrez de Pineda"), Grupo en Conservacion y Manejo de Vida Silvestre (Universidad Nacional de Colombia), the Smithsonian Tropical Research Institute, and the Max Planck Institute for Ornithology. D. Caillaud was supported by NSF grant DEB-0749097 to L. A. Meyers NR 45 TC 3 Z9 3 U1 5 U2 27 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0164-0291 EI 1573-8604 J9 INT J PRIMATOL JI Int. J. Primatol. PD DEC PY 2013 VL 34 IS 6 BP 1281 EP 1297 DI 10.1007/s10764-013-9740-6 PG 17 WC Zoology SC Zoology GA 269SO UT WOS:000328262400012 ER PT J AU Quattrocchio, ME Martinez, MA Hinojosa, LF Jaramillo, C AF Quattrocchio, Mirta E. Martinez, Marcelo A. Felipe Hinojosa, Luis Jaramillo, Carlos TI Quantitative analysis of Cenozoic palynofloras from Patagonia, southern South America SO PALYNOLOGY LA English DT Article DE Cenozoic; southern South America; Patagonia; palynofloras; statistics ID PALEOGENE-EARLY NEOGENE; HUITRERA FORMATION; ARGENTINA; MIOCENE; PALYNOLOGY; PALEOGEOGRAPHY; EVOLUTION; FORESTS; ANDES; PALYNOSTRATIGRAPHY AB The statistical analysis of published Paleocene-Late Miocene palynological data from Patagonia supports several major stages of vegetation. These stages represent distinctive floral assemblages, both in composition and structure. Detrended correspondence analysis shows that during the Paleocene, southern South America was dominated by Australasian, Neotropical and Pantropical phytogeographical elements (Gondwanic paleoflora). The climate was warm and very humid. The Early Eocene was dominated by Neotropical and Pantropical taxa (Subtropical Gondwanic Paleoflora) and a reduced proportion of Australasian and a low proportion of Antarctic elements. The Middle Eocene and Oligocene were characterized by the Mixed Paleoflora' with the exception of the Sloggett Formation. The climate was less humid due to the onset of the Antarctic glaciation. The presence of Antarctic palynomorphs (Nothofagaceae, Podocarpaceae, Proteaceae) in Patagonia is consistent with the global cooling trend during the Late Eocene and Early Oligocene. By the Late Oligocene-Early Miocene, warm climates allowed the southward dispersal of Neotropical elements (palms, Cupania, Alchornea, Rubiaceae, Combretaceae), adding megathermal elements to the local Gondwanic floras. The appearance of some Neotropical families (Symplocaceae, Euphorbiaceae Alchornea) may indicate the Late Oligocene global warming event. The rise of xerophytic and halophytic shrubby-herbaceous elements (Convolvulaceae, Asteraceae, Poaceae, Chenopodiaceae and Ephedraceae) during the Late Oligocene, becoming more abundant during the Early Miocene began to give a modern appearance to plant communities. The Early-Middle Miocene corresponds to the Transitional Paleophytogeoprovince of central and southeastern Argentina, defined by a mix of Neotropical and Austral components. The Middle-Late Miocene was characterized by the final demise of megathermal elements in Patagonia, coupled with an increasing diversity and abundance of xerophytic adapted taxa, including Asteraceae, Chenopodiaceae and Convolvulaceae. Late Miocene vegetation was similar to the present vegetation, with the steppe expanded across extra-Andean Patagonia and the forest restricted to western areas where rainfall was still abundant. C1 [Quattrocchio, Mirta E.; Martinez, Marcelo A.] Univ Nacl Sur, Dept Geol, CONICET, INGEOSUR, RA-8000 Bahia Blanca, Buenos Aires, Argentina. [Felipe Hinojosa, Luis] Univ Chile, Fac Ciencias, Dept Ecol, Santiago, Chile. [Felipe Hinojosa, Luis] Inst Ecol & Biodiversidad, Santiago, Chile. [Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa, Panama. RP Quattrocchio, ME (reprint author), Univ Nacl Sur, Dept Geol, CONICET, INGEOSUR, San Juan 670, RA-8000 Bahia Blanca, Buenos Aires, Argentina. EM mquattro@criba.edu.ar FU Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET); Secretaria General de Ciencia y Tecnologia (SeCyT), Universidad Nacional del Sur. L.F. Hinojosa; Millennium Institute of Ecology and Biodiversity (IEB); Mideplan [P05-002]; CONICYT [PFB 23]; FONDECYT, Chile [1120215] FX The authors thank the reviewers and the Editor for their helpful suggestions which improved the final version of the manuscript. This work was supported by grants from the Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET) and Secretaria General de Ciencia y Tecnologia (SeCyT), Universidad Nacional del Sur. L.F. Hinojosa thanks the Millennium Institute of Ecology and Biodiversity (IEB), and grants P05-002 from Mideplan and PFB 23 from CONICYT, FONDECYT 1120215, Chile. NR 65 TC 3 Z9 3 U1 0 U2 14 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0191-6122 EI 1558-9188 J9 PALYNOLOGY JI Palynology PD DEC 1 PY 2013 VL 37 IS 2 BP 246 EP 258 DI 10.1080/01916122.2013.787126 PG 13 WC Plant Sciences; Paleontology SC Plant Sciences; Paleontology GA 265JG UT WOS:000327946600007 ER PT J AU Zapico, SC Ubelaker, DH AF Zapico, Sara C. Ubelaker, Douglas H. TI Sex determination from dentin and pulp in a medicolegal context SO JOURNAL OF THE AMERICAN DENTAL ASSOCIATION LA English DT Article DE Basic sciences; disasters; forensic dentistry; genetics; molar; incisor; dental pulp; dentin; DNA; gene expression ID MITOCHONDRIAL-DNA EXTRACTION; HUMAN TEETH; SKELETAL REMAINS; IDENTIFICATION; QUANTIFICATION; AMPLIFICATION; POPULATION; RECOVERY; SAMPLES; TOOTH AB Background. The techniques used to determine the sex of skeletons are limited. The authors conducted a study to analyze the accuracy of sex identification from dentin and pulp via DNA isolation. Methods. The authors extracted DNA from the dentin and pulp of 14 teeth by using a silica-based methodology. They used the amelogenin gene to determine the sex via polymerase chain reaction. beta-actin, a housekeeping gene, was used as a control gene. The authors checked the results in agarose gel and semiquantified them by using gel analysis software. Results. The DNA yield depended on the type of tooth and was lowest in the smallest teeth (that is, incisors). In all cases, the authors were able to identify the sex, as well as the control gene, which suggests the potential to identify other genes, such as short tandem repeats. Conclusions. It is possible to correctly identify a person's sex from dentin and pulp; in instances in which one dental material is not available, the other material can be used with the same efficiency. Practical Implications. The results of this study are applicable to forensic dentistry, particularly in situations in which there is commingling of remains and fragmentary remains, and there may be only one tooth with which to identify a person's sex. C1 [Zapico, Sara C.; Ubelaker, Douglas H.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. RP Zapico, SC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, MRC112,10th & Constitut Ave NW,POB 37012, Washington, DC 20013 USA. EM saiczapico@gmail.com FU Peter Buck Postdoctoral Fellowship from the Smithsonian Institution, Washington FX Dr. C. Zapico is supported by a Peter Buck Postdoctoral Fellowship from the Smithsonian Institution, Washington. NR 27 TC 3 Z9 4 U1 0 U2 12 PU AMER DENTAL ASSOC PI CHICAGO PA 211 E CHICAGO AVE, CHICAGO, IL 60611 USA SN 0002-8177 EI 1943-4723 J9 J AM DENT ASSOC JI J. Am. Dent. Assoc. PD DEC PY 2013 VL 144 IS 12 BP 1379 EP 1385 PG 7 WC Dentistry, Oral Surgery & Medicine SC Dentistry, Oral Surgery & Medicine GA 262JV UT WOS:000327731900012 PM 24282268 ER PT J AU Wray, JJ Hansen, ST Dufek, J Swayze, GA Murchie, SL Seelos, FP Skok, JR Irwin, RP Ghiorso, MS AF Wray, James J. Hansen, Sarah T. Dufek, Josef Swayze, Gregg A. Murchie, Scott L. Seelos, Frank P. Skok, John R. Irwin, Rossman P., III Ghiorso, Mark S. TI Prolonged magmatic activity on Mars inferred from the detection of felsic rocks SO NATURE GEOSCIENCE LA English DT Article ID SURFACE; EVOLUTION; BASALT; CRUST AB Rocks dominated by the silicate minerals quartz and feldspar are abundant in Earth's upper continental crust(1). Yet felsic rocks have not been widely identified on Mars(2), a planet that seems to lack plate tectonics and the associated magmatic processes that can produce evolved siliceous melts on Earth(3). If Mars once had a feldspar-rich crust that crystallized from an early magma ocean such as that on the Moon, erosion, sedimentation and volcanism have erased any clear surface evidence for widespread felsic materials. Here we report near-infrared spectral evidence from the Compact Reconnaissance Imaging Spectrometer for Mars onboard the Mars Reconnaissance Orbiter for felsic rocks in three geographically disparate locations on Mars. Spectral characteristics resemble those of feldspar-rich lunar anorthosites(4,5), but are accompanied by secondary alteration products (clay minerals). Thermodynamic phase equilibrium calculations demonstrate that fractional crystallization of magma compositionally similar to volcanic flows near one of the detection sites can yield residual melts with compositions consistent with our observations. In addition to an origin by significant magma evolution, the presence of felsic materials could also be explained by feldspar enrichment by fluvial weathering processes. Our finding of felsic materials in several locations on Mars suggests that similar observations by the Curiosity rover in Gale crater(6) may be more widely applicable across the planet. C1 [Wray, James J.; Hansen, Sarah T.; Dufek, Josef] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Swayze, Gregg A.] US Geol Survey, Denver, CO 80225 USA. [Murchie, Scott L.; Seelos, Frank P.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Skok, John R.] Louisiana State Univ, Dept Geol & Geophys, Baton Rouge, LA 70803 USA. [Irwin, Rossman P., III] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Ghiorso, Mark S.] OFM Res, Seattle, WA 98115 USA. RP Wray, JJ (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. EM jwray@gatech.edu RI Wray, James/B-8457-2008; Murchie, Scott/E-8030-2015; Seelos, Frank/C-7875-2016 OI Wray, James/0000-0001-5559-2179; Murchie, Scott/0000-0002-1616-8751; Seelos, Frank/0000-0001-9721-941X FU NASA [NNX13AH80G] FX Portions of this work were supported by NASA Mars Data Analysis Program grant NNX13AH80G. We thank B. Horgan for a review and H. McSween, J. Mustard, B. Ehlmann, R. Clark and C. Viviano for discussions NR 30 TC 37 Z9 37 U1 5 U2 37 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD DEC PY 2013 VL 6 IS 12 BP 1013 EP 1017 DI 10.1038/NGEO1994 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 263HW UT WOS:000327799500012 ER PT J AU Jurcsik, J Smitola, P Hajdu, G Pilachowski, C Kolenberg, K Sodor, A Furesz, G Moor, A Kun, E Saha, A Prakash, P Blum, P Toth, I AF Jurcsik, J. Smitola, P. Hajdu, G. Pilachowski, C. Kolenberg, K. Sodor, A. Furesz, G. Moor, A. Kun, E. Saha, A. Prakash, P. Blum, P. Toth, I. TI WHAT IS THE DIFFERENCE? BLAZHKO AND NON-BLAZHKO RRab STARS AND THE SPECIAL CASE OF V123 IN M3 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE globular clusters: individual (M3); stars: individual (M3 V123); stars: oscillations (including pulsations); stars: variables: RR Lyrae; techniques: photometric; techniques: radial velocities ID LYRAE STARS; AC-ANDROMEDAE; ROTATION AB In an extended photometric campaign of RR Lyrae variables of the globular cluster M3, an aberrant-light-curve, non-Blazhko RRab star, V123, was detected. Based on its brightness, colors and radial-velocity curve, V123 is a bona fide member of M3. The light curve of V123 exhibits neither a bump preceding the light minimum, nor a hump on the rising branch, and has a longer than normal rise time, with a convex shape. A similar shape characterizes the mean light curves of some large-modulation-amplitude Blazhko stars, but none of the regular RRab variables with similar pulsation periods. This peculiar object thus mimics Blazhko variables without showing any evidence of periodic amplitude and/or phase modulation. We cannot find any fully convincing answer to the peculiar behavior of V123, however, the phenomenon raises again the possibility that rotation and aspect angle might play a role in the explanation of the Blazhko phenomenon, and that some source of inhomogeneity (magnetic field, chemical inhomogeneity) deforms the radial pulsation of Blazhko stars during the modulation. C1 [Jurcsik, J.; Smitola, P.; Sodor, A.; Moor, A.; Toth, I.] Konkoly Observ Budapest, H-1525 Budapest, Hungary. [Hajdu, G.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile. [Hajdu, G.] Milky Way Millennium Nucleus, Santiago 7820436, Chile. [Pilachowski, C.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Kolenberg, K.] Harvard Smithsonian Ctr Astrophys Astron, Cambridge, MA 02138 USA. [Kolenberg, K.; Furesz, G.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Sodor, A.] Royal Observ Belgium, B-1180 Brussels, Belgium. [Kun, E.] Univ Szeged, Dept Expt Phys, H-6720 Szeged, Hungary. [Kun, E.] Univ Szeged, Astron Observ, H-6720 Szeged, Hungary. [Saha, A.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Prakash, P.; Blum, P.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Jurcsik, J (reprint author), Konkoly Observ Budapest, POB 67, H-1525 Budapest, Hungary. EM jurcsik@konkoly.hu OI Hajdu, Gergely/0000-0003-0594-9138 FU Chilean Ministry for the Economy, Development, and Tourisms Programa Iniciativa Cientfica Milenio [P07-021-F]; Marie Curie Fellowship within the 7th European Community Framework Programme (FP7) [255267 SAS-RRL]; Belgian Federal Science Policy [M0/33/029] FX G.H. gratefully acknowledges support from the Chilean Ministry for the Economy, Development, and Tourisms Programa Iniciativa Cientfica Milenio through grant P07-021-F, awarded to the Milky Way Millennium Nucleus. WIYN observations were obtained through the WIYN Queue Program by Paul Smith and Daryl Willmarth, with assistance from G. Rosenstein and W. Hughes; their contributions are gratefully acknowledged. C. A. P. acknowledges the generosity of the Kirkwood Research Fund at Indiana University. K. K. is grateful for the support from a Marie Curie Fellowship (255267 SAS-RRL) within the 7th European Community Framework Programme (FP7). A.S. acknowledges support from the Belgian Federal Science Policy (project M0/33/029). NR 15 TC 1 Z9 1 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 1 PY 2013 VL 778 IS 2 AR UNSP L27 DI 10.1088/2041-8205/778/2/L27 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 258AA UT WOS:000327428400005 ER PT J AU Nynka, M Hailey, CJ Mori, K Baganoff, FK Bauer, FE Boggs, SE Craig, WW Christensen, FE Gotthelf, EV Harrison, FA Hong, J Perez, KM Stern, D Zhang, S Zhang, WW AF Nynka, Melania Hailey, Charles J. Mori, Kaya Baganoff, Frederick K. Bauer, Franz E. Boggs, Steven E. Craig, William W. Christensen, Finn E. Gotthelf, Eric V. Harrison, Fiona A. Hong, Jaesub Perez, Kerstin M. Stern, Daniel Zhang, Shuo Zhang, William W. TI HIGH-ENERGY X-RAYS FROM J174545.5-285829, THE CANNONBALL: A CANDIDATE PULSAR WIND NEBULA ASSOCIATED WITH Sgr A EAST SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: center; ISM: individual objects (Sagittarius A, Sagittarius A East); ISM: supernova remnants; stars: neutron; X-rays: individual (Cannonball) ID SAGITTARIUS-A-EAST; SUPERNOVA-REMNANT SAGITTARIUS; GALACTIC-CENTER; RADIATION; CHANDRA AB We report the unambiguous detection of non-thermal X-ray emission up to 30 keV from the Cannonball, a few-arcsecond long diffuse X-ray feature near the Galactic Center, using the NuSTAR X-ray observatory. The Cannonball is a high-velocity (v(proj) similar to 500 km s (1)) pulsar candidate with a cometary pulsar wind nebula (PWN) located similar to 2' north-east from Sgr A*, just outside the radio shell of the supernova remnant Sagittarius A (Sgr A) East. Its non-thermal X-ray spectrum, measured up to 30 keV, is well characterized by a Gamma similar to 1.6 power law, typical of a PWN, and has an X-ray luminosity of L(3-30 keV) = 1.3 x 10(34) erg s(-1). The spectral and spatial results derived from X-ray and radio data strongly suggest a runaway neutron star born in the Sgr A East supernova event. We do not find any pulsed signal from the Cannonball. The NuSTAR observations allow us to deduce the PWN magnetic field and show that it is consistent with the lower limit obtained from radio observations. C1 [Nynka, Melania; Hailey, Charles J.; Mori, Kaya; Gotthelf, Eric V.; Zhang, Shuo] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Baganoff, Frederick K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Hong, Jaesub] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Perez, Kerstin M.] Columbia Univ, New York, NY 10027 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Nynka, M (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. RI Boggs, Steven/E-4170-2015 OI Boggs, Steven/0000-0001-9567-4224 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration FX This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The authors wish to thank Jules Halpern for useful discussions. NR 25 TC 10 Z9 10 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 1 PY 2013 VL 778 IS 2 AR UNSP L31 DI 10.1088/2041-8205/778/2/L31 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 258AA UT WOS:000327428400009 ER PT J AU Paine, SN Turner, DD AF Paine, Scott N. Turner, David D. TI Processing and Calibration of Submillimeter Fourier Transform Radiometer Spectra From the RHUBC-II Campaign SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Fourier transform spectrometry; radiometric calibration; submillimeter radiometry ID NITROGEN AB The Radiative Heating in Underexplored Bands Campaign-II, conducted in 2009 from a high-altitude site in northern Chile, combined ground-based radiometry with radiosonde measurements of atmospheric state, for the purpose of testing atmospheric radiation models under conditions strongly influenced by water vapor in the middle to upper troposphere. A suite of broadband Fourier transform spectrometers (FTSs) measured the entire terrestrial thermal radiance spectrum from 1000- to 3.3-mu m wavelength. The submillimeter portion of the spectrum, from 1000 to 85 mu m (300-3500 GHz) was covered by a polarizing FTS referred to as the Smithsonian Astrophysical Observatory (SAO) FTS. Here, we describe data processing and radiometric calibration algorithms for this instrument. These include correction of interferograms for periodic sampled lag error, development of a temperature-dependent instrument calibration model, and principal component analysis of the complete set of spectra acquired during the campaign. C1 [Paine, Scott N.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Turner, David D.] NOAA, Natl Severe Storms Lab, Norman, OK 73072 USA. RP Paine, SN (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. EM spaine@cfa.harvard.edu; dave.turner@noaa.gov OI Paine, Scott/0000-0003-4622-5857 FU Climate and Environmental Sciences Division, Office of Biological and Environmental Research, Office of Science; Smithsonian Institution FX The Radiative Heating in Underexplored Bands Campaign-II (RHUBC-II) campaign was organized as part of the U. S. Department of Energy's Atmospheric Radiation Measurement program, which is sponsored by the Climate and Environmental Sciences Division, Office of Biological and Environmental Research, Office of Science. Additional support for the SAO FTS was provided by the Smithsonian Institution. The authors would like to thank the entire RHUBC-II team, particularly R. Cageao, A. Carrizo, J. Delamere, M. Diaz, G. Farnsworth, H. Li, E. Mlawer, K. Nitschke, L. Palchetti, D. Tobin, and M. Wojcik, for their efforts on deployment, continuous operation, and calibration of the SAO FTS for the duration of RHUBC-II; R. Blundell and J. Kawamura for their support of the SAO FTS redeployment; and R. Kimberk for useful discussions. Additional information on the RHUBC-II experiment can be found at http://acrf-campaign.arm.gov/rhubc. NR 17 TC 2 Z9 2 U1 0 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD DEC PY 2013 VL 51 IS 12 BP 5187 EP 5198 DI 10.1109/TGRS.2012.2231869 PG 12 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 259VE UT WOS:000327553600001 ER PT J AU Dickau, R Redwood, SD Cooke, RG AF Dickau, Ruth Redwood, Stewart D. Cooke, Richard G. TI A 4,000-year-old shaman's stone cache at Casita de Piedra, western Panama SO ARCHAEOLOGICAL AND ANTHROPOLOGICAL SCIENCES LA English DT Article DE Shamanism; Archaeology of ritual; Stone cache; Lithological description; Preceramic; Bribri; Cabecar; Panama ID CENTRAL-AMERICA; RELIGION; INDIANS; ORIGINS; HISTORY; BUFO AB During new excavations at the preceramic rockshelter of Casita de Piedra in western Panama, a cache of 12 unusual stones was recovered near the back wall, dating to between 4800 and 4000 cal bp. The stones include quartz, pyrite, a chalcedony vein nodule, a bladed quartz and jarosite aggregate and a human-modified dacite cylinder. Based on the unusual lithic types and the context of the cache, we suggest that these stones once belonged to a ritual specialist, such as a healer or shaman. Special stones are frequently mentioned as being an important component of a shaman's ritual paraphernalia in ethnographic records of various historic Native American groups throughout Central and South America, including the Bribri and Cab,car of southeastern Costa Rica and western Panama (formerly known as the 'Talamanca'). The cache of stones recovered at Casita de Piedra may represent the earliest material evidence in Central America of shamanistic practice. C1 [Dickau, Ruth] Univ Exeter, Dept Archaeol, Exeter EX4 4QE, Devon, England. [Redwood, Stewart D.] World Trade Ctr, Panama City, Panama. [Cooke, Richard G.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Dickau, R (reprint author), Univ Exeter, Dept Archaeol, Laver Bldg,North Pk Rd, Exeter EX4 4QE, Devon, England. EM rdickau@gmail.com FU Social Sciences and Humanities Research Council of Canada (SSHRC) FX Funding was provided by the Social Sciences and Humanities Research Council of Canada (SSHRC). The communities of Casita de Piedra and Quebrada Seca, Chiriqui, Panama, generously provided hospitality and help during excavation. Fieldwork and permits were facilitated by the Smithsonian Tropical Research Institute, Panama, and the Departmento del Patrimonio Historico of the Instituto Nacional de Cultura, Panama. Lab and logistical support was provided by the Department of Archaeology, University of Calgary. We owe a great debt of gratitude to Anthony J. Ranere for his insights, guidance, and excavation assistance. Thanks to Eduardo Bejerano and Drude Molbo for field assistance, Sonia Zarillo and Scott Raymond at the University of Calgary for helpful discussions, and Yvonne Kjorlien for comments on the manuscript. Initial observations and comments on the cache stones were made by members of the Geology Department at the University of Calgary. We thank two anonymous reviewers for their constructive comments. NR 107 TC 2 Z9 2 U1 0 U2 15 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1866-9557 EI 1866-9565 J9 ARCHAEOL ANTHROP SCI JI Archaeol. Anthropol. Sci. PD DEC PY 2013 VL 5 IS 4 SI SI BP 331 EP 349 DI 10.1007/s12520-012-0112-5 PG 19 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 250VM UT WOS:000326884400004 ER PT J AU Ley-Quinonez, CP Zavala-Norzagaray, AA Rendon-Maldonado, JG Espinosa-Carreon, TL Canizales-Roman, A Escobedo-Urias, DC Leal-Acosta, ML Hart, CE Aguirre, AA AF Ley-Quinonez, C. P. Zavala-Norzagaray, A. A. Rendon-Maldonado, J. G. Espinosa-Carreon, T. L. Canizales-Roman, A. Escobedo-Urias, D. C. Leal-Acosta, M. L. Hart, C. E. Aguirre, A. A. TI Selected Heavy Metals and Selenium in the Blood of Black Sea Turtle (Chelonia mydas agasiizzi) from Sonora, Mexico SO BULLETIN OF ENVIRONMENTAL CONTAMINATION AND TOXICOLOGY LA English DT Article DE Sea turtle; Chelonia mydas agasiizzi; Heavy metals; Cadmium; Sea Cortez; Mexico ID GULF-OF-CALIFORNIA; CARETTA-CARETTA; TRACE-ELEMENTS; MARINE TURTLES; GREEN TURTLES; MEDITERRANEAN SEA; ADRIATIC SEA; SUBCELLULAR-DISTRIBUTION; LEPIDOCHELYS-OLIVACEA; HEALTH PARAMETERS AB The concentration of heavy metals (Zn, Cd, Ni, Cu, Mn) and selenium (Se) was analyzed in blood collected from 12 black turtles (Chelonia mydas agasiizzi) captured in Canal del Infiernillo, Punta Chueca, Mexico. The most abundant metals were Zn (63.58 mu g g(-1)) and Se (7.66 mu g g(-1)), and Cd was the lower (0.99 mu g g(-1)). The sequential concentrations of trace metals were Zn > Se > Cu > Mn > Ni > Cd. In conclusion, this information is important as a baseline when using blood as tissue analysis of heavy metals; however, these levels could represent recent exposure in foraging grounds of black turtles in the Sea of Cortez. C1 [Ley-Quinonez, C. P.; Zavala-Norzagaray, A. A.; Rendon-Maldonado, J. G.; Canizales-Roman, A.] Univ Autonoma Sinaloa, Fac Ciencias Quim & Biol, Programa Doctorado Biotecnol, Culiacan, Sinaloa, Mexico. [Ley-Quinonez, C. P.] Serv Salud Sinaloa IV, Delegac Sanitaria 4, Dept Vectores & Zoonosis, Culiacan 80010, Sinaloa, Mexico. [Zavala-Norzagaray, A. A.; Espinosa-Carreon, T. L.; Escobedo-Urias, D. C.] Inst Politecn Nacl, CIIDIR SIN, Guasave, Sinaloa, Mexico. [Leal-Acosta, M. L.] Inst Politecn Nacl, CICIMAR, La Paz, Baja Calif Sur, Mexico. [Hart, C. E.] Univ Guadalajara, Ctr Univ Costa, Puerto Vallarta, Jalisco, Mexico. [Aguirre, A. A.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Aguirre, A. A.] Smithsonian Mason Sch Conservat, Front Royal, VA USA. RP Ley-Quinonez, CP (reprint author), Serv Salud Sinaloa IV, Delegac Sanitaria 4, Dept Vectores & Zoonosis, Escobedo 1026,Col Vegas, Culiacan 80010, Sinaloa, Mexico. EM cpley81@gmail.com FU CIIDIR-SIN IPN; GRUPO TORTUGUERO; EcoHealth Alliance; Instituto Politecnico Nacional [SIP-IPN 20090831] FX This work was supported by CIIDIR-SIN IPN, GRUPO TORTUGUERO and EcoHealth Alliance (formerly known as Wildlife Trust). The first author acknowledges the participation of the Seri community, Tiburon Island, Sonora, Mexico. This research was performed under Mexican regulation and laws under a permit provided by SEMARNAT (Secretaria de Medio Ambiente and Recursos Naturales) Permit number SGPA/DGVS/03481/09. Partial funding was provided by Project SIP-IPN 20090831 from Instituto Politecnico Nacional. NR 47 TC 4 Z9 4 U1 6 U2 37 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0007-4861 EI 1432-0800 J9 B ENVIRON CONTAM TOX JI Bull. Environ. Contam. Toxicol. PD DEC PY 2013 VL 91 IS 6 BP 645 EP 651 DI 10.1007/s00128-013-1114-4 PG 7 WC Environmental Sciences; Toxicology SC Environmental Sciences & Ecology; Toxicology GA 253XE UT WOS:000327122200007 PM 24072261 ER PT J AU Weldon, PJ AF Weldon, Paul J. TI Chemical aposematism SO CHEMOECOLOGY LA English DT Editorial Material DE Aposematism; Chemical defense ID PREY AB Discussions of aposematism traditionally have focused on the visual displays of prey that denote unpalatability or toxicity to predators. However, the construct of aposematism accommodates a spectrum of unprofitable traits signaled through various sensory modalities, including contact and distance chemoreception. Aposematism, involving learned aversions by signal receivers or selection for their unlearned avoidances, arises in predator-prey or other interspecific interactions where a mutually beneficial avoidance of signal emitters by signal receivers exists. Aposematism evolves by selection against signal receivers, e.g., predators, imposed by signal emitters, e.g., unprofitable prey, and vice versa, where both nondiscriminating signal receivers and unrecognized signal emitters are imperiled. Chemical aposematism entails concurrent reciprocal selection where signal emitters select for chemosensory avoidance responses in signal receivers, and where signal receivers select for the emission of identifiable (distinctive) chemicals in signal emitters. C1 Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Weldon, PJ (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM weldonp@si.edu NR 8 TC 7 Z9 7 U1 3 U2 37 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0937-7409 EI 1423-0445 J9 CHEMOECOLOGY JI Chemoecology PD DEC PY 2013 VL 23 IS 4 BP 201 EP 202 DI 10.1007/s00049-013-0140-3 PG 2 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA 250YW UT WOS:000326894100001 ER PT J AU Baeza, JA Fuentes, MS AF Antonio Baeza, Juan Fuentes, Maria Soledad TI Phylogeography of the shrimp Palaemon floridanus (Crustacea: Caridea: Palaemonidae): a partial test of meta-population genetic structure in the wider Caribbean SO MARINE ECOLOGY-AN EVOLUTIONARY PERSPECTIVE LA English DT Article DE Coalescence; demographic history; IMA2; Phylogeny; Prawn; skyline plot ID MITOCHONDRIAL-DNA VARIATION; CORAL-REEF FISH; MARINE POPULATIONS; PELAGIC LARVAE; NORTH-AMERICA; PACIFIC-OCEAN; DECAPODA; DIVERGENCE; ATLANTIC; SUBDIVISION AB Marine organisms with a pelagic stage are often assumed to display minor population structure given their extended larval development and subsequent high long-distance dispersal ability. Nonetheless, considerable population structure might still occur in species with high dispersal ability due to current oceanographic and/or historical processes. Specifically, for the wider Caribbean and Gulf of Mexico, theoretical and empirical considerations suggest that populations inhabiting each of the following areas should be genetically distinct: Panama, Belize, Southwest Florida (Tampa), and Southeast Florida (Fort Pierce). This study tests the hypothesis of significant genetic differentiation in Palaemon floridanus populations across the wider Caribbean and Gulf of Mexico. Population level comparisons were conducted using sequences of the mtDNA COI. In agreement with predictions, AMOVA and pairwise F-ST values demonstrated population differentiation among most pairs of the studied populations. Only Panama and East Florida populations were genetically similar. An isolation-with-migration population divergence model (implemented in IMA2) indicated that population divergence with incomplete lineage sorting can be invoked as the single mechanism explaining genetic dissimilarity between populations from the east and west coast of Florida. Historical demographic analyses indicated demographic expansion of P.floridanus in some localities [recent in Panama and ancient in East Florida and the wider Caribbean (entire dataset)] but constant population in other localities (in Belize and West Florida). This study rejects the idea of panmixia in marine species with high long-distance dispersal ability. Contemporary and historical processes might interact in a complex manner to determine current phylogeographic patterns. C1 [Antonio Baeza, Juan] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Antonio Baeza, Juan] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Antonio Baeza, Juan] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Coquimbo, Chile. [Fuentes, Maria Soledad] Algenol Biofuels, Ft Myers, FL USA. RP Baeza, JA (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM baezaa@si.edu OI Baeza, Juan Antonio/0000-0002-2573-6773 FU Marine Science Network Grant from the Smithsonian Institution through the Johnson and Hunterdon Oceanographic Research Endowment FX This study would have not been possible without the support of Valerie Paul and Raphael Ritson-Williams from the Smithsonian Marine Station at Fort Pierce (SMSFP, Florida), Anson (Tuc) Hines and Ilka (Candy) Feller from the Smithsonian Environmental Research Center (SERC, Maryland), Carla Piantonni and Klaus Ruetzler from the Caribbean Coral Reefs Ecosystem Program (CCRE, Washington, DC, USA) and John Christy from the Smithsonian Tropical Research Institute (STRI, Panama). Thanks to Jeff Hunt and Lee Weigt at the Laboratory of Analytical Biology, NMNH, Washington, DC for their invaluable logistical support. J.A.B. acknowledges an STRI Marine Postdoctoral Fellowship and an SMSFP Postdoctoral Fellowship. This research was partially funded by a Marine Science Network Grant from the Smithsonian Institution through the Johnson and Hunterdon Oceanographic Research Endowment (to J.A.B. and Candy Feller). This is contribution number 899 of the Smithsonian Marine Station at Fort Pierce. NR 75 TC 5 Z9 5 U1 1 U2 29 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0173-9565 EI 1439-0485 J9 MAR ECOL-EVOL PERSP JI Mar. Ecol.-Evol. Persp. PD DEC PY 2013 VL 34 IS 4 BP 381 EP 393 DI 10.1111/maec.12038 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 255PB UT WOS:000327251200001 ER PT J AU Lemoine, NP Drews, WA Burkepile, DE Parker, JD AF Lemoine, Nathan P. Drews, Willem A. Burkepile, Deron E. Parker, John D. TI Increased temperature alters feeding behavior of a generalist herbivore SO OIKOS LA English DT Article ID POPILLIA-JAPONICA NEWMAN; INSECT HERBIVORES; ELEVATED CO2; MULTIPLE ALLELOCHEMICALS; TROPHIC CASCADES; JAPANESE-BEETLE; METABOLIC-RATE; CARBON-CYCLE; PLANT; GROWTH AB Temperature can regulate a number of important biological processes and species interactions. For example, environmental temperature can alter insect herbivore consumption, growth and survivorship, suggesting that temperature-driven impacts on herbivory could influence plant community composition or nutrient cycling. However, few studies to date have examined whether rising temperature influences herbivore preference and performance among multiple plant species, which often dictates their impact at the community level. Here, we assessed the effects of temperature on the performance and preference of the generalist herbivore Popillia japonica among nine plant species. We show that, on average, consumption rates and herbivore performance increased at higher temperatures. However, there was considerable variation among plant species with consumption and performance increasing on some plant species at higher temperatures but decreasing on others. Plant nutritional quality appeared to influence these patterns as beetles increased feeding on high-nitrogen plants with increasing temperature, suggesting stronger nitrogen limitation. In addition to changes in feeding rates, feeding preferences of P. japonica shifted among temperatures, a pattern that was largely explained by differential deterrence of plant chemical extracts at different temperatures. In fact, temperature-induced changes in the efficacy of plant chemical extracts led P. japonica to reduce its diet breadth at higher temperatures. Our results indicate that rising temperatures will influence herbivore feeding behavior by altering the importance of plant nutritional and chemical traits, suggesting that climate change will alter the strength and sign of plant-insect interactions. C1 [Lemoine, Nathan P.; Burkepile, Deron E.] Florida Int Univ, Dept Biol, North Miami, FL 33181 USA. [Drews, Willem A.] Wabash Coll, Crawfordsville, IN 47933 USA. [Parker, John D.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Lemoine, NP (reprint author), Florida Int Univ, Dept Biol, MSB 350,3000 NE 151st St, North Miami, FL 33181 USA. EM nlemo001@fiu.edu RI Parker, John/F-9761-2010 OI Parker, John/0000-0002-3632-7625 FU FIU; Department of Biology at Wabash College; College of Arts and Sciences at FIU; Smithsonian Institution FX Author contributions: NPL and JDP conceived and designed the experiments. NPL and WAD performed the experiments. NPL, JDP and DEB analyzed the data and wrote the manuscript. We thank the staff of SERC, particularly J. Shue and P. Megonigal, for their support during this project, and S. Cook-Patton for feedback on earlier drafts. This manuscript was improved by comments from K. Mooney. This work was funded by a Presidential Fellowship from FIU (NPL), the Department of Biology at Wabash College (WAD), the College of Arts and Sciences at FIU (DEB), and the Smithsonian Institution (JDP). NR 67 TC 16 Z9 16 U1 11 U2 98 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 DEC PY 2013 VL 122 IS 12 BP 1669 EP 1678 DI 10.1111/j.1600-0706.2013.00457.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 254OX UT WOS:000327176100003 ER PT J AU Wright, EL Black, CR Turner, BL Sjogersten, S AF Wright, Emma L. Black, Colin R. Turner, Benjamin L. Sjoegersten, Sofie TI Environmental controls of temporal and spatial variability in CO2 and CH4 fluxes in a neotropical peatland SO GLOBAL CHANGE BIOLOGY LA English DT Review DE carbon dioxide; methane; nutrient gradient; Panama; peatland; tropical ID DISSOLVED ORGANIC-CARBON; AMAZON RAIN-FORESTS; METHANE EMISSIONS; SOIL RESPIRATION; TROPICAL PEATLAND; ROOT RESPIRATION; BIOGEOCHEMICAL PROCESSES; MICROBIAL CONTRIBUTIONS; NUTRIENT GRADIENT; ATMOSPHERIC CO2 AB Tropical peatlands play an important role in the global storage and cycling of carbon (C) but information on carbon dioxide (CO2) and methane (CH4) fluxes from these systems is sparse, particularly in the Neotropics. We quantified short and long-term temporal and small scale spatial variation in CO2 and CH4 fluxes from three contrasting vegetation communities in a domed ombrotrophic peatland in Panama. There was significant variation in CO2 fluxes among vegetation communities in the order Campnosperma panamensis>Raphia taedigera>Cyperus. There was no consistent variation among sites and no discernible seasonal pattern of CH4 flux despite the considerable range of values recorded (e.g. -1.0 to 12.6mgm(-2)h(-1) in 2007). CO2 fluxes varied seasonally in 2007, being greatest in drier periods (300-400mgm(-2)h(-1)) and lowest during the wet period (60-132mgm(-2)h(-1)) while very high emissions were found during the 2009 wet period, suggesting that peak CO2 fluxes may occur following both low and high rainfall. In contrast, only weak relationships between CH4 flux and rainfall (positive at the C. panamensis site) and solar radiation (negative at the C. panamensis and Cyperus sites) was found. CO2 fluxes showed a diurnal pattern across sites and at the Cyperus sp. site CO2 and CH4 fluxes were positively correlated. The amount of dissolved carbon and nutrients were strong predictors of small scale within-site variability in gas release but the effect was site-specific. We conclude that (i) temporal variability in CO2 was greater than variation among vegetation communities; (ii) rainfall may be a good predictor of CO2 emissions from tropical peatlands but temporal variation in CH4 does not follow seasonal rainfall patterns; and (iii) diurnal variation in CO2 fluxes across different vegetation communities can be described by a Fourier model. C1 [Wright, Emma L.; Black, Colin R.; Sjoegersten, Sofie] Univ Nottingham, Sch Biosci, Nottingham NG7 2RD, England. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Sjogersten, S (reprint author), Univ Nottingham, Sch Biosci, Nottingham NG7 2RD, England. EM Sofie.Sjogersten@nottingham.ac.uk RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU UK Biotechnology and Biological Sciences Research Council; University of Nottingham New Investigator Grant FX Emma Wright thanks the UK Biotechnology and Biological Sciences Research Council for her PhD scholarship and was also supported by a University of Nottingham New Investigator Grant. We thank Tania Romero for laboratory assistance, Alexander Cheesman and Eric Brown for field support and staff at the Smithsonian Tropical Research Institute station in Bocas del Toro for logistical support. We are also grateful for detailed and constructive comments from two reviewers which have improved the manuscript. NR 108 TC 9 Z9 11 U1 9 U2 105 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD DEC PY 2013 VL 19 IS 12 BP 3775 EP 3789 DI 10.1111/gcb.12330 PG 15 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 250FN UT WOS:000326836000019 PM 23873747 ER PT J AU Slik, JWF Paoli, G McGuire, K Amaral, I Barroso, J Bastian, M Blanc, L Bongers, F Boundja, P Clark, C Collins, M Dauby, G Ding, Y Doucet, JL Eler, E Ferreira, L Forshed, O Fredriksson, G Gillet, JF Harris, D Leal, M Laumonier, Y Malhi, Y Mansor, A Martin, E Miyamoto, K Araujo-Murakami, A Nagamasu, H Nilus, R Nurtjahya, E Oliveira, A Onrizal, O Parada-Gutierrez, A Permana, A Poorter, L Poulsen, J Ramirez-Angulo, H Reitsma, J Rovero, F Rozak, A Sheil, D Silva-Espejo, J Silveira, M Spironelo, W ter Steege, H Stevart, T Navarro-Aguilar, GE Sunderland, T Suzuki, E Tang, JW Theilade, I van der Heijden, G van Valkenburg, J Van Do, T Vilanova, E Vos, V Wich, S Woll, H Yoneda, T Zang, RG Zhang, MG Zweifel, N AF Slik, J. W. Ferry Paoli, Gary McGuire, Krista Amaral, Ieda Barroso, Jorcely Bastian, Meredith Blanc, Lilian Bongers, Frans Boundja, Patrick Clark, Connie Collins, Murray Dauby, Gilles Ding, Yi Doucet, Jean-Louis Eler, Eduardo Ferreira, Leandro Forshed, Olle Fredriksson, Gabriella Gillet, Jean-Francois Harris, David Leal, Miguel Laumonier, Yves Malhi, Yadvinder Mansor, Asyraf Martin, Emanuel Miyamoto, Kazuki Araujo-Murakami, Alejandro Nagamasu, Hidetoshi Nilus, Reuben Nurtjahya, Eddy Oliveira, Atila Onrizal, Onrizal Parada-Gutierrez, Alexander Permana, Andrea Poorter, Lourens Poulsen, John Ramirez-Angulo, Hirma Reitsma, Jan Rovero, Francesco Rozak, Andes Sheil, Douglas Silva-Espejo, Javier Silveira, Marcos Spironelo, Wilson ter Steege, Hans Stevart, Tariq Navarro-Aguilar, Gilberto Enrique Sunderland, Terry Suzuki, Eizi Tang, Jianwei Theilade, Ida van der Heijden, Geertje van Valkenburg, Johan Van Do, Tran Vilanova, Emilio Vos, Vincent Wich, Serge Woell, Hannsjoerg Yoneda, Tsuyoshi Zang, Runguo Zhang, Ming Gang Zweifel, Nicole TI Large trees drive forest aboveground biomass variation in moist lowland forests across the tropics SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE Climate; ectomycorrhizal associations; large tree density; pan-tropical analysis; soils; species traits; tree size; tropical forest biomass; wood density; wind dispersal ID RAIN-FOREST; WOOD DENSITY; SPECIES COMPOSITION; SPATIAL-PATTERNS; LANDSCAPE-SCALE; CARBON STOCKS; AMAZON; DIVERSITY; CLIMATE; MONODOMINANCE AB AimLarge trees (d.b.h.70cm) store large amounts of biomass. Several studies suggest that large trees may be vulnerable to changing climate, potentially leading to declining forest biomass storage. Here we determine the importance of large trees for tropical forest biomass storage and explore which intrinsic (species trait) and extrinsic (environment) variables are associated with the density of large trees and forest biomass at continental and pan-tropical scales. LocationPan-tropical. MethodsAboveground biomass (AGB) was calculated for 120 intact lowland moist forest locations. Linear regression was used to calculate variation in AGB explained by the density of large trees. Akaike information criterion weights (AICc-wi) were used to calculate averaged correlation coefficients for all possible multiple regression models between AGB/density of large trees and environmental and species trait variables correcting for spatial autocorrelation. ResultsDensity of large trees explained c. 70% of the variation in pan-tropical AGB and was also responsible for significantly lower AGB in Neotropical [287.8 (mean)105.0 (SD) Mg ha(-1)] versus Palaeotropical forests (Africa 418.3 +/- 91.8 Mg ha(-1); Asia 393.3 +/- 109.3 Mg ha(-1)). Pan-tropical variation in density of large trees and AGB was associated with soil coarseness (negative), soil fertility (positive), community wood density (positive) and dominance of wind dispersed species (positive), temperature in the coldest month (negative), temperature in the warmest month (negative) and rainfall in the wettest month (positive), but results were not always consistent among continents. Main conclusionsDensity of large trees and AGB were significantly associated with climatic variables, indicating that climate change will affect tropical forest biomass storage. Species trait composition will interact with these future biomass changes as they are also affected by a warmer climate. Given the importance of large trees for variation in AGB across the tropics, and their sensitivity to climate change, we emphasize the need for in-depth analyses of the community dynamics of large trees. C1 [Slik, J. W. Ferry; Oliveira, Atila] Chinese Acad Sci, Ctr Integrat Conservat, Xishuangbanna Trop Bot Garden, Menglun 666303, Yunnan, Peoples R China. [Paoli, Gary] Daemeter Consulting, Bogor, West Java, Indonesia. [McGuire, Krista] Columbia Univ Barnard Coll, Dept Biol, New York, NY 10027 USA. [Amaral, Ieda] INPA, TEAM Network, Manaus, Amazonas, Brazil. [Barroso, Jorcely] Univ Fed Acre, Ctr Multidisciplinar, Acre, Brazil. [Bastian, Meredith] Philadelphia Zoo, Philadelphia, PA USA. [Blanc, Lilian] EMBRAPA, CIRAD, Belem, Para, Brazil. [Bongers, Frans; Poorter, Lourens] Wageningen Univ, Ctr Ecosyst Studies, NL-6700 AP Wageningen, Netherlands. [Boundja, Patrick] TEAM Network, Nouabale Ndoki Natl Pk & periphery, Brazzaville, Congo. [Clark, Connie] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Collins, Murray] Inst Zool, Zool Soc London, London, England. [Collins, Murray] London Sch Econ & Polit Sci, Grantham Res Inst Climate Change & Environm, London, England. [Dauby, Gilles] Univ Libre Bruxelles, Brussels, Belgium. [Ding, Yi] Key Lab Forest Ecol & Environm, State Forestry Adm, Beijing, Peoples R China. [Ding, Yi] Chinese Acad Forestry, Inst Forest Ecol Environm & Protect, Beijing, Peoples R China. [Doucet, Jean-Louis; Poulsen, John] Univ Liege, Gembloux Agrobio Tech, Lab Trop & Subtrop forestry, Unit Forest & Nat Management, Gembloux, Belgium. [Ferreira, Leandro] Museu Paraense Emilio Goeldi, Belem, Para, Brazil. [Forshed, Olle] WWF, Solna, Sweden. [Fredriksson, Gabriella] Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, Amsterdam, Netherlands. [Gillet, Jean-Francois] Univ Liege, Gembloux Agrobio Tech, Lab Trop & Subtrop forestry Nat Plus, Unit Forest & Nat Management, Gembloux, Belgium. [Harris, David] Royal Bot Gardens, Edinburgh, Midlothian, Scotland. [Leal, Miguel] Wildlife Conservat Soc, Kabale, Uganda. [Laumonier, Yves; Sunderland, Terry] Ctr Int Forestry Res CIFOR, Bogor, West Java, Indonesia. [Malhi, Yadvinder] Univ Oxford, Sch Geog & Environm, Oxford, England. [Martin, Emanuel] Udzungwa Ecol Monitoring Ctr, Mangula, Tanzania. [Miyamoto, Kazuki] FFPRI, Shikoku Res Ctr, Kochi, Japan. [Araujo-Murakami, Alejandro; Parada-Gutierrez, Alexander] Univ Autonoma Gabriel Rene Moreno, Museo Hist Nat Noel Kempff Mercado, Santa Cruz, CA, Bolivia. [Nagamasu, Hidetoshi] Kyoto Univ, Kyoto Univ Museum, Kyoto, Japan. [Nilus, Reuben] Forest Res Ctr, Sabah Forestry Dept, Sandakan, Sabah, Malaysia. [Nurtjahya, Eddy] Univ Bangka Belitung, Bangka, Indonesia. [Onrizal, Onrizal] Univ Sumatera Utara, Fac Agr, Forestry Sci Dept, Medan, Indonesia. [Permana, Andrea] Univ Zurich, Anthropol Inst & Museum, Zurich, Switzerland. [Ramirez-Angulo, Hirma] Univ Los Andes, Merida, Venezuela. [Reitsma, Jan] Bur Waardenburg bv, Culemborg, Netherlands. [Rovero, Francesco] Trop Biodivers Sect, Museo Sci, Trento, Italy. [Rozak, Andes] Indonesian Inst Sci LIPI, Cibodas Bot Gardens, Cimacan, West Java, Indonesia. [Sheil, Douglas] So Cross Univ, Sch Environm Sci & Engn, Lismore, NSW 2480, Australia. [Sheil, Douglas] Inst Trop Forest Conservat, Kabale, Uganda. [Sheil, Douglas] Ctr Int Forestry Res, Bogor 16000, Indonesia. [Silva-Espejo, Javier] Univ San Abad Cusco, Cuzco, Peru. [Silveira, Marcos] Univ Fed Acre, Acre, Brazil. [ter Steege, Hans] Nat Biodivers Ctr, Leiden, Netherlands. [Stevart, Tariq] Africa & Madagascar Dept, Missouri Bot Garden, St Louis, MO USA. [Navarro-Aguilar, Gilberto Enrique] Univ Nacl Amazonia Peruana, Iquitos, Peru. [Suzuki, Eizi] Kagoshima Univ, Dept Earth & Environm Sci, Kagoshima 890, Japan. [Tang, Jianwei] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Menglun, Yunnan, Peoples R China. [Theilade, Ida] Univ Copenhagen, Fac Sci, Copenhagen, Denmark. [van der Heijden, Geertje] Univ Wisconsin, Milwaukee, WI 53201 USA. [van der Heijden, Geertje] Smithsonian Trop Res Inst, Panama City 03092, Panama. [van Valkenburg, Johan] Wageningen Univ, Plant Protect Serv, NL-6700 AP Wageningen, Netherlands. [Van Do, Tran] Kyoto Univ, Grad Sch Agr, Kyoto, Japan. [Vilanova, Emilio] Univ Los Andes, Inst Invest Desarrollo Forestal INDEFOR, Merida, Venezuela. [Vos, Vincent] Univ Autonoma Beni, Riberalta, Bolivia. [Wich, Serge] Liverpool John Moores Univ, Sch Nat Sci & Psychol, Res Ctr Evolutionary Anthropol & Palaeoecol, Liverpool L3 5UX, Merseyside, England. [Woell, Hannsjoerg] Conservat & Nat Resources Management, Bad Aussee, Austria. [Yoneda, Tsuyoshi] Kagoshima Univ, Fac Agr, Kagoshima 890, Japan. [Zang, Runguo] Chinese Acad Forestry, Inst Forest Ecol Environm & Protect, Key Lab Forest Ecol & Environm, State Forestry Adm, Beijing, Peoples R China. [Zhang, Ming Gang] Chinese Acad Sci, Inst Bot, Beijing, Peoples R China. [Zweifel, Nicole] Univ Zurich, Inst Evolutionary Biol & Biol Syst, Zurich, Switzerland. RP Slik, JWF (reprint author), Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Menglun 666303, Yunnan, Peoples R China. EM ferryslik@hotmail.com RI Theilade, Ida/A-6498-2010; ter Steege, Amaz/B-5866-2011; Silveira, Marcos/H-7906-2013; Sheil, Douglas/A-3867-2015; Rozak, Andes/E-8463-2015; M, Asyraf/A-6901-2011; OI Theilade, Ida/0000-0003-3502-1277; ter Steege, Amaz/0000-0002-8738-2659; Silveira, Marcos/0000-0003-0485-7872; Sheil, Douglas/0000-0002-1166-6591; Rozak, Andes/0000-0001-9641-5830; M, Asyraf/0000-0003-1255-7239; Harris, David/0000-0002-6801-2484; Vos, Vincent Antoine/0000-0002-0388-8530; Wich, Serge/0000-0003-3954-5174 FU Conservation International; Missouri Botanical Garden; Smithsonian Institution; Wildlife Conservation Society; Gordon and Betty Moore Foundation FX We thank all the participating institutional partners: 'Instituto Nacional de Pesquisas da Amazonia' (INPA), 'Silvicultural Treatment for the Regeneration of Logged-over Forest in East Kalimantan' (STREK), 'PlotNet Forest Database' (Lopez-Gonzalez et al., 2010), 'Tropical Ecology Assessment and Monitoring Network' (TEAM, 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), and 'The Forest Plots Network'. The following people are thanked for sharing their tree inventory data sets with us: Michel Baisie, John Terborgh, Ted Feldpausch, Anand Roopsind, Kyle Dexter, Meyner Nuscalawo, Luzmilla Arroyo, Lee White, Tim Baker, Gaby Lopez-Gonzalez, Raquel Thomas, Erasmo Alejo, Jerome Chave, Olaf Banki, Bonaventure Sonke, Fernando Cornejo, Rodolfo Vasquez, Campbell Webb, Euridice Honorio, Simon Lewis, Kade Sidiyasa, Roel Brienen, Ieda Amaral, Eric-Andre Nicolini, Oliver Phillips, Abel Monteagudo, James Singh, Vincent Bezard, Petrus Naisso, Miranda Nino, Timothy Paine, Casimiro Mendoza and Peter Ashton. We would also like to thank the large number of field assistants and botanists that helped measure, collect and identify all the plants. NR 50 TC 83 Z9 83 U1 8 U2 108 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 DEC PY 2013 VL 22 IS 12 BP 1261 EP 1271 DI 10.1111/geb.12092 PG 11 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 247UY UT WOS:000326649100003 ER PT J AU Kuntner, M Arnedo, MA Trontelj, P Lokovsek, T Agnarsson, I AF Kuntner, Matjaz Arnedo, Miquel A. Trontelj, Peter Lokovsek, Tjasa Agnarsson, Ingi TI A molecular phylogeny of nephilid spiders: Evolutionary history of a model lineage SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Sexual size dimorphism; Female gigantism; Coevolution; Biogeography; Sexual selection; Nephila ID ORB-WEB SPIDER; WESTERN MEDITERRANEAN BASIN; LOWER CRETACEOUS SPIDERS; GOLDEN SILK SPIDER; DNA-SEQUENCE DATA; WEAVING SPIDER; CLAVIPES ARANEAE; DRAGLINE SILK; SEXUAL CANNIBALISM; SPERM COMPETITION AB The pantropical orb web spider family Nephilidae is known for the most extreme sexual size dimorphism among terrestrial animals. Numerous studies have made Nephilidae, particularly Nephila, a mode] lineage in evolutionary research. However, a poorly understood phylogeny of this lineage, relying only on morphology, has prevented thorough evolutionary syntheses of nephilid biology. We here use three nuclear and five mitochondria] genes for 28 out of 40 nephilid species to provide a more robust nephilid phylogeny and infer clade ages in a fossil-calibrated Bayesian framework. We complement the molecular analyses with total evidence analysis including morphology. All analyses find strong support for nephilid monophyly and exclusivity and the monophyly of the genera Herennia and Clitaetra. The inferred phylogenetic structure within Nephilidae is novel and conflicts with morphological phylogeny and traditional taxonomy. Nephilengys species fall into two clades, one with Australasian species (true Nephilengys) as sister to Herennia, and another with Afrotropical species (Nephilingis Kuntner new genus) as sister to a clade containing Clitaetra plus most currently described Nephila. Surprisingly, Nephila is also diphyletic, with true Nephila containing N. pilipes + N. constricta, and the second clade with all other species sister to Clitaetra; this "Nephila" clade is further split into an Australasian clade that also contains the South American N. sexpunctata and the Eurasian N. clavata, and an African clade that also contains the Panamerican N. clavipes. An approximately unbiased test constraining the monophyly of Nephilengys, Nephila, and Nephilinae (Nephila, Nephilengys, Herennia), respectively, rejected Nephilengys monophyly, but not that of Nephila and Nephilinae. Further data are therefore necessary to robustly test these two new, but inconclusive findings, and also to further test the precise placement of Nephilidae within the Araneoidea. For divergence date estimation we set the minimum bound for the stems of Nephilidae at 40 Ma and of Nephila at 16 Ma to accommodate Palaeonephila from Baltic amber and Dominican Nephila species, respectively. We also calibrated and dated the phylogeny under three different interpretations of the enigmatic 165 Ma fossil Nephila jurassica, which we suspected based on morphology to be misplaced. We found that by treating N. jurassica as stem Nephila or nephilid the inferred clade ages were vastly older, and the mitochondrial substitution rates much slower than expected from other empirical spider data. This suggests that N. jurassica is not a Nephila nor a nephilid, but possibly a stem orbicularian. The estimated nephilid ancestral age (40-60 Ma) rejects a Gondwanan origin of the family as most of the southern continents were already split at that time. The origin of the family is equally likely to be African, Asian, or Australasian, with a global biogeographic history dominated by dispersal events. A reinterpretation of web architecture evolution suggests that a partially arboricolous, asymmetric orb web with a retreat, as exemplified by both groups of "Nephilengys", is plesiomorphic in Nephilidae, that this architecture was modified into specialized arboricolous webs in Herennia and independently in Clitaetra, and that the web became aerial, gigantic, and golden independently in both "Nephila" groups. The new topology questions previously hypothesized gradual evolution of female size from small to large, and rather suggests a more mosaic evolutionary pattern with independent female size increases from medium to giant in both "Nephila" clades, and two reversals back to medium and small; combined with male size evolution, this pattern will help detect gross evolutionary events leading to extreme sexual size dimorphism, and its morphological and behavioral correlates. (C) 2013 Elsevier Inc. All rights reserved. C1 [Kuntner, Matjaz; Lokovsek, Tjasa] Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Ljubljana 1000, Slovenia. [Kuntner, Matjaz; Agnarsson, Ingi] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Wuhan 430062, Hubei, Peoples R China. [Arnedo, Miquel A.] Univ Barcelona, Inst Recerca Biodiversitat, E-08007 Barcelona, Spain. [Arnedo, Miquel A.] Univ Barcelona, Dept Biol Anim, E-08007 Barcelona, Spain. [Trontelj, Peter] Univ Ljubljana, Biotech Fac, Dept Biol, Ljubljana 61000, Slovenia. [Agnarsson, Ingi] Univ Vermont, Dept Biol, Burlington, VT USA. RP Kuntner, M (reprint author), Slovenian Acad Sci & Arts, Ctr Sci Res, Novi Trg 2, Ljubljana 1000, Slovenia. EM kuntner@gmail.com OI Arnedo, Miquel/0000-0003-1402-4727 FU EU [MIRG-CT-2005 036536]; Slovenian Research Agency [Z1-7082-0618, BI-US/09-12-016, 1000-06-310141, Z1-9799-0618-07, ARRS-NRU/J1-2063-0618-2012/1]; National Science Foundation [DEB-1314749]; National Geographic Society [8655-09]; ICREA Academia Award for Excellence in Research from the Generalitat de Catalunya FX This research spanned over seven years and would not have been possible without numerous colleagues who helped with field work, loaned or donated specimens, or contributed to the study in other ways: G. Aljancic, M. Bedjanic, S. Benjamin, R. Bennet, A. Brescovit, R.-C. Cheng, J. Coddington, D. Court, V. Framenau, J. Frana, M. Gregoric, C. Haddad, A. Harmer, M. Harvey, S. Huber, R. Kostanjsek, S. Kralj-Fiser, I. Kuntner, D. Li, W. Maddison, J. Miller, T. Moreira, R. Neumann, T. Novak, S. Polak, R. Raven, M. Rix, J. Schneider, B. Sket, H. Smith, I.-M. Tso, J. Zhang, S. Zhang, and others. We thank S. Kralj-Fiser, M. Gregoric, R.-C. Cheng, Y. Ortiz-Ruiz, N. Vidergar, V. Zaksek and A. Moskric for kind help in- and outside the laboratory, Lauren Esposito for nomenclatural advice, Magdalena Naparus for producing a customized map, and C. Vink, M. Rix and an anonymous reviewer for their valuable suggestions. This research was supported by the EU 6th Framework Programme (a Marie Curie International Reintegration Grant MIRG-CT-2005 036536 to M. Kuntner), the Slovenian Research Agency (Grants Z1-7082-0618, BI-US/09-12-016 and 1000-06-310141 to M. Kuntner, Z1-9799-0618-07 to I. Agnarsson, and the program financing ARRS-NRU/J1-2063-0618-2012/1), and in part by the National Science Foundation (DEB-1314749 to I. Agnarsson), the National Geographic Society (Grant 8655-09 to I. Agnarsson and M. Kuntner), and by an ICREA Academia Award for Excellence in Research from the Generalitat de Catalunya to M. Arnedo. NR 160 TC 31 Z9 31 U1 4 U2 91 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 DEC PY 2013 VL 69 IS 3 BP 961 EP 979 DI 10.1016/j.ympev.2013.06.008 PG 19 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 244VF UT WOS:000326417600047 PM 23811436 ER PT J AU Coppard, SE Zigler, KS Lessios, HA AF Coppard, Simon E. Zigler, Kirk S. Lessios, H. A. TI Phylogeography of the sand dollar genus Mellita: Cryptic speciation along the coasts of the Americas SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Mellita; Leodia; Phylogeny; Divergence; Speciation ID SEA-URCHIN GENUS; POPULATION-STRUCTURE; REEF DEVELOPMENT; LATE NEOGENE; PANAMA; ECHINOIDEA; ATLANTIC; PACIFIC; ISTHMUS; CLYPEASTEROIDA AB Sand dollars of the genus Mellita are members of the sandy shallow-water fauna. The genus ranges in tropical and subtropical regions on the two coasts of the Americas. To reconstruct the phylogeography of the genus we sequenced parts of the mitochondrial cytochrome oxidase I and of 16S rRNA as well as part of the nuclear 28S rRNA gene from a total of 185 specimens of all ten described morphospecies from 31 localities. Our analyses revealed the presence of eleven species, including six cryptic species. Sequences of five morphospecies do not constitute monophyletic molecular units and thus probably represent ecophenotypic variants. The fossil-calibrated phylogeny showed that the ancestor of Mellita diverged into a Pacific lineage and an Atlantic + Pacific lineage close to the Miocene/Pliocene boundary. Atlantic M. tenuis, M. quinquiesperforata and two undescribed species of Mellita have non-overlapping distributions. Pacific Mellita consist of two highly divergent lineages that became established at different times, resulting in sympatric M. longifissa and M. notabilis. Judged by modern day ranges, not all divergence in this genus conforms to an allopatric speciation model. Only the separation of M. quinquiesperforata from M. notabilis is clearly due to vicariance as the result of the completion of the Isthmus of Panama. The molecular phylogeny calibrated on fossil evidence estimated this event as having occurred similar to 3 Ma, thus providing evidence that, contrary to a recent proposal, the central American Isthmus was not completed until this date. (C) 2013 Elsevier Inc. All rights reserved. C1 [Coppard, Simon E.; Zigler, Kirk S.; Lessios, H. A.] Smithsonian Trop Res Inst, Balboa, Panama. [Zigler, Kirk S.] Sewanee Univ South, Dept Biol, Sewanee, TN 37383 USA. RP Coppard, SE (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Panama. EM coppardse@gmail.com FU SENACYT (La Secretaria Nacional de Educacion Superior Ciencia Tecnologia e Innovacion) (Panama) [COL08-002]; Smithsonian Institution; Friday Harbor Laboratories; National Science Foundation [0202773]; Sigma Xi FX We thank A. Calderon, L. Calderon, L.B. Geyer, D. Gonzalez, S. Lockhart and A.H. Magallon for their assistance in the laboratory. We are grateful to R. Collin, S.W.C. Coppard, T. Duda, A. Hiller, J. Lawrence, S. Lockhart, D. McClay, A. O'Dea, D. Pope, R.W. Portell, L. Rocha, R. Riosmena-Rodriguez, F. Rodriguez, T.I. Sancho-Mejias, A.N. Suarez Castillo, and A. Sweeney for help with collecting samples. We thank R. Mooi for helpful discussion and A. O'Dea for his comments on the manuscript. This work was supported by a fellowship to SEC from SENACYT (La Secretaria Nacional de Educacion Superior Ciencia Tecnologia e Innovacion) (Panama) as part of project COL08-002, and fellowships to KSZ from the Smithsonian Institution, Friday Harbor Laboratories, the National Science Foundation (#0202773), and a Grant-in-Aid of Research from Sigma Xi. NR 74 TC 6 Z9 6 U1 3 U2 48 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 DEC PY 2013 VL 69 IS 3 BP 1033 EP 1042 DI 10.1016/j.ympev.2013.05.028 PG 10 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 244VF UT WOS:000326417600052 PM 23792155 ER PT J AU Fan, DM Chen, JH Meng, Y Wen, J Huang, JL Yang, YP AF Fan, Deng-Mei Chen, Jia-Hui Meng, Ying Wen, Jun Huang, Jin-Ling Yang, Yong-Ping TI Molecular phylogeny of Koenigia L. (Polygonaceae: Persicarieae): Implications for classification, character evolution and biogeography SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Koenigia; Classification; Character evolution; Biogeographic diversification; The Himalayan region ID CHLOROPLAST DNA; POLYGONEAE POLYGONACEAE; SYSTEMATIC SIGNIFICANCE; TRIBES PERSICARIEAE; NONCODING REGIONS; UNIVERSAL PRIMERS; TIBETAN PLATEAU; MORPHOLOGY; PLANTS; AMPLIFICATION AB To examine the phylogenetic relationships of Koenigia sensu lato (Polygonaceae), 43 samples representing all species of Koenigia and closely related taxa (e.g., Aconogonon, Bistorta, and Persicaria) were sequenced for nuclear ITS and four plastid regions (tmL-F, atpB-rbcL, rbcL, and rpl32-trnL((UAG))). Phylogenetic analyses indicate that Koenigia recognized by Hedberg is paraphyletic and that the basal species K. delicatula should be reassigned to a separate new genus. Based on these findings, we further propose that the genus Koenigia sensu lato be circumscribed to include five species. Ancestral state reconstruction showed that the pollen apertures likely evolved in parallel in the Aconogonon-Koenigia-Bistorta clade and Persicaria clade and that tricolpate pollen is most likely to be the ancestral state. Quincuncial aestivation likely evolved during the early evolution of Koenigia and its close relatives. Our findings suggest that the uplift of the Himalayas has played an important role in promoting species diversification of Koenigia. Koenigia islandica expanded its range during Pleistocene glacial cycles by tracking changes in newly available habitats. (C) 2013 Elsevier Inc. All rights reserved. C1 [Fan, Deng-Mei] Jiangxi Agr Univ, Lab Subtrop Biodivers, Nanchang 330045, Peoples R China. [Chen, Jia-Hui; Meng, Ying; Yang, Yong-Ping] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. [Chen, Jia-Hui; Meng, Ying; Yang, Yong-Ping] Chinese Acad Sci, Kunming Inst Bot, Inst Tibetan Plateau Res Kunming, Kunming 650204, Yunnan, Peoples R China. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Wen, Jun] Chinese Acad Sci, Inst Bot, Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. [Huang, Jin-Ling] E Carolina Univ, Dept Biol, Greenville, NC 27858 USA. RP Yang, YP (reprint author), 132 Lanhei Rd, Kunming 650204, Yunnan, Peoples R China. EM dmf.625@163.com FU Natural Science Foundation of China [40930209, 30370118]; Ministry of Science and Technology of China [2010CB951700]; Chinese Academy of Sciences [KSCX2-YW-Z-1019, 242009311211014]; John D. and Catherine T. MacArthur Foundation FX This study was supported by grants from the Natural Science Foundation of China (40930209 to H. Sun; 30370118 to Y.P. Yang), from the Ministry of Science and Technology of China (2010CB951700), from the Chinese Academy of Sciences (KSCX2-YW-Z-1019; 242009311211014), and the John D. and Catherine T. MacArthur Foundation (to J. Wen). We are grateful to Drs. Jianwen Zhang and Jipei Yue for assistance with the molecular techniques and data analysis. We also wish to thank Zelong Nie for helpful comments on earlier drafts of this manuscript. NR 63 TC 9 Z9 9 U1 0 U2 39 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 DEC PY 2013 VL 69 IS 3 BP 1093 EP 1100 DI 10.1016/j.ympev.2013.08.018 PG 8 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 244VF UT WOS:000326417600057 PM 23994356 ER PT J AU Ren, ZM Zhong, Y Kurosu, U Aoki, S Ma, EB von Dohlen, CD Wen, J AF Ren, Zhumei Zhong, Yang Kurosu, Utako Aoki, Shigeyuki Ma, Enbo von Dohlen, Carol D. Wen, Jun TI Historical biogeography of Eastern Asian-Eastern North American disjunct Melaphidina aphids (Hemiptera: Aphididae: Eriosomatinae) on Rhus hosts (Anacardiaceae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Gall aphids; Fordini; Holarctic biogeography; Intercontinental disjunctions; Melaphidina; Sumac ID ANCIENT RAPID RADIATIONS; NUCLEAR GENE EF-1-ALPHA; ATLANTIC LAND-BRIDGE; PHYLOGENETIC ANALYSIS; MOLECULAR PHYLOGENY; DNA-SEQUENCES; MITOCHONDRIAL-DNA; MIXED MODELS; EVOLUTION; HEMISPHERE AB Intercontinental biotic disjunctions have been documented and analyzed in numerous Holarctic taxa. Patterns previously synthesized for animals compared to plants suggest that the timing of animal disjunctions are mostly Early Tertiary and were generated by migration and vicariance events occurring in the North Atlantic, while plant disjunctions are mostly Mid-Late Tertiary and imply migration and vicariance over Beringia. Melaphidina aphids (Hemiptera: Aphididae: Fordini) exhibit host-alternating life cycles comprising an obligate seasonal shift between Rims subgenus Rhus species (Anacardiaceae) and mosses (Bryophyta). Similar to their Rhus hosts, melaphidines are distributed disjunctly between Eastern Asia and Eastern North America. We examined evolutionary relationships within Melaphidina to determine the position of the North American lineage, date its divergence from Asian relatives, and compare these results to a previous historical biogeographic study of Rhus. We sampled nine species and three subspecies representing all six genera of Melaphidina. Data included sequences of mitochondrial cytochrome c oxidase subunits I and II + leucine tRNA, cytochrome b, and nuclear elongation factor la genes. Phylogenetic analyses (Bayesian, maximum-likelihood, parsimony) of the combined data (3282 bp) supported the monophyly of all genera except Nurudea and Schlechtendalia, due to the position of N. ibofushi. While the exact position of the North American Melaphis was not well resolved, there was high support for a derived position within Asian taxa. The divergence of Melaphis from Asian relatives centered on the Eocene-Oligocene boundary (similar to 33-35 Ma), which coincides with closure of Beringian Land Bridge I. This also corresponded to the Asian-North American disjunction previously estimated for subgenus Rhus spp. We suggest the late-Eocene Bering Land Bridge as the most likely migration route for Melaphis ancestors, as was also hypothesized for North American Rhus ancestors. Results for the Melaphidina disjunction depart from the modal pattern in animal lineages, and present a case where insect and host-plant taxa apparently responded similarly to Tertiary climate change. (C) 2013 Elsevier Inc. All rights reserved. C1 [Ren, Zhumei; Ma, Enbo] Shanxi Univ, Sch Life Sci, Taiyuan 030006, Shanxi, Peoples R China. [Zhong, Yang] Fudan Univ, Sch Life Sci, Shanghai 200433, Peoples R China. [Kurosu, Utako] Rissho Univ, Fac Econ, Tokyo 1418602, Japan. [Aoki, Shigeyuki] Chuo Univ, Fac Econ, Hachioji, Tokyo 1920393, Japan. [von Dohlen, Carol D.] Utah State Univ, Dept Biol, Logan, UT 84322 USA. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot MRC 166, Washington, DC 20013 USA. RP von Dohlen, CD (reprint author), Utah State Univ, Dept Biol, 5305 Old Main Hill, Logan, UT 84322 USA. EM zmren@sxu.edu.cn; yangzhong@fudan.edu.cn; ukurosu@tamacc.chuo-u.ac.jp; oregma@rb3.so-net.ne.jp; maenbo2003@sxu.edu.cn; carol.vondohlen@usu.edu; WENJ@si.edu FU National Natural Science Foundation of China [30925004, 31040010, 31170359]; Natural Science Foundation Shanxi Province [2012011034-4]; Shanxi Scholarship Council of China; Shanghai Leading Academic Discipline Project [B111]; John D. and Catherine T. MacArthur Foundation; Laboratory of Analytical Biology of the National Museum of Natural History; Smithsonian Institution; National Science Foundation (USA) [DEB9807076, DEB0316508]; Utah Agricultural Experiment Station FX We thank Carol Rowe for laboratory work. This project was supported by the National Natural Science Foundation of China (30925004, 31040010 and 31170359), the Natural Science Foundation Shanxi Province (2012011034-4), the Research Project Supported by Shanxi Scholarship Council of China, Shanghai Leading Academic Discipline Project (B111), the John D. and Catherine T. MacArthur Foundation (to J.W.), the Laboratory of Analytical Biology of the National Museum of Natural History, the Smithsonian Institution, the National Science Foundation (USA, to C.D.v.D.; DEB9807076, DEB0316508) and the Utah Agricultural Experiment Station (to C.D.v.D.); approved as journal paper #8530. NR 111 TC 5 Z9 7 U1 2 U2 59 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 DEC PY 2013 VL 69 IS 3 BP 1146 EP 1158 DI 10.1016/j.ympev.2013.08.003 PG 13 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 244VF UT WOS:000326417600061 PM 23973894 ER PT J AU Bland, KJ Hendy, AJW Kamp, PJJ Nelson, CS AF Bland, Kyle J. Hendy, Austin J. W. Kamp, Peter J. J. Nelson, Campbell S. TI Macrofossil biofacies in the late Neogene of central Hawke's Bay: applications to palaeogeography SO NEW ZEALAND JOURNAL OF GEOLOGY AND GEOPHYSICS LA English DT Article DE Hawke's Bay; biofacies; palaeoenvironments; Tolaga Group; Mangaheia Group; palaeogeography; fossils ID SEA-LEVEL FLUCTUATIONS; WATER SHELF CARBONATES; NEW-ZEALAND; NORTH-ISLAND; SEQUENCE STRATIGRAPHY; LATE MIOCENE; PLIOCENE; PALEOECOLOGY; WANGANUI; LITHIFICATION AB The Late Miocene-Early Pleistocene (Tongaporutuan-Nukumaruan) sedimentary succession in the forearc basin in central and western Hawke's Bay, encompassed by the Tolaga and Mangaheia Groups, comprises a wide variety of variably fossiliferous lithofacies, ranging from non-marine greywacke-derived conglomerates to bathyal mudstone and flysch beds. Thirty molluscan biofacies, inferred to have accumulated in estuarine to outer shelf palaeoenvironments, have been identified and represent both in situ and transported assemblages. Although distributed through the late Neogene succession, most biofacies occur within the Late Pliocene-Early Pleistocene part of the Mangaheia Group. Using the spatial distribution of the different biofacies, we have constructed detailed palaeoenvironmental reconstructions for the Plio-Pleistocene of central Hawke's Bay. The stratigraphic occurrence of particular biofacies has been primarily controlled by relative sea-level positions and variations in sediment input during high-frequency glacio-eustatic sea-level oscillations. The distribution of biofacies reflects proximity to contemporaneous shorelines, localised sources of carbonate sediment or dominance of siliciclastic sedimentation, and records the interplay between tectonic and eustatic drivers of relative sea-level change. C1 [Bland, Kyle J.; Kamp, Peter J. J.; Nelson, Campbell S.] Univ Waikato, Dept Earth & Ocean Sci, Hamilton, New Zealand. [Hendy, Austin J. W.] Smithsonian Trop Res Inst, Ctr Trop Paleontol & Archaeol, Balboa, Panama. RP Bland, KJ (reprint author), GNS Sci, Lower Hutt, New Zealand. EM k.bland@gns.cri.nz OI Kamp, Peter/0000-0002-2563-884X FU Tertiary Education Commission TAD Scholarship; GNS Science QMAP; New Zealand Government; GNS Science FX KJB acknowledges financial assistance from a Tertiary Education Commission TAD Scholarship and GNS Science QMAP field support funding. We acknowledge Public Good Science Funding provided by the New Zealand Government to the University of Waikato and GNS Science. Alan Beu is thanked for palaeontological assistance. We gratefully acknowledge John Simes (GNS Science) for uploading much of the fossil dataset into FRED. Vincent Caron, Arne Pallentin, Dave Francis and Greg Browne are thanked for helpful discussions about East Coast stratigraphy. Rhys Graafhuis, Rachel Baggs and Sarah Dyer (University of Waikato) are acknowledged for their inputs into geological mapping and lithostratigraphy of central Hawke's Bay. Betty-Ann Kamp assisted with preparation of some figures. Reviews from Angela Griffin, Alan Beu, James Crampton and Kari Bassett significantly improved earlier versions of this paper. NR 51 TC 0 Z9 0 U1 0 U2 4 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0028-8306 EI 1175-8791 J9 NEW ZEAL J GEOL GEOP JI N. Z. J. Geol. Geophys. PD DEC 1 PY 2013 VL 56 IS 4 BP 200 EP 222 DI 10.1080/00288306.2013.815232 PG 23 WC Geology; Geosciences, Multidisciplinary SC Geology GA 250QK UT WOS:000326867800003 ER PT J AU Tian, H Tomczyk, S McIntosh, SW Bethge, C de Toma, G Gibson, S AF Tian, H. Tomczyk, S. McIntosh, S. W. Bethge, C. de Toma, G. Gibson, S. TI Observations of Coronal Mass Ejections with the Coronal Multichannel Polarimeter SO SOLAR PHYSICS LA English DT Article DE Active regions; Coronal mass ejections; Flares; Magnetic fields; Waves ID EUV IMAGING SPECTROMETER; SOLAR CORONA; LOOP OSCILLATIONS; MAGNETIC-FIELD; WAVES; HINODE; DIAGNOSTICS; CAVITIES; STEREO; ALFVEN AB The Coronal Multichannel Polarimeter (CoMP) measures not only the polarization of coronal emission, but also the full radiance profiles of coronal emission lines. For the first time, CoMP observations provide high-cadence image sequences of the coronal line intensity, Doppler shift, and line width simultaneously over a large field of view. By studying the Doppler shift and line width we may explore more of the physical processes of the initiation and propagation of coronal mass ejections (CMEs). Here we identify a list of CMEs observed by CoMP and present the first results of these observations. Our preliminary analysis shows that CMEs are usually associated with greatly increased Doppler shift and enhanced line width. These new observations provide not only valuable information to constrain CME models and probe various processes during the initial propagation of CMEs in the low corona, but also offer a possible cost-effective and low-risk means of space-weather monitoring. C1 [Tian, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tomczyk, S.; McIntosh, S. W.; Bethge, C.; de Toma, G.; Gibson, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO USA. RP Tomczyk, S (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, Pob 3000, Boulder, CO 80307 USA. EM hui.tian@cfa.harvard.edu; tomczyk@ucar.edu FU ASP Postdoctoral Fellowship Program; The National Center for Atmospheric Research is sponsored by the National Science Foundation; [8100002705] FX SDO is the first mission of NASA's Living With a Star (LWS) Program. SDO data a courtesy of NASA/SDO and the AIA science team. H. Tian's work at CfA is supported under contract 8100002705 from Lockheed-Martin to SAO. Part of this work was done at NCAR, where H. Tian was supported under the ASP Postdoctoral Fellowship Program. The National Center for Atmospheric Research is sponsored by the National Science Foundation. We thank L. Sitongia for processing the CoMP level-0 data. We also thank P. Judge, B.C. Low, and H. Peter for helpful discussions. NR 57 TC 7 Z9 7 U1 0 U2 5 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 DEC PY 2013 VL 288 IS 2 BP 637 EP 650 DI 10.1007/s11207-013-0317-5 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 249XK UT WOS:000326813900011 ER PT J AU Gingerich, O AF Gingerich, Owen TI Our Imperiled World SO AMERICAN SCHOLAR LA English DT Article C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 0 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 WIN PY 2013 VL 82 IS 1 BP 44 EP 50 PG 7 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA AS3ZJ UT WOS:000344213200019 ER PT J AU Dove, CJ Dahlan, NF Drovetski, SV AF Dove, Carla J. Dahlan, Nor Faridah Drovetski, Sergei V. TI MtDNA ND2 sequence identifies Streaked Horned Lark (Eremophila alpestris strigata) from birdstrike to US Air Force F-15 at Portland International Airport, Oregon SO CONSERVATION GENETICS RESOURCES LA English DT Article DE Portland International Airport; Birdstrike; F-15; DNA; Streaked Horned Lark ID DNA BARCODES AB The Streaked Horned Lark (SHL: Eremophila alpestris strigata) is the Northwest subspecies of the Horned Lark listed as endangered in Washington State, critical in Oregon, and is now being considered for listing as threatened by the US Fish & Wildlife Service. Some of the important breeding areas of SHL are associated with airports in western Washington and Oregon which raises concern over possible collisions between SHLs and aircraft. Here, we report a successful use of mtDNA ND2 gene sequence for identification of SHL feather and tissue remains from a bird collision with a US Air Force F-15-C on 4 October 2012 at Portland International Airport. Due to the conservation status of SHL, documentation of this event and a simple mtDNA-based molecular identification protocol may have management and conservation implications at airfields within the range of this rare subspecies. C1 [Dove, Carla J.; Dahlan, Nor Faridah] Smithsonian Inst, Div Birds, Feather Identificat Lab, Washington, DC 20560 USA. [Drovetski, Sergei V.] Tromso Univ Museum, N-9037 Tromso, Norway. RP Dove, CJ (reprint author), Smithsonian Inst, Div Birds, Feather Identificat Lab, NHB E-600,MRC 116, Washington, DC 20560 USA. EM dovec@si.edu RI Drovetski, Sergei/A-6002-2011 OI Drovetski, Sergei/0000-0002-1832-5597 FU USAF; US Navy; Federal Aviation Administration FX We thank Nick Atwell for the donation of a salvaged SHL specimen (USNM 602465) from PDX for this study and J. F. Whatton for specimen preparation. Randy Moore (Oregon State University) confirmed the status of SHL at PDX. Kevin Kerr provided comments on the manuscript. The Feather Lab is funded through interagency support from USAF, US Navy and the Federal Aviation Administration. Dan Sullivan and Tiffany Robertson provided information regarding this USAF birdstrike. We thank MSgt John Peterson (USAF) and Nick Atwell (PDX) for reporting this birdstrike. NR 10 TC 1 Z9 1 U1 1 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1877-7252 EI 1877-7260 J9 CONSERV GENET RESOUR JI Conserv. Genet. Resour. PD DEC PY 2013 VL 5 IS 4 BP 997 EP 999 DI 10.1007/s12686-013-9952-2 PG 3 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 244KS UT WOS:000326387800025 ER PT J AU Gardner-Vandy, KG Lauretta, DS McCoy, TJ AF Gardner-Vandy, Kathryn G. Lauretta, Dante S. McCoy, Timothy J. TI A petrologic, thermodynamic and experimental study of brachinites: Partial melt residues of an R chondrite-like precursor SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID UREILITE PARENT BODY; COMPOSITIONAL CLASSIFICATION; CARBONACEOUS CHONDRITES; OXYGEN ISOTOPES; ORIGIN; METEORITES; ACHONDRITE; OLIVINE; BEARING; CONSTRAINTS AB The primitive achondrites provide a window into the initial melting of asteroids in the early solar system. The brachinites are olivine-dominated meteorites with a recrystallized texture that we and others interpret as evidence of partial melting and melt removal on the brachinite parent body. We present a petrologic, thermodynamic and experimental study of the brachinites to evaluate the conditions under which they formed and test our hypothesis that the precursor material to the brachinites was FeO-rich compared to the precursors of other primitive achondrites. Petrologic analysis of six brachinites (Brachina, Allan Hills (ALH) 84025, Hughes 026, Elephant Moraine (EET) 99402, Northwest Africa (NWA) 3151, and NWA 4969) and one brachinite-like achondrite (NWA 5400) shows that they are meteorites with recrystallized texture that are enriched in olivine (>= 80 vol.%) and depleted in other minerals with respect to a chondritic mineralogy. Silicates in the brachinites are FeO-rich (Fa(32-36)). Brachinite-like achondrite Northwest Africa 5400 is similar in mineralogy and texture to the brachinites but with a slightly lower FeO-content (Fa(30)). Thermodynamic calculations yield equilibration temperatures above the Fe,Ni-FeS cotectic temperature (similar to 950 degrees C) for all meteorites studied here and temperatures above the silicate eutectic (similar to 1050 degrees C) for all but two. Brachina formed at an fO(2) of similar to IW, and the other brachinites and NWA 5400 formed at similar to IW - 1. All the meteorites show great evidence of formation by partial melting having approximately chondritic to depleted chondritic mineralogies, equilibrated mineral compositions, and recrystallized textures, and having reached temperatures above that required for melt generation. In an attempt to simulate the formation of the brachinite meteorites, we performed one-atmosphere, gas-mixing partial melting experiments of R4 chondrite LaPaz Ice Field 03639. Experiments at 1250 degrees C and an oxygen fugacity of IW - 1 produce residual phases that are within the mineralogy and mineral compositions of the brachinites. These experiments provide further evidence for the formation of brachinites as a result of partial melting of a chondritic precursor similar in mineralogy and mineral compositions to the R chondrites. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Gardner-Vandy, Kathryn G.; Lauretta, Dante S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Gardner-Vandy, Kathryn G.; McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20013 USA. RP Gardner-Vandy, KG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, POB 37012,MRC 119, Washington, DC 20013 USA. EM Gardner-VandyK@si.edu FU NASA [NNX10AH50G]; NASA Earth and Space Science Fellowship [NNX09AQ88H]; UA/Alfred P. Sloan Foundation Fellowship; UA/Alfred P. Sloan Foundation FX This work was supported by NASA Cosmochemistry grant NNX10AH50G to D. S. Lauretta, NASA Earth and Space Science Fellowship NNX09AQ88H to D. S. Lauretta and K. G. Gardner-Vandy, and the UA/Alfred P. Sloan Foundation Fellowship to K. G. Gardner-Vandy. We are very appreciative to: Ken Domanik for his help with EMPA, Dolores Hill for her help with sample preparations, John Jones and Nancy Chabot for helpful conversations about our experimental technique, and the late Michael Drake for imparting his experimental wisdom on Kat. We are also grateful for reviewers Klaus Keil and Cyrena Goodrich and associate editor Anders Meibom for helpful comments which improved this manuscript. This work is dedicated to Kat's grandmother-in-law Edna J. Howell (1928-2013) who is wholeheartedly missed. NR 74 TC 11 Z9 11 U1 0 U2 11 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 DEC 1 PY 2013 VL 122 BP 36 EP 57 DI 10.1016/j.gca.2013.07.035 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 242UY UT WOS:000326269800003 ER PT J AU Brandao, SN Yasuhara, M Irizuki, T Horne, DJ AF Brandao, Simone N. Yasuhara, Moriaki Irizuki, Toshiaki Horne, David J. TI The ostracod genus Trachyleberis (Crustacea; Ostracoda) and its type species SO MARINE BIODIVERSITY LA English DT Article DE Biogeography; Type species designation; Marine; Ostracoda; Trachyleberididae; Taxonomic revision ID LAST 100 YEARS; CENTRAL JAPAN; SOUTHWEST JAPAN; TEMPORAL-CHANGES; MIYAZAKI GROUP; HIROSHIMA BAY; SEA; ASSEMBLAGES; PLIOCENE; COAST AB The Trachyleberididae is one of the most diverse families of the Ostracoda in Mesozoic to present-day marine environments. Its type genus is Trachyleberis Brady, 1898, first described on the basis of specimens collected alive. Unfortunately the identity and morphological characteristics of the type species of Trachyleberis have long been the subject of confusion resulting from misidentifications and misunderstandings in the literature. We review the taxonomic history of this problem, providing extensive synonymies, new diagnoses, descriptions and illustrations of relevant species. We establish the identity of the type species of Trachyleberis, Cythere scabrocuneata Brady, 1880, by reference to a previously-designated lectotype from the Seto Inland Sea, Japan, noting that a second distinct species, Trachyleberis niitsumai Ishizaki, 1971, is represented in the original syntypic series. We consider that in the interests of nomenclatural and taxonomic stability C. scabrocuneata should be retained as the type species of Trachyleberis, despite the fact that the original description of the genus was based on a species misidentified as C. scabrocuneata and which was subsequently described as a new species, Trachyleberis lytteltonensis Harding and Sylvester-Bradley, 1953. The geographical and stratigraphical distributions of Trachyleberis are reconsidered in the light of our revision. Trachyleberis now comprises 18 known species inhabiting shallow marine environments of the Northwestern Pacific from Japan to the northern coast of the South China Sea off Hong Kong. The revised stratigraphic occurrence of Trachyleberis is from the Eocene to Recent. As many as 400 living and fossil species have been previously assigned to Trachyleberis and they range from the Cretaceous to the Recent; Cretaceous species formerly attributed to Trachyleberis are now re-assigned to other genera. We suggest that Trachyleberis most likely evolved from a Cythereis-like ancestor during the Eocene-Oligocene of Japan, the same area that is the centre of its modern distribution. C1 [Brandao, Simone N.] Univ Hamburg, Biozentrum Grindel, D-20146 Hamburg, Germany. [Brandao, Simone N.] Univ Hamburg, Zool Museum, D-20146 Hamburg, Germany. [Brandao, Simone N.] Senckenberg Meer, DZMB, D-26382 Wilhelmshaven, Germany. [Yasuhara, Moriaki] Univ Hong Kong, Sch Biol Sci, Hong Kong, Hong Kong, Peoples R China. [Yasuhara, Moriaki] Univ Hong Kong, Swire Inst Marine Sci, Hong Kong, Hong Kong, Peoples R China. [Yasuhara, Moriaki] Univ Hong Kong, Dept Earth Sci, Hong Kong, Hong Kong, Peoples R China. [Yasuhara, Moriaki] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Irizuki, Toshiaki] Shimane Univ, Interdisciplinary Grad Sch Sci & Engn, Dept Geosci, Matsue, Shimane 6908504, Japan. [Horne, David J.] Queen Mary Univ London, Sch Geog, London E1 4NS, England. [Horne, David J.] Nat Hist Museum, Dept Zool, London SW7 5BD, England. RP Brandao, SN (reprint author), Univ Fed Rio Grande do Norte, Dept Geol, Lab Geol & Geofis Marinha & Monitoramento Ambient, Campus Univ,Caixa Postal 1596, BR-59072970 Natal, RN, Brazil. EM brandao.sn.100@gmail.com RI Brandao, Simone/K-4672-2012; OI Horne, David J./0000-0002-2148-437X FU Alexander von Humboldt Foundation; Encyclopedia of Life and Hansische Universitats-Stiftung; SYNTHESYS Project; European Community; Programme for Basic Research of the University of Hong Kong [201111159140]; Smithsonian Postdoctoral Fellowship; Smithsonian Marine Science Network Postdoctoral Fellowship FX Miranda Lowe (NHM, London) carefully assisted the first author during five visits to the NHM and also kindly provided access to and permission for studying the Challenger and other ostracod specimens housed in the NHM. Dan Gordon (Discovery Museum) kindly facilitated the re-examination of the Brady collection material by DJH. Mark J. Grygier (Lake Biwa Museum) and Philippe Bouchet (MNHM) helped with correct interpretations of articles of the ICZN. Jorgen Olesen and Tom Schiotte (Natural History Museum of Denmark) loaned the specimens of Trachyleberis lytteltonensis. Alan Lord loaned the specimens from the Senckenberg Research Institute and Natural History Museum Frankfurt. Gene Hunt and Carlita Sanford assisted depositing specimens in the Smithsonian collection. Stephen Eager (Victoria University of Wellington), Katsura Yamada (Shinshu University), John Neil (La Trobe University), Robin J. Smith (Lake Biwa Museum), Hayato Tanaka (Shizuoka University), Mark Warne (Deakin University) kindly provided valuable information and/or papers on Trachyleberis. The suggestions of the editor Pedro Martinez Arbizu and four anonymous referees greatly improved the present publication. The first author thanks Dietmar Keyser (ZMH, Universitat Hamburg), Angelika Brandt (ZMH, Universitat Hamburg) and Pedro Martinez Arbizu (DZMB, Senckenberg Institute) for their mentorship. M.Y. thanks Gene Hunt (Smithsonian Institution) for discussion in the initial stage of this project, and Scott Whittaker (Smithsonian Institution) for help in SEM imaging. S. N. B. is/was financially supported by Alexander von Humboldt Foundation, Encyclopedia of Life and Hansische Universitats-Stiftung. Additionally, "this research received support from the SYNTHESYS Project http://www.synthesys.info/ which is financed by the European Community Research Infrastructure Action under the FP7 Integrating Activities Programme." M.Y. is supported by Seed Funding from the Programme for Basic Research of the University of Hong Kong (project code 201111159140), and was supported by Smithsonian Postdoctoral Fellowship and Smithsonian Marine Science Network Postdoctoral Fellowship. NR 149 TC 4 Z9 4 U1 2 U2 5 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1867-1616 EI 1867-1624 J9 MAR BIODIVERS JI Mar. Biodivers. PD DEC PY 2013 VL 43 IS 4 BP 363 EP 405 DI 10.1007/s12526-013-0163-6 PG 43 WC Biodiversity Conservation; Marine & Freshwater Biology SC Biodiversity & Conservation; Marine & Freshwater Biology GA 236SV UT WOS:000325820500013 ER PT J AU Gebruk, AV Rogacheva, AV Pawson, DL Hamel, JF Macisaac, KG Mercier, A AF Gebruk, Andrey V. Rogacheva, Antonina V. Pawson, David L. Hamel, Jean-Francois Macisaac, Kevin G. Mercier, Annie TI Penilidia desbarresi sp nov (Echinodermata: Holothuroidea: Elasipodida) from the upper slope of Newfoundland and re-description of P. ludwigi (von Marenzeller, 1893) SO MARINE BIOLOGY RESEARCH LA English DT Article DE Penilpidia; elpidiid holothurians; deep sea; upper slope; submarine canyons; reproduction; Canada; Newfoundland ID NORTHEAST ATLANTIC; SUBMARINE-CANYON; HOLOTHURIANS; BIOLOGY AB Penilpidia desbarresi sp. nov. was collected in the Desbarres Canyon at a depth of 525 m, off the southeastern coast of insular Newfoundland, eastern Canada. The new species differs from the type species Penilpidia ludwigi (von Marenzeller, 1983) in having larger middle spines on arched rod-type ossicles on the dorsum and by having the lobe around the posterior body end formed by six pairs of very small tube feet. Penilpidia desbarresi sp. nov was photographed in situ and sampled on a single occasion in July 2007. This gonochoric species (similar to 1-2 cm long) was found on a muddy substrate and individuals were aggregated, reaching a density of similar to 50 ind. m(-2). Preliminary evidence points to brooding, which would be a first for the family Elpidiidae. Penilpidia ludwigi, not recorded for more than 100 years after its first description, is re-described. C1 [Gebruk, Andrey V.; Rogacheva, Antonina V.] Russian Acad Sci, PP Shirshov Inst Oceanol, Moscow 117997, Russia. [Pawson, David L.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Hamel, Jean-Francois] SEVE, Portugal Cove St Philips, NF, Canada. [Macisaac, Kevin G.] Fisheries & Oceans Canada, Bedford Inst Oceanog, Dept Fisheries & Oceans, Dartmouth, NS B2Y 4A2, Canada. [Mercier, Annie] Mem Univ Newfoundland, Ctr Ocean Sci, St John, NF, Canada. RP Gebruk, AV (reprint author), Russian Acad Sci, PP Shirshov Inst Oceanol, Nakhimovsky Pr 36, Moscow 117997, Russia. EM agebruk@ocean.ru RI Mercier, Annie/B-4254-2012 FU International Fisheries and Oceans Governance Fund; DFO High Priority Funds; Natural Sciences and Engineering Research Council of Canada (NSERC) FX We would like to thank the captain and crew of the CCGS Hudson and the staff of the Department of Fisheries & Oceans Canada (DFO), as well as the ROPOS team for their help during the collection. The authors are grateful to Christian Borowski and Horst Weikert for specimens of Penilpidia ludwigi sampled in the Mediterranean on the Meteor 25/2 cruise. Helmut Sattmann kindly provided information on the specimens of P. ludwigi stored at the Naturhistorisches Museum, Wien. We thank Dieter Fiege for his kind help at various stages of our work. Many thanks also to Cam Lirette for the map and Doris Pawson for assistance in many ways. The research was partly funded by the International Fisheries and Oceans Governance Fund, DFO High Priority Funds and the Natural Sciences and Engineering Research Council of Canada (NSERC). NR 27 TC 2 Z9 3 U1 0 U2 29 PU TAYLOR & FRANCIS AS PI OSLO PA KARL JOHANS GATE 5, NO-0154 OSLO, NORWAY SN 1745-1000 J9 MAR BIOL RES JI Mar. Biol. Res. PD DEC 1 PY 2013 VL 9 IS 10 BP 1029 EP 1036 DI 10.1080/17451000.2013.793810 PG 8 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 174UD UT WOS:000321180000007 ER PT J AU Dohrmann, M Vargas, S Janussen, D Collins, AG Worheide, G AF Dohrmann, Martin Vargas, Sergio Janussen, Dorte Collins, Allen G. Woerheide, Gert TI Molecular paleobiology of early-branching animals: integrating DNA and fossils elucidates the evolutionary history of hexactinellid sponges SO PALEOBIOLOGY LA English DT Article ID SPICULE ASSEMBLAGE; PORIFERA; PHYLOGENY; CHINA; GLASS; MODELS; CLOCK; FAUNA; MOUNTAINS; AUSTRALIA AB Reconciliation of paleontological and molecular phylogenetic evidence holds great promise for a better understanding of the temporal succession of cladogenesis and character evolution, especially for taxa with a fragmentary fossil record and uncertain classification. In zoology, studies of this kind have largely been restricted to Bilateria. Hexactinellids (glass sponges) readily lend themselves to test such an approach for early-branching (non-bilaterian) animals: they have a long and rich fossil record, but for certain taxa paleontological evidence is still scarce or ambiguous. Furthermore, there is a lack of consensus for taxonomic interpretations, and discrepancies exist between neontological and paleontological classification systems. Using conservative fossil calibration constraints and the largest molecular phylogenetic data set assembled for this group, we infer divergence times of crown-group Hexactinellida in a Bayesian relaxed molecular clock framework. With some notable exceptions, our results are largely congruent with interpretations of the hexactinellid fossil record, but also indicate long periods of undocumented evolution for several groups. This study illustrates the potential of an integrated molecular/paleobiological approach to reconstructing the evolution of challenging groups of organisms. C1 [Dohrmann, Martin; Vargas, Sergio; Woerheide, Gert] Univ Munich, Dept Geo & Umweltwissensch, D-80333 Munich, Germany. [Woerheide, Gert] Univ Munich, GeoBioCtrLMU, D-80333 Munich, Germany. [Woerheide, Gert] Bayer Staatsammlung Palaontol & Geol, D-80333 Munich, Germany. [Janussen, Dorte] Forsch Inst Senckenberg, Sekt Marine Evertebraten 1, D-60325 Frankfurt, Germany. [Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Natl Systemat Lab, NMFS, Washington, DC 20013 USA. RP Worheide, G (reprint author), Univ Munich, Dept Geo & Umweltwissensch, Richard Wagner Str 10, D-80333 Munich, Germany. EM woerheide@lmu.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 Deutsche Forschungsgemeinschaft (DFG) [JA 1063/13-1-3, JA 1063/14-1-2, WO 896/9-1-2]; Smithsonian Institution; National Science Foundation [DEB-0829986] FX We thank the Deutsche Forschungsgemeinschaft (DFG) for funding our research projects on the phylogeny of Hexactinellida (JA 1063/13-1-3, JA 1063/14-1-2, WO 896/9-1-2). MD acknowledges the Smithsonian Institution for additional support through a Postdoctoral Fellowship. AGC acknowledges support from the National Science Foundation (DEB-0829986). We thank Kevin Peterson, an anonymous reviewer, and Associate Editor Martin Aberhan for their feedback on the manuscript. NR 77 TC 7 Z9 7 U1 3 U2 257 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0094-8373 EI 1938-5331 J9 PALEOBIOLOGY JI Paleobiology PD WIN PY 2013 VL 39 IS 1 BP 95 EP 108 DI 10.1666/0094-8373-39.1.95 PG 14 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 068XG UT WOS:000313398900006 ER PT J AU De Prins, J Davis, DR De Coninck, E Sohn, JC Triberti, P AF De Prins, Jurate Davis, Donald R. De Coninck, Eliane Sohn, Jae-Cheon Triberti, Paolo TI Systematics, phylogeny and biology of a new genus of Lithocolletinae (Lepidoptera: Gracillariidae) associated with Cistaceae SO ZOOTAXA LA English DT Article DE evolution; host specificity; leaf mining; morphology; taxonomy ID LEAF-MINING MOTHS; CISTUS CISTACEAE; BUTTERFLIES; MORPHOLOGY; SEQUENCE; FOSSIL; PLANTS; WORLD; L. AB The gracillariid genus Triberta gen. nov. (Lepidoptera: Gracillariidae: Lithocolletinae Stainton, 1854) is described to accommodate two species formerly assigned to the genus Phyllonorycter Hubner, 1822: Triberta helianthemella (Herrich-Schaffer, 1861) comb. nov. and T. cistifoliella (Groschke, 1944) comb. nov. Triberta cistifoliella bona sp. is restored from synonymy based on morphological characters. The new genus is biologically associated with the plant family Cistaceae of the order Malvales and is endemic to the Palaearctics. Our molecular analysis of eleven nuclear genes failed to unambiguously place Triberta in the lithocolletine phylogeny, but revealed that this genus is distinct from either clade Phyllonorycter + Cremastobombycia and Cameraria. The distinctiveness of Triberta is also supported by inferred traits in wing venation, micro morphology of the last instar larva, pupa, genital morphology of the adult and life history. A key to the species of Triberta is provided. The interspecific homogeneity in external morphology, coupled with minor differences in genital traits, an apparent narrow specialization on Cistaceae host plants, restricted geographical range and molecular evidence based on multi-nuclear genes jointly suggest that the generic diversification of Triberta is a relatively old phenomenon and driven strongly by host selection. C1 [De Prins, Jurate; De Coninck, Eliane] Royal Museum Cent Africa, Tervuren, Belgium. [Davis, Donald R.; Sohn, Jae-Cheon] Smithsonian Inst, Nat Museum Nat Hist, Washington, DC 20560 USA. [Triberti, Paolo] Museo Storia Nat, Verona, Italy. RP De Prins, J (reprint author), Royal Museum Cent Africa, Tervuren, Belgium. EM jurate.de.prins@africamuseum.be FU Belgian Science Policy Office FX Wolfram Mey (Museum fur Naturkunde der Humboldt-Universitat, Berlin) is kindly acknowledged for allowing us to study the historic Triberta specimens from the Staudinger collection and for information on additional Triberta specimens present in the collection under his care. We thank very much Andreas Zwick (Staatliches Museum fur Naturkunde Stuttgart) for his kind assistance in searching for the types of Lithocolletis cistifoliella and for very valuable information on the biography of Franz Groschke (1914-1956). Matthias Nuss (Staatliches Museum fur Tierkunde) in Dresden is sincerely thanked for the most valuable information on the deposition of specimens from the collection of the Forstliche Hochschule in Tharandt. Bernard Landry (Museum d'histoire naturelle, Geneve) was kind to donate the male specimen of Triberta which served to record SEM photographs of the last abdominal segments. We cordially thank David Wagner (University of Connecticut) for his helpful suggestions on the delimitation of the new genus Triberta. We also thank both reviewers for their highly pertinent comments and suggestions. Financial support was obtained from the Belgian Science Policy Office to the first author. NR 145 TC 5 Z9 6 U1 0 U2 5 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD NOV 27 PY 2013 VL 3741 IS 2 BP 201 EP 227 PG 27 WC Zoology SC Zoology GA 267XO UT WOS:000328131900001 PM 25112984 ER PT J AU Rath, SP Schmidt, R AF Rath, Steffen Patrick Schmidt, Richard TI Field-theoretical study of the Bose polaron SO PHYSICAL REVIEW A LA English DT Article ID FERMI-GAS; EINSTEIN CONDENSATE; FESHBACH RESONANCES; ULTRACOLD GASES; SUPERFLUID; IMPURITIES; TRANSITION; SCATTERING; MOLECULES; CESIUM AB We study the properties of the Bose polaron, an impurity strongly interacting with a Bose-Einstein condensate, using a field-theoretic approach and make predictions for the spectral function and various quasiparticle properties that can be tested in experiment. We find that most of the spectral weight is contained in a coherent attractive and a metastable repulsive polaron branch. We show that the qualitative behavior of the Bose polaron is well described by a non-self-consistent T-matrix approximation by comparing analytical results to numerical data obtained from a fully self-consistent T-matrix approach. The latter takes into account an infinite number of bosons excited from the condensate. C1 [Rath, Steffen Patrick; Schmidt, Richard] Tech Univ Munich, D-85748 Garching, Germany. [Schmidt, Richard] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Schmidt, Richard] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Rath, SP (reprint author), Tech Univ Munich, James Franck Str, D-85748 Garching, Germany. FU DFG [Forschergruppe 801] FX We thank Wilhelm Zwerger for suggesting the problem and for careful reading of this manuscript. We also acknowledge helpful discussions with Marcus Barth, Eugene Demler, Tilman Enss, Francesco Piazza, and Alessio Recati. This work has been supported by the DFG Forschergruppe 801. NR 91 TC 36 Z9 36 U1 1 U2 8 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 NOV 26 PY 2013 VL 88 IS 5 AR 053632 DI 10.1103/PhysRevA.88.053632 PG 16 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 257KS UT WOS:000327383400006 ER PT J AU Zhang, WT Shih, CK Labandeira, CC Sohn, JC Davis, DR Santiago-Blay, JA Flint, O Ren, D AF Zhang, Weiting Shih, Chungkun Labandeira, Conrad C. Sohn, Jae-Cheon Davis, Donald R. Santiago-Blay, Jorge A. Flint, Oliver Ren, Dong TI New Fossil Lepidoptera (Insecta: Amphiesmenoptera) from the Middle Jurassic Jiulongshan Formation of Northeastern China SO PLOS ONE LA English DT Article ID TRICHOPTERA; PHYLOGENY; DIVERSITY; EVOLUTION AB Background: The early history of the Lepidoptera is poorly known, a feature attributable to an inadequate preservational potential and an exceptionally low occurrence of moth fossils in relevant mid-Mesozoic deposits. In this study, we examine a particularly rich assemblage of morphologically basal moths that contribute significantly toward the understanding of early lepidopteran biodiversity. Methodology/Principal Findings: Our documentation of early fossil moths involved light-and scanning electron microscopic examination of specimens, supported by various illumination and specimen contrast techniques. A total of 20 moths were collected from the late Middle Jurassic Jiulongshan Formation in Northeastern China. Our principal results were the recognition and description of seven new genera and seven new species assigned to the Eolepidopterigidae; one new genus with four new species assigned to the Mesokristenseniidae; three new genera with three new species assigned to the Ascololepidopterigidae fam. nov.; and one specimen unassigned to family. Lepidopteran assignment of these taxa is supported by apomorphies of extant lineages, including the M-1 vein, after separation from the M-2 vein, subtending an angle greater than 60 degrees that is sharply angulate at the junction with the r-m crossvein (variable in Trichoptera); presence of a foretibial epiphysis; the forewing M vein often bearing three branches; and the presence of piliform scales along wing veins. Conclusions/Significance: The diversity of these late Middle Jurassic lepidopterans supports a conclusion that the Lepidoptera-Trichoptera divergence occurred by the Early Jurassic. C1 [Zhang, Weiting; Shih, Chungkun; Labandeira, Conrad C.; Ren, Dong] Capital Normal Univ, Coll Life Sci, Beijing, Peoples R China. [Labandeira, Conrad C.; Sohn, Jae-Cheon; Santiago-Blay, Jorge A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Labandeira, Conrad C.; Sohn, Jae-Cheon] Univ Maryland, Dept Entomol, College Pk, MD USA. [Labandeira, Conrad C.; Sohn, Jae-Cheon] Univ Maryland, BEES Program, College Pk, MD USA. [Sohn, Jae-Cheon; Davis, Donald R.; Flint, Oliver] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Santiago-Blay, Jorge A.] Univ Puerto Rico Mayaguez, Dept Crop & Agroenvironm Sci, Mayaguez, PR USA. [Zhang, Weiting] Shijiazhuang Univ Econ, Geosci Museum, Shijiazhuang, Peoples R China. RP Ren, D (reprint author), Capital Normal Univ, Coll Life Sci, Beijing, Peoples R China. EM rendong@mail.cnu.edu.cn FU National Basic Research Program of China (973 Program) [2012CB821906]; National Natural Science Foundation of China [31172143, 31230065, 31272352, 41272006]; Beijing Municipal Commission of Education [KZ201310028033]; China Geological Survey [1212011120115]; United States National Science Foundation [0531769]; Maryland Agricultural Experiment Station FX This research was supported by the National Basic Research Program of China (973 Program) (grant 2012CB821906), National Natural Science Foundation of China (grants 31172143, 31230065, 31272352 and 41272006), Project of Great Wall Scholar and KEY project of Beijing Municipal Commission of Education (grants KZ201310028033), and the China Geological Survey (grant 1212011120115). Support for JCS was provided by the United States National Science Foundation's Assembling the Tree of Life program, award 0531769, and the Maryland Agricultural Experiment Station. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 63 TC 16 Z9 16 U1 1 U2 13 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD NOV 22 PY 2013 VL 8 IS 11 AR e79500 DI 10.1371/journal.pone.0079500 PG 33 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 259QP UT WOS:000327541700009 PM 24278142 ER PT J AU Hu, AZ Lee, TE Clark, CW AF Hu, Anzi Lee, Tony E. Clark, Charles W. TI Spatial correlations of one-dimensional driven-dissipative systems of Rydberg atoms SO PHYSICAL REVIEW A LA English DT Article ID QUANTUM; ENTANGLEMENT; STATES; OPTICS AB We consider a one-dimensional lattice of atoms with laser excitation to a Rydberg state and spontaneous emission. The atoms are coupled due to the dipole-dipole interaction of the Rydberg states. This driven-dissipative system has a broad range of nonequilibrium phases, such as antiferromagnetic ordering and bistability. Using the quantum trajectory method, we calculate the spatial correlation function throughout the parameter space for up to 18 lattice sites. We show that bistability significantly strengthens the spatial correlations and the entanglement. C1 [Hu, Anzi; Clark, Charles W.] Univ Maryland, Joint Quantum Inst, Gaithersburg, MD USA. [Hu, Anzi; Clark, Charles W.] NIST, Gaithersburg, MD 20899 USA. [Lee, Tony E.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Hu, AZ (reprint author), Univ Maryland, Joint Quantum Inst, Gaithersburg, MD USA. RI Clark, Charles/A-8594-2009 OI Clark, Charles/0000-0001-8724-9885 FU NSF FX We thank Sarang Gopalakrishnan for useful discussions. This work was supported in part by NSF through a grant to ITAMP. NR 43 TC 30 Z9 30 U1 2 U2 14 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 NOV 22 PY 2013 VL 88 IS 5 AR 053627 DI 10.1103/PhysRevA.88.053627 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 255KN UT WOS:000327237900005 ER PT J AU Lewis, C Bentlage, B Yanagihara, A Gillan, W Van Blerk, J Keil, DP Bely, AE Collins, AG AF Lewis, Cheryl Bentlage, Bastian Yanagihara, Angel Gillan, William Van Blerk, Johan Keil, Daniel P. Bely, Alexandra E. Collins, Allen G. TI Redescription of Alatina alata (Reynaud, 1830) (Cnidaria: Cubozoa) from Bonaire, Dutch Caribbean SO ZOOTAXA LA English DT Article DE Neotype; Carybdea alata; Carybdeida; cubomedusae; box jellyfish; Atlantic Ocean; aggregation; sexual reproduction; deep-sea; taxonomy ID NEMATOCYST; CARYBDEIDA; EVOLUTION AB Here we establish a neotype for Alatina alata (Reynaud, 1830) from the Dutch Caribbean island of Bonaire. The species was originally described one hundred and eighty three years ago as Carybdea alata in La Centurie Zoologique-a monograph published by Rene Primevere Lesson during the age of worldwide scientific exploration. While monitoring monthly reproductive swarms of A. alata medusae in Bonaire, we documented the ecology and sexual reproduction of this cubozoan species. Examination of forty six A. alata specimens and additional archived multimedia material in the collections of the National Museum of Natural History, Washington, DC revealed that A. alata is found at depths ranging from surface waters to 675 m. Additional studies have reported it at depths of up to 1607 m in the tropical and subtropical Atlantic Ocean. Herein, we resolve the taxonomic confusion long associated with A. alata due to a lack of detail in the original description and conflicting statements in the scientific literature. A new cubozoan character, the velarial lappet, is described for this taxon. The complete description provided here serves to stabilize the taxonomy of the second oldest box jellyfish species, and provide a thorough redescription of the species. C1 [Lewis, Cheryl; Keil, Daniel P.] Univ Maryland, Biol Sci Grad Program, College Pk, MD 20742 USA. [Lewis, Cheryl; Bentlage, Bastian; Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Natl Systemat Lab, Washington, DC 20013 USA. [Bentlage, Bastian] Univ Maryland, Dept Cell Biol & Mol Genet, College Pk, MD 20742 USA. [Yanagihara, Angel] Univ Hawaii Manoa, John A Burns Sch Med, Dept Trop Med Med Microbiol & Pharmacol, Honolulu, HI 96822 USA. [Gillan, William] Boynton Beach Community High Sch, Palm Beach Cty FL Sch, Boynton Beach, FL 33426 USA. [Bely, Alexandra E.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Lewis, C (reprint author), Univ Maryland, Biol Sci Grad Program, College Pk, MD 20742 USA. EM clames1@umd.edu; bastian.bentlage@gmail.com; ayanagih@hawaii.edu; william.gillan@palmbeachschools.org; blerkbonaire@hotmail.com; dkeil@umd.edu; abely@umd.edu; collinsa@si.edu RI Yanagihara, Angel/O-5664-2016 OI Yanagihara, Angel/0000-0001-6908-8176 FU NIMHD NIH HHS [U54 MD007584] NR 31 TC 6 Z9 7 U1 0 U2 6 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD NOV 21 PY 2013 VL 3737 IS 4 BP 473 EP 487 PG 15 WC Zoology SC Zoology GA 267VV UT WOS:000328127300008 PM 25112765 ER PT J AU Pepe, F Cameron, AC Latham, DW Molinari, E Udry, S Bonomo, AS Buchhave, LA Charbonneau, D Cosentino, R Dressing, CD Dumusque, X Figueira, P Fiorenzano, AFM Gettel, S Harutyunyan, A Haywood, RD Horne, K Lopez-Morales, M Lovis, C Malavolta, L Mayor, M Micela, G Motalebi, F Nascimbeni, V Phillips, D Piotto, G Pollacco, D Queloz, D Rice, K Sasselov, D Segransan, D Sozzetti, A Szentgyorgyi, A Watson, CA AF Pepe, Francesco Cameron, Andrew Collier Latham, David W. Molinari, Emilio Udry, Stephane Bonomo, Aldo S. Buchhave, Lars A. Charbonneau, David Cosentino, Rosario Dressing, Courtney D. Dumusque, Xavier Figueira, Pedro Fiorenzano, Aldo F. M. Gettel, Sara Harutyunyan, Avet Haywood, Raphaelle D. Horne, Keith Lopez-Morales, Mercedes Lovis, Christophe Malavolta, Luca Mayor, Michel Micela, Giusi Motalebi, Fatemeh Nascimbeni, Valerio Phillips, David Piotto, Giampaolo Pollacco, Don Queloz, Didier Rice, Ken Sasselov, Dimitar Segransan, Damien Sozzetti, Alessandro Szentgyorgyi, Andrew Watson, Christopher A. TI An Earth-sized planet with an Earth-like density SO NATURE LA English DT Article ID ERROR-CORRECTION; MODEL SELECTION; KEPLER; STARS; ORBIT AB Recent analyses(1-4) of data from the NASA Kepler spacecraft(5) have established that planets with radii within 25 per cent of the Earth's (R-circle plus) are commonplace throughout the Galaxy, orbiting at least 16.5 per cent of Sun-like stars(1). Because these studies were sensitive to the sizes of the planets but not their masses, the question remains whether these Earth-sized planets are indeed similar to the Earth in bulk composition. The smallest planets for which masses have been accurately determined(6,7) are Kepler-10b (1.42R(circle plus)) and Kepler-36b (1.49R(circle plus)), which are both significantly larger than the Earth. Recently, the planet Kepler-78b was discovered(8) and found to have a radius of only 1.16R(circle plus). Here we report that the mass of this planet is 1.86 Earth masses. The resulting mean density of the planet is 5.57 g cm(-3), which is similar to that of the Earth and implies a composition of iron and rock. C1 [Pepe, Francesco; Udry, Stephane; Lovis, Christophe; Mayor, Michel; Motalebi, Fatemeh; Queloz, Didier; Segransan, Damien] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland. [Cameron, Andrew Collier; Haywood, Raphaelle D.; Horne, Keith] Univ St Andrews, Sch Phys & Astron, Scottish Univ Phys Alliance, St Andrews KY16 9SS, Fife, Scotland. [Latham, David W.; Buchhave, Lars A.; Charbonneau, David; Dressing, Courtney D.; Dumusque, Xavier; Gettel, Sara; Lopez-Morales, Mercedes; Phillips, David; Sasselov, Dimitar; Szentgyorgyi, Andrew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Molinari, Emilio; Cosentino, Rosario; Fiorenzano, Aldo F. M.; Harutyunyan, Avet] INAF Fdn Galileo Galilei, Brena Baja 38712, Spain. [Molinari, Emilio] INAF IASF Milano, I-20133 Milan, Italy. [Bonomo, Aldo S.; Sozzetti, Alessandro] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Cosentino, Rosario] INAF Osservatorio Astrofis Catania, I-95125 Catania, Italy. [Figueira, Pedro] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [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. [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, Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland. [Watson, Christopher A.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. RP Pepe, F (reprint author), Univ Geneva, Astron Observ, 51 Chemin Maillettes, CH-1290 Versoix, Switzerland. EM francesco.pepe@unige.ch RI Figueira, Pedro/J-4916-2013; Rice, Ken/H-5084-2011; OI Figueira, Pedro/0000-0001-8504-283X; Piotto, Giampaolo/0000-0002-9937-6387; Rice, Ken/0000-0002-6379-9185; Molinari, Emilio/0000-0002-1742-7735; Micela, Giuseppina/0000-0002-9900-4751; Malavolta, Luca/0000-0002-6492-2085; Sozzetti, Alessandro/0000-0002-7504-365X; Buchhave, Lars A./0000-0003-1605-5666 FU Prodex Program of the Swiss Space Office; Harvard University Origins of Life Initiative; Scottish Universities Physics Alliance; University of Geneva; Smithsonian Astrophysical Observatory; Italian National Astrophysical Institute; University of St Andrews; Queen's University Belfast; University of Edinburgh; European Research Council/European Community through the European Union [239953]; Fundacao para a Ciencia e a Tecnologia [PTDC/CTE-AST/098528/2008, PTDC/CTE-AST/098604/2008]; European Union [313014] FX This Letter was submitted simultaneously with the paper by Howard et al.17. Both papers are the result of a coordinated effort to carry out independent radial-velocity observations and studies of Kepler-78. Our team greatly appreciates the spirit of this collaboration, and we sincerely thank A. Howard and his team for the collegial work. We wish to thank the technical personnel of the Geneva Observatory, the Astronomical Technology Centre, the Smithsonian Astrophysical Observatory and the Telescopio Nazionale Galileo for their enthusiasm and competence, which made the HARPS-N project possible. The HARPS-N project was funded by the Prodex Program of the Swiss Space Office, the Harvard University Origins of Life Initiative, the Scottish Universities Physics Alliance, the University of Geneva, the Smithsonian Astrophysical Observatory, the Italian National Astrophysical Institute, the University of St Andrews, Queen's University Belfast and the University of Edinburgh. P.F. acknowledges support from the European Research Council/European Community through the European Union Seventh Framework Programme, Starting Grant agreement number 239953, and from the Fundacao para a Ciencia e a Tecnologia through grants PTDC/CTE-AST/098528/2008 and PTDC/CTE-AST/098604/2008. The research leading to these results received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement number 313014 (ETAEARTH). NR 28 TC 82 Z9 82 U1 3 U2 38 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 NOV 21 PY 2013 VL 503 IS 7476 BP 377 EP + DI 10.1038/nature12768 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 254KG UT WOS:000327163200036 PM 24172902 ER PT J AU Howard, AW Sanchis-Ojeda, R Marcy, GW Johnson, JA Winn, JN Isaacson, H Fischer, DA Fulton, BJ Sinukoff, E Fortney, JJ AF Howard, Andrew W. Sanchis-Ojeda, Roberto Marcy, Geoffrey W. Johnson, John Asher Winn, Joshua N. Isaacson, Howard Fischer, Debra A. Fulton, Benjamin J. Sinukoff, Evan Fortney, Jonathan J. TI A rocky composition for an Earth-sized exoplanet SO NATURE LA English DT Article ID SOLAR-TYPE STARS; PLANET-SEARCH; MASS; KEPLER; EVOLUTION; ROTATION; ORBIT; SPECTROMETER; PRECISION; TRANSITS AB Planets with sizes between that of Earth (with radius R-circle plus) and Neptune (about 4R(circle plus)) are now known to be common around Sun-like stars(1-3). Most such planets have been discovered through the transit technique, by which the planet's size can be determined from the fraction of starlight blocked by the planet as it passes in front of its star. Measuring the planet's mass-and hence its density, which is a clue to its composition-is more difficult. Planets of size 2-4R(circle plus) have proved to have a wide range of densities, implying a diversity of compositions(4,5), but these measurements did not extend to planets as small as Earth. Here we report Doppler spectroscopic measurements of the mass of the Earth-sized planet Kepler-78b, which orbits its host star every 8.5 hours (ref. 6). Given a radius of 1.20 +/- 0.09R(circle plus) and a mass of 1.69 +/- 0.41M(circle plus), the planet's mean density of 5.3 +/- 1.8 g cm(-3) is similar to Earth's, suggesting a composition of rock and iron. C1 [Howard, Andrew W.; Fulton, Benjamin J.; Sinukoff, Evan] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Sanchis-Ojeda, Roberto; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Sanchis-Ojeda, Roberto; Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06510 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Howard, AW (reprint author), Univ Hawaii Manoa, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM howard@ifa.hawaii.edu; rsanchis86@gmail.com OI Fortney, Jonathan/0000-0002-9843-4354; Fischer, Debra/0000-0003-2221-0861 FU NASA's Science Mission Directorate; Kepler Participating Scientist programme; NASA [NNX12AJ23G] FX This Letter and another10 were submitted simultaneously and are the result of coordinated, independent radial-velocity observations and analyses of Kepler-78. We thank the HARPS-N team for their collegiality. We also thank E. Chiang, I. Crossfield, R. Kolbl, E. Petigura, and D. Huber for discussions, S. Howard for support, C. Dressing for a convenient packaging of stellar models, and A. Hatzes for a thorough review. 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 thank those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are guests. Kepler was competitively selected as the tenth Discovery mission with funding provided by NASA's Science Mission Directorate. J.N.W. and R.S.-O. acknowledge support from the Kepler Participating Scientist programme. A.W.H. acknowledges funding from NASA grant NNX12AJ23G. NR 43 TC 73 Z9 73 U1 4 U2 43 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 NOV 21 PY 2013 VL 503 IS 7476 BP 381 EP + DI 10.1038/nature12767 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 254KG UT WOS:000327163200037 PM 24172898 ER PT J AU Laanbroek, HJ Keijzer, RM Verhoeven, JTA Whigham, DF AF Laanbroek, Hendrikus J. Keijzer, Rosalinde M. Verhoeven, Jos T. A. Whigham, Dennis F. TI Changes in community composition of ammonia-oxidizing betaproteobacteria from stands of Black mangrove (Avicennia germinans) in response to ammonia enrichment and more oxic conditions SO FRONTIERS IN MICROBIOLOGY LA English DT Article DE ammonia oxidation; betaproteobacteria; mangroves; slurries; oxygen ID MOLECULAR ANALYSIS; BACTERIA; SEDIMENTS; DIVERSITY; ESTUARY; ARCHAEA; PROTEOBACTERIA; SALINITY; GRADIENT; AMOA AB In flooded and non-flooded impounded forests of Black mangrove (Avicennia germinans), the community structure of the ammonia-oxidizing betaproteobacteria (beta-AOB) differed among distinct mangrove vegetation cover types and hydrological regimes. This had been explained by a differential response of lineages of beta-AOB to the prevailing soil conditions that included increased levels of moisture and ammonium. To test this hypothesis, slurries of soils collected from a flooded and a non-flooded impoundment were subjected to enhanced levels of ammonium in the absence and presence of additional shaking. After a period of 6 days, the community composition of the beta-AOB based on the 16S rRNA gene was determined and compared with the original community structures. Regardless of the incubation conditions and the origin of the samples, sequences belonging to the Nitrosomonas aestuarii lineage became increasingly dominant, whereas the number of sequences of the lineages of Nitrosospira (i.e., Cluster 1) and Nitrosomonas sp. Nm143 declined. Changes in community structure were related to changes in community sizes determined by quantitative PCR based on the amoA gene. The amoA gene copy numbers of beta-AOB were compared to those of the ammonia-oxidizing archaea (AOA). Gene copy numbers of the bacteria increased irrespective of incubation conditions, but the numbers of archaea declined in the continuously shaken cultures. This observation is discussed in relation to the distribution of the beta-AOB lineages in the impounded Black mangrove forests. C1 [Laanbroek, Hendrikus J.; Keijzer, Rosalinde M.] Netherlands Inst Ecol NIOO KNAW, Dept Microbial Ecol, NL-6700 AB Wageningen, Netherlands. [Laanbroek, Hendrikus J.; Verhoeven, Jos T. A.] Univ Utrecht, Inst Environm Biol, Ecol & Biodivers Grp, Utrecht, Netherlands. [Laanbroek, Hendrikus J.; Verhoeven, Jos T. A.; Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Laanbroek, HJ (reprint author), Netherlands Inst Ecol NIOO KNAW, Dept Microbial Ecol, Droevendaalsesteeg 10,POB 50, NL-6700 AB Wageningen, Netherlands. EM r.laanbroek@nioo.knaw.nl RI Laanbroek, Hendrikus J./C-3830-2008; OI Laanbroek, Hendrikus J./0000-0003-2400-3399; Whigham, Dennis/0000-0003-1488-820X FU Smithsonian Marine Science Network FX We want to acknowledge the help we obtained from Dr. Valery Paul, Woody Lee, and staff of the Smithsonian Marine Station at Fort Pierce. The research was supported by a grant of the Smithsonian Marine Science Network and by resources of the Smithsonian Environmental Research Center, Utrecht University and the Netherlands Institute of Ecology. This is publication number 5531 of the Netherlands Institute of Ecology (NIOO-KNAW) and publication number 934 of the Smithsonian Marine Station. NR 33 TC 2 Z9 2 U1 2 U2 23 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1664-302X J9 FRONT MICROBIOL JI Front. Microbiol. PD NOV 20 PY 2013 VL 4 DI 10.3389/fmicb.2013.00343 PG 9 WC Microbiology SC Microbiology GA AB1GQ UT WOS:000331539900001 ER PT J AU Willmott, KR Hall, JPW AF Willmott, Keith R. Hall, Jason P. W. TI A NEW SPECIES AND TWO NEW SUBSPECIES OF ADELPHA HUBNER, [1819] FROM THE TROPICAL ANDES (NYMPHALIDAE: LIMENITIDINAE) SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY LA English DT Article DE Ecuador; Peru; Bolivia; DNA barcode; COI ID LEPIDOPTERA; BUTTERFLIES; PHYLOGENY; SEQUENCES AB A new species, Adelpha margarita Willmott & Hall, new species, is described from Andean cloud forest habitats from southern Ecuador to Bolivia. Adelpha margarita garleppi Willmott, new subspecies, is described for southern Peruvian and Bolivian individuals, which differ from the nominate subspecies in having complete orange postdiscal bands on the dorsal surface. The new species differs from related species in the Adelpha serpa group in wing pattern, DNA sequence data and habitat. A lectotype is designated for Adelpha seriphia therasia Fruhstorfer, because the type series of this name contains individuals of both A. seriphia and A. margarita. Neighbor-joining and maximum parsimony analyses of 579 bp of the mitochondrial cytochrome oxidase I (COI) 'barcode' region, for 27 Adelpha specimens representing 9 species and 13 taxa, suggest that the closest relative to A. margarita is the Central American to west Andean taxon A. seriphia godmani Fruhstorfer. The DNA sequence data, coupled with a re-analysis of museum specimens, suggest that Adelpha godmani should be treated as a distinct species (revised status). Finally, a new subspecies, Adelpha justina pichincha Willmott & Hall, new subspecies, is described from Pichincha province in western Ecuador. C1 [Willmott, Keith R.] Univ Florida, Florida Museum Nat Hist, McGuire Ctr Lepidoptera & Biodivers, Gainesville, FL 32611 USA. [Hall, Jason P. W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Willmott, KR (reprint author), Univ Florida, Florida Museum Nat Hist, McGuire Ctr Lepidoptera & Biodivers, Gainesville, FL 32611 USA. EM kwillmott@flmnh.ufl.edu FU Leverhulme Trust; FLMNH Museum Associates; National Geographic Society (Research and Exploration) [5751-96]; NSF [0103746, 0639977, 0639861]; Darwin Initiative; National Science Foundation [0847582] FX We thank the museum curators who allowed us to examine the Adelpha collections under their care, and in particular R. Eastwood, B. Huertas and W Mey for providing photos of specimens. Gerardo Lamas provided typically wise and helpful advice concerning the identity of the therasia syntypes and information about MUSM specimens of A. margarita. We thank S. Villamarin, the MECN and Ecuadorian Ministerio del Ambiente for arranging the necessary permits for research in Ecuador. We thank the following for contributing information and/or specimens for study: I. Aldas, C. Brevignon, M. Costa, J. Radford, J. Salazar and C. Whelan. For their careful mentoring in the molecular lab we thank M. Elias, C. Jiggins, S. Mullen and G. Paulay, and we especially thank L. Xiao for her work in generating and editing the majority of the sequences used in this study. Museum and field work was funded in part by the Leverhulme Trust, the Darwin Initiative, the National Science Foundation (# 0847582) and the FLMNH Museum Associates, and field work by the National Geographic Society (Research and Exploration Grant # 5751-96) and NSF (# 0103746, #0639977, #0639861). Finally, we thank G. Lamas and A. Aiello for their helpful comments and suggestions which significantly improved the paper. NR 24 TC 1 Z9 3 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 NOV 20 PY 2013 VL 67 IS 4 BP 241 EP 252 PG 12 WC Entomology SC Entomology GA 302KJ UT WOS:000330603100001 ER PT J AU Sancho, G Funk, VA Roque, N AF Sancho, Gisela Funk, Vicki. A. Roque, Nadia TI Moquiniastrum (Gochnatieae, Asteraceae): disentangling the paraphyletic Gochnatia SO PHYTOTAXA LA English DT Article DE classification; Compositae; nomenclature; taxonomy ID COMPOSITAE; MUTISIEAE AB The new genus Moquiniastrum, the result of recent phylogenetic analyses, is described. Although these analyses are based on cpDNA and nDNA, they also involve documentation of the distinctive morphological characters supporting this new genus. The recognition of Moquiniastrum is necessary to accurately reflect the relationships of the taxa found in the tribe Gochnatieae. Moquiniastrum includes twenty-one species that are usually gynodioecious and found mainly in Brazil but with some species elsewhere in South America. A description of Moquiniastrum, together with the corresponding new combinations, new lectotypifications of three names and one new neotypification is here provided. C1 [Sancho, Gisela] UNLP, Fac Ciencias Nat & Museo, Museo La Plata, Div Plantas Vasc, RA-1900 La Plata, Buenos Aires, Argentina. [Funk, Vicki. A.] US Natl Herbarium, Dept Bot, Smithsonian Inst NMNH, Washington, DC 20560 USA. [Roque, Nadia] Univ Fed Bahia, Inst Biol, BR-40170110 Salvador, BA, Brazil. RP Sancho, G (reprint author), UNLP, Fac Ciencias Nat & Museo, Museo La Plata, Div Plantas Vasc, Paseo Bosque S-N, RA-1900 La Plata, Buenos Aires, Argentina. EM sancho@fcnym.unlp.edu.ar; funkv@si.edu; nadiaroque@gmail.com FU Smithsonian Institution's (SI) National Museum of Natural History small grant; SI's Department of Botany's Cuatrecasas fund Fellowship; Agencia Nacional de Promocion Cientifica y Tecnologica, SECYT, Argentina; Comision Nacional de Investigaciones Cientificas y Tecnologicas, CONICET; CAPES [BEX 0509/13-2]; CNPq [PQ 371248/2001-6] FX We acknowledge the reviewers for useful comments on the manuscript. We are also deeply grateful to the curators of the herbaria who provided the specimens we examined (F, G, ICN, K, LP, MO, NY, S, SP, SPSF, US) and their online resources. We are grateful for funding of fieldwork and museum studies provided by several sources: the Smithsonian Institution's (SI) National Museum of Natural History small grant (VAF), the SI's Department of Botany's Cuatrecasas fund Fellowship (NR), research funds (GS) from Agencia Nacional de Promocion Cientifica y Tecnologica, SECYT, Argentina and Comision Nacional de Investigaciones Cientificas y Tecnologicas, CONICET, and research scolarships (NR) from CAPES (BEX 0509/13-2) and CNPq (PQ 371248/2001-6). NR 42 TC 3 Z9 4 U1 0 U2 4 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 NOV 20 PY 2013 VL 147 IS 1 BP 26 EP 34 PG 9 WC Plant Sciences SC Plant Sciences GA 270LF UT WOS:000328319200003 ER PT J AU Reasenberg, RD AF Reasenberg, Robert D. TI Cavity length measurement: bias from misalignment and mismatching SO APPLIED OPTICS LA English DT Article ID OPTICAL-RESONATOR; ALIGNMENT; STABILIZATION AB SR-POEM, the sounding rocket principle of equivalence measurement, uses a set of six tracking-frequency laser gauges operating in Fabry-Perot cavities to determine the relative acceleration of two test masses (TMs) that are chemically different. One end of each cavity is a flat mirror on a TM; the other end is a concave coupling mirror mounted to a common reference plate. The tracking-frequency laser gauges work by locking a variable frequency laser to the cavity by the method of Pound, Drever, and Hall. Because the TMs are unconstrained, they are expected to rotate slightly during measurement. Although the distance measurements are intended to be based on the TEM00 cavity mode, any misalignment will couple into higher-order transverse modes, particularly the TEM10 and TEM01. Light thus coupled will contribute a spurious signal to the cavity locking servo that causes a bias (i.e., a systematic error) in the length determination. The spurious signal proportional to the misalignment has an anti-symmetric distribution at the detector and thus has a zero average, but causes a distance bias because of the inhomogeneity of the detector responsivity. To prevent such bias, SR-POEM includes a servo to keep the incoming laser beam aligned with the cavity. The required performance of that alignment servo is less stringent than has already been achieved by other projects. There is also a spurious signal proportional to the square of the misalignment that produces a symmetric distribution at the detector. This signal is also made unimportant by the operation of an alignment servo, even when operating well above the shot noise limit. We also look at the locking of a laser to a high finesse cavity and conclude that the alignment quality sets a bound on the ratio of measurement accuracy to cavity linewidth. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Reasenberg, RD (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM reasenberg@cfa.harvard.edu FU Smithsonian Institution; NASA Astrophysics Division [NNX08AO04G] FX This work was supported by the Smithsonian Institution. SR-POEM has been supported by the NASA Astrophysics Division through grant NNX08AO04G. I thank J.D. Phillips for bringing the work of Larason and Bruce to my attention and for his thoughtful comments on the manuscript. NR 13 TC 1 Z9 1 U1 1 U2 4 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD NOV 20 PY 2013 VL 52 IS 33 BP 8154 EP 8160 DI 10.1364/AO.52.008154 PG 7 WC Optics SC Optics GA 258NY UT WOS:000327467200040 PM 24513772 ER PT J AU Kiziltan, B Kottas, A De Yoreo, M Thorsett, SE AF Kiziltan, Buelent Kottas, Athanasios De Yoreo, Maria Thorsett, Stephen E. TI THE NEUTRON STAR MASS DISTRIBUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; methods: statistical; pulsars: general; stars: fundamental parameters; stars: neutron; stars: statistics ID EQUATION-OF-STATE; BINARY MILLISECOND PULSAR; MAXIMUM MASS; GENERAL-RELATIVITY; RADIO PULSARS; SUPER-NOVAE; OBSERVATIONAL CONSTRAINTS; GRAVITATIONAL CONSTANT; COSMIC-RAYS; DISCOVERY AB In recent years, the number of pulsars with secure mass measurements has increased to a level that allows us to probe the underlying neutron star (NS) mass distribution in detail. We critically review the radio pulsar mass measurements. For the first time, we are able to analyze a sizable population of NSs with a flexible modeling approach that can effectively accommodate a skewed underlying distribution and asymmetric measurement errors. We find that NSs that have evolved through different evolutionary paths reflect distinctive signatures through dissimilar distribution peak and mass cutoff values. NSs in double NS and NS-white dwarf (WD) systems show consistent respective peaks at 1.33 M-circle dot and 1.55 M-circle dot, suggesting significant mass accretion (Delta m approximate to 0.22 M-circle dot) has occurred during the spin-up phase. The width of the mass distribution implied by double NS systems is indicative of a tight initial mass function while the inferred mass range is significantly wider for NSs that have gone through recycling. We find a mass cutoff at similar to 2.1 M-circle dot for NSs with WD companions, which establishes a firm lower bound for the maximum NS mass. This rules out the majority of strange quark and soft equation of state models as viable configurations for NS matter. The lack of truncation close to the maximum mass cutoff along with the skewed nature of the inferred mass distribution both enforce the suggestion that the 2.1 M-circle dot limit is set by evolutionary constraints rather than nuclear physics or general relativity, and the existence of rare supermassive NSs is possible. C1 [Kiziltan, Buelent] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kiziltan, Buelent; Thorsett, Stephen E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Kiziltan, Buelent; Thorsett, Stephen E.] UCO Lick Observ, Santa Cruz, CA 95064 USA. [Kottas, Athanasios; De Yoreo, Maria] Univ Calif Santa Cruz, Dept Appl Math & Stat, Santa Cruz, CA 95064 USA. [Thorsett, Stephen E.] Willamette Univ, Dept Phys, Salem, OR 97031 USA. RP Kiziltan, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bkiziltan@cfa.harvard.edu OI Thorsett, Stephen/0000-0002-2025-9613 FU NSF [AST-0506453] FX The authors thank P. Freire for sharing updated probability distribution functions from which some of the NS mass estimates were extracted in Table 2. B. K. and S. E. T. acknowledge NSF grant AST-0506453. The authors thank the anonymous referee for a critical review. After this work was submitted for initial review, Ozel et al. (2012) discussed an alternate approach for estimating the NS mass distribution assuming a Gaussian underlying distribution. NR 91 TC 70 Z9 72 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 NOV 20 PY 2013 VL 778 IS 1 AR 66 DI 10.1088/0004-637X/778/1/66 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700066 ER PT J AU Kozarev, KA Evans, RM Schwadron, NA Dayeh, MA Opher, M Korreck, KE van der Holst, B AF Kozarev, Kamen A. Evans, Rebekah M. Schwadron, Nathan A. Dayeh, Maher A. Opher, Merav Korreck, Kelly E. van der Holst, Bart TI GLOBAL NUMERICAL MODELING OF ENERGETIC PROTON ACCELERATION IN A CORONAL MASS EJECTION TRAVELING THROUGH THE SOLAR CORONA SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; magnetohydrodynamics (MHD); shock waves; Sun: coronal mass ejections (CMEs); Sun: heliosphere; Sun: particle emission ID SELF-GENERATED TURBULENCE; GROUND-LEVEL EVENTS; PARTICLE-ACCELERATION; DRIVEN SHOCKS; COSMIC-RAYS; COLLISIONLESS SHOCKS; CHARGED-PARTICLES; SHEATH STRUCTURES; CYCLE VARIATIONS; MAGNETIC-FIELDS AB The acceleration of protons and electrons to high (sometimes GeV/nucleon) energies by solar phenomena is a key component of space weather. These solar energetic particle (SEP) events can damage spacecraft and communications, as well as present radiation hazards to humans. In-depth particle acceleration simulations have been performed for idealized magnetic fields for diffusive acceleration and particle propagation, and at the same time the quality of MHD simulations of coronal mass ejections (CMEs) has improved significantly. However, to date these two pieces of the same puzzle have remained largely decoupled. Such structures may contain not just a shock but also sizable sheath and pileup compression regions behind it, and may vary considerably with longitude and latitude based on the underlying coronal conditions. In this work, we have coupled results from a detailed global three-dimensional MHD time-dependent CME simulation to a global proton acceleration and transport model, in order to study time-dependent effects of SEP acceleration between 1.8 and 8 solar radii in the 2005 May 13 CME. We find that the source population is accelerated to at least 100 MeV, with distributions enhanced up to six orders of magnitude. Acceleration efficiency varies strongly along field lines probing different regions of the dynamically evolving CME, whose dynamics is influenced by the large-scale coronal magnetic field structure. We observe strong acceleration in sheath regions immediately behind the shock. C1 [Kozarev, Kamen A.; Opher, Merav] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Kozarev, Kamen A.; Korreck, Kelly E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Evans, Rebekah M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Schwadron, Nathan A.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Dayeh, Maher A.] Southwest Res Inst, Dept Space Sci, San Antonio, TX USA. [van der Holst, Bart] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. RP Kozarev, KA (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. RI van der Holst, Bart/A-3557-2013 FU NASA LWS EMMREM [NNX07AC14G]; NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program; NASA Postdoctoral Program at GSFC FX This work was supported under NASA LWS EMMREM project and grant no. NNX07AC14G. K.A.K. was partially supported under the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program, administered by the UCAR Visiting Scientist Programs. R.M.E. is supported through an appointment to the NASA Postdoctoral Program at GSFC, administered by Oak Ridge Associated Universities through a contract with NASA. NR 61 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 NOV 20 PY 2013 VL 778 IS 1 AR 43 DI 10.1088/0004-637X/778/1/43 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700043 ER PT J AU Landi, E Miralles, MP Raymond, JC Hara, H AF Landi, E. Miralles, M. P. Raymond, J. C. Hara, H. TI HOT PLASMA ASSOCIATED WITH A CORONAL MASS EJECTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar-terrestrial relations; Sun: activity; Sun: coronal mass ejections (CMEs); Sun: UV radiation; Sun: X-rays, gamma rays ID X-RAY; MAGNETIC RECONNECTION; IMAGING SPECTROMETER; ENERGETIC PARTICLES; DENSITY DIAGNOSTICS; PHYSICAL CONDITIONS; ATOMIC DATABASE; SOLAR CORONA; FE XIII; FLARE AB We analyze coordinated observations from the EUV Imaging Spectrometer (EIS) and X-Ray Telescope (XRT) on board Hinode of an X-ray Plasma Ejection (XPE) that occurred during the coronal mass ejection (CME) event of 2008 April 9. The XPE was trailing the CME core from behind, following the same trajectory, and could be identified both in EIS and XRT observations. Using the EIS spectrometer, we have determined the XPE plasma parameters, measuring the electron density, thermal distribution, and elemental composition. We have found that the XPE composition and electron density were very similar to those of the pre-event active region plasma. The XPE temperature was higher, and its thermal distribution peaked at around 3 MK; also, typical flare lines were absent from EIS spectra, indicating that any XPE component with temperatures in excess of 5 MK was likely either faint or absent. We used XRT data to investigate the presence of hotter plasma components in the XPE that could have gone undetected by EIS and found that-if at all present-these components have small emission measure values and their temperature is in the 8-12.5 MK range. The very hot plasma found in earlier XPE observations obtained by Yohkoh seems to be largely absent in this CME, although plasma ionization timescales may lead to non-equilibrium ionization effects that could make bright lines from ions formed in a 10 MK plasma not detectable by EIS. Our results supersede the XPE findings of Landi et al., who studied the same event with older response functions for the XRT Al-poly filter; the differences in the results stress the importance of using accurate filter response functions. C1 [Landi, E.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Miralles, M. P.; Raymond, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hara, H.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Landi, E (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. FU NASA [NNX10AQ58G, NNX13AG54G, NNX09AH22G, NNX11AB61G, NN09AB17G]; NSF [AGS-1154443] FX The work of E. Landi is supported by NASA grants NNX10AQ58G and NNX13AG54G, as well as NSF grant AGS-1154443. The work of M. P. Miralles is supported by NASA grants NNX09AH22G, NNX10AQ58G, and NNX11AB61G to the Smithsonian Astrophysical Observatory. The work of J. C. Raymond is supported by NASA grants NN09AB17G and NNX11AB61G to the Smithsonian Astrophysical Observatory. Hinode is a Japanese mission built and launched by JAXA/ISAS, collaborating with NAOJ as a domestic partner, NASA (USA), and PPARC (UK) as international partners. We thank the anonymous referee for comments that helped improve the paper. NR 51 TC 2 Z9 2 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 NOV 20 PY 2013 VL 778 IS 1 AR 29 DI 10.1088/0004-637X/778/1/29 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700029 ER PT J AU Lanzuisi, G Civano, F Marchesi, S Comastri, A Costantini, E Elvis, M Mainieri, V Hickox, R Jahnke, K Komossa, S Piconcelli, E Vignali, C Brusa, M Cappelluti, N Fruscione, A AF Lanzuisi, G. Civano, F. Marchesi, S. Comastri, A. Costantini, E. Elvis, M. Mainieri, V. Hickox, R. Jahnke, K. Komossa, S. Piconcelli, E. Vignali, C. Brusa, M. Cappelluti, N. Fruscione, A. TI THE XMM-NEWTON SPECTRUM OF A CANDIDATE RECOILING SUPERMASSIVE BLACK HOLE: AN ELUSIVE INVERTED P-CYGNI PROFILE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; surveys; X-rays: galaxies ID WIDE-FIELD SURVEY; QUASAR SDSS J092712.65+294344.0; ULTRA-FAST OUTFLOWS; X-RAY SOURCE; COSMOS FIELD; SEYFERT-GALAXIES; ABSORPTION-LINES; RADIATION RECOIL; SOURCE CATALOG; E1821+643 AB We present a detailed spectral analysis of new XMM-Newton data of the source CXOC J100043.1+020637, also known as CID-42, detected in the COSMOS survey at z = 0.359. Previous works suggested that CID-42 is a candidate recoiling supermassive black hole (SMBH) showing also an inverted P-Cygni profile in the X-ray spectra at similar to 6 keV (rest) with an iron emission line plus a redshifted absorption line (detected at 3 sigma in previous XMM-Newton and Chandra observations). Detailed analysis of the absorption line suggested the presence of ionized material flowing into the black hole at high velocity. In the new long XMM-Newton observation, while the overall spectral shape remains constant, the continuum 2-10 keV flux decrease of similar to 20% with respect to previous observation and the absorption line is undetected. The upper limit on the intensity of the absorption line is EW <162 eV. Extensive Monte Carlo simulations show that the nondetection of the line is solely due to variation in the properties of the inflowing material, in agreement with the transient nature of these features, and that the intensity of the line is lower than the previously measured with a probability of 98.8%. In the scenario of CID-42 as a recoiling SMBH, the absorption line can be interpreted as being due to an inflow of gas with variable density that is located in the proximity of the SMBH and recoiling with it. New monitoring observations will be requested to further characterize this line. C1 [Lanzuisi, G.; Civano, F.; Marchesi, S.; Hickox, R.] Dartmouth Coll, Wilder Lab, Dept Phys & Astron, Hanover, NH 03855 USA. [Lanzuisi, G.] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. [Civano, F.; Elvis, M.; Fruscione, A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Marchesi, S.; Vignali, C.; Brusa, M.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Comastri, A.; Cappelluti, N.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Costantini, E.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Mainieri, V.] European So Observ, D-85748 Garching, Germany. [Jahnke, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Komossa, S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Piconcelli, E.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. RP Lanzuisi, G (reprint author), Dartmouth Coll, Wilder Lab, Dept Phys & Astron, Hanover, NH 03855 USA. RI Vignali, Cristian/J-4974-2012; Lanzuisi, Giorgio/K-4378-2013; Comastri, Andrea/O-9543-2015; OI Vignali, Cristian/0000-0002-8853-9611; Brusa, Marcella/0000-0002-5059-6848; Lanzuisi, Giorgio/0000-0001-9094-0984; Comastri, Andrea/0000-0003-3451-9970; piconcelli, enrico/0000-0001-9095-2782; Jahnke, Knud/0000-0003-3804-2137; Cappelluti, Nico/0000-0002-1697-186X FU NASA [11-ADAP11-0218]; German Science Foundation (DFG) [Ja 1114/3-1]; DFG cluster of excellence "Origin and Structure of the Universe"; Aspen Center for Physics; National Science Foundation [PHYS-1066293]; INAF-PRIN; [ASI-INAFI/009/10/0] FX The authors thank A. Longinotti for useful discussions and the anonymous referee for the useful suggestions that improved the overall interpretation of this source. F. C., S. M., and G. L. acknowledge support by the NASA contract 11-ADAP11-0218. K.J. acknowledges support by the German Science Foundation (DFG), grant Ja 1114/3-1. S.K.'s research was supported by the DFG cluster of excellence "Origin and Structure of the Universe" (www.universe-cluster.de). M. E. and S. K. thank the Aspen Center for Physics for support and hospitality. The Aspen Center for Physics is supported by the National Science Foundation under grant No. PHYS-1066293. A. C. acknowledges financial contribution from the agreement ASI-INAFI/009/10/0 and INAF-PRIN 2011. NR 51 TC 2 Z9 2 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 62 DI 10.1088/0004-637X/778/1/62 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700062 ER PT J AU Margutti, R Soderberg, AM Wieringa, MH Edwards, PG Chevalier, RA Morsony, BJ Duran, RB Sironi, L Zauderer, BA Milisavljevic, D Kamble, A Pian, E AF Margutti, R. Soderberg, A. M. Wieringa, M. H. Edwards, P. G. Chevalier, R. A. Morsony, B. J. Duran, R. Barniol Sironi, L. Zauderer, B. A. Milisavljevic, D. Kamble, A. Pian, E. TI THE SIGNATURE OF THE CENTRAL ENGINE IN THE WEAKEST RELATIVISTIC EXPLOSIONS: GRB 100316D SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual (GRB 100316D) ID GAMMA-RAY BURSTS; 25 APRIL 1998; X-RAY; SHOCK BREAKOUT; LIGHT CURVES; PARTICLE-ACCELERATION; MILLISECOND PULSARS; UNUSUAL SUPERNOVA; BRIGHT SUPERNOVA; ENERGY INJECTION AB We present late-time radio and X-ray observations of the nearby sub-energetic gamma-ray burst (GRB)100316D associated with supernova (SN) 2010bh. Our broad-band analysis constrains the explosion properties of GRB 100316D to be intermediate between highly relativistic, collimated GRBs and the spherical, ordinary hydrogen-stripped SNe. We find that similar to 10(49) erg is coupled to mildly relativistic (Gamma = 1.5-2), quasi-spherical ejecta, expanding into a medium previously shaped by the progenitor mass-loss with a rate of (M) over dot similar to 10(-5) M-circle dot yr(-1) (for an assumed wind density profile and wind velocity v(w) = 1000 km s(-1)). The kinetic energy profile of the ejecta argues for the presence of a central engine and identifies GRB 100316D as one of the weakest central-engine-driven explosions detected to date. Emission from the central engine is responsible for an excess of soft X-ray radiation that dominates over the standard afterglow at late times (t > 10 days). We connect this phenomenology with the birth of the most rapidly rotating magnetars. Alternatively, accretion onto a newly formed black hole might explain the excess of radiation. However, significant departure from the standard fall-back scenario is required. C1 [Margutti, R.; Soderberg, A. M.; Sironi, L.; Zauderer, B. A.; Milisavljevic, D.; Kamble, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wieringa, M. H.; Edwards, P. G.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Chevalier, R. A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Morsony, B. J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Duran, R. Barniol] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Pian, E.] INAF IASF Bologna, I-40129 Bologna, Italy. RP Margutti, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Pian, Elena/0000-0001-8646-4858 FU ERC; I-CORE Program of the PBC; ISF [1829/12]; NASA [PF1-120090, NAS8-03060, NNX12AF90G]; NSF [AST1102796]; INAF; David and Lucile Packard Foundation; Commonwealth of Australia FX R.M. is indebted to Cristiano Guidorzi for many interesting discussions. R. M. and B.J.M. thank Dominic Ryan for useful conversations. R. M. thanks the KITP in Santa Barbara for support, hospitality, and the stimulating environment that partially inspired this work. R. B. D. was supported by an ERC advanced grant (GRB) and by the I-CORE Program of the PBC and the ISF (grant 1829/12). 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. B.J.M. is supported by an NSF Astronomy and Astrophysics Post-doctoral Fellowship under award AST1102796. E. P. acknowledges support from INAF PRIN 2011. R. A. C. acknowledges support from NASA grant NNX12AF90G. Support for this work was provided by the David and Lucile Packard Foundation Fellowship for Science and Engineering awarded to A. M. S. The Australia Telescope Compact Array is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. NR 99 TC 20 Z9 21 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 18 DI 10.1088/0004-637X/778/1/18 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700018 ER PT J AU Radigan, J Jayawardhana, R Lafreniere, D Dupuy, TJ Liu, MC Scholz, A AF Radigan, Jacqueline Jayawardhana, Ray Lafreniere, David Dupuy, Trent J. Liu, Michael C. Scholz, Alexander TI DISCOVERY OF A VISUAL T-DWARF TRIPLE SYSTEM AND BINARITY AT THE L/T TRANSITION SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: visual; brown dwarfs; stars: individual (2MASS J08381155+1511155) ID HUBBLE-SPACE-TELESCOPE; STAR ADAPTIVE OPTICS; LOW-MASS BINARIES; ALL-SKY SURVEY; BROWN DWARFS; ULTRACOOL DWARFS; MULTIPLE STARS; SPECTRAL CLASSIFICATION; DYNAMICAL INTERACTIONS; SOLAR NEIGHBORHOOD AB We present new high contrast imaging of eight L/T transition brown dwarfs (BDs) using the NIRC2 camera on the Keck II telescope. One of our targets, the T3.5 dwarf 2MASS J08381155+ 1511155, was resolved into a hierarchal triple with projected separations of 2.5 +/- 0.5 AU and 27 +/- 5 AU for the BC and A(BC) components, respectively. Resolved OSIRIS spectroscopy of the A(BC) components confirms that all system members are T dwarfs. The system therefore constitutes the first triple T-dwarf system ever reported. Using resolved photometry to model the integrated-light spectrum, we infer spectral types of T3 +/- 1, T3 +/- 1, and T4.5 +/- 1 for the A, B, and C components, respectively. The uniformly brighter primary has a bluer J - K-s color than the next faintest component, which may reflect a sensitive dependence of the L/T transition temperature on gravity, or alternatively divergent cloud properties among components. Relying on empirical trends and evolutionary models we infer a total system mass of 0.034-0.104M(circle dot) for the BC components at ages of 0.3-3 Gyr, which would imply a period of 12-21 yr assuming the system semimajor axis to be similar to its projection. We also infer differences in effective temperatures and surface gravities between components of no more than similar to 150 K and similar to 0.1 dex. Given the similar physical properties of the components, the 2M0838+15 system provides a controlled sample for constraining the relative roles of effective temperature, surface gravity, and dust clouds in the poorly understood L/T transition regime. For an age of 3 Gyr we estimate a binding energy of similar to 20 x 10(41) erg for the wide A(BC) pair, which falls above the empirical minimum found for typical BD binaries, and suggests that the system may have been able to survive a dynamical ejection during formation. Combining our imaging survey results with previous work we find an observed binary fraction of 4/18 or 22(-8)(+10) % for unresolved spectral types of L9-T4 at separations greater than or similar to 0 ''.1. This translates into a volume-corrected frequency of 13(-6)(+7) %, which is similar to values of similar to 9%-12% reported outside the transition. Our reported L/T transition binary fraction is roughly twice as large as the binary fraction of an equivalent L9-T4 sample selected from primary rather than unresolved spectral types (6(-4)(+6) -%); however, this increase is not yet statistically significant and a larger sample is required to settle the issue. C1 [Radigan, Jacqueline] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Radigan, Jacqueline; Jayawardhana, Ray] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Lafreniere, David] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Michael C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Scholz, Alexander] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. RP Radigan, J (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM radigan@stsci.edu OI Scholz, Aleks/0000-0001-8993-5053; Lafreniere, David/0000-0002-6780-4252 FU W.M. Keck Foundation FX 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. NR 94 TC 10 Z9 10 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 NOV 20 PY 2013 VL 778 IS 1 AR 36 DI 10.1088/0004-637X/778/1/36 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700036 ER PT J AU Sayers, J Mroczkowski, T Zemcov, M Korngut, PM Bock, J Bulbul, E Czakon, NG Egami, E Golwala, SR Koch, PM Lin, KY Mantz, A Molnar, SM Moustakas, L Pierpaoli, E Rawle, TD Reese, ED Rex, M Shitanishi, JA Siegel, S Umetsu, K AF Sayers, J. Mroczkowski, T. Zemcov, M. Korngut, P. M. Bock, J. Bulbul, E. Czakon, N. G. Egami, E. Golwala, S. R. Koch, P. M. Lin, K. -Y. Mantz, A. Molnar, S. M. Moustakas, L. Pierpaoli, E. Rawle, T. D. Reese, E. D. Rex, M. Shitanishi, J. A. Siegel, S. Umetsu, K. TI A MEASUREMENT OF THE KINETIC SUNYAEV-ZEL'DOVICH SIGNAL TOWARD MACS J0717.5+3745 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (MACS J0717.5+3745); galaxies: clusters: intracluster medium ID MASSIVE GALAXY CLUSTERS; SOUTH-POLE TELESCOPE; STAR-FORMING GALAXIES; 2 DISTANT CLUSTERS; X-RAY; RELATIVISTIC CORRECTIONS; LAMBDA-CDM; BULK FLOW; XMM-NEWTON; BACKGROUND ANISOTROPIES AB We report our analysis of MACS J0717.5+3745 using 140 and 268 GHz Bolocam data collected at the Caltech Submillimeter Observatory. We detect extended Sunyaev-Zel'dovich (SZ) effect signal at high significance in both Bolocam bands, and we employ Herschel-SPIRE observations to subtract the signal from dusty background galaxies in the 268 GHz data. We constrain the two-band SZ surface brightness toward two of the sub-clusters of MACS J0717.5+3745: the main sub-cluster (named C), and a sub-cluster identified in spectroscopic optical data to have a line-of-sight velocity of +3200 km s (1) (named B). We determine the surface brightness in two separate ways: via fits of parametric models and via direct integration of the images. For both sub-clusters, we find consistent surface brightnesses from both analysis methods. We constrain spectral templates consisting of relativistically corrected thermal and kinetic SZ signals, using a jointly-derived electron temperature from Chandra and XMM-Newton under the assumption that each sub-cluster is isothermal. The data show no evidence for a kinetic SZ signal toward sub-cluster C, but they do indicate a significant kinetic SZ signal toward sub-cluster B. The model-derived surface brightnesses for sub-cluster B yield a best-fit, line-of-sight velocity of v(z) = +3450 +/- 900 km s(-1), with (1 - Prob[v(z) >= 0]) = 1.3 x 10(-5) (4.2 sigma away from 0 for a Gaussian distribution). The directly integrated sub-cluster B SZ surface brightnesses provide a best-fit v(z) = +2550 +/- 1050 km s(-1), with (1 - Prob[ v(z) >= 0]) = 2.2 x 10(-3) (2.9 sigma). C1 [Sayers, J.; Mroczkowski, T.; Zemcov, M.; Bock, J.; Czakon, N. G.; Golwala, S. R.; Siegel, S.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Mroczkowski, T.; Zemcov, M.; Korngut, P. M.; Bock, J.; Moustakas, L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bulbul, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Egami, E.; Rawle, T. D.; Rex, M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Koch, P. M.; Lin, K. -Y.; Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Mantz, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Molnar, S. M.] Natl Taiwan Univ, LeCosPA Ctr, Taipei 10617, Taiwan. [Pierpaoli, E.; Shitanishi, J. A.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Reese, E. D.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Reese, E. D.] Moorpark Coll, Dept Phys Astron & Engn, Moorpark, CA 93021 USA. RP Sayers, J (reprint author), CALTECH, Div Phys Math & Astron, 1200 East Calif Blvd, Pasadena, CA 91125 USA. EM jack@caltech.edu OI Mroczkowski, Tony/0000-0003-3816-5372; Umetsu, Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360; Pierpaoli, Elena/0000-0002-7957-8993 FU Gordon and Betty Moore Foundation; Norris Foundation CCAT Postdoctoral Fellowship; NASA [PF0-110077, NAS8-0360]; Chandra X-ray Center; NASA Postdoctoral Program Fellowship; NASA Graduate Student Research Fellowship; NASA Earth and Space Science Fellowship [NASA/NNX12AL62H]; National Science Council of Taiwan [NSC100-2112-M-001-008-MY3]; Academia Sinica Career Development Award; [NSF/AST-0838261]; [NASA/NNX11AB07G]; [NSF/AST-0838187]; [NSF/AST-1140019]; [NASA/NNX07AH59G] FX We acknowledge the assistance of: the day crew and Hilo staff of the Caltech Submillimeter Observatory, who provided invaluable assistance during data-taking for this data set; Kathy Deniston, Barbara Wertz, and Diana Bisel, who provided effective administrative support at Caltech and in Hilo; the Bolocam observations were partially supported by the Gordon and Betty Moore Foundation. J.S. was supported by NSF/AST-0838261, NASA/NNX11AB07G, and the Norris Foundation CCAT Postdoctoral Fellowship; support for T.M. was provided by NASA through Einstein Fellowship Program grant No. PF0-110077 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060; P.M.K. was supported by a NASA Postdoctoral Program Fellowship; N.C. was partially supported by a NASA Graduate Student Research Fellowship; A.M. was partially supported by NSF/AST-0838187 and NSF/AST-1140019; E.P. and J. A. S. were partially supported by NASA/NNX07AH59G; S.S. was supported by NASA Earth and Space Science Fellowship NASA/NNX12AL62H; K.U. acknowledges partial support from the National Science Council of Taiwan grant NSC100-2112-M-001-008-MY3 and from the Academia Sinica Career Development Award. A portion of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This research made use of the Caltech Submillimeter Observatory, which was operated at the time by the California Institute of Technology under cooperative agreement with the National Science Foundation (NSF/AST-0838261). This work is also based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with a significant participation by NASA. Partial support for this work was provided by NASA through an award issued by JPL/Caltech. NR 101 TC 23 Z9 23 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 NOV 20 PY 2013 VL 778 IS 1 AR 52 DI 10.1088/0004-637X/778/1/52 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700052 ER PT J AU Virgili, FJ Mundell, CG Pal'Shin, V Guidorzi, C Margutti, R Melandri, A Harrison, R Kobayashi, S Chornock, R Henden, A Updike, AC Cenko, SB Tanvir, NR Steele, IA Cucchiara, A Gomboc, A Levan, A Cano, Z Mottram, CJ Clay, NR Bersier, D Kopac, D Japelj, J Filippenko, AV Li, W Svinkin, D Golenetskii, S Hartmann, DH Milne, PA Williams, G O'Brien, PT Fox, DB Berger, E AF Virgili, F. J. Mundell, C. G. Pal'Shin, V. Guidorzi, C. Margutti, R. Melandri, A. Harrison, R. Kobayashi, S. Chornock, R. Henden, A. Updike, A. C. Cenko, S. B. Tanvir, N. R. Steele, I. A. Cucchiara, A. Gomboc, A. Levan, A. Cano, Z. Mottram, C. J. Clay, N. R. Bersier, D. Kopac, D. Japelj, J. Filippenko, A. V. Li, W. Svinkin, D. Golenetskii, S. Hartmann, D. H. Milne, P. A. Williams, G. O'Brien, P. T. Fox, D. B. Berger, E. TI GRB 091024A AND THE NATURE OF ULTRA-LONG GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual (GRB 091024A) ID AUTOMATIC IMAGING TELESCOPE; REVERSE SHOCK EMISSION; CENTRAL ENGINE; LIGHT CURVES; PROMPT EMISSION; SPECTRAL EVOLUTION; AFTERGLOW EMISSION; OPTICAL-EMISSION; QUIESCENT TIMES; KINETIC-ENERGY AB We present a broadband study of gamma-ray burst (GRB) 091024A within the context of other ultra-long-duration GRBs. An unusually long burst detected by Konus-Wind (KW), Swift, and Fermi, GRB 091024A has prompt emission episodes covering similar to 1300 s, accompanied by bright and highly structured optical emission captured by various rapid-response facilities, including the 2 m autonomous robotic Faulkes North and Liverpool Telescopes, KAIT, S-LOTIS, and the Sonoita Research Observatory. We also observed the burst with 8 and 10 m class telescopes and determine the redshift to be z = 1.0924 +/- 0.0004. We find no correlation between the optical and gamma-ray peaks and interpret the optical light curve as being of external origin, caused by the reverse and forward shock of a highly magnetized jet (R-B approximate to 100-200). Low-level emission is detected throughout the near-background quiescent period between the first two emission episodes of the KW data, suggesting continued central-engine activity; we discuss the implications of this ongoing emission and its impact on the afterglow evolution and predictions. We summarize the varied sample of historical GRBs with exceptionally long durations in gamma-rays ( greater than or similar to 1000 s) and discuss the likelihood of these events being from a separate population; we suggest ultra-long GRBs represent the tail of the duration distribution of the long GRB population. C1 [Virgili, F. J.; Mundell, C. G.; Harrison, R.; Kobayashi, S.; Steele, I. A.; Mottram, C. J.; Clay, N. R.; Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Pal'Shin, V.; Svinkin, D.; Golenetskii, S.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Guidorzi, C.] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy. [Margutti, R.; Chornock, R.; Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Melandri, A.] INAF Brera Astron Observ, I-23807 Merate, LC, Italy. [Henden, A.] AAVSO, Cambridge, MA 02138 USA. [Updike, A. C.] Roger Williams Univ, Dept Chem & Phys, Bristol, RI 02809 USA. [Cenko, S. B.; Filippenko, A. V.; Li, W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Tanvir, N. R.; O'Brien, P. T.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Cucchiara, A.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Gomboc, A.; Kopac, D.; Japelj, J.] Univ Ljubljana, Fac Math & Phys, Ljubljana 1000, Slovenia. [Levan, A.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Cano, Z.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Hartmann, D. H.] Clemson Univ, Dept Phys & Astron, Kinard Lab 118, Clemson, SC 29631 USA. [Milne, P. A.; Williams, G.] Univ Arizona, MMT Observ, Tucson, AZ 85719 USA. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. RP Virgili, FJ (reprint author), Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. EM F.J.Virgili@ljmu.ac.uk RI Svinkin, Dmitry/C-1934-2014; Pal'shin, Valentin/F-3973-2014; Golenetskii, Sergey/B-3818-2015 FU UK Science and Technology Facilities Council; Royal Society; Wolfson Foundation; Sun Microsys-tems, Inc.; Hewlett-Packard Company; AutoScope Corporation; Lick Observatory; NSF; University of California; Sylvia and Jim Katzman Foundation; TABASGO Foundation; W. M. Keck Foundation; Gary and Cynthia Bengier; Christopher R. Redlich Fund; Richard and Rhoda Goldman Fund; NSF [AST-1211916]; NASA/Swift [NNX10AI21G, NNX12AD73G] FX F.J.V. acknowledges support from the UK Science and Technology Facilities Council. C.G.M. acknowledges funding from the Royal Society, the Wolfson Foundation, and the UK Science and Technology Facilities Council. We are grateful for excellent staff assistance at the various observatories where we obtained data. The Liverpool Telescope is operated by Liverpool John Moores University at the Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The Faulkes Telescopes, now owned by the Las Cumbres Observatory Global Telescope network, are operated with support from the Dill Faulkes Educational Trust. KAIT and its ongoing operation were made possible by donations from Sun Microsys-tems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia and Jim Katzman Foundation, and the TABASGO Foundation. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The Konus-Wind experiment is supported by a Russian Space Agency contract and RFBR grant 12-02-00032-a. Swift, launched in 2004 November, is a NASA mission in partnership with the Italian Space Agency and the UK Space Agency. A.V.F.'s group at UC Berkeley has received generous financial assistance from Gary and Cynthia Bengier, the Christopher R. Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, NSF grant AST-1211916, and NASA/Swift grants NNX10AI21G and NNX12AD73G. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. NR 137 TC 36 Z9 36 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 54 DI 10.1088/0004-637X/778/1/54 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700054 ER PT J AU Gupta, H Gottlieb, CA Lattanzi, V Pearson, JC McCarthy, MC AF Gupta, H. Gottlieb, C. A. Lattanzi, V. Pearson, J. C. McCarthy, M. C. TI LABORATORY MEASUREMENTS AND TENTATIVE ASTRONOMICAL IDENTIFICATION OF H2NCO+ SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: molecules ID GALACTIC-CENTER REGION; DIFFUSE INTERSTELLAR-MEDIUM; PROTONATED ISOCYANIC ACID; RAY IONIZATION RATE; LOW-TEMPERATURE; SAGITTARIUS B2; FULMINIC ACID; SGR B2; GAS; HNCO AB The rotational spectrum of H2NCO+, the ground-state isomer of protonated HNCO, has been measured in a molecular beam in the centimeter band with a Fourier transform microwave spectrometer and in a low-pressure laboratory discharge in absorption in the millimeter band. Spectroscopic constants, including the nitrogen-14 hyperfine coupling constant, derived from 30 a-type transitions between 20 and 367 GHz with J <= 18 and K-a <= 3 allow the principal rotational transitions to be calculated to 1 km s(-1) or better in equivalent radial velocity well into the far IR. Two low-lying rotational transitions of H2NCO+ in the centimeter band (0(0,0)-1(0,1) and 1(1,0)-2(1,1)) were tentatively identified in absorption in the PRIMOS spectral line survey of Sgr B2(N) with the Green Bank Telescope. The lines of H2NCO+ arise in a region of the Sgr B2(N) halo whose density is low (n < 1 x 10(4) cm(-3)). The derived column density of (6-14) x 10(11) cm(-2) implies that the fractional abundance is similar to 10(-12). Owing to the ubiquity of HNCO in galactic molecular clouds, H2NCO+ is a good candidate for detection in sources spanning a wide range of physical conditions. C1 [Gupta, H.; Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gottlieb, C. A.; Lattanzi, V.; McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gupta, H (reprint author), CALTECH, Infrared Proc & Anal Ctr, 770 S Wilson Ave, Pasadena, CA 91125 USA. FU NASA [NNX13AE59G, NNX08AE05G, NNX08AI41G]; National Aeronautics and Space Administration FX We are indebted to P. F. Goldsmith, M. Gerin, and D. C. Lis for helpful discussions; S. Thorwirth for communicating results of his high-level coupled cluster quantum calculations; J. Neill for sharing unpublished measurements of HNCO in Sgr B2(N) with Herschel; and F. Crim for advice and D. Kokkin for assistance with the preparation of the HNCO precursor in the laboratory experiments. The work in Cambridge was supported by NASA Grants NNX13AE59G, NNX08AE05G, and NNX08AI41G. A portion of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 35 TC 5 Z9 5 U1 1 U2 17 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 NOV 20 PY 2013 VL 778 IS 1 AR L1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 253VF UT WOS:000327116700001 ER PT J AU Zheng, WK Silverman, JM Filippenko, AV Kasen, D Nugent, PE Graham, M Wang, XF Valenti, S Ciabattari, F Kelly, PL Fox, OD Shivvers, I Clubb, KI Cenko, SB Balam, D Howell, DA Hsiao, E Li, WD Marion, GH Sand, D Vinko, J Wheeler, JC Zhang, JJ AF Zheng, WeiKang Silverman, Jeffrey M. Filippenko, Alexei V. Kasen, Daniel Nugent, Peter E. Graham, Melissa Wang, Xiaofeng Valenti, Stefano Ciabattari, Fabrizio Kelly, Patrick L. Fox, Ori D. Shivvers, Isaac Clubb, Kelsey I. Cenko, S. Bradley Balam, Dave Howell, D. Andrew Hsiao, Eric Li, Weidong Marion, G. Howie Sand, David Vinko, Jozsef Wheeler, J. Craig Zhang, JuJia TI THE VERY YOUNG TYPE Ia SUPERNOVA 2013dy: DISCOVERY, AND STRONG CARBON ABSORPTION IN EARLY-TIME SPECTRA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE supernovae: general; supernovae: individual (SN 2013dy) ID WHITE-DWARF STAR; SPECTROSCOPIC OBSERVATIONS; LIGHT CURVES; SN 2011FE; TELESCOPE; PROGRAM; 2009DC; SPECTROGRAPH; ULTRAVIOLET; PROGENITOR AB The Type Ia supernova (SN Ia) 2013dy in NGC 7250 (d approximate to 13.7 Mpc) was discovered by the Lick Observatory Supernova Search. Combined with a prediscovery detection by the Italian Supernova Search Project, we are able to constrain the first-light time of SN 2013dy to be only 0.10 +/- 0.05 days (2.4 +/- 1.2 hr) before the first detection. This makes SN 2013dy the earliest known detection of an SN Ia. We infer an upper limit on the radius of the progenitor star of R-0 less than or similar to 0.25 R-circle dot, consistent with that of a white dwarf. The light curve exhibits a broken power law with exponents of 0.88 and then 1.80. A spectrum taken 1.63 days after first light reveals a C II absorption line comparable in strength to Si II. This is the strongest C II feature ever detected in a normal SN Ia, suggesting that the progenitor star had significant unburned material. The C II line in SN 2013dy weakens rapidly and is undetected in a spectrum 7 days later, indicating that C II is detectable for only a very short time in some SNe Ia. SN 2013dy reached a B-band maximum of M-B = -18.72 +/- 0.03 mag similar to 17.7 days after first light. C1 [Zheng, WeiKang; Filippenko, Alexei V.; Nugent, Peter E.; Graham, Melissa; Kelly, Patrick L.; Fox, Ori D.; Shivvers, Isaac; Clubb, Kelsey I.; Li, Weidong] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Silverman, Jeffrey M.; Marion, G. Howie; Vinko, Jozsef; Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Kasen, Daniel; Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Kasen, Daniel] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Graham, Melissa; Valenti, Stefano; Howell, D. Andrew] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Graham, Melissa; Valenti, Stefano; Howell, D. Andrew] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wang, Xiaofeng] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Ciabattari, Fabrizio] Monte Agliale Observ, I-55023 Borgo A Mozzano, Lucca, Italy. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Balam, Dave] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Astrophys Observ, Victoria, BC V9E 2E7, Canada. [Hsiao, Eric] Las Campanas Observ, Carnegie Observ, Colina El Pino, Chile. [Marion, G. Howie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sand, David] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Vinko, Jozsef] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Zhang, JuJia] Chinese Acad Sci, Yunan Astron Observ, Beijing 650011, Yunnan, Peoples R China. [Zhang, JuJia] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650011, Peoples R China. RP Zheng, WK (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM zwk@astro.berkeley.edu RI Wang, Xiaofeng/J-5390-2015; OI Shivvers, Isaac/0000-0003-3373-8047 FU TABASGO Foundation; Sylvia and Jim Katzman Foundation; Christopher R. Redlich Fund; NSF [AST-1211916, AST-1302771, AST-1109801]; NNSFC [11073013, 11178003]; Foundation of Tsinghua University [2011Z02170]; Major State Basic Research Development Program [2013CB834903]; Hungarian OTKA [NN 107637]; DoE [DE-AC02-05CH11231]; W. M. Keck Foundation FX A.V.F.'s group (and KAIT) at UC Berkeley have received financial assistance from the TABASGO Foundation, the Sylvia and Jim Katzman Foundation, the Christopher R. Redlich Fund, and NSF grant AST-1211916. J.M.S. is supported by an NSF postdoctoral fellowship under award AST-1302771. X. Wang acknowledges NNSFC grants 11073013 and 11178003, the Foundation of Tsinghua University (2011Z02170), and the Major State Basic Research Development Program (2013CB834903). J.V. is grateful for Hungarian OTKA grant NN 107637. J.C.W. acknowledge support from NSF AST-1109801. This research used resources of NERSC, supported by DoE under Contract DE-AC02-05CH11231. Some data were obtained at the W. M. Keck Observatory, which was made possible by the generous financial support of the W. M. Keck Foundation. We thank the staffs of the various observatories at which data were obtained. We also thank the anonymous referee for useful suggestions which improved the Letter. NR 42 TC 28 Z9 28 U1 0 U2 17 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 NOV 20 PY 2013 VL 778 IS 1 AR L15 DI 10.1088/2041-8205/778/1/L15 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 253VF UT WOS:000327116700015 ER PT J AU Gilmour, CC Riedel, GS Riedel, G Kwon, S Landis, R Brown, SS Menzie, CA Ghosh, U AF Gilmour, Cynthia C. Riedel, Georgia S. Riedel, Gerhardt Kwon, Seokjoon Landis, Richard Brown, Steven S. Menzie, Charles A. Ghosh, Upal TI Activated Carbon Mitigates Mercury and Methylmercury Bioavailability in Contaminated Sediments SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID DISSOLVED ORGANIC-MATTER; AMPHIPOD LEPTOCHEIRUS-PLUMULOSUS; MARINE SEDIMENT; AQUATIC ECOSYSTEMS; CAPPING EFFICIENCY; CONTINENTAL-SHELF; CHESAPEAKE BAY; REDUCE PCB; METHYLATION; REMEDIATION AB There are few available in situ remediation options for Hg contaminated sediments, short of capping. Here we present the first tests of activated carbon and other sorbents as potential in situ amendments for remediation of mercury and methylmercury (MeHg), using a study design that combined 2 L sediment/water microcosms with 14 day bioaccumulation assays. Our key key end points were pore water concentrations, and bioaccumulation of total Hg and MeHg by a deposit-feeding oligo-chaete Lumbriculus variegatus. Four amendments were tested: an activated carbon (AG); CETCO Organoclay MRM (MRM); Thiol-SAMMS (TS), a thiol-functionalized mesoporous silica; and A/VIBERSEP GT74, an ion-exchange resin. Amendments were tested in four separate microcosm assays using Hg-contaminated sediments from two freshwater and two estuarine sites. AC and TS amendments, added at 2-7% of the dry weight of sediments significantly reduced both MeHg concentrations in pore waters, relative to unamended controls (by 45-95%) and bioaccumulation of MeHg by Lumbriculus (by between 30 and 90%). Both amendments had only small impacts on microcosm surface water, sediment and pore water chemistry, with the exception of significant reductions in pore water dissolved organic matter. The effectiveness of amendments in reducing bioaccumulation was well-correlated with their effectiveness in increasing sediment:water partitioning, especially of MeHg. Sediments with low native sediment:water MeHg partition coefficients were most effectively treated. Thus, in situ sediment sorbent amendments may be able to reduce the risk of biotic Hg and MeHg uptake in contaminated sediments, and subsequent contamination of food webs. C1 [Gilmour, Cynthia C.; Riedel, Georgia S.; Riedel, Gerhardt] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Kwon, Seokjoon; Ghosh, Upal] Univ Maryland Baltimore Cty, Dept Chem Biochem & Environm Engn, Baltimore, MD 21250 USA. [Landis, Richard] EI Pont Nemours & Co Chestnut Run Plaza, Wilmington, DE 19805 USA. [Brown, Steven S.] Dow Chem Co USA, Spring House, PA 19477 USA. [Menzie, Charles A.] Exponent, Alexandria, VA 22314 USA. RP Gilmour, CC (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM gilmourc@si.edu RI Gilmour, Cynthia/G-1784-2010 OI Gilmour, Cynthia/0000-0002-1720-9498 FU U.S. Department of Defense ESTCP Program [08 EB-ER4-017]; Dow Chemical Company; I.E. DuPont de Nemours FX We thank J. Tyler Bell, Tay Ian Morcol, Carl Mitchell, SERC REU students Sharmila Pal and Maya Nadimpali, and Ben Amos (Exponent) for assistance with these studies. The E.I. du Pont de Nemours Company (Rich Landis and Nancy Grosso) and The Dow Chemical Company (Steven Brown) provided some study sediments. Allison O'Brien and others at DOD/Aberdeen Proving Grounds helped with access and background data for the Canal Creek site. Three anonymous reviewers substantially improved the manuscript. This work was supported by the U.S. Department of Defense ESTCP Program through award 08 EB-ER4-017 to CAM., U.G., and C.G.; and through support from The Dow Chemical Company and I.E. DuPont de Nemours. NR 52 TC 15 Z9 17 U1 1 U2 82 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD NOV 19 PY 2013 VL 47 IS 22 BP 13001 EP 13010 DI 10.1021/es4021074 PG 10 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 257CI UT WOS:000327360600049 PM 24156748 ER PT J AU Kirk, NL Ritson-Williams, R Coffroth, MA Miller, MW Fogarty, ND Santos, SR AF Kirk, Nathan L. Ritson-Williams, Raphael Coffroth, Mary Alice Miller, Margaret W. Fogarty, Nicole D. Santos, Scott R. TI Tracking Transmission of Apicomplexan Symbionts in Diverse Caribbean Corals SO PLOS ONE LA English DT Article ID ANNULARIS SPECIES COMPLEX; SCLERACTINIAN CORALS; PORITES-ASTREOIDES; ACROPORA-PALMATA; PLANULA LARVAE; REEF CORALS; SEXUAL REPRODUCTION; GENUS SYMBIODINIUM; TOXOPLASMA-GONDII; PERKINSUS-MARINUS AB Symbionts in each generation are transmitted to new host individuals either vertically (parent to offspring), horizontally (from exogenous sources), or a combination of both. Scleractinian corals make an excellent study system for understanding patterns of symbiont transmission since they harbor diverse symbionts and possess distinct reproductive modes of either internal brooding or external broadcast spawning that generally correlate with vertical or horizontal transmission, respectively. Here, we focused on the under-recognized, but apparently widespread, coral-associated apicomplexans (Protista: Alveolata) to determine if symbiont transmission depends on host reproductive mode. Specifically, a PCR-based assay was utilized towards identifying whether planula larvae and reproductive adults from brooding and broadcast spawning scleractinian coral species in Florida and Belize harbored apicomplexan DNA. Nearly all (85.5%; n = 85/89) examined planulae of five brooding species (Porites astreoides, Agaricia tenuifolia, Agaricia agaricites, Favia fragum, Mycetophyllia ferox) and adults of P. astreoides were positive for apicomplexan DNA. In contrast, no (n = 0/10) apicomplexan DNA was detected from planulae of four broadcast spawning species (Acropora cervicornis, Acropora palmata, Pseudodiploria strigosa, and Orbicella faveolata) and rarely in gametes (8.9%; n = 5/56) of these species sampled from the same geographical range as the brooding species. In contrast, tissue samples from nearly all (92.0%; n = 81/88) adults of the broadcast spawning species A. cervicornis, A. palmata and O. faveolata harbored apicomplexan DNA, including colonies whose gametes and planulae tested negative for these symbionts. Taken together, these data suggest apicomplexans are transmitted vertically in these brooding scleractinian coral species while the broadcast spawning scleractinian species examined here acquire these symbionts horizontally. Notably, these transmission patterns are consistent with those of other scleractinian coral symbionts. While this study furthers knowledge regarding these symbionts, numerous questions remain to be addressed, particularly in regard to the specific interaction(s) between these apicomplexans and their hosts. C1 [Kirk, Nathan L.; Santos, Scott R.] Auburn Univ, Dept Biol Sci, Auburn, AL 36849 USA. [Kirk, Nathan L.; Santos, Scott R.] Auburn Univ, Molette Biol Lab Environm & Climate Change Studie, Auburn, AL 36849 USA. [Ritson-Williams, Raphael] Smithsonian Marine Stn, Ft Pierce, FL USA. [Coffroth, Mary Alice] SUNY Buffalo, Dept Geol, Buffalo, NY 14260 USA. [Miller, Margaret W.] NOAA, Southeast Fisheries Sci Ctr, Miami, FL USA. [Fogarty, Nicole D.] Nova SE Univ, Oceanog Ctr, Dania, FL USA. [Santos, Scott R.] Auburn Univ, Cellular & Mol Biosci Peak Program, Auburn, AL 36849 USA. RP Kirk, NL (reprint author), Auburn Univ, Dept Biol Sci, Auburn, AL 36849 USA. EM kirknat@gmail.com RI Santos, Scott/A-7472-2009 FU PADI Foundation [4005]; National Science Foundation [OCE-09-26822]; NOAA Coral Reef Conservation Program; MOTE protect our reefs grant [POR-2010-29] FX This work was funded by grants from the PADI Foundation (http://www.padifoundation.org/ #4005 to NLK), National Science Foundation (http://www.nsf.gov/: OCE-09-26822 to MAC), the NOAA Coral Reef Conservation Program (http://coralreef.noaa.gov/aboutcrcp/workwithus/funding/grants/) and the MOTE protect our reefs grant (http://isurus.mote.org/Keys/reef_plate.phtml: POR-2010-29 to VP). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 87 TC 1 Z9 1 U1 1 U2 26 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD NOV 19 PY 2013 VL 8 IS 11 AR e80618 DI 10.1371/journal.pone.0080618 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 256LO UT WOS:000327311900079 PM 24260438 ER PT J AU Carrejo, N Diaz, AE Woodley, NE AF Carrejo, Nancy Diaz, Ana E. Woodley, Norman E. TI A new species of Lixophaga Townsend (Diptera: Tachinidae) from Colombia, a parasitoid of Neoleucinodes elegantalis (Guenee) (Lepidoptera: Crambidae) SO ZOOTAXA LA English DT Article DE Diptera; Tachinidae; Lixophaga puscolulo; new species; Neotropical Region ID DIATRAEAE AB A new species of Lixophaga Townsend (Diptera: Tachinidae) from Colombia, Lixophaga puscolulo Carrejo & Woodley, sp. nov., is described and illustrated. It is a parasitoid of the tomato fruit borer, Neoleucinodes elegantalis (Guenee) (Lepidoptera: Crambidae), an insect pest of Solanum quitoense Lam., in Colombia. Aspects of its biology are briefly discussed. C1 [Carrejo, Nancy] Univ Valle, Dept Biol, Cali 25630, Colombia. [Diaz, Ana E.] CORPOICA, La Selva, Rionegro Antioq, Colombia. [Woodley, Norman E.] ARS, Systemat Entomol Lab, USDA, Smithsonian Inst NHB 168, Washington, DC 20013 USA. RP Woodley, NE (reprint author), ARS, Systemat Entomol Lab, USDA, Smithsonian Inst NHB 168, POB 37012, Washington, DC 20013 USA. EM nancy.carrejo@correounivalle.edu.co; aediaz@corpoica.org.co; norman.woodley@ars.usda.gov RI Woodley, Norman/M-6160-2014 FU Regional Fund for Agricultural Technology (FONTAGRO) FX Many thanks to the Regional Fund for Agricultural Technology (FONTAGRO) for funding this study; to research assistants Mr. Gilberto Higuinio and Mr. Manuel Hincapie (Corpoica, La Selva Research Station); to student Mrs. Bibiana Villada (Universidad Catolica de Oriente (UCO), Rionegro, Antioquia) for the collecting of L. puscolulo in the field and its rearing in the laboratory, and for kindly providing the wonderful photos in Figs. 11-14; to Dr. William H. White (USDA-ARS Sugarcane Research Unit) for the loan of specimens of Lixophaga diatraeae used in this study for comparison with L. puscolulo. We are grateful to Dr. D. M. Wood for discussion about the taxonomy of Lixophaga. Special thanks to Dr. Takumasa Kondo for translating the text originally written in Spanish, and for reviewing the manuscript. USDA is an equal opportunity provider and employer. NR 22 TC 0 Z9 0 U1 0 U2 5 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD NOV 18 PY 2013 VL 3737 IS 1 BP 68 EP 76 PG 9 WC Zoology SC Zoology GA 267VO UT WOS:000328126600005 PM 25112737 ER PT J AU Sosa-Calvo, J Schultz, TR Brandao, CRF Klingenberg, C Feitosa, RM Rabeling, C Bacci, M Lopes, CT Vasconcelos, HL AF Sosa-Calvo, Jeffrey Schultz, Ted R. Brandao, Carlos R. F. Klingenberg, Christiana Feitosa, Rodrigo M. Rabeling, Christian Bacci, Mauricio, Jr. Lopes, Caue T. Vasconcelos, Heraldo L. TI Cyatta abscondita: Taxonomy, Evolution, and Natural History of a New Fungus-Farming Ant Genus from Brazil SO PLOS ONE LA English DT Article ID LEAF-CUTTING ANTS; MYCOCEPURUS-SMITHII HYMENOPTERA; FORMICIDAE MYRMICINAE ATTINI; GROWING ANT; MICROBE SYMBIOSIS; THELYTOCOUS PARTHENOGENESIS; PHYLOGENETIC ANALYSES; ATTA-CEPHALOTES; INSECT ORDER; COEVOLUTION AB Cyatta abscondita, a new genus and species of fungus-farming ant from Brazil, is described based on morphological study of more than 20 workers, two dealate gynes, one male, and two larvae. Ecological field data are summarized, including natural history, nest architecture, and foraging behavior. Phylogenetic analyses of DNA sequence data from four nuclear genes indicate that Cyatta abscondita is the distant sister taxon of the genus Kalathomyrmex, and that together they comprise the sister group of the remaining neoattine ants, an informal clade that includes the conspicuous and well-known leaf-cutter ants. Morphologically, Cyatta abscondita shares very few obvious character states with Kalathomyrmex. It does, however, possess a number of striking morphological features unique within the fungus-farming tribe Attini. It also shares morphological character states with taxa that span the ancestral node of the Attini. The morphology, behavior, and other biological characters of Cyatta abscondita are potentially informative about plesiomorphic character states within the fungus-farming ants and about the early evolution of ant agriculture. C1 [Sosa-Calvo, Jeffrey] Univ Maryland, Dept Entomol, Maryland Ctr Systemat Entomol, College Pk, MD 20742 USA. [Sosa-Calvo, Jeffrey; Schultz, Ted R.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Brandao, Carlos R. F.] Univ Sao Paulo, Museu Zool, Sao Paulo, Brazil. [Klingenberg, Christiana] Staatl Museum Nat Kunde, Abt Entomol, Karlsruhe, Germany. [Feitosa, Rodrigo M.] Univ Fed Parana, Dept Zool, BR-80060000 Curitiba, Parana, Brazil. [Rabeling, Christian] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. [Bacci, Mauricio, Jr.] Univ Estadual Paulista, Ctr Estudos Insetos Sociais, Sao Paulo, Brazil. [Lopes, Caue T.; Vasconcelos, Heraldo L.] Univ Fed Uberlandia, Inst Biol, BR-38400 Uberlandia, MG, Brazil. RP Sosa-Calvo, J (reprint author), Univ Maryland, Dept Entomol, Maryland Ctr Systemat Entomol, College Pk, MD 20742 USA. EM sossajef@si.edu; schultzt@si.edu RI Feitosa, Rodrigo/D-2171-2012; Museu de Zoologia da USP, MZ-USP/Q-2192-2016 OI Feitosa, Rodrigo/0000-0001-9042-0129; FU United States National Science Foundation [DEB 0949689]; Smithsonian Institution Scholarly Studies Program; Smithsonian National Museum of Natural History (NMNH) Small Grants Program; Harvard Society of Fellows; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) [2006/00185-7]; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) [476250/2008-0, 310826/2006-3]; Max and Vera Britton Environmental Science Award (Cosmos Club Foundation); Peter Buck Pre-doctoral Fellowship (NMNH-SI); FAPESP [2011/24160-1] FX The authors gratefully acknowledge their funding sources: TRS was supported by United States National Science Foundation grant DEB 0949689 and by the Smithsonian Institution Scholarly Studies Program. TRS and JSC were supported by the Smithsonian National Museum of Natural History (NMNH) Small Grants Program. CR was supported by the Harvard Society of Fellows. MB was supported by the Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) (2006/00185-7) and the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq)(476250/2008-0 and 310826/2006-3). JSC was supported by a Max and Vera Britton Environmental Science Award (Cosmos Club Foundation) and a Peter Buck Pre-doctoral Fellowship (NMNH-SI). RMF was supported by FAPESP (2011/24160-1). CRFB was supported by FAPESP and CNPq. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 122 TC 9 Z9 9 U1 2 U2 37 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 NOV 15 PY 2013 VL 8 IS 11 AR e80498 DI 10.1371/journal.pone.0080498 PG 20 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 255RX UT WOS:000327258600066 PM 24260403 ER PT J AU Sangil, C Martin-Garcia, L Clemente, S AF Sangil, Carlos Martin-Garcia, Laura Clemente, Sabrina TI Assessing the impact of fishing in shallow rocky reefs: A multivariate approach to ecosystem management SO MARINE POLLUTION BULLETIN LA English DT Article DE Diadema africana; Trophic cascades; Conservation status; Zoning impacts; Canary Islands; NE Atlantic Ocean ID DIADEMA AFF. ANTILLARUM; MARINE PROTECTED AREAS; SEA-URCHIN; TROPHIC CASCADES; CORAL-REEFS; CANARIAN ARCHIPELAGO; ASSEMBLAGES; ISLANDS; RESERVES; COMMUNITIES AB In this paper we develop a tool to assess the impact of fishing on ecosystem functioning in shallow rocky reefs. The relationships between biological parameters (fishes, sea urchins, seaweeds), and fishing activities (fish traps, boats, land-based fishing, spearfishing) were tested in La Palma island (Canary Islands). Data from fishing activities and biological parameters were analyzed using principal component analyses. We produced two models using the first component of these analyses. This component was interpreted as a new variable that described the fishing pressure and the conservation status at each studied site. Subsequently the scores on the first axis were mapped using universal kriging methods and the models obtained were extrapolated across the whole island to display the expected fishing pressure and conservation status more widely. The fishing pressure and conservation status models were spatially related; zones where fishing pressure was high coincided with zones in the unhealthiest ecological state. