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 distur