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Sangil, Carlos] Smithsonian Inst, Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Martin-Garcia, Laura; Clemente, Sabrina] Univ La Laguna, Dept Biol Anim, San Cristobal la Laguna 38206, Spain. RP Sangil, C (reprint author), Smithsonian Inst, Smithsonian Trop Res Inst, Panama City 084303092, Panama. EM casangil@ull.es; lmargar@ull.es; msclemen@ull.es RI Clemente, Sabrina/B-3855-2014; Clemente, Sabrina/C-6909-2013 OI Clemente, Sabrina/0000-0003-1930-2052 FU Reserva Mundial de la Biosfera La Palma; Fundacion Biodiversidad (from the Spanish Ministry of Agriculture, food and Environmental Affairs) FX This study was part of Marcopalma Project. Funding for this project was provided by Reserva Mundial de la Biosfera La Palma and Fundacion Biodiversidad (from the Spanish Ministry of Agriculture, food and Environmental Affairs). We are thankful to Manfredi di Lorenzo, Laura Concepcion and Raul Fernandez for their collaboration during the field work. Jose Carlos Hernandez comments have greatly inspired many parts of this study. NR 66 TC 5 Z9 5 U1 1 U2 23 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 NOV 15 PY 2013 VL 76 IS 1-2 BP 203 EP 213 DI 10.1016/j.marpolbul.2013.08.041 PG 11 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 266EI UT WOS:000328005800037 PM 24045124 ER PT J AU Hong, T AF Hong, Terry TI On Such a Full Sea SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD NOV 15 PY 2013 VL 138 IS 19 BP 84 EP 85 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 253PT UT WOS:000327102500114 ER PT J AU Ruiz-Lopez, F Wilkerson, RC Ponsonby, DJ Herrera, M Sallum, MAM Velez, ID Quinones, ML Flores-Mendoza, C Chadee, DD Alarcon, J Alarcon-Ormasa, J Linton, YM AF Ruiz-Lopez, Freddy Wilkerson, Richard C. Ponsonby, David J. Herrera, Manuela Mureb Sallum, Maria Anice Dario Velez, Ivan Quinones, Martha L. Flores-Mendoza, Carmen Chadee, Dave D. Alarcon, Joubert Alarcon-Ormasa, Joubert Linton, Yvonne-Marie TI Systematics of the Oswaldoi Complex (Anopheles, Nyssorhynchus) in South America SO PARASITES & VECTORS LA English DT Article DE Anopheles oswaldoi species complex; An. oswaldoi s. s.; An. oswaldoi A; An. oswaldoi B; An. sp nr. konderi; COI barcoding; ITS2 ID INTERNAL TRANSCRIBED SPACER; SENSU-LATO DIPTERA; MALARIA VECTOR; PLASMODIUM-VIVAX; RIBOSOMAL DNA; COMPARATIVE SUSCEPTIBILITY; AMAZON REGION; INTRAGENOMIC HETEROGENEITY; PHYLOGENETIC-RELATIONSHIPS; MOLECULAR DIFFERENTIATION AB Background: Effective malaria control relies on accurate identification of those Anopheles mosquitoes responsible for the transmission of Plasmodium parasites. Anopheles oswaldoi s.l. has been incriminated as a malaria vector in Colombia and some localities in Brazil, but not ubiquitously throughout its Neotropical range. This evidence together with variable morphological characters and genetic differences supports that An. oswaldoi s.l. compromises a species complex. The recent fully integrated redescription of An. oswaldoi s.s. provides a solid taxonomic foundation from which to molecularly determine other members of the complex. Methods: DNA sequences of the Second Internal Transcribed Spacer (ITS2 - rDNA) (n = 192) and the barcoding region of the Cytochrome Oxidase I gene (COI - mtDNA) (n = 110) were generated from 255 specimens of An. oswaldoi s.l. from 33 localities: Brazil (8 localities, including the lectotype series of An. oswaldoi), Ecuador (4), Colombia (17), Trinidad and Tobago (1), and Peru (3). COI sequences were analyzed employing the Kimura-two-parameter model (K2P), Bayesian analysis (MrBayes), Mixed Yule-Coalescent model (MYC, for delimitation of clusters) and TCS genealogies. Results: Separate and combined analysis of the COI and ITS2 data sets unequivocally supported four separate species: two previously determined (An. oswaldoi s.s. and An. oswaldoi B) and two newly designated species in the Oswaldoi Complex (An. oswaldoi A and An. sp. nr. konderi). The COI intra-and inter-specific genetic distances for the four taxa were non-overlapping, averaging 0.012 (0.007 to 0.020) and 0.052 (0.038 to 0.064), respectively. The concurring four clusters delineated by MrBayes and MYC, and four independent TCS networks, strongly confirmed their separate species status. In addition, An. konderi of Sallum should be regarded as unique with respect to the above. Despite initially being included as an outgroup taxon, this species falls well within the examined taxa, suggesting a combined analysis of these taxa would be most appropriate. Conclusions: Through novel data and retrospective comparison of available COI and ITS2 DNA sequences, evidence is shown to support the separate species status of An. oswaldoi s.s., An. oswaldoi A and An. oswaldoi B, and at least two species in the closely related An. konderi complex (An. sp. nr. konderi, An. konderi of Sallum). Although An. oswaldoi s.s. has never been implicated in malaria transmission, An. oswaldoi B is a confirmed vector and the new species An. oswaldoi A and An. sp. nr. konderi are circumstantially implicated, most likely acting as secondary vectors. C1 [Ruiz-Lopez, Freddy; Wilkerson, Richard C.] Museum Support Ctr, Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Suitland, MD 20746 USA. [Ruiz-Lopez, Freddy; Dario Velez, Ivan] Univ Antioquia, Fac Med, Programa Estudio & Control Enfermedades Trop, Medellin, Colombia. [Wilkerson, Richard C.; Linton, Yvonne-Marie] Museum Support Ctr, Smithsonian Inst, Walter Reed Biosyst Unit, Suitland, MD 20746 USA. [Ponsonby, David J.] Canterbury Christ Church Univ, Dept Geog & Life Sci, Kent, OH USA. [Herrera, Manuela; Quinones, Martha L.] Univ Nacl Colombia, Fac Med, Bogota, Colombia. [Mureb Sallum, Maria Anice] Univ Sao Paulo, Fac Saude Publ, Dept Epidemiol, BR-01255 Sao Paulo, Brazil. [Flores-Mendoza, Carmen] Naval Med Res Unit NAMRU 6, Lima, Peru. [Chadee, Dave D.] Univ W Indies, Fac Sci & Technol, Dept Life Sci, West Indies, Trinid & Tobago. [Alarcon, Joubert; Alarcon-Ormasa, Joubert] Minist Salud Publ, Serv Nacl Control Enfermedades Transmitidas Vecto, Guayaquil, Ecuador. [Linton, Yvonne-Marie] Walter Reed Army Inst Res, Silver Spring, MD 20910 USA. RP Ruiz-Lopez, F (reprint author), Museum Support Ctr, Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Suitland, MD 20746 USA. EM fredyruiz9@gmail.com RI Sallum, Maria/B-8537-2012 FU UNICEF/UNDP/World Bank/WHO Special Programme for Research and Training in Tropical Diseases (TDR) [A50252]; Canterbury Christ Church University; Friends of the Natural History Museum, London; Mosquito Barcoding Initiative; Barcode of Life (CBOL); Sloane Foundation; National Institute of Health (NIH), USA [2R01AI054139]; COLCIENCIAS [110134319196] FX This study formed part of the PhD study of FRL conducted at the Natural History Museum, London, and awarded from Canterbury Christ Church University, Canterbury, Kent, U. K. This investigation received financial support from the UNICEF/UNDP/World Bank/WHO Special Programme for Research and Training in Tropical Diseases (TDR) (grant A50252 to YML), Canterbury Christ Church University (studentship to FRL). Additional funding was obtained through the Friends of the Natural History Museum, London to further the activities of the Mosquito Barcoding Initiative (to YML); the Consortium for the Barcode of Life (CBOL) ( to YML and RCW) and the Sloane Foundation (to YML and RCW); the National Institute of Health (NIH), USA (grant 2R01AI054139 to Jan E. Conn) and COLCIENCIAS (grant 110134319196 to MLQ). We thank Dr. A. Papadopoulou for help with the MYC analysis and Dr. S. Mahamdallie for helpful suggestions and discussions during preparation of the manuscript. NR 62 TC 8 Z9 8 U1 0 U2 7 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1756-3305 J9 PARASITE VECTOR JI Parasites Vectors PD NOV 12 PY 2013 VL 6 AR 324 DI 10.1186/1756-3305-6-324 PG 13 WC Parasitology SC Parasitology GA 277PX UT WOS:000328832800001 PM 24499562 ER PT J AU Kammer, TW Sumrall, CD Zamora, S Ausich, WI Deline, B AF Kammer, Thomas W. Sumrall, Colin D. Zamora, Samuel Ausich, William I. Deline, Bradley TI Oral Region Homologies in Paleozoic Crinoids and Other Plesiomorphic Pentaradial Echinoderms SO PLOS ONE LA English DT Article ID CAMBRIAN KAILI BIOTA; PHYLOGENETIC IMPLICATIONS; BURGESS SHALE; PELMATOZOAN ECHINODERMS; GUIZHOU PROVINCE; ORDOVICIAN; EOCRINOIDS; EVOLUTION; ORIGIN; CHINA AB The phylogenetic relationships between major groups of plesiomorphic pentaradial echinoderms, the Paleozoic crinoids, blastozoans, and edrioasteroids, are poorly understood because of a lack of widely recognized homologies. Here, we present newly recognized oral region homologies, based on the Universal Elemental Homology model for skeletal plates, in a wide range of fossil taxa. The oral region of echinoderms is mainly composed of the axial, or ambulacral, skeleton, which apparently evolved more slowly than the extraxial skeleton that forms the majority of the body. Recent phylogenetic hypotheses have focused on characters of the extraxial skeleton, which may have evolved too rapidly to preserve obvious homologies across all these groups. The axial skeleton conserved homologous suites of characters shared between various edrioasteroids and specific blastozoans, and between other blastozoans and crinoids. Although individual plates can be inferred as homologous, no directly overlapping suites of characters are shared between edrioasteroids and crinoids. Six different systems of mouth (peristome) plate organization (Peristomial Border Systems) are defined. These include four different systems based on the arrangement of the interradially-positioned oral plates and their peristomial cover plates, where PBS A1 occurs only in plesiomorphic edrioasteroids, PBS A2 occurs in plesiomorphic edrioasteroids and blastozoans, and PBS A3 and PBS A4 occur in blastozoans and crinoids. The other two systems have radially-positioned uniserial oral frame plates in construction of the mouth frame. PBS B1 has both orals and uniserial oral frame plates and occurs in edrioasterid and possibly edrioblastoid edrioasteroids, whereas PBS B2 has exclusively uniserial oral frame plates and is found in isorophid edrioasteroids and imbricate and gogiid blastozoans. These different types of mouth frame construction offer potential synapomorphies to aid in parsimony-based phylogenetics for exploring branching order among stem groups on the echinoderm tree of life. C1 [Kammer, Thomas W.] W Virginia Univ, Dept Geol & Geog, Morgantown, WV 26506 USA. [Sumrall, Colin D.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN USA. [Zamora, Samuel] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Ausich, William I.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. [Deline, Bradley] Univ West Georgia, Dept Geosci, Carrollton, GA USA. RP Kammer, TW (reprint author), W Virginia Univ, Dept Geol & Geog, Morgantown, WV 26506 USA. EM tkammer@wvu.edu FU National Science Foundation [1036356, 1036260, 1036416]; Smithsonian Institution FX This publication has been supported by the National Science Foundation (www.nsf.gov) collaborative project Assembling the Echinoderm Tree of Life by grants 1036356 (West Virginia University), 1036260 (University of Tennessee), 1036416 (The Ohio State University), and Research Award Opportunity Supplements to National Science Foundation grants 1036416 and 1036356 (University of West Georgia). SZ was supported by the Springer Fund of the Smithsonian Institution. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 91 TC 9 Z9 9 U1 0 U2 1 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 NOV 11 PY 2013 VL 8 IS 11 AR e77989 DI 10.1371/journal.pone.0077989 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 255EG UT WOS:000327221600012 PM 24244284 ER PT J AU Ak, NF Brandt, WN Hall, PB Schneider, DP Anderson, SF Hamann, F Lundgren, BF Myers, AD Paris, I Petitjean, P Ross, NP Shen, Y York, D AF Ak, N. Filiz Brandt, W. N. Hall, P. B. Schneider, D. P. Anderson, S. F. Hamann, F. Lundgren, B. F. Myers, Adam D. Paris, I. Petitjean, P. Ross, Nicholas P. Shen, Yue York, Don TI BROAD ABSORPTION LINE VARIABILITY ON MULTI-YEAR TIMESCALES IN A LARGE QUASAR SAMPLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars: absorption lines ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; OSCILLATION SPECTROSCOPIC SURVEY; RADIO-LOUD QUASARS; BLACK-HOLE MASSES; 7TH DATA RELEASE; X-RAY-SPECTRA; STELLAR OBJECTS; EMISSION-LINE; SDSS-III AB We present a detailed investigation of the variability of 428 C IV and 235 Si IV broad absorption line (BAL) troughs identified in multi-epoch observations of 291 quasars by the Sloan Digital Sky Survey-I/II/III. These observations primarily sample rest-frame timescales of 1-3.7 yr over which significant rearrangement of the BAL wind is expected. We derive a number of observational results on, e. g., the frequency of BAL variability, the velocity range over which BAL variability occurs, the primary observed form of BAL-trough variability, the dependence of BAL variability upon timescale, the frequency of BAL strengthening versus weakening, correlations between BAL variability and BAL-trough profiles, relations between C IV and Si IV BAL variability, coordinated multi-trough variability, and BAL variations as a function of quasar properties. We assess implications of these observational results for quasar winds. Our results support models where most BAL absorption is formed within an order-of-magnitude of the wind-launching radius, although a significant minority of BAL troughs may arise on larger scales. We estimate an average lifetime for a BAL trough along our line-of-sight of a few thousand years. BAL disappearance and emergence events appear to be extremes of general BAL variability, rather than being qualitatively distinct phenomena. We derive the parameters of a random-walk model for BAL EW variability, finding that this model can acceptably describe some key aspects of EW variability. The coordinated trough variability of BAL quasars with multiple troughs suggests that changes in "shielding gas" may play a significant role in driving general BAL variability. C1 [Ak, N. Filiz; Brandt, W. N.; Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Ak, N. Filiz; Brandt, W. N.; Schneider, D. P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Ak, N. Filiz] Erciyes Univ, Dept Astron & Space Sci, Fac Sci, TR-38039 Kayseri, Turkey. [Hall, P. B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Anderson, S. F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Hamann, F.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Lundgren, B. F.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Paris, I.] Univ Chile, Dept Astron, Santiago, Chile. [Petitjean, P.] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France. [Ross, Nicholas P.] Lawrence Berkeley Natl Lab, Berkeley, CA 92420 USA. [Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shen, Yue] Carnegie Observ, Pasadena, CA 91101 USA. [York, Don] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [York, Don] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. RP Ak, NF (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM nfilizak@astro.psu.edu RI Brandt, William/N-2844-2015; Filiz Ak, Nurten/C-9686-2015 OI Brandt, William/0000-0002-0167-2453; Filiz Ak, Nurten/0000-0003-3016-5490 FU National Science Foundation [AST-1108604]; NSERC; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX We gratefully acknowledge financial support from National Science Foundation grant AST-1108604 (N.F.A., W.N.B., D. P. S.) and from NSERC ( P. B. H.). We thank K. Dawson, M. Eracleous, and D. Schlegel for helpful discussions. We also thank the anonymous referee for constructive feedback.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. NR 91 TC 30 Z9 30 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 NOV 10 PY 2013 VL 777 IS 2 AR 168 DI 10.1088/0004-637X/777/2/168 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800087 ER PT J AU Beaumont, CN Offner, SSR Shetty, R Glover, SCO Goodman, AA AF Beaumont, Christopher N. Offner, Stella S. R. Shetty, Rahul Glover, Simon C. O. Goodman, Alyssa A. TI QUANTIFYING OBSERVATIONAL PROJECTION EFFECTS USING MOLECULAR CLOUD SIMULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; radiative transfer; techniques: image processing; techniques: spectroscopic ID RADIATION MAGNETOHYDRODYNAMICS CODE; SELF-GRAVITATIONAL HYDRODYNAMICS; PRINCIPAL COMPONENT ANALYSIS; ADAPTIVE MESH REFINEMENT; 2 SPACE DIMENSIONS; STAR-FORMATION; INTERSTELLAR-MEDIUM; X-FACTOR; VELOCITY MODIFICATION; ASTROPHYSICAL FLOWS AB The physical properties of molecular clouds are often measured using spectral-line observations, which provide the only probes of the clouds' velocity structure. It is hard, though, to assess whether and to what extent intensity features in position-position-velocity (PPV) space correspond to "real" density structures in position-position-position (PPP) space. In this paper, we create synthetic molecular cloud spectral-line maps of simulated molecular clouds, and present a new technique for measuring the reality of individual PPV structures. Using a dendrogram algorithm, we identify hierarchical structures in both PPP and PPV space. Our procedure projects density structures identified in PPP space into corresponding intensity structures in PPV space and then measures the geometric overlap of the projected structures with structures identified from the synthetic observation. The fractional overlap between a PPP and PPV structure quantifies how well the synthetic observation recovers information about the three-dimensional structure. Applying this machinery to a set of synthetic observations of CO isotopes, we measure how well spectral-line measurements recover mass, size, velocity dispersion, and virial parameter for a simulated star-forming region. By disabling various steps of our analysis, we investigate how much opacity, chemistry, and gravity affect measurements of physical properties extracted from PPV cubes. For the simulations used here, which offer a decent, but not perfect, match to the properties of a star-forming region like Perseus, our results suggest that superposition induces a similar to 40% uncertainty in masses, sizes, and velocity dispersions derived from (CO)-C-13 (J = 1-0). As would be expected, superposition and confusion is worst in regions where the filling factor of emitting material is large. The virial parameter is most affected by superposition, such that estimates of the virial parameter derived from PPV and PPP information typically disagree by a factor of similar to 2. This uncertainty makes it particularly difficult to judge whether gravitational or kinetic energy dominate a given region, since the majority of virial parameter measurements fall within a factor of two of the equipartition level alpha similar to 2. C1 [Beaumont, Christopher N.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Beaumont, Christopher N.; Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Offner, Stella S. R.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Shetty, Rahul; Glover, Simon C. O.] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany. RP Beaumont, CN (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM beaumont@ifa.hawaii.edu RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 FU NASA [HF-51311.01, NAS 5-26555]; Space Telescope Science Institute; Deutsche Forschungsgemeinschaft (DFG) [SFB 881]; National Science Foundation [AST-0908159] FX We thank Jens Kauffmann, Lukas Konstandin, Ralf Klessen, Eve Ostriker, Erik Rosolowsky, and Mark Heyer (the referee), whose comments improved this manuscript. Support for this work was provided by NASA through Hubble Fellowship grant #HF-51311.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, INC., for NASA, under contract NAS 5-26555 (SSRO). RS and SG acknowledge financial support from the Deutsche Forschungsgemeinschaft (DFG) via SFB 881 "The Milky Way System" (sub-projects B1 and B2). This material is based in part upon work supported by the National Science Foundation under Grant Number AST-0908159. NR 61 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 NOV 10 PY 2013 VL 777 IS 2 AR 173 DI 10.1088/0004-637X/777/2/173 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800092 ER PT J AU Best, WMJ Liu, MC Magnier, EA Aller, KM Deacon, NR Dupuy, TJ Redstone, J Burgett, WS Chambers, KC Hodapp, KW Kaiser, N Kudritzki, RP Morgan, JS Price, PA Tonry, JL Wainscoat, RJ AF Best, William M. J. Liu, Michael C. Magnier, Eugene A. Aller, Kimberly M. Deacon, Niall R. Dupuy, Trent J. Redstone, Joshua Burgett, W. S. Chambers, K. C. Hodapp, K. W. Kaiser, N. Kudritzki, R-P. Morgan, J. S. Price, P. A. Tonry, J. L. Wainscoat, R. J. TI A SEARCH FOR L/T TRANSITION DWARFS WITH Pan-STARRS1 AND WISE: DISCOVERY OF SEVEN NEARBY OBJECTS INCLUDING TWO CANDIDATE SPECTROSCOPIC VARIABLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; brown dwarfs; stars: atmospheres; stars: individual (PSO J140.2308+45.6487, PSO J307.6784+07.8236); stars: variables: general ID DIGITAL SKY SURVEY; STAR ADAPTIVE OPTICS; INFRARED-SURVEY-EXPLORER; HUBBLE-SPACE-TELESCOPE; WIDE-FIELD CAMERA; METHANE T-DWARFS; SPECTRAL TYPE-L; BROWN DWARF; ULTRACOOL DWARFS; PHOTOMETRIC VARIABILITY AB We present initial results from a wide-field (30,000 deg(2)) search for L/T transition brown dwarfs within 25 pc using the Pan-STARRS1 and Wide-field Infrared Survey Explorer (WISE) surveys. Previous large-area searches have been incomplete for L/T transition dwarfs, because these objects are faint in optical bands and have near-infrared (near-IR) colors that are difficult to distinguish from background stars. To overcome these obstacles, we have cross-matched the Pan-STARRS1 (optical) and WISE (mid-IR) catalogs to produce a unique multi-wavelength database for finding ultracool dwarfs. As part of our initial discoveries, we have identified seven brown dwarfs in the L/T transition within 9-15 pc of the Sun. The L9.5 dwarf PSO J140.2308+45.6487 and the T1.5 dwarf PSO J307.6784+07.8263 (both independently discovered by Mace et al.) show possible spectroscopic variability at the Y and J bands. Two more objects in our sample show evidence of photometric J-band variability, and two others are candidate unresolved binaries based on their spectra. We expect our full search to yield a well-defined, volume-limited sample of L/T transition dwarfs that will include many new targets for study of this complex regime. PSO J307.6784+07.8263 in particular may be an excellent candidate for in-depth study of variability, given its brightness (J = 14.2 mag) and proximity (11 pc). C1 [Best, William M. J.; Liu, Michael C.; Magnier, Eugene A.; Aller, Kimberly M.; Burgett, W. S.; Chambers, K. C.; Hodapp, K. W.; Kaiser, N.; Kudritzki, R-P.; Morgan, J. S.; Tonry, J. L.; Wainscoat, R. J.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Deacon, Niall R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Redstone, Joshua] Facebook, New York, NY 10017 USA. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Best, WMJ (reprint author), Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. EM wbest@ifa.hawaii.edu OI Chambers, Kenneth /0000-0001-6965-7789 FU National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877]; University of Maryland; Eotvos Lorand University (ELTE); NSF [AST09-09222] FX We thank the referee for helpful comments that improved the quality of this paper. 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, the University of Durham, the University of Edinburgh, Queens University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network, Inc., 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). We thank the PS1 observing and processing staff for obtaining the PS1 data, and Bill Sweeney, Heather Flewelling, and Mark Huber for assistance with accessing PS1 images. The United Kingdom Infrared Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the U. K. This paper makes use of observations processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge. We thank Mike Irwin, Simon Hodgkin, and the team at CASU for making the reduced WFCAM data available promptly, and Watson Varricatt and the UKIRT staff for carrying out our observations. We also thank John Rayner and Alan Tokunaga for making engineering time available for IRTF observations, and Katelyn Allers, Michael Kotson, Brian Cabreira, Bill Golisch, Dave Griep, and Eric Volqardsen for assisting with these. This project makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of the 2MASS data products; the UKIDSS data products; the VISTA data products; NASA's Astrophysical Data System; the SIMBAD database operated at CDS, Strasbourg, France, the SpeX Prism Spectral Libraries, maintained by Adam Burgasser at http://pono.ucsd.edu/similar to adam/browndwarfs/spexprism, and the Database of Ultracool Parallaxes, maintained by Trent Dupuy at https://www.cfa.harvard.edu/similar to tdupuy/plx. WMJB is supported by NSF grant AST09-09222. Finally, the authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always held within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 97 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 NOV 10 PY 2013 VL 777 IS 2 AR 84 DI 10.1088/0004-637X/777/2/84 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800003 ER PT J AU Connolly, SD Peris, CS Vrtilek, SD AF Connolly, S. D. Peris, C. S. Vrtilek, S. D. TI VARIABILITY OF THE ACCRETION DISK OF V926 Sco INFERRED FROM TOMOGRAPHIC ANALYSIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: individual (V926 Sco); stars: neutron ID X-RAY BINARIES; XTE J1118+480; QUIESCENCE; SUPERHUMPS; DOPPLER AB We present phase-resolved spectroscopic observations of the low-mass X-ray binary V926 Sco (4U 1735-44), covering the orbital period of 0.23 days, obtained with the Walter Baade 6.5 m Magellan Telescope at the Las Campanas Observatory in 2010 June and 2011 June. We use H alpha radial velocities to derive a systemic velocity of -109 +/- 4 km s(-1). The FWHM of the lines observed in common with previous authors are significantly lower during our observations suggesting much reduced velocities in the system. The equivalent width of the Bowen fluorescence lines with respect to He II lambda 4686 are factors of two or more lower during our observations in comparison to those previously reported for the system, suggesting reduced irradiation of the secondary. Doppler and modulation tomography of H alpha and He II lambda 4686 show asymmetric emission that can be attributed to a bulge in the accretion disk, as inferred from He II observations by previous authors. The X-ray fluxes from the source at times concurrent with the optical observations are significantly lower during our observations than during optical observations taken in 2003. We suggest that the system is in a lower accretion state compared to earlier observations; this explains both the lower velocities observed from the disk and the reduction of emission due to Bowen fluorescence detected from the secondary. C1 [Connolly, S. D.] Univ Southampton, Southampton S017 1BJ, Hants, England. [Peris, C. S.] Northeastern Univ, Dept Phys, Boston, MA 02115 USA. [Peris, C. S.; Vrtilek, S. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Connolly, SD (reprint author), Univ Southampton, Southampton S017 1BJ, Hants, England. EM sdc1g08@soton.ac.u; peris.c@husky.neu.edu; svrtilek@cfa.harvard.edu FU Smithsonian Institution Endowment Grant FX We would like to thank the Las Campanas Observatory for the use of the Baade Telescope and the RXTE/ASM team for the 15 yr X-ray lightcurve of V926 Sco. We would like to thank our referee for helpful comments. We gratefully acknowledge the use of the MOLLY and DOPPLER software written by T. R. Marsh and the MODMAP software written by D. Steeghs. Funded in part by a Smithsonian Institution Endowment Grant to S.D.V. NR 20 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 NOV 10 PY 2013 VL 777 IS 2 AR 171 DI 10.1088/0004-637X/777/2/171 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800090 ER PT J AU Gelfand, JD Castro, D Slane, PO Temim, T Hughes, JP Rakowski, C AF Gelfand, Joseph D. Castro, Daniel Slane, Patrick O. Temim, Tea Hughes, John P. Rakowski, Cara TI SUPERNOVA REMNANT KES 17: AN EFFICIENT COSMIC RAY ACCELERATOR INSIDE A MOLECULAR CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; gamma rays: ISM; ISM: individual objects (Kes 17); ISM: supernova remnants; X-rays: individual (Kes 17) ID LARGE-AREA TELESCOPE; MAGNETIC-FIELD AMPLIFICATION; PARTICLE-ACCELERATION; INTERSTELLAR-MEDIUM; X-RAY; NONTHERMAL EMISSION; INFRARED SURVEY; GALACTIC PLANE; CASSIOPEIA-A; HIGH-ENERGY AB The supernova remnant Kes 17 (SNR G304.6+ 0.1) is one of a few but growing number of remnants detected across the electromagnetic spectrum. In this paper, we analyze recent radio, X-ray, and gamma-ray observations of this object, determining that efficient cosmic ray acceleration is required to explain its broadband non-thermal spectrum. These observations also suggest that Kes 17 is expanding inside a molecular cloud, though our determination of its age depends on whether thermal conduction or clump evaporation is primarily responsible for its center-filled thermal X-ray morphology. Evidence for efficient cosmic ray acceleration in Kes 17 supports recent theoretical work concluding that the strong magnetic field, turbulence, and clumpy nature of molecular clouds enhance cosmic ray production in supernova remnants. While additional observations are needed to confirm this interpretation, further study of Kes 17 is important for understanding how cosmic rays are accelerated in supernova remnants. C1 [Gelfand, Joseph D.] NYU Abu Dhabi, New York, NY 10276 USA. [Castro, Daniel] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Temim, Tea] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Rakowski, Cara] US Patent & Trademark Off, Alexandria, VA USA. RP Gelfand, JD (reprint author), NYU Abu Dhabi, POB 903, New York, NY 10276 USA. EM jg168@cosmo.nyu.edu; cara.rakowski@gmail.com RI Gelfand, Joseph/F-1110-2015; OI Gelfand, Joseph/0000-0003-4679-1058; Temim, Tea/0000-0001-7380-3144 FU NASA [NNX10AR51G, NAS8-03060]; NSF Astronomy and Astrophysics Postdoctoral Fellowship grant [AST-0702957]; Commonwealth of Australia FX The authors thank the anonymous referee for usual comments and suggestions. J.D.G. acknowledges the support of NASA grant NNX10AR51G, and NSF Astronomy and Astrophysics Postdoctoral Fellowship grant AST-0702957, as well as the hospitality of the Center for Cosmology and Particle Physics at New York University where much of this work was conducted. P.O.S. acknowledges support from NASA contract NAS8-03060. The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). NR 85 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 NOV 10 PY 2013 VL 777 IS 2 AR 148 DI 10.1088/0004-637X/777/2/148 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800067 ER PT J AU Hoq, S Jackson, JM Foster, JB Sanhueza, P Guzman, A Whitaker, JS Claysmith, C Rathborne, JM Vasyunina, T Vasyunin, A AF Hoq, Sadia Jackson, James M. Foster, Jonathan B. Sanhueza, Patricio Guzman, Andres Whitaker, J. Scott Claysmith, Christopher Rathborne, Jill M. Vasyunina, Tatiana Vasyunin, Anton TI CHEMICAL EVOLUTION IN HIGH-MASS STAR-FORMING REGIONS: RESULTS FROM THE MALT90 SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: clouds; ISM: molecules; stars: formation ID INFRARED DARK CLOUDS; INTERSTELLAR MOLECULAR CLOUDS; COLLAPSING PRESTELLAR CORES; PROTOSTELLAR CORES; ABUNDANCE RATIO; MILKY-WAY; GALACTIC PLANE; HNC; HCN; CHEMISTRY AB The chemical changes of high-mass star-forming regions provide a potential method for classifying their evolutionary stages and, ultimately, ages. In this study, we search for correlations between molecular abundances and the evolutionary stages of dense molecular clumps associated with high-mass star formation. We use the molecular line maps from Year 1 of the Millimetre Astronomy Legacy Team 90 GHz (MALT90) Survey. The survey mapped several hundred individual star-forming clumps chosen from the ATLASGAL survey to span the complete range of evolution, from prestellar to protostellar to Hii regions. The evolutionary stage of each clump is classified using the Spitzer GLIMPSE/MIPSGAL mid-IR surveys. Where possible, we determine the dust temperatures and H-2 column densities for each clump from Herschel/Hi-GAL continuum data. From MALT90 data, we measure the integrated intensities of the N2H+, HCO+, HCN and HNC (1-0) lines, and derive the column densities and abundances of N2H+ and HCO+. The Herschel dust temperatures increase as a function of the IR-based Spitzer evolutionary classification scheme, with the youngest clumps being the coldest, which gives confidence that this classification method provides a reliable way to assign evolutionary stages to clumps. Both N2H+ and HCO+ abundances increase as a function of evolutionary stage, whereas the N2H+ (1-0) to HCO+ (1-0) integrated intensity ratios show no discernable trend. The HCN (1-0) to HNC(1-0) integrated intensity ratios show marginal evidence of an increase as the clumps evolve. C1 [Hoq, Sadia; Jackson, James M.; Foster, Jonathan B.; Sanhueza, Patricio; Claysmith, Christopher] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Foster, Jonathan B.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA. [Guzman, Andres] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Whitaker, J. Scott] Boston Univ, Dept Phys, Boston, MA 02215 USA. [Rathborne, Jill M.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW, Australia. [Vasyunina, Tatiana; Vasyunin, Anton] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Vasyunin, Anton] Ural Fed Univ, Ekaterinburg 620075, Russia. RP Hoq, S (reprint author), Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. EM shoq@bu.edu; jackson@bu.edu; jonathan.b.foster@yale.edu; patricio@bu.edu; aguzmanf@cfa.harvard.edu; scott@bu.edu; claysmit@bu.edu; rathborne@csiro.au; tv3h@virginia.edu; aiv3f@virginia.edu RI Vasyunin, Anton/N-9112-2016; OI Vasyunin, Anton/0000-0003-1684-3355; Guzman, Andres/0000-0003-0990-8990 FU Common wealth of Australia; Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; NSF [AST 09-07790]; National Science Foundation (U.S.); NASA [NNX12AI55G, NNX10AD68G] FX The Mopra radio telescope is part of the Australia Telescope National Facility which is funded by the Common wealth of Australia for operation as a National Facility managed by CSIRO. The University of New SouthWales Digital Filter Bank used for the observations with the Mopra Telescope was provided with support from the Australian Research Council. 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. NASA's Astrophysics Data System was used to access the literature given in the references. S. H. gratefully acknowledges funding support from NSF grant No. AST 09-07790. J.M.J gratefully acknowledges funding support from NSF grant No. AST-0808001. T.V. and A.V. wish to thank the National Science Foundation (U.S.) for its funding of the astrochemistry program at the University of Virginia. A.E.G. acknowledges partial support from NASA grants NNX12AI55G and NNX10AD68G. We thank the anonymous referee for providing valuable comments and suggestions. NR 59 TC 31 Z9 31 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 NOV 10 PY 2013 VL 777 IS 2 AR 157 DI 10.1088/0004-637X/777/2/157 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800076 ER PT J AU Kipping, DM Forgan, D Hartman, J Nesvorny, D Bakos, GA Schmitt, A Buchhave, L AF Kipping, D. M. Forgan, D. Hartman, J. Nesvorny, D. Bakos, G. A. Schmitt, A. Buchhave, L. TI THE HUNT FOR EXOMOONS WITH KEPLER (HEK). III. THE FIRST SEARCH FOR AN EXOMOON AROUND A HABITABLE-ZONE PLANET SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (Kepler-22, KOI-87, KIC 10593626); techniques: photometric ID SUPER-EARTH; STAR; CANDIDATES; PHOTOMETRY; EXOPLANETS AB Kepler-22b is the first transiting planet to have been detected in the habitable zone of its host star. At 2.4 R., Kepler-22b is too large to be considered an Earth analog, but should the planet host a moon large enough to maintain an atmosphere, then the Kepler-22 system may yet possess a telluric world. Aside from being within the habitable zone, the target is attractive due to the availability of previously measured precise radial velocities and low intrinsic photometric noise, which has also enabled asteroseismology studies of the star. For these reasons, Kepler-22b was selected as a target-of-opportunity by the "Hunt for Exomoons with Kepler" (HEK) project. In this work, we conduct a photodynamical search for an exomoon around Kepler-22b leveraging the transits, radial velocities, and asteroseismology plus several new tools developed by the HEK project to improve exomoon searches. We find no evidence for an exomoon around the planet and exclude moons of mass M-S > 0.5 M-circle plus. to 95% confidence. By signal injection and blind retrieval, we demonstrate that an Earth-likemoon is easily detected for this planet even when the time-correlated noise of the data set is taken into account. We provide updated parameters for the planet Kepler-22b, including a revised mass of M-P < 53 M-circle plus to 95% confidence and an eccentricity of 0.13(-0.13)(+0.36) by exploiting Single-body Asterodensity Profiling. Finally, we show that Kepler-22b has a > 95% probability of being within the empirical habitable zone but a <5% probability of being within the conservative habitable zone. C1 [Kipping, D. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Forgan, D.] Univ Edinburgh, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Hartman, J.; Bakos, G. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 05844 USA. [Nesvorny, D.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Buchhave, L.] Univ Copenhagen, Niels Bohr Inst, DK-1168 Copenhagen, Denmark. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu OI Forgan, Duncan/0000-0003-1175-4388; Buchhave, Lars A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166 FU NASA [NNX12AH91H]; STFC [ST/J001422/1]; NSF [AST-1108686, AST-1008890] FX This work made use of the Michael Dodds Computing Facility. We thank the anonymous reviewer for their thoughtful comments, which improved the quality of our manuscript. D. M. K. is funded by the NASA Carl Sagan Fellowships. D. F. gratefully acknowledges support from STFC grant ST/J001422/1. J.H. and G. B. acknowledge partial support from NSF grant AST-1108686 and NASA grant NNX12AH91H. D.N. acknowledges support from NSF AST-1008890. NR 48 TC 25 Z9 26 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 NOV 10 PY 2013 VL 777 IS 2 AR 134 DI 10.1088/0004-637X/777/2/134 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800053 ER PT J AU Lopez, LA Pearson, S Ramirez-Ruiz, E Castro, D Yamaguchi, H Slane, PO Smith, RK AF Lopez, Laura A. Pearson, Sarah Ramirez-Ruiz, Enrico Castro, Daniel Yamaguchi, Hiroya Slane, Patrick O. Smith, Randall K. TI UNRAVELING THE ORIGIN OF OVERIONIZED PLASMA IN THE GALACTIC SUPERNOVA REMNANT W49B SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (W49B); ISM: supernova remnants; plasmas; X-rays: ISM ID FORMED DENSE SHELL; X-RAY-SPECTRUM; RECOMBINING PLASMA; THERMAL CONDUCTION; MODELING W44; HOT INTERIOR; EMISSION; MORPHOLOGY; EXPLOSION; ABSORPTION AB Recent observations have shown several supernova remnants (SNRs) have overionized plasmas, where ions are stripped of more electrons than they would be if in equilibrium with the electron temperature. Rapid electron cooling is necessary to produce this situation, yet the physical origin of that cooling remains uncertain. To assess the cooling scenario responsible for overionization, in this paper we identify and map the overionized plasma in the Galactic SNRW49B based on a 220 ks Chandra Advanced CCD Imaging Spectrometer observation. We performed a spatially resolved spectroscopic analysis, measuring the electron temperature by modeling the continuum and comparing it to the temperature given by the flux ratio of the He-like and H-like lines of sulfur and argon. Using these results, we find that W49B is overionized in the west, with a gradient of overionization increasing from east to west. As the ejecta expansion is impeded by molecular material in the east but not in the west, our overionization maps suggest the dominant cooling mechanism is adiabatic expansion of the hot plasma. C1 [Lopez, Laura A.; Castro, Daniel] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Pearson, Sarah] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Ramirez-Ruiz, Enrico] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95060 USA. [Yamaguchi, Hiroya; Slane, Patrick O.; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 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 FU National Aeronautics and Space Administration through Chandra Award Number [GO2-13003A]; Smithsonian Astrophysical Observatory [SV3-73016]; NASA [NAS8-03060, PF1-120085]; David and Lucile Packard Foundation; NSF [AST-0847563]; MIT Pappalardo Fellowship FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO2-13003A and through Smithsonian Astrophysical Observatory contract SV3-73016 to MIT issued by the Chandra X-ray Observatory Center, which is operated by the SAO for and on behalf of NASA under contract NAS8-03060. We acknowledge support from the David and Lucile Packard Foundation and NSF grant AST-0847563. Support for L. A. L. was provided by NASA through the Einstein Fellowship Program, grant PF1-120085, and the MIT Pappalardo Fellowship in Physics. NR 32 TC 9 Z9 9 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2013 VL 777 IS 2 AR 145 DI 10.1088/0004-637X/777/2/145 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800064 ER PT J AU Pichara, K Protopapas, P AF Pichara, Karim Protopapas, Pavlos TI AUTOMATIC CLASSIFICATION OF VARIABLE STARS IN CATALOGS WITH MISSING DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; stars: statistics; stars: variables: general ID LARGE-MAGELLANIC-CLOUD; TIME-SERIES; CANDIDATES; ALGORITHM; SELECTION AB We present an automatic classification method for astronomical catalogs with missing data. We use Bayesian networks and a probabilistic graphical model that allows us to perform inference to predict missing values given observed data and dependency relationships between variables. To learn a Bayesian network from incomplete data, we use an iterative algorithm that utilizes sampling methods and expectation maximization to estimate the distributions and probabilistic dependencies of variables from data with missing values. To test our model, we use three catalogs with missing data (SAGE, Two Micron All Sky Survey, and UBVI) and one complete catalog (MACHO). We examine how classification accuracy changes when information from missing data catalogs is included, how our method compares to traditional missing data approaches, and at what computational cost. Integrating these catalogs with missing data, we find that classification of variable objects improves by a few percent and by 15% for quasar detection while keeping the computational cost the same. C1 [Pichara, Karim] Pontificia Univ Catolica Chile, Dept Comp Sci, Santiago, Chile. [Pichara, Karim; Protopapas, Pavlos] Harvard Univ, Inst Appl Computat Sci, Cambridge, MA 02138 USA. [Pichara, Karim] Milky Way Millennium Nucleus, Santiago 7820436, Chile. [Protopapas, Pavlos] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pichara, K (reprint author), Pontificia Univ Catolica Chile, Dept Comp Sci, Alameda 340, Santiago, Chile. FU Vicerrectoria de Investigacion (VRI) from Pontificia Universidad Catolica de Chile; Institute of Applied Computer Science at Harvard University; Chilean Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cientifica Milenio [P07-021-F] FX This work is supported by Vicerrectoria de Investigacion (VRI) from Pontificia Universidad Catolica de Chile, Institute of Applied Computer Science at Harvard University, and the Chilean Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cientifica Milenio through grant P07-021-F, awarded to The Milky Way Millennium Nucleus. NR 31 TC 10 Z9 10 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2013 VL 777 IS 2 AR 83 DI 10.1088/0004-637X/777/2/83 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800002 ER PT J AU Sliwa, K Wilson, CD Krips, M Petitpas, GR Iono, D Juvela, M Matsushita, S Peck, A Yun, M AF Sliwa, Kazimierz Wilson, Christine D. Krips, Melanie Petitpas, Glen R. Iono, Daisuke Juvela, Mika Matsushita, Satoki Peck, Alison Yun, Min TI LUMINOUS INFRARED GALAXIES WITH THE SUBMILLIMETER ARRAY. IV. (CO)-C-12 J=6-5 OBSERVATIONS OF VV 114 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (VV114, IC 1623, Arp 236, IRAS 01053-1746); galaxies: interactions; galaxies: starburst; radiative transfer; submillimeter: galaxies ID HERSCHEL-SPIRE SPECTROSCOPY; MOLECULAR GAS; ARP 220; INTERSTELLAR-MEDIUM; STARBURST GALAXIES; NGC 6240; VV-114; CLOUDS; RATIO; M82 AB We present high-resolution (similar to 2.'' 5) observations of (CO)-C-12 J = 6-5 toward the luminous infrared galaxy VV 114 using the Submillimeter Array. We detect (CO)-C-12 J = 6-5 emission from the eastern nucleus of VV 114 but do not detect the western nucleus or the central region. We combine the new (CO)-C-12 J = 6-5 observations with previously published or archival low-J CO observations, which include (CO)-C-13 J = 1-0 Atacama Large Millimeter/submillimeter Array cycle 0 observations, to analyze the beam-averaged physical conditions of the molecular gas in the eastern nucleus. We use the radiative transfer code RADEX and a Bayesian likelihood code to constrain the temperature (T-kin), density (n(H2)), and column density (N-12CO) of the molecular gas. We find that the most probable scenario for the eastern nucleus is a cold (T-kin = 38 K), moderately dense (n(H2) = 10(2.89) cm(-3)) molecular gas component. We find that the most probable (CO)-C-12 to (CO)-C-13 abundance ratio ([(CO)-C-12]/[(CO)-C-13]) is 229, which is roughly three times higher than the Milky Way value. This high abundance ratio may explain the observed high (CO)-C-12/(CO)-C-13 line ratio (>25). The unusual (CO)-C-13 J = 2-1/J = 1-0 line ratio of 0.6 is produced by a combination of moderate (CO)-C-13 optical depths (tau = 0.4-1.1) and extremely subthermal excitation temperatures. We measure the CO-to-H-2 conversion factor, alpha(CO), to be 0.5(-0.3)(+0.6) M-circle dot (K km s(-1) pc(2))(-1), which agrees with the widely used factor for ultra luminous infrared galaxies of Downes & Solomon (alpha(CO) = 0.8 M-circle dot (K km s(-1) pc(2))(-1)). C1 [Sliwa, Kazimierz; Wilson, Christine D.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Krips, Melanie] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Petitpas, Glen R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Iono, Daisuke] Natl Astron Observ Japan, Chile Observ, Mitaka, Tokyo 1818588, Japan. [Juvela, Mika] Univ Helsinki, FI-00014 Helsinki, Finland. [Matsushita, Satoki] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Peck, Alison] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Yun, Min] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Sliwa, K (reprint author), McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. EM sliwak@mcmaster.ca; wilson@physics.mcmaster.ca; krips@iram.fr; gpetitpa@cfa.harvard.edu; d.iono@nao.ac.jp; mika.juvela@helsinki.fi; satoki@asiaa.sinica.edu.tw; apeck@alma.cl; myun@astro.umass.edu FU Smithsonian Institution; Academia Sinica; Natural Science and Engineering Research Council of Canada (NSERC); Queen Elizabeth II Graduate Scholarship in Science and Technology (QEIIGSST); Academy of Finland [250741] FX We thank the anonymous referee for useful comments that greatly improved our analysis. We also thank the Z-Spec team for allowing us to use their likelihood code. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the National Research Council of Canada, and (until 2013 March 31) the Netherlands Organisation for Scientific Research. This paper makes use of the following ALMA data: ADS/JAO. ALMA#2011.0.00467.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. C. D. W. acknowledges support by the Natural Science and Engineering Research Council of Canada (NSERC). K. S. acknowledges support by the Queen Elizabeth II Graduate Scholarship in Science and Technology (QEIIGSST). M.J. acknowledges the support of the Academy of Finland grant No. 250741. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. NR 38 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2013 VL 777 IS 2 AR 126 DI 10.1088/0004-637X/777/2/126 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800045 ER PT J AU Strelnitski, V Bieging, JH Hora, J Smith, HA Armstrong, P Lagergren, K Walker, G AF Strelnitski, Vladimir Bieging, John H. Hora, Joseph Smith, Howard A. Armstrong, Peter Lagergren, Krister Walker, Gary TI THE PARSEC-SCALE ENVIRONMENT AND THE EVOLUTIONARY STATUS OF MWC 349A SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: emission-line, Be; stars: evolution; stars: individual (MWC 349, MWC 349A); stars: winds, outflows ID RADIO RECOMBINATION LINE; YOUNG STELLAR OBJECTS; EXTENDED ENVELOPES; CO OBSERVATIONS; BIPOLAR NEBULA; MASSIVE STARS; RING NEBULAE; ARRAY CAMERA; CYGNUS OB2; MWC-349 AB We report on a study of the similar to 10' (similar to 5 pc in projection) environs of the peculiar, high-luminosity emission-line star MWC 349A in the IR, radio, and visible domains. Besides the recently discovered X-shaped, arcmin-scale IR nebula centered on MWC 349A ("X nebula"), with the kinematic age of similar to 10(4) yr, we identify several young objects pointing toward an ongoing process of active star formation in this region and estimate some physical parameters of the newly discovered objects. The radiation of the X nebula is due to a geometrically and optically thin dust front heated to T-d approximate to 60-70 K by the radiation of the central star. The bipolar dust front probably results from the interaction of a powerful stellar wind with the circumstellar disk. One of the related objects is an elongated, cold molecular cloud, similar to 1 pc in size, adjacent to MWC 349A in projection and having the same radial velocity (V-LSR approximate to +9 km s(-1)). The proximity of the molecular cloud may indicate that MWC 349A was born locally rather than being a runaway object ejected from the core of Cyg OB2 several Myr ago. If it is still associated with its natal cloud, MWC 349A may be a rare example of the observable pre-main-sequence stage of a similar to 30 M-circle dot star. If the association with the molecular cloud is an effect of projection, however, MWC 349A may already be an evolved star, even if it was born locally. We discuss future observations that may shed more light on the evolutionary status of this unique object. C1 [Strelnitski, Vladimir; Armstrong, Peter; Lagergren, Krister; Walker, Gary] Maria Mitchell Observ, Nantucket, MA 02554 USA. [Bieging, John H.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Hora, Joseph; Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lagergren, Krister] Univ Virginia, Charlottesville, VA 22904 USA. RP Strelnitski, V (reprint author), Maria Mitchell Observ, 4 Vestal St, Nantucket, MA 02554 USA. EM vladimir@mariamitchell.org; jbieging@as.arizona.edu; jhora@cfa.harvard.edu; hsmith@cfa.harvard.edu; PeterArmstrong@limpiaobservatory.com; kal7q@virginia.edu; bailyhill14@gmail.com OI Hora, Joseph/0000-0002-5599-4650 FU National Science Foundation [AST-1140030]; NASA [NNX10AD68G]; NSF REU [AST-0851892]; Nantucket Maria Mitchell Association FX The Heinrich Hertz Submillimeter Telescope is operated by the Arizona Radio Observatory, a part of Steward Observatory at the University of Arizona. J.H.B. acknowledges partial support from National Science Foundation grant AST-1140030 to the University of Arizona, H. A. S. partial support from NASA Grant NNX10AD68G, and K. L. support from the NSF REU grant AST-0851892 and from the Nantucket Maria Mitchell Association. We thank the Spitzer Cygnus-X team for their help in reducing the Spitzer data set. We also gratefully acknowledge careful reprocessing and recalibrations of the Herschel images by A. Guzman. A careful reading of the paper and valuable comments by the anonymous referee are greatly appreciated. NR 64 TC 3 Z9 3 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2013 VL 777 IS 2 AR 89 DI 10.1088/0004-637X/777/2/89 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800008 ER PT J AU Tan, XY Payne, MJ Lee, MH Ford, EB Howard, AW Johnson, JA Marcy, GW Wright, JT AF Tan, Xianyu Payne, Matthew J. Lee, Man Hoi Ford, Eric B. Howard, Andrew W. Johnson, John. A. Marcy, Geoff W. Wright, Jason T. TI CHARACTERIZING THE ORBITAL AND DYNAMICAL STATE OF THE HD 82943 PLANETARY SYSTEM WITH KECK RADIAL VELOCITY DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; planetary systems; stars: individual (HD 82943) ID MEAN-MOTION RESONANCE; EXTRA-SOLAR PLANETS; CHAIN MONTE-CARLO; GJ 876; SECULAR EVOLUTION; HOST STARS; 4TH PLANET; GJ-876; TIME; HD-82943 AB We present an updated analysis of radial velocity data of the HD 82943 planetary system based on 10 yr of measurements obtained with the Keck telescope. Previous studies have shown that the HD 82943 system has two planets that are likely in 2:1 mean-motion resonance (MMR), with orbital periods about 220 and 440 days. However, alternative fits that are qualitatively different have also been suggested, with two planets in a 1:1 resonance or three planets in a Laplace 4:2:1 resonance. Here we use chi(2) minimization combined with a parameter grid search to investigate the orbital parameters and dynamical states of the qualitatively different types of fits, and we compare the results to those obtained with the differential evolution Markov chain Monte Carlo method. Our results support the coplanar 2:1 MMR configuration for the HD 82943 system, and show no evidence for either the 1:1 or three-planet Laplace resonance fits. The inclination of the system with respect to the sky plane is well constrained at 20(-5.5)(+4.9) degrees, and the system contains two planets with masses of about 4.78 M-J and 4.80 M-J (where M-J is the mass of Jupiter) and orbital periods of about 219 and 442 days for the inner and outer planet, respectively. The best fit is dynamically stable with both eccentricity-type resonant angles theta 1 and theta 2 librating around theta degrees. C1 [Tan, Xianyu; Lee, Man Hoi] Univ Hong Kong, Dept Earth Sci, Hong Kong, Hong Kong, Peoples R China. [Tan, Xianyu] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Tan, Xianyu] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Payne, Matthew J.; Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Payne, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lee, Man Hoi] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Howard, Andrew W.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Johnson, John. A.] CALTECH, Dept Planetary Sci, Pasadena, CA 91125 USA. [Marcy, Geoff W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Wright, Jason T.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Wright, Jason T.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. RP Tan, XY (reprint author), Univ Hong Kong, Dept Earth Sci, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China. EM xianyut@lpl.arizona.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Wright, Jason/0000-0001-6160-5888 FU W. M. Keck Foundation; Hong Kong RGC grant [HKU 7034/09P]; NASA Origins of Solar Systems grant [NNX09AB35G]; David and Lucile Packard Foundation; Alfred P. Sloan Foundation; NSF Astronomy and Astrophysics grant [AST-1211441]; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium FX We thank NASA and NExScI for providing Keck time in the 2011A semester for the study of multiplanet systems (NExScI ID40/Keck ID#N141Hr). Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We thank Howard Isaacson, R. P. Butler, and S. Vogt for help with observing at the telescope, and the referee for helpful comments on the manuscript. X. T. and M. H. L. were supported in part by the Hong Kong RGC grant HKU 7034/09P. Contributions by M. J. P. and E. B. F. were supported by NASA Origins of Solar Systems grant NNX09AB35G prior to 2011 August 8. J. A. J. was supported by generous grants from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation. J. T. W. was supported by NSF Astronomy and Astrophysics grant AST-1211441. 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. M. H. L. and E. B. F. also acknowledge the hospitality of the Isaac Newton Institute for Mathematical Sciences, where part of this work was completed. NR 56 TC 19 Z9 19 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2013 VL 777 IS 2 AR 101 DI 10.1088/0004-637X/777/2/101 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800020 ER PT J AU Zhang, B Sun, M Ji, L Sarazin, C Lin, XB Nulsen, PEJ Roediger, E Donahue, M Forman, W Jones, C Voit, GM Kong, X AF Zhang, B. Sun, M. Ji, L. Sarazin, C. Lin, X. B. Nulsen, P. E. J. Roediger, E. Donahue, M. Forman, W. Jones, C. Voit, G. M. Kong, X. TI THE NARROW X-RAY TAIL AND DOUBLE H alpha TAILS OF ESO 137-002 IN A3627 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (A3627); galaxies: individual (ESO 137-002, ESO 137-001); X-rays: galaxies: clusters ID CLUSTER MAGNETIC-FIELDS; MASSIVE GALAXY CLUSTER; STAR-FORMATION; VIRGO CLUSTER; INTRACLUSTER MEDIUM; SPIRAL GALAXIES; COMA CLUSTER; HOT GAS; DISC GALAXIES; XMM-NEWTON AB We present the analysis of a deep Chandra observation of a similar to 2L(*) late-type galaxy, ESO 137-002, in the closest rich cluster A3627. The Chandra data reveal a long (greater than or similar to 40 kpc) and narrow tail with a nearly constant width (similar to 3 kpc) to the southeast of the galaxy, and a leading edge similar to 1.5 kpc from the galaxy center on the upstream side of the tail. The tail is most likely caused by the nearly edge-on stripping of ESO 137-002's interstellar medium (ISM) by ram pressure, compared to the nearly face-on stripping of ESO 137-001 discussed in our previous work. Spectral analysis of individual regions along the tail shows that the gas throughout it has a rather constant temperature, similar to 1 keV, very close to the temperature of the tails of ESO 137-001, if the same atomic database is used. The derived gas abundance is low (similar to 0.2 solar with the single-kT model), an indication of the multiphase nature of the gas in the tail. The mass of the X-ray tail is only a small fraction (<5%) of the initial ISM mass of the galaxy, suggesting that the stripping is most likely at an early stage. However, with any of the single-kT, double-kT, and multi-kT models we tried, the tail is always "over-pressured" relative to the surrounding intracluster medium (ICM), which could be due to the uncertainties in the abundance, thermal versus non-thermal X-ray emission, or magnetic support in the ICM. The H alpha data from the Southern Observatory for Astrophysical Research show a similar to 21 kpc tail spatially coincident with the X-ray tail, as well as a secondary tail (similar to 12 kpc long) to the east of the main tail diverging at an angle of similar to 23 degrees and starting at a distance of similar to 7.5 kpc from the nucleus. At the position of the secondary H alpha tail, the X-ray emission is also enhanced at the similar to 2 sigma level. We compare the tails of ESO 137-001 and ESO 137-002, and also compare the tails to simulations. Both the similarities and differences of the tails pose challenges to the simulations. Several implications are briefly discussed. C1 [Zhang, B.; Lin, X. B.; Kong, X.] Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Anhui, Peoples R China. [Zhang, B.; Lin, X. B.; Kong, X.] Chinese Acad Sci, USTC, Key Lab Res Galaxies & Cosmol, Beijing 100864, Peoples R China. [Sun, M.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Ji, L.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. [Sarazin, C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Nulsen, P. E. J.; Forman, W.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Roediger, E.] Univ Hamburg, Germany Hamburger Sternwarte, D-21029 Hamburg, Germany. [Donahue, M.; Voit, G. M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Zhang, B (reprint author), Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Anhui, Peoples R China. EM mingsun.cluster@gmail.com; xkong@ustc.edu.cn FU National Aeronautics and Space Administration (NASA); NASA [GO1-12103A, GO0-11145C, GO0-11008B]; Chinese Academy of Sciences (CAS); Key Laboratory of Dark Matter and Space Astronomy of CAS; National Natural Science Foundation of China (NSFC) [11225315]; Specialized Research Fund for the Doctoral Program of Higher Education (SRFDP) [20123402110037]; Chinese Universities Scientific Fund (CUSF) FX We thank Pavel Jachym for providing the unpublished results of the observations with APEX. We thank Q.D. Wang for stimulating discussions. We thank the referee for thorough and constructive comments, which were very helpful in improving the quality of this paper. The scientific results reported in this article are based on observations made by the Chandra X-Ray Observatory, ObsIDs 12950 and 9518. We also present data obtained with the Southern Observatory for Astrophysical Research (SOAR) telescope, which is a joint project of the Ministerio da Ciencia, Tecnologia, e Inovacao (MCTI) da Republica Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). We 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 (NASA). M. S. is supported by the NASA grants GO1-12103A, GO0-11145C, and GO0-11008B. L.J. is supported by the 100 Talents program of Chinese Academy of Sciences (CAS) and the Key Laboratory of Dark Matter and Space Astronomy of CAS. X. K. is supported by the National Natural Science Foundation of China (NSFC, No. 11225315), the Specialized Research Fund for the Doctoral Program of Higher Education (SRFDP, No. 20123402110037), and the Chinese Universities Scientific Fund (CUSF). NR 79 TC 10 Z9 10 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 NOV 10 PY 2013 VL 777 IS 2 AR 122 DI 10.1088/0004-637X/777/2/122 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800041 ER PT J AU Zhao, JH Morris, MR Goss, WM AF Zhao, Jun-Hui Morris, Mark R. Goss, W. M. TI RADIO DETECTION OF A CANDIDATE NEUTRON STAR ASSOCIATED WITH GALACTIC CENTER SUPERNOVA REMNANT SAGITTARIUS A EAST SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; ISM: individual objects (Sagittarius A); ISM: supernova remnants; radio continuum: ISM; stars: neutron; stars: winds, outflows ID RAY POINT SOURCES; BOW-SHOCK; MAGNETIC-FIELD; A-ASTERISK; SGR-A; CHANDRA; CATALOG; PULSARS; COMPLEX; NEBULAE AB We report the Very Large Array (VLA) detection of the radio counterpart of the X-ray object referred to as the "Cannonball," which has been proposed to be the remnant neutron star resulting from the creation of the Galactic center supernova remnant, Sagittarius A East. The radio object was detected both in our new VLA image from observations in 2012 at 5.5 GHz and in archivalVLA images from observations in 1987 at 4.75 GHz and in the period from 1990 to 2002 at 8.31 GHz. The radiomorphology of this object is characterized as a compact, partially resolved point source located at the northern tip of a radio "tongue" similar to the X-ray structure observed by Chandra. Behind the Cannonball, a radio counterpart to the X-ray plume is observed. This object consists of a broad radio plume with a size of 30 '' x15 '', followed by a linear tail having a length of 30 ''. The compact head and broad plume sources appear to have relatively flat spectra (alpha nu(alpha)) with mean values of alpha = -0.44 +/- 0.08 and -0.10 +/- 0.02, respectively, and the linear tail shows a steep spectrum with the mean value of -1.94 +/- 0.05. The total radio luminosity integrated from these components is similar to 8 x 10(33) erg s(-1), while the emission from the head and tongue amounts for only similar to 1.5 x 10(31) erg s(-1). Based on the images obtained from the two epochs' observations at 5 GHz, we infer the proper motion of the object: mu(delta) = 0.001 +/- 0.003 arcsec yr(-1) and mu(delta) = 0.013 +/- 0.003 arcsec yr(-1). With an implied velocity of 500 km s(-1), a plausible model can be constructed in which a runaway neutron star surrounded by a pulsar wind nebula was created in the event that produced Sgr A East. The inferred age of this object, assuming that its origin coincides with the center of Sgr A East, is approximately 9000 yr. C1 [Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morris, Mark R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Goss, W. M.] NRAO, Socorro, NM 87801 USA. RP Zhao, JH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM jzhao@cfa.harvard.edu; morris@astro.ucla.edu; mgoss@aoc.nrao.edu NR 41 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2013 VL 777 IS 2 AR 146 DI 10.1088/0004-637X/777/2/146 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242DY UT WOS:000326218800065 ER PT J AU Liu, MC Magnier, EA Deacon, NR Allers, KN Dupuy, TJ Kotson, MC Aller, KM Burgett, WS Chambers, KC Draper, PW Hodapp, KW Jedicke, R Kaiser, N Kudritzki, RP Metcalfe, N Morgan, JS Price, PA Tonry, JL Wainscoat, RJ AF Liu, Michael C. Magnier, Eugene A. Deacon, Niall R. Allers, Katelyn N. Dupuy, Trent J. Kotson, Michael C. Aller, Kimberly M. Burgett, W. S. Chambers, K. C. Draper, P. W. Hodapp, K. W. Jedicke, R. Kaiser, N. Kudritzki, R. -P. Metcalfe, N. Morgan, J. S. Price, P. A. Tonry, J. L. Wainscoat, R. J. TI THE EXTREMELY RED, YOUNG L DWARF PSO J318.5338-22.8603: A FREE-FLOATING PLANETARY-MASS ANALOG TO DIRECTLY IMAGED YOUNG GAS-GIANT PLANETS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE brown dwarfs; parallaxes; planets and satellites: atmospheres; proper motions; solar neighborhood; surveys ID NEAR-INFRARED SPECTRA; PROPER-MOTION SURVEY; HR 8799 PLANETS; FIELD L-DWARFS; BROWN DWARFS; T-DWARFS; ULTRACOOL DWARFS; MODEL ATMOSPHERES; MOVING GROUP; COOL NEIGHBORS AB We have discovered using Pan-STARRS1 an extremely red late-L dwarf, which has (J - K)(MKO) = 2.78 and (J - K) (2MASS) = 2.84, making it the reddest known field dwarf and second only to 2MASS J1207-39b among substellar companions. Near-IR spectroscopy shows a spectral type of L7 +/- 1 and reveals a triangular H-band continuum and weak alkali (K I and Na I) lines, hallmarks of low surface gravity. Near-IR astrometry from the Hawaii Infrared Parallax Program gives a distance of 24.6 +/- 1.4 pc and indicates a much fainter J-band absolute magnitude than field L dwarfs. The position and kinematics of PSO J318.5-22 point to membership in the beta Pic moving group. Evolutionary models give a temperature of 1160(-40)(+30) K and a mass of 6.5(-1.0)(+1.3) M-Jup, making PSO J318.5-22 one of the lowest mass free-floating objects in the solar neighborhood. This object adds to the growing list of low-gravity field L dwarfs and is the first to be strongly deficient in methane relative to its estimated temperature. Comparing their spectra suggests that young L dwarfs with similar ages and temperatures can have different spectral signatures of youth. For the two objects with well constrained ages (PSO J318.5-22 and 2MASS J0355+11), we find their temperatures are approximate to 400 K cooler than field objects of similar spectral type but their luminosities are similar, i.e., these young L dwarfs are very red and unusually cool but not "underluminous." Altogether, PSO J318.5-22 is the first free-floating object with the colors, magnitudes, spectrum, luminosity, and mass that overlap the young dusty planets around HR 8799 and 2MASS J1207-39. C1 [Liu, Michael C.; Magnier, Eugene A.; Kotson, Michael C.; Aller, Kimberly M.; Burgett, W. S.; Chambers, K. C.; Hodapp, K. W.; Jedicke, R.; Kaiser, N.; Kudritzki, R. -P.; Morgan, J. S.; Tonry, J. L.; Wainscoat, R. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Deacon, Niall R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Allers, Katelyn N.] Bucknell Univ, Dept Phys & Astron, Lewisburg, PA 17837 USA. [Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Draper, P. W.; Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Metcalfe, N.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Liu, MC (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. OI Chambers, Kenneth /0000-0001-6965-7789; Metcalfe, Nigel/0000-0001-9034-4402 FU NSF [AST09-09222]; AFRL [FA9451-06-2-0338]; [AST-0709460] FX The Pan-STARRS1 surveys have been made possible by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the institutions of the Pan-STARRS1 Science Consortium (http://www.ps1sc.org), NSF, and NASA. We thank Brendan Bowler for assistance with the figures and Michael Cushing for providing a pre-release update of SpeXtool. Our research has employed the WISE and 2MASS data products, NASA's Astrophysical Data System, and the Spex Prism Spectral Libraries maintained by Adam Burgasser. This research was supported by NSF grants AST09-09222 (awarded to M.C.L.) and AST-0709460 (awarded to E.A.M.) as well as AFRL Cooperative Agreement FA9451-06-2-0338. Finally, 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 56 TC 64 Z9 65 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 10 PY 2013 VL 777 IS 2 AR L20 DI 10.1088/2041-8205/777/2/L20 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242TY UT WOS:000326266500002 ER PT J AU Crabtree, KN Martinez, O McCarthy, MC AF Crabtree, Kyle N. Martinez, Oscar, Jr. McCarthy, Michael C. TI Detection of Two Highly Stable Silicon Nitrides: HSiNSi and H3SiNSi SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID CHEMICAL-VAPOR-DEPOSITION; MICROWAVE-SPECTRA; MATRIX-ISOLATION; AB-INITIO; AMMONIA; SIN; SPECTROSCOPY; MECHANISM; SILANE; DICHLOROSILANE AB The formation mechanisms of silicon nitride and silicon nitrogen hydrogen films, both produced by chemical vapor deposition (CVD) techniques and widely used in electronic device fabrication, are poorly understood. Identification of gas-phase intermediates formed from starting materials, typically silane, ammonia, and/or nitrogen, is a critical step in assessing the interplay between gas and surface processes in film formation. Two potential intermediates in this process, HSiNSi and H3SiNSi, have now been detected in a molecular beam by means of rotational spectroscopy. Both molecules were produced in electrical discharges of CVD-like gas mixtures and are the most readily observed silicon-nitrogen-containing molecules in the 6-20 GHz frequency range, though neither has been the subject of prior experimental or theoretical studies. HSiNSi and H3SiNSi are likely formed from reactions involving the silanitrile radical (SiN, isoelectronic to CN), implying that similar gas-phase reactions may be involved in film growth. C1 [Crabtree, Kyle N.; Martinez, Oscar, Jr.; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu OI Crabtree, Kyle/0000-0001-5629-5192; McCarthy, Michael/0000-0001-9142-0008 FU Smithsonian Astrophysical Observatory; NSF [CHE-1058063] FX We thank B. H. Pate and D. Plusquellic for invaluable assistance with CP-FTMW spectroscopy, E. S. Palmer for technical expertise, and C. A. Gottlieb for helpful discussions. The work is supported by NSF Grant No. CHE-1058063. K.N.C. has been supported by a CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory. NR 52 TC 8 Z9 8 U1 2 U2 21 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD NOV 7 PY 2013 VL 117 IS 44 BP 11282 EP 11288 DI 10.1021/jp4068119 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 250ID UT WOS:000326845300018 PM 24131302 ER PT J AU Crouch, T AF Crouch, Tom TI Harold Melvin Agnew (1921-2013) OBITUARY SO NATURE LA English DT Biographical-Item C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Crouch, T (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. EM croucht@si.edu NR 0 TC 0 Z9 0 U1 0 U2 3 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 NOV 7 PY 2013 VL 503 IS 7474 BP 40 EP 40 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 247AS UT WOS:000326585600024 PM 24201273 ER PT J AU Boudinot, BE Sumnicht, TP Adams, RMM AF Boudinot, Brendon E. Sumnicht, Theodore P. Adams, Rachelle M. M. TI Central American ants of the genus Megalomyrmex Forel (Hymenoptera: Formicidae): six new species and keys to workers and males SO ZOOTAXA LA English DT Article DE Attini; ergatoid; genitalia; Mesoamerica; Myrmicinae; revision; social parasite; taxonomy ID MALAGASY REGION HYMENOPTERA; FUNGUS-GROWING ANTS; MORPHOLOGY HYMENOPTERA; REVISION; SUBFAMILIES; GENERA; MYRMICINAE; PHYLOGENY; EVOLUTION; ISLAND AB Megalomyrmex Forel is a distinctive lineage of Neotropical ants, some of which are specialized parasites or predators of the fungus-growing ants Attini. Here we review and key the Central American fauna. Six new species are described from both female castes: M. brandaoi sp. n., M. fungiraptor sp. n., M. longinoi sp. n., M. milenae sp. n., M. megadrifti sp. n. and M. osadrifti sp. n. A worker-based key to all Central American species is presented, and all species are illustrated. Megalomyrmex drifti Kempf is redescribed and the first descriptions of queens for M. miri Brandao and M. foreli Emery are provided. New biological information, several new geographic records, and a discussion of the species-group schema of Brandao (1990) are presented. The male sex of Megalomyrmex is diagnosed at the genus-level and keyed to species for the Central American fauna, where known. The male of each species treated in the key is diagnosed, described, or redescribed. Males are known for fourteen out of twenty total Central American Megalomyrmex species. A distinct but unassociated male is described and keyed (M. male 01). The males of M. miri Brandao and M. wettereri Brandao are described for the first time, and the distinctness of these two species is confirmed. One potential synapomorphy of Megalomyrmex present in males and workers is the presence of a carina which posteriorly delimits the basalmost region of the petiolar dorsum. C1 [Boudinot, Brendon E.; Sumnicht, Theodore P.] Univ Utah, Salt Lake City, UT 84112 USA. [Adams, Rachelle M. M.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Adams, Rachelle M. M.] Univ Copenhagen, Dept Biol, Ctr Social Evolut, DK-2100 Copenhagen, Denmark. RP Boudinot, BE (reprint author), Univ Utah, 247 S 1400 E, Salt Lake City, UT 84112 USA. EM boudinotb@gmail.com; sumnichtt@gmail.com; rmmadams@gmail.com FU National Science Foundation [DEB-0072702, DEB-0640015/DEB-1157383, IOS-0843120]; National Geographic Society [7331-02, 7751-04]; Conservation International and a Marie Curie International Incoming Fellowship [237266 - ANCEPS (RMMA)]; MCZ (BEB) FX We would like to extend our deep gratitude to John T. Longino for his support and guidance, as well as for reviewing our manuscript. We thank Zachary E. Lieberman for reviewing several drafts of the manuscript. For inspiration to study males we thank Masashi Yoshimura, and we extend our gratitude to both Masashi Yoshimura and Francisco Hita Garcia; their work and advice has positively influenced the development of this manuscript. Thanks to Eugenia Okonskie for specimen loans from the USNM, and Phil Ward and Matt Prebus for specimen loans from the UC Davis and Prebus collections, respectively. We are grateful to Rodrigo M. Feitosa and an anonymous reviewer for comments and suggestions that helped improve this article. This work was supported by National Science Foundation grants DEB-0072702 (Project ALAS) and DEB-0640015/DEB-1157383 (Project LLAMA), IOS-0843120 (S. Yanoviak); National Geographic Society grants 7331-02 and 7751-04, and Conservation International and a Marie Curie International Incoming Fellowship 237266 - ANCEPS (RMMA); and finally an Ernst Mayr travel grant from the MCZ (BEB). We thank the staff and researchers at the Smithsonian Tropical Research Institute and La Selva Biological Station for help with logistics. NR 71 TC 11 Z9 11 U1 0 U2 7 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 NOV 4 PY 2013 VL 3732 IS 1 BP 1 EP 82 PG 82 WC Zoology SC Zoology GA 245WH UT WOS:000326494000001 PM 25277714 ER PT J AU Schreiber, JB Pekarik, AJ Hanemann, N Doering, Z Lee, AJ AF Schreiber, James B. Pekarik, Andrew J. Hanemann, Nadine Doering, Zahava Lee, Ah-Jin TI Understanding Visitor Engagement and Behaviors SO JOURNAL OF EDUCATIONAL RESEARCH LA English DT Article DE behavioral engagement; museums; visitors ID CONCEPTUAL CHANGE; KNOWLEDGE; MEMORY AB The authors examine a model of visitor engagement that has been in development over the past 3years at the Smithsonian Institution. A total of 390 visitors comprised the sample with a subsample (n = 102) of visitors who were tracked through an exhibit in the National Museum of Natural History. A 5-factor visitor preference model was tested (idea, people, object, physical, and reflective). A 4-factor model was retained, and factor scores were linked to tracking data. Results from the tracking model indicate that the preference scores are associated with and predictive of behavioral patterns within the exhibit. C1 [Schreiber, James B.] Duquesne Univ, Pittsburgh, PA 15228 USA. [Pekarik, Andrew J.; Hanemann, Nadine; Doering, Zahava; Lee, Ah-Jin] Smithsonian Inst, Off Policy & Anal, Washington, DC 20560 USA. RP Schreiber, JB (reprint author), Duquesne Univ, 600 Forbes Ave, Pittsburgh, PA 15228 USA. EM jb-schreiber@gmail.com OI Schreiber, James/0000-0001-9232-3410 NR 41 TC 2 Z9 2 U1 1 U2 17 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0022-0671 EI 1940-0675 J9 J EDUC RES JI J. Educ. Res. PD NOV 2 PY 2013 VL 106 IS 6 SI SI BP 462 EP 468 DI 10.1080/00220671.2013.833011 PG 7 WC Education & Educational Research SC Education & Educational Research GA 225QK UT WOS:000324977200005 ER PT J AU Letten, AD Lyons, SK Moles, AT AF Letten, Andrew D. Lyons, S. Kathleen Moles, Angela T. TI The mid-domain effect: it's not just about space SO JOURNAL OF BIOGEOGRAPHY LA English DT Editorial Material ID SPECIES RICHNESS; GRADIENTS; DIVERSITY; MODEL C1 [Letten, Andrew D.] Univ New S Wales, Sch Biol Earth & Environm Sci, Australian Wetlands Rivers & Landscapes Ctr, Sydney, NSW, Australia. [Lyons, S. Kathleen] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Moles, Angela T.] Univ New S Wales, Sch Biol Earth & Environm Sci, Evolut & Ecol Res Ctr, Sydney, NSW, Australia. RP Letten, AD (reprint author), Univ New S Wales, Sch Biol Earth & Environm Sci, Australian Wetlands Rivers & Landscapes Ctr, Sydney, NSW, Australia. EM a.letten@unsw.edu.au RI Moles, Angela/C-3083-2008; OI Moles, Angela/0000-0003-2041-7762; Letten, Andew/0000-0001-6436-7942 NR 13 TC 5 Z9 5 U1 1 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 EI 1365-2699 J9 J BIOGEOGR JI J. Biogeogr. PD NOV PY 2013 VL 40 IS 11 BP 2017 EP 2019 DI 10.1111/jbi.12196 PG 3 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA AN6MV UT WOS:000340709500002 ER PT J AU Parenti, LR Ebach, MC AF Parenti, Lynne R. Ebach, Malte C. TI The explanatory power of biogeographical patterns: a reply to de Bruyn et al. SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Biogeography; cladistics; dispersal; diversification; general area cladograms; historical biogeography; molecular clock; Pandora; philosophy of science; vicariance ID CRITIQUE; ISLANDS AB Confusion between evidence and hypothesis in biogeographical studies was the focus of our recent Guest Editorial (Parenti & Ebach, 2013, Journal of Biogeography, 40, 813-820). That editorial was critiqued by de Bruyn et al. (2013, Journal of Biogeography, doi: 10.1111/jbi.12166) to whom we reply briefly here. Despite our shared goals - to understand what lives where and why - we argue from different philosophical premises. Although we may have little common ground, such debate encourages the good health of the field of biogeography. C1 [Parenti, Lynne R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Ebach, Malte C.] Univ New S Wales, Sch Biol Earth & Environm Sci, Sydney, NSW 2052, Australia. RP Parenti, LR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012,MRC 159, Washington, DC 20013 USA. EM parentil@si.edu OI Ebach, Malte/0000-0002-9594-9010 NR 23 TC 0 Z9 0 U1 3 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 EI 1365-2699 J9 J BIOGEOGR JI J. Biogeogr. PD NOV PY 2013 VL 40 IS 11 BP 2206 EP 2208 DI 10.1111/jbi.12205 PG 3 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA AN6MV UT WOS:000340709500004 ER PT J AU Vajda, V Lyson, TR Bercovici, A Doman, JH Pearson, DA AF Vajda, Vivi Lyson, Tyler R. Bercovici, Antoine Doman, Jessamy H. Pearson, Dean A. TI A snapshot into the terrestrial ecosystem of an exceptionally well-preserved dinosaur (Hadrosauridae) from the Upper Cretaceous of North Dakota, USA SO CRETACEOUS RESEARCH LA English DT Article DE Hell Creek; Maastrichtian; Paleoclimate; Palynology; Hadrosaur; Dinosaur; Swamp ID HELL CREEK FORMATION; HORSESHOE CANYON FORMATION; PALEOGENE BOUNDARY; TERTIARY BOUNDARY; PALEOECOLOGICAL IMPLICATIONS; SOUTHERN ALBERTA; SOFT-TISSUE; SEED FERNS; STRATIGRAPHY; AMERICA AB A palynological investigation of sedimentary rocks enclosing an exceptionally well-preserved fossil dinosaur (Hadrosauridae) discovered in the upper part of the Hell Creek Formation in south western North Dakota was conducted in order to document the immediate paleoenvironment of this dinosaur. The specimen, an Edmontosaurus annectens is remarkable in having exceptional three-dimensional preservation of soft tissue around the skeleton, indicating rapid burial. A well-preserved palynological assemblage dominated by fern and bryophyte spores, with lesser gymnosperm and angiosperm pollen was recovered. Sparse fresh-water algae and marine dinoflagellate cysts were also recorded. The palynofacies is dominated by wood fragments, including charcoal, with little amorphous organic matter. The presence of some typical pollen taxa of the Wodehouseia spinata Assemblage Zone including Striatellipollis striatellus, Tricolpites microreticulatus, Leptopecopites pocockii as well as a diverse suite of Aquilapollenites, is fully consistent with a Late Cretaceous (late Maastrichtian) age. The palynoflora indicates a local vegetation composed of a canopy of conifers dominated by Pinaceae and a minor sub-canopy of Taxodium and cycads, as well as an understory of hydrophilous ferns, mosses and herbaceous angiosperms, indicative of a warm and humid climate - an environment where this specific hadrosaur roamed over 66 million years ago. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Vajda, Vivi; Bercovici, Antoine] Lund Univ, Dept Geol, SE-22362 Lund, Sweden. [Lyson, Tyler R.] Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20013 USA. [Lyson, Tyler R.] Marmarth Res Fdn, Marmarth, ND 58643 USA. [Doman, Jessamy H.] Yale Univ, Dept Anthropol, New Haven, CT 06511 USA. [Pearson, Dean A.] Pioneer Trails Reg Museum, Dept Paleontol, Bowman, ND 58623 USA. RP Vajda, V (reprint author), Lund Univ, Dept Geol, Solvegatan 12, SE-22362 Lund, Sweden. EM vivi.vajda@geol.lu.se OI Vajda, Vivi/0000-0003-2987-5559 FU Knut and Alice Wallenberg Foundation; Swedish Research Council; Smithsonian Institution Peter Buck Postdoctoral Fellowship; Swedish Research Council (VR) [2011-7176] FX We thank landowners M. and J. Sonsalla for donating the material to the Marmarth Research Foundation. This material is based on work supported by the Royal Swedish Academy of Sciences Research Fellow funded through the Knut and Alice Wallenberg Foundation (to V.Vajda), the Swedish Research Council through Linnaeus grant (LUCCI) to V. Vajda and A. Bercovici. T.R. Lyson was supported by a Smithsonian Institution Peter Buck Postdoctoral Fellowship. A. Bercovici is supported through the Swedish Research Council (VR) postdoctoral fellowship grant 2011-7176. Two anonymous reviewers are thanked for constructive criticism that greatlyimproved this paper. Russ Harms, Global Geolab Ltd. is thanked for palynological processing. NR 88 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 0195-6671 EI 1095-998X J9 CRETACEOUS RES JI Cretac. Res. PD NOV PY 2013 VL 46 BP 114 EP 122 DI 10.1016/j.cretres.2013.08.010 PG 9 WC Geology; Paleontology SC Geology; Paleontology GA 287PE UT WOS:000329553900011 ER PT J AU Touwaide, A AF Touwaide, Alain TI Epidemiology and treatment of kidney conditions in antiquity SO JOURNAL OF NEPHROLOGY LA English DT Article C1 [Touwaide, Alain] Inst Preservat Med Tradit, Washington, DC 20044 USA. [Touwaide, Alain] Smithsonian Inst, Nat Hist Museum, Washington, DC 20560 USA. RP Touwaide, A (reprint author), Inst Preservat Med Tradit, POB 7606, Washington, DC 20044 USA. EM research@medicaltraditions.org FU Institute for the Preservation of Medical Traditions in Washington, DC-USA FX Financial support for this research was provided by the Institute for the Preservation of Medical Traditions in Washington, DC-USA, which also provided access to documentary resources. NR 15 TC 1 Z9 1 U1 0 U2 0 PU WICHTIG EDITORE PI MILAN PA 72/74 VIA FRIULI, 20135 MILAN, ITALY SN 1121-8428 EI 1724-6059 J9 J NEPHROL JI J. Nephrol. PD NOV-DEC PY 2013 VL 26 SU 22 BP S175 EP S179 DI 10.5301/jn.5000380 PG 5 WC Urology & Nephrology SC Urology & Nephrology GA 290NP UT WOS:000329765900033 ER PT J AU Alcolea, J Bujarrabal, V Planesas, P Teyssier, D Cernicharo, J De Beck, E Decin, L Dominik, C Justtanont, K de Koter, A Marston, AP Melnick, G Menten, KM Neufeld, DA Olofsson, H Schmidt, M Schoier, FL Szczerba, R Waters, LBFM AF Alcolea, J. Bujarrabal, V. Planesas, P. Teyssier, D. Cernicharo, J. De Beck, E. Decin, L. Dominik, C. Justtanont, K. de Koter, A. Marston, A. P. Melnick, G. Menten, K. M. Neufeld, D. A. Olofsson, H. Schmidt, M. Schoeier, F. L. Szczerba, R. Waters, L. B. F. M. TI HIFISTARS Herschel/HIFI observations of VY Canis Majoris Molecular-line inventory of the envelope around the largest known star SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; stars: mass-loss; stars: individual: VY Canis Majoris; circumstellar matter ID SIO MASER EMISSION; RED SUPERGIANT STARS; RICH EVOLVED STARS; OXYGEN-RICH; YELLOW HYPERGIANTS; LOSS HISTORY; CO EMISSION; 215-285 GHZ; CMA; SUBMILLIMETER AB Aims. The study of the molecular gas in the circumstellar envelopes of evolved stars is normally undertaken by observing lines of CO (and other species) in the millimetre-wave domain. In general, the excitation requirements of the observed lines are low at these wavelengths, and therefore these observations predominantly probe the cold outer envelope while studying the warm inner regions of the envelopes normally requires sub-millimetre (sub-mm) and far-infrared (FIR) observational data. Methods. To gain insight into the physical conditions and kinematics of the warm (100-1000 K) gas around the red hyper-giant VY CMa, we performed sensitive high spectral resolution observations of molecular lines in the sub-mm/FIR using the HIFI instrument of the Herschel Space Observatory. We observed CO, H2O, and other molecular species, sampling excitation energies from a few tens to a few thousand K. These observations are part of the Herschel guaranteed time key program HIFISTARS. Results. We detected the J = 6-5, J = 10-9, and J = 16-15 lines of (CO)-C-12 and (CO)-C-13 at similar to 100, 300, and 750K above the ground state (and the (CO)-C-13 J = 9-8 line). These lines are crucial for improving the modelling of the internal layers of the envelope around VY CMa. We also detected 27 lines of H2O and its isotopomers, and 96 lines of species such as NH 3, SiO, SO, SO2 HCN, OH and others, some of them originating from vibrationally excited levels. Three lines were not unambiguously assigned. Conclusions. Our observations confirm that VY CMa's envelope must consist of two or more detached components. The molecular excitation in the outer layers is significantly lower than in the inner ones, resulting in strong self-absorbed profiles in molecular lines that are optically thick in this outer envelope, for instance, low-lying lines of H2O. Except for the most abundant species, CO and H2O, most of the molecular emission detected at these sub-mm/FIR wavelengths arise from the central parts of the envelope. The spectrum of VY CMa is very prominent in vibrationally excited lines, which are caused by the strong IR pumping present in the central regions. Compared with envelopes of other massive evolved stars, VY CMa's emission is particularly strong in these vibrationally excited lines, as well as in the emission from less abundant species such as (HCN)-C-13, SO, and NH3. C1 [Alcolea, J.; Planesas, P.] Observatorio Astron Nacl IGN, Madrid 28014, Spain. [Bujarrabal, V.] Observatorio Astron Nacl IGN, Alcala De Henares 28803, Spain. [Teyssier, D.; Marston, A. P.] European Space Astron Ctr, Madrid 28080, Spain. [Cernicharo, J.] INTA CSIC, CAB, Torrejon De Ardoz 28850, Spain. [De Beck, E.; Decin, L.; de Koter, A.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [De Beck, E.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Decin, L.; Dominik, C.; de Koter, A.; Waters, L. B. F. M.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [Justtanont, K.; Olofsson, H.; Schoeier, F. L.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Schmidt, M.; Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Waters, L. B. F. M.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. RP Alcolea, J (reprint author), Observatorio Astron Nacl IGN, Madrid 28014, Spain. EM j.alcolea@oan.es RI Planesas, Pere/G-7950-2015; OI Planesas, Pere/0000-0002-7808-3040; /0000-0003-1689-9201 FU Spanish MICINN, program CONSOLIDER INGENIO, grant "ASTROMOL" [CSD2009-00038]; German Deutsche Forschungsgemeinschaft, DFG [Os 177/1-1]; National Science Center [N203 581040]; Swedish National Space Board; Spanish MICINN [AYA2009-07304] FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States under the leadership of SRON (Netherlands Institute for Space Research), Groningen, The Netherlands, and with major contributions from Germany, France, and the 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; The Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronmico Nacional (IGN), Centro de Astrobiologa (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, J.P.L., NHSC. HIFISTARS: The physical and chemical properties of circumstellar environments around evolved stars, P. I. V. Bujarrabal, is a Herschel/HIFI guaranteed time key program (KPGT_vbujarra_1) devoted to the study of the warm gas and water vapour contents of the molecular envelopes around evolved stars: AGB stars, red super-and hyper-giants; and their descendants: pre-planetary nebulae, planetary nebulae, and yellow hyper-giants. HIFISTARS comprises 366 observations, totalling 11 186 min of Herschel/HIFI telescope time. See http://hifistars.oan.es; and Key_Programmes. shtml and UserProvidedDataProducts. shtml in the Herschel web portal (http: //herschel.esac.esa.int/) for additional details. This work has been partially supported by the Spanish MICINN, program CONSOLIDER INGENIO 2010, grant "ASTROMOL" (CSD2009-00038); and by the German Deutsche Forschungsgemeinschaft, DFG project number Os 177/1-1. A portion of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. R.S.z. and M.S.ch. acknowledge support from grant N203 581040 of National Science Center. K.J., ES., and H.O. acknowledge funding from the Swedish National Space Board. J.C. thanks for funding from the Spanish MICINN, grant AYA2009-07304. NR 46 TC 8 Z9 8 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 NOV PY 2013 VL 559 AR A93 DI 10.1051/0004-6361/201321683 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263ZR UT WOS:000327847200093 ER PT J AU Goldman, B Roser, S Schilbach, E Magnier, EA Olczak, C Henning, T Juric, M Schlafly, E Chen, WP Platais, I Burgett, W Hodapp, K Heasley, J Kudritzki, RP Morgan, JS Price, PA Tonry, JL Wainscoat, R AF Goldman, B. Roeser, S. Schilbach, E. Magnier, E. A. Olczak, C. Henning, T. Juric, M. Schlafly, E. Chen, W. P. Platais, I. Burgett, W. Hodapp, K. Heasley, J. Kudritzki, R. P. Morgan, J. S. Price, P. A. Tonry, J. L. Wainscoat, R. TI Towards a complete stellar mass function of the Hyades I. Pan-STARRS1 optical observations of the low-mass stellar content SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE open clusters and associations: individual: Hyades; stars: luminosity function, mass function; stars: low-mass; stars: individual: 2MASSI J0230155+270406; stars: individual: 2MASS J05233822-1403022 ID DIGITAL SKY SURVEY; COLOR-MAGNITUDE DIAGRAMS; ULTRACOOL DWARFS; PROPER MOTIONS; BROWN DWARFS; COOL NEIGHBORS; PHOTOMETRIC CALIBRATION; LUMINOSITY FUNCTION; HIPPARCOS CATALOG; MAIN-SEQUENCE AB Aims. The Hyades cluster is an ideal target to study the dynamical evolution of a star cluster over the entire mass range due to its intermediate age and proximity to the Sun. Methods. We wanted to extend the Hyades mass function towards lower masses down to 0.1 M-circle dot and to use the full three-dimensional spatial information to characterize the dynamical evolution of the cluster. Results. We performed a kinematic and photometric selection using the PPMXL and Pan-STARRS 1 sky surveys, to search for cluster members up to 30 pc from the cluster centre. We determined our detection efficiency and field star contamination rate to derive the cluster luminosity and mass functions down to masses of 0.1 M-circle dot. The thorough astrometric and photometric constraints minimized the contamination. A minimum spanning tree algorithm was used to quantify the mass segregation. Conclusions. We discovered 43 new Hyades member candidates with velocity perpendicular to the Hyades motion up to 2 km s(-1). They have mass estimates between 0.43 and 0.09 M-circle dot, for a total mass of 10 M-circle dot. This doubles the number of Hyades candidates with masses smaller than 0.15 M-circle dot. We provide an additional list of 11 possible candidates with velocity perpendicular to the Hyades motion up to 4 km s(-1). The cluster is significantly mass segregated. The extension of the mass function towards lower masses provided an even clearer signature than estimated in the past. We also identified as likely Hyades member an L0 dwarf previously assumed to be a field dwarf. Finally we question the membership of a number of previously published candidates, including a L2.5-type dwarf. C1 [Goldman, B.; Olczak, C.; Henning, T.; Schlafly, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Roeser, S.; Schilbach, E.; Olczak, C.] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany. [Magnier, E. A.; Burgett, W.; Hodapp, K.; Heasley, J.; Kudritzki, R. P.; Morgan, J. S.; Tonry, J. L.; Wainscoat, R.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Olczak, C.] Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China. [Juric, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chen, W. P.] Natl Cent Univ, Grad Inst Astron, Jhongli 32054, Taiwan. [Platais, I.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Goldman, B (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM goldman@mpia.de OI Schlafly, Edward Ford/0000-0002-3569-7421 FU German Research Foundation (DFG) [Sonderforschungsbereich SFB 881, OL 350/1-1]; NAOC CAS; Global Networks and Mobility Program of the University of Heidelberg [ZUK 49/1 TP14.8 Spurzem]; NASA [HF-51255.01-A, NAS 5-26555]; Space Telescope Science Institute; National Aeronautics and Space Administration [NNX08AR22G]; Planetary Science Division of the NASA Science Mission Directorate; National Science Foundation [AST-1238877]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; National Aeronautics and Space Administration; Max-Planck Institute for Astronomy, Heidelberg; Max Planck Institute for Extraterrestrial Physics, Garching; Johns Hopkins University; Durham University; University of Edinburgh; Queen's University Belfast; Harvard-Smithsonian Center for Astrophysics; Las Cumbres Observatory Global Telescope Network Incorporated; National Central University of Taiwan FX We thank Steve Boudreault, Andreas Ernst and France Allard for providing material from their publications, as well as Mario Gennaro and Josh Schlieder for their comments. This work was supported by Sonderforschungsbereich SFB 881 "The Milky Way System" (subproject B6) of the German Research Foundation (DFG). C.O. appreciates funding by the German Research Foundation (DFG) grant OL 350/1-1, support by NAOC CAS through the Silk Road Project, and by Global Networks and Mobility Program of the University of Heidelberg (ZUK 49/1 TP14.8 Spurzem). M.J. acknowledges support by NASA through Hubble Fellowship grant #HF-51255.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. The 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. 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/. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France; and of the Washington Double Star Catalog maintained at the US Naval Observatory. NR 76 TC 7 Z9 7 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2013 VL 559 AR A43 DI 10.1051/0004-6361/201321727 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263ZR UT WOS:000327847200043 ER PT J AU Lombardi, M Lada, CJ Alves, J AF Lombardi, Marco Lada, Charles J. Alves, Joao TI Fitting density models to observational data The local Schmidt law in molecular clouds SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; dust, extinction; stars: formation; ISM: structure; ISM: individual objects: Orion molecular complex; methods: statistical ID YOUNG STELLAR OBJECTS; STAR-FORMATION; GALAXIES; ORION; GAS; CENSUS; I. AB We consider the general problem of fitting a parametric density model to discrete observations, taken to follow a non-homogeneous Poisson point process. This class of models is very common, and can be used to describe many astrophysical processes, including the distribution of protostars in molecular clouds. We give the expression for the likelihood of a given spatial density distribution of protostars and apply it to infer the most probable dependence of the protostellar surface density on the gas surface density. Finally, we apply this general technique to model the distribution of protostars in the Orion molecular cloud and robustly derive the local star formation scaling (Schmidt) law for a molecular cloud. We find that in this cloud the protostellar surface density, Sigma(YSO), is directly proportional to the square gas column density, here expressed as infrared extinction in the K-band, A(K): more precisely, Sigma(YSO) = (1.65 +/- 0.19) (A(K)/mag)(2.03 +/- 0.15) stars pc(-2). C1 [Lombardi, Marco] Univ Milan, Dept Phys, I-20133 Milan, Italy. [Lada, Charles J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Alves, Joao] Univ Vienna, A-1180 Vienna, Austria. RP Lombardi, M (reprint author), Univ Milan, Dept Phys, Via Celoria 16, I-20133 Milan, Italy. EM marco.lombardi@unimi.it OI LOMBARDI, MARCO/0000-0002-3336-4965; Alves, Joao/0000-0002-4355-0921 NR 18 TC 9 Z9 9 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 NOV PY 2013 VL 559 AR A90 DI 10.1051/0004-6361/201321827 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263ZR UT WOS:000327847200090 ER PT J AU Matrozis, E Ryde, N Dupree, AK AF Matrozis, E. Ryde, N. Dupree, A. K. TI Galactic chemical evolution of sulphur Sulphur abundances from the [SI] lambda 1082 nm line in giants SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Galaxy: evolution; stars: fundamental parameters; stars: abundances; infrared: stars ID METAL-POOR STARS; EFFECTIVE TEMPERATURE SCALE; INFRARED FLUX METHOD; STELLAR PARAMETERS; ZINC ABUNDANCES; DISK STARS; HALO STARS; FGK STARS; I LINE; NUCLEOSYNTHESIS AB Context. The Galactic chemical evolution of sulphur is still under debate. At low metallicities some studies find no correlation between [S/Fe] and [Fe/H], which is typical for a-elements, while others find [S/Fe] increasing towards lower metallicities, and still others find a combination of the two. Each scenario has different implications for the Galactic chemical evolution of sulphur. Aims. The aim of this study is to contribute to the discussion on the Galactic chemical evolution of sulphur by deriving sulphur abundances from non-local thermodynamic equilibrium (LTE) insensitive spectral diagnostics in disk and halo stars with homogeneously determined stellar parameters. Methods. We derived effective temperatures from photometric colours, surface gravities from stellar isochrones and Bayesian estimation, and metallicities and sulphur abundances from spectrum synthesis. We derived sulphur abundances from the [SI] lambda 1082 nm line in 39 mostly cool and metal-poor giants using 1D LTE MARCS model atmospheres to model our high-resolution near-infrared spectra obtained with the VLT, NOT, and Gemini South telescopes. Results. We derive homogeneous stellar parameters for 29 of the 39 stars. Our results argue for a chemical evolution of sulphur that is typical for a-elements, contrary to some previous studies that have found high sulphur abundances ([S/Fe] >= 0.6) for stars with -2.5 < [Fe/H] < -1. Our abundances are systematically higher by about 0.1 dex than those of other studies that arrived at similar conclusions using other sulphur diagnostics. Conclusions. We find the [SI] line to be a valuable diagnostic of sulphur abundances in cool giants down to [Fe/H] similar or equal to -2.3. We argue that a homogeneous determination of stellar parameters is necessary, since the derived abundances are sensitive to them. Our results ([S/Fe]) agree reasonably well with predictions of contemporary models of Galactic chemical evolution. In these models sulphur is predominantly created in massive stars by oxygen burning and is ejected into the interstellar medium during Type II supernovae explosions. Systematic differences with previous studies most likely fall within modelling uncertainties. C1 [Matrozis, E.; Ryde, N.] Lund Univ, Dept Astron & Theoret Phys, Lund Observ, S-22100 Lund, Sweden. [Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Matrozis, E (reprint author), Lund Univ, Dept Astron & Theoret Phys, Lund Observ, Box 43, S-22100 Lund, Sweden. EM ryde@astro.lu.se FU Knut and Alice Wallenberg Foundation; Kungl. Fysiografiska Sallskapet i Lund; Swedish Research Council, VR FX N.R. is a Royal Swedish Academy of Sciences Research Fellow supported by a grant from the Knut and Alice Wallenberg Foundation. Funds from Kungl. Fysiografiska Sallskapet i Lund and support from the Swedish Research Council, VR are acknowledged. The authors are grateful to L. Lindegren, S. Feltzing and the referee E. Caffau for providing valuable feedback that improved the quality of this paper. NR 72 TC 7 Z9 7 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 NOV PY 2013 VL 559 AR A115 DI 10.1051/0004-6361/201322317 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263ZR UT WOS:000327847200115 ER PT J AU Ness, JU Osborne, JP Henze, M Dobrotka, A Drake, JJ Ribeiro, VARM Starrfield, S Kuulkers, E Behar, E Hernanz, M Schwarz, G Page, KL Beardmore, AP Bode, MF AF Ness, J. -U. Osborne, J. P. Henze, M. Dobrotka, A. Drake, J. J. Ribeiro, V. A. R. M. Starrfield, S. Kuulkers, E. Behar, E. Hernanz, M. Schwarz, G. Page, K. L. Beardmore, A. P. Bode, M. F. TI Obscuration effects in super-soft-source X-ray spectra SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE novae, cataclysmic variables; X-rays: binaries; binaries: eclipsing ID LARGE-MAGELLANIC-CLOUD; NOVA V382 VELORUM; SOURCE RX J0019.8+2156; SOURCE CAL 83; RS-OPHIUCHI; U-SCORPII; MODEL ATMOSPHERES; LIGHT CURVES; WHITE-DWARF; XMM-NEWTON AB Context. Super-soft-source (SSS) X-ray spectra are blackbody-like spectra with effective temperatures similar to 3-7 x 10(5) K and luminosities of 10(35-38) erg s(-1). Grating spectra of SSS and novae in outburst that show SSS type spectra display atmospheric absorption lines. Radiation transport atmosphere models can be used to derive physical parameters. Blue-shifted absorption lines suggest that hydrostatic equilibrium is an insufficient assumption, and more sophisticated models are required. Aims. In this paper, we bypass the complications of spectral models and concentrate on the data in a comparative, qualitative study. We inspect all available X-ray grating SSS spectra to determine systematic, model-independent trends. Methods. We collected all grating spectra of conventional SSS like Cal83 and Cal87 plus observations of novae during their SSS phase. We used comparative plots of spectra of different systems to find common and different features. The results were interpreted in the context of system parameters obtained from the literature. Results. We find two distinct types of SSS spectra that we name SSa and SSe. Their main observational characteristics are either clearly visible absorption lines or emission lines, respectively, while both types contain atmospheric continuum emission. SSa spectra are highly structured with no spectral model currently able to reproduce all details. The emission lines clearly seen in SSe may also be present in SSa, hidden within the forest of complex atmospheric absorption and emission features. This suggests that SSe are in fact obscured SSa systems. Similarities between SSe and SSa with obscured and unobscured AGN, respectively, support this interpretation. We find all known or suspected high-inclination systems to emit permanently in an SSe state. Some sources are found to transition between SSa and SSe states, becoming SSe when fainter. Conclusions. SSS spectra are subject to various occultation processes. In persistent SSS spectra such as Cal87, the accretion disc blocks the central hot source when viewed edge on. In novae during their SSS phase, the accretion disc may have been destroyed during the initial explosion but could have reformed by the time of the SSS phase. In addition, clumpy ejecta may lead to temporary obscuration events. The emission lines stem from reprocessed emission in the accretion disc, its wind or further out in clumpy ejecta, while Thomson scattering allows continuum emission to be visible also during total obscuration of the central hot source. C1 [Ness, J. -U.; Henze, M.; Kuulkers, E.] ESAC, Sci Operat Dept ESA, Sci Operat Div, Villanueva De La Canada 28691, Madrid, Spain. [Ness, J. -U.; Page, K. L.; Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Dobrotka, A.] Slovak Univ Technol Bratislava, Fac Mat Sci & Technol, Inst Mat Sci, Dept Phys, Trnava 91724, Slovakia. [Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ribeiro, V. A. R. M.] Univ Cape Town, Dept Astron, Astrophys Cosmol & Grav Ctr, ZA-7701 Rondebosch, South Africa. [Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Behar, E.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Hernanz, M.] Inst Ciencies Espai CSIC IEEC, Fac Ciencies, Bellaterra 08193, Barcelona, Spain. [Schwarz, G.] Amer Astron Soc, Washington, DC 20009 USA. [Bode, M. F.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. RP Ness, JU (reprint author), ESAC, Sci Operat Dept ESA, Sci Operat Div, Villanueva De La Canada 28691, Madrid, Spain. EM juness@sciops.esa.int RI Hernanz, Margarita/K-1770-2014; OI Hernanz, Margarita/0000-0002-8651-7910; Roberts Machado Ribeiro, Valerio Alipio/0000-0003-3617-4400; Henze, Martin/0000-0001-9985-3406 FU UK Space Agency; Slovak Academy of Sciences [1/0511/13]; ESA international fellowship; ESA fellowship; South African SKA Project; Spanish grants [AYA2011-24704, 2009 SGR 315]; NASA; NSF; Israel Science Foundation [1163/10]; ESA Member States FX We thank the referee for a most inspiring and encouraging report. The authors appreciate useful discussions with M. Giustini about AGNs. We thank S. N. Shore who has helped with useful comments. This research has made use of data obtained with the gratings on board XMM-Newton and Chandra. XMM-Newton is an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. Software provided by the Chandra X-ray Center (CXC) in the application package CIAO was used to obtain science data. K. L. Page, J. P. Osborne, and A. P. Beardmore acknowledge financial support from the UK Space Agency. A. Dobrotka was supported by the Slovak Academy of Sciences Grant No. 1/0511/13 and by the ESA international fellowship. M. Henze acknowledges support from an ESA fellowship. V. A. R. M. Ribeiro acknowledges the South African SKA Project for funding the postdoctoral fellowship at the University of Cape Town. M. Hemanz acknowledges the Spanish grants AYA2011-24704 and 2009 SGR 315. S. Starrfield acknowledges partial support from NASA and NSF grants to ASU. E. Behar was supported by grant #1163/10 from the Israel Science Foundation. NR 117 TC 17 Z9 17 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 NOV PY 2013 VL 559 AR A50 DI 10.1051/0004-6361/201322415 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263ZR UT WOS:000327847200050 ER PT J AU Penna, RF Kulkarni, A Narayan, R AF Penna, Robert F. Kulkarni, Akshay Narayan, Ramesh TI A new equilibrium torus solution and GRMHD initial conditions SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; hydrodynamics; black hole physics ID RELATIVISTIC MAGNETOHYDRODYNAMIC SIMULATIONS; MAGNETIC-FIELD GEOMETRY; SAGITTARIUS A-ASTERISK; HOLE ACCRETION FLOWS; ROTATING BLACK-HOLE; FLUID DISKS; ANGULAR-MOMENTUM; STANDING SHOCKS; INSTABILITY; EVOLUTION AB Context. General relativistic magnetohydrodynamic (GRMHD) simulations are providing influential models for black hole spin measurements, gamma ray bursts, and supermassive black hole feedback. Many of these simulations use the same initial condition: a rotating torus of fluid in hydrostatic equilibrium. A persistent concern is that simulation results sometimes depend on arbitrary features of the initial torus. For example, the Bernoulli parameter (which is related to outflows), appears to be controlled by the Bernoulli parameter of the initial torus. Aims. In this paper, we give a new equilibrium torus solution and describe two applications for the future. First, it can be used as a more physical initial condition for GRMHD simulations than earlier torus solutions. Second, it can be used in conjunction with earlier torus solutions to isolate the simulation results that depend on initial conditions. Methods. We assume axisymmetry, an ideal gas equation of state, constant entropy, and ignore self-gravity. We fix an angular momentum distribution and solve the relativistic Euler equations in the Kerr metric. Results. The Bernoulli parameter, rotation rate, and geometrical thickness of the torus can be adjusted independently. Our torus tends to be more bound and have a larger radial extent than earlier torus solutions. Conclusions. While this paper was in preparation, several GRMHD simulations appeared based on our equilibrium torus. We believe it will continue to provide a more realistic starting point for future simulations. C1 [Penna, Robert F.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Penna, Robert F.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kulkarni, Akshay] Microsoft Corp, Redmond, WA 98052 USA. [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Penna, RF (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. EM rpenna@mit.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU Pappalardo Fellowship in Physics at MIT FX R.F.P was supported in part by a Pappalardo Fellowship in Physics at MIT. NR 39 TC 9 Z9 9 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2013 VL 559 AR A116 DI 10.1051/0004-6361/201219666 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263ZR UT WOS:000327847200116 ER PT J AU Laurin, M Sues, HD Modesto, SP Evans, DC AF Laurin, Michel Sues, Hans-Dieter Modesto, Sean P. Evans, David C. TI A tribute to Robert R. Reisz SO COMPTES RENDUS PALEVOL LA English DT Biographical-Item C1 [Laurin, Michel] CNRS MNHN UPMC, Museum Natl Hist Nat, Ctr Rech Paleobiodiversite & Paleoenvironm, Dept Hist Terre,UMR 7207, F-75231 Paris 05, France. [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Modesto, Sean P.] Cape Breton Univ, Dept Biol, Sydney, NS B1P 6L2, Canada. [Evans, David C.] Royal Ontario Museum, Dept Nat Hist, Toronto, ON M5S 2C6, Canada. RP Sues, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM SUESH@si.edu RI Laurin, Michel/B-7884-2008 OI Laurin, Michel/0000-0003-2974-9835 NR 1 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1631-0683 EI 1777-571X J9 CR PALEVOL JI C. R. Palevol PD NOV-DEC PY 2013 VL 12 IS 7-8 BP 389 EP 392 DI 10.1016/j.crpv.2013.09.002 PG 4 WC Paleontology SC Paleontology GA 287SR UT WOS:000329563000001 ER PT J AU Laurin, M Sues, HD AF Laurin, Michel Sues, Hans-Dieter TI Robert R. Reisz - Renaissance paleontologist SO COMPTES RENDUS PALEVOL LA English DT Article DE Paleontology; Vertebrates; Phylogenetics; Tetrapods; Amniotes; Paleozoic; Morphology ID EARLY EVOLUTION; RICHARDS SPUR; FOSSIL RECORD; 1ST RECORD; REPTILE; ORIGIN; PHYLOGENY; AMNIOTE; MICROSAUR; TETRAPODA AB Robert R. Reisz has published some 157 papers over 40 years, mostly on Permo-Carboniferous stegocephalians (sensu Laurin; "tetrapods" in traditional usage), especially amniotes, but also on other taxa and periods, from Devonian dipnoans to Neogene primates. He has been a leader in the study of early amniote phylogeny, publishing one of the first cladograms of these taxa in 1980. His work has proposed new hypotheses about the origin of turtles, extant amphibians and therapsids. His classical work on Paleozoic synapsids provided the basis for currently accepted taxonomies. He has also tackled several major evolutionary innovations, such as the origin of herbivory among tetrapods and the use of venom in mammals. Finally, he has proposed new calibration constraints for molecular dating. He has trained a number of postdoctoral fellows, doctoral and masters' students. (C) 2012 Academie des sciences. Published by Elsevier Masson SAS. All rights reserved. C1 [Laurin, Michel] CNRS MNHN UPMC, Museum Natl Hist Nat, Ctr Rech Paleodiversite & Paleoenvironm, Dept Hist Terre,UMR 7207, F-75231 Paris 05, France. [Sues, Hans-Dieter] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Laurin, M (reprint author), CNRS MNHN UPMC, Museum Natl Hist Nat, Ctr Rech Paleodiversite & Paleoenvironm, Dept Hist Terre,UMR 7207, Batiment Geol,Case Postale 48,57,Rue Cuvier, F-75231 Paris 05, France. EM michel.laurin@upmc.fr; suesh@si.edu RI Laurin, Michel/B-7884-2008 OI Laurin, Michel/0000-0003-2974-9835 NR 40 TC 0 Z9 0 U1 1 U2 5 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1631-0683 EI 1777-571X J9 CR PALEVOL JI C. R. Palevol PD NOV-DEC PY 2013 VL 12 IS 7-8 BP 393 EP 404 DI 10.1016/j.crpv.2012.09.001 PG 12 WC Paleontology SC Paleontology GA 287SR UT WOS:000329563000002 ER PT J AU Schoch, RR Sues, HD AF Schoch, Rainer R. Sues, Hans-Dieter TI A new dissorophid temnospondyl from the Lower Permian of north-central Texas SO COMPTES RENDUS PALEVOL LA English DT Article DE Tetrapoda; Temnospondyli; Dissorophoidea; Eucacopinae; Permian ID CACOPS-ASPIDEPHORUS; RICHARDS SPUR; OKLAHOMA; OSTEODERMS; VERTEBRAE AB Dissorophidae form a clade of terrestrially adapted temnospondyls, which were widely distributed in Euramerica and Asia during the Permian. After a long phase of neglect, study of exquisitely preserved new material of the Early Permian Cacops from Oklahoma has prompted reconsideration of other dissorophids, such as the Early Permian Conjunctio from New Mexico. Here we report on a specimen previously referred to Conjunctio from the Nocona Formation of north-central Texas. It actually represents a distinct new taxon, for which the binomen Scapanops neglecta is proposed. It represents a small dissorophid with derived characters combining to give a unique skull configuration: extremely short skull table, jaw joint situated well anterior to occiput, large orbits with wide interorbital distance, and a preorbital region more than twice as long as the postorbital region. The external nares are elongate, and the outline of the skull is ovoid, widest at mid-level of the orbits. S. neglecta shares with eucacopines the presence of a rounded internarial fenestra and an anteroposteriorly short supratemporal. Phylogenetic analysis places Scapanops at the base of the clade Eucacopinae, more crownward than Conjunctio and as the sister-taxon to a grouping comprising Cacops, Kamacops, and Zygosaurus. (C) 2012 Academie des sciences. Published by Elsevier Masson SAS. All rights reserved. C1 [Schoch, Rainer R.] Staatl Museum Nat Kunde, D-70191 Stuttgart, Germany. [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Schoch, RR (reprint author), Staatl Museum Nat Kunde, Rosenstein 1, D-70191 Stuttgart, Germany. EM rainer.schoch@smns-bw.de; suesh@si.edu NR 25 TC 1 Z9 1 U1 0 U2 2 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1631-0683 EI 1777-571X J9 CR PALEVOL JI C. R. Palevol PD NOV-DEC PY 2013 VL 12 IS 7-8 BP 437 EP 445 DI 10.1016/j.crpv.2013.04.002 PG 9 WC Paleontology SC Paleontology GA 287SR UT WOS:000329563000005 ER PT J AU Godfrey, SJ AF Godfrey, Stephen J. TI On the olfactory apparatus in the Miocene odontocete Squalodon sp (Squalodontidae) SO COMPTES RENDUS PALEVOL LA English DT Article DE Squalodontidae; Odontoceti; Olfaction; Miocene; Calvert Formation; Ethmoturbinates ID DIMETHYL SULFIDE; MITOCHONDRIAL GENOMES; RORQUAL WHALES; GENE; CETACEANS; ATTRACTION; PHYLOGENY; REDUCTION; RADIATION; SEABIRDS AB Most extant odontocetes appear to be anosmatic. However, some Miocene odontocetes, including a broken skull attributed to Squalodon sp. (Calvert Formation, Calvert Cliffs, Maryland, USA) preserve the osteological components associated with a well-developed sense of smell: dorsal nasal meatuses, ethmoturbinates within olfactory recesses, a perforate cribriform plate, and an olfactory bulb chamber. In Squalodon sp., the area within the olfactory recesses (i.e., covered in life by olfactory sensory epithelia) is 5367 mm(2) and the area occupied by the olfactory bulbs (i.e., the ethmoid area) is 769.8 mm(2). In most mammals, the area of the olfactory epithelium is typically circa 16 times larger than the ethmoid area. The area covered by olfactory epithelium in CMM-V-2287 is only about seven times larger than its ethmoid area, less than half the area in typical mammals. During the Miocene, most odontocetes variously lost the osteological proxies indicative of osmatic ability. Perhaps biosonar surpassed the efficiency of olfactory cues during predation and social/parental/sexual interactions rendering the latter redundant/obsolete in odontocete analysis of, and interactions with and within their aquatic environments. (C) 2012 Academie des sciences. Published by Elsevier Masson SAS. All rights reserved. C1 [Godfrey, Stephen J.] Calvert Marine Museum, Dept Paleontol, Solomons, MD 20688 USA. [Godfrey, Stephen J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Godfrey, SJ (reprint author), Calvert Marine Museum, Dept Paleontol, POB 97, Solomons, MD 20688 USA. EM Godfresj@co.cal.md.us FU Board of Calvert County Commissioners; citizens of Calvert County, MD; Clarissa and Lincoln Dryden Endowment for Paleontology at the Calvert Marine Museum FX This publication was made possible with funding from the Board of Calvert County Commissioners, the citizens of Calvert County, MD, and the Clarissa and Lincoln Dryden Endowment for Paleontology at the Calvert Marine Museum. NR 49 TC 8 Z9 9 U1 2 U2 10 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1631-0683 EI 1777-571X J9 CR PALEVOL JI C. R. Palevol PD NOV-DEC PY 2013 VL 12 IS 7-8 BP 519 EP 530 DI 10.1016/j.crpv.2013.03.002 PG 12 WC Paleontology SC Paleontology GA 287SR UT WOS:000329563000012 ER PT J AU Cortes, MC Uriarte, M Lemes, MR Gribel, R Kress, WJ Smouse, PE Bruna, EM AF Cortes, Marina C. Uriarte, Maria Lemes, Maristerra R. Gribel, Rogerio Kress, W. John Smouse, Peter E. Bruna, Emilio M. TI Low plant density enhances gene dispersal in the Amazonian understory herb Heliconia acuminata SO MOLECULAR ECOLOGY LA English DT Article DE hummingbird; manakin; pollination; reproductive dominance; seed dispersal; thrush ID MEDIATED SEED DISPERSAL; RAIN-FOREST FRAGMENTS; WIND-POLLINATED TREE; HABITAT FRAGMENTATION; POLLEN DISPERSAL; PARENTAGE ANALYSIS; MATING PATTERNS; POPULATIONS; CONSEQUENCES; LANDSCAPE AB In theory, conservation genetics predicts that forest fragmentation will reduce gene dispersal, but in practice, genetic and ecological processes are also dependent on other population characteristics. We used Bayesian genetic analyses to characterize parentage and propagule dispersal in Heliconia acuminata L. C. Richard (Heliconiaceae), a common Amazonian understory plant that is pollinated and dispersed by birds. We studied these processes in two continuous forest sites and three 1-ha fragments in Brazil's Biological Dynamics of Forest Fragments Project. These sites showed variation in the density of H.acuminata. Ten microsatellite markers were used to genotype flowering adults and seedling recruits and to quantify realized pollen and seed dispersal distances, immigration of propagules from outside populations, and reproductive dominance among parents. We tested whether gene dispersal is more dependent on fragmentation or density of reproductive plants. Low plant densities were associated with elevated immigration rates and greater propagule dispersal distances. Reproductive dominance among inside-plot parents was higher for low-density than for high-density populations. Elevated local flower and fruit availability is probably leading to spatially more proximal bird foraging and propagule dispersal in areas with high density of reproductive plants. Nevertheless, genetic diversity, inbreeding coefficients and fine-scale spatial genetic structure were similar across populations, despite differences in gene dispersal. This result may indicate that the opposing processes of longer dispersal events in low-density populations vs. higher diversity of contributing parents in high-density populations balance the resulting genetic outcomes and prevent genetic erosion in small populations and fragments. C1 [Cortes, Marina C.; Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Cortes, Marina C.; Bruna, Emilio M.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69083000 Manaus, Amazonas, Brazil. [Cortes, Marina C.; Bruna, Emilio M.] Smithsonian Trop Res Inst, BR-69083000 Manaus, Amazonas, Brazil. [Gribel, Rogerio] Inst Nacl de Pesquisas da Amazonia, Lab Genet & Biol Reprod Plantas, BR-69083000 Manaus, Amazonas, Brazil. [Lemes, Maristerra R.; Gribel, Rogerio] Inst Pesquisas Jardim Bot Rio de Janeiro, BR-22460030 Rio De Janeiro, RJ, Brazil. [Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Smouse, Peter E.] Rutgers State Univ, Dept Ecol Evolut & Nat Resources, New Brunswick, NJ 08901 USA. [Bruna, Emilio M.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. [Bruna, Emilio M.] Univ Florida, Ctr Latin Amer Studies, Gainesville, FL 32611 USA. RP Cortes, MC (reprint author), Columbia Univ, Dept Ecol Evolut & Environm Biol, 1200 Amsterdam Ave, New York, NY 10027 USA. EM marina.ccortes@gmail.com RI cortes, marina/I-2155-2012; Bruna, Elena/C-4939-2014; Gribel, Rogerio/C-5392-2013; Bruna, Emilio/H-2769-2012 OI Bruna, Elena/0000-0001-5427-1461; Gribel, Rogerio/0000-0002-0850-5578; Bruna, Emilio/0000-0003-3381-8477 FU US National Science Foundation [DEB-0614339, DEB-0614149, DEB-0309819, DBI-0109226, INT 98-06351]; Smithsonian Institution; CNPq/Brazil FX We thank Dustin Rubenstein and three anonymous reviewers for valuable comments on the manuscript. We would like to thank Jeffrey Hunt, Gabriel Johnson, Ida Lopez and David Erickson for assistance in the development of the molecular markers and Lee Weigt for facilitating our work in the Museum Support Center, Smithsonian Institution. We are grateful for the help provided by Carla Sardelli and Carolina Medeiros at LabGen, INPA and Osmaildo Ferreira da Silva for assistance in the field. We thank Emily Moran for sharing the code and helping with the model interpretation and Lora Murphy for help in adapting the code to our system. We also thank BDFFP and INPA for their logistical support. Financial support was provided by the US National Science Foundation (award DEB-0614339 to MU, DEB-0614149, DEB-0309819, DBI-0109226 and INT 98-06351 to EB) and the Smithsonian Institution. MRL and RG acknowledge research fellowships from CNPq/Brazil. This is publication number 626 in the BDFFP Technical Series. NR 86 TC 11 Z9 11 U1 7 U2 43 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 NOV PY 2013 VL 22 IS 22 BP 5716 EP 5729 DI 10.1111/mec.12495 PG 14 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 290VO UT WOS:000329786700016 PM 24730040 ER PT J AU Delaney, MA AF Delaney, Michelle Anne TI Native Performers in the Wild West Shows: From Buffalo Bill to Euro Disney SO PUBLIC HISTORIAN LA English DT Book Review C1 [Delaney, Michelle Anne] Smithsonian Inst, Washington, DC 20560 USA. RP Delaney, MA (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIFORNIA PRESS PI BERKELEY PA C/O JOURNALS & DIGITAL PUBLISHING DIVISION, 2000 CENTER ST, STE 303, BERKELEY, CA 94704-1223 USA SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD NOV PY 2013 VL 35 IS 4 BP 94 EP 96 PG 3 WC History SC History GA 286NP UT WOS:000329476300020 ER PT J AU Holm, JA Thompson, JR McShea, WJ Bourg, NA AF Holm, Jennifer A. Thompson, Jonathan R. McShea, William J. Bourg, Norman A. TI Interactive effects of chronic deer browsing and canopy gap disturbance on forest successional dynamics SO ECOSPHERE LA English DT Article DE community composition; forest simulator; Liriodendron tulipifera; sapling; Quercus; ZELIG ID WHITE-TAILED DEER; EASTERN NORTH-AMERICA; CLIMATE-CHANGE; VEGETATION STRUCTURE; DECIDUOUS FOREST; HARDWOOD FORESTS; COMPUTER-MODEL; OAK FOREST; GROWTH; POPULATIONS AB The interaction of browsing by white-tailed deer (Odocoileus virginianus) and canopy gap disturbances may affect long-term tree composition and lead to significant changes in forest structure. We used an individual-based forest gap model (ZELIG) to better understand the aggregate and interactive impacts of these processes on the long-term (200 years) successional dynamics of a mesic deciduous forest. We parameterized ZELIG to: (1) simulate successional dynamics within a temperate deciduous secondary forest typical of eastern North America; (2) simulate browsing impacts by white-tailed deer; and (3) simulate gap-scale disturbance of variable size and frequency. Our estimates of browsing impacts by species were derived from a 20-year, four-hectare deer exclusion study. Model calibration matched observed tree species composition, density by size class, and total basal area (39.92 m(2) ha(-1) vs. 37.13 m(2) ha(-1)). Simulated deer browsing had little impact on total basal area over two centuries. However, deer browsing had substantial impacts on community composition, creating a less diverse understory, lower species richness, and decreased abundance of Quercus species, while retaining the dominance of Liriodendron tulipifera. Simulated gap disturbances exacerbated the impacts of chronic deer browsing and these impacts became stronger over time. Our analyses suggest that recent increases in white-tailed deer density within many forests of eastern North America will result in altered community dynamics that persist beyond the sapling level, and that any increases in overstory disturbance frequency will exacerbate these impacts. C1 [Holm, Jennifer A.; Thompson, Jonathan R.; McShea, William J.; Bourg, Norman A.] Smithsonian Inst, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Holm, JA (reprint author), Smithsonian Inst, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM jennifer.holm@gmail.com FU HSBC Climate Partnership; SIGEO Initiative and the Smithsonian Institution FX Establishment of the SCBI SIGEO plot by William J. McShea and Norman A. Bourg was funded by the HSBC Climate Partnership, the SIGEO Initiative and the Smithsonian Institution. We thank the numerous technicians, interns and volunteers of the Conservation Ecology Center at SCBI who were essential in assisting with plot establishment and data collection, most notably Jennifer McGarvey, Xiaoli Shen, Shawn Behling, Megan Baker, Sumana Serchan and Chris Lewis. Additional thanks to Joseph Romond for helpful comments on later drafts of the paper and to Yuancho Fan, Evelyn Strombom, and Meghan Blumstein who helped with figures. NR 75 TC 1 Z9 1 U1 3 U2 36 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD NOV PY 2013 VL 4 IS 11 AR UNSP 144 DI 10.1890/ES13-00223 PG 23 WC Ecology SC Environmental Sciences & Ecology GA 285PH UT WOS:000329405600002 ER PT J AU Clough, GW AF Clough, G. Wayne TI From the Castle SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD NOV PY 2013 SI SI BP 10 EP 10 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 286QS UT WOS:000329484400001 ER PT J AU Braje, TJ Rick, TC AF Braje, Todd J. Rick, Torben C. TI From Forest Fires to Fisheries Management: Anthropology, Conservation Biology, and Historical Ecology SO EVOLUTIONARY ANTHROPOLOGY LA English DT Article DE applied archeobiology; human-environmental ecodynamics ID NORTHERN CHANNEL-ISLANDS; SANTA ROSA ISLAND; SOUTHERN CALIFORNIA; VEGETATION; IMPACTS; ABALONE; AREAS; PALEOBIOLOGY; HYPOTHESIS; MOUNTAINS AB Human-environmental relationships have long been of interest to a variety of scientists, including ecologists, biologists, anthropologists, and many others. In anthropology, this interest was especially prevalent among cultural ecologists of the 1970s and earlier, who tended to explain culture as the result of techno-environmental constraints. More recently researchers have used historical ecology, an approach that focuses on the long-term dialectical relationship between humans and their environments, as well as long-term prehuman ecological datasets. An important contribution of anthropology to historical ecology is that anthropological datasets dealing with ethnohistory, traditional ecological knowledge, and human skeletal analysis, as well as archeological datasets on faunal and floral remains, artifacts, geochemistry, and stratigraphic analysis, provide a deep time perspective (across decades, centuries, and millennia) on the evolution of ecosystems and the place of people in those larger systems. Historical ecological data also have an applied component that can provide important information on the relative abundances of flora and fauna, changes in biogeography, alternations in food webs, landscape evolution, and much more. C1 [Braje, Todd J.] San Diego State Univ, San Diego, CA 92182 USA. [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Braje, TJ (reprint author), San Diego State Univ, San Diego, CA 92182 USA. NR 64 TC 5 Z9 5 U1 3 U2 32 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1060-1538 EI 1520-6505 J9 EVOL ANTHROPOL JI Evol. Anthropol. PD NOV PY 2013 VL 22 IS 6 BP 303 EP 311 DI 10.1002/evan.21379 PG 9 WC Anthropology SC Anthropology GA 274MX UT WOS:000328611700004 PM 24347504 ER PT J AU de Silva, SL Spagnuolo, MG Bridges, NT Zimbelman, JR AF de Silva, S. L. Spagnuolo, M. G. Bridges, N. T. Zimbelman, J. R. TI Gravel-mantled megaripples of the Argentinean Puna: A model for their origin and growth with implications for Mars SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Article ID TRANSVERSE AEOLIAN RIDGES; LARGEST WIND RIPPLES; MERIDIANI-PLANUM; OFFSHORE WINDS; HIRISE IMAGES; CENTRAL ANDES; LANDING SITE; EARTH; IGNIMBRITES; PROFILES AB Gravel "megaripples" in the Puna of Argentina are the most extreme aeolian megaripples on Earth and are useful analogs for aeolian processes on Mars. Field observations, supplemented by experimental and numerical constraints on wind characteristics and aeolian transport, reveal their conditions of formation and growth to be an aeolian geomorphology "perfect storm." The bedforms are formed on a substrate of weakly indurated ignimbrite, aeolian defl ation of which yields a bimodal lag of lithics and pumice clasts onto an undulating surface. Under normal wind conditions in this region, the lithics are organized into bedforms on local upslopes and "highs" through creep induced by the impact of saltating sand and pumice. The gravel bedforms grow through "shadowing" and trap sand and silt that is gradually kinetically sieved down to "lift" the gravel mantle upwards to form the megaripples. These observations connote that the largest features are not ripples in the sense of migrating bedforms, but rather nucleation sites of windtransported sediment. Strong control by bedrock topography means that the largest bedform wavelengths are not a result of particle trajectories, and this complicates their comparison with other ripples and may require a new classifi cation. Of relevance to Mars, the Puna megaripples are morphologically and contextually similar to small ripple- like transverse aeolian ridges (TARs). Moreover, the Puna gravels have similar equivalent weight (mg) to those composing granule ripples at Meridiani Planum, and their local origin may have implications for the origin of sediment in martian aeolian bedforms. Finally, the stable yet dynamic character of the Puna megaripples could help reconcile current models of TARs with periodic bedrock ridges that may be produced by aeolian erosion. C1 [de Silva, S. L.; Spagnuolo, M. G.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Bridges, N. T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Zimbelman, J. R.] Smithsonian Inst, CEPS NASM MRC 315, Washington, DC 20013 USA. Univ Nacl Salta, RA-4400 Salta, Argentina. RP de Silva, SL (reprint author), Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA. EM desilvas@geo.oregonstate.edu RI de Silva, Shanaka/A-4630-2011; Bridges, Nathan/D-6341-2016 OI de Silva, Shanaka/0000-0002-0310-5516; FU NASA Mars Fundamental Research Program [NNX10AP79G]; NASA Planetary Geology and Geophysics program FX We dedicate this work to the memory of our collaborator Ron Greeley. His support, encouragement, and wisdom was critical to implementing this work. This work is conducted under the auspices of NASA Mars Fundamental Research Program grant NNX10AP79G (Principal Investigator de Silva). Jose Viramonte's knowledge, support, and enthusiasm were a major boon for this work. Ralph Lorenz designed and loaned us the time-lapse cameras; his advice and keen insight are always appreciated. Agustin Ortiz is thanked for enthusiastic support in the field and discussions about gravel componentry. We are also indebted to the staff at the Arizona State University wind tunnel facility (supported in part by the NASA Planetary Geology and Geophysics program) for their support and advice during our experiments there. Devon Burr is thanked for extensive discussions about volcaniclastic sediment sources and dark dunes and strong interest in this work. Josh Emery and Devon Burr provided the IDL code used to compute saltation friction speed using the Greeley and Iversen (1985) method. Rob Sullivan and Mary Bourke are thanked for their advice on the wind tunnel experiments. The interest, insight, and comments of two anonymous reviewers and Associate Editor Nadine Barlow are deeply appreciated. NR 58 TC 14 Z9 14 U1 2 U2 15 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 NOV-DEC PY 2013 VL 125 IS 11-12 BP 1912 EP 1929 DI 10.1130/B30916.1 PG 18 WC Geosciences, Multidisciplinary SC Geology GA 273BI UT WOS:000328507400014 ER PT J AU Becker, C Klaus, S Tudge, CC AF Becker, Carola Klaus, Sebastian Tudge, Christopher C. TI Male Internal Reproductive Structures of European Pea Crabs (Crustacea, Decapoda, Brachyura, Pinnotheridae): Vas Deferens Morphology and Spermatozoal Ultrastructure SO JOURNAL OF MORPHOLOGY LA English DT Article DE Pinnotheres; vas deferens appendices; spermatozoa; spermatophores; seminal plasma ID SPIDER CRAB; SEMINAL SECRETIONS; LIBINIA-EMARGINATA; SPERM METABOLISM; SCYLLA-SERRATA; GERYON-FENNERI; EASTERN GULF; SYSTEM; FEMALE; SPERMATOPHORES AB Pea crabs of the subfamily Pinnotherinae (Pinnotheridae) have a high investment in reproduction and an outstanding reproductive output, probably as an adaptation to the required increase in reproductive rate due to the pinnotherids small size and their parasitic, host-dependant way of life. In the present study, we investigate the male internal reproductive structures and the ultrastructure of spermatozoa of Pinnotheres pisum and Nepinnotheres pinnotheres by histological methods and both scanning- and transmission electron microscopy. In the Brachyura, the male internal reproductive systems generally consist of paired testes and corresponding vasa deferentia where spermatozoa develop and mature. Spermatozoal ultrastructure of the investigated pinnotherids conforms to the thoracotreme type, however, N. pinnotheres has an accessory opercular ring and a periopercular rim, neither of which are present in spermatozoa of P. pisum. Spermatozoa are enclosed within spermatophores in the secretory proximal vas deferens. Two types of secretions were observed in P. pisum and N. pinnotheres: an electron dense substance secreted in the proximal vas deferens involved in spermatophore formation, and large electron-luscent vesicles constituting the seminal plasma in the medial and distal vas deferens. The medial vas deferens is strongly widened compared to other brachyurans to purpose storing spermatophores embedded in seminal plasma. Tubular appendices, which produce and store large amounts of seminal plasma, arise from the distal region of the vas deferens. The appendices extend into the ventral cephalothorax and also in the first pleomere. The latter being an exceptional location for reproductive structures among male brachyurans. J. Morphol. 274:1312-1322, 2013. (c) 2013 Wiley Periodicals, Inc. C1 [Becker, Carola] Humboldt Univ, Dept Biol, D-10115 Berlin, Germany. [Klaus, Sebastian] Goethe Univ Frankfurt, Deptartment Ecol & Evolut, D-60438 Frankfurt, Germany. [Tudge, Christopher C.] Amer Univ, Dept Biol, Washington, DC 20016 USA. [Tudge, Christopher C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Becker, C (reprint author), Humboldt Univ, Dept Biol, Philippstr 13, D-10115 Berlin, Germany. EM Carola.Becker@Biologie.HU-Berlin.de NR 64 TC 1 Z9 1 U1 1 U2 7 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 NOV PY 2013 VL 274 IS 11 BP 1312 EP 1322 DI 10.1002/jmor.20184 PG 11 WC Anatomy & Morphology SC Anatomy & Morphology GA 270MP UT WOS:000328322800008 PM 24027013 ER PT J AU Penland, L Brooks, B Ochoa, E AF Penland, Laurie Brooks, Barrett Ochoa, Edgardo TI Long-Term Methods for High-Definition Image Maps of Benthic Surveys SO MARINE TECHNOLOGY SOCIETY JOURNAL LA English DT Article DE benthic survey; image maps; photo mosaic; coral monitoring; high definition AB Coral reef health assessment has relied on benthic photographic surveys as an essential measurement tool for decads. The emergence of gigapixel image (1 billion pixels) stitching technologies makes possible the creation of high-definition benthic image maps surveys (HDBIMS). These image maps provide the traditional overall percentage converage data. In addition, they allow zoom capabilities in such detail that scientists can, for example, count the polyps on a coral head. While the image maps are easily viewed over the Internet they are challenging to produce. Numerous previous studies have contributed to the advancement of high-definition benthic survey methods. This ongoing HDBIMS study is focused on production methods that (1) produce the best image quality for the lowest cost, (2) provide accurate and repeatable results at any depth over time, and (3) utilize off-the-shelf (OTS) stitching software that allows accurate results that can be reviewed in the field. This structured approach to image acquisition integrated with the OTS grid-oriented stitching software produces highly accurate benthic image maps. C1 [Penland, Laurie] Smithsonian Inst, Sci Diving Program, Washington, DC 20560 USA. [Brooks, Barrett] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Ochoa, Edgardo] Smithsonian Inst, Smithsonian Trop Res Inst, Panama City, Panama. RP Penland, L (reprint author), Smithsonian Inst, Sci Diving Program, Washington, DC 20560 USA. EM penlandl@si.edu FU Smithsonian Institution's Office of the Undersecretary for Science; Smithsonian Scientific Diving Program FX Funding of this project was provided by the Smithsonian Institution's Office of the Undersecretary for Science and the Smithsonian Scientific Diving Program. Team members include Barrett Brooks, Bill Ferrell, Amanda Feuerstein, Nancy Knowlton, Matt Leray, Edgardo Ochoa, Alex Penland, and Dane Penland. Logistical support provided by Keys Marine Lab, Smithsonian Caribbean Coral Reef Ecosystems, and NOAA Florida Keys National Marine Sanctuary. All photographs are by Laurie Penland unless otherwise noted. NR 30 TC 0 Z9 0 U1 1 U2 5 PU MARINE TECHNOLOGY SOC INC PI COLUMBIA PA 5565 STERRETT PLACE, STE 108, COLUMBIA, MD 21044 USA SN 0025-3324 EI 1948-1209 J9 MAR TECHNOL SOC J JI Mar. Technol. Soc. J. PD NOV-DEC PY 2013 VL 47 IS 6 BP 7 EP 15 PG 9 WC Engineering, Ocean; Oceanography SC Engineering; Oceanography GA 276AY UT WOS:000328721700002 ER PT J AU McSween, HY Binzel, RP De Sanctis, MC Ammannito, E Prettyman, TH Beck, AW Reddy, V Le Corre, L Gaffey, MJ McCord, TB Raymond, CA Russell, CT AF McSween, Harry Y., Jr. Binzel, Richard P. De Sanctis, M. Cristina Ammannito, Eleonora Prettyman, Thomas H. Beck, Andrew W. Reddy, Vishnu Le Corre, Lucille Gaffey, Michael J. McCord, Thomas B. Raymond, Carol A. Russell, Christopher T. CA Dawn Sci Team TI Dawn; the Vesta-HED connection; and the geologic context for eucrites, diogenites, and howardites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ASTEROID 4 VESTA; EARLY SOLAR-SYSTEM; PARENT BODY; MN-53-CR-53 SYSTEMATICS; BASALTIC ACHONDRITES; IMPACT SPHERULES; ORTHO-PYROXENE; DARK MATERIAL; METEORITES; ORIGIN AB The Dawn mission has provided new evidence strengthening the identification of asteroid Vesta as the parent body of the howardite, eucrite, and diogenite (HED) meteorites. The evidence includes Vesta's petrologic complexity, detailed spectroscopic characteristics, unique space weathering, diagnostic geochemical abundances and neutron absorption characteristics, chronology of surface units and impact history, occurrence of exogenous carbonaceous chondritic materials in the regolith, and dimensions of the core, all of which are consistent with HED observations and constraints. Global mapping of the distributions of HED lithologies by Dawn cameras and spectrometers provides the missing geologic context for these meteorites, thereby allowing tests of petrogenetic models and increasing their scientific value. C1 [McSween, Harry Y., Jr.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. [McSween, Harry Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Binzel, Richard P.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [De Sanctis, M. Cristina; Ammannito, Eleonora] Ist Nazl Astrofis, Ist Astrofis & Planetol Spaziali, Rome, Italy. [Prettyman, Thomas H.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Beck, Andrew W.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Reddy, Vishnu; Le Corre, Lucille] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Gaffey, Michael J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. [McCord, Thomas B.] Bear Fight Inst, Winthrop, WA 98862 USA. [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP McSween, HY (reprint author), Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. EM mcsween@utk.edu RI Beck, Andrew/J-7215-2015; OI Beck, Andrew/0000-0003-4455-2299; De Sanctis, Maria Cristina/0000-0002-3463-4437; Prettyman, Thomas/0000-0003-0072-2831; Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932 FU NASA's Discovery Program; NASA's Dawn at Vesta Participating Scientists Program; Italian Space Agency; Max Planck Society; German Space Agency (DLR); Planetary Science Institute under Jet Propulsion Laboratory, California Institute of Technology FX This work was funded by NASA's Discovery Program through a contract to the University of California, Los Angeles, by NASA's Dawn at Vesta Participating Scientists Program, by the Italian Space Agency, by the Max Planck Society and German Space Agency (DLR), and by the Planetary Science Institute under contract with the Jet Propulsion Laboratory, California Institute of Technology. We appreciate reviews by K. Keil, G. Consolmagno, and an anonymous reviewer. NR 113 TC 43 Z9 44 U1 4 U2 25 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 NOV PY 2013 VL 48 IS 11 BP 2090 EP 2104 DI 10.1111/maps.12108 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300003 ER PT J AU Beck, AW McCoy, TJ Sunshine, JM Viviano, CE Corrigan, CM Hiroi, T Mayne, RG AF Beck, Andrew W. McCoy, Timothy J. Sunshine, Jessica M. Viviano, Christina E. Corrigan, Catherine M. Hiroi, Takahiro Mayne, Rhiannon G. TI Challenges in detecting olivine on the surface of 4 Vesta SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID HED PARENT BODY; REFLECTANCE SPECTRA; DIOGENITES; METEORITES; DIVERSITY; PYROXENES; HOWARDITE; MIXTURES; EUCRITE; ORIGIN AB Identifying and mapping olivine on asteroid 4 Vesta are important components to understanding differentiation on that body, which is one of the objectives of the Dawn mission. Harzburgitic diogenites are the main olivine-bearing lithology in the howardite-eucrite-diogenite (HED) meteorites, a group of samples thought to originate from Vesta. Here, we examine all the Antarctic harzburgites and estimate that, on scales resolvable by Dawn, olivine abundances in putative harzburgite exposures on the surface of Vesta are likely at best in the 10-30% range, but probably lower due to impact mixing. We examine the visible/near-infrared spectra of two harzburgitic diogenites representative of the 10-30% olivine range and demonstrate that they are spectrally indistinguishable from orthopyroxenitic diogenites, the dominant diogenitic lithology in the HED group. This suggests that the visible/near-infrared spectrometer onboard Dawn (VIR) will be unable to resolve harzburgites from orthopyroxenites on the surface of Vesta, which may explain the current lack of identification of harzburgitic diogenite on Vesta. C1 [Beck, Andrew W.; McCoy, Timothy J.; Corrigan, Catherine M.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Sunshine, Jessica M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Viviano, Christina E.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Hiroi, Takahiro] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Mayne, Rhiannon G.] Texas Christian Univ, Dept Geol, Ft Worth, TX 76129 USA. RP Beck, AW (reprint author), Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM becka@si.edu RI Viviano-Beck, Christina/F-3942-2015; Beck, Andrew/J-7215-2015 OI Viviano-Beck, Christina/0000-0003-1601-2105; Beck, Andrew/0000-0003-4455-2299 FU NASA Dawn at Vesta Participating Scientist Grant FX We thank D. W. Mittlefehldt, B. J. Tkalcec, and K. Righter for providing images and information about harzburgitic diogenite thin sections; the Antarctic Search for Meteorites Program for recovering the samples studied here; and V. Reddy for opx/olivine mixture compositional data. This manuscript was improved by comments from the AE, D. W. Mittlefehldt, and reviews by E. Cloutis and an anonymous reviewer. Funding was provided by a NASA Dawn at Vesta Participating Scientist Grant to T. J. McCoy. NR 36 TC 19 Z9 20 U1 1 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 2013 VL 48 IS 11 BP 2155 EP 2165 DI 10.1111/maps.12160 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300006 ER PT J AU Prettyman, TH Mittlefehldt, DW Yamashita, N Beck, AW Feldman, WC Hendricks, JS Lawrence, DJ McCoy, TJ McSween, HY Peplowski, PN Reedy, RC Toplis, MJ Le Corre, L Mizzon, H Reddy, V Titus, TN Raymond, CA Russell, CT AF Prettyman, Thomas H. Mittlefehldt, David W. Yamashita, Naoyuki Beck, Andrew W. Feldman, William C. Hendricks, John S. Lawrence, David J. McCoy, Timothy J. McSween, Harry Y. Peplowski, Patrick N. Reedy, Robert C. Toplis, Michael J. Le Corre, Lucille Mizzon, Hugau Reddy, Vishnu Titus, Timothy N. Raymond, Carol A. Russell, Christopher T. TI Neutron absorption constraints on the composition of 4 Vesta SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID LUNAR PROSPECTOR; GAMMA-RAY; DAWN MISSION; PARENT BODY; MARS ODYSSEY; WATER-ICE; EPITHERMAL NEUTRONS; HED METEORITES; DARK MATERIAL; SOUTH-POLE AB Global maps of the macroscopic thermal neutron absorption cross section of Vesta's regolith by the Gamma Ray and Neutron Detector (GRaND) on board the NASA Dawn spacecraft provide constraints on the abundance and distribution of Fe, Ca, Al, Mg, and other rock-forming elements. From a circular, polar low-altitude mapping orbit, GRaND sampled the regolith to decimeter depths with a spatial resolution of about 300km. At this spatial scale, the variation in neutron absorption is about seven times lower than that of the Moon. The observed variation is consistent with the range of absorption for howardite whole-rock compositions, which further supports the connection between Vesta and the howardite, eucrite, and diogenite meteorites. We find a strong correlation between neutron absorption and the percentage of eucritic materials in howardites and polymict breccias, which enables petrologic mapping of Vesta's surface. The distribution of basaltic eucrite and diogenite determined from neutron absorption measurements is qualitatively similar to that indicated by visible and near infrared spectroscopy. The Rheasilvia basin and ejecta blanket has relatively low absorption, consistent with Mg-rich orthopyroxene. Based on a combination of Fe and neutron absorption measurements, olivine-rich lithologies are not detected on the spatial scales sampled by GRaND. The sensitivity of GRaND to the presence of mantle material is described and implications for the absence of an olivine signature are discussed. High absorption values found in Vesta's dark hemisphere, where exogenic hydrogen has accumulated, indicate that this region is richer in basaltic eucrite, representative of Vesta's ancient upper crust. C1 [Prettyman, Thomas H.; Yamashita, Naoyuki; Feldman, William C.; Reedy, Robert C.; Le Corre, Lucille; Reddy, Vishnu] Planetary Sci Inst, Tucson, AZ 85719 USA. [Mittlefehldt, David W.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Beck, Andrew W.; McCoy, Timothy J.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Hendricks, John S.] TechSource Inc, Los Alamos, NM 87544 USA. [Lawrence, David J.; Peplowski, Patrick N.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [McSween, Harry Y.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. [McSween, Harry Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Toplis, Michael J.; Mizzon, Hugau] Univ Toulouse, CNRS, Observ Midi Pyrenees, IRAP,UMR 5277, Toulouse, France. [Le Corre, Lucille; Reddy, Vishnu] Max Planck Inst Solar Syst Res, Lindau, Germany. [Titus, Timothy N.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP Prettyman, TH (reprint author), Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA. EM prettyman@psi.edu RI Beck, Andrew/J-7215-2015; Peplowski, Patrick/I-7254-2012; Lawrence, David/E-7463-2015; OI Beck, Andrew/0000-0003-4455-2299; Peplowski, Patrick/0000-0001-7154-8143; Lawrence, David/0000-0002-7696-6667; Reedy, Robert/0000-0002-2189-1303; Prettyman, Thomas/0000-0003-0072-2831; Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932 FU NASA Jet Propulsion Laboratory; NASA Discovery Program; NASA Dawn at Vesta Participating Scientist Program FX This work was carried out under contract with the NASA Jet Propulsion Laboratory. GRaND is operated by the Planetary Science Institute. The Dawn mission is led by the University of California, Los Angeles under the auspices of the NASA Discovery Program. Funding for U.S. Participating Scientists was provided by the NASA Dawn at Vesta Participating Scientist Program. Contributions by members of the Dawn Science, Spacecraft and Instrument-Operations teams at JPL and UCLA, including Carol Polanskey, Steve Joy, Joe Mafi, and Marc Rayman, are greatly appreciated. In addition, we are grateful for technical support provided by Joe Makowski and Mike Violet of Orbital Sciences Corporation. GRaND data are archived by the NASA Planetary Data System Small Bodies Node. Comments by the reviewers, Brad Jolliff and Josef Masarik, and the associate editor, Ingo Leya, helped improve the manuscript. Tomo Usui provided a portion of the HED whole-rock compositions used in this study. NR 108 TC 20 Z9 20 U1 1 U2 10 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 NOV PY 2013 VL 48 IS 11 BP 2211 EP 2236 DI 10.1111/maps.12244 PG 26 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300010 ER PT J AU Yamashita, N Prettyman, TH Mittlefehldt, DW Toplis, MJ McCoy, TJ Beck, AW Reedy, RC Feldman, WC Lawrence, DJ Peplowski, PN Forni, O Mizzon, H Raymond, CA Russell, CT AF Yamashita, N. Prettyman, T. H. Mittlefehldt, D. W. Toplis, M. J. McCoy, T. J. Beck, A. W. Reedy, R. C. Feldman, W. C. Lawrence, D. J. Peplowski, P. N. Forni, O. Mizzon, H. Raymond, C. A. Russell, C. T. TI Distribution of iron on Vesta SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID GAMMA-RAY SPECTROMETER; LUNAR-SURFACE; DAWN MISSION; MARS ODYSSEY; GLOBAL DISTRIBUTION; NEUTRON DETECTOR; HED METEORITES; DARK MATERIAL; PROSPECTOR; SPECTRA AB We have completed a mapping study of 7.6MeV gamma rays produced by neutron capture by Fe at the surface of the main belt asteroid 4 Vesta as measured by the bismuth germanate scintillator of the Gamma Ray and Neutron Detector (GRaND) on the Dawn spacecraft. The procedures used to determine Fe counting rates are presented, along with a global map, constituting the necessary initial step to quantify Fe abundances. While the final calibration of orbital data to absolute concentrations has not been determined, the range of fully corrected Fe counting rates is compared with that of Fe in howardites. We find that the global distribution of corrected Fe counting rates is generally consistent with mineralogy and composition determined independently by other instruments on the Dawn spacecraft, including measurements of pyroxene absorption bands by the Visible and Infrared Spectrometer and Framing Camera, and an index of diogenitic materials provided by neutron absorption measurements by GRaND. In addition, there is a distinctive low Fe region in the western hemisphere that was not reported by reflectance or optical observations, possibly indicating the presence of a cumulate eucrite component in Vesta's regolith. C1 [Yamashita, N.; Prettyman, T. H.; Reedy, R. C.; Feldman, W. C.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Mittlefehldt, D. W.] NASA, Astromat Res Off, Johnson Space Ctr, Houston, TX 77058 USA. [Toplis, M. J.; Forni, O.; Mizzon, H.] Univ Toulouse, UPS OMP, Inst Rech Astrophys & Planetol, Toulouse, France. [Toplis, M. J.; Forni, O.; Mizzon, H.] CNRS, IRAP, Toulouse, France. [McCoy, T. J.; Beck, A. W.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Lawrence, D. J.; Peplowski, P. N.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP Yamashita, N (reprint author), Planetary Sci Inst, Tucson, AZ 85719 USA. EM yamashita@psi.edu RI Beck, Andrew/J-7215-2015; Peplowski, Patrick/I-7254-2012; Lawrence, David/E-7463-2015; OI Beck, Andrew/0000-0003-4455-2299; Peplowski, Patrick/0000-0001-7154-8143; Lawrence, David/0000-0002-7696-6667; Reedy, Robert/0000-0002-2189-1303; Prettyman, Thomas/0000-0003-0072-2831 FU NASA Discovery Program Office; JPL; NASA; NASA's Dawn at Vesta Participating Scientist program FX We thank T. Usui and two anonymous reviewers for their valuable comments and suggestions that led to improvements in this manuscript. The Dawn mission is led by the University of California, Los Angeles, and managed by Jet Propulsion Laboratory (JPL) under the auspices of the NASA Discovery Program Office. A portion of this work was carried out by the Planetary Science Institute under contract with JPL, by JPL under contract with NASA, and by NASA's Dawn at Vesta Participating Scientist program. Science experimental data records and housekeeping data acquired by GRaND during Vesta encounter and used in this study are available from NASA's Planetary Data System. NR 61 TC 17 Z9 17 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 NOV PY 2013 VL 48 IS 11 BP 2237 EP 2251 DI 10.1111/maps.12139 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300011 ER PT J AU Peplowski, PN Lawrence, DJ Prettyman, TH Yamashita, N Bazell, D Feldman, WC Le Corre, L McCoy, TJ Reddy, V Reedy, RC Russell, CT Toplis, MJ AF Peplowski, Patrick N. Lawrence, David J. Prettyman, Thomas H. Yamashita, Naoyuki Bazell, Dave Feldman, William C. Le Corre, Lucille McCoy, Timothy J. Reddy, Vishnu Reedy, Robert C. Russell, Chris T. Toplis, Michael J. TI Compositional variability on the surface of 4 Vesta revealed through GRaND measurements of high-energy gamma rays SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID LUNAR PROSPECTOR; DAWN MISSION; MERCURYS SURFACE; NEUTRON-SPECTRA; HED METEORITES; WATER ICE; MOON; SPECTROMETER; MESOSIDERITES; ELEMENTS AB Measurements of the high-energy gamma-ray flux emanating from asteroid 4 Vesta by the Dawn Gamma-Ray and Neutron Detector (GRaND) have revealed variability in the near-surface elemental composition of the Vestan surface. These observations are consistent with the presence of large (8x10(4)km(2)) regions with distinct, HED-like elemental compositions. The results agree broadly with other global measurements, such as the macroscopic neutron absorption cross section and spectral reflectance-derived mineralogic maps. Two distinct regions with eucrite-like elemental compositions have been identified, the first located primarily within the Lucaria and Marcia quadrangles and the second within Oppia quadrangle. The former region is collocated with some of the oldest, most heavily cratered terrain on Vesta. The interior of the 500km diameter Rheasilvia impact basin is found to have a composition that is consistent with diogenite-like material. Taken together, these observations support the hypothesis that Vesta's original crust was composed of basaltic outflows in the form of eucritic-like material and that the Rheasilvia-basin-forming impact exposed lower-crustal, diogenite-like material. These measurements also constrain the maximum amount of mesosiderite-like material to <10% for each 15x15 degrees surface element. C1 [Peplowski, Patrick N.; Lawrence, David J.; Bazell, Dave] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Prettyman, Thomas H.; Yamashita, Naoyuki; Feldman, William C.; Le Corre, Lucille; Reddy, Vishnu; Reedy, Robert C.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Le Corre, Lucille; Reddy, Vishnu] Max Planck Inst Solar Syst Res, Lindau, Germany. [McCoy, Timothy J.] Smithsonian Inst, Washington, DC 20560 USA. [Russell, Chris T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Toplis, Michael J.] Univ Toulouse, Observ Midi Pyrenees, UMR 5527, Inst Rech Astrophys & Planetol, Toulouse, France. RP Peplowski, PN (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM patrick.peplowski@jhuapl.edu RI Peplowski, Patrick/I-7254-2012; Lawrence, David/E-7463-2015; OI Peplowski, Patrick/0000-0001-7154-8143; Lawrence, David/0000-0002-7696-6667; Reedy, Robert/0000-0002-2189-1303; Reddy, Vishnu/0000-0002-7743-3491; Prettyman, Thomas/0000-0003-0072-2831; Le Corre, Lucille/0000-0003-0349-7932 FU NASA Discovery Program Office; Dawn at Vesta Participating Scientist Program FX The Dawn mission is led by the University of California, Los Angeles, and managed by the NASA Jet Propulsion Laboratory under the auspices of the NASA Discovery Program Office. The work of P. N. Peplowski, D. J. Lawrence, D. Bazell, and R. C. Reedy was funded by the Dawn at Vesta Participating Scientist Program. We thank Larry Nittler, Lucy Lim, and an anonymous reviewer for providing thoughtful reviews that greatly improved this manuscript. Dawn data are archived with the NASA Planetary Data System. NR 54 TC 13 Z9 13 U1 3 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 2013 VL 48 IS 11 BP 2252 EP 2270 DI 10.1111/maps.12176 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300012 ER PT J AU Toplis, MJ Mizzon, H Monnereau, M Forni, O McSween, HY Mittlefehldt, DW McCoy, TJ Prettyman, TH De Sanctis, MC Raymond, CA Russell, CT AF Toplis, M. J. Mizzon, H. Monnereau, M. Forni, O. McSween, H. Y. Mittlefehldt, D. W. McCoy, T. J. Prettyman, T. H. De Sanctis, M. C. Raymond, C. A. Russell, C. T. TI Chondritic models of 4 Vesta: Implications for geochemical and geophysical properties SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID METEORITE PARENT BODIES; EARLY SOLAR-SYSTEM; MELT MIGRATION; CORE FORMATION; DIFFERENTIATED ASTEROIDS; PARTITION-COEFFICIENTS; EUCRITIC METEORITES; PHASE-RELATIONS; SILICATE MELTS; DIOGENITES AB Simple mass-balance and thermodynamic constraints are used to illustrate the potential geochemical and geophysical diversity of a fully differentiated Vesta-sized parent body with a eucrite crust (e.g., core size and density, crustal thickness). The results of this analysis are then combined with data from the howardite-eucrite-diogenite (HED) meteorites and the Dawn mission to constrain Vesta's bulk composition. Twelve chondritic compositions are considered, comprising seven carbonaceous, three ordinary, and two enstatite chondrite groups. Our analysis excludes CI and LL compositions as plausible Vesta analogs, as these are predicted to have a negative metal fraction. Second, the MELTS thermodynamic calculator is used to show that the enstatite chondrites, the CV, CK and L-groups cannot produce Juvinas-like liquids, and that even for the other groups, depletion in sodium is necessary to produce liquids of appropriate silica content. This conclusion is consistent with the documented volatile-poor nature of eucrites. Furthermore, carbonaceous chondrites are predicted to have a mantle too rich in olivine to produce typical howardites and to have Fe/Mn ratios generally well in excess of those of the HEDs. On the other hand, an Na-depleted H-chondrite bulk composition is capable of producing Juvinas-like liquids, has a mantle rich enough in pyroxene to produce abundant howardite/diogenite, and has a Fe/Mn ratio compatible with eucrites. In addition, its predicted bulk-silicate density is within 100kgm(-3) of solutions constrained by data of the Dawn mission. However, oxidation state and oxygen isotopes are not perfectly reproduced and it is deduced that bulk Vesta may contain approximately 25% of a CM-like component. Values for the bulk-silicate composition of Vesta and a preliminary phase diagram are proposed. C1 [Toplis, M. J.; Mizzon, H.; Monnereau, M.; Forni, O.] Univ Toulouse, Observ Midi Pyrenees, UMR 5277, IRAP,CNRS, F-31400 Toulouse, France. [McSween, H. Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Mittlefehldt, D. W.] NASA, Astromat Res Off, Johnson Space Ctr, Houston, TX 77058 USA. [McCoy, T. J.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. [Prettyman, T. H.] Planetary Sci Inst, Tucson, AZ 85719 USA. [De Sanctis, M. C.] Ist Astrofis & Planetol Spaziali INAF, I-00133 Rome, Italy. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP Toplis, MJ (reprint author), Univ Toulouse, Observ Midi Pyrenees, UMR 5277, IRAP,CNRS, 14 Ave E Belin, F-31400 Toulouse, France. EM mtoplis@irap.omp.eu RI De Sanctis, Maria Cristina/G-5232-2013; OI De Sanctis, Maria Cristina/0000-0002-3463-4437; Forni, Olivier/0000-0001-6772-9689; Prettyman, Thomas/0000-0003-0072-2831 FU Centre National d'Etudes Spatiales (CNES) FX Enlightening discussions with J.-A. Barrat and formal reviews by H. Takeda and G. J. Taylor are gratefully acknowledged. MT thanks the Centre National d'Etudes Spatiales (CNES) for their financial support, which enabled participation in this work and the Dawn mission. NR 92 TC 19 Z9 19 U1 1 U2 17 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 NOV PY 2013 VL 48 IS 11 BP 2300 EP 2315 DI 10.1111/maps.12195 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 273NY UT WOS:000328543300015 ER PT J AU McGovern, PJ Rumpf, ME Zimbelman, JR AF McGovern, Patrick J. Rumpf, M. Elise Zimbelman, James R. TI The influence of lithospheric flexure on magma ascent at large volcanoes on Venus SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE volcanoes; flexure; stress; edifices; coronae ID IMPACT CRATER DENSITIES; EISTLA REGIO; GLOBAL DISTRIBUTION; RESERVOIR FAILURE; MECHANICAL MODELS; CORONA FORMATION; EVOLUTION; MANTLE; STRESSES; BENEATH AB Large volcanoes on Venus exert large vertical loads on the lithosphere, which responds by deflecting downward. Stresses induced by this lithospheric flexure can have a strong influence on magma ascent pathways from the mantle source region to the surface. Here we propose that flexural stresses exert control over the shapes of volcanic edifices on Venus, applying criteria for magma ascent expressed in terms of stress orientations (can vertical dikes form?) and gradients (is magma squeezed upward or downward in a vertical dike?) to determine favored magma ascent paths and locations. For conical edifices emplaced on lithosphere with high elastic thickness T-e, (e.g., > 40 km) both sets of magma ascent criteria are satisfied over the entire lithosphere, allowing essentially unimpeded ascent of magma to the surface and the formation of relatively steep edifices. However, for lower values of T-e, high adverse stress gradients tend to cut off magma ascent beneath the summit, instead favoring lateral transport of magma at depth to distal regions with gentler stress gradients, resulting in domical edifice shapes. At the lowest values of T-e (< 10 km), large short-wavelength deflections of the lithosphere tend to produce narrow and widely spaced zones of magma ascent: Such zones may produce annular ridges of volcanic material, thereby generating forms characteristic of a subset of features known as coronae on Venus. Another subset of coronae may form by intrusive-based generation of annular fractures at the edge of the summit region of domical edifices, as proposed for Alba Mons on Mars. C1 [McGovern, Patrick J.] Univ Space Res Assoc, Lunar & Planetary Inst, Houston, TX 77058 USA. [Rumpf, M. Elise] Univ Hawaii, Hawaii Inst Geophys & Planetol, Manoa, HI USA. [Zimbelman, James R.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP McGovern, PJ (reprint author), Univ Space Res Assoc, Lunar & Planetary Inst, Houston, TX 77058 USA. EM mcgovern@lpi.usra.edu OI McGovern, Patrick/0000-0001-9647-3096 FU NASA Planetary Geology and Geophysics (PGG) [NNG05GJ92G, NNX08AL77G, NNX12AO49G] FX We thank Patricia Gregg, an anonymous reviewer, and Associate Editor David Baratoux for helpful comments. This research was supported by NASA Planetary Geology and Geophysics (PG&G) grants NNG05GJ92G, NNX08AL77G, and NNX12AO49G. This is LPI Contribution number 1762. NR 69 TC 4 Z9 4 U1 1 U2 3 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 NOV PY 2013 VL 118 IS 11 BP 2423 EP 2437 DI 10.1002/2013JE004455 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 270YJ UT WOS:000328355300011 ER PT J AU Freitas, CG Dambros, C Camargo, JLC AF Freitas, Cintia Gomes Dambros, Cristian Campana Camargo, Jose Luis TI Changes in seed rain across Atlantic Forest fragments in Northeast Brazil SO ACTA OECOLOGICA-INTERNATIONAL JOURNAL OF ECOLOGY LA English DT Article DE Biodiversity loss; Disturbance; Landscape ecology; Habitat loss ID DISPERSAL LIMITATION; EDGE; EXTINCTION; TREES; BIODIVERSITY; REGENERATION; ASSEMBLAGES; PATTERNS; RATES; SIZE AB The objectives of this study were to characterize the distribution of seeds in remnant fragments of the Atlantic Coastal Forest and to determine whether the species diversity, seed weight, and species composition of plant communities are altered by forest fragmentation. A transect of 100 m was established in the core of each of nine fragments of Atlantic Coastal Forest in a private sugarcane plantation in the state of Alagoas, NE Brazil, and ten seed-traps were distributed at intervals of 10 m each along the transects. For 12 consecutive months seeds were collected, dried, counted, weighed, and identified to species. Seeds were assigned to categories according to their size, dispersal mode, and shade tolerance. Multiple regression models and Mantel correlation tests were used to detect the effects of fragment size, percent forest cover nearby, distance from the source area, and distance from the nearest fragment on species diversity, mean seed weight, and species similarity. Analyses were carried out for all species and for subsets corresponding to each seed category. A total of 21,985 diaspores of 190 species were collected. Most seeds were small, shade-intolerant, and zoochoric, which corroborates other studies of fragmented forest landscapes and reflects the high disturbance levels in isolated forest remnants. Our data indicate that fragmentation processes such as habitat loss can alter species diversity and species composition by reducing habitat availability and increasing fragment isolation. We also found that large-seeded species are more affected by fragment isolation, possibly because their seed dispersers rarely cross non-forested areas between fragments, while zoochoric species are more strongly affected by fragment size and apparently more strongly associated with local edaphic conditions than with distance from seed sources. (C) 2013 Elsevier Masson SAS. All rights reserved. C1 [Freitas, Cintia Gomes] Univ Fed Pernambuco, Grad Program Plant Biol, BR-50670901 Recife, PE, Brazil. [Dambros, Cristian] Univ Vermont, Dept Biol, Burlington, VT 05405 USA. [Campana Camargo, Jose Luis] Smithsonian Trop Res Inst, Natl Inst Amazonian Res, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. RP Freitas, CG (reprint author), Natl Inst Amazonian Res, Grad Program Ecol, Ave Ephigenio Salles 2239, BR-69011970 Manaus, Amazonas, Brazil. EM cintuca@gmail.com; Cristian.Dambros@uvm.edu; zeluiscamargo@gmail.com RI Camargo, Jose Luis/C-3137-2015; Dambros, Cristian/B-5521-2013 OI Dambros, Cristian/0000-0002-5781-7471 FU CNPq (Brazil's National Council of Scientific and Technological Development) [479124/2003-5]; Fundacao Grupo Boticario [0592/20032] FX This work received financial support from CNPq (Brazil's National Council of Scientific and Technological Development; grant number 479124/2003-5) and the Fundacao Grupo Boticario (grant number 0592/20032). Conservation International Brazil, Centro de Pesquisas Ambientais do Nordeste, and Usina Serra Grande provided logistical support. We thank I. R. Leal for help with theoretical aspects of the study, M. Tabarelli for suggestions on statistical analysis, and M. Oliveira, A. Grillo (in memoriam), F. Melo, and B. Santos for help with seed identification. NR 44 TC 2 Z9 2 U1 1 U2 30 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 NOV PY 2013 VL 53 BP 49 EP 55 DI 10.1016/j.actao.2013.08.005 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 263KD UT WOS:000327806600006 ER PT J AU Tonra, CM Marra, PP Holberton, RL AF Tonra, Christopher M. Marra, Peter P. Holberton, Rebecca L. TI Experimental and observational studies of seasonal interactions between overlapping life history stages in a migratory bird SO HORMONES AND BEHAVIOR LA English DT Article DE American redstart; Carry-over effects; Departure timing; Migration; Setophaga ruticilla; Testosterone ID WHITE-CROWNED SPARROWS; DARK-EYED JUNCO; EXPERIMENTALLY-ELEVATED TESTOSTERONE; ZONOTRICHIA-LEUCOPHRYS-GAMBELII; STABLE-CARBON ISOTOPES; NONBREEDING SEASON; CLIMATE-CHANGE; HABITAT OCCUPANCY; FOOD AVAILABILITY; SPRING MIGRATION AB Prior to reproduction, migratory animals are at the juxtaposition of three life history stages in which they must finish the non-breeding stage, initiate and complete migration, and prepare for the onset of breeding. However, how these stages interact with one another is not fully understood. We provide evidence that, for migratory birds that begin breeding development prior to departure from non-breeding sites, the level of breeding preparation can drive migration phenology, a critical behavioral determinant of reproductive success. Specifically, male American redstart (Setophaga ruticilla) plasma androgen levels, which increase in males during the period leading into migration, were positively correlated with energetic condition. We empirically tested the hypothesis that elevated androgen simultaneously supports migratory and breeding preparation in a hormone manipulation field experiment. Males with testosterone implants showed advanced preparation for migration and breeding, and ultimately departed on migration earlier than controls. It is assumed that early departure leads to early arrival at breeding areas, which increases breeding success. Collectively, our observational and experimental results demonstrate how overlapping life history stages can interact to influence important components of an individual's fitness. This highlights the critical need for understanding population processes across the full life cycle of an organism to better understand the ecological and evolutionary origins of complex life history events. (C) 2013 Elsevier Inc. All rights reserved. C1 [Tonra, Christopher M.; Holberton, Rebecca L.] Univ Maine, Sch Biol & Ecol, Orono, ME USA. [Tonra, Christopher M.; Marra, Peter P.] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA. RP Tonra, CM (reprint author), Natl Zoo, POB 37012 MRC 5503, Washington, DC 20013 USA. EM TonraC@si.edu RI Tonra, Christopher/B-1620-2013 FU National Science Foundation [0649679, 0717338, 0615701, 1011123]; American Ornithologist Union Student Research Award; American Museum of Natural History Frank M. Chapman Award; Cooper Ornithological Society Joseph Grinnell Student Research Award; Wilson Ornithological Society Louis Agassiz Fuertes Award; Smithsonian Institution FX This work was supported by grants awarded by the National Science Foundation to Marra (0649679, 0717338), Holberton (0615701), and a Doctoral Dissertation Improvement Grant to Tonra (1011123). Additional funds were provided to Tonra by the American Ornithologist Union Student Research Award, the American Museum of Natural History Frank M. Chapman Award, the Cooper Ornithological Society Joseph Grinnell Student Research Award, the Wilson Ornithological Society Louis Agassiz Fuertes Award, and a Pre-doctoral Fellowship from the Smithsonian Institution. The Maine Agricultural and Forest Experimental Station, with funds awarded to Holberton, also helped to support this project. We are grateful to the Petroleum Corporation of Jamaica for permission to conduct this research at the Font Hill Nature Preserve. Colin Studds provided invaluable assistance in the field and with statistical analyses. We wish to thank Brent Horton, Scott Sillett, the Smithsonian Migratory Bird Reading Group, and two anonymous reviewers for comments on an earlier version of this manuscript. We are indebted to all of the dedicated biologists, too numerous to name here, who contributed to data collection for this study. We especially want to thank Frederic Angelier, Nathan Cooper, Rob Dobbs, Jeannine Randall, Sean Rune, and Mark Thomas. NR 65 TC 8 Z9 8 U1 3 U2 27 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0018-506X EI 1095-6867 J9 HORM BEHAV JI Horm. Behav. PD NOV PY 2013 VL 64 IS 5 BP 825 EP 832 DI 10.1016/j.yhbeh.2013.10.004 PG 8 WC Behavioral Sciences; Endocrinology & Metabolism SC Behavioral Sciences; Endocrinology & Metabolism GA 261TO UT WOS:000327687700009 PM 24128687 ER PT J AU Farnsworth, EJ Chu, M Kress, WJ Neill, AK Best, JH Pickering, J Stevenson, RD Courtney, GW VanDyk, JK Ellison, AM AF Farnsworth, Elizabeth J. Chu, Miyoko Kress, W. John Neill, Amanda K. Best, Jason H. Pickering, John Stevenson, Robert D. Courtney, Gregory W. VanDyk, John K. Ellison, Aaron M. TI Next-Generation Field Guides SO BIOSCIENCE LA English DT Article DE species identification; taxonomy; citizen science; Web applications; digital data ID IDENTIFICATION; SCIENCE; COMPUTER AB To conserve species, we must first identify them. Field researchers, land managers, educators, and citizen scientists need up-to-date and accessible tools to identify organisms, organize data, and share observations. Emerging technologies complement traditional, book-form field guides by providing users with a wealth of multimedia data. We review technical innovations of next-generation field guides, including Web-based and stand-alone applications, interactive multiple-access keys, visual-recognition software adapted to identify organisms, species checklists that can be customized to particular sites, online communities in which people share species observations, and the use of crowdsourced data to refine machine-based identification algorithms. Next-generation field guides are user friendly; permit quality control and the revision of data; are scalable to accommodate burgeoning data; protect content and privacy while allowing broad public access; and are adaptable to ever-changing platforms and browsers. These tools have great potential to engage new audiences while fostering rigorous science and an appreciation for nature. C1 [Farnsworth, Elizabeth J.] New England Wild Flower Soc, Framingham, MA USA. [Chu, Miyoko] Cornell Univ, Cornell Lab Ornithol, Ithaca, NY USA. [Kress, W. John] Consortium Understanding & Sustaining, Washington, DC 20560 USA. [Kress, W. John] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. [Neill, Amanda K.] Bot Res Inst Texas, Herbarium, Ft Worth, TX USA. [Best, Jason H.] Bot Res Inst Texas, Ft Worth, TX USA. [Pickering, John] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Stevenson, Robert D.] Univ Massachusetts Boston, Dept Biol, Boston, MA USA. [Courtney, Gregory W.] Iowa State Univ, Iowa State Insect Collect, Ames, IA USA. [VanDyk, John K.] Iowa State Univ, Dept Entomol, Ames, IA USA. [Ellison, Aaron M.] Harvard Univ Harvard Forest, Petersham, MA USA. RP Farnsworth, EJ (reprint author), New England Wild Flower Soc, Framingham, MA USA. EM efarnswo@mtholyoke.edu OI Ellison, Aaron/0000-0003-4151-6081 FU National Science Foundation [0840186, 1010818, 0325867, 9808462, 0111540, 0416835, 1136646]; Smithsonian Institution,; University of Maryland; Ambrose Monell Foundation; Vetlesen Foundation; US Geological Survey; US Department of Energy [DE-FG02-08ER64510]; Columbia University FX Funding for this work was provided by National Science Foundation grants no. 0840186 to EJF; no. 1010818 to MC; no. 0325867 to WJK; no. 9808462, no. 0111540, and no. 0416835 to RDS; and no. 1136646 to AME. We also acknowledge funding from the Smithsonian Institution, Columbia University, and the University of Maryland to WJK; the Ambrose Monell Foundation, the Vetlesen Foundation, and the US Geological Survey to JP; and US Department of Energy grant no. DE-FG02-08ER64510 to AME. MC thanks Jessie Barry at the Cornell Lab of Ornithology for additional information about the Merlin project. WJK thanks the Leafsnap team, including Peter Belhumeur, David Jacobs, Sean White, Ida Lopez, Steve Finer, the people at Finding Species, and many students and volunteers. NR 40 TC 11 Z9 13 U1 3 U2 34 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 NOV PY 2013 VL 63 IS 11 BP 891 EP 899 DI 10.1525/bio.2013.63.11.8 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 257WE UT WOS:000327417700008 ER PT J AU Clay, NA Lucas, J Kaspari, M Kay, AD AF Clay, Natalie A. Lucas, Jane Kaspari, Michael Kay, Adam D. TI Manna from heaven: Refuse from an arboreal ant links aboveground and belowground processes in a lowland tropical forest SO ECOSPHERE LA English DT Article DE biogeochemistry; community structure; detritus; food web; frass; landscape heterogeneity; nutrient subsidies ID RAIN-FOREST; SOIL NUTRIENTS; LITTER DECOMPOSITION; PLANT; HERBIVORY; CANOPY; DYNAMICS; FRASS; RESPONSES; NITROGEN AB Aboveground consumers can shape belowground processes by serving as conduits for resources. Social insects dominate in terms of biomass in tropical forests, but compared to studies on large mammals, or aggregate solitary insects, we know relatively little about the role of social insects as nutrient conduits particularly in complex environments like tropical forests. Social insects like ants in the tropical forest canopy can connect aboveground and belowground food webs by producing a nutrient stream (excreta) from large, long-lived and stationary nests. The excreta, in turn, would create enduring spatial heterogeneity in the forest floor. Here we evaluate this scenario in a lowland Neotropical forest using Azteca trigona, a dominant canopy ant that feeds on honeydew and insects and rains refuse out of its hanging nests onto the leaf litter below. We investigate decomposition rates and detrital communities associated with areas near nests versus 10 m away. Further, we directly test refuse's impact on decomposition and detrital communities in a common garden experiment. Relative to leaf litter, refuse is enriched 7-fold in P, 23-fold in K, and 3-fold in N, all elements shown to limit decomposition in this forest. Accordingly, both artificial substrates and natural leaf litter substrates decomposed over 1.5- and 1.2-fold faster respectively below A. trigona nests and areas under nests supported more invertebrate detritivores and predators compared to controls 10 m away. These decomposition results were replicated in a 6-wk common garden experiment, but the changes in detrital invertebrate composition were not. Canopy ants like A. trigona act as dependable nutritional conduits to patches of the forest floor, transferring significant quantities of aboveground exudates and necromass. The general capacity for such social insect colonies to generate ecosystem heterogeneity remains an open question. C1 [Clay, Natalie A.; Kaspari, Michael] Univ Oklahoma, Dept Biol, Grad Program Ecol & Evolutionary Biol, Norman, OK 73019 USA. [Lucas, Jane; Kay, Adam D.] Univ St Thomas, Dept Biol, St Paul, MN 55105 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama. RP Clay, NA (reprint author), Univ Oklahoma, Dept Biol, Grad Program Ecol & Evolutionary Biol, Norman, OK 73019 USA. EM naclay@ou.edu OI Kaspari, Michael/0000-0002-9717-5768 FU Zoology Department (OU); College of Arts and Sciences (OU); Graduate Student Senate (OU); NSF [DEB 0842038] FX We thank Taylor Zumbusch, David Donsoso, Matt Sweeney, Jon Shik, and Deana Flatt for assistance in the field and D. Flatt and Kendra Tholt for laboratory assistance. We also thank Oris Acevedo and Belkys Jimenez and STRI staff on BCI, Panama, ANAM for permits and OSU soil lab. ZEEB Discussion Group (OU) provided useful comments on earlier versions of the manuscript. Funding was provided by the Zoology Department (OU), the College of Arts and Sciences (OU), Graduate Student Senate (OU), and NSF DEB 0842038 (PI M. Kaspari, A. Kay). NR 63 TC 8 Z9 8 U1 3 U2 33 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD NOV PY 2013 VL 4 IS 11 AR UNSP 141 DI 10.1890/ES13-00220.1 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 257JY UT WOS:000327380900009 ER PT J AU Sessa, JA Callapez, PM Dinis, PA Hendy, AJW AF Sessa, Jocelyn A. Callapez, Pedro M. Dinis, Pedro A. Hendy, Austin J. W. TI PALEOENVIRONMENTAL AND PALEOBIOGEOGRAPHICAL IMPLICATIONS OF A MIDDLE PLEISTOCENE MOLLUSC ASSEMBLAGE FROM THE MARINE TERRACES OF BAIA DAS PIPAS, SOUTHWEST ANGOLA SO JOURNAL OF PALEONTOLOGY LA English DT Article ID CURRENT UPWELLING SYSTEM; CAPE-VERDE ARCHIPELAGO; EASTERN CANARY-ISLANDS; SEA-LEVEL CHANGES; BENGUELA CURRENT; CORAL-REEFS; TECTONIC IMPLICATIONS; VERTICAL MOVEMENTS; LARVAL DEVELOPMENT; STROMBUS-BUBONIUS AB Quaternary raised marine terraces containing the remains of diverse, shallow water marine invertebrate faunas are widespread across the coast of Angola. These deposits and faunas have not been studied in the same detail as contemporaneous features in northwest and southernmost Africa. We analyzed the fossil assemblages and sedimentology of two closely spaced middle Pleistocene marine terrace deposits in Baia das Pipas, southwest Angola. This revealed 46 gastropod and 29 bivalve species, along with scleractinian corals, encrusting bryozoans, polychaete tubes, barnacles, and echinoids. The fauna is characteristic of intertidal and nearshore rocky substrates and sandy soft-bottom habitats. Sedimentological analysis is consistent with faunal data and indicates an upper shoreface paleoenvironment along a gravel coast. This diverse fauna stands out as a rare example of a marine Pleistocene assemblage from over 6,000 km of the West African coast. The assemblage is dominated by extant tropical West African molluscs, including species from the "Senegalese fauna" that colonized northern Africa and beyond during Pleistocene interstadials. Additionally, as along the modern coast of the Namibe Desert, the influence of the cool-water Benguela Current is apparent in the paleofauna by the occurrence of a few temperate species. The distribution and thermal tolerances of extant species identified in the Pipas fauna indicate that this region experienced similar climatic and oceanographic conditions as that of the present during this interstadial. Seasonal temperature varied between similar to 20 and 28 degrees C and resulted from upwelling in this tropical setting. C1 [Sessa, Jocelyn A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Callapez, Pedro M.] Univ Coimbra, Ctr Geofis, P-3001272 Coimbra, Portugal. [Callapez, Pedro M.; Dinis, Pedro A.] Univ Coimbra, Dept Ciencias Terra, P-3001272 Coimbra, Portugal. [Dinis, Pedro A.] Univ Coimbra, Inst Mar, Ctr Mar & Ambiente, P-3001272 Coimbra, Portugal. [Hendy, Austin J. W.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Hendy, Austin J. W.] Smithsonian Trop Res Inst, Ctr Trop Paleontol & Archaeol, Panama City, Panama. RP Sessa, JA (reprint author), Amer Museum Nat Hist, Dept Paleontol, Cent Pk West 79th St, New York, NY 10024 USA. EM jsessa@amnh.org; callapez@dct.uc.pt; pdinis@dct.uc.pt; ahendy@flmnh.ufl.edu RI Callapez Tonicher, Pedro Miguel/L-7089-2014; Dinis, Pedro/D-9867-2016 OI Callapez Tonicher, Pedro Miguel/0000-0002-6493-2208; Dinis, Pedro/0000-0001-7558-7369 FU Smithsonian Institution; Office of the Undersecretary of Science; Centro de Geofisica da Universidade de Coimbra; Instituto do Mar-Centro do Mar e Ambiente, Portugal; Fundacao da Ciencia e Tecnologia; Smithsonian Tropical Research Institute (Panama); Jon A. and Beverly L. Thompson Endowment, Florida Museum of Natural History FX We are grateful to Instituto Politecnico Superior Tundavala in Lubango, Angola, and specifically to C. Ribeiro, for assistance during the weeks of field research and a cartography field course for MS students in the Namibe-Bentiaba coastal region. Our highest gratitude goes to J. Huvi and to the Katyavala Bwila University of Benguela and the Museu Arqueologico de Benguela, Angola for logistic support, including the curation of the studied collections. We are appreciative of D. Jones conducting strontium isotope analyses. This manuscript was improved by the detailed and throughtful comments of S. Gofas and M. Taviani. This research was supported by a Smithsonian Institution Fellowship, funded by the Office of the Undersecretary of Science, to JAS and the Centro de Geofisica da Universidade de Coimbra and the Instituto do Mar-Centro do Mar e Ambiente, Portugal, both research units financed by Fundacao da Ciencia e Tecnologia. JAS is grateful for the funding and support of G. Hunt and L. C. Ivany; AH acknowledges the funding and support of C. Jaramillo, the Smithsonian Tropical Research Institute (Panama), and the Jon A. and Beverly L. Thompson Endowment, Florida Museum of Natural History. This is Paleobiology Database official publication no. 183. NR 251 TC 3 Z9 3 U1 0 U2 3 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 NOV PY 2013 VL 87 IS 6 BP 1016 EP 1040 DI 10.1666/12-119 PG 25 WC Paleontology SC Paleontology GA 257BT UT WOS:000327359000005 ER PT J AU Wendler, JE Wendler, I Huber, BT AF Wendler, Jens E. Wendler, Ines Huber, Brian T. TI REVISION AND EVALUATION OF THE SYSTEMATIC AFFINITY OF THE CALCITARCH GENUS PITHONELLA BASED ON EXQUISITELY PRESERVED TURONIAN MATERIAL FROM TANZANIA SO JOURNAL OF PALEONTOLOGY LA English DT Article ID CALCAREOUS DINOFLAGELLATE CYSTS; THORACOSPHAERA-HEIMII DINOPHYCEAE; STABLE OXYGEN; BIOSTRATIGRAPHY; RECONSTRUCTION; BIOMINERALIZATION; LITHOSTRATIGRAPHY; CHEMOSTRATIGRAPHY; PALEOECOLOGY; STRATIGRAPHY AB Extraordinarily well-preserved pithonellid microfossils (calcitarchs, "calcispheres") from the Turonian (upper Cretaceous) of Tanzania reveal previously unknown morphological traits, crystallographic patterns, and chemical signatures, providing new insight to this enigmatic group of microfossils. Using combined transmitted-reflected light microscopy, scanning electron microscope imagery, electron microprobe elemental analysis and stable isotope geochemistry, the present study reveals four new aspects of the genus Pithonella, notably, the following. An affinity with cyst-forming organisms, potentially the dinoflagellates, is indicated by the presence of a hatch opening and corresponding operculum. The pristine outer wall architecture consists of thin, smooth shingle-shaped plates with regular rows of slit-shaped pores and an apical sub-angular or circular pore. This primary surface pattern is significantly different from previous descriptions of an outer wall consisting a "parquet-shaped" prismatic crystal rows; this latter surface pattern is formed by secondary overgrowth. The crystallographic pattern of the inner wall is crypto-crystalline. Unaltered pithonellids reveal a calcite chemistry characterized by comparably high Mg-contents, relatively enriched stable carbon isotope values, and stable oxygen values indicating a surface water habitat. Based on these previously unseen traits, the diagnosis of the genus Pithonella is emended. A new species, Pithonella diconica, is described from the lower-middle Turonian sediments of Tanzania. C1 [Wendler, Jens E.; Wendler, Ines; Huber, Brian T.] NMNH, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Wendler, Jens E.; Wendler, Ines] Univ Bremen, Dept Geosci, D-28334 Bremen, Germany. RP Wendler, JE (reprint author), NMNH, Smithsonian Inst, Dept Paleobiol, POB 37012, Washington, DC 20013 USA. EM wendler@uni-bremen.de FU German Science Foundation [WE 4587/1-1]; National Science Foundation [NSF EAR 0641956]; Smithsonian Institution FX This research was funded by the German Science Foundation (grant WE 4587/1-1), National Science Foundation (NSF EAR 0641956) and the Smithsonian Institution's Charles Walcott Fund and Scholarly Studies Program. We thank the Tanzania Petroleum Development Corporation, and particularly Dr. J. Singano, for logistical support and the Tanzania Commission for Science and Technology for permission to drill. J. Wingerath, S. Whittaker, A. Logan, T. Rose (Smithsonian Institution) are acknowledged for technical assistance. KG. MacLeod (University of Missouri) performed stable isotope measurements. M. Kirsch provided culture material and gave perspectives and comparisons with recent dinoflagellates. We acknowledge inspiring discussions with H. Keupp, G. Versteegh, and H. Willems. We thank S. Meier, M. Streng and M. Head for insightful reviews and fruitful communication that strongly improved the manuscript. NR 83 TC 7 Z9 7 U1 0 U2 6 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 NOV PY 2013 VL 87 IS 6 BP 1077 EP 1106 DI 10.1666/12-121 PG 30 WC Paleontology SC Paleontology GA 257BT UT WOS:000327359000010 ER PT J AU Geiger, M Wilson, LAB Costeur, L Sanchez, R Sanchez-Villagra, MR AF Geiger, M. Wilson, L. A. B. Costeur, L. Sanchez, R. Sanchez-Villagra, M. R. TI DIVERSITY AND BODY SIZE IN GIANT CAVIOMORPHS (RODENTIA) FROM THE NORTHERN NEOTROPICS-A STUDY OF FEMORAL VARIATION SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID BONE-DENSITY; EXTINCT MAMMALS; TERRESTRIAL; ADAPTATIONS; VENEZUELA; MASS AB New discoveries of numerous fossil femora from giant caviomorph rodents from the Miocene of Venezuela and a specimen of a Miocene giant rodent from Trinidad in the collections of the Naturhistorisches Museum in Basel made possible the first examination of taxonomic, ontogenetic, and functional variation in these animals. We provide comparisons of femoral shape, metrics, and growth (epiphyseal closure), finding that four morphotypes are distinguishable based largely on degrees of robustness or gracility. This indicates that the diversity of giant caviomorphs was larger than previously known; Phoberomys pattersoni was not the only giant caviomorph that inhabited the Miocene of the northern Neotropics. The study of cortical cross-sectional area of fossils serves to estimate the body mass for two giant caviomorphs at 420-580kg. The first description of patterns of bone microstructure in three fossil giant caviomorph femora reveals similarities to extant rodents: absence of Haversian tissue and presence of layers of lamellar followed by reticular-like bone. C1 [Geiger, M.] Univ Zurich, Palaontol Inst & Museum, CH-8006 Zurich, Switzerland. [Wilson, L. A. B.] Univ New S Wales, Sch Biol Earth & Environm Sci, Kensington, NSW 2052, Australia. [Costeur, L.] Nat Hist Museum Basel, CH-4001 Basel, Switzerland. [Sanchez, R.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Sanchez-Villagra, M. R.] Palaontol Inst & Museum, CH-8006 Zurich, Switzerland. RP Sanchez-Villagra, MR (reprint author), Palaontol Inst & Museum, Karl Schmid Str 4, CH-8006 Zurich, Switzerland. EM madeleine.geiger@pim.uzh.ch; laura.wilson@unsw.edu.au; loic.costeur@bs.ch; rodolfosanchez128@hotmail.com; m.sanchez@pim.uzh.ch RI Wilson, Laura/A-4881-2012 OI Wilson, Laura/0000-0002-3779-8277 FU Swiss National Fund [3100A0-133032/1]; Forschungskredit of the University of Zurich [3771]; Japanese Society for the Promotion of Science [PE10075] FX This work was supported by the Swiss National Fund (3100A0-133032/1) to M. R. S.-V. It would not have been possible without the support of O. Aguilera in the laboratory and in the field. We thank all institutions and colleagues who supported us with help and material, and especially C. Kolb and T. Scheyer for their advice and mentoring in our study of paleohistology. We further thank the Alcaldia de Urumaco, Estado Falcon (A. C. M. Perozo, encargado J. Hernandez), for the kind permission to examine their collections and J. X. Samuels and an anonymous reviewer for constructive suggestions, which served to improve the manuscript. L. A. B. W. was supported by Forschungskredit of the University of Zurich (3771) and the Japanese Society for the Promotion of Science (PE10075). NR 49 TC 5 Z9 5 U1 1 U2 6 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD NOV 1 PY 2013 VL 33 IS 6 BP 1449 EP 1456 DI 10.1080/02724634.2013.780952 PG 8 WC Paleontology SC Paleontology GA 251XA UT WOS:000326965500016 ER PT J AU Benamati, L Sozzetti, A Santos, NC Latham, DW AF Benamati, L. Sozzetti, A. Santos, N. C. Latham, D. W. TI A Combined Astrometric and Spectroscopic Study of Metal-Poor Binaries SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE Stars ID BROWN DWARF; STARS; MULTIPLICITY; COMPANIONS; PLANETS; SEARCH; SAMPLE; HIRES AB In this work we present a study of binary systems in a metal-poor sample of solar type stars. The stars analyzed were rejected from two planet search samples because they were found to be binaries. Using available radial velocity and Hipparcos astrometric data, we apply different methods to find, for every binary system, a possible range of solutions for the mass of the companion and its orbital period. In one case we find that the solution depends on the Hipparcos data used: the old and new reductions give different results. Some candidate low-mass companions are found, including some close to the brown dwarf regime. C1 [Benamati, L.; Santos, N. C.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Benamati, L.; Santos, N. C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4150762 Oporto, Portugal. [Sozzetti, A.] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, Italy. [Latham, D. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Benamati, L (reprint author), Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Oporto, Portugal. EM Lisa.Benamati@astro.up.pt RI Santos, Nuno/E-9957-2011; OI Santos, Nuno/0000-0003-4422-2919; Sozzetti, Alessandro/0000-0002-7504-365X FU Gaia Research for European Astronomy Training (GREAT-ITN) Marie Curie network; European Union [264895]; European Research Council/European Community [239953]; Investigador FCT; Fundacao para a Ciencia e a Tecnologia (FCT)/MCTES (Portugal); Fundacao para a Ciencia e a Tecnologia (FCT)/POPH/FSE (EC) FX This work was supported by the Gaia Research for European Astronomy Training (GREAT-ITN) Marie Curie network, funded through the European Union Seventh Framework Programme ([FP7/2007-2013]) under grant agreement number 264895). This work was supported in part by the European Research Council/European Community under the FP7 through Starting Grant agreement number 239953. NCS also acknowledges the support in the form of a Investigador FCT contract funded by Fundacao para a Ciencia e a Tecnologia (FCT)/MCTES (Portugal) and POPH/FSE (EC). NR 27 TC 2 Z9 2 U1 0 U2 1 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 NOV 1 PY 2013 VL 125 IS 933 BP 1315 EP 1328 DI 10.1086/674147 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262DG UT WOS:000327713700004 ER PT J AU Wozniak, RH Santiago-Blay, JA AF Wozniak, Robert H. Santiago-Blay, Jorge A. TI TROUBLE AT TYSON ALLEY: James Mark Baldwin's Arrest in a Baltimore Bordello SO HISTORY OF PSYCHOLOGY LA English DT Article DE James Mark Baldwin; Johns Hopkins University; prostitution; scandal; resignation ID BALDWIN,JAMES,MARK; PSYCHOLOGY; HISTORY AB In June 1908, James Mark Baldwin, then Professor of Psychology and Philosophy at Johns Hopkins University and at the pinnacle of his career, was arrested in a Baltimore house of prostitution. Although he insisted on both his legal and moral innocence and all legal charges against him were dismissed, the threat of scandal led Hopkins authorities to demand Baldwin's resignation and Baldwin to remove himself and his family permanently to France. While this is one of the most notorious events in the early history of American psychology, almost nothing has been known about the incident itself, because both Baldwin and Hopkins took great pains to keep these details private. Based on court records, contemporary newspaper accounts, and archival materials in the Presidential Records at Hopkins and elsewhere, it is now possible to reconstruct the events of 1908 and their aftermath in detail. This article describes these occurrences; places them in the context of Baldwin's life, personality, and career; presents newly obtained information on the immediate consequences of the arrest, including circumstances leading to Baldwin's forced resignation; and describes the long-term impact of Baldwin's removal from the United States. Although no definitive conclusion with regard to Baldwin's guilt or innocence can be reached, we conclude by contrasting the treatment received at the hands of his colleagues in psychology with the lifelong support received from his wife and family, and suggest that Baldwin may have been the victim of a premature rush to judgment. C1 [Wozniak, Robert H.] Bryn Mawr Coll, Dept Psychol, Bryn Mawr, PA 19010 USA. [Santiago-Blay, Jorge A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Wozniak, RH (reprint author), Bryn Mawr Coll, Dept Psychol, 101 North Mer Ave, Bryn Mawr, PA 19010 USA. EM rwozniak@brynmawr.edu NR 58 TC 3 Z9 3 U1 0 U2 6 PU EDUCATIONAL PUBLISHING FOUNDATION-AMERICAN PSYCHOLOGICAL ASSOC PI WASHINGTON PA 750 FIRST ST, NE, WASHINGTON, DC 20002-4242 USA SN 1093-4510 EI 1939-0610 J9 HIST PSYCHOL JI Hist. Psychol. PD NOV PY 2013 VL 16 IS 4 BP 227 EP 248 DI 10.1037/a0033575 PG 22 WC History Of Social Sciences; Psychology, Multidisciplinary SC Social Sciences - Other Topics; Psychology GA 252XW UT WOS:000327047200001 PM 23914848 ER PT J AU Cecil, CB AF Cecil, C. Blaine TI An overview and interpretation of autocyclic and allocyclic processes and the accumulation of strata during the Pennsylvanian-Permian transition in the central Appalachian Basin, USA SO INTERNATIONAL JOURNAL OF COAL GEOLOGY LA English DT Article DE Autocyclic; Allocyclic; Paleoclimate; Climate drying ID PALEOCLIMATE CONTROLS; WEST-VIRGINIA; CLIMATE; CYCLOTHEMS; MIDCONTINENT; DEGLACIATION; SEQUENCES; BRAZIL; PLAIN AB Autocyclic and allocyclic processes controlled the lithostratigraphy of strata that accumulated in the central Appalachian foreland basin during the Pennsylvanian and the transition to the Permian. The transition strata, from bottom to top, include the Late Pennsylvanian Pittsburgh and Uniontown formations of the Monongahela Group, the Waynesburg and Washington formations of the Dunkard Group and the Permian Greene Formation of the Dunkard. Variations in the amount of precipitation were the predominant allocyclic control on stratigraphic variations in terrestrial organic productivity, lacustrine base levels, basin-scale weathering, water table and pedogenesis, sediment supply, and sedimentary geochemistry. Tectonic subsidence controlled accommodation space and basin configuration. Eustasy had little or no effect on the stratigraphy of strata deposited in this continental basin during the Pennsylvanian-Permian transition. Autocyclic processes were the predominant spatial control on architecture of alluvial plain aggradation. Paleosols, delineating regional unconformities, show a gradual upward transition from kaolinitic underclay paleosols indicative of a humid climate in the Late Pennsylvanian Monongahela Group to petrocalcic paleosols indicative of a dry subhumid to semiarid climate during deposition of Dunkard strata. As in the Monongahela Group, the Dunkard Group Waynesburg and Washington Formations contain multi-bedded nonmarine lacustrine limestones with subareal exposure features. These limestones grade laterally into petrocalcic paleo-Vertisols in the up-dip alluvial plain. Subareal exposure features are uncommon in centimeter-scale micritic limestones in the Permian Greene Formation; equivalent up-dip paleosols have been lost to erosion. Coal bed continuity, thickness, and quality, also decrease up-section from the very thick (>m) and laterally continuous Pittsburgh Coal at the base of the Monongahela Group to thin (cm scale) and laterally discontinuous coal beds that unconformably overlie the paleosol/underclay/limestone complexes in the Greene Formation. Lacustrine shales and impure (wacke) fluvio-lacustrine sandstones, commonly with a weak pedogenic overprint, generally overlie coal beds. During accumulation of Monongahela and Dunkard (MDG) strata within the basin center, unconformities at the tops of regional paleosols, overlain by lacustrine strata, suggest allocyclic-induced repeated rise and fall of lacustrine conditions in a lacustrine-fan-delta complex analogous to the Okavango basin and fan in Namibia, southern Africa, and/or the Pantanal in southern Brazil. During maximum lake levels, progradation of fluvio-deltaic systems resulted in laminated shale conformably overlain by dark shale and flat-bottomed distributary mouth bar siltstones and sandstones. Prograding distributaries and/or fluvial channels subsequently incised the flat-bottom mouth bar sands. Where basin margin strata are preserved, south of the basin center, depositional environments consist of aggrading alluvial plain sequences with paleosols, fluvial channel sands, and flood plain deposits. Anastomosing fluvial systems prograded across a low gradient (similar to 1 ft/mile; similar to 20 cm/km) alluvial plain into the basin center. A weak pedogenic overprint, marked by ubiquitous root penetrations, occurs throughout most basin-centered fluvial deposits. The subtle but continuous decline in the repetition of cyclic lithostratigraphy up-section in the MDG, particularly in the Greene Formation, appears to be the result of a 10-myr-climate transition from the humid to dry subhumid climate cycles of the Late Pennsylvanian to the equable semiarid to arid climate of the Middle Permian in North America. Cyclothems, common in Pennsylvanian strata, become less distinct up-section in the Dunkard because of decreasing development of underclays, coal, and limestone. This 30-myr period of transition from the humid Pennsylvanian to the arid Permian has been referred to as the Dyassic Period. Published by Elsevier B.V. C1 [Cecil, C. Blaine] US Geol Survey, Rockbridge Baths, VA 24473 USA. [Cecil, C. Blaine] NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Cecil, CB (reprint author), US Geol Survey, 425 Brownsburg Turnpike, Rockbridge Baths, VA 24473 USA. EM cecilblaine@gmail.com NR 46 TC 7 Z9 7 U1 1 U2 19 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-5162 EI 1872-7840 J9 INT J COAL GEOL JI Int. J. Coal Geol. PD NOV 1 PY 2013 VL 119 SI SI BP 21 EP 31 DI 10.1016/j.coal.2013.07.012 PG 11 WC Energy & Fuels; Geosciences, Multidisciplinary SC Energy & Fuels; Geology GA 251EB UT WOS:000326909500003 ER PT J AU Montanez, IP Cecil, CB AF Montanez, Isabel P. Cecil, C. Blaine TI Paleoenvironmental clues archived in non-marine Pennsylvanian-lower Permian limestones of the Central Appalachian Basin, USA SO INTERNATIONAL JOURNAL OF COAL GEOLOGY LA English DT Article DE Late Paleozoic climate; Non-marine limestone; Appalachian Basin; Palustrine carbonate ID UPPER FREEPORT FORMATION; PALEOZOIC ICE-AGE; NORTH-AMERICA; PALUSTRINE CARBONATES; PALEOCLIMATE CONTROLS; MADRID BASIN; CLIMATE; RECORD; SPAIN; STRATIGRAPHY AB Nonmarine limestones are a key component of the upper Middle Pennsylvanian through lower Permian succession in the Appalachian Basin. Previous interpretations of their environments of deposition range from brackish coastal mudflats to hydrologically open freshwater lake complexes with peat-forming vegetated marshes to semi-closed or closed, possibly saline, shallow lakes developed on a distal alluvial plain. Ostracode wackestones/packstones, some exhibiting laminations, and with fish debris, articulated ostracode shells and phosphatic clasts define the lower portions of limestone beds or benches, passing upward into ostracode-peloidal wackestones/packstones and intraclastic-skeletal-peloidal pacicstones/grainstones. Desiccation features and rooting structures, which are developed in the upper portions of the limestones, record subaerial exposure, pedogenic alteration and desiccation. Pseudomicrokarst and caliche-like vadose and early diagenetic phreatic cements suggest a seasonally dry subhumid to semi-arid regional climate. Many of the sedimentologic and diagenetic features of the limestones are characteristic of palustrine carbonates, which coupled with their stratigraphic relation to paleo-Vertisols, siliciclastics, and coals, indicate that they formed in broad seasonal wetland-pond complexes that developed on distal regions of a low-gradient, distal alluvial plain under seasonally dry subhumid to semi-arid climates. Integration of Sr isotopic compositions of shark teeth with previously published stable isotope compositions of the limestones suggests that these purely continental environments were hydrologically semi-closed to closed systems. Repeated stacking of these features at the bed- to limestone bench-scale defines repeated shallowing upward, drying cycles at the 10(3) to 10(4) yr-scale, which were likely climate-driven. Published by Elsevier B.V. C1 [Montanez, Isabel P.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Cecil, C. Blaine] US Geol Survey, Rockbridge Baths, VA 24473 USA. [Cecil, C. Blaine] NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Montanez, IP (reprint author), Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. EM ipmontanez@ucdavis.edu FU NSF [EAR-05545654, EAR-1024737] FX The authors express their gratitude to Bill DiMichele for his willingness to share ideas, enlighten us on things 'floral', and engage us in enlightening discussions. This paper would not exist without his pro-active encouragement delivered in a multitude of ways. James Bishop and Vickie Pedone provided thoughtful and constructive reviews of an earlier version of this paper. Parts of this research were supported by NSF grants EAR-05545654 and EAR-1024737 to IPM. NR 88 TC 3 Z9 3 U1 3 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-5162 EI 1872-7840 J9 INT J COAL GEOL JI Int. J. Coal Geol. PD NOV 1 PY 2013 VL 119 SI SI BP 41 EP 55 DI 10.1016/j.coal.2013.08.009 PG 15 WC Energy & Fuels; Geosciences, Multidisciplinary SC Energy & Fuels; Geology GA 251EB UT WOS:000326909500005 ER PT J AU DiMichele, WA Kerp, H Sirmons, R Fedorko, N Skema, V Blake, BM Cecil, CB AF DiMichele, William A. Kerp, Hans Sirmons, Roberta Fedorko, Nick Skema, Viktoras Blake, Bascombe M., Jr. Cecil, C. Blaine TI Callipterid peltasperms of the Dunkard Group, Central Appalachian Basin SO INTERNATIONAL JOURNAL OF COAL GEOLOGY LA English DT Article DE Dunkard; Callipterids; Permian; Pennsylvanian; Paleoecology; Paleoclimate ID PERMIAN PALEOBOTANY; NORTH-AMERICA; CLIMATE-CHANGE; CONIFERS; PALYNOLOGY; TRANSITION; BOUNDARY; ORIGIN; FLORAS; WEST AB The Dunkard Group is the youngest late Paleozoic rock unit in the Central Appalachian Basin. Its age, however, remains controversial. In its southern and western two-thirds the Dunkard is comprised largely of red beds, sandstone and siltstone channel deposits and paleosols. In its thickest, most northerly exposures, in southwestern Pennsylvania, northern West Virginia, and east-central Ohio, much of the lower part of the unit is composed of coals, non-marine limestones and gray, often calcareous, paleosols. Age dating is confounded by the non-marine nature of the deposit and by the lack of dateable volcanic ash beds. Dunkard fossils include plants, vertebrates, and both aquatic and terrestrial invertebrates. Most of the fossil groups point to an age very close to, if not including, the Pennsylvanian Permian boundary, though the exact position of that boundary is uncertain. Callipterids make their first appearance in the Dunkard flora in the middle of the Washington Formation and continue into the Greene Formation, but in different beds from those containing wetland floral elements. Publication of these plants in the "Permian Flora" of Fontaine and White (1880) created an immediate controversy about the age of the unit because Callipteris conferta (now Autunia conferta) was, at the time, considered to be an index fossil for the base of the Permian. Subsequent collecting has revealed these callipterds to comprise four species: A. conferta, Autunia naumannii, Lodevia oxydata and Rhachiphyllum schenkii. Callipterids and the conifers with which they are sometimes associated are typically found in seasonally dry equatorial environments and most likely constitute an environmentally controlled biofacies. This biofacies is not well known, resulting in limited biostratigraphic utility. Published by Elsevier B.V. C1 [DiMichele, William A.; Sirmons, Roberta] NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Kerp, Hans] Univ Munster, Forsch Stelle Palaobot, Munster, Germany. [Fedorko, Nick] Cove Geol Serv, Moatsville, WV 26405 USA. [Skema, Viktoras] Penn Geol Survey, Middletown, PA 17057 USA. [Blake, Bascombe M., Jr.] West Virginia Geol & Econ Survey, Morgantown, WV 26508 USA. [Cecil, C. Blaine] US Geol Survey, Natl Ctr, Reston, VA 20192 USA. RP DiMichele, WA (reprint author), NMNH Smithsonian Inst, Dept Paleobiol, MRC 121, Washington, DC 20560 USA. EM dimichel@si.edu; kerp@uni-muenster.de; rsirmons@si.edu; nick.fedorko@gmail.com; skema@verizon.net; blake@geosrv.wvnet.edu; cecilblaine@gmail.com FU National Museum of Natural History small grants program; United States Geological Survey; Pennsylvania Geological Survey; West Virginia Geological and Economic Survey FX This research was supported in part by the National Museum of Natural History small grants program, the United States Geological Survey, Pennsylvania Geological Survey, and West Virginia Geological and Economic Survey. Historic USGS topographic maps are from the historic map collection made available by MyTopo, http://historical.mytopo.com/. We thank Benjamin Bomfleur and an anonymous reviewer for detailed, thoughtful comments on an earlier version of the paper that greatly improved it. NR 95 TC 10 Z9 11 U1 2 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-5162 EI 1872-7840 J9 INT J COAL GEOL JI Int. J. Coal Geol. PD NOV 1 PY 2013 VL 119 SI SI BP 56 EP 78 DI 10.1016/j.coal.2013.07.025 PG 23 WC Energy & Fuels; Geosciences, Multidisciplinary SC Energy & Fuels; Geology GA 251EB UT WOS:000326909500006 ER PT J AU Tabor, NJ DiMichele, WA Montanez, IP Chaney, DS AF Tabor, Neil J. DiMichele, William A. Montanez, Isabel P. Chaney, Dan S. TI Late Paleozoic continental warming of a cold tropical basin and floristic change in western Pangea SO INTERNATIONAL JOURNAL OF COAL GEOLOGY LA English DT Article DE Pennsylvanian; Permian; Paleoclimate; Paleobotany; Paleotemperature; Biological diversity ID HYDROGEN ISOTOPE COMPOSITIONS; NORTH-CENTRAL TEXAS; CLAY-MINERALS; CLIMATE; OXYGEN; FORESTS; RECORD; FLORAS; TRANSITION; VEGETATION AB An increase in mineral crystallization temperatures of similar to 13 +/- 3 degrees C is preserved in paleosol profiles (ancient soils) within a stratigraphic interval of <40 m thickness in Permo-Carboniferous strata in western equatorial Pangea (modern north-central Texas). Late Pennsylvanian and Early Permian soil-mineral crystallization temperatures are estimated through the study interval with oxygen and hydrogen isotope compositions of paleopedogenic phyllosilicates and hematites taken from paleosol profiles. Considering monthly soil- and air-temperature measurements from modern equatorial Africa, phyllosilicate crystallization temperatures likely exceed surface air temperatures by similar to 2 +/- 2 degrees C. Furthermore, the warming trend emerges from Pennsylvanian-age soil mineral crystallization temperatures, which are substantially cooler than soil temperatures observed in the modern lowland tropics, to Permian-age soil mineral crystallization temperatures, which are equivalent to, or slightly exceed, soil temperatures observed in modern lowland tropics. This record of mineral crystallization temperatures occurs at a time when some sources indicate the onset of the largest single glaciation of the Late Paleozoic Ice Age. The temperature change indicated by these paleosol minerals is accompanied by a unidirectional, irreversible change in the composition of tropical lowland vegetation. This transition delineates the magnitude and characteristics of vegetational changes in the modern tropics that might accompany continued atmospheric warming. Times of low surface temperatures coincide with a typical Late Pennsylvanian, tropical Pangean, "wet" biome dominated by Sigillaria, Macroneuropteris, other pteridosperms and marattialean ferns. This plant assemblage is replaced spatially by a xeromorphic biome dominated by conifers, callipterids, and other seed plants, characteristic of the tropical Permian across western and central Pangea. The fully xeromorphic flora appears initially in sub-meter-scale beds within outcrops otherwise characterized by wet flora, and becomes predominant once peak surface temperatures were reached in the earliest Permian. A narrow stratigraphic interval (20 m) separates these two biomes in the region, marking what was to be a permanent floristic change in western Pangea. The lower diversity floras of seasonally dry habitats apparently migrated from drier extrabasinal areas into increasingly dry landscapes formerly dominated by the wet biome. This study documents the regional disappearance of an entire tropical biome with a net reduction of biodiversity accompanying rapid environmental warming. (C) 2013 Elsevier B.V. All rights reserved. C1 [Tabor, Neil J.] So Methodist Univ, Huffington Dept Earth Sci, Dallas, TX 75275 USA. [DiMichele, William A.; Chaney, Dan S.] NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Montanez, Isabel P.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. RP Tabor, NJ (reprint author), So Methodist Univ, Huffington Dept Earth Sci, POB 750395, Dallas, TX 75275 USA. EM ntabor@smu.edu FU NMNH small grants program; Smithsonian Institution Scholarly Studies program; NSF-EAR [0844147, 0519336] FX WD and DSC acknowledge the NMNH small grants program and the Smithsonian Institution Scholarly Studies program for research support, particularly of north-central Texas fieldwork. We thank numerous property owners for granting access to their land during the period from 1989 until the present during which this study has been carried out. NJT was funded by NSF-EAR 0844147 and NSF-EAR 0519336. NR 86 TC 10 Z9 10 U1 3 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-5162 EI 1872-7840 J9 INT J COAL GEOL JI Int. J. Coal Geol. PD NOV 1 PY 2013 VL 119 SI SI BP 177 EP 186 DI 10.1016/j.coal.2013.07.009 PG 10 WC Energy & Fuels; Geosciences, Multidisciplinary SC Energy & Fuels; Geology GA 251EB UT WOS:000326909500014 ER PT J AU Clark, KE Capper, A Della Togna, G Paul, VJ Romero, LI Johns, T Cubilla-Rios, L Capson, TL AF Clark, Kathryn E. Capper, Angela Della Togna, Gina Paul, Valerie J. Romero, Luz I. Johns, Timothy Cubilla-Rios, Luis Capson, Todd L. TI Ecology- and Bioassay-Guided Drug Discovery for Treatments of Tropical Parasitic Disease: 5 alpha,8 alpha-Epidioxycholest-6-en-3 beta-ol Isolated from the Mollusk Dolabrifera dolabrifera Shows Significant Activity against Leishmania donovani SO NATURAL PRODUCT COMMUNICATIONS LA English DT Article DE Marine invertebrate; Antileishmanial; Endoperoxide; Chemical ecology ID NATURAL-PRODUCTS; MARINE SPONGE; SEA HARES; STEROLS; INVERTEBRATES; CHEMISTRY; PLANTS AB An ecology- and bioassay-guided search employed to discover compounds with activity against tropical parasitic diseases and cancer from the opisthobranch mollusk, Dolabrifera dolabrifera, led to the discovery of antileishmanial properties in the known compound, 5 alpha,8 alpha-epidioxycholest-6-en-3 beta-ol (1). Compound 1 was identified through nuclear magnetic resonance spectroscopy (H-1, C-13) and mass spectrometry. The compound was concentrated in the digestive gland of D. dolabrifera, but was not detected in other body parts, fecal matter or mucus. Compound 1 showed an IC50 of 4.9 mu M towards the amastigote form of Leishmania donovani compared with an IC50 of 281 mu M towards the control Vero cell line, a 57.3-fold difference, and demonstrated no measurable activity against Plasmodium falciparum, Trypanosoma cruzi, and the breast cancer cell line, MCF-7. C1 [Clark, Kathryn E.; Capson, Todd L.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Clark, Kathryn E.; Johns, Timothy; Capson, Todd L.] McGill Univ, Dept Plant Sci, Quebec City, PQ H9X 3V9, Canada. [Capper, Angela; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Della Togna, Gina; Romero, Luz I.] Inst Invest Cient Avanzadas & Serv Alta Tecnol, Panama City, Panama. [Cubilla-Rios, Luis] Univ Panama, Dept Quim Organ, Lab Bioorgan Trop, Panama City, Panama. RP Capson, TL (reprint author), 1743 18th St NW, Washington, DC 20009 USA. EM capsont@gmail.com FU Natural Sciences and Engineering Research Council of Canada Canadian Graduate Scholarship; Smithsonian Tropical Research Institute-McGill Neotropical Environmental Option; Fogarty International Center's International Cooperative Biodiversity Groups program [ICBG TW006634] FX We thank the Natural Sciences and Engineering Research Council of Canada Canadian Graduate Scholarship, and a Levinson Fellowship from the Smithsonian Tropical Research Institute-McGill Neotropical Environmental Option for support for K.E.C. and the Fogarty International Center's International Cooperative Biodiversity Groups program (ICBG TW006634). We thank A. Hermosillo (Universidad de Guadalajara) and A. Ibanez (Smithsonian Tropical Research Institute) for assistance with sea hare collections, C. Coates (Scripps Institution of Oceanography) for identifying cyanobacterial samples, R. Linington (University of California at Santa Cruz) for assistance in compound isolation and identification and for carrying out NMR. and MS procedures and A. Almanza, M. Ng, L. Herrera, L. Pineda and L.D. Urena for bioassay support. We thank P.K. Agrawal and an anonymous reviewer for input that greatly improved this manuscript. NR 38 TC 3 Z9 3 U1 2 U2 5 PU NATURAL PRODUCTS INC PI WESTERVILLE PA 7963 ANDERSON PARK LN, WESTERVILLE, OH 43081 USA SN 1934-578X EI 1555-9475 J9 NAT PROD COMMUN JI Nat. Prod. Commun. PD NOV PY 2013 VL 8 IS 11 BP 1537 EP 1540 PG 4 WC Chemistry, Medicinal; Food Science & Technology SC Pharmacology & Pharmacy; Food Science & Technology GA 250NK UT WOS:000326859300009 PM 24427935 ER PT J AU Ackermann, M Ajello, M Asano, K Axelsson, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Bhat, PN Bissaldi, E Bloom, ED Bonamente, E Bonnell, J Bouvier, A Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Burgess, JM Buson, S Byrne, D Caliandro, GA Cameron, RA Caraveo, PA Cecchi, C Charles, E Chaves, RCG Chekhtman, A Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Connaughton, V Conrad, J Cutini, S D'Ammando, F de Angelis, A de Palma, F Dermer, CD Desiante, R Digel, SW Dingus, BL Di Venere, L Drell, PS Drlica-Wagner, A Dubois, R Favuzzi, C Ferrara, EC Fitzpatrick, G Foley, S Franckowiak, A Fukazawa, Y Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Goldstein, A Granot, J Grenier, IA Grove, JE Gruber, D Guiriec, S Hadasch, D Hanabata, Y Hayashida, M Horan, D Hou, X Hughes, RE Inoue, Y Jackson, MS Jogler, T Johannesson, G Johnson, AS Johnson, WN Kamae, T Kataoka, J Kawano, T Kippen, RM Knodlseder, J Kocevski, D Kouveliotou, C Kuss, M Lande, J Larsson, S Latronico, L Lee, SH Longo, F Loparco, F Lovellette, MN Lubrano, P Massaro, F Mayer, M Mazziotta, MN McBreen, S McEnery, JE McGlynn, S Michelson, PF Mizuno, T Moiseev, AA Monte, C Monzani, ME Moretti, E Morselli, A Murgia, S Nemmen, R Nuss, E Nymark, T Ohno, M Ohsugi, T Omodei, N Orienti, M Orlando, E Paciesas, WS Paneque, D Panetta, JH Pelassa, V Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Porter, TA Preece, R Racusin, JL Raino, S Rando, R Rau, A Razzano, M Razzaque, S Reimer, A Reimer, O Reposeur, T Ritz, S Romoli, C Roth, M Ryde, F Parkinson, PMS Schalk, TL Sgro, C Siskind, EJ Sonbas, E Spandre, G Spinelli, P Suson, DJ Tajima, H Takahashi, H Takeuchi, Y Tanaka, Y Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tierney, D Tinivella, M Torres, DF Tosti, G Troja, E Tronconi, V Usher, TL Vandenbroucke, J van der Horst, AJ Vasileiou, V Vianello, G Vitale, V von Kienlin, A Winer, BL Wood, KS Wood, M Xiong, S Yang, Z AF Ackermann, M. Ajello, M. Asano, K. Axelsson, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Bhat, P. N. Bissaldi, E. Bloom, E. D. Bonamente, E. Bonnell, J. Bouvier, A. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Burgess, J. Michael Buson, S. Byrne, D. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cecchi, C. Charles, E. Chaves, R. C. G. Chekhtman, A. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Connaughton, V. Conrad, J. Cutini, S. D'Ammando, F. de Angelis, A. de Palma, F. Dermer, C. D. Desiante, R. Digel, S. W. Dingus, B. L. Di Venere, L. Drell, P. S. Drlica-Wagner, A. Dubois, R. Favuzzi, C. Ferrara, E. C. Fitzpatrick, G. Foley, S. Franckowiak, A. Fukazawa, Y. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Goldstein, A. Granot, J. Grenier, I. A. Grove, J. E. Gruber, D. Guiriec, S. Hadasch, D. Hanabata, Y. Hayashida, M. Horan, D. Hou, X. Hughes, R. E. Inoue, Y. Jackson, M. S. Jogler, T. Johannesson, G. Johnson, A. S. Johnson, W. N. Kamae, T. Kataoka, J. Kawano, T. Kippen, R. M. Knoedlseder, J. Kocevski, D. Kouveliotou, C. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lee, S. -H. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Massaro, F. Mayer, M. Mazziotta, M. N. McBreen, S. McEnery, J. E. McGlynn, S. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Moretti, E. Morselli, A. Murgia, S. Nemmen, R. Nuss, E. Nymark, T. Ohno, M. Ohsugi, T. Omodei, N. Orienti, M. Orlando, E. Paciesas, W. S. Paneque, D. Panetta, J. H. Pelassa, V. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Porter, T. A. Preece, R. Racusin, J. L. Raino, S. Rando, R. Rau, A. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Reposeur, T. Ritz, S. Romoli, C. Roth, M. Ryde, F. Parkinson, P. M. Saz Schalk, T. L. Sgro, C. Siskind, E. J. Sonbas, E. Spandre, G. Spinelli, P. Suson, D. J. Tajima, H. Takahashi, H. Takeuchi, Y. Tanaka, Y. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tierney, D. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Tronconi, V. Usher, T. L. Vandenbroucke, J. van der Horst, A. J. Vasileiou, V. Vianello, G. Vitale, V. von Kienlin, A. Winer, B. L. Wood, K. S. Wood, M. Xiong, S. Yang, Z. TI THE FIRST FERMI-LAT GAMMA-RAY BURST CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; gamma-ray burst: general; methods: data analysis ID LARGE-AREA TELESCOPE; INTERNAL SHOCK MODEL; HIGH-ENERGY EMISSION; DELAYED GEV EMISSION; SPECTRAL COMPONENT; PROMPT EMISSION; GRB 100728A; LIKELIHOOD RATIO; FLARING ACTIVITY; PHOTON-EMISSION AB In three years of observations since the beginning of nominal science operations in 2008 August, the Large Area Telescope (LAT) on board the Fermi Gamma-Ray Space Telescope has observed high-energy (greater than or similar to 20 MeV) gamma-ray emission from 35 gamma-ray bursts (GRBs). Among these, 28 GRBs have been detected above 100 MeV and 7 GRBs above similar to 20 MeV. The first Fermi-LAT catalog of GRBs is a compilation of these detections and provides a systematic study of high-energy emission from GRBs for the first time. To generate the catalog, we examined 733 GRBs detected by the Gamma-Ray Burst Monitor (GBM) on Fermi and processed each of them using the same analysis sequence. Details of the methodology followed by the LAT collaboration for the GRB analysis are provided. We summarize the temporal and spectral properties of the LAT-detected GRBs. We also discuss characteristics of LAT-detected emission such as its delayed onset and longer duration compared with emission detected by the GBM, its power-law temporal decay at late times, and the fact that it is dominated by a power-law spectral component that appears in addition to the usual Band model. C1 [Ackermann, M.; Mayer, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Asano, K.] Tokyo Inst Technol, Interact Res Ctr Sci, Meguro, Tokyo 1528551, Japan. [Axelsson, M.; Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Axelsson, M.; Conrad, J.; Jackson, M. S.; Larsson, S.; Moretti, E.; Nymark, T.; Ryde, F.; Yang, Z.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Axelsson, M.; Jackson, M. S.; Moretti, E.; Nymark, T.; Ryde, F.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Desiante, R.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.; Romoli, C.; Tronconi, V.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bechtol, K.; Bloom, E. D.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Di Venere, L.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Kocevski, D.; Lande, J.; Massaro, F.; Michelson, P. F.; Monzani, M. E.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tajima, H.; 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. [Bechtol, K.; Bloom, E. D.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Di Venere, L.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Kocevski, D.; Lande, J.; Massaro, F.; Michelson, P. F.; Monzani, M. E.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tajima, H.; 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. [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. [Bhat, P. N.; Burgess, J. Michael; Connaughton, V.; Goldstein, A.; Pelassa, V.; Preece, R.; Xiong, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Bissaldi, E.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Bissaldi, E.; Reimer, A.; Reimer, O.] 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. [Bonnell, J.; Brandt, T. J.; Ferrara, E. C.; Gehrels, N.; Guiriec, S.; McEnery, J. E.; Nemmen, R.; Perkins, J. S.; Racusin, J. L.; Sonbas, E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bonnell, J.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Bonnell, J.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Bouvier, A.; Razzano, M.; Ritz, S.; Parkinson, P. M. Saz; Schalk, T. 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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.; Giommi, P.] Agenzia Spaziale Italiana Sci Data Ctr, I-00044 Rome, Italy. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Rome, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France. [Conrad, J.; Larsson, S.; Yang, Z.] Stockholm Univ, AlbaNova, Dept 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.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Dingus, B. L.; Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Foley, S.; Gruber, D.; McBreen, S.; Rau, A.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Fukazawa, Y.; Hanabata, Y.; Kawano, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hou, X.; Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Kataoka, J.; Takeuchi, Y.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France. [Kouveliotou, C.; Moiseev, A. A.; Perkins, J. S.; van der Horst, A. J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Lee, S. -H.] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan. [McGlynn, S.] Tech Univ Munich, Exzellenzcluster Universe, D-85748 Garching, Germany. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Moiseev, A. A.; Perkins, J. S.] CRESST, 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. [Paciesas, W. S.; Sonbas, E.] USRA, Columbia, MD 21044 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. [Razzaque, S.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa. [Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Sonbas, E.] Adiyaman Univ, TR-02040 Adiyaman, Turkey. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Torres, D. F.] ICREA, Barcelona, Spain. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM nicola.omodei@stanford.edu; piron@in2p3.fr; soebur.razzaque@gmail.com; vlasios.vasileiou@lupm.in2p3.fr RI Di Venere, Leonardo/C-7619-2017; 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; Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Massaro, Francesco/L-9102-2016; Torres, Diego/O-9422-2016; Johnson, Neil/G-3309-2014; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Orlando, E/R-5594-2016; OI Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Axelsson, Magnus/0000-0003-4378-8785; Giroletti, Marcello/0000-0002-8657-8852; McBreen, Sheila/0000-0002-1477-618X; Moretti, Elena/0000-0001-5477-9097; Gasparrini, Dario/0000-0002-5064-9495; Di Venere, Leonardo/0000-0003-0703-824X; Inoue, Yoshiyuki/0000-0002-7272-1136; Giordano, Francesco/0000-0002-8651-2394; Dingus, Brenda/0000-0001-8451-7450; giommi, paolo/0000-0002-2265-5003; De Angelis, Alessandro/0000-0002-3288-2517; Preece, Robert/0000-0003-1626-7335; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Burgess, James/0000-0003-3345-9515; 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; Bissaldi, Elisabetta/0000-0001-9935-8106; Massaro, Francesco/0000-0002-1704-9850; Torres, Diego/0000-0002-1522-9065; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Baldini, Luca/0000-0002-9785-7726 FU National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atom-ique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France 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 Atom-ique 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), the High Energy Accelerator Research Organization (KEK), and the Japan Aerospace Exploration Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden.; Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. NR 297 TC 80 Z9 81 U1 1 U2 29 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 NOV PY 2013 VL 209 IS 1 AR UNSP 11 DI 10.1088/0067-0049/209/1/11 PG 90 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246WJ UT WOS:000326571000011 ER PT J AU Lee, J Lee, JE Lee, S Green, JD Evans, NJ Choi, M Kristensen, L Dionatos, O Jorgensen, JK AF Lee, Jinhee Lee, Jeong-Eun Lee, Seokho Green, Joel D. Evans, Neal J., II Choi, Minho Kristensen, Lars Dionatos, Odysseas Jorgensen, Jes K. CA DIGIT Team TI L1448-MM OBSERVATIONS BY THE HERSCHEL KEY PROGRAM, "DUST, ICE, AND GAS IN TIME" (DIGIT) SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM; individual objects; L1448-MM - ISM; jets and outflows - ISM; molecules - stars; protostars techniques; spectroscopic ID STAR-FORMING REGIONS; LOW-MASS PROTOSTARS; SPITZER-SPACE-TELESCOPE; INFRARED SPECTROGRAPH; PROTOSTELLAR OUTFLOWS; SPECTROSCOPIC SURVEY; MOLECULAR BULLETS; PACS SPECTROSCOPY; BIPOLAR OUTFLOW; EXCITING SOURCE AB We present Herschel/Photodetector Array Camera and Spectrometer (PACS) observations of L1448-MM, a Class 0 protostar with a prominent outflow. Numerous emission lines are detected at 55< gimel < 210 mu m including CO, OH, H2O, and [O I]. We investigate the spatial distribution of each transition to find that lines from low energy levels tend to distribute along the outflow direction while lines from high energy levels peak at the central spatial pixel. Spatial maps reveal that OH emission lines are formed in a relatively small area, while [O I] emission is extended. According to the rotational diagram analysis, the CO emission can be fitted by two (warm and hot) temperature components. For H2O, the ortho-to-para ratio is close to 3. The non-LTE large velocity gradient (LVG) calculations suggest that CO and H2O lines could instead be formed in a high kinetic temperature (T > 1000 K) environment, indicative of a shock origin. For OH, IR-pumping processes play an important role in the level population. The molecular emission in L1448-MM is better explained with a C-shock model, but the atomic emission of PACS [O I] and Spitzer/Infrared Spectrograph [Si II] emission is not consistent with C-shocks, suggesting multiple shocks in this region. Water is the major line coolant of L1448-MM in the PACS wavelength range, and the best-fit LVG models predict that H2O and CO emit (50%-80%) of their line luminosity in the PACS wavelength range. C1 [Lee, Jinhee; Lee, Jeong-Eun] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 449701, Kyungki Do, South Korea. [Lee, Seokho] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151742, South Korea. [Green, Joel D.; Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Choi, Minho] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Kristensen, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dionatos, Odysseas; Jorgensen, Jes K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. RP Lee, J (reprint author), Kyung Hee Univ, Dept Astron & Space Sci, Yongin 449701, Kyungki Do, South Korea. EM jeongeun.lee@khu.ac.kr RI Lee , Jeong-Eun/E-2387-2013; Kristensen, Lars/F-4774-2011; OI Kristensen, Lars/0000-0003-1159-3721; Dionatos, Odysseas/0000-0002-2689-8870 FU Herschel Open Time Key Project Program; NASA; Jet Propulsion Laboratory, California Institute of Technology; Basic Science Research Program through the National Research Foundation of Korea (NRF); Ministry of Education of the Korean government [NRF-2010-0008704, NRF-2012R1A1A2044689]; Core Research Program of NRF; Ministry of Science, ICT; Future Planning of the Korean government [NRF-2011-0015816]; Korea Astronomy and Space Science Institute; Korean government (MEST) FX Support for this work, part of the Herschel Open Time Key Project Program, was provided by NASA through an award issued by the Jet Propulsion Laboratory, California Institute of Technology. Jeong-Eun Lee was supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education of the Korean government (grant number NRF-2010-0008704 and NRF-2012R1A1A2044689). M. C. was supported by the Core Research Program of NRF funded by the Ministry of Science, ICT and Future Planning of the Korean government (grant number NRF-2011-0015816). This work is also supported by the Korea Astronomy and Space Science Institute (KASI) grant funded by the Korean government (MEST). NR 60 TC 9 Z9 9 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2013 VL 209 IS 1 DI 10.1088/0067-0049/209/1/4 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246WJ UT WOS:000326571000004 ER PT J AU Launius, RD AF Launius, Roger D. TI The Strange Career of the American Spaceplane: The Long History of Wings and Wheels in Human Space Operations SO CENTAURUS LA English DT Article DE astronauts; human spaceflight; NASA; spaceplane; space capsules; Space Shuttle ID DECISION; SHUTTLE; TECHNOLOGY AB What is it about the concept of a Space Shuttle that has been so inviting throughout the 20th century? A winged, reusable space vehicle for human flight beyond Earth dominated thinking about the task prior to the space age, but to compete with the Soviet Union in the human space spectaculars that began in the late 1950s the USA opted for easier to build and fly ballistic capsules. No sooner had that competition ebbed, however, than NASA returned to the pursuit of a spaceplane, resulting in the building of the winged, reusable Space Shuttle which flew for 30years. This essay reviews the more than 40-year history of the quest for a spaceplane that eventually found fruition with the operations of the Space Shuttle and continues with current attempts to create a replacement and ensure that spaceplane dreams are kept alive. Three major lessons concerning this quest come to the fore and are highlighted in this essay: (1) the power of an idea to push engineering reality, (2) the delta between technological knowledge and potential, and (3) the reality of how critical design elements are not only fostered by hard-headed engineering analysis but also by other conventions and priorities. C1 Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20013 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, POB 37012, Washington, DC 20013 USA. EM launiusr@si.edu NR 82 TC 0 Z9 0 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0008-8994 EI 1600-0498 J9 CENTAURUS JI Centaurus PD NOV PY 2013 VL 55 IS 4 BP 412 EP 432 DI 10.1111/1600-0498.12037 PG 21 WC History & Philosophy Of Science SC History & Philosophy of Science GA 248TB UT WOS:000326724900003 ER PT J AU Terrell, KA Quintero, RP Murray, S Kleopfer, JD Murphy, JB Evans, MJ Nissen, BD Gratwicke, B AF Terrell, Kimberly A. Quintero, Richard P. Murray, Suzan Kleopfer, John D. Murphy, James B. Evans, Matthew J. Nissen, Bradley D. Gratwicke, Brian TI Cryptic impacts of temperature variability on amphibian immune function SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE thermal physiology; salamander; protein complement; Cryptobranchus; climate change ID HELLBENDERS CRYPTOBRANCHUS-ALLEGANIENSIS; CLIMATE-CHANGE; CONSERVATION PHYSIOLOGY; TRANSPLANTATION IMMUNITY; POPULATION DECLINES; THERMAL TOLERANCE; MASS MORTALITY; RANA-SYLVATICA; ECTOTHERMS; HEMATOLOGY AB Ectothermic species living in temperate regions can experience rapid and potentially stressful changes in body temperature driven by abrupt weather changes. Yet, among amphibians, the physiological impacts of short-term temperature variation are largely unknown. Using an ex situ population of Cryptobranchus alleganiensis, an aquatic North American salamander, we tested the hypothesis that naturally occurring periods of temperature variation negatively impact amphibian health, either through direct effects on immune function or by increasing physiological stress. We exposed captive salamanders to repeated cycles of temperature fluctuations recorded in the population's natal stream and evaluated behavioral and physiological responses, including plasma complement activity (i.e. bacteria killing) against Pseudomonas aeruginosa, Escherichia coli and Aeromonas hydrophila. The best-fit model (Delta AIC(c)=0, w(i)=0.9992) revealed 70% greater P. aeruginosa killing after exposure to variable temperatures and no evidence of thermal acclimation. The same model predicted 50% increased E. coli killing, but had weaker support (Delta AIC(c)=1.8, w(i)=0.2882). In contrast, plasma defenses were ineffective against A. hydrophila, and other health indicators (leukocyte ratios, growth rates and behavioral patterns) were maintained at baseline values. Our data suggest that amphibians can tolerate, and even benefit from, natural patterns of rapid warming/cooling. Specifically, temperature variation can elicit increased activity of the innate immune system. This immune response may be adaptive in an unpredictable environment, and is undetectable by conventional health indicators (and hence considered cryptic). Our findings highlight the need to consider naturalistic patterns of temperature variation when predicting species' susceptibility to climate change. C1 [Terrell, Kimberly A.; Gratwicke, Brian] Smithsonian Conservat Biol Inst, Ctr Species Survival, Washington, DC 20008 USA. [Quintero, Richard P.; Murray, Suzan; Murphy, James B.; Evans, Matthew J.; Nissen, Bradley D.] Smithsonian Conservat Biol Inst, Ctr Anim Care Sci, Washington, DC 20008 USA. [Kleopfer, John D.] Virginia Dept Game & Inland Fisheries, Charles City, VA 23030 USA. RP Terrell, KA (reprint author), Smithsonian Conservat Biol Inst, Ctr Species Survival, Natl Zool Pk,3001 Connecticut Ave NW, Washington, DC 20008 USA. EM terrellk@si.edu FU David H. Smith Fellowship; Cedar Tree Foundation FX This research was supported by a David H. Smith Fellowship (to K. A. T.), which is funded by the Cedar Tree Foundation and administered by the Society for Conservation Biology. NR 72 TC 6 Z9 6 U1 11 U2 65 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 NOV PY 2013 VL 216 IS 22 BP 4204 EP 4211 DI 10.1242/jeb.089896 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 245YD UT WOS:000326499900014 PM 23948472 ER PT J AU Aiello, A AF Aiello, Annette TI The Infested Mind: Why Humans Fear, Loathe, and Love Insects SO LIBRARY JOURNAL LA English DT Book Review C1 [Aiello, Annette] Smithsonian Trop Res Inst, Balboa, Panama. RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 1 TC 0 Z9 0 U1 1 U2 5 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD NOV 1 PY 2013 VL 138 IS 18 BP 115 EP 115 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 247HK UT WOS:000326608300214 ER PT J AU Catinella, B Schiminovich, D Cortese, L Fabello, S Hummels, CB Moran, SM Lemonias, JJ Cooper, AP Wu, RN Heckman, TM Wang, J AF Catinella, Barbara Schiminovich, David Cortese, Luca Fabello, Silvia Hummels, Cameron B. Moran, Sean M. Lemonias, Jenna J. Cooper, Andrew P. Wu, Ronin Heckman, Timothy M. Wang, Jing TI The GALEX Arecibo SDSS Survey - VIII. Final data release. The effect of group environment on the gas content of massive galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: fundamental parameters; radio lines: galaxies; ultraviolet: galaxies ID DIGITAL SKY SURVEY; FAST ALPHA SURVEY; FRACTION SCALING RELATIONS; HERSCHEL REFERENCE SURVEY; STAR-FORMATION HISTORY; IRAM LEGACY SURVEY; DARK-MATTER HALOS; HI DATA STACKING; CLUSTER GALAXIES; VIRGO CLUSTER AB We present the final data release from the GALEX Arecibo SDSS Survey (GASS), a large Arecibo programme that measured the HI properties for an unbiased sample of similar to 800 galaxies with stellar masses greater than 10(10) M-circle dot and redshifts 0.025 < z < 0.05. This release includes new Arecibo observations for 250 galaxies. We use the full GASS sample to investigate environmental effects on the cold gas content of massive galaxies at fixed stellar mass. The environment is characterized in terms of dark matter halo mass, obtained by cross-matching our sample with the Sloan Digital Sky Survey (SDSS) group catalogue of Yang et al. Our analysis provides, for the first time, clear statistical evidence that massive galaxies located in haloes with masses of 10(13) - 10(14) M-circle dot have at least 0.4 dex less HI than objects in lower density environments. The process responsible for the suppression of gas in group galaxies most likely drives the observed quenching of the star formation in these systems. Our findings strongly support the importance of the group environment for galaxy evolution, and have profound implications for semi-analytic models of galaxy formation, which currently do not allow for stripping of the cold interstellar medium in galaxy groups. C1 [Catinella, Barbara; Wang, Jing] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Catinella, Barbara; Cortese, Luca] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Schiminovich, David; Lemonias, Jenna J.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Cortese, Luca] European So Observ, D-85748 Garching, Germany. [Fabello, Silvia] Autoliv Elect Germany, D-85221 Dachau, Germany. [Hummels, Cameron B.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Hummels, Cameron B.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Moran, Sean M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Cooper, Andrew P.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Wu, Ronin] CEA, F-91191 Gif Sur Yvette, France. [Heckman, Timothy M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Catinella, B (reprint author), Max Planck Inst Astrophys, D-85741 Garching, Germany. EM bcatinella@swin.edu.au OI Catinella, Barbara/0000-0002-7625-562X; Cooper, Andrew/0000-0001-8274-158X; Cortese, Luca/0000-0002-7422-9823 FU Australian Research Council [FT120100660]; National Natural Science Foundation of China [11250110509]; European Community [229517]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group, the 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 BC is the recipient of an Australian Research Council Future Fellowship (FT120100660). APC acknowledges the National Natural Science Foundation of China International Cooperation and Exchange Grant, no. 11250110509. The research leading to these results has received funding from the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement no. 229517.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/.; 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 79 TC 61 Z9 61 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 NOV PY 2013 VL 436 IS 1 BP 34 EP 70 DI 10.1093/mnras/stt1417 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 245BY UT WOS:000326435100027 ER PT J AU Vierdayanti, K Sadowski, A Mineshige, S Bursa, M AF Vierdayanti, K. Sadowski, A. Mineshige, S. Bursa, M. TI Inner disc obscuration in GRS 1915+105 based on relativistic slim disc model SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; stars: individual: GRS 1915+105; X-rays: binaries ID SUPERCRITICAL ACCRETION FLOW; GALACTIC BLACK-HOLE; X-RAY SOURCES; OBSERVATIONAL APPEARANCE; EDDINGTON LUMINOSITY; GRS-1915+105; SPIN; VARIABILITY; STATE; CONTINUUM AB We study the observational signatures of the relativistic slim disc of 10 M-circle dot black hole, in a wide range of mass accretion rate, (m) over dot, dimensionless spin parameter, a(*), and viewing angle, i. In general, the innermost temperature, T-in, increases with the increase of i for a fixed value of (m) over dot and a(*), due to the Doppler effect. However, for i > 50 degrees and (m) over dot > (m) over dot(turn), T-in starts to decrease with the increase of (m) over dot. This is a result of self-obscuration - the radiation from the innermost hot part of the disc is blocked by the surrounding cooler part. The value of (m) over dot(turn) and the corresponding luminosities depend on a(*) and i. Such obscuration effects cause an interesting behaviour on the disc luminosity (L-disc)-T-in plane for high inclinations. In addition to the standard disc branch which appears below (m) over dot(turn) and which obeys L-disc proportional to T-in(4) relation, another branch above (m) over dot(turn), which is nearly horizontal, may be observed at luminosities close to the Eddington luminosity. We show that these features are likely observed in a Galactic X-ray source, GRS 1915+105. We support a high spin parameter (a(*) > 0.9) for GRS 1915+105 since otherwise the high value of T-in and small size of the emitting region (r(in) < 1r(S)) cannot be explained. C1 [Vierdayanti, K.] Inst Teknol Bandung, FMIPA, Dept Astron, Bandung 40132, Indonesia. [Sadowski, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mineshige, S.] Kyoto Univ, Dept Astron, Kyoto 6068502, Japan. [Bursa, M.] Acad Sci Czech Republic, Astron Inst, CZ-14131 Prague, Czech Republic. RP Vierdayanti, K (reprint author), Inst Teknol Bandung, FMIPA, Dept Astron, Ganesha 10, Bandung 40132, Indonesia. EM kiki@as.itb.ac.id RI Bursa, Michal/G-9004-2014; OI Vierdayanti, Kiki/0000-0001-9989-5008 FU research grant 'Program Hibah Bersaing' (DIPA ITB) [003/TL-J/DIPA/SPK/2011]; Ministry of Education, Culture, Sports, Science, and Technology (MEXT) [22340045]; MEXT; NASA [NNX11AE16G]; [RVO:67985815] FX We gratefully thanks the referees for their comments that help improved this work. This work is supported in part by research grant 'Program Hibah Bersaing' (DIPA ITB 2011 No. 003/TL-J/DIPA/SPK/2011, KV), the Grant-in-Aid of Ministry of Education, Culture, Sports, Science, and Technology (MEXT) (22340045, SM) and by the Grant-in-Aid for the global COE programmes on The Next Generation of Physics, Spun from Diversity and Emergence from MEXT (KV, SM). AS was supported in part by NASA grant NNX11AE16G. MB was supported in part by RVO:67985815. KV thanks Jun Toshikawa and Mahasena Putra for fruitful discussion. NR 45 TC 2 Z9 2 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2013 VL 436 IS 1 BP 71 EP 81 DI 10.1093/mnras/stt1467 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 245BY UT WOS:000326435100028 ER PT J AU Srisawat, C Knebe, A Pearce, FR Schneider, A Thomas, PA Behroozi, P Dolag, K Elahi, PJ Han, JX Helly, J Jing, YP Jung, I Lee, J Mao, YY Onions, J Rodriguez-Gomez, V Tweed, D Yi, SK AF Srisawat, Chaichalit Knebe, Alexander Pearce, Frazer R. Schneider, Aurel Thomas, Peter A. Behroozi, Peter Dolag, Klaus Elahi, Pascal J. Han, Jiaxin Helly, John Jing, Yipeng Jung, Intae Lee, Jaehyun Mao, Yao-Yuan Onions, Julian Rodriguez-Gomez, Vicente Tweed, Dylan Yi, Sukyoung K. TI Sussing Merger Trees: The Merger Trees Comparison Project SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: evolution; galaxies: haloes; dark matter ID FINDER COMPARISON PROJECT; HIERARCHICAL GALAXY FORMATION; DARK-MATTER; HALO-FINDER; EVOLUTION; SUBHALOES; HISTORY; MODELS AB Merger trees follow the growth and merger of dark-matter haloes over cosmic history. As well as giving important insights into the growth of cosmic structure in their own right, they provide an essential backbone to semi-analytic models of galaxy formation. This paper is the first in a series to arise from the Sussing Merger Trees Workshop in which 10 different tree-building algorithms were applied to the same set of halo catalogues and their results compared. Although many of these codes were similar in nature, all algorithms produced distinct results. Our main conclusions are that a useful merger-tree code should possess the following features: (i) the use of particle IDs to match haloes between snapshots; (ii) the ability to skip at least one, and preferably more, snapshots in order to recover subhaloes that are temporarily lost during merging; (iii) the ability to cope with (and ideally smooth out) large, temporary fluctuations in halo mass. Finally, to enable different groups to communicate effectively, we defined a common terminology that we used when discussing merger trees and we encourage others to adopt the same language. We also specified a minimal output format to record the results. C1 [Srisawat, Chaichalit; Schneider, Aurel; Thomas, Peter A.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Knebe, Alexander] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, E-28049 Madrid, Spain. [Pearce, Frazer R.; Onions, Julian] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Behroozi, Peter; Mao, Yao-Yuan] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Behroozi, Peter; Mao, Yao-Yuan] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Behroozi, Peter; Mao, Yao-Yuan] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Dolag, Klaus] Univ Observ Munich, D-81679 Munich, Germany. [Dolag, Klaus] Max Planck Inst Astrophys, D-85740 Garching, Germany. [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; Helly, John] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Jing, Yipeng] Shanghai Jiao Tong Univ, Dept Phys, Ctr Astron & Astrophys, Shanghai 200240, Peoples R China. [Jung, Intae; Lee, Jaehyun; Yi, Sukyoung K.] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Jung, Intae; Lee, Jaehyun; Yi, Sukyoung K.] Yonsei Univ, Yonsei Univ Observ, Seoul 120749, South Korea. [Rodriguez-Gomez, Vicente] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tweed, Dylan] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. RP Srisawat, C (reprint author), Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. EM cs390@sussex.ac.uk RI Knebe, Alexander/N-1815-2014; Jing, Yipeng/P-3678-2015; OI Mao, Yao-Yuan/0000-0002-1200-0820; Knebe, Alexander/0000-0003-4066-8307; Onions, Julian/0000-0001-5192-6856; Schneider, Aurel/0000-0001-7055-8104; Rodriguez-Gomez, Vicente/0000-0002-9495-0079; Pearce, Frazer/0000-0002-2383-9250 FU European Commission through the Marie Curie Initial Training Network CosmoComp [PITN-GA-2009-238356]; HST Theory Grant, NASA through Space Telescope Science Institute; NASA [NAS5-26555]; DFG Cluster of Excellence 'Origin and Structure of the Universe'; SSimPL programme; Sydney Institute for Astronomy (SIfA); STFC; NSFC [11121062 11033006]; CAS/SAFEA International Partnership Program for Creative Research Teams [KJCX2-YW-T23]; Spanish Ministerio de Ciencia e Innovacion (MICINN) in Spain; ASTROMADRID network [AYA 2009-13875-C03-02, CSD2009-00064, CAM S2009/ESP-1496]; Ministerio de Economia y Competitividad (MINECO) [AYA2012-31101]; Consejo Nacional de Ciencia y Tecnologia (CONACyT); Fundacion Mexico en Harvard; Development and Promotion of Science and Technology Talents Project (DPST), Thailand; Science and Technology Facilities Council [ST/I000976/1]; National Research Foundation of Korea [20090078756, 2010-0027910]; Korea Research Council of Fundamental Science and Technology [FY 2012]; KISTI [KSC-2012-C2-11, KSC-2012-C3-10]; Weiland Family Stanford Graduate Fellowship 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.; PSB received support from HST Theory Grant HST-AR-12159.01-A, 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.; KD acknowledges the support by the DFG Cluster of Excellence 'Origin and Structure of the Universe'.; 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.; YPJ is sponsored by NSFC (11121062 11033006) and the CAS/SAFEA International Partnership Program for Creative Research Teams (KJCX2-YW-T23).; AK is supported by the Spanish Ministerio de Ciencia e Innovacion (MICINN) in Spain through the Ramon y Cajal programme as well as the grants AYA 2009-13875-C03-02, CSD2009-00064, CAM S2009/ESP-1496 (from the ASTROMADRID network) and the Ministerio de Economia y Competitividad (MINECO) through grant AYA2012-31101. He further thanks Curtis Mayfield for superfly.; VRG was supported in part by Consejo Nacional de Ciencia y Tecnologia (CONACyT) and Fundacion Mexico en Harvard.; 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).; SKY acknowledges support from National Research Foundation of Korea (Doyak Program No. 20090078756; SRC Program No. 2010-0027910) and DRC Grant of Korea Research Council of Fundamental Science and Technology (FY 2012). Numerical simulation was performed using the KISTI supercomputer under the program of KSC-2012-C2-11 and KSC-2012-C3-10. Much of this manuscript was written during the visit of SKY to the Universities of Nottingham and Oxford under the general support of the LG Yon-Am Foundation.; YYM received support from the Weiland Family Stanford Graduate Fellowship. NR 25 TC 31 Z9 31 U1 0 U2 12 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 NOV PY 2013 VL 436 IS 1 BP 150 EP 162 DI 10.1093/mnras/stt1545 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 245BY UT WOS:000326435100034 ER PT J AU Chakravorty, S Lee, JC Neilsen, J AF Chakravorty, Susmita Lee, Julia C. Neilsen, Joseph TI The effects of thermodynamic stability on wind properties in different low-mass black hole binary states SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; binaries: spectroscopic; stars: winds, outflows; X-rays: binaries; X-rays: stars ID TRANSMISSION GRATING SPECTROMETER; ACTIVE GALACTIC NUCLEI; ACCRETION DISK WIND; X-RAY-EMISSION; GRO J1655-40; WARM ABSORBERS; CHANDRA HETGS; CIRCINUS X-1; CYGNUS X-1; SPECTROSCOPY AB We present a systematic theory-motivated study of the thermodynamic stability condition as an explanation for the observed accretion disc wind signatures in different states of low-mass black hole binaries (BHB). The variability in observed ions is conventionally explained either by variations in the driving mechanisms or by the changes in the ionizing flux or due to density effects, whilst thermodynamic stability considerations have been largely ignored. It would appear that the observability of particular ions in different BHB states can be accounted for through simple thermodynamic considerations in the static limit. Our calculations predict that in the disc-dominated soft thermal and intermediate states, the wind should be thermodynamically stable and hence observable. On the other hand, in the power-law-dominated spectrally hard state the wind is found to be thermodynamically unstable for a certain range of 3.55 <= log xi <= 4.20. In the spectrally hard state, a large number of the He-like and H-like ions (including e. g. Fe XXV, ArXVIII and S XV) have peak ion fractions in the unstable ionization parameter (xi) range, making these ions undetectable. Our theoretical predictions have clear corroboration in the literature reporting differences in wind ion observability as the BHBs transition through the accretion states While this effect may not be the only one responsible for the observed gradient in the wind properties as a function of the accretion state in BHBs, it is clear that its inclusion in the calculations is crucial for understanding the link between the environment of the compact object and its accretion processes. C1 [Chakravorty, Susmita; Lee, Julia C.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Chakravorty, Susmita; Lee, Julia C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neilsen, Joseph] Boston Univ, Boston, MA 02215 USA. [Neilsen, Joseph] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Chakravorty, S (reprint author), Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA. EM schakravorty@head.cfa.harvard.edu RI Lee, Julia/G-2381-2015 OI Lee, Julia/0000-0002-7336-3588 FU Chandra theory grant [TM3-14004X] FX We thank Gary Ferland for making CLOUDY publicly available and for providing helpful tips. We acknowledge the generous support of the Chandra theory grant TM3-14004X that is administered by the Smithsonian Astrophysical Observatory. NR 51 TC 7 Z9 7 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 NOV PY 2013 VL 436 IS 1 BP 560 EP 569 DI 10.1093/mnras/stt1593 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 245BY UT WOS:000326435100068 ER PT J AU Tan, BK Leech, J Rigopoulou, D Warren, BE Wilson, CD Attewell, D Azimlu, M Bendo, GJ Butner, HM Brinks, E Chanial, P Clements, DL Heesen, V Israel, F Knapen, JH Matthews, HE Mortier, AMJ Muhle, S Sanchez-Gallego, JR Tilanus, RPJ Usero, A van der Werf, P Zhu, M AF Tan, Boon-Kok Leech, J. Rigopoulou, D. Warren, B. E. Wilson, C. D. Attewell, D. Azimlu, M. Bendo, G. J. Butner, H. M. Brinks, E. Chanial, P. Clements, D. L. Heesen, V. Israel, F. Knapen, J. H. Matthews, H. E. Mortier, A. M. J. Muehle, S. Sanchez-Gallego, J. R. Tilanus, R. P. J. Usero, A. van der Werf, P. Zhu, M. TI The James Clerk Maxwell Telescope Nearby Galaxies Legacy Survey - IX. (CO)-C-12 J=3 -> 2 observations of NGC 2976 and NGC 3351 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: molecules; galaxies: individual: NGC 2976; galaxies: individual: NGC 3351; galaxies: ISM-infrared: galaxies ID CIRCUMNUCLEAR STAR-FORMATION; WARM MOLECULAR GAS; SPIRAL GALAXIES; RADIAL-DISTRIBUTION; COLD DUST; INTERSTELLAR-MEDIUM; NUCLEAR RINGS; VIRGO CLUSTER; FORMATION LAW; BIMA SURVEY AB We present (CO)-C-12 J = 3 -> 2 maps of NGC 2976 and NGC 3351 obtained with the James Clerk Maxwell Telescope (JCMT), both early targets of the JCMT Nearby Galaxy Legacy Survey (NGLS). We combine the present observations with (CO)-C-12 J = 1 -> 0 data and find that the computed (CO)-C-12 J = 3 -> 2 to (CO)-C-12 J = 1 -> 0 line ratio (R-31) agrees with values measured in other NGLS field galaxies. We compute the M-H2 value and find that it is robust against the value of R-31 used. Using HI data from The HI Nearby Galaxy Survey, we find a tight correlation between the surface density of H-2 and star formation rate density for NGC 3351 when (CO)-C-12 J = 3 -> 2 data are used. Finally, we compare the (CO)-C-12 J = 3 -> 2 intensity with the polycyclic aromatic hydrocarbon (PAH) 8 mu m surface brightness and find a good correlation in the high surface brightness regions. We extend this study to include all 25 Spitzer Infrared Nearby Galaxies Survey galaxies within the NGLS sample and find a tight correlation at large spatial scales. We suggest that both PAH 8 mu m and (CO)-C-12 J = 3 -> 2 are likely to originate in regions of active star formation. C1 [Tan, Boon-Kok; Leech, J.; Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Tan, Boon-Kok] Wawasan Open Univ, Inst Res & Innovat, George Town 10050, Malaysia. [Rigopoulou, D.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Warren, B. E.; Wilson, C. D.; Attewell, D.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Warren, B. E.] Univ Western Australia, Intl Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Azimlu, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bendo, G. J.] Univ Manchester, Jodrell Bank, Ctr Astrophys, UK ALMA Reg Ctr Node, Manchester M13 9PL, Lancs, England. [Butner, H. M.; Usero, A.] James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA. [Brinks, E.; Heesen, V.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Chanial, P.; Clements, D. L.; Mortier, A. M. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Heesen, V.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Israel, F.; van der Werf, P.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Knapen, J. H.; Sanchez-Gallego, J. R.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Knapen, J. H.] Univ La Laguna, Dept Astrofis, E-38200 Tenerife, Spain. [Matthews, H. E.] DRAO, Herzberg Inst Astrophys, NRC, Penticton, BC V2A 69J, Canada. [Muehle, S.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Sanchez-Gallego, J. R.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Tilanus, R. P. J.] Joint Astron Ctr, Hilo, HI 96720 USA. [Tilanus, R. P. J.] Netherlands Org Sci Res, NL-2509 AC The Hague, Netherlands. [Usero, A.] Observ Astron Nacl, E-28014 Madrid, Spain. [Zhu, M.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RP Tan, BK (reprint author), Univ Oxford, Dept Astrophys, Keble Rd, Oxford OX1 3RH, England. EM tanbk@astro.ox.ac.uk OI Brinks, Elias/0000-0002-7758-9699 FU Royal Family of Malaysia through King Scholarship Award; UK Science & Technology Facilities Council (STFC); STFC; NSERC (Canada); European Union under REA [PITN-GA-2011-289313]; National Aeronautics and Space Administration FX The D.Phil. study of BKT at the University of Oxford was supported by the Royal Family of Malaysia through the King Scholarship Award. The work of JL was supported by a Post-Doctoral Research Assistantship from the UK Science & Technology Facilities Council (STFC). The research work of GJB was funded by the STFC, and CDW and BEW were supported by grants from NSERC (Canada). JHK acknowledges financial support to the DAGAL network from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme FP7/2007-2013/ under REA grant agreement number PITN-GA-2011-289313. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The travelling grants to the JCMT for observations are supported by STFC. We would like to thank Bruce Draine and Pauline Barmby for helpful discussions. We would also like to thank all of the staff at the JCMT for their support in carrying out our observations. We would like to thank the reviewer for all the constructive suggestions. NR 76 TC 2 Z9 2 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 NOV PY 2013 VL 436 IS 1 BP 921 EP 933 DI 10.1093/mnras/stt1625 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 245BY UT WOS:000326435100096 ER PT J AU De Marchi, G Panagia, N Guarcello, MG Bonito, R AF De Marchi, Guido Panagia, Nino Guarcello, M. G. Bonito, Rosaria TI Pre-main-sequence stars older than 8 Myr in the Eagle nebula SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; scattering; protoplanetary discs; circumstellar matter; Hertzsprung-Russell and colour-magnitude diagrams; stars: pre-main-sequence ID MASS ACCRETION RATES; YOUNG STELLAR OBJECTS; OPEN CLUSTER NGC-6611; H-ALPHA EMISSION; X-RAY-PROPERTIES; T-TAURI STARS; PHOTOMETRIC-DETERMINATION; CIRCUMSTELLAR DISKS; NGC 6611; PROTOPLANETARY DISKS AB Attention is given to a population of 110 stars in the NGC 6611 cluster of the Eagle nebula that have prominent near-infrared excess and optical colours typical of pre-main-sequence (PMS) stars older than 8 Myr. At least half of those for which spectroscopy exists have a H alpha emission line profile revealing active accretion. In principle, the V - I colours of all these stars would be consistent with those of young PMS objects (< 1 Myr) whose radiation is heavily obscured by a circumstellar disc seen at high inclination and in small part scattered towards the observer by the back side of the disc. However, using theoretical models it is shown here that objects of this type can only account for a few per cent of this population. In fact, the spatial distribution of these objects, their X-ray luminosities, their optical brightness, their positions in the colour-magnitude diagram and the weak Li absorption lines of the stars studied spectroscopically suggest that most of them are at least eight times older than the similar to 1 Myr-old PMS stars already known in this cluster and could be as old as similar to 30 Myr. This is the largest homogeneous sample to date of Galactic PMS stars considerably older than 8 Myr that are still actively accreting from a circumstellar disc and it allows us to set a lower limit of 7 per cent to the disc frequency at similar to 16 Myr in NGC 6611. These values imply a characteristic exponential lifetime of similar to 6 Myr for disc dissipation. C1 [De Marchi, Guido] European Space Agcy, European Space Res & Technol Ctr, NL-2200 AG Noordwijk, Netherlands. [Panagia, Nino] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Panagia, Nino] Osserv Astron Capodimonte, INAF NA, I-80131 Naples, Italy. [Panagia, Nino] Supernova Ltd, Virgin Gorda, W Ind Assoc St. [Guarcello, M. G.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Bonito, Rosaria] Univ Palermo, Dipartimento Fis & Chim, I-90134 Palermo, Italy. [Bonito, Rosaria] Osserv Astron Palermo, INAF PA, I-90134 Palermo, Italy. RP De Marchi, G (reprint author), European Space Agcy, European Space Res & Technol Ctr, Keplerlaan 1, NL-2200 AG Noordwijk, Netherlands. EM gdemarchi@rssd.esa.int FU STScI-DDRF [D0001.82435]; Agenzia Spaziale Italiana [ASI-INAF (I/009/10/0)]; [GO0-11040X] FX We are indebted to Jeffrey Linsky, the referee, for insightful comments and suggestions that have helped us to improve the presentation of this work. We are also grateful to Thayne Currie for interesting conversations about the time-scale of disc dissipation. NP acknowledges partial support by STScI-DDRF grant D0001.82435. MGG's research is supported by Chandra Grant GO0-11040X. RB acknowledges the support of the Agenzia Spaziale Italiana under contract ASI-INAF (I/009/10/0). NR 79 TC 10 Z9 10 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 NOV PY 2013 VL 435 IS 4 BP 3058 EP 3070 DI 10.1093/mnras/stt1499 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236DP UT WOS:000325774700022 ER PT J AU Reig, P Papadakis, IE Sobolewska, MA Malzac, J AF Reig, P. Papadakis, I. E. Sobolewska, M. A. Malzac, J. TI Evidence for a change in the radiation mechanism in the hard state of GRO J1655-40. Hysteresis in the broad-band noise components SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; X-rays: binaries ID BLACK-HOLE BINARIES; X-RAY BINARIES; QUASI-PERIODIC OSCILLATIONS; POWER SPECTRAL COMPONENTS; ACCRETION DISK CORONAE; CYGNUS X-1; TEMPORAL CORRELATIONS; TIMING PROPERTIES; 2005 OUTBURST; GX 339-4 AB We have analysed archival data from the Rossi X-ray Timing Explorer (RXTE) to study the aperiodic variability of the black hole binary GRO J1655-40 during the hard state of the 2005 outburst. This work was motivated by the recent finding of a spectral change in the hard state X-ray radiation mechanism in black hole binaries. We computed the 0.008-64 Hz power spectral density during the rise and decay of the 2005 outburst, and we found that they were reasonably well modelled by the sum of two, broad Lorenztian functions in most cases (plus a narrow QPO), which correspond to three different variability components. Our aim is to study the evolution of the timing properties of the source during the outburst, by studying the correlation between the characteristics of the broad-band noise components in the power spectra and the source luminosity. Our results suggest that the whole power spectrum shifts to high (low) frequencies as the source luminosity increases (decreases), in agreement with previous studies of other black hole binaries. However, we also detect a strong 'hysteresis' pattern in the 'frequency-luminosity' plots, and show that the 'critical' luminosity limit, above which the timing properties of the source change, is different during the rise and the decay phase of the outburst. We discuss the general implications of these results in the context of the truncated disc model. C1 [Reig, P.; Papadakis, I. E.] Fdn Res & Technol, IESL, GR-71110 Iraklion, Crete, Greece. [Reig, P.; Papadakis, I. E.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. [Reig, P.; Papadakis, I. E.] Univ Crete, Inst Theoret & Computat Phys, GR-71003 Iraklion, Crete, Greece. [Sobolewska, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Malzac, J.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France. [Malzac, J.] CNRS, IRAP, F-31028 Toulouse 4, France. RP Reig, P (reprint author), Fdn Res & Technol, IESL, GR-71110 Iraklion, Crete, Greece. EM pau@physics.uoc.gr RI Reig, Pablo/A-1198-2014; Papadakis, Iossif/C-3235-2011 OI Reig, Pablo/0000-0002-6446-3050; FU French Research National Agency: CHAOS project [ANR-12-BS05-0009]; PNHE in France FX JM acknowledges financial support from the French Research National Agency: CHAOS project ANR-12-BS05-0009 (http://www.chaos-project.fr) and from PNHE in France. This research has made use of data and 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. NR 44 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2013 VL 435 IS 4 BP 3395 EP 3405 DI 10.1093/mnras/stt1532 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236DP UT WOS:000325774700050 ER PT J AU van der Heijden, GM Schnitzer, SA Powers, JS Phillips, OL AF van der Heijden, Geertje M. Schnitzer, Stefan A. Powers, Jennifer S. Phillips, Oliver L. TI Liana Impacts on Carbon Cycling, Storage and Sequestration in Tropical Forests SO BIOTROPICA LA English DT Review DE carbon balance; carbon cycle; carbon sequestration; lianas; tree growth; tree mortality; tropical forests ID BELOW-GROUND COMPETITION; HOST LIQUIDAMBAR-STYRACIFLUA; NET PRIMARY PRODUCTIVITY; BARRO-COLORADO ISLAND; TIERRA-FIRME FOREST; LEAF-AREA INDEX; RAIN-FOREST; AMAZONIAN FORESTS; ELEVATED CO2; TREE GROWTH AB Mature tropical forests sequester large quantities of atmospheric CO2, which they store as plant biomass. These forests are changing however, including an increase in liana abundance and biomass over recent decades in Neotropical forests. We ask here how this increase in lianas might impact the tropical forest carbon cycle and their capacity for carbon storage and sequestration. Lianas reduce tree growth, survival, and leaf productivity; however, lianas also invest significantly in leaf production, and the increase in lianas could conceivably offset liana-induced reductions in tree canopy productivity with no adverse effects to the forest-level canopy productivity. By contrast, lianas decrease the total ecosystem uptake of carbon by reducing tree biomass productivity. Lianas themselves invest little in woody biomass, and store and sequester only a small proportion of the biomass in tropical forests. As lianas increase they may effectively displace trees, but the greater liana carbon stocks are unlikely to compensate for liana-induced losses in net carbon sequestration and storage by trees. A potentially important additional consideration is the impact of lianas on the tree community. By competing more intensely with shade-tolerant, more densely wooded trees than with fast-growing, light-wooded trees, lianas may shift tree composition toward faster-growing species, which store relatively little carbon, and thereby further reduce the carbon storage capacity of tropical forests. Overall, current evidence indicates that the increase in lianas will negatively impact the carbon balance of tropical forests, with potentially far-reaching consequences for global atmospheric CO2 levels and associated climate change. C1 [van der Heijden, Geertje M.; Schnitzer, Stefan A.] Univ Wisconsin Milwaukee, Milwaukee, WI 53201 USA. [van der Heijden, Geertje M.; Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Balboa, Panama. [Powers, Jennifer S.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. [Powers, Jennifer S.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. [Phillips, Oliver L.] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. RP Phillips, OL (reprint author), Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. EM o.phillips@leeds.ac.uk RI Phillips, Oliver/A-1523-2011; OI Phillips, Oliver/0000-0002-8993-6168; Schnitzer, Stefan/0000-0002-2715-9455 FU Explorer's Club; Coalbourn Trust; Alberta Mennega Foundation; University of Leeds; European Research Council; Royal Society Wolfson Research Merit Award; NSF [DEB-0613666, DEB-0845071, DEB-1019436, DEB-1019441]; University of Wisconsin-Milwaukee Research Growth Initiative program FX Fieldwork at Tambopata was possible through grants from the Explorer's Club, the Coalbourn Trust, and the Alberta Mennega Foundation, financial support from the University of Leeds and logistical support from the Instituto National para Recursos Naturales (INRENA) and Peruvian Safaris S.A. We thank Tatiana Boza Espinoza for help with liana data collection, Abel Monteagudo and Rodolfo Vasquez for their contribution to tree species determination at Tambopata and Yadvinder Malhi for sharing his carbon cycle graphics template. Support for OL Phillips was provided by an Advanced Grant from the European Research Council, "Tropical forests in the changing earth system" and by a Royal Society Wolfson Research Merit Award. Research and support for SA Schnitzer and GMF van der Heijden in Panama by was supported by NSF grants DEB-0613666, DEB-0845071, DEB-1019436, and the University of Wisconsin-Milwaukee Research Growth Initiative program. JS Powers gratefully acknowledges support from NSF grant DEB-1019441. NR 109 TC 30 Z9 30 U1 9 U2 61 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 NOV PY 2013 VL 45 IS 6 SI SI BP 682 EP 692 DI 10.1111/btp.12060 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 243RA UT WOS:000326333400004 ER PT J AU Krupnick, GA AF Krupnick, Gary A. TI Conservation of Tropical Plant Biodiversity: What Have We Done, Where Are We Going? SO BIOTROPICA LA English DT Review DE climate change; global strategy for plant conservation; management; protected areas; threatened species; tropical ecosystems ID TIMBER FOREST PRODUCT; SOUTHEAST-ASIAN BIODIVERSITY; FUTURE CLIMATE-CHANGE; RAIN-FOREST; GLOBAL CHANGE; ECOSYSTEM CONSEQUENCES; FRAGMENTATION GENETICS; HABITAT FRAGMENTATION; NORTHEASTERN BRAZIL; HERBARIUM SPECIMENS AB Plant biodiversity in the tropics is threatened by intense anthropogenic pressures. Deforestation, habitat degradation, habitat fragmentation, overexploitation, invasive species, pollution, global climate change, and the synergies among them have had a major impact on biodiversity. This review paper provides a brief, yet comprehensive and broad, overview of the main threats to tropical plant biodiversity and how they differ from threats in temperate regions. The Global Strategy for Plant Conservation, an international program with 16 global targets set for 2020 aimed at understanding, conserving, and using sustainably the world's plant biodiversity, is then used as a framework to explore efforts in assessing and managing tropical plant conservation in a changing world. Progress on 13 of the 16 outcome-oriented targets of the Strategy is explored at the pantropical scale. Within each target, I address current challenges in assessing and managing tropical plant biodiversity, identify key questions that should be addressed, and suggest ways for how these challenges might be overcome. C1 Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Krupnick, GA (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM krupnickg@si.edu OI Krupnick, Gary/0000-0002-1357-4826 NR 214 TC 4 Z9 4 U1 10 U2 117 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 NOV PY 2013 VL 45 IS 6 SI SI BP 693 EP 708 DI 10.1111/btp.12064 PG 16 WC Ecology SC Environmental Sciences & Ecology GA 243RA UT WOS:000326333400005 ER PT J AU Rick, TC Erlandson, JM Jew, NP Reeder-Myers, LA AF Rick, Torben C. Erlandson, Jon M. Jew, Nicholas P. Reeder-Myers, Leslie A. TI Archaeological survey, paleogeography, and the search for Late Pleistocene Paleocoastal peoples of Santa Rosa Island, California SO JOURNAL OF FIELD ARCHAEOLOGY LA English DT Article DE Paleoindian; Channel Islands; lithic scatter; coastal migration; sea level rise ID CHANNEL-ISLANDS; NORTH-AMERICA; OCCUPATIONS; ADAPTATIONS; CALIBRATION; UNDERWATER; ROUTES; SITES; FOOD AB The northern Pacific Coast is an important area for understanding human colonization of the Americas, but Late Pleistocene coastal sites are rare and interglacial sea level rise has inundated the continental shelf and the primary areas where Paleocoastal archaeological sites are likely to occur. Here we outline a terrestrial archaeological survey project designed to identify Paleocoastal sites on Santa Rosa Island, California. Using reconstructions of ancient shorelines and paleogeography, we predicted that sites might be found where lithic resources, freshwater springs, caves or rockshelters, and strategic vistas drew Paleocoastal peoples into the island interior. We identified nine new Paleocoastal sites, including four radiocarbon dated to >11,000 CAL B.P. that are among the oldest sites on North America's Pacific coast. Our targeted survey demonstrates an important technique for investigating island and coastal settings where sea level rise remains a significant challenge for locating early sites. C1 [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Jew, Nicholas P.] Univ Oregon, Eugene, OR 97403 USA. [Reeder-Myers, Leslie A.] So Methodist Univ, Dept Anthropol, Dallas, TX 75275 USA. RP Rick, TC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Dept Anthropol, Washington, DC 20013 USA. EM rickt@si.edu OI Erlandson, Jon/0000-0002-4705-4319 NR 46 TC 14 Z9 14 U1 1 U2 18 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0093-4690 EI 2042-4582 J9 J FIELD ARCHAEOL JI J. Field Archaeol. PD NOV PY 2013 VL 38 IS 4 BP 324 EP 331 DI 10.1179/0093469013Z.00000000065 PG 8 WC Archaeology SC Archaeology GA 242VU UT WOS:000326273100003 ER PT J AU Harrison, I Evans, M Lowe-McConnell, R Parenti, L Sanford, C Snyder, L Stiassny, M Vari, R AF Harrison, Ian Evans, Malcolm Lowe-McConnell, Rosemary Parenti, Lynne Sanford, Chris Snyder, Lex Stiassny, Melanie Vari, Rich TI Gordon John Howes 1938-2013 (Fish Systematist) OBITUARY SO JOURNAL OF FISH BIOLOGY LA English DT Biographical-Item C1 [Harrison, Ian] Conservat Int, Arlington, VA 22202 USA. [Harrison, Ian] Conservat Int, Ctr Environm & Peace, Amer Museum Nat Hist, Arlington, VA 22202 USA. [Parenti, Lynne; Vari, Rich] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Sanford, Chris] Hofstra Univ, Dept Biol, Hempstead, NY 11549 USA. [Snyder, Lex] 1 Univ New Mexico, Div Fishes, Museum Southwestern Biol, Albuquerque, NM 87131 USA. [Stiassny, Melanie] Amer Museum Nat Hist, Dept Ichthyol, New York, NY 10024 USA. RP Harrison, I (reprint author), Conservat Int, Ctr Environm & Peace, 2011 Crystal Dr,Suite 500, Arlington, VA 22202 USA. NR 17 TC 0 Z9 0 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1112 EI 1095-8649 J9 J FISH BIOL JI J. Fish Biol. PD NOV PY 2013 VL 83 IS 5 BP 1085 EP 1093 DI 10.1111/jfb.12260 PG 9 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 245PU UT WOS:000326476700001 PM 24580656 ER PT J AU Temkin, I Strong, EE AF Temkin, Ilya Strong, Ellen E. TI New insights on stomach anatomy of carnivorous bivalves SO JOURNAL OF MOLLUSCAN STUDIES LA English DT Article ID CARDIOMYA-PLANETICA DALL; FUNCTIONAL-MORPHOLOGY; DEEP-SEA; PREY CAPTURE; ANOMALODESMATA; MOLLUSCA; PHYLOGENY; DIGESTION; CLASSIFICATION; PECTINACEA AB Carnivory is unusual among bivalve molluscs and is limited to a few families in the distantly related orders Pectinida, Mytilida and Anomalodesmata. Despite the significance of dietary shifts in the evolution of the bivalves, the anatomy of the alimentary system, and of the gastric chamber in particular, has been described in detail for only a few carnivorous species. Here we describe the anatomy of the gastric chamber in a pectinid, Propeamussium jeffreysii, and an anomalodesmatan, Bathyneaera demistriata, expanding the known morphological disparity of the alimentary system in both groups. We found the stomachs of both to be modified to varying degrees for a carnivorous habit, with thickened, muscular walls, extensive cuticular linings, and reduced sorting areas and gastric chamber compartments (i.e. the dorsal hood, the left pouch and the food-sorting caecum). Despite some superficial similarity, each retains distinct hallmarks of their ancestry among filter-feeding relatives, allowing precise homology assessment of individual characters to differentiate between them. In addition, we found that the gastric chamber of P. jeffreysii represents an intermediate morphology between previously described P. lucidum and filter-feeding pectinids. Consequently, variation in the anatomy of the gastric chamber in Pectinida parallels a previously identified trend towards greater specialization for carnivory in the Anomalodesmata. Our results indicate that the current classification scheme of stomach types does not reflect phylogenetic affinity across the Bivalvia and highlight the need for accurate homology assessment of individual characters of the gastric chamber for inferring evolutionary relationships. C1 [Temkin, Ilya; Strong, Ellen E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Temkin, Ilya] No Virginia Community Coll, Dept Biol, Annandale, VA 22003 USA. RP Temkin, I (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012,MRC 163, Washington, DC 20013 USA. EM temkini@si.edu FU NSF [0726382]; Total Foundation; Prince Albert II of Monaco Foundation; Stavros Niarchos Foundation; NSF-AToL Bivalve Tree of Life Project [DEB-0732854/0732903/0732860] FX We are grateful to H. H. Dijkstra (University of Amsterdam, Zoological Museum, The Netherlands) for identification of Propeamussium jeffreysii from Mozambique, and E. M. Harper (University of Cambridge, UK), E. M. Krylova (P. P. Shirshov Institute of Oceanology, Moscow, Russia) and C. Oliveira (Universidade Federal do Rio de Janeiro, Rio de Janeiro, Brasil) for identification of Bathyneaera demistriata. We thank R. Bieler and S. Staubach (FMNH, Chicago, USA) for photographs of B. demistriata, and J.D. Zardus (The Citadel, Charleston, USA) for information on collection stations of this species. We also would like to thank E. M. Harper and A. Sartori (Museum National d'Histoire Naturelle, Paris, MNHN) for insightful comments and suggestions. The specimens of B. demistriata were collected by J. Zardus during the EN447 cruise in 2008 funded by NSF 0726382 grant (to R. Etter and M. Rex). The specimens from deep water off Mozambique were collected by R. V. Vizconde de Eza during the MAINBAZA cruise (PI, P. Bouchet) in April 2009. The cruise was operated by MNHN and Instituto Espanol de Oceanografia, as part of a cluster of Mozambique-Madagascar expeditions funded by the Total Foundation, Prince Albert II of Monaco Foundation and Stavros Niarchos Foundation, and conducted by MNHN and Pro-Natura International. This work was made possible by NSF-AToL Bivalve Tree of Life Project DEB-0732854/0732903/0732860 (to R. Bieler, G. Giribet and P.M. Mikkelsen). NR 48 TC 6 Z9 7 U1 1 U2 10 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0260-1230 EI 1464-3766 J9 J MOLLUS STUD JI J. Molluscan Stud. PD NOV PY 2013 VL 79 BP 332 EP 339 DI 10.1093/mollus/eyt031 PN 4 PG 8 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 244HW UT WOS:000326379600006 ER PT J AU Gordon, IE Rotger, M Tennyson, J AF Gordon, Iouli E. Rotger, Maud Tennyson, Jonathan TI Preface to the HITRAN 2012 special issue SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Editorial Material C1 [Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Rotger, Maud] Univ Reims, CNRS, UMR 7331, Grp Spectrometrie Mol & Atmospher, F-51687 Reims, France. [Tennyson, Jonathan] UCL, Dept Phys & Astron, London WC1E 6BT, England. RP Gordon, IE (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. EM igordon@cfa.harvard.edu; maud.rotger@univ-reims.fr; j.tennyson@ucl.ac.uk RI Tennyson, Jonathan/I-2222-2012; OI Tennyson, Jonathan/0000-0002-4994-5238; Gordon, Iouli/0000-0003-4763-2841 NR 0 TC 4 Z9 4 U1 3 U2 19 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 NOV PY 2013 VL 130 SI SI BP 1 EP 3 DI 10.1016/j.jqsrt.2013.07.007 PG 3 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 245RS UT WOS:000326482100001 ER PT J AU Rothman, LS Gordon, IE Babikov, Y Barbe, A Benner, DC Bernath, PF Birk, M Bizzocchi, L Boudon, V Brown, LR Campargue, A Chance, K Cohen, EA Coudert, LH Devi, VM Drouin, BJ Fayt, A Flaud, JM Gamache, RR Harrison, JJ Hartmann, JM Hill, C Hodges, JT Jacquemart, D Jolly, A Lamouroux, J Le Roy, RJ Li, G Long, DA Lyulin, OM Mackie, CJ Massie, ST Mikhailenko, S Muller, HSP Naumenko, OV Nikitin, AV Orphal, J Perevalov, V Perrin, A Polovtseva, ER Richard, C Smith, MAH Starikova, E Sung, K Tashkun, S Tennyson, J Toon, GC Tyuterev, VG Wagner, G AF Rothman, L. S. Gordon, I. E. Babikov, Y. Barbe, A. Benner, D. Chris Bernath, P. F. Birk, M. Bizzocchi, L. Boudon, V. Brown, L. R. Campargue, A. Chance, K. Cohen, E. A. Coudert, L. H. Devi, V. M. Drouin, B. J. Fayt, A. Flaud, J. -M. Gamache, R. R. Harrison, J. J. Hartmann, J. -M. Hill, C. Hodges, J. T. Jacquemart, D. Jolly, A. Lamouroux, J. Le Roy, R. J. Li, G. Long, D. A. Lyulin, O. M. Mackie, C. J. Massie, S. T. Mikhailenko, S. Mueller, H. S. P. Naumenko, O. V. Nikitin, A. V. Orphal, J. Perevalov, V. Perrin, A. Polovtseva, E. R. Richard, C. Smith, M. A. H. Starikova, E. Sung, K. Tashkun, S. Tennyson, J. Toon, G. C. Tyuterev, Vl. G. Wagner, G. TI The HITRAN2012 molecular spectroscopic database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE HITRAN; Spectroscopic database; Molecular spectroscopy; Molecular absorption; Spectroscopic line parameters; Absorption cross-sections; Aerosols ID MU-M REGION; ABSORPTION CROSS-SECTIONS; CW-CAVITY RING; COMPLEX REFRACTIVE-INDEXES; SPECTRAL-LINE PARAMETERS; O-2 A-BAND; INCLUDING TEMPERATURE DEPENDENCES; ELECTRIC QUADRUPOLE TRANSITIONS; ROTATIONAL-VIBRATIONAL SPECTRA; SUBMILLIMETER-WAVE SPECTRUM AB This paper describes the status of the 2012 edition of the HITRAN molecular spectroscopic compilation. The new edition replaces the previous HITRAN edition of 2008 and its updates during the intervening years. The HITRAN molecular absorption compilation is comprised of six major components structured into folders that are freely accessible on the internet. These folders consist of the traditional line-by-line spectroscopic parameters required for high-resolution radiative-transfer codes, infrared absorption cross-sections for molecules not yet amenable to representation in a line-by-line form, ultraviolet spectroscopic parameters, aerosol indices of refraction, collision-induced absorption data, and general tables such as partition sums that apply globally to the data. The new HITRAN is greatly extended in terms of accuracy, spectral coverage, additional absorption phenomena, and validity. Molecules and isotopologues have been added that address the issues of atmospheres beyond the Earth. Also discussed is a new initiative that casts HITRAN into a relational database format that offers many advantages over the long-standing sequential text-based structure that has existed since the initial release of HITRAN in the early 1970s. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Rothman, L. S.; Gordon, I. E.; Chance, K.; Li, G.; Mackie, C. J.; Richard, C.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Babikov, Y.; Lyulin, O. M.; Mikhailenko, S.; Naumenko, O. V.; Nikitin, A. V.; Perevalov, V.; Polovtseva, E. R.; Starikova, E.; Tashkun, S.] VE Zuev Inst Atmospher Opt SB RAS, Tomsk 634021, Russia. [Barbe, A.; Tyuterev, Vl. G.] Univ Reims, Grp Spectrometrie Mol & Atmospher, F-51062 Reims, France. [Benner, D. Chris; Devi, V. M.] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. [Bernath, P. F.] Old Dominion Univ, Dept Chem & Biochem, Norfolk, VA 23529 USA. [Birk, M.; Wagner, G.] DLR, Remote Sensing Technol Inst, D-82234 Wessling, Germany. [Bizzocchi, L.] Observ Astron Lisboa, CAAUL, Lisbon, Portugal. [Boudon, V.] Univ Bourgogne, CNRS, UMR 6303, Lab Interdisciplinaire Carnot Bourgogne, F-21078 Dijon, France. [Brown, L. R.; Cohen, E. A.; Drouin, B. J.; Sung, K.; Toon, G. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Campargue, A.] Univ Grenoble 1, CNRS, LIPhy UMR5588, F-38402 St Martin Dheres, France. [Coudert, L. H.; Flaud, J. -M.; Hartmann, J. -M.; Jolly, A.; Lamouroux, J.; Perrin, A.] Hop Henri Mondor, CNRS, F-94010 Creteil, France. [Coudert, L. H.; Flaud, J. -M.; Hartmann, J. -M.; Jolly, A.; Lamouroux, J.; Perrin, A.] Univ Paris 07, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. [Fayt, A.] Catholic Univ Louvain, Lab Spect Mol, B-1348 Louvain, Belgium. [Gamache, R. R.; Lamouroux, J.] Univ Mass Lowell, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. [Harrison, J. J.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Hill, C.; Tennyson, J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Hodges, J. T.; Long, D. A.] NIST, Gaithersburg, MD 20899 USA. [Jacquemart, D.] Univ Paris 06, UMR 7075, Lab Dynam Interact & React, F-75252 Paris, France. [Le Roy, R. J.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. [Massie, S. T.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Mueller, H. S. P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Orphal, J.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76344 Eggenstein Leopoldshafen, Germany. [Smith, M. A. H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM LSR_JQSRT@verizon.net RI Tennyson, Jonathan/I-2222-2012; Bernath, Peter/B-6567-2012; BOUDON, Vincent/A-4504-2010; Orphal, Johannes/A-8667-2012; Starikova, Evgeniya/E-8680-2014; Nikitin, Andrei/K-2624-2013; Tashkun, Sergey/E-8682-2014; Babikov, Yurii/E-8686-2014; Li, Gang/P-2272-2015; Harrison, Jeremy/L-1073-2016; Sung, Keeyoon/I-6533-2015; OI Tennyson, Jonathan/0000-0002-4994-5238; Bernath, Peter/0000-0002-1255-396X; Orphal, Johannes/0000-0002-1943-4496; Nikitin, Andrei/0000-0002-4280-4096; Li, Gang/0000-0002-5605-7896; Harrison, Jeremy/0000-0001-5530-7104; Bizzocchi, Luca/0000-0002-9953-8593; Mueller, Holger/0000-0002-0183-8927; Chance, Kelly/0000-0002-7339-7577; Mackie, Cameron/0000-0003-2885-2021; Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 FU NASA AURA [NNX11AF91G]; NASA [NNX10AB94G]; National Science Foundation; National Aeronautics and Space Administration FX The management and development of the HITRAN molecular database has been supported by NASA AURA mission Grant NNX11AF91G, and NASA Planetary Atmosphere Grant NNX10AB94G.; NCAR is sponsored by the National Science Foundation. Part of the research at the College of William and Mary, Langley Research Center, and the Jet Propulsion Laboratory an), California Institute of Technology was performed under contract with the National Aeronautics and Space Administration. NR 352 TC 988 Z9 1016 U1 36 U2 241 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 NOV PY 2013 VL 130 SI SI BP 4 EP 50 DI 10.1016/j.jqsrt.2013.07.002 PG 47 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 245RS UT WOS:000326482100002 ER PT J AU Hill, C Gordon, IE Rothman, LS Tennyson, J AF Hill, Christian Gordon, Iouli E. Rothman, Laurence S. Tennyson, Jonathan TI A new relational database structure and online interface for the HITRAN database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Line-lists; Radiative transfer; Databases; HITRAN ID MOLECULAR SPECTROSCOPIC DATABASE; INTERNAL PARTITION SUMS; MU-M; LINE; SPECTRA; BAND AB A new format for the HITRAN database is proposed. By storing the line-transition data in a number of linked tables described by a relational database schema, it is possible to overcome the limitations of the existing format, which have become increasingly apparent over the last few years as new and more varied data are being used by radiative-transfer models. Although the database in the new format can be searched using the well-established Structured Query Language (SQL), a web service. HITRANonline, has been deployed to allow users to make most common queries of the database using a graphical user interface in a web page. The advantages of the relational form of the database to ensuring data integrity and consistency are explored, and the compatibility of the online interface with the emerging standards of the Virtual Atomic and Molecular Data Centre (VAMDC) project is discussed. In particular, the ability to access HITRAN data using a standard query language from other websites, command line tools and from within computer programs is described. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Hill, Christian; Tennyson, Jonathan] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Gordon, Iouli E.; Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Hill, C (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM christian.hill@ucl.ac.uk RI Tennyson, Jonathan/I-2222-2012; OI Tennyson, Jonathan/0000-0002-4994-5238; Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 FU VAMDC; ERC [267219]; "Combination of Coordination and Support Actions" Funding Scheme of The Seventh Framework Program [INFRA-2012-3.3, 313284] FX This work is supported by the VAMDC project and ERC Advanced Investigator Project 267219 (ExoMol). VAMDC is funded under the "Combination of Coordination and Support Actions" Funding Scheme of The Seventh Framework Program. Call topic: INFRA-2012-3.3 Scientific Data Infrastructure. Grant Agreement number: 313284). NR 21 TC 18 Z9 18 U1 3 U2 18 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 NOV PY 2013 VL 130 SI SI BP 51 EP 61 DI 10.1016/j.jqsrt.2013.04.027 PG 11 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 245RS UT WOS:000326482100003 ER PT J AU Brown, LR Sung, K Benner, DC Devi, VM Boudon, V Gabard, T Wenger, C Campargue, A Leshchishina, O Kassi, S Mondelain, D Wang, L Daumont, L Regalia, L Rey, M Thomas, X Tyuterev, VG Lyulin, OM Nikitin, AV Niederer, HM Albert, S Bauerecker, S Quack, M O'Brien, JJ Gordon, IE Rothman, LS Sasada, H Coustenis, A Smith, MAH Carrington, T Wang, XG Mantz, AW Spickler, PT AF Brown, L. R. Sung, K. Benner, D. C. Devi, V. M. Boudon, V. Gabard, T. Wenger, C. Campargue, A. Leshchishina, O. Kassi, S. Mondelain, D. Wang, L. Daumont, L. Regalia, L. Rey, M. Thomas, X. Tyuterev, Vl G. Lyulin, O. M. Nikitin, A. V. Niederer, H. M. Albert, S. Bauerecker, S. Quack, M. O'Brien, J. J. Gordon, I. E. Rothman, L. S. Sasada, H. Coustenis, A. Smith, M. A. H. Carrington, T., Jr. Wang, X-G Mantz, A. W. Spickler, P. T. TI Methane line parameters in the HITRAN2012 database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Methane; Line parameters; Remote sensing; Planets; Exoplanets; HITRAN database ID MOLECULAR SPECTROSCOPIC DATABASE; M TRANSPARENCY WINDOW; MULTISPECTRUM FITTING TECHNIQUE; INDUCED SHIFT COEFFICIENTS; LISTS 5852-7919 CM(-1); BROADENED HALF-WIDTHS; MIRS COMPUTER PACKAGE; MU-M REGION; NU(3) BAND; INFRARED-SPECTRUM AB The compilation of methane molecular line parameters was updated to include new global analyses and measurements for (CH4)-C-12, (CH4)-C-13 and (CH3D)-C-12. Over 70% of the methane parameters in HITRAN2008 were replaced; existing parameters retained were the microwave lines and the Dyad of (CH4)-C-13 near 7 mu m and nu(6) of (CH3D)-C-13 near 8.7 mu m, (CH3D)-C-12 (7-4076 cm(-1)), hot bands of (CH4)-C-12 (1887-3370 cm(-1)) and normal sample CH4 (4800-5550 cm(-1) and 8000-9200 cm(-1)). With a minimum intensity at 296 K in units of cm(-1)/(molecule cm(-2)) set to 10(-37) for the far-IR and 10(-29) for the mid- and near-IR, the methane database increased from 290,091 lines in HITRAN2008 to 468,013 lines, and three-fourths of these involved the main isotopologue. For (CH4)-C-12 and (CH4)-C-13, bands from the ground state were revised up to 4800 cm(-1). For the first time, (CH4)-C-13 and (CH3D)-C-12 line parameters near 2.3 mu m were included. Above 5550 cm(-1), the new compilation was based on empirical measurements. Prior laboratory results were replaced with extensive new measurements using FTIR (5550-5852 cm(-1)), differential absorption spectroscopy (DAS) and Cavity Ring Down Spectroscopy (CRDS) (5852-7912 cm(-1)). Ground state J values for nearly half of the measured lines in this range were obtained, either by confirming quantum assignments of analyses or by using spectra at 80 and 296 K. Finally, over 11,000 measured positions, intensities and empirical lower state energies (obtained using cold CH4) were also added for the first time between 10,923 and 11,502 cm(-1). Available pressure broadening measurements from HITRAN2008 were transferred into the new compilation, but 99% of the lines were given crudely-estimated coefficients. New measured intensities and broadening coefficients were included for far-IR transitions, and high accuracy line positions were inserted for the stronger P, Q and R branch transitions of nu(3) at 3.3 mu m and 2 nu(3) at 1.66 mu m. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Brown, L. R.; Sung, K.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Benner, D. C.; Devi, V. M.] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. [Boudon, V.; Gabard, T.; Wenger, C.] Univ Bourgogne, CNRS, UMR 6303, Lab Interdisciplinaire Carnot Bourgogne, F-21078 Dijon, France. [Campargue, A.; Leshchishina, O.; Kassi, S.; Mondelain, D.; Wang, L.] Univ Grenoble 1, CNRS, LIPhy UMR5588, F-38041 Grenoble, France. [Daumont, L.; Regalia, L.; Rey, M.; Thomas, X.; Tyuterev, Vl G.] Univ Reims, CNRS, UMR 7331, Grp Spectrometrie Mol & Atmospher, F-51687 Reims 2, France. [Lyulin, O. M.; Nikitin, A. V.] SB RAS, VE Zuev Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634021, Russia. [Niederer, H. M.; Albert, S.; Bauerecker, S.; Quack, M.] ETH, Phys Chem Lab, CH-8093 Zurich, Switzerland. [O'Brien, J. J.] Univ Missouri, Dept Chem & Biochem, St Louis, MO 63121 USA. [Gordon, I. E.; Rothman, L. S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Sasada, H.] Keio Univ, Dept Phys, Fac Sci & Technol, Kohoku Ku, Yokohama, Kanagawa 2238522, Japan. [Coustenis, A.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Smith, M. A. H.] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA. [Carrington, T., Jr.; Wang, X-G] Queens Univ, Dept Chem, Kingston, ON K7L 3N6, Canada. [Mantz, A. W.] Connecticut Coll, Dept Phys Astron & Geophys, New London, CT 06320 USA. [Spickler, P. T.] Bridgewater Coll, Dept Phys, Bridgewater, VA 22812 USA. RP Brown, LR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM linda.r.brown@jpl.nasa.gov RI BOUDON, Vincent/A-4504-2010; CARRINGTON, Tucker/I-6727-2012; Nikitin, Andrei/K-2624-2013; Quack, Martin/H-4457-2016; Sung, Keeyoon/I-6533-2015; OI CARRINGTON, Tucker/0000-0002-5200-2353; Nikitin, Andrei/0000-0002-4280-4096; Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 FU ANR Project "CH4@Titan" [BLAN08-2_321467]; LEFE-Chat CNRS French; Groupement de Recherche International SAMIA [22]; fundamental problems of investigation and exploration of the Solar System of Russian Academia of Science; Ministry of Education, Culture, Sports, Science and Technology in Japan; Swiss National Science Foundation; ETH Zurich; Natural Sciences and Engineering Research Council of Canada; Canadian Space Agency and CAS (China); IDRIS/CINES computer centers of France; National Aeronautics and Space Administration; Martin Summer Science Research Institute; American Astronomical Society Small Research Grant FX This work is part of the ANR Project "CH4@Titan" (Ref: BLAN08-2_321467). The international funding support includes the LEFE-Chat CNRS French grant and the Groupement de Recherche International SAMIA between CNRS (France) and RFBR (Russia), Program Number 22: the fundamental problems of investigation and exploration of the Solar System of Russian Academia of Science; Grant in Aid for Scientific Research (A) and the Photon Frontier Network Program of the Ministry of Education, Culture, Sports, Science and Technology in Japan; the Swiss National Science Foundation, ETH Zurich; the Natural Sciences and Engineering Research Council of Canada, the Canadian Space Agency and CAS (China). We are grateful for the support from IDRIS/CINES computer centers of France and also the computer center Reims-Champagne-Ardenne.r Part of the research at the College of William and Mary, Connecticut College, Langley Research Center, the Harvard-Smithsonian Center for Astrophysics and the Jet Propulsion Laboratory (JPL) was performed under contract with National Aeronautics and Space Administration. Funding for research at Bridgewater College was provided by the Martin Summer Science Research Institute and from an American Astronomical Society Small Research Grant. NR 119 TC 51 Z9 52 U1 4 U2 44 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 NOV PY 2013 VL 130 SI SI BP 201 EP 219 DI 10.1016/j.jqsrt.2013.06.020 PG 19 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 245RS UT WOS:000326482100015 ER PT J AU Li, G Gordon, IE Hajigeorgiou, PG Coxon, JA Rothman, LS AF Li, Gang Gordon, Iouli E. Hajigeorgiou, Photos G. Coxon, John A. Rothman, Laurence S. TI Reference spectroscopic data for hydrogen halides, Part II: The line lists SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Hydrogen halides; Deuterated species; Line position calculation; Line-shape parameters; HITRAN database ID DIPOLE-MOMENT FUNCTION; HIGH-RESOLUTION MEASUREMENTS; VIBRATION-ROTATION BANDS; TUNABLE DIODE-LASERS; 1ST OVERTONE BAND; SHIFTING PARAMETERS; HYPERFINE-STRUCTURE; FUNDAMENTAL BANDS; HI MOLECULE; RARE-GASES AB Accurate spectroscopic parameters for the hydrogen halides, namely HF, HCl, HBr, and HI, together with their deuterated isotopologues, are crucial for the quantitative study of terrestrial and planetary atmospheres, astrophysical objects, and chemical lasers. A thorough evaluation of all the hydrogen halide line parameters in previous HITRAN editions has been carried out. A new set of line lists was generated for the HITRAN2012 edition using methods described here. In total, 131,798 entries were generated for numerous pure-rotational and to-vibrational transitions (fundamental, overtone, and hot bands) for hydrogen halides and their deuterated species in a standard HITRAN 160-character format. Data for the deuterated isotopologues have been entered into HITRAN for the first time. The calculations employ the recently developed semi-empirical dipole moment functions [Li G, et al. J Quant Spectrosc Radiat Transfer 2013;121:78-90] and very accurate analytical potential energy functions and associated functions characterizing Born-Oppenheimer breakdown effects. Line-shape parameters have also been updated using the most recent available experimental and theoretical studies. Comparison with the previous HITRAN compilation has shown significant improvements. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Li, Gang; Gordon, Iouli E.; Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Hajigeorgiou, Photos G.] Univ Nicosia, Dept Life & Hlth Sci, CY-1700 Nicosia, Cyprus. [Coxon, John A.] Dalhousie Univ, Dept Chem, Halifax, NS B3H 4J3, Canada. RP Li, G (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, MS 50,60 Garden St, Cambridge, MA 02138 USA. EM gangli@cfa.harvard.edu RI Li, Gang/P-2272-2015; OI Li, Gang/0000-0002-5605-7896; Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 FU NASA [NNX10AB94G]; University of Nicosia FX We thank R.J. Le Roy for useful suggestions and discussions for this project. Support from NASA Planetary Atmospheres Grant NNX10AB94G for this study is gratefully acknowledged. PGH acknowledges the University of Nicosia for financial support of research activities. NR 78 TC 10 Z9 10 U1 4 U2 29 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 NOV PY 2013 VL 130 SI SI BP 284 EP 295 DI 10.1016/j.jqsrt.2013.07.019 PG 12 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 245RS UT WOS:000326482100021 ER PT J AU Liu, C Liu, X Chance, K AF Liu, Cheng Liu, Xiong Chance, Kelly TI The impact of using different ozone cross sections on ozone profile retrievals from OMI UV measurements SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Ozone cross section; Ozone profile retrieval; OMI; UV; Ozonesonde; Validation ID ULTRAVIOLET AB We compare three datasets of high-resolution O-3 cross sections and evaluate the effects of using these cross sections on O-3 profile retrievals from OMI UV (270-330 nm) measurements. These O-3 cross sections include Brion-Daumont-Malicet (BDM), Bass-Paur (BP) and a new dataset measured by Serdyuchenko et al. (SGWCB), which is made from measurements at more temperatures and in a wider temperature range than BDM and BP, 193-293 K. Relative to the BDM dataset, the SGWCB data have systematic biases of -2 to +4% for 260-340 nm, and the BP data have smaller biases of 1-2% below 315 nm but larger spiky biases of up to +/- 6% at longer wavelengths. These datasets show distinctly different temperature dependences. Using different cross sections can significantly affect atmospheric retrievals. Using SGWCB data leads to retrieval failure for almost half of the OMI spatial pixels, producing large negative ozone values that cannot be handled by radiative transfer models and using BP data leads to large fitting residuals over 310-330 nm. Relative to the BDM retrievals, total ozone retrieved using original SGWCB data (with linear temperature interpolation/extrapolation) typically shows negative biases of 5-10 DU; retrieved tropospheric ozone column generally shows negative biases of 5-10 DU and 5-20 DU for parameterized and original SGWCB data, respectively. Compared to BDM retrievals, ozone profiles retrieved with BP/SGWCB data on average show large altitude-dependent oscillating differences of up to +/- 20-40% biases below 20 km with almost opposite bias patterns. Validation with ozonesonde observations demonstrates that the BDM retrievals agree well with ozonesondes, to typically within 10%, while both BP and SGWCB retrievals consistently show large altitude-dependent biases of up to +/- 20-70% below 20 km. Therefore, we recommend using the BDM dataset for ozone profile retrievals from UV measurements. Its improved performance is likely due to its better characterization of temperature dependence in the Hartley and Huggins bands. Published by Elsevier Ltd. C1 [Liu, Cheng; Liu, Xiong; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Liu, X (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM xliu@cfa.harvard.edu RI Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU NASA Aura Science Team Grant [NNX11AE95G]; Smithsonian Institution FX This study is supported by the NASA Aura Science Team Grant (NNX11AE95G) and the Smithsonian Institution. We thank the OMI science team for providing OMI level 1b data, and Aura AVDC, WOUDC, CMDL, and SHADOZ and their data originators for providing ozonesonde measurements. Finally, we acknowledge the two anonymous reviewers for providing constructive comments. NR 13 TC 2 Z9 2 U1 0 U2 4 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 NOV PY 2013 VL 130 SI SI BP 365 EP 372 DI 10.1016/j.jqsrt.2013.06.006 PG 8 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 245RS UT WOS:000326482100031 ER PT J AU Choi, S Onofrio, R Sundaram, B AF Choi, Stephen Onofrio, Roberto Sundaram, Bala TI Ehrenfest dynamics and frictionless cooling methods SO PHYSICAL REVIEW A LA English DT Article ID QUANTUM-MECHANICS; FREE-MASS; SYSTEMS; STATES; ADIABATICITY; POTENTIALS; CHAOS AB Recently introduced methods which result in shortcuts to adiabaticity, particularly in the context of frictionless cooling, are rederived and discussed in the framework of an approach based on Ehrenfest dynamics. This construction provides physical insights into the emergence of the Ermakov equation, the choice of its boundary conditions, and the use of minimum uncertainty states as indicators of the efficiency of the procedure. Additionally, it facilitates the extension of frictionless cooling to more general situations of physical relevance, such as optical dipole trapping schemes. In this context, we discuss frictionless cooling in the short-time limit, a complementary case to the one considered in the literature, making explicit the limitations intrinsic to the technique when the full three-dimensional case is analyzed. C1 [Choi, Stephen; Sundaram, Bala] Univ Massachusetts, Dept Phys, Boston, MA 02125 USA. [Onofrio, Roberto] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35131 Padua, Italy. [Onofrio, Roberto] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Choi, S (reprint author), Univ Massachusetts, Dept Phys, Harbor Campus, Boston, MA 02125 USA. NR 42 TC 5 Z9 5 U1 0 U2 5 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 NOV 1 PY 2013 VL 88 IS 5 AR 053401 DI 10.1103/PhysRevA.88.053401 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 245ZL UT WOS:000326504500002 ER PT J AU Banda, JM Angryk, RA Martens, PCH AF Banda, J. M. Angryk, R. A. Martens, P. C. H. TI Steps Toward a Large-Scale Solar Image Data Analysis to Differentiate Solar Phenomena SO SOLAR PHYSICS LA English DT Article DE Solar image data analysis; Content-based image retrieval (CBIR); Dissimilarity measures ID RETRIEVAL; FEATURES AB We detail the investigation of the first application of several dissimilarity measures for large-scale solar image data analysis. Using a solar-domain-specific benchmark dataset that contains multiple types of phenomena, we analyzed combinations of image parameters with different dissimilarity measures to determine the combinations that will allow us to differentiate between the multiple solar phenomena from both intra-class and inter-class perspectives, where by class we refer to the same types of solar phenomena. We also investigate the problem of reducing data dimensionality by applying multi-dimensional scaling to the dissimilarity matrices that we produced using the previously mentioned combinations. As an early investigation into dimensionality reduction, we investigate by applying multidimensional scaling (MDS) how many MDS components are needed to maintain a good representation of our data (in a new artificial data space) and how many can be discarded to enhance our querying performance. Finally, we present a comparative analysis of several classifiers to determine the quality of the dimensionality reduction achieved with this combination of image parameters, similarity measures, and MDS. C1 [Banda, J. M.; Angryk, R. A.] Montana State Univ, Dept Comp Sci, Bozeman, MT 59717 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 Banda, JM (reprint author), Montana State Univ, Dept Comp Sci, Bozeman, MT 59717 USA. EM juan.banda@cs.montana.edu; angryk@cs.montana.edu; martens@physics.montana.edu OI Banda, Juan/0000-0001-8499-824X FU NASA [08-SDOSC08-0008]; Solar Dynamics Observatory Science Center solicitation [NNH08ZDA001N-SDOSC] FX This work was supported in part by the NASA Grant Award No. 08-SDOSC08-0008, funded from NNH08ZDA001N-SDOSC: Solar Dynamics Observatory Science Center solicitation. We would also like to thank our internal reviewers Michael Schuh and Richard McAllister. NR 37 TC 2 Z9 2 U1 0 U2 2 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 NOV PY 2013 VL 288 IS 1 BP 435 EP 462 DI 10.1007/s11207-013-0304-x PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 242LK UT WOS:000326243200024 ER PT J AU Gowaty, PA AF Gowaty, Patricia Adair TI Adaptively flexible polyandry SO ANIMAL BEHAVIOUR LA English DT Article DE adaptively flexible behaviour; demographic stochasticity; multiple mating; phenotypic plasticity; polyandry; sexual selection; switch point theorem; within-sex selection ID OFFSPRING VIABILITY; SEXUAL SELECTION; MATING SUCCESS; DROSOPHILA-PSEUDOOBSCURA; NATURAL-POPULATIONS; EASTERN BLUEBIRDS; SIALIA-SIALIS; FEMALES; EVOLUTION; BENEFITS AB Mating theory (Hubbell & Johnson 1987, American Naturalist, 130, 91-112; Gowaty & Hubbell 2009, Proceedings of the National Academy of Sciences, U.S.A., 106, 10017-10024) says that reproductive decisions of individuals are flexibly expressed and adaptive. It also makes the following five predictions about polyandry. (1) Demography determines within-population, between-female variation in mating rates. That is, (a) an individual's encounters with potential mates, (b) an individual's risk of death, (c) the number of potential mates in the population, (d) the distribution of fitness under random mating, and (e) for nonvirgins, the duration of any postcopulation period of nonreceptivity together determine within-population, between-female variation in mating rate. (2) When demography is dynamic, there is unlikely to be an optimal female mating rate. That is, when potential mates enter or leave the pool of potential mates or when decision makers face survival risks from conspecifics, predators, parasites or pathogens, females who adaptively adjust their reproductive decisions in real-time outcompete females whose behaviour is fixed. (3) Female multiple mating often increases production of adult offspring through enhanced offspring viability (indirect fitness) and between-generation lineage success. (4) Polyandry will increase female exposure to pathogens and thus decrease female survival (direct fitness cost) unless females use environmental or intrinsic resources or opportunities to reduce survival risks. (5) Under many circumstances, female remating may enhance female survival (direct fitness benefit). Future research attention will focus on how intrinsic, ecological and social opportunities/constraints affect the likelihood of polyandry and its fitness effects for particular females. Future researchers may also consider that polyandrous mating is sometimes sexually collaborative and cooperative, rather than always sexually antagonistic. The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. C1 [Gowaty, Patricia Adair] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Gowaty, Patricia Adair] Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA 90095 USA. [Gowaty, Patricia Adair] Smithsonian Trop Res Inst, Washington, DC USA. [Gowaty, Patricia Adair] Polistes Fdn, Belmont, MA USA. RP Gowaty, PA (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, 621 Charles E Young Dr South, Los Angeles, CA 90095 USA. EM gowaty@eeb.ucla.edu FU National Science Foundation [IBN-9631801, IBN-0911606, IOS-1121797] FX I thank Steve Hubbell for helping to keep our collaborative work so interesting and outrageously fun, for making Fig. 3, and for our many conversations about variance in mating rate and mate number. I thank Wyatt W. Anderson, Lee C. Drickamer, Allen Moore and an anonymous referee for comments on an earlier version of the manuscript. I am grateful to the Editors of Animal Behaviour, particularly Michelle Pellissier Scott, who offered me the opportunity to write about polyandry for this Anniversary edition of Animal Behaviour and also provided useful comments on the manuscript. I acknowledge National Science Foundation Grants IBN-9631801, IBN-0911606, and IOS-1121797, each of which supported empirical work informing the ideas here. NR 62 TC 7 Z9 7 U1 4 U2 59 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD NOV PY 2013 VL 86 IS 5 BP 877 EP 884 DI 10.1016/j.anbehav.2013.08.015 PG 8 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 242VO UT WOS:000326272200005 ER PT J AU Knornschild, M Feifel, M Kalko, EKV AF Knoernschild, Mirjam Feifel, Marion Kalko, Elisabeth K. V. TI Mother-offspring recognition in the bat Carollia perspicillata SO ANIMAL BEHAVIOUR LA English DT Article DE Carollia perspicillata; male courtship; maternal care; maternal experience; playback experiment; Seba's short-tailed fruit bat ID TAILED FRUIT BAT; SPEAR-NOSED BATS; INDIVIDUAL RECOGNITION; SOCIAL-BEHAVIOR; MATERNAL-BEHAVIOR; VOCAL RECOGNITION; VERVET MONKEYS; ORGANIZATION; CHIROPTERA; EXPERIENCE AB Parental care is crucial for offspring survival in many taxa but its burden and costs are often not equally distributed between the sexes. In bats, the majority of parental care is provided by females, making examples of paternal support towards pups exceedingly rare. One exception to this general pattern seemed to be the polygynous Seba's short-tailed fruit bat Carollia perspicillata; two earlier studies suggested that paternal care occurs, i.e. that harem males prompt females to retrieve vocalizing pups. To corroborate this suggestion, we investigated the occurrence of maternal and paternal care in reaction to pup isolation calls in C. perspicillata. Acoustic measurements of 905 isolation calls from 17 pups revealed sufficient interindividual variation to encode an individual vocal signature. Correspondingly, mothers were capable of using this individual signature to discriminate between their own pups and age-matched pups from other females belonging to their colony. Maternal experience was positively correlated with the strength of response behaviour during playbacks. Thus, our results indicate that pup isolation calls were used to elicit maternal care and that mothers recognize their pups based on an individual signature in isolation calls. However, in contrast to the previous studies mentioned above, we found no evidence that harem males reacted to pup isolation calls by prompting the respective mothers to retrieve their vocalizing pups. Instead, our results demonstrate that harem males engaged in courtship activities that were unaffected by pup isolation calls. (C) 2013 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Knoernschild, Mirjam; Feifel, Marion; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, Fac Nat Sci, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Knornschild, M (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM mirjam.knoernschild@uni-ulm.de RI Knornschild, Mirjam/C-9401-2011 FU University of Ulm, Germany FX Valuable comments by M. Metz, M. Nagy and two anonymous referees substantially improved the manuscript. We are indebted to Stefanie Aichele and Simone Pechmann for supporting us when studying male courtship behaviour. We are especially grateful to the Bat Center GmbH Noctalis, Bad Segeberg, Germany (http://www.noctalis.de/) for taking care of all C. perspicillata after the completion of our study. This work was supported by a start-up grant from the University of Ulm, Germany (M.K.). NR 64 TC 10 Z9 11 U1 1 U2 32 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD NOV PY 2013 VL 86 IS 5 BP 941 EP 948 DI 10.1016/j.anbehav.2013.08.011 PG 8 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 242VO UT WOS:000326272200013 ER PT J AU Bayliss, D Zhou, G Penev, K Bakos, GA Hartman, JD Jordan, A Mancini, L Mohler-Fischer, M Suc, V Rabus, M Beky, B Csubry, Z Buchhave, L Henning, T Nikolov, N Csak, B Brahm, R Espinoza, N Noyes, RW Schmidt, B Conroy, P Wright, DJ Tinney, CG Addison, BC Sackett, PD Sasselov, DD Lazar, J Papp, I Sari, P AF Bayliss, D. Zhou, G. Penev, K. Bakos, G. A. Hartman, J. D. Jordan, A. Mancini, L. Mohler-Fischer, M. Suc, V. Rabus, M. Beky, B. Csubry, Z. Buchhave, L. Henning, T. Nikolov, N. Csak, B. Brahm, R. Espinoza, N. Noyes, R. W. Schmidt, B. Conroy, P. Wright, D. J. Tinney, C. G. Addison, B. C. Sackett, P. D. Sasselov, D. D. Lazar, J. Papp, I. Sari, P. TI HATS-3b: AN INFLATED HOT JUPITER TRANSITING AN F-TYPE STAR SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HATS-3, GSC 6926-00454); techniques: photometric; techniques: spectroscopic ID SOUTHERN-HEMISPHERE; RADIAL-VELOCITIES; PLANETARY SYSTEM; SURFACE-GRAVITY; FIELD; PHOTOMETRY; STELLAR; KEPLER; SPECTROGRAPH; OBLIQUITIES AB We report the discovery by the HATSouth survey of HATS-3b, a transiting extrasolar planet orbiting a V = 12.4 F dwarf star. HATS-3b has a period of P = 3.5479 days, mass of M-p = 1.07 M-J, and radius of R-p = 1.38 R-J. Given the radius of the planet, the brightness of the host star, and the stellar rotational velocity (nu sin i = 9.0 km s(-1)), this system will make an interesting target for future observations to measure the Rossiter-McLaughlin effect and determine its spin-orbit alignment. We detail the low-/medium-resolution reconnaissance spectroscopy that we are now using to deal with large numbers of transiting planet candidates produced by the HATSouth survey. We show that this important step in discovering planets produces log g and T-eff parameters at a precision suitable for efficient candidate vetting, as well as efficiently identifying stellar mass eclipsing binaries with radial velocity semi-amplitudes as low as 1 km s(-1). C1 [Bayliss, D.; Zhou, G.; Schmidt, B.; Conroy, P.; Sackett, P. D.] 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.; Beky, B.; Csubry, Z.; Noyes, R. W.; Sasselov, D. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jordan, A.; Suc, V.; Rabus, M.; Brahm, R.; Espinoza, N.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 7820436, Chile. [Mancini, L.; Mohler-Fischer, M.; Henning, T.; Nikolov, N.; Csak, B.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Buchhave, L.] Univ Copenhagen, Niels Bohr Inst, DK-1168 Copenhagen, Denmark. [Wright, D. J.; Tinney, C. G.; Addison, B. C.] Univ New S Wales, Sch Phys, Exoplanetary Sci UNSW, Sydney, NSW 2052, Australia. [Wright, D. J.; Tinney, C. G.; Addison, B. C.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Bayliss, D (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. EM daniel@mso.anu.edu.au RI Bayliss, Daniel/I-4635-2012; OI Jordan, Andres/0000-0002-5389-3944; Penev, Kaloyan/0000-0003-4464-1371; Schmidt, Brian/0000-0001-6589-1287; Tinney, Christopher/0000-0002-7595-0970; Buchhave, Lars A./0000-0003-1605-5666; Nikolov, Nikolay/0000-0002-6500-3574; Hartman, Joel/0000-0001-8732-6166 FU NASA [NNX09AB29G]; ARC [FL0992131, FS100100046]; BASAL [CATA PFB-06]; FONDECYT postdoctoral fellowship [3120097]; CONICYT-PCHA/Doctorado Nacional and Fondecyt [1130857]; Robert Martin Ayers Sciences Fund; SIMBAD database, operated at CDS, Strasbourg, France; [NSF/AST-1108686] FX Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074, operations are supported by NASA grant NNX09AB29G, 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, Ministry of Economy ICM Nucleus P10-022-F, Anillo ACT-086, and BASAL CATA PGB-06. V.S. acknowledges support from BASAL CATA PFB-06. M.R. acknowledges support from FONDECYT postdoctoral fellowship No. 3120097. 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 089. A-9006(A). This paper also uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope. Work at UNSW has been supported by ARC Australian Professorial Fellowship grant DP0774000, ARC LIEF grant LE0989347, and ARC Super Science Fellowships FS100100046. 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 highenergy group of MPE in collaboration with the LSW Tautenburg and ESO. We thank Timo Anguita and Regis Lachaume for their technical assistance during the observations at the MPG/ESO 2.2 m Telescope. NR 52 TC 29 Z9 29 U1 1 U2 6 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 NOV PY 2013 VL 146 IS 5 AR 113 DI 10.1088/0004-6256/146/5/113 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238UK UT WOS:000325976200010 ER PT J AU Cowperthwaite, PS Massaro, F D'Abrusco, R Paggi, A Tosti, G Smith, HA AF Cowperthwaite, Philip S. Massaro, F. D'Abrusco, R. Paggi, A. Tosti, G. Smith, Howard A. TI IDENTIFICATION OF NEW GAMMA-RAY BLAZAR CANDIDATES WITH MULTIFREQUENCY ARCHIVAL OBSERVATIONS SO ASTRONOMICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; galaxies: active; radiation mechanisms: non-thermal Online-only material: color figure ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; ALL-SKY SURVEY; BRIGHT SOURCE CATALOG; BL LACERTAE OBJECTS; DATA RELEASE; MICROQUASAR CANDIDATES; RADIO-SOURCES; SAMPLE; EMISSION AB Blazars are a highly variable, radio-loud subclass of active galactic nuclei. In order to better understand such objects we must be able to easily identify candidate blazars from the growing population of unidentified sources. Working toward this goal, we attempt to identify new gamma-ray blazar candidates from a sample of 102 previously unidentified sources. These sources are selected from The Astronomer's Telegram and the literature on the basis of non-periodic variability and multi-wavelength behavior. We then attempt to associate these objects to an IR counterpart in the Wide-field Infrared Survey Explorer all-sky survey. We are able to identify 16 candidate sources whose IR colors are consistent with those of the blazar population. Of those, 13 sources have IR colors indicative of being gamma-ray emitting blazar candidates. These sources all possess archival multi-wavelength observations that support their blazar-like nature. C1 [Cowperthwaite, Philip S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Cowperthwaite, Philip S.] Joint Space Sci Inst JSI, College Pk, MD 20742 USA. [Massaro, F.] SLAC Natl Lab, Menlo Pk, CA 94025 USA. [Massaro, F.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Cowperthwaite, Philip S.; D'Abrusco, R.; Paggi, A.; Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. RP Cowperthwaite, PS (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM pcowpert@umd.edu RI D'Abrusco, Raffaele/L-2767-2016; Massaro, Francesco/L-9102-2016; Paggi, Alessandro/C-1219-2017; OI D'Abrusco, Raffaele/0000-0003-3073-0605; Massaro, Francesco/0000-0002-1704-9850; Paggi, Alessandro/0000-0002-5646-2410; Cowperthwaite, Philip/0000-0002-2478-6939 FU NASA [NNX10AD50G, NNH09ZDA001N, NNX10AD68G]; NSF REU; DOD ASSURE programs under NSF [0754568]; Smithsonian Institution; NSF [DGE1144152]; National Science Foundation; National Aeronautics and Space Administration; Fermi [NNX13AP20G]; Foundation BLANCE-FLOR; ASI/INAF [I/005/12/0] FX We thank our anonymous referee for many helpful comments that greatly improved this paper. The work is supported by NASA grants NNX10AD50G, NNH09ZDA001N, and NNX10AD68G. P.S.C. is grateful for support by the NSF REU and DOD ASSURE programs under NSF grant no. 0754568, by the Smithsonian Institution, and for partial support through NSF GRFP grant DGE1144152. R.D'A. gratefully acknowledges the financial support of the US Virtual Astronomical Observatory, which is sponsored by the National Science Foundation and the National Aeronautics and Space Administration, and additional financial support from Fermi grant NNX13AP20G. F.M. acknowledges the Foundation BLANCE-FLOR Boncompagni-Ludovisi, n'ee Bildt for the grant awarded to him in 2010 to support his research. The work by G. T. is supported by the ASI/INAF contract I/005/12/0. TOPCAT12 (Taylor 2005) and SAOImage DS9 were used extensively in this work for the preparation and manipulation of the tabular data and the images. This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC) provided by NASA's Goddard Space Flight Center; the SIMBAD database operated at CDS, Strasbourg, France; and the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Part of this work is based on archival data, software, or online services provided by the ASI Science Data Center. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 136 TC 7 Z9 7 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 NOV PY 2013 VL 146 IS 5 AR 110 DI 10.1088/0004-6256/146/5/110 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238UK UT WOS:000325976200007 ER PT J AU Oliveira, I van der Laan, M Brown, JM AF Oliveira, Isa van der Laan, Margriet Brown, Joanna M. TI NEW X-RAY-SELECTED PRE-MAIN-SEQUENCE MEMBERS OF THE SERPENS MOLECULAR CLOUD SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; Hertzsprung-Russell and C-M diagrams; ISM: individual objects (Serpens); stars: pre-main-sequence ID SPITZER C2D SURVEY; T-TAURI STARS; YOUNG STELLAR OBJECTS; SYMMETRIC MODEL ATMOSPHERES; ORION ULTRADEEP PROJECT; LOW-MASS STARS; PROTOPLANETARY DISCS; INTERSTELLAR CLOUDS; BROWN DWARFS; EFFECTIVE TEMPERATURES AB The study of young stars no longer surrounded by disks can greatly add to our understanding of how protoplanetary disks evolve and planets form. We have used VLT/FLAMES optical spectroscopy to confirm the youth and membership of 19 new young diskless stars in the Serpens Molecular Cloud, identified at X-ray wavelengths. Spectral types, effective temperatures, and stellar luminosities were determined using optical spectra and optical/near-infrared photometry. Stellar masses and ages were derived based on pre-main-sequence evolutionary tracks. The results yield remarkable similarities for age and mass distribution between the diskless and disk-bearing stellar populations in Serpens. We discuss the important implications these similarities may have on the standard picture of disk evolution. C1 [Oliveira, Isa] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [van der Laan, Margriet] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Brown, Joanna M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Oliveira, I (reprint author), Univ Texas Austin, McDonald Observ, 1 Univ Stn,C1402, Austin, TX 78712 USA. EM oliveira@astro.as.utexas.edu FU ESO Telescopes at the Paranal Observatories [083.C-0766(B)] FX This work is based on observations made with the ESO Telescopes at the Paranal Observatories under program ID 083.C-0766(B). The authors would like to thank the anonymous referee for her/his suggestions, which greatly improved this manuscript. NR 62 TC 1 Z9 1 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD NOV PY 2013 VL 146 IS 5 AR 105 DI 10.1088/0004-6256/146/5/105 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238UK UT WOS:000325976200002 ER PT J AU Reipurth, B Bally, J Aspin, C Connelley, MS Geballe, TR Kraus, S Appenzeller, I Burgasser, A AF Reipurth, Bo Bally, John Aspin, Colin Connelley, M. S. Geballe, T. R. Kraus, Stefan Appenzeller, Immo Burgasser, Adam TI HH 222: A GIANT HERBIG-HARO FLOW FROM THE QUADRUPLE SYSTEM V380 ORI SO ASTRONOMICAL JOURNAL LA English DT Article DE Herbig-Haro objects; ISM: individual objects (HH 222); ISM: jets and outflows; proper motions; stars: individual (V380 Ori); stars: pre-main sequence ID REFLECTION NEBULA NGC-1999; YOUNG STELLAR OBJECTS; TRIPLE RADIO-SOURCE; T-TAURI STARS; AE/BE STARS; BODY PROBLEM; EMISSION; ORIONIS; REGION; OUTFLOWS AB HH 222 is a giant shocked region in the L1641 cloud, and is popularly known as the Orion Streamers or "the waterfall" on account of its unusual structure. At the center of these streamers are two infrared sources coincident with a nonthermal radio jet aligned along the principal streamer. The unique morphology of HH 222 has long been associated with this radio jet. However, new infrared images show that the two sources are distant elliptical galaxies, indicating that the radio jet is merely an improbable line-of-sight coincidence. Accurate proper motion measurements of HH 222 reveal that the shock structure is a giant bow shock moving directly away from the well-known, very young, Herbig Be star V380 Ori. The already known Herbig-Haro object HH 35 forms part of this flow. A new Herbig-Haro object, HH 1041, is found precisely in the opposite direction of HH 222 and is likely to form part of a counterflow. The total projected extent of this HH complex is 5.3 pc, making it among the largest HH flows known. A second outflow episode from V380 Ori is identified as a pair of HH objects, HH 1031 to the northwest and the already known HH 130 to the southeast, along an axis that deviates from that of HH 222/HH 1041 by only 3 degrees.7. V380 Ori is a hierarchical quadruple system, including a faint companion of spectral type M5 or M6, which at an age of similar to 1 Myr corresponds to an object straddling the stellar-to-brown dwarf boundary. We suggest that the HH 222 giant bow shock is a direct result of the dynamical interactions that led to the conversion from an initial non-hierarchical multiple system into a hierarchical configuration. This event occurred no more than 28,000 yr ago, as derived from the proper motions of the HH 222 giant bow shock. C1 [Reipurth, Bo; Aspin, Colin; Connelley, M. S.] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA. [Bally, John] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Geballe, T. R.] Gemini Observ, Hilo, HI 96720 USA. [Kraus, Stefan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Appenzeller, Immo] Landessternwarte Heidelberg, D-69117 Heidelberg, Germany. [Burgasser, Adam] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. RP Reipurth, B (reprint author), Univ Hawaii Manoa, Inst Astron, 640 North Aohoku Pl, Hilo, HI 96720 USA. EM reipurth@ifa.hawaii.edu; John.Bally@colorado.edu; caa@ifa.hawaii.edu; msc@ifa.hawaii.edu; tgeballe@gemini.edu; stefan.kraus@cfa.harvard.edu; iappenze@lsw.uni-heidelberg.de; aburgasser@ucsd.edu FU Gemini Observatory; National Science Foundation [NSF AST-0407005]; National Aeronautics and Space Administration through the NASA Astrobiology Institute [NNA09DA77A] FX We thank the referee, Thomas Stanke, for useful comments. B. R. thanks ESO for hospitality in Garching while much of this paper was written. This work is based in part on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan (NAOJ). I. A. would like to thank the staff of the ESO Paranal Observatory for the excellent support of the FORS team during the commissioning run (programme 60.A-9203(E). This project was supported by the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina, Australia, Brazil, Canada, Chile, the UK, and the US. M.S.C. and B.R. were Visiting Astronomers at the Infrared Telescope Facility, which is operated by the University of Hawaii under cooperative agreement No. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Bibliographic Services. B.R. acknowledges support by the National Science Foundation under grant NSF AST-0407005. This material is based upon work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under cooperative agreement No. NNA09DA77A issued through the Office of Space Science. This research has benefited from the SpeX Prism Spectral Libraries, maintained by Adam Burgasser at http://www.browndwarfs.org/spexprism. NR 58 TC 8 Z9 8 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD NOV PY 2013 VL 146 IS 5 AR 118 DI 10.1088/0004-6256/146/5/118 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 238UK UT WOS:000325976200015 ER PT J AU Appleton, PN Guillard, P Boulanger, F Cluver, ME Ogle, P Falgarone, E des Forets, GP O'Sullivan, E Duc, PA Gallagher, S Gao, Y Jarrett, T Konstantopoulos, I Lisenfeld, U Lord, S Lu, N Peterson, BW Struck, C Sturm, E Tuffs, R Valchanov, I van der Werf, P Xu, KC AF Appleton, P. N. Guillard, P. Boulanger, F. Cluver, M. E. Ogle, P. Falgarone, E. des Forets, G. Pineau O'Sullivan, E. Duc, P. -A. Gallagher, S. Gao, Y. Jarrett, T. Konstantopoulos, I. Lisenfeld, U. Lord, S. Lu, N. Peterson, B. W. Struck, C. Sturm, E. Tuffs, R. Valchanov, I. van der Werf, P. Xu, K. C. TI SHOCK-ENHANCED C+ EMISSION AND THE DETECTION OF H2O FROM THE STEPHAN'S QUINTET GROUP-WIDE SHOCK USING HERSCHEL SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: groups: individual (Stephan's Quintet); infrared: galaxies ID STAR-FORMING GALAXIES; SPECTRAL ENERGY-DISTRIBUTION; MOLECULAR-HYDROGEN EMISSION; RADIO-CONTINUUM EMISSION; INTERSTELLAR-MEDIUM; PHOTODISSOCIATION REGIONS; INFRARED-EMISSION; II LINE; X-RAY; TURBULENT DISSIPATION AB We present the first Herschel spectroscopic detections of the [O I] 63 mu m and [C II] 158 mu m fine-structure transitions, and a single para-H2O line from the 35 x 15 kpc(2) shocked intergalactic filament in Stephan's Quintet. The filament is believed to have been formed when a high-speed intruder to the group collided with a clumpy intergroup gas. Observations with the PACS spectrometer provide evidence for broad (>1000 km s(-1)) luminous [C II] line profiles, as well as fainter [O I] 63 mu m emission. SPIRE FTS observations reveal water emission from the p-H2O (1(11)-0(00)) transition at several positions in the filament, but no other molecular lines. The H2O line is narrow and may be associated with denser intermediate-velocity gas experiencing the strongest shock-heating. The [C II]/PAH(tot) and [C II]/FIR ratios are too large to be explained by normal photo-electric heating in photodissociation regions. H II region excitation or X-ray/cosmic-ray heating can also be ruled out. The observations lead to the conclusion that a large fraction the molecular gas is diffuse and warm. We propose that the [C II], [O I], and warm H-2 line emission is powered by a turbulent cascade in which kinetic energy from the galaxy collision with the intergalactic medium is dissipated to small scales and low velocities, via shocks and turbulent eddies. Low-velocity magnetic shocks can help explain both the [C II]/[O I] ratio, and the relatively high [C II]/H-2 ratios observed. The discovery that [C II] emission can be enhanced, in large-scale turbulent regions in collisional environments, has implications for the interpretation of [C II] emission in high-z galaxies. C1 [Appleton, P. N.; Lord, S.; Lu, N.; Xu, K. C.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Guillard, P.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Guillard, P.; Boulanger, F.; des Forets, G. Pineau] Univ Paris 11, Inst Astrophys Spatiale, Orsay, France. [Cluver, M. E.; Konstantopoulos, I.] Australian Astron Observ, Epping, NSW, Australia. [Ogle, P.] CALTECH, NASA Extragalact Database, IPAC, Pasadena, CA 91125 USA. [Falgarone, E.] Observ Paris, Ecole Normale Super, F-75231 Paris, France. [O'Sullivan, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Duc, P. -A.] Lab AIM, Paris, France. [Gallagher, S.] Univ Western Ontario, London, ON, Canada. [Gao, Y.] Purple Mt Observ, Nanjing, Jiangsu, Peoples R China. [Jarrett, T.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Lisenfeld, U.] Univ Granada, Granada, Spain. [Peterson, B. W.] Univ Wisconsin Barron Cty, Rice Lake, WI 54868 USA. [Struck, C.] Iowa State Univ, Ames, IA 50011 USA. [Sturm, E.] Max Planck Inst Extraterr Phys, Munich, Germany. [Tuffs, R.] MPI Kernphys, Heidelberg, Germany. [Valchanov, I.] ESAC, Herschel Sci Ctr, Madrid, Spain. [van der Werf, P.] Leiden Univ, Leiden Observ, Leiden, Netherlands. RP Appleton, PN (reprint author), CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. EM apple@ipac.caltech.edu RI Lisenfeld, Ute/A-1637-2015; OI Lisenfeld, Ute/0000-0002-9471-5423; Konstantopoulos, Iraklis/0000-0003-2177-0146; Struck, Curtis/0000-0002-6490-2156; Appleton, Philip/0000-0002-7607-8766; Cluver, Michelle/0000-0002-9871-6490 FU NASA through JPL/Caltech FX P.N.A. acknowledges interesting discussions with P. Goldsmith and W. Langer (JPL) regarding [C II] emission in the Galaxy. This work is based on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The authors thanks an anonymous referee for thoughtful comments on a previous version of the text. NR 79 TC 28 Z9 28 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2013 VL 777 IS 1 AR 66 DI 10.1088/0004-637X/777/1/66 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300066 ER PT J AU Baubock, M Berti, E Psaltis, D Ozel, F AF Bauboeck, Michi Berti, Emanuele Psaltis, Dimitrios Oezel, Feryal TI RELATIONS BETWEEN NEUTRON-STAR PARAMETERS IN THE HARTLE-THORNE APPROXIMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitation; relativistic processes; stars: neutron ID ROTATING RELATIVISTIC STARS; QUADRUPOLE-MOMENTS; MASS; EQUATIONS; MODELS; RADIUS AB Using stellar structure calculations in the Hartle-Thorne approximation, we derive analytic expressions connecting the ellipticity of the stellar surface to the compactness, the spin angular momentum, and the quadrupole moment of the spacetime. We also obtain empirical relations between the compactness, the spin angular momentum, and the spacetime quadrupole. Our formulae reproduce the results of numerical calculations to within a few percent and help reduce the number of parameters necessary to model the observational appearance of moderately spinning neutron stars. This is sufficient for comparing theoretical spectroscopic and timing models to observations that aim to measure the masses and radii of neutron stars and to determine the equation of state prevailing in their interiors. C1 [Bauboeck, Michi; Psaltis, Dimitrios; Oezel, Feryal] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Berti, Emanuele] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA. [Berti, Emanuele] CALTECH, Pasadena, CA 91125 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. RP Baubock, M (reprint author), Univ Arizona, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA. EM mbaubock@email.arizona.edu; berti@phy.olemiss.edu; dpsaltis@email.arizona.edu; fozel@email.arizona.edu RI Berti, Emanuele/C-9331-2016 OI Berti, Emanuele/0000-0003-0751-5130 FU NSF [AST-1108753]; NSF CAREER award [AST-0746549]; Chandra Theory grant [TM2-13002X]; NSF CAREER grant [PHY-1055103]; Radcliffe Institute for Advanced Study at Harvard University FX The work at the University of Arizona was supported in part by NSF grant AST-1108753, NSF CAREER award AST-0746549, and Chandra Theory grant TM2-13002X. E.B.'s research is supported by NSF CAREER grant No. PHY-1055103. F.O. gratefully acknowledges support from the Radcliffe Institute for Advanced Study at Harvard University. NR 36 TC 34 Z9 34 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 NOV 1 PY 2013 VL 777 IS 1 AR 68 DI 10.1088/0004-637X/777/1/68 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300068 ER PT J AU Boogert, ACA Chiar, JE Knez, C Oberg, KI Mundy, LG Pendleton, YJ Tielens, AGGM van Dishoeck, EF AF Boogert, A. C. A. Chiar, J. E. Knez, C. Oeberg, K. I. Mundy, L. G. Pendleton, Y. J. Tielens, A. G. G. M. van Dishoeck, E. F. TI INFRARED SPECTROSCOPIC SURVEY OF THE QUIESCENT MEDIUM OF NEARBY CLOUDS. I. ICE FORMATION AND GRAIN GROWTH IN LUPUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; infrared: stars; ISM: abundances; ISM: molecules; stars: formation ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; LOW-MASS PROTOSTARS; MOLECULAR CLOUDS; DARK CLOUD; INTERSTELLAR EXTINCTION; SOLID CO; H-I; EVOLUTION; WATER AB Infrared photometry and spectroscopy (1-25 mu m) of background stars reddened by the Lupus molecular cloud complex are used to determine the properties of grains and the composition of ices before they are incorporated into circumstellar envelopes and disks. H2O ices form at extinctions of A(K) = 0.25 +/- 0.07 mag (A(V) = 2.1 +/- 0.6). Such a low ice formation threshold is consistent with the absence of nearby hot stars. Overall, the Lupus clouds are in an early chemical phase. The abundance of H2O ice (2.3 +/- 0.1 x 10(-5) relative to NH) is typical for quiescent regions, but lower by a factor of three to four compared to dense envelopes of young stellar objects. The low solid CH3OH abundance (<3%-8% relative to H2O) indicates a low gas phase H/CO ratio, which is consistent with the observed incomplete CO freeze out. Furthermore it is found that the grains in Lupus experienced growth by coagulation. The mid-infrared (>5 mu m) continuum extinction relative to A(K) increases as a function of A(K). Most Lupus lines of sight are well fitted with empirically derived extinction curves corresponding to R-V similar to 3.5 (A(K) = 0.71) and R-V similar to 5.0 (A(K) = 1.47). For lines of sight with A(K) > 1.0 mag, the tau(9.7)/A(K) ratio is a factor of two lower compared to the diffuse medium. Below 1.0 mag, values scatter between the dense and diffuse medium ratios. The absence of a gradual transition between diffuse and dense medium-type dust indicates that local conditions matter in the process that sets the tau(9.7)/A(K) ratio. This process is likely related to grain growth by coagulation, as traced by the A(7.4)/A(K) continuum extinction ratio, but not to ice mantle formation. Conversely, grains acquire ice mantles before the process of coagulation starts. C1 [Boogert, A. C. A.] CALTECH, NASA, Herschel Sci Ctr, IPAC, Pasadena, CA 91125 USA. [Chiar, J. E.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. [Knez, C.; Mundy, L. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Knez, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Oeberg, K. I.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Oeberg, K. I.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Oeberg, K. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pendleton, Y. J.] NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA. [Tielens, A. G. G. M.; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. RP Boogert, ACA (reprint author), CALTECH, NASA, Herschel Sci Ctr, IPAC, Mail Code 100-22, Pasadena, CA 91125 USA. EM aboogert@ipac.caltech.edu FU National Aeronautics and Space Administration (NASA); NASA through JPL/Caltech; National Science Foundation FX We thank the anonymous referee for detailed comments that improved the presentation of the results. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech) under a contract with the National Aeronautics and Space Administration (NASA). Support for this work was provided by NASA through awards issued by JPL/Caltech to J.E.C. and C. K. 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 JPL/Caltech, funded by NASA. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/Caltech, funded by NASA and the National Science Foundation. NR 55 TC 12 Z9 12 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 NOV 1 PY 2013 VL 777 IS 1 AR 73 DI 10.1088/0004-637X/777/1/73 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300073 ER PT J AU Chan, CK Psaltis, D Ozel, F AF Chan, Chi-Kwan Psaltis, Dimitrios Oezel, Feryal TI GRay: A MASSIVELY PARALLEL GPU-BASED CODE FOR RAY TRACING IN RELATIVISTIC SPACETIMES SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitation; methods: numerical; radiative transfer ID SAGITTARIUS A-ASTERISK; BLACK-HOLE; NEUTRON-STARS; ACCRETION DISKS; HOT-SPOTS; MAGNETOHYDRODYNAMICS; OSCILLATIONS; SIMULATIONS; BURSTS; MODELS AB We introduce GRay, a massively parallel integrator designed to trace the trajectories of billions of photons in a curved spacetime. This graphics-processing-unit (GPU)-based integrator employs the stream processing paradigm, is implemented in CUDA C/C++, and runs on nVidia graphics cards. The peak performance of GRay using single-precision floating-point arithmetic on a single GPU exceeds 300 GFLOP (or 1 ns per photon per time step). For a realistic problem, where the peak performance cannot be reached, GRay is two orders of magnitude faster than existing central-processing-unit-based ray-tracing codes. This performance enhancement allows more effective searches of large parameter spaces when comparing theoretical predictions of images, spectra, and light curves from the vicinities of compact objects to observations. GRay can also perform on-the-fly ray tracing within general relativistic magnetohydrodynamic algorithms that simulate accretion flows around compact objects. Making use of this algorithm, we calculate the properties of the shadows of Kerr black holes and the photon rings that surround them. We also provide accurate fitting formulae of their dependencies on black hole spin and observer inclination, which can be used to interpret upcoming observations of the black holes at the center of the Milky Way, as well as M87, with the Event Horizon Telescope. C1 [Chan, Chi-Kwan; Psaltis, Dimitrios; Oezel, Feryal] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Chan, Chi-Kwan] NORDITA, KTH Royal Inst Technol, SE-10691 Stockholm, Sweden. [Chan, Chi-Kwan] Stockholm Univ, SE-10691 Stockholm, Sweden. [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. RP Chan, CK (reprint author), Univ Arizona, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA. FU NSF [AST-1108753]; NSF CAREER award [AST-0746549]; Chandra Theory grant [TM2-13002X]; Radcliffe Institute for Advanced Study at Harvard University FX This work was supported in part by the 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. NR 45 TC 16 Z9 16 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 NOV 1 PY 2013 VL 777 IS 1 AR 13 DI 10.1088/0004-637X/777/1/13 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300013 ER PT J AU Elshamouty, KG Heinke, CO Sivakoff, GR Ho, WCG Shternin, PS Yakovlev, DG Patnaude, DJ David, L AF Elshamouty, K. G. Heinke, C. O. Sivakoff, G. R. Ho, W. C. G. Shternin, P. S. Yakovlev, D. G. Patnaude, D. J. David, L. TI MEASURING THE COOLING OF THE NEUTRON STAR IN CASSIOPEIA A WITH ALL CHANDRA X-RAY OBSERVATORY DETECTORS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dense matter; neutrinos; pulsars: general; stars: neutron; supernovae: individual (Cassiopeia A); X-rays: stars ID A SUPERNOVA REMNANT; CENTRAL COMPACT OBJECTS; ANTI-MAGNETARS; SPIN-DOWN; EMISSION; ABSORPTION AB The thermal evolution of young neutron stars (NSs) reflects the neutrino emission properties of their cores. Heinke & Ho measured a 3.6% +/- 0.6% decay in the surface temperature of the Cassiopeia A (Cas A) NS between 2000 and 2009, using archival data from the Chandra X-ray Observatory ACIS-S detector in Graded mode. Page et al. and Shternin et al. attributed this decay to enhanced neutrino emission from a superfluid neutron transition in the core. Here we test this decline, combining analysis of the Cas A NS using all Chandra X-ray detectors and modes (HRC-S, HRC-I, ACIS-I, ACIS-S in Faint mode, and ACIS-S in Graded mode) and adding a 2012 May ACIS-S Graded mode observation, using the most current calibrations (CALDB 4.5.5.1). We measure the temperature changes from each detector separately and test for systematic effects due to the nearby filaments of the supernova remnant. We find a 0.92%-2.0% decay over 10 yr in the effective temperature, inferred from HRC-S data, depending on the choice of source and background extraction regions, with a best-fit decay of 1.0% +/- 0.7%. In comparison, the ACIS-S Graded data indicate a temperature decay of 3.1%-5.0% over 10 yr, with a best-fit decay of 3.5% +/- 0.4%. Shallower observations using the other detectors yield temperature decays of 2.6% +/- 1.9% (ACIS-I), 2.1% +/- 1.0% (HRC-I), and 2.1% +/- 1.9% (ACIS-S Faint mode) over 10 yr. Our best estimate indicates a decline of 2.9% +/- 0.5%(stat) +/- 1.0(sys)% over 10 yr. The complexity of the bright and varying supernova remnant background makes a definitive interpretation of archival Cas A Chandra observations difficult. A temperature decline of 1%-3.5% over 10 yr would indicate extraordinarily fast cooling of the NS that can be regulated by superfluidity of nucleons in the stellar core. C1 [Elshamouty, K. G.; Heinke, C. O.; Sivakoff, G. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Ho, W. C. G.] Univ Southampton, Sch Math, Southampton SO17 1BJ, Hants, England. [Shternin, P. S.; Yakovlev, D. G.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Patnaude, D. J.; David, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elshamouty, KG (reprint author), Univ Alberta, Dept Phys, CCIS 4-181, Edmonton, AB T6G 2E1, Canada. EM alshamou@ualberta.ca RI Sivakoff, Gregory/G-9602-2011; Shternin, Peter/A-7352-2014; OI Sivakoff, Gregory/0000-0001-6682-916X; Heinke, Craig/0000-0003-3944-6109 FU NSERC; Alberta Ingenuity New Faculty Award; STFC in the UK; RFBR [11-02-00253-a]; RF Presidential Programm NSh [4035.2012.2]; Ministry of Education and Science of Russian Federation [8409] FX We thank Harvey Tananbaum, Vinay Kashyap, Arturo Sanchez-Azofeifa, Una Hwang, Jeremy Drake, and Robert Rutledge for discussions. K. G. E. and C.O.H. are supported by an NSERC Discovery Grant and an Alberta Ingenuity New Faculty Award. W. C. G. H. acknowledges support from STFC in the UK. P. S. S. and D.G.Y. acknowledge support from RFBR (grant 11-02-00253-a), RF Presidential Programm NSh 4035.2012.2, and Ministry of Education and Science of Russian Federation (agreement No. 8409, 2012). G. R. S. is also supported by an NSERC Discovery Grant. NR 37 TC 40 Z9 40 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 NOV 1 PY 2013 VL 777 IS 1 AR 22 DI 10.1088/0004-637X/777/1/22 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300022 ER PT J AU Forbrich, J Berger, E Reid, MJ AF Forbrich, Jan Berger, Edo Reid, Mark J. TI AN ASTROMETRIC SEARCH FOR A SUB-STELLAR COMPANION OF THE M8.5 DWARF TVLM 513-46546 USING VERY LONG BASELINE INTERFEROMETRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; planetary systems; radio continuum: stars; stars: low-mass ID LOW-MASS STAR; RADIO-EMISSION; ULTRACOOL DWARF; BROWN DWARF; PROPER MOTION; MAIN-SEQUENCE; TVLM-513-46546; EARTH; CONSTRAINTS; PHOTOMETRY AB We conducted multi-epoch very long baseline interferometry observations to search for astrometric reflex motion that would be caused by a sub-stellar companion of the M8.5 dwarf TVLM 513-46546. The observations yield an absolute parallax corresponding to a distance of 10.762+/-0.027 pc and a proper motion of 78.09+/-0.17 mas yr(-1). The averaged flux density per epoch varies by a factor of at least three. From the absence of significant residual motion, we place an upper limit on any reflex motion caused by a companion, extending the parameter space covered by previous near-infrared direct-imaging searches. The data exclude a phase space of companion masses and orbital periods ranging from 3.8 M-Jup with an orbital radius of similar to 0.05 AU (and an orbital period of 16 days) to 0.3 M-Jup with an orbital radius of similar to 0.7 AU (and an orbital period of 710 days). C1 [Forbrich, Jan; Berger, Edo; Reid, Mark J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Forbrich, Jan] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. RP Forbrich, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Science Foundation [AST-1008361] FX The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. E.B. acknowledges support for this work from the National Science Foundation through Grant AST-1008361. NR 27 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2013 VL 777 IS 1 AR 70 DI 10.1088/0004-637X/777/1/70 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300070 ER PT J AU Hwang, HS Andrews, SM Geller, MJ AF Hwang, Ho Seong Andrews, Sean M. Geller, Margaret J. TI DUST PROPERTIES OF LOCAL DUST-OBSCURED GALAXIES WITH THE SUBMILLIMETER ARRAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: formation; galaxies: starburst; infrared: galaxies; submillimeter: galaxies ID SPECTRAL ENERGY-DISTRIBUTIONS; SIMILAR-TO 2; ULTRALUMINOUS INFRARED GALAXIES; DIGITAL SKY SURVEY; ULTRAVIOLET-SELECTED GALAXIES; STAR-FORMATION HISTORIES; GOODS-HERSCHEL; LUMINOSITY FUNCTIONS; INTERSTELLAR DUST; FORMING GALAXIES AB We report Submillimeter Array observations of the 880 mu m dust continuum emission for four dust-obscured galaxies (DOGs) in the local universe. Two DOGs are clearly detected with S-nu (880 mu m) = 10-13 mJy and S/N > 5, but the other two are not detected with 3 sigma upper limits of S-nu (880 mu m) = 5-9 mJy. Including an additional two local DOGs with submillimeter data from the literature, we determine the dust masses and temperatures for six local DOGs. The infrared luminosities and dust masses for these DOGs are in the ranges of 1.2-4.9 x 10(11)(L-circle dot) and 4-14 x 10(7)(M-circle dot), respectively. The dust temperatures derived from a two-component modified blackbody function are 23-26 K and 60-124 K for the cold and warm dust components, respectively. Comparison of local DOGs with other infrared luminous galaxies with submillimeter detections shows that the dust temperatures and masses do not differ significantly among these objects. Thus, as argued previously, local DOGs are not a distinctive population among dusty galaxies, but simply represent the high-end tail of the dust obscuration distribution. C1 [Hwang, Ho Seong; Andrews, Sean M.; Geller, Margaret J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Hwang, HS (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM hhwang@cfa.harvard.edu; sandrews@cfa.harvard.edu; mgeller@cfa.harvard.edu FU Smithsonian Institution; Academia Sinica FX We thank Jong Chul Lee, Gwang-Ho Lee, and Jubee Sohn for useful discussions. H. S. H. acknowledges the Smithsonian Institution for the support of his post-doctoral fellowship. The Smithsonian Institution also supports the research of M.J.G. 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. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. NR 68 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2013 VL 777 IS 1 AR 38 DI 10.1088/0004-637X/777/1/38 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300038 ER PT J AU Ito, H Nagataki, S Ono, M Lee, SH Mao, JR Yamada, S Pe'er, A Mizuta, A Harikae, S AF Ito, Hirotaka Nagataki, Shigehiro Ono, Masaomi Lee, Shiu-Hang Mao, Jirong Yamada, Shoichi Pe'er, Asaf Mizuta, Akira Harikae, Seiji TI PHOTOSPHERIC EMISSION FROM STRATIFIED JETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; radiation mechanisms: thermal; radiative transfer; scattering ID GAMMA-RAY-BURSTS; RADIATION-MEDIATED SHOCKS; RELATIVISTIC JETS; PROMPT EMISSION; PEAK ENERGY; MAGNETOHYDRODYNAMIC SIMULATIONS; NONTHERMAL EMISSION; SPECTRAL PROPERTIES; FERMI OBSERVATIONS; THERMAL EMISSION AB We explore photospheric emissions from stratified two-component jets, wherein a highly relativistic spine outflow is surrounded by a wider and less relativistic sheath outflow. Thermal photons are injected in regions of high optical depth and propagated until the photons escape at the photosphere. Because of the presence of shear in velocity (Lorentz factor) at the boundary of the spine and sheath region, a fraction of the injected photons are accelerated using a Fermi-like acceleration mechanism such that a high-energy power-law tail is formed in the resultant spectrum. We show, in particular, that if a velocity shear with a considerable variance in the bulk Lorentz factor is present, the high-energy part of observed gamma-ray bursts (GRBs) photon spectrum can be explained by this photon acceleration mechanism. We also show that the accelerated photons might also account for the origin of the extra-hard power-law component above the bump of the thermal-like peak seen in some peculiar bursts (e.g., GRB 090510, 090902B, 090926A). We demonstrate that time-integrated spectra can also reproduce the low-energy spectrum of GRBs consistently using a multi-temperature effect when time evolution of the outflow is considered. Last, we show that the empirical E-p-L-p relation can be explained by differences in the outflow properties of individual sources. C1 [Ito, Hirotaka; Nagataki, Shigehiro; Ono, Masaomi; Lee, Shiu-Hang; Mao, Jirong] RIKEN, Astrophys Big Bang Lab, Saitama 3510198, Japan. [Yamada, Shoichi] Waseda Univ, Dept Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Yamada, Shoichi] Waseda Univ, Adv Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Pe'er, Asaf] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Pe'er, Asaf] Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland. [Mizuta, Akira] KEK, Ctr Theory, Tsukuba, Ibaraki 3050801, Japan. [Mizuta, Akira] RIKEN, Computat Astrophys Lab, Saitama 3510198, Japan. [Harikae, Seiji] Mitsubishi UFJ Morgan Stanley Secur Co Ltd, Quants Res Dept, Financial Engn Div, Bunkyo Ku, Tokyo 1128688, Japan. RP Ito, H (reprint author), RIKEN, Astrophys Big Bang Lab, Saitama 3510198, Japan. EM hito@yukawa.kyoto-u.ac.jp OI Harikae, Seiji/0000-0002-6620-5899 FU Ministry of Education, Culture, Sports, Science and Technology [20105005, 23105709, 24244036]; Japan Society for the Promotion of Science [19104006, 23340069]; Global COE Program, "The Next Generation of Physics, Spun from University and Emergence from MEXT of Japan"; RIKEN; [2503018]; [24.02022] FX We thank Don Warren for comments and assistance that improved the clarity of the paper. We also thank Alexey Tolstov, Yudai Suwa and Yuichiro Sekiguchi for fruitful discussions. We are grateful to the anonymous referee for constructive comments. This work is supported by the support from the Ministry of Education, Culture, Sports, Science and Technology (Nos. 20105005, 23105709, and 24244036), the Japan Society for the Promotion of Science (Nos. 19104006 and 23340069), and the Global COE Program, "The Next Generation of Physics, Spun from University and Emergence from MEXT of Japan." S.-H. L. and J.M. acknowledge support from Grants-in-Aid for Foreign JSPS Fellow (Nos. 2503018 and 24.02022). We thank RIKEN for providing the facilities and financial support. NR 87 TC 13 Z9 13 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2013 VL 777 IS 1 AR 62 DI 10.1088/0004-637X/777/1/62 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300062 ER PT J AU Kannappan, SJ Stark, DV Eckert, KD Moffett, AJ Wei, LH Pisano, DJ Baker, AJ Vogel, SN Fabricant, DG Laine, S Norris, MA Jogee, S Lepore, N Hough, LE Weinberg-Wolf, J AF Kannappan, Sheila J. Stark, David V. Eckert, Kathleen D. Moffett, Amanda J. Wei, Lisa H. Pisano, D. J. Baker, Andrew J. Vogel, Stuart N. Fabricant, Daniel G. Laine, Seppo Norris, Mark A. Jogee, Shardha Lepore, Natasha Hough, Loren E. Weinberg-Wolf, Jennifer TI CONNECTING TRANSITIONS IN GALAXY PROPERTIES TO REFUELING SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution ID TULLY-FISHER RELATION; DIGITAL SKY SURVEY; STAR-FORMATION RATES; COLD DARK-MATTER; FAST ALPHA SURVEY; 40-PERCENT ALFALFA SURVEY; SUPERMASSIVE BLACK-HOLES; STELLAR MASS FUNCTIONS; NEARBY FIELD GALAXIES; BLUE COMPACT GALAXIES AB We relate transitions in galaxy structure and gas content to refueling, here defined to include both the external gas accretion and the internal gas processing needed to renew reservoirs for star formation. We analyze two z = 0 data sets: a high-quality similar to 200 galaxy sample (the Nearby Field Galaxy Survey, data release herein) and a volume-limited similar to 3000 galaxy sample with reprocessed archival data. Both reach down to baryonic masses similar to 10(9) M and span void-to-cluster environments. Two mass-dependent transitions are evident: (1) below the "gas-richness threshold" scale (V similar to 125 km s(-1)), gas-dominated quasi-bulgeless Sd-Im galaxies become numerically dominant; while (2) above the "bimodality" scale (V similar to 200 km s(-1)), gas-starved E/S0s become the norm. Notwithstanding these transitions, galaxy mass (or V as its proxy) is a poor predictor of gas-to-stellar mass ratio M-gas/M-*. Instead, M-gas/M-* correlates well with the ratio of a galaxy's stellar mass formed in the last Gyr to its preexisting stellar mass, such that the two ratios have numerically similar values. This striking correspondence between past-averaged star formation and current gas richness implies routine refueling of star-forming galaxies on Gyr timescales. We argue that this refueling underlies the tight M-gas/M-* versus color correlations often used to measure "photometric gas fractions." Furthermore, the threshold and bimodality scale transitions reflect mass-dependent demographic shifts between three refueling regimes-accretion-dominated, processing-dominated, and quenched. In this picture, gas-dominated dwarfs are explained not by inefficient star formation but by overwhelming gas accretion, which fuels stellar mass doubling in less than or similar to 1 Gyr. Moreover, moderately gas-rich bulged disks such as the Milky Way are transitional, becoming abundant only in the narrow range between the threshold and bimodality scales. C1 [Kannappan, Sheila J.; Stark, David V.; Eckert, Kathleen D.; Moffett, Amanda J.; Norris, Mark A.; Weinberg-Wolf, Jennifer] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Wei, Lisa H.; Fabricant, Daniel G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wei, Lisa H.] Atmospher & Environm Res, Lexington, MA 02421 USA. [Pisano, D. J.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Baker, Andrew J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Vogel, Stuart N.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Laine, Seppo] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Norris, Mark A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Jogee, Shardha] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Lepore, Natasha] Univ So Calif, Dept Radiol, Los Angeles, CA 90027 USA. [Lepore, Natasha] Childrens Hosp Los Angeles, Los Angeles, CA 90027 USA. [Hough, Loren E.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. RP Kannappan, SJ (reprint author), Univ N Carolina, Dept Phys & Astron, 290 Phillips Hall CB 3255, Chapel Hill, NC 27599 USA. EM sheila@physics.unc.edu OI Norris, Mark/0000-0002-7001-805X FU NSF CAREER grant [AST-0955368]; GAANN Fellowships; North Carolina Space Grant Fellowships; NRAO Charlottesville visitor program; NASA Harriet Jenkins Fellowship; University of North Carolina Royster Society of Fellows; North Carolina Space Grant Program; NSF under the CARMA cooperative agreement; SMA Postdoctoral Fellowship; Norman Hackerman Advanced Research Program (NHARP) [ARP-03658-0234-2009]; NSF [AST-0607748]; Hubble Space Telescope grant from STScI [GO-11082]; NASA [NAS5-26555]; National Aeronautics and Space Administration; National Science Foundation; NASA; JPL/Caltech; Alfred P. Sloan Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brookhaven National Laboratory, University of Cambridge; Carnegie Mellon University; University of Florida; Harvard University; Instituto de Astrofisica de Canarias; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University; [10A-070] FX We are grateful to Douglas Mar, Jacqueline van Gorkom, John Hibbard, Adam Leroy, Ari Maller, Martha Haynes, Sadegh Khochfar, and Eric Gawiser for illuminating conversations. The anonymous referee provided helpful feedback that improved this manuscript. We thank Perry Berlind, Barbara Carter, Marijn Franx, and the Mount Hopkins observatory staff for their help with the NFGS kinematics observing program. We thank the GBT operators and Green Bank staff for their support of program 10A-070. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. S.J.K., D. V. S., K. D. E., and M.A.N. were supported in this research by NSF CAREER grant AST-0955368. D. V. S. and K. D. E. also acknowledge support from GAANN Fellowships and North Carolina Space Grant Fellowships. S.J.K. acknowledges the hospitality and financial assistance of the NRAO Charlottesville visitor program during spring 2010. A.J.M. acknowledges support from a NASA Harriet Jenkins Fellowship, the University of North Carolina Royster Society of Fellows, and the North Carolina Space Grant Program. LHW was supported in part by the NSF under the CARMA cooperative agreement and in part by an SMA Postdoctoral Fellowship. S.J. acknowledges support from the Norman Hackerman Advanced Research Program (NHARP) ARP-03658-0234-2009, NSF grant AST-0607748, and Hubble Space Telescope grant GO-11082 from STScI, which is operated by AURA, Inc., for NASA, under NAS5-26555. This research has made use of the HyperLEDA database (http://leda.univ-lyon1.fr). This work has used the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work has made use of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This work is based in part on observations and on archival data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by an award issued by JPL/Caltech and by NASA. We acknowledge use of the Sloan Digital Sky Survey (SDSS). Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, 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 168 TC 18 Z9 18 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2013 VL 777 IS 1 AR 42 DI 10.1088/0004-637X/777/1/42 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300042 ER PT J AU Laha, S Dewangan, GC Chakravorty, S Kembhavi, AK AF Laha, Sibasish Dewangan, Gulab C. Chakravorty, Susmita Kembhavi, Ajit K. TI THE EFFECT OF UV/SOFT X-RAY EXCESS EMISSION ON THE WARM ABSORBER PROPERTIES OF ACTIVE GALACTIC NUCLEI-A CASE STUDY OF IRAS 13349+2438 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: Seyfert; quasars: absorption lines; X-rays: individual (IRAS 13349+2438) ID SEYFERT 1 GALAXIES; XMM-NEWTON RGS; IONIZED ABSORBER; NGC 4051; ABSORPTION LINES; PHOTOIONIZED GAS; CHANDRA-LETGS; ENVIRONMENT; SPECTRUM; IRAS-13349+2438 AB The ultraviolet (UV) to X-ray continuum of active galactic nuclei (AGNs) is important for maintaining the ionization and thermal balance of the warm absorbers (WAs). However, the spectra in the sensitive energy range similar to 13.6-300 eV are unobservable due to Galactic extinction. Moreover, many AGNs show soft X-ray excess emission of varying strength in the 0.1-2 keV band, whose origin is still highly debated. This soft excess connects to the UV bump in the unobserved region of 13.6-300 eV. Here, we investigate the effect of the assumed physical model for the soft excess on the flux of the unobserved part of the spectrum and its effect on the WA properties. We perform a case study using XMM-Newton observations of the bright Seyfert 1 galaxy IRAS 13349+2438 with WA features. Two different physical models for the soft excess (blurred Compton reflection from an ionized disk and optically thick thermal Comptonization of the disk photons) predict different fluxes in the unobserved energy range. However, the current X-ray data quality does not allow us to distinguish between them using derived WA parameters. This, in turn, implies that it is difficult to determine the origin of the soft excess emission using the WA features. C1 [Chakravorty, Susmita] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Chakravorty, Susmita] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM laha@iucaa.ernet.in; gulabd@iucaa.ernet.in FU ESA Member States; NASA; CSIR; Government of India; National Aeronautics and Space Administration FX This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. S. L. is grateful to CSIR and the Government of India for supporting this work. The authors are grateful to the anonymous referee for helpful comments and suggestions. NR 56 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 NOV 1 PY 2013 VL 777 IS 1 AR 2 DI 10.1088/0004-637X/777/1/2 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300002 ER PT J AU Lee, CW Kim, MR Kim, G Saito, M Myers, PC Kurono, Y AF Lee, Chang Won Kim, Mi-Ryang Kim, Gwanjeong Saito, Masao Myers, Philip C. Kurono, Yasutaka TI EARLY STAR-FORMING PROCESSES IN DENSE MOLECULAR CLOUD L328; IDENTIFICATION OF L328-IRS AS A PROTO-BROWN DWARF SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; ISM: individual objects (L328, L328-IRS); stars: formation; stars: low-mass ID SPITZER C2D SURVEY; LOW-LUMINOSITY OBJECT; PLANETARY-MASS OBJECTS; INFALL MOTIONS; STELLAR CLUSTERS; PRESTELLAR CORES; CS 2-1; DISCOVERY; OUTFLOW; TAURUS AB This paper presents the results of millimeter to sub-millimeter observations of CO, HCN, N2H+, and HCO+ lines in the dense molecular cloud L328, which harbors L328-IRS, a Very Low Luminosity Object (VeLLO). Our analysis of the line width finds that (CO)-C-13 and N2H+ lines are broadened right over the smallest sub-core S2 where L328-IRS is located, while they are significantly narrower in other regions of L328. Thus, L328-IRS has a direct association with the sub-core. CO observations show a bipolar outflow from this VeLLO with an extent of similar to 0.08 pc. The outflow momentum flux and efficiency are much less than those of low-mass protostars. The most likely mass accretion rate (similar to 3.6 x 10(-7) M-circle dot yr(-1)) inferred from the analysis of the CO outflow is an order of magnitude smaller than the canonical value for a protostar. If the main accretion lasts during the typical Class 0 period of a protostar, L328-IRS will accrete the mass of a brown dwarf, but not that of a star. Given that its envelope mass is small (similar to 0.09 M-circle dot) and 100% star formation rate is unlikely, we suggest that L328-IRS is likely a proto-brown dwarf. Inward motions are found in global scale in the L328 cloud and its sub-cores with a typical infall speed found in starless cores. L328 is found to be fairly well isolated from other nearby clouds and seems to be forming three sub-cores simultaneously through a gravitational fragmentation process. Altogether, these all leave L328-IRS as the best example supporting the idea that a brown dwarf forms like a normal star. C1 [Lee, Chang Won; Kim, Mi-Ryang; Kim, Gwanjeong] Korea Astron & Space Sci Inst, Taejon, South Korea. [Kim, Mi-Ryang] Chungbuk Natl Univ, Cheongju Chungbuk 361763, South Korea. [Kim, Gwanjeong] Univ Sci & Technol, Taejon 305333, South Korea. [Saito, Masao; Kurono, Yasutaka] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Myers, Philip C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lee, CW (reprint author), Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Taejon, South Korea. EM cwl@kasi.re.kr FU Basic Science Research Program through the National Research Foundation of Korea (NRF); Ministry of Education, Science and Technology [2010-0011605]; global research collaboration of Korea Research Council of Fundamental Science & Technology (KRCF) FX We thank an anonymous referee for a thorough reading of our manuscript and giving us very useful comments with which our paper was very much improved. This research was supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science and Technology (2010-0011605) and also by the global research collaboration of Korea Research Council of Fundamental Science & Technology (KRCF). NR 65 TC 14 Z9 14 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2013 VL 777 IS 1 AR 50 DI 10.1088/0004-637X/777/1/50 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300050 ER PT J AU Marion, GH Vinko, J Wheeler, JC Foley, RJ Hsiao, EY Brown, PJ Challis, P Filippenko, AV Garnavich, P Kirshner, RP Landsman, WB Parrent, JT Pritchard, TA Roming, PWA Silverman, JM Wang, XF AF Marion, G. H. Vinko, Jozsef Wheeler, J. Craig Foley, Ryan J. Hsiao, Eric Y. Brown, Peter J. Challis, Peter Filippenko, Alexei V. Garnavich, Peter Kirshner, Robert P. Landsman, Wayne B. Parrent, Jerod T. Pritchard, Tyler A. Roming, Peter W. A. Silverman, Jeffrey M. Wang, Xiaofeng TI HIGH-VELOCITY LINE FORMING REGIONS IN THE TYPE Ia SUPERNOVA 2009ig SO ASTROPHYSICAL JOURNAL LA English DT Article DE line: formation; line: identification; supernovae: general; supernovae: individual (SN 2009ig) ID HOBBY-EBERLY TELESCOPE; IMPROVED DISTANCES; SN 2001EL; SPECTRA; FEATURES; SPECTROSCOPY; EJECTA; RESOLUTION; SPECTROPOLARIMETRY; SPECTROGRAPH AB We report measurements and analysis of high-velocity (HVF) (>20,000 km s(-1)) and photospheric absorption features in a series of spectra of the Type Ia supernova (SN) 2009ig obtained between -14 days and +13 days with respect to the time of maximum B-band luminosity (B-max). We identify lines of Si II, Si III, S II, Ca II, and Fe II that produce both HVF and photospheric-velocity (PVF) absorption features. SN 2009ig is unusual for the large number of lines with detectable HVF in the spectra, but the light-curve parameters correspond to a slightly overluminous but unexceptional SN Ia (M-B = -19.46 mag and Delta m(15)(B) = 0.90 mag). Similarly, the Si II lambda 6355 velocity at the time of B-max is greater than "normal" for an SN Ia, but it is not extreme (upsilon(Si) = 13,400 km s(-1)). The -14 days and -13 days spectra clearly resolve HVF from Si II lambda 6355 as separate absorptions from a detached line forming region. At these very early phases, detached HVF are prevalent in all lines. From -12 days to -6 days, HVF and PVF are detected simultaneously, and the two line forming regions maintain a constant separation of about 8000 km s(-1). After -6 days all absorption features are PVF. The observations of SN 2009ig provide a complete picture of the transition from HVF to PVF. Most SNe Ia show evidence for HVF from multiple lines in spectra obtained before -10 days, and we compare the spectra of SN 2009ig to observations of other SNe. We show that each of the unusual line profiles for Si II lambda 6355 found in early-time spectra of SNe Ia correlate to a specific phase in a common development sequence from HVF to PVF. C1 [Marion, G. H.; Foley, Ryan J.; Challis, Peter; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marion, G. H.; Vinko, Jozsef; Wheeler, J. Craig; Silverman, Jeffrey M.] Univ Texas Austin, Austin, TX 78712 USA. [Vinko, Jozsef] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Hsiao, Eric Y.] Carnegie Observat, Campanas Observ, Colina El Pino, Casilla 601, Chile. [Brown, Peter J.; Wang, Xiaofeng] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA. [Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Garnavich, Peter] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Landsman, Wayne B.] NASA, Goddard Space Flight Ctr, Adnet Syst, Greenbelt, MD 20771 USA. [Parrent, Jerod T.] Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Parrent, Jerod T.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Pritchard, Tyler A.; Roming, Peter W. A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Roming, Peter W. A.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78228 USA. [Wang, Xiaofeng] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Wang, Xiaofeng] Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China. RP Marion, GH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gmarion@cfa.harvard.edu RI Wang, Xiaofeng/J-5390-2015 FU Hungarian OTKA Grants [K-76816, NN-107637]; NSF [AST-0707769, AST-1211196, AST-1008343, AST-1211916]; Texas Advanced Research Project [ARP-009]; Natural Science Foundation of China [NSFC 11178003, 11073013]; China-973 Program [2009CB824800]; TABASGO Foundation; Christopher R. Redlich Fund FX The authors wish to thank the Chairmen of the TACs from the University of Texas and Penn State University for providing Director's discretionary time for the HET/LRS observations. G. H. M. thanks Nick Suntzeff and Rob Robinson for insightful comments. G. H. M. also thanks Mark Phillips for providing perspective, as well as Michael Childress for helpful discussions and for sharing an advance copy of his paper on SN 2012fr. We thank Mark Sullivan, Isobel Hook, Peter Nugent, Andy Howell, and Bill Vacca for sharing their own data on line profiles in young SNe Ia. The authors make frequent use of David Bishop's excellent Web site listing recent supernovae and valuable references associated with them: http://www.rochesterastronomy.org/snimages/. J.V. is supported by Hungarian OTKA Grants K-76816 and NN-107637, NSF grant AST-0707769, and Texas Advanced Research Project ARP-009. The research of J.C.W. in supported in part by NSF grant AST-1109801. The CfA Supernova Program is supported by NSF grant AST-1211196 to the Harvard College Observatory. X. Wang is supported by the Natural Science Foundation of China (NSFC 11178003, 11073013), the China-973 Program 2009CB824800, and NSF grant AST-0708873 (through L. Wang). E.Y.H. is supported by NSF grant AST-1008343. A. V. F. is grateful for financial assistance from NSF grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. We greatly appreciate the valuable assistance provided by staff members at the observatories where SN 2009ig was observed. NR 57 TC 20 Z9 20 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2013 VL 777 IS 1 AR 40 DI 10.1088/0004-637X/777/1/40 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300040 ER PT J AU Nesvorny, D Kipping, D Terrell, D Hartman, J Bakos, GA Buchhave, LA AF Nesvorny, David Kipping, David Terrell, Dirk Hartman, Joel Bakos, Gaspar A. Buchhave, Lars A. TI KOI-142, THE KING OF TRANSIT VARIATIONS, IS A PAIR OF PLANETS NEAR THE 2:1 RESONANCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems ID TIMING VARIATIONS; MASS; CANDIDATES; SYSTEMS; EXOMOONS; HUNT AB The transit timing variations (TTVs) can be used as a diagnostic of gravitational interactions between planets in a multi-planet system. Many Kepler Objects of Interest (KOIs) exhibit significant TTVs, but KOI-142.01 stands out among them with an unrivaled similar or equal to 12 hr TTV amplitude. Here we report a thorough analysis of KOI-142.01's transits. We discover periodic transit duration variations (TDVs) of KOI-142.01 that are nearly in phase with the observed TTVs. We show that KOI-142.01's TTVs and TDVs uniquely detect a non-transiting companion with a mass similar or equal to 0.63 that of Jupiter (KOI-142c). KOI-142.01's mass inferred from the transit variations is consistent with the measured transit depth, suggesting a Neptune-class planet (KOI-142b). The orbital period ratio P-c/P-b = 2.03 indicates that the two planets are just wide of the 2: 1 resonance. The present dynamics of this system, characterized here in detail, can be used to test various formation theories that have been proposed to explain the near-resonant pairs of exoplanets. C1 [Nesvorny, David; Terrell, Dirk] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Kipping, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hartman, Joel; Bakos, Gaspar A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. RP Nesvorny, D (reprint author), SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. OI Buchhave, Lars A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166 FU NSF [AST-1008890, AST-1108686]; NASA Sagan fellowship; NASA [NNX09AB29G] FX We thank the Kepler Science Team, especially the DAWG, for making the data used here available. D.N. acknowledges support from NSF AST-1008890. D. M. K. is supported by the NASA Sagan fellowship. J.H. acknowledges support from NSF AST-1108686. G. B. acknowledges support from NASA grant NNX09AB29G. NR 38 TC 39 Z9 39 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 NOV 1 PY 2013 VL 777 IS 1 AR UNSP 3 DI 10.1088/0004-637X/777/1/3 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300003 ER PT J AU Somers, G Mathur, S Martini, P Watson, L Grier, CJ Ferrarese, L AF Somers, Garrett Mathur, Smita Martini, Paul Watson, Linda Grier, Catherine J. Ferrarese, Laura TI DISCOVERY OF A LARGE POPULATION OF ULTRALUMINOUS X-RAY SOURCES IN THE BULGELESS GALAXIES NGC 337 AND ESO 501-23 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: nuclei; X-rays: binaries; X-rays: galaxies ID SUPERMASSIVE BLACK-HOLES; NUCLEAR STAR CLUSTER; ACCRETION DISKS; NEARBY GALAXIES; HOST GALAXIES; DATA RELEASE; MASS; CHANDRA; COUNTERPART; EVOLUTION AB We have used Chandra observations of eight bulgeless disk galaxies to identify new ultraluminous X-ray source (ULX) candidates, study their high-mass X-ray binary (HMXB) population, and search for low-luminosity active galactic nuclei (AGNs). We report the discovery of 16 new ULX candidates in our sample of galaxies. Eight of these are found in the star forming galaxy NGC 337, none of which are expected to be background contaminants. The HMXB luminosity function of NGC 337 implies a star formation rate (SFR) of 6.8(-3.5)(+4.4) M-circle dot yr(-1), consistent at 1.5 sigma with a recent state of the art SFR determination. We also report the discovery of a bright ULX candidate (X-1) in ESO 501-23. X-1's spectrum is well fit by an absorbed power law with Gamma = 1.18(-0.11)(+0.19) and NH = 1.13(-1.13)(+7.07) x 10(20) cm(-2), implying a 0.3-8 keV flux of 1.08(-0.07)(+0.05) x 10(-12) erg s(-1) cm(-2). Its X-ray luminosity (LX) is poorly constrained due to uncertainties in the host galaxy's distance, but we argue that its spectrum implies L-X > 10(40) erg s(-1). An optical counterpart to this object may be present in an Hubble Space Telescope image. We also identify ULX candidates in IC 1291, PGC 3853, NGC 5964, and NGC 2805. We find no evidence of nuclear activity in the galaxies in our sample, placing a flux upper limit of 4 x 10(-15) erg s(-1) cm(-2) on putative AGN. Additionally, the Type II-P supernova SN 2011DQ in NGC 337, which exploded two months before our X-ray observation, is undetected. C1 [Somers, Garrett; Mathur, Smita; Martini, Paul; Grier, Catherine J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Mathur, Smita; Martini, Paul] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Watson, Linda] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ferrarese, Laura] Hertzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. RP Somers, G (reprint author), Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA. EM somers@astronomy.ohio-state.edu FU National Aeronautics and Space Administration through Chandra Award by the Chandra X-ray Observatory Center [GO1-12113X]; National Aeronautics Space Administration [NAS8-03060]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; University of Florida; French Participation Group; German Participation Group; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University; National Aeronautics and Space Administration FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO1-12113X 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. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, University of Florida, the French Participation Group, the German Participation Group, 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, 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 publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of the USNO Image and Catalogue Archive operated by the United States Naval Observatory, Flagstaff Station (http://www.nofs.navy.mil/data/fchpix/). G.S. thanks Dale Mudd for his helpful comments. NR 70 TC 2 Z9 2 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 NOV 1 PY 2013 VL 777 IS 1 AR 7 DI 10.1088/0004-637X/777/1/7 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241DT UT WOS:000326147300007 ER PT J AU Bourouaine, S Verscharen, D Chandran, BDG Maruca, BA Kasper, JC AF Bourouaine, Sofiane Verscharen, Daniel Chandran, Benjamin D. G. Maruca, Bennett A. Kasper, Justin C. TI LIMITS ON ALPHA PARTICLE TEMPERATURE ANISOTROPY AND DIFFERENTIAL FLOW FROM KINETIC INSTABILITIES: SOLAR WIND OBSERVATIONS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE instabilities; solar wind; turbulence; waves ID HYBRID SIMULATIONS; ION MEASUREMENTS; ALFVEN WAVES; PROTON; CYCLOTRON; ACCELERATION; COLLISIONS; TURBULENCE; RATIO; BEAM AB Previous studies have shown that the observed temperature anisotropies of protons and alpha particles in the solar wind are constrained by theoretical thresholds for pressure and anisotropy driven instabilities such as the Alfven/ion-cyclotron (A/IC) and fast-magnetosonic/whistler (FM/W) instabilities. In this Letter, we use a long period of in situ measurements provided by the Wind spacecraft's Faraday cups to investigate the combined constraint on the alpha proton differential flow velocity and the alpha particle temperature anisotropy due to A/IC and FM/W instabilities. We show that the majority of the data are constrained to lie within the region of parameter space in which A/IC and FM/W waves are either stable or have extremely low growth rates. In the minority of observed cases in which the growth rate of the A/IC (FM/W) instability is comparatively large, we find relatively higher values of T-perpendicular to alpha/T-perpendicular to p (T-parallel to a/T-parallel to p) when the alpha proton differential flow velocity is small, where T-perpendicular to alpha and T-perpendicular to p (T parallel to(alpha) and T parallel to(p)) are the perpendicular (parallel) temperatures of alpha particles and protons. We conjecture that this observed feature might arise from preferential alpha particle heating which can drive the alpha particles beyond the instability thresholds. C1 [Bourouaine, Sofiane; Verscharen, Daniel; Chandran, Benjamin D. G.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Maruca, Bennett A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Kasper, Justin C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bourouaine, S (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. EM s.bourouaine@unh.edu OI Verscharen, Daniel/0000-0002-0497-1096 FU NASA [NNX11AJ37G, NNS12AB27G] FX We thank Kris Klein for his helpful discussions. This work was supported in part by NASA grants NNX11AJ37G and NNS12AB27G. NR 44 TC 19 Z9 19 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 1 PY 2013 VL 777 IS 1 AR L3 DI 10.1088/2041-8205/777/1/L3 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241SH UT WOS:000326187400003 ER PT J AU Currie, T Cloutier, R Debes, JH Kenyon, SJ Kaisler, D AF Currie, Thayne Cloutier, Ryan Debes, John H. Kenyon, Scott J. Kaisler, Denise TI A DEEP KECK/NIRC2 SEARCH FOR THERMAL EMISSION FROM PLANETARY COMPANIONS ORBITING FOMALHAUT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: early-type; stars: individual (Fomalhaut) ID BETA-PICTORIS B; DEBRIS DISK; HR 8799; MU-M; GIANT PLANETS; SPACE-TELESCOPE; SOLAR-SYSTEM; DUST; STAR; MASS AB We present deep Keck/NIRC2 1.6 and 3.8 mu m imaging of Fomalhaut to constrain the near-infrared brightness of Fomalhaut b, recently confirmed as a likely planet, and search for additional planets at r(proj) = 15-150 AU. Using advanced/novel point spread function subtraction techniques, we identify seven candidate substellar companions Fomalhaut b-like projected separations. However, multi-epoch data show them to be background objects. We set a new 3 sigma upper limit for Fomalhaut b's H-band brightness of m(H) similar to 23.15 or 1.5-4.5 M-J. We do not recover the possible point source reported from Spitzer/IRAC data: at its location detection limits are similar to those for Fomalhaut b. Our data when combined with other recent work rule out planets with masses and projected separations comparable to HR 8799 bcde and M > 3 M-J planets at r(proj) > 45 AU. The James Webb Space Telescope will likely be required to shed substantial further light on Fomalhaut's planetary system in the next decade. C1 [Currie, Thayne; Cloutier, Ryan] Univ Toronto, Toronto, ON M5S 1A1, Canada. [Debes, John H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kenyon, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kaisler, Denise] Citrus Coll, Glendora, CA 91741 USA. RP Currie, T (reprint author), Univ Toronto, 50 St George St, Toronto, ON M5S 1A1, Canada. OI Kenyon, Scott/0000-0003-0214-609X FU National Aeronautics and Space Administration FX We thank Timothy Rodigas and Mickael Bonnefoy for draft comments; Hai Fu and Stanimir Metchev for discussions regarding the NIRC2 astrometric calibration; Christian Marois for discussions regarding observing techniques; Markus Janson and Matthew Kenworthy for providing their planet detection limits; Chas Beichman for helpful notes on JWST/NIRCAM performance; and Ray Jayawardhana for other helpful comments. This research has made use of the Keck Observatory Archive (KOA), which is operated by the W.M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. NR 49 TC 12 Z9 12 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 1 PY 2013 VL 777 IS 1 AR L6 DI 10.1088/2041-8205/777/1/L6 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241SH UT WOS:000326187400006 ER PT J AU Majewski, SR Hasselquist, S Lokas, EL Nidever, DL Frinchaboy, PM Perez, AEG Johnston, KV Meszaros, S Shetrone, M Prieto, CA Beaton, RL Beers, TC Bizyaev, D Cunha, K Damke, G Ebelke, G Eisenstein, DJ Hearty, F Holtzman, J Johnson, JA Law, DR Malanushenko, V Malanushenko, E O'Connell, RW Oravetz, D Pan, K Schiavon, RP Schneider, DP Simmons, A Skrutskie, MF Smith, VV Wilson, JC Zasowski, G AF Majewski, Steven R. Hasselquist, Sten Lokas, Ewa L. Nidever, David L. Frinchaboy, Peter M. Garcia Perez, Ana E. Johnston, Kathryn V. Meszaros, Szabolcs Shetrone, Matthew Allende Prieto, Carlos Beaton, Rachael L. Beers, Timothy C. Bizyaev, Dmitry Cunha, Katia Damke, Guillermo Ebelke, Garrett Eisenstein, Daniel J. Hearty, Fred Holtzman, Jon Johnson, Jennifer A. Law, David R. Malanushenko, Viktor Malanushenko, Elena O'Connell, Robert W. Oravetz, Daniel Pan, Kaike Schiavon, Ricardo P. Schneider, Donald P. Simmons, Audrey Skrutskie, Michael F. Smith, Verne V. Wilson, John C. Zasowski, Gail TI DISCOVERY OF A DYNAMICAL COLD POINT IN THE HEART OF THE SAGITTARIUS dSph GALAXY WITH OBSERVATIONS FROM THE APOGEE PROJECT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: dwarf; galaxies: individual (Sagittarius dSph); galaxies: interactions; galaxies: kinematics and dynamics; galaxies: stellar content; galaxies: structure ID DWARF SPHEROIDAL GALAXY; DARK-MATTER DISTRIBUTION; SKY SURVEY VIEW; MILKY-WAY; GLOBULAR-CLUSTERS; RADIAL-VELOCITIES; ACS SURVEY; KINEMATICS; EVOLUTION; STARS AB The dynamics of the core of the Sagittarius (Sgr) dwarf spheroidal (dSph) galaxy are explored using high-resolution (R similar to 22,500), H-band, near-infrared spectra of over 1000 giant stars in the central 3 deg(2) of the system, of which 328 are identified as Sgr members. These data, among some of the earliest observations from the Sloan Digital Sky Survey III/Apache Point Observatory Galactic Evolution Experiment (APOGEE) and the largest published sample of high resolution Sgr dSph spectra to date, reveal a distinct gradient in the velocity dispersion of Sgr from 11 to 14 km s(-1) for radii > 0 degrees.8 from center to a dynamical cold point of 8 km s(-1) in the Sgr center-a trend differing from that found in previous kinematical analyses of Sgr over larger scales that suggests a more or less flat dispersion profile at these radii. Well-fitting mass models with either cored and cusped dark matter distributions can be found to match the kinematical results, although the cored profile succeeds with significantly more isotropic stellar orbits than required for a cusped profile. It is unlikely that the cold point reflects an unusual mass distribution. The dispersion gradient may arise from variations in the mixture of populations with distinct kinematics within the dSph; this explanation is suggested (e. g., by detection of a metallicity gradient across similar radii), but not confirmed, by the present data. Despite these remaining uncertainties about their interpretation, these early test data (including some from instrument commissioning) demonstrate APOGEE's usefulness for precision dynamical studies, even for fields observed at extreme airmasses. C1 [Majewski, Steven R.; Hasselquist, Sten; Nidever, David L.; Garcia Perez, Ana E.; Beaton, Rachael L.; Damke, Guillermo; Hearty, Fred; O'Connell, Robert W.; Skrutskie, Michael F.; Wilson, John C.; Zasowski, Gail] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Hasselquist, Sten; Holtzman, Jon] New Mexico State Univ, Las Cruces, NM 88003 USA. [Lokas, Ewa L.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Nidever, David L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Frinchaboy, Peter M.] Texas Christian Univ, Ft Worth, TX 76129 USA. [Johnston, Kathryn V.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Meszaros, Szabolcs; Allende Prieto, Carlos] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Meszaros, Szabolcs; Allende Prieto, Carlos] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Shetrone, Matthew] Univ Texas Austin, McDonald Observ, Ft Davis, TX 79734 USA. [Beers, Timothy C.; Cunha, Katia; Smith, Verne V.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Beers, Timothy C.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Beers, Timothy C.] Michigan State Univ, JINA, E Lansing, MI 48824 USA. [Bizyaev, Dmitry; Ebelke, Garrett; Malanushenko, Viktor; Malanushenko, Elena; Oravetz, Daniel; Pan, Kaike; Simmons, Audrey] Apache Point Observ, Sunspot, NM 88349 USA. [Cunha, Katia] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Cunha, Katia] Observ Nacl, Rio De Janeiro, Brazil. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Johnson, Jennifer A.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Law, David R.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Schiavon, Ricardo P.] Gemini Observ, Hilo, HI 96720 USA. [Schiavon, Ricardo P.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 ILD, Merseyside, 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. [Zasowski, Gail] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Majewski, SR (reprint author), Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. EM srm4n@virginia.edu; sh6cy@virginia.edu; lokas@camk.edu.pl; dnidever@umich.edu; p.frinchaboy@tcu.edu; aeg4x@virginia.edu; kvj@astro.columbia.edu; meszi@iac.es; shetrone@astro.as.utexas.edu; callende@iac.es; rlb9n@virginia.edu; beers@pa.msu.edu; dmbiz@apo.nmsu.edu; cunha@email.noao.edu; gjd3r@virginia.edu; gebelke@apo.nmsu.edu; deisenstein@cfa.harvard.edu; frh3z@virginia.edu; holtz@nmsu.edu; jaj@astronomy.ohio-state.edu; drlaw@di.utoronto.ca; viktorm@apo.nmsu.edu; elenam@apo.nmsu.edu; rwo@virginia.edu; doravetz@apo.nmsu.edu; kpan@apo.nmsu.edu; rpschiavon@gmail.com; dps7@psu.edu; asimmons@apo.nmsu.edu; vsmith@email.noao.edu; jcw6z@virginia.edu; gail.zasowski@gmail.com RI Meszaros, Szabolcs/N-2287-2014; OI Meszaros, Szabolcs/0000-0001-8237-5209; Beaton, Rachael/0000-0002-1691-8217 FU National Science Foundation (NSF) [AST11-09718]; Polish National Science Centre [NN203580940]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; University of Arizona; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; Harvard University; Instituto de Astrofisica de Canarias; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX We gratefully acknowledge support from National Science Foundation (NSF) grant AST11-09718 and the Polish National Science Centre under grant NN203580940 to E.L.L.; 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 50 TC 5 Z9 5 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 1 PY 2013 VL 777 IS 1 AR L13 DI 10.1088/2041-8205/777/1/L13 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 241SH UT WOS:000326187400013 ER PT J AU Christian, S Holt, JW Byrne, S Fishbaugh, KE AF Christian, S. Holt, J. W. Byrne, S. Fishbaugh, K. E. TI Integrating radar stratigraphy with high resolution visible stratigraphy of the north polar layered deposits, Mars SO ICARUS LA English DT Article DE Mars; Mars, Polar geology; Mars, Polar caps; Radar observations ID PLEISTOCENE TEMPERATURES; ICE AGES; REGION; ORBITER AB Shallow Radar (SHARAD) on board NASA's Mars Reconnaissance Orbiter has successfully detected tens of reflectors in the subsurface of the north polar layered deposits (NPLD) of Mars. Radar reflections are hypothesized to originate from the same material interfaces that result in visible layering. As a first step towards verifying this assumption, this study uses signal analyses and geometric comparisons to quantitatively examine the relationship between reflectors and visible layers exposed in an NPLD outcrop. To understand subsurface structures and reflector geometry, reflector surfaces have been gridded in three dimensions, taking into account the influence of surface slopes to obtain accurate subsurface geometries. These geometries reveal reflector dips that are consistent with optical layer slopes. Distance-elevation profiling of subsurface reflectors and visible layer boundaries reveals that reflectors and layers demonstrate similar topography, verifying that reflectors represent paleosurfaces of the deposit. Statistical and frequency-domain analyses of the separation distances between successive layers and successive reflectors confirms the agreement of radar reflector spacing with characteristic spacing of certain visible layers. Direct elevation comparisons between individual reflectors and discrete optical layers, while necessary for a one-to-one correlation, are complicated by variations in subsurface structure that exist between the outcrop and the SHARAD observations, as inferred from subsurface mapping. Although these complications have prevented a unique correlation, a genetic link between radar reflectors and visible layers has been confirmed, validating the assumption that radar reflectors can be used as geometric proxies for visible stratigraphy. Furthermore, the techniques for conducting a stratigraphic integration have been generalized and improved so that the integration can be undertaken at additional locations. (C) 2013 Elsevier Inc. All rights reserved. C1 [Christian, S.; Holt, J. W.] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA. [Byrne, S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85745 USA. [Fishbaugh, K. E.] Smithsonian Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Christian, S (reprint author), Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA. EM schristian@utexas.edu NR 46 TC 9 Z9 9 U1 0 U2 15 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV-DEC PY 2013 VL 226 IS 2 BP 1241 EP 1251 DI 10.1016/j.icarus.2013.07.003 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 239DX UT WOS:000326003900007 ER PT J AU Loaiza, JR Miller, MJ AF Loaiza, Jose R. Miller, Matthew J. TI Seasonal pattern of avian Plasmodium-infected mosquitoes and implications for parasite transmission in central Panama SO PARASITOLOGY RESEARCH LA English DT Article ID CULEX MELANOCONION AIKENII; HOST-FEEDING PATTERNS; AFRICAN RAIN-FOREST; AEDEOMYIA-SQUAMIPENNIS; MALARIA PARASITES; VECTOR; ENCEPHALITIS; ASSOCIATIONS; CULICIDAE; LINEAGES AB Aedeomyia squamipennis and Culex (Melanoconion) ocossa, two ubiquitous Neotropical mosquito species, are likely involved in the transmission of several bird pathogens in Gamboa, central Panama. However, knowledge on their eco-epidemiological profiles is still incomplete. Our goal in this study was to investigate temporal trends of vector density and their relationship with avian plasmodia prevalence. This information is central to identifying the risk posed by each vector species to the avian community locally. We found that A. squamipennis maintains stable population size across climatic seasons and thus maybe a more efficient vector of avian malaria than C. ocossa. In contrast, C. ocossa, which undergoes considerable population expansion in the rainy season and contraction in the dry season, is likely only an important avian malaria vector during part of the year. This is consistent with the larger number of parasite isolations and Plasmodium cyt b lineages recovered from A. squamipennis than from C. ocossa and might be explained by marked differences in their seasonality and host-feeding preferences. More Plasmodium PCR testing in mosquito communities from other areas of Panama might reveal additional vectors of avian plasmodia. C1 [Loaiza, Jose R.] Inst Invest Cient & Serv Alta Tecnol, Ctr Biodiversidad & Descubrimiento Drogas, Ciudad Del Saber, Panama. [Loaiza, Jose R.] Univ Panama, Programa Ctr Amer Maestria Entomol Vicerrectoria, Panama City, Panama. [Miller, Matthew J.] Smithsonian Trop Res Inst, Panama City, Panama. RP Loaiza, JR (reprint author), Inst Invest Cient & Serv Alta Tecnol, Ctr Biodiversidad & Descubrimiento Drogas, Edificio 219,PO 0843-01103, Ciudad Del Saber, Panama. EM jloaiza@indicasat.org.pa OI Miller, Matthew/0000-0002-2939-0239 FU INDICASATAIP; STRI; National Secretariat for Science, Technology, and Innovation of Panama (SENACYT)-Research Investigator Award (SNI) FX We thank Andrea Gager, formerly from Princeton University, for the opportunity to collaborate on her Ph.D. thesis project; Eldredge Bermingham; and Oris I. Sanjur from the Smithsonian Tropical Research Institute (STRI) for logistical support and academic guidance. We acknowledge the help of Sara Veronica Pinzon, Jose R. Rovira, and Jorge Morales in collecting mosquito larvae in Gamboa. Additionally, we thank James Pecor from the Walter Reed Biosystematics Units (WRBU), U.S.A., and Luis Guillermo Chaverry from the National Institute of Biodiversity of Costa Rica (INBio) for assisting with species identification in the subgenus Melanoconion of Culex. Milton Solano produced the map on Fig. 1, Eyda Gomez offered logistic support throughout the study, and Marilyn Scott, from McGill University, critically commented on an earlier version of this work. Funding was provided by INDICASATAIP, STRI, and the National Secretariat for Science, Technology, and Innovation of Panama (SENACYT)-Research Investigator Award (SNI) granted to JRL. NR 45 TC 4 Z9 5 U1 3 U2 25 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0932-0113 EI 1432-1955 J9 PARASITOL RES JI Parasitol. Res. PD NOV PY 2013 VL 112 IS 11 BP 3743 EP 3751 DI 10.1007/s00436-013-3562-5 PG 9 WC Parasitology SC Parasitology GA 240RT UT WOS:000326115400008 PM 23974324 ER PT J AU Kajihara, H Sun, SC Chernyshev, AV Chen, HX Ito, K Asakawa, M Maslakova, SA Norenburg, JL Strand, M Sundberg, P Iwata, F AF Kajihara, Hiroshi Sun, Shi-Chun Chernyshev, Alexei V. Chen, Hai-Xia Ito, Katsutoshi Asakawa, Manabu Maslakova, Svetlana A. Norenburg, Jon L. Strand, Malin Sundberg, Per Iwata, Fumio TI Taxonomic Identity of a Tetrodotoxin-Accumulating Ribbon-worm Cephalothrix simula (Nemertea: Palaeonemertea): A Species Artificially Introduced from the Pacific to Europe SO ZOOLOGICAL SCIENCE LA English DT Article DE 3-D reconstruction; alien species; DNA barcoding; Cephalotrichidae; topogenetype; TTX accumulation ID PROCEPHALOTHRIX-SIMULUS; HIROSHIMA PREFECTURE; PHYLOGENETIC ANALYSIS; PHYLUM NEMERTEA; IWATA; ANOPLA; JAPAN; BAY; ANHYDROTETRODOTOXIN; CEPHALOTRICHIDAE AB We compared the anatomy of the holotype of the palaeonemertean Cephalothrix simula (Iwata, 1952) with that of the holotypes of Cephalothrix hongkongiensis Sundberg, Gibson and Olsson, 2003 and Cephalothrix fasciculus (Iwata, 1952), as well as additional specimens from Fukue (type locality of C. simula) and Hiroshima, Japan. While there was no major morphological discordance between these specimens, we found discrepancies between the actual morphology and some statements in the original description of C. simula with respect to supposedly species-specific characters. Our observation indicates that these three species cannot be discriminated by the anatomical characters so far used to distinguish congeners. For objectivity of scientific names, topogenetypes of the mitochondrial cytochrome c oxidase subunit I (COI) sequences are designated for C. simula, C. hongkongiensis, and C. fasciculus. Analysis of COI sequence showed that the Hiroshima population can be identified as C. simula, which has been found in previous studies from Trieste, Italy, and also from both the Mediterranean and Atlantic coasts of the Iberian Peninsula, indicating an artificial introduction via (1) ballast water, (2) ship-fouling communities, or (3) the commercially cultured oyster Crassostrea gigas (Thunberg, 1793) brought from Japan to France in 1970s. Cephalothrix simula is known to be toxic, as it contains large amounts of tetrodotoxin (TTX). We report here that the grass puffer Takifugu niphobles (Jordan and Snyder, 1901)-also known to contain TTX-consumes C. simula. We suggest that the puffer may be able to accumulate TTX by eating C. simula. C1 [Kajihara, Hiroshi; Iwata, Fumio] Hokkaido Univ, Fac Sci, Sapporo, Hokkaido 0600810, Japan. [Sun, Shi-Chun; Chen, Hai-Xia] Ocean Univ China, Inst Evolut & Marine Biodivers, Qingdao 266003, Peoples R China. [Chernyshev, Alexei V.] AV Zhirmunsky Inst Marine Biol, Vladivostok 690059, Russia. [Chernyshev, Alexei V.] Far Eastern Fed Univ, Vladivostok 690600, Russia. [Chen, Hai-Xia; Strand, Malin; Sundberg, Per] Univ Gothenburg, Dept Biol & Environm Sci, SE-40530 Gothenburg, Sweden. [Ito, Katsutoshi] Fisheries Res Agcy, Natl Res Inst Fisheries & Environm Inland Sea, Hiroshima 7390452, Japan. [Asakawa, Manabu] Hiroshima Univ, Grad Sch Biosphere, Higashihiroshima 7398528, Japan. [Maslakova, Svetlana A.] Univ Oregon, Oregon Inst Marine Biol, Charleston, OR 97420 USA. [Norenburg, Jon L.] Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Kajihara, H (reprint author), Hokkaido Univ, Fac Sci, Sapporo, Hokkaido 0600810, Japan. EM kazi@mail.sci.hokudai.ac.jp RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 FU Japan Society for the Promotion of Science [16770059, 16207005, 20770061]; Showa Seitoku Memorial Foundation; Research Institute of Marine Invertebrates Foundation [14]; National Natural Science Foundation of China [31172046]; Russian Federation Government [11.G34.31.0010]; Swedish Research Council; NSF PEET award [DEB 9712463] FX We are indebted to Prof. Susumu Ohtsuka (Takehara Marine Science Station, Hiroshima University) for providing facilities. We also thank Mrs. Junko Sato (Hokkaido University) for digital image photographing of serial sections, Dr. Elena M. Chaban (Zoological Institute, Russian Academy of Science) for sharing the information about the type slides of Procephalothrix mokievskii Korotkevitsch, 1982, and Prof. Martin Thiel (Universidad Catolica del Norte, Chile) and two anonymous reviewers for helpful comments that improved this manuscript. This work was partially funded by Grant-in-Aid from the Japan Society for the Promotion of Science (research grant numbers 16770059, 16207005, and 20770061), Showa Seitoku Memorial Foundation (FY 2007), and Research Institute of Marine Invertebrates Foundation (grant number 14) to HK; the National Natural Science Foundation of China (31172046) to SCS; the Russian Federation Government grant (No 11.G34.31.0010) to AVC; the Swedish Research Council to PS; and NSF PEET award (DEB 9712463) to JLN. NR 97 TC 2 Z9 3 U1 2 U2 12 PU ZOOLOGICAL SOC JAPAN PI TOKYO PA HONGO MT BUILDING 4F, HONGO 7-2-2, BUNKYO-KU, TOKYO, 113-0033, JAPAN SN 0289-0003 J9 ZOOL SCI JI Zool. Sci. PD NOV PY 2013 VL 30 IS 11 BP 985 EP 997 DI 10.2108/zsj.30.985 PG 13 WC Zoology SC Zoology GA 242ML UT WOS:000326246300013 PM 24199864 ER PT J AU Dittus, WPJ AF Dittus, Wolfgang P. J. TI Arboreal Adaptations of Body Fat in Wild Toque Macaques (Macaca sinica) and the Evolution of Adiposity in Primates SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Review DE adipose tissue patterning; arboreal primate; wild population; hominid evolution ID FEMALE RHESUS-MONKEYS; BABOONS PAPIO-ANUBIS; VERVET MONKEYS; NATURAL-POPULATION; SEX-DIFFERENCES; OLIVE BABOONS; SOMATOMETRIC GROWTH; FRUIT AVAILABILITY; CYNOMOLGUS MONKEYS; JAPANESE MACAQUES AB There is a paucity of information on body composition and fat patterning in wild nonhuman primates. Dissected adipose tissue from wild toque macaques (Macaca sinica) (WTM), feeding on a natural diet, accounted for 2.1% of body weight. This was far less than fatness reported for nonhuman primates raised in captivity or for contemporary humans. In WTM, fatness increased with age and diet richness, but did not differ by sex. In WTM (none of which were obese) intra-abdominal fat filled first, and excess fat was stored peripherally in a ratio of about 6:1. Intermuscular fat was minimal (0.1%). The superficial paunch held <15% of subcutaneous fat weight in contrast to its much larger proportions in obese humans and captive monkeys where most added fat accumulates subcutaneously. With increasing total adiposity, accumulating fat shifted in its distribution among eight different main internal and peripheral deposit areasconsistent with maintaining body balance and a low center of gravity. The available data suggest that, in arboreal primates, adaptations for agile locomotion and terminal branch feeding set constraints on the quantity and distribution of fat. The absence of a higher percentage of body fat in females and neonates (as are typical of humans) suggests that arboreal adaptations preclude the development of fat-dependent, large-brained infants and the adipose-rich mothers needed to sustain them. The lifestyle and body composition of wild primates represent a more appropriate model for early human foragers than well-fed captive monkeys do. Am J Phys Anthropol 152:333-344, 2013. (c) 2013 Wiley Periodicals, Inc. C1 [Dittus, Wolfgang P. J.] Natl Zool Pk, Conservat Ecol Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Dittus, Wolfgang P. J.] Natl Inst Fundamental Studies, Kandy 20000, Sri Lanka. RP Dittus, WPJ (reprint author), Natl Zool Pk, Conservat Ecol Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. EM wdittus@gmail.com FU US National Science Foundation; Earthwatch Institute FX Grant sponsors: US National Science Foundation; Earthwatch Institute. NR 134 TC 3 Z9 3 U1 0 U2 16 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 NOV PY 2013 VL 152 IS 3 BP 333 EP 344 DI 10.1002/ajpa.22351 PG 12 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 238VU UT WOS:000325980400004 PM 24022522 ER PT J AU Olsen, BJ Greenberg, R Walters, JR Fleischer, RC AF Olsen, Brian J. Greenberg, Russell Walters, Jeffrey R. Fleischer, Robert C. TI Sexual dimorphism in a feeding apparatus is driven by mate choice and not niche partitioning SO BEHAVIORAL ECOLOGY LA English DT Article DE allometry; foraging niche; male; male competition; Melospiza georgiana; sexual selection; swamp sparrow ID BILL SIZE; DARWINS FINCHES; SWAMP SPARROW; ECOLOGICAL CAUSATION; EXTRAPAIR PATERNITY; NATURAL-SELECTION; MARSH SPARROWS; VOCAL-TRACT; BODY SIZE; EVOLUTION AB The evolutionary origins of sexual dimorphism are credited to both natural and sexual selection. Sexual dimorphism in feeding structures, however, provides some of the clearest examples of ecologically driven dimorphism. Studies of bird bills have significantly aided these claims, but bird bills are also commonly used in pair formation behaviors, and thus their morphology could be subject to sexual selection. We tested 4 hypotheses of the evolution of sexual dimorphism using the feeding structure of a sexually dimorphic and a nondimorphic subspecies of the swamp sparrow, Melospiza georgiana. The increased bill volume of males was not explained by simple allometric relationships, ecological niche divergence between the sexes, or correlations with territory defense. Male bill volume was positively selected by female mate choice, as relative male bill volume predicted both the presence of and degree of cuckoldry. Further, male bill volume increased with age, and females may thus receive benefits by choosing larger billed males for social (direct benefits) or extrapair (indirect benefits) mates. It is clear from this example that sexual selection can play a role in the evolution of sexually dimorphic feeding structures, even in bird bills, which are a classic system for ecologically driven sexual dimorphism. C1 [Olsen, Brian J.] Univ Maine, Sch Biol & Ecol, Climate Change Inst, Orono, ME 04469 USA. [Greenberg, Russell] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Walters, Jeffrey R.] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA. [Fleischer, Robert C.] Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. RP Olsen, BJ (reprint author), Univ Maine, Sch Biol & Ecol, Climate Change Inst, 5722 Deering Hall, Orono, ME 04469 USA. EM brian.olsen@maine.edu FU Bailey Fund at Virginia Tech; Smithsonian Institution's Abbot Fund; Delaware Division of Fish and Wildlife; Maryland Ornithological Society; Washington Biologists' Field Club; Eastern Bird Banding Association; Virginia Tech's Graduate Research Development Program; Smithsonian Center for Conservation and Evolutionary Genetics; Smithsonian Institution Graduate Fellowship; Smithsonian Institution Predoctoral Fellowship FX Funding was supplied by grants from the Bailey Fund at Virginia Tech, the Smithsonian Institution's Abbot Fund, the Delaware Division of Fish and Wildlife, the Maryland Ornithological Society, the Washington Biologists' Field Club, the Washington Group of the Explorer's Club, the Eastern Bird Banding Association, Virginia Tech's Graduate Research Development Program, the Smithsonian Center for Conservation and Evolutionary Genetics, and Smithsonian Institution Graduate and Predoctoral Fellowships. NR 80 TC 3 Z9 3 U1 7 U2 73 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 NOV-DEC PY 2013 VL 24 IS 6 BP 1327 EP 1338 DI 10.1093/beheco/art071 PG 12 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 239BG UT WOS:000325995900009 ER PT J AU Suzuki, H Nunome, M Kinoshita, G Aplin, KP Vogel, P Kryukov, AP Jin, ML Han, SH Maryanto, I Tsuchiya, K Ikeda, H Shiroishi, T Yonekawa, H Moriwaki, K AF Suzuki, H. Nunome, M. Kinoshita, G. Aplin, K. P. Vogel, P. Kryukov, A. P. Jin, M-L Han, S-H Maryanto, I. Tsuchiya, K. Ikeda, H. Shiroishi, T. Yonekawa, H. Moriwaki, K. TI Evolutionary and dispersal history of Eurasian house mice Mus musculus clarified by more extensive geographic sampling of mitochondrial DNA SO HEREDITY LA English DT Article DE mitochondrial DNA; cytochrome b; control region; phylogeography; wild house mouse ID JAPANESE MICE; WILD MICE; MAXIMUM-LIKELIHOOD; MAMMAL ASSEMBLAGES; GENETIC-VARIATION; CULTIVATED RICE; HYBRID ORIGIN; MOUSE; COLONIZATION; DIVERSITY AB We examined the sequence variation of mitochondrial DNA control region and cytochrome b gene of the house mouse (Mus musculus sensu lato) drawn from ca. 200 localities, with 286 new samples drawn primarily from previously unsampled portions of their Eurasian distribution and with the objective of further clarifying evolutionary episodes of this species before and after the onset of human-mediated long-distance dispersals. Phylogenetic analysis of the expanded data detected five equally distinct clades, with geographic ranges of northern Eurasia (musculus, MUS), India and Southeast Asia (castaneus, CAS), Nepal (unspecified, NEP), western Europe (domesticus, DOM) and Yemen (gentilulus). Our results confirm previous suggestions of Southwestern Asia as the likely place of origin of M. musculus and the region of Iran, Afghanistan, Pakistan, and northern India, specifically as the ancestral homeland of CAS. The divergence of the subspecies lineages and of internal sublineage differentiation within CAS were estimated to be 0.37-0.47 and 0.14-0.23 million years ago (mya), respectively, assuming a split of M. musculus and Mus spretus at 1.7 mya. Of the four CAS sublineages detected, only one extends to eastern parts of India, Southeast Asia, Indonesia, Philippines, South China, Northeast China, Primorye, Sakhalin and Japan, implying a dramatic range expansion of CAS out of its homeland during an evolutionary short time, perhaps associated with the spread of agricultural practices. Multiple and non-coincident eastward dispersal events of MUS sublineages to distant geographic areas, such as northern China, Russia and Korea, are inferred, with the possibility of several different routes. C1 [Suzuki, H.; Nunome, M.; Kinoshita, G.] Hokkaido Univ, Grad Sch Environm Earth Sci, Lab Ecol & Genet, Sapporo, Hokkaido 0600810, Japan. [Aplin, K. P.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. [Vogel, P.] Univ Lausanne, Dept Ecol & Evolut, Lausanne, Switzerland. [Kryukov, A. P.] Russian Acad Sci, Inst Biol & Soil Sci, Vladivostok 690041, Russia. [Jin, M-L] Chinese Acad Sci, Shanghai Inst Biol Sci, Shanghai Res Ctr Biotechnol, Shanghai, Peoples R China. [Han, S-H] Natl Inst Biol Resources, Inchon, South Korea. [Maryanto, I.] Indonesian Inst Sci, Museum Zool Bogoriense, Cibinong, Indonesia. [Tsuchiya, K.] Appl Biol Co Ltd, Lab Bioresources, Minato Ku, Tokyo, Japan. [Ikeda, H.] Nippon Vet & Anim Sci Univ, Dept Vet Publ Hlth, Tokyo, Japan. [Shiroishi, T.] Res Org Informat & Syst, Natl Inst Genet, Mammalian Genet Lab, Mishima, Shizuoka 4118540, Japan. [Yonekawa, H.] Tokyo Metropolitan Inst Med Sci, Dept Lab Anim Sci, Tokyo 113, Japan. [Moriwaki, K.] RIKEN, Bioresource Ctr, Tsukuba, Ibaraki, Japan. RP Suzuki, H (reprint author), Hokkaido Univ, Grad Sch Environm Earth Sci, Lab Ecol & Genet, Kita Ku, North 10,West 5, Sapporo, Hokkaido 0600810, Japan. EM htsuzuki@ees.hokudai.ac.jp RI Suzuki, Hitoshi/F-8539-2012 OI Suzuki, Hitoshi/0000-0003-4426-385X FU Japan Society for the Promotion of Science (JSPS) [23570101]; Heiwa Nakajima Foundation FX We wish to express our appreciation to Kuniya Abe, Masahiro A. Iwasa, Martua H. Sinaga and Shumpei P. Yasuda for their valuable advice in this study. We thank Francois Catzeflis, Angela Frost, Naoto Hanzawa, Hideo Igawa, Oleg E. Lopatin, Hiromi Okamura, Yoshifumi Matsushima, Hidetoshi Matsuzawa, Natan Mise, Nobumoto Miyashita, Pavel Munclinger, Robert Palmer, Kenkichi Sasaki, Hironori Ueda, Keiichi Yokoyama and numerous other collectors of mice for kind help in supplying the valuable samples used in this study. This study was, in part, supported by the Grant-in-Aid for Scientific Research (C) from the Japan Society for the Promotion of Science (JSPS, 23570101). We would like to thank the Heiwa Nakajima Foundation for its generous support. NR 92 TC 22 Z9 26 U1 2 U2 51 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 NOV PY 2013 VL 111 IS 5 BP 375 EP 390 DI 10.1038/hdy.2013.60 PG 16 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 237KG UT WOS:000325868000003 PM 23820581 ER PT J AU Cicconardi, F Fanciulli, PP Emerson, BC AF Cicconardi, Francesco Fanciulli, Pietro P. Emerson, Brent C. TI Collembola, the biological species concept and the underestimation of global species richness SO MOLECULAR ECOLOGY LA English DT Article DE biodiversity; cryptic species; Lepidocyrtus; molecular lineage; Panama ID BAYESIAN-INFERENCE; BIODIVERSITY HOTSPOTS; LEPIDOCYRTUS BOURLET; CENTRAL-AMERICA; ENTOMOBRYIDAE; FOREST; SPRINGTAILS; PHYLOGENY; PATTERNS; HISTORY AB Despite its ancient origin, global distribution and abundance in nearly all habitats, the class Collembola is comprised of only 8000 described species and is estimated to number no more than 50000. Many morphologically defined species have broad geographical ranges that span continents, and recent molecular work has revealed high genetic diversity within species. However, the evolutionary significance of this genetic diversity is unknown. In this study, we sample five morphological species of the globally distributed genus Lepidocyrtus from 14 Panamanian sampling sites to characterize genetic diversity and test morphospecies against the biological species concept. Mitochondrial and nuclear DNA sequence data were analysed and a total of 58 molecular lineages revealed. Deep lineage diversification was recovered, with 30 molecular lineages estimated to have established more than 10million years ago, and the origin almost all contemporary lineages preceding the onset of the Pleistocene (similar to 2Mya). Thirty-four lineages were sampled in sympatry revealing unambiguous cosegregation of mitochondrial and nuclear DNA sequence variation, consistent with biological species. Species richness within the class Collembola and the geographical structure of this diversity are substantially misrepresented components of terrestrial animal biodiversity. We speculate that global species richness of Collembola could be at least an order of magnitude greater than a previous estimate of 50000 species. C1 [Cicconardi, Francesco] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Cicconardi, Francesco] Smithsonian Trop Res Inst, Panama City, Panama. [Fanciulli, Pietro P.] Univ Siena, Dept Life Sci, I-53100 Siena, Italy. [Emerson, Brent C.] IPNA CSIC, Isl Ecol & Evolut Res Grp, Tenerife 38206, Canary Islands, Spain. [Emerson, Brent C.] Univ E Anglia, Sch Biol Sci, Norwich NR4 7TJ, Norfolk, England. RP Cicconardi, F (reprint author), Univ Roma La Sapienza, Dept Phys, Ple A Moro 5, I-00185 Rome, Italy. EM francicco@gmail.com OI Emerson, Brent/0000-0003-4067-9858 FU Smithsonian Institution; Italian Ministry of Education, Universities and Research; Leverhulme Trust FX F.C. gratefully acknowledges the Smithsonian Institution for Tropical Research and thanks the National Environmental Authority of Panama's (ANAM) for granting collecting and export permits. He also wishes to thank Dr. Oris Sanjur for his extensive help with various aspects of the sampling campaign, Dr. Donald M. Windsor, Vanessa Sanchez and all the members of the Windsor Lab at STRI for their kind support and outstanding assistance throughout all phases of the stay in Panama. F.C. wants also to thank Prof. Alessandro Nardone from University of Tuscia, for letting use the molecular biology resource facility. This research was financial supported by the Smithsonian Institution Short-fellowship Program Partial, the Italian Ministry of Education, Universities and Research and by a Research Fellowship awarded to Brent Emerson from The Leverhulme Trust. We also would like to thank the editor and the four referees for helpful comments. NR 75 TC 16 Z9 17 U1 3 U2 61 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 NOV PY 2013 VL 22 IS 21 BP 5382 EP 5396 DI 10.1111/mec.12472 PG 15 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 238ZI UT WOS:000325990500009 PM 24112308 ER PT J AU Hungate, BA Dijkstra, P Wu, ZT Duval, BD Day, FP Johnson, DW Megonigal, JP Brown, ALP Garland, JL AF Hungate, Bruce A. Dijkstra, Paul Wu, Zhuoting Duval, Benjamin D. Day, Frank P. Johnson, Dale W. Megonigal, J. Patrick Brown, Alisha L. P. Garland, Jay L. TI Cumulative response of ecosystem carbon and nitrogen stocks to chronic CO2 exposure in a subtropical oak woodland SO NEW PHYTOLOGIST LA English DT Article DE carbon cycling; elevated CO2; global change; long-term experiment; nitrogen cycling; scrub oak; soil carbon; subtropical woodland ID ELEVATED ATMOSPHERIC CO2; FLORIDA SCRUB-OAK; SOIL ORGANIC-MATTER; DIOXIDE ENRICHMENT; FOREST PRODUCTIVITY; TERRESTRIAL ECOSYSTEMS; MICROBIAL COMMUNITIES; RHIZOSPHERE PROCESSES; ABOVEGROUND BIOMASS; CLIMATE FEEDBACKS AB Rising atmospheric carbon dioxide (CO2) could alter the carbon (C) and nitrogen (N) content of ecosystems, yet the magnitude of these effects are not well known. We examined C and N budgets of a subtropical woodland after 11yr of exposure to elevated CO2. We used open-top chambers to manipulate CO2 during regrowth after fire, and measured C, N and tracer N-15 in ecosystem components throughout the experiment. Elevated CO2 increased plant C and tended to increase plant N but did not significantly increase whole-system C or N. Elevated CO2 increased soil microbial activity and labile soil C, but more slowly cycling soil C pools tended to decline. Recovery of a long-term N-15 tracer indicated that CO2 exposure increased N losses and altered N distribution, with no effect on N inputs. Increased plant C accrual was accompanied by higher soil microbial activity and increased C losses from soil, yielding no statistically detectable effect of elevated CO2 on net ecosystem C uptake. These findings challenge the treatment of terrestrial ecosystems responses to elevated CO2 in current biogeochemical models, where the effect of elevated CO2 on ecosystem C balance is described as enhanced photosynthesis and plant growth with decomposition as a first-order response. C1 [Hungate, Bruce A.; Dijkstra, Paul; Wu, Zhuoting; Duval, Benjamin D.] No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. [Hungate, Bruce A.; Dijkstra, Paul; Wu, Zhuoting; Duval, Benjamin D.] No Arizona Univ, Ctr Ecosyst Sci & Soc, Flagstaff, AZ 86011 USA. [Wu, Zhuoting] US Geol Survey, Flagstaff, AZ 86001 USA. [Duval, Benjamin D.] ARS, US Dairy Forage Res Ctr, USDA, Madison, WI 53706 USA. [Day, Frank P.; Brown, Alisha L. P.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. [Johnson, Dale W.] Univ Nevada, Dept Nat Resources & Environm Sci, Reno, NV 89557 USA. [Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Garland, Jay L.] US EPA, Microbiol & Chem Exposure Assessment Res Div, Cincinnati, OH 45268 USA. RP Hungate, BA (reprint author), No Arizona Univ, Dept Biol Sci, Box 5640, Flagstaff, AZ 86011 USA. EM bruce.hungate@nau.edu FU US Department of Energy [DE-FG-02-95ER61993, 95-59, MPOOO02]; National Science Foundation [DEB 9873715, 0092642, 0445324]; National Aeronautics and Space Administration at the Kennedy Space Center; US Fish and Wildlife Service at Merritt Island National Wildlife Refuge FX This research was supported by the US Department of Energy (DE-FG-02-95ER61993, and subcontract 95-59, MPOOO02), and by the National Science Foundation (DEB 9873715, 0092642, and 0445324). The National Aeronautics and Space Administration at the Kennedy Space Center, the US Fish and Wildlife Service at Merritt Island National Wildlife Refuge provided generous support throughout the CO2 project. Thanks to Bert Drake for visionary leadership and opportunity. Victoria Albarracin, Mike Roberts, Mary Hummerick, Jan Bauer and Lanfang Levine assisted in the laboratory. NR 106 TC 15 Z9 15 U1 5 U2 93 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1469-8137 J9 NEW PHYTOL JI New Phytol. PD NOV PY 2013 VL 200 IS 3 BP 753 EP 766 DI 10.1111/nph.12333 PG 14 WC Plant Sciences SC Plant Sciences GA 233GI UT WOS:000325555400018 PM 23718224 ER PT J AU Hungate, BA Day, FP Dijkstra, P Duval, BD Hinkle, CR Langley, JA Megonigal, JP Stiling, P Johnson, DW Drake, BG AF Hungate, Bruce A. Day, Frank P. Dijkstra, Paul Duval, Benjamin D. Hinkle, C. Ross Langley, J. Adam Megonigal, J. Patrick Stiling, Peter Johnson, Dale W. Drake, Bert G. TI Fire, hurricane and carbon dioxide: effects on net primary production of a subtropical woodland SO NEW PHYTOLOGIST LA English DT Article DE disturbance; elevated CO2; fire; global environmental change; hurricane; net primary productivity (NPP); nitrogen cycling; oak woodland ID SCRUB-OAK ECOSYSTEM; ELEVATED ATMOSPHERIC CO2; NITROGEN-USE EFFICIENCY; LONG-TERM EXPOSURE; FOREST PRODUCTIVITY; FLORIDA SCRUB; TERRESTRIAL ECOSYSTEMS; ROOT BIOMASS; SOIL CARBON; ABOVEGROUND BIOMASS AB Disturbance affects most terrestrial ecosystems and has the potential to shape their responses to chronic environmental change. Scrub-oak vegetation regenerating from fire disturbance in subtropical Florida was exposed to experimentally elevated carbon dioxide (CO2) concentration (+350ll(-1)) using open-top chambers for 11yr, punctuated by hurricane disturbance in year 8. Here, we report the effects of elevated CO2 on aboveground and belowground net primary productivity (NPP) and nitrogen (N) cycling during this experiment. The stimulation of NPP and N uptake by elevated CO2 peaked within 2yr after disturbance by fire and hurricane, when soil nutrient availability was high. The stimulation subsequently declined and disappeared, coincident with low soil nutrient availability and with a CO2-induced reduction in the N concentration of oak stems. These findings show that strong growth responses to elevated CO2 can be transient, are consistent with a progressively limited response to elevated CO2 interrupted by disturbance, and illustrate the importance of biogeochemical responses to extreme events in modulating ecosystem responses to global environmental change. C1 [Hungate, Bruce A.; Dijkstra, Paul; Duval, Benjamin D.] No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. [Hungate, Bruce A.; Dijkstra, Paul; Duval, Benjamin D.] No Arizona Univ, Ecosyst Sci & Soc Ctr, Flagstaff, AZ 86011 USA. [Day, Frank P.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. [Duval, Benjamin D.] ARS, USDA, Dairy Forage Res Ctr, Madison, WI 53706 USA. [Hinkle, C. Ross] Univ Cent Florida, Orlando, FL 32816 USA. [Langley, J. Adam] Villanova Univ, Dept Biol, Villanova, PA 19085 USA. [Megonigal, J. Patrick; Drake, Bert G.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Stiling, Peter] Univ S Florida, Tampa, FL 33620 USA. [Johnson, Dale W.] Univ Nevada, Dept Nat Resources, Reno, NV 89557 USA. RP Hungate, BA (reprint author), No Arizona Univ, Dept Biol Sci, Box 5640, Flagstaff, AZ 86011 USA. EM Bruce.Hungate@nau.edu FU US Department of Energy [DE-FG-02-95ER61993, 95-59, MPOOO02]; National Science Foundation [DEB 0092642, 0445324]; National Aeronautics and Space Administration at the Kennedy Space Center; US Fish and Wildlife Service at Merritt Island National Wildlife Refuge FX The CO2 project was supported by the US Department of Energy (DE-FG-02-95ER61993 and subcontract 95-59, MPOOO02) and by the National Science Foundation (DEB 0092642 and 0445324). The National Aeronautics and Space Administration at the Kennedy Space Center and the US Fish and Wildlife Service at Merritt Island National Wildlife Refuge provided generous support throughout the CO2 project. The authors thank David Johnson, Graham Hymus, Jiahong Li, Debra Colavito, Hans Anderson, Dan Stover, Alisha Brown, Rachel Schroeder, John Butnor, John Dilustro and Troy Seiler for fieldwork. NR 64 TC 3 Z9 3 U1 3 U2 39 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1469-8137 J9 NEW PHYTOL JI New Phytol. PD NOV PY 2013 VL 200 IS 3 BP 767 EP 777 DI 10.1111/nph.12409 PG 11 WC Plant Sciences SC Plant Sciences GA 233GI UT WOS:000325555400019 PM 23869799 ER PT J AU Day, FP Schroeder, RE Stover, DB Brown, ALP Butnor, JR Dilustro, J Hungate, BA Dijkstra, P Duval, BD Seiler, TJ Drake, BG Hinkle, CR AF Day, Frank P. Schroeder, Rachel E. Stover, Daniel B. Brown, Alisha L. P. Butnor, John R. Dilustro, John Hungate, Bruce A. Dijkstra, Paul Duval, Benjamin D. Seiler, Troy J. Drake, Bert G. Hinkle, C. Ross TI The effects of 11 yr of CO2 enrichment on roots in a Florida scrub-oak ecosystem SO NEW PHYTOLOGIST LA English DT Article DE CO2 enrichment; disturbance; ground-penetrating radar; minirhizotrons; root biomass; root closure; scrub-oak ID ELEVATED ATMOSPHERIC CO2; GROUND-PENETRATING RADAR; LONG-TERM EXPOSURE; SOIL CARBON; FINE ROOTS; NITROGEN LIMITATION; ABOVEGROUND BIOMASS; NATURAL ECOSYSTEMS; TALLGRASS PRAIRIE; TEMPERATE FOREST AB Uncertainty surrounds belowground plant responses to rising atmospheric CO2 because roots are difficult to measure, requiring frequent monitoring as a result of fine root dynamics and long-term monitoring as a result of sensitivity to resource availability. We report belowground plant responses of a scrub-oak ecosystem in Florida exposed to 11yr of elevated atmospheric CO2 using open-top chambers. We measured fine root production, turnover and biomass using minirhizotrons, coarse root biomass using ground-penetrating radar and total root biomass using soil cores. Total root biomass was greater in elevated than in ambient plots, and the absolute difference was larger than the difference aboveground. Fine root biomass fluctuated by more than a factor of two, with no unidirectional temporal trend, whereas leaf biomass accumulated monotonically. Strong increases in fine root biomass with elevated CO2 occurred after fire and hurricane disturbance. Leaf biomass also exhibited stronger responses following hurricanes. Responses after fire and hurricanes suggest that disturbance promotes the growth responses of plants to elevated CO2. Increased resource availability associated with disturbance (nutrients, water, space) may facilitate greater responses of roots to elevated CO2. The disappearance of responses in fine roots suggests limits on the capacity of root systems to respond to CO2 enrichment. C1 [Day, Frank P.; Schroeder, Rachel E.; Brown, Alisha L. P.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. [Stover, Daniel B.] US DOE, Off Biol & Environm Res, Washington, DC 20585 USA. [Butnor, John R.] US Forest Serv, So Res Stn, USDA, Burlington, VT 05405 USA. [Dilustro, John] Chowan Univ, Dept Biol, Murfreesboro, NC 27855 USA. [Hungate, Bruce A.; Dijkstra, Paul] Univ Arizona, Dept Biol Sci, Flagstaff, AZ 86011 USA. [Hungate, Bruce A.; Dijkstra, Paul] Univ Arizona, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA. [Duval, Benjamin D.] Univ Illinois, Inst Genom Biol, Global Change Solut, Urbana, IL 61801 USA. [Seiler, Troy J.] ENSCO Inc, Melbourne, FL 32940 USA. [Drake, Bert G.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Hinkle, C. Ross] Univ Cent Florida, Dept Biol, Orlando, FL 32816 USA. RP Day, FP (reprint author), Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. EM fday@odu.edu RI Butnor, John/P-9738-2016 FU US Department of Energy [DE-FG-02-95ER61993]; Smithsonian Institution [95-59-MPOOO02]; National Science Foundation [DEB 9873715, 0092642, 0445324] FX This research was funded by US Department of Energy grant (DE-FG-02-95ER61993) to the Smithsonian Institution with subcontract (95-59-MPOOO02) to F. P. D. at Old Dominion University, and by grants from the National Science Foundation (DEB 9873715, 0092642 and 0445324) to B. A. H. at Northern Arizona University. We thank the US Fish and Wildlife Service at Merritt Island National Wildlife Refuge and the National Aeronautics and Space Administration at Kennedy Space Center for their cooperation. Soil coring was assisted by J. Brown, J. Blankinship, J. Coyle, C. LaViolete, Z. Wu, Tom Powell and Pat Megonigal. Kadrin Getman provided invaluable field assistance. Dan Welch of Geophysical Survey Systems Inc. provided help with data processing questions, and Dayanand Naik assisted with statistical analyses. NR 81 TC 13 Z9 14 U1 4 U2 54 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1469-8137 J9 NEW PHYTOL JI New Phytol. PD NOV PY 2013 VL 200 IS 3 BP 778 EP 787 DI 10.1111/nph.12246 PG 10 WC Plant Sciences SC Plant Sciences GA 233GI UT WOS:000325555400020 PM 23528147 ER PT J AU Stiling, P Moon, D Rossi, A Forkner, R Hungate, BA Day, FP Schroeder, RE Drake, B AF Stiling, Peter Moon, Daniel Rossi, Anthony Forkner, Rebecca Hungate, Bruce A. Day, Frank P. Schroeder, Rachel E. Drake, Bert TI Direct and legacy effects of long-term elevated CO2 on fine root growth and plant-insect interactions SO NEW PHYTOLOGIST LA English DT Article DE fine root growth; Florida; herbivory; legacy effects; long-term effects of elevated CO2; scrub oaks ID ATMOSPHERIC CARBON-DIOXIDE; SCRUB-OAK ECOSYSTEM; HERBIVORE INTERACTIONS; ABOVEGROUND BIOMASS; FOREST; ENRICHMENT; RESPONSES; QUALITY; FUTURE; METAANALYSIS AB Increasing atmospheric CO2 concentrations alter leaf physiology, with effects that cascade to communities and ecosystems. Yet, responses over cycles of disturbance and recovery are not well known, because most experiments span limited ecological time. We examined the effects of CO2 on root growth, herbivory and arthropod biodiversity in a woodland from 1996 to 2006, and the legacy of CO2 enrichment on these processes during the year after the CO2 treatment ceased. We used minirhizotrons to study root growth, leaf censuses to study herbivory and pitfall traps to determine the effects of elevated CO2 on arthropod biodiversity. Elevated CO2 increased fine root biomass, but decreased foliar nitrogen and herbivory on all plant species. Insect biodiversity was unchanged in elevated CO2. Legacy effects of elevated CO2 disappeared quickly as fine root growth, foliar nitrogen and herbivory levels recovered in the next growing season following the cessation of elevated CO2. Although the effects of elevated CO2 cascade through plants to herbivores, they do not reach other trophic levels, and biodiversity remains unchanged. The legacy of 10yr of elevated CO2 on plant-herbivore interactions in this system appear to be minimal, indicating that the effects of elevated CO2 may not accumulate over cycles of disturbance and recovery. C1 [Stiling, Peter] Univ S Florida, Dept Integrat Biol, Tampa, FL 33620 USA. [Moon, Daniel; Rossi, Anthony] Univ N Florida, Dept Biol, Jacksonville, FL 33224 USA. [Forkner, Rebecca] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Hungate, Bruce A.] Univ Arizona, Dept Biol Sci, Flagstaff, AZ 86011 USA. [Day, Frank P.; Schroeder, Rachel E.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. [Drake, Bert] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Stiling, P (reprint author), Univ S Florida, Dept Integrat Biol, Tampa, FL 33620 USA. EM pstiling@usf.edu FU Office of Science (BER), US Department of Energy, through Southeast Regional Center of the National Institute for Global Environmental Change grants; National Science Foundation (NSF) grant; Department of Energy grants; NASA Kennedy Space Center; Dynamac Corporation FX This research was supported by the Office of Science (BER), US Department of Energy, through Southeast Regional Center of the National Institute for Global Environmental Change grants to P. S., by a National Science Foundation (NSF) grant to B. A. H. and by Department of Energy grants to B. D. Jamie Colson-Moon helped collect the pitfall traps. Thanks are due to Sylvia Lukasiewicz, Terri Albarricin, Kerry Bohl, Heather Jezorek, Kara Winston, Christina Harris, Georgina Johnson, Heather Faulkner, Toni Gordon, Arnaldo Villafranca, Ciro Vasquez, Samvid Owivedi, Shawn Simmons, Andy Paluch, Matt Dumouchel, Crystal Bernarducci, Shalane Ponsell, Pauline Thai, Jessica Allen, Amanda Ditson, Hamid Hoveida, Caitlyn Palmby, Carl Franconi, Craig Beatty and Dianne Harshberger for help in sorting pitfall samples and leaf litter. Ben Duval, Paul Dijkstra and Rick Doucett helped with the nitrogen analyses. We acknowledge the support and encouragement of the NASA Kennedy Space Center and Dynamac Corporation, especially Ross Hinkle. Dave Johnson, Hans Anderson, Tom Powell and Graham Hymus provided a happy working environment at the field site. NR 43 TC 5 Z9 5 U1 4 U2 84 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1469-8137 J9 NEW PHYTOL JI New Phytol. PD NOV PY 2013 VL 200 IS 3 BP 788 EP 795 DI 10.1111/nph.12295 PG 8 WC Plant Sciences SC Plant Sciences GA 233GI UT WOS:000325555400021 PM 23638943 ER PT J AU Touchon, JC Jimenez, RR Abinette, SH Vonesh, JR Warkentin, KM AF Touchon, Justin C. Jimenez, Randall R. Abinette, Shane H. Vonesh, James R. Warkentin, Karen M. TI Behavioral plasticity mitigates risk across environments and predators during anuran metamorphosis SO OECOLOGIA LA English DT Article DE Complex life cycle; Escape performance; Phenotypic plasticity; Predation; Trade-off ID RED-EYED TREEFROGS; EARLY POSTSETTLEMENT MORTALITY; COMPLEX LIFE-CYCLES; DIFFERENTIAL PREDATION; RANA-SYLVATICA; TADPOLE SIZE; BUFO-BOREAS; REEF FISHES; TRADE-OFFS; WATER BUG AB Most animals metamorphose, changing morphology, physiology, behavior and ecological interactions. Size- and habitat-dependent mortality risk is thought to affect the evolution and plastic expression of metamorphic timing, and high predation during the morphological transition is posited as a critical selective force shaping complex life cycles. Nonetheless, empirical data on how risk changes across metamorphosis and stage-specific habitats, or how that varies with size, are rare. We examined predator-prey interactions of red-eyed treefrogs, Agalychnis callidryas, with an aquatic predator (giant water bug, Belostoma) and a semi-terrestrial predator (fishing spider, Thaumasia) across metamorphosis. We manipulated tadpole density to generate variation in metamorph size and conducted predation trials at multiple developmental stages. We quantified how frog behavior (activity) changes across metamorphic development, habitats, and predator presence or absence. In aquatic trials with water bugs, frog mortality increased with forelimb emergence, as hypothesized. In semi-terrestrial trials, contrary to predictions, predation by spiders increased, not decreased, with tail resorption. In neither case did frog size affect mortality. Frogs reduced activity upon forelimb emergence in the water, and further with emergence into air, then increased activity with tail resorption. Longer-tailed metamorphs were captured more often in spider attacks, but attacked less, as most attacks followed prey movements. Metamorphs behaviorally compensated for poor escape performance more effectively on land than in water, thus emergence timing may critically affect mortality. The developmental timing of the ecological transition between environments that select for different larval and juvenile phenotypes is an important, neglected variable in studies of complex life cycles. C1 [Touchon, Justin C.; Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Touchon, Justin C.; Warkentin, Karen M.] Smithsonian Trop Res Inst, Panama City, Panama. [Jimenez, Randall R.] Univ Nacl, Dept Biol Trop, Heredia 40101, Costa Rica. [Abinette, Shane H.; Vonesh, James R.] Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. RP Warkentin, KM (reprint author), Boston Univ, Dept Biol, 5 Cummington Mall, Boston, MA 02215 USA. EM kwarken@bu.edu RI Vonesh, James/I-1573-2013 OI Vonesh, James/0000-0003-2481-9988 FU US National Science Foundation [DEB-0716923, DEB-0717220]; Boston University; Virginia Commonwealth University; Smithsonian Tropical Research Institute FX We thank the Smithsonian Tropical Research Institute for use of their facilities and logistical support and the Autoridad Nacional del Ambiente de Panama for permission to conduct this research (SE/A-32-09, SE/A-73-09, SC/A-13-11). We thank T. Landberg for assistance and M. Hughey and R. Wassersug for comments on the manuscript. This research was funded by the US National Science Foundation (DEB-0716923 to K. M. W. and DEB-0717220 to J.R.V.), Boston University, Virginia Commonwealth University, and the Smithsonian Tropical Research Institute. NR 66 TC 10 Z9 10 U1 4 U2 60 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 NOV PY 2013 VL 173 IS 3 BP 801 EP 811 DI 10.1007/s00442-013-2714-8 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 236SO UT WOS:000325819700016 PM 23824140 ER PT J AU Feller, IC Chamberlain, AH Piou, C Chapman, S Lovelock, CE AF Feller, Ilka C. Chamberlain, Anne H. Piou, Cyril Chapman, Samantha Lovelock, Catherine E. TI Latitudinal Patterns of Herbivory in Mangrove Forests: Consequences of Nutrient Over-Enrichment SO ECOSYSTEMS LA English DT Article DE Aratus pisonii; Ecdytolopha; herbivory; loss of yield; mangrove; Marmara; nitrogen; phosphorus; Rhizophora mangle; latitude; nutrient enrichment ID CRAB ARATUS-PISONII; RHIZOPHORA-MANGLE; GLOBAL PATTERNS; SALT MARSHES; ECOSYSTEMS; NITROGEN; GROWTH; GRADIENT; DAMAGE; LIMITATION AB Ecosystems in the tropics are predicted to have stronger responses to nutrient enrichment, greater diversity, and more intense biotic interactions than in temperate areas. Mangrove forests, which occur across a broad biogeographic range from warm temperate to tropical, provide a unique opportunity to test these hypotheses by investigating the responses of herbivores to nutrient enrichment in temperate versus tropical latitudes. Mangroves are complex intertidal ecosystems with spatial differences in structure and diversity along tidal gradients and are threatened globally by human activities including nutrient over-enrichment. In this study, we used long-term fertilization experiments at the Indian River Lagoon, FL; Twin Cays, Belize; and Bocas del Toro, Panama to determine how increased nutrients impact herbivore abundance and herbivory of Rhizophora mangle at the tree, forest, and regional scales. At these locations, which span approximately 2185 km and 18.4A(0) of latitude, we fertilized individual trees with one of three treatments (Control, +N, +P) in two zones (fringe, scrub) along transects perpendicular to the shoreline and measured their responses for 4 years. Herbivory was measured as folivory, loss of yield, and tissue mining. Although nutrient enrichment altered plant growth, leaf traits, and nutrient dynamics, these variables had little effect on folivory at any location. Our results did not support the prediction that herbivory and per capita consumption are greatest at the most tropical location. Instead, folivory was highest at the most temperate location and lowest at the intermediate location. Folivory was generally higher in the fringe than in the scrub zone, but the pattern varied by location, herbivore, and nutrient treatment. Folivory by a dominant herbivore, Aratus pisonii, decreased from the highest to the lowest latitude. Our data suggest that factors controlling population dynamics of A. pisonii cascade to the mangrove canopy, linking herbivory to crab densities. C1 [Feller, Ilka C.; Chamberlain, Anne H.; Chapman, Samantha; Lovelock, Catherine E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Piou, Cyril] French Agr Res Ctr Int Dev CIRAD, UPR Bioagresseurs Anal & Maitrise Risque, F-34398 Montpellier, France. [Chapman, Samantha] Villanova Univ, Dept Biol, Villanova, PA 19085 USA. [Lovelock, Catherine E.] Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia. RP Feller, IC (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM felleri@si.edu RI Lovelock, Catherine/G-7370-2012; OI Lovelock, Catherine/0000-0002-2219-6855; Feller, Ilka/0000-0002-6391-1608 FU Smithsonian Marine Science Network; National Science Foundation [DEB9981535, EF1065821]; Australian Research Council [DP0879354, DP0986179] FX We thank the Smithsonian Marine Science Network for funding and the staffs of the Smithsonian Marine Station in Fort Pierce (SMS), the Smithsonian Marine Field Station in Belize (CCRE), and the Smithsonian Marine Laboratory in Bocas del Toro, Panama for logistical and field support. This material is based upon work supported by the National Science Foundation (DEB9981535, EF1065821) and the Australian Research Council (DP0879354 and DP0986179). We also thank the governments of Belize and Panama for permission to use study sites at Twin Cays and Bocas del Toro. This is CCRE Contribution No. 936 and SMS Contribution No. 906. NR 49 TC 7 Z9 7 U1 4 U2 101 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1432-9840 EI 1435-0629 J9 ECOSYSTEMS JI Ecosystems PD NOV PY 2013 VL 16 IS 7 BP 1203 EP 1215 DI 10.1007/s10021-013-9678-8 PG 13 WC Ecology SC Environmental Sciences & Ecology GA 231NT UT WOS:000325424500004 ER PT J AU Shik, JZ Donoso, DA Kaspari, M AF Shik, Jonathan Z. Donoso, David A. Kaspari, Michael TI The life history continuum hypothesis links traits of male ants with life outside the nest SO ENTOMOLOGIA EXPERIMENTALIS ET APPLICATA LA English DT Review DE Formicidae; sexual selection; pre-mating trait; scaling; Hymenoptera; male aggregation; female calling syndrome ID WESTERN HARVESTER ANT; HYMENOPTERA-FORMICIDAE; SOLENOPSIS-INVICTA; FIRE ANT; SOCIAL INSECTS; SPERM TRANSFER; POGONOMYRMEX-OCCIDENTALIS; REPRODUCTIVE-SYSTEM; GENETIC DIVERSITY; SEXUAL SELECTION AB An ant society, headed by a mated queen, can live for decades. Male ants, in contrast, are generally assumed to be ephemeral sperm delivery vessels programmed to die hours after leaving the nest to mate. However, the events from dispersal to mate location have rarely been studied, and the links between male traits and the ecological demands of diverse mating systems remain poorly understood. Here, we propose that interspecific variation in the length of mating flights has generated a life history continuum for male ants, and that the previously proposed male aggregating' and female calling' mating syndromes represent the endpoints. We also provide the first evidence for systematic divergence in pre-mating traits between males that attract females to brief nuptial swarms (Male aggregation syndrome) and those that must survive while searching for patchily distributed females that signal with pheromones (Female calling syndrome). Specifically, female-calling males tend to have larger eyes and mandibles, but the length of the basal antennal segment (scape) appears relatively constant across body sizes. After exploring these patterns, we review evidence that key components of fitness like mating frequency vary across a male life history continuum, and then explore links between male traits and a colony's per capita reproductive investment. Systematic variation in pre-flight provisioning of males relative to mating systems may have important ecological implications, given that ants are dominant consumers on a global scale, and colonies ultimately use large fractions of harvested resources to fuel reproduction. C1 [Shik, Jonathan Z.] N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. [Shik, Jonathan Z.; Kaspari, Michael] Smithsonian Trop Res Inst, Ancon 084303092, Panama. [Donoso, David A.] Univ Tecn Particular Loja, Dept Ciencias Nat, Loja 1101608, Ecuador. [Kaspari, Michael] Univ Oklahoma, Grad Program Ecol & Evolutionary Biol, Norman, OK 73019 USA. [Kaspari, Michael] Univ Oklahoma, Dept Zool, Norman, OK 73019 USA. RP Shik, JZ (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM jonathan.shik@gmail.com RI Donoso, David/A-2059-2016; OI Donoso, David/0000-0002-3408-1457; Kaspari, Michael/0000-0002-9717-5768 FU National Science Foundation [DEB 0842038] FX This study was supported by a grant from the National Science Foundation DEB 0842038. We thank antweb.org for use of images, J. Lattke for supplying male trait data, and R. Reisch and M. Sorger for help translating papers from German. J.J. Boomsma provided valuable comments on an earlier draft. We thank C. Peeters and an anonymous reviewer for helpful suggestions. NR 102 TC 10 Z9 10 U1 2 U2 24 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0013-8703 EI 1570-7458 J9 ENTOMOL EXP APPL JI Entomol. Exp. Appl. PD NOV PY 2013 VL 149 IS 2 BP 99 EP 109 DI 10.1111/eea.12117 PG 11 WC Entomology SC Entomology GA 230QD UT WOS:000325356200001 ER PT J AU Erickson, JE Peresta, G Montovan, KJ Drake, BG AF Erickson, John E. Peresta, Gary Montovan, Kathryn J. Drake, Bert G. TI Direct and indirect effects of elevated atmospheric CO2 on net ecosystem production in a Chesapeake Bay tidal wetland SO GLOBAL CHANGE BIOLOGY LA English DT Article DE carbon storage; ecosystem respiration; elevated CO2; net ecosystem CO2 exchange; nitrogen; photosynthesis; tidal wetlands ID SCRUB-OAK ECOSYSTEM; LONG-TERM EXPOSURE; OPEN-TOP CHAMBER; CARBON-DIOXIDE; ENVIRONMENTAL CONTROLS; SEASONAL-VARIATION; TALLGRASS PRAIRIE; DARK RESPIRATION; DECIDUOUS FOREST; EDDY COVARIANCE AB The rapid increase in atmospheric CO2 concentrations (C-a) has resulted in extensive research efforts to understand its impact on terrestrial ecosystems, especially carbon balance. Despite these efforts, there are relatively few data comparing net ecosystem exchange of CO2 between the atmosphere and the biosphere (NEE), under both ambient and elevated C-a. Here we report data on annual sums of CO2 (NEEnet) for 19years on a Chesapeake Bay tidal wetland for Scirpus olneyi (C-3 photosynthetic pathway)- and Spartina patens (C-4 photosynthetic pathway)-dominated high marsh communities exposed to ambient and elevated C-a (ambient+340ppm). Our objectives were to (i) quantify effects of elevated C-a on seasonally integrated CO2 assimilation (NEEnet = NEEday + NEEnight, kgCm(-2)y(-1)) for the two communities; and (ii) quantify effects of altered canopy N content on ecosystem photosynthesis and respiration. Across all years, NEEnet averaged 1.9kgm(-2)y(-1) in ambient C-a and 2.5kgm(-2)y(-1) in elevated C-a, for the C-3-dominated community. Similarly, elevated C-a significantly (P<0.01) increased carbon uptake in the C-4-dominated community, as NEEnet averaged 1.5kgm(-2)y(-1) in ambient C-a and 1.7kgm(-2)y(-1) in elevated C-a. This resulted in an average CO2 stimulation of 32% and 13% of seasonally integrated NEEnet for the C-3- and C-4-dominated communities, respectively. Increased NEEday was correlated with increased efficiencies of light and nitrogen use for net carbon assimilation under elevated C-a, while decreased NEEnight was associated with lower canopy nitrogen content. These results suggest that rising C-a may increase carbon assimilation in both C-3- and C-4-dominated wetland communities. The challenge remains to identify the fate of the assimilated carbon. C1 [Erickson, John E.; Peresta, Gary; Drake, Bert G.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Erickson, John E.; Montovan, Kathryn J.] Univ Florida, Dept Agron, Gainesville, FL 32611 USA. [Montovan, Kathryn J.] Bennington Coll, Bennington, VT 05201 USA. RP Drake, BG (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM drakeb@si.edu FU United States Department of Energy [DE-FG02-97ER62458]; Smithsonian Institution FX The authors acknowledge Francois Delage, Michelle Berger, and Melanie Muehe for their contributions to data analysis and to three anonymous reviewers for critical comments on an earlier version of the paper. This project was funded by the United States Department of Energy (DE-FG02-97ER62458) and supported by the Smithsonian Institution. NR 61 TC 6 Z9 6 U1 4 U2 64 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD NOV PY 2013 VL 19 IS 11 BP 3368 EP 3378 DI 10.1111/gcb.12316 PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 233KL UT WOS:000325567100012 PM 23828758 ER PT J AU Jesovnik, A Sosa-Calvo, J Lopes, CT Vasconcelos, HL Schultz, TR AF Jesovnik, A. Sosa-Calvo, J. Lopes, C. T. Vasconcelos, H. L. Schultz, T. R. TI Nest architecture, fungus gardens, queen, males and larvae of the fungus-growing ant Mycetagroicus inflatus Brando & Mayh-Nunes SO INSECTES SOCIAUX LA English DT Article DE Mycetagroicus inflatus; Ants; Attini; Fungus-growing ants; Symbiont fidelity; Nest architecture ID FORMICIDAE MYRMICINAE ATTINI; LEAF-CUTTING ANTS; HYMENOPTERA-FORMICIDAE; PHYLOGENETIC ANALYSIS; EVOLUTION; SYMBIOSIS; BEHAVIOR; GENUS; EMERY; AGRICULTURE AB All known fungus-growing ants (tribe Attini) are obligately symbiotic with their cultivated fungi. The fungal cultivars of "lower" attine ants are facultative symbionts, capable of living apart from ants, whereas the fungal cultivars of "higher" attine ants, including leaf-cutting genera Atta and Acromyrmex, are highly specialized, obligate symbionts. Since higher attine ants and fungi are derived from lower attine ants and fungi, understanding the evolutionary transition from lower to higher attine agriculture requires understanding the historical sequence of change in both ants and fungi. The biology of the poorly known ant genus Mycetagroicus is of special interest in this regard because it occupies a phylogenetic position intermediate between lower and higher ant agriculture. Here, based on the excavations of four nests in Para, Brazil, we report the first biological data for the recently described species Mycetagroicus inflatus, including the first descriptions of Mycetagroicus males and larvae. Like M. cerradensis, the only other species in the genus for which nesting biology is known, the garden chambers of M. inflatus are unusually deep and the garden is most likely relocated vertically in rainy and dry seasons. Due to the proximity of nests to the Araguaia River, it is likely that even the uppermost chambers and nest entrances of M. inflatus are submerged during the rainy season. Most remarkably, all three examined colonies of M. inflatus cultivate the same fungal species as their congener, M. cerradensis, over 1,000 km away, raising the possibility of long-term symbiont fidelity spanning speciation events within the genus. C1 [Jesovnik, A.; Sosa-Calvo, J.] Univ Maryland, Dept Entomol, Maryland Ctr Systemat Entomol, College Pk, MD 20742 USA. [Jesovnik, A.; Sosa-Calvo, J.; Schultz, T. R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Lopes, C. T.; Vasconcelos, H. L.] Univ Fed Uberlandia, Inst Biol, BR-38400902 Uberlandia, MG, Brazil. RP Jesovnik, A (reprint author), Univ Maryland, Dept Entomol, Maryland Ctr Systemat Entomol, 4112 Plant Sci Bldg, College Pk, MD 20742 USA. EM jesovnika@si.edu; schultzt@si.edu FU Brazilian Council of Research and Scientific Development [CNPq 001884/2012-3]; NSF [DEB 0949689]; TRS by a Smithsonian Institution National Museum of Natural History Small Grant Award; NMNH FX We thank the Brazilian Council of Research and Scientific Development for granting permission to conduct this research in Brazil (Processo CNPq 001884/2012-3). We also thank the Instituto Chico Mendes de Conservacao da Biodiversidade (ICMBio) for issuing collecting permit number 14789-6. We are grateful to the discoverers of Mycetagroicus inflatus, Rodrigo Feitosa and Rogerio Rosa da Silva, for their help and advice, which were essential to relocating nests of M. inflatus on the banks of the Araguaia River. We are grateful to two anonymous reviewers for greatly improving the manuscript. Thanks to Eliana Buenaventura (University of Copenhagen) for identifying the milichiid fly, to Michael Lloyd for molecular bench work, and to Eugenia Okonski for specimen preparation. Travel expenses for AJ were partly supported by an Explorers Club Washington Group Exploration and Field Research Grant awarded in 2012. TRS, AJ, and JSC were supported by NSF DEB 0949689 and TRS by a Smithsonian Institution National Museum of Natural History Small Grant Award. JSC was additionally supported by a NMNH Peter S. Buck graduate fellowship. NR 66 TC 1 Z9 1 U1 1 U2 45 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 EI 1420-9098 J9 INSECT SOC JI Insect. Soc. PD NOV PY 2013 VL 60 IS 4 BP 531 EP 542 DI 10.1007/s00040-013-0320-8 PG 12 WC Entomology SC Entomology GA 235HG UT WOS:000325707200013 ER PT J AU Crawford, AJ Cruz, C Griffith, E Ross, H Ibanez, R Lips, KR Driskell, AC Bermingham, E Crump, P AF Crawford, Andrew J. Cruz, Catalina Griffith, Edgardo Ross, Heidi Ibanez, Roberto Lips, Karen R. Driskell, Amy C. Bermingham, Eldredge Crump, Paul TI DNA barcoding applied to ex situ tropical amphibian conservation programme reveals cryptic diversity in captive populations SO MOLECULAR ECOLOGY RESOURCES LA English DT Review DE amphibian decline; cryptic species diversity; DNA barcode of life; ex situ conservation; species delimitation ID ELEUTHERODACTYLUS-RUGULOSUS GROUP; MITOCHONDRIAL-DNA; SPECIES DELIMITATION; INTEGRATIVE TAXONOMY; MAXIMUM-LIKELIHOOD; CENTRAL PANAMA; ANURA-LEPTODACTYLIDAE; CENTRAL-AMERICA; FROGS; DECLINES AB Amphibians constitute a diverse yet still incompletely characterized clade of vertebrates, in which new species are still being discovered and described at a high rate. Amphibians are also increasingly endangered, due in part to disease-driven threats of extinctions. As an emergency response, conservationists have begun ex situ assurance colonies for priority species. The abundance of cryptic amphibian diversity, however, may cause problems for ex situ conservation. In this study we used a DNA barcoding approach to survey mitochondrial DNA (mtDNA) variation in captive populations of 10 species of Neotropical amphibians maintained in an ex situ assurance programme at El Valle Amphibian Conservation Center (EVACC) in the Republic of Panama. We combined these mtDNA sequences with genetic data from presumably conspecific wild populations sampled from across Panama, and applied genetic distance-based and character-based analyses to identify cryptic lineages. We found that three of ten species harboured substantial cryptic genetic diversity within EVACC, and an additional three species harboured cryptic diversity among wild populations, but not in captivity. Ex situ conservation efforts focused on amphibians are therefore vulnerable to an incomplete taxonomy leading to misidentification among cryptic species. DNA barcoding may therefore provide a simple, standardized protocol to identify cryptic diversity readily applicable to any amphibian community. C1 [Crawford, Andrew J.; Ibanez, Roberto; Lips, Karen R.; Bermingham, Eldredge] Smithsonian Trop Res Inst, Panama City, Panama. [Crawford, Andrew J.; Ibanez, Roberto] Circulo Herpetol Panama, Panama City, Panama. [Crawford, Andrew J.; Cruz, Catalina] Univ Los Andes, Dept Ciencias Biol, Bogota 4976, Colombia. [Griffith, Edgardo; Ross, Heidi] El Valle Amphibian Conservat Ctr, Cocle, Panama. [Lips, Karen R.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Driskell, Amy C.] Smithsonian Inst, Labs Analyt Biol, Suitland, MD 20746 USA. [Crump, Paul] Houston Zoo, Dept Conservat & Sci, Houston, TX 77030 USA. RP Crawford, AJ (reprint author), Univ Los Andes, Dept Ciencias Biol, Inst Genet, Edif M1-304,Carrera 1E 18A-10, Bogota 4976, Colombia. EM andrew@dna.ac OI Crawford, Andrew J./0000-0003-3153-6898; Lips, Karen/0000-0002-2719-1551 FU Houston Zoo, the PARC project; Association of Zoos and Aquariums (AZA) Conservation Endowment Fund; National Geographic Committee for Research and Exploration grant; Bay and Paul Foundation FX EVACC was supported by the Houston Zoo, the PARC project partners, and numerous other institutions. Fieldwork was supported by an Association of Zoos and Aquariums (AZA) Conservation Endowment Fund grant to EVACC and a National Geographic Committee for Research and Exploration grant to AJC, KRL and RI. Analysis of EVACC samples was supported by a grant from the Bay and Paul Foundation to PC, with laboratory assistance from Sandra Flechas, Marta Vargas and Maribel Gonzalez. Wild-caught specimens were analysed at the LAB with the help of Andrea Ormos. Figure 1 was created by Lucas Barrientos. We would like to thank Editor Tim Vines for inviting us to submit this contribution. NR 119 TC 22 Z9 22 U1 7 U2 77 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 NOV PY 2013 VL 13 IS 6 SI SI BP 1005 EP 1018 DI 10.1111/1755-0998.12054 PG 14 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 234FN UT WOS:000325627700005 PM 23280343 ER PT J AU Kipping, DM AF Kipping, David M. TI Efficient, uninformative sampling of limb darkening coefficients for two-parameter laws SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: analytical; stars: atmospheres ID HUBBLE-SPACE-TELESCOPE; PROPER MOTION; PLANET; STARS; PHOTOMETRY; TRANSITS; EXOMOONS; PROJECT; BINARY; MODELS AB Stellar limb darkening affects a wide range of astronomical measurements and is frequently modelled with a parametric model using polynomials in the cosine of the angle between the line of sight and the emergent intensity. Two-parameter laws are particularly popular for cases where one wishes to fit freely for the limb darkening coefficients (i.e. an uninformative prior) due to the compact prior volume and the fact that more complex models rarely obtain unique solutions with the present data. In such cases, we show that the two limb darkening coefficients are constrained by three physical boundary conditions, describing a triangular region in the two-dimensional parameter space. We show that uniformly distributed samples may be drawn from this region with optimal efficiency by a technique developed by computer graphical programming: triangular sampling. Alternatively, one can make draws using a uniform, bivariate Dirichlet distribution. We provide simple expressions for these parametrizations for both techniques applied to the case of quadratic, square-root and logarithmic limb darkening laws. For example, in the case of the popular quadratic law, we advocate fitting for q(1) = (u(1) + u(2))(2) and q(2) = 0.5u(1)(u(1) + u(2))(-1) with uniform priors in the interval [0, 1] to implement triangular sampling easily. Employing these parametrizations allows one to derive model parameters which fully account for our ignorance about the intensity profile, yet never explore unphysical solutions, yielding robust and realistic uncertainty estimates. Furthermore, in the case of triangular sampling with the quadratic law, our parametrization leads to significantly reduced mutual correlations and provides an alternative geometric explanation as to why naively fitting the quadratic limb darkening coefficients precipitates strong correlations in the first place. 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 Carl Sagan Fellowships FX DMK has been supported by the NASA Carl Sagan Fellowships. Thanks to J. Irwin for useful discussions and comments in preparing this manuscript. Special thanks to the anonymous reviewer for his/her positive and constructive feedback. NR 36 TC 50 Z9 50 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 NOV PY 2013 VL 435 IS 3 BP 2152 EP 2160 DI 10.1093/mnras/stt1435 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236DA UT WOS:000325773000026 ER PT J AU Mashian, N Sternberg, A Loeb, A AF Mashian, Natalie Sternberg, Amiel Loeb, Abraham TI The ratio of CO to total gas mass in high-redshift galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: high-redshift; galaxies: ISM; galaxies: luminosity function; mass function; cosmology: theory ID STAR-FORMING GALAXIES; GALACTIC GAMMA-RAYS; HUBBLE DEEP FIELD; MOLECULAR GAS; RADIAL-DISTRIBUTION; EXCITATION; CLOUDS; H-2; LUMINOSITY; COLLISIONS AB Walter et al. have recently identified the J = 6 - 5, 5 - 4, and 2 - 1 CO rotational emission lines, and [C ii] fine-structure emission line from the star-forming interstellar medium (ISM) in the high-redshift submillimetre source HDF 850.1, at z = 5.183. We employ large velocity gradient (LVG) modelling to analyse the spectra of this source assuming the [C ii] and CO emissions originate from (i) separate virialized regions, (ii) separate unvirialized regions, (iii) uniformly mixed virialized regions and (iv) uniformly mixed unvirialized regions. We present the best-fitting set of parameters, including for each case the ratio alpha between the total hydrogen/helium gas mass and the CO(1-0) line luminosity. We also present computations of the ratio of H-2 mass to [C ii] line luminosity for optically thin conditions, for a range of gas temperatures and densities, for direct conversion of [C ii] line luminosities to 'CO-dark' H-2 masses. For HDF 850.1 we find that a model in which the CO and C+ are uniformly mixed in gas that is shielded from ultraviolet radiation requires a cosmic ray or X-ray ionization rate of zeta approximate to 3 x 10(-14) s(-1), plausibly consistent with the large star formation rate (similar to 10(3) M-circle dot yr(-1)) observed in this source. Enforcing the cosmological constraint posed by the abundance of dark matter haloes in the standard Lambda cold dark matter (Lambda CDM) cosmology and taking into account other possible contributions to the total gas mass, we find that the two models in which the virialization condition is enforced can be ruled out at the greater than or similar to 2 Sigma level, while the model assuming mixed unvirialized regions is less likely. We conclude that modelling HDF 850.1's ISM as a collection of unvirialized molecular clouds with distinct CO and C+ layers, for which alpha = 1.2 M-circle dot (K km s(-1) pc(2))(-1) for the CO to H-2 mass-to-luminosity ratio (similar to the standard ultraluminous infrared galaxy value), is most consistent with the Lambda CDM cosmology. C1 [Mashian, Natalie; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mashian, Natalie; Sternberg, Amiel; Loeb, Abraham] Tel Aviv Univ, Raymond & Beverly Sackler Sch Phys & Astron, IL-69978 Tel Aviv, Israel. RP Mashian, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nmashian@physics.harvard.edu; amiel@astro.tau.ac.il; aloeb@cfa.harvard.edu FU Raymond and Beverly Sackler Tel Aviv University-Harvard/ITC Astronomy Program; Sackler Professorship by Special Appointment at Tel Aviv University; NSF [AST-0907890]; NASA [NNX08AL496, NNA09DB30A] FX We thank Dean Mark for his assistance with the LVG computations. This work was supported by the Raymond and Beverly Sackler Tel Aviv University-Harvard/ITC Astronomy Program. AL acknowledges support from the Sackler Professorship by Special Appointment at Tel Aviv University. This work was also supported in part by NSF grant AST-0907890 and NASA grants NNX08AL496 and NNA09DB30A (for AL). NR 41 TC 7 Z9 7 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 NOV PY 2013 VL 435 IS 3 BP 2407 EP 2415 DI 10.1093/mnras/stt1449 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236DA UT WOS:000325773000044 ER PT J AU Ghirlanda, G Salvaterra, R Burlon, D Campana, S Melandri, A Bernardini, MG Covino, S D'Avanzo, P D'Elia, V Ghisellini, G Nava, L Prandoni, I Sironi, L Tagliaferri, G Vergani, SD Wolter, A AF Ghirlanda, G. Salvaterra, R. Burlon, D. Campana, S. Melandri, A. Bernardini, M. G. Covino, S. D'Avanzo, P. D'Elia, V. Ghisellini, G. Nava, L. Prandoni, I. Sironi, L. Tagliaferri, G. Vergani, S. D. Wolter, A. TI Radio afterglows of a complete sample of bright Swift GRBs: predictions from present days to the SKA era SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: non thermal; radio continuum: general ID GAMMA-RAY BURST; SPECTRAL-ENERGY CORRELATIONS; REVERSE SHOCKS; LIGHT CURVES; POPULATION; EVOLUTION; JET; GRB-030329; POLARIZATION; SIMULATIONS AB Radio observations of Gamma-Ray Bursts (GRBs) afterglows are fundamental in providing insights into their physics and environment, and in constraining the true energetics of these sources. Nonetheless, radio observations of GRB afterglows are presently sparse in the time/frequency domain. Starting from a complete sample of 58 bright Swift long bursts (BAT6), we constructed a homogeneous sub-sample of 38 radio detections/upper limits which preserves all the properties of the parent sample. One half of the bursts have detections between 1 and 5 d after the explosion with typical fluxes F greater than or similar to 100 mu Jy at 8.4 GHz. Through a Population SYnthesis Code coupled with the standard afterglow Hydrodynamical Emission model, we reproduce the radio flux distribution of the radio sub-sample. Based on these results, we study the detectability in the time/frequency domain of the entire long GRB population by present and future radio facilities. We find that the GRBs that typically trigger Swift can be detected at 8.4 GHz by Jansky Very Large Array within few days with modest exposures even at high redshifts. The final Square Kilometre Array (SKA) can potentially observe the whole GRB population provided that there will be a dedicated GRB gamma-ray detector more sensitive than Swift. For a sizeable fraction (50 per cent) of these bursts, SKA will allow us to perform radio calorimetry, after the trans-relativistic transition (occurring similar to 100 d), providing an estimate of the true (collimation corrected) energetics of GRBs. C1 [Ghirlanda, G.; Campana, S.; Melandri, A.; Bernardini, M. G.; Covino, S.; D'Avanzo, P.; Ghisellini, G.; Nava, L.; Tagliaferri, G.; Vergani, S. D.; Wolter, A.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Salvaterra, R.] INAF IASF Milano, I-20133 Milan, Italy. [Burlon, D.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Burlon, D.] Univ Sydney, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2006, Australia. [D'Elia, V.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [D'Elia, V.] INAF OAR, I-00040 Monte Porzio Catone, Italy. [Nava, L.] APC Univ Paris Diderot, F-75205 Paris 13, France. [Prandoni, I.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Sironi, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vergani, S. D.] Univ Paris Diderot, Observ Paris, CNRS, GEPI, F-92190 Meudon, France. RP Ghirlanda, G (reprint author), INAF Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy. EM giancarlo.ghirlanda@brera.inaf.it OI Tagliaferri, Gianpiero/0000-0003-0121-0723; Ghirlanda, Giancarlo/0000-0001-5876-9259; Prandoni, Isabella/0000-0001-9680-7092; Wolter, Anna/0000-0001-5840-9835; Campana, Sergio/0000-0001-6278-1576; D'Elia, Valerio/0000-0002-7320-5862; Ghisellini, Gabriele/0000-0002-0037-1974; Salvaterra, Ruben/0000-0002-9393-8078; Covino, Stefano/0000-0001-9078-5507 FU ASI [I/004/11/0]; PRIN-INAF grant; NASA [NNX10AF62G]; NSF [AST-1009863] FX We acknowledge D. Frail and P. Chandra for having provided the radio fluxes of two bursts. We thank P. Hancock for discussion. ASI I/004/11/0 and the 2011 PRIN-INAF grant are acknowledged for financial support. Development of the BOXFIT code (van Eerten et al. 2012) was supported in part by NASA through grant NNX10AF62G issued through the Astrophysics Theory Programme and by the NSF through grant AST-1009863. We acknowledge the anonymous referee for comments. NR 100 TC 13 Z9 13 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 NOV PY 2013 VL 435 IS 3 BP 2543 EP 2551 DI 10.1093/mnras/stt1466 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236DA UT WOS:000325773000055 ER PT J AU Knee, KL Jordan, TE AF Knee, Karen L. Jordan, Thomas E. TI Spatial Distribution of Dissolved Radon in the Choptank River and Its Tributaries: Implications for Groundwater Discharge and Nitrate Inputs SO ESTUARIES AND COASTS LA English DT Article DE Groundwater discharge; Radon; Choptank River; Chesapeake Bay; Nitrate ID CHESAPEAKE BAY; COASTAL-PLAIN; CONTINUOUS MONITOR; ORGANIC NITROGEN; SCALE ASSESSMENT; NUTRIENT INPUTS; SURFACE-WATER; RN-222; ESTUARY; OCEAN AB The Choptank River, Chesapeake Bay's largest eastern-shore tributary, is experiencing increasing nutrient loading and eutrophication. Productivity in the Choptank is predominantly nitrogen-limited, and most nitrogen inputs occur via discharge of high-nitrate groundwater into the river system's surface waters. However, spatial patterns in the magnitude and quality of groundwater discharge are not well understood. In this study, we surveyed the activity of Rn-222, a natural groundwater tracer, in the Choptank's main tidal channel, the large tidal tributary Tuckahoe Creek, smaller tidal and non-tidal tributaries around the basin, and groundwater discharging into those tributaries, measuring nitrate and salinity concurrently. Rn-222 activities were < 100 Bq m(-3) in the main tidal channel and 100-700 Bq m(-3) in the upper Choptank River and Tuckahoe Creek, while the median Rn activities of fresh tributaries and discharging groundwater were 1,000 and 7,000 Bq m(-3), respectively. Nitrate-N concentrations were < 0.01 mg L-1 throughout most of the tidal channel, 1.5-3 mg L-1 in the upper reaches, up to 13 mg L-1 in tributary samples, and up to 19.6 mg L-1 in groundwater. Nitrate concentrations in tributary surface water were correlated with Rn activity in three of five sub-watersheds, indicating a groundwater nitrate source. Rn-222 and salinity mass balances indicated that Rn-enriched groundwater discharges directly into the Choptank's tidal waters and suggested that it consists of a mixture of fresh groundwater and brackish re-circulated estuarine water. Further sampling is necessary to constrain the Rn activity and nitrate concentration of discharging groundwater and quantify direct discharge and associated nitrogen inputs. C1 [Knee, Karen L.] American Univ, Dept Environm Sci, Washington, DC 20016 USA. [Knee, Karen L.; Jordan, Thomas E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Knee, KL (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM knee@american.edu FU Smithsonian Institution Postdoctoral Fellowship; National Science Foundation [DEB-0919181, DEB-0919141] FX We thank Adina Paytan and Rick Peterson for the use of their RAD7 radon detectors and for advice about carrying out the study. Micah Ryder helped obtain and analyze geographic data, and David Culver generously provided access to GIS software. Dana Brenner, Nancy Goff, Christina Hill, Ryan Ihnacik, Alanna Lecher, Ginny Leviton, Joe Miklas, and Amelia Snyder assisted with sample collection and analysis. Rick Peterson, Thomas Fisher, and two anonymous reviewers provided comments that improved the quality of this manuscript. Financial support for this research came from a Smithsonian Institution Postdoctoral Fellowship (to K. Knee) and National Science Foundation grants (DEB-0919181 and DEB-0919141 to T. Jordan and T. Fisher). NR 61 TC 3 Z9 3 U1 0 U2 22 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 J9 ESTUAR COAST JI Estuaries Coasts PD NOV PY 2013 VL 36 IS 6 BP 1237 EP 1252 DI 10.1007/s12237-013-9619-y PG 16 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 227GP UT WOS:000325099900011 ER PT J AU Joyce, WG Werneburg, I Lyson, TR AF Joyce, Walter G. Werneburg, Ingmar Lyson, Tyler R. TI The hooked element in the pes of turtles (Testudines): a global approach to exploring primary and secondary homology SO JOURNAL OF ANATOMY LA English DT Article DE ansulate bone; chondrification; development; fossils; hooked fifth metatarsal; morphology; myology; ossification ID CHELYDRA-SERPENTINA REPTILIA; SKELETAL DEVELOPMENT; CARETTA-CARETTA; ALLIGATOR-MISSISSIPPIENSIS; INTRASPECIFIC VARIATION; PHYLOGENETIC POSITION; DEVELOPMENTAL BASIS; AMNIOTE PHYLOGENY; EARLY EVOLUTION; ORBITAL REGION AB The hooked element in the pes of turtles was historically identified by most palaeontologists and embryologists as a modified fifth metatarsal, and often used as evidence to unite turtles with other reptiles with a hooked element. Some recent embryological studies, however, revealed that this element might represent an enlarged fifth distal tarsal. We herein provide extensive new myological and developmental observations on the hooked element of turtles, and re-evaluate its primary and secondary homology using all available lines of evidence. Digital count and timing of development are uninformative. However, extensive myological, embryological and topological data are consistent with the hypothesis that the hooked element of turtles represents a fusion of the fifth distal tarsal with the fifth metatarsal, but that the fifth distal tarsal dominates the hooked element in pleurodiran turtles, whereas the fifth metatarsal dominates the hooked element of cryptodiran turtles. The term ansulate bone' is proposed to refer to hooked elements that result from the fusion of these two bones. The available phylogenetic and fossil data are currently insufficient to clarify the secondary homology of hooked elements within Reptilia. C1 [Joyce, Walter G.; Werneburg, Ingmar] Univ Tubingen, Dept Geosci, Tubingen, Germany. [Joyce, Walter G.] Univ Fribourg, Dept Geosci, CH-1700 Fribourg, Switzerland. [Werneburg, Ingmar] Univ Zurich, Palaontol Inst & Museum, Zurich, Switzerland. [Lyson, Tyler R.] Yale Univ, Dept Geol & Geophys, New Haven, CT USA. [Lyson, Tyler R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Joyce, WG (reprint author), Univ Fribourg, Dept Geosci, CH-1700 Fribourg, Switzerland. EM walter.joyce@unifr.ch OI Werneburg, Ingmar/0000-0003-1359-2036 FU DFG [JO 928/1-1]; JSPS [PE11027] FX The authors would cordially like to thank Marcelo R. Sanchez-Villagra for discussion, and for allowing us to study the serial section series and the skeletal preparations housed at his lab. The authors also thank Shigeru Kuratani for the access to his embryonic collection. For discussion, Erin E. Maxwell, Marton Rabi and Walter Salzburger are thanked. Four anonymous reviewers are thanked for providing insightful comments that significantly helped improve the quality of this manuscript. The study was supported by DFG grant JO 928/1-1 of WGJ and JSPS grant PE11027 to IW. NR 125 TC 5 Z9 5 U1 0 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8782 J9 J ANAT JI J. Anat. PD NOV PY 2013 VL 223 IS 5 BP 421 EP 441 DI 10.1111/joa.12103 PG 21 WC Anatomy & Morphology SC Anatomy & Morphology GA 232AK UT WOS:000325459700001 PM 24102560 ER PT J AU Burger, J Jehl, JR Gochfeld, M AF Burger, Joanna Jehl, Joseph R., Jr. Gochfeld, Michael TI Selenium:mercury molar ratio in eared grebes (Podiceps nigricollis) as a possible biomarker of exposure SO ECOLOGICAL INDICATORS LA English DT Article DE Selenium:mercury molar ratio; Biomarker; Brain; Liver; Muscle; Feathers; Grebe ID GREAT-SALT-LAKE; MERCURY TOXICITY; COMMON LOONS; METHYLMERCURY TOXICITY; KESTERSON RESERVOIR; HEAVY-METALS; FISH TISSUE; MIGRATION; DIETARY; HEALTH AB Mercury and selenium have adverse effects on health, and in the past their individual levels in tissues have been used as biomarkers of environmental contamination. These selenium:mercury molar ratios has been proposed as an alternative way to anticipate possible health risks to organisms. We examine selenium and mercury levels, their molar ratios, and variability in the ratios in the brain, liver, muscle, and feathers of a common waterbird, the eared grebe (Podiceps nigricollis), at several locations and phases of their annual cycle. We found: (1) Mean total mercury, for any site or tissue, ranged from 0.15 ppm in the brain to 29.2 ppm in breast feathers; (2) In any tissue, mean mercury levels varied by as much as 10-fold while selenium varied by 3-fold; (3) Mercury and selenium levels were correlated only in liver; (4) Selenium:mercury molar ratios varied significantly in regular patterns among tissues (less than 1 in feathers, up to 23 in brain), sites, and stages of annual cycle; (5) Molar ratios were affected by body weight (but not age), and the heaviest birds had the lowest ratios; and (6) Molar ratios varied more for brain than in other tissues. Low molar ratios are generally considered harmful, although no threshold ratio has been identified. Despite wide variation of molar ratios, field studies of eared grebes have not detected overt adverse effects. Before being adopted as a biomarkers, we suggest that selenium:mercury molar ratios be used in conjunction with studies of individual metal levels, and in accordance with detailed studies of selected species, to provide a baseline of variation in different organisms and tissues. (c) 2013 Elsevier Ltd. All rights reserved. C1 [Burger, Joanna] Rutgers State Univ, Div Life Sci, Piscataway, NJ 08855 USA. [Burger, Joanna; Gochfeld, Michael] Rutgers State Univ, Consortium Risk Evaluat Stakeholder Participat, Piscataway, NJ USA. [Burger, Joanna; Gochfeld, Michael] Rutgers State Univ, Environm & Occupat Hlth Sci Inst, Piscataway, NJ USA. [Jehl, Joseph R., Jr.] Smithsonian Inst, US Museum Nat Hist, Div Birds, Washington, DC 20560 USA. [Gochfeld, Michael] Robert Wood Johnson Med Sch, Environm & Occupat Med, Piscataway, NJ USA. RP Burger, J (reprint author), Rutgers State Univ, Div Life Sci, Piscataway, NJ 08855 USA. EM burger@biology.rutgers.edu FU NIEHS Center Grant [P30ES005022]; Consortium for Risk Evaluation with Stakeholder Participation (Department of Energy) [DE-FC01-06EW07053]; EOHSI FX We thank H. Ellis, J. Lutz, J. O'Neill, K. Day and the Utah Department of Wildlife Resources, for assistance in obtaining the grebe specimens. We particularly thank C. Jeitner, M. Donio and T. Pittfield for advice and logistical support throughout the study, and the many others who we have discussed mercury, selenium, and molar ratios with, including P. Copeland, J. Laskin, M. Lemire, K. Mahaffey, D. Mergler, N. Ralston, R. Schoeny, A. Stern, and H. Zarbl. The views and conclusions expressed in this paper are solely those of the authors, and do not reflect the funding agencies. This research was partly supported by the NIEHS Center Grant (P30ES005022), the Consortium for Risk Evaluation with Stakeholder Participation (Department of Energy, DE-FC01-06EW07053), and EOHSI. This research was conducted under a Rutgers University Animal Research Protocol. NR 80 TC 9 Z9 10 U1 6 U2 48 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1470-160X J9 ECOL INDIC JI Ecol. Indic. PD NOV PY 2013 VL 34 BP 60 EP 68 DI 10.1016/j.ecolind.2013.04.001 PG 9 WC Biodiversity Conservation; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 210UR UT WOS:000323860700008 ER PT J AU Seagle, CT Cottrell, E Fei, YW Hummer, DR Prakapenka, VB AF Seagle, Christopher T. Cottrell, Elizabeth Fei, Yingwei Hummer, Daniel R. Prakapenka, Vitali B. TI Electrical and thermal transport properties of iron and iron-silicon alloy at high pressure SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID DIAMOND-ANVIL CELL; CORE CONDITIONS; EARTHS CORE; RESISTIVITY; CONDUCTIVITY; TRANSITION; NICKEL; GPA; COMPRESSION; RESISTANCE AB The efficiency of heat transfer by conduction in the Earth's core controls the dynamics of convection and limits the power available for the geodynamo. We have measured the room temperature electrical resistivity of iron and iron-silicon alloy to 60 GPa and present a new model of the resistivity at high pressures and temperatures relevant to the Earth's core. The model is compared with available shock wave data and theoretical studies. For a power law and linear temperature dependence of electrical resistivity, the calculated thermal conductivity at the core-mantle boundary is similar to 67-145W/m/K for pure Fe and similar to 41-60 W/m/K for Fe-9wt % Si. Impurities in the core have a strong effect on the transport properties of iron that could significantly impact core thermal models. The models describing the data indicate higher thermal conductivity at core pressure than previously suggested, requiring additional energy sources in the past to operate the geodynamo. C1 [Seagle, Christopher T.; Cottrell, Elizabeth] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Seagle, Christopher T.; Fei, Yingwei; Hummer, Daniel R.] Carnegie Inst Sci, Geophys Lab, Washington, DC USA. [Prakapenka, Vitali B.] Univ Chicago, Ctr Adv Radiat Sources, Chicago, IL 60637 USA. RP Seagle, CT (reprint author), Sandia Natl Labs, POB 5800,MS 1189, Albuquerque, NM 87185 USA. EM ctseagl@sandia.gov RI Fei, Yingwei/F-3709-2011 OI Fei, Yingwei/0000-0001-9955-5353 FU National Science Foundation (Earth Sciences) [EAR-0622171]; Department of Energy (Geosciences) [DE-FG02-94ER14466]; State of Illinois; U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-06CH11357]; NSF [EAR-0738654, EAR-0738741] FX Portions of this work were performed at GeoSoilEnviroCARS (Sector 13), Advanced Photon Source (APS), Argonne National Laboratory. GeoSoilEnviroCARS is supported by the National Science Foundation (Earth Sciences) under grant EAR-0622171, the Department of Energy (Geosciences) under grant DE-FG02-94ER14466, and the State of Illinois. Use of the APS was supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under contract DE-AC02-06CH11357. This research was supported by NSF grant EAR-0738654 to E.C. and NSF grant EAR-0738741 to Y.F. NR 35 TC 20 Z9 21 U1 2 U2 32 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 28 PY 2013 VL 40 IS 20 BP 5377 EP 5381 DI 10.1002/2013GL057930 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 301DY UT WOS:000330514200009 ER PT J AU Yan, L Winter, HD Murphy, NA Jun, L Ning, W AF Yan, Li Winter, Henry D. Murphy, Nicholas A. Jun, Lin Ning, Wu TI The Dependence of Particle Acceleration on Initial Locations in Reconnecting Current Sheets SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE Sun: flares; Sun: magnetic reconnection; Sun: particle acceleration ID SOLAR-FLARES; PROTON ACCELERATION; MAGNETIC-FIELD; ELECTRON ACCELERATION; ENERGY-SPECTRA; ATMOSPHERE; MODEL AB Electron and proton acceleration by a super-Dreicer electric field is investigated in a reconnecting current sheet in the presence of a guide field. The electric field is assumed to vary in space. Electrons and protons are accelerated from initial positions randomly distributed over the whole acceleration region. The stability of the energy spectrum is investigated using different numbers of test particles. The energy spectrum eventually obtained is consistent with a power-law spectrum. The spectral index of electrons increases rapidly with increasing guide field, but the index for the protons does not vary significantly. The relation of the final energy to the initial position is also studied. The results indicate that the addition of a guide field not only allows the reconnecting electric field to selectively accelerate electrons and protons from different initial positions, but also increases the number of accelerated electrons and reduces the number of protons. The final position and the pitch angles of the accelerated particles are also investigated. Finally, we also calculate the energy spectrum of particles initially distributed at the boundary of the reconnection inflow. C1 [Yan, Li; Jun, Lin] Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Peoples R China. [Yan, Li] Chinese Acad Sci, Grad Univ, Beijing 100039, Peoples R China. [Winter, Henry D.; Murphy, Nicholas A.; Jun, Lin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ning, Wu] Yunnan Normal Univ, Sch Tourism & Geog, Kunming 650031, Peoples R China. RP Yan, L (reprint author), Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Peoples R China. EM liyan821@ynao.ac.cn OI Murphy, Nicholas/0000-0001-6628-8033 FU Program 973 [2011CB811403, 2013CBA01503]; NSFC [11273055]; CAS [2010Y2JB16, KJCX2-EW-T07]; NSF SHINE [AGS-1156076] FX We thank the anonymous referee for the constructive comments and suggestions that much improved the original version of the manuscript. This work was supported by Program 973 grants 2011CB811403 and 2013CBA01503, NSFC grant 11273055, CAS grants 2010Y2JB16 and KJCX2-EW-T07. H.W., N.M., and J.L. acknowledge support from NSF SHINE grant AGS-1156076. NR 38 TC 1 Z9 1 U1 1 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD OCT 25 PY 2013 VL 65 IS 5 AR UNSP 101 DI 10.1093/pasj/65.5.101 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 270DY UT WOS:000328300300010 ER PT J AU Finkelstein, SL Papovich, C Dickinson, M Song, M Tilvi, V Koekemoer, AM Finkelstein, KD Mobasher, B Ferguson, HC Giavalisco, M Reddy, N Ashby, MLN Dekel, A Fazio, GG Fontana, A Grogin, NA Huang, JS Kocevski, D Rafelski, M Weiner, BJ Willner, SP AF Finkelstein, S. L. Papovich, C. Dickinson, M. Song, M. Tilvi, V. Koekemoer, A. M. Finkelstein, K. D. Mobasher, B. Ferguson, H. C. Giavalisco, M. Reddy, N. Ashby, M. L. N. Dekel, A. Fazio, G. G. Fontana, A. Grogin, N. A. Huang, J. -S. Kocevski, D. Rafelski, M. Weiner, B. J. Willner, S. P. TI A galaxy rapidly forming stars 700 million years after the Big Bang at redshift 7.51 SO NATURE LA English DT Article ID LYMAN BREAK GALAXIES; EXTRAGALACTIC LEGACY SURVEY; LY-ALPHA EMITTERS; ULTRA-DEEP-FIELD; SPECTROSCOPIC CONFIRMATION; KECK SPECTROSCOPY; REIONIZATION; CANDELS; EVOLUTION; EMISSION AB Of several dozen galaxies observed spectroscopically that are candidates for having a redshift (z) in excess of seven, only five have had their redshifts confirmed via Lyman alpha emission, at z = 7.008, 7.045, 7.109, 7.213 and 7.215 (refs 1-4). The small fraction of confirmed galaxies may indicate that the neutral fraction in the intergalactic medium rises quickly at z > 6.5, given that Lyman alpha is resonantly scattered by neutral gas(3,5-8). The small samples and limited depth of previous observations, however, makes these conclusions tentative. Here we report a deep near-infrared spectroscopic survey of 43 photometrically-selected galaxies with z > 6.5. We detect a near-infrared emission line from only a single galaxy, confirming that some process is making Lyman alpha difficult to detect. The detected emission line at a wavelength of 1.0343 micrometres is likely to be Lyman alpha emission, placing this galaxy at a redshift z = 7.51, an epoch 700 million years after the Big Bang. This galaxy's colours are consistent with significant metal content, implying that galaxies become enriched rapidly. We calculate a surprisingly high star-formation rate of about 330 solar masses per year, which is more than a factor of 100 greater than that seen in the Milky Way. Such a galaxy is unexpected in a survey of our size(9), suggesting that the early Universe may harbour a larger number of intense sites of star formation than expected. C1 [Finkelstein, S. L.; Song, M.; Finkelstein, K. D.] Univ Texas Austin, Austin, TX 78712 USA. [Papovich, C.; Tilvi, V.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 78743 USA. [Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Koekemoer, A. M.; Ferguson, H. C.; Grogin, N. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Mobasher, B.; Reddy, N.] Univ Calif Riverside, Riverside, CA 92521 USA. [Giavalisco, M.] Univ Massachusetts, Amherst, MA 01003 USA. [Ashby, M. L. N.; Fazio, G. G.; Huang, J. -S.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dekel, A.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Fontana, A.] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Kocevski, D.] Univ Kentucky, Lexington, KY 40506 USA. [Rafelski, M.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Weiner, B. J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Finkelstein, SL (reprint author), Univ Texas Austin, 2515 Speedway,Stop C1400, Austin, TX 78712 USA. EM stevenf@astro.as.utexas.edu OI Koekemoer, Anton/0000-0002-6610-2048; fontana, adriano/0000-0003-3820-2823 FU W. M. Keck Foundation; NASA [NAS 5-26555]; Spitzer Space Telescope FX We thank M. Dijkstra, J. Rhoads and S. Malhotra for conversations, as well as N. Konidaris and C. Steidel for assistance with the MOSFIRE data reduction pipeline. Wealso thank our KeckSupport Astronomer G. Wirth for assistance duringour observing run. S. L. F. acknowledges support from the University of Texas at Austin, the McDonald Observatory and NASA through a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented here were obtained at the W. M. Keck Observatory from telescope time allocated to NASA through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the financial support of the W. M. Keck Foundation. Werecognize and acknowledge the cultural role and reverence that the summit of Mauna Kea has within the indigenous Hawaiian community. This work is also based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555, as well as the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 26 TC 102 Z9 102 U1 1 U2 19 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD OCT 24 PY 2013 VL 502 IS 7472 BP 524 EP 527 DI 10.1038/nature12657 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 238YN UT WOS:000325988400048 PM 24153304 ER PT J AU Hoving, HJT Zeidberg, LD Benfield, MC Bush, SL Robison, BH Vecchione, M AF Hoving, Hendrik J. T. Zeidberg, Louis D. Benfield, Mark C. Bush, Stephanie L. Robison, Bruce H. Vecchione, Michael TI First in situ observations of the deep-sea squid Grimalditeuthis bonplandi reveal unique use of tentacles SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE bathypelagic; behaviour; Cephalopoda; feeding; luring; mesopelagic ID CEPHALOPODA; BEHAVIOR; BIOLUMINESCENT; COMMUNICATION; MORPHOLOGY; EVOLUTION; HABITAT; MIMICRY; MEXICO; SHARK AB The deep-sea squid Grimalditeuthis bonplandi has tentacles unique among known squids. The elastic stalk is extremely thin and fragile, whereas the clubs bear no suckers, hooks or photophores. It is unknown whether and how these tentacles are used in prey capture and handling. We present, to our knowledge, the first in situ observations of this species obtained by remotely operated vehicles (ROVs) in the Atlantic and North Pacific. Unexpectedly, G. bonplandi is unable to rapidly extend and retract the tentacle stalk as do other squids, but instead manoeuvres the tentacles by undulation and flapping of the clubs' trabecular protective membranes. These tentacle club movements superficially resemble the movements of small marine organisms and suggest the possibility that G. bonplandi uses aggressive mimicry by the tentacle clubs to lure prey, which we find to consist of crustaceans and cephalopods. In the darkness of the meso-and bathypelagic zones the flapping and undulatory movements of the tentacle may: (i) stimulate bioluminescence in the surrounding water, (ii) create low-frequency vibrations and/or (iii) produce a hydrodynamic wake. Potential prey of G. bonplandi may be attracted to one or more of these as signals. This singular use of the tentacle adds to the diverse foraging and feeding strategies known in deep-sea cephalopods. C1 [Hoving, Hendrik J. T.; Robison, Bruce H.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. [Zeidberg, Louis D.] Calif Dept Fish & Wildlife, Monterey, CA 93940 USA. [Benfield, Mark C.] Louisiana State Univ, Dept Coastal & Oceanog Sci, Baton Rouge, LA 70803 USA. [Bush, Stephanie L.; Vecchione, Michael] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Hoving, HJT (reprint author), GEOMAR Helmholtz Ctr Ocean Res Kiel, D-24148 Kiel, Germany. EM hhoving@geomar.de FU Bureau of Ocean Energy Management (BOEM); BP; Shell; David and Lucile Packard Foundation; Netherlands Organization for Scientific Research; Royal Dutch Academy for Sciences (KNAW) FX Gulf SERPENT is supported by the Bureau of Ocean Energy Management (BOEM) with matching funds from BP and Shell. The David and Lucile Packard Foundation, the Netherlands Organization for Scientific Research and the Royal Dutch Academy for Sciences (KNAW) part funded the research. NR 41 TC 1 Z9 1 U1 48 U2 159 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 OCT 22 PY 2013 VL 280 IS 1769 AR 20131463 DI 10.1098/rspb.2013.1463 PG 5 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 298KF UT WOS:000330322000006 PM 23986106 ER PT J AU DeVience, SJ Walsworth, RL Rosen, MS AF DeVience, Stephen J. Walsworth, Ronald L. Rosen, Matthew S. TI Preparation of Nuclear Spin Singlet States Using Spin-Lock Induced Crossing SO PHYSICAL REVIEW LETTERS LA English DT Article ID NITROGEN-VACANCY SPIN; LONG-LIVED STATES; SOLUTION NMR; MAGNETIC-RESONANCE; SYSTEMS; DIAMOND; LIFETIMES AB We introduce a broadly applicable technique to create nuclear spin singlet states in organic molecules and other many-atom systems. We employ a novel pulse sequence to produce a spin-lock induced crossing (SLIC) of the spin singlet and triplet energy levels, which enables triplet-singlet polarization transfer and singlet-state preparation. We demonstrate the utility of the SLIC method by producing a long-lived nuclear spin singlet state on two strongly coupled proton pairs in the tripeptide molecule phenylalanine-glycine-glycine dissolved in D2O and by using SLIC to measure the J couplings, chemical shift differences, and singlet lifetimes of the proton pairs. We show that SLIC is more efficient at creating nearly equivalent nuclear spin singlet states than previous pulse sequence techniques, especially when triplet-singlet polarization transfer occurs on the same time scale as spin-lattice relaxation. C1 [DeVience, Stephen J.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Walsworth, Ronald L.] Harvard Univ, Ctr Brain Sci, Cambridge, MA 02138 USA. [Walsworth, Ronald L.; Rosen, Matthew S.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Rosen, Matthew S.] AA Martinos Ctr Biomed Imaging, Charlestown, MA 02129 USA. [Rosen, Matthew S.] Harvard Univ, Sch Med, Boston, MA 02115 USA. RP DeVience, SJ (reprint author), Harvard Univ, Dept Chem & Chem Biol, 12 Oxford St, Cambridge, MA 02138 USA. EM devience@fas.harvard.edu; rwalsworth@cfa.harvard.edu; mrosen@cfa.harvard.edu RI DeVience, Stephen/D-7274-2012 OI DeVience, Stephen/0000-0003-3142-7296 FU NSF; Army program; DARPA-QuASAR program; MURI QuISM program FX We acknowledge support from the NSF, Army, and DARPA-QuASAR and MURI QuISM programs. NR 31 TC 27 Z9 27 U1 2 U2 33 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 OCT 22 PY 2013 VL 111 IS 17 AR 173002 DI 10.1103/PhysRevLett.111.173002 PG 5 WC Physics, Multidisciplinary SC Physics GA 241ED UT WOS:000326148300007 PM 24206484 ER PT J AU Hazari, Z Potvin, G Lock, RM Lung, F Sonnert, G Sadler, PM AF Hazari, Zahra Potvin, Geoff Lock, Robynne M. Lung, Florin Sonnert, Gerhard Sadler, Philip M. TI Factors that affect the physical science career interest of female students: Testing five common hypotheses SO PHYSICAL REVIEW SPECIAL TOPICS-PHYSICS EDUCATION RESEARCH LA English DT Article ID SINGLE-SEX; HIGH-SCHOOL; SELF-CONCEPT; ROLE-MODELS; GENDER; ACHIEVEMENT; PERFORMANCE; GIRLS; TEACHERS; FACULTY AB There are many hypotheses regarding factors that may encourage female students to pursue careers in the physical sciences. Using multivariate matching methods on national data drawn from the Persistence Research in Science and Engineering (PRiSE) project (n = 7505), we test the following five commonly held beliefs regarding what factors might impact females' physical science career interest: (i) having a single-sex physics class, (ii) having a female physics teacher, (iii) having female scientist guest speakers in physics class, (iv) discussing the work of female scientists in physics class, and (v) discussing the underrepresentation of women in physics class. The effect of these experiences on physical science career interest is compared for female students who are matched on several factors, including prior science interests, prior mathematics interests, grades in science, grades in mathematics, and years of enrollment in high school physics. No significant effects are found for single-sex classes, female teachers, female scientist guest speakers, and discussing the work of female scientists. However, discussions about women's underrepresentation have a significant positive effect. C1 [Hazari, Zahra] Florida Int Univ, Dept Teaching & Learning, Miami, FL 33199 USA. [Hazari, Zahra; Potvin, Geoff] Florida Int Univ, Dept Phys, Miami, FL 33199 USA. [Hazari, Zahra; Potvin, Geoff; Lock, Robynne M.] Clemson Univ, Dept Engn & Sci Educ, Clemson, SC USA. [Lung, Florin] Mississippi State Univ, Dept Phys & Astron, Mississippi State, MS 39762 USA. [Sonnert, Gerhard; Sadler, Philip M.] Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, Cambridge, MA 02138 USA. RP Hazari, Z (reprint author), Florida Int Univ, Dept Teaching & Learning, Miami, FL 33199 USA. EM zahra@clemson.edu FU National Science Foundation [GSE-0624444, DRL-0952460] FX This material is based upon work supported by the National Science Foundation under Grants No. GSE-0624444 and No. DRL-0952460. NR 42 TC 8 Z9 8 U1 2 U2 28 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1554-9178 J9 PHYS REV SPEC TOP-PH JI Phys. Rev. Spec. Top.-Phys. Educ. R. PD OCT 22 PY 2013 VL 9 IS 2 AR UNSP 020115 DI 10.1103/PhysRevSTPER.9.020115 PG 8 WC Education & Educational Research; Education, Scientific Disciplines SC Education & Educational Research GA 239VO UT WOS:000326054100001 ER PT J AU Carmichael, MJ Carmichael, SK Santelli, CM Strom, A Brauer, SL AF Carmichael, Mary J. Carmichael, Sarah K. Santelli, Cara M. Strom, Amanda Braeuer, Suzanna L. TI Mn(II)-oxidizing Bacteria are Abundant and Environmentally Relevant Members of Ferromanganese Deposits in Caves of the Upper Tennessee River Basin SO GEOMICROBIOLOGY JOURNAL LA English DT Article DE cave geomicrobiology; ferromanganese deposits; manganese oxidation; Tennessee karst ID MOLECULAR PHYLOGENETIC ANALYSIS; BIOGENIC MN OXIDES; MICROBIAL COMMUNITIES; MANGANESE OXIDE; OXIDIZING BACTERIA; MN(II) OXIDATION; COPY NUMBER; DEINOCOCCUS-RADIODURANS; NICHE DIFFERENTIATION; KARTCHNER CAVERNS AB The upper Tennessee River Basin contains the highest density of our nation's caves; yet, little is known regarding speleogenesis or Fe and Mn biomineralization in these predominantly epigenic systems. Mn:Fe ratios of Mn and Fe oxide-rich biofilms, coatings, and mineral crusts that were abundant in several different caves ranged from ca. 0.1 to 1.0 as measured using ICP-OES. At sites where the Mn:Fe ratio approached 1.0 this represented an order of magnitude increase above the bulk bedrock ratio, suggesting that biomineralization processes play an important role in the formation of these cave ferromanganese deposits. Estimates of total bacterial SSU rRNA genes in ferromanganese biofilms, coatings, and crusts measured approximately 7x10(7)-9x10(9) cells/g wet weight sample. A SSU-rRNA based molecular survey of biofilm material revealed that 21% of the 34 recovered dominant (non-singleton) OTUs were closely related to known metal-oxidizing bacteria or clones isolated from oxidized metal deposits. Several different isolates that promote the oxidation of Mn(II) compounds were obtained in this study, some from high dilutions (10(-8)-10(-10)) of deposit material. In contrast to studies of caves in other regions, SSU rRNA sequences of Mn-oxidizing bacterial isolates in this study most closely matched those of Pseudomonas, Leptothrix, Flavobacterium, and Janthinobacterium. Combined data from geochemical analyses, molecular surveys, and culture-based experiments suggest that a unique consortia of Mn(II)-oxidizing bacteria are abundant and promoting biomineralization processes within the caves of the upper Tennessee River Basin. C1 [Carmichael, Mary J.; Strom, Amanda; Braeuer, Suzanna L.] Appalachian State Univ, Dept Biol, Boone, NC 28608 USA. [Carmichael, Sarah K.; Santelli, Cara M.] Appalachian State Univ, Dept Geol, Boone, NC 28608 USA. [Santelli, Cara M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Brauer, SL (reprint author), Appalachian State Univ, Dept Biol, 572 Rivers St,Rankin Sci Bldg, Boone, NC 28608 USA. EM brauersl@appstate.edu OI Santelli, Cara/0000-0001-8617-0008 FU National Science Foundation [0935270]; North Carolina Space Grant New Investigators Program; North Carolina Space Grant Graduate Research Fellowship; Appalachian State University FX The authors would like to thank Dr. Clara Chan for assistance with electron microscopy and sample preparation, and Dr. Guichuan Hou and Oliver Burns for assistance with light, confocal, and electron microscopy. We thank Dr. Yongli Gao, Taylor Burnham, Seth Hewitt, John Rossi, Milton Starnes, Robbie Winters, and John Matthews for providing field expertise and scouting locations of cave ferromanganese deposits, and to the landowners of the caves for site access. We are appreciative of assistance from Dr. Carol Babyak, Dr. Shea Tuberty, Daniel Jackson, and Yosuke Sakamachi in preparing samples and in conducting ICP-OES analyses. We are deeply grateful for the assistance of Dr. Trevor Craig, Zach Anderson, Jared Butler, Kornelia Galior, Ashley Hawkins, Daniel Parker, Leigh Anne Roble, Marlie Shelton, and Bryan Zorn in culture maintenance, field assistance, and procedural development. Partial support was provided through a National Science Foundation grant 0935270 to S. Brauer, two North Carolina Space Grant New Investigators Program Awards to S. Carmichael and to S. Brauer, and through a North Carolina Space Grant Graduate Research Fellowship awarded to M.J. Carmichael. Support was also provided by Appalachian State University. NR 131 TC 20 Z9 22 U1 3 U2 70 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0149-0451 J9 GEOMICROBIOL J JI Geomicrobiol. J. PD OCT 21 PY 2013 VL 30 IS 9 BP 779 EP 800 DI 10.1080/01490451.2013.769651 PG 22 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 189ZW UT WOS:000322307800002 ER PT J AU Archambault, S Arlen, T Aune, T Behera, B Beilicke, M Benbow, W Bird, R Bouvier, A Buckley, JH Bugaev, V Byrum, K Cesarini, A Ciupik, L Connolly, MP Cui, W Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Griffin, S Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Kaaret, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Kumar, S Lang, MJ Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Millis, J Moriarty, P Mukherjee, R de Bhroithe, AO Ong, RA Otte, AN Park, N Perkins, JS Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Richards, GT Roache, E Saxon, DB Sembroski, GH Smith, AW Staszak, D Telezhinsky, I Theiling, M Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Weekes, TC Weinstein, A Welsing, R Williams, DA Zitzer, B Bottcher, M Fegan, SJ Fortin, P Halpern, JP Kovalev, YY Lister, ML Liu, J Pushkarev, AB Smith, PS AF Archambault, S. Arlen, T. Aune, T. Behera, B. Beilicke, M. Benbow, W. Bird, R. Bouvier, A. Buckley, J. H. Bugaev, V. Byrum, K. Cesarini, A. Ciupik, L. Connolly, M. P. Cui, W. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Griffin, S. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Kumar, S. Lang, M. J. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Millis, J. Moriarty, P. Mukherjee, R. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Saxon, D. B. Sembroski, G. H. Smith, A. W. Staszak, D. Telezhinsky, I. Theiling, M. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Weekes, T. C. Weinstein, A. Welsing, R. Williams, D. A. Zitzer, B. Boettcher, M. Fegan, S. J. Fortin, P. Halpern, J. P. Kovalev, Y. Y. Lister, M. L. Liu, J. Pushkarev, A. B. Smith, P. S. CA VERITAS Collaboration TI DISCOVERY OF A NEW TeV GAMMA-RAY SOURCE: VER J0521+211 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (VER J0521+211); gamma rays: galaxies ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; EXTRAGALACTIC BACKGROUND LIGHT; ALL-SKY SURVEY; HIGH-ENERGY EMISSION; MULTIWAVELENGTH OBSERVATIONS; SOURCE CATALOG; BL-LAC; LINEAR-POLARIZATION; DETECTED BLAZARS AB We report the detection of a new TeV gamma-ray source, VER J0521+211, based on observations made with the VERITAS imaging atmospheric Cherenkov Telescope Array. These observations were motivated by the discovery of a cluster of >30 GeV photons in the first year of Fermi Large Area Telescope observations. VER J0521+211 is relatively bright at TeV energies, with a mean photon flux of (1.93 +/- 0.13(stat) +/- 0.78(sys)) x 10(-11) cm(-2) s(-1) above 0.2 TeV during the period of the VERITAS observations. The source is strongly variable on a daily timescale across all wavebands, from optical to TeV, with a peak flux corresponding to similar to 0.3 times the steady Crab Nebula flux at TeV energies. Follow-up observations in the optical and X-ray bands classify the newly discovered TeV source as a BL Lac-type blazar with uncertain redshift, although recent measurements suggest z = 0.108. VER J0521+211 exhibits all the defining properties of blazars in radio, optical, X-ray, and gamma-ray wavelengths. C1 [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Arlen, T.; Aune, T.; Majumdar, P.; Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Behera, B.; Federici, S.; Hughes, G.; Krawczynski, H.; 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.; Galante, N.; Roache, E.; Weekes, T. C.; Fortin, P.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bird, R.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cesarini, A.; Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Errando, M.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Fortson, L.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Gall, D.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Holder, J.; Kumar, S.; Saxon, D. B.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Kumar, S.; Saxon, D. B.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Humensky, T. B.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Krennrich, F.; Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Majumdar, P.] Saha Inst Nucl Phys, Kolkata 700064, India. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Dublin, 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. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Boettcher, M.] North West Univ, Ctr Space Res, ZA-2531 Potchefstroom, South Africa. [Fegan, S. J.] Ecole Polytech, CNRS, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Halpern, J. P.; Liu, J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kovalev, Y. Y.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kovalev, Y. Y.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Pushkarev, A. B.] Pulkovo Astron Observ, St Petersburg 196140, Russia. [Pushkarev, A. B.] Crimean Astrophys Observ, UA-98409 Nauchnyi, Crimea, Ukraine. [Smith, P. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Archambault, S (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM errando@astro.columbia.edu; jholder@physics.udel.edu; sfegan@llr.in2p3.fr; fortin@veritas.sao.arizona.edu RI Kovalev, Yuri/J-5671-2013; Khassen, Yerbol/I-3806-2015; Pushkarev, Alexander/M-9997-2015; OI Errando, Manel/0000-0002-1853-863X; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563; Kovalev, Yuri/0000-0001-9303-3263; Khassen, Yerbol/0000-0002-7296-3100; Smith, Paul/0000-0002-5083-3663; Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Liu, Jia/0000-0001-8219-1995 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the UK; INAF in Italy; CNES in France; NASA [NNX10AP66G, NNX12AJ30G, NNX10AF89G]; Russian Foundation for Basic Research [11-02-00368, 12-02-33101]; Russian Academy of Sciences; Dynasty Foundation; South African Department of Science and Technology through the National Research Foundation under NRF SARChI Chair [64789]; NASA-Fermi [NNX08AV67G, 11-Fermi11-0019, NNX09AU10G] FX VERITAS is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument.; The Fermi-LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged.; M. E. acknowledges support from the NASA grants NNX10AP66G and NNX12AJ30G. Y.Y.K. was supported in part by the Russian Foundation for Basic Research (projects 11-02-00368 and 12-02-33101), the basic research program "Active Processes in Galactic and Extragalactic Objects" of the Physical Sciences Division of the Russian Academy of Sciences, and the Dynasty Foundation. M. B. acknowledges support by the South African Department of Science and Technology through the National Research Foundation under NRF SARChI Chair grant No. 64789.; This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2009a). The MOJAVE project is supported under NASA-Fermi grants NNX08AV67G and 11-Fermi11-0019. The authors thank Julie Skinner for obtaining, as a target of opportunity, the first MDM spectrum of RGB J0521.8+2112 used in this paper, and Talvikki Hovatta for providing the OVRO radio data. Observations at Steward Observatory were supported by the NASA Fermi Guest Investigator Program grant NNX09AU10G. Finally, the authors thank the Swift team for accepting and carefully scheduling the target of opportunity observations of VER J0521+211 that were used in the paper and for support from the Swift Guest Investigator program, NASA grant NNX10AF89G. NR 93 TC 12 Z9 13 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 OCT 20 PY 2013 VL 776 IS 2 AR 69 DI 10.1088/0004-637X/776/2/69 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100006 ER PT J AU Battaglia, N Natarajan, A Trac, H Cen, R Loeb, A AF Battaglia, N. Natarajan, A. Trac, H. Cen, R. Loeb, A. TI REIONIZATION ON LARGE SCALES. III. PREDICTIONS FOR LOW-l COSMIC MICROWAVE BACKGROUND POLARIZATION AND HIGH-l KINETIC SUNYAEV-ZEL'DOVICH OBSERVABLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: theory; intergalactic medium; large-scale structure of universe; methods: numerical ID SOUTH-POLE TELESCOPE; SZ POWER SPECTRUM; INHOMOGENEOUS REIONIZATION; HIGH-REDSHIFT; NONUNIFORM REIONIZATION; INTERGALACTIC MEDIUM; PATCHY REIONIZATION; CMB ANISOTROPIES; GALAXY FORMATION; CLUSTER PHYSICS AB We present new predictions for cosmic microwave background (CMB) temperature (on small angular scales) and polarization (on large angular scales) anisotropies induced during the epoch of reionization (EoR). Using a novel method calibrated from radiation-hydrodynamic simulations, we model the EoR in large volumes (L greater than or similar to 2Gpc h(-1)). We find that the EoR contribution to the kinetic Sunyaev-Zel'dovich power spectrum (patchy kSZ) ranges between similar to 0.6-2.8 mu K-2 at l = 3000 for the explored parameter space. For each model, the patchy kSZ power spectrum is calculated from three large 15 degrees x 15 degrees maps for better numerical convergence. Decreasing the size of these maps biases the overall patchy kSZ power to higher values. We find that the amplitude of the patchy kSZ power spectrum at l = 3000 follows simple scalings of D-l=3000(kSZ) alpha (z) over bar and D(l=3000)kSZ alpha Delta(0.51)(z) for the mean redshift ((z) over bar) and duration (Delta(z)) of reionization. Using the constraints on (z) over barz from the Wilkinson Microwave Anisotropy Probe seven year results and the lower limit on Delta(z) from EDGES, we find a lower limit of similar to 0.4 mu K-2 at l = 3000. Planck will infer the mean redshift from the Thomson optical depth imprinted in the low-l polarization power spectrum. Future measurements of the high-l CMB power spectrum from the Atacama Cosmology Telescope and South Pole Telescope should detect the patchy kSZ signal if the cross correlation between the thermal SZ effect and the cosmic infrared background is constrained. We show that the combination of temperature and polarization measurements constrains both (z) over bar and Delta(z). The patchy kSZ maps, power spectra templates, and the polarization power spectra will be publicly available. C1 [Battaglia, N.; Natarajan, A.; Trac, H.] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Cen, R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Loeb, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Battaglia, N (reprint author), Carnegie Mellon Univ, McWilliams Ctr Cosmol, Wean Hall,5000 Forbes Ave, Pittsburgh, PA 15213 USA. RI Trac, Hy/N-8838-2014 OI Trac, Hy/0000-0001-6778-3861 FU McWilliams Center for Cosmology; NSF [AST-1109730, 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 Center for Cosmology. We thank Graeme Addison, Gil Holder, Eiichiro Komatsu, Andrei Mesinger, Paul La Plante, Christian Reichardt, Jonathan Sievers, and Oliver Zahn for useful discussions. H. T. is supported in part by NSF grant AST-1109730. 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 56 TC 17 Z9 17 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2013 VL 776 IS 2 AR 83 DI 10.1088/0004-637X/776/2/83 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100020 ER PT J AU Battaglia, N Trac, H Cen, R Loeb, A AF Battaglia, N. Trac, H. Cen, R. Loeb, A. TI REIONIZATION ON LARGE SCALES. I. A PARAMETRIC MODEL CONSTRUCTED FROM RADIATION-HYDRODYNAMIC SIMULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; intergalactic medium; large-scale structure of universe; methods: numerical ID COSMIC REIONIZATION; HIGH-REDSHIFT; PATCHY REIONIZATION; INHOMOGENEOUS REIONIZATION; COSMOLOGICAL REIONIZATION; HYDROGEN REIONIZATION; EDDINGTON TENSOR; TRANSFER SCHEME; RE-IONIZATION; 21-CM SIGNAL AB We present a new method for modeling inhomogeneous cosmic reionization on large scales. Utilizing high-resolution radiation-hydrodynamic simulations with 2048(3) dark matter particles, 2048(3) gas cells, and 17 billion adaptive rays in a L = 100 Mpc h(-1) box, we show that the density and reionization redshift fields are highly correlated on large scales (greater than or similar to 1 Mpc h(-1)). This correlation can be statistically represented by a scale-dependent linear bias. We construct a parametric function for the bias, which is then used to filter any large-scale density field to derive the corresponding spatially varying reionization redshift field. The parametric model has three free parameters that can be reduced to one free parameter when we fit the two bias parameters to simulation results. We can differentiate degenerate combinations of the bias parameters by combining results for the global ionization histories and correlation length between ionized regions. Unlike previous semi-analytic models, the evolution of the reionization redshift field in our model is directly compared cell by cell against simulations and performs well in all tests. Our model maps the high-resolution, intermediate-volume radiation-hydrodynamic simulations onto lower-resolution, larger-volume N-body simulations (greater than or similar to 2 Gpc h(-1)) in order to make mock observations and theoretical predictions. C1 [Battaglia, N.; Trac, H.] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Cen, R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Loeb, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Battaglia, N (reprint author), Carnegie Mellon Univ, McWilliams Ctr Cosmol, Wean Hall,5000 Forbes Ave, Pittsburgh, PA 15213 USA. RI Trac, Hy/N-8838-2014 OI Trac, Hy/0000-0001-6778-3861 FU NSF [AST-1109730, AST-1108700, AST-0907890]; NASA [NNX12AF91G, NNX08AL43G, NNA09DB30A]; McWilliams Center for Cosmology FX N.B. is supported by a McWilliams Center for Cosmology Postdoctoral Fellowship made possible by Bruce and Astrid McWilliams. We thank Aravind Natarajan, Paul La Plante, Jonathan Sievers, and Christian Reichardt for useful discussions. We thank N. Gnedin for his compilation of the ionization and recombination rates and D. Schaerer for the Population II spectral energy distributions. H. T. is supported in part by NSF grant AST-1109730. 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 63 TC 22 Z9 22 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2013 VL 776 IS 2 AR 81 DI 10.1088/0004-637X/776/2/81 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100018 ER PT J AU Kim, DW Fabbiano, G AF Kim, Dong-Woo Fabbiano, Giuseppina TI X-RAY SCALING RELATION IN EARLY-TYPE GALAXIES: DARK MATTER AS A PRIMARY FACTOR IN RETAINING HOT GAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; X-rays: galaxies ID SUPERMASSIVE BLACK-HOLES; ELLIPTIC GALAXIES; INTERSTELLAR-MEDIUM; MULTIPARAMETRIC ANALYSIS; LUMINOSITY FUNCTION; ATLAS(3D) PROJECT; EINSTEIN SAMPLE; EMISSION; MASS; HALOES AB We have revisited the X-ray scaling relations of early-type galaxies (ETG) by investigating, for the first time, the L-X,L-Gas-M-Total relation in a sample of 14 ETGs. In contrast to the large scatter (a factor of 10(2)-10(3)) in the L-X,L-Total-L-B relation, we found a tight correlation between these physically motivated quantities with an rms deviation of a factor of three in L-X,L-Gas = 10(38)-10(43) erg s(-1) or M-Total = a few x 10(10) to a few x 10(12) M-circle dot. More striking, this relation becomes even tighter with an rms deviation of a factor of 1.3 among the gas-rich galaxies (with L-X,L-Gas > 10(40) erg s(-1)). In a simple power-law form, the new relation is (L-X,L-Gas/10(40) erg s(-1)) = (M-Total/3.2 x 10(11) M-circle dot)(3). This relation is also consistent with the steep relation between the gas luminosity and temperature, L-X,L-Gas similar to T-Gas(4.5), identified by Boroson et al., if the gas is virialized. Our results indicate that the total mass of an ETG is the primary factor in regulating the amount of hot gas. Among the gas-poor galaxies (with L-X,L-Gas < a few x 10(39) erg s(-1)), the scatter in the L-X,L-Gas-M-Total (and L-X,L-Gas-T-Gas) relation increases, suggesting that secondary factors (e.g., rotation, flattening, star formation history, cold gas, environment, etc.) may become important. C1 [Kim, Dong-Woo; Fabbiano, Giuseppina] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kim, DW (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [NAS8-03060] FX We thank Alis Deason, Silvia Pellegrini, Aaron Romanowsky, and Mark Sarzi for helpful discussions. The data analysis was supported by the CXC CIAO software and CALDB. We have used the NASA NED and ADS facilities, and have extracted archival data from the Chandra archives. This work was supported by NASA contract NAS8-03060 (CXC). NR 47 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 OCT 20 PY 2013 VL 776 IS 2 AR 116 DI 10.1088/0004-637X/776/2/116 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100053 ER PT J AU Laskar, T Berger, E Zauderer, BA Margutti, R Soderberg, AM Chakraborti, S Lunnan, R Chornock, R Chandra, P Ray, A AF Laskar, T. Berger, E. Zauderer, B. A. Margutti, R. Soderberg, A. M. Chakraborti, S. Lunnan, R. Chornock, R. Chandra, P. Ray, A. TI A REVERSE SHOCK IN GRB 130427A SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: individual (GRB 130427A) ID GAMMA-RAY BURST; EARLY OPTICAL AFTERGLOWS; LIGHT CURVES; RADIO FLARE; TELESCOPE; MISSION; FLASH; CONNECTION; RADIATION; STARS AB We present extensive radio and millimeter observations of the unusually bright GRB 130427A at z = 0.340, spanning 0.67-12 days after the burst. We combine these data with detailed multi-band UV, optical, NIR, and Swift X-ray observations and find that the broadband afterglow emission is composed of distinct reverse shock and forward shock contributions. The reverse shock emission dominates in the radio/millimeter and at less than or similar to 0.1 days in the UV/optical/NIR, while the forward shock emission dominates in the X-rays and at greater than or similar to 0.1 days in the UV/optical/NIR. We further find that the optical and X-ray data require a wind circumburst environment, pointing to a massive star progenitor. Using the combined forward and reverse shock emission, we find that the parameters of the burst include an isotropic kinetic energy of E-K,E-iso approximate to 2 x 10(53) erg, a mass loss rate of (M)over dot approximate to 3 x 10(-8) M-circle dot yr(-1) (for a wind velocity of 1000 km s(-1)), and a Lorentz factor at the deceleration time of Gamma(200 s) approximate to 130. Due to the low density and large isotropic energy, the absence of a jet break to approximate to 15 days places only a weak constraint on the opening angle, theta(j) greater than or similar to 2 degrees.5, and therefore a total energy of E-gamma + E-K greater than or similar to 1.2 x 10(51) erg, similar to other gamma-ray bursts (GRBs). The reverse shock emission is detectable in this burst due to the low circumburst density, which leads to a slow cooling shock. We speculate that this property is required for the detectability of reverse shocks in radio and millimeter bands. Following on GRB 130427A as a benchmark event, observations of future GRBs with the exquisite sensitivity of the Very Large Array and ALMA, coupled with detailed modeling of the reverse and forward shock contributions, will test this hypothesis. C1 [Laskar, T.; Berger, E.; Zauderer, B. A.; Margutti, R.; Soderberg, A. M.; Chakraborti, S.; Lunnan, R.; Chornock, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chandra, P.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Ray, A.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. RP Laskar, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Lunnan, Ragnhild/0000-0001-9454-4639 FU National Science Foundation [AST-1107973]; state of California; state of Illinois; state of Maryland; James S. McDonnell Foundation; Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; University of Chicago; Associates of the California Institute of Technology FX We thank Shiho Kobayashi, Yuanchuan Zou, Xuefeng Wu, Zigao Dai, Richard Harrison, and the anonymous referee for their helpful comments on the manuscript. The Berger GRB group is supported by the National Science Foundation under Grant AST-1107973. The MMT Observatory is a joint facility of the Smithsonian Institution and the University of Arizona. 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 data supplied by the UK Swift Science Data Centre at the University of Leicester. CARMA observations were taken as part of the CARMA Key Project, c0999, "A Millimeter View of the Transient Universe" (PI: B. A. Zauderer) and VLA observations were taken as part of programs 13A-046 (PI: E. Berger), 13A-411 (PI: A. Corsi), SE0851 (PI: A. Fruchter), and S50386 (PI: S. B. Cenko). Support for CARMA construction was derived from the states of California, Illinois, and Maryland, the James S. McDonnell Foundation, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the University of Chicago, the Associates of the California Institute of Technology, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. The GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. NR 58 TC 33 Z9 34 U1 2 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2013 VL 776 IS 2 AR 119 DI 10.1088/0004-637X/776/2/119 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100056 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 THE GALEX ARECIBO SDSS SURVEY. VII. THE BIVARIATE NEUTRAL HYDROGEN-STELLAR MASS FUNCTION FOR MASSIVE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation ID STAR-FORMATION HISTORY; FAST ALPHA SURVEY; FRACTION SCALING RELATIONS; COLOR-MAGNITUDE DIAGRAM; LOW-REDSHIFT UNIVERSE; DIGITAL SKY SURVEY; LOCAL UNIVERSE; COSMOLOGICAL SIMULATIONS; GAS FRACTIONS; LUMINOSITY FUNCTION AB We present the bivariate neutral atomic hydrogen (H I)-stellar mass function (HISMF) phi(M-H (I), M-*) for massive (log M-*/M-circle dot > 10) galaxies derived from a sample of 480 local (0.025 < z < 0.050) galaxies observed in H I at Arecibo as part of the GALEX Arecibo SDSS Survey. We fit six different models to the HISMF and find that a Schechter function that extends down to a 1% Hi gas fraction, with an additional fractional contribution below that limit, is the best parameterization of the HISMF. We calculate Omega(H) (I), (M*>1010) and find that massive galaxies contribute 41% of the H I density in the local universe. In addition to the binned HISMF, we derive a continuous bivariate fit, which reveals that the Schechter parameters only vary weakly with stellar mass: M-H I*, the characteristic H I mass, scales as M-*(0.39); alpha, the slope of the HISMF at moderate H I masses, scales as M-*(0.07); and f, the fraction of galaxies with H I gas fraction greater than 1%, scales as M-*(-0.24). The variation of f with stellar mass should be a strong constraint for numerical simulations. To understand the physical mechanisms that produce the shape of the HISMF, we redefine the parameters of the Schechter function as explicit functions of stellar mass and star formation rate (SFR) to produce a trivariate fit. This analysis reveals strong trends with SFR. While M-H I* varies weakly with stellar mass and SFR (M-H I* proportional to M-*(0.22), M-H I* proportional to SFR-0.03), alpha is a stronger function of both stellar mass and especially SFR (alpha proportional to M-*(0.47), alpha proportional to SFR0.95). The HISMF is a crucial tool that can be used to constrain cosmological galaxy simulations, test observational predictions of the H I content of populations of galaxies, and identify galaxies whose properties deviate from average trends. C1 [Lemonias, Jenna J.; Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Catinella, Barbara] Max Planck Inst Astrophys, D-85741 Garching, Germany. [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 National Science Foundation [AST-1100968]; 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 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 83 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 OCT 20 PY 2013 VL 776 IS 2 AR 74 DI 10.1088/0004-637X/776/2/74 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100011 ER PT J AU Lemze, D Postman, M Genel, S Ford, HC Balestra, I Donahue, M Kelson, D Nonino, M Mercurio, A Biviano, A Rosati, P Umetsu, K Sand, D Koekemoer, A Meneghetti, M Melchior, P Newman, AB Bhatti, WA Voit, GM Medezinski, E Zitrin, A Zheng, W Broadhurst, T Bartelmann, M Benitez, N Bouwens, R Bradley, L Coe, D Graves, G Grillo, C Infante, L Jimenez-Teja, Y Jouvel, S Lahav, O Maoz, D Merten, J Molino, A Moustakas, J Moustakas, L Ogaz, S Scodeggio, M Seitz, S AF Lemze, Doron Postman, Marc Genel, Shy Ford, Holland C. Balestra, Italo Donahue, Megan Kelson, Daniel Nonino, Mario Mercurio, Amata Biviano, Andrea Rosati, Piero Umetsu, Keiichi Sand, David Koekemoer, Anton Meneghetti, Massimo Melchior, Peter Newman, Andrew B. Bhatti, Waqas A. Voit, G. Mark Medezinski, Elinor Zitrin, Adi Zheng, Wei Broadhurst, Tom Bartelmann, Matthias Benitez, Narciso Bouwens, Rychard Bradley, Larry Coe, Dan Graves, Genevieve Grillo, Claudio Infante, Leopoldo Jimenez-Teja, Yolanda Jouvel, Stephanie Lahav, Ofer Maoz, Dan Merten, Julian Molino, Alberto Moustakas, John Moustakas, Leonidas Ogaz, Sara Scodeggio, Marco Seitz, Stella TI THE CONTRIBUTION OF HALOS WITH DIFFERENT MASS RATIOS TO THE OVERALL GROWTH OF CLUSTER-SIZED HALOS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: clusters: individual (Abell 611, Abell 963, Abell 1423, Abell 2261, MACS J1206.2-0848, RX J2129.7+0005, CL 2130.4-0000); galaxies: kinematics and dynamics ID PROBE WMAP OBSERVATIONS; DARK-MATTER HALOES; DIGITAL SKY SURVEY; SCALE-INDEPENDENT METHOD; GALAXY CLUSTERS; VELOCITY ANISOTROPY; DENSITY PROFILES; DATA RELEASE; ACCELERATING UNIVERSE; MACS J1206.2-0847 AB We provide a new observational test for a key prediction of the Lambda CDM cosmological model: the contributions of mergers with different halo-to-main-cluster mass ratios to cluster-sized halo growth. We perform this test by dynamically analyzing 7 galaxy clusters, spanning the redshift range 0.13 < z(c) < 0.45 and caustic mass range 0.4-1.5 10(15) h(0.73)(-1) M-circle dot, with an average of 293 spectroscopically confirmed bound galaxies to each cluster. The large radial coverage (a few virial radii), which covers the whole infall region, with a high number of spectroscopically identified galaxies enables this new study. For each cluster, we identify bound galaxies. Out of these galaxies, we identify infalling and accreted halos and estimate their masses and their dynamical states. Using the estimated masses, we derive the contribution of different mass ratios to cluster-sized halo growth. For mass ratios between similar to 0.2 and 0.7, we find a similar to 1 sigma agreement with Lambda CDM expectations based on the Millennium simulations I and II. At low mass ratios, less than or similar to 0.2, our derived contribution is underestimated since the detection efficiency decreases at low masses, similar to 2 x 10(14) h(0.73)(-1) M-circle dot. At large mass ratios, greater than or similar to 0.7, we do not detect halos probably because our sample, which was chosen to be quite X-ray relaxed, is biased against large mass ratios. Therefore, at large mass ratios, the derived contribution is also underestimated. C1 [Lemze, Doron; Ford, Holland C.; Medezinski, Elinor; Zheng, Wei] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Postman, Marc; Koekemoer, Anton; Bradley, Larry; Coe, Dan; Ogaz, Sara] Space Telescope Sci Inst, Baltimore, MD 21208 USA. [Genel, Shy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Balestra, Italo; Nonino, Mario; Biviano, Andrea] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Balestra, Italo; Mercurio, Amata] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Kelson, Daniel; Voit, G. Mark] Carnegie Observ, Carnegie Inst Sci, Pasadena, CA USA. [Rosati, Piero] European So Observ, D-85748 Garching, Germany. [Umetsu, Keiichi] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Sand, David] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Meneghetti, Massimo] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Meneghetti, Massimo] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Melchior, Peter] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Melchior, Peter] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Newman, Andrew B.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Bhatti, Waqas A.; Graves, Genevieve] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Zitrin, Adi; Bartelmann, Matthias] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany. [Broadhurst, Tom] Univ Basque Country UPV EHU, Dept Theoret Phys, E-48080 Bilbao, Spain. [Broadhurst, Tom] Basque Fdn Sci, IKERBASQUE, E-48011 Bilbao, Spain. [Benitez, Narciso; Jimenez-Teja, Yolanda; Molino, Alberto] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Bouwens, Rychard] Leiden Univ, Leiden Observ, NL-2333 Leiden, Netherlands. [Graves, Genevieve] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Grillo, Claudio] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Infante, Leopoldo] Pontificia Univ Catolica Chile, Inst Astrophys, Santiago, Chile. [Infante, Leopoldo] Pontificia Univ Catolica Chile, Ctr Astroengn, Santiago, Chile. [Jouvel, Stephanie] Inst Cincies Espai IEE CSIC, E-08193 Bellaterra, Barcelona, Spain. [Lahav, Ofer] UCL, Dept Phys & Astron, London, England. [Maoz, Dan] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Merten, Julian; Moustakas, Leonidas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY USA. [Scodeggio, Marco] INAF IASF Milano, I-20133 Milan, Italy. [Seitz, Stella] Univ Sternwarte Munchen, Inst Astron, D-81679 Munich, Germany. [Seitz, Stella] Univ Sternwarte Munchen, Inst Astrophys, D-81679 Munich, Germany. [Seitz, Stella] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. RP Lemze, D (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. RI Bartelmann, Matthias/A-5336-2014; Molino Benito, Alberto/F-5298-2014; Jimenez-Teja, Yolanda/D-5933-2011; Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015; OI Grillo, Claudio/0000-0002-5926-7143; Meneghetti, Massimo/0000-0003-1225-7084; Bhatti, Waqas/0000-0002-0628-0088; Nonino, Mario/0000-0001-6342-9662; Balestra, Italo/0000-0001-9660-894X; Scodeggio, Marco/0000-0002-2282-5850; Umetsu, Keiichi/0000-0002-7196-4822; Biviano, Andrea/0000-0002-0857-0732; Genel, Shy/0000-0002-3185-1540; Moustakas, Leonidas/0000-0003-3030-2360; Koekemoer, Anton/0000-0002-6610-2048; Benitez, Narciso/0000-0002-0403-7455; Voit, Gerard/0000-0002-3514-0383 FU NASA [HST-GO-12065.01-A]; PRIN INAF; ASI; Baden Wurttemberg Stiftung FX We thank Margaret J. Geller, Kenneth Rines, Michael Kurtz, and Antonaldo Diaferio for providing their redshift data for A611 and CL2130 and for providing the redshift data for A963, A2261, A1423, and RXJ2129 in advance of publication. We also thank them for many helpful discussions. In addition, we acknowledge very useful discussions with Ana Laura Serra, Dan Gifford, Mark Neyrinck, Yuval Birnboim, Eyal Neistein, and Maxim Markevitch. We thank the anonymous referee for useful comments. D. L. thanks Eran Ofek for his publicly available Matlab scripts. This research is supported in part by NASA grant HST-GO-12065.01-A. M. M. acknowledges support from PRIN INAF 2009 and ASI (agreement Euclid phase B2/C). A.Z. is supported by contract research "Internationale Spitzenforschung II/2-6" of the Baden Wurttemberg Stiftung. NR 102 TC 21 Z9 21 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 OCT 20 PY 2013 VL 776 IS 2 AR 91 DI 10.1088/0004-637X/776/2/91 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 255CF UT WOS:000327216100028 ER PT J AU Favre, C Cleeves, LI Bergin, EA Qi, CH Blake, GA AF Favre, Cecile Cleeves, L. Ilsedore Bergin, Edwin A. Qi, Chunhua Blake, Geoffrey A. TI A SIGNIFICANTLY LOW CO ABUNDANCE TOWARD THE TW Hya PROTOPLANETARY DISK: A PATH TO ACTIVE CARBON CHEMISTRY? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: abundances; protoplanetary disks; stars: formation ID PHOTON-DOMINATED REGIONS; SUB-DOPPLER MEASUREMENTS; SUBMILLIMETER ARRAY; ROTATIONAL SPECTRUM; INTERSTELLAR ICES; D/HD TRANSITION; TAURI STARS; DM-TAU; GAS; LINE AB In this Letter we report the CO abundance relative to H-2 derived toward the circumstellar disk of the T-Tauri star TW Hya from the HD (1-0) and (CO)-O-18 (2-1) emission lines. The HD (1-0) line was observed by the Herschel Space Observatory Photodetector Array Camera and Spectrometer whereas (CO)-O-18 (2-1) observations were carried out with the Submillimeter Array at a spatial resolution of 2 ''.8 x 1 ''.9 (corresponding to similar to 151 x 103 AU). In the disk's warm molecular layer (T > 20 K) we measure a disk-averaged gas-phase CO abundance relative to H-2 of chi(CO) = (0.1-3) x 10(-5), substantially lower than the canonical value of chi(CO) = 10(-4). We infer that the best explanation of this low.(CO) is the chemical destruction of CO followed by rapid formation of carbon chains, or perhaps CO2, that can subsequently freeze-out, resulting in the bulk mass of carbon locked up in ice grain mantles and oxygen in water. As a consequence of this likely time-dependent carbon sink mechanism, CO may be an unreliable tracer of H-2 gas mass. C1 [Favre, Cecile; Cleeves, L. Ilsedore; Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Favre, C (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM cfavre@umich.edu OI Cleeves, L. Ilsedore/0000-0003-2076-8001 FU National Science Foundation [1008800]; Smithsonian Institution; Academia Sinica FX We thank the anonymous referee for raising interesting issues. This work was supported by the National Science Foundation under grant 1008800. This Letter makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00001. SV and SMA data. 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 Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NR 44 TC 39 Z9 39 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 20 PY 2013 VL 776 IS 2 AR L38 DI 10.1088/2041-8205/776/2/L38 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 232JO UT WOS:000325490200021 ER PT J AU Fragos, T Lehmer, BD Naoz, S Zezas, A Basu-Zych, A AF Fragos, T. Lehmer, B. D. Naoz, S. Zezas, A. Basu-Zych, A. TI ENERGY FEEDBACK FROM X-RAY BINARIES IN THE EARLY UNIVERSE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dark ages, reionization, first stars; galaxies: high-redshift; galaxies: stellar content; stars: evolution; X-rays: binaries; X-rays: diffuse background ID REGULATED STAR-FORMATION; ACTIVE GALACTIC NUCLEI; LUMINOSITY FUNCTION; BLACK-HOLES; HIGH-REDSHIFT; GALAXIES; EVOLUTION; MASS; REIONIZATION; EMISSION AB X-ray photons, because of their long mean-free paths, can easily escape the galactic environments where they are produced, and interact at long distances with the intergalactic medium, potentially having a significant contribution to the heating and reionization of the early universe. The two most important sources of X-ray photons in the universe are active galactic nuclei (AGNs) and X-ray binaries (XRBs). In this Letter we use results from detailed, large scale population synthesis simulations to study the energy feedback of XRBs, from the first galaxies (z similar to 20) until today. We estimate that X-ray emission from XRBs dominates over AGN at z greater than or similar to 6-8. The shape of the spectral energy distribution of the emission from XRBs shows little change with redshift, in contrast to its normalization which evolves by similar to 4 orders ofmagnitude, primarily due to the evolution of the cosmic star-formation rate. However, the metallicity and the mean stellar age of a given XRB population affect significantly its X-ray output. Specifically, the X-ray luminosity from high-mass XRBs per unit of star-formation rate varies an order of magnitude going from solar metallicity to less than 10% solar, and the X-ray luminosity from low-mass XRBs per unit of stellar mass peaks at an age of similar to 300 Myr and then decreases gradually at later times, showing little variation for mean stellar ages greater than or similar to 3 Gyr. Finally, we provide analytical and tabulated prescriptions for the energy output of XRBs, that can be directly incorporated in cosmological simulations. C1 [Fragos, T.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fragos, T.; Naoz, S.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Lehmer, B. D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Lehmer, B. D.; Basu-Zych, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Zezas, A.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. RP Fragos, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tfragos@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016; OI Zezas, Andreas/0000-0001-8952-676X; Fragos, Tassos/0000-0003-1474-1523; Naoz, Smadar/0000-0002-9802-9279 FU CfA prize fellowship program; ITC prize fellowship program; NASA through an Einstein Postdoctoral Fellowship [PF2-130096] FX T.F. acknowledges support from the CfA and the ITC prize fellowship programs. S.N. is supported by NASA through an Einstein Postdoctoral Fellowship (contract PF2-130096). NR 41 TC 45 Z9 45 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 20 PY 2013 VL 776 IS 2 AR L31 DI 10.1088/2041-8205/776/2/L31 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 232JO UT WOS:000325490200014 ER PT J AU Geach, JE Hickox, RC Bleem, LE Brodwin, M Holder, GP Aird, KA Benson, BA Bhattacharya, S Carlstrom, JE Chang, CL Cho, HM Crawford, TM Crites, AT de Haan, T Dobbs, MA Dudley, J George, EM Hainline, KN Halverson, NW Holzapfel, WL Hoover, S Hou, Z Hrubes, JD Keisler, R Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D Marrone, DP McMahon, JJ Mehl, J Meyer, SS Millea, M Mohr, JJ Montroy, TE Myers, AD Padin, S Plagge, T Pryke, C Reichardt, CL Ruhl, JE Sayre, JT Schaffer, KK Shaw, L Shirokoff, E Spieler, HG Staniszewski, Z Stark, AA Story, KT van Engelen, A Vanderlinde, K Vieira, JD Williamson, R Zahn, O AF Geach, J. E. Hickox, R. C. Bleem, L. E. Brodwin, M. Holder, G. P. Aird, K. A. Benson, B. A. Bhattacharya, S. Carlstrom, J. E. Chang, C. L. Cho, H. -M. Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. Dudley, J. George, E. M. Hainline, K. N. Halverson, N. W. Holzapfel, W. L. Hoover, S. Hou, Z. Hrubes, J. D. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. Marrone, D. P. McMahon, J. J. Mehl, J. Meyer, S. S. Millea, M. Mohr, J. J. Montroy, T. E. Myers, A. D. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Ruhl, J. E. Sayre, J. T. Schaffer, K. K. Shaw, L. Shirokoff, E. Spieler, H. G. Staniszewski, Z. Stark, A. A. Story, K. T. van Engelen, A. Vanderlinde, K. Vieira, J. D. Williamson, R. Zahn, O. TI A DIRECT MEASUREMENT OF THE LINEAR BIAS OF MID-INFRARED-SELECTED QUASARS AT z approximate to 1 USING COSMIC MICROWAVE BACKGROUND LENSING SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations ID ACTIVE GALACTIC NUCLEI; SOUTH-POLE TELESCOPE; DIGITAL SKY SURVEY; BOOTES FIELD; DARK-MATTER; MIDINFRARED SELECTION; LUMINOSITY FUNCTION; BLACK-HOLES; GALAXIES; EVOLUTION AB We measure the cross-power spectrum of the projected mass density as traced by the convergence of the cosmic microwave background lensing field from the South Pole Telescope (SPT) and a sample of Type 1 and 2 (unobscured and obscured) quasars at < z > similar to 1 selected with the Wide-field Infrared Survey Explorer, over 2500 deg(2). The cross-power spectrum is detected at approximate to 7 sigma, and we measure a linear bias b = 1.61 +/- 0.22, consistent with clustering analyses. Using an independent lensing map, derived from Planck observations, to measure the cross-spectrum, we find excellent agreement with the SPT analysis. The bias of the combined sample of Type 1 and 2 quasars determined in this work is similar to that previously determined for Type 1 quasars alone; we conclude that obscured and unobscured quasars trace the matter field in a similar way. This result has implications for our understanding of quasar unification and evolution schemes. C1 [Geach, J. E.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. [Geach, J. E.; Holder, G. P.; de Haan, T.; Dobbs, M. A.; Dudley, J.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Hickox, R. C.; Hainline, K. N.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Bleem, L. E.; Benson, B. A.; Bhattacharya, S.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Hoover, S.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K. T.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Keisler, R.; Meyer, S. S.; Story, K. T.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bleem, L. E.; Bhattacharya, S.; Carlstrom, J. E.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60440 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Meyer, S. S.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Cho, H. -M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Univ, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Myers, A. D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82072 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA. RP Geach, JE (reprint author), Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. EM j.geach@herts.ac.uk RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU NSF [ANT-0638937, ANT-0130612, 1211096, 1211112, PHYS-1066293]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NASA through ADAP [NNX12AE38G]; NSERC; CIfAR; Canada Research Chairs program; Office of Science of the U.S. DoE [DE-AC02-05CH11231]; ESA Member States; NASA FX SPT is supported by the NSF through grants ANT-0638937 and ANT-0130612. Support for this work is provided by: the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago; the Kavli Foundation and the Gordon and Betty Moore Foundation; NSF (grant numbers 1211096, 1211112 and PHYS-1066293); NASA through ADAP award NNX12AE38G; NSERC, CIfAR, and the Canada Research Chairs program. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. DoE under contract DE-AC02-05CH11231. Research at Argonne National Laboratory is supported by the Office of Science of the U.S. DoE under contract DE-AC02-06CH11357. Planck is an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada. NR 38 TC 26 Z9 26 U1 1 U2 8 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 OCT 20 PY 2013 VL 776 IS 2 AR L41 DI 10.1088/2041-8205/776/2/L41 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 232JO UT WOS:000325490200024 ER PT J AU Detto, M Muller-Landau, HC Mascaro, J Asner, GP AF Detto, Matteo Muller-Landau, Helene C. Mascaro, Joseph Asner, Gregory P. TI Hydrological Networks and Associated Topographic Variation as Templates for the Spatial Organization of Tropical Forest Vegetation SO PLOS ONE LA English DT Article ID DIGITAL ELEVATION DATA; ABOVEGROUND BIOMASS; AMAZONIAN FOREST; CARBON STOCKS; RAIN-FOREST; PUERTO-RICO; PATTERNS; SCALE; DISTURBANCE; LANDSCAPE AB An understanding of the spatial variability in tropical forest structure and biomass, and the mechanisms that underpin this variability, is critical for designing, interpreting, and upscaling field studies for regional carbon inventories. We investigated the spatial structure of tropical forest vegetation and its relationship to the hydrological network and associated topographic structure across spatial scales of 10-1000 m using high-resolution maps of LiDAR-derived mean canopy profile height (MCH) and elevation for 4930 ha of tropical forest in central Panama. MCH was strongly associated with the hydrological network: canopy height was highest in areas of positive convexity (valleys, depressions) close to channels draining 1 ha or more. Average MCH declined strongly with decreasing convexity (transition to ridges, hilltops) and increasing distance from the nearest channel. Spectral analysis, performed with wavelet decomposition, showed that the variance in MCH had fractal similarity at scales of similar to 30-600 m, and was strongly associated with variation in elevation, with peak correlations at scales of similar to 250 m. Whereas previous studies of topographic correlates of tropical forest structure conducted analyses at just one or a few spatial grains, our study found that correlations were strongly scale-dependent. Multi-scale analyses of correlations of MCH with slope, aspect, curvature, and Laplacian convexity found that MCH was most strongly related to convexity measured at scales of 20-300 m, a topographic variable that is a good proxy for position with respect to the hydrological network. Overall, our results support the idea that, even in these mesic forests, hydrological networks and associated topographical variation serve as templates upon which vegetation is organized over specific ranges of scales. These findings constitute an important step towards a mechanistic understanding of these patterns, and can guide upscaling and downscaling. C1 [Detto, Matteo; Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Panama City, Panama. [Mascaro, Joseph; Asner, Gregory P.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA USA. RP Detto, M (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM dettom@si.edu RI Asner, Gregory/G-9268-2013 OI Asner, Gregory/0000-0001-7893-6421 FU Smithsonian Institution Global Earth Observatories; HSBC Climate Partnership; National Science Foundation [DEB 0614055] FX This work was supported by the Smithsonian Institution Global Earth Observatories and the HSBC Climate Partnership. The Carnegie Airborne Observatory is made possible by the Gordon and Betty Moore Foundation, the John D. and Catherine T. MacArthur Foundation, Avatar Alliance Foundation, W. M. Keck Foundation, the Margaret A. Cargill Foundation, Grantham Foundation for the Protection of the Environment, Mary Anne Nyburg Baker and G. Leonard Baker Jr., and William R. Hearst III. This material is based upon work supported by the National Science Foundation under Grant Number DEB 0614055. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 58 TC 14 Z9 14 U1 1 U2 32 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD OCT 18 PY 2013 VL 8 IS 10 AR e76296 DI 10.1371/journal.pone.0076296 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 239MM UT WOS:000326029300018 PM 24204610 ER PT J AU Li, R Ma, PF Wen, J Yi, TS AF Li, Rong Ma, Peng-Fei Wen, Jun Yi, Ting-Shuang TI Complete Sequencing of Five Araliaceae Chloroplast Genomes and the Phylogenetic Implications SO PLOS ONE LA English DT Article ID COMPLETE NUCLEOTIDE-SEQUENCE; PLASTID GENOMES; MAXIMUM-LIKELIHOOD; SCALE DATA; EVOLUTION; DNA; GENES; MITOCHONDRIAL; ANGIOSPERMS; NUCLEAR AB Background: The ginseng family (Araliaceae) includes a number of economically important plant species. Previously phylogenetic studies circumscribed three major clades within the core ginseng plant family, yet the internal relationships of each major group have been poorly resolved perhaps due to rapid radiation of these lineages. Recent studies have shown that phyogenomics based on chloroplast genomes provides a viable way to resolve complex relationships. Methodology/Principal Findings: We report the complete nucleotide sequences of five Araliaceae chloroplast genomes using next-generation sequencing technology. The five chloroplast genomes are 156,333-156,459 bp in length including a pair of inverted repeats (25,551-26,108 bp) separated by the large single-copy (86,028-86,566 bp) and small single-copy (18,021-19,117 bp) regions. Each chloroplast genome contains the same 114 unique genes consisting of 30 transfer RNA genes, four ribosomal RNA genes, and 80 protein coding genes. Gene size, content, and order, AT content, and IR/SC boundary structure are similar among all Araliaceae chloroplast genomes. A total of 140 repeats were identified in the five chloroplast genomes with palindromic repeat as the most common type. Phylogenomic analyses using parsimony, likelihood, and Bayesian inference based on the complete chloroplast genomes strongly supported the monophyly of the Asian Palmate group and the Aralia-Panax group. Furthermore, the relationships among the sampled taxa within the Asian Palmate group were well resolved. Twenty-six DNA markers with the percentage of variable sites higher than 5% were identified, which may be useful for phylogenetic studies of Araliaceae. Conclusion: The chloroplast genomes of Araliaceae are highly conserved in all aspects of genome features. The large-scale phylogenomic data based on the complete chloroplast DNA sequences is shown to be effective for the phylogenetic reconstruction of Araliaceae. C1 [Li, Rong; Ma, Peng-Fei; Yi, Ting-Shuang] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming, Yunnan, Peoples R China. [Li, Rong; Ma, Peng-Fei; Yi, Ting-Shuang] Chinese Acad Sci, Kunming Inst Bot, Germplasm Bank Wild Species, Plant Germplasm & Genom Ctr, Kunming, Yunnan, Peoples R China. [Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Wen, J (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. EM wenj@si.edu; tingshuangyi@mail.kib.ac.cn FU Knowledge Innovation Engineering Program of the Chinese Academy of Sciences [KSCX2-EW-J-24]; Talent Project of Yunnan Province [2011CI042]; Open Fund of Key Laboratory of Biodiversity and Biogeography, Kunming Institute of Botany, Chinese Academy of Sciences [KLBB201204] FX This project is supported by the Knowledge Innovation Engineering Program of the Chinese Academy of Sciences (grant no. KSCX2-EW-J-24), the Talent Project of Yunnan Province (grant no. 2011CI042), and the Open Fund of Key Laboratory of Biodiversity and Biogeography, Kunming Institute of Botany, Chinese Academy of Sciences (grant no. KLBB201204). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 64 TC 15 Z9 17 U1 0 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 OCT 18 PY 2013 VL 8 IS 10 AR UNSP e78568 DI 10.1371/journal.pone.0078568 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 239MM UT WOS:000326029300159 PM 24205264 ER PT J AU ter Steege, H Nigel, CA Sabatier, D Baraloto, C Salomao, RP Guevara, JE Phillips, OL Castilho, CV Magnusson, WE Molino, JF Monteagudo, A Vargas, PN Montero, JC Feldpausch, TR Coronado, ENH Killeen, TJ Mostacedo, B Vasquez, R Assis, RL Terborgh, J Wittmann, F Andrade, A Laurance, WF Laurance, SGW Marimon, BS Marimon, BH Vieira, ICG Amaral, IL Brienen, R Castellanos, H Lopez, DC Duivenvoorden, JF Mogollon, HF Matos, FDD Davila, N Garcia-Villacorta, R Diaz, PRS Costa, F Emilio, T Levis, C Schietti, J Souza, P Alonso, A Dallmeier, F Montoya, AJD Piedade, MTF Araujo-Murakami, A Arroyo, L Gribel, R Fine, PVA Peres, CA Toledo, M Gerardo, AAC Baker, TR Ceron, C Engel, J Henkel, TW Maas, P Petronelli, P Stropp, J Zartman, CE Daly, D Neill, D Silveira, M Paredes, MR Chave, J Lima, DD Jorgensen, PM Fuentes, A Schongart, J Valverde, FC Di Fiore, A Jimenez, EM Mora, MCP Phillips, JF Rivas, G van Andel, TR von Hildebrand, P Hoffman, B Zent, EL Malhi, Y Prieto, A Rudas, A Ruschell, AR Silva, N Vos, V Zent, S Oliveira, AA Schutz, AC Gonzales, T Nascimento, MT Ramirez-Angulo, H Sierra, R Tirado, M Medina, MNU van der Heijden, G Vela, CIA Torre, EV Vriesendorp, C Wang, O Young, KR Baider, C Balslev, H Ferreira, C Mesones, I Torres-Lezama, A Giraldo, LEU Zagt, R Alexiades, MN Hernandez, L Huamantupa-Chuquimaco, I Milliken, W Cuenca, WP Pauletto, D Sandoval, EV Gamarra, LV Dexter, KG Feeley, K Lopez-Gonzalez, G Silman, MR AF ter Steege, Hans Pitman, Nigel C. A. Sabatier, Daniel Baraloto, Christopher Salomao, Rafael P. Guevara, Juan Ernesto Phillips, Oliver L. Castilho, Carolina V. Magnusson, William E. Molino, Jean-Franois Monteagudo, Abel Nunez Vargas, Percy Carlos Montero, Juan Feldpausch, Ted R. Coronado, Euridice N. Honorio Killeen, Tim J. Mostacedo, Bonifacio Vasquez, Rodolfo Assis, Rafael L. Terborgh, John Wittmann, Florian Andrade, Ana Laurance, William F. Laurance, Susan G. W. Marimon, Beatriz S. Marimon, Ben-Hur, Jr. Guimaraes Vieira, Ima Celia Amaral, Ieda Leao Brienen, Roel Castellanos, Hernan Cardenas Lopez, Dairon Duivenvoorden, Joost F. Mogollon, Hugo F. de Almeida Matos, Francisca Dionizia Davila, Nallarett Garcia-Villacorta, Roosevelt Stevenson Diaz, Pablo Roberto Costa, Flavia Emilio, Thaise Levis, Carolina Schietti, Juliana Souza, Priscila Alonso, Alfonso Dallmeier, Francisco Duque Montoya, Alvaro Javier Fernandez Piedade, Maria Teresa Araujo-Murakami, Alejandro Arroyo, Luzmila Gribel, Rogerio Fine, Paul V. A. Peres, Carlos A. Toledo, Marisol Gerardo, A. Aymard C. Baker, Tim R. Ceron, Carlos Engel, Julien Henkel, Terry W. Maas, Paul Petronelli, Pascal Stropp, Juliana Eugene Zartman, Charles Daly, Doug Neill, David Silveira, Marcos Rios Paredes, Marcos Chave, Jerome de Andrade Lima, Diogenes Jorgensen, Peter Moller Fuentes, Alfredo Schoengart, Jochen Cornejo Valverde, Fernando Di Fiore, Anthony Jimenez, Eliana M. Penuela Mora, Maria Cristina Fernando Phillips, Juan Rivas, Gonzalo van Andel, Tinde R. von Hildebrand, Patricio Hoffman, Bruce Zent, Eglee L. Malhi, Yadvinder Prieto, Adriana Rudas, Agustin Ruschell, Ademir R. Silva, Natalino Vos, Vincent Zent, Stanford Oliveira, Alexandre A. Cano Schutz, Angela Gonzales, Therany Nascimento, Marcelo Trindade Ramirez-Angulo, Hirma Sierra, Rodrigo Tirado, Milton Umana Medina, Maria Natalia van der Heijden, Geertje Vela, Cesar I. A. Vilanova Torre, Emilio Vriesendorp, Corine Wang, Ophelia Young, Kenneth R. Baider, Claudia Balslev, Henrik Ferreira, Cid Mesones, Italo Torres-Lezama, Armando Urrego Giraldo, Ligia Estela Zagt, Roderick Alexiades, Miguel N. Hernandez, Lionel Huamantupa-Chuquimaco, Isau Milliken, William Palacios Cuenca, Walter Pauletto, Daniela Valderrama Sandoval, Elvis Valenzuela Gamarra, Luis Dexter, Kyle G. Feeley, Ken Lopez-Gonzalez, Gabriela Silman, Miles R. TI Hyperdominance in the Amazonian Tree Flora SO SCIENCE LA English DT Article ID SPECIES ABUNDANCE; TROPICAL FOREST; RAIN-FOREST; GO EXTINCT; DISTRIBUTIONS; PATTERNS; DIVERSIFICATION; DIVERSITY; RARITY; PLANTS AB The vast extent of the Amazon Basin has historically restricted the study of its tree communities to the local and regional scales. Here, we provide empirical data on the commonness, rarity, and richness of lowland tree species across the entire Amazon Basin and Guiana Shield (Amazonia), collected in 1170 tree plots in all major forest types. Extrapolations suggest that Amazonia harbors roughly 16,000 tree species, of which just 227 (1.4%) account for half of all trees. Most of these are habitat specialists and only dominant in one or two regions of the basin. We discuss some implications of the finding that a small group of species-less diverse than the North American tree flora-accounts for half of the world's most diverse tree community. C1 [ter Steege, Hans; Maas, Paul; van Andel, Tinde R.; Hoffman, Bruce] Naturalis Biodivers Ctr, Leiden, Netherlands. [ter Steege, Hans] Univ Utrecht, Ecol & Biodivers Grp, NL-3508 TC Utrecht, Netherlands. [Pitman, Nigel C. A.; Terborgh, John] Duke Univ, Ctr Trop Conservat, Nicholas Sch Environm, Durham, NC 27708 USA. [Pitman, Nigel C. A.; Vriesendorp, Corine] Field Museum, Chicago, IL 60605 USA. [Sabatier, Daniel; Molino, Jean-Franois] Inst Dev Res, UMR Architecture Fonctionnement & Evolut Plantes, Montpellier, France. [Salomao, Rafael P.] Museu Paraense Emilio Goeldi Cordenadoria Bot, Minist Ciencia Tecnol & Inovacao, Belem, Para, Brazil. [Guevara, Juan Ernesto; Fine, Paul V. A.; Mesones, Italo] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Phillips, Oliver L.; Feldpausch, Ted R.; Coronado, Euridice N. Honorio; Brienen, Roel; Baker, Tim R.; Lopez-Gonzalez, Gabriela] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. [Castilho, Carolina V.] Embrapa Roraima, Boa Vista, RR, Brazil. [Magnusson, William E.; Carlos Montero, Juan; Assis, Rafael L.; de Almeida Matos, Francisca Dionizia; Costa, Flavia; Emilio, Thaise; Levis, Carolina; Schietti, Juliana; Souza, Priscila; Fernandez Piedade, Maria Teresa; Eugene Zartman, Charles; de Andrade Lima, Diogenes; Ferreira, Cid] Inst Nacl de Pesquisas da Amazonia, Manaus, Amazonas, Brazil. [Monteagudo, Abel; Vasquez, Rodolfo; Valenzuela Gamarra, Luis] Jardin Bot Missouri, Oxapampa, Peru. [Nunez Vargas, Percy] Univ Nacl San Antonio Abad del Cusco, Cuzco, Peru. [Carlos Montero, Juan] BOLFOR Bolivia Sustainable Forest Management Proj, Casilla 6204, Santa Cruz, Bolivia. [Feldpausch, Ted R.] Univ Exeter, Coll Life & Environm Sci, Exeter EX4 4RJ, Devon, England. [Coronado, Euridice N. Honorio] Inst Invest Amazonia Peruana, Iquitos, Peru. [Killeen, Tim J.] WWF, Washington, DC 20037 USA. [Mostacedo, Bonifacio] Univ Autonoma Gabriel Rene Moreno, Fac Ciencias Agr, Santa Cruz, Bolivia. [Assis, Rafael L.] Norwegian Univ Life Sci UMB, Dept Ecol & Nat Resource Management, As, Norway. [Wittmann, Florian; Schoengart, Jochen] Max Planck Inst Chem, D-55128 Mainz, Germany. [Andrade, Ana] Inst Nacl de Pesquisas da Amazonia, Projeto Dinam Biol Fragmentos Florestais, Manaus, Amazonas, Brazil. [Laurance, William F.] James Cook Univ, Ctr Trop Environm & Sustainabil Sci TESS, Cairns, Qld, Australia. [Laurance, William F.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld, Australia. [Laurance, Susan G. W.; Marimon, Beatriz S.; Marimon, Ben-Hur, Jr.] Univ Estado Mato Grosso, Nova Xavantina, MT, Brazil. [Guimaraes Vieira, Ima Celia] Museu Paraense Emilio Goeldi, Belem, Para, Brazil. [Amaral, Ieda Leao] INPA, Projeto TEAM Trop Ecol Assessment & Monitoring Ma, Manaus, Amazonas, Brazil. [Castellanos, Hernan; Hernandez, Lionel] Univ Nacl Expt Guayana, Puerto Ordaz, Bolivar, Venezuela. [Cardenas Lopez, Dairon] SINCHI Inst Amazon Invest Cient, Bogota, Colombia. [Duivenvoorden, Joost F.] Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, Amsterdam, Netherlands. [Mogollon, Hugo F.] Endangered Species Coalit, Silver Spring, MD 20901 USA. [Davila, Nallarett] Univ Estadual Campinas, Campinas, SP, Brazil. [Garcia-Villacorta, Roosevelt] Univ Edinburgh, Inst Mol Plant Sci, Edinburgh EH9 3JH, Midlothian, Scotland. [Garcia-Villacorta, Roosevelt] Royal Bot Garden Edinburgh, Edinburgh EH3 5LR, Midlothian, Scotland. [Stevenson Diaz, Pablo Roberto; Cano Schutz, Angela; Umana Medina, Maria Natalia] Univ Los Andes, Lab Ecol Bosques Trop & Primatol, Bogota, DF, Colombia. [Alonso, Alfonso; Dallmeier, Francisco] Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Duque Montoya, Alvaro Javier; Urrego Giraldo, Ligia Estela] Univ Nacl Colombia, Dept Ciencias Forest, Sede Medellin, Colombia. [Araujo-Murakami, Alejandro; Arroyo, Luzmila] Museo Hist Nat Noel Kempff Mercado, Santa Cruz, Bolivia. [Gribel, Rogerio] Inst Pesquisas Jardim Bot Rio de Janeiro, Rio De Janeiro, Brazil. [Peres, Carlos A.] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England. [Toledo, Marisol] Univ Autonoma Gabriel Rene Moreno, Inst Boliviano Invest Forestal, Santa Cruz, Bolivia. [Ceron, Carlos] Univ Cent Ecuador, Herbario Alfredo Paredes QAP, Quito, Ecuador. [Henkel, Terry W.] Humboldt State Univ, Dept Biol Sci, Arcata, CA 95521 USA. [Petronelli, Pascal] La Rech Agron Dev CIRAD, UMR Ecofog, Kourou, French Guiana. [Stropp, Juliana] Commiss European Communities, Land Resource & Management Unit, Joint Res Ctr, I-21027 Ispra, VA, Italy. [Daly, Doug] New York Bot Garden, Bronx, NY 10458 USA. [Neill, David] Univ Estatal Amaz, Puyo, Ecuador. [Silveira, Marcos] Univ Fed Acre, Museu Univ, Rio Branco, AC, Brazil. [Rios Paredes, Marcos] Serv Biodiversidad EIRL, Iquitos, Peru. [Chave, Jerome] CNRS, F-31000 Toulouse, France. [Chave, Jerome] Univ Toulouse 3, UMR EDB 5174, F-31000 Toulouse, France. [Jorgensen, Peter Moller; Fuentes, Alfredo] Missouri Bot Garden, St Louis, MO 63166 USA. [Fuentes, Alfredo] Herbario Nacl Bolivia, La Paz, Bolivia. [Cornejo Valverde, Fernando] Andes Amazon Biodivers Program, Madre De Dios, Peru. [Di Fiore, Anthony] Univ Texas Austin, Dept Anthropol, Austin, TX 78712 USA. [Jimenez, Eliana M.; Penuela Mora, Maria Cristina] Univ Nacl Colombia Sede Amazonia, Grp Ecol Ecosistemas Terrestres Trop, Leticia, Amazonas, Brazil. [Fernando Phillips, Juan; von Hildebrand, Patricio] Fdn Puerto Rastrojo, Bogota, Colombia. [Rivas, Gonzalo] Univ Florida, Gainesville, FL 32611 USA. [Zent, Eglee L.; Zent, Stanford] Inst Venezolano Invest Cient, Lab Human Ecol, Caracas 1020A, Venezuela. [Malhi, Yadvinder] Univ Oxford, Environm Change Inst, Sch Geog & Environm, Oxford, England. [Prieto, Adriana; Rudas, Agustin] Univ Nacl Colombia, Inst Ciencias Nat, Bogota, Colombia. [Ruschell, Ademir R.] Embrapa Amazonia Oriental, Belem, Para, Brazil. [Silva, Natalino] Univ Fed Rural Amazonia, Belem, Para, Brazil. [Vos, Vincent] Univ Autonoma Beni, Riberalta, Bolivia. [Oliveira, Alexandre A.; Baider, Claudia] Univ Sao Paulo, Inst Biociencias, Dept Ecol, Sao Paulo, Brazil. [Gonzales, Therany] Amazon Ctr Environm Educ & Res Fdn, Madre De Dios, Peru. [Nascimento, Marcelo Trindade] Univ Estadual Norte Fluminense, Lab Ciencias Ambientais, BR-28013620 Campos Dos Goyatacazes, RJ, Brazil. [Ramirez-Angulo, Hirma; Vilanova Torre, Emilio] Univ Los Andes, INDEFOR Res Inst Forestry Dev, Merida, Venezuela. [Sierra, Rodrigo; Tirado, Milton] Geoinformat & Sistemas Cia Ltda GeoIS, Quito, Ecuador. [van der Heijden, Geertje] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53202 USA. [van der Heijden, Geertje] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Vela, Cesar I. A.] Univ Nacl San Antonio Abad del Cusco, Fac Ciencias Forest & Medio Ambiente, Puerto Maldonado, Madre De Dios, Peru. [Wang, Ophelia] No Arizona Univ, Flagstaff, AZ 86011 USA. [Young, Kenneth R.] Univ Texas Austin, Austin, TX 78712 USA. [Baider, Claudia] Minist Agro Ind & Food Secur, Mauritius Herbarium Agr Serv, Reduit, Mauritius. [Balslev, Henrik] Univ Aarhus, Aarhus, Denmark. [Torres-Lezama, Armando] Univ Los Andes, Merida, Venezuela. [Zagt, Roderick] Tropenbos Int, Wageningen, Netherlands. [Alexiades, Miguel N.] Univ Kent, Sch Anthropol & Conservat, Canterbury CT2 7NR, Kent, England. [Huamantupa-Chuquimaco, Isau] Univ Nacl San Antonio Abad del Cusco, Herbario CUZ, Cuzco, Peru. [Milliken, William] Royal Bot Gardens, Richmond TW9 3AB, Surrey, England. [Palacios Cuenca, Walter] Univ Tecn Norte Herbario Nacl Euador, Quito, Ecuador. [Pauletto, Daniela] Serv Florestal Brasileiro, Santarem, PA, Brazil. [Valderrama Sandoval, Elvis] Univ Missouri, Dept Biol, St Louis, MO 63121 USA. [Valderrama Sandoval, Elvis] Univ Nacl Amazonia Peruana, Fac Biol, Iquitos, Peru. [Dexter, Kyle G.] Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JN, Midlothian, Scotland. [Feeley, Ken] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. [Feeley, Ken] Fairchild Trop Bot Garden, Coral Gables, FL 33156 USA. [Silman, Miles R.] Wake Forest Univ, Biol Dept, Winston Salem, NC 27106 USA. [Silman, Miles R.] Wake Forest Univ, Ctr Energy Environm & Sustainabil, Winston Salem, NC 27106 USA. RP ter Steege, H (reprint author), Naturalis Biodivers Ctr, Leiden, Netherlands. EM hans.tersteege@naturalis.nl RI ter Steege, Amaz/B-5866-2011; Oliveira, Alexandre/G-8830-2012; Feeley, Kenneth/A-7631-2009; Phillips, Oliver/A-1523-2011; James Cook University, TESS/B-8171-2012; Nascimento, Marcelo/D-2824-2013; Balslev, Henrik/J-9191-2013; Feldpausch, Ted/D-3436-2009; Silveira, Marcos/H-7906-2013; Magnusson, William/J-9408-2014; Marimon Junior, Ben Hur/E-7330-2013; Piedade, Maria Teresa/C-5372-2013; Research ID, CTBCC /O-3564-2014; Schietti, Juliana/B-8226-2015; icmol, icmol/I-5784-2015; Laurance, Susan/G-6021-2011; Honorio Coronado, Euridice/K-3412-2015; Gribel, Rogerio/C-5392-2013; Peres, Carlos/B-1276-2013; Schongart, Jochen/I-2659-2016; Marimon, Beatriz/J-6389-2012; OI ter Steege, Amaz/0000-0002-8738-2659; Oliveira, Alexandre/0000-0001-5526-8109; Phillips, Oliver/0000-0002-8993-6168; Nascimento, Marcelo/0000-0003-4492-3344; Balslev, Henrik/0000-0002-7101-7120; Feldpausch, Ted/0000-0002-6631-7962; Silveira, Marcos/0000-0003-0485-7872; Piedade, Maria Teresa/0000-0002-7320-0498; Vos, Vincent Antoine/0000-0002-0388-8530; Fine, Paul/0000-0002-0550-5628; Schietti, Juliana/0000-0002-1687-4373; Laurance, Susan/0000-0002-2831-2933; Honorio Coronado, Euridice/0000-0003-2314-590X; Gribel, Rogerio/0000-0002-0850-5578; Peres, Carlos/0000-0002-1588-8765; Valenzuela Gamarra, Luis/0000-0002-6191-0580 FU Alberta Mennega Stichting; ALCOA Suriname; Banco de la Republica; Center for Agricultural Research in Suriname; Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (Plano Nacional de Pos-Graduacao); Conselho Nacional de Desenvovimento Cientifico e Tecnologico of Brazil (CNPq) projects Programa de Pesquisas Ecologicas de Longa Duracao (PELD) [558069/2009-6]; Programa de Apoio a Nucleos de Excelencia da Fundacao de Amparo a Pesquisa do Estado do Amazonas (PRONEX-FAPEAM) [1600/2006]; Areas Umidas; MAUA; PELD [403792/2012-6]; PPBio; CENBAM; Universal [479599/2008-4, 307807-2009-6]; Fundacao de Amparo A Pesquisa Do Estado Do Amazonas (APEAM) projects [DCR/2006]; Hidroveg; FAPESP; PRONEX; CNPq; Colciencias; Duke University; Ecopetrol; FEPIM [044/2003]; Field Museum; Conservation International/DC (TEAM/INPA Manuas), Gordon; Betty Moore Foundation; Guyana Forestry Commission; Investissement d'Avenir grant of the French Agence Nationale de la Recherche (ANR) (Centre d'Etude de la Biodiversite Amazonienne) [ANR-10-LABX-0025]; Margaret Mee Amazon Trust; Miquel fonds; National Geographic Society [7754-04, 8047-06]; Netherlands Foundation for the Advancement of Tropical Research WOTRO grants [WB85- 335, W84-581]; Primate Conservation Incorporated; French Ministry of Ecology and Sustainable Development; Shell Prospecting and Development Peru; Smithsonian Institution's Biological Diversity of the Guiana Shield Program; Stichting het van Eeden-fonds; the Body Shop; Ministry of the Environment of Ecuador; TROBIT; Tropenbos International; NSF [NSF-0743457, NSF-0101775]; USAID; Variety Woods Guyana; WWF-Brazil; WWF-Guianas; XIIeme Contrat de Plan Etat Region-Guyane (French Government and European Union); European Union; UK Natural Environment Research Council; Gordon and Betty Moore Foundation; U.S. National Geographic Society; European Research Council Advanced Grant; Royal Society Wolfson Research Merit Award FX This paper is the result of the work of hundreds of different scientists and research institutions in the Amazon over the past 80 years. Without their hard work this analysis would have been impossible. This work was supported by Alberta Mennega Stichting; ALCOA Suriname; Banco de la Republica; Center for Agricultural Research in Suriname; Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (Plano Nacional de Pos-Graduacao); Conselho Nacional de Desenvovimento Cientifico e Tecnologico of Brazil (CNPq) projects Programa de Pesquisas Ecologicas de Longa Duracao (PELD) (558069/2009-6), Programa de Apoio a Nucleos de Excelencia da Fundacao de Amparo a Pesquisa do Estado do Amazonas (PRONEX-FAPEAM) (1600/2006), Areas Umidas, and MAUA; PELD (403792/2012-6), PPBio, CENBAM, Universal (479599/2008-4), and Universal 307807-2009-6; Fundacao de Amparo A Pesquisa Do Estado Do Amazonas (APEAM) projects DCR/2006, Hidroveg with FAPESP, and PRONEX with CNPq; FAPESP; Colciencias; Duke University; Ecopetrol; FEPIM 044/2003; the Field Museum; Conservation International/DC (TEAM/INPA Manuas), Gordon and Betty Moore Foundation; Guyana Forestry Commission; Investissement d'Avenir grant of the French Agence Nationale de la Recherche (ANR) (Centre d'Etude de la Biodiversite Amazonienne ANR-10-LABX-0025); Margaret Mee Amazon Trust; Miquel fonds; National Geographic Society (7754-04, 8047-06 to P.M.J.); Netherlands Foundation for the Advancement of Tropical Research WOTRO grants WB85- 335 and W84-581; Primate Conservation Incorporated; Programme Ecosystemes Tropicaux (French Ministry of Ecology and Sustainable Development; Shell Prospecting and Development Peru; Smithsonian Institution's Biological Diversity of the Guiana Shield Program; Stichting het van Eeden-fonds; the Body Shop; the Ministry of the Environment of Ecuador; TROBIT; Tropenbos International; NSF (NSF-0743457 and NSF-0101775 to P.M.J.); USAID; Variety Woods Guyana; WWF-Brazil; WWF-Guianas; XIIeme Contrat de Plan Etat Region-Guyane (French Government and European Union); and grants to RAINFOR from the European Union, UK Natural Environment Research Council, the Gordon and Betty Moore Foundation, and U.S. National Geographic Society. O.L.P. is supported by a European Research Council Advanced Grant and a Royal Society Wolfson Research Merit Award. A summary of the data is given in appendix 1. Plot metadata are given in appendix 4. NR 46 TC 168 Z9 176 U1 29 U2 247 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 OCT 18 PY 2013 VL 342 IS 6156 BP 325 EP + DI 10.1126/science.1243092 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 235XG UT WOS:000325755100034 ER PT J AU Huber, D Carter, JA Barbieri, M Miglio, A Deck, KM Fabrycky, DC Montet, BT Buchhave, LA Chaplin, WJ Hekker, S Montalban, J Sanchis-Ojeda, R Basu, S Bedding, TR Campante, TL Christensen-Dalsgaard, J Elsworth, YP Stello, D Arentoft, T Ford, EB Gilliland, RL Handberg, R Howard, AW Isaacson, H Johnson, JA Karoff, C Kawaler, SD Kjeldsen, H Latham, DW Lund, MN Lundkvist, M Marcy, GW Metcalfe, TS Aguirre, VS Winn, JN AF Huber, Daniel Carter, Joshua A. Barbieri, Mauro Miglio, Andrea Deck, Katherine M. Fabrycky, Daniel C. Montet, Benjamin T. Buchhave, Lars A. Chaplin, William J. Hekker, Saskia Montalban, Josefina Sanchis-Ojeda, Roberto Basu, Sarbani Bedding, Timothy R. Campante, Tiago L. Christensen-Dalsgaard, Jorgen Elsworth, Yvonne P. Stello, Dennis Arentoft, Torben Ford, Eric B. Gilliland, Ronald L. Handberg, Rasmus Howard, Andrew W. Isaacson, Howard Johnson, John Asher Karoff, Christoffer Kawaler, Steven D. Kjeldsen, Hans Latham, David W. Lund, Mikkel N. Lundkvist, Mia Marcy, Geoffrey W. Metcalfe, Travis S. Aguirre, Victor Silva Winn, Joshua N. TI Stellar Spin-Orbit Misalignment in a Multiplanet System SO SCIENCE LA English DT Article ID RED-GIANT STARS; EXOPLANETARY SYSTEMS; PLANETARY SYSTEM; ROTATION AXIS; HOT STARS; ALIGNMENT; KEPLER; OBLIQUITIES; MODES; TRANSIT AB Stars hosting hot Jupiters are often observed to have high obliquities, whereas stars with multiple coplanar planets have been seen to have low obliquities. This has been interpreted as evidence that hot-Jupiter formation is linked to dynamical disruption, as opposed to planet migration through a protoplanetary disk. We used asteroseismology to measure a large obliquity for Kepler-56, a red giant star hosting two transiting coplanar planets. These observations show that spin-orbit misalignments are not confined to hot-Jupiter systems. Misalignments in a broader class of systems had been predicted as a consequence of torques from wide-orbiting companions, and indeed radial velocity measurements revealed a third companion in a wide orbit in the Kepler-56 system. C1 [Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Carter, Joshua A.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barbieri, Mauro] Univ Padua, CISAS, I-35131 Padua, Italy. [Miglio, Andrea; Chaplin, William J.; Campante, Tiago L.; Elsworth, Yvonne P.; Handberg, Rasmus] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Miglio, Andrea; Chaplin, William J.; Bedding, Timothy R.; Campante, Tiago L.; Christensen-Dalsgaard, Jorgen; Elsworth, Yvonne P.; Stello, Dennis; Arentoft, Torben; Handberg, Rasmus; Karoff, Christoffer; Kjeldsen, Hans; Lund, Mikkel N.; Lundkvist, Mia; Metcalfe, Travis S.; Aguirre, Victor Silva] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Deck, Katherine M.; Sanchis-Ojeda, Roberto; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Montet, Benjamin T.; Johnson, John Asher] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Hekker, Saskia] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Montalban, Josefina] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Bedding, Timothy R.; Stello, Dennis] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Ford, Eric B.; Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Isaacson, Howard; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Metcalfe, Travis S.] Space Sci Inst, Boulder, CO 80301 USA. RP Huber, D (reprint author), NASA, Ames Res Ctr, MS 244-30, Moffett Field, CA 94035 USA. EM daniel.huber@nasa.gov RI Karoff, Christoffer/L-1007-2013; Basu, Sarbani/B-8015-2014; OI Kawaler, Steven/0000-0002-6536-6367; Fabrycky, Daniel/0000-0003-3750-0183; Karoff, Christoffer/0000-0003-2009-7965; Basu, Sarbani/0000-0002-6163-3472; Handberg, Rasmus/0000-0001-8725-4502; Montet, Benjamin/0000-0001-7516-8308; Barbieri, Mauro/0000-0001-8362-3462; Buchhave, Lars A./0000-0003-1605-5666; Bedding, Timothy/0000-0001-5943-1460; Metcalfe, Travis/0000-0003-4034-0416; Bedding, Tim/0000-0001-5222-4661; Lund, Mikkel Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571 FU NASA's Science Mission Directorate; NASA; NSF [DGE1144469, AST-1105930]; Netherlands Organisation for Scientific Research; BELSPO for contract PRODEX COROT; NASA Kepler Participating Scientist program; David and Lucile Packard foundation; Alfred P. Sloan foundation; Danish National Research Foundation [DNRF106]; ASTERISK; European Research Council [267864] FX We gratefully acknowledge the entire Kepler team for making this paper possible. Funding for the Kepler Mission is provided by NASA's Science Mission Directorate. We thank E. Agol and D. Raggozine for helpful comments on the manuscript. Supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA (D. H.); a NSF Graduate Research Fellowship (K. M. D.); a NSF Graduate Research Fellowship under grant DGE1144469 (B. T. M.); the Netherlands Organisation for Scientific Research (S. H.); BELSPO for contract PRODEX COROT (J.M.); the NASA Kepler Participating Scientist program (R.S.-O., J.N.W., and E. B. F.); NSF grant AST-1105930 (S. B.); and the David and Lucile Packard and Alfred P. Sloan foundations (J.A.J.). J.A.C. is a Hubble Fellow of the Harvard-Smithsonian Center for Astrophysics. Funding for the Stellar Astrophysics Centre is provided by Danish National Research Foundation grant DNRF106. The research is supported by the ASTERISK (Asteroseismic Investigations with SONG and Kepler) project funded by the European Research Council (grant agreement 267864). NR 30 TC 89 Z9 89 U1 0 U2 9 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 OCT 18 PY 2013 VL 342 IS 6156 BP 331 EP 334 DI 10.1126/science.1242066 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 235XG UT WOS:000325755100036 PM 24136961 ER PT J AU Nicholl, M Smartt, SJ Jerkstrand, A Inserra, C McCrum, M Kotak, R Fraser, M Wright, D Chen, TW Smith, K Young, DR Sim, SA Valenti, S Howell, DA Bresolin, F Kudritzki, RP Tonry, JL Huber, ME Rest, A Pastorello, A Tomasella, L Cappellaro, E Benetti, S Mattila, S Kankare, E Kangas, T Leloudas, G Sollerman, J Taddia, F Berger, E Chornock, R Narayan, G Stubbs, CW Foley, RJ Lunnan, R Soderberg, A Sanders, N Milisavljevic, D Margutti, R Kirshner, RP Elias-Rosa, N Morales-Garoffolo, A Taubenberger, S Botticella, MT Gezari, S Urata, Y Rodney, S Riess, AG Scolnic, D Wood-Vasey, WM Burgett, WS Chambers, K Flewelling, HA Magnier, EA Kaiser, N Metcalfe, N Morgan, J Price, PA Sweeney, W Waters, C AF Nicholl, M. Smartt, S. J. Jerkstrand, A. Inserra, C. McCrum, M. Kotak, R. Fraser, M. Wright, D. Chen, T-W Smith, K. Young, D. R. Sim, S. A. Valenti, S. Howell, D. A. Bresolin, F. Kudritzki, R. P. Tonry, J. L. Huber, M. E. Rest, A. Pastorello, A. Tomasella, L. Cappellaro, E. Benetti, S. Mattila, S. Kankare, E. Kangas, T. Leloudas, G. Sollerman, J. Taddia, F. Berger, E. Chornock, R. Narayan, G. Stubbs, C. W. Foley, R. J. Lunnan, R. Soderberg, A. Sanders, N. Milisavljevic, D. Margutti, R. Kirshner, R. P. Elias-Rosa, N. Morales-Garoffolo, A. Taubenberger, S. Botticella, M. T. Gezari, S. Urata, Y. Rodney, S. Riess, A. G. Scolnic, D. Wood-Vasey, W. M. Burgett, W. S. Chambers, K. Flewelling, H. A. Magnier, E. A. Kaiser, N. Metcalfe, N. Morgan, J. Price, P. A. Sweeney, W. Waters, C. TI Slowly fading super-luminous supernovae that are not pair-instability explosions SO NATURE LA English DT Article ID CORE-COLLAPSE SUPERNOVAE; IC SUPERNOVAE; LIGHT CURVES; ULTRALUMINOUS SUPERNOVAE; SUPERLUMINOUS SUPERNOVAE; LOW-METALLICITY; POPULATION III; MAGNETAR; GALAXIES; MODELS AB Super-luminous supernovae(1-4) that radiate more than 1044 ergs per second at their peak luminosity have recently been discovered in faint galaxies at redshifts of 0.1-4. Some evolve slowly, resembling models of 'pair-instability' supernovae(5,6). Such models involve stars with original masses 140-260 times that of the Sun that now have carbon-oxygen cores of 65-130 solar masses. In these stars, the photons that prevent gravitational collapse are converted to electron-positron pairs, causing rapid contraction and thermonuclear explosions. Many solar masses of Ni-56 are synthesized; this isotope decays to Fe-56 via Co-56, powering bright light curves(7,8). Such massive progenitors are expected to have formed from metal-poor gas in the early Universe(9). Recently, supernova 2007bi in a galaxy at redshift 0.127 (about 12 billion years after the Big Bang) with a metallicity one-third that of the Sun was observed to look like a fading pair-instability supernova(1,10). Here we report observations of two slow-to-fade super-luminous supernovae that show relatively fast rise times and blue colours, which are incompatible with pair-instability models. Their late-time light-curve and spectral similarities to supernova 2007bi call the nature of that event into question. Our early spectra closely resemble typical fast-declining super-luminous supernovae(2,11,12), which are not powered by radio-activity. Modelling our observations with 10-16 solar masses of magnetar-energized(13,14) ejecta demonstrates the possibility of a common explosion mechanism. The lack of unambiguous nearby pair-instability events suggests that their local rate of occurrence is less than 6 x 10(-6) times that of the core-collapse rate. C1 [Nicholl, M.; Smartt, S. J.; Jerkstrand, A.; Inserra, C.; McCrum, M.; Kotak, R.; Fraser, M.; Wright, D.; Chen, T-W; Smith, K.; Young, D. R.; Sim, S. A.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Valenti, S.; Howell, D. A.] Global Telescope Network, Las Cumbres Observ, Goleta, CA 93117 USA. [Valenti, S.; Howell, D. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bresolin, F.; Kudritzki, R. P.; Tonry, J. L.; Huber, M. E.; Burgett, W. S.; Chambers, K.; Flewelling, H. A.; Magnier, E. A.; Kaiser, N.; Morgan, J.; Sweeney, W.; Waters, C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Pastorello, A.; Tomasella, L.; Cappellaro, E.; Benetti, S.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Mattila, S.; Kankare, E.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Mattila, S.; Kankare, E.; Kangas, T.] Univ Turku, Tuorla Observ, Dept Phys & Astron, FI-21500 Piikkio, Finland. [Leloudas, G.] Stockholm Univ, Oskar Klein Ctr, Dept Phys, S-10691 Stockholm, Sweden. [Leloudas, G.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Sollerman, J.; Taddia, F.] Stockholm Univ, Oskar Klein Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Berger, E.; Chornock, R.; Narayan, G.; Stubbs, C. W.; Foley, R. J.; Lunnan, R.; Soderberg, A.; Sanders, N.; Milisavljevic, D.; Margutti, R.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kirshner, R. P.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Elias-Rosa, N.; Morales-Garoffolo, A.] Inst Ciencies Espai IEEC CSIC, Fac Ciencies, Bellaterra 08193, Spain. [Taubenberger, S.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Botticella, M. T.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Gezari, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Urata, Y.] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan. [Rodney, S.; Riess, A. G.; Scolnic, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Wood-Vasey, W. M.] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Metcalfe, N.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Nicholl, M (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. EM mnicholl03@qub.ac.uk RI Elias-Rosa, Nancy/D-3759-2014; Jerkstrand, Anders/K-9648-2015; Stubbs, Christopher/C-2829-2012; OI Elias-Rosa, Nancy/0000-0002-1381-9125; Jerkstrand, Anders/0000-0001-8005-4030; Stubbs, Christopher/0000-0003-0347-1724; Cappellaro, Enrico/0000-0001-5008-8619; Lunnan, Ragnhild/0000-0001-9454-4639; Benetti, Stefano/0000-0002-3256-0016; Sollerman, Jesper/0000-0003-1546-6615; Chen, Ting-Wan/0000-0002-1066-6098; Kotak, Rubina/0000-0001-5455-3653; Inserra, Cosimo/0000-0002-3968-4409; Fraser, Morgan/0000-0003-2191-1674; Narayan, Gautham/0000-0001-6022-0484; Chambers, Kenneth /0000-0001-6965-7789; Metcalfe, Nigel/0000-0001-9034-4402 FU NASA through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877]; University of Maryland; NSF [AST-1009749, AST-121196]; Swedish Research Council [623-2011-7117]; [291222] FX We thank D. Kasen and L. Dessart for sending us their model 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, NASA grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, National Science Foundation grant no. AST-1238877, and the University of Maryland. S.J.S. acknowledges FP7/2007-2013/ERC Grant agreement no. 291222; J.L.T. and R. P. Kirshner acknowledge NSF grants AST-1009749, AST-121196; G. L. acknowledges Swedish Research Council grant no. 623-2011-7117; A. P., L. T., E. C., S. B. and M. T. B. acknowledge PRIN-INAF 2011. Work is based on observations made with the following telescopes: the William Herschel Telescope, Gran Telescopio Canarias, the Nordic Optical Telescope, Telescopio Nazionale Galileo, the Liverpool Telescope, the Gemini Observatory, the Faulkes North Telescope, the Asiago Copernico Telescope and the United Kingdom Infrared Telescope. NR 31 TC 76 Z9 77 U1 1 U2 21 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 OCT 17 PY 2013 VL 502 IS 7471 BP 346 EP + DI 10.1038/nature12569 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 235GY UT WOS:000325706300047 PM 24132291 ER PT J AU Fioletov, VE McLinden, CA Krotkov, N Yang, K Loyola, DG Valks, P Theys, N Van Roozendael, M Nowlan, CR Chance, K Liu, X Lee, C Martin, RV AF Fioletov, V. E. McLinden, C. A. Krotkov, N. Yang, K. Loyola, D. G. Valks, P. Theys, N. Van Roozendael, M. Nowlan, C. R. Chance, K. Liu, X. Lee, C. Martin, R. V. TI Application of OMI, SCIAMACHY, and GOME-2 satellite SO2 retrievals for detection of large emission sources SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OZONE MONITORING INSTRUMENT; SULFUR-DIOXIDE; AIR-POLLUTION; ATMOSPHERIC COMPOSITION; MISSION; MEXICO; CHINA; ECOSYSTEM; QUALITY; PLUMES C1 [Fioletov, V. E.; McLinden, C. A.] Environm Canada, Toronto, ON M3H 5T4, Canada. [Krotkov, N.; Yang, K.] NASA Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD USA. [Yang, K.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Loyola, D. G.; Valks, P.] Deutsch Zentrum Luft & Raumfahrt, Wessling, Germany. [Theys, N.; Van Roozendael, M.] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium. [Nowlan, C. R.; Martin, R. V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Chance, K.; Liu, X.; Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lee, C.] Korea Meteorol Adm, Natl Inst Meteorol Res, Seoul, South Korea. RP Fioletov, VE (reprint author), Environm Canada, 4905 Dufferin St, Toronto, ON M3H 5T4, Canada. EM Vitali.Fioletov@ec.gc.ca RI Liu, Xiong/P-7186-2014; Martin, Randall/C-1205-2014; Krotkov, Nickolay/E-1541-2012; OI Liu, Xiong/0000-0003-2939-574X; Martin, Randall/0000-0003-2632-8402; Krotkov, Nickolay/0000-0001-6170-6750; Nowlan, Caroline/0000-0002-8718-9752; Fioletov, Vitali/0000-0002-2731-5956; Chance, Kelly/0000-0002-7339-7577 FU NASA Earth Science Division; O3M-SAF project; EUMETSAT; ESA within the TEMIS project; ESA within the SACS project; ESA within the GSE PROMOTE project; Advanced Research on Applied Meteorology of the Korea Meteorological Administration (KMA) FX We acknowledge the NASA Earth Science Division for funding of OMI SO2 product development and analysis. The Dutch-Finnish-built OMI instrument is part of the NASA EOS Aura satellite payload. The OMI project is managed by KNMI and the Netherlands Agency for Aerospace Programs (NIVR). The generation of the GOME-2 SO2 operational products has been funded by the O3M-SAF project with EUMETSAT and national contributions. The SCIAMACHY data product has been developed under ESA funding within the TEMIS, SACS, and GSE PROMOTE projects. The work of one of the coauthors (C.L.) was supported by the Advanced Research on Applied Meteorology of the Korea Meteorological Administration (KMA). NR 58 TC 40 Z9 42 U1 4 U2 36 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 OCT 16 PY 2013 VL 118 IS 19 BP 11399 EP 11418 DI 10.1002/jgrd.50826 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297PF UT WOS:000330266700027 ER PT J AU Woodman, N AF Woodman, Neal TI The type localities of the mule deer, Odocoileus hemionus (Rafinesque, 1817), and the Kansas white-tailed deer, Odocoileus virginianus macrourus (Rafinesque, 1817), are not where we thought they were SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Cervidae; Odocoileus virginianus dacotensis; Odocoileus virginianus texanus; taxonomy; type specimen AB Among the iconic mammals of the North American West is the mule deer (Odocoileus hemionus). This species and a western subspecies of the white-tailed deer (Odocoileus virginianus macrourus) were two of seven mammals originally named and described as new species in 1817 by Constantine S. Rafinesque. Rafinesque never saw the animals that he named. Instead, he followed the then-acceptable practice of basing his new species on animals characterized in another published work, in this case the putative journal of Charles Le Raye, a French Canadian fur trader who was said to have traversed the upper Missouri River region before the Lewis and Clark Expedition and whose journal described some of the wildlife in detail. Unlike the mule deer, whose existence has been established by generations of biologists, wildlife management professionals, and sportsmen, Le Raye and his journal have since been proven to be fraudulent. Because Rafinesque's names were published in accordance with the taxonomic conventions of his time, they remain available, but, based on the questionable source of his descriptions, the identities and type localities of the species must be viewed as unreliable. Fortunately, much of the Le Raye journal was derived from other, verifiable contemporary sources. In particular, the descriptions of the two deer were based on the published journal of Patrick Gass, a member of the Lewis and Clark Expedition. Using the Gass journal as the original source of Rafinesque's descriptions, the type localities for the two deer can be reliably placed in Lyman County, South Dakota. C1 Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Woodman, N (reprint author), Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, MRC 111,POB 37012, Washington, DC 20013 USA. EM woodmann@si.edu NR 55 TC 2 Z9 2 U1 1 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 16 PY 2013 VL 126 IS 3 BP 187 EP 198 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 238AL UT WOS:000325912700001 ER PT J AU Olson, SL AF Olson, Storrs L. TI A nomenclatural history of Audubon's Shearwater with designation of a neotype for Puffinus lherminieri Lesson, 1839 (Aves: Procellariidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Antilles; Ferdinand L'Herminier; Guadeloupe; Saint Barthelemy; seabirds; West Indies AB The nomenclatural history of the small Antillean species that now goes by the name Audubon's Shearwater Puffinus lherminieri is briefly summarized. The type material of Puffinus lherminieri Lesson, 1839, supposed to be in a museum in Rochefort, France, could not be located and is presumed lost.. The stated type locality "ad ripas Antillarum" is so general as to encompass almost the entire breeding range of the species, which is widely distributed in the Antillean region and has been regarded as showing variation meriting subspecific designation. Although the type locality was apparently legitimately restricted to Guadeloupe in 1948 or earlier, it was elsewhere erroneously restricted to "Straits of Florida" from 1931 to 1998 and up to the present. To resolve these numerous conflicts and uncertainties, a neotype collected in Saint Barthelemy, once administratively part of Guadeloupe, is here designated. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM olsons@si.edu NR 29 TC 0 Z9 1 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 16 PY 2013 VL 126 IS 3 BP 199 EP 203 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 238AL UT WOS:000325912700002 ER PT J AU Heyer, WR Heyer, MM AF Heyer, W. Ronald Heyer, Miriam M. TI Systematics, distribution, and bibliography of the frog Leptodactylus insularum Barbour, 1906 (Amphibia: Leptodactylidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE discriminant function analyses; external morphology; geographic sampling; species limits ID SKELETAL-MUSCLE FIBERS; BULLFROG RANA-CATESBEIANA; COSTA-RICA; PARENTAL CARE; POTASSIUM CONTRACTURES; ANURA LEPTODACTYLIDAE; ADVERTISEMENT CALLS; GENUS LEPTODACTYLUS; NATURAL-HISTORY; TIME-COURSE AB The Leptodactylus bolivianus complex has recently been assessed and determined to be comprised of three species - L. bolivianus, L. guianensis, and L. insularum (Heyer & de Sa. 2011). The aim of this study is to amplify data for L. insularum that were not included in the Heyer & de S (2011) publication. The earlier paper based distributional data only on specimens evaluated by Heyer. Later literature searches identified further information and a greater number of localities for Leptodactylus insularum resulting in a comprehensive summary and a more precise distribution for the species. The purpose of this paper is to summarize information for the currently understood single species Leptodactylus insularum. Pertinent literature is reviewed and summarized for biology, life history, systematics, nomenclature, conservation, and distribution. C1 [Heyer, W. Ronald; Heyer, Miriam M.] Smithsonian Inst, Washington, DC 20013 USA. RP Heyer, WR (reprint author), Smithsonian Inst, MRC 162,POB 37012, Washington, DC 20013 USA. EM heyerr@si.edu NR 402 TC 1 Z9 2 U1 1 U2 5 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 16 PY 2013 VL 126 IS 3 BP 204 EP 233 PG 30 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 238AL UT WOS:000325912700003 ER PT J AU Moron, S Fox, DL Feinberg, JM Jaramillo, C Bayona, G Montes, C Bloch, JI AF Moron, Sara Fox, David L. Feinberg, Joshua M. Jaramillo, Carlos Bayona, German Montes, Camilo Bloch, Jonathan I. TI Climate change during the Early Paleogene in the Bogota Basin (Colombia) inferred from paleosol carbon isotope stratigraphy, major oxides, and environmental magnetism SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Paleosols; Paleoclimate; Paleocene-Eocene; Elemental composition; Environmental magnetism ID EOCENE THERMAL MAXIMUM; CLAY-MINERAL EVIDENCE; EASTERN CORDILLERA; NORTHERN ANDES; SURFACE-TEMPERATURE; PARENT MATERIALS; LATE PALEOCENE; BIGHORN BASIN; BOUNDARY; SOILS AB Paleosols in the Bogota Basin, Colombia, record an increase in chemical weathering across the Paleocene-Eocene (P-E) transition. Rock magnetic properties and major element geochemistry exhibit an abrupt change in an interval identified as including the P-E boundary, as established by previously published biostratigraphy and a U/Pb date on volcanic zircons (56.2 +/- 1.6 Ma). During the stratigraphic interval that contains the P-E transition, magnetic susceptibility increases significantly, with an order of magnitude higher concentration of magnetite/maghemite and hematite. The preponderance of pure stoichiometric magnetite in the paleosols of this interval indicates that the increase in magnetic susceptibility is due to changes in the rate of pedogenesis, rather than an increase in the erosion of nearby volcanic rocks, which would contribute titanomagnetite. Pedogenic structures preserved within the paleosols, a lack of iron oxides as cement, friability of the sandstones, and previously published thermochronologic data are not consistent with burial diagenesis as an explanation for the origin of the magnetic mineral assemblage. These enhanced pedogenesis and related chemical weathering is also confirmed by increases in the concentration of Fe2O3 and Al2O3 and loss on ignition values. An increase in mean precipitation across this interval is inferred by the lack of carbonate nodules and a decrease in SiO2 in paleosols. Thus, we hypothesize that there was an intensification of chemical weathering during the interval that contains the P-E transition. (C) 2013 Elsevier B.V. All rights reserved. C1 [Moron, Sara; Fox, David L.; Feinberg, Joshua M.] Univ Minnesota, Dept Earth Sci, Minneapolis, MN 55455 USA. [Feinberg, Joshua M.] Univ Minnesota, Inst Rock Magnetism, Minneapolis, MN 55455 USA. [Moron, Sara; Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Bayona, German] Corp Geol Ares, Bogota, Colombia. [Montes, Camilo] Univ Los Andes, Bogota, Colombia. [Bloch, Jonathan I.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. RP Moron, S (reprint author), Univ Adelaide, Australian Sch Petr, Adelaide, SA 5005, Australia. EM sara.moronpolanco@adelaide.edu.au OI Bloch, Jonathan/0000-0003-1484-6931; Fox, David L/0000-0002-2291-6146; Montes, Camilo/0000-0002-3553-0787 FU Colombian Association of Geologists and Petroleum Geophysicists (Asociacion Colombiana de Geologos y Geofisicos del Petroleo); Instruments and Facilities Program, Earth Science Division, of the U.S. National Science Foundation FX This research was partially funded by the Colombian Association of Geologists and Petroleum Geophysicists (Asociacion Colombiana de Geologos y Geofisicos del Petroleo) through the Research Grant Corrigan and Promotion of Young Investigators-ARES Found. The Institute for Rock Magnetism is supported by a grant from the Instruments and Facilities Program, Earth Science Division, of the U.S. National Science Foundation. The Unidad Administrativa Especial de Seivicios Publicos kindly provided access to the outcrops located in the Dona Juana sanitary landfill. Special thanks to the residents of the Mochuelo town for their logistical support. Thanks to L. Quiroz, F. Lamus, O. Montenegro, L. Jimenez, M. C. Ruiz, G. Jimenez, J. Moreno, and the ARES team for their help in the field. Thanks to Dr. J. H. Escobar and Dr. J. Curtis for analyzing the carbon isotopes at the University of Florida. Thanks to Drs. K. Kleinsphen and E. Nater for their discussions about the paleosols and to Dr F. McInerney for her discussion about the manuscript. This manuscript was improved by reviews from P. Lippert, P. Hesse, and an anonymous reviewer. NR 90 TC 6 Z9 7 U1 2 U2 32 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 OCT 15 PY 2013 VL 388 BP 115 EP 127 DI 10.1016/j.palaeo.2013.08.010 PG 13 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 249JP UT WOS:000326773800011 ER PT J AU Gilmour, CC Podar, M Bullock, AL Graham, AM Brown, SD Somenahally, AC Johs, A Hurt, RA Bailey, KL Elias, DA AF Gilmour, Cynthia C. Podar, Mircea Bullock, Allyson L. Graham, Andrew M. Brown, Steven D. Somenahally, Anil C. Johs, Alex Hurt, Richard A., Jr. Bailey, Kathryn L. Elias, Dwayne A. TI Mercury Methylation by Novel Microorganisms from New Environments SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID SULFATE-REDUCING BACTERIA; PSYCHROPHILUS SP-NOV.; GEN. NOV.; METHYLMERCURY PRODUCTION; GEOBACTER-SULFURREDUCENS; AQUATIC ECOSYSTEMS; WASTE-WATER; METHANOGEN; RICE; BIOAVAILABILITY AB Microbial mercury (Hg) methylation transforms a toxic trace metal into the highly bioaccumulated neurotoxin methylmercury (MeHg). The lack of a genetic marker for microbial MeHg production has prevented a dear understanding of Hg-methylating organism distribution in nature. Recently, a specific gene cluster (hgcAB) was linked to Hg methylation in two bacteria.(1) Here we test if the presence of hgcAB orthologues is a reliable predictor of Hg methylation capability in microorganisms, a necessary confirmation for the development of molecular probes for Hg-methylation in nature. Although hgcAB orthologues are rare among all available microbial genomes, organisms are much more phylogenetically and environmentally diverse than previously thought. By directly measuring MeHg production in several bacterial and archaeal strains encoding hgcAB, we confirmed that possessing hgcAB predicts Hg methylation capability. For the first time, we demonstrated Hg methylation in a number of species other than sulfate- (SRB) and iron- (FeRB) reducing bacteria, including methanogens, and syntrophic, acetogenic, and fermentative Firmicutes. Several of these species occupy novel environmental niches for Hg methylation, including methanogenic habitats such as rice paddies, the animal gut, and extremes of pH and salinity. Identification of these organisms as Hg methylators now links methylation to discrete gene markers in microbial communities. C1 [Gilmour, Cynthia C.; Bullock, Allyson L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Podar, Mircea; Brown, Steven D.; Somenahally, Anil C.; Hurt, Richard A., Jr.; Bailey, Kathryn L.; Elias, Dwayne A.] Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA. [Johs, Alex] Oak Ridge Natl Lab, Environm Sci Div, Oak Ridge, TN 37831 USA. [Graham, Andrew M.] Grinnell Coll, Grinnell, IA 50112 USA. RP Elias, DA (reprint author), Oak Ridge Natl Lab, Biosci Div, POB 2008,MS 6036, Oak Ridge, TN 37831 USA. EM eliasda@ornl.gov RI Elias, Dwayne/B-5190-2011; Johs, Alexander/F-1229-2011; Brown, Steven/A-6792-2011; Gilmour, Cynthia/G-1784-2010; OI Elias, Dwayne/0000-0002-4469-6391; Johs, Alexander/0000-0003-0098-2254; Brown, Steven/0000-0002-9281-3898; Gilmour, Cynthia/0000-0002-1720-9498; Podar, Mircea/0000-0003-2776-0205 FU Subsurface Biogeochemical Research Program (SBR) within the U.S. Department of Energy, Office of Science, Biological and Environmental Research; Smithsonian Environmental Research Center; SBR; National Science Foundation [DEB0351050]; U.S. Department of Energy [DEAC05-00OR22725] FX This research was conducted by the Oak Ridge National Laboratory Mercury Subsurface Science Focus Area with support from the Subsurface Biogeochemical Research Program (SBR) within the U.S. Department of Energy, Office of Science, Biological and Environmental Research and by the Smithsonian Environmental Research Center with support from SBR and National Science Foundation Grant DEB0351050 to C.G. ORNL is managed by UT-Battelle LLC for the U.S. Department of Energy under contract DEAC05-00OR22725. We thank Robert Sanford for A. dehalogens strain K, Mike McInerney for S. acidotrophicus, and Joel Kostka for G. daltonii. Andrew Maizel, Taylan Morcol, Alyssa Wetterauer, and Georgia Riedel performed all mercury analyses at SERC. NR 67 TC 103 Z9 105 U1 19 U2 177 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD OCT 15 PY 2013 VL 47 IS 20 BP 11810 EP 11820 DI 10.1021/es403075t PG 11 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 240UQ UT WOS:000326123600056 PM 24024607 ER PT J AU Trumble, SJ Robinson, EM Berman-Kowalewski, M Potter, CW Usenko, S AF Trumble, Stephen J. Robinson, Eleanor M. Berman-Kowalewski, Michelle Potter, Charles W. Usenko, Sascha TI Blue whale earplug reveals lifetime contaminant exposure and hormone profiles SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE cetaceans; cerumen; persistent organic pollutants ID DOLPHINS TURSIOPS-TRUNCATUS; NORTH-ATLANTIC; ST-LAWRENCE; EAR PLUG; POLYCHLORINATED-BIPHENYLS; ORGANOCHLORINE COMPOUNDS; BALAENOPTERA-PHYSALUS; ORGANIC CONTAMINANTS; SEXUAL-MATURITY; MARINE MAMMALS AB Lifetime contaminant and hormonal profiles have been reconstructed for an individual male blue whale (Balaenoptera musculus, Linnaeus 1758) using the earplug as a natural aging matrix that is also capable of archiving and preserving lipophilic compounds. These unprecedented lifetime profiles (i.e., birth to death) were reconstructed with a 6-mo resolution for a wide range of analytes including cortisol (stress hormone), testosterone (developmental hormone), organic contaminants (e.g., pesticides and flame retardants), and mercury. Cortisol lifetime profiles revealed a doubling of cortisol levels over baseline. Testosterone profiles suggest this male blue whale reached sexual maturity at approximately 10 y of age, which corresponds well with and improves on previous estimates. Early periods of the reconstructed contaminant profiles for pesticides (such as dichlorodiphenyltrichloroethanes and chlordanes), polychlorinated biphenyls, and polybrominated diphenyl ethers demonstrate significant maternal transfer occurred at 0-12 mo. The total lifetime organic contaminant burden measured between the earplug (sum of contaminants in laminae layers) and blubber samples from the same organism were similar. Total mercury profiles revealed reduced maternal transfer and two distinct pulse events compared with organic contaminants. The use of a whale earplug to reconstruct lifetime chemical profiles will allow for a more comprehensive examination of stress, development, and contaminant exposure, as well as improve the assessment of contaminant use/emission, environmental noise, ship traffic, and climate change on these important marine sentinels. C1 [Trumble, Stephen J.] Baylor Univ, Dept Biol, Waco, TX 76798 USA. [Usenko, Sascha] Baylor Univ, Dept Environm Sci, Waco, TX 76798 USA. [Robinson, Eleanor M.; Usenko, Sascha] Baylor Univ, Inst Ecol Earth & Environm Sci, Waco, TX 76798 USA. [Berman-Kowalewski, Michelle] Santa Barbara Museum Nat Hist, Dept Vertebrate Zool, Santa Barbara, CA 93105 USA. [Potter, Charles W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Usenko, S (reprint author), Baylor Univ, Inst Ecol Earth & Environm Sci, Waco, TX 76798 USA. EM Sascha_Usenko@baylor.edu RI Guenat, Heather/H-6528-2014; Usenko, Sascha/N-8730-2015; OI Trumble, Stephen/0000-0001-6319-9633; Usenko, Sascha/0000-0003-3303-2909 FU Marine Mammal Commission FX We thank Mr. and Mrs. Anthony Robert for their generous donation, which was used to purchase equipment for this research; Rebel Sanders (S.J.T. Laboratory) for all hormone analyses; Dr. Bikram Subedi (S.U. Laboratory) for mercury analysis; Drs. Michael Moore and Dion Oxman for insightful comments; Dr. Rebecca R. Watson, of Watson & Stonehouse Enterprises, LLC, who provided writing support during the development of this article; and the Marine Mammal Commission for funding (to S.U. and S.J.T.). The permit for this research (National Marine Fisheries Service 17157) was issued to S.J.T. NR 44 TC 12 Z9 12 U1 9 U2 61 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 OCT 15 PY 2013 VL 110 IS 42 BP 16922 EP 16926 DI 10.1073/pnas.1311418110 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 234HT UT WOS:000325634200053 PM 24043814 ER PT J AU Hong, T AF Hong, Terry TI Boy in the Twilight: Stories of the Hidden China SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 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 OCT 15 PY 2013 VL 138 IS 17 BP 93 EP 93 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 230BJ UT WOS:000325311300134 ER PT J AU Al Shorman, MM Gharaibeh, MF Bizau, JM Cubaynes, D Guilbaud, S El Hassan, N Miron, C Nicolas, C Robert, E Sakho, I Blancard, C McLaughlin, BM AF Al Shorman, M. M. Gharaibeh, M. F. Bizau, J. M. Cubaynes, D. Guilbaud, S. El Hassan, N. Miron, C. Nicolas, C. Robert, E. Sakho, I. Blancard, C. McLaughlin, B. M. TI K-shell photoionization of Be-like and Li-like ions of atomic nitrogen: experiment and theory SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID X-RAY SPECTROSCOPY; DIELECTRONIC SATELLITE SPECTRA; DOUBLY-EXCITED RESONANCES; R-MATRIX THEORY; CROSS-SECTIONS; XMM-NEWTON; OSCILLATOR-STRENGTHS; HE-LIKE; ABSORPTION; AUGER AB Absolute cross sections for the K-shell photoionization of Be-like and Li-like atomic nitrogen ions were measured by employing the ion-photon merged-beam technique at the SOLEIL synchrotron radiation facility in Saint-Aubin, France. High-resolution spectroscopy at nominal resolutions of 38, 56, 111, 133 meV full width at half maximum (FWHM) for Be-like and 125 meV FWHM for Li-like atomic nitrogen ions was achieved for the photon energies ranging from 410 up to 460 eV. The experimental measurements are compared with theoretical estimates from the multi-configuration Dirac-Fock, R-matrix and an empirical method. The interplay between experiment and theory enabled the identification and characterization of the strong 1s -> 2p resonances features observed in the K-shell spectra of each ion and the region around 460 eV for the 1s -> 3p resonance of the N3+ ion yielding suitable agreement with experiment. C1 [Al Shorman, M. M.; Bizau, J. M.; Cubaynes, D.; Guilbaud, S.; El Hassan, N.] Univ Paris 11, CNRS, ISMO, UMR 8214, F-91405 Orsay, France. [Gharaibeh, M. F.] Jordan Univ Sci & Technol, Dept Phys, Irbid 22110, Jordan. [Bizau, J. M.; Cubaynes, D.; Miron, C.; Nicolas, C.; Robert, E.] Synchrotron SOLEIL Orme 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. [McLaughlin, B. M.] Queens Univ Belfast, Sch Math & Phys, CTAMOP, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Bizau, JM (reprint author), Univ Paris 11, CNRS, ISMO, UMR 8214, Bat 350, F-91405 Orsay, France. EM jean-marc.bizau@u-psud.fr; b.mclaughlin@qub.ac.uk OI MIRON, Catalin/0000-0002-8302-7158 FU National Science Foundation [OCI-1053575]; US National Science Foundation; Queen's University Belfast; University Assane Seck of Ziguinchor FX The experimental measurements were performed on the PLEIADES beamline [72, 73], at the SOLEIL Synchrotron radiation facility in Saint-Aubin, France. The authors would like to thank the SOLEIL staff and, in particular those of the PLEIADES beam line for their helpful assistance. B M McLaughlin acknowledges support from the US National Science Foundation through a grant to ITAMP at the HarvardSmithsonian Center for Astrophysics, the RTRA network Triangle de le Physique and a visiting research fellowship from Queen's University Belfast. I Sakho acknowledges the hospitality of the Universite Paris-Sud and support from the University Assane Seck of Ziguinchor during a recent visit. We thank Dr John C Raymond and Dr Randall K Smith at the Harvard-Smithsonian Center for Astrophysics for discussions on the astrophysical applications and Dr Javier Garcia for numerical values of the cross sections [9]. We gratefully acknowledge Dr Wayne C Stolte for assistance in fitting and interpreting the SOLEIL experimental measurements with the WinXAS software. The computational work was carried out at the National Energy Research Scientific Computing Center in Oakland, CA, USA, the Kraken XT5 facility at the National Institute for Computational Science (NICS) in Knoxville, TN, USA and at the High Performance Computing Center Stuttgart (HLRS) of the University of Stuttgart. We thank Stefan Andersson from Cray Research for his advice and assistance with the implementation of the parallel R-matrix codes on the Cray-XE6 at HLRS. The Kraken XT5 facility is a resource of the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number OCI-1053575. NR 104 TC 7 Z9 7 U1 0 U2 16 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 OCT 14 PY 2013 VL 46 IS 19 AR 195701 DI 10.1088/0953-4075/46/19/195701 PG 12 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 237GG UT WOS:000325856100009 ER PT J AU Pan, T Loeb, A AF Pan, Tony Loeb, Abraham TI Finding core-collapse supernovae from the epoch of reionization behind cluster lenses SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: strong; supernovae: general; galaxies: clusters: general; early Universe AB Current surveys are underway to utilize gravitational lensing by galaxy clusters with Einstein radii > 35 arcsec in the search for the highest redshift galaxies. Associated supernovae from the epoch of reionization would have their fluxes boosted above the detection threshold, extending their duration of visibility. We predict that the James Webb Space Telescope (JWST) will be able to discover lensed core-collapse supernovae at redshifts exceeding z = 7-8. C1 [Pan, Tony; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pan, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM span@physics.harvard.edu FU Hertz Foundation; National Science Foundation; NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A] FX We are grateful to Dan Kasen for providing the spectral time-series data for the Type IIP SN model used in this Letter. TP was supported by the Hertz Foundation and the National Science Foundation via a graduate research fellowship. This work was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A. NR 29 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 OCT 11 PY 2013 VL 435 IS 1 BP L33 EP L37 DI 10.1093/mnrasl/slt089 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA V40MZ UT WOS:000209484000008 ER PT J AU Hirsch, BT Prange, S Hauver, SA Gehrt, SD AF Hirsch, Ben T. Prange, Suzanne Hauver, Stephanie A. Gehrt, Stanley D. TI Raccoon Social Networks and the Potential for Disease Transmission SO PLOS ONE LA English DT Article ID PROCYON-LOTOR; CANINE-DISTEMPER; GENETIC RELATEDNESS; SEROLOGIC SURVEY; CONTACT RATES; UNITED-STATES; NEW-JERSEY; RABIES; ONTARIO; USA AB Raccoons are an important vector of rabies and other pathogens. The degree to which these pathogens can spread through a raccoon population should be closely linked to association rates between individual raccoons. Most studies of raccoon sociality have found patterns consistent with low levels of social connectivity within populations, thus the likelihood of direct pathogen transmission between raccoons is theoretically low. We used proximity detecting collars and social network metrics to calculate the degree of social connectivity in an urban raccoon population for purposes of estimating potential pathogen spread. In contrast to previous assumptions, raccoon social association networks were highly connected, and all individuals were connected to one large social network during 15 out of 18 months of study. However, these metrics may overestimate the potential for a pathogen to spread through a population, as many of the social connections were based on relatively short contact periods. To more closely reflect varying probabilities of pathogen spread, we censored the raccoon social networks based on the total amount of time spent in close proximity between two individuals per month. As this time criteria for censoring the social networks increased from one to thirty minutes, corresponding measures of network connectivity declined. These findings demonstrate that raccoon populations are much more tightly connected than would have been predicted based on previous studies, but also point out that additional research is needed to calculate more precise transmission probabilities by infected individuals, and determine how disease infection changes normal social behaviors. C1 [Hirsch, Ben T.; Gehrt, Stanley D.] Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA. [Hirsch, Ben T.] Smithsonian Trop Res Inst, Balboa, Panama. [Prange, Suzanne] Ohio Div Wildlife, Athens, OH USA. SUNY Binghamton, Sch Educ, Binghamton, NY USA. RP Hirsch, BT (reprint author), Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA. EM hirschb@si.edu FU National Science Foundation [0425203]; Cook County Animal and Rabies Control; Max McGraw Wildlife Foundation FX This project was funded in part by the National Science Foundation (ID-0425203), Cook County Animal and Rabies Control and the Max McGraw Wildlife Foundation. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 65 TC 13 Z9 13 U1 13 U2 84 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 OCT 10 PY 2013 VL 8 IS 10 AR e75830 DI 10.1371/journal.pone.0075830 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 236QM UT WOS:000325814200024 PM 24130746 ER PT J AU Ren, HB Condit, R Chen, B Mi, XC Cao, M Ye, WH Hao, ZQ Ma, KP AF Ren, Haibao Condit, Richard Chen, Bin Mi, Xiangcheng Cao, Min Ye, Wanhui Hao, Zhanqing Ma, Keping TI Geographical Range and Local Abundance of Tree Species in China SO PLOS ONE LA English DT Article ID SIZE RELATIONSHIPS; OCCUPANCY RELATIONSHIPS; SPATIAL VARIATION; BRITISH AVIFAUNA; LIFE-HISTORY; FOREST PLOT; PATTERNS; DISTRIBUTIONS; COMMUNITY; CONSERVATION AB Most studies on the geographical distribution of species have utilized a few well-known taxa in Europe and North America, with little research in China and its wide range of climate and forest types. We assembled large datasets to quantify the geographic ranges of tree species in China and to test several biogeographic hypotheses: 1) whether locally abundant species tend to be geographically widespread; 2) whether species are more abundant towards their range-centers; and 3) how abundances are correlated between sites. Local abundances of 651 species were derived from four tree plots of 2025 ha where all individuals >= 1 cm in stem diameter were mapped and identified taxonomically. Range sizes of these species across China were then estimated from over 460,000 geo-referenced records; a Bayesian approach was used, allowing careful measures of error of each range estimate. The log-transformed range sizes had a bell-shaped distribution with a median of 703,000 km(2), and >90% of 651 species had ranges. 10(5) km(2). There was no relationship between local abundance and range size, and no evidence for species being more abundant towards their range-centers. Finally, species' abundances were positively correlated between sites. The widespread nature of most tree species in China suggests few are vulnerable to global extinction, and there is no indication of the double-peril that would result if rare species also had narrow ranges. C1 [Ren, Haibao; Chen, Bin; Mi, Xiangcheng; Ma, Keping] Chinese Acad Sci, Inst Bot, Key Lab Vegetat & Environm Change, Beijing, Peoples R China. [Condit, Richard] Smithsonian Trop Res Inst, Panama City, Panama. [Cao, Min] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Kunming, Peoples R China. [Ye, Wanhui] Chinese Acad Sci, South China Bot Garden, Guangzhou, Guangdong, Peoples R China. [Hao, Zhanqing] Chinese Acad Sci, Inst Appl Ecol, Shenyang 110016, Peoples R China. RP Ma, KP (reprint author), Chinese Acad Sci, Inst Bot, Key Lab Vegetat & Environm Change, Beijing, Peoples R China. EM kpma@ibcas.ac.cn FU NSFC Project [30670311]; China National Program for R & D Infrastructure and Facility Development [2008BAC39B02]; CTFS-SiGEO workshop series; NSF [DEB-1046113] FX This study was supported by NSFC Project (30670311), China National Program for R & D Infrastructure and Facility Development (2008BAC39B02), and the CTFS-SiGEO workshop series, funded by NSF Award DEB-1046113. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 59 TC 3 Z9 3 U1 0 U2 43 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 OCT 10 PY 2013 VL 8 IS 10 AR e76374 DI 10.1371/journal.pone.0076374 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 236QM UT WOS:000325814200037 PM 24130772 ER PT J AU Batterman, SA Hedin, LO van Breugel, M Ransijn, J Craven, DJ Hall, JS AF Batterman, Sarah A. Hedin, Lars O. van Breugel, Michiel Ransijn, Johannes Craven, Dylan J. Hall, Jefferson S. TI Key role of symbiotic dinitrogen fixation in tropical forest secondary succession SO NATURE LA English DT Article ID NITROGEN-FIXATION; PHOSPHORUS LIMITATION; BIOMASS; DYNAMICS; GROWTH; AMAZONIA; SOILS; LAND AB Forests contribute a significant portion of the land carbon sink, but their ability to sequester CO2 may be constrained by nitrogen(1-6), a major plant-limiting nutrient. Many tropical forests possess tree species capable of fixing atmospheric dinitrogen (N-2)(7), but it is unclear whether this functional group can supply the nitrogen needed as forests recover from disturbance or previous land use(1), or expand in response to rising CO2 (refs 6, 8). Here we identify a powerful feedback mechanism in which N-2 fixation can overcome ecosystem-scale deficiencies in nitrogen that emerge during periods of rapid biomass accumulation in tropical forests. Over a 300-year chronosequence in Panama, N-2-fixing tree species accumulated carbon up to nine times faster per individual than their non-fixing neighbours (greatest difference in youngest forests), and showed species-specific differences in the amount and timing of fixation. As a result of fast growth and high fixation, fixers provided a large fraction of the nitrogen needed to support net forest growth (50,000 kg carbon per hectare) in the first 12 years. A key element of ecosystem functional diversity was ensured by the presence of different N-2-fixing tree species across the entire forest age sequence. These findings show that symbiotic N-2 fixation can have a central role in nitrogen cycling during tropical forest stand development, with potentially important implications for the ability of tropical forests to sequester CO2. C1 [Batterman, Sarah A.; Hedin, Lars O.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [van Breugel, Michiel; Hall, Jefferson S.] Smithsonian Trop Res Inst, Panama City, Panama. [Ransijn, Johannes] Wageningen Univ, Ctr Ecosyst Studies, Forest Ecol & Forest Management Grp, NL-6700 AA Wageningen, Netherlands. [Ransijn, Johannes] Univ Copenhagen, Dept Geosci & Nat Resource Management, DK-1958 Frederiksberg C, Denmark. [Craven, Dylan J.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. RP Batterman, SA (reprint author), Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. EM sbatterm@princeton.edu RI Ransijn, Johannes/D-5324-2015; Craven, Dylan/K-2717-2012; OI Ransijn, Johannes/0000-0003-0416-2210; Craven, Dylan/0000-0003-3940-833X; van Breugel, Michiel/0000-0003-2778-7803 FU National Science Foundation (NSF) [DEB-0614116]; National Oceanic and Atmospheric Association (NOAA) [NA17RJ262-344]; Cooperative Institute for Climate Science of Princeton University; Carbon Mitigation Initiative of Princeton University; Smithsonian Tropical Research Institute (STRI); HSBC; STRI; Frank Levinson Family Foundation; Motta Family Foundation FX We thank S. Adelberg and K. Zelazny for assisting with data collection, M. Baillon and A. Hernandez for botanical identifications, N. Wurzburger and A. Barron for species-specific N2 fixation rates, J. Sprent for advice about N2-fixing trees and P. Reich for comments. This work was supported by grants to L.O.H. from the National Science Foundation (NSF; DEB-0614116), the National Oceanic and Atmospheric Association (NOAA; grant NA17RJ262-344), the Cooperative Institute for Climate Science of Princeton University and the Carbon Mitigation Initiative of Princeton University; and to S. A. B. from the Smithsonian Tropical Research Institute (STRI). It is a contribution to the Agua Salud Project (ASP), a collaboration among STRI, the Panama Canal Authority (ACP) and the National Environmental Authority of Panama (ANAM). ASP funding came from the HSBC climate partnership, STRI, the Frank Levinson Family Foundation, the Motta Family Foundation and an anonymous donor. NR 40 TC 52 Z9 52 U1 17 U2 187 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 OCT 10 PY 2013 VL 502 IS 7470 BP 224 EP + DI 10.1038/nature12525 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 231RU UT WOS:000325436100048 PM 24037375 ER PT J AU Batygin, K Stanley, S Stevenson, DJ AF Batygin, Konstantin Stanley, Sabine Stevenson, David J. TI MAGNETICALLY CONTROLLED CIRCULATION ON HOT EXTRASOLAR PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: atmospheres; planets and satellites: magnetic fields ID 3-DIMENSIONAL ATMOSPHERIC CIRCULATION; INFRARED-EMISSION-SPECTRUM; HD 209458B; TEMPERATURE INVERSION; DYNAMO MODELS; JUPITERS; FIELDS; 189733B; WINDS; SIMULATIONS AB Through the process of thermal ionization, intense stellar irradiation renders hot Jupiter atmospheres electrically conductive. Simultaneously, lateral variability in the irradiation drives the global circulation with peak wind speeds of the order of similar to km s(-1). In turn, the interactions between the atmospheric flows and the background magnetic field give rise to Lorentz forces that can act to perturb the flow away from its purely hydrodynamical counterpart. Using analytical theory and numerical simulations, we show here that significant deviations away from axisymmetric circulation are unstable in presence of a non-negligible axisymmetric magnetic field. Specifically, our results suggest that dayside-to-nightside flows, often obtained within the context of three-dimensional circulation models, only exist on objects with anomalously low magnetic fields, while the majority of highly irradiated exoplanetary atmospheres are entirely dominated by zonal jets. C1 [Batygin, Konstantin] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Stanley, Sabine] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Stevenson, David J.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Batygin, K (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM kbatygin@cfa.harvard.edu FU ITC Prize Postdoctoral Fellowship at the Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics; Natural Sciences and Engineering Research Council of Canada (NSERC); Alfred P. Sloan Foundation FX We thank Adam Showman, Kristen Menou, Peter Goldreich, and Greg Laughlin for useful conversations, as well as the anonymous referee for a thorough and insightful report. K. B. acknowledges the generous support from the ITC Prize Postdoctoral Fellowship at the Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics. S. S. acknowledges funding by the Natural Sciences and Engineering Research Council of Canada (NSERC) and the Alfred P. Sloan Foundation. NR 48 TC 14 Z9 14 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2013 VL 776 IS 1 AR 53 DI 10.1088/0004-637X/776/1/53 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000053 ER PT J AU Chandran, BDG Verscharen, D Quataert, E Kasper, JC Isenberg, PA Bourouaine, S AF Chandran, B. D. G. Verscharen, D. Quataert, E. Kasper, J. C. Isenberg, P. A. Bourouaine, S. TI STOCHASTIC HEATING, DIFFERENTIAL FLOW, AND THE ALPHA-TO-PROTON TEMPERATURE RATIO IN THE SOLAR WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE plasmas; solar wind; Sun: corona; turbulence; waves ID ALFVEN-WAVE TURBULENCE; INCOMPRESSIBLE MAGNETOHYDRODYNAMIC TURBULENCE; ION-CYCLOTRON WAVES; MAGNETIC-FIELD; CORONAL HOLES; VELOCITY DISTRIBUTIONS; TRANSITION REGION; MINOR IONS; ANISOTROPY; FLUCTUATIONS AB We extend previous theories of stochastic ion heating to account for the motion of ions along the magnetic field B. We derive an analytic expression for the temperature ratio T-perpendicular to i/T-perpendicular to p in the solar wind assuming that stochastic heating is the dominant ion heating mechanism, where T-perpendicular to i is the perpendicular temperature of species i and T-perpendicular to p is the perpendicular proton temperature. This expression describes how T-perpendicular to i/T-perpendicular to p depends upon U-i and beta(parallel to p), where U-i is the average velocity along B of species i in the proton frame and beta(parallel to p) is the ratio of the parallel proton pressure to the magnetic pressure, which we take to be less than or similar to 1. We compare our model with previously published measurements of alpha particles and protons from the Wind spacecraft. We find that stochastic heating offers a promising explanation for the dependence of T-perpendicular to alpha/T-perpendicular to p on U-alpha and beta(parallel to p) when the fractional cross helicity and Alfven ratio at the proton-gyroradius scale have values that are broadly consistent with solar-wind measurements. We also predict how the temperatures of other ion species depend on their drift speeds. C1 [Chandran, B. D. G.; Verscharen, D.; Isenberg, P. A.; Bourouaine, S.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Chandran, B. D. G.; Verscharen, D.; Isenberg, P. A.; Bourouaine, S.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Chandran, B. D. G.] Univ Oxford, Merton Coll, Oxford OX1 4JD, England. [Quataert, E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Quataert, E.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chandran, BDG (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. EM benjamin.chandran@unh.edu; daniel.verscharen@unh.edu; eliot@astro.berkeley.edu; jkasper@cfa.harvard.edu; phil.isenberg@unh.edu; s.bourouaine@unh.edu OI Verscharen, Daniel/0000-0002-0497-1096 FU NASA [NNX11AJ37G, NNN06AA01C, NNX13AF97G]; NSF [AGS-0851005]; NSF/DOE [AGS-1003451]; DOE [DE-FG02-07-ER46372]; Merton College, University of Oxford; Simons Foundation; David and Lucile Packard Foundation; Thomas Alison Schneider Chair in Physics at UC Berkeley FX We thank A. Schekochihin for helpful discussions and the referee for valuable suggestions. This work was supported by grant NNX11AJ37G from NASA's Heliophysics Theory Program, NASA grant NNN06AA01C to the Solar Probe Plus FIELDS Experiment, NASA grant NNX13AF97G, NSF grant AGS-0851005, NSF/DOE grant AGS-1003451, and DOE grant DE-FG02-07-ER46372. B. Chandran was supported by a Visiting Research Fellowship from Merton College, University of Oxford. E. Quataert was supported by a Simons Investigator award from the Simons Foundation, the David and Lucile Packard Foundation, and the Thomas Alison Schneider Chair in Physics at UC Berkeley. NR 67 TC 17 Z9 17 U1 3 U2 15 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2013 VL 776 IS 1 AR 45 DI 10.1088/0004-637X/776/1/45 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000045 ER PT J AU Currie, T Burrows, A Madhusudhan, N Fukagawa, M Girard, JH Dawson, R Murray-Clay, R Kenyon, S Kuchner, M Matsumura, S Jayawardhana, R Chambers, J Bromley, B AF Currie, Thayne Burrows, Adam Madhusudhan, Nikku Fukagawa, Misato Girard, Julien H. Dawson, Rebekah Murray-Clay, Ruth Kenyon, Scott Kuchner, Marc Matsumura, Soko Jayawardhana, Ray Chambers, John Bromley, Ben TI A COMBINED VERY LARGE TELESCOPE AND GEMINI STUDY OF THE ATMOSPHERE OF THE DIRECTLY IMAGED PLANET, beta PICTORIS b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: early-type; stars: individual (beta Pictoris) ID SPECTRAL IRRADIANCE CALIBRATION; CANDIDATE SUBSTELLAR COMPANION; FINDING CAMPAIGN DISCOVERY; EXTRASOLAR GIANT PLANETS; DIRECT-IMAGING DISCOVERY; YOUNG SOLAR ANALOG; ORBITING HR 8799; MU-M; UPPER SCORPIUS; BROWN DWARFS AB We analyze new/archival VLT/NaCo and Gemini/NICI high-contrast imaging of the young, self-luminous planet beta Pictoris b in seven near-to-mid IR photometric filters, using advanced image processing methods to achieve high signal-to-noise, high precision measurements. While beta Pic b's near-IR colors mimic those of a standard, cloudy early-to-mid L dwarf, it is overluminous in the mid-infrared compared to the field L/T dwarf sequence. Few substellar/planet-mass objects-i.e., kappa And b and 1RXJ 1609B-match beta Pic b's JHK(s)L' photometry and its 3.1 mu m and 5 mu m photometry are particularly difficult to reproduce. Atmosphere models adopting cloud prescriptions and large (similar to 60 mu m) dust grains fail to reproduce the beta Pic b spectrum. However, models incorporating thick clouds similar to those found for HR 8799 bcde, but also with small (a few microns) modal particle sizes, yield fits consistent with the data within the uncertainties. Assuming solar abundance models, thick clouds, and small dust particles (< a > = 4 mu m), we derive atmosphere parameters of log(g) = 3.8 +/- 0.2 and T-eff = 1575-1650 K, an inferred mass of 7(-3)(+4) M-J, and a luminosity of log(L/L-circle dot) similar to -3.80 +/- 0.02. The best-estimated planet radius, approximate to 1.65 +/- 0.06 R-J, is near the upper end of allowable planet radii for hot-start models given the host star's age and likely reflects challenges constructing accurate atmospheric models. Alternatively, these radii are comfortably consistent with hot-start model predictions if beta Pic b is younger than approximate to 7 Myr, consistent with a late formation well after its host star's birth similar to 12(-4)(+8) Myr ago. C1 [Currie, Thayne; Jayawardhana, Ray] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Madhusudhan, Nikku] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Fukagawa, Misato] Osaka Univ, Toyonaka, Osaka 5600043, Japan. [Girard, Julien H.] European So Observ, Santiago 19, Chile. [Dawson, Rebekah; Murray-Clay, Ruth; Kenyon, Scott] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kuchner, Marc] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Matsumura, Soko] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Chambers, John] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Bromley, Ben] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Currie, T (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. FU McLean Postdoctoral Fellowship; NSF-GRFP [DGE-1144152] FX We thank Christian Thalmann, France Allard, and the anonymous referee for helpful comments and discussions and Michael Cushing for providing IRTF/SpeX and Subaru/IRCS spectra of field L dwarfs. We are grateful to the telescope staff at ESO Paranal Observatory and Gemini-South Cerro Pachon Observatory for support for our observations, all of which were obtained with "delegated visitor mode" or "eavesdropping mode." Finally, we thank Christian Marois for very detailed discussions on image processing techniques and extensive helpful suggestions that improved this manuscript. T. C. acknowledges support from a McLean Postdoctoral Fellowship. R. D. acknowledges NSF-GRFP grant DGE-1144152. NR 91 TC 38 Z9 38 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 OCT 10 PY 2013 VL 776 IS 1 AR 15 DI 10.1088/0004-637X/776/1/15 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000015 ER PT J AU Farrah, D Lebouteiller, V Spoon, HWW Bernard-Salas, J Pearson, C Rigopoulou, D Smith, HA Gonzalez-Alfonso, E Clements, DL Efstathiou, A Cormier, D Afonso, J Petty, SM Harris, K Hurley, P Borys, C Verma, A Cooray, A Salvatelli, V AF Farrah, D. Lebouteiller, V. Spoon, H. W. W. Bernard-Salas, J. Pearson, C. Rigopoulou, D. Smith, H. A. Gonzalez-Alfonso, E. Clements, D. L. Efstathiou, A. Cormier, D. Afonso, J. Petty, S. M. Harris, K. Hurley, P. Borys, C. Verma, A. Cooray, A. Salvatelli, V. TI FAR-INFRARED FINE-STRUCTURE LINE DIAGNOSTICS OF ULTRALUMINOUS INFRARED GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: ISM; galaxies: starburst; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; STAR-FORMATION RATE; SPECTRAL ENERGY-DISTRIBUTIONS; POLYCYCLIC AROMATIC-HYDROCARBONS; SPITZER-SPACE-TELESCOPE; BLACK-HOLE MASSES; SIMILAR-TO 2; 158 MU-M; HERSCHEL-PACS OBSERVATIONS; HUBBLE-DEEP-FIELD AB We present Herschel observations of 6 fine-structure lines in 25 ultraluminous infrared galaxies at z < 0.27. The lines, [O III]52 mu m, [N III] 57 mu m, [O I]63 mu m, [N II]122 mu m, [O I]145 mu m, and [C II]158 mu m, are mostly single Gaussians with widths < 600 km s(-1) and luminosities of 10(7)-10(9) L-circle dot. There are deficits in the [O I] 63/L-IR, [N II]/L-IR, [O I]145/L-IR, and [C II]/L-IR ratios compared to lower luminosity systems. The majority of the line deficits are consistent with dustier H II regions, but part of the [C II] deficit may arise from an additional mechanism, plausibly charged dust grains. This is consistent with some of the [C II] originating from photodissociation regions or the interstellar medium (ISM). We derive relations between far-IR line luminosities and both the IR luminosity and star formation rate. We find that [N II] and both [O I] lines are good tracers of the IR luminosity and star formation rate. In contrast, [C II] is a poor tracer of the IR luminosity and star formation rate, and does not improve as a tracer of either quantity if the [C II] deficit is accounted for. The continuum luminosity densities also correlate with the IR luminosity and star formation rate. We derive ranges for the gas density and ultraviolet radiation intensity of 10(1) < n < 10(2.5) and 10(2.2) < G(0) < 10(3.6), respectively. These ranges depend on optical type, the importance of star formation, and merger stage. We do not find relationships between far-IR line properties and several other parameters: active galactic nucleus (AGN) activity, merger stage, mid-IR excitation, and SMBH mass. We conclude that these far-IR lines arise from gas heated by starlight, and that they are not strongly influenced by AGN activity. C1 [Farrah, D.; Petty, S. M.; Harris, K.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Lebouteiller, V.; Spoon, H. W. W.] Cornell Univ, CRSR, Ithaca, NY 14853 USA. [Lebouteiller, V.] CEA Saclay, DSM IRFU SAp, F-91191 Gif Sur Yvette, France. [Bernard-Salas, J.; Pearson, C.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Pearson, C.; Rigopoulou, D.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Rigopoulou, D.; Verma, A.] Univ Oxford, Oxford Astrophys, Oxford OX1 3RH, England. [Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gonzalez-Alfonso, E.] Univ Alcala De Henares, Dept Fis & Matemat, E-28871 Madrid, Spain. [Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. [Efstathiou, A.] European Univ Cyprus, Sch Sci, CY-1516 Nicosia, Cyprus. [Cormier, D.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Afonso, J.] Univ Lisbon, Ctr Astron & Astrofis, Observ Astron Lisboa, P-1349018 Lisbon, Portugal. [Afonso, J.] Univ Lisbon, Fac Sci, Dept Phys, P-1749016 Lisbon, Portugal. [Hurley, P.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Borys, C.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Salvatelli, V.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Salvatelli, V.] Univ Roma La Sapienza, Ist Nazl Fis Nucl, I-00185 Rome, Italy. RP Farrah, D (reprint author), Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. RI Afonso, Jose/B-5185-2013; OI Afonso, Jose/0000-0002-9149-2973; Lebouteiller, Vianney/0000-0002-7716-6223 FU NASA; CEA/Marie Curie Eurotalents fellowship; Science and Technology Foundation (FCT, Portugal) [PTDC/CTE-AST/105287/2008, PEst-OE/FIS/UI2751/2011, PTDC/FIS-AST/2194/2012]; Spanish Ministerio de Economia y Competitividad [AYA2010-21697-C05-0, FIS2012-39162-C06-01] FX We thank the staff of the Herschel helpdesk for many valuable discussions, and the referee for a very helpful report. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work is based on observations made with the Spitzer Space Telescope. Spitzer is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This research has made extensive use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA, and of NASA's Astrophysics Data System. This research has also made use of Ned Wright's online cosmology calculator (Wright 2006). V. L. is supported by a CEA/Marie Curie Eurotalents fellowship. J.A. acknowledges support from the Science and Technology Foundation (FCT, Portugal) through the research grants PTDC/CTE-AST/105287/2008, PEst-OE/FIS/UI2751/2011, and PTDC/FIS-AST/2194/2012. E. G.-A. is a Research Associate at the Harvard-Smithsonian Center for Astrophysics and thanks the support by the Spanish Ministerio de Economia y Competitividad under projects AYA2010-21697-C05-0 and FIS2012-39162-C06-01. NR 169 TC 44 Z9 44 U1 2 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2013 VL 776 IS 1 AR 38 DI 10.1088/0004-637X/776/1/38 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000038 ER PT J AU Fong, W Berger, E AF Fong, W. Berger, E. TI THE LOCATIONS OF SHORT GAMMA-RAY BURSTS AS EVIDENCE FOR COMPACT OBJECT BINARY PROGENITORS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general ID CORE-COLLAPSE SUPERNOVAE; GALAXY LUMINOSITY FUNCTION; NEUTRON-STAR SYSTEMS; SHORT GRB 111117A; HOST GALAXIES; OBSERVATIONAL CONSTRAINTS; OPTICAL AFTERGLOWS; EXTENDED EMISSION; FORMATION RATES; EVOLUTION AB We present a detailed investigation of Hubble Space Telescope rest-frame UV/optical observations of 22 short gamma-ray burst (GRB) host galaxies and sub-galactic environments. Utilizing the high angular resolution and depth of HST we characterize the host galaxy morphologies, measure precise projected physical and host-normalized offsets between the bursts and host centers, and calculate the locations of the bursts with respect to their host light distributions (rest-frame UV and optical). We calculate a median short GRB projected physical offset of 4.5 kpc, about 3.5 times larger than that for long GRBs, and find that approximate to 25% of short GRBs have offsets of greater than or similar to 10 kpc. When compared to their host sizes, the median offset is 1.5 half-light radii (r(e)), about 1.5 times larger than the values for long GRBs, core-collapse supernovae, and Type Ia supernovae. In addition, approximate to 20% of short GRBs having offsets of greater than or similar to 5r(e), and only approximate to 25% are located within 1r(e). We further find that short GRBs severely under-represent their hosts' rest-frame optical and UV light, with approximate to 30%-45% of the bursts located in regions of their host galaxies that have no detectable stellar light, and approximate to 55% in the regions with no UV light. Therefore, short GRBs do not occur in regions of star formation or even stellar mass. This demonstrates that the progenitor systems of short GRBs must migrate from their birth sites to their eventual explosion sites, a signature of kicks in compact object binary systems. Utilizing the full sample of offsets, we estimate natal kick velocities of approximate to 20-140 km s(-1). These independent lines of evidence provide the strongest support to date that short GRBs result from the merger of compact object binaries (NS-NS/NS-BH). C1 [Fong, W.; Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fong, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Science Foundation [AST-1107973]; NASA/Swift [NNX10AI24G, NNX12AD69G]; NASA [NAS 5-26555] FX The Berger GRB group is supported by the National Science Foundation under grant AST-1107973, and previously by NASA/Swift AO6 grant NNX10AI24G and A07 grant NNX12AD69G. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This work is based in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 59.A-9002(D), 079.D-0909(C), 080.D-0906(G), 081.D-0588(C), 083.D-0606(C), and 084.D-0621(B). Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. NR 85 TC 53 Z9 55 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2013 VL 776 IS 1 AR 18 DI 10.1088/0004-637X/776/1/18 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000018 ER PT J AU Moullet, A Lellouch, E Moreno, R Gurwell, M Black, JH Butler, B AF Moullet, A. Lellouch, E. Moreno, R. Gurwell, M. Black, J. H. Butler, B. TI EXPLORING IO'S ATMOSPHERIC COMPOSITION WITH APEX: FIRST MEASUREMENT OF (SO2)-S-34 AND TENTATIVE DETECTION OF KCl SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: atmospheres; submillimeter: planetary systems ID SO2 ATMOSPHERE; VOLCANIC GASES; ISOTOPIC COMPOSITION; DRIVEN ATMOSPHERE; SULFUR MONOXIDE; NEUTRAL CLOUDS; PELE PLUME; SURFACE; SODIUM; SPECTROSCOPY AB The composition of Io's tenuous atmosphere is poorly constrained. Only the major species SO2 and a handful of minor species have been positively identified, but a variety of other molecular species should be present, based on thermochemical equilibrium models of volcanic gas chemistry and the composition of Io's environment. This paper focuses on the spectral search for expected yet undetected molecular species (KCl, SiO, S2O) and isotopes ((SO2)-S-34). We analyze a disk-averaged spectrum of a potentially line-rich spectral window around 345 GHz, obtained in 2010 at the APEX 12 m antenna. Using different models assuming either extended atmospheric distributions or a purely volcanically sustained atmosphere, we tentatively measure the KCl relative abundance with respect to SO2 and derive a range of 4 x 10(-4)-8 x 10(-3). We do not detect SiO or S2O and present new upper limits on their abundances. We also present the first measurement of the S-34/S-32 isotopic ratio in gas phase on Io, which appears to be twice as high as the Earth and interstellar medium reference values. Strong lines of SO2 and SO are also analyzed to check for longitudinal variations of column density and relative abundance. Our models show that, based on their predicted relative abundance with respect to SO2 in volcanic plumes, both the tentative KCl detection and SiO upper limit are compatible with a purely volcanic origin for these species. C1 [Moullet, A.] Natl Radio Astron Observ, Charlottesville, VA 22902 USA. [Lellouch, E.; Moreno, R.] Observ Paris, LESIA, F-92195 Meudon, France. [Gurwell, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Black, J. H.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Butler, B.] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Moullet, A (reprint author), Natl Radio Astron Observ, Charlottesville, VA 22902 USA. NR 60 TC 4 Z9 4 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2013 VL 776 IS 1 AR 32 DI 10.1088/0004-637X/776/1/32 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000032 ER PT J AU Pan, LB Padoan, P AF Pan, Liubin Padoan, Paolo TI TURBULENCE-INDUCED RELATIVE VELOCITY OF DUST PARTICLES. I. IDENTICAL PARTICLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE minor planets, asteroids: general; planets and satellites: formation; protoplanetary disks; turbulence ID BIDISPERSE INERTIAL PARTICLES; ISOTROPIC TURBULENCE; PROTOPLANETARY NEBULA; COLLISION RATES; PAIR DISPERSION; GROWTH PEBBLES; PREFERENTIAL CONCENTRATION; INTERMITTENT DISTRIBUTION; PLANETESIMAL FORMATION; SIZE DISTRIBUTION AB We study the relative velocity of inertial particles suspended in turbulent flows and discuss implications for dust particle collisions in protoplanetary disks. We simulate a weakly compressible turbulent flow, evolving 14 particle species with friction timescale, tau(p), covering the entire range of scales in the flow. The particle Stokes numbers, St, measuring the ratio of tau(p) to the Kolmogorov timescale, are in the range 0.1 less than or similar to St less than or similar to 800. Using simulation results, we show that the model by Pan & Padoan gives satisfactory predictions for the rms relative velocity between identical particles. The probability distribution function (PDF) of the relative velocity is found to be highly non-Gaussian. The PDF tails are well described by a 4/3 stretched exponential function for particles with tau(p) similar or equal to 1-2 T-L, where T-L is the Lagrangian correlation timescale, consistent with a prediction based on PP10. The PDF approaches Gaussian only for very large particles with tau(p) greater than or similar to 54 T-L. We split particle pairs at given distances into two types with low and high relative speeds, referred to as continuous and caustic types, respectively, and compute their contributions to the collision kernel. Although amplified by the effect of clustering, the continuous contribution vanishes in the limit of infinitesimal particle distance, where the caustic contribution dominates. The caustic kernel per unit cross section rises rapidly as St increases toward similar or equal to 1, reaches a maximum at tau(p) similar or equal to 2 T-L, and decreases as tau(-1/2)(p) for tau(p) >> T-L. C1 [Pan, Liubin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Padoan, Paolo] ICREA, E-08028 Barcelona, Spain. [Padoan, Paolo] Univ Barcelona, ICC, E-08028 Barcelona, Spain. RP Pan, LB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lpan@cfa.harvard.edu; ppadoan@icc.ub.edu OI Padoan, Paolo/0000-0002-5055-5800 FU FP7-PEOPLE-RG grant [PIRG07-GA-2010-261359] FX We thank the referee, Alexander Hubbard, for an extensive report that helped us improve the paper, and Anders Johansen for useful discussions and for support with the Pencil code. P.P. is supported by the FP7-PEOPLE-2010-RG grant PIRG07-GA-2010-261359. The simulations were carried out on the NASA/Ames Pleiades supercomputer. NR 81 TC 16 Z9 16 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2013 VL 776 IS 1 AR 12 DI 10.1088/0004-637X/776/1/12 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000012 ER PT J AU Rasia, E Borgani, S Ettori, S Mazzotta, P Meneghetti, M AF Rasia, E. Borgani, S. Ettori, S. Mazzotta, P. Meneghetti, M. TI ON THE DISCREPANCY BETWEEN THEORETICAL AND X-RAY CONCENTRATION-MASS RELATIONS FOR GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; galaxies: clusters: general; galaxies: clusters: intracluster medium; methods: numerical; X-rays: galaxies: clusters ID DARK-MATTER HALOES; CUSP-CORE TRANSFORMATIONS; ACTIVE GALACTIC NUCLEI; SCALING RELATIONS; HYDRODYNAMICAL SIMULATIONS; COSMOLOGICAL SIMULATIONS; ENERGY COSMOLOGIES; POWER SPECTRUM; TEMPERATURE RELATION; DENSITY PROFILES AB In the past 15 years, the concentration-mass relation has been investigated diffusely in theoretical studies. On the other hand, only recently has this relation been derived from X-ray observations. When that happened, the results caused a certain level of concern: the X-ray normalizations and slopes were found significantly dissimilar from those predicted by theory. We analyzed 52 galaxy clusters and groups, simulated with different descriptions of the physical processes that affect the baryonic component, with the purpose of determining whether these discrepancies are real or induced by biases in the computation of the concentration parameter or in the determination of the selection function of the cluster sample for which the analysis is carried out. In particular, we investigate how the simulated concentration-mass relation depends (1) on the radial range used to derive the concentration; (2) on the presence of baryons in the simulations, and on the effect of star formation and feedback from supernovae and active galactic nuclei (AGNs). Finally, we evaluate (3) how the results differ when adopting an X-ray approach for the analysis and (4) how the selection function based on X-ray luminosity can impact the results. All effects studied go in the direction of alleviating the discrepancy between observations and simulations, although with different significance: while the choice of the radial range to fit the profiles and the inclusion of the baryonic component play only a minor role, the X-ray approach to reconstruct the mass profiles and the selection of the cluster sample have a strong impact on the resulting concentration-mass relation. Extending the fit to the most central regions or reducing the fitting radius from the virial boundary to the typical X-ray external radius causes an increase of the normalization in radiative simulations by 5%-10%. In the second case, we measure a slope that is up to twice steeper than that derived by using the typical theoretical radial range. Radiative simulations including only supernova feedback produce 30% higher concentrations than the dark matter case. Such a difference is largely reduced when including the effect of AGN feedback. The concentration-mass relation derived from the X-ray synthetic catalog is significantly steeper due to the combination of several different effects, such as environment, dynamical state and dynamical history of the clusters, bias in mass and temperature measurements, and their dependence on the radius and on the mass of the system. Finally, selecting clusters according to their X-ray luminosity produces a net increase in both normalization and slope of the relation, since at fixed mass, the most luminous clusters are also the most concentrated. C1 [Rasia, E.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Borgani, S.] Univ Trieste, Dipartimento Fis, Sez Astron, I-34131 Trieste, Italy. [Borgani, S.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Borgani, S.] Ist Nazl Fis Nucl, Trieste, Italy. [Ettori, S.; Meneghetti, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Ettori, S.; Meneghetti, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Mazzotta, P.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Mazzotta, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rasia, E (reprint author), Univ Michigan, Dept Phys, 450 Church St, Ann Arbor, MI 48109 USA. RI Ettori, Stefano/N-5004-2015; Meneghetti, Massimo/O-8139-2015; Mazzotta, Pasquale/B-1225-2016; OI Ettori, Stefano/0000-0003-4117-8617; Meneghetti, Massimo/0000-0003-1225-7084; Mazzotta, Pasquale/0000-0002-5411-1748; rasia, elena/0000-0003-4175-002X; Borgani, Stefano/0000-0001-6151-6439 FU National Science Foundation [AST-1210973, SAO TM3-14008X]; NASA [NAS8-03060]; ASI-INAF [I/023/05/0, I/088/06/0]; Marie Curie Initial Training Network CosmoComp within the European Commission [PITN-GA-2009-238356]; PRIN-INAF; PRIN-MIUR; INFN PD51; Michigan Center for Theoretical Physics FX We are grateful to the sharp and attentive report by the anonymous referee. E. R. thanks Cosimo Fedeli for sharing his results on the concentration-mass relation and for discussions at the early stage of this project and Cristiano De Boni for making available the tables of the WMAP cosmological box of De Boni et al. (2011) and De Boni et al. (2013). We thank Volker Springel for providing us with the GADGET-3 code. Simulations have been carried out at the CINECA supercomputing centre in Bologna, with CPU time assigned through ISCRA proposals and through an agreement with University of Trieste. We acknowledge financial support by the following grants: National Science Foundation AST-1210973, SAO TM3-14008X (issued under NASA Contract No. NAS8-03060), ASI-INAF I/023/05/0 and I/088/06/0, Marie Curie Initial Training Network CosmoComp (PITN-GA-2009-238356) funded within the European Commission's Framework Programme 7, PRIN-INAF09 project "Towards an Italian Network for Computational Cosmology," PRIN-MIUR09 "Tracing the growth of structures in the Universe," and INFN PD51. E. R. and M. M. would like to thank the Michigan Center for Theoretical Physics for supporting the collaboration. NR 98 TC 10 Z9 10 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2013 VL 776 IS 1 AR 39 DI 10.1088/0004-637X/776/1/39 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000039 ER PT J AU Thyagarajan, N Shankar, NU Subrahmanyan, R Arcus, W Bernardi, G Bowman, JD Briggs, F Bunton, JD Cappallo, RJ Corey, BE deSouza, L Emrich, D Gaensler, BM Goeke, RF Greenhill, LJ Hazelton, BJ Herne, D Hewitt, JN Johnston-Hollitt, M Kaplan, DL Kasper, JC Kincaid, BB Koenig, R Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, EH Oberoi, D Ord, SM Pathikulangara, J Remillard, RA Rogers, AEE Roshi, DA Salah, JE Sault, RJ Srivani, KS Stevens, JB Thiagaraj, P Tingay, SJ Wayth, RB Waterson, M Webster, RL Whitney, AR Williams, AJ Williams, CL Wyithe, JSB AF Thyagarajan, Nithyanandan Shankar, N. Udaya Subrahmanyan, Ravi Arcus, Wayne Bernardi, Gianni Bowman, Judd D. Briggs, Frank Bunton, John D. Cappallo, Roger J. Corey, Brian E. deSouza, Ludi Emrich, David Gaensler, Bryan M. Goeke, Robert F. Greenhill, Lincoln J. Hazelton, Bryna J. Herne, David Hewitt, Jacqueline N. Johnston-Hollitt, Melanie Kaplan, David L. Kasper, Justin C. Kincaid, Barton B. Koenig, Ronald Kratzenberg, Eric Lonsdale, Colin J. Lynch, Mervyn J. McWhirter, S. Russell Mitchell, Daniel A. Morales, Miguel F. Morgan, Edward H. Oberoi, Divya Ord, Stephen M. Pathikulangara, Joseph Remillard, Ronald A. Rogers, Alan E. E. Roshi, D. Anish Salah, Joseph E. Sault, Robert J. Srivani, K. S. Stevens, Jamie B. Thiagaraj, Prabu Tingay, Steven J. Wayth, Randall B. Waterson, Mark Webster, Rachel L. Whitney, Alan R. Williams, Andrew J. Williams, Christopher L. Wyithe, J. Stuart B. TI A STUDY OF FUNDAMENTAL LIMITATIONS TO STATISTICAL DETECTION OF REDSHIFTED Hi FROM THE EPOCH OF REIONIZATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark ages, reionization, first stars; large-scale structure of universe; methods: statistical; radio continuum: galaxies; radio lines: general; techniques: interferometric ID MURCHISON-WIDEFIELD-ARRAY; PROBE WMAP OBSERVATIONS; 21 CENTIMETER FLUCTUATIONS; POWER SPECTRUM; INTERGALACTIC MEDIUM; COSMIC REIONIZATION; RADIO-SOURCES; CM RADIATION; DARK-AGES; 150 MHZ AB In this paper, we explore for the first time the relative magnitudes of three fundamental sources of uncertainty, namely, foreground contamination, thermal noise, and sample variance, in detecting the Hi power spectrum from the epoch of reionization (EoR). We derive limits on the sensitivity of a Fourier synthesis telescope to detect EoR based on its array configuration and a statistical representation of images made by the instrument. We use the Murchison Widefield Array (MWA) configuration for our studies. Using a unified framework for estimating signal and noise components in the Hi power spectrum, we derive an expression for and estimate the contamination from extragalactic point-like sources in three-dimensional k-space. Sensitivity for EoR Hi power spectrum detection is estimated for different observing modes with MWA. With 1000 hr of observing on a single field using the 128 tile MWA, EoR detection is feasible (S/N > 1 for k less than or similar to 0.8 Mpc(-1)). Bandpass shaping and refinements to the EoR window are found to be effective in containing foreground contamination, which makes the instrument tolerant to imaging errors. We find that for a given observing time, observing many independent fields of view does not offer an advantage over a single field observation when thermal noise dominates over other uncertainties in the derived power spectrum. C1 [Thyagarajan, Nithyanandan; Shankar, N. Udaya; Subrahmanyan, Ravi; Srivani, K. S.; Thiagaraj, Prabu] Raman Res Inst, Bangalore 560080, Karnataka, India. [Subrahmanyan, Ravi] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Subrahmanyan, Ravi; Briggs, Frank; Gaensler, Bryan M.; Mitchell, Daniel A.; Ord, Stephen M.; Wayth, Randall B.; Webster, Rachel L.; Wyithe, J. Stuart B.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [Arcus, Wayne; Emrich, David; Herne, David; Lynch, Mervyn J.; Ord, Stephen M.; Tingay, Steven J.; Wayth, Randall B.; Waterson, Mark; Williams, Andrew J.] Curtin Univ, Perth, WA 6845, Australia. [Bernardi, Gianni; Greenhill, Lincoln J.; Kasper, Justin C.; Ord, Stephen M.; Wayth, Randall B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Bowman, Judd D.] Arizona State Univ, Tempe, AZ USA. [Briggs, Frank; Waterson, Mark] Australian Natl Univ, Canberra, ACT, Australia. [Bunton, John D.; deSouza, Ludi; Koenig, Ronald; Pathikulangara, Joseph; Stevens, Jamie B.] CSIRO Astron & Space Sci, Sydney, NSW, Australia. [Cappallo, Roger J.; Corey, Brian E.; Kincaid, Barton B.; Kratzenberg, Eric; Lonsdale, Colin J.; McWhirter, S. Russell; Rogers, Alan E. E.; Salah, Joseph E.; Whitney, Alan R.] MIT, Haystack Observ, Westford, MA 01886 USA. [deSouza, Ludi; Gaensler, Bryan M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Goeke, Robert F.; Hewitt, Jacqueline N.; Morgan, Edward H.; Remillard, Ronald A.; Williams, Christopher L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hazelton, Bryna J.; Morales, Miguel F.] Univ Washington, Seattle, WA 98195 USA. [Johnston-Hollitt, Melanie] Victoria Univ Wellington, Wellington, New Zealand. [Kaplan, David L.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Mitchell, Daniel A.; Sault, Robert J.; Webster, Rachel L.; Wyithe, J. Stuart B.] Univ Melbourne, Melbourne, Vic, Australia. [Oberoi, Divya] Tata Inst Fundamental Res, Pune, Maharashtra, India. [Roshi, D. Anish] Natl Radio Astron Observ, Charlottesville, VA USA. [Stevens, Jamie B.] Univ Tasmania, Hobart, Tas, Australia. RP Thyagarajan, N (reprint author), Raman Res Inst, Bangalore 560080, Karnataka, India. EM nithya.rri@gmail.com RI Bunton, John/A-4944-2008; Wayth, Randall/B-2444-2013; Udayashankar , N/D-4901-2012; Williams, Andrew/K-2931-2013; M, Manjunath/N-4000-2014; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; OI Gaensler, Bryan/0000-0002-3382-9558; Wayth, Randall/0000-0002-6995-4131; Williams, Andrew/0000-0001-9080-0105; M, Manjunath/0000-0001-8710-0730; Emrich, David/0000-0002-4058-1837; Wyithe, Stuart/0000-0001-7956-9758 FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence); Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington [MED-E1799]; Victoria University of Wellington from the New Zealand Ministry of Economic Development; Victoria University of Wellington from IBM Shared University Research Grant; Australian Federal government; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University; Western Australian State government; [CE110001020] FX This scientific work makes use of the Murchison Radio-astronomy Observatory. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and the University of Western Australia, funded by the Western Australian State government. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 51 TC 44 Z9 44 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2013 VL 776 IS 1 AR 6 DI 10.1088/0004-637X/776/1/6 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 225UM UT WOS:000324989000006 ER PT J AU Fedele, D Bruderer, S van Dishoeck, EF Hogerheijde, MR Panic, O Brown, JM Henning, T AF Fedele, D. Bruderer, S. van Dishoeck, E. F. Hogerheijde, M. R. Panic, O. Brown, J. M. Henning, Th. TI PROBING THE RADIAL TEMPERATURE STRUCTURE OF PROTOPLANETARY DISKS WITH HERSCHEL/HIFI SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE protoplanetary disks ID MAIN-SEQUENCE STARS; HD 100546; CIRCUMSTELLAR DISKS; GAS TEMPERATURE; LINE EMISSION; MOLECULAR GAS; YOUNG STARS; WARM GAS; DM-TAU; MODELS AB Herschel/HIFI spectroscopic observations of CO J = 10-9, CO J = 16-15 and [C II] toward HD 100546 are presented. The objective is to resolve the velocity profile of the lines to address the emitting region of the transitions and directly probe the distribution of warm gas in the disk. The spectra reveal double-peaked CO line profiles centered on the systemic velocity, consistent with a disk origin. The J = 16-15 line profile is broader than that of the J = 10-9 line, which in turn is broader than those of lower-J transitions (6-5, 3-2, observed with APEX), thus showing a clear temperature gradient of the gas with radius. A power-law flat disk model is used to fit the CO line profiles and the CO rotational ladder simultaneously, yielding a temperature of T-0 = 1100 +/- 350 K (at r(0) = 13 AU) and an index of q = 0.85 +/- 0.1 for the temperature radial gradient. This indicates that the gas has a steeper radial temperature gradient than the dust (mean q(dust) 0.5), providing further proof of the thermal decoupling of gas and dust at the disk heights where the CO lines form. The [ C ii] line profile shows a strong single-peaked profile red-shifted by 0.5 km s-1 compared to the systemic velocity. We conclude that the bulk of the [C II] emission has a non-disk origin (e. g., remnant envelope or diffuse cloud). C1 [Fedele, D.; Bruderer, S.; van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [van Dishoeck, E. F.; Hogerheijde, M. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Panic, O.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Brown, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Fedele, D (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstra 1, D-85748 Garching, Germany. RI Fedele, Davide/L-8688-2013 OI Fedele, Davide/0000-0001-6156-0034 NR 34 TC 15 Z9 15 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 10 PY 2013 VL 776 IS 1 AR L3 DI 10.1088/2041-8205/776/1/L3 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 224TX UT WOS:000324913500003 ER PT J AU Schiavon, RP Caldwell, N Conroy, C Graves, GJ Strader, J MacArthur, LA Courteau, S Harding, P AF Schiavon, Ricardo P. Caldwell, Nelson Conroy, Charlie Graves, Genevieve J. Strader, Jay MacArthur, Lauren A. Courteau, Stephane Harding, Paul TI STAR CLUSTERS IN M31. V. EVIDENCE FOR SELF-ENRICHMENT IN OLD M31 CLUSTERS FROM INTEGRATED SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: star clusters: general; globular clusters: general ID MULTIPLE STELLAR POPULATIONS; GALACTIC GLOBULAR-CLUSTERS; MILKY-WAY; CHEMICAL EVOLUTION; ABUNDANCE PATTERNS; CATALOG; ORIGIN; PARAMETERS; GALAXIES; SPECTRA AB In the past decade, the notion that globular clusters (GCs) are composed of coeval stars with homogeneous initial chemical compositions has been challenged by growing evidence that they host an intricate stellar population mix, likely indicative of a complex history of star formation and chemical enrichment. Several models have been proposed to explain the existence of multiple stellar populations in GCs, but no single model provides a fully satisfactory match to existing data. Correlations between chemistry and global parameters such as cluster mass or luminosity are fundamental clues to the physics of GC formation. In this Letter, we present an analysis of the mean abundances of Fe, Mg, C, N, and Ca for 72 old GCs from the Andromeda galaxy. We show for the first time that there is a correlation between the masses of GCs and the mean stellar abundances of nitrogen, spanning almost two decades in mass. This result sheds new light on the formation of GCs, providing important constraints on their internal chemical evolution and mass loss history. C1 [Schiavon, Ricardo P.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Conroy, Charlie] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Graves, Genevieve J.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [MacArthur, Lauren A.] Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. [Courteau, Stephane] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON, Canada. [Harding, Paul] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. RP Schiavon, RP (reprint author), Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England. EM R.P.Schiavon@ljmu.ac.uk; caldwell@cfa.harvard.edu; cconroy@ucolick.org; graves@astro.princeton.edu; strader@pa.msu.edu; Lauren.MacArthur@nrc-cnrc.gc.ca; courteau@astro.queensu.ca; paul.harding@case.edu FU Gemini Observatory FX The authors thank the anonymous referee for a timely and very helpful review. R.P.S. thanks Bob Rood (in memoriam), Maurizio Salaris, Nate Bastian, and Inger Jorgensen for useful discussions. R.P.S. thanks the support of Gemini Observatory, where part of this research was conducted. NR 32 TC 8 Z9 8 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 OCT 10 PY 2013 VL 776 IS 1 AR L7 DI 10.1088/2041-8205/776/1/L7 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 224TX UT WOS:000324913500007 ER PT J AU Hayek, LAC Wilson, B AF Hayek, Lee-Ann C. Wilson, Brent TI Quantifying Assemblage Turnover and Species Contributions at Ecologic Boundaries SO PLOS ONE LA English DT Article ID QUATERNARY BENTHIC FORAMINIFERA; SEQUENCE STRATIGRAPHY; ORGANIC-CARBON; INDIAN-OCEAN; ARABIAN SEA; BLAKE RIDGE; NORTH-SEA; ATLANTIC; DIVERSITY; SLOPE AB Not all boundaries, whether stratigraphical or geographical, are marked by species-level changes in community composition. For example, paleodata for some sites do not show readily discernible glacial-interglacial contrasts. Rather, the proportional abundances of species can vary subtly between glacials and interglacials. This paper presents a simple quantitative measure of assemblage turnover (assemblage turnover index, ATI) that uses changes in species' proportional abundances to identify intervals of community change. A second, functionally-related index (conditioned-on-boundary index, CoBI) identifies species contributions to the total assemblage turnover. With these measures we examine benthonic foraminiferal assemblages to assess glacial/interglacial contrasts at abyssal depths. Our results indicate that these measures, ATI and CoBI, have potential as sequence stratigraphic tools in abyssal depth deposits. Many peaks in the set of values of ATI coincide with terminations at the end of glaciations and delineate peak-bounded ATI intervals (PATIs) separated by boundaries that approximate to glacial terminations and to transgressions at neritic depths. These measures, however, can be used to evaluate the assemblage turnover and composition at any defined ecological or paleoecological boundary. The section used is from Ocean Drilling Program (OPD) Hole 994C, drilled on the Blake Ridge, offshore SE USA. C1 [Hayek, Lee-Ann C.] Smithsonian Inst Math & Stat NMNH MRC 121, Washington, DC USA. [Wilson, Brent] Univ W Indies, Petr Geosci Programme, Dept Chem Engn, St Augustine, Trinid & Tobago. RP Wilson, B (reprint author), Univ W Indies, Petr Geosci Programme, Dept Chem Engn, St Augustine, Trinid & Tobago. EM brent.wilson@sta.uwi.edu FU U.S. National Science Foundation (NSF); Joint Oceanographic Institutions (JOI), Inc. FX This research used samples provided by the Ocean Drilling Program (ODP) that is sponsored by the U.S. National Science Foundation (NSF) and participating countries under management of Joint Oceanographic Institutions (JOI), Inc. Thanks are due to two anonymous reviewers, whose suggestions improved this paper markedly. NR 88 TC 4 Z9 5 U1 0 U2 10 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD OCT 9 PY 2013 VL 8 IS 10 AR e74999 DI 10.1371/journal.pone.0074999 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 236PJ UT WOS:000325810900014 PM 24130679 ER PT J AU Luiz, OJ Allen, AP Robertson, DR Floeter, SR Kulbicki, M Vigliola, L Becheler, R Madin, JS AF Luiz, Osmar J. Allen, Andrew P. Robertson, D. Ross Floeter, Sergio R. Kulbicki, Michel Vigliola, Laurent Becheler, Ronan Madin, Joshua S. TI Adult and larval traits as determinants of geographic range size among tropical reef fishes SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE macroecology; marine dispersal; colonization ID BODY-SIZE; DISPERSAL; PREDATORS; DURATION; CONNECTIVITY; BIOGEOGRAPHY; DIVERSITY; MORTALITY; ECOLOGY; OCEAN AB Most marine organisms disperse via ocean currents as larvae, so it is often assumed that larval-stage duration is the primary determinant of geographic range size. However, empirical tests of this relationship have yielded mixed results, and alternative hypotheses have rarely been considered. Here we assess the relative influence of adult and larval-traits on geographic range size using a global dataset encompassing 590 species of tropical reef fishes in 47 families, the largest compilation of such data to date for any marine group. We analyze this database using linear mixed-effect models to control for phylogeny and geographical limits on range size. Our analysis indicates that three adult traits likely to affect the capacity of new colonizers to survive and establish reproductive populations (body size, schooling behavior, and nocturnal activity) are equal or better predictors of geographic range size than pelagic larval duration. We conclude that adult life-history traits that affect the postdispersal persistence of new populations are primary determinants of successful range extension and, consequently, of geographic range size among tropical reef fishes. C1 [Luiz, Osmar J.; Allen, Andrew P.; Madin, Joshua S.] Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. [Robertson, D. Ross] Smithsonian Trop Res Inst, Balboa, Panama. [Floeter, Sergio R.] Univ Fed Santa Catarina, Dept Ecol & Zool, BR-88040900 Florianopolis, SC, Brazil. [Kulbicki, Michel] Inst Rech Dev UR227 CoReUs, LABEX Lab Excellence Arago, F-66651 Banyuls Sur Mer, France. [Vigliola, Laurent] Inst Rech Dev UR227 CoReUs, LABEX Lab Excellence Recifs Coralliens, Noumea 98848, New Caledonia. [Becheler, Ronan] IFREMER, Lab Environm Profond, F-29280 Plouzane, France. RP Luiz, OJ (reprint author), Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. EM osmarluizjr@gmail.com RI Floeter, Sergio/B-1438-2012; Luiz, Osmar/D-9202-2011; Vigliola, Laurent/J-7107-2016; OI Vigliola, Laurent/0000-0003-4715-7470; Luiz, Osmar/0000-0002-6995-6524; Madin, Joshua/0000-0002-5005-6227 FU International Macquarie University Research Excellence Scholarship; Smithsonian Tropical Research Institute; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq); Australian Research Council; "Resilience de communautes: role du couplage entre diversites taxonomique et fonctionnelle, les poissons de recif pour modele" (RESICOD) program; General Approach to Species-Abundance Relationships (GASPAR) program; US National Sea [R/LR-B-52] FX We thank R. Lecomte for her assistance with otholith work and for giving access to her laboratory facilities; C. Osenberg, C. St. Mary, T. Adam, B. Chockley, and many volunteers for their assistance in the field and at the laboratory; and Mark Hixon and two anonymous reviewers for comments in the manuscript. This study was supported in part by an International Macquarie University Research Excellence Scholarship (to O.J.L.); the Smithsonian Tropical Research Institute (D.R.R.); the SISBIOTA program by the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) (S.R.F.); and the Australian Research Council (J.S.M.). The Fondation de la Recherche pour la Biodiversite funded this research through the "Resilience de communautes: role du couplage entre diversites taxonomique et fonctionnelle, les poissons de recif pour modele" (RESICOD) program and the General Approach to Species-Abundance Relationships (GASPAR) program. Part of the data were collected through US National Sea Grant R/LR-B-52. NR 59 TC 35 Z9 35 U1 4 U2 65 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 OCT 8 PY 2013 VL 110 IS 41 BP 16498 EP 16502 DI 10.1073/pnas.1304074110 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 231ED UT WOS:000325395600054 PM 24065830 ER PT J AU Shaw, DW Escalante, P Rappole, JH Ramos, MA Oehlenschlager, RJ Warner, DW Winker, K AF Shaw, David W. Escalante, Patricia Rappole, John H. Ramos, Mario A. Oehlenschlager, Richard J. Warner, Dwain W. Winker, Kevin TI Decadal changes and delayed avian species losses due to deforestation in the northern Neotropics SO PEERJ LA English DT Article DE Birds; Ecology; Extinction; Conservation; Deforestation; Extirpation; Habitat loss; Species loss AB How avifauna respond to the long-term loss and fragmentation of tropical forests is a critical issue in biodiversity management. We use data from over 30 years to gain insights into such changes in the northernmost Neotropical rainforest in the Sierra de Los Tuxtlas of southern Veracruz, Mexico. This region has been extensively deforested over the past half-century. The Estacion de Biologia Tropical Los Tuxtlas, of the Universidad Nacional Autonoma de Mexico (UNAM), protects a 640 ha tract of lowland forest. It became relatively isolated from other forested tracts between 1975 and 1985, but it retains a corridor of forest to more extensive forests at higher elevations on Volcan San Martin. Most deforestation in this area occurred during the 1970s and early 1980s. Forest birds were sampled on the station and surrounding areas using mist nets during eight non-breeding seasons from 1973 to 2004 (though in some seasons netting extended into the local breeding season for some species). Our data suggested extirpations or declines in 12 species of birds subject to capture in mist nets. Six of the eight species no longer present were captured in 1992-95, but not in 2003-2004. Presence/absence data from netting and observational data suggested that another four low-density species also disappeared since sampling began. This indicates a substantial time lag between the loss of habitat and the apparent extirpation of these species. Delayed species loss and the heterogeneous nature of the species affected will be important factors in tropical forest management and conservation. C1 [Shaw, David W.; Winker, Kevin] Univ Alaska Museum, Fairbanks, AK 99775 USA. [Escalante, Patricia] Univ Nacl Autonoma Mexico, Inst Biol, Colecc Nacl Aves, Copilco, Coyoacan, Mexico. [Rappole, John H.] Smithsonians Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. [Oehlenschlager, Richard J.] Sci Museum Minnesota, St Paul, MN USA. RP Winker, K (reprint author), Univ Alaska Museum, Fairbanks, AK 99775 USA. EM kevin.winker@alaska.edu RI Winker, Kevin/M-2042-2014; Escalante, Patricia/B-8704-2014 OI Winker, Kevin/0000-0002-8985-8104; Escalante, Patricia/0000-0002-5531-263X FU University of Alaska Museum; Friends of Ornithology; Welder Wildlife Foundation; World Wildlife Fund (US); Smithsonian Institution; Friends of the National Zoo; Wildlife Conservation Society; Chicago Zoological Society; FOMIX (CONACyT-VERACRUZ) [109298] FX The University of Alaska Museum and the Friends of Ornithology provided financial support for this study in 2002 and 2004. Earlier seasons were supported by the Welder Wildlife Foundation, the World Wildlife Fund (US), the Smithsonian Institution, Friends of the National Zoo, the Wildlife Conservation Society, and the Chicago Zoological Society. This study is also part of project No. 109298 funded by FOMIX (CONACyT-VERACRUZ). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 90 TC 4 Z9 4 U1 0 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 OCT 8 PY 2013 VL 1 AR e179 DI 10.7717/peerj.179 PG 20 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA V36CH UT WOS:000209190500002 PM 24133637 ER PT J AU Andersson, N Baker, J Belczynski, K Bernuzzi, S Berti, E Cadonati, L Cerda-Duran, P Clark, J Favata, M Finn, LS Fryer, C Giacomazzo, B Gonzalez, JA Hendry, M Heng, IS Hild, S Johnson-McDaniel, N Kalmus, P Klimenko, S Kobayashi, S Kokkotas, K Laguna, P Lehner, L Levin, J Liebling, S MacFadyen, A Mandel, I Marka, S Marka, Z Neilsen, D O'Brien, P Perna, R Read, J Reisswig, C Rodriguez, C Ruffert, M Schnetter, E Searle, A Shawhan, P Shoemaker, D Soderberg, A Sperhake, U Sutton, P Tanvir, N Was, M Whitcomb, S AF Andersson, Nils Baker, John Belczynski, Krzystof Bernuzzi, Sebastiano Berti, Emanuele Cadonati, Laura Cerda-Duran, Pablo Clark, James Favata, Marc Finn, Lee Samuel Fryer, Chris Giacomazzo, Bruno Antonio Gonzalez, Jose Hendry, Martin Heng, Ik Siong Hild, Stefan Johnson-McDaniel, Nathan Kalmus, Peter Klimenko, Sergei Kobayashi, Shiho Kokkotas, Kostas Laguna, Pablo Lehner, Luis Levin, Janna Liebling, Steve MacFadyen, Andrew Mandel, Ilya Marka, Szabolcs Marka, Zsuzsa Neilsen, David O'Brien, Paul Perna, Rosalba Read, Jocelyn Reisswig, Christian Rodriguez, Carl Ruffert, Max Schnetter, Erik Searle, Antony Shawhan, Peter Shoemaker, Deirdre Soderberg, Alicia Sperhake, Ulrich Sutton, Patrick Tanvir, Nial Was, Michal Whitcomb, Stan TI The transient gravitational-wave sky SO CLASSICAL AND QUANTUM GRAVITY LA English DT Review ID GAMMA-RAY BURSTS; CORE-COLLAPSE SUPERNOVAE; MASS BLACK-HOLES; DIFFERENTIALLY ROTATING STARS; ACCRETING NEUTRON-STARS; ARMED SPIRAL INSTABILITY; POLOIDAL MAGNETIC-FIELDS; BAR-MODE INSTABILITY; EARLY WARNING SYSTEM; SPIN-DOWN LIMIT AB Interferometric detectors will very soon give us an unprecedented view of the gravitational-wave sky, and in particular of the explosive and transient Universe. Now is the time to challenge our theoretical understanding of short-duration gravitational-wave signatures from cataclysmic events, their connection to more traditional electromagnetic and particle astrophysics, and the data analysis techniques that will make the observations a reality. This paper summarizes the state of the art, future science opportunities, and current challenges in understanding gravitational-wave transients. C1 [Andersson, Nils] Univ Southampton, Sch Math, Southampton SO17 1BJ, Hants, England. [Baker, John] NASA GSFC, Gravitat Phys Lab, Greenbelt, MD 20771 USA. [Belczynski, Krzystof] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Belczynski, Krzystof] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA. [Bernuzzi, Sebastiano; Johnson-McDaniel, Nathan] Univ Jena, Inst Theoret Phys, D-07743 Jena, Germany. [Berti, Emanuele] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA. [Berti, Emanuele; Reisswig, Christian; Sperhake, Ulrich] CALTECH, Pasadena, CA 91125 USA. [Cadonati, Laura; Clark, James] Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. [Cerda-Duran, Pablo] Univ Valencia, Dept Astron & Astrofis, E-46100 Burjassot, Spain. [Favata, Marc] Montclair State Univ, Montclair, NJ 07043 USA. [Finn, Lee Samuel] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Finn, Lee Samuel] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fryer, Chris] Los Alamos Natl Lab, CCS 2, Los Alamos, NM 87545 USA. [Giacomazzo, Bruno; Perna, Rosalba] Univ Colorado, JILA, Boulder, CO 80309 USA. [Giacomazzo, Bruno; Perna, Rosalba] NIST, Boulder, CO 80309 USA. [Antonio Gonzalez, Jose] Univ Michoacana, Inst Fis & Matemat, Morelia 58040, Michoacan, Mexico. [Hendry, Martin; Heng, Ik Siong] Univ Glasgow, Sch Phys & Astron, SUPA, Glasgow G12 8QQ, Lanark, Scotland. [Hild, Stefan] Univ Glasgow, Inst Gravitat Res, Glasgow G12 8QQ, Lanark, Scotland. [Kalmus, Peter; Searle, Antony; Whitcomb, Stan] CALTECH, LIGO Lab, Pasadena, CA 91125 USA. [Klimenko, Sergei] Univ Florida, Gainesville, FL 32611 USA. [Kobayashi, Shiho] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Kokkotas, Kostas] Univ Tubingen, IAAT, D-72076 Tubingen, Germany. [Laguna, Pablo; Shoemaker, Deirdre] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Lehner, Luis; Schnetter, Erik] Perimeter Inst Theoret Phys, Waterloo, ON, Canada. [Levin, Janna] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Liebling, Steve] Long Isl Univ, Brookville, NY 11548 USA. [MacFadyen, Andrew] New York Univ, Dept Phys, New York, NY 10003 USA. [Mandel, Ilya] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Marka, Szabolcs] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Marka, Zsuzsa] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Neilsen, David] Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA. [O'Brien, Paul; Tanvir, Nial] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Read, Jocelyn] Calif State Univ Fullerton, Dept Phys, Fullerton, CA 92831 USA. [Rodriguez, Carl] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Ruffert, Max] Univ Edinburgh, Sch Math, Edinburgh EH16 5JN, Midlothian, Scotland. [Ruffert, Max] Univ Edinburgh, Maxwell Inst, Edinburgh EH16 5JN, Midlothian, Scotland. [Schnetter, Erik] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Schnetter, Erik] Louisiana State Univ, Ctr Computat & Technol, Baton Rouge, LA 70803 USA. [Shawhan, Peter] Univ Maryland, College Pk, MD 20742 USA. [Soderberg, Alicia] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sperhake, Ulrich] Ctr Math Sci, DAMTP, Cambridge CB3 0WA, England. [Sperhake, Ulrich] CENTRA IST, Lisbon, Portugal. [Sutton, Patrick] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Was, Michal] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. RP Andersson, N (reprint author), Univ Southampton, Sch Math, Southampton SO17 1BJ, Hants, England. EM plaguna@gatech.edu RI Hild, Stefan/A-3864-2010; Kokkotas, Kostas/B-7878-2010; Cerda-Duran, Pablo/D-7857-2015; Finn, Lee Samuel/A-3452-2009; Neilsen, David/J-4862-2015; Berti, Emanuele/C-9331-2016; Giacomazzo, Bruno/I-8088-2012 OI Schnetter, Erik/0000-0002-4518-9017; Reisswig, Christian/0000-0001-6855-9351; MacFadyen, Andrew/0000-0002-0106-9013; Mandel, Ilya/0000-0002-6134-8946; Kokkotas, Kostas/0000-0001-6048-2919; Cerda-Duran, Pablo/0000-0003-4293-340X; Finn, Lee Samuel/0000-0002-3937-0688; Neilsen, David/0000-0002-6142-5542; Berti, Emanuele/0000-0003-0751-5130; Giacomazzo, Bruno/0000-0002-6947-4023 FU National Science Foundation [0946361, 1231548, PHY-0847182, PHY-1055103, PHY-0653550, PHY-0955773, PHY-0653462, CBET-0940924, PHY-0969857, 0903973, 1205864, PHY-0925345, PHY-0955825]; Australian Research Council; International Science Linkages program of the Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Educacion y Ciencia; Conselleria d'Economia, Hisenda i Innovacio of the Govern de les Illes Balears; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P Sloan Foundation; NSF [PHY11-25915, HRD 1242090, AST-1009396]; Columbia University in the City of New York; NASA [NNX09AV06A, NNX12AO67G]; German Science Foundation [SFB/TR7]; NSERC; Industry Canada; Province of Ontario through the Ministry of Research and Innovation; Spanish Ministerio de Educacion y Ciencia [AYA 2010-21097-C03-01]; Generalitat Valenciana [PROMETEO-2009-103]; ERC [CAMAP-259276]; US Department of Energy [W-7405-ENG-36] FX The 'Gravitational Wave Bursts' workshops in Chichen-Itza, Mexico (9-1 December 2009) and Tobermory, Scotland (29-31 May 2012) were supported by National Science Foundation grant numbers 0946361 and 1231548. The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Educacion y Ciencia, the Conselleria d'Economia, Hisenda i Innovacio of the Govern de les Illes Balears, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P Sloan Foundation. We thank the Kavli Institute for Theoretical Physics at UC-Santa Barbara, supported in part by NSF grant PHY11-25915, for hosting the workshop 'Chirps, Mergers and Explosions: The Final Moments of Coalescing Compact Binaries.' The Columbia Experimental Gravity group is grateful for the generous support from Columbia University in the City of New York and from the National Science Foundation under cooperative agreement PHY-0847182. E.B. is supported by National Science Foundation through CAREER Award Number PHY-1055103. KB acknowledges NASA grant number NNX09AV06A and NSF grant numbers HRD 1242090 awarded to the Center for Gravitational Wave Astronomy, UTB. SB and KK acknowledge support from the German Science Foundation SFB/TR7 'Gravitational Wave Astronomy.' LC acknowledges National Science Foundation grant numbers PHY-0653550 and PHY-0955773. LL was supported in part by an NSERC through discovery grant. Research at Perimeter Institute is supported through Industry Canada and by the Province of Ontario through the Ministry of Research and Innovation. PCD acknowledges Spanish Ministerio de Educacion y Ciencia grant number AYA 2010-21097-C03-01, Generalitat Valenciana grant number PROMETEO-2009-103 and ERC starting grant number CAMAP-259276. The work of CF is under the auspices of the US Department of Energy, and supported by its contract W-7405-ENG-36 to Los Alamos National Laboratory. LSF acknowledges National Science Foundation grant numbers PHY-0653462, CBET-0940924 and PHY-0969857. BG and RP acknowledge support from NSF grant number AST-1009396 and NASA grant number NNX12AO67G. PL acknowledges National Science Foundation grant numbers 0903973 and 1205864. DMS acknowledges National Science Foundation grant numbers PHY-0925345 and PHY-0955825. We wish to thank Christian Ott and Harald Pfeiffer for useful contributions to this review. NR 421 TC 24 Z9 24 U1 1 U2 22 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD OCT 7 PY 2013 VL 30 IS 19 AR 193002 DI 10.1088/0264-9381/30/19/193002 PG 45 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 223PW UT WOS:000324819900002 ER PT J AU Knap, M Kantian, A Giamarchi, T Bloch, I Lukin, MD Demler, E AF Knap, Michael Kantian, Adrian Giamarchi, Thierry Bloch, Immanuel Lukin, Mikhail D. Demler, Eugene TI Probing Real-Space and Time-Resolved Correlation Functions with Many-Body Ramsey Interferometry SO PHYSICAL REVIEW LETTERS LA English DT Article ID ION QUANTUM SIMULATOR; TRAPPED IONS; INSULATOR-TRANSITION; OPTICAL LATTICES; SQUARE-LATTICE; MAGNETISM; SYSTEMS; ANTIFERROMAGNET; DYNAMICS; MODELS AB We propose to use Ramsey interferometry and single-site addressability, available in synthetic matter such as cold atoms or trapped ions, to measure real-space and time-resolved spin correlation functions. These correlation functions directly probe the excitations of the system, which makes it possible to characterize the underlying many-body states. Moreover, they contain valuable information about phase transitions where they exhibit scale invariance. We also discuss experimental imperfections and show that a spin-echo protocol can be used to cancel slow fluctuations in the magnetic field. We explicitly consider examples of the two-dimensional, antiferromagnetic Heisenberg model and the one-dimensional, longrange transverse field Ising model to illustrate the technique. C1 [Knap, Michael; Lukin, Mikhail D.; Demler, Eugene] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Knap, Michael] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Kantian, Adrian; Giamarchi, Thierry] Univ Geneva, DPMC MaNEP, CH-1211 Geneva, Switzerland. [Bloch, Immanuel] Max Planck Inst Quantum Opt, D-85748 Garching, Germany. [Bloch, Immanuel] Univ Munich, Fak Phys, D-80799 Munich, Germany. RP Knap, M (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM knap@physics.harvard.edu RI Kantian, Adrian/L-6464-2013; Bloch, Immanuel/G-3174-2010; Knap, Michael/H-3344-2011; Giamarchi, Thierry/B-5735-2008; OI Bloch, Immanuel/0000-0002-0679-4759; Knap, Michael/0000-0002-7093-9502; Giamarchi, Thierry/0000-0001-7409-5071; Kantian, Adrian/0000-0002-8439-3539 FU Harvard-MIT CUA; Austrian Science Fund (FWF) [J 3361-N20]; DARPA OLE program; AFOSR MURI on Ultracold Molecules; ARO-MURI on Atomtronics; Swiss NSF under MaNEP and Division II FX We thank S. Gopalakrishnan, R. Islam, C. Monroe, and S. Sachdev for useful discussions. The authors acknowledge support from Harvard-MIT CUA, the DARPA OLE program, AFOSR MURI on Ultracold Molecules, ARO-MURI on Atomtronics, the Austrian Science Fund (FWF) Project No. J 3361-N20, as well as the Swiss NSF under MaNEP and Division II. T.G. is grateful to the Harvard Physics Department and to Harvard-MIT CUA for support and hospitality during the completion of this work. Numerical calculations have been performed on the Odyssey cluster at Harvard University Research Computing. NR 61 TC 30 Z9 30 U1 0 U2 19 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD OCT 4 PY 2013 VL 111 IS 14 AR 147205 DI 10.1103/PhysRevLett.111.147205 PG 6 WC Physics, Multidisciplinary SC Physics GA 230VE UT WOS:000325370500005 PM 24138270 ER PT J AU Moser, WE Fend, SV Richardson, DJ Hammond, CI Lazo-Wasem, EA Govedich, FR Gullo, BS AF Moser, William E. Fend, Steven V. Richardson, Dennis J. Hammond, Charlotte I. Lazo-Wasem, Eric A. Govedich, Fredric R. Gullo, Bettina S. TI A new species of Helobdella (Hirudinida: Glossiphoniidae) from Oregon, USA SO ZOOTAXA LA English DT Article DE Helobdella californica; Helobdella simplex; Helobdella atli; Pacific Northwest; Oregon; Upper Klamath Lake; Glossiphoniidae; Hirudinea; Rhychobdellida; Clitellata; leech ID MITOCHONDRIAL GENE-SEQUENCES; LEECH FAMILY GLOSSIPHONIIDAE; MORPHOLOGICAL DATA; ANNELIDA; PHYLOGENY; TAXONOMY AB Helobdella bowermani n. sp. is described from specimens collected in fine sediment of open water benthos of Upper Klamath Lake, Klamath County, Oregon. The new species has pale yellow/buff coloration with scattered chromatophore blotches throughout the dorsal surface, lateral extensions or papillae only on the a2 annulus, dorsal medial row of papillae with small papilla on a1 and larger papillae on a2 and a3, and a small oval scute ( rarely triangular). Helobdella bowermani n. sp. is morphologically similar to Helobdella atli and Helobdella simplex. Molecular comparison of CO-I sequence data from H. bowermani n. sp. revealed differences of 10.6%-10.8% with Helobdella californica, differences of 12.2%-13.7% with H. atli, and differences of 12.7%-13.2% with H. simplex. C1 [Moser, William E.] Museum Support Ctr, Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Suitland, MD 20746 USA. [Fend, Steven V.] US Geol Survey, Menlo Pk, CA 94025 USA. [Richardson, Dennis J.; Hammond, Charlotte I.] Quinnipiac Univ, Sch Biol Sci, Hamden, CT 06518 USA. [Lazo-Wasem, Eric A.] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA. [Govedich, Fredric R.] Southern Utah Univ, Dept Biol Sci, Cedar City, UT 84720 USA. [Gullo, Bettina S.] Univ Nacl La Plata, Fac Ciencias Nat & Museo, Catedra Zool Invertebrados 1, La Plata, Buenos Aires, Argentina. RP Moser, WE (reprint author), Museum Support Ctr, Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM moserw@si.edu; svfend@usgs.gov; Dennis.Richardson@quinnipiac.edu; Charlotte.Hammond@quinnipiac.edu; eric.lazo-wasem@yale.edu; govedich@suu.edu; bgullo@fcnym.unlp.edu.ar NR 22 TC 4 Z9 4 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 4 PY 2013 VL 3718 IS 3 BP 287 EP 294 PG 8 WC Zoology SC Zoology GA 227QL UT WOS:000325128400005 PM 26258224 ER PT J AU Chesser, RT AF Chesser, R. Terry TI On the correct name of Icterus bullockii (Passeriformes: Icteridae) SO ZOOTAXA LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. RP Chesser, RT (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, POB 37012, Washington, DC 20013 USA. EM chessert@si.edu NR 8 TC 1 Z9 1 U1 0 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 J9 ZOOTAXA JI Zootaxa PD OCT 4 PY 2013 VL 3718 IS 3 BP 295 EP 296 PG 2 WC Zoology SC Zoology GA 227QL UT WOS:000325128400006 PM 26258225 ER PT J AU Peloso, PLV Mcdiarmid, RW Caramaschi, U AF Peloso, Pedro L. V. Mcdiarmid, Roy W. Caramaschi, Ulisses TI The gender of "cleis": correct spelling of Chiasmocleis supercilialbus Morales and McDiarmid, 2009, and Elachistocleis magnus Toledo, 2010 (Anura, Microhylidae) SO ZOOTAXA LA English DT Letter C1 [Peloso, Pedro L. V.] Amer Museum Nat Hist, Div Vertebrate Zool Herpetol, New York, NY 10024 USA. [Peloso, Pedro L. V.] Amer Museum Nat Hist, Richard Gilder Grad Sch, New York, NY 10024 USA. [Mcdiarmid, Roy W.] Natl Museum Nat Hist, Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. [Caramaschi, Ulisses] Univ Fed Rio de Janeiro, Museu Nacl, Dept Vertebrados, BR-20940040 Rio De Janeiro, RJ, Brazil. RP Peloso, PLV (reprint author), Amer Museum Nat Hist, Div Vertebrate Zool Herpetol, Cent Pk West & 79th St, New York, NY 10024 USA. EM pedropeloso@gmail.com; mcdiarmr@si.edu; ulisses@acd.ufrj.br RI Peloso, Pedro/I-3463-2015; Caramaschi, Ulisses/N-5189-2016 OI Peloso, Pedro/0000-0003-0127-8293; Caramaschi, Ulisses/0000-0003-1534-1038 NR 12 TC 1 Z9 1 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 4 PY 2013 VL 3718 IS 3 BP 297 EP 298 PG 2 WC Zoology SC Zoology GA 227QL UT WOS:000325128400007 PM 26258226 ER PT J AU Loreau, J Vranckx, S Desouter-Lecomte, M Vaeck, N Dalgarno, A AF Loreau, J. Vranckx, S. Desouter-Lecomte, M. Vaeck, N. Dalgarno, A. TI Photodissociation and Radiative Association of HeH+ in the Metastable Triplet State SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID GASEOUS NEBULAE; EARLY UNIVERSE; WHITE-DWARFS; HELIUM; DESTRUCTION; IONIZATION; EMISSION; SPECTRUM AB We investigate the photodissociation of HeH+ in the metastable triplet state as well as its formation through the inverse process, radiative association. In models of astrophysical plasmas, HeH+ is assumed to be present only in the ground state, and the influence of the triplet state has not been explored. It may be formed by radiative association during collisions between a proton and metastable helium, which are present in significant concentrations in nebulae. The triplet state can also be formed by association of He+ and H, although this process is less likely to occur. We compute the cross sections and rate coefficients corresponding to the photodissociation of the triplet state by UV photons from a central star using a wave packet method. We show, that the photodissociation cross sections depend strongly on the initial vibrational state and that the effects of excited electronic states and nonadiabatic couplings cannot be neglected. We then calculate the cross section and rate coefficient for the radiative association of HeH+ in the metastable triplet state. C1 [Loreau, J.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Loreau, J.; Vranckx, S.; Vaeck, N.] Univ Libre Brussels, Serv Chim Quant & Photophys, B-1050 Brussels, Belgium. [Vranckx, S.; Desouter-Lecomte, M.] Univ Paris 11, Chim Phys Lab, UMR8000, F-91405 Orsay, France. RP Loreau, J (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM jloreau@ulb.ac.be OI Loreau, Jerome/0000-0002-6142-1509 FU U.S. Department of Energy; Communaute francaise of Belgium (Action de Recherche Concertee); Belgian National Fund for Scientific Research (FRFC/IISN Convention); FRIA-FNRS FX This work was supported by the U.S. Department of Energy and by the Communaute francaise of Belgium (Action de Recherche Concertee) and the Belgian National Fund for Scientific Research (FRFC/IISN Convention). S. Vranckx would like to thank the FRIA-FNRS for financial support. NR 42 TC 4 Z9 4 U1 1 U2 24 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD OCT 3 PY 2013 VL 117 IS 39 BP 9486 EP 9492 DI 10.1021/jp312007q PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 243EV UT WOS:000326300600020 PM 23437906 ER PT J AU Crabtree, KN McCall, BJ AF Crabtree, Kyle N. McCall, Benjamin J. TI On the Symmetry and Degeneracy of H-3(+) SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID POTENTIAL-ENERGY SURFACE; DIFFUSE INTERSTELLAR-MEDIUM; NEAR-INFRARED SPECTROSCOPY; ABSORPTION-LINE SURVEY; RAY IONIZATION RATE; SELECTION-RULES; DISSOCIATIVE RECOMBINATION; DEUTERIUM FRACTIONATION; MOLECULAR CLOUDS; GALACTIC-CENTER AB The fundamental molecular ion H-3(+); has impacted astronomy, chemistry, and physics, particularly since the discovery of its rovibrational spectrum. Consisting of three identical fermions, its properties are profoundly influenced by the requirements of exchange symmetry, most notably the nonexistence of its ground rotational state. Spectroscopy of H-3(+) is often used to infer the relative abundances of its two nuclear spin modifications, ortho- and para-H-3(+), which are important in areas as diverse as electron dissociative recombination and deuterium fractionation in cold interstellar clouds. In this paper, we explore in detail the impact of exchange symmetry on the states of HI, with a particular focus on the state degeneracies necessary for converting spectral transition intensities to relative abundances. We address points of confusion in the literature surrounding these issues and discuss the implications for proton-transfer reactions of HI at low temperatures. C1 [Crabtree, Kyle N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McCall, Benjamin J.] Univ Illinois, Dept Chem, Urbana, IL 61801 USA. [McCall, Benjamin J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [McCall, Benjamin J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. RP Crabtree, KN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kcrabtree@cfa.harvard.edu; bjmccall@illinois.edu OI Crabtree, Kyle/0000-0001-5629-5192 FU CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory FX We thank Takeshi Oka for inspiring us over the years with his enthusiasm for H3+. K.N.C. has been supported by a CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory. NR 56 TC 2 Z9 2 U1 0 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD OCT 3 PY 2013 VL 117 IS 39 BP 9950 EP 9958 DI 10.1021/jp400080j PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 243EV UT WOS:000326300600075 PM 23537007 ER PT J AU McCarthy, MC Martinez, O Crabtree, KN Lattanzi, V Novick, SE Thorwirth, S AF McCarthy, Michael C. Martinez, Oscar, Jr. Crabtree, Kyle N. Lattanzi, Valerio Novick, Stewart E. Thorwirth, Sven TI Detection of Nitrogen-Protonated Nitrous Oxide (HNNO+) by Rotational Spectroscopy SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID 2ND DERIVATIVES; MICROWAVE-SPECTRA; BASIS-SETS; MANY-BODY; AB-INITIO; N2O; ION; ENERGY; CH4; MOLECULE AB The rotational spectrum of nitrogen-protonated nitrous oxide (HNNO+), an isomer whose existence was first inferred from kinetic studies more than 30 years ago, has now been detected by Fourier transform microwave spectroscopy, guided by new high-level coupled cluster calculations of its molecular structure. From high resolution measurements of the hyperfine splitting in its fundamental rotational transition, the rotational constant (B + C)/2 and the quadrupole tensor element chi(aa)(N) for both nitrogen atoms have been precisely determined The derived constants agree well with quantum chemical calculations here and others in the literature. The chi(aa)(N) values for the two isomers of protonated nitrous oxide are qualitatively consistent with the valence bond description of H-N=N+=O for the electronic structure of the nitrogen-protonated form and N N+-O-H for the oxygen-protonated form. HNNO+ is found to be 2-4 times less abundant than NNOH+ under a range of experimental conditions, as might be expected because this metastable isomer is known to be only similar to 6 kcal mol(-1) less stable than ground-state NNOH+ from kinetic measurements by Ferguson and co-workers. C1 [McCarthy, Michael C.; Martinez, Oscar, Jr.; Crabtree, Kyle N.; Lattanzi, Valerio] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Novick, Stewart E.] Wesleyan Univ, Dept Chem, Middletown, CT 06459 USA. [Thorwirth, Sven] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; Crabtree, Kyle/0000-0001-5629-5192; McCarthy, Michael/0000-0001-9142-0008 FU NSF [CHE-1058063, CHE-1011214]; Smithsonian Astrophysical Observatory; Deutsche Forschungsgemeinschaft [TH 1301/3-1, TH 1301/3-2] FX We thank E. S. Palmer for technical assistance. The work in Cambridge is supported by NSF Grant CHE-1058063. K.N.C. has been supported by a CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory. S.N. acknowledges support from the NSF, Grant CHE-1011214. S.T. gratefully acknowledges support from the Deutsche Forschungsgemeinschaft through Grants TH 1301/3-1 and TH 1301/3-2. NR 54 TC 4 Z9 4 U1 2 U2 8 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 EI 1520-5215 J9 J PHYS CHEM A JI J. Phys. Chem. A PD OCT 3 PY 2013 VL 117 IS 39 BP 9968 EP 9974 DI 10.1021/jp4002065 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 243EV UT WOS:000326300600077 PM 23574435 ER PT J AU Lorenzen, K Agnalt, AL Blankenship, HL Hines, AH Leber, KM Loneragan, NR Taylor, MD AF Lorenzen, Kai Agnalt, Ann-Lisbeth Blankenship, H. Lee Hines, Anson H. Leber, Kenneth M. Loneragan, Neil R. Taylor, Matthew D. TI Evolving Context and Maturing Science: Aquaculture-Based Enhancement and Restoration Enter the Marine Fisheries Management Toolbox SO REVIEWS IN FISHERIES SCIENCE LA English DT Article DE rights-based fisheries management; individual quotas; hatcheries; coastal zone ID STOCK ENHANCEMENT; WILD FISH; SURVIVAL; GROWTH; DOMESTICATION; CONSERVATION; POPULATIONS; STRATEGIES; RESOURCES; SALMONIDS AB Aquaculture-based enhancement of marine fisheries includes sea ranching, stock enhancement, and restocking. A rapidly evolving context and maturing science base have effectively put these approaches into the fisheries management toolbox. Among the contextual factors are (1) a rapid expansion of captive breeding and domestication to new marine species, (2) fisheries governance systems that address the common dilemma, and (3) global environmental change impacts on coastal fisheries that increasingly call for active approaches to maintaining or increasing fisheries yields and ecosystem services. The science base of marine restocking, stock enhancement, and sea ranching continues to advance rapidly and has now reached a point where it is becoming possible to assess the likely contribution of such approaches to fisheries management goals prior to major investments being undertaken and to design enhancement programs effectively and responsibly where good potential is judged to exist. This signifies an important transition of marine fisheries enhancement from an exploratory, research-oriented endeavor to a tool in the fisheries management tool box. C1 [Lorenzen, Kai] Univ Florida, Sch Forest Resource & Conservat, Gainesville, FL 32653 USA. [Agnalt, Ann-Lisbeth] Inst Marine Res, N-5024 Bergen, Norway. [Blankenship, H. Lee] Northwest Marine Technol, Shaw Isl, WA USA. [Hines, Anson H.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Leber, Kenneth M.] Mote Marine Lab, Sarasota, FL 34236 USA. [Loneragan, Neil R.; Taylor, Matthew D.] Murdoch Univ, Sch Vet & Life Sci, Perth, WA, Australia. [Taylor, Matthew D.] NSW Dept Primary Ind, Port Stephens Fisheries Inst, Nelson Bay, NSW, Australia. [Taylor, Matthew D.] Univ New S Wales, Sch Biol Earth & Environm Sci, Sydney, NSW, Australia. RP Lorenzen, K (reprint author), Univ Florida, Sch Forest Resource & Conservat, 7922 NW 71st St, Gainesville, FL 32653 USA. EM klorenzen@ufl.edu RI Taylor, Matthew/C-4833-2008; OI Leber, Kenneth/0000-0002-3252-818X FU Florida Fish and Wildlife Conservation Commissions [F-136-R] FX The authors thank the steering committee and fellow members of the International Scientific Committee of the Fourth International Symposium on Stock Enhancement and Sea Ranching for helping to organize this stimulating meeting at Shanghai Ocean University, China. They also thank the many colleagues who gave their time to review the manuscripts. The senior author (KL) acknowledges funding support from the Florida Fish and Wildlife Conservation Commissions' Federal Aid in Sport Fish Restoration Project F-136-R. NR 80 TC 11 Z9 12 U1 1 U2 42 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1064-1262 EI 1547-6553 J9 REV FISH SCI JI Rev. Fish. Sci. PD OCT 2 PY 2013 VL 21 IS 3-4 SI SI BP 213 EP 221 DI 10.1080/10641262.2013.837358 PG 9 WC Fisheries SC Fisheries GA 252NO UT WOS:000327013000001 ER PT J AU Knapp, LW Randall, JE AF Knapp, Leslie W. Randall, John E. TI Sunagocia omanensis, a new flathead fish (Scorpaeniformes, Platycephalidae) from the Western Indian Ocean, with comments on the distribution of Sunagocia carbuncula SO ZOOTAXA LA English DT Article DE Sunagocia omanensis sp nov.; Sunagocia carbuncula; Oman AB A new species of Platycephalidae having a weak development of sensory tubules on the cheek is placed in the genus Sunagocia Imamura. The description is based on two specimens taken at the Kuria Muria Ids., Oman. The new species may be distinguished from its congeners by having three preocular spines, ethmoid spines forming a rosette on mid-line with 5-6 tips coming from a common base, and a body coloration of tan with dark saddles reaching to lower sides. It is also characterized by having numerous small serrations along the supraorbital and suborbital ridges and sixgill rakers. A section concerning the status and range of Sunagocia carbuncula Valenciennes in the western Indian Ocean is also included. A key separating the species of Sunagocia appears below. C1 [Knapp, Leslie W.] Smithsonian Inst, Natl Museum Nat Hist, Div Fisheries, MRC 534, Washington, DC 20013 USA. [Randall, John E.] Bernice P Bishop Museum, Honolulu, HI 96819 USA. RP Knapp, LW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fisheries, MRC 534, POB 37012, Washington, DC 20013 USA. EM knappl@si.edu; jackr@hawaii.rr.com NR 9 TC 0 Z9 0 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 J9 ZOOTAXA JI Zootaxa PD OCT 2 PY 2013 VL 3718 IS 1 BP 97 EP 100 PG 4 WC Zoology SC Zoology GA 227QI UT WOS:000325128000009 PM 26258212 ER PT J AU Wen, J Ree, RH Ickert-Bond, SM Nie, ZL Funk, V AF Wen, Jun Ree, Richard H. Ickert-Bond, Stefanie M. Nie, Zelong Funk, Vicki TI Biogeography: Where do we go from here? SO TAXON LA English DT Article DE biogeography; biogeography data portal; historical biogeography; parametric models; phylogenomics; phylogeography ID DISPERSAL-VICARIANCE ANALYSIS; GEOGRAPHIC RANGE EVOLUTION; LONG-DISTANCE DISPERSAL; EASTERN NORTH-AMERICA; BIRTH-DEATH-MODELS; HISTORICAL BIOGEOGRAPHY; DIVERSIFICATION RATES; DIVERGENCE TIMES; COMPARATIVE PHYLOGEOGRAPHY; PHYLOGENETIC INFERENCE AB Biogeography is a multidisciplinary science concerned with how and why organisms are distributed as they are on Earth. It links fields such as systematics, ecology, paleontology, and climatology, and occupies a central position in evolutionary biology, being fundamental to the study of processes such as speciation and adaptive radiation. Here we provide a brief overview of some particularly dynamic areas of inquiry and offer some perspectives on future directions for the field. We hope that some historical debates, such as those over the importance of dispersal, or the validity of molecular dating, are finally being put to rest. Over the last decade, biogeography has become increasingly integrative, and has benefited from advances in statistical methods for inferring geographic range dynamics in a phylogenetic context, molecular estimation of lineage divergence times, and modeling lineage birth and death. These are enabling greater insights into patterns of organismal diversification in time and space. In the next decade, analytical challenges are emerging on several fronts. For example, phylogenies are increasing in size and taxonomic breadth and new sequencing technologies enabling phylogenetic and phylogeographic datasets are increasingly genomic in depth. In addition, geographic occurrence data are accumulating in online repositories, yet tools for data mining and synthetic analysis are lacking for comparative multi-lineage studies. Biogeography is thus entering an era characterized by phylogenomic datasets, increasingly comprehensive sampling of clades, and interdisciplinary synthesis. We anticipate continued progress in our understanding of biodiversity patterns at regional and global scales, but this will likely require greater collaboration with specialists in bioinformatics and computational science. Finally, it is clear that biogeography has an increasingly important role to play in the discovery and conservation of biodiversity. Lessons learned from biogeographic studies of islands are being applied to better understand extinction dynamics as continental ecosystems become more fragmented, and phylogeography and ecological niche modeling offer innovative paths toward the discovery of previously unknown species distributions and priority areas for conservation. The future of biogeography is bright and filled with exciting challenges and opportunities. C1 [Wen, Jun; Funk, Vicki] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Ree, Richard H.] Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA. [Ickert-Bond, Stefanie M.] Univ Alaska Fairbanks, UA Museum North Herbarium, Fairbanks, AK 99775 USA. [Ickert-Bond, Stefanie M.] Univ Alaska Fairbanks, Dept Biol & Wildlife, Fairbanks, AK 99775 USA. [Nie, Zelong] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. RP Wen, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. EM wenj@si.edu RI Nie, Ze-Long/N-8471-2015 OI Nie, Ze-Long/0000-0001-8065-3981 NR 230 TC 23 Z9 25 U1 6 U2 101 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 OCT PY 2013 VL 62 IS 5 BP 912 EP 927 PG 16 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA AG0RX UT WOS:000335124400005 ER PT J AU Diazgranados, M Funk, V AF Diazgranados, Mauricio Funk, Vicki TI IAPT PARTICIPATION AT THE VII CONGRESO COLOMBIANO DE BOTANICA SO TAXON LA English DT Article C1 [Diazgranados, Mauricio; Funk, Vicki] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. RP Diazgranados, M (reprint author), Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. EM DiazgranadosM@si.edu; Funkv@si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 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 OCT PY 2013 VL 62 IS 5 BP 1087 EP 1089 PG 3 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA AG0RX UT WOS:000335124400036 ER PT J AU de Moor, JM Fischer, TP Sharp, ZD King, PL Wilke, M Botcharnikov, RE Cottrell, E Zelenski, M Marty, B Klimm, K Rivard, C Ayalew, D Ramirez, C Kelley, KA AF de Moor, J. M. Fischer, T. P. Sharp, Z. D. King, P. L. Wilke, M. Botcharnikov, R. E. Cottrell, E. Zelenski, M. Marty, B. Klimm, K. Rivard, C. Ayalew, D. Ramirez, C. Kelley, K. A. TI Sulfur degassing at Erta Ale (Ethiopia) and Masaya (Nicaragua) volcanoes: Implications for degassing processes and oxygen fugacities of basaltic systems SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Article DE basalts; sulfur; oxygen fugacity; sulfur isotopes; gas chemistry ID STABLE-ISOTOPE FRACTIONATION; CENTRAL-AMERICAN ARC; SILICATE MELTS; OXIDATION-STATE; SUBDUCTION ZONES; LAVA LAKE; ANATAHAN VOLCANO; CALDERA COMPLEX; ABSORPTION SPECTROSCOPY; HYDROTHERMAL SYSTEMS AB We investigate the relationship between sulfur and oxygen fugacity at Erta Ale and Masaya volcanoes. Oxygen fugacity was assessed utilizing Fe3+/Sigma Fe and major element compositions measured in olivine-hosted melt inclusions and matrix glasses. Erta Ale melts have Fe3+/Sigma Fe of 0.15-0.16, reflecting fO(2) of Delta QFM 0.0 +/- 0.3, which is indistinguishable from fO(2) calculated from CO2/CO ratios in high-temperature gases. Masaya is more oxidized at Delta QFM + 1.7 +/- 0.4, typical of arc settings. Sulfur isotope compositions of gases and scoria at Erta Ale (delta S-34(gas) - 0.5 parts per thousand; delta S-34(scoria) + 0.9 parts per thousand) and Masaya (delta S-34(gas) + 4.8 parts per thousand; delta S-34(scoria) + 7.4 parts per thousand) reflect distinct sulfur sources, as well as isotopic fractionation during degassing (equilibrium and kinetic fractionation effects). Sulfur speciation in melts plays an important role in isotope fractionation during degassing and S6+/Sigma S is <0.07 in Erta Ale melt inclusions compared to >0.67 in Masaya melt inclusions. No change is observed in Fe3+/Sigma Fe or S6+/Sigma S with extent of S degassing at Erta Ale, indicating negligible effect on fO(2), and further suggesting that H2S is the dominant gas species exsolved from the S2--rich melt (i.e., no redistribution of electrons). High SO2/H2S observed in Erta Ale gas emissions is due to gas re-equilibration at low pressure and fixed fO(2). Sulfur budget considerations indicate that the majority of S injected into the systems is emitted as gas, which is therefore representative of the magmatic S isotope composition. The composition of the Masaya gas plume (+4.8 parts per thousand) cannot be explained by fractionation effects but rather reflects recycling of high delta S-34 oxidized sulfur through the subduction zone. C1 [de Moor, J. M.; Fischer, T. P.; Sharp, Z. D.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [King, P. L.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Wilke, M.] Helmholtzzentrum Potsdam, Deutsch GeoForschungsZentrum, Potsdam, Germany. [Botcharnikov, R. E.] Leibniz Univ Hannover, Inst Mineral, Hannover, Germany. [Cottrell, E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Zelenski, M.] Russian Acad Sci, Inst Expt Mineral, Moscow, Russia. [Marty, B.] Ecole Natl Super Geol, CNRS, Ctr Rech Petrograph & Geochim, Vandoeuvre Les Nancy, France. [Klimm, K.] Goethe Univ Frankfurt, Inst Geowissensch, D-60054 Frankfurt, Germany. [Rivard, C.] European Synchrotron Radiat Facil, F-38043 Grenoble, France. [Ayalew, D.] Univ Addis Ababa, Sch Earth & Planetary Sci, Dept Earth Sci, Addis Ababa, Ethiopia. [Ramirez, C.] Univ Costa Rica, Red Sismol Nacl, San Jose, Costa Rica. [Kelley, K. A.] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA. RP de Moor, JM (reprint author), Univ Nacl, Observ Vulcanol & Sismol Costa Rica, Heredia, Costa Rica. EM mdemoor@unm.edu RI Kelley, Katherine/J-3728-2013; King, Penelope/A-1791-2011 OI Kelley, Katherine/0000-0002-7516-2683; King, Penelope/0000-0002-8364-9168 FU National Science Foundation [EAR1049891]; NASA Earth and Space Science Fellowship [Planet09F-0044]; DOE [DE-AC02-98CH10886, DE-FG02-92ER14244]; [EAR/IF - 0743540]; [EAR-0841006]; [EAR-0841108] FX This research was made possible by the National Science Foundation through grant EAR1049891 (TF); and by a NASA Earth and Space Science Fellowship to JMdM/PLK (Planet09F-0044). We also acknowledge support through grants EAR/IF - 0743540 (TF), EAR-0841006 (EC) and EAR-0841108 (KAK). Viorel Atudorei, Vitchko Tsanev, Mike Spilde, and Paul Burger are thanked for analytical and technical assistance. We gratefully acknowledge the European Synchrotron Radiation Facility (ID21) for providing beamtime. Use of the National Synchrotron Light Source (X26A) was supported by DOE under Contracts No. DE-AC02-98CH10886 and DE-FG02-92ER14244. Jan De Hoog and an anonymous reviewer are thanked for thoughtful comments that improved this work. Charlie Mandeville and Chip Shearer are gratefully acknowledged for serving on the PhD committee of the first author and for reviewing a previous version of this manuscript. NR 151 TC 15 Z9 15 U1 2 U2 40 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1525-2027 J9 GEOCHEM GEOPHY GEOSY JI Geochem. Geophys. Geosyst. PD OCT PY 2013 VL 14 IS 10 BP 4076 EP 4108 DI 10.1002/ggge.20255 PG 33 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 301KO UT WOS:000330531400012 ER PT J AU Baczynski, AA McInerney, FA Wing, SL Kraus, MJ Bloch, JI Boyer, DM Secord, R Morse, PE Fricke, HC AF Baczynski, Allison A. McInerney, Francesca A. Wing, Scott L. Kraus, Mary J. Bloch, Jonathan I. Boyer, Doug M. Secord, Ross Morse, Paul E. Fricke, Henry C. TI Chemostratigraphic implications of spatial variation in the Paleocene-Eocene Thermal Maximum carbon isotope excursion, SE Bighorn Basin, Wyoming SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Article DE Paleocene-Eocene Thermal Maximum; global warming; chemostratigraphy; organic carbon; carbon isotopes; carbon isotope excursion ID SOIL ORGANIC-MATTER; WAIPAOA SEDIMENTARY SYSTEM; WILLWOOD FORMATION; CLIMATE-CHANGE; NORTH-AMERICA; NEW-ZEALAND; BOUNDARY; STRATIGRAPHY; PALEOGENE; SECTION AB The Paleocene-Eocene Thermal Maximum (PETM) is marked by a prominent negative carbon isotope excursion (CIE) of 3-5 parts per thousand that has a characteristic rapid onset, stable body, and recovery to near pre-CIE isotopic composition. Although the CIE is the major criterion for global correlation of the Paleocene-Eocene boundary, spatial variations in the position and shape of the CIE have not been systematically evaluated. We measured carbon isotope ratios of bulk organic matter (delta C-13(org)) and pedogenic carbonate (delta C-13(carb)) at six PETM sections across a 16 km transect in the SE Bighorn Basin, Wyoming. Bed tracing and high-resolution floral and faunal biostratigraphy allowed correlation of the sections independent of chemostratigraphy. The onset of the CIE in bulk organic matter at all six sections occurs within a single laterally extensive geosol. The magnitude of the CIE varies from 2.1 to 3.8 parts per thousand. The absolute and relative stratigraphic thickness of the body of the CIE in bulk organic matter varies significantly across the field area and underrepresents the thickness of the PETM body by 30%-80%. The variations cannot be explained by basinal position and instead suggest that delta C-13(org) values were influenced by local factors such as reworking of older carbon. The stratigraphic thickness and shape of the CIE have been used to correlate sections, estimate timing of biotic and climatic changes relative to the presumed carbon isotope composition of the atmosphere, and calculate rates of environmental and biotic change. Localized controls on delta C-13(org) values place these inferences in question by influencing the apparent shape and duration of the CIE. C1 [Baczynski, Allison A.] Northwestern Univ, Dept Earth & Planetary Sci, Inst Technol, Evanston, IL 60208 USA. [McInerney, Francesca A.] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL 60208 USA. [Wing, Scott L.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Kraus, Mary J.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Bloch, Jonathan I.; Secord, Ross; Morse, Paul E.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Boyer, Doug M.] Duke Univ, Dept Evolutionary Anthropol, Durham, NC USA. [Morse, Paul E.] Univ Florida, Dept Anthropol, Gainesville, FL 32611 USA. [Fricke, Henry C.] Colorado Coll, Dept Geol, Colorado Springs, CO 80903 USA. RP Baczynski, AA (reprint author), Northwestern Univ, Dept Earth & Planetary Sci, Inst Technol, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM allison@earth.northwestern.edu RI Kraus, Mary/C-3323-2008; McInerney, Francesca/B-7894-2009; OI Kraus, Mary/0000-0002-1721-2566; McInerney, Francesca/0000-0002-2020-6650; Bloch, Jonathan/0000-0003-1484-6931; Wing, Scott/0000-0002-2954-8905 FU NSF [EAR-0720268, EAR-0717892, EAR-0718740, EAR-0719941, EAR-0640076]; Initiative for Sustainability and Energy at Northwestern; Australian Research Council [FT110100793] FX We thank Alexa Socianu for help with carbonate isotope laboratory work, Stephen Chester for assisting with biostratigraphic and lithostratigraphic studies, Brady Foreman and Elizabeth Denis for sample collection, and the many students and volunteers who helped with fieldwork and laboratory work. We also thank two anonymous reviewers for their constructive comments. Funding was provided by NSF awards EAR-0720268 (F. A. M.), EAR-0717892 (S. L. W.), EAR-0718740 (M.J.K.), EAR-0719941 (J.I.B.), EAR-0640076 (J.I.B., R. S., and John Krigbaum), Initiative for Sustainability and Energy at Northwestern (F. A. M.), and Australian Research Council FT110100793 (F. A. M.). Vertebrate fossils were collected under Bureau of Land Management permits to J.I.B. (PA04-WY-113, PA10-WY-185). A portion of this manuscript was written when J.I.B. was supported as an Edward P. Bass Distinguished Visiting Environmental Scholar in the Yale Institute for Biospheric Studies (YIBS). NR 89 TC 8 Z9 8 U1 7 U2 30 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1525-2027 J9 GEOCHEM GEOPHY GEOSY JI Geochem. Geophys. Geosyst. PD OCT PY 2013 VL 14 IS 10 BP 4133 EP 4152 DI 10.1002/ggge.20265 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 301KO UT WOS:000330531400015 ER PT J AU Villanueva-Gutierrez, R Rubik, DW Colli-Ucan, W Guemez-Ricalde, FJ Buchmann, SL AF Villanueva-Gutierrez, Rogel Rubik, David W. Colli-Ucan, Wilberto Gueemez-Ricalde, Francisco J. Buchmann, Stephen L. TI A Critical View of Colony Losses in Managed Mayan Honey-Making Bees (Apidae: Meliponini) in the Heart of Zona Maya SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article DE Colony loss; husbandry; Melipona beecheii; meliponiculture; Mexico; Quintana Roo; traditional knowledge ID MELIPONICULTURE; POPULATIONS; YUCATAN; FOREST; MEXICO; IMPACT AB This research considered native Mayan stingless bees, Melipona beecheii, with special attention to decrease in their managed colonies. From a total of 155 beekeepers located in 60 communities, 58 were randomly selected to survey in 2011. Their experience ranged from less than one to 50 years, and initial colonies from one to 100. Both structured and open interviews were conducted. Participants generally reported they believed bees were obtaining less food, which could produce colony loss. The present and a previous survey in the Zona Maya show colony loss averages 4-5% each year. In this study, during an average of 10 years, 27 beekeepers lost none, 9 lost all, and the remainder lost 44% of their colonies. Further analysis revealed colony loss had no association with relative habitat disturbance, presumed Africanized honey bee abundance, or beekeeping experience. However, those initially with more colonies in a meliponary lost them at a greater rate, indicating competition for food. Initial colony number was near 11, but currently is near 4 per meliponary. Little colony propagation (husbandry) was the norm until recently, when initiatives including meliponiculture workshops stimulated more husbandry. Twenty-six percent of beekeepers had less than one year experience and they began meliponaries using wild colonies. Because established meliponicultors were found to very seldom rely on new wild colonies, increased husbandry efforts are necessary to offset natural mortality of managed colonies. Five meliponicultors increased their colonies over 300% in two years (40 to 123 colonies), whereas a 34% loss in nine years (480 to 206 colonies) was found among the individuals randomly surveyed. C1 [Villanueva-Gutierrez, Rogel; Colli-Ucan, Wilberto] El Colegio Frontera Sur, Chetmal 77014, Quintana Roo, Mexico. [Rubik, David W.] Smithsonian Trop Res Inst, Balboa, Panama. [Rubik, David W.] Unit 9100, DPO, AA 34002 USA. [Gueemez-Ricalde, Francisco J.] Univ Quintana Roo, Chetmal 77019, Quintana Roo, Mexico. [Buchmann, Stephen L.] Univ Arizona, Dept Entomol, Tucson, AZ 85721 USA. [Buchmann, Stephen L.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. RP Villanueva-Gutierrez, R (reprint author), El Colegio Frontera Sur, Av Centenario Km 5-5,Apdo Postal 424, Chetmal 77014, Quintana Roo, Mexico. EM rvillanu@ecosur.mx; roubikd@si.edu NR 33 TC 2 Z9 2 U1 1 U2 15 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 EI 1937-2353 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD OCT PY 2013 VL 86 IS 4 BP 352 EP 362 PG 11 WC Entomology SC Entomology GA 302JB UT WOS:000330599700006 ER PT J AU Cline, MH Strong, AM Sillett, TS Rodenhouse, NL Holmes, RT AF Cline, Mason H. Strong, Allan M. Sillett, T. Scott Rodenhouse, Nicholas L. Holmes, Richard T. TI CORRELATES AND CONSEQUENCES OF BREEDING DISPERSAL IN A MIGRATORY SONGBIRD SO AUK LA English DT Article DE Black-throated Blue Warbler; breeding dispersal; habitat structure; migratory passerine; movement; reproductive success; Setophaga caerulescens ID THROATED BLUE WARBLERS; DENSITY-DEPENDENT DISPERSAL; NEST-SITE FIDELITY; REPRODUCTIVE SUCCESS; COLLARED FLYCATCHER; DENDROICA-CAERULESCENS; INBREEDING AVOIDANCE; HABITAT SELECTION; AVIAN DISPERSAL; BIRD POPULATION AB Knowledge of breeding dispersal, defined as shifts in territory location between two successive breeding seasons, remains limited for migratory passerines. We investigated the relationship between two ecological factors, habitat structure and reproductive success, and 499 breeding dispersal events in a Nearctic-Neotropic migratory songbird, the Black-throated Blue Warbler (Setophaga caerulescens) breeding at the Hubbard Brook Experimental Forest, New Hampshire, from 1998 to 2008. Male dispersal distance was correlated with both individual age and habitat structure, with older males moving shorter distances than younger males, and males on the high-shrub-density plot (i.e., higher quality) moving shorter distances than males on the plot with lower shrub density. Female dispersal distance was also correlated with habitat structure; individuals on the higher-quality plot moved shorter distances than those on the lower-quality plot. In contrast to that of males, female dispersal distance was independent of age, but correlated with reproductive success: females that fledged relatively few offspring in a year subsequently dispersed farther than those that experienced high reproductive success. Mean ( SE) breeding dispersal distance for females (245 20 m) was greater than that of males (163 11 m). We also examined reproductive consequences of breeding dispersal and found that males that moved shorter distances fledged more offspring after dispersal than those that moved longer distances; no trend was found for females. These differences in dispersal patterns and outcomes suggest sex-specific selective pressures and life-history strategies. C1 [Cline, Mason H.; Strong, Allan M.] Univ Vermont, Rubenstein Sch Environm & Nat Resources, Burlington, VT 05405 USA. [Sillett, T. Scott] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Rodenhouse, Nicholas L.] Wellesley Coll, Dept Biol Sci, Wellesley, MA 02481 USA. [Holmes, Richard T.] Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. RP Cline, MH (reprint author), Univ Georgia, Warnell Sch Forestry & Nat Resources, 180 East Green St, Athens, GA 30602 USA. EM mcline@uga.edu FU U.S. National Science Foundation (NSF); University of Vermont's Rubenstein School of Environment and Natural Resources; U.S. Department of Agriculture (USDA) McIntire-Stennis Forestry Program; Smithsonian Institution; NSF FX This research was funded by the U.S. National Science Foundation (NSF), the University of Vermont's Rubenstein School of Environment and Natural Resources, the U.S. Department of Agriculture (USDA) McIntire-Stennis Forestry Program, and the Smithsonian Institution. We thank the many field assistants who worked on our research project and F. Sutti for assistance with GIS. We thank J. Hatt and reviewers for helpful comments on the manuscript. This manuscript is a contribution of the Hubbard Brook Ecosystem Study. Hubbard Brook is part of the Long-Term Ecological Research network, which is supported by the NSF. The Hubbard Brook Experimental Forest is operated and maintained by the USDA Forest Service, Northern Research Station, Newtown Square, Pennsylvania. NR 88 TC 10 Z9 10 U1 3 U2 44 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 EI 1938-4254 J9 AUK JI AUK PD OCT PY 2013 VL 130 IS 4 BP 742 EP 752 DI 10.1525/auk.2013.12244 PG 11 WC Ornithology SC Zoology GA 274EM UT WOS:000328588800019 ER PT J AU Ando, A Huber, BT Silva, IP AF Ando, Atsushi Huber, Brian T. Silva, Isabella Premoli TI Paraticinella rohri (Bolli, 1959) as the valid name for the latest Aptian zonal marker species of planktonic foraminifera traditionally called bejaouaensis or eubejaouaensis SO CRETACEOUS RESEARCH LA English DT Article DE Plankotnic foraminifera; Paraticinella eubejaouaensis; Paraticinella rohri; Synonymy; Biozonation; Aptian ID BIOSTRATIGRAPHIC ANALYSIS; APTIAN/ALBIAN BOUNDARY; CLASSIFICATION; EVOLUTION; TURNOVER; TRINIDAD; CRITERIA; ZONATION; EVENTS; SPAIN AB The planktonic foraminiferal taxon Ticinella bejaouaensis Sigal, 1966 had long been an important zonal biomarker for the latest Aptian characterized by its large test, numerous (8-10) final-whorl chambers, and rugose test surface, usually with an umbilical cover-plate. Upon confirmation that Sigal's Madagascan holotype was actually from the upper Albian, this species was renamed as T. eubejaouaensis Randrianasolo and Anglada, 1998 using Sigal's Tunisian bejaouaensis paratype, which is late Aptian in age, as the new holotype. Following emendation of the genus, Paraticinella eubejaouaensis has recently become the standard usage. However, the validity of this species is still uncertain because the original designation was given in very obscure publication(s). Meanwhile, albeit tenuous, a presumable senior name "Paraticinella rohri (Bolli, 1959)" has recently been proposed in place of eubejaouaensis. Rigorous assessment of the original species designation of T. eubejaouaensis ascertains that the method of publication used does not comply with the criteria required in the International Code of Zoological Nomenclature, thereby making this species an invalid name, or nomen nudum. New backscattered scanning electron microscopic observations of the primary types of Praeglobotruncana rohri Bolli, 1959 reveal that this hitherto unattended species is indeed synonymous to "T eubejaouaensis" particularly by exhibiting equatorially aligned rugosities on the wall surface, and that the holotype is sufficiently preserved and well qualified as the name-bearing type. The latest Aptian age of the rohri type level is robustly established by its co-occurrence with Pseudoplanomalina cheniourensis (Sigal, 1952) and Hedbergella trocoidea (Gandolfi, 1942) (= another rohri paratype). Upon confirmation of the absence of any potential nomenclatural acts for conservation of the junior name [eu]bejaouaensis," we are obliged to provide formal redescription and establish the valid, objective senior name Paraticinella rohri (Bolli, 1959), the binomen that should be of mandatory use henceforth. Accordingly, the uppermost Aptian "[eu]bejaouaensis" Zone should be referred to as the "Pt. rohri Zone." Having reviewed the supraspecific taxonomy, herein the type species of the genus Paraticinella is redefined as Pt. rohri, and the subfamily Pseudoplanomalininae is proposed. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Ando, Atsushi; Huber, Brian T.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Silva, Isabella Premoli] Univ Milan, Dipartimento Sci Terra A Desio, I-20133 Milan, Italy. RP Ando, A (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, POB 37012,MRC 121, Washington, DC 20013 USA. EM AndoA@si.edu NR 69 TC 7 Z9 7 U1 0 U2 1 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0195-6671 EI 1095-998X J9 CRETACEOUS RES JI Cretac. Res. PD OCT PY 2013 VL 45 BP 275 EP 287 DI 10.1016/j.cretres.2013.05.002 PG 13 WC Geology; Paleontology SC Geology; Paleontology GA 273GO UT WOS:000328523500019 ER PT J AU Neufeld, MJ AF Neufeld, Michael J. TI Eisenhower's Sputnik Moment: The Race for Space and International Prestige. 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 OCT PY 2013 VL 54 IS 4 BP 998 EP 999 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 272FK UT WOS:000328445500029 ER PT J AU Ivanova, MA Lorenz, CA Franchi, IA Bychkov, AY Post, JE AF Ivanova, Marina A. Lorenz, Cyril A. Franchi, Ian A. Bychkov, Andrei Y. Post, Jeffrey E. TI Experimental simulation of oxygen isotopic exchange in olivine and implication for the formation of metamorphosed carbonaceous chondrites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID THERMAL METAMORPHISM; CM CHONDRITES; PARENT BODIES; FRACTIONATION; PLANETESIMALS; SERPENTINE; SILICATES; EVOLUTION; MAGNETITE; ICARUS AB We have conducted hydration-dehydration experiments on terrestrial olivine to investigate the behavior of oxygen isotopic fractionation to test the hypothesis that multiple cycles of aqueous and thermal processing on a parent asteroid comprise a genetic relationship between CM2s and metamorphosed carbonaceous chondrites (MCCs). Two experiments were undertaken. In the first experiment, serpentine was obtained by hydrating terrestrial olivine (Fo(90.9)) in the laboratory. During this experiment, olivine was reacted with isotopically heavy water (O-18 21.5 parts per thousand) at T=300 degrees C, PH2O=300bar, for 100days. The oxygen isotopic composition of the experimental serpentine was enriched in O-18 (by 10 parts per thousand in O-18) due to exchange of oxygen isotopes between olivine and the O-18-rich water. Dehydrated serpentine was then produced during laboratory heating experiment in vacuum, at T=930 degrees C, for 1h. The oxygen isotopic composition of the dehydrated serpentine was enriched in O-18 by a further 7 parts per thousand. The net result of the hydration-dehydration process was an enrichment of O-18 in the final material by approximately 17 parts per thousand. The new experimental results suggest that the oxygen isotopic compositions of MCCs of the Belgica-like group, including Dhofar 225 and Dhofar 725, could be derived from those of typical CM2 chondrites via several cycles of hydration-dehydration caused by aqueous alteration and subsequent thermal metamorphism within their parent asteroids. C1 [Ivanova, Marina A.; Lorenz, Cyril A.] Russian Acad Sci, Vernadsky Inst Geochem, Moscow, Russia. [Franchi, Ian A.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. [Bychkov, Andrei Y.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia. [Post, Jeffrey E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Ivanova, MA (reprint author), Russian Acad Sci, Vernadsky Inst Geochem, Moscow, Russia. EM meteorite2000@mail.ru RI Bychkov, Andrey/R-6693-2016 OI Bychkov, Andrey/0000-0003-2560-6423 FU Programm-22 of the Russian Academy of Sciences; RFBR [12-05-01161]; STFC [ST/I001964/1] FX We thank Oleg I. Yakovlev, Michael A. Nazarov, Dmitriy D. Badyukov, and Vladimir S. Grinenko for useful advice in experimental works and fruitful discussions of any details in experimental procedures and results. We also thank Vyacheslav S. Sevastiyanov for determination of oxygen isotopic compositions of experimental water before and after experiment of olivine hydration. We thank Dr. John C. Eichelberger for his help in improvement of English language. Fruitful reviews by Michael E. Zolensky and A. J. Timothy Jull helped to improve the manuscript and are greatly appreciated. This study was supported by the Programm-22 of the Russian Academy of Sciences and the RFBR grant 12-05-01161. I. A. Franchi thanks STFC for funding to support this study through grant ST/I001964/1. NR 46 TC 2 Z9 2 U1 1 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD OCT PY 2013 VL 48 IS 10 BP 2059 EP 2070 DI 10.1111/maps.12204 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 268DY UT WOS:000328150100016 ER PT J AU Boisse, I Hartman, JD Bakos, GA Penev, K Csubry, Z Beky, B Latham, DW Bieryla, A Torres, G Kovacs, G Buchhave, LA Hansen, T Everett, M Esquerdo, GA Szklenar, T Falco, E Shporer, A Fulton, BJ Noyes, RW Stefanik, RP Lazar, J Papp, I Sari, P AF Boisse, I. Hartman, J. D. Bakos, G. A. Penev, K. Csubry, Z. Beky, B. Latham, D. W. Bieryla, A. Torres, G. Kovacs, G. Buchhave, L. A. Hansen, T. Everett, M. Esquerdo, G. A. Szklenar, T. Falco, E. Shporer, A. Fulton, B. J. Noyes, R. W. Stefanik, R. P. Lazar, J. Papp, I. Sari, P. TI HAT-P-42b and HAT-P-43b Two inflated transiting hot Jupiters from the HATNet Survey SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; techniques: radial velocities; techniques: photometric; stars: individual: HAT-P-42; stars: individual: HAT-P-43 ID EXTRA-SOLAR PLANETS; ECCENTRIC ORBIT; CORALIE SURVEY; BRIGHT STAR; SPIN-ORBIT; EXOPLANETS; FIELD; OBLIQUITIES; PARAMETERS; ALGORITHM AB Aims. We announce the discovery of two new transiting planets, and provide their accurate initial characterization. Methods. First identified from the HATNet wide-field photometric survey, these candidate transiting planets were then followed-up with a variety of photometric observations. Determining the planetary nature of the objects and characterizing the parameters of the systems were mainly done with the SOPHIE spectrograph at the 1.93m telescope at OHP and the TRES spectrograph at the 1.5m telescope at FLWO. Results. HAT-P-42b and HAT-P-43b are typical hot Jupiters on circular orbits around early-G/late-F main sequence host stars, with periods of 4.641878 +/- 0.000032 and 3.332687 +/- 0.000015 days, masses of 1.044 +/- 0.083 and 0.662 +/- 0.060 M-J, and radii of 1.280 +/- 0.153 and 1.281(0.033)(0.062) R-J, respectively. These discoveries increase the sample of planets with measured mean densities, which are needed to constrain theories of planetary interiors and atmospheres. Moreover, their hosts are relatively bright (V < 13.5), which facilitates further follow-up studies. C1 [Boisse, I.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Hartman, J. D.; Bakos, G. A.; Penev, K.; Csubry, Z.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Beky, B.; Latham, D. W.; Bieryla, A.; Torres, G.; Everett, M.; Esquerdo, G. A.; Szklenar, T.; Falco, E.; Noyes, R. W.; Stefanik, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kovacs, G.] Konkoly Observ Budapest, Budapest, Hungary. [Buchhave, L. A.; Hansen, T.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, L. A.; Hansen, T.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Shporer, A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Shporer, A.; Fulton, B. J.] LCOGT, Santa Barbara, CA USA. [Shporer, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Fulton, B. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. [Kovacs, G.] Univ N Dakota, Dept Phys & Astrophys, Grand Forks, ND 58201 USA. RP Boisse, I (reprint author), Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Oporto, Portugal. EM Isabelle.Boisse@astro.up.pt OI Boisse, Isabelle/0000-0001-8388-8399; Penev, Kaloyan/0000-0003-4464-1371; Buchhave, Lars A./0000-0003-1605-5666 FU Haute-Provence Observatory; European Research Council/European Community under the FP7; Fundaccao para a Ciencia e a Tecnologia (FCT), Portugal [SFRH/BPD/81084/2011]; NASA [NNX08AF23G]; NSF [NSFAST-1108686]; Hungarian Scientific Research Foundation (OTKA) [K-81373]; European Community's Seventh Framework Programme [FP7/2007-2013] FX The authors thank all the staff of Haute-Provence Observatory for their contribution to the success of the ELODIE and SOPHIE projects and their support at the 1.93-m telescope. I. B. acknowledges the support of the European Research Council/European Community under the FP7 through a Starting Grant, as well from Fundaccao para a Ciencia e a Tecnologia (FCT), Portugal, through SFRH/BPD/81084/2011 and the project PTDC/CTEAST/ 098528/2008. We acknowledge partial funding for HATNet operations by NASA grant NNX08AF23G, and support for performing follow-up observations by NSF grant NSFAST-1108686. G. K. acknowledges the support of the Hungarian Scientific Research Foundation (OTKA) through grant K-81373. The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement number RG226604 (OPTICON). We thank the referee for her/his comments. NR 51 TC 6 Z9 6 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 OCT PY 2013 VL 558 AR UNSP A86 DI 10.1051/0004-6361/201220993 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000086 ER PT J AU Cerruti, M Boisson, C Zech, A AF Cerruti, M. Boisson, C. Zech, A. TI Constraining the parameter space of the one-zone synchrotron-self-Compton model for GeV-TeV detected BL Lacertae objects SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiation mechanisms: non-thermal; relativistic processes; methods: numerical; BL Lacertae objects: general; galaxies: individual: 1RXS J101015.9-311909 ID SPECTRAL ENERGY-DISTRIBUTION; LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; X-RAY; MARKARIAN 421; BLAZARS; RADIO; RADIATION; ABSORPTION; QUASARS AB Context. The one-zone synchrotron-self-Compton (SSC) model aims to describe the spectral energy distribution (SED) of BL Lac objects via synchrotron emission by a non-thermal population of electrons and positrons in a single homogeneous emission region, partially upscattered to.-rays by the particles themselves. Aims. The model is usually considered as degenerate, given that the number of free parameters is higher than the number of observables. It is thus common to model the SED by choosing a single set of values for the SSC model parameters that provide a good description of the data, without studying the entire parameter space. We present here a new numerical algorithm that permits us to find the complete set of solutions, using the information coming from the detection in the GeV and TeV energy bands. Methods. The algorithm is composed of three separate steps: we first prepared a grid of simulated SEDs and extracted from each SED the values of the observables; we then parametrized each observable as a function of the SSC parameters; we finally solved the system for a given set of observables. We iteratively solved the system to take into account uncertainties in the values of the observables, producing a family of solutions. Results. We present a first application of our algorithm to the typical high-frequency-peaked BL Lac object 1RXS J101015.9-311909, provide constraints on the SSC parameters, and discuss the result in terms of our understanding of the blazar emitting region. C1 [Cerruti, M.; Boisson, C.; Zech, A.] Univ Paris Diderot, CNRS, Observ Paris, LUTH, F-92190 Meudon, France. [Cerruti, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cerruti, M (reprint author), Univ Paris Diderot, CNRS, Observ Paris, LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France. EM matteo.cerruti@cfa.harvard.edu NR 32 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 OCT PY 2013 VL 558 AR UNSP A47 DI 10.1051/0004-6361/201220963 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000047 ER PT J AU De Beck, E Kaminski, T Patel, NA Young, KH Gottlieb, CA Menten, KM Decin, L AF De Beck, E. Kaminski, T. Patel, N. A. Young, K. H. Gottlieb, C. A. Menten, K. M. Decin, L. TI PO and PN in the wind of the oxygen-rich AGB star IK Tauri SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; stars: individual: IK Tau; stars: mass-loss; astrochemistry ID VY-CANIS MAJORIS; SPECTRAL-LINE SURVEY; CIRCUMSTELLAR ENVELOPES; CARBON-RICH; MICROWAVE SPECTROSCOPY; MOLECULAR-SPECTROSCOPY; PHOSPHORUS CHEMISTRY; COLOGNE DATABASE; CW LEONIS; IRC+10216 AB Context. Phosphorus-bearing compounds have only been studied in the circumstellar environments of the asymptotic giant branch star IRC + 10 216 and the protoplanetary nebula CRL 2688, both carbon-rich objects, and the oxygen-rich red supergiant VY CMa. The current chemical models cannot reproduce the high abundances of PO and PN derived from observations of VY CMa. No observations have been reported of phosphorus in the circumstellar envelopes of oxygen-rich asymptotic giant branch stars. Aims. We aim to set observational constraints on the phosphorous chemistry in the circumstellar envelopes of oxygen-rich asymptotic giant branch stars, by focussing on the Mira-type variable star IK Tau. Methods. Using the IRAM 30m telescope and the Submillimeter Array, we observed four rotational transitions of PN (J = 2-1, 3-2, 6-5, 7-6) and four of PO (J = 5/2-3/2, 7/2-5/2, 13/2-11/2, 15/2-13/2). The IRAM 30m observations were dedicated line observations, while the Submillimeter Array data come from an unbiased spectral survey in the frequency range 279-355 GHz. Results. We present the first detections of PN and PO in an oxygen-rich asymptotic giant branch star and estimate abundances X(PN/H-2) approximate to 3 x 10(-7) and X(PO/H-2) in the range 0.5-6.0 x 10(-7). This is several orders of magnitude higher than what is found for the carbon-rich asymptotic giant branch star IRC + 10 216. The diameter (less than or similar to 0.'' 7) of the PN and PO emission distributions measured in the interferometric data corresponds to a maximum radial extent of about 40 stellar radii. The abundances and the spatial occurrence of the molecules are in very good agreement with the results reported for VY CMa. We did not detect PS or PH3 in the survey. Conclusions. We suggest that PN and PO are the main carriers of phosphorus in the gas phase, with abundances possibly up to several 10(-7). The current chemical models cannot account for this, underlining the strong need for updated chemical models that include phosphorous compounds. C1 [De Beck, E.; Kaminski, T.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [De Beck, E.; Decin, L.] Inst Sterrenkunde, Dept Nat Kunde Sterrenkunde, B-3001 Heverlee, Belgium. [Patel, N. A.; Young, K. H.; Gottlieb, C. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Decin, L.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. RP De Beck, E (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM edebeck@mpifr-bonn.mpg.de OI De Beck, Elvire/0000-0002-7441-7189 FU Smithsonian Institution; Academia Sinica FX The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NR 43 TC 11 Z9 11 U1 0 U2 10 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 OCT PY 2013 VL 558 AR A132 DI 10.1051/0004-6361/201321349 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000132 ER PT J AU Iacobelli, M Haverkorn, M Orru, E Pizzo, RF Anderson, J Beck, R Bell, MR Bonafede, A Chyzy, K Dettmar, RJ Ensslin, TA Heald, G Horellou, C Horneffer, A Jurusik, W Junklewitz, H Kuniyoshi, M Mulcahy, DD Paladino, R Reich, W Scaife, A Sobey, C Sotomayor-Beltran, C Alexov, A Asgekar, A Avruch, IM Bell, ME van Bemmel, I Bentum, MJ Bernardi, G Best, P Birzan, L Breitling, F Broderick, J Brouw, WN Bruggen, M Butcher, HR Ciardi, B Conway, JE de Gasperin, F de Geus, E Duscha, S Eisloffel, J Engels, D Falcke, H Fallows, RA Ferrari, C Frieswijk, W Garrett, MA Griessmeier, J Gunst, AW Hamaker, JP Hassall, TE Hessels, JWT Hoeft, M Horandel, J Jelic, V Karastergiou, A Kondratiev, VI Koopmans, LVE Kramer, M Kuper, G van Leeuwen, J Macario, G Mann, G McKean, JP Munk, H Pandey-Pommier, M Polatidis, AG Rottgering, H Schwarz, D Sluman, J Smirnov, O Stappers, BW Steinmetz, M Tagger, M Tang, Y Tasse, C Toribio, C Vermeulen, R Vocks, C Vogt, C van Weeren, RJ Wise, MW Wucknitz, O Yatawatta, S Zarka, P Zensus, A AF Iacobelli, M. Haverkorn, M. Orru, E. Pizzo, R. F. Anderson, J. Beck, R. Bell, M. R. Bonafede, A. Chyzy, K. Dettmar, R. -J. Ensslin, T. A. Heald, G. Horellou, C. Horneffer, A. Jurusik, W. Junklewitz, H. Kuniyoshi, M. Mulcahy, D. D. Paladino, R. Reich, W. Scaife, A. Sobey, C. Sotomayor-Beltran, C. Alexov, A. Asgekar, A. Avruch, I. M. Bell, M. E. van Bemmel, I. Bentum, M. J. Bernardi, G. Best, P. Birzan, L. Breitling, F. Broderick, J. Brouw, W. N. Brueggen, M. Butcher, H. R. Ciardi, B. Conway, J. E. de Gasperin, F. de Geus, E. Duscha, S. Eisloeffel, J. Engels, D. Falcke, H. Fallows, R. A. Ferrari, C. Frieswijk, W. Garrett, M. A. Griessmeier, J. Gunst, A. W. Hamaker, J. P. Hassall, T. E. Hessels, J. W. T. Hoeft, M. Hoerandel, J. Jelic, V. Karastergiou, A. Kondratiev, V. I. Koopmans, L. V. E. Kramer, M. Kuper, G. van Leeuwen, J. Macario, G. Mann, G. McKean, J. P. Munk, H. Pandey-Pommier, M. Polatidis, A. G. Roettgering, H. Schwarz, D. Sluman, J. Smirnov, O. Stappers, B. W. Steinmetz, M. Tagger, M. Tang, Y. Tasse, C. Toribio, C. Vermeulen, R. Vocks, C. Vogt, C. van Weeren, R. J. Wise, M. W. Wucknitz, O. Yatawatta, S. Zarka, P. Zensus, A. TI Studying Galactic interstellar turbulence through fluctuations in synchrotron emission First LOFAR Galactic foreground detection SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: general; ISM: magnetic fields; ISM: structure; radio continuum: general; radio continuum: ISM techniques; interferometric ID ANGULAR POWER SPECTRUM; MAGNETIC-FIELD; RADIO-EMISSION; W-PROJECTION; WIDE-FIELD; 350 MHZ; POLARIZATION; ALGORITHM; GALAXY; GHZ AB Aims. The characteristic outer scale of turbulence (i. e. the scale at which the dominant source of turbulence injects energy to the interstellar medium) and the ratio of the random to ordered components of the magnetic field are key parameters to characterise magnetic turbulence in the interstellar gas, which affects the propagation of cosmic rays within the Galaxy. We provide new constraints to those two parameters. Methods. We use the LOw Frequency ARray (LOFAR) to image the diffuse continuum emission in the Fan region at (l, b) (137.0., + 7.0.) at 80 '' x 70 '' resolution in the range [146, 174] MHz. We detect multi-scale fluctuations in the Galactic synchrotron emission and compute their power spectrum. Applying theoretical estimates and derivations from the literature for the first time, we derive the outer scale of turbulence and the ratio of random to ordered magnetic field from the characteristics of these fluctuations. Results. We obtain the deepest image of the Fan region to date and find diffuse continuum emission within the primary beam. The power spectrum displays a power law behaviour for scales between 100 and 8 arcmin with a slope a = -1.84 +/- 0.19. We find an upper limit of 20 pc for the outer scale of the magnetic interstellar turbulence toward the Fan region, which is in agreement with previous estimates in literature. We also find a variation of the ratio of random to ordered field as a function of Galactic coordinates, supporting different turbulent regimes. Conclusions. We present the first LOFAR detection and imaging of the Galactic diffuse synchrotron emission around 160 MHz from the highly polarized Fan region. The power spectrum of the foreground synchrotron fluctuations is approximately a power law with a slope a beta-1.84 up to angular multipoles of similar to 1300, corresponding to an angular scale of similar to 8 arcmin. We use power spectra fluctuations from LOFAR as well as earlier GMRT andWSRT observations to constrain the outer scale of turbulence (Lout) of the Galactic synchrotron foreground, finding a range of plausible values of 10-20 pc. Then, we use this information to deduce lower limits of the ratio of ordered to random magnetic field strength. These are found to be 0.3, 0.3, and 0.5 for the LOFAR, WSRT and GMRT fields considered respectively. Both these constraints are in agreement with previous estimates. C1 [Iacobelli, M.; Haverkorn, M.; Birzan, L.; Roettgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Iacobelli, M.; Orru, E.; Pizzo, R. F.; Heald, G.; Asgekar, A.; van Bemmel, I.; Bentum, M. J.; de Geus, E.; Duscha, S.; Fallows, R. A.; Frieswijk, W.; Gunst, A. W.; Hamaker, J. P.; Hessels, J. W. T.; Jelic, V.; Kondratiev, V. I.; Kuper, G.; van Leeuwen, J.; McKean, J. P.; Munk, H.; Polatidis, A. G.; Sluman, J.; Tang, Y.; Toribio, C.; Vermeulen, R.; Vogt, C.; Wise, M. W.; Yatawatta, S.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Haverkorn, M.; Orru, E.; Hoerandel, J.] Radboud Univ Nijmegen, NL-6525 AJ Nijmegen, Netherlands. [Anderson, J.; Beck, R.; Horneffer, A.; Kuniyoshi, M.; Mulcahy, D. D.; Reich, W.; Sobey, C.; Kramer, M.; Wucknitz, O.; Zensus, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Bell, M. R.; Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Bonafede, A.; Brueggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Chyzy, K.; Jurusik, W.] Jagiellonian Univ, PL-30244 Krakow, Poland. [Dettmar, R. -J.; Sotomayor-Beltran, C.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Ensslin, T. A.; Junklewitz, H.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Horellou, C.; Conway, J. E.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. [Scaife, A.; Broderick, J.; Hassall, T. E.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Avruch, I. M.] SRON Netherlands Insitute Space Res, NL-9700 AV Groningen, Netherlands. [Bell, M. E.] Univ Sydney, Sydney Inst Astron, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2006, Australia. [Bernardi, G.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Best, P.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Breitling, F.; Mann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Brouw, W. N.; Koopmans, L. V. E.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Obs, Weston, ACT 2611, Australia. [Eisloeffel, J.; Garrett, M. A.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Engels, D.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Ferrari, C.; Macario, G.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, F-06300 Nice, France. [Griessmeier, J.; Tagger, M.] CNRS, UMR 7328, LPC2E, F-45071 Orleans 02, France. [Karastergiou, A.] Univ Oxford, Oxford OX1 3RH, England. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Schwarz, D.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. [Smirnov, O.] Rhodes Univ, Dept Phys & Elect, Ctr Radio Astron Tech & Technol RATT, ZA-6140 Grahamstown, South Africa. [Hassall, T. E.; Stappers, B. W.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Tasse, C.; Zarka, P.] Observ Paris, CNRS, UMR 8109, LESIA, F-92195 Meudon, France. [Hessels, J. W. T.; Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Falcke, H.; Kondratiev, V. I.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [Wucknitz, O.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Paladino, R.] Univ Bologna, INAF ALMA Reg Ctr, I-40129 Bologna, Italy. RP Iacobelli, M (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM iacobelli@strw.leidenuniv.nl RI Jelic, Vibor/B-2938-2014; Tagger, Michel/O-6615-2014; Ciardi, Benedetta/N-7625-2015; Kondratiev, Vladislav/N-1105-2015; Yatawatta, Sarod/E-6037-2013; OI Jelic, Vibor/0000-0002-6034-8610; Tagger, Michel/0000-0003-2962-3220; Kondratiev, Vladislav/0000-0001-8864-7471; Yatawatta, Sarod/0000-0001-5619-4017; de Gasperin, Francesco/0000-0003-4439-2627; van Weeren, Reinout/0000-0002-0587-1660 FU Agence Nationale de la Recherche [ANR-09-JCJC-0001-01]; European Union's Seventh Framework Programme [239490]; Netherlands Organisation for Scientific Research (NWO) [639.042.915] FX The authors thank the anonymous referee for carefully reading the manuscript and providing helpful comments and suggestions in the preparation of the final manuscript. The authors wish to thank M. Brentjens for his help with the power spectral analysis of LOFAR data analysis. Chiara Ferrari and Giulia Macario acknowledge financial support by the Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. LOFAR, the LOw Frequency ARray designed and constructed by ASTRON, has facilities in several countries, which are owned by various parties (each with their own funding sources), and are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. 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 Organisation for Scientific Research (NWO). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 71 TC 24 Z9 24 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2013 VL 558 AR A72 DI 10.1051/0004-6361/201322013 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000072 ER PT J AU Magdis, GE Rigopoulou, D Helou, G Farrah, D Hurley, P Alonso-Herrero, A Bock, J Burgarella, D Chapman, S Charmandaris, V Cooray, A Dai, YS Dale, D Elbaz, D Feltre, A Hatziminaoglou, E Huang, JS Morrison, G Oliver, S Page, M Scott, D Shi, Y AF Magdis, G. E. Rigopoulou, D. Helou, G. Farrah, D. Hurley, P. Alonso-Herrero, A. Bock, J. Burgarella, D. Chapman, S. Charmandaris, V. Cooray, A. Dai, Y. Sophia Dale, D. Elbaz, D. Feltre, A. Hatziminaoglou, E. Huang, J. -S. Morrison, G. Oliver, S. Page, M. Scott, D. Shi, Y. TI Mid- to far-infrared properties of star-forming galaxies and active galactic nuclei SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; galaxies: active; galaxies: starburst; galaxies: star formation; infrared: galaxies ID SPITZER-SPACE-TELESCOPE; SPECTRAL ENERGY-DISTRIBUTIONS; POLYCYCLIC AROMATIC-HYDROCARBONS; NEED ULTRAVIOLET EXCITATION; PALOMAR-GREEN QUASARS; POWER-LAW GALAXIES; DEEP-FIELD-SOUTH; MIDINFRARED SPECTROSCOPY; INTERSTELLAR-MEDIUM; LUMINOUS GALAXIES AB We study the mid- to far-IR properties of a 24 mu m-selected flux-limited sample (S-24 > 5mJy) of 154 intermediate redshift (< z > similar to 0.15), infrared luminous galaxies, drawn from the 5 Milli-Jansky Unbiased Spitzer Extragalactic Survey. By combining existing mid-IR spectroscopy and new Herschel SPIRE submm photometry from the Herschel Multi-tiered Extragalactic Survey, we derived robust total infrared luminosity (L-IR) and dust mass (M-dust) estimates and infered the relative contribution of the AGN to the infrared energy budget of the sources. We found that the total (8-1000 mu m) infrared emission of galaxies with weak 6.2 mu m PAH emission (EW6.2 <= 0.2 mu m) is dominated by AGN activity, while for galaxies with EW6.2 > 0.2 mu m more than 50% of the L-IR arises from star formation. We also found that for galaxies detected in the 250-500 mu m Herschel bands an AGN has a statistically insignificant effect on the temperature of the cold dust and the far-IR colours of the host galaxy, which are primarily shaped by star formation activity. For star-forming galaxies we reveal an anti-correlation between the L-IR-to-rest-frame 8 mu m luminosity ratio, IR8 = L-IR/L-8 and the strength of PAH features. We found that this anti-correlation is primarily driven by variations in the PAHs emission, and not by variations in the 5-15 mu m mid-IR continuum emission. Using the [NeIII]/[NeII] line ratio as a tracer of the hardness of the radiation field, we confirm that galaxies with harder radiation fields tend to exhibit weaker PAH features, and found that they have higher IR8 values and higher dust-mass-weighted luminosities (L-IR/M-dust), the latter being a proxy for the dust temperature (T-d). We argue that these trends originate either from variations in the environment of the star-forming regions or are caused by variations in the age of the starburst. Finally, we provide scaling relations that will allow estimating L-IR, based on single-band observations with the mid-infrared instrument, on board the upcoming James Webb Space Telescope. C1 [Magdis, G. E.; Rigopoulou, D.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Rigopoulou, D.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Helou, G.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Farrah, D.] Virginia Polytech Inst & State Univ, Dept Phys, Blacksburg, VA 24061 USA. [Hurley, P.; Oliver, S.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Alonso-Herrero, A.] CSIC UC, Inst Fis Cantabria, Santander 39005, Spain. [Bock, J.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Burgarella, D.] Aix Marseille Univ, CNRS, LAM, F-13388 Marseille 13, France. [Chapman, S.] Dalhousie Univ, Halifax, NS B3H 4R2, Canada. [Charmandaris, V.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Charmandaris, V.] Univ Crete, ITCP, Iraklion 71003, Greece. [Charmandaris, V.] IESL Fdn Res & Technol Hellas, Iraklion 71110, Greece. [Charmandaris, V.] Observ Paris, F-75014 Paris, France. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dai, Y. Sophia; Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dale, D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Elbaz, D.] Univ Paris Diderot, CNRS, CEA,DSM,Irfu, Lab AIM Paris Saclay, F-19190 Gif Sur Yvette, France. [Feltre, A.] ESO, D-85748 Garching, Germany. [Feltre, A.; Hatziminaoglou, E.] Dipartimento Fis & Astron, I-35122 Padua, Italy. [Huang, J. -S.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Morrison, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Morrison, G.] Canada France Hawaii Telescope, Kamuela, HI 96743 USA. [Page, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Scott, D.] Univ British Columbia, Dept Phys Astron, Vancouver, BC V6T 1Z1, Canada. [Shi, Y.] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. RP Magdis, GE (reprint author), Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England. EM georgios.magdis@astro.ox.ac.uk RI Charmandaris, Vassilis/A-7196-2008; Magdis, Georgios/C-7295-2014; Alonso-Herrero, Almudena/H-1426-2015; OI Charmandaris, Vassilis/0000-0002-2688-1956; Magdis, Georgios/0000-0002-4872-2294; Alonso-Herrero, Almudena/0000-0001-6794-2519; Scott, Douglas/0000-0002-6878-9840 FU John Fell Oxford University Press (OUP); University of Oxford; Universidad de Cantabria August G. Linares Programme; EU [PIRSES-GA-20120316788] FX GEM acknowledges support from the John Fell Oxford University Press (OUP) Research Fund and the University of Oxford. A.A.-H. acknowledges funding through the Universidad de Cantabria August G. Linares Programme. VC acknowledges partial support from the EU FP7 Grant PIRSES-GA-20120316788. This paper uses data from Herschel's photometer SPIRE. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). NR 95 TC 15 Z9 15 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2013 VL 558 AR UNSP A136 DI 10.1051/0004-6361/201322226 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000136 ER PT J AU Mohler-Fischer, M Mancini, L Hartman, JD Bakos, GA Penev, K Bayliss, D Jordan, A Csubry, Z Zhou, G Rabus, M Nikolov, N Brahm, R Espinoza, N Buchhave, LA Beky, B Suc, V Csak, B Henning, T Wright, DJ Tinney, CG Addison, BC Schmidt, B Noyes, RW Papp, I Lazar, J Sari, P Conroy, P AF Mohler-Fischer, M. Mancini, L. Hartman, J. D. Bakos, G. A. Penev, K. Bayliss, D. Jordan, A. Csubry, Z. Zhou, G. Rabus, M. Nikolov, N. Brahm, R. Espinoza, N. Buchhave, L. A. Beky, B. Suc, V. Csak, B. Henning, T. Wright, D. J. Tinney, C. G. Addison, B. C. Schmidt, B. Noyes, R. W. Papp, I. Lazar, J. Sari, P. Conroy, P. TI HATS-2b: A transiting extrasolar planet orbiting a K-type star showing starspot activity SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; techniques: spectroscopic; stars: fundamental parameters; techniques: photometric stars; individual: HATS-2; stars: individual: GSC 6665-00236 ID JUPITER-MASS COMPANION; SOLAR-TYPE STAR; HOT-JUPITER; EXOPLANETARY SYSTEM; KEPLER FIELD; SPACED DATA; PHOTOMETRY; TELESCOPE; CANDIDATES; RADIUS AB We report the discovery of HATS-2b, the second transiting extrasolar planet detected by the HATSouth survey. HATS-2b is moving on a circular orbit around a V = 13.6 mag, K-type dwarf star (GSC 6665-00236), at a separation of 0.0230 +/- 0.0003 AU and with a period of 1.3541 days. The planetary parameters have been robustly determined using a simultaneous fit of the HATSouth, MPG/ESO 2.2m/GROND, Faulkes Telescope South/Spectral transit photometry, and MPG/ESO 2.2m/FEROS, Euler 1.2m/CORALIE, AAT 3.9m/CYCLOPS radial-velocity measurements. HATS-2b has a mass of 1.37 +/- 0.16 MJ, a radius of 1.14 +/- 0.03 RJ, and an equilibrium temperature of 1567 +/- 30 K. The host star has a mass of 0.88 +/- 0.04 M fi and a radius of 0.89 +/- 0.02 R fi, and it shows starspot activity. We characterized the stellar activity by analyzing two photometric follow-up transit light curves taken with the GROND instrument, both obtained simultaneously in four optical bands (covering the wavelength range of 3860 9520 angstrom). The two light curves contain anomalies compatible with starspots on the photosphere of the host star along the same transit chord. C1 [Mohler-Fischer, M.; Mancini, L.; Csak, B.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Nikolov, N.] Univ Exeter, Sch Phys, Astrophys Grp, Exeter EX4 4QL, Devon, England. [Wright, D. J.; Tinney, C. G.; Addison, B. C.] Univ New S Wales, Sch Phys, Exoplanetary Sci UNSW, Sydney, NSW 2052, Australia. [Wright, D. J.; Tinney, C. G.; Addison, B. C.] Univ New S Wales, Australian Ctr Astrobiol, Kensington, NSW 2052, Australia. [Hartman, J. D.; Bakos, G. A.; Penev, K.; Csubry, Z.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Hartman, J. D.; Bakos, G. A.; Penev, K.; Csubry, Z.; Beky, B.; Noyes, R. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, D.; Zhou, G.; Schmidt, B.; Conroy, P.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Jordan, A.; Rabus, M.; Brahm, R.; Espinoza, N.; Suc, V.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 7820436, Chile. [Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, L. A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Papp, I.; Lazar, J.; Sari, P.] Hungarian Astron Assoc, H-1158 Budapest, Hungary. [Csak, B.] ELTE Gothard Lendulet Res Grp, H-9700 Szombathely, Hungary. RP Mohler-Fischer, M (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM mohler@mpia.de OI Jordan, Andres/0000-0002-5389-3944; Hartman, Joel/0000-0001-8732-6166 FU NSF MRI grant [NSF/AST-0723074]; NASA [NNX09AB29G]; BASAL CATA [PFB-06]; STFC consolidated grant; FONDECYT [3120097]; Robert Martin Ayers Sciences Fund; SIMBAD database; ARC Australian Professorial Fellowship [DP0774000]; ARC LIEF [LE0989347]; ARC Super Science Fellowships [FS100100046]; [NSF/AST-1108686] FX Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074, operations are supported by NASA grant NNX09AB29G, and follow-up observations receive partial support from grant NSF/AST-1108686. Data presented in this paper is based partly on observations obtained with the HATSouth Station at the Las Campanas Observatory of the Carnegie Institution of Washington. This work is based on observations collected at the MPG/ESO 2.2 m Telescope located at the ESO Observatory in La Silla (Chile), under program IDs P087. A-9014(A), P088. A-9008(A), P089. A9008(A), 089. A-9006(A), and Chilean time P087. C-0508(A). Operations of this telescope are jointly performed by the Max Planck Gesellschaft and the European Southern Observatory. GROND has been built by the high-energy group of MPE in collaboration with the LSW Tautenburg and ESO, and is operating as a PI-instrument at the MPG/ESO 2.2 m telescope. We thank Timo Anguita and Regis Lachaume for their technical assistance during the observations at the MPG/ESO 2.2 m Telescope. A. J. acknowledges support from Fondecyt project 1130857, Anillo ACT-086, BASAL CATA PFB-06 and the Millenium Science Initiative, Chilean Ministry of Economy (Nucleus P10-022-F). V. S. acknowledges support form BASAL CATA PFB-06. R. B. and N. E. acknowledge support from Fondecyt project 1095213. N. N. acknowledges support from an STFC consolidated grant. M. R. acknowledges support from a FONDECYT postdoctoral fellowship N ffi 3120097. L. M. thanks Jeremy Tregloan-Reed for his help for using of the PRISM and GEMC codes, and John Southworth and Valerio Bozza for useful discussions. This paper also uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope. Work at the Australian National University is supported by ARC Laureate Fellowship Grant FL0992131. We acknowledge the use of the AAVSO Photometric AllSky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund, and the SIMBAD database, operated at the CDS, Strasbourg, France. Work at UNSW has been supported by ARC Australian Professorial Fellowship grant DP0774000, ARC LIEF grant LE0989347 and ARC Super Science Fellowships FS100100046. NR 78 TC 22 Z9 22 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2013 VL 558 AR A55 DI 10.1051/0004-6361/201321663 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000055 ER PT J AU Mottram, JC van Dishoeck, EF Schmalzl, M Kristensen, LE Visser, R Hogerheijde, MR Bruderer, S AF Mottram, J. C. van Dishoeck, E. F. Schmalzl, M. Kristensen, L. E. Visser, R. Hogerheijde, M. R. Bruderer, S. TI Waterfalls around protostars Infall motions towards Class 0/I envelopes as probed by water SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; line: profiles; stars: formation; stars: protostars; ISM: abundances; ISM: kinematics and dynamics ID STAR-FORMING REGIONS; YOUNG STELLAR OBJECTS; LOW-MASS PROTOSTARS; NGC-1333 IRAS-4 REGION; MOLECULAR CLOUD CORES; INNER 100 AU; PROTOSTELLAR ENVELOPES; HERSCHEL-HIFI; NGC 1333; RESOLUTION OBSERVATIONS AB Context. For stars to form, material must fall inwards from core scales through the envelope towards the central protostar. While theories of how this takes place have been around for some time, the velocity profile around protostars is poorly constrained. The combination of observations in multiple transitions of a tracer which is sensitive to kinematics and radiative transfer modelling of those lines has the potential to break this deadlock. Aims. Seven protostars observed with the Heterodyne Instrument for the Far-Infrared (HIFI) on board the Herschel Space Observatory as part of the "Water in star-forming regions with Herschel" (WISH) survey show infall signatures in water line observations. We aim to constrain the infall velocity and the radii over which infall is taking place within the protostellar envelopes of these sources. We will also use these data to constrain the chemistry of cold water. Methods. We use 1-D non-LTE ratran radiative transfer models of the observed water lines to constrain the infall velocity and chemistry in the protostellar envelopes of six Class 0 protostars and one Class I source. We assume a free-fall velocity profile and, having found the best fit, vary the radii over which infall takes place. Results. In the well-studied Class 0 protostar NGC1333-IRAS4A we find that our observations probe infall over the whole envelope to which our observations are sensitive (r greater than or similar to 1000 AU). For L1527, L1157, BHR71 and IRAS 15398 infall takes place on core to envelope scales (i.e. similar to 10000-3000 AU). In Serpens-SMM4 and GSS30 the inverse P-Cygni profiles seen in the ground-state lines are more likely due to larger-scale motions or foreground clouds. Models including a simple consideration of the chemistry are consistent with the observations, while using step abundance profiles are not. The non-detection of excited water in the inner envelope in six out of seven protostars is further evidence that water must be heavily depleted from the gas-phase at these radii. Conclusions. Infall in four of the sources is supersonic and in all sources must take place at the outer edge of the envelope, which may be evidence that collapse is global or outside-in rather than inside-out. The mass infall rate in NGC1333-IRAS4A is large (>= 10(-4) M-circle dot yr(-1)), higher than the mass outflow rate and expected mass accretion rates onto the star. This suggests that any flattened disk-like structure on small scales will be gravitationally unstable, potentially leading to rotational fragmentation and/or episodic accretion. C1 [Mottram, J. C.; van Dishoeck, E. F.; Schmalzl, M.; Kristensen, L. E.; Hogerheijde, M. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Bruderer, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Visser, R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Mottram, JC (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM mottram@strw.leidenuniv.nl RI Kristensen, Lars/F-4774-2011 OI Kristensen, Lars/0000-0003-1159-3721 FU Netherlands Organisation for Scientific Research (NWO) [614.001.008]; Netherlands Research School for Astronomy (NOVA); Spinoza grant; European Community [238 258] FX The authors would like to thank the anonymous referee, whose comments helped improved the clarity and content of the paper. We also thank Floris van der Tak, Mario Tafalla, Paola Caselli, Neal Evans and Audrey Coutens for their valuable comments on the manuscript, and Daniel Harsono, Catherine Walsh, Pamela Klaassen and Tobias Albertsson for stimulating discussions. JCM is funded by grant 614.001.008 from the Netherlands Organisation for Scientific Research (NWO). 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 238 258 (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, 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. NR 93 TC 30 Z9 30 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 OCT PY 2013 VL 558 AR A126 DI 10.1051/0004-6361/201321828 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000126 ER PT J AU Muller, TG Miyata, T Kiss, C Gurwell, MA Hasegawa, S Vilenius, E Sako, S Kamizuka, T Nakamura, T Asano, K Uchiyama, M Konishi, M Yoneda, M Ootsubo, T Usui, F Yoshii, Y Kidger, M Altieri, B Lorente, R Pal, A O'Rourke, L Metcalfe, L AF Mueller, T. G. Miyata, T. Kiss, C. Gurwell, M. A. Hasegawa, S. Vilenius, E. Sako, S. Kamizuka, T. Nakamura, T. Asano, K. Uchiyama, M. Konishi, M. Yoneda, M. Ootsubo, T. Usui, F. Yoshii, Y. Kidger, M. Altieri, B. Lorente, R. Pal, A. O'Rourke, L. Metcalfe, L. TI Physical properties of asteroid 308635 (2005 YU55) derived from multi-instrument infrared observations during a very close Earth approach SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE minor planets, asteroids: individual: (308635) 2005 YU55; radiation mechanisms: thermal; techniques: photometric; infrared: planetary systems ID THERMAL PHYSICS; THERMOPHYSICAL ANALYSIS; TARGET AB The near-Earth asteroid 308635 (2005 YU55) is a potentially hazardous asteroid which was discovered in 2005 and passed Earth on Nov. 8, 2011 at 0.85 lunar distances. This was the closest known approach by an asteroid of several hundred metres in diameter since 1976 when an object of similar size passed at 0.5 lunar distances. We observed 2005 YU55 from the ground with a recently developed mid-IR camera (miniTAO/MAX38) in N and Q bands and with the Submillimeter Array (SMA) at 1.3 mm. In addition, we obtained space observations with Herschel/PACS at 70, 100, and 160 mu m. Our thermal measurements cover a wide range of wavelengths from 8.9 mu m to 1.3 mm and were taken after opposition at phase angles between -97 degrees and -18 degrees. We performed a radiometric analysis via a thermophysical model and combined our derived properties with results from radar, adaptive optics, lightcurve observations, speckle, and auxiliary thermal data. We find that 308635 (2005 YU55) has an almost spherical shape with an effective diameter of 300 to 312 m and a geometric albedo p(V) of 0.055 to 0.075. Its spin axis is oriented towards celestial directions (lambda(ecl), beta(ecl)) = (60 degrees +/- 30 degrees, -60 degrees +/- 15 degrees), which means it has a retrograde sense of rotation. The analysis of all available data combined revealed a discrepancy with the radar-derived size. Our radiometric analysis of the thermal data together with the problem to find a unique rotation period might be connected to a non-principal axis rotation. A low to intermediate level of surface roughness (rms mean slope in the range 0.1-0.3) is required to explain the available thermal measurements. We found a thermal inertia in the range 350-800 Jm(-2) s(-0.5) K-1, very similar to the rubble-pile asteroid 25 143 Itokawa and indicating a surface with a mixture of low conductivity fine regolith with larger rocks and boulders of high thermal inertia. C1 [Mueller, T. G.; Vilenius, E.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Miyata, T.; Sako, S.; Kamizuka, T.; Asano, K.; Uchiyama, M.; Konishi, M.; Yoshii, Y.] Univ Tokyo, Inst Astron, Sch Sci, Mitaka, Tokyo 1810015, Japan. [Kiss, C.; Pal, A.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, H-1121 Budapest, Hungary. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hasegawa, S.; Usui, F.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Nakamura, T.] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Yoneda, M.] Tohoku Univ, Planetary Plasma & Atmospher Res Ctr, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Ootsubo, T.] Tohoku Univ, Astron Inst, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Kidger, M.; Altieri, B.; Lorente, R.; O'Rourke, L.; Metcalfe, L.] European Space Agcy, ESAC, Madrid 28691, Spain. RP Muller, TG (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr,Postfach 1312, D-85741 Garching, Germany. EM tmueller@mpe.mpg.de; tmiyata@ioa.s.u-tokyo.ac.jp FU Smithsonian Institution and the Academia Sinica; European Space Agency [PECS-98073]; Hungarian Space Office; Hungarian Research Fund (OTKA) [K-104607]; Hungarian Academy of Sciences; German DLR [50 OR 1108]; Space Plasma Laboratory, ISAS/JAXA; Hungarian [LP2012-31/2012] FX We would like to thank the Herschel operations team who supported the planning and scheduling of our fixed-time observations. Without their dedication and enthusiasm these measurements would not have been possible. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The work of C.K. has been supported by the PECS-98073 contract of the European Space Agency and the Hungarian Space Office, the K-104607 grant of the Hungarian Research Fund (OTKA), and the Bolyai Research Fellowship of the Hungarian Academy of Sciences. E. Vilenius acknowledges the support of the German DLR project number 50 OR 1108. S.H. is supported by the Space Plasma Laboratory, ISAS/JAXA. A.P. is supported by the Hungarian grant LP2012-31/2012. NR 40 TC 7 Z9 7 U1 3 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 OCT PY 2013 VL 558 AR UNSP A97 DI 10.1051/0004-6361/201321664 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000097 ER PT J AU Robitaille, TP Tollerud, EJ Greenfield, P Droettboom, M Bray, E Aldcroft, T Davis, M Ginsburg, A Price-Whelan, AM Kerzendorf, WE Conley, A Crighton, N Barbary, K Muna, D Ferguson, H Grollier, F Parikh, MM Nair, PH Guenther, HM Deil, C Woillez, J Conseil, S Kramer, R Turner, JEH Singer, L Fox, R Weaver, BA Zabalza, V Edwards, ZI Bostroem, KA Burke, DJ Casey, AR Crawford, SM Dencheva, N Ely, J Jenness, T Labrie, K Lim, PL Pierfederici, F Pontzen, A Ptak, A Refsdal, B Servillat, M Streicher, O AF Robitaille, Thomas P. Tollerud, Erik J. Greenfield, Perry Droettboom, Michael Bray, Erik Aldcroft, Tom Davis, Matt Ginsburg, Adam Price-Whelan, Adrian M. Kerzendorf, Wolfgang E. Conley, Alexander Crighton, Neil Barbary, Kyle Muna, Demitri Ferguson, Henry Grollier, Frederic Parikh, Madhura M. Nair, Prasanth H. Guenther, Hans M. Deil, Christoph Woillez, Julien Conseil, Simon Kramer, Roban Turner, James E. H. Singer, Leo Fox, Ryan Weaver, Benjamin A. Zabalza, Victor Edwards, Zachary I. Bostroem, K. Azalee Burke, D. J. Casey, Andrew R. Crawford, Steven M. Dencheva, Nadia Ely, Justin Jenness, Tim Labrie, Kathleen Lim, Pey Lian Pierfederici, Francesco Pontzen, Andrew Ptak, Andy Refsdal, Brian Servillat, Mathieu Streicher, Ole CA Astropy Collaboration TI Astropy: A community Python package for astronomy SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; methods: miscellaneous; virtual observatory tools ID OBSERVATIONS COSMOLOGICAL INTERPRETATION; FITS; REPRESENTATIONS AB We present the first public version (v0.2) of the open- source and community- developed Python package, Astropy. This package provides core astronomy- related functionality to the community, including support for domain- specific file formats such as flexible image transport system (FITS) files, Virtual Observatory (VO) tables, and common ASCII table formats, unit and physical quantity conversions, physical constants specific to astronomy, celestial coordinate and time transformations, world coordinate system (WCS) support, generalized containers for representing gridded as well as tabular data, and a framework for cosmological transformations and conversions. Significant functionality is under active development, such as a model fitting framework, VO client and server tools, and aperture and point spread function (PSF) photometry tools. The core development team is actively making additions and enhancements to the current code base, and we encourage anyone interested to participate in the development of future Astropy versions. C1 [Robitaille, Thomas P.; Crighton, Neil] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Tollerud, Erik J.] Yale Univ, Dept Astron, New Haven, CT 06510 USA. [Greenfield, Perry; Droettboom, Michael; Bray, Erik; Davis, Matt; Ferguson, Henry; Bostroem, K. Azalee; Dencheva, Nadia; Ely, Justin; Lim, Pey Lian; Pierfederici, Francesco] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Aldcroft, Tom; Guenther, Hans M.; Burke, D. J.; Refsdal, Brian; Servillat, Mathieu] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ginsburg, Adam; Conley, Alexander] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Price-Whelan, Adrian M.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Kerzendorf, Wolfgang E.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Barbary, Kyle] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Muna, Demitri] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Parikh, Madhura M.] SV Natl Inst Technol, Surat 395007, India. [Deil, Christoph; Zabalza, Victor] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Woillez, Julien] European So Observ, D-85748 Garching, Germany. [Conseil, Simon] Univ Aix Marseille, OAMP, Lab Astrophys Marseille, F-13388 Marseille, France. [Conseil, Simon] CNRS, F-13388 Marseille, France. [Kramer, Roban] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Turner, James E. H.] Gemini Observ, La Serena, Chile. [Singer, Leo] CALTECH, LIGO Lab, Pasadena, CA 91125 USA. [Weaver, Benjamin A.] New York Univ, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Edwards, Zachary I.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Casey, Andrew R.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia. [Crawford, Steven M.] SAAO, ZA-7925 Cape Town, South Africa. [Jenness, Tim] Joint Astron Ctr, Hilo, HI 96720 USA. [Jenness, Tim] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Labrie, Kathleen] Gemini Observ, Hilo, HI 96720 USA. [Pontzen, Andrew] Oxford Astrophys, Oxford OX1 3RH, England. [Pontzen, Andrew] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Ptak, Andy] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab Code 662, Greenbelt, MD 20771 USA. [Servillat, Mathieu] CEA Saclay, Lab AIM, F-91191 Gif Sur Yvette, France. [Streicher, Ole] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. RP Robitaille, TP (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM robitaille@mpia.de OI Burke, Douglas/0000-0003-4428-7835; Tollerud, Erik/0000-0002-9599-310X; Gunther, Hans Moritz/0000-0003-4243-2840; Jenness, Tim/0000-0001-5982-167X; Streicher, Ole/0000-0001-7751-1843; Ginsburg, Adam/0000-0001-6431-9633; Kerzendorf, Wolfgang/0000-0002-0479-7235; Casey, Andrew/0000-0003-0174-0564; Robitaille, Thomas/0000-0002-8642-1329 FU NASA [NAS8-39073] FX We thank the referee, Igor Chiligarian, for suggestions that helped improve this paper. We would like to thank the NumPy, SciPy (Jones et al. 2001), IPython and Matplolib communities for providing their packages which are invaluable to the development of Astropy. We thank the GitHub (h t t p : //www. github.com) team for providing us with an excellent free development platform. We also are grateful to Read the Docs (https : //readthedocs.org /), Shining Panda (https://www. shiningpanda-ci.com/), and Travis (htps://www.tavis-ci.org/) for providing free documentation hosting and testing respectively. Finally, we would like to thank all the a s t r o p y users that have provided feedback and submitted bug reports. The contribution by T. Aldcroft and D. Burke was funded by NASA contract NAS8-39073. The name resolution functionality shown in Fig. 4 makes use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 40 TC 274 Z9 274 U1 3 U2 16 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2013 VL 558 AR UNSP A33 DI 10.1051/0004-6361/201322068 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000033 ER PT J AU Wang, KS Bourke, TL Hogerheijde, MR van der Tak, FFS Benz, AO Megeath, ST Wilson, TL AF Wang, K. -S. Bourke, T. L. Hogerheijde, M. R. van der Tak, F. F. S. Benz, A. O. Megeath, S. T. Wilson, T. L. TI Dense molecular cocoons in the massive protocluster W3 IRS5: a test case for models of massive star formation SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: massive; stars: formation; ISM: kinematics and dynamics; ISM: individual objects: W3 IRS5 ID YOUNG STELLAR OBJECTS; FORMING REGION; HOT CORES; COLLISIONAL EXCITATION; SULFUR CHEMISTRY; COMPETITIVE ACCRETION; INTERSTELLAR-MEDIUM; CHEMICAL VARIATIONS; BEARING MOLECULES; RADIO-CONTINUUM AB Context. Two competing models describe the formation of massive stars in objects like the Orion Trapezium. In the turbulent core accretion model, the resulting stellar masses are directly related to the mass distribution of the cloud condensations. In the competitive accretion model, the gravitational potential of the protocluster captures gas from the surrounding cloud for which the individual cluster members compete. Aims. With high resolution submillimeter observations of the structure, kinematics, and chemistry of the proto-Trapezium cluster W3 IRS5, we aim to determine which mode of star formation dominates. Methods. We present 354 GHz Submillimeter Array observations at resolutions of 1 0 0 -3 0 0 (1800-5400 AU) of W3 IRS5. The dust continuum traces the compact source structure and masses of the individual cores, while molecular lines of CS, SO, SO2, HCN, H2CS, HNCO, and CH3OH (and isotopologues) reveal the gas kinematics, density, and temperature. Results. The observations show five emission peaks (SMM1-5). SMM1 and SMM2 contain massive embedded stars (similar to 20 M fi); SMM3-5 are starless or contain low-mass stars (< 8 M fi). The inferred densities are high, similar to 107 cm 3, but the core masses are small, 0 : 2 0 : 6 M fi. The detected molecular emission reveals four di ff erent chemical zones. Abundant (X similar to few 10 7 to 10 6) SO and SO2 are associated with SMM1 and SMM2, indicating active sulfur chemistry. A low abundance (5 similar to 10 8) of CH3OH concentrated on SMM3 /4 suggest the presence of a hot core that is only just turning on, possibly by external feedback from SMM1 /2. The gas kinematics are complex with contributions from a near pole-on outflow traced by CS, SO, and HCN; rotation in SO2, and a jet in vibrationally excited HCN. Conclusions. The proto-Trapezium cluster W3 IRS5 is an ideal test case to discriminate between models of massive star formation. Either the massive stars accrete locally from their local cores; in this case the small core masses imply that W3 IRS5 is at the very end stages (1000 yr) of infall and accretion, or the stars are accreting from the global collapse of a massive, cluster forming core. We find that the observed masses, densities and line widths observed toward W3 IRS 5 and the surrounding cluster forming core are consistent with the competitive accretion of gas at rates of. M similar to 10 4 M fi yr 1 by the massive young forming stars. Future mapping of the gas kinematics from large to small scales will determine whether large-scale gas inflow occurs and how the cluster members compete to accrete this material. C1 [Wang, K. -S.; Hogerheijde, M. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van der Tak, F. F. S.] SRON Netherlands Inst Space Res, NL-9712 Groningen, Netherlands. [van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9712 Groningen, Netherlands. [Benz, A. O.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Megeath, S. T.] Univ Toledo, Ritter Observ, Toledo, OH 43606 USA. [Wilson, T. L.] Naval Res Lab, Washington, DC 20375 USA. RP Wang, KS (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM kswang@strw.leidenuniv.nl FU Nederlandse Onderzoekschool voor Astronomie (NOVA) FX We thank the anonymous referee and the editor Malcolm Walmsley for reviewing our paper. We also thank the SMA staff for conducting our observations. The research of K.-S.W. at Leiden Observatory is supported through a Ph.D. grant from the Nederlandse Onderzoekschool voor Astronomie (NOVA). This research has made use of NASA's Astrophysics Data System Bibliographic Services. NR 63 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 OCT PY 2013 VL 558 AR A69 DI 10.1051/0004-6361/201322087 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000069 ER PT J AU Yildiz, UA Acharyya, K Goldsmith, PF van Dishoeck, EF Melnick, G Snell, R Liseau, R Chen, JH Pagani, L Bergin, E Caselli, P Herbst, E Kristensen, LE Visser, R Lis, DC Gerin, M AF Yildiz, Umut A. Acharyya, Kinsuk Goldsmith, Paul F. van Dishoeck, Ewine F. Melnick, Gary Snell, Ronald Liseau, Rene Chen, Jo-Hsin Pagani, Laurent Bergin, Edwin Caselli, Paola Herbst, Eric Kristensen, Lars E. Visser, Ruud Lis, Dariusz C. Gerin, Maryvonne TI Deep observations of O-2 toward a low-mass protostar with Herschel-HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; ISM: molecules; ISM: individual objects: NGC 1333 IRAS 4A ID DENSE INTERSTELLAR CLOUDS; STAR-FORMING REGIONS; WAVE-ASTRONOMY-SATELLITE; YOUNG STELLAR OBJECTS; NGC 1333; MOLECULAR-OXYGEN; DUST GRAINS; CHEMICAL HISTORY; WATER FORMATION; OPHIUCHI CLOUD AB Context. According to traditional gas-phase chemical models, O-2 should be abundant in molecular clouds, but until recently, attempts to detect interstellar O-2 line emission with ground-and space-based observatories have failed. Aims. Following the multi-line detections of O-2 with low abundances in the Orion and. Oph A molecular clouds with Herschel, it is important to investigate other environments, and we here quantify the O-2 abundance near a solar-mass protostar. Methods. Observations of molecular oxygen, O-2, at 487 GHz toward a deeply embedded low-mass Class 0 protostar, NGC 1333IRAS 4A, are presented, using the Heterodyne Instrument for the Far Infrared (HIFI) on the Herschel Space Observatory. Complementary data of the chemically related NO and CO molecules are obtained as well. The high spectral resolution data are analysed using radiative transfer models to infer column densities and abundances, and are tested directly against full gas-grain chemical models. Results. The deep HIFI spectrum fails to show O-2 at the velocity of the dense protostellar envelope, implying one of the lowest abundance upper limits of O-2/H-2 at = 6x 10-9 (3s). The O-2/CO abundance ratio is less than 0.005. However, a tentative (4.5s) detection of O-2 is seen at the velocity of the surrounding NGC 1333 molecular cloud, shifted by 1 km s-1 relative to the protostar. For the protostellar envelope, pure gas-phase models and gas-grain chemical models require a long pre-collapse phase (similar to 0.7-1 x 106 years), during which atomic and molecular oxygen are frozen out onto dust grains and fully converted to H2O, to avoid overproduction of O2 in the dense envelope. The same model also reproduces the limits on the chemically related NO molecule if hydrogenation of NO on the grains to more complex molecules such as NH2OH, found in recent laboratory experiments, is included. The tentative detection of O-2 in the surrounding cloud is consistent with a low-density PDR model with small changes in reaction rates. Conclusions. The low O-2 abundance in the collapsing envelope around a low-mass protostar suggests that the gas and ice entering protoplanetary disks is very poor in O-2. C1 [Yildiz, Umut A.; van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Acharyya, Kinsuk] SN Bose Natl Ctr Basic Sci, Kolkata 700098, Salt Lake, India. [Goldsmith, Paul F.; Chen, Jo-Hsin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Melnick, Gary; Kristensen, Lars E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Snell, Ronald] Univ Massachusetts, Dept Astron, LGRT 619, Amherst, MA 01003 USA. [Liseau, Rene] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Pagani, Laurent] Observ Paris, LERMA, F-75014 Paris, France. [Pagani, Laurent] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Bergin, Edwin; Visser, Ruud] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Caselli, Paola] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, Paola] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Herbst, Eric] Univ Virginia, Dept Chem, Charlottesville, VA USA. [Herbst, Eric] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Herbst, Eric] Univ Virginia, Dept Phys, Charlottesville, VA 22901 USA. [Lis, Dariusz C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Gerin, Maryvonne] Observ Paris, CNRS, UMR 8112, LRA,LERMA, F-75231 Paris 5, France. [Gerin, Maryvonne] Ecole Normale Super, F-75231 Paris 5, France. RP Yildiz, UA (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM yildiz@strw.leidenuniv.nl RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Goldsmith, Paul/H-3159-2016 OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; FU Netherlands Research School for Astronomy (NOVA); Spinoza grant; Netherlands Organisation for Scientific Research (NWO) [614.001.008]; European Community [238258, 291141]; NASA FX U. A. Y. and astrochemistry in Leiden are supported by the Netherlands Research School for Astronomy (NOVA), by a Spinoza grant and grant 614.001.008 from the Netherlands Organisation for Scientific Research (NWO), and by the European Community's Seventh Framework Programme FP7/2007-2013 under grant agreement 238258 (LASSIE) and 291141 (CHEMPLAN). This work was carried out in part at the Jet Propulsion Laboratory, which is operated by the California Institute of Technology under contract with NASA. The authors are grateful to many funding agencies and the HIFI-ICC staff, who has been contributing for the construction of Herschel and HIFI for many years. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiolog a (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, NASA/JPL, NHSC. NR 86 TC 24 Z9 25 U1 1 U2 17 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 OCT PY 2013 VL 558 AR A58 DI 10.1051/0004-6361/201321944 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 246XF UT WOS:000326574000058 ER PT J AU MacLeod, KG Huber, BT Berrocoso, AJ Wendler, I AF MacLeod, Kenneth G. Huber, Brian T. Jimenez Berrocoso, Alvaro Wendler, Ines TI A stable and hot Turonian without glacial delta O-18 excursions is indicated by exquisitely preserved Tanzanian foraminifera SO GEOLOGY LA English DT Article ID ISOTOPIC EVIDENCE; RECORD; GREENHOUSE; LITHOSTRATIGRAPHY; CHEMOSTRATIGRAPHY; BIOSTRATIGRAPHY; TEMPERATURE; SEDIMENTS; WARMTH AB A shift from the icehouse climate in which humans evolved to a Late Cretaceous-like greenhouse climate is an often-repeated cautionary prediction of the consequences of continued anthropogenic CO2 emissions. The corollary, that understanding the past might help predict the future, has justified many Late Cretaceous studies, but important questions remain about climate stability and sensitivity. New delta O-18 measurements of more than 1000 samples of exceptionally well preserved foraminifera (8 planktic and 11 benthic taxa) from two sites in Tanzania indicate that hot and remarkably stable conditions prevailed in the region during the Turonian, including during a proposed greenhouse glacial event. Planktic taxa have delta O-18 values largely between -4.0 parts per thousand and -5.0 parts per thousand, suggesting surface-water temperatures between 30 and 35 degrees C. Estimates for seafloor temperatures are between 18 and 25 degrees C. No parallel shifts in delta O-18 values are observed among planktic and benthic taxa, contradicting an often-cited line of evidence for greenhouse glaciations and supporting an effectively ice-free Turonian world. C1 [MacLeod, Kenneth G.] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. [Huber, Brian T.] Smithsonian Museum Nat Hist, MRC 121, Dept Paleobiol, Washington, DC 20013 USA. [Jimenez Berrocoso, Alvaro] Repsol Explorat SA, Madrid 28045, Spain. [Wendler, Ines] Univ Bremen, Dept Geol Sci, D-28334 Bremen, Germany. RP MacLeod, KG (reprint author), Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. EM MacLeodK@missouri.edu RI MacLeod, Kenneth/C-4042-2017 OI MacLeod, Kenneth/0000-0002-6016-0837 FU Tanzania Petroleum Development Corporation; National Science Foundation; Smithsonian Institution's Walcott Fund FX Support from the Tanzania Petroleum Development Corporation, especially J. Singano, M. Mkereme, E. Mgaya, E. Mchana, A. Mweneinda, E. Msaki, and F. Mayagilo, was essential. We thank S. Ehlinger, S. Haynes, L. Petruny, C. Rodriguez-Russo, and J. Vincent for picking foraminifera and for laboratory assistance. Funding was provided by the National Science Foundation (MacLeod, Huber) and the Smithsonian Institution's Walcott Fund (Huber). NR 29 TC 31 Z9 31 U1 2 U2 14 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 OCT PY 2013 VL 41 IS 10 BP 1083 EP 1086 DI 10.1130/G34510.1 PG 4 WC Geology SC Geology GA 257NJ UT WOS:000327391200011 ER PT J AU Weitz, CM Bishop, JL Grant, JA AF Weitz, Catherine M. Bishop, Janice L. Grant, John A. TI Gypsum, opal, and fluvial channels within a trough of Noctis Labyrinthus, Mars: Implications for aqueous activity during the Late Hesperian to Amazonian SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Mars; Hydrated minerals; Fluvial channels ID VALLES MARINERIS; OMEGA/MARS EXPRESS; MAWRTH VALLIS; SILICA; DEPOSITS; EVOLUTION; CRISTOBALITE; REFLECTANCE; SOLUBILITY; DIAGENESIS AB We investigate in detail the morphology, mineralogy, and stratigraphy of light-toned deposits within one trough of Noctis Labyrinthus, centered at -6.8 degrees N, 261.1 degrees E. CRISM spectra taken from light-toned layered deposits in the northern portion of the trough exhibit absorptions around 1.41, 1.92 and 2.21 gm, consistent with mixtures of opal and Al-clays that are exposed beneath younger lava flows and between high-standing mesas of chaotic terrain. In the southern portion of the trough, opal occurs as a patchy surficial deposit along the southwestern lower wall. Gypsum appears to be present in the southern portion of the trough where spectra show triplet absorptions at 1.44, 1.48, and 1.54 gm, and additional absorptions at 120, 1.74, 1.95, 2.22, 2.27, and 2.49 mu m. The gypsum-bearing materials consist of one to several beds that typically fill low-lying regions, including valleys. A bright mound on the trough floor exhibits spectral features at 1.43, 1.92 and 2.43 mu m, characteristic of polyhydrated sulfates. The bright mound appears distinct in morphology from chaotic terrain, and along its base are exposures of gypsum-bearing materials. Fluvial channels in the southwestern portion of the trough incise surface slopes at 4-6 degrees and lack obvious sources. The channels display first and second order tributaries arranged in a parallel pattern and may have formed by localized surface discharge from melting snow and/or ice. Both opal and gypsum occur in close proximity in the southwestern region of the trough, but gypsum is found alone in the southeast and opal in association with Al-clays is found to the northwest. We do not believe gypsum and opal formed coevally because they are not always found together, they require different aqueous conditions (i.e., opaline deposits require high silica availability while the gypsum deposits require high Ca availability in solution), and they appear at stratigraphically distinct levels. Although we identified evidence for fluvial landforms within the trough, cross-cutting relations indicate their incision post-dates deposition of the opal and pre-dates deposition of the gypsum. Hence, several periods of aqueous activity and alteration likely occurred within the trough from the Late Hesperian into the Amazonian that reflect favorable localized conditions within the Noctis Labyrinthus region and may be contemporaneous with late aqueous activity occurring elsewhere on Mars. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Weitz, Catherine M.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Bishop, Janice L.] SETI Inst, Mountain View, CA 94043 USA. [Grant, John A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. RP Weitz, CM (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA. EM weitz@psi.edu FU NASA [NNX11AH60G, JPL RSA 1433726] FX Funding for this project was provided by Grants from the NASA Mars Data Analysis Program (NNX11AH60G) and JPL RSA 1433726 for future Mars Landing Sites. We thank D. Berman for production of the HiRISE DTMs used in this study, and S. Purdy and C. Okubo for assistance with the Osiris software. The HRSC DTM is courtesy of HRSCview, Freie Universitaet Berlin and DLR Berlin, http:// hrscview.fu-berlin.de/. Comments provided by two anonymous reviewers are gratefully appreciated. This work could not have been accomplished without the dedicated efforts of the Mars Odyssey, Mars Reconnaissance Orbiter, and Mars Express teams. NR 88 TC 13 Z9 13 U1 3 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD OCT PY 2013 VL 87 BP 130 EP 145 DI 10.1016/j.pss.2013.08.007 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263LM UT WOS:000327810100013 ER PT J AU Nunez, L Sandoval, A Standen, VG Santoro, CM AF Nunez, Lautaro Sandoval, Abelardo Standen, Vivien G. Santoro, Calogero M. TI BETTY J. MEGGERS AND HER TRASCENDENTAL HEMISPHERIC DEDICATION TO LATIN AMERICAN ARCHAEOLOGY SO CHUNGARA-REVISTA DE ANTROPOLOGIA CHILENA LA Spanish DT Editorial Material ID CHILE C1 [Nunez, Lautaro] Univ Catolica Norte, Inst Invest Arqueol & Museo, San Pedro De Atacama, Chile. [Sandoval, Abelardo] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Standen, Vivien G.] Univ Tarapaca, Dept Antropol, Arica, Chile. [Santoro, Calogero M.] Univ Tarapaca, Inst Alta Invest, Arica, Chile. [Santoro, Calogero M.] Ctr Invest Hombre Desierto, Arica, Chile. RP Nunez, L (reprint author), Univ Catolica Norte, Inst Invest Arqueol & Museo, Calle Gustavo Le Paige S-N, San Pedro De Atacama, Chile. EM lautaro.nunez@hotmail.com; sandovaa@si.edu; vivien.standen@gmail.com; calogero_santoro@yahoo.com OI Santoro, Calogero M/0000-0002-3702-8408 NR 32 TC 1 Z9 1 U1 0 U2 3 PU UNIV TARAPACA PI ARICA PA CASILLA 6-D, ARICA, 1775, CHILE SN 0717-7356 J9 CHUNGARA JI Chungara PD OCT-DEC PY 2013 VL 45 IS 4 BP 505 EP 514 DI 10.4067/S0717-73562013000400001 PG 10 WC Anthropology SC Anthropology GA 254UU UT WOS:000327194400001 ER PT J AU Linse, K Griffiths, HJ Barnes, DKA Brandt, A Davey, N David, B De Grave, S d'Acoz, CD Eleaume, M Glover, AG Hemery, LG Mah, C Martin-Ledo, R Munilla, T O'Loughlin, M Pierrat, B Saucede, T Sands, CJ Strugnell, JM Enderlein, P AF Linse, Katrin Griffiths, Huw J. Barnes, Dave K. A. Brandt, Angelika Davey, Niki David, Bruno De Grave, Sammy d'Acoz, Cedric d'Udekem Eleaume, Marc Glover, Adrian G. Hemery, Lenaig G. Mah, Christopher Martin-Ledo, Rafael Munilla, Tomas O'Loughlin, Mark Pierrat, Benjamin Saucede, Thomas Sands, Chester J. Strugnell, Jan M. Enderlein, Peter TI The macro- and megabenthic fauna on the continental shelf of the eastern Amundsen Sea, Antarctica SO CONTINENTAL SHELF RESEARCH LA English DT Article DE Biodiversity; Abundance; Megabenthos; Southern Ocean; Pine Island ID PINE ISLAND GLACIER; SOUTH SHETLAND ISLANDS; WEST ANTARCTICA; BELLINGSHAUSEN SEA; ICE-SHEET; ROSS SEA; SEDIMENTARY PROCESSES; OCEAN; BIOGEOGRAPHY; COMMUNITIES AB In 2008 the BIOPEARL II expedition on board of RRS James Clark Ross sailed to the eastern Amundsen Sea Embayment and Pine Island Bay, one of the least studied Antarctic continental shelf regions due to its remoteness and ice cover. A total of 37 Agassiz trawls were deployed at depth transects along the continental and trough slopes. A total of 5469 specimens, belonging to 32 higher taxonomic groups and more than 270 species, were collected. Species richness per station varied from 1 to 55. The benthic assemblages were dominated by echinoderms and clearly different to those in the Ross, Scotia and Weddell seas. Here we present the macro- and megafaunal assemblage structure, its species richness and the presence of several undescribed species. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Linse, Katrin; Griffiths, Huw J.; Barnes, Dave K. A.; Sands, Chester J.; Enderlein, Peter] British Antarctic Survey, NERC, Cambridge CB3 0ET, England. [Brandt, Angelika] Univ Hamburg, Bioctr Grindel, D-20147 Hamburg, Germany. [Brandt, Angelika] Univ Hamburg, Zool Museum, D-20147 Hamburg, Germany. [Davey, Niki] Natl Inst Water & Atmosphere Res Ltd NIWA, Nelson, New Zealand. [David, Bruno; Pierrat, Benjamin; Saucede, Thomas] Univ Bourgogne, CNRS, UMR Biogeosci 6282, F-21000 Dijon, France. [De Grave, Sammy] Univ Oxford, Museum Nat Hist, Oxford OX1 3PW, England. [d'Acoz, Cedric d'Udekem] Museum Nat Sci, B-1000 Brussels, Belgium. [Eleaume, Marc; Hemery, Lenaig G.] Museum Natl Hist Nat, Dept Milieux & Peuplements Aquat, F-75005 Paris, France. [Glover, Adrian G.] Nat Hist Museum, Dept Zool, London SW7 5BD, England. [Mah, Christopher] Smithsonian Inst, Washington, DC 20013 USA. [Martin-Ledo, Rafael] Univ Extremadura, Fac Ciencias, Area Zool, Badajoz, Spain. [Munilla, Tomas] Univ Autonoma Barcelona, Zool Lab, E-08193 Barcelona, Spain. [O'Loughlin, Mark] Museum Victoria, Marine Biol Sect, Melbourne, Vic 3001, Australia. [Strugnell, Jan M.] La Trobe Univ, Sch Mol Sci, Dept Genet, Melbourne, Vic 3086, Australia. RP Linse, K (reprint author), British Antarctic Survey, NERC, Madingley Rd, Cambridge CB3 0ET, England. EM kl@bas.ac.uk RI Strugnell, Jan/P-9921-2016; OI De Grave, Sammy/0000-0002-2437-2445; Strugnell, Jan/0000-0003-2994-637X; Hemery, Lenaig/0000-0001-5337-4514 FU Natural Environment Research Council FX Thanks to Captain Jerry Burgan and his crew of RRS James Clark Ross for help and support on board and especially for getting us into Pine Island Bay. We are grateful to Dr Rob Larter and his team for swath support and to Dr Julian Gutt and two unknown reviewers for valuable comments on the manuscript. This study is part of the British Antarctic Survey Polar Science for Planet Earth Programme funded by The Natural Environment Research Council. NR 80 TC 4 Z9 6 U1 2 U2 19 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0278-4343 EI 1873-6955 J9 CONT SHELF RES JI Cont. Shelf Res. PD OCT 1 PY 2013 VL 68 BP 80 EP 90 DI 10.1016/j.csr.2013.08.012 PG 11 WC Oceanography SC Oceanography GA 254ML UT WOS:000327169700008 ER PT J AU Osborn, KJ Gebruk, AV Rogacheva, A Holland, ND AF Osborn, Karen J. Gebruk, Andrey V. Rogacheva, Antonina Holland, Nicholas D. TI An Externally Brooding Acorn Worm (Hemichordata, Enteropneusta, Torquaratoridae) from the Russian Arctic SO BIOLOGICAL BULLETIN LA English DT Article ID DEEP-SEA; KARA SEA; 18S RDNA; PHYLOGENETIC ANALYSES; MORPHOLOGY; ECHINODERMATA; SEQUENCES; POSITION; GENUS; WATER AB A single specimen of a previously undescribed acorn worm in the family Torquaratoridae was trawled from a bottom depth of about 350 m in the Kara Sea (Russian Arctic). The new species is the shallowest of the exclusively deep- sea torquaratorids found to date, possibly an example of high- latitude emergence. On the basis of ribosomal DNA sequences and morphology, the worm is described here as the holotype of Coleodesmium karaensis n. gen., n. sp. It is most similar in overall body shape to the previously described enteropneust genus Allapasus, but is uniquely characterized by a tubular component of the proboscis skeleton ensheathing the collar nerve cord. Additionally, within the proboscis, the sparseness of the musculature of C. karaensis clearly distinguishes it from the much more muscular members of Allapasus. The holotype is a female bearing about a dozen embryos on the surface of her pharyngeal region, each recessed within a shallow depression in the dorsal epidermis. The embryos, ranging from late gastrula to an early stage of coelom formation, are a little more than 1 mm in diameter and surrounded by a thin membrane. Each embryo comprises an external ectoderm of monociliated cells (not arranged in obvious ciliated bands) and an internal endo- mesoderm; the blastopore is closed. In the most advanced embryos, the anterior coelom is starting to constrict off from the archenteron. Coleodesmium karaensis is the first enteropneust (and indeed the first hemichordate) found brooding embryos on the surface of the mother's body. C1 [Osborn, Karen J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Gebruk, Andrey V.; Rogacheva, Antonina] Russian Acad Sci, PP Shirshov Oceanol Inst, Moscow 117997, Russia. [Holland, Nicholas D.] Univ Calif San Diego, Marine Biol Res Div, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Osborn, KJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. EM osbornk@si.edu OI Osborn, Karen/0000-0002-4226-9257 FU Russian foundation of Basic Research [12-05-33049] FX We are indebted to the crew of the R/V Akademik Mstislav Keldysh and to Sergey Galkin, Andrey Vedenin, Kirill Minin, and Tina Molodtsova for help with the dredging, sorting, and photography of the freshly collected worm. Greg Rouse kindly photographed the formalin-fixed specimen, and Linda Holland constructively criticized our manuscript. Matt Kweskin kindly facilitated use of the Smithsonian's Hydra cluster. This research was supported in part by the Russian foundation of Basic Research (grant number 12-05-33049). NR 42 TC 4 Z9 4 U1 0 U2 7 PU MARINE BIOLOGICAL LABORATORY PI WOODS HOLE PA 7 MBL ST, WOODS HOLE, MA 02543 USA SN 0006-3185 EI 1939-8697 J9 BIOL BULL-US JI Biol. Bull. PD OCT PY 2013 VL 225 IS 2 BP 113 EP 123 PG 11 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA 254PY UT WOS:000327178800006 PM 24243964 ER PT J AU Klimczak, C Ernst, CM Byrne, PK Solomon, SC Watters, TR Murchie, SL Preusker, F Balcerski, JA AF Klimczak, Christian Ernst, Carolyn M. Byrne, Paul K. Solomon, Sean C. Watters, Thomas R. Murchie, Scott L. Preusker, Frank Balcerski, Jeffrey A. TI Insights into the subsurface structure of the Caloris basin, Mercury, from assessments of mechanical layering and changes in long-wavelength topography SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Caloris basin; Mercury; Graben; Topographic undulations; Fault scaling; Mechanical stratigraphy ID LENGTH SCALING RELATIONS; SEGMENTED NORMAL FAULTS; 1ST MESSENGER FLYBY; LOBATE SCARPS; TERRESTRIAL PLANETS; OCEANIC LITHOSPHERE; DEFORMATION BANDS; PANTHEON FOSSAE; IMPACT CRATERS; SMOOTH PLAINS AB The volcanic plains that fill the Caloris basin, the largest recognized impact basin on Mercury, are deformed by many graben and wrinkle ridges, among which the multitude of radial graben of Pantheon Fossae allow us to resolve variations in the depth extent of associated faulting. Displacement profiles and displacement-to-length scaling both indicate that faults near the basin center are confined to a similar to 4-km-thick mechanical layer, whereas faults far from the center penetrate more deeply. The fault scaling also indicates that the graben formed in mechanically strong material, which we identify with dry basalt-like plains. These plains were also affected by changes in long-wavelength topography, including undulations with wavelengths of up to 1300 km and amplitudes of 2.5 to 3 km. Geographic correlation of the depth extent of faulting with topographic variations allows a first-order interpretation of the subsurface structure and mechanical stratigraphy in the basin. Further, crosscutting and superposition relationships among plains, faults, craters, and topography indicate that development of long-wavelength topographic variations followed plains emplacement, faulting, and much of the cratering within the Caloris basin. As several examples of these topographic undulations are also found outside the basin, our results on the scale, structural style, and relative timing of the topographic changes have regional applicability and may be the surface expression of global-scale interior processes on Mercury. C1 [Klimczak, Christian; Byrne, Paul K.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Ernst, Carolyn M.; Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Preusker, Frank] German Aerosp Ctr, Inst Planetary Res, Berlin, Germany. [Balcerski, Jeffrey A.] Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA. RP Klimczak, C (reprint author), Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd, Washington, DC 20015 USA. EM cklimczak@ciw.edu RI Ernst, Carolyn/I-4902-2012; Murchie, Scott/E-8030-2015 OI Murchie, Scott/0000-0002-1616-8751 FU NASA Discovery Program [NASW-00002, NAS5-97271] FX We thank the associate editor and two anonymous reviewers for helpful comments. CK also thanks Richard A. Schultz for sharing previously published work on confined fault growth. The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory. NR 88 TC 8 Z9 8 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD OCT PY 2013 VL 118 IS 10 BP 2030 EP 2044 DI 10.1002/jgre.20157 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 252RJ UT WOS:000327026900007 ER PT J AU Konstantinov, A Chamorro, ML Prathapan, KD Ge, SQ Yang, XK AF Konstantinov, Alexander Chamorro, Maria Lourdes Prathapan, K. D. Ge, Si-Qin Yang, Xing-Ke TI Moss-inhabiting flea beetles (Coleoptera: Chrysomelidae: Galerucinae: Alticini) with description of a new genus from Cangshan, China SO JOURNAL OF NATURAL HISTORY LA English DT Article DE moss; bryobionts; new genus; species; flea beetles; Asia ID SCHERER COLEOPTERA; SYNONYMY AB The world diversity of moss cushion-inhabiting and moss-feeding flea beetles is documented and discussed. A new genus (Cangshanaltica) with a single new species (Cangshanaltica nigra sp. nov.) from Yunnan Province in China is described and illustrated. It is similar to Benedictus Scherer, Ivalia Jacoby, Minota Weise, Paraminota Scherer, and Phaelota Jacoby. An identification key for all flea beetle genera known to occur in mosses in the eastern hemisphere is provided. C1 [Konstantinov, Alexander; Chamorro, Maria Lourdes] ARS, Systemat Entomol Lab, USDA, Smithsonian Inst,Natl Museum Nat Hist, Washington, DC USA. [Prathapan, K. D.] Kerala Agr Univ, Dept Entomol, Trivandrum, Kerala, India. [Ge, Si-Qin; Yang, Xing-Ke] Chinese Acad Sci, Inst Zool, Key Lab Zool Systemat & Evolut, Beijing, Peoples R China. RP Konstantinov, A (reprint author), ARS, Systemat Entomol Lab, USDA, Smithsonian Inst,Natl Museum Nat Hist, Washington, DC USA. EM alex.konstantinov@ars.usda.gov FU USDA, Forest Service, International Research Programs, Washington DC, USA; Indian Council of Agricultural Research Network Project on Insect Systematics; Kerala State Council for Science, Technology and Environment, Trivandrum FX We are grateful to D. Nelson (USDA, Forest Service, International Research Programs, Washington DC, USA) for partial funding for exploration in China. M. Volkovitsh (Zoological Institute, St Petersburg, Russia), Hongxia Xu (Institute of Zoology, Chinese Academy of Sciences, Beijing, China) and T. Petrice (USDA, Forest Service, Northern Research Station, MI, USA) are thanked for camaraderie and companionship during the 2011 explorations in China. M. Gates and A. Norrbom (Systematic Entomology Laboratory, Washington DC, USA), and C. Staines (Department of Entomology, Smithsonian Institution, Washington DC, USA) thoroughly reviewed earlier versions of this manuscript and provided valuable suggestions. We thank M. Buffington and M. Gates (Systematic Entomology Laboratory, Washington, DC) for their help with the digital cameras and image capture and editing. We are grateful to M. Nair (Department of Botany, Zamorin's Guruvayoorappan College, Kozhikode and the Malabar Botanic Garden, Calicut, Kerala, India) for identification of the moss samples from the gut of Cangshanaltica nigra. KDP is funded by the Indian Council of Agricultural Research Network Project on Insect Systematics and the Kerala State Council for Science, Technology and Environment, Trivandrum. Habitus illustration are the work of K. Arakawa (Ibaraki, Japan), A. N. Brown (USA), S. V. Edgerton (San Francisco CA), and E. Roberts (Systematic Entomology Laboratory, Washington DC, USA). USDA is an equal opportunity provider and employer. NR 16 TC 4 Z9 4 U1 1 U2 6 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 EI 1464-5262 J9 J NAT HIST JI J. Nat. Hist. PD OCT 1 PY 2013 VL 47 IS 37-38 BP 2459 EP 2477 DI 10.1080/00222933.2012.763068 PG 19 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 250QB UT WOS:000326866900005 ER PT J AU Gagne, RJ Doganlar, M AF Gagne, Raymond J. Doganlar, Mikdat TI A NEW SPECIES OF CELTICECIS (DTPTERA: CECIDOMYIIDAE) ON CELTIS CAUCASICA (CANNABACEAE) FROM TURKEY SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE gall midge; Palearctic; hackberries; Lasiopteridi AB A new species, Celticecis caucasicae Gagne, is described from leaf galls on Celtis caucasica Willd. found in southern Turkey. The new species, the first Celticecis known from the western Palearctic, is compared with previously described congeners. The leaf gall formed by this species affects a more extensive area of the leaf than do other Celticecis galls and the larval chamber uniquely remains open at its apex until sealed by the pupal cocoon. C1 [Gagne, Raymond J.] ARS, Systemat Entomol Lab, PSI, USDA, Washington, DC 20013 USA. [Doganlar, Mikdat] Mustefa Kemal Univ, Fac Agr, Dept Plant Protect, TR-34034 Antakya, Hatay, Turkey. RP Gagne, RJ (reprint author), ARS, Systemat Entomol Lab, PSI, USDA, C-O Smithsonian Inst MRC 168,POB 37012, Washington, DC 20013 USA. EM raymond.gagne@ars.usda.gov; doganlar@mku.edu.tr NR 2 TC 0 Z9 2 U1 1 U2 6 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 OCT PY 2013 VL 115 IS 4 BP 311 EP 315 DI 10.4289/0013-8797.115.4.311 PG 5 WC Entomology SC Entomology GA 251CB UT WOS:000326904300002 ER PT J AU Henry, TJ Perez-Gelabert, DE Steiner, WE Heiss, E AF Henry, Thomas J. Perez-Gelabert, Daniel E. Steiner, Warren E., Jr. Heiss, Ernst TI BRACHYRHYNCHUS MEMBRANACEUS (FABRICIUS), AN OLD WORLD FLAT BUG (HEMIPTERA: HETEROPTERA: ARADIDAE: MEZIRINAE) NEWLY DISCOVERED IN THE WESTERN HEMISPHERE SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE New World record; diagnosis; hosts; photographs AB The Old World aradid Brachyrhynchus membranaceus (Fabricius), belonging to the subfamily Mezirinae, is reported for the first time from the Western Hemisphere. Since 2005, eight specimens have been intercepted at United States ports-of-entry in international commerce from Costa Rica, Dominican Republic, Honduras, and Jamaica. Eventual study of specimens from the Bahamas, Costa Rica, Cuba, the Dominican Republic, and Panama allowed us to confirm that this flat bug is established in the New World. Diagnostic information and illustrations of the adult male and female are provided to help distinguish this Old World aradid from other New World Mezirinae. Host associations and habits are discussed. C1 [Henry, Thomas J.] Smithsonian Inst, Systemat Entomol Lab, Inst Plant Sci, ARS,USDA,Natl Museum Nat Hist, Washington, DC 20013 USA. [Perez-Gelabert, Daniel E.] Smithsonian Inst, Natl Museum Nat Hist, ITIS, Washington, DC 20013 USA. [Perez-Gelabert, Daniel E.; Steiner, Warren E., Jr.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Heiss, Ernst] Tiroler Landesmuseum, A-6020 Innsbruck, Austria. RP Henry, TJ (reprint author), Smithsonian Inst, Systemat Entomol Lab, Inst Plant Sci, ARS,USDA,Natl Museum Nat Hist, Washington, DC 20013 USA. EM thomas.henry@ars.usda.gov; perezd@si.edu; steinerw@si.edu; aradus@aon.at NR 31 TC 1 Z9 1 U1 1 U2 6 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 OCT PY 2013 VL 115 IS 4 BP 342 EP 348 DI 10.4289/0013-8797.115.4.342 PG 7 WC Entomology SC Entomology GA 251CB UT WOS:000326904300006 ER PT J AU Buffington, ML Condon, M AF Buffington, Matthew L. Condon, Marty TI THE DESCRIPTION AND BIONOMICS OF TROPIDEUCOILA BLEPHARONEURAE BUFFINGTON AND CONDON, NEW SPECIES (HYMENOPTERA: FIGITIDAE: ZAEUCOILINI), PARASITOID OF BLEPHARONEURA LOEW FRUIT FLIES (TEPHRITIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Peru; Gurania acuminata; Gurania spinulosus; Gurania lobata; host plant; parasitoid; phylogeny AB Tropideucoila blepharoneurae, a new species of Zaeucoilini, is described from Peru. Specimens were reared from numerous species of the tephritid genus Blepharoneura feeding on species of Gurania (Cucurbitaceae). Prior to the discovery of this species, it was hypothesized that species of Tropideucoila were restricted to Agromyzidae hosts; this new species is remarkable for its host association with Tephritidae. To support the inclusion of this new species in Tropideucoila, we performed a total evidence phylogenetic reconstruction of the Zaeucoilini; this new species was recovered (with strong branch support) within Tropideucoila. C1 [Buffington, Matthew L.] Smithsonian NMNH, Systemat Entomol Lab, USDA, Washington, DC 20013 USA. [Condon, Marty] Cornell Coll, Dept Biol, Mt Vernon, IA 52314 USA. RP Buffington, ML (reprint author), Smithsonian NMNH, Systemat Entomol Lab, USDA, 10th & Constitut Ave NW, Washington, DC 20013 USA. EM matt.buffington@ars.usda.gov; Mcondon@cornellcollege.edu FU NSF [NSF DEB-0330845, NSF DEB-0949361] FX We thank the Instituto Nacional de Recursos Naturales- Intendencia Forestal y de Fauna Silvestre del Peri for authorizing collections (Autorizacion No 110-2008-INRENA-IFFS-DCB) and exportation of specimens (Permiso No 011832-AG-INRENA). We are grateful for collaboration from Gerardo Lamas (Entomology) and Betty Millan (Herbarium) of the Muse de Historia Natural de la Universidad Nacional Mayor de San Marcos, and Eric Cosio of the Pontificia Universidad Catolica del Peru. We thank Luz Maria Huerto Santillan, Matthew Lewis, and Cornell College students for field assistance, and Sonja Scheffer and Matthew Lewis for molecular work. This research was supported in part by NSF grants to Condon: NSF DEB-0330845, NSF DEB-0949361. NR 9 TC 1 Z9 1 U1 0 U2 3 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2013 VL 115 IS 4 BP 349 EP 357 DI 10.4289/0013-8797.115.4.349 PG 9 WC Entomology SC Entomology GA 251CB UT WOS:000326904300007 ER PT J AU Buffington, ML Gates, MW AF Buffington, Matthew L. Gates, Michael W. TI THE DESCRIPTION OF PARAMBLYNOTUS DELANEYI (HYMENOPTERA: LIOPTERIDAE), A NEW SPECIES FROM JOSHUA TREE NATIONAL PARK SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Cynipoidea; zonatus; virginianus; Kiefferiella; desert AB A new species, Paramblynotus delaneyi, is described and characters separating it from the Nearctic species P. zonatus Weld and P. virginianus Liu are discussed. A discussion of the insect biodiversity survey at Joshua Tree National Park is provided. C1 [Buffington, Matthew L.; Gates, Michael W.] Smithsonian NMNH, Systemat Entomol Lab, USDA, Washington, DC 20013 USA. RP Buffington, ML (reprint author), Smithsonian NMNH, Systemat Entomol Lab, USDA, 10th & Constitut Ave NW, Washington, DC 20013 USA. EM matt.buffington@ars.usda.gov; michael.gates@ars.usda.gov NR 10 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 OCT PY 2013 VL 115 IS 4 BP 358 EP 368 DI 10.4289/0013-8797.115.4.358 PG 11 WC Entomology SC Entomology GA 251CB UT WOS:000326904300008 ER PT J AU Henry, TJ AF Henry, Thomas J. TI CYMAPAMPHANTUS VALENTINEORUM, A NEW GENUS AND SPECIES OF PAMPHANTINAE (HETEROPTERA: LYGAEOIDEA: GEOCORIDAE) FROM THE BRITISH VIRGIN ISLANDS, WITH A CHECKLIST OF THE SPECIES AND KEYS TO THE TRIBES AND GENERA OF THE SUBFAMILY SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Insecta; Hemiptera; Heteroptera; Geocoridae; Pamphantinae; new genus; new species; British Virgin Islands; Guana Island; keys; checklist ID HEMIPTERA HETEROPTERA; SOUTH-AMERICA; LYGAEIDAE; AUSTRALIA AB The new genus and new species Cymapamphantus valentineorum, belonging to the geocorid subfamily Pamphantinae, is described from one brachypterous male and six brachypterous females taken on Guana Island, British Virgin Islands. A dorsal habitus illustration, dorsal and lateral photographs of the male and female, diagnosis, and description of C. valentineorum are provided to help distinguish this new Caribbean bug from other New World pamphantines. A checklist of the species, keys to the three tribes and eight genera, and a color photograph of a representative species of each genus of the New World Pamphantinae are provided. C1 Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, ARS,USDA, Washington, DC 20013 USA. RP Henry, TJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, ARS,USDA, MRC 168, Washington, DC 20013 USA. EM thomas.henry@ars.usda.gov FU Falconwood Foundation, New York, NY FX I am grateful to Barry D. Valentine for donating his specimens of Cymapamphantus valentineorum to the National Museum of Natural History (USNM), Smithsonian Institution; Taina Litwak (SEL) for the habitus illustration; and Michele Touchet (SEL) for the color photographs. I also express thanks to James Lazell (The Conservation Agency [TCA], Jamestown, Rhode Island) for his invitation to participate in the faunal inventory of Guam. Island, Wenhua Lu (TCA) for access to island Malaise trap samples and other materials from 2007 to 2012, and Henry G. Jarecki (owner of Guana Island) and his family for their generous support and uncommon insight into understanding the importance of documenting the fauna of this species-rich island and its subsequent changes over time. Fieldwork for this study was funded in part by The Falconwood Foundation, New York, NY. I thank Pablo M. De nape (Museo de La Plata, La Plata, Argentina) and A. G. Wheeler, Jr. (Clemson University, Clemson, SC) for kindly reviewing the manuscript. NR 26 TC 4 Z9 4 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2013 VL 115 IS 4 BP 392 EP 401 DI 10.4289/0013-8797.115.4.392 PG 10 WC Entomology SC Entomology GA 251CB UT WOS:000326904300010 ER PT J AU O'Dea, A Collins, LS AF O'Dea, Aaron Collins, Laurel S. TI ENVIRONMENTAL, ECOLOGICAL, AND EVOLUTIONARY CHANGE IN SEAS ACROSS THE ISTHMUS OF PANAMA SO BULLETIN OF MARINE SCIENCE LA English DT Article ID ECOSYSTEMS; CLOSURE; SEAWAY AB This collection of 13 articles expands our knowledge of the historical and modern-day processes that have shaped tropical American seas. The articles deal with a wide range of topics and are brought together to stimulate collaborative research that breaks down the barriers among disciplines and time scales. Papers in this collection confront the recent challenge to the established age of the formation of the Isthmus of Panama, provide new methods that reveal marine paleoenvironments in the region, assess ecological and evolutionary events over deep time, and evaluate the pre-Columbian to modern-day influences of humans on Caribbean coasts of lower Central America. C1 [O'Dea, Aaron; Collins, Laurel S.] Smithsonian Trop Res Inst, Panama City, Panama. [Collins, Laurel S.] Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA. RP O'Dea, A (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Panama City, Panama. EM odeaa@si.edu FU MarineGEO; Smithsonian Tropical Research Institute; National System of Investigators (SNI) of Panama's National Secretariat for Science, Technology and Innovation (SENACYT) FX We are indebted to the authors for their significant contributions and all those that served as reviewers, providing essential critiques. JBC Jackson and AG Coates and all members of the Panama Paleontology Project laid the foundations to this and future work. The Smithsonian Marine Science Network (now MarineGEO) and the Smithsonian Tropical Research Institute financially supported the colloquium and the publication of this volume. AO was supported by the National System of Investigators (SNI) of Panama's National Secretariat for Science, Technology and Innovation (SENACYT). This is contribution number 264 to The Program in Tropical Biology at Florida International University. NR 39 TC 0 Z9 0 U1 3 U2 13 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD OCT PY 2013 VL 89 IS 4 BP 769 EP 777 DI 10.5343/bms.2013.1018 PG 9 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 246RD UT WOS:000326555900002 ER PT J AU Jackson, JBC O'Dea, A AF Jackson, Jeremy B. C. O'Dea, Aaron TI TIMING OF THE OCEANOGRAPHIC AND BIOLOGICAL ISOLATION OF THE CARIBBEAN SEA FROM THE TROPICAL EASTERN PACIFIC OCEAN SO BULLETIN OF MARINE SCIENCE LA English DT Article ID AMERICAN BIOTIC INTERCHANGE; PANAMA LAND-BRIDGE; BODY-SIZE; ENVIRONMENTAL-CHANGE; SOUTH-AMERICA; CUPULADRIID BRYOZOANS; NEOGENE CUPULADRIIDAE; CHEILOSTOME BRYOZOA; REEF DEVELOPMENT; OPPOSITE SIDES AB Geological uplift along the Central American Arc began in the Eocene with extensive development of emergent terrains by the early Miocene. Nevertheless, three independent lines of evidence are consistent with abundant seawater exchange between the oceans until about 4.7-3 Ma. (1) Isotopic and sedimentary data from ocean cores demonstrate that divergence in surface salinity and deep-sea carbonate accumulation between the Caribbean and eastern Pacific did not occur until 4.7-4.2 Ma. Moreover, strong upwelling comparable to the Pacific today persisted in Caribbean shelf environments until 4.5-3.5 Ma. (2) North and South American terrestrial mammals and tropical forest bird faunas remained overwhelmingly isolated until about 3 Ma. Some birds flew across the seaway and numerous small amphibians and plants began mixing millions of years earlier as expected due to their high probability of rafting. The rarity and ambiguity of reported exceptions to these result after a century of intensive sampling strengthen the general pattern. (3) Bathyal foraminifera first separated across the developing Isthmus approximately 13 Ma but numerous mollusks and cheilostomes are known from both oceans until the Middle Pliocene. Some species now restricted to the Pacific persisted in the Caribbean until the Pleistocene, but no species known to have originated after the Early Pliocene occurs in both oceans except for dispersal by shorebirds or human introductions. Molecular clock estimates for the timing of divergence of taxa strongly support these patterns. Isolation of the Caribbean from the Pacific about 3 Ma provides a robust model system for the study of vicariance in the oceans. C1 [Jackson, Jeremy B. C.; O'Dea, Aaron] Smithsonian Trop Res Inst, Panama City, Panama. [Jackson, Jeremy B. C.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Jackson, JBC (reprint author), Smithsonian Inst, Dept Paleobiol, POB 30172,MRC 121, Washington, DC 20013 USA. EM jeremybcjackson@gmail.com FU NSF [0921924]; National System of Investigators (SNI) of the National Research Secretariat for Science, Technology, and Innovation of Panama (SENACYT) FX We thank T Coates and N Knowlton for valuable discussions and the entire Panama Paleontology Project team over the past 25 yrs for their innumerable contributions and support. JBCJ was supported by NSF Grant 0921924. AO was supported by the National System of Investigators (SNI) of the National Research Secretariat for Science, Technology, and Innovation of Panama (SENACYT). NR 124 TC 25 Z9 26 U1 1 U2 40 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD OCT PY 2013 VL 89 IS 4 BP 779 EP 800 DI 10.5343/bms.2012.1096 PG 22 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 246RD UT WOS:000326555900003 ER PT J AU Tao, K Robbins, JA Grossman, EL O'Dea, A AF Tao, Kai Robbins, John A. Grossman, Ethan L. O'Dea, Aaron TI QUANTIFYING UP WELLING AND FRESHENING IN NEARSHORE TROPICAL AMERICAN ENVIRONMENTS USING STABLE ISOTOPES IN MODERN GASTROPODS SO BULLETIN OF MARINE SCIENCE LA English DT Article ID BOCAS-DEL-TORO; WATER TEMPERATURE; SHELL CARBONATE; EASTERN PACIFIC; SURFACE WATERS; CARIBBEAN SEA; MOLLUSK SHELL; PANAMA; OCEAN; ISTHMUS AB To identify and quantify upwelling and freshwater influences in contrasting tropical ecosystems, we performed stable isotope analyses (delta C-13 and delta O-18) on 13 serially-sampled modern Conus shells collected from coastal waters in the southwestern Caribbean (SWC, non-upwelling) and gulfs of Chiriqui (non-upwelling) and Panama (upwelling) in the tropical eastern Pacific (TEP). Most shells reveal seasonal variations in temperature and/or seawater delta O-18 in their delta O-18 profiles. Unusually high or low seasonal delta O-18 values measure the intensity of seasonal upwelling or freshwater input, respectively. To quantify upwelling and freshening signals, baseline delta O-18 values free of seasonal upwelling and freshening have been calculated from average temperatures during rainy (non-upwelling) seasons and average salinities during dry (upwelling) seasons. Baseline-normalized delta O-18 profiles reveal little or no upwelling in the SWC and Gulf of Chiriqui, and strong upwelling in the Gulf of Panama, as well as strong freshwater input in most areas. Dry-season delta O-18 values for Gulf of Panama Conus can exceed the baseline by as much as 2 parts per thousand, equivalent to seawater temperatures approximately 9 degrees C lower than normal. In contrast, rainy-season delta O-18 values can be as low as 1.8 parts per thousand below the baseline, equivalent to salinities approximately 7 units lower than dry-season values. We use shell delta O-18 range (Delta O-18) and delta O-18-delta C-13 (O-C) correlation to further identify upwelling and freshening environments and thus nutrient source and status. Eutrophic environments like the Gulf of Panama are characterized by high Delta O-18 (2.3 parts per thousand 0-3.2 parts per thousand) and little O-C correlation. In contrast, the oligotrophic environments of the SWC lead to low (0.4 parts per thousand) to moderate (1.6 parts per thousand) Delta O-18 and non-significant to positive O-C correlation. When applied to fossil shells, these methods can characterize the nutrient status of ancient ecosystems. C1 [Tao, Kai; Robbins, John A.; Grossman, Ethan L.] Texas A&M Univ, Dept Geol & Geophys, College Stn, TX 77843 USA. [O'Dea, Aaron] Smithsonian Trop Res Inst, Balboa, Panama. RP Grossman, EL (reprint author), Texas A&M Univ, Dept Geol & Geophys, College Stn, TX 77843 USA. EM e-grossman@tamu.edu FU Smithsonian Tropical Research Institution; Michel T Halbouty Chair in Geology; Michel T Halbouty Visiting Post-doctoral Fellowship; National System of Investigators (SNI) of the National Secretariat for Science, Technology and Innovation of Panama (SENACYT); US National Science Foundation [EAR-0345471] FX We thank J Morales and R Thompson for perseverance in sampling waters over many months, F Rodriquez for shell identification, and T Duda for specimens. We also thank three anonymous reviewers and guest editor L Collins for their constructive comments. The study was supported a short-term fellowship from the Smithsonian Tropical Research Institution, the Michel T Halbouty Chair in Geology, the Michel T Halbouty Visiting Post-doctoral Fellowship, the National System of Investigators (SNI) of the National Secretariat for Science, Technology and Innovation of Panama (SENACYT), and the US National Science Foundation (EAR-0345471). NR 59 TC 12 Z9 12 U1 2 U2 13 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD OCT PY 2013 VL 89 IS 4 BP 815 EP 835 DI 10.5343/bms.2012.1065 PG 21 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 246RD UT WOS:000326555900005 ER PT J AU Key, MM Hollenbeck, PM O'Dea, A Patterson, WP AF Key, Marcus M., Jr. Hollenbeck, Paige M. O'Dea, Aaron Patterson, William P. TI STABLE ISOTOPE PROFILING IN MODERN MARINE BRYOZOAN COLONIES ACROSS THE ISTHMUS OF PANAMA SO BULLETIN OF MARINE SCIENCE LA English DT Article ID BOCAS-DEL-TORO; EASTERN TROPICAL PACIFIC; HIGH-RESOLUTION OXYGEN; CUPULADRIID BRYOZOANS; TEMPERATURE-VARIATION; WATER TEMPERATURE; EARLY HOLOCENE; GROWTH; CARBON; SEA AB In the tropics, upwelling of cold, deep water is the principal source of major seasonal fluctuations in temperature. Along the tropical eastern Pacific (TEP) coast of the Isthmus of Panama, seasonal upwelling induces corresponding drops in temperature. Upwelling does not occur along the southwestern Caribbean (SWC) coast of the isthmus. Our goal was to use these oceanographic differences to test the use of stable isotope profiles of free-living modern cupuladriid bryozoans as a method for quantifying paleo-seasonality. We determined O and C stable isotope values from micromilled carbonates profiled along the growth axis in three colonies of Cupuladria exfragminis Herrera-Cubilla, Dick, Sanner and Jackson, 2006 from the upwelling Gulf of Panama in TEP and three colonies of Cupuladria surinamensis Cadee, 1975 from the non-upwelling Bocas del Toro Archipelago in SWC. Pacific colonies had inter-colony delta O-18(carb) values ranging from -2.1 parts per thousand to -0.2 parts per thousand on the international Vienna Pee Dee Belemnite scale, whereas SWC colonies ranged from -1.7 parts per thousand to -0.6 parts per thousand. Pacific colonies consistently reveal cyclical trends in delta O-18(carb) that are absent in the Caribbean colonies. Based on published measurements of temperature, salinity, and delta O-18(sw), the <= 2.5 yrs of cyclicity seen in the Pacific colonies reflects a combination of seasonal freshening and seasonal upwelling of colder water. This preliminary study suggests the potential for more exploration of bryozoans as a source of paleoclimate proxies. C1 [Key, Marcus M., Jr.; Hollenbeck, Paige M.] Dickinson Coll, Dept Earth Sci, Carlisle, PA 17013 USA. [O'Dea, Aaron] Smithsonian Trop Res Inst, Panama City, Panama. [Patterson, William P.] Univ Saskatchewan, Dept Geol Sci, Saskatoon, SK S7N 5E2, Canada. RP Key, MM (reprint author), Dickinson Coll, Dept Earth Sci, POB 1773, Carlisle, PA 17013 USA. EM key@dickinson.edu OI Patterson, William/0000-0003-3387-708X FU National System of Investigators (SNI) of the National Research of the National Secretariat for Science, Technology and Innovation of Panama (SENACYT); National Science Foundation [EAR03-45471]; National Geographic Society; NASA; Dickinson College Research and Development Committee FX R Collin, A Herrera-Cubilla, H Fortunato, B de Gracia, and F Rodriguez (Smithsonian Tropical Research Institute, Panama) helped with collecting and curating specimens. L Key (University of Dallas) and R Dean (Dickinson College) helped with imaging colonies. C Alexander and R Bowden (Carnegie Institution of Washington) helped with micromilling. D Besic (University of Saskatchewan Isotope Laboratory) helped with analyzing isotopes. R Rossi (Dickinson College) helped with drafting figures. K Tao (Texas A&M University) shared his oceanographic data. Funding for M Key's field work was provided by the Dickinson College Research and Development Committee. The National System of Investigators (SNI) of the National Research of the National Secretariat for Science, Technology and Innovation of Panama (SENACYT), the National Science Foundation (EAR03-45471) and the National Geographic Society gave financial support to A O'Dea. Funding for isotope analyses was provided by a NASA Cool Climate Grant to M Key from the Dickinson College Center for Sustainability Education. Helpful comments by L Collins (Florida International University) and three anonymous reviewers greatly improved this manuscript. NR 86 TC 3 Z9 3 U1 1 U2 10 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD OCT PY 2013 VL 89 IS 4 BP 837 EP 856 DI 10.5343/bms.2012.1056 PG 20 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 246RD UT WOS:000326555900006 ER PT J AU Leonard-Pingel, JS Jackson, JBC AF Leonard-Pingel, Jill S. Jackson, Jeremy B. C. TI DRILLING INTENSITY VARIES AMONG NEOGENE TROPICAL AMERICAN BIVALVIA IN RELATION TO SHELL FORM AND LIFE HABIT SO BULLETIN OF MARINE SCIENCE LA English DT Article ID FOSSIL RECORD; ENVIRONMENTAL-CHANGE; MASS EXTINCTION; COASTAL-PLAIN; PREDATION; GASTROPODS; EVOLUTION; ESCALATION; EPIBIONTS; BRYOZOANS AB We calculated the incidence of drilling on bivalve genera from the Neogene fossil record of Panama and Costa Rica to determine differences in predation intensity among groups based on shell architecture, life habit, mobility, and taxonomic affinity. Bulk samples from 28 localities yielded >106,000 bivalve specimens, which were examined for characteristic drilling traces of muricid and naticid gastropods. We calculated the drilling intensity for the 90 most common genera, and characterized the size, ornament, life habit, and mobility for each genus. Large size confers considerable protection from drilling, but shell ornamentation does not. Life habit is strongly linked with drilling intensity. Epifaunal bivalves experience higher predation than infaunal bivalves and shallow burrowers experience higher drilling than deep burrowers. Mobility is also important for epifaunal bivalves; cemented taxa are twice as likely to be drilled as their uncemented counterparts. Our results suggest that bivalve behavior and life habits are more important than shell architecture for defense against drilling predators. C1 [Leonard-Pingel, Jill S.; Jackson, Jeremy B. C.] Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, La Jolla, CA 92093 USA. [Leonard-Pingel, Jill S.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Jackson, Jeremy B. C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Jackson, Jeremy B. C.] Smithsonian Trop Res Inst, Balboa, Panama. RP Leonard-Pingel, JS (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, La Jolla, CA 92093 USA. EM jleonardpingel@uchicago.edu NR 49 TC 9 Z9 9 U1 0 U2 10 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD OCT PY 2013 VL 89 IS 4 BP 905 EP 919 DI 10.5343/bms.2012.1058 PG 15 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 246RD UT WOS:000326555900009 ER PT J AU Smith, CJ Collins, LS Hayek, LAC AF Smith, Carly J. Collins, Laurel S. Hayek, Lee-Ann C. TI BIOGEOGRAPHIC EFFECTS OF THE CLOSING CENTRAL AMERICAN SEAWAY ON BENTHIC FORAMINIFERA OF VENEZUELA SO BULLETIN OF MARINE SCIENCE LA English DT Article ID BOCAS-DEL-TORO; SOUTH-AMERICA; LATE MIOCENE; FAUNAL SIMILARITY; WATER CIRCULATION; ISOTOPE RECORD; WESTERN PANAMA; NEOGENE; CLOSURE; ATLANTIC AB Studies of the effects of the Central American Seaway's closure on microfossil taxa and stable isotopes of foraminifera previously addressed the timing of emplacement of the Caribbean tropical eastern Pacific sill, changes in marine nutrients, evolutionary and paleobiogeographic events associated with closure, and rates of uplift in Central America. However, there have been no quantitative studies of the transisthmian divergence of whole biotas. Here we assess biogeographic effects of the closing Central American Seaway by comparing middle Miocene to Pliocene, neritic benthic foraminiferal assemblages from Falcon State, Venezuela, to those of coeval deposits with similar paleoenvironments from Panama, Costa Rica, and Ecuador. Benthic foraminiferal assemblages from the Urumaco, Codore, Caujarao; and La Vela formations of Venezuela's central coast were compared to other Caribbean and tropical eastern Pacific assemblages with Simpson's, Dice, and Jaccard similarity coefficients. Results of the Simpson's Coefficient indicate that the Caribbean inner neritic faunas of Venezuela, Costa Rica, and Panama became significantly more similar from the late Miocene to Pliocene, as mixing with Pacific waters was reduced and modern oceanic conditions of the Caribbean Sea were established. C1 [Smith, Carly J.; Collins, Laurel S.] Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA. [Collins, Laurel S.] Smithsonian Trop Res Inst, Panama City, Panama. [Hayek, Lee-Ann C.] NMNH, Smithsonian Inst, Washington, DC 20013 USA. RP Collins, LS (reprint author), Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA. EM collinsl@fiu.edu FU Smithsonian Tropical Research Institute FX O Aguilera, Universidad Nacional Experimental Francisco de Miranda in Coro, Venezuela, graciously hosted our Venezuela fieldwork; C Jaramillo and the Smithsonian Tropical Research Institute generously provided the funds. Geological guidance in the field by LI Quiroz, S Moron, and R Sanchez was invaluable. We thank the two anonymous reviewers and A O'Dea for their helpful comments. This publication is contribution no. 262 to The Program in Tropical Biology of Florida International University. NR 62 TC 2 Z9 2 U1 3 U2 14 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD OCT PY 2013 VL 89 IS 4 BP 921 EP 936 DI 10.5343/bms.2013.1006 PG 16 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 246RD UT WOS:000326555900010 ER PT J AU Cramer, KL AF Cramer, Katie L. TI HISTORY OF HUMAN OCCUPATION AND ENVIRONMENTAL CHANGE IN WESTERN AND CENTRAL CARIBBEAN PANAMA SO BULLETIN OF MARINE SCIENCE LA English DT Article ID BOCAS-DEL-TORO; MAJOR OIL-SPILL; CORAL-REEFS; POPULATION CHARACTERISTICS; CONSERVATION STATUS; CONTINENTAL REEFS; CENTRAL-AMERICA; PHASE-SHIFTS; SITIO DRAGO; COAST AB Humans have altered terrestrial and marine coastal environments in Central America through land clearing and fishing for over 10,000 yrs. The intensity of human disturbance has been strongly influenced by local physiographic and climatic conditions that affect the productivity of the land and sea. The importance of these factors is readily apparent along the Caribbean coast of Panama. Environmental conditions have played an important role in the differing histories of population and environmental disturbance in Bocas del Toro along the western coast and Costa Arriba de Colon (Costa Arriba) along the central coast. Both regions suffered catastrophic mortality of indigenous peoples soon after European contact and did not return to pre-contact levels until at least the 19th century. During the Spanish colonial era, Bocas del Toro remained relatively sparsely populated until the early 20th century due to its isolation from the Pacific by high mountains, excessive rainfall, and relatively smaller area of alluvial flood plains for human habitation and agriculture. In contrast, the low-lying topography of Costa Arriba was conducive to early colonial occupation in the 16th century and rapid population growth and environmental disturbance since the mid-19th century. This earlier onset of intense human disturbance is likely responsible for the more degraded state of coral reefs in Costa Arriba compared to Bocas del Toro. The timeline of human interaction with the coastal environment of Caribbean Panama thus provides a deeper-time perspective from which to more accurately assess the causes of the recently observed collapse of Caribbean coral reefs. C1 [Cramer, Katie L.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Cramer, KL (reprint author), Natl Museum Nat Hist, Smithsonian Inst, 10th & Constitut Ave NW, Washington, DC 20560 USA. EM katie.cramer@gmail.com FU National Science Foundation Integrative Graduate Education and Research Traineeship (IGERT) Fellowship; Smithsonian Institution Predoctoral Fellowship; Center for Marine Biodiversity and Conservation Fellowship of Scripps Institution of Oceanography FX I wish to thank J Jackson for assistance with developing, refining, and editing the paper, A Spalding and R Cooke for assistance with identifying and obtaining historical references, J Cortes, S Heckadon Moreno, and T Wake for their helpful suggestions for improving the paper, and A O'Dea for the invitation to participate in the colloquium on ecological and evolutionary change in tropical American seas over broad time-scales. This work was supported by a National Science Foundation Integrative Graduate Education and Research Traineeship (IGERT) Fellowship, Smithsonian Institution Predoctoral Fellowship, and Center for Marine Biodiversity and Conservation Fellowship of Scripps Institution of Oceanography. NR 102 TC 12 Z9 12 U1 4 U2 43 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD OCT PY 2013 VL 89 IS 4 BP 955 EP 982 DI 10.5343/bms.2012.1028 PG 28 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 246RD UT WOS:000326555900012 ER PT J AU Fredston-Hermann, AL O'Dea, A Rodriguez, F Thompson, WG Todd, JA AF Fredston-Hermann, Alexa L. O'Dea, Aaron Rodriguez, Felix Thompson, William G. Todd, Jonathan A. TI MARKED ECOLOGICAL SHIFTS IN SEAGRASS AND REEF MOLLUSCAN COMMUNITIES SINCE THE MID-HOLOCENE IN THE SOUTHWESTERN CARIBBEAN SO BULLETIN OF MARINE SCIENCE LA English DT Article ID BOCAS-DEL-TORO; GREAT-BARRIER-REEF; CORAL-REEFS; DEATH ASSEMBLAGES; ENVIRONMENTAL-CHANGE; EASTERN PACIFIC; PHASE-SHIFTS; WEST-INDIES; PANAMA; ECOSYSTEMS AB Caribbean coastal ecosystems have undergone severe degradation both historically and recently, primarily caused by the synergistic effects of overfishing, eutrophication, sedimentation, disease, and other factors associated with humans. Baseline conditions from pristine Caribbean reefs and seagrass beds are required to understand and quantify degradation. Only the fossil record can provide pre-human baselines. We present preliminary results from a recently discovered mid-Holocene (7.2-5.7 ka) fossil fringing reef and seagrass system in Bocas del Toro, Panama. Molluscan assemblages from the fossil reef and seagrass habitats were compared to death assemblages in corresponding modern habitats. The proportion of suspension-feeding molluscs more than doubled from fossil to the present day in the reef habitat, and the proportion of herbivores declined by a third, reflecting declines in coral cover and architecture, and increased eutrophy. Conversely, in seagrass beds, the proportion of different mollusc guilds was remarkably similar between fossil and modern day, suggesting that unlike reefs, seagrass beds are functionally similar today compared to a "pristine" baseline, although key community members were different. Our study reveals novel evidence that the health of molluscan communities on Caribbean reefs may have declined to the extent observed in corals and fish, and that the decline follows a trajectory predicted by known ecosystem degradation. Molluscs represent a biodiverse and functionally crucial component of reefs and must be considered in ecosystem-scale research on reef conservation. Revealing the structure of baseline communities using the fossil record represents one important step toward this aim. C1 [Fredston-Hermann, Alexa L.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [O'Dea, Aaron; Rodriguez, Felix] Smithsonian Trop Res Inst, Balboa, Panama. [Thompson, William G.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. [Todd, Jonathan A.] Nat Hist Museum, Dept Earth Sci, London SW7 5BD, England. RP O'Dea, A (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Panama. EM aaronodea@gmail.com OI Fredston-Hermann, Alexa/0000-0002-5449-7054; Todd, Jonathan/0000-0002-0433-1611 FU Smithsonian Tropical Research Institute's Academic Programs; Princeton Environmental Institute; Department of Ecology and Evolutionary Biology at Princeton University; National System of Investigators (SNI) of the National Research of the National Secretariat for Science, Technology and Innovation of Panama (SENACYT) FX We thank B de Gracia, G Jacome, P Gondola, A Bilgray, U Gonzalez, and M Lukowiak for their valuable assistance with this project at STRI, and KL Cramer for her comments on the manuscript. M Aardema and S Rabin at Princeton offered advice on statistics, along with many members of the Pacala lab. We thank MA Kosnik, an anonymous reviewer and guest editor L Collins for their useful feedback. This research was generously supported by an internship from the Smithsonian Tropical Research Institute's Academic Programs, the Princeton Environmental Institute, and the Department of Ecology and Evolutionary Biology at Princeton University to Fredston-Hermann. The National System of Investigators (SNI) of the National Research of the National Secretariat for Science, Technology and Innovation of Panama (SENACYT) supported A O'Dea. NR 80 TC 5 Z9 5 U1 0 U2 24 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD OCT PY 2013 VL 89 IS 4 BP 983 EP 1002 DI 10.5343/bms.2012.1077 PG 20 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 246RD UT WOS:000326555900013 ER PT J AU Schloder, C O'Dea, A Guzman, HM AF Schloeder, Carmen O'Dea, Aaron Guzman, Hector M. TI BENTHIC COMMUNITY RECOVERY FROM SMALL-SCALE DAMAGE ON MARGINAL CARIBBEAN REEFS: AN EXAMPLE FROM PANAMA SO BULLETIN OF MARINE SCIENCE LA English DT Article ID BOCAS-DEL-TORO; CORAL-REEFS; PHASE-SHIFTS; ALTERNATIVE STATES; GROUNDING SITES; CLIMATE-CHANGE; STABLE STATES; ECOSYSTEMS; CONSERVATION; DISTURBANCE AB The frequency of small-scale physical damage to coral reefs is likely to increase as fishing and tourism pressures intensify. Predicting how reefs will respond to the effects of these types of damage requires empirical exploration, especially on reefs that are already heavily degraded. We replicated small-scale damage on four reefs that live close to their ecophysiological tolerance limits in the Bocas del Toro Archipelago of Caribbean Panama and quantified their recovery over 2 yrs. On each reef we cleared five replicate 1 x 1-m plots of all living benthos simulating physical damage by boat grounding, anchoring, or fishing practices. Recovery of the benthic community was quantitatively monitored and compared to adjacent non-cleared plots (treated as a control) every 6 mo. After 2 yrs, only one of the reefs exhibited evidence of recovery of the cleared plots. Poor recruitment of benthos appeared to slow down recovery of cleared plots on another reef. The other two reefs showed unequivocal shifts toward a macroalgae-dominated system, suggesting that small-scale disturbances could have lasting impacts on marginal reefs. We found no clear contemporary or historical environmental signal that could explain the differential dynamics of recovery amongst these reefs. C1 [Schloeder, Carmen; O'Dea, Aaron; Guzman, Hector M.] Smithsonian Trop Res Inst, Panama City, Panama. RP Schloder, C (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM schloederc@si.edu FU U Saint-Paul (ZMT); German Academic Exchange Service (DAAD); Smithsonian Tropical Research Institute (STRI); National Research System (SNI) of the National Secretariat of Science, Technology and Innovation (SENACYT) of Panama FX The authors are grateful to U Saint-Paul (ZMT) for his support to CS; A Castillo, A Laurence, M Salazar, E Toth, C Guevara, and G Jacome for field assistance; the Bocas del Toro Research Station staff for their support; T Smith, R Cipriani, and T Davidson for comments on earlier versions of the manuscript; the anonymous reviewers for their invaluable comments; the Smithsonian Tropical Research Institute for providing facilities; the German Academic Exchange Service (DAAD) and the Smithsonian Tropical Research Institute (STRI) for funding this study. AO would like to thank the National Research System (SNI) of the National Secretariat of Science, Technology and Innovation (SENACYT) of Panama for financial support. NR 55 TC 1 Z9 1 U1 2 U2 26 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD OCT PY 2013 VL 89 IS 4 BP 1003 EP 1013 DI 10.5343/bms.2012.1075 PG 11 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 246RD UT WOS:000326555900014 ER PT J AU O'Keefe, JMK Bechtel, A Christanis, K Dai, SF DiMichele, WA Eble, CF Esterle, JS Mastalerz, M Raymond, AL Valentim, BV Wagner, NJ Ward, CR Hower, JC AF O'Keefe, Jennifer M. K. Bechtel, Achim Christanis, Kimon Dai, Shifeng DiMichele, William A. Eble, Cortland F. Esterle, Joan S. Mastalerz, Maria Raymond, Anne L. Valentim, Bruno V. Wagner, Nicola J. Ward, Colin R. Hower, James C. TI On the fundamental difference between coal rank and coal type SO INTERNATIONAL JOURNAL OF COAL GEOLOGY LA English DT Review DE Rank; Type; Maceral; Depositional environment; Coalification; Geochemistry ID PALEOZOIC ICE-AGE; COPROPHILOUS FUNGUS SUCCESSION; ELECTRON-MICROPROBE ANALYSIS; NORTHERN APPALACHIAN BASIN; VOLATILE BITUMINOUS COALS; PLANT ANIMAL INTERACTIONS; TROPICAL PEAT DEPOSITS; MARITZA-EAST LIGNITE; BLACK-WARRIOR BASIN; WHITE-ROT FUNGI AB This article addresses the fundamental difference between coal rank and coal type. While theoretically settled long ago as being different aspects of coal systems science, the two concepts are still often confounded. In recent years, this has resulted in the publication of several works stating that coal type changes with coal rank. Coal type refers solely to coals' depositional origin and the maceral mineral admixture resulting from that origin. Coal types typically fall in to two categories: humic coals, developed from peat, and sapropelic coals, developed from organic mud. Either type may be allocthonous or autochthonous, and within types, further refinement of depositional environment can be made. Coal rank refers to the changes in geochemistry and resultant changes in reflectance caused by increasing thermal maturity of the coal. Thus, it provides an overprint of maturity on existing coal types. With proper techniques, such as use of crossed polars and etching, maceral forms can be differentiated even at high ranks, and the original coal type determined. (C) 2013 Elsevier B.V. All rights reserved. C1 [O'Keefe, Jennifer M. K.] Morehead State Univ, Dept Earth & Space Sci, Morehead, KY 40351 USA. [Bechtel, Achim] Montan Univ, Dept Appl Geosci & Geophys, Leoben, Austria. [Christanis, Kimon] Univ Patras, Dept Geol, Rion 26504, Greece. [Dai, Shifeng] China Univ Min & Technol, State Key Lab Coal Resources & Safe Min, Beijing 100083, Peoples R China. [DiMichele, William A.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Eble, Cortland F.] Univ Kentucky, Kentucky Geol Survey, Lexington, KY 40506 USA. [Esterle, Joan S.] Univ Queensland, Sch Earth Sci, Brisbane, Qld 4072, Australia. [Mastalerz, Maria] Indiana Univ, Indiana Geol Survey, Bloomington, IN 47405 USA. [Raymond, Anne L.] Dept Geol & Geophys, College Stn, TX 77843 USA. [Valentim, Bruno V.] Univ Porto, Dept Geosci Environm & Spatial Planning, Fac Sci, P-4169007 Oporto, Portugal. [Valentim, Bruno V.] Univ Porto, Geol Ctr, P-4169007 Oporto, Portugal. [Wagner, Nicola J.] Univ Witwatersrand, Sch Chem & Met Engn, ZA-2050 Johannesburg, South Africa. [Ward, Colin R.] Univ New S Wales, Sch Biol Earth & Environm Sci, Sydney, NSW, Australia. [Hower, James C.] Univ Kentucky, Ctr Appl Energy Res, Lexington, KY 40511 USA. RP O'Keefe, JMK (reprint author), Morehead State Univ, Dept Earth & Space Sci, Morehead, KY 40351 USA. EM j.okeefe@moreheadstate.edu RI Dai, Shifeng/K-1531-2014; OI Dai, Shifeng/0000-0002-9770-1369; Valentim, Bruno/0000-0002-1463-9126; Ward, Colin/0000-0001-7945-5777 NR 537 TC 45 Z9 45 U1 9 U2 52 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-5162 EI 1872-7840 J9 INT J COAL GEOL JI Int. J. Coal Geol. PD OCT 1 PY 2013 VL 118 BP 58 EP 87 DI 10.1016/j.coal.2013.08.007 PG 30 WC Energy & Fuels; Geosciences, Multidisciplinary SC Energy & Fuels; Geology GA 246SU UT WOS:000326560200006 ER PT J AU Hao, H Elvis, M Bongiorno, A Zamorani, G Merloni, A Kelly, BC Civano, F Celotti, A Ho, LC Jahnke, K Comastri, A Trump, JR Mainieri, V Salvato, M Brusa, M Impey, CD Koekemoer, AM Lanzuisi, G Vignali, C Silverman, JD Urry, CM Schawinski, K AF Hao, Heng Elvis, Martin Bongiorno, Angela Zamorani, Gianni Merloni, Andrea Kelly, Brandon C. Civano, Francesca Celotti, Annalisa Ho, Luis C. Jahnke, Knud Comastri, Andrea Trump, Jonathan R. Mainieri, Vincenzo Salvato, Mara Brusa, Marcella Impey, Chris D. Koekemoer, Anton M. Lanzuisi, Giorgio Vignali, Cristian Silverman, John D. Urry, C. Megan Schawinski, Kevin TI A quasar-galaxy mixing diagram: quasar spectral energy distribution shapes in the optical to near-infrared SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys - galaxies: evolution; quasars: general ID ACTIVE GALACTIC NUCLEI; WIDE-FIELD SURVEY; SUPERMASSIVE BLACK-HOLES; DIGITAL SKY SURVEY; SMALL-MAGELLANIC-CLOUD; COSMOS FIELD; EVOLUTIONARY SEQUENCES; STELLAR MODELS; HOST GALAXIES; RADIATIVE OPACITIES AB We define a quasar-galaxy mixing diagram using the slopes of their spectral energy distributions (SEDs) from 1 mu m to 3000 A and from 1 to 3 mu m in the rest frame. The mixing diagram can easily distinguish among quasar-dominated, galaxy-dominated and reddening-dominated SED shapes. By studying the position of the 413 XMM-selected type 1 AGN in the wide-field 'Cosmic Evolution Survey' in the mixing diagram, we find that a combination of the Elvis et al. mean quasar SED with various contributions from galaxy emission and some dust reddening is remarkably effective in describing the SED shape from 0.3 to 3 mu m for large ranges of redshift, luminosity, black hole mass and Eddington ratio of type 1 AGN. In particular, the location in the mixing diagram of the highest luminosity AGN is very close (within 1 Sigma) to that of the Elvis et al. SED template. The mixing diagram can also be used to estimate the host galaxy fraction and reddening in quasar. We also show examples of some outliers which might be AGN in different evolutionary stages compared to the majority of AGN in the quasar-host galaxy co-evolution cycle. C1 [Hao, Heng] SISSA, I-34136 Trieste, Italy. [Hao, Heng; Elvis, Martin; Civano, Francesca] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bongiorno, Angela; Merloni, Andrea; Brusa, Marcella; Lanzuisi, Giorgio] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Bongiorno, Angela] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Rome, Italy. [Zamorani, Gianni; Comastri, Andrea; Vignali, Cristian] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Kelly, Brandon C.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Civano, Francesca] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Celotti, Annalisa] Osserv Astron Brera, INAF, I-23807 Merate, Italy. [Ho, Luis C.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Jahnke, Knud] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Trump, Jonathan R.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Mainieri, Vincenzo] European So Observ, D-85748 Garching, Germany. [Salvato, Mara] Max Planck Inst Plasma Phys, IPP, D-85748 Garching, Germany. [Salvato, Mara] Excellence Cluster, D-85748 Garching, Germany. [Brusa, Marcella; Vignali, Cristian] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Impey, Chris D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Silverman, John D.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe, Kavli IPMU,WPI, Kashiwa, Chiba 2778583, Japan. [Urry, C. Megan] Yale Univ, Dept Phys, New Haven, CT 06511 USA. [Urry, C. Megan] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA. [Schawinski, Kevin] Swiss Fed Inst Technol, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. RP Hao, H (reprint author), SISSA, Via Bonomea 265, I-34136 Trieste, Italy. EM henghao@post.harvard.edu RI Urry, Claudia/G-7381-2011; Vignali, Cristian/J-4974-2012; Lanzuisi, Giorgio/K-4378-2013; Comastri, Andrea/O-9543-2015; OI Koekemoer, Anton/0000-0002-6610-2048; Urry, Claudia/0000-0002-0745-9792; Vignali, Cristian/0000-0002-8853-9611; Lanzuisi, Giorgio/0000-0001-9094-0984; Comastri, Andrea/0000-0003-3451-9970; Bongiorno, Angela/0000-0002-0101-6624; Jahnke, Knud/0000-0003-3804-2137; Schawinski, Kevin/0000-0001-5464-0888; Zamorani, Giovanni/0000-0002-2318-301X FU NASA Chandra grant [G07-8136A]; Italian Space Agency (ASI) [ASI-INAF I/088/06/0, I/009/10/0]; German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize [FKZ HA 1850/28-1]; Swiss National Science Foundation [PP00P2_138979/1] FX HH thanks Belinda Wilkes, Martin J. Ward and Zhenyi Cai for valuable discussions. This work was supported in part by NASA Chandra grant number G07-8136A (HH, ME, CV). Support from the Italian Space Agency (ASI) under the contracts ASI-INAF I/088/06/0 and I/009/10/0 is acknowledged (AC and CV). MS acknowledges support by the German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize (FKZ HA 1850/28-1). KS gratefully acknowledges support from Swiss National Science Foundation Grant PP00P2_138979/1. NR 102 TC 11 Z9 11 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2013 VL 434 IS 4 BP 3104 EP 3121 DI 10.1093/mnras/stt1228 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229KK UT WOS:000325262300033 ER PT J AU Greif, TH Springel, V Bromm, V AF Greif, Thomas H. Springel, Volker Bromm, Volker TI On the operation of the chemothermal instability in primordial star-forming clouds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; stars: formation; galaxies: formation; galaxies: high-redshift; cosmology: theory; early Universe ID POPULATION-III STARS; INITIAL MASS FUNCTION; DARK-MATTER ANNIHILATION; BARYONIC STRUCTURE FORMATION; 1ST COSMIC STRUCTURES; GALACTIC GAS CLOUDS; THERMAL-INSTABILITY; RADIATIVE FEEDBACK; MOLECULAR-HYDROGEN; MAGNETIC-FIELDS AB We investigate the operation of the chemothermal instability in primordial star-forming clouds with a suite of three-dimensional, moving-mesh simulations. In line with previous studies, we find that the gas at the centre of high-redshift minihaloes becomes chemothermally unstable as three-body reactions convert the atomic hydrogen into a fully molecular gas. The competition between the increasing rate at which the gas cools and the increasing optical depth to H-2 line emission creates a characteristic dip in the cooling time over the free-fall time on a scale of 100 au. As a result, the free-fall time decreases to below the sound-crossing time, and the cloud may become gravitationally unstable and fragment on a scale of a few tens of au during the initial free-fall phase. In three of the nine haloes investigated, secondary clumps condense out of the parent cloud, which will likely collapse in their own right before they are accreted by the primary clump. In the other haloes, fragmentation at such an early stage is less likely. However, given that previous simulations have shown that the infall velocity decreases substantially once the gas becomes rotationally supported, the amount of time available for perturbations to develop may be much greater than is evident from the limited period of time simulated here. C1 [Greif, Thomas H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Greif, Thomas H.] Max Planck Inst Astrophys, D-85740 Garching, Germany. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, Zentrum Astron, Astron Recheninst, D-69120 Heidelberg, Germany. [Bromm, Volker] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Bromm, Volker] Univ Texas Austin, Texas Cosmol Ctr, Austin, TX 78712 USA. RP Greif, TH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tgreif@cfa.harvard.edu FU NSF [AST-1009928] FX THG would like to thank Tom Abel and Naoki Yoshida for stimulating discussions that helped improve this work. The simulations were carried out at the Rechenzentrum Garching (RZG) and the Texas Advanced Computing Center (TACC) under XSEDE allocation AST130020 (for THG) and project A-astro (for VB). VB acknowledges support from NSF through grant AST-1009928. NR 125 TC 12 Z9 12 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 OCT PY 2013 VL 434 IS 4 BP 3408 EP 3422 DI 10.1093/mnras/stt1251 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229KK UT WOS:000325262300057 ER PT J AU Kilic, M Gianninas, A Brown, WR Harris, HC Dahn, CC Agueros, MA Heinke, CO Kenyon, SJ Panei, JA Camilo, F AF Kilic, Mukremin Gianninas, A. Brown, Warren R. Harris, Hugh C. Dahn, Conard C. Agueeros, M. A. Heinke, Craig O. Kenyon, S. J. Panei, J. A. Camilo, Fernando TI The runaway binary LP 400-22 is leaving the Galaxy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: close; stars: individual: LP 400-22; stars: individual: WD 2234+222; white dwarfs; Galaxy: kinematics and dynamics; Galaxy: stellar content ID LARGE-MAGELLANIC-CLOUD; WHITE-DWARF STARS; HYPERVELOCITY STARS; GALACTIC HALO; LOW-MASS; BLACK-HOLE; MILKY-WAY; O-STAR; DISCOVERY; VELOCITY AB We present optical spectroscopy, astrometry, radio and X-ray observations of the runaway binary LP 400-22. We refine the orbital parameters of the system based on our new radial velocity observations. Our parallax data indicate that LP 400-22 is significantly more distant (3 Sigma lower limit of 840 pc) than initially predicted. LP 400-22 has a tangential velocity in excess of 830 km s(-1); it is unbound to the Galaxy. Our radio and X-ray observations fail to detect a recycled millisecond pulsar companion, indicating that LP 400-22 is a double white dwarf system. This essentially rules out a supernova runaway ejection mechanism. Based on its orbit, a Galactic Centre origin is also unlikely. However, its orbit intersects the locations of several globular clusters; dynamical interactions between LP 400-22 and other binary stars or a central black hole in a dense cluster could explain the origin of this unusual binary. C1 [Kilic, Mukremin; Gianninas, A.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Brown, Warren R.; Kenyon, S. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Harris, Hugh C.; Dahn, Conard C.] US Naval Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Agueeros, M. A.; Camilo, Fernando] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Heinke, Craig O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Panei, J. A.] UNLP, CONICET, IALP, La Plata, Buenos Aires, Argentina. [Camilo, Fernando] Arecibo Observ, Arecibo, PR 00612 USA. RP Kilic, M (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. EM kilic@ou.edu RI Agueros, Marcel/K-7998-2014; Alexandros, Gianninas/B-8352-2016; OI Agueros, Marcel/0000-0001-7077-3664; Alexandros, Gianninas/0000-0002-8655-4308; Kenyon, Scott/0000-0003-0214-609X; Heinke, Craig/0000-0003-3944-6109 FU University of Oklahoma Research Council; College of Arts and Sciences; NSERC; Alberta Ingenuity New Faculty Award FX We thank P. Bergeron for useful discussions on mixed model atmospheres and S. Vennes for a constructive referee report. MK is thankful to the University of Oklahoma Research Council and the College of Arts and Sciences for a Junior Faculty Fellowship. CH is supported by an NSERC Discovery Grant and by an Alberta Ingenuity New Faculty Award. Part of the observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. The Robert C. Byrd Green Bank Telescope is operated by the National Radio Astronomy Observatory, which is a facility of the US National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 46 TC 7 Z9 7 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2013 VL 434 IS 4 BP 3582 EP 3589 DI 10.1093/mnras/stt1282 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229KK UT WOS:000325262300070 ER PT J AU DeVience, SJ Walsworth, RL Rosen, MS AF DeVience, Stephen J. Walsworth, Ronald L. Rosen, Matthew S. TI Nuclear spin singlet states as a contrast mechanism for NMR spectroscopy SO NMR IN BIOMEDICINE LA English DT Article DE quantum filter; nuclear spin singlet state; glutamine; spin locking ID MAGNETIC-RESONANCE-SPECTROSCOPY; GAMMA-AMINOBUTYRIC-ACID; LONG-LIVED STATES; BRAIN IN-VIVO; QUANTUM FILTER; H-1-NMR SPECTROSCOPY; RESOLVED GLUTAMATE; STEAM SEQUENCE; SLOW DIFFUSION; RAT-BRAIN AB Nuclear magnetic resonance (NMR) spectra of complex chemical mixtures often contain unresolved or hidden spectral components, especially when strong background signals overlap weaker peaks. In this article we demonstrate a quantum filter utilizing nuclear spin singlet states, which allows undesired NMR spectral background to be removed and target spectral peaks to be uncovered. The quantum filter is implemented by creating a nuclear spin singlet state with spin quantum numbers j=0, m(z)=0 in a target molecule, applying a continuous RF field to both preserve the singlet state and saturate the magnetization of undesired molecules and then mapping the target molecule singlet state back into an NMR observable state so that its spectrum can be read out unambiguously. The preparation of the target singlet state can be carefully controlled with pulse sequence parameters, so that spectral contrast can be achieved between molecules with very similar structures. We name this NMR contrast mechanism 'Suppression of Undesired Chemicals using Contrast-Enhancing Singlet States' (SUCCESS) and we demonstrate it in vitro for three target molecules relevant to neuroscience: aspartate, threonine and glutamine. Copyright (C) 2013 John Wiley & Sons, Ltd. C1 [DeVience, Stephen J.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Walsworth, Ronald L.] Harvard Univ, Ctr Brain Sci, Cambridge, MA 02138 USA. [Walsworth, Ronald L.; Rosen, Matthew S.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Rosen, Matthew S.] Harvard Univ, Sch Med, Boston, MA 02115 USA. [Rosen, Matthew S.] AA Martinos Ctr Biomed Imaging, Charlestown, MA 02129 USA. RP DeVience, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, MS 59,60 Garden St, Cambridge, MA 02138 USA. EM devience@fas.harvard.edu RI DeVience, Stephen/D-7274-2012 OI DeVience, Stephen/0000-0003-3142-7296 FU National Science Foundation (NSF) FX We acknowledge support from the National Science Foundation (NSF). NR 48 TC 7 Z9 7 U1 0 U2 13 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0952-3480 EI 1099-1492 J9 NMR BIOMED JI NMR Biomed. PD OCT PY 2013 VL 26 IS 10 BP 1204 EP 1212 DI 10.1002/nbm.2936 PG 9 WC Biophysics; Radiology, Nuclear Medicine & Medical Imaging; Spectroscopy SC Biophysics; Radiology, Nuclear Medicine & Medical Imaging; Spectroscopy GA 218WB UT WOS:000324462100002 PM 23606451 ER PT J AU Oter, K Gunay, F Tuzer, E Linton, YM Bellini, R Alten, B AF Oter, Kerem Gunay, Filiz Tuzer, Erkut Linton, Yvonne-Marie Bellini, Romeo Alten, Bulent TI First Record of Stegomyia albopicta in Turkey Determined By Active Ovitrap Surveillance and DNA Barcoding SO VECTOR-BORNE AND ZOONOTIC DISEASES LA English DT Article DE Stegomyia albopicta; Aedes albopictus; Turkey; Establishment; DNA barcoding ID MOSQUITO AEDES-ALBOPICTUS; WEST-NILE-VIRUS; DIPTERA-CULICIDAE; VECTOR COMPETENCE; EMILIA-ROMAGNA; SPREAD; TIGER; ESTABLISHMENT; DISPERSAL; INVASION AB Despite its confirmed establishment in neighboring Greece and Bulgaria, the presence of the Oriental invasive species Stegomyia albopicta (Skuse) (=Aedes albopictus) has never been confirmed in Turkey. Active surveillance for this container-breeding species was carried out using oviposition traps at 15 discrete sites in the towns of Ipsala (n=8 sites), Kesan (n=5) (Edirne District), and Malkara (n=2) (Tekirdag District) in the Thrace region of northwestern Turkey, from May 23 through November 10, 2011. Eggs collected were reared to the fourth larval instar and adult stages where possible to facilitate integrated morphological and molecular species identification. DNA barcodes (658bp of the mitochondrial cytochrome c oxidase I [COI] gene) were compared with all four potentially invasive Stegomyia species: St. aegypti, St. albopicta, St. cretina, and St. japonica. Sequences generated for samples collected in Thrace Region were herein confirmed as St. albopicta, the first record of this vector species in Turkey. Eggs of St. albopicta were detected in two discrete localities: (1) In the grounds of a restaurant in Kesan (in week 36), and (2) in the customs area of the Turkish-Greek border at Ipsala (in weeks 32 and 38). Multiple detection of St. albopicta eggs indicates the possible establishment of the species in northwestern Turkey. Finding this important disease vector has implications for public health and requires the implementation of active vector monitoring programs and targeted vector suppression strategies to limit the spread of this invasive vector species in Turkey. C1 [Oter, Kerem; Tuzer, Erkut] Istanbul Univ, Fac Vet Med, Dept Parasitol, Avcilar, Turkey. [Gunay, Filiz; Alten, Bulent] Hacettepe Univ, Fac Sci, Dept Biol, Ecol Div,ESRL Labs, Beytepe, Turkey. [Linton, Yvonne-Marie] Walter Reed Army Inst Res, Entomol Branch, Silver Spring, MD USA. [Bellini, Romeo] Ctr Agr Ambiente G Nicoli, Crevalcore, Italy. RP Linton, YM (reprint author), Smithsonian Inst, Walter Reed Biosystemat Unit, Museum Support Ctr, MSC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM linton.yvonne3@gmail.com FU Scientific Research Projects Coordination Unit of Istanbul University [11459]; Hacettepe University Scientific Research Unit, Ankara, Turkey; National Research Council (NRC) Research Associateship Award at the Walter Reed Army Institute of Research FX Funding for this study was provided by the Scientific Research Projects Coordination Unit of Istanbul University (Project Number 11459) and Hacettepe University Scientific Research Unit, Ankara, Turkey. DNA sequencing for this study was carried out as part of the activities of the Mosquito Barcoding Initiative (Project Leaders: Y.M.L. and Richard C. Wilkerson, Walter Reed Biosystematics Unit [WRBU], Smithsonian Institution, USA). We are grateful to MBI collaborators, Major Joshua Bast (USAMRU-Kenya) and Dr. G. Koliopoulos (Benaki Institute, Athens, Greece), for providing specimens used as outgroups in this study, and to Dr. Desmond Foley (WRBU) and Ssgt. Luke Mitchell (British Army) for assistance with the map figure. This manuscript was prepared while Y.M.L. held a National Research Council (NRC) 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 Defense. NR 54 TC 8 Z9 9 U1 2 U2 4 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1530-3667 EI 1557-7759 J9 VECTOR-BORNE ZOONOT JI Vector-Borne Zoonotic Dis. PD OCT 1 PY 2013 VL 13 IS 10 BP 753 EP 761 DI 10.1089/vbz.2012.1093 PG 9 WC Public, Environmental & Occupational Health; Infectious Diseases SC Public, Environmental & Occupational Health; Infectious Diseases GA 230RO UT WOS:000325360300009 PM 23808976 ER PT J AU Loaiza, JR Scott, ME Bermingham, E Sanjur, OI Rovira, JR Dutari, LC Linton, YM Bickersmith, S Conn, JE AF Loaiza, Jose R. Scott, Marilyn E. Bermingham, Eldredge Sanjur, Oris I. Rovira, Jose R. Dutari, Larissa C. Linton, Yvonne-Marie Bickersmith, Sara Conn, Jan E. TI Novel genetic diversity within Anopheles punctimacula s.l.: Phylogenetic discrepancy between the Barcode cytochrome c oxidase I (COI) gene and the rDNA second internal transcribed spacer (ITS2) SO ACTA TROPICA LA English DT Article DE Anopheles punctimacula s.l.; Molecular taxonomy; Arribalzagia Series; COI gene; Folmer region; rDNA-ITS2 ID DIPTERA-CULICIDAE; MALARIA VECTORS; CENTRAL-AMERICA; SOUTHEAST-ASIA; DNA BARCODES; MOLECULAR-IDENTIFICATION; POPULATION DIVERGENCE; SUNDAICUS DIPTERA; SPECIES COMPLEX; RIBOSOMAL DNA AB Anopheles punctimacula s.l. is a regional malaria vector in parts of Central America, but its role in transmission is controversial due to its unresolved taxonomic status. Two cryptic species, An. malefactor and An. calderoni, have been previously confused with this taxon, and evidence for further genetic differentiation has been proposed. In the present study we collected and morphologically identified adult female mosquitoes of An. punctimacula s.l. from 10 localities across Panama and one in Costa Rica. DNA sequences from three molecular regions, the three prime end of the mitochondrial cytochrome c oxidase I gene (3' C01), the Barcode region in the five prime end of the COI (5' C01), and the rDNA second internal transcribed spacer (ITS2) were used to test the hypothesis of new molecular lineages within An. punctimacula s.l. Phylogenetic analyses using the 3' COI depicted six highly supported molecular lineages (A F), none of which was An. malefactor. In contrast, phylogenetic inference with the 5' COI demonstrated paraphyly. Tree topologies based on the combined COI regions and ITS2 sequence data supported the same six lineages as the 3' COI alone. As a whole this evidence suggests that An. punctimacula s.l. comprises two geographically isolated lineages, but it is not clear whether these are true species. The phylogenetic structure of the An. punctimacula cluster as well as that of other unknown lineages (C type I vs C type II; D vs E) appears to be driven by geographic partition, because members of these assemblages did not overlap spatially. We report An. malefactor for the first time in Costa Rica, but our data do not support the presence of An. calderoni in Panama. (C) 2013 Elsevier B.V. All rights reserved. C1 [Loaiza, Jose R.; Dutari, Larissa C.] Inst Invest Cient & Serv Alta Tecnol, Ctr Biodiversidad & Descubrimiento Drogas, Clayton, Panama. [Loaiza, Jose R.] Univ Panama, Programa Ctr Amer Maestria Entomol Vicerrectoria, Panama City, Panama. [Scott, Marilyn E.] McGill Univ, Inst Parasitol, Montreal, PQ H3A 2T5, Canada. [Bermingham, Eldredge; Sanjur, Oris I.; Rovira, Jose R.; Dutari, Larissa C.] Smithsonian Trop Res Inst, U0948, Balboa Ancon, Panama. [Linton, Yvonne-Marie] Nat Hist Museum, London SW7 5BD, England. [Linton, Yvonne-Marie] Walter Reed Army Inst Res, Entomol Branch, Silver Spring, MD 20910 USA. [Bickersmith, Sara; Conn, Jan E.] New York State Dept Hlth, Wadsworth Ctr, Albany, NY 12205 USA. [Conn, Jan E.] SUNY Albany, Dept Biomed Sci, Albany, NY 12202 USA. RP Loaiza, JR (reprint author), Inst Invest Cient & Serv Alta Tecnol, Ctr Biodiversidad & Descubrimiento Drogas, Clayton, Panama. EM jloaiza@indicasat.org.pa; marilyn.scott@mcgill.ca; bermingham@si.edu; sanjuro@si.edu; jrrovira@yahoo.es; dutaril@si.edu; linton.yvonne3@gmail.com; sab19@health.state.ny.us; jconn@wadsworth.org RI Scott, Marilyn/L-5347-2015; OI Conn, Jan/0000-0002-5301-7020 FU Science, Technology and Innovation of Panama (SENACYT) [COL08-066]; National Research Investigator Board; Institute of Advanced Scientific Investigations and High Technology Services (INDICASAT AIP); Smithsonian Tropical Research Institute (STRI); Natural Sciences and Engineering Research Council of Canada (NSERC); NIH [2R0154139]; Fonds Quebecois de la recherche sur la nature et les technologies (FQRNT); Walter Reed Army Institute of Research FX We want to thank three anonymous reviewers who provided valuable comments to improve the quality, clarity and impact of this manuscript. We also thank Dr. Marta Moreno (Wadsworth Center, New York State Department of Health, Albany, NY) and Sasha McKeon (Department of Biomedical Sciences, School of Public Health, SUNY-Albany, NY) for assistance with analysis and experiments. We are grateful to Luis Guillermo Chaverri Sanchez and Alvaro Herrera Villalobos from the Instituto Nacional de Biodiversidad de Costa Rica (INBio) for helping us obtain the required collecting and export permits and for fieldwork guidance in Costa Rica. Mosquito sampling in Costa Rica was conducted under the research passport (No. 01573/resolution 096-2007) issued to JRL by the National System of Conservation Areas (SINAC). The export permit (DGVS-867-2007) was granted by the Ministry of Natural Resources, Energy, and Mines (MIRENEM). The Secretariat for Science, Technology and Innovation of Panama (SENACYT) through the research grant COL08-066 and the National Research Investigator Board (SNI) prize awarded to JRL, partially financed this study. Additional financial support was provided by The Institute of Advanced Scientific Investigations and High Technology Services (INDICASAT AIP), the Smithsonian Tropical Research Institute (STRI), Natural Sciences and Engineering Research Council of Canada (NSERC) and NIH grant (AI) 2R0154139 to JEC. Research at the Institute of Parasitology is supported by a regroupement strategique from Fonds Quebecois de la recherche sur la nature et les technologies (FQRNT) to MES. This manuscript was prepared while YML held a National Research Council (NRC) 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 Defense. NR 52 TC 8 Z9 9 U1 2 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0001-706X EI 1873-6254 J9 ACTA TROP JI Acta Trop. PD OCT PY 2013 VL 128 IS 1 BP 61 EP 69 DI 10.1016/j.actatropica.2018.06.012 PG 9 WC Parasitology; Tropical Medicine SC Parasitology; Tropical Medicine GA 239GA UT WOS:000326009400009 PM 23806568 ER PT J AU Kazin, EA Sanchez, AG Cuesta, AJ Beutler, F Chuang, CH Eisenstein, DJ Manera, M Padmanabhan, N Percival, WJ Prada, F Ross, AJ Seo, HJ Tinker, J Tojeiro, R Xu, XY Brinkmann, J Joel, B Nichol, RC Schlegel, DJ Schneider, DP Thomas, D AF Kazin, Eyal A. Sanchez, Ariel G. Cuesta, Antonio J. Beutler, Florian Chuang, Chia-Hsun Eisenstein, Daniel J. Manera, Marc Padmanabhan, Nikhil Percival, Will J. Prada, Francisco Ross, Ashley J. Seo, Hee-Jong Tinker, Jeremy Tojeiro, Rita Xu, Xiaoying Brinkmann, J. Joel, Brownstein Nichol, Robert C. Schlegel, David J. Schneider, Donald P. Thomas, Daniel TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measuring H(z) and D-A(z) at z=0.57 with clustering wedges SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmological parameters; distance scale; large-scale structure of Universe ID DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; LARGE-SCALE STRUCTURE; DARK ENERGY SURVEY; OBSERVATIONS COSMOLOGICAL INTERPRETATION; 2-POINT CORRELATION-FUNCTION; ACOUSTIC-OSCILLATIONS; POWER-SPECTRUM; DATA RELEASE; REDSHIFT-SPACE AB We analyse the 2D correlation function of the Sloan Digital Sky Survey-III Baryon Oscillation Spectroscopic Survey (BOSS) CMASS sample of massive galaxies of the ninth data release to measure cosmic expansion H and the angular diameter distance D-A at a mean redshift of < z > = 0.57. We apply, for the first time, a new correlation function technique called clustering wedges. xi(Delta mu) (s). Using a physically motivated model, the anisotropic baryonic acoustic feature in the galaxy sample is detected at a significance level of 4.7 sigma compared to a featureless model. The baryonic acoustic feature is used to obtain model-independent constraints cz/H/r(s) = 12.28 +/- 0.82 (6.7 percent accuracy) and D-A/r(s) = 9.05 +/- 0.27 (3.0 per cent) with a correlation coefficient of -0.5, where r(s) is the sound horizon scale at the end of the baryonic drag era. We conduct thorough tests on the data and 600 simulated realizations, finding robustness of the results regardless of the details of the analysis method. Combining this with r(s) constraints from the cosmic microwave background, we obtain H(0.57) = 90.8 +/- 6.2 km s(-1) Mpc(-1) and D-A(0.57) = 1386 +/- 45 Mpc. We use simulations to forecast results of the final BOSS CMASS data set. We apply the reconstruction technique on the simulations demonstrating that the sharpening of the anisotropic baryonic acoustic feature should improve the detection as well as tighten constraints of H and D-A by similar to 30 per cent on average. C1 [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. [Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Cuesta, Antonio J.; Padmanabhan, Nikhil] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Beutler, Florian; Seo, Hee-Jong; Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Chuang, Chia-Hsun; Prada, Francisco] Univ Autonoma Madrid, Inst Fis Teor UAM CSIC, E-28049 Madrid, Spain. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Manera, Marc; Percival, Will J.; Ross, Ashley J.; Tojeiro, Rita; Nichol, Robert C.; Thomas, Daniel] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Prada, Francisco] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Tinker, Jeremy] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Xu, Xiaoying] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Brinkmann, J.] Apache Point Observ, Sunspot, NM 88349 USA. [Joel, Brownstein] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. RP Kazin, EA (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia. EM eyalkazin@gmail.com FU Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; Trans-regional Collaborative Research Centre TR33 of the German Research Foundation (DFG); Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science FX It is a pleasure to thank Chris Blake for his insight. We also thank David Kirkby, Felipe Marin, Cameron McBride and Uros Seljak for useful discussions. EK is supported by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. AGS acknowledges support by the Trans-regional Collaborative Research Centre TR33 'The Dark Universe' of the German Research Foundation (DFG). EAK thanks Erin Sheldon for software used here. Numerical computations for the PTHalos mocks were done on the Sciama High Performance Compute (HPC) cluster which is supported by the ICG, SEPNet and the University of Portsmouth. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University. NR 92 TC 28 Z9 28 U1 0 U2 11 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 OCT PY 2013 VL 435 IS 1 BP 64 EP 86 DI 10.1093/mnras/stt1261 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236NL UT WOS:000325804300005 ER PT J AU Foley, RJ AF Foley, Ryan J. TI On spectral line profiles in Type Ia supernova spectra SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE line: identification; line: profiles; supernovae: general; supernovae: individual: SN 2010ae; supernovae: individual: SN 2011fe ID HIGH-VELOCITY FEATURES; HUBBLE-SPACE-TELESCOPE; SN 2011FE; CIRCUMSTELLAR INTERACTION; OPTICAL SPECTROSCOPY; EJECTA VELOCITY; LOW-LUMINOSITY; MAXIMUM-LIGHT; ULTRAVIOLET; EXPLOSION AB We present a detailed analysis of spectral line profiles in Type Ia supernova (SN Ia) spectra. We focus on the feature at similar to 3500-4000 angstrom, which is commonly thought to be caused by blueshifted absorption of Ca H&K. Unlike some other spectral features in SN Ia spectra, this feature often has two overlapping (blue and red) components. It is accepted that the red component comes from photospheric calcium. However, it has been proposed that the blue component is caused by either high-velocity calcium (from either abundance or density enhancements above the photosphere of the supernova, SN) or Si II lambda 3858. By looking at multiple data sets and model spectra, focusing on spectra near maximum brightness, we conclude that the blue component of the Ca H&K feature is caused by Si II lambda 3858 for most SNe Ia, although high-velocity calcium is likely important for some SNe. The strength of the Si II lambda 3858 feature varies strongly with the light-curve shape of an SN. As a result, the velocity measured from a single-Gaussian fit to the full line profile correlates with light-curve shape. The velocity of the Ca H&K component of the profile does not correlate with light-curve shape, contrary to previous claims. We detail the pitfalls of assuming that the blue component of the Ca H&K feature is caused by calcium, with implications for our understanding of SN Ia progenitors, explosions and cosmology. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rfoley@cfa.harvard.edu FU NASA [NAS 5-26555] FX This paper is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. NR 68 TC 14 Z9 14 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2013 VL 435 IS 1 BP 273 EP 288 DI 10.1093/mnras/stt1292 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236NL UT WOS:000325804300018 ER PT J AU Jensen, H Datta, KK Mellema, G Chapman, E Abdalla, FB Iliev, IT Mao, Y Santos, MG Shapiro, PR Zaroubi, S Bernardi, G Brentjens, MA de Bruyn, AG Ciardi, B Harker, GJA Jelic, V Kazemi, S Koopmans, LVE Labropoulos, P Martinez, O Offringa, AR Pandey, VN Schaye, J Thomas, RM Veligatla, V Vedantham, H Yatawatta, S AF Jensen, Hannes Datta, Kanan K. Mellema, Garrelt Chapman, Emma Abdalla, Filipe B. Iliev, Ilian T. Mao, Yi Santos, Mario G. Shapiro, Paul R. Zaroubi, Saleem Bernardi, G. Brentjens, M. A. de Bruyn, A. G. Ciardi, B. Harker, G. J. A. Jelic, V. Kazemi, S. Koopmans, L. V. E. Labropoulos, P. Martinez, O. Offringa, A. R. Pandey, V. N. Schaye, J. Thomas, R. M. Veligatla, V. Vedantham, H. Yatawatta, S. TI Probing reionization with LOFAR using 21-cm redshift space distortions SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: interferometers; methods: numerical; dark ages, reionization, first stars ID 21 CENTIMETER FLUCTUATIONS; BLIND SOURCE SEPARATION; STAR-FORMING GALAXIES; NORTH CELESTIAL POLE; POWER SPECTRUM; FOREGROUND REMOVAL; COSMIC REIONIZATION; NEUTRAL HYDROGEN; CM TOMOGRAPHY; EPOCH AB One of the most promising ways to study the epoch of reionization (EoR) is through radio observations of the redshifted 21-cm line emission from neutral hydrogen. These observations are complicated by the fact that the mapping of redshifts to line-of-sight positions is distorted by the peculiar velocities of the gas. Such distortions can be a source of error if they are not properly understood, but they also encode information about cosmology and astrophysics. We study the effects of redshift space distortions on the power spectrum of 21-cm radiation from the EoR using large-scale N-body and radiative transfer simulations. We quantify the anisotropy introduced in the 21-cm power spectrum by redshift space distortions and show how it evolves as reionization progresses and how it relates to the underlying physics. We go on to study the effects of redshift space distortions on LOFAR observations, taking instrument noise and foreground subtraction into account. We find that LOFAR should be able to directly observe the power spectrum anisotropy due to redshift space distortions at spatial scales around k similar to 0.1 Mpc(-1) after greater than or similar to 1000 h of integration time. At larger scales, sample errors become a limiting factor, while at smaller scales detector noise and foregrounds make the extraction of the signal problematic. Finally, we show how the astrophysical information contained in the evolution of the anisotropy of the 21-cm power spectrum can be extracted from LOFAR observations, and how it can be used to distinguish between different reionization scenarios. C1 [Jensen, Hannes; Datta, Kanan K.; Mellema, Garrelt] Stockholm Univ, Dept Astron, AlbaNova, SE-10691 Stockholm, Sweden. [Jensen, Hannes; Datta, Kanan K.; Mellema, Garrelt] Stockholm Univ, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden. [Chapman, Emma; Abdalla, Filipe B.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Iliev, Ilian T.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Mao, Yi] Univ Paris 06, CNRS, Inst Lagrange Paris, Inst Astrophys Paris,UMR7095, F-75014 Paris, France. [Santos, Mario G.] Univ Tecn Lisboa, CENTRA, Inst Super Tecn, P-1049001 Lisbon, Portugal. [Santos, Mario G.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Shapiro, Paul R.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Zaroubi, Saleem; Bernardi, G.; de Bruyn, A. G.; Jelic, V.; Kazemi, S.; Koopmans, L. V. E.; Martinez, O.; Offringa, A. R.; Thomas, R. M.; Veligatla, V.; Vedantham, H.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brentjens, M. A.; de Bruyn, A. G.; Jelic, V.; Labropoulos, P.; Pandey, V. N.; Yatawatta, S.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Ciardi, B.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Harker, G. J. A.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Offringa, A. R.] RSAA, Mt Stromlo Observ, Weston, ACT 2611, Australia. [Schaye, J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Jensen, H (reprint author), Stockholm Univ, Dept Astron, AlbaNova, SE-10691 Stockholm, Sweden. EM hannes.jensen@astro.su.se RI Jelic, Vibor/B-2938-2014; Thomas, Rajat/B-7105-2014; Mellema, Garrelt/K-4962-2014; Santos, Mario/F-2484-2011; Harker, Geraint/C-4885-2012; Ciardi, Benedetta/N-7625-2015; Mao, Yi/G-9288-2015; Yatawatta, Sarod/E-6037-2013; OI Jelic, Vibor/0000-0002-6034-8610; Thomas, Rajat/0000-0002-5362-4816; Mellema, Garrelt/0000-0002-2512-6748; Abdalla, Filipe/0000-0003-2063-4345; Schaye, Joop/0000-0002-0668-5560; Santos, Mario/0000-0003-3892-3073; Harker, Geraint/0000-0002-7894-4082; Yatawatta, Sarod/0000-0001-5619-4017; Iliev, Ilian/0000-0002-5174-1365 FU Swedish Research Council [2012-4144, 2009-4088]; Science and Technology Facilities Council [ST/I000976/1]; Southeast Physics Network (SEPNet); NSF [AST-1009799]; NASA [NNX07AH09G, NNX11AE09G]; TeraGrid grant [TG-AST0900005]; Royal Society via an RSURF; Swedish Research Council (VR) through the Oscar Klein Centre [2007-8709]; French state funds [ANR-11-IDEX-0004-02]; FCT-Portugal [PTDC/FIS/100170/2008] FX This study was supported by the Swedish Research Council grants 2012-4144 and 2009-4088, the Science and Technology Facilities Council [grant number ST/I000976/1] and The Southeast Physics Network (SEPNet). The authors acknowledge the Swedish National Infrastructure for Computing (SNIC) resources at HPC2N (Umea, Sweden) and PDC (Stockholm, Sweden) and the Texas Advanced Computing Center (TACC) at The University of Texas at Austin (http://www.tacc.utexas.edu) for providing HPC resources. This research was supported in part by NSF grant AST-1009799, NASA grants NNX07AH09G and NNX11AE09G and TeraGrid grant TG-AST0900005.; FBA acknowledges the support of the Royal Society via an RSURF.; KKD is grateful for financial support from Swedish Research Council (VR) through the Oscar Klein Centre (grant 2007-8709). KKD would also like to thank the Indian Institute of Science and Educational Research, Kolkata and Center for Theoretical Studies, IIT Kharagpur for the hospitality they provided during the period when a part of this work has been done.; YM was supported by French state funds managed by the ANR within the Investissements d'Avenir programme under reference ANR-11-IDEX-0004-02.; MGS acknowledges support from FCT-Portugal under grant PTDC/FIS/100170/2008. NR 72 TC 27 Z9 27 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 OCT PY 2013 VL 435 IS 1 BP 460 EP 474 DI 10.1093/mnras/stt1341 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236NL UT WOS:000325804300031 ER PT J AU Offringa, AR de Bruyn, AG Zaroubi, S Koopmans, LVE Wijnholds, SJ Abdalla, FB Brouw, WN Ciardi, B Iliev, IT Harker, GJA Mellema, G Bernardi, G Zarka, P Ghosh, A Alexov, A Anderson, J Asgekar, A Avruch, IM Beck, R Bell, ME Bell, MR Bentum, MJ Best, P Birzan, L Breitling, F Broderick, J Bruggen, M Butcher, HR de Gasperin, F de Geus, E de Vos, M Duscha, S Eisloeffel, J Fallows, RA Ferrari, C Frieswijk, W Garrett, MA Griessmeier, J Hassall, TE Horneffer, A Iacobelli, M Juette, E Karastergiou, A Klijn, W Kondratiev, VI Kuniyoshi, M Kuper, G van Leeuwen, J Loose, M Maat, P Macario, G Mann, G McKean, JP Meulman, H Norden, MJ Orru, E Paas, H Pandey-Pommier, M Pizzo, R Polatidis, AG Rafferty, D Reich, W van Nieuwpoort, R Roettgering, H Scaife, AMM Sluman, J Smirnov, O Sobey, C Tagger, M Tang, Y Tasse, C ter Veen, S Toribio, C Vermeulen, R Vocks, C van Weeren, RJ Wise, MW Wucknitz, O AF Offringa, A. R. de Bruyn, A. G. Zaroubi, S. Koopmans, L. V. E. Wijnholds, S. J. Abdalla, F. B. Brouw, W. N. Ciardi, B. Iliev, I. T. Harker, G. J. A. Mellema, G. Bernardi, G. Zarka, P. Ghosh, A. Alexov, A. Anderson, J. Asgekar, A. Avruch, I. M. Beck, R. Bell, M. E. Bell, M. R. Bentum, M. J. Best, P. Birzan, L. Breitling, F. Broderick, J. Brueggen, M. Butcher, H. R. de Gasperin, F. de Geus, E. de Vos, M. Duscha, S. Eisloeffel, J. Fallows, R. A. Ferrari, C. Frieswijk, W. Garrett, M. A. Griessmeier, J. Hassall, T. E. Horneffer, A. Iacobelli, M. Juette, E. Karastergiou, A. Klijn, W. Kondratiev, V. I. Kuniyoshi, M. Kuper, G. van Leeuwen, J. Loose, M. Maat, P. Macario, G. Mann, G. McKean, J. P. Meulman, H. Norden, M. J. Orru, E. Paas, H. Pandey-Pommier, M. Pizzo, R. Polatidis, A. G. Rafferty, D. Reich, W. van Nieuwpoort, R. Roettgering, H. Scaife, A. M. M. Sluman, J. Smirnov, O. Sobey, C. Tagger, M. Tang, Y. Tasse, C. ter Veen, S. Toribio, C. Vermeulen, R. Vocks, C. van Weeren, R. J. Wise, M. W. Wucknitz, O. TI The brightness and spatial distributions of terrestrial radio sources SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE atmospheric effects; instrumentation: interferometers; methods: observational; techniques: interferometric; dark ages, reionization, first stars; radio continuum: general ID INTERFERENCE MITIGATION; ASTRONOMY; PROPAGATION; TELESCOPES; EPOCH AB Faint undetected sources of radio-frequency interference (RFI) might become visible in long radio observations when they are consistently present over time. Thereby, they might obstruct the detection of the weak astronomical signals of interest. This issue is especially important for Epoch of Reionization (EoR) projects that try to detect the faint redshifted H I signals from the time of the earliest structures in the Universe. We explore the RFI situation at 30-163 MHz by studying brightness histograms of visibility data observed with Low-Frequency Array (LOFAR), similar to radio-source-count analyses that are used in cosmology. An empirical RFI distribution model is derived that allows the simulation of RFI in radio observations. The brightness histograms show an RFI distribution that follows a power-law distribution with an estimated exponent around -1.5. With several assumptions, this can be explained with a uniform distribution of terrestrial radio sources whose radiation follows existing propagation models. Extrapolation of the power law implies that the current LOFAR EoR observations should be severely RFI limited if the strength of RFI sources remains strong after time integration. This is in contrast with actual observations, which almost reach the thermal noise and are thought not to be limited by RFI. Therefore, we conclude that it is unlikely that there are undetected RFI sources that will become visible in long observations. Consequently, there is no indication that RFI will prevent an EoR detection with LOFAR. C1 [Offringa, A. R.; Butcher, H. R.] Australian Natl Univ, Mt Stromlo Observ, RSAA, Weston, ACT 2611, Australia. [Offringa, A. R.; Bell, M. E.] Mt Stromlo & Siding Spring Observ, ARC Ctr Excellence All Sky Astrophys CAASTRO, Weston, ACT 2611, Australia. [Offringa, A. R.; de Bruyn, A. G.; Zaroubi, S.; Koopmans, L. V. E.; Brouw, W. N.; Ghosh, A.; Avruch, I. M.] Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [de Bruyn, A. G.; Wijnholds, S. J.; Brouw, W. N.; Asgekar, A.; Bentum, M. J.; Butcher, H. R.; de Geus, E.; de Vos, M.; Duscha, S.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Klijn, W.; Kondratiev, V. I.; Kuper, G.; van Leeuwen, J.; Loose, M.; Maat, P.; McKean, J. P.; Meulman, H.; Norden, M. J.; Orru, E.; Pizzo, R.; Polatidis, A. G.; van Nieuwpoort, R.; Sluman, J.; Tang, Y.; Toribio, C.; Vermeulen, R.; Wise, M. W.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Abdalla, F. B.] UCL Dept Phys & Astron, London WC1E 6BT, England. [Ciardi, B.; Bell, M. R.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Iliev, I. T.] Univ Sussex, Brighton BN1 9QH, E Sussex, England. [Harker, G. J. A.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Mellema, G.] Stockholm Univ, AlbaNova Univ Ctr, Stockholm Observ, SE-10691 Stockholm, Sweden. [Bernardi, G.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zarka, P.; Tasse, C.] Observ Paris, CNRS, UMR 8109, LESIA, F-92195 Meudon, France. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Anderson, J.; Beck, R.; Horneffer, A.; Kuniyoshi, M.; Reich, W.; Sobey, C.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Avruch, I. M.] SRON Netherlands Insitute Space Res, NL-3584 CA Utrecht, Netherlands. [Bell, M. E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Best, P.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Birzan, L.; Garrett, M. A.; Iacobelli, M.; Rafferty, D.; Roettgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Breitling, F.; Mann, G.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Broderick, J.; Hassall, T. E.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Brueggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Eisloeffel, J.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Ferrari, C.; Macario, G.] Univ Nice Sophia Antipolis, UMR7293, Lab Lagrange, CNRS,Observ Cote Azur, F-06300 Nice, France. [Griessmeier, J.; Tagger, M.] CNRS, UMR 7328, LPC2E, F-45071 Orleans 02, France. [Juette, E.] Ruhr Univ Bochum, Inst Astron, D-44780 Bochum, Germany. [Karastergiou, A.] Univ Oxford, Oxford OX1 3RH, England. [Kondratiev, V. I.] PN Lebedev Phys Inst, Astro Space Ctr, Moscow 117997, Russia. [van Leeuwen, J.; Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Paas, H.] Univ Groningen, CIT, NL-9700 CA Groningen, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Smirnov, O.] Rhodes Univ, Ctr Radio Astron Tech & Technol RATT, Dept Phys & Elelct, ZA-6140 Grahamstown, South Africa. [Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [ter Veen, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Wucknitz, O.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. RP Offringa, AR (reprint author), Australian Natl Univ, Mt Stromlo Observ, RSAA, Via Cotter Rd, Weston, ACT 2611, Australia. EM offringa@mso.anu.edu.au RI Mellema, Garrelt/K-4962-2014; Tagger, Michel/O-6615-2014; Harker, Geraint/C-4885-2012; Ciardi, Benedetta/N-7625-2015; Kondratiev, Vladislav/N-1105-2015 OI van Weeren, Reinout/0000-0002-0587-1660; Mellema, Garrelt/0000-0002-2512-6748; Tagger, Michel/0000-0003-2962-3220; Harker, Geraint/0000-0002-7894-4082; Iliev, Ilian/0000-0002-5174-1365; de Gasperin, Francesco/0000-0003-4439-2627; Abdalla, Filipe/0000-0003-2063-4345; Kondratiev, Vladislav/0000-0001-8864-7471 FU Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX LOFAR, the Low-Frequency Array designed and constructed by ASTRON, has facilities in several countries, that are owned by various parties (each with their own funding sources), and that are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. CF and GM acknowledge financial support by the 'Agence Nationale de la Recherche' through grant ANR-09-JCJC-0001-01. NR 40 TC 5 Z9 5 U1 0 U2 9 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2013 VL 435 IS 1 BP 584 EP 596 DI 10.1093/mnras/stt1337 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236NL UT WOS:000325804300041 ER PT J AU Tetzlaff, N Torres, G Neuhauser, R Hohle, MM AF Tetzlaff, N. Torres, G. Neuhaeuser, R. Hohle, M. M. TI The neutron star born in the Antlia supernova remnant SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE pulsars: individual: PSR J0630-2834 ID LAMBDA-BOOTIS STARS; B-TYPE STARS; SPECTROSCOPIC SURVEY; PROBABLE BIRTHPLACE; PROPER-MOTION; EVOLUTION; CATALOG; ORIGIN; NEARBY; ASSOCIATIONS AB Among all known young nearby neutron stars, we search for the neutron star that was born in the same supernova event that formed the Antlia supernova remnant (SNR). We also look for a runaway star that could have been the former companion to the neutron star (if it exists) and then got ejected due to the same supernova. We find the pulsar PSR J0630-2834 to be the best candidate for a common origin with the Antlia SNR. In that scenario, the SNR is approximate to 1.2Myr old and is presently located at a distance of approximate to 138 pc. We consider the runaway star HIP 47155 a former companion candidate to PSR J0630-2834. The encounter time and place is consistent with both stars being ejected from the Antlia SNR. We measured the radial velocity of HIP 47155 as 32.42 +/- 0.70 km s(-1). C1 [Tetzlaff, N.; Neuhaeuser, R.; Hohle, M. M.] Inst Astrophys, D-07745 Jena, Germany. [Tetzlaff, N.; Neuhaeuser, R.; Hohle, M. M.] Univ Sternwarte Jena, D-07745 Jena, Germany. [Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tetzlaff, N (reprint author), Inst Astrophys, Schillergasschen 2-3, D-07745 Jena, Germany. EM nina.tetzlaff@uni-jena.de FU Carl-Zeiss-Stiftung; NSF [AST-1007992]; DFG [SFB/TR-7] FX NT acknowledges Carl-Zeiss-Stiftung for a scholarship. GT acknowledges partial support for this work from NSF grant AST-1007992. NT, RN and MMH acknowledge support from DFG in the SFB/TR-7 Gravitational Wave Astronomy. This work has made use of the Australia Telescope National Facility (ATNF) pulsar data base and the SIMBAD, operated at the Centre de Donnees astronomiques de Strasbourg (CDS). NR 47 TC 4 Z9 4 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2013 VL 435 IS 1 BP 879 EP 884 DI 10.1093/mnras/stt1358 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 236NL UT WOS:000325804300064 ER PT J AU Balogh, A Bykov, A Cargill, P Dendy, R de Wit, TD Raymond, J AF Balogh, Andre Bykov, Andrei Cargill, Peter Dendy, Richard de Wit, Thierry Dudok Raymond, John TI Microphysics of Cosmic Plasmas: Background, Motivation and Objectives SO SPACE SCIENCE REVIEWS LA English DT Review AB With the maturing of space plasma research in the solar system, a more general approach to plasma physics in general, applied to cosmic plasmas, has become appropriate. There are both similarities and important differences in describing the phenomenology of space plasmas on scales from the Earth's magnetosphere to galactic and inter-galactic scales. However, there are important aspects in common, related to the microphysics of plasma processes. This introduction to a coordinated collection of papers that address the several aspects of the microphysics of cosmic plasmas that have unifying themes sets out the scope and ambition of the broad sweep of topics covered in the volume, together with an enumeration of the detailed objectives of the coverage. C1 [Balogh, Andre; Cargill, Peter] Univ London Imperial Coll Sci Technol & Med, London SW7 2AZ, England. [Bykov, Andrei] Russian Acad Sci, Ioffe Inst Phys & Technol, St Petersburg 196140, Russia. [Bykov, Andrei] St Petersburg State Polytech Univ, St Petersburg 194021, Russia. [Dendy, Richard] UKAEA Euratom Fus Assoc, Culham Sci Ctr, Abingdon OX14 3DB, Oxon, England. [de Wit, Thierry Dudok] LPC2E CNRS 3A, F-45071 Orleans 2, France. [Raymond, John] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Balogh, A (reprint author), Univ London Imperial Coll Sci Technol & Med, Prince Consort Rd, London SW7 2AZ, England. EM a.balogh@imperial.ac.uk RI Bykov, Andrei/E-3131-2014 NR 0 TC 1 Z9 1 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD OCT PY 2013 VL 178 IS 2-4 BP 77 EP 80 DI 10.1007/s11214-013-0027-1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 240PZ UT WOS:000326110700001 ER PT J AU Massaro, F Giroletti, M Paggi, A D'Abrusco, R Tosti, G Funk, S AF Massaro, F. Giroletti, M. Paggi, A. D'Abrusco, R. Tosti, G. Funk, S. TI BLAZAR SPECTRAL PROPERTIES AT 74 MHz SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE BL Lacertae objects: general; galaxies: active; radiation mechanisms: non-thermal ID LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS; ACTIVE GALACTIC NUCLEI; EXTENDED RADIO-EMISSION; SKY SURVEY; SOURCE CATALOG; 1ST SURVEY; CENTIMETER WAVELENGTHS; HOST GALAXIES; FLUX DENSITY AB Blazars are the most extreme class of active galactic nuclei. Despite a previous investigation at 102 MHz for a small sample of BL Lac objects and our recent analysis of blazars detected in the Westerbork Northern Sky Survey, a systematic study of the blazar spectral properties at frequencies below 100 MHz has been never carried out. In this paper, we present the first analysis of the radio spectral behavior of blazars based on the recent Very Large Array Low-frequency Sky Survey (VLSS) at 74 MHz. We search for blazar counterparts in the VLSS catalog, confirming that they are detected at 74 MHz. We then show that blazars present radio-flat spectra (i.e., radio spectral indices of similar to 0.5) when evaluated, which also about an order of magnitude in frequency lower than previous analyses. Finally, we discuss the implications of our findings in the context of the blazars-radio galaxies connection since the low-frequency radio data provide a new diagnostic tool to verify the expectations of the unification scenario for radio-loud active galaxies. C1 [Massaro, F.; Funk, S.] SLAC Natl Lab, Menlo Pk, CA 94025 USA. [Massaro, F.; Funk, S.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Paggi, A.; D'Abrusco, R.] Harvard Univ, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. RP Massaro, F (reprint author), SLAC Natl Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA. RI D'Abrusco, Raffaele/L-2767-2016; Massaro, Francesco/L-9102-2016; Funk, Stefan/B-7629-2015; Paggi, Alessandro/C-1219-2017; OI D'Abrusco, Raffaele/0000-0003-3073-0605; Massaro, Francesco/0000-0002-1704-9850; Funk, Stefan/0000-0002-2012-0080; Paggi, Alessandro/0000-0002-5646-2410; Giroletti, Marcello/0000-0002-8657-8852 FU NASA [NNX12AO97G]; U.S. Virtual Astronomical Observatory; National Science Foundation; National Aeronautics and Space Administration; ASI/INAF [I/005/12/0] FX We thank our anonymous referee for many helpful comments and for stimulating the discussion on the possible effects of variability, which greatly improved this manuscript. We thank R. Morganti and D. Harris for their valuable comments and suggestions. F. M. is grateful to S. Digel, E. Mahony, M. Murgia, Howard Smith, and M. Urry for their helpful discussions. The work is supported by the NASA grants NNX12AO97G. R. D. gratefully acknowledges the financial support of the U.S. Virtual Astronomical Observatory, which is sponsored by the National Science Foundation and the National Aeronautics and Space Administration. The work by G. T. is supported by ASI/INAF contract I/005/12/0. The WENSS project was a collaboration between the Netherlands Foundation for Research in Astronomy and the 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 on-line 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 theNational Aeronautics and Space Administration. Part of this work is based on the NVSS (NRAO VLA Sky Survey) and on the VLA Low-Frequency Sky Survey (VLSS). 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 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. TOPCAT10 (Taylor 2005) for the preparation and manipulation of the tabular data and the images. NR 54 TC 16 Z9 16 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD OCT PY 2013 VL 208 IS 2 AR UNSP 15 DI 10.1088/0067-0049/208/2/15 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229OM UT WOS:000325276600002 ER PT J AU Mazeh, T Nachmani, G Holczer, T Fabrycky, DC Ford, EB Sanchis-Ojeda, R Sokol, G Rowe, JF Zucker, S Agol, E Carter, JA Lissauer, JJ Quintana, EV Ragozzine, D Steffen, JH Welsh, W AF Mazeh, Tsevi Nachmani, Gil Holczer, Tomer Fabrycky, Daniel C. Ford, Eric B. Sanchis-Ojeda, Roberto Sokol, Gil Rowe, Jason F. Zucker, Shay Agol, Eric Carter, Joshua A. Lissauer, Jack J. Quintana, Elisa V. Ragozzine, Darin Steffen, Jason H. Welsh, William TI TRANSIT TIMING OBSERVATIONS FROM KEPLER. VIII. CATALOG OF TRANSIT TIMING MEASUREMENTS OF THE FIRST TWELVE QUARTERS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE planetary systems; planets and satellites: detection; techniques: miscellaneous; techniques: photometric ID MULTIPLE-PLANET SYSTEMS; HOT-JUPITER; LIGHT CURVES; CONFIRMATION; CANDIDATES; MASS; ARCHITECTURE; PHOTOMETRY; OBLIQUITY; MODELS AB Following the works of Ford et al. and Steffen et al. we derived the transit timing of 1960 Kepler objects of interest (KOIs) using the pre-search data conditioning light curves of the first twelve quarters of the Kepler data. For 721 KOIs with large enough signal-to-noise ratios, we obtained also the duration and depth of each transit. The results are presented as a catalog for the community to use. We derived a few statistics of our results that could be used to indicate significant variations. Including systems found by previous works, we have found 130 KOIs that showed highly significant times of transit variations (TTVs) and 13 that had short-period TTV modulations with small amplitudes. We consider two effects that could cause apparent periodic TTV-the finite sampling of the observations and the interference with the stellar activity, stellar spots in particular. We briefly discuss some statistical aspects of our detected TTVs. We show that the TTV period is correlated with the orbital period of the planet and with the TTV amplitude. C1 [Mazeh, Tsevi; Nachmani, Gil; Holczer, Tomer; Sokol, Gil] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Ford, Eric B.; Ragozzine, Darin] Univ Florida, Dept Astron, Gainesville, FL 32111 USA. [Sanchis-Ojeda, Roberto] MIT, Dept Phys, Cambridge, MA 02139 USA. [Sanchis-Ojeda, Roberto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Rowe, Jason F.; Lissauer, Jack J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Zucker, Shay] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Dept Geophys Atmospher & Planetary Sci, IL-69978 Tel Aviv, Israel. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Carter, Joshua A.] Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Quintana, Elisa V.] SETI Inst, Mountain View, CA 94043 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Welsh, William] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Mazeh, T (reprint author), Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. OI /0000-0002-0802-9145; /0000-0001-6545-639X; Fabrycky, Daniel/0000-0003-3750-0183 FU European Research Council under the EU [291352]; ISRAEL SCIENCE FOUNDATION [1423/11]; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX We thank the referee for extremely valuable remarks and suggestions. The research leading to these results received funding from the European Research Council under the EU's Seventh Framework Programme (FP7/(2007-2013)/ERC Grant Agreement No. 291352) and from the ISRAEL SCIENCE FOUNDATION (grant No. 1423/11). All photometric data presented in this paper were obtained from the Mikulsky Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 43 TC 57 Z9 57 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD OCT PY 2013 VL 208 IS 2 AR UNSP 16 DI 10.1088/0067-0049/208/2/16 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229OM UT WOS:000325276600003 ER PT J AU Moser, WE Richardson, DJ Hammond, CI Lazo-Wasem, EA AF Moser, William E. Richardson, Dennis J. Hammond, Charlotte I. Lazo-Wasem, Eric A. TI Redescription of Placobdella parasitica (Say, 1824) Moore, 1901 (Hirudinida: Glossiphoniidae) SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article DE Rhychobdellida; Hirudinea; Clitellata; Glossiphoniidae; Placobdella; Minnesota; turtle; leech ID LEECH; RHYNCHOBDELLIDA; EMYDIDAE; TURTLE; HOST AB Placobdella parasitica (Say, 1824) was originally described from lakes of the "North-western region." Leeches collected during May and June, 2012, from Minnesota, USA, the type locality of Hirudo parasitica Say, 1824, were consistent with P. parasitica (Say, 1824) Moore, 1901 as described by Say (1824). The acquisition of these specimens from the type locality facilitated redescription of P. parasitica. A neotype is designated to stabilize the concept of P. parasitica. In contrast to the papillated members of the genus Placobdella, P. parasitica does not have a confusing and problematic taxonomic history. Placobdella parasitica is differentiated from its congeners by its smooth dorsal surface (or sensillae present), simple (medial unpigmented yellow line) to elaborate (medial and paramedial marbled patches) pigmentation, and ventrum with 8 to 12 stripes. Molecular comparison of CO-I sequence data from P. parasitica revealed differences of 14% from Placobdella multilineata, 14% from Placobdella papillifera, 15% to 17% from Placobdella rugosa, 15% from Placobdella ornata and 16% to 17% from Placobdella all. C1 [Moser, William E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. [Richardson, Dennis J.; Hammond, Charlotte I.] Quinnipiac Univ, Sch Biol Sci, Hamden, CT 06518 USA. [Lazo-Wasem, Eric A.] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA. RP Moser, WE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Museum Support Ctr MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM moserw@si.edu; Dennis.Richardson@quinnipiac.edu; Charlotte.Hammond@quinnipiac.edu; eric.lazo-wasem@yale.edu NR 43 TC 1 Z9 1 U1 2 U2 7 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118 USA SN 0079-032X EI 2162-4135 J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD OCT PY 2013 VL 54 IS 2 BP 255 EP 262 PG 8 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 238MW UT WOS:000325953000004 ER PT J AU Andrade, TY Thies, W Rogeri, PK Kalko, EKV Mello, MAR AF Andrade, Tiago Y. Thies, Wibke Rogeri, Patricia K. Kalko, Elisabeth K. V. Mello, Marco A. R. TI Hierarchical fruit selection by Neotropical leaf-nosed bats (Chiroptera: Phyllostomidae) SO JOURNAL OF MAMMALOGY LA English DT Article DE diet; foraging; frugivory; mutualism; nestedness; optimal foraging; plant-animal interactions; seed dispersal ID SEED DISPERSAL; CAROLLIA-PERSPICILLATA; ATLANTIC FOREST; RAIN-FOREST; PLANTS; ECHOLOCATION; FRUGIVORY; PATTERNS; DIVERSIFICATION; PIPERACEAE AB It is crucial to understand how Neotropical leaf-nosed bats select fruits, because their choices strongly affect the seed dispersal process, especially of pioneer plants. We tested the hypothesis of hierarchical fruit selection by phyllostomid bats at the levels of the bat genus and species by combining a literature database with field experiments. Considering our database for the whole Neotropics, Artibeus bats focus on Ficus (Moraceae) and Cecropia (Cecropiaceae), Carollia bats on Piper (Piperaceae), and Sturnira bats on Solanum (Solanaceae). Results from a field experiment in Brazil corroborated those preferences, because bats of those 3 genera selected 1st the fruits of their preferred plant genera, even when secondary fruits were offered in higher abundance. In another field experiment in Panama, we observed that 2 sympatric Carollia species, although focusing on the same plant genus, prefer different Piper species. Literature records for the whole range of the 2 Carollia species show that they have strongly nested diets. Our findings corroborate the hypothesis that frugivorous phyllostomids do not forage opportunistically, and, moreover, segregate their diets hierarchically at the genus and species levels. C1 [Andrade, Tiago Y.; Rogeri, Patricia K.] Univ Fed Sao Carlos, Dept Bot, BR-13565905 Sao Paulo, Brazil. [Thies, Wibke; Kalko, Elisabeth K. V.; Mello, Marco A. R.] Univ Ulm, Inst Expt Okol, D-89069 Ulm, Germany. [Rogeri, Patricia K.] Univ Estadual Campinas, Programa Posgrad Ecol, BR-13083970 Campinas, SP, Brazil. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Mello, Marco A. R.] Univ Fed Minas Gerais, Inst Ciencias Biol, Dept Biol Geral, BR-31270901 Belo Horizonte, MG, Brazil. RP Mello, MAR (reprint author), Univ Ulm, Inst Expt Okol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM marmello@gmail.com RI Mello, Marco/B-1095-2008 OI Mello, Marco/0000-0002-9098-9427 FU Sao Paulo Research Foundation [FAPESP 2006/00265-0, 2007/03405-0, 2007/03415-6]; Alexander von Humboldt Foundation [AvH 1134644]; Federal University of Minas Gerais [UFMG 2013/1] FX We thank many colleagues who helped us during the present study, in particular TYA's parents for their support. Our study was funded by the Sao Paulo Research Foundation (FAPESP 2006/00265-0, 2007/03405-0, and 2007/03415-6), the Alexander von Humboldt Foundation (AvH 1134644), and the Federal University of Minas Gerais (UFMG 2013/1). We dedicate our work to the memory of our mentor Elisabeth Kalko, who carried out the project together with us, but passed away before the manuscript was submitted. NR 45 TC 11 Z9 14 U1 2 U2 41 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD OCT PY 2013 VL 94 IS 5 BP 1094 EP 1101 DI 10.1644/12-MAMM-A-244.1 PG 8 WC Zoology SC Zoology GA 238NU UT WOS:000325955500012 ER PT J AU Clough, GW AF Clough, G. Wayne TI Untitled SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD OCT PY 2013 VL 44 IS 6 BP 10 EP 10 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 239GS UT WOS:000326011200009 ER PT J AU Shih, CK Qiao, X Labandeira, CC Dong, R AF Shih ChungKun Qiao Xiao Labandeira, Conrad C. Dong, Ren TI A New Mesopsychid (Mecoptera) from the Middle Jurassic of Northeastern China SO ACTA GEOLOGICA SINICA-ENGLISH EDITION LA English DT Article DE new genus and species; wing coupling; asymmetric wings; taxonomic diversity; Inner Mongolia ID INNER-MONGOLIA; INSECTA; ANGIOSPERMS; POLLINATION; DIPTERA AB The family Mesopsychidae Tillyard, 1917 presently consists of ten described genera from the Early Permian to the Early Cretaceous of Australia, China, Kyrgyzstan, Russia, South Africa, Tajikistan, and Ukraine. Herein, a new genus and a new species of fossil mesopsychid, Epicharmesopsyche pentavenulosa gen. et sp. nov., is described from the Middle Jurassic Jiulongshan Formation of Inner Mongolia, China, supplementing the family-level diversity. The well-preserved, new material reveals many characters, including antennae, wing venation, shape and genitalia that increase our morphological understanding of the family, although unfortunately the mouthparts and most of the legs are not preserved. Diagnosis of the Mesopsychidae is emended to include a four- or five-branched MP in both the fore- and hind wings. This is the first documentation of a wing coupling structure in the Mesopsychidae, consisting of three to four frenula bristles on the humeral lobe at the base of the costal margin of both hind wings. Asymmetrical shape and size of the left and right wings on a specimen of E. pentavenulosa gen. et sp. nov., seems to be a common condition for mesopsychid taxa from northeastern China. C1 [Shih ChungKun; Qiao Xiao; Labandeira, Conrad C.; Dong, Ren] Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. [Labandeira, Conrad C.] Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20013 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Rhodes Univ, Dept Geol, ZA-6140 Grahamstown, South Africa. RP Dong, R (reprint author), Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. EM rendong@mail.cnu.edu.cn FU National Basic Research Program of China (973 Program) [2012CB821906]; National Natural Science Foundation of China [31230065, 31272352, 41272006]; Beijing Municipal Commission of Education [KZ201310028033]; China Geological Survey [1212011120115] FX This research is supported by the National Basic Research Program of China (973 Program) (2012CB821906), National Natural Science Foundation of China (No. 31230065, 31272352, 41272006), Project of Great Wall Scholar and KEY project of Beijing Municipal Commission of Education (grants KZ201310028033), and China Geological Survey (grant 1212011120115). This is contribution 262 of the Evolution of Terrestrial Ecosystems consortium at the National Museum of Natural History in Washington, D.C., U.S.A. NR 39 TC 5 Z9 6 U1 0 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1000-9515 EI 1755-6724 J9 ACTA GEOL SIN-ENGL JI Acta Geol. Sin.-Engl. Ed. PD OCT PY 2013 VL 87 IS 5 BP 1235 EP 1241 DI 10.1111/1755-6724.12124 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 233FB UT WOS:000325550700004 ER PT J AU Olson, SL Levy, C AF Olson, Storrs L. Levy, Catherine TI Eleazar Albin in Don Saltero's coffee-house in 1736: how the Jamaican mango hummingbird got its name, Trochilus mango SO ARCHIVES OF NATURAL HISTORY LA English DT Biographical-Item DE Anthracothorax; Icterus icterus; mango-bird; Oriolus; James Salter; Hans Sloane; Trochilidae; troupial AB The Jamaican hummingbird that Eleazar Albin called the Mango Bird, which was the basis for the Linnean name Trochilus mango, is shown likely to have been based on a specimen he saw in Don Saltero's Coffee-House in Chelsea, London, in 1736, that was probably a gift of Sir Hans Sloane. The name mango-bird has long been in wide use for certain south Asian orioles, especially the Indian Golden Oriole (Oriolus kundoo), at least one specimen and nest of which was also on display in Don Saltero's. Albin's text concerning two species of Jamaican hummingbirds contains numerous dubious or erroneous statements and his use of Mango Bird for the hummingbird was most likely a lapsus confounding another bird he had heard of at Don Saltero's, particularly in light of the fact that the mango tree (Mangifera indica) was not introduced into Jamaica until 1782. Thus, the modern use of the word mango in connection with an entire group of hummingbirds arose through a purely fortuitous mistake and the birds never had any association with the mango tree. C1 [Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds,NHB MRC 116, Washington, DC 20013 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds,NHB MRC 116, POB 37012, Washington, DC 20013 USA. EM olsons@si.edu; bluequit@gmail.com NR 24 TC 0 Z9 0 U1 1 U2 4 PU EDINBURGH UNIV PRESS PI EDINBURGH PA 22 GEORGE SQUARE, EDINBURGH EH8 9LF, MIDLOTHIAN, SCOTLAND SN 0260-9541 EI 1755-6260 J9 ARCH NAT HIST JI Arch. Nat. Hist. PD OCT PY 2013 VL 40 IS 2 BP 340 EP 344 DI 10.3366/anh.2013.0180 PG 5 WC History & Philosophy Of Science; Multidisciplinary Sciences SC History & Philosophy of Science; Science & Technology - Other Topics GA 227VW UT WOS:000325144800013 ER PT J AU Overstreet, LK AF Overstreet, Leslie K. TI Bonelli's record of the demoiselle crane, Grus virgo from Piedmont, Italy SO ARCHIVES OF NATURAL HISTORY LA English DT Article C1 Smithsonian Inst Lib, Washington, DC 20013 USA. RP Overstreet, LK (reprint author), Smithsonian Inst Lib, NHB CE G15 MRC 154,POB 37012, Washington, DC 20013 USA. EM overstreetL@si.edu NR 1 TC 0 Z9 0 U1 0 U2 2 PU EDINBURGH UNIV PRESS PI EDINBURGH PA 22 GEORGE SQUARE, EDINBURGH EH8 9LF, MIDLOTHIAN, SCOTLAND SN 0260-9541 EI 1755-6260 J9 ARCH NAT HIST JI Arch. Nat. Hist. PD OCT PY 2013 VL 40 IS 2 BP 351 EP 354 DI 10.3366/anh.2013.0183 PG 4 WC History & Philosophy Of Science; Multidisciplinary Sciences SC History & Philosophy of Science; Science & Technology - Other Topics GA 227VW UT WOS:000325144800016 ER PT J AU Guzman, HM Gomez, CG Guevara, CA Kleivane, L AF Guzman, Hector M. Gomez, Catalina G. Guevara, Carlos A. Kleivane, Lars TI Potential vessel collisions with Southern Hemisphere humpback whales wintering off Pacific Panama SO MARINE MAMMAL SCIENCE LA English DT Article DE humpback whale; Megaptera novaeangliae; satellite telemetry; nursery area; vessel collision; traffic separation scheme; Gulf of Panama ID MEGAPTERA-NOVAEANGLIAE; WATCHING VESSELS; SHIP STRIKES; MIGRATION; MOVEMENTS; RESPONSES; ATLANTIC; RECORD; WATERS; AREAS AB Vessel collision is a threat to many whale species, and the risk has increased with expanding maritime traffic. This compromises international conservation efforts and requires urgent attention from the world's maritime industry. Humpback whales (Megaptera novaeangliae) are at the top of the death toll, and although Central America is a wintering area for populations from both the Northern and Southern Hemispheres, existing efforts to reduce ship-whale collisions are meager. Herein, we evaluated the potential collisions between vessels and humpback whales wintering off Pacific Panama by following the movements of 15 whales tagged with satellite transmitters and comparing these data with tracks plotted using AIS real-time latitude-longitude points from nearly 1,000 commercial vessels. Movements of whales (adults and calves) in the Gulf of Panama coincide with major commercial maritime routes. AIS vessel data analyzed for individual whale satellite tracks showed that 53% (8 whales) of whales had 98 encounters within 200 m with 81 different vessels in just 11 d. We suggest implementing a 65 nmi Traffic Separation Scheme and a 10 kn maximum speed for vessel routing into the Gulf of Panama during the wintering season. In so doing, the area for potential whale-vessel collisions could be reduced by 93%. C1 [Guzman, Hector M.; Gomez, Catalina G.; Guevara, Carlos A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Kleivane, Lars] Norwegian Def Res Estab FFI, NO-3191 Horten, Norway. RP Guzman, HM (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Ancon, Panama. EM guzmanh@si.edu FU Secretaria Nacional de Ciencia y Tecnologia de Panama (SENACYT); Smithsonian Tropical Research Institute; International Community Foundation; Fundacion MarViva FX We thank Fundacion MarViva, M. Limchin, and A. Aparicio for providing all of the necessary logistics and field support and J. J. Capella for advise on designing and testing the equipment. We thank R. Veale from IHS, Inc. for providing access with limited rights to vessel tracking coordinates. We thank A. S. Friedlander and two anonymous reviewers for valuable comments to early versions of the manuscript. We thank F. Jaen from the Panama Canal Authority for guiding and designing the traffic separation scheme. We thank the Autoridad de Recursos Acuaticos de Panama (ARAP) for providing fishing vessel locations and L. Trejos for providing whale stranding records. We thank the SEATURTLE Organization and the Marine Research Turtle Group for the permission to use the Satellite Tracking and Analysis Tool program. This study was sponsored by the Secretaria Nacional de Ciencia y Tecnologia de Panama (SENACYT), the Smithsonian Tropical Research Institute, the International Community Foundation, and the Fundacion MarViva. This study was conducted under permits issued by the Government of Panama and the Institutional Animal Care and Use Committee of the Smithsonian Tropical Research Institute. NR 43 TC 5 Z9 5 U1 7 U2 40 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 OCT PY 2013 VL 29 IS 4 BP 629 EP 642 DI 10.1111/j.1748-7692.2012.00605.x PG 14 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 232HF UT WOS:000325482800018 ER PT J AU West, KL Sanchez, S Rotstein, D Robertson, KM Dennison, S Levine, G Davis, N Schofield, D Potter, CW Jensen, B AF West, Kristi L. Sanchez, Susan Rotstein, David Robertson, Kelly M. Dennison, Sophie Levine, Gregg Davis, Nicole Schofield, David Potter, Charles W. Jensen, Brenda TI A Longman's beaked whale (Indopacetus pacificus) strands in Maui, Hawaii, with first case of morbillivirus in the central Pacific SO MARINE MAMMAL SCIENCE LA English DT Article ID STENELLA-COERULEOALBA; COMMON DOLPHINS; SITE FIDELITY; INFECTION; OCEAN; DNA; WATERS C1 [West, Kristi L.] Hawaii Pacific Univ, Coll Nat & Computat Sci, Kaneohe, HI 96744 USA. [Sanchez, Susan] Univ Georgia, Dept Infect Dis, Coll Vet Med, Athens, GA 30602 USA. [Robertson, Kelly M.] NOAA, Protected Resources Div, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla, CA 92037 USA. [Dennison, Sophie] Marine Mammal Radiol, San Francisco, CA 94107 USA. [Davis, Nicole; Schofield, David] Natl Marine Fisheries Serv, Pacific Isl Reg Off, Honolulu, HI 96814 USA. [Potter, Charles W.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Jensen, Brenda] Hawaii Pacific Univ, Coll Nat & Computat Sci, Kaneohe, HI 96744 USA. RP West, KL (reprint author), Hawaii Pacific Univ, Coll Nat & Computat Sci, 45-045 Kamehameha Highway, Kaneohe, HI 96744 USA. EM kwest@hpu.edu FU Prescott Grant Program FX We would like to thank Dera Look and Hawaii Stranding Response Network volunteers for their heroic efforts to recover this fresh specimen from Hana. We thank Dr. J. T. Saliki for his leadership, support and advice. We are also grateful to the staff of the Molecular Biology section of the Athens Veterinary Diagnostic lab for their dedication and assistance provided in the identification of this novel virus. We also thank Robin Baird for providing a preliminary species identification of the specimen. We are grateful to Whitney White, Susan Fertall White, and Robert Brownell. W. F. Perrin and Kerri Danil provided helpful comments that improved the manuscript. This work was funded by the Prescott Grant Program. NR 29 TC 15 Z9 15 U1 2 U2 15 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 OCT PY 2013 VL 29 IS 4 BP 767 EP 776 DI 10.1111/j.1748-7692.2012.00616.x PG 10 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 232HF UT WOS:000325482800026 ER PT J AU Sadler, PM Sonnert, G Coyle, HP Cook-Smith, N Miller, JL AF Sadler, Philip M. Sonnert, Gerhard Coyle, Harold P. Cook-Smith, Nancy Miller, Jaimie L. TI The Influence of Teachers' Knowledge on Student Learning in Middle School Physical Science Classrooms SO AMERICAN EDUCATIONAL RESEARCH JOURNAL LA English DT Article DE subject matter knowledge; pedagogical content knowledge; teacher; science education; misconceptions ID SUBJECT-MATTER KNOWLEDGE; PEDAGOGICAL CONTENT KNOWLEDGE; MATHEMATICAL KNOWLEDGE; MULTILEVEL ANALYSIS; ACHIEVEMENT; CONCEPTIONS; EDUCATION; PRECONCEPTIONS; UNDERSTANDINGS; PERFORMANCE AB This study examines the relationship between teacher knowledge and student learning for 9,556 students of 181 middle school physical science teachers. Assessment instruments based on the National Science Education Standards with 20 items in common were administered several times during the school year to both students and their teachers. For items that had a very popular wrong answer, the teachers who could identify this misconception had larger classroom gains, much larger than if the teachers knew only the correct answer. On items on which students did not exhibit misconceptions, teacher subject matter knowledge alone accounted for higher student gains. This finding suggests that a teacher's ability to identify students' most common wrong answer on multiple-choice items, a form of pedagogical content knowledge, is an additional measure of science teacher competence. C1 [Sadler, Philip M.] Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, Cambridge, MA 02138 USA. [Sonnert, Gerhard; Coyle, Harold P.; Cook-Smith, Nancy; Miller, Jaimie L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sadler, PM (reprint author), Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, 60 Garden St, Cambridge, MA 02138 USA. EM psadler@cfa.harvard.edu; gsonnert@cfa.harvard.edu; hcoyle@cfa.harvard.edu; ncook@cfa.harvard.edu; jlmiller@cfa.harvard.edu NR 87 TC 31 Z9 31 U1 8 U2 33 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0002-8312 J9 AM EDUC RES J JI Am. Educ. Res. J. PD OCT PY 2013 VL 50 IS 5 BP 1020 EP 1049 DI 10.3102/0002831213477680 PG 30 WC Education & Educational Research SC Education & Educational Research GA 222WJ UT WOS:000324762500006 ER PT J AU Leslie, HM Goldman, E Mcleod, KL Sievanen, L Balasubramanian, H Cudney-Bueno, R Feuerstein, A Knowlton, N Lee, K Pollnac, R Samhouri, JF AF Leslie, Heather M. Goldman, Erica Mcleod, Karen L. Sievanen, Leila Balasubramanian, Hari Cudney-Bueno, Richard Feuerstein, Amanda Knowlton, Nancy Lee, Kai Pollnac, Richard Samhouri, Jameal F. TI How Good Science and Stories Can Go Hand-In-Hand SO CONSERVATION BIOLOGY LA English DT Article ID GULF-OF-CALIFORNIA; CONSERVATION SCIENCE; ECOSYSTEM SERVICES; BIODIVERSITY C1 [Leslie, Heather M.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Leslie, Heather M.; Sievanen, Leila] Brown Univ, Ctr Environm Studies, Providence, RI 02912 USA. [Goldman, Erica] COMPASS, Silver Spring, MD 20910 USA. [Mcleod, Karen L.] Oregon State Univ, Dept Zool, COMPASS, Corvallis, OR 97331 USA. [Balasubramanian, Hari] Conservat Int, Arlington, VA 22202 USA. [Cudney-Bueno, Richard; Lee, Kai] David & Lucile Packard Fdn, Los Altos, CA 94022 USA. [Feuerstein, Amanda; Knowlton, Nancy] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Pollnac, Richard] Univ Rhode Isl, Dept Marine Affairs, Kingston, RI 02881 USA. [Samhouri, Jameal F.] NOAA, Natl Marine Fisheries Serv, Conservat Biol Div, NW Fisheries Sci Ctr, Seattle, WA 98112 USA. [Balasubramanian, Hari] EcoAdvisors, Halifax, NS B3H 3K6, Canada. RP Leslie, HM (reprint author), Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. EM heather_leslie@brown.edu OI Leslie, Heather/0000-0003-4512-9417 FU Helen R. Whiteley Center at University of Washington's Friday Harbor Laboratories; David and Lucile Packard Foundation FX We acknowledge the hospitality and support of the Helen R. Whiteley Center at University of Washington's Friday Harbor Laboratories, where we first began our conversations on the topic. We also thank O. Aburto, J. Castro, and many others associated with Cabo Pulmo who graciously shared their stories with us (H. L. and L. S.). We thank the editor and two anonymous reviewers for their comments on an earlier version of this manuscript. The workshop was facilitated by COMPASS and funding was provided by The David and Lucile Packard Foundation through grants to J. Lubchenco, S. Levin, and H.L. NR 24 TC 5 Z9 5 U1 7 U2 41 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD OCT PY 2013 VL 27 IS 5 BP 1126 EP 1129 DI 10.1111/cobi.12080 PG 4 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 224ZJ UT WOS:000324931700028 PM 23692176 ER PT J AU Ripperger, SP Tschapka, M Kalko, EKV Rodriguez-Herrera, B Mayer, F AF Ripperger, Simon P. Tschapka, Marco Kalko, Elisabeth K. V. Rodriguez-Herrera, Bernal Mayer, Frieder TI Life in a mosaic landscape: anthropogenic habitat fragmentation affects genetic population structure in a frugivorous bat species SO CONSERVATION GENETICS LA English DT Article DE Dermanura watsoni; Habitat fragmentation; Genetic diversity; Mitochondrial D-loop ID TROPICAL RAIN-FOREST; MITOCHONDRIAL-DNA; PHYLLOSTOMID BATS; ARTIBEUS-WATSONI; AGRICULTURAL LANDSCAPES; COSTA-RICA; DIVERSITY; CONSERVATION; CALIFORNIA; FLOW AB Bats are often considered highly mobile and hence less susceptible to habitat fragmentation than other animals. We tested this basic assumption by studying populations of Dermanura watsoni, a frugivorous phyllostomid bat, inhabiting forest fragments in an agriculturally dominated landscape in northeastern Costa Rica. We used the mitochondrial D-loop DNA-sequence data to examine genetic diversity and population structure. A significant population differentiation (F (ST) = 0.05, p < 0.001) over a geographical scale of approximately 20 km was detected. Genetic diversity within fragments correlated with patch size and the amount of suitable habitat in the surrounding matrix. The composition of the matrix in close proximity to the fragments explained variation in genetic diversity best. However, only habitat parameters measured from 1986 land cover conditions can explain current genetic diversity, and not those from 2001. Our study demonstrates that bats, despite their high mobility, are not secure from genetic erosion in anthropogenically modified landscapes. Population differentiation can occur on a surprisingly small geographic scale and after short time periods. Our findings illustrate the importance of considering several points in time when testing for an influence of habitat parameters as it might be decades until they are reflected by genetic diversity. C1 [Ripperger, Simon P.; Mayer, Frieder] Leibniz Inst Evolut & Biodivers Forsch, Museum Nat Kunde, D-10115 Berlin, Germany. [Ripperger, Simon P.; Tschapka, Marco; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Tschapka, Marco; Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Rodriguez-Herrera, Bernal] Univ Costa Rica, Escuela Biol, San Pedro, Costa Rica. [Rodriguez-Herrera, Bernal] Tirimbina Rainforest Ctr, Heredia, Costa Rica. RP Ripperger, SP (reprint author), Leibniz Inst Evolut & Biodivers Forsch, Museum Nat Kunde, Invalidenstr 43, D-10115 Berlin, Germany. EM simon.ripperger@mfn-berlin.de FU "Deutscher Akademischer Austauschdienst" (DAAD) FX We thank Alberto Quintana of Hacienda Pozo Azul and Giovanna Holbrook of Selva Verde Lodge for the permission to conduct fieldwork. Thanks to all private land owners for granting access to their properties. For assistance in the field we are grateful to Emanuel Rojas, Elder Miranda, and Katrin Heer, to Martina Nagy for help in the laboratory and Mirjam Knornschild for statistical advising. We thank Steven Sesnie for providing the land cover maps. Logistical support was provided by Chiquita Brands International. This work was approved by Javier Guevara (Resolutions: 047-2010-SINAC, 004-2011-SINAC, 128-2011-SINAC). Funding for field work was provided by a grant of the "Deutscher Akademischer Austauschdienst" (DAAD). NR 80 TC 8 Z9 8 U1 3 U2 78 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 J9 CONSERV GENET JI Conserv. Genet. PD OCT PY 2013 VL 14 IS 5 BP 925 EP 934 DI 10.1007/s10592-012-0434-y PG 10 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 227PZ UT WOS:000325127100001 ER PT J AU Brook, RD Cakmak, S Turner, MC Brook, JR Crouse, DL Peters, PA van Donkelaar, A Villeneuve, PJ Brion, O Jerrett, M Martin, RV Rajagopalan, S Goldberg, MS Pope, CA Burnett, RT AF Brook, Robert D. Cakmak, Sabit Turner, Michelle C. Brook, Jeffrey R. Crouse, Dan L. Peters, Paul A. van Donkelaar, Aaron Villeneuve, Paul J. Brion, Orly Jerrett, Michael Martin, Randall V. Rajagopalan, Sanjay Goldberg, Mark S. Pope, C. Arden, III Burnett, Richard T. TI Long-Term Fine Particulate Matter Exposure and Mortality From Diabetes in Canada SO DIABETES CARE LA English DT Article ID AMBIENT AIR-POLLUTION; CARDIOVASCULAR MORTALITY; INSULIN-RESISTANCE; LOS-ANGELES; ASSOCIATION; DISEASE; OBESITY; COHORT; INFLAMMATION; PREVALENCE AB OBJECTIVERecent studies suggest that chronic exposure to air pollution can promote the development of diabetes. However, whether this relationship actually translates into an increased risk of mortality attributable to diabetes is uncertain.RESEARCH DESIGN AND METHODSWe evaluated the association between long-term exposure to ambient fine particulate matter (PM2.5) and diabetes-related mortality in a prospective cohort analysis of 2.1 million adults from the 1991 Canadian census mortality follow-up study. Mortality information, including approximate to 5,200 deaths coded as diabetes being the underlying cause, was ascertained by linkage to the Canadian Mortality Database from 1991 to 2001. Subject-level estimates of long-term exposure to PM2.5 were derived from satellite observations. The hazard ratios (HRs) for diabetes-related mortality were related to PM2.5 and adjusted for individual-level and contextual variables using Cox proportional hazards survival models.RESULTSMean PM2.5 exposure levels for the entire population were low (8.7 mu g/m(3); SD, 3.9 mu g/m(3); interquartile range, 6.2 mu g/m(3)). In fully adjusted models, a 10-mu g/m(3) elevation in PM2.5 exposure was associated with an increase in risk for diabetes-related mortality (HR, 1.49; 95% CI, 1.37-1.62). The monotonic change in risk to the population persisted to PM2.5 concentration <5 mu g/m(3).CONCLUSIONSLong-term exposure to PM2.5, even at low levels, is related to an increased risk of mortality attributable to diabetes. These findings have considerable public health importance given the billions of people exposed to air pollution and the worldwide growing epidemic of diabetes. C1 [Brook, Robert D.] Univ Michigan, Div Cardiovasc Med, Ann Arbor, MI 48109 USA. [Cakmak, Sabit; Crouse, Dan L.; Villeneuve, Paul J.; Brion, Orly; Burnett, Richard T.] Hlth Canada, Ottawa, ON K1A 0L2, Canada. [Turner, Michelle C.; Burnett, Richard T.] Univ Ottawa, McLaughlin Ctr Populat Hlth Risk Assessment, Inst Populat Hlth, Ottawa, ON, Canada. [Brook, Jeffrey R.] Environm Canada, Downsview, ON, Canada. [Brook, Jeffrey R.; Villeneuve, Paul J.] Univ Toronto, Div Occupat & Environm Hlth, Toronto, ON, Canada. [Peters, Paul A.] Stat Canada, Ottawa, ON, Canada. [van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Jerrett, Michael] Univ Calif Berkeley, Environm Hlth Sci Dept, Berkeley, CA 94720 USA. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rajagopalan, Sanjay] Ohio State Univ, Sch Med, Davis Heart Lung Res Inst, Columbus, OH 43210 USA. [Goldberg, Mark S.] McGill Univ, Dept Med, Montreal, PQ, Canada. [Pope, C. Arden, III] Brigham Young Univ, Dept Econ, Provo, UT 84602 USA. RP Brook, RD (reprint author), Univ Michigan, Div Cardiovasc Med, Ann Arbor, MI 48109 USA. EM robdbrok@umich.edu RI Martin, Randall/C-1205-2014; OI Martin, Randall/0000-0003-2632-8402; Cakmak, Sabit/0000-0001-9921-2107; Peters, Paul/0000-0001-5225-2005 FU NIEHS NIH HHS [R01 ES015146] NR 34 TC 49 Z9 51 U1 3 U2 36 PU AMER DIABETES ASSOC PI ALEXANDRIA PA 1701 N BEAUREGARD ST, ALEXANDRIA, VA 22311-1717 USA SN 0149-5992 J9 DIABETES CARE JI Diabetes Care PD OCT PY 2013 VL 36 IS 10 BP 3313 EP 3320 DI 10.2337/dc12-2189 PG 8 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 222RT UT WOS:000324749500078 PM 23780947 ER PT J AU Carlstead, K Mench, JA Meehan, C Brown, JL AF Carlstead, Kathy Mench, Joy A. Meehan, Cheryl Brown, Janine L. TI An Epidemiological Approach to Welfare Research in Zoos: The Elephant Welfare Project SO JOURNAL OF APPLIED ANIMAL WELFARE SCIENCE LA English DT Article DE elephant; welfare; husbandry; management; epidemiology ID FEMALE AFRICAN ELEPHANTS; ANIMAL-WELFARE; LOXODONTA-AFRICANA; POSITIVE PSYCHOLOGY; OVARIAN ACYCLICITY; AQUARIUM RESEARCH; DICEROS-BICORNIS; ASIAN ELEPHANTS; BEHAVIOR; POPULATION AB Multi-institutional studies of welfare have proven to be valuable in zoos but are hampered by limited sample sizes and difficulty in evaluating more than just a few welfare indicators. To more clearly understand how interactions of husbandry factors influence the interrelationships among welfare outcomes, epidemiological approaches are needed as well as multifactorial assessments of welfare. Many questions have been raised about the housing and care of elephants in zoos and whether their environmental and social needs are being met in a manner that promotes good welfare. This article describes the background and rationale for a large-scale study of elephant welfare in North American zoos funded by the (U.S.) Institute of Museum and Library Services. The goals of this project are to document the prevalence of positive and negative welfare states in 291 elephants exhibited in 72 Association of Zoos and Aquariums zoos and then determine the environmental, management, and husbandry factors that impact elephant welfare. This research is the largest scale nonhuman animal welfare project ever undertaken by the zoo community, and the scope of environmental variables and welfare outcomes measured is unprecedented. C1 [Carlstead, Kathy] Honolulu Zoo Soc, Honolulu, HI 96815 USA. [Mench, Joy A.] Univ Calif Davis, Ctr Anim Welf, Davis, CA 95616 USA. [Meehan, Cheryl] Vistalogic Inc, Portland, OR USA. [Brown, Janine L.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. RP Carlstead, K (reprint author), Honolulu Zoo Soc, 151 Kapahulu Ave, Honolulu, HI 96815 USA. EM KCarlstead@honzoosoc.org NR 70 TC 11 Z9 11 U1 23 U2 123 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 1088-8705 J9 J APPL ANIM WELF SCI JI J. Appl. Anim. Welf. Sci. PD OCT 1 PY 2013 VL 16 IS 4 SI SI BP 319 EP 337 DI 10.1080/10888705.2013.827915 PG 19 WC Veterinary Sciences SC Veterinary Sciences GA 226PI UT WOS:000325047900003 PM 24079487 ER PT J AU Boehm, JT Woodall, L Teske, PR Lourie, SA Baldwin, C Waldman, J Hickerson, M AF Boehm, J. T. Woodall, Lucy Teske, Peter R. Lourie, Sara A. Baldwin, Carole Waldman, John Hickerson, Mike TI ORIGINAL ARTICLE Marine dispersal and barriers drive Atlantic seahorse diversification SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Atlantic Ocean; coalescent; demographic history; Hippocampus; marine barriers; ocean currents; rafting; seahorse; Syngnathidae ID APPROXIMATE BAYESIAN COMPUTATION; TROPICAL REEF FISHES; GULF-STREAM; COMPARATIVE PHYLOGEOGRAPHY; HIPPOCAMPUS-ERECTUS; POPULATION HISTORY; MITOCHONDRIAL-DNA; SPECIATION; EVOLUTION; OCEAN AB AimTo investigate how marine barriers shaped the demographic history of Atlantic seahorses (Syngnathidae: Hippocampus). LocationAtlantic Ocean. MethodsRange-wide sampling (n=390) at mitochondrial and up to five nuclear DNA loci was carried out across the Hippocampus erectus species complex (H.erectus from the Caribbean/North America, H.patagonicus from South America and H.hippocampus from Europe and West Africa). Multi-species coalescent and approximate Bayesian computation (ABC) frameworks were used to estimate support of competing biogeographical hypotheses and demographic parameters, including lineage divergence times, effective population sizes and magnitudes of population size change. ResultsWe identified four distinct lineages within the H.erectus complex. A posterior probability of 0.626 and corresponding Bayes factors ranging from 3.68 to 11.38 gave moderate to strong support for a basal divergence between South American populations of H.patagonicus and Caribbean/North American populations of H.erectus coincident with the inter-regional freshwater outflow of the Amazon River Barrier (ARB). Estimates of historical effective population sizes and divergence times indicate that European and West African populations of H.hippocampus expanded after colonization from a more demographically stable Caribbean/North American H.erectus. Main conclusionsOur findings of trans-Atlantic colonization followed by isolation across a deep oceanic divide, and isolation across a freshwater barrier, may demonstrate a contrast in marine divide permeability for this group of rafters. Demographic inference supports the establishment of an ancestral population of the H.erectus complex in the Americas, followed by the ARB splitting it into Caribbean/North and South American lineages at a time of increased sedimentation and outflow. Our estimates suggest that following this split, colonization occurred across the Atlantic via the Gulf Stream currents with subsequent trans-Atlantic isolation. These results illustrate that rafting can be a means of range expansion over large distances, but may be insufficient for sustaining genetic connectivity across major barriers, thereby resulting in lineage divergence. C1 [Boehm, J. T.; Hickerson, Mike] CUNY City Coll, Dept Biol, New York, NY 10031 USA. [Boehm, J. T.; Waldman, John; Hickerson, Mike] CUNY, Grad Ctr, New York, NY 10016 USA. [Woodall, Lucy] Nat Hist Museum, Dept Zool, London SW7 5BD, England. [Teske, Peter R.] Flinders Univ S Australia, Sch Biol Sci, Mol Ecol Lab, Adelaide, SA 5001, Australia. [Lourie, Sara A.] McGill Univ, Redpath Museum, Montreal, PQ H3A 2K6, Canada. [Baldwin, Carole] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Waldman, John] CUNY Queens Coll, Dept Biol, Flushing, NY 11367 USA. RP Boehm, JT (reprint author), CUNY City Coll, Dept Biol, Marshak Sci Bldg,J-526,160 Convent Ave, New York, NY 10031 USA. EM jtboehmjr@gmail.com FU National Science Foundation [40C33-00-01] FX We thank the Sackler Institute for Comparative Genomics (AMNH) and R. DeSalle for providing laboratory space, support, assistance and the collection of sequence data; the National Science Foundation (40C33-00-01) for supporting the dissertational research of J.T.B.; D. Luzzatto for data and discussion on H. patagonicus; N. Dunham (Florida Fish and Wildlife Conservation Commission), T. Tuckey (Virginia Institute of Marine Science), T. Gardner (Atlantis Aquarium), The River Project (Pier 40, Manhattan) and T. M. Grothues (Rutgers University) for help with fish collections and for providing samples. Lastly, we thank T. Demos, K. Ilves, L. Rocha and three anonymous referees for providing valuable feedback that improved the manuscript. NR 73 TC 11 Z9 12 U1 7 U2 67 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD OCT PY 2013 VL 40 IS 10 BP 1839 EP 1849 DI 10.1111/jbi.12127 PG 11 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 226JE UT WOS:000325030900003 ER PT J AU Canning, REA Sun, M Sanders, JS Clarke, TE Fabian, AC Giacintucci, S Lal, DV Werner, N Allen, SW Donahue, M Edge, AC Johnstone, RM Nulsen, PEJ Salome, P Sarazin, CL AF Canning, R. E. A. Sun, M. Sanders, J. S. Clarke, T. E. Fabian, A. C. Giacintucci, S. Lal, D. V. Werner, N. Allen, S. W. Donahue, M. Edge, A. C. Johnstone, R. M. Nulsen, P. E. J. Salome, P. Sarazin, C. L. TI A multiwavelength view of cooling versus AGN heating in the X-ray luminous cool-core of Abell 3581 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: clusters: intracluster medium; Galaxies: groups: individual: Abell 3581; galaxies: ISM ID BRIGHTEST CLUSTER GALAXIES; ACTIVE GALACTIC NUCLEI; MOLECULAR-HYDROGEN EMISSION; INTEGRAL FIELD SPECTROSCOPY; PERSEUS CLUSTER; STAR-FORMATION; CHANDRA OBSERVATION; 2A 0335+096; NGC 1275; TELESCOPE OBSERVATIONS AB We report the results of a multiwavelength study of the nearby galaxy group, Abell 3581 (z = 0.0218). This system hosts the most luminous cool core of any nearby group and exhibits active radio mode feedback from the supermassive black hole in its brightest group galaxy, IC 4374. The brightest galaxy has suffered multiple active galactic nucleus outbursts, blowing bubbles into the surrounding hot gas, which have resulted in the uplift of cool ionized gas into the surrounding hot intragroup medium. High velocities, indicative of an outflow, are observed close to the nucleus and coincident with the radio jet. Thin dusty filaments accompany the uplifted, ionized gas. No extended star formation is observed; however, a young cluster is detected just north of the nucleus. The direction of rise of the bubbles has changed between outbursts. This directional change is likely due to sloshing motions of the intragroup medium. These sloshing motions also appear to be actively stripping the X-ray cool core, as indicated by a spiralling cold front of high-metallicity, low-temperature, low entropy gas. C1 [Canning, R. E. A.; Werner, N.; Allen, S. W.] Stanford Univ, KIPAC, Stanford, CA 94305 USA. [Canning, R. E. A.; Werner, N.; Allen, S. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Sun, M.] Eureka Sci Inc, Oakland, CA 94602 USA. [Sanders, J. S.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. [Clarke, T. E.] Naval Res Lab, Washington, DC 20375 USA. [Fabian, A. C.; Johnstone, R. M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Giacintucci, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Giacintucci, S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Lal, D. V.] Natl Ctr Radio Astrophys NCRA TIFR, Pune 411007, Maharashtra, India. [Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Donahue, M.] Michigan State Univ, E Lansing, MI 48824 USA. [Edge, A. C.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Salome, P.] Observ Paris, LERMA, F-75014 Paris, France. [Salome, P.] Observ Paris, CNRS UMR8112, F-75014 Paris, France. [Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Canning, REA (reprint author), Stanford Univ, KIPAC, 452 Lomita Mall, Stanford, CA 94305 USA. EM rcanning@stanford.edu OI Edge, Alastair/0000-0002-3398-6916; Sanders, Jeremy/0000-0003-2189-4501; Nulsen, Paul/0000-0003-0297-4493 FU NASA issued by JPL/Caltech [1428053]; Cambridge Philosophical Society; Royal Astronomical Society; NASA [GO1-12103A, NNH12CG03C, HST-GO-12373, PF0-110071, NAS8-03060, G01-12169X]; National Aeronautics and Space Administration [GO1-12159Z]; 6.1 Base; Chandra X-ray Center (CXC); US Department of Energy [DE-AC02-76SF00515] FX Support for this work was provided by NASA through award number 1428053 issued by JPL/Caltech. REAC acknowledges a scholarship from the Cambridge Philosophical Society and a Royal Astronomical Society grant. MS is supported by the NASA grants GO1-12103A, NNH12CG03C and HST-GO-12373. TEC was supported in part for this work by the National Aeronautics and Space Administration, through Chandra Award Number GO1-12159Z. Basic research in radio astronomy at the Naval Research Laboratory is supported by 6.1 Base funding. SG acknowledges the support of NASA through Einstein Postdoctoral Fellowship PF0-110071 awarded by the Chandra X-ray Center (CXC), which is operated by SAO. SWA acknowledges support from the US Department of Energy under contract number DE-AC02-76SF00515. PEJN was supported by NASA contract NAS8-03060. CLS was supported in part by NASA Chandra Grant G01-12169X. REAC would also like to thank Anja von der Linden and Adam Mantz for interesting and enlightening discussions. 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 109 TC 11 Z9 11 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 OCT PY 2013 VL 435 IS 2 BP 1108 EP 1125 DI 10.1093/mnras/stt1345 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229KY UT WOS:000325264600017 ER PT J AU Genel, S Vogelsberger, M Nelson, D Sijacki, D Springel, V Hernquist, L AF Genel, Shy Vogelsberger, Mark Nelson, Dylan Sijacki, Debora Springel, Volker Hernquist, Lars TI Following the flow: tracer particles in astrophysical fluid simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; turbulence; methods: numerical; methods: statistical; galaxies: formation; cosmology: theory ID MOVING-MESH COSMOLOGY; GALAXY FORMATION; NUMERICAL SIMULATIONS; HYDRODYNAMICS; TURBULENCE; GAS; NUCLEOSYNTHESIS; ALGORITHM; HALOES; COMPUTATION AB We present two numerical schemes for passive tracer particles in the hydrodynamical moving-mesh code arepo, and compare their performance for various problems, from simple set-ups to cosmological simulations. The purpose of tracer particles is to allow the flow to be followed in a Lagrangian way, tracing the evolution of the fluid with time, and allowing the thermodynamical history of individual fluid parcels to be recorded. We find that the commonly used 'velocity field tracers', which are advected using the fluid velocity field, do not in general follow the mass flow correctly, and explain why this is the case. This method can result in order-of-magnitude biases in simulations of driven turbulence and in cosmological simulations, rendering the velocity field tracers inappropriate for following these flows. We then discuss a novel implementation of 'Monte Carlo tracers', which are moved along with fluid cells and are exchanged probabilistically between them following the mass flux. This method reproduces the mass distribution of the fluid correctly. The main limitation of this approach is that it is more diffusive than the fluid itself. Nonetheless, we show that this novel approach is more reliable than that has been employed previously and demonstrate that it is appropriate for following hydrodynamical flows in mesh-based codes. The Monte Carlo tracers can also naturally be transferred between fluid cells and other types of particles, such as stellar particles, so that the mass flow in cosmological simulations can be followed in its entirety. C1 [Genel, Shy; Vogelsberger, Mark; Nelson, Dylan; Sijacki, Debora; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sijacki, Debora] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sijacki, Debora] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, Zentrum Astron, ARI, D-69120 Heidelberg, Germany. RP Genel, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sgenel@cfa.harvard.edu OI Genel, Shy/0000-0002-3185-1540 FU European Research Council under ERC-StG [EXAGAL-308037] FX The simulations described in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. We thank Tom Abel, Andreas Bauer, Christoph Federrath, Ralf Klessen, Diego Munoz, Rudiger Pakmor, Paul Torrey and Franco Vazza for useful discussions. VS acknowledges support from the European Research Council under ERC-StG grant EXAGAL-308037. NR 57 TC 30 Z9 30 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2013 VL 435 IS 2 BP 1426 EP 1442 DI 10.1093/mnras/stt1383 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229KY UT WOS:000325264600036 ER PT J AU Knebe, A Pearce, FR Lux, H Ascasibar, Y Behroozi, P Casado, J Moran, CC Diemand, J Dolag, K Dominguez-Tenreiro, R Elahi, P Falck, B Gottlober, S Han, JX Klypin, A Lukic, Z Maciejewski, M McBride, CK Merchan, ME Muldrew, SI Neyrinck, M Onions, J Planelles, S Potter, D Quilis, V Rasera, Y Ricker, PM Roy, F Ruiz, AN Sgro, MA Springel, V Stadel, J Sutter, PM Tweed, D Zemp, M AF Knebe, Alexander Pearce, Frazer R. Lux, Hanni Ascasibar, Yago Behroozi, Peter Casado, Javier Moran, Christine Corbett Diemand, Juerg Dolag, Klaus Dominguez-Tenreiro, Rosa Elahi, Pascal Falck, Bridget Gottloeber, Stefan Han, Jiaxin Klypin, Anatoly Lukic, Zarija Maciejewski, Michal McBride, Cameron K. Merchan, Manuel E. Muldrew, Stuart I. Neyrinck, Mark Onions, Julian Planelles, Susana Potter, Doug Quilis, Vicent Rasera, Yann Ricker, Paul M. Roy, Fabrice Ruiz, Andres N. Sgro, Mario A. Springel, Volker Stadel, Joachim Sutter, P. M. Tweed, Dylan Zemp, Marcel TI Structure finding in cosmological simulations: the state of affairs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: haloes; galaxies: luminosity function; mass function; galaxies: statistics; cosmology: theory; dark matter ID DARK-MATTER HALOES; N-BODY SIMULATIONS; LAMBDA-CDM COSMOLOGY; MILKY-WAY SATELLITES; GAUSSIAN INITIAL CONDITIONS; PRIMORDIAL NON-GAUSSIANITY; FINDER COMPARISON PROJECT; DIGITAL SKY SURVEY; ADAPTIVE MESH REFINEMENT; SAGITTARIUS DWARF GALAXY AB The ever increasing size and complexity of data coming from simulations of cosmic structure formation demand equally sophisticated tools for their analysis. During the past decade, the art of object finding in these simulations has hence developed into an important discipline itself. A multitude of codes based upon a huge variety of methods and techniques have been spawned yet the question remained as to whether or not they will provide the same (physical) information about the structures of interest. Here we summarize and extent previous work of the 'halo finder comparison project': we investigate in detail the (possible) origin of any deviations across finders. To this extent, we decipher and discuss differences in halo-finding methods, clearly separating them from the disparity in definitions of halo properties. We observe that different codes not only find different numbers of objects leading to a scatter of up to 20 per cent in the halo mass and V-max function, but also that the particulars of those objects that are identified by all finders differ. The strength of the variation, however, depends on the property studied, e.g. the scatter in position, bulk velocity, mass and the peak value of the rotation curve is practically below a few per cent, whereas derived quantities such as spin and shape show larger deviations. Our study indicates that the prime contribution to differences in halo properties across codes stems from the distinct particle collection methods and - to a minor extent - the particular aspects of how the procedure for removing unbound particles is implemented. We close with a discussion of the relevance and implications of the scatter across different codes for other fields such as semi-analytical galaxy formation models, gravitational lensing and observables in general. C1 [Knebe, Alexander; Ascasibar, Yago; Casado, Javier; Dominguez-Tenreiro, Rosa] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, E-28049 Madrid, Spain. [Pearce, Frazer R.; Lux, Hanni; Elahi, Pascal; Muldrew, Stuart I.; Onions, Julian] Univ Nottingham, Sch Phys Astron, Nottingham NG7 2RD, England. [Lux, Hanni] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Behroozi, Peter] Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. [Behroozi, Peter] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Behroozi, Peter] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Moran, Christine Corbett; Diemand, Juerg; Potter, Doug; Stadel, Joachim] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland. [Dolag, Klaus; Maciejewski, Michal] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Dolag, Klaus] Univ Observ Munchen, D-81679 Munich, Germany. [Elahi, Pascal; Han, Jiaxin] Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Falck, Bridget] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Gottloeber, Stefan] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Han, Jiaxin] Chinese Acad Sci, Grad Sch, Beijing 100039, Peoples R China. [Han, Jiaxin] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Klypin, Anatoly] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Lukic, Zarija] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94610 USA. [Lukic, Zarija] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87544 USA. [McBride, Cameron K.] Vanderbilt Univ, Stevenson Ctr 6301, Dept Phys & Astron, Nashville, TN 37235 USA. [McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Merchan, Manuel E.; Ruiz, Andres N.; Sgro, Mario A.] UNC, CONICET, CCT Cordoba, Inst Astron Teor & Expt, Cordoba, Argentina. [Neyrinck, Mark] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Planelles, Susana] Univ Trieste, Dept Phys, Astron Unit, I-34131 Trieste, Italy. [Planelles, Susana] INAF, Osservatorio Astron Trieste, I-34131 Trieste, Italy. [Quilis, Vicent] Univ Valencia, Dept Astron & Astrofis, E-46100 Burjassot, Valencia, Spain. [Rasera, Yann; Roy, Fabrice] Univ Paris Diderot, Observ Paris, UMR CNRS 8102, CNRS,LUTh, F-92190 Meudon, France. [Ricker, Paul M.; Sutter, P. M.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Ricker, Paul M.; Sutter, P. M.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, Zentrum Astron, D-69120 Heidelberg, Germany. [Sutter, P. M.] Univ Paris 06, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Sutter, P. M.] CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Sutter, P. M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Tweed, Dylan] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Zemp, Marcel] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. RP Knebe, A (reprint author), Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, Modulo 15, E-28049 Madrid, Spain. EM alexander.knebe@uam.es RI Diemand, Juerg/G-9448-2011; Knebe, Alexander/N-1815-2014; Quilis, Vicent/E-8409-2016; OI Knebe, Alexander/0000-0003-4066-8307; Quilis, Vicent/0000-0002-2852-5031; Onions, Julian/0000-0001-5192-6856; Pearce, Frazer/0000-0002-2383-9250; Zemp, Marcel/0000-0002-0498-3812; Ascasibar Sequeiros, Yago/0000-0003-1577-2479 FU European Commission's Framework Programme 7, through the Marie Curie Initial Training Network CosmoComp [PITN-GA-2009-238356]; ASTROSIM network of the European Science Foundation [2910]; Spanish Ministerio de Ciencia e Innovacion (MICINN) in Spain through the Ramon y Cajal programme; ASTROMADRID network [AYA 2009-13875-C03-02, AYA2009-12792-C03-03, CSD2009-00064, CAM S2009/ESP-1496]; Ministerio de Econom'a y Competitividad (MINECO) [AYA2012-31101]; European Commissions Framework Programme 7, through the Marie Curie Initial Training Network CosmoComp [PITN-GA-2009-238356]; MICINN (Spain) [AYA2010-21887-C04-03]; Ramon y Cajal programme [RyC-2011-09461]; NASA HST Theory Grant [HST-AR-12159.01-A]; US Department of Energy [DE-AC02-76SF00515]; MICINN/MINECO (Spain) from the PNAyA [AYA2009-12792-C03-03]; MICINN (Spain) from the PNAyA [AYA2009-12792-C03-03]; regional Madrid V PRICIT programme through the ASTROMADRID network [CAM S2009/ESP-1496]; 'Supercomputacion y e-Ciencia' Consolider-Ingenio project [CSD2007-0050]; Gordon and Betty Moore Foundation; STFC [ST/H002774/1, ST/K0090X/1]; STFC Studentship Enhancement Programme (STEP); PRIN-INAF09 project; Spanish MINECO [AYA2010-21322-C03-01]; 985 grant from Peking University; National Science Foundation of China [11250110052] FX This paper was initiated at the Subhaloes going Notts workshop in Dovedale, UK, which was funded by the European Commission's Framework Programme 7, through the Marie Curie Initial Training Network CosmoComp (PITN-GA-2009-238356). It also uses data and results from the first halo finder comparison workshop 'Haloes going MAD' in Madrid, Spain, which was funded by the ASTROSIM network of the European Science Foundation (Science Meeting 2910).; AK is supported by the Spanish Ministerio de Ciencia e Innovacion (MICINN) in Spain through the Ramon y Cajal programme as well as the grants AYA 2009-13875-C03-02, AYA2009-12792-C03-03, CSD2009-00064 and CAM S2009/ESP-1496 (from the ASTROMADRID network), and the Ministerio de Econom'a y Competitividad (MINECO) through grant AYA2012-31101. He further thanks Calexico for tres avisos.; HL acknowledges a fellowship from the European Commissions Framework Programme 7, through the Marie Curie Initial Training Network CosmoComp (PITN-GA-2009-238356).; YA receives financial support from project AYA2010-21887-C04-03 from the MICINN (Spain), as well as the Ramon y Cajal programme (RyC-2011-09461), now managed by the MINECO (fiercely cutting back on the Spanish scientific infrastructure).; PB received support from NASA HST Theory Grant HST-AR-12159.01-A and was additionally supported by the US Department of Energy under contract number DE-AC02-76SF00515.; JC is supported by a contract from MICINN/MINECO (Spain) through the grant AYA2009-12792-C03-03 from the PNAyA.; RDT is supported by the MICINN (Spain) through the grant AYA2009-12792-C03-03 from the PNAyA, as well as by the regional Madrid V PRICIT programme through the ASTROMADRID network (CAM S2009/ESP-1496) and the 'Supercomputacion y e-Ciencia' Consolider-Ingenio CSD2007-0050 project. She also thanks the computer resources provided by BSC/RES (Spain) and the Centro de Computacion Cientifica (UAM, Spain).; BF acknowledges support from the Gordon and Betty Moore Foundation and the STFC grants ST/H002774/1 and ST/K0090X/1.; SIM acknowledges the support of the STFC Studentship Enhancement Programme (STEP).; SP also acknowledges a fellowship from the European Commission's Framework Programme 7, through the Marie Curie Initial Training Network CosmoComp (PITN-GA-2009-238356) as well as from the PRIN-INAF09 project 'Towards an Italian Network for Computational Cosmology'. SP and VQ thank partial financial support from Spanish MINECO (grant AYA2010-21322-C03-01).; MZ is supported by a 985 grant from Peking University and the International Young Scientist grant 11250110052 by the National Science Foundation of China. NR 304 TC 58 Z9 58 U1 1 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2013 VL 435 IS 2 BP 1618 EP 1658 DI 10.1093/mnras/stt1403 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229KY UT WOS:000325264600053 ER PT J AU Williams, JP Cieza, LA Andrews, SM Coulson, IM Barger, AJ Casey, CM Chen, CC Cowie, LL Koss, M Lee, N Sanders, DB AF Williams, Jonathan P. Cieza, Lucas A. Andrews, Sean M. Coulson, Iain M. Barger, Amy J. Casey, Caitlin M. Chen, Chian-Chou Cowie, Lennox L. Koss, Michael Lee, Nicholas Sanders, David B. TI A SCUBA-2 850-mu m survey of protoplanetary discs in the Sigma Orionis cluster SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE protoplanetary discs; submillimetre: stars ID CIRCUMSTELLAR DUST DISKS; GIANT PLANET FORMATION; UPPER SCORPIUS; STAR-FORMATION; TAURUS-AURIGA; HIGH-REDSHIFT; SOLAR-SYSTEM; MASS STARS; MU-M; EVOLUTION AB We present the results from a large m survey of the Sigma Orionis cluster using the SCUBA-2 camera on the James Clerk Maxwell Telescope. The 05 diameter circular region we surveyed contains 297 young stellar objects with an age estimated at about 3 Myr. We detect nine of these objects, eight of which have infrared excesses from an inner disc. We also serendipitously detect three non-stellar sources at > 5 Sigma that are likely background submillimetre galaxies. The nine detected stars have inferred disc masses ranging from 5 to about 17 M-Jup, assuming similar dust properties as Taurus discs and an interstellar medium gas-to-dust ratio of 100. There is a net positive signal towards the positions of the individually undetected infrared excess sources indicating a mean disc mass of 0.5 M-Jup. Stacking the emission towards those stars without infrared excesses constrains their mean disc mass to less than 0.3 M-Jup, or an equivalent Earth mass in dust. The submillimetre luminosity distribution is significantly different from that in the younger Taurus region, indicating disc mass evolution as star-forming regions age and the infrared excess fraction decreases. Submillimetre Array observations reveal CO emission towards four sources demonstrating that some, but probably not much, molecular gas remains in these relatively evolved discs. These observations provide new constraints on the dust and gas mass of protoplanetary discs during the giant planet building phase and provide a reference level for future studies of disc evolution. C1 [Williams, Jonathan P.; Cieza, Lucas A.; Barger, Amy J.; Casey, Caitlin M.; Chen, Chian-Chou; Cowie, Lennox L.; Koss, Michael; Lee, Nicholas; Sanders, David B.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Cieza, Lucas A.] Univ Diego Portales, Fac Ingn, Santiago, Chile. [Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Coulson, Iain M.] Joint Astron Ctr, Hilo, HI 96720 USA. [Barger, Amy J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Barger, Amy J.] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 USA. RP Williams, JP (reprint author), Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. EM jpw@ifa.hawaii.edu RI Koss, Michael/B-1585-2015; OI Koss, Michael/0000-0002-7998-9581; Williams, Jonathan/0000-0001-5058-695X FU NSF [AST-1208911]; Canada Foundation for Innovation; Smithsonian Institution; Academia Sinica; NASA; NSF FX This work is supported by funding from the NSF through grant AST-1208911. We thank Remo Tilanus for advice with the data reduction and the referee, Jane Greaves, for her comments. Jose Cabellero provided helpful notes on individual sources while this paper was in proof and pointed out that the apparent Class I source that we failed to detect with SCUBA-2 is not a cluster member but rather a background galaxy. The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the Netherlands Organisation for Scientific Research, and the National Research Council of Canada. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. The Submillimetre Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France and the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and NSF. NR 46 TC 14 Z9 14 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2013 VL 435 IS 2 BP 1671 EP 1679 DI 10.1093/mnras/stt1407 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 229KY UT WOS:000325264600055 ER PT J AU Brugler, MR Opresko, DM France, SC AF Brugler, Mercer R. Opresko, Dennis M. France, Scott C. TI The evolutionary history of the order Antipatharia (Cnidaria: Anthozoa: Hexacorallia) as inferred from mitochondrial and nuclear DNA: implications for black coral taxonomy and systematics SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE Antipathes griggi; COI barcode; deep sea; genetic variation; group I intron; illustrated key; intergenic region; morphological plasticity; Sibopathes; Stichopathes ID LONG-BRANCH ATTRACTION; BAYESIAN PHYLOGENETIC INFERENCE; SPECIES COMPLEX CNIDARIA; SUBUNIT RIBOSOMAL-RNA; DEEP-SEA OCTOCORALS; CHAIN MONTE-CARLO; PHYLUM CNIDARIA; NEW-ZEALAND; SCLERACTINIAN CORALS; MOLECULAR EVOLUTION AB Although black corals inhabit all the world's oceans, they have been relatively understudied as approximate to 185 of 247 species occur at depths >50m. Antipatharians have been included in several phylogenetic studies; however, sample sizes are small and taxonomic coverage minimal. Low levels of mitochondrial (mt) sequence divergence within Scleractinia and Octocorallia are assumed to apply to all anthozoans, although no formal study has been conducted on the order Antipatharia. To quantify genetic variation in the black coral mitogenome, we analysed DNA sequences of the two longest intergenic regions (IGRs) and cox3-cox1 for 26 of 41 genera, representing all families and subfamilies. We also quantified divergence at the intraspecific level using six mtIGRs and their flanking protein-coding genes and rRNA for 100+ colonies of Antipathes griggi. Utilizing sequence data from the two mtIGRs, cox3-cox1, as well as nuclear 18S and 28S, we constructed the first multi-locus phylogenies of the Antipatharia. Reconstructions revealed that species in the genus Stichopathes are split across two families, Sibopathes macrospina groups among North Atlantic Parantipathes (suggesting the actinopharynx and mesenteries were secondarily lost), and three families are polyphyletic. These and other results provide novel, independent insights into the evolutionary history of antipatharians and support placement of species into higher-level groupings based on microscopic skeletal features rather than gross colony morphology. An illustrated key to the seven currently recognized families is also provided.(c) 2013 The Linnean Society of London C1 [Brugler, Mercer R.; France, Scott C.] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. [Opresko, Dennis M.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. RP Brugler, MR (reprint author), Amer Museum Nat Hist, Sackler Inst Comparat Genom, Div Invertebrate Zool, Cent Pk West 79th St, New York, NY 10024 USA. EM mbrugler@amnh.org FU NOAA OE [NA03OAR4600-108/-110, NA04OAR46000-51/-71, UAF-040118]; New Zealand Foundation for Research, Science and Technology [C01X0224]; Ministry of Fisheries [ZBD2004-01)]; State of Louisiana Board of Regents Support Fund Fellowship [LEQSF[2004-09]-GF-21]; UL Lafayette; NOAA's Ocean Explorer Program [NA03OAR4600116, NA05OAR4601061]; Cnidarian Tree of Life Working Group (NSF) [EF-0531570, EF-0531779]; NSF's Ocean Sciences Division-Biological Oceanography Program [OCE-0624601]; NOAA/NMFS Auke Bay Laboratory [NFFS7400-5-00022]; NOAA's National Undersea Research Program [NA05OAR4301001, NA66RU0186]; Hawaii Department of Natural Resources FX M.R.B. would like to thank: Drs Joseph Neigel, Michael Hellberg, and Suzanne Fredericq for their support, instruction, and guidance with this project; Mary Alice Manning, Lance Renoux, Jana Thoma, Eric Pante, Esprit Heestand, and Joris van der Ham for their assistance in the laboratory; Dr Stephen Cairns for providing specimens from the Smithsonian's National Museum of Natural History; Emma Hickerson for inviting M.R.B. and D.M.O. to participate on a cruise to the Flower Garden Banks National Marine Sanctuary (permit number FGBNMS-2004-001); Tina Molodtsova for providing SEM photos of the spines for the type of S. dissimilis; Tony Montgomery (Hawaii Department of Land and Natural Resources) for collecting Antipathes griggi and other species from the Hawaiian Islands; and, for providing samples, Bob Stone (NOAA Fisheries Auke Bay Lab, Alaska), Darryl Felder (UL Lafayette), MBARI and NOAA's Monterey Bay National Marine Sanctuary (PI's David Clague, Jim Barry, Andrew Devogelaere and research technician Lonny Lundsten, funded by NOAA OE), and Amy Baco-Taylor (grant nos. NA03OAR4600-108/-110, NA04OAR46000-51/-71, UAF-040118). Samples were also supplied by the National Institute of Water and Atmospheric Research (NIWA) Invertebrate Collection [specific research programme: 'Seamounts: their importance to fisheries and marine ecosystems', undertaken by the NIWA and funded by the former New Zealand Foundation for Research, Science and Technology (contract C01X0224) and the former Ministry of Fisheries (project no. ZBD2004-01)]. We are indebted to the crews of the R/V Ronald H. Brown and IFE ROVs Argus and Hercules, and our colleagues on the NOAA-OE Deep Atlantic Stepping Stones 2005 cruise for their assistance at sea. M. R. B. was supported by a State of Louisiana Board of Regents Support Fund Fellowship (contract no. LEQSF[2004-09]-GF-21) and funding from UL Lafayette. This research was also supported in part by funding to S.C.F. from NOAA's Ocean Explorer Program (grant nos. NA03OAR4600116, NA05OAR4601061), the Cnidarian Tree of Life Working Group (NSF grants EF-0531570 to C. S. McFadden and EF-0531779 to P. Cartwright), NSF's Ocean Sciences Division-Biological Oceanography Program (OCE-0624601), NOAA/NMFS Auke Bay Laboratory (NFFS7400-5-00022), NOAA's National Undersea Research Program (NA05OAR4301001, NA66RU0186), and the Hawaii Department of Natural Resources. NR 197 TC 9 Z9 9 U1 10 U2 43 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 OCT PY 2013 VL 169 IS 2 BP 312 EP 361 DI 10.1111/zoj.12060 PG 50 WC Zoology SC Zoology GA 226FC UT WOS:000325019000002 ER PT J AU Fabre, PH Pages, M Musser, GG Fitriana, YS Fjeldsa, J Jennings, A Jonsson, KA Kennedy, J Michaux, J Semiadi, G Supriatna, N Helgen, KM AF Fabre, Pierre-Henri Pages, Marie Musser, Guy G. Fitriana, Yuli S. Fjeldsa, Jon Jennings, Andy Jonsson, Knud A. Kennedy, Jonathan Michaux, Johan Semiadi, Gono Supriatna, Nanang Helgen, Kristofer M. TI A new genus of rodent from Wallacea (Rodentia: Muridae: Murinae: Rattini), and its implication for biogeography and Indo-Pacific Rattini systematics SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE biodiversity; biogeography; Indo-Pacific; molecular systematics; morphology; Rattini; Wallacea ID MAXIMUM-LIKELIHOOD; MUROID RODENTS; PHYLOGENETIC-RELATIONSHIPS; EVOLUTIONARY HISTORY; MITOCHONDRIAL-DNA; SOFTWARE PACKAGE; GEOGRAPHIC RANGE; DIVERGENCE TIMES; ENDEMIC RODENTS; NUCLEAR GENES AB We describe Halmaheramys bokimekot Fabre, Pages, Musser, Fitriana, Semiadi & Helgengen.etsp.nov., a new genus and species of murine rodent from the North Moluccas, and study its phylogenetic placement using both molecular and morphological data. We generated a densely sampled mitochondrial and nuclear DNA data set that included most genera of Indo-Pacific Murinae, and used probabilistic methodologies to infer their phylogenetic relationships. To reconstruct their biogeographical history, we first dated the topology and then used a Lagrange analysis to infer ancestral geographic areas. Finally, we combined the ancestral area reconstructions with temporal information to compare patterns of murine colonization among Indo-Pacific archipelagos. We provide a new and comprehensive molecular phylogenetic reconstruction for Indo-Pacific Murinae, with a focus on the Rattus division. Using previous results and those presented in this study, we define a new Indo-Pacific group within the Rattus division, composed of Bullimus, Bunomys, Paruromys, Halmaheramys, Sundamys, and Taeromys. Our phylogenetic reconstructions revealed a relatively recent diversification from the Middle Miocene to Plio-Pleistocene associated with several major dispersal events. We identified two independent Indo-Pacific dispersal events from both western and eastern Indo-Pacific archipelagos to the isolated island of Halmahera, which led to the speciations of H.bokimekotgen.etsp.nov. and Rattus morotaiensis Kellogg, 1945. We propose that a Middle Miocene collision between the Halmahera and Sangihe arcs may have been responsible for the arrival of the ancestor of Halmaheramys to eastern Wallacea. Halmaheramys bokimekotgen. et sp.nov. is described in detail, and its systematics and biogeography are documented and illustrated.(c) 2013 The Linnean Society of London C1 [Fabre, Pierre-Henri; Fjeldsa, Jon; Jonsson, Knud A.; Kennedy, Jonathan] Univ Copenhagen, CMEC, Dept Biol, Zool Museum, DK-2100 Copenhagen, Denmark. [Pages, Marie] Univ Liege, Lab Genet Microorganismes, B-4000 Liege, Belgium. [Pages, Marie; Michaux, Johan] UMR CBGP INRA IRD Cirad Montpellier SupAgro, INRA, F-34988 Montferrier Sur Lez, France. [Musser, Guy G.] Amer Museum Nat Hist, Div Vertebrate Zool Mammal, New York, NY 10024 USA. [Fitriana, Yuli S.; Semiadi, Gono; Supriatna, Nanang] Indonesian Inst Sci LIPI, Museum Zool Bogoriense, Biol Res Ctr, Cibinong 16911, Indonesia. [Jennings, Andy] Museum Natl Hist Nat, Dept Systemat & Evolut, F-75231 Paris, France. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Fabre, PH (reprint author), Univ Copenhagen, CMEC, Dept Biol, Zool Museum, Univ Pk 15, DK-2100 Copenhagen, Denmark. EM phfmourade@gmail.com RI Fjeldsa, Jon/A-9699-2013; Pages, Marie/J-9003-2015; publist, CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017; OI Fjeldsa, Jon/0000-0003-0790-3600; SEMIADI, Gono/0000-0002-9351-9746; Jonsson, Knud/0000-0002-1875-9504 FU Danish National Research Foundation; National Geographic Society Research and Exploration Grant [8853-10]; National Geographic Society; Dybron Hoffs Foundation; FRS-FNRS fellowship (Belgian Fund for Scientific Research); SYNTHESYS Foundation [GB-TAF-2735]; Celebes Fund; Archbold Expeditions; American Museum of Natural History; Lembaga Ilmu Pengetahuan Indonesia (LIPI); Museum Zoologicum Bogoriense (MZB) in Indonesia; network 'Bibliotheque du Vivant'; CNRS; Museum National d'Histoire Naturelle; INRA; CEA (Centre National de Sequencage) FX We thank the State Ministry of Research and Technology (RISTEK, permit number: 028/SIP/FRP/SMII/2012) and the Ministry of Forestry, Republic of Indonesia, for providing permits to carry out fieldwork in the Moluccas. Likewise, we thank the Research Center for Biology, Indonesian Institute of Sciences (RCB-LIPI) and the Museum Zoologicum Bogoriense (MZB, Cibinong, Indonesia) for providing staff and support to carry out fieldwork in the Moluccas. We thank all the staff of Operation Wallacea, especially Nicola Grimwood. We thank Anne-Claire Fabre, Michael D. Carleton, Ken Aplin, Lionel Hautier, Julien Benoit, and one anonymous reviewer for their discussion and corrections to this article. We thank Francois Catzeflis for his comments and access to the Montpellier mammal skeleton and tissue collection. Tissue samples T-1288 and T-1289 were collected and preserved by Manuel Ruedi, and have been loaned from the collection of Mammalian Tissues of Montpellier, under the curation of Francois Catzeflis. We are grateful to the following people and institutions for granting access to study skins: Paula Jenkins, Samantha Oxford, and Roberto Portela Miguez (BMNH); Darrin Lunde (USNM); Eileen Westwig and Robert Voss (AMNH); Geraldine Veron, Violaine Nicolas, and Christiane Denis (MNHN); Chris Smeenk and Steve van Der Mije (RMNH); Hans Baagoe and Mogens Andersen (ZMUC). We thank Renaud Lebrun (ISEM, Case Postal 64, Place Eugne Bataillon, 34095 Montpellier cedex 5, France) for scanning the skulls of Halmaheramys and Lionel Hautier for processing the scanner output for the skulls in Figure 8. We thank Emmanuel Douzery and Benoit Nabholz for their help with phylogenetic and molecular evolutionary methodological designs, computational help, and other discussions. We are grateful to A.E. Balakirev for providing unpublished DNA sequences of species from the Dacnomys division. P.-H. F., J.K., and K.J. acknowledge the Danish National Research Foundation and a National Geographic Society Research and Exploration Grant (8853-10) for funding the Center for Macroecology, Evolution and Climate. P.-H.F and K.J. acknowledge the National Geographic Society for funding fieldwork in Indonesia. K.A.J. acknowledges the Dybron Hoffs Foundation for supplemental funding of the expedition. M.P. is currently funded by an FRS-FNRS fellowship (Belgian Fund for Scientific Research). P.-H.F. acknowledges the SYNTHESYS Foundation (project GB-TAF-2735) for funding his work in the BMNH collections. Many of the specimens of Bunomys, Taeromys, and Paruromys were collected during G.G.M.'s fieldwork in Sulawesi, and he acknowledges the support of the Celebes Fund and Archbold Expeditions, formerly of the American Museum of Natural History, the Lembaga Ilmu Pengetahuan Indonesia (LIPI), and the Museum Zoologicum Bogoriense (MZB) in Indonesia, and members of the US Navy Medical Research Unit no. 2 (NAMRU-2) in Jakarta. Analyses were performed on the CBGP HPC computational platform. This project was partly supported by the network 'Bibliotheque du Vivant' funded by the CNRS, the Museum National d'Histoire Naturelle, the INRA, and the CEA (Centre National de Sequencage). NR 122 TC 14 Z9 14 U1 1 U2 29 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 OCT PY 2013 VL 169 IS 2 BP 408 EP 447 DI 10.1111/zoj.12061 PG 40 WC Zoology SC Zoology GA 226FC UT WOS:000325019000006 ER PT J AU Isler, ML Bravo, GA Brumfield, RT AF Isler, Morton L. Bravo, Gustavo A. Brumfield, Robb T. TI Taxonomic revision of Myrmeciza (Aves: Passeriformes: Thamnophilidae) into 12 genera based on phylogenetic, morphological, behavioral, and ecological data SO ZOOTAXA LA English DT Article DE antbirds; Myrmeciza; phylogeny; systematics; Thamnophilidae ID TYPICAL ANTBIRDS THAMNOPHILIDAE; NEOTROPICAL OVENBIRDS; NEST ARCHITECTURE; 1ST DESCRIPTION; SPECIES LIMITS; BIRDS; GENUS; DIVERSIFICATION; FURNARIIDAE; LAEMOSTICTA AB A comprehensive molecular phylogeny of the family Thamnophilidae indicated that the genus Myrmeciza (Gray) is not monophyletic. Species currently assigned to the genus are found in three of the five tribes comprising the subfamily Thamnophilinae. Morphological, behavioral, and ecological character states of species within these tribes and their closest relatives were compared to establish generic limits. As a result of this analysis, species currently placed in Myrmeciza are assigned to Myrmeciza and eleven other genera, four of which (Myrmelastes Sclater, Myrmoderus Ridgway, Myrmophylax Todd, and Sipia Hellmayr) are resurrected, and seven of which (Ammonastes, Ampelornis, Aprositornis, Hafferia, Inundicola, Poliocrania, and Sciaphylax) are newly described. C1 [Isler, Morton L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool Birds, Washington, DC 20560 USA. [Bravo, Gustavo A.; Brumfield, Robb T.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Bravo, Gustavo A.; Brumfield, Robb T.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. RP Isler, ML (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool Birds, Washington, DC 20560 USA. EM antbird@cox.net RI Brumfield, Robb/K-6108-2015 OI Brumfield, Robb/0000-0003-2307-0688 FU Frank Chapman Memorial Fund - AMNH; American Ornithologists' Union; LSUMNS Big Day Fund; LSU Biograds; NSF [DBI-0400797, DEB-0841729, DEB-1011435] FX We are grateful to the curators and collection managers of the AMNH, ANSP, COP, FMNH, IAvH, ICN, INPA, KU, LGEMA, MCP, MPEG, MZUSP, UAM, USNM, and UWBM (see Table 1 for explanation of acronyms). N. Aristizabal assisted in obtaining sequences. A. M. Cuervo and C. D. Cadena provided sequences for some specimens housed at COP and IAvH. K. J. Zimmer kindly provided updated descriptions of tail and wing movements, J. Tello informed us of ongoing Cercomacra studies, and A. M. Cuervo, P. R. Isler, D. F. Lane, and B. M. Whitney offered valuable advice. We are grateful to R. T. Chesser for his support and assistance throughout, to J. V. Remsen, Jr. for reviewing an earlier draft, to N. David for his review and comments on proposed nomenclature, and to R. C. Banks and an anonymous reviewer for the final review. This research was supported by grants from the Frank Chapman Memorial Fund - AMNH, the American Ornithologists' Union, the LSUMNS Big Day Fund, LSU Biograds, and NSF grants DBI-0400797, DEB-0841729, and DEB-1011435 to GAB and RTB. NR 75 TC 8 Z9 8 U1 2 U2 13 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 OCT 1 PY 2013 VL 3717 IS 4 BP 469 EP 497 PG 29 WC Zoology SC Zoology GA 227QC UT WOS:000325127400003 PM 26176119 ER PT J AU Berta, ZK Irwin, J Charbonneau, D AF Berta, Zachory K. Irwin, Jonathan Charbonneau, David TI CONSTRAINTS ON PLANET OCCURRENCE AROUND NEARBY MID-TO-LATE M DWARFS FROM THE MEarth PROJECT SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: statistical; planetary systems; planets and satellites: individual (GJ 1214b); stars: low-mass ID EARTH GJ 1214B; LOW-MASS STARS; METAL-RICH ATMOSPHERE; IN SUPER-EARTHS; TRANSMISSION SPECTRUM; TRANSIT SURVEY; MAIN-SEQUENCE; ECLIPSING BINARY; SPACE-TELESCOPE; PROPER-MOTION AB The MEarth Project is a ground-based photometric survey intended to find planets transiting the closest and smallest main-sequence stars. In its first four years, MEarth discovered one transiting exoplanet, the 2.7R(circle plus) planet GJ1214b. Here, we answer an outstanding question: in light of the bounty of small planets transiting small stars uncovered by the Kepler mission, should MEarth have found more than just one planet so far? We estimate MEarth's ensemble sensitivity to exoplanets by performing end-to-end simulations of 1.25 x 10(6) observations of 988 nearby mid-tolate M dwarfs, gathered by MEarth between 2008 October and 2012 June. For 2-4R(circle plus) planets, we compare this sensitivity to results from Kepler and find that MEarth should have found planets at a rate of 0.05-0.36 planets yr(-1) in its first four years. As part of this analysis, we provide new analytic fits to the Kepler early M dwarf planet occurrence distribution. When extrapolating between Kepler's early M dwarfs and MEarth's mid-to-late M dwarfs, we find that assuming the planet occurrence distribution stays fixed with respect to planetary equilibrium temperature provides a good match to our detection of a planet with GJ1214b's observed properties. For larger planets, we find that the warm (600-700 K), Neptune-sized (4R(circle plus)) exoplanets that transit early M dwarfs like Gl436 and GJ3470 occur at a rate of < 0.15 star(-1) (at 95% confidence) around MEarth's later M dwarf targets. We describe a strategy with which MEarth can increase its expected planet yield by 2.5 x without new telescopes by shifting its sensitivity toward the smaller and cooler exoplanets that Kepler has demonstrated to be abundant. C1 [Berta, Zachory K.; Irwin, Jonathan; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Berta, ZK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM zberta@cfa.harvard.edu OI Berta-Thompson, Zachory/0000-0002-3321-4924 FU David and Lucile Packard Fellowship for Science and Engineering; National Science Foundation (NSF) [AST-0807690, AST-1109468] FX We thank Jason Dittmann and Elisabeth Newton for detailed discussions regarding the MEarth stellar sample and Courtney Dressing for discussing Kepler M dwarf planet statistics. We are grateful to Christopher Burke and Philip Nutzman for many conversations that led to this work. The MEarth Project gratefully acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering and from the National Science Foundation (NSF) under grants AST-0807690 and AST-1109468. We are greatly indebted to the staff at the Fred Lawrence Whipple Observatory for their efforts in construction and maintenance of the MEarth facility and thank Emilio Falco, Wayne Peters, Ted Groner, Karen Erdman-Myres, Grace Alegria, Rodger Harris, Bob Hutchins, Dave Martina, Dennis Jankovsky, Tom Welsh, Robert Hyne, Mike Calkins, Perry Berlind, and Gil Esquerdo for their support. This research has made use of NASA's Astrophysics Data System. NR 96 TC 26 Z9 26 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 OCT 1 PY 2013 VL 775 IS 2 AR 91 DI 10.1088/0004-637X/775/2/91 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 222ME UT WOS:000324734400011 ER PT J AU Dahlen, T Mobasher, B Faber, SM Ferguson, HC Barro, G Finkelstein, SL Finlator, K Fontana, A Gruetzbauch, R Johnson, S Pforr, J Salvato, M Wiklind, T Wuyts, S Acquaviva, V Dickinson, ME Guo, YC Huang, JS Huang, KH Newman, JA Bell, EF Conselice, CJ Galametz, A Gawiser, E Giavalisco, M Grogin, NA Hathi, N Kocevski, D Koekemoer, AM Koo, DC Lee, KS McGrath, EJ Papovich, C Peth, M Ryan, R Somerville, R Weiner, B Wilson, G AF Dahlen, Tomas Mobasher, Bahram Faber, Sandra M. Ferguson, Henry C. Barro, Guillermo Finkelstein, Steven L. Finlator, Kristian Fontana, Adriano Gruetzbauch, Ruth Johnson, Seth Pforr, Janine Salvato, Mara Wiklind, Tommy Wuyts, Stijn Acquaviva, Viviana Dickinson, Mark E. Guo, Yicheng Huang, Jiasheng Huang, Kuang-Han Newman, Jeffrey A. Bell, Eric F. Conselice, Christopher J. Galametz, Audrey Gawiser, Eric Giavalisco, Mauro Grogin, Norman A. Hathi, Nimish Kocevski, Dale Koekemoer, Anton M. Koo, David C. Lee, Kyoung-Soo McGrath, Elizabeth J. Papovich, Casey Peth, Michael Ryan, Russell Somerville, Rachel Weiner, Benjamin Wilson, Grant TI A CRITICAL ASSESSMENT OF PHOTOMETRIC REDSHIFT METHODS: A CANDELS INVESTIGATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: distances and redshifts; galaxies: high-redshift; galaxies: photometry; surveys ID DEEP FIELD-SOUTH; STAR-FORMING GALAXIES; EXTRAGALACTIC LEGACY SURVEY; ACTIVE GALACTIC NUCLEI; LYMAN BREAK GALAXIES; GOODS-SOUTH; MU-M; SPECTROSCOPIC REDSHIFTS; POPULATION SYNTHESIS; LUMINOSITY FUNCTIONS AB We present results from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) photometric redshift methods investigation. In this investigation, the results from 11 participants, each using a different combination of photometric redshift code, template spectral energy distributions (SEDs), and priors, are used to examine the properties of photometric redshifts applied to deep fields with broadband multi-wavelength coverage. The photometry used includes U-band through mid-infrared filters and was derived using the TFIT method. Comparing the results, we find that there is no particular code or set of template SEDs that results in significantly better photometric redshifts compared to others. However, we find that codes producing the lowest scatter and outlier fraction utilize a training sample to optimize photometric redshifts by adding zero-point offsets, template adjusting, or adding extra smoothing errors. These results therefore stress the importance of the training procedure. We find a strong dependence of the photometric redshift accuracy on the signal-to-noise ratio of the photometry. On the other hand, we find a weak dependence of the photometric redshift scatter with redshift and galaxy color. We find that most photometric redshift codes quote redshift errors (e.g., 68% confidence intervals) that are too small compared to that expected from the spectroscopic control sample. We find that all codes show a statistically significant bias in the photometric redshifts. However, the bias is in all cases smaller than the scatter; the latter therefore dominates the errors. Finally, we find that combining results from multiple codes significantly decreases the photometric redshift scatter and outlier fraction. We discuss different ways of combining data to produce accurate photometric redshifts and error estimates. C1 [Dahlen, Tomas; Ferguson, Henry C.; Grogin, Norman A.; Koekemoer, Anton M.; Ryan, Russell] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Faber, Sandra M.; Barro, Guillermo; Guo, Yicheng; Koo, David C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Finkelstein, Steven L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Finlator, Kristian] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-1168 Copenhagen, Denmark. [Fontana, Adriano; Galametz, Audrey] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Gruetzbauch, Ruth] Observ Astron Lisboa, Ctr Astron & Astrophys, P-1349018 Lisbon, Portugal. [Johnson, Seth; Giavalisco, Mauro; Wilson, Grant] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Pforr, Janine; Dickinson, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Salvato, Mara; Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Salvato, Mara] Excellence Cluster, D-85748 Garching, Germany. [Wiklind, Tommy] Joint ALMA Observ, Santiago, Chile. [Acquaviva, Viviana] CUNY NYC Coll Technol, Dept Phys, Brooklyn, NY 11201 USA. [Huang, Jiasheng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huang, Jiasheng] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Huang, Kuang-Han; Peth, Michael] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Conselice, Christopher J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Gawiser, Eric; Somerville, Rachel] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Hathi, Nimish] Carnegie Observ, Pasadena, CA 91101 USA. [Kocevski, Dale] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Lee, Kyoung-Soo] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [McGrath, Elizabeth J.] Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA. [Papovich, Casey] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Weiner, Benjamin] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Dahlen, T (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM dahlen@stsci.edu RI Finlator, Kristian/M-4809-2014; Pforr, Janine/J-3967-2015; Hathi, Nimish/J-7092-2014; OI Finlator, Kristian/0000-0002-0496-1656; Pforr, Janine/0000-0002-3414-8391; Hathi, Nimish/0000-0001-6145-5090; Weiner, Benjamin/0000-0001-6065-7483; Koekemoer, Anton/0000-0002-6610-2048; fontana, adriano/0000-0003-3820-2823; Bell, Eric/0000-0002-5564-9873 FU NASA [NAS 5-26555]; [GO-9352]; [GO-9425]; [GO-9583]; [GO-9728]; [GO-10189]; [GO-10339]; [GO-10340]; [GO-11359]; [GO-12060]; [GO-12061] FX We are grateful to our referee, Giuseppe Longo, for providing valuable comments and suggestions for improving this paper. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs GO-9352, GO-9425, GO-9583, GO-9728, GO-10189, GO-10339, GO-10340, GO-11359, GO-12060, and GO-12061. Observations have been carried out using the Very Large Telescope at the ESO Paranal Observatory under Program ID(s): LP168. A-0485. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 79 TC 97 Z9 97 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2013 VL 775 IS 2 AR 93 DI 10.1088/0004-637X/775/2/93 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 222ME UT WOS:000324734400013 ER PT J AU Nulsen, PEJ Li, ZY Forman, WR Kraft, RP Lal, DV Jones, C Zhuravleva, I Churazov, E Sanders, JS Fabian, AC Johnson, RE Murray, SS AF Nulsen, Paul E. J. Li, Zhiyuan Forman, William R. Kraft, Ralph P. Lal, Dharam V. Jones, Christine Zhuravleva, Irina Churazov, Eugene Sanders, Jeremy S. Fabian, Andrew C. Johnson, Ryan E. Murray, Stephen S. TI DEEP CHANDRA OBSERVATIONS OF A2199: THE INTERPLAY BETWEEN MERGER-INDUCED GAS MOTIONS AND NUCLEAR OUTBURSTS IN A COOL CORE CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (A2199); galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID RELAXED GALAXY CLUSTERS; X-RAY; INTRACLUSTER MEDIUM; COLD-FRONT; HYDRA-A; GASEOUS ATMOSPHERE; ELLIPTIC GALAXIES; PERSEUS CLUSTER; MASS PROFILES; BLACK-HOLES AB We present new Chandra observations of A2199 that show evidence of gas sloshing due to a minor merger, as well as impacts of the radio source, 3C 338, hosted by the central galaxy, NGC 6166, on the intracluster gas. The new data are consistent with previous evidence of a Mach similar or equal to 1.46 shock 100 '' from the cluster center, although there is still no convincing evidence for the expected temperature jump. Other interpretations of this feature are possible, but none is fully satisfactory. Large scale asymmetries, including enhanced X-ray emission 200 '' southwest of the cluster center and a plume of low entropy, enriched gas reaching 50 '' to the north of the center, are signatures of gas sloshing induced by core passage of a merging subcluster about 400 Myr ago. An association between the unusual radio ridge and low entropy gas are consistent with this feature being the remnant of a former radio jet that was swept away from the active galactic nucleus by gas sloshing. A large discrepancy between the energy required to produce the 100 '' shock and the enthalpy of the outer radio lobes of 3C 338 suggests that the lobes were formed by a more recent, less powerful radio outburst. The lack of evidence for shocks in the central 10 '' indicates that the power of the jet now is some two orders of magnitude smaller than when the 100 '' shock was formed. C1 [Nulsen, Paul E. J.; Li, Zhiyuan; Forman, William R.; Kraft, Ralph P.; Lal, Dharam V.; Jones, Christine; Murray, Stephen S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Li, Zhiyuan] UCLA Phys & Astron, Los Angeles, CA 90095 USA. [Lal, Dharam V.] TIFR, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Zhuravleva, Irina] Stanford Univ, KIPAC, Stanford, CA 94305 USA. [Zhuravleva, Irina] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Churazov, Eugene] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Sanders, Jeremy S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Sanders, Jeremy S.; Fabian, Andrew C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Johnson, Ryan E.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Murray, Stephen S.] Johns Hopkins Univ, Baltimore, MD 21205 USA. RP Nulsen, PEJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Churazov, Eugene/A-7783-2013; OI Sanders, Jeremy/0000-0003-2189-4501; Nulsen, Paul/0000-0003-0297-4493; Forman, William/0000-0002-9478-1682 FU NASA [NAS8-03060, NAS 5-26555] FX We thank Maxim Markevitch for his assistance and the referee for helping to improve the paper. P.E.J.N. was supported by NASA grant NAS8-03060. The scientific results in this article are based to a significant degree on observations made with the Chandra X-Ray Observatory. This research has made use of software provided by the Chandra X-Ray Center in the applications packages CIAO, Chips, and Sherpa. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program 9293. NR 49 TC 8 Z9 8 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2013 VL 775 IS 2 AR 117 DI 10.1088/0004-637X/775/2/117 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 222ME UT WOS:000324734400037 ER PT J AU Pan, LB Scannapieco, E Scalo, J AF Pan, Liubin Scannapieco, Evan Scalo, Jon TI MODELING THE POLLUTION OF PRISTINE GAS IN THE EARLY UNIVERSE SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark ages, reionization, first stars; evolution; galaxies: high-redshift; ISM: abundances; stars: Population III; turbulence ID LARGE-EDDY-SIMULATION; POPULATION-III STARS; TURBULENT REACTING FLOWS; INITIAL MASS FUNCTION; SUBGRID-SCALE-MODEL; EXTREMELY METAL-POOR; GALACTIC 1ST STARS; LY-ALPHA EMITTERS; COMPRESSIBLE TURBULENCE; INTERSTELLAR-MEDIUM AB We conduct a comprehensive theoretical and numerical investigation of the pollution of pristine gas in turbulent flows, designed to provide useful new tools for modeling the evolution of the first generation of stars. The properties of such Population III (Pop III) stars are thought to be very different than those of later stellar generations, because cooling is dramatically different in gas with a metallicity below a critical value Z(c), which lies between similar to 10(-6) and similar to 10(-3) Z(circle dot). The critical value is much smaller than the typical overall average metallicity, < Z >, and therefore the mixing efficiency of the pristine gas in the interstellar medium plays a crucial role in determining the transition from Pop III to normal star formation. The small critical value, Z(c), corresponds to the far left tail of the probability distribution function (PDF) of the metal abundance. Based on closure models for the PDF formulation of turbulent mixing, we derive evolution equations for the fraction of gas, P, lying below Z(c), in statistically homogeneous compressible turbulence. Our simulation data show that the evolution of the pristine fraction P can be well approximated by a generalized "self-convolution" model, which predicts that (P) over dot = -(n/tau(con))P(1 - P-1/n), where n is a measure of the locality of the mixing or PDF convolution events and the convolution timescale tau(con) is determined by the rate at which turbulence stretches the pollutants. Carrying out a suite of numerical simulations with turbulent Mach numbers ranging from M = 0.9 to 6.2, we are able to provide accurate fits to n and tau(con) as a function of M, Z(c)/< Z >, and the length scale, L-p, at which pollutants are added to the flow. For pristine fractions above P = 0.9, mixing occurs only in the regions surrounding blobs of pollutants, such that n = 1. For smaller values of P, n is larger as the mixing process becomes more global. We show how these results can be used to construct one-zone models for the evolution of Pop III stars in a single high-redshift galaxy, as well as subgrid models for tracking the evolution of the first stars in large cosmological numerical simulations. C1 [Pan, Liubin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Scannapieco, Evan] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Scalo, Jon] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Pan, LB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lpan@cfa.harvard.edu; evan.scannapieco@asu.edu; parrot@astro.as.utexas.edu FU NASA [NNX09AD106]; Astrobiology Institute [08-NAI5-0018]; National Science Foundation [AST 11-03608]; DOE ASC/Alliances FX We acknowledge support from NASA under theory Grant No. NNX09AD106 and Astrobiology Institute Grant 08-NAI5-0018 and from the National Science Foundation under grant AST 11-03608. All simulations were conducted at the Arizona State University Advanced Computing Center and the Texas Advanced Computing Center, using the FLASH code, a product of the DOE ASC/Alliances funded Center for Astrophysical Thermonuclear Flashes at the University of Chicago. NR 132 TC 5 Z9 5 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 OCT 1 PY 2013 VL 775 IS 2 AR 111 DI 10.1088/0004-637X/775/2/111 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 222ME UT WOS:000324734400031 ER PT J AU Rosenfeld, KA Andrews, SM Wilner, DJ Kastner, JH McClure, MK AF Rosenfeld, Katherine A. Andrews, Sean M. Wilner, David J. Kastner, J. H. McClure, M. K. TI THE STRUCTURE OF THE EVOLVED CIRCUMBINARY DISK AROUND V4046 Sgr SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planet-disk interactions; protoplanetary disks; stars: individual (V4046 Sgr); submillimeter: planetary systems ID EMISSION-LINE STARS; X-RAY-RADIATION; TWIN YOUNG SUNS; PROTOPLANETARY DISKS; ACCRETION DISKS; CIRCUMSTELLAR DISKS; TRANSITION DISKS; GRAIN-GROWTH; HYDRODYNAMIC MODELS; EXTREME-ULTRAVIOLET AB We present sensitive, sub-arcsecond resolution Submillimeter Array observations of the protoplanetary disk around the nearby, pre-main sequence spectroscopic binary V4046 Sgr. We report for the first time a large inner hole (r = 29 AU) spatially resolved in the 1.3 mm continuum emission and study the structure of this disk using radiative transfer calculations to model the spectral energy distribution, continuum visibilities, and spectral line emission of CO and its main isotopologues. Our modeling scheme demonstrates that the majority of the dust mass is distributed in a narrow ring (centered at 37 AU with a FWHM of 16 AU) that is similar to 5x more compact than the gas disk. This structure implies that the dust-to-gas mass ratio has a strong spatial variation, ranging from a value much larger than typical of the interstellar medium (ISM) at the ring to much smaller than that of the ISM at larger disk radii. We suggest that these basic structural features are potentially observational signatures of the accumulation of solids at a local gas pressure maximum. These models also require a substantial population of similar to mu m sized grains inside the central disk cavity. We suggest that this structure is likely the result of dynamical interactions with a low-mass companion, although photoevaporation may also play a secondary role. C1 [Rosenfeld, Katherine A.; Andrews, Sean M.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kastner, J. H.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. [McClure, M. K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Rosenfeld, KA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI McClure, Melissa/0000-0003-1878-327X FU NASA Origins of Solar Systems grant [NNX11AK63]; National Science Foundation [AST-1108950]; Smithsonian Institution; Academia Sinica; NASA FX We are grateful to Adam Kraus for sharing his K-band limit on a companion, Andrea Isella for teaching K.R. us about asymmetries, and Moritz Gunther for helping us with the X-ray luminosities. We are also indebted to Kees Dullemond, Guillermo Torres, and Matt Payne for insightful discussions. We acknowledge support from NASA Origins of Solar Systems grant No. NNX11AK63. J.K.'s research on V4046 Sgr and other nearby protoplanetary disks is supported in part by National Science Foundation grant AST-1108950 to RIT. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This work is based (in part) on archival data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA. NR 106 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 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2013 VL 775 IS 2 AR 136 DI 10.1088/0004-637X/775/2/136 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 222ME UT WOS:000324734400056 ER PT J AU Sanders, NE Levesque, EM Soderberg, AM AF Sanders, N. E. Levesque, E. M. Soderberg, A. M. TI USING COLORS TO IMPROVE PHOTOMETRIC METALLICITY ESTIMATES FOR GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: ISM; galaxies: photometry ID DIGITAL SKY SURVEY; STAR-FORMING GALAXIES; CORE-COLLAPSE SUPERNOVAE; BURST HOST GALAXIES; H II REGIONS; DATA RELEASE; RELATIVE FREQUENCIES; NITROGEN ABUNDANCES; HIGH-REDSHIFT; K-CORRECTIONS AB There is a well known correlation between the mass and metallicity of star-forming galaxies. Because mass is correlated with luminosity, this relation is often exploited, when spectroscopy is not available, to estimate galaxy metallicities based on single band photometry. However, we show that galaxy color is typically more effective than luminosity as a predictor of metallicity. This is a consequence of the correlation between color and the galaxy mass-to-light ratio and the recently discovered correlation between star formation rate (SFR) and residuals from the mass-metallicity relation. Using Sloan Digital Sky Survey spectroscopy of similar to 180,000 nearby galaxies, we derive "LZC relations," empirical relations between metallicity (in seven common strong line diagnostics), luminosity, and color (in 10 filter pairs and four methods of photometry). We show that these relations allow photometric metallicity estimates, based on luminosity and a single optical color, that are similar to 50% more precise than those made based on luminosity alone; galaxy metallicity can be estimated to within similar to 0.05-0.1 dex of the spectroscopically derived value depending on the diagnostic used. Including color information in photometric metallicity estimates also reduces systematic biases for populations skewed toward high or low SFR environments, as we illustrate using the host galaxy of the supernova SN 2010ay. This new tool will lend more statistical power to studies of galaxy populations, such as supernova and gamma-ray burst host environments, in ongoing and future wide-field imaging surveys. C1 [Sanders, N. E.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Levesque, E. M.] Univ Colorado, CASA, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. RP Sanders, NE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nsanders@cfa.harvard.edu FU National Science Foundation; NASA [PF0-110075, NAS8-03060]; Chandra X-Ray Center; David and Lucile Packard Foundation FX We thank an anonymous referee for very helpful suggestions. We thank the MPA/JHU teams for making available their catalog of measured properties for SDSS galaxies, and we thank E. Berger, D. Eisenstein, D. Erb, R. Foley, and A. Tripathi for helpful conversations. This work was supported by the National Science Foundation through a Graduate Research Fellowship provided to N.E.S.; E. M. L. is supported by NASA through Einstein Postdoctoral Fellowship grant number PF0-110075 awarded by the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060; and support for this work was provided by the David and Lucile Packard Foundation Fellowship for Science and Engineering awarded to A.M.S. NR 54 TC 6 Z9 6 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2013 VL 775 IS 2 AR 125 DI 10.1088/0004-637X/775/2/125 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 222ME UT WOS:000324734400045 ER PT J AU Spoon, HWW Farrah, D Lebouteiller, V Gonzalez-Alfonso, E Bernard-Salas, J Urrutia, T Rigopoulou, D Westmoquette, MS Smith, HA Afonso, J Pearson, C Cormier, D Efstathiou, A Borys, C Verma, A Etxaluze, M Clements, DL AF Spoon, H. W. W. Farrah, D. Lebouteiller, V. Gonzalez-Alfonso, E. Bernard-Salas, J. Urrutia, T. Rigopoulou, D. Westmoquette, M. S. Smith, H. A. Afonso, J. Pearson, C. Cormier, D. Efstathiou, A. Borys, C. Verma, A. Etxaluze, M. Clements, D. L. TI DIAGNOSTICS OF AGN-DRIVEN MOLECULAR OUTFLOWS IN ULIRGs FROM HERSCHEL-PACS OBSERVATIONS OF OH AT 119 mu m SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: galaxies; ISM: jets and outflows; galaxies: evolution; galaxies: ISM; quasars: absorption lines ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMATION; BLACK-HOLES; QUASAR FEEDBACK; EMISSION-LINE; BRIGHT GALAXIES; SCALE OUTFLOWS; LOCAL ULIRGS; SPECTROSCOPY AB We report on our observations of the 79 and 119 mu m doublet transitions of OH for 24 local (z < 0.262) ULIRGs observed with Herschel-PACS as part of the Herschel ULIRG Survey (HERUS). Some OH 119 mu m profiles display a clear P-Cygni shape and therefore imply outflowing OH gas, while other profiles are predominantly in absorption or are completely in emission. We find that the relative strength of the OH emission component decreases as the silicate absorption increases. This result locates the OH outflows inside the obscured nuclei. The maximum outflow velocities for our sources range from less than 100 to similar to 2000 km s(-1), with 15/24 (10/24) sources showing OH absorption at velocities exceeding 700 km s(-1) (1000 km s(-1)). Three sources show maximum OH outflow velocities exceeding that of Mrk231. Since outflow velocities above 500-700 km s(-1) are thought to require an active galactic nucleus (AGN) to drive them, about two-thirds of our ULIRG sample may host AGN-driven molecular outflows. This finding is supported by the correlation we find between the maximum OH outflow velocity and the IR-derived bolometric AGN luminosity. No such correlation is found with the IR-derived star formation rate. The highest outflow velocities are found among sources that are still deeply embedded. We speculate that the molecular outflows in these sources may be in an early phase of disrupting the nuclear dust veil before these sources evolve into less-obscured AGNs. Four of our sources show high-velocity wings in their [C II] fine-structure line profiles, implying neutral gas outflow masses of at least (2-4.5) x 10(8) M-circle dot. C1 [Spoon, H. W. W.; Lebouteiller, V.] Cornell Univ, CRSR, Ithaca, NY USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Lebouteiller, V.] CEA Saclay, DSM, IRFU, SAp, F-91191 Gif Sur Yvette, France. [Gonzalez-Alfonso, E.] Univ Alcala de Henares, Dept Fis Matemat, E-28871 Madrid, Spain. [Bernard-Salas, J.] Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Urrutia, T.] Leibniz Inst Astrophys, D-14482 Potsdam, Germany. [Rigopoulou, D.] Dept Phys, Oxford OX1 3RH, England. [Rigopoulou, D.] RAL Space Sci & Technol Facil Council, Didcot OX11 0QX, Oxon, England. [Westmoquette, M. S.] European So Observ, D-85748 Garching, Germany. [Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Afonso, J.] Univ Lisbon, Observ Astron Lisboa, Ctr Astron & Astrofis, P-1349018 Lisbon, Portugal. [Afonso, J.] Univ Lisbon, Fac Sci, Dept Phys, P-1749016 Lisbon, Portugal. [Pearson, C.] Rutherford Appleton Lab, RAL Space, Oxford OX11 0QX, England. [Pearson, C.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Cormier, D.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Efstathiou, A.] European Univ Cyprus, Sch Sci, CY-1516 Nicosia, Cyprus. [Borys, C.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Etxaluze, M.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, E-28850 Madrid, Spain. [Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. RP Spoon, HWW (reprint author), Cornell Univ, CRSR, Space Sci Bldg, Ithaca, NY USA. EM spoon@isc.astro.cornell.edu RI Afonso, Jose/B-5185-2013 OI Afonso, Jose/0000-0002-9149-2973 FU CEA/Marie Curie Eurotalents fellowship; Spanish Ministerio de Economia y Competitividad [AYA2010-21697-C05-0, FIS2012-39162-C06-01]; Science and Technology Foundation (FCT, Portugal) [PTDC/CTE-AST/105287/2008, PEst-OE/FIS/UI2751/2011, PTDC/FIS-AST/2194/2012]; ASTROMADRID [S2009ESP-1496]; Spanish MINECO [AYA2009-07304]; ASTROMOL [CSD2009-00038]; NASA through JPL/Caltech FX The authors thank the anonymous referee for constructive comments that led to an improvement of this paper. We are grateful to the SHINING team for their collegiality and for providing us with the OH119 line profile of Mrk 231. We further thank Jackie Fischer, Henny Lamers, Thomas Nikola, and Gordon Stacey for discussions, and Dan Weedman and Sylvain Veilleux for sharing OH line scans prior to their publication. V. L. is supported by a CEA/Marie Curie Eurotalents fellowship. E. G.-A. is a Research Associate at the Harvard-Smithsonian Center for Astrophysics, and thanks the Spanish Ministerio de Economia y Competitividad for support under projects AYA2010-21697-C05-0 and FIS2012-39162-C06-01. J.A. acknowledges support from the Science and Technology Foundation (FCT, Portugal) through the research grants PTDC/CTE-AST/105287/2008, PEst-OE/FIS/UI2751/2011 and PTDC/FIS-AST/2194/2012. M. E. thanks ASTROMADRID for support through grant S2009ESP-1496, from Spanish MINECO: AYA2009-07304 and from ASTROMOL: CSD2009-00038. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 60 TC 47 Z9 47 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 OCT 1 PY 2013 VL 775 IS 2 AR 127 DI 10.1088/0004-637X/775/2/127 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 222ME UT WOS:000324734400047 ER PT J AU Vivian, U Medling, A Sanders, D Max, C Armus, L Iwasawa, K Evans, A Kewley, L Fazio, G AF Vivian, U. Medling, Anne Sanders, David Max, Claire Armus, Lee Iwasawa, Kazushi Evans, Aaron Kewley, Lisa Fazio, Giovanni TI THE INNER KILOPARSEC OF Mrk 273 WITH KECK ADAPTIVE OPTICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Mrk 273); galaxies: interactions; galaxies: kinematics and dynamics; galaxies: nuclei ID ULTRALUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; SPATIALLY-RESOLVED SPECTROSCOPY; INTEGRAL-FIELD SPECTROSCOPY; SKY LIRG SURVEY; MOLECULAR-HYDROGEN; STAR-FORMATION; FE-II; CHANDRA OBSERVATIONS AB There is X-ray, optical, and mid-infrared imaging and spectroscopic evidence that the late-stage ultraluminous infrared galaxy merger Mrk 273 hosts a powerful active galactic nucleus (AGN). However, the exact location of the AGN and the nature of the nucleus have been difficult to determine due to dust obscuration and the limited wavelength coverage of available high-resolution data. Here we present near-infrared integral-field spectra and images of the nuclear region of Mrk 273 taken with OSIRIS and NIRC2 on the Keck II Telescope with laser guide star adaptive optics. We observe three spatially resolved components, and analyze the nuclear molecular and ionized gas emission lines and their kinematics. We confirm the presence of the hard X-ray AGN in the southwest nucleus. In the north nucleus, we find a strongly rotating gas disk whose kinematics indicate a central black hole of mass 1.04 +/- 0.1 x 10(9) M-circle dot. The H-2 emission line shows an increase in velocity dispersion along the minor axis in both directions, and an increased flux with negative velocities in the southeast direction; this provides direct evidence for a collimated molecular outflow along the axis of rotation of the disk. The third spatially distinct component appears to the southeast, 640 and 750 pc from the north and southwest nuclei, respectively. This component is faint in continuum emission but shows several strong emission line features, including [Si VI] 1.964 mu m which traces an extended coronal-line region. The geometry of the [Si VI] emission combined with shock models and energy arguments suggest that [Si VI] in the southeast component must be at least partly ionized by the SW AGN or a putative AGN in the northern disk, either through photoionization or through shock-heating from strong AGN- and circumnuclear-starburst-driven outflows. This lends support to a scenario in which Mrk 273 may be a dual AGN system. C1 [Vivian, U.; Sanders, David; Kewley, Lisa] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Medling, Anne; Max, Claire] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Armus, Lee] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Iwasawa, Kazushi] Univ Barcelona, IEEC UB, ICREA, E-08028 Barcelona, Spain. [Iwasawa, Kazushi] Univ Barcelona, IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain. [Evans, Aaron] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Evans, Aaron] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Kewley, Lisa] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Fazio, Giovanni] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vivian, U (reprint author), Univ Calif Riverside, Dept Phys & Astron, 900 Univ Ave, Riverside, CA 92521 USA. EM vivianu@ucr.edu FU W. M. Keck Foundation; NASA; Smithsonian Astrophysical Observatory Predoctoral Fellowship; NSF; Spanish Ministerio de Ciencia e Innovacion (MICINN) [AYA2010-21782-C03-01]; JPL Contract/IRAC GTO Grant [1256790] FX We thank the anonymous referee for a helpful discussion on alternative cases for photoionizing the SE component, and for various suggestions on strengthening the scenarios put forth in the paper. We acknowledge H. Inami and S. Stierwalt for providing their Spitzer-IRS spectra toward ease of target selection for our observing program, M. Ammons for help with data reduction and PSF estimation, R. da Silva for help with CLOUDY and shock-plot modeling, and D. Rupke for helpful conversations toward the results and their interpretations. We also thank the Keck staff for help with carrying out the observations and the UH/UC TACs for granting this observing time. The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. V. U. acknowledges funding support from the NASA Harriet G. Jenkins Predoctoral Fellowship Project and the Smithsonian Astrophysical Observatory Predoctoral Fellowship. A. M. acknowledges funding support from the NSF Graduate Fellowship. K. I. thanks support from Spanish Ministerio de Ciencia e Innovacion (MICINN) through grant (AYA2010-21782-C03-01). This work is partially supported by the JPL Contract/IRAC GTO Grant No. 1256790. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 92 TC 5 Z9 5 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2013 VL 775 IS 2 AR 115 DI 10.1088/0004-637X/775/2/115 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 222ME UT WOS:000324734400035 ER PT J AU Damjanov, I Chilingarian, I Hwang, HS Geller, MJ AF Damjanov, Ivana Chilingarian, Igor Hwang, Ho Seong Geller, Margaret J. TI DISCOVERY OF NINE INTERMEDIATE-REDSHIFT COMPACT QUIESCENT GALAXIES IN THE SLOAN DIGITAL SKY SURVEY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: evolution; galaxies: fundamental parameters; galaxies: stellar content; galaxies: structure ID SUPERDENSE MASSIVE GALAXIES; NEARBY ELLIPTIC GALAXIES; SIMILAR-TO 2; SIZE EVOLUTION; STAR-FORMATION; PASSIVE GALAXIES; RED NUGGETS; Z-SIMILAR-TO-2.5; SPECTROSCOPY; HISTORIES AB We identify nine galaxies with dynamical masses of M-dyn greater than or similar to 10(10) M-circle dot as photometric point sources, but with redshifts between z = 0.2 and z = 0.6, in the Sloan Digital Sky Survey (SDSS) spectro-photometric database. All nine galaxies have archival Hubble Space Telescope images. Surface brightness profile fitting confirms that all nine galaxies are extremely compact (0.4 < R-e,R-c < 6.6 kpc with the median R-e,R-c = 0.74 kpc) for their velocity dispersion (110 < sigma < 340 km s(-1); median sigma = 178 km s(-1)). From the SDSS spectra, three systems are dominated by very young stars; the other six are older than similar to 1 Gyr (two are E+A galaxies). The three young galaxies have disturbed morphologies and the older systems have smooth profiles consistent with a single-Sersic function. All nine lie below the z similar to 0 velocity dispersion-half-light radius relation. The most massive system-SDSSJ123657.44+631115.4-lies right within the locus for massive compact z > 1 galaxies and the other eight objects follow the high-redshift dynamical size-mass relation. C1 [Damjanov, Ivana] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chilingarian, Igor; Hwang, Ho Seong; Geller, Margaret J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Chilingarian, Igor] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. RP Damjanov, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Chilingarian, Igor/N-5117-2016 OI Chilingarian, Igor/0000-0002-7924-3253 FU Harvard College Observatory Menzel Fellowship; NSERC [PDF-421224-2012]; Smithsonian Institution; [MD-3288.2012.2] FX We acknowledge the use of the SDSS DR7 data (http://www.sdss.org/dr7/) and the MAST HST database (http://archive.stsci.edu/hst/). We thank the referee for prompt, helpful comments. I.D. is supported by the Harvard College Observatory Menzel Fellowship and NSERC (PDF-421224-2012). The Smithsonian Institution supports the research of I.C., H.S.H., and M.J.G. I.C. acknowledges support from grant MD-3288.2012.2. NR 45 TC 7 Z9 7 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2013 VL 775 IS 2 AR L48 DI 10.1088/2041-8205/775/2/L48 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220ZP UT WOS:000324626700015 ER PT J AU Kaltenegger, L Sasselov, D Rugheimer, S AF Kaltenegger, L. Sasselov, D. Rugheimer, S. TI WATER-PLANETS IN THE HABITABLE ZONE: ATMOSPHERIC CHEMISTRY, OBSERVABLE FEATURES, AND THE CASE OF KEPLER-62e AND-62f SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrobiology; planets and satellites: atmospheres; planets and satellites: detection; planets and satellites: individual (Kepler-62f, Kepler-62e, Kepler-69c) ID EARTH-LIKE PLANETS; MAIN-SEQUENCE STARS; SUPER-EARTHS; SYSTEM; MODEL; MASS; SPECTROSCOPY; EVOLUTION; SPECTRA; RADII AB Planets composed of large quantities of water that reside in the habitable zone are expected to have distinct geophysics and geochemistry of their surfaces and atmospheres. We explore these properties motivated by two key questions: whether such planets could provide habitable conditions and whether they exhibit discernable spectral features that distinguish a water-planet from a rocky Earth-like planet. We show that the recently discovered planets Kepler-62e and -62f are the first viable candidates for habitable zone water-planets. We use these planets as test cases for discussing those differences in detail. We generate atmospheric spectral models and find that potentially habitable water-planets show a distinctive spectral fingerprint in transit depending on their position in the habitable zone. C1 [Kaltenegger, L.] Max Planck Inst Astron, D-69115 Heidelberg, Germany. [Kaltenegger, L.; Sasselov, D.; Rugheimer, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kaltenegger, L (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69115 Heidelberg, Germany. EM kaltenegger@mpia.de OI Rugheimer, Sarah/0000-0003-1620-7658 FU DFG [ENP Ka 3142/1-1]; NASA [NNX09AJ50A] FX The authors thank J. McDowell for in depth discussions. L. K. acknowledges support from DFG funding ENP Ka 3142/1-1, D. S. partial support by NASA NNX09AJ50A (Kepler Mission science team). NR 39 TC 23 Z9 23 U1 3 U2 71 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2013 VL 775 IS 2 AR L47 DI 10.1088/2041-8205/775/2/L47 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220ZP UT WOS:000324626700014 ER PT J AU Kendrew, S Ginsburg, A Johnston, K Beuther, H Bally, J Cyganowski, CJ Battersby, C AF Kendrew, S. Ginsburg, A. Johnston, K. Beuther, H. Bally, J. Cyganowski, C. J. Battersby, C. TI EARLY-STAGE MASSIVE STAR FORMATION NEAR THE GALACTIC CENTER: Sgr C SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE infrared: ISM; ISM: jets and outflows; stars: formation ID EXTENDED GREEN OBJECTS; CENTER DUST RIDGE; MOLECULAR CLOUDS; CONTINUUM EMISSION; OUTFLOW CANDIDATES; FORMATION RATES; CENTER REGION; PLANE SURVEY; CATALOG; PC AB We present near-infrared spectroscopy and 1 mm line and continuum observations of a recently identified site of high mass star formation likely to be located in the Central Molecular Zone (CMZ) near Sgr C. Located on the outskirts of the massive evolved H II region associated with Sgr C, the area is characterized by an Extended Green Object (EGO) measuring similar to 10 '' in size (0.4 pc), whose observational characteristics suggest the presence of an embedded massive protostar driving an outflow. Our data confirm that early-stage star formation is taking place on the periphery of the Sgr C H II region, with detections of two protostellar cores and several knots of H-2 and Brackett gamma emission alongside a previously detected compact radio source. We calculate the cores' joint mass to be similar to 10(3) M-circle dot, with column densities of 1-2 x 10(24) cm(-2). We show the host molecular cloud to hold similar to 10(5) M-circle dot of gas and dust with temperatures and column densities favorable for massive star formation to occur, however, there is no evidence of star formation outside of the EGO, indicating that the cloud is predominantly quiescent. Given its mass, density, and temperature, the cloud is comparable to other remarkable non-star-forming clouds such as G0.253 in the eastern CMZ. C1 [Kendrew, S.; Johnston, K.; Beuther, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Ginsburg, A.; Bally, J.; Battersby, C.] Univ Colorado, CASA, Boulder, CO 80309 USA. [Cyganowski, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kendrew, S.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. RP Kendrew, S (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM kendrew@mpia.de OI Ginsburg, Adam/0000-0001-6431-9633; Kendrew, Sarah/0000-0002-7612-0469 FU Commonwealth of Australia FX S.K. thanks Jens Kauffmann, Sergio Molinari, Cornelia Lang and Yanett Contreras for sharing and discussing data. The Apache Point Observatory 3.5 m telescope is owned and operated by the Astrophysical Research Consortium. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics. The Mopra radio telescope is part of the ATNF, funded by the Commonwealth of Australia. NR 37 TC 7 Z9 7 U1 2 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2013 VL 775 IS 2 AR L50 DI 10.1088/2041-8205/775/2/L50 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220ZP UT WOS:000324626700017 ER PT J AU Payne, MJ Deck, KM Holman, MJ Perets, HB AF Payne, Matthew J. Deck, Katherine M. Holman, Matthew J. Perets, Hagai B. TI STABILITY OF SATELLITES IN CLOSELY PACKED PLANETARY SYSTEMS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE celestial mechanics; methods: numerical; planetary systems; planets and satellites: dynamical evolution and stability ID EXTRASOLAR GIANT PLANETS; IRREGULAR SATELLITES; DYNAMICAL CHAOS; EXOMOONS; DENSITIES; RESONANCE; KEPLER-11; EVOLUTION; HUNT; MAPS AB We perform numerical integrations of four-body (star, planet, planet, satellite) systems to investigate the stability of satellites in planetary systems with tightly packed inner planets (STIPs). We find that the majority of closely spaced stable two-planet systems can stably support satellites across a range of parameter-space which is only slightly decreased compared to that seen for the single-planet case. In particular, circular prograde satellites remain stable out to similar to 0.4 R-H (where R-H is the Hill radius) as opposed to 0.5 R-H in the single-planet case. A similarly small restriction in the stable parameter-space for retrograde satellites is observed, where planetary close approaches in the range 2.5-4.5 mutual Hill radii destabilize most satellites orbits only if a similar to 0.65 R-H. In very close planetary pairs (e.g., the 12:11 resonance) the addition of a satellite frequently destabilizes the entire system, causing extreme close approaches and the loss of satellites over a range of circumplanetary semi-major axes. The majority of systems investigated stably harbored satellites over a wide parameter-space, suggesting that STIPs can generally offer a dynamically stable home for satellites, albeit with a slightly smaller stable parameter-space than the single-planet case. As we demonstrate that multi-planet systems are not a priori poor candidates for hosting satellites, future measurements of satellite occurrence rates in multi-planet systems versus single-planet systems could be used to constrain either satellite formation or past periods of strong dynamical interaction between planets. C1 [Payne, Matthew J.; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Deck, Katherine M.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Deck, Katherine M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Perets, Hagai B.] Technion Israel Inst Technol, IL-32000 Haifa, Israel. RP Payne, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM matthewjohnpayne@gmail.com RI Perets, Hagai/K-9605-2015 OI Perets, Hagai/0000-0002-5004-199X FU NASA Origins of Solar Systems Program grant [NNX13A124G]; BSF grant [2012384]; NSFGRF FX This material is based upon work supported by the NASA Origins of Solar Systems Program grant NNX13A124G, and by the BSF grant number 2012384. K.M.D. acknowledges support from an NSFGRF. We thank the anonymous referee for their valuable input. NR 32 TC 8 Z9 8 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2013 VL 775 IS 2 AR L44 DI 10.1088/2041-8205/775/2/L44 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220ZP UT WOS:000324626700011 ER PT J AU Huang, JP Zhou, CH Lee, XH Bao, YX Zhao, XY Fung, J Richter, A Liu, X Zheng, YQ AF Huang, Jianping Zhou, Chenhong Lee, Xuhui Bao, Yunxuan Zhao, Xiaoyan Fung, Jimmy Richter, Andreas Liu, Xiong Zheng, Yiqi TI The effects of rapid urbanization on the levels in tropospheric nitrogen dioxide and ozone over East China SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Nitrogen dioxide; Ozone; Satellite retrieval; Seasonal change; Troposphere; Urbanization ID AIR-QUALITY; OBJECTIVES AB Over the past few decades, China has experienced a rapid increase in urbanization. The urban built-up areas (population) in Beijing, Shanghai, and Guangzhou increased by 197% (87%), 148% (65%), and 273% (25%), respectively, from 1996 to 2011. We use satellite retrieval data to quantify the effects of rapid urbanization on the yearly and seasonal changes in tropospheric nitrogen dioxide (NO2) over East China. The results show that rapid urbanization has a profound effect on tropospheric columns of NO2. During 1996-2011, the tropospheric columns of NO2 over the surrounding areas of Guangzhou, Shanghai, and Beijing increased by 82%, 292%, and 307%, respectively. The tropospheric columns of NO2 reach their maximum in winter and minimum in spring. The anthropogenic emissions related to urbanization are a dominant factor in the long-term changes in the yearly and seasonal mean tropospheric columns of NO2, whereas meteorological conditions such as the prevailing winds and precipitation account for the unique spatial patterns. Around the time of the 2008 Beijing Olympic Games, the tropospheric columns of NO2 over Beijing urban area significantly reduced by 48% in July, 35% in August, and 49% in September, relative to the same monthly averages over 2005-2007. However, this trend was reversed after the Games, and the increased rate was even larger than before. Our results show that the tropospheric NO2 above the three regions increased at rates 1.3-8 times faster than the rates in a recent inventory estimate of NO emissions for 2000-2010. We also discuss the influence of urbanization on tropospheric ozone and find that the Ozone Monitoring Instrument (OMI) retrieval tropospheric column shows that ozone levels are relatively insensitive to urbanization and changes in tropospheric NO2. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Huang, Jianping; Zhou, Chenhong; Lee, Xuhui] Nanjing Univ Informat Sci & Technol, Yale NUIST Ctr Atmospher Environm, Nanjing, Jiangsu, Peoples R China. [Huang, Jianping] Natl Ctr Environm Predict, NOAA, Environm Modeling Ctr, IM Syst Grp, College Pk, MD USA. [Lee, Xuhui] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Bao, Yunxuan; Zhao, Xiaoyan] Nanjing Univ Informat Sci & Technol, Sch Appl Meteorol, Nanjing, Jiangsu, Peoples R China. [Fung, Jimmy] Hong Kong Univ Sci & Technol, Dept Math, Hong Kong, Hong Kong, Peoples R China. [Richter, Andreas] Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. [Liu, Xiong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Zheng, Yiqi] Yale Univ, Dept Geol & Geophys, New Haven, CT USA. RP Huang, JP (reprint author), Nanjing Univ Informat Sci & Technol, Yale NUIST Ctr Atmospher Environm, Nanjing, Jiangsu, Peoples R China. EM jianping.huang@noaa.gov RI Richter, Andreas/C-4971-2008; Liu, Xiong/P-7186-2014; OI Richter, Andreas/0000-0003-3339-212X; Liu, Xiong/0000-0003-2939-574X; Fung, Jimmy/0000-0002-7859-8511 FU Ministry of Education of China (grant PCSIRT); Priority Academic Program Development of Jiangsu Higher Education Institutions (grant PAPD) FX This research was supported by the Ministry of Education of China (grant PCSIRT) and the Priority Academic Program Development of Jiangsu Higher Education Institutions (grant PAPD). NR 28 TC 13 Z9 22 U1 1 U2 74 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD OCT PY 2013 VL 77 BP 558 EP 567 DI 10.1016/j.atmosenv.2013.05.030 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 223YN UT WOS:000324848500059 ER PT J AU Collin, R AF Collin, Rachel TI Phylogenetic Patterns and Phenotypic Plasticity of Molluscan Sexual Systems SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article ID CORAL-INHABITING SNAIL; GASTROPOD CREPIDULA-FORNICATA; LIMPET PATELLA-VULGATA; CORALLIOPHILA-VIOLACEA; LIFE-HISTORY; POPULATION-DYNAMICS; SIMULTANEOUS HERMAPHRODITISM; BIVALVES GALEOMMATOIDEA; REPRODUCTIVE-CYCLES; LOTTIA-GIGANTEA AB Molluscs show a wide diversity of sexual systems and strategies. There are both gastropod and bivalve families that are each primarily dioecious, simultaneous hermaphrodites, or sequential hermaphrodites, and other families in which almost every sexual strategy occurs. The multiple evolutionary transitions of sexual systems within molluscs would allow comparative analyses of the associated ecological factors, but data on all but a few groups are too sparse to draw many solid conclusions. The phylogenetic distribution of sexual systems in the Mollusca shows that gastropods and bivalves demonstrate different patterns, possibly associated with the presence/absence of copulation. The distribution of change of sex suggests that, in gastropods, sequential hermaphrodites do not evolve from simultaneous hermaphrodites, and that sex reversal (flip-flopping) occurs in free-spawners but not in copulators. Three well-studied protandrous gastropod groups (calyptraeids, coralliophilids, and patellogastropods) show similar responses to environmental conditions and associations with conspecifics. They all have the following attributes: (1) they are sedentary, (2) they live in groups, patches, or aggregates, and (3) size at sex change varies among sites and among aggregates. In addition the available experimental evidence suggests that (4) the presence of females or large individuals represses growth and sex change of males, and (5) behavior seems to mediate the repressive influence of large females. Available data from other species tend to support these patterns. Finally, the repression of growth of males by females in protandry likely facilitates the evolution of dwarf males. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM collinr@si.edu FU SICB FX I thank Janet Leonard for organizing the symposium "Phenotypic plasticity and the evolution of gender roles" at the 2013 Society of Integrative and Comparative Biology (SICB) meeting, SICB for supporting the symposium, and Smithsonian Tropical Research Institute for supporting my research. I thank David R. Lindberg for discussion, an anonymous reviewer, and Greg Rouse, Julia Schmidt-Peterson and Arthur Anker for permission to use their photographs. NR 97 TC 12 Z9 12 U1 6 U2 59 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD OCT PY 2013 VL 53 IS 4 BP 723 EP 735 DI 10.1093/icb/ict076 PG 13 WC Zoology SC Zoology GA 223TO UT WOS:000324833500016 PM 23784696 ER PT J AU Olsen, K Ritson-Williams, R Ochrietor, JD Paul, VJ Ross, C AF Olsen, K. Ritson-Williams, R. Ochrietor, J. D. Paul, V. J. Ross, C. TI Detecting hyperthermal stress in larvae of the hermatypic coral Porites astreoides: the suitability of using biomarkers of oxidative stress versus heat-shock protein transcriptional expression SO MARINE BIOLOGY LA English DT Article ID ELEVATED-TEMPERATURE; MONTASTRAEA-FAVEOLATA; SCLERACTINIAN CORAL; GENE-EXPRESSION; CLIMATE-CHANGE; REEF CORALS; REDUCES SURVIVORSHIP; OCEAN ACIDIFICATION; ALGAL SYMBIONTS; THERMAL-STRESS AB Scleractinian coral populations are declining worldwide in response to a variety of factors including increases in sea surface temperatures. To evaluate the effects of predicted elevated seawater temperatures on coral recruitment, larvae from the coral Porites astreoides were exposed to seawater at ambient (27.3 A degrees C) or elevated temperature (30.8 A degrees C) conditions for 4, 24, or 48 h. Following exposure, larvae were tested for survival and settlement, oxidative stress, respiratory demand, and mRNA expression of heat-shock proteins (Hsps) 16 and 60. While elevated temperature had no effect on larval survival, settlement, or expression of Hsps, it did cause a significant increase in larval respiration, oxidative damage (lipid peroxidation), and antioxidant enzyme activity (catalase). The absence of a significant up-regulation of Hsp 16 or 60 expression in response to thermal stress suggests that the transcriptional expression of these genes is a less sensitive diagnostic tool compared to biomarkers of oxidative stress at the temperatures examined. The results of this study provide evidence that enhanced levels of oxidative stress are encountered in zooxanthellae-containing coral larvae in response to elevated temperatures and that this occurrence should be strongly considered for use as a biomarker when monitoring sub-lethal cellular responses to rising sea surface temperatures. C1 [Olsen, K.; Ochrietor, J. D.; Ross, C.] Univ N Florida, Dept Biol, Jacksonville, FL 32224 USA. [Ritson-Williams, R.; Paul, V. J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Ross, C (reprint author), Univ N Florida, Dept Biol, 1 UNF Dr, Jacksonville, FL 32224 USA. EM cliff.ross@unf.edu FU University of North Florida; Coastal Biology Program; Mote Protect our Reefs Grant [2011-21] FX We thank Tom Bartlett, Erin Hoover, Erica Robinson, and Rebecca Jamison for assistance with coral collection and larval husbandry. We thank Dr. Eric Johnson for assistance with statistical analysis. We also thank Erich Bartels for field assistance. This work was conducted under permit no. FKNMS-2011-038 issued by the Florida Keys National Marine Sanctuary. This work was supported by the University of North Florida's "Transformational Learning Opportunity" program and Coastal Biology Program. VP and RRW were supported by Mote Protect our Reefs Grant 2011-21. This is contribution #911 of the Smithsonian Marine Station at Ft. Pierce. NR 67 TC 6 Z9 6 U1 2 U2 44 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD OCT PY 2013 VL 160 IS 10 BP 2609 EP 2618 DI 10.1007/s00227-013-2255-z PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 224GP UT WOS:000324871300008 ER PT J AU Bjorndal, KA Schroeder, BA Foley, AM Witherington, BE Bresette, M Clark, D Herren, RM Arendt, MD Schmid, JR Meylan, AB Meylan, PA Provancha, JA Hart, KM Lamont, MM Carthy, RR Bolten, AB AF Bjorndal, Karen A. Schroeder, Barbara A. Foley, Allen M. Witherington, Blair E. Bresette, Michael Clark, David Herren, Richard M. Arendt, Michael D. Schmid, Jeffrey R. Meylan, Anne B. Meylan, Peter A. Provancha, Jane A. Hart, Kristen M. Lamont, Margaret M. Carthy, Raymond R. Bolten, Alan B. TI Temporal, spatial, and body size effects on growth rates of loggerhead sea turtles (Caretta caretta) in the Northwest Atlantic SO MARINE BIOLOGY LA English DT Article ID SOMATIC GROWTH; DEVELOPMENTAL HABITAT; CHELONIA-MYDAS; CLIMATE-CHANGE; POPULATION; DYNAMICS; FLORIDA; LIFE AB In response to a call from the US National Research Council for research programs to combine their data to improve sea turtle population assessments, we analyzed somatic growth data for Northwest Atlantic (NWA) loggerhead sea turtles (Caretta caretta) from 10 research programs. We assessed growth dynamics over wide ranges of geography (9-33A degrees N latitude), time (1978-2012), and body size (35.4-103.3 cm carapace length). Generalized additive models revealed significant spatial and temporal variation in growth rates and a significant decline in growth rates with increasing body size. Growth was more rapid in waters south of the USA (< 24A degrees N) than in USA waters. Growth dynamics in southern waters in the NWA need more study because sample size was small. Within USA waters, the significant spatial effect in growth rates of immature loggerheads did not exhibit a consistent latitudinal trend. Growth rates declined significantly from 1997 through 2007 and then leveled off or increased. During this same interval, annual nest counts in Florida declined by 43 % (Witherington et al. in Ecol Appl 19:30-54, 2009) before rebounding. Whether these simultaneous declines reflect responses in productivity to a common environmental change should be explored to determine whether somatic growth rates can help interpret population trends based on annual counts of nests or nesting females. Because of the significant spatial and temporal variation in growth rates, population models of NWA loggerheads should avoid employing growth data from restricted spatial or temporal coverage to calculate demographic metrics such as age at sexual maturity. C1 [Bjorndal, Karen A.; Witherington, Blair E.; Lamont, Margaret M.; Carthy, Raymond R.; Bolten, Alan B.] Univ Florida, Archie Carr Ctr Sea Turtle Res, Gainesville, FL 32611 USA. [Bjorndal, Karen A.; Bolten, Alan B.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Schroeder, Barbara A.] NOAA, Natl Marine Fisheries Serv, Silver Spring, MD 20910 USA. [Foley, Allen M.] Fish & Wildlife Res Inst, Florida Fish & Wildlife Conservat Commiss, Jacksonville, FL 32218 USA. [Witherington, Blair E.] Fish & Wildlife Res Inst, Florida Fish & Wildlife Conservat Commiss, Melbourne Beach, FL 32951 USA. [Witherington, Blair E.; Bresette, Michael; Clark, David; Herren, Richard M.] Inwater Res Grp Inc, Jensen Beach, FL 34957 USA. [Arendt, Michael D.] South Carolina Dept Nat Resources, Marine Resources Div, Charleston, SC 29412 USA. [Schmid, Jeffrey R.] Conservancy Southwest Florida, Dept Environm Sci, Naples, FL 34102 USA. [Meylan, Anne B.] Fish & Wildlife Res Inst, Florida Fish & Wildlife Conservat Commiss, St Petersburg, FL 33701 USA. [Meylan, Anne B.; Meylan, Peter A.] Smithsonian Trop Res Inst, Balboa, Panama. [Meylan, Peter A.] Eckerd Coll, Nat Sci Coll, St Petersburg, FL 33711 USA. [Provancha, Jane A.] InoMed Hlth Applicat, Kennedy Space Ctr, Merritt Isl, FL 32899 USA. [Hart, Kristen M.] US Geol Survey, Southeast Ecol Sci Ctr, Davie, FL 33314 USA. [Lamont, Margaret M.; Carthy, Raymond R.] Univ Florida, US Geol Survey, Florida Cooperat Fish & Wildlife Res Unit, Gainesville, FL 32611 USA. RP Bjorndal, KA (reprint author), Univ Florida, Archie Carr Ctr Sea Turtle Res, Gainesville, FL 32611 USA. EM bjorndal@ufl.edu OI Bjorndal, Karen/0000-0002-6286-1901 FU Disney Worldwide Conservation Fund; Florida Fish and Wildlife Conservation Commission; NASA-John F. Kennedy Space Center; National Marine Fisheries Service; National Park Service; US Geological Survey; Wildlife Conservation Society (New York) FX We are very grateful to the many people who assisted with turtle captures and measurements: B. Bolt, A. Brame, B. Brost, R. Burrows, J. Byrd, R. Cancro, E. Chadwick, M. Cherkiss, S. Connett, C. Crady, B. Crouchley, S. Gann, C. Hackett, T. Hirama, R. Lowers, K. Holloway-Adkins, K. Ludwig, K. Minch, H. Nixon, J. Nixon, S. Nixon, L. Ogren, M. Provancha, T. Redlow, E. Reyier, B. Reynolds, A. Sartain, D. Scheidt, J. Schwenter, A. Segars, B. Stephens, and W. Witzell. For logistical support, we thank C. Douglass, J. Douglass, T. Gottshall, K. Nimmo, J. Spade, and T. Ziegler. For data management, we thank P.E. Eliazar. We used the Maptool program (see www.seaturtle.org) to create the map in this paper. Our studies were supported by several funding sources: Disney Worldwide Conservation Fund, Florida Fish and Wildlife Conservation Commission, NASA-John F. Kennedy Space Center, National Marine Fisheries Service, National Park Service, US Geological Survey, and the Wildlife Conservation Society (New York). All turtle captures and handling were conducted with appropriate national and state research permits and approved IACUC protocols, where applicable. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the US Government. NR 33 TC 8 Z9 8 U1 3 U2 46 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD OCT PY 2013 VL 160 IS 10 BP 2711 EP 2721 DI 10.1007/s00227-013-2264-y PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 224GP UT WOS:000324871300016 ER PT J AU Hrcek, J Miller, SE Whitfield, JB Shima, H Novotny, V AF Hrcek, Jan Miller, Scott E. Whitfield, James B. Shima, Hiroshi Novotny, Vojtech TI Parasitism rate, parasitoid community composition and host specificity on exposed and semi-concealed caterpillars from a tropical rainforest SO OECOLOGIA LA English DT Article DE Lepidoptera; Specialization; Community structure; External feeding; Malesia ID PAPUA-NEW-GUINEA; HERBIVOROUS INSECTS; DNA BARCODES; SPECIES RICHNESS; TORTRICOID HOSTS; FLIES DIPTERA; LEAF QUALITY; FOOD WEBS; ASSEMBLAGES; LEPIDOPTERA AB The processes maintaining the enormous diversity of herbivore-parasitoid food webs depend on parasitism rate and parasitoid host specificity. The two parameters have to be evaluated in concert to make conclusions about the importance of parasitoids as natural enemies and guide biological control. We document parasitism rate and host specificity in a highly diverse caterpillar-parasitoid food web encompassing 266 species of lepidopteran hosts and 172 species of hymenopteran or dipteran parasitoids from a lowland tropical forest in Papua New Guinea. We found that semi-concealed hosts (leaf rollers and leaf tiers) represented 84 % of all caterpillars, suffered a higher parasitism rate than exposed caterpillars (12 vs. 5 %) and their parasitoids were also more host specific. Semi-concealed hosts may therefore be generally more amenable to biological control by parasitoids than exposed ones. Parasitoid host specificity was highest in Braconidae, lower in Diptera: Tachinidae, and, unexpectedly, the lowest in Ichneumonidae. This result challenges the long-standing view of low host specificity in caterpillar-attacking Tachinidae and suggests higher suitability of Braconidae and lower suitability of Ichneumonidae for biological control of caterpillars. Semi-concealed hosts and their parasitoids are the largest, yet understudied component of caterpillar-parasitoid food webs. However, they still remain much closer in parasitism patterns to exposed hosts than to what literature reports on fully concealed leaf miners. Specifically, semi-concealed hosts keep an equally low share of idiobionts (2 %) as exposed caterpillars. C1 [Hrcek, Jan; Novotny, Vojtech] Univ South Bohemia, Fac Sci, Ceske Budejovice 37005, Czech Republic. [Hrcek, Jan; Novotny, Vojtech] Acad Sci Czech Republic, Ctr Biol, Ceske Budejovice 37005, Czech Republic. [Miller, Scott E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Whitfield, James B.] Univ Illinois, Dept Entomol, Urbana, IL 61801 USA. [Shima, Hiroshi] Kyushu Univ, Kyushu Univ Museum, Higashi Ku, Fukuoka 8128581, Japan. RP Hrcek, J (reprint author), Univ South Bohemia, Fac Sci, Branisovska 31, Ceske Budejovice 37005, Czech Republic. EM janhrcek@gmail.com RI Novotny, Vojtech/G-9434-2014; Hrcek, Jan/D-7335-2015; U-ID, Kyushu/C-5291-2016; OI Novotny, Vojtech/0000-0001-7918-8023; Hrcek, Jan/0000-0003-0711-6447; Miller, Scott/0000-0002-4138-1378 FU US National Science Foundation [DEB 0841885]; Czech Science Foundation [206/09/0115, 13-10486S]; Academy of Sciences of the Czech Republic [IAA600960712]; Czech Ministry of Education [LH11008, MSM6007665801]; European Social Fund [CZ. 1.07/2.3.00/20.0064]; state budget of the Czech Republic; NSF; Genome Canada through the Ontario Genomics Institute FX We thank the New Guinea Binatang Research Center parataxonomists, village assistants, Lauren Helgen, Karolyn Darrow and Kristyna Hrckova for technical assistance and general support. Host plants were identified by George D. Weiblen. Lepidopteran taxonomy was assisted by Jeremy Holloway, Jadranka Rota, Michael Shaffer, Tosio Kumata, Issei Ohshima, and others acknowledged in Craft et al. (2010). Parasitoids were identified by: Kees van Achterberg (Macrocentrinae), Celso Oliveira Azevedo (Bethylidae), Yves Braet (Orgilinae), Michael W. Gates (Chalcidoidea), Ian D. Gauld (Ichneumonidae), Donald L. J. Quicke (Rogadinae and Hormiinae), Michael J. Sharkey (Agathidinae), David Wahl (Ichneumonidae), and Dicky Yu (Cheloninae). This paper is based on work supported by the US National Science Foundation (DEB 0841885), the Czech Science Foundation (206/09/0115 and 13-10486S), the Academy of Sciences of the Czech Republic (IAA600960712), the Czech Ministry of Education (LH11008 and MSM6007665801), and the project CZ. 1.07/2.3.00/20.0064 co-financed by the European Social Fund and the state budget of the Czech Republic. The Papua New Guinea caterpillar rearing campaign has been funded by NSF since 1995 in collaboration with George Weiblen and Yves Basset. We thank Paul Hebert, Alex Smith and the Biodiversity Institute of Ontario for the DNA barcodes. Laboratory reagents and BOLD infrastructure were funded by Genome Canada through the Ontario Genomics Institute. We also thank David Wahl, Tom Fayle, Kees van Achterberg, Becky Morris, Owen Lewis, David Storch and two anonymous reviewers for comments on the manuscript. NR 72 TC 18 Z9 18 U1 1 U2 61 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD OCT PY 2013 VL 173 IS 2 BP 521 EP 532 DI 10.1007/s00442-013-2619-6 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 226IJ UT WOS:000325028500018 PM 23463243 ER PT J AU Lambert, JB Donnelly, EW Heckenbach, EA Johnson, CL Kozminski, MA Wu, YY Santiago-Blay, JA AF Lambert, Joseph B. Donnelly, Eric W. Heckenbach, Eric A. Johnson, Connor L. Kozminski, Michael A. Wu, Yuyang Santiago-Blay, Jorge A. TI Molecular classification of the natural exudates of the rosids SO PHYTOCHEMISTRY LA English DT Article DE Exudates; Fabids; Gums; Malvids; Nuclear magnetic resonance spectroscopy; Resins; Rosids ID NUCLEAR-MAGNETIC-RESONANCE; GARCINIA-MANGOSTANA; RESINOUS EXUDATE; EUCALYPT KINOS; FLAVONOIDS; GUM; ANACARDIACEAE; FICUS; L.; SPECTROSCOPY AB Exudates of the rosid clade of the eudicots have been surveyed and characterized by carbon-13 and proton nuclear magnetic resonance spectroscopy. Of 554 samples divided roughly equally between the subclades fabids and malvids, about two-fifths are resins, a third gums, one-ninth gum resins, one-twelfth kinos, and the remaining not affiliated with these four main molecular classes. Two small new molecular classes, respectively from the Clusiaceae (xanthics) and the Zygophyllaceae (guaiacs), are identified and described. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Lambert, Joseph B.; Johnson, Connor L.] Trinity Univ, Dept Chem, San Antonio, TX 78212 USA. [Lambert, Joseph B.; Donnelly, Eric W.; Heckenbach, Eric A.; Kozminski, Michael A.; Wu, Yuyang] Northwestern Univ, Dept Chem, Evanston, IL 60208 USA. [Santiago-Blay, Jorge A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Santiago-Blay, Jorge A.] Univ Puerto Rico, Dept Crops & Agroenvironm Sci, Mayaguez, PR USA. RP Lambert, JB (reprint author), Trinity Univ, Dept Chem, 1 Trinity Pl, San Antonio, TX 78212 USA. EM jlambert@northwestern.edu RI Wu, Ying/B-7283-2009 FU Gallaudet University, Washington, DC; Penn State York FX The authors are grateful to grants from Gallaudet University, Washington, DC, and Penn State York for support of this work. The many individuals who provided samples are acknowledged in Table S1. We are particularly indebted to Lisa M. Campbell of the New York Botanical Garden, Christine Niezgoda of the Field Museum, and Stephanie Zabel of the Harvard University Herbaria. NR 54 TC 0 Z9 3 U1 5 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0031-9422 J9 PHYTOCHEMISTRY JI Phytochemistry PD OCT PY 2013 VL 94 BP 171 EP 183 DI 10.1016/j.phytochem.2013.06.013 PG 13 WC Biochemistry & Molecular Biology; Plant Sciences SC Biochemistry & Molecular Biology; Plant Sciences GA 222HF UT WOS:000324721100019 PM 23870288 ER PT J AU Drexler, JF Geipel, A Konig, A Corman, VM van Riel, D Leijten, LM Bremer, CM Rasche, A Cottontail, VM Maganga, GD Schlegel, M Muller, MA Adam, A Klose, SM Carneiro, AJB Stocker, A Franke, CR Gloza-Rausch, F Geyer, J Annan, A Adu-Sarkodie, Y Oppong, S Binger, T Vallo, P Tschapka, M Ulrich, RG Gerlich, WH Leroy, E Kuiken, T Glebe, D Drosten, C AF Drexler, Jan Felix Geipel, Andreas Koenig, Alexander Corman, Victor M. van Riel, Debby Leijten, Lonneke M. Bremer, Corinna M. Rasche, Andrea Cottontail, Veronika M. Maganga, Gael D. Schlegel, Mathias Mueller, Marcel A. Adam, Alexander Klose, Stefan M. Borges Carneiro, Aroldo Jose Stoecker, Andreas Franke, Carlos Roberto Gloza-Rausch, Florian Geyer, Joachim Annan, Augustina Adu-Sarkodie, Yaw Oppong, Samuel Binger, Tabea Vallo, Peter Tschapka, Marco Ulrich, Rainer G. Gerlich, Wolfram H. Leroy, Eric Kuiken, Thijs Glebe, Dieter Drosten, Christian TI Bats carry pathogenic hepadnaviruses antigenically related to hepatitis B virus and capable of infecting human hepatocytes SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE evolution; zoonosis; virome; metagenomics; reverse genetics ID WOOLLY MONKEY; ENTRY; TRANSMISSION; GENOTYPES; PRIMATES; PROTEIN; SURFACE; ORIGIN; MICE; DNA AB The hepatitis B virus (HBV), family Hepadnaviridae, is one of most relevant human pathogens. HBV origins are enigmatic, and no zoonotic reservoirs are known. Here, we screened 3,080 specimens from 54 bat species representing 11 bat families for hepadnaviral DNA. Ten specimens (0.3%) from Panama and Gabon yielded unique hepadnaviruses in coancestral relation to HBV. Full genome sequencing allowed classification as three putative orthohepadnavirus species based on genome lengths (3,149-3,377 nt), presence of middle HBV surface and X-protein genes, and sequence distance criteria. Hepatic tropism in bats was shown by quantitative PCR and in situ hybridization. Infected livers showed histopathologic changes compatible with hepatitis. Human hepatocytes transfected with all three bat viruses cross-reacted with sera against the HBV core protein, concordant with the phylogenetic relatedness of these hepadnaviruses and HBV. One virus from Uroderma bilobatum, the tent-making bat, cross-reacted with monoclonal antibodies against the HBV antigenicity determining S domain. Up to 18.4% of bat sera contained antibodies against bat hepadnaviruses. Infectious clones were generated to study all three viruses in detail. Hepatitis D virus particles pseudotyped with surface proteins of U. bilobatum HBV, but neither of the other two viruses could infect primary human and Tupaia belangeri hepatocytes. Hepatocyte infection occurred through the human HBV receptor sodium taurocholate cotransporting polypeptide but could not be neutralized by sera from vaccinated humans. Antihepadnaviral treatment using an approved reverse transcriptase inhibitor blocked replication of all bat hepadnaviruses. Our data suggest that bats may have been ancestral sources of primate hepadnaviruses. The observed zoonotic potential might affect concepts aimed at eradicating HBV. C1 [Drexler, Jan Felix; Corman, Victor M.; Rasche, Andrea; Mueller, Marcel A.; Gloza-Rausch, Florian; Binger, Tabea; Drosten, Christian] Univ Bonn, Med Ctr, Inst Virol, D-53127 Bonn, Germany. [Geipel, Andreas; Koenig, Alexander; Bremer, Corinna M.; Gerlich, Wolfram H.; Glebe, Dieter] Univ Giessen, Inst Med Virol, D-35392 Giessen, Germany. [van Riel, Debby; Leijten, Lonneke M.; Kuiken, Thijs] Erasmus MC, Depart Virosci, NL-3000 CA Rotterdam, Netherlands. [Cottontail, Veronika M.; Klose, Stefan M.; Vallo, Peter; Tschapka, Marco] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Cottontail, Veronika M.; Tschapka, Marco] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Maganga, Gael D.; Leroy, Eric] Ctr Int Rech Med Franceville, Franceville, Gabon. [Schlegel, Mathias; Ulrich, Rainer G.] Friedrich Loeffler Inst, Inst Novel & Emerging Infect Dis, D-17493 Greifswald, Germany. [Adam, Alexander] Univ Cologne, Med Ctr, Inst Pathol, D-50937 Cologne, Germany. [Borges Carneiro, Aroldo Jose; Franke, Carlos Roberto] Univ Fed Bahia, Sch Vet Med, BR-40170110 Salvador, BA, Brazil. [Stoecker, Andreas] Univ Fed Bahia, Univ Hosp Prof Edgard Santos, Infect Dis Res Lab, BR-40110060 Salvador, BA, Brazil. [Gloza-Rausch, Florian] Ctr Bat Protect & Informat, Noctalis, D-23795 Bad Segeberg, Germany. [Geyer, Joachim] Univ Giessen, Biomed Res Ctr, Inst Pharmacol & Toxicol, D-35392 Giessen, Germany. [Annan, Augustina] Kumasi Ctr Collaborat Res Trop Med KCCR, Kumasi, Ghana. [Adu-Sarkodie, Yaw; Oppong, Samuel] Kwame Nkrumah Univ Sci & Technol, Fac Renewable Nat Resources, Kumasi, Ghana. [Vallo, Peter] Acad Sci Czech Republic, Inst Vertebrate Biol, CS-60365 Brno, Czech Republic. [Leroy, Eric] Univ Montpellier I, CNRS, IRD, UMR 224,MIVEGEC, F-34032 Rennes, France. RP Glebe, D (reprint author), Univ Giessen, Inst Med Virol, D-35392 Giessen, Germany. EM dieter.glebe@viro.med.uni-giessen.de; drosten@virology-bonn.de RI Drexler, Jan Felix/C-1004-2014; Vallo, Peter/F-9650-2014; LEROY, Eric/I-4347-2016; OI Konig, Alexander/0000-0002-6137-9240; LEROY, Eric/0000-0003-0022-0890; Mueller, Marcel/0000-0003-2242-5117; Corman, Victor Max/0000-0002-3605-0136 FU German Research Foundation (DFG) [SPP 1596, DR 810/1-1, GL 595/4-1, TS 81/6-1, DR 772/3-1, KA1241/18-1]; Brazilian Foundation [SUS0038/2007]; European Union [223498]; Europan Virus Archive Grant [228292]; Anticipating the Global Onset of Novel Epidemics Grant [278976]; German Federal Ministry of Education and Research (BMBF) [01KI1016D]; Smithsonian Tropical Research Institute; German National Academic Foundation FX We thank Monika Eschbach-Bludau, Sebastian Brunink, Tobias Bleicker, Thomas Kruppa, Mathieu Bourgarel, Vanessa Russeler, and Sigrun Broehl for technical assistance; Barbara Doring for the hNTCP-FLAG construct; Micha Nubling for HBV standards; and Aurelija Zvirbliene for mAb HB1. This study was funded by German Research Foundation (DFG) SPP 1596 Grants DR 810/1-1 (to J.F.D., M. T., and D. G.), GL 595/4-1 (to J.F.D., M. T., and D. G.), TS 81/6-1 (to J.F.D., M. T., and D. G.), DR 772/3-1 (to C. D.), and KA1241/18-1 (to M. T.); Brazilian Foundation for Research Support of the State of Bahia Grant SUS0038/2007 (to J.F.D. and C. R. F.); European Union FP7 Projects European Management Platform for Emerging and Re-Emerging Infectious Disease Entities Grant 223498; Europan Virus Archive Grant 228292 (to C. D.); Anticipating the Global Onset of Novel Epidemics Grant 278976 (to C. D.); and German Federal Ministry of Education and Research (BMBF) Grant 01KI1016D (to C. D.). The subproject in Panama was supported by the Smithsonian Tropical Research Institute and a personal scholarship of the German National Academic Foundation (to V. M. Cottontail). NR 41 TC 61 Z9 63 U1 1 U2 23 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 OCT 1 PY 2013 VL 110 IS 40 BP 16151 EP 16156 DI 10.1073/pnas.1308049110 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 227II UT WOS:000325105500072 PM 24043818 ER PT J AU Stromberg, EE Power, ML MacCorkle, NM AF Stromberg, E. E. Power, M. L. MacCorkle, N. Meese TI POSITIVE REINFORCEMENT TRAINING AS A METHOD OF LONGITUDINAL MILK COLLECTION IN A WESTERN LOWLAND GORILLA (GORILLA GORILLA GORILLA) SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract CT 36th Annual Meeting of the American-Society-of-Primatologists CY JUN 19-22, 2013 CL San Juan, PR SP Amer Soc Primatologists C1 [Stromberg, E. E.; MacCorkle, N. Meese] Smithsonian Natl Zool Pk, Washington, DC 20008 USA. NR 0 TC 0 Z9 0 U1 0 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD OCT PY 2013 VL 75 SU 1 MA 125 BP 69 EP 69 PG 1 WC Zoology SC Zoology GA 205BF UT WOS:000323414700124 ER PT J AU Gregory, T Rueda, FC Deichmann, J Kolowski, J Alonso, A AF Gregory, T. Rueda, F. Carrasco Deichmann, J. Kolowski, J. Alonso, A. TI CANOPY CAMERA TRAPPING: AN EFFECTIVE TOOL FOR NON-INVASIVE DATA COLLECTION SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract CT 36th Annual Meeting of the American-Society-of-Primatologists CY JUN 19-22, 2013 CL San Juan, PR SP Amer Soc Primatologists C1 [Gregory, T.; Rueda, F. Carrasco; Deichmann, J.; Kolowski, J.; Alonso, A.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. NR 0 TC 0 Z9 0 U1 1 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD OCT PY 2013 VL 75 SU 1 MA 137 BP 73 EP 73 PG 1 WC Zoology SC Zoology GA 205BF UT WOS:000323414700135 ER PT J AU Bentley-Condit, VK Power, M AF Bentley-Condit, V. K. Power, M. TI MICRONUTRIENT CONTENT OF SELECTED YELLOW BABOON (PAPIO CYNOCEPHALUS) FOODS AT THE TANA RIVER PRIMATE NATIONAL RESERVE, KENYA SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract CT 36th Annual Meeting of the American-Society-of-Primatologists CY JUN 19-22, 2013 CL San Juan, PR SP Amer Soc Primatologists C1 [Bentley-Condit, V. K.] Grinnell Coll, Dept Anthropol, Grinnell, IA 50112 USA. [Power, M.] Smithsonian Inst, Conservat Ecol Ctr, Nutr Lab, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD OCT PY 2013 VL 75 SU 1 MA 174 BP 85 EP 85 PG 1 WC Zoology SC Zoology GA 205BF UT WOS:000323414700171 ER PT J AU DeLuycker, AM AF DeLuycker, A. M. TI DIET AND FORAGING ECOLOGY OF THE CRITICALLY ENDANGERED ANDEAN TITI MONKEY (CALLICEBUS OENANTHE) IN NORTHERN PERU SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract CT 36th Annual Meeting of the American-Society-of-Primatologists CY JUN 19-22, 2013 CL San Juan, PR SP Amer Soc Primatologists C1 [DeLuycker, A. M.] Smithsonian Conservat Biol Inst, Smithsonian Mason Sch Conservat, Front Royal, VA 22630 USA. NR 0 TC 0 Z9 0 U1 0 U2 20 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD OCT PY 2013 VL 75 SU 1 MA 200 BP 93 EP 93 PG 1 WC Zoology SC Zoology GA 205BF UT WOS:000323414700196 ER PT J AU Norconk, MA Gregory, T Thompson, CL AF Norconk, M. A. Gregory, T. Thompson, C. L. TI OVERVIEW OF THE PITHECIIDS WITH A FOCUS ON SOCIOECOLOGY SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract CT 36th Annual Meeting of the American-Society-of-Primatologists CY JUN 19-22, 2013 CL San Juan, PR SP Amer Soc Primatologists C1 [Norconk, M. A.] Kent State Univ, Kent, OH 44242 USA. [Gregory, T.] Smithsonian Inst, Washington, DC 20560 USA. [Thompson, C. L.] Northeast Ohio Med Univ, Rootstown, OH USA. NR 0 TC 0 Z9 0 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD OCT PY 2013 VL 75 SU 1 MA 198 BP 93 EP 93 PG 1 WC Zoology SC Zoology GA 205BF UT WOS:000323414700194 ER PT J AU Gregory, T Bowler, M AF Gregory, T. Bowler, M. TI BANDS OF BROTHERS? COMPARATIVE SOCIAL BEHAVIOR IN THE LARGE-BODIED PITHECIINES: CACAJAO AND CHIROPOTES SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract CT 36th Annual Meeting of the American-Society-of-Primatologists CY JUN 19-22, 2013 CL San Juan, PR SP Amer Soc Primatologists C1 [Gregory, T.] Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Bowler, M.] San Diego Zoo Global Inst Conservat Res, Escondido, CA 92027 USA. NR 0 TC 0 Z9 0 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD OCT PY 2013 VL 75 SU 1 MA 202 BP 94 EP 94 PG 1 WC Zoology SC Zoology GA 205BF UT WOS:000323414700197 ER PT J AU Evans, NR Bond, HE Schaefer, GH Mason, BD Karovska, M Tingle, E AF Evans, Nancy Remage Bond, Howard E. Schaefer, Gail H. Mason, Brian D. Karovska, Margarita Tingle, Evan TI BINARY CEPHEIDS: SEPARATIONS AND MASS RATIOS IN 5 M-circle dot BINARIES SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; stars: massive; stars: variables: Cepheids ID BRIGHTEST NORTHERN CEPHEIDS; HUBBLE-SPACE-TELESCOPE; SOLAR-TYPE STARS; CLASSICAL CEPHEID; V1334 CYGNI; V350 SGR; MULTIPLICITY; COMPANIONS; LUMINOSITY; ORBIT AB Deriving the distribution of binary parameters for a particular class of stars over the full range of orbital separations usually requires the combination of results from many different observing techniques (radial velocities, interferometry, astrometry, photometry, direct imaging), each with selection biases. However, Cepheids-cool, evolved stars of similar to 5 M-circle dot-are a special case because ultraviolet (UV) spectra will immediately reveal any companion star hotter than early type A, regardless of the orbital separation. We have used International Ultraviolet Explorer UV spectra of a complete sample of all 76 Cepheids brighter than V = 8 to create a list of all 18 Cepheids with companions more massive than 2.0 M-circle dot. Orbital periods of many of these binaries are available from radial-velocity studies, or can be estimated for longer-period systems from detected velocity variability. In an imaging survey with the Hubble Space Telescope Wide Field Camera 3, we resolved three of the companions (those of eta Aql, S Nor, and V659 Cen), allowing us to make estimates of the periods out to the long-period end of the distribution. Combining these separations with orbital data in the literature, we derive an unbiased distribution of binary separations, orbital periods, and mass ratios. The distribution of orbital periods shows that the 5 M-circle dot binaries have systematically shorter periods than do 1 M-circle dot stars. Our data also suggest that the distribution of mass ratios depends on both binary separation and system multiplicity. The distribution of mass ratios as a function of orbital separation, however, does not depend on whether a system is a binary or a triple. C1 [Evans, Nancy Remage; Karovska, Margarita; Tingle, Evan] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Bond, Howard E.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Bond, Howard E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schaefer, Gail H.] Georgia State Univ, CHARA Array, Atlanta, GA 30302 USA. [Mason, Brian D.] USN Observ, Washington, DC 20392 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA. EM nevans@cfa.harvard.edu; heb11@psu.edu; schaefer@chara-array.org FU HST grant [GO-12215.01-A]; Chandra X-Ray Center NASA Contract [NAS8-03060] FX It is a pleasure to thank H. Harris and K. Kratter for valuable discussions. IUE continues to provide a valuable foundation for Cepheid companion studies. Support for this work was also provided by HST grant GO-12215.01-A and from the Chandra X-Ray Center NASA Contract NAS8-03060. VizieR and SIMBAD were used in the preparation of this study. NR 43 TC 16 Z9 16 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2013 VL 146 IS 4 AR 93 DI 10.1088/0004-6256/146/4/93 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 218AL UT WOS:000324404800022 ER PT J AU Tingay, SJ Kaplan, DL McKinley, B Briggs, F Wayth, RB Hurley-Walker, N Kennewell, J Smith, C Zhang, K Arcus, W Bhat, NDR Emrich, D Herne, D Kudryavtseva, N Lynch, M Ord, SM Waterson, M Barnes, DG Bell, M Gaensler, BM Lenc, E Bernardi, G Greenhill, LJ Kasper, JC Bowman, JD Jacobs, D Bunton, JD deSouza, L Koenig, R Pathikulangara, J Stevens, J Cappallo, RJ Corey, BE Kincaid, BB Kratzenberg, E Lonsdale, CJ McWhirter, SR Rogers, AEE Salah, JE Whitney, AR Deshpande, A Prabu, T Shankar, NU Srivani, KS Subrahmanyan, R Ewall-Wice, A Feng, L Goeke, R Morgan, E Remillard, RA Williams, CL Hazelton, BJ Morales, MF Johnston-Hollitt, M Mitchell, DA Procopio, P Riding, J Webster, RL Wyithe, JSB Oberoi, D Roshi, A Sault, RJ Williams, A AF Tingay, S. J. Kaplan, D. L. McKinley, B. Briggs, F. Wayth, R. B. Hurley-Walker, N. Kennewell, J. Smith, C. Zhang, K. Arcus, W. Bhat, N. D. R. Emrich, D. Herne, D. Kudryavtseva, N. Lynch, M. Ord, S. M. Waterson, M. Barnes, D. G. Bell, M. Gaensler, B. M. Lenc, E. Bernardi, G. Greenhill, L. J. Kasper, J. C. Bowman, J. D. Jacobs, D. Bunton, J. D. deSouza, L. Koenig, R. Pathikulangara, J. Stevens, J. Cappallo, R. J. Corey, B. E. Kincaid, B. B. Kratzenberg, E. Lonsdale, C. J. McWhirter, S. R. Rogers, A. E. E. Salah, J. E. Whitney, A. R. Deshpande, A. Prabu, T. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Ewall-Wice, A. Feng, L. Goeke, R. Morgan, E. Remillard, R. A. Williams, C. L. Hazelton, B. J. Morales, M. F. Johnston-Hollitt, M. Mitchell, D. A. Procopio, P. Riding, J. Webster, R. L. Wyithe, J. S. B. Oberoi, D. Roshi, A. Sault, R. J. Williams, A. TI ON THE DETECTION AND TRACKING OF SPACE DEBRIS USING THE MURCHISON WIDEFIELD ARRAY. I. SIMULATIONS AND TEST OBSERVATIONS DEMONSTRATE FEASIBILITY SO ASTRONOMICAL JOURNAL LA English DT Article DE Earth; instrumentation: interferometers; planets and satellites: general; planets and satellites: individual (International Space Station); techniques: radar astronomy AB The Murchison Widefield Array (MWA) is a new low-frequency interferometric radio telescope, operating in the benign radio frequency environment of remote Western Australia. The MWA is the low-frequency precursor to the Square Kilometre Array (SKA) and is the first of three SKA precursors to be operational, supporting a varied science mission ranging from the attempted detection of the Epoch of Reionization to the monitoring of solar flares and space weather. In this paper we explore the possibility that the MWA can be used for the purposes of Space Situational Awareness (SSA). In particular we propose that the MWA can be used as an element of a passive radar facility operating in the frequency range 87.5-108 MHz (the commercial FM broadcast band). In this scenario the MWA can be considered the receiving element in a bi-static radar configuration, with FM broadcast stations serving as non-cooperative transmitters. The FM broadcasts propagate into space, are reflected off debris in Earth orbit, and are received at the MWA. The imaging capabilities of the MWA can be used to simultaneously detect multiple pieces of space debris, image their positions on the sky as a function of time, and provide tracking data that can be used to determine orbital parameters. Such a capability would be a valuable addition to Australian and global SSA assets, in terms of southern and eastern hemispheric coverage. We provide a feasibility assessment of this proposal, based on simple calculations and electromagnetic simulations, that shows that the detection of sub-meter size debris should be possible (debris radius of >0.5 m to similar to 1000 km altitude). We also present a proof-of-concept set of observations that demonstrate the feasibility of the proposal, based on the detection and tracking of the International Space Station via reflected FM broadcast signals originating in southwest Western Australia. These observations broadly validate our calculations and simulations. We discuss some significant challenges that need to be addressed in order to turn the feasible concept into a robust operational capability for SSA. The aggregate received power due to reflections off space debris in the FM band is equivalent to a <1 mJy increase in the background confusion noise for the long integrations needed for Epoch of Reionization experiments, which is insignificant. C1 [Tingay, S. J.; Wayth, R. B.; Hurley-Walker, N.; Kennewell, J.; Arcus, W.; Bhat, N. D. R.; Emrich, D.; Herne, D.; Kudryavtseva, N.; Lynch, M.; Ord, S. M.; Waterson, M.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Tingay, S. J.; McKinley, B.; Briggs, F.; Bell, M.; Gaensler, B. M.; Lenc, E.; Johnston-Hollitt, M.; Mitchell, D. A.; Procopio, P.; Riding, J.; Webster, R. L.; Wyithe, J. S. B.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [Kaplan, D. L.] Univ Wisconsin, Milwaukee, WI 53201 USA. [McKinley, B.; Briggs, F.] Australian Natl Univ, Canberra, ACT, Australia. [Smith, C.] Electro Opt Syst Pty Ltd, Canberra, ACT, Australia. [Zhang, K.] RMIT Univ, Melbourne, Vic, Australia. [Barnes, D. G.] Monash Univ, Monash eRes Ctr, Clayton, Vic, Australia. [Bell, M.; Gaensler, B. M.; Lenc, E.] Univ Sydney, Sydney, NSW 2006, Australia. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Bowman, J. D.; Jacobs, D.] Arizona State Univ, Tempe, AZ USA. [Cappallo, R. J.; Corey, B. E.; Kincaid, B. B.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Rogers, A. E. E.; Salah, J. E.; Whitney, A. R.] MIT Haystack Observ, Westford, MA USA. [Deshpande, A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Ewall-Wice, A.; Feng, L.; Goeke, R.; Morgan, E.; Remillard, R. A.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA USA. [Williams, C. L.; Hazelton, B. J.] Univ Washington, Seattle, WA 98195 USA. [Morales, M. F.] Victoria Univ Wellington, Wellington, New Zealand. [Johnston-Hollitt, M.; Mitchell, D. A.; Procopio, P.; Riding, J.; Webster, R. L.; Wyithe, J. S. B.; Sault, R. J.] Univ Melbourne, Melbourne, Vic, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune, Maharashtra, India. [Roshi, A.] Natl Radio Astron Observ, Charlottesville, VA USA. [Williams, A.] Univ Western Australia, Int Ctr Radio Astron Res, Perth, WA 6009, Australia. RP Tingay, SJ (reprint author), Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. EM s.tingay@curtin.edu.au RI Kudryavtseva, Nadezhda/F-2472-2013; Williams, Andrew/K-2931-2013; Bunton, John/A-4944-2008; Wayth, Randall/B-2444-2013; Udayashankar , N/D-4901-2012; M, Manjunath/N-4000-2014; Hurley-Walker, Natasha/B-9520-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; OI /0000-0002-0086-7363; Gaensler, Bryan/0000-0002-3382-9558; Lenc, Emil/0000-0002-9994-1593; Kudryavtseva, Nadia/0000-0002-1372-0942; Williams, Andrew/0000-0001-9080-0105; Wayth, Randall/0000-0002-6995-4131; M, Manjunath/0000-0001-8710-0730; Hurley-Walker, Natasha/0000-0002-5119-4808; Emrich, David/0000-0002-4058-1837; Wyithe, Stuart/0000-0001-7956-9758 FU U.S. National Science Foundation [AST CAREER-0847753, AST-0457585, AST-0908884, AST-1008353, PHY-0835713]; Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence); New Zealand Ministry of Economic Development [MED-E1799]; IBM Shared University Research Grant (via VUW Curtin); Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington; Australian Federal government via the National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; iVEC Petabyte Data Store; Initiative in Innovative Computing; NVIDIA; International Centre for Radio Astronomy Research; Curtin University; University of Western Australia; Western Australian State government; [CE110001020] FX We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (grants AST CAREER-0847753, AST-0457585, AST-0908884, AST-1008353, and PHY-0835713), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020), New Zealand Ministry of Economic Development (grant MED-E1799), an IBM Shared University Research Grant (via VUW & Curtin), the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, the Victoria University of Wellington, the Australian Federal government via the National Collaborative Research Infrastructure Strategy, Education Investment Fund and the Australia India Strategic Research Fund and Astronomy Australia Limited, under contract to Curtin University, the iVEC Petabyte Data Store, the Initiative in Innovative Computing and NVIDIA sponsored CUDA Center for Excellence at Harvard, and the International Centre for Radio Astronomy Research, a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. The electromagnetic simulations were performed by Gary Bedrosian and Randy Ward of Remcom Inc. NR 19 TC 8 Z9 8 U1 0 U2 18 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 OCT PY 2013 VL 146 IS 4 AR 103 DI 10.1088/0004-6256/146/4/103 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 218AL UT WOS:000324404800032 ER PT J AU Yoon, J Sillett, TS Morrison, SA Ghalambor, CK AF Yoon, Jongmin Sillett, T. Scott Morrison, Scott A. Ghalambor, Cameron K. TI Male's return rate, rather than territory fidelity and breeding dispersal, explains geographic variation in song sharing in two populations of an oscine passerine (Oreothlypis celata) SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Breeding dispersal; Geographic variation; Migratory behavior; Return rate; Song sharing; Territory fidelity ID INDIGO BUNTINGS; BIRD SONG; SPARROWS; CONSEQUENCES; SONGBIRDS; EVOLUTION; MIMICRY AB Males of some oscine passerines learn and share songs of neighboring males. This process can lead to the formation of song pattern neighborhoods or microhabitat song dialects. The degree to which song sharing occurs between populations and the spatial scale over which neighboring males share songs, however, can vary widely, and interpopulation comparisons have suggested that song sharing is more common in residents than in migrants. Here, we examine two populations of the orange-crowned warbler (Oreothlypis celata) to quantify patterns of song sharing at the northern (long-distance migrant) and southern (short-distance migrant) edges of the breeding distribution and to test if return rate, territory fidelity, and breeding dispersal explain the patterns found in the two populations. The southern population (O. celata sordida breeding on Santa Catalina Island, California; 33A degrees N) had a higher annual return rate to their territories and exhibited higher song sharing in neighborhoods than their counterparts (O. celata celata breeding in Fairbanks, Alaska; 64A degrees N). Year-to-year patterns of territory fidelity and breeding dispersal distances were similar between populations. Our results suggest that if migratory distance generally covaries with the proportion of returning males, this could explain different levels of song sharing between the short- and long-distance migrants. C1 [Yoon, Jongmin; Ghalambor, Cameron K.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Sillett, T. Scott] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Morrison, Scott A.] Nature Conservancy, San Francisco, CA 94105 USA. [Yoon, Jongmin] Korea Natl Univ Educ, Korea Inst Oriental White Stork Reintroduct Res, Cheongwon 363791, South Korea. RP Ghalambor, CK (reprint author), Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. EM cameron.ghalambor@colostate.edu FU Nature Conservancy; Smithsonian Institution; Colorado State University FX This study was funded by The Nature Conservancy, the Smithsonian Institution, and Colorado State University. The Catalina Island Conservancy (CIC) generously provided affordable housing and vehicles. Frank Starkey and Carlos de la Rosa of the CIC provided logistical support, and many people helped with the fieldwork, especially Luke Caldwell, Brent Horton, Kathryn Langin, Hannah Montag, and Helen Sofaer. NR 35 TC 3 Z9 3 U1 5 U2 55 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD OCT PY 2013 VL 67 IS 10 BP 1691 EP 1697 DI 10.1007/s00265-013-1579-5 PG 7 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 214BF UT WOS:000324104500014 ER PT J AU Alda, F Gonzalez, MA Olea, PP Ena, V Godinho, R Drovetski, SV AF Alda, Fernando Gonzalez, Manuel A. Olea, Pedro P. Ena, Vicente Godinho, Raquel Drovetski, Sergei V. TI Genetic diversity, structure and conservation of the endangered Cantabrian Capercaillie in a unique peripheral habitat SO EUROPEAN JOURNAL OF WILDLIFE RESEARCH LA English DT Article DE Gene flow; Historical distribution; Isolation; Quercus pyrenaica forests; Range contraction; Spain; Tetrao urogallus cantabricus ID TETRAO-UROGALLUS-CANTABRICUS; MULTILOCUS GENOTYPE DATA; POPULATION-STRUCTURE; CLIMATE-CHANGE; INDIVIDUAL IDENTIFICATION; RANGE; FRAGMENTATION; INFERENCE; DECLINE; FOREST AB Populations at the rear edge of the species' range are often at a high risk of extinction due to their isolation, fragmentation and small population sizes. However, these populations also play a relevant role in the conservation of biodiversity since they may represent a valuable genetic resource. The endangered Cantabrian Capercaillie (Tetrao urogallus cantabricus) inhabits deciduous forests of the Cantabrian Mountains of Spain, at the southwestern limit of the species' range. Recently, nine Cantabrian Capercaillie leks were discovered in Pyrenean oak forests of the southern slope of the Cantabrian range, where the subspecies historically occurred. To elucidate if the origin of this peripheral population nucleus is the result of a historical range contraction or a recent re-colonization from the core population, we sampled moulted feathers from all the known leks in the southern peripheral forests and from the adjacent main core population, based on nine microsatellite loci genotypes. No significant genetic differentiation was detected between main core and peripheral forests suggesting that gene flow is not interrupted between these nuclei. Contrary to expected, peripheral forests did not represent sink populations, since gene flow mainly occurred from southern peripheral to northern main core forests. Therefore, the origin of these birds inhabiting the peripheral nucleus seems not to be a recent colonization but relicts from the former distribution range that have remained unnoticed in a drier and warmer environment than described so far for the species. Cantabrian Capercaillie faces a high risk of extinction in the southernmost forests of its distribution, not only because of its peripheral location but also due to its small population size, low genetic diversity and low incoming gene flow. According to our results, this peripheral nucleus could represent an expanding edge for the population if Pyrenean oak forests continue to spread out southwards and consequently stress the need for conservation programs to preserve habitat availability and forest connectivity. C1 [Alda, Fernando; Olea, Pedro P.] CSIC UCLM JCCM, Inst Invest Recursos Cineget IREC, Ciudad Real 13005, Spain. [Alda, Fernando] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. [Gonzalez, Manuel A.; Ena, Vicente] Univ Leon, Dpto Biodiversidad & Gest Ambiental, E-24071 Leon, Spain. [Godinho, Raquel; Drovetski, Sergei V.] Ctr Invest Biodiversidade & Recursos Genet, CIBIO, P-4485661 Crasto, Vairao, Portugal. [Drovetski, Sergei V.] Tromso Univ Museum, NO-9037 Tromso, Norway. RP Gonzalez, MA (reprint author), Univ Leon, Dpto Biodiversidad & Gest Ambiental, Campus Vegazana S-N, E-24071 Leon, Spain. EM magong@unileon.es RI Godinho, Raquel/L-6804-2013; Drovetski, Sergei/A-6002-2011 OI Godinho, Raquel/0000-0002-4260-4799; Drovetski, Sergei/0000-0002-1832-5597 FU CIBIO (Centro de Investigacao em Biodiversidade e Recursos Geneticos, Portugal); Universidad de Leon [ULE AG-185]; FCT (Portugal) [SFRH/BPD/36021/2007]; Universidad de Leon (Spain) FX We thank Luis Robles for his help with the fieldwork in the Mediterranean peripheral forest. We are grateful to CTM technicians for their help in the lab, and to Jesus T. Garcia and Maria Calero-Riestra at IREC for helpful discussions and assistance with the statistical analyses. We also thank the anonymous referees that helped to improve the manuscript. Finally, we are grateful to Mark Herse for reviewing the English text. The funding for the lab work was provided by CIBIO (Centro de Investigacao em Biodiversidade e Recursos Geneticos, Portugal). Fieldwork was funded by Universidad de Leon (project ULE AG-185). Raquel Godinho was supported by a postdoctoral fellowship (SFRH/BPD/36021/2007) from FCT (Portugal) and Manuel A. Gonzalez by a predoctoral scholarship from the Universidad de Leon (Spain). NR 64 TC 5 Z9 5 U1 1 U2 65 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1612-4642 EI 1439-0574 J9 EUR J WILDLIFE RES JI Eur. J. Wildl. Res. PD OCT PY 2013 VL 59 IS 5 BP 719 EP 728 DI 10.1007/s10344-013-0727-6 PG 10 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA 216IV UT WOS:000324276700012 ER PT J AU Nunes, FMF Ihle, KE Mutti, NS Simoes, ZLP Amdam, GV AF Nunes, Francis M. F. Ihle, Kate E. Mutti, Navdeep S. Simoes, Zila L. P. Amdam, Gro V. TI The gene vitellogenin affects microRNA regulation in honey bee (Apis mellifera) fat body and brain SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE microRNA; microarrays; RNAi; social behavior ID COLONY-LEVEL SELECTION; DIVISION-OF-LABOR; JUVENILE-HORMONE; EXPRESSION PATTERNS; FORAGING BEHAVIOR; UP-REGULATION; DROSOPHILA; WORKERS; DIFFERENTIATION; FORAGERS AB In honey bees, vitellogenin (Vg) is hypothesized to be a major factor affecting hormone signaling, food-related behavior, immunity, stress resistance and lifespan. MicroRNAs, which play important roles in post-transcriptional gene regulation, likewise affect many biological processes. The actions of microRNAs and Vg are known to intersect in the context of reproduction; however, the role of these associations on social behavior is unknown. The phenotypic effects of Vg knockdown are best established and studied in the forager stage of workers. Thus, we exploited the well-established RNA interference (RNAi) protocol for Vg knockdown to investigate its downstream effects on microRNA population in honey bee foragers' brain and fat body tissue. To identify microRNAs that are differentially expressed between tissues in control and knockdown foragers, we used mu Paraflo microfluidic oligonucleotide microRNA microarrays. Our results showed that 76 and 74 microRNAs were expressed in the brain of control and knockdown foragers whereas 66 and 69 microRNAs were expressed in the fat body of control and knockdown foragers, respectively. Target prediction identified potential seed matches for a differentially expressed subset of microRNAs affected by Vg knockdown. These candidate genes are involved in a broad range of biological processes including insulin signaling, juvenile hormone (JH) and ecdysteroid signaling previously shown to affect foraging behavior. Thus, here we demonstrate a causal link between the Vg knockdown forager phenotype and variation in the abundance of microRNAs in different tissues, with possible consequences for the regulation of foraging behavior. C1 [Nunes, Francis M. F.] Univ Sao Paulo, Fac Med Ribeirao Preto, Dept Genet, BR-14049 Ribeirao Preto, SP, Brazil. [Nunes, Francis M. F.; Simoes, Zila L. P.] Univ Sao Paulo, Fac Filosofia Ciencias & Letras Ribeirao Preto, Dept Biol, Ribeirao Preto, SP, Brazil. [Ihle, Kate E.; Mutti, Navdeep S.; Amdam, Gro V.] Arizona State Univ, Sch Life Sci, Tempe, AZ USA. [Ihle, Kate E.] Smithsonian Trop Res Inst, Panama City, Panama. [Amdam, Gro V.] Norwegian Univ Life Sci, Dept Chem Biotechnol & Food Sci, As, Norway. RP Nunes, FMF (reprint author), Univ Fed Sao Carlos, Dept Genet & Evolucao, BR-13560 Sao Carlos, SP, Brazil. EM francis.nunes@ufscar.br; kateihle@gmail.com RI Simoes, Zila/H-7314-2014; Nunes, Francis/F-5871-2010 OI Nunes, Francis/0000-0002-7769-3058 FU Research Council of Norway [180504, 191699, 213976]; Pew Charitable Trust; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq), Brazil [481000/2009-7]; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP), Brazil [11/03171-5]; CNPq [161917/2011-9]; FAPESP [07/07594-2]; Arizona State University; Smithsonian Tropical Research Institute FX Funding was provided by the Research Council of Norway [grant nos 180504, 191699, 213976 to G. V. A.], The Pew Charitable Trust (to G. V. A.), Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq), Brazil [grant no. 481000/2009-7 to F.M.F.N.], and Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP), Brazil [grant no. 11/03171-5 to Z.L.P.S.]. F.M.F.N. was supported by a post-doctoral fellowship from CNPq [161917/2011-9] and FAPESP [07/07594-2]. K. E. I. was supported by a post-doctoral fellowship from Arizona State University and the Smithsonian Tropical Research Institute. NR 85 TC 15 Z9 17 U1 2 U2 69 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD OCT PY 2013 VL 216 IS 19 BP 3724 EP 3732 DI 10.1242/jeb.089243 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 215TN UT WOS:000324233500026 PM 23788711 ER PT J AU Eff-Darwich, A Korzennik, SG AF Eff-Darwich, A. Korzennik, S. G. TI The Dynamics of the Solar Radiative Zone SO SOLAR PHYSICS LA English DT Article DE Helioseismology; Inverse modeling; Observations; Interior; Radiative zone ID MAGNETIC-FIELD; ROTATION RATE; SUN; INVERSION; OSCILLATIONS; SPLITTINGS; INTERIOR; IMAGER; MODES; GONG AB The dynamics of the solar radiative interior are still poorly constrained by comparison to the convective zone. This disparity is even more marked when we attempt to derive meaningful temporal variations. Many data sets contain a small number of modes that are sensitive to the inner layers of the Sun, but we found that the estimates of their uncertainties are often inaccurate. As a result, these data sets allow us to obtain, at best, a low-resolution estimate of the solar-core rotation rate down to approximately 0.2R (aS (TM)). We present inferences based on mode determination resulting from an alternate peak-fitting methodology aimed at increasing the amount of observed modes that are sensitive to the radiative zone, while special care was taken in the determination of their uncertainties. This methodology has been applied to MDI and GONG data, for the whole Solar Cycle 23, and to the newly available HMI data. The numerical inversions of all these data sets result in the best inferences to date of the rotation in the radiative region. These results and the method used to obtain them are discussed. The resulting profiles are shown and analyzed, and the significance of the detected changes is discussed. C1 [Eff-Darwich, A.] Univ La Laguna, Dept Edafol & Geol, E-38206 Tenerife, Spain. [Eff-Darwich, A.] Inst Astrofis Canarias, Tenerife 38205, Spain. [Korzennik, S. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Korzennik, SG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM adarwich@ull.es; skorzennik@cfa.harvard.edu NR 27 TC 10 Z9 10 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD OCT PY 2013 VL 287 IS 1-2 BP 43 EP 56 DI 10.1007/s11207-012-0048-z PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 214FB UT WOS:000324115600003 ER PT J AU Estrada-Medina, H Santiago, LS Graham, RC Allen, MF Jimenez-Osornio, JJ AF Estrada-Medina, Hector Santiago, Louis S. Graham, Robert C. Allen, Michael F. Jose Jimenez-Osornio, Juan TI Source water, phenology and growth of two tropical dry forest tree species growing on shallow karst soils SO TREES-STRUCTURE AND FUNCTION LA English DT Article DE Ground water; Yucatan; Rooting depth; Seasonally dry tropical forest; Stable isotopes ID OXYGEN-ISOTOPE RATIOS; NORTHERN YUCATAN; DESICCATION-TOLERANCE; STOMATAL CONDUCTANCE; DECIDUOUS FOREST; STABLE OXYGEN; CANOPY TREES; STEM WATER; LONG-TERM; MEXICO AB Seasonally dry tropical forests are dominated by deciduous and evergreen tree species with a wide range of leaf phenology. We hypothesized that Piscidia piscipula is able to extend leaf senescence until later in the dry season due to deeper and more reliable water sources than Gymnopodium floribundum, which loses leaves earlier in the dry season. Physiological performance was assessed as timing of leaf production and loss, growth, leaf water potential, depth of water uptake determined by stable isotopes, and leaf stable isotopic composition of carbon (delta C-13) and oxygen (delta O-18). P. piscipula took water primarily from shallow sources, whereas G. floribundum took water from shallow and deep sources. The greatest variation in water sources occurred during the onset of the dry season, when G. floribundum was shedding old leaves and growing new leaves, but P. piscipula maintained its leaves from the previous wet season. P. piscipula showed greater relative growth rate, greater leaf expansion rates, and more negative predawn and midday water potentials than G. floribundum. P. piscipula also exhibited greater leaf organic delta C-13 and lower delta O-18 values, indicating that the decrease in photosynthetic carbon isotope discrimination was associated with greater stomatal conductance and greater photosynthesis. Our results indicate that the contrasting early and late dry season leaf loss phenology of these two species is not simply determined by rooting depth, but rather a more complicated suite of characteristics based on opportunistic use of dynamic water sources, maximizing carbon gain, and maintenance of water potential during the dry season. C1 [Estrada-Medina, Hector; Jose Jimenez-Osornio, Juan] Univ Autonoma Yucatan, Dept Manejo & Conservac Recursos Nat Trop PROTROP, Merida 97315, Yucatan, Mexico. [Estrada-Medina, Hector; Graham, Robert C.] Univ Calif Riverside, Dept Environm Sci, Soil & Water Sci Program, Riverside, CA 92521 USA. [Santiago, Louis S.] Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA. [Santiago, Louis S.] Smithsonian Trop Res Inst, Balboa, Panama. [Allen, Michael F.] Univ Calif Riverside, Ctr Conservat Biol, Riverside, CA 92521 USA. RP Estrada-Medina, H (reprint author), Univ Autonoma Yucatan, Dept Manejo & Conservac Recursos Nat Trop PROTROP, Campus Ciencias Biol & Agr,Km 15-5 Carretera Meri, Merida 97315, Yucatan, Mexico. EM hector.estrada@uady.mx RI Estrada Medina, Hector/A-7665-2014; Santiago, Louis/E-3185-2016 OI Santiago, Louis/0000-0001-5994-6122 FU CONACyT-UCMEXUS; UCMEXUS; National Science Foundation [DEB 0615427, DEB 0770 6813, EF 0410408, CRR 0120778]; UCR Center for Conservation Biology FX We thank to CONACyT-UCMEXUS for the scholarship granted to the first author for doctoral studies at the University of California Riverside. This work was supported by UCMEXUS through the projects: "Importance of limestone bedrock and subsurface pockets of soil as potential sources of water for dry deciduous tree species in northern Yucatan and "Water contribution by limestone bedrock and subsurface SP and its effect on the water use efficiency of two tree species in Yucatan, Mexico''; grants from the National Science Foundation (DEB 0615427, DEB 0770 6813, EF 0410408, and CRR 0120778), and the UCR Center for Conservation Biology. We would like to thank the owners of the quarry, especially Hector Buenfil Cervera; the workers of the quarry, especially Roger Armando Fernandez Paredes, and Augusto Cervera Buenfil for helping with the work logistics; Alfonso Castillo, Maria Jose Romero, Raul Hernandez and Ariel Esparza for helping with the field and laboratory work. NR 58 TC 5 Z9 5 U1 3 U2 74 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0931-1890 J9 TREES-STRUCT FUNCT JI Trees-Struct. Funct. PD OCT PY 2013 VL 27 IS 5 BP 1297 EP 1307 DI 10.1007/s00468-013-0878-9 PG 11 WC Forestry SC Forestry GA 216YB UT WOS:000324321600010 ER PT J AU Yao, XH Li, CH Dick, CW AF Yao, Xiaohong Li, Chenhong Dick, Christopher W. TI EXON-PRIMED INTRON-CROSSING (EPIC) MARKERS FOR EVOLUTIONARY STUDIES OF FICUS AND OTHER TAXA IN THE FIG FAMILY (MORACEAE) SO APPLICATIONS IN PLANT SCIENCES LA English DT Article DE exons; Ficus; Moraceae; nuclear DNA markers; phylogeny; transcriptome ID WASP; SEQUENCES AB Premise of the study: The genus Ficus (fig trees) comprises ca. 750 species of trees, vines, and stranglers found in tropical forests throughout the world. Fig trees are keystone species in many tropical forests, and their relationship with host-specific wasp pollinators has received much attention, although many questions remain unresolved regarding the levels of host specificity, cospeciation, and the role of hybridization in fig and wasp speciation. We developed exon-primed intron-crossing (EPIC) markers to obtain phylogenetic resolution needed to address these questions. Methods and Results: Expressed sequence tags (ESTs) from F. elastica were compared to Arabidopsis and Populus genomes to locate introns and to design primers in flanking exons. Primer pairs for 80 EPIC markers were tested in samples from divergent clades within Ficus and the outgroup Poulsenia (Moraceae). Conclusions: Thirty-one EPIC markers were successfully sequenced across Ficus, and 29 of the markers also amplified in Poulsenia, indicating broad transferability within Moraceae. All of the EPIC markers were polymorphic and showed levels of polymorphism similar to that of the widely used internal transcribed spacer (ITS). C1 [Yao, Xiaohong] Chinese Acad Sci, Key Lab Plant Germplasm Enhancement & Specialty A, Wuhan Bot Garden, Wuhan 430074, Hubei, Peoples R China. [Yao, Xiaohong; Dick, Christopher W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Li, Chenhong] Shanghai Ocean Univ, Key Lab Explorat & Utilizat Aquat Genet Resources, Minist Educ, Shanghai, Peoples R China. [Dick, Christopher W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Dick, CW (reprint author), Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. EM cwdick@umich.edu RI Dick, Christopher/A-8744-2008 FU National Science Foundation [DEB 0640379] FX Financial support was received from the National Science Foundation (DEB 0640379 to C.W.D.). The authors thank Allen Herre, Adalberto Gomez, and Katrin Heer for help in locating Panamanian Ficus, and the Smithsonian Tropical Research Institute and Autoridad Nacional del Ambiente (ANAM) for facilitating research and providing research permits for work in Panama. NR 12 TC 2 Z9 2 U1 2 U2 7 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 2168-0450 J9 APPL PLANT SCI JI Appl. Plant Sci. PD OCT PY 2013 VL 1 IS 10 AR 1300037 DI 10.3732/apps.1300037 PG 4 WC Plant Sciences SC Plant Sciences GA AQ1RI UT WOS:000342558300007 ER PT J AU Strang, CB AF Strang, Cameron B. TI Indian Storytelling, Scientific Knowledge, and Power in the Florida Borderlands SO WILLIAM AND MARY QUARTERLY LA English DT Article C1 Smithsonian Inst, Washington, DC 20560 USA. RP Strang, CB (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU INST EARLY AMER HIST CULT PI WILLIAMSBURG PA BOX 220, WILLIAMSBURG, VA 23187 USA SN 0043-5597 J9 WILLIAM MARY QUART JI William Mary Q. PD OCT PY 2013 VL 70 IS 4 BP 671 EP 700 DI 10.5309/willmaryquar.70.4.0671 PG 30 WC History SC History GA AR7DR UT WOS:000343740500002 ER PT J AU Tavzes, C Palcic, J Fackler, K Pohleven, F Koestler, RJ AF Tavzes, Crtomir Palcic, Jernej Fackler, Karin Pohleven, Franc Koestler, Robert J. TI Biomimetic system for removal of fungal melanin staining on paper SO INTERNATIONAL BIODETERIORATION & BIODEGRADATION LA English DT Article DE Biomimetic system; Colorimetry; Copper-pyridine complex; FTIR; Melanin degradation; UV-VIS ID HYDROGEN-PEROXIDE; BIOSYNTHESIS; LACCASE; DEGRADATION; OXIDATION; PIGMENTS AB Fungal melanin staining is a problem on many cultural objects, ranging from the French Palaeolithic cave at Lascaux to books and papers in museum collections. Melanin, because it is insoluble and resistant to bleaching, may leave behind undesirable stains long after the fungal infestation has been controlled. Research into removal of melanin stains from paper and other sensitive substrates using industrial biomimetic oxidizing systems has shown considerable success. We studied relative concentration of the bleaching reagents and the reaction kinetics both in liquid suspensions of melanin and on melanized paper samples. Liquid suspension samples were tested for changes in their chemical composition (appearance and relative representation of functional groups and chemical bonds) with FTIR spectrometry. Changes in color of melanized paper samples were investigated with a CIE L*a*b system, where the effectiveness of the treatment (bleaching) was determined as a change in lightness (Delta L). Melanin was oxidized in the liquid suspensions, and the intensity of modification depended on the procedure employed. Bleaching of melanin with the biomimetic copper-pyridine complex proved to be far superior to the effect of white-rot fungal oxidizing enzymes, previously reported on by this group. (c) 2012 Elsevier Ltd. All rights reserved. C1 [Tavzes, Crtomir] Inst Protect Cultural Heritage Slovenia, Conservat Ctr, Res Inst, Ljubljana, Slovenia. [Palcic, Jernej; Pohleven, Franc] Univ Ljubljana, Biotech Fac, Dept Wood Sci & Technol, Ljubljana 61000, Slovenia. [Fackler, Karin] Vienna Univ Technol, Inst Chem Engn, Vienna, Austria. [Koestler, Robert J.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD USA. [Tavzes, Crtomir] Inst Wood Sci & Technol & Sustainable Dev, SI-1000 Ljubljana, Slovenia. RP Tavzes, C (reprint author), Inst Wood Sci & Technol & Sustainable Dev, Celovska Cesta 268, SI-1000 Ljubljana, Slovenia. EM crtomir.tavzes@iltra.si NR 33 TC 1 Z9 1 U1 3 U2 24 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0964-8305 J9 INT BIODETER BIODEGR JI Int. Biodeterior. Biodegrad. PD OCT PY 2013 VL 84 SI SI BP 307 EP 313 DI 10.1016/j.ibiod.2012.07.022 PG 7 WC Biotechnology & Applied Microbiology; Environmental Sciences SC Biotechnology & Applied Microbiology; Environmental Sciences & Ecology GA 198SG UT WOS:000322942000041 ER PT J AU Baeza, JA AF Baeza, J. Antonio TI Molecular phylogeny of broken-back shrimps (genus Lysmata and allies): A test of the 'Tomlinson-Ghiselin' hypothesis explaining the evolution of hermaphroditism SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Sociobiology; Symbiosis; Lysmatidae; Barbouriidae; Merguiidae; Sex allocation ID PROTANDRIC SIMULTANEOUS HERMAPHRODITISM; ANCESTRAL CHARACTER STATES; JANICEA-ANTIGUENSIS CHACE; SEX ALLOCATION; MARINE SHRIMP; WURDEMANNI CARIDEA; SOCIAL MONOGAMY; EXHIPPOLYSMATA-OPLOPHOROIDES; REPRODUCTIVE SUCCESS; DECAPOD CRUSTACEANS AB The 'Tomlinson-Ghiselin' hypothesis (TGh) predicts that outcrossing simultaneous hermaphroditism (SH) is advantageous when population density is low because the probability of finding sexual partners is negligible. In shrimps from the family Lysmatidae, Bauer's historical contingency hypothesis (HCh) suggests that SH evolved in an ancestral tropical species that adopted a symbiotic lifestyle with, e.g., sea anemones and became a specialized fish-cleaner. Restricted mobility of shrimps due to their association with a host, and hence, reduced probability of encountering mating partners, would have favored SH. The HCh is a special case of the TGh. Herein, I examined within a phylogenetic framework whether the TGh/HCh explains the origin of SH in shrimps. A phylogeny of caridean broken-back shrimps in the families Lysmatidae, Barbouriidae, Merguiidae was first developed using nuclear and mitochondrial makers. Complete evidence phylogenetic analyses using maximum likelihood (ML) and Bayesian inference (BI) demonstrated that Lysmatidae + Barbouriidae are monophyletic. In turn, Merguiidae is sister to the Lysmatidae + Barbouriidae. ML and BI ancestral character-state reconstruction in the resulting phylogenetic trees indicated that the ancestral Lysmatidae was either gregarious or lived in small groups and was not symbiotic. Four different evolutionary transitions from a free-living to a symbiotic lifestyle occurred in shrimps. Therefore, the evolution of SH in shrimps cannot be explained by the TGh/HCh; reduced probability of encountering mating partners in an ancestral species due to its association with a sessile host did not favor SH in the Lysmatidae. It is proposed that two conditions acting together in the past; low male mating opportunities and brooding constraints, might have favored SH in the ancestral Lysmatidae + Barbouridae. Additional studies on the life history and phylogenetics of broken-back shrimps are needed to understand the evolution of SH in the ecologically diverse Caridea. (C) 2013 Elsevier Inc. All rights reserved. C1 [Baeza, J. Antonio] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Baeza, J. Antonio] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Coquimbo, Chile. RP Baeza, JA (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM baeza.antonio@gmail.com OI Baeza, Juan Antonio/0000-0002-2573-6773 FU SMSFP; Smithsonian Tropical Research Institute (STRI); National Geographic research grant FX JAB was supported by a postdoctoral fellowship from the SMSFP and Smithsonian Tropical Research Institute (STRI). This study was partially funded by a National Geographic research grant to JAB. Some specimens used in this study were provided by my colleagues: Adilson Fransozo, Maria Lucia Negreiros-Fransozo and Adriane Braga (NEBECC, Universidade Estadual Paulista, Sao Paulo, Brazil), Ka Hou Chu (The Chinese University of Hong Kong, Hong Kong, China), Scott R. Santos (Auburn University, Alabama), Xinzheng Li (Institute of Oceanology, Chinese Academy of Sciences, China), Luis M. Mejia (Universidad de Quintana Roo, Cozumel, Mexico), Arthur Anker and Gustav Paulay (FLMNH, USA), Sammy De Grave (OUMNH, United Kingdom), Ricardo J.G. Calado (CESAM, University of Aveiro, Portugal), Luis Ignacio Vilchis and William A. Newman (SIO, University of California at San Diego, USA), Ivan Hinojosa and Martin Thiel (UCN, Chile), and Tomas A. Luppi and Eduardo Spivak (IIMyC, Universidad Nacional de Mar del Plata, Argentina). Jeff Hunt and Lee Weigt (Laboratory of Analytical Biology, USNM) provided logistical support for the molecular analysis. Many thanks to Junda Lin (Florida Institute of Technology), for critically reviewing the content of earlier versions of this manuscript. Many thanks to Mike Dickson for improving the language of the manuscript. This is Smithsonian Marine Station at Fort Pierce contribution number 913. NR 117 TC 7 Z9 7 U1 2 U2 58 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 OCT PY 2013 VL 69 IS 1 BP 46 EP 62 DI 10.1016/j.ympev.2013.05.013 PG 17 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 196UM UT WOS:000322802900005 PM 23727055 ER PT J AU Noonan, BP Pramuk, JB Bezy, RL Sinclair, EA de Queiroz, K Sites, JW AF Noonan, Brice P. Pramuk, Jennifer B. Bezy, Robert L. Sinclair, Elizabeth A. de Queiroz, Kevin Sites, Jack W., Jr. TI Phylogenetic relationships within the lizard clade Xantusiidae: Using trees and divergence times to address evolutionary questions at multiple levels SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Xantusiidae; Phylogeny; Squamata; New World; Biogeography ID GENUS LEPIDOPHYMA SQUAMATA; NIGHT-LIZARD; PHYLOGEOGRAPHIC HISTORY; MOLECULAR PHYLOGENETICS; FOSSIL CALIBRATIONS; SUBSTITUTION RATES; FAMILY XANTUSIIDAE; MITOCHONDRIAL DATA; SPECIES COMPLEX; CENTRAL MEXICO AB Xantusiidae (night lizards) is a clade of small-bodied, cryptic lizards endemic to the New World. The clade is characterized by several features that would benefit from interpretation in a phylogenetic context, including: (1) monophyletic status of extant taxa Cricosaura, Lepidophyma, and Xantusia; (2) a species endemic to Cuba (Cricosaura typica) of disputed age; (3) origins of the parthenogenetic species of Lepidophyma; (4) pronounced micro-habitat differences accompanied by distinct morphologies in both Xantusia and Lepidophyma; and (5) placement of Xantusia riversiana, the only vertebrate species endemic to the California Channel Islands, which is highly divergent from its mainland relatives. This study incorporates extensive new character data from multiple gene regions to investigate the phylogeny of Xantusiidae using the most comprehensive taxonomic sampling available to date. Parsimony and partitioned Bayesian analyses of more than 7 kb of mitochondrial and nuclear sequence data from 11 loci all confirm that Xantusiidae is monophyletic, and comprises three well-supported clades: Cricosaura, Xantusia, and Lepidophyma. The Cuban endemic Cricosaura typica is well supported as the sister to all other xantusiids. Estimates of divergence time indicate that Cricosaura diverged from the (Lepidophyma + Xantusia) clade similar to 81 million years ago (Ma), a time frame consistent with the separation of the Antilles from North America. Our results also confirm and extend an earlier study suggesting that parthenogenesis has arisen at least twice within Lepidophyma without hybridization, that rock-crevice ecomorphs evolved numerous times (>9) within Xantusia and Lepidophyma, and that the large-bodied Channel Island endemic X. riversiana is a distinct, early lineage that may form the sister group to the small-bodied congeners of the mainland. (C) 2013 Elsevier Inc. All rights reserved. C1 [Noonan, Brice P.] Univ Mississippi, Dept Biol, University, MS 38677 USA. [Noonan, Brice P.; Pramuk, Jennifer B.; Sites, Jack W., Jr.] Brigham Young Univ, Dept Biol, Provo, UT 84602 USA. [Noonan, Brice P.; Pramuk, Jennifer B.; Sites, Jack W., Jr.] Brigham Young Univ, ML Bean Life Sci Museum, Provo, UT 84602 USA. [Pramuk, Jennifer B.] Woodland Pk Zoo, Dept Herpetol, Seattle, WA 98103 USA. [Bezy, Robert L.] Nat Hist Museum Los Angeles Cty, Los Angeles, CA 90007 USA. [Sinclair, Elizabeth A.] Univ Western Australia, Sch Plant Biol, Crawley, WA 6009, Australia. [de Queiroz, Kevin] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Noonan, BP (reprint author), Univ Mississippi, Dept Biol, University, MS 38677 USA. EM bnoonan@olemiss.edu RI Sinclair, Elizabeth/B-1179-2011 OI Sinclair, Elizabeth/0000-0002-5789-8945 FU NSF [DEB 0132227, EF 0334966, DEB 9318642, DEB 97050277, 0102303, 0613802] FX Thanks to the many individuals who have participated in fieldwork securing tissues, including: J. Alexander, K. Bezy, K. Bolles, J. Caldwell, the late J. Camarillo-R., J. Campbell, A. Chamizo-Lara, L. Canseco Marquez, J. Dixon, P. Elias, G. Fellers, R. Glor, M. Leal, D. Leavitt, C. Lieb, J. Losos, B. Mautz, J. McCranie, S. Poe, L. Rodriguez Schettino, L. Vitt, R. Vogt, B. Shaffer, J. Seems, E. Smith, W. Van Devender, and L. Wilson. Tissues were generously loaned by: the Museo de Zoologla of the Universidad Nacional Autonoma de Mexico (MZFC), University of California at Berkeley Museum of Vertebrate Zoology (MVZ), Collection of Vertebrates of the University of Texas at Arlington (UTA-R), and the U. S. National Museum of Natural History (USNM); and from the following individuals: O. Flores-Villela (new Lepidophyma from Mexico), and L.D. Wilson (Lepidophyma from Honduras). We are particularly appreciatiave of the insight on fossil species and their relationships provided by J. Gautier. Ted Townsend kindly provided divergence times for our calibration corrections. M. Whiting and M. Mirando kindly shared their unpublished cyt-b primers. Funding for this project was provided by NSF grants DEB 0132227 to J. W. Sites, Jr., R. L., Bezy, J. A. Gauthier, J. A. Maisano, and D. A. McClellan, and EF 0334966, to J.W. Sites, Jr., the Dept. of Biology and Bean Life Science Museum at Brigham Young University; Cricosaura tissue collection funded by an NSF Grant DEB 9318642 to J.B. Losos, A. Larson, and K. de Queiroz, and DEB 97050277, 0102303, and 0613802, to J.A. Campbell (for several taxa from southern Mexico and Guatemala). Figs. 1 and 6 were prepared by Kit Bezy. NR 109 TC 4 Z9 6 U1 2 U2 77 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 OCT PY 2013 VL 69 IS 1 BP 109 EP 122 DI 10.1016/j.ympev.2013.05.017 PG 14 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 196UM UT WOS:000322802900010 PM 23742886 ER PT J AU Liu, XH Wu, PF Songer, M Cai, Q He, XB Zhu, Y Shao, XM AF Liu, Xuehua Wu, Pengfeng Songer, Melissa Cai, Qiong He, Xiangbo Zhu, Yun Shao, Xiaoming TI Monitoring wildlife abundance and diversity with infra-red camera traps in Guanyinshan Nature Reserve of Shaanxi Province, China SO ECOLOGICAL INDICATORS LA English DT Article DE Relative abundance index (RAI); Activity pattern; Noctumality; Abundance estimation; Camera trapping ID PHOTOGRAPHIC RATES; ESTIMATE DENSITIES; CRYPTIC MAMMALS; PENINSULAR MALAYSIA; TIGERS; POPULATION; FOREST AB Ecological indicators or indices have been widely used to simplify and measure complex ecosystems. It is critical to identify suitable indicators or indices to improve monitoring and understanding of complex natural systems. Camera trapping is an objective technique that can provide a large amount of information on wildlife. The purpose of our study is to explore the effective ecological indices for wildlife diversity analysis and monitoring in Guanyinshan Nature Reserve of Shaanxi Province, China. Since July 2009, a total of 18 cameras were installed in the reserve from August 2009 to July 2011, collecting 2115 photo captures during these 24 months. We developed five abundance indices, including relative abundance index (RAI), monthly relative abundance index (MRAI), time-period relative abundance index (TRAI), night-time relative abundance index (NRAI) and species abundance index (N) to integrate the information derived from captures. Results are: (1) 27 species were detected and 6 species had high RAI values of over 79.3%, including takin (Budorcas taxicolor), common goral (Naemorhedus goral), tufted deer (Elaphodus cephalophus), golden pheasant (Chtysolophus pictus), wild boar (Sus scrofa), and mainland serow (Capricornis sumatraensis). (2) MRAI shows a consistent monthly activity pattern of all animals being active in June and July and inactive in February. (3) TRAIs of the most abundant six species show that takin, tufted deer and common goral have the similar daily activity pattern with one peak at dawn and one peak at dusk. The daily activity patterns of golden pheasant and wild boar show that they are most active during the day time, with wild boar being particularly active at noon. NRAIs of mainland serow show the highest nocturnality and of golden pheasant the lowest nocturnality. (4) We estimated abundance of takin, tufted deer and wild boar by using our developed index. The abundance for the three species shows an increasing trend during the 2-year study period, particularly for wild boar. Our results provided an interesting comparison of species diversity and their activity patterns. As trapping continues we will have a consistent source of monitoring data to evaluate changes in species abundance and activities. Therefore, the conclusion is that the methods we used and the indices we developed are capable to estimate species activity patterns and abundance dynamics which are useful for future wildlife management in Guanyinshan Nature Reserve and elsewhere. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Liu, Xuehua] State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100084, Peoples R China. [Liu, Xuehua] Tsinghua Univ, Sch Environm, Beijing 100084, Peoples R China. [Wu, Pengfeng; Shao, Xiaoming] China Agr Univ, Coll Biol Sci, Beijing 100193, Peoples R China. [Songer, Melissa] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA. [Cai, Qiong; Zhu, Yun] Shaanxi Guanyinshan Nat Reserve, Foping Cty 723400, Shaanxi, Peoples R China. [He, Xiangbo] Shaanxi Foping Natl Nat Reserve, Foping Cty 723400, Shaanxi, Peoples R China. RP Liu, XH (reprint author), State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100084, Peoples R China. EM xuehua-hjx@tsinghua.edu.cn; xiaowu0046@163.com; SongerM@si.edu; cai888qiong@126.com; fpxiangbo@163.com; gyshnr@21cn.com; shaoxm@cau.edu.cn FU State Key Joint Laboratory of Environment Simulation and Pollution Control; International Cooperation Programme of monitoring the restoration of giant panda habitat in the Qinling Mountains [WH0633]; State Forest Administration (SFA) of China; Friends of the National Zoo (FONZ), USA FX We acknowledge the financial supports from (1) special fund of State Key Joint Laboratory of Environment Simulation and Pollution Control, (2) International Cooperation Programme of monitoring the restoration of giant panda habitat in the Qinling Mountains (WH0633) sponsored by the State Forest Administration (SFA) of China, and (3) the Friends of the National Zoo (FONZ), USA. NR 23 TC 6 Z9 17 U1 8 U2 149 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1470-160X J9 ECOL INDIC JI Ecol. Indic. PD OCT PY 2013 VL 33 SI SI BP 121 EP 128 DI 10.1016/j.ecolind.2012.09.022 PG 8 WC Biodiversity Conservation; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 165OX UT WOS:000320494300013 ER PT J AU Aguilera, O Lundberg, J Birindelli, J Perez, MS Jaramillo, C Sanchez-Villagra, MR AF Aguilera, Orangel Lundberg, John Birindelli, Jose Perez, Mark Sabaj Jaramillo, Carlos Sanchez-Villagra, Marcelo R. TI Palaeontological Evidence for the Last Temporal Occurrence of the Ancient Western Amazonian River Outflow into the Caribbean SO PLOS ONE LA English DT Article ID NORTHWESTERN VENEZUELA; URUMACO FORMATION; ANDEAN TECTONICS; SOUTH-AMERICA; EARLY MIOCENE; FALCON STATE; BASIN; COLOMBIA; SILURIFORMES; NEOGENE AB Fossil catfishes from fluvio-lacustrine facies of late Miocene Urumaco, early Pliocene Castilletes and late Pliocene San Gregorio formations provide evidence of a hydrographic connection in what is today desert regions of northern Colombia and Venezuela. New discoveries and reevaluation of existing materials leads to the recognition of two new records of the pimelodid Brachyplatystoma cf. vaillantii, and of three distinct doradid taxa: Doraops sp., Rhinodoras sp., and an unidentified third form. The presence of fossil goliath long-whiskered catfishes and thorny catfishes are indicative of the persistence of a fluvial drainage system inflow into the South Caribbean during the Pliocene/Pleistocene boundary, complementary to the previous western Amazonian hydrographic system described from the Middle Miocene Villavieja Formation in central Colombia and Late Miocene Urumaco Formation in northwestern Venezuela. The Pliocene Castilletes and San Gregorio formations potentially represent the last lithostratigraphic units related with an ancient western Amazonian fish fauna and that drainage system in the Caribbean. Alternatively, it may preserve faunas from a smaller, peripheral river basin that was cut off earlier from the Amazon-Orinoco, today found in the Maracaibo basin and the Magdalena Rivers. C1 [Aguilera, Orangel] Univ Fed Fluminense, Inst Biol, Programa Posgrad Biol Marinha, Rio De Janeiro, Brazil. [Lundberg, John; Perez, Mark Sabaj] Acad Nat Sci Philadelphia, Dept Ichthyol, Philadelphia, PA 19103 USA. [Birindelli, Jose] Univ Estadual Londrina, Dept Biol Anim & Vegetal, Londrina, Parana, Brazil. [Jaramillo, Carlos] Smithsonian Trop Res Inst, Ancon, Panama, Panama. [Sanchez-Villagra, Marcelo R.] Univ Zurich, Palaeontol Inst & Museum, Zurich, Switzerland. RP Sanchez-Villagra, MR (reprint author), Univ Zurich, Palaeontol Inst & Museum, Zurich, Switzerland. EM m.sanchez@pim.uzh.ch RI Birindelli, Jose/F-4991-2015 FU Museum Paraense Emilio Goeldi (MPEG); Universidade Federal Fluminense (UFF); Conselho Nacional de Desenvolvimento Cientifico e Tecnologico, Brazil [CNPq 311783/2011-2]; Universidad Francisco de Miranda (UNEFM) in Venezuela; Smithsonian Tropical Research Institute (STRI) in Panama; U.S. National Science Foundation [DEB-1257813, DEB-0315963]; Swiss National Science Foundation Sinergia [CRSII3-136293] FX This research was supported by the Museum Paraense Emilio Goeldi (MPEG)(http://www.museu-goeldi.br/), the Universidade Federal Fluminense (UFF)(http://www.uff.br/), the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (Process CNPq 311783/2011-2 to OA) in Brazil (http://www.cnpq.br/), the Universidad Francisco de Miranda (UNEFM) in Venezuela (www.unefm.edu.ve), the Smithsonian Tropical Research Institute (STRI) in Panama (http://www.stri.si.edu), and the U.S. National Science Foundation (DEB-1257813 and DEB-0315963, All Catfish Species Inventory) (http://www.nsf.gov/). Marcelo R. Sanchez-Villagra was supported by the Swiss National Science Foundation Sinergia (CRSII3-136293)(www.snf.ch). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 73 TC 5 Z9 7 U1 0 U2 14 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 SEP 30 PY 2013 VL 8 IS 9 AR e76202 DI 10.1371/journal.pone.0076202 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 231NL UT WOS:000325423500148 PM 24098778 ER PT J AU Gurwick, NP Moore, LA Kelly, C Elias, P AF Gurwick, Noel P. Moore, Lisa A. Kelly, Charlene Elias, Patricia TI A Systematic Review of Biochar Research, with a Focus on Its Stability in situ and Its Promise as a Climate Mitigation Strategy SO PLOS ONE LA English DT Review ID SOIL CARBON SEQUESTRATION; ORGANIC-MATTER DYNAMICS; BLACK CARBON; SUSTAINABLE AGRICULTURE; ECOSYSTEM SERVICES; FOOD SECURITY; EMISSIONS; MANAGEMENT; IMPACT; PLANT AB Background: Claims about the environmental benefits of charring biomass and applying the resulting "biochar'' to soil are impressive. If true, they could influence land management worldwide. Alleged benefits include increased crop yields, soil fertility, and water-holding capacity; the most widely discussed idea is that applying biochar to soil will mitigate climate change. This claim rests on the assumption that biochar persists for hundreds or thousands of years, thus storing carbon that would otherwise decompose. We conducted a systematic review to quantify research effort directed toward ten aspects of biochar and closely evaluated the literature concerning biochar's stability. Findings: We identified 311 peer-reviewed research articles published through 2011. We found very few field studies that addressed biochar's influence on several ecosystem processes: one on soil nutrient loss, one on soil contaminants, six concerning non-CO2 greenhouse gas (GHG) fluxes (some of which fail to support claims that biochar decreases non-CO2 GHG fluxes), and 16-19 on plants and soil properties. Of 74 studies related to biochar stability, transport or fate in soil, only seven estimated biochar decomposition rates in situ, with mean residence times ranging from 8 to almost 4,000 years. Conclusions: Our review shows there are not enough data to draw conclusions about how biochar production and application affect whole-system GHG budgets. Wide-ranging estimates of a key variable, biochar stability in situ, likely result from diverse environmental conditions, feedstocks, and study designs. There are even fewer data about the extent to which biochar stimulates decomposition of soil organic matter or affects non-CO2 GHG emissions. Identifying conditions where biochar amendments yield favorable GHG budgets requires a systematic field research program. Finally, evaluating biochar's suitability as a climate mitigation strategy requires comparing its effects with alternative uses of biomass and considering GHG budgets over both long and short time scales. C1 [Gurwick, Noel P.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Moore, Lisa A.] Environm Def Fund, San Francisco, CA USA. [Kelly, Charlene] Western Carolina Univ, Cullowhee, NC 28723 USA. [Elias, Patricia] Union Concerned Scientists, Washington, DC USA. RP Gurwick, NP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM Noel.Gurwick@Gmail.Com FU The Tropical Forest and Climate Initiative at the Union of Concerned Scientists (UCS); Environmental Defense Fund (EDF); UCS FX The Tropical Forest and Climate Initiative at the Union of Concerned Scientists (UCS) briefly supported CK to perform an initial classification of some of the studies we reviewed. During the initial stages of this study, NPG was on staff at UCS, which paid his salary during that time. LAM is on staff at Environmental Defense Fund (EDF), which has covered her salary. EDF paid for NPG and LAM to attend a 5-day writing retreat that they used to make progress on this study. The material in this paper does not reflect any position of EDF. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 86 TC 41 Z9 42 U1 11 U2 270 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 SEP 30 PY 2013 VL 8 IS 9 AR e75932 DI 10.1371/journal.pone.0075932 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 231NL UT WOS:000325423500116 PM 24098746 ER PT J AU Kuznetsova, E Rajapakse, R Yelin, SF AF Kuznetsova, Elena Rajapakse, Renuka Yelin, S. F. TI Enhanced index of refraction in four-wave-mixing media SO PHYSICAL REVIEW A LA English DT Article ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; QUANTUM COHERENCE; ATOMIC VAPOR; LIGHT; INTERFERENCE; STORAGE; GAS AB Refractive index enhancement accompanied by vanishing absorption in a four-level atomic system interacting with two control and two probe fields in a regime of four-wave mixing (FWM) has been predicted and studied in the present work. We analyzed the maximal index enhancement in the four-level FWM system and gave index estimates for a real atomic gas of K-40, taking into account its multilevel structure and collisional and Doppler broadenings at large atomic densities. We also discussed how vanishing absorption with no nearby amplification can be realized in a two species system, consisting of a four-level FWM and a two-level system, where the latter provides additional absorption for one of the probe fields. We numerically estimated the index change in a system composed of K-40 and K-39 gases. C1 [Kuznetsova, Elena; Rajapakse, Renuka; Yelin, S. F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Kuznetsova, Elena; Yelin, S. F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Kuznetsova, Elena] Russian Quantum Ctr, Skolkovo 143025, Moscow Region, Russia. [Yelin, S. F.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Kuznetsova, E (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. FU Russian Quantum Center; NSF FX The authors gratefully acknowledge financial support from the Russian Quantum Center and NSF. NR 27 TC 6 Z9 6 U1 0 U2 8 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD SEP 30 PY 2013 VL 88 IS 3 AR 033850 DI 10.1103/PhysRevA.88.033850 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 228CC UT WOS:000325161700017 ER PT J AU Hanson, D Hoover, S Crites, A Ade, PAR Aird, KA Austermann, JE Beall, JA Bender, AN Benson, BA Bleem, LE Bock, JJ Carlstrom, JE Chang, CL Chiang, HC Cho, HM Conley, A Crawford, TM de Haan, T Dobbs, MA Everett, W Gallicchio, J Gao, J George, EM Halverson, NW Harrington, N Henning, JW Hilton, GC Holder, GP Holzapfel, WL Hrubes, JD Huang, N Hubmayr, J Irwin, KD Keisler, R Knox, L Lee, AT Leitch, E Li, D Liang, C Luong-Van, D Marsden, G McMahon, JJ Mehl, J Meyer, SS Mocanu, L Montroy, TE Natoli, T Nibarger, JP Novosad, V Padin, S Pryke, C Reichardt, CL Ruhl, JE Saliwanchik, BR Sayre, JT Schaffer, KK Schulz, B Smecher, G Stark, AA Story, KT Tucker, C Vanderlinde, K Vieira, JD Viero, MP Wang, G Yefremenko, V Zahn, O Zemcov, M AF Hanson, D. Hoover, S. Crites, A. Ade, P. A. R. Aird, K. A. Austermann, J. E. Beall, J. A. Bender, A. N. Benson, B. A. Bleem, L. E. Bock, J. J. Carlstrom, J. E. Chang, C. L. Chiang, H. C. Cho, H-M. Conley, A. Crawford, T. M. de Haan, T. Dobbs, M. A. Everett, W. Gallicchio, J. Gao, J. George, E. M. Halverson, N. W. Harrington, N. Henning, J. W. Hilton, G. C. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Huang, N. Hubmayr, J. Irwin, K. D. Keisler, R. Knox, L. Lee, A. T. Leitch, E. Li, D. Liang, C. Luong-Van, D. Marsden, G. McMahon, J. J. Mehl, J. Meyer, S. S. Mocanu, L. Montroy, T. E. Natoli, T. Nibarger, J. P. Novosad, V. Padin, S. Pryke, C. Reichardt, C. L. Ruhl, J. E. Saliwanchik, B. R. Sayre, J. T. Schaffer, K. K. Schulz, B. Smecher, G. Stark, A. A. Story, K. T. Tucker, C. Vanderlinde, K. Vieira, J. D. Viero, M. P. Wang, G. Yefremenko, V. Zahn, O. Zemcov, M. CA SPTpol Collaboration TI Detection of B-Mode Polarization in the Cosmic Microwave Background with Data from the South Pole Telescope SO PHYSICAL REVIEW LETTERS LA English DT Article ID POWER SPECTRA; GRAVITY-WAVES; LIGHT; TEMPERATURE; CMB AB Gravitational lensing of the cosmic microwave background generates a curl pattern in the observed polarization. This "B-mode" signal provides a measure of the projected mass distribution over the entire observable Universe and also acts as a contaminant for the measurement of primordial gravity-wave signals. In this Letter we present the first detection of gravitational lensing B modes, using first-season data from the polarization-sensitive receiver on the South Pole Telescope (SPTpol). We construct a template for the lensing B-mode signal by combining E-mode polarization measured by SPTpol with estimates of the lensing potential from a Herschel-SPIRE map of the cosmic infrared background. We compare this template to the B modes measured directly by SPTpol, finding a nonzero correlation at 7.7 sigma significance. The correlation has an amplitude and scale dependence consistent with theoretical expectations, is robust with respect to analysis choices, and constitutes the first measurement of a powerful cosmological observable. C1 [Hanson, D.; Bender, A. N.; de Haan, T.; Dobbs, M. A.; Holder, G. P.; Smecher, G.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Hoover, S.; Crites, A.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Chiang, H. C.; Crawford, T. M.; Gallicchio, J.; Keisler, R.; Leitch, E.; Liang, C.; Luong-Van, D.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Natoli, T.; Schaffer, K. K.; Story, K. T.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Hoover, S.; Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Crites, A.; Carlstrom, J. E.; Crawford, T. M.; Leitch, E.; Liang, C.; Meyer, S. S.; Mocanu, L.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Ade, P. A. R.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Aird, K. A.; Hrubes, J. D.] Univ Chicago, Chicago, IL 60637 USA. [Austermann, J. E.; Cho, H-M.; Conley, A.; Everett, W.; Halverson, N. W.; Henning, J. W.] Univ Colorado, CASA, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Beall, J. A.; Cho, H-M.; Gao, J.; Hilton, G. C.; Hubmayr, J.; Irwin, K. D.; Li, D.; Nibarger, J. P.] NIST, Boulder, CO 80305 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K. T.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bock, J. J.; Padin, S.; Schulz, B.; Vieira, J. D.; Viero, M. P.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J. J.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Carlstrom, J. E.; Chang, C. L.; Mehl, J.; Wang, G.; Yefremenko, V.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, ZA-4000 Durban, South Africa. [George, E. M.; Harrington, N.; Holzapfel, W. L.; Huang, N.; Lee, A. T.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Marsden, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. [Novosad, V.; Yefremenko, V.] Argonne Natl Lab, Div Mat Sci, Argonne, IL 60439 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Schulz, B.] CALTECH, Ctr Infrared Proc & Anal, JPL, Pasadena, CA 91125 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP Hanson, D (reprint author), McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. RI Novosad, Valentyn/C-2018-2014; Holzapfel, William/I-4836-2015; Novosad, V /J-4843-2015; OI Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169 FU National Science Foundation [ANT-0638937]; NSF [PHY-1125897, 0959620, AST-0956135]; Gordon and Betty Moore Foundation [GBMF 947]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231, DE-AC02-06CH11357]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs Program; Canadian Institute for Advanced Research; Lorne Trottier Chair program in Astrophysics and Cosmology at McGill; CITA National Fellowship program; NASA Hubble Fellowship [HF-51275] FX The SPT is supported by the National Science Foundation through Grant No. ANT-0638937, with partial support provided by NSF Grant No. PHY-1125897. Support for the development and construction of SPTpol were provided by the Gordon and Betty Moore Foundation through Grant No. GBMF 947 to the University of Chicago, a gift from the Kavli Foundation, and NSF Grant No. 0959620. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Award No. DE-AC02-05CH11231. It also used resources of the CLUMEQ supercomputing consortium, part of the Compute Canada network. Research at Argonne National Laboratory and use of the Center for Nanoscale Materials are supported by the Office of Science of the U.S. Department of Energy under Award No. DE-AC02-06CH11357. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs Program, and the Canadian Institute for Advanced Research. The C. U. Boulder group acknowledges support from NSF Grant No. AST-0956135. We thank P. Hargrave at Cardiff University for antireflection coating the SPTpol lens, A. Datesman for his work on TES detectors at Argonne, R. Divan for microfabrication support at Argonne, and the members of the Truce Collaboration for their efforts in the design of the 150 GHz polarization detectors, in particular D. Becker, J. Britton, M. D. Niemack, and K. W. Yoon at NIST. We thank M. Lueker, T. Plagge, Z. Staniszewski, E. Shirokoff, H. Spieler, and R. Williamson for their considerable contributions to the SPT program. D. H. was supported by the Lorne Trottier Chair program in Astrophysics and Cosmology at McGill and by the CITA National Fellowship program. R. K. acknowledges support from NASA Hubble Fellowship Grant No. HF-51275. NR 50 TC 148 Z9 148 U1 2 U2 20 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 SEP 30 PY 2013 VL 111 IS 14 AR 141301 DI 10.1103/PhysRevLett.111.141301 PG 6 WC Physics, Multidisciplinary SC Physics GA 230TO UT WOS:000325366100001 PM 24138230 ER PT J AU Mitchell, JC Smith, DG AF Mitchell, Joseph C. Smith, David G. TI The History of Copeia: Metamorphosis and the Academic Coup SO COPEIA LA English DT Editorial Material C1 [Mitchell, Joseph C.] Mitchell Ecol Res Serv LLC, High Springs, FL 32655 USA. [Smith, David G.] Smithsonian Inst, Museum Support Ctr, Suitland, MD 20746 USA. RP Mitchell, JC (reprint author), Mitchell Ecol Res Serv LLC, POB 2520, High Springs, FL 32655 USA. EM dr.joe.mitchell@gmail.com; smithd@si.edu NR 4 TC 1 Z9 1 U1 0 U2 1 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD SEP 27 PY 2013 IS 3 BP 361 EP 365 DI 10.1643/OT-13-069 PG 5 WC Zoology SC Zoology GA AG2WM UT WOS:000335277800001 ER PT J AU Vari, RP Ferraris, CJ AF Vari, Richard P. Ferraris, Carl J., Jr. TI Two New Species of the Catfish Genus Tatia (Siluriformes: Auchenipteridae) from the Guiana Shield and a Reevaluation of the Limits of the Genus SO COPEIA LA English DT Article AB Analysis of samples of the auchenipterid catfish genus Tatia collected during a recent ichthyological survey in the Cuyuni River basin in Guyana revealed them to be an undescribed species. Comparative studies associated with the evaluation of that new species demonstrated that a sample of the genus from a right bank tributary of the Rio Orinoco in Venezuela, also on the Guiana Shield, represents a second species unknown to science. The placement of Tatia musaica, previously considered incertae sedis in the Centromochlinae, is evaluated and the species is reassigned to Tatia. C1 [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. RP Vari, RP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. EM varir@si.edu; carlferraris@comcast.net FU Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes, National Museum of Natural History of the Smithsonian Institution FX Support for this project was provided by the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes, National Museum of Natural History of the Smithsonian Institution. The type series of Tatia carolae was collected with support from the Biodiversity of the Guiana Shield Program of the National Museum of Natural History. C. Bernard and G. Maharaj of the University of Guyana greatly facilitated the expedition that yielded the specimens. We thank M. Sabaj Perez and J. Lundberg (ANSP) for the loan of specimens. Radiographs of specimens and other assistance during the study were provided by S. Raredon (USNM). Figures 1 and 2 were prepared by T. Griswold. Images of the holotype of Tatia musaica were accessed at the All Catfish Species Inventory website. NR 7 TC 6 Z9 6 U1 0 U2 7 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD SEP 27 PY 2013 IS 3 BP 396 EP 402 DI 10.1643/CI-12-115 PG 7 WC Zoology SC Zoology GA AG2WM UT WOS:000335277800005 ER PT J AU Parenti, LR Hadiaty, RK Lumbantobing, D Herder, F AF Parenti, Lynne R. Hadiaty, Renny K. Lumbantobing, Daniel Herder, Fabian TI Two New Ricefishes of the Genus Oryzias (Atherinomorpha: Beloniformes: Adrianichthyidae) Augment the Endemic Freshwater Fish Fauna of Southeastern Sulawesi, Indonesia SO COPEIA LA English DT Article AB Oryzias asinua and O. wolasi are two new species of ricefishes described from several disjunct inland freshwater habitats in the Indonesian province of Sulawesi Tenggara or southeastern Sulawesi. With O. woworae, the first described endemic ricefish of Sulawesi Tenggara, they comprise a group of small, colorful species characterized by orange to deep red dorsal and ventral margins of the caudal fin and the ventral margin of the caudal peduncle and at least the posterior portion of the base of the anal fin, and a bluish sheen on the body in both sexes that is most pronounced in live adult males. The two new species are distinguished from O. woworae by elongate middle dorsal-fin rays in adult males that reach the posterior extent of the first principal caudal-fin ray and by an orange-colored olfactory epithelium that marks each nasal organ in females. Oryzias asinua is relatively slender compared to O. wolasi and O. woworae: the body is narrow (21-25% SL, with a mean 22.9, in O. asinua versus 23-32% SL, mean 25.3 in O. wolasi and 22-30% SL, mean 26 in O. woworae). Oryzias asinua has fewer procurrent caudal-fin rays in the lower lobe (4-5 versus 5-7 in O. wolasi and 5-6 in O. woworae). Oryzias wolasi is golden in life in both sexes and relatively deep-bodied, reaching 32% SL, and has a deeper caudal peduncle (11-12% SL, mean 11.2, versus 9-11, mean 10, in O. asinua and 8-11, mean 9.2, in O. woworae). Maximum parsimony and Bayesian inference analyses of the mitochondrial cytochrome c oxidase subunit 1 (COI) sequence, the DNA barcode, support our hypothesis that we sequenced representatives of three species. All species are allopatric. Description of O. asinua and O. wolasi brings the number of valid species in the beloniform family Adrianichthyidae to 35, 17 of which are endemic to Sulawesi. The two new species are just the second and third ricefishes described from the province of Sulawesi Tenggara, a neglected region in exploration and discovery of the freshwater fish fauna of the Indonesian islands of Sulawesi. C1 [Parenti, Lynne R.; Lumbantobing, Daniel] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Hadiaty, Renny K.] Indonesian Inst Sci LIPI, Biol Res Ctr, Div Zool, Museum Zool Bogoriense, Cibinong 16911, Indonesia. [Lumbantobing, Daniel] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Herder, Fabian] Zool Forsch Museum Alexander Koenig, Sekt Ichthyol, D-53113 Bonn, Germany. RP Parenti, LR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012,NHB MRC 159, Washington, DC 20013 USA. EM parentil@si.edu; renny_hadiaty@yahoo.com; dntobing@gwmail.gwu.edu; f.herder.zfmk@uni-bonn.de FU Division of Fishes (USNM) FX Fieldwork and preparation and publication of this manuscript were supported by the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes (USNM). H.-G. Evers uncovered a then unknown ricefish species, described here as O. wolasi, and kindly provided specific information on two of the collection localities. B. Asriyana (Universitas Haluoleo, Kendall) kindly helped us obtain field supplies and P. Asrul served as our able driver and field guide. Photographs in Figure 5 were taken by S. Raredon (USNM) who also skillfully prepared numerous radiographs. All other photographs are by the first three authors. J. Mounts (USNM) assisted with preparation of Figures 1, 5, 7, and 8. L. Weigt and J. Hunt (LAB) provided support for the molecular analysis. D. Cole (USNM) supplied a base map used in Figure 2. J. Clayton (USNM) provided additional valuable technical assistance. P. Ciccotto (University of Maryland, Baltimore County) helped sort specimens at the USNM. NR 29 TC 9 Z9 10 U1 0 U2 7 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD SEP 27 PY 2013 IS 3 BP 403 EP 414 DI 10.1643/CI-12-114 PG 12 WC Zoology SC Zoology GA AG2WM UT WOS:000335277800006 ER PT J AU Dupuy, TJ Kraus, AL AF Dupuy, Trent J. Kraus, Adam L. TI Distances, Luminosities, and Temperatures of the Coldest Known Substellar Objects SO SCIENCE LA English DT Article ID COOLEST BROWN DWARFS; EXTRASOLAR GIANT PLANETS; L/T TRANSITION; MASS FUNCTION; T-DWARFS; Y DWARFS; SPECTRA; DISCOVERY; BINARIES; MODELS AB The coolest known brown dwarfs are our best analogs to extrasolar gas-giant planets. The prolific detections of such cold substellar objects in the past 2 years have spurred intensive follow-up, but the lack of accurate distances is a key gap in our understanding. We present a large sample of precise distances based on homogeneous mid-infrared astrometry that robustly establishes absolute fluxes, luminosities, and temperatures. The coolest brown dwarfs have temperatures of 400 to 450 kelvin and masses almost equal to 5 to 20 times that of Jupiter, showing they bridge the gap between hotter brown dwarfs and gas-giant planets. At these extremes, spectral energy distributions no longer follow a simple correspondence with temperature, suggesting an increasing role of other physical parameters, such as surface gravity, vertical mixing, clouds, and metallicity. C1 [Dupuy, Trent J.; Kraus, Adam L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kraus, Adam L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Dupuy, TJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tdupuy@cfa.harvard.edu FU NASA [NAS 5-26555]; Hubble Fellowship [HST-HF-51271.01-A]; Space Telescope Science Institute; Clay Fellowship FX We thank M. C. Liu for many helpful suggestions for improving this article; C. V. Morley for fruitful discussions regarding her and collaborators' model atmospheres, particularly the Vega zero points; K. N. Allers for assistance in computing photometry from our IRAC data; and M. C. Cushing for making available published spectra of our targets. 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. T.J.D. acknowledges support from Hubble Fellowship grant HST-HF-51271.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy for NASA, under contract NAS 5-26555. A.L.K. is supported by a Clay Fellowship. Our imaging data are available in the Spitzer Heritage Archive at http://sha.ipac.caltech.edu/applications/Spitzer/SHA, and the astrometric measurements we derived are given in table S1. NR 25 TC 40 Z9 40 U1 0 U2 5 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 27 PY 2013 VL 341 IS 6153 BP 1492 EP 1495 DI 10.1126/science.1241917 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 224NS UT WOS:000324894600044 PM 24009359 ER PT J AU Tan, BK Yassin, G Grimes, P Jacobs, K AF Tan, B. -K. Yassin, G. Grimes, P. Jacobs, K. TI 650 GHz SIS mixer fabricated on silicon-on-insulator substrate SO ELECTRONICS LETTERS LA English DT Article C1 [Tan, B. -K.; Yassin, G.] Univ Oxford, Oxford OX1 3RH, England. [Grimes, P.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astron Observ, Cambridge, MA 02138 USA. [Jacobs, K.] Univ Cologne, Superconducting Microdevices Lab, KOSMA Phys Inst 1, D-50937 Cologne, Germany. RP Tan, BK (reprint author), Univ Oxford, Denys Wilkinson Bldg, Oxford OX1 3RH, England. EM g.yassin1@physics.ox.ac.uk FU Science and Technology Facilities Council [ST/J001503/1] NR 2 TC 4 Z9 4 U1 0 U2 3 PU INST ENGINEERING TECHNOLOGY-IET PI HERTFORD PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND SN 0013-5194 EI 1350-911X J9 ELECTRON LETT JI Electron. Lett. PD SEP 26 PY 2013 VL 49 IS 20 BP 1273 EP 1274 PG 2 WC Engineering, Electrical & Electronic SC Engineering GA 278AO UT WOS:000328860600012 ER PT J AU Gonzalez-Porter, GP Maldonado, JE Flores-Villela, O Vogt, RC Janke, A Fleischer, RC Hailer, F AF Gonzalez-Porter, Gracia P. Maldonado, Jesus E. Flores-Villela, Oscar Vogt, Richard C. Janke, Axel Fleischer, Robert C. Hailer, Frank TI Cryptic Population Structuring and the Role of the Isthmus of Tehuantepec as a Gene Flow Barrier in the Critically Endangered Central American River Turtle SO PLOS ONE LA English DT Article ID ALLELE FREQUENCY DATA; EVOLUTIONARY PROCESSES; COMPUTER-PROGRAM; CONSERVATION GENETICS; SEQUENCE DATA; F-STATISTICS; NUCLEAR; MITOCHONDRIAL; DIVERSITY; DIVERSIFICATION AB The critically endangered Central American River Turtle (Dermatemys mawii) is the only remaining member of the Dermatemydidae family, yet little is known about its population structuring. In a previous study of mitochondrial (mt) DNA in the species, three main lineages were described. One lineage (Central) was dominant across most of the range, while two other lineages were restricted to Papaloapan (PAP; isolated by the Isthmus of Tehuantepec and the Sierra de Santa Marta) or the south-eastern part of the range (1D). Here we provide data from seven polymorphic microsatellite loci and the R35 intron to re-evaluate these findings using DNA from the nuclear genome. Based on a slightly expanded data set of a total of 253 samples from the same localities, we find that mtDNA and nuclear DNA markers yield a highly congruent picture of the evolutionary history and population structuring of D. mawii. While resolution provided by the R35 intron (sequenced for a subset of the samples) was very limited, the microsatellite data revealed pronounced population structuring. Within the Grijalva-Usumacinta drainage basin, however, many populations separated by more than 300 kilometers showed signals of high gene flow. Across the entire range, neither mitochondrial nor nuclear DNA show a significant isolation-by-distance pattern, but both genomes highlight that the D. mawii population in the Papaloapan basin is genetically distinctive. Further, both marker systems detect unique genomic signals in four individuals with mtDNA clade 1D sampled on the southeast edge of the Grijalva-Usumacinta basin. These individuals may represent a separate cryptic taxon that is likely impacted by recent admixture. C1 [Gonzalez-Porter, Gracia P.; Maldonado, Jesus E.; Fleischer, Robert C.; Hailer, Frank] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Gonzalez-Porter, Gracia P.; Flores-Villela, Oscar] Univ Nacl Autonoma Mexico, Museo Zool, Fac Ciencias, Mexico City 04510, DF, Mexico. [Maldonado, Jesus E.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Vogt, Richard C.] Coordinacao Biodiversidade, Inst Nacl Pesquisas Amazonia, Manaus, Amazonas, Brazil. [Janke, Axel] Goethe Univ Frankfurt, Inst Ecol Evolut & Divers, Biologicum, D-60054 Frankfurt, Germany. [Janke, Axel; Hailer, Frank] Biodivers & Climate Res Ctr, Frankfurt, Germany. [Janke, Axel; Hailer, Frank] Senckenberg Gesell Nat Forsch, Frankfurt, Germany. RP Gonzalez-Porter, GP (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC 20008 USA. EM graciasyed@gmail.com; frashai@gmx.net RI Hailer, Frank/C-9114-2012 OI Hailer, Frank/0000-0002-2340-1726 FU Consejo Nacional de Ciencia y Tecnologia fellowship [210994]; Turtle Conservation Fund; Conservation International grants; Philadelphia Zoo Conservation Program; Philadelphia Zoo Docent council; Smithsonian Restricted Endowment funds; EA Schreiber; Seabird Research, Inc; "LOEWE - Landes-Offensive zur Entwicklung Wissenschaftlichokonomischer Exzellenz" of Hesse's Ministry of Higher Education, Research, and the Arts FX Funding was provided by Consejo Nacional de Ciencia y Tecnologia fellowship No. 210994; the Turtle Conservation Fund grants in 2004, 2006 and 2009; Conservation International grants in 2007 and 2009; the Philadelphia Zoo Conservation Program Financial Support for 2005, 2006, 2007, 2008; and an award from the Philadelphia Zoo Docent council in 2007. FH received support from the Smithsonian Restricted Endowment funds, EA Schreiber, Seabird Research, Inc, and "LOEWE - Landes-Offensive zur Entwicklung Wissenschaftlichokonomischer Exzellenz" of Hesse's Ministry of Higher Education, Research, and the Arts. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 77 TC 2 Z9 2 U1 4 U2 19 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 25 PY 2013 VL 8 IS 9 AR e71668 DI 10.1371/journal.pone.0071668 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 228VC UT WOS:000325218700002 PM 24086253 ER PT J AU Adams, RMM Liberti, J Illum, AA Jones, TH Nash, DR Boomsma, JJ AF Adams, Rachelle M. M. Liberti, Joanito Illum, Anders A. Jones, Tappey H. Nash, David R. Boomsma, Jacobus J. TI Chemically armed mercenary ants protect fungus-farming societies SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE evolutionary transition; symbiosis; Attini; Solenopsidini ID SOCIAL PARASITISM; HYMENOPTERA-FORMICIDAE; GENUS MEGALOMYRMEX; VENOM ALKALOIDS; GROWING ANTS; EVOLUTION; TRACHYMYRMEX; ADAPTATION; CHEMISTRY; SYMBIONT AB The ants are extraordinary in having evolved many lineages that exploit closely related ant societies as social parasites, but social parasitism by distantly related ants is rare. Here we document the interaction dynamics among a Sericomyrmex fungus-growing ant host, a permanently associated parasitic guest ant of the genus Megalomyrmex, and a raiding agro-predator of the genus Gnamptogenys. We show experimentally that the guest ants protect their host colonies against agro-predator raids using alkaloid venom that is much more potent than the biting defenses of the host ants. Relatively few guest ants are sufficient to kill raiders that invariably exterminate host nests without a cohabiting guest ant colony. We also show that the odor of guest ants discourages raider scouts from recruiting nestmates to host colonies. Our results imply that Sericomyrmex fungus-growers obtain a net benefit from their costly guest ants behaving as a functional soldier caste to meet lethal threats from agro-predator raiders. The fundamentally different life histories of the agro-predators and guest ants appear to facilitate their coexistence in a negative frequency-dependent manner. Because a guest ant colony is committed for life to a single host colony, the guests would harm their own interests by not defending the host that they continue to exploit. This conditional mutualism is analogous to chronic sickle cell anemia enhancing the resistance to malaria and to episodes in human history when mercenary city defenders offered either net benefits or imposed net costs, depending on the level of threat from invading armies. C1 [Adams, Rachelle M. M.; Liberti, Joanito; Illum, Anders A.; Nash, David R.; Boomsma, Jacobus J.] Univ Copenhagen, Dept Biol, Ctr Social Evolut, DK-2100 Copenhagen, Denmark. [Adams, Rachelle M. M.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Jones, Tappey H.] Virginia Mil Inst, Dept Chem, Lexington, VA 24450 USA. RP Adams, RMM (reprint author), Univ Copenhagen, Dept Biol, Ctr Social Evolut, DK-2100 Copenhagen, Denmark. EM rmmadams@gmail.com; drnash@bio.ku.dk RI Nash, David/B-2916-2009; Nash, David/H-4433-2012; Boomsma, Jacobus/M-2785-2014; OI Nash, David/0000-0002-0462-6794; Nash, David/0000-0002-0462-6794; Boomsma, Jacobus/0000-0002-3598-1609; Liberti, Joanito/0000-0002-4158-2591 FU Marie Curie International Incoming Fellowship [237266-evolutionAry traNsitions: Chemical Ecology of Parasitic Societies (ANCEPS)]; Smithsonian Molecular Evolution Postdoctoral Fellowship; Danish National Research Foundation [DNRF57] FX We thank the staff and researchers at the Smithsonian Tropical Research Institute for help with logistics and facilities, the Autoridad Nacional del Ambiente y el Mar for permission to sample ants in Panama and export them to Denmark, Friluftsland A/S and John B. Anderson for equipment, and Rozlyn E. Haley for the ant drawings. We also thank two anonymous reviewers for comments and suggestions that improved this article. This work was funded by a Marie Curie International Incoming Fellowship [237266-evolutionAry traNsitions: Chemical Ecology of Parasitic Societies (ANCEPS), to R. M. M. A.], a Smithsonian Molecular Evolution Postdoctoral Fellowship (to R. M. M. A.), and a grant from the Danish National Research Foundation (DNRF57, to J.J.B.). NR 31 TC 10 Z9 11 U1 4 U2 77 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 SEP 24 PY 2013 VL 110 IS 39 BP 15752 EP 15757 DI 10.1073/pnas.1311654110 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 222XE UT WOS:000324765100056 PM 24019482 ER PT J AU Macedo, CFB Pani, P Cardoso, V Crispino, LCB AF Macedo, Caio F. B. Pani, Paolo Cardoso, Vitor Crispino, Luis C. B. TI Astrophysical signatures of boson stars: Quasinormal modes and inspiral resonances SO PHYSICAL REVIEW D LA English DT Article ID NONBARYONIC COMPACT OBJECT; BLACK-HOLES; NONRADIAL OSCILLATIONS; GENERAL-RELATIVITY; GRAVITATIONAL-RADIATION; ACCRETION DISC; STELLAR MODELS; NEUTRON-STARS; STABILITY; EQUATION AB Compact bosonic field configurations, or boson stars, are promising dark matter candidates which have been invoked as an alternative description for the supermassive compact objects in active galactic nuclei. Boson stars can be comparable in size and mass to supermassive objects, and they might be hard to distinguish by electromagnetic observations. However, boson stars do not possess an event horizon, and their global spacetime structure is different from that of a black hole. This leaves a characteristic imprint in the gravitational-wave emission, which can be used as a discriminant between black holes and other horizonless compact objects. Here we perform a detailed study of boson stars and their gravitational-wave signatures in a fully relativistic setting, a study which was lacking in the existing literature in many respects. We construct several fully relativistic boson star configurations, and we analyze their geodesic structure and free oscillation spectra, or quasinormal modes. We explore the gravitational and scalar response of boson star spacetimes to an inspiraling stellar-mass object and compare it to its black hole counterpart. We find that a generic signature of compact boson stars is the resonant-mode excitation by a small compact object on stable quasicircular geodesic motion. C1 [Macedo, Caio F. B.; Cardoso, Vitor; Crispino, Luis C. B.] Fed Univ Para, Fac Fis, BR-66075110 Belem, Para, Brazil. [Macedo, Caio F. B.; Pani, Paolo; Cardoso, Vitor] Univ Tecn Lisboa, Inst Super Tecn, CENTRA, Dept Fis, P-1049 Lisbon, Portugal. [Pani, Paolo] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Cardoso, Vitor] Perimeter Inst Theoret Phys Waterloo, Waterloo, ON N2J 2W9, Canada. [Cardoso, Vitor] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA. RP Macedo, CFB (reprint author), Fed Univ Para, Fac Fis, BR-66075110 Belem, Para, Brazil. EM caiomacedo@ufpa.br; paolo.pani@ist.utl.pt; vitor.cardoso@ist.utl.pt; crispino@ufpa.br RI Cardoso, Vitor/K-1877-2015; Macedo, Caio/F-1143-2015; Pani, Paolo/G-7412-2012; Crispino, Luis/F-2148-2017 OI Cardoso, Vitor/0000-0003-0553-0433; Macedo, Caio/0000-0001-9251-4938; Pani, Paolo/0000-0003-4443-1761; Crispino, Luis/0000-0003-0710-7241 FU CAPES; CNPq; European Community through the Intra-European Marie Curie [aStronGR-2011-298297]; European Union's FP7 ERC Starting Grant "The dynamics of black holes: Testing the limits of Einstein's theory'' [DyBHo-256667]; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Economic Development and Innovation; NRHEP [295189 FP7-PEOPLE-2011-IRSES]; FCT-Portugal [PTDC/FIS/098025/2008, PTDC/FIS/098032/2008, PTDC/FIS/116625/2010, CERN/FP/116341/2010, CERN/FP/123593/2011]; BSC [AECT-2012-3-0012, AECT-2012-2-0014, AECT-2012-3-0011]; NSF [PHY-090003]; Finis Terrae [CESGA-ICTS-234] FX We are indebted to Emanuele Berti, Kazunari Eda, Luis Lehner, Joseph Silk and especially to Enrico Barausse for useful correspondence. C. M. and L. C. acknowledge CAPES and CNPq for partial financial support. L. C. is grateful to CENTRA-IST for kind hospitality. P. P. acknowledges financial support provided by the European Community through the Intra-European Marie Curie Contract No. aStronGR-2011-298297 and the kind hospitality of Kinki University in Osaka. V. C. acknowledges partial financial support provided under the European Union's FP7 ERC Starting Grant "The dynamics of black holes: Testing the limits of Einstein's theory'' Grant Agreement No. DyBHo-256667. Research at Perimeter Institute is supported by the Government of Canada through Industry Canada and by the Province of Ontario through the Ministry of Economic Development and Innovation. This work was supported by the NRHEP 295189 FP7-PEOPLE-2011-IRSES Grant, and by FCT-Portugal through Projects No. PTDC/FIS/098025/2008, No. PTDC/FIS/098032/2008, No. PTDC/FIS/116625/2010, No. CERN/FP/116341/2010 and No. CERN/FP/123593/2011. Computations were performed on the "Baltasar Sete-Sois'' cluster at IST, the cane cluster in Poland through PRACE DECI-7 "Black hole dynamics in metric theories of gravity,'' on Altamira in Cantabria through BSC Grant No. AECT-2012-3-0012, on Caesaraugusta in Zaragoza through BSC Grants No. AECT-2012-2-0014 and No. AECT-2012-3-0011, XSEDE clusters SDSC Trestles and NICS Kraken through NSF Grant No. PHY-090003, and Finis Terrae through Grant No. CESGA-ICTS-234. NR 65 TC 22 Z9 22 U1 1 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD SEP 23 PY 2013 VL 88 IS 6 AR 064046 DI 10.1103/PhysRevD.88.064046 PG 20 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 221WQ UT WOS:000324691500011 ER PT J AU Pogue, MG Ouellette, GD Harp, CE AF Pogue, Michael G. Ouellette, Gary D. Harp, Charles E. TI A revision of the Schinia volupia (Fitch) species complex (Lepidoptera: Noctuidae: Heliothinae) SO ZOOTAXA LA English DT Article DE DNA barcoding; COI; taxonomy; synonymy; host plants ID DNA BARCODES; SKIPPER BUTTERFLIES; MOTHS LEPIDOPTERA; GENUS AB DNA barcode analysis of cytochrome oxidase I (COI) could not differentiate between the species of the Schinia volupia (Fitch, 1868) complex including S. volupia, S. masoni Smith, S. fulleri (McElvare, 1961); S. sanrafaeli Opler, 2004; S. miniana (Grote, 1881); and S. biforma Smith, 1906. Genitalic characters could only differentiate S. biforma from the S. volupia complex. Based on forewing color and pattern, larval host plant utilization, and geographic distribution, S. volupia, S. sanrafaeli, S. fulleri, and S. miniana are recognized as valid species and S. masoni is considered a new synonym of S. volupia. Schinia volupia, S. fulleri, S. sanrafaeli, S. miniana, and S. biforma are diagnosed and described. A variety of adult images are presented to show the range of variation among these species. Male and female genitalia of all included taxa are illustrated. Host plant utilization is discussed and illustrated. Distribution maps for examined specimens are provided. C1 [Pogue, Michael G.; Ouellette, Gary D.] ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst,NMNH, Washington, DC 20013 USA. [Harp, Charles E.] Colorado State Univ, CP Gillette Museum Arthropod Divers, Ft Collins, CO 80523 USA. RP Pogue, MG (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst,NMNH, POB 37012,MRC 168, Washington, DC 20013 USA. EM michael.pogue@ars.usda.gov; gary.ouellette@ars.usda.gov; cehmoth@aol.com NR 49 TC 2 Z9 2 U1 0 U2 4 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 J9 ZOOTAXA JI Zootaxa PD SEP 23 PY 2013 VL 3716 IS 2 BP 157 EP 191 PG 35 WC Zoology SC Zoology GA 221UR UT WOS:000324685800003 PM 26106771 ER PT J AU Sharma, S Dutta, T Maldonado, JE Wood, TC Panwar, HS Seidensticker, J AF Sharma, Sandeep Dutta, Trishna Maldonado, Jesus E. Wood, Thomas C. Panwar, Hemendra Singh Seidensticker, John TI Forest corridors maintain historical gene flow in a tiger metapopulation in the highlands of central India SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Panthera tigris; central India; gene flow; connectivity; landscape genetics; non-invasive genetic analysis ID EFFECTIVE POPULATION-SIZE; MICROSATELLITE LOCI; HABITAT FRAGMENTATION; NATURAL-POPULATIONS; ANIMAL POPULATIONS; MIGRATION RATES; HUMAN FOOTPRINT; NORTH-AMERICA; CANADA LYNX; EXTINCTION AB Understanding the patterns of gene flow of an endangered species metapopulation occupying a fragmented habitat is crucial for landscape-level conservation planning and devising effective conservation strategies. Tigers (Panthera tigris) are globally endangered and their populations are highly fragmented and exist in a few isolated metapopulations across their range. We used multi-locus genotypic data from 273 individual tigers (Panthera tigris tigris) from four tiger populations of the Satpura-Maikal landscape of central India to determine whether the corridors in this landscape are functional. This 45 000 km(2) landscape contains 17% of India's tiger population and 12% of its tiger habitat. We applied Bayesian and coalescent-based analyses to estimate contemporary and historical gene flow among these populations and to infer their evolutionary history. We found that the tiger metapopulation in central India has high rates of historical and contemporary gene flow. The tests for population history reveal that tigers populated central India about 10 000 years ago. Their population sub-division began about 1000 years ago and accelerated about 200 years ago owing to habitat fragmentation, leading to four spatially separated populations. These four populations have been in migration-drift equilibrium maintained by high gene flow. We found the highest rates of contemporary gene flow in populations that are connected by forest corridors. This information is highly relevant to conservation practitioners and policy makers, because deforestation, road widening and mining are imminent threats to these corridors. C1 [Sharma, Sandeep; Dutta, Trishna; Maldonado, Jesus E.; Seidensticker, John] Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Sharma, Sandeep; Dutta, Trishna; Wood, Thomas C.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Sharma, Sandeep] Clemson Univ, Clemson Inst Pk, Clemson, SC 29631 USA. [Dutta, Trishna] Clemson Univ, Sch Agr Forest & Environm Sci, Clemson, SC 29631 USA. [Panwar, Hemendra Singh] PEACE Inst Charitable Trust, Delhi 110091, India. RP Sharma, S (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20013 USA. EM sandeeps17@gmail.com FU Smithsonian Conservation Biology Institute (SCBI); Friends of the National Zoo (FONZ); Kathryn Fuller Science for Nature Fund of World Wildlife Fund (WWF); International Bear Association (IBA); George Mason University FX Support for this study was provided by the Smithsonian Conservation Biology Institute (SCBI), Friends of the National Zoo (FONZ), Kathryn Fuller Science for Nature Fund of World Wildlife Fund (WWF) and International Bear Association (IBA). Support for manuscript preparation was provided by a dissertation completion grant from George Mason University. NR 67 TC 25 Z9 26 U1 8 U2 100 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 SEP 22 PY 2013 VL 280 IS 1767 AR 20131506 DI 10.1098/rspb.2013.1506 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 298JK UT WOS:000330319800015 PM 23902910 ER PT J AU Martinez-Garcia, R Calabrese, JM Lopez, C AF Martinez-Garcia, Ricardo Calabrese, Justin M. Lopez, Cristobal TI Spatial patterns in mesic savannas: The local facilitation limit and the role of demographic stochasticity SO JOURNAL OF THEORETICAL BIOLOGY LA English DT Article DE Vegetation models; Nonlinear dynamics; Stochastic processes ID AFRICAN SAVANNAS; VEGETATION PATTERNS; WOODY COVER; TIGER BUSH; TREE; KALAHARI; FIRE; COEXISTENCE; COMPETITION; DYNAMICS AB We propose a model equation for the dynamics of tree density in mesic savannas which considers long-range competition among trees and the effect of fire indirectly acting as a local facilitation mechanism. Despite the fact that we take short-range facilitation to the local-range limit, the standard full spectrum of spatial structures already obtained in self-organization models of vegetation is recovered. Nonlocal competition, in the limit of infinitesimally short facilitation, promotes the clustering of trees. The long time coexistence between trees and grass, and how fires affect the survival of trees as well as the maintenance of the patterns is studied. The influence of demographic noise is analyzed. The stochastic system, under the parameter constraints typical of mesic savannas, shows non-homogeneous patterns characteristic of realistic situations. The coexistence of trees and grass still remains at reasonable noise intensities. (c) 2013 Elsevier Ltd. All rights reserved. C1 [Martinez-Garcia, Ricardo; Lopez, Cristobal] UIB, Inst Fis Interdisciplinar & Sistemas Complejos CS, IFISC, E-07122 Palma De Mallorca, Spain. [Calabrese, Justin M.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA. RP Martinez-Garcia, R (reprint author), UIB, Inst Fis Interdisciplinar & Sistemas Complejos CS, IFISC, E-07122 Palma De Mallorca, Spain. EM ricardo@ifisc.uib-csic.es; CalabreseJ@si.edu; clopez@ifisc.uib-csic.es RI Martinez-Garcia, Ricardo/J-4836-2013; Calabrese, Justin/B-9131-2012; OI Martinez-Garcia, Ricardo/0000-0003-2765-8147; Lopez, Cristobal/0000-0002-3445-4284 FU JAEPredoc program of CSIC; MICINN (Spain); FEDER (EU) through Project FISICOS [FIS2007-60327] FX R.M.-G. is supported by the JAEPredoc program of CSIC. R.M.-G. and C.L. acknowledge support from MICINN (Spain) and FEDER (EU) through Project FISICOS (FIS2007-60327). We acknowledge Federico Vazquez and Emilio Hernandez-Garcia for their comments and discussion. We also acknowledge the detailed reading and insightful comments of three anonymous referees which greatly helped to improve this paper. NR 47 TC 9 Z9 9 U1 2 U2 33 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0022-5193 EI 1095-8541 J9 J THEOR BIOL JI J. Theor. Biol. PD SEP 21 PY 2013 VL 333 BP 156 EP 165 DI 10.1016/j.jtbi.2013.05.024 PG 10 WC Biology; Mathematical & Computational Biology SC Life Sciences & Biomedicine - Other Topics; Mathematical & Computational Biology GA 195FV UT WOS:000322688600017 PM 23747988 ER PT J AU Aliu, E Archambault, S Arlen, T Aune, T Beilicke, M Benbow, W Bird, R Bottcher, M Bouvier, A Bugaev, V Byrum, K Cesarini, A Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Dickherber, R Duke, C Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Griffin, S Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Kaaret, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lang, MJ Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Moriarty, P Mukherjee, R Nelson, T de Bhroithe, AO Ong, RA Orr, M Otte, AN Park, N Perkins, JS Pichel, A Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Saxon, DB Schroedter, M Sembroski, GH Skole, C Smith, AW Staszak, D Telezhinsky, I Theiling, M Tyler, J Varlotta, A Vassiliev, VV Wakely, SP Weekes, TC Weinstein, A Welsing, R Williams, DA Zitzer, B AF Aliu, E. Archambault, S. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bird, R. Boettcher, M. Bouvier, A. Bugaev, V. Byrum, K. Cesarini, A. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Dickherber, R. Duke, C. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Griffin, S. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Moriarty, P. Mukherjee, R. Nelson, T. de Bhroithe, A. O'Faolain Ong, R. A. Orr, M. Otte, A. N. Park, N. Perkins, J. S. Pichel, A. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Saxon, D. B. Schroedter, M. Sembroski, G. H. Skole, C. Smith, A. W. Staszak, D. Telezhinsky, I. Theiling, M. Tyler, J. Varlotta, A. Vassiliev, V. V. Wakely, S. P. Weekes, T. C. Weinstein, A. Welsing, R. Williams, D. A. Zitzer, B. TI MULTIWAVELENGTH OBSERVATIONS AND MODELING OF 1ES 1959+650 IN A LOW FLUX STATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; BL Lacertae objects: individual (1ES 1959+650=VER J1959+651); galaxies: active; gamma rays: galaxies ID BL-LACERTAE OBJECTS; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; LARGE-AREA TELESCOPE; GAMMA-RAYS; BLAZAR 1ES-1959+650; RELATIVISTIC JET; SOURCE CATALOG; LAC OBJECTS; TEV-FLARE; RADIATION AB We report on the VERITAS observations of the high-frequency peaked BL Lac object 1ES 1959+650 in the period 2007-2011. This source is detected at TeV energies by VERITAS at 16.4 standard deviation (sigma) significance in 7.6 hr of observation in a low flux state. A multiwavelength spectral energy distribution (SED) is constructed from contemporaneous data from VERITAS, Fermi-LAT, RXTE PCA, and Swift UVOT. Swift XRT data is not included in the SED due to a lack of simultaneous observations with VERITAS. In contrast to the orphan gamma-ray flare exhibited by this source in 2002, the X-ray flux of the source is found to vary by an order of magnitude, while other energy regimes exhibit less variable emission. A quasi-equilibrium synchrotron self-Compton model with an additional external radiation field is used to describe three SEDs corresponding to the lowest, highest, and average X-ray states. The variation in the X-ray spectrum is modeled by changing the electron injection spectral index, with minor adjustments of the kinetic luminosity in electrons. This scenario produces small-scale flux variability of the order of less than or similar to 2 in the high energy (E > 1MeV) and very high energy (E > 100 GeV) gamma-ray regimes, which is corroborated by the Fermi-LAT, VERITAS, and Whipple 10 m telescope light curves. C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Arlen, T.; Aune, T.; Majumdar, P.; Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Beilicke, M.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bird, R.; Collins-Hughes, E.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Boettcher, M.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Boettcher, M.] North West Univ, Ctr Space Res, ZA-2531 Potchefstroom, South Africa. [Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cesarini, A.; Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Dumm, J.; Fortson, L.; Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 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.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Finnegan, G.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Gall, D.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [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. [Humensky, T. B.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kertzman, M.] DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Majumdar, P.] Saha Inst Nucl Phys, Kolkata 700064, India. [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. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [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; OI Khassen, Yerbol/0000-0002-7296-3100; Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NARC'S in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K.; Irish Research Council "Embark Initiative" 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 NARC'S 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.; Anna O'Faolain de Bhroithe acknowledges the support of the Irish Research Council "Embark Initiative." NR 59 TC 7 Z9 7 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2013 VL 775 IS 1 AR 3 DI 10.1088/0004-637X/775/1/3 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220VU UT WOS:000324615800003 ER PT J AU Brown, WR Cohen, JG Geller, MJ Kenyon, SJ AF Brown, Warren R. Cohen, Judith G. Geller, Margaret J. Kenyon, Scott J. TI THE ORIGIN OF HVS17, AN UNBOUND MAIN SEQUENCE B STAR AT 50 kpc SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; Galaxy: halo; Galaxy: kinematics and dynamics; stars: early-type; stars: individual (SDSS J164156.39+472346.1) ID MASSIVE BLACK-HOLE; HORIZONTAL-BRANCH STARS; LARGE-MAGELLANIC-CLOUD; HYPERVELOCITY STARS; GALACTIC-CENTER; STELLAR ORBITS; MILKY-WAY; THEORETICAL ISOCHRONES; VELOCITY DISTRIBUTIONS; ROTATION VELOCITIES AB We analyze Keck Echellette Spectrograph and Imager spectroscopy of HVS17, a B-type star traveling with a Galactic rest frame radial velocity of +445 km s(-1) in the outer halo of the Milky Way. HVS17 has the projected rotation of a main sequence B star and is chemically peculiar, with solar iron abundance and sub-solar alpha abundance. Comparing measured T-eff and log g with stellar evolution tracks implies that HVS17 is a 3.91 +/- 0.09 M-circle dot, 153 +/- 9 Myr old star at a Galactocentric distance of r = 48.5 +/- 4.6 kpc. The time between its formation and ejection significantly exceeds 10 Myr and thus is difficult to reconcile with any Galactic disk runaway scenario involving massive stars. The observations are consistent, on the other hand, with a hypervelocity star ejection from the Galactic center. We show that Gaia proper motion measurements will easily discriminate between a disk and Galactic center origin, thus allowing us to use HVS17 as a test particle to probe the shape of the Milky Way's dark matter halo. C1 [Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Cohen, Judith G.] CALTECH, Palomar Observ, Pasadena, CA 91125 USA. RP Brown, WR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM wbrown@cfa.harvard.edu; jlc@astro.caltech.edu; mgeller@cfa.harvard.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X FU Smithsonian Institution; [AST-0908139] FX This work was supported in part by the Smithsonian Institution. J. Cohen acknowledges partial support from AST-0908139. This research makes use of NASA's Astrophysics Data System Bibliographic Services. We are grateful to the many people who have worked to make the Keck Telescopes and their instruments a reality, and who operate and maintain these observatories. The authors extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, none of the observations presented herein would have been possible. NR 73 TC 5 Z9 5 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2013 VL 775 IS 1 AR 32 DI 10.1088/0004-637X/775/1/32 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220VU UT WOS:000324615800032 ER PT J AU Burke, MJ Kraft, RP Soria, R Maccarone, TJ Raychaudhury, S Sivakoff, GR Birkinshaw, M Brassington, NJ Forman, WR Hardcastle, MJ Jones, C Murray, SS Worrall, DM AF Burke, Mark J. Kraft, Ralph P. Soria, Roberto Maccarone, Thomas J. Raychaudhury, Somak Sivakoff, Gregory R. Birkinshaw, Mark Brassington, Nicola J. Forman, William R. Hardcastle, Martin J. Jones, Christine Murray, Stephen S. Worrall, Diana M. TI THE FADING OF TWO TRANSIENT ULTRALUMINOUS X-RAY SOURCES TO BELOW THE STELLAR MASS EDDINGTON LIMIT SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: individual (Centaurus A, NGC 5128); X-rays: binaries; X-rays: galaxies; X-rays: individual (1RXH J132519.8-430312, CXOU J132518.2-430304) ID DISC INSTABILITY MODEL; EARLY-TYPE GALAXIES; BLACK-HOLE MASS; CENTAURUS-A; GLOBULAR-CLUSTER; NEARBY GALAXIES; BINARY CANDIDATE; HIGH/SOFT STATE; POINT SOURCES; DWARF NOVAE AB We report new detections of the two transient ultraluminous X-ray sources (ULXs) in NGC 5128 from an ongoing series of Chandra observations. Both sources have previously been observed L-x(2-3)x similar to 10(39) erg s(-1), at the lower end of the ULX luminosity range. The new observations allow us to study these sources in the luminosity regime frequented by the Galactic black hole X-ray binaries (BH XBs). We present the recent lightcurves of both ULXs. 1RXH J132519.8-430312 (ULX1) was observed at L-x approximate to 1 x 10(38) erg s(-1), while CXOU J132518.2-430304 (ULX2) declined to L-x approximate to 2 x 10(37) erg s(-1) and then lingered at this luminosity for hundreds of days. We show that a reasonable upper limit for both duty cycles is 0.2, with a lower limit of 0.12 for ULX2. This duty cycle is larger than anticipated for transient ULXs in old stellar populations. By fitting simple spectral models in an observation with similar to 50 counts we recover properties consistent with Galactic BH XBs, but inconclusive as to the spectral state. We utilize quantile analyses to demonstrate that the spectra are generally soft, and that in one observation the spectrum of ULX2 is inconsistent with a canonical hard state at >95% confidence. This is contrary to what would be expected of an accreting intermediate mass black hole primary, which we would expect to be in the hard state at these luminosities. We discuss the paucity of transient ULXs discovered in early-type galaxies and excogitate explanations. We suggest that the number of transient ULXs scales with the giant and sub-giant populations, rather than the total number of XBs. C1 [Burke, Mark J.; Raychaudhury, Somak] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Burke, Mark J.; Kraft, Ralph P.; Forman, William R.; Jones, Christine; Murray, Stephen S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Soria, Roberto] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Maccarone, Thomas J.] Texas Tech Univ, Astron & Astrophys Grp, Lubbock, TX 79409 USA. [Raychaudhury, Somak] Presidency Univ, Dept Phys, Kolkata 700073, India. [Sivakoff, Gregory R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Birkinshaw, Mark; Worrall, Diana M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Brassington, Nicola J.; Hardcastle, Martin J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Burke, MJ (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. EM mburke@star.sr.bham.ac.uk RI Sivakoff, Gregory/G-9602-2011; OI Sivakoff, Gregory/0000-0001-6682-916X; Forman, William/0000-0002-9478-1682; Hardcastle, Martin/0000-0003-4223-1117 FU NASA [NAS8-03060]; SAO; University of Birmingham; NSERC Discovery Grant FX This work was supported by NASA grant NAS8-03060. M.J.B. thanks SAO and the University of Birmingham for financial support. G.R.S. acknowledges the support of an NSERC Discovery Grant. We also thank Jeanette Gladstone, Chris Done, and Ewan O'Sullivan for useful discussions. We extend our thanks to the anonymous referee for useful comments that improved the paper. NR 64 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2013 VL 775 IS 1 AR 21 DI 10.1088/0004-637X/775/1/21 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220VU UT WOS:000324615800021 ER PT J AU Garcia, J Elhoussieny, EE Bautista, MA Kallman, TR AF Garcia, J. Elhoussieny, E. E. Bautista, M. A. Kallman, T. R. TI TIME-DEPENDENT PHOTOIONIZATION OF GASEOUS NEBULAE: THE PURE HYDROGEN CASE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: nuclei; galaxies: Seyfert; HII regions; methods: numerical; planetary nebulae: general; plasmas; quasars: general ID INTERGALACTIC MEDIUM; INTERSTELLAR-MEDIUM; MODEL ATMOSPHERES; GALAXY FORMATION; IONIZATION; EVOLUTION; RADIATION; EMISSION; FEEDBACK; SPECTRA AB We study the problem of time-dependent photoionization of low density gaseous nebulae subjected to sudden changes in the intensity of ionizing radiation. To this end, we write a computer code that solves the full time-dependent energy balance, ionization balance, and radiation transfer equations in a self-consistent fashion for a simplified pure hydrogen case. It is shown that changes in the ionizing radiation yield ionization/thermal fronts that propagate through the cloud, but the propagation times and response times to such fronts vary widely and nonlinearly from the illuminated face of the cloud to the ionization front (IF). IF/thermal fronts are often supersonic, and in slabs initially in pressure equilibrium such fronts yield large pressure imbalances that are likely to produce important dynamical effects in the cloud. Further, we studied the case of periodic variations in the ionizing flux. It is found that the physical conditions of the plasma have complex behaviors that differ from any steady-state solution. Moreover, even the time average of ionization and temperature is different from any steady-state case. This time average is characterized by overionization and a broader IF with respect to the steady-state solution for a mean value of the radiation flux. Around the time average of physical conditions there is a large dispersion in instantaneous conditions, particularly across the IF, which increases with the period of radiation flux variations. Moreover, the variations in physical conditions are asynchronous along the slab due to the combination of nonlinear propagation times for thermal fronts/IFs and equilibration times. C1 [Garcia, J.; Elhoussieny, E. E.; Bautista, M. A.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Garcia, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM javier@head.cfa.harvard.edu; ehab.elhoussieny@wmich.edu; manuel.bautista@wmich.edu; timothy.r.kallman@nasa.gov NR 40 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2013 VL 775 IS 1 AR 8 DI 10.1088/0004-637X/775/1/8 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220VU UT WOS:000324615800008 ER PT J AU Humphreys, EML Reid, MJ Moran, JM Greenhill, LJ Argon, AL AF Humphreys, E. M. L. Reid, M. J. Moran, J. M. Greenhill, L. J. Argon, A. L. TI TOWARD A NEW GEOMETRIC DISTANCE TO THE ACTIVE GALAXY NGC 4258. III. FINAL RESULTS AND THE HUBBLE CONSTANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; galaxies: individual (NGC 4258); galaxies: nuclei; masers; techniques: interferometric ID KEPLERIAN FLUID DISKS; SPIRAL STRUCTURE; SPACE-TELESCOPE; NGC-4258; MODELS AB We report a new geometric maser distance estimate to the active galaxy NGC 4258. The data for the new model are maser line-of-sight (LOS) velocities and sky positions from 18 epochs of very long baseline interferometry observations, and LOS accelerations measured from a 10 yr monitoring program of the 22 GHz maser emission of NGC 4258. The new model includes both disk warping and confocal elliptical maser orbits with differential precession. The distance to NGC 4258 is 7.60 +/- 0.17 +/- 0.15 Mpc, a 3% uncertainty including formal fitting and systematic terms. The resulting Hubble constant, based on the use of the Cepheid variables in NGC 4258 to recalibrate the Cepheid distance scale, is H-0 = 72.0 +/- 3.0 km s(-1) Mpc(-1). C1 [Humphreys, E. M. L.] European So Observ, D-85748 Garching, Germany. [Humphreys, E. M. L.; Reid, M. J.; Moran, J. M.; Greenhill, L. J.; Argon, A. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Humphreys, EML (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM ehumphre@eso.org OI Moran, James/0000-0002-3882-4414 NR 25 TC 77 Z9 77 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 SEP 20 PY 2013 VL 775 IS 1 AR 13 DI 10.1088/0004-637X/775/1/13 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220VU UT WOS:000324615800013 ER PT J AU Isella, A Perez, LM Carpenter, JM Ricci, L Andrews, S Rosenfeld, K AF Isella, Andrea Perez, Laura M. Carpenter, John M. Ricci, Luca Andrews, Sean Rosenfeld, Katherine TI AN AZIMUTHAL ASYMMETRY IN THE LkH alpha 330 DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE planet-disk interactions; protoplanetary disks; submillimeter: planetary systems; techniques: interferometric ID BAROCLINIC VORTICITY PRODUCTION; ORBITAL COROTATION TORQUE; PLANET-FORMING REGIONS; PROTOPLANETARY DISKS; TRANSITIONAL DISK; CIRCUMSTELLAR DISKS; ACCRETION DISKS; AB AURIGAE; MULTIPLE PLANETS; GIANT PLANETS AB Theory predicts that giant planets and low mass stellar companions shape circumstellar disks by opening annular gaps in the gas and dust spatial distribution. For more than a decade it has been debated whether this is the dominant process that leads to the formation of transitional disks. In this paper, we present millimeter-wave interferometric observations of the transitional disk around the young intermediate mass star LkH alpha 330. These observations reveal a lopsided ring in the 1.3 mm dust thermal emission characterized by a radius of about 100 AU and an azimuthal intensity variation of a factor of two. By comparing the observations with a Gaussian parametric model, we find that the observed asymmetry is consistent with a circular arc, that extends azimuthally by about 90 degrees and emits about 1/3 of the total continuum flux at 1.3 mm. Hydrodynamic simulations show that this structure is similar to the azimuthal asymmetries in the disk surface density that might be produced by the dynamical interaction with unseen low mass companions orbiting within 70AU from the central star. We argue that such asymmetries might lead to azimuthal variations in the millimeter-wave dust opacity and in the dust temperature, which will also affect the millimeter-wave continuum emission. Alternative explanations for the observed asymmetry that do not require the presence of companions cannot be ruled out with the existing data. Further observations of both the dust and molecular gas emission are required to derive firm conclusions on the origin of the asymmetry observed in the LkH alpha 330 disk. C1 [Isella, Andrea; Carpenter, John M.; Ricci, Luca] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Perez, Laura M.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Andrews, Sean; Rosenfeld, Katherine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Isella, A (reprint author), CALTECH, Dept Astron, MC 249-17, Pasadena, CA 91125 USA. EM isella@astro.caltech.edu FU 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; State of Illinois; State Maryland; National Science Foundation [AST-1140063]; CARMA partner universities; Owens Valley Radio Observatory; NSF [AST-1109334] FX We thank the OVRO/CARMA staff and the CARMA observers for their assistance in obtaining the data. 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. We acknowledge support from the Owens Valley Radio Observatory, which is supported by the National Science Foundation through grant AST-1140063. A.I. and J.M.C. acknowledge support from NSF award AST-1109334. We thank Adam Kraus for sharing unpublished results. NR 79 TC 65 Z9 65 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2013 VL 775 IS 1 AR 30 DI 10.1088/0004-637X/775/1/30 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220VU UT WOS:000324615800030 ER PT J AU Koch, PM Tang, YW Ho, PTP AF Koch, Patrick M. Tang, Ya-Wen Ho, Paul T. P. TI INTERPRETING THE ROLE OF THE MAGNETIC FIELD FROM DUST POLARIZATION MAPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (W51 e2, W51 North, Orion BN/KL, G5.89-0.39, M+0.25+0.01, Mon R2, CO+0.02-0.02, M-0.02-0.07); ISM: magnetic fields; polarization; techniques: polarimetric ID MASS STAR-FORMATION; H-II-REGIONS; MOLECULAR CLOUDS; FORMING REGION; INTERSTELLAR GRAINS; DYNAMICAL COLLAPSE; RADIATIVE TORQUES; PROPER MOTIONS; CORES; W51 AB Dust polarization observations from the Submillimeter Array (SMA) and the Caltech Submillimeter Observatory (CSO) are analyzed with the goal of providing a general tool to interpret the role of the magnetic field in molecular clouds. Magnetic field and dust emission gradient orientations are observed to show distinct patterns and features. The angle delta between these two orientations can be interpreted as a magnetic field alignment deviation, assuming the emission gradient orientation to coincide with the density gradient orientation in the magnetohydrodynamics force equation. In SMA high-resolution (collapsing) cores, additional symmetry properties in delta can reveal accretion and outflow zones. All these observational findings suggest the angle delta to be a relevant quantity that can assess the role of the magnetic field. Indeed, when comparing this angle with the (projection-free) magnetic field significance Sigma(B) (introduced by Koch and coworkers in 2012), it is demonstrated that vertical bar delta vertical bar yields an approximation to the change in Sigma(B). Thus, changes in the magnetic field alignment deviation delta trace changes in the role of the magnetic field. The angle delta is observationally straightforward to determine, providing a tool to distinguish between zones of minor or significant magnetic field impact. This is exemplified by the CSO M+0.25+0.01, Mon R2, CO+0.02-0.02, M-0.02-0.07 sources and by the SMA high-resolution data from W51 e2, W51 North, Orion BN/KL and g5.89. Additional CSO sources are analyzed, providing further support of this result. Finally, based on the different features found in our sample of 31 sources in total, covering sizes from large-scale complexes to collapsing cores, a schematic evolutionary scenario is proposed. Here, the significance of the magnetic field evolves both with position and scale, and can be assessed with the angle delta. C1 [Koch, Patrick M.; Tang, Ya-Wen; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Tang, Ya-Wen] Univ Bordeaux, Observ Aquitain Sci Univers, F-33271 Floirac, France. [Tang, Ya-Wen] CNRS, Lab Astrophys Bordeaux, UMR 5804, F-33271 Floirac, France. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Koch, PM (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. EM pmkoch@asiaa.sinica.edu.tw OI Tang, Ya-Wen/0000-0002-0675-276X FU NSC grant [NSC99-2119-M-001-002-MY4] FX The authors acknowledge the referees for very careful and thorough comments that led to further insight in this work. P.T.P.H. is supported by NSC grant NSC99-2119-M-001-002-MY4. NR 69 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 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2013 VL 775 IS 1 AR 77 DI 10.1088/0004-637X/775/1/77 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220VU UT WOS:000324615800077 ER PT J AU Sanchis-Ojeda, R Winn, JN Marcy, GW Howard, AW Isaacson, H Johnson, JA Torres, G Albrecht, S Campante, TL Chaplin, WJ Davies, GR Lund, MN Carter, JA Dawson, RI Buchhave, LA Everett, ME Fischer, DA Geary, JC Gilliland, RL Horch, EP Howell, SB Latham, DW AF Sanchis-Ojeda, Roberto Winn, Joshua N. Marcy, Geoffrey W. Howard, Andrew W. Isaacson, Howard Johnson, John Asher Torres, Guillermo Albrecht, Simon Campante, Tiago L. Chaplin, William J. Davies, Guy R. Lund, Mikkel N. Carter, Joshua A. Dawson, Rebekah I. Buchhave, Lars A. Everett, Mark E. Fischer, Debra A. Geary, John C. Gilliland, Ronald L. Horch, Elliott P. Howell, Steve B. Latham, David W. TI KEPLER-63b: A GIANT PLANET IN A POLAR ORBIT AROUND A YOUNG SUN-LIKE STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: activity; stars: individual (Kepler-63); stars: rotation; starspots ID TRANSITING PLANET; EXOPLANETARY SYSTEM; LIGHT-CURVE; INITIAL CHARACTERISTICS; NEPTUNE HAT-P-11B; STELLAR ROTATION; ERROR-CORRECTION; RADIAL-VELOCITY; HOT JUPITERS; CADENCE DATA AB We present the discovery and characterization of a giant planet orbiting the young Sun-like star Kepler-63 (KOI-63, m(Kp) = 11.6, T-eff = 5576 K, M-star = 0.98 M-circle dot). The planet transits every 9.43 days, with apparent depth variations and brightening anomalies caused by large starspots. The planet's radius is 6.1 +/- 0.2 R-circle plus, based on the transit light curve and the estimated stellar parameters. The planet's mass could not be measured with the existing radial-velocity data, due to the high level of stellar activity, but if we assume a circular orbit, then we can place a rough upper bound of 120M(circle plus) (3 sigma). The host star has a high obliquity (Psi= 104 degrees), based on the Rossiter-McLaughlin effect and an analysis of starspot-crossing events. This result is valuable because almost all previous obliquity measurements are for stars with more massive planets and shorter-period orbits. In addition, the polar orbit of the planet combined with an analysis of spot-crossing events reveals a large and persistent polar starspot. Such spots have previously been inferred using Doppler tomography, and predicted in simulations of magnetic activity of young Sun-like stars. C1 [Sanchis-Ojeda, Roberto; Winn, Joshua N.; Albrecht, Simon] MIT, Dept Phys, Cambridge, MA 02139 USA. [Sanchis-Ojeda, Roberto; Winn, Joshua N.; Albrecht, Simon] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Johnson, John Asher] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Torres, Guillermo; Carter, Joshua A.; Dawson, Rebekah I.; Geary, John C.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Campante, Tiago L.; Chaplin, William J.; Davies, Guy R.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Lund, Mikkel N.] Aarhus Univ, Stellar Astrophys Ctr SAC, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Gilliland, Ronald L.] Penn State Univ, Davey Lab 525, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Horch, Elliott P.] So Connecticut State Univ, New Haven, CT 06515 USA. [Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Sanchis-Ojeda, R (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Davies, Guy/0000-0002-4290-7351; Buchhave, Lars A./0000-0003-1605-5666; Fischer, Debra/0000-0003-2221-0861 FU NASA's Science Mission Directorate; NASA [NAS5-26555, HF-51267.01-A]; NASA Office of Space Science [NNX09AF08G]; NSF-GRFP [DGE-1144152]; Alfred P. Sloan Foundation; David and Lucile Packard Foundation; UK Science and Technology Facilities Council (STFC); Danish National Research Foundation [DNRF106]; ASTERISK project; European Research Council [267864]; NSF [AST-1007992] FX We thank the anonymous referee for numerous insightful suggestions that led to major improvements in this paper. We also thank Andrew Collier Cameron, Bryce Croll, and Benjamin Brown for helpful discussions, and the entire Kepler team for the success of the mission. R.S.O. and J.N.W. acknowledge NASA support through the Kepler Participating Scientist program. Kepler was competitively selected as the tenth Discovery mission. Funding for this mission was provided by NASA's Science Mission Directorate. The data presented in this article were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. J.A.C. acknowledges support by NASA through a Hubble Fellowship (grant HF-51267.01-A). R.I.D. is supported by the NSF-GRFP (DGE-1144152). J.A.J. is supported by generous grants from the Alfred P. Sloan Foundation and the David and Lucile Packard Foundation. T.L.C., W.J.C., and G.R.D. acknowledge the support of the UK Science and Technology Facilities Council (STFC). Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant agreement DNRF106). This research was partly supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement No. 267864). G.T. acknowledges partial support for this work from NSF grant AST-1007992. NR 87 TC 45 Z9 45 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2013 VL 775 IS 1 AR UNSP 54 DI 10.1088/0004-637X/775/1/54 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220VU UT WOS:000324615800054 ER PT J AU Shen, Y Liu, X Loeb, A Tremaine, S AF Shen, Yue Liu, Xin Loeb, Abraham Tremaine, Scott TI CONSTRAINING SUB-PARSEC BINARY SUPERMASSIVE BLACK HOLES IN QUASARS WITH MULTI-EPOCH SPECTROSCOPY. I. THE GENERAL QUASAR POPULATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; line: profiles; quasars: general; surveys ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; BROAD-LINE REGION; PEAKED EMISSION-LINES; TERM PROFILE VARIABILITY; GALAXY MERGERS; SYSTEMATIC SEARCH; ACCRETION DISKS; RADIO GALAXIES; NARROW LINES AB We perform a systematic search for sub-parsec binary supermassive black holes (BHs) in normal broad-line quasars at z < 0.8, using multi-epoch Sloan Digital Sky Survey (SDSS) spectroscopy of the broad H beta line. Our working model is that (1) one and only one of the two BHs in the binary is active; (2) the active BH dynamically dominates its own broad-line region (BLR) in the binary system, so that the mean velocity of the BLR reflects the mean velocity of its host BH; (3) the inactive companion BH is orbiting at a distance of a few R-BLR, where R-BLR similar to 0.01-0.1 pc is the BLR size. We search for the expected line-of-sight acceleration of the broad-line velocity from binary orbital motion by cross-correlating SDSS spectra from two epochs separated by up to several years in the quasar rest frame. Out of similar to 700 pairs of spectra for which we have good measurements of the velocity shift between two epochs (1 sigma error similar to 40 km s(-1)), we detect 28 systems with significant velocity shifts in broad H beta, among which 7 are the best candidates for the hypothesized binaries, 4 are most likely due to broad-line variability in single BHs, and the rest are ambiguous. Continued spectroscopic observations of these candidates will easily strengthen or disprove these claims. We use the distribution of the observed accelerations (mostly non-detections) to place constraints on the abundance of such binary systems among the general quasar population. Excess variance in the velocity shift is inferred for observations separated by longer than 0.4 yr (quasar rest frame). Attributing all the excess to binary motion would imply that most of the quasars in this sample must be in binaries, that the inactive BH must be on average more massive than the active one, and that the binary separation is at most a few times the size of the BLR. However, if this excess variance is partly or largely due to long-term broad-line variability, the requirement of a large population of close binaries is much weakened or even disfavored for massive companions. Future time-domain spectroscopic surveys of normal quasars can provide vital prior information on the structure function of stochastic velocity shifts induced by broad-line variability in single BHs. Such surveys with improved spectral quality, increased time baseline, and more epochs can greatly improve the statistical constraints of this method on the general binary population in broad-line quasars, further shrink the allowed binary parameter space, and detect true sub-parsec binaries. C1 [Shen, Yue] Carnegie Observ, Pasadena, CA 91101 USA. [Liu, Xin] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tremaine, Scott] Inst Adv Study, Princeton, NJ 08540 USA. RP Shen, Y (reprint author), Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. EM yshen@obs.carnegiescience.edu RI Tremaine, Scott/M-4281-2015 OI Tremaine, Scott/0000-0002-0278-7180 FU NASA [HST-HF-51314.01, HST-HF-51307.01, NNA09DB30A, NNX11AF29G]; Space Telescope Science Institute; Association of Universities for Research in Astronomy, Inc., for NASA [NAS 5-26555]; NSF [AST-0907890] FX We thank the anonymous referee and Mike Eracleous for useful comments on the manuscript. Support for the work of Y.S. and X.L. was provided by NASA through Hubble Fellowship grant number HST-HF-51314.01 and HST-HF-51307.01, 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-0907890 and NASA grant NNA09DB30A (A.L.), and NASA grant NNX11AF29G (S.T.) NR 106 TC 25 Z9 25 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2013 VL 775 IS 1 AR 49 DI 10.1088/0004-637X/775/1/49 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220VU UT WOS:000324615800049 ER PT J AU Simionescu, A Werner, N Urban, O Allen, SW Fabian, AC Mantz, A Matsushita, K Nulsen, PEJ Sanders, JS Sasaki, T Sato, T Takei, Y Walker, SA AF Simionescu, A. Werner, N. Urban, O. Allen, S. W. Fabian, A. C. Mantz, A. Matsushita, K. Nulsen, P. E. J. Sanders, J. S. Sasaki, T. Sato, T. Takei, Y. Walker, S. A. TI THERMODYNAMICS OF THE COMA CLUSTER OUTSKIRTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Coma); galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID X-RAY OBSERVATIONS; VIRIAL RADIUS; GALAXY CLUSTERS; XMM-NEWTON; REPRESENTATIVE SAMPLE; INTRACLUSTER MEDIUM; SUZAKU OBSERVATIONS; MAGNETIC-FIELDS; OUTER REGIONS; PKS 0745-191 AB We present results from a large mosaic of Suzaku observations of the Coma Cluster, the nearest and X-ray brightest hot (similar to 8 keV), dynamically active, non-cool core system, focusing on the thermodynamic properties of the intracluster medium on large scales. For azimuths not aligned with an infalling subcluster toward the southwest, our measured temperature and X-ray brightness profiles exhibit broadly consistent radial trends, with the temperature decreasing from about 8.5 keV at the cluster center to about 2 keV at a radius of 2 Mpc, which is the edge of our detection limit. The southwest merger significantly boosts the surface brightness, allowing us to detect X-ray emission out to similar to 2.2 Mpc along this direction. Apart from the southwestern infalling subcluster, the surface brightness profiles show multiple edges around radii of 30-40 arcmin. The azimuthally averaged temperature profile, as well as the deprojected density and pressure profiles, all show a sharp drop consistent with an outwardly-propagating shock front located at 40 arcmin, corresponding to the outermost edge of the giant radio halo observed at 352 MHz with the Westerbork Synthesis Radio Telescope. The shock front may be powering this radio emission. A clear entropy excess inside of r(500) reflects the violent merging events linked with these morphological features. Beyond r(500), the entropy profiles of the Coma Cluster along the relatively relaxed directions are consistent with the power-law behavior expected from simple models of gravitational large-scale structure formation. The pressure is also in agreement at these radii with the expected values measured from Sunyaev-Zel'dovich data from the Planck satellite. However, due to the large uncertainties associated with the Coma Cluster measurements, we cannot yet exclude an entropy flattening in this system consistent with that seen in more relaxed cool core clusters. C1 [Simionescu, A.; Werner, N.; Urban, O.; Allen, S. W.] Stanford Univ, KIPAC, Stanford, CA 94305 USA. [Simionescu, A.; Werner, N.; Urban, O.; Allen, S. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Simionescu, A.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Urban, O.; Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Fabian, A. C.; Sanders, J. S.; Walker, S. A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Mantz, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Mantz, A.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Matsushita, K.; Sasaki, T.; Sato, T.] Tokyo Univ Sci, Dept Phys, Shinjuku Ku, Tokyo 1628601, Japan. [Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sanders, J. S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Simionescu, A (reprint author), Stanford Univ, KIPAC, 452 Lomita Mall, Stanford, CA 94305 USA. RI XRAY, SUZAKU/A-1808-2009; OI Sanders, Jeremy/0000-0003-2189-4501; Nulsen, Paul/0000-0003-0297-4493 FU NASA [PF9-00070, NAS8-03060]; Chandra X-ray Center; U.S. Department of Energy [DE-AC02-76SF00515]; JAXA; [GO2-13145X]; [NNX12AE05G] FX We thank our referee, P. Mazzotta, for his constructive comments and L. Rudnick for providing the 352 MHz WSRT map. Support for this work was provided by NASA through Einstein Postdoctoral Fellowship grant number PF9-00070 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. We further acknowledge support from awards GO2-13145X and NNX12AE05G. The work was supported in part by the U.S. Department of Energy under contract number DE-AC02-76SF00515. The authors thank the Suzaku operation team and Guest Observer Facility, supported by JAXA and NASA. NR 52 TC 28 Z9 28 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 SEP 20 PY 2013 VL 775 IS 1 AR 4 DI 10.1088/0004-637X/775/1/4 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220VU UT WOS:000324615800004 ER PT J AU Simon, JB Bai, XN Armitage, PJ Stone, JM Beckwith, K AF Simon, Jacob B. Bai, Xue-Ning Armitage, Philip J. Stone, James M. Beckwith, Kris TI TURBULENCE IN THE OUTER REGIONS OF PROTOPLANETARY DISKS. II. STRONG ACCRETION DRIVEN BY A VERTICAL MAGNETIC FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; magnetohydrodynamics (MHD); protoplanetary disks; turbulence ID ANGULAR-MOMENTUM TRANSPORT; UNSPLIT GODUNOV METHOD; T TAURI STARS; MAGNETOROTATIONAL-INSTABILITY; CONSTRAINED TRANSPORT; AMBIPOLAR DIFFUSION; PROTOSTELLAR DISKS; FAR-ULTRAVIOLET; RIEMANN SOLVER; IDEAL MHD AB We carry out a series of local, vertically stratified shearing box simulations of protoplanetary disks that include ambipolar diffusion and a net vertical magnetic field. The ambipolar diffusion profiles we employ correspond to 30 AU and 100 AU in a minimum mass solar nebula (MMSN) disk model, which consists of a far-ultraviolet-ionized surface layer and low-ionization disk interior. These simulations serve as a follow-up to Simon et al., in which we found that without a net vertical field, the turbulent stresses that result from the magnetorotational instability (MRI) are too weak to account for observed accretion rates. The simulations in this work show a very strong dependence of the accretion stresses on the strength of the background vertical field; as the field strength increases, the stress amplitude increases. For a net vertical field strength (quantified by beta(0), the ratio of gas to magnetic pressure at the disk mid-plane) of beta(0) = 10(4) and beta(0) = 10(5), we find accretion rates M similar to 10(-8)-10(-7) M-circle dot yr(-1). These accretion rates agree with observational constraints, suggesting a vertical magnetic field strength of similar to 60-200 mu G and 10-30 mu G at 30 AU and 100 AU, respectively, in a MMSN disk. Furthermore, the stress has a non-negligible component due to a magnetic wind. For sufficiently strong vertical field strengths, MRI turbulence is quenched, and the flow becomes largely laminar, with accretion proceeding through large-scale correlations in the radial and toroidal field components as well as through the magnetic wind. In all simulations, the presence of a low-ionization region near the disk mid-plane, which we call the ambipolar damping zone, results in reduced stresses there. C1 [Simon, Jacob B.; Armitage, Philip J.; Beckwith, Kris] Univ Colorado, JILA, Boulder, CO 80309 USA. [Simon, Jacob B.; Armitage, Philip J.; Beckwith, Kris] NIST, Boulder, CO 80309 USA. [Bai, Xue-Ning] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Armitage, Philip J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Stone, James M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Beckwith, Kris] Tech X Corp, Boulder, CO 80303 USA. RP Simon, JB (reprint author), Univ Colorado, JILA, 440 UCB, Boulder, CO 80309 USA. EM jbsimon@jila.colorado.edu FU NASA [NNX09AB90G, NNX11AE12G, NNX13AI58G, HST-AR-12814, NAS 5-26555]; HST grant [HST-AR-12814.03-A]; Tech-X Corp., Boulder, CO; National Science Foundation [AST-0908269, CNS-0821794]; Space Telescope Science Institute; NASA through a Hubble Fellowship grant from the Space Telescope Science Institute [HST-HF-51301.01-A]; National Institute for Computational Sciences through XSEDE grant [TG-AST120062]; University of Colorado Boulder FX We thank Andrew Youdin, Sean O'Neill, and Matt Kunz for useful discussions and suggestions regarding this work. J.B.S., P.J.A., and K.B. acknowledge support from NASA through grants NNX09AB90G, NNX11AE12G, and NNX13AI58G. K.B. also acknowledges funding support from HST grant HST-AR-12814.03-A and from Tech-X Corp., Boulder, CO. X.N.B. and J.M.S. acknowledge support from the National Science Foundation through grant AST-0908269. P.J.A. acknowledges support from NASA under grant HST-AR-12814 awarded by the Space Telescope Science Institute. X.N.B. acknowledges support from program number HST-HF-51301.01-A provided by NASA through a Hubble Fellowship grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contact NAS 5-26555. This research was supported by an allocation of advanced computing resources provided by the National Science Foundation. The computations were performed on Kraken and Nautilus at the National Institute for Computational Sciences through XSEDE grant TG-AST120062. This work also utilized the Janus supercomputer, which is supported by the National Science Foundation (award number CNS-0821794) and the University of Colorado Boulder. The Janus supercomputer is a joint effort of the University of Colorado Boulder, the University of Colorado Denver, and the National Center for Atmospheric Research. NR 58 TC 41 Z9 41 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2013 VL 775 IS 1 AR 73 DI 10.1088/0004-637X/775/1/73 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220VU UT WOS:000324615800073 ER PT J AU Zhang, B Reid, MJ Menten, KM Zheng, XW Brunthaler, A Dame, TM Xu, Y AF Zhang, B. Reid, M. J. Menten, K. M. Zheng, X. W. Brunthaler, A. Dame, T. M. Xu, Y. TI PARALLAXES FOR W49N AND G048.60+0.02: DISTANT STAR FORMING REGIONS IN THE PERSEUS SPIRAL ARM SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: fundamental parameters; Galaxy: kinematics and dynamics; masers; stars: formation; techniques: high angular resolution ID BASE-LINE INTERFEROMETRY; MILKY-WAY; TRIGONOMETRIC PARALLAXES; FUNDAMENTAL PARAMETERS; GALACTIC STRUCTURE; VLBI ASTROMETRY; BESSEL SURVEY; KINEMATICS; GALAXY; MOTIONS AB We report trigonometric parallax measurements of 22 GHz H2O masers in two massive star-forming regions from Very Long Baseline Array observations as part of the Bar and Spiral Structure Legacy Survey. The distances of 11.11(-0.69)(+0.79) kpc to W49N (G043.16+0.01) and 10.75(-0.55)(+0.61) kpc to G048.60+0.02 locate them in a distant section of the Perseus arm near the solar circle in the first Galactic quadrant. This allows us to locate accurately the inner portion of the Perseus arm for the first time. Combining the present results with sources measured in the outer portion of the arm in the second and third quadrants yields a global pitch angle of 9 degrees.5 +/- 1 degrees.3 for the Perseus arm. We have found almost no H2O maser sources in the Perseus arm for 50 degrees < l < 80 degrees, suggesting that this approximate to 6 kpc section of the arm has little massive star formation activity. C1 [Zhang, B.; Menten, K. M.; Brunthaler, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Zhang, B.] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Reid, M. J.; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zheng, X. W.] Nanjing Univ, Dept Astron, Nanjing 210093, Jiangsu, Peoples R China. [Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. RP Zhang, B (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. FU National Science Foundation of China [10921063, 11073046, 11073054, 11133008]; Key Laboratory for Radio Astronomy, Chinese Academy of Sciences; ERC Advanced Investigator Grant GLOSTAR [247078] FX The work was supported by the National Science Foundation of China (under grants 10921063, 11073046, 11073054 and 11133008) and the Key Laboratory for Radio Astronomy, Chinese Academy of Sciences. This work was partially funded by the ERC Advanced Investigator Grant GLOSTAR (247078). We are grateful to Dr. James Urquhart for providing the ATLASGAL FITS files. We also acknowledge Dr. John D. Hunter, the creator of the Python matplotlib which was used extensively in our figures. NR 31 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 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2013 VL 775 IS 1 AR 79 DI 10.1088/0004-637X/775/1/79 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 220VU UT WOS:000324615800079 ER PT J AU Alexander, CE Walsh, RW Regnier, S Cirtain, J Winebarger, AR Golub, L Kobayashi, K Platt, S Mitchell, N Korreck, K DePontieu, B DeForest, C Weber, M Title, A Kuzin, S AF Alexander, Caroline E. Walsh, Robert W. Regnier, Stephane Cirtain, Jonathan Winebarger, Amy R. Golub, Leon Kobayashi, Ken Platt, Simon Mitchell, Nick Korreck, Kelly DePontieu, Bart DeForest, Craig Weber, Mark Title, Alan Kuzin, Sergey TI ANTI-PARALLEL EUV FLOWS OBSERVED ALONG ACTIVE REGION FILAMENT THREADS WITH HI-C SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: corona; Sun: filaments, prominences ID SOLAR PROMINENCES; HINODE; ALPHA; LOOPS; MOSS; AIA AB Plasma flows within prominences/filaments have been observed for many years and hold valuable clues concerning the mass and energy balance within these structures. Previous observations of these flows primarily come from Ha and cool extreme-ultraviolet (EUV) lines (e. g., 304 angstrom) where estimates of the size of the prominence threads has been limited by the resolution of the available instrumentation. Evidence of "counter-steaming" flows has previously been inferred from these cool plasma observations, but now, for the first time, these flows have been directly imaged along fundamental filament threads within the million degree corona (at 193 angstrom). In this work, we present observations of an AR filament observed with the High-resolution Coronal Imager (Hi-C) that exhibits anti-parallel flows along adjacent filament threads. Complementary data from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager are presented. The ultra-high spatial and temporal resolution of Hi-C allow the anti-parallel flow velocities to be measured (70-80 km s(-1)) and gives an indication of the resolvable thickness of the individual strands (0 ''.8 +/- 0 ''.1). The temperature of the plasma flows was estimated to be log T (K) = 5.45 +/- 0.10 using Emission Measure loci analysis. We find that SDO/AIA cannot clearly observe these anti-parallel flows or measure their velocity or thread width due to its larger pixel size. We suggest that anti-parallel/counter-streaming flows are likely commonplace within all filaments and are currently not observed in EUV due to current instrument spatial resolution. C1 [Alexander, Caroline E.; Walsh, Robert W.; Regnier, Stephane] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Cirtain, Jonathan; Winebarger, Amy R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Golub, Leon; Korreck, Kelly; Weber, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kobayashi, Ken] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA. [Platt, Simon; Mitchell, Nick] Univ Cent Lancashire, Sch Comp Engn & Phys Sci, Preston PR1 2HE, Lancs, England. [DePontieu, Bart; Title, Alan] Org ADBS, Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA USA. [DeForest, Craig] SW Res Inst, Boulder, CO 80302 USA. [Kuzin, Sergey] Russian Acad Sci, PN Lebedev Phys Inst, Moscow 119991, Russia. RP Alexander, CE (reprint author), Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. RI Regnier, Stephane/H-9107-2012; Platt, Simon/C-6048-2008; Kuzin, Sergey/M-3435-2015; Regnier, Stephane/K-2423-2015 OI Regnier, Stephane/0000-0001-8954-4183; Platt, Simon/0000-0003-4431-8814; Regnier, Stephane/0000-0001-8954-4183 NR 25 TC 18 Z9 18 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 20 PY 2013 VL 775 IS 1 AR L32 DI 10.1088/2041-8205/775/1/L32 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 217ET UT WOS:000324340500032 ER PT J AU Johnson, CI McWilliam, A Rich, RM AF Johnson, Christian I. McWilliam, Andrew Rich, R. Michael TI CHEMICAL ABUNDANCE ANALYSIS OF A NEUTRON-CAPTURE ENHANCED RED GIANT IN THE BULGE PLAUT FIELD SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: abundances; stars: abundances; stars: Population II ID METAL-POOR STARS; LABORATORY TRANSITION-PROBABILITIES; ALPHA ELEMENT ABUNDANCES; MILKY-WAY BULGE; R-PROCESS-RICH; OSCILLATOR-STRENGTHS; EARLY GALAXY; SOLAR ABUNDANCE; GALACTIC BULGE; S-PROCESS AB We present chemical abundances for 27 elements ranging from oxygen to erbium in the metal-poor ([Fe/H] = -1.67) bulge red giant branch star 2MASS 18174532-3353235. The results are based on equivalent width and spectrum synthesis analyses of a high-resolution (R similar to 30,000) spectrum obtained with the Magellan-MIKE spectrograph. While the light (Z less than or similar to 30) element abundance patterns match those of similar metallicity bulge and halo stars, the strongly enhanced heavy element abundances are more similar to "r-II" halo stars (e. g., CS 22892-052) typically found at [Fe/H] less than or similar to -2.5. We find that the heaviest elements (Z >= 56) closely follow the scaled-solar r-process abundance pattern. We do not find evidence supporting significant s-process contributions; however, the intermediate mass elements (e.g., Y and Zr) appear to have been produced through a different process than the heaviest elements. The light and heavy element abundance patterns of 2MASS 18174532-3353235 are in good agreement with the more metal-poor r-process enhanced stars CS 22892-052 and BD + 17 degrees 3248. 2MASS 18174532-3353235 also shares many chemical characteristics with the similar metallicity but comparatively alpha-poor Ursa Minor dwarf galaxy giant COS 82. Interestingly, the Mo and Ru abundances of 2MASS 18174532-3353235 are also strongly enhanced and follow a similar trend recently found to be common in moderately metal-poor main-sequence turn-off halo stars. C1 [Johnson, Christian I.; 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. [McWilliam, Andrew] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. RP Johnson, CI (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, 430 Portola Plaza,Box 951547, Los Angeles, CA 90095 USA. EM cijohnson@astro.ucla.edu; andy@obs.carnegiescience.edu; rmr@astro.ucla.edu FU National Science Foundation [AST-1003201]; NSF [AST-0709479, AST-12112099]; Clay Fellowship FX 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. C.I.J. acknowledges support through the Clay Fellowship administered by the Smithsonian Astrophysical Observatory. NR 48 TC 12 Z9 12 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 20 PY 2013 VL 775 IS 1 AR L27 DI 10.1088/2041-8205/775/1/L27 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 217ET UT WOS:000324340500027 ER PT J AU Rule, E Loeb, A Strelnitski, VS AF Rule, E. Loeb, A. Strelnitski, V. S. TI HIGH-n HYDROGEN RECOMBINATION LINES FROM THE FIRST GALAXIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: formation; HII regions; masers ID ULTRAVIOLET LUMINOSITY; LY-ALPHA; HE-II; REDSHIFT; REIONIZATION; CONSTRAINTS; POPULATION; STARBURST AB We investigate the prospects of blind and targeted searches in the radio domain (10 MHz to 1 THz) for high-n hydrogen recombination lines from the first generation of galaxies, at z less than or similar to 10. The expected optically thin spontaneous alpha-line luminosities are calculated as a function of the absolute AB magnitude of a galaxy at 1500 angstrom. For a blind search, semi-empirical luminosity functions are used to calculate the number of galaxies whose expected flux densities exceed an assumed detectability threshold. Plots of the minimum sky area, within which at least one detectable galaxy is expected at a given observing frequency, in the fiducial instantaneous passband of 10(4) km s(-1), allow us to assess the blind search time necessary for detection by a given facility. We show that the chances for detection are the highest in the millimeter and submillimeter domains, but finding spontaneous emission in a blind search, especially from redshifts z >> 1, is a challenge even with powerful facilities, such as the Actama Large Millimeter/Submillimeter Array and Square Kilometre Array. The probability of success is higher for a targeted search of lines with principal quantum number n similar to 10 in Lyman-break galaxies amplified by gravitational lensing. Detection of more than one hydrogen line in such a galaxy will allow for line identification and a precise determination of the galaxy's redshift. C1 [Rule, E.] Johns Hopkins Univ, Nantucket, MA 02554 USA. [Rule, E.; Strelnitski, V. S.] Maria Mitchell Observ, Nantucket, MA 02554 USA. [Loeb, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rule, E (reprint author), Johns Hopkins Univ, 4 Vestal St, Nantucket, MA 02554 USA. FU NSF REU [AST-0851892]; Nantucket Maria Mitchell Association; NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DBB30A] FX E.R. was a Maria Mitchell Observatory REU intern while working on this project. He gratefully acknowledges the support by the NSF REU grant AST-0851892 and by the Nantucket Maria Mitchell Association. The work was also supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DBB30A (for A.L.). The authors thank the anonymous referee for the careful reading of the Letter and several valuable suggestions. NR 15 TC 1 Z9 1 U1 2 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 20 PY 2013 VL 775 IS 1 AR L17 DI 10.1088/2041-8205/775/1/L17 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 217ET UT WOS:000324340500017 ER PT J AU Strader, J Seth, AC Forbes, DA Fabbiano, G Romanowsky, AJ Brodie, JP Conroy, C Caldwell, N Pota, V Usher, C Arnold, JA AF Strader, Jay Seth, Anil C. Forbes, Duncan A. Fabbiano, Giuseppina Romanowsky, Aaron J. Brodie, Jean P. Conroy, Charlie Caldwell, Nelson Pota, Vincenzo Usher, Christopher Arnold, Jacob A. TI THE DENSEST GALAXY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: dwarf; galaxies: elliptical and lenticular, cD; galaxies: individual (M60); galaxies: kinematics and dynamics; galaxies: star clusters: general ID COMPACT DWARF GALAXIES; INITIAL MASS FUNCTION; CHANDRA MONITORING OBSERVATIONS; VIRGO CLUSTER SURVEY; ACS FORNAX CLUSTER; DIGITAL SKY SURVEY; STAR-CLUSTERS; GLOBULAR-CLUSTERS; FUNDAMENTAL PLANE; STELLAR-SYSTEMS AB We report the discovery of a remarkable ultra-compact dwarf galaxy around the massive Virgo elliptical galaxy NGC 4649 (M60), which we call M60-UCD1. With a dynamical mass of 2.0 x 10(8) M-circle dot but a half-light radius of only similar to 24 pc, M60-UCD1 is more massive than any ultra-compact dwarfs of comparable size, and is arguably the densest galaxy known in the local universe. It has a two-component structure well fit by a sum of Sersic functions, with an elliptical, compact (r(h) = 14 pc; n similar to 3.3) inner component and a round, exponential, extended (r(h) = 49 pc) outer component. Chandra data reveal a variable central X-ray source with L-X similar to 10(38) erg s(-1) that could be an active galactic nucleus associated with a massive black hole or a low-mass X-ray binary. Analysis of optical spectroscopy shows the object to be old (greater than or similar to 10 Gyr) and of solar metallicity, with elevated [Mg/Fe] and strongly enhanced [N/Fe] that indicates light-element self-enrichment; such self-enrichment may be generically present in dense stellar systems. The velocity dispersion (sigma similar to 70 km s(-1)) and resulting dynamical mass-to-light ratio (M/L-V = 4.9 +/- 0.7) are consistent with-but slightly higher than-expectations for an old, metal-rich stellar population with a Kroupa initial mass function. The presence of a massive black hole or a mild increase in low-mass stars or stellar remnants is therefore also consistent with this M/L-V. The stellar density of the galaxy is so high that no dynamical signature of dark matter is expected. However, the properties of M60-UCD1 suggest an origin in the tidal stripping of a nucleated galaxy with M-B similar to -18 to -19. C1 [Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Seth, Anil C.] Univ Utah, Salt Lake City, UT 84112 USA. [Forbes, Duncan A.; Pota, Vincenzo; Usher, Christopher] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Fabbiano, Giuseppina; Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Romanowsky, Aaron J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Romanowsky, Aaron J.; Brodie, Jean P.; Arnold, Jacob A.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Conroy, Charlie] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Strader, J (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM strader@pa.msu.edu OI Usher, Christopher/0000-0002-7383-7106 FU ARC [DP130100388]; NSF [AST-1109878/AST-0909237] FX We thank L. Chomiuk, S. Mieske, and R. Schiavon for useful discussions and an anonymous referee for a helpful report. Based on observations made with the NASA/ESA Hubble Space Telescope and the Hubble Legacy Archive. Data obtained at Keck (Caltech/UC/NASA) and MMT (Arizona/Smithsonian). Products produced by the OIR Telescope Data Center (SAO). Support by ARC grant DP130100388 and NSF grants AST-1109878/AST-0909237. NR 50 TC 33 Z9 33 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 20 PY 2013 VL 775 IS 1 AR L6 DI 10.1088/2041-8205/775/1/L6 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 217ET UT WOS:000324340500006 ER PT J AU Marques, AC Maronna, MM Collins, AG AF Marques, Antonio C. Maronna, Maximiliano M. Collins, Allen G. TI Putting GenBank Data on the Map SO SCIENCE LA English DT Letter C1 [Marques, Antonio C.; Maronna, Maximiliano M.] Univ Sao Paulo, Inst Biosci, BR-05508090 Sao Paulo, Brazil. [Collins, Allen G.] NOAA, Natl Systemat Lab, Natl Marine Fisheries Serv, Washington, DC 20013 USA. [Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Marques, AC (reprint author), Univ Sao Paulo, Inst Biosci, BR-05508090 Sao Paulo, Brazil. EM marques@ib.usp.br RI Marques, Antonio/E-8049-2011; OI Marques, Antonio/0000-0002-2884-0541; Maronna, Maximiliano/0000-0002-2590-639X NR 2 TC 4 Z9 4 U1 0 U2 6 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 20 PY 2013 VL 341 IS 6152 BP 1341 EP 1341 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 220PK UT WOS:000324597200018 PM 24052287 ER PT J AU Schneps, MH Thomson, JM Chen, C Sonnert, G Pomplun, M AF Schneps, Matthew H. Thomson, Jenny M. Chen, Chen Sonnert, Gerhard Pomplun, Marc TI E-Readers Are More Effective than Paper for Some with Dyslexia SO PLOS ONE LA English DT Article ID VISUAL-ATTENTION SPAN; DEVELOPMENTAL DYSLEXIA; EYE-MOVEMENTS; READING-DISABILITY; LETTER RECOGNITION; SACCADIC CONTROL; PERCEPTUAL SPAN; FIXATED WORD; CHILDREN; INFORMATION AB E-readers are fast rivaling print as a dominant method for reading. Because they offer accessibility options that are impossible in print, they are potentially beneficial for those with impairments, such as dyslexia. Yet, little is known about how the use of these devices influences reading in those who struggle. Here, we observe reading comprehension and speed in 103 high school students with dyslexia. Reading on paper was compared with reading on a small handheld e-reader device, formatted to display few words per line. We found that use of the device significantly improved speed and comprehension, when compared with traditional presentations on paper for specific subsets of these individuals: Those who struggled most with phoneme decoding or efficient sight word reading read more rapidly using the device, and those with limited VA Spans gained in comprehension. Prior eye tracking studies demonstrated that short lines facilitate reading in dyslexia, suggesting that it is the use of short lines (and not the device per se) that leads to the observed benefits. We propose that these findings may be understood as a consequence of visual attention deficits, in some with dyslexia, that make it difficult to allocate attention to uncrowded text near fixation, as the gaze advances during reading. Short lines ameliorate this by guiding attention to the uncrowded span. C1 [Schneps, Matthew H.; Chen, Chen; Sonnert, Gerhard] Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, Cambridge, MA 02138 USA. [Thomson, Jenny M.; Chen, Chen] Harvard Univ, Harvard Grad Sch Educ, Cambridge, MA 02138 USA. [Pomplun, Marc] Univ Massachusetts, Dept Comp Sci, Boston, MA 02125 USA. RP Schneps, MH (reprint author), Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, 60 Garden St, Cambridge, MA 02138 USA. EM mschneps@cfa.harvard.edu OI Thomson, Jenny/0000-0002-4293-4851 FU National Science Foundation [HRD-0930962, HRD-1131039]; Youth Access Grant program at the Smithsonian Institution FX This article is based on work supported by the National Science Foundation under Grants No. HRD-0930962 and HRD-1131039, and the Youth Access Grant program at the Smithsonian Institution. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 68 TC 8 Z9 8 U1 3 U2 47 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 SEP 18 PY 2013 VL 8 IS 9 AR e75634 DI 10.1371/journal.pone.0075634 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 221YD UT WOS:000324695900123 PM 24058697 ER PT J AU Balke, M Schmidt, S Hausmann, A Toussaint, EFA Bergsten, J Buffington, M Hauser, CL Kroupa, A Hagedorn, G Riedel, A Polaszek, A Ubaidillah, R Krogmann, L Zwick, A Fikacek, M Hajek, J Michat, MC Dietrich, C La Salle, J Mantle, B Ng, PKL Hobern, D AF Balke, Michael Schmidt, Stefan Hausmann, Axel Toussaint, Emmanuel F. A. Bergsten, Johannes Buffington, Matthew Haeuser, Christoph L. Kroupa, Alexander Hagedorn, Gregor Riedel, Alexander Polaszek, Andrew Ubaidillah, Rosichon Krogmann, Lars Zwick, Andreas Fikacek, Martin Hajek, Jiri Michat, Mariano C. Dietrich, Christopher La Salle, John Mantle, Beth Ng, Peter K. L. Hobern, Donald TI Biodiversity into your hands - A call for a virtual global natural history 'metacollection' SO FRONTIERS IN ZOOLOGY LA English DT Article DE Mass digitization; Natural history collections; Collection access; Metacollection; Cybertaxonomy; Online resources; Robotic imaging; Accessions; DNA extraction vouchers ID COLLECTIONS; DIGITIZATION; TAXONOMY; SCIENCE AB Background: Many scientific disciplines rely on correct taxon delineations and identifications. So does a great part of the general public as well as decision makers. Researchers, students and enthusiastic amateurs often feel frustrated because information about species remains scattered, difficult to access, or difficult to decipher. Together, this affects almost anyone who wishes to identify species or verify identifications. Many remedies have been proposed, but we argue that the role of natural history collections remains insufficiently appreciated. We suggest using state-of-the-art mass imaging technology and to join forces to create a global natural history metacollection on the internet, providing access to the morphology of tens of millions of specimens and making them available for automated digital image analysis. Discussion: Robotic high-resolution imaging technology and fast (high performance) computer-based image stitching make it now feasible to digitize entire collection drawers typically used for arthropod collections, or trays or containers used for other objects. Resolutions of 500 megapixels and much higher are already utilized to capture the contents of 40x50 cm collection drawers, providing amazing detail of specimens. Flanked by metadata entry, this helps to create access to tens of thousands of specimens in days. By setting priorities and combining the holdings of the most comprehensive collections for certain taxa, drawer digitizing offers the unique opportunity to create a global, virtual metacollection. The taxonomic and geographic coverage of such a collection could never be achieved by a single institution or individual. We argue that by joining forces, many new impulses will emerge for systematic biology, related fields and understanding of biodiversity in general. Digitizing drawers containing unidentified, little-curated specimens is a contribution towards the beginning of a new era of online curation. It also will help taxonomists and curators to discover and process the millions of "gems" of undescribed species hidden in museum accessions. Summary: Our proposal suggests creating virtual, high-resolution image resources that will, for the first time in history, provide access for expert scientists as well as students and the general public to the enormous wealth of the world's natural history collections. We foresee that this will contribute to a better understanding, appreciation and increased use of biodiversity resources and the natural history collections serving this cause. C1 [Balke, Michael; Schmidt, Stefan; Hausmann, Axel; Toussaint, Emmanuel F. A.] Zool Staatssammlung, D-81247 Munich, Germany. [Balke, Michael; Toussaint, Emmanuel F. A.] Univ Munich, GeoBio Ctr, Munich, Germany. [Bergsten, Johannes] Swedish Museum Nat Hist, SE-10405 Stockholm, Sweden. [Buffington, Matthew] Smithsonian Inst, Systemat Entomol Lab, USDA ARS, NMNH, Washington, DC 20560 USA. [Haeuser, Christoph L.; Kroupa, Alexander; Hagedorn, Gregor] Museum Nat Kunde, D-10115 Berlin, Germany. [Riedel, Alexander] Staatliches Museum Nat Kunde Karlsruhe, D-76133 Karlsruhe, Germany. [Polaszek, Andrew] Nat Hist Museum, London SW7 5BD, England. [Ubaidillah, Rosichon] Museum Zool Bogoriense, LIPI Div Zool, Cibinong, West Java, Indonesia. [Krogmann, Lars; Zwick, Andreas] Staatliches Museum Nat Kunde Stuttgart, D-70191 Stuttgart, Germany. [Fikacek, Martin; Hajek, Jiri] Natl Museum, Dept Entomol, Prague 14800 4, Czech Republic. [Michat, Mariano C.] Univ Buenos Aires, Dept Biodiversidad & Biol Expt, CONICET, Entomol Lab, Buenos Aires, DF, Argentina. [Dietrich, Christopher] Univ Illinois, Illinois Nat Hist Survey, Champaign, IL 61801 USA. [La Salle, John] CSIRO Ecosyst Sci, Atlas Living Australia, Canberra, ACT 2601, Australia. [Mantle, Beth] CSIRO Ecosyst Sci, Australian Natl Insect Collect, Canberra, ACT 2601, Australia. [Ng, Peter K. L.] Natl Univ Singapore, Singapore 117543, Singapore. [Ng, Peter K. L.] Natl Univ Singapore, Dept Biol Sci, Raffles Museum Biodivers Res, Singapore 117543, Singapore. [Hobern, Donald] GBIF Secretariat, DK-2100 Copenhagen, Denmark. RP Balke, M (reprint author), Zool Staatssammlung, Munchhausenstr 21, D-81247 Munich, Germany. EM Coleoptera-ZSM@zsm.mwn.de RI Mantle, Beth/B-2524-2009; La Salle, John/B-9544-2008; Zwick, Andreas/A-5735-2015; Dietrich, Christopher/A-9169-2016 OI Mantle, Beth/0000-0001-5413-0159; La Salle, John/0000-0002-8816-9569; Hobern, Donald/0000-0001-6492-4016; Dietrich, Christopher/0000-0003-4005-4305 FU European Union; 4D4Life [238988]; pro-iBiosphere [312848]; EFRE EoS project at MFN Berlin FX This project was made possible with the help of BMBF GBIF grant 01LI1001B. Support was also granted by the European Union's 7th Framework Programme (FP7/2007-2013) with the projects 4D4Life (grant agreement No238988) and pro-iBiosphere (grant agreement No312848) and by the EFRE EoS project at MFN Berlin. We thank Dr John Ascher (National University of Singapore) for many helpful comments which improved this manuscript considerably, and Vojtech Novotny for his encouragement. NR 24 TC 8 Z9 9 U1 3 U2 47 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1742-9994 J9 FRONT ZOOL JI Front. Zool. PD SEP 17 PY 2013 VL 10 AR UNSP 55 DI 10.1186/1742-9994-10-55 PG 9 WC Zoology SC Zoology GA 223HD UT WOS:000324794400001 PM 24044698 ER PT J AU Wen, J Xiong, ZQ Nie, ZL Mao, LK Zhu, YB Kan, XZ Ickert-Bond, SM Gerrath, J Zimmer, EA Fang, XD AF Wen, Jun Xiong, Zhiqiang Nie, Ze-Long Mao, Likai Zhu, Yabing Kan, Xian-Zhao Ickert-Bond, Stefanie M. Gerrath, Jean Zimmer, Elizabeth A. Fang, Xiao-Dong TI Transcriptome Sequences Resolve Deep Relationships of the Grape Family SO PLOS ONE LA English DT Article ID DISPERSAL-VICARIANCE ANALYSIS; NUCLEAR GENE DATA; RNA-SEQ DATA; PHYLOGENETIC ANALYSIS; MOLECULAR PHYLOGENY; MAXIMUM-LIKELIHOOD; ANGIOSPERM DIVERSIFICATION; PARTHENOCISSUS VITACEAE; SEED MORPHOLOGY; EVOLUTION AB Previous phylogenetic studies of the grape family (Vitaceae) yielded poorly resolved deep relationships, thus impeding our understanding of the evolution of the family. Next-generation sequencing now offers access to protein coding sequences very easily, quickly and cost-effectively. To improve upon earlier work, we extracted 417 orthologous single-copy nuclear genes from the transcriptomes of 15 species of the Vitaceae, covering its phylogenetic diversity. The resulting transcriptome phylogeny provides robust support for the deep relationships, showing the phylogenetic utility of transcriptome data for plants over a time scale at least since the mid-Cretaceous. The pros and cons of transcriptome data for phylogenetic inference in plants are also evaluated. C1 [Wen, Jun; Zimmer, Elizabeth A.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC166, Washington, DC 20560 USA. [Xiong, Zhiqiang; Mao, Likai; Zhu, Yabing; Fang, Xiao-Dong] BGI Shenzhen, Shenzhen, Peoples R China. [Nie, Ze-Long] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming, Yunnan, Peoples R China. [Kan, Xian-Zhao] Anhui Normal Univ, Coll Life Sci, Wuhu, Anhui, Peoples R China. [Ickert-Bond, Stefanie M.] Univ Alaska Fairbanks, UA Museum North Herbarium, Fairbanks, AK USA. [Ickert-Bond, Stefanie M.] Univ Alaska Fairbanks, Dept Biol & Wildlife, Fairbanks, AK USA. [Gerrath, Jean] Univ No Iowa, Dept Biol, Cedar Falls, IA 50614 USA. RP Wen, J (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC166, Washington, DC 20560 USA. EM wenj@si.edu; fangxd@genomics.org.cn RI Nie, Ze-Long/N-8471-2015; Ickert-Bond, Stefanie/B-3216-2012 OI Nie, Ze-Long/0000-0001-8065-3981; Ickert-Bond, Stefanie/0000-0001-8198-8898 FU Office of the Smithsonian Undersecretary of Science; US National Science Foundation [DEB 0743474, DEB 0743499]; National Museum of Natural History of the Smithsonian Institution; trust funds FX This study was funded by grants from the Office of the Smithsonian Undersecretary of Science, the US National Science Foundation (grant DEB 0743474 to S. R. Manchester and J. Wen, and grant DEB 0743499 to J. Gerrath), the Small Grants Program of the National Museum of Natural History of the Smithsonian Institution to JW, and trust funds generated by EAZ. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 59 TC 30 Z9 32 U1 1 U2 51 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 SEP 17 PY 2013 VL 8 IS 9 AR e74394 DI 10.1371/journal.pone.0074394 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 219YJ UT WOS:000324547300039 PM 24069307 ER PT J AU Higginbotham, SJ Arnold, AE Ibanez, A Spadafora, C Coley, PD Kursar, TA AF Higginbotham, Sarah J. Arnold, A. Elizabeth Ibanez, Alicia Spadafora, Carmenza Coley, Phyllis D. Kursar, Thomas A. TI Bioactivity of Fungal Endophytes as a Function of Endophyte Taxonomy and the Taxonomy and Distribution of Their Host Plants SO PLOS ONE LA English DT Article ID NATURAL-PRODUCTS; TRYPANOSOMA-CRUZI; DRUG DISCOVERY; PLASMODIUM-FALCIPARUM; TROPICAL FOREST; METABOLITES; DIVERSITY; PANAMA; COLONIZATION; CONSERVATION AB Fungal endophytes - fungi that grow within plant tissues without causing immediate signs of disease - are abundant and diverse producers of bioactive secondary metabolites. Endophytes associated with leaves of tropical plants are an especially exciting and relatively untapped source of novel compounds. However, one major challenge in drug discovery lies in developing strategies to efficiently recover highly bioactive strains. As part of a 15-year drug discovery project, foliar endophytes were isolated from 3198 plant samples (51 orders, 105 families and at least 232 genera of angiosperms and ferns) collected in nine geographically distinct regions of Panama. Extracts from culture supernatants of >2700 isolates were tested for bioactivity (in vitro percent inhibition of growth, % IG) against a human breast cancer cell line (MCF-7) and the causative agents of malaria, leishmaniasis, and Chagas' disease. Overall, 32.7% of endophyte isolates were highly active in at least one bioassay, including representatives of diverse fungal lineages, host lineages, and collection sites. Up to 17% of isolates tested per assay were highly active. Most bioactive strains were active in only one assay. Fungal lineages differed in the incidence and degree of bioactivity, as did fungi from particular plant taxa, and greater bioactivity was observed in endophytes isolated from plants in cloud forests vs. lowland forests. Our results suggest that using host taxonomy and forest type to tailor plant collections, and selecting endophytes from specific orders or families for cultivation, will markedly increase the efficiency and efficacy of discovering bioactive metabolites for particular pharmaceutical targets. C1 [Higginbotham, Sarah J.; Ibanez, Alicia; Coley, Phyllis D.; Kursar, Thomas A.] Smithsonian Trop Res Inst, Panama City, Panama. [Arnold, A. Elizabeth] Univ Arizona, Sch Plant Sci, Tucson, AZ USA. [Coley, Phyllis D.; Kursar, Thomas A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Spadafora, Carmenza] Inst Invest Cient & Serv Alta Tecnol, Panama City, Panama. RP Higginbotham, SJ (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM higginbothams@si.edu RI Trilety, Roman/I-8225-2014; OI Trilety, Roman/0000-0002-3778-0368; Spadafora, Carmenza/0000-0002-3002-9467 FU International Cooperative Biodiversity Groups program [2 U01 TW006634-06]; College of Agriculture and Life Sciences at the University of Arizona FX This work was supported by the International Cooperative Biodiversity Groups program (ICBG-Panama http://www.icbg.org/, grant number 2 U01 TW006634-06) and the College of Agriculture and Life Sciences at the University of Arizona. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 60 TC 26 Z9 26 U1 1 U2 71 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 SEP 16 PY 2013 VL 8 IS 9 AR e73192 DI 10.1371/journal.pone.0073192 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 219GJ UT WOS:000324494000018 PM 24066037 ER PT J AU Yager, J AF Yager, Jill TI Speleonectes cokei, new species of Remipedia (Crustacea: Speleonectidae) from a submerged ocean cave near Caye Chapel, Belize SO ZOOTAXA LA English DT Article DE remipede; Speleonectes; Belize; seafloor cave; anchialine cave ID ANCHIALINE; BAHAMAS; ISLAND AB Speleonectes cokei n. sp. is the 15th species of Speleonectes to be described. It is the first remipede described from a submerged cave off the mainland of Belize. The species is the third found along the Caribbean coast of the Yucatan Peninsula. S. cokei can be distinguished from S. tulumensis Yager, 1987 and S. fuchscockburni Neiber et al., 2012 by the number of antenna 1 segments, number of antenna 2 exopod setae, spines on maxilla 1 segment 2, and caudal rami to anal segment length. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Yager, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM jill.yager@gmail.com NR 5 TC 2 Z9 2 U1 0 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 SEP 16 PY 2013 VL 3710 IS 4 BP 354 EP 362 PG 9 WC Zoology SC Zoology GA 217YB UT WOS:000324397900004 PM 26106696 ER PT J AU D'Apolito, C Absy, ML Latrubesse, EM AF D'Apolito, Carlos Absy, Maria Lucia Latrubesse, Edgardo M. TI The Hill of Six Lakes revisited: new data and re-evaluation of a key Pleistocene Amazon site SO QUATERNARY SCIENCE REVIEWS LA English DT Article DE Amazonia; Palaeoecology; Ice age; Pollen ID QUATERNARY ENVIRONMENTAL-CHANGES; NEOTROPICAL RAIN-FOREST; POLLEN RECORD; TROPICAL FORESTS; LOWLAND AMAZONIA; AEOLIAN ACTIVITY; PLANT DIVERSITY; CLIMATE-CHANGE; TIME-SCALES; RIO-NEGRO AB The new analyses of a sedimentary record of Lake Pata in the Hill of Six Lakes, in NW Amazon and its correlation with other Quaternary proxy records in the region provide new insights regarding the vegetation and climate of the lowland forest during the Last Glacial. Despite what has been reported previously in the literature, the sedimentary and pollen records are not continuous. The hill remained forested; however, clear signals of structural change are seen in the record, which indicate that the area experienced a significantly drier climate during the Last Glacial Maximum (LGM). The herbs and taxa that are known to be more dominant in seasonally dry forests were all more abundant during the glacial part of the record, and the cool-adapted elements were mixed with warm lowland elements, which indicates a temperature depression. A comparison of the palaeoecological data with other regional geoenvironmental records of the Upper Negro River basin and other areas of the Amazon provides additional support for a cooler and more seasonal environment during the middle Pleniglacial, which then became drier during the LGM. A "wet" LGM is strongly refuted; therefore, the palaeoclimatic and ecological models that used the previous proxy data from Six Lakes to sustain "wet" conditions and a "continuous forest record" during the LGM to reconstruct the palaeoenvironmental conditions in the Amazon should be reviewed. (c) 2013 Elsevier Ltd. All rights reserved. C1 [D'Apolito, Carlos; Absy, Maria Lucia] INPA, BR-69067375 Manaus, Amazonas, Brazil. [D'Apolito, Carlos] Smithsonian Trop Res Inst, Ancon, Panama. [Latrubesse, Edgardo M.] Univ Texas Austin, Dept Geog & Environm, Austin, TX 78712 USA. RP D'Apolito, C (reprint author), Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England. EM carlosdapolito@gmail.com FU CNPq [575747/2008-0-CT-Amazonia, 477127/2011-8] FX This work is dedicated to the memories of Thomas Van Der Hammen and Antonio Rossi. We would like to express our sincere thanks to Elena Franzineli, who kindly provided the sediment samples. We are much indebted to Henry Hooghiemstra, Francis Mayle and journal editor Neil Roberts for their valuable critical reviews. We thank also an anonymous reviewer and Blanca de Leon for reviewing an earlier version of the manuscript. Mario Terra Araujo is also thanked for kindly permitting access to botanical collections of the Six Lakes Hill, Maria de Nazare C. Bastos and Antonio Elielson Sousa da Rocha for herbarium information and Bruce W. Nelson for collecting the moss sample at the hill. This work was supported by CNPq (processes 575747/2008-0-CT-Amazonia and 477127/2011-8) and by a scholarship awarded to Carlos D'Apolito. All administrative duties were facilitated by the Botany Department at the National Institute for Amazon Research (INPA), in Manaus. NR 78 TC 15 Z9 15 U1 2 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0277-3791 J9 QUATERNARY SCI REV JI Quat. Sci. Rev. PD SEP 15 PY 2013 VL 76 BP 140 EP 155 DI 10.1016/j.quascirev.2013.07.013 PG 16 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 218RD UT WOS:000324449200012 ER PT J AU Berger, E Fong, W Chornock, R AF Berger, E. Fong, W. Chornock, R. TI AN r-PROCESS KILONOVA ASSOCIATED WITH THE SHORT-HARD GRB 130603B SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual (130603B) ID GAMMA-RAY BURST; NEUTRON-STAR MERGERS; HOST GALAXY; OPTICAL AFTERGLOW; SUPERNOVA; NUCLEOSYNTHESIS; CONSTRAINTS; PROGENITOR; EMISSION; OFFSETS AB We present ground-based optical and Hubble Space Telescope (HST) optical and near-IR observations of the short-hard GRB 130603B at z = 0.356, which demonstrate the presence of excess near-IR emission matching the expected brightness and color of an r-process powered transient (a "kilonova"). The early afterglow fades rapidly with alpha <= -2.6 at t approximate to 8-32 hr post-burst and has a spectral index of beta approximate to -1.5 (F-nu proportional to t(alpha)nu(beta)), leading to an expected near-IR brightness at the time of the first HST observation of m(F160W) (t = 9.4 days) >= 29.3 AB mag. Instead, the detected source has m(F160W) = 25.8 +/- 0.2 AB mag, corresponding to a rest-frame absolute magnitude of M-J approximate to -15.2mag. The upper limit in the HST optical observations is m(F606W) >= 27.7 AB mag (3 sigma), indicating an unusually red color of V - H >= 1.9mag. Comparing the observed near-IR luminosity to theoretical models of kilonovae produced by ejecta from the merger of an NS-NS or NS-BH binary, we infer an ejecta mass of M-ej approximate to 0.03-0.08 M-circle dot for v(ej) approximate to 0.1-0.3c. The inferred mass matches the expectations from numerical merger simulations. The presence of a kilonova provides the strongest evidence to date that short GRBs are produced by compact object mergers, and provides initial insight on the ejected mass and the primary role that compact object merger may play in the r-process. Equally important, it demonstrates that gravitational wave sources detected by Advanced LIGO/Virgo will be accompanied by optical/near-IR counterparts with unusually red colors, detectable by existing and upcoming large wide-field facilities (e.g., Pan-STARRS, DECam, Subaru, LSST). C1 [Berger, E.; Fong, W.; Chornock, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Berger, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Science Foundation [AST-1107973]; NASA [NAS 5-26555]; [13497] FX We thank Ryan Foley and Paul Harding for obtaining the Magellan observations, and Dan Kasen for sharing his kilonova models. The Berger GRB group at Harvard is supported by the National Science Foundation under Grant AST-1107973. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program 13497. This Letter includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. NR 49 TC 141 Z9 142 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 10 PY 2013 VL 774 IS 2 AR L23 DI 10.1088/2041-8205/774/2/L23 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 216TR UT WOS:000324307900008 ER PT J AU Lingafelter, SW Nearns, EH AF Lingafelter, Steven W. Nearns, Eugenio H. TI Elucidating Article 45.6 of the International Code of Zoological Nomenclature: A dichotomous key for the determination of subspecific or infrasubspecific rank SO ZOOTAXA LA English DT Article DE available name; binomen; ICZN; subspecies; trinomen AB We present an overview of the difficulties sometimes encountered when determining whether a published name following a binomen is available or infrasubspecific and unavailable, following Article 45.6 of the International Code of Zoological Nomenclature (ICZN, 1999). We propose a dichotomous key that facilitates this determination and as a preferable method, given the convoluted and subordinate discussion, exceptions, and qualifications laid out in ICZN (1999: 49-50). Examples and citations are provided for each case one can encounter while making this assessment of availability status of names following the binomen. C1 [Lingafelter, Steven W.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist, Washington, DC 20013 USA. [Nearns, Eugenio H.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Lingafelter, SW (reprint author), ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist, MRC 168,POB 37012, Washington, DC 20013 USA. EM steve.lingafelter@ars.usda.gov; gino@nearns.com NR 9 TC 2 Z9 4 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 J9 ZOOTAXA JI Zootaxa PD SEP 10 PY 2013 VL 3709 IS 6 BP 597 EP 600 PG 4 WC Zoology SC Zoology GA 212YX UT WOS:000324020300009 PM 26240934 ER PT J AU Basu-Zych, AR Lehmer, BD Hornschemeier, AE Goncalves, TS Fragos, T Heckman, TM Overzier, RA Ptak, AF Schiminovich, D AF Basu-Zych, Antara R. Lehmer, Bret D. Hornschemeier, Ann E. Goncalves, Thiago S. Fragos, Tassos Heckman, Timothy M. Overzier, Roderik A. Ptak, Andrew F. Schiminovich, David TI EVIDENCE FOR ELEVATED X-RAY EMISSION IN LOCAL LYMAN BREAK GALAXY ANALOGS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: starburst; X-rays: binaries ID STAR-FORMING GALAXIES; ULTRAVIOLET-LUMINOUS GALAXIES; MASS-METALLICITY RELATION; ACTIVE GALACTIC NUCLEI; FORMATION RATE INDICATOR; DIGITAL SKY SURVEY; FIELD-NORTH SURVEY; METAL-POOR STARS; DEEP FIELD; STELLAR MASS AB Our knowledge of how X-ray emission scales with star formation at the earliest times in the universe relies on studies of very distant Lyman break galaxies (LBGs). In this paper, we study the relationship between the 2-10 keV X-ray luminosity (L-X), assumed to originate from X-ray binaries (XRBs), and star formation rate (SFR) in ultraviolet (UV) selected z < 0.1 Lyman break analogs (LBAs). We present Chandra observations for four new Galaxy Evolution Explorer selected LBAs. Including previously studied LBAs, Haro 11 and VV 114, we find that LBAs demonstrate L-X/SFR ratios that are elevated by similar to 1.5 sigma compared to local galaxies, similar to the ratios found for stacked LBGs in the early universe (z > 2). Unlike some of the composite LBAs studied previously, we show that these LBAs are unlikely to harbor active galactic nuclei, based on their optical and X-ray spectra and the spatial distribution of the X-rays in three spatially extended cases. Instead, we expect that high-mass X-ray binaries (HMXBs) dominate the X-ray emission in these galaxies, based on their high specific SFRs (sSFRs SFR/M-star >= 10(-9) yr(-1)), which suggest the prevalence of young stellar populations. Since both UV-selected populations (LBGs and LBAs) have lower dust attenuations and metallicities compared to similar samples of more typical local galaxies, we investigate the effects of dust extinction and metallicity on the L-X/SFR for the broader population of galaxies with high sSFRs (>10(-10) yr(-1)). The estimated dust extinctions (corresponding to column densities of N-H < 10(22) cm(-2)) are expected to have insignificant effects on observed L-X/SFR ratio for the majority of galaxy samples. We find that the observed relationship between L-X/SFR and metallicity appears consistent with theoretical expectations from XRB population synthesis models. Therefore, we conclude that lower metallicities, related to more luminous HMXBs such as ultraluminous X-ray sources, drive the elevated L-X/SFR observed in our sample of z < 0.1 LBAs. The relatively metal-poor, active mode of star formation in LBAs and distant z > 2 LBGs may yield higher total HMXB luminosity than found in typical galaxies in the local universe. C1 [Basu-Zych, Antara R.; Lehmer, Bret D.; Hornschemeier, Ann E.; Ptak, Andrew F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lehmer, Bret D.; Hornschemeier, Ann E.; Heckman, Timothy M.; Ptak, Andrew F.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Goncalves, Thiago S.] Univ Fed Rio de Janeiro, Observ Valongo, BR-22240060 Rio De Janeiro, RJ, Brazil. [Fragos, Tassos] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Overzier, Roderik A.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Overzier, Roderik A.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA. RP Basu-Zych, AR (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM antara.r.basu-zych@nasa.gov RI Fragos, Tassos/A-3581-2016 OI Fragos, Tassos/0000-0003-1474-1523 FU Chandra Cycle 12 program [12620841]; CfA; ITC prize fellowship programs; National Aeronautics and Space Administration FX This research was supported by Chandra Cycle 12 program No. 12620841 (PI: Basu-Zych). We thank our anonymous referee for helpful suggestions, A. Prestwich for sharing her work on ULXs in extremely low metallicity galaxies, S. Mineo for providing useful comparison data, and J. Mullaney for sharing his IR code. The author gratefully acknowledges B. D. Johnson, A. Henry, and V. Antoniou for helpful discussions. T.F. acknowledges support from CfA and ITC prize fellowship programs. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 100 TC 24 Z9 24 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2013 VL 774 IS 2 AR 152 DI 10.1088/0004-637X/774/2/152 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 211EW UT WOS:000323888900061 ER PT J AU Deck, KM Payne, M Holman, MJ AF Deck, Katherine M. Payne, Matthew Holman, Matthew J. TI FIRST-ORDER RESONANCE OVERLAP AND THE STABILITY OF CLOSE TWO-PLANET SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; chaos; planets and satellites: dynamical evolution and stability ID GENERAL 3-BODY PROBLEM; N-BODY PROBLEM; PLANETARY SYSTEMS; OSCILLATOR SYSTEMS; DYNAMICAL CHAOS; SYMPLECTIC MAPS; SOLAR-SYSTEM; INSTABILITY; BEHAVIOR; LIMITS AB Motivated by the population of observed multi-planet systems with orbital period ratios 1 < P-2/P-1 less than or similar to 2, we study the long-term stability of packed two-planet systems. The Hamiltonian for two massive planets on nearly circular and nearly coplanar orbits near a first-order mean motion resonance can be reduced to a one-degree-of-freedom problem. Using this analytically tractable Hamiltonian, we apply the resonance overlap criterion to predict the onset of large-scale chaotic motion in close two-planet systems. The reduced Hamiltonian has only a weak dependence on the planetary mass ratio m(1)/m(2), and hence the overlap criterion is independent of the planetary mass ratio at lowest order. Numerical integrations confirm that the planetary mass ratio has little effect on the structure of the chaotic phase space for close orbits in the low-eccentricity (e less than or similar to 0.1) regime. We show numerically that orbits in the chaotic web produced primarily by first-order resonance overlap eventually experience large-scale erratic variation in semimajor axes and are therefore Lagrange unstable. This is also true of the orbits in this overlap region which satisfy the Hill criterion. As a result, we can use the first-order resonance overlap criterion as an effective stability criterion for pairs of observed planets. We show that for low-mass (less than or similar to 10 M-circle plus) planetary systems with initially circular orbits the period ratio at which complete overlap occurs and widespread chaos results lies in a region of parameter space which is Hill stable. Our work indicates that a resonance overlap criterion which would apply for initially eccentric orbits likely needs to take into account second-order resonances. Finally, we address the connection found in previous work between the Hill stability criterion and numerically determined Lagrange instability boundaries in the context of resonance overlap. C1 [Deck, Katherine M.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Deck, Katherine M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Payne, Matthew; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Deck, KM (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM kdeck@mit.edu FU NSF; NASA Kepler Participating Scientists Program; NASA Origins of Solar Systems Program FX K.M.D. acknowledges support from an NSF Graduate Research Fellowship. M.J.P. acknowledges supports from the NASA Kepler Participating Scientists Program and from the NASA Origins of Solar Systems Program. We also thank the anonymous referee for reading the text so closely and for many helpful suggestions. NR 36 TC 31 Z9 31 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2013 VL 774 IS 2 AR 129 DI 10.1088/0004-637X/774/2/129 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 211EW UT WOS:000323888900038 ER PT J AU Deming, D Wilkins, A McCullough, P Burrows, A Fortney, JJ Agol, E Dobbs-Dixon, I Madhusudhan, N Crouzet, N Desert, JM Gilliland, RL Haynes, K Knutson, HA Line, M Magic, Z Mandell, AM Ranjan, S Charbonneau, D Clampin, M Seager, S Showman, AP AF Deming, Drake Wilkins, Ashlee McCullough, Peter Burrows, Adam Fortney, Jonathan J. Agol, Eric Dobbs-Dixon, Ian Madhusudhan, Nikku Crouzet, Nicolas Desert, Jean-Michel Gilliland, Ronald L. Haynes, Korey Knutson, Heather A. Line, Michael Magic, Zazralt Mandell, Avi M. Ranjan, Sukrit Charbonneau, David Clampin, Mark Seager, Sara Showman, Adam P. TI INFRARED TRANSMISSION SPECTROSCOPY OF THE EXOPLANETS HD 209458b AND XO-1b USING THE WIDE FIELD CAMERA-3 ON THE HUBBLE SPACE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: atmospheres; techniques: photometric; techniques: spectroscopic ID TRANSITING PLANET ATMOSPHERES; HOT-JUPITER XO-1B; EXTRASOLAR PLANET; GJ 1214B; ABSORPTION FEATURES; CIRCULATION MODELS; SUPER-EARTHS; SPECTRUM; 189733B; WATER AB Exoplanetary transmission spectroscopy in the near-infrared using the Hubble Space Telescope (HST) NICMOS is currently ambiguous because different observational groups claim different results from the same data, depending on their analysis methodologies. Spatial scanning with HST/WFC3 provides an opportunity to resolve this ambiguity. We here report WFC3 spectroscopy of the giant planets HD 209458b and XO-1b in transit, using spatial scanning mode for maximum photon-collecting efficiency. We introduce an analysis technique that derives the exoplanetary transmission spectrum without the necessity of explicitly decorrelating instrumental effects, and achieves nearly photon-limited precision even at the high flux levels collected in spatial scan mode. Our errors are within 6% (XO-1) and 26% (HD 209458b) of the photon-limit at a resolving power of lambda/delta lambda similar to 70, and are better than 0.01% per spectral channel. Both planets exhibit water absorption of approximately 200 ppm at the water peak near 1.38 mu m. Our result for XO-1b contradicts the much larger absorption derived from NICMOS spectroscopy. The weak water absorption we measure for HD209458b is reminiscent of the weakness of sodium absorption in the first transmission spectroscopy of an exoplanet atmosphere by Charbonneau et al. Model atmospheres having uniformly distributed extra opacity of 0.012 cm(2) g(-1) account approximately for both our water measurement and the sodium absorption. Our results for HD 209458b support the picture advocated by Pont et al. in which weak molecular absorptions are superposed on a transmission spectrum that is dominated by continuous opacity due to haze and/or dust. However, the extra opacity needed for HD 209458b is grayer than for HD 189733b, with a weaker Rayleigh component. C1 [Deming, Drake; Wilkins, Ashlee] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [McCullough, Peter; Crouzet, Nicolas] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Agol, Eric; Dobbs-Dixon, Ian] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Madhusudhan, Nikku] Yale Univ, Yale Ctr Astron Astrophys, New Haven, CT 06511 USA. [Desert, Jean-Michel; Knutson, Heather A.; Line, Michael] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Haynes, Korey] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Haynes, Korey; Mandell, Avi M.; Clampin, Mark] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Magic, Zazralt] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Magic, Zazralt] Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Ranjan, Sukrit; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Deming, D (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM ddeming@astro.umd.edu OI Dobbs-Dixon, Ian/0000-0002-4989-6501; Fortney, Jonathan/0000-0002-9843-4354; Ranjan, Sukrit/0000-0002-5147-9053; /0000-0002-0802-9145 NR 75 TC 110 Z9 111 U1 5 U2 26 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2013 VL 774 IS 2 AR 95 DI 10.1088/0004-637X/774/2/95 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 211EW UT WOS:000323888900004 ER PT J AU Kerzendorf, WE Yong, D Schmidt, BP Simon, JD Jeffery, CS Anderson, J Podsiadlowski, P Gal-Yam, A Silverman, JM Filippenko, AV Nomoto, K Murphy, SJ Bessell, MS Venn, KA Foley, RJ AF Kerzendorf, Wolfgang E. Yong, David Schmidt, Brian P. Simon, Joshua D. Jeffery, C. Simon Anderson, Jay Podsiadlowski, Philipp Gal-Yam, Avishay Silverman, Jeffrey M. Filippenko, Alexei V. Nomoto, Ken'ichi Murphy, Simon J. Bessell, Michael S. Venn, Kim A. Foley, Ryan J. TI A HIGH-RESOLUTION SPECTROSCOPIC SEARCH FOR THE REMAINING DONOR FOR TYCHO'S SUPERNOVA SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: supernova remnants; supernovae: individual (SN1572) ID DIFFUSE INTERSTELLAR BANDS; RELATIVE OSCILLATOR-STRENGTHS; FE-I TRANSITIONS; SINGLE-DEGENERATE SCENARIO; BRAHES 1572 SUPERNOVA; X-RAY OBSERVATIONS; MASS WHITE-DWARFS; RED GIANT BRANCH; SN 2011FE; PRECISION-MEASUREMENT AB In this paper, we report on our analysis using Hubble Space Telescope astrometry and Keck-I HIRES spectroscopy of the central six stars of Tycho's supernova remnant (SN 1572). With these data, we measured the proper motions, radial velocities, rotational velocities, and chemical abundances of these objects. Regarding the chemical abundances, we do not confirm the unusually high [Ni/Fe] ratio previously reported for Tycho-G. Rather, we find that for all metrics in all stars, none exhibit the characteristics expected from traditional Type Ia supernova single-degenerate-scenario calculations. The only possible exception is Tycho-B, a rare, metal-poor A-type star; however, we are unable to find a suitable scenario for it. Thus, we suggest that SN 1572 cannot be explained by the standard single-degenerate model. C1 [Kerzendorf, Wolfgang E.; Yong, David; Schmidt, Brian P.; Murphy, Simon J.; Bessell, Michael S.] Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Kerzendorf, Wolfgang E.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Simon, Joshua D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Jeffery, C. Simon] Armagh Observ, Armagh BT61 9DG, North Ireland. [Anderson, Jay] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Podsiadlowski, Philipp] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Gal-Yam, Avishay] Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Silverman, Jeffrey M.; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Silverman, Jeffrey M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Nomoto, Ken'ichi] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan. [Venn, Kim A.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kerzendorf, WE (reprint author), Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Cotter Rd, Weston, ACT 2611, Australia. EM wkerzend@mso.anu.edu.au OI Kerzendorf, Wolfgang/0000-0002-0479-7235; Schmidt, Brian/0000-0001-6589-1287; Jeffery, C. Simon/0000-0003-1759-0302 FU Schmidt's ARC Laureate Fellowship [FL0992131]; Israeli Science Foundation; Christopher R. Redlich Fund; TABASGO Foundation; NSF [AST-0908886, AST-1211916]; NASA from the Space Telescope Science Institute [GO-10098, GO-12469, AR-12623]; NASA [NAS 5-26555]; Clay Fellowship; W. M. Keck Foundation FX B. P. Schmidt and W. E. Kerzendorf were supported by Schmidt's ARC Laureate Fellowship (FL0992131). A. Gal-Yam acknowledges support by the Israeli Science Foundation. A. V. Filippenko is grateful for the support of the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grants AST-0908886 and AST-1211916; funding was also provided by NASA grants GO-10098, GO-12469, and AR-12623 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. R. J. Foley was supported by a Clay Fellowship.; Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 95 TC 21 Z9 22 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2013 VL 774 IS 2 AR 99 DI 10.1088/0004-637X/774/2/99 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 211EW UT WOS:000323888900008 ER PT J AU Tzanavaris, P Fragos, T Tremmel, M Jenkins, L Zezas, A Lehmer, BD Hornschemeier, A Kalogera, V Ptak, A Basu-Zych, AR AF Tzanavaris, P. Fragos, T. Tremmel, M. Jenkins, L. Zezas, A. Lehmer, B. D. Hornschemeier, A. Kalogera, V. Ptak, A. Basu-Zych, A. R. TI MODELING X-RAY BINARY EVOLUTION IN NORMAL GALAXIES: INSIGHTS FROM SINGS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; galaxies: spiral; stars: evolution; X-rays: binaries ID STAR-FORMATION RATE; BLACK-HOLE BINARIES; CHANDRA MONITORING OBSERVATIONS; FORMATION RATE INDICATOR; INITIAL MASS FUNCTION; LOCAL VOLUME SURVEY; SOLAR-TYPE STARS; LUMINOSITY FUNCTION; POPULATION SYNTHESIS; ELLIPTIC GALAXIES AB We present the largest-scale comparison to date between observed extragalactic X-ray binary (XRB) populations and theoretical models of their production. We construct observational X-ray luminosity functions (oXLFs) using Chandra observations of 12 late-type galaxies from the Spitzer Infrared Nearby Galaxy Survey. For each galaxy, we obtain theoretical XLFs (tXLFs) by combining XRB synthetic models, constructed with the population synthesis code StarTrack, with observational star formation histories (SFHs). We identify highest-likelihood models both for individual galaxies and globally, averaged over the full galaxy sample. Individual tXLFs successfully reproduce about half of the oXLFs, but for some galaxies we are unable to find underlying source populations, indicating that galaxy SFHs and metallicities are not well matched and/or that XRB modeling requires calibration on larger observational samples. Given these limitations, we find that the best models are consistent with a product of common envelope ejection efficiency and central donor concentration similar or equal to 0.1, and a 50% uniform-50% "twins" initial mass-ratio distribution. We present and discuss constituent subpopulations of tXLFs according to donor, accretor, and stellar population characteristics. The galaxy-wide X-ray luminosity due to low-mass and high-mass XRBs, estimated via our best global model tXLF, follows the general trend expected from the L-X-star formation rate and L-X-stellar mass relations of Lehmer et al. Our best models are also in agreement with modeling of the evolution of both XRBs over cosmic time and of the galaxy X-ray luminosity with redshift. C1 [Tzanavaris, P.; Jenkins, L.; Lehmer, B. D.; Hornschemeier, A.; Ptak, A.; Basu-Zych, A. R.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Tzanavaris, P.; Lehmer, B. D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Fragos, T.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. [Tremmel, M.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Zezas, A.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. [Kalogera, V.] Northwestern Univ, Ctr Interdisciplinary Res & Explorat Astrophys, Evanston, IL 60208 USA. [Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. RP Tzanavaris, P (reprint author), NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Mail Code 662, Greenbelt, MD 20771 USA. RI Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016 OI Zezas, Andreas/0000-0001-8952-676X; Fragos, Tassos/0000-0003-1474-1523 FU NASA at NASA Goddard Space Flight Center; NASA [ADAP 09-ADP09-0071]; MSHE [N203404939] FX We thank Stephan Noll for providing star formation histories from SED fitting with CIGALE for the galaxies in this sample. We thank Chris Belczynski for making StarTrack available to us. P.T. acknowledges support through a NASA Postdoctoral Program Fellowship at NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. T.F. is a CfA and ITC prize fellow. B.D.L. thanks the Einstein Fellowship Program. K.B. acknowledges support from MSHE grant N203404939. A.H., P.T., A.Z., and V.K. were also supported by NASA ADAP 09-ADP09-0071 (PI: Hornschemeier). Computational resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center and by the Northwestern University Quest High Performance Computing (HPC) cluster. NR 97 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 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2013 VL 774 IS 2 AR 136 DI 10.1088/0004-637X/774/2/136 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 211EW UT WOS:000323888900045 ER PT J AU Holt, JS Welles, SR Silvera, K Heap, IM Heredia, SM Martinez-Berdeja, A Palenscar, KT Sweet, LC Ellstrand, NC AF Holt, Jodie S. Welles, Shana R. Silvera, Katia Heap, Ian M. Heredia, Sylvia M. Martinez-Berdeja, Alejandra Palenscar, Kai T. Sweet, Lynn C. Ellstrand, Norman C. TI Taxonomic and Life History Bias in Herbicide Resistant Weeds: Implications for Deployment of Resistant Crops SO PLOS ONE LA English DT Article ID GLYPHOSATE; EVOLUTION; MANAGEMENT AB Evolved herbicide resistance (EHR) is an important agronomic problem and consequently a food security problem, as it jeopardizes herbicide effectiveness and increases the difficulty and cost of weed management. EHR in weeds was first reported in 1970 and the number of cases has accelerated dramatically over the last two decades. Despite 40 years of research on EHR, why some weeds evolve resistance and others do not is poorly understood. Here we ask whether weed species that have EHR are different from weeds in general. Comparing taxonomic and life history traits of weeds with EHR to a control group (''the world's worst weeds''), we found weeds with EHR significantly over-represented in certain plant families and having certain life history biases. In particular, resistance is overrepresented in Amaranthaceae, Brassicaceae and Poaceae relative to all weeds, and annuality is ca. 1.5 times as frequent in weeds with EHR as in the control group. Also, for perennial EHR weeds, vegetative reproduction is only 60% as frequent as in the control group. We found the same trends for subsets of weeds with EHR to acetolactate synthase (ALS), photosystem II (PSII), and 5-enolpyruvylshikimate-3phosphate (EPSP) synthase-inhibitor herbicides and with multiple resistance. As herbicide resistant crops (transgenic or not) are increasingly deployed in developing countries, the problems of EHR could increase in those countries as it has in the USA if the selecting herbicides are heavily applied and appropriate management strategies are not employed. Given our analysis, we make some predictions about additional species that might evolve resistance. C1 [Holt, Jodie S.; Welles, Shana R.; Heredia, Sylvia M.; Martinez-Berdeja, Alejandra; Palenscar, Kai T.; Sweet, Lynn C.; Ellstrand, Norman C.] Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA. [Silvera, Katia] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Heap, Ian M.] Int Survey Herbicide Resistant Weeds, Corvallis, OR USA. RP Welles, SR (reprint author), Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA. EM shana.welles@email.ucr.edu RI Sweet, Lynn/A-1896-2012 FU John Simon Guggenheim Memorial Fellowship; NSF OPUS [DEB-1020799]; [NSFDGE-0813967] FX Support for NCE was provided by a John Simon Guggenheim Memorial Fellowship and NSF OPUS grant #DEB-1020799. Support for SRW is supported under grant NSFDGE-0813967. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 32 TC 3 Z9 3 U1 2 U2 32 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 9 PY 2013 VL 8 IS 9 AR e71916 DI 10.1371/journal.pone.0071916 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 244QV UT WOS:000326405300004 PM 24039727 ER PT J AU Boamah, MD Oberg, K Fayolle, EC Garrod, RT Cyganowski, C van der Tak, F AF Boamah, Mavis D. Oberg, Karin Fayolle, Edith C. Garrod, Robin T. Cyganowski, Claudia van der Tak, Floris TI Spatial distribution of organics toward the high-mass young stellar object-NGC7538 IRS9 SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 246th National Meeting of the American-Chemical-Society (ACS) CY SEP 08-12, 2013 CL Indianapolis, IN SP Amer Chem Soc C1 [Boamah, Mavis D.] Wellesley Coll, Dept Chem, Wellesley, MA 02481 USA. [Oberg, Karin] Univ Virginia, Dept Chem, Charlottesvile, VA 22904 USA. [Oberg, Karin] Univ Virginia, Dept Astron, Charlottesvile, VA 22904 USA. [Fayolle, Edith C.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Garrod, Robin T.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Cyganowski, Claudia] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van der Tak, Floris] Univ Groningen, Kapteyn Astron Inst, Groningen, Netherlands. EM mboamah@wellesley.edu NR 0 TC 0 Z9 0 U1 2 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 8 PY 2013 VL 246 MA 525-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 288NJ UT WOS:000329618406309 ER PT J AU Crabtree, KN Martinez, O Gupta, H Thorwirth, S McCarthy, MC AF Crabtree, Kyle N. Martinez, Oscar Gupta, Harshal Thorwirth, Sven McCarthy, Michael C. TI Exploring chemical diversity in Titan's atmosphere with laboratory microwave spectroscopy SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 246th National Meeting of the American-Chemical-Society (ACS) CY SEP 08-12, 2013 CL Indianapolis, IN SP Amer Chem Soc C1 [Crabtree, Kyle N.; Martinez, Oscar; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gupta, Harshal] CALTECH, Pasadena, CA 91125 USA. [Thorwirth, Sven] Univ Cologne, Inst Phys 1, Cologne, Germany. EM kcrabtree@cfa.harvard.edu NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 8 PY 2013 VL 246 MA 583-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 288NJ UT WOS:000329618406360 ER PT J AU Oberg, KI Qi, CH Wilner, D Bergin, E AF Oeberg, Karin I. Qi, Chunhua Wilner, David Bergin, Edwin TI Ice-gas interactions during planet formation SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 246th National Meeting of the American-Chemical-Society (ACS) CY SEP 08-12, 2013 CL Indianapolis, IN SP Amer Chem Soc C1 [Oeberg, Karin I.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Qi, Chunhua; Wilner, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bergin, Edwin] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. EM oberg@virginia.edu NR 0 TC 0 Z9 0 U1 1 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 8 PY 2013 VL 246 MA 581-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 288NJ UT WOS:000329618406358 ER PT J AU Baldeck, CA Harms, KE Yavitt, JB John, R Turner, BL Valencia, R Navarrete, H Bunyavejchewin, S Kiratiprayoon, S Yaacob, A Supardi, MNN Davies, SJ Hubbell, SP Chuyong, GB Kenfack, D Thomas, DW Dalling, JW AF Baldeck, C. A. Harms, K. E. Yavitt, J. B. John, R. Turner, B. L. Valencia, R. Navarrete, H. Bunyavejchewin, S. Kiratiprayoon, S. Yaacob, A. Supardi, M. N. N. Davies, S. J. Hubbell, S. P. Chuyong, G. B. Kenfack, D. Thomas, D. W. Dalling, J. W. TI Habitat filtering across tree life stages in tropical forest communities SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE redundancy analysis; multivariate regression tree; beta diversity; topography; soil; Center for Tropical Forest Science ID RAIN-FOREST; BETA DIVERSITY; NEOTROPICAL FOREST; SPECIES ASSEMBLAGES; DIPTEROCARP FOREST; NEIGHBOR MATRICES; ECOLOGICAL DATA; SOIL NUTRIENTS; ASSOCIATIONS; DISTRIBUTIONS AB Tropical tree communities are shaped by local-scale habitat heterogeneity in the form of topographic and edaphic variation, but the life-history stage at which habitat associations develop remains poorly understood. This is due, in part, to the fact that previous studies have not accounted for the widely disparate sample sizes (number of stems) that result when trees are divided into size classes. We demonstrate that the observed habitat structuring of a community is directly related to the number of individuals in the community. We then compare the relative importance of habitat heterogeneity to tree community structure for saplings, juveniles and adult trees within seven large (24-50 ha) tropical forest dynamics plots while controlling for sample size. Changes in habitat structuring through tree life stages were small and inconsistent among life stages and study sites. Where found, these differences were an order of magnitude smaller than the findings of previous studies that did not control for sample size. Moreover, community structure and composition were very similar among tree sub-communities of different life stages. We conclude that the structure of these tropical tree communities is established by the time trees are large enough to be included in the census (1 cm diameter at breast height), which indicates that habitat filtering occurs during earlier life stages. C1 [Baldeck, C. A.] Univ Illinois, Program Ecol Evolut & Conservat Biol, Urbana, IL 61801 USA. [Baldeck, C. A.; Dalling, J. W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Harms, K. E.; Turner, B. L.; Davies, S. J.; Hubbell, S. P.; Dalling, J. W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Harms, K. E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Yavitt, J. B.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. [John, R.] Indian Inst Sci Educ & Res, Mohanpur 741252, W Bengal, India. [Valencia, R.; Navarrete, H.] Pontificia Univ Catolica Ecuador, Escuela Ciencias Biol, Lab Ecol Plantas & Herbario QCA, Quito, Ecuador. [Bunyavejchewin, S.] Natl Pk Wildlife & Plant Conservat Dept, Bangkok 10900, Thailand. [Kiratiprayoon, S.] Thammasat Univ Rangsit, Fac Sci & Technol, Klongluang 12121, Patumtani, Thailand. [Yaacob, A.] Univ Teknol MARA, Fac Plantat & Agrotechnol, Shah Alam 40450, Selangor, Malaysia. [Supardi, M. N. N.] Forest Res Inst Malaysia, Div Forest Environm, Kepong 52109, Selangor Darul, Malaysia. [Davies, S. J.; Kenfack, D.] Harvard Univ, Arnold Arboretum Asia Program, Ctr Trop Forest Sci, Cambridge, MA 02138 USA. [Hubbell, S. P.] Univ Calif Los Angeles, Dept Ecol & Evolut Biol, Los Angeles, CA 90095 USA. [Chuyong, G. B.] Univ Buea, Dept Plant & Anim Sci, Buea, Cameroon. [Thomas, D. W.] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. RP Baldeck, CA (reprint author), Univ Illinois, Program Ecol Evolut & Conservat Biol, 505 S Goodwin Ave, Urbana, IL 61801 USA. EM baldeck2@life.illinois.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU National Science Foundation [DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9405933, DEB9221033, 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; US National Science Foundation [DEB 0211004, DEB 0211115, DEB 0212284, DEB 0212818, OISE 0314581]; CTFS FX The BCI forest dynamics research project was made possible by National Science Foundation grants to S.P.H.: DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9615226, DEB-9405933, DEB9221033, 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 and the Small World Institute Fund. Funding for soils work was provided by the US National Science Foundation Grants DEB 0211004, DEB 0211115, DEB 0212284, DEB 0212818 and OISE 0314581, the soils initiative of the Smithsonian Tropical Research Institute, and a CTFS grant to cover collection and extraction of soils from Korup. NR 43 TC 24 Z9 26 U1 9 U2 82 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD SEP 7 PY 2013 VL 280 IS 1766 AR 20130548 DI 10.1098/rspb.2013.0548 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 180TR UT WOS:000321621000002 PM 23843384 ER PT J AU Lewis, SL Sonke, B Sunderland, T Begne, SK Lopez-Gonzalez, G van der Heijden, GMF Phillips, OL Affum-Baffoe, K Baker, TR Banin, L Bastin, JF Beeckman, H Boeckx, P Bogaert, J De Canniere, C Chezeaux, E Clark, CJ Collins, M Djagbletey, G Djuikouo, MNK Droissart, V Doucet, JL Ewango, CEN Fauset, S Feldpausch, TR Foli, EG Gillet, JF Hamilton, AC Harris, DJ Hart, TB de Haulleville, T Hladik, A Hufkens, K Huygens, D Jeanmart, P Jeffery, KJ Kearsley, E Leal, ME Lloyd, J Lovett, JC Makana, JR Malhi, Y Marshall, AR Ojo, L Peh, KSH Pickavance, G Poulsen, JR Reitsma, JM Sheil, D Simo, M Steppe, K Taedoumg, HE Talbot, J Taplin, JRD Taylor, D Thomas, SC Toirambe, B Verbeeck, H Vleminckx, J White, LJT Willcock, S Woell, H Zemagho, L AF Lewis, Simon L. Sonke, Bonaventure Sunderland, Terry Begne, Serge K. Lopez-Gonzalez, Gabriela van der Heijden, Geertje M. F. Phillips, Oliver L. Affum-Baffoe, Kofi Baker, Timothy R. Banin, Lindsay Bastin, Jean-Francois Beeckman, Hans Boeckx, Pascal Bogaert, Jan De Canniere, Charles Chezeaux, Eric Clark, Connie J. Collins, Murray Djagbletey, Gloria Djuikouo, Marie Noel K. Droissart, Vincent Doucet, Jean-Louis Ewango, Cornielle E. N. Fauset, Sophie Feldpausch, Ted R. Foli, Ernest G. Gillet, Jean-Francois Hamilton, Alan C. Harris, David J. Hart, Terese B. de Haulleville, Thales Hladik, Annette Hufkens, Koen Huygens, Dries Jeanmart, Philippe Jeffery, Kathryn J. Kearsley, Elizabeth Leal, Miguel E. Lloyd, Jon Lovett, Jon C. Makana, Jean-Remy Malhi, Yadvinder Marshall, Andrew R. Ojo, Lucas Peh, Kelvin S-H Pickavance, Georgia Poulsen, John R. Reitsma, Jan M. Sheil, Douglas Simo, Murielle Steppe, Kathy Taedoumg, Hermann E. Talbot, Joey Taplin, James R. D. Taylor, David Thomas, Sean C. Toirambe, Benjamin Verbeeck, Hans Vleminckx, Jason White, Lee J. T. Willcock, Simon Woell, Hannsjorg Zemagho, Lise TI Above-ground biomass and structure of 260 African tropical forests SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE climate; soil; wood density; Congo Basin; east Africa; west Africa ID SPATIAL-PATTERNS; WOOD DENSITY; AMAZONIAN FORESTS; TREE ALLOMETRY; CLIMATE-CHANGE; CARBON STOCKS; RAIN-FOREST; GROWTH; SENSITIVITY; SOILS AB We report above-ground biomass (AGB), basal area, stem density and wood mass density estimates from 260 sample plots (mean size: 1.2 ha) in intact closed-canopy tropical forests across 12 African countries. Mean AGB is 395.7 Mg dry mass ha(-1) (95% CI: 14.3), substantially higher than Amazonian values, with the Congo Basin and contiguous forest region attaining AGB values (429 Mg ha(-1)) similar to those of Bornean forests, and significantly greater than East or West African forests. AGB therefore appears generally higher in palaeo-compared with neotropical forests. However, mean stem density is low(426 +/- 11 stems ha(-1) greater than or equal to 100 mm diameter) compared with both Amazonian and Bornean forests (cf. approx. 600) and is the signature structural feature of African tropical forests. While spatial autocorrelation complicates analyses, AGB shows a positive relationship with rainfall in the driest nine months of the year, and an opposite association with the wettest three months of the year; a negative relationship with temperature; positive relationship with clay-rich soils; and negative relationships with C : Nratio (suggesting a positive soil phosphorus-AGB relationship), and soil fertility computed as the sum of base cations. The results indicate that AGB is mediated by both climate and soils, and suggest that the AGB of African closed-canopy tropical forests may be particularly sensitive to future precipitation and temperature changes. C1 [Lewis, Simon L.] UCL, Dept Geog, London WC1E 6BT, England. [Lewis, Simon L.; Begne, Serge K.; Lopez-Gonzalez, Gabriela; Phillips, Oliver L.; Baker, Timothy R.; Fauset, Sophie; Feldpausch, Ted R.; Lloyd, Jon; Lovett, Jon C.; Peh, Kelvin S-H; Pickavance, Georgia; Talbot, Joey; Willcock, Simon] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. [Sonke, Bonaventure; Begne, Serge K.; Djuikouo, Marie Noel K.; Simo, Murielle; Taedoumg, Hermann E.; Zemagho, Lise] Univ Yaounde I, Higher Teachers Training Coll, Dept Biol, Plant Systemat & Ecol Lab, Yaounde, Cameroon. [Sunderland, Terry; Sheil, Douglas] Ctr Int Forestry Res, Bogor, Indonesia. [van der Heijden, Geertje M. F.] Univ Wisconsin, Milwaukee, WI 53201 USA. [van der Heijden, Geertje M. F.] Smithsonian Trop Res Inst, Panama City, Panama. [Affum-Baffoe, Kofi] Forestry Commiss Ghana, Mensurat Unit, Kumasi, Ghana. [Banin, Lindsay] Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland. [Bastin, Jean-Francois; De Canniere, Charles] Univ Libre Brussels, Landscape Ecol & Vegetal Prod Syst Unit, Brussels, Belgium. [Bastin, Jean-Francois; Bogaert, Jan; de Haulleville, Thales] Univ Liege, Gembloux Agrobio Tech, Biodivers & Landscape Unit, Gembloux, Belgium. [Banin, Lindsay] Ecole Reg Postuniv Amenagement & Gest Integres Fo, Kinshasa, Zaire. [Beeckman, Hans; de Haulleville, Thales; Kearsley, Elizabeth; Toirambe, Benjamin] Royal Museum Cent Africa, Lab Wood Biol & Xylarium, Tervuren, Belgium. [Boeckx, Pascal; Hufkens, Koen; Huygens, Dries; Kearsley, Elizabeth] Univ Ghent, Fac Biosci Engn, Isotope Biosci Lab ISOFYS, Dept Appl Analyt & Phys Chem, B-9000 Ghent, Belgium. [Chezeaux, Eric] Rougier Gabon, Libreville, Gabon. [Clark, Connie J.; Poulsen, John R.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Collins, Murray] London Sch Econ, Grantham Res Inst Climate Change & Environm, London WC2A 2AZ, England. [Djagbletey, Gloria; Foli, Ernest G.] KNUST, Forestry Res Inst Ghana FORIG, Kumasi, Ghana. [Djuikouo, Marie Noel K.] Univ Buea, Fac Sci, Dept Bot & Plant Physiol, Buea, Cameroon. [Droissart, Vincent] IRD, Unite Mixte Rech AMAP Bot & Bioinformat Architect, Montpellier, France. [Doucet, Jean-Louis] Univ Liege, Unit Forest & Nat Management, Lab Trop & Subtrop Forest Reg, Gembloux, Belgium. [Doucet, Jean-Louis; Gillet, Jean-Francois] Univ Liege, Gembloux Agrobio Tech, Nat, Gembloux, Belgium. [Ewango, Cornielle E. N.; Makana, Jean-Remy] Wildlife Conservat Soc DR Congo, Kinshasa, Zaire. [Ewango, Cornielle E. N.] Ctr Format & Rech Conservat Forestiere CEFRECOF, Kinshasa, Zaire. [Harris, David J.] Royal Bot Garden Edinburgh, Edinburgh EH3 5LR, Midlothian, Scotland. [Hart, Terese B.] Lukuru Wildlife Res Fdn, Kinshasa, Gombe, Zaire. [Hart, Terese B.] Yale Peabody Museum Nat Hist, Div Vertebrate Zool, New Haven, CT USA. [Hladik, Annette] Museum Natl Hist Nat, Dept Hommes Nat Soc, Brunoy, France. [Huygens, Dries] Univ Austral Chile, Fac Agr Sci, Inst Agr Engn & Soil Sci, Valdivia, Chile. [Jeanmart, Philippe] Precious Woods Gabon, Libreville, Gabon. [Jeffery, Kathryn J.; White, Lee J. T.] Agence Natl Parcs Nationaux, Libreville, Gabon. [Jeffery, Kathryn J.; White, Lee J. T.] Inst Rech Ecol Trop, Libreville, Gabon. [Jeffery, Kathryn J.; White, Lee J. T.] Univ Stirling, Sch Nat Sci, Stirling FK9 4LA, Scotland. [Kearsley, Elizabeth; Steppe, Kathy; Verbeeck, Hans] Univ Ghent, Fac Biosci Engn, Lab Plant Ecol, Dept Appl Ecol & Environm Biol, B-9000 Ghent, Belgium. [Leal, Miguel E.] Wildlife Conservat Soc, Kampala, Uganda. [Lloyd, Jon] James Cook Univ, Sch Earth & Environm Sci, Cairns, Australia. [Malhi, Yadvinder] Univ Oxford, Sch Geog & Environm, Oxford OX1 3QY, England. [Marshall, Andrew R.] Univ York, Dept Environm, CIRCLE, York YO10 5DD, N Yorkshire, England. [Marshall, Andrew R.] Flamingo Land Ltd, Kirby Misperton YO17 6UX, N Yorkshire, England. [Ojo, Lucas] Univ Agr, Dept Environm Management & Toxicol, Abeokuta, Ogun, Nigeria. [Peh, Kelvin S-H] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. [Reitsma, Jan M.] Bureau Waardenburg Bv, NL-4100 AJ Culemborg, Netherlands. [Sheil, Douglas] So Cross Univ, Sch Environm Sci & Engn, Lismore, NSW 2480, Australia. [Sheil, Douglas] Inst Trop Forest Conservat, Kabale, Uganda. [Taplin, James R. D.] Forum Future, London EC1V 3QN, England. [Taylor, David] Natl Univ Singapore, Dept Geog, Singapore 119615, Singapore. [Thomas, Sean C.] Univ Toronto, Fac Forestry, Toronto, ON M5S 3B3, Canada. [Vleminckx, Jason] Univ Libre Brussels, Fac Sci, Serv Evolut Biol & Ecol, Brussels, Belgium. [Willcock, Simon] Univ Southampton, Dept Life Sci, Southampton SO17 1BJ, Hants, England. RP Lewis, SL (reprint author), UCL, Dept Geog, Mortimer St, London WC1E 6BT, England. EM s.l.lewis@leeds.ac.uk RI Phillips, Oliver/A-1523-2011; Peh, Kelvin/C-3408-2013; James Cook University, TESS/B-8171-2012; Lloyd, Jonathan/F-8893-2010; Feldpausch, Ted/D-3436-2009; Sheil, Douglas/A-3867-2015; Huygens, Dries/A-8395-2008; Jeffery, Kathryn/G-2530-2013; OI Lovett, Jonathan/0000-0002-5839-3770; Harris, David/0000-0002-6801-2484; Lewis, Simon/0000-0002-8066-6851; Phillips, Oliver/0000-0002-8993-6168; Peh, Kelvin/0000-0002-2921-1341; Lloyd, Jonathan/0000-0002-5458-9960; Feldpausch, Ted/0000-0002-6631-7962; Sheil, Douglas/0000-0002-1166-6591; Huygens, Dries/0000-0003-2423-6926; Jeffery, Kathryn/0000-0002-2632-0008; Hufkens, Koen/0000-0002-5070-8109 FU USAID/CIFOR; GEOCARBON; European Research Council; NERC; David Foundation; Lucile Packard Foundation; Leverhulme Trust; Missouri Botanical Garden; Royal Society joint project; Royal Society University Research Fellowship; Gordon and Betty Moore Foundation; University of Leeds; Royal Society FX USAID/CIFOR (to S.L.L. and T.S.), GEOCARBON (to S.L.L. and B.S.) and European Research Council (to O.L.P., S.L.L. and Y.M.), NERC (New Investigators award to S.L.; TROBIT Consortium award to J.L. and S.L.L.), Gordon and Betty Moore and David and Lucile Packard Foundations (to L.J.T.W., S.L.L. and Y.M.), Leverhulme Trust (to S.L.L.), Missouri Botanical Garden (to M. L.), Royal Society joint project (to T.R.F and E.F.) and Royal Society University Research Fellowship (to S.L.L.) grants all part-funded AfriTRON(www.afritron.net) and this work. ForestPlots.net development is funded by the Gordon and Betty Moore Foundation, NERC, The University of Leeds, European Research Council and the Royal Society. NR 61 TC 51 Z9 52 U1 5 U2 82 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 EI 1471-2970 J9 PHILOS T R SOC B JI Philos. Trans. R. Soc. B-Biol. Sci. PD SEP 5 PY 2013 VL 368 IS 1625 AR 20120295 DI 10.1098/rstb.2012.0295 PG 14 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AA6PO UT WOS:000331220500002 PM 23878327 ER PT J AU Thompson, JR Carpenter, DN Cogbill, CV Foster, DR AF Thompson, Jonathan R. Carpenter, Dunbar N. Cogbill, Charles V. Foster, David R. TI Four Centuries of Change in Northeastern United States Forests SO PLOS ONE LA English DT Article ID LAND-USE HISTORY; WESTERN NEW-YORK; CENTRAL NEW-ENGLAND; PRESETTLEMENT FORESTS; CENTRAL PENNSYLVANIA; SURVEY RECORDS; OAK FORESTS; VEGETATION; DISTURBANCE; PATTERNS AB The northeastern United States is a predominately-forested region that, like most of the eastern U. S., has undergone a 400-year history of intense logging, land clearance for agriculture, and natural reforestation. This setting affords the opportunity to address a major ecological question: How similar are today's forests to those existing prior to European colonization? Working throughout a nine-state region spanning Maine to Pennsylvania, we assembled a comprehensive database of archival land-survey records describing the forests at the time of European colonization. We compared these records to modern forest inventory data and described: (1) the magnitude and attributes of forest compositional change, (2) the geography of change, and (3) the relationships between change and environmental factors and historical land use. We found that with few exceptions, notably the American chestnut, the same taxa that made up the pre-colonial forest still comprise the forest today, despite ample opportunities for species invasion and loss. Nonetheless, there have been dramatic shifts in the relative abundance of forest taxa. The magnitude of change is spatially clustered at local scales (<125 km) but exhibits little evidence of regional-scale gradients. Compositional change is most strongly associated with the historical extent of agricultural clearing. Throughout the region, there has been a broad ecological shift away from late successional taxa, such as beech and hemlock, in favor of early- and mid-successional taxa, such as red maple and poplar. Additionally, the modern forest composition is more homogeneous and less coupled to local climatic controls. C1 [Thompson, Jonathan R.] Smithsonian Inst Front Royal, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Carpenter, Dunbar N.] Univ Wisconsin, Dept Forest & Wildlife Ecol, Madison, WI USA. [Cogbill, Charles V.; Foster, David R.] Harvard Univ, Harvard Forest, Petersham, MA USA. RP Thompson, JR (reprint author), Smithsonian Inst Front Royal, Smithsonian Conservat Biol Inst, Front Royal, VA USA. EM thompsonjr@si.edu FU US National Science Foundation [DEB 06-20443] FX This research was supported by the US National Science Foundation through its programs in Long Term Ecological Research (DEB 06-20443). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 75 TC 56 Z9 58 U1 12 U2 92 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 SEP 4 PY 2013 VL 8 IS 9 AR e72540 DI 10.1371/journal.pone.0072540 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 219OE UT WOS:000324515600028 PM 24023749 ER PT J AU Kassi, S Gordon, IE Campargue, A AF Kassi, Samir Gordon, Iouli E. Campargue, Alain TI First detection of transitions in the second quadrupole overtone band of nitrogen near 1.44 mu m by CW-CRDS with 6 x 10(-13) cm(-1) sensitivity SO CHEMICAL PHYSICS LETTERS LA English DT Article ID M TRANSPARENCY WINDOW; CAVITY RING; ABSORPTION-SPECTRUM; LINE PARAMETERS; SPECTROSCOPY; N-14(2); COEFFICIENTS; WATER AB The extremely weak S(4) and S(6) electric quadrupole transitions of the 3-0 band of nitrogen have been detected by very high sensitivity CW-Cavity Ring Down spectroscopy near 6950 cm(-1). A noise equivalent absorption on the order of alpha(min) similar to 6 x 10(-13) cm(-1) was achieved by averaging several thousand 0.5 cm(-1) wide spectra recorded successively over several days. The studied N-14(2) lines are among the weakest ever measured in the laboratory (intensity on the order of 1.5 x 10(-31) cm/molecule). The positions determined with a 0.002 cm(-1) uncertainty and the line intensities are compared with theoretical values included in the HITRAN2012 database. (C) 2013 Elsevier B.V. All rights reserved. C1 [Kassi, Samir; Campargue, Alain] Univ Grenoble 1, CNRS, LIPhy UMR5588, F-38041 Grenoble, France. [Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Campargue, A (reprint author), Univ Grenoble 1, CNRS, LIPhy UMR5588, F-38041 Grenoble, France. EM Alain.Campargue@ujf-grenoble.fr NR 22 TC 2 Z9 2 U1 2 U2 23 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD SEP 4 PY 2013 VL 582 BP 6 EP 9 DI 10.1016/j.cplett.2013.07.031 PG 4 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 213SQ UT WOS:000324080900002 ER PT J AU Cipollini, ML Culberson, J Whigham, D Johnson, K Knight, T O'Neill, J AF Cipollini, Martin L. Culberson, Joshua Whigham, Dennis Johnson, Kartee Knight, Troy O'Neill, Jay TI Spatial and temporal patterns of sexual dimorphism and sex ratio in Lindera benzoin L. (Lauraceae) SO JOURNAL OF THE TORREY BOTANICAL SOCIETY LA English DT Article DE biased sex ratio; differential costs of reproduction; dioecy; within- and among-site variation in growth and herbivory ID REPRODUCTIVE EFFORT; VEGETATIVE GROWTH; PLANT-POPULATIONS; TROPICAL FOREST; SHRUB; COSTS; SIZE; ALLOCATION; HERBIVORY; DISPERSAL AB The focus of this study is spatial and temporal variation in sex ratio and sexual dimorphism in the woody dioecious shrub Lindera benzoin (spicebush, Lauraceae). This species has been shown to express female-biased flowering sex ratios in a focal study population in Maryland. Sex ratio variation and sexual dimorphism in dioecious plants has attracted the focus of many short-term, single site studies, particularly in light of Fisher's (1930) elucidation of the selective pressures favoring the production of unbiased progeny sex ratios. As informative as such studies have been, long term, multi-site studies are necessary for full evaluation of the factors leading to differential expression of sex within and among populations. Female-biased sex ratios, relatively rare among plant species, are particularly difficult to explain when many studies, including ours of L. benzoin, show females to have higher costs of reproduction and lower modular growth rates suggesting a competitive disadvantage in comparison with males. This study focuses intensively on a single population in Maryland, and is augmented by flowering censuses, and plant size and growth estimates in populations at 11 nearby sites in Maryland, and four distant sites in Pennsylvania, Virginia and West Virginia. Data were collected at most sites in the early 1990s and again in 2010, so that long-term variation in sex ratio could be explored. Results show tendencies for overall female-bias, for female bias in small size classes and male bias in large size classes, for an increase in the proportion of males within populations over time, and for sex ratios to be biased toward females in relatively recently established populations but unbiased or male-biased in older populations. Sexual dimorphism favoring males was consistent across sites, but no sexual dimorphism in herbivory by mammals or by foliage feeding insects was detected. These field observations combined with data derived from a separate but concurrent garden study suggest that early establishment of female-biased sex ratios may occur via a faster early growth rate and possible better tolerance of herbivory by females. This model further suggests that early advantages of females are followed by post-reproductive demographic changes favoring males, resulting in a tendency for sex ratios to shift toward maleness over time. C1 [Cipollini, Martin L.; Johnson, Kartee] Berry Coll, Dept Biol, Mt Berry, GA 30149 USA. [Whigham, Dennis; O'Neill, Jay] Smithsonian Environm Res Ctr, Plant Ecol Lab, Edgewater, MD 21037 USA. [Knight, Troy] St Johns Univ, New Sci Ctr 116, Collegeville, MN 56321 USA. RP Cipollini, ML (reprint author), Berry Coll, Dept Biol, POB 430, Mt Berry, GA 30149 USA. EM mcipollini@berry.edu FU Smithsonian Environmental Research Center (SERC); faculty Development Grant from Berry College; SERC Internship Program; Berry College student work program FX Funding and logistical support was provided via Postdoctoral Fellowship and Research Collaborator programs at the Smithsonian Environmental Research Center (SERC) and by a faculty Development Grant from Berry College (awards to M. Cipollini), by the SERC Internship Program (award to J. Culberson), and by the Berry College student work program. NR 44 TC 1 Z9 1 U1 3 U2 14 PU TORREY BOTANICAL SOC PI LAWRENCE PA 810 E 10TH ST, LAWRENCE, KS 66044 USA SN 1095-5674 EI 1940-0616 J9 J TORREY BOT SOC JI J. Torrey Bot. Soc. PD SEP PY 2013 VL 140 IS 3 BP 280 EP 299 DI 10.3159/TORREY-D-13-00013.1 PG 20 WC Plant Sciences SC Plant Sciences GA AM2CH UT WOS:000339655700005 ER PT J AU Cipollini, ML Whigham, D O'Neill, J AF Cipollini, Martin L. Whigham, Dennis O'Neill, Jay TI Seed size, sexual dimorphism, and sex ratio in Lindera benzoin L. (Lauraceae) SO JOURNAL OF THE TORREY BOTANICAL SOCIETY LA English DT Article DE differential costs of reproduction; dioecy; early growth in male and female plants; intraspecific competition ID IN-THE-PULPIT; ANTENNARIA-DIOICA ASTERACEAE; SPATIAL-DISTRIBUTION; DIOECIOUS PLANTS; ARISAEMA-TRIPHYLLUM; TROPICAL FOREST; GENDER; REPRODUCTION; DISPERSAL; POLLEN AB The adult genet sex ratio of a wild population of the dioecious woody shrub Lindera benzoin (spicebush) in Maryland has shown a persistent female-bias over a time span of over 17 years. Female-biased sex ratios are relatively rare in dioecious plants, and are not easily explained by costs of reproduction, which are often higher in females. In fact, data from reproductive adults in this population showed modular growth favoring males, which led to questions concerning the source of female-bias. Using seeds collected from 20 maternal plants in 1992, a garden study was conducted from 1993-2003 in which periodic flowering censuses were conducted, and plant size parameters were recorded. The plants were grown in a relatively tightly packed array which likely forced early intraspecific competition. The results suggested that L. benzoin females may compensate for differential costs of reproduction via larger initial seed size and early growth rate, but that sexual dimorphism in such a highly competitive scenario can favor males even more dramatically than in typical field conditions. Despite larger early size and faster growth in female seedlings, males showed clear advantages over females in the post-reproductive period and mortality was much higher in female genets. Sex ratios were close to the same level of female bias seen in the wild population around the time of initial flowering, but trended toward maleness as post-reproductive stage genet mortality ensued. Explanations for the development and persistence of female bias include larger seedling size that may give females a competitive advantage over males in the prereproductive stage, which under certain circumstances may lead to greater survival of female seedlings. Variation among habitats in herbivory and other environmental factors that influence survival and sex expression could ameliorate the competitive advantage of males associated with their lower reproductive costs. C1 [Cipollini, Martin L.] Berry Coll, Dept Biol, Mt Berry, GA 30149 USA. [Whigham, Dennis; O'Neill, Jay] Smithsonian Environm Res Ctr, Plant Ecol Lab, Edgewater, MD 21037 USA. RP Cipollini, ML (reprint author), Berry Coll, Dept Biol, POB 430, Mt Berry, GA 30149 USA. EM mcipollini@berry.edu FU Postdoctoral Fellowship and Research Collaborator programs at the Smithsonian Environmental Research Center; Faculty Development Grant from Berry College FX Funding and logistical support was provided via Postdoctoral Fellowship and Research Collaborator programs at the Smithsonian Environmental Research Center, and by a Faculty Development Grant from Berry College (awards to M. Cipollini). NR 49 TC 1 Z9 1 U1 5 U2 21 PU TORREY BOTANICAL SOC PI LAWRENCE PA 810 E 10TH ST, LAWRENCE, KS 66044 USA SN 1095-5674 EI 1940-0616 J9 J TORREY BOT SOC JI J. Torrey Bot. Soc. PD SEP PY 2013 VL 140 IS 3 BP 300 EP 312 DI 10.3159/TORREY-D-13-00014.1 PG 13 WC Plant Sciences SC Plant Sciences GA AM2CH UT WOS:000339655700006 ER PT J AU Witte, CL Lamberski, N Rideout, BA Fields, V Teare, CS Barrie, M Haefele, H Junge, R Murray, S Hungerford, LL AF Witte, Carmel L. Lamberski, Nadine Rideout, Bruce A. Fields, Victoria Teare, Cyd Shields Barrie, Michael Haefele, Holly Junge, Randall Murray, Suzan Hungerford, Laura L. TI DEVELOPMENT OF A CASE DEFINITION FOR CLINICAL FELINE HERPESVIRUS INFECTION IN CHEETAHS (ACINONYX JUBATUS) HOUSED IN ZOOS SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Acinonyx jubatus; case definition; cheetah; epidemiology; feline herpesvirus; upper respiratory disease ID CATS AB The identification of feline herpesvirus (FHV) infected cheetahs (Acinonyx jubatus) and characterization of shedding episodes is difficult due to nonspecific clinical signs and limitations of diagnostic tests. The goals of this study were to develop a case definition for clinical FHV and describe the distribution of signs. Medical records from six different zoologic institutions were reviewed to identify cheetahs with diagnostic test results confirming FHV. Published literature, expert opinion, and results of a multiple correspondence analysis (MCA) were used to develop a clinical case definition based on 69 episodes in FHV laboratory confirmed (LC) cheetahs. Four groups of signs were identified in the MCA: general ocular signs, serious ocular lesions, respiratory disease, and cutaneous lesions. Ocular disease occurred with respiratory signs alone, with skin lesions alone, and with both respiratory signs and skin lesions. Groups that did not occur together were respiratory signs and skin lesions. The resulting case definition included 1) LC cheetahs; and 2) clinically compatible (CC) cheetahs that exhibited a minimum of 7 day's duration of the clinical sign groupings identified in the MCA or the presence of corneal ulcers or keratitis that occurred alone or in concert with other ocular signs and skin lesions. Exclusion criteria were applied. Application of the case definition to the study population identified an additional 78 clinical episodes, which represented 58 CC cheetahs. In total, 28.8% (93/322) of the population was identified as LC or CC. The distribution of identified clinical signs was similar across LC and CC cheetahs. Corneal ulcers and/or keratitis, and skin lesions were more frequently reported in severe episodes; in mild episodes, there were significantly more cheetahs with ocular-only or respiratory-only disease. Our results provide a better understanding of the clinical presentation of FHV, while presenting a standardized case definition that can both contribute to earlier diagnoses and be used for population-level studies. C1 [Witte, Carmel L.; Rideout, Bruce A.; Fields, Victoria] San Diego Zoo Global, Inst Conservat Res, Wildlife Dis Labs, Escondido, CA 92027 USA. [Lamberski, Nadine] San Diego Zoo Safari Pk, Escondido, CA 92027 USA. [Teare, Cyd Shields] White Oak Conservat Ctr, Yulee, FL 32097 USA. [Barrie, Michael] Columbus Zoo & Aquarium, Columbus, OH 43065 USA. [Haefele, Holly] Fossil Rim Wildlife Ctr, Glen Rose, TX 76043 USA. [Junge, Randall] St Louis Zoo, St Louis, MO 63110 USA. [Murray, Suzan] Smithsonian Natl Zool Pk, Washington, DC 20008 USA. [Hungerford, Laura L.] Univ Maryland, Sch Med, Dept Epidemiol & Prevent Med, Baltimore, MD 21201 USA. RP Witte, CL (reprint author), San Diego Zoo Global, Inst Conservat Res, Wildlife Dis Labs, 15600 San Pasqual Valley Rd, Escondido, CA 92027 USA. EM cwitte@sandiegozoo.org FU Morris Animal Foundation FX Support for this research was provided by the Morris Animal Foundation. The authors extend a special thanks to the many veterinarians, administrative personnel, volunteers, and institutions that contributed to the retrieval of archived data. Specifically, the authors would like to thank Duane Jensen, Valerie Stoddard, Susanne Schofield, Donna Vader, Billie Bearden, and Paula Augustus from San Diego Zoo and San Diego Zoo Safari Park; Debbie Wolf from St. Louis Zoo; Deb Krum from Columbus Zoo and Aquarium; Veronica Acosta from Smithsonian National Zoological Park; Gail Bullard, Bob Bullard, and Mary Jo Stearns from Fossil Rim Wildlife Center. The authors also thank Dr. Benji Alcantar from Wildlife Safari and Dr. Laurie Marker from the Cheetah Conservation Fund for providing additional historic information on cheetahs in this study. NR 18 TC 1 Z9 1 U1 0 U2 10 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 SEP PY 2013 VL 44 IS 3 BP 634 EP 644 DI 10.1638/2012-0183R.1 PG 11 WC Veterinary Sciences SC Veterinary Sciences GA AM1WM UT WOS:000339639100013 PM 24063091 ER PT J AU Smith, ND AF Smith, Nathan D. TI NEW DIRECTIONS IN VERTEBRATE PALEONTOLOGICAL RESEARCH IN THE TRANSANTARCTIC MOUNTAINS, ANTARCTICA SO PALAIOS LA English DT Editorial Material ID HANSON FORMATION; TETRAPODS; DINOSAUR; ANATOMY C1 [Smith, Nathan D.] Howard Univ, Dept Biol, Washington, DC 20059 USA. [Smith, Nathan D.] Smithsonian Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Smith, Nathan D.] Field Museum Nat Hist, Dept Geol, Chicago, IL 60605 USA. RP Smith, ND (reprint author), Howard Univ, Dept Biol, Washington, DC 20059 USA. EM nathan.smith@howard.edu NR 19 TC 0 Z9 0 U1 0 U2 7 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 EI 1938-5323 J9 PALAIOS JI Palaios PD SEP-OCT PY 2013 VL 28 IS 9-10 BP 680 EP 682 DI 10.2110/palo.2013.SO5 PG 3 WC Geology; Paleontology SC Geology; Paleontology GA AD8XH UT WOS:000333548500009 ER PT J AU Crofoot, MC AF Crofoot, Margaret C. TI The Cost of Defeat: Capuchin Groups Travel Further, Faster and Later After Losing Conflicts with Neighbors SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE intergroup competition; Cebus capucinus; Barro Colorado Island; radio telemetry ID MONKEYS CEBUS-APELLA; GROUP-SIZE; INTERGROUP ENCOUNTERS; CONTEST COMPETITION; NOCTURNAL ACTIVITY; JAPANESE MACAQUES; COLOBUS-GUEREZA; PRIMATE GROUPS; RESOURCE SIZE; FOOD AB Although competition between social groups is central to hypotheses about the evolution of human social organization, competitive interactions among group-mates are thought to play a more dominant role in shaping the behavior and ecology of other primate species. However, few studies have directly tested the impact of intergroup conflicts in non-human primates. What is the cost of defeat? To address this question, the movements of six neighboring white-faced capuchin (Cebus capucinus) social groups living on Barro Colorado Island, Panama were tracked simultaneously using an Automated Radio Telemetry System (ARTS), for a period of six months. Groups moved 13% (441 m) further on days they lost interactions compared with days they won interactions. To cover these larger distances, they traveled faster, stopped less frequently, and remained active later in the evening. Defeat also caused groups to alter their patterns of space use. Losing groups had straighter travel paths than winning groups, larger net displacements and were more likely to change their sleeping site. These results demonstrate that losing groups pay increased travel costs and suggest that they forage in low-quality areas. They provide some of the first direct evidence that intergroup conflicts have important energetic consequences for members of competitively unsuccessful primate social groups. A better understanding of how intergroup competition impacts patterns of individual fitness is thus needed to clarify the role that this group-level process plays in shaping the evolution of human- and non-human primate behavior. (C) 2013 Wiley Periodicals, Inc. C1 [Crofoot, Margaret C.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Crofoot, Margaret C.] Max Planck Inst Ornithol, Div Migrat & Immunoecol, Radolfzell am Bodensee, Germany. [Crofoot, Margaret C.] Princeton Univ, Dept Ecol & Evolut Biol, Princeton, NJ 08544 USA. RP Crofoot, MC (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama. EM crofootm@si.edu FU Frederik Sheldon Travel Grant; American Society of Primatologists Small Research Grant; Smithsonian Tropical Research Institute; Department of Biology at Armstrong Atlantic State University (Savannah, GA); Harvard University FX Grant sponsors: Frederik Sheldon Travel Grant; American Society of Primatologists Small Research Grant; Smithsonian Tropical Research Institute Short-term Fellowship; Sigma Xi Grant-in-Aid of Research, the Department of Biology at Armstrong Atlantic State University (Savannah, GA); Research Award from the Program in Biological Anthropology, Harvard University. NR 70 TC 8 Z9 8 U1 3 U2 33 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 SEP PY 2013 VL 152 IS 1 BP 79 EP 85 DI 10.1002/ajpa.22330 PG 7 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 297DB UT WOS:000330234400009 PM 23900797 ER PT J AU Dutta, T Sharma, S Maldonado, JE Wood, TC Panwar, HS Seidensticker, J AF Dutta, Trishna Sharma, Sandeep Maldonado, Jesus E. Wood, Thomas C. Panwar, Hemendra S. Seidensticker, John TI Gene flow and demographic history of leopards (Panthera pardus) in the central Indian highlands SO EVOLUTIONARY APPLICATIONS LA English DT Article DE effective population size; forest corridors; gene flow; India; leopards; metapopulation; noninvasive genetics ID EFFECTIVE POPULATION-SIZE; ALLELE FREQUENCY DATA; MAXIMUM-LIKELIHOOD-ESTIMATION; HUMAN-DOMINATED LANDSCAPES; LINKAGE DISEQUILIBRIUM; MIGRATION RATES; FRAGMENTED POPULATIONS; HABITAT FRAGMENTATION; NATURAL-POPULATIONS; MICROSATELLITE LOCI AB Gene flow is a critical ecological process that must be maintained in order to counteract the detrimental effects of genetic drift in subdivided populations, with conservation benefits ranging from promoting the persistence of small populations to spreading adaptive traits in changing environments. We evaluated historical and contemporary gene flow and effective population sizes of leopards in a landscape in central India using noninvasive sampling. Despite the dramatic changes in land-use patterns in this landscape through recent times, we did not detect any signs that the leopard populations have been through a genetic bottleneck, and they appear to have maintained migration-drift equilibrium. We found that historical levels of gene flow (mean m(h) = 0.07) were significantly higher than contemporary levels (mean m(c) = 0.03), and populations with large effective population sizes (Satpura and Kanha Tiger Reserves) are the larger exporters of migrants at both timescales. The greatest decline in historical versus contemporary gene flow is between pairs of reserves that are currently not connected by forest corridors (i.e., Melghat-Pench m(h) - m(c) = 0.063; and Kanha-Satpura m(h) - m(c) = 0.054). We attribute this reduction in gene flow to accelerated fragmentation and habitat alteration in the landscape over the past few centuries, and suggest protection of forest corridors to maintain gene flow in this landscape. C1 [Dutta, Trishna; Sharma, Sandeep; Maldonado, Jesus E.; Seidensticker, John] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20013 USA. [Dutta, Trishna; Sharma, Sandeep; Wood, Thomas C.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Panwar, Hemendra S.] Peace Inst Charitable Trust, Delhi, India. RP Dutta, T (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, POB 37012, Washington, DC 20013 USA. EM trishnad@gmail.com FU Smithsonian Conservation Biology Institute (SCBI); Friends of the National Zoo; George Mason University FX Funding was provided by Smithsonian Conservation Biology Institute (SCBI), Friends of the National Zoo, and George Mason University. We thank the Principal Chief Conservator of Forests (PCCF) Wildlife, Madhya Pradesh and Maharashtra, and field directors and staff of all five tiger reserves (Kanha, Satpura, Melghat, Pench MP, and Mh) and territorial divisions (Seoni, Chindwara, Balaghat, Harda, Mandla, Betul) for providing research permissions, facilitating field work, and logistical help. We thank Robert Fleischer, Center for Conservation and Evolutionary Genetics, SCBI, and Yogesh S. Shouche, National Center for Cell Sciences (NCCS), Pune, Maharashtra, India, for providing laboratory space and facilitating lab work. We thank Nancy Rotzel, Libby Dougan, and Hitendra Munot for logistical support and Susan Lumpkin for her comments and editorial help with the manuscript. We thank the three anonymous reviewers and associate editor for their suggestions that considerably improved the manuscript. NR 79 TC 11 Z9 12 U1 3 U2 47 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1752-4571 J9 EVOL APPL JI Evol. Appl. PD SEP PY 2013 VL 6 IS 6 BP 949 EP 959 DI 10.1111/eva.12078 PG 11 WC Evolutionary Biology SC Evolutionary Biology GA 296IH UT WOS:000330178000007 PM 24062803 ER PT J AU Canning-Clode, J Fofonoff, P McCann, L Carlton, JT Ruiz, G AF Canning-Clode, Joao Fofonoff, Paul McCann, Linda Carlton, James T. Ruiz, Gregory TI Marine invasions on a subtropical island: fouling studies and new records in a recent marina on Madeira Island (Eastern Atlantic Ocean) SO AQUATIC INVASIONS LA English DT Article DE biofouling; invasive species; Madeira; marinas; marine invasions; new records; non-indigenous species (NIS) ID COMMUNITIES; DISTURBANCE; WATERS; COAST; ASCIDIACEA; DIVERSITY; SUBSTRATE; FAUNA AB In recent years, several marine non-indigenous species (NIS) lists have been produced for many European countries but little is known about the diversity and distribution of fouling NIS in Portugal (mainland and islands). We conducted a six-year survey of a marina located on the south coast of Madeira island, Portugal to assess NIS diversity on the island, constituting the first NIS inventory for the archipelago. We found 16 NIS, of which 9 are new records. Both species richness and abundance changed during the course of colonization whether total, NIS, or native diversity were considered. The number of native species decreased with colonization while the number of NIS significantly increased. More importantly, we demonstrated that the number of NIS detections in the marina was correlated with increasing ship traffic over the years. C1 [Canning-Clode, Joao] Univ Azores, Ctr IMAR, Dept Oceanog & Fisheries UAz, PT-9901862 Horta, Azores, Portugal. [Canning-Clode, Joao] Univ Azores, Ctr IMAR, LARSyS Associated Lab, PT-9901862 Horta, Azores, Portugal. [Canning-Clode, Joao; Fofonoff, Paul; McCann, Linda; Ruiz, Gregory] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Canning-Clode, Joao] Univ Lisbon, Fac Sci, Ctr Oceanog, P-1699 Lisbon, Portugal. [Carlton, James T.] Williams Coll Myst Seaport, Mystic, CT USA. RP Canning-Clode, J (reprint author), Univ Azores, Ctr IMAR, Dept Oceanog & Fisheries UAz, Rua Prof Dr Frederico Machado 4, PT-9901862 Horta, Azores, Portugal. EM canning-clode@uac.pt; fofonoffp@si.edu; mccannl@si.edu; James.T.Carlton@williams.edu; ruizg@si.edu RI Canning Clode, Joao/G-5142-2011; OI Canning Clode, Joao/0000-0003-2143-6535; Ruiz, Gregory/0000-0003-2499-441X FU FCT [SFRH/BPD/75775/2011]; "LARSyS Associated Laboratory" through FCT/MCE project [PEst-OE/EEI/LA0009/2013] FX We thank Quinta do Lorde Marina for allowing us to perform this survey and particularly Catia Carvalho for logistic support. We thank Xavier Turon, Rolando Bastida-Zavala, Sara Ferreira, Ana Neto, Konstantinos Tsiamis, Joana Xavier, Francis Kerckhof and Peter Wirtz for species identifications. We thank three anonymous reviewers for helpful criticism and suggestions that significantly improved the early version of this manuscript. Joao Canning-Clode holds a FCT post-doctoral grant (SFRH/BPD/75775/2011). The service charges for this open access publication have been covered by "LARSyS Associated Laboratory" through FCT/MCE project PEst-OE/EEI/LA0009/2013. This is contribution number 20 from Marine Biology Station of Funchal. NR 43 TC 12 Z9 14 U1 1 U2 19 PU REGIONAL EURO-ASIAN BIOLOGICAL INVASIONS CENTRE-REABIC PI HELSINKI PA PL 3, HELSINKI, 00981, FINLAND SN 1798-6540 EI 1818-5487 J9 AQUAT INVASIONS JI Aquat. Invasions PD SEP PY 2013 VL 8 IS 3 BP 261 EP 270 DI 10.3391/ai.2013.8.3.02 PG 10 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 283XD UT WOS:000329279400002 ER PT J AU Freeman, AS Blakeslee, AMH Fowler, AE AF Freeman, Aaren S. Blakeslee, April M. H. Fowler, Amy E. TI Northward expansion of the rhizocephalan Loxothylacus panopaei (Gissler, 1884) in the northwest Atlantic SO AQUATIC INVASIONS LA English DT Article DE estuarine; Eurypanopeus depressus; invasion; Long Island Sound; marine; panopeid; parasite ID RHITHROPANOPEUS-HARRISII GOULD; DNA-SEQUENCE VARIATION; LIFE-CYCLE; PARASITE; RANGE; HOST; CIRRIPEDIA; XANTHIDAE; GENETICS; CRABS AB This report describes the first occurrence of the rhizocephalan Loxothylacus panopaei (Gissler, 1884) in North America, north of Virginia and the Chesapeake Bay. Of the panopeid mud crabs suitable for infection by L. panopaei (Panopeus herbstii, Rhithropanopeus harrisii, etc.), the parasite only infected Eurypanopeus depressus. In particular, L. panopaei disproportionately infected small E. depressus (20.5% of crabs with carapace width (CW) of 5-10 mm and 11.8% of crabs with 10-15 mm CW) but did not infect any crabs over 15 mm CW. Analysis of genetic data (COI sequences) suggests this Long Island Sound population could have derived from a range expansion from the mid-Atlantic, where the parasite is invasive. Given the parasite's disjunct distribution, human-mediated dispersal is the most likely vector for this northward range expansion. C1 [Freeman, Aaren S.] Adelphi Univ, Dept Biol, Garden City, NY 11530 USA. [Blakeslee, April M. H.] Long Isl Univ Post, Dept Biol, Brookville, NY 11548 USA. [Fowler, Amy E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Freeman, AS (reprint author), Adelphi Univ, Dept Biol, 1 South Ave, Garden City, NY 11530 USA. EM afreeman@adelphi.edu; April.Blakeslee@liu.edu; fowlera@si.edu FU Adelphi University; LIU FX Support for this work was provided by Adelphi University and LIU. M. Record and T. Corey assisted with surveys. J. Carlton assisted with species identification. S. Tettlebach provided invaluable input. We also thank the four anonymous reviewers that contributed substantially to the revisions of this manuscript. NR 26 TC 7 Z9 7 U1 2 U2 8 PU REGIONAL EURO-ASIAN BIOLOGICAL INVASIONS CENTRE-REABIC PI HELSINKI PA PL 3, HELSINKI, 00981, FINLAND SN 1798-6540 EI 1818-5487 J9 AQUAT INVASIONS JI Aquat. Invasions PD SEP PY 2013 VL 8 IS 3 BP 347 EP 353 DI 10.3391/ai.2013.8.3.11 PG 7 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 283XD UT WOS:000329279400011 ER PT J AU Collins, M AF Collins, Martin TI Untitled SO HISTORY AND TECHNOLOGY LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Collins, M (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 2 TC 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 SEP 1 PY 2013 VL 29 IS 3 SI SI BP 227 EP 228 DI 10.1080/07341512.2013.875757 PG 2 WC History SC History GA 272PC UT WOS:000328471700001 ER PT J AU Irsic, V Slosar, A Bailey, S Eisenstein, DJ Font-Ribera, A Le Goff, JM Lundgren, B McDonald, P O'Connell, R Palanque-Delabrouille, N Petitjean, P Rich, J Rossi, G Schneider, DP Sheldon, ES Yeche, C AF Irsic, Vid Slosar, Anze Bailey, Stephen Eisenstein, Daniel J. Font-Ribera, Andreu Le Goff, Jean-Marc Lundgren, Britt McDonald, Patrick O'Connell, Ross Palanque-Delabrouille, Nathalie Petitjean, Patrick Rich, Jim Rossi, Graziano Schneider, Donald P. Sheldon, Erin S. Yeche, Christophe TI Detection of Ly beta auto-correlations and Ly alpha-Ly beta cross-correlations in BOSS Data Release 9 SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE Lyman alpha forest; intergalactic media; dark energy experiments; cosmic web ID DIGITAL SKY SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; POWER SPECTRUM; SDSS-III; TRANSMITTED FLUX; TARGET SELECTION; FOREST; CONSTRAINTS; TELESCOPE; QUASARS AB The Lyman-beta forest refers to a region in the spectra of distant quasars that lies between the rest-frame Lyman-beta and Lyman-gamma emissions. The forest in this region is dominated by a combination of absorption due to resonant Ly alpha and Ly beta scattering. When considering the 1D Ly beta forest in addition to the 1D Lya forest, the full statistical description of the data requires four 1D power spectra: Lya and Ly beta auto-power spectra and the Ly alpha-Ly beta real and imaginary cross-power spectra. We describe how these can be measured using an optimal quadratic estimator that naturally disentangles Ly alpha and Ly beta contributions. Using a sample of approximately 60,000 quasar sight-lines from the BOSS Data Release 9, we make the measurement of the one-dimensional power spectrum of fluctuations due to the Ly beta resonant scattering. While we have not corrected our measurements for resolution damping of the power and other systematic effects carefully enough to use them for cosmological constraints, we can robustly conclude the following: i) Ly beta power spectrum and Ly alpha-Ly beta cross spectra are detected with high statistical significance; ii) the cross-correlation coefficient is approximate to 1 on large scales; iii) the Ly beta measurements are contaminated by the associated OVI absorption, which is analogous to the SiIII contamination of the Ly alpha forest. Measurements of the Ly beta forest will allow extension of the usable path-length for the Ly alpha measurements while allowing a better understanding of the physics of intergalactic medium and thus more robust cosmological constraints. C1 [Irsic, Vid] Univ Ljubljana, Fac Math & Phys, Ljubljana 1000, Slovenia. [Slosar, Anze; Sheldon, Erin S.] Brookhaven Natl Lab, Upton, NY 11375 USA. [Bailey, Stephen; Font-Ribera, Andreu; McDonald, Patrick] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Font-Ribera, Andreu] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland. [Le Goff, Jean-Marc; Palanque-Delabrouille, Nathalie; Rich, Jim; Rossi, Graziano; Yeche, Christophe] CEA, Ctr Saclay, IRFU, F-91191 Gif Sur Yvette, France. [Lundgren, Britt] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [O'Connell, Ross] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Petitjean, Patrick] Univ Paris 06, F-75014 Paris, France. [Petitjean, Patrick] Inst Astrophys Paris, CNRS, UMP7095, F-75014 Paris, France. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, Davey Lab 525, University Pk, PA 16802 USA. RP Irsic, V (reprint author), Univ Ljubljana, Fac Math & Phys, Jadranska 19, Ljubljana 1000, Slovenia. EM vid.irsic@fmf.uni-lj.si; anze@bnl.gov; stephenbailey@lbl.gov; deisenstein@cfa.harvard.edu; font@physik.uzh.ch; jmlegoff@cea.fr; lundgren@astro.wisc.ed; pvmcdonald@lbl.gov; rcoconne@andrew.cmu.edu; nathalie.palanque-delabrouille@cea.fr; ppetitje@iap.fr; james.rich@cea.fr; graziano.rossi@cea.fr; dps7@psu.edu; esheldon@bnl.gov; christophe.yeche@cea.fr OI Irsic, Vid/0000-0002-5445-461X FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http : //www.sdps3.org/. NR 43 TC 3 Z9 3 U1 0 U2 1 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 SEP PY 2013 IS 9 AR 016 DI 10.1088/1475-7516/2013/09/016 PG 22 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 250BU UT WOS:000326826000016 ER PT J AU Rodrigues, BHG Grindlay, JE Allen, B Hong, J Barthelmy, S Braga, J D'Amico, F Rothschild, RE AF Rodrigues, B. H. G. Grindlay, J. E. Allen, B. Hong, J. Barthelmy, S. Braga, J. D'Amico, F. Rothschild, R. E. TI The high resolution X-ray imaging detector planes for the MIRAX mission SO JOURNAL OF INSTRUMENTATION LA English DT Article DE Gamma detectors (scintillators, CZT, HPG, HgI etc); X-ray detectors and telescopes; Data analysis; Detector alignment and calibration methods (lasers, sources, particle-beams) AB The MIRAX X-ray observatory, the first Brazilian-led astrophysics space mission, is designed to perform an unprecedented wide-field, wide-band hard X-ray (5-200 keV) survey of Galactic X-ray transient sources. In the current configuration, MIRAX will carry a set of four coded-masks telescopes with high spatial resolution Cadmium Zinc Telluride (CZT) detector planes, each one consisting of an array of 64 closely tiled CZT pixelated detectors. Taken together, the four telescopes will have a total detection area of 959 cm(2), a large field of view (60 degrees x 60 degrees FWHM), high angular resolution for this energy range (6 arcmin) and very good spectral resolution (similar to 2 keV @ 60 keV). A stratospheric balloon-borne prototype of one of the MIRAX telescopes has been developed, tested and flown by the Harvard-Smithsonian Center for Astrophysics (CfA) as part of the ProtoEXIST program. In this paper we show results of validation and calibration tests with individual CZT detectors of the ProtoEXIST second generation experiment (P2). Each one of 64 detector units of the P2 detector plane consists of an ASIC, developed by Caltech for the NuSTAR telescope, hybridized to a CZT crystal with 0.6mm pixel size. The performance of each detector was evaluated using radioactive sources in the laboratory. The calibration results show that the P2 detectors have average energy resolution of similar to 2.1 keV @ 60 keV and 2.3 @ 122 keV. P2 was also successfully tested on near-space environment on a balloon flight, demonstrating the detector unit readiness for integration on a space mission telescope, as well as satisfying all MIRAX mission requirements. C1 [Rodrigues, B. H. G.; Braga, J.; D'Amico, F.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [Rodrigues, B. H. G.; Grindlay, J. E.; Allen, B.; Hong, J.] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. [Barthelmy, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rothschild, R. E.] Univ Calif San Diego, La Jolla, CA 92093 USA. RP Rodrigues, BHG (reprint author), Inst Nacl Pesquisas Espaciais, Av Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP, Brazil. EM barbara@das.inpe.br FU NASA [NNX09AD76G, NNX11AF35G]; CAPES FX We would like to thank MIRAX and ProtoEXIST technical teams for the great effort done for this mission development. Special thanks to J. Grindlay and CAPES for fellowship grants. Development of the ProtoEXIST program and P2 detector and telescope at Harvard is currently supported by NASA grants NNX09AD76G and NNX11AF35G. NR 15 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-0221 J9 J INSTRUM JI J. Instrum. PD SEP PY 2013 VL 8 AR P09010 DI 10.1088/1748-0221/8/09/P09010 PG 14 WC Instruments & Instrumentation SC Instruments & Instrumentation GA 248FL UT WOS:000326680200024 ER PT J AU Fine, S Shanks, T Green, P Kelly, BC Croom, SM Webster, RL Berger, E Chornock, R Burgett, WS Chambers, KC Kaiser, N Price, PA AF Fine, S. Shanks, T. Green, P. Kelly, B. C. Croom, S. M. Webster, R. L. Berger, E. Chornock, R. Burgett, W. S. Chambers, K. C. Kaiser, N. Price, P. A. TI Stacked reverberation mapping SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; quasars: emission lines; quasars: general; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; DIGITAL SKY SURVEY; LINE REGION SIZES; CENTRAL MASSES; DATA RELEASE; QUASARS; SELECTION; GALAXIES; SPECTRA AB Over the past 20 years reverberation mapping has proved one of the most successful techniques for studying the local (<1 pc) environment of supermassive black holes that drive active galactic nuclei. Key successes of reverberation mapping have been direct black hole mass estimates, the radius-luminosity relation for the H beta line and the calibration of single-epoch mass estimators commonly employed up to z similar to 7. However, observing constraints mean that few studies have been successful at z > 0.1, or for the more-luminous quasars that make up the majority of current spectroscopic samples, or for rest-frame ultraviolet emission lines available in optical spectra of z > 0.5 objects. Previously, we described a technique for stacking cross-correlations to obtain reverberation mapping results at high z. Here, we present the first results from a campaign designed for this purpose. We construct stacked cross-correlation functions for the C IV and Mg II lines and find a clear peak in both. We find that the peak in the Mg II correlation is at longer lags than C IV consistent with previous results at low redshift. For the C IV sample, we are able to bin by luminosity and find evidence for increasing lags for more-luminous objects. This C IV radius-luminosity relation is consistent with previous studies but with a fraction of the observational cost. C1 [Fine, S.] Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa. [Shanks, T.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Green, P.; Kelly, B. C.; Berger, E.; Chornock, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Croom, S. M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Burgett, W. S.; Chambers, K. C.; Kaiser, N.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Fine, S (reprint author), Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa. EM s.lb.fine@gmail.com OI Chambers, Kenneth /0000-0001-6965-7789 FU SKA South Africa; NRF; National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G] FX SF would like to acknowledge SKA South Africa and the NRF for their funding support. The data presented in this work came from the Pan-STARRS1 telescope and the Multiple Mirror Telescope. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its Participating Institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, and the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate. NR 26 TC 3 Z9 3 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP PY 2013 VL 434 IS 1 BP L16 EP L20 DI 10.1093/mnrasl/slt069 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 250SY UT WOS:000326875900004 ER PT J AU Kipping, DM AF Kipping, David M. TI Parametrizing the exoplanet eccentricity distribution with the Beta distribution SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; planets and satellites: general ID SINGLE-PLANET SYSTEMS; EFFICIENT AB It is suggested that the distribution of orbital eccentricities for extrasolar planets is well described by the Beta distribution. Several properties of the Beta distribution make it a powerful tool for this purpose. For example, the Beta distribution can reproduce a diverse range of probability density functions (PDFs) using just two shape parameters (a and b). We argue that this makes it ideal for serving as a parametric model in Bayesian comparative population analysis. The Beta distribution is also uniquely defined over the interval zero to unity, meaning that it can serve as a proper prior for eccentricity when analysing the observations of bound extrasolar planets. Using nested sampling, we find that the distribution of eccentricities for 396 exoplanets detected through radial velocity with high signal-to-noise is well described by a Beta distribution with parameters a = 0.867(-0.044)(+0.044) and b = 3.03(-0.16)(+0.17). The Beta distribution is shown to be 3.7 times more likely to represent the underlying distribution of exoplanet eccentricities than the next best model: a Rayleigh + exponential distribution. The same data are also used in an example population comparison utilizing the Beta distribution, where we find that the short- and long-period planets are described by distinct Beta distributions at a confidence of 11.6 sigma and display a signature consistent with the effects of tidal circularization. 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 Carl Sagan Fellowships FX DMK has been supported by the NASA Carl Sagan Fellowships. Thanks to Joel Hartman and Kevin Schlaufman for useful discussions in preparing this manuscript. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. NR 15 TC 52 Z9 52 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP PY 2013 VL 434 IS 1 BP L51 EP L55 DI 10.1093/mnrasl/slt075 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 250SY UT WOS:000326875900011 ER PT J AU Pau, S Wolkovich, EM Cook, BI Nytch, CJ Regetz, J Zimmerman, JK Wright, SJ AF Pau, Stephanie Wolkovich, Elizabeth M. Cook, Benjamin I. Nytch, Christopher J. Regetz, James Zimmerman, Jess K. Wright, S. Joseph TI Clouds and temperature drive dynamic changes in tropical flower production SO NATURE CLIMATE CHANGE LA English DT Article ID RAIN-FOREST TREE; AMAZON FOREST; DROUGHT; GROWTH; CLIMATE; PLANTS AB Tropical forests are incredibly dynamic, showing rapid and longer-term changes in growth, mortality and net primary productivity(1-3). Tropical species may be highly sensitive to temperature increases associated with climate change because of their narrow thermal tolerances. However, at the ecosystem scale the competing effects of temperature, light and precipitation on tropical forest productivity have been difficult to assess. Here we quantify cloudiness over the past several decades to investigate how clouds, together with temperature and precipitation, affect flower production in two contrasting tropical forests. Our results show that temperature, rather than clouds, is critically important to tropical forest flower production. Warmer temperatures increased flower production over seasonal, interannual and longer timescales, contrary to recent evidence that some tropical forests are already near their temperature threshold(4,5). Clouds were primarily important seasonally, and limited production in a seasonally dry forest but enhanced production in an ever-wet forest. A long-term increase in flower production at the seasonally dry forest is not driven by clouds and instead may be tied to increasing temperatures. These relationships show that tropical forest productivity, which is not widely thought to be controlled by temperature, is indeed sensitive to small temperature changes (1-4 degrees C) across multiple timescales. C1 [Pau, Stephanie] Florida State Univ, Dept Geog, Tallahassee, FL 32306 USA. [Pau, Stephanie; Regetz, James] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. [Wolkovich, Elizabeth M.] Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V6T 1Z4, Canada. [Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Cook, Benjamin I.] Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Nytch, Christopher J.; Zimmerman, Jess K.] Univ Puerto Rico, Inst Trop Ecosyst Studies, Rio Piedras, PR 00931 USA. [Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. RP Pau, S (reprint author), Florida State Univ, Dept Geog, Tallahassee, FL 32306 USA. EM spau@fsu.edu RI Cook, Benjamin/H-2265-2012; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU National Center for Ecological Analysis and Synthesis (NCEAS); NSF [EF-0553768, DEB-0639393, BSR-8811902, DEB-9411973, DEB-008538, DEB-0218039, DEB-0620910]; University of California, Santa Barbara; State of California; Environmental Sciences Program; Center for Tropical Forest Science of the Smithsonian Institution; NCEAS; NSERC CREATE training programme in biodiversity research FX We thank K. Knapp at NOAA NCDC for providing a beta version of the full GridSat data set, and D. K. Okamoto for input on statistical analyses, and are also grateful to H.G.B. This work was conducted as a part of the Forecasting Phenology Working Group supported by the National Center for Ecological Analysis and Synthesis (NCEAS), a Center funded by the NSF (Grant #EF-0553768), the University of California, Santa Barbara, and the State of California. The BCI portion of the study was supported by funds from the Environmental Sciences Program and the Center for Tropical Forest Science of the Smithsonian Institution. At Luquillo research was supported by NSF grant DEB-0639393 and by NSF funds (BSR-8811902, DEB-9411973, DEB-008538, DEB-0218039 and DEB-0620910) to the Luquillo Long-Term Ecological Research Program. S.P. was a Postdoctoral Associate supported by NCEAS. E.M.W. was supported by the NSERC CREATE training programme in biodiversity research. NR 30 TC 15 Z9 15 U1 7 U2 37 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 SEP PY 2013 VL 3 IS 9 BP 838 EP 842 DI 10.1038/NCLIMATE1934 PG 5 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 249YD UT WOS:000326816100024 ER PT J AU Corman, VM Rasche, A Diallo, TD Cottontail, VM Stocker, A Souza, BFDD Correa, JI Carneiro, AJB Franke, CR Nagy, M Metz, M Knornschild, M Kalko, EKV Ghanem, SJ Morales, KDS Salsamendi, E Spinola, M Herrler, G Voigt, CC Tschapka, M Drosten, C Drexler, JF AF Corman, Victor Max Rasche, Andrea Diallo, Thierno Diawo Cottontail, Veronika M. Stoecker, Andreas de Carvalho Dominguez Souza, Breno Frederico Correa, Jefferson Ivan Borges Carneiro, Aroldo Jose Franke, Carlos Roberto Nagy, Martina Metz, Markus Knoernschild, Mirjam Kalko, Elisabeth K. V. Ghanem, Simon J. Sibaja Morales, Karen D. Salsamendi, Egoitz Spinola, Manuel Herrler, Georg Voigt, Christian C. Tschapka, Marco Drosten, Christian Drexler, Jan Felix TI Highly diversified coronaviruses in neotropical bats SO JOURNAL OF GENERAL VIROLOGY LA English DT Article ID ACUTE-RESPIRATORY-SYNDROME; INFECTIOUS-DISEASES; DESMODUS-ROTUNDUS; EMERGING VIRUSES; VAMPIRE BATS; IDENTIFICATION; PREDATION; EMERGENCE; PATTERNS; BIODIVERSITY AB Bats host a broad diversity of coronaviruses (CoVs), including close relatives of human pathogens. There is only limited data on neotropical bat CoVs. We analysed faecal, blood and intestine specimens from 1562 bats sampled in Costa Rica, Panama, Ecuador and Brazil for CoVs by broad-range PCR. CoV RNA was detected in 50 bats representing nine different species, both frugivorous and insectivorous. These bat CoVs were unrelated to known human or animal pathogens, indicating an absence of recent zoonotic spill-over events. Based on RNA-dependent RNA polymerase (RdRp)-based grouping units (RGUs) as a surrogate for CoV species identification, the 50 viruses represented five different alphacoronavirus RGUs and two betacoronavirus RGUs. Closely related alphacoronaviruses were detected in Carollia perspicillata and C. brevicauda across a geographical distance exceeding 5600 km. Our study expands the knowledge on CoV diversity in neotropical bats and emphasizes the association of distinct CoVs and bat host genera. C1 [Corman, Victor Max; Rasche, Andrea; Diallo, Thierno Diawo; Drosten, Christian; Drexler, Jan Felix] Univ Bonn, Med Ctr, Inst Virol, Bonn, Germany. [Rasche, Andrea; Herrler, Georg] Univ Vet Med Hannover, Hannover, Germany. [Cottontail, Veronika M.; Knoernschild, Mirjam; Kalko, Elisabeth K. V.; Salsamendi, Egoitz; Tschapka, Marco] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Stoecker, Andreas; de Carvalho Dominguez Souza, Breno Frederico; Correa, Jefferson Ivan] Univ Fed Bahia, Univ Hosp Prof Edgard Santos, Infect Dis Res Lab, Salvador, BA, Brazil. [Borges Carneiro, Aroldo Jose; Franke, Carlos Roberto] Univ Fed Bahia, Sch Vet Med, Salvador, BA, Brazil. [Nagy, Martina] Leibniz Inst Res Evolut & Biodivers, Museum Nat Kunde, Berlin, Germany. [Metz, Markus] Fdn Edmund Mach, Res & Innovat Ctr, Dept Biodivers & Mol Ecol, San Michele All Adige, Italy. [Kalko, Elisabeth K. V.; Tschapka, Marco] Smithsonian Trop Res Inst, Balboa, Panama. [Ghanem, Simon J.; Voigt, Christian C.] Leibniz Inst Zoo & Wildlife Res, Berlin, Germany. [Sibaja Morales, Karen D.; Spinola, Manuel] Univ Nacl, Inst Int Conservac & Manejo de Vida Silvestre, Heredia, Costa Rica. [Salsamendi, Egoitz] Univ Basque Country, Dept Zool & Anim Cell Biol, Bilbao, The Basque Coun, Spain. RP Drosten, C (reprint author), Univ Bonn, Med Ctr, Inst Virol, Bonn, Germany. EM drosten@virology-bonn.de; drexler@virology-bonn.de RI Nagy, Martina/D-2636-2012; Knornschild, Mirjam/C-9401-2011; Metz, Markus/C-5471-2011; Drexler, Jan Felix/C-1004-2014; OI Metz, Markus/0000-0002-4038-8754; Corman, Victor Max/0000-0002-3605-0136 FU Foundation for Research Support of the State of Bahia, Brazil [SUS0038/2007]; European Union FP7 project European Management Platform for Emerging and Re-emerging Infectious Disease Entities [223498]; German Federal Ministry of Education and Research (BMBF) [01KI0116D, 01KI1005A, 01KI1005-B]; Deutsche Forschungsgemeinschaft (DFG) [SFB621, SFB587]; Smithsonian Tropical Research Institute (STRI); German National Academic Foundation; German Academic Exchange Service (DAAD); DFG [Vo890]; BONFOR intramural program at the University of Bonn FX This study was supported by a research grant from the Foundation for Research Support of the State of Bahia, Brazil (project code SUS0038/2007), the European Union FP7 project European Management Platform for Emerging and Re-emerging Infectious Disease Entities (contract number 223498) and the German Federal Ministry of Education and Research (BMBF) (grants 01KI0116D and 01KI1005A to C. D. and 01KI1005-B to G. H.), G. H. was additionally supported by Deutsche Forschungsgemeinschaft (DFG), (SFB621 and SFB587). Trust funds from the Smithsonian Tropical Research Institute (STRI) and a personal scholarship granted to V. M. Cottontail by the German National Academic Foundation contributed to field work in Panama). A personal scholarship granted to A. R. from the German Academic Exchange Service (DAAD) supported field work in Costa Rica and DFG support (Vo890) to C. C. V. contributed to field work in Ecuador. T. D. D. received a personal scholarship from the BONFOR intramural program at the University of Bonn. We would like to thank Tobias Bleicker, Sebastian Brunink, Monika Eschbach-Bludau, Adriana Fumie Tateno and Rodrigo Melim Zerbinati at the Institute of Virology, Bonn, for technical assistance and Leonardo Calderon Obaldia, Valeska Schugt and Veronika Zeus for field assistance. Fernando Felipe Teran Alvarado kindly provided his property for field work in Costa Rica. We are grateful to Comision Nacional para la Gestion de la Biodiversidad (CONAGEBIO), Servicio Nacional de Salud Animal (SENASA) and the Ministerio de Ambiente, Energia y Telecomunicaciones (MINAET) in Costa Rica, Autoridad Nacional del Ambiente (ANAM) in Panama, Ministerio de Agricultura, Ganaderia, Acuacultura y Pesca (MAGAP) in Ecuador and Instituto Brasileiro do Meio Ambiente e dos Recursos Naturals Renoviveis (IBAMA) and Instituto Chico Mendes de Conservacao da Biodiversidade (ICMBio) in Brazil for providing permits. NR 61 TC 11 Z9 11 U1 1 U2 24 PU SOC GENERAL MICROBIOLOGY PI READING PA MARLBOROUGH HOUSE, BASINGSTOKE RD, SPENCERS WOODS, READING RG7 1AG, BERKS, ENGLAND SN 0022-1317 EI 1465-2099 J9 J GEN VIROL JI J. Gen. Virol. PD SEP PY 2013 VL 94 BP 1984 EP 1994 DI 10.1099/vir.0.054841-0 PN 9 PG 11 WC Biotechnology & Applied Microbiology; Virology SC Biotechnology & Applied Microbiology; Virology GA 243GJ UT WOS:000326304600006 PM 23761408 ER PT J AU Woody, RC Schmidt, R AF Woody, Rachael Cristine Schmidt, Rich TI Following the Roots of Oregon Wine SO OREGON HISTORICAL QUARTERLY LA English DT Article C1 [Woody, Rachael Cristine] Linfield Coll, McMinnville, OR 97128 USA. [Woody, Rachael Cristine] Smithsonian Inst, Washigton, DC USA. [Woody, Rachael Cristine] Linfield Coll, Oregon Wine Hist Arch, McMinnville, OR USA. [Schmidt, Rich] Willamettes Hatfield Lib, Interlib Loans & Digitizat Dept, Hatfield, Herts, England. [Schmidt, Rich] Linfield, Resource Sharing, McMinnville, OR USA. RP Woody, RC (reprint author), Linfield Coll, McMinnville, OR 97128 USA. NR 22 TC 0 Z9 0 U1 0 U2 0 PU OREGON HISTORICAL SOC PI PORTLAND PA 1230 SW PARK AVE, PORTLAND, OR 97205 USA SN 0030-4727 J9 OREG HIST QUART JI Oregon Hist. Q. PD FAL PY 2013 VL 114 IS 3 BP 324 EP 339 DI 10.5403/oregonhistq.114.3.0324 PG 16 WC History SC History GA 241LV UT WOS:000326169300005 ER EF